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Funding text: This work is part of the project 'Transient Astrophysical Objects' GINOP 2.3.2-15-2016-00033 of the National Research, Development and Innovation Office (NKFIH), Hungary, funded by the European Union.; Laszlo Molnar was supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences. The research leading to these results has received funding from the LP2018-7 Lendulet grant of the Hungarian Academy of Sciences.; Funding for the SDSS-IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org.0false2026-05-20T03:10:21.404+00002026-01-23T07:49:26.319+00002020-08-05T09:24:33.890+0000true10066055TurtóczkiTímea
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REVIEWEDtruefalse3275false3275true0035-87111365-2966JournalFOREIGN4963372537403725162020We present observations and analysis of PSN J17292918+7542390, a low-luminosity Type II-P supernova (LL SN IIP). The observed sample of such events is still low, and their nature is still under debate. Such SNe are similar to SN 2005cs, a well-observed LL Type II-P event, having low expansion velocities, and small ejected 56Ni mass. We have developed a robust and relatively fast Monte Carlo code that fits semi-analytic models to light curves of core-collapse SNe. This allows the estimation of the most important physical parameters, like the radius of the progenitor star, the mass of the ejected envelope, the mass of the radioactive nickel synthesized during the explosion, among others. PSN J17292918+7542390 has $R_0 = 91_{-70}^{+119} \times 10^{11} \, \text{cm}$, $M_\text{ej} = 9.89_{-1.00}^{+2.10} \, \mathrm{ M}_{\odot }$, $E_{\mbox{kin}} = 0.65_{-0.18}^{+0.19} \, \text{foe}$, and $v_{\mbox{exp}} = 3332_{-347}^{+216}$ km s−1, for its progenitor radius, ejecta mass, kinetic energy, and expansion velocity, respectively. The initial nickel mass of the PSN J17292918+7542390 turned out to be $1.55_{-0.70}^{+0.75} \times 10^{-3} \, \mathrm{M}_{\odot }$. The measured photospheric velocity at the earliest observed phase is 7000 km s−1. As far as we can tell based on the small population of observed LL SNe IIP, the determined values are typical for these events.true2020truetruetruefalsetruefalseGREEN2026-05-20truehttp://real.mtak.hu/15830312011110111111911111111120012121111066FolyóiratcikkJournal Article2411KönyvrészletChapter in Book250KönyvBook230Egyéb konferenciaközleményConference paper310Egyéb konferenciakötetConference proceedings320Oltalmi formákProtection forms260DisszertációThesis280EgyébMiscellaneous291AlkotásAchievement220Kutatási adatResearch data330FolyóiratcikkJournal Article24000KönyvrészletChapter in Book25000KönyvBook23000Egyéb konferenciaközleményConference paper31000Egyéb konferenciakötetConference proceedings32000Oltalmi formákProtection forms26000DisszertációThesis28000EgyébMiscellaneous29000AlkotásAchievement22000Kutatási adatResearch data33000202103333202202222202302222202401111202503333202601111Q1false10009807,10054959falsefalsefalse2020-08-09T08:54:33.729+0000Fizikai Intézet (ELTE / TTK); Konkoly Thege Miklós Csillagászati Intézet (HRN CSFK); MTA CSFK Lendület Lokális Kozmológia Kutatócsoport (HRN CSFK / CSKI); Optikai és Kvantumelektronikai Tanszék (SZTE / TTIK / FI); Optikai és Kvantumelektronikai Tanszék (SZTE / TTIK / FTCS); Szegedi Tudományegyetem Bajai Obszervatóriuma (SZTE)827690true10065569Language10002
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<div class="JournalArticle Publication short-list"> <div class="authors"> <span class="author-name" mtid="10083232"> <a href="/gui2/?type=authors&mode=browse&sel=10083232" target="_blank">Jäger, Zoltán Jr. ✉</a> </span> <span class="author-type"> </span> ; <span class="author-name" mtid="10001530"> <a href="/gui2/?type=authors&mode=browse&sel=10001530" target="_blank">Vinkó, József</a> </span> <span class="author-type"> </span> ; <span class="author-name" mtid="10026009"> <a href="/gui2/?type=authors&mode=browse&sel=10026009" target="_blank">Bíró, Barna I.