Kavli Affiliate: Qingjuan Yu
| First 5 Authors: , , , ,
| Summary:
Pulsar timing arrays (PTAs) are anticipated to detect the stochastic
gravitational wave background (GWB) from supermassive binary black holes (BBHs)
as well as the gravitational waves from individual BBHs. Recently, a common
process signal was reported by several PTAs. In this paper, we investigate the
constraints on the BBH population model(s) by current PTA observations and
further study the detections of both the GWB and individual BBHs by
current/future PTAs. We find that the MBH–host galaxy scaling relation, an
important ingredient of the BBH population model, is required to either evolve
significantly with redshift or have a normalization $sim0.86-1.1$ dex higher
than the empirical ones, if the GWB is the same as the common process signal.
For both cases, the estimated detection probability for individual BBHs is too
small for a positive detection by current PTAs. By involving either the
constrained scaling relations or those empirical ones into the BBH population
models, we estimate that the GWB may be detected with a signal-to-noise ratio
$gtrsim3$ by the PTAs based on the Five hundred meter Aperture Spherical radio
Telescope (CPTA) and the Square Kilometer Array (SKAPTA) after $sim2-3$ (or
$sim6-11$) years’ observation, if it is the same as (or an order of magnitude
lower than) the common process signal. The detection time of individual BBHs by
CPTA and SKAPTA is close to that of the GWB detection. We show that the BBH
population model can be strongly constrained by the number and property
distributions of BBHs to be detected by future PTAs.
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