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

Publishing date

2009-06-04

URL

arxiv.org/abs/0906.1010v1

Journals

Astrophys.J.699:1307-1320,2009

Science

Astronomy and Astrophysics

Field

Astrophysics

SubField

Galaxy Astrophysics

Additional info

35 pages, 10 Figures, accepted for publication in ApJ

Type

Scientific paper

Digital Object Identifier

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

Abstract

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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