MCMC chains representing stellar halo fits for Lane et al. (2023) paper published in MNRAS (Q6709880)

Results for the paper entitled The stellar mass of the Gaia-Sausage/Enceladus accretion remnant published in MNRAS by Lane, Bovy, Mackereth. The results are in the form of MCMC posterior chains, which are used to generate the results recorded in Table 1 of the manuscript. The process used to generate these data is outlined in section2 (data sample preparation), section 3 (Density modelling framework), and section 4 (Presentation of results) of the manuscript. The data are contained within a single gzipped .tar file,organized in two directories: gse/ containing the results for fits to the GS/E kinematic samples, and all/ containing the results for the fits to the whole halo sample. In the gse/ directory, there are three directories: eLz/, AD/, and JRLz/, containing the results for the fits to each of the respective kinematically defined subsamples. Within these directories, as well as within all/, are a final set of directories for each of the eight density profiles considered in the work. Within each of these directories are a single file named samples.npy which is abinary file (seethis linkfor format information) containing a numpy array of shape (# of parameters, # of posterior samples). The number of posterior samples is the number of walkers (100) times the number of samples per walker (10,000), minus the number of burn-in steps per walker (1,000) = 900,000. The number of parameters can be inferred from the density profiles definitions in section 3 of the manuscript, and the ordering of the parameters is the same as in Table 1. The units of the parameters are as in Table 1, except for the parameters theta and phi which are scaled such that they are defined on the interval (0,1), representing the intervals (0,2pi) and (0,pi) respectively.