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Title:
A Wide-Field 90 Centimeter VLA Image of the Galactic Center Region [ Erratum: 2000AJ....119.3145L ]
Authors:
LaRosa, T. N.; Kassim, Namir E.; Lazio, T. Joseph W.; Hyman, S. D.
Affiliation:
AA(Department of Biological and Physical Sciences, Kennesaw State University, 1000 Chastain Road, Kennesaw, GA 30144; ), AB(Remote Sensing Division, Naval Research Laboratory, Code 7213, Washington, DC 20375-5351 , ), AC(Remote Sensing Division, Naval Research Laboratory, Code 7213, Washington, DC 20375-5351 , ), AD(Department of Physics, Sweet Briar College, Sweet Briar, VA 24595; )
Publication:
The Astronomical Journal, Volume 119, Issue 1, pp. 207-240. (AJ Homepage)
Publication Date:
01/2000
Origin:
UCP
AJ Keywords:
GALAXY: CENTER, RADIO CONTINUUM
DOI:
10.1086/301168
Bibliographic Code:
2000AJ....119..207L

Abstract

We present a wide-field, high dynamic range, high-resolution, long-wavelength (λ=90 cm) VLA image of the Galactic center region. The image is centered on Sgr A, covers an area of 4degx5deg with an angular resolution of 43", and has a rms sensitivity of ~5 mJy beam-1. The image was constructed from archival (1989 and 1991) VLA data of Pedlar et al. and Anantharamaiah et al. using new three-dimensional image restoration techniques. These three-dimensional imaging techniques resolve the problem of non-coplanar baselines encountered at long wavelengths and yield distortion-free imaging of far-field sources with improved sensitivity. At λ=90 cm the VLA is sensitive to both thermal and nonthermal emission and the resulting image gives an unprecedented contextual perspective of the large-scale radio structure in this unique and complicated region. We have catalogued over a hundred sources from this image and present for each source its 90 cm flux density, position, and size. For many of the small- diameter sources, we also derive the 20/90 cm spectral index. The spectral index as a function of length along several of the isolated nonthermal filaments has been estimated and found to be constant. We have found six new small-diameter sources, as well as several extended regions of emission, which are clearly distinct sources that have not been previously identified at higher frequencies. These data are presented as a first epoch of VLA observations that can be used to search for source variability in conjunction with a second epoch of observations that were recently initiated.

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