J/AJ/163/179ivo://CDS.VizieR/J/AJ/163/179doi:10.26093/cds/vizier.51630179CDSPetigura E.A.Rogers J.G.Isaacson H.Owen J.E.Kraus A.L.Winn J.N.,MacDougall M.G.Howard A.W.Fulton B.Kosiarek M.R.Weiss L.M.,Behmard A.Blunt S.2026-05-22T20:03:49Z2022-05-16T07:43:37ZCDS support team

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

cds-question@unistra.frexoplanetsstellar-radiistellar-ageseffective-temperaturestellar-massesparallaxspectroscopymetallicityvisible-astronomyIn 2017, the California-Kepler Survey (CKS) published its first data release (DR1) of high-resolution optical spectra of 1305 planet hosts. Refined CKS planet radii revealed that small planets are bifurcated into two distinct populations, super-Earths (smaller than 1.5R{Earth}) and sub-Neptunes (between 2.0 and 4.0R{Earth}), with few planets in between (the "radius gap"). Several theoretical models of the radius gap predict variation with stellar mass, but testing these predictions is challenging with CKS DR1 due to its limited M{star} range of 0.8-1.4M{sun}. Here we present CKS DR2 with 411 additional spectra and derived properties focusing on stars of 0.5-0.8M{sun}. We found that the radius gap follows Rp{prop}Pm with m=-0.10{+/-}0.03, consistent with predictions of X-ray and ultraviolet- and core-powered mass-loss mechanisms. We found no evidence that m varies with M{star}. We observed a correlation between the average sub-Neptune size and M{star}. Over 0.5-1.4M{sun}, the average sub-Neptune grows from 2.1 to 2.6R{Earth}, following R_p_{prop}M_star_^{alpha}^ with {alpha}=0.25{+/-}0.03. In contrast, there is no detectable change for super-Earths. These M{star}-Rp trends suggest that protoplanetary disks can efficiently produce cores up to a threshold mass of Mc, which grows linearly with stellar mass according to Mc~10M{Earth}(M_star_/M{sun}). There is no significant correlation between sub-Neptune size and stellar metallicity (over -0.5 to +0.5dex), suggesting a weak relationship between planet envelope opacity and stellar metallicity. Finally, there is no significant variation in sub-Neptune size with stellar age (over 1-10Gyr), which suggests that the majority of envelope contraction concludes after ~1Gyr.2022AJ....163..179Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/163/179CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/345 : Gaia DR2 (Gaia Collaboration, 2018)VI/120 : High-resolution synthetic stellar library (Coelho+, 2005)J/AJ/142/112 : KIC photometric calibration (Brown+, 2011)J/ApJ/767/95 : Improved stellar parameters of small KICstars (Dressing+, 2013)J/ApJ/800/85 : Teff, radii and luminosities of cool dwarfs (Newton+, 2015)J/ApJ/831/125 : ALMA 887{mu}m obs. ChaI star-forming region (Pascucci+, 2016)J/ApJ/825/19 : Mass-radius relationship planets with Rp<4 (Wolfgang+, 2016)J/ApJ/836/167 : K2 planetary syst. around low-mass stars. I. (Dressing+, 2017)J/AJ/154/109 : California-Kepler Survey. III. Planet radii (Fulton+, 2017)J/ApJ/844/102 : KIC star parallaxes from asteroseismology/Gaia (Huber+, 2017)J/ApJS/229/30 : Revised stellar properties Q1-17 Kepler targets (Mathur+, 2017)J/AJ/154/107 : California-Kepler Survey (CKS). I. 1305 stars (Petigura+, 2017)J/ApJ/836/77 : Library of high-S/N optical spectra of FGKM stars (Yee+, 2017)J/ApJ/855/115 : Lithium abundances of KOIs from CKS spectra (Berger+, 2018)J/ApJ/866/99 : Revised radii of KIC stars & planets, Gaia