TY - JOUR

T1 - Photometric properties of Lyα emitters at z ≈ 4.86 in the cosmos 2 square degree field

AU - Shioya, Y.

AU - Taniguchi, Y.

AU - Sasaki, S. S.

AU - Nagao, T.

AU - Murayama, T.

AU - Saito, T.

AU - Ideue, Y.

AU - Nakajima, A.

AU - Matsuoka, K.

AU - Trump, J.

AU - Scoville, N. Z.

AU - Sanders, D. B.

AU - Mobasher, B.

AU - Aussel, H.

AU - Capak, P.

AU - Kartaltepe, J.

AU - Koekemoer, A.

AU - Carilli, C.

AU - Ellis, R. S.

AU - Garilli, B.

AU - Giavalisco, M.

AU - Kitzbichler, M. G.

AU - Impey, C.

AU - Lefevre, O.

AU - Schinnerer, E.

AU - Smolcic, V.

PY - 2009/5/1

Y1 - 2009/5/1

N2 - We present results of a survey for Lyα emitters at z ≈ 4.86 based on optical narrowband (λc = 7126 Å, Δλ = 73 Å) and broadband (B, V, r', i', and z') observations of the Cosmic Evolution Survey field using Suprime-Cam on the Subaru Telescope. We find 79 Lyα emitter (LAE) candidates at z ≈ 4.86 over a contiguous survey area of 1.83 deg2, down to the Lyα line flux of 1.47 × 10 -17erg s-1 cm-2. We obtain the Lyα luminosity function with a best-fit Schechter parameters of logL * = 42.9+0.5-0.3 erg s-1 and φ* = 1.2+8.0-1.1 × 10 -4 Mpc-3 for α = -1.5 (fixed). The two-point correlation function for our LAE sample is ξ (r) = (r/4.4+5.7 -2.9 Mpc)-1.90±0.22. In order to investigate the field-to-field variations of the properties of Lyα emitters, we divide the survey area into nine tiles of 0°5 × 0°5 each. We find that the number density varies with a factor of ≃2 from field to field with high statistical significance. However, we find no significant field-to-field variance when we divide the field into four tiles with 0.7 × 0°7 each. We conclude that at least 0.5 deg2 survey area is required to derive averaged properties of LAEs at z ∼ 5, and our survey field is wide enough to overcome the cosmic variance.

AB - We present results of a survey for Lyα emitters at z ≈ 4.86 based on optical narrowband (λc = 7126 Å, Δλ = 73 Å) and broadband (B, V, r', i', and z') observations of the Cosmic Evolution Survey field using Suprime-Cam on the Subaru Telescope. We find 79 Lyα emitter (LAE) candidates at z ≈ 4.86 over a contiguous survey area of 1.83 deg2, down to the Lyα line flux of 1.47 × 10 -17erg s-1 cm-2. We obtain the Lyα luminosity function with a best-fit Schechter parameters of logL * = 42.9+0.5-0.3 erg s-1 and φ* = 1.2+8.0-1.1 × 10 -4 Mpc-3 for α = -1.5 (fixed). The two-point correlation function for our LAE sample is ξ (r) = (r/4.4+5.7 -2.9 Mpc)-1.90±0.22. In order to investigate the field-to-field variations of the properties of Lyα emitters, we divide the survey area into nine tiles of 0°5 × 0°5 each. We find that the number density varies with a factor of ≃2 from field to field with high statistical significance. However, we find no significant field-to-field variance when we divide the field into four tiles with 0.7 × 0°7 each. We conclude that at least 0.5 deg2 survey area is required to derive averaged properties of LAEs at z ∼ 5, and our survey field is wide enough to overcome the cosmic variance.

KW - Galaxies: distances and redshifts

KW - Galaxies: evolution

KW - Galaxies: luminosity function

KW - Mass function

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UR - http://www.scopus.com/inward/citedby.url?scp=70449605247&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/696/1/546

DO - 10.1088/0004-637X/696/1/546

M3 - Article

AN - SCOPUS:70449605247

VL - 696

SP - 546

EP - 561

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

ER -