The arizona radio observatory CO mapping survey of galactic molecular clouds. I. the W51 region in CO and 13CO J = 2-1 emission

John H Bieging, William L. Peters, Miju Kang

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Abstract

We present 38'' resolution maps of the CO and 13CO J = 2-1 lines in the molecular clouds toward the HII region complex W51. The maps cover a 1.°25 × 1° section of the galactic plane and span +30 to +85 km s-1 (LSR) in velocity. The spectral resolution is ̃1.3 km s -1. The velocity range of the images includes all the gas in the Sagittarius spiral arm. Color figures display the peak line brightness temperature, the velocity-integrated intensity, and 2 km s-1 channel-averaged maps for both isotopologs, and also the CO/13CO J = 2-1 line intensity ratio as a function of velocity. The CO and 13CO line intensity image cubes are made available in standard FITS format as electronically readable tables. We compare our molecular line maps with the 1.1 mm continuum image from the BOLOCAM Galactic Plane Survey. From our 13CO image cube, we derive kinematic information for the 99 BGPS sources in the mapped field in the form of Gaussian component fits. The integrated 13CO line intensity and the 1.1 mm source flux density show only a modest degree of correlation for the 99 sources, likely due to a range of dust and gas physical conditions within the sources. However, the 1.1 mm continuum surface brightness and the integrated 13CO line intensity for small regions containing single BGPS sources and molecular clouds show very good correlations in many cases. Differences in the shapes of these correlations from one spatial region to another probably result from different physical conditions or structure in the clouds.

Original languageEnglish (US)
Pages (from-to)232-246
Number of pages15
JournalAstrophysical Journal, Supplement Series
Volume191
Issue number2
DOIs
StatePublished - Dec 2010

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molecular clouds
observatories
observatory
radio
continuums
spectral resolution
gas
brightness temperature
gases
kinematics
format
dust
brightness
flux density
color
physical conditions

Keywords

  • H II regions
  • ISM: clouds
  • ISM: individual objects (W51)
  • ISM: kinematics and dynamics
  • ISM: molecules

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

The arizona radio observatory CO mapping survey of galactic molecular clouds. I. the W51 region in CO and 13CO J = 2-1 emission. / Bieging, John H; Peters, William L.; Kang, Miju.

In: Astrophysical Journal, Supplement Series, Vol. 191, No. 2, 12.2010, p. 232-246.

Research output: Contribution to journalArticle

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AB - We present 38'' resolution maps of the CO and 13CO J = 2-1 lines in the molecular clouds toward the HII region complex W51. The maps cover a 1.°25 × 1° section of the galactic plane and span +30 to +85 km s-1 (LSR) in velocity. The spectral resolution is ̃1.3 km s -1. The velocity range of the images includes all the gas in the Sagittarius spiral arm. Color figures display the peak line brightness temperature, the velocity-integrated intensity, and 2 km s-1 channel-averaged maps for both isotopologs, and also the CO/13CO J = 2-1 line intensity ratio as a function of velocity. The CO and 13CO line intensity image cubes are made available in standard FITS format as electronically readable tables. We compare our molecular line maps with the 1.1 mm continuum image from the BOLOCAM Galactic Plane Survey. From our 13CO image cube, we derive kinematic information for the 99 BGPS sources in the mapped field in the form of Gaussian component fits. The integrated 13CO line intensity and the 1.1 mm source flux density show only a modest degree of correlation for the 99 sources, likely due to a range of dust and gas physical conditions within the sources. However, the 1.1 mm continuum surface brightness and the integrated 13CO line intensity for small regions containing single BGPS sources and molecular clouds show very good correlations in many cases. Differences in the shapes of these correlations from one spatial region to another probably result from different physical conditions or structure in the clouds.

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