期刊
ASTRONOMY & ASTROPHYSICS
卷 577, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201425401
关键词
galaxies: active; galaxies: Seyfert; X-rays: galaxies
资金
- NASA
- ESA Member States
- USA (NASA)
- French-Italian International Project of Scientific Collaboration: PICS-INAF project [181542]
- CNES
- Universite Franco-Italienne (Vinci Ph.D. fellowship)
- Italian Space Agency [ASI/INAF I/037/12/0-011/13]
- NASA [13184, NAS5-26555]
- US NSF [AST-1008882]
- E.U. Marie Curie Intra-European fellowship [FP-PEOPLE-2012-IEF- 331095]
- Fondo Fortalecimiento de la Productividad Cientifica VRIDT
- ISSI in Bern
- Netherlands Organization for Scientific Research
- UK STFC
- French CNES
- CNRS/PICS
- CNRS/PNHE
- Swiss SNSF
- Italian INAF/PICS
- German Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR) [FKZ 50 OR 1408]
- STFC [ST/K000977/1] Funding Source: UKRI
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1008882] Funding Source: National Science Foundation
We describe the analysis of the seven broad-band X-ray continuum observations of the archetypal Seyfert 1 galaxy NGC 5548 that were obtained with XMM-Newton or Chandra, simultaneously with high-energy (>10 keV) observations with NuSTAR and INTEGRAL. These data were obtained as part of a multiwavelength campaign undertaken from the summer of 2013 till early 2014. We find evidence of a high-energy cut-off in at least one observation, which we attribute to thermal Comptonization, and a constant reflected component that is likely due to neutral material at least a few light months away from the continuum source. We confirm the presence of strong, partial covering X-ray absorption as the explanation for the sharp decrease in flux through the soft X-ray band. The obscurers appear to be variable in column density and covering fraction on time scales as short as weeks. A fit of the average spectrum over the range 0.3-400 keV with a realistic Comptonization model indicates the presence of a hot corona with a temperature of 40(-10)(+40) keV and an optical depth of 2.7(-1.2)(+0.7) if a spherical geometry is assumed.
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