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A compact system of small planets around a former red-giant star | Nature

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They have the shortest orbital periods so far reported, at about 5.8 and 8.2 hours, and are only 0.006 and 0.0076 astronomical units (AU) away from their parent star. Planets orbiting within 1 AU of a parent star are expected to be engulfed when the star becomes a red giant, so these bodies have probably survived immersion in the former red giant envelope. Planets that orbit their parent star at less than about one astronomical unit (1 au is the Earth–Sun distance) are expected to be engulfed when the star becomes a red giant1. Previous observations have revealed the existence of post-red-giant host stars with giant planets2,3,4 orbiting as close as 0.116 au or with brown dwarf companions5,6 in tight orbits, showing that these bodies can survive engulfment. What has remained unclear is whether planets can be dragged deeper into the red-giant envelope without being disrupted and whether the evolution of the parent star itself could be affected7,8,9. Here we report the presence of two nearly Earth-sized bodies orbiting the post-red-giant, hot B subdwarf star KIC 05807616 at distances of 0.0060 and 0.0076 au, with orbital periods of 5.7625 and 8.2293 hours, respectively. These bodies probably survived deep immersion in the former red-giant envelope. They may be the dense cores of evaporated giant planets that were transported closer to the star during the engulfment and triggered the mass loss necessary for the formation of the hot B subdwarf, which might also explain how some stars of this type did not form in binary systems.","datePublished":"2011-12-21T00:00:00Z","dateModified":"2011-12-21T00:00:00Z","pageStart":"496","pageEnd":"499","sameAs":"https://doi.org/10.1038/nature10631","keywords":["Planetary science","Science","Humanities and Social Sciences","multidisciplinary"],"image":["https://media.springernature.com/lw1200/springer-static/image/art%3A10.1038%2Fnature10631/MediaObjects/41586_2011_Article_BFnature10631_Fig1_HTML.jpg","https://media.springernature.com/lw1200/springer-static/image/art%3A10.1038%2Fnature10631/MediaObjects/41586_2011_Article_BFnature10631_Fig2_HTML.jpg"],"isPartOf":{"name":"Nature","issn":["1476-4687","0028-0836"],"volumeNumber":"480","@type":["Periodical","PublicationVolume"]},"publisher":{"name":"Nature Publishing Group UK","logo":{"url":"https://www.springernature.com/app-sn/public/images/logo-springernature.png","@type":"ImageObject"},"@type":"Organization"},"author":[{"name":"S. 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They have the shortest orbital periods so far reported, at about 5.8 and 8.2 hours, and are only 0.006 and 0.0076 astronomical units (AU) away from their parent star. Planets orbiting within 1 AU of a parent star are expected to be engulfed when the star becomes a red giant, so these bodies have probably survived immersion in the former red giant envelope. Planets that orbit their parent star at less than about one astronomical unit (1&#8201;au is the Earth&#8211;Sun distance) are expected to be engulfed when the star becomes a red giant1. Previous observations have revealed the existence of post-red-giant host stars with giant planets2,3,4 orbiting as close as 0.116&#8201;au or with brown dwarf companions5,6 in tight orbits, showing that these bodies can survive engulfment. What has remained unclear is whether planets can be dragged deeper into the red-giant envelope without being disrupted and whether the evolution of the parent star itself could be affected7,8,9. Here we report the presence of two nearly Earth-sized bodies orbiting the post-red-giant, hot B subdwarf star KIC 05807616 at distances of 0.0060 and 0.0076&#8201;au, with orbital periods of 5.7625 and 8.2293 hours, respectively. These bodies probably survived deep immersion in the former red-giant envelope. 