The PEPSI Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy
Recent observations have shown that the atmospheres of ultrahot Jupiters (UHJs) commonly possess temperature inversions, where the temperature increases with increasing altitude. Nonetheless, which opacity sources are responsible for the presence of these inversions remains largely observationally u...
| Main Authors: | , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/acb7e2 |
| _version_ | 1827826802456788992 |
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| author | Marshall C. Johnson Ji Wang Anusha Pai Asnodkar Aldo S. Bonomo B. Scott Gaudi Thomas Henning Ilya Ilyin Engin Keles Luca Malavolta Matthias Mallonn Karan Molaverdikhani Valerio Nascimbeni Jennifer Patience Katja Poppenhaeger Gaetano Scandariato Everett Schlawin Evgenya Shkolnik Daniela Sicilia Alessandro Sozzetti Klaus G. Strassmeier Christian Veillet Fei Yan |
| author_facet | Marshall C. Johnson Ji Wang Anusha Pai Asnodkar Aldo S. Bonomo B. Scott Gaudi Thomas Henning Ilya Ilyin Engin Keles Luca Malavolta Matthias Mallonn Karan Molaverdikhani Valerio Nascimbeni Jennifer Patience Katja Poppenhaeger Gaetano Scandariato Everett Schlawin Evgenya Shkolnik Daniela Sicilia Alessandro Sozzetti Klaus G. Strassmeier Christian Veillet Fei Yan |
| author_sort | Marshall C. Johnson |
| collection | DOAJ |
| description | Recent observations have shown that the atmospheres of ultrahot Jupiters (UHJs) commonly possess temperature inversions, where the temperature increases with increasing altitude. Nonetheless, which opacity sources are responsible for the presence of these inversions remains largely observationally unconstrained. We used LBT/PEPSI to observe the atmosphere of the UHJ KELT-20 b in both transmission and emission in order to search for molecular agents which could be responsible for the temperature inversion. We validate our methodology by confirming a previous detection of Fe i in emission at 16.9 σ . Our search for the inversion agents TiO, VO, FeH, and CaH results in non-detections. Using injection-recovery testing we set 4 σ upper limits upon the volume mixing ratios for these constituents as low as ∼1 × 10 ^−9 for TiO. For TiO, VO, and CaH, our limits are much lower than expectations from an equilibrium chemical model, while we cannot set constraining limits on FeH with our data. We thus rule out TiO and CaH as the source of the temperature inversion in KELT-20 b, and VO only if the line lists are sufficiently accurate. |
| first_indexed | 2024-03-12T03:17:34Z |
| format | Article |
| id | doaj.art-f15cc6a21e2047738c8a247a7785fde6 |
| institution | Directory Open Access Journal |
| issn | 1538-3881 |
| language | English |
| last_indexed | 2024-03-12T03:17:34Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj.art-f15cc6a21e2047738c8a247a7785fde62023-09-03T14:08:27ZengIOP PublishingThe Astronomical Journal1538-38812023-01-01165415710.3847/1538-3881/acb7e2The PEPSI Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission SpectroscopyMarshall C. Johnson0https://orcid.org/0000-0002-5099-8185Ji Wang1https://orcid.org/0000-0002-4361-8885Anusha Pai Asnodkar2https://orcid.org/0000-0002-8823-8237Aldo S. Bonomo3https://orcid.org/0000-0002-6177-198XB. Scott Gaudi4https://orcid.org/0000-0003-0395-9869Thomas Henning5https://orcid.org/0000-0002-1493-300XIlya Ilyin6https://orcid.org/0000-0002-0551-046XEngin Keles7Luca Malavolta8https://orcid.org/0000-0002-6492-2085Matthias Mallonn9https://orcid.org/0000-0003-2865-042XKaran Molaverdikhani10https://orcid.org/0000-0002-0502-0428Valerio Nascimbeni11https://orcid.org/0000-0001-9770-1214Jennifer Patience12Katja Poppenhaeger13Gaetano Scandariato14https://orcid.org/0000-0003-2029-0626Everett Schlawin15https://orcid.org/0000-0001-8291-6490Evgenya Shkolnik16https://orcid.org/0000-0002-7260-5821Daniela Sicilia17Alessandro Sozzetti18https://orcid.org/0000-0002-7504-365XKlaus G. Strassmeier19https://orcid.org/0000-0002-6192-6494Christian Veillet20https://orcid.org/0000-0003-0272-0418Fei Yan21https://orcid.org/0000-0001-9585-9034Department of Astronomy, The Ohio State University , 4055 McPherson Laboratory, 140 West 18th Avenue, Columbus, OH 43210 USA ; johnson.7240@osu.eduDepartment of Astronomy, The Ohio State University , 4055 McPherson Laboratory, 140 West 18th Avenue, Columbus, OH 43210 USA ; johnson.7240@osu.eduDepartment of Astronomy, The Ohio State University , 4055 McPherson Laboratory, 140 West 18th Avenue, Columbus, OH 43210 USA ; johnson.7240@osu.eduINAF–Osservatorio Astrofisico di Torino , Strada Osservatorio 20, I-10025 Pino Torinese, ItalyDepartment of Astronomy, The Ohio State University , 4055 McPherson Laboratory, 140 West 18th