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.

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Contents

Figure Sets:
fig-10-figureset.pdf
fig-11-figureset.pdf
fig-12-figureset-stellaronly.pdf
fig-12-figureset-stellarnlr.pdf
fig-12-figureset-stellarnlragncontinuum.pdf

Tables:
table-2-sample-table.fits
table-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)