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They have the shortest orbital periods so far reported, at about 5.8 and 8.2 hours, and are only 0.006 and 0.0076 astronomical units (AU) away from their parent star. Planets orbiting within 1 AU of a parent star are expected to be engulfed when the star becomes a red giant, so these bodies have probably survived immersion in the former red giant envelope. Planets that orbit their parent star at less than about one astronomical unit (1&#8201;au is the Earth&#8211;Sun distance) are expected to be engulfed when the star becomes a red giant1. Previous observations have revealed the existence of post-red-giant host stars with giant planets2,3,4 orbiting as close as 0.116&#8201;au or with brown dwarf companions5,6 in tight orbits, showing that these bodies can survive engulfment. What has remained unclear is whether planets can be dragged deeper into the red-giant envelope without being disrupted and whether the evolution of the parent star itself could be affected7,8,9. 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S."/> <meta name="citation_author_institution" content="Mt Suhora Observatory, Cracow Pedagogical University, ulica Podchorazych 2, 30-084 Krakow, Poland, "/> <meta name="citation_author_institution" content="Department of Physics and Astronomy, Iowa State University, 12 Physics Hall, Ames, USA"/> <meta name="citation_author" content="&#216;stensen, R. H."/> <meta name="citation_author_institution" content="Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium, "/> <meta name="citation_author" content="Kawaler, S. D."/> <meta name="citation_author_institution" content="Department of Physics and Astronomy, Iowa State University, 12 Physics Hall, Ames, USA"/> <meta name="citation_author" content="Telting, J. H."/> <meta name="citation_author_institution" content="Nordic Optical Telescope, Apartado 474, 38700 Santa Cruz de La Palma, Spain, "/> <meta name="access_endpoint" content="https://www.nature.com/platform/readcube-access"/> <meta name="twitter:site" content="@nature"/> <meta name="twitter:card" content="summary_large_image"/> <meta name="twitter:image:alt" content="Content cover image"/> <meta name="twitter:title" content="A compact system of small planets around a former red-giant star"/> <meta name="twitter:description" content="Nature - Two small planets of nearly Earth size have been discovered orbiting the evolved post-red-giant star KIC 05807616. They have the shortest orbital periods so far reported, at about 5.8 and..."/> <meta name="twitter:image" content="https://media.springernature.com/full/springer-static/image/art%3A10.1038%2Fnature10631/MediaObjects/41586_2011_Article_BFnature10631_Fig1_HTML.jpg"/> <meta property="og:url" content="https://www.nature.com/articles/nature10631"/> <meta property="og:type" content="article"/> <meta property="og:site_name" content="Nature"/> <meta property="og:title" content="A compact system of small planets around a former red-giant star - Nature"/> <meta property="og:description" content="Two planets around the post-red-giant star KIC 05807616 are shown to have survived being engulfed by the former red giant"/> <meta property="og:image" content="https://media.springernature.com/m685/springer-static/image/art%3A10.1038%2Fnature10631/MediaObjects/41586_2011_Article_BFnature10631_Fig1_HTML.jpg"/> <script> window.eligibleForRa21 = 'true'; </script> </head> <body class="article-page"> <noscript><iframe src="https://www.googletagmanager.com/ns.html?id=GTM-MRVXSHQ" height="0" width="0" style="display:none;visibility:hidden"></iframe></noscript> <div class="position-relative cleared z-index-50 background-white" data-test="top-containers"> <a class="c-skip-link" href="#content">Skip to main content</a> <div class="c-grade-c-banner u-hide"> <div class="c-grade-c-banner__container"> <p>Thank you for visiting nature.com. 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data-test="article-identifier"> <li class="c-article-identifiers__item" data-test="article-category">Letter</li> <li class="c-article-identifiers__item">Published: <time datetime="2011-12-21">21 December 2011</time></li> </ul> <h1 class="c-article-title" data-test="article-title" data-article-title="">A compact system of small planets around a former red-giant star</h1> <ul class="c-article-author-list c-article-author-list--short" data-test="authors-list" data-component-authors-activator="authors-list"><li class="c-article-author-list__item"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-S_-Charpinet-Aff1-Aff2" data-author-popup="auth-S_-Charpinet-Aff1-Aff2" data-author-search="Charpinet, S." data-corresp-id="c1">S. 