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The Luminosity Function of Lyman Alpha Emitters at Redshift z~5.7 | | Esther M. Hu
; Lennox L. Cowie
; Peter Capak
; Richard G. McMahon
; Tomoki Hayashino
; Yutaka Komiyama
; | | Date: |
24 Nov 2003 | | Journal: | Astron.J. 127 (2004) 563-575 DOI: 10.1086/381302 | | Subject: | astro-ph | | Affiliation: | IfA, Univ. of Hawaii, IOA, Cambridge, Tohoku Univ., Subaru Telescope | | Abstract: | We report results of a deep wide-field narrowband survey for redshift z~5.7 Ly alpha emitters carried out with SuprimeCam on Subaru 8.3-m telescope. Deep narrowband imaging of the SSA22 field through a 120 A bandpass filter centered at 8150 A was combined with deep multicolor RIz’ SuprimeCam broadband imaging, and BVRZ imaging taken with CFHT’s CFH12K camera to select high-redshift galaxy candidates. Spectroscopic observations were made using the new wide-field multi-object DEIMOS spectrograph on Keck for 22 of the 26 candidate objects. Eighteen objects were identified as z~5.7 Lyman alpha emitters, and a further nineteenth candidate was identified based on an LRIS spectrum. At the 3.3 A resolution of the DEIMOS spectra the asymmetric profile for Ly alpha emission with its steep blue fall-off can be clearly seen. We use this to describe the distribution of equivalent widths and the continuum color break properties for z~5.7 Ly alpha galaxies compared with foreground objects. The large majority (>75%) of Ly alpha lines have rest frame equivalent widths less than 240 A and can be understood in terms of young star forming galaxies with a Salpeter initial mass function for the stars. With narrowband selection criteria of I-N > 0.7 and N<25.05 (AB mags) we find a surface density of Ly alpha emitters of 0.03 per square arcminute per (deltaz=0.1) to a limiting flux just under 2e-17 erg/cm2/s. The luminosity function of the Ly alpha emitters is similar to that at lower redshifts to the lowest measurable luminosity of 1e43 ergs/s as is the universal star formation rate based on their continuum properties. We note that the objects are highly structured in both spatial and spectral properties on the angular scale of the fields (~60 Mpc), and that multiple fields will have to be averaged to accurately measure their ensemble properties. | | Source: | arXiv, astro-ph/0311528 | | Services: | Forum | Review | PDF | Favorites | |
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