DR2 (Berger+, 2018)J/AJ/156/264 : California-Kepler Survey VII. Planet radius gap (Fulton+, 2018)J/AJ/155/205 : Occurrence rates Q1-Q16 KOI catalog planet cand. (Hsu+, 2018)J/AJ/155/21 : Planet candidates from K2 campaigns 5-8 (Petigura+, 2018)J/AJ/155/89 : California-Kepler Survey (CKS). IV. Planets (Petigura+, 2018)J/ApJS/235/38 : Kepler planetary cand. VIII. DR25 reliability (Thompson+, 2018)J/AJ/155/48 : California-Kepler Survey. V. Masses and radii (Weiss+, 2018)J/ApJ/875/29 : Spectroscopic analysis of the CKS sample. I. (Martinez+, 2019)J/AJ/160/108 : Gaia-Kepler stellar properties cat. II. Planets (Berger+, 2020)J/AJ/159/280 : Gaia-Kepler stellar properties cat.I. KIC stars (Berger+, 2020)J/AJ/160/239 : Cluster difference imaging photo. survey. II. (Bouma+, 2020)J/AJ/159/211 : Exoplanets parameters from Kepler and K2 (Cloutier+, 2020)J/AJ/161/265 : Compared rotation periods 1189 CKS host stars (David+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/163/179https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/163/179http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/163/179https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/163/179https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/163/179http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/163/179GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/163/179/table1 (Stellar properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/163/179/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/163/179/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/163/179/table1?GETtext/xml+votable180.050000true286.8084949.31641420.005555555555555556Cone search capability for table J/AJ/163/179/table2 (Planet properties for the 888 star CXM sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/163/179/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/163/179/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/163/179/table2?GETtext/xml+votable180.050000true286.808491449.31641420.0055555555555555564/922-923 933-935 945-946 5/3645-3647 3683 3704 3706 3729-3731 3776-3778 3788-3789 3792-3793 6/14567 14573 14575 14578-14579 14730-14731 14738 14744 14746 14750-14751 14792 14794-14795 14828 14830 14914-14915 15040-15041 15043-15045 15057 15059-15062 15116 15118-15119 15160-15161 15176 15178 15200 152328.650015785639275e-20 9.710690472292815e-20https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/163/179?format=asciiOpticaldefaultJ/AJ/163/179/table1Stellar propertiesKOI? Kepler Object identifiermeta.id;meta.mainintnullableprimarySimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaia? Gaia DR2 identifiermeta.id.crossnullableKsmag[6.49/14.7] 2MASS Ks band magnitudemagphot.mag;em.IR.Kfloate_Ksmag[0.01/0.2]? Uncertainty in Ksmagmagstat.error;phot.magfloatnullableGplx[-2.97/27.5]? Gaia DR2 parallaxmaspos.parallax.trigfloatnullablee_Gplx[0.01/0.8]? Uncertainty in parmasstat.errorfloatnullableTeff[3395/6662] Surface effective temperatureKphys.temperature.effectiveinte_Teff[70/110] Uncertainty for TeffKstat.error;phys.temperature.effectiveintFeH[-0.85/0.45] Metallicityphys.abund.Fefloate_FeH[0.06/0.09] Uncertainty for FeHstat.errorfloatvsini[0/180]? Projected rotational velocity (1)km/sphys.veloc.rotatfloatnullablerstar[0.36/11.8]? Adopted stellar radius, Stefan-Boltzmann lawsolRadphys.size.radiusfloatnullableE_rstar[0.01/10]? Upper uncertainty on