A Radio-selected Population of Dark, Long Gamma-ray Bursts: Comparison to the Long Gamma-ray Burst Population and Implications for Host Dust Distributions. (arXiv:2205.01124v2 [astro-ph.HE] UPDATED)

A Radio-selected Population of Dark, Long Gamma-ray Bursts: Comparison to the Long Gamma-ray Burst Population and Implications for Host Dust Distributions. (arXiv:2205.01124v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Schroeder_G/0/1/0/all/0/1">Genevieve Schroeder</a> (Northwestern/CIERA), <a href="http://arxiv.org/find/astro-ph/1/au:+Laskar_T/0/1/0/all/0/1">Tanmoy Laskar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fong_W/0/1/0/all/0/1">Wen-fai Fong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nugent_A/0/1/0/all/0/1">Anya E. Nugent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berger_E/0/1/0/all/0/1">Edo Berger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chornock_R/0/1/0/all/0/1">Ryan Chornock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alexander_K/0/1/0/all/0/1">Kate D. Alexander</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrews_J/0/1/0/all/0/1">Jennifer Andrews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bussmann_R/0/1/0/all/0/1">R. Shane Bussmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castro_Tirado_A/0/1/0/all/0/1">Alberto J. Castro-Tirado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goyal_A/0/1/0/all/0/1">Armaan V. Goyal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kilpatrick_C/0/1/0/all/0/1">Charles D. Kilpatrick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lally_M/0/1/0/all/0/1">Maura Lally</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_A/0/1/0/all/0/1">Adam Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milne_P/0/1/0/all/0/1">Peter Milne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paterson_K/0/1/0/all/0/1">Kerry Paterson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Escorial_A/0/1/0/all/0/1">Alicia Rouco Escorial</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stroh_M/0/1/0/all/0/1">Michael C. Stroh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Terreran_G/0/1/0/all/0/1">Giacomo Terreran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zauderer_B/0/1/0/all/0/1">Bevin Ashley Zauderer</a>

We present cm-band and mm-band afterglow observations of five long-duration
$gamma$-ray bursts (GRBs; GRB 130131A, 130420B, 130609A, 131229A, 140713A)
with dust-obscured optical afterglow emission, known as “dark” GRBs. We detect
the radio afterglow of two of the dark GRBs (GRB 130131A and 140713A), along
with a tentative detection of a third (GRB 131229A) with the Karl G. Jansky
Very Large Array (VLA). Supplemented by three additional VLA-detected dark GRBs
from the literature, we present uniform modeling of their broadband afterglows.
We derive high line-of-sight dust extinctions of $A_{V, rm GRB} gtrsim 2.2 –
10.6~{rm mag}$. Additionally, we model the host galaxies of the six bursts in
our sample, and derive host galaxy dust extinctions of $A_{V, rm Host} approx
0.3-4.7~{rm mag}$. Across all tested $gamma$-ray (fluence and duration) and
afterglow properties (energy scales, geometries and circumburst densities), we
find dark GRBs to be representative of more typical unobscured long GRBs,
except in fluence, for which observational biases and inconsistent
classification may influence the dark GRB distribution. Additionally, we find
that $A_{V, rm GRB}$ is not related to a uniform distribution of dust
throughout the host, nor to the extremely local environment of the burst,
indicating that a larger scale patchy dust distribution is the cause of the
high line-of-sight extinction. Since radio observations are invaluable to
revealing heavily dust-obscured GRBs, we make predictions for the detection of
radio emission from host star formation with the next generation VLA.

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