ERRATUM: “A Redshift [CLC][ITAL]z[/ITAL][/CLC] = 6.56 Galaxy behind the Cluster Abell 370” ([URL ADDRESS="/cgi-bin/resolve?2002ApJ...568L..75H" STATUS="OKAY"]A[CLC]p[/CLC]J, 568, L75 [2002][/URL])

Hu, E. M.; Cowie, L. L.; McMahon, R. G.; Capak, P.; Iwamuro, Fumihide; Kneib, Jean-Paul; Maihara, Toshinori; Motohara, Kentaro

doi:10.1086/343105

Cited by 36 publications

(83 citation statements)

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“…The earliest observable structure dates back to the beginning of this era at the surface of last scattering traced by the cosmic microwave background. The next most distant observable represents the populations of galaxies, gamma-ray bursts, and quasars at z ' 6.2Y7.0 (Hu et al 2002;Iye et al 2006;Totani et al 2006;Kashikawa et al 2006;Fan et al 2006;. The interval between z ' 1000 and z ' 6.5 contains many landmark events: the formation of the first stars, the assembly of first galaxies, the growth of the first supermassive black holes that power quasars, and the reionization of neutral hydrogen in the intergalactic medium.…”

Section: Introductionmentioning

confidence: 99%

“…Even with HST and 8 m class telescopes, continuum (''dropout'') and narrowband imaging Ly searches probe only the most luminous, rare sources at these redshifts; the contribution to the reionization flux from these sources may well be small. While narrowband surveys have had significant success at detecting Ly emitters at z ' 6 (Hu et al 1998(Hu et al , 2002(Hu et al , 2004Malhotra & Rhoads 2004;Hu et al 2005;Stern et al 2005; Kashikawa et al 2006;Shimasaku et al 2006), only one Ly emitter has been convincingly detected at z ' 7 . At z ' 9, narrowband surveys for relatively luminous Ly emitters (k10 42.5 ergs s À1 ) have yet to find any sources (Willis & Courbin 2005;Cuby et al 2007).…”

Section: Introductionmentioning

confidence: 99%

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A Keck Survey for Gravitationally Lensed Lyα Emitters in the Redshift Range 8.5 < z < 10.4: New Constraints on the Contribution of Low‐Luminosity Sources to Cosmic Reionization

Stark

Ellis

Richard

et al. 2007

ApJ

159

161

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We discuss new observational constraints on the abundance of faint high-redshift Ly emitters secured from a deep Keck near-infrared spectroscopic survey that utilizes the strong magnification provided by lensing galaxy clusters. In each of nine clusters, we have undertaken a systematic ''blind'' search for line emission with NIRSPEC in the J band within carefully selected regions that offer very high magnifications (k10; Y50;) for background sources with redshifts z ' 10. The high magnification enables the detection of emission at unprecedented flux limits (10 41 Y10 42 ergs s À1 ). As the comoving volumes probed are small, our survey is designed to address the important question of whether low-luminosity galaxies could provide the dominant ionizing flux at z $ 10. Our survey has yielded six promising (>5 ) candidate Ly emitters that lie between z = 8.7 and z = 10.2. We carefully discuss the validity of our detections and the likelihood that the detected line is Ly in light of earlier, apparently false, claims. Lower redshift line interpretations can be excluded, with reasonable assumptions, through the nondetection of secondary emission in further spectroscopy undertaken with LRIS and NIRSPEC. Nonetheless, as a result of our tests, we argue that at least two of our candidates are likely to be at z ' 10. Given the small survey volume, this suggests there is a large abundance of low-luminosity star-forming sources at z ' 8Y10. While the predicted reionization photon budget depends upon a large number of physical assumptions, our first glimpse at the z ' 10 universe suggests that low-luminosity starforming galaxies contribute a significant proportion of the UV photons necessary for cosmic reionization.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A Keck Survey for Gravitationally Lensed Lyα Emitters in the Redshift Range 8.5 < z < 10.4: New Constraints on the Contribution of Low‐Luminosity Sources to Cosmic Reionization

Stark

Ellis

Richard

et al. 2007

ApJ

159

161

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“…The current statistics of high-z galaxies reflects these problems. Few serendipitous objects have been identified (e.g., Spinrad et al 1998), mostly because of a large equivalent width emission line identified as Ly (e.g., Chen, Lanzetta, & Pascarelle 1999;Hu, Cowie, & McMahon 1998;Hu, McMahon, & Cowie 1999;Hu et al 2002). Some identifications have been later disputed on the basis of deep imaging shortward of the (presumed) Lyman limit (Chen et al 2000;Stern et al 2000b).…”

Section: Introductionmentioning

confidence: 99%

A European Southern Observatory Very Large Telescope Survey of Near‐Infrared (Z≤ 25) Selected Galaxies at Redshifts 4.5 <z< 6: Constraining the Cosmic Star Formation Rate near the Reionization Epoch

