Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 475, Issue 1, Pages 735-747Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx3165
Keywords
galaxies: bulges; galaxies: evolution; galaxies: star formation; galaxies: structure; galaxies: luminosity function, mass function
Categories
Funding
- CNPq [152120/2016-5]
- CNPq (through PCI-DA) [302388/2013-3]
- Foundation for Science and Technology (FCT Portugal) [PTDC/F1S/100170/2008]
- Netherlands Organisation for Scientific research (NWO) through a Veni fellowship
- Science and Technology Foundation (FCT. Portugal) [PTDC/FIS-AST/2194/2012, DID/EIS/04434/2013, SERWEPD/95578/2013, PD/BD/52706/2014]
- Portuguese Science and Technology Foundation (FCT, Portugal) [PTDC/CTE-AST/105287/2008]
- program CSF - CONF
- CNPq (PCINICT/ON program)
- STFC [ST/P00038X/1, ST/R000514/1] Funding Source: UKRI
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Combining the catalogue of galaxy morphologies in the COSMOS field and the sample of H alpha emitters at redshifts z = 0.4 and z = 0.84 of the HiZELS survey, we selected similar to 220 star-forming bulgeless systems (Sdrsic index n <= 1.5) at both epochs. We present their star formation properties and we investigate their contribution to the star formation rate function (SFRF) and global star formation rate density (SFRD) at z < 1. For comparison, we also analyse H alpha emitters with more structurally evolved morphologies that we split into two classes according to their Sdrsic index n: intermediate (1.5 < n <= 3) and bulge-dominated (n > 3). At both redshifts, the SFRF is dominated by the contribution of bulgeless galaxies and we show that they account for more than 60 per cent of the cosmic SFRD at z < 1. The decrease of the SFRD with redshift is common to the three morphological types, but it is stronger for bulge-dominated systems. Star-forming bulgeless systems are mostly located in regions of low to intermediate galaxy densities (Sigma similar to 1-4 Mpc(-2)) typical of field-like and filament-like environments and their specific star formation rates (sSFRs) do not appear to vary strongly with local galaxy density. Only few bulgeless galaxies in our sample have high (sSFR > 10(-9) yr(-1)) and these are mainly low-mass systems. Above M-* similar to 10(10) M circle dot bulgeless are evolving at a 'normal' rate (10(-9) yr(-1) < sSFR < 10(-10) yr(-1)) and in the absence of an external trigger (i.e. mergers/strong interactions) they might not be able to develop a central classical bulge.
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