J/A+A/659/A135ivo://CDS.VizieR/J/A+A/659/A135doi:10.26093/cds/vizier.36590135CDSPearce T.D.Launhardt R.Ostermann R.Kennedy G.M.Gennaro M.,Booth M.Krivov A.V.Cugno G.Henning T.K.Quirrenbach A.,Barcucci A.M.Matthews E.C.Ruh H.L.Stone J.M.2023-01-30T11:32:25Z2022-09-28T13:03:24ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsstellar-massesstellar-agesgalaxy-classification-systemsvisible-astronomyWe know little about the outermost exoplanets in planetary systems because our detection methods are insensitive to moderate-mass planets on wide orbits. However, debris discs can probe the outer-planet population because dynamical modelling of observed discs can reveal properties of perturbing planets. We use four sculpting and stirring arguments to infer planet properties in 178 debris-disc systems from the ISPY, LEECH, and LIStEN planet-hunting surveys. Similar analyses are often conducted for individual discs, but we consider a large sample in a consistent manner. We aim to predict the population of wide-separation planets, gain insight into the formation and evolution histories of planetary systems, and determine the feasibility of detecting these planets in the near future. We show that a 'typical' cold debris disc likely requires a Neptune- to Saturn-mass planet at 10-100 au, with some needing Jupiter-mass perturbers. Our predicted planets are currently undetectable, but modest detection-limit improvements (e.g. from JWST) should reveal many such perturbers. We find that planets thought to be perturbing debris discs at late times are similar to those inferred to be forming in protoplanetary discs, so these could be the same population if newly formed planets do not migrate as far as currently thought. Alternatively, young planets could rapidly sculpt debris before migrating inwards, meaning that the responsible planets are more massive (and located farther inwards) than debris-disc studies assume. We combine self-stirring and size-distribution modelling to show that many debris discs cannot be self-stirred without having unreasonably high masses; planet- or companion-stirring may therefore be the dominant mechanism in many (perhaps all) debris discs. Finally, we provide catalogues of planet predictions and identify promising targets for future planet searches.2022A&A...659A.135Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/659/A135CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/659/A135https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/659/A135http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/659/A135https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/659/A135https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/659/A135http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/659/A135GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/659/A135/tablea1 (System parameters used in this paper)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/659/A135/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/659/A135/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/659/A135/tablea1?GETtext/xml+votable180.050000true129.7319278-52.96435530.0055555555555555566/155 350 2340 2690 2816 5311 6082 6766 7227 7332 7763 8357 8571 8687 8717 8788 9331 10568 10695 10812 11844 11910 11917 11946 12467 12592 12848 13313 15946 16543 16606 17266 17421 17425 17486 17552 17607 17887 17953 18455 18797 19192 19509 19585 19598 20125 20166 20328 20657 21082-21083 21177 21285 21289 21386 21788 22067 22146 22334 22773 23140 23190 23376 23408 23502 24019 24221 24924 25056 26216 27163 27395 27735 27884 28041 28737 30467 31399 31776 32087 32491 33500 33508 33694 33976 34164 34168 34244 34508 34680 34683 34823 34825 34905 34947 34993 35064 35474 35753 36130 36288 36487 36664 36697 36713 37231 37787 37816 37953 37968 38151 38765 38924 38932 39693 39735 40692 40932 41361 41607 41759 42174 42296 42555 42601 42613 42910 43029 43037 43059 43095 43139 43166 43168 43171 43197 43202 43224 43244 43292 43298 43308 43369 43433 43492 43527 43540 43809 44052 44069 44106 44321 44359 44368 44921 45247 45351 45412 45430 45746 46113 46297 46640 46734 46908 46987 47061 47205 47414 47464-47465 47758 48055 48274 48334 48651https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/659/A135?format=asciiOpticaldefaultJ/A+A/659/A135/tablea1System parameters used in this paperrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSimbadSimbad column added by the CDSmeta.ref.urlcharSystemSystem namemeta.id;meta.maincharNameOther Namemeta.idcharDistDistancepcpos.distancefloate_DistDistance 1{sigma} errorpcstat.errorfloatlog10(L*)Stellar