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MEASUREMENT OF PULSAR PARALLAX BY VERY LONG BASELINE INTERFEROMETRY.

机译：通过非常长的基线干涉测量脉冲状视差。

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摘要

Using Very Long Baseline Interferometry, I have measured the parallax of two pulsars and have observed absence of relative motion between members of pairs of quasars. Observations were made over a ten-month period at 18 cm, with antennas and data recorders at Green Bank, WV, Owens Valley, CA, and Arecibo, PR. Each program source was observed alternately with a nearby reference source. The recorded signals were processed to produce interference fringes, which were corrected for the effects of polar motion, the troposphere and the ionosphere. The fringe phases of each program source were then differenced with those of its reference, reducing residual systematic errors. Variations of this difference between epochs reflected program source proper motion and parallax.; I obtain a parallax of 7.8 (+OR-) 0.6 mas for PSR 0950 + 08, corresponding to a distance of 130 (+OR-) 10 pc, and a parallax of 1.8 (+OR-) 0.4 mas for PSR 0823 + 26, corresponding to a distance of 560 (+OR-) 130 pc. In combination with published measurements of pulse dispersion for these pulsars, these yield average free electron densities of 0.023 (+OR-) 0.002 cm('-3) along the line of sight to PSR 0950 + 08 and 0.035 (+OR-) 0.008 cm('-3) along the line of sight to PSR 0823 + 26. These are in good agreement with free electron densities measured by other techniques along lines of sight 1 kpc or more in length. Both parallax measurements are subject to systematic errors and questions of interpretation which have not yet been fully explored.
机译：使用甚长基线干涉测量法，我测量了两个脉冲星的视差，并观察到成对类星体之间没有相对运动。在18厘米处的十个月时间内进行了观测，并使用天线和数据记录仪在美国西弗吉尼亚州的格林班克，加利福尼亚的欧文斯谷和宾夕法尼亚的阿雷西博。每个节目源与附近的参考源交替观察。对记录的信号进行处理以产生干涉条纹，并对其进行了极移，对流层和电离层影响的校正。然后，将每个程序源的边缘阶段与其参考阶段的边缘阶段进行区别，以减少残留的系统误差。历元之间的这种差异的变化反映了节目源的适当运动和视差。对于PSR 0950 + 08，我获得了7.8（+ OR-）0.6 mas的视差，对应于130（+ OR-）10 pc的距离，对于PSR 0823 + 26得到了1.8（+ OR-）0.4 mas的视差，对应于560（+ OR-）130 pc的距离。结合已发布的这些脉冲星的脉冲色散测量结果，这些视场沿PSR 0950 + 08和0.035（+ OR-）0.008产生的平均自由电子密度为0.023（+ OR-）0.002 cm（'-3） cm（'-3）沿视线到达PSR 0823 +26。这与通过其他技术沿1 kpc或更长视线测量的自由电子密度高度吻合。两种视差测量都受到系统误差和解释问题的影响，这些问题尚未得到充分探讨。

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  • 作者

    GWINN, CARL ROSS.;

  • 作者单位

    Princeton University.;

  • 授予单位 Princeton University.;
  • 学科 Physics Astronomy and Astrophysics.
  • 学位 Ph.D.
  • 年度 1984
  • 页码 148 p.
  • 总页数 148
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类 天文学;
  • 关键词

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