Optical Lever (Room Temperature)

Related subgroups: VIS, IOO, MIF, VAC, CRY...

Contents

Optical Lever (Room Temperature)

Scope

Sensing local motions including longitudinal dof and all alignment dofs (pitch, yaw and roll) of any mirrors supported by vibration isolation system.

Note on the operating temperature: here the system is assumed to be utilized at room temperature, not in cryogenic temperature.

Applicable Documents

TBD; just see the links below.

General Description

Naming Conventions

TBD

Locations

BS chamber
ITM chambers (X,Y)
ETM chambers (X,Y)
PRC chambers (PRC, PR2, PR3)
SRC chambers (SRC, SR2, SR3)
MC chambers (MC1, MC2...)

Requirements

Sensor noise should be less than xxx.
Sensor's dynamic range should be greater than xxx.
At least horizontal degrees of freedom (X,Y)
Preferably a vertical sensor (Z) and side
The sensors have to be rigidly mounted on the ground so that these are useful for remembering the position of the mirror and recording the drifts.

Characteristics

Each optical lever consists of an optical system, a frontend circuit, and a human interface software. The optical system consists of the following parts: a light source, optical fibers, a focusing telescope, viewport windows, a detector, and pylons which support the focusing telescope and the detector. The frontend circuit is TBD. Maybe we need analog cables (and what kind of connector should we use?), whitening filters and antialiasing filters. Maybe the matrix circuit will be realized using the digital systems, but in commissioning phase, we will need analog matrix. The human interface software is TBD, which shows the mirrors' dofs monitored by Optical Levers.

Light source

For the light source, proposed candidates are

superluminous LED (SLED) or
laser light source as LIGO.

Optical Fibers

The optical fibers transmit the light from the source to the focusing telescope.

Focusing Telescopes

TBD. Moving linear stage with micrometer and some optical components like collimators?

Viewport windows

See also the viewport subsystem. It should be transparent for the light source wavelength. The wedge should be avoided; otherwise the multiple spots of light would be problematic.

Detectors

The detector will be an ordinary quadruplet photocondutive circuit with QPD.

Inspection plans

TBD

Procurement process and plans

TBD

Links

Some of the LIGO documents listed below are NOT public; to access them, you may need your own LSC account.