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arXiv · 1507.07938

Pathways to quiescence: SHARDS view on the Star Formation Histories of massive quiescent galaxies at 1.0 < z < 1.5

Helena Domínguez Sánchez·Pablo G. Pérez-González·Pilar Esquej·M. Carmen Eliche-Moral·Guillermo Barro·Antonio Cava·Anton M. Koekemoer·Belén Alcalde Pampliega·Almudena Alonso Herrero·Gustavo Bruzual·Nicolás Cardiel·Javier Cenarro·Daniel Ceverino·Stéphane Charlot·Antonio Hernán Caballero
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Abstract

We present Star Formation Histories (SFHs) for a sample of 104 massive (stellar mass M > 10$^{10}$ M$_{\odot}$) quiescent galaxies (MQGs) at $z$=1.0-1.5 from the analysis of spectro-photometric data from the SHARDS and HST/WFC3 G102 and G141 surveys of the GOODS-N field, jointly with broad-band observations from ultraviolet (UV) to far-infrared (Far-IR). The sample is constructed on the basis of rest-frame UVJ colours and specific star formation rates (sSFR=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%) by galaxies with young mass-weighted ages, tM $<$ 2 Gyr, short star formation timescales, $\langle τ\rangle$ $\sim$ 60-200 Myr, and masses log(M/M$_{\odot}$) $\sim$ 10.5. There is an older population (15%) with tM$=$2 - 4 Gyr, longer star formation timescales, $\langle τ\rangle$$\sim$ 400 Myr, and larger masses, log(M/M$_{\odot}$) $\sim$ 10.7. The SFHs of our MQGs are consistent with the slope and the location of the Main Sequence (MS) 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 (LIRG) phase that lasts for $\sim$ 500 Myr, and half of them an Ultra Luminous Infrared Galaxy (ULIRG) phase for $\sim$ 100 Myr. We find that the MQG population is almost assembled at $z$ $\sim$ 1, and continues evolving passively with few additions to the population.

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Helena Domínguez Sánchez, Pablo G. Pérez-González, Pilar Esquej, M. Carmen Eliche-Moral, Guillermo Barro, Antonio Cava, Anton M. Koekemoer, Belén Alcalde Pampliega, Almudena Alonso Herrero, Gustavo Bruzual, Nicolás Cardiel, Javier Cenarro, Daniel Ceverino, Stéphane Charlot, Antonio Hernán Caballero. 2016-01-21. Pathways to quiescence: SHARDS view on the Star Formation Histories of massive quiescent galaxies at 1.0 < z < 1.5. https://doi.org/10.1093/mnras%2Fstw201

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