2014A&A...565A.113S


Query : 2014A&A...565A.113S

2014A&A...565A.113S - Astronomy and Astrophysics, volume 565A, 113-113 (2014/5-1)

The Gaia-ESO Survey: processing FLAMES-UVES spectra.

SACCO G.G., MORBIDELLI L., FRANCIOSINI E., MAIORCA E., RANDICH S., MODIGLIANI A., GILMORE G., ASPLUND M., BINNEY J., BONIFACIO P., DREW J., FELTZING S., FERGUSON A., JEFFRIES R., MICELA G., NEGUERUELA I., PRUSTI T., RIX H.-W., VALLENARI A., ALFARO E., ALLENDE PRIETO C., BABUSIAUX C., BENSBY T., BLOMME R., BRAGAGLIA A., FLACCOMIO E., FRANCOIS P., HAMBLY N., IRWIN M., KOPOSOV S., KORN A., LANZAFAME A., PANCINO E., RECIO-BLANCO A., SMILJANIC R., VAN ECK S., WALTON N., BERGEMANN M., COSTADO M.T., DE LAVERNY P., HEITER U., HILL V., HOURIHANE A., JACKSON R., JOFRE P., LEWIS J., LIND K., LARDO C., MAGRINI L., MASSERON T., PRISINZANO L. and WORLEY C.

Abstract (from CDS):

The Gaia-ESO Survey is a large public spectroscopic survey that aims to derive radial velocities and fundamental parameters of about 105 Milky Way stars in the field and in clusters. Observations are carried out with the multi-object optical spectrograph FLAMES, using simultaneously the medium-resolution (R∼20000) GIRAFFE spectrograph and the high-resolution (R∼47000) UVES spectrograph. In this paper we describe the methods and the software used for the data reduction, the derivation of the radial velocities, and the quality control of the FLAMES-UVES spectra. Data reduction has been performed using a workflow specifically developed for this project. This workflow runs the ESO public pipeline optimizing the data reduction for the Gaia-ESO Survey, automatically performs sky subtraction, barycentric correction and normalisation, and calculates radial velocities and a first guess of the rotational velocities. The quality control is performed using the output parameters from the ESO pipeline, by a visual inspection of the spectra and by the analysis of the signal-to-noise ratio of the spectra. Using the observations of the first 18 months, specifically targets observed multiple times at different epochs, stars observed with both GIRAFFE and UVES, and observations of radial velocity standards, we estimated the precision and the accuracy of the radial velocities. The statistical error on the radial velocities is σ∼0.4km/s and is mainly due to uncertainties in the zero point of the wavelength calibration. However, we found a systematic bias with respect to the GIRAFFE spectra (∼0.9km/s) and to the radial velocities of the standard stars (∼0.5km/s) retrieved from the literature. This bias will be corrected in the future data releases, when a common zero point for all the set-ups and instruments used for the survey is be established.

Abstract Copyright:

Journal keyword(s): methods: data analysis - techniques: spectroscopic - techniques: radial velocities - surveys - stars: general

Simbad objects: 25

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Number of rows : 25
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 HD 22879 Pe* 03 40 22.0652879951 -03 13 01.124265616 7.146 7.222 6.667 6.346 6.016 G0VmF2 469 0
2 HD 38459 PM* 05 43 26.4567750528 -47 49 22.711279188   9.37 8.50     K1IV-V 55 0
3 HD 42581 Er* 06 10 34.6149358167 -21 51 52.656352926 10.801 9.607 8.125 7.164 6.121 M1V 436 0
4 HD 46828 PM* 06 35 03.0322312272 -12 36 27.580536864   8.17 7.70     F6V 30 0
5 HD 48381 * 06 41 42.9530764512 -33 28 11.103788640   9.57 8.50     K0IV 25 0
6 HD 49035 PM* 06 42 23.2469339328 -61 13 29.892053388   9.27 8.53     G5/6IV/V 47 0
7 HD 64942 * 07 55 58.2271040472 -09 47 49.935359904   9.00 8.34     G3/5V 57 0
8 HD 79601 PM* 09 13 44.6281491888 -42 18 37.473060456   8.55 8.02     G2V 85 0
9 HD 88725 PM* 10 14 08.3343804089 +03 09 04.671822250 8.34 8.33 7.73 7.24 6.89 G3/5V 185 0
10 BD-09 3070 PM* 10 25 10.8371110693 -10 13 43.290945639 12.834 11.631 10.139 9.161 8.051 M1V 128 0
11 UCAC2 543380 * 11 03 49.3930155192 -77 00 09.966241836   15.200 13.080 12.67 10.38 ~ 6 0
12 GES J11034945-7700101 * 11 03 49.45 -77 00 10.1           ~ 2 0
13 * ksi Hya ** 11 33 00.1150559 -31 51 27.443449 5.17 4.47 3.54 2.84 2.36 G7IIIb 247 0
14 HD 103932 PM* 11 57 56.2063477236 -27 42 25.366588848 9.23 8.114 6.964 6.298 5.758 K4+V 151 0
15 GES J13011600-4101507 * 13 01 16.0089286104 -41 01 50.654563716   13.488 12.946 12.773   ~ 4 0
16 BD+11 2576 PM* 13 29 59.7858994351 +10 22 37.784532575 11.728 10.524 9.029 8.07 7.013 M1.0V 225 0
17 GES J14572655-4056351 * 14 57 26.5548831768 -40 56 35.173961088   15.673 14.934 15.006   ~ 3 0
18 HD 141105 PM* 15 47 24.1458423840 -01 03 48.302515548   8.83 8.04     G8V 27 0
19 2MASS J18280330+0639516 NIR 18 28 03.300 +06 39 51.64           ~ 1 0
20 GES J18280330+0639516 * 18 28 03.3028796688 +06 39 51.659436672           ~ 5 0
21 HD 201219 PM* 21 07 56.5197854640 +07 25 58.594324908       7.6   G5 63 0
22 HD 203021 PM* 21 21 23.5931692896 -51 45 09.420450516   7.40 6.75     G8/K1III+(F/G) 29 0
23 HD 204587 PM* 21 30 02.7560054580 -12 30 36.245166319 11.59 10.36 9.075 8.28 7.586 K7Vk: 111 0
24 HD 207970 PM* 21 53 41.8140417264 -28 40 14.204335188   8.55 7.82     G7V 51 0
25 HD 217357 PM* 23 00 16.1221501260 -22 31 27.649676482 10.494 9.251 7.869 7.014 6.238 K7+Vk 167 0

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2022.10.07-05:47:50

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