J/A+A/710/A27ivo://CDS.VizieR/J/A+A/710/A27CDSIrureta-Goyena B.Y.Altieri B.Kneib J.-P.Poentinen M.Hainaut O.R.,Alarcon M.R.Granvik M.Nucita A.A.Carry B.Devogele M.Mahlke M.,Vavrek R.Mueller T.Vilenius E.Snodgrass C.Kohley R.Lemon C.,Gomez-Alvarez P.Verdoes Kleijn G.Licandro S.Kruk J.Conversi L.,Franco A.Buenadicha G.Mas-Buitrago P.Kuijken K.Andreon S.,Baccigalupi C.Baldi M.Balestra A.Battaglia P.Biviano A.,Branchini E.Brescia M.Camera S.Capobianco V.Carbone C.,Carretero J.Casas R.Castellano M.Castignani G.Cavuoti S.,Chambers K.C.Cimatti A.Colodro-Conde C.Congedo G.Conselice C.J.,Copin Y.Courbin F.Courtois H.M.Cropper M.Degaudenzi H.De Lucia G.,Dolding C.Dole H.Dubath F.Dupac X.Farina M.Farinelli R.,Ferriol S.Frailis M.Fumana M.Galeotta S.George K.Gillis B.,Giocoli C.Gracia-Carpio J.Grazian A.Grupp F.Haugan S.V.H.,Hoekstra H.Holmes W.Hook I.M.Hormuth F.Hornstrup A.Jahnke K.,Jhabvala M.Kiessling A.Kubik B.Kuemmel M.Kunz M.Kurki-Suonio H.,Le Brun A.M.C.Ligori S.Lilje P.B.Lindholm V.Lloro I.Mainetti G.,Mansutti O.Marggraf O.Martinelli M.Martinet N.Marulli F.,Massey R.J.Medinaceli E.Mei S.Merlin E.Meylan G.Mora A.,Moscardini L.Nakajima R.Neissner C.Niemi S.-M.Padilla C.,Paltani S.Pasian F.Pedersen K.Percival W.J.Pettorino V.Polenta G.,Popa L.A.Raison F.Rebolo R.Renzi A.Rhodes J.Riccio G.Romelli E.,Roncarelli M.Saglia R.Sakr Z.Sapone D.Schirmer M.Schneider P.,Secroun A.Sihvola E.Simon P.Sirignano C.Sirri G.Stanco L.,Tallada-Crespi P.Tereno I.Toft S.Toledo-Moreo R.Torradeflot F.,Tutusaus I.Valiviita J.Vassallo T.Wang Y.Weller J.Zerbi F.M.,Garcia-Bellido J.Martin-Fleitas J.Scottez V.Helou G.Scott D.2026-06-02T07:26:44Z2026-06-02T08:23:43ZCDS support team

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

cds-question@unistra.frasteroidsapparent-magnitudevisible-astronomyThe Euclid Ecliptic Survey was conducted during the calibration phase of the mission, from 23 to 31 December 2023, as a campaign to study Solar System objects. We use data from this survey to analyse more than 23000 appearances of 2321 known asteroids. Due to their high apparent angular motion relative to the background stars (5-60"/h), these objects appear as streaks in VIS long-exposure images. We set out to estimate their spin periods, since only 7% of them have periods published in the literature. We use multiple apertures along each streak to increase the time resolution of our lightcurves. Our method combines a Lomb--Scargle approach with a Markov chain Monte Carlo (MCMC) algorithm to characterise the posterior distributions. Some asteroids show multimodality in the MCMC search, indicating period aliases; in these cases, we report all aliases and their likelihoods. We validate our pipeline by comparing our fitted periods with 48 published periods, including period harmonics. We find that 44% of our periods are within 1% of those published and 98% are within 15%, and we establish that with 98% confidence the best solution can be found among the first three aliases. All reliable periods reported are in agreement with our current understanding of the spin-period distribution for asteroids. We find 16 periods below the spin barrier of 2.2h with absolute magnitudes below 19, and thus candidate super-fast rotators. We provide lightcurves for all 2321 objects observed and 889 high-quality periods in an open-access catalogue. The asteroids with reported periods include five Mars crossers, four Cybeles, four Hildas, three Hungarias, and 877 asteroids in other regions of the Main Belt. Our results represent the first batch of spin periods extracted from Euclid lightcurves and include the first-ever period measurements for 93% of the objects.2026A&A...710A..27Ihttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/710/A27CatalogResearchIsServedByTAP 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/710/A27https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/710/A27http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/710/A27https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/710/A27https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/710/A27http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/710/A27GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/710/A27/tablea2All high-quality periodsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameAsteroid name (not including number for named asteroids)meta.id;meta.maincharP1hMost likely periodhtime.periodfloatE_P1hMost likely period upper uncertaintyhstat.error;stat.maxfloatP2h? Second most likely periodhtime.periodfloatnullablee_P1hMost likely period lower uncertaintyhstat.errorfloatE_P2h? Second most likely period upper uncertaintyhstat.error;stat.maxfloatnullablee_P2h? Second most likely period lower uncertaintyhstat.errorfloatnullableP3h? Third most likely periodhtime.periodfloatnullableE_P3h? Third most likely period upper uncertaintyhstat.error;stat.maxfloatnullablee_P3h? Third most likely period lower uncertaintyhstat.errorfloatnullableAp2pmagPeak-to-peak amplitude associated to the most likely periodmagmeta.id.assoc;src.var.amplitudefloatmagFitted magnitude associated to the most likely periodmagphot.mag;em.optfloatE_magFitted magnitude associated to the most likely period upper uncertaintymagstat.error;stat.maxfloate_magFitted magnitude associated to the most likely period lower uncertaintymagstat.error;phot.magfloatNdataptsNumber of datapoints in the lightcurvemeta.numberintNmodesNumber of aliasesmeta.numberintThetaPhase-dispersion metricpos.posAngfloatHourRangeTime coveragehtime.intervalfloatPhaseCovFraction of the rotation sampled by our datastat.fit.paramfloatrchi2mcmcReduced chi-square for the first periodmeta.notefloatJ/A+A/710/A27/tableb1Lightcurves that did not show enough variability in the observed range (reduced chi-square<=2 when fitting a constant)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameAsteroid name (not including number for named asteroids)meta.id;meta.maincharmagcstMagnitude (value of the fitted constant)magphot.mag;em.optfloats_magcstStandard deviation of the datapointsmagstat.stdev;phot.magfloatNdataptsNumber of datapoints in the lightcurvemeta.numberintRangeTime coveragehtime.intervalfloatchi2redcstReduced chi-square when fitting the constant magnitudemeta.notefloatJ/A+A/710/A27/tableb2Periods considered low-quality fits (202 with theta>0.8 and 105 below the spin barrier with theta>0.5)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameAsteroid name (not including number for named asteroids)meta.id;meta.maincharmagFitted magnitude associated to the most likely periodmagphot.mag;em.optfloatE_magFitted magnitude associated to the most likely period upper uncertaintymagstat.error;stat.maxfloate_magFitted magnitude associated to the most likely period lower uncertaintymagstat.error;phot.magfloats_magStandard deviation of the datapointsmagstat.stdev;phot.magfloatNdataptsNumber of datapointsmeta.numberintRangeTime coveragehtime.intervalfloatThetaPhase-dispersion metricpos.posAngfloatJ/A+A/710/A27/tableLightcurves discarded because they had fewer than 50 points (408) or the fitting failed to find relevant modes (12)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameAsteroid name (not including number for named asteroids)meta.id;meta.maincharNdataptsNumber of datapointsmeta.numberint