The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the correlation function of LOWZ and CMASS galaxies in Data Release 12

By A. Cuesta, M. Vargas-Magaña, F. Beutler, A. Bolton, J. Brownstein, Daniel J. Eisenstein, H. Gil-Marín, Shirley Ho, Cameron McBride, C. Maraston and 13 more. 2015

152 citations recorded by the source corpus.

AJC and LV are supported by supported by the European Research Council under the European Community's Seventh Framework Programme FP7-IDEAS-Phys.LSS 240117. Funding for this work was partially provided by the Spanish MINECO under projects AYA2014-58747-P and MDM-2014-0369 of ICCUB (Unidad de Excelencia ‘Maria de Maeztu’). The Science, Technology and Facilities Council is acknowledged for support through the Survey Cosmology and Astrophysics consolidated grant, ST/I001204/1.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2ce65a9bd89ee3d22c77abc4de6b402c59528eff

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Citations in the corpus

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering (2013, methodology): “…al. 2012, 2014; Tojeiro et al. 2012, 2014; Anderson et al. 2013, 2014a,b; Chuang et al. 2013; Kazin et al. 2013; Manera et al. 2013; Nuza et al. 2013; Samushia et al. 2013, 2014; Sanchez et al. 2013a; Beutler et al. 2014; Wang 2014; Alam et al. 2015; Gil-Marin et al. 2015a,b; Cuesta et al. 2016).”
The trouble with H0 (2016, methodology): “We use constraints on BAO from the following galaxy surveys: Six Degree Field Galaxy Survey (6dF) [33], the Main Galaxy Sample of Data Release 7 of Sloan Digital Sky Survey (SDSS-MGS) [34], the LOWZ and CMASS galaxy samples of the Baryon Oscillation Spectroscopic Survey (BOSSLOWZ and BOSS-CMASS, res”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample (2016, methodology): “For comparison, we focus on theDV constraints, as these provide the most information from the post-reconstruction BAO analysis and we regard the LOWZ volume as too small to obtain robust H(z) likelihoods (the LOWZ DV likelihood is what was used in the Cuesta et al. 2016a cosmological analysis).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: tomographic BAO analysis of DR12 combined sample in Fourier space (2016, methodology): “…part of SDSSIII project (Eisenstein et al. 2011), has reached percent level BAO measurements at zeff = 0.32 and zeff = 0.57 (Anderson et al. 2014; Cuesta et al. 2016; Gil-Marı́n et al. 2016; Ross et al. 2017; Beutler et al. 2017) using the ‘low-redshift’ (LOWZ; 0.15 < z < 0.43) and ‘constant…”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: observational systematics and baryon acoustic oscillations in the correlation function (2016, methodology): “…BOSS data sets produce precise and robust BAO and RSD measurements (c.f., Reid et al. 2012; Anderson et al. 2012; Chuang et al. 2013a; Kazin et al. 2013; Sánchez et al. 2013; Anderson et al. 2014a,b; Sánchez et al. 2014; Samushia et al. 2014; Cuesta et al. 2016; Gil-Marı́n et al. 2015a,b).”
Elucidating ΛCDM: Impact of Baryon Acoustic Oscillation Measurements on the Hubble Constant Discrepancy (2017, background): “The same effect is apparent in Figure 8 of Cuesta et al. (2016).”
A 6% measurement of the Hubble parameter at z∼0.45: direct evidence of the epoch of cosmic re-acceleration (2016, methodology): “As a comparison, we report the results obtained from the BAO analysis in the final BOSS DR12 [71], where it is found H(z = 0.57)rd/r fid d = 100.3 ± 3.7 km/s/Mpc and H(z = 0.32)rd/r fid d = 79.2 ± 5.6 km/s/Mpc.”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedges (2016, methodology): “…et al. (2016b) perform BAO-only fits to the Legengre multipoles of order = 0, 2 of the two-point functions in configuration and Fourier space obtained after the application of the reconstruction technique (Eisenstein et al. 2007; Padmanabhan et al. 2012) as described in Cuesta et al. (2016).”