English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We examine the dust distribution around a sample of 70 000 low‐redshift galaxy groups and clusters derived from the Sloan Digital Sky Survey (SDSS). 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 cluster‐centric distance of 30 Mpc   h  −1   in all four independent SDSS colours, consistent with the expectations of weak‐lensing masses of similar mass haloes 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  (∼10 14   h  −1  M ⊙ )  is ∼3 per cent of the local interstellar medium (ISM) value, while in small groups  (∼10 12.7   h  −1  M ⊙ )  it is ∼55 per cent of the local ISM value. We also find that the dust must have a covering fraction of the order of 10 per cent to explain the observed colour 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 centre. 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.

Dust accretion and destruction in galaxy groups and clusters