2014A&A...570A.122S


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.20CET19:44:25

2014A&A...570A.122S - Astronomy and Astrophysics, volume 570A, 122-122 (2014/10-1)

The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars.

SMILJANIC R., KORN A.J., BERGEMANN M., FRASCA A., MAGRINI L., MASSERON T., PANCINO E., RUCHTI G., SAN ROMAN I., SBORDONE L., SOUSA S.G., TABERNERO H., TAUTVAISIENE G., VALENTINI M., WEBER M., WORLEY C.C., ADIBEKYAN V.Z., ALLENDE PRIETO C., BARISEVICIUS G., BIAZZO K., BLANCO-CUARESMA S., BONIFACIO P., BRAGAGLIA A., CAFFAU E., CANTAT-GAUDIN T., CHORNIY Y., DE LAVERNY P., DELGADO-MENA E., DONATI P., DUFFAU S., FRANCIOSINI E., FRIEL E., GEISLER D., GONZALEZ HERNANDEZ J.I., GRUYTERS P., GUIGLION G., HANSEN C.J., HEITER U., HILL V., JACOBSON H.R., JOFRE P., JOENSSON H., LANZAFAME A.C., LARDO C., LUDWIG H.-G., MAIORCA E., MIKOLAITIS S., MONTES D., MOREL T., MUCCIARELLI A., MUNOZ C., NORDLANDER T., PASQUINI L., PUZERAS E., RECIO-BLANCO A., RYDE N., SACCO G., SANTOS N.C., SERENELLI A.M., SORDO R., SOUBIRAN C., SPINA L., STEFFEN M., VALLENARI A., VAN ECK S., VILLANOVA S., GILMORE G., RANDICH S., ASPLUND M., BINNEY J., DREW J., FELTZING S., FERGUSON A., JEFFRIES R., MICELA G., NEGUERUELA I., PRUSTI T., RIX H-W., ALFARO E., BABUSIAUX C., BENSBY T., BLOMME R., FLACCOMIO E., FRANCOIS P., IRWIN M., KOPOSOV S., WALTON N., BAYO A., CARRARO G., COSTADO M.T., DAMIANI F., EDVARDSSON B., HOURIHANE A., JACKSON R., LEWIS J., LIND K., MARCONI G., MARTAYAN C., MONACO L., MORBIDELLI L., PRISINZANO L. and ZAGGIA S.

Abstract (from CDS):

The ongoing Gaia-ESO Public Spectroscopic Survey is using FLAMES at the VLT to obtain high-quality medium-resolution Giraffe spectra for about 105 stars and high-resolution UVES spectra for about 5000 stars. With UVES, the Survey has already observed 1447 FGK-type stars. These UVES spectra are analyzed in parallel by several state-of-the-art methodologies. Our aim is to present how these analyses were implemented, to discuss their results, and to describe how a final recommended parameter scale is defined. We also discuss the precision (method-to-method dispersion) and accuracy (biases with respect to the reference values) of the final parameters. These results are part of the Gaia-ESO second internal release and will be part of its first public release of advanced data products. The final parameter scale is tied to the scale defined by the Gaia benchmark stars, a set of stars with fundamental atmospheric parameters. In addition, a set of open and globular clusters is used to evaluate the physical soundness of the results. Each of the implemented methodologies is judged against the benchmark stars to define weights in three different regions of the parameter space. The final recommended results are the weighted medians of those from the individual methods. The recommended results successfully reproduce the atmospheric parameters of the benchmark stars and the expected Teff-logg relation of the calibrating clusters. Atmospheric parameters and abundances have been determined for 1301 FGK-type stars observed with UVES. The median of the method-to-method dispersion of the atmospheric parameters is 55K for Teff, 0.13dex for logg and 0.07dex for [Fe/H]. Systematic biases are estimated to be between 50-100K for Teff, 0.10-0.25dex for logg and 0.05-0.10dex for [Fe/H]. Abundances for 24 elements were derived: C, N, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Mo, Ba, Nd, and Eu. The typical method-to-method dispersion of the abundances varies between 0.10 and 0.20dex. The Gaia-ESO sample of high-resolution spectra of FGK-type stars will be among the largest of its kind analyzed in a homogeneous way. The extensive list of elemental abundances derived in these stars will enable significant advances in the areas of stellar evolution and Milky Way formation and evolution.

