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108 results on '"Particle-acceleration"'

1. MAGIC upper limits on the GRB 090102 afterglow

Author: Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Satalecka, Konstanzja, Scapin, Valeria, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Satalecka, Konstanzja, and Scapin, Valeria
Abstract: © 2014 The Royal Astronomical Society. We would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPANCSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence 'Origin and Structure of the Universe', by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3 and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States; CEA/Irfu and IN2P3/CNRS in France; ASI and INFN in Italy; MEXT, KEK and JAXA in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. This research is partially supported by NASA through the Fermi Guest Investigator Grants NNX09AT92G and NNX10AP22G. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester., Indications of a GeV component in the emission from gamma-ray bursts (GRBs) are known since the Energetic Gamma-Ray Experiment Telescope observations during the 1990s and they have been confirmed by the data of the Fermi satellite. These results have, however, shown that our understanding of GRB physics is still unsatisfactory. The new generation of Cherenkov observatories and in particular the MAGIC telescope, allow for the first time the possibility to extend the measurement of GRBs from several tens up to hundreds of GeV energy range. Both leptonic and hadronic processes have been suggested to explain the possible GeV/TeV counterpart of GRBs. Observations with ground-based telescopes of very high energy (VHE) photons (E > 30 GeV) from these sources are going to play a key role in discriminating among the different proposed emission mechanisms, which are barely distinguishable at lower energies. MAGIC telescope observations of the GRB 090102 (z = 1.547) field and Fermi Large Area Telescope data in the same time interval are analysed to derive upper limits of the GeV/TeV emission. We compare these results to the expected emissions evaluated for different processes in the framework of a relativistic blastwave model for the afterglow. Simultaneous upper limits with Fermi and a Cherenkov telescope have been derived for this GRB observation. The results we obtained are compatible with the expected emission although the difficulties in predicting the HE and VHE emission for the afterglow of this event makes it difficult to draw firmer conclusions. Nonetheless, MAGIC sensitivity in the energy range of overlap with space-based instruments (above about 40 GeV) is about one order of magnitude better with respect to Fermi. This makes evident the constraining power of ground-based observations and shows that the MAGIC telescope has reached the required performance to make possible GRB multiwavelength studies in the VHE range., German BMBF, German MPG, Italian INFN, Swiss National Fund SNF, Spanish MICINN, Spanish Consolider-Ingenio programme, Bulgarian NSF, Academy of Finland, DFG Cluster of Excellence 'Origin and Structure of the Universe', DFG Collaborative Research Centers, Polish MNiSzW, NASA through the Fermi Guest Investigator, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2023

2. MAGIC observation of the GRB 080430 afterglow

Author: Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, Nieto, Daniel, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, and Nieto, Daniel
Abstract: © ESO 2010. We would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN and Spanish MICINN is gratefully acknowledged. This work was also supported by ETH Research Grant TH 34/043, by the Polish MNiSzW Grant N N203 390834, and by the YIP of the Helmholtz Gemeinschaft. We also thank Yizhong Fan for continuous theoretical support. Lorenzo Amati, Cristiano Guidorzi, Alessandra Galli, Daniele Malesani and Ruben Salvaterra for useful discussions. We finally remark the very constructive report from the referee which helped to substantially improve the paper., Context. Gamma-ray bursts are cosmological sources emitting radiation from the gamma-rays to the radio band. Substantial observational efforts have been devoted to the study of gamma-ray bursts during the prompt phase, i.e. the initial burst of high-energy radiation, and during the long-lasting afterglows. In spite of many successes in interpreting these phenomena, there are still several open key questions about the fundamental emission processes, their energetics and the environment. Aims. Independently of specific gamma-ray burst theoretical recipes, spectra in the GeV/TeV range are predicted to be remarkably simple, being satisfactorily modeled with power-laws, and therefore offer a very valuable tool to probe the extragalactic background light distribution. Furthermore, the simple detection of a component at very-high energies, i.e. at similar to 100GeV, would solve the ambiguity about the importance of various possible emission processes, which provide barely distinguishable scenarios at lower energies. Methods. We used the results of the MAGIC telescope observation of the moderate resdhift (z similar to 0.76) GRB 080430 at energies above about 80 GeV, to evaluate the perspective for late-afterglow observations with ground based GeV/TeV telescopes. Results. We obtained an upper limit of F(95% CL) = 5.5 x 10(-11) erg cm(-2) s(-1) for the very-high energy emission of GRB 080430, which cannot set further constraints on the theoretical scenarios proposed for this object also due to the difficulties in modeling the low-energy afterglow. Nonetheless, our observations show that Cherenkov telescopes have already reached the required sensitivity to detect the GeV/TeV emission of GRBs at moderate redshift (z less than or similar to 0.8), provided the observations are carried out at early times, close to the onset of their afterglow phase., German BMBF, German MPG, Italian INFN, Spanish MICINN, ETH, Polish MNiSzW, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2023

3. Discovery of VHE gamma-rays from the blazar 1ES 1215+303 with the MAGIC telescopes and simultaneous multi-wavelength observations

Author: Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Nieto, Daniel, Satalecka, Konstanzja, Scapin, Valeria, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Nieto, Daniel, Satalecka, Konstanzja, and Scapin, Valeria
Abstract: © ESO 2012. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the Marie Curie program, by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the YIP of the Helmholtz Gemeinschaft, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The Metsähovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Instituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Instituto Nazionale di Astrofisica in Italy and the Centre Nati, Context. We present the discovery of very high energy (VHE, E > 100 GeV) gamma-ray emission from the BL Lac object 1ES 1215+303 by the MAGIC telescopes and simultaneous multi-wavelength data in a broad energy range from radio to gamma-rays. Aims. We study the VHE gamma-ray emission from 1ES 1215+303 and its relation to the emissions in other wavelengths. Methods. Triggered by an optical outburst, MAGIC observed the source in 2011 January-February for 20.3 h. The target was monitored in the optical R-band by the KVA telescope that also performed optical polarization measurements. We triggered target of opportunity observations with the Swift satellite and obtained simultaneous and quasi-simultaneous data from the Fermi Large Area Telescope and from the Metsahovi radio telescope. We also present the analysis of older MAGIC data taken in 2010. Results. The MAGIC observations of 1ES 1215+303 carried out in 2011 January-February resulted in the first detection of the source at VHE with a statistical significance of 9.4 sigma. Simultaneously, the source was observed in a high optical and X-ray state. In 2010 the source was observed in a lower state in optical, X-ray, and VHE, while the GeV gamma-ray flux and the radio flux were comparable in 2010 and 2011. The spectral energy distribution obtained with the 2011 data can be modeled with a simple one zone SSC model, but it requires extreme values for the Doppler factor or the electron energy distribution., German BMBF, German MPG, Italian INFN, Swiss National Fund SNF, Spanish MICINN, Marie Curie program, CPAN project of the Spanish Consolider-Ingenio programme, MultiDark project of the Spanish Consolider-Ingenio programme, Bulgarian NSF, Academy of Finland, YIP of the Helmholtz Gemeinschaft, DFG Cluster of Excellence "Origin and Structure of the Universe", DFG Collaborative Research Centers, Polish MNiSzW grant, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2023

4. Observations of the Crab pulsar between 25 and 100 GeV with the MAGIC I telescope

Author: Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Satalecka, Konstanzja, Scapin, Valeria, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Satalecka, Konstanzja, and Scapin, Valeria
Abstract: © The American Astronomical Society. We thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the Marie Curie program, by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the YIP of the Helmholtz Gemeinschaft, by the DFG Cluster of Excellence "Origin and Structure of the Universe," by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. This work is also supported by the Formosa Program between National Science Council in Taiwan and Consejo Superior de Investigaciones Cientificas in Spain administered through grant number NSC100-2923-M-007-001-MY3. We acknowledge the use of public tools and data provided by the Fermi Science Support Center., We report on the observation of gamma-rays above 25 GeV from the Crab pulsar (PSR B0532+ 21) using the MAGIC I telescope. Two data sets from observations during the winter period 2007/2008 and 2008/2009 are used. In order to discuss the spectral shape from 100 MeV to 100 GeV, one year of public Fermi Large Area Telescope (Fermi-LAT) data are also analyzed to complement the MAGIC data. The extrapolation of the exponential cutoff spectrum determined with the Fermi-LAT data is inconsistent with MAGIC measurements, which requires a modification of the standard pulsar emission models. In the energy region between 25 and 100 GeV, the emission in the P1 phase (from -0.06 to 0.04, location of the main pulse) and the P2 phase (from 0.32 to 0.43, location of the interpulse) can be described by power laws with spectral indices of -3.1 +/- 1.0(stat) +/- 0.3(syst) and -3.5 +/- 0.5(stat) +/- 0.3(syst), respectively. Assuming an asymmetric Lorentzian for the pulse shape, the peak positions of the main pulse and the interpulse are estimated to be at phases -0.009 +/- 0.007 and 0.393 +/- 0.009, while the full widths at half- maximum are 0.025 +/- 0.008 and 0.053 +/- 0.015, respectively., BMBF, MPG, Italian INFN, Swiss National Fund SNF, Spanish MICINN, CPAN, Bulgarian NSF, Academy of Finland, YIP of the Helmholtz Gemeinschaft, DFG Cluster of Excellence "Origin and Structure of the Universe,", DFG Collaborative Research Centers, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2023

5. Insights into the high-energy gamma-ray emission of Markarian 501 from extensive multifrequency observations in the Fermi era

Author: Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, Nieto, Daniel, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, and Nieto, Daniel
Abstract: © The American Astronomical Society. Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation.Partially supported by the International Doctorate on Astroparticle Physics (IDAPP) program.Supported by INFN Padova.We acknowledge the use of public data from the Swift and RXTE data archive. The Metsahovi team acknowledges the support from the Academy of Finland to the observing projects (numbers 212656, 210338, among others). This research has made use of data obtained from the National Radio Astronomy Observatory's Very Long Baseline Array (VLBA), projects BK150, BP143, and MOJAVE. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. St. Petersburg University team acknowledges support from Russian RFBR foundation via grant 09-02-00092. AZT-24 observations are made within an agreement between Pulkovo, Rome and Teramo observatories. This research is partly based on observations with the 100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg, as well as with the Medicina and Noto telescopes operated by INAF-Istituto di Radioastronomia. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. M. Villata organized the optical-to-radio observations by GASP-WEBT as the president of the collaboration. Abastumani Observatory team acknowledges financial support by the Georgian National Science Foundation through grant GNSF/ST07/4-180. The OVRO 40 m program was funded in part by NASA (NNX08AW31G) and the NSF (AST-0808050)., We report on the gamma-ray activity of the blazar Mrk 501 during the first 480 days of Fermi operation. We find that the average Large Area Telescope (LAT) gamma-ray spectrum of Mrk 501 can be well described by a single power-law function with a photon index of 1.78 +/- 0.03. While we observe relatively mild flux variations with the Fermi-LAT (within less than a factor of two), we detect remarkable spectral variability where the hardest observed spectral index within the LAT energy range is 1.52 +/- 0.14, and the softest one is 2.51 +/- 0.20. These unexpected spectral changes do not correlate with the measured flux variations above 0.3 GeV. In this paper, we also present the first results from the 4.5 month long multifrequency campaign (2009 March 15-August 1) on Mrk 501, which included the Very Long Baseline Array (VLBA), Swift, RXTE, MAGIC, and VERITAS, the F-GAMMA, GASP-WEBT, and other collaborations and instruments which provided excellent temporal and energy coverage of the source throughout the entire campaign. The extensive radio to TeV data set from this campaign provides us with the most detailed spectral energy distribution yet collected for this source during its relatively low activity. The average spectral energy distribution of Mrk 501 is well described by the standard one-zone synchrotron self-Compton (SSC) model. In the framework of this model, we find that the dominant emission region is characterized by a size less than or similar to 0.1 pc (comparable within a factor of few to the size of the partially resolved VLBA core at 15-43 GHz), and that the total jet power (similar or equal to 10(44) erg s(-1)) constitutes only a small fraction (similar to 10(-3)) of the Eddington luminosity. The energy distribution of the freshly accelerated radiating electrons required to fit the time-averaged data has a broken power-law form in the energy range 0.3 GeV-10 TeV, with spectral indices 2.2 and 2.7 below and above the break energy of 20 GeV. We argue that su, K. A. Wallenberg Foundation, International Doctorate on Astroparticle Physics (IDAPP) program, INFN Padova, Academy of Finland, National Radio Astronomy Observatory's Very Long Baseline Array (VLBA), Russian RFBR foundation, Georgian National Science Foundation, NASA, NSF, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2023

6. Simultaneous multiwavelength observation of Mkn 501 in a low state in 2006

Author: Antoranz Canales, Pedro, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, Nieto, Daniel, Antoranz Canales, Pedro, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, and Nieto, Daniel
Abstract: © The American Astronomical Society. We thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, and Spanish MCINN is gratefully acknowledged. This work was also supported by ETH Research Grant TH 34/043, by the Polish MNiSzW Grant N N203 390834, by the YIP of the Helmholtz Gemeinschaft and by the U.S. Department of Energy contract to SLAC no. DEAC376SF00515., We present results of the multiwavelength campaign on the TeV blazar Mkn 501 performed in 2006 July, including MAGIC for the very-high-energy (VHE) gamma-ray band and Suzaku for the X-ray band. A VHE gamma-ray signal was clearly detected with an average flux above 200 GeV of similar to 20% of the Crab Nebula flux, which indicates a low state of source activity in this energy range. No significant variability has been found during the campaign. The VHE gamma-ray spectrum can be described by a simple power law from 80 GeV to 2 TeV with a photon index of 2.8 +/- 0.1, which corresponds to one of the steepest photon indices observed in this energy range so far for this object. The X-ray spectrum covers a wide range from 0.6 to 40 keV, and is well described by a broken power law, with photon indices of 2.257 +/- 0.004 and 2.420 +/- 0.012 below and above the break energy of 3.24(-0.12)(+0.13) keV. No apparent high-energy cut-off is seen above the break energy. Although an increase of the flux of about 50% is observed in the X-ray band within the observation, the data indicate a consistently low state of activity for this source. Time-resolved spectra show an evidence for spectral hardening with a flux level. A homogeneous one-zone synchrotron self-Compton (SSC) model can adequately describe the spectral energy distribution (SED) from the X-ray to the VHE gamma-ray bands with a magnetic field intensity B = 0.313 G and a Doppler beaming factor delta = 20, which are similar to the values in the past multiwavelength campaigns in high states. Based on our SSC parameters derived for the low state, we are able to reproduce the SED of the high state by just changing the Lorentz factor of the electrons corresponding to the break energy in the primary electron spectrum. This suggests that the variation of the injected electron population in the jet is responsible for the observed low-high state variation of the SED., ETH Research, Polish MNiSzW, Helmholtz Gemeinschaft, U.S. Department of Energy, German BMBF, Italian INFN, Spanish MCINN, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2023

7. Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes

Author: Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Satalecka, Konstanzja, Scapin, Valeria, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Satalecka, Konstanzja, and Scapin, Valeria
Abstract: © ESO. We would like to thank Felix Aharonian and Dmitry Khangulyan for useful discussions on the pulsar emission models. We would also like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de losMuchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MINECO is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0, by the Croatian Science Foundation (HrZZ) Project 09/186 and by the Formosa Program between National Science Council in Taiwan and Consejo Superior de Investigaciones Cientificas in Spain administered through grant number NSC100-2923-M-007-001-MY3., Context. The Crab pulsar is the only astronomical pulsed source detected at very high energy (VHE, E > 100 GeV) gamma rays. The emission mechanism of VHE pulsation is not yet fully understood, although several theoretical models have been proposed. Aims. In order to test new models, we measured the light curve and the spectra of the Crab pulsar with high precision by means of deep observations. Methods. We analyzed 135 h of selected MAGIC data taken between 2009 and 2013 in stereoscopic mode. In order to discuss the spectral shape in connection with lower energies, 5.5 years of Fermi-LAT data were also analyzed. Results. The known two pulses per period were detected with a significance of 8.0 sigma and 12.6 sigma. In addition, significant emission was found between the two pulses with 6.2 sigma. Conclusions. We discovered the bridge emission above 50 GeV between the two main pulses. This emission can not be explained with the existing theories. These data can be used for testing new theoretical models., German BMBF, German MPG, Italian INFN, Swiss National Fund SNF, Spanish MINECO, Spanish Consolider-Ingenio 2010, Bulgarian NSF, Academy of Finland, DFG Cluster of Excellence “Origin and Structure of the Universe”, DFG Collaborative Research Centers, Polish MNiSzW, Croatian Science Foundation (HrZZ), National Science Council in Taiwan, Consejo Superior de Investigaciones Cientificas in Spain, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2023

8. First NuSTAR observations of MRK 501 within a radio to TeV multi-instrument capaign

Author: Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Nievas Rosillo, Mireia, Satalecka, Konstanzja, Scapin, Valeria, Otros, ..., Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Nievas Rosillo, Mireia, Satalecka, Konstanzja, Scapin, Valeria, and Otros, ...
Abstract: © 2015. The American Astronomical Society. Artículo firmado por 278 autores. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The MAGIC Collaboration would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO, and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV- 2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. This research is also supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/ RFP/AST2748), and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the VERITAS instrument. The VERITAS Coll, We report on simultaneous broadband observations of the TeV-emitting blazar Markarian 501 between 2013 April 1 and August 10, including the first detailed characterization of the synchrotron peak with Swift and NuSTAR. During the campaign, the nearby BL Lac object was observed in both a quiescent and an elevated state. The broadband campaign includes observations with NuSTAR, MAGIC, VERITAS, the Fermi Large Area Telescope, Swift X-ray Telescope and UV Optical Telescope, various ground-based optical instruments, including the GASPWEBT program, as well as radio observations by OVRO, Metsähovi, and the F-Gamma consortium. Some of the MAGIC observations were affected by a sand layer from the Saharan desert, and had to be corrected using eventby-event corrections derived with a Light Detection and Ranging (LIDAR) facility. This is the first time that LIDAR information is used to produce a physics result with Cherenkov Telescope data taken during adverse atmospheric conditions, and hence sets a precedent for the current and future ground-based gamma-ray instruments. The NuSTAR instrument provides unprecedented sensitivity in hard X-rays, showing the source to display a spectral energy distribution (SED) between 3 and 79 keV consistent with a log-parabolic spectrum and hard X-ray variability on hour timescales. None (of the four extended NuSTAR observations) show evidence of the onset of inverse-Compton emission at hard X-ray energies. We apply a single-zone equilibrium synchrotron selfCompton (SSC) model to five simultaneous broadband SEDs. We find that the SSC model can reproduce the observed broadband states through a decrease in the magnetic field strength coinciding with an increase in the luminosity and hardness of the relativistic leptons responsible for the high-energy emission., Ministerio de Economía y Competitividad (MINECO), España, NASA, German BMBF and MPG, Italian INFN and INAF, Swiss National Fund SNF, Japanese JSPS and MEXT, Centro de Excelencia Severo Ochoa, Spanish Consolider-Ingenio 2010 programme, Academy of Finland, Croatian Science Foundation (HrZZ), University of Rijeka, DFG Collaborative Research Centers, Polish MNiSzW, U.S. Department of Energy Office of Science, U.S. National Science Foundation, Smithsonian Institution, NSERC in Canada, Science Foundation Ireland, STFC in the U.K, National Aeronautics and Space Administration and the Department of Energy in the United States, Commissariat à l’Energie Atomique in France, Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France, Agenzia Spaziale Italiana, Istituto Nazionale di Fisica Nucleare in Italy, Ministry of Education, Culture, Sports, Science and Technology (MEXT) in Japan, High Energy Accelerator Research Organization (KEK) in Japan, Japan Aerospace Exploration Agency (JAXA), K. A. Wallenberg Foundation the Swedish Research Council, Swedish National Space Board in Sweden, Istituto Nazionale di Astrofisica in Italy, Centre National d’Études Spatiales in France, INSU/CNRS (France), IGN (Spain), Istanbul University, Bilim Akademisi, TUBITAK, Russian RFBR, St. Petersburg University, NASA Fermi Guest Investigator, Swift Guest Investigator, Scientific Research Fund of the Bulgarian Ministry of Education and Sciences, Shota Rustaveli National Science Foundation, Institute of Astronomy and Rozhen National Astronomical Observatory, Bulgarian Academy of Sciences, Ministry of Education, Science and Technological Development of the Republic of Serbia, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2023

9. MAGIC TeV gamma-ray observations of Markarian 421 during multiwavelength campaigns in 2006

Author: Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, Nieto, Daniel, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, and Nieto, Daniel
Abstract: © ESO 2010. We thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN and Spanish MICINN is gratefully acknowledged. This work was also supported by ETH Research Grant TH 34/043, by the Polish MNiSzW Grant N N203 390834, and by the YIP of the Helmholtz Gemeinschaft., Context. Wide-range spectral coverage of blazar-type active galactic nuclei is of paramount importance for understanding the particle acceleration mechanisms assumed to take place in their jets. The Major Atmospheric Gamma Imaging Cerenkov (MAGIC) telescope participated in three multiwavelength (MWL) campaigns, observing the blazar Markarian (Mkn) 421 during the nights of April 28 and 29, 2006, and June 14, 2006. Aims. We analyzed the corresponding MAGIC very-high energy observations during 9 nights from April 22 to 30, 2006 and on June 14, 2006. We inferred light curves with sub-day resolution and night-by-night energy spectra. Methods. MAGIC detects gamma-rays by observing extended air showers in the atmosphere. The obtained air-shower images were analyzed using the standard MAGIC analysis chain. Results. A strong gamma-ray signal was detected from Mkn 421 on all observation nights. The flux (E > 250 GeV) varied on night-by-night basis between (0.92 +/- 0.11) x 10(-10) cm(-2) s(-1) (0.57 Crab units) and (3.21 +/- 0.15) x 10(-10) cm(-2) s(-1) (2.0 Crab units) in April 2006. There is a clear indication for intra-night variability with a doubling time of 36 +/- 10(stat) min on the night of April 29, 2006, establishing once more rapid flux variability for this object. For all individual nights gamma-ray spectra could be inferred, with power-law indices ranging from 1.66 to 2.47. We did not find statistically significant correlations between the spectral index and the flux state for individual nights. During the June 2006 campaign, a flux substantially lower than the one measured by the Whipple 10-m telescope four days later was found. Using a log-parabolic power law fit we deduced for some data sets the location of the spectral peak in the very-high energy regime. Our results confirm the indications of rising peak energy with increasing flux, as expected in leptonic acceleration models., German BMBF, German MPG, Italian INFN, Spanish MICINN, ETH, Polish MNiSzW, YIP of the Helmholtz Gemeinschaft, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2023

10. Exploring the physics behind the non-thermal emission from star-forming galaxies detected in gamma rays

Author: Kornecki, P., Peretti, E., del Palacio, S., Benaglia, P., Pellizza, L. J., Kornecki, P., Peretti, E., del Palacio, S., Benaglia, P., and Pellizza, L. J.
Abstract: Context. Star-forming galaxies emit non-thermal radiation from radio to gamma rays. Observations show that their radio and gamma-ray luminosities scale with their star formation rates, supporting the hypothesis that non-thermal radiation is emitted by cosmic rays produced by their stellar populations. However, the nature of the main cosmic-ray transport processes that shape the emission in these galaxies is still poorly understood, especially at low star formation rates.Aims. Our aim is to investigate the main mechanisms of global cosmic-ray transport and cooling in star-forming galaxies. The way they contribute to shaping the relations between non-thermal luminosities and star formation rates could shed light onto their nature, and allow us to quantify their relative importance at different star formation rates.Methods. We developed a model to compute the cosmic-ray populations of star-forming galaxies, taking into account their production, transport, and cooling. The model is parametrised only through global galaxy properties, and describes the non-thermal emission in radio (at 1.4 GHz and 150 MHz) and gamma rays (in the 0.1 100 GeV band). We focused on the role of diffusive and advective transport by galactic winds, either driven by turbulent or thermal instabilities. We compared model predictions to observations, for which we compiled a homogeneous set of luminosities in these radio bands, and updated those available in gamma rays.Results. Our model reproduces reasonably well the observed relations between the gamma-ray or 1.4 GHz radio luminosities and the star formation rate, assuming a single power-law scaling of the magnetic field (with index beta = 0:3) and winds blowing either at Alfvenic speeds (similar to tens of km s(-1), for less than or similar to 5 M-circle dot yr(-1)) or typical starburst wind velocities (similar to hundreds of km s(-1), for greater than or similar to 5 M-circle dot yr(-1)). Escape of cosmic rays is negligibl
Published: 2022

