Recent Results:

Artist's view of a transiting exoplanet
Artist's impression of a planet around an M dwarf.
ESO/L. Calçada
2016 Jul: Our team has just announced the discovery of hundreds of planet candidates from K2, including over 100 fully validated planets. These true, bona fide planets (no longer mere candidates!) provide an excellent laboratory for measuring planet masses (via RVs and TTVs), atmospheric composition (with HST and JWST), and for studying planetary habitability. Read all about the new results online here, here, here, or here, or read the full paper here. 2015 Jan: Surveys for new planets using the transit and radial velocity techniques reveal the high frequency with which small, short-period planets occur around main sequence stars. However, only a few of these smaller planets can be easily observed to characterize their atmosphere; even fewer are known around low-mass M stars, though these planetary systems may be the most common in the Galaxy. Our team has just discovered three small planets orbiting a bright, nearby M star using data collected by K2, a new mission using the re-purposed Kepler spacecraft. We find that the system hosts three transiting planets, all with sizes just 1.5 to 2 times larger than the Earth. Thus these new planets likey straddle the transition region between rocky and increasingly gas-dominated compositions. With an orbital period ('years') of 45 days, the third planet receives roughly as much heat from its star as do Earth or Venus, placing the planet near its star's habitable zone and making it one of the coolest small planets known orbiting a nearby star. The bright, low-mass star makes this system an excellent laboratory to determine the planets' masses via Doppler spectroscopy and to constrain their atmospheric compositions via transit observations with the Hubble and James Webb Space Telescope. Download the paper or read all about it here.

First Global 2D Map of an Extrasolar Substellar Body

Luhman 16B: the
		        first global map of a brown dwarf.
Map of Luhman 16B: the first global map of a brown dwarf. Bright regions are gaps in the clouds, where infrared light from the hotter, deeper atmosphere can escape to space.
(I. Crossfield, MPIA)
2014 May: Following our recent paper presenting the first global, 2D map of patchy clouds in a brown dwarf, I present a new investigation of how many other brown dwarfs or extrasolar planets might eventually be mapped in this way. The results are favorable: although no targets are as easy to map as our neighbor Luhman 16B, many brown dwarfs -- and a few planets -- will eventually be mapped using future instruments on future giant telescopes. This conclusion is further supported by an analysis recently published by Snellen et al. As part of this analysis I also compiled all previous measurements of rotation and varying brightness for brown dwarfs and exoplanets. Read all about it here. 2014 Jan: In our recent paper we present the first global, 2D map of the patchy clouds in the atmosphere of a brown dwarf, our neighbor Luhman 16B. We see large-scale brightness variations that we interpret as being regions of thicker (dark) and thinner (bright) clouds. Click here to read more about this exciting discovery, or read a summary of the work here on Astrobites.

Atmospheric Studies of Cool planets

2013 Sep: Surveys for new planets using the transit and radial velocity techniques reveal the high frequency with which small, short-period planets occur around main sequence stars. However, only a few of these smaller planets can be easily observed to characterize their atmosphere. One such planet is GJ 3470b, which is about the size and mass of Uranus but much hotter: over 300 C (550 F). I led an analysis of this planet by observing the planet's transit with the new Keck/MOSFIRE spectrograph to look for evidence of water or methane absorption in the planet's atmosphere from 2.09-2.36 micron. As seen for other small, cool, low-mass planets, the current ensemble of measurements is consistent with a flat transmission spectrum, which suggests that the atmosphere is explained by some combination of high-altitude clouds and haze, disequilibrium chemistry, unexpected abundance patterns, or an extremely metal-rich atmosphere. Read our full paper here.

Artist's view of a transiting exoplanet
Artist's impression of a planet around an M dwarf.
ESO/L. Calçada

Our analysis predicted that transit observations at shorter wavelengths would provide the best opportunity to discriminate between plausible scenarios. Indeed, a simultaneous and independent analysis using optical photometry shows strong evidence for Rayleigh scattering in GJ 3470b's atmosphere, consistent with an atmosphere dominated by a scattering haze. If this haze is not too optically thick, GJ 3470b's relatively deep primary transit, bright host star, and low density will permit a detailed characterization of its atmosphere via transmission spectroscopy during transit.

Studying Small, Cool, Nearby Exoplanets

Artist's view of the planet candidate alpha Cen Bb
Artist's impression of the planet candidate alpha Cen Bb
(ESO)
2013 Jan: Surveys for new planets using the transit and radial velocity techniques are beginning to reveal the frequency with which small, short-period planets occur around main sequence stars. Using these results, I have made the first direct prediction of the number and types of such planets that will be amenable to direct characterization by high-contrast instruments on future giant segmented-mirror telescopes. I predict of order 10 planets should be accessible around stars within 8 pc of the Sun; these planets will have sizes from 1-8 Earth radii and have equilibrium temperatures under 400 K. In particular, I predict a 40% chance that a 1-2 Earth radius planet and an equilibrium temperature comparable to Earth's (200-250 K) will accessible to high-contrast thermal infrared characterization; this would be an exciting object to study! Several planets already discovered by radial velocity surveys will be accessible to near-infrared high-contrast GSMT observations, including those around the nearby stars alpha Cen, GJ 139, GJ 876, and tau Cet. In the paper, I suggest that theorists begin to explore the range of possible atmospheric and/or surface compositions of these planets, and that more work should be done to precisely characterize the stars in the solar neighborhood. Read the full paper (accepted to A and A).

