KELT-18b: Puffy Planet, Hot Host, Probably Perturbed
We report the discovery of KELT-18b, a transiting hot Jupiter in a 2.87d orbit around the bright (V=10.1), hot, F4V star BD+60 1538 (TYC 3865-1173-1). We present follow-up photometry, spectroscopy, and adaptive optics imaging that allow a detailed characterization of the system. Our preferred model...
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| creator | McLeod, Kim K Rodriguez, Joseph E Oelkers, Ryan J Collins, Karen A Bieryla, Allyson Fulton, Benjamin J Stassun, Keivan G Gaudi, B Scott Penev, Kaloyan Stevens, Daniel J Colón, Knicole D Pepper, Joshua Narita, Norio Ryu Tsuguru Fukui, Akihiko Reed, Phillip A Tirrell, Bethany Visgaitis, Tiffany Kielkopf, John F Cohen, David H Jensen, Eric L N Gregorio, Joao Baştürk, Özgür Oberst, Thomas E Melton, Casey Kempton, Eliza M -R Baldridge, Andrew Zhao, Y Sunny Zambelli, Roberto Latham, David W Esquerdo, Gilbert A Berlind, Perry Calkins, Michael L Howard, Andrew W Isaacson, Howard Weiss, Lauren M Beatty, Thomas G Eastman, Jason D Penny, Matthew T Siverd, Robert J Lund, Michael B Labadie-Bartz, Jonathan Zhou, G Curtis, Ivan A Joner, Michael D Manner, Mark Relles, Howard Scarpetta, Gaetano Stephens, Denise C Stockdale, Chris Tan, T G DePoy, D L Marshall, Jennifer L Pogge, Richard W Trueblood, Mark Trueblood, Patricia |
| description | We report the discovery of KELT-18b, a transiting hot Jupiter in a 2.87d orbit around the bright (V=10.1), hot, F4V star BD+60 1538 (TYC 3865-1173-1). We present follow-up photometry, spectroscopy, and adaptive optics imaging that allow a detailed characterization of the system. Our preferred model fits yield a host stellar temperature of 6670+/-120 K and a mass of 1.524+/-0.069 Msun, situating it as one of only a handful of known transiting planets with hosts that are as hot, massive, and bright. The planet has a mass of 1.18+/-0.11 Mjup, a radius of 1.57+/-0.04 Rjup, and a density of 0.377+/-0.040 g/cm^3, making it one of the most inflated planets known around a hot star. We argue that KELT-18b's high temperature and low surface gravity, which yield an estimated ~600 km atmospheric scale height, combined with its hot, bright host make it an excellent candidate for observations aimed at atmospheric characterization. We also present evidence for a bound stellar companion at a projected separation of ~1100 AU, and speculate that it may have contributed to the strong misalignment we suspect between KELT-18's spin axis and its planet's orbital axis. The inferior conjunction time is 2457542.524998 +/-0.000416 (BJD_TDB) and the orbital period is 2.8717510 +/- 0.0000029 days. We encourage Rossiter-McLaughlin measurements in the near future to confirm the suspected spin-orbit misalignment of this system. |
| doi_str_mv | 10.48550/arxiv.1702.01657 |
| format | Article |
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We present follow-up photometry, spectroscopy, and adaptive optics imaging that allow a detailed characterization of the system. Our preferred model fits yield a host stellar temperature of 6670+/-120 K and a mass of 1.524+/-0.069 Msun, situating it as one of only a handful of known transiting planets with hosts that are as hot, massive, and bright. The planet has a mass of 1.18+/-0.11 Mjup, a radius of 1.57+/-0.04 Rjup, and a density of 0.377+/-0.040 g/cm^3, making it one of the most inflated planets known around a hot star. We argue that KELT-18b's high temperature and low surface gravity, which yield an estimated ~600 km atmospheric scale height, combined with its hot, bright host make it an excellent candidate for observations aimed at atmospheric characterization. We also present evidence for a bound stellar companion at a projected separation of ~1100 AU, and speculate that it may have contributed to the strong misalignment we suspect between KELT-18's spin axis and its planet's orbital axis. The inferior conjunction time is 2457542.524998 +/-0.000416 (BJD_TDB) and the orbital period is 2.8717510 +/- 0.0000029 days. We encourage Rossiter-McLaughlin measurements in the near future to confirm the suspected spin-orbit misalignment of this system.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1702.01657</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Adaptive optics ; Adaptive systems ; Extrasolar planets ; Gas giant planets ; High temperature ; Hot stars ; Misalignment ; Orbits ; Photometry ; Physics - Earth and Planetary Astrophysics ; Scale height ; Stellar temperature ; Transit</subject><ispartof>arXiv.org, 2017-04</ispartof><rights>2017. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27902</link.rule.ids><backlink>$$Uhttps://doi.org/10.3847/1538-3881/aa6d5d$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.1702.01657$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>McLeod, Kim K</creatorcontrib><creatorcontrib>Rodriguez, Joseph E</creatorcontrib><creatorcontrib>Oelkers, Ryan J</creatorcontrib><creatorcontrib>Collins, Karen A</creatorcontrib><creatorcontrib>Bieryla, Allyson</creatorcontrib><creatorcontrib>Fulton, Benjamin J</creatorcontrib><creatorcontrib>Stassun, Keivan G</creatorcontrib><creatorcontrib>Gaudi, B Scott</creatorcontrib><creatorcontrib>Penev, Kaloyan</creatorcontrib><creatorcontrib>Stevens, Daniel J</creatorcontrib><creatorcontrib>Colón, Knicole D</creatorcontrib><creatorcontrib>Pepper, Joshua</creatorcontrib><creatorcontrib>Narita, Norio</creatorcontrib><creatorcontrib>Ryu Tsuguru</creatorcontrib><creatorcontrib>Fukui, Akihiko</creatorcontrib><creatorcontrib>Reed, Phillip A</creatorcontrib><creatorcontrib>Tirrell, Bethany</creatorcontrib><creatorcontrib>Visgaitis, Tiffany</creatorcontrib><creatorcontrib>Kielkopf, John F</creatorcontrib><creatorcontrib>Cohen, David H</creatorcontrib><creatorcontrib>Jensen, Eric L N</creatorcontrib><creatorcontrib>Gregorio, Joao</creatorcontrib><creatorcontrib>Baştürk, Özgür</creatorcontrib><creatorcontrib>Oberst, Thomas E</creatorcontrib><creatorcontrib>Melton, Casey</creatorcontrib><creatorcontrib>Kempton, Eliza M -R</creatorcontrib><creatorcontrib>Baldridge, Andrew</creatorcontrib><creatorcontrib>Zhao, Y Sunny</creatorcontrib><creatorcontrib>Zambelli, Roberto</creatorcontrib><creatorcontrib>Latham, David W</creatorcontrib><creatorcontrib>Esquerdo, Gilbert A</creatorcontrib><creatorcontrib>Berlind, Perry</creatorcontrib><creatorcontrib>Calkins, Michael L</creatorcontrib><creatorcontrib>Howard, Andrew W</creatorcontrib><creatorcontrib>Isaacson, Howard</creatorcontrib><creatorcontrib>Weiss, Lauren M</creatorcontrib><creatorcontrib>Beatty, Thomas G</creatorcontrib><creatorcontrib>Eastman, Jason D</creatorcontrib><creatorcontrib>Penny, Matthew T</creatorcontrib><creatorcontrib>Siverd, Robert J</creatorcontrib><creatorcontrib>Lund, Michael B</creatorcontrib><creatorcontrib>Labadie-Bartz, Jonathan</creatorcontrib><creatorcontrib>Zhou, G</creatorcontrib><creatorcontrib>Curtis, Ivan A</creatorcontrib><creatorcontrib>Joner, Michael D</creatorcontrib><creatorcontrib>Manner, Mark</creatorcontrib><creatorcontrib>Relles, Howard</creatorcontrib><creatorcontrib>Scarpetta, Gaetano</creatorcontrib><creatorcontrib>Stephens, Denise C</creatorcontrib><creatorcontrib>Stockdale, Chris</creatorcontrib><creatorcontrib>Tan, T G</creatorcontrib><creatorcontrib>DePoy, D L</creatorcontrib><creatorcontrib>Marshall, Jennifer L</creatorcontrib><creatorcontrib>Pogge, Richard W</creatorcontrib><creatorcontrib>Trueblood, Mark</creatorcontrib><creatorcontrib>Trueblood, Patricia</creatorcontrib><title>KELT-18b: Puffy Planet, Hot Host, Probably Perturbed</title><title>arXiv.org</title><description>We report the discovery of KELT-18b, a transiting hot Jupiter in a 2.87d orbit around the bright (V=10.1), hot, F4V star BD+60 1538 (TYC 3865-1173-1). We present follow-up photometry, spectroscopy, and adaptive optics imaging that allow a detailed characterization of the system. Our preferred model fits yield a host stellar temperature of 6670+/-120 K and a mass of 1.524+/-0.069 Msun, situating it as one of only a handful of known transiting planets with hosts that are as hot, massive, and bright. The planet has a mass of 1.18+/-0.11 Mjup, a radius of 1.57+/-0.04 Rjup, and a density of 0.377+/-0.040 g/cm^3, making it one of the most inflated planets known around a hot star. We argue that KELT-18b's high temperature and low surface gravity, which yield an estimated ~600 km atmospheric scale height, combined with its hot, bright host make it an excellent candidate for observations aimed at atmospheric characterization. We also present evidence for a bound stellar companion at a projected separation of ~1100 AU, and speculate that it may have contributed to the strong misalignment we suspect between KELT-18's spin axis and its planet's orbital axis. The inferior conjunction time is 2457542.524998 +/-0.000416 (BJD_TDB) and the orbital period is 2.8717510 +/- 0.0000029 days. We encourage Rossiter-McLaughlin measurements in the near future to confirm the suspected spin-orbit misalignment of this system.