Abstract Copyright:

Journal keyword(s): methods: data analysis - surveys - stars: abundances - stars: fundamental parameters - stars: late-type

Simbad objects: 45

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Number of rows : 45

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 NGC 104 GlC 00 24 05.359 -72 04 53.20   5.78 4.09     ~ 3473 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 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1067 1
4 * eps For PM* 03 01 37.6304831834 -28 05 29.376723799   6.68 5.85     G9:V 155 0
5 * alf Cet LP? 03 02 16.77307 +04 05 23.0596 6.10 4.17 2.53 1.18 0.02 M1.5IIIa 437 0
6 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1660 1
7 HD 22879 Pe* 03 40 22.0654223510 -03 13 01.124769689 7.146 7.222 6.667 6.346 6.016 G0VmF2 422 0
8 * del Eri RS* 03 43 14.9008787 -09 45 48.208444 5.13 4.46 3.54 2.82 2.32 K0+IV 535 0
9 * alf Tau LP? 04 35 55.23907 +16 30 33.4885 4.32 2.40 0.86 -0.37 -1.31 K5+III 1168 1
10 NGC 1851 GlC 05 14 06.76 -40 02 47.6   8.80 7.23     ~ 1209 0
11 HD 49933 ** 06 50 49.831 -00 32 27.18           F3V 321 1
12 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1742 0
13 * bet Gem PM* 07 45 18.94987 +28 01 34.3160 3.00 2.14 1.14 0.39 -0.11 K0IIIb 1038 1
14 Cl* NGC 2682 YBP 1194 * 08 51 00.8053336097 +11 48 52.796026050 15.546 15.28 14.676   13.876 G5V 45 1
15 NGC 2682 OpC 08 51 18 +11 48.0           ~ 1990 0
16 IRAS 09110-6439 GlC 09 12 03.10 -64 51 48.6   7.77 5.69     ~ 1204 0
17 HD 84937 PM* 09 48 56.09801 +13 44 39.3237 8.49 8.68 8.32 7.97 7.70 F8Vm-5 708 0
18 * mu. Leo PM* 09 52 45.8165435 +26 00 25.031882 6.50 5.10 3.88 2.97 2.39 K2IIIbCN1Ca1 395 1
19 NGC 3532 OpC 11 05 39 -58 45.2           ~ 262 0
20 * ksi Hya ** 11 33 00.1150559 -31 51 27.443449 5.17 4.47 3.54 2.84 2.36 G7IIIb 229 0
21 * bet Vir PM* 11 50 41.7182390 +01 45 52.991019 4.26 4.15 3.60 3.13 2.85 F9V 845 0
22 * c Vir PM* 12 20 20.9813348 +03 18 45.260365 7.27 6.12 4.96 4.07 3.46 K0.5IIIbFe-0.5 331 0
23 NGC 4372 GlC 12 25 45.43 -72 39 32.7   10.86 9.85     ~ 251 0
24 Cl* Trumpler 20 MG 781 * 12 39 44.7456624627 -60 38 33.927560972 15.728 16.005 14.610   13.283 ~ 8 0
25 Cl Trumpler 20 OpC 12 39 45 -60 38.1     10.1     ~ 68 0
26 NGC 4815 OpC 12 58 01 -64 57.6   9.61 8.6     ~ 66 0
27 NGC 4833 GlC 12 59 33.92 -70 52 35.4   8.72 7.79     ~ 333 0
28 * 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
29 * eta Boo SB* 13 54 41.07892 +18 23 51.7946 3.440 3.250 2.680 2.24 1.95 G0IV 648 1
30 HD 122563 Pe* 14 02 31.8456299772 +09 41 09.942736952 7.47 7.10 6.19 5.37 4.79 G8:III:Fe-5 729 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 2097 0
32 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1110 0
33 NGC 5927 GlC 15 28 00.69 -50 40 22.9   10.13 8.86     ~ 389 0
34 HD 140283 Pe* 15 43 03.0967798658 -10 56 00.595803430 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 845 0
35 * 18 Sco PM* 16 15 37.2703721200 -08 22 09.981989277   6.15 5.50     G2Va 470 0
36 * bet Ara * 17 25 17.9883527 -55 31 47.586765 5.87 4.31 2.85     K0/1Ib 113 0
37 * mu. Ara PM* 17 44 08.7036342277 -51 50 02.591049123   5.85 5.15     G3IV-V 458 2
38 NGC 6705 OpC 18 51 05 -06 16.2   6.32 5.8     ~ 350 0
39 NGC 6752 GlC 19 10 52.11 -59 59 04.4   6.96 6.28     ~ 1766 0
40 * 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
41 * 61 Cyg A BY* 21 06 53.9396100677 +38 44 57.897024357 7.50 6.39 5.21 4.19 3.54 K5V 930 0
42 * 61 Cyg B Fl* 21 06 55.2640651855 +38 44 31.362140913 8.63 7.40 6.03 4.86 3.55 K7V 659 1
43 * tau Cyg B PM* 21 14 47.462719 +38 02 44.14010   7.50 6.57     ~ 16 0
44 M 15 GlC 21 29 58.33 +12 10 01.2   3       ~ 2851 0
45 * 7 Psc PM* 23 20 20.5830620142 +05 22 52.700020565   6.262 5.069     K1IV 105 0

    Equat.    Gal    SGal    Ecl

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2019.11.20-19:44:25

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