2023A&A...679A.110G


Query : 2023A&A...679A.110G

2023A&A...679A.110G - Astronomy and Astrophysics, volume 679A110 (2023/11-1)

TITANS metal-poor reference stars II. Red giants and CEMP stars.

GIRIBALDI R.E., VAN ECK S., MERLE T., JORISSEN A., KRYNSKI P., PLANQUART L., VALENTINI M., CHIAPPINI C. and VAN WINCKEL H.

Abstract (from CDS):

Context. Representative samples of F-, G-, K-type stars located outside of the solar neighbourhood have started to become available in spectroscopic surveys. The fraction of metal-poor ([Fe/H] ≲ -0.8 dex) giants becomes increasingly relevant towards greater distances. In metal-poor stars, effective temperatures (Teff) based on local thermodynamic equilibrium (LTE) spectroscopy and on former colour-Teff relations - which are still widely used - have been reported to be inaccurate. It is necessary to recalibrate chemical abundances based on these Teff scales in the multiple available surveys in order to bring them to the same standard scale for their simultaneous use. To this end, a complete sample of standards is required, which until now has been restricted to a few stars with quasi-direct Teff measurements.
Aims. We aim to provide a legacy sample of metal-poor standards with proven accurate atmospheric parameters. We add 47 giants to the TITANS metal-poor reference stars.
Methods. We derived Teff using 3D non-LTE Hα modelling, the accuracy of which was tested against interferometry and with the Infra Red Flux Method (IRFM). We derived surface gravity (log ɡ) by fitting Mg I b triplet lines, and tested their accuracy against asteroseismology. Metallicity was derived using Fe II lines, and we find our results to be identical to the [Fe/H] derived from non-LTE spectral synthesis.
Results. The Teff that we find using 3D non-LTE Hα is equivalent to interferometric and IRFM temperatures within a ±46 K uncertainty. We achieve precision of ∼50 K for 34 stars with spectra with the highest signal-to-noise ratio (S/N). For log ɡ, we achieve a total uncertainty of ±0.15 dex. For [Fe/H], we obtain a total uncertainty of ±0.09 dex. We find that the ionisation equilibrium of Fe lines under LTE is not valid in metal-poor giants. LTE leads to a small but significant metallicity underestimation of ∼0.1 dex when derived from weak Fe I lines, and only provided accurate Teff and log ɡ. This bias totally disappears under non-LTE.

Abstract Copyright: © The Authors 2023

Journal keyword(s): surveys - techniques: spectroscopic - stars: atmospheres - stars: fundamental parameters - stars: Population II - stars: carbon

