VLBI for Gravity Probe B. I. Overview

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VLBI for Gravity Probe B. I. Overview

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Title: VLBI for Gravity Probe B. I. Overview
Author: Bartel, N.; Bietenholz, M. F.; Lebach, D. E.; Lestrade, J.-F.; Ransom, R. R.; Ratner, M. I.; Shapiro, Irwin Ira

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Citation: Shapiro, I. I., N. Bartel, M. F. Bietenholz, D. E. Lebach, J.-F. Lestrade, R. R. Ransom, and M. I. Ratner. 2012. “VLBI for Gravity Probe B. I. Overview.” The Astrophysical Journal Supplement Series 201, no. 1: 1-10.
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Abstract: We describe the NASA/Stanford gyroscope relativity mission, Gravity Probe B (GP-B), and provide an overview of the following series of six astrometric and astrophysical papers that report on our radio observations and analyses made in support of this mission. The main goal of this 8.5 year program of differential very long baseline interferometry astrometry was to determine the proper motion of the guide star of the GP-B mission, the RS CVn binary IM Pegasi (IM Peg; HR 8703). This proper motion is determined with respect to compact, extragalactic reference sources. The results are −20.833 ± 0.090 mas yr−1 and −27.267 ± 0.095 mas yr−1 for, respectively, the right ascension and declination, in local Cartesian coordinates, of IM Peg’s proper motion, and 10.370 ± 0.074 mas (i.e., 96.43 ± 0.69 pc) for its parallax (and distance). Each quoted uncertainty is meant to represent an ∼70% confidence interval that includes the estimated contribution from systematic error. These results are accurate enough not to discernibly degrade the GP-B estimates of its gyroscopes’ relativistic precessions: the frame-dragging and geodetic effects.
Published Version: doi:10.1088/0067-0049/201/1/1
Terms of Use: This article is made available under the terms and conditions applicable to Other Posted Material, as set forth at http://nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of-use#LAA
Citable link to this page: http://nrs.harvard.edu/urn-3:HUL.InstRepos:11858824
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