NGC 2770: High supernova rate due to interaction

Autor: Peter Kamphuis, Natalia Gotkiewicz, Christina C. Thöne, Michał J. Michałowski, Jens Hjorth, Antonio de Ugarte Postigo, Wojciech Dimitrov, A. Leśniewska, M. P. Koprowski
Přispěvatelé: National Science Centre (Poland), Fulbright Commission, Ministerio de Economía y Competitividad (España), European Commission, Villum Fonden, Federal Ministry of Education and Research (Germany)
Rok vydání: 2020
Předmět:
Zdroj: Digital.CSIC. Repositorio Institucional del CSIC
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Michałowski, M J, Thöne, C, De Ugarte Postigo, A, Hjorth, J, Leśniewska, A, Gotkiewicz, N, Dimitrov, W, Koprowski, M P & Kamphuis, P 2020, ' NGC 2770 : High supernova rate due to interaction ', Astronomy and Astrophysics, vol. 642, A84 . https://doi.org/10.1051/0004-6361/202038719
Popis: 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.
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).
Databáze: OpenAIRE
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