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1. Stochastic re-acceleration and magnetic-field damping in Tycho ’s supernova remnant

Author

Vikram V. Dwarkadas, I. Telezhinsky, Martin Pohl, and A. Wilhelm

Subjects
Shock wave, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, ISM: individual objects: Tycho’s SNR, 01 natural sciences, Momentum, Acceleration, cosmic rays, 0103 physical sciences, 010306 general physics, Supernova remnant, 010303 astronomy & astrophysics, ISM: supernova remnants, acceleration of particles, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Computer Science::Information Retrieval, supernova remnants [ISM], Astronomy and Astrophysics, shock waves, radiation mechanisms: non-thermal, non-thermal [radiation mechanisms], individual objects: Tycho’s SNR [ISM], Shock (mechanics), Supernova, Space and Planetary Science, ddc:520, Induction equation, Astrophysics - High Energy Astrophysical Phenomena, Event (particle physics)
Abstract

Astronomy and astrophysics 639, A124 (2020). doi:10.1051/0004-6361/201936079, Context. Tycho’s supernova remnant (SNR) is associated with the historical supernova (SN) event SN 1572 of Type Ia. The explosion occurred in a relatively clean environment, and was visually observed, providing an age estimate. This SNR therefore represents an ideal astrophysical test-bed for the study of cosmic-ray acceleration and related phenomena. A number of studies suggest that shock acceleration with particle feedback and very efficient magnetic-field amplification combined with Alfvénic drift are needed to explain the rather soft radio spectrum and the narrow rims observed in X-rays.Aims. We show that the broadband spectrum of Tycho’s SNR can alternatively be well explained when accounting for stochastic acceleration as a secondary process. The re-acceleration of particles in the turbulent region immediately downstream of the shock should be efficient enough to impact particle spectra over several decades in energy. The so-called Alfvénic drift and particle feedback on the shock structure are not required in this scenario. Additionally, we investigate whether synchrotron losses or magnetic-field damping play a more profound role in the formation of the non-thermal filaments.Methods. We solved the full particle transport equation in test-particle mode using hydrodynamic simulations of the SNR plasma flow. The background magnetic field was either computed from the induction equation or follows analytic profiles, depending on the model considered. Fast-mode waves in the downstream region provide the diffusion of particles in momentum space.Results. We show that the broadband spectrum of Tycho can be well explained if magnetic-field damping and stochastic re-acceleration of particles are taken into account. Although not as efficient as standard diffusive shock acceleration, stochastic acceleration leaves its imprint on the particle spectra, which is especially notable in the emission at radio wavelengths. We find a lower limit for the post-shock magnetic-field strength ∼330 μG, implying efficient amplification even for the magnetic-field damping scenario. Magnetic-field damping is necessary for the formation of the filaments in the radio range, while the X-ray filaments are shaped by both the synchrotron losses and magnetic-field damping., Published by EDP Sciences, Les Ulis

Published
2020
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2. 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
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3. Very-high-energy γ-ray observations of the blazar 1es 2344+514 with veritas

Author

A. Flinders, R. Mukherjee, P. Kaaret, E. Pueschel, A. McCann, D. S. Hanna, Martin Pohl, Maria Krause, Wei Cui, R. A. Ong, David Kieda, F. Krennrich, Daniel Nieto, M. K. Daniel, Wystan Benbow, A. N. Otte, Sinéad M. Griffin, M. P. Connolly, A. Wilhelm, A. Archer, Robert Brose, Moritz Hütten, Cameron H. Allen, J. Grube, C. Rulten, A. Petrashyk, G. H. Gillanders, Etienne Bourbeau, Lucy Fortson, N. H. Park, A. C. Rovero, P. Kar, P. T. Reynolds, N. Håkansson, Henrike Fleischhack, Gordon T. Richards, J. V. Tucci, Gernot Maier, M. Kertzman, A. O'Faolain de Bhroithe, J. Tyler, G. H. Sembroski, Matteo Cerruti, G. Hughes, J. H. Buckley, S. Archambault, M. Buchovecky, Amy Furniss, S. P. Wakely, S. O'Brien, I. Sadeh, A. Popkow, Marcos Santander, Thanh Huy Nguyen, J. V. Cardenzana, C. A. Johnson, K. Ragan, Jodi Christiansen, P. Moriarty, Xuhui Chen, M. Fernandez-Alonso, K. Meagher, Q. Feng, T. B. Humensky, J. P. Finley, John L. Quinn, S. Kumar, A. Pichel, E. Roache, Abraham D. Falcone, Karlen Shahinyan, Ralph Bird, S. McArthur, V. Bugaev, O. Hervet, J. D. Eisch, A. Weinstein, M. J. Lang, N. Kelley-Hoskins, I. Telezhinsky, Jamie Holder, and David A. Williams

Subjects
gamma-rays: galaxies, Point source, Ciencias Físicas, bl-lacertae objects, Astrophysics, telescope, 01 natural sciences, Spectral line, spectrum, purl.org/becyt/ford/1 [https], 0103 physical sciences, emission, ASTROPARTICLE PHYSICS, Blazar, 010303 astronomy & astrophysics, Physics, GALAXIES [GAMMA-RAYS], 010308 nuclear & particles physics, variability, Attenuation, Gamma ray, Astronomy, Institut für Physik und Astronomie, background-radiation, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], bl lacertae objects: individual: 1es 2344+514=verj2347+517, Light curve, Astronomía, radio, Extragalactic background light, x-ray, Space and Planetary Science, astroparticle physics, active galactic nuclei, ddc:520, BL LACERTAE OBJECTS, Astrophysics - High Energy Astrophysical Phenomena, constraints, CIENCIAS NATURALES Y EXACTAS, BL Lac object
Abstract

We present very-high-energy $\gamma$-ray observations of the BL Lac object 1ES 2344+514 taken by the Very Energetic Radiation Imaging Telescope Array System (VERITAS) between 2007 and 2015. 1ES 2344+514 is detected with a statistical significance above background of $20.8\sigma$ in $47.2$ hours (livetime) of observations, making this the most comprehensive very-high-energy study of 1ES 2344+514 to date. Using these observations the temporal properties of 1ES 2344+514 are studied on short and long times scales. We fit a constant flux model to nightly- and seasonally-binned light curves and apply a fractional variability test, to determine the stability of the source on different timescales. We reject the constant-flux model for the 2007-2008 and 2014-2015 nightly-binned light curves and for the long-term seasonally-binned light curve at the $> 3\sigma$ level. The spectra of the time-averaged emission before and after correction for attenuation by the extragalactic background light are obtained. The observed time-averaged spectrum above 200 GeV is satisfactorily fitted (${\chi^2/NDF = 7.89/6}$) by a power-law function with index $\Gamma = 2.46 \pm 0.06_{stat} \pm 0.20_{sys} $ and extends to at least 8 TeV. The extragalactic-background-light-deabsorbed spectrum is adequately fit (${\chi^2/NDF = 6.73/6}$) by a power-law function with index $\Gamma = 2.15 \pm 0.06_{stat} \pm 0.20_{sys} $ while an F-test indicates that the power-law with exponential cutoff function provides a marginally-better fit ($\chi^2/NDF $ = $2.56 / 5 $) at the 2.1$\sigma$ level. The source location is found to be consistent with the published radio location and its spatial extent is consistent with a point source., Comment: 7 pages, 2 figures. Published in Monthly Notices of the Royal Astronomical Society

Published
2017
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4. Dark Matter Constraints from a Joint Analysis of Dwarf Spheroidal Galaxy Observations with VERITAS

Author

Ralph Bird, Q. Feng, Marita Krause, Martin Pohl, M. J. Lang, J. Tyler, Matteo Cerruti, J. H. Buckley, A. N. Otte, Amy Furniss, I. Telezhinsky, E. Roache, Jamie Holder, M. P. Connolly, Wystan Benbow, N. Kelley-Hoskins, P. Kaaret, Olivier Hervet, Alex Geringer-Sameth, Karlen Shahinyan, B. Zitzer, J. Grube, M. Buchovecky, G. H. Sembroski, F. Krennrich, S. McArthur, N. H. Park, David Kieda, C. B. Rulten, P. Kar, Etienne Bourbeau, T. T.Y. Lin, N. Håkansson, Henrike Fleischhack, J. V. Tucci, A. Popkow, C. A. Johnson, M. Kertzman, Sinéad M. Griffin, R. Mukherjee, P. Moriarty, S. P. Wakely, Karen Byrum, R. A. Ong, Lucy Fortson, A. Weinstein, Marcos Santander, B. Hummensky, M. K. Daniel, John L. Quinn, T. Brantseg, E. Pueschel, David A. Williams, Gordon T. Richards, P. T. Reynolds, K. Ragan, Daniel Nieto, Moritz Hütten, A. Archer, D. Staszak, S. Trepanier, Jodi Christiansen, P. Wilcox, I. Sadeh, Wei Cui, Savvas M. Koushiappas, A. W. Smith, J. P. Finley, S. Archambault, D. S. Hanna, V. Bugaev, S. O'Brien, and G. Hughes

Subjects
particle, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, IACT, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Bottom quark, models, gamma-ray astronomy, 0103 physical sciences, ddc:530, 010303 astronomy & astrophysics, milky-way, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, parameters, High Energy Astrophysical Phenomena (astro-ph.HE), Gauge boson, Annihilation, 010308 nuclear & particles physics, Astronomy, Institut für Physik und Astronomie, Dwarf spheroidal galaxy, kinematics, Weakly interacting massive particles, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present constraints on the annihilation cross section of WIMP dark matter based on the joint statistical analysis of four dwarf galaxies with VERITAS. These results are derived from an optimized photon weighting statistical technique that improves on standard imaging atmospheric Cherenkov telescope (IACT) analyses by utilizing the spectral and spatial properties of individual photon events. We report on the results of $\sim$230 hours of observations of five dwarf galaxies and the joint statistical analysis of four of the dwarf galaxies. We find no evidence of gamma-ray emission from any individual dwarf nor in the joint analysis. The derived upper limit on the dark matter annihilation cross section from the joint analysis is $1.35\times 10^{-23} {\mathrm{ cm^3s^{-1}}}$ at 1 TeV for the bottom quark ($b\bar{b}$) final state, $2.85\times 10^{-24}{\mathrm{ cm^3s^{-1}}}$ at 1 TeV for the tau lepton ($\tau^{+}\tau^{-}$) final state and $1.32\times 10^{-25}{\mathrm{ cm^3s^{-1}}}$ at 1 TeV for the gauge boson ($\gamma\gamma$) final state., Comment: 14 pages, 9 figures, published in PRD, Ascii tables containing annihilation cross sections limits are available for download as ancillary files with readme.txt file description of limits

Published
2017
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5. 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
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6. 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
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7. Gamma-ray Observations Under Bright Moonlight with VERITAS

Author

G. H. Gillanders, A. Weinstein, Martin Pohl, M. Kertzman, S. McArthur, Sinéad M. Griffin, Wystan Benbow, O. Hervet, P. Moriarty, Henrike Fleischhack, Q. Feng, A. Popkow, John L. Quinn, P. Kaaret, M. J. Lang, D. S. Hanna, David Kieda, Gordon T. Richards, Lucy Fortson, R. A. Ong, Ralph Bird, P. T. Reynolds, J. P. Finley, Wei Cui, J. V. Cardenzana, E. Pueschel, Maria Krause, David A. Williams, M. Buchovecky, C. A. Johnson, N. H. Park, Daniel Nieto, E. Roache, L. Ciupik, A. Bouvier, Gernot Maier, Abraham D. Falcone, M. K. Daniel, S. P. Wakely, A. N. Otte, Karlen Shahinyan, S. Archambault, S. O'Brien, K. Ragan, I. Telezhinsky, Jamie Holder, Matteo Cerruti, Amy Furniss, M. P. Connolly, G. Hughes, Etienne Bourbeau, B. Zitzer, A. Archer, T. T.Y. Lin, G. H. Sembroski, T. B. Humensky, Moritz Hütten, Manel Errando, I. Sadeh, R. Mukherjee, D. Staszak, S. Trepanier, P. Wilcox, V. Bugaev, C. Rulten, and P. Kar

Subjects
Moonlight, Astrophysics and Astronomy, Photomultiplier, Instrumentation, FOS: Physical sciences, IACT, Astrophysics, telescope, 01 natural sciences, law.invention, moon, iact, Positron, law, veritas, 0103 physical sciences, ddc:530, crab-nebula, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, Physics, instrumentation, 010308 nuclear & particles physics, Gamma ray, Institut für Physik und Astronomie, Astronomy and Astrophysics, moonlight, radiation, 13. Climate action, ddc:540, ddc:520, observing methods, Astrophysics - Instrumentation and Methods for Astrophysics, astro-ph.IM, Flare
Abstract

Astroparticle physics 91, 34 - 43 (2017). doi:10.1016/j.astropartphys.2017.03.001, Imaging atmospheric Cherenkov telescopes (IACTs) are equipped with sensitive photomultiplier tube (PMT) cameras. Exposure to high levels of background illumination degrades the efficiency of and potentially destroys these photo-detectors over time, so IACTs cannot be operated in the same configuration in the presence of bright moonlight as under dark skies. Since September 2012, observations have been carried out with the VERITAS IACTs under bright moonlight (defined as about three times the night-sky-background (NSB) of a dark extragalactic field, typically occurring when Moon illumination > 35%) in two observing modes, firstly by reducing the voltage applied to the PMTs and, secondly, with the addition of ultra-violet (UV) bandpass filters to the cameras. This has allowed observations at up to about 30 times previous NSB levels (around 80% Moon illumination), resulting in 30% more observing time between the two modes over the course of a year. These additional observations have already allowed for the detection of a flare from the 1ES 1727 + 502 and for an observing program targeting a measurement of the cosmic-ray positron fraction. We provide details of these new observing modes and their performance relative to the standard VERITAS observations., Published by Elsevier, Amsterdam [u.a.]

Published
2017
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8. Very high energy observations of the binaries V 404 CYG AND 4U 0115+634 during giant X-Ray outbursts

Author

Wystan Benbow, Daniel Nieto, D. Staszak, Sanjay Kumar, P. Kaaret, A. Flinders, K. Ragan, Gernot Maier, S. Griffin, Matteo Cerruti, I. Telezhinsky, David Kieda, Jamie Holder, S. P. Wakely, P. Moriarty, John L. Quinn, Karen Byrum, N. Kelley-Hoskins, R. Mukherjee, A. Furniss, T. B. Humensky, R. A. Ong, Wei Cui, E. Pueschel, M. Fernandez-Alonso, S. Schlenstedt, O. Hervet, Q. Feng, E. Roache, D. S. Hanna, P. Wilcox, M. P. Connolly, A. C. Rovero, N. H. Park, Gordon T. Richards, M. Kertzman, J. H. Buckley, Abraham D. Falcone, C. A. Johnson, V. Bugaev, Karlen Shahinyan, David A. Williams, E. Bourbeau, H. Fleischhack, Ralph Bird, T. T.Y. Lin, Julien Rousselle, P. T. Reynolds, I. Sadeh, M. Hütten, P. Kar, M. J. Lang, A. Popkow, J. Tyler, J. Grube, Manel Errando, A. Archer, Stephan O'Brien, G. H. Sembroski, Lucy Fortson, Martin Pohl, M. Buchovecky, J. P. Finley, Maria Krause, and A. Wilhelm

Subjects
transients, black-hole, Astrophysics::High Energy Astrophysical Phenomena, Ciencias Físicas, X-ray binary, Flux, FOS: Physical sciences, Astrophysics, stars: individual (v 404 cyg, 4u 0115+634), 01 natural sciences, VERY HIGH ENERGY GAMMA RAYS, Luminosity, spectrum, X-RAY TRANSIENTS, purl.org/becyt/ford/1 [https], symbols.namesake, Observatory, 0103 physical sciences, Binary star, emission, tev, 010306 general physics, 010303 astronomy & astrophysics, acceleration of particles, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), ls i+61-degrees 303, Gamma ray, v404 cygni, Astronomy and Astrophysics, gamma rays: general, purl.org/becyt/ford/1.3 [https], veritas observations, Astronomía, Stars, binaries: general, 13. Climate action, Space and Planetary Science, Eddington luminosity, symbols, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, BINARY STARS
Abstract

Transient X-ray binaries produce major outbursts in which the X-ray flux can increase over the quiescent level by factors as large as $10^7$. The low-mass X-ray binary V 404 Cyg and the high-mass system 4U 0115+634 underwent such major outbursts in June and October 2015, respectively. We present here observations at energies above hundreds of GeV with the VERITAS observatory taken during some of the brightest X-ray activity ever observed from these systems. No gamma-ray emission has been detected by VERITAS in 2.5 hours of observations of the microquasar V 404 Cyg from 2015, June 20-21. The upper flux limits derived from these observations on the gamma-ray flux above 200 GeV of F $< 4.4\times 10^{-12}$ cm$^{-2}$ s$^{-1}$ correspond to a tiny fraction (about $10^{-6}$) of the Eddington luminosity of the system, in stark contrast to that seen in the X-ray band. No gamma rays have been detected during observations of 4U 0115+634 in the period of major X-ray activity in October 2015. The flux upper limit derived from our observations is F $< 2.1\times 10^{-12}$ cm$^{-2}$ s$^{-1}$ for gamma rays above 300 GeV, setting an upper limit on the ratio of gamma-ray to X-ray luminosity of less than 4%., Accepted for publication in the Astrophysical Journal

Published
2016
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10. Transport of magnetic turbulence in Supernova remnants

Author

I. Telezhinsky, Robert Brose, and Martin Pohl

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Turbulence, Scattering, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Institut für Physik und Astronomie, Astronomy and Astrophysics, Cosmic ray, Astrophysics, 01 natural sciences, Computational physics, Bohm diffusion, Supernova, Acceleration, Space and Planetary Science, 0103 physical sciences, ddc:520, Diffusion (business), Convection–diffusion equation, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

Astronomy and astrophysics 593, A20(2016). doi:10.1051/0004-6361/201527345, Supernova remnants are known as sources of Galactic cosmic rays for their nonthermal emission of radio waves, X-rays, and gamma rays. However, the observed soft broken power-law spectra are hard to reproduce within standard acceleration theory based on the assumption of Bohm diffusion and steady-state calculations.Aims. We point out that a time-dependent treatment of the acceleration process together with a self-consistent treatment of the scattering turbulence amplification is necessary.Methods. We numerically solve the coupled system of transport equations for cosmic rays and isotropic Alfvénic turbulence. The equations are coupled through the growth rate of turbulence determined by the cosmic-ray gradient and the spatial diffusion coefficient of cosmic rays determined by the energy density of the turbulence. The system is solved on a comoving expanding grid extending upstream for dozens of shock radii, allowing for the self-consistent study of cosmic-ray diffusion in the vicinity of their acceleration site. The transport equation for cosmic rays is solved in a test-particle approach.Results. We demonstrate that the system is typically not in a steady state. In fact, even after several thousand years of evolution, no equilibrium situation is reached. The resulting time-dependent particle spectra strongly differ from those derived assuming a steady state and Bohm diffusion. Our results indicate that proper accounting for the evolution of the scattering turbulence and hence the particle diffusion coefficient is crucial for the formation of the observed soft spectra. In any case, the need to continuously develop magnetic turbulence upstream of the shock introduces nonlinearity in addition to that imposed by cosmic-ray feedback., Published by EDP Sciences, Les Ulis

Published
2016
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11. Discovery of very high energy gamma rays from 1es 1440+122

Author

A. N. Otte, Geza Gyuk, E. Roache, M. P. Connolly, J. V. Tucci, Gernot Maier, S. P. Wakely, Abraham D. Falcone, Karlen Shahinyan, Wystan Benbow, N. Håkansson, Anna Barnacka, P. T. Reynolds, R. A. Ong, John L. Quinn, Ralph Bird, S. T. Griffiths, K. Sweeney, I. Telezhinsky, Jamie Holder, S. Federici, Martin Pohl, N. H. Park, J. Millis, J. Dumm, B. Zitzer, G. H. Sembroski, J. Grube, P. Kar, S. Godambe, Manel Errando, M. Kertzman, R. Welsing, M. J. Lang, L. C. Reyes, S. Kumar, K. Berger, Hugh Dickinson, D. S. Hanna, Xuhui Chen, Matteo Cerruti, Amy Furniss, Wei Cui, Henric Krawczynski, Y. Khassen, A. McCann, Q. Feng, A. O'Faolain de Bhroithe, David A. Williams, P. Kaaret, Lucy Fortson, D. Staszak, A. Popkow, Vladimir Vassiliev, H. Prokoph, Matthias Beilicke, J. S. Perkins, E. Pueschel, Markus Böttcher, J. Tyler, A. Wilhelm, A. Varlotta, A. Archer, J. V. Cardenzana, C. A. Johnson, E. Collins-Hughes, G. Hughes, David Kieda, Jodi Christiansen, J. D. Eisch, J. P. Finley, G. H. Gillanders, T. J. N. Nelson, S. McArthur, S. Griffin, K. Meagher, Jean-Francois Rajotte, S. Archambault, L. Ciupik, K. Ragan, V. Bugaev, H. Fleischhack, J. H. Buckley, A. W. Smith, A. S Madhavan, Gordon T. Richards, B. Behera, Daniel Nieto, and P. Moriarty

Subjects
extragalactic background light, multiwavelength observations, Astrophysics::High Energy Astrophysical Phenomena, bl-lacertae objects, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, bright blazars, 01 natural sciences, 7. Clean energy, law.invention, Telescope, law, 0103 physical sciences, intergalactic magnetic-field, Blazar, 010303 astronomy & astrophysics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, bl lacertae objects: general, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, tev blazars, Gamma ray, Astronomy, Institut für Physik und Astronomie, Astronomy and Astrophysics, source catalog, gamma-rays: general, Redshift, large-area telescope, einstein slew survey, Crab Nebula, 13. Climate action, Space and Planetary Science, active galactic nuclei, ddc:520, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object, Fermi Gamma-ray Space Telescope
Abstract

The BL Lacertae object 1ES 1440+122 was observed in the energy range from 85 GeV to 30 TeV by the VERITAS array of imaging atmospheric Cherenkov telescopes. The observations, taken between 2008 May and 2010 June and totalling 53 hours, resulted in the discovery of $\gamma$-ray emission from the blazar, which has a redshift $z$=0.163. 1ES 1440+122 is detected at a statistical significance of 5.5 standard deviations above the background with an integral flux of (2.8$\pm0.7_{\mathrm{stat}}\pm0.8_{\mathrm{sys}}$) $\times$ 10$^{-12}$ cm$^{-2}$ s$^{-1}$ (1.2\% of the Crab Nebula's flux) above 200 GeV. The measured spectrum is described well by a power law from 0.2 TeV to 1.3 TeV with a photon index of 3.1 $\pm$ 0.4$_{\mathrm{stat}}$ $\pm$ 0.2$_{\mathrm{sys}}$. Quasi-simultaneous multi-wavelength data from the Fermi Large Area Telescope (0.3--300 GeV) and the Swift X-ray Telescope (0.2--10 keV) are additionally used to model the properties of the emission region. A synchrotron self-Compton model produces a good representation of the multi-wavelength data. Adding an external-Compton or a hadronic component also adequately describes the data., Comment: 8 pages, 4 figures. Accepted for publication in MNRAS

Published
2016
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12. A search for brief optical flashes associated with the seti target kic 8462852

Author

M. Buchovecky, Q. Feng, J. Grube, I. Telezhinsky, Jamie Holder, S. O'Brien, P. T. Reynolds, A. McCann, P. Fortin, Ralph Bird, Hugh Dickinson, Wystan Benbow, Anushka Udara Abeysekara, S. Archambault, Reshmi Mukherjee, A. Archer, D. Staszak, Martin Pohl, A. N. Otte, K. Meagher, S. McArthur, E. Pueschel, Maria Krause, O. M. Weiner, D. J. Fegan, Karen Byrum, J. D. Eisch, Abraham D. Falcone, Daniel Nieto, A. Weinstein, Karlen Shahinyan, S. Vincent, G. H. Gillanders, N. H. Park, D. S. Hanna, L. Ciupik, David A. Williams, N. Håkansson, Henrike Fleischhack, P. Kaaret, J. V. Cardenzana, J. V. Tucci, M. J. Lang, Moritz Hütten, Gernot Maier, John L. Quinn, N. Kelley-Hoskins, C. A. Johnson, K. Ragan, Geza Gyuk, Lucy Fortson, S. P. Wakely, R. A. Ong, David Kieda, F. Krennrich, Sinéad M. Griffin, J. Tyler, Matteo Cerruti, J. H. Buckley, Amy Furniss, Gordon T. Richards, E. Roache, P. Moriarty, J. P. Finley, G. Ratliff, Xuhui Chen, J. S. Perkins, Jodi Christiansen, T. B. Humensky, G. H. Sembroski, B. Zitzer, Manel Errando, S. Kumar, T. T.Y. Lin, A. Popkow, M. Kertzman, A. O'Faolain de Bhroithe, Wei Cui, A. Petrashyk, P. Kar, Marcos Santander, and ~

Subjects
stars, Photon, spectra, Astrophysics::High Energy Astrophysical Phenomena, astrobiology, FOS: Physical sciences, system, 01 natural sciences, oseti, extraterrestrial intelligence, law.invention, Telescope, Physics::Popular Physics, techniques: photometric, Observatory, law, veritas, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Pulse intensity, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Cherenkov radiation, Search for extraterrestrial intelligence, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, bursts, Extraterrestrial intelligence, Astrophysics::Instrumentation and Methods for Astrophysics, Institut für Physik und Astronomie, Astronomy, Astronomy and Astrophysics, telescopes, stars: individual ( kic 8462852), Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, ddc:520, Astrophysics::Earth and Planetary Astrophysics, methods: observational, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The astrophysical journal / 2 818(2), L33(2016). doi:10.3847/2041-8205/818/2/L33, The F-type star KIC 8462852 has recently been identified as an exceptional target for search for extraterrestrial intelligence (SETI) observations. We describe an analysis methodology for optical SETI, which we have used to analyze nine hours of serendipitous archival observations of KIC 8462852 made with the VERITAS gamma-ray observatory between 2009 and 2015. No evidence of pulsed optical beacons, above a pulse intensity at the Earth of approximately $1\;\mathrm{photon}\;{{\rm{m}}}^{-2}$, is found. We also discuss the potential use of imaging atmospheric Cherenkov telescope arrays in searching for extremely short duration optical transients in general., Published by Institute of Physics Publ., London

