2014A&A...570A.104C


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.16CET03:56:15

2014A&A...570A.104C - Astronomy and Astrophysics, volume 570A, 104-104 (2014/10-1)

Improving the surface brightness-color relation for early-type stars using optical interferometry.

CHALLOUF M., NARDETTO N., MOURARD D., GRACZYK D., AROUI H., CHESNEAU O., DELAA O., PIETRZYNSKI G., GIEREN W., LIGI R., MEILLAND A., PERRAUT K., TALLON-BOSC I., McALISTER H., TEN BRUMMELAAR T., STURMANN J., STURMANN L., TURNER N., FARRINGTON C., VARGAS N. and SCOTT N.

Abstract (from CDS):

The method of distance determination of eclipsing binaries consists in combining the radii of both components determined from spectro-photometric observations with their respective angular diameters derived from the surface brightness-color relation (SBC). However, the largest limitation of the method comes from the uncertainty on the SBC relation: about 2% for late-type stars (or 0.04-magnitude) and more than 10% for early-type stars (or 0.2mag). The aim of this work is to improve the SBC relation for early-type stars in the -1≤V-K≤0 color domain, using optical interferometry. Observations of eight B- and A-type stars were secured with the VEGA/CHARA instrument in the visible. The derived uniform disk angular diameters were converted into limb darkened angular diameters and included in a larger sample of 24 stars, already observed by interferometry, in order to derive a revised empirical relation for O, B, A spectral type stars with a V-K color index ranging from -1 to 0. We also took the opportunity to check the consistency of the SBC relation up to V-K≃4 using 100 additional measurements. We determined the uniform disk angular diameter for the eight following stars: γ Ori, ζ Per, 8 Cyg, ι Her, λ Aql, ζ Peg, γ Lyr, and δ Cyg with V-K color ranging from -0.70 to 0.02 and typical precision of about 1.5%. Using our total sample of 132 stars with V-K colors index ranging from about -1 to 4, we provide a revised SBC relation. For late-type stars (0≤V-K≤4), the results are consistent with previous studies. For early-type stars (-1≤V-K≤0), our new VEGA/CHARA measurements combined with a careful selection of the stars (rejecting stars with environment or stars with a strong variability), allows us to reach an unprecedented precision of about 0.16 magnitude or ≃7% in terms of angular diameter. We derive for the first time a SBC relation for stars between O9 and A3, which provides a new and reliable tool for the distance scale calibration.

Abstract Copyright:

Journal keyword(s): stars: early-type - techniques: interferometric - stars: distances - binaries: eclipsing - methods: observational - stars: atmospheres

Simbad objects: 32

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Number of rows : 32

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 * zet Cas Pu* 00 36 58.2841866 +53 53 48.867311 2.58 3.47 3.66 3.74 3.95 B2IV 417 0
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9141 1
3 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5038 1
4 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5410 1
5 HD 22780 Be* 03 41 07.8568858723 +37 34 48.728888670 5.09 5.50 5.57     B7Vn 88 0
6 * zet Per V* 03 54 07.9224751 +31 53 01.081262 2.19 2.97 2.85 2.71 2.62 B1Ib 810 0
7 HD 34989 *iN 05 21 43.5619157417 +08 25 42.841350828 4.79 5.67 5.80 5.79 5.92 B1V 141 1
8 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14392 1
9 * gam Ori V* 05 25 07.86325 +06 20 58.9318 0.54 1.42 1.64 1.73 1.95 B2V 494 1
10 HD 37320 * 05 38 01.1187375483 +07 32 29.104301700 5.44 5.788 5.852     B8III 41 0
11 * zet Ori ** 05 40 45.52666 -01 56 33.2649   1.59 1.79     O9.7Ib+B0III 324 0
12 * kap Ori s*b 05 47 45.3888404 -09 40 10.577707 0.87 1.88 2.06 2.09 2.27 B0.5Ia 545 0
13 * 134 Tau * 05 49 32.9297423 +12 39 04.758221 4.68 4.811 4.875     B9IV 177 0
14 * gam02 Vel WR* 08 09 31.95013 -47 20 11.7108 0.64 1.58 1.83 1.85 2.00 WC8+O7.5III-V 829 0
15 * alf Vir bC* 13 25 11.57937 -11 09 40.7501 -0.20 0.74 0.97 1.06 1.30 B1V 810 2
16 * del Sco SB* 16 00 20.00528 -22 37 18.1431 1.30 2.20 2.32 2.36 2.49 B0.3IV 684 0
17 * zet Oph Be* 16 37 09.5390545 -10 34 01.529471 1.73 2.58 2.56 2.46 2.50 O9.2IVnn 1710 2
18 * iot Her bC* 17 39 27.8860861 +46 00 22.800110 2.940 3.630 3.800     B3IV 427 1
19 HD 167965 * 18 15 38.7772216860 +42 09 33.643941549 4.98 5.434 5.556     B7IV 59 0
20 * gam Sct * 18 29 11.8538827 -14 33 56.931865   4.739 4.675     A1IV/V 102 0
21 * nu. Lyr * 18 49 52.9175323922 +32 33 03.815606116   5.316 5.226     A3V 61 0
22 * gam Lyr * 18 58 56.6224137 +32 41 22.400295 3.140 3.200 3.250 3.27 3.28 B9III 266 0
23 * lam Aql PM* 19 06 14.9397099975 -04 52 57.231496924 3.07 3.34 3.43 3.46 3.55 B8.5V 206 0
24 HD 178233 PM* 19 06 37.7342976797 +28 37 42.934142277 5.88 5.84 5.55     F0III 56 0
25 * 8 Cyg * 19 31 46.3218386 +34 27 10.687443 3.95 4.60 4.72     B3IV 114 0
26 HD 184875 * 19 34 41.2618545206 +42 24 45.039482154   5.396 5.336     A2V 44 0
27 * iot Aql * 19 36 43.2774420564 -01 17 11.784474592 3.84 4.28 4.36 4.34 4.42 B5III 155 0
28 * 14 Cyg * 19 39 26.4883502571 +42 49 05.781730557 5.10 5.32 5.40     B9III 83 0
29 * del Cyg PM* 19 44 58.4785413 +45 07 50.916066 2.75 2.85 2.87 2.88 2.90 A0IV 277 0
30 * 42 Peg PM* 22 41 27.7207176 +10 49 52.907917 3.10 3.33 3.41 3.43 3.50 B8V 281 0
31 * rho Peg PM* 22 55 13.6670582219 +08 48 58.238700099 4.90 4.90 4.90 4.86 4.88 A1V 111 0
32 NAME Local Group GrG ~ ~           ~ 6701 0

    Equat.    Gal    SGal    Ecl

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2019.12.16-03:56:15

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