11. Investigation of the correlation patterns and the Compton dominance variability of Mrk 421 in 2017

Author: Katsuaki Asano, I. Jiménez, A. Fuentes, C. M. Raiteri, D. Dominis Prester, E. Molina, E. Colombo, Y. V. Troitskaya, Nikola Godinovic, Sidika Merve Colak, Jenni Jormanainen, Yuki Iwamura, Alessandra Lamastra, Lab Saha, Antoniya Valcheva, Sunay Ibryamov, Elena G. Larionova, B. De Lotto, Evgeni Ovcharov, D. Zarić, Kazuma Ishio, David A. Green, M. Villata, D. Horan, Givi N. Kimeridze, Alexander Hahn, S. Nozaki, M. Perri, Michael D. Joner, D. Neise, S. Loporchio, R. J. García López, Marcello Giroletti, Victor A. Acciari, V. Fallah Ramazani, Tomohiko Oka, Daniela Dorner, Narek Sahakyan, J. Kushida, M. Kopp, Lorenzo Bellizzi, Noah Biederbeck, Joseph Moody, M. Gaug, L. Schneider, A. López-Oramas, Daniel Morcuende, N. Rizzi, Jose Luis Contreras, G. Vanzo, Rodolfo Carosi, L. Maraschi, Andrés Baquero, M. I. Carnerero, R. Iotov, Mosè Mariotti, A. Paravac, John Hoang, Ashwani Pandey, Z. R. Weaver, Francesco Longo, F. D'Ammando, S. Paiano, Elina Lindfors, Moritz Hütten, J. Herrera, Koji Noda, Abelardo Moralejo, Laura Eisenberger, E. Moretti, Julian Sitarek, Marcos López-Moya, Wlodek Bednarek, L. Di Venere, Ashot Chilingarian, U. Barres de Almeida, Elisa Bernardini, I. Agudo, M. Feige, R. Z. Ivanidze, O. A. Merkulova, D. Depaoli, M. Spencer, Massimo Persic, J. van Scherpenberg, Pratik Majumdar, L. Kunkel, K. Nishijima, Stefano Ansoldi, Juan Cortina, Kai Phillip Schmidt, A. Berti, Riccardo Paoletti, Saverio Lombardi, Daniel Mazin, M. V. Fonseca, Damir Lelas, R. J. C. Vera, Sanae Inoue, Giacomo D'Amico, Dominik Baack, C. Perennes, A. A. Nikiforova, Yating Chai, Stefan Cikota, G. M. Madejski, A. Arbet Engels, Daniel Kerszberg, Manuel Artero, E. Do Souto Espiñeira, Tomislav Terzić, J. Becerra González, Martin Makariev, R. Mirzoyan, Yoshiki Ohtani, G. A. Borman, Pawel Gliwny, Jose Miguel Miranda, A. De Angelis, Vitaly Neustroev, Wara Chamani, Oscar Blanch, T. S. Grishina, Martin Will, M. Vazquez Acosta, Nicola Giglietto, L. V. Larionova, Lea Heckmann, Francesco Gabriele Saturni, Jorge Otero-Santos, R. A. Chigladze, M. Balbo, N. Marchili, D. Hadasch, P. G. Prada Moroni, A. A. Vasilyev, M. G. Nikolashvili, Jordi Delgado, V. Ramakrishnan, Christian Fruck, G. Busetto, Victoria Moreno, Luca Tosti, A. Rugliancich, C. Nigro, Marina Manganaro, Valeri M. Larionov, M. Balokovic, Manuel Delfino, A. Strigachev, J. M. Paredes, Manash R. Samal, Stefano Covino, I. Vovk, H. C. Lin, Ž. Bošnjak, Stefano Menchiari, Rumen Bachev, Marc Ribó, Dorota Sobczyńska, Carolin Wunderlich, Bernd Schleicher, M. Minev, Antonio Stamerra, Maria-Isabel Bernardos, I. S. Troitskiy, Merja Tornikoski, E. N. Kopatskaya, Shunsuke Sakurai, Camilla Maggio, Chiara Righi, F. Verrecchia, P. Temnikov, S. G. Jorstad, T. Schweizer, Hidetoshi Kubo, Lluis Font, A. Y. Lien, Toshiaki Inada, A. Scherbantin, Lorand A. Sigua, G. Maneva, Stefano Truzzi, B. Machado de Oliveira Fraga, V. Bozhilov, M. Palatiello, Alessandro Marchini, Chaitanya Priyadarshi, Alessia Spolon, Léa Jouvin, Konstancja Satalecka, Tomoki Saito, Giovanni Ceribella, Michele Doro, S. O. Kurtanidze, Carlo Vigorito, Pablo Peñil, D. Strom, Giacomo Bonnoli, Adrian Biland, Ana Babić, Alicia Fattorini, D. Hildebrand, Satoshi Fukami, G. Ferrara, Y. Kajiwara, Matteo Cerruti, P. Da Vela, Vassil Verguilov, Lovro Pavletić, C. Delgado Mendez, Emilia Järvelä, S. Mićanović, Sergey S. Savchenko, Ivica Puljak, M. Noethe, Simone Mender, Francesco Dazzi, V. Vitale, Manuela Mallamaci, Ivana Batković, F. Leone, M. I. Martínez, J. Rico, Alan P. Marscher, C. Lorey, S. Ventura, Tjark Miener, Anne Lähteenmäki, David Paneque, Masahiro Teshima, Jarred Gershon Green, Wrijupan Bhattacharyya, Kari Nilsson, R. Walter, M. Strzys, D. Reinhart, E. Zaharieva, Wen Ping Chen, Vitalii Sliusar, Jürgen Besenrieder, Francesco Giordano, Antonio Tutone, Thomas Bretz, J. Buss, Alok C. Gupta, Simona Righini, O. M. Kurtanidze, Ciro Bigongiari, O. Vince, D. Elsaesser, C. Leto, M. Garczarczyk, Sargis Gasparyan, J. Kania, Dario Hrupec, R. López-Coto, Wolfgang Rhode, I. Snidaric, D. A. Morozova, Vladimir A. Hagen-Thorn, Mitsunari Takahashi, J. A. Acosta-Pulido, E. Prandini, Marie Karjalainen, D. Miceli, Goran Damljanović, Evgeni Semkov, Alice Donini, L. A. Antonelli, J. A. Barrio, Y. Suda, D. Carosati, V. D'Elia, Fabrizio Tavecchio, A. C. Sadun, Tihomir Surić, C. Casadio, Karl Mannheim, Santiago Ubach, Y. Kobayashi, F. Di Pierro, European Commission, European Research Council, Ministerio de Ciencia e Innovación (España), Generalitat de Catalunya, Federal Ministry of Education and Research (Germany), German Research Foundation, Swiss National Science Foundation, Croatian Science Foundation, Ministry of Education, Science and Technological Development (Serbia), Bulgarian National Science Fund, National Aeronautics and Space Administration (US), Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Artero, M., Asano, K., Babi??, A., Baquero, A., Barres de Almeida, U., Barrio, J. A., Batkovi??, I., Becerra Gonz??lez, J., Bednarek, W., Bellizzi, L., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Blanch, O., Bo??njak, ??., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S. M., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D???amico, G., D???elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Delgado Mendez, C., Depaoli, D., Di Pierro, F., Di Venere, L., Do Souto Espi??eira, E., Dominis Prester, D., Donini, A., Doro, M., Fallah Ramazani, V., Fattorini, A., Ferrara, G., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., Garc??a L??pez, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinovi??, N., Green, J. G., Green, D., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., H??tten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jim??nez, I., Jormanainen, J., Jouvin, L., Kajiwara, Y., Karjalainen, M., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., L??pez-Coto, R., L??pez-Moya, M., L??pez-Oramas, A., Loporchio, S., Machado de Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Maraschi, L., Mariotti, M., Mart??nez, M., Mazin, D., Menchiari, S., Mender, S., Mi??anovi??, S., Miceli, D., Miener, T., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Neustroev, V., Nigro, C., Nilsson, K., Nishijima, K., Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavleti??, L., Pe??il, P., Perennes, C., Persic, M., Prada Moroni, P. G., Prandini, E., Priyadarshi, C., Puljak, I., Rib??, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Saturni, F. G., Schmidt, K., Schweizer, T., Sitarek, J., nidari??, I., Sobczynska, D., Spolon, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Suri??, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzi??, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Ventura, S., Verguilov, V., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Wunderlich, C., Zari??, D., Baack, D., Balbo, M., Biederbeck, N., Biland, A., Bretz, T., Buss, J., Dorner, D., Eisenberger, L., Elsaesser, D., Hildebrand, D., Iotov, R., Mannheim, K., Neise, D., Noethe, M., Paravac, A., Rhode, W., Schleicher, B., Sliusar, V., Walter, R., D???ammando, F., Horan, D., Lien, A. Y., Balokovi??, M., Madejski, G. M., Perri, M., Verrecchia, F., Leto, C., L??hteenm??ki, A., Tornikoski, M., Ramakrishnan, V., J??rvel??, E., Vera, R. J. C., Chamani, W., Villata, M., Raiteri, C. M., Gupta, A. C., Pandey, A., Fuentes, A., Agudo, I., Casadio, C., Semkov, E., Ibryamov, S., Marchini, A., Bachev, R., Strigachev, A., Ovcharov, E., Bozhilov, V., Valcheva, A., Zaharieva, E., Damljanovic, G., Vince, O., Larionov, V. M., Borman, G. A., Grishina, T. S., Hagen-Thorn, V. A., Kopatskaya, E. N., Larionova, E. G., Larionova, L. V., Morozova, D. A., Nikiforova, A. A., Savchenko, S. S., Troitskiy, I. S., Troitskaya, Y. V., Vasilyev, A. A., Merkulova, O. A., Chen, W. P., Samal, M., Lin, H. C., Moody, J. W., Sadun, A. C., Jorstad, S. G., Marscher, A. P., Weaver, Z. R., Feige, M., Kania, J., Kopp, M., Kunkel, L., Reinhart, D., Scherbantin, A., Schneider, L., Lorey, C., Acosta-Pulido, J. A., Carnerero, M. I., Carosati, D., Kurtanidze, S. O., Kurtanidze, O. M., Nikolashvili, M. G., Chigladze, R. A., Ivanidze, R. Z., Kimeridze, G. N., Sigua, L. A., Joner, M. D., Spencer, M., Giroletti, M., Marchili, N., Righini, S., Rizzi, N., Bonnoli, G., Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), MAGIC, FACT, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University
Subjects: electron, PARTICLE-ACCELERATION, ELECTRON ACCELERATION, Radiation mechanisms: non-thermal, RAY, VHE [gamma ray], galaxies: active, BL Lacertae objects: individual: Mrk 421, radiation mechanisms: non-thermal, Electron, Astrophysics, GeV, 01 natural sciences, 7. Clean energy, LARGE-AREA TELESCOPE, law.invention, OBSERVATIONS, law, ultraviolet, optical, MAGIC (telescope), correlation [flux], 010303 astronomy & astrophysics, X-ray: flux, model: leptonic, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), BL-LACERTAE, individual: Mrk 421 [BL Lacertae objects], flux [X-ray], Gamma ray, flux: correlation, Galaxies: active, non-thermal [radiation mechanisms], Synchrotron, SWIFT OBSERVATIONS, active [galaxies], Spectral energy distribution, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, Lorentz, Flare, LOG-PARABOLIC SPECTRA, ACTIVE GALACTIC NUCLEI, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, radiation, mechanisms: non-thermal, LIGHT CURVES, X-RAY, MULTIWAVELENGTH, GLAST, leptonic [model], blazar, 0103 physical sciences, TeV, Blazar, 010308 nuclear & particles physics, Astronomy and Astrophysics, MAGIC, gamma ray: VHE, Space and Planetary Science, ddc:520, spectral, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract: Full list of authors: Acciari, V. A.; Ansoldi, S.; Antonelli, L. A.; Arbet Engels, A.; Artero, M.; Asano, K.; Babić, A.; Baquero, A.; Barres de Almeida, U.; Barrio, J. A.; Batković, I.; Becerra González, J.; Bednarek, W.; Bellizzi, L.; Bernardini, E.; Bernardos, M.; Berti, A.; Besenrieder, J.; Bhattacharyya, W.; Bigongiari, C.; Blanch, O.; Bošnjak, Ž.; Busetto, G.; Carosi, R.; Ceribella, G.; Cerruti, M.; Chai, Y.; Chilingarian, A.; Cikota, S.; Colak, S. M.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; D'Amico, G.; D'Elia, V.; da Vela, P.; Dazzi, F.; de Angelis, A.; de Lotto, B.; Delfino, M.; Delgado, J.; Delgado Mendez, C.; Depaoli, D.; di Pierro, F.; di Venere, L.; Do Souto Espiñeira, E.; Dominis Prester, D.; Donini, A.; Doro, M.; Fallah Ramazani, V.; Fattorini, A.; Ferrara, G.; Fonseca, M. V.; Font, L.; Fruck, C.; Fukami, S.; García López, R. J.; Garczarczyk, M.; Gasparyan, S.; Gaug, M.; Giglietto, N.; Giordano, F.; Gliwny, P.; Godinović, N.; Green, J. G.; Green, D.; Hadasch, D.; Hahn, A.; Heckmann, L.; Herrera, J.; Hoang, J.; Hrupec, D.; Hütten, M.; Inada, T.; Inoue, S.; Ishio, K.; Iwamura, Y.; Jiménez, I.; Jormanainen, J.; Jouvin, L.; Kajiwara, Y.; Karjalainen, M.; Kerszberg, D.; Kobayashi, Y.; Kubo, H.; Kushida, J.; Lamastra, A.; Lelas, D.; Leone, F.; Lindfors, E.; Lombardi, S.; Longo, F.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Machado de Oliveira Fraga, B.; Maggio, C.; Majumdar, P.; Makariev, M.; Mallamaci, M.; Maneva, G.; Manganaro, M.; Maraschi, L.; Mariotti, M.; Martínez, M.; Mazin, D.; Menchiari, S.; Mender, S.; Mićanović, S.; Miceli, D.; Miener, T.; Minev, M.; Miranda, J. M.; Mirzoyan, R.; Molina, E.; Moralejo, A.; Morcuende, D.; Moreno, V.; Moretti, E.; Neustroev, V.; Nigro, C.; Nilsson, K.; Nishijima, K.; Noda, K.; Nozaki, S.; Ohtani, Y.; Oka, T.; Otero-Santos, J.; Paiano, S.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Pavletić, L.; Peñil, P.; Perennes, C.; Persic, M.; Prada Moroni, P. G.; Prandini, E.; Priyadarshi, C.; Puljak, I.; Ribó, M.; Rico, J.; Righi, C.; Rugliancich, A.; Saha, L.; Sahakyan, N.; Saito, T.; Sakurai, S.; Satalecka, K.; Saturni, F. G.; Schmidt, K.; Schweizer, T.; Sitarek, J.; Šnidarić, I.; Sobczynska, D.; Spolon, A.; Stamerra, A.; Strom, D.; Strzys, M.; Suda, Y.; Surić, T.; Takahashi, M.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Teshima, M.; Tosti, L.; Truzzi, S.; Tutone, A.; Ubach, S.; van Scherpenberg, J.; Vanzo, G.; Vazquez Acosta, M.; Ventura, S.; Verguilov, V.; Vigorito, C. F.; Vitale, V.; Vovk, I.; Will, M.; Wunderlich, C.; Zarić, D.; Baack, D.; Balbo, M.; Biederbeck, N.; Biland, A.; Bretz, T.; Buss, J.; Dorner, D.; Eisenberger, L.; Elsaesser, D.; Hildebrand, D.; Iotov, R.; Mannheim, K.; Neise, D.; Noethe, M.; Paravac, A.; Rhode, W.; Schleicher, B.; Sliusar, V.; Walter, R.; D'Ammando, F.; Horan, D.; Lien, A. Y.; Baloković, M.; Madejski, G. M.; Perri, M.; Verrecchia, F.; Leto, C.; Lähteenmäki, A.; Tornikoski, M.; Ramakrishnan, V.; Järvelä, E.; Vera, R. J. C.; Chamani, W.; Villata, M.; Raiteri, C. M.; Gupta, A. C.; Pandey, A.; Fuentes, A.; Agudo, I.; Casadio, C.; Semkov, E.; Ibryamov, S.; Marchini, A.; Bachev, R.; Strigachev, A.; Ovcharov, E.; Bozhilov, V.; Valcheva, A.; Zaharieva, E.; Damljanovic, G.; Vince, O.; Larionov, V. M.; Borman, G. A.; Grishina, T. S.; Hagen-Thorn, V. A.; Kopatskaya, E. N.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Nikiforova, A. A.; Savchenko, S. S.; Troitskiy, I. S.; Troitskaya, Y. V.; Vasilyev, A. A.; Merkulova, O. A.; Chen, W. P; Samal, M.; Lin, H. C.; Moody, J. W.; Sadun, A. C.; Jorstad, S. G.; Marscher, A. P.; Weaver, Z. R.; Feige, M.; Kania, J.; Kopp, M.; Kunkel, L.; Reinhart, D.; Scherbantin, A.; Schneider, L.; Lorey, C.; Acosta-Pulido, J. A.; Carnerero, M. I.; Carosati, D.; Kurtanidze, S. O.; Kurtanidze, O. M.; Nikolashvili, M. G.; Chigladze, R. A.; Ivanidze, R. Z.; Kimeridze, G. N.; Sigua, L. A.; Joner, M. D.; Spencer, M.; Giroletti, M.; Marchili, N.; Righini, S.; Rizzi, N.; Bonnoli, G.; MAGIC Collaboration; Fact Collaboration.-- This is an Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Aims. We present a detailed characterisation and theoretical interpretation of the broadband emission of the paradigmatic TeV blazar Mrk 421, with a special focus on the multi-band flux correlations. Methods. The dataset has been collected through an extensive multi-wavelength campaign organised between 2016 December and 2017 June. The instruments involved are MAGIC, FACT, Fermi-LAT, Swift, GASP-WEBT, OVRO, Medicina, and Metsahovi. Additionally, four deep exposures (several hours long) with simultaneous MAGIC and NuSTAR observations allowed a precise measurement of the falling segments of the two spectral components. Results. The very-high-energy (VHE; E 100 GeV) gamma rays and X-rays are positively correlated at zero time lag, but the strength and characteristics of the correlation change substantially across the various energy bands probed. The VHE versus X-ray fluxes follow dierent patterns, partly due to substantial changes in the Compton dominance for a few days without a simultaneous increase in the X-ray flux (i.e., orphan gamma-ray activity). Studying the broadband spectral energy distribution (SED) during the days including NuSTAR observations, we show that these changes can be explained within a one-zone leptonic model with a blob that increases its size over time. The peak frequency of the synchrotron bump varies by two orders of magnitude throughout the campaign. Our multi-band correlation study also hints at an anti-correlation between UV-optical and X-ray at a significance higher than 3. A VHE flare observed on MJD 57788 (2017 February 4) shows gamma-ray variability on multi-hour timescales, with a factor ten increase in the TeV flux but only a moderate increase in the keV flux. The related broadband SED is better described by a two-zone leptonic scenario rather than by a one-zone scenario.We find that the flare can be produced by the appearance of a compact second blob populated by high energetic electrons spanning a narrow range of Lorentz factors, from 0 min = 2104 to 0 max = 6105. © 2021 Georg Thieme Verlag. All rights reserved., The MAGIC Collaboration would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF, MPG and HGF; the Italian INFN and INAF; the Swiss National Fund SNF; the ERDF under the Spanish Ministerio de Ciencia e Innovación (MICINN) (FPA2017-87859-P, FPA2017-85668-P, FPA2017-82729-C6-5-R, FPA2017-90566-REDC, PID2019-104114RB-C31, PID2019-104114RB-C32, PID2019-105510GB-C31,PID2019-107847RB-C41, PID2019-107847RB-C42, PID2019-107847RB-C44, PID2019-107988GB-C22); the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-268/16.12.2019 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2016-0588, SEV-2017-0709 and CEX2019-000920-S, and “María de Maeztu” CEX2019-000918-M, the Unidad de Excelencia “María de Maeztu” MDM-2015-0509-18-2 and the “la Caixa” Foundation (fellowship LCF/BQ/PI18/11630012) and by the CERCA program of the Generalitat de Catalunya; by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02; by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3; the Polish National Research Centre grant UMO-2016/22/M/ST9/00382; and by the Brazilian MCTIC, CNPq and FAPERJ. The important contributions from ETH Zurich grants ETH-10.08-2 and ETH-27.12-1 as well as the funding by the Swiss SNF and the German BMBF (Verbundforschung Astro- und Astroteilchenphysik) and HAP (Helmoltz Alliance for Astroparticle Physics) are gratefully acknowledged. Part of this work is supported by Deutsche Forschungsgemeinschaft (DFG) within the Collaborative Research Center SFB 876 “Providing Information by Resource-Constrained Analysis”, project C3. We are thankful for the very valuable contributions from E. Lorenz, D. Renker and G. Viertel during the early phase of the project. We thank the Instituto de Astrofísica de Canarias for allowing us to operate the telescope at the Observatorio del Roque de los Muchachos in La Palma, the Max-Planck-Institut für Physik for providing us with the mount of the former HEGRA CT3 telescope, and the MAGIC collaboration for their support. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. This work performed in part under DOE Contract DE-AC02-76SF00515. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC; Italy) and the California Institute of Technology (USA). This research has also made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. A.A.E and D.P acknowledge support from the Deutsche Forschungs gemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy – EXC-2094 – 390783311. M. B. acknowledges support from the YCAA Prize Postdoctoral Fellowship and from the Black Hole Initiative at Harvard University, which is funded in part by the Gordon and Betty Moore Foundation (grant GBMF8273) and in part by the John Templeton Foundation. This publication makes use of data obtained at the Metsähovi Radio Observatory, operated by Aalto University in Finland. This research has made use of data from the OVRO 40-m monitoring program (Richards et al. 2011) which is supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G and NSF grants AST-0808050 and AST-1109911. I.A. acknowledges financial support from the Spanish “Ministerio de Ciencia e Innovación” (MCINN) through the “Center of Excellence Severo Ochoa” award for the Instituto de Astrofísica de Andalucía-CSIC (SEV-2017-0709). Acquisition and reduction of the MAPCAT data was supported in part by MICINN through grants AYA2016-80889-P and PID2019-107847RB-C44. The MAPCAT observations were carried out at the German-Spanish Calar Alto Observatory, which is jointly operated by Junta de Andalucía and Consejo Superior de Investigaciones Científicas. C.C. acknowledges support from the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program under the grant agreement No 771282. This research was partially supported by the Bulgarian National Science Fund of the Ministry of Education and Science under grants KP-06-H28/3 (2018), KP-06-H38/4 (2019) and KP-06-KITAJ/2 (2020). We acknowledge support by Bulgarian National Science Fund under grant DN18-10/2017 and National RI Roadmap Projects DO1-277/16.12.2019 and DO1-268/16.12.2019 of the Ministry of Education and Science of the Republic of Bulgaria. This research was supported by the Ministry of Education, Science and Technological Development of the Republic of Serbia (contract No 451-03-68/2020-14/200002). G.D. acknowledges observing grant support from the Institute of Astronomy and Rozhen NAO BAS through the bilateral joint research project “Gaia Celestial Reference Frame (CRF) and fast variable astronomical objects” (2020–2022, head – G. Damljanovic). The BU group was supported in part by NASA Fermi guest investigator program grants 80NSSC19K1505 and 80NSSC20K1566. This study was based in part on observations conducted using the 1.8 m Perkins Telescope Observatory (PTO) in Arizona, which is owned and operated by Boston University. This article is partly based on observations made with the LCOGT Telescopes, one of whose nodes is located at the Observatorios de Canarias del IAC on the island of Tenerife in the Observatorio del Teide. This article is also based partly on data obtained with the STELLA robotic telescopes in Tenerife, an AIP facility jointly operated by AIP and IAC. The Abastumani team acknowledges financial support by the Shota Rustaveli National Science Foundation under contract FR-19-6174. Based on observations with the Medicina telescope operated by INAF – Istituto di Radioastronomia.
Published: 2021

12. Investigation of the correlation patterns and the Compton dominance variability of Mrk 421 in 2017

Author: Baquero Larriva, Orlando Andrés, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Hoang, Kim Dinh, López Moya, Marcos, Miener, Tjark, Morcuende, D., Peñil del Campo, Pablo, Saha, Lab, otros, ..., Baquero Larriva, Orlando Andrés, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Hoang, Kim Dinh, López Moya, Marcos, Miener, Tjark, Morcuende, D., Peñil del Campo, Pablo, Saha, Lab, and otros, ...
Abstract: Artículo firmado por 275 autores. © MAGIC Collaboration et al. 2021. The journal referee is gratefully acknowledged for a constructive list of remarks that helped us improve the contents and clarity of the manuscript. The MAGIC Collaboration would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF, MPG and HGF; the Italian INFN and INAF; the Swiss National Fund SNF; the ERDF under the Spanish Ministerio de Ciencia e Innovacion (MICINN) (FPA2017-87859-P, FPA2017-85668-P, FPA2017-82729-C6-5-R, FPA2017-90566-REDC, PID2019-104114RB-C31, PID2019-104114RB-C32, PID2019-105510GB-C31,PID2019-107847RB-C41, PID2019-107847RB-C42, PID2019-107847RB-C44, PID2019-107988GB-C22); the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-268/16.12.2019 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2016-0588, SEV-2017-0709 and CEX2019-000920-S, and "Maria de Maeztu" CEX2019-000918-M, the Unidad de Excelencia "Maria de Maeztu" MDM-2015-0509-18-2 and the "la Caixa" Foundation (fellowship LCF/BQ/PI18/11630012) and by the CERCA program of the Generalitat de Catalunya; by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02; by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3; the Polish National Research Centre grant UMO-2016/22/M/ST9/00382; and by the Brazilian MCTIC, CNPq and FAPERJ. The important contributions from ETH Zurich grants ETH-10.082 and ETH-27.12-1 as well as the funding by the Swiss SNF and the German BMBF (Verbundforschung Astro-und Astroteilchenphysik) and HAP (Helmoltz Alliance for Astroparticle Physics) are gratefully acknowledged, Aims. We present a detailed characterisation and theoretical interpretation of the broadband emission of the paradigmatic TeV blazar Mrk 421, with a special focus on the multi-band flux correlations. Methods. The dataset has been collected through an extensive multi-wavelength campaign organised between 2016 December and 2017 June. The instruments involved are MAGIC, FACT, Fermi-LAT, Swift, GASP-WEBT, OVRO, Medicina, and Metsahovi. Additionally, four deep exposures (several hours long) with simultaneous MAGIC and NuSTAR observations allowed a precise measurement of the falling segments of the two spectral components. Results. The very-high-energy (VHE; E > 100 GeV) gamma rays and X-rays are positively correlated at zero time lag, but the strength and characteristics of the correlation change substantially across the various energy bands probed. The VHE versus X-ray fluxes follow different patterns, partly due to substantial changes in the Compton dominance for a few days without a simultaneous increase in the X-ray flux (i.e., orphan gamma-ray activity). Studying the broadband spectral energy distribution (SED) during the days including NuSTAR observations, we show that these changes can be explained within a one-zone leptonic model with a blob that increases its size over time. The peak frequency of the synchrotron bump varies by two orders of magnitude throughout the campaign. Our multi-band correlation study also hints at an anti-correlation between UV-optical and X-ray at a significance higher than 3 sigma. A VHE flare observed on MJD 57788 (2017 February 4) shows gamma-ray variability on multi-hour timescales, with a factor ten increase in the TeV flux but only a moderate increase in the keV flux. The related broadband SED is better described by a two-zone leptonic scenario rather than by a one-zone scenario. We find that the flare can be produced by the appearance of a compact second blob populated by high energetic electrons spanning a narrow range of Lorentz, Unión Europea. Horizonte 2020, Ministerio de Ciencia e Innovación (MICINN)/FEDER, Centro de Excelencia Severo Ochoa, Unidad de Excelencia María de Maeztu, German BMBF Federal Ministry of Education & Research, MPG Max Planck Society, HGF, Italian INFN Istituto Nazionale di Fisica Nucleare, INAF Istituto Nazionale Astrofisica, Swiss National Fund SNF Swiss National Science Foundation (SNSF), Indian Department of Atomic Energy, Japanese ICRR, JSPS Ministry of Education, Culture, Sports, Science and Technology, Japan, University of Tokyo, MEXT Ministry of Education, Culture, Sports, Science and Technology, Japan, Bulgarian Ministry of Education and Science, National RI Roadmap Project, Academy of Finland European Commission, Fundación La Caixa, CERCA program of the Generalitat de Catalunya, Croatian Science Foundation (HrZZ), University of Rijeka Project, DFG Collaborative Research Centers German Research Foundation (DFG), Polish National Research Centre, Brazilian MCTIC, CNPq Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ), FAPERJ Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ), ETH Zurich, Swiss SNF Swiss National Science Foundation (SNSF), German BMBF (Verbundforschung Astro-und Astroteilchenphysik) Federal Ministry of Education & Research (BMBF), HAP (Helmoltz Alliance for Astroparticle Physics), Deutsche Forschungsgemeinschaft (DFG) within the Collaborative Research Center German Research Foundation (DFG), MAGIC collaboration, DOE United States Department of Energy (DOE), National Aeronautics and Space Administration (NASA), Deutsche Forschungs gemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy, YCAA Prize Postdoctoral Fellowship, Black Hole Initiative at Harvard University, Gordon and Betty Moore Foundation, John Templeton Foundation, NASA National Aeronautics & Space Administration, Bulgarian National Science Fund of the Ministry of Education and Science, NSF National Science Foundation, Bulgarian National Science Fund, National RI Roadmap of the Ministry of Education and Science of the Republic of Bulgaria, Ministry of Education, Science and Technological Development of the Republic of Serbia, Institute of Astronomy and Rozhen NAO BAS through the bilateral joint research project "Gaia Celestial Reference Frame (CRF) and fast variable astronomical objects", NASA Fermi guest investigator program, Shota Rustaveli National Science Foundation, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2021

13. Study of the variable broadband emission of Markarian 501 during the most extreme Swift X-ray activity

Author: Barrio Uña, Juan Abel, Contreras González, José Luis, Domínguez Díaz, Alberto, Fidalgo, David Friedrich Carreto, Fonseca González, Mª Victoria, Hoang, Kim Dinh, Nievas Rosillo, Mireia, Peñil del Campo, Pablo, Saha, Lab, otros, ..., Barrio Uña, Juan Abel, Contreras González, José Luis, Domínguez Díaz, Alberto, Fidalgo, David Friedrich Carreto, Fonseca González, Mª Victoria, Hoang, Kim Dinh, Nievas Rosillo, Mireia, Peñil del Campo, Pablo, Saha, Lab, and otros, ...
Abstract: © ESO 2020. Artículo firmado por 185 autores. The authors thank the anonymous referee for providing a constructive list of remarks that allowed us to clarify and improve some of the results reported in the manuscript. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, FPA2017-90566-REDC), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia "María de Maeztu" MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA, Context. Markarian 501 (Mrk 501) is a very high-energy (VHE) gamma-ray blazar located at z=0.034, which is regularly monitored by a wide range of multi-wavelength instruments, from radio to VHE gamma rays. During a period of almost two weeks in July 2014, the highest X-ray activity of Mrk 501 was observed in similar to 14 years of operation of the Neil Gehrels Swift Gamma-ray Burst Observatory.Aims. We characterize the broadband variability of Mrk 501 from radio to VHE gamma rays during the most extreme X-ray activity measured in the last 14 years, and evaluate whether it can be interpreted within theoretical scenarios widely used to explain the broadband emission from blazars.Methods. The emission of Mrk 501 was measured at radio with Metsahovi, at optical-UV with KVA and Swift/UVOT, at X-ray with Swift/XRT and Swift/BAT, at gamma ray with Fermi-LAT, and at VHE gamma rays with the FACT and MAGIC telescopes. The multi-band variability and correlations were quantified, and the broadband spectral energy distributions (SEDs) were compared with predictions from theoretical models.Results. The VHE emission of Mrk 501 was found to be elevated during the X-ray outburst, with a gamma-ray flux above 0.15 TeV varying from similar to 0.5 to similar to 2 times the Crab nebula flux. The X-ray and VHE emission both varied on timescales of 1 day and were found to be correlated. We measured a general increase in the fractional variability with energy, with the VHE variability being twice as large as the X-ray variability. The temporal evolution of the most prominent and variable segments of the SED, characterized on a day-by-day basis from 2014 July 16 to 2014 July 31, is described with a one-zone synchrotron self-Compton model with variations in the break energy of the electron energy distribution (EED), and with some adjustments in the magnetic field strength and spectral shape of the EED. These results suggest that the main flux variations during this extreme X-ray outburst are, Ministerio de Economía y Competitividad (MINECO)/FEDER, Centro de Excelencia "Severo Ochoa", Unidad de Excelencia "María de Maeztu", German BMBF Federal Ministry of Education & Research (BMBF), German MPG, Italian INFN Istituto Nazionale di Fisica Nucleare (INFN), Italian INAF Istituto Nazionale Astrofisica (INAF), Swiss National Fund SNF Swiss National Science Foundation (SNSF), Japanese JSPS, Japanese MEXT, Croatian Science Foundation (HrZZ), University of Rijeka Project, DFG Collaborative Research Centers German Research Foundation (DFG), Polish National Research Centre, Brazilian MCTIC, Brazilian CNPq National Council for Scientific and Technological Development, Brazilian FAPERJ, ETH Zurich, German BMBF (Verbundforschung Astro- und Astroteilchenphysik), German HAP (Helmoltz Alliance for Astroparticle Physics), Deutsche Forschungsgemeinschaft (DFG) within the Collaborative Research Center German Research Foundation (DFG), Viera y Clavijo program - ACIISI, ULL, Project "Promotion inklusive" of the Universitat zu Koln, German Bundesministerium fur Arbeit und Soziales, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2020

