Data release for the SCM analysis:
"An improved standardization framework for Type II-P supernovae using a hierarchical Bayesian approach" (Holas et al. A&A, 2026, in press)

Contact: Alexander Holas <alexander.holas@mailbox.org>

These files contain the spectra of each of the supernovae observed
and used in the above paper.  The spectra are redshift-corrected
and corrected for Milky Way extinction using the extinction maps
of Schlafly & Finkbeiner (2011) and a Fitzpatrick et al. (2019)
extinction curve through the built-in dust extinction correction
of the Python package specutils.

Each sub-directory contains all spectra of each supernova, and a csv
file containing various information such as the redshift, extinction
values, and MJD of each observed spectrum.

Column explanation:
File:                Associated spectral file
MJD:                 Observation date
MFR_unc:             Multi-filter ratio uncertainty
Repeat_unc:          Repeatability uncertainty
Grey_unc:            Combined MFR and repeatability uncertainty (added in quadrature)
Host_sub:            TRUE if host galaxy was subtracted.
Redshift:            Cosmological redshift
Redshift_PV:         Redshifts corrected for peculiar velocities using the 2M++-SDSS map
Redshift_Helio:      Heliocentric redshift
Redshfit_Error:      Redshift uncertainty
A_V:                 Milky Way extinction value
IAU_name:            IAU name
MJD_Explosion:       Median time of explosion in MJD
MJD Explosion Error: Standard deviation of time of explosion in days.

The individual spectral files contain one spectrum each, with three
columns of wavelength, flux, and flux uncertainty.

These results are based on flux-calibrated spectra from the SuperNova
Integral Field Spectrograph (SNIFS), built and operated by the Nearby
Supernova Factory.

If you wish to provide access to these data via your own website, please
make a link to this website; please do not host the data directly on
your site.


References when using these data:

\bibitem[Holas et al.(2026)]{} Holas, A., Taubenberger, S., Vogl, C. et al.\ 2026, arXiv:TBD
