Issue 
A&A
Volume 604, August 2017



Article Number  A42  
Number of page(s)  10  
Section  Stellar structure and evolution  
DOI  https://doi.org/10.1051/00046361/201731057  
Published online  01 August 2017 
Anomalies in the Kepler Asteroseismic Legacy Project Data A reanalysis of 16 Cyg A & B, KIC 8379927 and 6 solarlike stars
Astronomy Unit, Queen Mary University of London, Mile End Road, London E1 4NS, UK
email: i.w.roxburgh@qmul.ac.uk
Received: 27 April 2017
Accepted: 4 July 2017
I compare values of the frequencies, separation ratios, errors and covariance matrices from a new analysis of 9 solarlike stars with the Legacy project values reported by Lund et al and, for 16Cyg A&B and KIC 8379927, with values derived by Davies et al. There is good agreement between my results and Davies’s for these 3 stars, but no such agreement with the Legacy project results. My frequencies differ from the Legacy values, there are inconsistencies in the Legacy frequency covariance matrices which are not positive definite, and the Legacy errors on separation ratios are up to 40 times larger than mine and the values and upper limits derived from the Legacy frequency covariances. There are similar anomalies for 6 other solarlike stars: frequencies and separation ratio errors disagree and 2 have non positive definite covariance matrices. There are inconsistencies in the covariance matrices of 27 the 66 stars in the full Legacy set and problems with the ratio errors for the vast majority of these stars.
Key words: stars: oscillations / asteroseismology / methods: data analysis / methods: analytical
© ESO, 2017
1. Introduction
The Kepler Asteroseismic Legacy Project (Lund et al. 2017b) analysed 66 Kepler main sequence targets determining frequencies, separation ratios, error estimates and covariance matrices. From the outset of this project I queried the data (cf. Roxburgh 2015, 2016) so I developed my own mode fitting routine, applied this to the Legacy power spectra for 9 solarlike stars, and here compare my results with the Legacy project’s values.
In Sects. 3 to 7 I compare my results for 3 Kepler targets, 16 Cyg A & B and KIC 8379927, with the Legacy values and results from independent analyses by Davies et al. (2015), Davies (2015), using Davies’ power spectra. My results agree well with those of Davies et al., but do not agree with the Legacy project’s values.
The Legacy frequencies are different and the error estimates on separation ratios are up to a factor 40 larger and exceed upper limits derived from covariance matrices by a similar factor. The covariance matrices are inconsistent as they have negative eigenvalues and are therefore not positive semidefinite as they should be, giving negative χ^{2} when comparing frequency sets.
Fig. 1 16 Cyg B: top 2 panels: frequency differences LegacyRoxburgh, DaviesRoxburgh and χ^{2} of fits; bottom panel: error estimates σ_{02} on the frequency separation ratios r_{02}, Legacy, Davies, Roxburgh. 
In Sect. 8 I compare Legacy and my results for a further 6 solarlike Legacy stars; 2 have non positive definite covariance matrices, none give good agreement on frequencies or separation errors. In Sect. 9 I inspect the covariance matrices and errors on separation ratios for all 66 Legacy targets and find similar anomalies. Something is amiss with the Legacy data.
The differences between the Legacy results and those of Roxburgh and Davies are clearly shown in Fig. 1, which compares the different frequency sets for 16 Cyg B for modes with heights greater than the background (S/N> 1). I also gives the χ^{2} of the fits using the different error estimates. The bottom panel compares errors on the separation ratios r_{02} from all 4 analyses. The agreement between Roxburgh and Davies is up to 35 times better than between the Roxburgh and Legacy values.
2. Roxburgh’s mode fitting algorithm
My mode fitting algorithm searches for a minimum in the negative log likelihood (cf. Toutain & Appourchaux 1994) of a global fit of mode power + background to a section of the power spectrum that extends ~300 μHz beyond both ends of the range of frequencies to be fitted, with unconstrained parameters X_{k}: frequencies ν_{n,ℓ}; mode heights h_{n} and widths w_{n} of the ℓ = 0 modes; mode height ratios h_{10},h_{20},h_{30} of modes ℓ = 1,2,3 to the heights of modes with ℓ = 0 (with the geometrical constraint 1 + h_{20} = h_{10} + h_{30}), the same for all modes; rotational splitting ν_{Ω} and inclination i (the same for all modes); and 4 parameters of a Harveylike model of the background (A/ [1 + Bν^{c}] + D). The heights and widths of the ℓ = 1,2,3 modes are determined by (linear) interpolation in the values for the ℓ = 0 modes at the respective frequencies and, for mode heights, then multiplied by the mode height ratios. The modes are fitted with symmetric rotationally split Lorentzians. The covariance matrix is the inverse of the Hessian H(i,j) = ∂^{2}MLE/∂X_{i}∂X_{j} and the errors on the X_{k} are given as .
Power spectra
For comparison with Davies’s results I used their power spectra kindly supplied to me by Guy Davies, and for comparison with the Legacy results I used the Legacy power spectra taken from the kasoc web site namely:
Star/KIC  kasoc power spectrum  Quarters  


