<i>GALEX</i>-SELECTED LYMAN BREAK GALAXIES AT<i>z</i>∼ 2: COMPARISON WITH OTHER POPULATIONS

Haberzettl, L.; Williger, G. M.; Lehnert, M. D.; Nesvadba, N. P. H.; Davies, Luke J. M.

doi:10.1088/0004-637x/745/1/96

Cited by 21 publications

(52 citation statements)

References 69 publications

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“…We choose to use a somewhat younger, 100 Myr, stellar population (Haberzettl et al 2012;Hathi et al 2013) than is typically used at these redshifts for star forming galaxies (∼300 Myr, e.g., Shapley et al 2005;Reddy et al 2008) as the Kim et al (1997) and Moller & Jakobsen (1990).…”

Section: Simulating the Faint Galaxiesmentioning

confidence: 99%

ULTRA-FAINT ULTRAVIOLET GALAXIES ATz∼ 2 BEHIND THE LENSING CLUSTER A1689: THE LUMINOSITY FUNCTION, DUST EXTINCTION, AND STAR FORMATION RATE DENSITY

Alavi

Siana

Richard

et al. 2013

ApJ

133

183

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We have obtained deep ultraviolet imaging of the lensing cluster A1689 with the WFC3/UVIS camera onboard the Hubble Space Telescope in the F275W (30 orbits) and F336W (4 orbits) filters. These images are used to identify z ∼ 2 star-forming galaxies via their Lyman break, in the same manner that galaxies are typically selected at z 3. Because of the unprecedented depth of the images and the large magnification provided by the lensing cluster, we detect galaxies 100× fainter than previous surveys at this redshift. After removing all multiple images, we have 58 galaxies in our sample in the range −19.5 < M 1500 < −13 AB mag. Because the mass distribution of A1689 is well constrained, we are able to calculate the intrinsic sensitivity of the observations as a function of source plane position, allowing for accurate determinations of effective volume as a function of luminosity. We fit the faint-end slope of the luminosity function to be α = −1.74 ± 0.08, which is consistent with the values obtained for 2.5 < z < 6. Notably, there is no turnover in the luminosity function down to M 1500 = −13 AB mag. We fit the UV spectral slopes with photometry from existing Hubble optical imaging. The observed trend of increasingly redder slopes with luminosity at higher redshifts is observed in our sample, but with redder slopes at all luminosities and average reddening of E(B − V ) = 0.15 mag. We assume the stars in these galaxies are metal poor (0.2 Z ) compared to their brighter counterparts (Z ), resulting in bluer assumed intrinsic UV slopes and larger derived values for dust extinction. The total UV luminosity density at z ∼ 2 is 4.31 +0.68 −0.60 × 10 26 erg s −1 Hz −1 Mpc −3 , more than 70% of which is emitted by galaxies in the luminosity range of our sample. Finally, we determine the global star formation rate density from UV-selected galaxies at z ∼ 2 (assuming a constant dust extinction correction of 4.2 over all luminosities and a Kroupa initial mass function) of 0.148 +0.023 −0.020 M yr −1 Mpc −3 , significantly higher than previous determinations because of the additional population of fainter galaxies and the larger dust correction factors.

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Section: Simulating the Faint Galaxiesmentioning

confidence: 99%

ULTRA-FAINT ULTRAVIOLET GALAXIES ATz∼ 2 BEHIND THE LENSING CLUSTER A1689: THE LUMINOSITY FUNCTION, DUST EXTINCTION, AND STAR FORMATION RATE DENSITY

Alavi

Siana

Richard

et al. 2013

ApJ

133

183

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“…The Lyman break can be defined by optical imaging in only three bands (Guhathakurta et al 1990;Steidel et al 1996). Thus optical LBG selection has yielded the largest samples of galaxies in the early universe (Steidel et al 1999;Shapley et al 2001;Steidel et al 2003;Ouchi et al 2004a;Giavalisco et al 2004;Dickinson et al 2004;Capak et al 2004;Sawicki & Thompson 2006;Yoshida et al 2006;Iwata et al 2007;Bouwens et al 2007Bouwens et al , 2008Bouwens et al , 2010aLy et al 2009;McLure et al 2009;Fontana et al 2010;Hathi et al 2010;Castellano et al 2010;Basu-Zych et al 2011;Bielby et al 2011;Haberzettl et al 2012;Bian et al 2013;Tilvi et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Lyman-break Galaxies at z ∼ 3 in the Subaru Deep Field: Luminosity Function, Clustering, and [O iii] Emission

