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

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

3. 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

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

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

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

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

8. Finkelstein et al. 2009

9. Mass-dust relationship?
Finkelstein, PhD Thesis 2008

10. Pannella et al. 2009 (astro-ph 0905.1674)

11. Manucci et al. 2008

12. 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

13. 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.