Issue 
A&A
Volume 595, November 2016



Article Number  C2  
Number of page(s)  3  
Section  Stellar structure and evolution  
DOI  https://doi.org/10.1051/00046361/201323317e  
Published online  09 November 2016 
Oscillation mode linewidths and heights of 23 mainsequence stars observed by Kepler (Corrigendum)
^{1} Univ. ParisSud, Institut d’Astrophysique Spatiale, UMR 8617, CNRS, Bâtiment 121, 91405 Orsay Cedex, France
email: Thierry.Appourchaux@ias.upsud.fr
^{2} Tata Institute of Fundamental Research, Homi Bhabha Road, 400005 Mumbai, India
^{3} Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, New South Wales 2006, Australia
^{4} Department of Astronomy, The University of Tokyo, Tokyo 113033, Japan
^{5} School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
^{6} Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain
^{7} Universidad de La Laguna, Dpto. de Astrofísica, 38206 La Laguna, Tenerife, Spain
^{8} LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Denis Diderot, 5 place Jules Janssen, 92195 Meudon Cedex, France
^{9} Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, 8000 Aarhus C, Denmark
^{10} Laboratoire AIM, CEA/DSMCNRSUniversité Paris Diderot, IRFU/SAp, Centre de Saclay, 91191 GifsurYvette Cedex, France
Key words: stars: interiors / asteroseismology / methods: data analysis / errata, addenda
In Appourchaux et al. (2014), the correct Eq. (1) should have been written with a minus sign in front of the second bracket as (1)where ν is the mode frequency, ν_{max} is the frequency of maximum mode height, α is the power law index, Γ_{α} is the factor of the power law, ΔΓ_{dip} is the depth of the dip, W_{dip} is the width of the dip and ν_{dip} is the frequency of the dip. The fits in Appourchaux et al. (2014) were indeed performed with the minus sign.
Another error was also found in the original Table 3 of Appourchaux et al. (2014) pretending to give the parameters of Eq. (1). As a matter of fact, in that Table 3, the parameter W_{dip} as reported is related to the full width at half maximum (FWHM) calculated in frequency space, and in addition wrongly computed as it should have been about 1.5 times larger. Using Eq. (1) given above, we can deduce the proper relation between FWHM_{dip} and W_{dip} as (2)
In Table 1, we give the parameters that were not affected by the mistake supplemented by the value of ν_{dip} which was not given in Appourchaux et al. (2014). In Table 2, we give the parameter W_{dip} that was not properly given in the Table 3 of Appourchaux et al. (2014), together with the corrected FWHM_{dip}, a value which was not correct in Table 3 of Appourchaux et al. (2014) and was wrongly named. We also note that from the expression of Eq. (1), there are two solutions for W_{dip} since we have (3)where is the solution greater than ν_{max}, while is the solution smaller than ν_{max}. Here the solution chosen for W_{dip} is the former solution.
These corrections do not affect the conclusions reached for the dependence of these parameters upon the effective temperature and ν_{max}.
Fig. 6
Parameters of Eq. (1) as a function of the effective temperature for all 28 stars, for the power law dependence (left) and for the Lorentzian fit (right). The median value together with the credible intervals at 33% and 66% were derived from a MonteCarlo simulation of the fit. The orange line shows the temperature dependence of the linewidth at the frequency of maximum mode height as derived by Appourchaux et al. (2012). The open diamond is the result of the fit for the solar data of the LOI. The open triangles are the results of the fit for the subgiant stars of Benomar et al. (2013). The solid lines show a linear fit of the parameters with respect to the effective temperature. The Lorentzian parameters for stars for which the Lorentzian fit is not significant are not plotted. 

Open with DEXTER 
Fig. 7
Parameters of Eq. (1) as a function of the frequency of maximum mode height for all 28 stars, for the power law dependence (left) and for the Lorentzian fit (right). The median value together with the credible intervals of 33% and 66% were derived from a MonteCarlo simulation of the fit. The open diamond is the result of the fit for the solar LOI data. The open triangles are the result of the fit for the subgiant stars of Benomar et al. (2013). The error bars are derived from a MonteCarlo simulation using credible intervals of 33% and 66%. The solid lines show a linear fit of the parameters with respect to the frequency. The Lorentzian parameters for stars for which the Lorentzian fit is not significant are not plotted. 

Open with DEXTER 
Linewidth parameters as per Eq. (1).
Width of the linewidth (W_{dip}) as per Eq. (1) and of FWHM_{dip} as per Eq. (2).
Acknowledgments
We are grateful to Mikkel N. Lund for having found a discrepancy leading to the main author to find the source of the mistake.
References
 Appourchaux, T., Benomar, O., Gruberbauer, M., et al. 2012, A&A, 537, A134 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Appourchaux, T., Antia, H. M., Benomar, O., et al. 2014, A&A, 566, A20 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Benomar, O., Bedding, T. R., Mosser, B., et al. 2013, ApJ, 767, 158 [NASA ADS] [CrossRef] [Google Scholar]
© ESO, 2016
All Tables
Width of the linewidth (W_{dip}) as per Eq. (1) and of FWHM_{dip} as per Eq. (2).
All Figures
Fig. 6
Parameters of Eq. (1) as a function of the effective temperature for all 28 stars, for the power law dependence (left) and for the Lorentzian fit (right). The median value together with the credible intervals at 33% and 66% were derived from a MonteCarlo simulation of the fit. The orange line shows the temperature dependence of the linewidth at the frequency of maximum mode height as derived by Appourchaux et al. (2012). The open diamond is the result of the fit for the solar data of the LOI. The open triangles are the results of the fit for the subgiant stars of Benomar et al. (2013). The solid lines show a linear fit of the parameters with respect to the effective temperature. The Lorentzian parameters for stars for which the Lorentzian fit is not significant are not plotted. 

Open with DEXTER  
In the text 
Fig. 7
Parameters of Eq. (1) as a function of the frequency of maximum mode height for all 28 stars, for the power law dependence (left) and for the Lorentzian fit (right). The median value together with the credible intervals of 33% and 66% were derived from a MonteCarlo simulation of the fit. The open diamond is the result of the fit for the solar LOI data. The open triangles are the result of the fit for the subgiant stars of Benomar et al. (2013). The error bars are derived from a MonteCarlo simulation using credible intervals of 33% and 66%. The solid lines show a linear fit of the parameters with respect to the frequency. The Lorentzian parameters for stars for which the Lorentzian fit is not significant are not plotted. 

Open with DEXTER  
In the text 
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