As I've mentioned in yesterday's elog MC mirrors start to move in a synchronistic manner. I've plotted DELTA_GUR = GUR1_X - alpha * GUR2_X, where alpha = const to make the transfer functions SEISMOMETER -> ADC equal for each channel. I've noticed that DELTA_GUR decreases below 10 Hz compared to GUR1_X as theoretically predicted. But starting from 1 Hz DELTA_GUR starts to increase. I decided that this is Guralp noise floor. Today I checked this, this is indeed the case.

In the frequency range 0.01 - 1.5 Hz Gur noise is comparable to the signal DELTA_GUR. For that reason we see low coherence between MC_F and GUR1_X in this frequency range. 

Guralp noise floor was determined by placing 2 seimometers close to each other and subtracting by Wiener filtering.

Conclusion: To filter seismic noise out of MC_F we need more sensitive seimometeres.

The beam at the dark port was largely clipped.
The arm transmissions (TRX/TRY) were ~0.6 no matter how you try to align.

The PZT1/2 X was scanned and TRX/TRY are now both ~0.9.
This means that the beam was mostly clipped in or after the mode mathing optics.

FPMI contrast is (2.45-0.02)/(2.45+0.02) = 98%
Not so bad although it does not tell anything about clipping before the IFO.

In the next opportunity, we should try to "pin" the beam axis on the arm mirrors using A2L.

1. I am not sure exactly where the clipping was. It means that a small clipping might still be there.

2. I am afraid that the beam is still clipped in the faraday. The beam can be scanned using the steering on the PSL table.

 MC_F low frequency noise might be due to local damping electronics. I did not measure OSEM noise, but even without it electronics (AA -> ICS 110 -> ADC) provide sufficient amount of noise. 

These 2 image show electronics noise and coherence between OSEM signal / seismic

From these 2 plots we might think that SNR > 10 and coherence OSEM / GUR is high at the frequency range 0.1 - 10 Hz and this is not a big problem.

However, at low frequencies the length of seismic waves becomes large enough and relative oscillations of MC2 and MC13 decrease.

For 1 wave ( u(MC2) - u(MC1) ) / u(MC2) = sin(2 * pi * L  * f  / c), L - distance between MC1 and MC2 where 2 seismometers are located. So MC123 move according to seismic motion and electronics noise is not seen unless we look at MC Length. Here this noise is seen, because mirrors move in a synchronistic manner. 

To check this I measured seismic noise with 2 guralps at distance 12 meters - at MC1 and MC2. Then I've computed the difference between these signals. And indeed at low frequencies, relative motion is much less.

Green, blue - GUR1,2_X

Red - differential motion GUR1_X - GUR2_X

The following plot illustrates how electronics noise effects MC_F. Green is the signal to coils. Red - electronics noise. Blue, black, cyan - simulated contribution to MC_F for different seismic waves speed. Most probably seismic waves have waves in the range 50 - 800 m/s, others are deep. The plot shows that electronics noise is big enough to disturb coherence between MC_F and seismic noise. 

Here is a rough calculation of the seismic waves speed. The following plot shows the ratio of psd of differential MC2-MC1 motion to MC2 motion.

If seismometers would be very far, ratio would be 1 if we neglect the difference in transfer function SEISMOMETER -> ADC for each channel. The drift of the ratio from 1 to 1.3 demonstrates this effect. Ratio starts to decrease at 15 Hz according to sin (2*pi*L*f/c) ~ 2*pi*L/c * f. So 2*pi*L/c * f_0 = pi/2 => c = 4 * L * f = 600 m / sec.

