Star formation and chemical abundances in clumpy irregular galaxies

Details Star formation and chemical abundances in clumpy irregular galaxies Star formation and chemical abundances in clumpy irregular galaxies

Jan 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...252..487b&link_type=abstract

Astrophysical Journal, Part 1, vol. 252, Jan. 15, 1982, p. 487-495.

Astronomy and Astrophysics

Astrophysics

25

B Stars, Chemical Composition, Galactic Structure, O Stars, Star Formation, Abundance, Data Reduction, Electron Density (Concentration), Electron Energy, Galactic Nuclei, H Ii Regions, Nebulae, Supernova Remnants

Scientific paper

Clumpy irregular galaxies consist of several bright clumps which are huge H II complexes (about 100 times brighter and more massive than 30 Doradus) and contain about 100,000 O and B stars. Image-tube spectrograms with 1-3 A resolution have been obtained of the brightest emission regions of three clumpy galaxies and one candidate clumpy galaxy with the Mauna Kea 2.24 m telescope. The electron temperatures were found to be in the range 7000-9000 K and electron densities a few hundred per cu cm - quite typical for normal H II regions. The abundances of O, N, S in Mrk 432 are comparable to those in Orion, while the three clumpy galaxies are slightly deficient in O and S (by factors of 2 to 4) and N (by factors of 3 to 6). The galaxies appear to be normal (like Sc galaxies) in mass and composition. Supernovae remnants are indicated by the high forbidden S II/H alpha ratio. Possible triggering mechanisms for the exceptional star formation activity are discussed.

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