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We present and analyse an extensive dataset of the superluminous supernova(SLSN) LSQ14mo (z = 0.256), consisting of a multi-colour lightcurve from -30 dto +70 d in the rest-frame and a series of 6 spectra from PESSTO covering -7 dto +50 d. This is among the densest spectroscopic coverage, andbest-constrained rising lightcurve, for a fast-declining hydrogen-poor SLSN.The bolometric lightcurve can be reproduced with a millisecond magnetar modelwith ~ 4 M_sol ejecta mass, and the temperature and velocity evolution is alsosuggestive of a magnetar as the power source. Spectral modelling indicates thatthe SN ejected ~ 6 M_sol of CO-rich material with a kinetic energy of ~ 7 x10^51 erg, and suggests a partially thermalised additional source of luminositybetween -2 d and +22 d. This may be due to interaction with a shell of materialoriginating from pre-explosion mass loss. We further present a detailedanalysis of the host galaxy system of LSQ14mo. PESSTO and GROND imaging showthree spatially resolved bright regions, and we used the VLT and FORS2 toobtain a deep (five-hour exposure) spectra of the SN position and the threestar-forming regions, which are at a similar redshift. The FORS spectrum at+300 days shows no trace of SN emission lines and we place limits on thestrength of [O I] from comparisons with other Ic SNe. The deep spectra providesa unique chance to investigate spatial variations in the host star-formationactivity and metallicity. The specific star-formation rate is similar in allthree components, as is the presence of a young stellar population. However,the position of LSQ14mo exhibits a lower metallicity, with 12 + log(O/H) = 8.2in both the R23 and N2 scales (corresponding to ~ 0.3 Z_sol). We propose thatthe three bright regions in the host system are interacting, which thustriggers star-formation and forms young stellar populations.

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