Issue 
A&A
Volume 516, JuneJuly 2010



Article Number  A33  
Number of page(s)  5  
Section  Stellar structure and evolution  
DOI  https://doi.org/10.1051/00046361/201014326  
Published online  23 June 2010 
An improved method for estimating the masses of stars with transiting planets
B. Enoch^{1}  A. Collier Cameron^{1}  N. R. Parley^{1}  L. Hebb^{2}
1  School of Physics and Astronomy, University of St. Andrews, North
Haugh, St Andrews, KY16 9SS, UK
2  Vanderbilt University, Department of Physics and Astronomy,
Nashville, TN 37235, USA
Received 26 February 2010 / Accepted 6 April 2010
Abstract
Context. To determine the physical parameters of a
transiting planet and its host star from photometric and spectroscopic
analysis, it is essential to independently measure the stellar mass.
This is often achieved by the use of evolutionary tracks and
isochrones, but the mass result is only as reliable as the models used.
Aims. The recent paper by Torres et al. (2010,
A&ARv, 18, 67) showed that accurate values for stellar masses
and radii could be obtained from a calibration using
,
and [Fe/H].
We investigate whether a similarly good calibration can be obtained by
substituting log
 the fundamental parameter measured for the host star of a transiting
planet  for ,
and apply this to starexoplanet systems.
Methods. We perform a polynomial fit to stellar
binary data provided in Torres et al. (2010) to obtain the stellar mass
and radius as functions of ,
and [Fe/H],
with uncertainties on the fit produced from a Monte Carlo analysis. We
apply the resulting equations to measurements for seventeen SuperWASP
host stars, and also demonstrate the application of the calibration in
a Markov Chain Monte Carlo analysis to obtain accurate system
parameters where spectroscopic estimates of effective stellar
temperature and metallicity are available.
Results. We show that the calibration using log
produces accurate values for the stellar masses and radii; we obtain
masses and radii of the SuperWASP stars in good agreement with
isochrone analysis results. We ascertain that the mass calibration is
robust against uncertainties resulting from poor photometry, although a
good estimate of stellar radius requires goodquality transit light
curve to determine the duration of ingress and egress.
Key words: planetary systems
1 Introduction
There are currently over 400 known exoplanets, of which more than 60 transit their host stars^{}. This important transiting subset are the only planets for which the orbital inclination, and hence precise stellar and planetary parameters, may be determined. The fundamental parameters found for the host star and transiting planet are stellar density (see below) and planetary surface gravity (Southworth et al. 2004). To convert these into values for the radii of both, it is necessary to find the stellar mass. This is often arrived at iteratively via deriving a stellar density from the lightcurve analysis and a stellar effective temperature from spectroscopy and using these with model evolutionary tracks and isochrones of appropriate metallicity to find a stellar mass and age (Sozzetti et al. 2007). Further photometric and spectroscopic analysis may then be performed to arrive at final values for the masses and radii of the star and planet, see e.g. Hebb et al. (2009). The resulting values for masses and radii are therefore only as reliable as the evolutionary models used. A recent study by Southworth (2009) highlighted the fact that discrepancies between different sets of evolutionary models represent the dominant source of systematic uncertainty in planetary parameters. For example, they find that the spread of mass values obtained for HD 209458 using different models is around .
Here we develop a new onestep approach to determining the masses of exoplanet host stars from their effective temperatures, metallicities and photometric bulk densities. We base our method on the recent study by Torres et al. (2010) of the masses and radii of a large sample of wellcharacterised mainsequence stars belonging to noninteracting, eclipsing spectroscopic binaries. Torres et al. (2010) showed that accurate stellar masses and radii could be obtained using a calibration of stellar surface gravity, effective temperature and metallicity. They used a set of welldetermined measurements of , , [Fe/H], M and R from binary stars to obtain coefficients that allow mass and radius to be calculated directly for any normal star, without isochrone fitting.
Recently, the use of log in place of in the determination of starplanet system parameters has become widespread, see for example Sozzetti et al. (2007), Winn et al. (2008), Sozzetti et al. (2009) and Fernandez et al. (2009). Where high quality photometric data can be obtained of the transit event, the stellar parameters can be obtained more precisely using the stellar density value derived from the lightcurve than using the stellar surface gravity value from spectral analysis (Sozzetti et al. 2007).
In Sect. 2 we review the methodology for determining exoplanet hoststar densities from the transit geometry. We redetermine the mass and radius calibrations of Torres et al. (2010) using their data, and obtain comparably tight mass and radius calibrations using log in place of . In Sect. 3 we apply the method to the host stars of several transiting planets for which isochrone mass determinations have been published recently. In Sect. 4 we show how the method can be incorporated directly in a Markovchain Monte Carlo (MCMC) analysis, to give the stellar mass as a derived parameter.
