Energetic Quantum Limit in Large-Scale Interferometers

For each optical topology of an interferometric gravitational wave detector, quantum mechanics dictates a minimum optical power (the ``energetic quantum limit'') to achieve a given sensitivity. For standard topologies, when one seeks to beat the standard quantum limit by a substantial factor, the energetic quantum limit becomes impossibly large. Intracavity readout schemes may do so with manageable optical powers.Comment: Revised version; to be published in Proceedings of the 1999 Edoardo Amaldi Conference on Gravitational Waves; 11 pages including figures; manuscript is RevTex; figures are .eps; an AIP style file is include

Dual-Resonator Speed Meter for a Free Test Mass

A description and analysis are given of a ``speed meter'' for monitoring a classical force that acts on a test mass. This speed meter is based on two microwave resonators (``dual resonators''), one of which couples evanescently to the position of the test mass. The sloshing of the resulting signal between the resonators, and a wise choice of where to place the resonators' output waveguide, produce a signal in the waveguide that (for sufficiently low frequencies) is proportional to the test-mass velocity (speed) rather than its position. This permits the speed meter to achieve force-measurement sensitivities better than the standard quantum limit (SQL), both when operating in a narrow-band mode and a wide-band mode. A scrutiny of experimental issues shows that it is feasible, with current technology, to construct a demonstration speed meter that beats the wide-band SQL by a factor 2. A concept is sketched for an adaptation of this speed meter to optical frequencies; this adaptation forms the basis for a possible LIGO-III interferometer that could beat the gravitational-wave standard quantum limit h_SQL, but perhaps only by a factor 1/xi = h_SQL/h ~ 3 (constrained by losses in the optics) and at the price of a very high circulating optical power --- larger by 1/xi^2 than that required to reach the SQL.Comment: RevTex: 13 pages with 4 embedded figures (two .eps format and two drawn in TeX); Submitted to Physical Review

The noise in gravitational-wave detectors and other classical-force measurements is not influenced by test-mass quantization

It is shown that photon shot noise and radiation-pressure back-action noise are the sole forms of quantum noise in interferometric gravitational wave detectors that operate near or below the standard quantum limit, if one filters the interferometer output appropriately. No additional noise arises from the test masses' initial quantum state or from reduction of the test-mass state due to measurement of the interferometer output or from the uncertainty principle associated with the test-mass state. Two features of interferometers are central to these conclusions: (i) The interferometer output (the photon number flux N(t) entering the final photodetector) commutes with itself at different times in the Heisenberg Picture, [N(t), N(t')] = 0, and thus can be regarded as classical. (ii) This number flux is linear in the test-mass initial position and momentum operators x_o and p_o, and those operators influence the measured photon flux N(t) in manners that can easily be removed by filtering -- e.g., in most interferometers, by discarding data near the test masses' 1 Hz swinging freqency. The test-mass operators x_o and p_o contained in the unfiltered output N(t) make a nonzero contribution to the commutator [N(t), N(t')]. That contribution is cancelled by a nonzero commutation of the photon shot noise and radiation-pressure noise, which also are contained in N(t). This cancellation of commutators is responsible for the fact that it is possible to derive an interferometer's standard quantum limit from test-mass considerations, and independently from photon-noise considerations. These conclusions are true for a far wider class of measurements than just gravitational-wave interferometers. To elucidate them, this paper presents a series of idealized thought experiments that are free from the complexities of real measuring systems.Comment: Submitted to Physical Review D; Revtex, no figures, prints to 14 pages. Second Revision 1 December 2002: minor rewording for clarity, especially in Sec. II.B.3; new footnote 3 and passages before Eq. (2.35) and at end of Sec. III.B.

