2020A&A...640A...2S


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.26CET13:22:28

2020A&A...640A...2S - Astronomy and Astrophysics, volume 640A, 2-2 (2020/8-1)

Precise calibration of the dependence of surface brightness-colour relations on colour and class for late-type stars.

SALSI A., NARDETTO N., MOURARD D., CREEVEY O., HUBER D., WHITE T.R., HOCDE V., MORAND F., TALLON-BOSC I., FARRINGTON C.D., CHELLI A. and DUVERT G.

Abstract (from CDS):


Context. Surface brightness-colour relations (SBCRs) are used to derive the stellar angular diameters from photometric observations. They have various astrophysical applications, such as the distance determination of eclipsing binaries or the determination of exoplanet parameters. However, strong discrepancies between the SBCRs still exist in the literature, in particular for early and late-type stars.
Aims. We aim to calibrate new SBCRs as a function of the spectral type and the luminosity class of the stars. Our goal is also to apply homogeneous criteria to the selection of the reference stars and in view of compiling an exhaustive and up-to-date list of interferometric late-type targets.
Methods. We implemented criteria to select measurements in the JMMC Measured Diameters Catalog. We then applied additional criteria on the photometric measurements used to build the SBCRs, together with stellar characteristics diagnostics.
Results. We built SBCRs for F5/K7-II/III, F5/K7-IV/V, M-II/III and M-V stars, with respective rms of σFV=0.0022mag, σFV=0.0044mag, σFV=0.0046mag, and σFV=0.0038mag. This results in a precision on the angular diameter of 1.0%, 2.0%, 2.1%, and 1.7%, respectively. These relations cover a large V-K colour range of magnitude, from 1 to 7.5. Our work demonstrates that SBCRs are significantly dependent on the spectral type and the luminosity class of the star. Through a new set of interferometric measurements, we demonstrate the critical importance of the selection criteria proposed for the calibration of SBCR. Finally, using the Gaia photometry for our samples, we obtained (G-K) SBCRs with a precision on the angular diameter between 1.1% and 2.4%.
Conclusions. By adopting a refined and homogeneous methodology, we show that the spectral type and the class of the star should be considered when applying an SBCR. This is particularly important in the context of PLATO.

Abstract Copyright: © A. Salsi et al. 2020

Journal keyword(s): techniques: interferometric - stars: atmospheres - stars: late-type - stars: fundamental parameters

VizieR on-line data: <Available at CDS (J/A+A/640/A2): dwarfs.dat giants.dat m_dwarfs.dat m_giants.dat>

Errata: erratum vol. 641, art. C3 (2020)

Status at CDS : Tables of objects will be appraised for possible ingestion in SIMBAD.

