Hot Star Spectral Library (HST/STIS)


September 2017 version is available in a collection of FITS files or text files. This version has been put on a common logarithmic wavelength scale (see python code at the bottom of the page) and an extinction correction has been applied. The spectra are also available in the last column of the tables below.

In December 2017, we added stars 21, 22, 23, 33, and 70.

Stars 3 and 18 duplicate the same object, separately reduced.

1. PAGB stars

Visit Obs? Name V B-V Tefflog g[Fe/H] R.A. (2000) dec.(2000) Literature notesReduction notesAstrophysical notesSpectra
01 N GJ 398.2 11.14 -0.23 80000 5.0 0.0 10 39 36.74039 +43 06 09.2551 sdO, Feige 34 flux std., params from Thejll A&A 248 448 (1991)
02 N PN A66 36 11.57 -0.30 95000 5.3 0.0 13 40 41.34369 -19 52 55.3200 sdO, Werner 2003 hot CSPN, H-rich
03 Y NGC 1535 (dupl. no. 18) 12.11 J-K=-0.038 70000 4.6 0.0 04 14 15.782 -12 44 21.68 Werner 2003 hot CSPN, H-rich, NGC 1535, Has companion: Ciradullo et al. 1999 AJ 118, 488MgII is interstellar. B-V guess based on J-K = -0.08. FITS | txt
04 Y HD 107969 13.2 -0.4 82000 5.5 -1.0 12 24 30.76 -18 47 05.4 Werner 2003 hot CSPN, H-rich halo object NGC 4361MgII is interstellar. FITS | txt
05 Y LSS 1362 12.30 -0.22 100000 5.3 0.0 09 52 44.524 -46 16 47.47 Werner 2003 hot CSPN, H-richNo helium lines. MgII is interstellar. FITS | txt
06 Y PN A66 78 13.25 -0.21 110000 5.5 0.0 21 35 29.38 +31 41 45.3 Werner 2003 hot CSPN, H-deficientEmission lines. MgII is interstellar. FITS | txt
07 N NGC 1360 11.16 -0.21 110000 5.6 0.0 03 33 14.64755 -25 52 17.9955 Werner 2003 hot CSPN, H-rich
08 Y NGC 7094 13.68 J-K=-0.050 110000 5.7 0.0 21 36 52.97 +12 47 19.0 Werner 2003 hot CSPN, H-deficient MgII is interstellar. B-V guess based on J-K = -0.1. FITS | txt
09 Y PN K 1-16 14.96 -0.52 140000 6.4 0.0 18 21 52.111 +64 21 53.22 Werner 2003 hot CSPN, H-deficientMgII is interstellar. FITS | txt
10 Y NGC 6853 14.09 -0.34 110000 6.7 0.0 19 59 36.379 +22 43 15.75 Werner 2003 hot CSPN, H-richMgII is interstellar. FITS | txt
11 Y LSV+46 21 12.87 -0.37 83000 6.7 0.0 04 43 21.270 +46 42 05.84 Werner 2003 hot CSPN, H-richMgII is interstellar. FITS | txt
12 N NGC 7293 13.52 -0.37 105000 7.0 0.0 22 29 38.541 -20 50 13.64 Werner 2003 hot CSPN, H-rich
13 Y LSIII+52 24 12.51 0.72 24000 3.0 0.0 22 04 12.302 +53 04 01.37 Sarkar et al. 2012 MNRAS 421 679 FITS | txt
14 Y LSIV-12 111 11.4 -0.1 20500 2.35 -0.4 20 01 49.8373 -12 41 17.600 Ryans et al. 2003 A&A 401 1119MgII is mostly interstellar. FITS | txt
15 N HD 341617 11.39 0.02 20750 2.35 -0.5 18 08 20.0860 +24 10 43.358 Ryans et al. 2003 A&A 401 1119
16 Y GLMP 334 12.3 0.8 7400 1.4 -0.4 12 38 53.10 -57 56 31.9 Pereira et al. 2012 A&A 538 A48Spectrum not reliable at lambda < 3050 A due to probable scattered light. FITS | txt
17 Y NGC 3242 10.3 0.0 68000 4.6 0.0 10 24 46.107 -18 38 32.64 HD 90255; Mendez et al. 1988 A&A 190 113MgII is interstellar. FITS | txt
18 Y NGC 1535 (dupl. no. 3) 12.11J-K=-0.038 58000 4.3 0.0 04 14 15.782 -12 44 21.68 Mendez et al. 1988 A&A 190 113MgII is interstellar. B-V guess based on J-K = -0.08. FITS | txt
19 Y IC 2448 11.1 0.0 55000 4.5 0.0 09 07 06.262 -69 56 30.57 Mendez et al. 1988 A&A 190 113 MgII is interstellar. FITS | txt
20 N NGC 6891 12.51 -0.4 50000 3.9 0.0 20 15 08.838 +12 42 15.63 Mendez et al. 1988 A&A 190 113
21 Y NGC 2392 10.521 -0.15 47000 3.6 0.0 07 29 10.76590 +20 54 42.4830 Mendez et al. 1988 A&A 190 113 MgII mostly interstellar. Fit with a He-rich model, 35000 K, log g =44. FITS | txt
22 Y Hen 2-182 11.72 0.31 36000 3.4 0.0 16 54 35.168 -64 14 28.44 Mendez et al. 1988 A&A 190 113 Difficult to cross-correlate due to complex emission linesMgII is interstellar.FITS | txt
23 Y PN Tc 1 11.49 -0.19 33000 3.2 0.0 17 45 35.3020 -46 05 23.682 Mendez et al. 1988 A&A 190 113 MgII is interstellar.FITS | txt
24 N Hen 2-138 10.95 -0.20 27000 2.7 0.0 15 56 01.69413 -66 09 09.2307 Mendez et al. 1988 A&A 190 113

