2006A&A...458..609D


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.19CET07:33:04

2006A&A...458..609D - Astronomy and Astrophysics, volume 458, 609-623 (2006/11-1)

Basic physical parameters of a selected sample of evolved stars.

DA SILVA L., GIRARDI L., PASQUINI L., SETIAWAN J., VON DER LUEHE O., DE MEDEIROS J.R., HATZES A., DOELLINGER M.P. and WEISS A.

Abstract (from CDS):

We present the detailed spectroscopic analysis of 72 evolved stars, which were previously studied for accurate radial velocity variations. Using one Hyades giant and another well studied star as the reference abundance, we determine the [Fe/H] for the whole sample. These metallicities, together with the Teff values and the absolute V-band magnitude derived from Hipparcos parallaxes, are used to estimate basic stellar parameters (ages, masses, radii, (B-V)0 and logg) using theoretical isochrones and a Bayesian estimation method. The (B-V)0 values so estimated turn out to be in excellent agreement (to within ∼0.05mag) with the observed (B-V), confirming the reliability of the Teff-(B-V)0 relation used in the isochrones. On the other hand, the estimated logg values are typically 0.2dex lower than those derived from spectroscopy; this effect has a negligible impact on [Fe/H] determinations. The estimated diameters θ have been compared with limb darkening-corrected ones measured with independent methods, finding an agreement better than 0.3mas within the 1<θ<10mas interval (or, alternatively, finding mean differences of just 6%). We derive the age-metallicity relation for the solar neighborhood; for the first time to our knowledge, such a relation has been derived from observations of field giants rather than from open clusters and field dwarfs and subdwarfs. The age-metallicity relation is characterized by close-to-solar metallicities for stars younger than ∼4Gyr, and by a large [Fe/H] spread with a trend towards lower metallicities for higher ages. In disagreement with other studies, we find that the [Fe/H] dispersion of young stars (less than 1Gyr) is comparable to the observational errors, indicating that stars in the solar neighbourhood are formed from interstellar matter of quite homogeneous chemical composition. The three giants of our sample which have been proposed to host planets are not metal rich; this result is at odds with those for main sequence stars. However, two of these stars have masses much larger than a solar mass so we may be sampling a different stellar population from most radial velocity searches for extrasolar planets. We also confirm the previous indication that the radial velocity variability tends to increase along the RGB, and in particular with the stellar radius.

Abstract Copyright:

Journal keyword(s): stars: fundamental parameters - stars: evolution - stars: oscillations - Hertzsprung-Russell (HR) and C-M diagrams - stars: late-type - stars: luminosity function, mass function

