Aims The standard method of searching parameter space for transits is ill-suited to data sets with long time baselines and poor temporal coverage, such as that anticipated from Gaia In this paper, we present an alternative method for identifying transit candidates is such data, one focusing on finding periodicity in high S/N outliersMethods We describe a technique for testing a small number of flux measurements for periodicity and consistency with an origin in a transit with a constant change in flux and test their performance with Monte Carlo simulations To complement this, we also include a description of a statistical method to analyze the distribution of these measurements to determine if they are normally distributed around a constant, reduce flux consistent with a planetary transitsResults Large numbers of light curves can be quickly scanned for transit signatures with minimal loss in effectiveness for data sets with long time baselines and poor temporal coverage, where one observation per transit is the norm by testing for periodicity and analyzing their distribution Conclusions If the noise characteristics of the data set and the intrinsic noise of the individual stars are understood, this method focusing on statistical outliers is nearly equivalent to the standard method of scanning parameter space and significantly faster, if the signal  ≫  noise, the individual transits are sampled no more than once and a periodicity test is employed Moreover, the test for a transit origin can eliminate additional false positives

https://www.aanda.org/articles/aa/pdf/2011/05/aa15885-10.pdf

Searching for transits in data with long time baselines and poor sampling

We derive analytic expressions for the detectability of exoplanets in radial velocity (RV), astrometric (AST), and transit (TR) data. We quantify detectability based on the total signal-to-noise ratio, S N , but we do not attempt to determine the appropriate S N value required for a robust detection. We first find analytic expressions for S N in the limit of small, uniform errors, continuous sampling, and monitoring campaigns much longer than the orbital period. In this limit, we find exact expressions for S N for RV and AST measurements considering arbitrary eccentricity and orbit viewing geometry. Eccentricity affects RV data in two ways. First, the semi-amplitude of the signal increases, which also increases S N . However, the RV curve becomes skewed such that the deviation from the average velocity is smaller over most of the orbit and greater only near periastron, which decreases S N . These two effects approximately cancel for e . 0.6, thus making S N only weakly dependent on e and differing by < 30% for e < 0.95. We also consider the effects of finite, uniform sampling, finding that detectability drops precipitously when e & [ 1 − ( Nd 8 ) −2 3 ] 1 2 , where Nd is the number of data points. For random sampling, the detectability is less sensitive to e. For RV, we further consider the effect on S N when the duration of observations is less than the orbital period. For AST, S N declines with increasing e in a manner that depends

Analytic Expressions for the Detectability of Exoplanets in Radial Velocity, Astrometric, and Transit Surveys

1. Introduction 2. Radial velocities 3. Astrometry 4. Timing 5. Microlensing 6. Transits 7. Imaging 8. Host stars 9. Brown dwarfs and free-floating planets 10. Formation and evolution 11. Interiors and atmospheres 12. The Solar System Appendixes References Index.

/pdf/the-exoplanet-handbook-3g3nzlvc20.pdf

The Exoplanet Handbook

We present detailed simulations of the Pan-STARRS-1 (PS1) multi-epoch, multiband 3pi Survey in order to assess its potential yield of transiting planets and eclipsing binaries This survey differs from dedicated transit surveys in that it will cover the entire northern sky but provide only sparsely sampled light curves Since most eclipses would be detected at only a single epoch, the 3pi Survey will be most sensitive to deep eclipses (approx>010 mag) caused by Jupiters transiting M dwarfs and eclipsing stellar/substellar binaries The survey will measure parallaxes for the approx4 x 10{sup 5} stars within 100 pc, which will enable a volume-limited eclipse search, reducing the number of astrophysical false positives compared with previous magnitude-limited searches Using the best available empirical data, we constructed a model of the extended solar neighborhood that includes stars, brown dwarfs, and a realistic binary population We computed the yield of deeply eclipsing systems using both a semianalytic and a full Monte Carlo approach We examined statistical tests for detecting single-epoch eclipses in sparsely sampled data and assessed their vulnerability to false positives due to stellar variability Assuming a short-period planet frequency of 05% for M dwarfs, our simulations predict that about a dozen transiting Jupitersmore » around low-mass stars (M {sub *} < 03 M {sub sun}) within 100 pc are potentially detectable in the PS1 3pi Survey, along with approx300 low-mass eclipsing binaries (both component masses <05 M {sub sun}), including approx10 eclipsing field brown dwarfs Extensive follow-up observations would be required to characterize these candidate eclipsing systems, thereby enabling comprehensive tests of structural models and novel insights into the planetary architecture of low-mass stars« less

Detectability of transiting jupiters and low-mass eclipsing binaries in sparsely sampled pan-starrs-1 survey data

The small sizes of low mass stars in principle provide an opportunity to find Earth-like planets and "super-Earths" in habitable zones via transits. Large area synoptic surveys like Pan-STARRS and LSST will observe large numbers of low mass stars, albeit with widely spaced (sparse) time sampling relative to the planets' periods and transit durations. We present simple analytical equations that can be used to estimate the feasibility of a survey by setting upper limits to the number of transiting planets that will be detected. We use Monte Carlo simulations to find upper limits for the number of transiting planets that may be discovered in the Pan-STARRS Medium Deep and 3-pi surveys. Our search for transiting planets and M-dwarf eclipsing binaries in the SDSS-II supernova data is used to illustrate the problems (and successes) in using sparsely sampled surveys.

Detecting Transits in Sparsely Sampled Surveys

The small sizes of low mass stars in principle provide an opportunity to find Earth‐like planets and “super Earths” in habitable zones via transits. Large area synoptic surveys like Pan‐STARRS and LSST will observe large numbers of low mass stars, albeit with widely spaced (sparse) time sampling relative to the planets’ periods and transit durations. We present simple analytical equations that can be used to estimate the feasibility of a survey by setting upper limits to the number of transiting planets that will be detected. We use Monte Carlo simulations to find upper limits for the number of transiting planets that may be discovered in the Pan‐STARRS Medium Deep and 3π surveys. Our search for transiting planets and M‐dwarf eclipsing binaries in the SDSS‐II supernova data is used to illustrate the problems (and successes) in using sparsely sampled surveys.

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Detecting Transits in Sparsely Sampled Surveys

Detecting Transits in Sparsely Sampled Surveys