Context :

Aims : We present optical photometry and spectroscopy of the Type II supernova ASASSN-14jb , together with VLT MUSE IFU observations of its host galaxy and a nebular-phase spectrum .

Methods : This supernova , in the nearby galaxy ESO 467-G051 ( z = 0.006 ) , was discovered and followed-up by the All Sky Automated Survey for SuperNovae ( ASAS-SN ) .
We obtained well-sampled LCOGTN BVgri and Swift w 2 m 1 w 1 ubv optical and near-UV/optical light curves and several optical spectra in the early photospheric phases .
ASASSN-14jb exploded \sim 2 kpc above the star-forming disk of ESO 467-G051 , an edge-on disk galaxy .
The large projected distance from the disk and non-detection of any H II region in a 1.4 kpc radius in projection are in conflict with the standard environment of core-collapse supernova progenitors and suggests the possible scenario that the progenitor received a kick in a binary interaction .

Results : We present analysis of the optical light curves and spectra , from which we derive a distance of 25 \pm 1 Mpc using state of the art empirical methods for Type II SNe , physical properties of the SN explosion ( ^ { 56 } Ni mass , explosion energy , and ejected mass ) and properties of the progenitor , namely the progenitor radius , mass and metallicity .
Our analysis yields a ^ { 56 } Ni mass of 0.0210 \pm 0.0025 M _ { \odot } , an explosion energy of \approx 0.25 \times 10 ^ { 5 } 1 ergs and an ejected mass of \approx 6 M _ { \odot } .
We also constrain the progenitor radius to be R _ { * } = 580 \pm 28 R _ { \odot } which seems to be consistent with the sub-Solar metallicity of 0.3 \pm 0.1 Z _ { \odot } derived from the supernova Fe II \lambda 5018 line .
The nebular spectrum constrains strongly the progenitor mass to be in the range 10-12 M _ { \odot } .
From Spitzer data archive we detect ASASSN-14jb \approx 330 days past explosion and we derive a total dust mass of 10 ^ { -4 } M _ { \odot } from the 3.6 \mu m and 4.5 \mu m photometry .
Using the FUV , NUV , BVgri , K _ { s } , 3.6 \mu m , and 4.5 \mu m total magnitudes for the host galaxy , we fit stellar population synthesis models which gives an estimate of M _ { * } \approx 1 \times 10 ^ { 9 } M _ { \odot } , an age of 3.2 Gyr , and a SFR \approx 0.07 M _ { \odot } /yr .
We also discuss the low oxygen abundance of the host galaxy derived from the MUSE data , having an average of 12 + \log { ( O / H ) } = 8.27 ^ { +0.16 } _ { -0.20 } using the O3N2 diagnostic , with strong line methods and compare it with the supernova spectra , which is also consistent with a sub-Solar metallicity progenitor .
Following recent observations of extraplanar H II regions in nearby edge-on galaxies , we derive the metallicity offset from the disk , being positive ( but consistent with zero at 2 \sigma ) , suggesting enrichment from disk outflows .
We finally discuss the possible scenarios for the unusual environment for ASASSN-14jb and conclude that either the in-situ star formation or runaway scenario would imply a low mass progenitor , agreeing with our estimate from the supernova nebular spectrum .
Regardless of the true origin of ASASSN-14jb we show in this work that the detailed study of the environment can roughly agree with the stronger constrains of the transient observations .

Conclusions :