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The outer rotation curve project with VERA: Trigonometric parallax of IRAS 05168+3634

Published online by Cambridge University Press:  26 February 2013

Nobuyuki Sakai
Affiliation:
The Graduate University for Advanced Studies (Sokendai), Mitaka, Tokyo 181-8588, Japan email: nobuyuki.sakai@nao.ac.jp
Mareki Honma
Affiliation:
The Graduate University for Advanced Studies (Sokendai), Mitaka, Tokyo 181-8588, Japan email: nobuyuki.sakai@nao.ac.jp Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan
Hiroyuki Nakanishi
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan
Hirofumi Sakanoue
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan
Tomoharu Kurayama
Affiliation:
Center for Fundamental Education, Teikyo University of Science, 2525 Yatsusawa, Uenohara, Yamanashi 409-0193, Japan
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Abstract

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We present a measurement of the trigonometric parallax of IRAS 05168+3634 with VERA. The parallax is 0.532 ± 0.053 milli-arcsec, corresponding to a distance of 1.88+0.21−0.17 kpc. This is significantly closer than the previous distance estimate of 6 kpc based on a kinematic distance measurement. This drastic change in the source distance implies the need for revised values of not only the physical parameters of IRAS 05168+3634, but it also impies a different location in the Galaxy, placing it in the Perseus arm rather than the Outer arm. We also measured the proper motion of the source. A combination of the distance and proper motion with the systemic velocity yields a rotation velocity Θ = 227+9−11 km s−1 at the source position, assuming Θ0 = 240 km s−1. Our result, combined with previous VLBI results for six sources in the Perseus arm, indicates that the sources rotate systematically more slowly than the Galactic rotation velocity at the local standard of rest. In fact, we derive peculiar motions in the disk averaged over the seven sources in the Perseus arm of (Umean, Vmean) = (11 ± 3, −17 ± 3) km s−1, which indicates that these seven sources are moving systematically toward the Galactic Center and lag behind the overall Galactic rotation.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013

References

Bronfman, L., Nyman, L.-Å., & May, J. 1996, A&A, 115, 81Google Scholar
Georgelin, Y. M. & Georgelin, Y. P. 1976, A&A, 49, 57Google Scholar
Lin, C. C. & Shu, F. H. 1964, ApJ, 140, 646Google Scholar
McCutcheon, W. H., Sato, T., Dewdney, P. E., & Purton, C. R. 1991, AJ, 101, 1435Google Scholar
Mel'nik, A. M., Dambis, A. K., & Rastorguev, A. S. 1999, Astron. Lett., 25, 518Google Scholar
Molinari, S., Brand, J., Cesaroni, R., Palla, F., & Palumbo, G. G. C. 1998, A&A, 336, 339Google Scholar
Molinari, S., Brand, J., Cesaroni, R., & Palla, F. 1996, A&A, 308, 573Google Scholar
Nagayama, T., Omodaka, T., Handa, T., et al. 2011, PASJ, 63, 719Google Scholar
Perryman, M. A. C. 1989, Nature, 340, 111CrossRefGoogle Scholar
Sakai, N., Honma, M., Nakanishi, H., et al. 2012c, ASP Conf. Ser., 458, 243Google Scholar
Sakai, N., Honma, M., Nakanishi, H., Sakanoue, H., Kurayama, T., Shibata, K. M., & Shizugami, M. 2012a, PASJ, 64, in press (arXiv:1204.4782)Google Scholar
Sanna, A., Reid, M. J., Dame, T. H., et al. 2012, ApJ, 745, 82Google Scholar
Sofue, Y. 2011a, PASJ, 63, 813Google Scholar
Sofue, Y., Honma, M., & Omodaka, T. 2009, PASJ, 61, 227CrossRefGoogle Scholar
Sofue, Y., Tutui, Y., Honma, M., Tomita, A., Takamiya, T., Koda, J., & Takeda, Y. 1999, ApJ, 523, 136Google Scholar