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首页> 外文期刊>The Astrophysical journal >THE GAMMA-RAY PULSAR POPULATION
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THE GAMMA-RAY PULSAR POPULATION

机译：伽马射线脉冲群

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We apply a likelihood analysis to pulsar detections, pulsar upper limits, and diffuse background measurements from the OSSE and EGRET instruments on the Compton Gamma Ray Observatory to constrain the luminosity law for gamma-ray pulsars and some properties of the gamma-ray pulsar population. We find that the dependence of luminosity on spin period and dipole magnetic field is much steeper at OSSE than at EGRET energies (50-200 keV and > 100 MeV, respectively), suggesting that different emission mechanisms are responsible for low- and high-energy gamma-ray emission. Incorporating a spin-down model and assuming a pulsar spatial distribution, we estimate the fraction of the Galactic gamma-ray background due to unidentified pulsars and find that pulsars may be an important component of the OSSE diffuse flux but are most likely not important at EGRET energies. Using measurements of the diffuse background flux from these instruments, we are able to place constraints on the braking index, initial spin period, and magnetic field of the Galactic pulsar population and are also able to constrain the pulsar birthrate to be between 1/25 yr~(-1) and 1/500 yr~(-1). Our results are based on a large gamma-ray beam, but they do not scale in a simple way with beam size. We estimate that about 20 of the 169 unidentified EGRET sources are probably gamma-ray pulsars. We use our model to predict the pulsar population that will be seen by future gamma-ray instruments and estimate that Gamma Ray Large Area Space Telescope will detect roughly 750 gamma-ray pulsars as steady sources, only 120 of which are currently known radio pulsars.
机译：我们对康普顿伽玛射线天文台的OSSE和EGRET仪器的脉冲星探测，脉冲星上限和散射本底测量应用似然分析，以约束伽玛射线脉冲星的光度定律和伽玛射线脉冲星总体的某些属性。我们发现，OSSE的光度对自旋周期和偶极磁场的依赖性比EGRET的能量（分别为50-200 keV和> 100 MeV）要陡得多，这表明低和高能量负责的发射机理不同伽马射线发射。结合自旋降落模型并假设脉冲星空间分布，我们估计由于未识别的脉冲星而导致的银河伽马射线背景的比例，并发现脉冲星可能是OSSE扩散通量的重要组成部分，但在EGRET上最不重要能量。使用这些仪器对散射本底通量的测量，我们可以对银河脉冲星种群的制动指数，初始自旋周期和磁场施加约束，并且还可以将脉冲星的出生率限制在1/25年〜（-1）和1/500 yr〜（-1）。我们的结果基于大的伽马射线束，但是它们无法以简单的方式随光束大小缩放。我们估计169个未识别的EGRET源中约有20个可能是伽马射线脉冲星。我们使用我们的模型预测未来的伽马射线仪器将看到的脉冲星数量，并估计伽马射线大面积空间望远镜将探测到大约750个伽马射线脉冲星作为稳定源，其中只有120个是当前已知的无线电脉冲星。

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