Star formation in Herschel's Monsters versus semi-analytic models
Date Issued
2015
Author(s)
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Pozzi, F.
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Berta, S.
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Franceschini, A.
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Marchetti, L.
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Vaccari, M.
Description
CG and FP acknowledge financial contribution from the contracts PRIN-INAF 1.06.09.05 and ASI-INAF I00507/1 and I005110. FF acknowledges financial support from the grants PRIN MIUR 2009 ‘The Intergalactic Medium as a probe of the growth of cosmic structures’ and PRIN INAF 2010 ‘From the dawn of galaxy formation’. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
Abstract
We present a direct comparison between the observed star formation rate functions (SFRFs) and the state-of-the-art predictions of semi-analytic models (SAMs) of galaxy formation and evolution. We use the PACS Evolutionary Probe Survey and Herschel Multi-tiered Extragalactic Survey data sets in the COSMOS and GOODS-South fields, combined with broad-band photometry from UV to sub-mm, to obtain total (IR+UV) instantaneous star formation rates (SFRs) for individual Herschel galaxies up to z ̃ 4, subtracted of possible active galactic nucleus (AGN) contamination. The comparison with model predictions shows that SAMs broadly reproduce the observed SFRFs up to z ̃ 2, when the observational errors on the SFR are taken into account. However, all the models seem to underpredict the bright end of the SFRF at z ≳ 2. The cause of this underprediction could lie in an improper modelling of several model ingredients, like too strong (AGN or stellar) feedback in the brighter objects or too low fallback of gas, caused by weak feedback and outflows at earlier epochs.
Volume
451
Issue
4
Start page
3419
Issn Identifier
0035-8711
Ads BibCode
2015MNRAS.451.3419G
Rights
open.access
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