Differences between revisions 33 and 34

Optical Levers

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

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Contents

Optical Levers

Scope

The scope of optical levers is to sense local angular motions (pitch and yaw) of any mirrors supported by vibration isolation system and other suspended stuffs including suspeded optical benches.

Applicable Documents

TBD; just see the links below.

General Description

Naming Conventions

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.
There should be no wedge; otherwise the multiple spots of light would be problematic.
See JGW-T1201231, Effect due to viewports for optical lever (in Japanese)

Detectors

The detector will be an ordinary quadruplet photocondutive circuit with QPD. The noise level at xxx Hz should be xxx m/Hz²

Pylons

The pylons must be designed.

-  ⇤ ← Revision 33 as of 2012-09-16 20:35:29 → 
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+   ← Revision 34 as of 2012-09-16 20:42:10 → ⇥
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-Deletions are marked like this.
+Additions are marked like this.
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-The scope of optical levers is to sense local angular motions (pitch and yaw) of any mirrors supported by vibration isolation system and other suspended stuffs including suspeded optical benches.
+ . The scope of optical levers is to sense local angular motions (pitch and yaw) of any mirrors supported by vibration isolation system and other suspended stuffs including suspeded optical benches.
 Line 11:
-TBD; just see the links below.
+ . TBD; just see the links below.
 Line 16:
-TBD
+ . TBD
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-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.
+ . 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.
 Line 37:
-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.
+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.
-Line 43:
+Line 41:
-For the light source, proposed candidates are
 * superluminous LED (SLED) or
 * laser light source as LIGO.
+ . For the light source, proposed candidates are
  * superluminous LED (SLED) or
  * laser light source as LIGO.
-Line 48:
+Line 46:
-The optical fibers transmit the light from the source to the focusing telescope.
+ . The optical fibers transmit the light from the source to the focusing telescope.
-Line 51:
+Line 49:
-TBD. Moving linear stage with micrometer and some optical components like collimators?
+ . TBD. Moving linear stage with micrometer and some optical components like collimators?
-Line 54:
+Line 52:
-See also the [[../Viewport1|viewport subsystem]].
It should be transparent for the light source wavelength.
There should be no wedge; otherwise the multiple spots of light would be problematic.
+ . See also the [[../Viewport1|viewport subsystem]].
 . It should be transparent for the light source wavelength.
 . There should be no wedge; otherwise the multiple spots of light would be problematic.
-Line 58:
+Line 56:
-See [[http://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=1231|JGW-T1201231, Effect due to viewports for optical lever (in Japanese)]]
+ . See [[http://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=1231|JGW-T1201231, Effect due to viewports for optical lever (in Japanese)]]
-Line 61:
+Line 59:
-The detector will be an ordinary quadruplet photocondutive circuit with QPD.
The noise level at '''xxx''' Hz should be '''xxx''' m/Hz^2^
+ . The detector will be an ordinary quadruplet photocondutive circuit with QPD. The noise level at '''xxx''' Hz should be '''xxx''' m/Hz^2^
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+Line 62:
-The pylons must be designed.
+ . The pylons must be designed.
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+Line 65:
-TBD
+ . TBD
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+Line 68:
-TBD
+ . TBD
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+Line 73:
-<!> Some of the LIGO documents listed below are '''NOT''' public; to access them, you may need your own LSC account.
+ . <!> Some of the LIGO documents listed below are '''NOT''' public; to access them, you may need your own LSC account.