Lyα Emission‐Line Galaxies at<i>z</i>= 3.1 in the Extended Chandra Deep Field–South

Grönwall, C.; Ciardullo, Robin; Hickey, Thomas J.; Gawiser, Eric; Feldmeier, John J.; Dokkum, Pieter van; Urry, C. Megan; Herrera, David; Lehmer, Bret; Infante, L.; Orsi, Álvaro; Marchesini, Danilo; Blanc, Guillermo A.; Francke, Harold; Lira, P.; Treister, Ezequiel

doi:10.1086/520324

Cited by 362 publications

(760 citation statements)

References 74 publications

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“…With modern observing facilities, is has been possible to study emission-selected galaxies to much deeper rest-frame flux limits (e.g. Sawicki & Thompson 2006;Gronwall et al 2007;Ouchi et al 2008;Rauch et al 2008;Grove et al 2009;Reddy & Steidel 2009;Cassata et al 2011;Trainor & Steidel 2012;Alavi et al 2014). Dedicated campaigns to detect emitting counterparts of DLAs have been carried out: using long-slit spectroscopy (e.g.…”

Section: Galaxy Counterparts Of Metal-rich Dlas 2739mentioning

confidence: 99%

Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Hartoog

Fynbo

Kaper

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: http://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. ABSTRACTWe present observations of three new sources in the European Southern Observatory VLT/Xshooter survey dedicated to the detection of the emitting counterparts of damped Lyα (DLA) systems towards bright quasars (QSOs). The aim is to bridge the observational gap between absorption (i.e. DLAs) and emission-selected galaxies at z ∼ 2.2-2.5, in order to get a more complete picture of (proto)galaxies around this epoch. The hypothesis is that because DLA galaxies fulfil metallicity-velocity width and luminosity-metallicity relations, highmetallicity DLAs are more likely to be detected in emission. The region around each QSO is covered with slits (1. We conclude that focusing on metal-rich DLAs is a good way to find counterparts, but the non-detections at high metallicity (e.g. that of the DLA in J105744.5+062914) show that there is not a one-to-one relationship, and cautions us to not naively apply the properties of the DLA counterparts to all metal-rich DLAs.

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Section: Galaxy Counterparts Of Metal-rich Dlas 2739mentioning

confidence: 99%

Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Hartoog

Fynbo

Kaper

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…The study of the high-redshift universe and the early evolution of galaxies has primarily relied on two techniques to obtain large samples of high-redshift galaxies, the Lyman break technique (LBGs; Steidel et al 1999;Ouchi et al 2004;Bouwens & Illingworth 2006, and references therein) and narrowband surveys targeting Lyα emitting galaxies (LAEs; Hu & McMahon 1996;Rhoads & Malhotra 2001;Ajiki et al 2003;Hu et al 2004Hu et al , 2010Taniguchi et al 2005;Murayama et al 2007;Gronwall et al 2007;Ouchi et al 2008, and references therein). Studying the difference in the nature and properties of the two populations, selected by these two techniques, helps to understand early stages of galaxy formation and provides constraints on reionization.…”

Section: Introductionmentioning

confidence: 99%

“…The varying degree of overlap between the two techniques and how it changes with redshift is still an open question. Several authors have explored this by comparing spectral energy distribution (SED) properties of these two populations (Gawiser et al 2006;Gronwall et al 2007). Even less understood is the degree of overlap in the Lyα properties of the populations selected by these two techniques.…”

Section: Introductionmentioning

confidence: 99%

Lyα EMISSION FROM HIGH-REDSHIFT SOURCES IN COSMOS

Mallery

Mobasher

Capak

et al. 2012

ApJ

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We investigate spectroscopically measured Lyα equivalent widths (EWs) and escape fractions of 244 sources of which 95 are Lyman break galaxies (LBGs) and 106 Lyman alpha emitters (LAEs) at z ∼ 4.2, z ∼ 4.8, and z ∼ 5.6 selected from intermediate and narrowband observations. The sources were selected from the Cosmic Evolution Survey and observed with the DEIMOS spectrograph. We find that the distribution of EWs shows no evolution with redshift for both the LBG selected sources and the intermediate/narrowband LAEs. We also find that the Lyα escape fraction of intermediate/narrowband LAEs is on average higher and has a larger variation than the escape fraction of LBG selected sources. The escape fraction does not show a dependence with redshift. Similar to what has been found for LAEs at low redshifts, the sources with the highest extinctions show the lowest escape fractions. The range of escape fractions increases with decreasing extinction. This is evidence that the dust extinction is the most important factor affecting the escape of Lyα photons, but at low extinctions other factors, such as the H i covering fraction and gas kinematics, can be just as effective at inhibiting the escape of Lyα photons.

