Astronomy & Astrophysics

All Tables

Table 1: Chronologically ordered optical and NIR observations carried out for the GRB 000418 host galaxy.
Table 2: Magnitudes of the host in the STIS CL and the ground-based $UBVRIZJ_{\rm s}K_{\rm s}$ bands. Several characteristics of the filters are displayed: filter name (1), effective wavelength (2) and bandpass width (3). The fourth column shows the measured magnitudes (in the Vega system and corrected from Galactic reddening, considering E(B-V)=0.033 given by Schlegel et al. 1998). To facilitate the calculation of the AB magnitudes, and consequently the flux densities for each band, the AB offsets are provided in the fifth column.
Table 3: The table displays the parameters of the best host galaxy SED fit when several IMFs and extinction laws, indicated in the first and second columns, are adopted. The rest of the columns display the inferred parameters under the assumed IMF and extinction law. The third column provides the confidence of the best fit (given by $\chi ^2/\rm d.o.f.$ , being $\rm d.o.f.=8$ ). The derived photometric redshift is displayed in the fourth column (and the corresponding 68% and 99% percentile errors). In the fifth and sixth columns the template family of the best fitted SED and the age of the stellar population are given. The seventh column displays the derived value of the host galaxy extinction A_V. The eighth column displays the derived rest frame absolute B-band magnitude, M_B. The ninth column gives the Luminosity of the host in units of $L^{\star }$ (Schechter 1976). The last column displays SFR $_{\rm UV}$ derived from the 2800 Å flux once it is corrected for the corresponding reddening (see Sect. 4.2.4 for a detailed discussion on the SFR $_{\rm UV}$ estimation). The table is divided in three sub-tables. The upper sub-table displays the derived parameters when a constant solar metallicity is assumed. The middle one assumes a metallicity evolving in time. The lower sub-table displays the results when no extinction is assumed.
Table 4: Results obtained based on the empirical templates by Kinney et al. (1996). The templates have been ordered according to their colour, bluer on the top (Stb1) and redder on the bottom (B). As it can be seen there is a clear correlation between the goodness of the fit and the colour of the template: the bluer the colour the lower $\chi ^2/\rm d.o.f.$ While Stb type galaxies (Stb1, Stb2, Stb3, Stb4, Stb5 and Stb6) have their extinction fixed by the template definition, for the quiescent ones (Sc, Sb, Sa, S0, E and B) the extinction can take any arbitrary value. In all these early and mid type cases the blue SED predicted by our photometric data is reproduced more closely by the bluest fit possible. Introduction of dust reddening for Sc, Sb, Sa, S0, E and B would just worsen the fit. This is why in the last column of the table E(B-V)=0.0 for the quiescent galaxies.