Simbad objects: 78

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Number of rows : 78

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * 44 Psc ** 00 25 24.2083431267 +01 56 22.892599678   6.616 5.770     G8III 59 0
2 * bet Hyi PM* 00 25 45.07036 -77 15 15.2860 3.52 3.41 2.79 2.28 1.94 G0V 530 0
3 * 39 Cet RS* 01 16 36.2882494986 -02 30 01.329588503   6.310 5.428     G6III:eFe-2 242 0
4 * eta02 Hyi PM* 01 54 56.1320498641 -67 38 50.294625663   5.623 4.685     G8IIIb 89 1
5 * pi. For PM* 02 01 14.7226685359 -30 00 06.585108110   6.23 5.35     G8III 56 0
6 HD 13189 * 02 09 40.1721335781 +32 18 59.160743793   9.04 7.56     K1II-III 66 1
7 * lam02 For PM* 02 36 58.6079324808 -34 34 40.713450652 6.67 6.45 5.79     G1V 174 1
8 * eta Eri PM* 02 56 25.6494839 -08 53 53.322099 5.97 4.99 3.87 3.08 2.50 K1+IIIb 176 0
9 * eps For PM* 03 01 37.6304831834 -28 05 29.376723799   6.68 5.85     G9:V 155 0
10 HD 18885 * 03 01 56.1189723705 -09 57 41.050973426   6.939 5.837     K1III 37 0
11 * omi Tau SB* 03 24 48.7914590778 +09 01 43.994132248 5.090 4.490 3.600 2.92 2.47 G6III 213 0
12 * y Eri * 03 37 05.6791528245 -40 16 28.740766703 6.39 5.62 4.58 3.74 3.17 K1III 51 0
13 * h Eri HB* 03 42 50.0552747 -37 18 48.659746   5.783 4.583     K1.5IIIbCN0.5 54 0
14 * rho For RG* 03 47 56.0407172208 -30 10 04.380679097   6.52 5.54     G6III 52 0
15 * alf Ret PM* 04 14 25.4841381 -62 28 25.891671 4.90 4.27 3.36 2.71 2.27 G8IIIa: 105 0
16 HD 26923 BY* 04 15 28.8004956278 +06 11 12.699896698 6.910 6.860   5.9   G0IV 180 0
17 HD 27130 EB* 04 17 38.9458416476 +16 56 52.210019080   9.075 8.315 8.79   G8V 223 0
18 * 51 Tau SB* 04 18 23.2088106790 +21 34 45.202215421   5.945 5.631     F0V 245 0
19 * gam Tau ** 04 19 47.6038491 +15 37 39.515422 5.46 4.64 3.65 4.83   G9.5IIIabCN0.5 507 0
20 * del Tau SB* 04 22 56.1010361735 +17 32 33.055967140 5.56 4.74 3.76 5.56   G9.5IIICN0.5 488 0
21 * tet02 Tau dS* 04 28 39.7445471109 +15 52 15.122606898 3.690 3.600 3.410 5.43   A7III 414 0
22 * eps Lep PM* 05 05 27.6653698 -22 22 15.723893 6.41 4.64 3.18 2.08 1.27 K4III 140 0
23 * omi Col PM* 05 17 29.0892938 -34 53 42.744408 6.62 5.83 4.83 4.09 3.54 K1IV 76 0
24 * lam Dor * 05 26 19.2666877189 -58 54 45.067948687   6.107 5.129     G8III 35 0
25 HD 36848 * 05 32 51.4129167133 -38 30 48.119001540   6.687 5.456     K2/3III 26 0
26 * nu.02 CMa PM* 06 36 41.0375756 -19 15 21.165905 5.96 5.011 3.91 3.13 2.61 K1.5III-IVFe1 236 1
27 HD 47536 PM* 06 37 47.6183014773 -32 20 23.033515609   6.43 5.258     K1III 90 1
28 * tet CMa PM* 06 54 11.3997692336 -12 02 19.061054441 7.20 5.51 4.08 2.95 2.17 K3/4III 207 0
29 * alf Mon PM* 07 41 14.8325688 -09 33 04.071083 5.83 4.95 3.93 3.16 2.64 G9.5III-IIIbFe-0.5 181 0
30 HD 62644 PM* 07 42 57.0929163265 -45 10 23.216409952   5.84 5.04     G8IV-V 105 0
31 HD 62902 PM* 07 46 02.1908054187 -06 46 21.047597872   6.888 5.496     K5III 40 0
32 * 6 Pup PM* 07 49 41.2012025731 -17 13 42.264757552   6.462 5.162     K3III 49 0
33 * 27 Mon PM* 07 59 44.1536824502 -03 40 46.501791759   6.137 4.934     K1III 76 0
34 HD 70982 * 08 21 07.6386877458 -64 06 21.606792612   7.043 6.108     G6/8III 19 0
35 HD 72650 * 08 31 29.5864691525 -54 23 38.433461521   7.641 6.333     K3III 18 0
36 NGC 2632 OpC 08 40 24 +19 40.0           ~ 1182 0
37 NGC 2682 OpC 08 51 18 +11 48.0           ~ 1990 0
38 HD 76376 * 08 55 12.4299733226 -18 14 28.285942389   7.084 5.741     K2/3III 34 0
39 * alf Hya * 09 27 35.24270 -08 39 30.9583 5.14 3.42 1.97 0.93 0.16 K3IIIa 401 0
