期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 440, 期 2, 页码 1880-1898出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu212
关键词
methods: statistical; galaxies: fundamental parameters; galaxies: luminosity function; mass function; galaxies: photometry; galaxies: statistics; galaxies: stellar content
资金
- European Research Council
- European Career Re-integration Grant
- EC [312725]
- National Science Foundation [PHYS-1066293]
- STFC [ST/L000695/1, ST/I001212/1, ST/F007043/1, ST/J001422/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/J001422/1, ST/L000695/1, ST/F007043/1, ST/I001212/1] Funding Source: researchfish
We present a new method to classify the broad-band optical-near-infrared spectral energy distributions (SEDs) of galaxies using three shape parameters (super-colours) based on a principal component analysis of model SEDs. As well as providing a compact representation of the wide variety of SED shapes, the method allows for easy visualization of information loss and biases caused by the incomplete sampling of the rest-frame SED as a function of redshift. We apply the method to galaxies in the United Kingdom Infrared Telescope Infrared Deep Sky Survey Ultra Deep Survey with 0.9 < z < 1.2, and confirm our classifications by stacking rest-frame optical spectra for a fraction of objects in each class. As well as cleanly separating a tight red sequence from star-forming galaxies, three unusual populations are identifiable by their unique colours: very dusty star-forming galaxies with high metallicity and old mean stellar age; post-starburst galaxies which have formed greater than or similar to 10 per cent of their mass in a recent unsustained starburst event; and metal-poor quiescent dwarf galaxies. We find that quiescent galaxies account for 45 per cent of galaxies with log M*/M-circle dot > 11, declining steadily to 13 per cent at log M*/M-circle dot = 10. The properties and mass function of the post-starburst galaxies are consistent with a scenario in which gas-rich mergers contribute to the growth of the low- and intermediate-mass range of the red sequence.
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