de.mpg.escidoc.pubman.appbase.FacesBean
English
 
Help Guide Disclaimer Contact us Login
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
  Estimating the parameters of non-spinning binary black holes using ground-based gravitational-wave detectors: Statistical errors

Ajith, P., & Bose, S. (2009). Estimating the parameters of non-spinning binary black holes using ground-based gravitational-wave detectors: Statistical errors. Physical Review D., 79: 084032. doi:10.1103/PhysRevD.79.084032.

Item is

Basic

show hide
Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0012-9C8D-5 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0012-9C8E-3
Genre: Journal Article

Files

show Files
hide Files
:
0901.4936 (Preprint), 3MB
Description:
File downloaded from arXiv at 2010-04-21 12:59
Visibility:
Public
MIME-Type / Checksum:
application/pdf / [MD5]
Technical Metadata:
Copyright Date:
-
Copyright Info:
-

Locators

show

Creators

show
hide
 Creators:
Ajith, P., Author
Bose, Sukanta1, Author              
Affiliations:
1Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, escidoc:24011              

Content

show
hide
Free keywords: General Relativity and Quantum Cosmology, gr-qc,Astrophysics, Cosmology and Extragalactic Astrophysics, astro-ph.CO
 Abstract: (Abridged): We assess the statistical errors in estimating the parameters of non-spinning black-hole binaries using ground-based gravitational-wave detectors. While past assessments were based on only the inspiral/ring-down pieces of the coalescence signal, the recent progress in analytical and numerical relativity enables us to make more accurate projections using "complete" inspiral-merger-ringdown waveforms. We employ the Fisher matrix formalism to estimate how accurately the source parameters will be measurable using a single interferometer as well as a network of interferometers. Those estimates are further vetted by Monte-Carlo simulations. We find that the parameter accuracies of the complete waveform are, in general, significantly better than those of just the inspiral waveform in the case of binaries with total mass M > 20 M_sun. For the case of the Advanced LIGO detector, parameter estimation is the most accurate in the M=100-200 M_sun range. For an M=100M_sun system, the errors in measuring the total mass and the symmetric mass-ratio are reduced by an order of magnitude or more compared to inspiral waveforms. For binaries located at a luminosity distance d_L and observed with the Advanced LIGO--Advanced Virgo network, the sky-position error varies widely across the sky: For M=100M_sun systems at d_L=1Gpc, this variation ranges from ~0.01 square-degrees to one square-degree, with an average value of ~0.1 square-degrees. This is more than forty times better than the average sky-position accuracy of inspiral waveforms at this mass-range. The error in estimating d_L is dominated by the error in measuring the wave's polarization and is ~43% for low-mass binaries and ~23% for high-mass binaries located at d_L=1Gpc.

Details

show
hide
Language(s):
 Dates: 2009-01-302009-04-212009
 Publication Status: Published in print
 Pages: 20 pages, 19 figures, Version published in Phys. Rev. D
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 0901.4936
DOI: 10.1103/PhysRevD.79.084032
URI: http://arxiv.org/abs/0901.4936
 Degree: -

Event

show

Legal Case

show

Project information

show

Source 1

show
hide
Title: Physical Review D.
  Alternative Title : Phys. Rev. D.
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: Lancaster, Pa. : Published for the American Physical Society by the American Institute of Physics
Pages: - Volume / Issue: 79 Sequence Number: 084032 Start / End Page: - Identifier: Other: 111088197762258
Other: 0556-2821