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<ri:Resource created="2020-10-16T12:06:31Z" status="active" updated="2025-06-13T15:25:00Z" version="1.2" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>TOI-1235 Radial velocities &amp; optical spectroscopy</title><shortName>J/AJ/160/22</shortName><identifier>ivo://CDS.VizieR/J/AJ/160/22</identifier><altIdentifier>doi:10.26093/cds/vizier.51600022</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Cloutier R.</name></creator><creator><name>Rodriguez J.E.</name></creator><creator><name>Irwin J.</name></creator><creator><name>Charbonneau D.</name></creator><creator><name>Stassun K.G.,Mortier A.</name></creator><creator><name>Latham D.W.</name></creator><creator><name>Isaacson H.</name></creator><creator><name>Howard A.W.</name></creator><creator><name>Udry S.</name></creator><creator><name>Wilson T.G.,Watson C.A.</name></creator><creator><name>Pinamonti M.</name></creator><creator><name>Lienhard F.</name></creator><creator><name>Giacobbe P.</name></creator><creator><name>Guerra P.,Collins K.A.</name></creator><creator><name>Beiryla A.</name></creator><creator><name>Esquerdo G.A.</name></creator><creator><name>Matthews E.</name></creator><creator><name>Matson R.A.,Howell S.B.</name></creator><creator><name>Furlan E.</name></creator><creator><name>Crossfield I.J.M.</name></creator><creator><name>Winters J.G.</name></creator><creator><name>Nava C.</name></creator><creator><name>Ment K.,Lopez E.D.</name></creator><creator><name>Ricker G.</name></creator><creator><name>Vanderspek R.</name></creator><creator><name>Seager S.</name></creator><creator><name>Jenkins J.M.</name></creator><creator><name>Ting E.B.,Tenenbaum P.</name></creator><creator><name>Sozzetti A.</name></creator><creator><name>Sha L.</name></creator><creator><name>Segransan D.</name></creator><creator><name>Schlieder J.E.,Sasselov D.</name></creator><creator><name>Roy A.</name></creator><creator><name>Robertson P.</name></creator><creator><name>Rice K.</name></creator><creator><name>Poretti E.</name></creator><creator><name>Piotto G.,Phillips D.</name></creator><creator><name>Pepper J.</name></creator><creator><name>Pepe F.</name></creator><creator><name>Molinari E.</name></creator><creator><name>Mocnik T.</name></creator><creator><name>Micela G.,Mayor M.</name></creator><creator><name>Martinez Fiorenzano A.F.</name></creator><creator><name>Mallia F.</name></creator><creator><name>Lubin J.</name></creator><creator><name>Lovis C.,Lopez-Morales M.</name></creator><creator><name>Kosiarek M.R.</name></creator><creator><name>Kielkopf J.F.</name></creator><creator><name>Kane S.R.</name></creator><creator><name>Jensen E.L.N.,Isopi G.</name></creator><creator><name>Huber D.</name></creator><creator><name>Hill M.L.</name></creator><creator><name>Harutyunyan A.</name></creator><creator><name>Gonzales E.</name></creator><creator><name>Giacalone S.,Ghedina A.</name></creator><creator><name>Ercolino A.</name></creator><creator><name>Dumusque X.</name></creator><creator><name>Dressing C.D.</name></creator><creator><name>Damasso M.</name></creator><creator><name>Dalba P.A.,Cosentino R.</name></creator><creator><name>Conti D.M.</name></creator><creator><name>Colon K.D.</name></creator><creator><name>Collins K.I.</name></creator><creator><name>Cameron A.C.</name></creator><creator><name>Ciardi D.,Christiansen J.</name></creator><creator><name>Chontos A.</name></creator><creator><name>Cecconi M.</name></creator><creator><name>Caldwell D.A.</name></creator><creator><name>Burke C.,Buchhave L.</name></creator><creator><name>Beichman C.</name></creator><creator><name>Behmard A.</name></creator><creator><name>Beard C.</name></creator><creator><name>Akana Murphy J.M.