/ftp/cats/J/ApJS/175/./128



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J/ApJS/175/128        Halpha emitting galaxies in COSMOS         (Shioya+, 2008)
The following files can be converted to FITS (extension .fit or fit.gz)
	table1.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/ApJS/175/128
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Beginning of ReadMe : J/ApJS/175/128 Halpha emitting galaxies in COSMOS-2 field (Shioya+, 2008) ================================================================================ The Halpha luminosity function and star formation rate at z 0.24 in the COSMOS 2 square degree field. Shioya Y., Taniguchi Y., Sasaki S.S., Nagao T., Murayama T., Takahashi M.I., Ajiki M., Ideue Y., Mihara S., Nakajima A., Scoville N.Z., Mobasher B., Aussel H., Giavalisco M., Guzzo L., Hasinger G., Impey C., Le Fevre O., Lilly S., Renzini A., Rich M., Sanders D.B., Schinnerer E., Shopbell P., Leauthaud A., Kneib J.-P., Rhodes J., Massey R. <Astrophys. J. Suppl. Ser., 175, 128-137 (2008)> =2008ApJS..175..128S ================================================================================ ADC_Keywords: Galaxies, optical ; Photometry, SDSS ; Equivalent widths Keywords: galaxies: distances and redshifts - galaxies: evolution - galaxies: luminosity function, mass function Abstract: To derive a new Halpha luminosity function and to understand the clustering properties of star-forming galaxies at z 0.24, we have made a narrowband imaging survey for Halpha-emitting galaxies in the Hubble Space Telescope (HST) COSMOS 2 square degree field. We used the narrowband filter NB816 (lambda_c_=8150AA, Deltalambda=120AA) and sampled Halpha emitters with EW_obs_(Halpha+[NII])>12AA in a redshift range between z=0.233 and 0.251 corresponding to a depth of 70Mpc. We obtained 980 Halpha-emitting galaxies in a sky area of 5540arcmin^2^, corresponding to a survey volume of 3.1x10^4^Mpc^3^. Description: In this analysis, we use the COSMOS official photometric redshift catalog (Capak et al., 2007, Cat. II/284 and Mobasher et al., 2007ApJS..172..117M). Details of the Subaru Suprime-Cam observations are given in Taniguchi et al. (2007ApJS..172....9T).