755 research outputs found
Trade-off between quantum and thermal fluctuations in mirror coatings yields improved sensitivity of gravitational-wave interferometers
We propose a simple way to improve the laser gravitational-wave detectors
sensitivity by means of reduction of the number of reflective coating layers of
the core optics mirrors. This effects in the proportional decrease of the
coating thermal noise, the most notorious among the interferometers technical
noise sources. The price for this is the increased quantum noise, as well as
high requirements for the pump laser power and power at the beamsplitter.
However, as far as these processes depend differently on the coating thickness,
we demonstrate that a certain trade-off is possible, yielding a 20-30% gain
(for diverse gravitational wave signal types and interferometer
configurations), providing that feasible values of laser power and power on the
beamsplitter are assumed.Comment: 11 pages, 4 figures, 4 table
Quantum noise of non-ideal Sagnac speed meter interferometer with asymmetries
The speed meter concept has been identified as a technique that can
potentially provide laser-interferometric measurements at a sensitivity level
which surpasses the Standard Quantum Limit (SQL) over a broad frequency range.
As with other sub-SQL measurement techniques, losses play a central role in
speed meter interferometers and they ultimately determine the quantum noise
limited sensitivity that can be achieved. So far in the literature, the quantum
noise limited sensitivity has only been derived for lossless or lossy cases
using certain approximations (for instance that the arm cavity round trip loss
is small compared to the arm cavity mirror transmission). In this article we
present a generalised, analytical treatment of losses in speed meters that
allows accurate calculation of the quantum noise limited sensitivity of Sagnac
speed meters with arm cavities. In addition, our analysis allows us to take
into account potential imperfections in the interferometer such as an
asymmetric beam splitter or differences of the reflectivities of the two arm
cavity input mirrors. Finally,we use the examples of the proof-of-concept
Sagnac speed meter currently under construction in Glasgow and a potential
implementation of a Sagnac speed meter in the Einstein Telescope (ET) to
illustrate how our findings affect Sagnac speed meters with meter- and
kilometre-long baselines.Comment: 22 pages, 8 figures, 1 table, (minor corrections and changes made to
text and figures in version 2
To the practical design of the optical lever intracavity topology of gravitational-wave detectors
The QND intracavity topologies of gravitational-wave detectors proposed
several years ago allow, in principle, to obtain sensitivity significantly
better than the Standard Quantum Limit using relatively small anount of optical
pumping power. In this article we consider an improved more ``practical''
version of the optical lever intracavity scheme. It differs from the original
version by the symmetry which allows to suppress influence of the input light
amplitude fluctuation. In addition, it provides the means to inject optical
pumping inside the scheme without increase of optical losses.
We consider also sensitivity limitations imposed by the local meter which is
the key element of the intracavity topologies. Two variants of the local meter
are analyzed, which are based on the spectral variation measurement and on the
Discrete Sampling Variation Measurement, correspondingly. The former one, while
can not be considered as a candidate for a practical implementation, allows, in
principle, to obtain the best sensitivity and thus can be considered as an
ideal ``asymptotic case'' for all other schemes. The DSVM-based local meter can
be considered as a realistic scheme but its sensitivity, unfortunately, is by
far not so good just due to a couple of peculiar numeric factors specific for
this scheme.
