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1. THE 2009 DECEMBER GAMMA-RAY FLARE OF 3C 454.3: THE MULTIFREQUENCY CAMPAIGN

Author

L. Salotti, E. Moretti, Mark Gurwell, C. Pittori, M. Tavani, S. Vercellone, V. Vittorini, F. Longo, T. Sakamoto, Martino Marisaldi, A. Morselli, M. Galli, P. Santolamazza, G. Barbiellini P. Caraveo, Elena Pian, C. M. Raiteri, M. Pilia, Francesco Lucarelli, A. Trois, A. Rubini, F. D'Ammando, F. Verrecchia, Michael C. Stroh, M. Prest, F. Perotti, Andrea Tiengo, E. Vallazza, P. W. Cattaneo, M. Feroci, Merja Tornikoski, M. Villata, L. Pacciani, P. Picozza, A. Pellizzoni, E. Costa, E. Del Monte, A. Rappoldi, M. Fiorini, Ryosuke Itoh, P. A. Curran, Masayuki Yamanaka, G. Pucella, F. Lazzarotto, Valeri M. Larionov, C. S. Lin, F. Gianotti, A. C. Sadun, A. Giuliani, V. Cocco, Arnaud Ferrari, P. Lipari, M. Trifoglio, M. Fiocchi, E. Morelli, Andrei Berdyugin, G. Piano, H. A. Krimm, Sandro Mereghetti, L. O. Takalo, A. D. Falcone, S. Colafrancesco, Claudio Labanti, D. Zanello, F. Fuschino, D. Fugazza, G. Di Cocco, M. Rapisarda, A. Argan, Andrea Bulgarelli, Makoto Uemura, P. Giommi, Anne Lähteenmäki, G. De Paris, I. Donnarumma, Y. Evangelista, P. Soffitta, A. W. Chen, Paolo Leto, Hugh D. Aller, E. Striani, Mahito Sasada, I. Lapshov, M. F. Aller, S. Sabatini, Pacciani L, Vittorini V, Tavani M, Fiocchi MT, Vercellone S, DAmmando F, Sakamoto T, Pian E, Raiteri CM, Villata M, Sasada M, Itoh R, Yamanaka M, Uemura M, Striani E, Fugazza D, Tiengo A, Krimm HA, Stroh MC, Falcone AD, Curran PA, Sadun AC, Lahteenmaki A, Tornikoski M, Aller HD, Aller MF, Lin CS, Larionov VM, Leto P, Takalo LO, Berdyugin A, Gurwell MA, Bulgarelli A, Chen AW, Donnarumma I, Giuliani A, Longo F, Pucella G, Argan A, Barbiellini G, Caraveo P, Cattaneo PW, Costa E, De Paris G, Del Monte E, Di Cocco G, Evangelista Y, Ferrari A, Feroci M, Fiorini M, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Marisaldi M, Mereghetti S, Morelli E, Moretti E, Morselli A, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Prest M, Rapisarda M, Rappoldi A, Rubini A, Sabatini S, Soffitta P, Trifoglio M, Trois A, Vallazza E, Zanello D, Colafrancesco S, Pittori C, Verrecchia F, Santolamazza P, Lucarelli F, Giommi P, Salotti L, L., Pacciani, V., Vittorini, M., Tavani, M. T., Fiocchi, S., Vercellone, F., D'Ammando, T., Sakamoto, E., Pian, C. M., Raiteri, M., Villata, M., Sasada, R., Itoh, M., Yamanaka, M., Uemura, E., Striani, D., Fugazza, A., Tiengo, H. A., Krimm, M. C., Stroh, A. D., Falcone, P. A., Curran, A. C., Sadun, A., Lahteenmaki, M., Tornikoski, H. D., Aller, M. F., Aller, C. S., Lin, V. M., Larionov, P., Leto, L. O., Takalo, A., Berdyugin, M. A., Gurwell, A., Bulgarelli, A. W., Chen, I., Donnarumma, A., Giuliani, Longo, Francesco, G., Pucella, A., Argan, G., Barbiellini, P., Caraveo, P. W., Cattaneo, E., Costa, G. D., Pari, E. D., Monte, G. D., Cocco, Y., Evangelista, A., Ferrari, M., Feroci, M., Fiorini, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, S., Sabatini, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, D., Zanello, S., Colafrancesco, C., Pittori, F., Verrecchia, P., Santolamazza, F., Lucarelli, P., Giommi, and L., Salotti

