Here are some figures from my recent first-author papers that may be useful in presentations.
Some are the same versions as can be found in the papers themselves; some are tweaked slightly
to be optimized for large displays.
Feel free to use any of these, but please cite the relevant papers if you do.
Other figures available upon request.
The figures on this page are image files (some are transparent). You can access these directly
by right-clicking and saving the image, or opening it in a new tab. Clicking directly on the
image will open a pdf version.
(top left) "Postcard'' FFI image of the region around a sample star, KIC 8462852, from the Kepler data.
The image is 300 pixels square (20 arcmin on a side). (top right) The same, with automated apertures
drawn over reference stars. (middle) A representative sample of 12 stars with Sun-like stellar parameters
and non-Sun-like magnetic activity. These stars have quasi-periodic brightness variations ranging from 0.5%
to 2% over 4 years. For comparison, the Sun's brightness varies by 0.1% over an 11 year cycle. (bottom left)
Distribution of targets with observed variable behavior across the Kepler field of view. (bottor right)
Stars with observed long-term variability either correlated (facula-dominated, red) or anticorrelated
(spot-dominated, blue) with
short-term starspot variability observed in Kepler long cadence data. For example, 13% of all Sun-like stars
with rotation periods of 13 days have detectable spot-dominated variability.
The fraction of stars with facula-dominated variability increases in time, with the two equal at a rotation
period of 24 days. Beyond 26 days, we do not detect any stars with spot-dominated variability.
(top) Full-frame image data for the region near KIC 8462852. The target star aperture is shown in red, while seven bright
comparison stars are highlighted in blue. (bottom) Light curve for KIC 8462852. The points with error bars are relative flux
measurements recorded approximately monthly through the full-frame images of the entire Kepler field. The four different colors
and shapes correspond to the four spacecraft orientations (also shown in subplots). Due to the uncertainties of the underlying flat
field, a linear offset between flux recorded at different spacecraft orientations may be required. The gray curve in the background
corresponds to one possible realization of the true long cadence light curve of KIC 8462852, conditioned on the FFI data. The now-famous
dips originally published in Boyajian et al. 2016 correspond to the narrow dips seen here.
(top) Astrometry for the GJ 3305 AB system. Red dashed lines show the maximum likelihood model, blue dashed lines
draws from the posterior distribution of allowed orbits, and black points are the data. These figures show the
predicted orbit throughout the next few years as well, through the next periastron passage. (middle) Same as
the above's top two panels, but with a different scaling of the orbit. (bottom) Comparison with BHAC15 stellar
models, showing that while star A is well-represented by stellar models, star B is fainter than predicted in the
(top left) Photometry for (black) all K2 Campaign 1 stars, (fuschia) all
Campaign 1 planet host candidates, (blue) all known K2 planet host stars, and (yellow)
the Sun. (top right) Phase-folded Kepler
photometry for all K2 Campaign 1 planet
candidates. Names in blue are validated planets, names in black are planet candidates, and
names in red are false positives. (bottom) Proper motion for EPIC 201912552, a star hosting
a mini-Neptune that receives Earthlike insolation. Sixty years of motion show there is no
background object behind this star.
(top left) Joint constraints on the temperature of LHS 6343 A and B from the combined near-IR spectrum.
Shaded region and dashed line show the temperature of A expected from the observed light curve and
empirical main-sequence relation, converting mass to temperature through the Dartmouth models.
(top right) Phase-folded Kepler
photometry for LHS 6343 ABC.
(bottom left) Phase-folded Keck/HIRES radial velocities for LHS 6343 A relative to LHS 6343 B.
(bottom right) Brown dwarf mass-radius diagram, including isodensity contours and isochrones from
the Baraffe models.
(top left) Mass and metallicity distributions of M dwarfs in our sample, with systems exhibiting long-term
RV acceleration marked. (top right) Occurence rate of giant planets orbiting M dwarfs. 6.5 +/- 3.0 percent of
M dwarfs host a 1-13 Jupiter mass planet with a < 20 AU. (bottom left) Measured occurence rate as a function
of assumed power law in planet mass and orbital semimajor axis. (bottom right) Measured power law in mass and
orbital semimajor axis, assuming the planets orbiting M dwarfs detected from microlensing surveys are drawn from the same
population as the planets orbiting M dwarfs detected in RV surveys.