The Discovery of Two Lyman α Emitters beyond Redshift 6 in the Subaru Deep Field

By K. Kodaira, Yoshiaki Taniguchi, N. Kashikawa, N. Kaifu, H. Ando, H. Karoji, M. Ajiki, M. Akiyama, K. Aoki, M. Doi and 35 more. 2003

155 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

Observational Constraints on Cosmic Reionization (2006, methodology): “…S. 1998, Physical Re- view Letters, 81, 2004 Knox & Song(2002)Knox, L., & Song, Y.-S. 2002, Physical Review Letters, 89, 011303 Knox(2003)Knox, L. 2003, New Astronomy Review, 47, 883 Kodaira et al. 2003Kodaira, K., et al. 2003, PASJ, 55: L17-L21 Kogut et al.(2003)Kogut, A., et al. 2003, Ap.”
Probing reionization with Lyman α emission lines (2003, methodology): “7+273058 (hereafter ‘K’; Kodaira et al. 2003) (in our cosmology).”
Reionization and Galaxy Evolution Probed by z = 7 Lyα Emitters (2007, background): “Out of these lower redshift galaxies, z = 6.5–6.6 LAEs can be removed by requiring no detection in the narrowband filter NB921 image whose bandpass corresponds to the Lyα emissions at this redshift range (Kodaira et al. 2003; Taniguchi et al. 2005; Kashikawa et al. 2006b).”
Luminosity Functions of Lyα Emitters at Redshifts z = 6.5 and z = 5.7: Evidence against Reionization at z ≤ 6.5 (2004, background): “The last, by T04, has , , and (including two galaxiesN p 58 N p 20 N p 9can spec conf confirmed earlier by Kodaira et al. 2003).”
Protoclusters associated with z > 2 radio galaxies - I. Characteristics of high redshift protoclusters (2006, methodology): “This test, which makes use of the characteristic blue wing absorption profile of the Lyα emission line, has been successfully applied to confirmz > 4.5 Lyα emitters (e.g., Kodaira et al., 2003; Rhoads et al., 2003; Dawson et al., 2004; Hu et al., 2004).”
SPECTROSCOPIC CONFIRMATION OF TWO LYMAN BREAK GALAXIES AT REDSHIFT BEYOND 7 (2010, background): “Indeed most LAEs and LBGs at high redshift are too faint to detect the break in the continuum caused by IGM attenuation, with the exception of few very bright objects (Kodaira et al. 2003).”
Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly (2009, unknown): “…Shimasaku et al. (2006) 5.700 0.050 >0.0007 Lyα Murayama et al. (2007) 5.735 0.062 >0.0005 Lyα Rhoads et al. (2003) 6.500 0.050 >0.0036 Lyα Malhotra & Rhoads (2004) 6.550 0.050 >0.0006 Lyα Taniguchi et al. (2005) 6.578 0.002 >0.0005 Lyα Kodaira et al. (2003) 3.000 1.000 >0.0818 submm Hughes et…”
Probing the Ionization State of the Universe at z > 6 (2003, background): “Recently several groups have discovered Ly α-emitting galaxies at z ∼ 6.5 (Hu et al. 2002, Kodaira et al. 2003).”
Lyα Emission-Line Galaxies at z = 3.1 in the Extended Chandra Deep Field-South (2007, unknown): “…(Ciardullo et al. 2002; Hayashino et al. 2004; Venemans et al. 2005; Gawiser et al. 2006a), z 3:7 (Fujita et al. 2003), z 4:5 (Rhoads et al. 2000), z 4:9 (Ouchi et al. 2003), z 5:7 (Rhoads et al. 2003; Ajiki et al. 2003; Tapken et al. 2006), and z 6:5 (Kodaira et al. 2003; Taniguchi et al. 2005).”
Galaxies at z ~ 6: The UV Luminosity Function and Luminosity Density from 506 HUDF, HUDF Parallel ACS Field, and GOODS i-Dropouts (2005, background): “Moreover, a significant contribution from Lyα to the J110 flux seems unlikely given constraints from emission line searches at z ∼ 6 (Ajiki et al. 2003; Kodaira et al. 2003; Hu et al. 2004; BSEM04; Stanway et al. 2004a; Nagao et al. 2004; Dow-Hygelund et al. 2006).”