Re-evaluating hot Jupiter WASP-12b

Artist's view of the extremely hot Jupiter WASP-12b
Artist's impression of WASP-12b
(NASA)
2012 Nov: The hot Jupiter WASP-12b is one of the largest and hottest transiting planets, and has been studied by many groups; on the basis of these analysis, the planet has been claimed to have a very high carbon to oxygen ratio in its atmosphere. Such a carbon-rich atmosphere is predicted to show strong absorption features from carbon monoxide at a wavelength of 2.31 microns. We observed this planet with the Subaru Telescope and found no absorption at this wavelength: instead, our observations are consistent with a featureless spectrum, indicating an atmosphere whos temperature is approximately constant with altitude. Therefore our results argue against the current carbon-rich interpretation for this planet. Our analysis is being published in the Astrophysical Journal; read it here or read Caroline Morley's summaryhere on Astrobites.

Precise 24 micron Observations of HD 209458b

2012 June: The transiting hot Jupiter HD 209458b was the first known transiting planets, and is one of the best studied. Because it is one of the few transiting planets that was known during the Spitzer Space Telescope's cryogenic mission, HD 209458b has been characterized over a broader range of wavelengths than have most transiting planets. We recently conducted an archival analysis of all 24 micron observations of this planet to derive a homogeneous set of mid-infrared parameters for this system. Our analysis provides the most precise 24 micron eclipse measurement of any known planet; along with transit observations, our work demonstrates once again that this short-period planet's orbit is precisely consistent with zero eccentricity.

Artist's view of a transiting exoplanet
Artist's impression of GJ 1214b
ESO/L. Calçada

Unraveling the mystery of GJ 1214b

2011: The nearby star GJ 1214 hosts a planet intermediate in radius and mass between Earth and Neptune, resulting in some uncertainty as to its nature. We have observed this planet, GJ 1214b, during transit with the near-infrared NIRSPEC spectrograph on the Keck II telescope to characterize the planet's atmosphere. When taken in concert with constraints from other groups, our results support a consensus model in which the atmosphere of GJ 1214b contains significant H and He, but where methane is depleted. Our paper has been published in the Astrophysical Journal; you can access the official version (or free preprint) here, or read Caroline Morley's summary here on Astrobites.

Artist's view of a transiting extrasolar planet
Artist's view of a transiting extrasolar planet
NASA, ESA, and G. Bacon (STSci)

upsilon Andromedae b's phase curve:

2010: We report a new 24 micron phase curve for the planet upsilon Andromedae b, showing that the hottest part of the planet (at that wavelength) is shifted 80 degrees from the substellar point. This is a much larger shift than has been seen on other planets (ref1, ref2, ref3), and it's certainly not clear (at least, to me) what could be responsible for such a large shift of the planet's hot regions. See the Spitzer Press Release, or read the paper here.

Artist's view of a transiting extrasolar planet
Artist's view of a transiting extrasolar planet
NASA, ESA, and G. Bacon (STSci)

Exoplanet Characterization

My primary research interest lies in the field of exoplanetary formation, detection, and characterization. While at JPL I had the good fortune to work with Dr. Mark Swain of the JPL Exoplanet Center. Our work focused on ground-based spectroscopic observations of transiting extrasolar planets. By comparing observations in and out of secondary eclipse we hoped to be able to draw conclusions about the composition of the exoplanet atmosphere. A paper describing our results is in preparation, pending follow-up observations confirming our initial findings.

Instrumentation

GPI Planet Detection
Simulation of GPI
planet detection (GPI website)

Gemini Planet Imager

"The Gemini Planet Imager is the next generation adaptive optics instrument being built for the Gemini Telescope. The goal is to image extrasolar planets orbiting nearby stars." --(GPI website). The GPI is being constructed by a consortium of institutions including UCSC, UCLA, University of Victoria, Universite de Montreal, JPL, and probably a few others. It is scheduled to see "first light" on the Gemini South telescope sometime in 2010.

At NASA/JPL I worked on GPI's backend wavefront calibration system, which will allow the measurement and removal of residual and non-common path wavefront errors in the GPI optics.

Thirty Meter Telescope

Thirty Meter Telescope
Thirty Meter Telescope
(artist's conception).
The Thirty Meter Telescope (TMT) is a collaborative project between the University of California, Caltech, ACURA, and other partners. It is an effort to develop the world's largest optical and near-infrared telescope, offering unprecendented sensitivity and resolution. According to current plans, construction of TMT will begin in 2009 or early 2010.

I contributed to several aspects of this exciting new facility, but spent most of my time working with the Planet Formation Instrument (PFI), the proposed high-contrast imaging spectrograph for TMT. PFI will ultimately achieve contrast levels of 108-109 at an inner working angle of only 33 milliarcseconds in H band, allowing the first detections and characterizations of mature, reflected-light jovian planets in significant numbers. Among other tasks, I used the stringent requirements set by PFI to "backwards design" the telescope system so that these ambitious goals will not be precluded. This resulted in the first referreed publication discussing the use of a specific high-contrast imaging method on an extremely large segmented telescope.


Publications, Proceedings, and Talks

Curriculum Vitae