luminositylog(solLum)phys.luminosityfloatTeffEffective temperatureKphys.temperature.effectiveinte_log10(L*)Stellar luminosity 1{sigma} errorlog(solLum)stat.errorfloate_TeffEffective temperature 1{sigma} errorKstat.error;phys.temperature.effectiveintM*Stellar masssolMassphys.massfloatE_M*Stellar mass 1{sigma} error (upper value)solMassstat.error;stat.maxfloate_M*Stellar mass 1{sigma} error (lower value)solMassstat.errorfloatAgeRefAge reference(s) (3)meta.bibchart*Stellar ageMyrtime.ageintE_t*Stellar age 1{sigma} error (upper value)Myrstat.error;stat.maxinte_t*Stellar age 1{sigma} error (lower value)Myrstat.errorintrSED? Corrected blackbody radius (for disc location is estimated from SED data) (2)auphys.angSize;srcfloatnullablee_rSED? Corrected blackbody radius 1{sigma} error (for disc location is estimated from SED data)austat.errorfloatnullableai? Disc inner edge (for disc resolved and fitted with an axisymmetric model) (2)ausrc.orbitalfloatnullableE_ai? ai 1{sigma} error (upper value)austat.error;stat.maxfloatnullablee_ai? ai 1{sigma} error (lower value)austat.errorfloatnullableao? Disc outer edge (for disc resolved and fitted with an axisymmetric model) (2)ausrc.orbitalfloatnullableE_ao? ao 1{sigma} error (upper value)austat.error;stat.maxfloatnullablee_ao? ao 1{sigma} error (lower value)austat.errorfloatnullableqi? Inner edge pericentre (for disc resolved and fitted with an asymmetric model) (2)ausrc.orbitalfloatnullableE_qi? qi 1{sigma} error (upper value)austat.error;stat.maxfloatnullablee_qi? qi 1{sigma} error (lower value)austat.errorfloatnullableQi? Inner edge apocentre (for disc resolved and fitted with an asymmetric model) (2)ausrc.orbitalfloatnullableE_Qi? Qi 1{sigma} error (upper value)austat.error;stat.maxfloatnullablee_Qi? Qi 1{sigma} error (lower value)austat.errorfloatnullableqo? Outer edge pericentre (for disc resolved and fitted with an asymmetric model) (2)ausrc.orbitalfloatnullableE_qo? qo 1{sigma} error (upper value)austat.error;stat.maxfloatnullablee_qo? qo 1{sigma} error (lower value)austat.errorfloatnullableQo? Outer edge apocentre (for disc resolved and fitted with an asymmetric model) (2)ausrc.orbitalfloatnullableE_Qo? Qo 1{sigma} error (upper value)austat.error;stat.maxfloatnullablee_Qo? Qo 1{sigma} error (lower value)austat.errorfloatnullableDiscDataData source used to determine the debris disc properties (plus PACS wavelength for Herschel data)meta.bibchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainn_System[*] Note on System (1)meta.notecharJ/A+A/659/A135/tablea2Planet and debris disc constraints calculated in this paperep? Planet minimum eccentricity (1)src.orbital.eccentricityfloatnullableE_ep? Error on ep (upper value)stat.error;stat.maxfloatnullablee_ep? Error on ep (lower value)stat.errorfloatnullableQpMaximum apocentre distance that a single planet requires to sculpt the disc inner edgearcsecsrc.orbitalfloatE_QpError on Qp (upper limit)arcsecstat.error;stat.maxfloate_QpError on Qp (lower limit)arcsecstat.errorfloatMpnMinimum mass that each individual planet requires if instead multiple planets sculpt the disc inner edge(1.898187x10+27kg)phys.massdoubleE_MpnError on Mpn (upper value)(1.898187x10+27kg)stat.error;stat.maxdoublee_MpnError on Mpn (lower value)(1.898187x10+27kg)stat.errordoublerPnMaximum projected separation of the outermost planet in the multi-planet scenarioarcsecpos.angDistance;src.orbitalfloatE_rPnError on rPn (upper value)arcsecstat.error;stat.maxfloate_rPnError on rPn (lower value)arcsecstat.errorfloatMpstirMinimum mass that a planet requires to stir the disc, assuming the planet eccentricity is <=0.3(1.898187x10+27kg)phys.massdoubleE_MpstirError on Mpstir (upper value)(1.898187x10+27kg)stat.error;stat.maxdoublee_Mpstir? Error on Mpstir (lower value)(1.898187x10+27kg)stat.errordoublenullableMdiscstir? Minimum mass that the disc requires to self-stir (2)(5.97236x10+24kg)phys.massfloatnullableE_Mdiscstir? Error on Mdiscstir (upper value)(5.97236x10+24kg)stat.error;stat.maxfloatnullablee_Mdiscstir? Error on Mdiscstir (lower value)(5.97236x10+24kg)stat.errorfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSystemSystem namemeta.id;meta.maincharMpPlanet minimum mass that a single planet requires to sculpt the disc inner edge(1.898187x10+27kg)phys.massfloatE_MpError on Mp (upper value)(1.898187x10+27kg)stat.error;stat.maxfloate_MpError on Mp (lower value)(1.898187x10+27kg)stat.errorfloatapPlanet maximum semi-major axis that a single planet requires to sculpt the disc inner edgeauphys.angSize;srcfloatE_apError on ap (upper value)austat.error;stat.maxfloate_apError on ap (lower value)austat.errorfloat