J/other/Sci/392.ivo://CDS.VizieR/J/other/Sci/392.L2348CDSWilson T.G.Simpson A.M.Collier Cameron A.Cloutier R.Adibekyan V.,Anna John A.Alibert Y.Stalport M.Egger J.A.Bonfanti A.Billot N.,Guterman P.Maxted P.F.L.Simon A.E.Sousa S.G.Fridlund M.,Beck M.Bekkelien A.SalmonS.Van Grootel V.Fossati L.,Mustill A.J.Osborn H.P.Zingales T.Hooton M.J.Affer L.,Aigrain S.Alonso R.Anglada G.Antoniadis-Karnavas A.Barczy T.,Barrado Navascues D.Barros S.C.C.Baumjohann W.Beck T.Benz W.,Biondi F.Bonfils X.Borsato L.Brandeker A.Broeg C.Buchhave L.A.,Buder M.Cabrera J.Carrazco Gaxiola S.Charbonneau D.Charnoz S.,Ciardi D.R.Collins K.A.Collins K.I.Cosentino R.Csizmadia S.,Cubillos P.E.Dalal S.Damasso M.Davenport J.R.A.Davies M.B.,Deleuil M.Delrez L.Demangeon O.D.S.Demory B.-O.DiTomasso V.,Dragomir D.Dressing C.D.Dumusque X.Ehrenreich D.Erikson A.,Esparza-Borges E.Fortier A.Fukuda I.Fukui A.Gandolfi D.Ghedina A.,Giacalone S.Gill H.Gillon M.Gomez Maqueo Chew Y.G1uedel M.,Guerra P.Guenther M.N.Hara N.Harutyunyan A.Hayashi Y.Haywood R.D.,Holcomb R.Horne K.Hoyer S.Huang C.X.Ikoma M.Isaak K.G.,Jackman J.A.G.Jenkins J.M.Jensen E.L.N.Jontof-Hutter D.,Kawai Y.Kiss L.L.Lakeland B.S.Laskar J.Latham D.W.,Lecavelier des Etangs A.Leleu A.Lendl M.de Leon J.Lienhard F.,Lopez-Morales M.Lovis C.Lund M.B.Luque R.Magrin D.Malavolta L.,Martinez Fiorenzano A.F.Mayo A.W.Mayor M.Mordasini C.Mortier A.,Murgas F.Narita N.Nascimbeni V.Nicholson B.A.Olofsson G.,Ottensamer R.Pagano I.Palethorpe L.Palle E.Parviainen H.Pedani M.,Pepe F.A.Peter G.Pinamonti M.Piotto G.Pollacco D.Poretti E.,Queloz D.Quinn S.N.Ragazzoni R.Rando N.Rapetti D.Ratti F.,Rauer H.Rescigno F.Ribas I.Rice K.Ricker G.R.Robertson P.,de Roche T.Sabin L.Santos N.C.Sasselov D.D.Savel A.B.,Scandariato G.Schanche N.Schroffenegger U.Schwarz R.P.Seager S.,Sefako R.Segransan D.Shporer A.Silva A.M.Smith A.M.S.,Sozzetti A.Steller M.Szabo G.M.Tamura M.Thomas N.Tuson A.,Udry S.Vanderburg A.Vanderspek R.K.Venturini J.Verrecchia F.,Walton N.A.Watson C.A.Wells R.D.Winn J.N.Zambelli R.Ziegler C.2026-08-13T10:36:27Z2026-08-13T11:12:49ZCDS support team

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

cds-question@unistra.frmultiple-starsm-starsdwarf-starsexoplanetsradial-velocityphotometryvisible-astronomySmall exoplanet radii show two populations, referred to as super-Earths and sub-Neptunes, separated by a gap known as the radius valley. This may be produced by the removal of atmospheres due to stellar or internal heating, or lack of an initial envelope. We use transit photometry and radial velocity measurements to detect and characterize four planets orbiting LHS 1903, a red dwarf (M-dwarf) star in the Milky Way's thick disk. The planets have orbital periods between 2.2 and 29.3 days, and span the radius valley within a single planetary system. The derived densities indicate that LHS 1903 b is rocky, while LHS 1903 c and LHS 1903 d have extended atmospheres. 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