Astrophys. J., 907, 106-106 (2021/February-1)
Stellar feedback on the earliest stage of massive star formation.
NAYAK O., MEIXNER M., OKADA Y., LEE M.Y., CHEVANCE M., BUCHBENDER C., FUKUI Y., ONISHI T., PARIKKA A. and STUTZKI J.
Abstract (from CDS):
We report SOFIA/GREAT observations of high-J CO lines and [C II] observations of the super star cluster candidate H72.97-69.39 in the Large Magellanic Cloud (LMC), which is in its very early formation stage. We use our observations to determine if shocks are heating the gas or if photon-dominated regions (PDRs) are being heated by local far-UV radiation. We use a PDR model and a shock model to determine whether the CO and [C II] lines arise from PDRs or shocks. We can reproduce the observed high-J CO and [C II] emission with a clumpy PDR model with the following properties: a density of 104.7 cm–3, a mass of 104 M☉, and UV radiation of 103.5 in units of Draine field. Comparison with the ALMA beam-filling factor suggests a higher density within the uncertainty of the fit. We find the lower-limit [C II]/total infrared (TIR) ratio (ε) traced by [C II]/TIR to be 0.026%, lower than other known young star-forming regions in the LMC. Our shock models may explain the CO (16-15) and CO (11-10) emission lines with shock velocity of 8-11 km s–1, pre-shock density of 104-105 cm–3, and GUV = 0 in units of Draine field. However, the [C II] line emission cannot be explained by a shock model, thus it is originating in a different gas component. Observations of [O I] 63 µm predicted to be 1.1 x 10–13 W m–2 by PDR models and 7.8 x 10–15 W m–2 by shock models will help distinguish between the PDR and shock scenarios.
© 2021. The American Astronomical Society. All rights reserved.
Star formation - Young stellar objects - Protostars - Photodissociation regions - Shocks
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