期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 404, 期 1, 页码 247-252出版社
WILEY-BLACKWELL
DOI: 10.1111/j.1365-2966.2010.16266.x
关键词
galaxies: evolution; galaxies: general; galaxies: ISM
资金
- NSF [AST95-09298, AST-0071048, AST-0071198, AST-0507428, AST-0507483]
- NASA LTSA [NNG04GC89G]
- W. M. Keck Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0908368] Funding Source: National Science Foundation
A novel technique is employed for estimating attenuation curves in galaxies where only photometry and spectroscopic redshifts are available. This technique provides a powerful measure of particular extinction features such as the UV bump at 2175 angstrom, which has been observed in environments ranging from the MilkyWay to high-redshift star-forming galaxies. Knowledge of the typical strength of the UV bump as a function of environment and redshift is crucial for converting rest-frame UV flux into star formation rates. The UV bump will impart a unique signature as it moves through various filters due to redshifting; its presence can therefore be disentangled from other stellar population effects. The utility of this technique is demonstrated with a large sample of galaxies drawn from the DEEP2 Galaxy Redshift Survey. The observed B - R colour of star-forming galaxies at 0.6 < z < 1.4 disfavours the presence of a UV bump as strong as observed in the Milky Way, and instead favours rest-frame UV (1800 angstrom < lambda < 3000 angstrom) attenuation curves similar to the Milky Way without a UV bump, a power law with index delta = - 0.7, or a form advocated by Calzetti and collaborators. Stronger constraints on the strength of the UV bump in galaxies can be achieved if independent constraints on the V-band optical depth are available.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据