RESCUER: Cosmological K-corrections for star clusters

**RESCUER: Cosmological K-corrections for star clusters**
Authors: Marta Reina-Campos and William E. Harris
Date: May 2024

Manuscript arXiV ID: arXiv:2310.02307 -- Accepted by MNRAS on May 2024

* These tables contain the K-corrections and their uncertainties calculated for star clusters using the E-MILES stellar library.
* The authors assumed that star clusters are well represented by single-age and metallicity simple stellar populations (SSPs) described by the BaSTi stellar isochrones and the Chabrier 2003 initial mass function.
* Each table corresponds to the K-corrections and their uncertainties for a given combination of filters. The authors considered eleven broad-band filters from the HST/ACS and the JWST/NIRCam cameras. 
* The uncertainties are estimated using all models within 0.3 dex and 20% in metallicity and age space, respectively, of the target model, and they correspond to the distances to the 10-90th percentiles of the K-corrections of these models.
* The tables labeled "csv_homo_filter_X_" correspond to homochromatic K-corrections within the wavelength range of the filter X, whereas those labeled "csv_hetero_filter_X_filter_Y_" contain the K-correction from the observed filter X to the rest-frame filter Y.

Within every table:
* The K-corrections are given in AB mags
* The first column represents the redshift at which the K-correction has been calculated
* All of the subsequent columns correspond to the redshift evolution of the K-correction (_target) and their asymmetric uncertainties (_lower and _upper) for a given stellar population, as indicated at the top
* The stellar populations are labeled as in the E-MILES stellar library: e.g. "Ech1.30Zm2.27T01.0000", corresponds to a SSP of [M/H] = -2.27 and 1 Gyr old
* Dummy values of -100 are placed in the redshifts larger than than the one allowed by the Planck 2018 cosmology.
* When an uncertainty equals zero indicates that the target K-correction was smaller/larger than the 10th/90th percentile of the distribution of K-corrections. This typically occurs in models at the edge of the grid of models (i.e. at a corner).