Radio-to-γ-ray monitoring of the narrow-line Seyfert 1 galaxy PMN J0948+0022 from 2008 to 2011

被引:46
作者
Foschini, L. [1 ]
Angelakis, E. [2 ]
Fuhrmann, L. [2 ]
Ghisellini, G. [1 ]
Hovatta, T. [3 ]
Lahteenmaki, A. [4 ]
Lister, M. L. [5 ]
Braito, V. [1 ]
Gallo, L. [6 ]
Hamilton, T. S. [7 ]
Kino, M. [8 ]
Komossa, S. [2 ]
Pushkarev, A. B. [2 ,9 ,10 ]
Thompson, D. J. [11 ]
Tibolla, O. [12 ]
Tramacere, A. [13 ]
Carraminana, A. [14 ]
Carrasco, L. [14 ]
Falcone, A. [15 ]
Giroletti, M. [16 ]
Grupe, D. [15 ]
Kovalev, Y. Y. [2 ,17 ]
Krichbaum, T. P. [2 ]
Max-Moerbeck, W. [3 ]
Nestoras, I. [2 ]
Pearson, T. J. [3 ]
Porras, A. [14 ]
Readhead, A. C. S. [3 ]
Recillas, E. [14 ]
Richards, J. L. [5 ]
Riquelme, D. [18 ]
Sievers, A. [18 ]
Tammi, J. [4 ]
Tornikoski, M. [4 ]
Ungerechts, H. [18 ]
Zensus, J. A. [2 ]
Celotti, A. [1 ,19 ]
Bonnoli, G. [1 ]
Doi, A. [20 ]
Maraschi, L. [1 ]
Tagliaferri, G. [1 ]
Tavecchio, F. [1 ]
机构
[1] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy
[2] Max Planck Inst Radioastron, D-53121 Bonn, Germany
[3] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA
[4] Aalto Univ, Metsahovi Radio Observ, Kylmala, Finland
[5] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA
[6] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada
[7] Shawnee State Univ, Dept Nat Sci, Portsmouth, OH 45662 USA
[8] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan
[9] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine
[10] Pulkovo Observ, St Petersburg 196140, Russia
[11] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
[12] Univ Wurzburg, ITPA, D-97074 Wurzburg, Germany
[13] ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland
[14] Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico
[15] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA
[16] Ist Radioastron, INAF, I-40129 Bologna, Italy
[17] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia
[18] Inst Radioastron Milimetr IRAM, Granada 18012, Spain
[19] SISSA, I-34136 Trieste, Italy
[20] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan
基金
日本学术振兴会; 美国国家航空航天局; 美国国家科学基金会; 芬兰科学院; 俄罗斯基础研究基金会;
关键词
galaxies: jets; galaxies: Seyfert; gamma rays: galaxies; galaxies: individual: PMN J0948+0022; LARGE-AREA TELESCOPE; INVERSE-COMPTON CATASTROPHE; ACTIVE GALACTIC NUCLEI; MULTIWAVELENGTH OBSERVATIONS; BRIGHTNESS TEMPERATURE; RELATIVISTIC JET; LOUD; VARIABILITY; QUASAR; FLUX;
D O I
10.1051/0004-6361/201220225
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present more than three years of observations at different frequencies, from radio to high-energy gamma-rays, of the Narrow-Line Seyfert 1 (NLS1) Galaxy PMN J0948+0022 (z = 0.585). This source is the first NLS1 detected at energies above 100 MeV and therefore can be considered the prototype of this emerging new class of gamma-ray emitting active galactic nuclei (AGN). The observations performed from 2008 August 1 to 2011 December 31 confirmed that PMN J0948+0022 generates a powerful relativistic jet, which is able to develop an isotropic luminosity at gamma-rays of the order of 10(48) erg s(-1), at the level of powerful quasars. The evolution of the radiation emission of this source in 2009 and 2010 followed the canonical expectations of relativistic jets with correlated multiwave-length variability (gamma-rays followed by radio emission after a few months), but it was difficult to retrieve a similar pattern in the light curves of 2011. The comparison of gamma-ray spectra before and including 2011 data suggested that there was a softening of the high-energy spectral slope. We selected five specific epochs to be studied by modelling the broad-band spectrum, which are characterised by an outburst at gamma-rays or very low/high flux at other wavelengths. The observed variability can largely be explained by changes in the injected power, the bulk Lorentz factor of the jet, or the electron spectrum. The characteristic time scale of doubling/halving flux ranges from a few days to a few months, depending on the frequency and the sampling rate. The shortest doubling time scale at gamma-rays is 2.3 +/- 0.5 days. These small values underline the need of highly sampled multiwavelength campaigns to better understand the physics of these sources.
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页数:14
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