CaII Absorbers in the Sloan Digital Sky Survey: Element Abundances and Dust

TL;DR

This study analyzes CaII absorbers in SDSS data, revealing two distinct populations with different physical properties and dust content, contributing to understanding galaxy halo and disk gas characteristics.

Contribution

It identifies two physically different CaII absorber populations based on equivalent width, and characterizes their element abundances and dust extinction properties.

Findings

Weaker absorbers resemble halo gas with lower dust extinction.

Stronger absorbers show properties between halo and disk gas.

Stronger absorbers are nearly 6 times more reddened than weaker ones.

Abstract

We present measurements of element abundance ratios and dust in CaII~absorbers identified in SDSS DR7+DR9. In an earlier paper we formed a statistical sample of 435 CaII absorbers and postulated that their statistical properties might be representative of at least two populations of absorbers. Here we show that if the absorbers are roughly divided into two subsamples with CaII rest equivalent widths larger and smaller than $W_0^{\lambda 3934} = 0.7$ \AA, they are then representative of two physically different populations. Comparisons of abundance ratios between the two CaII absorber populations indicate that the weaker $W_0^{\lambda 3934}$ absorbers have properties consistent with halo-type gas, while the stronger absorbers have properties intermediate between halo- and disk-type gas. We also show that, on average, the dust extinction properties of the overall sample is consistent with a LMC or SMC dust law, and the stronger absorbers are nearly 6 times more reddened than their weaker counterparts. The absorbed-to-unabsorbed composite flux ratio at $\lambda_{rest} = 2200$ \AA\ is $\mathcal{R} \approx 0.73$ and $E(B-V) \approx 0.046$ for the stronger CaII absorbers ($W_0^{\lambda 3934} \ge 0.7$ \AA), and $\mathcal{R} \approx 0.95$ and $E(B-V) \approx 0.011$ for the weaker CaII absorbers ($W_0^{\lambda 3934} < 0.7$ \AA).