Search

Your search keyword '"K. V., Sokolovsky"' showing total 4 results
Start Over Author "K. V., Sokolovsky" Topic 0103 physical sciences
4 results on '"K. V., Sokolovsky"'

1. Radio Transients in the Era of Multi-Messenger Astrophysics

Author

R. P. Fender, P. A. Woudt, M. Giroletti, M. L. Graham, G. E. Anderson, I. Andreoni, M. Caleb, D. Coppejans, S. Corbel, K. V. Sokolovsky, and Benjamin Stappers

Subjects
Square kilometre array, Exploit, 010308 nuclear & particles physics, Space and Planetary Science, Computer science, 0103 physical sciences, Real-time computing, Cataclysmic variable star, The Renaissance, Astronomy and Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences
Abstract

Radio emission from astrophysical transients allows us to derive calorimetry of kinetic feedback and detailed imaging in ways that are not possible at other wavelengths, and as such it forms an important part of the multi-messenger follow-ups of these events. The field is burgeoning, with a renaissance of interest in accretion, stellar explosions and jetted supernovæ, alongside newer classes of phenomena such as fast radio bursts and tidal disruption events. The purpose of this workshop was to discuss the infrastructure and techniques for detecting, identifying and probing radio transients, with a particular focus on how best to exploit transient alerts from multi-messenger facilities. We examined the type of transient alerts those facilities will broadcast, and methods for following them up, such as rapid-response triggering and shadowing. In break-out groups, participants chose a science question related to a particular radio transient type or class and discussed whether the planned transient strategies and observing techniques on the Square Kilometre Array will be adequate to address the particular question. The classes they chose included fast radio bursts, supernovæ, cataclysmic variable and unknown transients. Any proposed adaptation or suggestion was relayed to a panel of experts for further discussion. The second part of the workshop concentrated on the application of long baseline interferometry for detecting and measuring radio transients.

Published
2017
Full Text
View/download PDF

2. The Hubble Catalog of Variables (HCV)

Author

K. V. Sokolovsky, A. Z. Bonanos, P. Gavras, M. Yang, D. Hatzidimitriou, M. I. Moretti, A. Karampelas, I. Bellas-Velidis, Z. Spetsieri, E. Pouliasis, I. Georgantopoulos, V. Charmandaris, K. Tsinganos, N. Laskaris, G. Kakaletris, A. Nota, D. Lennon, C. Arviset, B. C. Whitmore, T. Budavari, R. Downes, S. Lubow, A. Rest, L. Strolger, and R. White

Subjects
010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

The Hubble Source Catalog (HSC) combines lists of sources detected on images obtained with the WFPC2, ACS and WFC3 instruments aboard the Hubble Space Telescope (HST) available in the Hubble Legacy Archive. The catalog contains time-domain information with about two million of its sources detected with the same instrument and filter in at least five HST visits. The Hubble Catalog of Variables (HCV) project aims to identify HSC sources showing significant brightness variations. A magnitude-dependent threshold in the median absolute deviation of photometric measurements (an outlier-resistant measure of lightcurve scatter) is adopted as the variability-detection statistic. It is supplemented with a cut in $\chi_{\rm red}^2$ that removes sources with large photometric errors. A pre-processing procedure involving bad image identification, outlier rejection and computation of local magnitude zero-point corrections is applied to HSC lightcurves before computing the variability detection statistic. About 52000 HSC sources are identified as candidate variables, among which 7800 show variability in more than one filter. Visual inspection suggests that $\sim 70\%$ of the candidates detected in multiple filters are true variables while the remaining $\sim 30\%$ are sources with aperture photometry corrupted by blending, imaging artifacts or image processing anomalies. The candidate variables have AB magnitudes in the range 15-27$^{m}$ with the median 22$^{m}$. Among them are the stars in our own and nearby galaxies as well as active galactic nuclei., Comment: 4 pages, 1 figure, proceedings of the IAU Symposium 339 Southern Horizons in Time-Domain Astronomy, 13-17 November 2017, Stellenbosch, South Africa

