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The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

T.-W. ChenArgelander Institute for Astronomy, University of Bonn, Auf dem Hgel 71, 53121 Bonn, GermanyM. NichollHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USAS. J. SmarttAstrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UKP. A. MazzaliAstrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UKR. M. YatesMax-Planck-Institut fr Extraterrestrische Physik, Giessenbachstrae 1, 85748 Garching, GermanyT. J. MoriyaDivision of Theoretical Astronomy, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, 181-8588 Tokyo, JapanC. InserraAstrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UKN. LangerArgelander Institute for Astronomy, University of Bonn, Auf dem Hgel 71, 53121 Bonn, GermanyT. KrühlerY.-C. PanDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USAR. KotakAstrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UKL. GalbanyPhysics and Astronomy Department, University of Pittsburgh, Pittsburgh, PA 15260, USAP. SchadyMax-Planck-Institut fr Extraterrestrische Physik, Giessenbachstrae 1, 85748 Garching, GermanyP. WisemanMax-Planck-Institut fr Extraterrestrische Physik, Giessenbachstrae 1, 85748 Garching, GermanyJ. GreinerMax-Planck-Institut fr Extraterrestrische Physik, Giessenbachstrae 1, 85748 Garching, GermanyS. SchulzeDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, 76100 Rehovot, IsraelA. W. S. ManESO, Karl-Schwarzschild-Strasse 2, 85748 Garching-bei-Mnchen, GermanyA. JerkstrandMax-Planck-Institut fr Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching-bei-Mnchen, GermanyK. W. SmithAstrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UKM. DennefeldInstitut d'Astrophysique de Paris, CNRS, and Universit Pierre et Marie Curie, 98bis boulevard Arago, 75014 Paris, FranceC. BaltayPhysics Department, Yale University, 217 Prospect Street, New Haven, CT 06511-8499, USAJ. BolmerEuropean Southern Observatory, Alonso de Crdova 3107, Vitacura, Casilla 19001, Santiago 19, ChileE. KankareAstrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UKF. KnustMax-Planck-Institut fr Extraterrestrische Physik, Giessenbachstrae 1, 85748 Garching, GermanyK. MaguireAstrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UKD. RabinowitzPhysics Department, Yale University, 217 Prospect Street, New Haven, CT 06511-8499, USAS. RostamiPhysics Department, Yale University, 217 Prospect Street, New Haven, CT 06511-8499, USAM. SullivanDepartment of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UKD. R. YoungAstrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UK

2017en

ABI

Annotatsiya

We present and analyse an extensive dataset of the superluminous supernova (SLSN) LSQ14mo (z = 0.256), consisting of a multicolour light curve from -30 d to +70 d in the rest-frame (relative to maximum light) and a series of six spectra from PESSTO covering -7 d to +50 d. This is among the densest spectroscopic coverage, and best-constrained rising light curve, for a fast-declining hydrogen-poor SLSN. The bolometric light curve can be reproduced with a millisecond magnetar model with 4 M ejecta mass, and the temperature and velocity evolution is also suggestive of a magnetar as the power source. Spectral modelling indicates that the SN ejected 6 M of CO-rich material with a kinetic energy of 7 10 51 erg, and suggests a partially thermalised additional source of luminosity between -2 d and +22 d. This may be due to interaction with a shell of material originating from pre-explosion mass loss. We further present a detailed analysis of the host galaxy system of LSQ14mo. PESSTO and GROND imaging show three spatially resolved bright regions, and we used the VLT and FORS2 to obtain a deep (five-hour exposure) spectra of the SN position and the three star-forming regions, which are at a similar redshift. The FORS2 spectrum at +300 days shows no trace of SN emission lines and we place limits on the strength of [O i] from comparisons with other Ic supernovae. The deep spectra provides a unique chance to investigate spatial variations in the host star-formation activity and metallicity. The specific star-formation rate is similar in all three components, as is the presence of a young stellar population. However, the position of LSQ14mo exhibits a lower metallicity, with 12 + log(O/H) = 8.2 in both the R 23 and N2 scales (corresponding to 0.3 Z ). We propose that the three bright regions in the host system are interacting, which could induce gas flows triggering star formation in low-metallicity regions.

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DOI: 10.1051/0004-6361/201630163

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