Detection of visible light from the darkest world
Abstract
We present the detection of visible light from the planet TrES2b, the darkest exoplanet currently known. By analysis of the orbital photometry from publicly available Kepler data (0.40.9 m), we determine a daynight contrast amplitude of ppm, constituting the lowest amplitude orbital phase variation discovered. The signal is detected to 3.7 confidence and persists in six different methods of modelling the data and thus appears robust. In contrast, we are unable to detect ellipsoidal variations or beaming effects, but we do provide confidence intervals for these terms. If the daynight contrast is interpreted as being due to scattering, it corresponds to a geometric albedo of . However, our models indicate that there is a significant emission component to dayside brightness, and the true albedo is even lower (%). By combining our measurement with Spitzer and groundbased data, we show that a model with moderate redistribution () and moderate extra optical opacity () provide a compatible explanation to the data.
keywords:
techniques: photometric — stars: individual (TrES2)1 Introduction
Orbital photometric phase variations have long been used in the study and characterisation of eclipsing binaries (Wilson, 1994), where the large masses and small orbital radii result in phase variations at the magnitude to millimagnitude level. The three dominant components of these variations are i) ellipsoidal variations, due to the nonspherical nature of a star caused by gravitational distortion (e.g. Welsh et al. 2010) ii) relativistic beaming, due to the radial motion of the star shifting the stellar spectrum (e.g. Maxted et al. 2000) iii) reflected/emitted light, which varies depending on what phase of a body is visible (e.g. For et al. 2010).
The visible bandpass orbital phase variations of a star due to a hotJupiter companion are much smaller  around the partpermillion (ppm) level  and thus have eluded detection until relatively recently. The high precision spacebased photometry of CoRoT (0.560.71 m) (Baglin et al., 2009) and Kepler (Basri et al., 2005) have opened up this exciting new way of studying exoplanets for first time, with several detections recently reported in the literature:

CoRoT1b (Snellen et al., 2009); reflected/emitted light amplitude ppm

HATP7b (Welsh et al., 2010); ellipsoidal amplitude ppm, reflected/emitted light amplitude ppm

CoRoT3b (Mazeh & Faigler, 2010); ellipsoidal amplitude ppm, beaming amplitude ppm

Kepler7b (Demory et al., 2011); reflected/emitted light amplitude ppm
In this letter, we investigate the hotJupiter orbiting the G0V star TrES2 (O’Donovan et al., 2006), where we detect a reflected/emitted light amplitude of ppm to a confidence of , or 99.98%. We also measure the ellipsoidal variation and relativistic beaming amplitudes to be ppm and ppm respectively, which are broadly consistent with theoretical expectation.
If our detected signal is interpreted as being purely due to scattering, then the corresponding geometric albedo would be (using system parameters from Table 2, column 2 of Kipping & Bakos 2011 (KB11), as will be done throughout this work), meaning that just four months of Kepler’s exquisite photometry has detected light from the darkest exoplanet yet found. Extrapolating to a 6 year baseline, one can expect to detect albedos (to 3 confidence) at similar orbital radii down to . This clearly highlights the extraordinary potential which would be granted by an extended mission for Kepler.
2 Observations & Analysis
2.1 Data Acquisition
We make use of “Data Release 3” (DR3) from the Kepler Mission, which consists of quarters 0, 1 and 2 (Q0, Q1 & Q2). Full details on the data processing pipeline can be found in the DR3 handbook. The data includes the use of BJD (Barycentric Julian Date) time stamps for each flux measurement, which is crucial for time sensitive measurements. All data used are publicly available via MAST.
We use the “raw” (labelled as “AP_RAW_FLUX” in the header) shortcadence (SC) data processed by the DR3 pipeline and a detailed description can be found in the accompanying release notes. The “raw” data has been subject to PA (Photometric Analysis), which includes cleaning of cosmic ray hits, Argabrightenings, removal of background flux, aperture photometry and computation of centroid positions. It does not include PDC (Presearch Data Conditioning) algorithm developed by the DAWG (Data Analysis Working Group). As detailed in DR3, this data is not recommended for scientific use, owing to, in part, the potential for under/overfitting of the systematic effects.
