2020A&A...639A.127C


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.28CET06:46:09

2020A&A...639A.127C - Astronomy and Astrophysics, volume 639A, 127-127 (2020/7-1)

The Gaia-ESO survey: the non-universality of the age-chemical-clocks-metallicity relations in the Galactic disc.

CASALI G., SPINA L., MAGRINI L., KARAKAS A.I., KOBAYASHI C., CASEY A.R., FELTZING S., VAN DER SWAELMEN M., TSANTAKI M., JOFRE P., BRAGAGLIA A., FEUILLET D., BENSBY T., BIAZZO K., GONNEAU A., TAUTVAISIENE G., BARATELLA M., ROCCATAGLIATA V., PANCINO E., SOUSA S., ADIBEKYAN V., MARTELL S., BAYO A., JACKSON R.J., JEFFRIES R.D., GILMORE G., RANDICH S., ALFARO E., KOPOSOV S.E., KORN A.J., RECIO-BLANCO A., SMILJANIC R., FRANCIOSINI E., HOURIHANE A., MONACO L., MORBIDELLI L., SACCO G., WORLEY C. and ZAGGIA S.

Abstract (from CDS):


Context. In the era of large spectroscopic surveys, massive databases of high-quality spectra coupled with the products of the Gaia satellite provide tools to outline a new picture of our Galaxy. In this framework, an important piece of information is provided by our ability to infer stellar ages, and consequently to sketch a Galactic timeline.
Aims. We aim to provide empirical relations between stellar ages and abundance ratios for a sample of stars with very similar stellar parameters to those of the Sun, namely the so-called solar-like stars. We investigate the dependence on metallicity, and we apply our relations to independent samples, that is, the Gaia-ESO samples of open clusters and of field stars.
Methods. We analyse high-resolution and high-signal-to-noise-ratio HARPS spectra of a sample of solar-like stars to obtain precise determinations of their atmospheric parameters and abundances for 25 elements and/or ions belonging to the main nucleosynthesis channels through differential spectral analysis, and of their ages through isochrone fitting.
Results. We investigate the relations between stellar ages and several abundance ratios. For the abundance ratios with a steeper dependence on age, we perform multivariate linear regressions, in which we include the dependence on metallicity, [Fe/H]. We apply our best relations to a sample of open clusters located from the inner to the outer regions of the Galactic disc. Using our relations, we are able to recover the literature ages only for clusters located at RGC>7kpc. The values that we obtain for the ages of the inner-disc clusters are much greater than the literature ones. In these clusters, the content of neutron capture elements, such as Y and Zr, is indeed lower than expected from chemical evolution models, and consequently their [Y/Mg] and [Y/Al] are lower than in clusters of the same age located in the solar neighbourhood. With our chemical evolution model and a set of empirical yields, we suggest that a strong dependence on the star formation history and metallicity-dependent stellar yields of s-process elements can substantially modify the slope of the [s/α]-[Fe/H]-age relation in different regions of the Galaxy.
Conclusions. Our results point towards a non-universal relation [s/α]-[Fe/H]-age, indicating the existence of relations with different slopes and intercepts at different Galactocentric distances or for different star formation histories. Therefore, relations between ages and abundance ratios obtained from samples of stars located in a limited region of the Galaxy cannot be translated into general relations valid for the whole disc. A better understanding of the s-process at high metallicity is necessary to fully understand the origin of these variations.

Abstract Copyright: © ESO 2020

Journal keyword(s): stars: abundances - Galaxy: abundances - Galaxy: disk - Galaxy: evolution - open clusters and associations: general

VizieR on-line data: <Available at CDS (J/A+A/639/A127): table2.dat table3.dat table1.dat>

Status at CDS : Tables of objects will be appraised for possible ingestion in SIMBAD.