16 Cyg A  kplr012069424_kasocwpsd_slc_v1.pow  Q617.2  
16 Cyg B  kplr012069449_kasocwpsd_slc_v2.pow  Q617.2  
8379927  kplr008379927_kasocwpsd_slc_v2.pow  Q217.2  
9098294  kplr009098294_kasocwpsd_slc_v1.pow  Q517.2  
8760414  kplr008760414_kasocwpsd_slc_v1.pow  Q517.2  
6603624  kplr006603624_kasocpsd_slc_v1.pow  Q517.2  
6225718  kplr006225718_kasocwpsd_slc_v1.pow  Q617.2  
6116048  kplr006106415_kasocwpsd_slc_v2.pow  Q517.2  
6106415  kplr006106415_kasocwpsd_slc_v2.pow  Q616.3 
3. Results for frequencies: 16 Cyg A & B, KIC 8379927
Tables 1 to 3 gives the χ^{2} of the fits of one set of frequencies to another both for all modes and just for modes with modeheight/background =S/N> 1 (as determined by my fits). I used frequency errors in the fits as I encountered severe problems when using Legacy covariance matrices (see Sect. 5 below).
Table 1 compares the fit of the Legacy frequencies and errors (ν_{L} ± σ_{L}) to those of Roxburgh (ν_{LR} ± σ_{LR}) (using the Legacy power spectra), is the value using Legacy errors and using Roxburgh’s errors. is the value using Legacy errors but only comparing frequencies with S/N> 1, and likewise . The first row is for the full frequency sets and the second for frequency sets with “misfits” (discussed below) removed. Table 2 gives the fit of Roxburgh’s frequencies ν_{DR} (using Davies’s power spectra) to Davies’s frequencies, ν_{D} and Table 3 compares the Legacy and Davies’s values.
The RoxburghDavies fit for modes with S/N> 1 is very good for all 3 stars, much better than that of Davies’s or Roxburgh’s fits to the Legacy values. The RoxburghDavies fit to 16 Cyg B for all frequencies is strongly influenced by the misfit of the ν_{14,3} mode which has S/N = 0.15 and is unreliable; the RoxburghDavies fit for 16 Cyg A for modes with S/N< 1 is strongly influenced by the ν_{25,0} mode which has S/N = 1.08, if this is excluded , .
The frequency sets obtained from my analysis for both the Legacy and Davies power spectra, the Legacy and Davies frequencies, and my S/N values, are given in the Appendix.
χ^{2} of fits of Roxburgh (ν_{LR}) to Legacy (ν_{L}) frequencies.
χ^{2} of fits of Roxburgh (ν_{DR}) to Davies (ν_{D}) frequencies.
χ^{2} of fits of Davies (ν_{D}) to Legacy (ν_{L}) frequencies.
Fit for rotation Davies, Roxburgh (Dspec).
Table 4 compares the rotational parameters as determined by Davies et al. and as determined by Roxburgh’s fits to the Davies power spectra; there is very good agreement for all 3 stars, Roxburgh’s fits to the Davies spectra yielding almost the same values as those obtained by Davies.
4. Fitting low frequency modes
Fig. 2 16 Cyg A: legacy and Roxburgh fits to Legacy power spectrum. 
As stated above and in the footnotes to the tables there are some problems in fitting some low frequency modes. For 16 Cyg A Legacy fits (Table 1) the problem is illustrated in Fig. 2 which shows the kasoc power spectrum for 16 Cyg A smoothed by a Gaussian smoother (with σ = 0.1 μHz), and overlaid the Roxburgh fit to the full power spectrum and the location of the Legacy and Roxburgh frequencies for modes ν_{12,0} and the pair ν_{13.2},ν_{14,0}. The Legacy values for ν_{12,0} and ν_{13.2} are poor fits and and Roxburgh’s error estimates (from the Hessian of the MLE fit) are considerably smaller than the Legacy values. Excluding these 2 modes reduces and from 7.077 and 8.590 to 1.540 and 1.427 respectively. A similar problem exists for the fit to ν_{12,2} for 16 Cyg B; excluding this mode reduces the of the fit using Roxburgh’s errors from 5.067 to 1.412. The S/N values remain unchanged since this mode has S/N< 1.
Davies’s value of ν_{12,2} for 16 Cyg B is also a poor fit to his power spectrum. ν_{14,3} (which has S/N = 0.15) differs from my value by ~3 μHz so I determined the quality of fits to the section of the Davies power spectrum between 1982.6 ± 29 μHz for a 100^{2} matrix of values of ν_{15,1}, ν_{14,3} and 10 values of height ratio h_{31} between 0.01 to 0.1, with fitting parameters the ℓ = 1 mode height, one width for both ℓ = 1 and 3 and a constant background; all with { ν_{Ω}sini,i } = { 0.27,34 }. Figure 3 shows the quality of fits (MLE−MLE_{min}) for 2 values of h_{31}; the best fits for all h_{31} have ν_{14,3} = 1973.71 μHz; my full fit value is 1973.69 ± 0.37 μHz.
