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Title

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

AuthorsLópez-Sanjuan, C.; Tempel, E.; Benítez, Narciso ; Molino, Alberto ; Viironen, Kerttu; Díaz-García, L. A.; Fernández-Soto, Alberto ; Santos, W. A.; Varela, Jesús ; Cenarro, A. J.; Moles, Mariano ; Arnalte-Mur, P. ; Ascaso, Begoña ; Montero-Dorta, Antonio D. ; Pović, Mirjana; Martínez, Vicente J.; Nieves-Seoane, L.; Stefanon, Mauro; Hurtado-Gil, L.; Márquez, Isabel ; Perea, Jaime ; Aguerri, J. A. L.; Alfaro, Emilio J. ; Aparicio Villegas, Teresa ; Broadhurst, T.; Cabrera-Caño, Jesús; Castander, Francisco J. ; Cepa, Jordi; Cerviño, Miguel ; Cristóbal-Hornillos, David ; González Delgado, Rosa M. ; Husillos, César ; Infante, Leopoldo; Masegosa, Josefa ; Olmo, Ascensión del ; Prada, Francisco ; Quintana, José María
KeywordsGalaxies: statistics
Galaxies: evolution
Galaxies: luminosity function, mass function
Issue Date2017
PublisherEDP Sciences
CitationAstronomy and Astrophysics 599: A62 (2017)
Abstract[Aims]: 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 ∝ Q is Q = -1.03±0.08 and Q = -0.80±0.08, and of logφ ∝ P is P = -0.01±0.03 and P = -0.41 ± 0.05. The measured faint-end slopes are α = -1.29 ± 0.02 and α = -0.53 ± 0.04. We find a significant population of faint quiescent galaxies with M ≳ -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 j of star-forming galaxies, and a factor 1.25 ± 0.16 increase in the j 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 j 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.
Publisher version (URL)https://doi.org/10.1051/0004-6361/201629517
URIhttp://hdl.handle.net/10261/170647
Identifiersdoi: 10.1051/0004-6361/201629517
e-issn: 1432-0746
issn: 0004-6361
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