Two ultrashort eclipsing binaries from K2

Two white dwarfs in ultrashort binaries with detached, eclipsing, likely substellar companions detected by K2

S. G. Parsons, J. J. Hermes, T. R. Marsh, B. T. Gänsicke, P.-E. Tremblay, S. P. Littlefair, D. I. Sahman, R. P. Ashley, M. Green, S. Rattanasoon, V. S. Dhillon, M. R. Burleigh, S. L. Casewell, D. A. H. Buckley, I. P. Braker, P. Irawati, E. Dennihy, P. Rodríguez-Gil, D. E. Winget, K. I. Winget, Keaton J. Bell, and Mukremin Kilic
Department of Physics and Astronomy, University of Sheffield, Sheffield, S3 7RH, UK
Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA
Department of Physics, University of Warwick, Coventry CV4 7AL, UK
National Astronomical Research Institute of Thailand, 191 Siriphanich Bldg., Huay Kaew Road, Chiang Mai 50200, Thailand
Instituto de Astrofísica de Canarias, Vía Lactea s/n, La Laguna, E-38205 Tenerife, Spain
Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK
South African Astronomical Observatory, PO Box 9, Observatory, 7935, Cape Town, South Africa
Universidad de La Laguna, Departamento de Astrofísica, E-38206 La Laguna, Tenerife, Spain
Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA
McDonald Observatory, Fort Davis, TX 79734, USA
Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USA Fellow
Accepted 2017 June 22. Received 2017 June 16; in original form 2017 April 28

Using data from the extended Kepler mission in K2 Campaign 10 we identify two eclipsing binaries containing white dwarfs with cool companions that have extremely short orbital periods of only 71.2 min (SDSS J12050242, a.k.a. EPIC 201283111) and 72.5 min (SDSS J1231+0041, a.k.a. EPIC 248368963). Despite their short periods, both systems are detached with small, low-mass companions, in one case a brown dwarf, and the other case either a brown dwarf or a low-mass star. We present follow-up photometry and spectroscopy of both binaries, as well as phase-resolved spectroscopy of the brighter system, and use these data to place preliminary estimates on the physical and binary parameters. SDSS J12050242 is composed of a helium-core white dwarf which is totally eclipsed by a () brown dwarf companion, while SDSS J1231+0041 is composed of a white dwarf which is partially eclipsed by a companion of mass . In the case of SDSS J12050242 we look at the combined constraints from common-envelope evolution and brown dwarf models; the system is compatible with similar constraints from other post common-envelope binaries given the current parameter uncertainties, but has potential for future refinement.

binaries: eclipsing – stars: fundamental parameters – stars: low mass – white dwarfs – brown dwarfs
pubyear: 2017pagerange: Two white dwarfs in ultrashort binaries with detached, eclipsing, likely substellar companions detected by K2Two white dwarfs in ultrashort binaries with detached, eclipsing, likely substellar companions detected by K2

1 Introduction

Date at Telescope/ Filter Start Orbital Exposure Number of Conditions
start of run Instrument (UT) phase time (s) exposures (Transparency, seeing)
SDSS J12050242:
2016/07/13 K2 Campaign 10 Kepler 02:09 1765.3 2656 Space-based
2017/01/03 McDonald/ProEM 09:46 30.0 380 Clear, 1.7 arcsec
2017/01/19 TNT/ULTRASPEC 19:43 14.5 481 Clear, 1.5 arcsec
2017/01/19 TNT/ULTRASPEC kg5 20:59 8.5 277 Clear, 1.0 arcsec
2017/01/22 TNT/ULTRASPEC kg5 20:15 8.5 244 Clear, 1.2 arcsec
2017/01/25 TNT/ULTRASPEC kg5 19:31 10.0 575 Clear, 1.5 arcsec
2017/01/26 SOAR/Goodman - 07:36 300.0 17 Clear, 1.4 arcsec
2017/01/29 TNT/ULTRASPEC clear 17:45 10.0 614 Some clouds, 2.0 arcsec
2017/02/18 TNT/ULTRASPEC 20:25 12.8 142 Clear, 2.0 arcsec
2017/02/19 TNT/ULTRASPEC 17:41 12.8 121 Clear, 2.0 arcsec
2017/02/22 TNT/ULTRASPEC 16:45 15.0 163 Clear, 2.0 arcsec
2017/03/04 SALT/SALTICAM 22:00 10.0 216 Clear, 1.4 arcsec
2017/03/27 GTC/OSIRIS - 23:27 240.5 25 Clear, 1.2 arcsec
SDSS J12310041:
2016/07/13 K2 Campaign 10 Kepler 02:10 1765.3 2649 Space-based
2017/01/20 TNT/ULTRASPEC kg5 21:15 20.0 329 Clear, 1.0 arcsec
2017/01/22 TNT/ULTRASPEC kg5 20:53 20.0 410 Clear, 1.2 arcsec
2017/02/21 TNT/ULTRASPEC kg5 17:18 15.0 529 Clear, 2.0 arcsec
2017/02/22 TNT/ULTRASPEC kg5 17:45 15.0 548 Clear, 2.0 arcsec
2017/03/01 SOAR/Goodman - 05:33 600.0 13 Clear, 1.5 arcsec
Table 1: Journal of observations. The eclipse of the white dwarf occurs at Phase 1, 2, etc.

Roughly 75 per cent of main-sequence binaries are born wide enough that they evolve essentially as single stars (Willems & Kolb, 2004). However, for the remaining 25 per cent, the expansion of the more massive star at the end of its main-sequence lifetime causes the two stars to interact, often initiating a common-envelope event. The frictional forces experienced by the stars during the common-envelope phase result in a dramatic reduction in the separation of the two stars, down to as low as a few solar radii. Angular momentum loss via magnetic braking and gravitational radiation drives the resulting post-common-envelope binary (PCEB) to shorter periods, eventually creating a cataclysmic variable system.

Large-scale surveys have led to an explosion in the number of known PCEBs (Silvestri et al., 2006; Rebassa-Mansergas et al., 2010; Rebassa-Mansergas et al., 2016), with more than 100 systems having measured periods (e.g. Nebot Gómez-Morán et al., 2011; Parsons et al., 2015). The vast majority of these systems have M-dwarf companions, with the spectral type distribution of the secondaries peaking near M3–M4, in good agreement with the peak in the initial mass function of single stars (Chabrier, 2003). Just six PCEBs are known to be composed of white dwarfs with brown-dwarf companions (Dobbie et al., 2005; Burleigh et al., 2006; Casewell et al., 2012; Steele et al., 2013; Littlefair et al., 2014; Farihi et al., 2017).