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Silvotti</a><sup class="u-js-hide"><a href="#Aff8">8</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-A__S_-Baran-Aff9-Aff10" data-author-popup="auth-A__S_-Baran-Aff9-Aff10" data-author-search="Baran, A. S.">A. S. Baran</a><sup class="u-js-hide"><a href="#Aff9">9</a>,<a href="#Aff10">10</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-R__H_-_stensen-Aff11" data-author-popup="auth-R__H_-_stensen-Aff11" data-author-search="Østensen, R. H.">R. H. Østensen</a><sup class="u-js-hide"><a href="#Aff11">11</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-S__D_-Kawaler-Aff10" data-author-popup="auth-S__D_-Kawaler-Aff10" data-author-search="Kawaler, S. D.">S. D. Kawaler</a><sup class="u-js-hide"><a href="#Aff10">10</a></sup> &amp; </li><li class="c-article-author-list__show-more" aria-label="Show all 11 authors for this article" title="Show all 11 authors for this article">…</li><li class="c-article-author-list__item"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-J__H_-Telting-Aff12" data-author-popup="auth-J__H_-Telting-Aff12" data-author-search="Telting, J. H.">J. H. Telting</a><sup class="u-js-hide"><a href="#Aff12">12</a></sup> </li></ul><button aria-expanded="false" class="c-article-author-list__button"><svg width="16" height="16" focusable="false" role="img" aria-hidden="true" class="u-icon"><use xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="#icon-eds-i-chevron-down-medium"></use></svg><span>Show authors</span></button> <p class="c-article-info-details" data-container-section="info"> <a data-test="journal-link" href="/" data-track="click" data-track-action="journal homepage" data-track-category="article body" data-track-label="link"><i data-test="journal-title">Nature</i></a> <b data-test="journal-volume"><span class="u-visually-hidden">volume</span> 480</b>, <span class="u-visually-hidden">pages </span>496–499 (<span data-test="article-publication-year">2011</span>)<a href="#citeas" class="c-article-info-details__cite-as u-hide-print" data-track="click" data-track-action="cite this article" data-track-label="link">Cite this article</a> </p> <div class="c-article-metrics-bar__wrapper u-clear-both"> <ul class="c-article-metrics-bar u-list-reset"> <li class=" c-article-metrics-bar__item" data-test="access-count"> <p class="c-article-metrics-bar__count">6385 <span class="c-article-metrics-bar__label">Accesses</span></p> </li> <li class="c-article-metrics-bar__item" data-test="citation-count"> <p class="c-article-metrics-bar__count">134 <span class="c-article-metrics-bar__label">Citations</span></p> </li> <li class="c-article-metrics-bar__item" data-test="altmetric-score"> <p class="c-article-metrics-bar__count">122 <span class="c-article-metrics-bar__label">Altmetric</span></p> </li> <li class="c-article-metrics-bar__item"> <p class="c-article-metrics-bar__details"><a href="/articles/nature10631/metrics" data-track="click" data-track-action="view metrics" data-track-label="link" rel="nofollow">Metrics <span class="u-visually-hidden">details</span></a></p> </li> </ul> </div> </header> <div class="u-js-hide" data-component="article-subject-links"> <h3 class="c-article__sub-heading">Subjects</h3> <ul class="c-article-subject-list"> <li class="c-article-subject-list__subject"><a href="/subjects/planetary-science" data-track="click" data-track-action="view subject" data-track-label="link">Planetary science</a></li> </ul> </div> </div> <div class="c-article-body"> <section aria-labelledby="Abs3" data-title="Abstract" lang="en"><div class="c-article-section" id="Abs3-section"><h2 class="c-article-section__title js-section-title js-c-reading-companion-sections-item" id="Abs3">Abstract</h2><div class="c-article-section__content" id="Abs3-content"><p>Planets that orbit their parent star at less than about one astronomical unit (1 <span class="u-small-caps">au</span> is the Earth–Sun distance) are expected to be engulfed when the star becomes a red giant<sup><a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 1" title="Udry, S. &amp; Santos, N. C. Statistical properties of exoplanets. Annu. Rev. Astron. Astrophys. 