Radio continuum and radio recombination line observations of sagittarius B1 and G0.6-0.0

David M. Mehringer*, F. Yusef-Zadeh, Patrick Palmer, W. M. Goss

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

32 Scopus citations

Abstract

The Very Large Array (VLA) was used to make high-resolution 3.6, 6, and 20 cm continuum and H110α recombination line observations of the Sgr B region. Although Sgr B2 has been the subject of numerous VLA investigations, this study is the first VLA investigation of Sgr B1 (G0.5-0.0) and G0.6-0.0. A major goal of this study was to image the ionized gas in Sgr B1 at high resolution. Unlike Sgr B2, which is dominated by numerous compact components, the emission from Sgr B1 arises from a wealth of extended bright rim and shell-like structures. One of these features is a bar of ionized gas approximately 6 pc in length. No other feature of this type and size has been previously discovered in the star-forming region. The presence of these large structures might be the result of individual compact H II regions having expanded and coalesced over time Thus Sgr B1 may be an evolved star-forming region. Another purpose of this study was to investigate the kinematics of the ionized gas in Sgr B1. The recombination line data indicate that there are two regions in Sgr B1 that differ substantially in their kinematics. A single line with a width of ∼30 km s-1 is observed on the western side of the region, while multiple velocity components are observed on the eastern side. The ionized gas in Sgr B1 has velocities predominantly in the range of 30-50 km s-1, although emission on the eastern side can be seen over a velocity range of 120 km s-1. Since the velocity of the ionized gas in Sgr B2 is near 65 km s-1 the proximity of Sgr B1 and Sgr B2 seems to be more than a chance superposition. The region G0.6-0.0 lies between the two major components of Sgr B and contains at least four compact sources. Its velocity is intermediate between Sgr B1 and Sgr B2. In addition, an arc of emission to the east and south of these compact components seems to bridge Sgr B1 and Sgr B2, thus strengthening the argument that these regions are physically related.

Original languageEnglish (US)
Pages (from-to)168-181
Number of pages14
JournalAstrophysical Journal
Volume401
Issue number1
DOIs
StatePublished - Dec 10 1992

Keywords

  • Galaxy: center
  • H II regions
  • ISM: Individual (Sgr B)
  • ISM: kinematics and dynamics
  • Radio continuum: interstellar
  • Radio lines: atomic

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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