Eigenspectra: a framework for identifying spectra from 3D eclipse mapping
Adams, Arthur D
Feng, Y Katherina
Stevenson, Kevin B
Beatty, Thomas G
AffiliationDepartment of Astronomy and Steward Observatory, University of Arizona
Keywordsmethods: data analysis
planets and satellites: atmospheres
planets and satellites: gaseous planets
MetadataShow full item record
PublisherOxford University Press
CitationMansfield, M., Schlawin, E., Lustig-Yaeger, J., Adams, A. D., Rauscher, E., Arcangeli, J., ... & Beatty, T. G. (2020). Eigenspectra: a framework for identifying spectra from 3D eclipse mapping. Monthly Notices of the Royal Astronomical Society, 499(4), 5151-5162.
Rights© 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractPlanetary atmospheres are inherently 3D objects that can have strong gradients in latitude, longitude, and altitude. Secondary eclipse mapping is a powerful way to map the 3D distribution of the atmosphere, but the data can have large correlations and errors in the presence of photon and instrument noise. We develop a technique to mitigate the large uncertainties of eclipse maps by identifying a small number of dominant spectra to make them more tractable for individual analysis via atmospheric retrieval. We use the eigencurves method to infer a multiwavelength map of a planet from spectroscopic secondary eclipse light curves. We then apply a clustering algorithm to the planet map to identify several regions with similar emergent spectra. We combine the similar spectra together to construct an 'eigenspectrum' for each distinct region on the planetary map. We demonstrate how this approach could be used to isolate hot from cold regions and/or regions with different chemical compositions in observations of hot Jupiters with the James Webb Space Telescope (JWST). We find that our method struggles to identify sharp edges in maps with sudden discontinuities, but generally can be used as a first step before a more physically motivated modelling approach to determine the primary features observed on the planet. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
VersionFinal published version
SponsorsNational Aeronautics and Space Administration