PCEBs with brown-dwarf companions are difficult to identify from optical data alone. However, infrared surveys have demonstrated that these systems are intrinsically rare, with only 0.42 per cent of white dwarfs having a sub-stellar companion (Farihi et al., 2005; Girven et al., 2011; Steele et al., 2011; Debes et al., 2011), including both wide binaries that never interacted (e.g. Becklin & Zuckerman 1988; Steele et al. 2009; Luhman et al. 2011) and PCEBs. The small number of white dwarfs with brown dwarf companions reflects the rarity of sub-stellar objects both in the field (Kirkpatrick et al., 2012) and in binaries (Grether & Lineweaver, 2006).

The short orbital periods of PCEBs provide for many deeply eclipsing binaries, which offer a unique opportunity to directly probe the structures of both components by allowing for model-independent, high-precision mass and radius measurements (e.g., Parsons et al. 2012b). This is especially useful for uncommon objects. For example, there are very few known eclipsing binaries composed of at least one brown dwarf.

There is only one double-lined, eclipsing brown dwarf binary known to date, 2MASS J053521840546085 (Stassun et al., 2006), although another has tentatively been identified (David et al., 2016). Both of these systems are young (10 Myr), however, which will affect their radii, as brown dwarfs contract throughout their lifetime. The remainder of brown dwarfs with direct measurements of their radii are in systems where they are highly irradiated. For example, Kelt-1b is a 27  brown dwarf in a 29-hr orbit around an F star (Siverd et al., 2012); it is known to be highly inflated, at the 10 level compared to models. However, Wasp-30b (Anderson et al., 2011) is a 61 brown dwarf orbiting an F8 star every 4.16 d and has a radius that agrees with model predictions. SDSS J141126.20+200911.1, the only known brown dwarf to be eclipsing in a detached PCEB, also has a radius which is consistent with model predictions (Littlefair et al., 2014).

There is thus considerable value in finding more eclipsing PCEBs containing a brown dwarf. As part of a search for transits and variability in white dwarfs observed during K2 Campaign 10, we have discovered two new eclipsing PCEBs composed of a white dwarf and a likely brown dwarf companion. K2 (Howell et al., 2014) is an extension of the Kepler planet-hunting mission (Borucki et al., 2010) in which a number of fields along the ecliptic are continuously observed with high photometric precision over a period of approximately 75 days, hence it is ideal for detecting eclipsing PCEBs. We report here follow-up photometry and spectroscopy for these two new eclipsing systems, and furthermore detail and constrain their binary and stellar parameters.

2 Observations and their reduction

A full journal of observations is given in Table 1.

2.1 Target selection

We have proposed multiple Guest Observer programs to search for transits and variability from hundreds of known and candidate white dwarfs in every campaign of the K2 mission. As part of an analysis of targets observed with long-cadence (29.4-min) exposures during K2 Campaign 10, we flagged two spectroscopically confirmed white dwarfs with high-amplitude, short-period variability. The first, SDSS J120515.80024222.6 (a.k.a. EPIC 201283111111Proposed by K2 Guest Observer programs led by PIs Kilic (GO10006), Hermes (GO10018), and Burleigh (GO10019)., hereafter SDSS J12050242), showed variability near 71.2 min, very near the Nyquist frequency of our dataset. The other, SDSS J123127.14+004132.9 (a.k.a. EPIC 248368963222Targeted by the program led by PI Kilic (GO10006)., henceforth SDSS J1231+0041), showed variability at a similarly short period of 72.5 min.

2.2 K2 photometry

We examined preliminary extractions of our known and candidate white dwarfs using light curves produced by the Kepler Guest Observer (GO) office (Van Cleve et al., 2016), available through the Barbara A. Mikulski Archive for Space Telescopes (MAST). The Kepler bandpass covers roughly 40009000 Å. Each K2 long-cadence observation represents a co-add of 2706.02 s exposures.

We improved our extraction of SDSS J12050242 (=18.8 mag) by downloading the processed target pixel file from MAST and using the PyKE software tools (Still & Barclay, 2012). Using a large (17-px) fixed aperture, we extracted the light curve, fit out a quadratic function to 3-day windows, and corrected for K2 motion artifacts using the kepsff software package (Vanderburg & Johnson, 2014). Subsequently, we clipped by-hand any highly discrepant points. All data obtained in K2 Campaign 10 suffer from a large gap caused by the failure of a CCD module onboard the spacecraft roughly 7 d into the campaign, which powered off the photometer for roughly 14 d. Still, our final 69.12-d light curve of SDSS J12050242 has 2656 points and a duty cycle exceeding 78 per cent.

For SDSS J1231+0041 (=20.0 mag), we saw little improvement with our custom PyKE extraction, and used the light curve produced by the GO office for our final dataset, which was extracted with a 2-px aperture. After clipping, the final 69.12-day light curve of SDSS J1231+0041 has 2644 points.

2.3 McDonald+ProEM photometry

We obtained the first follow-up data of SDSS J12050242 on 2017 January 3 using the ProEM frame-transfer camera mounted at the Cassegrain focus of the 2.1-m Otto Struve telescope at McDonald Observatory in West Texas. The data were collected through an filter. We performed differential, circular aperture photometry by extracting the target and a nearby comparison star using the IRAF task CCD_HSP (Kanaan et al., 2002), and applied a barycentric correction using the WQED software package (Thompson & Mullally, 2013).

2.4 TNT+ULTRASPEC photometry

We observed both our targets with the high-speed frame-transfer EMCCD camera ULTRASPEC (Dhillon et al., 2014) mounted on the 2.4-m Thai National Telescope (TNT) on Doi Inthanon, Thailand in January and February 2017. Our observations were made using the band filter, a broad ++ filter known as kg5 (as described in Dhillon et al. 2014, see also the appendix of Hardy et al. 2017), as well as the band and “clear” (fused silica) filters. Exposure times were adjusted depending upon the conditions. The dead time between each exposure is 15 ms. All of these data were reduced using the ULTRACAM pipeline software. The source flux was determined with aperture photometry using a variable aperture scaled according to the full width at half maximum. Variations in observing conditions were accounted for by determining the flux relative to a comparison star in the field of view.

2.5 SOAR+Goodman spectroscopy

To better constrain the atmospheric parameters of the primary white dwarfs in both systems, we obtained low-resolution spectra of the upper Balmer series using the high-throughput Goodman spectrograph (Clemens et al., 2004) on the 4.1-m SOAR telescope at Cerro Pachón in Chile. We used a 930 line mm grating, and our setup covers roughly Å at a resolution of roughly 4Å, set by the seeing.