Fig. 3 16 Cyg B: quality of free mode fits to Davies power spectrum. 
χ^{2} of covariance fits of Roxburgh (ν_{LR}) to Legacy (ν_{L}).
χ^{2} of covariance fits of Davies (ν_{D}) to Legacy (ν_{L}).
χ^{2} of covariance fits of Roxburgh (ν_{DR}) to Davies (ν_{D}).
5. Covariance matrices and frequency comparison
The χ^{2}s of the fit of N frequencies incorporating their correlations are given by [DC^{1}D^{T}] /N where D is the vector of frequency differences and C^{1} the inverse of the frequency covariance matrix C. Tables 5–7 give the results of such fits for 16 Cyg A & B and KIC 8379927 for both the full frequency sets and for modes with S/N> 1 using Legacy (L), Davies (D) and Roxburgh (R) inverse covariance matrices (determined using the SVD algorithm). Whilst the χ^{2} for the RoxburghDavies fits are compatible (and small) and consistent with the values using frequency errors as given in Table 2, the χ^{2}s using the Legacy covariance matrices give negative values, which should not be the case since covariance matrices and their inverses are necessarily positive semidefinite so should always give positive χ^{2}.
Since a symmetric matrix C is positive semidefinite if and only if all its eigenvalues are nonnegative, I determined the eigenvalues for the Legacy covariance matrices for all 3 stars. The absolute value of the eigenvalues w_{j} is given by SVD and the sign from which of det(C−w_{j}U) and det(C + w_{j}U), is zero, or closest to zero given rounding errors [U is the unit matrix]. All 3 Legacy covariance matrices have negative eigenvalues, 16 Cyg A having 10, 16 Cyg B 12, KIC 8379927 10. The Roxburgh and Davies covariance matrices are all positive definite.
The stark difference between Legacy and Roxburgh matrices is illustrated in Fig. 4 which displays their inverse covariance matrices for 16 Cyg A [magnitude=size of points, black +ve, red ve]. Something is clearly amiss with the Legacy evaluation of the covariance matrices from their Markov chain Monte Carlo (MCMC) analysis.
Fig. 4 16 Cyg A: inverse covariance matrices. Top: legacy; bottom: Roxburgh [black +ve, red ve, magnitude = size of points]. 
6. Frequency separation ratios
The ratios of small (d) to large (Δ) frequency separations are widely used in model fitting since they are (almost) independent of the structure of the outer layers of a star. These ratios are defined as (Roxburgh & Vorontsov 2003, 2013, Roxburgh 2005) (1a)where The Legacy project and Davies give values of the ratios, errors and ratio covariance matrices for the 3 stars analysed here. They also give values for r_{010} ratios but these do not contain any additional information since from 2N (ℓ = 0,1) frequencies one can only determine N surface layer independent quantities.
Fig. 5 Top panel: error estimates σ_{101} on ratios r_{101}(n) from Legacy, Davies, and Roxburgh analyses of 16Cyg A&B, and KIC 8379927; bottom errors σ_{02} on ratios r_{02}. 
The values of the ratios r_{101} and r_{02} as determined by the different analyses are similar but, as shown in Fig. 5 the error estimates are wildly different. The top panel shows the 4 determinations of error estimates σ_{101} on the ratios r_{101} by Legacy, Davies, and Roxburgh using both the kasoc and Davies power spectra, all limited to modes with S/N> 1. The bottom panel shows the error estimates σ_{02} on r_{02}. Davies’s and the two Roxburgh values are very close but the Legacy error estimates are very much larger than those of Davies and Roxburgh, by a factor of up to 40.
7. Error estimates and upper limits for separation ratios from frequency covariances
The covariance of two linear functions r_{n}(ν_{j}) = ∑ A_{j}ν_{j}, and r_{m}(ν_{k}) = ∑ B_{k}ν_{k} of variables ν_{i} is given by (2)and the error estimate σ_{n} on r_{n}(ν_{k}) is given by the variance (3)where corr_{jk} are the correlations and σ_{i} the error estimates on ν_{i}. Since  corr_{jk}  ≤ 1 it follows that an upper bound on σ_{n} is given by taking corr_{jk} = + 1 if A_{j}A_{k}> 0 and −1 if negative, hence (4)The small separations d_{n} [both d_{101}(n) and d_{02}(n)] are linear functions of ν, d_{n} = ∑ D_{k}ν_{k} (cf Eqs. (1b), (1c)), but the contribution of the large separation Δ_{n} introduces a small non linearity in the ratios. To a good approximation (1 in 10^{3} see below) the variance of the separation ratios r_{n}(ν_{k}) is given by (5)and so, with the A_{k} defined through Eq. (5) (see below), the error estimate σ_{n} on r_{n} is given by Eq. (3) and the upper limit σ_{L} by Eq. (4).