14. A new lepto-hadronic model applied to the first simultaneous multiwavelength data set for Cygnus X-1

Author: Kantzas, D., Markoff, S., Beuchert, T., Lucchini, M., Chhotray, A., Ceccobello, C., Tetarenko, A.J., Miller-Jones, James, Bremer, M., Garcia, J.A., Grinberg, V., Uttley, P., Wilms, J., Kantzas, D., Markoff, S., Beuchert, T., Lucchini, M., Chhotray, A., Ceccobello, C., Tetarenko, A.J., Miller-Jones, James, Bremer, M., Garcia, J.A., Grinberg, V., Uttley, P., and Wilms, J.
Abstract: Cygnus X-1 is the first Galactic source confirmed to host an accreting black hole. It has been detected across the entire electromagnetic spectrum from radio to GeV gamma-rays. The source's radio through mid-infrared radiation is thought to originate from the relativistic jets. The observed high degree of linear polarization in the MeV X-rays suggests that the relativistic jets dominate in this regime as well, whereas a hot accretion flow dominates the soft X-ray band. The origin of the GeV non-thermal emission is still debated, with both leptonic and hadronic scenarios deemed to be viable. In this work, we present results from a new semi-analytical, multizone jet model applied to the broad-band spectral energy distribution of Cygnus X-1 for both leptonic and hadronic scenarios. We try to break this degeneracy by fitting the first-ever high-quality, simultaneous multiwavelength data set obtained from the CHOCBOX campaign (Cygnus X-1 Hard state Observations of a Complete Binary Orbit in X-rays). Our model parametrizes dynamical properties, such as the jet velocity profile, the magnetic field, and the energy density. Moreover, the model combines these dynamical properties with a self-consistent radiative transfer calculation including secondary cascades, both of leptonic and hadronic origin. We conclude that sensitive TeV gamma-ray telescopes like Cherenkov Telescope Array (CTA) will definitively answer the question of whether hadronic processes occur inside the relativistic jets of Cygnus X-1.
Published: 2020

15. Exploring the physics behind the non-thermal emission from star-forming galaxies detected in gamma rays

Author: P. Kornecki, Paula Benaglia, Leonardo J. Pellizza, S. del Palacio, and E. Peretti
Subjects: PARTICLE-ACCELERATION, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Electron, Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetohydrodynamic turbulence, COSMIC-RAY, ARP 220, 01 natural sciences, LARGE-AREA TELESCOPE, Radio spectrum, Luminosity, 0103 physical sciences, Diffusion (business), GALACTIC WINDS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), starburst [galaxies], 010308 nuclear & particles physics, Advection, STARBURST GALAXIES, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, galaxies [radio continuum], NGC 253, Galaxy, Interstellar medium, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies [gamma rays], INFRARED-RADIO CORRELATION, HIGH-ENERGY EMISSION, star formation [galaxies], Astrophysics - High Energy Astrophysical Phenomena, FREE-FREE ABSORPTION
Abstract: Star-forming galaxies (SFGs) emit non-thermal radiation from radio to gamma-rays. We aim to investigate the main mechanisms of global CR transport and cooling in SFGs. The way they contribute in shaping the relations between non-thermal luminosities and SFR could shed light onto their nature. We develop a model to compute the CR populations of SFGs, taking into account their production, transport, and cooling. The model is parameterised only through global galaxy properties, and describes the non-thermal emission in both radio and gamma-rays. We focus on the role of diffusive and advective transport by galactic winds, either driven by turbulent or thermal instabilities. We compare model predictions to observations, for which we compile a homogeneous set of luminosities in these radio bands, and update those available in gamma-rays. Our model reproduces reasonably well the observed relations between the gamma-ray or 1.4 GHz radio luminosities and the SFR, assuming a single power-law scaling of the magnetic field with the latter with index beta=0.3, and winds blowing either at Alfvenic speeds or typical starburst wind velocities. Escape of CR is negligible for > 30 Mo/yr. A constant ionisation fraction of the interstellar medium fails to reproduce the 150 MHz radio luminosity throughout the whole SFR range. Our results reinforce the idea that galaxies with high SFR are CR calorimeters, and that the main mechanism driving proton escape is diffusion, whereas electron escape also proceeds via wind advection. They also suggest that these winds should be CR or thermally-driven at low and intermediate SFR, respectively. Our results globally support that magnetohydrodynamic turbulence is responsible for the dependence of the magnetic field strength on the SFR and that the ionisation fraction is strongly disfavoured to be constant throughout the whole SFR range., Accepted for publication in Astronomy & Astrophysics (on 18/09/2021)
Published: 2021
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16. MeerKAT view of the diffuse radio sources in Abell 3667 and their interactions with the thermal plasma

Author: F. de Gasperin, L. Rudnick, A. Finoguenov, D. Wittor, H. Akamatsu, M. Brüggen, J. O. Chibueze, T. E. Clarke, W. Cotton, V. Cuciti, P. Domínguez-Fernández, K. Knowles, S. P. O’Sullivan, L. Sebokolodi, Department of Physics, and Doctoral Programme in Particle Physics and Universe Sciences
Subjects: PARTICLE-ACCELERATION, Cosmology and Nongalactic Astrophysics (astro-ph.CO), MAGNETOHYDRODYNAMIC SIMULATIONS, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 114 Physical sciences, radio continuum, MAGNETIC-FIELDS, galaxies, LARGE-SCALE STRUCTURE, MERGING CLUSTER, clusters, individual, intracluster medium, Astrophysics::Galaxy Astrophysics, XMM-NEWTON, Astronomy and Astrophysics, 115 Astronomy, Space science, general, Space and Planetary Science, 2 GALAXY CLUSTERS, COLD-FRONT, Abell 3667, PHOTON IMAGING CAMERA, INTERGALACTIC MEDIUM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: During their lifetime, galaxy clusters grow through the accretion of matter from the filaments of the large scale structure and from mergers with other clusters. These mergers release a large amount of energy into the intracluster medium (ICM) through merger shocks and turbulence. These phenomena are associated with the formation of radio sources known as radio relics and radio halos, respectively. Radio relics and halos are unique proxies to study the complex properties of these dynamically active regions of clusters and in general the micro physics of the ICM. Abell 3667 is a spectacular examples of a merging system hosting a large pair of radio relics. Due to its proximity (z=0.0553) and large mass, the system enables the study of these sources to a uniquely high level of detail. We observed Abell 3667 with MeerKAT as part of the MeerKAT Galaxy Cluster Legacy Survey. We used these data to study the large scale emission of the cluster, including its polarisation and spectral properties. We present the most detailed view of the radio relic system in Abell 3667 to date, with a resolution reaching 3 kpc. The relics are filled with a network of filaments with different spectral and polarisation properties that are likely associated with multiple regions of particle acceleration and local enhancements of the magnetic field. Conversely, the magnetic field in the space between filaments has strengths close to that expected in unperturbed regions at the same cluster-centric distance. Comparisons with MHD simulations supports the idea of filaments as multiple acceleration sites. Our observations also confirm the presence of an elongated radio halo, developed in the wake of the bullet-like sub-cluster that merged from the South-East. Finally, we associate the process of magnetic draping to a thin polarised radio source surrounding the remnant of the bullet's cool core., 28 pages, 30 figures, accepted A&A
Published: 2022

17. Ultra-steep spectrum emission in the merging galaxy cluster Abell 1914

Author: Mandal, S., Intema, Huib, Shimwell, T.W., Van Weeren, R.J., Botteon, A., Röttgering, H.J.A., Hoang, D.N., Brunetti, G., De Gasperin, F., Giacintucci, S., Hoekstra, H., Stroe, A., Brüggen, M., Cassano, R., Shulevski, A., Drabent, A., Rafferty, D., Mandal, S., Intema, Huib, Shimwell, T.W., Van Weeren, R.J., Botteon, A., Röttgering, H.J.A., Hoang, D.N., Brunetti, G., De Gasperin, F., Giacintucci, S., Hoekstra, H., Stroe, A., Brüggen, M., Cassano, R., Shulevski, A., Drabent, A., and Rafferty, D.
Abstract: A number of radio observations have revealed the presence of large synchrotron-emitting sources associated with the intra-cluster medium. There is strong observational evidence that the emitting particles have been (re-)accelerated by shocks and turbulence generated during merger events. The particles that are accelerated are thought to have higher initial energies than those in the thermal pool but the origin of such mildly relativistic particles remains uncertain and needs to be further investigated. The galaxy cluster Abell 1914 is a massive galaxy cluster in which X-ray observations show clear evidence of merging activity. We carried out radio observations of this cluster with the LOw Frequency ARay (LOFAR) at 150 MHz and the Giant Metrewave Radio Telescope (GMRT) at 610 MHz. We also analysed Very Large Array (VLA) 1.4 GHz data, archival GMRT 325 MHz data, CFHT weak lensing data and Chandra observations. Our analysis shows that the ultra-steep spectrum source (4C38.39; α -2), previously thought to be part of a radio halo, is a distinct source with properties that are consistent with revived fossil plasma sources. Finally, we detect some diffuse emission to the west of the source 4C38.39 that could belong to a radio halo.
Published: 2019

18. ALMA observations of A0620–00: Fresh clues on the nature of quiescent black hole X-ray binary jets

Author: Gallo, E., Teague, R., Plotkin, Richard, Miller-Jones, James, Russell, D.M., Dinçer, T., Bailyn, C., Maccarone, T.J., Markoff, S., Fender, R.P., Gallo, E., Teague, R., Plotkin, Richard, Miller-Jones, James, Russell, D.M., Dinçer, T., Bailyn, C., Maccarone, T.J., Markoff, S., and Fender, R.P.
Abstract: © 2019 The Author(s). We report on Atacama Large Millimeter Array (ALMA) continuum observations of the black hole X-ray binary A0620–00 at an X-ray luminosity nine orders of magnitude sub-Eddington. The system was significantly detected at 98 GHz (at 44 ± 7 μJy) and only marginally at 233 GHz (20 ± 8 μJy), about 40 d later. These results suggest either an optically thin sub-mm synchrotron spectrum, or highly variable sub-mm jet emission on month time-scales. Although the latter appears more likely, we note that, at the time of the ALMA observations, A0620–00 was in a somewhat less active optical-IR state than during all published multiwavelength campaigns when a flat-spectrum, partially self-absorbed jet has been suggested to extend from the radio to the mid-IR regime. Either interpretation is viable in the context of an internal shock model, where the jet’s spectral shape and variability are set by the power density spectrum of the shells’ Lorentz factor fluctuations. While strictly simultaneous radio–mm-IR observations are necessary to draw definitive conclusions for A0620–00, the data presented here, in combination with recent radio and sub-mm results from higher luminosity systems, demonstrate that jets from black hole X-ray binaries exhibit a high level of variability – either in flux density or intrinsic spectral shape, or both – across a wide spectrum of Eddington ratios. This is not in contrast with expectations from an internal shock model, where lower jet power systems can be expected to exhibit larger fractional variability owing to an overall decrease in synchrotron absorption.
Published: 2019

19. Radio observations of the merging galaxy cluster Abell 520

Author: Hoang, D.N., Shimwell, T.W., Van Weeren, R.J., Brunetti, G., Röttgering, H.J.A., Andrade-Santos, F., Botteon, A., Brüggen, M., Cassano, R., Drabent, A., De Gasperin, F., Hoeft, M., Intema, Huib, Rafferty, D.A., Shweta, A., Stroe, A., Hoang, D.N., Shimwell, T.W., Van Weeren, R.J., Brunetti, G., Röttgering, H.J.A., Andrade-Santos, F., Botteon, A., Brüggen, M., Cassano, R., Drabent, A., De Gasperin, F., Hoeft, M., Intema, Huib, Rafferty, D.A., Shweta, A., and Stroe, A.
Abstract: Context. Extended synchrotron radio sources are often observed in merging galaxy clusters. Studies of the extended emission help us to understand the mechanisms in which the radio emitting particles gain their relativistic energies. Aims. We examine the possible acceleration mechanisms of the relativistic particles that are responsible for the extended radio emission in the merging galaxy cluster Abell 520. Methods. We performed new 145 MHz observations with the LOw Frequency ARay (LOFAR) and combined these with archival Giant Metrewave Radio Telescope (GMRT) 323 MHz and Very Large Array (VLA) 1.5 GHz data to study the morphological and spectral properties of extended cluster emission. The observational properties are discussed in the framework of particle acceleration models associated with cluster merger turbulence and shocks. Results. In Abell 520, we confirm the presence of extended (760 × 950 kpc 2 ) synchrotron radio emission that has been classified as a radio halo. The comparison between the radio and X-ray brightness suggests that the halo might originate in a cocoon rather than from the central X-ray bright regions of the cluster. The halo spectrum is roughly uniform on the scale of 66 kpc. There is a hint of spectral steepening from the SW edge towards the cluster centre. Assuming diffusive shock acceleration (DSA), the radio data are suggestive of a shock Mach number of SW = 2.6-0.2 +0.3 that is consistent with the X-ray derived estimates. This is in agreement with the scenario in which relativistic electrons in the SW radio edge gain their energies at the shock front via acceleration of either thermal or fossil electrons. We do not detect extended radio emission ahead of the SW shock that is predicted if the emission is the result of adiabatic compression. An X-ray surface brightness discontinuity is detected towards the NE region that may be a counter shock of Mach number NE X = 1.52±0.05. This is lower than the value predicted from the radio emission
Published: 2019

20. Sensitivity of the KM3NeT/ARCA neutrino telescope to point-like neutrino sources

Author: T. Thakore, J. Zúñiga, Soebur Razzaque, C. De Sio, Antoine Kouchner, V. Bertin, Alessia Capone, Joao A B Coelho, A. Enzenhöfer, P.M. Kooijman, Alba Domi, D. Calvo, Silvia Celli, Stefano Ottonello, M. Colomer Molla, Salvatore Viola, R. Muller, S. R. Gozzini, D. Zaborov, Nhan Chau, C. Biernoth, A. Giuliante, H. Brânzaş, Thomas Eberl, M. Lotze, M. de Jong, A. Sharma, D. Stransky, Vladimir Kulikovskiy, Mario Musumeci, N. Randazzo, Dídac Diego-Tortosa, V. Popa, R. Bruijn, A. Martini, Vitaliano Chiarella, J. Manczak, Fabio Marzaioli, F. Raffaelli, L. K. Resvanis, P. de Jong, E. Buis, D. Stavropoulos, Steffen Hallmann, Gisela Anton, V. Sciacca, A. Rovelli, Abdelilah Moussa, M. Morganti, Sebastiano Aiello, J. Brunner, Michael Kreter, Francesca Tatone, Louis-Marie Rigalleau, Ofelia Pisanti, A. Sinopoulou, S.F. Biagi, E. A. De Wolf, Corinne Donzaud, G. Grella, L. Martin, E. Tenllado, E. Tzamariudaki, Paolo Fermani, S. Sánchez Navas, Alessandro Lonardo, M. Perrin-Terrin, Luigi Antonio Fusco, Timothée Grégoire, P. Coyle, Giulia Illuminati, Emanuele Leonora, Carlo Alessandro Nicolau, A. Orlando, Raffaele Buompane, Giacomo Cuttone, Piotr Kalaczyński, L. Quinn, I. Di Palma, C. Poirè, Antonio F. Díaz, P. Piattelli, D. Dornic, D. Kießling, V. Panagopoulos, C. Markou, Francesco Simeone, H. van Haren, Kay Graf, Karel Melis, G. Maggi, K. Pikounis, D. van Eijk, Giuseppina Larosa, H. Hamdaoui, Sara Pulvirenti, M. Ardid, Hassnae Eljarrari, Rosanna Cocimano, M. Organokov, M. Dörr, M. Jongen, Matthias Kadler, B. Ó Fearraigh, Fabio Longhitano, N. R. Khan Chowdhury, Mohamed Chabab, M. Circella, Robert Lahmann, J.J. Hernández-Rey, R. Le Breton, F. Versari, T. Gal, D. Lopez Coto, R. Mele, M. Saffer, C. Distefano, D. F. E. Samtleben, I. Salvadori, Andrea Biagioni, Yahya Tayalati, Giuseppe Levi, Simona Maria Stellacci, Jos Steijger, L. Nauta, A. Hekalo, P. Migliozzi, V. Van Elewyck, M. Bouta, T. Avgitas, M. Post, Antonio D'Onofrio, J. Seneca, C. Bagatelas, R. Donà, M. Taiuti, Tommaso Chiarusi, Miroslav Filipovic, Carlos Maximiliano Mollo, Rezo Shanidze, Annarita Margiotta, Diego Real, Riccardo Papaleo, J. Barrios-Martí, Richard Dallier, Thierry Pradier, Michel André, S.E. Akrame, G. Androulakis, J. Reubelt, T. Heid, Matteo Sanguineti, L. Maderer, G. Pühlhofer, A.M. van den Berg, Jörn Wilms, A. Trovato, G. Polydefki, Francesco Leone, Massimiliano Lincetto, A. Belias, D. Tzanetatos, Julien Aublin, Bruny Baret, Cristiano Bozza, Els Koffeman, G. Riccobene, T. Stüven, U. Katz, Daniele Vivolo, R. Coniglione, I. El Bojaddaini, Maurizio Spurio, M. Anghinolfi, J. Busto, G.E. Păvălaş, A.J. Heijboer, A. Garcia, L. S. Miranda, G. C. Barbarino, M. Durocher, Silvio Cherubini, Carmelo Pellegrino, F. Garufi, J. Hofestädt, Andrea Santangelo, E. Migneco, B. Spisso, M. Richer, E. Berbee, G. Ferrara, Jihad Boumaaza, I. Sgura, R. Gracia, J. Schumann, O. Kalekin, M. Bruchner, P. Mijakowski, M. Kunhikannan Kannichankandy, G. Papalashvili, Karl Mannheim, Lucio Gialanella, J.D. Zornoza, Domenico Santonocito, Michael Moser, E. G. Anassontzis, Dominik Elsaesser, C. Nielsen, A. Creusot, S. Bourret, B. Strandberg, C. W. James, A. Marinelli, A. Sánchez Losa, M.C. Bouwhuis, Paolo Sapienza, J.A. Martínez-Mora, Alexis Coleiro, Dario Grasso, Fabrizio Ameli, Emidio Giorgio, KM3NeT (IHEF, IoP, FNWI), ATLAS (IHEF, IoP, FNWI), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), KM3NeT, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Aiello, S, Akrame, Se, Ameli, F, Anassontzis, Eg, Andre, M, Androulakis, G, Anghinolfi, M, Anton, G, Ardid, M, Aublin, J, Avgitas, T, Bagatelas, C, Barbarino, G, Baret, B, Barrios-Marti, J, Belias, A, Berbee, E, van den Berg, A, Bertin, V, Biagi, S, Biagioni, A, Biernoth, C, Boumaaza, J, Bourret, S, Bouta, M, Bouwhuis, M, Bozza, C, Branzas, H, Bruchner, M, Bruijn, R, Brunner, J, Buis, E, Buompane, R, Busto, J, Calvo, D, Capone, A, Celli, S, Chabab, M, Chau, N, Cherubini, S, Chiarella, V, Chiarusi, T, Circella, M, Cocimano, R, Coelho, Jab, Coleiro, A, Molla, Mc, Coniglione, R, Coyle, P, Creusot, A, Cuttone, G, D'Onofrio, A, Dallier, R, De Sio, C, Di Palma, I, Diaz, Af, Diego-Tortosa, D, Distefano, C, Domi, A, Dona, R, Donzaud, C, Dornic, D, Dorr, M, Durocher, M, Eberl, T, van Eijk, D, El Bojaddaini, I, Eljarrari, H, Elsaesser, D, Enzenhofer, A, Fermani, P, Ferrara, G, Filipovic, Md, Fusco, La, Gal, T, Garcia, A, Garufi, F, Gialanella, L, Giorgio, E, Giuliante, A, Gozzini, Sr, Gracia, R, Graf, K, Grasso, D, Gregoire, T, Grella, G, Hallmann, S, Hamdaoui, H, van Haren, H, Heid, T, Heijboer, A, Hekalo, A, Hernandez-Rey, Jj, Hofestadt, J, Illuminati, G, James, Cw, Jongen, M, de Jong, M, de Jong, P, Kadler, M, Kalaczynski, P, Kalekin, O, Katz, Uf, Chowdhury, Nrk, Kiessling, D, Koffeman, En, Kooijman, P, Kouchner, A, Kreter, M, Kulikovskiy, V, Kannichankandy, Mk, Lahmann, R, Larosa, G, Le Breton, R, Leone, F, Leonora, E, Levi, G, Lincetto, M, Lonardo, A, Longhitano, F, Coto, Dl, Lotze, M, Maderer, L, Maggi, G, Manczak, J, Mannheim, K, Margiotta, A, Marinelli, A, Markou, C, Martin, L, Martinez-Mora, Ja, Martini, A, Marzaioli, F, Mele, R, Melis, Kw, Migliozzi, P, Migneco, E, Mijakowski, P, Miranda, L, Mollo, Cm, Morganti, M, Moser, M, Moussa, A, Muller, R, Musumeci, M, Nauta, L, Navas, S, Nicolau, Ca, Nielsen, C, Fearraigh, Bo, Organokov, M, Orlando, A, Ottonello, S, Panagopoulos, V, Papalashvili, G, Papaleo, R, Pavalas, Ge, Pellegrino, C, Perrin-Terrin, M, Piattelli, P, Pikounis, K, Pisanti, O, Poire, C, Polydefki, G, Popa, V, Post, M, Pradier, T, Puhlhofer, G, Pulvirenti, S, Quinn, L, Raffaelli, F, Randazzo, N, Razzaque, S, Real, D, Resvanis, L, Reubelt, J, Riccobene, G, Richer, M, Rigalleau, L, Rovelli, A, Saffer, M, Salvadori, I, Samtleben, Dfe, Losa, A, Sanguineti, M, Santangelo, A, Santonocito, D, Sapienza, P, Schumann, J, Sciacca, V, Seneca, J, Sgura, I, Shanidze, R, Sharma, A, Simeone, F, Sinopoulou, A, Spisso, B, Spurio, M, Stavropoulos, D, Steijger, J, Stellacci, Sm, Strandberg, B, Stransky, D, Stuven, T, Taiuti, M, Tatone, F, Tayalati, Y, Tenllado, E, Thakore, T, Trovato, A, Tzamariudaki, E, Tzanetatos, D, Van Elewyck, V, Versari, F, Viola, S, Vivolo, D, Wilms, J, de Wolf, E, Zaborov, D, Zornoza, Jd, Zuniga, J, Aiello, S., Akrame, S.E., Ameli, F., G. Anassontzis, E., Andre, M., Androulakis, G., Anghinolfi, M., Anton, G., Ardid, M., Aublin, J., Avgitas, T., Bagatelas, C., Barbarino, G., Baret, B., Barrios-Martí, J., Belias, A., Berbee, E., van den Berg, A., Bertin, V., Biagi, S., Biagioni, A., Biernoth, C., Boumaaza, J., Bourret, S., Bouta, M., Bouwhuis, M., Bozza, C., Brânzaş, H., Bruchner, M., Bruijn, R., Brunner, J., Buis, E., Buompane, R., Busto, J., Calvo, D., Capone, A., Celli, S., Chabab, M., Chau, N., Cherubini, S., Chiarella, V., Chiarusi, T., Circella, M., Cocimano, R., Coelho, J.A.B., Coleiro, A., Molla, M. Colomer, Coniglione, R., Coyle, P., Creusot, A., Cuttone, G., D'Onofrio, A., Dallier, R., De Sio, C., Di Palma, I., Díaz, A.F., Diego-Tortosa, D., Distefano, C., Domi, A., Donà, R., Donzaud, C., Dornic, D., Dörr, M., Durocher, M., Eberl, T., van Eijk, D., El Bojaddaini, I., Eljarrari, H., Elsaesser, D., Enzenhöfer, A., Fermani, P., Ferrara, G., D. Filipović, M., Fusco, L.A., Gal, T., Garcia, A., Garufi, F., Gialanella, L., Giorgio, E., Giuliante, A., Gozzini, S.R., Gracia, R., Graf, K., Grasso, D., Grégoire, T., Grella, G., Hallmann, S., Hamdaoui, H., van Haren, H., Heid, T., Heijboer, A., Hekalo, A., Hernández-Rey, J.J., Hofestädt, J., Illuminati, G., James, C.W., Jongen, M., de Jong, M., de Jong, P., Kadler, M., Kalaczyński, P., Kalekin, O., Katz, U.F., Khan Chowdhury, N.R., Kießling, D., Koffeman, E.N., Kooijman, P., Kouchner, A., Kreter, M., Kulikovskiy, V., Kunhikannan Kannichankandy, M., Lahmann, R., Larosa, G., Le Breton, R., Leone, F., Leonora, E., Levi, G., Lincetto, M., Lonardo, A., Longhitano, F., Lopez Coto, D., Lotze, M., Maderer, L., Maggi, G., Mańczak, J., Mannheim, K., Margiotta, A., Marinelli, A., Markou, C., Martin, L., Martínez-Mora, J.A., Martini, A., Marzaioli, F., Mele, R., Melis, K.W., Migliozzi, P., Migneco, E., Mijakowski, P., Miranda, L.S., Mollo, C.M., Morganti, M., Moser, M., Moussa, A., Muller, R., Musumeci, M., Nauta, L., Navas, S., Nicolau, C.A., Nielsen, C., Ó Fearraigh, B., Organokov, M., Orlando, A., Ottonello, S., Panagopoulos, V., Papalashvili, G., Papaleo, R., Păvălaş, G.E., Pellegrino, C., Perrin-Terrin, M., Piattelli, P., Pikounis, K., Pisanti, O., Poiré, C., Polydefki, G., Popa, V., Post, M., Pradier, T., Pühlhofer, G., Pulvirenti, S., Quinn, L., Raffaelli, F., Randazzo, N., Razzaque, S., Real, D., Resvanis, L., Reubelt, J., Riccobene, G., Richer, M., Rigalleau, L., Rovelli, A., Saffer, M., Salvadori, I., Samtleben, D.F.E., Sánchez Losa, A., Sanguineti, M., Santangelo, A., Santonocito, D., Sapienza, P., Schumann, J., Sciacca, V., Seneca, J., Sgura, I., Shanidze, R., Sharma, A., Simeone, F., Sinopoulou, A., Spisso, B., Spurio, M., Stavropoulos, D., Steijger, J., Stellacci, S.M., Strandberg, B., Stransky, D., Stüven, T., Taiuti, M., Tatone, F., Tayalati, Y., Tenllado, E., Thakore, T., Trovato, A., Tzamariudaki, E., Tzanetatos, D., Van Elewyck, V., Versari, F., Viola, S., Vivolo, D., Wilms, J., de Wolf, E., Zaborov, D., Zornoza, J.D., Zúñiga, J., Akrame, S. E., Barrios-Marti, J., VAN DEN BERG, Michiel, DI BIAGI, Paola, Branzas, H., Buompane, Angela, Coelho, J. A. B., Molla, M. C., Diaz, A. F., Distefano, Giuliana, Dona, R., Dorr, M., VAN EIJK, Ernst, Enzenhofer, A., Filipovic, Jelena, Fusco, L. A., Sambataro, GIOVANNI ANTONIO LUCA, Gozzini, S. R., Gregoire, T., Hernandez-Rey, J. J., Hofestadt, J., James, C. W., DE JONGE, KRISTA VIRGINIA, Kalaczynski, P., Katz, U. F., Khan Chowdhury, N. R., Kiessling, D., Koffeman, E. N., Levi, Donata, Manczak, J., Martinez-Mora, J. A., Melis, K. W., Miranda, L. S., Mollo, C. M., Nicolau, C. A., O Fearraigh, B., Pavalas, G. E., Piattelli, Adriano, Poire, C., Popa, CRISTINA MARIA, Puhlhofer, G., Pulvirenti, Emanuela, Samtleben, D. F. E., Sanchez Losa, A., SPURIO VENNARUCCI, Giacomo, Stellacci, S. M., Stuven, T., Tatone, Carla, Zornoza, J. D., Zuniga, J., Research unit Astroparticle Physics, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Ferrara, Giuseppina, and D. Filipovic, M.
Subjects: Astrofísica, PARTICLE-ACCELERATION, neutrino: energy: high, Flux, Astrophysics, telescope, 01 natural sciences, 7. Clean energy, neutrino: flux, neutrino, site, Cherenkov, gamma ray: flux, 010303 astronomy & astrophysics, KM3NeT, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysical neutrino source, astro-ph.HE, Astrophysics::Instrumentation and Methods for Astrophysics, COSMIC-RAYS, Supernova, neutrino: detector, Neutrino detector, GALACTIC SOURCES, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, REMNANT RX J1713.7-3946, sources, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysical neutrino sources, Astrophysics::High Energy Astrophysical Phenomena, SHELL, FOS: Physical sciences, Cosmic ray, underwater, ICECUBE, hadronic, Astrophysical, 0103 physical sciences, supernova, Neutrins, 14. Life underwater, Neutrinos, Cherenkov underwater neutrino telescope, 010308 nuclear & particles physics, resolution, Astronomy and Astrophysics, Galactic plane, sensitivity, Neutrino astrophysics, Galaxy, 13. Climate action, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], FISICA APLICADA, network, RADIATION, TEV, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: KM3NeT will be a network of deep-sea neutrino telescopes in the Mediterranean Sea. The KM3NeT/ARCA detector, to be installed at the Capo Passero site (Italy), is optimised for the detection of high-energy neutrinos of cosmic origin. Thanks to its geographical location on the Northern hemisphere, KM3NeT/ARCA can observe upgoing neutrinos from most of the Galactic Plane, including the Galactic Centre. Given its effective area and excellent pointing resolution, KM3NeT/ARCA will measure or significantly constrain the neutrino flux from potential astrophysical neutrino sources. At the same time, it will test flux predictions based on gamma-ray measurements and the assumption that the gamma-ray flux is of hadronic origin. Assuming this scenario, discovery potentials and sensitivities for a selected list of Galactic sources and to generic point sources with an $E^{-2}$ spectrum are presented. These spectra are assumed to be time independent. The results indicate that an observation with $3\sigma$ significance is possible in about six years of operation for the most intense sources, such as Supernovae Remnants RX\,J1713.7-3946 and Vela Jr. If no signal will be found during this time, the fraction of the gamma-ray flux coming from hadronic processes can be constrained to be below 50\% for these two objects., Comment: 32 pages, 9 figures, submitted to Astroparticle Physics
Published: 2019

