Eating Disorders

Ross, Carolyn

doi:10.1007/978-1-4939-0548-5_30

Cited by 14 publications

(18 citation statements)

References 50 publications

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“…From the full 2PCF, Ross et al (2014) uses 540, 505 CMASS galaxies in DR10 to measure the real-space linear bias, finding b1 = 1.96 ± 0.05. σ8(z = 0) = 0.8 for this work, and rescaling as discussed above reduces this value to b1 = 1.89, comparable to our expected real-space range of b1 ∼ 1.77−1.85. We caution that the galaxy samples used in Guo et al (2013) and in Ross et al (2014) are again proper subsets of our own (roughly 30% and 70%, respectively) so one would not necessarily expect the bias values to be equal.…”

Section: Discussionmentioning

confidence: 99%

The large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies

Slepian

Eisenstein

Beutler

et al. 2017

Monthly Notices of the Royal Astronomical Society

103

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We report a measurement of the large-scale 3-point correlation function of galaxies using the largest dataset for this purpose to date, 777, 202 Luminous Red Galaxies in the Sloan Digital Sky Survey Baryon Acoustic Oscillation Spectroscopic Survey (SDSS BOSS) DR12 CMASS sample. This work exploits the novel algorithm of Slepian & Eisenstein (2015b) to compute the multipole moments of the 3PCF in O(N 2 ) time, with N the number of galaxies. Leading-order perturbation theory models the data well in a compressed basis where one triangle side is integrated out. We also present an accurate and computationally efficient means of estimating the covariance matrix. With these techniques the redshift-space linear and non-linear bias are measured, with 2.6% precision on the former if σ 8 is fixed. The data also indicates a 2.8σ preference for the BAO, confirming the presence of BAO in the 3-point function.

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Section: Discussionmentioning

confidence: 99%

The large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies

Slepian

Eisenstein

Beutler

et al. 2017

Monthly Notices of the Royal Astronomical Society

103

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“…The observed galaxy data have been analysed, and the cosmological results delivered, using both the power spectrum (see, e.g., Tegmark et al 2004;Hutsi 2005;Padmanabhan et al 2007;Blake et al 2007;Percival et al 2007Percival et al , 2010Reid et al 2010;Montesano et al 2012), and the correlation function (see, e.g., Eisenstein et al 2005;Okumura et al 2008;Martinez et al 2009;Sanchez et al 2009;Kazin et al 2010;Samushia et al 2012;Padmanabhan et al 2012;Xu et al 2013;Oka et al 2014;Hemantha et al 2014). Similar analyses have been also applied to the SDSS-III BOSS (Ahn et al 2012) galaxy sample (Anderson et al 2013;Manera et al 2012;Nuza et al 2013;Reid et al 2012;Samushia et al 2013;Tojeiro et al 2012;Anderson et al 2014b;Chuang et al 2013a;Sanchez et al 2013;Kazin et al 2013;Wang 2014;Anderson et al 2014a;Beutler et al 2014;Samushia et al 2014;Chuang et al 2013b;Sanchez et al 2014;Ross et al 2014;Tojeiro et al 2014;Reid et al 2014;Alam et al 2015;Gil-Marín et al 2015a,b;...…”

Section: Introductionmentioning

confidence: 96%

The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from DR12 galaxy clustering – towards an accurate model

Chuang

Pellejero-Ibáñez

Rodríguez-Torres

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We analyse the broad-range shape of the monopole and quadrupole correlation functions of 2 Chuang et al.the BOSS Data Release 12 (DR12) CMASS and LOWZ galaxy sample to obtain constraints on the Hubble expansion rate H(z), the angular-diameter distance D A (z), the normalised growth rate f (z)σ 8 (z), and the physical matter density Ω m h 2 . We adopt wide and flat priors on all model parameters in order to ensure the results are those of a 'single-probe' galaxy clustering analysis. We also marginalise over three nuisance terms that account for potential observational systematics affecting the measured monopole. The Monte Carlo Markov Chain analysis with such wide priors and additional polynomial functions is computationally expensive for advanced theoretical models. We develop a new methodology to speed up by scanning the parameter space using a fast model first and then applying importance sampling using a slower but more accurate model.Our measurements for DR12 galaxy sample, using the range, Ω m h 2 } = {956 ± 28 Mpc, 75.0 ± 4.0 km s −1 Mpc −1 , 0.397 ± 0.073, 0.143 ± 0.017} at z = 0.32 and {1421 ± 23 Mpc, 96.7 ± 2.7 km s −1 Mpc −1 , 0.497 ± 0.058, 0.137 ± 0.015} at z = 0.59 where r s is the comoving sound horizon at the drag epoch and r s,f id = 147.66 Mpc is the sound scale of the fiducial cosmology used in this study.In addition, we divide each sample (CMASS and LOWZ) into two redshift bins (four bins in total) to increase the sensitivity of redshift evolution. However, we do not find improvements in terms of constraining dark energy model parameters. Combining our measurements with Planck data, we obtain Ω m = 0.306 ± 0.009, H 0 = 67.9 ± 0.7 km s −1 Mpc −1 , and σ 8 = 0.815 ± 0.009 assuming ΛCDM; Ω k = 0.000 ± 0.003 assuming oCDM; w = −1.01 ± 0.06 assuming wCDM; and w 0 = −0.95 ± 0.22 and w a = −0.22 ± 0.63 assuming w 0 w a CDM. Our results show no tension with the flat ΛCDM cosmological paradigm. This paper is part of a set that analyses the final galaxy clustering dataset from BOSS.

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“…& White 2007a;Seo et al 2010;Mehta et al 2011;Sherwin & Zaldarriaga 2012). Measurements of the BAO scale using samples with considerable differences in galaxy bias that share the same volume have obtained results consistent with such small shifts (Ross et al 2014;Beutler et al 2016). A key element of recent BAO analyses is reconstruction, which attempts to reverse non-linear effects so as to sharpen the BAO peak and thereby restore measurement precision (Eisenstein et al 2007b;Padmanabhan et al 2012;Burden, Percival & Howlett 2015;Schmittfull et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample

Alam

Ata

Bailey

et al. 2017

Monthly Notices of the Royal Astronomical Society

2,744

2,404

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We present cosmological results from the final galaxy clustering data set of the Baryon Oscillation Spectroscopic Survey, part of the Sloan Digital Sky Survey III. Our combined galaxy sample comprises 1.2 million massive galaxies over an effective area of 9329 deg 2 and volume of 18.7 Gpc 3 , divided into three partially overlapping redshift slices centred at effective redshifts 0.38, 0.51 and 0.61. We measure the angular diameter distance D M and Hubble parameter H from the baryon acoustic oscillation (BAO) method, in combination with a cosmic microwave background prior on the sound horizon scale, after applying reconstruction to reduce non-linear effects on the BAO feature. Using the anisotropic clustering of the Hubble Fellow.

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Eating Disorders

Cited by 14 publications

References 50 publications

The large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies

The large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies

The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from DR12 galaxy clustering – towards an accurate model

The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample

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