The influence of nonuniform cloud cover on transit transmission spectra
We model the impact of nonuniform 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...
| Hoofdauteurs: | , |
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| Formaat: | Journal article |
| Gepubliceerd in: |
American Astronomical Society
2016
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| _version_ | 1826277152278970368 |
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| author | Line, MR Parmentier, V |
| author_facet | Line, MR Parmentier, V |
| author_sort | Line, MR |
| collection | OXFORD |
| description | We model the impact of nonuniform 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 μm). 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 nonuniform 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 finding is that the HST WFC3 transit transmission spectra of two well-observed objects, the hot Jupiter HD 189733b 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 that the transit timing is known to seconds. |
| first_indexed | 2024-03-06T23:24:36Z |
| format | Journal article |
| id | oxford-uuid:69ee29b3-9d9b-4e39-8377-cdefef0be2ac |
| institution | University of Oxford |
| last_indexed | 2024-03-06T23:24:36Z |
| publishDate | 2016 |
| publisher | American Astronomical Society |
| record_format | dspace |
| spelling | oxford-uuid:69ee29b3-9d9b-4e39-8377-cdefef0be2ac2022-03-26T18:54:11ZThe influence of nonuniform cloud cover on transit transmission spectraJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:69ee29b3-9d9b-4e39-8377-cdefef0be2acSymplectic Elements at OxfordAmerican Astronomical Society2016Line, MRParmentier, VWe model the impact of nonuniform 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 μm). 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 nonuniform 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 finding is that the HST WFC3 transit transmission spectra of two well-observed objects, the hot Jupiter HD 189733b 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 that the transit timing is known to seconds. |
| spellingShingle | Line, MR Parmentier, V The influence of nonuniform cloud cover on transit transmission spectra |
| title | The influence of nonuniform cloud cover on transit transmission spectra |
| title_full | The influence of nonuniform cloud cover on transit transmission spectra |
| title_fullStr | The influence of nonuniform cloud cover on transit transmission spectra |
| title_full_unstemmed | The influence of nonuniform cloud cover on transit transmission spectra |
| title_short | The influence of nonuniform cloud cover on transit transmission spectra |
| title_sort | influence of nonuniform cloud cover on transit transmission spectra |
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