Resolving Individual Signals in the Presence of Stochastic Background in Future Pulsar Timing Arrays

TL;DR

This paper enhances the F-statistic detection method for pulsar timing arrays by modeling unresolved gravitational waves as a stochastic background, improving the identification of individual SMBH binary signals in future PTA data.

Contribution

It introduces a new modeling approach for the F-statistic that accounts for unresolved GWs as a stochastic background, improving detection accuracy for individual signals.

Findings

Improved sky position estimation for CGWs.

Enhanced amplitude estimation when GWB dominates.

Successful application to mock datasets with mixed signals.

Abstract

Recent pulsar timing array (PTA) observations have reported evidence of a gravitational wave background (GWB). If supermassive black holes (SMBHs) are indeed the primary source of this signal, future PTA observations, such as those from the Square Kilometer Array (SKA), are expected to simultaneously capture multiple continuous gravitational waves (CGWs) emitted by bright individual SMBH binaries alongside a gravitational wave background (GWB). To address this anticipated scenario in the SKA era, we revisit the F-statistic, a detection method for single source signals in PTA datasets, and introduce a new modeling that accounts for unresolved GWs as a stochastic GWB. Here, we applied this improved F-statistic to the mock datasets that include both CGW and GWB and evaluated how accurately F-statistic can identify the parameters of CGW. As a result, we demonstrate that our approach can successfully improve the estimation of the sky position and the amplitude of CGW, particularly when the GWB is dominant over white noise. This work serves as an initial step toward developing an efficient and robust algorithm based on the F-statistic for future PTA observations.