An algorithm for photometric identification of transiting circumbinary planets

Ofir, A.

doi:10.1111/j.1365-2966.2008.13336.x

Cited by 43 publications

(19 citation statements)

References 26 publications

(47 reference statements)

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“…4 shows the correct identification rate as a function of the amplitude of the (white) noise. Similar results were obtain when we varied the planetary period or the planetary orbital inclination (Ofir 2008). …”

Section: Tests On Simulated Datasupporting

confidence: 85%

Identifying Transiting Circumbinary Planets

Ofir

2008

Proc. IAU

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Abstract. Transiting planets manifest themselves by a periodic dimming of their host star by a fixed amount. On the other hand, light curves of transiting circumbinary (CB) planets are expected to be neither periodic nor to have a single depth while in transit, making the BoxLeast-Squares (BLS) transit detection method almost ineffective. Therefore, a modified version for the identification of CB planets was developed -CB-BLS. We show that using CB-BLS it is possible to find CB planets in the residuals of light curves of eclipsing binaries (EBs) that have noise levels of 1% or more. Using CB-BLS will allow us to use the massive ground-and spacebased photometric surveys to look for these objects. Detecting transiting CB planets is expected to have a wide range of implications. For instance, the frequency of CB planets depends on the planetary formation mechanism -and planets in close pairs of stars provide a most restrictive constraint on planet formation models. Furthermore, understanding very high precision light curves is limited by stellar parameters -and since for EBs the stellar parameters are much better determined, the resultant planetary structure models will have significantly smaller error bars, maybe even small enough to challenge theory. The ChallengeLight curves (LCs) of transiting planets around single stars have precise depths, durations and epochs -and changes in any of these tell us something about the system. Light curves of transiting CB planets are expected to have very different photometric and temporal characteristics (Fig. 1), where none of these properties hold (Schneider & Chevreton 1990, Schneider 1994. In general, photometric signal = blocked flux / total flux, but for CB planets neither is constant: the total flux changes all the time because of ellipsoidal variation and binary eclipses. The blocked flux varies according to the surface brightness of the binary component being transited. The temporal characteristics arise from the fact that the transits are not periodic, and that their duration is highly variable -depending more on the transversal velocity of the binary components than on the planetary motion (the binary components can move either parallel or anti-parallel to the planet's motion, enabling long and short transits, respectively). Deeg et al. 1998). The leftmost panel shows the normal case, with two short and separated transits. The second panel shows a planetary transit near a binary mutual eclipse -producing a long transit. The two rightmost panels show transits of a planet with a long period: such planets have a transversal velocity that is slower than the binary components, and multiple transits with complicated shapes are more likely to occur.

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Section: Tests On Simulated Datasupporting

confidence: 85%

Identifying Transiting Circumbinary Planets

Ofir

2008

Proc. IAU

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“…Yet, eclipsing binaries represent an attractive class of targets for the photometric method. On the one hand planetary transits are more likely to occur is these edge-on systems, and high-precision photometry should allow the detection of transiting circumstellar, circumbinary (Deeg et al 1998;Doyle et al 2000;Ofir 2008), and Trojan planets (Caton et al 2000). On the other hand, the same photometric data can be used to search for nontransiting giant planets in circumbinary orbits through the precise timing of eclipse minima (Deeg et al , 2008Lee et al 2009).…”

Section: Observational Methods To Detect Extrasolar Planets In Binarymentioning

confidence: 99%

Detection and Characterization of Planets in Binary and Multiple Systems

Eggenberger

2010

EAS Publications Series

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Abstract. Moderately close binaries are a special class of targets for planet searches. From a theoretical standpoint, their hospitality to giant planets is uncertain and debated. From an observational standpoint, many of these systems present technical difficulties for precise radial-velocity measurements and classical Doppler surveys avoid them accordingly. In spite of these adverse factors, present data support the idea that giant planets residing in binary and hierarchical systems provide unique observational constraints on the processes of planet formation and evolution. The interest and the importance of including various types of binary stars in extrasolar planet studies have thus grown over time and significant efforts have recently been put into: (i) searching for stellar companions to the known planet-host stars using direct imaging, and (ii) extending Doppler planet searches to spectroscopic and moderately close visual binaries. In this contribution we review the observational progresses made over the past years to detect and study extrasolar planets in binary systems, putting special emphasis on the two developments mentioned above.

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“…The best-fitting LC is found using a 100 000-step MCMC chain, which also allows for the determination of all associated errors. Importantly, the above procedure was born in the context of searching for circumbinary planets (Ofir 2008) and therefore our model assumes two central bodies, around which other bodies may revolve. For a sufficiently low mass ratio q = m 2 m 1 +m 2 → 0 these central bodies can just as well be the host star and the first (easiest) detected planet.…”

Section: Modeling Multi-transiting Systemsmentioning

confidence: 99%

An independent planet search in theKeplerdataset

Ofir

Dreizler

2013

A&A

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Aims. We present first results of our efforts to re-analyze the Kepler photometric dataset, searching for planetary transits using an alternative processing pipeline to the one used by the Kepler mission Methods. The SARS pipeline was tried and tested extensively by processing all available CoRoT mission data. For this first paper of the series we used this pipeline to search for (additional) planetary transits only in a small subset of stars -the Kepler objects of interest (KOIs), which are already known to include at least one promising planet candidate. Results. Although less than 1% of the Kepler dataset are KOIs we are able to significantly update the overall statistics of planetary multiplicity: we find 84 new transit signals on 64 systems on these light curves (LCs) only, nearly doubling the number of transit signals in these systems. Forty-one of the systems were singly-transiting systems that are now multiply-transiting. This significantly reduces the chances of false positive in them. Notable among the new discoveries are KOI 435 as a new six-candidate system (of which kind only Kepler-11 was known before), KOI 277 (which includes two candidates in a 6:7 period commensurability that has anti-correlated transit timing variations) -all but validating the system, KOIs 719, 1574, and 1871 that have small planet candidates (1.15, 2.05 and 1.71 R ⊕ ) in the habitable zone of their host star, and KOI 1843 that exhibits the shortest period (4.25 h) and is among the smallest (0.63 R ⊕ ) of all planet candidates. We are also able to reject 11 KOIs as eclipsing binaries based on photometry alone, update the ephemeris for five KOIs and otherwise discuss a number of other objects, which brings the total of new signals and revised KOIs in this study to more than one hundred. Interestingly, a large fraction, about ∼1/3, of the newly detected candidates participate in period commensurabilities. Finally, we discuss the possible overestimation of parameter errors in the current list of KOIs and point out apparent problems in at least two of the parameters. Conclusions. Our results strengthen previous analyses of the multi-transiting ensemble, and again highlight the great importance of this dataset. Nevertheless, we conclude that despite the phenomenal success of the Kepler mission, parallel analysis of the data by multiple teams is required to make full use of the data.

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An algorithm for photometric identification of transiting circumbinary planets

Cited by 43 publications

References 26 publications

Identifying Transiting Circumbinary Planets

Identifying Transiting Circumbinary Planets

Detection and Characterization of Planets in Binary and Multiple Systems

An independent planet search in theKeplerdataset

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