Subaru Deep Survey. II. Luminosity Functions and Clustering Properties of Lyα Emitters at<i>z</i> = 4.86 in the Subaru Deep Field

Ouchi, Masami; Shimasaku, Kazuhiro; Furusawa, Hisanori; Miyazaki, Masayuki; Doi, Mamoru; Hamabe, M.; Hayashino, T.; Kimura, Masahiko; Kodaira, Keiichi; Komiyama, Yutaka; Matsuda, Yoshihisa; Miyazaki, Satoshi; Nakata, Fumiaki; Okamura, S.; Sekiguchi, M.; Shioya, Yasuhiro; Tamura, H.; Taniguchi, Yoshiaki; Yagi, Masafumi; Yasuda, Naoki

doi:10.1086/344476

Cited by 246 publications

(260 citation statements)

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“…Wide-field narrowband surveys for line-emitting galaxies (e.g., Rhoads & Malhotra 2001;Ouchi et al 2003) are efficient at detecting the most extreme line emitters at high redshift. None of the galaxies in Rhoads et al (2003) have sufficient line flux alone to be detected by us in the broadband filters given our flux limit.…”

Section: Surface Densities Of High-redshift Lbgsmentioning

confidence: 99%

Luminous Lyman Break Galaxies atz > 5 and the Source of Reionization

Lehnert

Bremer²

2003

ApJ

124

183

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We have discovered six galaxies with spectroscopically confirmed redshifts of 4:8 < z < 5:8 in a single 44 arcmin 2 field deeply imaged in R, I, and z bands. All the spectra show an emission line in the region around 7000-8400 Å with a spectroscopically detected faint continuum break across the line. These six were drawn from 13 sources with I AB < 26:2 and R AB À I AB > 1:5 in the field; this photometric cut is designed to select galaxies at z > 4:8. The line fluxes range between 0.2 and 2:5 Â 10 À17 ergs cm À2 s À1 , indicating luminosities of around 10 42 -10 43 ergs s À1 for Ly , and their high emission line equivalent widths suggest very young ages (d10 8 yr). A further line-emitting object with no detectable continuum was serendipitously detected by spectroscopy. If this line is Ly , then it is from a source at z ¼ 6:6, making this the most distant galaxy known. However, the redshift cannot be considered secure as it is based on a single line. No broad emission line objects (quasars) were detected. The 13 sources at I AB < 26:2 are less than that expected if the luminosity function of dropout galaxies remained unchanged between z ¼ 3 and 6, although the deficit is not highly significant given possible cosmic variance. The UV luminosity density from galaxies brighter than our flux limit is considerably less than that necessary to keep the volume probed by our field at z h i $ 5:3 ionized. These galaxies are observed within several hundred megayears of the end of the epoch of reionization (z ¼ 6 7), with little time for the luminosity function to evolve. This and the lack of detected quasars imply that the bulk of the UV flux that reionized the universe came from faint galaxies with M AB ð1700 GÞ > À21.

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Section: Surface Densities Of High-redshift Lbgsmentioning

confidence: 99%

Luminous Lyman Break Galaxies atz > 5 and the Source of Reionization

Lehnert

Bremer²

2003

ApJ

124

183

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“…Steidel et al 1996Steidel et al , 2003Cooke et al 2006;Bielby et al 2011) and Lyα emission (e.g. Cowie & Hu 1998;Ouchi et al 2003;Gawiser et al 2006). However, to follow the galaxy population into the redshift range 1 z 2.5, near-infrared observations are essential as all spectral features move out of visible bands.…”

