NGC 2770: High supernova rate due to interaction
Context. Galaxies that hosted many core-collapse supernova (SN) explosions can be used to study the conditions necessary for the formation of massive stars. NGC 2770 was dubbed an SN factory because it hosted four core-collapse SNe in 20 years (three type Ib and one type IIn). Its star formation rat...
| Autores: | , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2020 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/222465 |
| Acceso en línea: | http://hdl.handle.net/10261/222465 |
| Access Level: | acceso abierto |
| Palabra clave: | Galaxies: evolution Galaxies: individual: NGC 2770 Galaxies: ISM Galaxies: star formation Supernovae: general Radio lines: galaxies |
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NGC 2770: High supernova rate due to interaction |
| title |
NGC 2770: High supernova rate due to interaction |
| spellingShingle |
NGC 2770: High supernova rate due to interaction Michałowski, M. J. Galaxies: evolution Galaxies: individual: NGC 2770 Galaxies: ISM Galaxies: star formation Supernovae: general Radio lines: galaxies |
| title_short |
NGC 2770: High supernova rate due to interaction |
| title_full |
NGC 2770: High supernova rate due to interaction |
| title_fullStr |
NGC 2770: High supernova rate due to interaction |
| title_full_unstemmed |
NGC 2770: High supernova rate due to interaction |
| title_sort |
NGC 2770: High supernova rate due to interaction |
| dc.creator.none.fl_str_mv |
Michałowski, M. J. Thöne, Cristina Carina Ugarte Postigo, Antonio de Hjorth, Jens Leśniewska, A. Gotkiewicz, N. Dimitrov, W. Koprowski, M. P. Kamphuis, P. |
| author |
Michałowski, M. J. |
| author_facet |
Michałowski, M. J. Thöne, Cristina Carina Ugarte Postigo, Antonio de Hjorth, Jens Leśniewska, A. Gotkiewicz, N. Dimitrov, W. Koprowski, M. P. Kamphuis, P. |
| author_role |
author |
| author2 |
Thöne, Cristina Carina Ugarte Postigo, Antonio de Hjorth, Jens Leśniewska, A. Gotkiewicz, N. Dimitrov, W. Koprowski, M. P. Kamphuis, P. |
| author2_role |
author author author author author author author author |
| dc.contributor.none.fl_str_mv |
National Science Centre (Poland) Fulbright Commission Ministerio de Economía y Competitividad (España) European Commission Villum Fonden Federal Ministry of Education and Research (Germany) Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| dc.subject.none.fl_str_mv |
Galaxies: evolution Galaxies: individual: NGC 2770 Galaxies: ISM Galaxies: star formation Supernovae: general Radio lines: galaxies |
| topic |
Galaxies: evolution Galaxies: individual: NGC 2770 Galaxies: ISM Galaxies: star formation Supernovae: general Radio lines: galaxies |
| description |
Context. Galaxies that hosted many core-collapse supernova (SN) explosions can be used to study the conditions necessary for the formation of massive stars. NGC 2770 was dubbed an SN factory because it hosted four core-collapse SNe in 20 years (three type Ib and one type IIn). Its star formation rate (SFR) was reported to not be enhanced and, therefore, not compatible with such a high SN rate. Aims. We aim to explain the high SN rate of NGC 2770. Methods. We used archival HI line data for NGC 2770 and reinterpreted the Hα and optical continuum data. Results. Even though the continuum-based SFR indicators do not yield high values, the dust-corrected Hα luminosity implies a high SFR, consistent with the high SN rate. Such a disparity between the SFR estimators is an indication of recently enhanced star formation activity because the continuum indicators trace long timescales of the order of 100 Myr, unlike the line indicators, which trace timescales of the order of 10 Myr. Hence, the unique feature of NGC 2770 compared to other galaxies is the fact that it was observed very shortly after the enhancement of the SFR. It also has high dust extinction, E(B - V) above 1 mag. We provide support for the hypothesis that the increased SFR in NGC 2770 is due to the interaction with its companion galaxies. We report an HI bridge between NGC 2770 and its closest companion and the existence of a total of four companions within 100 kpc (one identified for the first time). There are no clear HI concentrations close to the positions of SNe in NGC 2770 such as those detected for hosts of gamma-ray bursts (GRBs) and broad-lined SNe type Ic (IcBL). This suggests that the progenitors of type Ib SNe are not born out of recently accreted atomic gas, as was suggested for GRB and IcBL SN progenitors. © ESO 2020. |
| publishDate |
2020 |
| dc.date.none.fl_str_mv |
2020 2020 2020 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 Publisher's version info:eu-repo/semantics/publishedVersion |
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article |
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publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/10261/222465 |
| url |
http://hdl.handle.net/10261/222465 |
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Inglés |
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Inglés |
