We present the discovery and timing of the young (age ∼28.6 kyr) pulsar PSR J0837–2454. Based on its high latitude (b = 9.8) and dispersion measure (DM = 143 pc cm⁻³), the pulsar appears to be at a z-height of >1 kpc above the Galactic plane, but near the edge of our Galaxy. This is many times the observed scale height of the canonical pulsar population, which suggests this pulsar may have been born far out of the plane. If accurate, the young age and high z-height imply that this is the first pulsar known to be born from a runaway O/B star. In follow-up imaging with the Australia Telescope Compact Array (ATCA), we detect the pulsar with a flux density S ₁₄₀₀ = 0.18 0.05 mJy. We do not detect an obvious supernova remnant around the pulsar in our ATCA data, but we detect a colocated, low-surface-brightness region of ∼1.5 extent in archival Galactic and Extragalactic All-sky MWA Survey data. We also detect colocated Hα emission from the Southern Hα Sky Survey Atlas. Distance estimates based on these two detections come out to ∼0.9 kpc and ∼0.2 kpc, respectively, both of which are much smaller than the distance predicted by the NE2001 model (6.3 kpc) and YMW model (>25 kpc) and place the pulsar much closer to the plane of the Galaxy. If the pulsar/remnant association holds, this result also highlights the inherent difficulty in the classification of transients as “Galactic” (pulsar) or “extragalactic” (fast radio burst) toward the Galactic anticenter based solely on the modeled Galactic electron contribution to a detection.

我们介绍了年轻（年龄约 28.6 kyr）脉冲星 PSR J0837-2454 的发现和时间。基于其高纬度 ( b = 9.8) 和色散测量 (DM = 143 pc cm ^-3 )，脉冲星似乎位于银河平面上方 >1 kpc的z高度，但靠近我们银河系的边缘。这是标准脉冲星群观测到的标度高度的许多倍，这表明这颗脉冲星可能出生在远离平面的地方。如果准确的话，年轻的年龄和高z高度意味着这是已知的第一颗由失控的 O/B 恒星诞生的脉冲星。在澳大利亚望远镜紧凑阵列 (ATCA) 的后续成像中，我们探测到了通量密度为S ₁₄₀₀的脉冲星= 0.18 0.05 毫焦耳。在我们的 ATCA 数据中，我们没有在脉冲星周围检测到明显的超新星遗迹，但我们在存档的银河和河外全天 MWA 勘测数据中检测到了一个约 1.5 度的共同定位的低表面亮度区域。我们还检测到来自南部 H α 的同位H α发射天空测量图集。基于这两次探测的距离估计分别为 ~0.9 kpc 和 ~0.2 kpc，这两者都远小于 NE2001 模型（6.3 kpc）和 YMW 模型（>25 kpc）预测的距离，并将脉冲星放置在更接近银河位面。如果脉冲星/残余协会成立，这个结果也突出了将瞬变分类为“银河”（脉冲星）或“银河外”（快速无线电爆发）的固有困难，仅基于模拟的银河电子对银河反中心的贡献检测。