OBA stars membersSelection of OBA star members of IC1613 is based on the CMD rSDSS vs. (rSDSS-gSDSS). To guarantee the reliability of our selection, we first apply some cuts:rSDSS_MAG0_PSF < 21gSDSS_MAG0_PSF < 26SNR_rSDSS > 3SNR_gSDSS > 3rSDSS_chi2dof > 2gSDSS_chi2dof > 2 Note that magnitudes denoted as XXXX_MAG0_PSF correspond to PSF magnitudes corrected byextinction according to Planck et al. 2016 (https://ui.adsabs.harvard.edu/abs/2016A%26A...596A.109P/abstract). The catalog containing all the sources (3165) that satisfy the cuts above is named asIC1613_OBA_PSF.fits. As the separation is clear in the (rSDSS - gSDSS) color between stars in the IC1613 field and inthe parallel fields, we determine the probability of being a member according to only the (rSDSS -gSDSS) color. We take into account uncertainties in color. We find a color cut at (rSDSS - gSDSS) < 0.065 for a purity of OBA members of 95%. Theprobability of being an OBA star member is denoted as P_blue in the corresponding catalog. A cutin P_blue > 0.5 ensures the 95% purity of OBA star members (612 candidates). Red giant star membersSelection of red giant star members of IC1613 is based on the CCD (J0515 - gSDSS) vs.(gSDSS-iSDSS). To guarantee the reliability of our selection, we first apply some cuts:14 < J0510_MAG0_PSF < 21.514 < gSDSS_MAG0_PSF < 21.514 < iSDSS_MAG0_PSF < 21.5J0510_MAG_PSF_ERROR > 0iSDSS_MAG_PSF_ERROR > 0gSDSS_MAG_PSF_ERROR > 0SNR_J0515 > 3SNR_gSDSS > 3SNR_iSDSS > 3J0515_chi2dof > 1.8J0515_chi2dof > 1.8J0515_chi2dof > 1.8(gSDSS_MAG0_PSF - iSDSS_MAG0_PSF) > 0.5 The catalog containing all the sources (275) that satisfy the cuts above is named asIC1613_Predgiant.fits. We determine the probability of being a red giant star member according to a 2D density criteriabased on (J0515 - gSDSS) vs. (gSDSS-iSDSS) and the position of the stars in the IC1613 fieldand in the parallel fields. We take into account uncertainties in both colors. We obtain a probability for each source for a purity of red giant star members of 95%. Theprobability of being a red giant star member is denoted as P_RG in the corresponding catalog.The cut in P_RG > 0.74 ensures the 95% purity of red giant star members (103 candidates).CatalogsBoth catalogs, OBA and red giant star members, include the same number of columns (219). Column 1 (ID): arbitrary ID.Column 2 (catalog): JPLUS, only JPLUS photometry available; GNU, detected by gnuastro andPSF photometry available; BOTH, both photometries available.Column 3 (RA): right ascension from detection in the rSDSS band with gnuastro.Column 4 (DEC): declination from detection in the rSDSS band with gnuastro.Columns 5-56: JPLUS catalog entriesColumns 57-98: BANNJOS catalog entriesColumns 99-106: Flux and magnitude aperture corrected for 3 and 6 arcsec. Uncertaintiesincluded.Column 107 (match_sep_arcsec): separation un arcsec between JPLUS and gnuastro detectedsources.Columns 108-131: PSF magnitudes and their uncertainties obtained with astrophot.Columns 132-15: PSF uxes and their uncertainties in log obtained with astrophot.Columns 156-167: Zero Points for each band.Columns 168-179: Zero Point corrections according to the position in the image of each sourcefor each band.Columns 180-191: chi2dof of the point-source t to each source in each band obtained withastrophot.Column 192 (conv): yes, convergence achieved; no, no-convergence achieved; in, convergenceachieved by immobility. These are the results of the astrophotographers t to each sourceassuming a point-source model.Column 193 (chi2dof): Total chi2dof in all bands obtained with astrophot.Column 194 (E_BV): Dust extinction according to the position in the sky of each source usinghttps://dustmaps.readthedocs.io/en/latest/maps.html and considering Planck et al. 2016 (https://ui.adsabs.harvard.edu/abs/2016A%26A...596A.109P/abstract).Columns 195-218: Correction of dust extinction in each band (A_XXXX) and magnitude correctedby dust extinction in each band (XXX_MAG0_PSF).Column 219: probability of being an OBA star member (P_blue) or red giant member (P_RG)