Quantum Measurement Group @ MIT

The Quantum Measurement Group @ MIT is a subgroup of the LIGO MIT laboratory. All the members contribute to the Quantum Measurement Group, but here are the personnel of the scientists who devote themselves to experimental research on squeezed light.

Presently, knowledge of the Universe comes from observing the light that is radiated by stars; from the spectacular light shows that accompany the explosive births and deaths of stars; and ancient light from the Big Bang itself. But is not be the only messenger to carry the secrets of the distant Universe to us. Many of these spectacular events also emit gravitational waves. Gravitational waves are ripples in the fabric of space and time that were predicted to exist by Einstein in 1916. They are very faint, however, and have never been directly observed. My work involves making instruments, based on very sensitive interferometry using lasers to sense the position of test masses that move in response to gravitational waves (see LIGO).

The sensitivity of a detector determines how far into the distant skies it can "see." Over the years, as the LIGO detectors have become increasingly more sensitive in the quest to see ever more distant events in our Universe, the very basic laws of quantum mechanics have become an impediment to the LIGO mission. This leads us to the focus of the Quantum Measurement group at MIT.

The primary goal of this research is to study non-classical states of light for improving the measurement sensitivity of the LIGO detectors. Theoretical research on the generation of squeezed light is under way at MIT while starting experimental research this summer.

The effect of a gravitational-wave on interferometers like those of LIGO is to cause the distances between the mirrors of the interferometer to change at the frequency of the GW. This relative displacement of mirrors can be measured as a phase shift of the light traveling in the arms of the interferometer using the interference of the laser light at the anti-symmetric port of the interferometer. The principle is straightforward, but the relative displacements being measured are one-thousandth the size of an atomic nucleus, i.e. 10-18 m for present-day detectors, and another factor of 10 smaller in next-generation detectors.

Since laser light is used to make precise measurements of the positions of the mirrors of the interferometer, the noise on the light sets important limits on how well the displacements can be measured.

The effect of a gravitational-wave on interferometers like those of LIGO is to cause the distances between the mirrors of the interferometer to change at the frequency of the GW. This effective displacement of mirrors can be measured as a phase shift of the light traveling in the arms of the interferometer using the interference of the laser light at the anti-symmetric port of the interferometer. Easy enough, except that the relative displacements being measured are one-thousandth the size of an atomic nucleus, i.e. 10-18 m for present-day detectors, and another factor of 10 smaller in next-generation detectors.

Since laser light is used to make precise measurements of the positions of the mirrors of the interferometer, the noise on the light sets important limits on how well the displacements can be measured. When a pristine laser beam is stripped of all technical noise (such as fluctuations or drifts in the power or the frequency), it still has quantum mechanical noise on it. The easiest way to think of noise on the laser light is in terms of the Heisenberg Uncertainty Principle: amplitude and phase are complementary variables, so uncertainty in amplitude (DA) and in phase (Df) must satisfy (DA).(Df) > 1. For quantum-limited laser light with minimum uncertainty, DA = Df and the light is in a coherent state. In the amplitude-phase plane, the coherent state is best represented as a vector (stick) whose length and phase angle correspond to the classical amplitude and phase, respectively, while the ball at the end of the stick corresponds to the uncertainty.

The consequences of this uncertainty in amplitude and phase have a profound effect on our ability to use light to measure the position of a particle (mirrors of an interferometer, e.g.). Two effects are important: (1) Radiation-pressure noise: We know that light can impart momentum when it reflects of a mirror, and that momentum is proportional to the intensity of the light beam. Since the quantum uncertainty leads to fluctuations in the amplitude of the light, the momentum – and hence the force -- acting on the mirror will also fluctuate. This limits our ability to measure the position of the mirror, since our measurement itself disturbs the mirror position -- an effect known as back-action; and (2) Shot noise: The mirror position is inferred from phase shifts of the laser light traveling in two arms of the interferometer. The uncertainty in the phase of the light due to the quantum fluctuations then directly limits our ability to measure the mirror position.

So even quantum-limited laser light limits our ability to measure the position of the mirror: in the first case, the amplitude fluctuations kick the mirror around; in the second case, phase fluctuations make the light an inaccurate meter.

There’s an even more interesting effect hidden in all this: even if no light were impinging on the mirror, it would still be buffeted around due to vacuum fluctuations. Only in this case, we wouldn’t care, since without laser light we couldn’t measure the position of the mirror anyway.

One way to get around this problem is to create more exotic state of light, sometimes call a “squeezed” state. The Heisenberg Uncertainty Principle requires that area of the ball be unity, but it doesn’t say the ball can’t be turned into an ellipse of unit area. This leads to the concept of squeezing: we can reduce the fluctuations in one quadrature at the expense of increasing them in the orthogonal quadrature.

Why is this useful? Well, say we squeeze the noise in the phase quadrature, then our ability to measure the phase shift of the light gets better (same “signal” but less “noise”). But wait, doesn’t that make the amplitude fluctuations larger and then doesn’t the back-action noise get worse? Yes, that’s true. So this trick only works if the mirrors are very heavy and aren’t easily kicked by the light, or if the light power is not too large, so the radiation pressure force is not too big.

This leads to a quantity called the standard quantum limit. Suppose we try to measure the position of a particle of mass M with power I0 circulating in our interferometer. If the radiation pressure noise (which is proportional to I0/(M W2)) is not correlated with the shot noise (which is proportional to1/I0), then we reach the standard quantum limit (SQL) when the radiation pressure noise is equal to the shot noise. In general we have a few knobs to turn in making a measurement at the SQL: The mass of the particle, the laser light power, and the frequency at which we make the measurement.

If we wish to make a more precise measurement than allowed by the SQL (or the minimum uncertainty state), we must correlate the amplitude and phase quadratures.

There are a number of ways to create these correlations, but we are pursuing an experimental program to generate squeezed states. There are two very different methods for generating these squeezed states:

(1) Squeezing using non-linear crystals
(2) Squeezing using radiation pressure effects in interferometers