STUDYING LARGE- AND SMALL-SCALE ENVIRONMENTS OF ULTRAVIOLET LUMINOUS GALAXIES

Journal Article · Fri Jul 10 00:00:00 EDT 2009 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/699/2/1307; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21333727

Basu-Zych, Antara R; Schiminovich, David ^[1]; Heinis, Sebastien; Heckman, Tim; Bianchi, Luciana ^[2]; Overzier, Roderik ^[3]; Zamojski, Michel; Barlow, Tom A; Conrow, Tim; Forster, Karl G; Friedman, Peter G; Martin, D Christopher; Morrissey, Patrick ^[4]; Ilbert, Olivier ^[5]; Koekemoer, Anton M ^[6]; Donas, Jose; Milliard, Bruno ^[7]; Lee, Young-Wook ^[8]; Madore, Barry F ^[9]

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1. Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027 (United States)
2. Center for Astrophysical Sciences, The Johns Hopkins' University, 3400 N. Charles St., Baltimore, MD 21218 (United States)
3. Max-Planck-Institut fuer Astrophysik, D-85748 Garching (Germany)
4. California Institute of Technology, MC 405-47, 1200 East California Boulevard, Pasadena, CA 91125 (United States)
5. Institute for Astronomy, 2680 Woodlawn Dr., University of Hawaii, Honolulu, HI 96822 (United States)
6. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)
7. Laboratoire d'Astrophysique de Marseille, BP8, Traverse du Siphon, F-13376 Marseille (France)
8. Center for Space Astrophysics, Yonsei University, Seoul 120-749 (Korea, Republic of)
9. Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 (United States)

Studying the environments of 0.4 < z < 1.2 ultraviolet (UV)-selected galaxies, as examples of extreme star-forming galaxies (with star formation rates (SFRs) in the range of 3-30 M{sub sun} yr{sup -1}), we explore the relationship between high rates of star formation, host halo mass, and pair fractions. We study the large- and small-scale environments of local ultraviolet luminous galaxies (UVLGs) by measuring angular correlation functions. We cross-correlate these systems with other galaxy samples: a volume-limited sample (ALL), a blue luminous galaxy sample, and a luminous red galaxy (LRG) sample. We determine the UVLG comoving correlation length to be r{sub 0} = 4.8{sup +11.6}{sub -2.4} h {sup -1} Mpc at (z) = 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 SFRs, metallicities, and dust content). Recent Hubble Space Telescope images of z {approx} 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.

• OSTI ID: 21333727
• Journal Information: Astrophysical Journal, Vol. 699, Issue 2; Other Information: DOI: 10.1088/0004-637X/699/2/1307; Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ANGULAR CORRELATION
BRIGHTNESS
COLOR
DUSTS
GALACTIC EVOLUTION
GALAXIES
MASS
MORPHOLOGY
RED SHIFT
STARS
TELESCOPES
ULTRAVIOLET RADIATION