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KVN Single-dish Water and Methanol Maser Line Surveys of Galactic YSOs

Published online by Cambridge University Press:  24 July 2012

Kee-Tae Kim ,
Do-Young Byun ,
Jae-Han Bae ,
Won-Ju Kim ,
Hyun-Woo Kang ,
Chung Sik Oh  and
So-Young Youn
Kee-Tae Kim
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-Gu, Daejeon 305-348, South Korea email: ktkim@kasi.re.kr
Do-Young Byun
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-Gu, Daejeon 305-348, South Korea email: ktkim@kasi.re.kr
Jae-Han Bae
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-Gu, Daejeon 305-348, South Korea email: ktkim@kasi.re.kr
Won-Ju Kim
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-Gu, Daejeon 305-348, South Korea email: ktkim@kasi.re.kr
Hyun-Woo Kang
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-Gu, Daejeon 305-348, South Korea email: ktkim@kasi.re.kr
Chung Sik Oh
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-Gu, Daejeon 305-348, South Korea email: ktkim@kasi.re.kr
So-Young Youn
Affiliation:
Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-Gu, Daejeon 305-348, South Korea email: ktkim@kasi.re.kr
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Abstract

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We have carried out simultaneous 22 GHz H2O and 44 GHz Class I CH3OH maser line surveys of more than 1500 intermediate- and high-mass YSOs in the Galaxy using newly-constructed KVN 21-m telescopes. As the central (proto)stars evolve, the detection rates of the two masers rapidly decrease for intermediate-mass YSOs while the rates increase for high-mass YSOs. These results suggest that the occurrence of the two masers is closely related both to the evolutionary stage of the central objects and to the circumstellar environments. CH3OH masers always have very similar velocities (<10 km s−1) to the natal dense cores, whereas H2O masers often have significantly different velocities. The isotropic luminosities of both masers are well correlated with the bolometric luminosities of the central (proto)stars.

Keywords

maserwatermethanolstar formationyoung stellar object
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S287: Cosmic Masers - from OH to H0 , January 2012 , pp. 488 - 491
Copyright
Copyright © International Astronomical Union 2012

References

Bae, J.-H., Kim, K.-T., Youn, S.-Y., Kim, W.-J., Byun, D.-Y., Kang, H.-W., & Oh, C. S. 2011, ApJS, 196, 21Google Scholar
Fontani, F., Cesaroni, R., & Furuya, R. S. 2010, A&A, 517, A56Google Scholar
Furuya, R. S., Kitamura, Y., Wootten, H. A., Claussen, M. J., & Kawabe, R. 2003, ApJS, 144, 71Google Scholar
Kim, H.-G., et al. 2004, in: Bachiller, R. et al. (eds.), Proceedings of the 7th Symposium of the European VLBI Network, (Toledo: OAN), 281Google Scholar
Kim, K.-T., et al. 2004, J. Korean Astron. Soc., 44, 81Google Scholar
Kurtz, S., Hofner, P. & Carlos Vargas, A. 2004, ApJS, 155, 149Google Scholar
Han, S.-T., et al. 2008, Int. J. Infrared and Millimeter Waves, 29, 69Google Scholar
Lee, S.-S., et al. 2011, PASP, 123, 1398CrossRefGoogle Scholar
Sridharan, T. K., Beuther, H., Schilke, P., Menten, K. M., & Wyrowski, F. 2002, ApJ, 566, 931CrossRefGoogle Scholar
Wood, D. O. C. & Churchwell, E. 1989, ApJS, 69, 831Google Scholar
Yi, J. & Jung, T.-H. 2008, P. Korean Astron. Soc., 23, 37Google Scholar