Document Type
Article
Publication Date
2-1-1994
Abstract
We present UBVI surface photometry of a sample of low surface brightness (LSB) disk galaxies. LSB disk galaxies are fairly well described as exponential disks with no preferred value for either scale length, central surface brightness, or rotational velocity. Indeed, the distribution of scale lengths is indistinguishable from that of high surface brightness spirals, indicating that dynamically similar galaxies (e.g., those with comparable v2R) exist over a large range in surface density. These LSB galaxies are strikingly blue. The complete lack of correlation between central surface brightness and color rules out any fading scenario. Similarly, the oxygen abundances inferred from H II region spectra are uncorrelated with color so the low metallicities are not the primary cause of the blue colors. While these are difficult to interpret in the absence of significant star formation, the most plausible scenario is a stellar population with a young mean age stemming from late formation and subsequent slow evolution. These properties suggest that LSB disks formed from low initial overdensities with correspondingly late collapse times.
Keywords
astronomical photometry, brightness, disk galaxies, galactic evolution, galactic structure; H Ii regions, spiral galaxies, star formation, stellar composition, stellar luminosity, surface properties, abundance, charge coupled devices, interplanetary magnetic fields, metallicity, oxygen, radial distribution, stellar color, astronomy, galaxies: stellar content, galaxies: spiral, astrophysics
Publication Title
Astronomical Journal
Rights
© The American Astronomical Society. All rights reserved. This content is free to access, download, and share. For all other uses, you must obtain permission to reuse content: https://journals.aas.org/article-charges-and-copyright/#AAS_material
Recommended Citation
McGaugh, S. S. and Bothun, G. D., “Structural Characteristics and Stellar Composition of Low Surface Brightness Disk Galaxies”, The Astronomical Journal, vol. 107, IOP, p. 530, 1994. doi:10.1086/116874.
Manuscript Version
Final Publisher Version