The default or reference catalog is the one that uses Milky Way extinction, averaged aperture correction method, and Padova stellar evolutionary tracks (i.e., Row 1, Column 2, green link in the table). For further details on these catalogs, please see Adamo et al. 2017, ApJ, 841, 131.
Table of aperture corrections based on the CI of the source in each band. The first column contains the aperture correction and the second column the CI of simulated sources.
Table of aperture corrections based on the CI of the source in each band. The first column contains the aperture correction and the second column the CI of simulated sources.
Table of aperture corrections based on the CI of the source in each band. The first column contains the aperture correction and the second column the CI of simulated sources.
Table of aperture corrections based on the CI of the source in each band. The first column contains the aperture correction and the second column the CI of simulated sources.
Table of aperture corrections based on the CI of the source in each band. The first column contains the aperture correction and the second column the CI of simulated sources.
The stochastic models use a Bayesian model to derive the cluster properties from broadband photometry. The method, described in detail in Krumholz et al. 2015, ApJ, 812, 147, returns the full marginal posterior probability distributions of mass, age and extinction given priors on the mass, age and extinction distribution. All the models available here assume Padova stellar evolutionary tracks, solar metallicity, Milky Way extinction, a Kroupa IMF and a 50% fraction for the ionizing photons that are reprocessed into nebular emission within the observational aperture.
The prior on the mass distribution is dN/dM ~ M^(-beta), with beta taking values of 1, 1.5 and 2, and written as "ms" in the table. The prior on the age distribution is dN/dt ~ T^(-gamma), with gamma taking values of 0, 0.5 and 1, and written as "ts" in the table. The prior for the extinction A_V is considered as a flat distribution. The fiducial prior distribution is p(_prior) (log M, log T, A_V) ~ M^(-1) T^(-0.5), and are denoted by the green links in the FITS table below.
The FITS files contain the full marginal posterior probability distributions for the mass, age, and extinction together with the photometric distance, and normalized photometric distance of each cluster (see Krumholz et al. 2015, ApJ, 812, 147 for details). The "_{avgapcor, cibased}.txt" files contain a summary of the posterior probability distributions for each cluster. See the "_readme.txt" file for details.