2017A&A...605A..98C


C.D.S. - SIMBAD4 rel 1.7 - 2020.05.27CEST06:18:49

2017A&A...605A..98C - Astronomy and Astrophysics, volume 605A, 98-98 (2017/9-1)

NGC 6752 AGB stars revisited. I. Improved AGB temperatures remove apparent overionisation of Fe I.

CAMPBELL S.W., MacLEAN B.T., D'ORAZI V., CASAGRANDE L., DE SILVA G.M., YONG D., COTTRELL P.L. and LATTANZIO J.C.

Abstract (from CDS):

Context. A recent study reported a strong apparent depression of FeI, relative to FeII, in the AGB stars of NGC 6752. This depression is much greater than that expected from the neglect of non-local thermodynamic equilibrium effects, in particular the dominant effect of overionisation. The iron abundances derived from FeI were then used to scale all other neutral species in the study.
Aims. Here we attempt to reproduce the apparent Fe discrepancy, and investigate differences in reported sodium abundances.
Methods. We compare in detail the methods and results of the recent study with those of an earlier study of NGC 6752 AGB stars.Iron and sodium abundances are derived using FeI, FeII, and NaI lines. We explore various uncertainties to test the robustness of our abundance determinations.
Results. We reproduce the large FeI depression found by the recent study, using different observational data and computational tools. Further investigation shows that the degree of the apparent FeI depression is strongly dependent on the adopted stellar effective temperature. To minimise uncertainties in FeI we derive temperatures for each star individually using the infrared flux method (IRFM). We find that the Teff scales used by both the previous studies are cooler, by up to 100K; such underestimated temperatures amplify the apparent FeI depression. OurIRFM temperatures result in negligible apparent depression, consistent with theory. We also re-derived sodium abundances and, remarkably, found them to be unaffected by the new temperature scale. [Na/H] in the AGB stars is consistent between all studies. Since Fe is constant, it follows that [Na/Fe] is also consistent between studies, apart from any systematic offsets in Fe.
Conclusions. We recommend the use of (V-K) relations for AGB stars, based on comparisons with our individually-derivedIRFM temperatures, and their inherently low uncertainties. We plan to investigate the effect of the improved temperature scale on other elements, and re-evaluate the subpopulation distributions on the AGB, in the next paper of this series.

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: AGB and post-AGB - stars: abundances - stars: evolution - techniques: spectroscopic - globular clusters: general - globular clusters: general

Status at CDS:  

CDS comments: Table A1: The A/RGB stars from 2013Natur.498..198C are not in SIMBAD (no coordinates).

Simbad objects: 9

goto Full paper

goto View the reference in ADS

Number of rows : 9

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 NGC 104 GlC 00 24 05.359 -72 04 53.20   5.78 4.09     ~ 3531 0
2 IRAS 09110-6439 GlC 09 12 03.10 -64 51 48.6   7.77 5.69     ~ 1236 0
3 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2256 0
4 M 5 GlC 15 18 33.22 +02 04 51.7   7.34 5.95     ~ 1763 0
5 M 4 GlC 16 23 35.22 -26 31 32.7           ~ 1669 0
6 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2000 0
7 M 62 GlC 17 01 12.60 -30 06 44.5   8.55 7.39     ~ 507 0
8 NGC 6752 GlC 19 10 52.11 -59 59 04.4   6.96 6.28     ~ 1800 0
9 M 2 GlC 21 33 27.02 -00 49 23.7     6.25     ~ 892 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2017A&A...605A..98C and select 'bookmark this link' or equivalent in the popup menu


2020.05.27-06:18:49

© Université de Strasbourg/CNRS

    • Contact