Galaxy Catalogues for SDSS


a) Outputs available for  z=0, 0.06, 0.13, 0.2, 0.27, 0.35, 0.42, 0.52  


 Redshift    Galaxy Catalogue          Dark Matter Output File
  0.00        galsl_sdss.cat_1178        compd4001.1178
  0.06        galsl_sdss.cat_1092        compd4001.1092
  0.13        galsl_sdss.cat_1014        compd4001.1014
  0.20        galsl_sdss.cat_0938        compd4001.0938
  0.27        galsl_sdss.cat_0870        compd4001.0870
  0.35        galsl_sdss.cat_0797        compd4001.0797
  0.42        galsl_sdss.cat_0731        compd4001.0731
  0.52        galsl_sdss.cat_0671        compd4001.0671



b) Galaxy Catalogue format (ascii)

 Each dark matter halo at the given output time  is described by the following:

  IH, VIRM, NGAL

     IH: halo index (refers to corresponding halo in the halo catalogs:  halos.propl_****)
     VIRM: log (virial mass of halo)
     NGAL: number of galaxies in halo

  
   For each galaxy in the halo, there are now 4 lines:

                                                          
   1) u,g,r,i,z (SDSS bands), j, h, k_s (2MASS bands) -- 
        observer frame apparent magnitudes of the whole galaxy

   2) M(u), M(g), M(r), M(i), M(z), J, H, K_s -- 
        rest-frame absolute magnitudes of the whole galaxy

   3) u,g,r,i,z (SDSS bands), j, h, k_s (2MASS bands) -- 
        observer frame apparent magnitudes of the bulge component

   4) mstar, gas, sfr, igal 

      mstar is log(stellar mass) in solar masses

      gas is log(gas mass) in solar masses

      sfr is the star formation rate in solar masses per year

      igal is the particle index of the galaxy: to get positions or velocities of this
       galaxy, look up particle igal in the corresponding compd4001 file (instructions
       for reading thiese files are available when they are downloaded).


c) WARNINGS about the use of these catalogues:

1) Resolution limits: Accurate star formation histories and merging histories are only
    obtained for galaxies that form inside dark matter halos of a few hundred particles 
    or more. To be conservative, this means adopting a cutoff in stellar mass of
    2e10 M_sol in your analyses of morphology or colour distributions.  

2) Incomplete physics: These simulations DO NOT include chemical evolution (colours are
   all for solar metallicity) or dust.