Published
2018

3. The simultaneous low state spectral energy distribution of 1ES 2344+514 from radio to very high energies

Author

MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, Spain), L. A. Antonelli(INAF National Institute for Astrophysics, Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, Italy), M. Asensio(Universidad Complutense, Spain), M. Backes(Technische Universität Dortmund, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, München, Germany), J. A. Barrio(Universidad Complutense, Spain), W. Bednarek(University of Łódź, Poland), K. Berger(Inst. de Astrofísica de Canarias, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, Spain), R. K. Bock(Max-Planck-Institut für Physik, München, Germany), A. Boller(ETH Zurich, Switzerland), S. Bonnefoy(Universidad Complutense, Spain), G. Bonnoli(INAF National Institute for Astrophysics, Rome, Italy), D. Borla Tridon(Max-Planck-Institut für Physik, München, Germany), T. Bretz(Universität Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Spain), A. Carosi(INAF National Institute for Astrophysics, Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, Tenerife, Spain), J. L. Contreras(Universidad Complutense, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, Spain), L. Cossio(Università di Udine, and INFN Trieste, Italy), S. Covino(INAF National Institute for Astrophysics, Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, Italy), F. Dazzi(Università di Udine, and INFN Trieste, Italy), A. De Angelis(Università di Udine, and INFN Trieste, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Spain), M. Doert(Technische Universität Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Dorner(Universität Würzburg, Germany), M. Doro(Universitat Autònoma de Barcelona, Spain), D. Eisenacher(Universität Würzburg, Germany), D. Elsaesser(Universität Würzburg, Germany), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), M. V. Fonseca(Universidad Complutense, Spain), L. Font(Universitat Autònoma de Barcelona, Spain), C. Fruck(Max-Planck-Institut für Physik, München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, Tenerife, Spain), M. Garczarczyk(Inst. de Astrofísica de Canarias, Tenerife, Spain), D. Garrido Terrats(Universitat Autònoma de Barcelona, Spain), M. Gaug(Universitat Autònoma de Barcelona, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, Tenerife, Spain), J. Hose(Max-Planck-Institut für Physik, München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), F. Jankowski(Deutsches Elektronen-Synchrotron), V. Kadenius(Tuorla Observatory, University of Turku, Finland), S. Klepser(IFAE, Edifici Cn., Campus UAB, Spain), M. L. Knoetig(Max-Planck-Institut für Physik, München, Germany), T. Krähenbühl(ETH Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), E. Leonardo(Università di Siena, and INFN Pisa, Italy), N. Lewandowska(Universität Würzburg, Germany), E. Lindfors(Tuorla Observatory, University of Turku, Finland), S. Lombardi(INAF National Institute for Astrophysics, Rome, Italy), M. López(Universidad Complutense, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, Spain), E. Lorenz(Max-Planck-Institut für Physik, München, Germany), I. Lozano(Universidad Complutense, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, Italy), K. Mannheim(Universität Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, Spain), J. Masbou(Università di Padova and INFN Padova, Italy), D. Mazin(Max-Planck-Institut für Physik, München, Germany), M. Meucci(Università di Siena, and INFN Pisa, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, München, Germany), J. Moldón(Universitat de Barcelona), A. Moralejo(IFAE, Edifici Cn., Campus UAB, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Max-Planck-Institut für Physik, München, Germany), A. Niedzwiecki(University of Łódź, Poland), D. Nieto(Universidad Complutense, Spain), K. Nilsson(Tuorla Observatory, University of Turku, Finland), N. Nowak(Max-Planck-Institut für Physik, München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), S. Paiano(Università di Padova and INFN Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, Italy), D. Paneque(Max-Planck-Institut für Physik, München, Germany), R. Paoletti(Università di Siena, and INFN Pisa, Italy), J. M. Paredes(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, Italy), M. Persic(Università di Udine, and INFN Trieste, Italy), M. Pilia(Università dell'Insubria, Como, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, Italy), E. Prandini(Università di Padova and INFN Padova, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), I. Reichardt(IFAE, Edifici Cn., Campus UAB, Spain), R. Reinthal(Tuorla Observatory, University of Turku, Finland), W. Rhode(Technische Universität Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(ICREA, Barcelona, Spain), S. Rügamer(Universität Würzburg, Germany), A. Saggion(Università di Padova and INFN Padova, Italy), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), T. Y. Saito(Max-Planck-Institut für Physik, München, Germany), M. Salvati(INAF National