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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