Published
2016
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13. A search for very high energy gamma rays from the missing link binary pulsar J1023+0038 with VERITAS

Author

Wystan Benbow, John L. Quinn, A. Petrashyk, M. J. Lang, P. Kar, O. M. Weiner, Jonathan Biteau, J. P. Finley, B. Zitzer, N. Håkansson, Henrike Fleischhack, David Kieda, A. W. Smith, A. Flinders, Q. Feng, Abraham D. Falcone, Gordon T. Richards, E. Roache, Karlen Shahinyan, E. Pueschel, Geza Gyuk, S. Vincent, Nahee Park, A. Varlotta, N. Kelley-Hoskins, T. B. Humensky, Maria Krause, P. Moriarty, K. L. Byrum, Wei Cui, J. Grube, P. Kaaret, J. V. Cardenzana, J. D. Eisch, S. McArthur, A. McCann, Xuhui Chen, V. Bugaev, L. Ciupik, S. Archambault, Reshmi Mukherjee, Daniel Nieto, A. O'Faolain de Bhroithe, Sinéad M. Griffin, A. Popkow, E. Aliu, Maria Chernyakova, Lucy Fortson, J. Tyler, Matteo Cerruti, Moritz Hütten, J. H. Buckley, R. A. Ong, A. N. Otte, Amy Furniss, Marcos Santander, M. Kertzman, Martin Pohl, S. P. Wakely, P. Fortin, V. Pelassa, C. B. Rulten, Ralph Bird, G. H. Sembroski, A. Loo, K. Meagher, Hugh Dickinson, Mallory S. E. Roberts, M. Buchovecky, M. P. Connolly, D. Pandel, P. T. Reynolds, A. J.R. Weinstein, C. A. Johnson, J. V. Tucci, Gernot Maier, A. Wilhelm, D. Staszak, K. Ragan, I. Telezhinsky, Jamie Holder, David A. Williams, Thanh Huy Nguyen, A. Archer, and G. H. Gillanders

Subjects
nustar observations, Astrophysics::High Energy Astrophysical Phenomena, Flux, Binary number, FOS: Physical sciences, Astrophysics, telescope, 01 natural sciences, Binary pulsar, Pulsar, pulsars: general, psr j1023+0038, emission, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Millisecond, state change, 010308 nuclear & particles physics, pulsars: individual (psr j1023+0038), periastron, Gamma ray, transition, Institut für Physik und Astronomie, Astronomy and Astrophysics, gamma rays: general, 1st j102347.6+003841, Magnetic field, Neutron star, binaries: general, 13. Climate action, Space and Planetary Science, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, millisecond pulsar, discovery
Abstract

The binary millisecond radio pulsar PSR J1023+0038 exhibits many characteristics similar to the gamma-ray binary system PSR B1259--63/LS 2883, making it an ideal candidate for the study of high-energy non-thermal emission. It has been the subject of multi-wavelength campaigns following the disappearance of the pulsed radio emission in 2013 June, which revealed the appearance of an accretion disk around the neutron star. We present the results of very high-energy gamma-ray observations carried out by VERITAS before and after this change of state. Searches for steady and pulsed emission of both data sets yield no significant gamma-ray signal above 100 GeV, and upper limits are given for both a steady and pulsed gamma-ray flux. These upper limits are used to constrain the magnetic field strength in the shock region of the PSR J1023+0038 system. Assuming that very high-energy gamma rays are produced via an inverse-Compton mechanism in the shock region, we constrain the shock magnetic field to be greater than $\sim$2 G before the disappearance of the radio pulsar and greater than $\sim$10 G afterwards., 7 pages, 3 figures, accepted for publication in ApJ

Published
2016
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14. Multiband variability studies and novel broadband SED modeling of Mrk 501 in 2009

Author

K. Nishijima, J. L. Richards, Stefano Covino, G. Piner, D. Dominis Prester, U. Menzel, A. Flinders, D. Tescaro, Louis Antonelli, D. Galindo, Aaron Dominguez, S. Schröder, Elena G. Larionova, Kari Nilsson, Paul S. Smith, A. McCann, T. S. Grishina, Wen Ping Chen, M. Will, Pratik Majumdar, J. E. Ward, Daniela Dorner, Dariusz Gora, P. Moriarty, C. Rulten, Soebur Razzaque, D. Garrido Terrats, K. Frantzen, Joseph Moody, Wystan Benbow, G. Hughes, K. Ragan, Ralph Bird, L. Perri, M. Gaug, T. Sakamoto, Valeri M. Larionov, Elina Lindfors, G. H. Sembroski, Daniel Mazin, Ievgen Vovk, A. Hahn, M. Hütten, N. H. Park, Alexander B. Pushkarev, G. Maccaferri, Thomas Bretz, P. Wilcox, P. Kar, D. Nakajima, R. Zanin, J. Herrera, Wei Cui, Amanda Weinstein, J. Palacio, P. G. Prada Moroni, Frank Krennrich, Matthew L. Lister, A. Berti, A. Cesarini, M. Kertzman, A. La Barbera, Walter Max-Moerbeck, E. Colombo, M. Villata, M. P. Connolly, Adrian Biland, D. S. Hanna, Ana Babić, D. Eisenacher Glawion, Juan Abel Barrio, John L. Quinn, M. Capalbi, Koji Noda, Arka Chatterjee, Elisa Bernardini, A. Sillanpää, Adrian Rovero, Antonio Stamerra, J. V. Tucci, M. Nievas Rosillo, M. Palatiello, L. V. Larionova, S. N. Shore, R. Mukherjee, M. J. Lang, Daniel Nieto, M. I. Martínez, S. Bonnefoy, J. Kushida, P. Giammaria, P. Bangale, Wolfgang Rhode, Gernot Maier, G. Pedaletti, L. O. Takalo, Margo F. Aller, Jose Luis Contreras, Andrei Berdyugin, J. A. Zensus, E. Roache, V. Verguilov, D. Fidalgo, C. Pace, Thomas P. Krichbaum, Francesco Dazzi, Juan Cortina, M. Engelkemeier, G. H. Gillanders, A. Carraminyana, S. P. Wakely, Mosè Mariotti, J. Rico, A. Fernández-Barral, R. Clavero, J. Becerra González, A.-K. Overkemping, S. O. Kurtanidze, Sabrina Einecke, Abraham D. Falcone, A. González Muñoz, Evgenia N. Kopatskaya, Lars Fuhrmann, Nikola Godinovic, Benito Marcote, Karlen Shahinyan, Takashi Saito, W. Bednarek, C. Schultz, Marcos Santander, Fabrizio Tavecchio, J. Rodriguez Garcia, E. Pueschel, Ll. Font, A. C. Sadun, A. Popkow, J. Grube, V. Bugaev, Anthony C. S. Readhead, R. Ligustri, A. Archer, I. Snidaric, Yusuke Konno, P. Calcidese, M. Strzys, A. Pichel, Saverio Lombardi, B. De Lotto, Markus Garczarczyk, N. Kelley-Hoskins, J. Tyler, Ann E. Wehrle, B. Banerjee, S. Buson, D. Hadasch, N. Otte, Maria G. Nikolashvili, Gordon T. Richards, L. Nogués, B. Biasuzzi, Juri Poutanen, U. Barres de Almeida, J. P. Finley, K. Mallot, S. Paiano, Marcello Giroletti, I. Nestoras, A. De Angelis, A. Treves, Vitaly Neustroev, X. Paredes-Fortuny, T. B. Humensky, R. A. Ong, Karl Mannheim, J. H. Buckley, Yu. A. Kovalev, R. J. García López, H. Fleischhack, G. N. Kimeridze, I. Sadeh, David A. Williams, Y. Mori, M. V. Fonseca, W. Idec, Matthias Kadler, Yuri Y. Kovalev, Stefano Ansoldi, Riccardo Paoletti, K. Kodani, J. P. Norris, O. M. Kurtanidze, N. V. Efimova, Y. Hanabata, Arkady A. Arkharov, Anne Lähteenmäki, Abelardo Moralejo, G. Maneva, Masahiro Teshima, A. C. Zook, Dario Hrupec, P. Antoranz, B. Zitzer, Hugh Dickinson, R. A. Chigladze, M. Peresano, Ekaterina Koptelova, S. Archambault, M. A. Lopez, T. Steinbring, P. Temnikov, P. Leto, Massimo Persic, J. M. Paredes, Hugh D. Aller, F. Borracci, S. O'Brien, T. Surić, I. Telezhinsky, I. Reichardt, Jamie Holder, G. Vanzo, R. Pearson, Julia Thaele, G. Bonnoli, Mark Gurwell, Eduardo Ros, Andrea Orlati, S. Griffin, L. A. Sigua, Diego F. Torres, Alessandro Carosi, Ruben Lopez-Coto, Maria Krause, Y. Yatsu, A. Wilhelm, Jose Miguel Miranda, Anushka Udara Abeysekara, T. Schweizer, P. Cassaro, Razmik Mirzoyan, E. Moretti, Damir Lelas, Francesco Longo, V. Fallah Ramazani, P. Kaaret, Dorota Sobczyńska, L. Maraschi, Kirill Sokolovsky, Tomislav Terzić, Lucy Fortson, E. de Ona Wilhelmi, Julian Sitarek, C. Fruck, T. Toyama, Ivica Puljak, Max Ludwig Ahnen, David Kieda, F. Di Pierro, Pierre Colin, M. Buchovecky, Oscar Blanch, P. Da Vela, A. Niedzwiecki, Emmanouil Angelakis, M. Doert, M. H. Wu, Ivan S. Troitsky, C. Pagani, David Paneque, Q. Feng, Vladimir A. Hagen-Thorn, E. De la Fuente, E. Prandini, C. M. Raiteri, L. Carrasco, D. Guberman, Jeremy S. Perkins, Martin Pohl, Marina Manganaro, H. A. Krimm, Merja Tornikoski, Konstancja Satalecka, Michele Doro, Dmitry A. Blinov, M. Perri, J. Hose, D. Elsaesser, Daria A. Morozova, P. T. Reynolds, M. Hayashida, Marc Ribó, Hidetoshi Kubo, M. Makariev, Swiss Federal Institute of Technology Zurich, University of Udine, INAF National Institute for Astrophysics, University of Siena, University of Rijeka, Saha Institute of Nuclear Physics, Max Planck Institute for Physics, Complutense University, University of La Laguna, University of Łódź, German Electron Synchrotron, Autonomous University of Barcelona, University of Würzburg, University of Padova, Institute of Space Studies of Catalonia, Dortmund University, Finnish MAGIC Consortium, University of Barcelona, The University of Tokyo, Bulgarian Academy of Sciences, Osservatorio Astronomicodi Roma, University of Pisa, ICREA, University of Maryland, College Park, McGill University, Washington University St. Louis, Harvard University, University College Dublin, University of California Los Angeles, National University of Ireland, Galway, Purdue University, Iowa State University, Pennsylvania State University, University of Utah, University of Minnesota Twin Cities, Adler Planetarium and Astronomy Museum, University of Delaware, Columbia University, University of Iowa, DePauw University, Georgia Institute of Technology, University of Chicago, NASA Goddard Space Flight Center, Universidad de Buenos Aires, Cork Institute of Technology, University of California Santa Cruz, Argonne National Laboratory, University of Johannesburg, University of Michigan, Ann Arbor, St. Petersburg State University, RAS - Pulkovo Astronomical Observatory, Circolo Astrofili Talmassons, Osservatorio Astrofisico della Regione Autonoma Valle d'Aosta, Georgian National Academy of Sciences, National Central University, Aoyama Gakuin University, University of Colorado Denver, Brigham Young University, Tokyo Institute of Technology, Instituto Nacional de Astrofisica Optica y Electronica, Universidad de Guadalajara, University of Denver, University of Arizona, Space Science Institute, Pomona College, University of Leicester, ASI Science Data Center, University of Trento, RAS - P.N. Lebedev Physics Institute, Max Planck Institute for Radio Astronomy, Whittier College, Metsähovi Radio Observatory, INAF Istituto di Radioastronomia, Osservatorio Astrofisico di Catania, California Institute of Technology, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, Ahnen, M. L., Ansoldi, S., 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., Berti, Alessio, Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Buson, S., 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 Oña Wilhelmi, E., Di Pierro, F., Doert, M., Domã­nguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Engelkemeier, M., Fallah Ramazani, V., 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., Godinoviä , N., González Muñoz, A., Gora, D., Guberman, D., Hadasch, 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, Lã³pez, M., López Coto, R., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martã­nez, 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., Noguã©s, L., Overkemping, A., Paiano, S., Palacio, J., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Reichardt, I., Rhode, W., Ribã³, M., Rico, J., Rodriguez Garcia, J., Saito, T., Satalecka, K., Schrã¶der, S., Schultz, C., Schweizer, T., Shore, S. N., Sillanpã¤ã¤, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Suriä , T., Takalo, L., Tavecchio, F., Temnikov, P., Terziä , T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Vanzo, G., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., Zanin, R., Abeysekara, A. U., Archambault, S., Archer, A., Benbow, W., Bird, R., Buchovecky, M., Buckley, J. H., Bugaev, V., Connolly, M. P., Cui, W., Dickinson, H. J., Falcone, A., Feng, Q., Finley, J. P., Fleischhack, H., Flinders, A., Fortson, L., Gillanders, G. H., Griffin, S., Grube, J., Hã¼tten, M., Hanna, D., Holder, J., Humensky, T. B., Kaaret, P., Kar, P., Kelley Hoskins, N., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Lang, M. J., Maier, G., Mccann, A., Moriarty, P., Mukherjee, R., Nieto, D., O'Brien, S., Ong, R. A., Otte, N., Park, N., Perkins, J., Pichel, A., Pohl, M., Popkow, A., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Richards, G. T., Roache, E., Rovero, A. C., Rulten, C., Sadeh, I., Santander, M., Sembroski, G. H., Shahinyan, K., Telezhinsky, I., Tucci, J. V., Tyler, J., Wakely, S. P., Weinstein, A., Wilcox, P., Wilhelm, A., Williams, D. A., Zitzer, B., Razzaque, S., Villata, M., Raiteri, C. M., Aller, H. D., Aller, M. F., Larionov, V. M., Arkharov, A. A., Blinov, D. A., Efimova, N. V., Grishina, T. S., Hagen Thorn, V. A., Kopatskaya, E. N., Larionova, L. V., Larionova, E. G., Morozova, D. A., Troitsky, I. S., Ligustri, R., Calcidese, P., Berdyugin, A., Kurtanidze, O. M., Nikolashvili, M. G., Kimeridze, G. N., Sigua, L. A., Kurtanidze, S. O., Chigladze, R. A., Chen, W. P., Koptelova, E., Sakamoto, T., Sadun, A. C., Moody, J. W., Pace, C., Pearson, R., Yatsu, Y., Mori, Y., Carraminyana, A., Carrasco, L., De La Fuente, E., Norris, J. P., Smith, P. S., Wehrle, A., Gurwell, M. A., Zook, A., Pagani, C., Perri, M., Capalbi, M., Cesarini, A., Krimm, H. A., Kovalev, Y. Y., Kovalev, Y. u. A., Ros, E., Pushkarev, A. B., Lister, M. L., Sokolovsky, K. V., Kadler, M., Piner, G., Lã¤hteenmã¤ki, A., Tornikoski, M., Angelakis, E., Krichbaum, T. P., Nestoras, I., Fuhrmann, L., Zensus, J. A., Cassaro, P., Orlati, A., Maccaferri, G., Leto, P., Giroletti, M., Richards, J. L., Max Moerbeck, W., and Readhead, A. C. S.

Subjects
extragalactic background light, multiwavelength observations, Astrophysics::High Energy Astrophysical Phenomena, bl-lacertae objects, Galaxies: BL Lacertae objects: individual: Markarian 501, Methods: data analysis, observational, Polarization, spectral energy-distribution, Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, individual: Markarian 501 [BL Lacertae objects], law, Coincident, 0103 physical sciences, ddc:530, MAGIC (telescope), crab-nebula, Blazar, data analysis [Methods], 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), tev blazars, 010308 nuclear & particles physics, stochastic acceleration, telescope observations, Institut für Physik und Astronomie, Astronomy and Astrophysics, Astronomy and Astrophysic, gamma-ray emission, methods: data analysis, BL Lacertae objects: individual: Markarian 501, Synchrotron, data analysi [Methods], Space and Planetary Science, x-ray, ddc:520, Electrónica, Física nuclear, Electricidad, Degeneracy (mathematics), Astrophysics - High Energy Astrophysical Phenomena, Flare, BL Lac object
Abstract

Astronomy and astrophysics 603, A31 (2017). doi:10.1051/0004-6361/201629540, We present an extensive study of the BL Lac object Mrk 501 based on a data set collected during the multi-instrument campaign spanning from 2009 March 15 to 2009 August 1, which includes, among other instruments, MAGIC, VERITAS, Whipple 10 m, and Fermi-LAT to cover the γ-ray range from 0.1 GeV to 20 TeV; RXTE and Swift to cover wavelengths from UV tohard X-rays; and GASP-WEBT, which provides coverage of radio and optical wavelengths. Optical polarization measurements were provided for a fraction of the campaign by the Steward and St. Petersburg observatories. We evaluate the variability of the source and interband correlations, the γ-ray flaring activity occurring in May 2009, and interpret the results within two synchrotron self-Compton (SSC) scenarios. Aims. The multiband variability observed during the full campaign is addressed in terms of the fractional variability, and the possible correlations are studied by calculating the discrete correlation function for each pair of energy bands where the significance was evaluated with dedicated Monte Carlo simulations. The space of SSC model parameters is probed following a dedicated grid-scan strategy, allowing for a wide range of models to be tested and offering a study of the degeneracy of model-to-data agreement in the individual model parameters, hence providing a less biased interpretation than the “single-curve SSC model adjustment” typically reported in the literature. Methods. We find an increase in the fractional variability with energy, while no significant interband correlations of flux changes are found on the basis of the acquired data set. The SSC model grid-scan shows that the flaring activity around May 22 cannot be modeled adequately with a one-zone SSC scenario (using an electron energy distribution with two breaks), while it can be suitably described within a two (independent) zone SSC scenario. Here, one zone is responsible for the quiescent emission from the averaged 4.5-month observing period, while the other one, which is spatially separated from the first, dominates the flaring emission occurring at X-rays and very-high-energy (>100 GeV, VHE) γ rays. The flaring activity from May 1, which coincides with a rotation of the electric vector polarization angle (EVPA), cannot be satisfactorily reproduced by either a one-zone or a two-independent-zone SSC model, yet this is partially affected by the lack of strictly simultaneous observations and the presence of large flux changes on sub-hour timescales (detected at VHE γ rays). Results. The higher variability in the VHE emission and lack of correlation with the X-ray emission indicate that, at least during the 4.5-month observing campaign in 2009, the highest energy (and most variable) electrons that are responsible for the VHE γ rays do not make a dominant contribution to the ~1 keV emission. Alternatively, there could be a very variable component contributing to the VHE γ-ray emission in addition to that coming from the SSC scenario. The studies with our dedicated SSC grid-scan show that there is some degeneracy in both the one-zone and the two-zone SSC scenarios probed, with several combinations of model parameters yielding a similar model-to-data agreement, and some parameters better constrained than others. The observed γ-ray flaring activity, with the EVPA rotation coincident with the first γ-ray flare, resembles those reported previously for low frequency peaked blazars, hence suggesting that there are many similarities in the flaring mechanisms of blazars with different jet properties., Published by EDP Sciences, Les Ulis

Published
2016
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15. VERITAS and multiwavelength observations of the BL Lacertae object 1ES 1741+196

Author

J. V. Cardenzana, J. Biteau, C. A. Johnson, A. McCann, N. Kelley-Hoskins, K. Reynolds, R. A. Ong, Sinéad M. Griffin, D. Petry, D. S. Hanna, A. N. Otte, M. P. Connolly, Lucy Fortson, P. Kaaret, S. McArthur, V. Bugaev, J. Tyler, E. Roache, J. P. Finley, David Kieda, J. H. Buckley, B. Zitzer, A. Archer, F. Krennrich, G. H. Gillanders, J. Grube, G. Ratliff, Wystan Benbow, Manel Errando, A. Flinders, M. J. Lang, Xuhui Chen, Q. Feng, Abraham D. Falcone, Karlen Shahinyan, A. Popkow, E. Pueschel, Maria Krause, M. Huetten, O. M. Weiner, M. Kertzman, M. Buchovecky, A. O'Faolain de Bhroithe, Karen Byrum, J. D. Eisch, A. Weinstein, K. Meagher, Henrike Fleischhack, A. W. Smith, T. B. Humensky, S. Archambault, Martin Pohl, Gordon T. Richards, Geza Gyuk, P. Fortin, Marcos Santander, J. Dumm, Ralph Bird, Jodi Christiansen, John L. Quinn, P. T. Reynolds, C. B. Rulten, Matteo Cerruti, Amy Furniss, P. Moriarty, Daniel Nieto, L. Ciupik, K. Ragan, A. Wilhelm, S. Vincent, Hugh Dickinson, N. H. Park, S. O'Brien, J. V. Tucci, Gernot Maier, S. P. Wakely, R. Mukherjee, Anushka Udara Abeysekara, V. Pelassa, A. Petrashyk, P. Kar, G. H. Sembroski, David A. Williams, D. Staszak, I. Telezhinsky, Jamie Holder, L. C. Reyes, and Wei Cui

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, telescope, 01 natural sciences, law.invention, Telescope, swift, law, gamma-ray astronomy, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, relativistic processes, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, 010308 nuclear & particles physics, tev blazars, Institut für Physik und Astronomie, Astronomy, Astronomy and Astrophysics, Gamma-ray astronomy, source catalog, lac objects, spectral energy-distributions, Crab Nebula, x-ray, Space and Planetary Science, astroparticle physics, Spectral energy distribution, ddc:520, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, fermi, galaxies: individual: 1es 1741+196=ver j1744+195, discovery, BL Lac object
Abstract

Monthly notices of the Royal Astronomical Society 459(3), 2550 - 2557 (2016). doi:10.1093/mnras/stw664, We present results from multiwavelength observations of the BL Lacertae object 1ES 1741 + 196, including results in the very high energy γ-ray regime using the Very Energetic Radiation Imaging Telescope Array System (VERITAS). The VERITAS time-averaged spectrum, measured above 180 GeV, is well modelled by a power law with a spectral index of 2.7 ± 0.7$_{stat}$ ± 0.2syst. The integral flux above 180 GeV is (3.9 ± 0.8$_{stat}$ ± 1.0$_{syst}$) × 10$^{−8}$ m$^{−2}$ s$^{−1}$, corresponding to 1.6 per cent of the Crab nebula flux on average. The multiwavelength spectral energy distribution of the source suggests that 1ES 1741+196 is an extreme-high-frequency-peaked BL Lacertae object. The observations analysed in this paper extend over a period of six years, during which time no strong flares were observed in any band. This analysis is therefore one of the few characterizations of a blazar in a non-flaring state., Published by Oxford Univ. Press, Oxford

Published
2016
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16. TeV Gamma-ray Observations of The Galactic Center Ridge By VERITAS

Author

Julien Rousselle, V. V. Vassiliev, J. V. Tucci, A. Furniss, Avery Archer, S. P. Wakely, T. B. Humensky, M. J. Lang, Maria Krause, Wystan Benbow, A. Popkow, J. Tyler, P. Kaaret, K. Ragan, Lucy Fortson, A. Flinders, J. H. Buckley, B. Zitzer, M. Kertzman, John L. Quinn, N. Håkansson, S. McArthur, Martin Pohl, Marcos Santander, E. Roache, P. T. Reynolds, Matteo Cerruti, Geza Gyuk, J. V. Cardenzana, D. A. Williams, K. Meagher, G. Ratliff, S. Griffin, Abraham D. Falcone, Karlen Shahinyan, C. A. Johnson, H. Fleischhack, M. Buchovecky, Sanjay Kumar, E. Collins-Hughes, J. Millis, David Kieda, F. Krennrich, Ralph Bird, A. McCann, D. S. Hanna, Q. Feng, N. H. Park, J. P. Finley, V. Bugaev, I. Telezhinsky, Karen Byrum, Jamie Holder, A. Weinstein, O. M. Weiner, N. Kelley-Hoskins, A. Wilhelm, R. A. Ong, M. P. Connolly, Xian Chen, J. Eisch, G. H. Sembroski, R. Mukherjee, L. Ciupik, V. Pelassa, Farhad Yusef-Zadeh, M. Hütten, P. Kar, G. H. Gillanders, J. Grube, Daniel Nieto, D. Staszak, P. Moriarty, E. Pueschel, A. W. Smith, and Gordon T. Richards

Subjects
galaxy: center, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, molecular clouds, Astrophysics::Cosmology and Extragalactic Astrophysics, telescope, 01 natural sciences, supernovae: individual (g0.9+0.1), 0103 physical sciences, emission, center region, chandra observations, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Supermassive black hole, 010308 nuclear & particles physics, Molecular cloud, Galactic Center, Institut für Physik und Astronomie, Astronomy and Astrophysics, gamma rays: general, Galactic plane, Galaxy, Black hole, Supernova, Space and Planetary Science, sagittarius b2 cloud, ddc:520, High Energy Physics::Experiment, high-energy, Astrophysics - High Energy Astrophysical Phenomena, sgr-a-asterisk, stellar clusters, center black-hole
Abstract

The astrophysical journal 821(2), 129 (2016). doi:10.3847/0004-637X/821/2/129, The Galactic Center ridge has been observed extensively in the past by both GeV and TeV gamma-ray instrumentsrevealing a wealth of structure, including a diffuse component and the point sources G0.9+0.1 (a compositesupernova remnant) and Sgr A*(believed to be associated with the supermassive black hole located at the center of our Galaxy). Previous very high energy (VHE) gamma-ray observations with the H.E.S.S. experiment have also detected an extended TeV gamma-ray component along the Galactic plane in the > 300 GeV gamma-ray regime. Here we report on observations of the Galactic Center ridge from 2010 to 2014 by the VERITAS telescope array in the > 2 TeV energy range. From these observations we (1) provide improved measurements of the differential energy spectrum for Sgr A* in the > 2 TeV gamma-ray regime, (2) provide a detection in the > 2 TeV gamma-ray emission from the composite SNR G0.9+0.1 and an improved determination of its multi-TeV gamma-ray energy spectrum, and (3) report on the detection of VER J1746-289, a localized enhancement of > 2 TeV gamma-rayemission along the Galactic plane., Published by Univ.11032, Chicago, Ill. [u.a.]