Coefficients A _{ k } for errors σ_{02}(n),σ_{101}(n) on r_{02}(n),r_{101}(n)
For r_{0} = r_{02}(n), Δ_{0} = ν_{n,1}−ν_{n−1,1}(6)For r_{0} = r_{101}(n), Δ_{0} = ν_{n,1}−ν_{n−1,1}(7)Figure 6 shows the fractional differences between the σ’s given by Davies’s analysis of 16 Cyg A & B and KIC 8379927, and the σ_{Dcov} given by Eqs. (3), (6) and (7), using Davies’s frequencies and frequency covariances; all but two are less than 10^{3}. The two are KIC 8379927 σ_{02}(n), n = 14,15, which have values −2.5 × 10^{3}, 4.4 × 10^{3}, and are derived from modes with S/N < 1.
Fig. 6 Fractional difference between Davies’s MCMC values for the errors σ_{101}, σ_{02} and the values from Eqs. (3), (6), (7). All but two <10^{3}. 
Fig. 7 Fractional difference between the Legacy MCMC values for the errors σ_{101}, σ_{02} and the σ_{Lcov} values from Eqs. (3), (6), (7). 
Fig. 8 Ratios of Legacy error estimates σ_{101}, σ_{02} to the upper limits σ_{L} from Eq. (4) for 16 Cyg A & B and KIC 8379927, for modes with S/N> 1. The Legacy values exceed the upper limits by a factor of up to 30. 
Figure 7 shows the same comparison but between Legacy σ’s and the values σ_{Lcov} derived using the Legacy frequencies and frequency covariances; here many of the differences are huge.
As shown in Fig. 8 the Legacy σ’s also exceed the upper limits σ_{L} given by Eq. (4), whereas Davies’s and Roxburgh’s values, and the rederived Legacy values σ_{Lcov}, are less than their corresponding upper limits. Something seems to be amiss with the Legacy values.
8. Comparison of Legacy and Roxburgh results for a further 6 solarlike stars
Having verified that my code gives results in agreement with Davies et al., I then applied my analysis to the 6 other solarlike stars from the Legacy short list of 22 high priority targets which have large separations Δ in the range 100–120 μHz and ν_{max} in the range 2138–2470 μHz, namely KIC 9098294, 8760414, 6603624, 6225718, 6116048, 6106415. The fit of the Roxburgh to Legacy frequencies for KIC 6225718 is shown in Fig. 9.
Table 8 gives the fits of the Legacy frequencies to Roxburgh’s for all 6 stars using the frequency errors (rows labelled σ) and the inverse covariance matrices (labelled cov) both for all frequencies and for the subset with S/N> 1.
Fig. 9 KIC 6225718: frequency differences, LegacyRoxburgh. 
For KIC 9098294, 6603264, there is good agreement between χ^{2} using the Legacy covariance matrices and uncorrelated errors, and reasonable agreement for 6225718 and 6106415, but the χ^{2} are still an order of magnitude larger than the 3 RoxburghDavies fits for S/N> 1. The fits for KIC 8760414 and 6116048 are not so good: KIC 8760414 having a negative χ^{2} and KIC 6116048 a factor 3 difference between values with the Legacy covariance matrix and uncorrelated errors. Analysis of the covariance matrices revealed that for the best 4 of the 6 stars the Legacy covariance matrices had no negative eigenvalues and are therefore positive definite, whilst the other 2 have negative eigenvalues and are therefore inconsistent.
Figure 10 plots the Legacy error estimates σ_{101} and σ_{02} on the separation ratios r_{101} and r_{02} which show a similar behaviour to those of 16 Cyg A & B and KIC 8379927 in that the Legacy estimates are all larger than Roxburgh’s for all 6 stars. For KIC 9098294 this is only by a factor ~2 but for KIC 6116048 the Legacy value is up to a factor 50 larger then Roxburgh’s.
As was the case for 16 Cyg A & B and KIC 8379927, the Legacy ratio errors for all of these 6 stars also exceed the upper limits calculated as described in Sect. 7 above, and likewise new values for errors on the Legacy ratios calculated using the Legacy covariance matrices gave lower values, all of which are less than the corresponding upper limits.
Fit of Roxburgh to Legacy frequencies: 6 solarlike stars.
Fig. 10 Logarithm of the error estimates on the ratios r_{101},r_{02} for all 6 solarlike stars. The Legacy values exceed Roxburgh’s values by factors ranging from 2 to 50. 
9. Covariance matrices and errors on separation ratios for all 66 Legacy target stars