Subjects
Agile, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, galaxies: active, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, gamma-ray source, High Energy Gamma-ray Astronomy, AGILE satellite, Active Galactic Nuclei, Spectral line, blazar, law.invention, Accretion disc, multi wavelength observation, law, quasars: general, Blazar, media_common, Physics, galaxies: individual (3C 454.3), Gamma ray, Astronomy and Astrophysics, radiation mechanisms: non-thermal, Wavelength, Space and Planetary Science, Sky, Flare
Abstract

During the month of 2009 December, the blazar 3C 454.3 became the brightest gamma-ray source in the sky, reaching a peak flux F 2000 × 10 -8 photons cm-2 s-1 for E > 100 MeV. Starting in 2009 November intensive multifrequency campaigns monitored the 3C 454 gamma-ray outburst. Here, we report on the results of a two-month campaign involving AGILE, INTEGRAL, Swift/XRT, Swift/BAT, and Rossi XTE for the high-energy observations and Swift/UVOT, KANATA, Goddard Robotic Telescope, and REM for the near-IR/optical/UV data. GASP/WEBT provided radio and additional optical data. We detected a long-term active emission phase lasting 1 month at all wavelengths: in the gamma-ray band, peak emission was reached on 2009 December 2-3. Remarkably, this gamma-ray super-flare was not accompanied by correspondingly intense emission in the optical/UV band that reached a level substantially lower than the previous observations in 2007-2008. The lack of strong simultaneous optical brightening during the super-flare and the determination of the broadband spectral evolution severely constrain the theoretical modeling. We find that the pre- and post-flare broadband behavior can be explained by a one-zone model involving synchrotron self-Compton plus external Compton emission from an accretion disk and a broad-line region. However, the spectra of the 2009 December 2-3 super-flare and of the secondary peak emission on 2009 December 9 cannot be satisfactorily modeled by a simple one-zone model. An additional particle component is most likely active during these states. © 2010. The American Astronomical Society. All rights reserved.

Published
2010
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2. CRAB NEBULA: FIVE-YEAR OBSERVATION WITH ARGO-YBJ

