PANCHROMATIC ESTIMATION OF STAR FORMATION RATES IN BzK GALAXIES AT 1 < z < 3
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Kurczynski-2012-PANCHROMATIC ESTIMAT.pdf
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Author(s)
Kurczynski, Peter
Gawiser, Eric
Huynh, Minh
Ivison, Rob J.
Treister, Ezequiel
Smail, Ian
Blanc, Guillermo A.
Greve, Thomas R.
Schinnerer, Eva
Urry, Meg
Date Issued
April 2012
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Kurczynski, Peter, Eric Gawiser, Minh Huynh, Rob J. Ivison, Ezequiel Treister, Ian Smail, Guillermo A. Blanc, et al. “PANCHROMATIC ESTIMATION OF STAR FORMATION RATES IN BzK GALAXIES AT 1 < z < 3.” The Astrophysical Journal 750, no. 2 (April 23, 2012): 117. © 2012 The American Astronomical Society
Version
Final published version
Abstract
We determine star formation rates (SFRs) in a sample of color-selected, star-forming (sBzK) galaxies (K [subscript AB] < 21.8) in the Extended Chandra Deep Field-South. To identify and avoid active galactic nuclei, we use X-ray, IRAC color, and IR/radio flux ratio selection methods. Photometric redshift-binned, average flux densities are measured with stacking analyses in Spitzer-MIPS IR, BLAST and APEX/LABOCA submillimeter, VLA and GMRT radio, and Chandra X-ray data. We include averages of aperture fluxes in MUSYC UBVRIz'JHK images to determine UV-through-radio spectral energy distributions. We determine the total IR luminosities and compare SFR calibrations from FIR, 24 μm, UV, radio, and X-ray wavebands. We find consistency with our best estimator, SFR[subscript IR + UV], to within errors for the preferred radio SFR calibration. Our results imply that 24 μm only and X-ray SFR estimates should be applied to high-redshift galaxies with caution. Average IR luminosities are consistent with luminous infrared galaxies. We find SFR[subscript IR + UV] for our stacked sBzKs at median redshifts 1.4, 1.8, and 2.2 to be 55 ± 6 (random error), 74 ± 8, and 154 ± 17 M [subscript ☉] yr[superscript –1], respectively, with additional systematic uncertainty of a factor of ~2.
MIT Department
Massachusetts Institute of Technology. Department of Physics
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DOI of Published Version
https://doi.org/10.1088/0004-637x/750/2/117