Avenue, Columbus, OH 43210 USA ; johnson.7240@osu.eduMax-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, GermanyLeibniz-Institute for Astrophysics Potsdam (AIP) , An der Sternwarte 16, D-14482 Potsdam, GermanyLeibniz-Institute for Astrophysics Potsdam (AIP) , An der Sternwarte 16, D-14482 Potsdam, GermanyINAF—Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, I-35122 Padova, Italy; Dipartimento di Fisica e Astronomia “Galileo Galilei”, Universita degli Studi di Padova , I-35122 Padova, ItalyLeibniz-Institute for Astrophysics Potsdam (AIP) , An der Sternwarte 16, D-14482 Potsdam, GermanyMax-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, Germany; Universitäts-Sternwarte , Ludwig-Maximilians-Universität München, Scheinerstrasse 1, D-81679 München, Germany; Exzellenzcluster Origins , Boltzmannstraße 2, D-85748 Garching, GermanyINAF—Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, I-35122 Padova, ItalySchool of Earth and Space Exploration, Arizona State University , 660 S. Mill Avenue, Tempe, AZ 85281, USALeibniz-Institute for Astrophysics Potsdam (AIP) , An der Sternwarte 16, D-14482 Potsdam, Germany; Institute of Physics & Astronomy, University of Potsdam , Karl-Liebknecht-Str. 24/25, D-14476 Potsdam, GermanyINAF—Osservatorio Astrofisico di Catania , via S. Sofia 78, I-95123 Catania, ItalySteward Observatory, University of Arizona , 933 N. Cherry Avenue, Tucson, AZ 85721, USASchool of Earth and Space Exploration, Arizona State University , 660 S. Mill Avenue, Tempe, AZ 85281, USAINAF—Osservatorio Astrofisico di Catania , via S. Sofia 78, I-95123 Catania, ItalyINAF–Osservatorio Astrofisico di Torino , Strada Osservatorio 20, I-10025 Pino Torinese, ItalyLeibniz-Institute for Astrophysics Potsdam (AIP) , An der Sternwarte 16, D-14482 Potsdam, Germany; Institute of Physics & Astronomy, University of Potsdam , Karl-Liebknecht-Str. 24/25, D-14476 Potsdam, GermanyLarge Binocular Telescope Observatory , 933 N. Cherry Avenue, Tucson, AZ 85721, USAMax-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, Germany; Institute of Astrophysics, University of Göttingen , Friedrich-Hund-Platz 1 , D-37077 Göttingen, GermanyRecent observations have shown that the atmospheres of ultrahot Jupiters (UHJs) commonly possess temperature inversions, where the temperature increases with increasing altitude. Nonetheless, which opacity sources are responsible for the presence of these inversions remains largely observationally unconstrained. We used LBT/PEPSI to observe the atmosphere of the UHJ KELT-20 b in both transmission and emission in order to search for molecular agents which could be responsible for the temperature inversion. We validate our methodology by confirming a previous detection of Fe i in emission at 16.9 σ . Our search for the inversion agents TiO, VO, FeH, and CaH results in non-detections. Using injection-recovery testing we set 4 σ upper limits upon the volume mixing ratios for these constituents as low as ∼1 × 10 ^−9 for TiO. For TiO, VO, and CaH, our limits are much lower than expectations from an equilibrium chemical model, while we cannot set constraining limits on FeH with our data. We thus rule out TiO and CaH as the source of the temperature inversion in KELT-20 b, and VO only if the line lists are sufficiently accurate.https://doi.org/10.3847/1538-3881/acb7e2Exoplanet astronomyExoplanet atmospheresTransmission spectroscopy |
| spellingShingle | Marshall C. Johnson Ji Wang Anusha Pai Asnodkar Aldo S. Bonomo B. Scott Gaudi Thomas Henning Ilya Ilyin Engin Keles Luca Malavolta Matthias Mallonn Karan Molaverdikhani Valerio Nascimbeni Jennifer Patience Katja Poppenhaeger Gaetano Scandariato Everett Schlawin Evgenya Shkolnik Daniela Sicilia Alessandro Sozzetti Klaus G. Strassmeier Christian Veillet Fei Yan The PEPSI Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy The Astronomical Journal Exoplanet astronomy Exoplanet atmospheres Transmission spectroscopy |
| title | The PEPSI Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy |
| title_full | The PEPSI Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy |
| title_fullStr | The PEPSI Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy |
| title_full_unstemmed | The PEPSI Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy |
| title_short | The PEPSI Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy |
| title_sort | pepsi exoplanet transit survey pets ii a deep search for thermal inversion agents in kelt 20 b mascara 2 b with emission and transmission spectroscopy |
| topic | Exoplanet astronomy Exoplanet atmospheres Transmission spectroscopy |
| url | https://doi.org/10.3847/1538-3881/acb7e2 |
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