Published
2016
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17. Aspect angle for interstellar magnetic field in SN 1006

Author

Marco Miceli, G. Castelletti, Salvatore Orlando, Oleh Petruk, I. Telezhinsky, M. G. F. Kirsch, Fabrizio Bocchino, Gloria Mabel Dubner, and Dmytro Iakubovskyi

Subjects
Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, Electron, NON-THERMAL [RADIATION MECHANISMS], law.invention, ACCELERATION OF PARTICLES, INDIVIDUAL: SN 1006 [ISM], purl.org/becyt/ford/1 [https], law, Surface brightness, Astrophysics::Galaxy Astrophysics, Physics, Line-of-sight, Astrophysics (astro-ph), Astronomy and Astrophysics, COSMIC RAYS, purl.org/becyt/ford/1.3 [https], Synchrotron, Magnetic field, Astronomía, Azimuth, Supernova, Space and Planetary Science, CIENCIAS NATURALES Y EXACTAS
Abstract

A number of important processes taking place around strong shocks in supernova remnants (SNRs) depend on the shock obliquity. The measured synchrotron flux is a function of the aspect angle between interstellar magnetic field (ISMF) and the line of sight. Thus a model of non-thermal emission from SNRs should account for the orientation of the ambient magnetic field. We develop a new method for the estimation of the aspect angle, based on the comparison between observed and synthesized radio maps of SNRs, making different assumptions about the dependence of electron injection efficiency on the shock obliquity. The method uses the azimuthal profile of radio surface brightness as a probe for orientation of ambient magnetic field because it is almost insensitive to the downstream distribution of magnetic field and emitting electrons. We apply our method to a new radio image of SN 1006 produced on the basis of archival VLA and Parkes data. The image recovers emission from all spatial structures with angular scales from few arcseconds to 15 arcmin. We explore different models of injection efficiency and find the following best-fitting values for the aspect angle of SN 1006: phi=70 +/- 4.2 deg if the injection is isotropic, phi=64 +/- 2.8 deg for quasi-perpendicular injection (SNR has an equatorial belt in both cases) and phi=11 +/- 0.8 deg for quasi-parallel injection (polar-cap model of SNR). In the last case, SN 1006 is expected to have a centrally-peaked morphology contrary to what is observed. Therefore, our analysis provides some indication against the quasi-parallel injection model., Comment: Accepted for publication in MNRAS

Published
2009
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18. HIGH ENERGY SIGNATURES OF POST ADIABATIC SUPERNOVA REMNANTS

Author

I. Telezhinsky and Bohdan Hnatyk

Subjects
Physics, Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, General Physics and Astronomy, Astronomy and Astrophysics, Astrophysics, Near-Earth supernova, Luminosity, Interstellar medium, Supernova, Radiative transfer, Gamma-ray burst, Adiabatic process, Supernova remnant, Astrophysics::Galaxy Astrophysics
Abstract

Between the well-known adiabatic and radiative stages of the Supernova remnant (SNR) evolution there is, in fact, a transition stage with a duration comparable to the duration of adiabatic one. Physical existence of the transition stage is motivated by cooling of some part of the downstream hot gas with formation of a thin cold shell that is joined to a shell of swept up interstellar medium (ISM). We give an approximate analytical method for full hydrodynamical description of the transition stage. On its base we investigate the evolution of X-ray and γ-ray radiation during this stage. It is shown that formation of a dense shell during the transition stage is accompanied by the decrease of X-ray luminosity because of hot gas cooling and increase of gamma-ray flux according to the increase of target proton density and CR energy in the newly born shell. The role of nonuniformity of ISM and its influence on the high energy fluxes from the SNRs is also discussed.

Published
2007
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20. Gamma rays from the quasar PKS 1441+25: story of an escape

Author

Wystan Benbow, S. McArthur, O. M. Weiner, N. Håkansson, Henrike Fleischhack, M. J. Lang, P. Fortin, Ralph Bird, N. Kelley-Hoskins, L. Ciupik, R. Reeves, Geza Gyuk, Paul S. Smith, G. M. Madejski, Martin Pohl, Thomas W.-S. Holoien, A. O'Faolain de Bhroithe, J. Grube, Matthew J. Graham, R. A. Ong, A. McCann, K. Ragan, A. Petrashyk, K. Meagher, E. Pueschel, Marcos Santander, A. Wilhelm, Maria Krause, P. Kar, Benjamin J. Shappee, Talvikki Hovatta, S. G. Djorgovski, Paolo De Coppi, J. Tyler, M. P. Connolly, A. A. Mahabal, G. Ratliff, A. Archer, Xuhui Chen, J. H. Buckley, Lucy Fortson, Jodi Christiansen, S. Archambault, Q. Feng, P. Moriarty, Anthony C. S. Readhead, V. V. Vassiliev, A. Flinders, J. S. Perkins, Reshmi Mukherjee, Abraham D. Falcone, Hugh Dickinson, G. H. Gillanders, Karlen Shahinyan, David Kieda, Y. Khassen, T. B. Humensky, J. V. Tucci, Matteo Cerruti, N. W. Todd, Amy Furniss, G. H. Sembroski, D. S. Hanna, F. Krennrich, Daniel Nieto, A. Popkow, T. J. Pearson, Gernot Maier, J. L. Richards, Christopher S. Kochanek, T. Aune, Moritz Hütten, Wei Cui, John L. Quinn, B. Zitzer, P. Kaaret, J. V. Cardenzana, P. T. Reynolds, Walter Max-Moerbeck, Julien Rousselle, Manel Errando, S. Kumar, S. P. Wakely, C. A. Johnson, J. L. Prieto, Sinéad M. Griffin, Jonathan Biteau, Andrew J. Drake, J. P. Finley, J. P. Dumm, S. Vincent, A. W. Smith, J. D. Eisch, A. Weinstein, Gordon T. Richards, E. Roache, V. Bugaev, K. Z. Stanek, Nahee Park, Anushka Udara Abeysekara, Anna Barnacka, A. N. Otte, I. Telezhinsky, Jamie Holder, David A. Williams, D. Staszak, and ~

Subjects
extragalactic background light, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), spectra, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, telescope, Astrophysical jet, gamma rays: galaxies, emission, complete sample, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Supermassive black hole, variability, Gamma ray, Astronomy and Astrophysics, Quasar, radiation mechanisms: non-thermal, Galaxy, diffuse radiation, radiation, Extragalactic background light, mission, Space and Planetary Science, cosmology: observations, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, Schwarzschild radius, absorption, fermi blazars, quasars: individual (pks 1441+25-ver j1443+250), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The astrophysical journal / 2 815(2), L22 -(2015). doi:10.1088/2041-8205/815/2/L22, Outbursts from gamma-ray quasars provide insights on the relativistic jets of active galactic nuclei and constraints on the diffuse radiation fields that fill the universe. The detection of significant emission above 100 GeV from a distant quasar would show that some of the radiated gamma-rays escape pair-production interactions with low-energy photons, be it the extragalactic background light (EBL), or the radiation near the supermassive black hole lying at the jet's base. VERITAS detected gamma-ray emission up to ~200 GeV from PKS 1441+25 (z = 0.939) during 2015 April, a period of high activity across all wavelengths. This observation of PKS 1441+25 suggests that the emission region is located thousands of Schwarzschild radii away from the black hole. The gamma-ray detection also sets a stringent upper limit on the near-ultraviolet to near-infrared EBL intensity, suggesting that galaxy surveys have resolved most, if not all, of the sources of the EBL at these wavelengths., Published by Institute of Physics Publ., London

Published
2015
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21. Introducing the CTA concept

Author

A. Mathieu, R. G. Wagner, K. Panagiotidis, S Rosier Lees, Julien Rousselle, M. Gómez Berisso, Michela Uslenghi, Stephen Maxfield, R. C. Shellard, Ivica Puljak, T. Le Flour, Thomas Schanz, Tobias C. Walther, Juanan Aguilar, Pierre Colin, M. Chikawa, N. Fouque, Mosè Mariotti, G. Fontaine, Merja Tornikoski, V. Diez-Blanco, Enrico Giro, A. Krepps, G. Koss, J. M. Martin, Sergio Billotta, E. de Oña Wilhelmi, Keitaro Takahashi, S. Buson, P. Brook, S. Steiner, M. Dyrda, Joseph Silk, Sera Markoff, P. Lubinski, U. Schwanke, Sauvik Bhattacharyya, J. Ripken, T. Haubold, C. Zurbach, H. Wetteskind, R. Hermel, J. Darling, J. Nicolau-Kukliński, Konstancja Satalecka, M. Videla, Stefan Funk, P. Conconi, S. Bajtlik, Lukasz Stawarz, J. M. Paredes, K. Reitberger, Stefan Wagner, Teresa Mineo, David Kieda, G. Pareschi, Shigeto Kabuki, Makoto Sawada, Antonio Stamerra, Rodolfo Canestrari, N. Baby, G. Crimi, P. Kostka, J. Grube, R. Zanin, I. K. Kominis, L. Mc Comb, R. Sternberger, M. Fesquet, M. Tokarz, David Fink, Daniela Dorner, N. Hamer Heras, A. Moralejo Olaizola, M. de Naurois, Diego F. Torres, Claes Fransson, K. Nishijima, Yutaka Fujita, L. Fresnillo, B. García, R. Kossakowski, A. Masserot, H. von Gunten, Alkiviadis F. Bais, Ciro Bigongiari, A. Saggion, G. Papyan, I. Mrusek, K. Farakos, J. Michałowski, A. Franckowiak, Fernando Martinez, M. Doert, R. Wawrzaszek, Michele Doro, L. Sapozhnikov, Claudia Lavalley, D. Thuermann, A.A. Zdziarski, Cristina Knapic, Karen Byrum, N. Neyroud, Petr Schovanek, W. Domainko, D. Kastana, E. Birsin, Adrian Biland, F. Sánchez, Alexandre Marcowith, M. Errando, R. L. C. Starling, J. Schultze, A. Weinstein, B. B. Singh, Yassir Moudden, Jelena Aleksić, C. L. Naumann, V. Waegebaert, M. Shayduk, U. F. Katz, Gianpiero Tagliaferri, M. Schroedter, A. Vollhardt, O. Reimann, Hideyuki Ohoka, Vincenzo Testa, C. Jablonski, Tsuguya Naito, J. Schäfer, Stavros Maltezos, A. Wierzcholska, P. Wawer, L. Nellen, F. Mirabel, Tatsuo Yoshida, P. H. Carton, Nina Nowak, L. Platos, Riccardo Rando, P. P. Krueger, R. Wischnewski, W. Romaszkan, E. Fede, Martino Marisaldi, Markus Gaug, Richard Willingale, J. H. Buckley, U. De AlmeidaBarres, J. Knapp, Saverio Lombardi, D. della Volpe, A. Herrero, A. Bottani, E. Delagnes, Martin J. Hardcastle, C. Morello, Anna Lipniacka, T. Greenshaw, M. Renaud, Giancarlo Cusumano, Jonathan Biteau, M. Sowiński, J. R. T. de Mello Neto, T. B. Humensky, Michael G. Richer, G. Parks, G. Grasseau, H. Baba, Gino Tosti, Damir Lelas, H. Krawzcynski, David Paneque, M. Barcelo, R. Dickherber, P. Ferrando, Shinji Hara, D. Florin, Hideaki Katagiri, T. Shibata, Fuyuki Tokanai, N. A. McCubbin, J. Gomez-Ortega, D. Nakajima, A. Liolios, P. Laporte, Orjan Dale, A. Sillanpää, Dainis Dravins, Timothée Grégoire, Nu. Komin, A. Mihailidis, L. Sidoli, Shiu-Hang Lee, A. W. Chen, J. M. Illa, A. Kuznetsov, P. Munar-Adrover, D. Dominis Prester, Marcos Daniel Actis, Abraham D. Falcone, L. Journet, D. Hadasch, N. Galante, A. Murphy, C. J. Todero Peixoto, S. Wiesand, A. Aravantinos, A. C. Rovero, J. L. Dournaux, P. Romano, M. Hrabovsky, R. de los Reyes Lopez, M. Ostrowski, J. Pallota, Geza Gyuk, Petar Temnikov, R. Dubois, Jan Ebr, R. Koul, David J. Smith, S. Schwarzburg, P. Manigot, Chad Finley, Tarek M. Hassan, Giuseppe Sottile, Evgeni Ovcharov, P. J. Rajda, F. Krennrich, Peter L. Moore, W. B. Focke, W. Bednarek, Elena Amato, Kazunori Kohri, J. Gamez-Garcia, I. Oya, A. Shibuya, German Hermann, William H. Lee, Dorota Sobczyńska, X. Zhou, C. Balkowski, G. Vallejo, M. Hayashida, M. Bitossi, Loukas Vlahos, H. Lockart, N. Geffroy, L. Tibaldo, Marek Jamrozy, Luke O'c. Drury, Pratik Majumdar, P. Sutcliffe, S. Schlenstedt, M. Palatka, Christophe Champion, H. Ueno, M. Rupiński, P. Giommi, J. Schwarz, G. Pühlhofer, Takashi Saito, W. van Driel, C. van Eldik, Q. Xiong, Yasuo Fukui, A. Donat, A. Ibarra, R. S. Warwick, Michiko Ohishi, A. W. Smith, J.-P. Lenain, Aion Viana, Terry Ashton, Guillaume Dubus, Jacek Niemiec, K. Kodani, Luis Ángel Tejedor, A. Wörnlein, Takanori Yoshikoshi, Masahiro Teshima, W. Gäbele, Ll. Font, Olaf Reimer, J. F. Valdés-Galicia, Lucy Fortson, J. P. Osborne, Mattia Fornasa, Keith Bechtol, Masayuki Tanaka, Shigehiro Nagataki, M. Rataj, M. Ribordy, Emmanuel Moulin, I. de la Calle, K. Winiarski, C. Jeanney, I. Mognet, I. Vegas, C. Juffroy, Yutaka Ohira, A. Jacholkowska, Matthew Wood, A. E. Suárez, J. Bähr, K. M. Schure, J. Maya, M. Dafonseca, J. Tasan, R. Sugawara, M. Bourgeat, A. Mancilla, D. Pelat, Olga Botner, D. Nedbal, G. Depaola, Robert Wagner, T. Okuda, H. Arnaldi, Josep Martí, P. Corona, T. Bonev, D. Yelos, J. Sieiro, V. Scalzotto, Jacco Vink, D. Languignon, Marco Ajello, J. Vandenbrouke, Philipp Mertsch, M. Mordalska, P. Wegner, P. Ziółkowski, P. T. O'Brien, A. Nozato, Robert D. Preece, B. Huber, Matteo Balbo, J.R. Bogart, R. Kankanyan, K. Mori, T. Jogler, Seth Digel, Claudio Vuerli, Hiromitsu Takahashi, Thomas Lohse, K. Saito, A. W. Borgland, Elisa Prandini, Helene Sol, Ryan Heller, M. Bogdan, D. Dumas, M. Stodulski, Y. Awane, Piercarlo Bonifacio, Pedro L. Luque-Escamilla, Judith H. Croston, Fabio Pizzolato, P. M. Chadwick, M. K. Daniel, Riccardo Paoletti, Reiko Orito, Katsuaki Asano, R. Frei, G. Disset, Valerie Connaughton, Juhani Huovelin, Hiroyasu Tajima, S. Vercellone, F. Feinstein, G. Decerprit, Riccardo Smareglia, S. Spyrou, Gustavo E. Romero, J. Shi, J. Carr, N. Girard, Dirk L. Hoffmann, Andreas Zech, Markus Boettcher, Osvaldo Catalano, Akira Okumura, M. Dohmke, C. Föhr, Sabrina Casanova, R. A. Cameron, Jan Conrad, K. Umehara, K. K. Yadav, A. Paizis, John L. Quinn, L. Pogosyan, C. Farnier, William J. Potter, Domenico Impiombato, Tadashi Kifune, Jonathan Granot, Gernot Maier, M. Cieślar, S. Palanque, G.W. Fraser, J. Prast, R. Bose, Heidi Sandaker, G. Lamanna, Dusan Mandat, J.F. Glicenstein, J. Harris, D. Naumann, J. Ziolkowski, Michał Szanecki, C. Delgado, J. Kocot, W. Lustermann, Sabine Elles, J. Schmoll, L. Gérard, M. López, Norita Kawanaka, V. Gika, B. Lieunard, A. Pichel, Martin Pohl, Mariusz Sterzel, S. Vincent, Paolo De Coppi, J. Lande, O. Blanch Bigas, Gianluca Giavitto, Yusuke Konno, Julian Sitarek, M. Panter, P.-O. Petrucci, F. Henault, M. Prouza, Philip Kaaret, Josep Colomé, Luciano Nicastro, German Martinez, L. Gebremedhin, J. M. Yebras, Apostolos Mastichiadis, A. S. Madhavan, Thomas J. Maccarone, K. Berger, R. Buehler, P. Jean, N. Sartore, F. Toussenel, Aris Karastergiou, W. Kluźniak, A. Djannati-Ataï, S. J. Fegan, Louis Antonelli, A. González Muñoz, J. Berdugo, S. S. Upadhya, M. Sidz, F. Mottez, Patrick Vogler, F. Di Pierro, Wystan Benbow, B. Sacco, L. Chiappetti, J. Dumm, R. Firpo Curcoll, David Gascon, V. Boccone, J. Krause, J. P. Avernet, B. Peyaud, B. De Lotto, Ana Babić, T. O. B. Schmidt, I. M. McHardy, T. Schweizer, S. P. Wakely, Daniel Gall, Frank M. Rieger, E. Sant'Ambrogio, M. Kagaya, P. Vincent, R. C. Rannot, Sandro Mereghetti, A. De Angelis, M. Scarcioffolo, R. White, G. H. Sembroski, Takeshi Nakamori, C. Medina, M. A. De Oliveira Leigui, Subir Sarkar, A. Marszałek, Reshmi Mukherjee, K. Nakayama, A. Fiasson, S. Giarrusso, T. Bernardino, J. P. Finley, D. Neise, L. O. Takalo, F. Grañena, Nikola Godinovic, H. Sasaki, P. Zychowski, Francesco Dazzi, B. Courty, A. Basili, Vitaly Neustroev, B. Khélifi, T. Glanzman, M. Trifoglio, Regis Terrier, R. A. Ong, E. M. Santos, M. Minuti, Thomas Bretz, R. Moderski, J. Kushida, S. Royer, Emilio Molinari, Etienne Lyard, J. Houles, Juan Abel Barrio, T. Lerch, S. Rivoire, T. Kishimoto, M. Cailles, M. Casiraghi, Nikolaos Stergioulas, J. Gaweda, S. Koyama, Ingomar Allekotte, E. Ismailova, Elina Giannakaki, S. Schwemmer, Ryo Yamazaki, G. Fasola, Christoph Deil, Jose Luis Contreras, T. Bird, Miguel A. Sánchez-Conde, J. Dick, E. Edy, D. Parsons, R. Pyzioł, R. Mirzoyan, Manjuli R. Sharma, J. Borkowski, Jonathan S. Lapington, Cameron B Rulten, Rino Bandiera, Volker Beckmann, Jun Kakuwa, Dimitris Balis, Kenji Toma, Anna Barnacka, Andrea Santangelo, L. Padilla, Peter Eger, G. Decock, Karol Seweryn, N. Sakaki, Darko Veberič, Andrea Bulgarelli, B. Rudak, M. Pérez, H. Koppel, Felix Spanier, M. I. Martínez, D. Horville, Marco Molinaro, R. Walter, P. Ramon, S. Brau-Nogue, J. Camprecios, K. Kärcher, John H. Seiradakis, S. Criswell, D. J. Leopold, V. J. Guarino, R. Gredig, S. Vorobiov, Viktor Gruev, Gareth Hughes, Daniele Spiga, Quirin Weitzel, N. Håkansson, Susumu Inoue, U. Straumann, Juan Cortina, B. Behera, Jürgen Knödlseder, Daniel Nieto, Tomasz Szepieniec, H. Prokoph, Jerzy Grygorczuk, G. De La Vega, Jim Hinton, E. Chabanne, M. Mahabir, R. Krobot, M. Capalbi, Miroslav Pech, C. Díaz, J. Ludwin, F. Gianotti, Garret Cotter, Claudio Melioli, Hiroaki Yamamoto, C. Veyssiere, Kunihito Ioka, S. Sun, J. M. Parraud, L. Rob, Felix Aharonian, G. Maneva, D. Melkumyan, T. Schwab, J. Kasperek, J. M. Huet, E. Lorenz, S. Tanaka, Y. A. Gallant, S. Couturier, B.W. Favill, J. Boix Gargallo, Andrea Tiengo, Leszek Bogacz, Andreu Sanuy, Christian Fruck, J. Sykes, C. Martens, A. Yoshida, Marek Sikora, E. Racero, G. Rouaix, N. Bhat, A. Salini, A. S. Barber, Mauro Ghigo, Jan Ridky, K. Kosack, Konrad Bernlöhr, C. Tenzer, Alice Allafort, M. Torres, Catherine Boisson, Grzegorz Kowal, M. Karczewski, G. Agnetta, Victor Stamatescu, Anthony H. Gonzalez, S. Rousselle, Giovanni Bonanno, A. Zajczyk, A. Gadola, P. Martin, V. Zitelli, I. Manthos, N. Maragos, A. Dettlaff, F. Profeti, S. Colonges, S. Gunji, S. Cazaux, S. Colafrancesco, M. Paz Arribas, Rika Hagiwara, Darell Engelhaupt, Nestor Mirabal, Johann Cohen-Tanugi, S. Grunewald, Abby M. Green, I. D. Davids, D. Nosek, T. Yamamoto, Gagik Tovmassian, R. Sakonaka, Miguel Alcubierre, C. Baixeras, T. L. Usher, Kazufumi Torii, H. Lüdecke, L. Wiśniewski, B. Kellner-Leidel, P. Demange, F. Gonzalez, B. Moal, V. De Caprio, V. Golev, K. Katarzyński, V. Bugaev, A. Reimer, J. Koziol, G. Pojmanski, Alessandro Carosi, J. Bolmont, A. Nikolaidis, R. J. García López, V. A. Kudryavtsev, C. Stegmann, J.-P. Ernenwein, M. Fiorini, Ivone F. M. Albuquerque, Marco Tavani, P. Korohoda, A. Giuliani, E. Carmona, C. Bauer, Kostas D. Kokkotas, O. Tibolla, G. Deleglise, Pierre Brun, Dinko Dimitrov, I. Jung, R. Steenkamp, Marc Ribó, Kathrin Egberts, P. Reardon, Adriano Ghedina, Stefan Rosén, N. Hidaka, Trygve Buanes, A. Segreto, H. Huan, Juri Poutanen, Ruben Lopez-Coto, S. Cavazzani, Massimiliano Belluso, A. Kretzschmann, F. De Frondat, A. Riviere, J. F. Olive, Tsunefumi Mizuno, Serena Mattiazzo, M. González, D. Fantinel, Matteo Cerruti, S. Vergani, Sabrina Einecke, N. La Palombara, Reinhard Schlickeiser, P. Antoranz, Pol Bordas, D. Paillot, V. de Souza, Yasushi Fukazawa, Phil Evans, Werner Hofmann, Hugh Dickinson, F. Roy, Yvonne Becherini, E. O. Angüner, D. Corti, T. C. Arlen, Francesco Russo, V. R. Chitnis, D. Ross, R. Gabriele, Massimo Persic, E. Fokitis, A. Bonardi, D. Garrido, A. Niedźwiecki, L. Cossio, Hidetoshi Kubo, Y. de Oliveira, F. Mattana, Anna Szostek, M. Compin, S. Blake, F. Lucarelli, Petter Hofverberg, Felix Ryde, M. Gougerot, C. Boutonnet, Dimitrios Emmanoulopoulos, A. Mangano, P. Vallania, Jose Miguel Miranda, A. Manalaysay, M. Raue, A. Bouvier, Shohei Yanagita, Nektarios Vlahakis, Joni Tammi, M. Naumann-Godo, Kohta Murase, E. Fillin-Martino, Jiri Chudoba, K. Hatanaka, A. Lopatin, N. Otte, G. Rojas, Tomonori Totani, K. S. Gothe, J. P. Vialle, D. Kolitzus, K. Warda, Hironori Matsumoto, J. Rico, P. Ringegni, James Chiang, R. McKay, A. Bobkov, Aya Bamba, H. Takami, B. Giebels, O. Grimm, S. Basso, F. Dubois, Victor Zabalza, A. Förster, Pasquale Blasi, Alexandros Papayannis, A. G. Akhperjanian, Eckhard Kendziorra, James A. Anderson, Giuseppe Malaguti, R. Welsing, S. Pita, A. Ozieblo, Heide Costantini, D. Tezier, J.-H. Köhne, M. Tluczykont, Ll. Garrido, Alexander Varón Sandoval, Matthew R. Orr, Dominique Durand, F. Chollet, O. Luz, E. O. Saemann, Jun Kataoka, M. Proyetti, C. Barbier, Jürgen Barnstedt, L. Bouchet, Hiroshi Muraishi, Anton N. Baushev, L. A. Otero, Denis Bastieri, S. Incorvaia, Tihomir Surić, V. La Parola, Nathan Smith, Karl-Heinz Sulanke, F. Bernard, Luca Stringhetti, S. Paiano, S. Federici, Hector Flores, Karl Mannheim, Michael S. Briggs, Giovanna Pedaletti, E. M. de Gouveia Dal Pino, J. D. Smith, G. La Rosa, Alicia López-Oramas, M. Janiak, Gary Drake, G. Talbot, Petr Travnicek, Elisabetta Bissaldi, Mario Meucci, R. Northrop, V. Scapin, Vito Conforti, J. D. Ponz, T. Aghajani, J. J. Jimenez, A. D. Supanitsky, Hernán Asorey, M. Werner, Brian Reville, A. Haupt, C. Skole, Gilles Henri, Daniele Gardiol, V. Vassiliev, R. Platzer, Y. Saito, A. La Barbera, Allan Hallgren, C. Eleftheriadis, S. Cantu, G. Maurin, K. Lacombe, A. Le Padellec, F. Stinzing, T. Hayakawa, A. Cillis, M. Suchenek, I. Monteiro, V. Sahakian, A. Di Paola, Grzegorz Madejski, A. De Luca, Andreas Quirrenbach, P. A. Caraveo, N. A. 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K., Yadav, H., Yamamoto, T., Yamamoto, R., Yamazaki, S., Yanagita, J. M., Yebra, D., Yelo, A., Yoshida, T., Yoshida, T., Yoshikoshi, V., Zabalza, M., Zacharia, A., Zajczyk, R., Zanin, A., Zdziarski, A., Zech, A., Zhao, X., Zhou, K., Zietara, J., Ziolkowski, P., Ziolkowski, V., Zitelli, C., Zurbach, P., Zychowski, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), 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), AstroParticule et Cosmologie (APC (UMR_7164)), 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), APC - Astrophysique des Hautes Energies (APC - AHE), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Centre de Physique des Particules de Marseille (CPPM), 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 de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, CTA, 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Laboratoire d'Annecy de Physique des Particules (LAPP), 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)-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)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Aix Marseille Université (AMU)-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 Paris Diderot - Paris 7 (UPD7), 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), 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)-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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Next generation Cherenkov telescopes, Ciencias Físicas, 01 natural sciences, 7. Clean energy, TeV GAMMA-RAY ASTRONOMY, Observatory, Air showers, HESS, Cherenkov Telescopes, 010303 astronomy & astrophysics, MISSION, SUPERNOVA REMNANT W44, TELESCOPE, ASTRONOMY, EMISSION, Physics, ta213, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, TeV gamma-ray astronomy, ddc:540, CIENCIAS NATURALES Y EXACTAS, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Air shower, AIR SHOWERS, Astrophysics::High Energy Astrophysical Phenomena, 0103 physical sciences, Preparatory phase, ta115, TeV gamma-ray astronomy Air showers Cherenkov Telescopes, 010308 nuclear & particles physics, business.industry, CHERENKOV TELESCOPES, Física, Astronomy, Institut für Physik und Astronomie, Astronomy and Astrophysics, ASTROFÍSICA, Cherenkov Telescope Array, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astronomía, Design study, Telecommunications, business
Abstract

