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12 - Radio astrometry

from Part III - Observing through the atmosphere

Published online by Cambridge University Press:  05 December 2012

By
Edward B. Fomalont
Edited by
William F. van Altena
William F. van Altena
Affiliation:
Yale University, Connecticut
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Summary

Introduction

Astrometry is the branch of astronomy that studies the position and motion of celestial objects in the Solar System, in the Milky Way Galaxy, and for galaxies that are near the limit of the observable Universe. In radio astronomy, the study can be separated into microastrometry and macro-astrometry. Micro-astrometry deals with the motion of individual or a small number of associated objects in order to determine their space motion, their distance from the Solar System, and their kinetic properties with respect to neighboring stars and planets. The observational techniques and reductions measure the separation of the target object from a nearby calibrator radio source with known and stable properties.

Macro-astrometry, on the other hand, deals with the absolute position of radio sources, which also requires the determination of the Earth's deformations, complex rotations, and space motion. This type of astrometric experiment observes many well-known compact radio sources over the sky within a 24-hour period. From the analysis of systematic residuals in the data, the absolute positions of the sources, as well as the astrometric and geodetic properties the Earth, are determined. From this 30+ year effort, the fundamental celestial inertial frame has been defined to an accuracy of about 0.01 milliarcsec (mas) using the position of nearly 300 radio sources.

For nearly 30 years, the highest astrometric precision has been obtained using radio-interferometric techniques because of several properties of radio waves. First, astronomers and engineers have been able to connect arrays of radio telescopes that span the Earth (even into Earth orbit) to achieve resolutions of a few mas and obtain positional accuracies well under 1 mas.

Type
Chapter
Information
Astrometry for Astrophysics
Methods, Models, and Applications
 , pp. 175 - 198
Publisher: Cambridge University Press
Print publication year: 2012

