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The Galactic Center at 327 MHz

Published online by Cambridge University Press:  26 May 2016

T.N. LaRosa ,
Namir E. Kassim ,
T. Joseph W. Lazio  and
S.D. Hyman
T.N. LaRosa
Affiliation:
Department of Biological and Physical Sciences, Kennesaw State University, 1000 Chastain Rd., Kennesaw, GA 30144 USA
Namir E. Kassim
Affiliation:
Code 7213, Remote Sensing Division, Naval Research Laboratory, Washington, DC 20375—5351 USA
T. Joseph W. Lazio
Affiliation:
Code 7213, Remote Sensing Division, Naval Research Laboratory, Washington, DC 20375—5351 USA
S.D. Hyman
Affiliation:
Department of Physics, Sweet Briar College, Sweet Briar, VA 24595 USA

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Figure 1 presents a wide-field, high dynamic-range, 327 MHz VLA2 image of the Galactic center (GC). This image was constructed from archival VLA data using new 3-D image restoration techniques which resolve the problem of non-coplanar baselines encountered at long wavelengths. In a recent paper (LaRosa et al. 2000) we presented a catalog of over a hundred sources from this image, 23 extended sources and 78 small-diameter sources. The catalog contains flux densities, positions, sizes, and, where possible, a 20/90 cm spectral index. We also present subimages of all the extended sources. We refer the reader to LaRosa et al. (2000) for the details. In this note we will concentrate on observations of the nonthermal filaments and briefly describe a new model for their formation.

The origin and evolution of the nonthermal filaments (NTFs) observed in the GC is an outstanding problem. All of the 7 classified NTFs are visible on Figure 1: Four of these are labeled threads, the other three are the “Snake,” the “Pelican,” and the Sgr C filament. The wide-field imaging at 327 MHz lead to the discovery of the “Pelican” (Lang et al. 1999). This filament has the distinction of being the farthest NTF in projection from Sgr A and the only NTF that is parallel to the Galactic plane. One critical issue for understanding the activity and overall structure of the GC is whether these filamentary sources trace a pervasive, large-scale magnetic field or are local independent structures (e.g., Yusef-Zadeh 1989; Morris 1994, 1996; Uchida & Gusten 1995; Yusef-Zadeh, Wardle & Parastaran 1997; Shore & LaRosa 1999; Lang et al. 1999; Lang, Morris & Echevarria 1999; LaRosa et al. 2000).

Type
Part 5: Galactic Surveys and Extended Emission
Information
Symposium - International Astronomical Union , Volume 199: The Universe at Low Radio Frequencies , 2002 , pp. 268 - 271
Copyright
Copyright © Astronomical Society of the Pacific 2002 

References

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