Interview with Vladimir B. Braginsky

Interview, January 15, 1997, with Vladimir B. Braginsky, experimental physicist, Moscow State University. Recalls family background and childhood in the USSR during World War II. Matriculates at Moscow State University 1955, PhD 1959, joins faculty 1969. Work with Y. B. Zel'dovich on search for quarks and detection of gravitational radiation; work with Vitaly Ginzburg on detecting time dependence of gravitational constant. Comments on Andrei Sakharov. Joins Communist Party in Khrushchev era. Science hierarchy in the USSR. Constraints on foreign travel. Meets John A. Wheeler in 1968 at international conference; gives a talk on quantum measurement; invited to visit Princeton, Harvard, University of Maryland, and Caltech, 1970. Discusses Joseph Weber's gravitational-wave experiment. Admiration for Kip S. Thorne. Early impressions of LIGO project on visits to Caltech in 1981 and 1984. His group at Moscow State University becomes LIGO collaborator. Comments on 1962 work of M. E. Gerzenstein and V. I. Pustovoit in gravitational-wave detection. Visit from Thorne in Moscow, 1977, with invitation to join LIGO. Comments on R. W. P. Drever and Rainer Weiss; on disagreements between Drever and Rochus (Robbie) Vogt, LIGO director 1987-1994. Fairchild Scholar at Caltech, 1990; LIGO's technical difficulties; project's disarray. Expresses optimism re LIGO directorship of Barry Barish and potential improvements in LIGO sensitivity. His laboratory's work on mirror suspension

Frequency tuning of the whispering gallery modes of silica microspheres for CQED and spectroscopy

We have tuned the whispering gallery modes of a fused silica microresonator over nearly 1 nm at 800 nm, i.e. over 0.5 FSR or 10^6 linewidths of the resonator. This has been achieved by a new method based on the stretching of a two-stem microsphere. The devices described below will permit new Cavity-QED experiments with this high-Q optical resonator when it is desirable to optimize its coupling to emitters with given transition frequencies. The tuning capability demonstrated here is compatible with both UHV and low temperature operation, which should be useful for future experiments with laser cooled atoms or single quantum dots.Comment: ReVTeX, 4 pages, 3 figure

Foucault pendulum at the South Pole: Proposal for an experiment to detect the Earth's general relativistic gravitomagnetic field

An experiment is proposed for measuring the earth's gravitomagnetic field by monitoring its effect on the plane of swing of a Foucault pendulum at the south pole ("dragging of inertial frames by earth's rotation"). With great effort a 10% experiment in a measurement time of several months might be achieved

Laboratory experiments to test relativistic gravity

Advancing technology will soon make possible a new class of gravitation experiments: pure laboratory experiments with laboratory sources of non-Newtonian gravity and laboratory detectors. This paper proposes seven such experiments; and for each one it describes, briefly, the dominant sources of noise and the technology required. Three experiments would utilize a high-Q torque balance as the detector. They include (i) an "Ampère-type" experiment to measure the gravitational spin-spin coupling of two rotating bodies, (ii) a search for time changes of the gravitation constant, and (iii) a measurement of the gravity produced by magnetic stresses and energy. Three experiments would utilize a high-Q dielectric crystal as the detector. They include (i) a "Faraday-type" experiment to measure the "electric-type" gravity produced by a time-changing flux of "magnetic-type" gravity, (ii) a search for "preferred-frame" and "preferred-orientation" effects in gravitational coupling, and (iii) a measurement of the gravitational field produced by protons moving in a storage ring at nearly the speed of light. One experiment would use a high-Q toroidal microwave cavity as detector to search for the dragging of inertial frames by a rotating body

Microtorus: a High Finesse Microcavity with Whispering-Gallery Modes

We have demonstrated a 165 micron oblate spheroidal microcavity with free spectral range 383.7 GHz (3.06nm), resonance bandwidth 25 MHz (Q ~ 10^7) at 1550nm, and finesse F > 10^4. The highly oblate spheroidal dielectric microcavity combines very high Q-factor, typical of microspheres, with vastly reduced number of excited whispering-gallery (WG) modes (by two orders of magnitude). The very large free spectral range in the novel microcavity - few hundred instead of few GigaHertz in typical microspheres - is desirable for applications in spectral analysis, narrow-linewidth optical and RF oscillators, and cavity QED.Comment: 11 pages, 3 figure