论文标题
鳗鱼脉冲风星云：HAWC J1826-128和HESS J1826-130
The Eel Pulsar Wind Nebula: a PeVatron-Candidate Origin for HAWC J1826-128 and HESS J1826-130
论文作者
论文摘要
HAWC J1826-128是高空水Cherenkov（HAWC）天文台检测到的最明亮的银河TEV伽马射线来源之一，光子能量延长了近$ \ sim $ 100 tev。该HAWC来源在空间上与H.E.S.S. TEV源Hess J1826-130和与GEV Pulsar PSR J1826-1256相关的“ Eel” Pulsar Wind Nebula（PWN）。在X射线乐队中，Chandra和XMM-Newton在eel PWN中表明，鳗鱼pwn既由紧凑型星云（$ \ sim $ 15”）和diffuse X射线排放（$ \ sim $ 6'$ \ times $ 2'）组成同步燃烧效果，除了Hess J1826-130和漫射的X射线PWN之间的空间巧合，我们使用X射线和伽马射线数据的多波长光谱分布（SED）分析确立了与EEL PWN相关的Leptonic pwn pwn的leptonig pwn。 $ \ sim $ 1 $μ$ g，（2）比特征年龄（$ t \ sim5.7 $ kyr）明显年轻的年龄（$τ= 14.4 $ kyr）和（3）最大的电子能量为$ E_ {max}我们的结果表明，EEL PWN可能是由$ \ sim $ 6 kyr-gred Pulsar PSR PSR J1826-1256提供动力的Leptonic Pevatron粒子加速器，其旋转功率为$ 3.6 \ times 10^{36} $ ERG S $^{ - 1} $。
HAWC J1826-128 is one of the brightest Galactic TeV gamma-ray sources detected by the High Altitude Water Cherenkov (HAWC) Observatory, with photon energies extending up to nearly $\sim$100 TeV. This HAWC source spatially coincides with the H.E.S.S. TeV source HESS J1826-130 and the "Eel" pulsar wind nebula (PWN), which is associated with the GeV pulsar PSR J1826-1256. In the X-ray band, Chandra and XMM-Newton revealed that the Eel PWN is composed of both a compact nebula ($\sim$15") and diffuse X-ray emission ($\sim$6'$\times$2') extending away from the pulsar. Our NuSTAR observation detected hard X-ray emission from the compact PWN up to $\sim$20 keV and evidence of the synchrotron burn-off effect. In addition to the spatial coincidence between HESS J1826-130 and the diffuse X-ray PWN, our multi-wavelength spectral energy distribution (SED) analysis using X-ray and gamma-ray data establishes a leptonic origin of the TeV emission associated with the Eel PWN. Furthermore, our evolutionary PWN SED model suggests (1) a low PWN B-field of $\sim$1 $μ$G, (2) a significantly younger pulsar age ($t \sim5.7$ kyr) than the characteristic age ($τ= 14.4$ kyr) and (3) a maximum electron energy of $E_{max} = 2$ PeV. The low B-field as well as the putative supersonic motion of the pulsar may account for the asymmetric morphology of the diffuse X-ray emission. Our results suggest that the Eel PWN may be a leptonic PeVatron particle accelerator powered by the $\sim$6-kyr-old pulsar PSR J1826-1256 with a spin-down power of $3.6 \times 10^{36}$ erg s$^{-1}$.
