Two-Dimensional Eclipse Mapping of the Hot Jupiter WASP-43b with JWST MIRI/LRS
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| author | Hammond, Mark Bell, Taylor J. Challener, Ryan C. Lewis, Neil T. Mansfield, Megan Weiner Malsky, Isaac Rauscher, Emily Bean, Jacob L. Carone, Ludmila Mendonça, João M. Teinturier, Lucas Tan, Xianyu Crouzet, Nicolas Kreidberg, Laura Morello, Giuseppe Parmentier, Vivien Blecic, Jasmina Désert, Jean-Michel Helling, Christiane Lagage, Pierre-Olivier Molaverdikhani, Karan Nixon, Matthew C. Rackham, Benjamin V. Yang, Jingxuan |
| author_facet | Hammond, Mark Bell, Taylor J. Challener, Ryan C. Lewis, Neil T. Mansfield, Megan Weiner Malsky, Isaac Rauscher, Emily Bean, Jacob L. Carone, Ludmila Mendonça, João M. Teinturier, Lucas Tan, Xianyu Crouzet, Nicolas Kreidberg, Laura Morello, Giuseppe Parmentier, Vivien Blecic, Jasmina Désert, Jean-Michel Helling, Christiane Lagage, Pierre-Olivier Molaverdikhani, Karan Nixon, Matthew C. Rackham, Benjamin V. Yang, Jingxuan |
| contents | We present eclipse maps of the two-dimensional thermal emission from the dayside of the hot Jupiter WASP-43b, derived from an observation of a phase curve with the JWST MIRI/LRS instrument. The observed eclipse shapes deviate significantly from those expected for a planet emitting uniformly over its surface. We fit a map to this deviation, constructed from spherical harmonics up to order $\ell_{\rm max}=2$, alongside the planetary, orbital, stellar, and systematic parameters. This yields a map with a meridionally-averaged eastward hot-spot shift of $(7.75 \pm 0.36)^{\circ}$, with no significant degeneracy between the map and the additional parameters. We show the latitudinal and longitudinal contributions of the day-side emission structure to the eclipse shape, finding a latitudinal signal of $\sim$200 ppm and a longitudinal signal of $\sim$250 ppm. To investigate the sensitivity of the map to the method, we fix the non-mapping parameters and derive an "eigenmap" fitted with an optimised number of orthogonal phase curves, which yields a similar map to the $\ell_{\rm max}=2$ map. We also fit a map up to $\ell_{\rm max}=3$, which shows a smaller hot-spot shift, with a larger uncertainty. These maps are similar to those produced by atmospheric simulations. We conclude that there is a significant mapping signal which constrains the spherical harmonic components of our model up to $\ell_{\rm max}=2$. Alternative mapping models may derive different structures with smaller-scale features; we suggest that further observations of WASP-43b and other planets will drive the development of more robust methods and more accurate maps. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2404_16488 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Two-Dimensional Eclipse Mapping of the Hot Jupiter WASP-43b with JWST MIRI/LRS Hammond, Mark Bell, Taylor J. Challener, Ryan C. Lewis, Neil T. Mansfield, Megan Weiner Malsky, Isaac Rauscher, Emily Bean, Jacob L. Carone, Ludmila Mendonça, João M. Teinturier, Lucas Tan, Xianyu Crouzet, Nicolas Kreidberg, Laura Morello, Giuseppe Parmentier, Vivien Blecic, Jasmina Désert, Jean-Michel Helling, Christiane Lagage, Pierre-Olivier Molaverdikhani, Karan Nixon, Matthew C. Rackham, Benjamin V. Yang, Jingxuan Earth and Planetary Astrophysics We present eclipse maps of the two-dimensional thermal emission from the dayside of the hot Jupiter WASP-43b, derived from an observation of a phase curve with the JWST MIRI/LRS instrument. The observed eclipse shapes deviate significantly from those expected for a planet emitting uniformly over its surface. We fit a map to this deviation, constructed from spherical harmonics up to order $\ell_{\rm max}=2$, alongside the planetary, orbital, stellar, and systematic parameters. This yields a map with a meridionally-averaged eastward hot-spot shift of $(7.75 \pm 0.36)^{\circ}$, with no significant degeneracy between the map and the additional parameters. We show the latitudinal and longitudinal contributions of the day-side emission structure to the eclipse shape, finding a latitudinal signal of $\sim$200 ppm and a longitudinal signal of $\sim$250 ppm. To investigate the sensitivity of the map to the method, we fix the non-mapping parameters and derive an "eigenmap" fitted with an optimised number of orthogonal phase curves, which yields a similar map to the $\ell_{\rm max}=2$ map. We also fit a map up to $\ell_{\rm max}=3$, which shows a smaller hot-spot shift, with a larger uncertainty. These maps are similar to those produced by atmospheric simulations. We conclude that there is a significant mapping signal which constrains the spherical harmonic components of our model up to $\ell_{\rm max}=2$. Alternative mapping models may derive different structures with smaller-scale features; we suggest that further observations of WASP-43b and other planets will drive the development of more robust methods and more accurate maps. |
| title | Two-Dimensional Eclipse Mapping of the Hot Jupiter WASP-43b with JWST MIRI/LRS |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2404.16488 |