Lyα Emitters at z = 5.7 in the Subaru Deep Field

By K. Shimasaku, N. Kashikawa, M. Doi, C. Ly, M. Malkan, Y. Matsuda, M. Ouchi, T. Hayashino, M. Iye, K. Motohara and 7 more. 2006

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PASJ: Publ. Astron. Soc. Japan , 1–??, c 2008. Astronomical Society of Japan. Lyα Emitters at z = 5.7 in the Subaru Deep Field Kazuhiro Shimasaku, 1,2 Nobunari Kashikawa, 3,4 Mamoru Doi, 5,2 Chun Ly, 6 Matthew A.Malkan, 6 Yuichi Matsuda, 7 Masami Ouchi, 8,‡ Tomoki Hayashino, 9 Masanori Iye, 3,4 Kentaro Motohara, 5 Takashi Murayama, Tohru Nagao, 3,11 Kouji Ohta, 12 Sadanori Okamura, 1,2 Toshiyuki Sasaki, 13 Yasuhiro Shioya, 10 Yoshiaki Taniguchi 10 arXiv:astro-ph/0602614v1 28 Feb 2006 Department of Astronomy, School of Science, The University of Tokyo, Tokyo 113-0033 Email (KS): shimasaku@astron.s.u-tokyo.ac.jp Research Center for the Early Universe, School of Science, The University of Tokyo, Tokyo 113-0033 Optical and Infrared Astronomy Division, National Astronomical Observatory, Mitaka, Tokyo 181-8588 Department of Astronomy, School of Science, Graduate University for Advanced Studies, Mitaka, Tokyo 181-8588 Institute of Astronomy, School of Science, The University of Tokyo, Mitaka 181-0015 Department of Astronomy, University of California at Los Angeles, Los Angeles, CA 90095-1547, USA Department of Astronomy, Graduate School of Science, Kyoto University, Kyoto 606-8502 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Research Center for Neutrino Science, Graduate School of Science, Tohoku University, Aramaki, Aoba, Sendai 980-8578 Astronomical Institute, Graduate School of Science, Tohoku University, Aramaki, Aoba, Sendai 980-8578, Japan INAF / Osservatorio Astrofisico di Arcetri Largo E. Fermi 5, 50125 Firenze, Italy Kouji Ohta Department of Astronomy, Kyoto University, Kyoto 606-8502 Subaru Telescope, National Astronomical Observatory of Japan, 650 N. A’ohoku Place, Hilo, HI 96720, USA (Received 2005 October 26; accepted 2006 February 27) Abstract We present the properties of Lyα emitters (LAEs) at z = 5.7 in the Subaru Deep Field. A photometric sample of 89 LAE candidates is constructed from narrow-band (NB816) data down to N B816 = 26.0 (AB) in a continuous 725 arcmin 2 area. Spectra of 39 objects satisfying the photometric selection criteria for LAEs were obtained with Subaru and Keck II Telescopes, among which 28 were confirmed LAEs, one was a nearby galaxy, and eight were unclassified. We also obtained spectra of another 24 NB816-excess objects in the field, identifying six additional LAEs. We find that the Lyα luminosity function derived from the photometric sample is reproduced well by a Schechter function with L ⋆ = 7.9 +3.0 erg s −1 and φ ⋆ = 6.3 −2.0 × 10 −4 Mpc −3 for α = −1.5 (fixed) over the whole luminosity range of L ≃ 3 × 10 42 – 3 × 10 43 erg s −1 . We then measure rest-frame Lyα equivalent widths (EWs) for the confirmed LAEs, to find that the median among the 28 objects satisfying the photometric selection criteria is W i0 = 233 ˚ A. We infer that 30% – 40% of LAEs at z = 5.7 exceed W i0 = 240 ˚ A. These large-EW objects probably cannot be accounted for by ordinary star-forming populations with a Salpeter IMF. We also find that LAEs with fainter far-UV luminosities have larger EWs. Finally, we derive the far-UV luminosity function of LAEs down to M UV ≃ −19.6 using the photometric sample, and compare it with that of Lyman-break galaxies (LBGs). We find that as high as about 80% of LBGs at z ∼ 6 have W i0 ≥ 100 ˚ A, in sharp contrast to lower-z counterparts. Key words: galaxies: evolution — galaxies: high-redshift — galaxies: luminosity function, mass function — galaxies: photometry

