J/A+A/624/A38ivo://CDS.VizieR/J/A+A/624/A38doi:10.26093/cds/vizier.36240038CDSDamasso M.Zeng L.Malavolta L.Mayo A.Sozzetti A.Mortier A.,Buchhave L.A.Vanderburg A.Lopez-Morales M.Bonomo A.S.Cameron A.C.,Coffinet A.Figueira P.Latham D.W.Mayor M.Molinari E.Pepe F.,Phillips D.F.Poretti E.Rice K.Udry S.Watson C.A.2019-04-08T14:51:55Z2019-04-08T08:07:39ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmultiple-starsexoplanetsradial-velocityK2-36 is a K dwarf orbited by two small (R_b_=1.43+/-0.08R_{earth}_ and R_c_=3.2+/-0.3R_{earth}_, close-in (a_b_=0.022AU and a_c_=0.054AU) transiting planets discovered by the Kepler/K2 space observatory. They are representatives of two distinct families of small planets (R_p_<4R_{earth}_) recently emerged from the analysis of Kepler data, with likely a different structure, composition and evolutionary pathways. We revise the fundamental stellar parameters and the sizes of the planets, and provide the first measurement of their masses and bulk densities, which we use to infer their structure and composition. We observed K2-36 with the HARPS-N spectrograph over ~3.5-years, collecting 81 useful radial velocity measurements. The star is active, with evidence for increasing levels of magnetic activity during the observing time span. The radial velocity scatter is ~17m/s due to the stellar activity contribution, which is much larger that the semi-amplitudes of the planetary signals. We tested different methods for mitigating the stellar activity contribution to the radial velocity time variations and measuring the planet masses with good precision. We find that K2-36 is likely a ~1Gyr old system, and by treating the stellar activity through a Gaussian process regression, we measured the planet masses m_b_=3.9+/-1.1M_{earth}_ and m_c_=7.8+/-2.3M_{earth}_. The derived planet bulk densities {rho}_b_=7.2^+2.5^_-2.1_g/cm^3^ and {rho}_c_=1.3^+0.7^_-0.5^g/cm^3^ point out that K2-36b has a rocky, Earth-like composition, and K2-36c is a low-density sub-Neptune. Composed of two planets with similar orbital separations but different densities, K2-36 represents an optimal laboratory for testing the role of the atmospheric escape in driving the evolution of close-in, low-mass planets after ~1Gyr from their formation. Due to their similarities, we performed a preliminary comparative analysis between the systems K2-36 and Kepler-36, which we deem worthy of a more detailed investigation.2019A&A...624A..38Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/624/A38CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/624/A38https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/624/A38http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/624/A38https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/624/A38https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/624/A38http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/624/A38GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/624/A38/tablea1Spectroscopic activity/CCF asymmetry indicators for K2-36 with data extracted from the 81 spectra used in this workBJDTime of observation, TDB (BJD-2400000)dtime.epochdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFWHMFWHM of the CCFm/sspect.line.widthfloatBISCCF Bisector Inverse Slope (BIS)m/sphys.velocfloatlogR'HKMount Wilson logR_HK indexphot.flux;arith.ratiofloate_logR'HKError on Mount Wilson logR_HK indexstat.errorfloatHalphaActivity index based on the H{alpha} linemeta.code;spect.indexdoublee_HalphaError on the H{alpha} activity indexstat.errordoubleVasy? CCF line asymmetryspect.line.asymmetry;spect.linedoublenullablee_Vasy? Error on the CCF line asymmetrystat.errordoublenullableJ/A+A/624/A38/tablea2Radial velocities of K2-36 extracted from the 81 HARPS-N spectra analysed in this workrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDTime of observation, TDB (BJD-2400000)dtime.epochdoubleRVdrsRadial velocity (DRS pipeline)m/sphys.veloc;pos.heliocentricdoublee_RVdrsError radial velocity (DRS pipeline)m/sstat.errorfloatRVterraRelative radial velocity (TERRA pipeline)m/sphys.veloc;pos.heliocentricfloate_RVterraError Radial velocity (TERRA pipeline)m/sstat.errorfloat