A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters
Although exoplanetary science was not initially projected to be a substantial part of the Spitzer mission, its exoplanet observations set the stage for current and future surveys with JWST and Ariel. We present a comprehensive reduction and analysis of Spitzer’s 4.5 μ m phase curves of 29 hot Jupite...
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2024-01-01
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| Online Access: | https://doi.org/10.3847/1538-3881/ad8dd7 |
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| author | Lisa Dang Taylor J. Bell Ying (Zoe) Shu Nicolas B. Cowan Jacob L. Bean Drake Deming Eliza M.-R. Kempton Megan Weiner Mansfield Emily Rauscher Vivien Parmentier Alexandra Rochon Kevin B. Stevenson Mark Swain Laura Kreidberg Tiffany Kataria Jean-Michel Désert Robert Zellem Jonathan J. Fortney Nikole K. Lewis Michael Line Caroline Morley Adam Showman |
| author_facet | Lisa Dang Taylor J. Bell Ying (Zoe) Shu Nicolas B. Cowan Jacob L. Bean Drake Deming Eliza M.-R. Kempton Megan Weiner Mansfield Emily Rauscher Vivien Parmentier Alexandra Rochon Kevin B. Stevenson Mark Swain Laura Kreidberg Tiffany Kataria Jean-Michel Désert Robert Zellem Jonathan J. Fortney Nikole K. Lewis Michael Line Caroline Morley Adam Showman |
| author_sort | Lisa Dang |
| collection | DOAJ |
| description | Although exoplanetary science was not initially projected to be a substantial part of the Spitzer mission, its exoplanet observations set the stage for current and future surveys with JWST and Ariel. We present a comprehensive reduction and analysis of Spitzer’s 4.5 μ m phase curves of 29 hot Jupiters on low-eccentricity orbits. The analysis, performed with the Spitzer Phase Curve Analysis pipeline, confirms that BLISS mapping is the best detrending scheme of the three independent schemes we tested for most, but not all, observations. Visual inspection remains necessary to ensure consistency across detrending methods due to the diversity of phase-curve data and systematics. Regardless of the model selection scheme, whether using the lowest BIC or a uniform detrending approach, we observe the same trends, or lack thereof. We explore phase-curve trends as a function of irradiation temperature, orbital period, planetary radius, mass, and stellar effective temperature. We discuss the trends that are robustly detected and provide potential explanations for those that are not observed. While it is almost tautological that planets receiving greater instellation are hotter, we are still far from confirming dynamical theories of heat transport in hot Jupiter atmospheres due to the sample’s diversity. Even among planets with similar temperatures, other factors like rotation and metallicity vary significantly. Larger, curated sample sizes and higher-fidelity phase-curve measurements from JWST and Ariel are needed to firmly establish the parameters governing day–night heat transport on synchronously rotating planets. |
| format | Article |
| id | doaj-art-123f9b96b7214bc8a90a31ae941fea0e |
| institution | DOAJ |
| issn | 1538-3881 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astronomical Journal |
| spelling | doaj-art-123f9b96b7214bc8a90a31ae941fea0e2025-08-20T02:49:40ZengIOP PublishingThe Astronomical Journal1538-38812024-01-0116913210.3847/1538-3881/ad8dd7A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot JupitersLisa Dang0https://orcid.org/0000-0003-4987-6591Taylor J. Bell1https://orcid.org/0000-0003-4177-2149Ying (Zoe) Shu2https://orcid.org/0009-0002-5701-6276Nicolas B. Cowan3https://orcid.org/0000-0001-6129-5699Jacob L. Bean4https://orcid.org/0000-0003-4733-6532Drake Deming5https://orcid.org/0000-0001-5727-4094Eliza M.-R. Kempton6https://orcid.org/0000-0002-1337-9051Megan Weiner Mansfield7https://orcid.org/0000-0003-4241-7413Emily Rauscher8https://orcid.org/0000-0003-3963-9672Vivien Parmentier9https://orcid.org/0000-0001-9521-6258Alexandra Rochon10Kevin B. Stevenson11https://orcid.org/0000-0002-7352-7941Mark Swain12Laura Kreidberg13https://orcid.org/0000-0003-0514-1147Tiffany Kataria14https://orcid.org/0000-0003-3759-9080Jean-Michel Désert15https://orcid.org/0000-0002-0875-8401Robert Zellem16https://orcid.org/0000-0001-7547-0398Jonathan J. Fortney17https://orcid.org/0000-0002-9843-4354Nikole K. Lewis18https://orcid.org/0000-0002-8507-1304Michael Line19https://orcid.org/0000-0002-2338-476XCaroline Morley20https://orcid.org/0000-0002-4404-0456Adam Showman21Trottier Institute for Research on Exoplanets and Département de Physique, Université de Montréal , 1375 Avenue Thérèse-Lavoie-Roux, Montréal, QC H2V 0B3, Canada ; kha.han.lisa.dang@umontreal.caBay Area Environmental Research Institute, NASA Ames Research Center , Moffett Field, CA 94035, USA; Space Science and Astrobiology Division, NASA Ames Research Center , Moffett Field, CA 94035, USATrottier Institute for Research on Exoplanets and Département