Author

X. C. Yang, B. Bartoli, R. Cardarelli, X. Y. Zhang, G. Marsella, B. D'Ettorre Piazzoli, Minghui Liu, Zhenyong Feng, H. H. He, C. Y. Wu, L. Xue, Q. B. Gou, Q. Y. Yang, M. Iacovacci, M. Zha, G. Zizzi, P. Salvini, L. Perrone, X. D. Sheng, Paolo Bernardini, J. W. Zhao, H. R. Wu, Piero Vallania, P. Creti, H. Y. Jia, Paolo Camarri, I. De Mitri, Zihuang Cao, L. Zhang, T. L. Chen, Haifeng Li, Cunfeng Feng, M. Panareo, S. M. Mari, B. Z. Dai, Pengnian Shen, Lanqing Ma, Z. G. Yao, F. Ruggieri, Danzengluobu, S. Catalanotti, Hongbo Hu, A. Surdo, Yicheng Guo, A. Budano, Y. H. Tan, S. W. Cui, R. Santonico, X. J. Bi, Fudong Shi, Chang-Chun Ning, X. H. Ma, H. Lu, P. Branchini, Zhaoyang Feng, G. Liguori, S. Z. Chen, S. Mastroianni, G. Mancarella, Paolo Montini, F. R. Zhu, R. Iuppa, C. X. Liu, S. Vernetto, G. Di Sciascio, E. Striani, Q. Q. Zhu, H. W. Wang, A. D'Amone, J. K. K. Liu, Zhaxiciren, Labaciren, A. F. Yuan, P. Pistilli, H. M. Zhang, X. X. Zhou, Haibing Hu, Y. Zhang, D. Martello, Carlo Vigorito, T. Di Girolamo, Zhaxisangzhu, ITA, Bartoli, B., Bernardini, P., Bi, X. J., Branchini, P., Budano, A., Camarri, P., Cao, Z., Cardarelli, R., Catalanotti, S., Chen, S. Z., Chen, T. L., Creti, P., Cui, S. W., Dai, B. Z., D'Amone, A., Danzengluobu, De Mitri, I., D'Ettorre Piazzoli, B., Di Girolamo, T., Di Sciascio, G., Feng, C. F., Feng, Zhaoyang, Feng, Zhenyong, Gou, Q. B., Guo, Y. Q., He, H. H., Hu, Haibing, Hu, Hongbo, Iacovacci, M., Iuppa, R., Jia, H. Y., Labaciren, Li, H. J., Liguori, G., Liu, C., Liu, J., Liu, M. Y., Lu, H., Ma, L. L., Ma, X. H., Mancarella, G., Mari, S. M., Marsella, G., Martello, D., Mastroianni, S., Montini, P., Ning, C. C., Panareo, M., Perrone, L., Pistilli, P., Ruggieri, F., Salvini, P., Santonico, R., Shen, P. R., Sheng, X. D., Shi, F., Surdo, A., Tan, Y. H., Vallania, P., Vernetto, S., Vigorito, C., Wang, H., Wu, C. Y., Wu, H. R., Xue, L., Yang, Q. Y., Yang, X. C., Yao, Z. G., Yuan, A. F., Zha, M., Zhang, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhao, J., Zhaxisangzhu, Zhaxiciren, Zhou, X. X., Zhu, F. R., Zhu, Q. Q., Zizzi, G., Striani, E., B., Bartoli, Bernardini, Paolo, X. J., Bi, P., Branchini, A., Budano, P., Camarri, Z., Cao, R., Cardarelli, S., Catalanotti, S. Z., Chen, T. L., Chen, P., Creti, S. W., Cui, B. Z., Dai, D'Amone, Antonio, DE MITRI, Ivan, B., D'Ettorre Piazzoli, T., Di Girolamo, G., Di Sciascio, C. F., Feng, Zhaoyang, Feng, Zhenyong, Feng, Q. B., Gou, Y. Q., Guo, H. H., He, Haibing, Hu, Hongbo, Hu, M., Iacovacci, R., Iuppa, H. Y., Jia, H. J., Li, G., Liguori, C., Liu, J., Liu, M. Y., Liu, H., Lu, L. L., Ma, X. H., Ma, Mancarella, Giovanni, S. M., Mari, Marsella, Giovanni, Martello, Daniele, S., Mastroianni, P., Montini, C. C., Ning, Panareo, Marco, Perrone, Lorenzo, P., Pistilli, F., Ruggieri, P., Salvini, R., Santonico, P. R., Shen, X. D., Sheng, F., Shi, A., Surdo, Y. H., Tan, P., Vallania, S., Vernetto, C., Vigorito, H., Wang, C. Y., Wu, H. R., Wu, L., Xue, Q. Y., Yang, X. C., Yang, Z. G., Yao, A. F., Yuan, M., Zha, H. M., Zhang, L., Zhang, X. Y., Zhang, Y., Zhang, J., Zhao, Zhaxiciren, Zhaxisangzhu, X. X., Zhou, F. R., Zhu, Q. Q., Zhu, G., Zizzi, E., Striani, Bartoli, Bruno, Catalanotti, Sergio, Danzengluobu, Null, D'ETTORRE PIAZZOLI, Benedetto, DI GIROLAMO, Tristano, Iacovacci, Michele, Labaciren, Null, Zhaxiciren, Null, and Zhaxisangzhu, Null

Subjects
Physics, Spectral index, Astrophysics::High Energy Astrophysical Phenomena, Settore FIS/01 - Fisica Sperimentale, individual (Crab Nebula) [pulsars], Flux, Astronomy and Astrophysics, Astrophysics, Light curve, Power law, star [gamma rays], Air shower, Crab Nebula, Pulsar, Space and Planetary Science, Cutoff, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The ARGO-YBJ air shower detector monitored the Crab Nebula gamma ray emission from 2007 November to 2013 February. The integrated signal, consisting of $\sim$3.3 $\times$ 10$^5$ events,reached the statistical significance of 21.1 standard deviations. The obtained energy spectrum in the energy range 0.3-20 TeV can be described by a power law function dN/dE = I$_0$ (E / 2 TeV)$^{-\alpha}$, with a flux normalization I$_0$ = (5.2 $\pm$ 0.2) $\times$ 10$^{-12}$ photons cm$^{-2}$ s$^{-1}$ TeV$^{-1}$ and $\alpha$ = 2.63 $\pm$ 0.05, corresponding to an integrated flux above 1 TeV of 1.97 $\times$ 10$^{-11}$ photons cm$^{-2}$ s$^{-1}$. The systematic error is estimated to be less than 30$\%$ for the flux normalization and 0.06 for the spectral index. Assuming a power law spectrum with an exponential cutoff dN/dE = I$_0$ (E / 2 TeV)$^{-\alpha}$ $\exp$ (-E / E$_{cut}$), the lower limit of the cutoff energy E$_{cut}$ is 12 TeV, at 90$\%$ confidence level. Our extended dataset allows the study of the TeV emission over long timescales. Over five years, the light curve of the Crab Nebula in 200-day bins is compatible with a steady emission with a probability of 7.3 $\times$ 10$^{-2}$. A correlated analysis with Fermi-LAT data over $\sim$4.5 years using the light curves of the two experiments gives a Pearson correlation coefficient $r$ = 0.56 $\pm$ 0.22. Concerning flux variations on timescales of days, a "blind" search for flares with a duration of 1-15 days gives no excess with a significance higher than four standard deviations. The average rate measured by ARGO-YBJ during the three most powerful flares detected by Fermi-LAT is 205 $\pm$ 91 photons day$^{-1}$, consistent with the average value of 137 $\pm$ 10 day$^{-1}$., Comment: 12 pages, 10 figures

