Mon. Not. R. Astron. Soc. 000, 1–?? (2002) Printed 29 August 2014 (MN LATEX style file v2.2)

On the mass estimation for FGK stars: comparison of several methods

F. J. G. Pinheiro1,2⋆, J. M. Fernandes1,2,3, M. S. Cunha4,5, M. J. P. F. G. Monteiro4,5,6, N. C. Santos4,5,6, S. G. Sousa4,5,6, J. P. Marques7, J.-J. Fang8, A. Mortier9 and J. Sousa4,5 1Centro de Geofísica da Universidade de Coimbra 2Observatório Geofísico e Astronómico da Universidade de Coimbra 3Departamento de Matemática da Universidade de Coimbra, Largo D. Dinis, P-3001-454 Coimbra, Portugal 4Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, PT4150-762 Porto, Portugal 5Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 6Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal 7The Institut d’Astrophysique Spatiale, Orsay, France 8Centro de Física Computacional, Department of Physics, University of Coimbra, P-3004-516 Coimbra, Portugal 9SUPA, School of Physics and Astronomy, University of St Andrews, St Andrews KY16 9SS, UK

Accepted . Received

ABSTRACT Stellar evolutionary models simulate well binary stars when individual stellar mass and system metallicity are known. The mass can be derived directly from observations only in the case of multiple stellar systems, mainly binaries. Yet the number of such stars for which ls accurate stellar masses are available is rather small. The main goal of this project is to provide realistic mass estimates for an homogeneous sample of about a thousand FGK single stars, using four different methods and techniques. We present the masses inferred according to each one of these methods as well as a final mass estimate consisting in the median of the four mass estimates. The proceduresevaluated here include the use of stellar evolutionary models, mass- luminosity relation and surface gravity spectroscopic observations. By combining the results obtained with different methods, we determine the best mass-value for each individual star, as well as the associated error budget. Our results confirm the expected consistency between the different mass estimation methods. Nonetheless, for masses above 1.2M⊙ the spectroscopic surface gravities seem to overestimate the mass. This result may be a consequence of the spectroscopic surface gravities used in this analysis. Nevertheless this problem is minimized by the fact the we have available several approaches for deriving stellar masses. Moreover, we suggest an empirical procedure to overcome this issue. Key words: Methods: numerical, Stars: fundamental parameters, Stars: Hertzsprung-Russell (HR) and C-M, Stars: binaries

1 INTRODUCTION by Torres et al. 2010). Unfortunately, the number of stars for which accurate stellar masses are available is less than 180 (Torres et al. The mass is a fundamental stellar parameter. Moreover, the stellar 2010). Moreover, in most cases these are members of eclipsing mass has a major impact in other astrophysical contexts, such as in binaries for which the metallicity (for example) is currently un- studies of the initial mass function, of the mass-luminosity relation, known or poorly known. Different methods are commonly used to the study of extra-solar planets and their frequency for stars of dif- determine the mass of single stars. In particular, for FGK stars we ferent mass, and of the definition of the star-brown dwarf limit. All can find semi-observational, empirical and theoretical methods for these aspects are fundamental when studying the global proprieties mass determination. of the Galaxy and when attempting to improve the characterization of stellar populations in galaxies. As a semi-observational method we may consider the deter- Stellar masses can be determined with accuracy only for vi- mination of the mass through the surface gravity. Spectroscopic sual, spectroscopic and eclipsing binaries. For the latter an accu- analysis of a star allows for the determination of effective tempera- racy of 1 to 3% can be achieved (Andersen 1991; recently revised ture, metallicity and surface gravity (e.g. Sousa et al. 2006; Santos et al. 2005). Currently, the knowledge of the photometry (including bolometric correction) and parallax allows the luminosity (L) to be ⋆ E-mail:[email protected] determined and then the mass can be estimated. This methodology

c 2002 RAS 2 F. J. G. Pinheiro et al. is potentially interesting for nearby stars, where the uncertainty in 2 OBSERVATIONAL DATA AND METHODOLOGY the distance (and thus in the luminosity) is more likely to be small. The objects used in our analysis were taken from the works of Errors affecting this method include the usually high uncertainties Sousa & et al. (2008) and Sousa et al. (2011) for which informa- in the spectroscopic surface gravities, or for the case of stars at tion on their effective temperature (T ), luminosity (L), surface more than 50pc, the errors in the measured parallax (for some stars eff gravity (log g) and metal abundance ([Fe/H]) has been derived this problem will be solved with the GAIA mission). The present in a consistent way. This sample comprises more than a thousand accuracy on the mass determinations using this method is not better objects located in the solar neighbourhood (up to 58 pc away), than 10-20% (Sousa et al. 2011). presenting slow rotation velocities and no signs of stellar activ- ity. for which have been excluded any known binaries and variable As an empirical method we may consider the determination of stars (Sousa & et al. 2008; Sousa et al. 2011). A detailed descrip- mass through the Mass-Luminosity Relation (MLR). Henry (2004) tion of these targets can be found in the works of Mayor et al. published the best known MLR for stars ranging in mass from (2003) and Lo Curto et al. (2010). In general terms, the global 0.07M⊙ up to 33M⊙. If the luminosity is known, this relation al- properties of these targets are within the range of those typical lows an estimation of the stellar mass with an accuracy of 8-10% for FGK type stars(3.68parallaxes from Hipparcus (van relative error on the mass estimation of about 5%. One of the major Leeuwen 2007), the respective magnitudes and the bolometric cor- drawbacks of the MLR is the (quantitatively) unknown contribu- rections from Flower (1996). The spectroscopic surface gravity tion of the evolution and chemical composition of different stars to inferences of Sousa et al. used in our study determined with the the intrinsic dispersion (e.g. Gafeira et al. 2012). ARES+MOOG codes. These computations are based on equivalent widths of iron lines. Unlike other works, the computations based Regarding a theoretical method, we consider the mass estima- on specific line list of Sousa & et al. (2008) show little dependence tion through stellar models in the HR diagram and/or using astero- between surface gravities and effective temperature (Mortier et al. seismology. The former is the most current method used to estimate (2013)). A similar behaviour was also shown in the paper from Tor- the mass. Pre-computed (grids of) stellar evolutionary models are res et al. (2012) for a similar procedure also based on equivalent compared to luminosity and effective temperature on the HR Dia- widths. The reason for this is that the surface gravity is constrained gram. This is frequently known as an HRD analysis. The degener- using the Fe II lines that are much less number than the Fe I lines acy between mass and other parameters, like the abundance of he- that are used to constrain the effective temperature. lium and metals results in a systematic uncertainty of this method Taking into account these global properties, we apply four dif- (accuracy) of the order of 10% (Fernandes & Santos 2004). On the ferent mass inference approaches, namely: other hand several asteroseismic tools for the determination of stel- lar masses of solar-type stars have been developed for application to Method 1 - "Direct" determination of the stellar mass by taking stars whose oscillation spectra have already been observed thanks, into account surface gravities and stellar radii derived from the in particularly, to projects as KEPLER or COROT (Bigot & et al. well known luminosity-radius-effective temperature relation. In 2011; Metcalfe & et al. 2010). Asteroseismology complements the the particular case of using a spectroscopic surface gravity, one global observables available for a single star. This technique can obtains what is known as the spectroscopic mass. Mortier et al. result in mass uncertainties below 5% if a few frequencies with (2013) discuss the impact that different methods of surface gravity an uncertainty below 0.1 micro-Hz are available (e.g. Kjeldsen estimation can have on the determination of stellar masses. In a et al. 2009, Huber et al. 2012, Mathur et al. 2012, Creevey & similar way, Huber et al. (2012) compare asteroseismic surface et al. 2013, Chaplin et al. 2014 and references therein). The main gravities with those obtained from the analysis of photometric light drawback for this is the fact that the number of stars that full-fill the curves. above precision in frequencies is still small. Method 2 - Use of Torres et al. (2010) empirical relation between We would like to stress that one of the strongest advantages stellar mass, effective temperature, surface gravity and metal abun- of this work is the fact that we treat a large and homogeneous sam- dance, derived from the analysis of stellar binaries: ple of 451+582 FGK stars from the works from Sousa et al. (Sousa et al. 2006; Sousa & et al. 2008; Sousa et al. 2011) and Santos et al. M 2 3 2 log = a1 + a2 X + a3 X + a4 X + a5 (log g) (2005). All the stars were spectroscopically analysed by same tech- M⊙   nique and procedure. We recall that the study of the frequency of 3 +a6 (log g) + a7 [Fe/H], (1) extra-solar planets as a function of stellar mass is a stronger con- straint to the formation of exoplanets. Only a few studies have dis- where X = log(Teff )−4.1, a1=1.5689±0.058, a2=1.3787±0.029, cussed this issue, and no major correlation has yet been found yet a3=0.4243±0.029, a4=1.139±0.24, a5=-0.1425±0.011, for solar-type stars, possibly due to the relatively large error bars a6=0.01969±0.0019, a7=0.1010±0.014 and M⊙ is the solar in the determination of stellar masses (e.g. Johnson et al. 2010; mass. For main sequence stars with masses above 0.6M⊙ the

Mortier et al. 2013; Neves et al. 2013). scatter for this calibration is σlogM/M⊙ =0.027. Notice that there is a slight offset between the solar mass and the Our paper is organized as follows. The observational data is one expected from this method. Santos et al. (2013) propose a discussed in Section 2, where the different methods used to esti- calibration of these results similar to the predictions of the Padova mate the stellar mass are described. We then report and discuss in isochrones. Section 3 the results for the selected sample. Finally, in Section 4, we draw some conclusions and suggest future work. Method 3 - Use of the empirical mass-luminosity relation of

c 2002 RAS, MNRAS 000, 1–?? On the mass estimation for FGK stars:comparison of several methods 3

Henry & McCarthy (1993), calibrated by taking into account bi- Table 1. Comparison between different mass estimation methods for Sousa nary stars, wich, for stars ranging between 0.5M⊙ and 2.0M⊙ is: et al. (2008), Sousa et al. (2011) and Bruntt et al.’s (2010) data, including the root mean square of the mass estimates and a linear fit with parameters M × −3 2 − × −2 log = 2.456 10 Mv 9.711 10 Mv (a, b) to these predictions, given by M2=aM1+b (last column). M⊙   +4.365 × 10−1, (2) M1 M2 RMSM1−M2 (a, b) in which absolute magnitudes (Mv) were derived taking into MTorres MHenry 0.067 (1.02, +0.01) account the bolometric correction of Torres (2010). In this case the MTorres MPadova 0.072 (1.07, -0.13) RMS of the fit is 0.032 (in logM/M⊙). Sousa et al. MHenry MPadova 0.115 (0.91, -0.00) (2008) MTorres MDirect 0.260 (2.15, -1.19) Method 4 - Comparison of the targets’ position in the HR dia- MHenry MDirect 0.247 (2.12, -1.24) gram against the theoretical predictions of the Padova isochrones MPadova MDirect 0.233 (1.99, -0.92) 2 (as in Fernandes et al. 2011). This is done through a χ minimiza- MTorres MHenry 0.089 (1.17, -0.13) tion procedure, by minimizing the following quantity: MTorres MPadova 0.073 (1.17, -0.21) Sousa et al. MHenry MPadova 0.110 (0.91, +0.01) X − X 2 S = i model , (3) (2011) MTorres MDirect 0.544 (3.24, -2.12) ∆Xi M M 0.494 (2.81, -1.82) i=1,4   Henry Direct X MPadova MDirect 0.506 (2.89, -1.67) in which Xi is one of the four observables (L, Teff , log g and MTorres MHenry 0.183 (1.05, +0.07) [Fe/H]) and ∆Xi is the uncertainty associated with it. Notice that 0.177 (1.42, -0.51) in the case of the Sun, the models used here fail to predict its mass MTorres MPadova Bruntt et al. MHenry MPadova 0.241 (1.18, -0.38) by 0.023M⊙. For this reason we associate a 0.05M⊙ systematic (2010) MTorres MDirect 0.220 (1.22, -0.12) uncertainty to this method . MHenry MDirect 0.184 (1.03, -0.05) MPadova MDirect 0.181 (0.87, +0.30) The asteroseismic properties of solar type stars can also be used to infer stellar masses. Indeed, there are two relationships relating the stellar density and surface gravity with the large fre- In the latter case we took into account the luminosities, spec- quency separation ∆ν0, i.e. the separation between modes of the troscopic effective temperatures and metal abundances provided by same degree and consecutive radial order (Ulrich 1986) and the Bruntt et al. On the other hand, surface gravities were derived using frequency νmax at which solar-type oscillations have maximum the expression of Kjeldsen & Bedding (1995), relating the stellar power (Brown et al. 1991; Kjeldsen & Bedding 1995). Unfortu- surface gravity with the frequency of maximum power oscillations nately, unlike in the case of the work of Bruntt & et al. (2010), our (Equation 5 in their work). dataset contains no such asteroseismic information. Therefore, we Figure 1 and Table 1 point out towards a relatively good agree- cannot apply this latter approach. ment between both empirical methods and the predictions of the For all methods Monte-Carlo simulations were used to in- Padova isochrones. Indeed a linear fit to these methods’ predictions fer the mass uncertainties that arise from the uncertainties on the lies close to the expected 1:1 relation. global stellar parameters. Moreover, in the case of the empirical ap- The scatter of the data can be partially explained by the uncer- proaches and the HRD analysis, our Monte-Carlo simulations also tainties associated with each method’s predictions. However, for took into account the systematic uncertainties associated with these higher masses (M>1.1M⊙) this no longer occurs between these methods (in particular uncertainty associated with the goodness of three methods’ predictions and some of the (direct) spectroscopic the empirical fits). masses of Sousa et al.’s targets. This could be a source of concern Given these four mass estimates, we want to investigate the since, in theory, the "direct" approach could be seen as the most re- better way to use the four mass predictions available minimizing liable approach. Unlike the other methods, it relies exclusively on the impact of any outlier values in the final mass estimate. For this well known physical relationships between global stellar parame- reason we evaluated three different methods for merging this infor- ters (instead of empirical relationships or models). Nevertheless, an mation into a single mass prediction: the computation of the statis- inspection of the masses inferred for Bruntt et al.’s targets, clearly tical mean, the median and a weighted mean: shows that the 1:1 relation between the four mass predictions is 4 4 −1 reasonably satisfied. This indicates that the problem must lie on the

M = Miwi × wi , (4) values of the global parameters used in these computations and not i=1 ! i=1 ! on the methods themselves. X X 2 A simple test to Sousa et al.’s (2011) data revealed that, from where wi = 1/σi and σi is the mass uncertainty associated with the four approaches considered here, the direct method is the most method "i". sensitive to errors in the luminosity and effective temperature. The test consisted in introducing a 0.05 dex increase on the surface gravity and luminosity of each star and determining the corre- sponding impact on the final mass estimate(see Fig. 2). This anal- 3 RESULTS AND DISCUSSION ysis only evaluates the individual impact that these parameters Figure 1 shows a comparison between the mass estimates, obtained have in the mass determination. Correlations between the ef- according to each method, for data from Sousa et al.. As a reference fective temperature and surface gravity uncertainties were dis- we also plotted each method’s prediction for 22 stars from the work regarded since, the computations based on specific line list of of Bruntt & et al. (2010). Sousa & et al. (2008) show little dependence between surface

c 2002 RAS, MNRAS 000, 1–?? 4 F. J. G. Pinheiro et al.

Figure 1. Comparison between the mass estimates obtained using the different methods. The squares and black dots correspond, respectively, to Sousa et al.’s 2008 and 2011 data, while the circles correspond to Bruntt et al.’s 2010 data. The boxes on the top left hand side of each panel correspond to the typical mass uncertainties associated with each method, while the dashed line shows the 1:1 relation expected if each two methods were in perfect agreement. gravities and effective temperature (Mortier et al. 2013). In this to Fig. 3 shows that, as it should be expected, the non-weighted way we observed that the fraction of stars in the sample which suf- average can be strongly affected by errors in a given mass esti- fer a significant mass shift when this procedure is applied is largest mate. On the other hand, the median and the weighted mean of the for the spectroscopic approach. This provides a plausible justifica- mass estimates are very close to the 1:1 relation. For instance, for tion for the weaker agreement between the spectroscopic masses Sousa et al.’s (2008) data we get: MWeighted=0.92MMedian+0.04. and other mass estimates. Moreover, an inspection of the RMS between the different mass es- timates (Table 2) shows that both, the weighted mass and the me- After finding a possible justification for the discrepancy be- dian of the four mass estimates, are equally good for combining tween the different mass estimations, we proceeded to identify the the four values. The RMS between the median and the weighted stellar parameter causing this discrepancy. In order to do so we re- averages is 0.055 for the 2008 and 0.053 for the 2011 data. Again, quire what can be called as the "final mass estimate", which re- sults from combining the four individual estimates. An inspection

c 2002 RAS, MNRAS 000, 1–?? On the mass estimation for FGK stars:comparison of several methods 5