Institute for Astrophysics, Rome, Italy), K. Satalecka(Universidad Complutense, Spain), V. Scalzotto(Università di Padova and INFN Padova, Italy), V. Scapin(Universidad Complutense, Spain), C. Schultz(Università di Padova and INFN Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, Italy), A. Sillanpää(Tuorla Observatory, University of Turku, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Sobczynska(University of Łódź, Poland), F. Spanier(Universität Würzburg, Germany), S. Spiro(INAF National Institute for Astrophysics, Rome, Italy), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, Spain), A. Stamerra(Università di Siena, and INFN Pisa, Italy), B. Steinke(Max-Planck-Institut für Physik, München, Germany), J. Storz(Universität Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), L. Takalo(Tuorla Observatory, University of Turku, Finland), H. Takami(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), F. Tavecchio(INAF National Institute for Astrophysics, Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, München, Germany), O. Tibolla(Universität Würzburg, Germany), D. F. Torres(ICREA, Barcelona, Spain), T. Toyama(Max-Planck-Institut für Physik, München, Germany), A. Treves(Università dell'Insubria, Como, Italy), M. Uellenbeck(Technische Universität Dortmund, Germany), P. Vogler(ETH Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, München, Germany), Q. Weitzel(ETH Zurich, Switzerland), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), The MAGIC Collaboration(Università di Trieste, and INFN Trieste, Italy), F. Longo(Università di Trieste, and INFN Trieste, Italy), F. Lucarelli(Agenzia Spaziale Italiana), C. Pittori(Agenzia Spaziale Italiana), S. Vercellone(INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Italy), for the AGILE team(Università di Padova and INFN Padova, Italy), D. Bastieri(Università di Padova and INFN Padova, Italy), C. Sbarra(INFN Padova, Italy), for the Fermi-LAT Collaboration(Max-Planck-Institut für Radioastronomie, Germany), E. Angelakis(Max-Planck-Institut für Radioastronomie, Germany), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Germany), I. Nestoras(Max-Planck-Institut für Radioastronomie, Germany), T. P. Krichbaum(Max-Planck-Institut für Radioastronomie, Germany), A. Sievers(Instituto de Radio Astronoma Milimétrica, Spain), J. A. Zensus(Max-Planck-Institut für Radioastronomie, Germany), for the F-GAMMA program(Crimean Astrophysical Observatory, Ukraine), K. A. Antonyuk(Crimean Astrophysical Observatory, Ukraine), W. Baumgartner(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), A. Berduygin(Tuorla Observatory, University of Turku, Finland), M. Carini(Department of Physics and Astronomy, Western Kentucky University, USA), K. Cook(Department of Physics and Astronomy, Western Kentucky University, USA), N. Gehrels(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), M. Kadler(Universität Würzburg, Germany), Yu. A. Kovalev(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), Y. Y. Kovalev(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), F. Krauss(Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany), H. A. Krimm(Universities Space Research Association, Columbia, MD 21044, USA), A. Lähteenmäki(Aalto University Metsähovi Radio Observatory, Finland), M. L. Lister(Department of Physics, Purdue University, USA), W. Max-Moerbeck(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, USA), M. Pasanen(Tuorla Observatory, University of Turku, Finland), A. B. Pushkarev(Pulkovo Observatory, St. Petersburg, Russia), A. C. S. Readhead(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, USA), J. L. Richards(Department of Physics, Purdue University, USA), J. Sainio(Tuorla Observatory, University of Turku, Finland), D. N. Shakhovskoy(Crimean Astrophysical Observatory, Ukraine), K. V. Sokolovsky(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), M. Tornikoski(Aalto University Metsähovi Radio Observatory, Finland), J. Tueller(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), M. Weidinger(Theoretische Physik IV, Ruhr-Universität Bochum, Germany), J. Wilms(Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany), Anne Lähteenmäki Group, Aalto-yliopisto, Aalto University, Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Politecnico di Milano [Milan] (POLIMI), Universitá degli Studi dell’Insubria, Technische Universität Dortmund [Dortmund] (TU), IEEC-CSIC, Departamento de Ecología e Hidrología, Universidad de Murcia, Deutsches Elektronen-Synchrotron [Zeuthen] (DESY), Helmholtz-Gemeinschaft = Helmholtz Association, Laboratoire de l'Accélérateur Linéaire (LAL), 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 d'études dynamiques et structurales de la sélectivité (LEDSS), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), 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, Departament d'Astronomia i Meteorologia [Barcelona] (DAM), Universitat de Barcelona (UB), Universita degli Studi di Padova, Universidad de Cantabria [Santander], Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), Instituto