Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12666/589
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dc.rights.licenseCopyright © 2021, Oxford University Press-
dc.contributor.authorOsborn, Hugh P.-
dc.contributor.authorArmstrong, D. J.-
dc.contributor.authorAdibekyan, V.-
dc.contributor.authorCollins, K. A.-
dc.contributor.authorDelgado Mena, E.-
dc.contributor.authorHowell, Steve B.-
dc.contributor.authorHellier, C.-
dc.contributor.authorKing, G. W.-
dc.contributor.authorLillo Box, J.-
dc.contributor.authorNielsen, L. D.-
dc.contributor.authorOtegi, J. F.-
dc.contributor.authorSantos, N. C.-
dc.contributor.authorZiegler, C.-
dc.contributor.authorAnderson, D. R.-
dc.contributor.authorBriceño, C.-
dc.contributor.authorBurke, C. J.-
dc.contributor.authorBayliss, D.-
dc.contributor.authorBarrado, D.-
dc.contributor.authorBryant, E. M.-
dc.contributor.authorBrown, D. J. A.-
dc.contributor.authorBarros, S. C. C.-
dc.contributor.authorBouchy, F.-
dc.contributor.authorCaldwell, D. A.-
dc.contributor.authorConti, D.-
dc.contributor.authorDíaz, R. F.-
dc.contributor.authorDragomir, D.-
dc.contributor.authorDeleuil, M.-
dc.contributor.authorDemanegon, O. D. S.-
dc.contributor.authorDorn, C.-
dc.contributor.authorDaylan, T.-
dc.contributor.authorFigueira, P.-
dc.contributor.authorHelled, R.-
dc.contributor.authorHoyer, S.-
dc.contributor.authorJenkins, J. S.-
dc.contributor.authorJensen, E. L. N.-
dc.contributor.authorLatham, D. W.-
dc.contributor.authorLaw, N.-
dc.contributor.authorLouie, D.-
dc.contributor.authorMann, A. W.-
dc.contributor.authorOsborn, A.-
dc.contributor.authorPollacco, D.-
dc.contributor.authorRodríguez, D. R.-
dc.contributor.authorRackham, B. V.-
dc.contributor.authorRicker, G.-
dc.contributor.authorScott, N. J.-
dc.contributor.authorSousa, S. G.-
dc.contributor.authorSeager, S.-
dc.contributor.authorStassun, K. G.-
dc.contributor.authorSmith, J. C.-
dc.contributor.authorStrom, P.-
dc.contributor.authorUdry, S.-
dc.contributor.authorVillaseñor, J.-
dc.contributor.authorVanderspek, R.-
dc.contributor.authorWest, R.-
dc.contributor.authorWheatley, P. J.-
dc.contributor.authorWinn, J. N.-
dc.contributor.otherUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737-
dc.date.accessioned2022-02-15T14:20:43Z-
dc.date.available2022-02-15T14:20:43Z-
dc.date.issued2021-01-25-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 502(4): 4842–4857(2021)es
dc.identifier.issn0035-8711-
dc.identifier.otherhttps://academic.oup.com/mnras/article-abstract/502/4/4842/6119926-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/589-
dc.description.abstractWe report the discovery of HD 110113 b (TESS object of interest-755.01), a transiting mini-Neptune exoplanet on a 2.5-d orbit around the solar-analogue HD 110113 (Teff = 5730 K). Using TESS photometry and High Accuracy Radial velocity Planet Searcher (HARPS) radial velocities gathered by the NCORES program, we find that HD 110113 b has a radius of 2.05 ± 0.12  R⊕ and a mass of 4.55 ± 0.62  M⊕. The resulting density of 2.90+0.75−0.59  g cm−3 is significantly lower than would be expected from a pure-rock world; therefore HD 110113 b must be a mini-Neptune with a significant volatile atmosphere. The high incident flux places it within the so-called radius valley; however, HD 110113 b was able to hold on to a substantial (0.1–1 per cent) H–He atmosphere over its ∼4 Gyr lifetime. Through a novel simultaneous Gaussian process fit to multiple activity indicators, we were also able to fit for the strong stellar rotation signal with period 20.8 ± 1.2  d from the RVs and confirm an additional non-transiting planet, HD 110113 c, which has a mass of 10.5 ± 1.2  M⊕ and a period of 6.744+0.008−0.009  d.es
dc.description.sponsorshipWe thank Raphaelle Haywood, Maximillian Gunther and FB for discussion on disentangling RV activity from signals. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program and NASA's Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This study is based on observations collected at the European Southern Observatory under ESO programme 1102.C-0249. We thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support to our planet search programs. This work has been in particular carried out in the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). This publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualization, exchange, and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch.This work makes use of observations from the LCOGT network. (Some of the) Observations in the paper made use of the HighResolution Imaging instrument(s) `Alopeke (and/or Zorro). `Alopeke (and/or Zorro) was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by SBH, NJS, Elliott P. Horch, and Emmett Quigley. Datawere reduced using a software pipeline