The extraplanar type II supernova ASASSN-14jb in the nearby edge-on galaxy ESO 467-G051
The extraplanar type II supernova ASASSN-14jb in the nearby edge-on galaxy ESO 467-G051
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DOI：
10.1051/0004-6361/201834972
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发表时间：
2018-11
影响因子：
6.5
通讯作者：
N. Meza;J. Prieto;A. Clocchiatti;L. Galbany;Joseph P. Anderson;E. Falco;C. Kochanek;H. Kuncarayakti;S. Sánchez;J. Brimacombe;T. Holoien;B. Shappee;K. Stanek;T. Thompson
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作者：
N. Meza;J. Prieto;A. Clocchiatti;L. Galbany;Joseph P. Anderson;E. Falco;C. Kochanek;H. Kuncarayakti;S. Sánchez;J. Brimacombe;T. Holoien;B. Shappee;K. Stanek;T. Thompson
我们展示 II 型超新星 ASASSN-14jb 的光学光度测量和光谱学，以及甚大望远镜 (VLT) 多单元光谱探测器 (MUSE) 对其宿主星系的整体现场观测和星云相位光谱。这颗超新星位于附近的星系 ESO 467-G051 (z = 0.006)，是由全天空自动超新星巡天 (ASAS-SN) 发现并跟踪的。我们获得了良好采样的 las cumbres 网络 (LCOGTN) BVgri 和 Swift w2m1w1ubv 光学、近紫外/光学光曲线以及早期光球阶段的几个光谱。瞬态 ASASSN-14jb 在 ESO 467-G051（一个边缘盘状星系）的恒星形成盘上方约 2 kpc 处爆炸。超新星位置距圆盘的投影距离较大，并且在投影中未检测到 1.4 kpc 半径内的任何 H II 区域，这与核心塌缩超新星前身星的标准环境相冲突，并表明前身星在双星相互作用中受到踢击的可能情况。我们对光学光曲线和光谱进行了分析，从中我们使用 II 型超新星最先进的经验方法得出了 25 ± 2 Mpc 的距离、超新星爆炸的物理特性（56Ni 质量、爆炸能量和喷射质量）以及前体的特性；即原体半径、质量和金属丰度。我们的分析得出 56Ni 质量为 0.0210 ± 0.0025 M⊙，爆炸能量为 ≈0.25 × 1051 尔格，喷射质量为 ≈6 M⊙。我们还将前身星半径限制为 R* = 580 ± 28 R⊙，这似乎与源自超新星 Fe II λ5018 线的亚太阳金属丰度 0.3 ± 0.1 Z⊙ 一致。星云光谱强烈地将前身星质量限制在 10–12 M⊙ 范围内。从 Spitzer 数据档案中，我们检测到 ASASSN-14jb 约在爆炸后 330 天，并通过 3.6 μm 和 4.5 μm 光度测定得出总尘埃质量为 10−4 M⊙。使用宿主星系的 FUV、NUV、BVgri,Ks、3.6 μm 和 4.5 μm 总星等，我们拟合了恒星族合成模型，该模型给出了 M* ≈ 1 × 109 M⊙ 的估计，年龄为 3.2 Gyr，SFR ≈0.07 M⊙ yr−1。我们还讨论了从 MUSE 数据得出的宿主星系的低氧丰度，使用强线方法的 O3N2 诊断，其平均值为 12 + log(O/H) = 8.27+0.16−0.20。我们将其与超新星光谱进行了比较，这也与亚太阳金属量前体一致。根据最近对附近边缘星系中的面外 H II 区域的观测，我们得出了与圆盘的金属丰度偏移量，该偏移量为正，但在 2σ 处与零一致，表明圆盘流出的富集。最后，我们讨论了 ASASSN-14jb 异常环境的可能情况，并得出结论，无论是原位恒星形成还是失控情况都意味着存在低质量前身星，这与我们对超新星星云光谱的估计一致。无论 ASASSN-14jb 的真实起源如何，我们表明对环境的详细研究大致符合瞬态观测的更强约束。
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 w2m1w1ubv optical, near-UV/optical light curves, and several optical spectra in the early photospheric phases. The transient ASASSN-14jb exploded ∼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 (56Ni mass, explosion energy, and ejected mass), and properties of the progenitor; namely the progenitor radius, mass, and metallicity. Our analysis yields a 56Ni mass of 0.0210 ± 0.0025 M⊙, an explosion energy of ≈0.25 × 1051 ergs, and an ejected mass of ≈6 M⊙. We also constrained the progenitor radius to be R* = 580 ± 28 R⊙ which seems to be consistent with the sub-Solar metallicity of 0.3 ± 0.1 Z⊙ derived from the supernova Fe II λ5018 line. The nebular spectrum constrains strongly the progenitor mass to be in the range 10–12 M⊙. From the Spitzer data archive we detect ASASSN-14jb ≈330 days past explosion and we derived a total dust mass of 10−4 M⊙ from the 3.6 μm and 4.5 μm photometry. Using the FUV, NUV, BVgri,Ks, 3.6 μm, and 4.5 μm total magnitudes for the host galaxy, we fit stellar population synthesis models, which give an estimate of M* ≈ 1 × 109 M⊙, an age of 3.2 Gyr, and a SFR ≈0.07 M⊙ 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+0.16−0.20 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 2σ, 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.