de Biotecnología, Departamento de Biología Molecular de Plantas, UNAM, Institute for Physical Research (IPR), National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA), Netherlands Institute for Radio Astronomy (ASTRON), 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), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), INAF-Cagliari Astronomical Observatory, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, 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), Dept. of Physics, Institut de Ciencies del Cosmos (ICCUB), Kao Group, Centre de Recherches sur les Macromolécules Végétales (CERMAV), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Optoelectronic Research Centre, University of Southampton, Department of Chemistry, Oulu, INAF - Osservatorio Astronomico di Brera (OAB), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Università degli Studi di Udine - University of Udine [Italie], Universita degli studi di Napoli 'Parthenope' [Napoli], Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Vecteurs - Infections tropicales et méditerranéennes (VITROME), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut de Recherche Biomédicale des Armées (IRBA), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), DAAA, ONERA, Université Paris Saclay (COmUE) [Meudon], ONERA-Université Paris-Saclay, University of Bath [Bath], Waves and Solitons LLC, 918 W. Windsong Dr., Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), J., Aleksić, L. A., Antonelli, P., Antoranz, M., Asensio, M., Backe, U., Barres de Almeida, J. A., Barrio, W., Bednarek, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, S., Bonnefoy, G., Bonnoli, D., Borla Tridon, T., Bretz, E., Carmona, A., Carosi, D., Carreto Fidalgo, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, P., Da Vela, F., Dazzi, A., De Angeli, G., De Caneva, B., De Lotto, C., Delgado Mendez, M., Doert, A., Domínguez, D., Dominis Prester, D., Dorner, M., Doro, D., Eisenacher, D., Elsaesser, D., Ferenc, M. V., Fonseca, L., Font, C., Fruck, R. J., García López, M., Garczarczyk, D., Garrido Terrat, M., Gaug, G., Giavitto, N., Godinović, A., González Muñoz, S. R., Gozzini, A., Hadamek, D., Hadasch, A., Herrero, J., Hose, D., Hrupec, F., Jankowski, V., Kadeniu, S., Klepser, M. L., Knoetig, T., Krähenbühl, J., Krause, J., Kushida, A., La Barbera, D., Lela, E., Leonardo, N., Lewandowska, E., Lindfor, S., Lombardi, M., López, R., López Coto, A., López Orama, E., Lorenz, I., Lozano, M., Makariev, K., Mallot, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, B., Marcote, M., Mariotti, M., Martínez, J., Masbou, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, J., Moldón, A., Moralejo, P., Munar Adrover, D., Nakajima, A., Niedzwiecki, D., Nieto, K., Nilsson, N., Nowak, R., Orito, S., Paiano, M., Palatiello, D., Paneque, R., Paoletti, J. M., Parede, S., Partini, M., Persic, M., Pilia, F., Prada, P. G., Prada Moroni, E., Prandini, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribó, J., Rico, S., Rügamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, S. N., Shore, A., Sillanpää, J., Sitarek, I., Snidaric, D., Sobczynska, F., Spanier, S., Spiro, V., Stamatescu, A., Stamerra, B., Steinke, J., Storz, S., Sun, T., Surić, L., Takalo, H., Takami, F., Tavecchio, P., Temnikov, T., Terzić, D., Tescaro, M., Teshima, O., Tibolla, D. F., Torre, T., Toyama, A., Treve, M., Uellenbeck, P., Vogler, R. M., Wagner, Q., Weitzel, F., Zandanel, R., Zanin, Longo, Francesco, F., Lucarelli, C., Pittori, S., Vercellone, D., Bastieri, C., Sbarra, E., Angelaki, L., Fuhrmann, I., Nestora, T. P., Krichbaum, A., Siever, J. A., Zensu, K. A., Antonyuk, W., Baumgartner, A., Berduygin, M., Carini, K., Cook, N., Gehrel, M., Kadler, Kovalev, Y. u. A., Y. Y., Kovalev, F., Krau, H. A., Krimm, A., Lähteenmäki, M. L., Lister, W., Max Moerbeck, M., Pasanen, A. B., Pushkarev, A. C. S., Readhead, J. L., Richard, J., Sainio, D. N., Shakhovskoy, K. V., Sokolovsky, M., Tornikoski, J., Tueller, M., Weidinger, J., Wilms, UAM. Departamento de Física Teórica, Universitá degli Studi dell’Insubria = University of Insubria [Varese] (Uninsubria), 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 Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Università degli Studi di Padova = University of Padua (Unipd), 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), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut de Recherche Biomédicale des Armées [Brétigny-sur-Orge] (IRBA), Universitat Autònoma de Barcelona [Barcelona] (UAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universitat de València (UV), Helmholtz-Gemeinschaft, National Institute for Nuclear Physics (INFN), National Academy of Sciences of Armenia, The Netherlands Institute for Radio Astronomy (ASTRON), 7990-AA Dwingeloo, Netherlands, Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), 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), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), INAF-OAB, and DAAA, ONERA, Université Paris Saclay [Meudon]

