2019A&A...629A..62C


Query : 2019A&A...629A..62C

2019A&A...629A..62C - Astronomy and Astrophysics, volume 629A, 62-62 (2019/9-1)

The Gaia-ESO survey: Calibrating a relationship between age and the [C/N] abundance ratio with open clusters.

CASALI G., MAGRINI L., TOGNELLI E., JACKSON R., JEFFRIES R.D., LAGARDE N., TAUTVAISIENE G., MASSERON T., DEGL'INNOCENTI S., PRADA MORONI P.G., KORDOPATIS G., PANCINO E., RANDICH S., FELTZING S., SAHLHOLDT C., SPINA L., FRIEL E., ROCCATAGLIATA V., SANNA N., BRAGAGLIA A., DRAZDAUSKAS A., MIKOLAITIS S., MINKEVICIUTE R., STONKUTE E., CHORNIY Y., BAGDONAS V., JIMENEZ-ESTEBAN F., MARTELL S., VAN DER SWAELMEN M., GILMORE G., VALLENARI A., BENSBY T., KOPOSOV S.E., KORN A., WORLEY C., SMILJANIC R., BERGEMANN M., CARRARO G., DAMIANI F., PRISINZANO L., BONITO R., FRANCIOSINI E., GONNEAU A., HOURIHANE A., JOFRE P., LEWIS J., MORBIDELLI L., SACCO G., SOUSA S.G., ZAGGIA S., LANZAFAME A.C., HEITER U., FRASCA A. and BAYO A.

Abstract (from CDS):


Context. In the era of large high-resolution spectroscopic surveys such as Gaia-ESO and APOGEE, high-quality spectra can contribute to our understanding of the Galactic chemical evolution by providing abundances of elements that belong to the different nucleosynthesis channels, and also by providing constraints to one of the most elusive astrophysical quantities: stellar age.
Aims. Some abundance ratios, such as [C/N], have been proven to be excellent indicators of stellar ages. We aim at providing an empirical relationship between stellar ages and [C/N] using open star clusters, observed by the Gaia-ESO and APOGEE surveys, as calibrators.
Methods. We used stellar parameters and abundances from the Gaia-ESO Survey and APOGEE Survey of the Galactic field and open cluster stars. Ages of star clusters were retrieved from the literature sources and validated using a common set of isochrones. We used the same isochrones to determine for each age and metallicity the surface gravity at which the first dredge-up and red giant branch bump occur. We studied the effect of extra-mixing processes in our sample of giant stars, and we derived the mean [C/N] in evolved stars, including only stars without evidence of extra mixing. By combining the Gaia-ESO and APOGEE samples of open clusters, we derived a linear relationship between [C/N] and (logarithmic) cluster ages.
Results. We apply our relationship to selected giant field stars in the Gaia-ESO and APOGEE surveys. We find an age separation between thin- and thick-disc stars and age trends within their populations, with an increasing age towards lower metallicity populations.
Conclusions. With this empirical relationship, we are able to provide an age estimate for giant stars in which C and N abundances are measured. For giant stars, the isochrone fitting method is indeed less sensitive than for dwarf stars at the turn-off. Our method can therefore be considered as an additional tool to give an independent estimate of the age of giant stars. The uncertainties in their ages is similar to those obtained using isochrone fitting for dwarf stars.

Abstract Copyright: © ESO 2019

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

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 - 2023
#notes
1 [FSR2007] 0494 OpC 00 25 40 +63 45.2           ~ 22 0
2 NGC 188 OpC 00 47 12 +85 14.6           ~ 876 0
3 IC 166 OpC 01 52 23 +61 51.4   13.0 11.7     ~ 81 0
4 Cl Berkeley 66 OpC 03 04 07 +58 43.9           ~ 61 0
5 NGC 1193 OpC 03 05 57 +44 23.0     12.6     ~ 80 0
6 Cl King 5 OpC 03 14 44 +52 41.7           ~ 65 0
7 NGC 1245 OpC 03 14 46 +47 14.1   9.16 8.4     ~ 140 0
8 Cl King 7 OpC 03 59 08 +51 47.1           ~ 56 0
9 NGC 1798 OpC 05 11 39 +47 41.5           ~ 64 0
10 Cl Berkeley 17 OpC 05 20 31 +30 34.4           ~ 159 0
11 Cl Berkeley 71 OpC 05 40 56 +32 16.3           ~ 32 0
12 DSH J0553.8+2649 OpC 05 53 51.9 +26 49 47           ~ 21 0
13 NGC 2158 OpC 06 07 27 +24 05.9           ~ 274 0
14 NGC 2243 OpC 06 29 35 -31 16.9   10.12 9.4     ~ 248 0
15 Cl Trumpler 5 OpC 06 36 30 +09 27.9           ~ 108 0
16 Cl Berkeley 26 OpC 06 50 11 +05 45.3           ~ 14 1
17 Cl Berkeley 31 OpC 06 57 37 +08 17.1           ~ 114 0
18 Cl Berkeley 36 OpC 07 16 25 -13 11.8           ~ 31 0
19 Cl Melotte 71 OpC 07 37 32 -12 03.9   7.44 7.1     ~ 115 0
20 NGC 2420 OpC 07 38 24 +21 34.5   9.0 8.3     ~ 448 0
21 Ass Vel OB 2 As* 08 09 22.478 -47 21 03.46           ~ 254 0
22 NGC 2682 OpC 08 51 23 +11 48.8           ~ 2218 0
23 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1085 1
24 Cl Trumpler 20 OpC 12 39 32 -60 38.2           ~ 96 0
25 NGC 4815 OpC 12 58 00 -64 57.6   9.61 8.6     ~ 85 0
26 Cl Pismis 18 OpC 13 36 54 -62 05.5   10.30 9.7     ~ 49 0
27 NGC 6005 OpC 15 55 49 -57 26.3   11.90 10.7     ~ 51 0
28 Cl Trumpler 23 OpC 16 00 52 -53 32.3     11.2     ~ 41 0
29 NGC 6067 OpC 16 13 12 -54 13.6           ~ 196 0
30 NGC 6259 OpC 17 00 47 -44 40.7   8.85 8.0     ~ 69 0
31 Cl Ruprecht 134 OpC 17 52 44 -29 32.2           ~ 30 0
32 NGC 6705 OpC 18 51 04 -06 16.3   6.32 5.8     ~ 391 0
33 HD 229716 SB* 18 51 10.5982053024 +10 18 05.504942880   10.30 9.05     K0 19 0
34 Cl Berkeley 81 OpC 19 01 41 -00 27.2           ~ 69 0
35 Cl Berkeley 44 OpC 19 17 18.0 +19 32 27           ~ 39 0
36 NGC 6791 OpC 19 20 53 +37 46.7   10.52 9.5     ~ 979 0
37 NGC 6802 OpC 19 30 36.0 +20 15 34   10.07 8.8     ~ 94 0
38 NGC 6811 OpC 19 37 22 +46 22.7   7.47 6.8     ~ 320 0
39 NGC 6819 OpC 19 41 18 +40 11.4   8.21 7.3     ~ 561 0
40 NGC 6866 OpC 20 03 56 +44 09.5   8.04 7.6     ~ 148 0
41 Cl Berkeley 53 OpC 20 55 54 +51 03.6           ~ 28 0
42 NGC 7789 OpC 23 57 20 +56 43.6   7.68 6.7     ~ 492 0

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2022.11.26-10:58:55

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