J/A+A/709/A35ivo://CDS.VizieR/J/A+A/709/A35CDSZhang Z.Wang W.Ma X.Chen Z.Wang Y.Yu C.Liu S.Gao Y.Tang B.,Chen D.Ma B.2026-05-19T14:14:26Z2026-04-29T08:40:35ZCDS support team

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

cds-question@unistra.frmultiple-starsexoplanetsephemeridesvisible-astronomyCo-orbital objects, also known as Trojans, are celestial bodies that share a 1:1 mean motion resonance orbit with a planet. Many planets in our Solar System hold Trojans, yet none has been confirmed in exoplanetary systems. While theoretical models suggest that hot Jupiters are unlikely to retain co-orbitals, their high transit cadence and deep transits make them accessible targets for constraining the existence of massive companions using transit timing variations (TTVs). The Exoplanet Ephemerides Change Observations (ExoEcho) project aims to study TTVs in exoplanetary systems using high- precision photometry from space- and ground-based telescopes. As the third paper in the ExoEcho project, we investigate the potential existence of exotrojans in hot-Jupiter systems through a TTV analysis of TESS observations. In this work, we analyzed TESS photometry for 260 confirmed hot Jupiters with published radial-velocity-based (RV-based) mass measurements to search for TTV signals compatible with Trojan companions. We derived transit times and assessed the compatibility of TTV residuals with co-orbital models through N-body simulation using the REBOUND N-body code. Accounting for the physical degeneracy between Trojan mass and libration amplitude, we placed upper mass limits on possible companions for typical libration amplitudes. For a typical libration amplitude of 15{deg}, we rule out exotrojans more massive than 1 Earth mass in 130 systems (~50% of our sample). A more conservative chi^2^ analysis incorporating observational uncertainties places this limit at 3 Earth masses. Additionally, we used the stability boundaries of the 1:1 resonance to exclude dynamically unstable configurations, ensuring our derived mass limits fall within the stable regime. Our results provide stringent constraints on co-orbital formation in short-period systems and establish a framework for future high-precision missions such as the PLAnetary Transits and Oscillations of stars (PLATO) or Earth 2.0 (ET) mission.2026A&A...709A..35Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/709/A35CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/709/A35https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/709/A35http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/709/A35https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/709/A35https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/709/A35http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/709/A35GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/709/A35/sources (List of studied sources)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/709/A35/sources?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/709/A35/sources?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/709/A35/sources?GETtext/xml+votable180.050000true102.079875-3.10213890.0055555555555555566/790 876 913 935 960 1275 1292 1814 1823 1971 2177 2250 2308 2335 2532 2551 2555 2584 2596 2711 2715 2740 2953 3344 3876 4145 4241 4272 4632 4799 4990 5170 5475 5730 6017 6058 6181 6349 6381 6539 6638 7036 7208 7447 7502 7649 7652 7917 8197 8237 8825 8992 9173 9355 9482 9524 9651 9653 9811 10066 10118 10407 10654 10701 10730 10953 11279 11455 11686 12342 12424 12436 12486 12853 12862 12935 12983 13044 13143 13250 13439 13569 13680 13702 13941 14446 14598 14667 14825 14886 14914 14993 15029 15129 15143 15162 15218 15550 15928 15950 16074 16366 16405 16432 16512 16534 16633 16768 16947 17040 17162 17172 17202 17226 17344 17430 17753 17819 17851 17865 18093 18208 18437 18452 18510 18569 18766 18880 19024 19829 20116 20186 20339 20382 20453 20455 20501 20565 20648 20659 20682 20741 20780 20790 20872 21026 21079 21176 21254 21820 21876 21885 21989 22001 22065 22331 22396 22505 22519 22816 22963 23387 24039 24057 24409 24617 24622 24752 24815 24858 24981 25132 25140 25153 25194 25283 25604 25885 25950 26028 26062 26727 26771 26844 26918 27057 27488 27780 28400 28433 30009 30157 30466 30485 32217 32564 32640 32659 32727 32748-32749 33157 33200 33220 33470 33719 33723 33798 34260 34370 34471 34526 34566 34643 34708 34755 34812 34847-34848 34860 34898 34940 34957 35210 35456 35486 35993 36142 36165 36196-36197 36497 36667 36794 37247 37274 38199 38233 38381 38452 38644 38682 38883 39007 39474 39487 39512 39542 39611 39673 39733 39812 39826 39829 39851 39912 40014 40022 40189 40194 40320 40347 40669 40862 40864 42001 42659 42865 42936 43180 43233 43247-43248 43257 43336 43432 43541 43544 43586 43623 43625 43656 43733 43775 43847 43864-43865 43960 44041 44200 44648 44672 44685 45041 45051 45380 45800 45855 45897 45922 46121 46316 46421 46429 46437 46771 46873 47000 47154 47168 47186 47307 47310 47330 47449 47476 48005 48178 48338 48358 48415 49103https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/709/A35?format=asciiOpticaldefaultJ/A+A/709/A35/sourcesList of studied sourcesrecnoRecord number assigned by the VizieR team. 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