Fontana

Poli

Menci

et al. 2003

ApJ

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We present the results of a Very Large Telescope (VLT) and Hubble Space Telescope imaging survey aimed at the identification of 4:5 < z < 6 galaxies. In the VLT data, a set of broadband and intermediate-band filters has been used to select 13 high-z candidates in a Z AB 25 mag catalog, over an area of about 30 arcmin 2 . Discrimination against lower redshift interlopers (mainly early-type galaxies at high redshift and cool Galactic stars) has been done combining morphological and spectral classification. This sample has been combined with a deeper I AB 27:2 mag sample obtained from the Hubble Deep Field (HDF) campaigns. The VLT final sample consists of 13 high-z candidates, four of which are identified with high confidence as z > 4:5 galaxies. The resulting integral surface density of the Z AB < 25 candidates at z > 4:5 is in the range 0.13-0.44 arcmin À2 , and that in the highest redshift bin 5 < z 6 is between 0.07 and 0.13 arcmin À2 . In the two HDFs, we identify 25 galaxies at I AB 27:2 in the range 4:5 z < 5 and 16 at 5 z 6, corresponding to surface densities of 3.1 and 2 arcmin À2 , respectively. We show that the observed Z AB < 25 UV luminosity density (LD) appears to drop by about 1 order of magnitude from z ' 3 to 6. However, if we apply a threshold to obtain an absolute magnitude-limited sample, the UV LD is roughly constant up to z ' 6. We finally show that recent semianalytic hierarchical models for galaxy formation, while predicting a nearly constant total UV LD up to z ' 6, underpredict the observed UV LD at Z AB 25 and overpredict the I AB 27:2 one. This behavior can be understood in terms of a poor match to the slope of the UV luminosity function.

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“…To make the above discussion more general, He ii emission should be investigated in many more galaxies at , 6 Շ z Շ 7 and, indeed, the most recent observational facilities have allowed us to find some galaxies in this redshift range with spectroscopically confirmed redshifts (e.g., Hu et al 2002;Kodaira et al 2003;Kurk et al 2004;Rhoads et al 2004;Nagao et al 2004Nagao et al , 2005Stern et al 2005;Taniguchi et al 2005 ]. However, it may be more promising to search for Population III stars at much higher redshifts because the probability that galaxies are dominated by Population III stars increases dramatically as a function of z, as demonstrated by Scannapieco et al (2003).…”

mentioning

confidence: 99%

An Observational Pursuit for Population III Stars in a Lyα Emitter at z = 6.33 through He ii Emission

Nagao

Motohara

Maiolino

et al. 2005

ApJ

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We present a very deep near-infrared spectroscopic observation of a strong Lya emitter at , SDF z p 6.33 J132440.6ϩ273607, which we used to search for He ii l1640. This emission line is expected if the target hosts a significant number of Population III stars. Even after 42 ks of integration with the Subaru/OHS spectrograph, no emission-line features are detected in the J and H bands, which confirms that SDF J132440.6ϩ273607 is neither an active galactic nucleus nor a low-z emission-line object. We obtained a 2 j upper limit of 9.06 # ergs s Ϫ1 cm Ϫ2 on the He ii l1640 emission-line flux, which corresponds to a luminosity of Ϫ18 42 10 4.11 # 10 ergs s Ϫ1 . This upper limit on the He ii l1640 luminosity implies that the upper limit on the Population III star formation rate is in the range 4.9-41.2 M , yr Ϫ1 if Population III stars suffer no mass loss and in the range 1.8-13.2 M , yr Ϫ1 if strong mass loss is present. The nondetection of He ii in SDF J132440.6ϩ273607 at z p may thus disfavor weak feedback models for Population III stars. 6.33

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ERRATUM: “A Redshift [CLC][ITAL]z[/ITAL][/CLC] = 6.56 Galaxy behind the Cluster Abell 370” ([URL ADDRESS="/cgi-bin/resolve?2002ApJ...568L..75H" STATUS="OKAY"]A[CLC]p[/CLC]J, 568, L75 [2002][/URL])

Cited by 36 publications

References 0 publications

A Keck Survey for Gravitationally Lensed Lyα Emitters in the Redshift Range 8.5 < z < 10.4: New Constraints on the Contribution of Low‐Luminosity Sources to Cosmic Reionization

A Keck Survey for Gravitationally Lensed Lyα Emitters in the Redshift Range 8.5 < z < 10.4: New Constraints on the Contribution of Low‐Luminosity Sources to Cosmic Reionization

A European Southern Observatory Very Large Telescope Survey of Near‐Infrared (Z≤ 25) Selected Galaxies at Redshifts 4.5 <z< 6: Constraining the Cosmic Star Formation Rate near the Reionization Epoch

An Observational Pursuit for Population III Stars in a Lyα Emitter at z = 6.33 through He ii Emission

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