The Legacy Project analysed a total of 66 main sequence stars (Lund et al. 2017b) only 9 of which have been analysed by my code and compared with the Legacy data. Whilst this may ultimately be expanded to all the Legacy targets, I here just examine the Legacy data on all 66 stars to see whether their covariance matrices are positive semidefinite or whether they have negative eigenvalues, and whether they have anomalously large error estimates σ_{101},σ_{02} for the separation ratios r_{101},r_{02}.
The eigenvalues of all 66 Legacy covariance matrices were determined by the same procedure as applied to 16 Cyg A & B and KIC 8379927, the absolute magnitudes w from SVD, and the sign from the determinants   C ± wU  . 27 have covariance matrices with negative eigenvalues and are therefore inconsistent, the remaining 39 stars have positive definite covariance matrices.
Fig. 11 Logarithm of the ratio of the error estimates to the upper limits on the ratios r_{101},r_{02} for all 66 Legacy stars. The blue triangles are stars with inconsistent covariance matrices, the red stars the values recomputed from the covariance matrices. 59 of the Legacy values exceed one or both upper limits on σ. 
Next I compare the Legacy values for the error estimates σ_{101},σ_{02} on the separation ratios r_{101},r_{02} with the values rederived from the frequency covariance matrices and the upper limits as determined by Eqs. (3), (4), (6), and (7) in Sect. 7. Figure 11 shows the Legacy data error estimates σ_{101},σ_{02} divided by the upper limits and the rederived values divided by the upper limits all averaged over 3 values around their ν_{max}. The blue triangles are stars with inconsistent covariance matrices (negative eigenvalues). 7 stars have values of σ_{101} and σ_{02} less than their upper limits all of which have positive definite covariance matrices, of which KIC 3427720, 8938364, 9353712 and 10079226 have Legacy values for ratio errors within 2% of the rederived values from their covariance matrices.
I selected KIC 3427720, the brightest and most solarlike of the 4 to test if, for such a star, the Legacy frequencies agreed with values obtained on applying my mode fitting algorithm to the power spectrum ( kplr003427720_kasocwpsd_slc_v1.pow). The details of the fits are given in Table 9; as anticipated the χ^{2}s of the fits using errors and those using covariance matrices are in good agreement, but the values for modes with S/N> 1 are still more than a factor 10 larger than those of the RoxburghDavies fits to 16 Cyg A & B and KIC 8379927.
Fit of Roxburgh to Legacy frequencies: KIC 3427720.
10. Conclusions and discussion
1) I developed a new mode fitting code different from, and independent of, the codes used by Davies et al and the Legacy project which, when applied to the Davies et al power spectra for 16 Cyg A, 16 Cyg B and KIC 8379927, reproduces the frequencies, separation ratios, errors, rotational parameters and covariance matrices of Davies’s analysis to good accuracy, especially for modes with S/N = heights/background >1 which are least sensitive to differences in the modelling of the background and the possibility of misidentification of fluctuations in noise as signal. For modes with S/N> 1 the χ^{2} of the fits of Roxburgh to Davies’s frequencies are ≤0.062, both for comparisons using only error estimates and using full covariance matrices (≤0.035 if one mode with S/N = 1.08 is excluded).
The same code when applied to the Legacy power spectra for 16 Cyg A, 16 Cyg B and KIC 8379927 does not reproduce the Legacy values. Frequency comparison when using covariance matrices produces anomalous results including negative χ^{2}; all 3 covariance matrices are inconsistent as they have negative eigenvalues and are therefore not positive semidefinite as any covariance matrix should be.
The Legacy errors on separation ratios are up to 40 times larger than my values and exceed values and upper limits derived from the Legacy frequency covariances by a similar factor.
