论文标题
与新兴的脉冲星云一致的122 MPC的平面射击瞬变
A Flat-Spectrum Radio Transient at 122 Mpc consistent with an Emerging Pulsar Wind Nebula
论文作者
论文摘要
我们报告了VT 1137-0337的发现和随访观察结果：在VLA Sky Survey（Vlass）中系统地搜索时搜索外层次爆炸的不寻常的无线电瞬变。 VT 1137-0337位于矮星星系中最亮的区域（Stellar Mass $ \ SIM \ SIM 10^{8.3} M _ {\ odot} $，Star形成率$ \ sim 0.5 m _ {\ odot} $ yr $ $ yr $^{ - 1} $ yr $^{ - 1} $）at luminsusy con。它的3 GHz亮度为$ \ sim 2.5 \ times 10^{28} $ erg s $^{ - 1} $ hz $^{ - 1} $与与密集的杂物交互和相关性相关的发光无线电超新星相当。 However, its broadband radio spectrum - a featureless power law $\propto ν^{-0.35 \pm 0.02}$ over a range of $\gtrsim$10$\times$ in frequency and fading at a rate of $\sim$ 5% per year over 4 years - cannot be directly explained by the shock of a stellar explosion.由各种积聚的黑洞发起的喷气式飞机也很难说明VT 1137-0337的观察性质组合。取而代之的是，我们建议VT 1137-0337是$ \ sim $数十年来的pulsar风星云，最近从其周围超新星弹射器的自由不透明度中出现。如果星云由Spindow提供动力，则中央中子星应高度磁化，并具有$ \ sim 10^{13}的表面偶极场 - 10^{14} $ g，而当今的自旋周期为$ \ sim 10-100-100 $ ms。或者，星云可以通过从磁场中释放磁能提供动力。已经提出了磁性星云来解释与重复的快速无线电爆发FRB 121102和FRB 190520b相关的持续无线电源。这些FRB持续的来源以前尚未被视为瞬态，但在其无线电发光，光谱指数和宿主星系性能中确实与VT 1137-0337具有显着相似之处。
We report the discovery and follow-up observations of VT 1137-0337: an unusual radio transient found in our systematic search for extragalactic explosions in the VLA Sky Survey (VLASS). VT 1137-0337 is located in the brightest region of a dwarf starburst galaxy (stellar mass $\sim 10^{8.3} M_{\odot}$, star formation rate $\sim 0.5 M_{\odot}$ yr$^{-1}$) at a luminosity distance of 121.6 Mpc. Its 3 GHz luminosity of $\sim 2.5 \times 10^{28}$ erg s$^{-1}$ Hz$^{-1}$ is comparable to luminous radio supernovae associated with dense circumstellar interaction and relativistic outflows. However, its broadband radio spectrum - a featureless power law $\propto ν^{-0.35 \pm 0.02}$ over a range of $\gtrsim$10$\times$ in frequency and fading at a rate of $\sim$ 5% per year over 4 years - cannot be directly explained by the shock of a stellar explosion. Jets launched by various classes of accreting black holes also struggle to account for VT 1137-0337's combination of observational properties. Instead, we propose that VT 1137-0337 is a $\sim$decades old pulsar wind nebula that has recently emerged from within the free-free opacity of its surrounding supernova ejecta. If the nebula is powered by spindown, the central neutron star should be highly magnetized, with a surface dipole field of $\sim 10^{13} - 10^{14}$ G and a present-day spin period of $\sim 10 - 100$ ms. Alternatively, the nebula may be powered by the release of magnetic energy from a magnetar. Magnetar nebulae have been proposed to explain the persistent radio sources associated with the repeating fast radio bursts FRB 121102 and FRB 190520B. These FRB persistent sources have not previously been observed as transients, but do bear a striking resemblance to VT 1137-0337 in their radio luminosity, spectral index, and host galaxy properties.
