The dust mass function from z~0 to z~2. (arXiv:1909.11333v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Pozzi_F/0/1/0/all/0/1">F. Pozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calura_F/0/1/0/all/0/1">F. Calura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zamorani_G/0/1/0/all/0/1">G. Zamorani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delvecchio_I/0/1/0/all/0/1">I. Delvecchio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruppioni_C/0/1/0/all/0/1">C. Gruppioni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Santini_P/0/1/0/all/0/1">P. Santini</a>
We derive for the first time the dust mass function (DMF) in a wide redshift We derive for the first time the dust mass function (DMF) in a wide redshift http://arxiv.org/icons/sfx.gif
range, from z~0.2 up to z~2.5. In order to trace the dust emission, we start
from a far-IR (160-um) Herschel selected catalogue in the COSMOS field. We
estimate the dust masses by fitting the far-IR data (lam_rest>50um) with a
modified black body function and we present a detailed analysis to take into
account the incompleteness in dust masses from a far-IR perspective. By
parametrizing the observed DMF with a Schechter function in the redshift range
0.1
range, from z~0.2 up to z~2.5. In order to trace the dust emission, we start
from a far-IR (160-um) Herschel selected catalogue in the COSMOS field. We
estimate the dust masses by fitting the far-IR data (lam_rest>50um) with a
modified black body function and we present a detailed analysis to take into
account the incompleteness in dust masses from a far-IR perspective. By
parametrizing the observed DMF with a Schechter function in the redshift range
0.1<z<0.25, where we are able to sample faint dust masses, we measure a steep
slope (alpha~1.48), as found by the majority of works in the Local Universe. We
detect a strong dust mass evolution, with M_d^star at z~2.5 almost one dex
larger than in the local Universe, combined with a decrease in their number
density. Integrating our DMFs we estimate the dust mass density (DMD), finding
a broad peak at z~1, with a decrease by a factor of ~3 towards z~0 and z~2.5.
In general, the trend found for the DMD mostly agrees with the derivation of
Driver et al. (2018), another DMD determination based also on far-IR
detections, and with other measures based on indirect tracers.
