Kepler/K2 Status Update & New Software Tools

A talk presented by Geert Barentsen (NASA Ames) 
at #TASC4/#KASC11 in Aarhus, Denmark, on July 9, 2018.

Transcript

1. 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
   

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2. *
   Photo by Marc Schiele on unsplash.com
   

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3. https://keplerscience.arc.nasa.gov
   

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

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7. 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
   

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8. 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.
   

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9. 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
   

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10. Beehive cluster (600 Myr) before K2
    Late M-dwarfs spin down

    in a radically different way
    

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11. 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.
    

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12. 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.
    

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13. 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
    

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

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

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

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

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18. 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).
    

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19. 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)
    

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20. 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
    

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21. 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)
    

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

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

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24. 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
    

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25. R⊙ = 1.04 R⊙?
    Gaulme+ 2016
    

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26. 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
    

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27. 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
    

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28. 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
    

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

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

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31. Video by Christina Hedges
    

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

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34. Work led by Christina Hedges (@TheChedgehog)
    

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

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

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37. 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)
    

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38. 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!
    

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39. 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
    

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

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