Carbon monoxide emission lines reveal an inverted atmosphere in the ultra hot Jupiter WASP-33 b consistent with an eastward hot spot
ABSTRACT We report the first detection of CO emission at high spectral resolution in the day-side infrared thermal spectrum of an exoplanet. These emission lines, found in the atmosphere of the transiting ultra hot Jupiter (UHJ) WASP-33 b, provide unambiguous evidence of its thermal inversion. Using...
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Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2023-04, Vol.522 (2), p.2145-2170 |
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creator | van Sluijs, Lennart Birkby, Jayne L Lothringer, Joshua Lee, Elspeth K H Crossfield, Ian J M Parmentier, Vivien Brogi, Matteo Kulesa, Craig McCarthy, Don Charbonneau, David |
description | ABSTRACT
We report the first detection of CO emission at high spectral resolution in the day-side infrared thermal spectrum of an exoplanet. These emission lines, found in the atmosphere of the transiting ultra hot Jupiter (UHJ) WASP-33 b, provide unambiguous evidence of its thermal inversion. Using spectra from the MMT Exoplanet Atmosphere Survey (MEASURE, R ∼ 15 000), covering pre- and post-eclipse phases, we cross-correlate with 1D PHOENIX spectral templates to detect CO at S/N = 7.9 ($v_{\rm {sys}}=0.15^{+0.64}_{-0.65}$ km s−1, $K_{\rm {p}}=229.5^{+1.1}_{-1.0}$ km s−1). Moreover, using cross-correlation-to-log-likelihood mapping, we find that the scaling parameter which controls the spectral line contrast changes with phase. We thus use the general circulation model SPARC/MITgcm post-processed by the 3D gCMCRT radiative transfer code to interpret this variation, finding it consistent with an eastward-shifted hot spot. Pre-eclipse, when the hot spot faces Earth, the thermal profiles are shallower leading to smaller line contrast despite greater overall flux. Post-eclipse, the western part of the day-side faces Earth and has much steeper thermal profiles, leading to larger line contrast despite less overall flux. This demonstrates that within the log-likelihood framework, even relatively moderate resolution spectra can be used to understand the 3D nature of close-in exoplanets, and that resolution can be traded for photon-collecting power when the induced Doppler-shift is sufficiently large. We highlight CO as a good probe of UHJ thermal structure and dynamics that does not suffer from stellar activity, unlike species that are also present in the host star e.g. iron lines. |
doi_str_mv | 10.1093/mnras/stad1103 |
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We report the first detection of CO emission at high spectral resolution in the day-side infrared thermal spectrum of an exoplanet. These emission lines, found in the atmosphere of the transiting ultra hot Jupiter (UHJ) WASP-33 b, provide unambiguous evidence of its thermal inversion. Using spectra from the MMT Exoplanet Atmosphere Survey (MEASURE, R ∼ 15 000), covering pre- and post-eclipse phases, we cross-correlate with 1D PHOENIX spectral templates to detect CO at S/N = 7.9 ($v_{\rm {sys}}=0.15^{+0.64}_{-0.65}$ km s−1, $K_{\rm {p}}=229.5^{+1.1}_{-1.0}$ km s−1). Moreover, using cross-correlation-to-log-likelihood mapping, we find that the scaling parameter which controls the spectral line contrast changes with phase. We thus use the general circulation model SPARC/MITgcm post-processed by the 3D gCMCRT radiative transfer code to interpret this variation, finding it consistent with an eastward-shifted hot spot. Pre-eclipse, when the hot spot faces Earth, the thermal profiles are shallower leading to smaller line contrast despite greater overall flux. Post-eclipse, the western part of the day-side faces Earth and has much steeper thermal profiles, leading to larger line contrast despite less overall flux. This demonstrates that within the log-likelihood framework, even relatively moderate resolution spectra can be used to understand the 3D nature of close-in exoplanets, and that resolution can be traded for photon-collecting power when the induced Doppler-shift is sufficiently large. We highlight CO as a good probe of UHJ thermal structure and dynamics that does not suffer from stellar activity, unlike species that are also present in the host star e.g. iron lines.