2. normal O type stars
c.f., Vacca, Garmany & Shull (1996) ApJ, 460, 914
Visit Obs? Name V B-V Teff log g [Fe/H] R.A. (2000) dec.(2000) Literature notesReduction notesAstrophysical notesSpectra
25 Y HD 93250 7.50 0.16 51000 3.90 0.00 10 44 45.02626 -59 33 54.6841 VGS96 O3 VMgII is interstellar. FITS | txt
26 Y HDE 303308 6.17 0.13 48000 3.91 0.00 10 45 05.848 -59 40 06.36 VGS96 O3 VMgII is interstellar. FITS | txt
27 Y HD 164794 5.97 0.00 47000 3.90 0.00 18 03 52.44466 -24 21 38.6269 VGS96 O4 VThe first UV observation was rejected. The second blue observation was scaled by 1.025.MgII is interstellar. FITS | txt
28 Y HD 46150 6.73 0.13 46900 3.85 0.00 06 31 55.520 +04 56 34.28 VGS96 O5 VMgII is interstellar. FITS | txt
29 Y HD 168075 8.77 0.55 49000 3.95 0.00 18 18 36.061 -13 47 36.51 VGS96 O6 VMgII is interstellar. FITS | txt
30 Y BD +60 513 9.39 0.49 40000 3.70 0.00 02 34 02.5285 +61 23 10.848 VGS96 O7 VMgII is interstellar. FITS | txt
31 Y HD 217086 7.66 0.64 40000 3.71 0.00 22 56 47.19030 +62 43 37.6487 VGS96 O7 VThe second red observation was scaled by 1.18.MgII is interstellar. FITS | txt
32 Y HD 46966 6.87 -0.04 38100 3.89 0.00 06 36 25.88773 +06 04 59.4769 VGS96 O8 VMgII is interstellar. FITS | txt
33 Y NGC6611 367 9.45 0.26 35000 4.15 0.00 18 18 52.67456 -13 49 42.6158 VGS96 O9.5 VThe first red observation was scaled by 1.025, the second by 1.04.MgII is interstellar.FITS | txt
34 Y HD 93521 7.03 -0.24 33500 3.95 0.00 10 48 23.51137 +37 34 13.0922 VGS96 O9.5 VMgII is interstellar. FITS | txt
35 Y HD 228199 9.34 0.07 30000 3.91 0.00 20 11 27.2625 +36 29 56.845 VGS96 B0.5 VMgII: probable interstellar component. FITS | txt
36 Y HD 15570 8.11 0.69 49000 3.51 0.00 02 32 49.42013 +61 22 42.0956 MgII is interstellar. FITS | txt
37 Y HD 192639 7.11 0.35 38000 3.37 0.00 20 14 30.42806 +37 21 13.8107 MgII is interstellar. FITS | txt
38 Y HD 207198 5.94 0.31 34000 3.31 0.00 21 44 53.27923 +62 27 38.0479 The second blue observation was scaled by 1.035.MgII is interstellar. FITS | txt
39 Y HD 210839 5.05 0.24 40000 3.50 0.00 22 11 30.57571 +59 24 52.1546 The second blue observation was scaled by 1.032.MgII is interstellar. FITS | txt