2.2 Cleaning of the Data
The raw data exhibit numerous systematic artifacts, including pointing tweaks (jumps in the photometry), safe mode recoveries (exponential decays) and focus drifts (longterm trends). The first effect may be corrected by applying an offset surrounding the jump, computed using a 30point interpolative function either side. Due to the exponential nature of the second effect, we chose to exclude the affected data rather than attempt to correct it. The third effect may be corrected for using a detrending technique.
For this latter effect, we use the cosine filter utilised to detect ellipsoidal variations in CoRoT data by Mazeh & Faigler (2010). The technique acts as a highpass filter allowing any frequencies of the orbital period or higher through and all other longterm trends are removed. Thus, we protect any physical flux variations on the time scale of interest. We applied the filter independently to Q0+Q1 data and then Q2 data. This is because the Kepler spacecraft was rotated in the intervening time and so the longterm trend will not be continuous over this boundary. After removing 3 outliers with a running 20point median and transits using the ephemeris of KB11, we applied the filter, with the resulting fitted trends shown in Fig 1. Our final cleaned data consists of 154,832 SC measurements with a mean SNR.
2.3 Three Models
We first define our null hypothesis, , where we employ a flat line model across the entire time series, described by a constant . For a physical description of the orbital phase variations, we first tried the same model as that used by Sirko & Paczynski (2003) and Mazeh & Faigler (2010). This simple model is sufficient for cases where one is dealing with low signaltonoise and reproduces the broad physical features. The model, , is given by
(1) 
where is the orbital phase (defined as being 0 at the time of transit minimum) and are coefficients related to the physical model. is simply a constant to remove any DC (directcurrent) component in the data. corresponds to the reflection/emission effect and is expected to be have a negative amplitude. corresponds to the relativistic beaming effect and is expected to be positive. corresponds to the ellipsoidal variations and should be negative. is a dummy term which should be zero and ensures the ellipsoidal variation is detected with the correct phase.
We also tried a third model, , where the term is replaced by the reflection caused by a Lambertian sphere:
(2) 
2.4 Three Data Modes
In addition to three models, we have three data input modes. The first is simply corrected for detrending and nothing else, denoted . The second mode renormalises each orbital period epoch. This renormalisation is done by computing the median of each epoch and dividing each segmented time series by this value and we denote this mode as . Finally, we tried allowing each orbital period epoch to have its own variable renormalisation parameter, which is simultaneously fitted to the data along with the orbital phase curve model. This parameter is dubbed for the orbital period epoch. Denoting this data input mode as , the fits now include an additional 51 free parameters.
The models are fitted to the unbinned data using a Markov Chain Monte Carlo algorithm described in KB11 (method A) with accepted trials burning out the first 25,000. In total, there are nine ways of combining the three models with the three data modes. All nine models are fitted and results are given in Table 1, with our preferred model description being , (since thermal emission is likely dominant over scattering, see §4).
3 Results
3.1 Orbital Photometry
Table 1 presents the results of fitting the detrended Kepler photometry. Our models make no prior assumption on the sign or magnitude of the coefficients. The orbital period and transit epoch are treated as Gaussian priors from the circular orbit results of KB11.
Model ,  [ppm]  [ppm]  [ppm]  [ppm]  
Data  (reflec./emiss.)  (beaming)  (ellipsoidal)  (dummy)  
,  162603.5431  
,  162583.4014  
,  162583.3162  
,  161875.4005  
,  161859.6732  
,  161859.6095  
,  161837.6648  
,  
,  161821.7232  
Theory Expectation  0   
When considering statistical significance, what one is really interested in is the confidence of detecting each physical effect i.e. reflection/emission, ellipsoidal and beaming. For this reason, model comparison tools, such as the Bayesian Information Criterion (BIC) or an Ftest are inappropriate. This is because these methods evaluate the preference of one hypothesis over another, where the two models would be a nullhypothesis and a hypothesis including reflection/emission, ellipsoidal variations, beaming and the dummy term. Thus, any inference drawn from this would be for the entire model and not for each individual effect. In the analysis presented here, simple inspection of the posteriors from Fig 2 shows that only one effect is actually detected (reflection/emission), but a model comparison method would evaluate the significance of all four physical effects (including the dummy term) versus no effect.
