2000A&A...364..102K


Query : 2000A&A...364..102K

2000A&A...364..102K - Astronomy and Astrophysics, volume 364, 102-136 (2000/12-1)

A spectroscopic study of field BHB star candidates.

KINMAN T., CASTELLI F., CACCIARI C., BRAGAGLIA A., HARMER D. and VALDES F.

Abstract (from CDS):

New spectroscopic observations are presented for a sample of thirty-one blue horizontal branch (BHB) star candidates that are sufficiently nearby to have reliable proper motions. Comments are given on a further twenty-five stars that have previously been suggested as BHB star candidates but which were not included in our sample. Moderately high-resolution spectra (λ/Δλ≃15000) of twenty five of our program stars were taken with the coude feed spectrograph at Kitt Peak. Twelve of the program stars were also observed with the CAT spectrograph at ESO. Six of these program stars were observed from both hemispheres. IUE low-resolution spectra are available for most of our candidates and were used, in addition to other methods, in the determination of their Teff and reddening. A compilation of the visual photometry for these stars (including new photometry obtained at Kitt Peak) is also given. Abundances were obtained from these spectra using models computed by Castelli with an updated version of the ATLAS9 code (Kurucz, 1993, ATLAS9, CD-ROM No. 13). All thirty one candidates are halo stars. Of these, twenty eight are classified as BHB stars because: (o) [(1)]they lie close to the ZAHB (in a similar position to the BHB stars in globular clusters) in the Teff versus logg plot. For all but one of these stars, far-UV data were available which were consistent with other data (Stroemgren photometry, energy distributions, Hγ profiles) for deriving Teff and logg. (o) [(2)]they have a distribution of vsini (≤40km/s) that is similar to that found for the BHB in globular clusters. Peterson et al. (1995ApJ...453..214P) and Cohen & McCarthy (1997AJ....113.1353C) have shown that the BHB stars in the globular clusters M13 and M92 have a higher vsini (≤ 40km/s) than those in M3 and NGC 288 (≤20km/s). The mean deprojected rotational velocity (<v>) was calculated for both the two globular clusters and the nearby BHB star samples. A comparison of these suggests that both globular cluster vsini types are present in our nearby sample. No obvious trend is seen between vsini and either (B-V)0 or [Fe/H]. (o) [(3)]they have -0.99≥[Fe/H]≥-2.95 (mean [Fe/H] -1.67; dispersion 0.42dex), which is similar to that found for field halo RR Lyrae and red HB stars. These local halo field stars appear (on average) to be more metal-poor than the halo globular clusters. The local sample of red giant stars given by Chiba & Yoshii (1998AJ....115..168C) contains a greater fraction of metal-poor stars than either our halo samples or the halo globular clusters. The stars in our sample that have a Teff that exceeds about 8500K show the HeI (λ 4471) line with a strength that corresponds to the solar helium abundance. (o) [(4)]they show a similar enhancement of the α-elements (<[Mg/Fe]≥+0.43±0.04 and also <[Ti/Fe]≥+0.44±0.02) to that found for other halo field stars of similar metallicity.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: fundamental parameters - stars: horizontal-branch - stars: AGB and post-AGB - stars: white dwarfs - Galaxy: halo

VizieR on-line data: <Available at CDS (J/A+A/364/102): stars.dat table4.dat table5.dat>

