The Arizona-Montréal spectroscopic survey of hot subluminous stars -- Additional Table and Figures

These files are additional material from Appendix D and E of the paper entitled "The Arizona-Montréal spectroscopic survey of hot subluminous stars" accepted for publication in Astronomy and Astrophysics and currently available at https://arxiv.org/abs/2511.02539. 

Table D.1 is an excerpt of our complete table of results, which is available online as an ascii file at the Strasbourg astronomical Data Center (CDS). 

Figure E.1 shows the MMT spectral atlas, where the spectra of all stars in the MMT sample are ordered by increasing effective temperature. 

Figure E.2 shows the Bok spectra of all stars in the Bok sample. The observed spectra is shown in black and the best fitting model in red. Each page shows the full spectral range (divided into 2 intervals) for a given star whose name is printed at the top of the page. For each interval, we show four panels. The top panels show the observed spectra and best fit in the original flux-calibrated scale, the middle panels show the original flux-calibrated spectra along with the best fit of the continuum (red line), the bottom panels show a normalized version of the observed spectra and best-fit models. Finally, residuals are shown at the very bottom of each wavelength interval. The shaded regions on the curves show intervals excluded from the fit, mostly regions affected by interstellar features, such as the Na D and Ca H and K lines. 

Figure E.3 shows the best fit of the Spectral Energy Distribution (SED) for all stars in the Bok sample. For each star we show, as crosses of various colors, all photometric data retrieved from the queried catalogs. Grey crosses are excluded from the fits due to a low-quality flag in their respective catalog, or because they were more than 5 sigmas away from the best-fit solution. The filter name is indicated for most of the crosses, except for the series of black symbols, which are from the Gaia XP spectra. Below each fit, we show the uncertainty-weighted residuals where chi = (mag_model-mag_observed)/uncertainty. In addition to magnitudes, some stars also have colors available from certain catalogs. When this is the case, the residuals from the best fit are shown in an additional panel on the right-hand side. For stars with IR-excess, the flux contribution from the cool companion is shown with the pink curve, the flux of the hot subdwarf with the blue curve, and the total flux with the grey curve.