Using a 1.69″ slit, we obtained 18300 s exposures of SDSS J12050242 on 2017 January 26. The data were optimally extracted (Marsh, 1989) using the pamela package within starlink and flux calibrated using the standard Feige 67. The final summed spectrum has a signal-to-noise (S/N) of 65 per resolution element in the continuum around 4600Å. We obtained 13600 s exposures of SDSS J1231+0041 on 2017 March 1 using a 3.0″ slit. The optimally extracted spectra were flux calibrated against LTT 2415 and have a summed S/N of 24 per resolution element around 4600Å. SOAR spectroscopy of both targets were obtained at minimal airmass.

2.6 SALT+SALTICAM photometry

We obtained time-series photometry of SDSS J12050242 using the high-speed camera SALTICAM (O’Donoghue et al., 2006) mounted on the 10-m Southern African Large Telescope (SALT) on 2017 March 4. We used SALTICAM in the frame-transfer mode, whereby the moving mask occults half the CCD (the storage array), and we took 10 s exposures with 44 binning, yielding a plate scale of 0.56 arcsec/pixel. All SALTICAM observations had essentially zero deadtime (6 ms) between frames.

2.7 GTC+OSIRIS spectroscopy

We observed SDSS J12050242 with the Optical System for Imaging and low-Intermediate-Resolution Integrated Spectroscopy (OSIRIS) on the 10.4-m Gran Telescopio Canarias (GTC) on La Palma. We used the R2500R grism with a 0.6″ slit centred on the H line, giving a resolution of R2500. We used exposure times of 240 s and recorded a total of 25 spectra of SDSS J12050242, as well as one spectrum of the spectrophotometric standard star Hiltner 600.

The data were optimally extracted using pamela. An arc spectrum was used to wavelength calibrate the data. In total 34 lines (mostly neon) were fitted with a sixth-order polynomial giving an rms of 0.01Å. We then applied additional pixel shifts to each exposure (0.3 pixels maximum) based on the positions of three skylines (6300Å, 6863Å and 7276Å) to correct for instrument flexure. Finally, the instrumental response was removed using the spectrum of the standard star.

3 A 71.2-min Binary: SDSS J1205-0242

SDSS J12050242 ( mag) was classified as a white dwarf based on a serendipitous spectrum from the fourth data release of the Sloan Digital Sky Survey (SDSS) by Eisenstein et al. (2006). The SDSS spectrum shows no sign of a companion and no obvious red excess, but an automated fit to the spectrum yields a mass of (Kleinman et al., 2013), which is extremely low for a white dwarf, implying a binary origin (Marsh et al., 1995; Rebassa-Mansergas et al., 2011).

Figure 1: The averaged spectrum of SDSS J12050242 (left) and SDSS J1231+0041 (right) obtained with the Goodman spectrograph on the 4.1-m SOAR telescope. Our best fits to the Balmer lines (shown in red) yield updated atmospheric parameters for the primary white dwarfs in each system.

To confirm if this white dwarf genuinely has a low mass we analyzed our follow-up, higher-S/N spectrum from SOAR using the fitting procedures and pure-hydrogen, one-dimensional model atmospheres for white dwarfs described in Tremblay et al. (2011). The fit to our SOAR spectrum is consistent with the SDSS fit, giving a temperature of  K and surface gravity of , implying a mass of and cooling age of 50 Myr calculated using the helium-core white dwarf models of Panei et al. (2007). The Balmer lines and best fit to SDSS J12050242 are shown in the left panel of Fig. 1.

Figure 2: Top: Phase-folded, binned K2 light curve of SDSS J12050242. It is strongly smeared, since each long-cadence exposure lasts 29.4 min of the 71.2-min orbit. Still, a sinusoidal variation and eclipse stand out. Bottom: Phase-folded, ULTRASPEC kg5 light curve of SDSS J12050242 with higher time sampling. The deep eclipse of the white dwarf is clear, as is the out-of-eclipse reflection effect. There is no detection of the companion during the eclipse. Over-plotted in red is the best-fit model light curve (phase smearing is accounted for in the K2 plot at top).

The K2 light curve (Fig. 2) shows strong variations on a period of 0.04946539(9) days (71.2 min). The K2 data were obtained in long-cadence mode (29.4-min exposures), so any sharp features in the light curve are significantly smeared out. Nevertheless, a clear reflection effect is seen, along with steep eclipse features, implying that the system is likely to be fully eclipsing.

We display in the bottom panel of Fig. 2 our high-speed, follow-up ULTRASPEC light curve of SDSS J12050242, which shows a deep eclipse of the white dwarf, lasting just 5 min from the first to fourth contact points. The reflection effect is also evident out of eclipse. We recorded a total of seven eclipses, although due to the low S/N of the three band eclipses we excluded these from our ephemeris calculations. The four remaining eclipse times are listed in Table 2. We fitted each of these eclipses with a code specifically designed for binaries containing at least one white dwarf (Copperwheat et al., 2010) in order to determine the mid-eclipse times. From these we determined the ephemeris for the system to be


where is the orbital phase, with corresponding to the centre of the white dwarf eclipse.

Figure 3: Trailed spectra of the H line of SDSS J12050242 with time running upwards. The left-hand panel shows our GTC/OSIRIS data (the eclipse of the white dwarf occurs during spectrum 10). The centre panel shows our best fit model to the line, including both the absorption from the white dwarf and the emission from its companion. The right-hand panel shows the residuals of the fit.
Cycle MJD(BTDB) Source
SDSS J12050242:
3061 57616.626169(18) K2 Campaign 10
234 57756.4644612(78) McDonald band
97 57772.837463(30) ULTRASPEC band
118 57773.8762091(87) ULTRASPEC kg5 band
158 57775.8548125(63) ULTRASPEC kg5 band
218 57778.8227308(78) ULTRASPEC kg5 band
301 57782.9283510(78) ULTRASPEC clear
SDSS J1231+0041:
2575 57616.774090(86) K2 Campaign 10
546 57773.928207(40) ULTRASPEC kg5 band
585 57775.892041(30) ULTRASPEC kg5 band
1178 57805.751893(35) ULTRASPEC kg5 band
1198 57806.758914(31) ULTRASPEC kg5 band
Table 2: Mid-eclipse times.

To further improve the physical constraints of each component of the binary, we obtained GTC+OSIRIS time-series spectroscopy of the H line (left-hand panel of Fig. 3). The spectroscopy shows both a clear absorption component from the white dwarf as well as an emission component moving in anti-phase that is strongest around Phase 0.5 and disappears near the eclipse, the classic signature of irradiation-induced emission lines from the inner face of the companion to the white dwarf.

We fitted the H line with the following components: (1) A second-order polynomial representing the continuum of the white dwarf, which is scaled according to the light-curve model during phases affected by the eclipse. (2) A first-order polynomial representing the irradiation. Its level is modulated as , where is the orbital phase. (3) Three Gaussian absorption components for the white dwarf, that change position according to . (4) Two Gaussian emission components from the companion star, with strengths modulated in the same way as the irradiation component and that change position according to . We also take into account the smearing of the lines caused by the finite exposure times, and the best model was found using the Levenburg-Marquardt minimisation method.