45, 397–439 (2007)" href="/articles/nature10631#ref-CR1" id="ref-link-section-d99993321e567">1</a></sup>. Previous observations have revealed the existence of post-red-giant host stars with giant planets<sup><a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 2" title="Setiawan, J. et al. A giant planet around a metal-poor star of extragalactic origin. Science 330, 1642–1644 (2010)" href="/articles/nature10631#ref-CR2" id="ref-link-section-d99993321e571">2</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 3" title="Silvotti, R. et al. A giant planet orbiting the ‘extreme horizontal branch’ star V391 Pegasi. Nature 449, 189–191 (2007)" href="/articles/nature10631#ref-CR3" id="ref-link-section-d99993321e574">3</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 4" title="Lee, J. W. et al. The sdB+M eclipsing system HW Virginis and its circumbinary planets. Astron. J. 137, 3181–3190 (2009)" href="/articles/nature10631#ref-CR4" id="ref-link-section-d99993321e577">4</a></sup> orbiting as close as 0.116 <span class="u-small-caps">au</span> or with brown dwarf companions<sup><a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 5" title="Maxted, P. F. L., Napiwotzki, R., Dobbie, P. D. &amp; Burleigh, M. R. Survival of a brown dwarf after engulfment by a red giant star. Nature 442, 543–545 (2006)" href="/articles/nature10631#ref-CR5" id="ref-link-section-d99993321e584">5</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 6" title="Geier, S. et al. Binaries discovered by the MUCHFUSS project: SDSS J08205+0008 — an eclipsing subdwarf B binary with a brown dwarf companion. Astrophys. J. 731, L22–L26 (2011)" href="/articles/nature10631#ref-CR6" id="ref-link-section-d99993321e587">6</a></sup> in tight orbits, showing that these bodies can survive engulfment. What has remained unclear is whether planets can be dragged deeper into the red-giant envelope without being disrupted and whether the evolution of the parent star itself could be affected<sup><a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 7" title="D'Cruz, N. L., Dorman, B., Rood, R. T. &amp; O'Connell, R. W. The origin of extreme horizontal branch stars. Astrophys. J. 466, 359–371 (1996)" href="/articles/nature10631#ref-CR7" id="ref-link-section-d99993321e592">7</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 8" title="Heber, U. Hot subdwarf stars. Annu. Rev. Astron. Astrophys. 47, 211–251 (2009)" href="/articles/nature10631#ref-CR8" id="ref-link-section-d99993321e595">8</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 9" title="Soker, N. Can planets influence the horizontal branch morphology? Astron. J. 116, 1308–1313 (1998)" href="/articles/nature10631#ref-CR9" id="ref-link-section-d99993321e598">9</a></sup>. Here we report the presence of two nearly Earth-sized bodies orbiting the post-red-giant, hot B subdwarf star KIC 05807616 at distances of 0.0060 and 0.0076 <span class="u-small-caps">au</span>, with orbital periods of 5.7625 and 8.2293 hours, respectively. These bodies probably survived deep immersion in the former red-giant envelope. They may be the dense cores of evaporated giant planets that were transported closer to the star during the engulfment and triggered the mass loss necessary for the formation of the hot B subdwarf, which might also explain how some stars of this type did not form in binary systems.</p></div></div></section> <noscript> <div class="c-nature-box c-nature-box--side " data-component="entitlement-box"> <div class="js-access-button"> <a href="https://wayf.springernature.com?redirect_uri&#x3D;https%3A%2F%2Fwww.nature.com%2Farticles%2Fnature10631" class="c-article__button" data-test="ra21"> <svg class="u-icon" width="18" height="18" aria-hidden="true" focusable="false"><use href="#icon-institution"></use></svg> <span class="c-article__button-text">Access through your institution</span> </a> </div> <div class="js-buy-button"> <a href="#access-options" class="c-article__button c-article__button--inverted" data-test="ra21"> <span>Buy or subscribe</span> </a> </div> </div> </noscript> <div 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G.F. acknowledges the support of the NSERC of Canada and the contribution of the Canada Research Chair Program. MMT spectra for KIC 05807616 were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. A.S.B. acknowledges funding from the Polish Ministry of Science and Higher Education. S.C. thanks R. Gilliland for help in managing Kepler's procedures. We acknowledge the Kepler team and all who have contributed to making this mission possible. Funding for the Kepler mission is provided by NASA’s Science Mission Directorate.