2020A&A...640A.123B


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.26CET14:55:15

2020A&A...640A.123B - Astronomy and Astrophysics, volume 640A, 123-123 (2020/8-1)

The GAPS Programme at TNG. XXV. Stellar atmospheric parameters and chemical composition through GIARPS optical and near-infrared spectra.

BARATELLA M., D'ORAZI V., BIAZZO K., DESIDERA S., GRATTON R., BENATTI S., BIGNAMINI A., CARLEO I., CECCONI M., CLAUDI R., COSENTINO R., GHEDINA A., HARUTYUNYAN A., LANZA A.F., MALAVOLTA L., MALDONADO J., MALLONN M., MESSINA S., MICELA G., MOLINARI E., PORETTI E., SCANDARIATO G. and SOZZETTI A.

Abstract (from CDS):


Context. The detailed chemical composition of stars is important in many astrophysical fields, among which is the characterisation of exoplanetary systems. Previous studies seem to indicate an anomalous chemical pattern of the youngest stellar population in the solar vicinity that has sub-solar metal content. This can influence various observational relations linking the properties of exoplanets to the characteristics of the host stars, for example the giant planet-metallicity relation.
Aims.In this framework, we aim to expand our knowledge of the chemical composition of intermediate-age stars and understand whether these peculiarities are real or related to spectroscopic analysis techniques.
Methods. We analysed high-resolution optical and near-infrared spectra of intermediate-age stars (<700Myr) that have been observed simultaneously with HARPS-N and GIANO-B spectrographs in GIARPS mode. To overcome issues related to the young ages of the stars, we applied a new spectroscopic method that uses titanium lines to derive the atmospheric parameters, in particular surface gravities and microturbulence velocity parameter. We derived abundances of CI, NaI, MgI, AlI, SiI, CaI, TiI, TiII, CrI, CrII, FeI, FeII, NiI, and ZnI.
Results. The lack of systematic trends between elemental abundances and effective temperatures validates our methods. However, we observed that the coolest stars in the sample, where Teff<5400K, display higher abundances for the ionised species, in particular CrII, and for high-excitation potential CI lines.
Conclusions. We found a positive correlation between the higher abundances measured of CI and CrII and the activity index logR'HK. Instead, we found no correlations between the C abundances obtained from CH molecular band at 4300Å and both effective temperatures and activity. Thus, we suggest that these are better estimates for C abundances in young and cool stars. Finally, we found an indication of an increasing abundance ratio [X/H] with the condensation temperature for HD 167389, indicating possible episodes of planet engulfment.

Abstract Copyright: © ESO 2020

Journal keyword(s): stars: abundances - stars: fundamental parameters - stars: solar-type

Simbad objects: 17

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Number of rows : 17

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 HD 3765 PM* 00 40 49.2699101367 +40 11 13.819725965   8.30   6.8   K2V 236 0
2 V* V376 And WU* 02 35 11.6317542662 +49 51 37.211957484   8.02 7.77     A4V 44 0
3 NAME lam Ori Complex SFR 05 35 06 +09 56.0           ~ 55 0
4 NAME Ori Complex Cld 05 35.3 -05 23           ~ 341 0
5 HD 59967 PM* 07 30 42.5117283582 -37 20 21.704201159 7.386 7.274 6.635 6.28 5.945 G3V 131 0
6 HD 59747 BY* 07 33 00.5803322465 +37 01 47.450630754   8.58 7.70     G5V 84 0
7 V* V478 Hya BY* 08 22 49.9528448767 +01 51 33.554224835   9.30 8.711   7.999 G1/2V 87 2
8 Arty 132 * 12 21 15.6150569540 +26 09 14.046375861   12.50 11.5 10.87 10.41 K3.5 21 0
9 BD+26 2342 * 12 24 05.7338003307 +26 07 42.922404090   11.26 10.46     ~ 34 0
10 BD+27 2139 * 12 28 56.4263434758 +26 32 57.398105712   11.67 10.8 10.53 10.25 G9IV 24 0
11 NAME Ursa Major Moving Group MGr 12 32 +57.0           ~ 383 2
12 BD+36 2278 * 12 32 31.0727461250 +35 19 52.315506502   10.14 9.7     G0 29 0
13 HD 159222 PM* 17 32 00.9922730198 +34 16 16.130879367 7.38 7.21   6.1   G1V 207 0
14 HD 167389 PM* 18 13 07.2257142711 +41 28 31.311389409   7.96 7.39     F8V: 65 0
15 NAME Lyra reg ~ ~           ~ 49 0
16 NAME Hercules-Lyra Moving Group MGr ~ ~           ~ 54 0
17 NAME Coma Berenices Moving Group MGr ~ ~           ~ 60 0

    Equat.    Gal    SGal    Ecl

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2020.10.26-14:55:15

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