J/A+A/688/A211ivo://CDS.VizieR/J/A+A/688/A211doi:10.26093/cds/vizier.36880211CDSLeleu A.Delisle J.-B.Delrez L.Bryant E.M.Brandeker A.Osborn H.P.,Hara N.Wilson T.G.Billot N.Lendl M.Ehrenreich D.Chakraborty H.,Guenther M.N.Hooton M.J.Alibert Y.Alonso R.Alves D.R.,Anderson D.R.Apergis I.Armstrong D.Barczy T.Barrado Navascues D.,Barros S.C.Battley M.P.Baumjohann W.Bayliss D.Beck T.Benz W.,Borsato L.Broeg C.Burleigh M.R.Casewell S.L.Collier Cameron A.,Correia A.C.M.Csizmadia Sz.Cubillos P.E.Davies M.B.Deleuil M.,Deline A.Demangeon O.D.S.Demory B.-O.Derekas A.Edwards B.,Erikson A.Fortier A.Fossati L.Fridlund M.Gandolfi D.Gazeas K.,Gillen E.Gillon M.Goad M.R.Guedel M.Hawthorn F.Heitzmann A.,Helling Ch.Isaak K.G.Jenkins J.S.Jenkins J.M.Kendall A.Kiss L.,Korth J.Lam K.W.F.Laskar J.Latham D.W.Lecavelier des Etangs A.,Magrin D.Maxted P.F.L.McCormac J.Mordasini C.Moyano M.,Nascimbeni V.Olofsson G.Osborn A.Ottensamer R.Pagano I.Palle E.,Peter G.Piotto G.Pollacco D.Queloz D.Ragazzoni R.Rando N.,Rauer H.Ribas I.Ricker G.Saha S.Santos N.C.Scandariato G.,Seager S.Segransan D.Simon A.E.Smith A.M.S.Sousa S.G.Stalport M.,Sulis S.Szabo M.Gy.Udry S.Ulmer-Moll S.Van Grootel V.,Vanderspek R.Venturini J.Villaver E.Vines J.I.Walton N.A.,West R.G.Wheatley P.J.Winn J.Zivave T.2024-11-21T20:02:48Z2024-08-26T07:11:51ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsorbitsphotometryvisible-astronomyThe TOI-178 system consists of a nearby, late-K-dwarf with six transiting planets in the super-Earth to mini-Neptune regime,with radii ranging from ~1.1 to 2.9R_{Earth}_ and orbital periods between 1.9 and 20.7 days. All the planets, but the innermost one, form a chain of Laplace resonances. Mass estimates derived from a preliminary radial velocity (RV) dataset suggest that the planetary densities do not decrease in a monotonic way with the orbital distance to the star,contrary to what one would expect based on simple formation and evolution models. The fine-tuning and fragility of such orbital configurations ensure that no significant scattering or collision event has taken place since the {formation and migration} of the planets in the protoplanetary disc, thereby providing important anchors for planet formation models. We aim to improve the characterisation of the architecture of this key system and, in particular, the masses and radii of its planets. In addition, since this system is one of the few resonant chains that can be characterised by both photometry and radial velocities, we propose to use it as a test bench for the robustness of the planetary mass determination with each technique. We performed a global analysis of all the available photometry from CHEOPS, TESS and NGTS, and radial velocity from ESPRESSO, using a photo-dynamical modelling of the light curve. We also tried different sets of priors on the masses and eccentricity, as well as different stellar activity models, to study their effects on the masses estimated by transit-timing variations (TTVs) and radial velocities (RVs). We demonstrate how stellar activity prevents a robust mass estimation for the three outer planets using radial velocity data alone.We also show that our joint photo-dynamical and radial velocity analysis has resulted in a robust mass determination for planets c to g, with precision of ~12% for the mass of planet c, and better than 10% for planets $d$ to g. The new precisions on the radii range from 2 to 3%. The understanding of this synergy between photometric and radial velocity measurements will be valuable for the PLATO mission. We also show that TOI-178 is indeed currently locked in the resonant configuration, librating around an equilibrium of the chain.2024A&A...688A.211Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/688/A211CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/649/A26 : TOI-178 six transiting planets (Leleu+, 2021)J/A+A/678/A200 : TOI-178 raw and detrended photometry (Delrez+, 2023)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/688/A211https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/688/A211http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/688/A211https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/688/A211https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/688/A211http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/688/A211GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/688/A211/eulerdDetrended Euler datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeDate of the observation (BJD)dtime.epochdoublee_FluxNormalised flux errorstat.error;phot.fluxdoubleFluxDetNormalised detrended fluxphot.flux;arith.ratiodoubleFluxNormalised raw fluxphot.flux;arith.ratiodoubleJ/A+A/688/A211/samples*Planetary and stellar parameters samples the joint photo-dynamical+RV fith0ecc * sin (long of pericenter) planet csrc.orbital.eccentricitydoubleP0Orbital period planet cdtime.perioddoublek0ecc * cos (long of pericenter) planet csrc.orbital.eccentricitydoublelambda1Mean longitude planet ddegpos.galactic.londoubleP1orbital period planet ddtime.perioddoublek1ecc * cos (long of pericenter) planet dsrc.orbital.eccentricitydoubleh1ecc * sin (long of pericenter) planet dsrc.orbital.eccentricitydoublem1Mass planet dsolMassphys.massdoublelambda2Mean longitude planet edegpos.galactic.londoubleP2Orbital period planet edtime.perioddoublek2ecc * cos (long of pericenter) planet esrc.orbital.eccentricitydoubleh2ecc * sin (long of pericenter) planet esrc.orbital.eccentricitydoublem2Mass planet esolMassphys.massdoublelambda3Mean longitude planet fdegpos.galactic.londoubleP3Orbital period planet fdtime.perioddoublek3ecc * cos (long of pericenter) planet fsrc.orbital.eccentricitydoubleh3ecc * sin (long of pericenter) planet fsrc.orbital.eccentricitydoublem3mass planet fsolMassphys.massdoublelambda4Mean longitude planet gdegpos.galactic.londoubleP4Orbital period planet gdtime.perioddoublek4ecc * cos (long of pericenter) planet gsrc.orbital.eccentricitydoubleh4ecc * sin (long of pericenter) planet gsrc.orbital.eccentricitydoublem4Mass planet gsolMassphys.massdoubleR0Radius planet c, in star radiusphys.size.radius;arith.ratiodoubleR1Radius planet d, in star radiusphys.size.radius;arith.ratiodoubleR2Radius planet e, in star radiusphys.size.radius;arith.ratiodoubleR3Radius planet f, in star radiusphys.size.radius;arith.ratiodoubleR4Radius planet g, in star radiusphys.size.radius;arith.ratiodoubleb0Impact parameter planet cstat.fit.paramdoubleb1Impact parameter planet dsrc.impactParamdoubleb2Impact parameter planet esrc.impactParamdoubleb3Impact parameter planet fstat.fit.paramdoubleb4Impact parameter planet gsrc.impactParamdoublerhoDensity of the starSunsrc.densitydoubleRstarRadius of the starsolRadphys.size.radiusdoublet0circ0Date of transit of planet b (BJD-2457000)dtime.epochdoublePcirc0Orbital period of planet bdtime.perioddoubleRcirc0Radius of planet b, in star radiusphys.size.radius;arith.ratiodoublebcirc0Impact parameter of planet bsrc.impactParamdoublemcirc0Mass of planet bsolMassphys.massdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda0Mean longitude planet cdegpos.galactic.londoublem0Mass planet csolMassphys.massdoubleJ/A+A/688/A211/timingsTransit timings and errors from the final posterior of the joint photo-dynamical+RV fitrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of the transiting planetmeta.id;meta.maincharDateMedian transit date, BJD-2457000.0dtime.epoch;stat.mediandoublee_DateDate 0.15865 quantile, BJD-2457000.0dstat.error;time.epochdoubleE_DateDate 0.84135 quantile, BJD-2457000.0dstat.error;stat.maxdoubleJ/A+A/688/A211/cheopsprRaw CHEOPS data extracted by PIPEFluxRaw flux normalized by dividing by the median of the raw flux over the visitphot.flux;arith.ratiodoublee_FluxRaw flux error normalized by dividing by the median of the raw flux over the visitstat.error;phot.fluxdoubleRollAngleCHEOPS roll angleradpos.posAngdoubleYCPosition of the centroid along the Y direction, normalised by deducing its mean value and dividing it by its standard deviation over the visitpos.cartesian.y;instr.detdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDateDate of the observation (BJD-2457000)dtime.epochdoubleindexedTemp2Telescope tube temperature, normalised by deducing its mean value and dividing it by its standard deviation over the visitphys.temperaturedoubleBGBackground contamination, normalised by deducing its mean value and dividing it by its standard deviation over the visitinstr.backgrounddoubleJ/A+A/688/A211/cheopsdDetrended CHEOPS dataFluxDetrended normalised fluxphot.flux;arith.ratiodoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDateDate of the observation (BJD-2457000)dtime.epochdoubleindexede_FluxDetrended normalised flux errorstat.error;phot.fluxdoubleJ/A+A/688/A211/ngtsdDetrended NGTS datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDateDate of the observation (BJD-2457000)dtime.epochdoubleindexedFluxDetrended normalised fluxphot.flux;arith.ratiodoublee_FluxDetrended normalised flux errorstat.error;phot.fluxdoubleJ/A+A/688/A211/tessdDetrended TESS datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDateDate of the observation (BJD-2457000)dtime.epochdoubleindexedFluxDetrended normalised fluxphot.flux;arith.ratiodoublee_FluxDetrended normalised flux errorstat.error;phot.fluxdoubleJ/A+A/688/A211/ngtsrRaw NGTS datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDateDate of the observation (BJD-2457000)dtime.epochdoubleindexedFluxRaw flux normalized by dividing by the median of the raw flux over the visitphot.flux;arith.ratiodoublee_FluxRaw flux error normalized by dividing by the median of the raw flux over the visitstat.error;phot.fluxdoubleAirmassAirmass, normalised by deducing its mean value and dividing it by its standard deviation over the visitobs.airMassdouble