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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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 -