A Future Percent-level Measurement of the Hubble Expansion at Redshift 0.8 with Advanced LIGO
A Future Percent-level Measurement of the Hubble Expansion at Redshift 0.8 with Advanced LIGO
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DOI：
10.3847/2041-8213/ab4284
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发表时间：
2019-08
期刊：
影响因子：
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通讯作者：
W. Farr;M. Fishbach;Jiani Ye;D. Holz
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文献类型：
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作者：
W. Farr;M. Fishbach;Jiani Ye;D. Holz
同时测量距离和红移可以用来限制宇宙的膨胀历史和相关的宇宙学参数。合并的双黑洞（BBH）系统是标准的警报器-它们的引力波形提供了关于到源的光度距离的直接信息。然而，在源质量和红移之间存在着一个完美的简并;一些非引力信息是打破简并确定源红移所必需的。在这里，我们建议，对不稳定性超新星（PISN）的过程，被认为是所观察到的上限的黑洞质量在合并BBH系统的来源，在人口中的BBH合并的质量尺度，并允许测量的红移，光度，距离与这些来源的关系。我们模拟了五年的BBH探测在先进的LIGO和处女座探测器与现实的BBH合并率，质量分布与平滑PISN截止，和测量不确定性。我们表明，经过一年的操作在设计灵敏度的BBH人口可以限制H（z）在枢轴红移。五年后，约束改善为。如果PISN截止是尖锐的，则不确定性小约两倍。这种测量只依赖于广义相对论和存在一个在宇宙时间内近似固定或校准的质量尺度;它独立于任何距离阶梯。未来的“第三代”引力波探测器可以观测到整个宇宙中的BBH合并，这将允许在一个月的观测时间内对z ≥ 4进行宇宙学测量。
Simultaneous measurements of distance and redshift can be used to constrain the expansion history of the universe and associated cosmological parameters. Merging binary black hole (BBH) systems are standard sirens—their gravitational waveform provides direct information about the luminosity distance to the source. There is, however, a perfect degeneracy between the source masses and redshift; some nongravitational information is necessary to break the degeneracy and determine the redshift of the source. Here we suggest that the pair instability supernova (PISN) process, thought to be the source of the observed upper limit on the black hole mass in merging BBH systems at , imprints a mass scale in the population of BBH mergers and permits a measurement of the redshift–luminosity–distance relation with these sources. We simulate five years of BBH detections in the Advanced LIGO and Virgo detectors with a realistic BBH merger rate, mass distribution with smooth PISN cutoff, and measurement uncertainty. We show that after one year of operation at design sensitivity the BBH population can constrain H(z) to at a pivot redshift . After five years the constraint improves to . If the PISN cutoff is sharp, the uncertainty is smaller by about a factor of two. This measurement relies only on general relativity and the presence of a mass scale that is approximately fixed or calibrated across cosmic time; it is independent of any distance ladder. Observations by future “third-generation” gravitational wave detectors, which can see BBH mergers throughout the universe, would permit subpercent cosmographical measurements to z ≳ 4 within one month of observation.