Studying Large and Small Scale Environments of Ultraviolet Luminous Galaxies

Details Studying Large and Small Scale Environments of Ultraviolet Luminous Galaxies Studying Large and Small Scale Environments of Ultraviolet Luminous Galaxies

2009-06-04

arxiv.org/abs/0906.1010v1

Astrophys.J.699:1307-1320,2009

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

35 pages, 10 Figures, accepted for publication in ApJ

Scientific paper

10.1088/0004-637X/699/2/1307

Studying the environments of 0.4 =1.0, which is unable to constrain the halo mass for this sample. However, we find that UVLGs form close (separation < 30 kpc) pairs with the ALL sample, but do not frequently form pairs with LRGs. A rare subset of UVLGs, those with the highest FUV surface brightnesses, are believed to be local analogs of high redshift Lyman Break Galaxies (LBGs) and are called Lyman Break Analogs (LBAs). LBGs and LBAs share similar characteristics (i.e., color, size, surface brightness, specific star formation rates, metallicities, and dust content). Recent HST images of z~0.2 LBAs show disturbed morphologies, signs of mergers and interactions. UVLGs may be influenced by interactions with other galaxies and we discuss this result in terms of other high star-forming, merging systems.

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