Supermassive binary black hole evolution can be traced by a small SKA pulsar timing array

Yi Feng, Di Li, Zheng Zheng, and Chao-Wei Tsai
Phys. Rev. D 102, 023014 – Published 8 July 2020

Abstract

Supermassive black holes are commonly found in the centers of galaxies and evolve with their hosts. Supermassive binary black holes (SMBBH) are thus expected to exist in close galaxy pairs; however, none has been unequivocally detected. The square kilometer array (SKA) is a multipurpose radio telescope with a collecting area approaching 106 square meters, with great potential for detecting nanohertz gravitational waves (GWs). In this paper, we quantify the GW detectability by SKA for a realistic SMBBH population using a pulsar timing array (PTA) technique, and we quantify its impact on revealing SMBBH evolution with redshift for the first time. With only 20 pulsars, a much smaller requirement than in previous work, the SKAPTA is expected to obtain detection within about 5 years of operation and to achieve a detection rate of more than 100 SMBBHs/yr after about 10 years. Although beyond the scope of this paper, we must acknowledge that the presence of persistent red noise will reduce the number of expected detections here. It is thus imperative to understand and mitigate red noise in the PTA data. The GW signatures from a few well-known SMBBH candidates, such as OJ 287, 3C 66B, NGC 5548, and Ark 120, will be detected given the currently best-known parameters of each system. Within 30 years of operation, about 60 individual SMBBH detections with z<0.05 and more than 104 with z<1 are expected. The detection rate drops precipitately beyond z=1. The substantial number of expected detections and their discernible evolution with redshift by the SKAPTA will make SKA a significant tool for studying SMBBHs.

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  • Received 16 November 2019
  • Accepted 17 June 2020

DOI:https://doi.org/10.1103/PhysRevD.102.023014

© 2020 American Physical Society

Physics Subject Headings (PhySH)

Gravitation, Cosmology & Astrophysics

Authors & Affiliations

Yi Feng*, Di Li, Zheng Zheng, and Chao-Wei Tsai

  • CAS Key Laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China‡

  • *yifeng@nao.cas.cn
  • dili@nao.cas.cn
  • University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China.

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Vol. 102, Iss. 2 — 15 July 2020

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