21. Forbush decreases and <2 day GCR flux non-recurrent variations studied with LISA pathfinder

Author: N. Korsakova, Jacob Slutsky, Valerio Ferroni, D. Hoyland, Ian Harrison, Henri Inchauspe, Monica Laurenza, J. Grzymisch, Davor Mance, Ph. Jetzer, H. Ward, E. D. Fitzsimons, D. Texier, R. Giusteri, W. J. Weber, Gerhard Heinzel, Antoine Petiteau, Paul McNamara, Ignacio Mateos, Lluis Gesa, Ivan Lloro, Carlos F. Sopuerta, Rita Dolesi, D. I. Robertson, Martin Hewitson, Domenico Giardini, Daniel Hollington, J. Martino, J. P. López-Zaragoza, B. Kaune, M. Hueller, Daniele Vetrugno, J. A. Lobo, Michael Perreur-Lloyd, Ferran Gibert, R. Maarschalkerweerd, M. Born, Víctor S. Martín, L. Martin-Polo, James Ira Thorpe, P. Pivato, Luigi Ferraioli, A. Wittchen, Stefano Vitale, F. Rivas, M. Fabi, Gudrun Wanner, Juan Ramos-Castro, José F. F. Mendes, A. Cesarini, G. Russano, Heather Audley, Peter Wass, Eric Plagnol, Ingo Diepholz, N. Finetti, Karsten Danzmann, Pierre Binétruy, L. Wissel, Antonella Cavalleri, Peter Zweifel, Daniele Bortoluzzi, L. Mendes, J. Reiche, Miquel Nofrarías, J. Baird, Michele Armano, M. Freschi, S. Paczkowski, A. M. Cruise, N. Karnesis, Simone Benella, Mattia Villani, F. Martin-Porqueras, N. Meshksar, Daniele Telloni, Oliver Jennrich, Karel Kudela, T. J. Sumner, L. Liu, E. Castelli, M. de Deus Silva, Catia Grimani, Christian J. Killow, G. Dixon, Universitat Politècnica de Catalunya. Departament d'Enginyeria Electrònica, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: Ciències de la visió::Òptica física [Àrees temàtiques de la UPC], PARTICLE-ACCELERATION, solar–terrestrial relations, 010504 meteorology & atmospheric sciences, Energies::Energia solar fotovoltaica [Àrees temàtiques de la UPC], Flux, Astrophysics, Photovoltaic power generation, 01 natural sciences, 0305 Organic Chemistry, Heliosphere, Physics - Space Physics, Interferòmetres, instrumentation: interferometers, 010303 astronomy & astrophysics, Solar–terrestrial relations, Energia solar fotovoltaica, Physics, 0306 Physical Chemistry (incl. Structural), COROTATING INTERACTION REGIONS, heliosphere [Sun], Sun, solar-terrestrial relations, interferometers, interplanetary medium, Sun: heliosphere [cosmic rays, instrumentation], COSMIC-RAY PROTON, Astrophysics - Solar and Stellar Astrophysics, SOLAR-WIND, Physical Sciences, Lagrangian point, Astronomy & Astrophysics, Interferometers [Instrumentation], cosmic rays, 0103 physical sciences, 0201 Astronomical and Space Sciences, MODULATION, FIELD, Sun: heliosphere, Cosmic rays, 0105 earth and related environmental sciences, Geomagnetic storm, SPECTRUM, Science & Technology, Interferometers, Astronomy and Astrophysics, Plasma, Pathfinder, 13. Climate action, Space and Planetary Science, Heliospheric current sheet, Interplanetary spaceflight, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Intensity (heat transfer), Interplanetary medium, Astrophysics - Earth and Planetary Astrophysics
Abstract: International audience; Non-recurrent short-term variations of the galactic cosmic-ray (GCR) flux above 70 MeV n−1 were observed between 2016 February 18 and 2017 July 3 on board the European Space Agency LISA Pathfinder (LPF) mission orbiting around the Lagrange point L1 at 1.5 × 106 km from Earth. The energy dependence of three Forbush decreases is studied and reported here. A comparison of these observations with others carried out in space down to the energy of a few tens of MeV n−1 shows that the same GCR flux parameterization applies to events of different intensity during the main phase. FD observations in L1 with LPF and geomagnetic storm occurrence are also presented. Finally, the characteristics of GCR flux non-recurrent variations (peaks and depressions) of duration
Published: 2019

22. Interplanetary spread of solar energetic protons near a high-speed solar wind stream

Author: Angels Aran, Stefaan Poedts, Jens Pomoell, Nicolas Wijsen, and Department of Physics
Subjects: IONS, Shock wave, PARTICLE-ACCELERATION, 010504 meteorology & atmospheric sciences, Field line, FOS: Physical sciences, PROPAGATION, Astrophysics, FOCUSED TRANSPORT, 01 natural sciences, Physics - Space Physics, Sun: particle emission, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Sun: magnetic fields, 010303 astronomy & astrophysics, acceleration of particles, 0105 earth and related environmental sciences, Physics, Astronomy and Astrophysics, 115 Astronomy, Space science, Space Physics (physics.space-ph), Computational physics, Particle acceleration, Solar wind, solar wind, Deflection (physics), Space and Planetary Science, Physics::Space Physics, Particle, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight, Heliosphere
Abstract: We study how a high-speed solar wind stream embedded in a slow solar wind influences the spread of solar energetic protons in interplanetary space. To model the energetic protons, we used a recently developed particle transport code that computes particle distributions in the heliosphere by solving the focused transport equation in a stochastic manner. The particles are propagated in a solar wind containing a CIR, which was generated by the heliospheric magnetohydrodynamic model, EUHFORIA. We study four cases in which we assume a delta injection of 4 MeV protons spread uniformly over different regions at the inner boundary of the model. These source regions have the same size and shape, yet are shifted in longitude from each other, and are therefore magnetically connected to different solar wind conditions. The intensity and anisotropy profiles along selected IMF lines vary strongly according to the different solar wind conditions encountered along the field line. The IMF lines crossing the shocks bounding the CIR show the formation of accelerated particle populations, with the reverse shock wave being a more efficient accelerator than the forward shock wave. Moreover, we demonstrate that the longitudinal width of the particle intensity distribution can increase, decrease, or remain constant with heliographic radial distance, reflecting the underlying IMF structure. Finally, we show how the deflection of the IMF at the shock waves and the compression of the IMF in the CIR deforms the three-dimensional shape of the particle distribution in such a way that the original shape of the injection profile is lost., 12 pages, 8 figures
Published: 2019

23. Investigation of two Fermi-LAT gamma-ray blazars coincident with high-energy neutrinos detected by IceCube

Author: Collaboration, F. -L., Collaboration, A. -S., Collaboration, I., Garrappa, S., Buson, S., Franckowiak, A., Shappee, B. J., Beacom, J. F., Dong, S., Holoien, T. W. -S., Kochanek, C. S., Prieto, J. L., Stanek, K. Z., Thompson, T. A., Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Alispach, C., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Arguelles, C., Auffenberg, J., Axani, S., Backes, P., Bagherpour, H., Bai, X., Barbano, A., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Becker, K. -H., Tjus, J. B., Benzvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Borner, M., Boser, S., Botner, O., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Bretz, H. -P., Bron, S., Brostean-Kaiser, J., Burgman, A., Busse, R. S., Carver, T., Chen, C., Cheung, E., Chirkin, D., Clark, K., Classen, L., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., De Andre, J. P. A. M., Clercq, C. D., Delaunay, J. J., Dembinski, H., Deoskar, K., Ridder, S. D., Desiati, P., Vries, K. D. D., Wasseige, G. D., With, M. D., Deyoung, T., Diaz, A., Diaz-Velez, J. C., Dujmovic, H., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Friedman, E., Fritz, A., Gaisser, T. K., Gallagher, J., Ganster, E., Gerhardt, L., Ghorbani, K., Glauch, T., Glusenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Griffith, Z., Gunder, M., Gunduz, M., Haack, C., Hallgren, A., Halve, L., Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Henningsen, F., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., Hunnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karl, M., Karle, A., Katz, U., Kauer, M., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Kopke, L., Kopper, C., Kopper, S., Koskinen, D. J., Kowalski, M., Krings, K., Kruckl, G., Kulacz, N., Kunwar, S., Kurahashi, N., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Lazar, J. P., Leonard, K., Leuermann, M., Liu, Q. R., Lohfink, E., Mariscal, C. J. L., Lu, L., Lucarelli, F., Lunemann, J., Luszczak, W., Madsen, J., Maggi, G., Mahn, K. B. M., Makino, Y., Mallot, K., Mancina, S., Maris, I. C., Maruyama, R., Mase, K., Maunu, R., Meagher, K., Medici, M., Medina, A., Meier, M., Meighen-Berger, S., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Momente, G., Montaruli, T., Moore, R. W., Moulai, M., Nagai, R., Nahnhauer, R., Nakarmi, P., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Pollmann, A. O., Olivas, A., O'Murchadha, A., O'Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Park, N., Peiffer, P., De Los Heros, C. P., Pieloth, D., Pinat, E., Pizzuto, A., Plum, M., Price, P. B., Przybylski, G. T., Raab, C., Raissi, A., Rameez, M., Rauch, L., Rawlins, K., Rea, I. C., Reimann, R., Relethford, B., Renzi, G., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Safa, I., Herrera, S. E. S., Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Schaufel, M., Schlunder, P., Schmidt, T., Schneider, A., Schneider, J., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Silva, M., Snihur, R., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stasik, A., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stossl, A., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Sutherland, M., Taboada, I., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Tomankova, L., Tonnis, C., Toscano, S., Tosi, D., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Ty, B., Unger, E., Elorrieta, M. A. U., Usner, M., Vandenbroucke, J., Driessche, W. V., Eijk, D. V., Eijndhoven, N. V., Vanheule, S., Santen, J. V., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandkowsky, N., Watson, T. B., Weaver, C., Weiss, M. J., Weldert, J., Wendt, C., Werthebach, J., Westerhoff, S., Whelan, B. J., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, J., Wood, T. R., Woschnagg, K., Wrede, G., D. L., Xu, X. W., Xu, Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Yuan, T., Physics, Faculty of Sciences and Bioengineering Sciences, Vriendenkring VUB, and Elementary Particle Physics
Subjects: SELECTION, PARTICLE-ACCELERATION, SAMPLE, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, M87, FOS: Physical sciences, Flux, Astrophysics, 01 natural sciences, Coincidence, law.invention, HADRONIC MODEL, law, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, COSMIC cancer database, Gamma ray, COUNTERPARTS, Astronomy and Astrophysics, COSMIC-RAYS, CATALOG, QUASARS, Physics and Astronomy, Space and Planetary Science, Physique des particules élémentaires, ddc:520, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope, Flare
Abstract: After the identification of the gamma-ray blazar TXS 0506+056 as the first compelling IceCube neutrino source candidate, we perform a systematic analysis of all high-energy neutrino events satisfying the IceCube realtime trigger criteria. We find one additional known gamma-ray source, the blazar GB6 J1040+0617, in spatial coincidence with a neutrino in this sample. The chance probability of this coincidence is 30% after trial correction. For the first time, we present a systematic study of the gamma-ray flux, spectral and optical variability, and multiwavelength behavior of GB6 J1040+0617 and compare it to TXS 0506+056. We find that TXS 0506+056 shows strong flux variability in the Fermi-Large Area Telescope gamma-ray band, being in an active state around the arrival of IceCube-170922A, but in a low state during the archival IceCube neutrino flare in 2014/15. In both cases the spectral shape is statistically compatible (≤2σ) with the average spectrum showing no indication of a significant relative increase of a high-energy component. While the association of GB6 J1040+0617 with the neutrino is consistent with background expectations, the source appears to be a plausible neutrino source candidate based on its energetics and multiwavelength features, namely a bright optical flare and modestly increased gamma-ray activity. Finding one or two neutrinos originating from gamma-ray blazars in the given sample of high-energy neutrinos is consistent with previously derived limits of neutrino emission from gamma-ray blazars, indicating the sources of the majority of cosmic high-energy neutrinos remain unknown., 0, SCOPUS: ar.j, info:eu-repo/semantics/published
Published: 2019

24. LOFAR Observations of 4C+19.44: On the Discovery of Low-frequency Spectral Curvature in Relativistic Jet Knots

Author: D. E. Harris, J. Moldón, J. R. R. Oonk, F. Massaro, A. Paggi, A. Deller, L. Godfrey, R. Morganti, S. G. Jorstad, and Astronomy
Subjects: PARABOLIC SPECTRA, PARTICLE-ACCELERATION, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Low frequency, Curvature, 01 natural sciences, Spectral line, Jansky, X-RAY-EMISSION, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Jet (fluid), RADIO, Astronomy and Astrophysics, Quasar, LOFAR, galaxies: jets, radiation mechanisms: non-thermal, Astrophysics - Astrophysics of Galaxies, BLAZARS, EVOLUTION, quasars: individual: 4C+19.44, Space and Planetary Science, HOT-SPOTS, Astrophysics of Galaxies (astro-ph.GA), LUMINOSITY, galaxies: active galaxies, Radio frequency, BEPPOSAX, Astrophysics - High Energy Astrophysical Phenomena, CYGNUS-A
Abstract: We present the first LOFAR observations of the radio jet in the quasar 4C+19.44 (a.k.a. PKS 1354+19) obtained with the long baselines. The achieved resolution is very well matched to that of archival Jansky Very Large Array (JVLA) observations at higher radio frequencies as well as the archival X-ray images obtained with {\it Chandra}. We found that, for several knots along the jet, the radio flux densities measured at hundreds of MHz lie well below the values estimated by extrapolating the GHz spectra. This clearly indicates the presence of spectral curvature. Radio spectral curvature has been already observed in different source classes and/or extended radio structures and it has been often interpreted as due to intrinsic processes, as a curved particle energy distribution, rather than absorption mechanisms ({ Razin-Tsytovich} effect, free-free or synchrotron self absorption to name a few). Here we discuss our results according to the scenario where particles undergo stochastic acceleration mechanisms also in quasar jet knots., Comment: 13 pages, 4 tables, 4 figures, pre-proof version, published on the Astrophysical Journal (Harris, et al. 2019 ApJ, 873, 21)
Published: 2019

25. Relativistic Jet Simulations of the Weibel Instability in the Slab Model to Cylindrical Jets with Helical Magnetic Fields

Author: Oleh Kobzar, Ioana Duţan, Athina Meli, Dieter H. Hartmann, Helene Sol, Ken-Ichi Nishikawa, Yosuke Mizuno, José L. Gómez, Nicholas R. MacDonald, Jacek Niemiec, Martin Pohl, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas (España), National Science Centre (Poland), European Commission, European Research Council, and German Research Foundation
Subjects: PARTICLE-ACCELERATION, Mushroom instability, MAGNETOHYDRODYNAMIC SIMULATIONS, magnetic fields, 01 natural sciences, SHOCKS, lcsh:QB1-991, The Weibel instability, Astrophysical jet, Particle-in-cell simulations, KELVIN-HELMHOLTZ INSTABILITY, 010303 astronomy & astrophysics, relativistic jets, Physics, Jet (fluid), PLASMA, Mechanics, recollimation shocks, COSMIC-RAYS, Magnetic field, Weibel instability, Global jets, Physics::Space Physics, Slab, the Weibel instability, Astrophysical plasma, ELECTRON SHOCK, helical, Recollimation shocks, lcsh:Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Helical magnetic fields, Kinetic energy, kink-like instability, Pulsar, Kink-like instability, Physics::Plasma Physics, 0103 physical sciences, ddc:530, particle-in-cell simulations, 010306 general physics, helical magnetic fields, mushroom instability, Institut für Physik und Astronomie, Astronomy and Astrophysics, Plasma, astronomy_astrophysics, Computational physics, Physics and Astronomy, [SDU]Sciences of the Universe [physics], COLLISIONLESS, TURBULENCE, ddc:520, Relativistic jets, EMISSION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], GENERATION, global jets
Abstract: The particle-in-cell (PIC) method was developed to investigate microscopic phenomena, and with the advances in computing power, newly developed codes have been used for several fields, such as astrophysical, magnetospheric, and solar plasmas. PIC applications have grown extensively, with large computing powers available on supercomputers such as Pleiades and Blue Waters in the US. For astrophysical plasma research, PIC methods have been utilized for several topics, such as reconnection, pulsar dynamics, non-relativistic shocks, relativistic shocks, and relativistic jets. PIC simulations of relativistic jets have been reviewed with emphasis placed on the physics involved in the simulations. This review summarizes PIC simulations, starting with the Weibel instability in slab models of jets, and then focuses on global jet evolution in helical magnetic field geometry. In particular, we address kinetic Kelvin-Helmholtz instabilities and mushroom instabilities., This work is supported by NSF AST-0908010, AST-0908040, NASA-NNX09AD16G, NNX12AH06G, NNX13AP-21G, and NNX13AP14G grants. The work of J.N. and O.K. has been supported by Narodowe Centrum Nauki through research project DEC-2013/10/E/ST9/00662. Y.M. is supported by the ERC Synergy Grant “BlackHoleCam—Imaging the Event Horizon of Black Holes” (Grant No. 610058). M.P. acknowledges support through grant PO 1508/1-2 of the Deutsche orschungsgemeinschaft. Simulations were performed using Pleiades and Endeavor facilities at NASA Advanced Supercomputing (NAS), and using Gordon and Comet at The San Diego Supercomputer Center (SDSC), and Stampede at The Texas Advanced Computing Center, which are supported by the NSF. This research was started during the program “Chirps, Mergers and Explosions: The Final Moments of Coalescing Compact Binaries” at the Kavli Institute for Theoretical Physics, which is supported by the National Science Foundation under grant No. PHY05-51164. The first velocity shear results using an electron−positron plasma were obtained during the Summer Aspen workshop “Astrophysical Mechanisms of Particle Acceleration and Escape from the Accelerators” held at the Aspen Center for Physics (1–15 September 2013), We acknowledge support by the CSIC Open Access Publication Initiative through its Unit of Information Resources for Research (URICI)
Published: 2019
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26. LoTSS DR1: Double-double radio galaxies in the HETDEX field

Author: Aleksandar Shulevski, Martin J. Hardcastle, Matt J. Jarvis, G. Gürkan, Kenneth Duncan, N. Jurlin, V. H. Mahatma, C. Tasse, Leah K. Morabito, Huub Röttgering, Jeremy J. Harwood, Philip Best, M. Brienza, Rachel Cochrane, Beatriz Mingo, Timothy W. Shimwell, R. Morganti, J. Sabater, Judith H. Croston, David J. Smith, Wendy L. Williams, Marek Jamrozy, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), High Energy Astrophys. & Astropart. Phys (API, FNWI), and Astronomy
Subjects: ACTIVE GALACTIC NUCLEI, Brightness, Active galactic nucleus, DOUBLE-DOUBLE MORPHOLOGY, PARTICLE-ACCELERATION, Radio galaxy, media_common.quotation_subject, DATA RELEASE, astro-ph.GA, galaxies: active, jets [galaxies], FOS: Physical sciences, Astrophysics, 01 natural sciences, LOUD AGN, 0103 physical sciences, Galaxy formation and evolution, ACCRETION, 010303 astronomy & astrophysics, media_common, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), radio continuum: galaxies, 010308 nuclear & particles physics, INTERMITTENT ACTIVITY, Astronomy and Astrophysics, LOFAR, galaxies: jets, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Galaxy, galaxies [radio continuum], HOST GALAXIES, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], JET ACTIVITY, Astrophysics - High Energy Astrophysical Phenomena, SKY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Double-double radio galaxies (DDRGs) represent a short but unique phase in the life-cycle of some of the most powerful radio-loud active galactic nuclei (RLAGN). These galaxies display large-scale remnant radio plasma in the intergalactic medium left behind by a past episode of active galactic nuclei (AGN) activity, and meanwhile, the radio jets have restarted in a new episode. The knowledge of what causes the jets to switch off and restart is crucial to our understanding of galaxy evolution, while it is important to know if DDRGs form a host galaxy dichotomy relative to RLAGN. We utilised the LOFAR Two-Metre Sky Survey DR1, using a visual identification method to compile a sample of morphologically selected candidate DDRGs, showing two pairs of radio lobes. To confirm the restarted nature in each of the candidate sources, we obtained follow-up observations with the VLA at higher resolution to observe the inner lobes or restarted jets, the confirmation of which created a robust sample of 33 DDRGs. We created a comparison sample of 777 RLAGN from the DR1 catalogue, and compared the optical and infrared magnitudes and colours of their host galaxies. We find that there is no statistically significant difference in the brightness of the host galaxies between double-doubles and single-cycle RLAGN. The DDRG and RLAGN samples also have similar distributions in WISE mid-infrared colours, indicating similar ages of stellar populations and dust levels in the hosts of DDRGs. We conclude that DDRGs and 'normal' RLAGN are hosted by galaxies of the same type, and that DDRG activity is simply a normal part of the life cycle of RLAGN. Restarted jets, particularly for the class of low-excitation radio galaxies, rather than being a product of a particular event in the life of a host galaxy, must instead be caused by smaller scale changes, such as in the accretion system surrounding the black hole., Comment: 20 pages, 2 tables, 54 figures. This paper is part of the LOFAR surveys data release 1 and has been accepted for publication in a special edition of A&A that will appear in Feb 2019, volume 622. The catalogues and images from the data release will be publicly available on lofar-surveys.org upon publication of the journal
Published: 2019

27. Modelling three-dimensional transport of solar energetic protons in a corotating interaction region generated with EUHFORIA

Author: Nicolas Wijsen, Jens Pomoell, Angels Aran, Stefaan Poedts, Department of Physics, and Space Physics Research Group
Subjects: Shock wave, PARTICLE-ACCELERATION, EFFICIENCY, 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, PROPAGATION, Astrophysics, FOCUSED TRANSPORT, 01 natural sciences, 7. Clean energy, EVENTS, Magnetic mirror, Physics - Space Physics, Sun: particle emission, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Adiabatic process, education, Sun: magnetic fields, 010303 astronomy & astrophysics, acceleration of particles, 0105 earth and related environmental sciences, INTERPLANETARY TRANSPORT, Physics, education.field_of_study, Astronomy and Astrophysics, WIND, 115 Astronomy, Space science, DIFFUSION, Space Physics (physics.space-ph), ADIABATIC DECELERATION, Computational physics, Solar wind, solar wind, Space and Planetary Science, Physics::Space Physics, Particle, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight, Heliosphere
Abstract: We introduce a new solar energetic particle (SEP) transport code that aims at studying the effects of different solar wind configurations on SEP events. We focus on the influence of varying solar wind velocities on the energy changes of SEPs, and study how a non-Parker background solar wind can trap particles temporarily at small heliocentric radial distances (r, 17 pages, 12 figures, published in Astronomy & Astrophysics
Published: 2019
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28. The Acceleration of Charged Particles in Corotating Interaction Regions (Cir) – a Review with Particular Emphasis on the Ulysses Mission.

Author: Keppler, Erhard
Abstract: Observations on the acceleration of charged particles to higher energies in corotating interaction regions in interplanetary space are reviewed. Particular emphasis is given to the Ulysses observations which at the moment provide the latest extensive set. By comparison with Pioneer 10/11, Voyager, ISEE 3, and IMP 8, data collected during solar minimum periods, the nature of these phenomena now become much clearer. The introduction describes the formation and peculiarities of corotating interaction regions starting with a brief description of the formation of shocks in the interplanetary medium. Section 2 gives a brief description of the Ulysses mission and its orbit and is followed in Section 3 by the observational material. It is organized such that after earlier observations are introduced upstream effects are described, then we mention the different shapes of energy spectra, and describe what is known on elementary composition. Particular emphasis is given to the observations of the proton to alpha particle ratio, which is related to the important question on the origin of the accelerated particles: Are there energetic seed particles of some 10 keV energy, or do the accelerated particles stem from the solar wind flow reservoir? Are there other sources? After the angular distribution of the accelerated population are described we turn to the question of the efficiency of acceleration by corotating shocks: Is the efficiency a function of certain shock parameters only? Is there a latitudinal dependence? Can the observations be understood by assuming a pure heliodistance dependence? We also discuss the acceleration of electrons in corotating shocks to quite high energies (which is not understood), and mention the effects of corotating structures on extremely high energetic particles like the cosmic rays or the anomalous component before closing this section with a summary of the observational facts. Section 4 briefly summarizes theoretical aspects of the acceleration of particles by CIR-shocks and finally we discuss the material with particular emphasis on three aspects: The latitudinal and/or heliodistance dependence of the phenomena, the elemental composition and the role of pick up ions in the Heliosphere, especially with respect to acceleration in corotating shocks. [ABSTRACT FROM AUTHOR]
Published: 1998
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29. Statistical analysis of mirror mode waves in sheath regions driven by interplanetary coronal mass ejection

Author: Andrew Dimmock, J. Soucek, Matti Ala-Lahti, Adnane Osmane, Emilia Kilpua, Tuija Pulkkinen, Department of Physics, Space Physics Research Group, University of Helsinki, Department of Electronics and Nanoengineering, Czech Academy of Sciences, Aalto-yliopisto, and Aalto University
Subjects: Atmospheric Science, PARTICLE-ACCELERATION, 010504 meteorology & atmospheric sciences, MAGNETOPAUSE, 01 natural sciences, ANISOTROPY INSTABILITIES, Astronomi, astrofysik och kosmologi, Earth and Planetary Sciences (miscellaneous), EARTHS MAGNETOSHEATH, Interplanetary physics, Astronomy, Astrophysics and Cosmology, Bow shock (aerodynamics), lcsh:Science, 010303 astronomy & astrophysics, Physics, Shock (fluid dynamics), solar wind plasma, Geology, Space physics, Fusion, Plasma and Space Physics, lcsh:QC1-999, Solar wind, space plasma physics (waves and instabilities), Physics::Space Physics, symbols, Magnetopause, HYBRID SIMULATIONS, BOW SHOCK, Astrophysics::High Energy Astrophysical Phenomena, Interplanetary physics (plasma waves and turbulence, solar wind plasma), symbols.namesake, Fusion, plasma och rymdfysik, SOLAR MAXIMUM, Physics::Plasma Physics, 0103 physical sciences, space plasma physics, MAGNETOSPHERIC STORMS, 0105 earth and related environmental sciences, waves and instabilities, lcsh:QC801-809, CLUSTER, Astronomy and Astrophysics, Plasma, HELIOSPHERE, 115 Astronomy, Space science, Computational physics, lcsh:Geophysics. Cosmic physics, Mach number, Space and Planetary Science, plasma waves and turbulence, lcsh:Q, lcsh:Physics, Heliosphere
Abstract: We present a comprehensive statistical analysis of mirror mode waves and the properties of their plasma surroundings in sheath regions driven by interplanetary coronal mass ejection (ICME). We have constructed a semi-automated method to identify mirror modes from the magnetic field data. We analyze 91 ICME sheath regions from January 1997 to April 2015 using data from the Wind spacecraft. The results imply that similarly to planetary magnetosheaths, mirror modes are also common structures in ICME sheaths. However, they occur almost exclusively as dip-like structures and in mirror stable plasma. We observe mirror modes throughout the sheath, from the bow shock to the ICME leading edge, but their amplitudes are largest closest to the shock. We also find that the shock strength (measured by Alfvén Mach number) is the most important parameter in controlling the occurrence of mirror modes. Our findings suggest that in ICME sheaths the dominant source of free energy for mirror mode generation is the shock compression. We also suggest that mirror modes that are found deeper in the sheath are remnants from earlier times of the sheath evolution, generated also in the vicinity of the shock. Keywords. Interplanetary physics (plasma waves and turbulence; solar wind plasma) – space plasma physics (waves and instabilities)
Published: 2018
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30. The Cherenkov Telescope Array potential for the study of young supernova remnants