2) I then fitted the power spectra for 6 additional solarlike stars taken from the Legacy high priority list. Here the agreement is not as bad as for 16 Cyg A & B and KIC 8739927, for modes with S/N> 1 the best fit of Roxburgh to Legacy (KIC 6603624) has a χ^{2}< 0.27 (still an order of magnitude larger than the RoxburghDavies fits), and good agreement between fits using errors and fits using covariance matrices; the worst fit (KIC 8760414) gave a negative χ^{2} on fitting with the Legacy covariance matrix. The 4 best fits have positive definitive covariance matrices, the 2 worst fits do not. For all 6 stars the Legacy error estimates on the separation ratios exceed the values and upper limits derived using their covariances; KIC 9098294 is the one for which the Legacy values are closest to the values obtained using the frequency covariances.
3) Finally I examined all 66 Legacy targets both to test if their covariance matrices were positive semidefinite, and whether or not the errors on separation ratios satisfied their upper limits. The covariance matrices of 27 stars have negative eigenvalues and are therefore inconsistent, 39 have positive definite covariance matrices. 59 did not satisfy the upper limits on their separation ratio errors, and 4 had ratio errors consistent to within 2% of the rederived values from their (positive definite) covariance matrices. On fitting the power spectrum of one of these, KIC 3427720; my resulting frequencies still did not agree with the Legacy values, all the fits having a χ^{2} ~ 0.5 whether using Roxburgh or Legacy errors or covariance matrices.
To summarise: results using my mode fitting code agree with those of Davies et al.; results from my code do not agree with the Legacy values; many of the Legacy covariance matrices are inconsistent having negative eigenvalues and therefore are not positive semidefinite; almost all of the Legacy values for errors on the separation ratios do not agree with values and upper limits derived using the Legacy covariance matrices.
It is difficult to escape the conclusion that there is something amiss with the Legacy analysis.
Note added in proof. Lund et al. (2017a) have now produced a draft addendum to their original paper in which they have identified the reason for the overestimation of uncertainties on separation ratios as a missing trimming in their postprocessing of the MCMC chains, which reduces their estimates to values comparable to the values obtained by the analysis given in this paper. They will also provide covariance matrices for the mode frequencies, separation ratios and second differences.
Lund M. N., SilvaAguirre V., Davies G. R., et al. 2017a, manuscript published on the KASOC web site 12/06/2017
Acknowledgments
The author thanks Dr. G. R. Davies for supplying and giving permission to use detailed files of the results of his analyses of 16 Cyg A, 16 Cyg B, and KIC 8379927, and Dr M. N. Lund for supplying and giving permission to use the updated (robust) results of the Legacy analyses including the unpublished covariance matrices. The author gratefully acknowledges support from the UK Science and Technology Facilities Council (STFC) under grant ST/M000621/1.
References
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Appendix A: Frequency tables
The following tables give the frequencies for 16 Cyg A, 16 Cyg B and KIC 8379927 as determined by the Legacy project, Roxburgh (Legacy), Davies, and Roxburgh (Davies), and the values of S/N from my analyses where S/N is defined as the maximum height of a rotationally split mode divided by the local background.
16 Cyg A: frequencies and errors (in μHz) for Legacy, Roxburgh (Legacy), Davies, Roxburgh (Davies) and S/N values.
16 Cyg B: frequencies and errors (in μHz) for Legacy, Roxburgh (Legacy), Davies, Roxburgh (Davies) and S/N values.
KIC 8379927: Frequencies and errors (in μHz) for Legacy, Roxburgh (Legacy), Davies, Roxburgh (Davies) and S/N values.
All Tables
16 Cyg A: frequencies and errors (in μHz) for Legacy, Roxburgh (Legacy), Davies, Roxburgh (Davies) and S/N values.
16 Cyg B: frequencies and errors (in μHz) for Legacy, Roxburgh (Legacy), Davies, Roxburgh (Davies) and S/N values.
KIC 8379927: Frequencies and errors (in μHz) for Legacy, Roxburgh (Legacy), Davies, Roxburgh (Davies) and S/N values.
All Figures
Fig. 1 16 Cyg B: top 2 panels: frequency differences LegacyRoxburgh, DaviesRoxburgh and χ^{2} of fits; bottom panel: error estimates σ_{02} on the frequency separation ratios r_{02}, Legacy, Davies, Roxburgh. 

