J/A+A/682/A29ivo://CDS.VizieR/J/A+A/682/A29doi:10.26093/cds/vizier.36820029CDSFenucci M.Micheli M.Gianotto F.Faggioli L.Oliviero D.Porru A.,Rudawska R.Cano J.L.Conversi L.Moissl R.2024-11-07T20:01:09Z2024-02-01T08:28:08ZCDS support team

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

cds-question@unistra.frsolar-systemasteroidsThe measurement of the Yarkovsky effect on near-Earth asteroids (NEAs) is common practice in orbit determination today, and the number of detections will increase with the developments of new and more accurate telescopic surveys. However, the process of finding new detections and identifying spurious ones is not yet automated, and it often relies on personal judgment. We aim to introduce a more automated procedure that can search for NEA candidates to measure the Yarkovsky effect, and that can identify spurious detections. The expected semi-major axis drift on an NEA caused by the Yarkovsky effect was computed with a Monte Carlo method on a statistical model of the physical parameters of the asteroid that relies on the most recent NEA population models and data. The expected drift was used to select candidates in which the Yarkovsky effect might be detected, according to the current knowledge of their orbit and the length of their observational arc. Then, a nongravitational acceleration along the transverse direction was estimated through orbit determination for each candidate. If the detected acceleration was statistically significant, we performed a statistical test to determine whether it was compatible with the Yarkovsky effect model. Finally, we determined the dependence on an isolated tracklet. Among the known NEAs, our procedure automatically found 348 detections of the Yarkovsky effect that were accepted. The results are overall compatible with the predicted trend with the the inverse of the diameter, and the procedure appears to be efficient in identifying and rejecting spurious detections. This algorithm is now adopted by the ESA NEO Coordination Centre to periodically update the catalogue of NEAs with a measurable Yarkovsky effect, and the results are automatically posted on the web portal.2024A&A...682A..29Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/682/A29CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/astorb : Orbits of Minor Planets (Bowell+, 2014-)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/682/A29https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/682/A29http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/682/A29https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/682/A29https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/682/A29http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/682/A29GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/682/A29/tableb1Determinations of A2 with S/N>3recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAsteroidName of the asteroidmeta.id;meta.maincharHAbsolute magnitudemagphys.magAbsfloatRMSRMS of normalized residuals, 7D ODstat.fit.residual;arith.ratiodoubleRMS6DRMS of normalized residuals, 6D ODstat.fit.residual;arith.ratiodoubleA2Transversal acceleration componentau.d**-2stat.fit.paramdoublee_A2Error in A2au.d**-2stat.errordoubleda/dtSemi-major axis driftau/Myrsrc.orbitaldoublee_da/dtError in da/dtau/Myrstat.errordoublemax(da/dt)Maximum da/dt from Monte Carlo modelau/Myrsrc.orbitaldoubleSNRSignal-to-noise of A2 detectionstat.snrdoubleFAccept[1 Rej.] Flag for acceptance of the detectionmeta.codecharNOptObsNumber of optical observationsmeta.numberintNRejOptNumber of rejected optical observations in 7D ODmeta.numberintNRej6DNumber of rejected optical observations in 6D ODmeta.numberintNRadObsNumber of radar observationsmeta.numberintNRejRadNumber of rejected radar obs in 7D ODmeta.numberintNRejRad6DNumber of rejected radar obs in 6D ODmeta.numberintNOptOldNumber of old observationsmeta.numberintDlow15-th percentile of diametermphys.size.diameterdoubleDmed50-th percentile of diametermphys.size.diameterdoubleDhigh85-th percentile of diametermphys.size.diameterdoubleModFlag[0/1] Flag for model used in Monte Carlometa.codeintProt? Rotation period of the asteroidhtime.periodfloatnullableTaxTaxonomic complex of the asteroidsrc.classchardeltatLength of observational arcyrtime;arith.difffloatJ/A+A/682/A29/tableb2Comparisons with JPL datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAsteroidName of the asteroidmeta.id;meta.maincharA2Transversal acceleration from NEOCCau.d**-2stat.fit.paramdoublee_A2Error in A2 from NEOCCau.d**-2stat.errordoubleSNRSignal-to-noise of A2 from NEOCCstat.snrdoubleA2j? Transversal acceleration from JPLau.d**-2stat.fit.paramdoublenullablee_A2j? Error in A2 from JPLau.d**-2stat.errordoublenullableSNRj? Signal-to-noise of A2 from JPLstat.snrdoublenullableModel[1/3]? Dynamical model of JPLmeta.id;stat.fitintnullableErr1? Relative error of JPL determinationstat.errordoublenullableErr2? Relative error of NEOCC determinationstat.errordoublenullablechiA2? Chi value of determinationstat.fit.chi2doublenullableJ/A+A/682/A29/tableb3Comparisons with JPL data not accepted or not found by NEOCCrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAsteroidName of the asteroidmeta.id;meta.maincharda/dt(NEOCC)? Semi-major axis drift from NEOCCau/Myrsrc.orbitaldoublenullablee_da/dt(NEOCC)? Error of NEOCC determinationau/Myrstat.errordoublenullableSNR(NEOCC)? Signal-to-noise of NEOCC determinationstat.snrdoublenullableYM? Maximum da/dt from Monte Carlo modelsrc.orbitaldoublenullableda/dt(JPL)Semi-major axis drift from JPLau/Myrsrc.orbitaldoublee_da/dt(JPL)Error of JPL determinationau/Myrstat.errordoubleSNR(JPL)Signal-to-noise of JPL determinationstat.snrdoubleModel[1/3] Dynamical model used by JPLmeta.id;stat.fitint