A CANDELS-3D-HST SYNERGY: RESOLVED STAR FORMATION PATTERNS AT 0.7 < z < 1.5

We analyze the resolved stellar populations of 473 massive star-forming galaxies at 0.7 < z < 1.5, with multi-wavelength broadband imaging from CANDELS and H alpha surface brightness profiles at the same kiloparsec resolution from 3D-HST. We find the H alpha morphologies to resemble more close...

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Bibliographic Details
Published in:The Astrophysical journal 2013-12, Vol.779 (2), p.1-16
Main Authors: Wuyts, Stijn, SCHREIBER, NATASCHA M FORSTER, Nelson, Erica J, van Dokkum, Pieter G, Brammer, Gabe, Chang, Yu-Yen, Faber, Sandra M, Ferguson, Henry C, Franx, Marijn, Fumagalli, Mattia
Format: Article
Language:English
Subjects:
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BRIGHTNESS
Broadband
Clumps
COLOR
COMPARATIVE EVALUATIONS
CORRECTIONS
DENSITY
Deviation
Dust
DUSTS
Equivalence
GALAXIES
LUMINOSITY
MASS
MONOCHROMATIC RADIATION
RED SHIFT
RESOLUTION
Star formation
STARS
SURFACES
VISIBLE RADIATION
WAVELENGTHS
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Summary:We analyze the resolved stellar populations of 473 massive star-forming galaxies at 0.7 < z < 1.5, with multi-wavelength broadband imaging from CANDELS and H alpha surface brightness profiles at the same kiloparsec resolution from 3D-HST. We find the H alpha morphologies to resemble more closely those observed in the ACS I band than in the WFC3 H band, especially for the larger systems. We next derive a novel prescription for H alpha dust corrections, which accounts for extra extinction toward H II regions. Deviations from this relation toward lower equivalent widths are found in the inner regions of galaxies. Their H alpha /UV luminosity ratio is lower than that of the underlying disk, suggesting that the ACS clump selection preferentially picks up those regions of elevated star formation activity that are the least obscured by dust. Our analysis emphasizes that monochromatic studies of galaxy structure can be severely limited by mass-to-light ratio variations due to dust and spatially inhomogeneous star formation histories.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/779/2/135