Figure 2. Impact of a 0.05 dex surface gravity (top) and 0.05 dex luminosity Figure 3. Comparison between the median of the four mass predictions and (bottom) increase on the mass predictions for data from Sousa et al. (2011). the mean (top) and the weighted mean (bottom) of the mass predictions. The squares and black dots correspond, respectively, to Sousa et al.’s 2008 and 2011 data, while the circles correspond to Bruntt et al.’s 2010 data. The boxes on the upper left corners correspond to the typical mass uncertainties this result points out the similarities between these methods of mass associated with each method, while the dashed lines correspond to the 1:1 combination. relation. The main problem of using a non-weighted average is that er- rors in one of the mass estimates can have a significant impact in the final result (as it will be seen later in Table 2 & Fig. 3). Moreover, Table 2. Root mean square of the four mass estimates (Mi) using three the error associated with a given mass estimate may not necessarily options for combining the values (mean, median and weighted average). reflect the reliability of its corresponding mass estimation method. On the other hand, medians are good indicators of central tenden- Data Mean Median Weighted cies which tend to be far less sensitive to such issues. Thus, given the median’s robustness to outliers, it was decided to use this value MSpec 0.181 0.225 0.235 as the ‘final’ mass estimate. Sousa et al. MTorres 0.080 0.044 0.036 An initial inspection to our database showed no indication that (2008) MHenry 0.083 0.060 0.070 the large uncertainties associated with some stars’s global parame- MPadova 0.073 0.062 0.047 ters could be responsible for the discrepancies found between the MSpec 0.384 0.493 0.512 spectroscopic masses and the remaining predictions. For instance, Sousa et al. MTorres 0.161 0.064 0.048 on Fig. 4’s lower right panel we can notice that objects which (2011) MHenry 0.121 0.056 0.077 display large discrepancies between the spectroscopic and median MPadova 0.131 0.060 0.043 mass (i.e. that of the median of the four mass estimates) do not nec- essarily have large uncertainties on their surface gravity estimates. Indeed, even if we do not take into into account the data points for which there are such large uncertainties (for instance luminosity or ancies (as seen in Fig. 4 upper left panel). This should come as surface gravity uncertainty above 0.1 dex), which is the case for no surprise if we recall the well known correlations between the some of the largest mass/furthest stars, we still find a 2:1 relation mass, effective temperature and luminosity of main sequence stars between the median of the mass estimates and the spectroscopic (Kippenhahn & Weigert 1990) and the fact that a linear fit to masses (as seen in Fig. 4’s upper right panel). the spectroscopic masses and median of the mass estimates of all Likewise, we find no hints of a correlation between the targets’ of Sousa et al.’s targets yields a function of the type: MSpec = surface gravity or metal abundance and the differences between the 2.58MMedian − 1.53. mass estimates (c.f. Fig. 4’s lower left panel). On the other hand, the fact that Bruntt et al.’s (2010) data does Nevertheless, we found hints of a correlation between the not show a significant discrepancy between the mass estimate ob- stars’ effective temperature and luminosity and the mass discrep- tained through any method, and given that in this case surface grav-

c 2002 RAS, MNRAS 000, 1–?? 6 F. J. G. Pinheiro et al. ities were not obtained though spectroscopy, rises the suspicion that the problem may lie within the spectroscopic surface gravities. These discrepancies between the asteroseismic and spectro- scopic surface gravities are further corroborated by recent studies such as the one of Bruntt & et al. (2012). In this particular case we see that the differences between the spectroscopic surface gravities and the asteroseismic ones can be larger than the sum of the un- certainties associated with these parameters. Moreover, in Bruntt et al.’s (2012) Fig. 1, there are hints of a correlation between their tar- gets’ effective temperature and the discrepancy between the spec- troscopic and asteroseismic surface gravities. Furthermore, in their work Bruntt et al. propose a calibration of their micro-turbulence values, which have a deep impact on the inference of spectroscopic surface gravities. Comparing the targets’ spectroscopic mass and micro- turbulence shown in Fig. 5 it is noticeable a relation between these two parameters. This is expectable since both are correlated with the star’s effective temperature. This suggests once more that a problem with micro-turbulence might have an impact in the spec- troscopic surface gravity. A micro-turbulence recalibration for Sousa et al.’s 2008 and 2011 data goes far beyond the objectives of this work. Neverthe- less we can proceed to an empirical calibration of the spectroscopic masses given the median of the four mass estimates. Figure 6’s up- per panel shows the expected median of the mass estimates given an object’s spectroscopic mass (MSpec). The dashed line corresponds to a quadratic fit to the data: − 2 MMedian = 0.097 MSpec + 0.585 MSpec + 0.520 . (5) Figure 5. Comparison between the micro-turbulent velocity against the A more ambitious step consists in determining what should spectroscopic mass (top) and the median of the for mass estimates (bot- tom) for Sousa et al.’s data. Each data point’s colour provides an indication be the re-calibration of the surface gravity. From an observational of the discrepancy between its spectroscopic mass and the median of the point-of-view it is useful to compute this calibration as a function four mass estimates (as seen in Fig. 4). The dashed lines correspond to the of the targets’ effective temperature. In order to achieve this we best linear fits to the data, respectively: Vturb = 0.53 MSpec + 0.36 and took into account the median of the four mass estimates and the Vturb = 1.54 MMedian − 0.60 physical relations used in the direct method. Figure 6’s lower panel shows a comparison between the effective temperatures of Sousa at al.’s targets against the difference between the spectroscopic sur- consistent for Bruntt et al.’s 2008 and 2011 data. An extension of face gravities and those expected from the median of the four mass this analysis to Bruntt et al.’s (2010) data seems to indicate that, as estimates. The dashed line corresponds to a cubic fit to the data, in the case of the work of Bruntt et al. (Bruntt & et al. 2012), the which can be seen as a possible method for re-calibrating the spec- problem should lie within the spectroscopic surface gravities used troscopic surface gravities: in this work. Concerning the combination of the mass estimates, our results 3 indicate that the use of a weighted average and the median produce log(g ) − log(gSpec)= −290.03 log(T /5777) Median eff similar results. Indeed, our analysis does not show any particular − 2 − − 19.68 log(Teff /5777) 3.16 log(Teff /5777) 0.02 . (6) advantage in the use of a weighed mean in respect to the median. This function can be seen as an empirical calibration to the For the four methods evaluated here, Torres et al.’s empirical spectroscopic surface gravities if the object’s effective temperature approach is the one that gives the best agreement (i.e. the smallest if known. R.M.S.) in respect to the weighted mean of the four mass estimates. On the other hand, regarding the median, the best agreement occurs for Henry & McCarthy’s Mass-Luminosity relation (although Tor- res et al.’s method presents a similar agreement). 4 CONCLUSIONS & FUTURE WORK Finally, our final mass estimate allow us to derive an expres- In this study we have estimated the masses for about a thousand F, sion for "predicting" what should be the median of the four mass G and K type stars using four different methods. These approaches estimates given a set of spectroscopic masses. Of greater relevance include two empirical relationships, a comparison of global stel- is the expression obtained for an empirical "correction" to the spec- lar parameters against theoretical models and a method which "di- troscopic surface gravities derived using Sousa et al.’s approach rectly" takes into account the surface gravity and the luminosity- (Sousa & et al. 2008). It is of utmost importance to determine if radius-effective temperature relation. In the later case, spectro- this method (or a similar one) can be applied to spectroscopic sur- scopic surface gravities give rise to a spectroscopic mass estima- face gravities derived using other procedures. tion. A comparison between the different mass estimates shows that In the present work we have discussed the use of a weighted these methods produce fairly consistent results, except in the case mean in which the weights are proportional to the uncertainties as- 2 of the computation of the spectroscopic masses. The result is also sociated with each mass estimate (i.e.: wi = 1/σi ). In addition,

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Figure 4. Top left: position of Sousa et al.’s stars in the HR diagram. Top right: comparison between the spectroscopic mass and the median of the four mass estimates. Bottom left: comparison of the metal abundance against the discrepancy between spectroscopic and the median mass discrepancy. Bottom right: Same as the previous panel in respect to the surface gravity’s uncertainties. The circles correspond to the targets with a high luminosity uncertainty, ∆ log(L/L⊙) > 0.1. The color of each data provides an indication of the discrepancy between its spectroscopic mass and the median of the four mass estimates (as seen in the lower panels).

one can associate to each weight a quality factor Qi, which reflects M.S.C. is supported by an Investigador FCT contract funded by 2 each method’s reliability, corresponding to a weight: wi = Qi/σi ). FCT/MCTES (Portugal) and POPH/FSE (EC) and by funds from In order to calibrate these quality factors we would require a data the ERC, under FP7/EC, through the project FP7-SPACE-2012- sample for which stellar masses have been derived through an in- 31284. N.C.S, S.G.S., and A.M. acknowledge the support by the dependent method (such as the use of binary stars or asteroseismol- European Research Council/European Community under the FP7 ogy). Nevertheless, as shown here, the reliability of a given method through Starting Grant agreement number 239953. NCS is sup- clearly depends on the reliability of global stellar parameters re- ported by FCT through the Investigador FCT contract reference quired by each method and thus, on the way how each parameter IF/00169/2012 and POPH/FSE (EC) by FEDER funding through has been derived. Therefore, the calibration of the quality factors the program "Programa Operacional de Factores de Competitivi- for a specific sample might not be valid for a different sample. dade - COMPETE. We have used the CDS-Strasbourg Database. Concerning the spectroscopic surface gravities, Creevey & Thévenin (2012) and Creevey & et al. (2013) present an alternative to the use of asteroseismic surface gravities. Moreover, in the case REFERENCES of planetary transits one can use photometric light curves in order to derive accurate surface gravities (Torres et al. 2012 & Mortier et al. Andersen J., 1991, A&A Rev., 3, 91 2013). Such possibilities will be taken into account in a future in- Bigot L., et al. 2011, A&A, 534, L3 vestigation of the systematic difference between the spectroscopic Brown T. M., Gilliland R. L., Noyes R. W., Ramsey L. W., 1991, surface gravity estimations and the predictions resulting from other ApJ, 368, 599 approaches. Moreover we will also address the important issue of Bruntt H., et al. 2010, MNRAS, 405, 1907 the calibration of the spectroscopic predictions. Bruntt H., et al. 2012, MNRAS, 423, 122 Chaplin W. J., Basu S., Huber D., Serenelli A., Casagrande L., et al. 2014, ApJS, 210, 1 Creevey O. L., et al. 2013, MNRAS, 431, 2419 ACKNOWLEDGMENTS Creevey O. L., Thévenin F., 2012, in Boissier S., de Laverny The authors thank the anonymous referee for the valuable re- P., Nardetto N., Samadi R., Valls-Gabaud D., Wozniak H., eds, marks. Support was provided by FCT under project /PTDC/CTE- SF2A-2012: Proceedings of the Annual meeting of the French AST/66181/2006 and the /SFRH/BPD/37491/2007 research grant Society of Astronomy and Astrophysics Asteroseismic con- of F.J.G.P., both co-financed by the European Social Fund. straints for Gaia. pp 189–193

c 2002 RAS, MNRAS 000, 1–?? 8 F. J. G. Pinheiro et al.

Mayor M., Pepe F., Queloz D., et al. 2003, The Messenger, 114, 20 Metcalfe T., et al. 2010, ApJ, 723, 1583 Mortier A., Santos N., Sousa S., Israelian G., Mayor M., Udry S., 2013, A&A, 551, A112 Mortier A., Santos N. C., Sousa S. G., Fernandes J. M., Adibekyan V. Z., Delgado Mena E., Montalto M., Israelian G., 2013, A&A, 558, A106 Neves V., Bonfils X., Santos N. C., Delfosse X., Forveille T., Al- lard F., Udry S., 2013, A&A, 551, A36 Santos N. C., Israelian G., Mayor M., 2004, A&A, 415, 1153 Santos N. C., Israelian G., Mayor M., Bento J. P., Almeida P. C., Sousa S. G., Ecuvillon A., 2005, A&A, 437, 1127 Santos N. C., Sousa S. G., Mortier A., Neves V., Adibekyan V., Tsantaki M., Delgado Mena E., Bonfils X., Israelian G., Mayor M., Udry S., 2013, A&A, 556, A150 Sousa S. G., et al. 2008, A&A, 487, 373 Sousa S. G., Santos N. C., Israelian G., Lovis C., Mayor M., Silva P. B., Udry S., 2011, A&A, 526, A99 Sousa S. G., Santos N. C., Israelian G., Mayor M., Monteiro M. J. P. F. G., 2006, A&A, 458, 873 Sousa S. G., Santos N. C., Israelian G., Mayor M., Udry S., 2011, A&A, 533, A141 Torres G., 2010, AJ, 140, 1158 Torres G., Andersen J., Giménez A., 2010, A&A Rev., 18, 67 Torres G., Fischer D. A., Sozzetti A., Buchhave L. A., Winn J. N., Holman M. J., Carter J. A., 2012, ApJ, 757, 161 Ulrich R. K., 1986, ApJ, 306, L37 Figure 6. Top: empirical calibration of the stellar mass given the spectro- van Leeuwen F., 2007, A&A, 474, 653 scopic masses. Bottom: calibration of the surface gravities given an object’s Xia F., Fu Y.-N., 2010, Chinese Astronomy and Astrophysics, 34, effective temperature. The squares and black dots correspond, respectively, 277 to Sousa et al.’s 2008 and 2011 data. The black lines correspond to two polynomial fits to the data.

APPENDIX A: MASS ESTIMATES ACCRODING TO THE Fernandes J., Santos N., 2004, A&A, 427, 607 DIFFERENT METHODS Fernandes J., Vaz A., Vicente L., 2011, A&A, 532, A20 Flower P. J., 1996, ApJ, 469, 355 The following tables contain the mass estimates obtained according Gafeira R., Patacas C., Fernandes J., 2012, Ap&SS, 341, 405 the four methods presented here (plus the median of these four mass Henry T., 2004, in R. W. Hilditch H. H., Pavlovski K., eds, Spec- estimates) for Sousa et al.’s 2008 and 2011 targets and those of troscopically and Spatially Resolving the Components of the Bruntt et al. (2010). Close Binary Stars, Proceedings of the Workshop held 20-24 Oc- tober 2003 in Dubrovnik, Croatia The mass-luminosity relation from end to end. ASP Conference Series, Vol. 318. San Fran- cisco: Astronomical Society of the Pacific, pp 159–165 Henry T., McCarthy D. J., 1993, AJ, 106, 773 Huber D., Ireland M. J., Bedding T. R., Brandão I. M., et al. 2012, ApJ, 760, 32 Johnson J. A., Aller K. M., Howard A. W., Crepp J. R., 2010, PASP, 122, 905 Kippenhahn R., Weigert A., 1990, Stellar Structure and Evolution. Springer-Verlag Kjeldsen H., Bedding T. R., 1995, A&A, 293, 87 Kjeldsen H., Bedding T. R., Christensen-Dalsgaard J., 2009, in Pont F., Sasselov D., Holman M. J., eds, IAU Symposium Vol. 253 of IAU Symposium, Measurements of Stellar Properties through Asteroseismology: A Tool for Planet Transit Studies. pp 309–317 Lo Curto G., Mayor M., Benz W., Bouchy F., Lovis C., Moutou C., Naef D., Pepe F., Queloz D., Santos N. C., Segransan D., Udry S., 2010, A&A, 512, A48 Mathur S., Metcalfe T. S., Woitaszek M., Bruntt H., Verner G. A., et al. 2012, ApJ, 749, 152

c 2002 RAS, MNRAS 000, 1–?? On the mass estimation for FGK stars:comparison of several methods 9

Table A1. Mass estimate for Sousa et al’s 2008 targets according to different methods (in solar units).

