effect

standard quantum limit

The standard quantum limit is the fundamental lower bound on measurement precision imposed by quantum noise in sensors and detectors.
24 related articles · 2 formulas · 3 who worked here

Description

In the 1970s, Vladimir Braginsky, analyzing the limits of measurement precision in macroscopic quantum systems, introduced the concept of the standard quantum limit. It stems from the Heisenberg uncertainty principle, but applies to continuous measurements. If you illuminate a mirror with a laser to track its position, quantum fluctuations in the photon number create radiation pressure that randomly displaces the mirror. The total coordinate error has a minimum, known as the SQL. Interestingly, this limit can be circumvented using quantum non-demolition measurements and squeezed states of light.

History

Vladimir Braginsky in 1967 first pointed out the quantum sensitivity limit in gravitational wave antennas. Further development of the SQL theory is associated with the work of Carlton Caves, who formalized the concept of the standard quantum limit in the 1980s. Experimental surpassing of the SQL was achieved at LIGO in collaboration with Caroline McKenzie and others, where using squeezed states of light improved sensitivity by 3 dB. Key contributions to understanding and overcoming the SQL were also made by Yu. I. Vorontsov and Kip Thorne.

How it works

SQL limits the precision of interferometric measurements, such as gravitational wave detectors, atomic force microscopes, and optical traps. For free masses, the limit depends on the measurement time: Δx SQL ~ √(ħτ/m). For a harmonic oscillator, there is a resonant regime where the SQL is reached when measuring amplitude. Overcoming the SQL is possible using quantum non-demolition measurements (measuring only one quadrature without disturbing the other) or squeezed states. Modern LIGO interferometers already operate below the SQL for certain frequency bands.

In practice

LIGO and Virgo gravitational wave detectors constantly hit this limit, requiring sophisticated quantum tricks to overcome it and detect tiny fluctuations of space-time.

Fun fact

LIGO gravitational wave observatories already operate in a regime where sensitivity is limited by quantum effects rather than classical noise.

Concept graph →

Formulas

$$\Delta \theta \ge \frac{1}{N}$$
Quantum measurement precision scales as 1/N.
What is in the formula
\Delta \thetavariableUncertainty in the estimated parameter — parameter uncertainty
NvariableNumber of independent probes or particles — particle number
\geoperatorIndicates a lower bound — greater than or equal
δθ\ge\frac{1}{n} · 2601.05457
$$\text{LOD} = k \frac{\sigma_{\text{noise}}}{\text{sensitivity}}$$
Minimum detectable concentration is proportional to noise standard deviation divided by sensitivity.
What is in the formula
LODvariablelimit of detection — limit of detection mole per cubic metre
kvariableconfidence factor (typically 3) — confidence factor
σ_noisevariablestandard deviation of the blank signal — noise standard deviation
sensitivityvariableslope of calibration curve (signal per concentration) — sensitivity cubic metre per mole
lod=3.3\frac{σ_{{noise}}}{α_{{local}}} · 2607.05629v1

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