A Search for Lyman Break Galaxies in the Chandra Deep Field South Using Swift Ultraviolet/Optical Telescope

Details A Search for Lyman Break Galaxies in the Chandra Deep Field South Using Swift Ultraviolet/Optical Telescope A Search for Lyman Break Galaxies in the Chandra Deep Field South Using Swift Ultraviolet/Optical Telescope

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...739...98b&link_type=abstract

The Astrophysical Journal, Volume 739, Issue 2, article id. 98 (2011).

Astronomy and Astrophysics

Astronomy

Galaxies: Evolution, Galaxies: Starburst, Methods: Analytical, Ultraviolet: Galaxies

Scientific paper

While the Swift satellite is primarily designed to study gamma-ray bursts, its ultraviolet and optical imaging and spectroscopy capabilities are also being used for a variety of scientific programs. In this study, we use the UV/Optical Telescope (UVOT) instrument on board Swift to discover 0.5 < z < 2 Lyman break galaxies (LBGs). UVOT has covered ~266 arcmin2 at >60 ks exposure time, achieving a limiting magnitude of u < 24.5, in the Chandra Deep Field South (CDF-S). Applying UVOT near-ultraviolet color selection, we select 50 UV-dropouts from this UVOT CDF-S data. We match the selected sources with available multiwavelength data from Great Observatories Origins Deep Survey (GOODS) South, Multiwavelength Survey by Yale-Chile, and COMBO-17 to characterize the spectral energy distributions for these galaxies and determine stellar masses, star formation rates (SFRs), and dust attenuations. We compare these properties for LBGs selected in this paper versus z ~ 3 LBGs and other CDF-S galaxies in the same redshift range (0.5 < z < 2), identified using photometric redshift techniques. The z ~ 1 LBGs have stellar masses of langlogM */M sunrang = 9.4 ± 0.6, which is slightly lower than z ~ 3 LBGs (langlogM */M sunrang = 10.2 ± 0.4) and slightly higher compared with the z ~ 1 CDF-S galaxies (langlogM */M sunrang = 8.7 ± 0.7). Similarly, our sample of z ~ 1 LBGs has SFRs (derived using both ultraviolet and infrared data, where available) of langlogSFR/(M sun yr-1)rang = 0.7 ± 0.6, nearly an order of magnitude lower than z ~ 3 LBGs (langlogSFR/M sun yr-1rang = 1.5 ± 0.4), but slightly higher than the comparison z ~ 1 sample of CDF-S galaxies (langlogSFR/M sun yr-1rang = 0.2 ± 0.7). We find that our z ~ 1 UV-dropouts have langA FUVrang = 2.0 ± 1.0, which is higher than z ~ 3 LBGs (langA FUVrang = 1.0 ± 0.5), but similar to the distribution of dust attenuations in the other CDF-S galaxies (langA FUVrang ~ 2.8 ± 1.5). Using the GOODS-South multiwavelength catalog of galaxies, we simulate a larger and fainter sample of LBGs to compare their properties with those of the UVOT-selected LBG sample. We conclude that UVOT can be useful for finding and studying the bright end of 0.5 < z < 2.0 LBGs.

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