3. Horizontal branch stars
Visit Obs? Name V B-V Teff log g [Fe/H] R.A. (2000) dec.(2000) Literature notesReduction notesAstrophysical notesSpectra
40 N HW Vir 10.69 -0.23 26000 5.57 0.00 12 44 20.23731 -08 40 16.8338 Wlodarczyk & Olszewski 1994 Acta Astron 44 407
41 Y GJ 894.3 11.50 -0.05 40000 5.00 0.00 23 19 58.39814 -05 09 56.1604 sdO Feige 110 Heber et al 1984MgII is interstellar. FITS | txt
42 N Feige 86 10.02 -0.13 17500 4.2 0.00 13 38 24.76522 +29 21 56.0188 Heber 1987 MitAG 70, 79
43 Y PHL 382 11.4 -0.1 18200 4.1 0.00 22 43 06.0147 -14 50 37.393 Heber 1987 MitAG 70, 79MgII may have an interstellar component. FITS | txt
44 N PHL 25 11.1 0.4 19500 5.0 0.00 21 32 04.6260 -17 18 39.562 Heber 1987 MitAG 70, 79
45 N SB 290 10.26 -0.07 28200 5.5 0.00 00 42 58.31003 -38 07 37.2941 Heber 1987 MitAG 70, 79
46 N UV 1758+36 11.39 -0.22 31800 5.6 0.00 18 00 18.86556 +36 28 56.3192 Lamontagne et al. 1985 ApJ 299, 496
47 Y SB 707 11.9 -0.3 34000 6.0 0.00 01 43 48.54613 -24 05 10.2360 Lamontagne et al. 1985 ApJ 299, 496 =Ton s 227 FITS | txt
48 N Feige 66 10.59 -0.33 36000 6.0 0.00 12 37 23.51704 +25 03 59.8806 Baschek 1982 A&A 112 76; in cluster Mel 111 = Coma Berenices
49 N PG 0342+026 11.12 -0.26 21800 5.0 0.00 03 45 34.578 +02 47 52.81 Lamontagne et al. 1987; E(B-V)=0.06
50 Y HD 205805 10.158 -0.241 25000 5.0 0.00 21 39 10.61355 -46 05 51.5321 Altmann & de Boer 2000 FITS | txt
51 N BD+36 2242 9.904 -0.065 11400 4.4 0.00 12 09 15.83348 +35 42 42.9449 Altmann & de Boer 2000
52 N HD 117880 9.059 0.082 9200 3.4 0.00 13 33 29.80575 -18 30 54.2885 Altmann & de Boer 2000
53 N HD 130095 8.155 0.032 8800 3.15 0.00 14 46 51.21208 -27 14 53.9589 Altmann & de Boer 2000
54 N HD 139961 8.857 0.098 8750 3.3 0.00 15 42 52.81942 -44 56 40.8282 Altmann & de Boer 2000
55 N U Com 11.76 0.16 7050 2.3 -1.38 12 40 03.19721 +27 29 56.1489 Pancino et al. 2015
56 N BK Eri 12.00 -9.99 6950 2.3 -1.54 02 49 55.856 -01 25 11.88 Pancino et al. 2015 - RR Lyr variable
57 N X Ari 8.97 0.28 6950 3.1 -2.19 03 08 30.88520 +10 26 45.2282 Pancino et al. 2015 - RR Lyr variable
58 Y DR And 12.42 1.24 6200 2.3 -1.53 01 05 10.704 +34 13 06.32 Pancino et al. 2015 - RR Lyr variable FITS | txt
59 N SS Leo 10.38 0.14 7700 2.5 -1.46 11 33 54.496 -00 02 00.00 Pancino et al. 2015 - RR Lyr variable
60 Y EGB 5 14.2 -0.9 42000 5.8 0.0 08 11 12.768 +10 57 17.10 Mendez et al. 1988 A&A 190 113 MgII: probable interstellar component. FITS | txt
