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<ri:Resource created="2024-07-18T13:56:22Z" status="active" updated="2025-05-19T09:50:00Z" 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>LC analysis of type I superluminous SNe</title><shortName>J/ApJ/933/14</shortName><identifier>ivo://CDS.VizieR/J/ApJ/933/14</identifier><altIdentifier>doi:10.26093/cds/vizier.19330014</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Hosseinzadeh G.</name></creator><creator><name>Berger E.</name></creator><creator><name>Metzger B.D.</name></creator><creator><name>Gomez S.</name></creator><creator><name>Nicholl M.,Blanchard P.</name></creator><date role="Updated">2024-11-06T20:26:06Z</date><date role="Created">2024-07-18T13:56:22Z</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><subject>spectroscopy</subject><description>Recent work has revealed that the light curves of hydrogen-poor (TypeI) superluminous supernovae (SLSNe), thought to be powered by magnetar central engines, do not always follow the smooth decline predicted by a simple magnetar spin-down model. Here we present the first systematic study of the prevalence and properties of "bumps" in the post-peak light curves of 34 SLSNe. We find that the majority (44%-76%) of events cannot be explained by a smooth magnetar model alone. We do not find any difference in supernova properties between events with and without bumps. By fitting a simple Gaussian model to the light-curve residuals, we characterize each bump with an amplitude, temperature, phase, and duration. We find that most bumps correspond with an increase in the photospheric temperature of the ejecta, although we do not see drastic changes in spectroscopic features during the bump. We also find a moderate correlation ({rho}~0.5; p~0.01) between the phase of the bumps and the rise time, implying that such bumps tend to happen at a certain "evolutionary phase," (3.7+/-1.4)t_rise_. Most bumps are consistent with having diffused from a central source of variable luminosity, although sources further out in the ejecta are not excluded. With this evidence, we explore whether the cause of these bumps is intrinsic to the supernova (e.g., a variable central engine) or extrinsic (e.g., circumstellar interaction). Both cases are plausible, requiring low- level variability in the magnetar input luminosity, small decreases in the ejecta opacity, or a thin circumstellar shell or disk.</description><source format="bibcode">2022ApJ...933...14H</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/933/14</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/sn">B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/147">V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/349">II/349 : The Pan-STARRS release 1 (PS1) Survey - DR1 (Chambers+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/696/870">J/ApJ/696/870 : Catalina Real-time Transient Survey (CRTS) (Drake+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/other/Nat/474.484">J/other/Nat/474.484 : Light curves of 4 supernovae (Quimby+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/437/656">J/MNRAS/437/656 : SN PS1-11ap light curves (McCrum+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/797/24">J/ApJ/797/24 : Imaging observations of iPTF 13ajg (Vreeswijk+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/459/3939">J/MNRAS/459/3939 : Type II supernova light curves (Valenti+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/836/25">J/ApJ/836/25 : Swift UVOT light curves of ASASSN-15lh (Margutti+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/835/58">J/ApJ/835/58 : PTF 12dam &amp; iPTF 13dcc follow-up (Vreeswijk+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/860/100">J/ApJ/860/100 : LCs of 26 hydrogen-poor superluminous SNe (De Cia+, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/852/81">J/ApJ/852/81 : 17 PS1 superluminous SNe LCs + classif. sp. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>MJD</name><description>Modified Julian Date of observation (JD-2400000.5)</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>Filt</name><description>Filter (BVgriz)</description><ucd>meta.id;instr.filter</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>l_omag</name><description>Upper limit flag on omag</description><ucd>meta.code.error;phot.mag</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>omag</name><description>[14.57/22.72] Apparent magnitude in Filt</description><unit>mag</unit><ucd>phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_omag</name><description>[0.005/0.4]? 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