Molecular hydrogen in the young starburst in NGC 253

Details Molecular hydrogen in the young starburst in NGC 253 Molecular hydrogen in the young starburst in NGC 253

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986inpr.conf..109r&link_type=abstract

In NASA. Ames Research Center Summer School on Interstellar Processes; Abstracts of Contributed Papers p 109 (SEE N87-15043 06-

Physics

Emission Spectra, Flare Stars, Hydrogen Clouds, Line Spectra, Molecular Gases, Starburst Galaxies, Acceleration (Physics), Galactic Evolution, Luminosity, Supernovae

Scientific paper

Shocked molecular hydrogen has been observed around the nucleus of the nearby galaxy, NGC 253. This galaxy has a relatively modest luminosity (approx. 3 x 10 to the 10th power solar luminosities) and appears to have no distortions or companions that would indicate a possible interaction. The energy of the galaxy appears to be derived primarily from a starburst. Thus, our observations have caused us to examine the starburst process in some detail to identify how the molecular hydrogen is excited. It is proposed that the molecular hydrogen emission is produced by collisions of dense molecular clouds accelerated by supernovae explosions. Within the nucleus, this process occurs early in the life of the starbust. This suggest a sequence of nuclear starburst development; examples along this sequence from young to old would include NGC 253, M82, NGC 1097, and M31.

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