Rstar (2)solRadstat.error;stat.maxfloatnullablee_rstar[-5.5/-0.01]? Lower uncertainty on Rstar (2)solRadstat.errorfloatnullableMstar[0/1.91]? Stellar mass (3)solMassphys.massfloatnullableE_Mstar[0/0.5]? Upper uncertainty on Mstar (2)solMassstat.error;stat.maxfloatnullablee_Mstar[-0.8/0]? Lower uncertainty on Mstar (2)solMassstat.errorfloatnullableRstar[0/11.2]? Stellar Radius (3)solRadphys.size.radiusfloatnullableE_Rstar[0/4]? Upper uncertainty on Rstar (2)solRadstat.error;stat.maxfloatnullablee_Rstar[-2/0]? Lower uncertainty on Rstar (2)solRadstat.errorfloatnullablerho[0/7.09]? Stellar density (3)g.cm**-3src.densityfloatnullableE_rho[0/2]? Upper uncertainty on rho (2)g.cm**-3stat.error;stat.maxfloatnullablee_rho[-2/0]? Lower uncertainty on rho (2)g.cm**-3stat.errorfloatnullableage[0/19.5]? Age, Gyr (3)Gyrtime.agefloatnullableE_age[0/12]? Upper uncertainty on age (2)Gyrstat.error;stat.maxfloatnullablee_age[-8/0]? Lower uncertainty on age (2)Gyrstat.error;time.agefloatnullableplx[0.08/33.1]? Spectroscopic parallax (3)maspos.parallax.spectfloatnullableE_plx[0.01/5]? Upper uncertainty on (2)masstat.error;stat.maxfloatnullablee_plx[-193/-0.01]? Lower uncertainty on (2)masstat.error;pos.parallaxfloatnullableprovMethod for Teff, FeH, vsini values (4)meta.notecharSB2[1/5] Limits on spectroscopic binaries (5)meta.code.multipintCXM[0/1] In the CKS Extended Mass subset?meta.codeint_RAPosition from SIMBAD (right ascension part)degpos.eq.ra;meta.mainnullable_DEPosition from SIMBAD (declination part)degpos.eq.dec;meta.mainnullableJ/AJ/163/179/table2Planet properties for the 888 star CXM sampleSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPlanetPlanet identifiermeta.id;meta.maincharPer[0.25/506] Orbital Period (1)dtime.perioddoubleE_Per[3e-08/0.03] Upper uncertainty on Per (1)dstat.error;stat.maxdoublee_Per[-0.03/-3e-08] Lower uncertainty on Per (1)dstat.errordoubleRp/Rs[0.4/7469] Ratio, Planet to Star Radius (1)%phys.size;arith.ratiodoubleE_Rp/Rs[0.001/2251] Upper uncertainty on Rp/Rstar (1)%stat.error;stat.maxdoublee_Rp/Rs[-2251/-0.001] Lower uncertainty on Rp/Rstar (1)%stat.errordoubleT[0.37/22.5]? Transit duration, hours (1)htime.intervalfloatnullableE_T[0.0004/7]? Upper uncertainty on T (1)hstat.error;stat.maxfloatnullablee_T[-7/-0.0004]? Lower uncertainty on T (1)hstat.errorfloatnullableRp[0.41/6063] Planet Radius from Rp/Rs and Rstar(6.3781x10+6m)phys.size.radiusfloatE_Rp[0.03/2347] Upper uncertainty on Rp(6.3781x10+6m)stat.error;stat.maxfloate_Rp[-2347/-0.03] Lower uncertainty on Rp(6.3781x10+6m)stat.errordoubleTmax[0.86/24.1] Expected duration of a centrally transiting object on a circular orbithtime.durationfloatE_Tmax[0.02/0.8] Upper uncertainty on Tmaxhstat.error;stat.maxfloate_Tmax[-0.8/-0.02] Lower uncertainty on Tmaxhstat.errorfloata[0.006/1.15] semi-major axis, au (2)auphys.angSize.smajAxis;src.orbitalfloatE_a[0.0001/0.02] Upper uncertainty on a (2)austat.error;stat.maxfloate_a[-0.02/-0.0001] Lower uncertainty on a (2)austat.errorfloatS[0.14/5949] Incident bolometric flux, Earth unit (2)phot.flux.boldoubleE_S[0.01/609] Upper uncertainty on S (2)stat.error;stat.maxdoublee_S[-609/-0.01] Lower uncertainty on S (2)stat.errordoubleSamp[0/1] In curated list of 970 planets; Section 5meta.codeint_RAPosition from SIMBAD (right ascension part)degpos.eq.ra;meta.mainnullable_DEPosition from SIMBAD (declination part)degpos.eq.dec;meta.mainnullable