2 Analysis
We used the tabulated data of Torres
et al. (2010) to perform our calibration. Those data
consist of 19 binary systems, i.e. 38 stars, for which the
metallicity is known, after excluding systems that contain preMain
Sequence stars. We fit a similar polynomial calibration, replacing
log g with log ,
and apply it to starexoplanet systems. The stellar density can be
obtained directly from only photometric measurements via fitting of a
transit event (Seager &
MallénOrnelas 2003): the ratio of semimajor axis to stellar
radius depends on the ratio of transit duration to orbital period via
(1) 
where , b is the impact parameter, T is the transit duration and P is the orbital period.
Combining this with Kepler's Third Law,
(2) 
where G is the gravitational constant, leads to an expression for the stellar density (Seager & MallénOrnelas 2003)
since (this is strictly true for planets on circular orbits only). Thus the stellar density may be obtained directly from parameters measurable from a highquality lightcurve: the duration and depth of transit, the impact parameter and the orbital period.
We used a Singular Value Decomposition (SVD) fit, weighted by
error on the mass or radius measurements, to obtain coefficients on
significant variables. The final fit gives coefficients for
,
X^{2}, log ,
log ,
log
and [Fe/H] for mass, and X,
and [Fe/H] for radius (the secondary terms are insignificant for the
radius fit). Thus the mass or radius may be computed by
To obtain errors on the coefficients, we carried out a Monte Carlo analysis of 50 000 runs in which, for each run, each value for , , [Fe/H] and M or R were perturbed randomly on a gaussian with standard deviation the error for that measurement. The set of 50 000 resulting coefficients were recorded, and the standard deviation of each coefficient within that set gave the error value for that coefficient. The fitted and error values for each of the mass and radius fits are given in Table 1. The resulting scatter in fitted less measured values is and . Figure 1 shows calibrated versus measured mass and radius.
Table 1: Coefficients for mass and radius fits.
Figure 1: Shows the scatter in fitted (calibrated) and measured a) mass and b) radius values for the 38 stars used in the calibration. 

Open with DEXTER 
Table 2: Comparison of mass and radius values obtained from isochrone fitting with those from the calibrated equations and from an MCMC analysis using those equations.
3 Application to WASP host stars
Seventeen WASP host stars have now been published. We use values for and metallicity obtained from spectral analyses with the coefficients given in Table 1 in Eqs. (4) and (5) to calculate the mass and radius of each, and compare these to the values obtained from isochrone interpolations. WASP1 data was obtained from Cameron et al. (2007), Stempels et al. (2007), Charbonneau et al. (2007) and Shporer et al. (2007), WASP2 data from Cameron et al. (2007) and Charbonneau et al. (2007), WASP3 data from Pollacco et al. (2008), WASP4 data from Wilson et al. (2008), WASP5 data from Anderson et al. (2008), WASP6 data from Gillon et al. (2009), WASP7 data from Hellier et al. (2009b), WASP10 data from Johnson et al. (2009) and Christian et al. (2009), WASP11 data from West et al. (2009b) and Bakos et al. (2009), WASP12 data from Hebb et al. (2009), WASP13 data from Skillen et al. (2009), WASP14 data from Joshi et al. (2009), WASP15 data from West et al. (2009a), WASP16 data from Lister et al. (2009), WASP17 data from Anderson et al. (2010), WASP18 data from Hellier et al. (2009a) and WASP19 data from Hebb et al. (2010). Table 2 shows that the agreement in results from the two methods is very good, demonstrating that computing stellar masses and radii from these coefficients is a valid, and simple, alternative to isochrone interpolation.
The only values in Table 2 that do not quite agree, within errors, are the results for the radius of WASP10. Johnson et al. (2009) find a radius of , whereas the calibration produces . WASP10 is an unusual host star, with a high density of (Johnson et al. 2009) and a high level of activity (Smith et al. 2009). Such calibration discrepancies in lowmass, highactivity stars are discussed in Sect. 6 of Torres et al. (2010).
4 Application to Markov Chain Monte Carlo analysis
Having established that our modification of the Torres calibration yields stellar masses that agree well with those obtained from isochrone fitting, we now describe its implementation in our Markovchain Monte Carlo (MCMC) parameter fitting code. This is followed by a discussion of a Main Sequence massradius constraint generally imposed on the parameter fitting, and objects for which this constraint is removed. We also discuss the effect on the final mass and radius values of uncertainty in eccentricity due to imperfect radial velocity and photometry.
