Hostname: page-component-78c5997874-fbnjt Total loading time: 0 Render date: 2024-10-31T23:28:24.068Z Has data issue: false hasContentIssue false

VLBI astrometry of two millisecond pulsars

Published online by Cambridge University Press:  20 March 2013

Zhen Yan
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China email: yanzhen@shao.ac.cn University of Chinese Academy of Sciences, Beijing 100039, China Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, China
Zhi-qiang Shen
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China email: yanzhen@shao.ac.cn Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, China
Jian-ping Yuan
Affiliation:
Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, China
Na Wang
Affiliation:
Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, China
Helge Rottmann
Affiliation:
Max Planck Institute for Radio Astronomy, Bonn 53121, Germany
Walter Alef
Affiliation:
Max Planck Institute for Radio Astronomy, Bonn 53121, Germany
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present astrometric results on two millisecond pulsars, PSR B1257+12 and PSR J1022+1001, as carried out through VLBI. For PSR B1257+12, a model-independent distance of 710−38+43 pc and proper motion of (μα = 46.44 ± 0.08 mas/yr, μδ=−84.87 ± 0.32 mas/yr) were obtained from 5 epochs of VLBA and 4 epochs of EVN observations, spanning about 2 years. The two dimensional proper motion of PSR J1022+1001 (μα~−10.13 mas/yr, μδ~16.89 mas/yr) was also estimated, using 3 epochs of EVN observations. Based on our results, the X-ray efficiency of PSR B1257+12 should be in the same range as other millisecond pulsars, and not as low as previously thought.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013

References

Brisken, W. F., Benson, J. M., Goss, W. M., & Thorsett, S. E., 2002, ApJ, 571, 906CrossRefGoogle Scholar
Campbell, R. M., et al., 1996, ApJ, 461, L95Google Scholar
Chatterjee, S., et al., 2009, ApJ, 698, 250Google Scholar
Cordes, J. M. & Lazio, T. J. W., 2002, ArXiv Astrophysics e-prints 0207156Google Scholar
Deller, A. T., Tingay, S. J., Bailes, M., & West, C., 2007, PASP, 119, 318Google Scholar
Deller, A. T., Tingay, S. J., & Brisken, W., 2009, ApJ, 690, 198Google Scholar
Fomalont, E. B., Goss, W. M., Beasley, A. J., & Chatterjee, S., 1999, AJ, 117, 3025CrossRefGoogle Scholar
Hotan, A. W., Bailes, M., & Ord, S. M., 2004, MNRAS, 355, 941Google Scholar
Konacki, M. & Wolszczan, A., 2003, ApJ, 591, L147Google Scholar
Kramer, M., et al., 1999, ApJ, 520, 324Google Scholar
Pavlov, G. G., Kargaltsev, O., Garmire, G. P., & Wolszczan, A., 2007, ApJ, 664, 1072CrossRefGoogle Scholar
Shklovskii, I. S., 1970, Soviet Astronomy, 13, 562Google Scholar
Taylor, J. H. & Cordes, J. M., 1993, ApJ, 411, 674CrossRefGoogle Scholar
Wolszczan, A., 2008, in ASP Conf. Ser. 398, Extreme Solar Systems, ed. Fischer, D., Rasio, F. A., Thorsett, S. E. & Wolszczan, A. (San Francisco, CA: ASP)Google Scholar
Wolszczan, A., et al., 2000, ApJ, 528, 907CrossRefGoogle Scholar