</description><subject>Adaptive optics</subject><subject>Adaptive systems</subject><subject>Extrasolar planets</subject><subject>Gas giant planets</subject><subject>High temperature</subject><subject>Hot stars</subject><subject>Misalignment</subject><subject>Orbits</subject><subject>Photometry</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Scale height</subject><subject>Stellar 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Gregorio, Joao ; Baştürk, Özgür ; Oberst, Thomas E ; Melton, Casey ; Kempton, Eliza M -R ; Baldridge, Andrew ; Zhao, Y Sunny ; Zambelli, Roberto ; Latham, David W ; Esquerdo, Gilbert A ; Berlind, Perry ; Calkins, Michael L ; Howard, Andrew W ; Isaacson, Howard ; Weiss, Lauren M ; Beatty, Thomas G ; Eastman, Jason D ; Penny, Matthew T ; Siverd, Robert J ; Lund, Michael B ; Labadie-Bartz, Jonathan ; Zhou, G ; Curtis, Ivan A ; Joner, Michael D ; Manner, Mark ; Relles, Howard ; Scarpetta, Gaetano ; Stephens, Denise C ; Stockdale, Chris ; Tan, T G ; DePoy, D L ; Marshall, Jennifer L ; Pogge, Richard W ; Trueblood, Mark ; Trueblood, Patricia</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a522-b0ecfb9faca2218691808c77efc33792b94dd5db436a92faa03e78980f54f0bd3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2017</creationdate><topic>Adaptive optics</topic><topic>Adaptive systems</topic><topic>Extrasolar 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Bethany</au><au>Visgaitis, Tiffany</au><au>Kielkopf, John F</au><au>Cohen, David H</au><au>Jensen, Eric L N</au><au>Gregorio, Joao</au><au>Baştürk, Özgür</au><au>Oberst, Thomas E</au><au>Melton, Casey</au><au>Kempton, Eliza M -R</au><au>Baldridge, Andrew</au><au>Zhao, Y Sunny</au><au>Zambelli, Roberto</au><au>Latham, David W</au><au>Esquerdo, Gilbert A</au><au>Berlind, Perry</au><au>Calkins, Michael L</au><au>Howard, Andrew W</au><au>Isaacson, Howard</au><au>Weiss, Lauren M</au><au>Beatty, Thomas G</au><au>Eastman, Jason D</au><au>Penny, Matthew T</au><au>Siverd, Robert J</au><au>Lund, Michael B</au><au>Labadie-Bartz, Jonathan</au><au>Zhou, G</au><au>Curtis, Ivan A</au><au>Joner, Michael D</au><au>Manner, Mark</au><au>Relles, Howard</au><au>Scarpetta, Gaetano</au><au>Stephens, Denise C</au><au>Stockdale, Chris</au><au>Tan, T G</au><au>DePoy, D L</au><au>Marshall, Jennifer L</au><au>Pogge, Richard W</au><au>Trueblood, Mark</au><au>Trueblood, Patricia</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>KELT-18b: Puffy Planet, Hot Host, Probably Perturbed</atitle><jtitle>arXiv.org</jtitle><date>2017-04-10</date><risdate>2017</risdate><eissn>2331-8422</eissn><abstract>We report the discovery of KELT-18b, a transiting hot Jupiter in a 2.87d orbit around the bright (V=10.1), hot, F4V star BD+60 1538 (TYC 3865-1173-1). We present follow-up photometry, spectroscopy, and adaptive optics imaging that allow a detailed characterization of the system. Our preferred model fits yield a host stellar temperature of 6670+/-120 K and a mass of 1.524+/-0.069 Msun, situating it as one of only a handful of known transiting planets with hosts that are as hot, massive, and bright. The planet has a mass of 1.18+/-0.11 Mjup, a radius of 1.57+/-0.04 Rjup, and a density of 0.377+/-0.040 g/cm^3, making it one of the most inflated planets known around a hot star. We argue that KELT-18b's high temperature and low surface gravity, which yield an estimated ~600 km atmospheric scale height, combined with its hot, bright host make it an excellent candidate for observations aimed at atmospheric characterization. We also present evidence for a bound stellar companion at a projected separation of ~1100 AU, and speculate that it may have contributed to the strong misalignment we suspect between KELT-18's spin axis and its planet's orbital axis. The inferior conjunction time is 2457542.524998 +/-0.000416 (BJD_TDB) and the orbital period is 2.8717510 +/- 0.0000029 days. We encourage Rossiter-McLaughlin measurements in the near future to confirm the suspected spin-orbit misalignment of this system.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1702.01657</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2017-04 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_1702_01657 |
| source | arXiv.org; Free E- Journals |
| subjects | Adaptive optics Adaptive systems Extrasolar planets Gas giant planets High temperature Hot stars Misalignment Orbits Photometry Physics - Earth and Planetary Astrophysics Scale height Stellar temperature Transit |
| title | KELT-18b: Puffy Planet, Hot Host, Probably Perturbed |
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