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<ri:Resource created="2024-05-13T11:43:34Z" status="active" updated="2025-05-19T09:50:00Z" 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>HD 136164 Ab IR spectrum with VLTI/GRAVITY</title><shortName>J/AJ/167/64</shortName><identifier>ivo://CDS.VizieR/J/AJ/167/64</identifier><altIdentifier>doi:10.26093/cds/vizier.51670064</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Balmer W.O.</name></creator><creator><name>Pueyo L.</name></creator><creator><name>Lacour S.</name></creator><creator><name>Wang J.J.</name></creator><creator><name>Stolker T.</name></creator><creator><name>Kammerer J.,Pourre N.</name></creator><creator><name>Nowak M.</name></creator><creator><name>Rickman E.</name></creator><creator><name>Blunt S.</name></creator><creator><name>Sivaramakrishnan A.</name></creator><creator><name>Sing D.,Wagner K.</name></creator><creator><name>Marleau G.-D.</name></creator><creator><name>Lagrange A.-M.</name></creator><creator><name>Abuter R.</name></creator><creator><name>Amorim A.,Asensio-Torres R.</name></creator><creator><name>Berger J.-P.</name></creator><creator><name>Beust H.</name></creator><creator><name>Boccaletti A.</name></creator><creator><name>Bohn A.,Bonnefoy M.</name></creator><creator><name>Bonnet H.</name></creator><creator><name>Bordoni M.S.</name></creator><creator><name>Bourdarot G.</name></creator><creator><name>Brandner W.,Cantalloube F.</name></creator><creator><name>Caselli P.</name></creator><creator><name>Charnay B.</name></creator><creator><name>Chauvin G.</name></creator><creator><name>Chavez A.</name></creator><creator><name>Choquet E.,Christiaens V.</name></creator><creator><name>Clenet Y.</name></creator><creator><name>du Foresto V.C.</name></creator><creator><name>Cridland A.</name></creator><creator><name>Davies R.,Dembet R.</name></creator><creator><name>Drescher A.</name></creator><creator><name>Duvert G.</name></creator><creator><name>Eckart A.</name></creator><creator><name>Eisenhauer F.,Schreiber N.M.F.</name></creator><creator><name>Garcia P.</name></creator><creator><name>Garcia Lopez R.</name></creator><creator><name>Gendron E.</name></creator><creator><name>Genzel R.,Gillessen S.</name></creator><creator><name>Girard J.H.</name></creator><creator><name>Grant S.</name></creator><creator><name>Haubois X.</name></creator><creator><name>Heissel G.</name></creator><creator><name>Henning T.,Hinkley S.</name></creator><creator><name>Hippler S.</name></creator><creator><name>Houlle M.</name></creator><creator><name>Hubert Z.</name></creator><creator><name>Jocou L.</name></creator><creator><name>Keppler M.,Kervella P.</name></creator><creator><name>Kreidberg L.</name></creator><creator><name>Kurtovic N.T.</name></creator><creator><name>Lapeyrere V.</name></creator><creator><name>Le Bouquin J.-B.,Lena P.</name></creator><creator><name>Lutz D.</name></creator><creator><name>Maire A.-L.</name></creator><creator><name>Mang F.</name></creator><creator><name>Merand A.</name></creator><creator><name>Molliere P.,Mordasini C.</name></creator><creator><name>Mouillet D.</name></creator><creator><name>Nasedkin E.</name></creator><creator><name>Ott T.</name></creator><creator><name>Otten G.P.P.L.,Paladini C.</name></creator><creator><name>Paumard T.</name></creator><creator><name>Perraut K.</name></creator><creator><name>Perrin G.</name></creator><creator><name>Pfuhl O.</name></creator><creator><name>Ribeiro D.C.,Rodet L.</name></creator><creator><name>Rustamkulov Z.</name></creator><creator><name>Shangguan J.</name></creator><creator><name>Shimizu T.</name></creator><creator><name>Straubmeier C.,Sturm E.</name></creator><creator><name>Tacconi L.J.</name></creator><creator><name>Vigan A.</name></creator><creator><name>Vincent F.</name></creator><creator><name>Ward-Duong K.</name></creator><creator><name>Widmann F.,Winterhalder T.</name></creator><creator><name>Woillez J.</name></creator><creator><name>Yazici S.</name></creator><creator><name>the GRAVITY Collaboration</name></creator><date role="Updated">2024-11-06T20:20:42Z</date><date role="Created">2024-05-13T11:43:34Z</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>brown-dwarfs</subject><subject>exoplanets</subject><subject>infrared-astronomy</subject><subject>spectroscopy</subject><description>Young, low-mass brown dwarfs orbiting early-type stars, with low mass ratios (q&lt;~0.01), appear to be intrinsically rare and present a formation dilemma: could a handful of these objects be the highest-mass outcomes of "planetary" formation channels (bottom up within a protoplanetary disk), or are they more representative of the lowest-mass "failed binaries" (formed via disk fragmentation or core fragmentation)? Additionally, their orbits can yield model-independent dynamical masses, and when paired with wide wavelength coverage and accurate system age estimates, can constrain evolutionary models in a regime where the models have a wide dispersion depending on the initial conditions. We present new interferometric observations of the 16Myr substellar companion HD136164Ab (HIP75056Ab) made with the Very Large Telescope Interferometer (VLTI)/GRAVITY and an updated orbit fit including proper motion measurements from the Hipparcos-Gaia Catalog of Accelerations. We estimate a dynamical mass of 35{+/-}10MJ (q~0.02), making HD136164Ab the youngest substellar companion with a dynamical mass estimate. The new mass and newly constrained orbital eccentricity (e=0.44{+/-}0.03) and separation (22.5{+/-}1au) could indicate that the companion formed via the low-mass tail of the initial mass function. Our atmospheric fit to a SPHINX M-dwarf model grid suggests a subsolar C/O ratio of 0.45 and 3 x solar metallicity, which could indicate formation in a circumstellar disk via disk fragmentation. Either way, the revised mass estimate likely excludes bottom-up formation via core accretion in a circumstellar disk. HD136164Ab joins a select group of young substellar objects with dynamical mass estimates; epoch astrometry from future Gaia data releases will constrain the dynamical mass of this crucial object further.</description><source format="bibcode">2024AJ....167...64B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/167/64</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/246">II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+AS/141/371">J/A+AS/141/371 : Low-mass stars evolution tracks &amp; isochrones (Girardi+, 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/464/581">J/A+A/464/581 : Sco OB2 intermediate-mass stars (Kouwenhoven+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/144/64">J/AJ/144/64 : Solar neighborhood XXVIII. 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