1,191 research outputs found
The Influence of Non-Uniform Cloud Cover on Transit Transmission Spectra
We model the impact of non-uniform cloud cover on transit transmission
spectra. Patchy clouds exist in nearly every solar system atmosphere, brown
dwarfs, and transiting exoplanets. Our major findings suggest that fractional
cloud coverage can exactly mimic high mean molecular weight atmospheres and
vice-versa over certain wavelength regions, in particular, over the Hubble
Space Telescope (HST) Wide Field Camera 3 (WFC3) bandpass (1.1-1.7 m). We
also find that patchy cloud coverage exhibits a signature that is different
from uniform global clouds. Furthermore, we explain analytically why the
"patchy cloud-high mean molecular weight" degeneracy exists. We also explore
the degeneracy of non-uniform cloud coverage in atmospheric retrievals on both
synthetic and real planets. We find from retrievals on a synthetic solar
composition hot Jupiter with patchy clouds and a cloud free high mean molecular
weight warm Neptune, that both cloud free high mean molecular weight
atmospheres and partially cloudy atmospheres can explain the data equally well.
Another key find is that the HST WFC3 transit transmission spectra of two well
observed objects, the hot Jupiter HD189733b and the warm Neptune HAT-P-11b, can
be explained well by solar composition atmospheres with patchy clouds without
the need to invoke high mean molecular weight or global clouds. The degeneracy
between high molecular weight and solar composition partially cloudy
atmospheres can be broken by observing the molecular Rayleigh scattering
differences between the two. Furthermore, the signature of partially cloudy
limbs also appears as a 100 ppm residual in the ingress and egress of the
transit light curves, provided the transit timing is known to seconds.Comment: Accepted to ApJ Feb. 8, 201
Retrieving Temperatures and Abundances of Exoplanet Atmospheres with High-Resolution Cross-Correlation Spectroscopy
Hi-resolution spectroscopy (R > 25,000) has recently emerged as one of the
leading methods to detect atomic and molecular species in the atmospheres of
exoplanets. However, it has so far been lacking in a robust method to extract
quantitative constraints on temperature structure and molecular/atomic
abundances. In this work we present a novel Bayesian atmospheric retrieval
framework applicable to high resolution cross-correlation spectroscopy (HRCCS)
that relies upon the cross-correlation between data and models to extract the
planetary spectral signal. We successfully test the framework on simulated data
and show that it can correctly determine Bayesian credibility intervals on
atmospheric temperatures and abundances allowing for a quantitative exploration
of the inherent degeneracies. Furthermore, our new framework permits us to
trivially combine and explore the synergies between HRCCS and low-resolution
spectroscopy (LRS) to provide maximal leverage on the information contained
within each. This framework also allows us to quantitatively assess the impact
of molecular line opacities at high resolution. We apply the framework to VLT
CRIRES K-band spectra of HD 209458 b and HD 189733 b and retrieve abundant
carbon monoxide but sub-solar abundances for water, largely invariant under
different model assumptions. This confirms previous analysis of these datasets,
but is possibly at odds with detections of water at different wavelengths and
spectral resolutions. The framework presented here is the first step towards a
true synergy between space observatories and ground-based hi-resolution
observations.Comment: Accepted Version (01/16/19
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