40 HD 83441 * 09 37 28.4007675693 -36 05 45.574607306   7.083 5.950     K2III 16 0
41 HD 85035 * 09 48 47.0377594932 -19 18 48.903264248   8.10 7.02     K1III 14 0
42 HD 90957 PM* 10 29 28.9734162313 -29 39 49.793640391   6.992 5.565     K3III 28 0
43 * 33 Sex PM* 10 41 24.1859207379 -01 44 29.366215211   7.145 6.250     G9IV 148 0
44 * m Leo PM* 10 46 24.5460025885 +18 53 29.475859361   6.640 5.492     K3III 59 0
45 HD 93773 PM* 10 48 41.4695007850 -47 44 59.624863586   7.46 6.50     G8III 14 0
46 * eps Crt * 11 24 36.5904786153 -10 51 33.557849078   6.338 4.802     K4III 83 0
47 HD 101321 PM* 11 39 30.1652007688 -13 11 03.722636129   7.81 6.80     K0III 14 0
48 * eps Cru PM* 12 21 21.6093625 -60 24 04.129070   5.01 3.59     K3III 81 0
49 * chi Vir ** 12 39 14.7669232892 -07 59 44.041075962   5.886 4.643 6.45   K2+IIICN0.5 131 1
50 HD 111884 PM* 12 53 04.1639829235 -54 57 08.902700447   7.217 5.908     K2III 21 0
51 * eps Vir PM* 13 02 10.5978496 +10 57 32.941443 4.45 3.71 2.79 2.16 1.71 G8III-IIIb 510 0
52 HD 115478 * 13 17 15.6282353768 +13 40 32.700484933 8.130 6.630 5.330     K3III 65 0
53 HD 122430 * 14 02 22.7817289987 -27 25 47.199212657   6.799 5.469     K2/3III 37 1
54 * 20 Boo PM* 14 19 45.2350539949 +16 18 24.995504868       4.1   K3III 143 0
55 * del Oct PM* 14 26 55.2324425 -83 40 04.386830   5.615 4.304     K2III 36 0
56 HD 131109 PM* 14 57 52.9827420078 -76 39 45.562563855   6.811 5.359     K4III: 26 0
57 HD 136014 PM* 15 19 31.7205806277 -37 05 49.772625381   7.142 6.178     G8III/IV 26 0
58 HD 148760 * 16 31 22.8477059946 -26 32 15.518404431   7.169 6.081     K1III 33 0
59 * eta Ara * 16 49 47.1565275 -59 02 28.957499   5.306 3.744     K5III 60 0
60 * zet02 Sco PM* 16 54 35.0043467 -42 21 40.740679   4.99 3.62     K3III 66 0
61 * eps01 Ara * 16 59 35.0487987 -53 09 37.571300   5.489 4.050     K3III 45 0
62 HD 159194 * 17 35 06.2775008685 -38 47 58.095898115   7.99 6.76     K3III 10 0
63 * 71 Oph * 18 07 18.3588843509 +08 44 01.918091638   5.592 4.640     G8III 161 0
64 HD 169370 RG* 18 24 42.1275107629 -07 04 33.359158917   7.447 6.296     K0/1III 21 0
65 * kap Tel PM* 18 52 39.6443585621 -52 06 26.542660007   6.138 5.173     G8/K0III 27 0
66 * eta Sct PM* 18 57 03.6702664576 -05 50 46.730466051   5.904 4.818     K1-III 91 0
67 HD 177389 PM* 19 09 52.8681650178 -68 25 28.021373885   6.205 5.305     K0IV 25 0
68 HD 179799 PM* 19 14 16.0186701874 -08 43 08.675830464   7.53 6.54     K4III 21 0
69 HD 187195 * 19 49 02.2035774449 -10 52 14.777785948 8.64 7.28 6.04     K2III 34 0
70 * gam Sge PM* 19 58 45.4286265 +19 29 31.728079 6.97 5.04 3.47 2.27 1.35 M0-III 239 0
71 * eta Sge PM* 20 05 09.4931440591 +19 59 27.856193232   6.139 5.093     K2III 78 0
72 * alf Mic * 20 49 58.0767496899 -33 46 46.997429373   5.879 4.890     G8III 32 0
73 HD 198431 PM* 20 50 41.7766331839 -12 32 41.654232090   6.948 5.872     K1III 26 0
74 * 18 Del PM* 20 58 25.9336470966 +10 50 21.426095258   6.432 5.506     G6III 73 1
75 * 3 Psc * 23 00 37.9071898242 +00 11 09.133877584   7.109 6.224     G8/K0III 26 0
76 * 5 Psc PM* 23 08 40.9095327701 +02 07 40.355833093       4.9   G6IIIb 83 0
77 * gam Psc PM* 23 17 09.9374911 +03 16 56.237975 5.20 4.62 3.70 2.98 2.47 G9III:Fe-2 249 0
78 * 27 Psc ** 23 58 40.3770768 -03 33 21.537918   5.814 4.886     G8III 93 0

    Equat.    Gal    SGal    Ecl

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2019.11.19-07:33:04

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