The Extraplanar Type II Supernova ASASSN-14jb in the Nearby Edge-on Galaxy ESO 467-G051. (arXiv:1811.11771v1 [astro-ph.HE])

The Extraplanar Type II Supernova ASASSN-14jb in the Nearby Edge-on Galaxy ESO 467-G051. (arXiv:1811.11771v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Meza_N/0/1/0/all/0/1">Nicolas Meza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prieto_J/0/1/0/all/0/1">J. L. Prieto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clocchiatti_A/0/1/0/all/0/1">A. Clocchiatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galbany_L/0/1/0/all/0/1">L. Galbany</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_J/0/1/0/all/0/1">J. P. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falco_E/0/1/0/all/0/1">E. Falco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kochanek_C/0/1/0/all/0/1">C. S. Kochanek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuncarayakti_H/0/1/0/all/0/1">H. Kuncarayakti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brimacombe_J/0/1/0/all/0/1">J. Brimacombe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holoien_T/0/1/0/all/0/1">T. W.-S. Holoien</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shappee_B/0/1/0/all/0/1">B. J. Shappee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stanek_K/0/1/0/all/0/1">K. Z. Stanek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thompson_T/0/1/0/all/0/1">T. A. Thompson</a>

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. This SN, 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 present LCOGTN $BVgri$ and $Swift$ $w2m1w1ubv$ optical and
near-UV/optical light curves and several optical spectra in the early
photospheric phase. 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. Our analysis yields $D=25pm 1$ Mpc, $M(^{56}Ni)
= 0.0210 pm 0.0025$ M$_odot$, $E_{exp}approx 0.25 times 10^{51}$ ergs,
$M_{ej}approx 6$ M$_odot$, and progenitor $R_* = 580 pm 28$ R$_odot$, which
seems to be consistent with the sub-Solar metallicity of $0.3 pm 0.1$
Z$_odot$ derived from the SN spectrum. The nebular spectrum constrains
$M_{prog} simeq 10-12 $ M$_{odot}$. We discuss the low oxygen abundance of
the host galaxy derived from the MUSE data, $12+log{(O/H)} =
8.27^{+0.16}_{-0.20}$ (O3N2 strong line method), and compare it with the
supernova spectra, which is also consistent with a sub-Solar metallicity
progenitor. We finally discuss the possible scenarios for the unusual
environment for ASASSN-14jb and conclude that either the in-situ star formation
or a runaway would imply a low mass progenitor, agreeing with our estimate from
the supernova nebular spectrum. We show that the detailed study of the
environment can agree with the stronger constrains of the transient
observations. (abridged)

http://arxiv.org/icons/sfx.gif