61 N FHB 6 13.05 -0.03 10775 3.6 -1.0 12 42 57.707 +32 04 03.58 Gray et al. 1996 AJ 112 2291 GSC 02531-00549
62 N PG_1104+243 11.39 0.10 27200 5.5 0.4 11 07 26.231 +24 03 11.16 ([N/H] not [Fe/H]) Lamontagne et al. 1987 E(B-V)=0.03 has G2V companion
63 N HD_4539 10.29 -0.17 24800 5.4 0.6 00 47 29.21992 +09 58 55.6953 ([N/H] not [Fe/H]) Baschek et al. 1972
64 Y HD_269696 11.138 -0.297 40000 5.5 0.0 05 31 40.3489 -69 53 02.183 Lynas-Gray et al. 1984 (aka. LB 3459)MgII: probable interstellar component. FITS | txt
65 N Feige_65 12.01 -0.23 26200 5.3 0.3 12 35 51.14325 +42 22 39.7210 ([N/H] not [Fe/H]) Lamontagne et al. 1985
66 Y RX_Cet 11.2 0.4 6186 2.0 -1.38 00 33 38.28188 -15 29 14.7888 Pancino et al. 2015 - RR Lyr A_V=0.078 FITS | txt
67 N RV_UMa 10.9 0.07 6068 2.3 -1.19 13 33 18.08438 +53 59 14.6081 Pancino et al. 2015 - RR Lyr A_V=0.053
68 N UZ_CVn 12.11 0.12 6780 2.35 -2.22 12 30 27.70242 +40 30 32.0210 Pancino et al. 2015 - RR Lyr A_V=0.065
69 N VX_Her 11.31 -0.57 6959 2.15 -1.61 16 30 40.79990 +18 22 00.5524 Pancino et al. 2015 - RR Lyr A_V=0.133
70 Y RX J0122.9-7521 15.4 -0.4 180000 7.5 0.3 01 22 53.37 -75 21 13.8 Werner & Herwig 2006 PASP 118 183 Difficult to cross-correlate because of extreme temperature. Both red observations scaled by 0.90 to match optical.MgII is interstellar.FITS | txt



# Python code to read and plot one of the text files:
import matplotlib.pyplot as plot
from pylab import *

userstarnum = int(raw_input("Enter star number: "))
intystr = str(userstarnum).zfill(2)  # pad a leading zero, if needed

# set up a logarithmic wavelength scale where
# log10(lam_n+1) - log10(lam_n) = 0.0002.
# wbegin = 1640.000 (log = 3.215)  wend = 10256 (log = 4.011)
nw = 1 + int((4.011 - 3.215)/0.0002 + 0.000001)
# nw = 3981 pixels in this scheme
wlog = []
for i in range(nw):
    wave = 3.215 + i*0.0002
    wlog.append(10.00**wave)

flux=[]; ferr=[]
with open('dustcor_star'+intystr+'.txt') as ftxt:
    for line in ftxt:
        data = line.split()
        flux.append(float(data[0]))
        ferr.append(float(data[1]))

# make a linear (not semi-log) plot.
step(wlog,flux,where='mid',label='flux',color='b')
errorbar(wlog,flux,yerr=ferr,color='b',ls='None')
xlabel('Wavelength (Angstroms)')
ylabel('Dust-corrected flux (erg/s/cm**2/Angstrom)')
show()