Washington github.com/dfm // dfm.io // @exoplaneteer Creative Commons Attribution 4.0 International License with Tim Morton (Princeton), Bernhard Schölkopf (MPIS), David W. Hogg (NYU), Eric Agol (UW)
Previ break in et al. 20 (d) Final for altern dwarf sa (Dressin power la Sympt model o constrain When Rb become meaning Rp in the which w otherwis lower l Figure 7. Same as Figure 6, but marginalized over 0.75 < Rp < 2.5 Å R and bins of dP orb = 31.25 days. Figure 8. Shows the underlying planet occurrence rate model. Marginalized over 50 < P orb < 300 days and bins of dRp =0.25 Å R planet occurrence rates for the model parameters that maximize the likelihood (white dash line). Posterior distribution for the underlying planet occurrence rate for the median Figure 9. S of dP orb =
hortcoming ipeline and a et al. coming by ness of the 14) through this study, ler pipeline the planet epler planet er highlight systematic rates with nd Dong & where we alculate the ut assump- eccentricity, Figure 1. Fractional completeness model for the host to Kepler-22b (KIC: 10593626) in the Q1-Q16 pipeline run using the analytic model described in Section 2. Burke et al.
modified QATS planet discovery pipeline, we searched all K2 stars (C0-7) for transiting planets. We have discovered over 800 K2 planet candidates (500+ new), including high multiplicity systems (eight systems with 4+ planets). NOTE: These are preliminary results. See our paper (Kruse et al., nearing submission) for final planet counts, planet and stellar properties, etc. Planets ion of the Quasiperiodic tion to finding periodic ore effectively discover d quality of the data n near that of the ore details). compared to any other a, and the bottom panel is ter fire outliers are Figure 4: Results showing only our new (unreported in the literature) K2 planet candidates. Planets with 0 radius do not have stellar parameters yet. Rodrigo Luger et al. (ApJ accepted), Ethan Kruse et al. (in prep)
modified QATS planet discovery pipeline, we searched all K2 stars (C0-7) for transiting planets. We have discovered over 800 K2 planet candidates (500+ new), including high multiplicity systems (eight systems with 4+ planets). NOTE: These are preliminary results. See our paper (Kruse et al., nearing submission) for final planet counts, planet and stellar properties, etc. Planets ion of the Quasiperiodic tion to finding periodic ore effectively discover d quality of the data n near that of the ore details). compared to any other a, and the bottom panel is ter fire outliers are Figure 4: Results showing only our new (unreported in the literature) K2 planet candidates. Planets with 0 radius do not have stellar parameters yet. Rodrigo Luger et al. (ApJ accepted), Ethan Kruse et al. (in prep) See posters by Rodrigo Luger (30) & Ethan Kruse (29)
to "remove" systematics 2 Template-based grid of likelihoods (restricted to systems with >=3 transits) 3 Remove false alarms using magic* * I will use similar magic shortly. See F. Mullally et al. (2016); Coughlin et al. (2016)
2 Template-based grid of likelihoods (restricted to systems with >=3 transits) 3 Remove false alarms using magic* * I will use similar magic shortly. See F. Mullally et al. (2016); Coughlin et al. (2016)
data to "remove" systematics 2 Template-based grid of likelihoods (restricted to high signal-to-noise candidates) 3 Remove false alarms using model comparison* * The aforementioned "magic"
data to "remove" systematics 2 Template-based grid of likelihoods (restricted to high signal-to-noise candidates) 3 Remove false alarms using model comparison
(2016); Shvartzvald et al. (2016) RE – RN ~0.40 RN – RJ ~0.17 per G/K- dwarf, per ln-radius, per ln-period occurrence rate in period range 2 – 25 years
(63) 1 Hard to follow up – because Kepler 2 False positive quantification 3 Quantitative comparison & joint analysis with other catalogs 4 Probabilistic follow-up prioritization