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

HD 55 0.639 0.046 0.340 0.349 0.704 0.055 0.600 0.054 0.619 0.038 HD 16714 0.940 0.060 0.777 0.119 0.982 0.074 0.833 0.051 0.886 0.059 HD 142 1.205 0.079 2.703 0.779 1.298 0.097 1.300 0.052 1.299 0.047 HD 17051 1.202 0.077 1.486 0.372 1.177 0.088 1.200 0.051 1.201 0.049 HD 283 0.768 0.050 0.632 0.182 0.858 0.066 0.716 0.053 0.742 0.048 HD 17970 0.777 0.053 0.616 0.231 0.873 0.066 0.731 0.052 0.754 0.052 HD 361 1.026 0.065 1.264 0.118 1.057 0.079 1.046 0.051 1.051 0.043 HD 18386 1.008 0.066 0.618 0.160 0.944 0.072 0.950 0.056 0.947 0.045 HD 750 0.812 0.054 0.492 0.188 0.845 0.065 0.743 0.053 0.777 0.034 HD 18719 0.896 0.059 0.633 0.204 0.904 0.069 0.814 0.054 0.855 0.038 HD 870 0.926 0.060 0.620 0.136 0.921 0.069 0.852 0.054 0.887 0.039 HD 19034 0.875 0.056 0.734 0.123 0.971 0.073 0.762 0.051 0.819 0.048 HD 967 0.835 0.053 0.964 0.167 0.989 0.075 0.738 0.051 0.899 0.060 HD 19467 1.037 0.066 1.057 0.054 1.124 0.084 0.911 0.051 1.047 0.040 HD 1237 0.983 0.064 0.877 0.265 0.966 0.072 0.957 0.054 0.962 0.043 HD 19994 1.246 0.081 2.890 0.558 1.382 0.103 1.346 0.064 1.364 0.062 HD 1320 0.951 0.060 0.901 0.096 1.002 0.075 0.866 0.054 0.926 0.046 HD 20003 0.990 0.064 0.828 0.188 0.991 0.074 0.900 0.054 0.945 0.052 HD 1388 1.103 0.070 1.152 0.099 1.133 0.085 1.070 0.052 1.118 0.040 HD 20407 0.957 0.061 1.060 0.045 1.060 0.079 0.904 0.052 1.008 0.034 HD 1461 1.111 0.071 1.049 0.129 1.097 0.082 1.058 0.052 1.078 0.059 HD 20619 0.964 0.061 0.970 0.094 1.014 0.076 0.926 0.056 0.967 0.038 HD 1581 1.043 0.066 1.255 0.148 1.107 0.083 1.018 0.053 1.075 0.044 HD 20781 0.903 0.059 0.613 0.161 0.916 0.070 0.811 0.052 0.857 0.034 HD 2025 0.740 0.049 0.597 0.305 0.793 0.061 0.700 0.055 0.720 0.038 HD 20782 1.053 0.067 1.058 0.056 1.105 0.083 0.967 0.052 1.055 0.039 HD 2071 1.006 0.064 0.895 0.083 1.017 0.076 0.985 0.054 0.996 0.036 HD 20794 0.873 0.056 0.787 0.091 0.974 0.073 0.796 0.051 0.834 0.036 HD 2638 0.922 0.063 0.694 0.349 0.904 0.071 0.836 0.060 0.870 0.061 HD 20807 1.001 0.064 1.096 0.132 1.057 0.079 0.953 0.053 1.029 0.044 HD 3569 0.803 0.052 0.695 0.248 0.860 0.067 0.748 0.053 0.776 0.054 HD 21019 1.047 0.067 1.552 0.120 1.374 0.102 1.072 0.051 1.223 0.048 HD 3823 1.083 0.069 1.455 0.111 1.251 0.093 1.043 0.052 1.167 0.058 HD 21209A 0.709 0.056 0.305 0.295 0.741 0.060 0.657 0.054 0.683 0.043 HD 4208 0.939 0.060 0.812 0.090 0.993 0.075 0.822 0.052 0.881 0.043 HD 21411 0.898 0.057 0.902 0.136 0.964 0.072 0.807 0.055 0.900 0.054 HD 4307 1.120 0.072 1.311 0.105 1.304 0.097 1.033 0.051 1.212 0.051 HD 21693 0.974 0.063 0.677 0.120 0.961 0.072 0.877 0.054 0.919 0.044 HD 4308 0.951 0.061 0.942 0.114 1.053 0.079 0.841 0.051 0.947 0.065 HD 21749 0.772 0.116 0.380 2.460 0.752 0.060 0.741 0.058 0.746 0.074 HD 4915 0.953 0.061 0.883 0.123 0.983 0.074 0.945 0.053 0.949 0.033 HD 21938 0.956 0.061 0.955 0.085 1.080 0.081 0.840 0.051 0.956 0.059 HD 6348 0.753 0.049 0.644 0.197 0.850 0.066 0.683 0.052 0.718 0.051 HD 22049 0.844 0.055 0.639 0.188 0.850 0.064 0.801 0.051 0.823 0.034 HD 6673 0.774 0.053 0.540 0.322 0.810 0.063 0.722 0.055 0.748 0.045 HD 22610 0.810 0.055 0.490 0.241 0.825 0.064 0.736 0.053 0.773 0.032 HD 6735 1.105 0.070 1.314 0.110 1.144 0.085 1.134 0.052 1.139 0.040 HD 22879 0.880 0.056 1.037 0.082 1.073 0.080 0.785 0.051 0.958 0.050 HD 7134 1.030 0.065 1.147 0.106 1.128 0.084 0.940 0.052 1.079 0.048 HD 23079 1.065 0.067 1.323 0.110 1.130 0.084 1.036 0.052 1.098 0.043 HD 7199 1.035 0.071 0.737 0.269 0.981 0.074 0.911 0.057 0.946 0.050 HD 23249 1.114 0.088 1.395 0.479 1.280 0.095 1.185 0.054 1.232 0.070 HD 7449 1.072 0.068 1.196 0.159 1.106 0.083 1.084 0.052 1.095 0.047 HD 23356 0.799 0.054 0.590 0.327 0.828 0.062 0.745 0.055 0.772 0.046 HD 8326 0.830 0.060 0.627 0.579 0.836 0.065 0.788 0.063 0.809 0.054 HD 23456 1.050 0.067 1.760 0.213 1.191 0.089 0.998 0.052 1.120 0.050 HD 8389A 1.010 0.073 0.755 0.476 0.955 0.072 0.871 0.060 0.913 0.068 HD 24331 0.763 0.051 0.572 0.259 0.813 0.062 0.716 0.053 0.739 0.049 HD 8406 0.999 0.063 0.939 0.075 1.014 0.076 1.002 0.052 1.001 0.040 HD 24892 1.019 0.068 1.167 0.192 1.236 0.092 0.947 0.052 1.093 0.063 HD 8638 0.897 0.058 0.826 0.206 0.985 0.075 0.793 0.052 0.861 0.067 HD 25105 0.888 0.058 0.693 0.200 0.909 0.069 0.804 0.055 0.846 0.041 HD 8828 0.911 0.058 0.721 0.109 0.933 0.070 0.829 0.055 0.870 0.035 HD 25120 0.836 0.055 0.611 0.237 0.860 0.065 0.770 0.054 0.803 0.041 HD 8859 0.963 0.062 0.724 0.148 0.969 0.073 0.858 0.054 0.910 0.045 HD 25565 0.898 0.060 0.597 0.283 0.870 0.067 0.883 0.060 0.877 0.041 HD 8912 0.886 0.059 0.536 0.201 0.868 0.067 0.805 0.058 0.837 0.042 HD 25673 0.776 0.051 0.443 0.222 0.818 0.068 0.703 0.053 0.740 0.037 HD 9246 0.736 0.049 0.426 0.226 0.787 0.065 0.700 0.054 0.718 0.036 HD 26965A 0.831 0.056 0.592 0.209 0.886 0.066 0.797 0.052 0.814 0.038 HD 9782 1.145 0.073 1.186 0.103 1.148 0.086 1.155 0.052 1.152 0.043 HD 27063 1.060 0.067 0.814 0.124 1.022 0.077 1.043 0.052 1.032 0.038 HD 9796 0.852 0.056 0.495 0.161 0.867 0.067 0.761 0.052 0.807 0.036 HD 27894 0.879 0.076 0.558 0.884 0.844 0.066 0.800 0.066 0.822 0.067 HD 10002 0.972 0.065 0.745 0.244 0.945 0.071 0.879 0.060 0.912 0.062 HD 28185 1.077 0.069 1.048 0.191 1.062 0.080 1.028 0.054 1.055 0.049 HD 10166 0.815 0.053 0.421 0.208 0.819 0.068 0.756 0.055 0.786 0.037 HD 28471 1.048 0.066 0.960 0.050 1.080 0.081 0.950 0.052 1.004 0.039 HD 10180 1.120 0.071 1.214 0.148 1.146 0.086 1.077 0.052 1.133 0.048 HD 28701 0.965 0.061 1.119 0.101 1.085 0.081 0.859 0.051 1.025 0.043 HD 10647 1.132 0.072 1.670 0.267 1.153 0.086 1.150 0.051 1.151 0.043 HD 28821 1.005 0.064 1.002 0.064 1.068 0.080 0.896 0.052 1.003 0.048 HD 10700 0.819 0.052 0.697 0.081 0.918 0.069 0.770 0.051 0.795 0.033 HD 30278 0.922 0.060 0.714 0.119 0.956 0.072 0.824 0.051 0.873 0.040 HD 11226 1.174 0.074 1.445 0.123 1.244 0.093 1.151 0.052 1.209 0.046 HD 30306 1.056 0.068 0.898 0.151 1.049 0.078 0.939 0.054 0.994 0.048 HD 11505 1.006 0.064 1.130 0.113 1.112 0.083 0.892 0.052 1.059 0.050 HD 31527 1.038 0.066 1.132 0.105 1.101 0.082 0.985 0.052 1.070 0.046 HD 11683 0.807 0.056 0.512 0.320 0.833 0.065 0.741 0.053 0.774 0.045 HD 31560 0.785 0.067 0.357 0.506 0.768 0.059 0.726 0.055 0.747 0.049 HD 11964A 1.156 0.076 1.147 0.133 1.274 0.095 1.100 0.052 1.152 0.067 HD 31822 1.046 0.066 1.137 0.163 1.072 0.080 1.053 0.052 1.062 0.054 HD 12345 0.902 0.058 0.661 0.153 0.925 0.071 0.805 0.054 0.853 0.044 HD 32724 1.073 0.068 1.270 0.110 1.209 0.090 0.969 0.051 1.141 0.049 HD 12387 0.985 0.064 1.108 0.242 1.089 0.081 0.873 0.051 1.037 0.063 HD 33725 0.886 0.058 0.677 0.165 0.923 0.070 0.804 0.052 0.845 0.045 HD 12617 0.827 0.065 0.537 0.689 0.806 0.064 0.776 0.063 0.791 0.052 HD 34449 1.034 0.066 0.935 0.129 1.035 0.078 1.028 0.051 1.031 0.041 HD 13060 0.938 0.065 0.497 0.225 0.894 0.068 0.852 0.060 0.873 0.039 HD 34688 0.846 0.055 0.544 0.197 0.860 0.068 0.766 0.053 0.806 0.035 HD 13724 1.115 0.071 1.232 0.161 1.082 0.081 1.115 0.052 1.115 0.050 HD 35854 0.794 0.055 0.559 0.311 0.818 0.062 0.752 0.055 0.773 0.033 HD 13789 0.784 0.065 0.399 0.459 0.780 0.061 0.726 0.053 0.753 0.046 HD 36003 0.739 0.068 0.322 0.570 0.744 0.057 0.700 0.052 0.719 0.037 HD 13808 0.834 0.056 0.561 0.215 0.866 0.065 0.770 0.052 0.802 0.040 HD 36108 1.066 0.068 1.408 0.176 1.214 0.090 1.028 0.064 1.140 0.058 HD 14374 0.938 0.060 0.792 0.169 0.944 0.072 0.885 0.057 0.912 0.048 HD 36379 1.116 0.071 1.427 0.118 1.257 0.094 1.098 0.053 1.187 0.055 HD 14635 0.782 0.063 0.408 0.652 0.760 0.062 0.764 0.058 0.762 0.051 HD 37962 0.978 0.063 0.961 0.172 1.027 0.077 0.902 0.053 0.970 0.062 HD 14680 0.808 0.056 0.524 0.353 0.825 0.064 0.745 0.055 0.776 0.049 HD 37986 1.082 0.073 0.664 0.173 1.004 0.075 0.955 0.058 0.980 0.046 HD 14744 0.795 0.054 0.616 0.357 0.834 0.067 0.749 0.053 0.772 0.046 HD 38277 1.086 0.069 1.365 0.118 1.193 0.089 1.041 0.051 1.139 0.050 HD 14747 0.897 0.057 0.868 0.086 0.996 0.075 0.796 0.051 0.882 0.050 HD 38382 1.138 0.072 1.274 0.099 1.157 0.086 1.157 0.052 1.157 0.036 HD 15337 0.913 0.062 0.526 0.256 0.873 0.068 0.843 0.061 0.858 0.047 HD 38858 0.972 0.062 1.017 0.051 1.027 0.077 0.954 0.054 0.994 0.043 HD 16141 1.183 0.075 1.102 0.098 1.212 0.090 1.100 0.053 1.142 0.055 HD 38973 1.133 0.072 1.220 0.094 1.152 0.086 1.116 0.053 1.142 0.049 HD 16270 0.805 0.069 0.451 0.797 0.786 0.061 0.750 0.058 0.768 0.048 HD 39091 1.140 0.073 1.213 0.141 1.150 0.086 1.142 0.053 1.146 0.031 HD 16297 0.946 0.061 0.859 0.177 0.960 0.072 0.877 0.056 0.911 0.046 HD 39194 0.763 0.049 0.681 0.161 0.867 0.065 0.707 0.052 0.735 0.043 HD 16417 1.198 0.076 1.328 0.099 1.280 0.095 1.217 0.052 1.248 0.041 HD 40105 1.114 0.078 1.201 0.234 1.264 0.094 1.143 0.051 1.172 0.067

c 2002 RAS, MNRAS 000, 1–?? 10 F. J. G. Pinheiro et al.

Table A1. Continuation

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

HD 40307 0.772 0.056 0.446 0.451 0.794 0.060 0.740 0.054 0.756 0.033 HD 86140 0.753 0.051 0.562 0.305 0.788 0.062 0.716 0.057 0.734 0.041 HD 40397 0.965 0.062 0.807 0.141 0.999 0.075 0.852 0.051 0.909 0.051 HD 86171 0.889 0.057 0.669 0.122 0.917 0.070 0.807 0.053 0.848 0.040 HD 44120 1.220 0.078 1.521 0.116 1.302 0.097 1.236 0.051 1.269 0.054 HD 87521 0.809 0.062 0.414 0.392 0.793 0.064 0.749 0.055 0.771 0.049 HD 44420 1.155 0.074 1.035 0.136 1.109 0.083 1.090 0.053 1.099 0.042 HD 88084 1.028 0.065 0.988 0.095 1.067 0.080 0.944 0.052 1.008 0.056 HD 44447 1.073 0.068 1.312 0.103 1.195 0.089 1.012 0.051 1.134 0.039 HD 88218 1.136 0.072 1.337 0.103 1.289 0.096 1.070 0.054 1.212 0.046 HD 44573 0.839 0.057 0.585 0.303 0.840 0.064 0.779 0.060 0.809 0.046 HD 88656 0.859 0.056 0.672 0.218 0.887 0.068 0.790 0.053 0.825 0.047 HD 44594 1.122 0.071 1.040 0.083 1.108 0.083 1.075 0.052 1.092 0.033 HD 88742 1.082 0.068 1.237 0.102 1.102 0.082 1.100 0.051 1.101 0.042 HD 45184 1.078 0.068 1.146 0.092 1.092 0.082 1.067 0.054 1.085 0.042 HD 89454 1.059 0.067 0.951 0.142 1.032 0.077 1.052 0.051 1.042 0.041 HD 45289 1.062 0.067 1.122 0.041 1.129 0.084 0.987 0.052 1.092 0.031 HD 90156 0.939 0.060 0.898 0.081 0.994 0.074 0.843 0.052 0.919 0.043 HD 45364 0.934 0.060 0.623 0.092 0.945 0.071 0.824 0.051 0.879 0.035 HD 90711 1.026 0.068 0.749 0.201 0.970 0.073 0.969 0.059 0.969 0.042 HD 47186 1.101 0.071 0.970 0.170 1.075 0.080 1.018 0.052 1.047 0.053 HD 90812 0.807 0.052 0.537 0.149 0.843 0.065 0.729 0.053 0.768 0.032 HD 48611 0.844 0.054 0.736 0.262 0.907 0.074 0.767 0.053 0.806 0.060 HD 92588 1.166 0.086 1.228 0.307 1.321 0.098 1.244 0.051 1.236 0.069 HD 50590 0.776 0.058 0.488 0.416 0.811 0.065 0.732 0.054 0.754 0.041 HD 92719 1.023 0.065 0.999 0.129 1.036 0.077 1.028 0.051 1.026 0.030 HD 50806 1.131 0.073 1.128 0.133 1.223 0.091 1.024 0.051 1.130 0.068 HD 92788 1.122 0.072 0.959 0.166 1.073 0.080 1.079 0.054 1.076 0.044 HD 51608 0.941 0.061 0.646 0.146 0.945 0.071 0.834 0.051 0.888 0.031 HD 93083 0.890 0.062 0.636 0.359 0.877 0.067 0.818 0.063 0.848 0.050 HD 52265 1.229 0.079 1.256 0.143 1.212 0.090 1.227 0.054 1.228 0.050 HD 93380 0.647 0.105 0.175 1.346 0.669 0.059 0.568 0.062 0.608 0.076 HD 52919 0.744 0.063 0.364 0.577 0.750 0.059 0.700 0.055 0.722 0.042 HD 93385 1.114 0.071 1.240 0.109 1.148 0.086 1.092 0.053 1.131 0.038 HD 55693 1.166 0.075 1.355 0.222 1.152 0.086 1.124 0.053 1.159 0.055 HD 94151 1.022 0.065 0.886 0.092 1.030 0.077 0.925 0.053 0.974 0.048 HD 59468 1.027 0.066 0.896 0.107 1.036 0.077 0.944 0.053 0.985 0.047 HD 95456 1.259 0.081 1.691 0.269 1.318 0.098 1.283 0.052 1.301 0.056 HD 59711A 1.002 0.064 0.997 0.103 1.043 0.078 0.935 0.053 1.000 0.042 HD 95521 1.002 0.064 0.955 0.088 1.028 0.077 0.967 0.054 0.985 0.033 HD 63454 0.841 0.068 0.374 0.388 0.798 0.062 0.765 0.055 0.782 0.046 HD 96423 1.081 0.069 0.951 0.083 1.079 0.081 0.998 0.052 1.038 0.046 HD 63765 0.927 0.059 0.674 0.096 0.941 0.071 0.822 0.052 0.874 0.041 HD 96700 1.037 0.066 1.209 0.102 1.138 0.085 0.950 0.051 1.088 0.045 HD 65216 0.967 0.061 0.798 0.078 0.993 0.074 0.881 0.054 0.924 0.040 HD 97037 1.089 0.069 1.233 0.102 1.170 0.087 1.038 0.052 1.130 0.050 HD 65277 0.736 0.058 0.426 0.545 0.770 0.061 0.687 0.056 0.711 0.051 HD 97343 0.950 0.061 0.743 0.097 0.968 0.073 0.850 0.051 0.900 0.033 HD 65562 0.852 0.058 0.552 0.257 0.863 0.066 0.777 0.053 0.815 0.041 HD 97998 0.914 0.058 1.031 0.097 1.002 0.075 0.880 0.054 0.958 0.043 HD 65907A 1.002 0.064 1.337 0.101 1.111 0.083 0.931 0.052 1.057 0.047 HD 98281 0.892 0.058 0.680 0.123 0.936 0.070 0.800 0.051 0.846 0.041 HD 66221 1.063 0.068 0.960 0.178 1.050 0.079 1.003 0.055 1.026 0.057 HD 98356 0.956 0.063 0.693 0.217 0.930 0.071 0.879 0.057 0.905 0.050 HD 66428 1.131 0.075 1.006 0.283 1.109 0.083 1.034 0.053 1.072 0.051 HD 100508 1.058 0.073 0.939 0.388 1.001 0.075 0.939 0.065 0.970 0.062 HD 67458 1.022 0.065 1.171 0.102 1.071 0.080 1.033 0.052 1.052 0.031 HD 100777 1.075 0.070 0.967 0.230 1.063 0.080 0.963 0.053 1.015 0.061 HD 68607 0.920 0.062 0.633 0.253 0.900 0.069 0.838 0.058 0.869 0.045 HD 101581 0.681 0.049 0.333 0.305 0.723 0.055 0.641 0.053 0.661 0.032 HD 68978A 1.101 0.070 1.204 0.093 1.112 0.083 1.111 0.051 1.111 0.038 HD 101930 0.921 0.065 0.672 0.378 0.904 0.069 0.843 0.058 0.874 0.045 HD 69655 1.055 0.067 1.178 0.144 1.125 0.084 0.982 0.052 1.090 0.042 HD 102117 1.125 0.073 1.255 0.209 1.149 0.086 1.043 0.055 1.137 0.049 HD 69830 0.945 0.061 0.715 0.114 0.954 0.071 0.834 0.053 0.890 0.043 HD 102365 0.944 0.061 0.904 0.101 1.018 0.076 0.836 0.052 0.924 0.055 HD 70642 1.075 0.069 0.945 0.156 1.050 0.078 1.042 0.054 1.046 0.051 HD 102438 0.934 0.060 0.770 0.099 0.992 0.074 0.822 0.051 0.878 0.041 HD 70889 1.141 0.072 1.152 0.100 1.112 0.083 1.128 0.051 1.134 0.039 HD 103949 0.790 0.061 0.523 0.668 0.795 0.062 0.746 0.059 0.768 0.053 HD 71334 1.024 0.065 0.872 0.123 1.051 0.079 0.914 0.052 0.969 0.050 HD 104006 0.690 0.045 0.656 0.185 0.823 0.063 0.647 0.052 0.673 0.064 HD 71479 1.187 0.075 1.553 0.134 1.209 0.090 1.184 0.052 1.198 0.052 HD 104067 0.816 0.058 0.594 0.427 0.831 0.063 0.770 0.058 0.793 0.053 HD 71835 0.962 0.062 0.718 0.138 0.966 0.073 0.850 0.054 0.906 0.040 HD 104263 0.999 0.065 0.819 0.160 1.015 0.076 0.881 0.052 0.940 0.045 HD 72579 1.056 0.069 0.736 0.126 1.019 0.076 0.921 0.053 0.970 0.048 HD 104982 0.983 0.062 0.909 0.094 1.026 0.077 0.887 0.052 0.946 0.044 HD 72673 0.820 0.053 0.608 0.101 0.881 0.066 0.744 0.051 0.782 0.032 HD 105671 0.774 0.071 0.408 0.897 0.758 0.059 0.753 0.056 0.755 0.057 HD 72769 1.112 0.072 0.959 0.160 1.069 0.080 1.001 0.053 1.035 0.065 HD 105837 0.944 0.060 1.321 0.175 1.091 0.082 0.843 0.052 1.018 0.050 HD 73121 1.203 0.077 1.652 0.195 1.301 0.097 1.235 0.051 1.268 0.044 HD 106116 1.071 0.068 0.999 0.135 1.065 0.080 1.008 0.052 1.036 0.039 HD 73256 1.041 0.068 0.787 0.212 0.985 0.074 1.017 0.052 1.001 0.046 HD 106275 0.834 0.056 0.654 0.292 0.859 0.065 0.781 0.054 0.807 0.048 HD 73524 1.160 0.074 1.243 0.151 1.151 0.086 1.171 0.052 1.165 0.043 HD 107148 1.148 0.073 1.228 0.116 1.126 0.084 1.096 0.054 1.137 0.041 HD 74014 1.075 0.070 0.819 0.143 1.032 0.077 0.967 0.053 1.000 0.051 HD 108147 1.223 0.078 1.462 0.170 1.206 0.090 1.223 0.052 1.223 0.044 HD 75289 1.259 0.080 1.269 0.148 1.213 0.090 1.227 0.052 1.243 0.048 HD 108309 1.147 0.074 1.167 0.141 1.196 0.089 1.041 0.051 1.157 0.062 HD 76151 1.073 0.068 1.051 0.082 1.053 0.079 1.063 0.051 1.058 0.034 HD 109200 0.804 0.052 0.682 0.175 0.862 0.065 0.767 0.051 0.785 0.041 HD 78429 1.099 0.070 1.112 0.091 1.131 0.084 1.022 0.052 1.105 0.052 HD 109409 1.270 0.082 1.608 0.180 1.339 0.100 1.300 0.052 1.319 0.041 HD 78538 1.032 0.066 0.974 0.156 1.030 0.077 1.037 0.051 1.031 0.047 HD 109423 0.847 0.056 0.492 0.184 0.830 0.064 0.779 0.055 0.804 0.036 HD 78558 0.951 0.061 1.207 0.105 1.123 0.084 0.855 0.051 1.037 0.047 HD 110619 0.901 0.057 0.770 0.084 0.956 0.072 0.819 0.054 0.860 0.034 HD 78612 1.056 0.067 1.287 0.115 1.209 0.090 0.941 0.051 1.133 0.061 HD 111031 1.139 0.073 1.219 0.151 1.130 0.084 1.083 0.052 1.134 0.044 HD 78747 0.895 0.057 1.134 0.099 1.077 0.081 0.791 0.051 0.986 0.049 HD 111232 0.875 0.056 0.841 0.113 0.981 0.073 0.786 0.051 0.858 0.045 HD 80883 0.853 0.056 0.642 0.182 0.894 0.068 0.786 0.053 0.819 0.049 HD 112540 0.928 0.059 0.907 0.126 0.969 0.073 0.877 0.058 0.917 0.056 HD 81639 0.953 0.061 0.747 0.111 0.983 0.074 0.837 0.052 0.895 0.040 HD 114386 0.814 0.072 0.462 0.816 0.811 0.065 0.758 0.062 0.784 0.057 HD 82342 0.705 0.051 0.383 0.314 0.766 0.059 0.669 0.054 0.687 0.040 HD 114613 1.279 0.082 1.429 0.104 1.389 0.103 1.230 0.051 1.334 0.062 HD 82516 0.867 0.060 0.717 0.405 0.881 0.067 0.810 0.054 0.839 0.053 HD 114729 1.078 0.069 1.164 0.098 1.230 0.092 0.952 0.053 1.121 0.073 HD 82943 1.179 0.075 1.258 0.100 1.149 0.086 1.181 0.052 1.180 0.051 HD 114747 0.932 0.065 0.662 0.377 0.890 0.068 0.900 0.063 0.895 0.054 HD 83443 1.061 0.071 1.009 0.374 1.020 0.077 0.969 0.059 1.015 0.073 HD 114783 0.887 0.061 0.595 0.294 0.872 0.066 0.814 0.061 0.843 0.052 HD 83529 1.054 0.067 1.165 0.051 1.156 0.086 0.977 0.051 1.105 0.041 HD 114853 0.977 0.062 0.905 0.082 1.030 0.077 0.882 0.052 0.941 0.042 HD 85119 0.897 0.057 0.647 0.131 0.897 0.069 0.847 0.057 0.872 0.043 HD 115585 1.174 0.077 1.208 0.250 1.168 0.087 1.030 0.058 1.171 0.065 HD 85390 0.883 0.060 0.614 0.269 0.889 0.067 0.801 0.055 0.842 0.042 HD 115617 1.007 0.064 0.785 0.091 1.012 0.076 0.874 0.053 0.940 0.044 HD 85512 0.719 0.079 0.254 0.964 0.708 0.055 0.647 0.052 0.677 0.060 HD 115674 0.968 0.062 0.844 0.112 0.993 0.074 0.916 0.058 0.942 0.038 HD 86065 0.826 0.057 0.530 0.375 0.815 0.065 0.799 0.057 0.807 0.049 HD 116858 0.786 0.053 0.630 0.342 0.827 0.065 0.741 0.055 0.763 0.050

