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  • R.~C. Hickox
  • L.~E. Bleem
  • M. Brodwin
  • G.~P. Holder
  • K.~A. Aird
  • B.~A. Benson
  • S. Bhattacharya
  • J.~E. Carlstrom
  • C.~L. Chang
  • H.-M. Cho
  • T.~M. Crawford
  • A.~T. Crites
  • T. de Haan
  • M.~A. Dobbs
  • J. Dudley
  • E.~M. George
  • K.~N. Hainline
  • N.~W. Halverson
  • W.~L. Holzapfel
  • S. Hoover
  • Z. Hou
  • J.~D. Hrubes
  • R. Keisler
  • L. Knox
  • A.~T. Lee
  • E.~M. Leitch
  • M. Lueker
  • D. Luong-Van
  • D.~P. Marrone
  • J.~J. McMahon
  • J. Mehl
  • S.~S. Meyer
  • M. Millea
  • J.~J. Mohr
  • T.~E. Montroy
  • A.~D. Myers
  • S. Padin
  • T. Plagge
  • C. Pryke
  • C.~L. Reichardt
  • J.~E. Ruhl
  • J.~T. Sayre
  • K.~K. Schaffer
  • L. Shaw
  • E. Shirokoff
  • H.~G. Spieler
  • Z. Staniszewski
  • A.~A. Stark
  • K.~T. Story
  • A. van Engelen
  • K. Vanderlinde
  • J.~D. Vieira
  • R. Williamson
  • O. Zahn
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Original languageEnglish
Number of pages6
JournalAstrophysical Journal Letters
Journal publication date20 Oct 2013
Volume776
Issue2
DOIs
Publication statusPublished - 20 Oct 2013

Abstract

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 langzrang ~ 1 selected with the Wide-field Infrared Survey Explorer, over 2500 deg2. The cross-power spectrum is detected at ≈7σ, 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.

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