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

Latour, Marilyn

Publisher
Zenodo
DOI
10.5281/zenodo.17523833
Repository
zenodo.org
Language
en

Abstract

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.

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Latour et al.: The Arizona-Montréal survey of hot subdwarf stars Appendix E: Additional Figures 4000 4200 4400 4600 4800 5000 Wavelength (Å) 1 2 3 4 5 Relative flux BD+48_2721 21949, 4.95, -2.09 He I He II PG1432+004 23208, 5.27, -2.40 He I He II PG1627+017 23573, 5.34, -2.95 He I He II PG1111-077 23614, 5.54, -3.52 He I He II HD4539 24393, 5.31, -2.32 He I He II PG0856+121 24890, 5.60, -3.80 He I He II PG1538+269 25108, 5.40, -3.18 He I He II PB7352 25377, 5.35, -2.54 He I He II PG0250+189 25562, 5.75, -3.84 He I He II PG1340+607 25606, 5.30, -2.62 He I He II KPD0716+0258 25690, 5.31, -2.55 He I He II PG0342+026 25713, 5.52, -2.73 He I He II Fig. E.1: MMT spectra of all stars in the MMT sample ordered by increasing Teff. Under the name of each star, we indicate the Teff, logg, and helium abundance (log N(He)/N(H)) of the stars, obtained from the fit of their Bok spectrum. None of the stars is sufficiently hot and He-rich to display the Heii lines at 4200 Å and 4542 Å. The spectra of the most reddened stars, show a small diffuse interstellar band absorption around 4450 Å. Examples are PG0250+189, PG0215+183 and some of the KPD objects. Article number, page 29 of 38 A&A proofs: manuscript no. output 4000 4200 4400 4600 4800 5000 Wavelength (Å) 1 2 3 4 5 Relative flux PG1233+427 25922, 5.52, -2.57 He I He II KPD0422+5421 25957, 5.57, -2.29 He I He II PG1432+158 26001, 5.61, -2.49 He I He II PG2345+318 26118, 5.57, -2.59 He I He II PG1635+414 26126, 5.40, -2.83 He I He II US719 26141, 5.40, -2.50 He I He II PG1417+257 26165, 5.39, -2.78 He I He II PG1739+489 26304, 5.42, -2.84 He I He II KPD0629-0016 26373, 5.53, -2.82 He I He II PG1224+672 26458, 4.60, -1.79 He I He II PG1716+426 26587, 5.44, -2.95 He I He II PG0907+123 26645, 5.40, -2.92 He I He II Fig. E.1: Continued. Article number, page 30 of 38 Latour et al.: The Arizona-Montréal survey of hot subdwarf stars 4000 4200 4400 4600 4800 5000 Wavelength (Å) 1 2 3 4 5 Relative flux PG0850+170 26722, 5.44, -2.74 He I He II PG1743+477 26731, 5.49, -2.17 He I He II PG2358+107 26830, 5.56, -2.69 He I He II PG0940+068 26953, 5.41, -2.79 He I He II PG0001+275 27019, 5.58, -2.85 He I He II PHL457 27081, 5.47, -2.48 He I He II PG0101+039 27108, 5.53, -2.75 He I He II PB7032 27122, 5.49, -2.82 He I He II FEIGE109 27188, 5.69, -3.91 He I He II PG1338+481 27244, 5.42, -2.84 He I He II PG1230+052 27317, 5.58, -2.87 He I He II PG2349+002 27502, 5.69, -3.78 He I He II Fig. E.1: Continued. Article number, page 31 of 38 A&A proofs: manuscript no. output 4000 4200 4400 4600 4800 5000 Wavelength (Å) 1 2 3 4 5 Relative flux KPD0025+5402 27529, 5.45, -3.00 He I He II PG1156-037 27548, 5.52, -2.89 He I He II PG1433+239 27681, 5.41, -3.00 He I He II PG1232-136 27739, 5.75, -1.41 He I He II PG1329+159 27865, 5.44, -2.93 He I He II PG1725+252 27894, 5.44, -3.02 He I He II PG1343-102 27930, 5.50, -3.15 He I He II PG1115+201 28154, 5.46, -2.59 He I He II PG1438-029 28223, 5.52, -2.94 He I He II PG1043+760 28262, 5.59, -3.06 He I He II PB9286 28447, 5.68, -2.53 He I He II PG1241-084 28648, 5.66, -2.38 He I