Detecting black-hole binary clustering via the second-generation gravitational-wave detectors

被引：24

作者：

Namikawa, Toshiya ^{[1
,2
]}

Nishizawa, Atsushi ^{[3
,4
]}

Taruya, Atsushi ^{[5
,6
]}

机构：

[1] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

[2] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA

[3] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA

[4] CALTECH, Theoret Astrophys 350 17, Pasadena, CA 91125 USA

[5] Kyoto Univ, Yukawa Inst Theoret Phys, Ctr Gravitat Phys, Kyoto 6068502, Japan

[6] Univ Tokyo, Kavli Inst Phys & Math Universe, Todai Inst Adv Study, Kashiwa, Chiba 2778583, Japan

来源：

PHYSICAL REVIEW D | 2016年 / 94卷 / 02期

基金：

美国国家科学基金会;

关键词：

PHYSICS; COSMOLOGY; MODEL;

D O I：

10.1103/PhysRevD.94.024013

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The first discovery of the gravitational-wave (GW) event, GW150914, suggests a higher merger rate of black-hole (BH) binaries. If this is true, a number of BH binaries will be observed via the second-generation GW detectors, and the statistical properties of the observed BH binaries can be scrutinized. A naive but important question to ask is whether the spatial distribution of BH binaries faithfully traces the matter inhomogeneities in the Universe or not. Although the BH binaries are thought to be formed inside the galaxies in most of the scenarios, there is no observational evidence to confirm such a hypothesis. Here, we estimate how well the second-generation GW detectors can statistically confirm the BH binaries to be a tracer of the large-scale structure by looking at the auto-and cross-correlation of BH binaries with photometric galaxies and weak-lensing measurements, finding that, with a 3 year observation, the >3 sigma detection of a nonzero signal is possible if the BH merger rate today is n(0) greater than or similar to 100 Gpc(-3) yr(-1) and the clustering bias of BH binaries is b(BH,0) greater than or similar to 1.5.

引用

页数：8

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