2020A&A...642A.182A


Query : 2020A&A...642A.182A

2020A&A...642A.182A - Astronomy and Astrophysics, volume 642A, 182-182 (2020/10-1)

Benchmark stars, benchmark spectrographs. Detailed spectroscopic comparison of ESPRESSO, PEPSI, and HARPS data for Gaia benchmark stars.

ADIBEKYAN V., SOUSA S.G., SANTOS N.C., FIGUEIRA P., ALLENDE PRIETO C., DELGADO MENA E., GONZALEZ HERNANDEZ J.I., DE LAVERNY P., RECIO-BLANCO A., CAMPANTE T.L., TSANTAKI M., HAKOBYAN A.A., OSHAGH M., FARIA J.P., BERGEMANN M., ISRAELIAN G. and BOULET T.

Abstract (from CDS):


Context. Gaia benchmark stars are selected to be calibration stars for different spectroscopic surveys. Very high-quality and homogeneous spectroscopic data for these stars are therefore required. We collected ultrahigh-resolution ESPRESSO spectra for 30 of the 34 Gaia benchmark stars and made them public.
Aims. We quantify the consistency of the results that are obtained with different high- (R∼115000), and ultrahigh- (R∼220000) resolution spectrographs. We also comprehensively studied the effect of using different spectral reduction products of ESPRESSO on the final spectroscopic results.
Methods. We used ultrahigh- and high-resolution spectra obtained with the ESPRESSO, PEPSI, and HARPS spectrographs to measure spectral line characteristics (line depth; line width; and equivalent width, EW) and determined stellar parameters and abundances for a subset of 11 Gaia benchmark stars. We used the ARES code for automatic measurements of the spectral line parameters.
Results. Our measurements reveal that the same individual spectral lines measured from adjacent 2D (spectrum in the wavelength-order space) echelle orders of ESPRESSO spectra differ slightly in line depth and line width. When a long list of spectral lines is considered, the EW measurements based on the 2D and 1D (the final spectral product) ESPRESSO spectra agree very well. The EW spectral line measurements based on the ESPRESSO, PEPSI, and HARPS spectra also agree to within a few percent. However, we note that the lines appear deeper in the ESPRESSO spectra than in PEPSI and HARPS. The stellar parameters derived from each spectrograph by combining the several available spectra agree well overall.
Conclusions. We conclude that the ESPRESSO, PEPSI, and HARPS spectrographs can deliver spectroscopic results that are sufficiently consistent for most of the science cases in stellar spectroscopy. However, we found small but important differences in the performance of the three spectrographs that can be crucial for specific science cases.

Abstract Copyright: © ESO 2020

Journal keyword(s): stars: fundamental parameters - techniques: spectroscopic - stars: abundances - instrumentation: spectrographs

Simbad objects: 29

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Number of rows : 29
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 * bet Hyi PM* 00 25 45.07036 -77 15 15.2860 3.52 3.41 2.79 2.28 1.94 G0V 576 0
2 * tau Cet PM* 01 44 04.0831371922 -15 56 14.927607677 4.43 4.22 3.50 2.88 2.41 G8V 1184 1
3 * psi Phe LP* 01 53 38.7410337 -46 18 09.604795 7.71 6.00 4.41 2.68 1.17 M4III 102 0
4 * eps For PM* 03 01 37.6288785045 -28 05 29.373792325   6.68 5.85     G9:V 176 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 450 0
6 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 1822 1
7 HD 22879 Pe* 03 40 22.0652879951 -03 13 01.124265616 7.146 7.222 6.667 6.346 6.016 G0VmF2 469 0
8 * del Eri * 03 43 14.9005379551 -09 45 48.210955899 5.13 4.46 3.54 2.82 2.32 K0+IV 575 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 1221 1
10 HD 49933 PM* 06 50 49.8309774552 -00 32 27.167495244   6.147 5.771 7.04   F3V 361 2
11 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1828 0
12 * bet Gem PM* 07 45 18.94987 +28 01 34.3160 3.00 2.14 1.14 0.39 -0.11 K0IIIb 1079 1
13 HD 84937 PM* 09 48 56.0992891997 +13 44 39.326709913 8.49 8.68 8.32 7.97 7.70 F8Vm-5 757 0
14 * mu. Leo PM* 09 52 45.8165435 +26 00 25.031882 6.50 5.10 3.88 2.97 2.39 K2IIIbCN1Ca1 428 0
15 * ksi Hya ** 11 33 00.1150559 -31 51 27.443449 5.17 4.47 3.54 2.84 2.36 G7IIIb 247 0
16 * bet Vir PM* 11 50 41.7185158616 +01 45 53.001539131 4.26 4.15 3.60 3.13 2.85 F9V 895 0
17 * c Vir RG* 12 20 20.9813922197 +03 18 45.255217001 7.27 6.12 4.96 4.07 3.46 K0.5IIIbFe-0.5 353 0
18 * eps Vir PM* 13 02 10.5978496 +10 57 32.941443 4.45 3.71 2.79 2.16 1.71 G8III-IIIb 537 0
19 * eta Boo SB* 13 54 41.07892 +18 23 51.7946 3.440 3.250 2.680 2.24 1.95 G0IV 682 1
20 HD 122563 Pe* 14 02 31.8455084952 +09 41 09.944391876 7.47 7.10 6.19 5.37 4.79 G8:III:Fe-5 804 0
21 * 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 2234 0
22 * alf Cen B PM* 14 39 35.06311 -60 50 15.0992 2.89 2.21 1.33     K1V 972 1
23 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1217 0
24 HD 140283 Pe* 15 43 03.0971190219 -10 56 00.595693188 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 897 0
25 * 18 Sco PM* 16 15 37.2702755653 -08 22 09.982125430   6.15 5.50     G2Va 549 0
26 * bet Ara * 17 25 17.9878053183 -55 31 47.574076000 5.87 4.31 2.85     K0/1Ib 120 0
27 * mu. Ara PM* 17 44 08.7031414872 -51 50 02.591603160   5.85 5.15     G3IV-V 501 2
28 * gam Sge PM* 19 58 45.4286265 +19 29 31.728079 6.97 5.04 3.47 2.27 1.35 M0-III 253 0
29 * 7 Psc PM* 23 20 20.5830465120 +05 22 52.708387620   6.262 5.069     K1IV 115 0

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2022.10.07-04:03:38

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