Our best-fit model is shown in the centre panel of Fig. 3, with the residuals of the fit plotted in the right-hand panel. Our best fit parameters were , , , and . The offset between the radial-velocity amplitudes of the two stars is effectively the gravitational redshift of the white dwarf. For a 0.39 white dwarf the expected gravitational redshift is 11.2  (Panei et al., 2007). Correcting this value for the redshift of companion star, the difference in transverse Doppler shifts, and the potential at the companion owing to the white dwarf reduces this to 10.0 , within of the measured value. This provides an external consistency check on the spectroscopically determined mass.

The implied mass ratio of the binary is . Assuming a white dwarf mass of 0.39 gives a companion mass of 0.055 or 57. However, since this emission line originates only from the heated hemisphere of the companion, does not represent its true centre-of-mass velocity, but rather a lower limit on , the true radial velocity semi-amplitude of the companion. Therefore, 0.055 represents an upper limit on the mass of the companion; the companion in SDSS J12050242 is therefore definitely substellar.

The radial velocity amplitude of the companion’s centre-of-mass, , is related to via the formula


where is the radius of the brown dwarf scaled by the orbital separation () and is a constant between 0 and 1 which depends upon the location of the centre of light (Parsons et al., 2012a). We assume a value of , which roughly corresponds to optically thick emission from the inner hemisphere, which is what has been found for H emission in similar systems (Parsons et al., 2012b). This can be combined with the light curve fit to determine a more accurate value of .

The combination of the eclipse light curve and the radial velocity information enables us to place constraints on the stellar and binary parameters. When fitting data of the white dwarf eclipse alone there is a degeneracy between the inclination and both stellar radii (scaled by the orbital separation). However, we can establish the relationship between the masses and radii as a function of inclination. To do this we fitted the phase-folded light curve with a binary model (see Copperwheat et al., 2010, for details of the code). We fixed the mass ratio to 0.14 (maximum value from the spectroscopy) and the temperature of the white dwarf was fixed at 24 000 K. We used Claret 4-parameter limb-darkening coefficients for a 25000 K white dwarf (Gianninas et al., 2013) in the kg5 filter333Limb-darkening parameters in the filter kindly provided by Alex Gianninas.. The limb-darkening parameters of the brown dwarf have a negligible impact on the eclipse profile and so were fixed at the linear value for a 2400 K star in the SDSS band (Claret et al., 2012). The brown dwarf temperature was also fixed at 2400 K; again this makes no difference to the eclipse fit, since it is undetected during totality. We then varied the inclination from 90 to 84 degrees in steps of 1 degree and allowed the scaled radii, and , to vary. At each inclination we then used the value of to compute via Eq. 2 and combined this with and the inclination to determine the two masses, as well as and hence the two radii.

Figure 4: SALTICAM band light curve of the transit of the white dwarf in front of the heated face of the brown dwarf (i.e. the secondary eclipse). Also shown are models with inclinations of (blue), (red) and (green). Inclinations lower than predict a secondary eclipse that is too shallow.
Figure 5: Constraints on the mass and radius of the white dwarf in SDSS J12050242 based on our radial velocity and eclipse fitting. The black line shows how the mass and radius varies as a function of inclination. The red line shows the theoretical mass-radius relationship for a  K helium-core white dwarf with a canonically thick surface hydrogen layer (Panei et al., 2007). The blue line shows the same theoretical mass-radius relationship but for a carbon-oxygen core white dwarf (Fontaine et al., 2001), also with a canonically thick surface hydrogen layer. The vertical dashed line marks the white dwarf mass as determined from the Balmer-line fits to our SOAR spectrum, with the shaded area showing the the 1 uncertainties on this fit. The hatched region shows the inclinations excluded by the secondary eclipse data. The uncertainty on the white dwarf’s mass from the radial velocity data is shown on the model.
Figure 6: Constraints on the mass and radius of the brown dwarf in SDSS J12050242. The black line shows how the mass and radius varies as a function of inclination given our observational constraints. Note that the radius measurements correspond to the volume-averaged radius of the brown dwarf. Inclinations less than 85 are ruled out, as the brown dwarf would fill its Roche lobe. The hatched region shows the inclinations excluded by the secondary eclipse data. Also shown in red are theoretical mass-radius relationships for solar metallicity brown dwarfs of different ages (Baraffe et al., 2003). The uncertainty on the brown dwarf’s mass from the radial velocity data (which dominates over the inclination uncertainty) is shown on the model. The implication of these models is that SDSS J12050242 has a total system age between  Gyr.

In addition to the eclipse of the white dwarf, we also detect the transit of the white dwarf across the irradiated face of the brown dwarf, as shown in Fig. 4. The depth of this feature is strongly dependent upon the ratio of the radii and can be combined with the primary eclipse to place stringent constraints upon the inclination (e.g. Parsons et al., 2010, 2012a). In this case, the model had a of 369 (fitting 217 points). Models with inclinations lower than had values higher than 434 (), since they predict eclipses that are too shallow. Additionally, the shape of the brown dwarf is more distorted in the lower inclination models (since it is closer to Roche lobe filling) leading to much poorer fits (e.g. the model in Fig. 4). Therefore, our secondary eclipse data place a lower limit of on the inclination.

Our final constraints on the stellar parameters are shown in Fig. 5 and Fig. 6 for the white dwarf and brown dwarf, respectively, and are listed in full in Table 3. We found that the minimum inclination of the system is ; below this the radius of the brown dwarf needs to be so large to fit the eclipse width that it fills its Roche lobe. This places a hard upper limit on the mass of the white dwarf of 0.43. Our results from the secondary eclipse () further constrain this upper limit to 0.40. The uncertainty on the measurement dominates the error on the brown dwarf’s mass, leading to a mass range of ().

Fig. 5 shows that the measured radius of the white dwarf is fully consistent with theoretical predictions for helium-core white dwarfs (red line) by Panei et al. (2007) at an inclination of and is slightly oversized at lower inclinations, although this is still well within the uncertainties. The radii predicted by the carbon-oxygen core models (blue line) of Fontaine et al. (2001) are significantly smaller compared to our measurements. Both models have canonically thick hydrogen-layer masses, and we conclude that SDSS J12050242 has a helium core. At the highest inclinations the fit is also consistent with the white dwarf parameters found from the SOAR spectroscopy, implying that the true inclination is somewhere close to . Fig. 6 shows that the brown dwarf’s (volume-averaged) radius is consistent with theoretical predictions if it is older than 2.5 Gyr (3.5 Gyr for the solution). We did not detect the brown dwarf in our band light curves, placing an upper limit on its spectral type of L0, consistent with its classification as a brown dwarf.