A more useful statistical test would consider the significance of each physical effect individually from a joint fit. An excellent tool to this end is the odds ratio test discussed in Kipping et al. (2010). If a parameter was equal to zero, we would expect 50% of the MCMC runs to give a positive value and 50% to give a negative value. Consider that some asymmetry exists and a fraction of all MCMC trial were positive and were negative. The reverse could also be true and so we define such that i.e. it represents the majority of the MCMC trials. The odds ratio of the asymmetric model over the 50:50 model is:
(3) 
For only two possible models, the probability of the asymmetric model being the correct one is . We perform this test on each of the four parameters fitted for, , , and . The associated results are visible in the topleft corners of each posterior shown in Fig 2, for our preferred model and data mode i.e. , . To summarise, only one parameter presents a significant detection  the reflection/emission effect. Here, we find ’s posterior is sufficiently asymmetric to have a probability of occurring by random chance of just 0.02%, which equates to 3.67. We consider any signal detected above 3 confidence to merit the claim of a “detection” rather than a measurement and thus we find TrES2b to be the darkest exoplanet from which visible light has been detected.
As discussed in §2.3, we tried two different models for the reflection/emission effect; a simple sinusoid () and the reflected light from a perfectly Lambertian sphere (). Between the two models, there is negligible difference in the goodnessoffit, as seen in Table 1, for all three data modes. Including the Lambertian model takes some power away from the ellipsoidal variations though and thus the current data does not yield a preference between a Lambertian sphere model or stronger ellipsoidal variations.
3.2 Occultation Measurement
The duration of the transit, and thus occultation since TrES2b maintains negligible eccentricity, is equal to seconds (defined as the time between when the planet’s centre crosses the stellar limb to exiting under the same condition). In contrast, the orbital period of TrES2b is days. We therefore obtain 46 times more integration time of the orbit than the occultation event. This indicates that we should expect to be able to reach a sensitivity of times greater, purely from photon statistics. The uncertainty on our phase curve measurement is ppm. We therefore estimate that one should have an uncertainty on the occultation depth of ppm. If we assume the nightside has a negligible flux, then the depth of the occultation is expected to be ppm (i.e. equal to the daynight contrast), and this already suggests that the present publicly available Kepler photometry will be insufficient to detect the occultation. To test this hypothesis, we will here fit the occultation event including the Q0, Q1 and Q2 data.
To perform our fit, we use the same Gaussian priors on and as earlier. We also adopt priors for other important system parameters from KB11, such as , % and seconds. We stress that these are all priors and not simply fixed parameters. We also make use of the priors on the coefficients from the , fit. Data are trimmed to be within days of the expected time of occultation to prevent the phase curve polluting our signal, leaving us with 8457 SC measurements. Assuming a circular orbit, the data were fitted using an MCMC algorithm.
The marginalised posterior of the occultation depth yields ppm, which is clearly not a significant detection. The derived uncertainty of 1314 ppm is very close to our estimation of ppm and thus supports our hypothesis that the current Kepler data are insufficient to detect the occultation of TrES2b. We also note that the inclusion of the Q2 data does improve the constraints on the occultation event (KB11 found ppm using Q0 & Q1 only).
4 Discussion
HotJupiters are generally expected to be dark. Significant absorption due to the broad wings of the sodium and potassium D lines is thought to dominate their visible spectra (Sudarsky et al., 2000), leading to low albedos of a few percent. Indeed, aside from the recent report of Kepler7b’s % Keplerband geometric albedo (KB11), searches for visible light from hotJupiters have generally revealed mere upper limits (Collier Cameron et al. 2002; Leigh et al. 2003; Rowe et al. 2008; Burrows et al. 2008).