</name></creator><date role="Updated">2021-09-16T09:54:29Z</date><date role="Created">2020-10-16T12:06:31Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>dwarf-stars</subject><subject>m-stars</subject><subject>visible-astronomy</subject><subject>spectroscopy</subject><subject>photometry</subject><subject>radial-velocity</subject><subject>exoplanets</subject><description>Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/nonrocky transition in period-radius space. Here we present the confirmation of TOI-1235b (P=3.44days, r_p_=1.738_-0.076_^+0.087^R_{Earth}_), a planet whose size and period are intermediate between the competing model predictions, thus making the system an important test case for emergence models of the rocky/nonrocky transition around early M dwarfs (R_s_=0.630{+/-}0.015R_{sun}_, M_s_=0.640{+/-}0.016M_{sun}_). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high- resolution imaging, and a set of 38 precise radial velocities (RVs) from HARPS-N and HIRES. We measure a planet mass of 6.91_-0.85_^+0.75^M_{Earth}_, which implies an iron core mass fraction of 20_-12_^+15^% in the absence of a gaseous envelope. The bulk composition of TOI-1235b is therefore consistent with being Earth-like, and we constrain an H/He envelope mass fraction to be &lt;0.5% at 90% confidence. Our results are consistent with model predictions from thermally driven atmospheric mass loss but not with gas-poor formation, suggesting that the former class of processes remains efficient at sculpting close-in planets around early M dwarfs. Our RV analysis also reveals a strong periodicity close to the first harmonic of the photometrically determined stellar rotation period that we treat as stellar activity, despite other lines of evidence favoring a planetary origin (P=21.8_-0.8_^+0.9^days, m_p_sini=13.0_-5.3_^+3.8^M_{Earth}_) that cannot be firmly ruled out by our data.</description><source format="bibcode">2020AJ....160...22C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/160/22</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/I/259">I/259 : The Tycho-2 Catalogue (Hog+ 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/335">II/335 : Revised catalog of GALEX UV sources (GUVcat_AIS GR6+7)(Bianchi+ 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/IV/38">IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/123/2822">J/AJ/123/2822 : Photometry of southern NLTT stars (Reid+, 2002)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/370/954">J/MNRAS/370/954 : VRIHalpha photometry of M34 (Irwin+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/468/1115">J/A+A/468/1115 : Thorium and argon lines in the visible (Lovis+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/529/A75">J/A+A/529/A75 : Limb-darkening coefficients (Claret+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/142/19">J/AJ/142/19 : Speckle observations of KOI (Howell+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/743/48">J/ApJ/743/48 : Stars with Prot and X-ray luminosities (Wright+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/200/15">J/ApJS/200/15 : HARPS-TERRA project. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>BJD</name><description>[1828/1922] Barycentric Julian Date, BJD-2457000</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>RVel</name><description>[-7.9/9.7] Radial velocity</description><unit>m/s</unit><ucd>phys.veloc;pos.heliocentric</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_RVel</name><description>[0.81/2.2] Uncertainty in RV</description><unit>m/s</unit><ucd>stat.error;spect.dopplerVeloc</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Inst</name><description>Instrument used (1)</description><ucd>instr.setup</ucd><dataType xsi:type="vs:VOTableType" arraysize="7*">char</dataType></column></table><table><name>J/AJ/160/22/fig3</name><description>TOI-1235 differential light curve from archival MEarth-North photometry</description><column><name>recno</name><description>Record number assigned by the VizieR team. Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>BJD</name><description>[2454741/2457337] Barycentric Julian Date</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>Flux</name><description>[0.89/1.1] Normalized flux</description><ucd>phot.flux;arith.ratio</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>e_Flux</name><description>[0.001/0.03] Error, Flux</description><ucd>stat.error;phot.flux</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column></table></schema></tableset></ri:Resource>