Simbad objects: 73

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Number of rows : 73
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20   5.78 4.09     ~ 3723 0
2 HD 2188 * 00 26 12.9640779408 +49 23 21.444833400   8.49 8.41     A0 8 0
3 HD 2309 PM* 00 26 21.9669697440 -68 10 47.052407712   10.26 9.36     K0III 10 0
4 HD 2602 * 00 29 43.3650205104 +17 36 38.805188436   10.01 8.43     K2 5 0
5 HD 2857 HB* 00 31 53.7908406120 -05 15 42.870486708 10.52 10.17 9.98     A2IV 102 0
6 HD 4850 PM* 00 50 00.1733287728 -47 17 31.916444640   9.67 9.64     A0V 20 0
7 NGC 288 GlC 00 52 45.24 -26 34 57.4   10 8.13     ~ 984 0
8 BD+00 145 PM* 00 56 27.0390816312 +01 43 42.749482188   10.74 10.6     AV 20 0
9 NGC 362 GlC 01 03 14.26 -70 50 55.6     6.58     ~ 1012 0
10 HD 8376 HB* 01 23 28.2884815632 +31 47 12.260544648   9.74 9.61     A0 18 0
11 HD 13780 PM* 02 12 51.3680023776 -49 03 17.088564672   9.90 9.83     A1IV 23 0
12 HD 14829 PM* 02 23 09.2476174920 -10 40 39.279956448 10.37 10.31 10.29     sdA0IVHe0 52 0
13 HD 15042 * 02 25 41.4039648792 +10 30 21.755626956   7.66 7.60     B9 19 0
14 V* CS Eri RR* 02 37 05.7588329711 -42 57 48.035460221   9.25 9.03     A2/3(IIw) 70 0
15 HD 31943 PM* 04 57 40.6126428168 -43 01 57.500498820   8.38 8.25     A2IV 28 0
16 HD 252940 HB* 06 11 37.2505420824 +26 27 30.113583840   9.31 9.03     ~ 23 0
17 HD 42999 * 06 14 26.5286315520 +11 48 48.924202716   7.67 7.62     A0 15 0
18 HD 47706 * 06 40 21.2115517776 +08 08 58.107927660   8.13 8.04     A3IV 9 0
19 HD 48567 * 06 44 22.1622212928 +08 19 46.947094572   8.34 8.30     B6/9 10 0
20 HD 49224 * 06 47 30.4367276904 +00 41 34.682733348   8.34 8.29     B3II/III 17 0
21 HD 52057 * 06 58 09.9345075336 -36 16 30.562115448   9.33 9.28     B8IV/V 30 0
22 HD 53042 * 07 02 02.3585966304 -34 47 15.274652676   9.42 9.27     A2IV 4 0
23 HD 57336 * 07 09 30.5119377408 -79 25 55.109368164   7.97 7.81     A0IV 37 0
24 HD 60778 HB* 07 36 11.7736405176 -00 08 15.571268556 9.34 9.20 9.10     A0III/IV 106 0
25 HD 67426 * 08 08 14.4538259304 +08 13 42.188825784   8.51 8.42     A3 8 0
26 HD 67542 * 08 09 35.1826787568 +29 05 35.073431628   7.259 6.465     G0II 22 0
27 HD 74721 HB* 08 45 59.2614567408 +13 15 48.591616392 8.88 8.75 8.72     A0V 144 0
28 HD 78913 HV* 09 06 54.8319003960 -68 29 21.947767800   9.34 9.29     A0V 35 0
29 HD 79566 * 09 14 51.9899279232 -01 35 13.595883972   7.04 6.97     A2/3V 18 0
30 HD 83751 * 09 40 34.1265294864 -01 06 48.545904636   8.68 8.66     A0III/IV 7 0
31 HD 86986 HB* 10 02 29.5667305272 +14 33 25.186874796 8.27 8.11   7.9   A1V 171 0
32 HD 87047 HB* 10 03 12.7491822360 +31 03 19.068708168   9.85 9.74     A0 20 0
33 HD 87112 PM* 10 04 38.7702647088 +57 49 56.106828012   9.68 9.71     A0 20 0
34 HD 93329 HB* 10 46 36.6443174328 +11 11 02.846922036 8.980 8.880 8.800     A0 50 0
35 HD 94509 Be* 10 53 27.2624240616 -58 25 24.524985288   9.28 9.73 9.65   Bp_sh 46 0
36 HD 304325 * 11 28 45.1726806624 -58 23 39.503724108   8.26 8.14     A2 10 0
