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A free scan shows the junk files, broken settings and background clutter dragging Windows down - then fixes them in one click.Free scan · Windows 10 & 11Infrared light gives LIGO a way to use its next-generation crystalline mirror coatings without losing the control system that keeps the interferometer locked. Researchers demonstrated an auxiliary 1596-nanometre locking laser that can acquire control of a cavity, then hand that control to LIGO’s 1064-nanometre science laser in about 60 seconds. The transition was repeated successfully over several days.
Why a better mirror coating creates a locking problem
LIGO measures passing gravitational waves by monitoring incredibly small changes in the lengths of two perpendicular four-kilometre arms. Each arm ends in a 40-kilogram test mass. Those mirrors must remain in precisely controlled positions while the instrument looks for distance changes about one thousand times smaller than the width of a proton.
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The main measurement laser operates at 1064 nm. Before the detector can make science measurements, an auxiliary arm-length-stabilization (ALS) system helps acquire and hold the optical cavities. The current ALS arrangement uses green 532 nm light.
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The coating trade-off
LIGO’s planned upgrade uses crystalline mirror coatings intended to reduce optical thermal noise and improve sensitivity. The problem is that the new coating absorbs the 532 nm green light used by the existing locking system. Absorption adds heat and makes that wavelength unsuitable for reliable operation with the upgraded test masses.
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The engineering requirement is therefore twofold: find a locking wavelength the crystalline coating can tolerate, and keep a precise phase relationship with the 1064 nm laser that performs the gravitational-wave measurement.
How the 1596 nm infrared locking method works
An auxiliary wavelength the coating can tolerate
The demonstrated solution uses a 1596 nm infrared laser for lock acquisition. The upgraded crystalline coating is designed not to absorb this infrared wavelength, so the auxiliary beam can be used to control the cavity without introducing the green-light problem.
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Frequency conversion links infrared control to the science laser
The 1596 nm laser cannot simply replace the 1064 nm science beam. Instead, nonlinear optical crystals generate related frequencies through second-harmonic generation and sum-frequency generation. These converted signals provide a phase reference between the auxiliary laser and the 1064 nm laser.
That phase relationship lets the control system transfer the cavity lock from the infrared beam to the science beam. The infrared laser handles the difficult acquisition step; the 1064 nm laser then resumes the role required for normal gravitational-wave observations.
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What the transition requires
- Acquire the cavity lock with 1596 nm light. The infrared beam interacts with the cavity while avoiding absorption in the crystalline coating.
- Generate frequency-converted reference signals. Second-harmonic and sum-frequency crystals create optical signals that connect the infrared and 1064 nm frequencies.
- Phase-lock the two lasers. The control system establishes a stable phase relationship before attempting the transfer.
- Hand control to the 1064 nm science laser. The cavity remains locked as authority moves from the auxiliary beam to the main measurement beam.
What researchers demonstrated
The team reported a stable hand-over from the locking laser to the main laser in approximately 60 seconds. The result was described as faster than the current system, and the procedure was repeated successfully over several days rather than working only as a one-off demonstration.
They estimated the measurement error between the two lasers at roughly one-tenth the width of an atom when measured along a four-kilometre LIGO arm. This is an estimate of the inter-laser length or phase measurement in the demonstrated transfer; it is not a claim that LIGO has already achieved a corresponding improvement in its complete gravitational-wave sensitivity.
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Existing green locking versus the infrared approach
| Comparison point | Current ALS approach | 1596 nm approach for the upgrade |
|---|---|---|
| Locking wavelength | 532 nm green light | 1596 nm infrared light |
| Interaction with planned crystalline coating | The coating absorbs the green light | The new coating is intended not to absorb this wavelength |
| Relationship to the 1064 nm science laser | Current system uses the established ALS-to-science transition | Nonlinear frequency conversion phase-relates 1596 nm to 1064 nm so control can be transferred |
| Hand-over time | Exact time not stated; the new result was described as faster | About 60 seconds in the reported demonstration |
| Repeatability | Not stated in the announcement | Repeated successfully over several days |
| Reported transfer measurement error | Not stated | About one-tenth the width of an atom over a four-kilometre arm, according to the team’s estimate |
| Compatibility with future low-thermal-noise test masses | Limited by 532 nm absorption in the new coating | Designed to work with the planned crystalline coatings |
Where the project stood in 2025 and 2026
OzGrav’s annual report describes an A# system containing the 1596 nm auxiliary laser, second-harmonic and sum-frequency-generation crystals, and science-cavity mirrors. It records observation of a 532 nm beat signal in August 2025 and initial phase locking between the 1596 nm and 1064 nm lasers in November 2025.
The report set a 2026 goal of demonstrating the locking transition in a suspended cavity and publishing the experimental paper. That suspended-cavity step matters because a laboratory optical setup must ultimately operate with mirrors hung as they are in a gravitational-wave detector, not merely with a rigid bench-top substitute.
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Why this matters for LIGO’s sensitivity roadmap
Mirror coatings are central to detector sensitivity because coating thermal noise can mask the tiny mirror motions caused by gravitational waves. Lower-noise crystalline coatings could improve the instrument, but only if the detector can still acquire and maintain lock. The infrared method removes the specific wavelength conflict instead of forcing the upgrade to keep the older coating or abandon the established 1064 nm measurement architecture.
A 2020 Massachusetts Institute of Technology report on a tested LIGO mirror sample cited 99.9995% infrared reflectivity. That figure describes a particular sample and test, not every future crystalline coating, but it illustrates why coating characterization remains essential before a material is installed in a detector.
What remains to be established
The University of Western Australia announcement reports the headline demonstration and identifies collaborators at the University of Western Australia, the Australian National University and the University of Adelaide through OzGrav. It also says the study was published in Physical Review D.
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Detailed uncertainty budgets, apparatus diagrams, control-loop limits and the full peer-reviewed method are not contained in the announcement itself. The published paper and the suspended-cavity demonstration are therefore the appropriate references for judging performance beyond the reported 60-second transfer, multi-day repeatability and estimated one-tenth-atom measurement error.
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