de Physique, Université de Montréal , 1375 Avenue Thérèse-Lavoie-Roux, Montréal, QC H2V 0B3, Canada ; kha.han.lisa.dang@umontreal.caDepartment of Physics, McGill University , 3600 University Street, Montreal, QC H3A 2T8, Canada; Department of Earth & Planetary Sciences, McGill University , 3450 University Street, Montréal, QC H3A 2A7, CanadaDepartment of Astronomy and Astrophysics, University of Chicago , Chicago, IL 60637, USADepartment of Astronomy, University of Maryland , College Park, MD 20742-2421, USADepartment of Astronomy, University of Maryland , College Park, MD 20742-2421, USASteward Observatory, University of Arizona , Tucson, AZ 85721, USADepartment of Astronomy, University of Michigan , 1085 S. University, Ann Arbor, MI 48109, USALaboratoire Lagrange , Observatoire de la Côte d’Azur, CNRS, Université Côte d’Azur, Nice, FranceDepartment of Physics, McGill University , 3600 University Street, Montreal, QC H3A 2T8, Canada; Department of Earth & Planetary Sciences, McGill University , 3450 University Street, Montréal, QC H3A 2A7, CanadaJHU Applied Physics Laboratory , 11100 Johns Hopkins Road, Laurel, MD 20723, USANASA Jet Propulsion Laboratory , 4800 Oak Grove Drive, Pasadena, CA 91109, USAMax-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, GermanyNASA Jet Propulsion Laboratory , 4800 Oak Grove Drive, Pasadena, CA 91109, USAAnton Pannekoek Institute for Astronomy, University of Amsterdam , Noord Holland, NL-1090GE Amsterdam, The NetherlandsNASA Goddard Space Flight Center , 8800 Greenbelt Road, Greenbelt, MD 20771, USADepartment of Astronomy and Astrophysics, University of California , Santa Cruz, CA 95064, USADepartment of Astronomy and Carl Sagan Institute, Cornell University , 122 Sciences Drive, Ithaca, NY 14853, USASchool of Earth and Space Exploration, Arizona State University , Tempe, AZ 85287, USADepartment of Astronomy, University of Texas at Austin , 2515 Speedway, Austin, TX 78712, USALunar and Planetary Lab, University of Arizona , Tucson, AZ 85721-0092, USAAlthough exoplanetary science was not initially projected to be a substantial part of the Spitzer mission, its exoplanet observations set the stage for current and future surveys with JWST and Ariel. We present a comprehensive reduction and analysis of Spitzer’s 4.5 μ m phase curves of 29 hot Jupiters on low-eccentricity orbits. The analysis, performed with the Spitzer Phase Curve Analysis pipeline, confirms that BLISS mapping is the best detrending scheme of the three independent schemes we tested for most, but not all, observations. Visual inspection remains necessary to ensure consistency across detrending methods due to the diversity of phase-curve data and systematics. Regardless of the model selection scheme, whether using the lowest BIC or a uniform detrending approach, we observe the same trends, or lack thereof. We explore phase-curve trends as a function of irradiation temperature, orbital period, planetary radius, mass, and stellar effective temperature. We discuss the trends that are robustly detected and provide potential explanations for those that are not observed. While it is almost tautological that planets receiving greater instellation are hotter, we are still far from confirming dynamical theories of heat transport in hot Jupiter atmospheres due to the sample’s diversity. Even among planets with similar temperatures, other factors like rotation and metallicity vary significantly. Larger, curated sample sizes and higher-fidelity phase-curve measurements from JWST and Ariel are needed to firmly establish the parameters governing day–night heat transport on synchronously rotating planets.https://doi.org/10.3847/1538-3881/ad8dd7Exoplanet atmospheresExoplanet astronomyExoplanet atmospheric dynamics |
| spellingShingle | Lisa Dang Taylor J. Bell Ying (Zoe) Shu Nicolas B. Cowan Jacob L. Bean Drake Deming Eliza M.-R. Kempton Megan Weiner Mansfield Emily Rauscher Vivien Parmentier Alexandra Rochon Kevin B. Stevenson Mark Swain Laura Kreidberg Tiffany Kataria Jean-Michel Désert Robert Zellem Jonathan J. Fortney Nikole K. Lewis Michael Line Caroline Morley Adam Showman A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters The Astronomical Journal Exoplanet atmospheres Exoplanet astronomy Exoplanet atmospheric dynamics |
| title | A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters |
| title_full | A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters |
| title_fullStr | A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters |
| title_full_unstemmed | A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters |
| title_short | A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters |
| title_sort | comprehensive analysis of spitzer 4 5 μm phase curves of hot jupiters |
| topic | Exoplanet atmospheres Exoplanet astronomy Exoplanet atmospheric dynamics |
| url | https://doi.org/10.3847/1538-3881/ad8dd7 |
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