1. The high-mass end of the red sequence at z ~ 0.55 from SDSS-III/BOSS: completeness, bimodality and luminosity function.
- Author
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Montero-Dorta, Antonio D., Bolton, Adam S., Brownstein, Joel R., Swanson, Molly, Dawson, Kyle, Prada, Francisco, Eisenstein, Daniel, Maraston, Claudia, Thomas, Daniel, Comparat, Johan, Chia-Hsun Chuang, McBride, Cameron K., Favole, Ginevra, Hong Guo, Rodríguez-Torres, Sergio, and Schneider, Donald P.
- Subjects
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STELLAR luminosity function , *STELLAR mass , *COVARIANCE matrices , *BARYONS , *GALACTIC redshift , *GALACTIC evolution - Abstract
We have developed an analytical method based on forward-modelling techniques to characterize the high-mass end of the red sequence (RS) galaxy population at redshift z ~ 0.55, from the DR10 BOSS (Baryon Oscillation Spectroscopic Survey) CMASS spectroscopic sample, which comprises ~600 000 galaxies. The method, which follows an unbinned maximum likelihood approach, allows the deconvolution of the intrinsic CMASS colour-colour-magnitude distributions from photometric errors and selection effects. This procedure requires modelling the covariance matrix for the i-band magnitude, g - r colour and r - i colour using Stripe 82 multi-epoch data. Our results indicate that the error-deconvolved intrinsic RS distribution is consistent, within the photometric uncertainties, with a single point (<0.05 mag) in the colour-colour plane at fixed magnitude, for a narrow redshift slice. We have computed the high-mass end (0.55Mi≲ -22) of the 0.55i-band RS luminosity function (RS LF) in several redshift slices within the redshift range 0.52 < z < 0.63. In this narrow redshift range, the evolution of the RS LF is consistent, within the uncertainties in the modelling, with a passively evolving model with Φ* = (7.248 ± 0.204) × 10-4 Mpc-3 mag-1, fading at a rate of 1.5 ± 0.4 mag per unit redshift. We report RS completeness as a function of magnitude and redshift in the CMASS sample, which will facilitate a variety of galaxy-evolution and clustering studies using BOSS. Our forward-modelling method lays the foundations for future studies using other dark-energy surveys like the Extended Baryon Oscillation Spectroscopic Survey or the Dark Energy Spectroscopic Instrument, which are affected by the same type of photometric blurring/selection effects. [ABSTRACT FROM AUTHOR]
- Published
- 2016
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