960 research outputs found
LISA observations of supermassive black holes: parameter estimation using full post-Newtonian inspiral waveforms
We study parameter estimation of supermassive black hole binary systems in
the final stage of inspiral using the full post-Newtonian gravitational
waveforms. We restrict our analysis to systems in circular orbit with
negligible spins, in the mass range 10^8\Ms-10^5\Ms, and compare the results
with those arising from the commonly used restricted post-Newtonian
approximation. The conclusions of this work are particularly important with
regard to the astrophysical reach of future LISA measurements. Our analysis
clearly shows that modeling the inspiral with the full post-Newtonian waveform,
not only extends the reach to higher mass systems, but also improves in general
the parameter estimation. In particular, there are remarkable improvements in
angular resolution and distance measurement for systems with a total mass
higher than 5\times10^6\Ms, as well as a large improvement in the mass
determination.Comment: Final version. Accepted for publication in Phys. Rev.
Higher harmonics increase LISA's mass reach for supermassive black holes
Current expectations on the signal to noise ratios and masses of supermassive
black holes which the Laser Interferometer Space Antenna (LISA) can observe are
based on using in matched filtering only the dominant harmonic of the inspiral
waveform at twice the orbital frequency. Other harmonics will affect the
signal-to-noise ratio of systems currently believed to be observable by LISA.
More significantly, inclusion of other harmonics in our matched filters would
mean that more massive systems that were previously thought to be {\it not}
visible in LISA should be detectable with reasonable SNRs. Our estimates show
that we should be able to significantly increase the mass reach of LISA and
observe the more commonly occurring supermassive black holes of masses More specifically, with the inclusion of all known harmonics LISA
will be able to observe even supermassive black hole coalescences with total
mass (and mass-ratio 0.1) for a low frequency
cut-off of with an SNR up to
at a distance of 3 Gpc. This is important from the astrophysical
viewpoint since observational evidence for the existence of black holes in this
mass range is quite strong and binaries containing such supermassive black
holes will be inaccessible to LISA if one uses as detection templates only the
dominant harmonic.Comment: minor corrections mad
Higher-order spin effects in the amplitude and phase of gravitational waveforms emitted by inspiraling compact binaries: Ready-to-use gravitational waveforms
We provide ready-to-use time-domain gravitational waveforms for spinning
compact binaries with precession effects through 1.5PN order in amplitude and
compute their mode decomposition using spin-weighted -2 spherical harmonics. In
the presence of precession, the gravitational-wave modes (l,m) contain
harmonics originating from combinations of the orbital frequency and precession
frequencies. We find that the gravitational radiation from binary systems with
large mass asymmetry and large inclination angle can be distributed among
several modes. For example, during the last stages of inspiral, for some
maximally spinning configurations, the amplitude of the (2,0) and (2,1) modes
can be comparable to the amplitude of the (2,2) mode. If the mass ratio is not
too extreme, the l=3 and l=4 modes are generally one or two orders of magnitude
smaller than the l = 2 modes. Restricting ourselves to spinning, non-precessing
compact binaries, we apply the stationary-phase approximation and derive the
frequency-domain gravitational waveforms including spin-orbit and spin(1)-
spin(2) effects through 1.5PN and 2PN order respectively in amplitude, and
2.5PN order in phase. Since spin effects in the amplitude through 2PN order
affect only the first and second harmonics of the orbital phase, they do not
extend the mass reach of gravitational-wave detectors. However, they can
interfere with other harmonics and lower or raise the signal-to-noise ratio
depending on the spin orientation. These ready-to-use waveforms could be
employed in the data-analysis of the spinning, inspiraling binaries as well as
in comparison studies at the interface between analytical and numerical
relativity.Comment: 43 pages, 10 Postscript figures. submitted to Physical Review D.
Includes corrections due to errat
Using Full Information When Computing Modes of Post-Newtonian Waveforms From Inspiralling Compact Binaries in Circular Orbit
The increasing sophistication and accuracy of numerical simulations of
compact binaries (especially binary black holes) presents the opportunity to
test the regime in which post-Newtonian (PN) predictions for the emitted
gravitational waves are accurate. In order to confront numerical results with
those of post-Newtonian theory, it is convenient to compare multipolar
decompositions of the two waveforms. It is pointed out here that the individual
modes can be computed to higher post-Newtonian order by examining the radiative
multipole moments of the system, rather than by decomposing the 2.5PN
polarization waveforms. In particular, the dominant (l = 2, m = 2) mode can be
computed to 3PN order. Individual modes are computed to as high a
post-Newtonian order as possible given previous post-Newtonian results.Comment: 15 page
Parameter estimation of coalescing supermassive black hole binaries with LISA
Laser Interferometer Space Antenna (LISA) will routinely observe coalescences
of supermassive black hole (BH) binaries up to very high redshifts. LISA can
measure mass parameters of such coalescences to a relative accuracy of
, for sources at a distance of 3 Gpc. The problem of parameter
estimation of massive nonspinning binary black holes using post-Newtonian (PN)
phasing formula is studied in the context of LISA. Specifically, the
performance of the 3.5PN templates is contrasted against its 2PN counterpart
using a waveform which is averaged over the LISA pattern functions. The
improvement due to the higher order corrections to the phasing formula is
examined by calculating the errors in the estimation of mass parameters at each
order. The estimation of the mass parameters and are
significantly enhanced by using the 3.5PN waveform instead of the 2PN one. For
an equal mass binary of at a luminosity distance of 3 Gpc,
the improvement in chirp mass is and that of is .