The MCMC analysis, described in Collier Cameron et al. (2007) and Pollacco et al. (2008), derives starplanet system parameters from simultaneous modelling of stellar lightcurve and radial velocity measurements. The host star`s radial velocity motion is parametrised by the radial velocity amplitude, the centreofmass velocity, the orbital eccentricity and the longitude of periastron, while the transit is modelled using the formulation of Mandel & Agol (2002) incorporating the 4coefficient limbdarkening model of Claret (2000). The form of the transit profile is determined by five parameters: the epoch of transit, orbital period, duration and depth of transit and the impact parameter of orbit. The best model is found using a constrained optimization of for both photometric and radial velocity data, combined with Bayesian priors on epoch, period, transit duration and depth, impact parameter, stellar mass, radial velocity semiamplitude, eccentricity and the longitude of periastron.
Here, we adapted this analysis to take the spectral and metallicity as input values when modelling all available photometry and radial velocity observations of a host star. The MCMC code determines the stellar density value for the calculations from the observations at each step in the chain, now using Bayesian priors on the temperature and metallicity also, and uses the equations and coefficients above to calculate the stellar mass. These modifications make the MCMC analysis more robust since the stellar mass is now a derived quantity in the chain instead of a jump parameter constrained by a prior.
Where there is highquality followup photometry of a transit
event, the duration of ingress and egress, and hence the impact
parameter, are tightly constrained. However, where such photometry is
not available and thus the duration of ingress and egress cannot be
accurately measured, an additional constraint is needed in the MCMC
analysis. In such a case, the transit ingress and egress durations are
overestimated in modelling the photometry since the sharp transitions
to ingress and egress become blurred, allowing a shallower slope to be
fitted. This leads to an underestimation of the impact parameter, b,
from
(6) 
from Winn (2009) where is the transit depth, T is the total transit duration and is the partial, flat transit duration. This leads to an overestimation of the stellar radius, from
for a circular orbit, modified from Winn (2009), where a is semimajor axis and i is orbital inclination. To avoid this overestimation of stellar radius, the MCMCfitted stellar radii are generally constrained to reasonably closely follow a Main Sequence relationship to the stellar mass, i.e. (Cox 2000). To achieve this, a Bayesian prior is imposed on the stellar radius within the MCMC analysis such that a penalty is added to a chain step with a stellar radius different to that expected for the stellar mass value of that step, i.e.
(8) 
where is the stellar radius value for the current step in the Monte Carlo chain, is the stellar mass of this chain step and is the estimated uncertainty on the powerlaw estimate of the stellar radius. This penalty is added to the value for the chain step, giving the model a lower chance of being accepted.
However, WASP1, 12 and 15 have this Main Sequence constraint relaxed due to being more evolved stars, each with an estimated age greater than their expected Main Sequence lifetime. WASP1 and 12 are late Ftype stars with an estimated main sequence lifetime of 1 Gyr but estimated ages of around 2 Gyr. The highquality photometry of Charbonneau et al. (2007) and Shporer et al. (2007) (for WASP1) and Hebb et al. (2009) (for WASP12) constrains the impact parameter and stellar density satisfactorily, allowing a good estimate of stellar age, and at the same time removing the need for the additional MCMC constraint. WASP15 is an F5 star of around 3.9 Gyr compared to a normal F5 age of 3.6 Gyr, also with highquality photometry (West et al. 2009a) which again constrains the impact parameter and stellar density. Restraining the radii of these stars to lower values with the Main Sequence constraint on leads to an overestimation of their density. In addition, we used the very highquality photometry for WASP10 given in Johnson et al. (2009), and therefore had no need for the Main Sequence constraint in that case. For all other objects, without extremely high quality followup data and expected to be on the Main Sequence, the constraint was kept.
With high precision photometry the precise shape of the
transit would help constrain the eccentricity of the planetary orbit
through the measured duration of transit. A planet moving on an
eccentric orbit has its velocity modified by
compared to an identical planet on a circular orbit. Therefore for a
planet on an eccentric orbit, the duration of transit, T,
given by the length of the chord crossed in front of the star divided
by the planet's velocity, is modified by
compared to the duration in a circular orbit. Without very high quality
photometry, a source of uncertainty in the stellar density can arise
from the fitting of the eccentricity of the planet`s orbit from the
radial velocity measurements. With stellar density as an input, this
leads to uncertainty in the results for stellar mass and radius using
the calibrated equations and coefficients. This may especially be an
issue for low mass planets which have a lower ratio of radial velocity
amplitude to scatter than more massive planets, making an accurate
determination of orbital eccentricity more difficult. Using the
simplified version of the equation for density, Eq. (19) from Seager & MallénOrnelas (2003),
using
so that ,
and then including this factor gives
(9) 
where is the partial transit duration consisting of the ``flat'' part only.
