J/A+A/682/A164ivo://CDS.VizieR/J/A+A/682/A164doi:10.26093/cds/vizier.36820164CDSVaessen T.van Roestel J.2024-11-28T20:06:21Z2024-02-20T08:50:16ZCDS support team

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

cds-question@unistra.freclipsing-binary-starsvisible-astronomyorbitsDouble eclipsing binaries are gravitationally bound quadruple systems in a '2+2' configuration where both of the binaries are eclipsing. These systems are interesting objects to better understand stellar formation, to investigate the dynamical interaction between the two binary systems or to study certain stages of stellar evolution, such as common-envelope events or Type Ia Supernovae. With this work, we aim to determine if double eclipsing binaries can be found using ZTF data and what the difficulties are in doing so. Secondly, we aim to significantly increase the number of known double eclipsing systems and determine how this sample differs from samples of double eclipsing binaries found with other telescopes. Methods. We develop a new method to systematically search for double eclipsing binaries in sparsely sampled light curves. For this we use Box-Least-Squares (BLS) to search for the period of the first binary in the system. We then remove that signal from the light curves, and search the residual light curve again with BLS to find the second period. We applied this method to ZTF light curves of 575 526 eclipsing binaries known in the Gaia eclipsing binary catalogue. We report the discovery of 198 new double eclipsing binary systems. The shortest and longest orbital periods of the newly detected systems are 0.11 days to 323 days respectively. Conclusions. We successfully implemented a method that systematically searches for double eclipsing binary systems in sparsely sampled data. In total 198 new double eclipsing binary systems have been found in 575 526 light curves (~0.034%). The ZTF sample typically contains more short period binaries compared to the TESS sample, but is also able to find systems with longer periods than what is currently known. We expect that at least three to four times more quadruples can be found by applying this method to all ZTF stellar light curves, by increasing the number of data points as a result of longer observations,and by implementing an automatic detection mechanism that replaces visual inspection.2024A&A...682A.164Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/682/A164CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/682/A164https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/682/A164http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/682/A164https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/682/A164https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/682/A164http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/682/A164GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/682/A164/table1 (Parameters of the quadruple candidates)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/682/A164/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/682/A164/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/682/A164/table1?GETtext/xml+votable180.050000true1.46150231644.447714480.0055555555555555566/1123 1310 1436 1466 1477 1621 1736 1830 1833 1854 1867 1928 2347 2685 2715 2733 2746 2777 2838 2880 2896-2897 2937 2941 3036 3062 3165 3247 3275 3279 3304-3305 3336 3594 3598 3605 3632 3634 3652 3654 3712 3721 3752 6222 6328 9405 9545 10050 11326 11821 12512 12793 12970-12972 12986 13000 13034 13052 13214 13227 13232 13275 13283 13307 13350 13542 13634 13799 13870 13883 13933 13969 13977 14021 14054 14061 14076 14102 14116 14191 14202 14223 14225 14235 14238 14243 14249 14252 14262-14263 14287 14301 14303 14353 14356 14359 14363 14365 14389-14390 14402-14403 14425-14427 14437-14439 14449 14451 14454-14455 14481 14496 14506 14547 14553 14565 14567 14613 14623 14627 14630-14631 14643-14644 14649 14698 14742 14764 14862 14987 15136 15258 15384 15386 15391 15393 15402 15424 15467 15470 15476 15479 15617 15619 15625-15626 15631 15644 15650 15693 15706 15748 15957 20821 20859 21631 21651 21755 22111 22114 22122 23632 23697 23839 23988 24159 24466 24505 29245 29533 29565 29856 29872-29873 29893 30245 30290 30299 30501 30504 30614 30657 30681 30700 30718 32003 32013-32014 32033 32068 32073 32090 32097 32117 32125 36708 49006https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/682/A164?format=asciiOpticaldefaultJ/A+A/682/A164/table1Parameters of the quadruple candidatesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right ascension (J2000.0)degpos.eq.ra;meta.mainDEJ2000Declination (J2000.0)degpos.eq.dec;meta.mainGaiaDR3Gaia EDR3 identifiermeta.id;meta.mainPerAOrbital period of A componentdtime.perioddoubleDepthAEclipse depth of A componentsrc.var.amplitudedoublePerBOrbital period of B componentdtime.perioddoubleDepthBEclipse depth of B componentsrc.var.amplitudedoubleSimbadSimbad column added by the CDSmeta.ref.urlchar