:  Photometry

The magnitudes in the lightcones are available for two stellar populations synthesis models: Bruzual & Charlot (2003) and Maraston (2005). For both models the same Chabrier (2003) IMF was adopted. All magnitudes are in the AB system.

We have significantly expanded the number and wavelegth coverage of photometric bands for which fluxes are computed, from observed-frame UV to the IRAC near-infrared. The 40 filters available are presented in the following figure and their curves are available in this link.

Top panel: GALEX FUV and NUV, Johnson-Bessel U, B, V, Cousins Rc, Ic, VISTA Z, Y, J, H, Ks, Johnson-Bessel K and IRAC 3.6μm, 4.5μm, 5.8μm and 8.0 μm bands;
Second panel: SDSS u, g, r, i, z bands;
Third panel: bands from HST instruments, three UV bands from the WFC3-UVIS (0.225μm, 0.275μm, 0.336μm), seven optical bands from the ACS-WFC (0.435μm, 0.475μm, 0.606μm, 0.625μm, 0.775μm, 0.814μm, 0.850μm) and three near-infrared bands from the WFC3-IR (1.05μm, 1.25μm, 1.60μm);
Bottom panel: VIMOS U band, 2 NICMOS near-infrared bands (1.1μm and 1.6μm) and two WFPC2 bands (0.30μm and 0.45μm).

Together with the observed-frame photometry we also provide rest-frame data for a restricted set of bands (SDSS and VISTA/2MASS). This is aimed at making the lightcones a better tool to test observational derivations of intrinsic galaxy properties. The wide wavelength coverage of observed- and rest-frame photometry, together with the two stellar population synthesis models considered, can be used to check derivations of rest-frame magnitudes from observed photometry, as well as the reliability of properties obtained from SED fitting, such as stellar masses, ages and star-formation histories (intrinsically predicted by the semi-analytic model).