Detection of Sagittarius A* at 330 MHz With the Very Large Array
Abstract
The central radio-bright region of our Galaxy, known as the Sagittarius Complex, is composed of three major components: the supernova remnant (SNR) Sgr A East, the Sgr A West H II region, and Sgr A*, recently established as our Galaxy's central massive black hole (e.g., Ghez et al. 2000; Eckart et al. 2002). Models attempting to explain the emission from Sgr A* fall into three broad classes. Emission is modeled as arising from thermal sources, such as a low-temperature accretion disk, from nonthermal sources such as a jet (e.g., Melia & Falcke 2001 and references therein), or from a mixture of the two. Such models are constrained primarily by the observed spectrum of Sgr A*, but large gaps in frequency coverage exist. For this reason, filling in such gaps, as with the recent near-IR detections (Ghez et al. 2004; Genzel et al. 2003), and extending the range of frequencies over which the source is observed is important in order to place additional observational constraints on these models.
Document Details
- Document Type
- Technical Report
- Publication Date
- Jan 20, 2004
- Accession Number
- ADA464418
Entities
People
- Michael E. Nord
- N. Duric
- Namir E. Kassim
- T. Joseph W. Lazio
- W. M. Goss
Organizations
- United States Naval Research Laboratory