37 BD+32 2188 * 11 47 00.5017548720 +31 50 08.632636188   10.66 10.65     B8/9V 50 0
38 BD+33 2171 PM* 11 56 13.8354790704 +32 54 10.924220844   10.78   10.6   ~ 38 0
39 HD 106304 PM* 12 13 53.5605552696 -40 52 24.673044432   9.10 9.07     B9V 45 0
40 BD+42 2309 * 12 28 22.1632181880 +41 38 52.416055320   10.80 10.82     A0 42 0
41 HD 109995 HB* 12 38 47.5985869392 +39 18 31.626312732 7.83 7.68   7.6   A0V 219 0
42 BD+25 2602 HB* 13 09 25.5879361200 +24 19 25.102149672   10.14 10.04     A0 34 0
43 HD 117880 PM* 13 33 29.8062159888 -18 30 54.289275660 9.14 9.12 9.06     B9IV/V 99 0
44 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2374 0
45 HD 120401 * 13 50 40.5370268616 -57 59 17.185788060   8.94 8.82     A2IV 13 0
46 HD 123664 * 14 10 10.9205104224 -45 54 49.717218744   7.71 7.63     A1V 16 0
47 HD 128801 HB* 14 38 48.0934141488 +07 54 40.351784616   8.71 8.74     B9 48 0
48 HD 128855 * 14 40 30.8386771776 -40 36 29.071229616   7.41 7.35     A1/2IV 15 0
49 HD 130095 PM* 14 46 51.2128847304 -27 14 53.963045736 8.28 8.20 8.12     B9V 94 0
50 HD 130201 * 14 48 19.9117697808 -45 40 12.123745968   10.15 10.07     A0IV/V 24 0
51 M 5 GlC 15 18 33.22 +02 04 51.7   7.34 5.95     ~ 1872 0
52 HD 139961 PM* 15 42 52.8187022784 -44 56 40.803236664   8.94 8.86     A0V 58 0
53 HD 140194 * 15 43 26.3580908304 -30 32 05.971846668   7.53 7.43     A2V 13 0
54 M 4 GlC 16 23 35.22 -26 31 32.7           ~ 1758 0
55 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2099 0
56 M 92 GlC 17 17 07.39 +43 08 09.4     6.52     ~ 1997 0
57 NGC 6388 GlC 17 36 17.461 -44 44 08.34   7.40       ~ 860 1
58 NGC 6397 GlC 17 40 42.09 -53 40 27.6   7.39 5.17     ~ 1876 1
59 HD 161817 HB* 17 46 40.6293849144 +25 44 56.940630540 7.23 7.13 6.97     sdA2 263 0
60 NGC 6441 GlC 17 50 13.06 -37 03 05.2   9.26 8.00     ~ 828 0
61 HD 167105 HB* 18 11 06.3095613216 +50 47 32.413621164 9.020 8.970 8.950     A0 36 0
62 V* MT Tel RR* 19 02 12.2792561239 -46 39 12.083789084   9.14 8.94     A0w 67 0
63 NGC 6752 GlC 19 10 52.11 -59 59 04.4   6.96 6.28     ~ 1894 0
64 HD 181119 * 19 18 00.8593529040 +31 01 18.710144616   6.780 6.687     A3V 27 0
65 HD 180903 PM* 19 19 16.2900301608 -24 23 10.935574440   9.78 9.55     A1III 19 0
66 NGC 6791 OpC 19 20 53 +37 46.7   10.52 9.5     ~ 956 0
67 HD 185174 * 19 36 34.4822468064 +31 14 09.647127708   8.08 8.01     A3 15 0
68 V* AW Mic RR* 21 19 05.9161670520 -33 55 07.921872120   9.29 9.05     A0(III)w 47 0
69 HD 203563 PM* 21 22 59.9692545264 +02 14 37.293712476   8.24 8.19     A0/1(III) 10 0
70 V* DH Peg RR* 22 15 25.6397704896 +06 49 21.439610112 9.72 9.51 9.25 9.23   kA4hF0.5 179 0
71 HD 212468 * 22 23 34.0457847120 +45 21 00.008237628   8.58 7.5 8.03   G5 9 0
72 HD 213468 * 22 32 17.2394429736 -42 34 48.578116728   10.88 10.78     B9IV 42 0
73 HD 214539 * 22 40 47.9915719680 -67 41 18.830422428   7.250 7.253     B8/9Ib 57 0

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2022.05.29-01:58:52

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