Hostname: page-component-cd9895bd7-8ctnn Total loading time: 0 Render date: 2024-12-25T15:51:36.559Z Has data issue: false hasContentIssue false
  • English
  • Français

The W51 Main/South SFR complex seen through 6-GHz OH and methanol masers

Published online by Cambridge University Press:  24 July 2012

Sandra Etoka ,
Malcolm D. Gray  and
Gary A. Fuller
Sandra Etoka
Affiliation:
Jodrell Bank Centre for AstrophysicsSchool of Physics and AstronomyThe University of Manchester, Manchester M13 9PL, UK email: [email protected]
Malcolm D. Gray
Affiliation:
Jodrell Bank Centre for AstrophysicsSchool of Physics and AstronomyThe University of Manchester, Manchester M13 9PL, UK email: [email protected]
Gary A. Fuller
Affiliation:
Jodrell Bank Centre for AstrophysicsSchool of Physics and AstronomyThe University of Manchester, Manchester M13 9PL, UK email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

W51 Main/South is one of the brightest and richest high-mass star-forming regions (SFR) in the complex W51. It is known to host many ultra-compact HII (UCHII) regions thought to be the site of massive young stellar objects. Maser emission from various species is also found in the region. We have performed MERLIN astrometric observations of excited-OH maser emission at 6.035 GHz and Class II methanol maser emission at 6.668 GHz towards W51 to investigate the relationship between the maser emission and the compact continuum sources in this SFR complex. Here we present the astrometric distributions of both 6.668-GHz methanol and 6.035-GHz excited-OH maser emission in the W51 Main/South region. The location of maser emission in the two lines is compared with that of previously published OH groundstate emission. The interesting coherent velocity and spatial structure observed in the methanol maser distribution as well as the relationship of the masers to infall or outflow in the region are discussed. It appears that the masers are excited by multiple objects potentially at different stages of evolution.

Keywords

astrometrycircumstellar mattermasersmagnetic fieldspolarizationstars: formationISM: individual objects: W51radio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S287: Cosmic Masers - from OH to H0 , January 2012 , pp. 171 - 175
Copyright
Copyright © International Astronomical Union 2012

References

Bartkiewicz, A., Szymczak, M., van Langevelde, H. J., Richards, A. M. S., & Pihlström, Y. M. 2009, A&A, 502, 155Google Scholar
Cragg, D. M., Sobolev, A. M., & Godfrey, P. D. 2002, MNRAS, 331, 521CrossRefGoogle Scholar
Churchwell, E. 2002, ARA&A, 40, 27Google Scholar
Etoka, S., Gray, M. D., & Fuller, G. A. 2012, accepted in MNRASGoogle Scholar
Etoka, S., Cohen, R. J., & Gray, M. D. 2005, MNRAS, 360, 1162CrossRefGoogle Scholar
Fish, V. L. & Reid, M. J. 2007, ApJ, 670, 1172CrossRefGoogle Scholar
Gaume, R. A., Johnston, K. L., & Wilson, T. L. 1993, ApJ, 417, 645CrossRefGoogle Scholar
Genzel, R. et al. 1981, ApJ, 247, 1039CrossRefGoogle Scholar
Gray, M. D., Field, D., & Doel, R. C. 1992, A&A, 262, 555Google Scholar
Imai, H. et al. 2002, PASJ, 54, 741CrossRefGoogle Scholar
Menten, K. M., Melnick, G. J., Phillips, T. G., & Neufeld, D. A. 1990, ApJ, 363, L27CrossRefGoogle Scholar
Phillips, C. & van Langevelde, H. 2005, ASPC, 340, 342Google Scholar
Keto, E. & Klaasen, P. 2008, ApJ, 678, L109CrossRefGoogle Scholar
Sato, M., Reid, M. J., Brunthaler, A., & Menten, K. M. 2010, ApJ, 720, 1055CrossRefGoogle Scholar
Shi, H., Zhao, J.-H., & Han, J. L. 2010a, ApJ, 710, 843CrossRefGoogle Scholar
Shi, H., Zhao, J.-H., & Han, J. L. 2010b, ApJ, 718L, 181CrossRefGoogle Scholar
Zhang, Q. & Ho, P. T. P. 1997, ApJ, 488, 241CrossRefGoogle Scholar
Zhang, Q., Ho, P. T. P., & Ohashi, N. 1998, ApJ, 494, 636CrossRefGoogle Scholar