2010A&A...517A...3C


Query : 2010A&A...517A...3C

2010A&A...517A...3C - Astronomy and Astrophysics, volume 517, A3-3 (2010/7-1)

Characterization of Kepler early-type targets.

CATANZARO G., FRASCA A., MOLENDA-ZAKOWICZ J. and MARILLI E.

Abstract (from CDS):

Stellar pulsation offers a unique opportunity to constrain the intrinsic parameters of stars and unveil their inner structure. The Kepler satellite is collecting an enormous amount of data of unprecedent photometric precision, which will allow us to test theory and obtain a very precise tomography of stellar interiors. We attempt to determine the stars' fundamental parameters (Teff, logg, vsin i, and luminosity) needed for computing asteroseismic models and interpreting Kepler data. We report spectroscopic observations of 23 early-type Kepler asteroseismic targets, 13 other stars in the Kepler field, that had not been selected to be observed. We measured the radial velocity by performing a cross-correlation with template spectra to help us identify non-single stars. Spectral synthesis was performed to derive the stellar parameters of our target stars, and the state-of-the-art LTE atmospheric models were computed. For all the stars of our sample, we derived the radial velocity, Teff, logg, vsini, and luminosities. For 12 stars, we performed a detailed abundance analysis of 20 species, for 16, we could derive only the [Fe/H] ratio. A spectral classification was also performed for 17 stars in the sample. We identify two double-lined spectroscopic binaries, HIP96299 and HIP98551, the former of which is an already known eclipsing binary, and two single-lined spectroscopic binaries, HIP97254 and HIP97724. We also report two suspected spectroscopic binaries, HIP92637 and HIP96762, and the detection of a possible variability in the radial velocity of HIP96277. Two of our program stars are chemically peculiar, namely HIP93941, which we classify as B2He-weak, and HIP96210, which we classify as B6Mn. Finally, we find that HIP93522, HIP93941, HIP93943, HIP96210 and HIP96762, are very slow rotators (vsini<20km/s) which makes them very interesting and promising targets for asteroseismic modeling.

Abstract Copyright:

Journal keyword(s): stars: early-type - stars: abundances - stars: fundamental parameters - binaries: spectroscopic

VizieR on-line data: <Available at CDS (J/A+A/517/A3): table2.dat table3.dat table4.dat sp/*>

Simbad objects: 42

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Number of rows : 42
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 * alf Scl Ro* 00 58 36.3593029 -29 21 26.824714 3.52 4.09 4.27 4.30 4.43 B7IIIp 247 0
2 * del03 Tau a2* 04 25 29.3847186643 +17 55 40.463442784   4.369 4.298 6.18 4.24 A2IV-Vs 396 0
3 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1808 1
4 HD 172084 * 18 36 03.6476914128 +44 28 01.621678368   9.10 9.161     A2 7 0
5 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2615 0
6 BD+48 2768 dS* 18 48 00.0845727432 +48 32 31.990894764   9.49 9.307     A6IV 45 0
7 BD+47 2698 * 18 48 07.3201578408 +47 13 47.912512152   9.67 9.524     A9V 7 0
8 BD+48 2781 Er* 18 52 28.7613807192 +48 24 14.085011988   9.65 9.840     B2.5V 17 0
9 BD+38 3367 * 18 57 31.1868862392 +38 56 21.470941752   9.51 9.410     A2 5 0
10 HD 177484 * 19 02 51.8395913712 +44 55 46.555879008   10.28 10.196     A3V 9 0
11 HD 178565 * 19 07 30.7661973960 +37 07 14.843487216   9.07 9.139     A0 6 0
12 BD+42 3250 HS* 19 07 40.5353192280 +42 18 22.016219580   10.40 10.656     sdB0/1 24 0
13 HD 234806 Pu* 19 07 41.3780290752 +50 57 02.013786288 10.070 9.920 9.700     A5 10 1
14 BD+36 3425 * 19 09 44.7464035440 +37 02 38.594812992   10.12 9.849     A5 5 0
15 HD 180757 Ro* 19 15 51.2232316752 +43 12 08.490086496   9.34 9.29     B8.5V 22 0
16 HD 181143 * 19 17 30.7389910080 +42 16 02.379008820   9.63 9.32     F 7 0
17 HD 181879 * 19 20 34.3706203122 +39 11 04.816418636   9.29 9.27 9.407   A1 8 0
18 BD+48 2880 * 19 20 45.6629193864 +48 46 13.656821052   9.85 9.82     A0 6 0
19 HD 182192 * 19 21 42.0847805712 +41 05 48.159184236   9.08 9.05     A0.5nn: 16 0
20 BD+49 3002 * 19 25 26.9566185624 +49 54 45.426448008   9.47 9.268     A2 9 0
21 HD 234892 * 19 25 31.2329268576 +52 24 08.783951580 9.240 9.200 9.150     A1 9 0
22 BD+52 2452B * 19 31 56.3896800720 +52 59 03.637793904   9.72 9.59     A3 8 1
23 HD 184468 * 19 31 57.6215115816 +52 59 06.863296056   8.91 8.579     A1 9 0
24 BD+41 3394 Ro* 19 33 49.6851728352 +41 28 45.244839072   9.13 9.19     B6 16 0
25 BD+47 2868 dS* 19 34 36.4589021928 +47 50 14.052404112   10.22 9.93     A7III 13 0
26 BD+38 3661 EB* 19 34 46.9048562832 +38 58 58.050283332   9.72 9.28   8.942 kA8hF0mF2.5IIIm: 49 0
27 HD 234941 * 19 35 14.7493679520 +52 33 10.741507992   9.82 9.68     B9 8 0
28 HD 185980 Ro* 19 40 07.7519851296 +39 20 38.265111852   9.19 9.20     B9 15 0
29 HD 234963 * 19 40 15.9906806208 +52 23 22.531897392 9.840 9.720 9.520     A3 8 0
30 HD 186997 Ro* 19 45 56.1997981560 +39 39 55.756911456   9.18 9.06     B9III 15 0
31 HIP 97486 Ro* 19 48 50.8850226192 +46 21 31.783594608   10.06 9.95     A0 6 0
32 BD+43 3377 * 19 50 03.3505734456 +43 44 03.924199968   9.48 9.20     F0 5 0
33 HD 226221 Ro* 19 51 33.6413141232 +39 42 49.809672036   9.108 9.058     A1IV-s 14 0
34 HD 188209 s*b 19 51 59.0687638680 +47 01 38.419078944 4.61 5.55 5.63 5.54 5.64 O9.5Iab 300 0
35 HD 226571 * 19 55 19.4220231240 +40 29 57.449588712   9.161 9.113     B6 12 0
36 HD 189013 gD* 19 55 54.0715569456 +47 05 24.197509500   7.013 6.873     A2 25 0
37 HD 189159 Ro* 19 56 55.3316148504 +44 20 30.679221336   9.27 9.14     B9.5IV-V 20 0
38 HD 189915 * 20 00 28.0405917840 +46 39 56.529508248   9.73 9.57     A2 6 0
39 BD+42 3560 * 20 01 09.6279607824 +42 47 59.492994180   10.47 10.33     A0 5 0
40 V* WW Cyg EB* 20 04 02.7108881088 +41 35 16.462624380   10.163 10.10   9.875 B8k:+G? 110 0
41 HD 215399 * 22 44 09.6542043216 +46 37 06.720722040   9.13 8.72     F1V 24 0
42 * iot Psc PM* 23 39 57.0413764 +05 37 34.647529 4.640 4.620 4.120 3.68 3.37 F7V 599 0

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2022.12.07-05:29:29

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