Published
2015
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3. THE CRAB NEBULA SUPER-FLARE IN 2011 APRIL: EXTREMELY FAST PARTICLE ACCELERATION AND GAMMA-RAY EMISSION

Author

A. Pellizzoni, M. Galli, Allyn F. Tennant, A. Giuliani, F. Verrecchia, Francesco Lazzarotto, C. Pittori, G. Piano, G. De Paris, A. Argan, Sandro Mereghetti, A. Morselli, Martin C. Weisskopf, Arnaud Ferrari, E. Striani, P. Santolamazza, Andrea Bulgarelli, F. Fuschino, I. Lapshov, I. Donnarumma, Y. Evangelista, Massimo Rapisarda, G. Di Cocco, Enrico Costa, S. Sabatini, P. W. Cattaneo, G. Pucella, P. Picozza, Marco Tavani, G. Barbiellini, Martino Marisaldi, A. Rappoldi, F. Perotti, V. Vittorini, A. W. Chen, Claudio Labanti, P. Giommi, M. Cardillo, P. A. Caraveo, M. Trifoglio, E. Del Monte, F. Longo, Marco Feroci, Luigi Pacciani, Fabrizio Lucarelli, Maura Pilia, Alessio Trois, Fulvio Gianotti, Paolo Soffitta, S. Vercellone, E., Striani, M., Tavani, G., Piano, I., Donnarumma, G., Pucella, V., Vittorini, A., Bulgarelli, A., Troi, C., Pittori, F., Verrecchia, E., Costa, M., Weisskopf, A., Tennant, A., Argan, G., Barbiellini, P., Caraveo, M., Cardillo, P. W., Cattaneo, A. W., Chen, Paris, G., Monte, E., Cocco, G., Y., Evangelista, A., Ferrari, M., Feroci, F., Fuschino, M., Galli, F., Gianotti, A., Giuliani, C., Labanti, I., Lapshov, F., Lazzarotto, Longo, Francesco, M., Marisaldi, S., Mereghetti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, P., Picozza, M., Pilia, M., Rapisarda, A., Rappoldi, S., Sabatini, P., Soffitta, M., Trifoglio, S., Vercellone, F., Lucarelli, P., Santolamazza, and P., Giommi

Subjects
individual: Crab Nebula [pulsars], Astrophysics::High Energy Astrophysical Phenomena, acceleration of particles, gamma rays: stars, pulsars: individual: Crab Nebula, FOS: Physical sciences, Flux, Astrophysics, star [gamma rays], Spectral line, law.invention, law, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, acceleration of particle, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gamma ray, Astronomy and Astrophysics, Particle acceleration, Crab Nebula, Space and Planetary Science, Magnetohydrodynamics, Astrophysics - High Energy Astrophysical Phenomena, Flare
Abstract

