2,576 research outputs found
How serious can the stealth bias be in gravitational wave parameter estimation?
The upcoming direct detection of gravitational waves will open a window to
probing the strong-field regime of general relativity (GR). As a consequence,
waveforms that include the presence of deviations from GR have been developed
(e.g. in the parametrized post-Einsteinian approach). TIGER, a data analysis
pipeline which builds Bayesian evidence to support or question the validity of
GR, has been written and tested. In particular, it was shown recently that data
from the LIGO and Virgo detectors will allow to detect deviations from GR
smaller than can be probed with Solar System tests and pulsar timing
measurements or not accessible with conventional tests of GR. However, evidence
from several detections is required before a deviation from GR can be
confidently claimed. An interesting consequence is that, should GR not be the
correct theory of gravity in its strong field regime, using standard GR
templates for the matched filter analysis of interferometer data will introduce
biases in the gravitational wave measured parameters with potentially
disastrous consequences on the astrophysical inferences, such as the
coalescence rate or the mass distribution. We consider three heuristic possible
deviations from GR and show that the biases introduced by assuming GR's
validity manifest in various ways. The mass parameters are usually the most
affected, with biases that can be as large as standard deviations for the
symmetric mass ratio, and nearly one percent for the chirp mass, which is
usually estimated with sub-percent accuracy. We conclude that statements about
the nature of the observed sources, e.g. if both objects are neutron stars,
depend critically on the explicit assumption that GR it the right theory of
gravity in the strong field regime.Comment: 10 pages, 9 figures, 5 table
Frequency-Dependent Responses in 3rd Generation Gravitational-Wave Detectors
Interferometric gravitational wave detectors are dynamic instruments.
Changing gravitational-wave strains influence the trajectories of null
geodesics and therefore modify the interferometric response. These effects will
be important when the associated frequencies are comparable to the round-trip
light travel time down the detector arms. The arms of advanced detectors
currently in operation are short enough that the strain can be approximated as
static, but planned 3 generation detectors, with arms an order of
magnitude longer, will need to account for these effects. We investigate the
impact of neglecting the frequency-dependent detector response for compact
binary coalescences and show that it can introduce large systematic biases in
localization, larger than the statistical uncertainty for 1.4-1.4
neutron star coalescences at . Analysis of
generation detectors therefore must account for these effects.Comment: 6 pages, 5 figure
Astrophysical implications of GW190412 as a remnant of a previous black-hole merger
Two of the dominant channels to produce merging stellar-mass black-hole
binaries are believed to be the isolated evolution of binary stars in the field
and dynamical formation in star clusters. The first reported black-hole binary
event from the third LIGO/Virgo observing run (GW190412) is unusual in that it
has unequal masses, nonzero effective spin, and nonzero primary spin at 90\%
confidence interval. We show that this event should be exceedingly rare in the
context of both the field and cluster formation scenarios. Interpreting
GW190412 as a remnant of a previous black-hole merger provides a promising
route to explain its features. If GW190412 indeed formed hierarchically, we
show that the region of the parameter space that is best motivated from an
astrophysical standpoint (low natal spins and light clusters) cannot
accommodate the observation. We analyze public GW190412 LIGO/Virgo data with a
Bayesian prior where the more massive black hole resulted from a previous
merger, and find that this interpretation is equally supported by the data. If
the heavier component of GW190412 is indeed a merger remnant, then its spin
magnitude is , which is higher than the value
previously reported by the LIGO/Virgo collaboration.Comment: 7 pages, 3 figures, 1 table. Published in PR
Detecting Stellar Lensing of Gravitational Waves with Ground-Based Observatories
We investigate the ability of ground based gravitational wave observatories
to detect gravitational wave lensing events caused by stellar mass lenses. We
show that LIGO and Virgo possess the sensitivities required to detect lenses
with masses as small as provided that the gravitational wave
is observed with a signal-to-noise ratio of . Third generation
observatories will allow detection of gravitational wave lenses with masses of
. Finally, we discuss the possibility of lensing by multiple
stars, as is the case if the gravitational radiation is passing through
galactic nucleus or a dense star cluster.Comment: PRD accepte
Three observational differences for binary black holes detections with second- and third-generation gravitational-wave detectors
Advanced gravitational-wave observatories, such as LIGO and Virgo, will detect hundreds of gravitational-wave signals emitted by binary black holes in the next few years. The collection of detected sources is expected to have certain properties. It is expected that a selection bias will exist toward higher-mass systems, that most events will be oriented with their angular momentum pointing to or away from Earth, and that quiet events will be much more numerous than loud events. In this paper, we show how all these assumptions are only true for existing detectors and do not have any universality. Using a network of proposed third-generation gravitational-wave detectors, we show how each of these assumptions must be revised, and we discuss several consequences on the characterization of the sources.National Science Foundation (U.S.) (Cooperative Agreement PHY-0757058
Prospects and challenges in the electromagnetic follow-up of LIGO-Virgo gravitational wave transients
The kilometer-scale ground based gravitational wave (GW) detectors, LIGO and Virgo, are being upgraded to their advanced configurations. We expect the two LIGO observatories to undertake a 3 month science run in 2015 with a limited sensitivity. Virgo should come online in 2016, and join LIGO for a 6 month science run. Through a sequence of science runs and commissioning periods, the final sensitivity should be reached by ~2019. LIGO and Virgo are expected to deliver the first direct detection of gravitational wave transients in the next few years. Most of the known sources of GWs targeted by LIGO and Virgo will likely be luminous in the electromagnetic (EM) spectrum as well. Compact binary coalescences are thought to be progenitors of short gamma-ray bursts, while long gamma-ray bursts are likely to be associated with core collapse supernova. A joint detection of gravitational and EM radiation may help confirm these associations, and expand our understanding of those astrophysical systems. Due to the transient nature, a search for the EM counterparts to GW events should be done with the shortest latency. In this paper we describe the EM follow-up program of Advanced LIGO and Virgo, from the search for GWs to the production of sky maps. Furthermore, we quantify the expected sky localization errors in the first two years of operation of the advanced detectors network.National Science Foundation (U.S.
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