The Kepler-454 System: A Small, Not-rocky Inner Planet, a Jovian World, and a Distant Companion
Kepler-454 (KOI-273) is a relatively bright (V = 11.69 mag), Sun-like starthat hosts a transiting planet candidate in a 10.6 d orbit. From spectroscopy, we estimate the stellar temperature to be 5687 +/- 50 K, its metallicity to be [m/H] = 0.32 +/- 0.08, and the projected rotational velocity to be v...
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| creator | Gettel, Sara Charbonneau, David Dressing, Courtney D Buchhave, Lars A Dumusque, Xavier Vanderburg, Andrew Bonomo, Aldo S Malavolta, Luca Pepe, Francesco Andrew Collier Cameron Latham, David W Udry, Stephane Marcy, Geoffrey W Isaacson, Howard Howard, Andrew W Davies, Guy R Victor Silva Aguirre Kjeldsen, Hans Bedding, Timothy R Lopez, Eric Affer, Laura Cosentino, Rosario Figueira, Pedro Fiorenzano, Aldo F M Harutyunyan, Avet John Asher Johnson Lopez-Morales, Mercedes Lovis, Christophe Mayor, Michel Micela, Giusi Molinari, Emilio Motalebi, Fatemeh Phillips, David F Piotto, Giampaolo Queloz, Didier Rice, Ken Sasselov, Dimitar Segransan, Damien Sozzetti, Alessandro Watson, Chris Basu, Sarbani Campante, Tiago L Christensen-Dalsgaard, Jorgen Kawaler, Steven D Metcalfe, Travis S Handberg, Rasmus Lund, Mikkel N Lundkvist, Mia S Huber, Daniel Chaplin, William J |
| description | Kepler-454 (KOI-273) is a relatively bright (V = 11.69 mag), Sun-like starthat hosts a transiting planet candidate in a 10.6 d orbit. From spectroscopy, we estimate the stellar temperature to be 5687 +/- 50 K, its metallicity to be [m/H] = 0.32 +/- 0.08, and the projected rotational velocity to be v sin i 10 years and mass >12.1M_J . The twelve exoplanets with radii |
| doi_str_mv | 10.48550/arxiv.1511.09097 |
| format | Article |
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From spectroscopy, we estimate the stellar temperature to be 5687 +/- 50 K, its metallicity to be [m/H] = 0.32 +/- 0.08, and the projected rotational velocity to be v sin i <2.4 km s-1. We combine these values with a study of the asteroseismic frequencies from short cadence Kepler data to estimate the stellar mass to be 1.028+0:04-0:03 M_Sun, the radius to be 1.066 +/- 0.012 R_Sun and the age to be 5.25+1:41-1:39 Gyr. We estimate the radius of the 10.6 d planet as 2.37 +/- 0.13 R_Earth. Using 63 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 36 observations made with the HIRES spectrograph at Keck Observatory, we measure the mass of this planet to be 6.8 +/- 1.4M_Earth. We also detect two additional non-transiting companions, a planet with a minimum mass of 4.46 +/- 0.12 M_J in a nearly circular 524 d orbit and a massive companion with a period >10 years and mass >12.1M_J . The twelve exoplanets with radii <2.7 R_Earth and precise mass measurements appear to fall into two populations, with those <1.6 R_Earth following an Earth-like composition curve and larger planets requiring a significant fraction of volatiles. With a density of 2.76 +/- 0.73 g cm-3, Kepler-454b lies near the mass transition between these two populations and requires the presence of volatiles and/or H/He gas.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1511.09097</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Earth ; Extrasolar planets ; Metallicity ; Physics - Earth and Planetary Astrophysics ; Physics - Solar and Stellar Astrophysics ; Planetary composition ; Populations ; Radial velocity ; Rotation ; Spectrographs ; Stellar temperature ; Transit</subject><ispartof>arXiv.org, 2015-11</ispartof><rights>2015. 