We report on the extremely intense and fast gamma-ray are above 100 MeV detected by AGILE from the Crab Nebula in mid-April 2011. This event is the fourth of a sequence of reported major gamma-ray flares produced by the Crab Nebula in the period 2007/mid-2011. These events are attributed to strong radiative and plasma instabilities in the inner Crab Nebula, and their properties are crucial for theoretical studies of fast and efficient particle acceleration up to 10^15 eV. Here we study the very rapid flux and spectral evolution of the event that reached on April 16, 2011 the record-high peak flux of F = (26 +/- 5) x 10^-6 ph cm^-2 s^-1 with a risetime timescale that we determine to be in the range 6-10 hrs. The peak flaring gamma-ray spectrum reaches a distinct maximum near 500 MeV with no substantial emission above 1 GeV. The very rapid risetime and overall evolution of the Crab Nebula are strongly constrain the acceleration mechanisms and challenge MHD models. We briefly discuss the theoretical implications of our observations., Comment: 4 pages, 2 figures. Accepted for pubblication in ApJL

Published
2011
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4. THE BLOB CRASHES INTO THE MIRROR: MODELING THE EXCEPTIONAL γ-RAY FLARING ACTIVITY OF 3C 454.3 IN 2010 NOVEMBER

Author

E. Striani, A. Cavaliere, Marco Tavani, V. Vittorini, and S. Vercellone

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Compton scattering, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Galaxy, law.invention, Black hole, Space and Planetary Science, law, Blazar, Line (formation), Flare
Abstract

3C 454.3 is a prominent flat-spectrum radio quasar that in recent years attracted considerable attention because of its variable high-energy emissions. In this paper, we focus on the exceptional flaring activity of 3C 454.3 that was detected by AGILE and by Fermi-LAT in 2010 November. In the light of the time-varying data ranging from the radio, optical, and X-ray up to GeV γ-ray bands, we discuss a theoretical framework addressing all data in their overall evolution. For two weeks, the source has shown a plateau of enhanced GeV emission preceding a sudden major flare lasting about three days before decaying. The γ-ray flare onset is abrupt (about six hours), and is characterized by a prominent "Compton dominance" with the GeV flux exceeding the pre-flare values by a factor of four to five. During this episode, the optical and X-ray fluxes increased by a factor of around two. Within the standard framework of a jet launched with a Lorentz bulk factor Γ ~ 10 from a central black hole, we explore the yields of two alternatives. Case 1, with high-energy emission originating within the broad line region (BLR); and Case 2, with most of it produced outside at larger distances of a few parsecs. We show that Case 1 has considerable problems in explaining the whole set of multifrequency data. Case 2, instead, leads to a consistent and interesting interpretation based on the enhanced inverse Compton radiation that is produced as the jet crashes onto a mirror cloud positioned at parsec scales. This model explains the γ-ray versus optical/X-ray behavior of 3C 454.3, including the otherwise puzzling phenomena such as the prominent "orphan" optical flare, and the enhanced line emission with no appreciable γ-ray counterpart that preceded the GeV γ-ray flare. It also accounts for the delayed onset of the latter on top of the long plateau. Our modeling of the exceptional 3C 454.3 γ-ray flare shows that while emission inside the canonical BLR is problematic, major and rapid variations can be produced at parsec scales with moderate bulk Lorentz factors Γ ≈ 15. Our "crashed mirror" model is also applicable to other blazar flares marked by large Compton dominance of the emitted radiation such as the flare of PKS 1830–211 in 2010 October.

Published
2014
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5. SPECTRAL EVOLUTION OF THE 2010 SEPTEMBER GAMMA-RAY FLARE FROM THE CRAB NEBULA

Author

Sandro Mereghetti, Arnaud Ferrari, Luigi Pacciani, S. Colafrancesco, I. Donnarumma, Y. Evangelista, G. Pucella, Marco Tavani, M. Pilia, Francesco Lazzarotto, G. Barbiellini, Andrea Bulgarelli, E. Del Monte, E. Striani, A. Pellizzoni, A. Giuliani, Alessio Trois, P. A. Caraveo, C. Pittori, V. Vittorini, and P. W. Cattaneo

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy and Astrophysics, Astrophysics, Synchrotron, Spectral line, law.invention, Particle acceleration, Acceleration, Crab Nebula, Pulsar, Space and Planetary Science, law, Physics::Accelerator Physics, Flare
Abstract

Strong gamma-ray flares from the Crab Nebula have been recently discovered by AGILE and confirmed by Fermi-LAT. We study here the spectral evolution in the gamma-ray energy range above 50 MeV of the 2010 September flare that was simultaneously detected by AGILE and Fermi-LAT. We revisit the AGILE spectral data and present an emission model based on rapid (within 1 day) acceleration followed by synchrotron cooling. We show that this model successfully explains both the published AGILE and Fermi-LAT spectral data showing a rapid rise and a decay within 2 and 3 days. Our analysis constrains the acceleration timescale and mechanism, the properties of the particle distribution function, and the local magnetic field. The combination of very rapid acceleration, emission well above 100 MeV, and the spectral evolution consistent with synchrotron cooling contradicts the idealized scenario predicting an exponential cutoff at photon energies above 100 MeV. We also consider a variation of our model based on even shorter acceleration and decay timescales, which can be consistent with the published averaged properties.