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“…These include narrow band imaging (e.g., Ouchi et al 2003, Gronwall et al 2007, serendipitous slit spectroscopy (e.g., Cassata et al 2011) and integral field spectroscopy (e.g., van Bruekelen et al 2005, Blanc et al 2011. These techniques have resulted in the compilation of catalogs of several hundred to a few thousand Lyα emitting galaxies from redshifts z ∼ 2.1 to the redshifts associated with the end of reionization.…”

mentioning

confidence: 99%

“…The clustering of these galaxies has been measured on scales of up to 10 Mpc by Gauita et al (2010) and Gawiser et al (2007), who find that at redshifts z = 2 − 3 they have a bias factor with respect to the underlying matter (in CDM models) of b ∼ 1.5 − 2. Integrating the luminosity functions of Lyα emitting galaxies, assuming a power-law extrapolation for the faint end slope, has revealed that the comoving volume emissivity of Lyα photons declines significantly from z ∼ 6 to z ∼ 2 (Cassata et al 2011, Gronwall et al 2007, Ouchi et al 2008). This behaviour can be compared to the opposite evolution in redshift of galaxies measured in optically thin parts of the rest-frame UV spectrum (or using the Hα line, e.g., Hayes et al 2011).…”

mentioning

confidence: 99%

Large-scale clustering of Lyman α emission intensity from SDSS/BOSS

Croft¹,

Miralda-Escudé²,

Zheng³

et al. 2016

Mon. Not. R. Astron. Soc.

105

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We detect the large-scale structure of Lyα emission in the Universe at redshifts z = 2 − 3.5 by measuring the cross-correlation of Lyα surface brightness with quasars in the Sloan Digital Sky Survey (SDSS/BOSS). We use nearly a million spectra targeting Luminous Red Galaxies (LRGs) at z < 0.8, after subtracting a best fit model galaxy spectrum from each one, as an estimate of the high-redshift Lyα surface brightness. The quasar-Lyα emission cross-correlation we detect has a shape consistent with a linear ΛCDM model with Ω m = 0.30 +0.10 −0.07 . The predicted amplitude of this crosscorrelation is proportional to the product of the mean Lyα surface brightness, µ α , the amplitude of mass density fluctuations, and the quasar and Lyα emission bias factors. Using published cosmological observations to constrain the amplitude of mass fluctuations and the quasar bias factor, we infer the value of the product µ α (b α /3) = (3.9±0.9)×10 −21 erg s −1 cm −2Å−1 arcsec −2 , where b α is the Lyα emission linear bias factor. If the dominant sources of Lyα emission we measure are star forming galaxies, we infer a total mean star formation rate density of ρ SFR = (0.28 ± 0.07)(3/b α ) yr −1 Mpc −3 at z = 2 − 3.5. For b α = 3, this value is a factor of 21 − 35 above previous estimates relying on individually detected Lyα emitters, although it is consistent with the total star-formation density derived from dust-corrected, continuum UV surveys. Our observations therefore imply that 97% of the Lyα emission in the Universe at these redshifts is undetected in previous surveys of Lyα emitters. Our detected Lyα emission is also much greater, by at least an order of magnitude, than that measured from stacking analyses of faint halos surrounding previously detected Lyα emitters, but we speculate that it arises from similar low surface brightness Lyα halos surrounding all luminous star-forming galaxies. We also detect a redshift space anisotropy of the quasar-Lyα emission cross-correlation, finding evidence at the 3.0σ level that it is radially elongated, contrary to the prediction for linear gravitational evolution, but consistent with distortions caused by radiative-transfer effects, as predicted by Zheng et al. (2011). Our measurements represent the first application of the intensity mapping technique to optical observations.

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Lyα Emission‐Line Galaxies atz= 3.1 in the Extended Chandra Deep Field–South

Cited by 362 publications

References 74 publications

Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Lyα EMISSION FROM HIGH-REDSHIFT SOURCES IN COSMOS

Large-scale clustering of Lyman α emission intensity from SDSS/BOSS

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