The dust attenuation curve versus stellar mass for emission line galaxies at z ∼ 2
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802 (United States)
- Department of Physics and Astronomy, Rutgers, The State University of New Jersey, Piscataway, NJ 08854 (United States)
We derive the mean wavelength dependence of stellar attenuation in a sample of 239 high redshift (1.90<2.35) galaxies selected via Hubble Space Telescope WFC3 IR grism observations of their rest-frame optical emission lines. Our analysis indicates that the average reddening law follows a form similar to that derived by Calzetti et al. for local starburst galaxies. However, over the mass range 7.2≲logM/M{sub ⊙}≲10.2, the slope of the attenuation law in the ultraviolet (UV) is shallower than that seen locally, and the UV slope steepens as the mass increases. These trends are in qualitative agreement with Kriek and Conroy, who found that the wavelength dependence of attenuation varies with galaxy spectral type. However, we find no evidence of an extinction “bump” at 2175 Å in any of the three stellar mass bins, or in the sample as a whole. We quantify the relation between the attenuation curve and stellar mass and discuss its implications.
- OSTI ID:
- 22882376
- Journal Information:
- Astrophysical Journal, Vol. 814, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Since 2009, the country of publication for this journal is the UK.; ISSN 0004-637X
- Country of Publication:
- United Kingdom
- Language:
- English
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