Published
2011
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6. ERRATUM: 'THE FIRST FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS' (2010, ApJS, 187, 460)

Author

Na Wang, James Chiang, Roger Blandford, B. Lott, Cristobal M. Espinoza, Jun Kataoka, Ö. Çelik, V. M. Kaspi, A. S. Johnson, S. Cutini, F. Piron, Jean Ballet, Gudlaugur Johannesson, Sinéad McGlynn, I. A. Grenier, M. Hayashida, M. Roth, A. De Luca, C. Favuzzi, Stefano Ciprini, Felix Ryde, Lucas Guillemot, B. Giebels, A. Tramacere, A. Noutsos, Stefan Funk, Guido Barbiellini, H. Tajima, Nicola Omodei, S. Murgia, V. Vasileiou, Richard Dubois, Luca Baldini, T. Mizuno, M. Marelli, M. Frailis, P. Spinelli, Scott M. Ransom, Seth Digel, M. S. Jackson, F. de Palma, Matthew G. Baring, Alice K. Harding, Fernando Camilo, Benjamin Stappers, C. Farnier, Elliott D. Bloom, B. M. Baughman, L. Tibaldo, L. R. Cominsky, Igor V. Moskalenko, T. A. Porter, Jürgen Knödlseder, Brian L Winer, Sylvain Guiriec, Gloria Spandre, S. Rainò, Eric V. Gotthelf, S. Germani, Mn Mazziotta, Olaf Reimer, A. A. Moiseev, Christo Venter, A. van Etten, Francesco Longo, P. Fusco, W. B. Atwood, Diego F. Torres, Omar Tibolla, Paul J. Wang, Andrew W. Strong, Denise A. Smith, A. Sellerholm, Roger W. Romani, Grzegorz Madejski, Nicola Giglietto, Hartmut Sadrozinski, Robert R. Rando, M. Kramer, David Sánchez, Dario Gasparrini, F. Gargano, Ronaldo Bellazzini, Gilles Theureau, Hideaki Katagiri, Luca Latronico, A. Sander, C. Meurer, T. J. Johnson, Y. Hanabata, M. N. Lovellette, F. Loparco, Paolo Giommi, Carmelo Sgrò, Denis Bastieri, P. D. Smith, Persis S. Drell, Alessandro Brez, E. Do Couto E Silva, Aous A. Abdo, T. L. Schalk, E. Nuss, W. N. Johnson, G. A. Caliandro, Paul S. Ray, C. Gwon, Elizabeth C. Ferrara, Gottfried Kanbach, David Paneque, M. Kuss, A. Y. Rodriguez, Randall P. Johnson, P. Weltevrede, Robin H. D. Corbet, D. Parent, J. E. Grove, Yasushi Fukazawa, P. Caraveo, Karen Watters, E. Hays, Jan Conrad, Pascal Bruel, Ismaël Cognard, Y. Uchiyama, Johann Cohen-Tanugi, P. M. Saz Parkinson, M. Dormody, Nanda Rea, Melissa Pesce-Rollins, M. S. Strickman, Andrew Lyne, A. P. Waite, T. Kamae, Peter F. Michelson, Richard N. Manchester, M. Lemoine-Goumard, G.L. Godfrey, Charles D. Dermer, A. Makeev, K. S. Wood, J. G. Thayer, Matthew Kerr, Tadayuki Takahashi, W. Mitthumsiri, R. Claus, S. J. Fegan, M. E. Monzani, J. B. Thayer, P. R. den Hartog, Jean-Luc Starck, J. P. Norris, W. B. Focke, A. Morselli, V. Vitale, A. Chekhtman, J. Bregeon, A. Reimer, Keith Bechtol, Marco Ajello, S. Buson, J. Lande, M. Razzano, A. De Angelis, M. Brigida, T. L. Usher, M.-H. Grondin, R. E. Hughes, Stephen E. Thorsett, E. Charles, M. Ozaki, J. F. Ormes, Emanuele Bonamente, D. J. Thompson, Francesco Giordano, Hiromitsu Takahashi, D. Dumora, P. L. Nolan, N. Gehrels, Takaaki Tanaka, T. Mineo, Claudia Cecchi, T. Glanzman, E. Orlando, V. Pelassa, T. Ylinen, R. A. Cameron, Julie McEnery, Steven Ritz, D. J. Suson, T. H. Burnett, B. Berenji, Gianluca Giavitto, M. Ziegler, Takeshi Nakamori, J. M. Casandjian, E. J. Siskind, T. Ohsugi, C. C. Cheung, Magnus Axelsson, Paulo C. C. Freire, W. Mcconville, N. Vilchez, E. Striani, P. Fortin, G. Tosti, Markus Ackermann, P. Lubrano, Simon Johnston, M. Pepe, Margaret A. Livingstone, Jeffrey D. Scargle, N. Kawai, M. L. Kocian, C. Monte, T. Reposeur, A. W. Borgland, and J. H. Panetta