c 2002 RAS, MNRAS 000, 1–?? On the mass estimation for FGK stars:comparison of several methods 11

Table A1. Continuation

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

HD 116920 0.798 0.054 0.521 0.216 0.824 0.063 0.736 0.053 0.767 0.046 HD 160691 1.181 0.077 1.183 0.185 1.182 0.088 1.099 0.051 1.182 0.065 HD 117105 1.017 0.065 1.198 0.110 1.133 0.085 0.922 0.052 1.075 0.047 HD 161098 0.927 0.059 0.821 0.092 0.983 0.074 0.822 0.052 0.875 0.052 HD 117207 1.109 0.072 0.954 0.163 1.089 0.081 1.017 0.052 1.053 0.059 HD 161612 1.042 0.067 0.944 0.170 1.018 0.076 1.012 0.054 1.015 0.044 HD 117618 1.123 0.071 1.288 0.115 1.168 0.087 1.090 0.052 1.146 0.050 HD 162020 0.779 0.058 0.537 0.569 0.795 0.065 0.743 0.058 0.761 0.059 HD 119638 1.095 0.070 1.153 0.145 1.149 0.086 1.054 0.052 1.122 0.047 HD 162236 0.910 0.059 0.635 0.161 0.915 0.071 0.813 0.054 0.861 0.039 HD 119782 0.870 0.057 0.695 0.211 0.896 0.068 0.805 0.053 0.838 0.060 HD 162396 1.096 0.070 1.577 0.121 1.311 0.098 1.088 0.052 1.204 0.050 HD 121504 1.141 0.072 1.462 0.197 1.157 0.086 1.172 0.051 1.164 0.034 HD 165920 1.010 0.069 0.791 0.293 0.966 0.073 0.900 0.061 0.933 0.067 HD 122862 1.142 0.073 1.405 0.108 1.281 0.095 1.147 0.051 1.214 0.051 HD 166724 0.859 0.058 0.532 0.255 0.853 0.069 0.777 0.054 0.815 0.040 HD 123265 1.015 0.069 0.599 0.201 0.958 0.073 0.885 0.057 0.922 0.041 HD 167359 0.890 0.058 0.685 0.181 0.917 0.070 0.799 0.054 0.845 0.046 HD 124106 0.827 0.055 0.654 0.265 0.858 0.066 0.784 0.053 0.805 0.047 HD 168159 0.760 0.055 0.400 0.357 0.762 0.062 0.717 0.054 0.739 0.044 HD 124292 0.948 0.061 0.729 0.129 0.978 0.073 0.844 0.051 0.896 0.034 HD 168746 0.999 0.064 0.965 0.136 1.070 0.080 0.889 0.051 0.982 0.067 HD 124364 0.929 0.059 0.732 0.099 0.957 0.072 0.839 0.054 0.884 0.038 HD 168871 1.088 0.069 1.415 0.116 1.184 0.088 1.057 0.052 1.136 0.053 HD 125072 0.859 0.070 0.716 1.135 0.835 0.063 0.842 0.056 0.839 0.053 HD 169830 1.347 0.087 1.808 0.206 1.438 0.107 1.400 0.051 1.419 0.062 HD 125184 1.216 0.083 1.162 0.237 1.244 0.093 1.100 0.051 1.189 0.059 HD 170493 0.848 0.096 0.344 0.941 0.789 0.061 0.758 0.059 0.774 0.049 HD 125455 0.834 0.054 0.738 0.241 0.876 0.066 0.783 0.054 0.808 0.048 HD 171665 1.013 0.064 0.846 0.055 1.024 0.077 0.924 0.052 0.968 0.039 HD 125881 1.123 0.071 1.263 0.163 1.128 0.084 1.129 0.051 1.128 0.032 HD 171990 1.249 0.080 1.747 0.132 1.406 0.105 1.305 0.055 1.355 0.055 HD 126525 1.007 0.064 0.848 0.089 1.036 0.078 0.890 0.052 0.948 0.038 HD 172513 0.971 0.062 0.735 0.122 0.971 0.073 0.877 0.055 0.924 0.042 HD 128674 0.894 0.057 0.984 0.180 0.995 0.075 0.796 0.051 0.939 0.054 HD 174545 0.956 0.067 0.857 0.486 0.955 0.072 0.871 0.055 0.913 0.067 HD 129642 0.828 0.060 0.715 0.653 0.860 0.066 0.783 0.056 0.805 0.050 HD 176157 0.864 0.058 0.568 0.196 0.876 0.067 0.783 0.053 0.823 0.044 HD 130322 0.951 0.062 0.565 0.150 0.921 0.070 0.858 0.055 0.889 0.056 HD 176986 0.844 0.058 0.598 0.347 0.846 0.065 0.786 0.058 0.815 0.044 HD 130930 0.849 0.059 0.712 0.479 0.872 0.068 0.797 0.055 0.823 0.057 HD 177409 1.061 0.067 1.024 0.102 1.062 0.079 1.069 0.051 1.062 0.039 HD 130992 0.774 0.056 0.566 0.514 0.790 0.061 0.764 0.055 0.769 0.034 HD 177565 1.041 0.067 0.874 0.108 1.033 0.077 0.963 0.053 0.998 0.043 HD 132648 0.865 0.055 0.774 0.117 0.936 0.070 0.776 0.051 0.821 0.053 HD 177758 0.944 0.060 1.382 0.112 1.157 0.086 0.859 0.051 1.051 0.061 HD 134060 1.140 0.073 1.247 0.153 1.143 0.085 1.134 0.052 1.141 0.046 HD 179949 1.222 0.078 1.637 0.260 1.205 0.090 1.231 0.051 1.227 0.034 HD 134606 1.093 0.071 1.085 0.225 1.079 0.081 1.002 0.053 1.082 0.060 HD 180409 1.053 0.067 1.166 0.100 1.093 0.082 1.068 0.051 1.081 0.032 HD 134664 1.081 0.068 1.152 0.121 1.067 0.080 1.100 0.052 1.090 0.036 HD 181433 0.914 0.100 0.484 1.477 0.833 0.065 0.820 0.064 0.827 0.066 HD 134985 0.753 0.054 0.542 0.338 0.847 0.069 0.695 0.055 0.724 0.054 HD 183658 1.075 0.068 1.088 0.100 1.101 0.082 1.011 0.052 1.081 0.045 HD 134987 1.145 0.074 1.068 0.176 1.134 0.085 1.051 0.053 1.101 0.051 HD 183783 0.730 0.067 0.368 0.586 0.756 0.060 0.700 0.055 0.715 0.035 HD 136352 0.954 0.061 0.963 0.077 1.059 0.079 0.841 0.051 0.958 0.043 HD 183870 0.826 0.055 0.630 0.271 0.842 0.063 0.797 0.058 0.812 0.044 HD 136713 0.852 0.062 0.577 0.473 0.838 0.065 0.800 0.060 0.819 0.048 HD 185615 1.040 0.067 0.788 0.121 1.024 0.077 0.927 0.053 0.976 0.052 HD 136894 0.949 0.061 0.769 0.112 0.983 0.074 0.847 0.051 0.898 0.037 HD 186061 0.829 0.058 0.609 0.454 0.828 0.064 0.826 0.059 0.827 0.049 HD 137303 0.705 0.050 0.527 0.508 0.766 0.062 0.675 0.054 0.690 0.058 HD 187456 0.824 0.058 0.421 0.218 0.803 0.061 0.751 0.054 0.777 0.035 HD 137388 0.949 0.066 0.650 0.408 0.905 0.072 0.900 0.062 0.903 0.056 HD 188559 0.787 0.068 0.374 0.594 0.780 0.062 0.720 0.056 0.750 0.047 HD 138549 0.998 0.064 0.717 0.113 0.969 0.073 0.967 0.054 0.968 0.037 HD 188748 0.983 0.063 0.750 0.119 0.987 0.074 0.897 0.055 0.940 0.045 HD 140901 1.022 0.065 0.935 0.112 1.011 0.076 0.991 0.053 1.001 0.032 HD 189242 0.746 0.050 0.578 0.275 0.820 0.066 0.700 0.052 0.723 0.048 HD 141937 1.112 0.071 1.099 0.148 1.097 0.082 1.108 0.051 1.103 0.047 HD 189567 0.987 0.063 0.959 0.039 1.057 0.079 0.887 0.052 0.973 0.037 HD 142022A 1.046 0.069 0.931 0.196 1.039 0.078 0.943 0.054 0.991 0.047 HD 189625 1.117 0.071 1.052 0.137 1.087 0.081 1.106 0.052 1.096 0.038 HD 142709 0.709 0.054 0.338 0.433 0.729 0.056 0.675 0.055 0.692 0.045 HD 190248 1.140 0.077 0.917 0.223 1.093 0.082 1.010 0.052 1.051 0.062 HD 143114 0.966 0.061 1.132 0.101 1.109 0.083 0.846 0.051 1.037 0.047 HD 190647 1.156 0.076 1.184 0.205 1.199 0.090 1.061 0.053 1.170 0.065 HD 143295 0.834 0.058 0.476 0.270 0.817 0.065 0.772 0.057 0.795 0.044 HD 190954 0.866 0.055 0.798 0.137 0.954 0.072 0.769 0.051 0.832 0.054 HD 144411 0.754 0.052 0.351 0.245 0.766 0.068 0.700 0.052 0.727 0.040 HD 191847 0.834 0.056 0.518 0.275 0.833 0.069 0.773 0.054 0.803 0.046 HD 144497 0.813 0.056 0.631 0.397 0.838 0.067 0.761 0.057 0.787 0.058 HD 192031 0.749 0.049 0.586 0.166 0.895 0.068 0.669 0.051 0.709 0.052 HD 144585 1.201 0.076 1.508 0.117 1.218 0.091 1.155 0.052 1.210 0.050 HD 192117 0.952 0.062 0.786 0.223 0.950 0.072 0.912 0.061 0.931 0.042 HD 144628 0.774 0.050 0.578 0.155 0.831 0.063 0.710 0.052 0.742 0.046 HD 192310 0.865 0.057 0.711 0.294 0.874 0.066 0.822 0.057 0.843 0.050 HD 145598 0.788 0.051 0.656 0.138 0.911 0.070 0.700 0.051 0.744 0.047 HD 192961 0.708 0.061 0.236 0.340 0.705 0.057 0.635 0.054 0.670 0.043 HD 145666 1.069 0.068 1.159 0.077 1.079 0.081 1.077 0.052 1.078 0.031 HD 193193 1.102 0.070 1.605 0.141 1.221 0.091 1.093 0.051 1.161 0.041 HD 145809 1.084 0.069 1.400 0.112 1.285 0.096 1.015 0.052 1.184 0.043 HD 193844 0.787 0.052 0.477 0.242 0.818 0.066 0.734 0.052 0.760 0.040 HD 146233 1.069 0.068 1.040 0.084 1.072 0.080 1.058 0.053 1.063 0.035 HD 195302 0.862 0.059 0.569 0.372 0.849 0.068 0.800 0.058 0.825 0.048 HD 147512 0.975 0.062 0.845 0.085 1.007 0.075 0.872 0.052 0.923 0.039 HD 195564 1.191 0.076 1.142 0.087 1.281 0.095 1.100 0.051 1.166 0.045 HD 147513 1.066 0.068 1.061 0.128 1.059 0.079 1.054 0.051 1.060 0.051 HD 196050 1.185 0.075 1.248 0.105 1.192 0.089 1.134 0.052 1.188 0.037 HD 148303 0.806 0.061 0.699 0.802 0.826 0.065 0.790 0.061 0.798 0.047 HD 196761 0.889 0.057 0.702 0.089 0.943 0.071 0.794 0.051 0.841 0.046 HD 150433 0.940 0.060 1.033 0.099 1.051 0.079 0.835 0.051 0.986 0.040 HD 196800 1.184 0.076 1.405 0.176 1.212 0.090 1.169 0.052 1.198 0.035 HD 151504 0.998 0.065 0.845 0.158 1.010 0.076 0.885 0.052 0.941 0.047 HD 197210 0.994 0.064 0.788 0.151 0.991 0.075 0.932 0.055 0.962 0.039 HD 153851 0.797 0.052 0.637 0.242 0.844 0.067 0.748 0.053 0.772 0.047 HD 197823 0.981 0.064 0.863 0.246 0.981 0.074 0.884 0.056 0.933 0.044 HD 154088 1.023 0.069 0.785 0.238 0.976 0.073 0.901 0.059 0.939 0.050 HD 198075 0.987 0.063 0.928 0.118 1.006 0.076 0.985 0.053 0.986 0.043 HD 154363 0.669 0.062 0.237 0.580 0.697 0.054 0.600 0.055 0.635 0.047 HD 199190 1.187 0.075 1.223 0.097 1.219 0.091 1.144 0.052 1.203 0.044 HD 154577 0.681 0.045 0.521 0.198 0.786 0.060 0.646 0.052 0.663 0.045 HD 199288 0.893 0.057 1.123 0.092 1.056 0.079 0.810 0.052 0.974 0.037 HD 154962 1.244 0.080 1.562 0.178 1.312 0.098 1.268 0.052 1.290 0.076 HD 199933 0.767 0.061 0.334 0.365 0.759 0.064 0.700 0.054 0.729 0.038 HD 157172 1.000 0.065 0.826 0.194 0.989 0.074 0.900 0.054 0.945 0.056 HD 199960 1.192 0.077 1.461 0.302 1.201 0.090 1.154 0.052 1.196 0.046 HD 157338 1.097 0.070 1.258 0.110 1.153 0.086 1.074 0.053 1.125 0.050 HD 200505 0.765 0.051 0.506 0.183 0.822 0.063 0.711 0.053 0.738 0.047 HD 157347 1.043 0.067 0.931 0.115 1.057 0.079 0.965 0.053 1.004 0.035 HD 202206 1.110 0.071 1.152 0.168 1.072 0.080 1.100 0.053 1.105 0.047 HD 157830 0.920 0.058 0.800 0.102 0.960 0.072 0.837 0.055 0.879 0.049 HD 202605 1.050 0.067 1.127 0.176 1.041 0.078 1.061 0.053 1.055 0.066 HD 159868 1.153 0.074 1.194 0.100 1.304 0.097 1.078 0.052 1.174 0.063 HD 203384 1.071 0.070 0.876 0.198 1.022 0.077 1.000 0.057 1.011 0.051 c 2002 RAS, MNRAS 000, 1–?? 12 F. J. G. Pinheiro et al.

