A DIRECT MEASUREMENT OF THE LINEAR BIAS OF MID-INFRARED-SELECTED QUASARS AT z ≈ 1 USING COSMIC MICROWAVE BACKGROUND LENSING

被引：51

作者：

Geach, J. E. ^{[1
,2
]}

Hickox, R. C. ^{[3
]}

Bleem, L. E. ^{[4
,5
,6
]}

Brodwin, M. ^{[7
]}

Holder, G. P. ^{[2
]}

Aird, K. A. ^{[8
]}

Benson, B. A. ^{[4
,9
]}

Bhattacharya, S. ^{[4
,6
]}

Carlstrom, J. E. ^{[4
,5
,6
,9
,10
]}

Chang, C. L. ^{[4
,9
]}

Cho, H. -M. ^{[11
]}

Crawford, T. M. ^{[4
,10
]}

Crites, A. T. ^{[4
,10
]}

de Haan, T. ^{[2
]}

Dobbs, M. A. ^{[2
]}

Dudley, J. ^{[2
]}

George, E. M. ^{[12
]}

Hainline, K. N. ^{[3
]}

Halverson, N. W. ^{[13
,14
]}

Holzapfel, W. L. ^{[12
]}

Hoover, S. ^{[4
,5
]}

Hou, Z.

Hrubes, J. D. ^{[8
]}

Keisler, R. ^{[5
]}

Knox, L. ^{[15
]}

Lee, A. T. ^{[12
,16
]}

Leitch, E. M.

Lueker, M. ^{[17
]}

Luong-Van, D. ^{[8
]}

Marrone, D. P. ^{[18
]}

McMahon, J. J. ^{[19
]}

Mehl, J. ^{[4
]}

Meyer, S. S. ^{[4
,5
,9
,10
]}

Millea, M.

Mohr, J. J. ^{[20
,21
,22
]}

Montroy, T. E. ^{[23
]}

Myers, A. D. ^{[24
]}

Padin, S. ^{[4
,10
,17
]}

Plagge, T. ^{[4
,10
]}

Pryke, C. ^{[25
]}

Reichardt, C. L.

Ruhl, J. E.

Sayre, J. T. ^{[23
]}

Schaffer, K. K. ^{[4
,9
,26
]}

Shaw, L.

Shirokoff, E. ^{[12
]}

Spieler, H. G. ^{[16
]}

Staniszewski, Z. ^{[23
]}

Stark, A. A. ^{[27
]}

Story, K. T. ^{[4
,5
]}

机构：

[1] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England

[2] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada

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

[4] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[5] Univ Chicago, Dept Phys, Chicago, IL 60637 USA

[6] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60440 USA

[7] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA

[8] Univ Chicago, Chicago, IL 60637 USA

[9] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA

[10] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

[11] NIST Quantum Devices Grp, Boulder, CO 80305 USA

[12] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[13] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[14] Univ Colorado, Dept Phys, Boulder, CO 80309 USA

[15] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

[16] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA

[17] CALTECH, Pasadena, CA 91125 USA

[18] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

[19] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[20] Univ Munich, Dept Phys, D-81679 Munich, Germany

[21] Excellence Cluster Univ, D-85748 Garching, Germany

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

[23] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA

[24] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82072 USA

[25] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA

[26] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA

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

[28] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada

[29] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada

[30] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2013年 / 776卷 / 02期

基金：

美国国家科学基金会; 加拿大自然科学与工程研究理事会;

关键词：

cosmology:; observations; ACTIVE GALACTIC NUCLEI; DARK-MATTER; MIDINFRARED SELECTION; BLACK-HOLES; EVOLUTION; GALAXIES; MODEL;

D O I：

10.1088/2041-8205/776/2/L41

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We measure the cross-power spectrum of the projected mass density as traced by the convergence of the cosmic microwave background lensing field from the South Pole Telescope (SPT) and a sample of Type 1 and 2 (unobscured and obscured) quasars at < z > similar to 1 selected with the Wide-field Infrared Survey Explorer, over 2500 deg(2). The cross-power spectrum is detected at approximate to 7 sigma, and we measure a linear bias b = 1.61 +/- 0.22, consistent with clustering analyses. Using an independent lensing map, derived from Planck observations, to measure the cross-spectrum, we find excellent agreement with the SPT analysis. The bias of the combined sample of Type 1 and 2 quasars determined in this work is similar to that previously determined for Type 1 quasars alone; we conclude that obscured and unobscured quasars trace the matter field in a similar way. This result has implications for our understanding of quasar unification and evolution schemes.

引用

页数：6

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