Subjects
galaxies [Gamma rays], Radiation mechanisms: non-thermal, Flux, Astrophysics, 01 natural sciences, LARGE-AREA TELESCOPE, law.invention, law, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], BL Lacertae objects: individual: 1ES 2344+514, MAGIC (telescope), 010303 astronomy & astrophysics, galaxies: active, BL Lacerae objects: individual: 1ES 2344+514, gamma rays: galaxies, X-rays: individuals: 1ES 2344+514, radiation mechanisms: non-thermal, ComputingMilieux_MISCELLANEOUS, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, ACTIVE GALACTIC NUCLEI, BL-LACERTAE OBJECTS, GAMMA-RAY EMISSION, SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS, SELF-COMPTON MODEL, X-RAY, LAC OBJECTS, RELATIVISTIC JETS, MARKARIAN 501, Gamma ray, non-thermal [radiation mechanisms], active [galaxies], astro-ph.CO, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Flare, Astrophysics - Cosmology and Nongalactic Astrophysics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, galaxie [gamma rays], 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, Light curve, individual: 1ES 2344+514 [BL Lacertae objects], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], galaxies [gamma-rays], Space and Planetary Science, ddc:520, individuals: 1ES 2344+514 [X-rays], Fermi Gamma-ray Space Telescope
Abstract

