论文标题
Gaia Pulsars和在哪里可以找到它们
Gaia pulsars and where to find them
论文作者
论文摘要
虽然大多数大型恒星都有出色的伴侣，但大多数脉冲星似乎是孤立的。从表面上看，这表明，由于超新星爆炸中获得的强烈出生踢，大多数巨大的二进制室破裂。但是，观察到的二进制部分仍然可以受到强烈的选择效果的影响，因为对新发现的脉冲星的监测很少足够长，可以最终排除多样性。在这里，我们使用第二个Gaia数据发布（DR2）来寻找1534个旋转驱动的脉冲星的伴侣，其位置已知比0.5弧秒更好。我们发现了22种与已知脉冲星的比赛，其中包括其他地方没有报道的一场比赛，以及与年轻脉冲星的8个新的可能同伴。我们检查了这些系统的光度和运动学特性，并提供了用潜在的脉冲星伴侣识别GAIA来源的经验关系。我们的结果证实了观察到的多重性分数很小。但是，我们表明，我们样本中Gaia和无线电时间敏感性低于Gaia和无线电时间的二进制数量仍然可能更高。我们将年轻脉冲星的二元分数限制为$ f _ {\ rm Young}^{\ rm true} \ leq 5.3（8.3）\％$在现实（保守的）假设的二进制属性和当前敏感性阈值下。特别是对于庞大的星星（$ \ geq 10 $ m $ _ {\ odot} $），我们发现$ f _ {\ rm ob}^{\ rm true} \ leq 3.7 \％$，该\％$ $ $ $ $ $ $ $ \ leq $ \ leq 7.2 \ yr $ $} $^yr $^$}正在进行的和未来的项目，例如Chime/Pulsar计划，Meertime，Hirax以及最终的SKA，将来将显着改善这些限制。
While the majority of massive stars have a stellar companion, most pulsars appear to be isolated. Taken at face value, this suggests that most massive binaries break apart due to strong natal kicks received in supernova explosions. However, the observed binary fraction can still be subject to strong selection effects, as monitoring of newly discovered pulsars is rarely carried out for long enough to conclusively rule out multiplicity. Here, we use the second Gaia Data Release (DR2) to search for companions to 1534 rotation-powered pulsars with positions known to better than 0.5 arcseconds. We find 22 matches to known pulsars, including one not reported elsewhere, and 8 new possible companions to young pulsars. We examine the photometric and kinematic properties of these systems and provide empirical relations for identifying Gaia sources with potential millisecond pulsar companions. Our results confirm that the observed multiplicity fraction is small. However, we show that the number of binaries below the sensitivity of Gaia and radio timing in our sample could still be significantly higher. We constrain the binary fraction of young pulsars to be $f_{\rm young}^{\rm true}\leq 5.3(8.3)\%$ under realistic(conservative) assumptions for the binary properties and current sensitivity thresholds. For massive stars ($\geq 10$ M$_{\odot}$) in particular, we find $f_{\rm OB}^{\rm true}\leq 3.7\%$ which sets a firm independent upper limit on the galactic neutron-star merger rate, $\leq 7.2\times 10^{-4}$ yr$^{-1}$. Ongoing and future projects such as the CHIME/pulsar program, MeerTime, HIRAX and ultimately the SKA, will significantly improve these constraints in the future.
