RT Journal Article
T1 Spectral energy distribution of Markarian 501: quiescent state versus extreme outburst
A1 Antoranz Canales, Pedro
A1 Barrio Uña, Juan Abel
A1 Contreras González, José Luis
A1 Fonseca González, Mª Victoria
A1 Miranda Pantoja, José Miguel
A1 Nieto, Daniel
AB The very high energy (VHE; E > 100 GeV) blazar Markarian 501 (Mrk 501) has a well-studied history of extreme spectral variability and is an excellent laboratory for studying the physical processes within the jets of active galactic nuclei. However, there are few detailed multiwavelength studies of Mrk 501 during its quiescent state, due to its low luminosity. A short-term multiwavelength study of Mrk 501 was coordinated in 2009 March, focusing around a multi-day observation with the Suzaku X-ray satellite and including gamma-ray data from VERITAS, MAGIC, and the Fermi Gamma-ray Space Telescope with the goal of providing a well-sampled multiwavelength baseline measurement of Mrk 501 in the quiescent state. The results of these quiescent-state observations are compared to the historically extreme outburst of 1997 April 16, with the goal of examining variability of the spectral energy distribution (SED) between the two states. The derived broadband SED shows the characteristic double-peaked profile. We find that the X-ray peak shifts by over two orders of magnitude in photon energy between the two flux states while the VHE peak varies little. The limited shift in the VHE peak can be explained by the transition to the Klein-Nishina (KN) regime. Synchrotron self-Compton models are matched to the data and the implied KN effects are explored.
PB IOP Publishing
SN 0004-637X
YR 2011
FD 2011-02-01
LK https://hdl.handle.net/20.500.14352/43897
UL https://hdl.handle.net/20.500.14352/43897
LA eng
NO Abdo, A. A., et al. 2010, ApJS, 188, 405.Abdo, A. A., et al. 2011, ApJ, 727, 129.Acciari, V. A., et al. (VERITAS Collaboration) 2008, ApJ, 679, 1427.Aharonian, F. A. 2000, New Astron., 5, 377.Aharonian, F. A., et al. 2001, A&A, 366, 62.Albert, J., et al. (MAGIC Collaboration) 2007a, ApJ, 669, 862.Albert, J., et al. (MAGIC Collaboration) 2007b, Nucl. Instrum. Methods, A583, 494.Albert, J., et al. (MAGIC Collaboration) 2008a, ApJ, 674, 1037.Albert, J., et al. (MAGIC Collaboration) 2008b, Nucl. Instrum. Methods, A588, 424.Aliu, E., et al. (MAGIC Collaboration) 2009, Astropart. Phys., 30, 293.Anderhub, H., et al. (MAGIC Collaboration) 2009, ApJ, 705, 1624.Arnaud, K. A. 1996, in ASP Conf. Ser. 101, Astronomical Data Analysis Software and Systems V, ed. G. Jacoby, J. Barnes (San Francisco, CA: ASP), 17.Atwood, W. B., et al. 2009, ApJ, 697, 1071.Berge, D., Funk, S., Hinton, J. 2007, A&A, 466, 1219.Boldt, E. 1987, in IAU Symp. 124, Observational Cosmology (Dordrecht: Reidel), 611B.Böttcher, M., Mause, H., Schlickeiser, R. 1997, A&A, 324, 395.Catanese, M., et al. 1997, ApJ, 487, L143.Cogan, P., et al. 2007, Proc. 30th ICRC (Merida), 3, 1385.Daum, A., et al. (HEGRA Collaboration) 1997, Astropart. Phys., 8, 1.Dermer, C. D., Schlickeiser, R., Mastichiadis, A. 1992, A&A, 256, L27.Djannati-Ataï, A., et al. 1999, A&A, 350, 17.Fomin,V. P., Stepanian,A. A., Lamb, R. C., Lewis, D. A., Punch, M.,&Weekes, T. C. 1994, Astropart. Phys., 2, 137.Franceschini, A., Rodighiero, G., & Vaccari, M. 2008, A&A, 487, 837.Hillas, A. M. 1985, Proc. 19th ICRC (La Jolla), 3, 445 (available at: http://catalog.hathitrust.org/Record/006239301).Holder, J., et al. (VERITAS Collaboration) 2008, in AIP Conf. Proc. 1085, High Energy Gamma-Ray Astronomy, ed. F. A. Aharonian,W. Hofmann, F. Rieger (Melville, NY: AIP), 657.Huang, D., et al. (VERITAS Collaboration) 2009, in 2009 Fermi Symp., ed. W. N. Johnson & D. J. Thompson, eConf C0911022 (arXiv:0912.3772).Koyama, K., et al. 2007, PASJ, 59, S23.Krawczynski, H., et al. 2004, ApJ, 601, 151.Li, T., Ma, Y. 1983, ApJ, 272, 317.Maeda, Y., et al. 2008, JX-ISAS-SUZAKU-MEMO-2008-06, ftp://legacy.gsfc.nasa.gov/suzaku/doc/xrt/suzakumemo-2008-06.pdf.Mannheim, K. 1993, A&A, 269, 67.Maraschi, L., Ghisellini, G., Celotti, A. 1992, ApJ, 397, L5.Marscher, A. P., Gear, W. K. 1985, ApJ, 298, 114.Mattox, J. R., et al. 1996, ApJ, 461, 396.Petry, D., et al. 2000, ApJ, 536, 742.Pian, E., et al. 1998, ApJ, 492, L17.Pichel, A., et al. (VERITAS Collaboration) 2009, Proc. 31st ICRC (Lodz), arXiv:0908.0010.Pohl, M., Schlickeiser, R. 2000, A&A, 354, 395.Quinn, J., et al. 1996, ApJ, 456, L83.Rybicki, G. B., Lightman, A. P. 1979, Radiative Processes in Astrophysics (New York: Wiley).Sambruna, R. M., et al. 2000, ApJ, 538, 127.Serlemitsos, P. J., et al. 2007, PASJ, 59, 9.Sikora, M., Begelman, M. C., Rees, M. J. 1994, ApJ, 421, 153.Stark, A. A., Gammie, C. F., Wilson, R. W., Bally, J., Linke, R. A., Heiles, C., Hurwitz, M. 1992, ApJS, 79, 77.Takahashi, T., et al. 2007, PASJ, 59, 35.Tavecchio, F., Maraschi, L., Ghisellini, G. 1998, ApJ, 509, 608.Urry, C. M., Padovani, P. 1995, PASP, 107, 803.Xue, Y., Cui, W. 2005, ApJ, 622, 160.
NO © The American Astronomical Society. Supported by INFN Padova.We thank Elena Pian for providing the BeppoSAX data. This work was supported in part by NASA through grants NNX08AZ98G and NNX08AX53G. This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and USA (NASA). The VERITAS research is supported by grants from the U.S. Department of Energy, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and the collaborating institutions in the construction and operation of the instrument.The MAGIC Collaboration thanks the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the Marie Curie program, by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 program, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the YIP of the Helmholtz Gemeinschaft, by the DFG Cluster of Excellence "Origin and Structure of the Universe," and by the Polish MNiSzW Grant N N203 390834.
NO INFN Padova
NO German BMBF
NO German MPG
NO Italian INFN
NO Swiss National Fund SNF
NO Spanish MICINN
NO NASA
NO U.S. Department of Energy
NO U.S. National Science Foundation
NO Smithsonian Institution
NO NSERC in Canada
NO Science Foundation Ireland
NO STFC in the UK
DS Docta Complutense
RD 7 may 2024