Kepler/K2 update &
 new software tools A talk presented by Geert Barentsen (@GeertHub)
 at KASC11 in Aarhus, Denmark, on July 9, 2018 Cartoon by Christina Hedges 

* Photo by Marc Schiele on unsplash.com 

https://keplerscience.arc.nasa.gov 

At present, 2.1 publications per day use Kepler or K2 data Photo credit: motorverso.com (cc-by) 2016: 1.2 per day 2013: 0.8 per day 2010: 0.2 per day 

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Many of Kepler’s most intriguing discoveries are still emerging. 

The distribution of planet radii is bimodal Photoevaporation appears to herd small planets into either bare cores or mini-Neptunes.
 
 Fulton+ 2017 Owen & Wu 2017 and others 

Atmospheric erosion appears to be a function of incident flux High-precision planet radii obtained via asteroseismology reveal a slope in the planet radius bimodality.
 Van Eylen+ 2017 See talks by Thompson, Lundkvist, Montet, Kjeldsen, Chaplin, Huber, Chontos, and others. 

The number of planets discovered across open clusters is starting to constrain the timescales of inward planet migration. Rizzuto+ in prep Mann+ 2017 and others 1 10 100 1000 Age (Myr) 0.0 0.2 0.4 0.6 0.8 1.0 1.2 Relative Planet Occurence (P < 20 d) Migration? Kepler Upper Scorpius Pleiades Hyades & Praesepe Close-in planets appear to be less common around young stars 

Beehive cluster (600 Myr) before K2 Late M-dwarfs spin down
 in a radically different way 

Late M-dwarfs spin down
 in a radically different way Also: Rebull+ 2016a,b, 2017,
 Somers+ 2017,
 Barnes+ 2016,
 Stauffer+ 2016,
 Nardiello+ 2015,
 Scholz+ 2015,
 and others. 

Model prediction: Matt et al. (2015), 653 Myr Late M-dwarfs spin down
 in a radically different way Also: Rebull+ 2016a,b, 2017,
 Somers+ 2017,
 Barnes+ 2016,
 Stauffer+ 2016,
 Nardiello+ 2015,
 Scholz+ 2015,
 and others. 

Transients can have the shape of a Type Ia SN but show a rise time of just 2 days The median rise time of Type Ia SN is ~17 days?! 
 Rest+ 2018 

Oscillation frequencies in active galaxies appear to be predictive of the central black hole mass Smith+ 2018 

These results were all published within the past year … nine years after Kepler’s launch! 

Kepler’s discoveries will continue 1) new data 2) new methods 3) new tools 

1. new data Photo by Samuel Zeller on unsplash.com 

The number of targets with Kepler data increased by 30% over the past year +150,000 targets K2 observed 2,065 targets in 1-minute cadence so far;
 564 are bright (Kp < 10). 

Red squares indicate pipeline features not used during the original processing.
 cf. https://keplerscience.arc.nasa.gov/k2-uniform-global-reprocessing-underway.html K2’s re-processing will ensure that all Campaigns benefit from a high-quality, uniform calibration Work led by Jeff Coughlin (@JeffLCoughlin) 

Campaign 20 plans to target Taurus-Auriga
 and the Hyades cluster region Target proposal deadline:
 July 19, 2018 Aug 16, 2018 Details: https://keplerscience.arc.nasa.gov 

K2 has observed two dozen clusters across all ages • Young open clusters (1-10 Myr)
 Taurus, Upper Sco, rho Ophiuchus, Lagoon (NGC 6530). • Moderately young open clusters (0.1-1 Gyr)
 Pleiades, Hyades, M35, M44 (Beehive), NGC 1647, NGC 1746, NGC 1750, NGC 1758, NGC 1817. • Middle-aged clusters
 M67, Ruprecht 147, NGC 2158. • Globular clusters
 M4, M9, M19, M80, Terzan 5.
 NGC 5897, NGC 6293, NGC 6355. Campaigns 5, 16, & 18 overlap
 => M67 & M44 were observed for 3 x 80 days (3-yr baseline) 

See talks by Brown, Hall, Huber, Martig, Pedersen, and others. GAIA! Photo by Sebastian Davenport on unsplash.com 

2. new methods Photo by Jens Lelie on unsplash.com 

Probabilistic measurements of asteroseismic parameters in the time domain are becoming computationally tractable.
 
 Foreman-Mackey+ 2017
 Ambikasaran+ 2015 + talk by Pereira Opportunity: who wants to trial this method on K2’s 2,000 short cadence targets? Gaussian Processes 

R⊙ = 1.04 R⊙? Gaulme+ 2016 

Creative use of pixels in the PSF wings of bright stars enables the investigation of bright stars, including OB- type supergiants. 
 Pope+ 2016 White+ 2017 Aerts+ 2017 Aerts+ 2018 See talks by White & Aerts HD 188209 (O9.5Iab) rho Leo (B1Iab) Creative analyses enable the study of stars brighter than ~5th magnitude 

The intra-pixel response function of Kepler’s CCDs is being measured to an unprecedented precision A new measurement apparatus was designed which uses small spots of light across a range of wavelengths. 
 Vorobiev+ in prep => opens the door towards high-precision PSF-fitting photometry with Kepler 

The field is getting ever better at leveraging machine learning Careful feature engineering allows a classifier to provide a complete and unbiased census of different types of stars.
 Hedges+ 2018 and others 

3. new tools Photo by Todd Quackenbush on unsplash.com 

Also look out for new tools in talks by Colman, Townsend, Hon + posters 

Video by Christina Hedges 

KeplerTargetPixelFile(filename).interact() Work led by Michael-Gully Santiago (@gully_) 

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Work led by Christina Hedges (@TheChedgehog) 

KeplerTargetPixelFile(filename).to_lightcurve().periodogram().plot() 

TessTargetPixelFile(filename).to_lightcurve().periodogram().plot() 

http://lightkurve.keplerscience.org/tutorials/2.09-how-to-use-lightkurve-for-asteroseismology.html Our latest tutorial demonstrates how you can investigate the dependency of a periodogram on aperture mask and detrending parameters Work led by Christina Hedges (@TheChedgehog) 

Ann Marie Cody Michael Gully-Santiago Christina Hedges Zé Vinícius https://github.com/KeplerGO/lightkurve Everyone is welcome to join the development and become a co-author on the lightkurve paper! 

While Kepler’s fuel is running low, the space photometry revolution
 is only just getting started! 
 
 
 
 
 Try lightkurve today at
 https://keplerscience.arc.nasa.gov/lightkurve Cartoon by Christina Hedges 

KEPLER&K2 SciConV: 2019 10 years since launch March 4 – 8, 2019 Glendale, CA Abstracts due Nov 15, 2018