Bibcode
Cava, A.; Pérez-González, P. G.; Eliche-Moral, M. Carmen; Ricciardelli, Elena; Vidal-García, Alba; Alcalde Pampliega, Belen; Alonso-Herrero, Almudena; Barro, Guillermo; Cardiel, Nicolas; Cenarro, A. Javier; Charlot, Stephane; Daddi, Emanuele; Dessauges-Zavadsky, Miroslava; Domínguez Sánchez, Helena; Espino-Briones, Nestor; Esquej, Pilar; Gallego, Jesus; Hernán-Caballero, Antonio; Huertas-Company, Marc; Koekemoer, Anton M.; Muñoz-Tuñon, C.; Rodríguez-Espinosa, J. M.; Rodríguez-Muñoz, Lucia; Tresse, Laurence; Villar, Victor
Referencia bibliográfica
The Astrophysical Journal, Volume 812, Issue 2, article id. 155, 22 pp. (2015).
Fecha de publicación:
10
2015
Revista
Número de citas
17
Número de citas referidas
16
Descripción
In this paper, we present a comprehensive analysis of star-forming
galaxies (SFGs) at intermediate redshifts (z ∼ 1). We combine the
ultra-deep optical spectro-photometric data from the Survey for High-z
Absorption Red and Dead Sources (SHARDS) with deep UV-to-FIR
observations in the GOODS-N field. Exploiting two of the 25 SHARDS
medium-band filters, F687W17 and F823W17, we select [O ii] emission line
galaxies at z ∼ 0.84 and z ∼ 1.23 and characterize their
physical properties. Their rest-frame equivalent widths
(EWrf([O ii])), line fluxes, luminosities, star formation
rates (SFRs), and dust attenuation properties are investigated. The
evolution of EWrf([O ii]) closely follows the SFR density
evolution of the universe, with a trend of EWrf([O ii])
\propto (1 + z)3 up to redshift z ≃ 1, followed by a
possible flattening. The SF properties of the galaxies selected on the
basis of their [O ii] emission are compared with complementary samples
of SFGs selected by their MIR and FIR emission, and also with a general
mass-selected sample of galaxies at the same redshifts. We demonstrate
observationally that the UVJ diagram (or, similarly, a cut in the
specific SFR) is only partially able to distinguish the quiescent
galaxies from the SFGs. The SFR–M* relation is
investigated for the different samples, yielding a logarithmic slope
∼1, in good agreement with previous results. The dust attenuations
derived from different SFR indicators (UV(1600), UV(2800), [O ii], IR)
are compared and show clear trends with respect to both the stellar mass
and total SFR, with more massive and highly star-forming galaxies being
affected by stronger dust attenuation.
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Casiana
Muñoz Tuñón