2020A&A...640A..25K


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.26CET14:54:34

2020A&A...640A..25K - Astronomy and Astrophysics, volume 640A, 25-25 (2020/8-1)

Fundamental stellar parameters of benchmark stars from CHARA interferometry. I. Metal-poor stars.

KAROVICOVA I., WHITE T.R., NORDLANDER T., CASAGRANDE L., IRELAND M., HUBER D. and JOFRE P.

Abstract (from CDS):


Context. Benchmark stars are crucial as validating standards for current as well as future large stellar surveys of the Milky Way. However, the number of suitable metal-poor benchmark stars is currently limited, owing to the difficulty in determining reliable effective temperatures (Teff) in this regime.
Aims. We aim to construct a new set of metal-poor benchmark stars based on reliable interferometric effective temperature determinations and a homogeneous analysis. The aim is to reach a precision of 1% in Teff, as is crucial for sufficiently accurate determinations of the full set of fundamental parameters and abundances for the survey sources.
Methods. We observed ten late-type metal-poor dwarfs and giants: HD 2665, HD 6755, HD 6833, HD 103095, HD 122563, HD 127243, HD 140283, HD 175305, HD 221170, and HD 224930. Only three of them (HD 103095, HD 122563, and HD 140283) have previously been used as benchmark stars. For the observations, we used the high-angular-resolution optical interferometric instrument PAVO at the CHARA array. We modelled angular diameters using 3D limb-darkening models and determined effective temperatures directly from the Stefan-Boltzmann relation, with an iterative procedure to interpolate over tables of bolometric corrections. Surface gravities (log(g)) were estimated from comparisons to Dartmouth stellar evolution model tracks. We collected spectroscopic observations from the ELODIE and FIES spectrographs and estimated metallicities ([Fe/H]) from a 1D non-local thermodynamic equilibrium (NLTE) abundance analysis of unblended lines of neutral and singly ionised iron.
Results. We inferred Teff to better than 1% for five of the stars (HD 103095, HD 122563, HD 127243, HD 140283, and HD 224930). The effective temperatures of the other five stars are reliable to between 2 and 3%; the higher uncertainty on the Teff for those stars is mainly due to their having a larger uncertainty in the bolometric fluxes. We also determined log(g) and [Fe/H] with median uncertainties of 0.03dex and 0.09dex, respectively.
Conclusions. This study presents reliable and homogeneous fundamental stellar parameters for ten metal-poor stars that can be adopted as a new set of benchmarks. The parameters are based on our consistent approach of combining interferometric observations, 3D limb-darkening-modelling and spectroscopic observations. The next paper in this series will extend this approach to dwarfs and giants in the metal-rich regime.