[Koji, Yuta, Suresh]

We measured the MC spot positions after re-aligning the MC.  The spot positions are listed below:

spot positions in mm (MC1,2,3 pit MC1,2,3 yaw):
    3.9073    6.6754    2.8591   -7.6985   -0.9492    7.0423

Procedure:

1) In the directory /opt/rtcds/caltech/c1/scripts/ASS/MC  we have the following scripts

      a) mcassUp:    This sets up the MCASS lockins to excite each of the MC mirrors at a different frequency

      b) mcassOn:    This sets the MCASS output matrix to actually send the excitation signals to the mirrors

      c) senseMCdecenter:  This sequentially introduces a 10% offset into the coil gains of each mirror degree of freedom.   It also sends the lockin output data to the screen. 

      d) sensemcass.m :  This is a matlab file which digests the data gathered by the senseMCdecenter script to print a couple of plots and compute the spot positions.

      e) MCASS_StripTool.stp:  This is a set-up file for the StripTool which allows us to see the MCASS-lockin_outputs.  It is nice to see the action of senseMCdecenter  script  at work.

2) So the series of commands to use are

      a) ./StripTool  <-- MCASS_StripTool.stp

      b) ./mcassUp

      c) ./mcassOn

      d) ./senseMCdecenter | tee Output_file

       e) ./mcassOff

      f) ./mcassDown

       g) matlab <-- sensemcass.m  <---- Output_file

There is now a job in the crontab that will run the shell wrapper every hour, so the pages _should_ take care of themselves. If you make adjustments to the configuration file they will get picked up on the hour, or you can just run the script by hand at any time.

$ crontab -l
# m h  dom mon dow   command
0 */1 * * * bash /home/controls/public_html/summary/bin/c1_summary_page.sh > /dev/null 2>&1

40m summary webpages

 The aLIGO-style summary webpages are now running on 40m data! They are running on megatron so can be viewed from within the martian network at:

http://192.168.113.209/~controls/summary

At the moment I have configured the 5 seismic BLRMS bands, and a random set of PSL channels taken from a strip tool.

Technical notes

• The code is in python depending heavily on the LSCSoft PyLAL and GLUE modules.
  • /home/controls/public_html/summary/bin/summary_page.py
• The HTML is supported by a CSS script and a JS script which are held locally in the run directory, and JQuery linked from the google repo.
  • /home/controls/public_html/summary/summary_page.css
  • /home/controls/public_html/summary/pylaldq.js
• The configuration is controlled via a single INI format file
  • /home/controls/public_html/summary/share/c1_summary_page.ini

Getting frames

Since there are no segments or triggers for C1, the only data sources are GWF frames. These are mounted from the framebuilder under /frames on megatron. There is a python script that takes in a pair of GPS times and a frame type that will locate the frames for you. This is how you use it to find T type frames (second trends) for May 25 2012:

python /home/controls/public_html/summary/bin/framecache.py --ifo C1 --gps-start-time 1021939215 --gps-end-time 1022025615 --type T -o framecache.lcf

If you don't have GPS times, you can use the tconvert tool to generate them

$ tconvert May 25
1021939215

The available frame types, as far as I'm aware are R (raw), T (seconds trends), and M (minute trends).

Running the code

The code is designed to be fairly easy to use, with most of the options set in the ini file. The code has three modes - day, month, or GPS start-stop pair. The month mode is a little sketchy so don't expect too much from it. To run in day mode:

python /home/controls/public_html/summary/bin/summary_page.py --ifo C1 --config-file /home/controls/public_html/summary/share/c1_summary_page.ini --output-dir . --verbose --data-cache framecache.lcf -SRQDUTAZBVCXH --day 20120525

Please forgive the large apparently arbitrary collection of letters, since the 40m doesn't use segments or triggers, these options disable processing of these elements, and there are quite a few of them. They correspond to --skip-something options in long form. To see all the options, run

python /home/controls/public_html/summary/bin/summary_page.py --help

There is also a convenient shell script that will run over today's data in day mode, doing everything for you. This will run framecache.py to find the frames, then run summary_page.py to generate the results in the correct output directory. To use this, run

bash /home/controls/public_html/summary/bin/c1_summary_page.sh

Configuration

Different data tabs are disabled via command link --skip-this-tab style options, but the content of tabs is controlled via the ini file. I'll try to give an overview of how to use these. The only configuration required for the Seismic BLRMS 0.1-0.3 Hz tab is the following section:

[data-Seismic 0.1-0.3 Hz]
channels = C1:PEM-RMS_STS1X_0p1_0p3,C1:PEM-RMS_STS1Y_0p1_0p3,C1:PEM-RMS_STS1Z_0p1_0p3
labels = STS1X,STS1Y,STS1Z
frame-type = R
plot-dataplot1 =
plot-dataplot3 =
amplitude-log = True
amplitude-lim = 1,500
amplitude-label = BLRMS motion ($\mu$m/s)

The entries can be explained as follows:

1. '[data-Seismic 0.1-0.3 Hz] - This is the section heading. The 'data-' mark identifies this as data, and is a relic of how the code is written, the 'Seismic 0.1-0.3 Hz' part is the name of the tab to be displayed in the output.
2. 'channels = ...' - This is a comma-separated list of channels as they are named in the frames. These must be exact so the code knows how to find them.
3. 'labels = STS1X,STS1Y,STS1Z' - This is a comma-separated list of labels mapping channel names to something more readable for the plots, this is optional.
4. 'frame-type = R' - This tells the code what frame type the channels are, so it can determine from which frames to read them, this is not optional, I think.
5. 'plot-dataplotX' - This tells the code I want to run dataplotX for this tab. Each 'dataplot' is defined in it's own section, and if none of these options are given, the code tries to use all of them. In this configuration 'plot-dataplot1' tells the code I want to display the time-series of data for this tab.
6. 'amplitude-XXX = YYY' - This gives the plotter specific information about this tab that overrides the defaults defined in the dataplotX section. The options in this example tell the plotter that when plotting amplitude on any plot, that axis should be log-scale, with a limit of 1-500 and with a specific label. The possible plotting configurations for this style of option are: 'lim', 'log', 'label', I think.

Other compatible options not used in this example are:

• scale = X,Y,Z - a comma-separated list of scale factors to apply to the data. This can either be a single entry for all channels, or one per channel, nothing in between.
• offset = X,Y,Z - another comma-separate list of DC offsets to apply to the data (before scaling, by default). DAQ noise may mean a channel that should read zero during quick times is offset by some fixed amount, so you can correct that here. Again either one for all channels, or one per channel.
• transform = lambda x: f(x) - a python format lambda function. This is basically any mathematical function that can be applied to each data sample. By default the code constructs the function 'lambda d: scale * (d-offset)', i.e. it calibrates the data by removing the offset an applying the scale.
• band = fmin, fmax - a low,high pair of frequencies within which to bandpass the data. Sketchy at best...
• ripple_db = X - the ripple in the stopband of the bandpass filter
• width = X - the width in the passband of the bandpass filter
• rms_average = X - number of seconds in a single RMS average (combine with band to make BLRMS)
• spectrum-segment-length = X - the length of FFT to use when calculating the spectrum, as a number of samples
• spectrum-overlap = X - the overlap (samples) between neighbouring FFTs when calculating the spectrum
• spectrum-time-step = X - the length (seconds) of a single median-mean average for the spectrogram

At the moment a package version issue means the spectrogram doesn't work, but the spectrum should. At the time of writing, to use the spectrum simple add 'plot-dataplot2'.

You can view the configuration file within the webpage via the 'About' link off any page.

Please e-mail any suggestions/complaints/praise to duncan.macleod@ligo.org.

The last of the control room machines is now upgraded.

Apparently the environment was not being properly inherited by the scripts launched from medmrun.  We modified the medmrum script so that it executes things with an interactive shell ("bash -i -c ...") and this fixed the problem (by assuring that it sources all the interactive environment configs (i.e. ~/.bashrc)).  I'm still not sure why we were seeing different behavior on pianosa, but at least the solution we have now should be robust.