Author: Tomasz Szepieniec, K. Nishijima, T. Grabarczyk, M. C. Maccarone, Thomas Lohse, F. de Palma, Jacek Niemiec, R. J. García López, S. Rainò, Stefan Ohm, G. Busetto, F. Nunio, G. Pareschi, Emmanuel Moulin, Michał Szanecki, Jiri Chudoba, Saverio Lombardi, M. Nievas, Massimo Persic, A. Wilhelm, A. Bonardi, D. Garrido, J. L. Dournaux, A. Förster, Vikram V. Dwarkadas, Juan Abel Barrio, F. Di Pierro, K. Meagher, A. C. Rovero, Paweł Wójcik, Martina Bohacova, A. Sillanpää, Giuseppe Malaguti, R. A. Ong, Jörg R. Hörandel, Włodek Kluźniak, Henrike Fleischhack, Valerie Connaughton, Juhani Huovelin, Dusan Mandat, B. De Lotto, M. Palatka, Francesco Dazzi, A. De Franco, Carla Aramo, Martin Pohl, Anton N. Baushev, H. Siejkowski, G. Lamanna, David Berge, P. Vallania, M. Shayduk, C. van Eldik, N. Giglietto, Alicja Wierzcholska, S. Kaufmann, A. Giuliani, T. B. Humensky, T. Di Girolamo, R. López-Coto, L. Tibaldo, Masatoshi Ohishi, Pratik Majumdar, Luis Ángel Tejedor, B. S. Acharya, B. García, Gernot Maier, D. Nosek, Gagik Tovmassian, J.-P. Lenain, B. Khélifi, Takanori Yoshikoshi, Stanislav Stefanik, P. M. Chadwick, I. de la Calle, Garret Cotter, Masahiro Teshima, M. Fesquet, S. P. Wakely, William H. Lee, Andreas Quirrenbach, U. F. Katz, M. Garczarczyk, P. Romano, P. A. Caraveo, O. Tibolla, Marek Jamrozy, Nikola Godinovic, N. Otte, Hidetoshi Kubo, M. Fuessling, G. Fontaine, Rodolfo Carosi, Tarek M. Hassan, S. Vercellone, R. de los Reyes Lopez, Vito Conforti, Carlo Vigorito, Ll. Font, M. Prouza, V. Bugaev, Petr Travnicek, M. Hrabovsky, Jan Ebr, G. Rodriguez Fernandez, Miroslav Pech, Reiko Orito, J. Kocot, Ana Babić, A. Morselli, A. M. Brown, B. Rudak, M. N. Mazziotta, Kathrin Egberts, F. Lucarelli, Nukri Komin, J. Kushida, Jose Luis Contreras, Ferdinando Giordano, Alicia López-Oramas, J. Carr, Nestor Mirabal, C. Di Giulio, P. Kaaret, Petr Janecek, M. Trzeciak, Stefan Wagner, T. Stolarczyk, M. Gaug, Michael G. Burton, Petr Schovanek, A. Weinstein, Maria Magdalena González, I. Telezhinsky, J. Becker Tjus, F. Gargano, Dario Hrupec, Tomasz Bulik, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), CTA Collaboration, Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), High Energy Astrophys. & Astropart. Phys (API, FNWI), Acharya, B. S., Aramo, C., Babic, A., Barrio, J. A., Baushev, A., Becker Tjus, J., Berge, D., Bohacova, M., Bonardi, A., Brown, A., Bugaev, V., Bulik, T., Burton, M., Busetto, G., Caraveo, P., Carosi, R., Carr, J., Chadwick, P., Chudoba, J., Conforti, V., Connaughton, V., Contreras, J. L., Cotter, G., Dazzi, F., De Franco, A., de la Calle, I., de los Reyes Lopez, R., De Lotto, B., De Palma, F., DI GIROLAMO, Tristano, Di Giulio, C., Di Pierro, F., Dournaux, J. L., Dwarkadas, V., Ebr, J., Egberts, K., Fesquet, M., Fleischhack, H., Font, L., Fontaine, G., Förster, A., Fuessling, M., Garcia, B., Garcia López, R., Garczarczyk, M., Gargano, F., Garrido, D., Gaug, M., Giglietto, N., Giordano, F., Giuliani, A., Godinovic, N., Gonzalez, M. M., Grabarczyk, T., Hassan, T., Hörandel, J., Hrabovsky, M., Hrupec, D., Humensky, T. B., Huovelin, J., Jamrozy, M., Janecek, P., Kaaret, P. E., Katz, U., Kaufmann, S., Khélifi, B., Kluźniak, W., Kocot, J., Komin, N., Kubo, H., Kushida, J., Lamanna, G., Lee, W. H., Lenain, J. P., Lohse, T., Lombardi, S., López Coto, R., López Oramas, A., Lucarelli, F., Maccarone, M. C., Maier, G., Majumdar, P., Malaguti, G., Mandat, D., Mazziotta, M. N., Meagher, K., Mirabal, N., Morselli, A., Moulin, E., Niemiec, J., Nievas, M., Nishijima, K., Nosek, D., Nunio, F., Ohishi, M., Ohm, S., Ong, R. A., Orito, R., Otte, N., Palatka, M., Pareschi, G., Pech, M., Persic, M., Pohl, M., Prouza, M., Quirrenbach, A., Rainó, S., Rodriguez Fernandez, G., Romano, P., Rovero, A. C., Rudak, B., Schovanek, P., Shayduk, M., Siejkowski, H., Sillanpää, A., Stefanik, S., Stolarczyk, T., Szanecki, M., Szepieniec, T., Tejedor, L. A., Telezhinsky, I., Teshima, M., Tibaldo, L., Tibolla, O., Tovmassian, G., Travnicek, P., Trzeciak, M., Vallania, P., van Eldik, C., Vercellone, S., Vigorito, C., Wagner, S. J., Wakely, S. P., Weinstein, A., Wierzcholska, A., Wilhelm, A., Wojcik, P., and Yoshikoshi, T.
Subjects: Non-termal. [Radiation mechanisms], [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Acceleration of particles, PARTICLE-ACCELERATION, GAMMA RAYS, Ciencias Físicas, Milky Way, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Cosmic ray, Astrophysics, 7. Clean energy, REVERSE SHOCKS, Gamma rays: General, ISM: Supernova remnants, Radiation mechanisms: Non-termal, General, non-termal [radiation mechanisms], Cherenkov radiation, Astrophysics::Galaxy Astrophysics, acceleration of particles, Physics, CTA, supernova remnants [ISM], MAGNETIC-FIELD, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, AMPLIFICATION, Gamma-ray astronomy, Cherenkov Telescope Array, COSMIC-RAYS, DIFFUSIVE SHOCK ACCELERATION, GAMMA-RAY ASTRONOMY, CASSIOPEIA-A, MILKY-WAY, EMISSION, Astronomía, Particle acceleration, Cassiopeia A, Supernova, SUPERNOVA REMNANTS, ddc:540, general [gamma rays], CIENCIAS NATURALES Y EXACTAS
Abstract: Supernova remnants (SNRs) are among the most important targets for γ-ray observatories. Being prominent non-thermal sources, they are very likely responsible for the acceleration of the bulk of Galactic cosmic rays (CRs). To firmly establish the SNR paradigm for the origin of cosmic rays, it should be confirmed that protons are indeed accelerated in, and released from, SNRs with the appropriate flux and spectrum. This can be done by detailed theoretical models which account for microphysics of acceleration and various radiation processes of hadrons and leptons. The current generation of Cherenkov telescopes has insufficient sensitivity to constrain theoretical models. A new facility, the Cherenkov Telescope Array (CTA), will have superior capabilities and may finally resolve this long standing issue of high-energy astrophysics. We want to assess the capabilities of CTA to reveal the physics of various types of SNRs in the initial 2000 years of their evolution. During this time, the efficiency to accelerate cosmic rays is highest. We perform time-dependent simulations of the hydrodynamics, the magnetic fields, the cosmic-ray acceleration, and the non-thermal emission for type Ia, Ic and IIP SNRs. We calculate the CTA response to the γ-ray emission from these SNRs for various ages and distances, and we perform a realistic analysis of the simulated data. We derive distance limits for the detectability and resolvability of these SNR types at several ages. We test the ability of CTA to reconstruct their morphological and spectral parameters as a function of their distance. Finally, we estimate how well CTA data will constrain the theoretical models. Fil: Acharya, B. S.. Tata Institute of Fundamental Research; India Fil: Aramo, C.. INFN; Italia Fil: Babic, A.. Rudjer Boskovic Institute; Croacia Fil: Barrio, J. A.. Universidad Complutense de Madrid; España Fil: Baushev, A.. Universität Potsdam; Alemania Fil: Becker Tjus, J.. Ruhr-universität Bochum; Alemania Fil: Berge, D.. University of Amsterdam; Países Bajos Fil: Bohacova, M.. Institute of Physics of the Academy of Sciences of the Czech Republic; República Checa Fil: Bonardi, A.. Universität Tübingen; Alemania Fil: Brown, A.. Durham University; Reino Unido Fil: Bugaev, V.. Washington University; Estados Unidos Fil: Bulik, T.. University of Warsaw; Polonia Fil: Burton, M.. University Of New South Wales; Australia Fil: Busetto, G.. Universitá degli Studi di Padova; Italia Fil: Caraveo, P.. Istituto di Astrofisica Spaziale e Fisica Cosmica; Italia Fil: Carosi, R.. INFN; Italia Fil: Carr, J.. Aix-Marseille Université; Francia Fil: Chadwick, P.. Durham University; Reino Unido Fil: Chudoba, J.. Institute of Physics of the Academy of Sciences of the Czech Republic; República Checa Fil: Conforti, V.. Istituto di Astrofisica Spaziale e Fisica Cosmica; Italia Fil: Connaughton, V.. University of Alabama; Estados Unidos Fil: Contreras, J. L.. Universidad Complutense de Madrid; España Fil: Cotter, G.. University of Oxford; Reino Unido Fil: Dazzi, F.. Universitá degli Studi di Padova; Italia Fil: De Franco, A.. t University of Oxford; Reino Unido Fil: de la Calle, I.. Universidad Complutense de Madrid; España Fil: de los Reyes Lopez, R.. Max-Planck-Institut für Kernphysik; Alemania Fil: De Lotto, B.. University of Udine; Italia Fil: Garcia, Beatriz Elena. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Parque Centenario. Instituto de Tecnologías en Detección y Astropartículas. Subsede del Instituto de Tecnologías en Detección y Astropartículas Mendoza; Argentina Fil: Rovero, Adrian Carlos. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: The Cta Consortium.
Published: 2015

31. Prospects for Cherenkov Telescope Array observations of the young supernova remnant RX J1713.7-3946

Author: Arqueros Martínez, Fernando, Barrio Uña, Juan Abel, Contreras González, José Luis, Franco Peláez, Francisco Javier, López Moya, Marcos, Mirabal Barrios, Néstor, Nievas Rosillo, Mireia, Rosado Vélez, Jaime, Tejedor Álvarez, Luis Ángel, Arqueros Martínez, Fernando, Barrio Uña, Juan Abel, Contreras González, José Luis, Franco Peláez, Francisco Javier, López Moya, Marcos, Mirabal Barrios, Néstor, Nievas Rosillo, Mireia, Rosado Vélez, Jaime, and Tejedor Álvarez, Luis Ángel
Abstract: © 2017 The American Astronomical Society. Artículo firmado por 381 autores. We gratefully acknowledge financial support from the following agencies and organizations: Ministerio de Ciencia, Tecnología e Innovación Productiva (MinCyT), Comisión Nacional de Energía Atómica (CNEA), Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Argentina; State Committee of Science of Armenia, Armenia; Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq), Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ), Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Brasil; Croatian Science Foundation, Croatia; Ministry of Education, Youth and Sports, MEYS LE13012, LG14019, 7AMB14AR005, and the Czech Science Foundation grant 14-17501S, Czech Republic; Ministry of Higher Education and Research, CNRS-INSU and CNRS-IN2P3, CEA-Irfu, ANR, Regional Council Ile de France, Labex ENIGMASS, OSUG2020 and OCEVU, France; Max Planck Society, BMBF, DESY, Helmholtz Association, Germany; Department of Atomic Energy, Department of Science and Technology, India; Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare (INFN), MIUR, Italy; ICRR, University of Tokyo, JSPS, Japan; Netherlands Research School for Astronomy (NOVA), Netherlands Organization for Scientific Research (NWO), Netherlands; The Bergen Research Foundation, Norway; Ministry of Science and Higher Education, the National Centre for Research and Development and the National Science Centre, Poland; Slovenian Research Agency, Slovenia; MINECO support through the National R + D + I, Subprograma Severo Ochoa, CDTI funding plans and the CPAN and MultiDark Consolider-Ingenio 2010 program, Spain; Swedish Research Council, Royal Swedish Academy of Sciences, Sweden; Swiss National Science Foundation (SNSF), Ernest Boninchi Foundation, Switzerland; Durham University, Leverhulme Trust, Liverpool University, University of Leicester, University of Oxford, Royal Society, Sc, We perform simulations for future Cherenkov Telescope Array (CTA) observations of RX J1713.7−3946, a young supernova remnant (SNR) and one of the brightest sources ever discovered in very high energy (VHE) gamma rays. Special attention is paid to exploring possible spatial (anti)correlations of gamma rays with emission at other wavelengths, in particular X-rays and CO/H I emission. We present a series of simulated images of RX J1713.7−3946 for CTA based on a set of observationally motivated models for the gamma-ray emission. In these models, VHE gamma rays produced by high-energy electrons are assumed to trace the nonthermal X-ray emission observed by XMM-Newton, whereas those originating from relativistic protons delineate the local gas distributions. The local atomic and molecular gas distributions are deduced by the NANTEN team from CO and H I observations. Our primary goal is to show how one can distinguish the emission mechanism(s) of the gamma rays (i.e., hadronic versus leptonic, or a mixture of the two) through information provided by their spatial distribution, spectra, and time variation. This work is the first attempt to quantitatively evaluate the capabilities of CTA to achieve various proposed scientific goals by observing this important cosmic particle accelerator., Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Argentina, Ministerio de Ciencia, Tecnología e Innovación Productiva (MinCyT), Argentina, Comisión Nacional de Energía Atómica (CNEA), Argentina, Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq), Brasil, Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ), Brasil, Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Brasil, Croatian Science Foundation, Croatia, Ministry of Education, Youth and Sports, MEYS, Czech Republic, Czech Science Foundation, Czech Republic, Ministry of Higher Education and Research, Czech Republic, Regional Council Ile de France, France, Max Planck Society, Germany, BMBF, Germany, DESY, Germany, Helmholtz Association, Germany, Department of Atomic Energy, India, Department of Science and Technology, India, Istituto Nazionale di Astrofisica (INAF), Italy, Istituto Nazionale di Fisica Nucleare (INFN), Italy, MIUR, Italy, ICRR, Japan, University of Tokyo, JSPS, Japan, Netherlands Research School for Astronomy (NOVA), Netherlands Organization for Scientific Research (NWO), The Bergen Research Foundation, Norway, Ministry of Science and Higher Education, Poland, the National Centre for Research and Development, Poland, the National Science Centre, Poland, Slovenian Research Agency, Slovenia, Subprograma Severo Ochoa, Spain, CDTI, Spain, CPAN, Spain, MultiDark Consolider-Ingenio 2010 program, Spain, Swedish Research Council, Royal Swedish Academy of Sciences, Sweden, Swiss National Science Foundation (SNSF), Ernest Boninchi Foundation, Switzerland, Durham University, UK, Leverhulme Trust, UK, Liverpool University, UK, University of Leicester, UK, University of Oxford, UK, Royal Society, Science and Technologies Facilities Council, UK, U.S. National Science Foundation, USA, U.S. Department of Energy, USA, Argonne National Laboratory, USA, Barnard College, USA, University of California, USA, University of Chicago, USA, Columbia University, USA, Georgia Institute of Technology, USA, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI program), USA, Iowa State University, USA, Washington University McDonnell Center for the Space Sciences, USA, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2017

32. Excitation and Control of Plasma Wakefields by Multiple Laser Pulses

Author: G. Cheung, C. Thornton, Christopher D. Gregory, J. Cowley, Simon M. Hooker, Dan Symes, Nicholas H. Matlis, Roman Walczak, Laura Corner, Stuart Mangles, Christopher Arran, R. J. Shalloo, Science and Technology Facilities Council (STFC), and Commission of the European Communities
Subjects: Accelerator Physics (physics.acc-ph), PARTICLE-ACCELERATION, ELECTRON ACCELERATION, X-RAYS, FOS: Physical sciences, General Physics and Astronomy, Radiation, 01 natural sciences, Physics, Particles & Fields, 010305 fluids & plasmas, law.invention, Optics, law, Physics::Plasma Physics, 0103 physical sciences, WAKE, ddc:550, 010306 general physics, Physics, Science & Technology, Waves in plasmas, business.industry, AMPLITUDE, Plasma, DRIVEN, Laser, Physics - Plasma Physics, Pulse (physics), BEAT-WAVE, Plasma Physics (physics.plasm-ph), Particle acceleration, Physics, Nuclear, Amplitude, Physical Sciences, RADIATION, Physics::Accelerator Physics, Physics - Accelerator Physics, INJECTED ELECTRONS, business, Excitation, GENERATION
Abstract: Physical review letters 119(4), 044802 (2017). doi:10.1103/PhysRevLett.119.044802, We demonstrate experimentally the resonant excitation of plasma waves by trains of laser pulses. We also take an important first step to achieving an energy recovery plasma accelerator by showing that a plasma wave can be damped by an out-of-resonance trailing laser pulse. The measured laser wakefields are found to be in excellent agreement with analytical and numerical models of wakefield excitation in the linear regime. Our results indicate a promising direction for achieving highly controlled, GeV-scale laserplasma accelerators operating at multikilohertz repetition rates., Published by APS, College Park, Md.
Published: 2017

33. Blazar spectral variability as explained by a twisted inhomogeneous jet

Author: M. S. Butuzova, C. Espinosa, O. Vince, K. Kuratov, Sergey S. Savchenko, Joseph Moody, A. Di Paola, Boyko Mihov, Ivan S. Troitsky, L. V. Larionova, José L. Gómez, T. S. Grishina, Mark Gurwell, Sol N. Molina, Brian Skiff, V. Bozhilov, G. V. Baida, D. A. Morozova, A. A. Mokrushina, Katsura Matsumoto, Sofia O. Kurtanidze, G. A. Borman, A. Strigachev, C. S. Lin, J. Echevarría, S. V. Nazarov, Raul Michel, G. Rodriguez-Coira, Alan P. Marscher, M. I. Carnerero, C. M. Raiteri, Joni Tammi, N. V. Efimova, Omar M. Kurtanidze, F. Pinna, Iain A. Steele, B. Jordan, B. McBreen, Kozo Sadakane, Paul S. Smith, C. Protasio, Manasvita Joshi, J. M. Ohlert, F. J. Redondo-Lorenzo, Clemens Thum, Elena G. Larionova, T. A. Polakis, L. Slavcheva-Mihova, Carolina Casadio, Anne Lähteenmäki, D. N. Okhmat, M. Villata, Helen Jermak, Erika Benítez, E. N. Kopatskaya, Arkady A. Arkharov, N. Rizzi, J. A. Acosta-Pulido, A. A. Vasilyev, Michael P. Malmrose, M. Minev, N. Castro-Segura, M. G. Nikolashvili, P. Calcidese, Manash R. Samal, Sh. A. Ehgamberdiev, Merja Tornikoski, C. Lázaro, Filippo D'Ammando, W. Boschin, T. Pursimo, D. Carosati, Rumen Bachev, A. C. Sadun, Goran Damljanović, Evgeni Semkov, D. O. Mirzaqulov, Evgeni Ovcharov, Yu. V. Troitskaya, Svetlana G. Jorstad, David Hiriart, A. Giunta, Antonio Fuentes, Ivan Agudo, Valeri M. Larionov, and Wen Ping Chen
Subjects: ACTIVE GALACTIC NUCLEI, Brightness, Active galactic nucleus, PARTICLE-ACCELERATION, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Relativistic beaming, Astrophysical jet, 0103 physical sciences, HELICAL JETS, PHOTOMETRY, OUTBURST, Blazar, 010303 astronomy & astrophysics, QC, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Multidisciplinary, ta115, ta114, 010308 nuclear & particles physics, EXTRAGALACTIC RADIO-SOURCES, COMPARISON STARS, Quasar, Astrophysics - Astrophysics of Galaxies, Galaxy, CTA-102, QUASARS, WEBT CAMPAIGN, Astrophysics of Galaxies (astro-ph.GA), RELATIVISTIC JETS, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Blazar emission is dominated by non-thermal radiation from a relativistic jet pointing toward us, therefore undergoing Doppler beaming. This is responsible for flux enhancement and contraction of the variability time scales, so that most blazars appear as luminous sources characterized by noticeable and fast flux changes at all frequencies. The mechanisms producing their unpredictable variability are debated and include injection, acceleration and cooling of particles, with possible intervention of shock waves or turbulence. Changes in the viewing angle of the emitting knots or jet regions have also been suggested to explain flaring events or specific properties such as intraday variability, quasi-periodicities, or the delay of radio flux variations relative to optical changes. However, such a geometric interpretation has not been universally accepted because alternative explanations based on changes of physical conditions can also work in many cases. Here we report the results of optical-to-radio monitoring of the blazar CTA 102 by the Whole Earth Blazar Telescope Collaboration and show that the observed long-term flux and spectral variability is best explained by an inhomogeneous, curved jet that undergoes orientation changes. We propose that magnetohydrodynamic instabilities or rotation of a twisted jet cause different jet regions to change their orientation and hence their relative Doppler factors. In particular, the recent extreme optical outburst (six magnitudes) occurred when the corresponding jet emitting region acquired a minimum viewing angle., Comment: 31 pages, 11 figures. This is the accepted version (before Nature editing) of the paper published by Nature, online version at http://dx.doi.org/10.1038/nature24623, Nature 2017/12/04/online
Published: 2017

34. Gamma-ray observations of tycho’s supernova remnant with veritas andfermi

Author: Q. Feng, P. T. Reynolds, C. A. Johnson, Wystan Benbow, A. Popkow, J. P. Finley, D. S. Hanna, B. Zitzer, Manel Errando, S. Kumar, D. B. Kieda, Karlen Shahinyan, Daniel Nieto, Henrike Fleischhack, Gernot Maier, Lucy Fortson, Moritz Hütten, David A. Williams, S. O'Brien, J. Tyler, M. Pohl, P. Kaaret, R. A. Ong, Thomas Weisgarber, Nahee Park, S. McArthur, J. H. Buckley, G. H. Sembroski, I. Sadeh, P. Wilcox, I. Telezhinsky, Jamie Holder, John L. Quinn, E. Pueschel, M. Buchovecky, P. Moriarty, P. Kar, A. N. Otte, S. Trepanier, Patrick Slane, A. J.R. Weinstein, A. Wilhelm, Ralph Bird, M. P. Connolly, D. Staszak, K. Ragan, Wei Cui, A. Archer, Gordon T. Richards, M. J. Lang, Marcos Santander, E. Roache, A. D. Falcone, Etienne Bourbeau, S. Archambault, Reshmi Mukherjee, Dwarkadas, N. Kelley-Hoskins, Bugaev, Matteo Cerruti, Amy Furniss, Sinéad M. Griffin, M. Kertzman, A. McCann, S. P. Wakely, and Marita Krause
Subjects: molecular cloud, shock acceleration, Astrophysics::High Energy Astrophysical Phenomena, stars-supernovae, cosmic-rays, Astrophysics, Type (model theory), telescope, 01 natural sciences, 0103 physical sciences, emission, ddc:530, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Spectral index, Range (particle radiation), particle-acceleration, 010308 nuclear & particles physics, brahes 1572 supernova, data behind figure, Gamma ray, Center (category theory), magnetic-field, electrons, Institut für Physik und Astronomie, individual(tycho's snr) supporting material, Astronomy and Astrophysics, gamma rays, Supernova, Space and Planetary Science, ddc:520, High Energy Physics::Experiment, high-energy, Energy (signal processing), Fermi Gamma-ray Space Telescope
Abstract: The astrophysical journal 836(1), 23 (2017). doi:10.3847/1538-4357/836/1/23, High-energy gamma-ray emission from supernova remnants (SNRs) has provided a unique perspective for studies of Galactic cosmic-ray acceleration. Tycho's SNR is a particularly good target because it is a young, type Ia SNR that has been well-studied over a wide range of energies and located in a relatively clean environment. Since the detection of gamma-ray emission from Tycho's SNR by VERITAS and Fermi-LAT, there have been several theoretical models proposed to explain its broadband emission and high-energy morphology. We report on an update to the gamma-ray measurements of Tycho's SNR with 147 hr of VERITAS and 84 months of Fermi-LAT observations, which represent about a factor of two increase in exposure over previously published data. About half of the VERITAS data benefited from a camera upgrade, which has made it possible to extend the TeV measurements toward lower energies. The TeV spectral index measured by VERITAS is consistent with previous results, but the expanded energy range softens a straight power-law fit. At energies higher than 400 GeV, the power-law index is 2.92 ± 0.42$_{stat}$ ± 0.20$_{sys}$. It is also softer than the spectral index in the GeV energy range, 2.14 ± 0.09$_{stat}$ ± 0.02$_{sys}$, measured in this study using Fermi-LAT data. The centroid position of the gamma-ray emission is coincident with the center of the remnant, as well as with the centroid measurement of Fermi-LAT above 1 GeV. The results are consistent with an SNR shell origin of the emission, as many models assume. The updated spectrum points to a lower maximum particle energy than has been suggested previously., Published by IOP Publ., Chicago, Ill. [u.a.]
Published: 2017

35. A luminous and isolated gamma-ray flare from the blazar B2 1215+30

Author: Veritas, Collaboration, Abeysekara, A. U., Archambault, S., Archer, A., Benbow, W., Bird, R., Buchovecky, M., Buckley, J. H., Bugaev, V., Byrum, K., Cerruti, M., Chen, X., Ciupik, L., Cui, W., Dickinson, H. J., Eisch, J. D., Errando, M., Falcone, A., Feng, Q., Finley, J. P., Fleischhack, H., Fortson, L., Furniss, A., Gillanders, G. H., Griffin, S., Grube, J., Hutten, M., Hakansson, N., Hanna, D., Holder, J., Humensky, T. B., Johnson, C. A., Kaaret, P., Kar, P., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Kumar, S., Lang, M. J., Gernot Maier, Mcarthur, S., Mccann, A., Meagher, K., Moriarty, P., Mukherjee, R., Nguyen, T., Nieto, D., Ong, R. A., Otte, A. N., Park, N., Pelassa, V., Pohl, M., Popkow, A., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Richards, G. T., Roache, E., Rulten, C., Santander, M., Sembroski, G. H., Shahinyan, K., Staszak, D., Telezhinsky, I., Tucci, J. V., Tyler, J., Wakely, S. P., Weiner, O. M., Weinstein, A., Wilhelm, A., Williams, D. A., Fermi-LAT Collaboration, Fegan, S., Giebels, B., Horan, D., Berdyugin, A., Kuan, J., Lindfors, E., Nilsson, K., Oksanen, A., Prokoph, H., Reinthal, R., Takalo, L., Zefi, F., AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), VERITAS, Fermi-LAT, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire Leprince-Ringuet ( LLR ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: multiwavelength observations, 010504 meteorology & atmospheric sciences, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, swift ultraviolet/optical telescope, 01 natural sciences, law.invention, bl lacertae objects, law, Observatory, 0103 physical sciences, gamma rays: galaxies, Astrophysics::Solar and Stellar Astrophysics, ddc:530, MAGIC (telescope), Blazar, 010303 astronomy & astrophysics, Cherenkov radiation, 0105 earth and related environmental sciences, BL Lacertae objects: individual, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, particle-acceleration, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Institut für Physik und Astronomie, Astronomy and Astrophysics, source catalog, galaxies: jets, spectral energy-distributions, bl lacertae objects: individual (b2 1215+30, ver j1217+301), large-area telescope, Crab Nebula, Space and Planetary Science, active galactic nuclei, reconnection, ddc:520, galaxies: nuclei, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], discovery, Flare
Abstract: The astrophysical journal 836(2), 205 (2017). doi:10.3847/1538-4357/836/2/205, B2 1215+30 is a BL-Lac-type blazar that was first detected at TeV energies by the MAGIC atmospheric Cherenkov telescopes and subsequently confirmed by the Very Energetic Radiation Imaging Telescope Array System (VERITAS) observatory with data collected between 2009 and 2012. In 2014 February 08, VERITAS detected a large-amplitude flare from B2 1215+30 during routine monitoring observations of the blazar 1ES 1218+304, located in the same field of view. The TeV flux reached 2.4 times the Crab Nebula flux with a variability timescale of $\lt 3.6\,\mathrm{hr}$. Multiwavelength observations with Fermi-LAT, Swift, and the Tuorla Observatory revealed a correlated high GeV flux state and no significant optical counterpart to the flare, with a spectral energy distribution where the gamma-ray luminosity exceeds the synchrotron luminosity. When interpreted in the framework of a one-zone leptonic model, the observed emission implies a high degree of beaming, with Doppler factor $\delta \gt 10$, and an electron population with spectral index $p\lt 2.3$., Published by IOP Publ., Chicago, Ill. [u.a.]
Published: 2017

