English
 
User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
  Distinguishing high-mass binary neutron stars from binary black holes with second- and third-generation gravitational wave observatories

Chen, A., Johnson-McDaniel, N. K., Dietrich, T., & Dudi, R. (2020). Distinguishing high-mass binary neutron stars from binary black holes with second- and third-generation gravitational wave observatories. Physical Review D, 101(10): 103008. doi:10.1103/PhysRevD.101.103008.

Item is

Basic

show hide
Item Permalink: http://hdl.handle.net/21.11116/0000-0005-C18A-5 Version Permalink: http://hdl.handle.net/21.11116/0000-0006-690A-A
Genre: Journal Article

Files

show Files
hide Files
:
2001.11470.pdf (Preprint), 960KB
Name:
2001.11470.pdf
Description:
File downloaded from arXiv at 2020-03-03 08:52
Visibility:
Public
MIME-Type / Checksum:
application/pdf / [MD5]
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
:
PhysRevD.101.103008.pdf (Publisher version), 2MB
 
File Permalink:
-
Name:
PhysRevD.101.103008.pdf
Description:
-
Visibility:
Restricted (Max Planck Institute for Gravitational Physics (Albert Einstein Institute), MPGR; )
MIME-Type / Checksum:
application/pdf
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
License:
-

Locators

show

Creators

show
hide
 Creators:
Chen, An, Author
Johnson-McDaniel, Nathan K., Author
Dietrich , Tim, Author
Dudi, Reetika1, Author              
Affiliations:
1Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_2541714              

Content

show
hide
Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE, Astrophysics, Solar and Stellar Astrophysics, astro-ph.SR,General Relativity and Quantum Cosmology, gr-qc
 Abstract: (Abridged) While the gravitational-wave (GW) signal GW170817 was accompanied by a variety of electromagnetic (EM) counterparts, sufficiently high-mass binary neutron star (BNS) mergers are expected to be unable to power bright EM counterparts. The putative high-mass binary BNS merger GW190425, for which no confirmed EM counterpart has been identified, may be an example of such a system. It is thus important to understand how well we will be able to distinguish high-mass BNSs and low-mass binary black holes (BBHs) solely from their GW signals. To do this, we consider the imprint of the tidal deformability of the neutron stars on the GW signal for systems undergoing prompt black hole formation after merger. We model the BNS signals using hybrid numerical relativity -- tidal effective-one-body waveforms. Specifically, we consider a set of five nonspinning equal-mass BNS signals with masses of 2.7, 3.0, 3.2 Msun and with three different equations of state, as well as the analogous BBH signals. We perform parameter estimation on these signals in three networks: Advanced LIGO-Advanced Virgo and Advanced LIGO-Advanced Virgo-KAGRA with sensitivities similar to O3 and O4, respectively, and a 3G network of two Cosmic Explorers (CEs) and one Einstein Telescope, with a CE sensitivity similar to Stage 2. Our analysis suggests that we cannot distinguish the signals from high-mass BNSs and BBHs at a 90% credible level with the O3-like network even at 40 Mpc. However, we can distinguish all but the most compact BNSs that we consider in our study from BBHs at 40 Mpc at a >= 95% credible level using the O4-like network, and can even distinguish them at a > 99.2% (>= 97%) credible level at 369 (835) Mpc using the 3G network. Additionally, we present a simple method to compute the leading effect of the Earth's rotation on the response of a gravitational wave detector in the frequency domain.

Details

show
hide
Language(s):
 Dates: 2020-01-302020
 Publication Status: Published in print
 Pages: 18 pages, 10 figures
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 2001.11470
URI: http://arxiv.org/abs/2001.11470
DOI: 10.1103/PhysRevD.101.103008
 Degree: -

Event

show

Legal Case

show

Project information

show

Source 1

show
hide
Title: Physical Review D
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: -
Pages: - Volume / Issue: 101 (10) Sequence Number: 103008 Start / End Page: - Identifier: -