We estimate the distance to the white dwarf by fitting the SDSS photometry with the Panei et al. (2007) models. We sample the posterior probability distributions for the parameter set using a Markov-Chain Monte-Carlo (MCMC) analysis. Posteriors on come from the SOAR spectral fits, whilst the posterior on is uniform between 0 and the maximum extinction along the line of sight. To minimise the effects of contamination by the irradiated companion, we only fit the photometry and find a distance of pc. Fitting the full dataset does not change the distance significantly.

By combining this distance with an estimate of the proper motion based upon SDSS and PanSTARRS (Tian et al., 2017) and adopting as an estimate of the radial velocity of the system we can calculate its Galactic space velocity, relative to the local standard of rest, as . We adopt the convention that the sign of is positive towards the Galactic anti-centre. Following Bensby et al. (2014), we find that SDSS J12050242 is ten times more likely to belong to the thin disk than the thick disk, and 50,000 times more likely to belong to the thin disk than the halo, justifying the adoption of solar metallicity models for the brown dwarf.

4 A 72.5-min Binary: SDSS J1231+0041

The second of our two systems, SDSS J1231+0041, is a faint () white dwarf identified from a serendipitous SDSS spectrum. Spectroscopic fits by Rebassa-Mansergas et al. (2016) to the SDSS spectrum found the white dwarf to be a  K white dwarf; their solution suggested a possible photometric excess at longer wavelengths, sufficient for them to classify it as a possible white dwarf plus main-sequence star system.

We have fit our higher-S/N SOAR spectrum to better constrain the white dwarf atmospheric parameters, as we did for SDSS J12050242. Our updated SOAR fits find the primary white dwarf has  K, , which yields a white dwarf mass of using the models of Fontaine et al. (2001). The SOAR spectrum and best fit are shown in the right panel of Fig. 1. Following the same method as for SDSS J12050242, we estimate a distance of  pc by fitting the carbon-oxygen core white dwarf models of Fontaine et al. (2001) to the SDSS photometry.

Figure 7: Top: Phase-folded, binned K2 light curve of SDSS J1231+0041. As with SDSS J12050242, the data are smeared since each long-cadence exposure comprises more than 40 per cent of the 72.5-min orbital period. Still, it shows a strong reflection effect, as well as slight evidence for an eclipse. Bottom: Phase-folded, ULTRASPEC kg5 light curve of SDSS J1231+0041 with higher time sampling. The partial eclipse of the white dwarf is clear, as is the out-of-eclipse reflection effect. A model light curve is over-plotted in red (and smeared in the top panel to match the K2 exposures).

The K2 light curve of SDSS J1231+0041 shows clear variations on a period of 0.050353815(28) days (72.5 min), displayed in Fig. 7. However, since these data were taken in long-cadence mode (with 29.4-min exposures) it was not immediately clear whether this is the true binary period, or if the period is twice this value. If this is the binary period, then the light curve variations must be the result of reprocessed light on the inner hemisphere of the companion to the white dwarf (i.e. reflection effect). The period could also be double this value, with the variations then caused by the Roche-distorted companion presenting different surface areas throughout the orbit (i.e. ellipsoidal modulation). The long exposure times of the K2 data relative to the variability make it difficult to distinguish between these two possibilities. There is also marginal evidence for an eclipse in the form of a steeper curve just before and after the minimum.

Our ground-based follow-up high-speed photometry (Fig. 7) shows that the true binary period is 72.5 min, and establishes that the system is eclipsing, albeit only partially (we do not detect any secondary eclipse). In total we covered four eclipses of the white dwarf (see Table 2). From these we determined the ephemeris for the system to be

Figure 8: Theoretical mass–radius relationships (solid lines) for solar metallicity brown dwarfs and low-mass stars (Baraffe et al., 2003) with ages of 0.5 Gyr (black), 1 Gyr (red), 5 Gyr (green) and 10 Gyr (blue). The grey dashed lines show the possible loci of Roche-lobe-filling companions to a white dwarf of mass  for fixed orbital period (in steps of 5 min). The figure shows that the most dense brown dwarfs are those with masses 0.065 that could still fit within their Roche lobes at periods as short as 45 min, provided they are old enough. It also shows that, to fit within its Roche lobe at a period of 72.5 min (indicated by the solid grey line), the companion to the white dwarf in SDSS J1231+0041 must have a mass of less than 0.095.

Since SDSS J1231+0041 is only partially eclipsing, determining accurate parameters from the light curve is complicated due to the extra level of degeneracy. However, with such a short orbital period we can place an upper limit on the mass of the companion to the white dwarf, based on the fact that it does not fill its Roche lobe. In Fig. 8 we show several mass-radius relationships for low-mass stars and brown dwarfs of different ages and solar metallicity. Also shown are lines of constant density at different orbital periods, which effectively shows the Roche lobe radius at different orbital periods. It is interesting to note how the radii of these low-mass objects are strongly related to their ages, to the extent that some binary configurations could only be possible with older brown dwarfs. For example, any detached system with a period 50 minutes must be older than 5 Gyr and must have a mass 0.07. With a period of 72.5 min we can only say that SDSS J1231+0041 must be older than 1 Gyr, since at this period most of the models converge. We can also place an upper limit on the mass of the companion to the white dwarf of 0.095; anything more massive than this would fill its Roche lobe. Therefore, it is quite likely that the companion in SDSS J1231+0041 is a brown dwarf, although radial-velocity data are required to confirm this.

Such a low-mass companion is completely outshone by the white dwarf at visible wavelengths, but Rebassa-Mansergas et al. (2016) suggested a possible photometric excess at red optical wavelengths. We have phased the SDSS photometry to the ephemeris established here and find it was all taken within 5 min of orbital phase 0.25. The apparent photometric red excess is therefore likely the result of irradiation, since the heated face of the companion has a much lower temperature but larger area than the white dwarf.

Our final parameters for both systems are listed in Table 3.

Parameter SDSS J1205-0242 SDSS J1231+0041
Orbital period (d) 0.049465250(6) 0.050353796(23)
Orbital separation () 0.420.45 -
Orbital inclination (deg) 8790 -
WD mass ()
WD radius () 0.02170.0223 -
WD (K)
WD cooling age (Myr) 50 5
Secondary mass ()
Secondary radius () 0.0810.087
App. magnitude () 18.5 20.1
Distance (pc)
Table 3: Stellar and binary parameters for the two systems presented in this paper. WD refers to the white dwarf.

