Volume 610, February 2018
|Number of page(s)||11|
|Published online||12 February 2018|
The host of the Type I SLSN 2017egm
A young, sub-solar metallicity environment in a massive spiral galaxy
1 Instituto de Astrofisica de Andalucia (IAA-CSIC), Glorieta de la Astronomia s/n, 18008 Granada, Spain
2 Dark Cosmology Centre, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark
3 INAF – Capodimonte Observatory, Salita Moiariello 16, 80131 Napoli, Italy
4 International Center for Relativistic Astrophysics, Piazzale della Repubblica, 2, 65122 Pescara, Italy
5 Centro Astronómico Hispano-Alemán, Calar Alto, CSIC-MPG, Sierra de los Filabres-04550 Gérgal ( Almería), Spain
Received: 12 August 2017
Accepted: 1 October 2017
Context. Type I superluminous supernova (SLSN) host galaxies are predominantly low-metallicity, highly star-forming (SF) dwarfs. One of the current key questions is whether Type I SLSNe can only occur in such environments and hosts.
Aims. Here we present an integral-field study of the massive, high-metallicity spiral NGC 3191, the host of SN 2017egm, the closest Type I SLSN known to date. We use data from PMAS/CAHA and the public MaNGA survey to shed light on the properties of the SLSN site and the origin of star formation in this non-starburst spiral galaxy.
Methods. We map the physical properties of different H ii regions throughout the galaxy and characterise their stellar populations using the STARLIGHT fitting code. Kinematical information allows us to study a possible interaction with its neighbouring galaxy as the origin of recent star formation activity which could have caused the SLSN.
Results. NGC 3191 shows intense star formation in the western part with three large SF regions of low metallicity. Taking only the properties of emitting gas, the central regions of the host have a higher metallicity, a lower specific star formation rate, and lower ionisation. Modelling the stellar populations gives a different picture: the SLSN region has two dominant stellar populations with different ages, the younger one with an age of 2–10 Myr and lower metallicity, likely the population from which the SN progenitor originated. Emission line kinematics of NGC 3191 show indications of interaction with its neighbour MCG+08-19-017 at ~45 kpc, which might be responsible for the recent starburst. In fact, this galaxy pair has hosted a total of four SNe, 1988B (Type Ia), SN 2003ds (Type Ic in MCG+08-19-017), PTF10bgl (Type II), and 2017egm, underlying the enhanced SF in both galaxies due to interaction.
Conclusions. Our study shows that care should be taken when interpreting global host and even gas properties without looking at the stellar population history of the region. The SLSNe seem to be consistent with massive stars (>20 M⊙) requiring low metallicity (<0.6 Z⊙), environments that can also occur in massive late-type galaxies, but not necessarily with starbursts.
Key words: supernovae: individual: 2017egm / galaxies: general
© ESO, 2018
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