Reddy, N. and Dickinson, M. and Elbaz, D. and Morrison, G. and Giavalisco, M. and Ivison, R. and Papovich, C. and Scott, D. and Buat, V. and Burgarella, D. and Charmandaris, V. and Daddi, E. and Magdis, G. and Murphy, E. and Altieri, B. and Aussel, H. and Dannerbauer, H. and Dasyra, K. and Hwang, H. S. and Kartaltepe, J. and Leiton, R. and Magnelli, B. and Popesso, P. (2012) GOODS-Herschel Measurements of the Dust Attenuation of Typical Star-forming Galaxies at High Redshift: Observations of Ultraviolet-selected Galaxies at z ~ 2. Astrophysical Journal, 744 (2). p. 154. ISSN 0004-637X http://resolver.caltech.edu/CaltechAUTHORS:20120130-114106930
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We take advantage of the sensitivity and resolution of the Herschel Space Observatory at 100 and 160 μm to directly image the thermal dust emission and investigate the infrared luminosities (L_IR) and dust obscuration of typical star-forming (L*) galaxies at high redshift. Our sample consists of 146 UV-selected galaxies with spectroscopic redshifts 1.5 ≤ z_spec < 2.6 in the GOODS-North field. Supplemented with deep Very Large Array and Spitzer imaging, we construct median stacks at the positions of these galaxies at 24, 100, and 160 μm, and 1.4 GHz. The comparison between these stacked fluxes and a variety of dust templates and calibrations implies that typical star-forming galaxies with UV luminosities L_UV ≳ 10^(10) L_☉ at z ~ 2 are luminous infrared galaxies with a median L_IR = (2.2 ± 0.3) × 10^(11) L_☉. Their median ratio of L IR to rest-frame 8 μm luminosity (L_8) is L_(IR)/L_8 = 8.9 ± 1.3 and is ≈80% larger than that found for most star-forming galaxies at z ≲ 2. This apparent redshift evolution in the L_(IR)/L_8 ratio may be tied to the trend of larger infrared luminosity surface density for z ≳ 2 galaxies relative to those at lower redshift. Typical galaxies at 1.5 ≤ z < 2.6 have a median dust obscuration L_(IR)/L_(UV) = 7.1 ± 1.1, which corresponds to a dust correction factor, required to recover the bolometric star formation rate (SFR) from the unobscured UV SFR, of 5.2 ± 0.6. This result is similar to that inferred from previous investigations of the UV, Hα, 24 μm, radio, and X-ray properties of the same galaxies studied here. Stacking in bins of UV slope (β) implies that L* galaxies with redder spectral slopes are also dustier and that the correlation between β and dustiness is similar to that found for local starburst galaxies. Hence, the rest-frame ≃30 and 50 μm fluxes validate on average the use of the local UV attenuation curve to recover the dust attenuation of typical star-forming galaxies at high redshift. In the simplest interpretation, the agreement between the local and high-redshift UV attenuation curves suggests a similarity in the dust production and stellar and dust geometries of starburst galaxies over the last 10 billion years.
|Additional Information:||© 2012 American Astronomical Society. Received 2011 July 8; accepted 2011 October 26; published 2011 December 22. Support for N.A.R. was provided by NASA through Hubble Fellowship grant HST-HF-01223.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. This work is based on observations made with the Herschel Space Observatory, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.|
|Subject Keywords:||dust; extinction; galaxies: high-redshift; infrared: galaxies|
|Official Citation:||GOODS-Herschel Measurements of the Dust Attenuation of Typical Star-forming Galaxies at High Redshift: Observations of Ultraviolet-selected Galaxies at z ~ 2 N. Reddy et al. 2012 ApJ 744 154|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||30 Jan 2012 22:36|
|Last Modified:||26 Dec 2012 14:45|
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