A Rapid Evolution in the Observed Mbh/M* Relation at z > 3 Revealed via Spectro-photometric SED-Modeling: Additional Figures and Machine-Readable Tables

Machine-readable tables and full sets of additional figures for the paper "A Rapid Evolution in the Observed Mbh/M* Relation at z > 3 Revealed via Spectro-photometric SED-Modeling" by Gupta, Taylor, Curtis-Lake et al. submitted 2026. If you make use of these data, Contents Figure Sets:fig-10-figureset.pdffig-11-figureset.pdffig-12-figureset-stellaronly.pdffig-12-figureset-stellarnlr.pdffig-12-figureset-stellarnlragncontinuum.pdf Tables:table-2-sample-table.fitstable-3-literature-sample-table.fits File Descriptions Files are named to match their associated figure/table in the text. The following are brief descriptions for each file. fig-10-figureset.pdf Comparison of the best-fit stellar-only (top), stellar+NLR (middle), and stellar+NLR+AGN-continuum (bottom) model spectra to the observed PRISM spectrum for BL AGN in our sample. Inset plots show the M* posterior distributions for each model, and text in bottom two panels reports the BF for the stellar+NLR and stellar+NLR+AGN-continuum model, respectively, computed relative to the stellar-only model. Note that we only fit the narrow component of Ha, so the best-fit spectrum may not visually match the observed Ha emission line even in a well-fitting model. fig-11-figureset.pdf Comparison of the best-fit stellar-only, stellar+NLR, and stellar+NLR+AGN-continuum model emission line fluxes to the line fluxes measured from the observed PRISM spectrum (applying ratios from a G395M decomposition) for BL AGN in our sample. The best-fit model fluxes (as measured by our BF comparison) are shown in full opacity, and results from the remaining fits are indicated by partially transparent markers. fig-12-figureset-stellaronly.pdf "Corner" plot generated using the PYP-BEAGLE Python package showing posterior distributions for fitted parameters and their co-variances in the stellar-only model fit to each BL AGN in our sample. Parameter names and descriptions match those listed in Table 1 in the paper. fig-12-figureset-stellarnlr.pdf "Corner" plot generated using the PYP-BEAGLE Python package showing posterior distributions for fitted parameters and their co-variances in the stellar+NLR model fit to each BL AGN in our sample. Parameter names and descriptions match those listed in Table 1 in the paper. fig-12-figureset-stellarnlragncontinuum.pdf "Corner" plot generated using the PYP-BEAGLE Python package showing posterior distributions for fitted parameters and their co-variances in the stellar+NLR+AGN-continuum model fit to each BL AGN in our sample. Parameter names and descriptions match those listed in Table 1 in the paper. table-2-sample-table.fits Table containing basic information and fitted parameter values for our BL AGN sample.Columns: (1) Source ID(2) Right ascension(3) Declination(4) Redshift(5) LRD flag(6) log (Mbh/Msun)(7) log (M*/Msun)(8) log (Z*/Zsun)(9) log (tau_SFR / yr)(10) log (t_max / yr)(11) log (SFR / [Msun/yr])(12) log U^HII(13) log tau_V(14) log (Z_NLR/Zsun)(15) log U^NLR(16) log L_acc(17) log f_AGN(18) log tau_V,cont table-3-literature-sample-table.fits Table containing basic information, Mbh, and M* for our literature sample.Columns: (1) Source ID(2) Right ascension(3) Declination(4) Redshift(5) LRD flag(6) log (Mbh/Msun)(7) log (M*/Msun)