The 6.51.9 ppm contrast (determined from our preferred model , ) between the dayside and nightside photon flux that we measure for TrES2b represents the most sensitive measurement yet of emergent radiation in the visible from a hotJupiter, and is a factor of 20 and 6 dimmer than the corresponding differences for HATP7b (Welsh et al., 2010) and Kepler7b.
In order to interpret the visible flux, we use the planetary atmosphere modelling code COOLTLUSTY (Hubeny et al., 2003). For simplicity, we adopt equilibrium chemistry with nearly Solar abundance of elements, although we leave titanium oxide and vanadium oxide (TiO and VO) out of the atmosphere model. These compounds could, if present in the upper atmosphere of a hotJupiter, strongly affect the atmosphere structure and the visible and near infrared spectra, by making the atmosphere more opaque in the visible and by leading to a thermal inversion if the stellar irradiation exceeds 10 (Hubeny et al., 2003; Fortney et al., 2008). We leave TiO and VO out of our calculations, however, because of the difficulty of maintaining heavy, condensible species high in the atmospheres (Spiegel et al., 2009). Instead, we use an ad hoc extra opacity source , as described in Spiegel & Burrows (2010).
We calculate a grid of models with ranging (in ) from 0 to 0.6 in steps of 0.1 and with redistribution ranging from 0 to 0.5 in steps of 0.1 ( represents the fraction of incident irradiation that is transported to the nightside, which is assumed in our models to occur in a pressure range from 10 to 100 mbars). For each of these 42 parameter combinations, we calculate a dayside model, a nightside model, and a model that has the same temperature/pressure structure as the dayside but that has the star turned off, so as to calculate the emitted (and not scattered) flux (thus also giving the scattered component).
We draw several inferences from our models and the data. First, the nightside contributes negligible flux in the Keplerband (always 12% of the dayside, and for most models significantly less than that), meaning that the 6.5 ppm number represents essentially the entire dayside flux.
Second, by also including the available infrared secondary eclipse data on TrES2b (O’Donovan et al., 2010; Croll et al., 2010), we find that in our model set there must be some redistribution (but not too much) and there must be some extra absorber (but not too much). For each model, we compute a value, including 6 data points: Keplerband, Ksband, and the four Spitzer IRAC channels (3.6, 4.5, 5.8 & 8.0m). Fig 3 portrays the values of our grid of models, with the colour ranges corresponding to the values bounding 68.3% of the integrated probability (1), 95.5% (2), 99.7% (3) and 99.99% (4). The models that best explain the available data correspond to and (30% of incident flux redistributed to the night). In particular, models with no extra absorber are completely inconsistent with observations, even on the basis of the Kepler data alone. The upshot is that some extra opacity source appears to be required to explain the emergent radiation from this extremely dark world. Owing to this optical opacity, our models that are consistent with the data have thermal inversions in their upper atmosphere, as in Spiegel & Burrows (2010). We note that Madhusudhan & Seager (2010) find that the IR data of TrES2b may be explained by models both with and without thermal inversions; nevertheless, we believe that optical opacity sufficient to explain the Kepler data is likely to heat the upper atmosphere, as per Hubeny et al. (2003).
Finally, by computing the scattered contribution to the total flux, we find that for all parameter combinations the scattered light contributes 10% of the Keplerband flux, and for the bestfit models the scattered light is 1.5% of the total. TrES2b, therefore, appears to have an extremely low geometric albedo (for all models, the geometric albedo is %, and for the bestfit models it is 0.04%). Exact values for the amount of extra optical opacity, redistribution and the albedo cannot be presently provided because inferences about them depend on unknown quantities such as the wavelength dependence of the extra opacity source and the altitude dependence of winds.
Acknowledgments
We thank the Kepler Science Team, especially the DAWG, for making the data used here available. Thanks to A. Burrows, M. Nikku & the anonymous referee for helpful comments and I. Hubeny & A. Burrows for the development and continued maintenance of COOLTLUSTY and associated opacity database. DMK is supported by Smithsonian Instit. Restricted Endowment Funds.
Footnotes
 pagerange: Detection of visible light from the darkest world–Detection of visible light from the darkest world
 pubyear: 2011
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