COMPLETING THE CENSUS OF Lyα EMITTERS AT THE REIONIZATION EPOCH (2011, background): “In our previous papers (Kashikawa et al. 2006: K06, Shimasaku et al. 2006: S06), we have presented spectroscopic confirmations of 17 and 34 LAEs at z = 6.5 and 5.7, respectively, in the Subaru Deep Field (SDF); see also Kodaira et al. (2003) and Taniguchi et al. (2005) for LAEs at z = 6.5.”
The End of the Reionization Epoch Probed by Lyα Emitters at z = 6.5 in the Subaru Deep Field (2006, background): “Although some bright LAEs show the continuum breaks (Kodaira et al. 2003) caused by IGM attenuation, most are too faint to detect the break at the highest z epoch.”
Unusually Large Fluctuations in the Statistics of Galaxy Formation at High Redshift (2003, background): “For example, there are a large number of programs searching for galaxies at the highest accessible redshifts (6.5 and beyond) using their strong Lyα emission (Hu et al. 2002; Rhoads et al. 2003; Maier et al. 2003; Kodaira et al. 2003).”
The Subaru/XMM-Newton Deep Survey (SXDS). IV. Evolution of Lyα Emitters from z = 3.1 to 5.7 in the 1 deg2 Field: Luminosity Functions and AGN (2007, background): “LAEs are usually identified by a redshifted Ly emission line that falls in a passband of narrowband filter (e.g., Hu et al. 2002; Kodaira et al. 2003), tuned at z 3 up to z 9 (e.g., Iye et al. 2006; Willis et al. 2006).”
The Luminosity Function and Star Formation Rate between Redshifts of 0.07 and 1.47 for Narrowband Emitters in the Subaru Deep Field (2006, background): “For example, Hu et al. (2002), Ajiki et al. (2003), Kodaira et al. (2003), Taniguchi et al. (2003), Hu et al. (2004), Kashikawa et al. (2006), and Shimasaku et al. (2006) have confirmed candidate Lyα emitters (LAEs) at z = 5.7 and 6.6 with follow-up spectroscopy.”
Early and Rapid Merging as a Formation Mechanism of Massive Galaxies: Empirical Constraints (2005, background): “This has been accomplished to a degree with the discovery and systematic study of sub-mm sources (Blain et al. 2002), Lyman-α emitters (Kodaira et al. 2003), extremely red objects (Moustakas et al. 2004) and Lyman-Break galaxies (LBGs; Giavalisco 2002).”
Constraints on the Equation of State of Dark Energy and the Hubble Constant from Stellar Ages and the Cosmic Microwave Background (2003, background): “Numerous starforming galaxies have now been observed up to redshift z ¼ 6:6 (e.g., Kodaira et al. 2003).”
The First Cosmic Structures and Their Effects (2004, methodology): “Lyα Line Profiles Lyα emission has been crucial in determining the redshift of distant galaxies (e.g. Hu et al. 2002; Kodaira et al. 2003; Rhoads et al. 2003; Hu et al. 2004; Pelló et al. 2004) and it represents an invaluable tool to probe the high redshift universe and, possibly, the sources…”
CO(J = 1→0) IN z > 2 QUASAR HOST GALAXIES: NO EVIDENCE FOR EXTENDED MOLECULAR GAS RESERVOIRS (2006, background): “…(QSOs), and emission-line galaxies are observed up to redshifts of z ¼ 6:6 (e.g., Fan et al. 2001; Rhoads & Malhotra 2001; Hu et al. 2002; Kodaira et al. 2003; Taniguchi et al. 2005), less than 1 Gyr after recombination, implies that galactic-scale ( 10 kpc), gravitationally bound…”