Table A1. Continuation

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

HD 203413 0.803 0.065 0.454 0.583 0.792 0.063 0.751 0.058 0.771 0.058 HD 214759 1.024 0.069 0.738 0.272 0.982 0.074 0.971 0.060 0.977 0.050 HD 203432 1.099 0.071 1.079 0.190 1.076 0.081 1.011 0.053 1.077 0.042 HD 215152 0.813 0.060 0.477 0.391 0.817 0.063 0.755 0.055 0.784 0.050 HD 203850 0.681 0.046 0.467 0.259 0.772 0.060 0.634 0.052 0.658 0.050 HD 215456 1.150 0.075 1.265 0.153 1.294 0.096 1.066 0.052 1.207 0.060 HD 204313 1.111 0.071 1.043 0.105 1.099 0.082 1.058 0.054 1.079 0.046 HD 216435 1.263 0.084 1.715 0.339 1.360 0.101 1.220 0.071 1.312 0.064 HD 204385 1.138 0.072 1.453 0.121 1.183 0.088 1.141 0.052 1.162 0.049 HD 216770 1.025 0.069 0.828 0.264 0.992 0.075 0.920 0.061 0.956 0.053 HD 204941 0.812 0.055 0.573 0.267 0.838 0.064 0.753 0.055 0.782 0.037 HD 216777 0.910 0.058 0.857 0.115 0.979 0.074 0.812 0.054 0.883 0.064 HD 205536 0.963 0.062 0.724 0.121 0.973 0.073 0.850 0.052 0.907 0.044 HD 218249 0.756 0.050 0.515 0.253 0.804 0.065 0.709 0.054 0.732 0.037 HD 206163 0.985 0.063 0.657 0.114 0.948 0.072 0.918 0.055 0.933 0.038 HD 218511 0.732 0.087 0.276 1.039 0.711 0.056 0.667 0.056 0.689 0.053 HD 206172 0.940 0.060 0.691 0.133 0.946 0.072 0.895 0.055 0.917 0.040 HD 218572 0.674 0.046 0.438 0.334 0.741 0.058 0.637 0.053 0.656 0.046 HD 207129 1.081 0.068 1.193 0.096 1.100 0.082 1.100 0.052 1.100 0.037 HD 219077 1.060 0.069 1.363 0.157 1.267 0.094 1.065 0.051 1.166 0.045 HD 207583 0.982 0.063 0.793 0.122 0.972 0.073 0.928 0.056 0.950 0.044 HD 219249 0.873 0.056 0.767 0.122 0.939 0.071 0.781 0.053 0.827 0.049 HD 207700 1.073 0.069 1.110 0.140 1.131 0.084 0.945 0.057 1.091 0.061 HD 220256 0.866 0.058 0.755 0.267 0.916 0.070 0.801 0.053 0.834 0.060 HD 207970 1.022 0.066 0.874 0.119 1.026 0.077 0.915 0.054 0.969 0.037 HD 220339 0.766 0.051 0.658 0.336 0.829 0.063 0.725 0.053 0.745 0.052 HD 208272 0.882 0.059 0.634 0.217 0.894 0.068 0.801 0.054 0.842 0.034 HD 220367 1.110 0.072 1.675 0.267 1.277 0.095 1.129 0.062 1.203 0.052 HD 208487 1.161 0.074 1.362 0.180 1.167 0.087 1.176 0.052 1.171 0.048 HD 220507 1.074 0.069 1.108 0.146 1.138 0.085 0.959 0.056 1.091 0.055 HD 208573 0.823 0.063 0.444 0.579 0.800 0.096 0.774 0.058 0.787 0.070 HD 221146 1.150 0.075 1.441 0.236 1.244 0.093 1.100 0.051 1.197 0.049 HD 208704 1.057 0.067 1.137 0.059 1.124 0.084 0.981 0.052 1.090 0.050 HD 221287 1.183 0.075 1.665 0.209 1.178 0.088 1.181 0.052 1.182 0.050 HD 209100 0.739 0.059 0.455 0.645 0.765 0.058 0.700 0.053 0.719 0.053 HD 221356 1.069 0.069 1.363 0.215 1.136 0.085 1.100 0.057 1.118 0.040 HD 209458 1.135 0.073 1.413 0.245 1.160 0.087 1.158 0.051 1.159 0.046 HD 221420 1.326 0.086 1.459 0.164 1.383 0.103 1.346 0.051 1.365 0.053 HD 209742 0.837 0.056 0.677 0.273 0.871 0.067 0.770 0.054 0.804 0.051 HD 222237 0.729 0.055 0.394 0.315 0.774 0.059 0.700 0.052 0.715 0.049 HD 210277 1.058 0.069 0.854 0.138 1.048 0.078 0.929 0.054 0.988 0.052 HD 222335 0.863 0.056 0.714 0.154 0.899 0.068 0.787 0.053 0.825 0.037 HD 210752 0.948 0.060 1.193 0.152 1.106 0.083 0.828 0.052 1.027 0.058 HD 222422 0.938 0.060 0.733 0.108 0.949 0.071 0.864 0.054 0.901 0.042 HD 210918 1.046 0.066 1.098 0.090 1.118 0.083 0.952 0.051 1.072 0.044 HD 222582 1.067 0.068 1.064 0.150 1.106 0.083 0.988 0.052 1.065 0.050 HD 210975 0.713 0.055 0.298 0.336 0.736 0.063 0.648 0.053 0.681 0.042 HD 222595 1.013 0.065 0.751 0.117 0.979 0.074 1.000 0.051 0.990 0.045 HD 211038 1.085 0.078 1.116 0.224 1.303 0.097 1.035 0.060 1.101 0.071 HD 222669 1.089 0.069 1.066 0.093 1.086 0.081 1.088 0.052 1.087 0.036 HD 211369 0.845 0.059 0.521 0.342 0.825 0.064 0.800 0.059 0.813 0.050 HD 223121 0.895 0.071 0.406 0.432 0.836 0.068 0.800 0.062 0.818 0.057 HD 211415 1.031 0.066 0.936 0.153 1.084 0.081 0.939 0.053 0.985 0.059 HD 223171 1.178 0.075 1.370 0.107 1.265 0.094 1.200 0.066 1.233 0.040 HD 212301 1.207 0.077 1.602 0.197 1.190 0.089 1.200 0.052 1.204 0.047 HD 223282 0.836 0.053 0.736 0.162 0.914 0.070 0.751 0.052 0.793 0.048 HD 212563 0.828 0.056 0.609 0.366 0.827 0.067 0.802 0.059 0.814 0.051 HD 224393 0.941 0.060 0.870 0.166 0.993 0.074 0.900 0.052 0.921 0.044 HD 212580 0.861 0.057 0.553 0.205 0.860 0.066 0.790 0.054 0.825 0.035 HD 224619 0.926 0.059 0.701 0.102 0.960 0.072 0.820 0.051 0.873 0.040 HD 212708 1.116 0.072 0.972 0.167 1.080 0.081 1.021 0.054 1.050 0.055 HD 224789 0.885 0.058 0.638 0.208 0.884 0.067 0.807 0.055 0.845 0.034 HD 213042 0.824 0.094 0.412 1.568 0.785 0.061 0.751 0.057 0.768 0.060 HD 330075 0.882 0.070 0.617 0.583 0.894 0.071 0.800 0.055 0.841 0.063 HD 213240 1.197 0.077 1.503 0.182 1.275 0.095 1.212 0.051 1.244 0.045 HIP 21539 0.695 0.065 0.265 0.478 0.706 0.065 0.641 0.057 0.668 0.051 HD 213575 1.067 0.068 1.088 0.091 1.185 0.088 0.928 0.051 1.077 0.054 HIP 22059 0.724 0.057 0.334 0.486 0.739 0.080 0.675 0.056 0.699 0.053 HD 213628 0.993 0.063 0.796 0.117 0.982 0.074 0.929 0.054 0.956 0.041 HIP 26542 0.677 0.049 0.357 0.349 0.728 0.060 0.626 0.053 0.652 0.035 HD 213941 0.891 0.057 0.946 0.128 1.020 0.076 0.805 0.052 0.918 0.054 HIP 98764 0.766 0.055 0.398 0.358 0.777 0.065 0.710 0.055 0.738 0.048 HD 214385 0.942 0.060 1.004 0.108 1.046 0.078 0.828 0.051 0.973 0.057

Table A2. Mass estimate for Sousa et al’s 2011 targets according to different methods (in solar units).

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

HD 67 1.024 0.065 0.883 0.297 0.983 0.074 1.000 0.054 0.991 0.038 HD 4597 1.023 0.065 1.153 0.388 1.137 0.086 0.939 0.053 1.080 0.077 HD 208 1.005 0.064 1.230 0.403 1.112 0.083 0.911 0.053 1.058 0.070 HD 4838 0.702 0.045 0.551 0.317 0.730 0.055 0.700 0.053 0.701 0.042 HD 457 1.230 0.078 1.881 0.598 1.262 0.095 1.220 0.051 1.246 0.047 HD 5349 1.179 0.083 0.741 0.396 1.126 0.085 0.968 0.052 1.047 0.048 HD 564 1.015 0.064 1.258 0.436 1.085 0.082 0.994 0.058 1.050 0.053 HD 5388 1.185 0.076 2.043 0.644 1.447 0.108 1.198 0.069 1.323 0.080 HD 1171 0.808 0.052 0.462 0.214 0.845 0.065 0.728 0.054 0.768 0.040 HD 6718 1.019 0.065 1.104 0.357 1.071 0.080 0.944 0.054 1.045 0.054 HD 1979 0.972 0.062 1.067 0.395 1.014 0.077 0.955 0.054 0.993 0.045 HD 8038 1.062 0.067 1.088 0.366 1.058 0.080 1.042 0.053 1.060 0.051 HD 2014 0.857 0.056 0.491 0.277 0.850 0.065 0.779 0.052 0.815 0.047 HD 8535 1.169 0.074 1.356 0.432 1.203 0.090 1.172 0.052 1.187 0.055 HD 2567 1.179 0.075 1.686 0.559 1.221 0.092 1.183 0.051 1.202 0.062 HD 8930 0.956 0.061 0.913 0.286 0.994 0.075 0.922 0.055 0.939 0.046 HD 2768 0.991 0.063 0.676 0.259 0.972 0.074 0.912 0.054 0.942 0.046 HD 8985 1.187 0.078 3.748 1.539 1.203 0.090 1.193 0.055 1.198 0.051 HD 3220 1.000 0.063 0.864 0.294 1.014 0.076 0.985 0.051 0.993 0.047 HD 9578 1.135 0.072 1.401 0.500 1.140 0.086 1.155 0.054 1.147 0.043 HD 3229 1.363 0.088 2.865 0.882 1.697 0.126 1.567 0.069 1.632 0.082 HD 9608 1.036 0.066 1.291 0.423 1.147 0.086 0.967 0.053 1.092 0.066 HD 3808 0.952 0.060 0.964 0.362 1.011 0.077 0.848 0.052 0.958 0.071 HD 10895 0.947 0.060 0.963 0.328 1.004 0.076 0.878 0.061 0.955 0.055 HD 3964 1.036 0.066 1.080 0.412 1.041 0.078 1.043 0.054 1.042 0.048 HD 11397 0.863 0.055 0.839 0.358 0.970 0.074 0.765 0.054 0.851 0.065 HD 4021 1.026 0.065 1.430 0.552 1.019 0.077 1.022 0.054 1.024 0.043 HD 11608 0.902 0.063 0.426 0.519 0.831 0.063 0.808 0.058 0.819 0.043 HD 4457 0.761 0.048 0.678 0.324 0.838 0.063 0.718 0.053 0.739 0.052 HD 11938 0.806 0.056 0.321 0.261 0.769 0.058 0.736 0.052 0.752 0.032

c 2002 RAS, MNRAS 000, 1–?? On the mass estimation for FGK stars:comparison of several methods 13

Table A2. Continuation

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

HD 13252 0.910 0.059 0.579 0.272 0.938 0.071 0.800 0.051 0.855 0.046 HD 30177 1.121 0.072 0.941 0.311 1.064 0.080 0.984 0.051 1.024 0.057 HD 13578 1.146 0.075 1.183 0.394 1.240 0.093 1.044 0.051 1.164 0.081 HD 30523 0.706 0.045 0.403 0.316 0.705 0.053 0.649 0.056 0.677 0.044 HD 14452 0.880 0.056 0.791 0.292 0.918 0.069 0.804 0.052 0.842 0.057 HD 30669 0.995 0.064 0.743 0.354 0.973 0.074 0.894 0.053 0.934 0.057 HD 14745 1.103 0.070 2.092 0.668 1.165 0.087 1.137 0.052 1.151 0.048 HD 30858 0.862 0.055 0.651 0.296 0.886 0.067 0.786 0.053 0.824 0.043 HD 14868 1.079 0.068 0.887 0.293 1.053 0.079 1.055 0.052 1.054 0.048 HD 31103 1.143 0.072 1.238 0.398 1.130 0.085 1.138 0.053 1.140 0.066 HD 15612 0.877 0.056 0.667 0.312 0.886 0.068 0.829 0.055 0.853 0.043 HD 31532 1.199 0.077 1.879 0.495 1.444 0.108 1.228 0.052 1.336 0.075 HD 15906 0.800 0.051 0.591 0.369 0.809 0.061 0.762 0.055 0.781 0.047 HD 32804 1.081 0.068 1.226 0.375 1.084 0.081 1.100 0.052 1.092 0.037 HD 16008 1.016 0.065 1.003 0.381 1.057 0.080 0.933 0.052 1.009 0.067 HD 33081 1.146 0.072 2.676 0.940 1.334 0.100 1.206 0.066 1.270 0.072 HD 16280 0.752 0.050 0.374 0.262 0.758 0.057 0.692 0.054 0.722 0.043 HD 33473 1.191 0.080 1.679 0.519 1.439 0.108 1.228 0.072 1.333 0.092 HD 16382 1.091 0.069 1.552 0.447 1.153 0.086 1.096 0.054 1.125 0.043 HD 33811 1.075 0.068 0.921 0.337 1.031 0.077 0.979 0.051 1.005 0.051 HD 16536 0.911 0.058 0.651 0.294 0.922 0.070 0.819 0.051 0.865 0.038 HD 33822 1.147 0.073 1.226 0.441 1.165 0.088 1.071 0.051 1.156 0.071 HD 16548 1.260 0.082 1.275 0.382 1.357 0.101 1.214 0.051 1.268 0.070 HD 34327 1.142 0.074 1.719 0.574 1.330 0.099 1.107 0.051 1.236 0.062 HD 16905 0.854 0.058 0.458 0.343 0.814 0.061 0.800 0.056 0.807 0.052 HD 36051 1.084 0.068 1.396 0.444 1.094 0.082 1.094 0.055 1.094 0.068 HD 17439 1.054 0.067 0.963 0.301 1.046 0.078 1.035 0.051 1.041 0.039 HD 36179 0.910 0.058 0.606 0.259 0.896 0.068 0.880 0.052 0.888 0.031 HD 17548 0.984 0.063 1.140 0.377 1.127 0.085 0.877 0.053 1.056 0.099 HD 37226 1.227 0.080 2.683 0.818 1.559 0.116 1.431 0.055 1.495 0.066 HD 18001 1.032 0.066 0.819 0.308 1.022 0.077 1.011 0.057 1.016 0.055 HD 37548 1.143 0.074 1.509 0.518 1.276 0.096 1.161 0.091 1.218 0.074 HD 18083 1.111 0.070 1.873 0.622 1.129 0.084 1.122 0.051 1.125 0.056 HD 37990 1.141 0.072 1.577 0.523 1.172 0.088 1.170 0.052 1.171 0.061 HD 18777 0.870 0.056 0.539 0.290 0.856 0.065 0.800 0.052 0.828 0.032 HD 38078 0.944 0.060 0.852 0.321 0.998 0.075 0.852 0.054 0.898 0.067 HD 18822 0.902 0.058 0.730 0.290 0.926 0.070 0.819 0.052 0.860 0.054 HD 38265 0.959 0.061 0.889 0.305 1.004 0.076 0.852 0.055 0.924 0.062 HD 18838 0.929 0.059 0.752 0.305 0.948 0.072 0.865 0.054 0.897 0.048 HD 38355 0.967 0.062 0.665 0.279 0.946 0.071 0.851 0.055 0.898 0.045 HD 19230 0.770 0.049 0.820 0.310 0.869 0.066 0.719 0.055 0.795 0.057 HD 38385 1.425 0.090 4.054 1.764 1.572 0.117 1.600 0.054 1.586 0.067 HD 19423 1.085 0.070 1.017 0.305 1.163 0.087 0.937 0.069 1.051 0.073 HD 38772 1.099 0.070 1.328 0.407 1.211 0.091 1.053 0.056 1.155 0.068 HD 19641 1.068 0.068 1.004 0.313 1.091 0.082 1.008 0.053 1.038 0.066 HD 39427 0.966 0.061 0.956 0.347 1.002 0.075 0.976 0.056 0.971 0.055 HD 20492 0.814 0.059 0.372 0.340 0.785 0.059 0.748 0.055 0.767 0.035 HD 40483 1.209 0.077 3.035 0.925 1.475 0.110 1.355 0.066 1.414 0.069 HD 20852 1.173 0.075 3.724 1.422 1.373 0.103 1.256 0.051 1.314 0.055 HD 40503 0.858 0.056 0.456 0.209 0.849 0.064 0.784 0.053 0.817 0.034 HD 20868 0.839 0.061 0.361 0.365 0.798 0.061 0.752 0.057 0.775 0.039 HD 40865 0.937 0.060 0.922 0.300 1.015 0.076 0.830 0.052 0.930 0.069 HD 21132 1.047 0.066 1.824 0.590 1.192 0.089 1.030 0.051 1.120 0.061 HD 41087 0.947 0.060 0.935 0.306 0.982 0.074 0.933 0.055 0.941 0.059 HD 21161 1.178 0.076 1.131 0.386 1.211 0.091 1.105 0.053 1.154 0.066 HD 41248 0.937 0.059 0.811 0.255 0.992 0.074 0.844 0.057 0.891 0.068 HD 21251 0.809 0.052 0.621 0.354 0.847 0.064 0.767 0.054 0.788 0.038 HD 41323 0.949 0.060 0.964 0.303 0.999 0.075 0.920 0.056 0.956 0.049 HD 21759 0.755 0.048 0.611 0.291 0.854 0.066 0.700 0.052 0.727 0.058 HD 42505 0.740 0.050 0.295 0.243 0.725 0.055 0.664 0.053 0.695 0.038 HD 21977 1.114 0.071 1.248 0.445 1.130 0.085 1.114 0.053 1.122 0.061 HD 43197 1.086 0.070 0.666 0.340 0.989 0.075 0.930 0.051 0.959 0.051 HD 22177 1.124 0.072 1.271 0.373 1.176 0.088 1.045 0.051 1.150 0.067 HD 44219 1.135 0.073 1.042 0.339 1.185 0.089 1.007 0.054 1.088 0.084 HD 22249 1.000 0.063 1.188 0.431 1.009 0.076 1.002 0.052 1.005 0.053 HD 44804 0.938 0.060 0.831 0.301 0.943 0.071 0.872 0.053 0.905 0.046 HD 22282 1.016 0.066 0.838 0.347 1.020 0.077 0.900 0.051 0.958 0.062 HD 45977 0.793 0.057 0.367 0.472 0.769 0.058 0.737 0.059 0.753 0.054 HD 22897 0.753 0.049 0.408 0.289 0.768 0.059 0.707 0.055 0.730 0.042 HD 48115 1.008 0.064 0.876 0.273 1.028 0.077 0.988 0.052 0.998 0.046 HD 22918 1.179 0.087 1.126 0.504 1.324 0.099 1.168 0.095 1.173 0.093 HD 49035 1.096 0.070 0.900 48.868 1.056 0.125 1.014 0.052 1.035 0.063 HD 23030 1.170 0.075 1.760 0.757 1.253 0.096 1.181 0.053 1.217 0.048 HD 52449 1.215 0.077 1.648 0.482 1.210 0.090 1.221 0.051 1.218 0.048 HD 23472 0.769 0.051 0.441 0.309 0.790 0.060 0.720 0.053 0.745 0.044 HD 54521 1.078 0.068 1.336 0.475 1.106 0.083 1.100 0.053 1.103 0.057 HD 23901 0.999 0.066 1.047 0.328 1.221 0.091 0.894 0.051 1.023 0.113 HD 56380 0.860 0.055 0.633 0.238 0.939 0.071 0.763 0.051 0.812 0.050 HD 24062 1.177 0.074 3.117 1.078 1.283 0.096 1.250 0.052 1.267 0.064 HD 57568 0.701 0.045 0.345 0.157 0.727 0.055 0.662 0.052 0.681 0.032 HD 24085 1.165 0.074 1.827 0.528 1.227 0.092 1.200 0.053 1.214 0.038 HD 58489 0.830 0.060 0.400 0.388 0.791 0.060 0.770 0.056 0.780 0.053 HD 24112 1.229 0.078 1.854 0.572 1.319 0.099 1.275 0.054 1.297 0.051 HD 58676 0.881 0.056 0.550 0.237 0.872 0.066 0.798 0.052 0.835 0.028 HD 24558 0.828 0.053 0.592 0.225 0.906 0.068 0.751 0.055 0.789 0.046 HD 61051 0.933 0.060 0.631 0.233 0.939 0.071 0.829 0.052 0.881 0.050 HD 24633 0.926 0.060 0.851 0.407 0.977 0.075 0.840 0.052 0.888 0.062 HD 61383 0.990 0.064 1.373 0.417 1.239 0.093 0.888 0.051 1.115 0.096 HD 25061 0.926 0.059 0.848 0.331 0.948 0.071 0.851 0.052 0.888 0.055 HD 61447 1.072 0.068 0.881 0.337 1.044 0.079 1.003 0.053 1.023 0.041 HD 25171 1.127 0.071 1.422 0.404 1.208 0.090 1.104 0.053 1.167 0.060 HD 61986 0.949 0.060 0.885 0.313 1.013 0.076 0.856 0.065 0.917 0.070 HD 25357 0.831 0.053 0.840 0.534 0.822 0.062 0.810 0.054 0.826 0.037 HD 62128 1.225 0.078 1.270 0.392 1.232 0.092 1.113 0.068 1.228 0.075 HD 25587 1.112 0.070 3.206 1.344 1.321 0.099 1.185 0.059 1.253 0.059 HD 62364 1.142 0.072 2.001 0.649 1.285 0.096 1.163 0.054 1.224 0.061 HD 25912 1.095 0.069 1.165 0.414 1.073 0.080 1.100 0.052 1.098 0.045 HD 62847 0.878 0.056 0.632 0.213 0.898 0.068 0.810 0.052 0.844 0.034 HD 26430 0.793 0.051 0.517 0.277 0.840 0.064 0.736 0.052 0.764 0.033 HD 63685 1.110 0.073 1.177 0.336 1.238 0.092 1.018 0.052 1.144 0.074 HD 26729 1.206 0.078 1.533 0.509 1.284 0.096 1.121 0.052 1.245 0.066 HD 63754 1.308 0.085 2.188 0.725 1.467 0.110 1.418 0.051 1.442 0.064 HD 26887 1.023 0.065 0.924 0.311 1.075 0.081 0.970 0.053 0.996 0.057 HD 64640 0.959 0.063 0.588 0.311 0.918 0.069 0.854 0.052 0.886 0.041 HD 27471 1.164 0.075 1.554 0.519 1.274 0.095 1.200 0.073 1.237 0.055 HD 65982 1.076 0.068 1.157 0.390 1.128 0.085 1.022 0.056 1.102 0.061 HD 28254 1.209 0.079 1.205 0.420 1.222 0.092 1.068 0.051 1.207 0.063 HD 66039 1.177 0.074 1.589 0.490 1.183 0.088 1.200 0.052 1.192 0.058 HD 28807 1.243 0.078 3.242 1.364 1.355 0.101 1.338 0.055 1.346 0.054 HD 66040 1.004 0.065 0.623 0.350 0.924 0.069 0.853 0.051 0.888 0.055 HD 28969 1.131 0.071 1.993 0.786 1.169 0.088 1.161 0.054 1.165 0.053 HD 66168 1.110 0.070 1.866 0.644 1.143 0.086 1.140 0.052 1.142 0.045 HD 29137 1.174 0.075 1.325 0.383 1.198 0.089 1.100 0.052 1.186 0.067 HD 66340 0.943 0.060 0.553 0.204 0.910 0.068 0.834 0.057 0.872 0.038 HD 29263 1.083 0.069 1.116 0.401 1.129 0.085 1.001 0.054 1.099 0.068 HD 66740 1.289 0.081 2.325 0.872 1.388 0.104 1.378 0.059 1.383 0.068 HD 29303 1.015 0.064 1.043 0.334 1.039 0.078 1.018 0.055 1.028 0.058 HD 66838 0.993 0.063 0.536 0.210 0.947 0.071 0.858 0.055 0.903 0.050 HD 29428 1.017 0.065 0.755 0.286 0.988 0.074 0.988 0.053 0.988 0.046 HD 67200 1.227 0.078 1.544 0.472 1.209 0.090 1.211 0.051 1.219 0.042 HD 29980 1.100 0.070 2.367 0.938 1.151 0.087 1.154 0.055 1.152 0.054 HD 68287 1.173 0.074 2.234 0.919 1.233 0.093 1.232 0.055 1.232 0.050 HD 29985 0.727 0.050 0.239 0.213 0.695 0.053 0.645 0.052 0.670 0.038 HD 70903 0.777 0.049 0.819 0.361 0.885 0.067 0.731 0.055 0.798 0.070 HD 30053 1.074 0.068 1.294 0.396 1.142 0.086 1.077 0.063 1.109 0.060 HD 71685 1.001 0.063 1.334 0.511 1.099 0.083 0.987 0.055 1.050 0.067

