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Table 13

Table to replace Table 4 of Moehler et al. (1990). Physical parameters derived for the programme sdB stars.

Object T eff log g V or y AV or Ay d l b z
(K) (cm s-2) (mag) (mag) (pc) (deg) (deg) (pc)
PG 0004+133 24 700 4.5 13.060 0.482 1500 ± 580 106.9 −47.9 1120 ± 430
PG 0039+049 26 700 4.7 12.889 0.629 1100 ± 420 118.6 −57.6 940 ± 350
PG 0101+039a 25 700 5.3 12.070 0.038 500 ± 190 129.1 −58.5 430 ± 160
PG 0133+114 26 400 4.9 12.280 0.152 840 ± 320 140.1 −49.7 640 ± 240
PHL 1079 32 000 5.5 13.38 0.593 650 ± 240 144.9 −57.1 540 ± 200
PG 0142+148 26 200 5.1 13.726 0.146 1310 ± 500 141.9 −45.8 940 ± 360
PG 0209−015 23 500 4.9 14.047 0.000 1790 ± 680 162.9 −57.7 1510 ± 580
PG 0212+148 25 000 5.0 14.482 0.226 1890 ± 760 151.2 −43.2 1300 ± 520
PG 0212+143 25 400 5.0 14.584 0.226 1990 ± 780 151.7 −43.6 1380 ± 540
PG 0242+132 26 500 4.7 13.220 0.341 1500 ± 560 160.9 −40.9 980 ± 370
PG 0342+026b 24 000 4.9 10.944 0.324 380 ± 140 184.4 −38.5 230 ± 90
PG 0856+121 23 800 5.1 13.473 0.094 1050 ± 390 216.5 +33.7 580 ± 330
PG 0907+123 26 300 5.0 13.937 0.094 1620 ± 610 217.7 +36.3 960 ± 360
PG 0918+029 29 300 5.2 13.319 0.000 1080 ± 420 229.4 +34.3 610 ± 230
PG 1255+544 31 300 5.5 13.533 0.040 890 ± 330 120.9 +62.7 790 ± 300
PG 1303−114 28 500 5.1 13.959 −0.081∗ 1630 ± 610 308.7 +51.0 1260 ± 480
PG 1432+004 22 400 5.0 12.759 0.105 810 ± 310 350.1 +53.3 650 ± 250
PG 1452+198 26 400 5.0 12.476 −0.035∗ 880 ± 320 24.7 +60.8 760 ± 280
PG 1458+423 28 000 5.3 13.79 0.058 1140 ± 430 71.0 +59.8 580 ± 220
PG 1519+640 27 000 5.2 12.458 −0.047∗ 690 ± 250 100.3 +46.2 500 ± 190
PG 1532+523 29 800 5.4 14.043 −0.037∗ 1240 ± 460 83.8 +50.8 960 ± 360
PG 1559+533 26 300 5.2 14.392 −0.193∗ 1660 ± 610 83.0 +46.5 1200 ± 460
PG 1613+467 25 000 5.3 14.58 −0.102∗ 1560 ± 590 73.0 +45.8 1110 ± 420
PG 1619+522 31 000 5.5 13.297 0.004 790 ± 300 80.5 +44.0 550 ± 210
PG 1644+403 31 000 5.6 15.40 0.179 1720 ± 650 64.1 +40.4 1110 ± 420
PG 1645+610 26 200 5.3 14.507 0.343 1360 ± 520 90.9 +38.6 850 ± 320
PG 1648+536 30 100 5.3 14.055 0.180 1300 ± 490 81.4 +39.4 830 ± 310
PG 1656+600 25 000 5.3 15.82 0.000 2750 ± 1030 89.3 +37.5 1680 ± 630
PG 1710+490 28 300 5.3 12.900 0.075 770 ± 290 75.4 +36.1 450 ± 170
PG 1716+426 25 200 5.3 13.967 −0.002∗ 1170 ± 440 67.7 +34.6 660 ± 250
PG 1743+477 25 900 5.5 13.787 0.088 840 ± 310 74.4 +30.7 430 ± 160
PG 2204+035 29 800 5.4 14.245 0.200 1240 ± 470 64.4 −39.8 800 ± 310
PG 2314+076 25 700 5.1 13.758 0.238 1250 ± 480 86.5 −48.3 940 ± 350
PG 2331+038 26 900 5.5 14.929 0.384 1290 ± 490 89.1 −53.6 1040 ± 390
PG 2337+070 27 000 5.2 13.47 0.486 880 ± 330 93.8 −51.4 690 ± 250
PG 2349+002 24 700 5.2 13.268 0.149 860 ± 340 93.1 −58.9 740 ± 290
PG 2358+107 25 500 5.3 13.624 0.260 900 ± 340 103.5 −50.0 690 ± 260

Notes.

(a)

Heber & Langhans (1986) derived Teff = 26 900 K , log g = 5.5, and AV = 0.016.

(b)

Lamontagne et al. (1987) derived Teff = 21 800 K, log g = 5.0, and AV = 0.192.

(∗)

A negative extinction resulted from colour (b−y) respectively (B−V) that were bluer than predicted from the model atmospheres. For the determinations of the stars’ distance they were set equal to 0.000.

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