J/A+A/709/A130ivo://CDS.VizieR/J/A+A/709/A130doi:10.26093/cds/vizier/bc-p5/lbdaCDSSubjak J.Brahm R.Liptak J.Eberhardt J.Tala Pinto M.Casewell S.L.,Henning T.Hesse K.Trifonov T.Jordan A.Rojas F.I.Vitkova M.,Salinas H.Boyle G.Suc V.Antonucci L.Bernacki K.Briceno C.,Collins K.A.Fernandez Fernandez J.Gill S.Janik J.Law N.Mann A.W.,McCormac J.Popowicz A.Sebastian D.Skarka M.Vaclavik J.Vanzi L.,West R.G.Wilkin F.P.Ziegler C.2026-05-19T14:19:56Z2026-05-08T17:03:42ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsspectroscopyradial-velocityvisible-astronomyWe present four newly validated transiting brown dwarfs identified through TESS photometry and confirmed with high-precision radial velocity measurements obtained from the FEROS and PLATOSpec spectrographs. Notably, three of these companions exhibit orbital periods exceeding 100 days, thereby expanding the sample of long-period transiting brown dwarfs from four to seven systems. The host stars of long-period brown dwarfs show mild subsolar metallicity. These discoveries highlight the expansion of the metal-poor, long-period distribution and help us better understand the brown dwarf desert. In our comparative analysis of eccentricity and metallicity demographics, we utilize catalogues of long-period giant planets, brown dwarfs, and low-mass stellar companions. After accounting for tidal influences, the eccentricity distribution aligns with that of low-mass stellar binaries, presenting a different profile than that observed within the giant planet population. Additionally, the metallicity of the host stars reveals a noteworthy trend: short-period transiting brown dwarfs are predominantly associated with metal-rich stars, whereas long-period brown dwarfs are more often found around metal-poor stars, demonstrating statistical similarities to low-mass stellar hosts. This trend has also been previously observed in studies of hot and cold Jupiters and points to a period-coded mixture of channels. A natural explanation is that most brown dwarfs originate from fragmentation at wider separations, with long-period systems retaining this stellar-like imprint, while only those embedded in massive, long-lived, metal-rich protoplanetary discs are efficiently delivered and stabilised to short orbits.2026A&A...709A.130Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/709/A130CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toIV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/709/A130https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/709/A130http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/709/A130https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/709/A130https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/709/A130http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/709/A130GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/709/A130/stars (Studied stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/709/A130/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/709/A130/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/709/A130/stars?GETtext/xml+votable180.050000true72.793875-8.44733890.0055555555555555566/16665 20992 22642 33339https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/709/A130?format=asciiOpticaldefaultJ/A+A/709/A130/starsStudied starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar namemeta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainVCShow the Radial Velocity curvesmeta.ref.urlcharJ/A+A/709/A130/rvsFEROS and PLATOSpec radial velocitiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar namemeta.id;meta.maincharBJDBarycentric Julian date (BJD-2457000)dtime.epochdoubleRVRelative radial velocitykm/sphys.veloc;pos.heliocentricfloate_RVRadial velocity uncertaintykm/sstat.errorfloatSpecSpectrographmeta.id;instrchar