c 2002 RAS, MNRAS 000, 1–?? 14 F. J. G. Pinheiro et al.

Table A2. Continuation

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

HD 72374 1.050 0.067 0.963 0.306 1.095 0.082 0.942 0.053 1.006 0.071 HD 103197 0.954 0.061 0.697 0.410 0.908 0.069 0.913 0.054 0.910 0.043 HD 72659 1.149 0.074 1.205 0.381 1.227 0.092 1.084 0.054 1.177 0.070 HD 103720 0.844 0.055 0.484 0.270 0.822 0.062 0.813 0.055 0.817 0.041 HD 73267 0.969 0.062 0.842 0.322 0.990 0.075 0.876 0.051 0.922 0.064 HD 103891 1.231 0.081 2.050 0.631 1.525 0.114 1.370 0.110 1.447 0.085 HD 73583 0.715 0.046 0.526 0.367 0.758 0.057 0.692 0.051 0.703 0.030 HD 104760 1.131 0.072 1.247 0.515 1.141 0.087 1.123 0.052 1.136 0.056 HD 74698 1.121 0.072 1.068 0.304 1.157 0.086 1.029 0.052 1.094 0.054 HD 105779 0.980 0.062 0.916 0.336 1.018 0.077 0.970 0.055 0.975 0.058 HD 74957 1.022 0.065 1.424 0.454 1.110 0.083 0.999 0.056 1.066 0.050 HD 105938 1.231 0.079 2.371 0.809 1.446 0.108 1.353 0.084 1.400 0.081 HD 75328 1.048 0.066 1.196 0.366 1.128 0.084 0.993 0.055 1.088 0.058 HD 106290 1.122 0.071 1.264 0.447 1.096 0.083 1.118 0.052 1.120 0.052 HD 75530 0.808 0.052 0.953 0.434 0.957 0.073 0.744 0.052 0.880 0.090 HD 106589 0.966 0.061 0.893 0.358 1.040 0.078 0.853 0.051 0.930 0.076 HD 75881 1.194 0.076 3.149 1.098 1.422 0.106 1.357 0.056 1.389 0.054 HD 107094 0.864 0.055 0.895 0.357 0.965 0.074 0.776 0.055 0.879 0.067 HD 76188 1.124 0.075 1.295 0.413 1.352 0.101 1.020 0.051 1.209 0.117 HD 108063 1.429 0.095 3.244 1.129 1.634 0.122 1.622 0.051 1.628 0.057 HD 76440 1.047 0.066 0.975 0.310 1.057 0.079 1.000 0.052 1.023 0.042 HD 108341 0.880 0.056 0.707 0.340 0.887 0.067 0.812 0.052 0.846 0.049 HD 78964 0.903 0.057 1.348 1.193 0.988 0.092 0.834 0.058 0.945 0.098 HD 108768 1.042 0.066 0.843 0.333 1.001 0.076 1.020 0.055 1.010 0.061 HD 79601 0.943 0.060 1.359 0.461 1.169 0.088 0.857 0.054 1.056 0.078 HD 108935 0.801 0.059 0.323 0.417 0.759 0.058 0.729 0.057 0.744 0.037 HD 81700 1.088 0.069 1.194 0.384 1.073 0.081 1.100 0.051 1.094 0.040 HD 109098 1.202 0.078 1.301 0.394 1.296 0.097 1.200 0.084 1.249 0.074 HD 81767 0.842 0.054 0.693 0.428 0.857 0.065 0.800 0.052 0.821 0.051 HD 109271 1.125 0.072 1.338 0.465 1.203 0.091 1.057 0.053 1.164 0.072 HD 82114 1.169 0.075 1.645 0.462 1.325 0.099 1.221 0.057 1.273 0.064 HD 109368 0.724 0.049 0.318 0.253 0.730 0.055 0.677 0.054 0.700 0.033 HD 82783 0.980 0.063 0.671 0.389 0.927 0.071 0.930 0.054 0.928 0.044 HD 109723 0.999 0.063 0.746 0.329 0.976 0.074 0.974 0.054 0.975 0.044 HD 84305 1.028 0.065 1.230 0.401 1.098 0.083 0.997 0.057 1.063 0.047 HD 109988 0.919 0.059 0.873 0.433 0.929 0.070 0.850 0.052 0.896 0.052 HD 84627 1.055 0.067 0.310 0.207 0.884 0.075 0.976 0.057 0.930 0.056 HD 110291 0.980 0.063 0.668 0.281 0.964 0.073 0.877 0.053 0.921 0.059 HD 85725 1.364 0.092 2.040 0.690 1.578 0.118 1.536 0.052 1.557 0.064 HD 110557 0.919 0.059 0.473 0.230 0.883 0.068 0.814 0.054 0.848 0.044 HD 86652 1.118 0.071 1.183 0.403 1.104 0.083 1.117 0.053 1.118 0.030 HD 110668 1.110 0.070 1.191 0.416 1.105 0.083 1.102 0.052 1.108 0.058 HD 87320 0.981 0.062 1.141 0.444 1.077 0.081 0.878 0.052 1.029 0.079 HD 111564 1.150 0.073 1.572 0.525 1.233 0.093 1.130 0.055 1.191 0.059 HD 87838 1.034 0.065 1.235 0.355 1.146 0.086 0.977 0.053 1.090 0.073 HD 112100 0.832 0.053 0.548 0.298 0.845 0.065 0.769 0.055 0.800 0.041 HD 88885 0.910 0.058 0.792 0.292 0.942 0.071 0.829 0.055 0.870 0.065 HD 112283 1.137 0.073 2.892 0.896 1.198 0.090 1.166 0.052 1.182 0.038 HD 89147 0.903 0.057 0.577 0.268 0.885 0.068 0.842 0.053 0.864 0.039 HD 113101 0.965 0.062 0.740 0.294 0.980 0.074 0.847 0.052 0.906 0.044 HD 89668 0.769 0.051 0.427 0.425 0.766 0.058 0.744 0.054 0.755 0.037 HD 113513 1.063 0.067 0.977 0.388 1.010 0.076 1.031 0.052 1.021 0.058 HD 89749 0.890 0.056 0.908 0.358 0.972 0.074 0.807 0.053 0.899 0.059 HD 113569 0.804 0.052 0.507 0.249 0.833 0.063 0.741 0.052 0.772 0.041 HD 89839 1.193 0.076 1.745 0.656 1.249 0.093 1.232 0.052 1.240 0.055 HD 114076 0.796 0.051 0.581 0.284 0.894 0.068 0.731 0.052 0.763 0.051 HD 89920 0.815 0.055 0.520 0.335 0.834 0.063 0.761 0.058 0.788 0.041 HD 114561 1.033 0.065 1.022 0.377 1.046 0.079 1.037 0.051 1.035 0.043 HD 89965 0.827 0.053 0.622 0.297 0.843 0.064 0.779 0.055 0.803 0.049 HD 115341 1.099 0.069 1.532 0.540 1.146 0.086 1.131 0.054 1.138 0.045 HD 90081 1.064 0.068 0.992 0.324 1.129 0.085 0.957 0.055 1.028 0.068 HD 115499 1.001 0.063 0.799 0.308 0.976 0.074 0.968 0.055 0.972 0.048 HD 90133 0.831 0.053 0.634 0.312 0.872 0.066 0.774 0.052 0.803 0.049 HD 115773 1.246 0.080 2.174 0.642 1.472 0.110 1.347 0.052 1.410 0.072 HD 90702 1.069 0.068 1.220 0.458 1.043 0.079 1.082 0.053 1.076 0.063 HD 115902 1.041 0.066 0.879 0.389 1.046 0.080 0.956 0.054 0.999 0.053 HD 90722 1.159 0.074 1.087 0.381 1.140 0.085 1.043 0.051 1.114 0.061 HD 116259 1.130 0.073 1.107 0.355 1.177 0.088 1.026 0.056 1.118 0.087 HD 90926 1.040 0.066 0.821 0.281 1.025 0.077 0.936 0.055 0.981 0.055 HD 116284 1.110 0.074 1.317 0.397 1.298 0.097 1.160 0.059 1.229 0.073 HD 90936 1.089 0.069 1.149 0.392 1.097 0.083 1.100 0.051 1.099 0.037 HD 116410 1.157 0.073 1.141 0.444 1.121 0.085 1.152 0.051 1.147 0.052 HD 91267 0.804 0.052 0.657 0.430 0.834 0.063 0.770 0.054 0.787 0.049 HD 116883 0.794 0.052 0.482 0.274 0.824 0.063 0.741 0.052 0.767 0.038 HD 91345 0.786 0.050 0.972 0.375 1.001 0.076 0.738 0.051 0.879 0.071 HD 116963 0.762 0.050 0.420 0.380 0.757 0.057 0.728 0.053 0.742 0.043 HD 91379 1.087 0.069 0.889 0.306 1.114 0.084 1.044 0.054 1.065 0.047 HD 117359 0.882 0.056 0.795 0.386 0.934 0.071 0.808 0.052 0.845 0.064 HD 92547 1.021 0.065 1.237 0.429 1.140 0.086 0.939 0.057 1.080 0.056 HD 117938 0.785 0.056 0.373 0.291 0.788 0.060 0.728 0.057 0.757 0.038 HD 93351 0.908 0.058 0.812 0.330 0.972 0.073 0.820 0.052 0.864 0.070 HD 118466 0.919 0.061 0.640 0.470 0.898 0.068 0.834 0.052 0.866 0.049 HD 93745 1.190 0.076 1.897 0.651 1.311 0.098 1.236 0.053 1.273 0.056 HD 118563 0.958 0.061 0.677 0.258 0.938 0.071 0.902 0.056 0.920 0.036 HD 93932 1.152 0.074 1.334 0.443 1.223 0.092 1.104 0.063 1.188 0.062 HD 119173 0.957 0.062 0.479 0.187 1.001 0.076 0.787 0.052 0.872 0.038 HD 94771 1.222 0.079 1.171 0.341 1.276 0.095 1.119 0.051 1.197 0.064 HD 119291 0.769 0.057 0.220 0.208 0.718 0.054 0.682 0.051 0.700 0.032 HD 94964 1.105 0.070 1.605 0.531 1.169 0.087 1.161 0.056 1.165 0.050 HD 119503 0.811 0.053 0.480 0.320 0.809 0.061 0.761 0.057 0.785 0.050 HD 95533 0.995 0.064 0.684 0.331 0.956 0.073 0.883 0.051 0.919 0.065 HD 119629 1.229 0.079 2.087 0.612 1.491 0.111 1.343 0.056 1.417 0.089 HD 95542 1.077 0.068 1.167 0.370 1.088 0.081 1.082 0.052 1.084 0.048 HD 120344 0.970 0.062 0.859 0.342 1.016 0.077 0.847 0.052 0.914 0.064 HD 95922 1.134 0.072 2.326 0.757 1.239 0.093 1.209 0.054 1.224 0.064 HD 120362 0.988 0.063 0.762 0.326 0.943 0.071 0.959 0.053 0.951 0.053 HD 96116 1.045 0.066 1.162 0.395 1.066 0.080 1.055 0.052 1.060 0.059 HD 120491 0.691 0.045 0.338 0.233 0.708 0.053 0.636 0.052 0.663 0.032 HD 96276 1.114 0.070 1.444 0.487 1.166 0.088 1.145 0.054 1.155 0.051 HD 122308 0.844 0.054 0.563 0.226 0.877 0.066 0.762 0.053 0.803 0.034 HD 96290 1.150 0.073 1.673 0.487 1.184 0.088 1.178 0.052 1.181 0.049 HD 122474 1.084 0.069 0.886 0.381 1.060 0.081 1.013 0.054 1.036 0.047 HD 96673 0.773 0.052 0.418 0.315 0.780 0.059 0.717 0.053 0.745 0.039 HD 123319 0.872 0.055 0.813 0.344 0.949 0.072 0.822 0.052 0.847 0.058 HD 97320 0.881 0.056 1.343 0.424 1.124 0.084 0.827 0.051 1.003 0.071 HD 123619 1.070 0.068 1.648 0.612 1.231 0.093 1.002 0.053 1.150 0.066 HD 98284 0.879 0.056 1.074 0.379 1.061 0.080 0.785 0.051 0.970 0.094 HD 123651 0.954 0.060 1.412 0.486 1.104 0.083 0.856 0.052 1.029 0.069 HD 100289 0.982 0.062 0.742 0.300 0.967 0.073 0.900 0.055 0.933 0.051 HD 125271 0.765 0.051 0.343 0.212 0.768 0.058 0.700 0.052 0.733 0.028 HD 101339 1.005 0.064 0.990 0.400 1.035 0.079 0.970 0.053 0.997 0.048 HD 125522 0.716 0.046 0.414 0.244 0.767 0.059 0.671 0.052 0.693 0.044 HD 101367 1.093 0.070 1.224 0.494 1.100 0.083 1.000 0.051 1.097 0.059 HD 125595 0.839 0.073 0.285 0.344 0.775 0.058 0.756 0.055 0.765 0.039 HD 101612 1.099 0.070 1.453 0.448 1.244 0.093 1.041 0.051 1.171 0.058 HD 125612 1.152 0.073 1.021 0.385 1.092 0.083 1.133 0.051 1.113 0.049 HD 101644 0.875 0.055 0.996 0.421 0.985 0.075 0.824 0.053 0.930 0.065 HD 126681 0.730 0.046 0.832 0.294 0.888 0.067 0.679 0.054 0.781 0.069 HD 101650 0.696 0.083 0.161 0.366 0.671 0.051 0.600 0.056 0.635 0.050 HD 126793 0.916 0.058 1.192 0.428 1.111 0.084 0.803 0.053 1.014 0.097 HD 102136 0.918 0.058 0.611 0.249 0.909 0.069 0.855 0.053 0.882 0.042 HD 126803 0.830 0.053 0.923 0.382 0.970 0.074 0.752 0.051 0.876 0.093 HD 102300 1.094 0.071 1.145 0.437 1.233 0.092 1.038 0.083 1.119 0.089 HD 126829 0.733 0.047 0.513 0.387 0.758 0.058 0.708 0.053 0.720 0.042 HD 102843 1.017 0.065 0.507 0.215 0.921 0.070 0.961 0.054 0.941 0.041 HD 127124 0.857 0.055 0.686 0.383 0.884 0.068 0.798 0.052 0.827 0.063

c 2002 RAS, MNRAS 000, 1–?? On the mass estimation for FGK stars:comparison of several methods 15