5 Discussion

The white dwarfs in both the systems presented in this paper are the remnants of giant stars that were once much larger than their current orbits. This implies significant orbital shrinkage and points towards their emergence from common-envelopes that formed around both components of the binaries when mass transfer from the giant stars to their low mass companions took place (Paczynski, 1976). Common-envelope evolution is one of the most poorly understood and yet significant phases of close binary evolution (Ivanova et al., 2013), and well-constrained examples of its effects are worth examination for the constraints they may raise.

In this case, SDSS J12050242 offers the most interesting test, first because it is better constrained, second because it contains a moderately low-mass, helium-core white dwarf. The helium white dwarf in SDSS J12050242 is a remnant of the first ascent red giant branch (RGB). As Nelemans et al. (2000) pointed out, the close relation between the core-mass and radius of RGB stars (Refsdal & Weigert, 1970) can allow tight constraints to be derived on the prior evolution of binary stars containing helium white dwarfs. The radius of an RGB star rises rapidly with the helium core mass (approximately , Iben & Tutukov, 1985), thus helium white dwarfs of low mass that have emerged from common-envelopes are of particular interest since they come from relatively small, tightly-bound RGB stars. They can therefore lead to the most stringent constraints upon the efficiency with which the envelope is ejected. We express the effect of the common-envelope upon the orbital separation, , through the relation


which equates a fraction of the orbital energy change on the left with the binding energy of the RGB’s envelope on the right (Webbink, 1984; Dewi & Tauris, 2000). Here the subscripts and refer to the initial and final values of the respective parameter when they differ. The parameters and encapsulate the efficiency with which orbital energy is used to eject the envelope and the internal structure of the envelope respectively.

There are alternative formulations for the binding energy of the envelope (Iben & Livio, 1993). We claim no advantage for our choice other than its popularity, which eases comparison with other studies; we refer the reader to Ivanova et al. (2013) and Zorotovic et al. (2010) for further discussions of such variations and their effect upon the outcome of the common-envelope phase. Like Zorotovic et al. (2010), we condense what we can deduce from the system into a single constraint upon the combination parameter, .

The core mass-radius relation means that is largely defined by the mass of the white dwarf , with only a modest dependence upon its progenitor’s mass . Therefore, as the progenitor mass increases, both terms in the numerator of the right-hand side of Eq. 4 increase with little change in the denominator. On the left-hand side, however, there is relatively little change with the progenitor mass, as it is the first term in the brackets that dominates, since . The result is that the value of required to produce SDSS J12050242 increases rapidly with the progenitor mass, . These constraints are encapsulated in Fig. 9

Figure 9: The value of the combined common-envelope / RGB structure parameter (Dewi & Tauris, 2000) required to match the parameters of SDSS J12050242. The curved lines were calculated for three values of white dwarf mass, the value of from spectroscopy and either side of it and set . The shaded regions show the ranges of progenitor mass consistent with the age of the brown dwarf for the models of Baraffe et al. (2015) (upper-right, shaded blue) and Saumon & Marley (2008) (lower-left, shaded orange), allowing for the white dwarf’s cooling age of Myr (Panei et al., 2007) and using the formula for the time taken to reach the base of the RGB from Hurley et al. (2000). Solar metallicity has been assumed (Section 3).

which is based on the formulae presented by Hurley et al. (2000) and Eggleton (1983) in order to calculate and for a given choice of progenitor mass.

Ranges of progenitor mass consistent with the age of the brown dwarf for two sets of models (Baraffe et al., 2015; Saumon & Marley, 2008) are highlighted in Fig. 9. The range of runs from 0.1 – 2.2, consistent with many of the systems studied in a similar manner by Zorotovic et al. (2010). If brown dwarf models can be improved, there is potential for sharper constraints upon the common-envelope parameters, and, given the easily-detectable secondary eclipse in SDSS J12050242 (Fig. 4), there are good prospects for tightening the parameter constraints significantly beyond those shown in Fig. 9. There are caveats however: first are the significant existing uncertainties of cloud physics, molecular opacity and convection in brown dwarf models (Saumon & Marley, 2008; Baraffe et al., 2015), and second, it is possible that the unusual environment of rapid rotation and irradiation could affect the brown dwarf’s size, although the 50 Myr since the common-envelope is a blink of an eye compared to the brown dwarf’s Kelvin-Helmholtz timescale. Resolving such uncertainties is motivation for finding more examples of such systems.

The usual aim of studies such as this is to constrain the common-envelope efficiency parameter , but as we have seen it is the combination that is directly constrained. Unfortunately, the structure parameter , often taken to be (de Kool, 1990), is almost as ill-defined as , as it is not known to what extent the internal (thermal) energy of the envelope needs to be taken into account when calculating it (Han et al., 1995; Dewi & Tauris, 2000; Camacho et al., 2014); a contribution from internal energy can increase significantly. The relatively tightly-bound RGB star in this instance should make this uncertainty relatively small compared to later stages of stellar evolution, and once the parameters of the binary are firmed up, it will be worth investigating stellar models to define the range of for this specific instance. In any event, it is clear that SDSS J12050242 and similar white dwarf / brown dwarf systems have significant potential for both common-envelope evolution and brown dwarf physics.

Prior to the formation of the common-envelope, the binary would have had an orbital period in the range  days, placing it within or close to the “brown dwarf desert” where few brown dwarf companions to solar-type stars are seen (Marcy & Butler, 2000; Ma & Ge, 2014). It would be interesting to ascertain whether or not the numbers of white dwarf / brown dwarf PCEBs are consistent with the rarity of their progenitors in radial-velocity surveys.

These systems will transfer mass in the near future (300 Myr for SDSS J12050242), and presumably appear as cataclysmic variable stars. Their existence in this form, however, may be brief, if recent suggestions of the destabilising effects of novae on cataclysmic variables containing low mass white dwarfs are correct (Schreiber et al., 2016; Nelemans et al., 2016). They may then soon merge to become single white dwarfs, and, in the case of SDSS J12050242, a single white dwarf of low mass (Zorotovic & Schreiber, 2017), a number of which are known (Marsh et al., 1995; Brown et al., 2011). Their emergence from the common-envelope phase so close to Roche-lobe filling also suggests that had the companions been even less massive, these systems might not have survived the common-envelope at all but simply have merged. This exact scenario has been suggested as another way to form single low-mass white dwarfs (Nelemans & Tauris, 1998).

6 Conclusions

Using long-cadence photometry from the Kepler space telescope we have discovered two new ultrashort, detached eclipsing binaries composed of white dwarfs plus cool companions. The binaries have such short orbital periods — 71.2 min and 72.5 min — that the companions are likely substellar on the basis of their periods alone, in order that they do not fill their respective Roche lobes.

Follow-up photometry and spectroscopy significantly constrain both systems. SDSS J12050242 contains a hot ( K), low-mass () white dwarf with a radius consistent with a helium-core white dwarf (0.02170.0223). It is totally eclipsed every 71.2 min by a brown dwarf companion that has a radius consistent with an age greater than 2.5 Gyr (0.0810.087). Detection of secondary eclipses constrains the orbital inclination to  deg.