originally written by Elliott Horch and Mark Everett. `Alopeke (and/or Zorro) was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF's Optical-Infrared Astronomy Research (NOIR) Lab, which is managed by the Association ofUniversities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (USA), National Research Council (Canada), Agencia Nacional de Investigaci ' on y Desarrollo (Chile), Ministerio de Ciencia, Tecnolog ' ia e Innovaci ' on (Argentina), Minist ' erio da Ci <^>encia, Tecnologia, Inovac comma ~oes e Comunicac comma ~oes (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea).; Based in part on observations obtained at the SOAR telescope, which is a joint project of the Minist ' erio da Ci <^>encia, Tecnologia e Inovaccomma ~oes (MCTI/LNA) do Brasil, the US National Science Foundation's NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU) and the international Gemini Observatory, a program of NSF's NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini Observatory partnership: the National Science Foundation (USA), National Research Council (Canada), Agencia Nacional de Investigaci ' on y Desarrollo (Chile), Ministerio de Ciencia, Tecnolog ' ia e Innovaci ' on (Argentina), Minist ' erio da Ci<^>encia, Tecnologia, Inovaccomma ~oes e Comunicaccomma ~oes (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). HPO acknowledges support from NCCR/Planet-S via the CHESS fellowship. DJA acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). VA, ED-M, NCS, ODSD, and SCCB acknowledge support by FCT -Fundaccomma ~ao para a Ci<^>encia e a Tecnologia (Portugal) through national funds and by FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizaccomma ~ao by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER- 028953. VA and EDM further acknowledge the support from FCT through Investigador FCT contracts IF/00650/2015/CP1273/CT0001 and IF/00849/2015/CP1273/CT0003. ODSD and SCCB are supported through Investigador contract (DL 57/2016/CP1364/CT0004) funded by FCT. JL-B is supported by the Spanish State Research Agency (AEI) Projects No. ESP2017-87676-C5-1-R and No. MDM-2017-0737 Unidad de Excelencia `Mar ' ia de Maeztu'-Centro de Astrobiolog ' ia (INTA-CSIC) DD acknowledges support from the TESS Guest Investigator Program grant 80NSSC19K1727 and NASA Exoplanet Research P rogram grant 18-2XRP18 2-0136. BVR thanks the Heising-Simons Foundation for support. TD acknowledges support from MIT's Kavli Institute as a Kavli postdoctoral fellow AO acknowledges support from an STFC studentship. SH acknowledges CNES funding through the grant 837319 DJAB acknowledges support by the UK Space Agency. This research made use of the following python software: EXOPLANET (Foreman-Mackey et al. 2020) and its dependencies (Astropy Collaboration 2013, 2018; Salvatier et al. 2016; TheanoDevelopment Team 2016; Foreman-Mackey et al. 2017, 2020; Foreman-Mackey 2018; Luger et al. 2019; Agol, Luger & Foreman-Mackey 2020); NUMPY (Harris et al. 2020); SCIPY (Virtanen et al. 2020); PANDAS (McKinney et al. 2011); ASTROPY (Robitaille et al. 2013); MATPLOTLIB (Hunter 2007); ASTROIMAGJ (Collins et al. 2017); TAPIR (Jensen 2013).es
dc.language.isoenges
dc.publisherOxford Academics: Oxford University Presses
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2017-87676-C5-1-R-
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.subjectPlanets and satellites: detectiones
dc.subjectStars: individual: HD110113es
dc.titleA hot mini-Neptune in the radius valley orbiting solar analogue HD 110113es
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidDorn, C. [0000-0001-6110-4610]-
dc.contributor.orcidAnderson, D. [0000-0001-7416-7522]-
dc.contributor.orcidBarros, S. [0000-0003-2434-3625]-
dc.contributor.orcidAdibekyan, V. [0000-0002-0601-6199]-
dc.contributor.orcidArmstrong, D. [0000-0002-5080-4117]-
dc.contributor.orcidSantos, N. [0000-0003-4422-2919]-
dc.identifier.doi10.1093/mnras/stab182-
dc.identifier.e-issn1365-2966-
dc.contributor.funderFundacao para a Ciencia e a Tecnologia (FCT)-
dc.contributor.funderScience and Technology Facilities Council (STFC)-
dc.contributor.funderAgencia Estatal de Investigación (AEI)-
dc.contributor.funderNational Aeronautics and Space Administration (NASA)-
dc.contributor.funderUK Space Agency-
dc.description.peerreviewedPeerreviewes
dc.identifier.funderhttp://dx.doi.org/10.13039/501100001871-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000271-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100011033-
dc.identifier.funderhttp://dx.doi.org/10.13039/100000104-
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion-
dc.rights.accessRightsinfo:eu-repo/semantics/openAccess-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501-
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