Other
Scientific paper
Oct 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...380..384w&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 380, Oct. 20, 1991, p. 384-391. Research supported by W.M. Keck Foundation
Other
44
Molecular Excitation, Molecular Gases, Spiral Galaxies, Emission Spectra, Far Ultraviolet Radiation, Galactic Nuclei, Interstellar Matter, Star Formation
Scientific paper
Observational results are reported for the J = 3-2 and J = 2-1 lines of (C-13)O and (C-12)O with 22-24-arcsec resolution in the central region of the spiral galaxy NGC 253. Most of the (C-13) J = 3-2 line emission is found to originate in a source less than approximately 15 arcsec (180 pc), while the 40 x 10 arcsec FWHM barlike feature observed by Canzian et al. (1988) dominates the emission in other CO lines. Far-UV heating of PDRs by a central source or by distributed OB stars can warm the molecular gas sufficiently to explain the observed temperatures of the nuclear component. The molecular gas outside the central 20-arcsec diameter region is both cooler and less dense than inside this region, as determined from the spatial variation of the (C-13)O J = 3-2 intensity relative to that of (C-13)O J = 2-1 and to the lines of high dipole moment molecules. The density of molecular gas at a position greater than approximately 30 arcsec to the northeast of the nucleus is not greater than 10,000/cu cm, which accounts for the low (R-12)32 observed.
Bash Frank N.
Israel Frank P.
Jaffe Daniel T.
Wall William F.
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