The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project., La lista completa de autores puede consultarse en el documento o en la página web de la revista., Facultad de Ingeniería

Published
2013
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22. Erratum: VERITAS deep observations of the dwarf spheroidal galaxy Segue 1 [Phys. Rev. D85, 062001 (2012)]

Author

M. P. Connolly, D. Staszak, K. Ragan, R. Dickherber, S. Thibadeau, L. Ciupik, A. Varlotta, H. J. Rose, D. S. Hanna, T. C. Arlen, P. Kaaret, D. B. Saxon, E. Collins-Hughes, G. H. Sembroski, G. Hughes, Matthias Beilicke, A. McCann, A. Cesarini, M. Vivier, John L. Quinn, Francesc Ferrer, S. Archambault, Reshmi Mukherjee, K. Tsurusaki, Gernot Maier, Nahee Park, S. P. Wakely, C. Skole, A. Bouvier, Geza Gyuk, J. E. Ward, R. A. Ong, Thomas Weisgarber, Daniel Gall, E. Aliu, Matthew R. Orr, David Kieda, K. L. Byrum, Jodi Christiansen, J. S. Perkins, S. M. Bradbury, G. Tešić, David A. Williams, Lucy Fortson, A. Cannon, Pratik Majumdar, V. V. Vassiliev, T. Aune, I. Telezhinsky, Jamie Holder, S. Godambe, J. P. Dumm, J. Ruppel, Q. Feng, L. C. Reyes, Henric Krawczynski, Amy Furniss, A. J.R. Weinstein, T. B. Humensky, M. Schroedter, Wei Cui, S. McArthur, V. Bugaev, Wystan Benbow, F. Krennrich, G. Finnegan, A. W. Smith, M. Theiling, A. S Madhavan, A. D. Falcone, E. Roache, G. D. Şentürk, H. Huan, J. H. Buckley, P. Moriarty, Nicola Galante, J. Grube, R. G. Wagner, N. Karlsson, Sinéad M. Griffin, Y. Khassen, G. Decerprit, S. Vincent, M. Kertzman, A. N. Otte, P. T. Reynolds, B. Zitzer, Manel Errando, J. P. Finley, T. C. Weekes, M. Pohl, K. Lee, and H. Prokoph

Subjects
Physics, Gravitation, Nuclear and High Energy Physics, Dark matter, Gamma ray, Astronomy, Astrophysics, Segue, Cosmology, Dwarf galaxy, Dwarf spheroidal galaxy
Published
2015
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23. Multiwavelength observations of Mrk 501 in 2008

Author

MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Ansoldi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), A. Babic(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), P. Bangale(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Lodz, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Bonnefoy(Universidad Complutense, E-28040 Madrid, Spain), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), F. Borracci(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, D-97074 Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), M. Doert(Technische Universität Dortmund, D-44221 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, HR-10000 Zagreb, Croatia), D. Dorner(Universität Würzburg, D-97074 Würzburg, Germany), M. Doro(Università di Padova and INFN, I-35131 Padova, Italy), S. Einecke(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), E. Farina(Università dell'Insubria, Como, I-22100 Como, Italy), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), K. Frantzen(Technische Universität Dortmund, D-44221 Dortmund, Germany), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Deutsches Elektronen-Synchrotron), D. Garrido Terrats(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), M. Gaug(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), W. Idec(University of Lodz, PL-90236 Lodz, Poland), V. Kadenius(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), M. L. Knoetig(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), S. Lombardi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), I. Lozano(Universidad Complutense, E-28040 Madrid, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(2,*), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Menzel(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Niedzwiecki(University of Lodz, PL-90236 Lodz, Poland), K. Nilsson(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), N. Nowak(Max-Planck-Institut für Physik, D-80805 München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Overkemping(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), D. Paneque(6,*), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Paredes(Universitat de Barcelona), X. Paredes-Fortuny(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), S. Preziuso(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), R. Reinthal(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), J. Rodriguez Garcia(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), T. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(7,*), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Lodz, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(INAF National Institute for Astrophysics, I-00136 Rome, Italy), T. Steinbring(Universität Würzburg, D-97074 Würzburg, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Thaele(Technische Universität Dortmund, D-44221 Dortmund, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(Institut de Ciències de l'Espai), T. Toyama(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), VERITAS Collaboration(Deutsches Elektronen-Synchrotron), (Deutsches Elektronen-Synchrotron), B. Behera(Deutsches Elektronen-Synchrotron), M. Beilicke(Department of Physics, Washington University, St. Louis, MO 63130, USA), W. Benbow(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Bird(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), A. Bouvier(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), V. Bugaev(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. Cerruti(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), X. Chen(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), L. Ciupik(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), E. Collins-Hughes(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), W. Cui(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), C. Duke(Department of Physics, Grinnell College, Grinnell, IA 50112-1690, USA), J. Dumm(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Falcone(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA), S. Federici(now at GRAPPA Institute, University of Amsterdam, 1098XH), Q. Feng(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), J. P. Finley(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), L. Fortson(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Furniss(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), N. Galante(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), G. H. Gillanders(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), S. Griffin(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. T. Griffiths(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), J. Grube(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), G. Gyuk(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), D. Hanna(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Holder(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), C. A. Johnson(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), P. Kaaret(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), M. Kertzman(Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA), D. Kieda(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), H. Krawczynski(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. J. Lang(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), A. S Madhavan(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), G. Maier(Deutsches Elektronen-Synchrotron), P. Majumdar(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), K. Meagher(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), P. Moriarty(Department of Life and Physical Sciences, Galway-Mayo Institute of Technology, Dublin Road, Galway, Ireland), R. Mukherjee(Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA), D. Nieto(Physics Department, Columbia University, New York, NY 10027, USA), A. O'Faoláin de Bhróithe(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), R. A. Ong(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), A. N. Otte(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), A. Pichel(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), M. Pohl(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), A. Popkow(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), H. Prokoph(Deutsches Elektronen-Synchrotron), J. Quinn(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), J. Rajotte(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), G. Ratliff(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), L. C. Reyes(Physics Department, California Polytechnic State University, San Luis Obispo, CA 94307, USA), P. T. Reynolds(Department of Applied Physics and Instrumentation, Cork Institute of Technology, Bishopstown, Cork, Ireland), G. T. Richards(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), E. Roache(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), G. H. Sembroski(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), K. Shahinyan(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), F. Sheidaei(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), A. W. Smith(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), D. Staszak(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), I. Telezhinsky(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), M. Theiling(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), J. Tyler(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), A. Varlotta(Department of Physics, Purdue University, West Lafayette, IN 47907, USA), S. Vincent(Deutsches Elektronen-Synchrotron), S. P. Wakely(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), T. C. Weekes(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Welsing(Deutsches Elektronen-Synchrotron), D. A. Williams(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), A. Zajczyk(Department of Physics, Washington University, St. Louis, MO 63130, USA), B. Zitzer(Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA), External Collaborators(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), (INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Villata(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), C. M. Raiteri(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Ajello(Space Sciences Laboratory, 7 Gauss Way, University of California, Berkeley, CA 94720-7450, USA), M. Perri(ASI-Science Data Center, Via del Politecnico, I-00133 Rome, Italy), H. D. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), M. F. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), V. M. Larionov(Astron. Inst., St.-Petersburg State Univ., Russia), N. V. Efimova(Astron. Inst., St.-Petersburg State Univ., Russia), T. S. Konstantinova(Astron. Inst., St.-Petersburg State Univ., Russia), E. N. Kopatskaya(Astron. Inst., St.-Petersburg State Univ., Russia), W. P. Chen(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), E. Koptelova(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), H. Y. Hsiao(Graduate Institute of Astronomy, National Central University, 300 Jhongda Rd., Jhongli 32001, Taiwan), O. M. Kurtanidze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), M. G. Nikolashvili(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), G. N. Kimeridze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), B. Jordan(School of Cosmic Physics, Dublin Institute For Advanced Studies, Ireland), P. Leto(INAF - Osservatorio Astrofisico di Catania, Italy), C. S. Buemi(INAF - Osservatorio Astrofisico di Catania, Italy), C. Trigilio(INAF - Osservatorio Astrofisico di Catania, Italy), G. Umana(INAF - Osservatorio Astrofisico di Catania, Italy), A. Lahtenmaki(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), E. Nieppola(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), M. Tornikoski(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), J. Sainio(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), M. Giroletti(INAF Istituto di Radioastronomia, 40129 Bologna, Italy), A. Cesarini(University of Trento, Department of Physics, I38050 Povo, Trento, Italy), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), Yu. A. Kovalev(Astro Space Center of the Lebedev Physical Institute, 117997), Y. Y. Kovalev(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), Anne Lähteenmäki Group, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, Universitat de Barcelona, School services, ELEC, and ~

Subjects
extragalactic background light, Ciencias Físicas, Flux, Electron, Astrophysics, 7. Clean energy, law.invention, purl.org/becyt/ford/1 [https], Raigs gamma, bl lacertae objects, law, individual: Mrk 501 [BL Lacertae objects], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, 213 Electronic, automation and communications engineering, electronics, Astroparticle physics, BL Lacertae objects: individual: Mrk 501, Gamma rays: general, Astronomy and Astrophysics, Space and Planetary Science, Synchrotron, individual: Mrk 50 [BL Lacertae objects], Homogeneous, astroparticle physics, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, 1171 Geosciences, Astrophysics::High Energy Astrophysical Phenomena, emitting electrons, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 114 Physical sciences, bl lacertae objects: individual: mrk 501, crab-nebula, Blazar, Astrophysics::Galaxy Astrophysics, tev blazars, variability, 221 Nanotechnology, Gamma rays, Individual: Mrk 501, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], gamma rays: general, Galaxies, gamma-ray emission, telescope system, Galàxies, Active Galaxies, blazars, gamma-rays, Mrk 501, Astronomía, Crab Nebula, x-ray, 115 Astronomy and space science, Low emission, 216 Materials engineering, Galàxies actives, active galactic nuclei, Active galaxies, ddc:520, general [gamma rays]
Abstract

Mrk 501 is one of the brightest blazars at TeV energies and has been extensively studied since its first VHE detection in 1996. Our goal is to characterize in detail the source gamma-ray emission, together with the radio-to-X-ray emission, during the non-flaring (low) activity, which is less often studied than the occasional flaring (high) activity. We organized a multiwavelength (MW) campaign on Mrk 501 between March and May 2008. This multi-instrument effort included the most sensitive VHE gamma-ray instruments in the northern hemisphere, namely the imaging atmospheric Cherenkov telescopes MAGIC and VERITAS, as well as Swift, RXTE, the F-GAMMA, GASP-WEBT, and other collaborations and instruments. Mrk 501 was found to be in a low state of activity during the campaign, with a VHE flux in the range of 10%-20% of the Crab nebula flux. Nevertheless, significant flux variations were detected with various instruments, with a trend of increasing variability with energy. The broadband spectral energy distribution during the two different emission states of the campaign can be adequately described within the homogeneous one-zone synchrotron self-Compton model, with the (slightly) higher state described by an increase in the electron number density. This agrees with previous studies of the broadband emission of this source during flaring and non-flaring states. We report for the first time a tentative X-ray-to-VHE correlation during a low VHE activity. Although marginally significant, this positive correlation between X-ray and VHE, which has been reported many times during flaring activity, suggests that the mechanisms that dominate the X-ray/VHE emission during non-flaring-activity are not substantially different from those that are responsible for the emission during flaring activity., Comment: Accepted for publication in A&A

Published
2015
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24. The 2009 multiwavelength campaign on Mrk 421: Variability and correlation studies

Author

MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Ansoldi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), L. A. Antonelli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), A. Babic(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), P. Bangale(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, D-80805 München, Germany), J. A. Barrio(Universidad Complutense, E-28040 Madrid, Spain), J. Becerra González(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), W. Bednarek(University of Lodz, PL-90236 Lodz, Poland), K. Berger(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, CH-8093 Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), R. K. Bock(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Bonnefoy(Universidad Complutense, E-28040 Madrid, Spain), G. Bonnoli(INAF National Institute for Astrophysics, I-00136 Rome, Italy), F. Borracci(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Bretz(Universität Würzburg, D-97074 Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), A. Carosi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, D-97074 Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, D-80805 München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), J. L. Contreras(Universidad Complutense, E-28040 Madrid, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. Covino(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), F. Dazzi(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), A. De Angelis(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain), M. Doert(Technische Universität Dortmund, D-44221 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, HR-10000 Zagreb, Croatia), D. Dorner(Universität Würzburg, D-97074 Würzburg, Germany), M. Doro(Università di Padova and INFN, I-35131 Padova, Italy), S. Einecke(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Eisenacher(Universität Würzburg, D-97074 Würzburg, Germany), D. Elsaesser(Universität Würzburg, D-97074 Würzburg, Germany), E. Farina(Università dell'Insubria, Como, I-22100 Como, Italy), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), M. V. Fonseca(Universidad Complutense, E-28040 Madrid, Spain), L. Font(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), K. Frantzen(Technische Universität Dortmund, D-44221 Dortmund, Germany), C. Fruck(Max-Planck-Institut für Physik, D-80805 München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Garczarczyk(Deutsches Elektronen-Synchrotron), D. Garrido Terrats(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), M. Gaug(Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), A. González Mu\ noz(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, D-44221 Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), D. Hildebrand(ETH Zurich, CH-8093 Zurich, Switzerland), J. Hose(Max-Planck-Institut für Physik, D-80805 München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), W. Idec(University of Lodz, PL-90236 Lodz, Poland), V. Kadenius(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), H. Kellermann(Max-Planck-Institut für Physik, D-80805 München, Germany), M. L. Knoetig(ETH Zurich, CH-8093 Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, I-00136 Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), N. Lewandowska(Universität Würzburg, D-97074 Würzburg, Germany), E. Lindfors(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Longo(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), S. Lombardi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), M. López(Universidad Complutense, E-28040 Madrid, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), E. Lorenz(Max-Planck-Institut für Physik, D-80805 München, Germany), I. Lozano(Universidad Complutense, E-28040 Madrid, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), K. Mannheim(Universität Würzburg, D-97074 Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, I-00136 Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN, I-35131 Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), D. Mazin(Max-Planck-Institut für Physik, D-80805 München, Germany), U. Menzel(Max-Planck-Institut für Physik, D-80805 München, Germany), M. Meucci(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Moralejo(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Niedzwiecki(University of Lodz, PL-90236 Lodz, Poland), K. Nilsson(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), N. Nowak(6,32,*), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. Overkemping(Technische Universität Dortmund, D-44221 Dortmund, Germany), S. Paiano(Università di Padova and INFN, I-35131 Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), D. Paneque(6,*), R. Paoletti(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), J. M. Paredes(Universitat de Barcelona), X. Paredes-Fortuny(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), M. Persic(Università di Udine, and INFN Trieste, I-33100 Udine, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), E. Prandini(Università di Padova and INFN, I-35131 Padova, Italy), S. Preziuso(Università di Siena, and INFN Pisa, I-53100 Siena, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), R. Reinthal(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), W. Rhode(Technische Universität Dortmund, D-44221 Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), J. Rodriguez Garcia(Max-Planck-Institut für Physik, D-80805 München, Germany), S. Rügamer(Universität Würzburg, D-97074 Würzburg, Germany), A. Saggion(Università di Padova and INFN, I-35131 Padova, Italy), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), M. Salvati(INAF National Institute for Astrophysics, I-00136 Rome, Italy), K. Satalecka(Universidad Complutense, E-28040 Madrid, Spain), V. Scalzotto(Università di Padova and INFN, I-35131 Padova, Italy), V. Scapin(Universidad Complutense, E-28040 Madrid, Spain), C. Schultz(Università di Padova and INFN, I-35131 Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, D-80805 München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy), A. Sillanpää(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Sobczynska(University of Lodz, PL-90236 Lodz, Poland), F. Spanier(Universität Würzburg, D-97074 Würzburg, Germany), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, E-08193 Bellaterra, Spain), A. Stamerra(INAF National Institute for Astrophysics, I-00136 Rome, Italy), T. Steinbring(Universität Würzburg, D-97074 Würzburg, Germany), J. Storz(Universität Würzburg, D-97074 Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, D-80805 München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), L. Takalo(Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Department of Physics, University of Oulu, Finland), F. Tavecchio(INAF National Institute for Astrophysics, I-00136 Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, HR-10000 Zagreb, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, D-80805 München, Germany), J. Thaele(Technische Universität Dortmund, D-44221 Dortmund, Germany), O. Tibolla(Universität Würzburg, D-97074 Würzburg, Germany), D. F. Torres(Institut de Ciències de l'Espai), T. Toyama(Max-Planck-Institut für Physik, D-80805 München, Germany), A. Treves(Università dell'Insubria, Como, I-22100 Como, Italy), M. Uellenbeck(Technische Universität Dortmund, D-44221 Dortmund, Germany), P. Vogler(ETH Zurich, CH-8093 Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, D-80805 München, Germany), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), VERITAS collaboration(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), (Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. Archambault(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), B. Behera(Deutsches Elektronen-Synchrotron), M. Beilicke(Department of Physics, Washington University, St. Louis, MO 63130, USA), W. Benbow(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), R. Bird(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), J. H. Buckley(Department of Physics, Washington University, St. Louis, MO 63130, USA), V. Bugaev(Department of Physics, Washington University, St. Louis, MO 63130, USA), M. Cerruti(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), X. Chen(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), L. Ciupik(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), E. Collins-Hughes(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), W. Cui(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. Dumm(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), J. D. Eisch(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), A. Falcone(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA), S. Federici(DESY, Platanenallee 6, 15738 Zeuthen, Germany), Q. Feng(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. P. Finley(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), H. Fleischhack(Deutsches Elektronen-Synchrotron), P. Fortin(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA), L. Fortson(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), A. Furniss(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), S. Griffin(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), S. T. Griffiths(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), J. Grube(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), G. Gyuk(Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA), D. Hanna(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Holder(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), G. Hughes(Deutsches Elektronen-Synchrotron), T. B. Humensky(Physics Department, Columbia University, New York, NY 10027, USA), C. A. Johnson(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), P. Kaaret(Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA), M. Kertzman(Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA), Y. Khassen(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), D. Kieda(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), H. Krawczynski(Department of Physics, Washington University, St. Louis, MO 63130, USA), F. Krennrich(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), S. Kumar(Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), M. J. Lang(School of Physics, National University of Ireland Galway, University Road, Galway, Ireland), G. Maier(Deutsches Elektronen-Synchrotron), S. McArthur(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), K. Meagher(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), P. Moriarty(Department of Life and Physical Sciences, Galway-Mayo Institute of Technology, Dublin Road, Galway, Ireland), R. Mukherjee(Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA), R. A. Ong(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), A. N. Otte(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), N. Park(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), A. Pichel(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), M. Pohl(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), A. Popkow(Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA), H. Prokoph(Deutsches Elektronen-Synchrotron), J. Quinn(School of Physics, University College Dublin, Belfield, Dublin 4, Ireland), K. Ragan(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), J. Rajotte(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), P. T. Reynolds(Department of Applied Physics and Instrumentation, Cork Institute of Technology, Bishopstown, Cork, Ireland), G. T. Richards(School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430), E. Roache(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), A. C. Rovero(Instituto de Astronomia y Fisica del Espacio, Casilla de Correo 67 - Sucursal 28), G. H. Sembroski(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), K. Shahinyan(School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA), D. Staszak(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), I. Telezhinsky(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), M. Theiling(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. V. Tucci(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), J. Tyler(Physics Department, McGill University, Montreal, QC H3A 2T8, Canada), A. Varlotta(Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA), S. P. Wakely(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA), T. C. Weekes(Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA), A. Weinstein(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), R. Welsing(Deutsches Elektronen-Synchrotron), A. Wilhelm(Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany), D. A. Williams(Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA), B. Zitzer(Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA), External collaborators(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), (INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), M. Villata(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), C. Raiteri(INAF, Osservatorio Astronomico di Torino, I-10025 Pino Torinese), H. D. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), M. F. Aller(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA), W. P. Chen(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), B. Jordan(School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin, 2, Ireland), E. Koptelova(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), O. M. Kurtanidze(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), A. Lähteenmäki(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), B. McBreen(University College Dublin, Belfield, Dublin 4, Ireland), V. M. Larionov(Isaac Newton Institute of Chile, St. Petersburg Branch, St. Petersburg, Russia), C. S. Lin(Graduate Institute of Astronomy, National Central University, Jhongli 32054, Taiwan), M. G. Nikolashvili(Abastumani Observatory, Mt. Kanobili, 0301 Abastumani, Georgia), E. Angelakis(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), M. Capalbi(ASI-Science Data Center, Via del Politecnico, I-00133 Rome, Italy), A. Carrami\ nana(Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, Mexico), L. Carrasco(Instituto Nacional de Astrofísica, Óptica y Electrónica, Tonantzintla, Puebla 72840, Mexico), P. Cassaro(INAF Istituto di Radioastronomia, Sezione di Noto, Contrada Renna Bassa, 96017 Noto), A. Cesarini(Department of Physics, University of Trento, I38050, Povo, Trento, Italy), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), M. Giroletti(INAF Istituto di Radioastronomia, 40129 Bologna, Italy), T. Hovatta(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), T. P. Krichbaum(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), H. A. Krimm(Astro Space Center of the Lebedev Physical Institute, 117997 Moscow, Russia), W. Max-Moerbeck(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), J. W. Moody(Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA), G. Maccaferri(INAF Istituto di Radioastronomia, Stazione Radioastronomica di Medicina, I-40059 Medicina), Y. Mori(Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan), I. Nestoras(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), A. Orlati(INAF Istituto di Radioastronomia, Stazione Radioastronomica di Medicina, I-40059 Medicina), C. Pace(Indiana University, Department of Astronomy, Swain Hall West 319, Bloomington, IN 47405-7105, USA), R. Pearson(Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA), M. Perri(INAF National Institute for Astrophysics, I-00136 Rome, Italy), A. C. S. Readhead(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125), J. L. Richards(Department of Physics, Purdue University, 525 Northwestern Ave, West Lafayette, IN 47907), A. C. Sadun(Department of Physics, University of Colorado, Denver, CO 80220, USA), T. Sakamoto(Department of Physics and Mathematics, College of Science and 952 Engineering, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuoku, Sagamihara-shi Kanagawa 252-5258, Japan), J. Tammi(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), M. Tornikoski(Aalto University Metsähovi Radio Observatory Metsähovintie 114 FIN-02540 Kylmälä Finland), Y. Yatsu(Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan), A. Zook(Department of Physics and Astronomy, Pomona College, Claremont CA 91711-6312, USA), Aleksić, J, Ansoldi, Stefano, Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Berger, K., Bernardini, E., Biland, A., Blanch, O., Bock, R. K., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Carreto Fidalgo, D., 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., Delgado Mendez, C., Doert, M., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher, D., Elsaesser, D., Farina, E., Ferenc, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giavitto, G., Godinović, N., González Muñoz, A., Gozzini, S. R., Hadamek, A., Hadasch, D., Herrero, A., Hildebrand, D., Hose, J., Hrupec, D., Idec, W., Kadenius, V., Kellermann, H., Knoetig, M. L., Krause, J., Kushida, J., La Barbera, A., Lelas, D., Lewandowska, N., Lindfors, E., Longo, Francesco, Lombardi, S., López, M., López Coto, R., López Oramas, A., Lorenz, E., Lozano, I., Makariev, M., Mallot, K., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Meucci, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Munar Adrover, P., Nakajima, D., Niedzwiecki, A., Nilsson, K., Nowak, N., Orito, R., Overkemping, A., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Partini, S., Persic, M., Prada, F., Prada Moroni, P. G., Prandini, E., Preziuso, S., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguezgarcia, J., Rügamer, S., Saggion, A., Saito, K., Salvati, M., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schweizer, T., Shore, S. N., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Spanier, F., Stamatescu, V., Stamerra, A., Steinbring, T., Storz, J., Sun, S., Surić, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Tibolla, O., Torres, D. F., Toyama, T., Treves, A., Uellenbeck, M., Vogler, P., Wagner, R. M., Zandanel, F., Zanin, R., Archambault, S., Behera, B., Beilicke, M., Benbow, W., Bird, R., Buckley, J. H., Bugaev, V., Cerruti, M., Chen, X., Ciupik, L., Collins Hughes, E., Cui, W., Dumm, J., Eisch, J. D., Falcone, A., Federici, S., Feng, Q., Finley, J. P., Fleischhack, H., Fortin, P., Fortson, L., Furniss, A., Griffin, S., Griffiths, S. T., Grube, J., Gyuk, G., Hanna, D., Holder, J., Hughes, G., Humensky, T. B., Johnson, C. A., Kaaret, P., Kertzman, M., Khassen, Y., Kieda, D., Krawczynski, H., Krennrich, F., Kumar, S., Lang, M. J., Maier, G., Mcarthur, S., Meagher, K., Moriarty, P., Mukherjee, R., Ong, R. A., Otte, A. N., Park, N., Pichel, A., Pohl, M., Popkow, A., Prokoph, H., Quinn, J., Ragan, K., Rajotte, J., Reynolds, P. T., Richards, G. T., Roache, E., Rovero, A. C., Sembroski, G. H., Shahinyan, K., Staszak, D., Telezhinsky, I., Theiling, M., Tucci, J. V., Tyler, J., Varlotta, A., Wakely, S. P., Weekes, T. C., Weinstein, A., Welsing, R., Wilhelm, A., Williams, D. A., Zitzer, B., Villata, M., Raiteri, C., Aller, H. D., Aller, M. F., Chen, W. P., Jordan, B., Koptelova, E., Kurtanidze, O. M., Lähteenmäki, A., Mcbreen, B., Larionov, V. M., Lin, C. S., Nikolashvili, M. G., Angelakis, E., Capalbi, M., Carramiñana, A., Carrasco, L., Cassaro, P., Cesarini, A., Fuhrmann, L., Giroletti, M., Hovatta, T., Krichbaum, T. P., Krimm, H. A., Max Moerbeck, W., Moody, J. W., Maccaferri, G., Mori, Y., Nestoras, I., Orlati, A., Pace, C., Pearson, R., Perri, M., Readhead, A. C. S., Richards, J. L., Sadun, A. C., Sakamoto, T., Tammi, J., Tornikoski, M., Yatsu, Y., Zook, A., Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, and Universitat de Barcelona

