根据10年费米大面积望远镜gamma-ray源目录对太阳系附近反星部分的限制
Constraints on the antistar fraction in the Solar system neighborhood from the 10-years Fermi Large Area Telescope gamma-ray source catalog
摘要：
人们通常认为我们的宇宙是没有反物质物体和领域的。这种确定性最近受到AMS-02可能探测到反氦核的挑战。如果观测结果得到证实，附近反星的存在将成为解释反核起源的合理假设。在本文中，我们使用10年的费米大面积望远镜（LAT）的伽马射线源目录设置限制的反恒星围绕太阳的丰度。我们确定在目录中的14个antistar候选人不与任何对象属于已建立的伽马射线源类，并与重子-反重子湮灭兼容的频谱。我们使用它们与反星的LAT敏感性的估计，以设置上限的本地反星分数$f_{\bar{\ast}}$相对于正常的恒星。我们提供参数限制作为最近的反星质量，速度和周围物质密度的函数。我们还采用了一种新的Monte~Carlo方法来设定一些关于反星人口的假设的限制。对于人口的属性相当于那些集中在银河系盘的常规恒星，我们得到$f_{\bar{\ast}} < 2.5 \times 10^{-6}$在95\%的置信水平，这是20倍以上的限制比以前可用的。对于分布在银河晕中的原始反星种群，我们得到了新的局部上限，它随反星质量$M$的变化而减小，从95%置信水平的$f_{\bar{\ast}} < 0.2$（$M = 1 \; M_\odot$）减小到95%置信水平的$f_{\bar{\ast}} < 1.6 \times 10^{-4}$（$M = 10 \; M_\odot$）.通过结合这些限制与现有的麦哲伦云中较轻的物体的微透镜约束，我们推断，一个原始的人口晕反星必须有一个密度低于$\mathcal{O}(10^{-5}\;\text{pc}^{-3})$到$\mathcal{O}(10^{-2}\;\text{pc}^{-3})$取决于他们的质量。我们的极限可以约束宇宙射线中反核的起源和传播模型。
英文摘要：
It is generally taken for granted that our Universe is free of antimatter objects and domains. This certitude has recently been challenged by the possible detection of anti-helium nuclei by AMS-02. Should the observation be confirmed, the existence of nearby antistars would make a plausible hypothesis to explain the origin of the antinuclei. In this paper we use the 10-years Fermi Large Area Telescope (LAT) gamma-ray source catalog to set constraints on the abundance of antistars around the Sun. We identify in the catalog 14 antistar candidates not associated with any objects belonging to established gamma-ray source classes and with a spectrum compatible with baryon-antibaryon annihilation. We use them along with an estimate of the LAT sensitivity to antistars to set upper limits on the local antistar fraction $f_{\bar{\ast}}$ with respect to normal stars. We provide parametric limits as a function of the closest antistar mass, velocity, and surrounding matter density. We also employ a novel Monte~Carlo method to set limits for a few hypotheses about the antistar population. For a population with properties equivalent to those of regular stars concentrated in the Galactic disk we obtain $f_{\bar{\ast}} < 2.5 \times 10^{-6}$ at 95\% confidence level, which is 20 times more constraining than limits previously available. For a primordial population of antistars distributed in the Galactic halo we obtain new local upper limits which decrease as a function of antistar mass $M$ from $f_{\bar{\ast}} < 0.2$ at 95\% confidence level for $M = 1 \; M_\odot$ to $f_{\bar{\ast}} < 1.6 \times 10^{-4}$ at 95\% confidence level for $M = 10 \; M_\odot$. By combining these limits with existing microlensing constraints for lighter objects in the Magellanic clouds, we infer that a primordial population of halo antistars must have a density lower than $\mathcal{O}(10^{-5}\;\text{pc}^{-3})$ to $\mathcal{O}(10^{-2}\;\text{pc}^{-3})$ depending on their masses. Our limits can constrain models for the origin and propagation of antinuclei in cosmic rays.
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