Astronomy and Astrophysics 556 (2013): A67 reproduced with permission from Astronomy and Astrophysics, Context. BL Lacertae objects are variable at all energy bands on time scales down to minutes. To construct and interpret their spectral energy distribution (SED), simultaneous broad-band observations are mandatory. Up to now, the number of objects studied during such campaigns is very limited and biased towards high flux states. Aims.We present the results of a dedicated multi-wavelength study of the high-frequency peaked BL Lacertae (HBL) object and known TeV emitter 1ES 2344+514 by means of a pre-organised campaign. Methods.The observations were conducted during simultaneous visibility windows of MAGIC and AGILE in late 2008. The measurements were complemented by Metsähovi, RATAN-600, KVA+Tuorla, Swift and VLBA pointings. Additional coverage was provided by the ongoing long-term F-GAMMA and MOJAVE programs, the OVRO 40-m and CrAO telescopes as well as the Fermi satellite. The obtained SEDs are modelled using a one-zone as well as a self-consistent two-zone synchrotron self-Compton model. Results. 1ES 2344+514 was found at very low flux states in both X-rays and very high energy gamma rays. Variability was detected in the low frequency radio and X-ray bands only, where for the latter a small flare was observed. The X-ray flare was possibly caused by shock acceleration characterised by similar cooling and acceleration time scales. MOJAVE VLBA monitoring reveals a static jet whose components are stable over time scales of eleven years, contrary to previous findings. There appears to be no significant correlation between the 15 GHz and R-band monitoring light curves. The observations presented here constitute the first multi-wavelength campaign on 1ES 2344+514 from radio to VHE energies and one of the few simultaneous SEDs during low activity states. The quasi-simultaneous Fermi-LAT data poses some challenges for SED modelling, but in general the SEDs are described well by both applied models. The resulting parameters are typical for TeV emitting HBLs. Consequently it remains unclear whether a so-called quiescent state was found in this campaign, 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 CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, 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 AGILE Mission is funded by the Italian Space Agency (ASI), with scientific and programmatic participation by the Italian Institute of Astrophysics (INAF) and the Italian Institute of Nuclear Physics (INFN). Research partially supported through the ASI grants no. I/089/06/2 and I/042/10/0. 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

