REVIEW 2 cited by
Footprints of population III stars in the gravitational-wave background
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Signed reviews
read the original abstract
We investigate detection prospects of the gravitational-wave background (GWB) that originates from the merging of compact objects formed by the collapse of population III stars. Younger population I/II stars lead to a GWB in the LIGO/Virgo frequency band at the inspiral phase, while population III stars would likely show up at the later merger and ringdown phases. We show that, using a network of third-generation detectors, we may be able to separate a population I/II signal from a population III one, provided we can subtract individual coalescence events. A detection of a population III GWB could reveal important information, such as the average redshifted total mass.
Forward citations
Cited by 2 Pith papers
-
Constraining Population III stellar demographics with next-generation gravitational-wave observatories
A simulation study shows that one year of Cosmic Explorer and Einstein Telescope data could separate Population III black-hole mergers from ordinary ones and constrain the Population III initial mass function slope an...
-
Upper Limits on the Isotropic Gravitational-Wave Background from the first part of LIGO, Virgo, and KAGRA's fourth Observing Run
No gravitational-wave background is detected in O1-O4a data; the new CBC-spectrum limit Ω_GW(25 Hz) = 2.0×10^-9 (95%) is 1.7x tighter and remains roughly 2-3x above the GWTC-4-predicted astrophysical background of 0.9×10^-9.
Discussion (0). Continue with ORCID to comment.