Section: Introductionmentioning

confidence: 99%

The WIRCam Deep Survey

Bielby

Hudelot

McCracken

et al. 2012

A&A

171

208

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We present a new near-infrared imaging survey in the four CFHTLS deep fields: the WIRCam Deep Survey or "WIRDS". WIRDS comprises extremely deep, high quality (FWHM ∼ 0.6 ) J, H, and K s imaging covering a total effective area of 2.1 deg 2 and reaching AB 50% completeness limits of ≈24.5. We combine our images with the CFHTLS to create a unique eight-band ugrizJHK S photometric catalogues in the four CFHTLS deep fields; these four separate fields allow us to make a robust estimate of the effect of cosmic variance for all our measurements. We use these catalogues in combination with ≈9800 spectroscopic redshifts to estimate precise photometric redshifts (σ Δz/(1+z) 0.03 at i < 25), galaxy types, star-formation rates and stellar masses for a unique sample of ≈1.8 million galaxies. Our JHK s number counts are consistent with previous studies. We apply the "BzK" selection to our gzK filter set and find that the star forming BzK selection successfully selects 76% of star-forming galaxies in the redshift range 1.4 < z < 2.5 in our photometric catalogue, based on our photometric redshift measurement. Similarly the passive BzK selection returns 52% of the passive 1.4 < z < 2.5 population identified in the photometric catalogue. We present the mass functions of the total galaxy population as a function of redshift up to z = 2 and present fits using double Schechter functions. A mass-dependent evolution of the mass function is seen with the numbers of galaxies with masses of M 10 10.75 still evolving at z 1, but galaxies of higher mass reaching their present day numbers by z ∼ 0.8−1. This is consistent with the present picture of downsizing in galaxy evolution. We compare our results with the predictions of the GALFORM semi-analytical galaxy formation model and find that the simulations provide a relatively successful fit to the observed mass functions at intermediate masses (i.e. 10 log (M/M ) 11). However, as is common with semi-analytical predictions of the mass function, the GALFORM results under-predict the mass function at low masses (i.e. log (M/M ) 10), whilst the fit as a whole degrades beyond redshifts of z ∼ 1.2. All photometric catalogues and images are made publicly available from TERAPIX and CADC.

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“…While our analysis is specifically prompted by the SDSS quasars, it should be applicable to other objects for which significant lensing amplification would be important, such as highredshift galaxies discovered in ''blank'' fields 4 (i.e., fields not specifically chosen for the presence of a massive cluster lens; e.g., Rhoads et al 2000;Rhoads & Malhotra 2001;Steidel et al 2003;Bouwens et al 2003;Ouchi et al 2003;Stanway et al 2004;Pirzkal et al 2004). …”

Section: Introductionmentioning

confidence: 99%

Gravitational Lensing Magnification without Multiple Imaging

Keeton

Kuhlen

Haiman

2005

ApJ

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Gravitational lensing can amplify the apparent brightness of distant sources. Images that are highly magnified are often part of multiply imaged systems, but we consider the possibility of having large magnifications without additional detectable images. In rare but nonnegligible situations, lensing can produce a single highly magnified image; this phenomenon is mainly associated with massive cluster-scale halos (k10 13.5 M ). Alternatively, lensing can produce multiply imaged systems in which the extra images are either unresolved or too faint to be detectable. This phenomenon is dominated by galaxies and lower mass halos (P10 12 M ) and is very sensitive to the inner density profile of the halos. Although we study the general problem, we customize our calculations to four quasars at redshift z % 6 in the Sloan Digital Sky Survey (SDSS), for which Richards et al. (2004) have ruled out the presence of extra images down to an image splitting of Á ¼ 0B3 and a flux ratio of f ¼ 0:01. We predict that 9%-29% of all z % 6 quasars that are magnified by a factor of > 10 would lack detectable extra images, with 5%-10% being true singly imaged systems. The maximum of 29% is reached only in the unlikely event that all low-mass (P10 10 M ) halos have highly concentrated (isothermal) profiles. In more realistic models in which dwarf halos have flatter (Navarro-Frenk-White) inner profiles, the maximum probability is $10%. We conclude that the probability that all four SDSS quasars are magnified by a factor of 10 is P10 À4 . The only escape from this conclusion is if there are many (>10) multiply imaged z % 6 quasars in the SDSS database that have not yet been identified, which seems unlikely. In other words, lensing cannot explain the brightnesses of the z % 6 quasars, and models that invoke lensing to avoid having billion-solar-mass black holes in the young universe are not viable.

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Subaru Deep Survey. II. Luminosity Functions and Clustering Properties of Lyα Emitters atz = 4.86 in the Subaru Deep Field

Cited by 246 publications

References 40 publications

Luminous Lyman Break Galaxies atz > 5 and the Source of Reionization

Luminous Lyman Break Galaxies atz > 5 and the Source of Reionization

The WIRCam Deep Survey

Gravitational Lensing Magnification without Multiple Imaging

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