In the text 
Fig. 2 16 Cyg A: legacy and Roxburgh fits to Legacy power spectrum. 

In the text 
Fig. 3 16 Cyg B: quality of free mode fits to Davies power spectrum. 

In the text 
Fig. 4 16 Cyg A: inverse covariance matrices. Top: legacy; bottom: Roxburgh [black +ve, red ve, magnitude = size of points]. 

In the text 
Fig. 5 Top panel: error estimates σ_{101} on ratios r_{101}(n) from Legacy, Davies, and Roxburgh analyses of 16Cyg A&B, and KIC 8379927; bottom errors σ_{02} on ratios r_{02}. 

In the text 
Fig. 6 Fractional difference between Davies’s MCMC values for the errors σ_{101}, σ_{02} and the values from Eqs. (3), (6), (7). All but two <10^{3}. 

In the text 
Fig. 7 Fractional difference between the Legacy MCMC values for the errors σ_{101}, σ_{02} and the σ_{Lcov} values from Eqs. (3), (6), (7). 

In the text 
Fig. 8 Ratios of Legacy error estimates σ_{101}, σ_{02} to the upper limits σ_{L} from Eq. (4) for 16 Cyg A & B and KIC 8379927, for modes with S/N> 1. The Legacy values exceed the upper limits by a factor of up to 30. 

In the text 
Fig. 9 KIC 6225718: frequency differences, LegacyRoxburgh. 

In the text 
Fig. 10 Logarithm of the error estimates on the ratios r_{101},r_{02} for all 6 solarlike stars. The Legacy values exceed Roxburgh’s values by factors ranging from 2 to 50. 

In the text 
Fig. 11 Logarithm of the ratio of the error estimates to the upper limits on the ratios r_{101},r_{02} for all 66 Legacy stars. The blue triangles are stars with inconsistent covariance matrices, the red stars the values recomputed from the covariance matrices. 59 of the Legacy values exceed one or both upper limits on σ. 

In the text 
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