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

By M. Ouchi, K. Shimasaku, M. Akiyama, C. Simpson, Tomoki Saito, Y. Ueda, H. Furusawa, K. Sekiguchi, Toru Yamada, T. Kodama and 6 more. 2007

498 citations recorded by the source corpus.

We present luminosity functions (LFs) and various properties of Lyα emitters (LAEs) at z = 3.1, 3.7, and 5.7, in a 1 deg2 sky of the Subaru/XMM–Newton Deep Survey (SXDS) Field. We obtain a photometric sample of 858 LAE candidates based on deep Subaru Suprime-Cam imaging data and a spectroscopic sample of 84 confirmed LAEs from Subaru FOCAS and VLT VIMOS spectroscopy in a survey volume of ~106 Mpc3 with a limiting Lyα luminosity of ~3 × 1042 ergs s−1. We derive the LFs of the Lyα and UV continuum (≃1500 Å) for each redshift, taking into account the statistical error and the field-to-field variation. We find that the apparent Lyα LF shows no significant evolution between z = 3.1 and 5.7 within factors of 1.8 and 2.7 in L* and φ*, respectively. On the other hand, the UV LF of LAEs increases from z = 3.1 to 5.7, indicating that galaxies with Lyα emission are more common at earlier epochs. We identify six LAEs with AGN activities from our spectra combined with VLA, Spitzer, and XMM-Newton data. Among the photometrically selected LAEs at z = 3.1 and 3.7, only ≃1% show AGN activities, while the brightest LAEs with log L(Ly α) ≳ 43.4–43.6 ergs s−1 appear to always host AGNs. Our LAEs are bluer in UV-continuum color than dropout galaxies, suggesting lower extinction and/or younger stellar populations. Our stacking analyses provide upper limits to the radio luminosity and the fHe II/fLyα line fraction and constrain the hidden star formation (+low-luminosity AGN) and the primordial population in LAEs.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/19420b66a769ad5a8ccd058909f25f103997d63a