He II Fig. E.1: Continued. Article number, page 32 of 38 Latour et al.: The Arizona-Montréal survey of hot subdwarf stars 4000 4200 4400 4600 4800 5000 Wavelength (Å) 1 2 3 4 5 Relative flux PG0004+133 28650, 5.46, -1.88 He I He II PB5450 28743, 5.74, -2.80 He I He II FEIGE14 28748, 5.69, -2.83 He I He II PG1101+249 28841, 5.67, -2.01 He I He II HS2201+2610 28848, 5.48, -3.01 He I He II PG0215+183 28902, 5.85, -3.01 He I He II PG1458+423 28972, 5.52, -3.73 He I He II BD+42_3250 29000, 5.20, -1.48 He I He II PG1452+198 29034, 5.72, -1.97 He I He II BAL090100001 29080, 5.48, -2.73 He I He II PG0133+114 29112, 5.68, -2.43 He I He II PG0142+148 29176, 5.48, -3.11 He I He II Fig. E.1: Continued. Article number, page 33 of 38 A&A proofs: manuscript no. output 4000 4200 4400 4600 4800 5000 Wavelength (Å) 1 2 3 4 5 Relative flux PG1610+529 29195, 5.64, -2.23 He I He II PG1710+490 29290, 5.60, -2.47 He I He II PG0941+280 29372, 5.57, -3.44 He I He II PG1512+244 29393, 5.77, -2.06 He I He II PG1626+471 29662, 5.55, -3.03 He I He II PG1114+072 29726, 5.69, -2.50 He I He II PG1738+505 29784, 5.41, -1.85 He I He II PG2337+070 29894, 5.76, -2.05 He I He II FEIGE48 30043, 5.53, -2.78 He I He II PG1519+640 30218, 5.72, -2.07 He I He II HD76431 30563, 4.65, -1.67 He I He II PG1604+504 30566, 5.75, -1.61 He I He II Fig. E.1: Continued. Article number, page 34 of 38 Latour et al.: The Arizona-Montréal survey of hot subdwarf stars 4000 4200 4400 4600 4800 5000 Wavelength (Å) 1 2 3 4 5 Relative flux N188II-91 30771, 5.75, -2.28 He I He II FEIGE91 30810, 5.93, -1.99 He I He II PG1403+316 30848, 5.74, -2.35 He I He II KPD2109+4401 30991, 5.66, -2.33 He I He II PG0242+132 31341, 5.32, -1.57 He I He II KPD2118+3841 31376, 5.78, -1.78 He I He II PG0918+029 31387, 5.83, -2.42 He I He II PG1032+406 31601, 5.86, -2.28 He I He II PHL197 31687, 5.73, -1.97 He I He II PG0911+456 31988, 5.81, -2.50 He I He II PG1303-114 32033, 5.84, -2.64 He I He II UVO1758+36 32250, 5.77, -1.63 He I He II Fig. E.1: Continued. Article number, page 35 of 38 A&A proofs: manuscript no. output 4000 4200 4400 4600 4800 5000 Wavelength (Å) 1 2 3 4 5 Relative flux PG1619+522 32605, 5.80, -2.03 He I He II PG0919+273 32791, 5.86, -2.35 He I He II PG1605+072 33082, 5.34, -2.60 He I He II FEIGE108 33814, 5.88, -2.92 He I He II PG2151+100 33946, 5.61, -3.66 He I He II PG1039+219 33988, 5.80, -2.19 He I He II PG1255+547 34388, 5.79, -1.49 He I He II PG0057+155 34736, 5.75, -1.68 He I He II PG1219+534 34886, 5.85, -1.52 He I He II PB7409 35005, 5.81, -1.53 He I He II FEIGE66 35112, 5.94, -1.76 He I He II PG1538+401 35310, 5.98, -5.05 He I He II Fig. E.1: Continued. Article number, page 36 of 38 Latour et al.: The Arizona-Montréal survey of hot subdwarf stars 4000 4200 4400 4600 4800 5000 Wavelength (Å) 1 2 3 4 5 Relative flux PG1051+501 35353, 5.17, -1.44 He I He II PG1618+563 35405, 5.83, -1.70 He I He II HD149382 35519, 5.80, -1.50 He I He II PG0014+067 35638, 5.93, -1.63 He I He II PG1047+003 36125, 5.86, -1.94 He I He II PG0909+276 36300, 5.87, -0.97 He I He II KPD1930+2752 36438, 5.61, -1.56 He I He II PG1616+144 37063, 5.87, -1.50 He I He II PG0934+186 37291, 5.75, -3.37 He I He II LSI+63_198 37376, 5.84, -1.63 He I He II PG1722+286 37387, 6.05, -1.76 He I He II PHL1548 39381, 5.89, -1.89 He I He II Fig. E.1: Continued. Article number, page 37 of 38