Malkan

Cohen

Maruyama

et al. 2017

ApJ

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We combined deep U -band imaging from the KPNO-4m/MOSAIC camera with very deep multiwaveband imaging data from optical to near-infrared wavelengths, to select Lyman Break Galaxies (LBGs) at z ∼ 3 using U − V and V − R c colors in the Subaru Deep Field. With the resulting sample of 5161 LBGs, we construct the UV luminosity function down to M UV = −18 and find a steep faint-end slope of α = −1.78 ± 0.05. We analyze rest-frame UV-to-NIR spectral energy distributions (SEDs) generated from the median optical photometry and photometry on median-composite IR images (formed from stacks around the optical positions of LBGs). In the stacks of faint LBGs, we find a systematic background depression centered on the position of the galaxy. A series of experiments confirmed our view that this deficit results from the systematic difficulty of SExtractor (or any other object-finding routine) in finding faint galaxies in regions with higher-than-average surface densities of foreground galaxies. We corrected our stacked magnitudes for this effect and suggest that other stacking studies should also make such corrections. Best-fit stellar population templates for the stacked LBG SEDs indicate stellar masses and star-formation rates (SFRs) of log 10 (M * /M ⊙ ) ≃ 10 and ≃ 50 M ⊙ yr 1500Å (rest-frame) in the faintest bin. Such strong [OIII] emission is seen only in a miniscule fraction of the most extreme local emission-line galaxies, but it probably universal in the faint galaxies that reionized the universe. This finding has strong implications for finding and studying the most common galaxies at high redshifts with upcoming surveys. Finally, we analyze clustering by computing the angular correlation function and performing halo occupation distribution (HOD) analysis. We find a mean dark halo mass of log 10 ( M h /h −1 M ⊙ ) = 11.29 ± 0.12 for the full sample of LBGs, and log 10 ( M h /h −1 M ⊙ ) = 11.49±0.1 for the brightest half of the sample. The results support the notion that more massive dark matter halos host more luminous LBGs.

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“…From our original sample of 73 LBGs at z ∼ 1 − 2, we have identified a small subsample of 14 ILLBGs, which may represent a significant portion of the overall star formation rates in galaxies at this redshift (Haberzettl et al 2012). The properties of these galaxies make them analogous to sources in the local universe, such as LIRGs and ULIRGs (Petty et al 2009).…”

Section: Dust In Star Forming Galaxies: Infrared-luminous Lbgsmentioning

confidence: 99%

“…Our sample of 14 ILLBGs were color-magnitude selected using ground-based optical data and Spitzer data (Haberzettl et al 2012). For this study, we used Spitzer 24 µm priors to verify the locations of the objects in our sample.…”

Section: Datamentioning

confidence: 99%

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Dust properties of Z~2 infrared-luminous lyman break galaxies.

Wojno¹

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GALEX-SELECTED LYMAN BREAK GALAXIES ATz∼ 2: COMPARISON WITH OTHER POPULATIONS

Cited by 21 publications

References 69 publications

ULTRA-FAINT ULTRAVIOLET GALAXIES ATz∼ 2 BEHIND THE LENSING CLUSTER A1689: THE LUMINOSITY FUNCTION, DUST EXTINCTION, AND STAR FORMATION RATE DENSITY

ULTRA-FAINT ULTRAVIOLET GALAXIES ATz∼ 2 BEHIND THE LENSING CLUSTER A1689: THE LUMINOSITY FUNCTION, DUST EXTINCTION, AND STAR FORMATION RATE DENSITY

Lyman-break Galaxies at z ∼ 3 in the Subaru Deep Field: Luminosity Function, Clustering, and [O iii] Emission

Dust properties of Z~2 infrared-luminous lyman break galaxies.

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