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High Resolution LAsMA \(^{12}\)CO and \(^{13}\)CO Observation of the G305 Giant Molecular Cloud Complex: I. Feedback on the Molecular Gas

Mazumdar, P., Wyrowski, F., Colombo, D., Urquhart, J.S., Thompson, M.A., Menten, K.M. (2021) High Resolution LAsMA \(^{12}\)CO and \(^{13}\)CO Observation of the G305 Giant Molecular Cloud Complex: I. Feedback on the Molecular Gas. Astronomy & Astrophysics, 650 . Article Number A164. ISSN 0004-6361. (doi:10.1051/0004-6361/202040205) (KAR id:88361)


Context. Understanding the effect of feedback, the interaction of young massive stars with their parental Giant Molecular Clouds, is of central importance for studies of the interstellar medium and star formation. Aims. We observed the G305 star forming complex in the J = 3-2 lines of \(^{12}\)CO and \(^{13}\)CO to investigate how molecular gas surrounding the central stellar clusters is being impacted by feedback. Methods. The APEX telescope’s LAsMA multi-beam receiver was used to observe the region. Excitation temperatures and column density maps were produced. Combining our data with data from the SEDIGISM survey resulted in a \(^{13}\)CO J = 3-2/2-1 excitation map. To verify whether feedback from stellar clusters is responsible for exciting the gas, the distribution of CO excitation was compared with that of 8 µm emission imaged with Spitzer, which is dominated by UV-excited emission from PAHs. Line centroid velocities, as well as stacked line profiles were examined to investigate the effect of feedback on the gas dynamics. Results. Line profiles along radially outward directions demonstrate that the excitation temperature and \(^{13}\)CO J = 3-2/2-1 ratio increase steeply by factors of ∼ 2–3 at the edge of the denser gas traced by \(^{13}\)CO that faces the hot stars at the center of the complex and steadily decreases away from it. Column density also increases at the leading edge, but does not always decrease steadily outward. Regions with higher 8 µm flux have higher median excitation temperatures, column densities and \(^{13}\)CO J = 3-2/2-1 ratio. The centroid velocity probability distribution function of the region shows exponential wings, indicative of turbulence driven by strong stellar winds. Stacked spectra in regions with stronger feedback have higher skewness and narrower peaks with pronounced wings compared to regions with weaker feedback. Conclusions. Feedback from the stellar cluster in G305 has demonstrable effects on the excitation as well as on the dynamics of the giant molecular cloud.

Item Type: Article
DOI/Identification number: 10.1051/0004-6361/202040205
Uncontrolled keywords: Submillimeter: ISM – ISM:clouds – ISM: kinematics and dynamics – ISM: evolution – Line: profiles – Turbulence
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Divisions > Division of Natural Sciences > Physics and Astronomy
Depositing User: James Urquhart
Date Deposited: 25 May 2021 15:52 UTC
Last Modified: 12 Jan 2024 14:24 UTC
Resource URI: (The current URI for this page, for reference purposes)

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Urquhart, J.S..

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Thompson, M.A..

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