Published
2013
Full Text
View/download PDF

4. The Brightest Gamma-Ray Flaring Blazar in the Sky: AGILE and Multi-wavelength Observations of 3C 454.3 During 2010 November

Author

Sofia O. Kurtanidze, Valeri M. Larionov, M. F. Aller, Lorand A. Sigua, M. Trifoglio, V. Strelnitski, S. G. Sergeev, Fulvio Gianotti, J. L. Gomez, M. Cardillo, Pietro Ubertini, I. M. McHardy, Angela Bazzano, Fabrizio Lucarelli, Kirill Sokolovsky, C. M. Raiteri, A. Trois, T. Krajci, F. Lazzarotto, Mark Gurwell, I. Donnarumma, A. C. Sadun, Y. Evangelista, G. Walker, Manasvita Joshi, P. Santolamazza, M. Pasanen, D. A. Morozova, R. Reinthal, Elena Pian, M. G. Nikolashvili, M. Tavani, G. A. Borman, P. W. Cattaneo, A. Sillanpää, A. A. Arkharov, L. Maraschi, N. V. Efimova, Givi N. Kimeridze, E. Del Monte, F. Longo, G. Pucella, C. Pittori, K. Nilsson, A. Pellizzoni, E. Striani, V. Vittorini, Marc Türler, V. Bianchin, M. Rapisarda, A. Giuliani, Carlo Ferrigno, P. Soffitta, S. V. Nazarov, Hugh D. Aller, G. Barbiellini, R. A. Chigladze, E. Lindfors, Arnaud Ferrari, F. Verrecchia, S. Sabatini, M. Pilia, M. Villata, M. Giusti, F. Fuschino, Andrei Berdyugin, Uwe Bach, I. Agudo, L. O. Takalo, A. W. Chen, Brian W. Taylor, P. Giommi, Omar M. Kurtanidze, S. N. Molina, J. A. Ros, G. Piano, Stephanie Sallum, M. Feroci, Andrea Bulgarelli, T. Sakamoto, Yu. S. Efimov, P. Romano, S. Vercellone, L. Pacciani, Mariateresa Fiocchi, A. Rappoldi, R. D. Schwartz, S., Vercellone, E., Striani, V., Vittorini, I., Donnarumma, L., Pacciani, G., Pucella, M., Tavani, C. M., Raiteri, M., Villata, P., Romano, M., Fiocchi, A., Bazzano, V., Bianchin, C., Ferrigno, L., Maraschi, E., Pian, M., T\urler, P., Ubertini, A., Bulgarelli, A. W., Chen, A., Giuliani, Longo, Francesco, G., Barbiellini, M., Cardillo, P. W., Cattaneo, Monte, E., Y., Evangelista, M., Feroci, A., Ferrari, F., Fuschino, F., Gianotti, M., Giusti, F., Lazzarotto, A., Pellizzoni, G., Piano, M., Pilia, M., Rapisarda, A., Rappoldi, S., Sabatini, P., Soffitta, M., Trifoglio, A., Troi, P., Giommi, F., Lucarelli, C., Pittori, P., Santolamazza, F., Verrecchia, I., Agudo, H. D., Aller, M. F., Aller, A. A., Arkharov, U., Bach, A., Berdyugin, G. A., Borman, R., Chigladze, Y. S., Efimov, N. V., Efimova, J. L., Gomez, M. A., Gurwell, I. M., Mchardy, M., Joshi, G. N., Kimeridze, T., Krajci, O. M., Kurtanidze, S. O., Kurtanidze, V. M., Larionov, E., Lindfor, S. N., Molina, D. A., Morozova, S. V., Nazarov, M. G., Nikolashvili, K., Nilsson, M., Pasanen, R., Reinthal, J. A., Ro, A. C., Sadun, T., Sakamoto, S., Sallum, S. G., Sergeev, R. D., Schwartz, L. A., Sigua, A., Sillanp\a\a, K. V., Sokolovsky, V., Strelnitski, L., Takalo, B., Taylor, and G., Walker

Subjects
galaxies: active, galaxies: jets, radiation mechanisms: non-thermal, quasars: general, quasars: individual: 3C 454.3, Photon, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Vela, 01 natural sciences, law.invention, Pulsar, law, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), general [quasars], 010308 nuclear & particles physics, individual: 3C 454.3 [quasars], Gamma ray, Astronomy and Astrophysics, non-thermal [radiation mechanisms], jet [galaxies], Space and Planetary Science, Sky, active [galaxies], Astrophysics - High Energy Astrophysical Phenomena, Flare
Abstract

Since 2005, the blazar 3C 454.3 has shown remarkable flaring activity at all frequencies, and during the last four years it has exhibited more than one gamma-ray flare per year, becoming the most active gamma-ray blazar in the sky. We present for the first time the multi-wavelength AGILE, SWIFT, INTEGRAL, and GASP-WEBT data collected in order to explain the extraordinary gamma-ray flare of 3C 454.3 which occurred in November 2010. On 2010 November 20 (MJD 55520), 3C 454.3 reached a peak flux (E>100 MeV) of F_gamma(p) = (6.8+-1.0)E-5 ph/cm2/s on a time scale of about 12 hours, more than a factor of 6 higher than the flux of the brightest steady gamma-ray source, the Vela pulsar, and more than a factor of 3 brighter than its previous super-flare on 2009 December 2-3. The multi-wavelength data make a thorough study of the present event possible: the comparison with the previous outbursts indicates a close similarity to the one that occurred in 2009. By comparing the broadband emission before, during, and after the gamma-ray flare, we find that the radio, optical and X-ray emission varies within a factor 2-3, whereas the gamma-ray flux by a factor of 10. This remarkable behavior is modeled by an external Compton component driven by a substantial local enhancement of soft seed photons., Accepted for publication in ApJ Letters. 18 Pages, 4 Figures, 1 Table

Published
2011

Catalog

Books, media, physical & digital resources
See catalog results