Orion A Giant Molecular Cloud in N2H+, HC3N, and CCS

Details Orion A Giant Molecular Cloud in N2H+, HC3N, and CCS Orion A Giant Molecular Cloud in N2H+, HC3N, and CCS

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21113913t&link_type=abstract

American Astronomical Society, AAS Meeting #211, #139.13; Bulletin of the American Astronomical Society, Vol. 39, p.987

Astronomy and Astrophysics

Astronomy

Scientific paper

The "integral-shaped filament" of the Orion A giant molecular cloud was mapped in N2H+ J = 1-0 (93 GHz), and its northern end, OMC-2/3 region was observed also in HC3N J =5-4 (45 GHz) and CCS (45 and 82 GHz). The observations were carried out with Nobeyama 45-m Radio Telescope. Their distribution was compared with our previous H13CO+ map (Aso et al. 2000) and with the dust map in the literature. N2H+ distribution is similar to the dust distribution, except for the central part of the Orion Nebula, where gas temperature is high. We identified 34 cloud cores from N2H+ data, and carried out hyperfine fitting to spectra. Their average physical parameters are N2H+ excitation temperature Tex = 9.3±4.3 K, linewidth Δv = 0.92±0.52 km/s, core radius R = 0.086±0.018 pc, column density N (H2) = 4.2±1.6 1022 cm -2, average density n (H2)=7±3; 104 cm-3, and core mass M = 30.3±20.5 M&sun;. The excitation temperature is twice as high as that in Taurus cores (Tatematsu et al. 2004). The masses of cores identified both in N2H+ and in H13CO+ in OMC-2/3 are very consistent. We found one peculiar H13CO+ core which is not prominent in either N2H+, HC3N or dust. This core overlaps with the lobe of the intense outflow, which might cause H13CO+ intensity enhancement. In OMC-2/3, we detected no CCS emission. In general N2H+ and HC3N distribution is quite similar in OMC-2/3, but we observed displacement between N2H+ and HC3N over 2 arcmin scale along the OMC-3 ridge, which has a chain of Class 0-I protostars (and candidates) including X-ray protostars.

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