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<ri:Resource created="2019-09-18T12:38:47Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" 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/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>Type IIP supernova SN 2004dj radio observations</title><shortName>J/ApJ/863/163</shortName><identifier>ivo://CDS.VizieR/J/ApJ/863/163</identifier><altIdentifier>doi:10.26093/cds/vizier.18630163</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Nayana A. J.</name></creator><creator><name>Chandra P.</name></creator><creator><name>Ray A. K</name></creator><date role="Updated">2019-09-18T12:27:47Z</date><date role="Created">2019-09-18T12:38:47Z</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>radio-continuum-emission</subject><description>We present radio observations and modeling of one of the nearest and brightest Type IIP supernova SN 2004dj exploded in the galaxy NGC2403 at a distance of ~3.5Mpc. Our observations span a wide frequency and temporal range of 0.24-43GHz and ~1d to 12yrs since the discovery. We model the radio light curves and spectra with the synchrotron emission. We estimate the mass-loss rate of the progenitor star to be dM/dt~1x10^-6^M_{sun}_/yr for a wind speed of 10km/s. We calculate the radio spectral indices using 1.06, 1.40, 5.00, and 8.46GHz flux density measurements at multiple epochs. We witness steepening in the spectral index values for an extended period predominantly at higher frequencies. We explain this as a signature of electron cooling happening at the supernova shock in the plateau phase of the supernova. We estimate the cooling timescales for inverse Compton cooling and synchrotron cooling and find that inverse Compton cooling is the dominant cooling process.</description><source format="bibcode">2018ApJ...863..163N</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/863/163</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>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/J/A+AS/96/269">J/A+AS/96/269 : Stellar Models from 0.8 to 120 Msolar (Schaller+, 1992)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/PASP/117/773">J/PASP/117/773 : Classif. of SN host galaxies. 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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>Date</name><description>Observation date (UT)</description><ucd>time.epoch;obs</ucd><flag>nullable</flag></column><column><name>Age</name><description>[34.1/4190.3] Days since explosion assuming date of explosion as 2004 June 28.00 (UT)</description><unit>d</unit><ucd>time.interval</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Freq</name><description>[0.2/43.4] Frequency of observation</description><unit>GHz</unit><ucd>em.freq;obs</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Fnu</name><description>[0.1/10.5] Supernova flux</description><unit>mJy</unit><ucd>phot.flux.density;em.radio</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_Fnu</name><description>[0.04/0.6]? Uncertainty in Supernova flux</description><unit>mJy</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>r_Fnu</name><description>Source for Fnu if not this work (1)</description><ucd>meta.ref;pos.frame</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>RMS</name><description>[0.03/4] RMS noise</description><unit>mJy/beam</unit><ucd>instr.det.noise</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>cFnu</name><description>[0.1/9.8]? Calibration flux</description><unit>Jy</unit><ucd>phot.flux.density;em.radio;obs.calib</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Tel</name><description>Telescope/Instrument used (VLA, GMRT or MERLIN)</description><ucd>instr.setup</ucd><dataType xsi:type="vs:VOTableType" arraysize="12*">char</dataType></column></table></schema></tableset></ri:Resource>