As a reminder, all scripts launched from MEDM should use medmrun:

/opt/rtcds/caltech/c1/scripts/medmrun

I have setup a shared .bashrc for all the workstations that is symlinked to the normal location on all machines:

controls@rossa:~ 0$ ls -al /home/controls/.bashrc 
lrwxrwxrwx 1 controls controls 23 2012-05-25 15:37 /home/controls/.bashrc -> /users/controls/.bashrc
controls@rossa:~ 0$ 

This should help simplify maintenance considerably.  Editing that file on one machine will edit it for all.  Just edit this one file!  Don't try to get fancy and add extra files!

I also added a bunch of aliases that had previously been missing.  This should help with some of the problems that people had been having.

NOTE: PLEASE DO NOT CHANGE THE DEFAULT SHELL!  We are using bash, because that's what the sites are now using and we want to be as compatible as possible.

You can of course still write scripts in csh/tcsh or use tcsh in a shell if you wish.   Just don't change the default shell for the controls user.

ssh -X pianosa

On pianosa

StripTool PSL.strip&
StripTool IOO.strip&
StripTool seismic.strip&

AA IN -> COIL DRIVER IN transfer function for MC3

I've provided excitation to the AA input, the same for all OSEM channels. In the digital domain coherence between C1:SUS-MC3_ULSEN_INMON / C1:SUS-MC3_ULCOIL_INMON and other channels OSEM -> COIL is 1 starting from 0.1Hz.

The only thing left to understand is why the coherence AA IN / COIL DRIVER IN measured in the analog domain is not 1 in the frequency range 0.1 - 1 Hz. It does not look like just SRS noise. I've connected Ch 1 and 2 to the source, coherence is close to 1.

I've terminated input to AA filters and measured signal to coils C1:SUS-MC3_??COIL_OUT.

I compared this noise to the signal when OSEM are connected to ADC.

I made BNC -> LEMO board such that all LEMOs have the same signal equal to BNC signal. I provided excitation of 50 mV as white noise to the input of the AA filter and measured coherence between excitation and MC3 coil driver. The path is

AA -> ICS 110 -> Pentium -> Pentek -> AI -> Univ Dewhitening -> Coil Driver

As all inputs have the same signal, matrices that recombine the signals should not affect coherence. But what I got for coherence between AA IN / Dewhitening OUT is

[Yuta, Suresh]

We found that the MC was not locking and that the alignment between PSL and MC was too poor to obtain a TEM00 mode in the MC.   To correct the situation we went through the following steps:

1) We burt restored the MC alignment slider values to their values at 3:07 AM of today

2) We turned off the MC-autolocker and the ASC signal to the coils.   Then aligned the PSL beam into the MC (with the MC servo loop off) to obtain the TEM00 mode.  We had to adjust the zig-zag at the PSL output by quite a bit to maximise MC transmission.

3) We then centered the spot on the MC2 face and centered the transmitted beam on the MC2_TRANS_QPD

4) Next, we centered the beams on the MC_WFS sensors.

5) Turning on the WFS loops after this showed that everything works fine and WFS loops do not accumulate large offsets.

3 strip charts monitoring on 24 hours time scale: Vac,  PSL-IFO,  SUS and 10 channel video monitoring inside - outside  of 40m lab

[Den, Yuta]

Background:
 ASS and many other scripts don't work on new ubuntu machines.

What we did:
1. Installed C-shell on rossa and rosalba(Ubuntu machine).
  sudo apt-get insall csh

2. Find out that
  /opt/rtcds/caltech/c1/scripts/AutoDither/alignY

runs, but
  /opt/rtcds/caltech/c1/scripts/medmrun /opt/rtcds/caltech/c1/scripts/AutoDither/alignY

doesn't run. It gives us the following error messages.

ezcawrite: error while loading shared libraries: libca.so: cannot open shared object file: No such file or directory
ezcaswitch: error while loading shared libraries: libca.so: cannot open shared object file: No such file or directory

Result:
 ASS scripts run on rossa and rosalba, but not with medmrun.
 At least ASS scripts run on pianosa(ubuntu machine) with medmrun. So we decided to wait for JAMIE to fix it.

