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<ri:Resource created="2026-09-02T08:57:50Z" status="active" updated="2026-09-02T08:46:05Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>Eclipse depths &amp; times for 7 systems from KELT &amp; TESS</title><shortName>J/AJ/170/331</shortName><identifier>ivo://CDS.VizieR/J/AJ/170/331</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Baum A.C.</name></creator><creator><name>Pepper J.</name></creator><creator><name>Davenport J.R.A.</name></creator><creator><name>Howell S.B.</name></creator><date role="Updated">2026-09-02T08:46:05Z</date><date role="Created">2026-09-02T08:57:50Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>eclipsing-binary-stars</subject><subject>photometry</subject><subject>visible-astronomy</subject><subject>multiple-stars</subject><description>A set of eclipsing binary systems exhibit a changing inclination over time due to the gravitational influence of a third stellar companion. These changing inclinations manifest in photometric observations over time as eclipse depth variations. To detect changing eclipse depths, it is advantageous to have a long time baseline of observations, which can be attained by combining data from multiple surveys. We collect ground-based photometry from the Kilodegree Extremely Little Telescope and space-based photometry from the Transiting Exoplanet Survey Satellite (TESS) for seven known changing-inclination eclipsing binaries: HS Hya, RW Per, IU Aur, AH Cep, SV Gem, V685 Cen, and SS Lac. We measure eclipse depth variations and eclipse timing variations in six systems; SS Lac no longer eclipses. As of observations presented here from TESS Sector 35, eclipses are no longer visible in HS Hya (as noted in J. R. A. Davenport et al. 2021). SV Gem, previously believed to have stopped eclipsing, exhibits eclipse-like features across all years of observation, as well as evidence of the negative "O'Connell Effect." We also present high-resolution speckle imaging from Gemini-North, Gemini-South, and the NESSI instrument on the WIYN telescope for RW Per, AH Cep, SV Gem, and SS Lac, none of which revealed a third companion. Speckle imaging of IU Aur from NESSI revealed the presence of a third companion at an angular separation of 0.14"; we report the details of this detection.</description><source format="bibcode">2025AJ....170..331B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/170/331</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/B/wds">B/wds : The Washington Visual Double Star Catalog (Mason+ 2001-)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/264">II/264 : ASAS Variable Stars in Southern hemisphere (Pojmanski+, 2002-2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/355">I/355 : Gaia DR3 Part 1. 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Approximate fraction of flux within the TESS aperture originating from the target star; from TIC</description><ucd>phot.flux;arith.ratio</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Ref</name><description>Reference of the effective temperatures (1)</description><ucd>meta.bib</ucd><dataType xsi:type="vs:VOTableType" arraysize="3*">char</dataType></column><column><name>Fig1</name><description>KELT and TESS light curves in JPG format (Figure 1)</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="9*">char</dataType></column><column><name>Fig11</name><description>Eclipse time O-C vs. median time of observation in JPG format (Figure 11)</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="3*">char</dataType></column><column><name>nEcl</name><description>Number of eclipse depth and timing measurements (link to Table 4)</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column></table><table><name>J/AJ/170/331/table4</name><description>Eclipse depth and timing measurements</description><column><name>Depth</name><description>[2e-4/0.69] Eclipse Depth (3)</description><unit>mag</unit><ucd>src.var.amplitude</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>recno</name><description>Record number assigned by the VizieR team. 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