How hot is the molecular gas in the Galactic Center?

Content Provider	Scilit
Author	Immer, Katharina Kauffmann, Jens Pillai, Thushara Ginsburg, Adam Menten, Karl M.
Copyright Year	2015
Description	The molecular clouds in the Central Molecular Zone of our Galaxy (CMZ; inner ~200 pc) show systematically higher gas than dust temperatures (>50 K vs <30 K) in recent $H_{2}$CO line and dust continuum surveys. This discrepancy is puzzling since gas and dust temperatures should become equal over short times at the high densities observed in these clouds. In deep $H_{2}$CO(3–2) and (4–3) observations of seven clouds in the CMZ, we detected not only large temperature differences between the clouds but also large gradients within the clouds. Comparing the temperatures and the main $H_{2}$CO lines at 218 and 291 GHz, we found a positive correlation between those two parameters, indicating that turbulence plays an important role in the heating of the gas. As a follow-up, we mapped the temperature tracers $CH_{3}$CCH and $CH_{3}$CN in these seven clouds to derive multiple temperature estimates and test the accuracy of high gas temperatures.
Related Links	https://www.cambridge.org/core/services/aop-cambridge-core/content/view/043969C20355CB44E55DEF75DEDFE9A4/S1743921316012278a.pdf/div-class-title-how-hot-is-the-molecular-gas-in-the-galactic-center-div.pdf
Ending Page	114
Page Count	4
Starting Page	111
ISSN	17439213
e-ISSN	17439221
DOI	10.1017/s1743921316012278
Journal	Proceedings of the International Astronomical Union
Issue Number	S322
Volume Number	11
Language	English
Publisher	Cambridge University Press (CUP)
Publisher Date	2016-07-01
Access Restriction	Open
Subject Keyword	Proceedings of the International Astronomical Union Astronomy and Astrophysics Center Molecules Structure Clouds Ism
Content Type	Text
Resource Type	Article
Subject	Astronomy and Astrophysics Space and Planetary Science