Table 3: Result of fixing e = 0 for WASP13.
Figure 2: Shows the scatter in isochrone a) mass and b) radius values versus values from MCMC analysis for 17 SuperWASP host stars. 

Open with DEXTER 
As an example, WASP13b is a planet of mass orbiting a G1 type star with a radial velocity semiamplitude of 56 m s^{1} (Skillen et al. 2009). The only transit photometry available is from SuperWASP and the 0.87 m James Gregory Telescope in St Andrews, Scotland. Running the MCMC analysis as described above results in an eccentricity value of , with . However, holding the eccentricity fixed at 0 and repeating the analysis leads to an output with a very slightly higher value of 15 140, so clearly the larger eccentricity value is not a secure result. The difference in resulting parameters are given in Table 3, showing that there is only a small effect of about six percent on the final stellar mass value despite a change of over 50% in the stellar density. Therefore it may be concluded that the effect of the uncertainty in eccentricity on the final fitted mass value is small. The stellar radius is altered by around 18%, due to the change in density value.
The results of the MCMC analysis on each of the 17 SuperWASP host stars are also presented in Table 2, and are shown in Fig. 2. Eccentricities are held fixed at 0 in all cases where this was done in the original papers WASP3, 4, 5, 7, 11, 13, 15, 16 and 19). Almost all mass and radius values from the MCMC analysis agree with the isochrone values, within errors; the MCMC mass and radius ranges of WASP6 and the radius range of WASP19 do not quite overlap with the isochrone values, but all these values agree at the level.
5 Summary
We have presented a new calibration for stellar masses and radii based on stellar effective temperature, metallicity and stellar density. We have shown that the resulting equations provide a good fit to data for 38 stars from Torres et al. (2010), and also to values for masses and radii of exoplanet host stars obtained from isochrone analyses. We have demonstrated that accurate stellar masses may be obtained for such exoplanet host stars via a Markovchain Monte Carlo analysis of photometric and spectroscopic data, using spectroscopically determined temperatures and metallicities as input.
Even where poor photometry yields an uncertain estimate of stellar density, the mass estimate from the calibration is encouragingly robust. However, the stellar radius depends strongly on the stellar density estimate which in turn requires good knowlege of the impact parameter. Thus in establishing planet radii there is no substitute for good quality photometry, though the Main Sequence prior can provide a useful additional constraint if the star can be shown via independent means to be unevolved.
AcknowledgementsThe WASP Consortium consists of astronomers primarily from the Queen's University Belfast, Keele, Leicester, The Open University, and St Andrews, the Isaac Newton Group (La Palma), the Instituto de Astrofisica de Canarias (Tenerife) and the South African Astronomical Observatory. The SuperWASPN and WASPS Cameras were constructed and operated with funds made available from Consortium Universities and the UK`s Science and Technology Facilities Council.
References
 Anderson, D. R., Gillon, M., Hellier, C., et al. 2008, MNRAS, 387, L4 [NASA ADS] [Google Scholar]
 Anderson, D. R., Hellier, C., Gillon, M., et al. 2010, ApJ, 709, 159 [NASA ADS] [CrossRef] [Google Scholar]
 Bakos, G. Á., Pál, A., Torres, G., et al. 2009, ApJ, 696, 1950 [NASA ADS] [CrossRef] [Google Scholar]
 Cameron, A. C., Bouchy, F., Hébrard, G., et al. 2007, MNRAS, 375, 951 [NASA ADS] [CrossRef] [Google Scholar]
 Charbonneau, D., Winn, J. N., Everett, M. E., et al. 2007, ApJ, 658, 1322 [NASA ADS] [CrossRef] [Google Scholar]
 Christian, D. J., Gibson, N. P., Simpson, E. K., et al. 2009, MNRAS, 392, 1585 [NASA ADS] [CrossRef] [Google Scholar]
