The Inner 200pc: Hot Dense Gas

Christopher L. Martin, Wilfred M. Walsh, Kecheng Xiao, Adair P. Lane, Christopher K Walker, Antony A. Stark

Research output: Contribution to journalArticle

1 Citation (Scopus)

Abstract

We present fully-sampled maps of 461GHz CO J = 4 → 3, 807GHz CO J = 7 → 6, and 492GHz [CI]3P13P0 emission from the inner 3 degrees of the Galactic Center region taken with the Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) in 2001-2002. The data cover -1°.3 < ℐ < 2°, -0°.3 < b < 0°.2 with 0.5′ spacing, resulting in spectra in 3 transitions at over 24,000 positions on the sky. The CO J = 4 → 3 emission is found to be essentially coextensive with lower-J transitions of CO. The CO J = 7 → 6 emission is spatially confined to a far smaller region than the lower-J CO lines. The [CI] 3P13P0 emission has a spatial extent similar to the low-J CO emission, but is more diffuse. Bright CO J = 7 → 6 emission is detected in the well-known Galactic Center clouds SgrA and SgrB. Analyzing our CO J = 7 → 6 and CO J = 4 → 3 data in conjunction with J = 1 → 0 12CO and 13CO data previously observed with the Bell Laboratories 7-m antenna, we apply a Large Velocity Gradient (LVG) model to estimate the kinetic temperature and density of molecular gas in the inner 200 pc of the Galactic Center region. Typical pressures in the Galactic Center gas are n(H2) · Tkin ∼ 105.2 Kcm-3. We present an (ℐ, b) map of molecular hydrogen column density derived from our LVG results.

Original languageEnglish (US)
Pages (from-to)93-99
Number of pages7
JournalAstronomische Nachrichten
Volume324
Issue numberSUPPL.1
DOIs
StatePublished - Sep 2003

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gases
gas
gradients
molecular gases
bells
sky
antenna
observatories
spacing
antennas
observatory
telescopes
hydrogen
kinetics
estimates
temperature

Keywords

  • Galaxy: center
  • Galaxy: kinematics and dynamics
  • ISM: atoms
  • ISM: general
  • ISM: molecules

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Martin, C. L., Walsh, W. M., Xiao, K., Lane, A. P., Walker, C. K., & Stark, A. A. (2003). The Inner 200pc: Hot Dense Gas. Astronomische Nachrichten, 324(SUPPL.1), 93-99. https://doi.org/10.1002/asna.200385109

The Inner 200pc : Hot Dense Gas. / Martin, Christopher L.; Walsh, Wilfred M.; Xiao, Kecheng; Lane, Adair P.; Walker, Christopher K; Stark, Antony A.

In: Astronomische Nachrichten, Vol. 324, No. SUPPL.1, 09.2003, p. 93-99.

Research output: Contribution to journalArticle

Martin, CL, Walsh, WM, Xiao, K, Lane, AP, Walker, CK & Stark, AA 2003, 'The Inner 200pc: Hot Dense Gas', Astronomische Nachrichten, vol. 324, no. SUPPL.1, pp. 93-99. https://doi.org/10.1002/asna.200385109
Martin CL, Walsh WM, Xiao K, Lane AP, Walker CK, Stark AA. The Inner 200pc: Hot Dense Gas. Astronomische Nachrichten. 2003 Sep;324(SUPPL.1):93-99. https://doi.org/10.1002/asna.200385109
Martin, Christopher L. ; Walsh, Wilfred M. ; Xiao, Kecheng ; Lane, Adair P. ; Walker, Christopher K ; Stark, Antony A. / The Inner 200pc : Hot Dense Gas. In: Astronomische Nachrichten. 2003 ; Vol. 324, No. SUPPL.1. pp. 93-99.
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AU - Stark, Antony A.

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AB - We present fully-sampled maps of 461GHz CO J = 4 → 3, 807GHz CO J = 7 → 6, and 492GHz [CI]3P1 → 3P0 emission from the inner 3 degrees of the Galactic Center region taken with the Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) in 2001-2002. The data cover -1°.3 < ℐ < 2°, -0°.3 < b < 0°.2 with 0.5′ spacing, resulting in spectra in 3 transitions at over 24,000 positions on the sky. The CO J = 4 → 3 emission is found to be essentially coextensive with lower-J transitions of CO. The CO J = 7 → 6 emission is spatially confined to a far smaller region than the lower-J CO lines. The [CI] 3P1 → 3P0 emission has a spatial extent similar to the low-J CO emission, but is more diffuse. Bright CO J = 7 → 6 emission is detected in the well-known Galactic Center clouds SgrA and SgrB. Analyzing our CO J = 7 → 6 and CO J = 4 → 3 data in conjunction with J = 1 → 0 12CO and 13CO data previously observed with the Bell Laboratories 7-m antenna, we apply a Large Velocity Gradient (LVG) model to estimate the kinetic temperature and density of molecular gas in the inner 200 pc of the Galactic Center region. Typical pressures in the Galactic Center gas are n(H2) · Tkin ∼ 105.2 Kcm-3. We present an (ℐ, b) map of molecular hydrogen column density derived from our LVG results.

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KW - ISM: general

KW - ISM: molecules

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