</a> </span> <span class="author-type"> </span> ; <span class="author-name" mtid="10009807"> <a href="/gui2/?type=authors&mode=browse&sel=10009807" target="_blank">Hegedüs, Tibor</a> </span> <span class="author-type"> </span> ; <span class="author-name" mtid="10032717"> <a href="/gui2/?type=authors&mode=browse&sel=10032717" target="_blank">Borkovits, Tamás</a> </span> <span class="author-type"> </span> ; <span class="author-name" > Jäger, Zoltán Sr. </span> <span class="author-type"> </span> ; <span class="author-name" mtid="10054959"> <a href="/gui2/?type=authors&mode=browse&sel=10054959" target="_blank">Nagy, Andrea P.</a> </span> <span class="author-type"> </span> ; <span class="author-name" mtid="10017692"> <a href="/gui2/?type=authors&mode=browse&sel=10017692" target="_blank">Molnár, László</a> </span> <span class="author-type"> </span> ; <span class="author-name" mtid="10027559"> <a href="/gui2/?type=authors&mode=browse&sel=10027559" target="_blank">Kriskovics, Levente</a> </span> <span class="author-type"> </span> </div ><div class="title"><a href="/gui2/?mode=browse¶ms=publication;31395641" mtid="31395641" target="_blank">A low-luminosity core-collapse supernova very similar to SN 2005cs</a></div> <div class="pub-info"> <span class="journal-title">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</span> <span class="journal-volume">496</span> : <span class="journal-issue">3</span> <span class="page"> pp. 3725-3740. , 16 p. </span> <span class="year">(2020)</span> </div> <div class="pub-end"><div class="identifier-list"> <span class="identifiers"> <span class="id identifier oa_PAY" title=" Pay "> <a style="color:blue" title="10.1093/mnras/staa1743" target="_blank" href="https://doi.org/10.1093/mnras/staa1743"> DOI </a> </span> <span class="id identifier oa_none" title="none"> <a style="color:blue" title="000574919300071" target="_blank" href="https://www.webofscience.com/wos/woscc/full-record/000574919300071"> WoS </a> </span> <span class="id identifier oa_GREEN" title=" Green "> <a style="color:black" title="158303" target="_blank" href="http://real.mtak.hu/158303"> REAL </a> </span> <span class="id identifier oa_none" title="none"> <a style="color:blue" title="85101313843" target="_blank" href="http://www.scopus.com/record/display.url?origin=inward&eid=2-s2.0-85101313843"> Scopus </a> </span> <span class="id identifier oa_none" title="none"> <a style="color:blue" title="2020MNRAS.496.3725J luminosity Type II-P supernova (LL SN IIP). The observed sample of such events is still low, and their nature is still under debate. Such SNe are similar to SN 2005cs, a well-observed LL Type II-P event, having low expansion velocities, and small ejected 56Ni mass. We have analytic models to light curves of core-collapse SNe. This allows the estimation of the most important physical parameters, like the radius of the progenitor star, the mass of the ejected envelope, the mass of the radioactive nickel synthesized during the explosion, among others. PSN J17292918+7542390 has $R_0 = 91_{-70}^{+119} \times 10^{11} \, \text{cm}$ , $M_\text{ej} = 9.89_{-1.00}^{+2.10} \, \mathrm{ M}_{\odot }$ , $E_{\mbox{kin}} = 0.65_{-0.18}^{+0.19} \, \text{foe}$ , and $v_{\mbox{exp}} = 3332_{-347}^{+216}$ km s−1, for its progenitor radius, ejecta mass, kinetic energy, and expansion velocity, respectively. The initial nickel mass of the PSN J17292918+7542390 turned out to be $1.55_{-0.70" target="_blank" href="http://ui.adsabs.harvard.edu/abs/2020MNRAS.496.3725J luminosity Type II-P supernova (LL SN IIP). The observed sample of such events is still low, and their nature is still under debate. Such SNe are similar to SN 2005cs, a well-observed LL Type II-P event, having low expansion velocities, and small ejected 56Ni mass. We have analytic models to light curves of core-collapse SNe. This allows the estimation of the most important physical parameters, like the radius of the progenitor star, the mass of the ejected envelope, the mass of the radioactive nickel synthesized during the explosion, among others. PSN J17292918+7542390 has $R_0 = 91_{-70}^{+119} \times 10^{11} \, \text{cm}$ , $M_\text{ej} = 9.89_{-1.00}^{+2.10} \, \mathrm{ M}_{\odot }$ , $E_{\mbox{kin}} = 0.65_{-0.18}^{+0.19} \, \text{foe}$ , and $v_{\mbox{exp}} = 3332_{-347}^{+216}$ km s−1, for its progenitor radius, ejecta mass, kinetic energy, and expansion velocity, respectively. The initial nickel mass of the PSN J17292918+7542390 turned out to be $1.55_{-0.70"> ADS </a> </span> <span class="id identifier oa_none" title="none"> <a style="color:blue" title="2020MNRAS.496.3725J" target="_blank" href="http://ui.adsabs.harvard.edu/abs/2020MNRAS.496.3725J"> ADS </a> </span> <span class="id identifier oa_GREEN" title=" Green "> <a style="color:blue" title="2007.07650" target="_blank" href="http://arxiv.org/abs/2007.07650"> arXiv </a> </span> <span class="id identifier oa_GREEN" title=" Green "> <a style="color:blue" title="39118" target="_blank" href="http://publicatio.bibl.u-szeged.hu/39118"> SZTE Publicatio </a> </span> </span> </div> <div class="short-pub-prop-list"> <span class="deleted-record">Centrally managed</span> <span class="short-pub-mtid"> Publication:31395641 </span> <span class="status-holder"><span class="status-data status-VALIDATED"> Validated </span></span> <span class="pub-core">Core Citing </span> <span class="pub-type">Journal Article (Article ) </span> <!-- && !record.category.scientific --> <span class="pub-category">Scientific</span> <div class="publication-citation" style="margin-left: 0.5cm;"> <span title="" class="citingPub-count">Citing papers: 12</span> | Independent citation: 12 | Self citation: 0 | Unknown citation: 0 | Number of citations in WoS: 11 | Number of citations in Scopus: 9 | WoS/Scopus assigned: 11 | Number of citations with DOI: 11 </div> </div> </div> </div><div class="JournalArticle Publication long-list">
<div class="authors">
<img title="Forrásközlemény" style="float: left" src="/frontend/resources/grid/publication-core-icon.png">
<img title="Idézőközlemény" style="float: left" src="/frontend/resources/grid/publication-citation-icon.png">
<div class="autype autype0"> <span class="author-name" mtid="10083232"><a
href="/gui2/?type=authors&mode=browse&sel=10083232" target="_blank">Jäger Zoltán Jr. ✉
(<span class="authorship-author-name">Jäger Zoltán</span>
<span class="authorAux-mtmt"> Fizika, csillagászat</span>)
</a>
</span>
<span class="author-affil"><span title="University of Szeged">SZTE</span>/Baja Astronomical Observatory of Szeged University</span>
;
<span class="author-name" mtid="10001530"><a
href="/gui2/?type=authors&mode=browse&sel=10001530" target="_blank">Vinkó József
(<span class="authorship-author-name">Vinkó József</span>
<span class="authorAux-mtmt"> Csillagászat asztrofizika</span>)
</a>
</span>
<span class="author-affil"><span title="Research Centre for Astronomy and Earth Sciences">CSFK</span>/Konkoly Observatory; <span title="University of Szeged">SZTE</span>/<span title="Faculty of Science and Informatics">TTIK</span>/<span title="Institute of Physics">FTCS</span>/Department of Optics and Quantum Electronics</span>
;
<span class="author-name" mtid="10026009"><a
href="/gui2/?type=authors&mode=browse&sel=10026009" target="_blank">Bíró Barna I.
(<span class="authorship-author-name">Bíró Imre Barna</span>
<span class="authorAux-mtmt"> Csillagászat</span>)
</a>
</span>
<span class="author-affil"><span title="University of Szeged">SZTE</span>/Baja Astronomical Observatory of Szeged University</span>
;
<span class="author-name" mtid="10009807"><a
href="/gui2/?type=authors&mode=browse&sel=10009807" target="_blank">Hegedüs Tibor
(<span class="authorship-author-name">Hegedüs Tibor</span>
<span class="authorAux-mtmt"> Asztrofizika</span>)
</a>
</span>
<span class="author-affil"><span title="University of Szeged">SZTE</span>/Baja Astronomical Observatory of Szeged University</span>
;
<span class="author-name" mtid="10032717"><a
href="/gui2/?type=authors&mode=browse&sel=10032717" target="_blank">Borkovits Tamás
(<span class="authorship-author-name">Borkovits Tamás</span>
<span class="authorAux-mtmt"> Csillagászat</span>)
</a>
</span>
<span class="author-affil"><span title="Research Centre for Astronomy and Earth Sciences">CSFK</span>/Konkoly Observatory; <span title="University of Szeged">SZTE</span>/Baja Astronomical Observatory of Szeged University</span>
;
<span class="author-name" >Jäger Zoltán Sr.
