CO in mergers. III - NGC 1614 and NGC 3256

Details CO in mergers. III - NGC 1614 and NGC 3256 CO in mergers. III - NGC 1614 and NGC 3256

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...251....1c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 251, no. 1, Nov. 1991, p. 1-10.

Astronomy and Astrophysics

Astrophysics

36

Carbon Monoxide, Elliptical Galaxies, Galactic Evolution, Interstellar Gas, Astronomical Spectroscopy, Emission Spectra, Line Shape, Molecular Gases, Spiral Galaxies

Scientific paper

The (C-12)O (1-0) and (2-1) maps presented for two southern merger remnants, NGCs 1614 and 3256 show that the molecular component is more concentrated in mergers than in parent spirals. The (C-13)O (1-0) and (2-1) spectra are also obtained; these lines are much weaker than those of (C-12)O, in keeping with determinations for such other mergers as Arp 220 and 229 and NGC 6240. The far-IR color temperature T(60/100) and the ratios L(FIR)/L(B) and L(FIR)/M(H2) evolve in the course of the merging in a correlated manner.

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