Table A2. Continuation

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

HD 128113 0.824 0.053 0.493 0.255 0.857 0.065 0.745 0.052 0.785 0.035 HD 156098 1.400 0.090 3.954 1.244 1.743 0.130 1.723 0.054 1.733 0.078 HD 128431 0.886 0.056 0.744 0.293 0.956 0.072 0.788 0.054 0.837 0.054 HD 156411 1.238 0.082 1.719 0.520 1.478 0.110 1.246 0.055 1.362 0.077 HD 128571 1.068 0.068 1.399 0.442 1.219 0.092 0.997 0.054 1.144 0.064 HD 156423 0.802 0.051 0.631 0.314 0.877 0.067 0.731 0.051 0.767 0.064 HD 129191 1.140 0.073 1.093 0.425 1.114 0.085 1.100 0.051 1.107 0.042 HD 156517 0.849 0.054 0.615 0.356 0.847 0.064 0.787 0.053 0.817 0.034 HD 129829 1.080 0.068 1.692 0.651 1.134 0.086 1.109 0.059 1.121 0.055 HD 156991 1.048 0.066 1.005 0.423 1.027 0.079 1.042 0.056 1.035 0.047 HD 130989 1.215 0.077 2.364 0.749 1.493 0.111 1.344 0.053 1.419 0.076 HD 157668 0.838 0.053 0.663 0.303 0.876 0.067 0.761 0.056 0.800 0.040 HD 131183 1.104 0.071 1.127 0.352 1.162 0.087 0.994 0.052 1.115 0.079 HD 160089 1.171 0.075 2.655 1.024 1.191 0.090 1.200 0.051 1.195 0.065 HD 131218 1.018 0.064 0.986 0.353 1.012 0.076 1.012 0.053 1.012 0.038 HD 160836 0.749 0.048 0.382 0.240 0.739 0.056 0.681 0.058 0.710 0.037 HD 131565 0.962 0.061 1.017 0.411 1.024 0.077 0.864 0.053 0.990 0.071 HD 161256 1.101 0.070 0.886 0.301 1.095 0.082 0.982 0.053 1.039 0.061 HD 131664 1.150 0.073 1.541 0.522 1.145 0.086 1.137 0.051 1.147 0.051 HD 161555 1.203 0.078 1.422 0.514 1.306 0.098 1.232 0.085 1.269 0.092 HD 132411 0.728 0.048 0.368 0.266 0.761 0.058 0.681 0.053 0.705 0.035 HD 161566 1.179 0.077 2.286 0.772 1.490 0.111 1.288 0.062 1.389 0.074 HD 132569 0.790 0.050 0.537 0.275 0.820 0.063 0.734 0.053 0.762 0.044 HD 163102 1.185 0.075 2.588 1.199 1.283 0.096 1.272 0.058 1.277 0.058 HD 133633 0.888 0.057 1.111 0.490 1.030 0.079 0.800 0.053 0.959 0.086 HD 163436 0.838 0.055 0.560 0.368 0.844 0.065 0.779 0.055 0.808 0.045 HD 134702 1.028 0.065 1.044 0.438 1.044 0.079 1.031 0.054 1.038 0.038 HD 165131 1.088 0.069 1.076 0.389 1.085 0.082 1.086 0.053 1.086 0.035 HD 134929 0.965 0.062 1.228 1.392 1.055 0.111 0.863 0.053 1.010 0.101 HD 166745 1.106 0.071 0.892 0.395 1.070 0.082 0.994 0.051 1.031 0.064 HD 135468 1.285 0.082 2.816 0.868 1.562 0.116 1.477 0.055 1.519 0.081 HD 167677 0.907 0.058 0.996 0.382 1.014 0.077 0.828 0.054 0.952 0.067 HD 135625 1.179 0.075 1.525 0.578 1.257 0.094 1.177 0.054 1.218 0.065 HD 168769 0.934 0.059 0.585 0.256 0.897 0.069 0.894 0.055 0.896 0.048 HD 137010 0.753 0.050 0.300 0.252 0.734 0.057 0.676 0.056 0.705 0.044 HD 168863 0.855 0.059 0.578 0.610 0.837 0.064 0.798 0.052 0.817 0.047 HD 137676 0.966 0.065 1.210 0.424 1.249 0.094 0.896 0.051 1.088 0.112 HD 168870 0.864 0.055 0.782 0.367 0.946 0.073 0.771 0.054 0.823 0.064 HD 138799 0.924 0.059 0.732 0.370 0.944 0.072 0.842 0.052 0.883 0.055 HD 170958 0.948 0.060 1.093 0.549 0.894 0.068 0.915 0.054 0.932 0.049 HD 138914 0.826 0.053 0.555 0.304 0.853 0.065 0.776 0.052 0.801 0.045 HD 171825 0.787 0.050 0.531 0.279 0.802 0.060 0.740 0.054 0.764 0.041 HD 139189 0.872 0.056 0.635 0.400 0.879 0.068 0.800 0.053 0.836 0.061 HD 171942 0.988 0.063 0.819 0.306 1.005 0.076 0.898 0.054 0.943 0.061 HD 139332 0.846 0.056 0.392 0.235 0.815 0.062 0.762 0.054 0.788 0.034 HD 172568 0.926 0.059 1.075 0.382 1.008 0.076 0.861 0.053 0.967 0.058 HD 139536 0.853 0.054 1.068 0.893 0.875 0.069 0.862 0.058 0.869 0.064 HD 172643 0.967 0.061 0.732 0.288 0.958 0.073 0.948 0.053 0.953 0.052 HD 139590 1.187 0.075 2.091 0.699 1.277 0.096 1.228 0.054 1.253 0.047 HD 173885 1.148 0.073 2.490 0.859 1.408 0.106 1.148 0.053 1.278 0.047 HD 139710 0.864 0.055 0.461 0.251 0.839 0.065 0.791 0.056 0.815 0.036 HD 174153 1.129 0.071 1.659 0.572 1.217 0.091 1.140 0.053 1.178 0.052 HD 139879 1.211 0.076 2.287 0.849 1.226 0.092 1.251 0.051 1.238 0.038 HD 176354 1.224 0.083 1.078 0.390 1.277 0.095 1.147 0.085 1.185 0.071 HD 140785 1.142 0.075 1.486 0.460 1.312 0.098 1.084 0.054 1.227 0.061 HD 176535 0.758 0.051 0.312 0.221 0.740 0.056 0.685 0.055 0.713 0.035 HD 141128 1.287 0.081 2.664 0.974 1.328 0.099 1.313 0.053 1.320 0.060 HD 176666 1.009 0.064 1.665 0.537 1.128 0.085 1.000 0.056 1.069 0.041 HD 141597 1.098 0.070 1.514 0.590 1.273 0.096 1.054 0.057 1.186 0.084 HD 177033 0.785 0.051 0.461 0.343 0.780 0.060 0.764 0.054 0.772 0.035 HD 141598 0.995 0.064 0.892 0.372 1.040 0.079 0.873 0.052 0.943 0.056 HD 177122 1.072 0.068 1.157 0.418 1.092 0.082 1.084 0.054 1.088 0.062 HD 141624 0.994 0.063 0.939 0.325 1.083 0.082 0.875 0.053 0.967 0.078 HD 178904 1.066 0.068 1.193 0.438 1.102 0.083 1.000 0.054 1.084 0.064 HD 142879 0.928 0.059 0.841 0.280 0.988 0.074 0.850 0.060 0.889 0.055 HD 179346 1.113 0.071 2.061 0.764 1.132 0.085 1.140 0.052 1.136 0.062 HD 143638 1.022 0.065 1.091 0.423 1.088 0.083 0.962 0.059 1.055 0.076 HD 181249 0.836 0.056 0.404 0.215 0.836 0.063 0.752 0.052 0.794 0.038 HD 143790 1.381 0.090 2.643 0.917 1.689 0.126 1.552 0.061 1.620 0.085 HD 181428 1.165 0.074 1.914 0.690 1.266 0.095 1.191 0.053 1.229 0.051 HD 144342 0.959 0.061 0.807 0.317 0.947 0.071 0.910 0.053 0.929 0.051 HD 181720 0.984 0.064 1.318 0.523 1.219 0.093 0.881 0.051 1.101 0.103 HD 144846 1.153 0.073 1.320 0.544 1.132 0.087 1.164 0.053 1.159 0.064 HD 185283 0.804 0.060 0.482 0.477 0.812 0.061 0.761 0.058 0.782 0.044 HD 144880 1.090 0.070 1.655 0.589 1.269 0.095 1.071 0.067 1.179 0.068 HD 186302 1.012 0.064 0.845 0.303 1.011 0.076 0.990 0.055 1.000 0.047 HD 145377 1.135 0.072 1.410 0.513 1.137 0.086 1.155 0.054 1.146 0.055 HD 187760 0.685 0.044 0.388 0.303 0.723 0.055 0.652 0.058 0.669 0.041 HD 145927 1.062 0.067 0.840 0.300 1.046 0.079 1.034 0.056 1.040 0.042 HD 188091 0.919 0.060 0.519 0.297 0.886 0.068 0.814 0.052 0.850 0.047 HD 147147 0.761 0.049 0.511 0.413 0.779 0.060 0.741 0.053 0.751 0.040 HD 188815 1.061 0.067 1.323 0.416 1.249 0.094 0.999 0.061 1.155 0.075 HD 147195 0.971 0.062 1.171 0.494 1.037 0.079 0.885 0.054 1.004 0.056 HD 189004 0.870 0.056 0.671 0.345 0.906 0.069 0.804 0.052 0.837 0.040 HD 148156 1.230 0.078 1.515 0.546 1.196 0.090 1.231 0.052 1.231 0.055 HD 189987 0.805 0.057 0.393 0.293 0.803 0.061 0.749 0.055 0.776 0.039 HD 148211 0.968 0.062 1.329 0.461 1.198 0.090 0.857 0.051 1.083 0.082 HD 190204 0.932 0.059 1.199 0.672 0.965 0.075 0.949 0.053 0.957 0.035 HD 148577 1.054 0.067 1.237 0.438 1.168 0.088 0.937 0.054 1.111 0.091 HD 190524 1.018 0.064 1.102 0.400 1.063 0.080 1.014 0.056 1.041 0.053 HD 149200 1.223 0.077 2.991 0.963 1.321 0.099 1.310 0.052 1.315 0.048 HD 190613 1.081 0.069 1.017 0.353 1.118 0.084 0.979 0.055 1.049 0.057 HD 149396 1.057 0.067 1.298 0.471 1.079 0.082 1.024 0.051 1.068 0.040 HD 191033 1.108 0.070 1.497 0.524 1.204 0.090 1.101 0.054 1.156 0.053 HD 149724 1.202 0.078 1.206 0.476 1.194 0.090 1.061 0.051 1.198 0.077 HD 191285 0.702 0.046 0.353 0.250 0.726 0.055 0.658 0.053 0.680 0.042 HD 150139 1.019 0.066 1.389 0.527 1.245 0.094 0.899 0.054 1.132 0.092 HD 191797 0.835 0.053 0.788 0.397 0.877 0.067 0.796 0.052 0.815 0.046 HD 150437 1.188 0.076 1.129 0.436 1.167 0.088 1.089 0.051 1.148 0.064 HD 191902 0.768 0.053 0.456 0.366 0.811 0.063 0.713 0.052 0.741 0.049 HD 150474 1.110 0.073 1.409 0.483 1.285 0.096 1.115 0.052 1.200 0.071 HD 192865 1.230 0.078 2.607 0.798 1.385 0.104 1.320 0.053 1.353 0.054 HD 151692 0.766 0.052 0.407 0.382 0.762 0.058 0.747 0.059 0.754 0.047 HD 193406 0.701 0.045 0.294 0.219 0.698 0.053 0.640 0.055 0.669 0.035 HD 151772 1.125 0.071 3.790 1.511 1.317 0.098 1.188 0.051 1.252 0.051 HD 194717 0.894 0.058 0.521 0.210 0.929 0.070 0.795 0.052 0.845 0.033 HD 151933 1.061 0.068 0.710 0.297 1.075 0.082 0.926 0.056 0.993 0.047 HD 195145 1.057 0.067 0.916 0.386 1.030 0.079 1.000 0.052 1.015 0.050 HD 152433 1.111 0.070 1.900 0.741 1.241 0.094 1.107 0.055 1.176 0.065 HD 195200 1.143 0.073 1.620 0.562 1.240 0.093 1.140 0.053 1.192 0.063 HD 152533 0.803 0.055 0.424 0.336 0.793 0.060 0.738 0.057 0.765 0.042 HD 196384 1.183 0.075 2.915 0.966 1.256 0.094 1.226 0.055 1.241 0.053 HD 153276 1.111 0.070 1.491 0.575 1.163 0.088 1.108 0.054 1.137 0.048 HD 196397 1.038 0.067 0.626 0.348 0.955 0.073 0.912 0.051 0.934 0.050 HD 153950 1.142 0.072 1.595 0.484 1.243 0.093 1.136 0.052 1.192 0.060 HD 197300 1.077 0.068 1.364 0.549 1.048 0.079 1.067 0.054 1.072 0.048 HD 154195 1.043 0.066 1.043 0.514 1.081 0.084 1.030 0.057 1.043 0.070 HD 197921 0.861 0.058 0.545 0.403 0.844 0.064 0.800 0.052 0.822 0.042 HD 154387 0.714 0.046 0.405 0.275 0.731 0.055 0.700 0.053 0.707 0.037 HD 199086 1.157 0.073 1.996 0.717 1.167 0.088 1.200 0.052 1.184 0.057 HD 155717 0.796 0.051 0.449 0.268 0.788 0.060 0.756 0.054 0.772 0.039 HD 199289 0.840 0.053 1.525 0.502 1.087 0.082 0.777 0.052 0.963 0.070 HD 155968 1.099 0.070 1.029 0.394 1.076 0.081 1.074 0.055 1.075 0.047 HD 199868 1.114 0.071 1.591 0.502 1.220 0.091 1.094 0.053 1.167 0.049 HD 156079 1.222 0.078 1.713 0.570 1.307 0.098 1.218 0.055 1.264 0.060 HD 200083 0.783 0.052 0.469 0.354 0.790 0.060 0.732 0.053 0.757 0.036

c 2002 RAS, MNRAS 000, 1–?? 16 F. J. G. Pinheiro et al.