</span>
;
<span class="author-name" mtid="10054959"><a
href="/gui2/?type=authors&mode=browse&sel=10054959" target="_blank">Nagy Andrea P.
(<span class="authorship-author-name">Nagy Andrea</span>
<span class="authorAux-mtmt"> Asztrofizika</span>)
</a>
</span>
<span class="author-affil"><span title="Research Centre for Astronomy and Earth Sciences">CSFK</span>/Konkoly Observatory; <span title="University of Szeged">SZTE</span>/<span title="Faculty of Science and Informatics">TTIK</span>/<span title="Fizikai Intézet">FI</span>/Department of Optics and Quantum Electronics</span>
;
<span class="author-name" mtid="10017692"><a
href="/gui2/?type=authors&mode=browse&sel=10017692" target="_blank">Molnár László
(<span class="authorship-author-name">Molnár László</span>
<span class="authorAux-mtmt"> Csillagászat</span>)
</a>
</span>
<span class="author-affil"><span title="Research Centre for Astronomy and Earth Sciences">CSFK</span>/Konkoly Observatory; <span title="Eötvös Loránd University">ELTE</span>/<span title="Faculty of Science">ELU FoS</span>/Institute of Physics; <span title="Research Centre for Astronomy and Earth Sciences">CSFK</span>/<span title="Konkoly Observatory">CSI</span>/MTA CSFK Lendület Near-Field Cosmology Research Group</span>
;
<span class="author-name" mtid="10027559"><a
href="/gui2/?type=authors&mode=browse&sel=10027559" target="_blank">Kriskovics Levente
(<span class="authorship-author-name">Kriskovics Levente</span>
<span class="authorAux-mtmt"> Csillagaktivitás</span>)
</a>
</span>
<span class="author-affil"><span title="Research Centre for Astronomy and Earth Sciences">CSFK</span>/Konkoly Observatory; <span title="Eötvös Loránd University">ELTE</span>/<span title="Faculty of Science">ELU FoS</span>/Institute of Physics</span>
</div>
</div>
<div class="title"><a href="/gui2/?mode=browse¶ms=publication;31395641" target="_blank">A low-luminosity core-collapse supernova very similar to SN 2005cs</a></div> <div> <span class="journal-title">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</span>
<span class="journal-issn">(<a target="_blank" href="https://portal.issn.org/resource/ISSN/0035-8711">0035-8711</a> <a target="_blank" href="https://portal.issn.org/resource/ISSN/1365-2966">1365-2966</a>)</span>:
<span class="journal-volume">496</span> <span class="journal-issue">3</span>
<span class="page">
pp 3725-3740
</span> <span class="year">(2020)</span>
</div>
<div class="pub-footer">
<span class="language" xmlns="http://www.w3.org/1999/html">Language:
English
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<span class="id identifier oa_PAY" title=" Pay
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<a style="color:blue" title="10.1093/mnras/staa1743" target="_blank" href="https://doi.org/10.1093/mnras/staa1743">
DOI
</a>
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<span class="id identifier oa_none" title="none">
<a style="color:blue" title="000574919300071" target="_blank" href="https://www.webofscience.com/wos/woscc/full-record/000574919300071">
WoS
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<span class="id identifier oa_GREEN" title=" Green
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<a style="color:black" title="158303" target="_blank" href="http://real.mtak.hu/158303">
REAL
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<a style="color:blue" title="85101313843" target="_blank" href="http://www.scopus.com/record/display.url?origin=inward&eid=2-s2.0-85101313843">
Scopus
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<a style="color:blue" title="2020MNRAS.496.3725J luminosity Type II-P supernova (LL SN IIP). The observed sample of such events is still low, and their nature is still under debate. Such SNe are similar to SN 2005cs, a well-observed LL Type II-P event, having low expansion velocities, and small ejected 56Ni mass. We have analytic models to light curves of core-collapse SNe. This allows the estimation of the most important physical parameters, like the radius of the progenitor star, the mass of the ejected envelope, the mass of the radioactive nickel synthesized during the explosion, among others. PSN J17292918+7542390 has $R_0 = 