Submillimeter observations of CO in the W3 core

Details Submillimeter observations of CO in the W3 core Submillimeter observations of CO in the W3 core

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...426..215h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 426, no. 1, p. 215-233

Astronomy and Astrophysics

Astronomy

18

Carbon Monoxide, Gas Jets, Gas Temperature, H Ii Regions, Infrared Spectra, Molecular Clouds, Molecular Excitation, Radio Astronomy, Submillimeter Waves, Infrared Astronomy, Radio Telescopes

Scientific paper

We present observations of CO J = 3 goes to 2 and J = 6 goes to 5 emission from the W3 IRS 5-IRS 4 region. A high-sensitivity spectrum in CO J = 3 goes to 2 at IRS 5 shows extremely high velocity gas with a total velocity width of 200 km/s. The CO J = 3 goes to 2 map shows the presence of compact blueshifted and redshifted lobes centered on IRS 5. Both lobes have diameters at half-maximum of about 8 sec. Spectra in CO and (13)CO J = 3 goes to 2 toward IRS 4 have red and blue pedestal features, indicating moving gas associated with IRS 4. The new observations are combined with our previous data in CO and (13)CO J = 2 goes to 1 lines to determine the gas temperature of the wing components associated with IRS 5 and IRS 4. the gas temperature for the red and blue outer (or (13)CO emission-free) wings in IRS 5 is similar at 60 K. The gas temperature is 76 K for the red inner wing and is 38 K for the blue inner wing. The blueshifted gas toward IRS 4 has an average gas temperature of 49 K, although there is a systematic increase in gas temperature with velocity, the temperature reaching to 160 K. For the outer red pedestal part in IRS 4, the gas temperature is at least 45 K. The excitation temperature for the widespread -38 km/s absorption feature in CO J = 2 goe to 1 and J = 3 goes to 2 spectra is about 24 K at the IRS 5 position, and is about 16 K at the IRS 4 position. The excitation temperatures and velocities from submillimeter CO observations are compared with those independently found from IR observations of CO in absorption. We suggest that the -38 km/s absorption component in the submillimeter CO spectra at IRS 5 corresponds to the cold component with N(CO) = 1.1 x 1019/sq cm found from the infrared CO spectra of IRS 5. The blue outer wing (VLSR = -105 to -50 km/s) in the CO J = 3 goes to 2 spectra at IRS 5 probably corresponds to the blueshifted absorption component found in the IR CO spectrum of IRS 5.

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