VizieR Online Data Catalog: MUSEWide Lyman alpha luminosity function 3<z<6 (Herenz+, 2019)
Abstract
This data release consists of the Lyman alpha emitter galaxy catalogue and the selection functions used in the calculation of the Lyman alpha luminosity function from the first instalment from the MUSEWide survey (Herenz et al. 2017A&A...606A..12H, Cat. J/A+A/606/A12). We release both the point source selection function and the realistic source selection function (see Sect. 3.3 of the paper). Note, that the reported Lyman alpha line fluxes in the galaxy catalogue are corrected for fluxlosses with respect to Herenz et al. (2017A&A...606A..12H); see Sect. 2.3 of the paper.
Moreover, in this data release we also provide the inverted loglikelihood function (S=2lnL) for a Schechter parametrisation (Schechter, 1976ApJ...203..297S). This function S was obtained with the maximum likelihood formalism described in Sect. 4.3 of the paper. As this method does not constrain the normalisation parameter φ^{*} of the Schechter function, we also release a map of this parameter as a function of the two other parameters α and L^{*}. A visualisation of these maps is presented in Figure 12 of our paper.
The selection functions are stored as FITS files (Pence et al., 2010A&A...524A..42P). The file MW_{124}LAE_{LF}selfun_ps.fits stores the point source selection function, while the file MW_{124}LAE_{LF}selfun.fits stores the realistic source selection function. Each FITS file consists of 3 headerdata units (HDUs). HDU 1 contains a 2D array of dimension 1000*3681 containing the probability f (0<=f<=1) that a Lyman alpha emitter at a given flux and wavelength is contained in the survey catalogue. The first axis of length 1000 corresponds to Lyman alpha flux and the second axis of length 3000 corresponds to wavelength. The translation table between wavelength index of HDU 1 and wavelength value (in units of Angstrom) is given in HDU 2 as an 1D array of length 3681. The translation table between flux index of HDU 1 and flux value F (in units of  logF[erg/s/cm^{2}]) is provided in HDU 2 as an 1D array of length 1000. Section 4 in the paper describes how this function and the catalogue were used to construct the nonparametric and parametric determinations of the Lyman alpha emitter luminosity function.
The values of the inverted loglikelihood map (Equation 22 in the paper) for the Schechter function parameters alpha and logL* (in erg/s) are stored as a twodimensional 401*401 array in the FITS file MW_{124}LAE_{LF}sf_{logL}map.fits. The first axis (NAXIS1) in this FITS encodes logL*, while the second axis (NAXIS2) encodes the faintend slope alpha. The transformation between array coordinates and logL* and alpha values is linear, with the CRVALi, CRPIXi, and CDELTi (i=1,2) keywords defining the transformation as described in Wells et al. (1981A&AS...44..363W). The corresponding normalisation log(phi*[Mpc^{3}]) is stored in the FITS file MW_{124}LAE_{LF}logphi_map.fits which follows the same axis conventions as MW_{124}LAE_{LF}sf_{logL}map.fits.
(3 data files).
 Publication:

VizieR Online Data Catalog
 Pub Date:
 November 2018
 Bibcode:
 2018yCat..36210107H
 Keywords:

 Surveys;
 Galaxy catalogs