The NuSTAR Extragalactic Survey: Average Broadband X-Ray Spectral Properties of the NuSTAR-detected AGNs

被引：17

作者：

Del Moro, A. ^{[1
,2
]}

Alexander, D. M. ^{[2
]}

Aird, J. A. ^{[3
]}

Bauer, F. E. ^{[4
,5
,6
,7
]}

Civano, F. ^{[8
,9
]}

Mullaney, J. R. ^{[10
]}

Ballantyne, D. R. ^{[11
]}

Brandt, W. N. ^{[12
,13
,14
]}

Comastri, A. ^{[15
]}

Gandhi, P. ^{[16
]}

Harrison, F. A. ^{[17
]}

Lansbury, G. B. ^{[2
,3
]}

Lanz, L. ^{[8
]}

Luo, B. ^{[18
]}

Marchesi, S. ^{[19
]}

Puccetti, S. ^{[20
,21
]}

Ricci, C. ^{[4
,5
,22
,23
]}

Saez, C. ^{[24
]}

Stern, D. ^{[25
]}

Treister, E. ^{[4
,5
]}

Zappacosta, L.

机构：

[1] Max Planck Inst Extraterrestr Phys MPE, Giessenbachstr 1, D-85748 Garching, Germany

[2] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England

[3] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[4] Pontificia Univ Catolica Chile, Inst Astrofis, Casilla 306, Santiago 22, Chile

[5] Pontificia Univ Catolica Chile, Ctr Astroingn, Casilla 306, Santiago 22, Chile

[6] Millennium Inst Astrophys MAS, Nuncio Monsenor Sotero Sanz 100, Santiago, Chile

[7] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA

[8] Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA

[9] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[10] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England

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

[12] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

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

[14] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA

[15] INAF, Osservatorio Astron Bologna, Via Gobetti 93-3, I-40129 Bologna, Italy

[16] Univ Southampton, Fac Phys Sci & Engn, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England

[17] CALTECH, Cahill Ctr Astrophys, 1216 East Calif Blvd, Pasadena, CA 91125 USA

[18] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China

[19] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA

[20] INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy

[21] Agenzia Spaziale Italiana Unita Ric Sci, Via Politecn, I-00133 Rome, Italy

[22] EMBIGGEN Anillo, Concepcion, Chile

[23] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China

[24] Univ Chile, Dept Astron, Observ Astron Cerro Calan, Casilla 36-D, Santiago, Chile

[25] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-221, Pasadena, CA 91109 USA

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 849卷 / 01期

基金：

英国科学技术设施理事会;

关键词：

galaxies: active; quasars: general; surveys; X-rays: galaxies; ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; LUMINOSITY FUNCTION; STAR-FORMATION; SKY SURVEY; CHANDRA; SAMPLE; EVOLUTION; REFLECTION; CONSTRAINTS;

D O I：

10.3847/1538-4357/aa9115

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a study of the average X-ray spectral properties of the sources detected by the NuSTAR extragalactic survey, comprising observations of the Extended Chandra Deep Field South (E-CDFS), Extended Groth Strip (EGS), and the Cosmic Evolution Survey (COSMOS). The sample includes 182 NuSTAR sources (64 detected at 8-24 keV), with 3-24 keV fluxes ranging between f3(-24keV) approximate to 10(-14) and 6 x 10(-13) erg cm(-2) S-1 (f(8-24 keV) approximate to 3 x 10(-14)-3 x 10(-13) erg cm(-2) S-1) and redshifts in the range of z = 0.04-3.21. We produce composite spectra from the Chandra + NuSTAR data (E approximate to 2-40 keV, rest frame) for all the sources with redshift identifications (95%) and investigate the intrinsic, average spectra of the sources, divided into broad-line (BL) and narrow-line (NL) active galactic nuclei (AGNs), and also in different bins of X-ray column density and luminosity. The average power-law photon index for the whole sample is Gamma = 1.651(-0.03)(+0.03), flatter than the Gamma approximate to 1.8 typically found for AGNs. While the spectral slope of BL and X-ray unabsorbed AGNs is consistent with the typical values (Gamma = 1.79(-0.01)(+0.01)), a significant flattening is seen in NL AGNs and heavily absorbed sources (Gamma = 1.60(-0.05)(+0.08) and Gamma = 1.38(-0.12)(+0.12), respectively), likely due to the effect of absorption and to the contribution from the Compton reflection component to the high-energy flux (E > 10 keV). We find that the typical reflection fraction in our spectra is R approximate to 0.5 (for F = 1.8), with a tentative indication of an increase of the reflection strength with X-ray column density. While there is no significant evidence for a dependence of the photon index on X-ray luminosity in our sample, we find that R decreases with luminosity, with relatively high levels of reflection (R approximate to 1.2) for L10-40 keV < 10(44) erg s(-1) and R approximate to 0.3 for L10-40 (keV) > 10(44) erg s(-1) AGNs, assuming a fixed spectral slope of Gamma = 1.8.

引用

页数：19

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