CLEAR: Paschen-$beta$ Star Formation Rates and Dust Attenuation of Low Redshift Galaxies. (arXiv:2009.00617v3 [astro-ph.GA] UPDATED)

CLEAR: Paschen-$beta$ Star Formation Rates and Dust Attenuation of Low Redshift Galaxies. (arXiv:2009.00617v3 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Cleri_N/0/1/0/all/0/1">Nikko J. Cleri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trump_J/0/1/0/all/0/1">Jonathan R. Trump</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Backhaus_B/0/1/0/all/0/1">Bren E. Backhaus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Momcheva_I/0/1/0/all/0/1">Ivelina Momcheva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Papovich_C/0/1/0/all/0/1">Casey Papovich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simons_R/0/1/0/all/0/1">Raymond Simons</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weiner_B/0/1/0/all/0/1">Benjamin Weiner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Estrada_Carpenter_V/0/1/0/all/0/1">Vicente Estrada-Carpenter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Finkelstein_S/0/1/0/all/0/1">Steven L. Finkelstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giavalisco_M/0/1/0/all/0/1">Mauro Giavalisco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ji_Z/0/1/0/all/0/1">Zhiyuan Ji</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jung_I/0/1/0/all/0/1">Intae Jung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matharu_J/0/1/0/all/0/1">Jasleen Matharu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_F/0/1/0/all/0/1">Felix Martinez III</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sturm_M/0/1/0/all/0/1">Megan R. Sturm</a>

We use Pab (1282~nm) observations from the Hubble Space Telescope ($HST$)
G141 grism to study the star-formation and dust attenuation properties of a
sample of 29 low-redshift ($z < 0.287$) galaxies in the CANDELS Ly$alpha$
Emission at Reionization (CLEAR) survey. We first compare the nebular
attenuation from $Pab/Ha$ with the stellar attenuation inferred from the
spectral energy distribution, finding that the galaxies in our sample are
consistent with an average ratio of the continuum attenuation to the nebular
gas of 0.44, but with a large amount of excess scatter beyond the observational
uncertainties. Much of this scatter is linked to a large variation between the
nebular dust attenuation as measured by (space-based) $Pab$ to (ground-based)
$Ha$ to that from (ground-based) $Ha/Hb$. This implies there are important
differences between attenuation measured from grism-based / wide-aperture
$Pab$ fluxes and the ground-based / slit-measured Balmer decrement. We next
compare star-formation rates (SFRs) from $Pab$ to those from dust-corrected
UV. We perform a survival analysis to infer a census of Pab emission implied
by both detections and non-detections. We find evidence that galaxies with
lower stellar mass have more scatter in their ratio of Pab to
attenuation-corrected UV SFRs. When considering our Pab detection limits,
this observation supports the idea that lower mass galaxies experience
“burstier” star-formation histories. Together, these results show that Pab is
a valuable tracer of a galaxy’s SFR, probing different timescales of
star-formation and potentially revealing star-formation that is otherwise
missed by UV and optical tracers.

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