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The Distance to the Center of the Galaxy

Published online by Cambridge University Press:  04 August 2017

M. J. Reid ,
M. H. Schneps ,
J. M. Moran ,
C. R. Gwinn ,
R. Genzel ,
D. Downes  and
B. Ronnang
M. J. Reid
Affiliation:
Harvard-Smithsonian Center for Astrophysics
M. H. Schneps
Affiliation:
Harvard-Smithsonian Center for Astrophysics
J. M. Moran
Affiliation:
Harvard-Smithsonian Center for Astrophysics
C. R. Gwinn
Affiliation:
Harvard-Smithsonian Center for Astrophysics
R. Genzel
Affiliation:
University of California, Berkeley
D. Downes
Affiliation:
Institut de Radio Astronomie Millimetrique
B. Ronnang
Affiliation:
Onsala Space Observatory

Extract

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The distance to a star forming region can be determined by measuring the proper motions within H2O maser clusters. If the motions of the maser spots are random, the distance can be determined by applying the technique known as statistical parallax. Alternatively, if organized motions are evident in the proper motions, one can model the source to estimate its the distance. Both methods rely on a comparison of the radial component of the motion (in km/s) and the proper motion on the plane of the sky (in milli-arcseconds/year).

Type
II. Large Scale Processes of Star Formation
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 554 - 555
Copyright
Copyright © Reidel 1987