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Pathways to quiescence: SHARDS view on the star formation histories of massive quiescent galaxies at 1.0 < z < 1.5

AuthorsDomínguez-Sánchez, H.; Pérez-González, Pablo G.; Esquej, Pilar ; Cava, Antonio; Alonso-Herrero, A. ; Cardiel, Nicolás; Cenarro, A. J.; Ceverino, Daniel; Hernán-Caballero, Antonio
KeywordsGalaxies: stellar content
Galaxies: evolution
Galaxies: formation
Galaxies: high-redshift
Issue Date2016
PublisherOxford University Press
CitationMonthly Notices of the Royal Astronomical Society 457(4): 3743-3768 (2016)
AbstractWe present star formation histories (SFHs) for a sample of 104 massive (stellar massM> 1010 M) quiescent galaxies (MQGs) at z = 1.0-1.5 from the analysis of spectrophotometric data from the Survey for High-z Absorption Red and Dead Sources (SHARDS) and HST/WFC3 G102 and G141 surveys of the GOODS-North field, jointly with broad-band observations from ultraviolet (UV) to far-infrared (far-IR). The sample is constructed on the basis of restframe UVJ colours and specific star formation rates (sSFRs = SFR/Mass). The spectral energy distributions (SEDs) of each galaxy are compared to models assuming a delayed exponentially declining SFH. A Monte Carlo algorithm characterizes the degeneracies, which we are able to break taking advantage of the SHARDS data resolution, by measuring indices such as MgUV and D4000. The population of MQGs shows a duality in their properties. The sample is dominated (85 per cent) by galaxies with young mass-weighted ages, t < 2 Gyr, short star formation time-scales, (τ) ~ 60-200 Myr, and masses log(M/M) ~ 10.5. There is an older population (15 per cent) with t = 2-4 Gyr, longer star formation time-scales, (τ) ~ 400 Myr, and larger masses, log(M/M) ~ 10.7. The SFHs of our MQGs are consistent with the slope and the location of the main sequence of star-forming galaxies at z > 1.0, when our galaxies were 0.5-1.0 Gyr old. According to these SFHs, all the MQGs experienced a luminous infrared galaxy phase that lasts for ~500 Myr, and half of them an ultraluminous infrared galaxy phase for ~100 Myr. We find that the MQG population is almost assembled at z ~ 1, and continues evolving passively with few additions to the population.
Descriptionet al.
Publisher version (URL)https://doi.org/10.1093/mnras/stw201
Identifiersdoi: 10.1093/mnras/stw201
e-issn: 1365-2966
issn: 0035-8711
Appears in Collections:(CAB) Artículos
(IFCA) Artículos
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