J/AJ/152/111ivo://CDS.VizieR/J/AJ/152/111doi:10.26093/cds/vizier.51520111CDSAlexandersen M.Gladman B.Kavelaars J.J.Petit J.-M.Gwyn S.D.J.,Shankman C.J.Pike R.E.2017-05-22T15:09:03Z2017-04-21T13:26:51ZCDS support team

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

cds-question@unistra.frsolar-systemasteroidssurveysapparent-magnitudeThe trans-Neptunian objects (TNOs) preserve evidence of planet building processes in their orbital and size distributions. While all populations show steep size distributions for large objects, a relative deficit of Neptunian trojans and scattering objects with diameters of D<100km has been detected. We investigated this deficit with a 32 square degree survey, in which we detected 77 TNOs that are brighter than a limiting r-band magnitude of 24.6. Our plutino sample (18 objects in 3:2 mean-motion resonance with Neptune) shows a deficit of D<100km objects, rejecting a single power-law size distribution at >99% confidence. Combining our survey with the Canada-France Ecliptic Plane Survey, we perform a detailed analysis of the allowable parameters for the plutino size distribution, including knees and divots. We surmise the existence of 9000+/-3000 plutinos with an absolute magnitude of H_r_{<=}8.66 and 37000_-10000_^+12000^ with H_r_{<=}10.0 (95% confidence). Our survey also discovered one temporary Uranian trojan, one temporary Neptunian trojan, and one stable Neptunian trojan, for which we estimate populations of 110_-100_^+500^, 210_-200_^+900^, and 150_-140_^+600^ with H_r_{<=}10.0, respectively. All three populations are thus less numerous than the main belt asteroids (592 asteroids with H_r_{<=}10.0). With such population sizes, the temporary Neptunian trojans cannot be previously stable trojans diffusing out of the resonance now; they must be recently captured Centaurs or scattering objects. As the bias against the detection of objects grows with larger semimajor axes, our discovery of three 3:1 resonators and one 4:1 resonator adds to the growing evidence that the high-order resonances are far more populated than is typically predicted.2016AJ....152..111Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/152/111CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/astorb : Orbits of Minor Planets (Bowell+ 2014)http://www.minorplanetcenter.net/iau/MPCORB.html : MPC databasehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/152/111https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/152/111http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/152/111https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/152/111https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/152/111http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/152/111GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tap2.925376584943135e-19 3.4952848286853267e-19defaultJ/AJ/152/111/table3List of all objects detected in our surveyQ[0/10] Q resonance indexsrc.orbitalintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDInternal object designation (1)meta.id;meta.maincharOIDOld internal designation (2)meta.idcharMPCMinor Planet Center (MPC) designation (3)meta.idcharEpoch[5803/6221.9] Epoch (JD-2450000) (4)dtime.epochfloatJD[5858.9/6221.9] Julian Date at discovery (JD-2450000)dtime.epochfloatDist[20/52.7] Heliocentric distance at discovery (r)AUpos.distance;pos.heliocentricfloate_Dist[0/5.135] Uncertainty in DistAUstat.errorfloatNobs[3/43] Number of astrometric measurements (N)meta.numberintTime[0.0002/2.4] Arc length: time from first to last observation (t)yrsrc.orbitalfloata[19/92.4] Semi-major axis (5)AUphys.size.smajAxisdoublee_a[0.0009/25] Uncertainty in a (6)AUstat.errordoublee[0.01/0.62] Eccentricity (5)src.orbital.eccentricitydoublee_e[0/0.58] Uncertainty in e (6)stat.errordoublei[1.2/53.9] Inclination (5)degsrc.orbital.inclinationfloate_i[0/25.4] Uncertainty in i (6)degstat.errorfloatOmega[4.8/358.4] Longitude of ascending node ({Omega}) (5)degsrc.orbital.nodefloate_Omega[0/303.6] Uncertainty in Omega (6)degstat.errorfloatomega[2.9/352.2] Argument of pericenter ({omega}) (5)degsrc.orbital.periastronfloate_omega[0.011/1789] Uncertainty in omega (6)degstat.errordoubleM[0.6/360] Mean anomaly measured at JD epoch (5)degsrc.orbital.meanAnomalyfloate_M[0/34.3] Uncertainty in M (6)degstat.errorfloat<rmag>[21.5/24.9] Average apparent magnitude in CFHT/MegaCam r-band (m_r_) (7)magphot.mag;em.opt.Rfloate_<rmag>[0/0.262] Uncertainty in rmagmagstat.error;phot.mag;em.opt.RfloatrMag[5.58/10.65] Absolute magnitude in CFHT/MegaCam r-band; phase corrected (H_r_) (8)magphys.magAbsfloatMotion[2.53/6.27] Rate of motion at discoveryarcsec/harith.rate;phys.veloc;src.orbital.meanMotionfloatalpha[0.034/0.777] Phase angle at discovery ({alpha})degpos.phaseAngfloatC[0/1] Characterization flag (1=characterized, or 0=uncharacterized) (9)meta.code.classintS[NSI] Security of the classification (N=not classified, I=insecure, or S=secure)meta.code.classcharClassClassification type (classical, detached, notclass, or resonant)src.classcharf_Class[0NUimo] Additional classification flag (type of resonant, or type of classical) (10)meta.codecharP[0/19] P resonance indexsrc.orbitalintCbf[60/180]? Libration center of best-fit clone (C_bf_) (11)deginstr.offsetintnullableCmx[60/180]? Libration center of max-a clone (C_mx_) (11)deginstr.offsetintnullableCmn[60/180]? Libration center of min-a clone (C_mn_) (11)deginstr.offsetintnullableLbf[12/170]? Libration amplitude of best-fit clone (L_bf_) (11)deginstr.offsetintnullableLmx[13/150]? Libration amplitude of max-a clone (L_mx_) (11)deginstr.offsetintnullableLmn[14/164]? Libration amplitude of min-a clone (L_mn_) (11)deginstr.offsetintnullableCLK[90/270]? Lidov-Kozai libration center (C_LK_)deginstr.offsetintnullableLLKbf[40/85]? Lidov-Kozai libration amplitude of best-fit clone (L_LKbf_)deginstr.offsetfloatnullableLLKmx[40/57]? Lidov-Kozai libration amplitude of max-a clone (L_LKmx_)deginstr.offsetfloatnullableLLKmn[40/83]? Lidov-Kozai libration amplitude of min-a clone (L_LKmn_)deginstr.offsetfloatnullablesigma5[1.6/13000] Long-axis of on-sky uncertainty ellipse 5 years after 1st observation ({sigma}_5_) (12)arcsecstat.errorfloatsigma10[8/30000] Long-axis of on-sky uncertainty ellipse 10 years after 1st observation ({sigma}_10_) (12)arcsecstat.errorintComComments (13)meta.notechar