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A Search for Lyman alpha Emitters at Redshift 3.7 | | Shinobu S. Fujita
; Masaru Ajiki
; Yasuhiro Shioya
; Tohru Nagao
; Takashi Murayama
; Yoshiaki Taniguchi
; Sadanori Okamura
; Masami Ouchi
; Kazuhiro Shimasaku
; Mamoru Doi
; Hisanori Furusawa
; Masaru Hamabe
; Masahiko Kimura
; Yutaka Komiyama
; Masayuki Miyazaki
; Satoshi Miyazaki
; Fumiaki Nakata
; Maki Sekiguchi
; Masafumi Yagi
; Naoki Yasuda
; Yuichi Matsuda
; Hajime Tamura
; Tomoki Hayashino
; Keiichi Kodaira
; Hiroshi Karoji
; Toru Yamada
; Kouji Ohta
; Masayuki Umemura
; | | Date: |
2 Oct 2002 | | Subject: | astro-ph | | Abstract: | We present the results of a survey for emission-line objects based on optical intermediate-band ($lambda_{
m c}$ = 5736 AA ~ and $Deltalambda$ = 280 AA) and broad-band ($B$, $V$, $R$, and $i^prime$) observations of the Subaru/XMM-Newton Deep Field on the 8.2 m Subaru telescope with the Subaru Prime Focus Camera, Suprime-Cam. All the data were obtained during the guaranteed time observations of the Suprime-Cam instrument. The intermediate-band image covered a sky area with 10minpoint62 $ imes 12minpoint40 approx 132$ arcmin$^2$ in the Subaru/XMM-Newton Deep Field (Ouchi et al.). Using this image, we have found 23 emission-line sources whose observed emission-line equivalent widths are greater than 250 AA. Their optical multicolor properties indicate that six emission-line sources are Ly$alpha$ emitters at $z approx$ 3.7 ($Delta z approx 0.22$). They are either intense starburst galaxies or active galactic nuclei like quasars at $z approx$ 3.7. Two more emission-line sources may also be Ly$alpha$ emitters at $z approx$ 3.7 although their multicolor properties are marginal. Among the remaining 15 emission-line objects, eight objects appear strong emission-line galaxies at lower redshift; e.g., [O {sc ii}] $lambda$3727 emitters at $z approx 0.54$, H$eta$ at $z approx 0.18$, or [O {sc iii}]$lambda$5007 emitters at $z approx 0.15$. The remaining seven objects are unclassified because they are too faint to be detected in broad-band images. We discuss observational properties of these strong emission-line sources. In particular, our data allow us to estimate the star formation density at $z approx 3.7$ for the first time. | | Source: | arXiv, astro-ph/0210055 | | Services: | Forum | Review | PDF | Favorites | |
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