Gaps in the cloud cover? Comparing extinction measures in spiral disks

TL;DR

This study compares two methods of measuring dust extinction in galaxy disks to understand the distribution and structure of interstellar dust, revealing that infrared color maps underestimate dust presence due to assumptions about dust geometry.

Contribution

It introduces a comparative analysis of stellar reddening and background galaxy counts to assess dust distribution in galaxy disks, highlighting limitations of infrared color mapping.

Findings

Distant background galaxies are found mainly in low-extinction regions.

Infrared color maps underestimate total dust content due to dust geometry assumptions.

Dust structures are primarily associated with spiral arms and diffuse disk components.

Abstract

Dust in galaxies can be mapped by either the FIR/sub-mm emission, the optical or infrared reddening of starlight, or the extinction of a known background source. We compare two dust extinction measurements for a set of fifteen sections in thirteen nearby galaxies, to determine the scale of the dusty ISM responsible for disk opacity: one using stellar reddening and the other a known background source. In our earlier papers, we presented extinction measurements of 29 galaxies, based on calibrated counts of distant background objects identified though foreground disks in HST/WFPC2 images. For the 13 galaxies that overlap with the Spitzer Infrared Nearby Galaxies Survey (SINGS), we now compare these results with those obtained from an I-L color map. Our goal is to determine whether or not a detected distant galaxy indicates a gap in the dusty ISM, and hence to better understand the nature and geometry of the disk extinction. We find that distant galaxies are predominantly in low-extinction sections marked by the color maps, indicating that their number depends both on the cloud cover of {\it Spitzer}-resolved dust structures --mostly the spiral arms--and a diffuse, unresolved underlying disk. We note that our infrared color map (E[I-L]) underestimates the overall dust presence in these disks severely, because it implicitly assumes the presence of a dust screen in front of the stellar distribution.