</p></div></div></section><section aria-labelledby="author-information" data-title="Author information"><div class="c-article-section" id="author-information-section"><h2 class="c-article-section__title js-section-title js-c-reading-companion-sections-item" id="author-information">Author information</h2><div class="c-article-section__content" id="author-information-content"><h3 class="c-article__sub-heading" id="affiliations">Authors and Affiliations</h3><ol class="c-article-author-affiliation__list"><li id="Aff1"><p class="c-article-author-affiliation__address">Université de Toulouse, UPS-OMP, IRAP, F-31400 Toulouse, France, </p><p class="c-article-author-affiliation__authors-list">S. Charpinet</p></li><li id="Aff2"><p class="c-article-author-affiliation__address">CNRS, IRAP, 14 avenue Edouard Belin, F-31400 Toulouse, France, </p><p class="c-article-author-affiliation__authors-list">S. Charpinet</p></li><li id="Aff3"><p class="c-article-author-affiliation__address">Département de Physique, Université de Montréal, CP 6128, Succursale Centre-Ville, Montréal QC H3C 3J7, Canada, </p><p class="c-article-author-affiliation__authors-list">G. Fontaine &amp; P. Brassard</p></li><li id="Aff4"><p class="c-article-author-affiliation__address">Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, Arizona 85721, USA, </p><p class="c-article-author-affiliation__authors-list">E. M. Green</p></li><li id="Aff5"><p class="c-article-author-affiliation__address">Institut d’Astrophysique et de Géophysique, Université de Liège, 17 Allée du 6 Août, B-4000 Liège, Belgium, </p><p class="c-article-author-affiliation__authors-list">V. Van Grootel</p></li><li id="Aff6"><p class="c-article-author-affiliation__address">FNRS, rue d’Egmont 5, B-1000 Bruxelles, Belgium, </p><p class="c-article-author-affiliation__authors-list">V. Van Grootel</p></li><li id="Aff7"><p class="c-article-author-affiliation__address">ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany, </p><p class="c-article-author-affiliation__authors-list">S. K. Randall</p></li><li id="Aff8"><p class="c-article-author-affiliation__address">INAF-Osservatorio Astronomico di Torino, Strada dell’Osservatorio 20, 10025 Pino Torinese, Italy, </p><p class="c-article-author-affiliation__authors-list">R. Silvotti</p></li><li id="Aff9"><p class="c-article-author-affiliation__address">Mt Suhora Observatory, Cracow Pedagogical University, ulica Podchorazych 2, 30-084 Krakow, Poland, </p><p class="c-article-author-affiliation__authors-list">A. S. Baran</p></li><li id="Aff10"><p class="c-article-author-affiliation__address">Department of Physics and Astronomy, Iowa State University, 12 Physics Hall, Ames, 50011, Iowa, USA</p><p class="c-article-author-affiliation__authors-list">A. S. Baran &amp; S. D. Kawaler</p></li><li id="Aff11"><p class="c-article-author-affiliation__address">Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium, </p><p class="c-article-author-affiliation__authors-list">R. H. Østensen</p></li><li id="Aff12"><p class="c-article-author-affiliation__address">Nordic Optical Telescope, Apartado 474, 38700 Santa Cruz de La Palma, Spain, </p><p class="c-article-author-affiliation__authors-list">J. H. Telting</p></li></ol><div class="u-js-hide u-hide-print" data-test="author-info"><span class="c-article__sub-heading">Authors</span><ol class="c-article-authors-search u-list-reset"><li id="auth-S_-Charpinet-Aff1-Aff2"><span class="c-article-authors-search__title u-h3 js-search-name">S. 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Kawaler</span><div class="c-article-authors-search__list"><div class="c-article-authors-search__item c-article-authors-search__list-item--left"><a href="/search?author=S.%20D.