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Evolution in the Colors of Lyman-Break Galaxies from Z~4 to Z~3 | Casey Papovich
; Mark Dickinson
; Henry C. Ferguson
; Mauro Giavalisco
; Jennifer Lotz
; Piero Madau
; Rafal Idzi
; Claudia Kretchmer
; Leonidas A. Moustakas
; Duilia F. de Mello
; Jonathan P. Gardner
; Marcia J. Rieke
; Rachel S. Somerville
; Daniel Stern
; | Date: |
30 Oct 2003 | Journal: | Astrophys.J. 600 (2004) L111-L114 | Subject: | astro-ph | Affiliation: | 2 and 3), Henry C. Ferguson (2 and 3), Mauro Giavalisco , Jennifer Lotz , Piero Madau , Rafal Idzi , Claudia Kretchmer , Leonidas A. Moustakas , Duilia F. de Mello , Jonathan P. Gardner , Marcia J. Rieke , Rachel S. Somerville , Daniel Stern ( Stewar | Abstract: | The integrated colors of distant galaxies provide a means for interpreting the properties of their stellar content. Here, we use rest-frame UV-to-optical colors to constrain the spectral-energy distributions and stellar populations of color-selected, B-dropout galaxies at z ~ 4 in the Great Observatories Origins Deep Survey. We combine the ACS data with ground-based near-infrared images, which extend the coverage of galaxies at z ~ 4 to the rest-frame B-band. We observe a color-magnitude trend in the rest-frame m(UV) - B versus B diagram for the z ~ 4 galaxies that has a fairly well-defined "blue-envelope", and is strikingly similar to that of color-selected, U-dropout galaxies at z ~ 3. We also find that although the co-moving luminosity density at rest-frame UV wavelengths (1600 Angstroms) is roughly comparable at z ~ 3 and z ~ 4, the luminosity density at rest-frame optical wavelengths increases by about one-third from z ~ 4 to z ~ 3. Although the star-formation histories of individual galaxies may involve complex and stochastic events, the evolution in the global luminosity density of the UV-bright galaxy population corresponds to an average star-formation history with a star-formation rate that is constant or increasing over these redshifts. This suggests that the evolution in the luminosity density corresponds to an increase in the stellar-mass density of more than 33%. | Source: | arXiv, astro-ph/0310888 | Services: | Forum | Review | PDF | Favorites |
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