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Intermittent maser flare around the high-mass young stellar object G353.273+0.641

Published online by Cambridge University Press:  24 July 2012

Kazuhito Motogi ,
Kazuo Sorai ,
Kenta Fujisawa ,
Koichiro Sugiyama  and
Mareki Honma
Kazuhito Motogi
Affiliation:
Department of Cosmosciences, Graduate School of Science, Hokkaido University, N10 W8, Sapporo 060-0810, Japan email: [email protected]
Kazuo Sorai
Affiliation:
Department of Cosmosciences, Graduate School of Science, Hokkaido University, N10 W8, Sapporo 060-0810, Japan email: [email protected] Department of Physics, Faculty of Science, Hokkaido University, N10 W8, Sapporo 060-0810, Japan
Kenta Fujisawa
Affiliation:
Department of Physics, Faculty of Science, Yamaguchi University, Yoshida 1677-1, Yamaguchi-city, Yamaguchi 753-8512 2, Japan The Research Institute of Time Studies, Yamaguchi University, Yoshida 1677-1, Yamaguchi-city, Yamaguchi 753-8511, Japan
Koichiro Sugiyama
Affiliation:
Department of Physics, Faculty of Science, Yamaguchi University, Yoshida 1677-1, Yamaguchi-city, Yamaguchi 753-8512 2, Japan
Mareki Honma
Affiliation:
Department of Astronomical Science, The Graduate University for Advanced Studies, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-12 Hoshi-ga-oka, Mizusawa-ku, Oshu, Iwate 023-0861, Japan
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Abstract

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The water maser site associated with G353.273+0.641 is classified as a dominant blueshifted H2O maser, which shows an extremely wide velocity range (± 100 km s−1) with almost all flux concentrated in the highly blueshifted emission. The previous study has proposed that this peculiar H2O maser site is excited by a pole-on jet from high mass protostellar object. We report on the monitoring of 22-GHz H2O maser emission from G353.273+0.641 with the VLBI Exploration of Radio Astrometry (VERA) and the Tomakamai 11-m radio telescope. Our VLBI imaging has shown that all maser features are distributed within a very small area of 200 × 200 au2, in spite of the wide velocity range (> 100 km s−1). The light curve obtained by weekly single-dish monitoring shows notably intermittent variation. We have detected three maser flares during three years. Frequent VLBI monitoring has revealed that these flare activities have been accompanied by a significant change of the maser alignments. We have also detected synchronized linear acceleration (−5 km s−1yr−1) of two isolated velocity components, suggesting a lower-limit momentum rate of 10−3 M⊙ km s−1yr−1 for the maser acceleration. All our results support the previously proposed pole-on jet scenario, and finally, a radio jet itself has been detected in our follow-up ATCA observation. If highly intermittent maser flares directly reflect episodic jet-launchings, G353.273+0.641 and similar dominant blueshifted water maser sources can be suitable targets for a time-resolved study of high mass protostellar jet.

Keywords

masersstars: early-typestars: formationISM: jets and outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S287: Cosmic Masers - from OH to H0 , January 2012 , pp. 98 - 102
Copyright
Copyright © International Astronomical Union 2012

References

Arce, H. G., et al. 2007, in Reipurth, B., Jewitt, D., & Keil, K., eds, Protostars and Planets V. Univ. of Arizona Press, Tucson, p. 245Google Scholar
Breen, S. L., Caswell, J. L., Ellingsen, S. P., & Phillips, C. J. 2010, MNRAS, 406, 1487Google Scholar
Caswell, J. L. 1997, MNRAS, 209, 203CrossRefGoogle Scholar
Caswell, J. L. 2004, MNRAS, 351, 279CrossRefGoogle Scholar
Caswell, J. L. & Phillips, C. J. 2008, MNRAS, 386, 1521 (CP08)CrossRefGoogle Scholar
Caswell, J. L. & Breen, S. L. 2010, MNRAS, 407, 2599CrossRefGoogle Scholar
Curiel, S., et al. 2006, ApJ, 638, 878CrossRefGoogle Scholar
Hofner, P., Cesaroni, R., Olmi, L., Rodrígues, L. F., Martí, J. & Araya, E. 2007, A&A, 465, 197Google Scholar
Martí, J., Rodrígues, L. F., & Reipurth, B. 1998, ApJ, 502, 337CrossRefGoogle Scholar
Minier, V., Ellingsen, S. P., Norris, R. P. & Booth, R. S. 2003, A&A, 403, 1095Google Scholar
Motogi, K., et al. 2011, MNRAS, 417, 238CrossRefGoogle Scholar
Neckel, T. 1978, A&A, 69, 51Google Scholar
Sakellis, S., Taylor, M. I., Taylor, K. N. R., Vaile, K. A., & Han, T. D. 1984, PASP, 96, 543CrossRefGoogle Scholar
Wilson, W. E., et al. 2011, MNRAS, 416, 832CrossRefGoogle Scholar