2016A&A...585A..75D


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.05CET17:31:47

2016A&A...585A..75D - Astronomy and Astrophysics, volume 585A, 75-75 (2016/1-1)

Consistent metallicity scale for cool dwarfs and giants. A benchmark test using the Hyades.

DUTRA-FERREIRA L., PASQUINI L., SMILJANIC R., PORTO DE MELLO G.F. and STEFFEN M.

Abstract (from CDS):

In several instances chemical abundances of main-sequence and giant stars are used simultaneously under the assumption that they share the same abundance scale. This assumption, if wrong, might have important implications in different astrophysical contexts. It is therefore crucial to understand whether the metallicity or abundance differences among dwarfs and giants are real or are produced by systematic errors in the analysis. We aim to ascertain a methodology capable of producing a consistent metallicity scale for giants and dwarfs. To achieve that, we analyzed giants and dwarfs in the Hyades open cluster, under the assumption that they share the same chemical composition. All the stars in this cluster have archival high-resolution spectroscopic data obtained with HARPS and UVES. In addition, the giants have interferometric measurements of the angular diameters. We analyzed the sample with two methods. The first method constrains the atmospheric parameters independently from spectroscopic method. For that we present a novel calibration of microturbulence based on 3D model atmospheres. The second method is the classical spectroscopic analysis based on Felines. We also tested two different line lists in an attempt to minimize possible non-LTE effects and to optimize the treatment of the giants. We show that it is possible to obtain a consistent metallicity scale between dwarfs and giants. The preferred method should constrain the three parameters Teff, logg, and ξ independent of spectroscopy. A careful selection of Fe lines is also important. In particular, the lines should not be chosen based on the Sun or other dwarfs, but specifically to be free of blends in the spectra of giants. When attention is paid to the line list, the classical spectroscopic method can also produce consistent results. In our test, the metallicities derived with the well-constrained set of stellar parameters are consistent independent of the line list used. Therefore, for this cluster we favor the metallicity of +0.18±0.03dex obtained with this method. The classical spectroscopic analysis, using the line list optimized for the giants, provides a metallicity of +0.14±0.03dex, in agreement with previous works.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: fundamental parameters - stars: late-type - techniques: spectroscopic - Galaxy: evolution - planets and satellites: formation

Simbad objects: 23

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Number of rows : 23

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 V* BZ Cet BY* 03 00 02.8120517172 +07 44 59.117432323 9.635 8.908 7.955 7.436 6.994 K2.5Vk 118 0
2 BD+23 465 PM* 03 32 50.0789017819 +23 41 31.873847085   9.719   8.3   G5 76 0
3 HD 285348 PM* 04 03 39.0408158530 +19 27 18.043699697   11.162 10.095     K2 60 0
4 HD 285367 PM* 04 05 39.6750094705 +17 56 15.762174280   10.190 9.291     K0 63 0
5 HD 25825 PM* 04 06 16.1277831435 +15 41 53.234613641   8.416 7.811 7.484 7.169 G0V 168 0
6 HD 285507 PM* 04 07 01.2254128574 +15 20 06.108426912   11.670 10.473     K4 63 0
7 HD 26756 PM* 04 14 25.6502208510 +14 37 30.119616339   9.125 8.419 8.039 7.682 G5V 185 0
8 HD 26736 BY* 04 14 32.3143718674 +23 34 29.798017740   8.711 8.047 7.691 7.356 G5V 192 0
9 V* V984 Tau BY* 04 16 33.4774691433 +21 54 26.882967639   9.944 9.125     ~ 149 0
10 V* V893 Tau BY* 04 18 57.9744787270 +19 54 24.125770975   9.345 8.597 8.192 7.829 G9V 127 0
11 HD 27282 PM* 04 19 08.0080652475 +17 31 29.118551040 9.46 9.157 8.427 8.034 7.675 G8V 169 0
12 * gam Tau ** 04 19 47.6038491 +15 37 39.515422 5.46 4.64 3.65 4.83   G9.5IIIabCN0.5 520 0
13 * del Tau SB* 04 22 56.1010361735 +17 32 33.055967140 5.56 4.74 3.76 5.56   G9.5IIICN0.5 500 0
14 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2743 0
15 * tet01 Tau SB* 04 28 34.4960341 +15 57 43.849432 5.510 4.780 3.840 5.48   G9IIIFe-0.5 474 0
16 * eps Tau ** 04 28 36.9988174 +19 10 49.544603 5.42 4.54 3.53     G9.5IIICN0.5 552 1
17 HD 28344 BY* 04 28 48.2983169461 +17 17 07.686115512 8.57 8.456 7.837 7.498 7.180 G2V 258 0
18 HD 28635 SB* 04 31 29.3444023836 +13 54 12.322586634   8.300 7.746 7.445 7.147 F9V 129 0
19 HD 30500 * 04 46 31.9269121212 -37 27 21.327085149   9.08 7.59     K3III 7 0
20 HD 30589 PM* 04 49 32.1249664135 +15 53 19.474471734   8.324 7.739 7.412 7.111 F8 111 0
21 HD 30809 PM* 04 51 23.2149187922 +15 26 00.474500594   8.418 7.886 7.591 7.302 F8 80 0
22 IC 4651 OpC 17 24 49 -49 56.0           ~ 316 0
23 NAME Galactic Bulge reg ~ ~           ~ 3535 0

    Equat.    Gal    SGal    Ecl

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2021.03.05-17:31:47

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