36. Combined fit of spectrum and composition data as measured by the Pierre Auger Observatory

Author: Pierre Auger Collaboration, Aab, A., Anastasi, G. A., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Farrar, G., Fauth, A. C., Fazzini, N., Fick, B., Anchordoqui, L., Figueira, J. M., Filipčič, A., Fratu, O., Freire, M. M., Fujii, T., Fuster, A., Gaior, R., García, B., Garcia-Pinto, D., Gaté, F., Andrada, B., Gemmeke, H., Gherghel-Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Golup, G., Berisso, M. Gómez, Andringa, S., Vitale, P. F. Gómez, González, N., Gorgi, A., Gorham, P., Grillo, A. F., Grubb, T. D., Guarino, F., Guedes, G. P., Hampel, M. R., Hansen, P., Aramo, C., Harari, D., Harrison, T. A., Harton, J. L., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hill, G. C., Hojvat, C., Arqueros, F., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Jandt, I., Arsene, N., Jansen, S., Johnsen, J. A., Josebachuili, M., Kääpä, A., Kambeitz, O., Kampert, K. H., Katkov, I., Keilhauer, B., Kemp, E., Kemp, J., Asorey, H., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Mezek, G. Kukec, Kunka, N., Awad, A. Kuotb, Assis, P., LaHurd, D., Lauscher, M., Legumina, R., de Oliveira, M. A. Leigui, Letessier-Selvon, A., Lhenry-Yvon, I., Link, K., Lopes, L., López, R., Casado, A. López, Aublin, J., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Mariş, I. C., Marsella, G., Martello, D., Abreu, P., Avila, G., Martinez, H., Bravo, O. Martínez, Meza, J. J. Masías, Mathes, H. J., Mathys, S., Matthews, J., Matthews, J. A. J., Matthiae, G., Mayotte, E., Mazur, P. O., Badescu, A. M., Medina, C., Medina-Tanco, G., Melo, D., Menshikov, A., Micheletti, M. I., Middendorf, L., Minaya, I. A., Miramonti, L., Mitrica, B., Mockler, D., Balaceanu, A., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Müller, A. L., Müller, G., Muller, M. A., Müller, S., Mussa, R., Naranjo, I., Luz, R. J. Barreira, Nellen, L., Nguyen, P. H., Niculescu-Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, H., Beatty, J. J., Núñez, L. A., Ochilo, L., Oikonomou, F., Olinto, A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Becker, K. H., Pech, M., Pedreira, F., Pękala, J., Pelayo, R., Peña-Rodriguez, J., Pereira, L. A. S., Perlín, M., Perrone, L., Peters, C., Petrera, S., Bellido, J. A., Phuntsok, J., Piegaia, R., Pierog, T., Pieroni, P., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porowski, C., Prado, R. R., Berat, C., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos-Pollan, R., Rautenberg, J., Ravignani, D., Revenu, B., Ridky, J., Bertaina, M. E., Risse, M., Ristori, P., Rizi, V., de Carvalho, W. Rodrigues, Fernandez, G. Rodriguez, Rojo, J. Rodriguez, Rogozin, D., Roncoroni, M. J., Roth, M., Roulet, E., Bertou, X., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salamida, F., Salazar, H., Saleh, A., Greus, F. Salesa, Salina, G., Sánchez, F., Aglietta, M., Biermann, P. L., Sanchez-Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento, C. A., Sato, R., Schauer, M., Scherini, V., Schieler, H., Billoir, P., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Biteau, J., Settimo, M., Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Śmiałkowski, A., Šmída, R., Snow, G. R., Sommers, P., Blaess, S. G., Sonntag, S., Sorokin, J., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Strafella, F., Suarez, F., Durán, M. Suarez, Blanco, A., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Tapia, A., Theodoro, V. M., Timmermans, C., Blazek, J., Peixoto, C. J. Todero, Tomankova, L., Tomé, B., Elipe, G. Torralba, Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Galicia, J. F. Valdés, Bleve, C., Valiño, I., Valore, L., van Aar, G., van Bodegom, P., Berg, A. M. van den, van Vliet, A., Varela, E., Cárdenas, B. Vargas, Varner, G., Vázquez, J. R., Boháčová, M., Vázquez, R. A., Veberič, D., Quispe, I. D. Vergara, Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Boncioli, D., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczyński, H., Winchen, T., Wirtz, M., Wittkowski, D., Wundheiler, B., Yang, L., Bonifazi, C., Yelos, D., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Samarai, I. Al, Borodai, N., Botti, A. M., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Albuquerque, I. F. M., Buscemi, M., Caballero-Mora, K. S., Caccianiga, L., Cancio, A., Canfora, F., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Allekotte, I., Chavez, A. G., Chinellato, J. A., Chudoba, J., Clay, R. W., Colalillo, R., Coleman, A., Collica, L., Coluccia, M. R., Conceição, R., Contreras, F., Almela, A., Cooper, M. J., Coutu, S., Covault, C. E., Cronin, J., D'Amico, S., Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., Castillo, J. Alvarez, de Jong, S. J., De Mauro, G., Neto, J. R. T. de Mello, De Mitri, I., de Oliveira, J., de Souza, V., Debatin, J., Deligny, O., Di Giulio, C., Di Matteo, A., Alvarez-Muñiz, J., Castro, M. L. Díaz, Diogo, F., Dobrigkeit, C., D'Olivo, J. C., Dorosti, Q., Anjos, R. C. dos, Dova, M. T., Dundovic, A., Ebr, J., Engel, R., Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), Pierre Auger Collaboration, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Aab, A., Abreu, P., Aglietta, M., Samarai, I. Al, Albuquerque, I. F. M., Allekotte, I., Almela, A., Castillo, J. Alvarez, Alvarez Muñiz, J., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Badescu, A. M., Balaceanu, A., Luz, R. J. Barreira, Beatty, J. J., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Billoir, P., Biteau, J., Blaess, S. G., Blanco, A., Blazek, J., Bleve, C., Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Botti, A. M., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero Mora, K. S., Caccianiga, L., Cancio, A., Canfora, F., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Chavez, A. G., Chinellato, J. A., Chudoba, J., Clay, R. W., Colalillo, Roberta, Coleman, A., Collica, L., Coluccia, M. R., Conceição, R., Contreras, F., Cooper, M. J., Coutu, S., Covault, C. E., Cronin, J., D'Amico, S., Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., de Jong, S. J., Mauro, G. De, Neto, J. R. T. de Mello, Mitri, I. De, de Oliveira, J., de Souza, V., Debatin, J., Deligny, O., Giulio, C. Di, di Matteo, A., Castro, M. L. Díaz, Diogo, F., Dobrigkeit, C., D'Olivo, J. C., Dorosti, Q., Anjos, R. C. do, Dova, M. T., Dundovic, A., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Farrar, G., Fauth, A. C., Fazzini, N., Fick, B., Figueira, J. M., Filipčič, A., Fratu, O., Freire, M. M., Fujii, T., Fuster, A., Gaior, R., García, B., Garcia Pinto, D., Gaté, F., Gemmeke, H., Gherghel Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Golup, G., Berisso, M. Gómez, Vitale, P. F. Gómez, González, N., Gorgi, A., Gorham, P., Grillo, A. F., Grubb, T. D., Guarino, Fausto, Guedes, G. P., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Harton, J. L., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hill, G. C., Hojvat, C., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Jandt, I., Jansen, S., Johnsen, J. A., Josebachuili, M., Kääpä, A., Kambeitz, O., Kampert, K. H., Katkov, I., Keilhauer, B., Kemp, E., Kemp, J., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Mezek, G. Kukec, Kunka, N., Awad, A. Kuotb, Lahurd, D., Lauscher, M., Legumina, R., de Oliveira, M. A. Leigui, Letessier Selvon, A., Lhenry Yvon, I., Link, K., Lopes, L., López, R., Casado, A. López, Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Mariš, I. C., Marsella, G., Martello, D., Martinez, H., Bravo, O. Martínez, Meza, J. J. Masía, Mathes, H. J., Mathys, S., Matthews, J., Matthews, J. A. J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina, C., Medina Tanco, G., Melo, D., Menshikov, A., Micheletti, M. I., Middendorf, L., Minaya, I. A., Miramonti, L., Mitrica, B., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Müller, A. L., Müller, G., Muller, M. A., Müller, S., Mussa, R., Naranjo, I., Nellen, L., Nguyen, P. H., Niculescu Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, H., Núñez, L. A., Ochilo, L., Oikonomou, F., Olinto, A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pȩkala, J., Pelayo, R., Peña Rodriguez, J., Pereira, L. A. S., Perlín, M., Perrone, L., Peters, C., Petrera, S., Phuntsok, J., Piegaia, R., Pierog, T., Pieroni, P., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos Pollan, R., Rautenberg, J., Ravignani, D., Revenu, B., Ridky, J., Risse, M., Ristori, P., Rizi, V., de Carvalho, W. Rodrigue, Fernandez, G. Rodriguez, Rojo, J. Rodriguez, Rogozin, D., Roncoroni, M. J., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salamida, F., Salazar, H., Saleh, A., Greus, F. Salesa, Salina, G., Sánchez, F., Sanchez Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento, C. A., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Settimo, M., Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Śmiałkowski, A., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Sorokin, J., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Strafella, F., Suarez, F., Durán, M. Suarez, Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Tapia, A., Theodoro, V. M., Timmermans, C., Peixoto, C. J. Todero, Tomankova, L., Tomé, B., Elipe, G. Torralba, Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Galicia, J. F. Valdé, Valiño, I., Valore, Laura, Aar, G. van, Bodegom, P. van, Berg, A. M. van den, Vliet, A. van, Varela, E., Cárdenas, B. Varga, Varner, G., Vázquez, J. R., Vázquez, R. A., Veberič, D., Quispe, I. D. Vergara, Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczyński, H., Winchen, T., Wirtz, M., Wittkowski, D., Wundheiler, B., Yang, L., Yelos, D., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Research unit Astroparticle Physics, Bleve, Carla, Colalillo, R., Coluccia, MARIA RITA, D'Amico, Stefano, DE MITRI, Ivan, Guarino, F., Marsella, Giovanni, Martello, Daniele, Perrone, Lorenzo, Strafella, Francesco, and Valore, L.
Subjects: PARTICLE-ACCELERATION, Astronomy, UNIVERSE, Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, inter-galactic media, TALYS, 010303 astronomy & astrophysics, Chemical composition, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, UHECR, Spectrum (functional analysis), Astrophysics::Instrumentation and Methods for Astrophysics, cosmic ray experiments, cosmic ray theory, intergalactic media, ultra high energy cosmic rays, Astronomy and Astrophysics, ENERGY COSMIC-RAYS, NEUTRINOS, ultra high energy cosmic rays, cosmic ray experiments, cosmic ray theory, intergalactic media, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Mass composition, 0103 physical sciences, Energy spectrum, ddc:530, High Energy Physics, Ciencias Exactas, Physical quantity, Pierre Auger Observatory, CONSEQUENCES, NUCLEI, 010308 nuclear & particles physics, GAMMA-RAYS, Física, ASTROFÍSICA, Composition (combinatorics), EXTRAGALACTIC BACKGROUND LIGHT, 13. Climate action, Experimental High Energy Physics
Abstract: We present a combined fit of a simple astrophysical model of UHECR sources to both the energy spectrum and mass composition data measured by the Pierre Auger Observatory. The fit has been performed for energies above 5 · 1018 eV, i.e. the region of the all-particle spectrum above the so-called “ankle” feature. The astrophysical model we adopted consists of identical sources uniformly distributed in a comoving volume, where nuclei are accelerated through a rigidity-dependent mechanism. The fit results suggest sources characterized by relatively low maximum injection energies, hard spectra and heavy chemical composition. We also show that uncertainties about physical quantities relevant to UHECR propagation and shower development have a non-negligible impact on the fit results., Este documento tiene una corrección (ver documento relacionado)., La nómina completa de autores puede verse en el archivo asociado a este ítem., Facultad de Ciencias Exactas, Instituto de Física La Plata
Published: 2017

37. Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946

Author: Csaba Balázs, M. Servillat, F. D'Ammando, D. Nosek, T. Yamamoto, A. Bilinsky, H.-S. Zechlin, Francesco Dazzi, A. Fernández-Barral, Satoshi Yoshiike, Catherine Boisson, Philippe Laporte, K. Nishijima, Yutaka Fujita, T. Armstrong, A. Shalchi, S. Kimura, D. Nakajima, Fuyuki Tokanai, Francesco Longo, S. Pavy, Philip Kaaret, W. van Driel, Gianpiero Tagliaferri, L. Nogués, F. Di Pierro, Wystan Benbow, T. Stolarczyk, Marco Padovani, T. Di Girolamo, Johan Bregeon, J. Rico, R. Wischnewski, A. Sillanpää, T. Grabarczyk, E. Pueschel, P. Blasi, S. D. Vergani, A. De Franco, C. Bonavolontà, J. Prast, J. Zorn, Elisabetta Bissaldi, Giuseppe Malaguti, A. Pe'Er, Stefano Covino, Akira Okumura, Takashi Saito, C. Aramo, Hermine Landt, R. Zanin, E. Fedorova, Shinji Hara, Yutaka Ohira, Petr Janecek, Petar Temnikov, T. B. Humensky, E. Fiandrini, C. Townsley, R. J. White, A. Fiasson, Koji Noda, Takanori Yoshikoshi, Y. Ikeno, Elena Amato, Yasuo Fukui, J. P. Lees, M. Nievas-Rosillo, Vito Conforti, Kazunori Kohri, I. Oya, M. Trifoglio, Gavin Rowell, Jacek Niemiec, Juan Abel Barrio, R. Walter, Stefan Wagner, Teresa Mineo, J. J. Watson, Reiko Orito, Masahiro Teshima, Jim Hinton, A. Pisarski, G. Rodriguez Fernandez, F. De Frondat, Robert Wagner, Pedro L. Luque-Escamilla, G. Morlino, Thomas Lohse, B. Rudak, Olaf Reimer, Josep Martí, Subir Sarkar, Martin White, Johann Cohen-Tanugi, Michiyuki Chikawa, Dusan Mandat, T. Montaruli, M. Mohammed, M. Iori, Oscar Blanch, Giovanni Bonanno, Benjamin Koch, M. A. Lopez, Julien Rousselle, M. Heller, Yusuke Konno, G. Maurin, J. Palacio, S. Gunji, C. Di Giulio, M. Zavrtanik, J.-P. Lenain, Adrian Biland, Michael Backes, Miroslav Filipovic, M. I. Martínez, M. Vazquez Acosta, Nicola Giglietto, J. M. Paredes, G. Fontaine, R. Moderski, A.A. Zdziarski, D. Tescaro, V. Vassiliev, C. van Eldik, H. Siejkowski, Stefan Kimeswenger, Shu Koyama, A. Bonardi, R. Gnatyk, S. Vorobiov, Oleh Petruk, M. Del Santo, Michał Szanecki, C. Delgado, Carole Mundell, Tomasz Szepieniec, Michael G. Burton, Bohdan Hnatyk, M. Capalbi, Kunihito Ioka, Jonathan Granot, Bohdan Novosyadlyj, Petr Schovanek, A. Weinstein, M. Stephan, Vikram V. Dwarkadas, L. Valore, Sabrina Einecke, P. Goldoni, J. Jacquemier, Hiroshi Muraishi, Andreas Quirrenbach, Takeshi Nakamori, Stefan Ohm, G. Busetto, Marcos Santander, A. Wierzcholska, Jaime Rosado, M. Yoshida, M. Huetten, S. Eschbach, Tatsuo Yoshida, Tomasz Bulik, Gino Tosti, Valentina Fioretti, Makoto Sawada, D. Zavrtanik, P. A. Caraveo, Mohamed Rameez, Sylvain Chaty, Nu. Komin, D. Dumas, Michael Zacharias, J. M. Huet, Reshmi Mukherjee, F. Lucarelli, L. Di Venere, Shuta J. Tanaka, F. de Palma, Shiu-Hang Lee, A. W. Chen, A. Giuliani, R. L. C. Starling, V. Beshley, Jonathan S. Lapington, Gilles Ferrand, Giovanni Covone, Rodrigo Nemmen, Tsuyoshi Inoue, R. C. Shellard, P. Cumani, G. Lamanna, Stefan Funk, Michele Doro, Koji Mori, G. Pühlhofer, Hidetoshi Sano, Susumu Inoue, Luis Ángel Tejedor, G. Kukec Mezek, Anderson Caproni, L. Freixas Coromina, M. de Naurois, D. Jankowsky, Yoshiyuki Inoue, Elina Lindfors, Saverio Lombardi, D. della Volpe, Giancarlo Cusumano, Andrea Orlati, S. Mangano, Samar Safi-Harb, Alexandre Marcowith, R. López-Coto, Martin Pohl, J. Lefaucheur, Vincenzo Rizi, Masayuki Tanaka, Shigehiro Nagataki, J. L. Rodriguez, Diego Falceta-Gonçalves, J. E. Ward, Petr Travnicek, I. Sadeh, Dominik Elsässer, P. Wilcox, Tsunefumi Mizuno, Kohta Murase, K. Lalik, M. Ostrowski, Vincenzo Testa, Tsuguya Naito, Matteo Cerruti, N. La Palombara, Yukikatsu Terada, Emmanuel Moulin, A. Balzer, M. Palatka, Samo Stanič, D. D'Urso, Łukasz Stawarz, D. Simone, Giuseppe Romeo, Francesco Giordano, Luca Zampieri, Michiko Ohishi, Giuseppe Leto, J.F. Glicenstein, G. De Cesare, Eleonora Torresi, R. A. Cameron, Katsuaki Asano, Ricardo Graciani, Gernot Maier, Paweł Wójcik, R. A. Ong, Jörg R. Hörandel, Carlo Vigorito, S. P. Wakely, Valerio Vagelli, Andrea Bulgarelli, J. Takeda, S. Brau-Nogué, Garret Cotter, Claudio Melioli, Hiroaki Yamamoto, M. Vrastil, Ryo Yamazaki, G. Maneva, N. Maxted, David A. Williams, K. Kosack, Konrad Bernlöhr, Markus Böttcher, Andreas Zech, Jürgen Knödlseder, Daniel Nieto, Paola Grandi, Maria Concetta Maccarone, Y. Inome, I. Telezhinsky, Fabio Acero, Michael C. B. Ashley, D. A. Sanchez, C. de Lisio, Francisco J. Franco, J. L. Dournaux, M. Kraus, G. Bonnoli, Xian Chen, Massimo Persic, Jonathan Blazek, Giacomo Principe, Louis Antonelli, H. Hakobyan, A. De Angelis, Marek Nikolajuk, F. Schüssler, T. Nagayoshi, P.-O. Petrucci, P. Sangiorgi, N. Sakaki, Anthony M. Brown, S. Tsujimoto, J. J. Rodríguez Vázquez, A. Morselli, B. De Lotto, Juan Carlos Helo, S. Nozaki, M. Takahashi, Lili Yang, H. Schoorlemmer, Catherine Braiding, Justin Vandenbroucke, J. A. Graham, P. Vallania, Stanislav Stefanik, M. Fesquet, Roberto Aloisio, Diego F. Torres, Ciro Bigongiari, C. Díaz, Shohei Yanagita, M. Garczarczyk, Abelardo Moralejo, Hideaki Katagiri, R. de los Reyes Lopez, A. Burtovoi, M. Hussein, Hiroyasu Tajima, M. Prouza, M. Renaud, C. Trichard, M. K. Daniel, Maria Chernyakova, Tarek M. Hassan, A. Ziegler, E. M. de Gouveia Dal Pino, Ll. Font, J. Kocot, Jiri Chudoba, J. P. Amans, Enrico Junior Schioppa, Alessandro Costa, Aya Bamba, A. Förster, F. Arqueros, Jan Ebr, M. Hayashida, A. J. Green, Marc Ribó, Olga Sergijenko, Hidetoshi Kubo, A. Porcelli, Tomohiro Inada, J. Biteau, J. Kushida, Jose Luis Contreras, S. Colafrancesco, Nestor Mirabal, V. Bugaev, R. J. García López, Vitalii Sliusar, I. Jung, Kathrin Egberts, G. Fasola, Maxim V. Barkov, Seiji Masuda, P. Romano, Enrico Cascone, V. I. Zhdanov, Elisa Prandini, Helene Sol, Rodolfo Carosi, S. Vercellone, Manuela Vecchi, German Martinez, A. Gadola, S. Griffiths, Satyendra Thoudam, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CTA Consortium, High Energy Astrophys. & Astropart. Phys (API, FNWI), Acero F., Aloisio R., Amans J., Amato E., Antonelli L. A., Aramo C., Armstrong T., Arqueros F., Asano K., Ashley M., Backes M., Balazs C., Balzer A., Bamba A., Barkov M., Barrio J. A., Benbow W., Bernlöhr K., Beshley V., Bigongiari C., Biland A., Bilinsky A., Bissaldi E., Biteau J., Blanch O., Blasi P., Blazek J., Boisson C., Bonanno G., Bonardi A., Bonavolontà C., Bonnoli G., Braiding C., Brau-Nogué S., Bregeon J., Brown A. M., Bugaev V., Bulgarelli A., Bulik T., Burton M., Burtovoi A., Busetto G., Böttcher M., Cameron R., Capalbi M., Caproni A., Caraveo P., Carosi R., Cascone E., Cerruti M., Chaty S., Chen A., Chen X., Chernyakova M., Chikawa M., Chudoba J., Cohen-Tanugi J., Colafrancesco S., Conforti V., Contreras J. L., Costa A., Cotter G., Covino S., Covone G., Cumani P., Cusumano G., D’Ammando F., D’Urso D., Daniel M., Dazzi F., De Angelis A., De Cesare G., De Franco A., De Frondat F., de Gouveia Dal Pino E. M., De Lisio C., de los Reyes Lopez R., De Lotto B., de Naurois M., De Palma F., Del Santo M., Delgado C., della Volpe D., Di Girolamo T., Di Giulio C., Di Pierro F., Di Venere L., Doro M., Dournaux J., Dumas D., Dwarkadas V., Díaz C., Ebr J., Egberts K., Einecke S., Elsässer D., Eschbach S., Falceta-Goncalves D., Fasola G., Fedorova E., Fernández-Barral A., Ferrand G., Fesquet M., Fiandrini E., Fiasson A., Filipovíc M. D., Fioretti V., Font L., Fontaine G., Franco F. J., Coromina L. Freixa, Fujita Y., Fukui Y., Funk S., Förster A., Gadola A., López R. Garcia, Garczarczyk M., Giglietto N., Giordano F., Giuliani A., Glicenstein J., Gnatyk R., Goldoni P., Grabarczyk T., Graciani R., Graham J., Grandi P., Granot J., Green A. J., Griffiths S., Gunji S., Hakobyan H., Hara S., Hassan T., Hayashida M., Heller M., Helo J. C., Hinton J., Hnatyk B., Huet J., Huetten M., Humensky T. B., Hussein M., Hörandel J., Ikeno Y., Inada T., Inome Y., Inoue S., Inoue T., Inoue Y., Ioka K., Iori M., Jacquemier J., Janecek P., Jankowsky D., Jung I., Kaaret P., Katagiri H., Kimeswenger S., Kimura S., Knödlseder J., Koch B., Kocot J., Kohri K., Komin N., Konno Y., Kosack K., Koyama S., Kraus M., Kubo H., Mezek G. Kukec, Kushida J., Palombara N. La, Lalik K., Lamanna G., Landt H., Lapington J., Laporte P., Lee S., Lees J., Lefaucheur J., Lenain J.-P., Leto G., Lindfors E., Lohse T., Lombardi S., Longo F., Lopez M., Lucarelli F., Luque-Escamilla P. L., López-Coto R., Maccarone M. C., Maier G., Malaguti G., Mandat D., Maneva G., Mangano S., Marcowith A., Martí J., Martínez M., Martínez G., Masuda S., Maurin G., Maxted N., Melioli C., Mineo T., Mirabal N., Mizuno T., Moderski R., Mohammed M., Montaruli T., Moralejo A., Mori K., Morlino G., Morselli A., Moulin E., Mukherjee R., Mundell C., Muraishi H., Murase K., Nagataki S., Nagayoshi T., Naito T., Nakajima D., Nakamori T., Nemmen R., Niemiec J., Nieto D., Nievas-Rosillo M., Nikołajuk M., Nishijima K., Noda K., Nogues L., Nosek D., Novosyadlyj B., Nozaki S., Ohira Y., Ohishi M., Ohm S., Okumura A., Ong R. A., Orito R., Orlati A., Ostrowski M., Oya I., Padovani M., Palacio J., Palatka M., Paredes J. M., Pavy S., Pe’Er A., Persic M., Petrucci P., Petruk O., Pisarski A., Pohl M., Porcelli A., Prandini E., Prast J., Principe G., Prouza M., Pueschel E., Pühlhofer G., Quirrenbach A., Rameez M., Reimer O., Renaud M., Ribó M., Rico J., Rizi V., Rodriguez J., Fernandez G. Rodriguez, Vázquez J. J. Rodríguez, Romano P., Romeo G., Rosado J., Rousselle J., Rowell G., Rudak B., Sadeh I., Safi-Harb S., Saito T., Sakaki N., Sanchez D., Sangiorgi P., Sano H., Santander M., Sarkar S., Sawada M., Schioppa E. J., Schoorlemmer H., Schovanek P., Schussler F., Sergijenko O., Servillat M., Shalchi A., Shellard R. C., Siejkowski H., Sillanpää A., Simone D., Sliusar V., Sol H., Stanič S., Starling R., Stawarz Ł., Stefanik S., Stephan M., Stolarczyk T., Szanecki M., Szepieniec T., Tagliaferri G., Tajima H., Takahashi M., Takeda J., Tanaka M., Tanaka S., Tejedor L. A., Telezhinsky I., Temnikov P., Terada Y., Tescaro D., Teshima M., Testa V., Thoudam S., Tokanai F., Torres D. F., Torresi E., Tosti G., Townsley C., Travnicek P., Trichard C., Trifoglio M., Tsujimoto S., Vagelli V., Vallania P., Valore L., van Driel W., van Eldik C., Vandenbroucke J., Vassiliev V., Vecchi M., Vercellone S., Vergani S., Vigorito C., Vorobiov S., Vrastil M., Acosta M. L. Vázquez, Wagner S. J., Wagner R., Wakely S. P., Walter R., Ward J. E., Watson J. J., Weinstein A., White M., White R., Wierzcholska A., Wilcox P., Williams D. A., Wischnewski R., Wojcik P., Yamamoto T., Yamamoto H., Yamazaki R., Yanagita S., Yang L., Yoshida T., Yoshida M., Yoshiike S., Yoshikoshi T., Zacharias M., Zampieri L., Zanin R., Zavrtanik M., Zavrtanik D., Zdziarski A., Zech A., Zechlin H., Zhdanov V., Ziegler A., Zorn J., Acero, F., Aloisio, R., Amans, J., Amato, E., Antonelli, L. A., Aramo, C., Armstrong, T., Arqueros, F., Asano, K., Ashley, M., Backes, M., Balazs, C., Balzer, A., Bamba, A., Barkov, M., Barrio, J. A., Benbow, W., Bernlöhr, K., Beshley, V., Bigongiari, C., Biland, A., Bilinsky, A., Bissaldi, E., Biteau, J., Blanch, O., Blasi, P., Blazek, J., Boisson, C., Bonanno, G., Bonardi, A., Bonavolontà, C., Bonnoli, G., Braiding, C., Brau Nogué, S., Bregeon, J., Brown, A. M., Bugaev, V., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Böttcher, M., Cameron, R., Capalbi, M., Caproni, A., Caraveo, P., Carosi, R., Cascone, E., Cerruti, M., Chaty, S., Chen, A., Chen, X., Chernyakova, M., Chikawa, M., Chudoba, J., Cohen Tanugi, J., Colafrancesco, S., Conforti, V., Contreras, J. L., Costa, A., Cotter, G., Covino, S., Covone, G., Cumani, P., Cusumano, G., D’Ammando, F., D’Urso, D., Daniel, M., Dazzi, F., De Angelis, A., De Cesare, G., De Franco, A., De Frondat, F., de Gouveia Dal Pino, E. M., De Lisio, C., de los Reyes Lopez, R., De Lotto, B., de Naurois, M., De Palma, F., Del Santo, M., Delgado, C., della Volpe, D., Di Girolamo, T., Di Giulio, C., Di Pierro, F., Di Venere, L., Doro, M., Dournaux, J., Dumas, D., Dwarkadas, V., Díaz, C., Ebr, J., Egberts, K., Einecke, S., Elsässer, D., Eschbach, S., Falceta Goncalves, D., Fasola, G., Fedorova, E., Fernández Barral, A., Ferrand, G., Fesquet, M., Fiandrini, E., Fiasson, A., Filipovíc, M. D., Fioretti, V., Font, L., Fontaine, G., Franco, F. J., Coromina, L. Freixa, Fujita, Y., Fukui, Y., Funk, S., Förster, A., Gadola, A., López, R. Garcia, Garczarczyk, M., Giglietto, N., Giordano, F., Giuliani, A., Glicenstein, J., Gnatyk, R., Goldoni, P., Grabarczyk, T., Graciani, R., Graham, J., Grandi, P., Granot, J., Green, A. J., Griffiths, S., Gunji, S., Hakobyan, H., Hara, S., Hassan, T., Hayashida, M., Heller, M., Helo, J. C., Hinton, J., Hnatyk, B., Huet, J., Huetten, M., Humensky, T. B., Hussein, M., Hörandel, J., Ikeno, Y., Inada, T., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Ioka, K., Iori, M., Jacquemier, J., Janecek, P., Jankowsky, D., Jung, I., Kaaret, P., Katagiri, H., Kimeswenger, S., Kimura, S., Knödlseder, J., Koch, B., Kocot, J., Kohri, K., Komin, N., Konno, Y., Kosack, K., Koyama, S., Kraus, M., Kubo, H., Mezek, G. Kukec, Kushida, J., Palombara, N. La, Lalik, K., Lamanna, G., Landt, H., Lapington, J., Laporte, P., Lee, S., Lees, J., Lefaucheur, J., Lenain, J. P., Leto, G., Lindfors, E., Lohse, T., Lombardi, S., Longo, Francesco, Lopez, M., Lucarelli, F., Luque Escamilla, P. L., López Coto, R., Maccarone, M. C., Maier, G., Malaguti, G., Mandat, D., Maneva, G., Mangano, S., Marcowith, A., Martí, J., Martínez, M., Martínez, G., Masuda, S., Maurin, G., Maxted, N., Melioli, C., Mineo, T., Mirabal, N., Mizuno, T., Moderski, R., Mohammed, M., Montaruli, T., Moralejo, A., Mori, K., Morlino, G., Morselli, A., Moulin, E., Mukherjee, R., Mundell, C., Muraishi, H., Murase, K., Nagataki, S., Nagayoshi, T., Naito, T., Nakajima, D., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Nievas Rosillo, M., Nikołajuk, M., Nishijima, K., Noda, K., Nogues, L., Nosek, D., Novosyadlyj, B., Nozaki, S., Ohira, Y., Ohishi, M., Ohm, S., Okumura, A., Ong, R. A., Orito, R., Orlati, A., Ostrowski, M., Oya, I., Padovani, M., Palacio, J., Palatka, M., Paredes, J. M., Pavy, S., Pe’Er, A., Persic, M., Petrucci, P., Petruk, O., Pisarski, A., Pohl, M., Porcelli, A., Prandini, E., Prast, J., Principe, G., Prouza, M., Pueschel, E., Pühlhofer, G., Quirrenbach, A., Rameez, M., Reimer, O., Renaud, M., Ribó, M., Rico, J., Rizi, V., Rodriguez, J., Fernandez, G. Rodriguez, Vázquez, J. J. Rodríguez, Romano, P., Romeo, G., Rosado, J., Rousselle, J., Rowell, G., Rudak, B., Sadeh, I., Safi Harb, S., Saito, T., Sakaki, N., Sanchez, D., Sangiorgi, P., Sano, H., Santander, M., Sarkar, S., Sawada, M., Schioppa, E. J., Schoorlemmer, H., Schovanek, P., Schussler, F., Sergijenko, O., Servillat, M., Shalchi, A., Shellard, R. C., Siejkowski, H., Sillanpää, A., Simone, D., Sliusar, V., Sol, H., Stanič, S., Starling, R., Stawarz, Ł., Stefanik, S., Stephan, M., Stolarczyk, T., Szanecki, M., Szepieniec, T., Tagliaferri, G., Tajima, H., Takahashi, M., Takeda, J., Tanaka, M., Tanaka, S., Tejedor, L. A., Telezhinsky, I., Temnikov, P., Terada, Y., Tescaro, D., Teshima, M., Testa, V., Thoudam, S., Tokanai, F., Torres, D. F., Torresi, E., Tosti, G., Townsley, C., Travnicek, P., Trichard, C., Trifoglio, M., Tsujimoto, S., Vagelli, V., Vallania, P., Valore, L., van Driel, W., van Eldik, C., Vandenbroucke, J., Vassiliev, V., Vecchi, M., Vercellone, S., Vergani, S., Vigorito, C., Vorobiov, S., Vrastil, M., Acosta, M. L. Vázquez, Wagner, S. J., Wagner, R., Wakely, S. P., Walter, R., Ward, J. E., Watson, J. J., Weinstein, A., White, M., White, R., Wierzcholska, A., Wilcox, P., Williams, D. A., Wischnewski, R., Wojcik, P., Yamamoto, T., Yamamoto, H., Yamazaki, R., Yanagita, S., Yang, L., Yoshida, T., Yoshida, M., Yoshiike, S., Yoshikoshi, T., Zacharias, M., Zampieri, L., Zanin, R., Zavrtanik, M., Zavrtanik, D., Zdziarski, A., Zech, A., Zechlin, H., Zhdanov, V., Ziegler, A., Zorn, J., Acero et al, F., PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Acero, F, Aloisio, R, Amans, J, De Lisio, C, Di Girolamo, T, Valore, L, Covone, G, and Al., Et
Subjects: electron, Supernova Remnants, PARTICLE-ACCELERATION, Cherenkov Telescope Array, Astronomy, leptonic, Telescope Array Experiment, pi, Astrophysics, 01 natural sciences, Supernova Remnant, LARGE-AREA TELESCOPE, Spectral line, spectrum, ISM: individual objects, HESS, Supernova remnant, 010303 astronomy & astrophysics, cosmic ray, Physics, cosmic rays gamma rays: ISM ISM: individual objects (RX J1713.7-3946, G347.3-0.5), spatial distribution, Gamma Ray, Cherenkov radiation, MAGNETIC-FIELD, Gamma ray, COSMIC-RAYS, ISM: individual objects (RX J1713.7–3946, G347.3–0.5), Supernova, cosmic rays, gamma rays: ISM, ISM: individual objects (RX J1713.7-3946, G347.3-0.5), Astronomy and Astrophysics, Space and Planetary Science, gamma ray: emission, G347.3–0.5, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, DIFFUSIVE SHOCK ACCELERATION, Electrónica, Física nuclear, Electricidad, individual objects: RX J1713.7–3946 [ISM], Compton scattering, Gamma Rays, G347.3-0.5), NONTHERMAL, accelerator, X-RAYS, Astrophysics::High Energy Astrophysical Phenomena, INSTABILITY, Cosmic ray, hadronic, GLAST, ISM: individual objects (RX J1713.7-3946, ISM [gamma rays], gas, 0103 physical sciences, supernova, ddc:530, X-ray: emission, GAMMA-RAY EMISSION, AMPLIFICATION, BROAD-BAND EMISSION, MOLECULAR CLOUDS, STREAMING, Astrophysics::Galaxy Astrophysics, Astroparticle physics, 010308 nuclear & particles physics, p: relativistic, Institut für Physik und Astronomie, ASTROFÍSICA, gamma ray: VHE, ddc:520, time dependence, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], RAIOS CÓSMICOS
Abstract: 著者人数: 382名 (JAXA職員: 井上, 芳幸 : 小山, 志勇 : Lee, Shiu-Hang), Accepted: 2017-04-12, 資料番号: SA1170071000
Published: 2017