Abstract Copyright: © ESO 2020

Journal keyword(s): standards - techniques: interferometric - surveys

VizieR on-line data: <Available at CDS (J/A+A/640/A25): stars.dat tables.dat>

Simbad objects: 47

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Number of rows : 47

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 * 85 Peg SB* 00 02 10.3411392575 +27 04 54.476788744 6.47 6.42 5.75 5.16 4.73 G5VbFe-2 526 0
2 HD 584 * 00 10 29.6754479323 +57 09 55.711615191   6.634 6.720     B8III 30 0
3 HD 1439 PM* 00 18 38.2577501436 +31 31 02.029366028   5.851 5.875     A0IV 58 0
4 HD 1606 V* 00 20 24.4010747071 +30 56 08.209925665   5.769 5.869     B7V 49 0
5 HD 2665 PM* 00 30 45.4467882867 +57 03 53.626973228 8.66 8.51 7.72     G5IIIw 168 0
6 HD 3519 * 00 38 49.2722389146 +59 49 34.148620723   6.75 6.74     A0 16 0
7 HD 3802 * 00 41 12.7091928272 +52 11 51.589316135   6.80 6.73     A0 6 0
8 HD 6028 * 01 02 18.4621840612 +51 02 05.805940928 6.760 6.610 6.490     A3V 33 0
9 HD 6676 * 01 08 33.4659858425 +58 15 48.422303987   5.744 5.767     B8V 40 0
10 HD 6755 SB* 01 09 43.0595349996 +61 32 50.293373799 8.48 8.40   7.3   G5 227 0
11 HD 6833 * 01 09 52.2649551382 +54 44 20.273398737 8.81 7.91 6.74     K0IIIbFe-2 187 0
12 * f Psc PM* 01 17 47.9567070 +03 36 52.084814   5.210 5.137     A1V 95 0
13 HD 9878 * 01 38 12.6353673856 +62 21 06.419320474   6.686 6.709     B7V 17 0
14 HD 12256 PM* 01 59 45.0715422316 -26 56 20.387696056   10.51 9.70     K1IV 11 0
15 V* CX UMa dS* 11 23 53.3328111259 +37 14 05.385882273   7.18 6.94     F0 31 0
16 HD 103095 PM* 11 52 58.7683801554 +37 43 07.240082865 7.38 7.20 6.45 5.80 5.35 K1V_Fe-1.5 750 1
17 HD 103288 Pu* 11 53 47.5948999254 +33 36 55.033500301   7.297 6.990     F0 27 0
18 HD 103928 PM* 11 58 07.1738223601 +32 16 26.070179245   6.735 6.422     A9V 76 0
19 HD 107053 * 12 18 29.0760410342 +32 44 56.023945208   6.901 6.668     A5V 36 0
20 HD 120448 * 13 49 29.3042689820 +06 20 37.644915844   6.83 6.76     A0 12 0
21 HD 120934 * 13 52 18.4064391938 +12 09 54.496999812   6.138 6.098     A1V 31 0
22 * 10 Boo * 13 58 38.9210098429 +21 41 46.330222532   5.743 5.748     A0Vs 58 0
23 HD 122365 * 14 01 20.4266447039 +08 53 41.622795427   6.058 5.973     A2V 30 0
24 HD 122563 Pe* 14 02 31.8456299772 +09 41 09.942736952 7.47 7.10 6.19 5.37 4.79 G8:III:Fe-5 760 0
25 HD 122866 * 14 02 59.7578621026 +50 58 18.510167854   6.16 6.15     A2V 37 0
26 HD 125349 * 14 17 21.1387685499 +51 18 26.408038511   6.245 6.195     A2IV 31 0
27 * g Boo PM* 14 28 37.8130531842 +49 50 41.461096501   6.44   5.1   G4III-IVFe-1 96 0
28 HD 128184 * 14 34 05.0214146587 +46 47 11.353753050   6.558 6.507     A0 12 0
29 HD 128481 * 14 36 43.6576193399 +12 52 41.237202361   7.05 6.98     A0 10 0
30 HD 128998 * 14 38 15.2218594014 +54 01 24.024858887 5.830 5.830 5.830     A1V 47 0
31 * k Boo PM* 15 05 25.8346425267 +48 09 03.494251617   5.568 5.577     A0Vs 74 0
32 HD 139909 * 15 41 15.9724058287 -13 58 13.139760144   6.91 6.86     B9.5V 19 0
33 V* BP Boo a2* 15 42 50.7608176135 +52 21 39.244410993   5.430 5.482     A0VpSiCr 123 0
34 HD 140283 Pe* 15 43 03.0967798658 -10 56 00.595803430 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 862 0
35 HD 143259 * 15 59 41.2937821016 -07 18 07.414156972   6.70 6.64     B9V 11 0
36 * 19 UMi * 16 10 49.5277376675 +75 52 39.214606251   5.370 5.473     B8V 55 0
37 HD 146214 * 16 15 33.2641792523 -12 40 48.155405221   7.65 7.49     A1V 16 0
38 HD 146929 * 16 17 27.3780447579 +34 16 52.484899666   8.61 8.20     F2IV 12 0
39 HD 157774 * 17 18 57.4966307549 +70 47 16.235835409   7.183 7.129     A0 9 0
40 * 38 Dra PM* 18 16 58.7413362595 +68 44 29.238599129   6.707 6.785     A0 51 0
41 HD 175305 Pe* 18 47 06.4424234462 +74 43 31.448124921 8.07 7.93 7.18 6.52 6.03 G5III 194 0
42 HD 178738 * 18 53 53.8725079427 +82 22 12.090093572 6.880 6.890 6.890     A0 12 0
43 HD 175303 * 18 57 06.4659246865 -47 34 42.856081071   9.62 8.11     K3III 5 0
44 HD 197637 * 20 36 00.6840541580 +79 25 49.376732290 6.050 6.800 6.940     B3 22 0
45 * 67 Peg * 23 24 50.8321730463 +32 23 05.569957514 5.22 5.470 5.548     B9III 63 0
46 HD 221170 Pe* 23 29 28.8087923676 +30 25 57.847432750 9.43 8.74 7.66     G2IV 266 0
47 HD 221491 * 23 32 24.7857464644 +34 57 08.425529850   6.595 6.643     B8V 31 0

    Equat.    Gal    SGal    Ecl

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2020.10.26-14:54:34

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