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EVLA imaging of the water masers in the massive protostellar cluster NGC6334I

Published online by Cambridge University Press:  24 July 2012

Todd R. Hunter  and
Crystal L. Brogan
Todd R. Hunter
Affiliation:
NRAO, 520 Edgemont Rd, Charlottesville, VA 22903, USA; email: thunter@nrao.edu
Crystal L. Brogan
Affiliation:
NRAO, 520 Edgemont Rd, Charlottesville, VA 22903, USA; email: thunter@nrao.edu
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Abstract

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We have used the recently-upgraded Karl G. Jansky Very Large Array (VLA) in A-configuration to observe the water masers in the massive protostellar cluster NGC6334I with broad bandwidth and high spectral resolution. Four groups of maser spots are found. The two groups with the broadest velocity span (40 km/s) are towards the UCHII region and the hot core SMA1. The spatial kinematics of the SMA1 masers are consistent in sense and orientation with the large-scale CO outflow and appear to trace the base of the outflow from a protostar at the dust peak of SMA1. Additional masers at the southern end of SMA1 provide evidence for a second protostar. The highest intensity maser lies about 2″ north of SMA1. Interestingly, no water masers are seen on the equally impressive hot core SMA2. Finally, we have detected maser emission toward the enigmatic source SMA4, which shows no millimeter molecular lines despite having strong, compact submillimeter continuum and may trace another protostar.

Keywords

masersstars: formationISM: jets and outflowsISM: moleculesradio lines: ISMradio continuum: ISMinfrared: ISMsubmillimeter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S287: Cosmic Masers - from OH to H0 , January 2012 , pp. 502 - 503
Copyright
Copyright © International Astronomical Union 2012

References

Breen, S., Ellingsen, S., Caswell, J., et al. 2012, arXiv:1201.1330Google Scholar
Beuther, H., Thorwirth, S., Zhang, Q., et al. 2005, ApJ, 627, 834CrossRefGoogle Scholar
Brogan, C. L., Hunter, T. R., Cyganowski, C. J., Indebetouw, R., et al. 2009, ApJ, 707, 1CrossRefGoogle Scholar
Hunter, T. R., Brogan, C. L., Megeath, S., Menten, K., et al. 2006, ApJ, 649, 888CrossRefGoogle Scholar
Gómez, L., Luis, L., Hernández-Curiel, I., et al. 2010, ApJS, 191, 207CrossRefGoogle Scholar
Kurtz, S., Hofner, P. & Álvarez, C. V. 2004, ApJS, 155, 149CrossRefGoogle Scholar
Leurini, S., Schilke, P., Parise, B., et al. 2006, A&A, 454, L83Google Scholar
Qiu, K., Wyrowski, F., Menten, K. M., et al. 2011, ApJ, 743, L25CrossRefGoogle Scholar
Tofani, G., Felli, M., Taylor, G. B., & Hunter, T. R., 1995, A&AS, 112, 299Google Scholar
Zhang, Q., Hunter, T. R., Beuther, H., et al. 2007, ApJ, 658, 1152CrossRefGoogle Scholar