VLBI for Gravity Probe B: the guide star, IM Pegasi

被引：6

作者：

Bartel, N. ^{[1
]}

Bietenholz, M. F. ^{[1
,2
]}

Lebach, D. E. ^{[3
]}

Ransom, R. R. ^{[4
,5
]}

Ratner, M. I. ^{[3
]}

Shapiro, I. I. ^{[3
]}

机构：

[1] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada

[2] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa

[3] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[4] Okanagan Coll, Penticton, BC V2A 8E1, Canada

[5] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6K3, Canada

来源：

CLASSICAL AND QUANTUM GRAVITY | 2015年 / 32卷 / 22期

关键词：

VLBI; astrometry; radio star; IM Pegasi; proper motion; parallax; active galactic nuclei; RADIO; ASTROMETRY; HIPPARCOS; POSITION;

D O I：

10.1088/0264-9381/32/22/224021

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We review the radio very long baseline interferometry (VLBI) observations of the guide star, IM Peg, and three compact extragalactic reference sources, made in support of the NASA/Stanford gyroscope relativity mission, Gravity Probe B (GP-B). The main goal of the observations was the determination of the proper motion of IM Peg relative to the distant Universe. VLBI observations made between 1997 and 2005 yield a proper motion of IM Peg of -20.83 +/- 0.09 mas yr(-1) in alpha and -27.27 +/- 0.09 mas yr(-1) in delta in a celestial reference frame of extragalactic radio galaxies and quasars virtually identical to the International Celestial Reference Frame 2 (ICRF2). They also yield a parallax for IM Peg of 10.37 +/- 0.07 mas, corresponding to a distance of 96.4 +/- 0.7 pc. The uncertainties are standard errors with statistical and estimated systematic contributions added in quadrature. These results met the pre-launch requirements of the GP-B mission to not discernibly degrade the estimates of the geodetic and frame-dragging effects.

引用

页数：21

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