Simbad objects: 46

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Number of rows : 46

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 HD 360 HB* 00 08 17.5326960386 -08 49 26.804940279   7.014 5.980     K1II 37 0
2 HD 1367 PM* 00 17 47.6987294262 +01 41 19.425461276   7.126 6.176     K0III 36 0
3 HD 236459 * 00 32 58.0268011314 +57 38 40.823336985   9.09 9.03     B8 5 0
4 * 54 Psc PM* 00 39 21.8055114029 +21 15 01.716052732 7.29 6.71 5.88 5.21 4.82 K0.5V 531 1
5 HD 4628 PM* 00 48 22.9763438736 +05 16 50.209562003 7.22 6.64 5.74 4.99 4.52 K2.5V 451 0
6 HD 10142 PM* 01 38 27.4838187196 -36 31 41.701755016   6.991 5.939     K0III 41 0
7 * nu. Psc * 01 41 25.8939097 +05 29 15.406225 7.36 5.81 4.44 3.38 2.67 K3III 225 0
8 HD 11092 * 01 51 16.9242407065 +64 51 17.837737056 10.96 8.66 6.57     K4Ib-IIa 42 0
9 * eta02 Hyi PM* 01 54 56.1320498641 -67 38 50.294625663   5.623 4.685     G8IIIb 92 1
10 * pi. For PM* 02 01 14.7226685359 -30 00 06.585108110   6.23 5.35     G8III 59 0
11 * alf Ari PM* 02 07 10.40570 +23 27 44.7032 4.29 3.17 2.01 1.15 0.54 K2-IIIbCa-1 606 1
12 * 63 Cet HB* 02 11 35.8353394624 -01 49 31.535483058   6.903 5.933     K0III 40 0
13 HD 13686 * 02 15 55.3931311650 +63 14 10.676120231   8.845 7.016     K2.5Ib-II 33 0
14 * 66 Ari ** 03 28 26.5672397544 +22 48 14.432797937 7.670 6.990 6.030     G9IV 47 0
15 HD 23526 PM* 03 46 09.3640043225 +06 48 12.686057175   6.896 5.922     G9III 28 0
16 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14993 1
17 HD 40020 PM* 05 56 49.4500025832 +11 31 15.811538004   7.008 5.884     K2III 49 0
18 * 39 Cnc * 08 40 06.4182331380 +20 00 28.033945888 8.20 7.37 6.39 5.67 5.20 G8+III-IIIb 173 0
19 * rho01 Cnc PM* 08 52 35.8113282132 +28 19 50.956901366 7.45 6.82   5.4   K0IV-V 980 1
20 * ksi Hya ** 11 33 00.1150559 -31 51 27.443449 5.17 4.47 3.54 2.84 2.36 G7IIIb 233 0
21 HD 102328 * 11 46 55.6228714511 +55 37 41.487866598   6.528 5.254     K2.5IIIbCN1 139 0
22 * 66 UMa * 11 55 58.4171879842 +56 35 54.805694004   6.928 5.824     K1III 51 0
23 HD 104985 PM* 12 05 15.1177022665 +76 54 20.638478373       5.2   G8.5IIIb 135 1
24 HD 106574 * 12 15 08.4925341122 +70 12 00.029373523   6.909 5.719     K2III 28 0
25 * gam Com PM* 12 26 56.2720731 +28 16 06.321081 6.64 5.47 4.34 3.53 3.01 K1IIIFe0.5 192 0
26 HD 113049 * 12 58 47.3525269194 +75 28 21.030499091   7.027 5.990     K0III 30 0
27 * eps Vir PM* 13 02 10.5978496 +10 57 32.941443 4.45 3.71 2.79 2.16 1.71 G8III-IIIb 518 0
28 * 41 Com PM* 13 07 10.7300255 +27 37 29.058512 8.14 6.22 4.69 3.64 2.83 K5-III 142 0
29 HD 118904 * 13 37 10.9884718637 +71 14 32.105470389   6.711 5.496     K2III 31 0
30 * ups Boo PM* 13 49 28.6407858 +15 47 52.460283 7.46 5.59 4.07 2.87 2.00 K5.5III 137 0
31 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2148 0
32 * rho Boo PM* 14 31 49.7896173 +30 22 17.178087 6.33 4.89 3.59 2.67 2.02 K3-III 247 0
33 * bet UMi V* 14 50 42.32580 +74 09 19.8142 5.32 3.55 2.08 0.97 0.21 K4-III 304 0
34 * bet Boo Er* 15 01 56.7623786 +40 23 26.040607 5.21 4.47 3.52 2.85 2.37 G8IIIaFe-0.5 242 0
35 * ome Boo * 15 02 06.5086200004 +25 00 29.278223486 8.14 6.31 4.81 3.62 2.83 K4III 102 0
36 * del Boo PM* 15 15 30.1629518 +33 18 53.392558 5.12 4.44 3.49 2.76 2.25 G8IIIFe-1 360 0
37 * 11 UMi * 15 17 05.8915364232 +71 49 26.037470516   6.384 5.015     K4III 103 1
38 HD 140283 Pe* 15 43 03.0967798658 -10 56 00.595803430 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 862 0
39 HD 167042 PM* 18 10 31.6406187667 +54 17 11.593233378   6.89   5.4   K1III 133 1
40 HD 175740 * 18 54 52.1775810576 +41 36 09.793361516 7.400 6.490 5.440     G8III 41 0
41 HD 178208 SB* 19 05 09.8356256323 +49 55 23.329717378 9.400 7.800 6.430     K3III 42 0
42 HD 180756 Er* 19 15 19.1767403711 +50 04 16.037882610 7.850 7.240 6.310 7.18   G8III 27 0
43 HD 181069 Er* 19 17 19.9790805210 +39 07 15.893663565   7.693 6.559     K1III 15 0
44 HD 181597 * 19 18 37.8722185239 +49 34 10.035499564   7.442 6.317     K1III 52 0
45 HD 182896 Er* 19 25 18.1494374784 +37 14 42.716385466   7.93 6.80     K0 12 0
46 HD 185657 SB* 19 37 56.7084506199 +49 17 03.817760030 8.260 7.480 6.460     G6V 62 0

    Equat.    Gal    SGal    Ecl

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2020.10.26-13:22:28

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