Estimation of coalescence time worsens by 43%. The improvement is larger
for the unequal mass binary mergers. These results are compared to the ones
obtained using a non-pattern averaged waveform. The errors depend very much on
the location and orientation of the source and general conclusions cannot be
drawn without performing Monte Carlo simulations. Finally the effect of the
choice of the lower frequency cut-off for LISA on the parameter estimation is
studied.Comment: 12 pages, 5 figures (eps) significant revision, accepted for
publication in Phys. Rev. D. Matches with the published versio
Matched-filter study and energy budget suggest no detectable gravitational-wave 'extended emission' from GW170817
Van Putten & Della Valle (2018) have reported a possible detection of
gravitational-wave 'extended emission' from a neutron star remnant of GW170817.
Starting from the time-frequency evolution and total emitted energy of their
reported candidate, we show that such an emission is not compatible with the
current understanding of neutron stars. We explore the additional required
physical assumptions to make a full waveform model, for example, taking the
optimistic emission from a spining-down neutron star with fixed quadrupolar
deformation, and study whether even an ideal single-template matched-filter
analysis could detect an ideal, fully phase-coherent signal. We find that even
in the most optimistic case an increase in energy and extreme parameters would
be required for a confident detection with LIGO sensitivity as of 2018-08-17.
The argument also holds for other waveform models following a similar
time-frequency track and overall energy budget. Single-template matched
filtering on the LIGO data around GW170817, and on data with added simulated
signals, verifies the expected sensitivity scaling and the overall statistical
expectation.Comment: 9 pages, 6 figures, updated version as accepted by MNRA
Binary black hole detection rates in inspiral gravitational wave searches
The signal-to-noise ratios (SNRs) for quasi-circular binary black hole
inspirals computed from restricted post-Newtonian waveforms are compared with
those attained by more complete post-Newtonian signals, which are
superpositions of amplitude-corrected harmonics of the orbital phase. It is
shown that if one were to use the best available amplitude-corrected waveforms
for detection templates, one should expect SNRs in actual searches to be
significantly lower than those suggested by simulations based purely on
restricted waveforms.Comment: 9 pages, 1 figur
Parameter estimation of compact binaries using the inspiral and ringdown waveforms
We analyze the problem of parameter estimation for compact binary systems
that could be detected by ground-based gravitational wave detectors.
So far this problem has only been dealt with for the inspiral and the
ringdown phases separately. In this paper, we combine the information from both
signals, and we study the improvement in parameter estimation, at a fixed
signal-to-noise ratio, by including the ringdown signal without making any
assumption on the merger phase. The study is performed for both initial and
advanced LIGO and VIRGO detectors.Comment: matching cqg versio
Lie groups of conformal motions acting on null orbits
Space-times admitting a 3-dimensional Lie group of conformal motions
acting on null orbits are studied. Coordinate expressions for the metric and
the conformal Killing vectors (CKV) are provided (irrespectively of the matter
content) and then all possible perfect fluid solutions are found, although none
of these verify the weak and dominant energy conditions over the whole
space-time manifold.Comment: 5 pages, Late
Spectral Line Removal in the LIGO Data Analysis System (LDAS)
High power in narrow frequency bands, spectral lines, are a feature of an
interferometric gravitational wave detector's output. Some lines are coherent
between interferometers, in particular, the 2 km and 4 km LIGO Hanford
instruments. This is of concern to data analysis techniques, such as the
stochastic background search, that use correlations between instruments to
detect gravitational radiation. Several techniques of `line removal' have been
proposed. Where a line is attributable to a measurable environmental
disturbance, a simple linear model may be fitted to predict, and subsequently
subtract away, that line. This technique has been implemented (as the command
oelslr) in the LIGO Data Analysis System (LDAS). We demonstrate its application
to LIGO S1 data.Comment: 11 pages, 5 figures, to be published in CQG GWDAW02 proceeding
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