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/10.3847/0004-637X/816/2/95$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.1511.09097$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Gettel, Sara</creatorcontrib><creatorcontrib>Charbonneau, David</creatorcontrib><creatorcontrib>Dressing, Courtney D</creatorcontrib><creatorcontrib>Buchhave, Lars A</creatorcontrib><creatorcontrib>Dumusque, Xavier</creatorcontrib><creatorcontrib>Vanderburg, Andrew</creatorcontrib><creatorcontrib>Bonomo, Aldo S</creatorcontrib><creatorcontrib>Malavolta, Luca</creatorcontrib><creatorcontrib>Pepe, Francesco</creatorcontrib><creatorcontrib>Andrew Collier Cameron</creatorcontrib><creatorcontrib>Latham, David W</creatorcontrib><creatorcontrib>Udry, Stephane</creatorcontrib><creatorcontrib>Marcy, Geoffrey W</creatorcontrib><creatorcontrib>Isaacson, Howard</creatorcontrib><creatorcontrib>Howard, Andrew W</creatorcontrib><creatorcontrib>Davies, Guy R</creatorcontrib><creatorcontrib>Victor Silva Aguirre</creatorcontrib><creatorcontrib>Kjeldsen, Hans</creatorcontrib><creatorcontrib>Bedding, Timothy R</creatorcontrib><creatorcontrib>Lopez, Eric</creatorcontrib><creatorcontrib>Affer, Laura</creatorcontrib><creatorcontrib>Cosentino, Rosario</creatorcontrib><creatorcontrib>Figueira, Pedro</creatorcontrib><creatorcontrib>Fiorenzano, Aldo F M</creatorcontrib><creatorcontrib>Harutyunyan, Avet</creatorcontrib><creatorcontrib>John Asher Johnson</creatorcontrib><creatorcontrib>Lopez-Morales, Mercedes</creatorcontrib><creatorcontrib>Lovis, Christophe</creatorcontrib><creatorcontrib>Mayor, Michel</creatorcontrib><creatorcontrib>Micela, Giusi</creatorcontrib><creatorcontrib>Molinari, Emilio</creatorcontrib><creatorcontrib>Motalebi, Fatemeh</creatorcontrib><creatorcontrib>Phillips, David F</creatorcontrib><creatorcontrib>Piotto, Giampaolo</creatorcontrib><creatorcontrib>Queloz, Didier</creatorcontrib><creatorcontrib>Rice, Ken</creatorcontrib><creatorcontrib>Sasselov, Dimitar</creatorcontrib><creatorcontrib>Segransan, Damien</creatorcontrib><creatorcontrib>Sozzetti, Alessandro</creatorcontrib><creatorcontrib>Watson, Chris</creatorcontrib><creatorcontrib>Basu, Sarbani</creatorcontrib><creatorcontrib>Campante, Tiago L</creatorcontrib><creatorcontrib>Christensen-Dalsgaard, Jorgen</creatorcontrib><creatorcontrib>Kawaler, Steven D</creatorcontrib><creatorcontrib>Metcalfe, Travis S</creatorcontrib><creatorcontrib>Handberg, Rasmus</creatorcontrib><creatorcontrib>Lund, Mikkel N</creatorcontrib><creatorcontrib>Lundkvist, Mia S</creatorcontrib><creatorcontrib>Huber, Daniel</creatorcontrib><creatorcontrib>Chaplin, William J</creatorcontrib><title>The Kepler-454 System: A Small, Not-rocky Inner Planet, a Jovian World, and a Distant Companion</title><title>arXiv.org</title><description>Kepler-454 (KOI-273) is a relatively bright (V = 11.69 mag), Sun-like starthat hosts a transiting planet candidate in a 10.6 d orbit. From spectroscopy, we estimate the stellar temperature to be 5687 +/- 50 K, its metallicity to be [m/H] = 0.32 +/- 0.08, and the projected rotational velocity to be v sin i <2.4 km s-1. We combine these values with a study of the asteroseismic frequencies from short cadence Kepler data to estimate the stellar mass to be 1.028+0:04-0:03 M_Sun, the radius to be 1.066 +/- 0.012 R_Sun and the age to be 5.25+1:41-1:39 Gyr. We estimate the radius of the 10.6 d planet as 2.37 +/- 0.13 R_Earth. Using 63 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 36 observations made with the HIRES spectrograph at Keck Observatory, we measure the mass of this planet to be 6.8 +/- 1.4M_Earth. We also detect two additional non-transiting companions, a planet with a minimum mass of 4.46 +/- 0.12 M_J in a nearly circular 524 d orbit and a massive companion with a period >10 years and mass >12.1M_J . The twelve exoplanets with radii <2.7 R_Earth and precise mass measurements appear to fall into two populations, with those <1.6 R_Earth following an Earth-like composition curve and larger planets requiring a significant fraction of volatiles. With a density of 2.76 +/- 0.73 g cm-3, Kepler-454b lies near the mass transition between these two populations and requires the presence of volatiles and/or H/He gas.