A modest view of dust at high redshifts Sangeeta Malhotra Steve Finkelstein (U Texas, A&M) Nimish Hathi (UC Riverside)

When doing high redshifts, rest-frame UV is the most accessible, and also the most variable.

Why we can even do this for whole galaxies Why we can even do this for whole galaxies? The intrinsic slope in the UV is fairly constant

Extinction correction matters for calculating Star-formation density and metal production e.g. Bouwens et al. 2006

Definitely see an evolution with redshift (Hathi, Malhotra, Rhoads 2008)

Relation between UV absorption and FIR emission Meurer et al.1997

Dust in Lyman-alpha emitters. (Finkelstein et al. 2009)

Finkelstein et al. 2009

Mass-dust relationship? Finkelstein, PhD Thesis 2008

Pannella et al. 2009 (astro-ph 0905.1674)

Manucci et al. 2008

2175 Angstrom feature Malhotra et al. 1997, detection of 2175 feature by coadding 90 MgII absorbers. No detection of 2175 feature using coaddition of 900 MgII absorbers in SDSS: York et al. 2006.

A few words from my sponsor Astro Faculty: Desch, Groppi, Malhotra, Rhoads, Scannapieco, Starrfield, Timmes, Windhorst, Young Planetary / solar system: Christiansen, Greeley, Robinson, Wadhwa. 25 assorted geologists, 5 engineers. http://SESE.ASU.EDU