Journal
PHYSICAL REVIEW D
Volume 101, Issue 10, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.101.103036
Keywords
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Funding
- NSF [PHY-1836779, AST-1716394, AST-1708146, PHY-1841464, AST-1841358, NSF PHY-1748958]
- Leverhulme Trust [RPG-2019-350]
- Swarnajayanti Fellowship [DST/SJF/PSA01/2017-18]
- Infosys Foundation
- NSF-XSEDE Grant [PHY-090003]
- NASA ATP Grant [17-ATP17-0225, 19-ATP19-0051]
- Amaldi Research Center - MIUR program Dipartimento di Eccellenza [CUP: B81I18001170001]
- EU H2020 research and innovation programme under the Marie Sklodowska-Curie Grant [690904]
- COST Action [CA16104]
- EPSRC [EP/P020232/1]
- Maryland Advanced Research Computing Center
- IUCAA LDG cluster Sarathi
- EPSRC [EP/P020232/1] Funding Source: UKRI
Ask authors/readers for more resources
Binary neutron-star mergers will predominantly produce black-hole remnants of mass similar to 3-4 M-circle dot, thus populating the putative low-mass gap between neutron stars and stellar-mass black holes. If these low-mass black holes are in dense astrophysical environments, mass segregation could lead to second-generation compact binaries merging within a Hubble time. In this paper, we investigate possible signatures of such low-mass compact binary mergers in gravitational-wave observations. We show that this unique population of objects, if present, will be uncovered by the third-generation gravitational-wave detectors, such as Cosmic Explorer and Einstein Telescope. Future joint measurements of chirp mass M and effective spin chi(eff) could clarify the formation scenario of compact objects in the low-mass gap. As a case study, we show that the recent detection of GW190425 (along with GW170817) favors a double Gaussian mass model for neutron stars, under the assumption that the primary in GW190425 is a black hole formed from a previous binary neutron-star merger.
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