The Subaru-XMM-Newton Deep Survey (SXDS). VIII. Multi-wavelength identification, optical/NIR spectroscopic properties, and photometric redshifts of X-ray sources

被引：31

作者：

Akiyama, Masayuki ^{[1
]}

Ueda, Yoshihiro ^{[2
]}

Watson, Mike G. ^{[3
]}

Furusawa, Hisanori ^{[4
]}

Takata, Tadafumi ^{[4
]}

Simpson, Chris ^{[5
]}

Morokuma, Tomoki ^{[6
]}

Yamada, Toru ^{[1
]}

Ohta, Kouji ^{[2
]}

Iwamuro, Fumihide ^{[2
]}

Yabe, Kiyoto ^{[4
]}

Tamura, Naoyuki ^{[7
]}

Moritani, Yuuki ^{[8
]}

Takato, Naruhisa ^{[4
]}

Kimura, Masahiko ^{[9
]}

Maihara, Toshinori ^{[2
]}

Dalton, Gavin ^{[10
,11
]}

Lewis, Ian ^{[10
]}

Lee, Hanshin ^{[10
,12
]}

Curtis-Lake, Emma ^{[10
,13
]}

Macaulay, Edward ^{[10
,14
]}

Clarke, Frazer ^{[10
]}

Silverman, John D. ^{[7
]}

Croom, Scott ^{[15
]}

Ouchi, Masami ^{[16
]}

Hanami, Hitoshi ^{[17
]}

Diaz Tello, Jorge ^{[18
]}

Yoshikawa, Tomohiro ^{[19
]}

Fujishiro, Naofumi ^{[20
]}

Sekiguchi, Kazuhiro ^{[4
]}

机构：

[1] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan

[2] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto, Kyoto 6068502, Japan

[3] Univ Leicester, Dept Phys & Astron, XROA Grp, Leicester LE1 7RH, Leics, England

[4] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[5] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England

[6] Univ Tokyo, Inst Astron, Grad Sch Sci, Mitaka, Tokyo 1810015, Japan

[7] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan

[8] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan

[9] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan

[10] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England

[11] STFC Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England

[12] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA

[13] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland

[14] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia

[15] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia

[16] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan

[17] Iwate Univ, Phys Sect, Fac Humanities & Social Sci, Morioka, Iwate 0208550, Japan

[18] Univ Nacl Cordoba, Observ Astron Cordoba, IATE, RA-5000 Cordoba, Argentina

[19] Kyoto Nijikoubou Co Ltd, Sakyo Ku, Kyoto, Kyoto 6060003, Japan

[20] Kyoto Sangyo Univ, Koyama Astron Observ, Kita Ku, Kyoto, Kyoto 6038047, Japan

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN | 2015年 / 67卷 / 05期

基金：

美国国家航空航天局; 美国国家科学基金会;

关键词：

catalogs; galaxies: active; quasars: general; surveys; X-rays: galaxies; ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; BULGE MASS RELATION; DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; SIMILAR-TO; LUMINOSITY FUNCTION; HOST GALAXIES;

D O I：

10.1093/pasj/psv050

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the multi-wavelength identification of the X-ray sources found in the Subaru-XMM-Newton Deep Survey (SXDS) using deep imaging data covering the wavelength range between the far-UV and mid-IR (MIR). We select a primary counterpart of each X-ray source by applying the likelihood ratio method to R-band, 3.6 mu m, near-UV, and 24 mu m source catalogs as well as matching catalogs of active galactic nucleus (AGN) candidates selected in 1.4 GHz radio and i'-band variability surveys. Once candidates for Galactic stars, ultra-luminous X-ray sources in a nearby galaxy, and clusters of galaxies are removed there are 896 AGN candidates in the sample. We conduct spectroscopic observations of the primary counterparts with multi-object spectrographs in the optical and NIR; 65% of the X-ray AGN candidates are spectroscopically identified. For the remaining X-ray AGN candidates, we evaluate their photometric redshift with photometric data in 15 bands. Utilizing the multi-wavelength photometric data of the large sample of X-ray-selected AGNs, we evaluate the stellar masses, M-*, of the host galaxies of the narrow-line AGNs. The distribution of the stellarmass is remarkably constant from z=0.1 to 4.0. The relation between M-* and 2-10 keV luminosity can be explained with strong cosmological evolution of the relationship between the black hole mass and M-*. We also evaluate the scatter of the UV-MIR spectral energy distribution (SED) of the X-ray AGNs as a function of X-ray luminosity and absorption by the nucleus. The scatter is compared with galaxies which have redshift and stellarmass distributionmatched with the X-ray AGN. The UV-NIR (near-IR) SEDs of obscured X-ray AGNs are similar to those of the galaxies in the matched sample. In the NIR-MIR range, the median SEDs of X-ray AGNs are redder, but the scatter of the SEDs of the X-ray AGN broadly overlaps that of the galaxies in the matched sample.

引用

页数：38

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