Galaxy and Mass Assembly (GAMA): the stellar mass budget of galaxy spheroids and discs
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We build on a recent photometric decomposition analysis of 7506 Galaxy and Mass Assembly (GAMA) survey galaxies to derive stellar mass function fits to individual spheroid and disc component populations down to a lower mass limit of log(M*/M⊙) = 8. We find that the spheroid/disc mass distributions for individual galaxy morphological types are well described by single Schechter function forms. We derive estimates of the total stellar mass densities in spheroids (ρspheroid = 1.24 ± 0.49 × 108 M⊙ Mpc -3h0.7) and discs (ρdisc = 1.20 ± 0.45 × 108 M⊙ Mpc -3h0.7), which translates to approximately 50 per cent of the local stellar mass density in spheroids and 48 per cent in discs. The remaining stellar mass is found in the dwarf 'little blue spheroid' class, which is not obviously similar in structure to either classical spheroid or disc populations. We also examine the variation of component mass ratios across galaxy mass and group halo mass regimes, finding the transition from spheroid to disc mass dominance occurs near galaxy stellar mass ~1011 M⊙ and group halo mass ~1012.5 M⊙h-1. We further quantify the variation in spheroid-to-total mass ratio with group halo mass for central and satellite populations as well as the radial variation of this ratio within groups.
Moffett , A J , Lange , R , Driver , S P , Robotham , A S G , Kelvin , L S , Alpaslan , M , Andrews , S K , Bland-Hawthorn , J , Brough , S , Cluver , M E , Colless , M , Davies , L J M , Holwerda , B W , Hopkins , A M , Kafle , P R , Liske , J & Meyer , M 2016 , ' Galaxy and Mass Assembly (GAMA): the stellar mass budget of galaxy spheroids and discs ' , Monthly Notices of the Royal Astronomical Society , vol. 462 , no. 4 , pp. 4336-4348 . https://doi.org/10.1093/mnras/stw1861
Monthly Notices of the Royal Astronomical Society
© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.1093/mnras/stw1861
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