38. Interplanetary coronal mass ejection observed at STEREO-A, Mars, comet 67P/Churyumov-Gerasimenko, Saturn, and New Horizons en route to Pluto : Comparison of its Forbush decreases at 1.4, 3.1, and 9.9 AU

Author: Witasse, O, Sanchez-Cano, B, Mays, ML, Kajdic, P, Opgenoorth, H, Elliott, HA, Richardson, IG, Zouganelis, I, Zender, J, Wimmer-Schweingruber, RF, Turc, L, Taylor, MGGT, Roussos, E, Rouillard, A, Richter, I, Richardson, JD, Ramstad, R, Provan, G, Posner, A, Plaut, JJ, Odstrcil, D, Nilsson, H, Niemenen, P, Milan, SE, Mandt, K, Lohf, H, Lester, M, Lebreton, J-P, Kuulkers, E, Krupp, N, Koenders, C, James, MK, Intzekara, D, Holmstrom, M, Hassler, DM, Hall, BES, Guo, J, Goldstein, R, Goetz, C, Glassmeier, KH, Genot, V, Evans, H, Espley, J, Edberg, NJT, Dougherty, M, Cowley, SWH, Burch, J, Behar, E, Barabash, S, Andrews, DJ, and Altobelli, N
Subjects: COROTATING INTERACTION REGIONS, COSMIC-RAY MODULATION, Science & Technology, 3-DIMENSIONAL PROPAGATION, PARTICLE-ACCELERATION, INSTRUMENT, ROSETTA PLASMA CONSORTIUM, ENERGETIC PARTICLES, MAGNETIC CLOUDS, Mars, comet 67P, Astronomy & Astrophysics, New Horizons, Saturn, Astronomi, astrofysik och kosmologi, SOLAR-WIND, Physical Sciences, Astronomy, Astrophysics and Cosmology, interplanetary coronal mass ejection, VOYAGER-2 OBSERVATIONS, Forbush decrease
Abstract: We discuss observations of the journey throughout the Solar System of a large interplanetary coronal mass ejection (ICME) that was ejected at the Sun on 14 October 2014. The ICME hit Mars on 17 October, as observed by the Mars Express, Mars Atmosphere and Volatile EvolutioN Mission (MAVEN), Mars Odyssey, and Mars Science Laboratory (MSL) missions, 44h before the encounter of the planet with the Siding-Spring comet, for which the space weather context is provided. It reached comet 67P/Churyumov-Gerasimenko, which was perfectly aligned with the Sun and Mars at 3.1 AU, as observed by Rosetta on 22 October. The ICME was also detected by STEREO-A on 16 October at 1 AU, and by Cassini in the solar wind around Saturn on the 12 November at 9.9AU. Fortuitously, the New Horizons spacecraft was also aligned with the direction of the ICME at 31.6 AU. We investigate whether this ICME has a nonambiguous signature at New Horizons. A potential detection of this ICME by Voyager 2 at 110-111 AU is also discussed. The multispacecraft observations allow the derivation of certain properties of the ICME, such as its large angular extension of at least 116 degrees, its speed as a function of distance, and its magnetic field structure at four locations from 1 to 10 AU. Observations of the speed data allow two different solar wind propagation models to be validated. Finally, we compare the Forbush decreases (transient decreases followed by gradual recoveries in the galactic cosmic ray intensity) due to the passage of this ICME at Mars, comet 67P, and Saturn.
Published: 2017

39. The Origin of the Most Energetic Galactic Cosmic Rays: Supernova Explosions into Massive Star Plasma Winds

Author: Athina Meli, Philipp P. Kronberg, Eun-Suk Seo, Michael L. Allen, and Peter L. Biermann
Subjects: RADIO-SOURCES, PARTICLE-ACCELERATION, VERY-HIGH-ENERGY, lcsh:Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, massive star supernovae, lcsh:QB1-991, NONLINEAR AMPLIFICATION, cosmic rays, cosmic ray knee and ankle, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Red supergiant, 010306 general physics, Supernova remnant, 010303 astronomy & astrophysics, COMPACT, Astrophysics::Galaxy Astrophysics, Physics, MAXIMUM ENERGY, IA SUPERNOVAE, MAGNETIC-FIELD, FLUX-DENSITY VARIATIONS, Astronomy and Astrophysics, Galaxy, Black hole, Stars, Supernova, Physics and Astronomy, HOT-SPOTS, DIFFUSIVE SHOCK ACCELERATION, Supergiant
Abstract: We propose that the high energy Cosmic Ray particles up to the upturn commonly called the ankle, from around the spectral turn-down commonly called the knee, mostly come from Blue Supergiant star explosions. At the upturn, i.e., the ankle, Cosmic Rays probably switch to another source class, most likely extragalactic sources. To show this we recently compiled a set of Radio Supernova data where we compute the magnetic field, shock speed and shock radius. This list included both Blue and Red Supergiant star explosions; both data show the same magnetic field strength for these two classes of stars despite very different wind densities and velocities. Using particle acceleration theory at shocks, those numbers can be transformed into characteristic ankle and knee energies. Without adjusting any free parameters both of these observed energies are directly indicated by the supernova data. In the next step in the argument, we use the Supernova Remnant data of the starburst galaxy M82. We apply this analysis to Blue Supergiant star explosions: The shock will race to their outer edge with a magnetic field that is observed to follow over several orders of magnitude B ( r ) × r ∼ c o n s t . , with in fact the same magnetic field strength for such stellar explosions in our Galaxy, and other galaxies including M82. The speed is observed to be ∼0.1 c out to about 10 16 cm radius in the plasma wind. The Supernova shock can run through the entire magnetic plasma wind region at full speed all the way out to the wind-shell, which is of order parsec scale in M82. We compare and identify the Cosmic Ray spectrum in other galaxies, in the starburst galaxy M82 and in our Galaxy with each other; we suggest how Blue Supergiant star explosions can provide the Cosmic Ray particles across the knee and up to the ankle energy range. The data from the ISS-CREAM (Cosmic Ray Energetics and Mass Experiment at the International Space Station) mission will test this cosmic ray concept which is reasonably well grounded in two independent radio supernova data sets. The next step in developing our understanding will be to obtain future more accurate Cosmic Ray data near to the knee, and to use unstable isotopes of Cosmic Ray nuclei at high energy to probe the “piston„ driving the explosion. We plan to incorporate these data with the physics of the budding black hole which is probably forming in each of these stars.
Published: 2019

40. Acceleration of plasma in current sheet during substorm dipolarizations in the Earth's magnetotail: Comparison of different mechanisms

Author: Elena Grigorenko, Patrick W. Daly, Victor Popov, Dominique Delcourt, A. A. Petrukovich, Lev Zelenyi, Elena A. Kronberg, Helmi Malova, Elena Parkhomenko, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Lomonosov Moscow State University (MSU), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Max Planck Institute for Solar System Research (MPS), and Max-Planck-Gesellschaft
Subjects: DYNAMICS, FRONTS, PARTICLE-ACCELERATION, Magnetosphere, Electron, ELECTRIC-FIELD, 01 natural sciences, 010305 fluids & plasmas, Ion, Current sheet, MAGNETIC RECONNECTION, 0103 physical sciences, BURSTS, 010306 general physics, Physics, HEAVY-ION ACCELERATION, CLUSTER, Plasma, Condensed Matter Physics, Plasma acceleration, Magnetic field, Particle acceleration, STOCHASTIC FLUCTUATIONS, [SDU]Sciences of the Universe [physics], SIMULATION, Atomic physics
Abstract: This work is devoted to the investigation of particle acceleration during magnetospheric dipolarizations. A numerical model is presented taking into account the four scenarios of plasma acceleration that can be realized: (A) total dipolarization with characteristic time scales of ≈3 min; (B) single peak value of the normal magnetic component B z occurring on the time scale of less than 1 min; (C) a sequence of rapid jumps of B z interpreted as the passage of a chain of multiple dipolarization fronts (DFs); and (D) the simultaneous action of mechanism (C) followed by the consequent enhancement of electric and magnetic fluctuations with the small characteristic time scale ≤1 s. In a frame of the model, we have obtained and analyzed the energy spectra of four plasma populations: electrons e−, protons H+, helium He+, and oxygen O+ ions, accelerated by the above-mentioned processes (A)–(D). It is shown that O+ ions can be accelerated mainly due to the mechanism (A); H+ and He+ ions (and to some extent electrons) can be more effectively accelerated due to the mechanism (C) than the single dipolarization (B). It is found that high-frequency electric and magnetic fluctuations accompanying multiple DFs (D) can strongly accelerate electrons e− and really weakly influence other populations of plasma. The results of modeling demonstrated clearly the distinguishable spatial and temporal resonance character of particle acceleration processes. The maximum particle energies depending on the scale of the magnetic acceleration region and the value of the magnetic field are estimated. The shapes of energy spectra are discussed.This work is devoted to the investigation of particle acceleration during magnetospheric dipolarizations. A numerical model is presented taking into account the four scenarios of plasma acceleration that can be realized: (A) total dipolarization with characteristic time scales of ≈3 min; (B) single peak value of the normal magnetic component B z occurring on the time scale of less than 1 min; (C) a sequence of rapid jumps of B z interpreted as the passage of a chain of multiple dipolarization fronts (DFs); and (D) the simultaneous action of mechanism (C) followed by the consequent enhancement of electric and magnetic fluctuations with the small characteristic time scale ≤1 s. In a frame of the model, we have obtained and analyzed the energy spectra of four plasma populations: electrons e−, protons H+, helium He+, and oxygen O+ ions, accelerated by the above-mentioned processes (A)–(D). It is shown that O+ ions can be accelerated mainly due to the mechanism (A); H+ and He+ ions (and to some exten...
Published: 2019

41. Universal behaviour of shock precursors in the presence of efficient cosmic ray acceleration

Author: Brian Reville and Anthony R. Bell
Subjects: PARTICLE-ACCELERATION, Field (physics), Astrophysics::High Energy Astrophysical Phenomena, INSTABILITY, FOS: Physical sciences, Cosmic ray, SN 1006, 01 natural sciences, Acceleration, cosmic rays, 0103 physical sciences, Radiative transfer, SPECTRA, Diffusion (business), 010306 general physics, 010303 astronomy & astrophysics, acceleration of particles, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, SUPERNOVA-REMNANTS, OBLIQUE SHOCKS, MAGNETIC-FIELD, AMPLIFICATION, Astronomy and Astrophysics, plasmas, SIMULATIONS, Magnetic field, Computational physics, Particle acceleration, Bohm diffusion, Classical mechanics, instabilities, Space and Planetary Science, TURBULENCE, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The self-consistent interaction between energetic particles and self-generated hydromagnetic waves in a cosmic-ray pressure dominated plasma is considered. Using a three-dimensional hybrid MHD-kinetic code, which utilises a spherical harmonic expansion of the Vlasov-Fokker-Planck equation, high resolution simulations of the magnetic field growth including feedback on the cosmic rays are carried out. It is found that for shocks with high cosmic-ray acceleration efficiency, the magnetic fields become highly disorganised, resulting in near isotropic diffusion, independent of the initial orientation of the ambient magnetic field. The possibility of sub-Bohm diffusion is demonstrated for parallel shocks, while the diffusion coefficient approaches the Bohm limit from below for oblique shocks. This universal behaviour suggests that Bohm diffusion in the root mean squared field inferred from observation may provide a realistic estimate for the maximum energy acceleration timescale in young supernova remnants. Although disordered, the magnetic field is not self-similar suggesting non-uniform energy dependent behaviour of the energetic particle transport in the precursor. Possible indirect radiative signatures of cosmic-ray driven magnetic field amplification are discussed., Comment: Accepted for publication in MNRAS
Published: 2016

42. Microscopic Processes In Global Relativistic Jets Containing Helical Magnetic Fields

Author: Martin Pohl, Dieter H. Hartmann, Aake Nordlund, Jacek Niemiec, A. Meli, José L. Gómez, Ioana Dutan, Yosuke Mizuno, Asaf Pe'er, H. Sol, Philip E. Hardee, Ken-Ichi Nishikawa, Oleh Kobzar, Jacob Trier Frederiksen, Consejo Superior de Investigaciones Científicas (España), National Aeronautics and Space Administration (US), European Research Council, German Research Foundation, Kavli Institute for Theoretical Physics, and National Science Centre (Poland)
Subjects: PARTICLE-ACCELERATION, lcsh:Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Electron, Kink instability, Kinetic energy, 01 natural sciences, kink instability, Computer Science::Digital Libraries, Instability, CURRENT-DRIVEN INSTABILITY, SHOCKS, lcsh:QB1-991, Astrophysical jet, 0103 physical sciences, SPATIAL GROWTH, particle-in-cell simulations, kinetic instabilities, KELVIN-HELMHOLTZ INSTABILITY, 010306 general physics, 010303 astronomy & astrophysics, helical magnetic fields, relativistic jets, global jets, High Energy Astrophysical Phenomena (astro-ph.HE), GAMMA-RAY BURSTS, Physics, Jet (fluid), Institut für Physik und Astronomie, Astronomy and Astrophysics, Plasma, astronomy_astrophysics, Magnetic field, Weibel instability, WEIBEL INSTABILITY, TheoryofComputation_MATHEMATICALLOGICANDFORMALLANGUAGES, Physics and Astronomy, SIMULATION, ddc:520, Computer Science::Programming Languages, Mathematisch-Naturwissenschaftliche Fakultät, Atomic physics, EMISSION, Astrophysics - High Energy Astrophysical Phenomena, GENERATION
Abstract: Galaxies 4(4), 38 (2016). doi:10.3390/galaxies4040038, In the study of relativistic jets one of the key open questions is their interaction with the environment on the microscopic level. Here, we study the initial evolution of both electron–proton ( e$^−$ – p$^+$ ) and electron–positron ( e$^{±}$ ) relativistic jets containing helical magnetic fields, focusing on their interaction with an ambient plasma. We have performed simulations of “global” jets containing helical magnetic fields in order to examine how helical magnetic fields affect kinetic instabilities such as the Weibel instability, the kinetic Kelvin-Helmholtz instability (kKHI) and the Mushroom instability (MI). In our initial simulation study these kinetic instabilities are suppressed and new types of instabilities can grow. In the e$^−$ – p$^+$ jet simulation a recollimation-like instability occurs and jet electrons are strongly perturbed. In the e$^{±}$ jet simulation a recollimation-like instability occurs at early times followed by a kinetic instability and the general structure is similar to a simulation without helical magnetic field. Simulations using much larger systems are required in order to thoroughly follow the evolution of global jets containing helical magnetic fields., Published by MDPI, Basel
Published: 2016

43. Suprathermal electrons at Saturn's bow shock

Author: Masters, A., Sulaiman, A. H., Sergis, N., Stawarz, L., Coates, A. J., Dougherty, M. K., Fujimoto, Masaki, The Royal Society, Science and Technology Facilities Council (STFC), and Science and Technology Facilities Council
Subjects: Shock wave, HIGH-ENERGY, PARTICLE-ACCELERATION, 010504 meteorology & atmospheric sciences, Whistler, 0306 Physical Chemistry (Incl. Structural), observational [methods], Astrophysics, 0305 Organic Chemistry, 01 natural sciences, Physics - Space Physics, Saturn, COLLISIONLESS SHOCKS, Bow shock (aerodynamics), 010303 astronomy & astrophysics, acceleration of particles, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Earth and Planetary Astrophysics (astro-ph.EP), SUPERNOVA-REMNANTS, PLASMA, Shock (fluid dynamics), MAGNETIC-FIELD, shock waves, UPSTREAM, Particle acceleration, Solar wind, solar wind, Physical Sciences, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Astronomy & Astrophysics, 0103 physical sciences, data analysis [methods], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Science & Technology, Astronomy and Astrophysics, plasmas, methods: data analysis, Space Physics (physics.space-ph), 0201 Astronomical And Space Sciences, Space and Planetary Science, WAVE, INJECTION, Astrophysics - Earth and Planetary Astrophysics
Abstract: The leading explanation for the origin of galactic cosmic rays is particle acceleration at the shocks surrounding young supernova remnants (SNRs), although crucial aspects of the acceleration process are unclear. The similar collisionless plasma shocks frequently encountered by spacecraft in the solar wind are generally far weaker (lower Mach number) than these SNR shocks. However, the Cassini spacecraft has shown that the shock standing in the solar wind sunward of Saturn (Saturn's bow shock) can occasionally reach this high-Mach number astrophysical regime. In this regime Cassini has provided the first in situ evidence for electron acceleration under quasi-parallel upstream magnetic conditions. Here we present the full picture of suprathermal electrons at Saturn's bow shock revealed by Cassini. The downstream thermal electron distribution is resolved in all data taken by the low-energy electron detector (CAPS-ELS, 18 keV) measured a suprathermal electron signature at 31 of 508 crossings, where typically only the lowest energy channels (, 22 pages, 5 figures. Accepted for publication in ApJ
Published: 2016

44. Multiple current sheet systems in the outer heliosphere: Energy release and turbulence

Author: David Burgess, Lorenzo Matteini, and Peter Gingell
Subjects: ANOMALOUS COSMIC-RAYS, PARTICLE-ACCELERATION, astro-ph.SR, 0306 Physical Chemistry (Incl. Structural), Population, FOS: Physical sciences, BLUNT TERMINATION SHOCK, Astronomy & Astrophysics, 7. Clean energy, 01 natural sciences, Instability, 0305 Organic Chemistry, Current sheet, KINETIC INSTABILITIES, Physics - Space Physics, MAGNETIC RECONNECTION, 0103 physical sciences, VOYAGER 1, Sun: heliosphere, 010306 general physics, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, education.field_of_study, Science & Technology, turbulence, Astronomy and Astrophysics, Magnetic reconnection, Mechanics, Space Physics (physics.space-ph), Particle acceleration, Solar wind, HELIOSHEATH, 0201 Astronomical And Space Sciences, Astrophysics - Solar and Stellar Astrophysics, solar wind, 13. Climate action, Space and Planetary Science, physics.space-ph, SOLAR-WIND, Physical Sciences, Physics::Space Physics, PROTON TEMPERATURE ANISOTROPY, Heliospheric current sheet, PLASMA TURBULENCE, Heliosphere
Abstract: In the outer heliosphere, beyond the solar wind termination shock, it is expected that the warped heliospheric current sheet forms a region of closely-packed, multiple, thin current sheets. Such a system may be subject to the ion-kinetic tearing instability, and hence generate magnetic islands and hot populations of ions associated with magnetic reconnection. Reconnection processes in this environment have important implications for local particle transport, and for particle acceleration at reconnection sites and in turbulence. We study this complex environment by means of three-dimensional hybrid simulations over long time scales, in order to capture the evolution from linear growth of the tearing instability to a fully developed turbulent state at late times. The final state develops from the highly ordered initial state via both forward and inverse cascades. Component and spectral anisotropy in the magnetic fluctuations is present when a guide field is included. The inclusion of a population of new-born interstellar pickup protons does not strongly affect these results. Finally, we conclude that reconnection between multiple current sheets can act as an important source of turbulence in the outer heliosphere, with implications for energetic particle acceleration and propagation., Comment: Accepted for publication in The Astrophysical Journal, March 21, 2016
Published: 2016
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45. Multiwavelength study of quiescent states of MRK 421 with unprecedented hard x-ray coverage provided by NuSTAR in 2013

Author: Baloković, M., Paneque, D., Madejski, G., Furniss, A., Chiang, J., the NuSTAR team, Ajello, M., Alexander, D. M., Barret, D., Blandford, R., Boggs, S. E., Christensen, F. E., Craig, W. W., Forster, K., Giommi, P., Grefenstette, B. W., Hailey, C. J., Harrison, F. A., Hornstrup, A., Kitaguchi, T., Koglin, J. E., Madsen, K. K., Mao, P. H., Miyasaka, H., Mori, K., Perri, M., Pivovaroff, M. J., Simonetta Puccetti, Rana, V., Stern, D., Tagliaferri, G., Urry, C. M., Westergaard, N. J., Zhang, W. W., Zoglauer, A., Veritas, The Collaboration, Archambault, S., Archer, A. A., Barnacka, A., Benbow, W., Bird, R., Buckley, J., Bugaev, V., Cerruti, M., Chen, X., Ciupik, L., Connolly, M. P., Cui, W., Dickinson, H. J., Dumm, J., Eisch, J. D., Falcone, A., Feng, Q., Finley, J. P., Fleischhack, H., Fortson, L., Griffin, S., Griffiths, S. T., Grube, J., Gyuk, G., Huetten, M., Haakansson, N., Holder, J., Humensky, T. B., Johnson, C. A., Kaaret, P., Kertzman, M., Khassen, Y., Kieda, D., Krause, M., Krennrich, F., Lang, M. J., Maier, G., Mcarthur, S., Meagher, K., Moriarty, P., Nelson, T., Nieto, D., Ong, R. A., Park, N., Pohl, M., Popkow, A., Pueschel, E., Reynolds, P. T., Richards, G. T., Roache, E., Santander, M., Sembroski, G. H., Shahinyan, K., Smith, A. W., Staszak, D., Telezhinsky, I., Todd, N. W., Tucci, J. V., Tyler, J., Vincent, S., Weinstein, A., Wilhelm, A., Williams, D. A., Zitzer, B., Magic, The Collaboration, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., Barres Almeida, U., Barrio, J., Becerra González, J., Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., Angelis, A., Lotto, B., Oña Wilhelmi, E. D., Delgado Mendez, C., Di Pierro, F., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giammaria, P., Eisenacher, D., Godinović, N., González Muñoz, A., Guberman, D., Hahn, A., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Coto, R., López-Oramas, A., Lorenz, E., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas-Rosillo, M., Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palacio, S., Palatiello, M., Paoletti, R., Paredes, J. M., Paredes-Fortuny, X., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Saito, T., Satalecka, K., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Takalo, L. O., Takami, H., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zanin, R., Collaborators, External, Perkins, J., Verrecchia, F., Leto, C., Böttcher, M., Villata, M., Raiteri, C. M., Acosta-Pulido, J. A., Bachev, R., Berdyugin, A., Blinov, D. A., Carnerero, M. I., Chen, W. P., Chinchilla, P., Damljanovic, G., Eswaraiah, C., Grishina, T. S., Ibryamov, S., Jordan, B., Jorstad, S. G., Joshi, M., Kopatskaya, E. N., Kurtanidze, O. M., Kurtanidze, S. O., Larionova, E. G., Larionova, L. V., Larionov, V. M., Latev, G., Lin, H. C., Marscher, A. P., Mokrushina, A. A., Morozova, D. A., Nikolashvili, M. G., Semkov, E., Strigachev, A., Troitskaya, Yu V., Troitsky, I. S., Vince, O., Barnes, J., Güver, T., Moody, J. W., Sadun, A. C., Sun, S., Hovatta, T., Richards, J. L., Max-Moerbeck, W., Readhead, A. C., Lähteenmäki, A., Tornikoski, M., Tammi, J., Ramakrishnan, V., Reinthal, R., Angelakis, E., Fuhrmann, L., Myserlis, I., Karamanavis, V., Sievers, A., Ungerechts, H., Zensus, J. A., Universitat de Barcelona, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, Glawion , D., ~, Baloković, M., Paneque, D., Madejski, G., Furniss, A., Chiang, J., Ajello, M., Alexander, D. M., Barret, D., Blandford, R. D., Boggs, S. E., Christensen, F. E., Craig, W. W., Forster, K., Giommi, P., Grefenstette, B., Hailey, C., Harrison, F. A., Hornstrup, A., Kitaguchi, T., Koglin, J. E., Madsen, K. K., Mao, P. H., Miyasaka, H., Mori, K., Perri, M., Pivovaroff, M. J., Puccetti, S., Rana, V., Stern, D., Tagliaferri, G., Urry, C. M., Westergaard, N. J., Zhang, W. W., Zoglauer, A., Archambault, S., Archer, A., Barnacka, A., Benbow, W., Bird, R., Buckley, J. H., Bugaev, V., Cerruti, M., Chen, X., Ciupik, L., Connolly, M. P., Cui, W., Dickinson, H. J., Dumm, J., Eisch, J. D., Falcone, A., Feng, Q., Finley, J. P., Fleischhack, H., Fortson, L., Griffin, S., Griffiths, S. T., Grube, J., Gyuk, G., Huetten, M., Håkansson, N., Holder, J., Humensky, T. B., Johnson, C. A., Kaaret, P., Kertzman, M., Khassen, Y., Kieda, D., Krause, M., Krennrich, F., Lang, M. J., Maier, G., Mcarthur, S., Meagher, K., Moriarty, P., Nelson, T., Nieto, D., Ong, R. A., Park, N., Pohl, M., Popkow, A., Pueschel, E., Reynolds, P. T., Richards, G. T., Roache, E., Santander, M., Sembroski, G. H., Shahinyan, K., Smith, A. W., Staszak, D., Telezhinsky, I., Todd, N. W., Tucci, J. V., Tyler, J., Vincent, S., Weinstein, A., Wilhelm, A., Williams, D. A., Zitzer, B., Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., De Almeida, U. Barre, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., De Ońa Wilhelmi, E., Mendez, C. Delgado, Di Pierro, F., Prester, D. Domini, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Fernández Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Terrats, D. Garrido, Gaug, M., Giammaria, P., Glawion, D., Godinović, N., González Muñoz, A., Guberman, D., Hahn, A., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., López Oramas, A., Lorenz, E., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nieva, Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palacio, J., Palatiello, Michele, Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Persic, M., Poutanen, J., Moroni, P. G. Prada, Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Garcia, J. Rodriguez, Saito, T., Satalecka, K., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Takalo, L., Takami, H., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zanin, R., Perkins, J., Verrecchia, F., Leto, C., Böttcher, M., Villata, M., Raiteri, C. M., Acosta Pulido, J. A., Bachev, R., Berdyugin, A., Blinov, D. A., Carnerero, M. I., Chen, W. P., Chinchilla, P., Damljanovic, G., Eswaraiah, C., Grishina, T. S., Ibryamov, S., Jordan, B., Jorstad, S. G., Joshi, M., Kopatskaya, E. N., Kurtanidze, O. M., Kurtanidze, S. O., Larionova, E. G., Larionova, L. V., Larionov, V. M., Latev, G., Lin, H. C., Marscher, A. P., Mokrushina, A. A., Morozova, D. A., Nikolashvili, M. G., Semkov, E., Smith, P. S., Strigachev, A., Troitskaya, Y. u. V., Troitsky, I. S., Vince, O., Barnes, J., Güver, T., Moody, J. W., Sadun, A. C., Sun, S., Hovatta, T., Richards, J. L., Max Moerbeck, W., Readhead, A. C. R., Lähteenmäki, A., Tornikoski, M., Tammi, J., Ramakrishnan, V., Reinthal, R., Angelakis, E., Fuhrmann, L., Myserlis, I., Karamanavis, V., Sievers, A., Ungerechts, H., and Zensus, J. A.
Subjects: galaxie [X-rays], Photon, PARTICLE-ACCELERATION, ELECTRON ACCELERATION, BACKGROUND-RADIATION, Astrophysics, Electron, Nonthermal, BL Lacertae objects: individual (Markarian 421), galaxies: active, gamma rays: general, radiation mechanisms: nonthermal, X-rays: galaxies, 01 natural sciences, individual: Markarian 421 [BL Lacertae objects], LARGE-AREA TELESCOPE, individual (Markarian 421) [BL Lacertae objects], law.invention, Raigs gamma, law, MAGNETIC RECONNECTION, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Large area telescope, TEV BLAZARS, gamma, rays: general, ACTIVE GALACTIC NUCLEI, BL LACERTAE OBJECTS, LAC OBJECTS, CORRELATED VARIABILITY, Synchrotron, galaxies [X-rays], Spectral energy distribution, Degree of polarization, Electrónica, Física nuclear, Raigs X, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object, Astronomy and Astrophysics, Space and Planetary Science, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, Particle acceleration, general [Gamma rays], FOS: Physical sciences, Photon energy, 0103 physical sciences, X-rays, Radiation mechanisms, BL Lacertae objects, individual, Markarian 421, galaxies, active, gamma rays, general, radiation mechanisms, nonthermal, 010308 nuclear & particles physics, Gamma rays, Astronomy and Astrophysic, nonthermal [Radiation mechanisms], Light curve, Galaxies, Galàxies, Background radiation, ddc:520
Abstract: The astrophysical journal 819(2), 156 (2016). doi:10.3847/0004-637X/819/2/156, We present coordinated multiwavelength observations of the bright, nearby BL Lacertae object Mrk 421 taken in 2013 January–March, involving GASP-WEBT, Swift, NuSTAR, Fermi-LAT, MAGIC, VERITAS, and other collaborations and instruments, providing data from radio to very high energy (VHE) γ-ray bands. NuSTAR yielded previously unattainable sensitivity in the 3–79 keV range, revealing that the spectrum softens when the source is dimmer until the X-ray spectral shape saturates into a steep ${\rm{\Gamma }}\approx 3$ power law, with no evidence for an exponential cutoff or additional hard components up to ~80 keV. For the first time, we observed both the synchrotron and the inverse-Compton peaks of the spectral energy distribution (SED) simultaneously shifted to frequencies below the typical quiescent state by an order of magnitude. The fractional variability as a function of photon energy shows a double-bump structure that relates to the two bumps of the broadband SED. In each bump, the variability increases with energy, which, in the framework of the synchrotron self-Compton model, implies that the electrons with higher energies are more variable. The measured multi band variability, the significant X-ray-to-VHE correlation down to some of the lowest fluxes ever observed in both bands, the lack of correlation between optical/UV and X-ray flux, the low degree of polarization and its significant (random) variations, the short estimated electron cooling time, and the significantly longer variability timescale observed in the NuSTAR light curves point toward in situ electron acceleration and suggest that there are multiple compact regions contributing to the broadband emission of Mrk 421 during low-activity states., Published by Univ.11032, Chicago, Ill. [u.a.]
Published: 2016