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References

Argon, A. L., Greenhill, L. J., Reid, M. J., Moran, J. M., and Humphreys, E. M. L. (2007). ApJ, 659, 1040.Google Scholar
Asaki, Y., Sudou, H., Kono, Y., et al. (2007). PASJ, 59, 397.CrossRef
Beasley, A. J. and Conway, J. E. (1995). ASP conf. Ser., 82, 327.
Bietenholz, M. F., Bartel, N., and Rupen, M. P. (2004). ApJ, 615, 173–180.Google Scholar
Born, M. and Wolf, E. (1999). Principles of Optics, 7th edn. Cambridge: Cambridge University.CrossRefGoogle Scholar
Brisken, W. F., Benson, J. M., Beasley, A. J., et al. (2000). ApJ, 541, 959.Google Scholar
Charlot, P. (2004). IVS 2004 General Meeting Proceedings, Ottawa, Canada, February 9–11, pp. 12–21. See http://ivscc.gsfc.nasa.gov/publications/gm2004/charlot/Google Scholar
Clark, T. A., Corey, B. E., Davis, J. L., et al. (1985). IEEE Trans. Geosci. Remote Sensing, GE-23, 391–397.Google Scholar
Chatterjee, S., Ma, C., Arias, E. F., et al. (2009). ApJ, 698, 250.Google Scholar
Fey, A. L., Briskin, W. F., Vlemmings, W. H. T., et al. (2004). AJ, 127, 3587.Google Scholar
Fey, A. L., Gordon, D., and Jacobs, C. S., eds. (2009). IERS Technical Note 35, Frankfurt am Main: Verlag des Bundesamts für Kartographie und Geodäsie. See http://www.iers.org/MainDisp.csl?pid=46-1100252.
Fomalont, E. B. and Kopeikin, S. M. (2003). ApJ, 598, 704.Google Scholar
Fomalont, E. B., Kopeikin, S. M., Lanyi, G., and Benson, J. M. (2009). ApJ, 699, 1395.Google Scholar
Fomalont, E. B., Johnston, K. J., Fey, A., et al. (2011). AJ, 141, 91.CrossRef
Haas, R. (2006). IVS 2006 General Meeting Proceedings, Concepción, Chile, January 9–11. See http://ivscc.gsfc.nasa.gov/publications/gm2006/haas.
Herring, T. A., Davis, J. L., and Shapiro, I. I. (1990). J. Geophys. Res., 95, 12561.CrossRef
Kim, M. K., Hirota, T., Honma, M., et al. (2008). PASJ, 60, 991–999.CrossRef
Kovalev, Y. Y., Lobanov, A. P., Pushkarev, A. B., and Zensus, J. A. (2008). A&A, 493, 759.Google Scholar
Kovalevsky, J. and Seidelmann, P. K. (2004). Fundamentals of Astrometry, Cambridge: Cambridge University Press.CrossRefGoogle Scholar
Lanyi, G. (1984). TDAPR, 78, 152.
Lovell, J. E. J., Rickett, B. J., Macquart, J. P., et al. (2008). ApJ, 689, 108.Google Scholar
Ma, C., Arias, E. F., Eubanks, T. M., et al. (1998). AJ, 116, 516.CrossRef
Niell, A. (2006). IVS 2006 General Meeting Proceedings, Concepción, Chile, January 9–11. See http://ivscc.gsfc.nasa.gov/publications/gm2006/niell.
Nikolic, B., Richer, J., Bolton, R., and Hills, R. (2011). The Messenger, 143, 11.
Ohja, R., Fey, A. L., Charlot, P., et al. (2005). AJ, 130, 2529.
,PASJ (2008). Publ Astr. Soc. Jn., 60, No. 5.
Petrov, L., Kovalev, Y. Y., Fomalont, E., and Gordon, D. (2008). AJ, 136, 580.CrossRef
Petrov, L., Phillips, C., Bertarini, A., Murphy, T., and Sadler, E. M. (2011). MNRAS, 414, 2528.Google Scholar
Pradel, N., Charlot, P., and Lestrade, J.-F. (2006). A&A, 452, 1099.Google Scholar
Readhead, A. C. S., Walker, R. C., Pearson, T. J., and Cohen, M. H. (1980). Nature, 285, 137.CrossRef
Reid, M. J. and Brunthaler, A. (2004). ApJ, 616, 872.Google Scholar
Reid, M. J., Menton, K. M., Brunthaler, A., et al. (2009). ApJ, 693, 397.Google Scholar
Rogers, A. R. R. (1970). Radio Science, 5, 1289.
Shepherd, M. C., Pearson, J. J., and Taylor, G. B. (1994). BAAS, 26, 987.
Sovers, J., Fanselow, J. L., and Jacobs, C. S. (1998). Reviews of Modern Physics, 70, 1393.CrossRef
Sovers, J., Jacobs, S., and Lanyi, G. E. (2004). IVS 2004 General Meeting Proceedings, Ottawa, Canada, February 9–11. See http://ivscc.gsfc.nasa.gov/publications/gm2004/sovers.
Taylor, G. B., Carilli, C. L., and Perley, R. A. (2003). Synthesis imaging in radio astronomy II. ASP Conf. Ser., 180. (TCP)Google Scholar
Thompson, A. R.,Moran, J. M., and Swenson, G.W. Jr. (2001). Interferometry and Synthesis in Radio Astronomy, 2nd edn. New York, NY: John Wiley & Sons. (TMS)CrossRefGoogle Scholar
Titov, O. (2006). IVS 2006 General Meeting Proceedings, Concepción, Chile, January 9–11. See http://ivscc.gsfc.nasa.gov/publications/gm2006/titov.
Verbiest, J. P. W., Bailes, M., van Straten, W., et al. (2008). ApJ, 679, 675–680.Google Scholar
Walter, Hans G. and Sovers, O. (2000). Astrometry of Fundamental Catalogs. Heidelberg: Springer.CrossRefGoogle Scholar

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