论文标题
从随机重力波背景搜索中限制紧凑型二进制对象的延迟时间分布
Constraining the delay time distribution of compact binary objects from the stochastic gravitational wave background searches
论文作者
论文摘要
巨大恒星二进制的初始分离设定了时间尺度，其紧凑的残留物通过引力波的发射融合。我们表明，可以从随机重力波背景（SGWB）推断出二进制中子星或黑洞的延迟时间分布（DTD）。如果人口的DTD很长，则大多数合并发生在低红移时，与DTD短路相比，背景会很安静，因为DTD短，导致低红移的单独检测很少，但背景很大。我们表明，不同的DTD预测重力波背景能量密度的大小差异为5倍（$ω_ {\ rm gw} $），并且对$ω_ {\ rm gw} $具有显着效应，而不是其他因素，例如主要BH质量，$ p（m_1）$的质量，$ p（m_1）$（$ p（m_1）$），$ mm _ mm（mm mm imm），mm rm nmm（mm mm immm imm immm rmm），黑洞的旋转（$χ_ {\ rm eff} $）。这种背景的非检测可以排除简短的DTD方案。我们表明，SGWB搜索可以在高级LIGO设计敏感的时间内观察时间的大约四年内排除BBHS的简短DTD场景，其本地合并率为30 $ \ rm GPC^{ - 3} yr^{ - 1} $ p（M_1）\ PROPTO $ p（M_1）\ PROPTO $ PROPTO M_1^$ __ max} = 50 m _ {\ odot} $。
The initial separation of massive star binaries sets the timescale over which their compact remnants merge through the emission of gravitational waves. We show that the delay time distribution (DTD) of binary neutron stars or black holes can be inferred from the stochastic gravitational wave background (SGWB). If the DTD of a population is long, most of the mergers take place at low redshifts and the background would be rather quiet compared to a scenario in which the DTD is short leading to few individual detections at low redshift but a rather loud background. We show that different DTDs predict a factor of 5 difference in the magnitude of the gravitational wave background energy density ($Ω_{\rm GW}$) and have the dominant effect on $Ω_{\rm GW}$ over other factors such as the mass function of the primary BH mass, $p(m_1)$, the maximum considered BH mass ($M_{\rm max}$), and the effective spin of the black hole ($χ_{\rm eff}$). A non-detection of such a background can rule out the short DTD scenario. We show that SGWB searches can rule out the short DTD scenario for the BBHs within about four years of observing time at advanced LIGO design sensitivty for a local merger rate of 30 $\rm Gpc^{-3} yr^{-1}$ assuming $p(m_1)\propto m_1^{-1}$, and $M_{\rm max}=50 M_{\odot}$.
