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Any changes to this file will be lost if it is regenerated by Mendeley.  BibTeX export options can be customized via Options -> BibTeX in Mendeley Desktop  @article{Elmegreen2005,  author={Debra Meloy Elmegreen and Bruce G. Elmegreen and Douglas S. Rubin and Meredith A. Schaffer},  title={Galaxy Morphologies in the Hubble Ultra Deep Field: Dominance of Linear Structures at the Detection Limit},  journal={The Astrophysical Journal},  volume={631},  number={1},  pages={85},  url={http://stacks.iop.org/0004-637X/631/i=1/a=85},  year={2005},  abstract={Galaxies in the Hubble Ultra Deep Field (UDF) larger than 10 pixels (0 ##IMG## [http://ej.iop.org/icons/Entities/farcs.gif] {farcs} 3) have been classified according to morphology, and their photometric properties are presented. There are 269 spiral, 100 elliptical, 114 chain, 126 double-clump, 97 tadpole, and 178 clump-cluster galaxies. We also cataloged 30 B -band and 13 V -band dropouts and calculated their star formation rates. Chains, doubles, and tadpoles dominate the other types at faint magnitudes. The fraction of obvious bars among spirals is ~10%, a factor of 2-3 lower than in other deep surveys. The distribution function of axial ratios for elliptical galaxies is similar to that seen locally, suggesting that ellipticals relaxed quickly to a standardized shape. The distribution of axial ratios for spiral galaxies is significantly different than locally, having a clear peak at ~0.55 instead of a nearly flat distribution. The falloff at small axial ratio occurs at a higher value than locally, indicating thicker disks by a factor of ~2. The falloff at high axial ratio could be from intrinsic triaxial shapes or selection effects. Inclined disks should be more highly sampled than face-on disks near the surface brightness limit of a survey. Simple models and data distributions demonstrate these effects. The decreased numbers of obvious spiral galaxies at high redshifts could be partly the result of surface brightness selection.}  }  @ARTICLE{Hou2009,  author = {{Hou}, A. and {Parker}, L.~C. and {Harris}, W.~E. and {Wilman}, D.~J.  },