46. Evolution of global relativistic jets : collimations and expansion with kKHI and the Weibel instability

Author: Martin Pohl, Jacek Niemiec, P. E. Hardee, Åke Nordlund, Ioana Duţan, A. Meli, José L. Gómez, Helene Sol, Yosuke Mizuno, K-I Nishikawa, Jacob Trier Frederiksen, Dieter H. Hartmann, Asaf Pe'er, National Science Foundation (US), National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), European Research Council, and German Research Foundation
Subjects: ACTIVE GALACTIC NUCLEI, Acceleration of particles, PARTICLE-ACCELERATION, Radiation mechanisms: non-thermal, Event horizon, Astrophysics::High Energy Astrophysical Phenomena, CIRCULAR-POLARIZATION, FOS: Physical sciences, Stars: jets, 01 natural sciences, Astrophysical jet, PLASMA SHOCKS, 0103 physical sciences, COLLISIONLESS SHOCKS, KELVIN-HELMHOLTZ INSTABILITY, 010306 general physics, 010303 astronomy & astrophysics, Sun: magnetic fields, acceleration of particles, relativistic processes, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, GAMMA-RAY BURSTS, EXTERNAL MEDIUM, Relativistic processes, Institut für Physik und Astronomie, Astronomy and Astrophysics, plasmas, non-thermal [radiation mechanisms], Weibel instability, jets [stars], Physics and Astronomy, magnetic fields [Sun], MAGNETIC-FIELD GENERATION, Space and Planetary Science, Plasmas, ddc:520, Physics::Accelerator Physics, RADIATION, Christian ministry, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, Humanities
Abstract: The astrophysical journal 820(2), 94 (2016). doi:10.3847/0004-637X/820/2/94, In the study of relativistic jets one of the key open questions is their interaction with the environment. Here we study the initial evolution of both electron–proton (${e}^{\mbox{-}}-{p}^{+}$) and electron–positron (e$^{±}$) relativistic jets, focusing on their lateral interaction with ambient plasma. We follow the evolution of toroidal magnetic fields generated by both the kinetic Kelvin–Helmholtz and Mushroom instabilities. For an ${e}^{\mbox{-}}-{p}^{+}$ jet, the induced magnetic field collimates the jet and electrons are perpendicularly accelerated. As the instabilities saturate and subsequently weaken, the magnetic polarity switches from clockwise to counterclockwise in the middle of the jet. For an e$^{±}$ jet, we find strong mixing of electrons and positrons with the ambient plasma, resulting in the creation of a bow shock. The merging of current filaments generates density inhomogeneities that initiate a forward shock. Strong jet–ambient plasma mixing prevents a full development of the jet (on the scale studied), revealing evidence for both jet collimation and particle acceleration in the forming bow shock. Differences in the magnetic field structure generated by ${e}^{\mbox{-}}-{p}^{+}$ and e± jets may contribute to the polarization properties of the observed emission in AGN jets and gamma-ray bursts., Published by Univ.11032, Chicago, Ill. [u.a.]
Published: 2016

47. OBSERVATIONS OF THE SHELL-TYPE SUPERNOVA REMNANT CASSIOPEIA A AT TeV ENERGIES WITH VERITAS

Author: R. G. Wagner, Gernot Maier, Stephanie Wissel, C. M. Hui, M. J. Lang, S. P. Wakely, T. B. Humensky, Daniel Gall, B. R. Smith, Geza Gyuk, Y. Butt, D. Boltuch, J. E. Ward, A. Cesarini, John L. Quinn, R. Dickherber, A. J.R. Weinstein, M. Bautista, S. Thibadeau, S. McArthur, V. A. Acciari, D. S. Hanna, David Kieda, J. P. Finley, R. A. Ong, Thomas Weisgarber, N. Karlsson, Jamie Holder, A. McCann, Martin Pohl, Wystan Benbow, T. C. Weekes, M. Beilicke, D. Steele, R. Guenette, V. Bugaev, S. LeBohec, F. Krennrich, E. Roache, P. Fortin, H. J. Rose, J. Grube, A. Furniss, S. P. Swordy, J. Millis, K. Byrum, Matthew J.A. Wood, Tulun Ergin, P. Moriarty, Nicola Galante, J. S. Perkins, M. Kertzman, S. J. Fegan, S. Vincent, M. Schroedter, G. H. Sembroski, P. T. Reynolds, Lucy Fortson, A. Varlotta, Wei Cui, D. Huang, M. Theiling, P. Cogan, T. Aune, Y. C. Chow, V. V. Vassiliev, P. Kaaret, G. Finnegan, A. W. Smith, C. Duke, J. H. Buckley, A. Konopelko, G. H. Gillanders, T. Arlen, L. Ciupik, E. Aliu, H. Krawczynski, K. Ragan, S. M. Bradbury, A. Cannon, D. Pandel, and M. McCutcheon
Subjects: Photon, Astrophysics::High Energy Astrophysical Phenomena, cosmic-rays, Shell (structure), Flux, Astrophysics, 01 natural sciences, Power law, cosmic rays, 0103 physical sciences, air cerenkov telescopes, crab-nebula, Supernova remnant, ism: individual objects (cassiopeia a), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Cherenkov radiation, acceleration of particles, Physics, magnetic-fields, electron acceleration, particle-acceleration, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy and Astrophysics, gamma-ray emission, Cassiopeia A, gamma rays: ism, rx j1713.7-3946, 13. Climate action, Space and Planetary Science, ism: supernova remnants, a supernova, magic telescope
Abstract: We report on observations of very high energy gamma rays from the shell-type supernova remnant (SNR) Cassiopeia A with the Very Energetic Radiation Imaging Telescope Array System stereoscopic array of four imaging atmospheric Cherenkov telescopes in Arizona. The total exposure time for these observations is 22 hr, accumulated between September and November of 2007. The gamma-ray source associated with the SNR Cassiopeia A was detected above 200 GeV with a statistical significance of 8.3 sigma. The estimated integral flux for this gamma-ray source is about 3% of the Crab-Nebula flux. The photon spectrum is compatible with a power law dN/dE proportional to E(-Gamma) with an index Gamma = 2.61 +/- 0.24(stat) +/- 0.2(sys). The data are consistent with a point-like source. We provide a detailed description of the analysis results and discuss physical mechanisms that may be responsible for the observed gamma-ray emission.
Published: 2010

48. Variable Very High Energy γ‐Ray Emission from Markarian 501

Author: J. Albert, E. Aliu, H. Anderhub, P. Antoranz, A. Armada, C. Baixeras, J. A. Barrio, H. Bartko, D. Bastieri, J. K. Becker, W. Bednarek, K. Berger, C. Bigongiari, A. Biland, R. K. Bock, P. Bordas, V. Bosch‐Ramon, T. Bretz, I. Britvitch, M. Camara, E. Carmona, A. Chilingarian, J. A. Coarasa, S. Commichau, J. L. Contreras, J. Cortina, M. T. Costado, V. Curtef, V. Danielyan, F. Dazzi, A. De Angelis, C. Delgado, R. de los Reyes, B. De Lotto, E. Domingo‐Santamaria, D. Dorner, M. Doro, M. Errando, M. Fagiolini, D. Ferenc, E. Fernandez, R. Firpo, J. Flix, M. V. Fonseca, L. Font, M. Fuchs, N. Galante, R. J. Garcia‐Lopez, M. Garczarczyk, M. Gaug, M. Giller, F. Goebel, D. Hakobyan, M. Hayashida, T. Hengstebeck, A. Herrero, D. Hohne, J. Hose, D. Hrupec, C. C. Hsu, P. Jacon, T. Jogler, R. Kosyra, D. Kranich, R. Kritzer, A. Laille, E. Lindfors, S. Lombardi, F. Longo, J. Lopez, M. Lopez, E. Lorenz, P. Majumdar, G. Maneva, K. Mannheim, O. Mansutti, M. Mariotti, M. Martinez, D. Mazin, C. Merck, M. Meucci, M. Meyer, J. M. Miranda, R. Mirzoyan, S. Mizobuchi, A. Moralejo, D. Nieto, K. Nilsson, J. Ninkovic, E. Ona‐Wilhelmi, N. Otte, I. Oya, D. Paneque, M. Panniello, R. Paoletti, J. M. Paredes, M. Pasanen, D. Pascoli, F. Pauss, R. Pegna, M. Persic, L. Peruzzo, A. Piccioli, E. Prandini, N. Puchades, A. Raymers, W. Rhode, M. Ribo, J. Rico, M. Rissi, A. Robert, S. Rugamer, A. Saggion, T. Saito, A. Sanchez, P. Sartori, V. Scalzotto, V. Scapin, R. Schmitt, T. Schweizer, M. Shayduk, K. Shinozaki, S. N. Shore, N. Sidro, A. Sillanpaa, D. Sobczynska, A. Stamerra, L. S. Stark, L. Takalo, F. Tavecchio, P. Temnikov, D. Tescaro, M. Teshima, D. F. Torres, N. Turini, H. Vankov, V. Vitale, R. M. Wagner, T. Wibig, W. Wittek, F. Zandanel, R. Zanin, J. Zapatero, J., Albert, E., Aliu, H., Anderhub, P., Antoranz, A., Armada, C., Baixera, J. A., Barrio, H., Bartko, D., Bastieri, J. K., Becker, W., Bednarek, K., Berger, C., Bigongiari, A., Biland, R. K., Bock, P., Borda, V., Bosch Ramon, T., Bretz, I., Britvitch, M., Camara, E., Carmona, A., Chilingarian, J. A., Coarasa, S., Commichau, J. L., Contrera, J., Cortina, M. T., Costado, V., Curtef, V., Danielyan, F., Dazzi, A. D., Angeli, C., Delgado, R. D. L., Reye, B. D., Lotto, E., Domingo Santamaria, D., Dorner, M., Doro, M., Errando, M., Fagiolini, D., Ferenc, E., Fernandez, R., Firpo, J., Flix, M. V., Fonseca, L., Font, M., Fuch, N., Galante, R. J., Garcia Lopez, M., Garczarczyk, M., Gaug, M., Giller, F., Goebel, D., Hakobyan, M., Hayashida, T., Hengstebeck, A., Herrero, D., Hohne, J., Hose, D., Hrupec, C. C., Hsu, P., Jacon, T., Jogler, R., Kosyra, D., Kranich, R., Kritzer, A., Laille, E., Lindfor, S., Lombardi, Longo, Francesco, J., Lopez, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, K., Mannheim, O., Mansutti, M., Mariotti, M., Martinez, D., Mazin, C., Merck, M., Meucci, M., Meyer, J. M., Miranda, R., Mirzoyan, S., Mizobuchi, A., Moralejo, D., Nieto, K., Nilsson, J., Ninkovic, E., Ona Wilhelmi, N., Otte, I., Oya, D., Paneque, M., Panniello, R., Paoletti, J. M., Parede, M., Pasanen, D., Pascoli, F., Pau, R., Pegna, M., Persic, L., Peruzzo, A., Piccioli, E., Prandini, N., Puchade, A., Raymer, W., Rhode, M., Ribo, J., Rico, M., Rissi, A., Robert, S., Rugamer, A., Saggion, T., Saito, A., Sanchez, P., Sartori, V., Scalzotto, V., Scapin, R., Schmitt, T., Schweizer, M., Shayduk, K., Shinozaki, S. N., Shore, N., Sidro, A., Sillanpaa, D., Sobczynska, A., Stamerra, L. S., Stark, L., Takalo, F., Tavecchio, P., Temnikov, D., Tescaro, M., Teshima, D. F., Torre, N., Turini, H., Vankov, V., Vitale, R. M., Wagner, T., Wibig, W., Wittek, F., Zandanel, R., Zanin, and J., Zapatero
Subjects: PARTICLE-ACCELERATION, Photon, ACTIVE GALACTIC NUCLEI, BL-LAC OBJECTS, CHERENKOV TELESCOPE SYSTEM, LOG-PARABOLIC SPECTRA, 23 DAY PERIODICITY, BLACK-HOLE MODELS, X-RAY, MKN 501, MULTIWAVELENGTH OBSERVATIONS, Flux, Electron, Astrophysics, 01 natural sciences, Spectral line, Luminosity, law.invention, law, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Gamma ray, Active Galactic Nuclei, Astronomy and Astrophysics, MAGIC telescope, Very High Energy Gamma-ray Astronomy, Space and Planetary Science, Electrónica, Física nuclear, Electricidad, Markarian 501, BL Lac, AGN, VHE gamma-ray, imaging air Cherenkov telescope, MAGIC, Flare
Abstract: The blazar Markarian 501 (Mrk 501) was observed at energies above 0.10 TeV with the MAGIC telescope from May through July 2005. The high sensitivity of the instrument enabled the determination of the flux and spectrum of the source on a night-by-night basis. Throughout our observational campaign, the flux from Mrk 501 was found to vary by an order of magnitude. Intra-night flux variability with flux-doubling times down to 2 minutes was observed during the two most active nights, namely June 30 and July 9. These are the fastest flux variations ever observed in Mrk 501. The ~20-minute long flare of July 9 showed an indication of a 4 +/- 1 min time delay between the peaks of F(1.2 TeV), which may indicate a progressive acceleration of electrons in the emitting plasma blob. The flux variability was quantified for several energy ranges, and found to increase with the energy of the gamma-ray photons. The spectra hardened significantly with increasing flux, and during the two most active nights, a spectral peak was clearly detected at 0.43 +/- 0.06 TeV and 0.25 +/- 0.07 TeV, respectively for June 30 and July 9. There is no evidence of such spectral feature for the other nights at energies down to 0.10 TeV, thus suggesting that the spectral peak is correlated with the source luminosity. These observed characteristics could be accommodated in a Synchrotron-Self-Compton (SSC) framework in which the increase in gamma-ray flux is produced by a freshly injected (high energy) electron population.
Published: 2007

49. HIGH BRIGHTNESS LASER INDUCED MULTI-MEV ELECTRON/PROTON SOURCES

Author: Danilo Giulietti, Paolo Tomassini, P. Monot, L. Labate, Ph. Martin, E. Breschi, M. Calvetti, Angelo Schiavi, Oswald Willi, Marco Borghesi, Marco Galimberti, P. De Olivera, Satyabrata Kar, L. A. Gizzi, Petra Koester, Antonio Giulietti, Lorenzo Romagnani, T. Ceccotti, and S. Bertolucci
Subjects: Chirped pulse amplification, Nuclear and High Energy Physics, PARTICLE-ACCELERATION, Proton, PLASMA INTERACTION, Electron, DOSIMETRIC MEASUREMENTS, WAKEFIELD EXPERIMENT, PROTON-BEAMS, ALGORITHM, PULSES, Collimated light, law.invention, Acceleration, Optics, law, Electric field, Physics, business.industry, Astronomy and Astrophysics, Plasma, Laser, Atomic and Molecular Physics, and Optics, Physics::Accelerator Physics, business
Abstract: The chirped pulse amplification (CPA) technique has opened new perspectives in the radiation-matter interaction studies using ultra-short laser pulses at ultra-relativistic intensities. In particular the original idea, proposed by Tajima and Dawson, of accelerating electrons by the huge electric fields of plasma waves which develop in the wake of a laser pulse propagating in a plasma, become feasible. Some laboratories all over the world have produced by such a technique collimated electron busts of hundreds of MeV along acceleration lengths of a few hundreds of microns. In other experiments, using thin solid targets, intense bursts of energetic protons have been at the same time detected. The proton acceleration mechanism is essentially based on the Coulomb force appearing at the thin solid target surface as a consequence of the previous escape of the energetic electrons from the target. In the paper some experimental results will be presented as well as the opportunities the INFN PLASMONX project will offer in this research field at LNF.
Published: 2007

50. First NuSTAR Observations of Mrk 501 within a Radio to TeV Multi-Instrument Campaign

Author: Furniss, A., Noda, K., Boggs, S., Chiang, J., Christensen, F., Craig, W., Giommi, P., Hailey, C., Harisson, F., Madejski, G., Nalewajko, K., PERRI, Matteo, Stern, D., Urry, M., VERRECCHIA, Francesco, Zhang, W., NuSTAR Team, Ahnen, M. L., ANTONELLI, Lucio Angelo, Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., Barres de Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., COVINO, Stefano, Da Vela, P., Dazzi, F., De Angelis, A., De Caneva, G., De Lotto, B., de Oña Wilhelmi, E., Delgado Mendez, C., Di Pierro, F., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giammaria, P., Godinović, N., González Muñoz, A., Guberman, D., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kellermann, H., Kodani, K., Konno, Y., Kubo, H., Kushida, J., LA BARBERA, ANTONINO, Lelas, D., Lewandowska, N., Lindfors, E., LOMBARDI, Saverio, Longo, F., López, M., López-Coto, R., López-Oramas, A., Lorenz, E., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Nishijima, K., Orito, R., Overkemping, A., PAIANO, Simona, Palacio, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes-Fortuny, X., Persic, M., Poutanen, J., Prada Moroni, P. G., PRANDINI, ELISA, Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Saito, T., Saito, K., Satalecka, K., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., STAMERRA, Antonio, Steinbring, T., Strzys, M., Takalo, L., Takami, H., TAVECCHIO, Fabrizio, Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Verguilov, V., Vovk, I., Will, M., Zanin, R., MAGIC Collaboration, Archer, A., Benbow, W., Bird, R., Biteau, J., Bugaev, V., Cardenzana, J. V., Cerruti, M., Chen, X., Ciupik, L., Connolly, M. P., Cui, W., Dickinson, H. J., Dumm, J., Eisch, J. D., Falcone, A., Feng, Q., Finley, J. P., Fleischhack, H., Fortin, P., Fortson, L., Gerard, L., Gillanders, G. H., Griffin, S., Griffiths, S. T., Grube, J., Gyuk, G., Håkansson, N., Holder, J., Humensky, T. B., Johnson, C. A., Kaaret, P., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Lang, M. J., Lin, T. T. Y., Maier, G., McArthur, S., McCann, A., Meagher, K., Moriarty, P., Mukherjee, R., Nieto, D., O'Faoláin de Bhróithe, A., Ong, R. A., Park, N., Petry, D., Pohl, M., Popkow, A., Ragan, K., Ratliff, G., Reyes, L. C., Reynolds, P. T., Richards, G. T., Roache, E., Santander, M., Sembroski, G. H., Shahinyan, K., Staszak, D., Telezhinsky, I., Tucci, J. V., Tyler, J., Vassiliev, V. V., Wakely, S. P., Weiner, O. M., Weinstein, A., Wilhelm, A., Williams, D. A., Zitzer, B., VERITAS Collaboration, Vince, O., Fuhrmann, L., Angelakis, E., Karamanavis, V., Myserlis, I., Krichbaum, T. P., Zensus, J. A., Ungerechts, H., Sievers, A., F-Gamma Consortium, The, Bachev, R., Böttcher, M., Chen, W. P., Damljanovic, G., Eswaraiah, C., Güver, T., Hovatta, T., Hughes, Z., Ibryamov, S. I., Joner, M. D., Jordan, B., Jorstad, S. G., Joshi, M., Kataoka, J., Kurtanidze, O. M., Kurtanidze, S. O., Lähteenmäki, A., Latev, G., Lin, H. C., Larionov, V. M., Mokrushina, A. A., Morozova, D. A., Nikolashvili, M. G., RAITERI, Claudia Maria, Ramakrishnan, V., Readhead, A. C. R., Sadun, A. C., Sigua, L. A., Semkov, E. H., Strigachev, A., Tammi, J., Tornikoski, M., Troitskaya, Y. V., Troitsky, I. S., VILLATA, Massimo, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, Universitat de Barcelona, Furniss, A., Noda, K., Boggs, S., Chiang, J., Christensen, F., Craig, W., Giommi, P., Hailey, C., Harisson, F., Madejski, G., Nalewajko, K., Perri, M., Stern, D., Urry, M., Verrecchia, F., Zhang, W., Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., Barres De Almeida, U., J., A. Barrio, Becerra González, J., Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Caneva, G., De Lotto, B., De Oña Wilhelmi, E., Delgado Mendez, C., Di Pierro, F., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Fernández Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giammaria, P., Godinović, N., González Muñoz, A., Guberman, D., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kellermann, H., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lewandowska, N., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., López Oramas, A., Lorenz, E., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Nakajima, D., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nilsson, K., Nishijima, K., Orito, R., Overkemping, A., Paiano, S., Palacio, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Saito, T., Saito, K., Satalecka, K., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpä, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Takalo, L., Takami, H., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Verguilov, V., Vovk, I., Will, M., Zanin, R., Archer, A., Benbow, W., Bird, R., Biteau, J., Bugaev, V., Cardenzana, J. V., Cerruti, M., Chen, X., Ciupik, L., Connolly, M. P., Cui, W., Dickinson, H. J., Dumm, J., Eisch, J. D., Falcone, A., Feng, Q., Finley, J. P., Fleischhack, H., Fortin, P., Fortson, L., Gerard, L., Gillanders, G. H., Griffin, S., Griffiths, S. T., Grube, J., Gyuk, G., Håkansson, N., Holder, J., Humensky, T. B., Johnson, C. A., Kaaret, P., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Lang, M. J., Lin, T. T. Y., Maier, G., Mcarthur, S., Mccann, A., Meagher, K., Moriarty, P., Mukherjee, R., Nieto, D., O'Faoláin De Bhróithe, A., Ong, R. A., Park, N., Petry, D., Pohl, M., Popkow, A., Ragan, K., Ratliff, G., Reyes, L. C., Reynolds, P. T., Richards, G. T., Roache, E., Santander, M., Sembroski, G. H., Shahinyan, K., Staszak, D., Telezhinsky, I., Tucci, J. V., Tyler, J., Vassiliev, V. V., Wakely, S. P., Weiner, O. M., Weinstein, A., Wilhelm, A., Williams, D. A., Zitzer, B., Vince, O., Fuhrmann, L., Angelakis, E., Karamanavis, V., Myserlis, I., Krichbaum, T. P., Zensus, J. A., Ungerechts, H., Sievers, A., Bachev, R., Böttcher, M., Chen, W. P., Damljanovic, G., Eswaraiah, C., Güver, T., Hovatta, T., Hughes, Z., Ibryamov, S. I., Joner, M. D., Jordan, B., Jorstad, S. G., Joshi, M., Kataoka, J., Kurtanidze, O. M., Kurtanidze, S. O., Lähteenmäki, A., Latev, G., Lin, H. C., Larionov, V. M., Mokrushina, A. A., Morozova, D. A., Nikolashvili, M. G., Raiteri, C. M., Ramakrishnan, V., A. C., R. Readhead, Sadun, A. C., Sigua, L. A., Semkov, E. H., Strigachev, A., Tammi, J., Tornikoski, M., Troitskaya, Y. V., Troitsky, I. S., Villata, M., ~, and 24420530 - Böttcher, Markus
Subjects: galaxie [X-rays], Astrophysics, galaxies BL Lacs, galaxies individual (Markarian 501), X-rays, 01 natural sciences, Luminosity, law.invention, bl lacertae objects, law, MAGIC (telescope), individual: Markarian 501 [galaxies], 010303 astronomy & astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), BL Lacertae objects: general, galaxies: individual: Markarian 501, X-rays: galaxies, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, fermi-lat, galaxies [X-rays], large-area telescope, BL Lacertae objects: general, galaxies: individual (Markarian 501), X-rays: galaxies, individual (Markarian 501) [galaxies], Spectral energy distribution, Electrónica, Física nuclear, Individual (Markarian 501), Raigs X, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Nuclear and High Energy Physics, BL Lac object, multiwavelength observations, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Optical telescope, Telescope, 0103 physical sciences, crab-nebula, Blazar, galaxies: individual (markarian 501), particle-acceleration, 010308 nuclear & particles physics, general [BL Lacertae objects], galaxies: individual: Markarian 501, Institut für Physik und Astronomie, Astronomy and Astrophysics, gamma-ray emission, Galaxies, Galàxies, x-ray, Space and Planetary Science, ddc:520, magic telescope, log-parabolic spectra, Fermi Gamma-ray Space Telescope
Abstract: We report on simultaneous broadband observations of the TeV-emitting blazar Markarian 501 between 1 April and 10 August 2013, including the first detailed characterization of the synchrotron peak with Swift and NuSTAR. During the campaign, the nearby BL Lac object was observed in both a quiescent and an elevated state. The broadband campaign includes observations with NuSTAR, MAGIC, VERITAS, the Fermi Large Area Telescope (LAT), Swift X-ray Telescope and UV Optical Telescope, various ground-based optical instruments, including the GASP-WEBT program, as well as radio observations by OVRO, Mets\"ahovi and the F-Gamma consortium. Some of the MAGIC observations were affected by a sand layer from the Saharan desert, and had to be corrected using event-by-event corrections derived with a LIDAR (LIght Detection And Ranging) facility. This is the first time that LIDAR information is used to produce a physics result with Cherenkov Telescope data taken during adverse atmospheric conditions, and hence sets a precedent for the current and future ground-based gamma-ray instruments. The NuSTAR instrument provides unprecedented sensitivity in hard X-rays, showing the source to display a spectral energy distribution between 3 and 79 keV consistent with a log-parabolic spectrum and hard X-ray variability on hour timescales. None (of the four extended NuSTAR observations) shows evidence of the onset of inverse-Compton emission at hard X-ray energies. We apply a single-zone equilibrium synchrotron self-Compton model to five simultaneous broadband spectral energy distributions. We find that the synchrotron self-Compton model can reproduce the observed broadband states through a decrease in the magnetic field strength coinciding with an increase in the luminosity and hardness of the relativistic leptons responsible for the high-energy emission., Comment: Accepted for publication in ApJ
Published: 2015

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