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arXiv 0705.2378astro-ph
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来自PSR J1809-1917及其脉冲星风星云的X射线发射，可能与TeV gamma-ray源HESS J1809-193有关

X-ray emission from PSR J1809-1917 and its pulsar wind nebula, possibly associated with the TeV gamma-ray source HESS J1809-193

O. Kargaltsev, G. G. Pavlov

备注：
13 pages, 10 figures and 3 tables, submitted to ApJ. Version with the high-resolution figures is available at http://www.astro.psu.edu/users/green/J1809/ms_astroph.pdf
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摘要：

利用Chandra探测到了50千光年的脉冲星J1809-1917的X射线辐射，并对脉冲星风星云进行了分辨。当n_{H} =0.7 \times 10^{22} cm^{-2}时，脉冲星光谱符合PL+BB模型，光子指数为1.2，BB温度为2 MK.在3.5 kpc的合理距离处，PL分量（在0.5-8 keV波段）的光度为（4 \pm 1）\times 10^{31}尔格s^{-1}，BB分量（测辐射热）的光度为~1 \times 10^{32}尔格s^{-1}。明亮的内部PWN分量的3“\times 12”大小在南北方向上被拉长，脉冲星靠近其南端。该部件浸没在较大的（20“\times 40”）、类似的较低表面亮度的细长外部PWN部件中。紧凑PWN的细长形状可以解释为由于脉冲星的超声速运动的脉冲星风的冲压压力约束。PWN光谱符合PL模型，光子指数为1.4 \pm 0.1，0.5-8 keV光度为4 \times 10^{32} ergs ^{-1}。紧凑的PWN似乎是在一个大规模的（~4' \times 4'）发射更扩展到南部的脉冲星，即在所谓的脉冲星运动的方向。为了解释运动脉冲星前方的扩展X射线发射，必须调用脉冲星风的强内禀各向异性，或者假设这种发射来自被不对称反向SNR激波扫过的遗迹PWN。脉冲星及其PWN位于未确认的TeV源HESS J1809-193的范围内，HESS J1809-193的最亮部分在脉冲星以南偏移约8'，即与大尺度X射线发射方向相同。虽然J1809-1917和HESS J1809-193之间的联系似乎是合理的，但为HESS J1809-193提供动力的相对论电子的另一个来源可能是偶然发现的X射线源CXFJ 180940.7 -192544。

英文摘要：

We detected X-ray emission from the 50-kyr-old pulsar J1809-1917 and resolved its pulsar wind nebula (PWN) with Chandra. The pulsar spectrum fits PL+BB model with the photon index of 1.2 and the BB temperature of 2 MK for n_{H}=0.7\times 10^{22} cm^{-2}. The luminosities are(4\pm 1)\times 10^{31} ergs s^{-1} for the PL component (in the 0.5-8 keV band) and ~1\times 10^{32} ergs s^{-1} for the BB component (bolometric) at a plausible distance of 3.5 kpc. The bright inner PWN component of a 3''\times12'' size is elongated in the north-south direction, with the pulsar close to its south end. This component is immersed in a larger (20''\times40''), similarly elongated outer PWN component of lower surface brightness. The elongated shape of the compact PWN can be explained by the ram pressure confinement of the pulsar wind due to the supersonic motion of the pulsar. The PWN spectrum fits a PL model with photon index of 1.4\pm0.1 and 0.5-8 keV luminosity of 4\times10^{32} ergs s^{-1}. The compact PWN appears to be inside a large-scale (~4'\times4') emission more extended to the south of the pulsar, i.e. in the direction of the alleged pulsar motion. To explain the extended X-ray emission ahead of the moving pulsar, one has to invoke strong intrinsic anisotropy of the pulsar wind or assume that this emission comes from a relic PWN swept by the asymmetrical reverse SNR shock. The pulsar and its PWN are located within the extent of the unidentified TeV source HESS J1809-193 whose brightest part is offset by ~8' to the south of the pulsar, i.e. in the same direction as the large-scale X-ray emission. Although the association between J1809-1917 and HESS J1809-193 is plausible, an alternative source of relativistic electrons powering HESS J1809-193 might be the serendipitously discovered X-ray source CXOU J180940.7-192544.

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