THE CLUSTERING OF MASSIVE GALAXIES AT<i>z</i>∼ 0.5 FROM THE FIRST SEMESTER OF BOSS DATA

White, Martin; Blanton, Michael R.; Bolton, A.; Schlegel, David J.; Tinker, Jeremy L.; Berlind, Andreas A.; Costa, L. N. da; Kazin, Eyal; Lin, Yen Ting; Maia, M. A. G.; McBride, Cameron K.; Padmanabhan, Nikhil; Parejko, John K.; Percival, Will J.; Prada, Francisco; Ramos, B.; Sheldon, E.; Simoni, F. de; Skibba, Ramin; Thomas, Daniel; Wake, David A.; Zehavi, Idit; Zheng, Zheng; Nichol, R. C.; Schneider, Donald P.; Strauss, Michael A.; Weaver, B. A.; Weinberg, David H.

doi:10.1088/0004-637x/728/2/126

Cited by 280 publications

(430 citation statements)

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“…The rightmost column gives the tSZ distortion brightness temperature at 148 GHz, with the next-largest component due to dust emission projected out [21]; this is obtained from a linear combination of ACT 148 and 218 GHz signals. Galaxies in the three highest luminosity bins, corresponding to about 20% of the total, show mean temperature decrements consistent with halo-model cluster masses [27] and with the mean temperature decrements found in Ref. [19].…”

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confidence: 88%

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Cosmic Microwave Background Carries Imprint of Moving Galaxies

Holder¹

2012

Physics

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Using high-resolution microwave sky maps made by the Atacama Cosmology Telescope, we for the first time present strong evidence for motions of galaxy clusters and groups via microwave background temperature distortions due to the kinematic Sunyaev-Zel'dovich effect. Galaxy clusters are identified by their constituent luminous galaxies observed by the Baryon Oscillation Spectroscopic Survey, part of the Sloan Digital Sky Survey III. We measure the mean pairwise momentum of clusters, with a probability of the signal being due to random errors of 0.002, and the signal is consistent with the growth of cosmic structure in the standard model of cosmology. DOI: 10.1103/PhysRevLett.109.041101 PACS numbers: 98.80.Es, 98.62.Py, 98.65.Cw, 98.70.Vc PRL 109, 041101 (2012 Selected for a Viewpoint in Physics P H Y S I C A L R E V I E W L E T T E R S week ending 0031-9007=12=109(4)=041101 (6) 041101-1 Ó 2012 American Physical SocietyIntroduction.-The growth of cosmic structure over the history of the Universe inevitably results not only in the formation of dense objects, but also in motions of these objects. Measurements of these motions have the potential to provide both a valuable consistency check on the standard cosmological model, and also an independent route to constraining cosmological parameters and the nature of dark energy.In 1972, Sunyaev and Zel'dovich realized that a moving galaxy cluster, which is largely composed of hot, ionized gas in a dark matter potential well, will induce a small brightness temperature shift in the microwave radiation passing through it. The shift is proportional to both the mass in electrons and the line-of-sight velocity of the cluster with respect to the microwave background rest frame [1,2]. This kinematic Sunyaev-Zel'dovich (kSZ) effect is distinct from the thermal SZ (tSZ) effect, in which scattering from the same hot cluster gas creates a spectral distortion (see [3] for a review). In high-mass clusters (M ' 10 15 solar masses), the tSZ signal is typically a factor of 20 larger than the kSZ signal; however, the two signals are comparable for the lowmass clusters (M ' 10 13 M ) which are far more abundant. (For brevity, we refer to any object with mass larger than 10 13 M as a cluster, even though objects below 10 14 M are usually referred to as ''groups.'') The tSZ effect from large clusters is now regularly observed in blind surveys [4][5][6][7], but only upper limits for the kSZ effect from individual galaxy clusters have been achieved to date [8][9][10][11][12].In this Letter, we present clear statistical evidence of the motions of galaxy clusters through their kSZ signal in arcminute-resolution microwave maps made with the Atacama Cosmology Telescope (ACT) [13]. Luminous galaxies are associated with galaxy clusters [14,15], and we use the Sloan Digital Sky Survey III (SDSS-III) Baryon Oscillation Spectroscopic Survey (BOSS) [16] catalog of these galaxies as galaxy cluster proxies, giving the sky location and redshift for thousands of potential clusters. We then treat the effe...

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confidence: 88%

“…week ending masses around 10 13 solar masses, with around 10% to 15% in haloes as large as 10 14 M [27]. To estimate the microwave temperature distortion T i associated with galaxy i, we follow the procedure used in Ref.…”

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confidence: 99%

Cosmic Microwave Background Carries Imprint of Moving Galaxies

Holder¹

2012

Physics

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“…To cull areas of the survey that greatly affect the quasar density, we use veto masks developed to analyze BOSS galaxy clustering 12 (see, e.g., White et al 2011;Anderson et al 2012;Ross et al 2012a). The angular completeness of the survey is tracked in regions defined by a unique set of overlapping spectroscopic tiles (called a sector; see Blanton et al 2003).…”

Section: Discussionmentioning

confidence: 99%

“…Appendix A introduces the software that we used to generate a uniform random catalog from the survey mask. We adopt a ΛCDM cosmological model with Ωm = 0.274, ΩΛ = 0.726, h = 0.7 and σ8 = 0.8 as assumed in other BOSS analyses (e.g., White et al 2011;Reid et al 2012;White et al 2012;Anderson et al 2012). We express magnitudes in the AB system (Oke & Gunn 1983).…”

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confidence: 99%

Clustering of intermediate redshift quasars using the final SDSS III-BOSS sample

Eftekharzadeh

Myers

White

et al. 2015

Mon. Not. R. Astron. Soc.

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“…The parameter M 0 is generally poorly constrained and we decided in this analysis to fix M 0 = M min (see also White et al 2011;de la Torre & Guzzo 2012). In the halo model formalism, the galaxy power spectrum or two-point correlation function can be written as the sum of two The VIPERS results are compared to the pervious measurements performed in the DEEP2 (Zheng et al 2007), BOSS , and CFHTLS (Coupon et al 2012) surveys.…”

Section: Real-space Clusteringmentioning

confidence: 99%

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Torre¹,

Guzzo²,

Peacock³

et al. 2013

A&A

287

117

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We present the general real-and redshift-space clustering properties of galaxies as measured in the first data release of the VIPERS survey. VIPERS is a large redshift survey designed to probe in detail the distant Universe and its large-scale structure at 0.5 < z < 1.2. We describe in this analysis the global properties of the sample and discuss the survey completeness and associated corrections. This sample allows us to measure the galaxy clustering with an unprecedented accuracy at these redshifts. From the redshift-space distortions observed in the galaxy clustering pattern we provide a first measurement of the growth rate of structure at z = 0.8: f σ 8 = 0.47 ± 0.08. This is completely consistent with the predictions of standard cosmological models based on Einstein gravity, although this measurement alone does not discriminate between different gravity models.

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THE CLUSTERING OF MASSIVE GALAXIES ATz∼ 0.5 FROM THE FIRST SEMESTER OF BOSS DATA

Cited by 280 publications

References 60 publications

Cosmic Microwave Background Carries Imprint of Moving Galaxies

Cosmic Microwave Background Carries Imprint of Moving Galaxies

Clustering of intermediate redshift quasars using the final SDSS III-BOSS sample

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

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