Subjects
Physics, 010308 nuclear & particles physics, Gamma ray, Astronomy, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, law.invention, Telescope, Pulsar, Space and Planetary Science, law, 0103 physical sciences, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Published
2011
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7. Magic Constraints on γ-ray Emission from Cygnus X-3

Author

Aleksic, J, Antonelli, La, Antoranz, P, Backes, M, Baixeras, C, Barrio, Ja, Bastieri, Denis, Gonzalez, Jb, Bednarek, W, Berdyugin, A, Berger, K, Bernardini, E, Biland, A, Blanch, O, Bock, Rk, Boller, A, Bonnoli, G, Bordas, P, Tridon, Db, BOSCH RAMON, V, Bose, D, Braun, I, Bretz, T, Britzger, D, Camara, M, Carmona, E, Carosi, A, Colin, P, Contreras, Jl, Cortina, J, Costado, Mt, Covino, S, Dazzi, F, DE ANGELIS, A, DEL POZO EDC, DE LOTTO, B, DE MARIA, M, DE SABATA, F, Mendez, Cd, Doert, M, Dominguez, A, Prester, Dd, Dorner, D, Doro, Michele, Elsaesser, D, Errando, M, Ferenc, D, Fonseca, Mv, Font, L, Lopez, Rjg, Garczarczyk, M, Gaug, M, Godinovic, N, Goebel, F, Hadasch, D, Herrero, A, Hildebrand, D, HOHNE MONCH, D, Hose, J, Hrupec, D, Hsu, Cc, Jogler, T, Klepser, S, Krahenbuhl, T, Kranich, D, LA BARBERA, A, Laille, A, Leonardo, E, Lindfors, E, Lombardi, S, Longo, F, Lopez, M, Lorenz, E, Majumdar, P, Maneva, G, Mankuzhiyil, N, Mannheim, K, Maraschi, L, Mariotti, Mose', Martinez, M, Mazin, D, Meucci, M, Miranda, Jm, Mirzoyan, R, Miyamoto, H, Moldon, J, Moles, M, Moralejo, A, Nieto, D, Nilsson, K, Ninkovic, J, Orito, R, Oya, I, Paiano, S, Paoletti, R, Paredes, Jm, Partini, S, Pasanen, M, Pascoli, Donatella, Pauss, F, Pegna, Rg, PEREZ TORRES MA, Persic, M, Peruzzo, L, Prada, F, Prandini, Elisa, Puchades, N, Puljak, I, Reichardt, I, Rhode, W, Ribo, M, Rico, J, Rissi, M, Rugamer, S, Saggion, Antonio, Saito, K, Saito, Ty, Salvati, M, SANCHEZ CONDE, M, Satalecka, K, Scalzotto, VILLI MARIO, Scapin, V, Schultz, C, Schweizer, T, Shayduk, M, Shore, Sn, SIERPOWSKA BARTOSIK, A, Sillanpaa, A, Sitarek, J, Sobczynska, D, Spanier, F, Spiro, S, Stamerra, A, Steinke, B, Struebig, Jc, Suric, T, Takalo, L, Tavecchio, F, Temnikov, P, Terzic, T, Tescaro, D, Teshima, M, Torres, Df, Vankov, H, Wagner, Rm, Weitzel, Q, Zabalza, V, Zandanel, F, Zanin, R, Bulgarelli, A, MAX MOERBECK, W, Piano, G, Pooley, G, Readhead, Acs, Richards, Jl, Sabatini, S, Striani, E, Tavani, M, Trushkin, S., J., Aleksic, L. A., Antonelli, P., Antoranz, M., Backe, C., Baixera, J. A., Barrio, D., Bastieri, J. B., Gonzalez, W., Bednarek, A., Berdyugin, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, G., Bonnoli, P., Borda, D. B., Tridon, V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, D., Britzger, M., Camara, E., Carmona, A., Carosi, P., Colin, J. L., Contrera, J., Cortina, M. T., Costado, S., Covino, F., Dazzi, A. D., Angeli, E. D. C., Del Pozo, B. D., Lotto, M. D., Maria, F. D., Sabata, C. D., Mendez, M., Doert, A., Dominguez, D. D., Prester, D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, M. V., Fonseca, L., Font, R. J. G., Lopez, M., Garczarczyk, M., Gaug, N., Godinovic, F., Goebel, D., Hadasch, A., Herrero, D., Hildebrand, D., Hohne Monch, J., Hose, D., Hrupec, C. C., Hsu, T., Jogler, S., Klepser, T., Krahenbuhl, D., Kranich, A. L., Barbera, A., Laille, E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Martinez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, M., Mole, A., Moralejo, D., Nieto, K., Nilsson, J., Ninkovic, R., Orito, I., Oya, S., Paiano, R., Paoletti, J. M., Parede, S., Partini, M., Pasanen, D., Pascoli, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, F., Prada, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, W., Rhode, M., Ribo, J., Rico, M., Rissi, S., Rugamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, M., Shayduk, S. N., Shore, A., Sierpowska Bartosik, A., Sillanpaa, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, B., Steinke, J. C., Struebig, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, T., Terzic, D., Tescaro, M., Teshima, D. F., Torre, H., Vankov, R. M., Wagner, Q., Weitzel, V., Zabalza, F., Zandanel, R., Zanin, A., Bulgarelli, W., Max Moerbeck, G., Piano, G., Pooley, A. C. S., Readhead, J. L., Richard, S., Sabatini, E., Striani, M., Tavani, and S., Trushkin

