Chemodynamics of Lyman alpha emitters, Lyman break galaxies and elliptical galaxies

Mori, Masao; Umemura, Masayuki

doi:10.1051/eas:2007031

Cited by 2 publications

(1 citation statement)

References 15 publications

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“…Despite having been selected as primordial systems, LBGs exhibit sufficient metal enrichment to exclude them from being the most primitive galaxies (e.g., Pettini et al 2002 study the gravitationally lensed LBG, cB58, and find Type II supernovae residue, such as O, Mg, Si). Mori & Umemura (2007) have conducted high resolution hydrodynamic simulations that follow the chemical evolution of primordial galaxies, finding that LBGs resemble infant versions of elliptical and bulge systems in the local universe.…”

Section: Introductionmentioning

confidence: 99%

A Search for Lyman Break Galaxies in the CDF-S Using Swift UVOT

Basu-Zych,

Hornschemeier,

Hoversten

et al. 2011

Preprint

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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 aboard Swift to discover 0.5 < z < 2 Lyman break galaxies (LBGs). UVOT has covered ∼ 266 arcmin 2 at >60ks 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 GOODS-South, MUSYC, 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 Log M * /M ⊙ = 9.4 ± 0.6, which is slightly lower than z ∼ 3 LBGs ( Log M * /M ⊙ = 10.2 ± 0.4) and slightly higher compared to the z ∼ 1 CDF-S galaxies ( Log M * /M ⊙ = 8.7 ± 0.7). Similarly, our sample of z ∼ 1 LBGs has SFRs (derived using both ultraviolet and infrared data, where available) of Log SFR/(M ⊙ yr −1 ) = 0.7 ± 0.6, which is nearly an order of magnitude lower than z ∼ 3 LBGs ( Log SFR/M ⊙ yr −1 = 1.5 ± 0.4), but slightly higher than the comparison z ∼ 1 sample of CDF-S galaxies ( Log SFR/M ⊙ yr −1 = 0.2 ± 0.7). We find that our z ∼ 1 UV-dropouts have A FUV = 2.0 ± 1.0, which is higher than z ∼ 3 LBGs ( A FUV = 1.0 ± 0.5), but is similar to the distribution of dust attenuations in the other CDF-S galaxies ( A FUV ∼ 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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Section: Introductionmentioning

confidence: 99%

A Search for Lyman Break Galaxies in the CDF-S Using Swift UVOT

Basu-Zych,

Hornschemeier,

Hoversten

et al. 2011

Preprint

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The Young and the Dustless: Interpreting Radio Observations of Ultraviolet‐Luminous Galaxies

Basu-Zych

Schiminovich

Johnson

et al. 2007

ASTROPHYS J SUPPL S

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Ultraviolet Luminous Galaxies (UVLGs) have been identified as intensely star-forming, nearby galaxies. A subset of these, the supercompact UVLGs, are believed to be local analogs of high redshift Lyman Break Galaxies. Here we investigate the radio continuum properties of this important population for the first time. We have observed 42 supercompact UVLGs with the VLA, all of which have extensive coverage in the UV/optical by GALEX and SDSS. Our analysis includes comparison samples of multiwavelength data from the Spitzer First Look Survey and from the SDSS-Galex matched catalogs. In addition we have Spitzer MIPS data for 24 of our galaxies and find that they fall on the -2radio-FIR correlation of normal star-forming galaxies. We find that our galaxies have lower radio-to-UV ratios and lower Balmer decrements than other local galaxies with similar (high) star formation rates. Optical spectra show they have lower D n (4000) and Hδ A indices, higher Hβ emission-line equivalents widths, and higher [OIII]5007/Hβ emission-line ratios than normal star forming galaxies. Comparing these results to galaxy spectral evolution models we conclude that supercompact UVLGs are distinguished from normal star forming galaxies firstly by their high specific star formation rates. Moreover, compared to other types of galaxies with similar star formation rates, they have significantly less dust attenuation. In both regards they are similar to Lyman Break Galaxies. This suggests that the process that causes star formation in the supercompact UVLGs differs from other local star forming galaxies, but may be similar to Lyman Break Galaxies.

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Chemodynamics of Lyman alpha emitters, Lyman break galaxies and elliptical galaxies

Cited by 2 publications

References 15 publications

A Search for Lyman Break Galaxies in the CDF-S Using Swift UVOT

A Search for Lyman Break Galaxies in the CDF-S Using Swift UVOT

The Young and the Dustless: Interpreting Radio Observations of Ultraviolet‐Luminous Galaxies

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