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 - 2020
#notes
1 * 9 Cet BY* 00 22 51.7883318927 -12 12 33.972374893 7.29 7.05 6.39     G2.5V 454 0
2 HD 6434 PM* 01 04 40.1503743342 -39 29 17.585568452   8.32 7.71     G2/3V 207 1
3 HD 11505 PM* 01 53 06.1989698822 -01 19 36.988964012   8.05 7.42     G5V 97 0
4 * 66 Cet B PM* 02 12 46.6412523732 -02 23 46.792715544   8.42 7.74     G1V 73 0
5 HD 26756 PM* 04 14 25.6502208510 +14 37 30.119616339   9.125 8.419 8.039 7.682 G5V 184 0
6 HD 28701 PM* 04 25 45.8487808862 -69 59 37.263812500   8.48 7.87     G2V 66 0
7 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2696 0
8 * 58 Eri BY* 04 47 36.2917607568 -16 56 04.041927355   6.14 5.50     G2.5IV-V 388 0
9 NGC 2243 OpC 06 29 34 -31 17.0   10.12 9.4     ~ 216 0
10 HD 49983 PM* 06 49 45.6355683297 -29 33 21.472926431   10.65 9.99     G3V 10 0
11 Cl Berkeley 31 OpC 06 57 36 +08 16.0           ~ 96 0
12 Cl Berkeley 36 OpC 07 16 23 -13 11.8           ~ 19 0
13 Cl Melotte 71 OpC 07 37 34 -12 03.3   7.44 7.1     ~ 95 0
14 NGC 2420 OpC 07 38 23 +21 34.4   9.0 8.3     ~ 405 0
15 V* V401 Hya BY* 08 37 50.2937802584 -06 48 24.777904953 7.577 7.394 6.725 6.365 6.029 G8/K0(IV) 140 0
16 IC 2391 OpC 08 40 32 -53 02.0           ~ 723 0
17 NGC 2682 OpC 08 51 18 +11 48.0           ~ 2055 0
18 HD 89124 * 10 13 46.8660354576 -71 34 36.548578367   9.66 8.97     G5V 21 0
19 Cl Trumpler 20 OpC 12 39 45 -60 38.1     10.1     ~ 76 0
20 NGC 4815 OpC 12 58 01 -64 57.6   9.61 8.6     ~ 73 0
21 HD 114174 ** 13 08 51.0231461021 +05 12 26.064930541   7.47   6.3   G3IV+D 144 0
22 HD 114853 PM* 13 13 52.2256855782 -45 11 08.881921063 7.681 7.583 6.940 6.559 6.226 G1.5V 91 0
23 HD 115231 PM* 13 15 36.9677847869 +09 00 57.705796967   9.14   8.0   G9 49 0
24 HD 117126 SB* 13 28 18.7098973401 -00 50 24.697923338   8.08 7.44     G3/5V 79 0
25 Cl Pismis 18 OpC 13 36 56 -62 03.9   10.30 9.7     ~ 37 0
26 * psi Ser PM* 15 44 01.8189306784 +02 30 54.600773948       5.4   G2.5V 185 0
27 NGC 6005 OpC 15 55 59 -57 26.4   11.90 10.7     ~ 36 0
28 Cl Trumpler 23 OpC 16 00 52 -53 32.0     11.2     ~ 29 0
29 NGC 6067 OpC 16 13 11 -54 13.1           ~ 173 0
30 NGC 6259 OpC 17 00 45 -44 39.3   8.85 8.0     ~ 57 0
31 C 1749-295 OpC 17 52 43 -29 33.0           ~ 19 0
32 NGC 6633 OpC 18 27 31.2 +06 34 12           ~ 326 0
33 NGC 6705 OpC 18 51 05 -06 16.2   6.32 5.8     ~ 359 0
34 Cl Berkeley 81 OpC 19 01 37 -00 27.6           ~ 51 0
35 [CWW2013] 97 * 19 17 02.8552985849 -16 05 16.597469832   13.56 12.76 12.67   ~ 5 0
36 Cl Berkeley 44 OpC 19 17 18.0 +19 32 27           ~ 26 0
37 NGC 6802 OpC 19 30 36.0 +20 15 34   10.07 8.8     ~ 79 0
38 HD 184768 PM* 19 36 00.6522387968 +00 05 28.270119217   8.22 7.54 7.1   G5V 78 0
39 HD 207700 PM* 21 54 45.2048277280 -73 26 18.545574824   8.12 7.43     G4V 74 0
40 V* NT Aqr BY* 22 06 05.3019536483 -05 21 29.385255187   8.26 7.58     G5V 79 0
41 HD 220507 PM* 23 24 42.1153597454 -52 42 06.761247344   8.28 7.58     G5V 81 0
42 HD 223238 PM* 23 47 52.4055816312 +04 10 31.716576348   8.33   7.3   G5V 74 0

    Equat.    Gal    SGal    Ecl

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2020.10.28-06:46:09

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