   Here is the suggested layout of the MC health check web page layout. I will update the Omnigraffle file as people comment and suggest changes.  If you want the file let me know.

Top tab categolies:

• Summary
• CDS
  • CDS Status
• PEM
  • Seismic 24h trend
  • Accoustic 24h trend
  • Weather/Temp/Barometer/etc 24h trend
• PSL/IOO
  • PSL summary trend / duty ratio
  • IOO summary (MC Health Check/IOO QPD trends / IFO QPD trends / Transmon QPD trends) duty ratio
• SUS
  • Summary
  • OSEM PSD/trend
  • OPLEV PSD/trend
• IFO
  • DC Mon
  • RF ports
  • OMC
• Steve
  • Vacuum
• Misc.

IFO

• DC Monitors
  • Incident beam power trend (24h)
  • AS/REFL/POP/TRX/TRY bean power trend (24h)
  • AS/POP RF beam power trend (24h)
• RF port
  • DARM sensitivity PSD (mean/min/max/reference) for an hour
  • DARM/CARM/PRCL/MICH/SRCL PSD
  • DARM/CARM/PRCL/MICH/SRCL (freq vs Gaussianity)
  • DARM/CARM/PRCL/MICH/SRCL calibration trend
• OMC
  • TBD

HEPA filter was running at 90% of max. I reduced it to 20%. Acoustic noise moved down

The range of MCL oscillations has also decreased but fluctuations in the frequency range 10-100 are still present.

MCL is much more stable now.

The main page of connection error monitor can be a scheme of computers and models with connections. If there is an error in connection, the corresponding arrows turns from green to red.

Each arrow is a line to a more detailed information about the channels.

 The PMC  behavior is not changed.

Mic in the PSL showed that fluctuations in the MCL in the frequency range 10 - 100 Hz are due to acoustic noise. I've measured MCL, MCL / PSL mic coherence 2 times with interval 300 seconds.

Surprisingly, acoustic noise level did not change but MC sometimes is more sensitive to acoustic noise, sometimes less.

 I wrote auto-locker for PMC. It is called autolocker_pmc, located in the scripts directory, svn commited. I connected it to the channel C1:PSL-PMC_LOCK.  It is currently running on rosalba. MC autolocker runs on op340m, but I could not execute the script on that machine

op340m:scripts>./autolock_pmc
./autolock_pmc: Stale NFS file handle.

I did several tests, usually, the script locks PMC is a few seconds. However, if PMC DC output has been drift significantly, if might take longer as discussed below.

The algorithm:

       if autolocker if enabled, monitor PSL-PMC_PMCTRANSPD channel
       if TRANS is less then 0.4, start locking:
               disengage PMC servo by enabling PMC TEST 1
               change PSL-PMC_RAMP unless TRANS is higher then 0.4 (*)
               engage PMC servo by disabling PMC TEST 1
       else sleep for 1 sec
 

(*) is tricky. If RAMP (DC offset) is specified then TRANS will be oscillating in the range ( TRANS_MIN, TRANS_MAX ). We are interested only in the TRANS_MAX. To make sure, we estimate it right, TRANS channel is read 10 times and the maximum value is chosen. This works good.

Next problem is to find the proper range and step to vary DC offset RAMP. Of coarse, we can choose the maximum range (-7, 0) and minimum step 0.0001, but it will take too long to find the proper DC offset. For that reason autolocker tries to find a resonance close to the previous DC offset in the range (RAMP_OLD - delta, RAMP_OLD + delta), initial delta is 0.03 and step is 0.003. It resonance is not found in this region, then delta is multiplied by a factor of 2 and so on. During this process RAMP range is controlled not to be wider then (-7, 0).