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Citations in the corpus

• UV Luminosity Functions at z~4, 5, and 6 from the Hubble Ultra Deep Field and Other Deep Hubble Space Telescope ACS Fields: Evolution and Star Formation History (2007, background): “…a narrowband selection, claim that & 80% of star-forming galaxies at the high-redshift end of our range (z ∼ 5.7) have Lyα equivalent widths of & 100Å (Shimasaku et al. 2006), while spectroscopic follow-up of pure dropout selections indicate that the fraction is closer to ∼ 32%, with typical Lyα…”
• Lyα Emission-Line Galaxies at z = 3.1 in the Extended Chandra Deep Field-South (2007, background): “However, if the z ¼ 5:7 LAE luminosity function of Shimasaku et al. (2006) is correct, then evolution is occurring in the opposite direction, i.e., the star formation rate density is declining with time.”
• LARGE AREA SURVEY FOR z = 7 GALAXIES IN SDF AND GOODS-N: IMPLICATIONS FOR GALAXY FORMATION AND COSMIC REIONIZATION (2009, methodology): “We check the spectroscopic catalogs of SDF and GOODS-N, which are obtained by Kashikawa et al. (2003), Shimasaku et al. (2003), Ouchi et al. (2004a), Shimasaku et al. (2006), Kashikawa et al. (2006), Yoshida et al. (2006), Iye et al. (2006), Nagao et al. (2007), Hayashi et al. (2009), and Ly et al.…”
• SPECTROSCOPIC CONFIRMATION OF TWO LYMAN BREAK GALAXIES AT REDSHIFT BEYOND 7 (2010, methodology): “We also calculated the weighted skewness Sw introduced by Shimasaku et al. (2006), to quantify the asymmetry of the two lines.”
• STATISTICS OF 207 Lyα EMITTERS AT A REDSHIFT NEAR 7: CONSTRAINTS ON REIONIZATION AND GALAXY FORMATION MODELS (2010, methodology): “6 LAEs whose Lyα lines do not enter the z′ band (e.g. Hu et al. 2004; Shimasaku et al. 2006; Ouchi et al. 2008), and near-infrared photometry is required to derive reliable UV LF of LAEs at z = 6.6.”
• 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, methodology): “Thus, the Ly LFs in Figure 19 (solid lines) should be called ‘‘apparent’’ Ly LFs.”
• SILVERRUSH. IV. Lyα luminosity functions at z = 5.7 and 6.6 studied with ∼1300 Lyα emitters on the 14–21 deg2 sky (2017, methodology): “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…”
• Reionization and Galaxy Evolution Probed by z = 7 Lyα Emitters (2007, methodology): “…densities at z = 7 obtained by this study were compared to those at z = 5.7 and 6.6 derived from the latest samples obtained by the SDF surveys (Shimasaku et al. 2006; Kashikawa et al. 2006b) down to our detection limit, and clear evolution of density deficits with increasing redshifts was…”
• Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly (2009, unknown): “…4.860 0.030 >0.0063 Lyα Ouchi et al. (2003); van Breukelen et al. (2005) 5.690 0.090 >0.0032 Lyα Ouchi et al. (2008) 5.700 0.100 >0.0012 Lyα Ajiki et al. (2003) 5.700 0.050 >0.0018 Lyα Malhotra & Rhoads (2004) 5.700 0.050 >0.0023 Lyα Shimasaku et al. (2006) 5.700 0.050 >0.0007 Lyα Murayama et al.…”
• Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV Luminosity Functions at $z \sim 4-7$ Derived with the Half-Million Dropouts on the 100 deg$^2$ Sky (2017, background): “…the shorter wavelength of the peak and a slowly decaying red tail, which are characteristic features of Lyα at high redshift (Kashikawa et al. 2006; Shimasaku et al. 2006).3 Their redshifts are 3 We confirm that no other emission lines are detected in their spectra, which determined based on the…”
• Keck spectroscopy of faint 3 < z < 7 Lyman break galaxies – I. New constraints on cosmic reionization from the luminosity and redshift-dependent fraction of Lyman α emission (2010, result): “Finally, we compare our results to those determined from studies of narrowband-selected LAEs in the same redshift range (e.g. Shimasaku et al. 2006; Kashikawa et al. 2006; Ouchi et al. C© 2010 The Authors.”
• The End of the Reionization Epoch Probed by Lyα Emitters at z = 6.5 in the Subaru Deep Field (2006, methodology): “Although our primary targets for this observation were z = 5.7 LAEs (Shimasaku et al. 2006) in the SDF, three slits were allocated for the z6p5LAE sample.”
• SPECTROSCOPIC CONFIRMATION OF THREE z-DROPOUT GALAXIES AT z = 6.844–7.213: DEMOGRAPHICS OF Lyα EMISSION IN z ∼ 7 GALAXIES (2011, background): “…+0.6 −0.7Å for SDF-46975, and Sw = 4.1 ± 0.7Å for GN-108036, which means that all the three lines have an asymmetric profile with a sharp decline on the blue side and a long tail on the red side, as is commonly seen in Lyα at high redshifts (e.g., Shimasaku et al. 2006; Kashikawa et al. 2006).”
• AN ATLAS OF z = 5.7 AND z = 6.5 Lyα EMITTERS, (2010, background): “…& Rhoads (2004) LF based on their spectroscopic sample (purple dashed curve), but it is about a factor of slightly more than two lower than either the Ouchi et al. (2008) (black dash-dotted curve) or the Shimasaku et al. (2006) (black dotted curve) LFs, which are based on their photometric samples.”
• The luminosity function, halo masses and stellar masses of luminous Lyman-break galaxies at redshifts 5 < z < 6 (2008, background): “By exploiting the wide-field imaging capabilities of Suprime-Cam on Subaru, several recent studies have investigated the number densities, luminosity functions and clusteringproperties of LAEs atz = 5.7 andz = 6.6 (e.g. Ouchi et al. 2008; Shimasaku et al. 2006; Taniguchi et al. 2005).”
• Evolution in the properties of Lyman-α emitters from redshifts z ~ 3 to z ~ 2 (2008, background): “At higher redshift (z & 4), emitters with EWs larger than240 Å have been predicted (Schaerer 2003; Tumlison et al. 2003) and observed (Malhotra & Rhoads 2002; Shimasaku et al. 2006; Stanway et al. 2007).”
• Hyper-Eddington accretion flows on to massive black holes (2015, background): “Among highz galaxies, Lyα emitters (LAE) have prominent Lyα emission, typically LLyα ∼ 1042−44 erg s−1 (Ouchi et al. 2003; Hu et al. 2004; Malhotra & Rhoads 2004; Kashikawa et al. 2006; Shimasaku et al. 2006; Ouchi et al. 2008, 2010; Ono et al. 2010, 2012).”
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