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The ALHAMBRA survey⋆: B-band luminosity function of quiescent and star-forming galaxies at 0.2 ≤ z < 1 by PDF analysis

AutorLopez-Sanjuan, C.; Benítez, Narciso ; Molino, Alberto ; Fernández-Soto, Alberto ; Moles, Mariano ; Pović, Mirjana; Nieves-Seoane, L.; Márquez, Isabel ; Perea, Jaime ; Alfaro, Emilio J. ; Aparicio Villegas, Teresa ; Castander, F. J.; Cerviño, Miguel ; González Delgado, Rosa M. ; Husillos, César ; Masegosa, Josefa ; Olmo, Ascensión del ; Prada, Francisco ; Quintana, José María
Palabras claveGalaxies: evolution
Galaxies: luminosity function, mass function
Galaxies: statistics
Fecha de publicación1-mar-2017
EditorEDP Sciences
CitaciónAstronomy & Astrophysics 599(A62) (2017)
ResumenAims. Our goal is to study the evolution of the B-band luminosity function (LF) since z ∼ 1 using ALHAMBRA data. Methods. We used the photometric redshift and the I-band selection magnitude probability distribution functions (PDFs) of those ALHAMBRA galaxies with I ≤ 24 mag to compute the posterior LF. We statistically studied quiescent and star-forming galaxies using the template information encoded in the PDFs. The LF covariance matrix in redshift - magnitude - galaxy type space was computed, including the cosmic variance. That was estimated from the intrinsic dispersion of the LF measurements in the 48 ALHAMBRA sub-fields. The uncertainty due to the photometric redshift prior is also included in our analysis. Results. We modelled the LF with a redshift-dependent Schechter function affected by the same selection effects than the data. The measured ALHAMBRA LF at 0.2 ≤ z < 1 and the evolving Schechter parameters both for quiescent and star-forming galaxies agree with previous results in the literature. The estimated redshift evolution of M∗B ∝ Qz is QSF = -1.03±0.08 and QQ = -0.80±0.08, and of log10φ∗ ∝ Pz is PSF = -0.01±0.03 and PQ = -0.41 ± 0.05. The measured faint-end slopes are αSF = -1.29 ± 0.02 and αQ = -0.53 ± 0.04. We find a significant population of faint quiescent galaxies with MB ≳ -18, modelled by a second Schechter function with slope β = -1.31 ± 0.11. Conclusions. We present a robust methodology to compute LFs using multi-filter photometric data. The application to ALHAMBRA shows a factor 2.55 ± 0.14 decrease in the luminosity density jB of star-forming galaxies, and a factor 1.25 ± 0.16 increase in the jB of quiescent ones since z = 1, confirming the continuous build-up of the quiescent population with cosmic time. The contribution of the faint quiescent population to jB increases from 3% at z = 1 to 6% at z = 0. The developed methodology will be applied to future multi-filter surveys such as J-PAS. © 2017 ESO.
DescripciónLopez-Sanjuan, C. et. al.
Versión del editorhttp://dx.doi.org/10.1051/0004-636/201629517
URIhttp://hdl.handle.net/10261/148994
DOI10.1051/0004-636/201629517
ISSN1432-0746
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