From our point of view search of new methods of mechanical QND measurements
probably based on improved DSVM scheme or which combine the local meter with
the pondermotive squeezing technique, is necessary.Comment: 27 pages, 6 figure
Achieving ground state and enhancing entanglement by recovering information
For cavity-assisted optomechanical cooling experiments, it has been shown in
the literature that the cavity bandwidth needs to be smaller than the
mechanical frequency in order to achieve the quantum ground state of the
mechanical oscillator, which is the so-called resolved-sideband or good-cavity
limit. We provide a new but physically equivalent insight into the origin of
such a limit: that is information loss due to a finite cavity bandwidth. With
an optimal feedback control to recover those information, we can surpass the
resolved-sideband limit and achieve the quantum ground state. Interestingly,
recovering those information can also significantly enhance the optomechanical
entanglement. Especially when the environmental temperature is high, the
entanglement will either exist or vanish critically depending on whether
information is recovered or not, which is a vivid example of a quantum eraser.Comment: 9 figures, 18 page
QND measurements for future gravitational-wave detectors
Second-generation interferometric gravitational-wave detectors will be
operating at the Standard Quantum Limit, a sensitivity limitation set by the
trade off between measurement accuracy and quantum back action, which is
governed by the Heisenberg Uncertainty Principle. We review several schemes
that allows the quantum noise of interferometers to surpass the Standard
Quantum Limit significantly over a broad frequency band. Such schemes may be an
important component of the design of third-generation detectors.Comment: 22 pages, 6 figures, 1 table; In version 2, more tutorial information
on quantum noise in GW interferometer and several new items into Reference
list were adde
Sensitivity limitations in optical speed meter topology of gravitational-wave antennae
The possible design of QND gravitational-wave detector based on speed meter
principle is considered with respect to optical losses. The detailed analysis
of speed meter interferometer is performed and the ultimate sensitivity that
can be achieved is calculated. It is shown that unlike the position meter
signal-recycling can hardly be implemented in speed meter topology to replace
the arm cavities as it is done in signal-recycled detectors, such as GEO 600.
It is also shown that speed meter can beat the Standard Quantum Limit (SQL) by
the factor of in relatively wide frequency band, and by the factor of
in narrow band. For wide band detection speed meter requires quite
reasonable amount of circulating power MW. The advantage of the
considered scheme is that it can be implemented with minimal changes in the
current optical layout of LIGO interferometer.Comment: 20 pages, 12 figure
Optimizing the regimes of Advanced LIGO gravitational wave detector for multiple source types
We develop here algorithms which allow to find regimes of signal-recycled
Fabry-Perot--Michelson interferometer (for example, Advanced LIGO), optimized
concurrently for two (binary inspirals + bursts) and three (binary inspirals +
bursts + millisecond pulsars) types of gravitational waves sources. We show
that there exists a relatevely large area in the interferometer parameters
space where the detector sensitivity to the first two kinds of sources differs
only by a few percent from the maximal ones for each kind of source. In
particular, there exists a specific regime where this difference is ~0.5 for
both of them. Furthermore we show that even more multipurpose regimes are also
possible, that provide significant sensitivity gain for millisecond pulsars
with only minor sensitivity degradation for binary inspirals and bursts.Comment: 10 pages, 14 figures, 3 tables. Minor corrections in main text are
done in version 2 and two plots and one table are added for the sake of
clarity of the obtained result
Local-Oscillator Noise Coupling in Balanced Homodyne Readout for Advanced Gravitational Wave Detectors
The second generation of interferometric gravitational wave detectors are
quickly approaching their design sensitivity. For the first time these
detectors will become limited by quantum back-action noise. Several back-action
evasion techniques have been proposed to further increase the detector
sensitivity. Since most proposals rely on a flexible readout of the full
amplitude- and phase-quadrature space of the output light field, balanced
homodyne detection is generally expected to replace the currently used DC
readout. Up to now, little investigation has been undertaken into how balanced
homodyne detection can be successfully transferred from its ubiquitous
application in table-top quantum optics experiments to large-scale
interferometers with suspended optics. Here we derive implementation
requirements with respect to local oscillator noise couplings and highlight
potential issues with the example of the Glasgow Sagnac Speed Meter experiment,
as well as for a future upgrade to the Advanced LIGO detectors.Comment: 7 pages, 5 figure
Design of a speed meter interferometer proof-of-principle experiment
The second generation of large scale interferometric gravitational wave
detectors will be limited by quantum noise over a wide frequency range in their
detection band. Further sensitivity improvements for future upgrades or new
detectors beyond the second generation motivate the development of measurement
schemes to mitigate the impact of quantum noise in these instruments. Two
strands of development are being pursued to reach this goal, focusing both on
modifications of the well-established Michelson detector configuration and
development of different detector topologies. In this paper, we present the
design of the world's first Sagnac speed meter interferometer which is
currently being constructed at the University of Glasgow. With this
proof-of-principle experiment we aim to demonstrate the theoretically predicted
lower quantum noise in a Sagnac interferometer compared to an equivalent
Michelson interferometer, to qualify Sagnac speed meters for further research
towards an implementation in a future generation large scale gravitational wave
detector, such as the planned Einstein Telescope observatory.Comment: Revised version: 16 pages, 6 figure
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