VII/288ivo://CDS.VizieR/VII/288CDSMahlke M.Carry B.Denneau L.2021-04-27T11:04:58Z2020-09-21T13:23:43ZCDS support team

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

cds-question@unistra.frasteroidsccd-photometryAsteroid phase curves are used to derive fundamental physical properties through the determination of the absolute magnitude H. The upcoming visible Legacy Survey of Space and Time (LSST) and mid-infrared Near-Earth Object Surveillance Mission (NEOSM) surveys rely on these absolute magnitudes to derive the colours and albedos of millions of asteroids. Furthermore, the shape of the phase curves reflects their surface compositions, allowing for conclusions on their taxonomy. We derive asteroid phase curves from dual-band photometry acquired by the Asteroid Terrestrial-impact Last Alert System telescopes. Using Bayesian parameter inference, we retrieve the absolute magnitudes and slope parameters of 127012 phase curves of 94777 asteroids in the photometric H, G1, G2- and H, G12*-systems. The taxonomic complexes of asteroids separate in the observed G1, G2-distributions, correlating with their mean visual albedo. This allows for differentiating the X-complex into the P-, M-, and E-complexes using the slope parameters as alternative to albedo measurements. Further, taxonomic misclassifications from spectrophotometric datasets as well as interlopers in dynamical families of asteroids reveal themselves in G1, G2-space. The H, G12*-model applied to the serendipitous observations is unable to resolve target taxonomy. The G1, G2 phase coefficients show wavelength-dependency for the majority of taxonomic complexes. Their values allow for estimating the degree of phase reddening of the spectral slope. The uncertainty of the phase coefficients and the derived absolute magnitude is dominated by the observational coverage of the opposition effect rather than the magnitude dispersion induced by the asteroids' irregular shapes and orientations. Serendipitous asteroid observations allow for reliable phase curve determination for a large number of asteroids. To ensure that the acquired absolute magnitudes are suited for colour computations, it is imperative that future surveys densely cover the opposition effects of the phase curves, minimizing the uncertainty on H. The phase curve slope parameters offer an accessible dimension for taxonomic classification, correlating with the albedo and complimentary to the spectral dimension.2020yCat.7288....0Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/VII/288CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/astorb : Orbits of Minor Planets (Bowell+ 2014-)https://newton.spacedys.com/astdys : AstDyS-2 Home Pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=VII/288https://vizier.iucaa.in/viz-bin/VizieR-2?-source=VII/288http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=VII/288https://vizier.cds.unistra.fr/viz-bin/votable?-source=VII/288https://vizier.iucaa.in/viz-bin/votable?-source=VII/288http://vizieridia.saao.ac.za/viz-bin/votable?-source=VII/288GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultVII/288/phasePhase curve coefficients of asteroidsb_H12Lower HDI of H from H,G12*-model fitmagphot.mag;meta.modelleddoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNumber? Asteroid numbermeta.idintnullableNameAsteroid name or designationmeta.id;meta.maincharBand[co] Observation band: (c)yan or (o)range)instr.bandpass;obscharClassTaxonomic class from referencesrc.classcharSchemeTaxonomic scheme from referencemeta.code.classcharr_ClassBibcode of taxonomy referencemeta.ref;pos.framecharap? Proper semi-major axisAUpos.pm;phys.size.smajAxisdoublenullableep? Proper eccentricitysrc.orbital.eccentricitydoublenullableip? Proper inclinationsrc.orbital.inclinationdoublenullableNNumber of ATLAS observationsmeta.numberintphminMinimum observed phase angledegpos.phaseAng;stat.mindoublephmaxMaximum observed phase angledegpos.phaseAng;stat.maxdoubleH? H from H,G1,G2-model fitmagphys.magAbs;meta.modelleddoublenullableG1? G1 from H,G1,G2-model fitstat.fit.paramdoublenullableG2? G2 from H,G1,G2-model fitstat.fit.paramdoublenullablermsRoot-mean-square error of H,G1,G2-model fitmagstat.stdevdoubleH12H12 from H,G12*-model fitmagphys.magAbs;meta.modelleddoubleG12H12 from H,G12*-model fitstat.fit.paramdoublerms12Root-mean-square error of H,G12*-model fitmagstat.stdev;phot.magdoubleB_H? Upper HDI of H from H,G1,G2-model fitmagphot.mag;meta.modelleddoublenullableb_H? Lower HDI of H from H,G1,G2-model fitmagphot.mag;meta.modelleddoublenullableB_G1? Upper HDI of G1 from H,G1,G2-model fitmeta.notedoublenullableb_G1? Lower HDI of G1 from H,G1,G2-model fitmeta.notedoublenullableB_G2? Upper HDI of G2 from H,G1,G2-model fitmeta.notedoublenullableb_G2? Lower HDI of G2 from H,G1,G2-model fitmeta.notedoublenullableB_H12Upper HDI of H from H,G12*-model fitmagphot.mag;meta.modelleddoubleB_G12Upper HDI of G12 from H,G12*-model fitmeta.notedoubleb_G12Lower HDI of G12 from H,G12*-model fitmeta.notedoublealbedo? Weighted mean of reference albedo valuesphys.albedo;stat.meandoublenullablee_albedo? Error of weighted mean of albedostat.error;phys.albedodoublenullabler_albedoBibcodes of albedo reference valuesmeta.ref;pos.framecharFamilyNumber? Family number of asteroid from AstDySmeta.idintnullableFamilyNameFamily name of asteroid from AstDySmeta.idcharFamilyStatusFamily status of asteroid from AstDySmeta.code.classchar