 Claret, A. 2000, VizieR Online Data Catalog, 336, 31081 [NASA ADS] [Google Scholar]
 Collier Cameron, A., Wilson, D. M., West, R. G., et al. 2007, MNRAS, 380, 1230 [NASA ADS] [CrossRef] [Google Scholar]
 Cox, A. N. 2000, Allen's Astrophysical Quantities, 4th edn. (Berlin: Springer) [Google Scholar]
 Fernandez, J. M., Holman, M. J., Winn, J. N., et al. 2009, AJ, 137, 4911 [NASA ADS] [CrossRef] [Google Scholar]
 Gillon, M., Anderson, D. R., Triaud, A. H. M. J., et al. 2009, A&A, 501, 785 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Hebb, L., CollierCameron, A., Loeillet, B., et al. 2009, ApJ, 693, 1920 [NASA ADS] [CrossRef] [Google Scholar]
 Hebb, L., CollierCameron, A., Triaud, A. H. M. J., et al. 2010, ApJ, 708, 224 [NASA ADS] [CrossRef] [Google Scholar]
 Hellier, C., Anderson, D. R., Cameron, A. C., et al. 2009a, Nature, 460, 1098 [NASA ADS] [CrossRef] [Google Scholar]
 Hellier, C., Anderson, D. R., Gillon, M., et al. 2009b, ApJ, 690, L89 [NASA ADS] [CrossRef] [Google Scholar]
 Johnson, J. A., Winn, J. N., Cabrera, N. E., & Carter, J. A. 2009, ApJ, 692, L100 [NASA ADS] [CrossRef] [Google Scholar]
 Joshi, Y. C., Pollacco, D., Cameron, A. C., et al. 2009, MNRAS, 392, 1532 [NASA ADS] [CrossRef] [Google Scholar]
 Lister, T. A., Anderson, D. R., Gillon, M., et al. 2009, ApJ, 703, 752 [NASA ADS] [CrossRef] [Google Scholar]
 Mandel, K., & Agol, E. 2002, ApJ, 580, L171 [NASA ADS] [CrossRef] [Google Scholar]
 Pollacco, D., Skillen, I., Collier Cameron, A., et al. 2008, MNRAS, 385, 1576 [NASA ADS] [CrossRef] [Google Scholar]
 Seager, S., & MallénOrnelas, G. 2003, ApJ, 585, 1038 [NASA ADS] [CrossRef] [Google Scholar]
 Shporer, A., Tamuz, O., Zucker, S., & Mazeh, T. 2007, MNRAS, 376, 1296 [NASA ADS] [CrossRef] [Google Scholar]
 Skillen, I., Pollacco, D., Collier Cameron, A., et al. 2009, A&A, 502, 391 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Smith, A. M. S., Hebb, L., Collier Cameron, A., et al. 2009, MNRAS, 398, 1827 [NASA ADS] [CrossRef] [Google Scholar]
 Southworth, J. 2009, MNRAS, 394, 272 [NASA ADS] [CrossRef] [Google Scholar]
 Southworth, J., Zucker, S., Maxted, P. F. L., & Smalley, B. 2004, MNRAS, 355, 986 [NASA ADS] [CrossRef] [Google Scholar]
 Sozzetti, A., Torres, G., Charbonneau, D., et al. 2007, ApJ, 664, 1190 [NASA ADS] [CrossRef] [Google Scholar]
 Sozzetti, A., Torres, G., Charbonneau, D., et al. 2009, ApJ, 691, 1145 [NASA ADS] [CrossRef] [Google Scholar]
 Stempels, H. C., Collier Cameron, A., Hebb, L., Smalley, B., & Frandsen, S. 2007, MNRAS, 379, 773 [NASA ADS] [CrossRef] [Google Scholar]
 Torres, G., Andersen, J., & Giménez, A. 2010, A&ARv, 18, 67 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 West, R. G., Anderson, D. R., Gillon, M., et al. 2009a, AJ, 137, 4834 [NASA ADS] [CrossRef] [Google Scholar]
 West, R. G., Collier Cameron, A., Hebb, L., et al. 2009b, A&A, 502, 395 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Wilson, D. M., Gillon, M., Hellier, C., et al. 2008, ApJ, 675, L113 [NASA ADS] [CrossRef] [Google Scholar]
 Winn, J. N. 2009, in IAU Symp., 253, 99 [Google Scholar]
 Winn, J. N., Holman, M. J., Torres, G., et al. 2008, ApJ, 683, 1076 [NASA ADS] [CrossRef] [Google Scholar]
Footnotes
 ... stars^{}
 www.exoplanet.eu
All Tables
Table 1: Coefficients for mass and radius fits.
Table 2: Comparison of mass and radius values obtained from isochrone fitting with those from the calibrated equations and from an MCMC analysis using those equations.
Table 3: Result of fixing e = 0 for WASP13.
All Figures
Figure 1: Shows the scatter in fitted (calibrated) and measured a) mass and b) radius values for the 38 stars used in the calibration. 

Open with DEXTER  
In the text 
Figure 2: Shows the scatter in isochrone a) mass and b) radius values versus values from MCMC analysis for 17 SuperWASP host stars. 

Open with DEXTER  
In the text 
Copyright ESO 2010
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.