Subjects
Photon, HIGH-ENERGY EMISSION, MICROQUASAR GRS 1915+105, X-RAY, RELATIVISTIC JET, CYG X-3, RADIO OUTBURST, CRAB-NEBULA, BINARY, TELESCOPE, PULSAR, Astrophysics, 01 natural sciences, law.invention, Raigs gamma, law, Observacions astronòmiques, 010303 astronomy & astrophysics, Estels binaris de raigs X, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Very High Energy Gamma-ray Astronomy, MAGIC telescope, Black Holes, Gamma ray, X-ray binaries, Electrónica, Física nuclear, Radio frequency, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Astronomical observations, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Compact star, Radiation, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, Telescope, 0103 physical sciences, acceleration of particles, binaries: general, gamma rays: observations, X-rays: bina- ries — X-rays: individual (Cygnus X-3), Cherenkov radiation, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Gamma rays, Magic (programming), Astronomy, Astronomy and Astrophysics, Space and Planetary Science
Abstract

Cygnus X-3 is a microquasar consisting of an accreting compact object orbiting around a Wolf-Rayet star. It has been detected at radio frequencies and up to high-energy gamma rays (above 100 MeV). However, many models also predict a very high energy (VHE) emission (above hundreds of GeV) when the source displays relativistic persistent jets or transient ejections. Therefore, detecting such emission would improve the understanding of the jet physics. The imaging atmospheric Cherenkov telescope MAGIC observed Cygnus X-3 for about 70 hours between 2006 March and 2009 August in different X-ray/radio spectral states and also during a period of enhanced gamma-ray emission. MAGIC found no evidence for a VHE signal from the direction of the microquasar. An upper limit to the integral flux for energies higher than 250 GeV has been set to 2.2 x 10-12 photons cm-2 s-1 (95% confidence level). This is the best limit so far to the VHE emission from this source. The non-detection of a VHE signal during the period of activity in the high-energy band sheds light on the location of the possible VHE radiation favoring the emission from the innermost region of the jets, where absorption is significant. The current and future generations of Cherenkov telescopes may detect a signal under precise spectral conditions., 14 pages, 11 figures, This manuscript has been accepted by ApJ (2010)

Published
2010
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