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|Title:||Oxygen abundances in low surface brightness disk galaxies|
|Authors:||McGaugh, Stacy S.|
|Affiliation:||AA(University of Michigan, Ann Arbor, MI, US)|
|Publication:||Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 426, no. 1, p. 135-149 (ApJ Homepage)|
|NASA/STI Keywords:||Abundance, Brightness, Disk Galaxies, Galactic Evolution, H Ii Regions, Line Spectra, Metallicity, Oxygen, Star Formation Rate, Balmer Series, Cameras, Charge Coupled Devices, Interstellar Magnetic Fields, Ionization, Massive Stars, Reflecting Telescopes, Spectrographs|
The oxygen abundances in the H II regions of a sample of low surface
brightness (LSB) disk galaxies are presented. In general, LSB galaxies
are found to be metal poor (Z less than (1/3) x Zsolar).
Indeed, some LSB galaxies rival the lowest abundance extragalactic
objects known, and this sample greatly increases the number of very low
metallicity systems known. These low metallicities indicate that LSB
galaxies evolve slowly, forming relatively few stars over a Hubble time.
The low metallicities of LSB galaxies occur even though many are
comparable in size and mass to the prominent spirals which define the
Hubble sequence. As well as being low in surface brightness, these
galaxies tend to be isolated. This suggests that surface mass density
and environment are more relevant to galaxy evolution than gross size.
Despite the low surface brightness of the disks, massive (M greater than
60 solar masses) stars are inferred to be present and no abnormality of
the interstellar magnetic field (IMF) is indicated. Many low-excitation
H II regions exist at low metallicity in LSB galaxies, and the
ionization parameter is not tightly correlated with metallicity.
However, there does seem to be a significant envelope of maximum
ionization at a given metallicity.
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