Subjects
Astrofísica, Brightness, Ciencias Físicas, blazars, Astrophysics, telescope, x-ray variability, 01 natural sciences, Spectral line, BL Lacertae objects, individual, Mrk 421, purl.org/becyt/ford/1 [https], Raigs gamma, emission, MAGIC (telescope), 010303 astronomy & astrophysics, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), individual: Mrk 421 [BL Lacertae objects], Galaxies: BL Lacertae objects: individual: Markarian 421, Spectral energy distribution, Electrónica, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, power spectra, BL Lacertae object, tev photons, 0103 physical sciences, Nucli galàctic actiu, bl lacertae objects: individual: mrk 421, Blazar, Astronomy and Astrophysics, Space and Planetary Science, Active galactic nuclei, 010308 nuclear & particles physics, light curves, Gamma rays, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], Light curve, Galaxies, Galàxies, Astronomía, Crab Nebula, optical variability, active galactic nuclei, Galàxies actives, Active galaxies, markarian-421, ddc:520
Abstract

We performed a 4.5-month multi-instrument campaign (from radio to VHE gamma rays) on Mrk421 between January 2009 and June 2009, which included VLBA, F-GAMMA, GASP-WEBT, Swift, RXTE, Fermi-LAT, MAGIC, and Whipple, among other instruments and collaborations. Mrk421 was found in its typical (non-flaring) activity state, with a VHE flux of about half that of the Crab Nebula, yet the light curves show significant variability at all wavelengths, the highest variability being in the X-rays. We determined the power spectral densities (PSD) at most wavelengths and found that all PSDs can be described by power-laws without a break, and with indices consistent with pink/red-noise behavior. We observed a harder-when-brighter behavior in the X-ray spectra and measured a positive correlation between VHE and X-ray fluxes with zero time lag. Such characteristics have been reported many times during flaring activity, but here they are reported for the first time in the non-flaring state. We also observed an overall anti-correlation between optical/UV and X-rays extending over the duration of the campaign. The harder-when-brighter behavior in the X-ray spectra and the measured positive X-ray/VHE correlation during the 2009 multi-wavelength campaign suggests that the physical processes dominating the emission during non-flaring states have similarities with those occurring during flaring activity. In particular, this observation supports leptonic scenarios as being responsible for the emission of Mrk421 during non-flaring activity. Such a temporally extended X-ray/VHE correlation is not driven by any single flaring event, and hence is difficult to explain within the standard hadronic scenarios. The highest variability is observed in the X-ray band, which, within the one-zone synchrotron self-Compton scenario, indicates that the electron energy distribution is most variable at the highest energies., Comment: Accepted for publication in A&A, 18 pages, 14 figures (v2 has a small modification in the acknowledgments, and also corrects a typo in the field "author" in the metadata)

Published
2015
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25. The most powerful flaring activity from the NLSy1 PMN J0948+0022

Author

V. Bugaev, D. Staszak, J. P. Finley, Daniel Nieto, K. Ragan, T. B. Humensky, Josefin Larsson, Reshmi Mukherjee, K. Meagher, Talvikki Hovatta, G. H. Sembroski, L. Ciupik, P. Fortin, Abraham D. Falcone, J. V. Tucci, Gernot Maier, B. Zitzer, Ralph Bird, J. Tyler, Wystan Benbow, J. Grube, Manel Errando, S. Kumar, R. A. Ong, C. M. Raiteri, S. P. Wakely, S. T. Griffiths, Filippo D'Ammando, J. D. Eisch, K. Berger, Julien Rousselle, Hugh Dickinson, A. Weinstein, M. J. Lang, P. Kar, David A. Williams, John L. Quinn, N. Håkansson, Henrike Fleischhack, A. Varlotta, A. N. Otte, A. O'Faolain de Bhroithe, A. W. Smith, A. McCann, A. Popkow, Geza Gyuk, I. Telezhinsky, G. H. Gillanders, Gordon T. Richards, E. Roache, Jamie Holder, F. Krennrich, Marcos Santander, Matteo Cerruti, Walter Max-Moerbeck, Anthony C. S. Readhead, H. Prokoph, J. S. Perkins, David Kieda, J. V. Cardenzana, M. Pohl, Amy Furniss, L. Gérard, P. Moriarty, Matthias Beilicke, Lucy Fortson, M. Kertzman, J. L. Richards, Xuhui Chen, Y. Khassen, Vladimir Vassiliev, M. Orienti, E. Pueschel, P. T. Reynolds, Justin D. Finke, R. Welsing, Aalto-yliopisto, Aalto University, D'Ammando, F., Orienti, M., Finke, J., Raiteri, C. M., Hovatta, T., Larsson, J., Max-Moerbeck, W., Perkins, J., Readhead, A. C. S., Richards, J. L., Beilicke, M., Benbow, W., Berger, K., Bird, R., Bugaev, V., Cardenzana, J. V., Cerruti, M., Chen, X., Ciupik, L., Dickinson, H. J., Eisch, J. D., Errando, M., Falcone, A., Finley, J. P., Fleischhack, H., Fortin, P., Fortson, L., Furniss, A., Gerard, L., Gillanders, G. H., Griffiths, S. T., Grube, J., Gyuk, G., Håkansson, N., Holder, J., Humensky, T. B., Kar, P., Kertzman, M., Khassen, Y., Kieda, D., Krennrich, F., Kumar, S., Lang, M. J., Maier, G., Mccann, A., Meagher, K., Moriarty, P., Mukherjee, R., Nieto, D., de Bhróithe, A. O'Faoláin, Ong, R. A., Otte, A. N., Pohl, M., Popkow, A., Prokoph, H., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Richards, G. T., Roache, E., Rousselle, J., Santander, M., Sembroski, G. H., Smith, A. W., Staszak, D., Telezhinsky, I., Tucci, J. V., Tyler, J., Varlotta, A., Vassiliev, V. V., Wakely, S. P., Weinstein, A., Welsing, R., Williams, D. A., and Zitzer, B.

Subjects
extragalactic background light, multiwavelength observations, Active galactic nucleus, spectrum radio quasars, individual: PMN J0948+0022 [galaxies], Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, nuclei [galaxies], FOS: Physical sciences, galaxies: active, galaxies: individual: PMN J0948+0022, galaxies: nuclei, galaxies: Seyfert, gamma-rays: general, Owens Valley Radio Observatory, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, galaxies: active-galaxies: individual: pmn j0948+0022, line seyfert 1, Luminosity, law.invention, Telescope, law, Seyfert [galaxies], quasar pks 1510-089, relativistic jets, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, galactic nuclei, ta115, ta213, galaxies: individual: PMN J0948+0022, Astronomy, Astronomy and Astrophysics, gamma-rays: general, gamma-ray emission, galaxies: Seyfert, large-area telescope, x-ray, 13. Climate action, Space and Planetary Science, active [galaxies], ddc:520, Spectral energy distribution, galaxies: nuclei, Astrophysics - High Energy Astrophysical Phenomena, Radio astronomy, Flare, Fermi Gamma-ray Space Telescope, general [gamma-rays]
Abstract

Monthly notices of the Royal Astronomical Society 446(3), 2456 - 2467 (2015). doi:10.1093/mnras/stu2251, We report on multifrequency observations performed during 2012 December–2013 August of the first narrow-line Seyfert 1 galaxy detected in $\gamma$-rays, PMN J0948+0022 (z = 0.5846). A γ-ray flare was observed by the Large Area Telescope on board Fermi during 2012 December–2013 January, reaching a daily peak flux in the 0.1–100 GeV energy range of (155 $\pm$ 31) × $10^{−8}$ ph $cm^{−2} s^{−1}$ on 2013 January 1, corresponding to an apparent isotropic luminosity of $\sim$ 1.5 × $10^{48}$ erg $s^{−1}$. The $\gamma$-ray flaring period triggered Swift and Very Energetic Radiation Imaging Telescope Array System (VERITAS) observations in addition to radio and optical monitoring by Owens Valley Radio Observatory, Monitoring Of Jets in Active galactic nuclei with VLBA Experiments, and Catalina Real-time Transient Survey. A strong flare was observed in optical, UV, and X-rays on 2012 December 30, quasi-simultaneously to the $\gamma$-ray flare, reaching a record flux for this source from optical to $\gamma$-rays. VERITAS observations at very high energy (E > 100 GeV) during 2013 January 6–17 resulted in an upper limit of $F_{>0.2 TeV}$ < 4.0 × $10^{−12} ph cm^{−2} s^{−1}$. We compared the spectral energy distribution (SED) of the flaring state in 2013 January with that of an intermediate state observed in 2011. The two SEDs, modelled as synchrotron emission and an external Compton scattering of seed photons from a dust torus, can be modelled by changing both the electron distribution parameters and the magnetic field., Published by Oxford Univ. Press, Oxford

Published
2015
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26. Discovery of Very-high-energy Emission from RGB J2243+203 and Derivation of Its Redshift Upper Limit

Author

D. Staszak, Daniel Nieto, M. J. Lang, Marcos Santander, Moritz Hütten, M. P. Connolly, Anushka Udara Abeysekara, M. Buchovecky, N. Kelley-Hoskins, Sinéad M. Griffin, David A. Williams, John L. Quinn, P. Moriarty, R. A. Ong, Q. Feng, Ralph Bird, J. Grube, I. Telezhinsky, Wystan Benbow, M. Kertzman, Lucy Fortson, Maria Krause, M. Poh, P. Wilcox, E. Roache, A. Archer, P. T. Reynolds, Gordon T. Richards, A. N. Otte, J. Tyler, J. H. Buckley, F. Krennrich, Jamie Holder, A. Wilhelm, S. McArthur, V. Bugaev, O. Hervet, O. M. Weiner, Henrike Fleischhack, P. Kaaret, David Kieda, V. V. Vassiliev, Abraham D. Falcone, Karlen Shahinyan, A. Weinstein, J. P. Finley, Matteo Cerruti, Amy Furniss, N. H. Park, Gernot Maier, S. P. Wakely, C. A. Johnson, G. H. Gillanders, E. Puesche, B. Zitzer, K. Ragan, S. Kumar, T. B. Humensky, A. Popkow, I. Sadeh, S. Archambault, S. O'Brien, R. Mukherjee, D. S. Hanna, G. H. Sembroski, Robert Brose, C. Rulten, A. Petrashyk, P. Kar, and Wei Cui

Subjects
extragalactic background light, catalog, Photon, Astrophysics::High Energy Astrophysical Phenomena, blazars, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, telescope, 01 natural sciences, Power law, bl lacertae objects, galaxies: individual (rgb j2243+203), 0103 physical sciences, Blazar, Electronic band structure, 010303 astronomy & astrophysics, parameters, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, 010308 nuclear & particles physics, Institut für Physik und Astronomie, Astronomy and Astrophysics, Cherenkov Telescope Array, Redshift, Space and Planetary Science, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract

Very-high-energy (VHE; $>$ 100 GeV) gamma-ray emission from the blazar RGB J2243+203 was discovered with the VERITAS Cherenkov telescope array, during the period between 21 and 24 December 2014. The VERITAS energy spectrum from this source can be fit by a power law with a photon index of $4.6 \pm 0.5$, and a flux normalization at 0.15 TeV of $(6.3 \pm 1.1) \times 10^{-10} ~ \textrm{cm}^{-2} \textrm{s}^{-1} \textrm{TeV}^{-1}$. The integrated \textit{Fermi}-LAT flux from 1 GeV to 100 GeV during the VERITAS detection is $(4.1 \pm 0.8) \times 10^{\textrm{-8}} ~\textrm{cm}^{\textrm{-2}}\textrm{s}^{\textrm{-1}}$, which is an order of magnitude larger than the four-year-averaged flux in the same energy range reported in the 3FGL catalog, ($4.0 \pm 0.1 \times 10^{\textrm{-9}} ~ \textrm{cm}^{\textrm{-2}}\textrm{s}^{\textrm{-1}}$). The detection with VERITAS triggered observations in the X-ray band with the \textit{Swift}-XRT. However, due to scheduling constraints \textit{Swift}-XRT observations were performed 67 hours after the VERITAS detection, not simultaneous with the VERITAS observations. The observed X-ray energy spectrum between 2 keV and 10 keV can be fitted with a power-law with a spectral index of $2.7 \pm 0.2$, and the integrated photon flux in the same energy band is $(3.6 \pm 0.6) \times 10^{-13} ~\textrm{cm}^{-2} \textrm{s}^{-1}$. EBL model-dependent upper limits of the blazar redshift have been derived. Depending on the EBL model used, the upper limit varies in the range from z $

Published
2017
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27. Unprecedented study of the broadband emission of Mrk 421 during flaring activity in March 2010

Author

E. Pueschel, J. Hose, Svetlana G. Jorstad, M. F. Aller, David A. Williams, G. H. Sembroski, D. Nakajima, M. Strzys, R. Welsing, A. Archer, E. Colombo, B. Biasuzzi, F. Borracci, Stefano Ansoldi, Riccardo Paoletti, I. Telezhinsky, Jamie Holder, D. Elsaesser, D. Staszak, Dario Hrupec, L. Ciupik, L. C. Reyes, G. Bonnoli, K. Ragan, M. A. Lopez, N. Galante, Hajime Takami, J. M. Paredes, P. T. Reynolds, Natalia Lewandowska, Hugh D. Aller, L. O. Takalo, G. H. Gillanders, T. Schweizer, Mosè Mariotti, Wystan Benbow, A.-K. Overkemping, D. Hadasch, Victor Stamatescu, J. Biteau, Paul S. Smith, Gordon T. Richards, Wei Cui, A. La Barbera, Sinéad M. Griffin, E. Roache, A. López-Oramas, S. Rügamer, Juan Abel Barrio, J. A. Ros, O. M. Kurtanidze, Alessandro Carosi, Ruben Lopez-Coto, X. Paredes-Fortuny, Mark Gurwell, U. Menzel, Saverio Lombardi, Calvin A. Johnson, P. Kar, M. Villata, K. Mallot, R. J. García López, Felix Spanier, M. Kertzman, A. C. S. Readhead, E. Prandini, D. Galindo, Merja Tornikoski, Yusuke Konno, Diego F. Torres, M. G. Nikolashvili, D. Eisenacher, Antonio Stamerra, K. Kodani, Givi N. Kimeridze, Julian Sitarek, Lorand A. Sigua, K. Nishijima, J. V. Tucci, A. Cesarini, M. Perri, P. Kaaret, J. Storz, D. Dominis Prester, Martin Pohl, C. M. Raiteri, Markus Garczarczyk, C. Fruck, A. Sillanpää, N. Håkansson, M. Makariev, T. Toyama, L. Maraschi, A. Pichel, Jose Miguel Miranda, Matteo Cerruti, Konstancja Satalecka, J. Becerra González, P. Antoranz, Amy Furniss, S. P. Wakely, B. Jordan, Elena G. Larionova, Xuhui Chen, H. C. Lin, Geza Gyuk, Louis Antonelli, Michele Doro, Abelardo Moralejo, Jelena Aleksić, S. McArthur, M. L. Knoetig, P. G. Prada Moroni, P. Munar-Adrover, Ivica Puljak, E. Collins-Hughes, K. Meagher, Nikola Godinovic, Benito Marcote, T. Steinbring, W. Idec, M. V. Fonseca, Pierre Colin, P. Temnikov, M. Hayashida, Patrick Vogler, J. Tyler, A. Niedzwiecki, C. Schultz, V. Scapin, J. H. Buckley, P. Moriarty, Tomislav Terzić, K. Berger, T. Sakamoto, C. Delgado Mendez, S. R. Gozzini, B. McBreen, O. Tibolla, Shan Sun, E. de Oña Wilhelmi, Ivan S. Troitsky, David Paneque, I. Snidaric, Marc Ribó, P. Da Vela, D. Hildebrand, B. Steinke, Steven N. Shore, Q. Feng, K. Frantzen, Massimo Persic, Hidetoshi Kubo, A. Boller, D. A. Morozova, A. Wilhelm, R. Reinthal, Thomas Bretz, Sofia O. Kurtanidze, Kari Nilsson, Elina Lindfors, Justin D. Finke, J. Krause, B. De Lotto, Walter Max-Moerbeck, K. Saito, Razmik Mirzoyan, U. Barres de Almeida, A. González Muñoz, V. Kadenius, Damir Lelas, N. Mankuzhiyil, J. P. Finley, J. S. Perkins, Wen Ping Chen, S. Paiano, E. Lorenz, Karl Mannheim, H. Prokoph, Hanna Kellermann, Daniel Mazin, I. Lozano, Dorota Sobczyńska, J. D. Eisch, Wolfgang Rhode, Daniela Dorner, M. Palatiello, Joseph Moody, Lucy Fortson, M. I. Martínez, M. Gaug, P. Bangale, G. De Caneva, J. Herrera, Matthias Beilicke, Koji Noda, J. Millis, Abraham D. Falcone, Francesco Dazzi, Karlen Shahinyan, Elisa Bernardini, S. Bonnefoy, Sabrina Einecke, J. Rodriguez Garcia, W. Bednarek, Fabrizio Tavecchio, Ll. Font, A. C. Sadun, Anne Lähteenmäki, Stefano Covino, M. J. Lang, A. Varlotta, Masahiro Teshima, A. McCann, Ekaterina Koptelova, A. C. Rovero, J. Kushida, D. Tescaro, Jose Luis Contreras, G. Hughes, M. Uellenbeck, Takashi Saito, Y. Hanabata, A. Popkow, Juan Cortina, V. Bugaev, David Kieda, Reiko Orito, S. Buson, J. L. Richards, Ann E. Wehrle, D. Garrido Terrats, P. Fortin, Oscar Blanch, Ralph Bird, S. Archambault, Valeri M. Larionov, V. Scalzotto, Ana Babić, Julia Thaele, E. Carmona, A. De Angelis, A. Treves, R. A. Ong, G. Maneva, R. Zanin, A. N. Otte, Adrian Biland, J. Rico, Alan P. Marscher, Universitat de Barcelona, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, and ~

Subjects
extragalactic background light, Ciencias Físicas, spectral energy-distribution, Flux, Non-thermal / galaxies, Astrophysics, law.invention, Relativistic particle, purl.org/becyt/ford/1 [https], atmospheric cherenkov telescopes, Raigs gamma, bl lacertae objects, law, MAGIC (telescope), Active / BL Lacertae objects, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, individual: Mrk 421 [BL Lacertae objects], education.field_of_study, gamma-ray outburst, non-thermal [radiation mechanisms], BL Lacertae objects: individual: Mrk 421, Galaxies: active, Gamma rays: galaxies, Radiation mechanisms: non-thermal, Astronomy and Astrophysics, Space and Planetary Science, Particle acceleration, NON THERMAL RADIATION, large-area telescope, active [galaxies], galaxies [gamma rays], BL LACERTAE OBJECTS, Electrónica, self-compton model, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Flare, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio telescope, radiation mechanisms: non-thermal, gamma rays: galaxies, Radiation mechanisms, BL Lacertae objects: individual, simultaneous multiwavelength observations, AGN, education, Blazar, Individual: Mrk 421 / gamma rays, tev blazars, Gamma rays, Institut für Physik und Astronomie, purl.org/becyt/ford/1.3 [https], Galaxies, Astronomía, x-ray, Galàxies actives, Active galaxies, ddc:520
Abstract

A flare from the TeV blazar Mrk 421, occurring in March 2010, was observed for 13 consecutive days from radio to very high energy (VHE, E > 100 GeV) gamma-rays with MAGIC, VERITAS, Whipple, FermiLAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We model the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigate the physical parameters, and evaluate whether the observed broadband SED variability can be associated to variations in the relativistic particle population. Flux variability was remarkable in the X-ray and VHE bands while it was minor or not significant in the other bands. The one-zone SSC model can describe reasonably well the SED of each day for the 13 consecutive days. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission while the other smaller zone, which is spatially separated from the first one, contributes to the daily-variable emission occurring in X-rays and VHE gamma-rays. Both the one-zone SSC and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly to the underlying particle population. This shows that the particle acceleration and cooling mechanism producing the radiating particles could be the main one responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement to the observed SED at the narrow peaks of the low- and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by the variation of the parameters related to the emitting region itself ($\delta$, $B$ and $R$), in addition to the parameters related to the particle population., Comment: Published in A&A, 30 pages, 15 figures, 6 tables. Online-data: multi-wavelength light curves (data in Fig. 1) and broadband spectral energy distributions (the data in Figs. 6, and B1-B4) are available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/578/A22. Corresponding authors: David Paneque (dpaneque@mpp.mpg.de), Shangyu Sun (sysun@mpp.mpg.de), Hajime Takami (takami@post.kek.jp)

Published
2014
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28. Reacceleration of electrons in supernova remnants

Author

I. Telezhinsky, Martin Pohl, and A. Wilhelm

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Institut für Physik und Astronomie, Astronomy and Astrophysics, Cosmic ray, Electron, Astrophysics, Spectral line, Computational physics, Momentum diffusion, Supernova, Space and Planetary Science, ddc:520, Convection–diffusion equation, Astrophysics - High Energy Astrophysical Phenomena, Dynamo
Abstract

The radio spectra of many shell-type supernova remnants show deviations from those expected on theoretical grounds. In this paper we determine the effect of stochastic reacceleration on the spectra of electrons in the GeV band and at lower energies, and we investigate whether or not reacceleration can explain the observed variation of radio spectral indices. We explicitely calculate the momentum diffusion coefficient for 3 types of turbulence expected downstream of the forward shock: fast-mode waves, small-scale non-resonant modes, and large-scale modes arising from turbulent dynamo activity. Noting that low-energy particles are efficiently coupled to the quasi-thermal plasma, a simplified cosmic-ray transport equation can be formulated and is numerically solved. Only fast-mode waves can provide momentum diffusion fast enough to significantly modify the spectra of particles. Using a synchrotron emissivity that accurately reflects a highly turbulent magnetic field, we calculate the radio spectral index and find that soft spectra with index $\alpha\lesssim -0.6$ can be maintained over more than 2 decades in radio frequency, even if the electrons experience reacceleration for only one acceleration time. A spectral hardening is possible but considerably more frequency-dependent. The spectral modification imposed by stochastic reacceleration downstream of the forward shock depends only weakly on the initial spectrum provided by, e.g., diffusive shock acceleration at the shock itself., Comment: A&A submitted, version revised as per referee comments

Published
2014
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29. VERITAS Observations of the BL Lac Object PG 1553+113

