Applying_magnets

A LIGO Optics Technician applies servo magnets to one of LIGO's fused silica masses. (Photo: LIGO)

LIGO Optics

LIGO Optics Beam Splitter????

(Credit: Kim Fetrow/Imageworks)

 

LIGO’s primary interferometer optics include four test masses (two in each interferometer arm), beam splitters, a power-recycling mirror, and a signal recycling mirror. The mirror technology in LIGO’s detectors represents the accomplishments of a decades-long global collaboration.

LIGO Optics ETMs Before Install

Two of LIGO's 'test masses' (mirrors), so called because they 'test' (or feel for) changes in LIGO's arm-lengths caused by a passing gravitational wave. Each silica cylinder weighs 40 kg. (Credit: Caltech/MIT/LIGO Lab)

LIGO’s test masses are made of fused silica, cast from ultra-pure material with low OH (hydroxide) content to minimize infrared (IR) absorption. Since LIGO’s laser is an IR laser, its optics must not absorb IR radiation. Doing so would result in heating and in significant changes to the shape of the mirrors, thus critically affecting LIGO’s ability to make the precise measurements it must make. LIGO’s main mirrors only absorb one out of every 3.3 million photons, the rest being reflected (or transmitted). Some heating does occur, but an auxiliary system using a CO2 laser heats the mirrors precisely enough to counteract the shape-changes that occur as a result of heating from LIGO’s main laser.

LIGO Optics ITM Inspection

Technicians inspect the "First Contact" coating on one of LIGO's Input Test Masses. (Credit: Caltech/MIT/LIGO Lab)

LIGO’s optics are also hefty. The input and end test masses each weigh 40 kg giving them large inertial masses that intrinsically provide some level of vibration resistance (although much more is required. See Vibration Isolation). The image at right shows two LIGO test masses before they were installed in the interferometer.

The mirrors are coated with dozens of layers of optical coatings and polished to nanometer smoothness. Again, this level of precision is required to ensure that LIGO’s laser has a clean, stable, and perfectly tooled reflective surface that enables it to follow a clean path as it travels through the interferometer, making around 280 reflections before impacting the photodetector. Without these precautions, detecting a gravitational wave would be impossible.