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Probing Early Phases of High Mass Stars with 6.7 GHz Methanol Masers

Published online by Cambridge University Press:  16 July 2018

Sonu Tabitha Paulson  and
Jagadheep D. Pandian
Sonu Tabitha Paulson
Affiliation:
Indian Institute of Space Science and Technology, Trivandrum, India email: [email protected],[email protected]
Jagadheep D. Pandian
Affiliation:
Indian Institute of Space Science and Technology, Trivandrum, India email: [email protected],[email protected]
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Abstract

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Methanol masers at 6.7 GHz are the brightest of class II methanol masers and have been found exclusively towards massive star forming regions. These masers can thus be used as a unique tool to probe the early phases of massive star formation. We present here the SED studies of 284 methanol masers chosen from the MMB catalogue, which falls in the Hi-GAL range (|l| ≤ 60°, |b| ≤ 1°). The masers are studied using the ATLASGAL, MIPSGAL and Hi-GAL data at wavelengths ranging from 24−870 micrometers. A single grey body component fit was used to model the cold dust emission whereas the emission from the warm dust is modelled by a black body. The clump properties such as isothermal mass, FIR luminosity and MIR luminosity were obtained using the best fit parameters of the SED fits. We discuss the physical properties of the sources and explore the evolutionary stages of the sources having 6.7 GHz maser emission in the timeline of high mass star formation.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S336: Astrophysical Masers: Unlocking the Mysteries of the Universe , September 2017 , pp. 323 - 324
Copyright
Copyright © International Astronomical Union 2018 

References

Green, J. A., & McClure-Griffiths, N. M., 2011, MNRAS, 417, 2500Google Scholar
Kauffmann, J., Pillai, T., Shetty, R., Myers, P. C., & Goodman, A. A., 2010, ApJ, 716, 433Google Scholar
Molinari, S., Pezzuto, S., Cesaroni, R., Brand, J., Faustini, F., & Testi, L., 2008, A&A, 481, 345Google Scholar
Pandian, J. D., Momjian, E., Xu, Y., Menten, K. M., & Goldsmith, P. F., 2010, A&A, 522, A8Google Scholar
Traficante, A., Fuller, G. A., Pineda, J. E., & Pezzuto, S., 2015, A&A, 574, A119Google Scholar
Urquhart, J. S., Moore, T. J. T., & Schuller F.,2013, MNRAS, 431, 1752Google Scholar
Walsh, A. J., Macdonald, G. H., Alvey, N. D. S., Burton, M. G., & Lee, J. K., 2003, A&A, 410, 597Google Scholar