Dust accretion and destruction in galaxy groups and clusters

TL;DR

This study investigates the distribution and properties of dust in galaxy groups and clusters using SDSS data, revealing how dust content varies with halo mass and is affected by destruction processes.

Contribution

It provides the first large-scale measurement of dust distribution around galaxy groups and clusters, showing the dust-to-gas ratio decreases with increasing halo mass and suggesting dust destruction mechanisms.

Findings

Dust detected out to 30 Mpc/h in all SDSS colours.

Dust-to-gas ratio is about 3% in massive clusters and 55% in small groups.

Dust covering fraction is approximately 10%, decreasing towards cluster centers.

Abstract

We examine the dust distribution around a sample of 70,000 low redshift galaxy groups and clusters derived from the Sloan Digital Sky Survey. By correlating spectroscopically identified background quasars with the galaxy groups we obtain the relative colour excess due to dust reddening. We present a significant detection of dust out to a clustercentric distance of 30 Mpc/h in all four independent SDSS colours, consistent with the expectations of weak lensing masses of similar mass halos and excess galaxy counts. The wavelength dependence of this colour excess is consistent with the expectations of a Milky Way dust law with R_V=3.1. Further, we find that the halo mass dependence of the dust content is much smaller than would be expected by a simple scaling, implying that the dust-to-gas ratio of the most massive clusters (~10E14 Msun/h) is ~3% of the local ISM value, while in small groups (~10E12.7 Msun/h) it is ~55% of the local ISM value. We also find that the dust must have a covering fraction on the order of 10% to explain the observed color differences, which means the dust is not just confined to the most massive galaxies. Comparing the dust profile with the excess galaxy profile, we find that the implied dust-to-galaxy ratio falls significantly towards the group or cluster center. This has a significant halo mass dependence, such that the more massive groups and clusters show a stronger reduction. This suggests that either dust is destroyed by thermal sputtering of the dust grains by the hot, dense gas or the intrinsic dust production is reduced in these galaxies.