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stad1103</identifier><language>eng</language><publisher>Oxford University Press</publisher><ispartof>Monthly notices of the Royal Astronomical Society, 2023-04, Vol.522 (2), p.2145-2170</ispartof><rights>The Author(s) 2023. Published by Oxford University Press on behalf of Royal Astronomical Society 2023</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c313t-8cc7667c01178afd4b8949f694ae48de5da0ef5edc912dfb03d099a2da04751c3</citedby><cites>FETCH-LOGICAL-c313t-8cc7667c01178afd4b8949f694ae48de5da0ef5edc912dfb03d099a2da04751c3</cites><orcidid>0000-0002-4125-0140</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>315,781,785,1605,27926,27927</link.rule.ids></links><search><creatorcontrib>van Sluijs, Lennart</creatorcontrib><creatorcontrib>Birkby, Jayne L</creatorcontrib><creatorcontrib>Lothringer, Joshua</creatorcontrib><creatorcontrib>Lee, Elspeth K H</creatorcontrib><creatorcontrib>Crossfield, Ian J M</creatorcontrib><creatorcontrib>Parmentier, Vivien</creatorcontrib><creatorcontrib>Brogi, Matteo</creatorcontrib><creatorcontrib>Kulesa, Craig</creatorcontrib><creatorcontrib>McCarthy, Don</creatorcontrib><creatorcontrib>Charbonneau, David</creatorcontrib><title>Carbon monoxide emission lines reveal an inverted atmosphere in the ultra hot Jupiter WASP-33 b consistent with an eastward hot spot</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
We report the first detection of CO emission at high spectral resolution in the day-side infrared thermal spectrum of an exoplanet. These emission lines, found in the atmosphere of the transiting ultra hot Jupiter (UHJ) WASP-33 b, provide unambiguous evidence of its thermal inversion. Using spectra from the MMT Exoplanet Atmosphere Survey (MEASURE, R ∼ 15 000), covering pre- and post-eclipse phases, we cross-correlate with 1D PHOENIX spectral templates to detect CO at S/N = 7.9 ($v_{\rm {sys}}=0.15^{+0.64}_{-0.65}$ km s−1, $K_{\rm {p}}=229.5^{+1.1}_{-1.0}$ km s−1). Moreover, using cross-correlation-to-log-likelihood mapping, we find that the scaling parameter which controls the spectral line contrast changes with phase. We thus use the general circulation model SPARC/MITgcm post-processed by the 3D gCMCRT radiative transfer code to interpret this variation, finding it consistent with an eastward-shifted hot spot. Pre-eclipse, when the hot spot faces Earth, the thermal profiles are shallower leading to smaller line contrast despite greater overall flux. Post-eclipse, the western part of the day-side faces Earth and has much steeper thermal profiles, leading to larger line contrast despite less overall flux. This demonstrates that within the log-likelihood framework, even relatively moderate resolution spectra can be used to understand the 3D nature of close-in exoplanets, and that resolution can be traded for photon-collecting power when the induced Doppler-shift is sufficiently large. We highlight CO as a good probe of UHJ thermal structure and dynamics that does not suffer from stellar activity, unlike species that are also present in the host star e.g. iron lines.</description><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>TOX</sourceid><recordid>eNqFkDtPwzAURi0EEqWwMntlSGvHeXmsKp6qBBIgxsixbxSjxo583RZ2fjgphZnpSkf3fMMh5JKzGWdSzHsXFM4xKsM5E0dkwkWRJ6ksimMyYUzkSVVyfkrOEN8ZY5lIiwn5WqrQeEd77_yHNUCht4h2JGvrAGmALag1VY5at4UQwVAVe49DBwFGRmMHdLOOQdHOR_qwGWyEQN8Wz0-JELSh2ju0GMFFurOx2y-BwrhTwfwYOPh4Tk5atUa4-L1T8npz_bK8S1aPt_fLxSrRgouYVFqXRVFqxnlZqdZkTSUz2RYyU5BVBnKjGLQ5GC15atqGCcOkVOmIszLnWkzJ7LCrg0cM0NZDsL0KnzVn9b5h_dOw_ms4ClcHwW-G_36_AW30eCQ</recordid><startdate>20230421</startdate><enddate>20230421</enddate><creator>van Sluijs, Lennart</creator><creator>Birkby, Jayne L</creator><creator>Lothringer, Joshua</creator><creator>Lee, Elspeth K H</creator><creator>Crossfield, Ian J M</creator><creator>Parmentier, Vivien</creator><creator>Brogi, Matteo</creator><creator>Kulesa, Craig</creator><creator>McCarthy, Don</creator><creator>Charbonneau, David</creator><general>Oxford