SDSS J1231+0041 contains a hot ( K), white dwarf that is partially eclipsed every 72.5 min by a companion of less than 0.095, likely also to be a brown dwarf. Details of all physical constraints to both systems are listed in Table 3.

The shorter-period system, SDSS J12050242, places useful constraints upon common-envelope evolution, because of its helium-core white dwarf and the need for the white dwarf’s total age to match the age of its brown dwarf companion. This demonstrates that ultrashort-period white dwarf plus brown dwarf binaries can be used to test theories of common-envelope evolution, because of the time-dependent radii of brown dwarfs, although uncertainties in brown dwarf models require clarification for this method to be applied with confidence.

Both systems were discovered as part of a search for transits and variability among white dwarfs in K2 Campaign 10; we expect to find more similar short-period eclipsing binaries as K2 continues surveying new fields along the ecliptic. The results here also help build expectations for the next space-based photometric mission, TESS (Ricker et al., 2014), which can be used to target many bright white dwarfs all-sky at 2-min cadence.


SGP acknowledges the support of the Leverhulme Trust. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013) / ERC Grant Agreement numbers 340040 (HiPERCAM) and 320964 (WDTracer), as well as the European Union’s Horizon 2020 Research and Innovation Programme / ERC Grant Agreement number 677706 (WD3D). ULTRACAM, TRM, VSD, SPL are supported by the Science and Technology Facilities Council (STFC) under grants ST/L000733 and ST/M001350. DAHB is supported by the National Research Foundation of South Africa. Support for this work was provided by NASA through Hubble Fellowship grant #HST-HF2-51357.001-A, by NASA K2 Cycle 4 Grant NNX17AE92G, as well as NSF grants AST-1413001 and AST-1312983. This work has made use of data obtained at the Thai National Observatory on Doi Inthanon, operated by NARIT; the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, e Inovação da República Federativa do Brasil, the U.S. National Optical Astronomy Observatory, the University of North Carolina at Chapel Hill, and Michigan State University; the McDonald Observatory of the University of Texas at Austin; as well as the Southern African Large Telescope (SALT), through DDT programme 2016-2-DDT-006, where the assistance of Marissa Kotze is acknowledged. Data for this paper have been obtained under the International Time Programme of the CCI (International Scientific Committee of the Observatorios de Canarias of the IAC) with the Gran Telescopio Canarias (GTC) operated on the island of La Palma in the Observatorio del Teide/Roque de los Muchachos.

Facilities: K2, Otto Struve (ProEM), TNT (ULTRASPEC), SOAR (Goodman), SALT (SALTICAM), GTC (OSIRIS)


