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Determination of robust metallicities for metal-rich red giant branch stars : An application to the globular cluster NGC 6528

Liu, C. LU ; Ruchti, G. LU ; Feltzing, S. LU and Primas, F (2017) In Astronomy and Astrophysics 601.
Abstract

Context. The study of the Milky Way relies on our ability to interpret the light from stars correctly. With the advent of the astrometric ESA mission Gaia we will enter a new era where the study of the Milky Way can be undertaken on much larger scales than currently possible. In particular we will be able to obtain full 3D space motions of red giant stars at large distances. This calls for a reinvestigation of how reliably we can determine, for example, iron abundances in such stars and how well they reproduce those of dwarf stars. Aims. Here we explore robust ways of determining the iron content of metal-rich giant stars. We aim to understand what biases and shortcomings the widely applied methods suffer from. Methods. In this study we... (More)

Context. The study of the Milky Way relies on our ability to interpret the light from stars correctly. With the advent of the astrometric ESA mission Gaia we will enter a new era where the study of the Milky Way can be undertaken on much larger scales than currently possible. In particular we will be able to obtain full 3D space motions of red giant stars at large distances. This calls for a reinvestigation of how reliably we can determine, for example, iron abundances in such stars and how well they reproduce those of dwarf stars. Aims. Here we explore robust ways of determining the iron content of metal-rich giant stars. We aim to understand what biases and shortcomings the widely applied methods suffer from. Methods. In this study we were mainly concerned with standard methods of analysing stellar spectra. These include the analysis of individual lines to determine stellar parameters, and analysis of the broad wings of certain lines (e.g. Hα and calcium lines) to determine effective temperature and surface gravity for the stars. Results. For NGC 6528 we find that [Fe/H] = + 0.04 dex with a scatter of σ = 0.07 dex, which gives an error in the derived mean abundance of 0.02 dex. Conclusions. Our work has two important conclusions for analysis of metal-rich red giant branch stars. Firstly, for spectra with S/N of below about 35 per reduced pixel, [Fe/H] becomes too high. Secondly, determination of Teff using the wings of the Hα line results in [Fe/H] values about 0.1 dex higher than if excitational equilibrium is used. The last conclusion is perhaps unsurprising, as we expect the NLTE effect to become more prominent in cooler stars and we can not use the wings of the Hα line to determine Teff for the cool stars in our sample. We therefore recommend that in studies of metal-rich red giant stars care should be taken to obtain sufficient calibration data to enable use of the cooler stars.

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author
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
Galaxy: bulge, Globular clusters: individual: NGC 6528, Stars: Atmospheres, Stars: fundamental parameters
in
Astronomy and Astrophysics
volume
601
publisher
EDP Sciences
external identifiers
  • scopus:85017929715
  • wos:000402313500031
ISSN
0004-6361
DOI
10.1051/0004-6361/201628967
language
English
LU publication?
yes
id
7d8a3eb4-6a0c-4db5-a90c-42ff4b930bdb
date added to LUP
2017-05-12 08:27:01
date last changed
2017-09-18 11:35:44
@article{7d8a3eb4-6a0c-4db5-a90c-42ff4b930bdb,
  abstract     = {<p>Context. The study of the Milky Way relies on our ability to interpret the light from stars correctly. With the advent of the astrometric ESA mission Gaia we will enter a new era where the study of the Milky Way can be undertaken on much larger scales than currently possible. In particular we will be able to obtain full 3D space motions of red giant stars at large distances. This calls for a reinvestigation of how reliably we can determine, for example, iron abundances in such stars and how well they reproduce those of dwarf stars. Aims. Here we explore robust ways of determining the iron content of metal-rich giant stars. We aim to understand what biases and shortcomings the widely applied methods suffer from. Methods. In this study we were mainly concerned with standard methods of analysing stellar spectra. These include the analysis of individual lines to determine stellar parameters, and analysis of the broad wings of certain lines (e.g. Hα and calcium lines) to determine effective temperature and surface gravity for the stars. Results. For NGC 6528 we find that [Fe/H] = + 0.04 dex with a scatter of σ = 0.07 dex, which gives an error in the derived mean abundance of 0.02 dex. Conclusions. Our work has two important conclusions for analysis of metal-rich red giant branch stars. Firstly, for spectra with S/N of below about 35 per reduced pixel, [Fe/H] becomes too high. Secondly, determination of T<sub>eff</sub> using the wings of the Hα line results in [Fe/H] values about 0.1 dex higher than if excitational equilibrium is used. The last conclusion is perhaps unsurprising, as we expect the NLTE effect to become more prominent in cooler stars and we can not use the wings of the Hα line to determine T<sub>eff</sub> for the cool stars in our sample. We therefore recommend that in studies of metal-rich red giant stars care should be taken to obtain sufficient calibration data to enable use of the cooler stars.</p>},
  articleno    = {A33},
  author       = {Liu, C. and Ruchti, G. and Feltzing, S. and Primas, F},
  issn         = {0004-6361},
  keyword      = {Galaxy: bulge,Globular clusters: individual: NGC 6528,Stars: Atmospheres,Stars: fundamental parameters},
  language     = {eng},
  month        = {05},
  publisher    = {EDP Sciences},
  series       = {Astronomy and Astrophysics},
  title        = {Determination of robust metallicities for metal-rich red giant branch stars : An application to the globular cluster NGC 6528},
  url          = {http://dx.doi.org/10.1051/0004-6361/201628967},
  volume       = {601},
  year         = {2017},
}