VARIABLE PARTIAL COVERING AND A RELATIVISTIC IRON LINE IN NGC 1365

Journal Article · Fri May 01 04:00:00 EDT 2009 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/696/1/160; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21296209

Risaliti, G; Elvis, M; Fabbiano, G; Baldi, A; Zezas, A ^[1]; Miniutti, G ^[2]; Salvati, M ^[3]; Braito, V ^[4]; Bianchi, S; Matt, G ^[5]; Reeves, J ^[6]

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1. Harvard-Smithsonian Center for Astrophysics, 60 Garden St. Cambridge, MA 02138 (United States)
2. Laboratoire Astroparticule et Cosmologie (APC), UMR 7164, 10 Rue A. Domon et L. Duquet, 75205 Paris (France)
3. INAF-Osservatorio di Arcetri, Largo E. Fermi 5, I-50125 Firenze (Italy)
4. Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom)
5. Dipartimento di Fisica, Universita degli Studi 'Roma Tre', Via della Vasca Navale 84, I-00146 Roma (Italy)
6. Astrophysics Group, School of Physical and Geographical Science, Keele University, Keele, Staffordshire ST5 5BG (United Kingdom)

We present a complete analysis of the hard X-ray (2-10 keV) properties of the Seyfert galaxy NGC 1365, based on a 60 ks XMM-Newton observation performed in 2004 January. The two main results are as follows. (1) We detect an obscuring cloud with N{sub H} {approx} 3.5 x 10{sup 23} cm{sup -2} crossing the line of sight in {approx}25 ks. This implies a dimension of the X-ray source not larger than a few 10{sup 13} cm and a distance of the obscuring cloud of the order of 10{sup 16} cm. Adopting the black hole mass M {sub BH} estimated from the M {sub BH}-velocity dispersion relation, the source size is D {sub S} < 20R{sub G} and the distance and density of the obscuring clouds are R {approx} 3000-10, 000R{sub G} and n {approx} 10{sup 10} cm{sup -3}, i.e., typical values for broad-line region clouds. (2) An iron emission line with a relativistic profile is detected with high statistical significance. A time-integrated fit of the line+continuum reflection components suggests a high iron abundance (approximately three times solar) and an origin of these components in the inner part (within {approx}10R{sub G} ) of the accretion disk, in agreement with the small source size inferred from the analysis of the absorption variability.

• OSTI ID: 21296209
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 696; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

99 GENERAL AND MISCELLANEOUS
ABUNDANCE
ACCRETION DISKS
BLACK HOLES
DISPERSION RELATIONS
HARD X RADIATION
IRON
RELATIVISTIC RANGE
SEYFERT GALAXIES
X-RAY GALAXIES