Author

D. Staszak, K. Ragan, S. McArthur, E. Aliu, A. Varlotta, J. Tyler, I. Telezhinsky, J. H. Buckley, B. Zitzer, Jamie Holder, L. C. Reyes, A. Archer, Matteo Cerruti, Hugh Dickinson, Amy Furniss, L. Ciupik, David A. Williams, D. S. Hanna, J. Grube, Manel Errando, A. N. Otte, Karen Byrum, Martin Pohl, A. O'Faolain de Bhroithe, J. D. Eisch, Geza Gyuk, M. P. Connolly, H. Prokoph, S. Kumar, A. Weinstein, J. Dumm, J. V. Tucci, J. P. Finley, P. Moriarty, G. Hughes, A. McCann, K. Meagher, G. H. Gillanders, Jean-Francois Rajotte, S. P. Wakely, Vladimir Vassiliev, Wystan Benbow, K. Berger, N. Galante, E. Pueschel, T. B. Humensky, David Kieda, Henric Krawczynski, A. S Madhavan, N. Håkansson, Gordon T. Richards, E. Roache, Sinéad M. Griffin, Anna Barnacka, Frank Krennrich, Xuhui Chen, B. Behera, P. Kaaret, J. V. Cardenzana, Daniel Nieto, A. Wilhelm, R. A. Ong, M. Kertzman, A. Popkow, C. A. Johnson, Lucy Fortson, S. T. Griffiths, N. H. Park, J. Millis, Q. Feng, S. Federici, Matthias Beilicke, V. Bugaev, Wei Cui, T. Aune, P. T. Reynolds, G. H. Sembroski, R. Welsing, Matthew R. Orr, J. S. Perkins, Y. Khassen, P. Kar, P. Fortin, Ralph Bird, M. J. Lang, John L. Quinn, Abraham D. Falcone, Karlen Shahinyan, and ~

Subjects
extragalactic background light, spectra, Astrophysics::High Energy Astrophysical Phenomena, blazars, pg-1553+113, FOS: Physical sciences, Flux, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, telescope, 10. No inequality, Blazar, optical spectroscopy, bl lacertae objects: general, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, model, Gamma rays, Institut für Physik und Astronomie, Astronomy and Astrophysics, gamma-rays, Redshift, radiation, Crab Nebula, Pair production, Extragalactic background light, Space and Planetary Science, ddc:520, lacertae objects, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object
Abstract

We present results from VERITAS observations of the BL Lac object PG 1553+113 spanning the years 2010, 2011, and 2012. The time-averaged spectrum, measured between 160 and 560\,GeV, is well described by a power law with a spectral index of $4.33 \pm 0.09$. The time-averaged integral flux above $200\,$GeV measured for this period was $(1.69 \pm 0.06) \times 10^{-11} \, \mathrm{ph} \, \mathrm{cm}^{-2} \, \mathrm{s}^{-1}$, corresponding to 6.9\% of the Crab Nebula flux. We also present the combined $\gamma$-ray spectrum from the Fermi Large Area Telescope and VERITAS covering an energy range from 100~MeV to 560~GeV. The data are well fit by a power law with an exponential cutoff at $\rm {101.9 \pm 3.2 \, \mathrm{GeV}} $. The origin of the cutoff could be intrinsic to PG~1553+113 or be due to the $\gamma$-ray opacity of our universe through pair production off the extragalactic background light (EBL). Given lower limits to the redshift of $\rm z \negthinspace > \negthinspace 0.395$ based on optical/UV observations of PG~1553+113, the cutoff would be dominated by EBL absorption. Conversely, the small statistical uncertainties of the VERITAS energy spectrum have allowed us to provide a robust upper limit on the redshift of PG 1553+113 of $z \negthinspace \leq \negthinspace 0.62$. A strongly-elevated mean flux of $(2.50 \pm 0.14) \times 10^{-11} \, \mathrm{ph} \, \mathrm{cm}^{-2} \, \mathrm{s}^{-1}$ (10.3\% of the Crab Nebula flux) was observed during 2012, with the daily flux reaching as high as $(4.44 \pm 0.71) \times 10^{-11} \, \mathrm{ph} \, \mathrm{cm}^{-2} \, \mathrm{s}^{-1}$ (18.3\% of the Crab Nebula flux) on MJD 56048. The light curve measured during the 2012 observing season is marginally inconsistent with a steady flux, giving a $\chi^2$ probability for a steady flux of 0.03\%., Comment: in press in ApJ, 2014

Published
2014
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30. Constraints on very high energy emission from grb 130427a

Author

P. Kaaret, S. McArthur, Wei Cui, J. Grube, Manel Errando, Q. Feng, H. Prokoph, R. Welsing, A. McCann, Geza Gyuk, J. V. Tucci, P. Fortin, Gernot Maier, Valerie Connaughton, L. Ciupik, O. M. Weiner, G. H. Sembroski, Péter Veres, K. Berger, S. Federici, A. Popkow, H. Fleischhack, J. H. Buckley, S. P. Wakely, Xuhui Chen, H. Krawczynski, I. Telezhinsky, Jamie Holder, M. J. Lang, A. Wilhelm, David Kieda, Anna Barnacka, A. S. Madhavan, K. Ragan, P. Moriarty, J. Tyler, A. Furniss, John L. Quinn, B. Zitzer, Wystan Benbow, G. H. Gillanders, E. Pueschel, Jonathan Biteau, A. Varlotta, N. Galante, Gareth Hughes, Frank Krennrich, Y. Khassen, T. B. Humensky, Julie McEnery, M. Kertzman, Jean-Francois Rajotte, A. W. Smith, Vladimir Vassiliev, A. O'Faolain de Bhroithe, Luis C. Reyes, J. V. Cardenzana, E. Roache, Gordon T. Richards, C. A. Johnson, N. Håkansson, David A. Williams, N. H. Park, Karen Byrum, M. Beilicke, Abraham D. Falcone, Karlen Shahinyan, J. D. Eisch, A. Weinstein, P. Kar, P. T. Reynolds, S. Vincent, Daniel Nieto, J. Millis, R. Mukherjee, Lucy Fortson, D. Staszak, Matteo Cerruti, Sylvia J. Zhu, Martin Pohl, K. Meagher, R. A. Ong, D. S. Hanna, V. Bugaev, S. T. Griffiths, J. S. Perkins, A. N. Otte, E. Aliu, T. Aune, S. Griffin, Hugh Dickinson, and J. P. Finley

Subjects
spectra, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, telescope, law.invention, Telescope, swift, Spitzer Space Telescope, law, component, tev, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, gamma-ray bursts, Gamma ray, GRB 130427A, Institut für Physik und Astronomie, Astronomy and Astrophysics, afterglows, Cherenkov Telescope Array, Redshift, gamma-ray burst: individual (grb 130427a), mission, 13. Climate action, Space and Planetary Science, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, limits, Fermi Gamma-ray Space Telescope
Abstract

Prompt emission from the very fluent and nearby (z=0.34) gamma-ray burst GRB 130427A was detected by several orbiting telescopes and by ground-based, wide-field-of-view optical transient monitors. Apart from the intensity and proximity of this GRB, it is exceptional due to the extremely long-lived high-energy (100 MeV to 100 GeV) gamma-ray emission, which was detected by the Large Area Telescope on the Fermi Gamma-ray Space Telescope for ~70 ks after the initial burst. The persistent, hard-spectrum, high-energy emission suggests that the highest-energy gamma rays may have been produced via synchrotron self-Compton processes though there is also evidence that the high-energy emission may instead be an extension of the synchrotron spectrum. VERITAS, a ground-based imaging atmospheric Cherenkov telescope array, began follow-up observations of GRB 130427A ~71 ks (~20 hr) after the onset of the burst. The GRB was not detected with VERITAS; however, the high elevation of the observations, coupled with the low redshift of the GRB, make VERITAS a very sensitive probe of the emission from GRB 130427A for E > 100 GeV. The non-detection and consequent upper limit derived place constraints on the synchrotron self-Compton model of high-energy gamma-ray emission from this burst., 22 pages, 4 figures, 1 table

Published
2014
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31. Very-high energy observations of the galactic center region by veritas in 2010-2012

Author

W. Chen, J. P. Finley, A. N. Otte, M. P. Connolly, Daniel Nieto, Abraham D. Falcone, Karlen Shahinyan, Matteo Cerruti, Amy Furniss, A. Wilhelm, L. Ciupik, B. Zitzer, M. J. Lang, J. Grube, S. Kumar, Xuhui Chen, Sinéad M. Griffin, J. Tyler, A. O'Faolain de Bhroithe, E. Pueschel, J. H. Buckley, N. H. Park, R. A. Ong, M. Kertzman, John L. Quinn, P. Kaaret, J. V. Cardenzana, P. Moriarty, J. V. Tucci, Gernot Maier, C. A. Johnson, J. Biteau, S. Federici, Reshmi Mukherjee, Karen Byrum, J. D. Eisch, S. P. Wakely, A. Popkow, Ralph Bird, Martin Pohl, A. Weinstein, S. T. Griffiths, S. McArthur, J. Dumm, G. H. Sembroski, Q. Feng, J. S. Perkins, Anna Barnacka, N. Galante, A. Archer, R. Welsing, A. McCann, Wei Cui, Anna Zajczyk, David A. Williams, A. W. Smith, V. Bugaev, Gordon T. Richards, David Kieda, E. Roache, P. Kar, D. Staszak, K. Ragan, K. Meagher, Jean-Francois Rajotte, Matthias Beilicke, Lucy Fortson, K. Berger, Henric Krawczynski, I. Telezhinsky, Jamie Holder, L. C. Reyes, P. T. Reynolds, S. Vincent, Y. Khassen, Hugh Dickinson, D. S. Hanna, A. Varlotta, Wystan Benbow, G. Hughes, N. Håkansson, Henrike Fleischhack, H. Prokoph, and Geza Gyuk

Subjects
Astrophysics::High Energy Astrophysical Phenomena, galaxy: center, Dark matter, black hole physics, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, molecular clouds, gamma-ray source, gamma rays: galaxies, emission, crab-nebula, Supernova remnant, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Astroparticle physics, Physics, Supermassive black hole, variability, Galactic Center, Institut für Physik und Astronomie, Astronomy, Astronomy and Astrophysics, source catalog, radiation mechanisms: non-thermal, Astrophysics - Astrophysics of Galaxies, methods: data analysis, Galaxy, dark-matter, Space and Planetary Science, astroparticle physics, Astrophysics of Galaxies (astro-ph.GA), ddc:520, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, sgr-a-asterisk, magic telescope, discovery, Fermi Gamma-ray Space Telescope
Abstract

The Galactic center is an interesting region for high-energy (0.1-100 GeV) and very-high-energy (E > 100 GeV) gamma-ray observations. Potential sources of GeV/TeV gamma-ray emission have been suggested, e.g., the accretion of matter onto the supermassive black hole, cosmic rays from a nearby supernova remnant (e.g. SgrA East), particle acceleration in a plerion, or the annihilation of dark matter particles. The Galactic center has been detected by EGRET and by Fermi/LAT in the MeV/GeV energy band. At TeV energies, the Galactic center was detected with moderate significance by the CANGAROO and Whipple 10 m telescopes and with high significance by H.E.S.S., MAGIC, and VERITAS. We present the results from three years of VERITAS observations conducted at large zenith angles resulting in a detection of the Galactic center on the level of 18 standard deviations at energies above ~2.5TeV. The energy spectrum is derived and is found to be compatible with hadronic, leptonic and hybrid emission models discussed in the literature. Future, more detailed measurements of the high-energy cutoff and better constraints on the high-energy flux variability will help to refine and/or disentangle the individual models., 15 pages, 7 figures, accepted for publication in ApJ

Published
2014
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32. Spatially Resolving the very high Energy Emission from MGRO J2019+37 with VERITAS

Author

I. Telezhinsky, Jamie Holder, S. Vincent, A. Popkow, L. C. Reyes, A. Bouvier, Abraham D. Falcone, Eric V. Gotthelf, Karlen Shahinyan, Sinéad M. Griffin, P. Fortin, P. Kaaret, Jean-Francois Rajotte, Ralph Bird, T. Aune, B. Behera, Daniel Nieto, J. P. Finley, Martin Pohl, C. A. Johnson, M. Kertzman, D. Staszak, D. S. Hanna, T. B. Humensky, J. Dumm, Wystan Benbow, K. Ragan, A. O'Faolain de Bhroithe, L. Ciupik, F. Krennrich, John L. Quinn, V. Bugaev, E. Aliu, R. A. Ong, Matthias Beilicke, B. Zitzer, Oleg Kargaltsev, J. V. Tucci, S. T. Griffiths, Mallory S. E. Roberts, Gernot Maier, K. Berger, J. Grube, Manel Errando, A. McCann, Q. Feng, N. Galante, Y. Khassen, H. Prokoph, Amanda Weinstein, S. McArthur, Xuhui Chen, A. N. Otte, S. P. Wakely, M. P. Connolly, Dirk Pandel, A. W. Smith, S. Federici, A. S Madhavan, David Kieda, Henrike Fleischhack, Gordon T. Richards, E. Roache, G. H. Gillanders, Reshmi Mukherjee, G. Hughes, M. J. Lang, A. Wilhelm, Matteo Cerruti, Amy Furniss, David A. Williams, Wei Cui, P. T. Reynolds, Geza Gyuk, Vikram V. Dwarkadas, J. Tyler, Lucy Fortson, P. Moriarty, N. H. Park, J. Millis, J. H. Buckley, G. H. Sembroski, and R. Welsing

Subjects
stars, Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, supernovae : individual (ctb 87), galactic plane, 01 natural sciences, Spectral line, Pulsar, pulsars : individual (psr j2021+3651), Observatory, 0103 physical sciences, pulsar wind nebula, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, cygnus region, hess, 010308 nuclear & particles physics, Star formation, Institut für Physik und Astronomie, Astronomy, Astronomy and Astrophysics, gamma-ray emission, gamma rays : stars, psr j2021+3651, milagro, Supernova, 13. Climate action, Space and Planetary Science, Milagro, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, discovery, associations
Abstract

We present very high energy (VHE) imaging of MGRO J2019+37 obtained with the VERITAS observatory. The bright extended ($\sim2^{\circ}$) unidentified Milagro source is located towards the rich star formation region Cygnus-X. MGRO J2019+37 is resolved into two VERITAS sources. The faint point-like source VER J2016+371 overlaps CTB 87, a filled-center remnant (SNR) with no evidence of a supernova remnant shell at the present time. Its spectrum is well fit in the $0.65 - 10$ TeV energy range by a power-law model with photon index $2.3\pm0.4$. VER J2019+368 is a bright extended ($\sim1^{\circ}$) source, that likely accounts for the bulk of the Milagro emission and is notably coincident with PSR J2021+3651 and the star formation region Sh 2-104. Its spectrum in the range $1-30$ TeV is well fit with a power-law model of photon index $1.75\pm0.3$, among the hardest values measured in the VHE band, comparable to that observed near Vela-X. We explore the unusual spectrum and morphology in the radio and X-ray bands to constrain possible emission mechanisms for this source., 9 pages, 8 figures, accepted for publication in the Astrophysical Journal

Published
2014
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33. Investigating the TeV morpholoy of MGRO J1908+06 with veritas

Author

P. Kaaret, J. Grube, S. Archambault, M. P. Connolly, Manel Errando, J. V. Cardenzana, J. E. Ward, Wei Cui, K. Berger, John L. Quinn, M. Kertzman, J. V. Tucci, P. Fortin, A. Varlotta, Gernot Maier, E. Collins-Hughes, Frank Krennrich, A. O'Faolain de Bhroithe, S. Vincent, G. H. Sembroski, M. Beilicke, H. Prokoph, R. Mukherjee, N. Galante, S. P. Wakely, M. J. Lang, R. Welsing, D. Gall, G. Ratliff, A. Wilhelm, Q. Feng, Gareth Hughes, Martin Pohl, H. Fleischhack, R. A. Ong, Xuhui Chen, A. W. Smith, Y. Khassen, S. Federici, David Kieda, Dirk Pandel, J. Dumm, J. H. Buckley, Gordon T. Richards, T. B. Humensky, K. Meagher, S. T. Griffiths, Vikram V. Dwarkadas, K. Ragan, E. Roache, D. S. Hanna, B. Behera, Luis C. Reyes, A. Furniss, Daniel Nieto, D. Staszak, Abraham D. Falcone, Karlen Shahinyan, N. H. Park, P. T. Reynolds, Jean-Francois Rajotte, V. Bugaev, Lucy Fortson, J. P. Finley, Sunil Kumar, A. Popkow, F. Sheidaei, J. Millis, J. Tyler, A. Weinstein, P. Moriarty, S. Griffin, E. Aliu, Ralph Bird, I. Telezhinsky, Jamie Holder, A. S. Madhavan, Wystan Benbow, A. N. Otte, Geza Gyuk, Julien Rousselle, L. Ciupik, K. Tsurusaki, G. H. Gillanders, Vladimir Vassiliev, Matteo Cerruti, T. Aune, and A. McCann

Subjects
High energy, Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, g40.5-0.5, Astrophysics, array, 01 natural sciences, Pulsar wind nebula, galactic plane, remnant, Pulsar, pulsars: individual (psr j1907+0602), Observatory, 0103 physical sciences, pulsar wind nebula, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, gamma-ray burst: individual (mgro j1908+06, ver j1907+062), 010308 nuclear & particles physics, Sigma, Institut für Physik und Astronomie, Astronomy and Astrophysics, gamma rays: general, gamma-ray emission, milagro, psr j1907+0602, 13. Climate action, Space and Planetary Science, ism: supernova remnants, ddc:520, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report on deep observations of the extended TeV gamma-ray source MGRO J1908+06 made with the VERITAS very high energy (VHE) gamma-ray observatory. Previously, the TeV emission has been attributed to the pulsar wind nebula (PWN) of the Fermi-LAT pulsar PSR J1907+0602. We detect MGRO J1908+06 at a significance level of 14 standard deviations (14 sigma) and measure a photon index of 2.20 +/- 0.10_stat +/- 0.20_sys. The TeV emission is extended, covering the region near PSR J1907+0602 and also extending towards SNR G40.5--0.5. When fitted with a 2-dimensional Gaussian, the intrinsic extension has a standard deviation of sigma_src = 0.44 +/- 0.02 degrees. In contrast to other TeV PWNe of similar age in which the TeV spectrum softens with distance from the pulsar, the TeV spectrum measured near the pulsar location is consistent with that measured at a position near the rim of G40.5--0.5, 0.33 degrees away., To appear in ApJ, 8 pages

Published
2014
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34. Test of Models of the Cosmic Infrared Background with Multiwavelength Observations of the Blazar 1ES 1218+30.4 in 2009

Author

Wystan Benbow, Daniel Nieto, A. N. Otte, M. P. Connolly, A. Bouvier, L. Ciupik, R. Dickherber, Geza Gyuk, T. Aune, P. T. Reynolds, P. Moriarty, S. McArthur, Ralph Bird, S. Federici, J. P. Finley, J. H. Buckley, Sinéad M. Griffin, Matthias Beilicke, P. Majumdar, Lucy Fortson, N. Galante, M. J. Lang, R. A. Ong, A. Varlotta, M. Kertzman, A. S Madhavan, Markus Böttcher, A. Lamerato, Q. Feng, John L. Quinn, Gordon T. Richards, E. Roache, G. D. Şentürk, Gernot Maier, D. S. Hanna, T. C. Arlen, Wei Cui, C. Gusbar, P. Roustazadeh, G. Hughes, Vladimir Vassiliev, H. Prokoph, S. P. Wakely, R. Welsing, Matthew R. Orr, V. Bugaev, C. Skole, G. H. Gillanders, Daniel Gall, P. Kaaret, Y. Khassen, E. Collins-Hughes, A. Iii. Garson, G. Tešić, Amy Furniss, Henric Krawczynski, S. Vincent, D. B. Saxon, N. H. Park, J. Millis, K. Li, J. S. Perkins, Martin Pohl, J. Dumm, G. H. Sembroski, S. Archambault, Reshmi Mukherjee, A. Weinstein, A. D. Falcone, A. McCann, A. O'Faolain de Bhroithe, David Kieda, M. Theiling, I. Telezhinsky, Jamie Holder, David A. Williams, D. Staszak, K. Ragan, B. Zitzer, J. Grube, Manel Errando, and A. Popkow

Subjects
Smithsonian institution, Astrophysics::High Energy Astrophysical Phenomena, Cosmic background radiation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, timing explorer, Cosmic infrared background, gamma rays: galaxies, strong flares, Blazar, bl lacertae objects: general, Diffuse radiation, Physics, gamma-ray observations, bl lacertae objects: individual (1es1218+30.4), particle-acceleration, tev blazars, Astronomy, Institut für Physik und Astronomie, Astronomy and Astrophysics, Visible radiation, galaxies: jets, veritas observations, diffuse radiation, Red shift, large-area telescope, x-ray, Space and Planetary Science, active galactic nuclei, extragalactic magnetic-fields, ddc:520
Abstract

We present the results of a multi-wavelength campaign targeting the blazar 1ES 1218+30.4 with observations with the 1.3 m McGraw-Hill optical telescope, the Rossi X-ray Timing Explorer (RXTE), the Fermi Gamma-Ray Space Telescope, and the Very Energetic Radiation Imaging Telescope Array System (VERITAS). The RXTE and VERITAS observations were spread over a 13 day period and revealed clear evidence for flux variability, and a strong X-ray and gamma-ray flare on 2009 February 26 (MJD 54888). The campaign delivered a well-sampled broadband energy spectrum with simultaneous RXTE and VERITAS very high energy (VHE, > 100 GeV) observations, as well as contemporaneous optical and Fermi observations. The 1ES 1218+30.4 broadband energy spectrum-the first with simultaneous X-ray and VHE gamma-ray energy spectra-is of particular interest as the source is located at a high cosmological redshift for a VHE source (z = 0.182), leading to strong absorption of VHE gamma rays by photons from the optical/infrared extragalactic background light (EBL) via gamma VHE +gamma EBL -> e(+) e(-)pair-creation processes. We model the data with a one-zone synchrotron self-Compton (SSC) emission model and with the extragalactic absorption predicted by several recent EBL models. We find that the observations are consistent with the SSC scenario and all the EBL models considered in this work. We discuss observational and theoretical avenues to improve on the EBL constraints.