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

A large Hα survey at z = 2.23, 1.47, 0.84 and 0.40: the 11 Gyr evolution of star-forming galaxies from HiZELS (2012, background): “Spectroscopic redshift are also available for a fraction of the selected lineemitters (Lilly et al. 2009; Yamada et al. 2005; Simpson et al. 2006; Geach et al. 2008; van Breukelen et al. 2007; Ouchi et al. 2008; Smail et al. 2008; Ono et al. 2010)6.”
AN ATLAS OF z = 5.7 AND z = 6.5 Lyα EMITTERS, (2010, methodology): “At z = 5.7 our distribution of luminosities is very similar to that of Ouchi et al. (2008), despite some methodological differences.”
COMPLETING THE CENSUS OF Lyα EMITTERS AT THE REIONIZATION EPOCH (2011, methodology): “The coincidence of UV LFs of LBG and LAE at z ∼ 6 was confirmed by S06 and Ouchi et al. 2008.”
VERY STRONG EMISSION-LINE GALAXIES IN THE WFC3 INFRARED SPECTROSCOPIC PARALLEL SURVEY AND IMPLICATIONS FOR HIGH-REDSHIFT GALAXIES, (2011, background): “Using R − i > 1 and i − z > 1.2, Ouchi et al. (2008, 2010) found in their spectroscopic follow-up that such contamination is very small for their sample of z ∼ 5.7 and z ∼ 6.6 candidates, respectively.”
Evolution in the properties of Lyman-α emitters from redshifts z ~ 3 to z ~ 2 (2008, methodology): “…Møller & Warren 1993; Cowie & Hu 1998; Steidel et al. 2000; Fynbo et al. 2001, 2003; Matsuda et al. 2005; Venemans et al. 2007; Nilsson et al. 2007; Ouchi et al. 2008),z ∼ 4.5 (Finkelstein et al. 2007), z ∼ 5.7 (Malhotra et al. 2005; Shimasaku et al. 2006; Tapken et al. 2006) andz ∼ 6.5…”
LARGE AREA SURVEY FOR z = 7 GALAXIES IN SDF AND GOODS-N: IMPLICATIONS FOR GALAXY FORMATION AND COSMIC REIONIZATION (2009, methodology): “We add a Lyα luminosity to these 30% of dropout galaxies with the EW0 probability distribution of LAEs at z = 5.7 derived by Ouchi et al. (2008).”
ON THE REDSHIFT EVOLUTION OF THE Lyα ESCAPE FRACTION AND THE DUST CONTENT OF GALAXIES (2010, methodology): “It is already at this juncture in redshift that we lose the possibility to use Hα, and therefore we proceed using published UV LFs and Equation 3.”
THE SPECTRAL EVOLUTION OF THE FIRST GALAXIES. I. JAMES WEBB SPACE TELESCOPE DETECTION LIMITS AND COLOR CRITERIA FOR POPULATION III GALAXIES (2011, methodology): “…& Shull 2000; Tumlinson et al. 2001; Oh et al. 2001; Malhotra & Rhoads 2002; Schaerer 2002, 2003; Inoue 2010) and several searches have since tried to apply these techniques (e.g. Dawson et al. 2004; Nagao et al. 2005; Dijkstra & Wyithe 2007; Ouchi et al. 2008; Nagao et al. 2008; Cai et al. 2011).”
EVIDENCE FOR PopIII-LIKE STELLAR POPULATIONS IN THE MOST LUMINOUS Lyα EMITTERS AT THE EPOCH OF REIONIZATION: SPECTROSCOPIC CONFIRMATION (2015, background): “…function declines from z ∼ 3− 6 (e.g. Bouwens et al. 2014) while the Lyα luminosity function (LF) is roughly constant over the same redshift range (e.g. Ouchi et al. 2008) implies that the cosmic average Lyα escape fraction is likely increasing, from ∼ 5% at z ∼ 2 (e.g. Hayes et al. 2010;…”
DIFFUSE Lyα EMITTING HALOS: A GENERIC PROPERTY OF HIGH-REDSHIFT STAR-FORMING GALAXIES (2011, background): “…noted in many individual cases both in the nearby (e.g. Mas-Hesse et al. 2003; Hayes et al. 2007; Östlin et al. 2009) and high redshift (e.g.,Franx et al. 1997; Moller & Warren 1998; Steidel et al. 2000; Fynbo et al. 2003; Matsuda et al. 2004; Adelberger et al. 2006; Ouchi et al. 2008) universe.”
Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly (2009, unknown): “…Ouchi et al. (2008) 3.140 0.040 >0.0300 Lyα Kudritzki et al. (2000) 3.400 0.030 >0.0060 Lyα Hu et al. (1998) 3.438 0.033 >0.0100 Lyα Cowie & Hu (1998) 3.463 0.982 >0.0220 Lyα van Breukelen et al. (2005) 3.690 0.060 >0.0021 Lyα Ouchi et al. (2008) 3.700 0.220 >0.0004 Lyα Fujita et al. (2003a); van…”
The bright end of the galaxy luminosity function at z≃7: before the onset of mass quenching? (2013, methodology): “Furthermore, in the UDS dataset we have independently selected the brightest z = 6.6 LAE in the field, which was initially found using narrow-band imaging (where it is > 1 mag brighter than in the continuum bands that we use for selection) by Ouchi et al. (2008).”
Reionization and Galaxy Evolution Probed by z = 7 Lyα Emitters (2007, background): “…use φ∗ = (9.2+2.5 −2.1, 3.4 +1.0 −0.9, 7.7 +7.4 −3.9) × 10 −4Mpc−3 and L∗ = (5.8+0.9 −0.7, 10.2 +1.8 −1.5, 6.8 +3.0 −2.1) × 10 42 erg s−1 with α = −1.5 for Lyα LFs of LAEs at z = 3.1, 3.7 and 5.7 in ∼ 1.0 deg2 of the SXDS field (Ouchi et al. 2007). ρLyα is converted to SFRDLyα by using equation 1.”