A5005499353- Stellar, planetary, and galactic studies
- Astronomy and Astrophysical Research
- Astro and Planetary Science
- Astrophysics and Star Formation Studies
- Astronomical Observations and Instrumentation
- Scientific Research and Discoveries
- Geophysics and Gravity Measurements
- Atmospheric Ozone and Climate
- Planetary Science and Exploration
- Calibration and Measurement Techniques
- Adaptive optics and wavefront sensing
- Gamma-ray bursts and supernovae
The University of Texas at Austin
2022
University of California, Berkeley
2019
TESS is finding transiting planet candidates around bright, nearby stars across the entire sky. The large field-of-view, however, results in low spatial resolution, therefore multiple contribute to almost every light curve. High-angular resolution imaging can detect previously unknown companions planetary candidate hosts that dilute transit depths, lead host star ambiguity, and some cases are source of false-positive signals. We use speckle on SOAR search for 542 Southern provide correction...
Abstract We present observations of the 1.35 ± 0.07 Earth radius planet L 98-59 c, collected using Wide Field Camera 3 on Hubble Space Telescope (HST). is a nearby (10.6 pc), bright ( H = 7.4 mag) M3V star that harbors three small, transiting planets. As one closest known multi-planet systems, offers best opportunities to probe and compare atmospheres rocky planets formed in same stellar environment. measured transmission spectrum extracted showed marginal evidence (2.1 σ ) for...
Abstract The coldest Y spectral type brown dwarfs are similar in mass and temperature to cool warm (∼200–400 K) giant exoplanets. We can therefore use their atmospheres as proxies for planetary atmospheres, testing our understanding of physics chemistry these complex, worlds. At cold temperatures, enough water clouds form, chemical timescales increase, increasing the likelihood disequilibrium compared warmer classes planets. JWST observations revolutionizing characterization worlds with high...
Abstract Water clouds are expected to form on Y dwarfs and giant planets with equilibrium temperatures near or below that of Earth, drastically altering their atmospheric compositions albedos thermal emission spectra. Here we use the 1D Community Aerosol Radiation Model for Atmospheres (CARMA) investigate microphysics water cool substellar worlds constrain typical particle sizes vertical extent, taking into consideration nucleation condensation, which have not been considered in detail H/He...
The coldest Y spectral type brown dwarfs are similar in mass and temperature to cool warm ($\sim$200 -- 400 K) giant exoplanets. We can therefore use their atmospheres as proxies for planetary atmospheres, testing our understanding of physics chemistry these complex, worlds. At cold temperatures, enough water clouds form, chemical timescales increase, increasing the likelihood disequilibrium compared warmer classes planets. JWST observations revolutionizing characterization worlds with high...
We present observations of the 1.35+/-0.07 Earth-radius planet L 98-59 c using Wide Field Camera~3 on Hubble Space Telescope. is a nearby (10.6 pc), bright (H=7.4 mag), M3V star that harbors three small, transiting planets. As one closest known multi-planet systems, offers best opportunities to probe and compare atmospheres rocky planets formed in same stellar environment. measured transmission spectrum during single transit, with extracted showing marginal evidence for wavelength-dependent...
Water must condense into ice clouds in the coldest brown dwarfs and exoplanets. When they form, these icy change emergent spectra, temperature structure, albedo of substellar atmosphere. The properties are governed by complex microphysics but complexities often not captured simpler parameterized cloud models used climate or retrieval models. Here, we combine microphysical modeling 1D to incorporate insights from a self-consistent, model. Using Community Aerosol Radiation Model for...
Abstract Water must condense into ice clouds in the coldest brown dwarfs and exoplanets. When they form, these icy change emergent spectra, temperature structure, albedo of substellar atmosphere. The properties are governed by complex microphysics but complexities often not captured simpler parameterized cloud models used climate or retrieval models. Here, we combine microphysical modeling 1D to incorporate insights from a self-consistent, model. Using Community Aerosol Radiation Model for...