Published
2014
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35. Observation of Markarian 421 in TeV gamma rays over a 14-year time span

Author

M. J. Lang, J. Tyler, J. H. Buckley, D. A. Carter-Lewis, E. Collins-Hughes, G. H. Gillanders, S. P. Wakely, Daniel Gall, L. Ciupik, N. Galante, E. Roache, A. N. Otte, H. Krawczynski, T. Reynolds, M. P. Connolly, D. S. Hanna, Ralph Bird, G. Finnegan, Geza Gyuk, K. Ragan, A. W. Smith, C. Duke, A. Pichel, G. H. Sembroski, Lucy Fortson, R. Welsing, Abraham D. Falcone, T. C. Arlen, V. Bugaev, Matthew R. Orr, J. P. Finley, Wei Cui, Y. Khassen, V. A. Acciari, T. Aune, T. C. Weekes, S. M. Bradbury, John Toner, A. C. Rovero, A. Cesarini, A. S. Madhavan, Wystan Benbow, Martin Pohl, John L. Quinn, P. Moriarty, R. A. Ong, K. G. Gibbs, J. Dumm, J. S. Perkins, S. J. Fegan, S. Federici, A. Weinstein, Stephanie Wissel, M. Schroedter, I. de la Calle Perez, A. Varlotta, A. Bouvier, P. Kaaret, J. E. Ward, David Kieda, M. Theiling, Sinéad M. Griffin, M. Kertzman, A. O'Faolain de Bhroithe, D. J. Fegan, T. J. N. Nelson, J. A. Gaidos, David A. Williams, I. Telezhinsky, T. B. Humensky, Julie McEnery, D. Horan, D. Petry, J. Grube, M. Vivier, and F. Krennrich

Subjects
multiwavelength observations, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, telescope, timing explorer, 01 natural sciences, Spectral line, law.invention, purl.org/becyt/ford/1 [https], Telescope, law, blazar markarian-421, emission, 0103 physical sciences, crab-nebula, flare, AGN, Blazar, tev gamma rays, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Markarian 421, 010308 nuclear & particles physics, markarian 421, Gamma ray, Astronomy, Institut für Physik und Astronomie, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], TeV gamma rays, Astronomía, Crab Nebula, correlated variability, active galactic nuclei, ddc:540, agn, Astrophysics - High Energy Astrophysical Phenomena, Markarian galaxies, CIENCIAS NATURALES Y EXACTAS, energy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The variability of the blazar Markarian 421 in TeV gamma rays over a 14-year time period has been explored with the Whipple 10 m telescope. It is shown that the dynamic range of its flux variations is large and similar to that in X-rays. A correlation between the X-ray and TeV energy bands is observed during some bright flares and when the complete data sets are binned on long timescales. The main database consists of 878.4 hours of observation with the Whipple telescope, spread over 783 nights. The peak energy response of the telescope was 400 GeV with 20% uncertainty. This is the largest database of any TeV-emitting active galactic nucleus (AGN) and hence was used to explore the variability profile of Markarian 421. The time-averaged flux from Markarian 421 over this period was 0.446$\pm$0.008 Crab flux units. The flux exceeded 10 Crab flux units on three separate occasions. For the 2000-2001 season the average flux reached 1.86 Crab units, while in the 1996-1997 season the average flux was only 0.23 Crab units., Comment: 29 pages, 15 figures. Accepted for publication in Astroparticle Physics

Published
2014
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36. A Three-Year Multi-Wavelength Study of the Very-High-Energy $\gamma$-Ray Blazar 1ES 0229+200

Author

F. Krennrich, A. McCann, A. Popkow, E. Aliu, M. Theiling, T. Aune, B. Zitzer, J. S. Perkins, J. H. Buckley, Wystan Benbow, V. V. Vassiliev, Manel Errando, A. O'Faolain de Bhroithe, A. Varlotta, K. Meagher, D. B. Kieda, P. Fortin, A. N. Otte, Anna Zajczyk, J. P. Dumm, Henrike Fleischhack, M. P. Connolly, John L. Quinn, Matthias Beilicke, S. Federici, Ralph Bird, P. Moriarty, Nicola Galante, J. Grube, I. Telezhinsky, Gernot Maier, J. P. Finley, B. Behera, Daniel Nieto, L. Ciupik, T. C. Weekes, Jamie Holder, Nahee Park, Xuhui Chen, K. L. Byrum, H. Prokoph, R. A. Ong, Y. Khassen, L. C. Reyes, S. McArthur, S. T. Griffiths, S. Archambault, Reshmi Mukherjee, J. Millis, S. P. Wakely, Wei Cui, V. Bugaev, D. Staszak, K. Ragan, A. W. Smith, D. S. Hanna, A. S Madhavan, C. Duke, Gordon T. Richards, T. C. Arlen, E. Roache, P. Kaaret, P. T. Reynolds, David A. Williams, R. Welsing, C. A. Johnson, Lucy Fortson, S. Vincent, Henric Krawczynski, A. J.R. Weinstein, M. J. Lang, Martin Pohl, G. H. Sembroski, A. D. Falcone, Q. Feng, T. B. Humensky, K. Berger, Matteo Cerruti, Amy Furniss, Sinéad M. Griffin, Gareth Hughes, M. Kertzman, A. Bouvier, Geza Gyuk, Pratik Majumdar, and G. H. Gillanders

Subjects
extragalactic background light, bl lacertae objects: individual (1es 0229+200, ver j0232+202), Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, magnetic fields, 01 natural sciences, bl lacertae objects, 0103 physical sciences, intergalactic magnetic-field, Blazar, 010303 astronomy & astrophysics, bl lacertae objects: general, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, space-telescope, distant blazars, tev blazars, 010308 nuclear & particles physics, Institut für Physik und Astronomie, Astronomy and Astrophysics, gamma rays: general, diffuse radiation, large-area telescope, Crab Nebula, x-ray, Extragalactic background light, Space and Planetary Science, active galactic nuclei, Spectral energy distribution, Intergalactic travel, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, lorentz factor, Fermi Gamma-ray Space Telescope, BL Lac object
Abstract

The high-frequency-peaked BL Lacertae object 1ES 0229+200 is a relatively distant (z = 0.1396), hard-spectrum (Gamma ~ 2.5), very-high-energy-emitting (E > 100 GeV) gamma-ray blazar. Very-high-energy measurements of this active galactic nucleus have been used to place constraints on the intensity of the extragalactic background light and the intergalactic magnetic field. A multi-wavelength study of this object centered around very-high-energy observations by VERITAS is presented. This study obtained, over a period of three years, an 11.7 standard deviation detection and an average integral flux F(E>300 GeV) = (23.3 +- 2.8_stat +- 5.8_sys) x 10^-9 photons m^-2 s^-1, or 1.7% of the Crab Nebula's flux (assuming the Crab Nebula spectrum measured by H.E.S.S). Supporting observations from Swift and RXTE are analyzed. The Swift observations are combined with previously published Fermi observations and the very-high-energy measurements to produce an overall spectral energy distribution which is then modeled assuming one-zone synchrotron-self-Compton emission. The chi^2 probability of the TeV flux being constant is 1.6%. This, when considered in combination with measured variability in the X-ray band, and the demonstrated variability of many TeV blazars, suggests that the use of blazars such as 1ES 0229+200 for intergalactic magnetic field studies may not be straightforward and challenges models that attribute hard TeV spectra to secondary gamma-ray production along the line of sight., Accepted for publication in ApJ

Published
2014
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37. Discovery of TeV Gamma-ray Emission Toward Supernova Remnant SNR G78.2+2.1

Author

M. Kertzman, A. O'Faolain de Bhroithe, M. Schroedter, Vikram V. Dwarkadas, S. Vincent, Wei Cui, M. J. Lang, S. Thibadeau, A. N. Otte, M. P. Connolly, A. McCann, R. Mukherjee, D. B. Saxon, N. H. Park, J. Millis, T. Aune, J. E. Ward, A. Cesarini, P. Moriarty, John L. Quinn, T. B. Humensky, A. Furniss, Frank Krennrich, A. S. Madhavan, G. Tešić, Gernot Maier, H. Prokoph, A. Varlotta, Wystan Benbow, S. P. Wakely, Eric V. Gotthelf, E. Roache, J. P. Finley, S. Archambault, H. J. Rose, R. A. Ong, Ralph Bird, G. H. Sembroski, P. Kaaret, Amanda Weinstein, Abraham D. Falcone, R. Welsing, Vladimir Vassiliev, L. Ciupik, T. C. Weekes, J. Grube, D. Gall, Geza Gyuk, K. Tsurusaki, S. Federici, Manel Errando, T. C. Arlen, J. H. Buckley, G. H. Gillanders, P. Majumdar, T. J. N. Nelson, S. McArthur, N. Galante, S. Godambe, Dirk Pandel, S. Griffin, G. Finnegan, C. Skole, C. Duke, David A. Williams, N. Karlsson, G. D. Şentürk, T. Weisgarber, H. Huan, E. Aliu, I. Telezhinsky, K. Lee, Jamie Holder, A. Popkow, J. Tyler, A. Bouvier, D. S. Hanna, V. Bugaev, J. S. Perkins, Martin Pohl, Q. Feng, J. Dumm, P. T. Reynolds, David Kieda, M. Theiling, Lucy Fortson, Karen Byrum, S. M. Bradbury, A. Cannon, E. Collins-Hughes, H. Krawczynski, M. Beilicke, M. Orr, G. Hughes, K. Ragan, B. Zitzer, J. Ruppel, R. Dickherber, Y. Khassen, and Luis C. Reyes

Subjects
catalog, Astrophysics::High Energy Astrophysical Phenomena, Hadron, Flux, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, cosmic rays, Observatory, 0103 physical sciences, origin, Supernova remnant, 010303 astronomy & astrophysics, 2cg078+2, Astrophysics::Galaxy Astrophysics, acceleration of particles, Physics, search, High Energy Astrophysical Phenomena (astro-ph.HE), particle-acceleration, 010308 nuclear & particles physics, hess, Gamma ray, Institut für Physik und Astronomie, counterpart, Astronomy and Astrophysics, gamma rays: general, Particle acceleration, Crab Nebula, Space and Planetary Science, ism: supernova remnants, ddc:520, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, fermi
Abstract

We report the discovery of an unidentified, extended source of very-high-energy (VHE) gamma-ray emission, VER J2019+407, within the radio shell of the supernova remnant SNR G78.2+2.1, using 21.4 hours of data taken by the VERITAS gamma-ray observatory in 2009. These data confirm the preliminary indications of gamma-ray emission previously seen in a two-year (2007-2009) blind survey of the Cygnus region by VERITAS. VER J2019+407, which is detected at a post-trials significance of 7.5 standard deviations in the 2009 data, is localized to the northwestern rim of the remnant in a region of enhanced radio and X-ray emission. It has an intrinsic extent of 0.23^{\circ} \pm 0.03^{\circ} (stat)+0.04^{\circ}_{-0.02}^{\circ}(sys) and its spectrum is well-characterized by a differential power law (dN/dE = N_0 \times (E/TeV)^{-\Gamma}) with a photon index of {\Gamma} = 2.37 \pm 0.14 (stat) \pm 0.20 (sys) and a flux normalization of N0 = 1.5 \pm 0.2 (stat) \pm 0.4(sys) \times 10^-12 ph TeV^{-1} cm^{-2} s^{-1}. This yields an integral flux of 5.2 \pm 0.8 (stat) \pm 1.4 (sys) \times 10^-12 ph cm^{-2} s^{-1} above 320 GeV, corresponding to 3.7% of the Crab Nebula flux. We consider the relationship of the TeV gamma-ray emission with the GeV gamma-ray emission seen from SNR G78.2+2.1 as well as that seen from a nearby cocoon of freshly accelerated cosmic rays. Multiple scenarios are considered as possible origins for the TeV gamma-ray emission, including hadronic particle acceleration at the supernova remnant shock., Comment: 18 pages, 5 figures, accepted for publication in ApJ

Published
2013
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38. VERITAS Observations of the Microquasar Cygnus X-3

Author

A. Varlotta, Martin Pohl, J. S. Perkins, David Kieda, P. Moriarty, Nicola Galante, J. Grube, M. P. Connolly, David A. Williams, M. J. Lang, Xuhui Chen, Matthias Beilicke, Abraham D. Falcone, I. Telezhinsky, A. McCann, G. H. Sembroski, Daniel Nieto, Wei Cui, Q. Feng, A. O'Faolain de Bhroithe, G. H. Gillanders, Jamie Holder, Y. Khassen, H. Prokoph, Henric Krawczynski, A. J.R. Weinstein, D. S. Hanna, F. Sheidaei, K. Berger, Geza Gyuk, T. B. Humensky, L. C. Reyes, Karen Byrum, P. T. Reynolds, Pratik Majumdar, Sinéad M. Griffin, D. Staszak, K. Ragan, Matteo Cerruti, Gareth Hughes, M. Kertzman, B. Zitzer, Lucy Fortson, R. A. Ong, Amy Furniss, S. Vincent, A. W. Smith, A. S Madhavan, Ralph Bird, C. Duke, Gordon T. Richards, Manel Errando, E. Roache, S. Federici, S. T. Griffiths, Michael L. McCollough, A. Bouvier, P. Kaaret, Wystan Benbow, S. McArthur, S. Archambault, Reshmi Mukherjee, A. Popkow, A. N. Otte, V. Bugaev, John L. Quinn, N. H. Park, J. V. Tucci, Gernot Maier, J. P. Finley, S. P. Wakely, T. C. Weekes, D. Pandel, L. Ciupik, Jean-Francois Rajotte, J. Tyler, J. H. Buckley, J. P. Dumm, and M. Theiling

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Radiation imaging, FOS: Physical sciences, Astrophysics, gamma rays: stars, 01 natural sciences, law.invention, Telescope, x-rays: individual (cygnus x-3), law, 0103 physical sciences, cyg x-3, 010303 astronomy & astrophysics, acceleration of particles, Physics, search, High Energy Astrophysical Phenomena (astro-ph.HE), binaries: close, 010308 nuclear & particles physics, Gamma ray, Institut für Physik und Astronomie, Astronomy and Astrophysics, gamma-ray emission, large-area telescope, scattering halo, x-ray, mission, Space and Planetary Science, cherenkov telescopes, ddc:520, relativistic jet, Astrophysics - High Energy Astrophysical Phenomena, constraints
Abstract

We report results from TeV gamma-ray observations of the microquasar Cygnus X-3. The observations were made with the Very Energetic Radiation Imaging Telescope Array System (VERITAS) over a time period from 2007 June 11 to 2011 November 28. VERITAS is most sensitive to gamma rays at energies between 85 GeV to 30 TeV. The effective exposure time amounts to a total of about 44 hours, with the observations covering six distinct radio/X-ray states of the object. No significant TeV gamma-ray emission was detected in any of the states, nor with all observations combined. The lack of a positive signal, especially in the states where GeV gamma rays were detected, places constraints on TeV gamma-ray production in Cygnus X-3. We discuss the implications of the results., Comment: 23 pages, 4 figures, 3 tables, accepted for publication in ApJ

Published
2013
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39. MULTIWAVELENGTH OBSERVATIONS OF THE TeV BINARY LS I +61° 303 WITH VERITAS, Fermi -LAT, AND Swift /XRT DURING A TeV OUTBURST

Author

S. Archambault, Gernot Maier, A. McCann, R. A. Ong, P. T. Reynolds, Lucy Fortson, N. Galante, S. P. Wakely, J. P. Finley, P. Fortin, A. D. Falcone, S. T. Griffiths, Y. Khassen, T. C. Weekes, A. W. Smith, Martin Pohl, Gordon T. Richards, Geza Gyuk, M. J. Lang, J. Dumm, M. Beilicke, S. Griffin, A. N. Otte, P. Majumdar, M. P. Connolly, K. Berger, L. Ciupik, B. Behera, D. Staszak, N. H. Park, Wystan Benbow, D. S. Hanna, John L. Quinn, G. H. Gillanders, Matteo Cerruti, E. Aliu, C. Skole, V. Bugaev, A. Varlotta, S. Federici, Q. Feng, A. Furniss, J. S. Perkins, David Kieda, G. Ratliff, S. Vincent, P. Kaaret, Gareth Hughes, E. Roache, R. Mukherjee, I. Telezhinsky, P. Moriarty, Jamie Holder, Ralph Bird, M. Kertzman, Xuhui Chen, J. Grube, A. O'Faolain de Bhroithe, A. Weinstein, A. Bouvier, Frank Krennrich, S. McArthur, F. Sheidaei, Wei Cui, H. Prokoph, T. B. Humensky, A. Popkow, Anna Zajczyk, J. Tyler, K. Ragan, B. Zitzer, Jean-Francois Rajotte, G. H. Sembroski, and R. Welsing

Subjects
Swift, Astrophysics::High Energy Astrophysical Phenomena, Binary number, FOS: Physical sciences, Astrophysics, telescope, gamma rays: stars, 01 natural sciences, law.invention, spectrum, Telescope, star, law, gamma-ray binary, 0103 physical sciences, emission, +61-degrees-303, 010303 astronomy & astrophysics, computer.programming_language, acceleration of particles, relativistic processes, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy and Astrophysics, binaries: general, x-ray, Space and Planetary Science, x-rays: binaries, Spectral energy distribution, ddc:520, Satellite, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, computer, Fermi Gamma-ray Space Telescope
Abstract

We present the results of a multiwavelength observational campaign on the TeV binary system LS I +61 303 with the VERITAS telescope array (>200 GeV), Fermi-LAT (0.3-300 GeV), and Swift-XRT (2-10 keV). The data were taken from December 2011 through January 2012 and show a strong detection in all three wavebands. During this period VERITAS obtained 24.9 hours of quality selected livetime data in which LS I +61 303 was detected at a statistical sig- nificance of 11.9 sigma. These TeV observations show evidence for nightly variability in the TeV regime at a post-trial significance of 3.6 sigma. The combination of the simultaneously obtained TeV and X-ray fluxes do not demonstrate any evidence for a correlation between emission in the two bands. For the first time since the launch of the Fermi satellite in 2008, this TeV detection allows the construction of a detailed MeV-TeV spectral energy distribution from LS I +61 303. This spectrum shows a distinct cutoff in emission near 4 GeV, with emission seen by the VERITAS observations following a simple power-law above 200 GeV. This feature in the spectrum of LS I +61 303, obtained from overlapping observations with Fermi-LAT and VERITAS, may indicate that there are two distinct populations of accelerated particles producing the GeV and TeV emission., Accepted for Publication in ApJ

Published
2013
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40. Acceleration of cosmic rays by young core-collapse supernova remnants

Author

Martin Pohl, Vikram V. Dwarkadas, and I. Telezhinsky

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Shock wave, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Context (language use), Astrophysics, Type II supernova, Shock (mechanics), Supernova, Acceleration, Stars, Space and Planetary Science, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

Context. Supernova remnants (SNRs) are thought to be the primary candidates for the sources of Galactic cosmic rays. According to the diffusive shock acceleration theory, SNR shocks produce a power-law spectrum with an index of s = 2, perhaps nonlinearly modified to harder spectra at high energy. Observations of SNRs often indicate particle spectra that are softer than that and show features not expected from classical theory. Known drawbacks of the standard approach are the assumption that SNRs evolve in a uniform environment, and that the reverse shock does not accelerate particles. Relaxing these assumptions increases the complexity of the problem, because one needs reliable hydrodynamical data for the plasma flow as well as good estimates for the magnetic field (MF) at the reverse shock. Aims. We show that these two factors are especially important when modeling young core-collapse SNRs that evolve in a complicated circumstellar medium shaped by the winds of progenitor stars. Methods. We used high-resolution numerical simulations for the hydrodynamical evolution of the SNR. Instead of parametrizations of the MF profiles inside the SNR, we followed the advection of the frozen-in MF inside the SNR, and thus obtained the B-field value at all locations, in particular at the reverse shock. To model cosmic-ray acceleration we solved the cosmic-ray transport equation in test-particle approximation. Results. We find that the complex plasma-flow profiles of core-collapse SNRs significantly modify the particle spectra. Additionally, the reverse shock strongly affects the emission spectra and the surface brightness., 12 pages, 7 figures, accepted for publication in Astronomy and Astrophysics

Published
2013
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41. Discovery of TeV Gamma-ray Emission from CTA 1 by VERITAS

Author

A. N. Otte, G. H. Sembroski, M. P. Connolly, E. Aliu, T. J. N. Nelson, R. Welsing, K. Lee, L. Ciupik, M. Theiling, P. Moriarty, Eric V. Gotthelf, Geza Gyuk, N. Karlsson, J. P. Finley, Wei Cui, Q. Feng, Gernot Maier, T. C. Weekes, I. Telezhinsky, Jamie Holder, S. Thibadeau, D. Gall, Oleg Kargaltsev, A. O'Faolain de Bhroithe, H. Krawczynski, A. Furniss, N. Galante, S. P. Wakely, R. Mukherjee, R. A. Ong, E. Roache, R. Dickherber, H. Prokoph, S. Vincent, A. S. Madhavan, Wystan Benbow, Abraham D. Falcone, S. Griffin, G. Finnegan, A. W. Smith, Mallory S. E. Roberts, S. McArthur, C. Duke, B. Zitzer, P. T. Reynolds, P. Kaaret, K. Ragan, J. Tyler, F. Krennrich, Y. Khassen, M. Schroedter, A. Bouvier, Vikram V. Dwarkadas, M. Vivier, J. Grube, M. Beilicke, Manel Errando, D. Staszak, S. Federici, J. H. Buckley, P. Majumdar, J. S. Perkins, David Kieda, D. B. Saxon, E. Collins-Hughes, Luis C. Reyes, N. H. Park, David A. Williams, Patrick Slane, M. Orr, T. B. Humensky, T. Aune, S. Godambe, G. Hughes, T. Arlen, Lucy Fortson, A. Cesarini, John L. Quinn, Martin Pohl, J. Dumm, Vladimir Vassiliev, A. Varlotta, M. J. Lang, A. Weinstein, K. Tsurusaki, G. H. Gillanders, D. S. Hanna, G. Tešić, V. Bugaev, S. Archambault, and A. McCann

Subjects
catalog, gamma-rays: stars, Photon, Astrophysics::High Energy Astrophysical Phenomena, supernova remnant cta-1, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar wind nebula, atmospheric cherenkov telescopes, Pulsar, Observatory, hess j1825-137, evolution, 0103 physical sciences, pulsations, crab-nebula, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, pulsars: individual (psr j0007+7303), 010308 nuclear & particles physics, Gamma ray, Astronomy and Astrophysics, x-rays: individual (rx j0007.0+7303), astronomy, supernovae: individual (g119.5+10.2), x-ray, Space and Planetary Science, ddc:520, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, pulsar-wind nebulae, Fermi Gamma-ray Space Telescope
Abstract

We report the discovery of TeV gamma-ray emission coincident with the shell-type radio supernova remnant (SNR) CTA 1 using the VERITAS gamma-ray observatory. The source, VER J0006+729, was detected as a 6.5 standard deviation excess over background and shows an extended morphology, approximated by a two-dimensional Gaussian of semi-major (semi-minor) axis 0.30 degree (0.24 degree) and a centroid 5' from the Fermi gamma-ray pulsar PSR J0007+7303 and its X-ray pulsar wind nebula (PWN). The photon spectrum is well described by a power-law dN/dE = N_0 (E/3 TeV)^(-\Gamma), with a differential spectral index of \Gamma = 2.2 +- 0.2_stat +- 0.3_sys, and normalization N_0 = (9.1 +- 1.3_stat +- 1.7_sys) x 10^(-14) cm^(-2) s^(-1) TeV^(-1). The integral flux, F_\gamma = 4.0 x 10^(-12) erg cm^(-2) s^(-1) above 1 TeV, corresponds to 0.2% of the pulsar spin-down power at 1.4 kpc. The energetics, co-location with the SNR, and the relatively small extent of the TeV emission strongly argue for the PWN origin of the TeV photons. We consider the origin of the TeV emission in CTA 1., Comment: 10 pages, 9 figures, accepted for publication in ApJ

Published
2012
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42. Search for a correlation between very-high-energy gamma rays and giant radio pulses in the Crab pulsar

Author

Matthias Beilicke, J. P. Dumm, Martin Pohl, G. Tešić, Q. Feng, V. Bugaev, T. Aune, A. Varlotta, R. Dickherber, T. B. Humensky, T. J. N. Nelson, S. Thibadeau, A. McCann, M. P. Connolly, Maxim Lyutikov, R. G. Wagner, Henric Krawczynski, E. Aliu, A. J.R. Weinstein, I. Telezhinsky, Jamie Holder, F. Krennrich, H. Prokoph, S. Vincent, L. C. Reyes, K. Lee, Sinéad M. Griffin, D. B. Saxon, Karen Byrum, D. S. Hanna, N. H. Park, Lucy Fortson, D. Staszak, K. Tsurusaki, M. Theiling, T. C. Arlen, K. Ragan, Gareth Hughes, Amy Furniss, P. Kaaret, M. Schroedter, B. Zitzer, E. Collins-Hughes, Gernot Maier, M. J. Lang, G. H. Gillanders, S. Godambe, S. P. Wakely, G. H. Sembroski, Daniel Gall, R. Welsing, A. N. Otte, Matthew R. Orr, L. Ciupik, A. Cesarini, R. A. Ong, V. Kondratiev, David A. Williams, John L. Quinn, A. Bouvier, J. H. Buckley, A. D. Falcone, J. P. Finley, M. Vivier, T. C. Weekes, S. LeBohec, David Kieda, S. McArthur, Y. Khassen, P. T. Reynolds, Geza Gyuk, Pratik Majumdar, S. Archambault, Reshmi Mukherjee, Wystan Benbow, J. S. Perkins, P. Moriarty, Nicola Galante, J. Grube, N. Karlsson, G. Finnegan, A. W. Smith, A. S Madhavan, C. Duke, E. Roache, G. D. Şentürk, H. Huan, A. O'Faolain de Bhroithe, S. Federici, and Wei Cui

Subjects
High energy, nebula, pulsars: individual: b0531+21, Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, Arrival time, law.invention, Radio telescope, Telescope, law, Time windows, 0103 physical sciences, emission, photons, rays: stars, geminga, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), model, 010308 nuclear & particles physics, Crab Pulsar, Gamma ray, Institut für Physik und Astronomie, Astronomy and Astrophysics, telescopes, universe, Space and Planetary Science, range, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the results of a joint observational campaign between the Green Bank radio telescope and the VERITAS gamma-ray telescope, which searched for a correlation between the emission of very-high-energy (VHE) gamma rays ($E_{\gamma} >$ 150 GeV) and Giant Radio Pulses (GRPs) from the Crab pulsar at 8.9 GHz. A total of 15366 GRPs were recorded during 11.6 hours of simultaneous observations, which were made across four nights in December 2008 and in November and December 2009. We searched for an enhancement of the pulsed gamma-ray emission within time windows placed around the arrival time of the GRP events. In total, 8 different time windows with durations ranging from 0.033 ms to 72 s were positioned at three different locations relative to the GRP to search for enhanced gamma-ray emission which lagged, led, or was concurrent with, the GRP event. Further, we performed separate searches on main pulse GRPs and interpulse GRPs and on the most energetic GRPs in our data sample. No significant enhancement of pulsed VHE emission was found in any of the preformed searches. We set upper limits of 5-10 times the average VHE flux of the Crab pulsar on the flux simultaneous with interpulse GRPs on single-rotation-period time scales. On $\sim$8-second time scales around interpulse GRPs, we set an upper limit of 2-3 times the average VHE flux. Within the framework of recent models for pulsed VHE emission from the Crab pulsar, the expected VHE-GRP emission correlations are below the derived limits., Comment: 12 pages, 12 figures, To appear in The Astrophysical Journal

Published
2012
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43. VERITAS Observations of the Nova in V407 Cygni

Author

H. J. Rose, A. Cesarini, John L. Quinn, Gernot Maier, S. Griffin, M. Orr, A. Varlotta, Martin Pohl, D. Staszak, G. Hughes, E. Aliu, S. P. Wakely, J. Dumm, S. Vincent, K. Lee, D. S. Hanna, G. Tešić, M. Theiling, T. Weisgarber, S. M. Bradbury, A. Cannon, P. Kaaret, J. P. Finley, S. Godambe, M. Kertzman, T. B. Humensky, T. C. Weekes, K. Tsurusaki, Geza Gyuk, Dirk Pandel, M. J. Lang, S. Thibadeau, H. Krawczynski, V. Bugaev, T. Arlen, N. Galante, J. Ruppel, M. Schroedter, Vikram V. Dwarkadas, B. Zitzer, G. Finnegan, J. Grube, A. W. Smith, Manel Errando, S. Archambault, Lucy Fortson, G. H. Sembroski, M. Vivier, Abraham D. Falcone, C. Duke, M. Beilicke, Wystan Benbow, J. H. Buckley, David A. Williams, R. Welsing, D. B. Saxon, H. Huan, N. H. Park, K. Ragan, S. McArthur, I. Telezhinsky, David Kieda, Paul D. Nuñez, A. McCann, Wei Cui, Jamie Holder, P. Majumdar, E. Roache, P. Moriarty, J. E. Ward, G. Decerprit, C. Skole, A. Weinstein, H. Prokoph, J. Tyler, Karen Byrum, R. A. Ong, A. N. Otte, M. P. Connolly, Q. Feng, T. Aune, F. Krennrich, J. S. Perkins, E. Collins-Hughes, L. Ciupik, J. Millis, A. Bouvier, P. T. Reynolds, D. Gall, R. Mukherjee, Luis C. Reyes, N. Karlsson, A. Furniss, R. Dickherber, and Y. Khassen

