J/A+A/610/A7ivo://CDS.VizieR/J/A+A/610/A7doi:10.26093/cds/vizier.36100007CDSMarciniak A.Bartczak P.Mueller T.Sanabria J.J.Ali-Lagoa V.,Antonini P.Behrend R.Bernasconi L.Bronikowska M.Butkiewicz-Bkak M.,Cikota A.Crippa R.Ditteon R.Dudzinski G.Duffard R.Dziadura K.,Fauvaud S.Geier S.Hirsch R.Horbowicz J.Hren M.Jerosimic L.,Kaminski K.Kankiewicz P.Konstanciak I.Korlevic P.Kosturkiewicz E.,Kudak V.Manzini F.Morales N.Murawiecka M.Ogloza W.Oszkiewicz D.,Pilcher F.Polakis T.Poncy R.Santana-Ros T.Siwak M.Skiff B.,Sobkowiak K.Stoss R.Zejmo M.Zukowski K.2019-04-18T11:36:05Z2018-02-09T14:43:53ZCDS support team

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

cds-question@unistra.frsolar-systemasteroidsphotometryThe available set of spin and shape modelled asteroids is strongly biased against slowly rotating targets and those with low lightcurve amplitudes. This is due to the observing selection effects. As a consequence, the current picture of asteroid spin axis distribution, rotation rates, radiometric properties, or aspects related to the object's internal structure might be affected too. To counteract these selection effects, we are running a photometric campaign of a large sample of main belt asteroids omitted in most previous studies. Using least chi-squared fitting we determined synodic rotation periods and verified previous determinations. When a dataset for a given target was sufficiently large and varied, we performed spin and shape modelling with two different methods to compare their performance. We used the convex inversion method and the non-convex SAGE algorithm, applied on the same datasets of dense lightcurves. Both methods search for the lowest deviations between observed and modelled lightcurves, though using different approaches. Unlike convex inversion, the SAGE method allows for the existence of valleys and indentations on the shapes based only on lightcurves. We obtain detailed spin and shape models for the first five targets of our sample: (159) Aemilia, (227) Philosophia, (329) Svea, (478) Tergeste, and (487) Venetia. When compared to stellar occultation chords, our models obtained an absolute size scale and major topographic features of the shape models were also confirmed. When applied to thermophysical modelling (TPM), they provided a very good fit to the infrared data and allowed their size, albedo, and thermal inertia to be determined. Convex and non-convex shape models provide comparable fits to lightcurves. However, some non-convex models fit notably better to stellar occultation chords and to infrared data in sophisticated thermophysical modelling (TPM). In some cases TPM showed strong preference for one of the spin and shape solutions. Also, we confirmed that slowly rotating asteroids tend to have higher-than-average values of thermal inertia, which might be caused by properties of the surface layers underlying the skin depth.2018A&A...610A...7Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/610/A7CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/astorb : Orbits of Minor Planets (Bowell+ 2014)J/A+A/465/331 : Asteroid brightness and geometry (Durech+, 2007)J/A+A/498/313 : Photometry of 3 main belt asteroids (Marciniak+, 2009)J/A+A/508/1503 : Photometry of 3 main belt asteroids (Marciniak+, 2009)J/A+A/529/A107 : Photometry of 4 main belt asteroids (Marciniak+, 2011)J/A+A/545/A131 : Photometry of 8 main belt asteroids (Marciniak+, 2012)J/A+A/546/A72 : Light curves of Flora region asteroids (Kryszczynska+, 2012)J/A+A/598/A63 : 2015 TB145 light curve (Mueller+, 2017)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/610/A7https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/610/A7http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/610/A7https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/610/A7https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/610/A7http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/610/A7GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/610/A7/329lcsAsteroid 329 Svea individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrRelative brightness in intensity units, mean brightness of each lightcurve is unityphot.flux;arith.ratiodoubleSxx component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.xdoubleSyy component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.dirCosdoubleSzz component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.zdoubleExx component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.xdoubleEyy component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.dirCosdoubleEzz component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.zdoubleJ/A+A/610/A7/478lcsAsteroid 478 Tergeste individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrRelative brightness in intensity units, mean brightness of each lightcurve is unityphot.flux;arith.ratiodoubleSxx component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.xdoubleSyy component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.dirCosdoubleSzz component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.zdoubleExx component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.xdoubleEyy component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.dirCosdoubleEzz component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.zdoubleJ/A+A/610/A7/581dataAsteroid 581 Tauntonia individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrBrightness in magnitude unitsmagphot.magfloatJ/A+A/610/A7/830dataAsteroid 830 Petropolitana individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrBrightness in magnitude unitsmagphot.magfloatJ/A+A/610/A7/923dataAsteroid 923 Herluga individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrBrightness in magnitude unitsmagphot.magfloatJ/A+A/610/A7/932dataAsteroid 932 Hooveria individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrBrightness in magnitude unitsmagphot.magfloatJ/A+A/610/A7/table2Synodic periods and amplitude values found within this project compared to literature data gathered previously in LCDBLCShow the light curvesmeta.ref.urlcharNameAsteroid namemeta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAmpAmplitude (LCDB and this work)src.var.amplitudecharPerLCBDLCBD periodhtime.periodfloatq_PerLCBDPeriod quality codemeta.code.qualcharPerPeriod (this work)htime.periodfloate_Perrms uncertainty on Perhstat.errorfloatn_Per[*] * for period determinations substantially differing from previously accepted valuesmeta.notecharNote[nm] n for Targets with new periods, m for Targets with modelsmeta.notecharFileNameName of the tabel with light curve datameta.idcharJ/A+A/610/A7/159lcsAsteroid 159 Aemilia individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrRelative brightness in intensity units, mean brightness of each lightcurve is unityphot.flux;arith.ratiodoubleSxx component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.xdoubleSyy component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.dirCosdoubleSzz component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.zdoubleExx component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.xdoubleEyy component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.dirCosdoubleEzz component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.zdoubleJ/A+A/610/A7/227lcsAsteroid 227 Philosophia individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrRelative brightness in intensity units, mean brightness of each lightcurve is unityphot.flux;arith.ratiodoubleSxx component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.xdoubleSyy component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.dirCosdoubleSzz component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.zdoubleExx component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.xdoubleEyy component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.dirCosdoubleEzz component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.zdoubleJ/A+A/610/A7/487lcsAsteroid 487 Venetia individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrRelative brightness in intensity units, mean brightness of each lightcurve is unityphot.flux;arith.ratiodoubleSxx component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.xdoubleSyy component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.dirCosdoubleSzz component of the vector from the asteroid to the Sun in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.zdoubleExx component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.xdoubleEyy component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.dirCosdoubleEzz component of the vector from the asteroid to the Earth in J2000 ecliptic Cartesian coordinatesAUpos.cartesian.zdoubleJ/A+A/610/A7/551dataAsteroid 551 Ortrud individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrBrightness in magnitude unitsmagphot.magfloatJ/A+A/610/A7/995dataAsteroid 995 Sternberga individual lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJD epoch corrected for the light-time corresponding to the Earth-asteroid distancedtime.epochdoublebrBrightness in magnitude unitsmagphot.magfloat