VizieR on-line data: <Available at CDS (J/A+A/679/A110): table2.dat>

Simbad objects: 52

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Number of rows : 52
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 HD 224959 SB* 00 02 08.0214788256 -02 49 12.232785144   10.6 9.6     CEMP-rs 104 0
2 HD 26 SB* 00 05 22.2071891760 +08 47 16.095353028 9.80 9.29 8.25 7.49 7.03 C-H1.5 179 0
3 HD 2265 V* 00 26 40.8429664632 +34 11 01.864297824   9.10 7.54     M2 16 0
4 HD 2665 PM* 00 30 45.4469338728 +57 03 53.628989292 8.66 8.51 7.72     G5IIIw 188 0
5 HD 3179 PM* 00 34 50.5935786096 -21 52 55.806000384   10.43 9.75 9.37 9.065 F8V 51 0
6 HD 5223 SB* 00 54 13.6098985200 +24 04 01.515842760   9.87 8.47     C-H2IIIb: 126 0
7 CD-30 298 RG* 00 58 43.8709169280 -30 05 57.717373920   11.43 10.83     F6Vwl 66 1
8 BPS CS 22953-0003 Pe* 01 02 15.8723379360 -61 43 45.836012208   14.43 13.75 13.339 12.886 KIIvw 78 0
9 HD 6229 HB* 01 03 36.4558954200 +23 46 06.376430388   9.35 8.58     G5III:Sr 71 0
10 BPS CS 29518-0051 Pe* 01 24 10.0049733024 -28 15 21.115362312 13.567 13.62 13.02 12.594 12.162 ~ 35 0
11 BD-16 251 RG* 01 29 31.1311443552 -16 00 45.495314460 12.527 12.427 11.642 11.189 10.713 CEMP 318 0
12 HD 13359 Pe* 02 10 07.0245081144 -20 45 51.651745596   10.36 9.67     G1/2V 46 0
13 HD 17072 PM* 02 40 40.0947823008 -69 13 58.815073128   7.22 6.59     F9IIIm-2 62 0
14 HE 0239-1340 Pe* 02 41 42.3721546152 -13 28 10.603797240   14.73 13.97 13.566 13.080 CEMP-no 64 0
15 HD 22117 PM* 03 33 28.9160848296 -09 51 15.140873124   10.03 9.46     F6V 6 0
16 BPS CS 22186-0025 Pe* 04 24 32.7982834272 -37 09 02.518136460   14.99 14.24 13.740 13.269 ~ 40 0
17 HE 0507-1653 SB* 05 09 16.5603215496 -16 50 04.688981556   13.633 12.507 12.002 11.579 CEMP-s 26 0
18 HD 45282 Pe* 06 26 40.7720940072 +03 25 29.792391024 8.71 8.69 8.03     Gwl 164 0
19 HD 76396 SB* 08 57 58.9267711584 +51 25 47.661787776   9.96 8.85 8.5   C-H2IV: 69 0
20 HD 105740 PM* 12 10 16.9641290928 +16 22 13.349248932   9.39 8.40     G9III 58 0
21 HD 115444 Pe* 13 16 42.4590842616 +36 22 52.692135420   9.77 8.97 8.3 7.88 G9V 252 0
22 HD 122563 Pe* 14 02 31.8455084952 +09 41 09.944391876 7.47 7.10 6.19 5.37 4.79 G8:III:Fe-5 920 0
23 BD+09 2860 Pe* 14 13 19.7440024872 +08 36 40.040730972   11.39 10.77     ~ 54 0
24 * 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 2417 1
25 BD+09 2870 Pe* 14 16 29.9462349936 +08 27 52.952766408   10.58 9.70     KIIvw 82 0
26 2MASS J14543927+0421380 Pe* 14 54 39.2685981792 +04 21 38.099145888   13.02 12.32 11.849 11.376 ~ 53 0
27 HD 140283 Pe* 15 43 03.0971190219 -10 56 00.595693188 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 985 0
28 * 18 Sco PM* 16 15 37.2702755653 -08 22 09.982125430   6.15 5.50     G2Va 671 0
29 BD+11 2998 HB* 16 30 16.7822155632 +10 59 51.752312592   9.73 9.10     F8 89 0
30 BD+17 3248 HB* 17 28 14.4690179544 +17 30 35.847574776   10.02 9.34     KIIvw 239 0
31 HD 175305 RG* 18 47 06.4416868934 +74 43 31.451436187 8.07 7.93 7.18 6.52 6.03 G5III 239 0
32 HD 174036 PM* 18 50 35.7533178408 -43 22 31.647287316   10.10 9.26     G6/8wF6/8 13 0
33 TYC 6888-1277-1 * 19 25 59.8771921584 -29 20 45.804129036   11.83 11.20     ~ 5 0
34 BPS CS 22891-0209 Pe* 19 42 02.1802427088 -61 03 44.534898612   13.03 12.18     KIIvw 64 0
35 UCAC2 7177623 Pe* 19 42 26.8926894816 -56 58 34.059037980   14.27 13.63     ~ 57 0
36 HD 186478 SB* 19 45 14.1409752672 -17 29 27.071239056   10.116 9.302 8.527 7.961 K2III 166 0
37 BD-18 5550 Pe* 19 58 49.7371417608 -18 12 11.140126164 10.18 10.03 9.35 9.04 8.74 CEMP-no 185 0
38 HD 196944 SB* 20 40 46.0815001992 -06 47 50.604476604   9.01 8.40 8.08   CEMP-rs 117 0
39 BPS CS 22897-0008 Pe* 21 03 11.8565397504 -65 05 08.852220600   14.02 13.33     CEMP-no 80 0
40 CD-62 1346 Pe* 21 06 02.9219229360 -61 33 44.645403600   10.55 9.85 9.56 9.027 CEMP-s 70 0
41 HD 201626 SB* 21 09 59.2755833184 +26 36 55.001033532 9.73 9.26 8.16 7.34 6.82 C-H2IV: 159 0
42 BPS CS 22956-0050 Pe* 21 58 05.8340681280 -65 13 27.160682772   14.95 14.25 13.745 13.211 CEMP-no 42 0
43 BPS BS 17569-0049 Pe* 22 04 58.3605927288 +04 01 32.135832984 14.503 14.263 13.126 13.122 12.259 ~ 40 0
44 BPS CS 22892-0052 Pe* 22 17 01.6558764360 -16 39 27.051026544   14.03 13.20 13.06 12.19 KIIvw 472 0
45 2MASS J22214882+0228448 Pe* 22 21 48.8262598080 +02 28 44.867730936 13.291 13.4 12.74 12.325 12.013 ~ 46 0
46 BPS CS 29491-0053 Pe* 22 36 56.2965716592 -28 31 06.577096368   13.76 12.92 12.380 11.812 ~ 36 0
47 CD-41 15048 Pe* 22 50 14.0199769224 -40 57 42.839116956   10.65 10.2     F8 25 0
48 HD 218857 Pe* 23 11 24.5948299440 -16 15 04.026507912   9.60 9.0     G5/8w(a) 124 0
49 BPS CS 22949-0048 Pe* 23 26 07.4169241824 -05 50 06.903492036   14.48 13.67 13.154 12.639 CEMP-no 38 0
50 HD 221170 Pe* 23 29 28.8087143040 +30 25 57.849303180 9.43 8.74 7.66     CEMP-r 306 0
51 HD 221580 PM* 23 33 40.1543223408 -53 39 29.293955892   9.86 9.21     G8/K1wF 50 0
52 2MASS J23485776-2939228 Pe* 23 48 57.7540034928 -29 39 22.824085392 14.759   14.3   13.512 ~ 38 0

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