Table A2. Continuation

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

HD 200143 0.872 0.056 0.655 0.356 0.871 0.067 0.800 0.052 0.835 0.047 HD 221638 1.129 0.071 1.538 0.623 1.209 0.090 1.146 0.058 1.177 0.065 HD 200349 0.743 0.048 0.473 0.269 0.771 0.058 0.694 0.054 0.718 0.041 HD 221974 0.988 0.067 0.572 0.477 0.915 0.071 0.859 0.052 0.887 0.048 HD 200538 1.165 0.074 1.535 0.516 1.232 0.093 1.150 0.054 1.199 0.058 HD 222721 0.875 0.056 0.755 0.315 0.945 0.072 0.794 0.054 0.835 0.063 HD 200633 1.067 0.067 1.168 0.419 1.073 0.081 1.077 0.054 1.075 0.058 HD 223272 0.906 0.058 0.609 0.393 0.878 0.067 0.817 0.056 0.848 0.044 HD 201161 0.820 0.055 0.388 0.283 0.793 0.060 0.766 0.053 0.779 0.037 HD 223315 1.089 0.069 0.700 0.295 0.975 0.074 1.027 0.051 1.001 0.052 HD 201422 0.994 0.063 1.175 0.450 1.020 0.077 0.989 0.055 1.007 0.053 HD 224047 0.842 0.054 0.694 0.333 0.899 0.069 0.778 0.052 0.810 0.047 HD 201496 1.093 0.069 1.186 0.403 1.131 0.085 1.066 0.054 1.112 0.055 HD 224063 1.083 0.070 0.869 0.381 1.079 0.082 0.959 0.053 1.019 0.063 HD 202209 1.067 0.067 1.352 0.539 1.050 0.079 1.078 0.055 1.073 0.063 HD 224230 0.802 0.052 0.492 0.358 0.801 0.061 0.780 0.053 0.791 0.045 HD 202389 0.728 0.048 0.415 0.336 0.755 0.058 0.687 0.052 0.708 0.032 HD 224287 0.882 0.056 0.561 0.256 0.911 0.070 0.777 0.052 0.829 0.033 HD 202819 0.733 0.049 0.377 0.297 0.753 0.057 0.700 0.052 0.717 0.033 HD 224432 0.796 0.052 0.451 0.341 0.797 0.061 0.749 0.057 0.773 0.036 HD 202871 1.079 0.068 1.258 0.469 1.108 0.083 1.099 0.052 1.103 0.058 HD 224433 1.008 0.064 0.744 0.272 0.972 0.073 0.969 0.052 0.971 0.040 HD 203335 1.154 0.073 2.261 0.820 1.271 0.095 1.205 0.056 1.238 0.055 HD 224578 1.107 0.070 1.755 0.697 1.132 0.086 1.134 0.053 1.133 0.056 HD 203771 0.859 0.057 0.504 0.446 0.820 0.063 0.792 0.055 0.806 0.042 HD 224685 0.884 0.056 0.678 0.293 0.936 0.071 0.788 0.053 0.836 0.055 HD 203897 0.858 0.055 0.497 0.231 0.856 0.065 0.766 0.053 0.811 0.055 HD 225297 1.110 0.070 1.664 0.521 1.183 0.089 1.159 0.054 1.171 0.069 HD 204287 1.128 0.073 1.264 0.397 1.254 0.094 1.040 0.056 1.191 0.089 HD 290038 0.849 0.055 0.660 0.417 0.870 0.067 0.797 0.053 0.823 0.049 HD 205294 1.186 0.076 1.998 0.671 1.414 0.106 1.163 0.054 1.300 0.068 HD 290327 0.952 0.061 0.816 0.357 0.992 0.076 0.841 0.055 0.897 0.057 HD 205591 1.189 0.075 3.579 1.252 1.325 0.099 1.300 0.055 1.313 0.054 HD 291763 0.718 0.046 0.646 0.409 0.836 0.065 0.671 0.052 0.694 0.061 HD 206116 1.209 0.076 2.235 0.847 1.248 0.094 1.260 0.051 1.254 0.063 HD 297396 0.807 0.057 0.340 0.310 0.765 0.058 0.743 0.057 0.754 0.041 HD 206630 0.723 0.046 0.448 0.251 0.771 0.058 0.671 0.052 0.697 0.022 HD 309701 0.748 0.048 0.400 0.141 0.776 0.059 0.700 0.051 0.724 0.048 HD 207190 1.082 0.069 1.430 0.477 1.268 0.095 1.018 0.053 1.175 0.063 HD 323631 0.784 0.050 0.559 0.423 0.835 0.069 0.734 0.053 0.759 0.040 HD 207699 0.802 0.052 0.436 0.281 0.806 0.061 0.740 0.053 0.771 0.032 HD 324492 0.854 0.068 0.061 0.111 0.654 0.064 0.629 0.059 0.641 0.057 HD 207832 1.068 0.068 0.825 0.311 1.012 0.076 1.041 0.054 1.026 0.052 HD 326267 0.747 0.051 0.233 0.191 0.719 0.055 0.658 0.056 0.688 0.038 HD 208068 0.983 0.062 1.249 0.444 1.051 0.079 0.977 0.057 1.017 0.044 HD 329788 0.886 0.057 0.371 0.235 0.831 0.064 0.791 0.059 0.811 0.048 HD 208672 1.105 0.070 1.556 0.526 1.106 0.083 1.126 0.053 1.116 0.053 BD-002387 0.797 0.052 0.451 0.366 0.771 0.059 0.777 0.054 0.774 0.033 HD 209449 1.283 0.083 1.347 0.411 1.285 0.096 1.241 0.055 1.284 0.060 BD-010184 0.729 0.050 0.357 0.240 0.761 0.057 0.700 0.052 0.715 0.048 HD 209566 1.018 0.065 0.824 0.322 1.003 0.076 0.933 0.052 0.968 0.055 BD-012505 0.742 0.048 0.359 0.274 0.719 0.054 0.700 0.053 0.710 0.044 HD 210272 1.081 0.070 1.557 0.478 1.312 0.098 1.068 0.052 1.197 0.068 BD-033746 0.604 0.039 0.343 0.267 0.683 0.052 0.571 0.055 0.587 0.041 HD 210320 1.064 0.069 0.871 0.361 1.061 0.080 0.946 0.053 1.004 0.082 BD-034797 0.804 0.066 0.283 0.374 0.751 0.057 0.731 0.054 0.741 0.032 HD 210329 0.806 0.053 0.609 0.358 0.857 0.066 0.757 0.052 0.781 0.064 BD-044138 0.726 0.052 0.206 0.293 0.670 0.051 0.621 0.057 0.645 0.037 HD 210507 0.859 0.055 0.573 0.353 0.847 0.065 0.800 0.052 0.824 0.043 BD-050484 0.692 0.046 0.351 0.315 0.729 0.056 0.646 0.058 0.669 0.036 HD 210573 0.799 0.051 0.560 0.368 0.810 0.062 0.758 0.053 0.779 0.039 BD-050578 1.000 0.064 0.470 0.224 0.902 0.069 0.937 0.051 0.920 0.050 HD 211188 0.838 0.054 0.494 0.246 0.837 0.064 0.761 0.053 0.799 0.049 BD-053176 0.770 0.051 0.390 0.365 0.763 0.059 0.723 0.054 0.743 0.041 HD 211317 1.217 0.079 1.568 0.545 1.266 0.095 1.214 0.052 1.241 0.057 BD-053596 0.699 0.048 0.276 0.210 0.715 0.054 0.641 0.053 0.670 0.030 HD 211534 0.793 0.051 0.461 0.274 0.817 0.064 0.725 0.051 0.759 0.035 BD-054065 0.766 0.049 0.416 0.239 0.789 0.061 0.710 0.054 0.738 0.027 HD 211583 0.797 0.055 0.359 0.398 0.754 0.057 0.753 0.053 0.753 0.029 BD-060904 0.822 0.052 0.472 0.252 0.817 0.063 0.774 0.054 0.795 0.044 HD 212036 1.031 0.066 0.975 0.398 1.054 0.080 0.953 0.055 1.003 0.061 BD-063481 0.782 0.053 0.435 0.315 0.795 0.060 0.728 0.053 0.755 0.036 HD 212231 1.047 0.068 0.981 0.308 1.170 0.088 0.897 0.051 1.014 0.078 BD-064196 0.782 0.054 0.435 0.391 0.790 0.060 0.774 0.060 0.778 0.045 HD 212918 0.807 0.051 0.550 0.279 0.827 0.063 0.755 0.054 0.781 0.052 BD-064756 0.694 0.045 0.369 0.305 0.700 0.053 0.657 0.054 0.676 0.036 HD 213852 0.906 0.060 0.414 0.251 0.849 0.064 0.800 0.052 0.825 0.041 BD-082534 0.794 0.051 0.618 0.278 0.920 0.070 0.700 0.051 0.747 0.056 HD 214094 1.239 0.079 2.295 0.665 1.448 0.108 1.351 0.081 1.400 0.065 BD-082823 0.783 0.051 0.467 0.364 0.784 0.060 0.738 0.054 0.760 0.042 HD 214383 0.774 0.049 0.412 0.257 0.767 0.059 0.741 0.054 0.754 0.029 BD-090872 0.735 0.050 0.276 0.199 0.718 0.054 0.656 0.054 0.687 0.032 HD 214867 1.022 0.065 1.049 0.435 0.981 0.075 1.000 0.053 1.011 0.044 BD-091261 0.618 0.040 0.345 0.292 0.669 0.051 0.574 0.051 0.596 0.039 HD 214954 1.064 0.068 1.378 0.619 1.102 0.083 1.041 0.054 1.083 0.054 BD-092670 0.772 0.050 0.476 0.320 0.776 0.059 0.723 0.053 0.748 0.043 HD 214998 0.826 0.054 0.417 0.305 0.793 0.060 0.753 0.059 0.773 0.050 BD-094191 0.733 0.049 0.522 0.572 0.793 0.068 0.700 0.053 0.716 0.046 HD 215497 0.921 0.061 0.732 0.532 0.908 0.069 0.846 0.052 0.877 0.051 BD-112763 0.770 0.049 0.355 0.184 0.763 0.058 0.694 0.054 0.728 0.035 HD 215625 1.182 0.075 1.702 0.618 1.190 0.089 1.200 0.054 1.195 0.051 BD-120327 0.715 0.049 0.374 0.342 0.756 0.058 0.675 0.054 0.695 0.040 HD 215722 0.759 0.051 0.341 0.295 0.740 0.056 0.721 0.053 0.730 0.040 BD-123458 0.621 0.042 0.296 0.336 0.629 0.048 0.500 0.052 0.561 0.039 HD 215902 0.905 0.058 0.678 0.281 0.932 0.071 0.824 0.060 0.864 0.043 BD-130116 0.679 0.052 0.171 0.230 0.666 0.052 0.573 0.052 0.620 0.039 HD 215906 1.080 0.068 1.944 0.762 1.227 0.092 1.057 0.067 1.153 0.077 BD-130321 0.790 0.054 0.330 0.314 0.740 0.056 0.737 0.053 0.739 0.039 HD 216008 1.055 0.067 1.009 0.334 1.088 0.082 0.967 0.053 1.032 0.062 BD-131161 0.983 0.063 0.618 0.259 0.940 0.071 0.900 0.053 0.920 0.039 HD 216215 0.857 0.055 0.510 0.251 0.854 0.065 0.792 0.054 0.823 0.049 BD-140184 0.723 0.051 0.353 0.342 0.763 0.058 0.680 0.054 0.701 0.038 HD 217221 0.891 0.057 0.669 0.342 0.889 0.068 0.824 0.053 0.857 0.055 BD-145003 0.667 0.045 0.289 0.304 0.705 0.056 0.612 0.054 0.639 0.041 HD 217395 1.038 0.066 1.104 0.359 1.068 0.080 1.046 0.052 1.057 0.054 BD-160308 0.802 0.051 0.592 0.293 0.862 0.067 0.735 0.054 0.769 0.043 HD 217786 1.091 0.070 1.357 0.490 1.203 0.090 1.068 0.063 1.147 0.083 BD-160931 0.790 0.053 0.493 0.414 0.810 0.062 0.743 0.061 0.767 0.047 HD 217958 1.174 0.074 1.422 0.578 1.165 0.088 1.159 0.051 1.169 0.046 BD-170063 0.812 0.059 0.293 0.253 0.768 0.058 0.736 0.056 0.752 0.040 HD 218340 1.108 0.071 0.984 0.434 1.087 0.082 1.100 0.051 1.094 0.046 BD-173242 0.688 0.046 0.393 0.437 0.719 0.055 0.677 0.054 0.682 0.033 HD 218379 1.258 0.081 1.616 0.504 1.385 0.104 1.323 0.055 1.354 0.061 BD-195953 0.745 0.049 0.568 0.509 0.778 0.059 0.717 0.054 0.731 0.037 HD 218750 0.914 0.059 0.712 0.419 0.917 0.071 0.833 0.052 0.873 0.070 BD-213153 0.723 0.049 0.309 0.255 0.717 0.054 0.660 0.052 0.688 0.042 HD 218885 0.976 0.062 0.650 0.303 0.971 0.074 0.935 0.051 0.953 0.038 BD-223528 0.778 0.054 0.293 0.227 0.757 0.057 0.697 0.054 0.727 0.046 HD 219495 0.817 0.054 0.433 0.341 0.778 0.058 0.759 0.053 0.768 0.036 HIP102025 0.732 0.049 0.431 0.317 0.782 0.060 0.694 0.053 0.713 0.037 HD 220456 1.061 0.067 0.994 0.365 1.050 0.079 1.056 0.053 1.053 0.053 HIP102964 0.748 0.048 0.446 0.231 0.775 0.059 0.700 0.052 0.724 0.025 HD 220894 1.157 0.073 1.912 0.710 1.206 0.091 1.200 0.053 1.203 0.051 HIP103867 0.716 0.056 0.117 0.111 0.664 0.051 0.585 0.053 0.625 0.029 HD 221343 1.075 0.068 1.101 0.403 1.049 0.079 1.064 0.052 1.069 0.046 HIP104856 0.804 0.051 0.570 0.266 0.845 0.064 0.748 0.052 0.776 0.036

c 2002 RAS, MNRAS 000, 1–?? On the mass estimation for FGK stars:comparison of several methods 17

Table A2. Mass estimate for Bruntt et al’s targets according to different methods (in solar units).

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

HIP105506 0.811 0.053 0.412 0.346 0.790 0.060 0.740 0.060 0.765 0.044 HIP 38324 0.698 0.050 0.292 0.273 0.707 0.054 0.642 0.052 0.670 0.033 HIP 10741 0.784 0.051 0.342 0.224 0.762 0.058 0.737 0.054 0.749 0.025 HIP 39470 0.671 0.045 0.245 0.192 0.679 0.052 0.618 0.052 0.644 0.030 HIP108216 0.694 0.045 0.399 0.289 0.740 0.056 0.653 0.053 0.673 0.034 HIP 41659 0.802 0.052 0.542 0.246 0.884 0.067 0.725 0.052 0.763 0.044 HIP109149 0.810 0.052 0.329 0.225 0.765 0.059 0.752 0.052 0.759 0.033 HIP 45301 0.760 0.053 0.517 0.582 0.783 0.059 0.744 0.053 0.752 0.041 HIP109421 0.688 0.050 0.305 0.374 0.698 0.055 0.634 0.056 0.661 0.043 HIP 46933 0.711 0.063 0.244 0.328 0.709 0.054 0.651 0.053 0.680 0.040 HIP113596 0.733 0.053 0.217 0.210 0.704 0.054 0.643 0.056 0.674 0.037 HIP 5114 0.690 0.046 0.300 0.342 0.747 0.057 0.627 0.057 0.659 0.032 HIP116374 0.770 0.051 0.233 0.291 0.704 0.053 0.700 0.055 0.702 0.036 HIP 5158 0.850 0.066 0.260 0.337 0.743 0.058 0.758 0.056 0.750 0.046 HIP116939 0.843 0.055 0.499 0.266 0.848 0.064 0.782 0.053 0.812 0.047 HIP 54446 0.793 0.051 0.595 0.328 0.823 0.063 0.745 0.053 0.769 0.047 HIP 12147 0.783 0.050 0.697 0.338 0.855 0.065 0.736 0.052 0.760 0.048 HIP 54597 0.750 0.049 0.417 0.263 0.767 0.058 0.700 0.054 0.725 0.033 HIP 15587 0.877 0.056 0.482 0.229 0.847 0.065 0.840 0.052 0.843 0.040 HIP 57688 0.764 0.051 0.312 0.212 0.748 0.056 0.700 0.055 0.724 0.033 HIP 16094 0.801 0.052 0.453 0.312 0.788 0.059 0.774 0.053 0.781 0.033 HIP 58348 0.817 0.055 0.358 0.312 0.779 0.060 0.747 0.054 0.763 0.035 HIP 17346 0.757 0.053 0.302 0.252 0.742 0.056 0.700 0.055 0.721 0.034 HIP 59925 0.696 0.048 0.310 0.299 0.707 0.054 0.647 0.058 0.672 0.031 HIP 1745 0.871 0.056 0.519 0.226 0.911 0.069 0.763 0.052 0.817 0.031 HIP 61406 0.812 0.054 0.378 0.390 0.767 0.061 0.777 0.054 0.772 0.040 HIP 18918 0.726 0.052 0.289 0.271 0.727 0.056 0.668 0.056 0.697 0.040 HIP 64965 0.610 0.040 0.257 0.185 0.643 0.050 0.550 0.052 0.580 0.035 HIP 20444 0.800 0.052 0.385 0.261 0.781 0.059 0.744 0.053 0.763 0.036 HIP 67126 0.777 0.053 0.402 0.296 0.808 0.062 0.713 0.051 0.745 0.045 HIP 21934 0.819 0.076 0.197 0.268 0.723 0.055 0.700 0.052 0.712 0.038 HIP 69224 0.847 0.055 0.415 0.225 0.842 0.064 0.761 0.052 0.801 0.044 HIP 25612 0.663 0.049 0.227 0.226 0.683 0.052 0.600 0.052 0.631 0.031 HIP 7058 0.740 0.048 0.427 0.455 0.729 0.055 0.680 0.055 0.705 0.039 HIP 26013 0.822 0.054 0.508 0.356 0.814 0.061 0.763 0.055 0.789 0.040 HIP 7743 0.739 0.051 0.437 0.378 0.766 0.058 0.716 0.052 0.727 0.036 HIP 31639 0.821 0.052 0.670 0.301 0.896 0.069 0.744 0.053 0.783 0.062 HIP 78242 0.914 0.058 0.642 0.339 0.909 0.070 0.827 0.052 0.868 0.055 HIP 32127 0.795 0.051 0.712 0.305 0.923 0.070 0.734 0.052 0.764 0.075 HIP 80083 0.625 0.041 0.341 0.409 0.659 0.053 0.574 0.052 0.600 0.060 HIP 32812 0.837 0.056 0.486 0.361 0.824 0.063 0.775 0.056 0.800 0.041 HIP 88316 0.895 0.058 0.651 0.340 0.906 0.069 0.821 0.052 0.858 0.045 HIP 33392 0.804 0.051 0.587 0.331 0.810 0.061 0.792 0.053 0.798 0.038 HIP 9398 0.690 0.046 0.250 0.251 0.684 0.052 0.612 0.052 0.648 0.026 HIP 35992 0.867 0.057 0.393 0.242 0.838 0.064 0.772 0.052 0.805 0.025 HIP 96240 0.769 0.049 0.506 0.338 0.788 0.061 0.725 0.053 0.746 0.035 HIP 36347 0.769 0.052 0.301 0.260 0.729 0.056 0.713 0.055 0.721 0.033 HIP 99606 1.025 0.066 0.037 0.036 0.675 0.067 0.790 0.051 0.732 0.047

Table A3. Mass estimate for Bruntt et al’s targets according to different methods (in solar units).

star ID MDirect MTorres MHenry MPadova MMedian star ID MDirect MTorres MHenry MPadova MMedian M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M M ∆M

β Hyi 1.224 0.120 1.159 0.578 1.354 0.101 1.127 0.058 1.192 0.088 αCen B 0.925 0.072 1.027 0.548 0.916 0.069 0.859 0.059 0.920 0.055 τCet 0.799 0.059 1.002 0.526 0.921 0.069 0.776 0.052 0.860 0.062 HR5803 1.228 0.109 1.486 0.738 1.348 0.101 1.239 0.070 1.293 0.088 ιHor 1.185 0.098 1.212 0.595 1.175 0.088 1.200 0.062 1.192 0.062 γSer 1.166 0.105 1.296 0.631 1.324 0.099 1.148 0.070 1.231 0.085 αFor 1.214 0.120 1.522 0.780 1.455 0.109 1.145 0.084 1.334 0.114 µAra 1.160 0.100 1.248 0.648 1.177 0.088 1.045 0.058 1.168 0.074 δEri 1.144 0.130 1.225 0.624 1.282 0.096 1.257 0.073 1.241 0.083 70 Oph A 0.922 0.067 1.175 0.583 0.949 0.071 0.874 0.067 0.935 0.054 Procyon 1.463 0.140 1.566 0.777 1.594 0.119 1.500 0.077 1.533 0.093 ηSer 1.653 0.219 1.438 0.697 1.803 0.136 1.435 0.181 1.546 0.167 171 Pup 0.888 0.075 1.020 0.504 1.137 0.085 0.822 0.051 0.954 0.098 βAql 1.210 0.135 1.357 0.674 1.459 0.110 1.282 0.120 1.320 0.126 ξHya 2.125 0.269 2.811 1.372 2.404 0.180 2.848 0.088 2.607 0.233 δPav 1.120 0.095 1.057 0.516 1.092 0.082 1.000 0.060 1.074 0.068 βVir 1.284 0.112 1.326 0.644 1.351 0.101 1.295 0.067 1.310 0.071 γPav 0.948 0.074 1.140 0.580 1.159 0.087 0.836 0.054 1.043 0.100 ηBoo 1.489 0.159 1.830 1.045 1.644 0.123 1.590 0.068 1.617 0.095 τPsA 1.238 0.106 1.378 0.693 1.306 0.098 1.218 0.059 1.272 0.077 αCen A 1.128 0.092 1.209 0.623 1.146 0.086 1.062 0.060 1.137 0.065 νInd 0.960 0.112 0.990 0.487 1.477 0.111 0.815 0.052 0.975 0.171

c 2002 RAS, MNRAS 000, 1–??