AC24
From planet catalogs to populations
Follow a small shadow through a noisy search. Keep the stars with no discoveries, then ask what the surviving catalog tells you about planets.
L1
Why do large planets fill a discovery catalog?
Planet catalogs favour signals a search can find. Follow transit geometry, observing gaps and noise to separate discoveries from the true population.
L1
Keep the stars with no detected planet
Transit geometry and every searched star set planet occurrence. Derive alignment and distinguish planet counts from host fractions.
L2
Which transits survive the survey?
Transit recovery depends on finite exposures, orbital alignment and observing windows. Derive a Gaussian test and combine the probabilities consistently.
L3
From a few detections to a population
Planet occurrence needs an integer catalog and effective search exposure. Derive its posterior and track classification, selection and radius errors.
L3
Replay a bounded DR25 parent sample
Kepler DR25 occurrence can be rerun from fixed source bytes. Rebuild the searched-star sample and propagate unmeasured selection into rate bounds.
L4
Read the evidence for the radius valley
Radius-valley figures combine selected samples, radius errors and physical models. Read fixed CKS, host-mass and planetary-architecture evidence.
Turn the detector dial and compare the population
Sources and calculation scope
- NASA Exoplanet Archive DR25 completeness/reliability and simulated products
Official DR25 product roles and the INJ1 source tables.
- Christiansen 2017, Pixel-Level Transit Injection Tests of Pipeline Detection Efficiency for DR25
KSCI-19110-001, sections 2–4 and pp. 9–12: ephemeris matching, aperture-corrected depth, expected MES and original table columns.
- Burke and Catanzarite 2017, Per-Target Detection Contours for DR25
KSCI-19111-002, Equations 1–2, sections 3.5–3.6 and 4–7: OSD, windows and target-dependent transfer.
- Coughlin, Robovetter Completeness and Effectiveness for DR25
KSCI-19114-002: injected, inverted and scrambled products; Robovetter dispositions and reliability.
- Measuring Transit Signal Recovery in the Kepler Pipeline IV
Version 2010.04796v1, sections II–IV: pixel-injection design and pooled recovery response.
- A Probabilistic Approach to Kepler Completeness and Reliability for Exoplanet Occurrence Rates
Version 1906.03575v4, sections II–VI, Equations 10–12 and Appendix B: externally weighted integer catalogs and occurrence likelihoods.
- Reliability Correction is Key for Robust Kepler Occurrence Rates
Version 2006.15719v1, sections II–III and Figures 4–5: classification reliability, scores and catalog sensitivity.
- The California-Kepler Survey III. A Gap in the Radius Distribution of Small Planets
Version 1703.10375v2, Figure 7, sections II–V and Appendix C: selected CKS population, weighted radius distribution and synthetic checks.
- Shallower radius valley around low-mass hosts
Version 2401.12378v2, Equations 1–6, Figures 4–8 and section 3.3: normalized valley contrast, host dependence and radius-cell migration.
- About 30 percent of Sun-like Stars Have Kepler-like Planetary Systems
Version 1802.09526v2, section III.1, Equations 1–4, sections III.4–III.5 and Figures 7–9: planets per star, host fraction and system architecture.
- IAU 2015 Resolution B3 nominal conversion constants
IAU 2015 Resolution B3 conversion constants, version 1510.07674v1.
- NASA Exoplanet Archive reuse and acknowledgment guidance
NASA Exoplanet Archive reuse and original-source acknowledgments.