Speaker
Description
Star-formation rate (SFR) is currently measured with electromagnetic probes. However, these probes often track luminosity which is then converted to SFR depending on various factors such as initial mass function, dust extinction, etc. Moreover, data points about redshift of $z=4$ are difficult to obtain through electromagnetic probes. Gravitational Waves (GWs) provide an independent probe to constrain star-formation rate at high redshift. In our study, we explore three population models for star-formation and demonstrate that we do not need to wait for the next-generation (XG) detectors such as Cosmic Explorer and Einstein Telescope to obtain bounds on the peak of redshift distribution. This is achievable with upgraded LIGO detectors such as LIGO-A#. Further, we compare the results with XG network and demonstrate how the SFR curve will be extremely well measured with future detectors, and compare this across various mass bins for binary black hole sources.