University Press</general><scope>TOX</scope><scope>AAYXX</scope><scope>CITATION</scope><orcidid>https://orcid.org/0000-0002-4125-0140</orcidid></search><sort><creationdate>20230421</creationdate><title>Carbon monoxide emission lines reveal an inverted atmosphere in the ultra hot Jupiter WASP-33 b consistent with an eastward hot spot</title><author>van Sluijs, Lennart ; Birkby, Jayne L ; Lothringer, Joshua ; Lee, Elspeth K H ; Crossfield, Ian J M ; Parmentier, Vivien ; Brogi, Matteo ; Kulesa, Craig ; McCarthy, Don ; Charbonneau, David</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c313t-8cc7667c01178afd4b8949f694ae48de5da0ef5edc912dfb03d099a2da04751c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>van Sluijs, Lennart</creatorcontrib><creatorcontrib>Birkby, Jayne L</creatorcontrib><creatorcontrib>Lothringer, Joshua</creatorcontrib><creatorcontrib>Lee, Elspeth K H</creatorcontrib><creatorcontrib>Crossfield, Ian J M</creatorcontrib><creatorcontrib>Parmentier, Vivien</creatorcontrib><creatorcontrib>Brogi, Matteo</creatorcontrib><creatorcontrib>Kulesa, Craig</creatorcontrib><creatorcontrib>McCarthy, Don</creatorcontrib><creatorcontrib>Charbonneau, David</creatorcontrib><collection>Oxford Journals Open Access Collection</collection><collection>CrossRef</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>van Sluijs, Lennart</au><au>Birkby, Jayne L</au><au>Lothringer, Joshua</au><au>Lee, Elspeth K H</au><au>Crossfield, Ian J M</au><au>Parmentier, Vivien</au><au>Brogi, Matteo</au><au>Kulesa, Craig</au><au>McCarthy, Don</au><au>Charbonneau, David</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Carbon monoxide emission lines reveal an inverted atmosphere in the ultra hot Jupiter WASP-33 b consistent with an eastward hot spot</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2023-04-21</date><risdate>2023</risdate><volume>522</volume><issue>2</issue><spage>2145</spage><epage>2170</epage><pages>2145-2170</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
We report the first detection of CO emission at high spectral resolution in the day-side infrared thermal spectrum of an exoplanet. These emission lines, found in the atmosphere of the transiting ultra hot Jupiter (UHJ) WASP-33 b, provide unambiguous evidence of its thermal inversion. Using spectra from the MMT Exoplanet Atmosphere Survey (MEASURE, R ∼ 15 000), covering pre- and post-eclipse phases, we cross-correlate with 1D PHOENIX spectral templates to detect CO at S/N = 7.9 ($v_{\rm {sys}}=0.15^{+0.64}_{-0.65}$ km s−1, $K_{\rm {p}}=229.5^{+1.1}_{-1.0}$ km s−1). Moreover, using cross-correlation-to-log-likelihood mapping, we find that the scaling parameter which controls the spectral line contrast changes with phase. We thus use the general circulation model SPARC/MITgcm post-processed by the 3D gCMCRT radiative transfer code to interpret this variation, finding it consistent with an eastward-shifted hot spot. Pre-eclipse, when the hot spot faces Earth, the thermal profiles are shallower leading to smaller line contrast despite greater overall flux. Post-eclipse, the western part of the day-side faces Earth and has much steeper thermal profiles, leading to larger line contrast despite less overall flux. This demonstrates that within the log-likelihood framework, even relatively moderate resolution spectra can be used to understand the 3D nature of close-in exoplanets, and that resolution can be traded for photon-collecting power when the induced Doppler-shift is sufficiently large. We highlight CO as a good probe of UHJ thermal structure and dynamics that does not suffer from stellar activity, unlike species that are also present in the host star e.g. iron lines.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/stad1103</doi><tpages>26</tpages><orcidid>https://orcid.org/0000-0002-4125-0140</orcidid><oa>free_for_read</oa></addata></record> |
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title | Carbon monoxide emission lines reveal an inverted atmosphere in the ultra hot Jupiter WASP-33 b consistent with an eastward hot spot |
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