在未编目的年轻银河系超新星遗迹G310中发现与IGR J14003-6326有关的高能脉冲星
Discovery of a highly energetic pulsar associated with IGR J14003-6326 in a young uncataloged Galactic supernova remnant G310.6-1.6
摘要：
我们报告发现31.18毫秒脉动的积分源IGR J14003-6326使用罗西X射线定时探测器（RXTE）。这颗脉冲星很可能与位于G310.6-1.6中心的明亮钱德拉X射线点源有关，G310.6-1.6是一个以前未被识别的银河系复合超新星遗迹，具有明亮的中央非热射电和X射线星云，被认为是脉冲星风星云（PWN）。PSR J1400-6325是银河系中最具能量的旋转动力恒星之一，其下旋光度为Edot = 5.1E+37 erg.s-1。在旋转偶极模型中，地表偶极磁场强度为Bs = 1.1E+12 G，特征年龄τ c = P/2 Pdot = 12.7kyr。脉冲星和星云的硬光谱指数分别为1.22 +/- 0.15和1.83 +/- 0.08，以及2-10 keV的通量比F_PWN/F_PSR ~ 8。后续的Parkes观测发现PSR J1400-6325在10和20厘米处的射电辐射，色散测量值约为560 cm-3 pc，这意味着相对较大的距离为10 +/- 3 kpc。然而，离银道面约280 pc的位置将比分子盘的典型厚度大得多，我们认为G310.6-1.6位于约7 kpc的距离。在迄今为止公布的费米数据中，还没有与星云或脉冲星对应的伽马射线。对这一新的复合超新星遗迹的多波长研究（从射电到甚高能γ射线）表明，这是一个年轻（< 1000年）的超新星遗迹，是由一次低密度（n 0 ~ 0.01 cm-3）环境中的次高能（~ 1 E +50尔格）、低喷出物质量（M_ej ~ 3 Msun）超新星爆发形成的。
英文摘要：
We report the discovery of 31.18 ms pulsations from the INTEGRAL source IGR J14003-6326 using the Rossi X-ray Timing Explorer (RXTE). This pulsar is most likely associated with the bright Chandra X-ray point source lying at the center of G310.6-1.6, a previously unrecognised Galactic composite supernova remnant with a bright central non-thermal radio and X-ray nebula, taken to be the pulsar wind nebula (PWN). PSR J1400-6325 is amongst the most energetic rotation-powered pulsars in the Galaxy, with a spin-down luminosity of Edot = 5.1E+37 erg.s-1. In the rotating dipole model, the surface dipole magnetic field strength is B_s = 1.1E+12 G and the characteristic age tau_c = P/2Pdot = 12.7 kyr. The high spin-down power is consistent with the hard spectral indices of the pulsar and the nebula of 1.22 +/- 0.15 and 1.83 +/- 0.08, respectively, and a 2-10 keV flux ratio F_PWN/F_PSR ~ 8. Follow-up Parkes observations resulted in the detection of radio emission at 10 and 20 cm from PSR J1400-6325 at a dispersion measure of ~ 560 cm-3 pc, which implies a relatively large distance of 10 +/- 3 kpc. However, the resulting location off the Galactic Plane of ~ 280 pc would be much larger than the typical thickness of the molecular disk, and we argue that G310.6-1.6 lies at a distance of ~ 7 kpc. There is no gamma-ray counterpart to the nebula or pulsar in the Fermi data published so far. A multi-wavelength study of this new composite supernova remnant, from radio to very-high energy gamma-rays, suggests a young (< 1000 yr) system, formed by a sub-energetic (~ 1E+50 ergs), low ejecta mass (M_ej ~ 3 Msun) SN explosion that occurred in a low-density environment (n_0 ~ 0.01 cm-3).
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