%20Kawaler" class="c-article-button" data-track="click" data-track-action="author link - publication" data-track-label="link" rel="nofollow">View author publications</a></div><div class="c-article-authors-search__item c-article-authors-search__list-item--right"><p class="search-in-title-js c-article-authors-search__text">You can also search for this author in <span class="c-article-identifiers"><a class="c-article-identifiers__item" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?cmd=search&amp;term=S.%20D.%20Kawaler" data-track="click" data-track-action="author link - pubmed" data-track-label="link" rel="nofollow">PubMed</a><span class="u-hide"> </span><a class="c-article-identifiers__item" href="http://scholar.google.co.uk/scholar?as_q=&amp;num=10&amp;btnG=Search+Scholar&amp;as_epq=&amp;as_oq=&amp;as_eq=&amp;as_occt=any&amp;as_sauthors=%22S.%20D.%20Kawaler%22&amp;as_publication=&amp;as_ylo=&amp;as_yhi=&amp;as_allsubj=all&amp;hl=en" data-track="click" data-track-action="author link - scholar" data-track-label="link" rel="nofollow">Google Scholar</a></span></p></div></div></li><li id="auth-J__H_-Telting-Aff12"><span class="c-article-authors-search__title u-h3 js-search-name">J. H. Telting</span><div class="c-article-authors-search__list"><div class="c-article-authors-search__item c-article-authors-search__list-item--left"><a href="/search?author=J.%20H.%20Telting" class="c-article-button" data-track="click" data-track-action="author link - publication" data-track-label="link" rel="nofollow">View author publications</a></div><div class="c-article-authors-search__item c-article-authors-search__list-item--right"><p class="search-in-title-js c-article-authors-search__text">You can also search for this author in <span class="c-article-identifiers"><a class="c-article-identifiers__item" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?cmd=search&amp;term=J.%20H.%20Telting" data-track="click" data-track-action="author link - pubmed" data-track-label="link" rel="nofollow">PubMed</a><span class="u-hide"> </span><a class="c-article-identifiers__item" href="http://scholar.google.co.uk/scholar?as_q=&amp;num=10&amp;btnG=Search+Scholar&amp;as_epq=&amp;as_oq=&amp;as_eq=&amp;as_occt=any&amp;as_sauthors=%22J.%20H.%20Telting%22&amp;as_publication=&amp;as_ylo=&amp;as_yhi=&amp;as_allsubj=all&amp;hl=en" data-track="click" data-track-action="author link - scholar" data-track-label="link" rel="nofollow">Google Scholar</a></span></p></div></div></li></ol></div><h3 class="c-article__sub-heading" id="contributions">Contributions</h3><p>S.C. wrote the manuscript, and analysed and interpreted the data from which the presence of planetary bodies was inferred. S.C., G.F., P.B. and V.V.G. derived and checked the calculations to estimate the planets’ properties. G.F., P.B. and S.K.R. computed the cut-off frequencies and the theoretical mode visibilities based on a model of the star from V.V.G. E.M.G. obtained and analysed radial velocity measurements. S.D.K., A.S.B., R.H.Ø, R.S. and J.H.T. from the KASC WG11 group independently checked the detection of the orbital signals in the data. All authors discussed the results and contributed to their interpretation.</p><h3 class="c-article__sub-heading" id="corresponding-author">Corresponding author</h3><p id="corresponding-author-list">Correspondence to <a id="corresp-c1" href="mailto:stephane.charpinet@ast.obs-mip.fr">S. 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P. <i>et al.</i> A compact system of small planets around a former red-giant star. <i>Nature</i> <b>480</b>, 496–499 (2011). https://doi.org/10.1038/nature10631</p><p class="c-bibliographic-information__download-citation u-hide-print"><a data-test="citation-link" data-track="click" data-track-action="download article citation" data-track-label="link" data-track-external="" rel="nofollow" href="https://citation-needed.springer.com/v2/references/10.1038/nature10631?format=refman&amp;flavour=citation">Download citation<svg width="16" height="16" focusable="false" role="img" aria-hidden="true" class="u-icon"><use xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="#icon-eds-i-download-medium"></use></svg></a></p><ul class="c-bibliographic-information__list" data-test="publication-history"><li class="c-bibliographic-information__list-item"><p>Received<span class="u-hide">: </span><span class="c-bibliographic-information__value"><time datetime="2011-07-06">06 July 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