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

[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 poster...

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Detalles Bibliográficos
Autores: López-Sanjuan, Carlos, 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, Tom, 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
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2017
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/170647
Acceso en línea:http://hdl.handle.net/10261/170647
Access Level:acceso abierto
Palabra clave:Galaxies: statistics
Galaxies: evolution
Galaxies: luminosity function, mass function
Descripción
Sumario:[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.

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