91_{-70}^{+119} \times 10^{11} \, \text{cm}$ , $M_\text{ej} = 9.89_{-1.00}^{+2.10} \, \mathrm{ M}_{\odot }$ , $E_{\mbox{kin}} = 0.65_{-0.18}^{+0.19} \, \text{foe}$ , and $v_{\mbox{exp}} = 3332_{-347}^{+216}$ km s−1, for its progenitor radius, ejecta mass, kinetic energy, and expansion velocity, respectively. The initial nickel mass of the PSN J17292918+7542390 turned out to be $1.55_{-0.70" target="_blank" href="http://ui.adsabs.harvard.edu/abs/2020MNRAS.496.3725J luminosity Type II-P supernova (LL SN IIP). The observed sample of such events is still low, and their nature is still under debate. Such SNe are similar to SN 2005cs, a well-observed LL Type II-P event, having low expansion velocities, and small ejected 56Ni mass. We have analytic models to light curves of core-collapse SNe. This allows the estimation of the most important physical parameters, like the radius of the progenitor star, the mass of the ejected envelope, the mass of the radioactive nickel synthesized during the explosion, among others. PSN J17292918+7542390 has $R_0 = 91_{-70}^{+119} \times 10^{11} \, \text{cm}$ , $M_\text{ej} = 9.89_{-1.00}^{+2.10} \, \mathrm{ M}_{\odot }$ , $E_{\mbox{kin}} = 0.65_{-0.18}^{+0.19} \, \text{foe}$ , and $v_{\mbox{exp}} = 3332_{-347}^{+216}$ km s−1, for its progenitor radius, ejecta mass, kinetic energy, and expansion velocity, respectively. The initial nickel mass of the PSN J17292918+7542390 turned out to be $1.55_{-0.70">
ADS
</a>
</span>
<span class="id identifier oa_none" title="none">
<a style="color:blue" title="2020MNRAS.496.3725J" target="_blank" href="http://ui.adsabs.harvard.edu/abs/2020MNRAS.496.3725J">
ADS
</a>
</span>
<span class="id identifier oa_GREEN" title=" Green
">
<a style="color:blue" title="2007.07650" target="_blank" href="http://arxiv.org/abs/2007.07650">
arXiv
</a>
</span>
<span class="id identifier oa_GREEN" title=" Green
">
<a style="color:blue" title="39118" target="_blank" href="http://publicatio.bibl.u-szeged.hu/39118">
SZTE Publicatio
</a>
</span>
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<OnlyViewableByAuthor><div class="ratings">
<div class="journal-subject">Journal subject: Scopus - Astronomy and Astrophysics Rank: Q1</div>
<div class="journal-subject">Journal subject: Scopus - Space and Planetary Science Rank: Q1</div>
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<div class="publication-citation" style="margin-left: 0.5cm;">
<span title="" class="citingPub-count">Citing papers: 12</span>
| Independent citation: 12
| Self citation: 0
| Unknown citation: 0
| Number of citations in WoS: 11
| Number of citations in Scopus: 9
| WoS/Scopus assigned: 11
| Number of citations with DOI: 11
</div>
<div class="publication-citation">
<a target="_blank" href="/api/publication?cond=citations.related;eq;31395641&sort=publishedYear,desc&sort=title">
Number of cited publications: 6
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<div class="mtid"><span class="long-pub-mtid">Publication: 31395641</span>
| <span class="status-data status-VALIDATED"> Validated
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Core Citing
| <span class="type-subtype">Journal Article
( Article
)
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| <span class="pub-category">Scientific</span>
| <span class="publication-sourceOfData">RIS-ADS</span>
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<div class="lastModified">Last Modified: 2026.01.23. 08:49 Lilian Vasvari (MTMT Központ, admin)
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<div class="lockedBy">Centrally managed 2023.07.24. 15:11 Éva Pécsi (MTMT Közp 2,3, admin)
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<pre class="comment" style="margin-top: 0; margin-bottom: 0;"><u>Comments</u>: Funding Agency and Grant Number: European Union [GINOP 2.3.2-15-2016-00033]; Premium Postdoctoral Research Program of the Hungarian Academy of Sciences; Lendulet grant of the Hungarian Academy of Sciences [LP2018-7]; Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science; Center for High-Performance Computing at the University of Utah
Funding text: This work is part...</pre>
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