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VLBI Observations and NH3 Mapping of the Star-forming Region NGC2264

Published online by Cambridge University Press:  21 March 2013

Tatsuya Kamezaki
Affiliation:
Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065 email: kamezaki@milkyway.sci.kagoshima-u.ac.jp
Kenji Imura
Affiliation:
Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065 email: kamezaki@milkyway.sci.kagoshima-u.ac.jp
Takumi Nagayama
Affiliation:
Mizusawa VLBI Observatory, Mitaka Office, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588
Toshihiro Omodaka
Affiliation:
Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065 email: kamezaki@milkyway.sci.kagoshima-u.ac.jp
Toshihiro Handa
Affiliation:
Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065 email: kamezaki@milkyway.sci.kagoshima-u.ac.jp
Yoshiyuki Yamaguchi
Affiliation:
Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065 email: kamezaki@milkyway.sci.kagoshima-u.ac.jp
James O. Chibueze
Affiliation:
Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065 email: kamezaki@milkyway.sci.kagoshima-u.ac.jp
Kazuyoshi Sunada
Affiliation:
Mizusawa VLBI Observatory, Mitaka Office, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588
Makoto Nakano
Affiliation:
Faculty of Education and Welfare Science, Oita University, Oita 870-1192
Corresponding
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Abstract

We have measured the annual parallax of the water maser source associated with star forming region NGC2264 from observations with VLBI Exploration of Radio Astrometry (VERA). We detected masers at VLSR = 7.2 km s−1. We discussed its driving sources of detected maser spots. One of the maser spots was associated with a centimeter continuum source observed with VLA. Neither optical, infrared nor X-ray sources is catalogued near the spot. The other maser spot is located close to an X-ray source, although there is no optical or infrared counterpart. The proper motion of the former spot was (μα, μδ) = (23.91 ± 4.29, −29.81 ± 4.27) and the proper motion of latter spot was (μα, μδ) = (−0.96 ± 0.58, −6.05 ± 3.06). For the latter spot, the peculiar motion is ∼ 150 km s−1 and it has the high velocity and this may be a jet or an outflow from a young star. The observed parallax is 1.365 ± 0.098 mas, corresponding to the distance of 738+57−50 pc. This value is constant with the photometric distance of NGC2264 previously measured. The fitting result of the parallax is shown in figure 1. We also observed in NH3 (1,1), (2,2), (3,3) lines of NGC2264 with the Kashima 34m telescope. We estimated the star formation efficiency (SFE) of NGC2264 from the dense molecular mass of NH3 and the stellar mass calculated by Teixeira et al. (2012). The SFE is 9 – 12% which is consistent with previous results.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013

References

Teixeira, P. S., Lada, C. J., Marengo, M., & Lada, E. A. 2012, A&A, 540, A83Google Scholar

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