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#PLACEHOLDER_PARENT_METADATA_VALUE# #PLACEHOLDER_PARENT_METADATA_VALUE# #PLACEHOLDER_PARENT_METADATA_VALUE# info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/RyC-2012-09975 info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/RyC-2012-09984 info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2017-89384-P http://dx.doi.org/10.1051/0004-6361/202038719 Sí |
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info:eu-repo/semantics/openAccess |
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openAccess |
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EDP Sciences |
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EDP Sciences |
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reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC instname:Consejo Superior de Investigaciones Científicas (CSIC) |
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Consejo Superior de Investigaciones Científicas (CSIC) |
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DIGITAL.CSIC. Repositorio Institucional del CSIC |
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DIGITAL.CSIC. Repositorio Institucional del CSIC |
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1869420581999345664 |
| spelling |
NGC 2770: High supernova rate due to interactionMichałowski, M. J.Thöne, Cristina CarinaUgarte Postigo, Antonio deHjorth, JensLeśniewska, A.Gotkiewicz, N.Dimitrov, W.Koprowski, M. P.Kamphuis, P.Galaxies: evolutionGalaxies: individual: NGC 2770Galaxies: ISMGalaxies: star formationSupernovae: generalRadio lines: galaxiesContext. Galaxies that hosted many core-collapse supernova (SN) explosions can be used to study the conditions necessary for the formation of massive stars. NGC 2770 was dubbed an SN factory because it hosted four core-collapse SNe in 20 years (three type Ib and one type IIn). Its star formation rate (SFR) was reported to not be enhanced and, therefore, not compatible with such a high SN rate. Aims. We aim to explain the high SN rate of NGC 2770. Methods. We used archival HI line data for NGC 2770 and reinterpreted the Hα and optical continuum data. Results. Even though the continuum-based SFR indicators do not yield high values, the dust-corrected Hα luminosity implies a high SFR, consistent with the high SN rate. Such a disparity between the SFR estimators is an indication of recently enhanced star formation activity because the continuum indicators trace long timescales of the order of 100 Myr, unlike the line indicators, which trace timescales of the order of 10 Myr. Hence, the unique feature of NGC 2770 compared to other galaxies is the fact that it was observed very shortly after the enhancement of the SFR. It also has high dust extinction, E(B - V) above 1 mag. We provide support for the hypothesis that the increased SFR in NGC 2770 is due to the interaction with its companion galaxies. We report an HI bridge between NGC 2770 and its closest companion and the existence of a total of four companions within 100 kpc (one identified for the first time). There are no clear HI concentrations close to the positions of SNe in NGC 2770 such as those detected for hosts of gamma-ray bursts (GRBs) and broad-lined SNe type Ic (IcBL). This suggests that the progenitors of type Ib SNe are not born out of recently accreted atomic gas, as was suggested for GRB and IcBL SN progenitors. © ESO 2020.M.J.M. acknowledges the support of the National Science Centre, Poland through the SONATA BIS grant 2018/30/E/ST9/00208, and of the Polish-U.S. Fulbright Commission. A.d.U.P. and C.C.T. acknowledge the support from Ramon y Cajal fellowships (RyC-2012-09975 and RyC-2012-09984) and from the Spanish research project AYA2017-89384-P. A.L. acknowledges the support of the National Science Centre, Poland through the SONATA BIS grant 2018/30/E/ST9/00208. J.H. was supported by a VILLUM FONDEN Investigator grant (project number 16599). M.P.K. acknowledges support from the First TEAM grant of the Foundation for Polish Science No. POIR.04.04.00-00-5D21/18-00. P.K. is partially supported by the BMBF project 05A17PC2 for D-MeerKAT. The WSRT is operated by the Netherlands Foundation for Research in Astronomy with financial support from the Netherlands Organization for Scientific Research (NWO).Peer reviewedEDP SciencesNational Science Centre (Poland)Fulbright CommissionMinisterio de Economía y Competitividad (España)European CommissionVillum FondenFederal Ministry of Education and Research (Germany)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202020202020info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/222465reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/RyC-2012-09975info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/RyC-2012-09984info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2017-89384-Phttp://dx.doi.org/10.1051/0004-6361/202038719Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2224652026-05-22T06:33:51Z |
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15,811543 |