Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 499, Issue 2, Pages 2896-2911Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa2648
Keywords
galaxies: evolution; galaxies: fundamental parameters; galaxies: luminosity function, mass function; galaxies: statistics; galaxies: stellar content
Categories
Funding
- Australian Government through an Australian Research Council Future Fellowship [FT150100269]
- Vici grant - Netherlands Organisation for Scientific Research (NWO) [639.043.512]
- European Union'sHorizon 2020 research and innovation programme [792916]
- DutchMinistry of Education, Culture and Science (OCW)
- Heisenberg grant of the Deutsche Forschungsgemeinschaft [Hi 1495/5-1]
- ERC Consolidator Grant [770935]
- Agencia Nacional de Investigacion y Desarrollo (ANID) through FONDECYT Iniciacion grant [11191125]
- STFC [ST/M000907/1, ST/R000700/1] Funding Source: UKRI
- Marie Curie Actions (MSCA) [792916] Funding Source: Marie Curie Actions (MSCA)
- Australian Research Council [FT150100269] Funding Source: Australian Research Council
Ask authors/readers for more resources
We use KiDS weak lensing data to measure variations in mean halo mass as a function of several key galaxy properties (namely stellar colour, specific star formation rate, Sersic index, and effective radius) for a volume-limited sample of GAMA galaxies in a narrow stellar mass range [M* similar to (2-5) x 10(10) M-circle dot]. This mass range is particularly interesting, inasmuch as it is where bimodalities in galaxy properties are most pronounced, and near to the break in both the galaxy stellar mass function and the stellar-to-halo mass relation (SHMR). In this narrow mass range, we find that both size and Sersic index are better predictors of halo mass than either colour or SSFR, with the data showing a slight preference for Sersic index. In other words, we find that mean halo mass is more tightly correlated with galaxy structure than either past star formation history or current star formation rate. Our results lead to an approximate lower bound on the dispersion in halo masses among logM* approximate to 10.5 galaxies: We find that the dispersion is greater than or similar to 0.3 dex. This would imply either that offsets from the mean SHMR are closely coupled to size/structure or that the dispersion in the SHMR is larger than what past results have suggested. Our results thus provide new empirical constraints on the relationship between stellar and halo mass assembly at this particularly interesting mass range.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available