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dc.contributor.authorBeers, T.C.
dc.contributor.authorRossi, S.
dc.contributor.authorNorris, J.E.
dc.contributor.authorRyan, Sean G.
dc.contributor.authorShefler, T.
dc.date.accessioned2008-12-23T11:15:27Z
dc.date.available2008-12-23T11:15:27Z
dc.date.issued1999
dc.identifier.citationBeers , T C , Rossi , S , Norris , J E , Ryan , S G & Shefler , T 1999 , ' Estimation of Stellar Metal Abundance. II : A Recalibration of the Ca II K Technique, and the Autocorrelation Function Method ' , The Astronomical Journal , vol. 117 , pp. 981-1009 . https://doi.org/10.1086/300727
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 150346
dc.identifier.otherPURE UUID: 8703dcba-95b2-4555-83c1-c8e8aae8a0e3
dc.identifier.otherdspace: 2299/2728
dc.identifier.otherScopus: 0000815530
dc.identifier.otherORCID: /0000-0001-9069-5122/work/30501377
dc.identifier.urihttp://hdl.handle.net/2299/2728
dc.descriptionOriginal article can be found at: http://www.iop.org/EJ/journal/aj Copyright American Astronomical Society DOI: 10.1086/300727 [Full text of this article is not available in the UHRA]
dc.description.abstractWe have recalibrated a method for the estimation of stellar metal abundance, parameterized as [Fe/H], based on medium-resolution (1–2 Å) optical spectra (the majority of which cover the wavelength range 3700–4500 Å). The equivalent width of the Ca II K line (3933 Å) as a function of [Fe/H] and broadband B-V color, as predicted from spectrum synthesis and model atmosphere calculations, is compared with observations of 551 stars with high-resolution abundances available from the literature (a sevenfold increase in the number of calibration stars that were previously available). A second method, based on the Fourier autocorrelation function technique first described by Ratnatunga & Freeman, is used to provide an independent estimate of [Fe/H], as calibrated by comparison with 405 standard-star abundances. Metallicities based on a combination of the two techniques for dwarfs and giants in the color range 0.30 ≤ (B-V)0 ≤ 1.2 exhibit an external 1 σ scatter of approximately 0.10–0.20 dex over the abundance range -4.0 ≤ [Fe/H] ≤ 0.5. Particular attention has been given to the determination of abundance estimates at the metal-rich end of the calibration, where our previous attempt suffered from a considerable zero-point offset. Radial velocities, accurate to approximately 10 km s-1, are reported for all 551 calibration stars.en
dc.language.isoeng
dc.relation.ispartofThe Astronomical Journal
dc.titleEstimation of Stellar Metal Abundance. II : A Recalibration of the Ca II K Technique, and the Autocorrelation Function Methoden
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1086/300727
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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