LoCuSS: exploring the connection between local environment, star formation and dust mass in Abell 1758. (arXiv:2001.04478v1 [astro-ph.GA])

LoCuSS: exploring the connection between local environment, star formation and dust mass in Abell 1758. (arXiv:2001.04478v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bianconi_M/0/1/0/all/0/1">Matteo Bianconi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_G/0/1/0/all/0/1">Graham P. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haines_C/0/1/0/all/0/1">Chris P. Haines</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McGee_S/0/1/0/all/0/1">Sean L. McGee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Finoguenov_A/0/1/0/all/0/1">Alexis Finoguenov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Egami_E/0/1/0/all/0/1">Eiichi Egami</a>

We explore the connection between dust and star formation, in the context of
environmental effects on galaxy evolution. In particular, we exploit the
susceptibility of dust to external processes to assess the influence of dense
environment on star-forming galaxies. We have selected cluster Abell 1758 from
the Local Cluster Substructure Survey (LoCuSS). Its complex dynamical state is
an ideal test-bench to track dust removal and destruction in galaxies due to
merger and accretion shocks. We present a systematic panchromatic study (from
0.15 $rm mu$m with GALEX to 500 $rm mu$m with Herschel) of
spectroscopically confirmed star-forming cluster galaxies at intermediate
redshift. We observe that the main subclusters (A1758N and A1758S) belong to
two separate large-scale structures, with no overlapping galaxy members.
Star-forming cluster members are distributed preferentially outside cluster
central regions, and are not grouped in substructures. Rather, these galaxies
are being funneled towards the main subclusters along separate accretion
filaments. Additionally, we present the first study of dust-to-stellar (DTS)
mass ratio used as indicator for local environmental influence on galaxy
evolution. Star-forming cluster members show lower mean values (32% at 2.4$rm
sigma$) of DTS mass ratio and lower levels of infrared emission from birth
clouds with respect to coeval star-forming field galaxies. This picture is
consistent with the majority of star-forming cluster members infalling in
isolation. Upon accretion, star-formation is observed to decrease and warm dust
is destroyed due to heating from the intracluster medium radiation,
ram-pressure stripping and merger shocks.

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