The CARMA-NRO Orion Survey: Statistical Signatures of Feedback in the Orion A Molecular Cloud. (arXiv:1903.05104v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Feddersen_J/0/1/0/all/0/1">Jesse R. Feddersen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arce_H/0/1/0/all/0/1">Héctor G. Arce</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kong_S/0/1/0/all/0/1">Shuo Kong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ossenkopf_Okada_V/0/1/0/all/0/1">Volker Ossenkopf-Okada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carpenter_J/0/1/0/all/0/1">John M. Carpenter</a>
We investigate the relationship between turbulence and feedback in the Orion
A molecular cloud using maps of $^{12}$CO(1-0), $^{13}$CO(1-0) and
C$^{18}$O(1-0) from the CARMA-NRO Orion survey. We compare gas statistics with
the impact of feedback in different parts of the cloud to test whether feedback
changes the structure and kinematics of molecular gas. We use principal
component analysis, the spectral correlation function, and the spatial power
spectrum to characterize the cloud. We quantify the impact of feedback with
momentum injection rates of protostellar outflows and wind-blown shells as well
as the surface density of young stars. We find no correlation between shells or
outflows and any of the gas statistics. However, we find a significant
anti-correlation between young star surface density and the slope of the
$^{12}$CO spectral correlation function, suggesting that feedback may influence
this statistic. While calculating the principal components, we find peaks in
the covariance matrix of our molecular line maps offset by 1-3 km s$^{-1}$
toward several regions of the cloud which may be produced by feedback. We
compare these results to predictions from molecular cloud simulations.
We investigate the relationship between turbulence and feedback in the Orion
A molecular cloud using maps of $^{12}$CO(1-0), $^{13}$CO(1-0) and
C$^{18}$O(1-0) from the CARMA-NRO Orion survey. We compare gas statistics with
the impact of feedback in different parts of the cloud to test whether feedback
changes the structure and kinematics of molecular gas. We use principal
component analysis, the spectral correlation function, and the spatial power
spectrum to characterize the cloud. We quantify the impact of feedback with
momentum injection rates of protostellar outflows and wind-blown shells as well
as the surface density of young stars. We find no correlation between shells or
outflows and any of the gas statistics. However, we find a significant
anti-correlation between young star surface density and the slope of the
$^{12}$CO spectral correlation function, suggesting that feedback may influence
this statistic. While calculating the principal components, we find peaks in
the covariance matrix of our molecular line maps offset by 1-3 km s$^{-1}$
toward several regions of the cloud which may be produced by feedback. We
compare these results to predictions from molecular cloud simulations.
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