THE NuSTAR VIEW OF NEARBY COMPTON-THICK ACTIVE GALACTIC NUCLEI: THE CASES OF NGC 424, NGC 1320, AND IC 2560

被引：95

作者：

Balokovic, M. ^{[1
]}

Comastri, A. ^{[2
]}

Harrison, F. A. ^{[1
]}

Alexander, D. M. ^{[3
]}

Ballantyne, D. R. ^{[4
]}

Bauer, F. E. ^{[5
,6
]}

Boggs, S. E. ^{[7
]}

Brandt, W. N. ^{[8
,9
]}

Brightman, M. ^{[10
]}

Christensen, F. E. ^{[11
]}

Craig, W. W. ^{[7
,12
]}

Del Moro, A. ^{[3
]}

Gandhi, P. ^{[3
]}

Hailey, C. J. ^{[13
]}

Koss, M. ^{[14
,15
]}

Lansbury, G. B. . ^{[3
]}

Luo, B. ^{[8
,9
]}

Madejski, G. M. ^{[16
]}

Marinucci, A. ^{[17
]}

Matt, G. ^{[17
]}

Markwardt, C. B. ^{[18
]}

Puccetti, S. ^{[19
,20
]}

Reynolds, C. S. ^{[21
,22
]}

Risaliti, G. ^{[23
,24
]}

Rivers, E. ^{[1
]}

Stern, D. ^{[25
]}

Walton, D. J. ^{[1
]}

Zhang, W. W. ^{[18
]}

机构：

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

[2] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy

[3] Univ Durham, Dept Phys, Durham DH1 3LE, England

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

[5] Pontificia Univ Catolica Chile 306, Fac Fis, Inst Astrofis, Santiago 22, Chile

[6] Space Sci Inst, Boulder, CO 80301 USA

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

[8] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[9] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA

[10] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

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

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

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

[14] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[15] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland

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

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

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

[19] ASI Sci Data Ctr, I-00044 Frascati, Italy

[20] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy

[21] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[22] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA

[23] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy

[24] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

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

来源：

ASTROPHYSICAL JOURNAL | 2014年 / 794卷 / 02期

基金：

瑞士国家科学基金会; 美国国家航空航天局;

关键词：

galaxies:; individual; (NGC; 424; NGC; 1320; IC; 2560); galaxies: nuclei; galaxies: Seyfert; techniques: spectroscopic; X-rays: galaxies; RAY LUMINOSITY FUNCTION; XMM-NEWTON OBSERVATIONS; STAR-FORMATION; LINE REGION; MIDINFRARED SPECTROSCOPY; SEYFERT-GALAXIES; EDDINGTON RATIOS; KEV SPECTRUM; X-RAYS; MU-M;

D O I：

10.1088/0004-637X/794/2/111

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present X-ray spectral analyses for three Seyfert 2 active galactic nuclei (AGNs), NGC 424, NGC 1320, and IC 2560, observed by NuSTAR in the 3-79 keV band. The high quality hard X-ray spectra allow detailed modeling of the Compton reflection component for the first time in these sources. Using quasi-simultaneous NuSTAR and Swift/XRT data, as well as archival XMM-Newton data, we find that all three nuclei are obscured by Compton-thick material with column densities in excess of similar to 5 x 10(24) cm(-2), and that their X-ray spectra above 3 keV are dominated by reflection of the intrinsic continuum on Compton-thick material. Due to the very high obscuration, absorbed intrinsic continuum components are not formally required by the data in any of the sources. We constrain the intrinsic photon indices and the column density of the reflecting medium through the shape of the reflection spectra. Using archival multi-wavelength data we recover the intrinsic X-ray luminosities consistent with the broadband spectral energy distributions. Our results are consistent with the reflecting medium being an edge-on clumpy torus with a relatively large global covering factor and overall reflection efficiency of the order of 1%. Given the unambiguous confirmation of the Compton-thick nature of the sources, we investigate whether similar sources are likely to be missed by commonly used selection criteria for Compton-thick AGNs, and explore the possibility of finding their high-redshift counterparts.

引用

页数：17

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