The might be a better way to do this. For example, use the gradient descent algorithm and control the step adaptively. I'll do that if this realization will be too slow.

I've disabled autolocker_pmc for the night.

    The only script that can currently take this action is the MC autolocker.  If that is disabled first and the PMC unlocks later, the WFS will not be turned off.  During the last round of discussions we had about the autolocker script, sometime last Nov, we decided that too much automation is not desirable and that the autolocker should be kept as simple as possible.

 [Koji, Suresh]

  We tried to locate the sixteen analog output channels we need to control the four tip-tilts (four coils on each).  We have only 8 available channels on the C1SUS machine. 

  So we will have to plug-in a new DAC output card on one of the machines and it would be logical to do that on the C1IOO machine as the active tip-tilts are conceptually part of the IOO sub-system.   We have to procure this card if we do not already have it.  We have to make an interface between this card output and a front panel on the 1X2 rack.  We may have to move some of the sub-racks on the 1X2 rack to accommodate this front panel.

  We checked out the availability of cards (De-whitening, Anti-imaging, SOS coil drivers)  yesterday.  In summary: we have all the cards we need (and some spares too).  As the De-whitening and Anti-imaging cards each have 8 channels, we need only two of each to address the sixteen channels.  And we need four of the SOS coil drivers, one for each tip-tilt.  There are 9 slots available on the C1IOO satellite expansion chassis (1X1 rack), where these eight cards could be accommodated.

  There are two 25 pin feed-thoughs, where the PZT drive signals currently enter the BS chamber.  We will have to route the SOS coil driver outputs to these two feed-throughs. 

   Inside the BS chamber, there are cables which carry the PZT signals from the chamber wall to the the table top, where they are anchored to a post (L- bracket).  We need a 25-pin-to-25-pin cable (~2m length) to go from the post to the tip-tilt (one for each tip-tilt).  And then, of course, we need quadrapus cables (requested from Rich) which fit inside each tip-tilt to go to the BOSEMs.

   I am summarising it all here to give an overview of the work involved.

PRIORITY ITEMS:

Align Ygreen beam - JENNE, YUTA

Arm cavity sweeps, mode scan - JENNE, YUTA

ASS doesn't run on Ubuntu! or CentOS Fix it! - YUTA, JENNE, JAMIE's help

Input matricies, output filters to tune SUS.  check after upgrade. - JENNE

POX11 whitening is not toggling the analog whitening??? - JAMIE, JENNE, KOJI

Decide on plots for 40m Summary page - DEN, STEVE, JENNE, KOJI, JAMIE, YUTA, SURESH, RANA, DUNCAN from Cardiff/AEI

 Look into PMC PZT drift - PZT failing? Real MC length change? - JENNE, KOJI, YUTA

THE FULL LIST:

• General
  • Revamp control room - more monitors, maybe move TV shelves. - JENNE
  • Audio system for the signals!!!! Even a crappy one! - LEO
• SUS
  
  • Input matricies, output filters to tune SUS.  check after upgrade. - JENNE
• IFO
  • Fix occasional common-mode power transient in the arm transmissions. Probably an alignment thing. Would ISS help? - MIKEJ?
  • Drift of the green incident axis -> Assess the amount of the drift / replace the mount - JENNE, KOJI
  • Calibration of POP22 / AS110 - JENNE
  • PMC/IMC/ARM characterization (loss, finesse, reflectivity, etc) - JENNE
  • Align green beam - JENNE, YUTA
    
