Influence of conservative corrections on parameter estimation for extreme-mass-ratio inspirals

Journal Article · Wed Apr 15 00:00:00 EDT 2009 · Physical Review. D, Particles Fields

DOI:https://doi.org/10.1103/PHYSREVD.79.084021· OSTI ID:21308316

Huerta, E A; Gair, Jonathan R ^[1]

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1. Institute of Astronomy, Madingley Road, CB3 0HA Cambridge (United Kingdom)

We present an improved numerical kludge waveform model for circular, equatorial extreme-mass-ratio inspirals (EMRIs). The model is based on true Kerr geodesics, augmented by radiative self-force corrections derived from perturbative calculations, and in this paper for the first time we include conservative self-force corrections that we derive by comparison to post-Newtonian results. We present results of a Monte Carlo simulation of parameter estimation errors computed using the Fisher matrix and also assess the theoretical errors that would arise from omitting the conservative correction terms we include here. We present results for three different types of system, namely, the inspirals of black holes, neutron stars, or white dwarfs into a supermassive black hole (SMBH). The analysis shows that for a typical source (a 10M{sub {center_dot}} compact object captured by a 10{sup 6}M{sub {center_dot}} SMBH at a signal to noise ratio of 30) we expect to determine the two masses to within a fractional error of {approx}10{sup -4}, measure the spin parameter q to {approx}10{sup -4.5}, and determine the location of the source on the sky and the spin orientation to within 10{sup -3} steradians. We show that, for this kludge model, omitting the conservative corrections leads to a small error over much of the parameter space, i.e., the ratio R of the theoretical model error to the Fisher matrix error is R<1 for all ten parameters in the model. For the few systems with larger errors typically R<3 and hence the conservative corrections can be marginally ignored. In addition, we use our model and first-order self-force results for Schwarzschild black holes to estimate the error that arises from omitting the second-order radiative piece of the self-force. This indicates that it may not be necessary to go beyond first order to recover accurate parameter estimates.

• OSTI ID: 21308316
• Journal Information: Physical Review. D, Particles Fields, Vol. 79, Issue 8; Other Information: DOI: 10.1103/PhysRevD.79.084021; (c) 2009 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA); ISSN 0556-2821
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
BLACK HOLES
COMPARATIVE EVALUATIONS
COMPUTERIZED SIMULATION
CORRECTIONS
GEODESICS
MASS
MONTE CARLO METHOD
NEUTRON STARS
SCHWARZSCHILD METRIC
SIGNAL-TO-NOISE RATIO
SPACE
SPIN
SPIN ORIENTATION
WAVE FORMS
WHITE DWARF STARS