We report the follow-up of 10 pulsars discovered by the Five-hundred-metre Aperture Spherical radio-Telescope (FAST) during its commissioning. The pulsars were discovered at a frequency of 500-MHz using the ultrawide-band (UWB) receiver in drift-scan mode, as part of the Commensal Radio Astronomy FAST Survey (CRAFTS). We carried out the timing campaign with the 100-m Effelsberg radio-telescope at L-band around 1.36 GHz. Along with 11 FAST pulsars previously reported, FAST seems to be uncovering a population of older pulsars, bordering and/or even across the pulsar death-lines. We report here two sources with notable characteristics. PSR J1951+4724 is a young and energetic pulsar with nearly 100 per cent of linearly polarized flux density and visible up to an observing frequency of 8 GHz. PSR J2338+4818, a mildly recycled pulsar in a 95.2-d orbit with a Carbon–Oxygen white dwarf (WD) companion of |$\gtrsim 1\, \rm {M}_{\odot }$|⁠, based on estimates from the mass function. This system is the widest WD binary with the most massive companion known to-date. Conspicuous discrepancy was found between estimations based on NE2001 and YMW16 electron density models, which can be attributed to underrepresentation of pulsars in the sky region between Galactic longitudes 70° < l < 100°. This work represents one of the early CRAFTS results, which start to show potential to substantially enrich the pulsar sample and refine the Galactic electron density model.

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FAST 早期脉冲星发现：埃菲尔斯堡后续行动

我们报告了五百米孔径球面射电望远镜 (FAST) 在调试期间发现的 10 颗脉冲星的后续行动。作为公共射电天文快速测量 (CRAFTS) 的一部分，使用超宽带 (UWB) 接收器在漂移扫描模式下以 500 MHz 的频率发现了这些脉冲星。我们使用位于L的 100 米 Effelsberg 射电望远镜进行了计时活动- 1.36 GHz 左右的频段。连同之前报道的 11 颗 FAST 脉冲星，FAST 似乎正在发现一批更老的脉冲星，它们接近和/或什至跨越脉冲星死亡线。我们在这里报告两个具有显着特征的来源。PSR J1951+4724 是一颗年轻而充满活力的脉冲星，具有近 100% 的线性极化通量密度，并且在高达 8 GHz 的观测频率下可见。PSR J2338+4818，一颗在 95.2 d 轨道上温和回收的脉冲星，与碳氧白矮星 (WD) 伴星|$\gtrsim 1\, \rm {M}_{\odot }$|⁠，基于质量函数的估计。该系统是最宽的 WD 二进制文件，拥有迄今为止已知的最庞大的伴星。在基于 NE2001 和 YMW16 电子密度模型的估计之间发现了明显的差异，这可归因于在银河经度 70° < l < 100°之间的天空区域中脉冲星的代表性不足。这项工作代表了早期的 CRAFTS 结果之一，它开始显示出极大地丰富脉冲星样本和改进银河电子密度模型的潜力。