  • Anderson et al. (2011) Anderson D. R., et al., 2011, ApJ, 726, L19
  • Baraffe et al. (2003) Baraffe I., Chabrier G., Barman T. S., Allard F., Hauschildt P. H., 2003, A&A, 402, 701
  • Baraffe et al. (2015) Baraffe I., Homeier D., Allard F., Chabrier G., 2015, A&A, 577, A42
  • Becklin & Zuckerman (1988) Becklin E. E., Zuckerman B., 1988, Nature, 336, 656
  • Bensby et al. (2014) Bensby T., Feltzing S., Oey M. S., 2014, A&A, 562, A71
  • Borucki et al. (2010) Borucki W. J., et al., 2010, Science, 327, 977
  • Brown et al. (2011) Brown J. M., Kilic M., Brown W. R., Kenyon S. J., 2011, ApJ, 730, 67
  • Burleigh et al. (2006) Burleigh M. R., Hogan E., Dobbie P. D., Napiwotzki R., Maxted P. F. L., 2006, MNRAS, 373, L55
  • Camacho et al. (2014) Camacho J., Torres S., García-Berro E., Zorotovic M., Schreiber M. R., Rebassa-Mansergas A., Nebot Gómez-Morán A., Gänsicke B. T., 2014, A&A, 566, A86
  • Casewell et al. (2012) Casewell S. L., et al., 2012, ApJ, 759, L34
  • Chabrier (2003) Chabrier G., 2003, PASP, 115, 763
  • Claret et al. (2012) Claret A., Hauschildt P. H., Witte S., 2012, A&A, 546, A14
  • Clemens et al. (2004) Clemens J. C., Crain J. A., Anderson R., 2004, in Moorwood A. F. M., Iye M., eds, Proc. SPIEVol. 5492, Ground-based Instrumentation for Astronomy. pp 331–340, doi:10.1117/12.550069
  • Copperwheat et al. (2010) Copperwheat C. M., Marsh T. R., Dhillon V. S., Littlefair S. P., Hickman R., Gänsicke B. T., Southworth J., 2010, MNRAS, 402, 1824
  • David et al. (2016) David T. J., Hillenbrand L. A., Cody A. M., Carpenter J. M., Howard A. W., 2016, ApJ, 816, 21
  • Debes et al. (2011) Debes J. H., Hoard D. W., Wachter S., Leisawitz D. T., Cohen M., 2011, ApJS, 197, 38
  • Dewi & Tauris (2000) Dewi J. D. M., Tauris T. M., 2000, A&A, 360, 1043
  • Dhillon et al. (2014) Dhillon V. S., et al., 2014, MNRAS, 444, 4009
  • Dobbie et al. (2005) Dobbie P. D., Burleigh M. R., Levan A. J., Barstow M. A., Napiwotzki R., Holberg J. B., Hubeny I., Howell S. B., 2005, MNRAS, 357, 1049
  • Eggleton (1983) Eggleton P. P., 1983, ApJ, 268, 368
  • Eisenstein et al. (2006) Eisenstein D. J., et al., 2006, ApJS, 167, 40
  • Farihi et al. (2005) Farihi J., Becklin E. E., Zuckerman B., 2005, ApJS, 161, 394
  • Farihi et al. (2017) Farihi J., Parsons S. G., Gänsicke B. T., 2017, Nature Astronomy, 1, 0032
  • Fontaine et al. (2001) Fontaine G., Brassard P., Bergeron P., 2001, PASP, 113, 409
  • Gianninas et al. (2013) Gianninas A., Strickland B. D., Kilic M., Bergeron P., 2013, ApJ, 766, 3
  • Girven et al. (2011) Girven J., Gänsicke B. T., Steeghs D., Koester D., 2011, MNRAS, 417, 1210
  • Grether & Lineweaver (2006) Grether D., Lineweaver C. H., 2006, ApJ, 640, 1051
  • Han et al. (1995) Han Z., Podsiadlowski P., Eggleton P. P., 1995, MNRAS, 272, 800
  • Hardy et al. (2017) Hardy L. K., et al., 2017, MNRAS, 465, 4968
  • Howell et al. (2014) Howell S. B., et al., 2014, PASP, 126, 398
  • Hurley et al. (2000) Hurley J. R., Pols O. R., Tout C. A., 2000, MNRAS, 315, 543
  • Iben & Livio (1993) Iben Jr. I., Livio M., 1993, PASP, 105, 1373
  • Iben & Tutukov (1985) Iben Jr. I., Tutukov A. V., 1985, ApJS, 58, 661
  • Ivanova et al. (2013) Ivanova N., et al., 2013, A&ARv, 21, 59
  • Kanaan et al. (2002) Kanaan A., Kepler S. O., Winget D. E., 2002, A&A, 389, 896
  • Kirkpatrick et al. (2012) Kirkpatrick J. D., et al., 2012, ApJ, 753, 156
  • Kleinman et al. (2013) Kleinman S. J., et al., 2013, ApJS, 204, 5
  • Littlefair et al. (2014) Littlefair S. P., et al., 2014, MNRAS, 445, 2106
  • Luhman et al. (2011) Luhman K. L., Burgasser A. J., Bochanski J. J., 2011, ApJ, 730, L9
  • Ma & Ge (2014) Ma B., Ge J., 2014, MNRAS, 439, 2781
  • Marcy & Butler (2000) Marcy G. W., Butler R. P., 2000, PASP, 112, 137
  • Marsh (1989) Marsh T. R., 1989, PASP, 101, 1032
  • Marsh et al. (1995) Marsh T. R., Dhillon V. S., Duck S. R., 1995, MNRAS, 275, 828
  • Nebot Gómez-Morán et al. (2011) Nebot Gómez-Morán A., et al., 2011, A&A, 536, A43
  • Nelemans & Tauris (1998) Nelemans G., Tauris T. M., 1998, A&A, 335, L85
  • Nelemans et al. (2000) Nelemans G., Verbunt F., Yungelson L. R., Portegies Zwart S. F., 2000, A&A, 360, 1011
  • Nelemans et al. (2016) Nelemans G., Siess L., Repetto S., Toonen S., Phinney E. S., 2016, ApJ, 817, 69
  • O’Donoghue et al. (2006) O’Donoghue D., et al., 2006, MNRAS, 372, 151
  • Paczynski (1976) Paczynski B., 1976, in Eggleton P., Mitton S., Whelan J., eds, IAU Symposium Vol. 73, Structure and Evolution of Close Binary Systems. p. 75
  • Panei et al. (2007) Panei J. A., Althaus L. G., Chen X., Han Z., 2007, MNRAS, 382, 779
  • Parsons et al. (2010) Parsons S. G., Marsh T. R., Copperwheat C. M., Dhillon V. S., Littlefair S. P., Gänsicke B. T., Hickman R., 2010, MNRAS, 402, 2591
  • Parsons et al. (2012a) Parsons S. G., et al., 2012a, MNRAS, 419, 304
  • Parsons et al. (2012b) Parsons S. G., et al., 2012b, MNRAS, 420, 3281
  • Parsons et al. (2015) Parsons S. G., et al., 2015, MNRAS, 449, 2194
  • Rebassa-Mansergas et al. (2010) Rebassa-Mansergas A., Gänsicke B. T., Schreiber M. R., Koester D., Rodríguez-Gil P., 2010, MNRAS, 402, 620
  • Rebassa-Mansergas et al. (2011) Rebassa-Mansergas A., Nebot Gómez-Morán A., Schreiber M. R., Girven J., Gänsicke B. T., 2011, MNRAS, 413, 1121
  • Rebassa-Mansergas et al. (2016) Rebassa-Mansergas A., Ren J. J., Parsons S. G., Gänsicke B. T., Schreiber M. R., García-Berro E., Liu X.-W., Koester D., 2016, MNRAS, 458, 3808
  • Refsdal & Weigert (1970) Refsdal S., Weigert A., 1970, A&A, 6, 426
  • Ricker et al. (2014) Ricker G. R., et al., 2014, in Space Telescopes and Instrumentation 2014: Optical, Infrared, and Millimeter Wave. p. 914320 (arXiv:1406.0151), doi:10.1117/12.2063489
  • Saumon & Marley (2008) Saumon D., Marley M. S., 2008, ApJ, 689, 1327
  • Schreiber et al. (2016) Schreiber M. R., Zorotovic M., Wijnen T. P. G., 2016, MNRAS, 455, L16
  • Silvestri et al. (2006) Silvestri N. M., et al., 2006, AJ, 131, 1674
  • Siverd et al. (2012) Siverd R. J., et al., 2012, ApJ, 761, 123
  • Stassun et al. (2006) Stassun K. G., Mathieu R. D., Valenti J. A., 2006, Nature, 440, 311
  • Steele et al. (2009) Steele P. R., Burleigh M. R., Farihi J., Gänsicke B. T., Jameson R. F., Dobbie P. D., Barstow M. A., 2009, A&A, 500, 1207
  • Steele et al. (2011) Steele P. R., Burleigh M. R., Dobbie P. D., Jameson R. F., Barstow M. A., Satterthwaite R. P., 2011, MNRAS, 416, 2768
  • Steele et al. (2013) Steele P. R., et al., 2013, MNRAS, 429, 3492
  • Still & Barclay (2012) Still M., Barclay T., 2012, PyKE: Reduction and analysis of Kepler Simple Aperture Photometry data, Astrophysics Source Code Library (ascl:1208.004)
  • Thompson & Mullally (2013) Thompson S., Mullally F., 2013, Wqed: Lightcurve Analysis Suite, Astrophysics Source Code Library (ascl:1304.004)
  • Tian et al. (2017) Tian H.-J., et al., 2017, preprint (arXiv:1703.06278)
  • Tremblay et al. (2011) Tremblay P.-E., Bergeron P., Gianninas A., 2011, ApJ, 730, 128
  • Van Cleve et al. (2016) Van Cleve J. E., et al., 2016, PASP, 128, 075002
  • Vanderburg & Johnson (2014) Vanderburg A., Johnson J. A., 2014, PASP, 126, 948
  • Webbink (1984) Webbink R. F., 1984, ApJ, 277, 355
  • Willems & Kolb (2004) Willems B., Kolb U., 2004, A&A, 419, 1057
  • Zorotovic & Schreiber (2017) Zorotovic M., Schreiber M. R., 2017, MNRAS, 466, L63
  • Zorotovic et al. (2010) Zorotovic M., Schreiber M. R., Gänsicke B. T., Nebot Gómez-Morán A., 2010, A&A, 520, A86
  • de Kool (1990) de Kool M., 1990, ApJ, 358, 189
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description