Subjects
High energy, blast wave, FOS: Physical sciences, Radiation imaging, Flux, array, Astrophysics, galactic plane, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, novae, cataclysmic variables, 010306 general physics, 010303 astronomy & astrophysics, Zenith, white dwarfs, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gamma ray, Institut für Physik und Astronomie, Astronomy and Astrophysics, gamma rays: general, Nova (laser), gamma-ray emission, Astrophysics - Astrophysics of Galaxies, rs-ophiuchi, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), cherenkov telescopes, Astrophysics - High Energy Astrophysical Phenomena, 2006 outburst, discovery
Abstract

We report on very high energy (E > 100 GeV) gamma-ray observations of V407 Cygni, a symbiotic binary that underwent a nova outburst producing 0.1-10 GeV gamma rays during 2010 March 10-26. Observations were made with the Very Energetic Radiation Imaging Telescope Array System during 2010 March 19-26 at relatively large zenith angles, due to the position of V407 Cyg. An improved reconstruction technique for large zenith angle observations is presented and used to analyze the data. We do not detect V407 Cygni and place a differential upper limit on the flux at 1.6 TeV of 2.3 \times 10^(-12) erg cm^(-2) s^(-1) (at the 95% confidence level). When considered jointly with data from Fermi-LAT, this result places limits on the acceleration of very high energy particles in the nova., 17 pages, 4 figures, accepted for publication in ApJ

Published
2012
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44. Particle spectra from acceleration at forward and reverse shocks of young Type Ia Supernova Remnants

Author

I. Telezhinsky, Martin Pohl, and Vikram V. Dwarkadas

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Scattering, Astrophysics::High Energy Astrophysical Phenomena, Population, Time evolution, FOS: Physical sciences, Institut für Physik und Astronomie, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Shock (mechanics), Particle acceleration, Supernova, Acceleration, Astrophysics - High Energy Astrophysical Phenomena, education, Astrophysics::Galaxy Astrophysics
Abstract

We study cosmic-ray acceleration in young Type Ia Supernova Remnants (SNRs) by means of test-particle diffusive shock acceleration theory and 1-D hydrodynamical simulations of their evolution. In addition to acceleration at the forward shock, we explore the particle acceleration at the reverse shock in the presence of a possible substantial magnetic field, and consequently the impact of this acceleration on the particle spectra in the remnant. We investigate the time evolution of the spectra for various time-dependent profiles of the magnetic field in the shocked region of the remnant. We test a possible influence on particle spectra of the Alfv\'enic drift of scattering centers in the precursor regions of the shocks. In addition, we study the radiation spectra and morphology in a broad band from radio to gamma-rays. It is demonstrated that the reverse shock contribution to the cosmic-ray particle population of young Type Ia SNRs may be significant, modifying the spatial distribution of particles and noticeably affecting the volume-integrated particle spectra in young SNRs. In particular spectral structures may arise in test-particle calculations that are often discussed as signatures of non-linear cosmic-ray modification of shocks. Therefore, the spectrum and morphology of emission, and their time evolution, differ from pure forward-shock solutions., Comment: Accepted in Astroparticle Physics

Published
2012

45. Discovery of High-energy and Very High Energy Gamma-ray Emission from the Blazar RBS 0413

Author

D. Gall, M. P. Connolly, R. Mukherjee, G. H. Sembroski, S. McArthur, T. B. Humensky, S. Archambault, S. Griffin, P. Fortin, H. J. Rose, A. Pichel, P. T. Reynolds, J. E. Ward, A. Cesarini, A. N. Otte, John L. Quinn, A. S. Madhavan, Wystan Benbow, A. Varlotta, P. Majumdar, I. Telezhinsky, J. Grube, R. A. Ong, Manel Errando, Jamie Holder, A. Bouvier, M. J. Lang, M. Theiling, J. P. Finley, S. M. Bradbury, K. Ragan, Wei Cui, S. Thibadeau, T. Aune, Markus Böttcher, T. C. Weekes, Abraham D. Falcone, G. Decerprit, L. C. Reyes, A. McCann, H. Prokoph, E. Roache, N. Palma, Geza Gyuk, G. Tešić, E. Aliu, D. Horan, J. Ruppel, L. Ciupik, Gareth Hughes, M. Kertzman, B. Zitzer, T. Weisgarber, K. Lee, D. S. Hanna, V. Bugaev, A. Weinstein, M. Vivier, David A. Williams, H. Krawczynski, K. Tsurusaki, S. Godambe, T. Arlen, Lucy Fortson, Martin Pohl, J. Dumm, Keith Hawkins, Karen Byrum, M. Schroedter, M. Beilicke, David Kieda, J. H. Buckley, J. S. Perkins, E. Collins-Hughes, F. Krennrich, M. Orr, Q. Feng, A. Cannon, P. Kaaret, D. B. Saxon, N. H. Park, Gernot Maier, S. P. Wakely, N. Galante, G. Finnegan, A. W. Smith, G. D. Şentürk, H. Huan, Paolo De Coppi, P. Moriarty, A. Furniss, D. Staszak, R. Dickherber, Y. Khassen, and N. Karlsson

Subjects
catalog, Astrophysics::High Energy Astrophysical Phenomena, bl-lacertae objects, Flux, FOS: Physical sciences, Astrophysics, swift ultraviolet/optical telescope, bright blazars, 7. Clean energy, 01 natural sciences, law.invention, Telescope, law, gamma rays: galaxies, 0103 physical sciences, bl lacertae objects: individual (rbs 0413-ver j0319+187), Blazar, Nuclear Experiment, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), model, 010308 nuclear & particles physics, Institut für Physik und Astronomie, Astronomy and Astrophysics, lac objects, Synchrotron, radiation, large-area telescope, Crab Nebula, mission, 13. Climate action, Space and Planetary Science, active galactic nuclei, Spectral energy distribution, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object, Fermi Gamma-ray Space Telescope
Abstract

We report on the discovery of high-energy (HE; E > 0.1 GeV) and very high-energy (VHE; E > 100 GeV) gamma-ray emission from the high-frequency-peaked BL Lac object RBS 0413. VERITAS, a ground-based gamma-ray observatory, detected VHE gamma rays from RBS 0413 with a statistical significance of 5.5 standard deviations (sigma) and a gamma-ray flux of (1.5 \pm 0.6stat \pm 0.7syst) \times 10^(-8) photons m^(-2) s^(-1) (\sim 1% of the Crab Nebula flux) above 250 GeV. The observed spectrum can be described by a power law with a photon index of 3.18 \pm 0.68stat \pm 0.30syst. Contemporaneous observations with the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope detected HE gamma rays from RBS 0413 with a statistical significance of more than 9 sigma, a power-law photon index of 1.57 \pm 0.12stat +0.11sys -0.12sys and a gamma-ray flux between 300 MeV and 300 GeV of (1.64 \pm 0.43stat +0.31sys -0.22sys) \times 10^(-5) photons m^(-2) s^(-1). We present the results from Fermi-LAT and VERITAS, including a spectral energy distribution modeling of the gamma-ray, quasi-simultaneous X-ray (Swift-XRT), ultraviolet (Swift-UVOT) and R-band optical (MDM) data. We find that, if conditions close to equipartition are required, both the combined synchrotron self-Compton/external-Compton and the lepto-hadronic models are preferred over a pure synchrotron self-Compton model., 14 pages, 3 figures, accepted to ApJ, corresponding author: G. D. Senturk

Published
2012
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46. VERITAS deep observations of the dwarf spheroidal galaxy Segue 1

Author

A. McCann, I. Telezhinsky, R. A. Ong, Jamie Holder, T. Arlen, G. Teić, Philip Kaaret, A. S. Madhavan, Wystan Benbow, S. Vincent, N. Galante, G. D. Entürk, A. Bouvier, G. H. Sembroski, S. McArthur, G. Finnegan, A. W. Smith, S. M. Bradbury, Gernot Maier, M. P. Connolly, S. P. Wakely, Abraham D. Falcone, A. Varlotta, T. Aune, J. Grube, A. Cannon, E. Roache, H. Huan, Matthew R. Orr, R. Dickherber, Manel Errando, Daniel Gall, Karen Byrum, K. Ragan, S. Thibadeau, J. H. Buckley, E. Collins-Hughes, M. Kertzman, Lucy Fortson, J. S. Perkins, H. J. Rose, G. Decerprit, V. Bugaev, Q. Feng, P. Moriarty, M. Vivier, M. Beilicke, M. Schroedter, David A. Williams, Y. Khassen, T. Weisgarber, D. Staszak, J. E. Ward, S. Archambault, Reshmi Mukherjee, T. B. Humensky, A. Furniss, Francesc Ferrer, Geza Gyuk, D. B. Saxon, A. Cesarini, John L. Quinn, B. Zitzer, P. T. Reynolds, N. H. Park, Henric Krawczynski, L. Ciupik, P. Majumdar, E. Aliu, K. Tsurusaki, Jodi Christiansen, C. Skole, D. Hanna, Martin Pohl, S. Godambe, J. Dumm, K. Lee, L. C. Reyes, Vladimir Vassiliev, N. Karlsson, J. P. Finley, T. C. Weekes, Wei Cui, H. Prokoph, R. G. Wagner, David Kieda, M. Theiling, J. Ruppel, Amanda Weinstein, A. N. Otte, Frank Krennrich, Sinéad M. Griffin, and Gareth Hughes

Subjects
Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, Dwarf galaxy problem, cosmic-rays, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, dark-matter annihilation, 01 natural sciences, local group, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), 0103 physical sciences, upper limits, ddc:530, 010303 astronomy & astrophysics, Light dark matter, galactic-center, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Hot dark matter, Institut für Physik und Astronomie, Astronomy, Segue, gamma-ray emission, Galaxy, Dwarf spheroidal galaxy, Dark matter halo, large-area telescope, cherenkov telescopes, Astrophysics - High Energy Astrophysical Phenomena, magic telescope, empirical-models
Abstract

The VERITAS array of Cherenkov telescopes has carried out a deep observational program on the nearby dwarf spheroidal galaxy Segue 1. We report on the results of nearly 48 hours of good quality selected data, taken between January 2010 and May 2011. No significant $\gamma$-ray emission is detected at the nominal position of Segue 1, and upper limits on the integrated flux are derived. According to recent studies, Segue 1 is the most dark matter-dominated dwarf spheroidal galaxy currently known. We derive stringent bounds on various annihilating and decaying dark matter particle models. The upper limits on the velocity-weighted annihilation cross-section are $\mathrm{^{95% CL} \lesssim 10^{-23} cm^{3} s^{-1}}$, improving our limits from previous observations of dwarf spheroidal galaxies by at least a factor of two for dark matter particle masses $\mathrm{m_{\chi}\gtrsim 300 GeV}$. The lower limits on the decay lifetime are at the level of $\mathrm{\tau^{95% CL} \gtrsim 10^{24} s}$. Finally, we address the interpretation of the cosmic ray lepton anomalies measured by ATIC and PAMELA in terms of dark matter annihilation, and show that the VERITAS observations of Segue 1 disfavor such a scenario., Comment: Added recently published erratum at the end of the original article

Published
2012
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47. Multiwavelength observations of the AGN 1ES 0414+009 with veritas, FERMI-LAT, SWIFT-XRT, AND MDM

Author

E. Aliu, S. Archambault, T. Arlen, T. Aune, M. Beilicke, W. Benbow, M. Böttcher, A. Bouvier, V. Bugaev, A. Cannon, A. Cesarini, L. Ciupik, E. Collins-Hughes, M. P. Connolly, W. Cui, R. Dickherber, J. Dumm, M. Errando, A. Falcone, S. Federici, Q. Feng, J. P. Finley, G. Finnegan, L. Fortson, A. Furniss, N. Galante, D. Gall, S. Godambe, S. Griffin, J. Grube, G. Gyuk, D. Hanna, J. Holder, H. Huan, G. Hughes, C. M. Hui, A. Imran, O. Jameil, P. Kaaret, N. Karlsson, M. Kertzman, J. Kerr, Y. Khassen, D. Kieda, H. Krawczynski, F. Krennrich, M. J. Lang, K. Lee, A. S. Madhavan, P. Majumdar, S. McArthur, A. McCann, P. Moriarty, R. Mukherjee, T. Nelson, A. O'Faoláin de Bhróithe, R. A. Ong, M. Orr, A. N. Otte, N. Park, J. S. Perkins, A. Pichel, M. Pohl, J. Quinn, K. Ragan, P. T. Reynolds, E. Roache, J. Ruppel, D. B. Saxon, M. Schroedter, G. H. Sembroski, G. D. Şentürk, A. W. Smith, D. Staszak, M. Stroh, I. Telezhinsky, G. Tešić, M. Theiling, S. Thibadeau, K. Tsurusaki, A. Varlotta, V. V. Vassiliev, M. Vivier, S. P. Wakely, J. E. Ward, A. Weinstein, R. Welsing, D. A. Williams, and B. Zitzer

Subjects
stars, Photon, Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, blazars, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, telescope, 01 natural sciences, Power law, purl.org/becyt/ford/1 [https], gamma-ray astronomy, 0103 physical sciences, gamma rays: galaxies, emission, bl lacertae objects: individual (1es 0414+009, erj0416+011), Nuclear Experiment, 010303 astronomy & astrophysics, Cherenkov radiation, Physics, search, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Institut für Physik und Astronomie, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], sample, Astronomía, Crab Nebula, individual (1ES 0414+009, VERJ0416+011) [BL Lacertae objects], Space and Planetary Science, bl lacertae object, galaxies [gamma rays], Spectral energy distribution, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, discovery, Fermi Gamma-ray Space Telescope, BL Lac object
Abstract

We present observations of the BL Lac object 1ES 0414+009 in the >200 GeV gamma-ray band by the VERITAS array of Cherenkov telescopes. 1ES 0414+009 was observed by VERITAS between January 2008 and February 2011, resulting in 56.2 hours of good quality pointed observations. These observations resulted in a detection of 822 events from the source corresponding to a statistical significance of 6.4 standard deviations (6.4 sigma) above the background. The source flux, showing no evidence for variability, is measured as 5.2 +/- 1.1_stat +/- 2.6_sys * 10^-12 photons cm^-2 s^-1 above 200 GeV, equivalent to approximately 2% of the Crab Nebula flux above this energy. The differential photon spectrum from 230 GeV to 850 GeV is well fit by a power law with an photon index of Gamma 3.4 +/- 0.5_stat +/- 0.3_sys and a flux normalization of 1.6 +/- 0.3_stat +/- 0.8_sys * 10^-11 photons cm^-2 s^-1 at 300 GeV. We also present multiwavelength results taken in the optical (MDM), X-ray (Swift-XRT), and GeV (Fermi-LAT) bands and use these results to construct a broadband spectral energy distribution (SED). Modeling of this SED indicates that homogenous one-zone leptonic scenarios are not adequate to describe emission from the system, with a lepto-hadronic model providing a better fit to the data., Accepted for publication in The Astrophysical Journal

Published
2012
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48. VERITAS Observations of Six Bright, Hard-Spectrum Fermi-LAT Blazars

Author

S. McArthur, Martin Pohl, T. Aune, J. Dumm, A. O'Faolain de Bhroithe, H. Krawczynski, D. B. Saxon, S. Griffin, A. N. Otte, D. S. Hanna, S. Thibadeau, Jason X. Prochaska, N. H. Park, R. A. Ong, Markus Böttcher, D. Horan, A. Bouvier, F. Krennrich, J. H. Buckley, M. Orr, Wystan Benbow, L. Ciupik, P. T. Reynolds, Gernot Maier, K. Ragan, S. P. Wakely, H. Prokoph, V. V. Vassiliev, N. Galante, S. Vincent, Abraham D. Falcone, D. Gall, David A. Williams, R. Mukherjee, J. S. Perkins, A. Pichel, E. Collins-Hughes, P. Fortin, T. Arlen, M. P. Connolly, G. Finnegan, A. McCann, B. Zitzer, A. Cesarini, A. S Madhavan, C. Duke, Q. Feng, John L. Quinn, E. Aliu, A. Varlotta, Geza Gyuk, Lucy Fortson, H. Huan, K. Lee, Pratik Majumdar, J. Grube, Manel Errando, Kyle F. Kaplan, I. Telezhinsky, Jamie Holder, J. P. Finley, E. Roache, A. Furniss, L. C. Reyes, T. C. Weekes, R. Dickherber, G. H. Sembroski, R. Welsing, D. Staszak, Michele Fumagalli, Y. Khassen, P. Kaaret, N. Karlsson, S. Federici, P. Moriarty, Wei Cui, S. Archambault, M. Theiling, G. Tešić, T. J. N. Nelson, V. Bugaev, A. Weinstein, M. Vivier, M. Beilicke, David Kieda, K. Tsurusaki, S. Godambe, Aliu, E, Archambault, S, Arlen, T, Aune, T, Beilicke, M, Benbow, W, Bottcher, M, Bouvier, A, Buckley, J, Bugaev, V, Cesarini, A, Ciupik, L, Collins-Hughes, E, Connolly, M, Cui, W, Dickherber, R, Duke, C, Dumm, J, Errando, M, Falcone, A, Federici, S, Feng, Q, Finley, J, Finnegan, G, Fortson, L, Furniss, A, Galante, N, Gall, D, Godambe, S, Griffin, S, Grube, J, Gyuk, G, Hanna, D, Holder, J, Huan, H, Kaaret, P, Karlsson, N, Khassen, Y, Kieda, D, Krawczynski, H, Krennrich, F, Lee, K, Madhavan, A, Maier, G, Majumdar, P, Mcarthur, S, Mccann, A, Moriarty, P, Mukherjee, R, Nelson, T, De Bhroithe, A, Ong, R, Orr, M, Otte, A, Park, N, Perkins, J, Pichel, A, Pohl, M, Prokoph, H, Quinn, J, Ragan, K, Reyes, L, Reynolds, P, Roache, E, Saxon, D, Sembroski, G, Staszak, D, Telezhinsky, I, Tesic, G, Theiling, M, Thibadeau, S, Tsurusaki, K, Varlotta, A, Vassiliev, V, Vincent, S, Vivier, M, Wakely, S, Weekes, T, Weinstein, A, Welsing, R, Williams, D, Zitzer, B, Fortin, P, Horan, D, Fumagalli, M, Kaplan, K, and Prochaska, J

Subjects
Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, purl.org/becyt/ford/1 [https], Telescope, law, 0103 physical sciences, gamma rays: galaxie, Astrophysics::Solar and Stellar Astrophysics, Blazar, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, general [BL Lacertae objects], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Institut für Physik und Astronomie, Spectral density, Astronomy and Astrophysics, BL Lacertae objects: general, purl.org/becyt/ford/1.3 [https], Synchrotron, Redshift, Astronomía, Extragalactic background light, Space and Planetary Science, Sky, galaxies [gamma rays], Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Fermi Gamma-ray Space Telescope
Abstract

We report on VERITAS very high energy (VHE; E > 100 GeV) observations of six blazars selected from the Fermi Large Area Telescope First Source Catalog (1FGL). The gamma-ray emission from 1FGL sources was extrapolated up to the VHE band, taking gamma-ray absorption by the extragalactic background light into account. This allowed the selection of six bright, hard-spectrum blazars that were good candidate TeV emitters. Spectroscopic redshift measurements were attempted with the Keck Telescope for the targets without Sloan Digital Sky Survey spectroscopic data. No VHE emission is detected during the observations of the six sources described here. Corresponding TeV upper limits are presented, along with contemporaneous Fermi observations and non-concurrent Swift UVOT and X-Ray Telescope data. The blazar broadband spectral energy distributions (SEDs) are assembled and modeled with a single-zone synchrotron self-Compton model. The SED built for each of the six blazars shows a synchrotron peak bordering between the intermediate- and high-spectrum-peak classifications, with four of the six resulting in particle-dominated emission regions. Fil: Aliu, E.. Columbia University; Estados Unidos Fil: Archambault, S.. McGill University; Canadá Fil: Arlen, T.. University of California; Estados Unidos Fil: Aune, E.. University of California; Estados Unidos Fil: Beilicke, M.. University of Washington; Estados Unidos Fil: Benbow, W.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Bottcher, M.. Ohio University; Estados Unidos Fil: Bouvier, A.. University of California; Estados Unidos Fil: Buckley, J. H.. University of Washington; Estados Unidos Fil: Bugaev, V.. University of Washington; Estados Unidos Fil: Cesarini, A.. National University of Ireland Galway; Irlanda Fil: Ciupik, L.. Adler Planetarium and Astronomy Museum; Estados Unidos Fil: Collin Hughes, E.. University College Dublin; Irlanda Fil: Connolly, M. P.. National University of Ireland Galway; Irlanda Fil: Cui, W.. Purdue University; Estados Unidos Fil: Dickherber, R.. University of Washington; Estados Unidos Fil: Duke, C.. Grinnell College; Estados Unidos Fil: Dumm, J.. University Of Minnesota; Estados Unidos Fil: Errando, M.. Columbia University; Estados Unidos Fil: Falcone, A.. University of Pennsylvania; Estados Unidos Fil: Federici, S.. Desy; Alemania Fil: Feng, Q.. Purdue University; Estados Unidos Fil: Finley, J. P.. Purdue University; Estados Unidos Fil: Finnegan, G.. University of Utah; Estados Unidos Fil: Fortson, L.. University Of Minnesota; Estados Unidos Fil: Furniss, A.. University of California; Estados Unidos Fil: Galante, N.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Gall, D.. University of Iowa; Estados Unidos Fil: Godambe, S.. University of Utah; Estados Unidos Fil: Griffin, S.. McGill University; Canadá Fil: Pichel, Ana Carolina. 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 Veritas Collaboration.

Published
2012
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49. On the maximum energy and escape of accelerated particles in young supernova remnants

Author

I. Telezhinsky, Martin Pohl, and Vikram V. Dwarkadas

Subjects
Physics, Supernova, Stars, Astrophysics::High Energy Astrophysical Phenomena, Time evolution, Astrophysics::Solar and Stellar Astrophysics, Astronomy, Astrophysics, Astrophysics::Galaxy Astrophysics, Energy (signal processing), Magnetic field
Abstract

Using analytic expressions and self-similar solutions, we explore different environments in which supernova remnants (SNRs) evolve, and investigate how the maximum energy to which particles are accelerated, and its time evolution, is a function of the complex environment. We take into account the ambient magnetic field and its amplification by resonant or non-resonant modes. We find that particles reach the maximum energies in the ejecta-dominated stage, much earlier than Sedov stage, particularly in the case of core-collapse SNe expanding in the winds of massive stars.

Published
2012
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50. Constraints on Cosmic Rays, Magnetic Fields, and Dark Matter from Gamma-Ray Observations of the Coma Cluster of Galaxies with VERITAS and Fermi

Author

T. Arlen, T. Aune, M. Beilicke, W. Benbow, A. Bouvier, J. H. Buckley, V. Bugaev, K. Byrum, A. Cannon, A. Cesarini, L. Ciupik, E. Collins-Hughes, M. P. Connolly, W. Cui, R. Dickherber, J. Dumm, A. Falcone, S. Federici, Q. Feng, J. P. Finley, G. Finnegan, L. Fortson, A. Furniss, N. Galante, D. Gall, S. Godambe, S. Griffin, J. Grube, G. Gyuk, J. Holder, H. Huan, G. Hughes, T. B. Humensky, A. Imran, P. Kaaret, N. Karlsson, M. Kertzman, Y. Khassen, D. Kieda, H. Krawczynski, F. Krennrich, K. Lee, A. S Madhavan, G. Maier, P. Majumdar, S. McArthur, A. McCann, P. Moriarty, R. Mukherjee, T. Nelson, A. O’Faoláin de Bhróit, R. A. Ong, M. Orr, A. N. Otte, N. Park, J. S. Perkins, M. Pohl, H. Prokoph, J. Quinn, K. Ragan, L. C. Reyes, P. T. Reynolds, E. Roache, J. Ruppel, D. B. Saxon, M. Schroedter, G. H. Sembroski, C. Skole, A. W. Smith, I. Telezhinsky, G. Tešić, M. Theiling, S. Thibadeau, K. Tsurusaki, A. Varlotta, M. Vivier, S. P. Wakely, J. E. Ward, A. Weinstein, R. Welsing, D. A. Williams, B. Zitzer, C. Pfrommer, and A. Pinzke

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, nonthermal emission, FOS: Physical sciences, Coma (optics), Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: clusters: individual (coma (aco 1656)), magnetic fields, dark matter, large-scale structure, shock-waves, atmospheric cherenkov telescopes, diffuse radio-emission, cosmic rays, all-sky survey, Coma Cluster, upper limits, galactic-center, Galaxy cluster, Cherenkov radiation, gamma rays: galaxies: clusters, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Institut für Physik und Astronomie, Astronomy and Astrophysics, source catalog, Galaxy, x-ray, galaxies: clusters: general, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

Observations of radio halos and relics in galaxy clusters indicate efficient electron acceleration. Protons should likewise be accelerated, suggesting that clusters may also be sources of very high-energy (VHE; E>100 GeV) gamma-ray emission. We report here on VHE gamma-ray observations of the Coma galaxy cluster with the VERITAS array of imaging Cherenkov telescopes, with complementing Fermi-LAT observations at GeV energies. No significant gamma-ray emission from the Coma cluster was detected. Integral flux upper limits at the 99% confidence level were measured to be on the order of (2-5)*10^-8\ ph. m^-2 s^-1 (VERITAS, >220 GeV} and ~2*10^-6 ph. m^-2 s^-1 (Fermi, 1-3 GeV), respectively. We use the gamma-ray upper limits to constrain CRs and magnetic fields in Coma. Using an analytical approach, the CR-to-thermal pressure ratio is constrained to be < 16% from VERITAS data and < 1.7% from Fermi data (averaged within the virial radius). These upper limits are starting to constrain the CR physics in self-consistent cosmological cluster simulations and cap the maximum CR acceleration efficiency at structure formation shocks to be, ApJ in press

Published
2012
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