A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä

The extraplanar type II supernova ASASSN-14jb in the nearby edge-on galaxy ESO 467-G051




TekijätMeza N, Prieto JL, Clocchiatti A, Galbany L, Anderson JP, Falco E, Kochanek CS, Kuncarayakti H, Sanchez SF, Brimacombe J, Holoien TWS, Shappee BJ, Stanek KZ, Thompson TA

Nicolás Meza, J. L. Prieto, A. Clocchiatti, L. Galbany, J. P. Anderson, E. Falco, C. S. Kochanek,
H. Kuncarayakti, S. F. Sánchez, J. Brimacombe, T. W.-S. Holoien, B. J. Shappee,
K. Z. Stanek, T. A. Thompson

KustantajaEDP SCIENCES S A

Julkaisuvuosi2019

JournalAstronomy and Astrophysics

Tietokannassa oleva lehden nimiASTRONOMY & ASTROPHYSICS

Lehden akronyymiASTRON ASTROPHYS

Artikkelin numeroARTN A57

Vuosikerta629

Sivujen määrä23

ISSN1432-0746

DOIhttps://doi.org/10.1051/0004-6361/201834972

Rinnakkaistallenteen osoitehttps://research.utu.fi/converis/portal/detail/Publication/42497459


Tiivistelmä
We present optical photometry and spectroscopy of the Type II supernova ASASSN-14jb, together with Very Large Telescope (VLT) Multi Unit Spectroscopic Explorer (MUSE) integral field observations of its host galaxy and a nebular-phase spectrum. 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 las cumbres network (LCOGTN) BVgri and Swift omega 2m1 omega 1ubv optical, near-UV/optical light curves, and several optical spectra in the early photospheric phases. The transient ASASSN-14jb exploded similar to 2 kpc above the star-forming disk of ESO 467-G051, an edge-on disk galaxy. The large projected distance from the disk of the supernova position and the 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. We present analysis of the optical light curves and spectra, from which we derived a distance of 25 +/- 2 Mpc using state-of-the-art empirical methods for Type II SNe, physical properties of the SN explosion (Ni-56 mass, explosion energy, and ejected mass), and properties of the progenitor; namely the progenitor radius, mass, and metallicity. Our analysis yields a Ni-56 mass of 0.0210 +/- 0.0025 M-circle dot, an explosion energy of approximate to 0.25 x 10(51) ergs, and an ejected mass of approximate to 6 M-circle dot. We also constrained the progenitor radius to be R-* = 580 +/- 28 R-circle dot which seems to be consistent with the sub-Solar metallicity of 0.3 +/- 0.1 Z(circle dot) 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-circle dot. From the Spitzer data archive we detect ASASSN-14jb approximate to 330 days past explosion and we derived a total dust mass of 10(-4) M-circle dot 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 give an estimate of M-* approximate to 1 x 10(9) M-circle dot, an age of 3.2 Gyr, and a SFR approximate to 0.07 M-circle dot yr(-1). 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(-0.20)(+0.16) using the O3N2 diagnostic with strong line methods. We compared 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 derived 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 that the detailed study of the environment roughly agree with the stronger constraints from the observation of the transient.

Ladattava julkaisu

This is an electronic reprint of the original article.
This reprint may differ from the original in pagination and typographic detail. Please cite the original version.





Last updated on 2024-26-11 at 20:18