COMPLETING THE CENSUS OF Lyα EMITTERS AT THE REIONIZATION EPOCH

By N. Kashikawa, K. Shimasaku, Y. Matsuda, E. Egami, Linhua Jiang, Tohru Nagao, M. Ouchi, M. Malkan, T. Hattori, K. Ota and 9 more. 2011

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We carried out extended spectroscopic confirmations of Lyα emitters (LAEs) at z = 6.5 and 5.7 in the Subaru Deep Field. Now, the total number of spectroscopically confirmed LAEs is 45 and 54 at z = 6.5 and 5.7, respectively, and at least 81% (70%) of our photometric candidates at z = 6.5 (5.7) have been spectroscopically identified as real LAEs. We made careful measurements of the Lyα luminosity, both photometrically and spectroscopically, to accurately determine the Lyα and rest-UV luminosity functions (LFs). The substantially improved evaluation of the Lyα LF at z = 6.5 shows an apparent deficit from z = 5.7 at least at the bright end, and a possible decline even at the faint end, though small uncertainties remain. The rest-UV LFs at z = 6.5 and 5.7 are in good agreement, at least at the bright end, in clear contrast to the differences seen in the Lyα LF. These results imply an increase in the neutral fraction of the intergalactic medium from z = 5.7 to 6.5. The rest-frame equivalent width (EW0) distribution at z = 6.5 seems to be systematically smaller than z = 5.7, and it shows an extended tail toward larger EW0. The bright end of the rest-UV LF can be reproduced from the observed Lyα LF and a reasonable EW0–UV luminosity relation. Integrating this rest-UV LF provides the first measurement of the contribution of LAEs to the photon budget required for reionization. The derived UV LF suggests that the fractional contribution of LAEs to the photon budget among Lyman break galaxies significantly increases toward faint magnitudes. Low-luminosity LAEs could dominate the ionizing photon budget, though this inference depends strongly on the uncertain faint-end slope of the Lyα LF.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Full-data Results of Hubble Frontier Fields: UV Luminosity Functions at z ∼ 6–10 and a Consistent Picture of Cosmic Reionization (2017, background): “Observational studies show that the reionization occurred at z & 6 (Fan et al. 2006; Pentericci et al. 2011, 2014; Ono et al. 2012; Totani et al. 2006, 2014; Kashikawa et al. 2011; Ouchi et al. 2010; Konno et al. 2014; Treu et al. 2013).”
CRITICAL STAR FORMATION RATES FOR REIONIZATION: FULL REIONIZATION OCCURS AT REDSHIFT z ≈ 7 (2012, background): “Recent surveys of high-redshift galaxies and Lyα emitters (Bouwens et al. 2011a; Ouchi et al. 2010; Kashikawa et al. 2011; Ono et al. 2012; Schenker et al. 2012) infer an increasing IGM neutral fraction from the declining populations in the range z = 6–8.”
VERY STRONG EMISSION-LINE GALAXIES IN THE WFC3 INFRARED SPECTROSCOPIC PARALLEL SURVEY AND IMPLICATIONS FOR HIGH-REDSHIFT GALAXIES, (2011, background): “Using similar con- straints, Kashikawa et al. (2011) report 81% (70”
NEW OBSERVATIONS OF z ∼ 7 GALAXIES: EVIDENCE FOR A PATCHY REIONIZATION (2014, background): “…galaxies and their clustering have the potential to reveal the signature of patchy reionization, although early results have been inconclusive (Kashikawa et al. 2011, Ouchi et al. 2010) In this paper we present new observations of z∼ 7 candidates, significantly increasing the statistics of…”
HUBBLE FRONTIER FIELDS FIRST COMPLETE CLUSTER DATA: FAINT GALAXIES AT z ∼ 5–10 FOR UV LUMINOSITY FUNCTIONS AND COSMIC REIONIZATION (2014, background): “…moderately large neutral hydrogen fraction at z & 6 is implied by the Lyα damping wing absorption features in the spectra of gammaray bursts (GRBs) at z ∼ 6 (Totani et al. 2006, 2013) and Lyα emitters at z ∼ 6 − 7 (Kashikawa et al. 2006; Ouchi et al. 2010; Kashikawa et al. 2011; Konno et al. 2014).”
SPECTROSCOPIC CONFIRMATION OF THREE z-DROPOUT GALAXIES AT z = 6.844–7.213: DEMOGRAPHICS OF Lyα EMISSION IN z ∼ 7 GALAXIES (2011, result): “This result has been further supported by Kashikawa et al. (2011), who studied the evolution of the LAE luminosity function in the Subaru Deep Field (SDF; Kashikawa et al. 2004) and found an increase in the neutral fraction of the IGM from z = 5.7 to 6.5.”
Systematic Identification of LAEs for Visible Exploration and Reionization Research Using Subaru HSC (SILVERRUSH). I. Program strategy and clustering properties of ∼2000 Lyα emitters at z = 6–7 over the 0.3–0.5 Gpc2 survey area (2017, background): “…et al. 2006, 2014, 2016; see also Greiner et al. 2009), and galaxies including LAEs (Malhotra & Rhoads 2004; Ouchi et al. 2010; Ota et al. 2010; Kashikawa et al. 2011; Pentericci et al. 2011; Ono et al. 2012; Treu et al. 2013; Caruana et al. 2014; Konno et al. 2014, 2018; Schenker et al.…”
Lyα EMISSION FROM GREEN PEAS: THE ROLE OF CIRCUMGALACTIC GAS DENSITY, COVERING, AND KINEMATICS (2015, background): “…are identifying the building blocks of present-day galaxies and the sources that are most important for metal enrichment and reionization of the IGM (Martin et al. 2008; Ouchi et al. 2010; Hu et al. 2010; Dressler et al. 2011, 2015; Kashikawa et al. 2011; Henry et al. 2012; Rhoads et al. 2012).”
Identification of the brightest Lyα emitters at z = 6.6 : Implications for the evolution of the luminosity function in the reionization era (2015, background): “As noted by Kashikawa et al. (2011), the difference between the results from Hu et al. (2010) and the others is due to incompleteness of the sample of Hu et al. (2010), since they rely on spectroscopic follow-up with too short integration times.”
SILVERRUSH. IV. Lyα luminosity functions at z = 5.7 and 6.6 studied with ∼1300 Lyα emitters on the 14–21 deg2 sky (2017, background): “These survey areas are 70− 87 times larger than those of the Subaru Deep Field studies (Shimasaku et al. 2006; Kashikawa et al. 2011), 14− 21 times larger than those of the Subaru/XMM-Newton Deep Survey (Ouchi et al. 2008; Ouchi et al. 2010), and 2− 5 times larger than those of other subsequent…”
KECK SPECTROSCOPY OF FAINT 3 < z < 8 LYMAN BREAK GALAXIES: EVIDENCE FOR A DECLINING FRACTION OF EMISSION LINE SOURCES IN THE REDSHIFT RANGE 6 < z < 8 (2011, methodology): “Our derived values of XHI are slightly higher than that of Kashikawa et al. (2011), perhaps consistent with our survey probing to higher redshifts than their z = 6.5 LAEs.”
Lyα Emitting Galaxies as a Probe of Reionisation (2014, background): “In contrast, the Lyα luminosity of LAEs does evolve at z > 6 (e.g. Kashikawa et al. 2006; Ouchi et al. 2010; Ota et al. 2010; Kashikawa et al. 2011), as is shown in the right panel of Figure 16.”