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<ri:Resource created="2025-02-14T09:19:09Z" status="active" updated="2025-05-21T20:01:18Z" 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>ZTF SN Ia DR2. Secondary maximum in Type Ia SN</title><shortName>J/A+A/694/A12</shortName><identifier>ivo://CDS.VizieR/J/A+A/694/A12</identifier><altIdentifier>doi:10.26093/cds/vizier.36940012</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Deckers M.</name></creator><creator><name>Maguire K.</name></creator><creator><name>Shingles L.</name></creator><creator><name>Dimitriadis G.</name></creator><creator><name>Rigault M.</name></creator><creator><name>Smith M.,Goobar A.</name></creator><creator><name>Nordin J.</name></creator><creator><name>Johansson J.</name></creator><creator><name>Amenouche M.</name></creator><creator><name>Burgaz U.</name></creator><creator><name>Dhawan S.,Ginolin M.</name></creator><creator><name>Harvey L.</name></creator><creator><name>Kenworthy W.D.</name></creator><creator><name>Kim Y.-L.</name></creator><creator><name>Laher R.R.</name></creator><creator><name>Luo N.,Kulkarni S.R.</name></creator><creator><name>Masci F.J.</name></creator><creator><name>Galbany L.</name></creator><creator><name>Mueller-Bravo T.E.</name></creator><creator><name>Nugent P.E.,Pletskova N.</name></creator><creator><name>Purdum J.</name></creator><creator><name>Racine B.</name></creator><creator><name>Sollerman J.</name></creator><creator><name>Terwel J.H.</name></creator><date role="Updated">2025-05-21T20:01:18Z</date><date role="Created">2025-02-14T09:19:09Z</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>supernovae</subject><subject>photometry</subject><subject>visible-astronomy</subject><description>Type Ia supernova (SN Ia) light curves have a secondary maximum that exists in the r, i, and near-infrared filters. The secondary maximum is relatively weak in the r band, but holds the advantage that it is accessible, even at high redshift. We used Gaussian Process fitting to parameterise the light curves of 893 SNe Ia from the Zwicky Transient Facility's (ZTF) second data release (DR2), and we were able to extract information about the timing and strength of the secondary maximum. We found &gt;5{sigma} correlations between the light curve decline rate ({DELTA}m15(g)) and the timing and strength of the secondary maximum in the r band. Whilst the timing of the secondary maximum in the i band also correlates with {DELTA}m15(g), the strength of the secondary maximum in the i band shows significant scatter as a function of {DELTA}m15(g). We found that the transparency timescales of 97 per cent of our sample are consistent with double detonation models, and that SNe Ia with small transparency timescales (&lt;32d) reside predominantly in locally red environments. We measured the total ejected mass for the normal SNe Ia in our sample using two methods, and both were consistent with medians of 1.3+/-0.3 and 1.2+/-0.2 solar masses. We find that the strength of the secondary maximum is a better standardisation parameter than the SALT light curve stretch (x1). Finally, we identified a spectral feature in the r band as FeII, which strengthens during the onset of the secondary maximum. The same feature begins to strengthen at &lt;3d post maximum light in 91bg-like SNe. Finally, the correlation between x1 and the strength of the secondary maximum was best fit with a broken line, with a split at x0^1^=-0.5+/-0.2, suggestive of the existence of two populations of SNe Ia.</description><source format="bibcode">2025A&amp;A...694A..12D</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/694/A12</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/J/A+A/694/A9">J/A+A/694/A9 : Spectral Measurements of ZTF SN Ia DR2 (Burgaz+, 2025)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/694/A10">J/A+A/694/A10 : ZTF SN Ia DR2 (Dimitriadis+, 2025)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/694/A11">J/A+A/694/A11 : SN 2020alm spectrum (Terwel+, 2025)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL use="full">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/694/A12</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/694/A12</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/694/A12</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/694/A12</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/694/A12</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, 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