</description><subject>Earth</subject><subject>Extrasolar planets</subject><subject>Metallicity</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Planetary composition</subject><subject>Populations</subject><subject>Radial velocity</subject><subject>Rotation</subject><subject>Spectrographs</subject><subject>Stellar 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Kepler-454 System: A Small, Not-rocky Inner Planet, a Jovian World, and a Distant Companion</title><author>Gettel, Sara ; Charbonneau, David ; Dressing, Courtney D ; Buchhave, Lars A ; Dumusque, Xavier ; Vanderburg, Andrew ; Bonomo, Aldo S ; Malavolta, Luca ; Pepe, Francesco ; Andrew Collier Cameron ; Latham, David W ; Udry, Stephane ; Marcy, Geoffrey W ; Isaacson, Howard ; Howard, Andrew W ; Davies, Guy R ; Victor Silva Aguirre ; Kjeldsen, Hans ; Bedding, Timothy R ; Lopez, Eric ; Affer, Laura ; Cosentino, Rosario ; Figueira, Pedro ; Fiorenzano, Aldo F M ; Harutyunyan, Avet ; John Asher Johnson ; Lopez-Morales, Mercedes ; Lovis, Christophe ; Mayor, Michel ; Micela, Giusi ; Molinari, Emilio ; Motalebi, Fatemeh ; Phillips, David F ; Piotto, Giampaolo ; Queloz, Didier ; Rice, Ken ; Sasselov, Dimitar ; Segransan, Damien ; Sozzetti, Alessandro ; Watson, Chris ; Basu, Sarbani ; Campante, Tiago L ; Christensen-Dalsgaard, Jorgen ; Kawaler, Steven D ; Metcalfe, Travis S ; Handberg, Rasmus ; 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Companion</atitle><jtitle>arXiv.org</jtitle><date>2015-11-29</date><risdate>2015</risdate><eissn>2331-8422</eissn><abstract>Kepler-454 (KOI-273) is a relatively bright (V = 11.69 mag), Sun-like starthat hosts a transiting planet candidate in a 10.6 d orbit. From spectroscopy, we estimate the stellar temperature to be 5687 +/- 50 K, its metallicity to be [m/H] = 0.32 +/- 0.08, and the projected rotational velocity to be v sin i <2.4 km s-1. We combine these values with a study of the asteroseismic frequencies from short cadence Kepler data to estimate the stellar mass to be 1.028+0:04-0:03 M_Sun, the radius to be 1.066 +/- 0.012 R_Sun and the age to be 5.25+1:41-1:39 Gyr. We estimate the radius of the 10.6 d planet as 2.37 +/- 0.13 R_Earth. Using 63 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 36 observations made with the HIRES spectrograph at Keck Observatory, we measure the mass of this planet to be 6.8 +/- 1.4M_Earth. We also detect two additional non-transiting companions, a planet with a minimum mass of 4.46 +/- 0.12 M_J in a nearly circular 524 d orbit and a massive companion with a period >10 years and mass >12.1M_J . The twelve exoplanets with radii <2.7 R_Earth and precise mass measurements appear to fall into two populations, with those <1.6 R_Earth following an Earth-like composition curve and larger planets requiring a significant fraction of volatiles. With a density of 2.76 +/- 0.73 g cm-3, Kepler-454b lies near the mass transition between these two populations and requires the presence of volatiles and/or H/He gas.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1511.09097</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2015-11 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_1511_09097 |
| source | arXiv.org; Free E- Journals |
| subjects | Earth Extrasolar planets Metallicity Physics - Earth and Planetary Astrophysics Physics - Solar and Stellar Astrophysics Planetary composition Populations Radial velocity Rotation Spectrographs Stellar temperature Transit |
| title | The Kepler-454 System: A Small, Not-rocky Inner Planet, a Jovian World, and a Distant Companion |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-30T00%3A29%3A17IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_arxiv&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=The%20Kepler-454%20System:%20A%20Small,%20Not-rocky%20Inner%20Planet,%20a%20Jovian%20World,%20and%20a%20Distant%20Companion&rft.jtitle=arXiv.org&rft.au=Gettel,%20Sara&rft.date=2015-11-29&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.1511.09097&rft_dat=%3Cproquest_arxiv%3E2077980576%3C/proquest_arxiv%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2077980576&rft_id=info:pmid/&rfr_iscdi=true |