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This article is based on an invited talk given by V. P. Kulkarni at the 8thCosmic Dust meeting. Dust has a profound effect on the physics and chemistry ofthe interstellar gas in galaxies and on the appearance of galaxies.Understanding the cosmic evolution of dust with time is therefore crucial forunderstanding the evolution of galaxies. Despite the importance of interstellardust, very little is known about its nature and composition in distantgalaxies. We summarize the results of our ongoing programs using observationsof distant quasars to obtain better constraints on dust grains in foregroundgalaxies that happen to lie along the quasar sightlines. These observationsconsist of a combination of mid-infrared data obtained with the Spitzer SpaceTelescope and optical/UV data obtained with ground-based telescopes and/or theHubble Space Telescope. The mid-IR data target the 10 $\mu$m and 18 $\mu$msilicate absorption features, while the optical/UV data allow determinations ofelement depletions, extinction curves, 2175 {\AA} bumps, etc. Measurements ofsuch properties in absorption-selected galaxies with redshifts ranging from$z\sim0$ to $z>2$ provide constraints on the evolution of interstellar dustover the past $> 10$ Gyr. The optical depth of the 10 $\mu$m silicateabsorption feature ($\tau_{10}$) in these galaxies is correlated with theamount of reddening along the sightline. But there are indications [e.g., basedon the $\tau_{10}$ /$E(B-V)$ ratio and possible grain crystallinity] that thedust in these distant galaxies differs in structure and composition from thedust in the Milky Way and the Magellanic Clouds. We briefly discuss theimplications of these results for the evolution of galaxies and their starformation history.

Probing the Interstellar Dust in Galaxies over > 10 Gyr of Cosmic History