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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

Accurate effective temperature from H alpha profiles

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Autor(es):
Giribaldi, R. E. [1, 2] ; Ubaldo-Melo, M. L. [1] ; Porto de Mello, G. F. [1] ; Pasquini, L. [2] ; Ludwig, H-G [3] ; Ulmer-Moll, S. [4, 5] ; Lorenzo-Oliveira, D. [6]
Número total de Autores: 7
Afiliação do(s) autor(es):
[1] Univ Fed Rio de Janeiro, Observ Valongo, Ladeira Pedro Antonio 43, BR-20080090 Rio De Janeiro, RJ - Brazil
[2] European Southern Observ, Karl Schwarzchild Str 2, D-85748 Garching - Germany
[3] Heidelberg Univ, Zentrum Astron, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg - Germany
[4] Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre 687, P-4169007 Porto - Portugal
[5] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Porto - Portugal
[6] Univ Sao Paulo, Dept Astron, IAG, Rua Matao 1226, Cidade Univ, BR-05508900 Sao Paulo, SP - Brazil
Número total de Afiliações: 6
Tipo de documento: Artigo Científico
Fonte: Astronomy & Astrophysics; v. 624, APR 1 2019.
Citações Web of Science: 0
Resumo

Context. The determination of stellar effective temperature (T-eff) in F, G, and K stars using Ha profile fitting is a quite remarkable and powerful tool because it does not depend on reddening and is only slightly sensitive to other atmospheric parameters. Nevertheless, this technique is not frequently used because of the complex procedure needed to recover the profile of broad lines in echelle spectra. As a consequence, tests performed on different models have sometimes provided ambiguous results. Aims. The main aim of this work is to test the ability of the H alpha profile fitting technique to derive T-eff. We also aim to improve the applicability of this technique to echelle spectra and to test how well 1D + LTE models perform on a variety of F-K stars. We also apply the technique to HARPS spectra and test the reliability and the stability of the HARPS response over several years using the Sun. Methods. We have developed a normalization method for recovering undistorted H alpha profiles and we have first applied it to spectra acquired with the single-order Conde instrument (resolution R = 45 000) at do Pico dos Dias Observatory to avoid the problem of blaze correction. The continuum location around H alpha is optimised using an iterative procedure, where the identification of minute telluric features is performed. A set of spectra was acquired with the MUSICOS echelle spectrograph (R = 40 000) to independently validate the normalization method. The accuracy of the method and of the 1D + LTE model is determined using Coude/HARPS/MUSICOS spectra of the Sun and Coude-only spectra of a sample of ten Gaia Benchmark Stars with T-eff determined from interferometric measurements. HARPS, Conde, and MUSICOS spectra are used to determine T-eff of 43 sample stars. Results. We find that a proper choice of spectral windows of fits plus the identification of telluric features allow for a very careful normalization of the spectra and produce reliable Ha profiles. We also find that the most used solar atlases cannot be used as templates for H alpha temperature diagnostics without renormalization. The comparison with the Sun shows that H alpha profiles from 1D + LTE models underestimate the solar T-eff by 28 K. We find the same agreement between H alpha and interferometry and between H alpha and Infrared Flux Method: a shallow dependency on metallicity according to the relation T-eff =T-eff(H alpha) -159{[}Fe/H] + 28 K within the metallicity range -0.70 to +0.40 dex. The comparison with the Infrared Flux Method shows a scatter of 59 K dominated by photometric errors (52 K). In order to investigate the origin of this dependency, we analyzed spectra from 3D models and found that they produce hotter temperatures, and that their use largely improves the agreement with the interferometric and Infrared Flux Method measurements. Finally, we find HARPS spectra to be fully suitable for Ha profile temperature diagnostics; they are perfectly compatible with the Conde spectra, and lead to the same Teff for the Sun as that found when analysing HARPS spectra over a timespan of more than 7 yr. (AU)

Processo FAPESP: 16/20667-8 - Cronômetros estelares: a conexão entre idade, atividade cromosférica, rotação e abundâncias de lítio em estrelas de tipo solar
Beneficiário:Diego Lorenzo de Oliveira
Linha de fomento: Bolsas no Brasil - Pós-Doutorado