MEASURING THE CORONAL PROPERTIES OF IC 4329A WITH NuSTAR

被引：34

作者：

Brenneman, L. W. ^{[1
]}

Madejski, G. ^{[2
]}

Fuerst, F. ^{[3
]}

Matt, G. ^{[4
]}

Elvis, M. ^{[1
]}

Harrison, F. A. ^{[3
]}

Ballantyne, D. R. ^{[5
]}

Boggs, S. E. ^{[6
]}

Christensen, F. E. ^{[7
]}

Craig, W. W. ^{[7
,8
]}

Fabian, A. C. ^{[9
]}

Grefenstette, B. W. ^{[3
]}

Hailey, C. J. ^{[10
]}

Madsen, K. K. ^{[3
]}

Marinucci, A. ^{[4
]}

Rivers, E. ^{[3
]}

Stern, D. ^{[11
]}

Walton, D. J. ^{[3
]}

Zhang, W. W. ^{[12
]}

机构：

[1] Harvard Smithsonian CfA, Cambridge, MA 02138 USA

[2] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA

[3] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA

[4] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy

[5] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA

[6] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[7] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark

[8] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA

[9] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

[10] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA

[11] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[12] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

来源：

ASTROPHYSICAL JOURNAL | 2014年 / 781卷 / 02期

基金：

美国国家航空航天局;

关键词：

accretion; accretion disks; galaxies: active; galaxies: individual (IC 4329A); galaxies: nuclei galaxies: Seyfert; X-rays: galaxies; ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRA; SEYFERT-GALAXIES; COMPTONIZATION MODELS; BEPPOSAX OBSERVATIONS; IC-4329A; EMISSION; CATALOG; SUZAKU;

D O I：

10.1088/0004-637X/781/2/83

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present an analysis of a similar to 160 ks NuSTAR observation of the nearby bright Seyfert galaxy IC 4329A. The high-quality broadband spectrum enables us to separate the effects of distant reflection from the direct coronal continuum, and to therefore accurately measure the high-energy cutoff to be E-cut = 178(-40)(+74) keV. The coronal emission arises from accretion disk photons Compton up-scattered by a thermal plasma, with the spectral index and cutoff being due to a combination of the finite plasma temperature and optical depth. Applying standard Comptonization models, we measure both physical properties independently using the best signal to noise obtained to date in an active galactic nucleus over the 3-79 keV band. We derive kTe = 37+ 6 keV with tau = 1.25(-0.10)(+0.20) assuming a slab geometry for the plasma, and kT(e) = 33(-6)(+6) keV with tau = 3.41(-0.38)(+0.58) for a spherical geometry, with both having an equivalent goodness-of-fit.

引用

页数：6

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