Primary Beam and Dish Surface Characterization at the Allen Telescope Array by Radio Holography

Autor: ATA GROUP, Atkinson, Shannon, Backer, D. C., Backus, P. R., Barott, William, Bauermeister, Amber, Blitz, Leo, Bock, D. C. -J., Bower, Geoffrey C., Bradford, Tucker, Cheng, Calvin, Croft, Steve, Dexter, Matt, Dreher, John, Engargiola, Greg, Fields, Ed, Heiles, Carl, Helfer, Tamara, Jordan, Jane, Jorgensen, Susan, Kilsdonk, Tom, Gutierrez-Kraybill, Colby, Keating, Garrett, Law, Casey, Lugten, John, MacMahon, D. H. E., McMahon, Peter, Milgrome, Oren, Siemion, Andrew, Smolek, Ken, Thornton, Douglas, Pierson, Tom, Randall, Karen, Ross, John, Shostak, Seth, Tarter, J. C., Urry, Lynn, Werthimer, Dan, Williams, Peter K. G., Whysong, David, Harp, G. R., Ackermann, R. F., Nadler, Z. J., Blair, Samantha K., Davis, M. M., Wright, M. C. H., Forster, J. R., DeBoer, D. R., Welch, W. J.
Rok vydání: 2012
Předmět:
Zdroj: IEEE Transactions on Antennas and Propagation, 59 (2011) p. 2004
Druh dokumentu: Working Paper
DOI: 10.1109/TAP.2011.2122214
Popis: The Allen Telescope Array (ATA) is a cm-wave interferometer in California, comprising 42 antenna elements with 6-m diameter dishes. We characterize the antenna optical accuracy using two-antenna interferometry and radio holography. The distortion of each telescope relative to the average is small, with RMS differences of 1 percent of beam peak value. Holography provides images of dish illumination pattern, allowing characterization of as-built mirror surfaces. The ATA dishes can experience mm-scale distortions across -2 meter lengths due to mounting stresses or solar radiation. Experimental RMS errors are 0.7 mm at night and 3 mm under worst case solar illumination. For frequencies 4, 10, and 15 GHz, the nighttime values indicate sensitivity losses of 1, 10 and 20 percent, respectively. The ATA.s exceptional wide-bandwidth permits observations over a continuous range 0.5 to 11.2 GHz, and future retrofits may increase this range to 15 GHz. Beam patterns show a slowly varying focus frequency dependence. We probe the antenna optical gain and beam pattern stability as a function of focus and observation frequency, concluding that ATA can produce high fidelity images over a decade of simultaneous observation frequencies. In the day, the antenna sensitivity and pointing accuracy are affected. We find that at frequencies greater than 5 GHz, daytime observations greater than 5 GHz will suffer some sensitivity loss and it may be necessary to make antenna pointing corrections on a 1 to 2 hourly basis.
Comment: 19 pages, 23 figures, 3 tables, Authors indicated by an double dagger ({\ddag}) are affiliated with the SETI Institute, Mountain View, CA 95070. Authors indicated by a section break ({\S}) are affiliated with the Hat Creek Radio Observatory and/or the Radio Astronomy Laboratory, both affiliated with the University of California Berkeley, Berkeley CA
Databáze: arXiv
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