  • Arm cavity sweeps, mode scan - JENNE, YUTA
    
  • Align AS OSA (others?) - JENNE  
  • Investigate PRMI glitches, instability - JENNE
  • PZT or Picomotor mounts for PSL/ALS beams - WHO??
  • ALS on the both arm simultaneously / common / diff ALS scripts - JENNE
• CDS
  • Capture OSA signals in CDS (the 'scope TDS1001B has a USB port in the back for connecting to the computer) - WHO??
  • Transmon (arms) for high and low power - WHO??
  • POX11 whitening is not toggling the analog whitening??? - JAMIE, JENNE, KOJI
  • Install guardians to monitor EPICS values - WHO??
• Electronics
  • Actuator noise level characterization (coil driver response in V/m & coil driver noise level V/rtHz) - WHO??
  • Beat box - KOJI
  • I/Q DFD - WHO??
  • Improvement of POP22/110/AS110 RF circuits. - WHO??
• MEDM
  
  • Complete 40m overview screen - everything should be clickable with pseudo 3D icons - JENNE
  • Better suspension screen - copy from sites. - WHO??
  • Script to generate a MEDM tree - WHO??
  • Resurrect MEDM snapshots - WHO??
  • New ! buttons on every screen, include wiki page - WHO??
  • Screen for errors in signal transmission between models - DEN
• SCRIPT
  • Locking scripts with integrator triggers / disabling when unlocked - JENNE
  • Daily diagnosis of the MC spot positions (there must be something already...) - SURESH?
  • Daily/occasional adjustment of the incident axis on the MC - SURESH?
  • IFO_CONFIGURE scripts still do a burt restore, so step the optics.  Need to remove optic alignment from config .snap files, use reg restore script instead. - JENNE
    
  • OPLEV/OSEM trending script before the IFO work for diagnosis. Put into 40m summary screen. - JENNE, DUNCAN from Cardiff/AEI
    
  • Auto-locker for arms - JENNE
  • Auto-locker for PMC, PSL things - DEN
  • Diagnostic script for CDS - mx_stream, other stuff. - WHO??
• Video
  • If each video screen has a caption, that would be great - WHO??
  • GUI interface of "videoswitch" - MIKEJ
  • Mouse Jiggler for Zita (called Swinput?) - JENNE
• Ubuntu vs. CentOS
  • burttoday is not aliased in ubuntu.    burttoday:      aliased to cd /opt/rtcds/caltech/c1/burt/autoburt/today/ - JAMIE

  • Upgrade Allegra, make sure connect to DTT, Dataviewer, AWG. - JAMIE
    
  • ASS doesn't run on Ubuntu! or CentOS Fix it! - JENNE, JAMIE's help
  • CentOS machines cannot open simulink models properly (get "Bad Link"s everywhere, so you can't do anything useful) - JAMIE
• MM
  • IPPOS beam measurement - SURESH with JENNE
  • AS beam measurement (if beam is bright enough) - SURESH and JENNE
  • Mode matching calculations, sensitivity to MC waist measurement errors, PRM position - JENNE
  • Think up diagnostic measurement to determine mode matching to PRC while chambers are open, while we tweak MMT - JAMIE, JENNE, KOJI, SURESH
  • Use sensoray to capture, measure beam mode at AS, POP - YUTA
• Stray Light
  • Scattered light measurement at the end stations: design / confirmation of the mechanical parts/optics/cameras - JAN
  • Align AUX laser into dark port - KOJI, YUTA
    
• OAF
  • OAF comparison plot, both online and offline, comparing static, adaptive and static+adaptive - DEN
  • Static-only OAF noise budget (Adaptive noise budget as next step) - DEN
  • Script for daily / weekly re-calculation of Wiener, post to elog if need changing - DEN
    
• Tip Tilts
  • Prepare electronics for TTs (coil drivers) - JAMIE
  • In-air TT testing to confirm we can control / move TTs before we vent - SURESH
  • Connect TTs to digital system and controls, lay cables if needed - JAMIE with SURESH
• RF Photodiodes
  • Opto Energy diode laser - purchase - ERICG
  • Purchase fibers, splitters, other supplies - ERICG
  • Set everything up - ERICG

New self checking emergency back up lights were installed at 13 locations in the 40m lab.

I've put 5 EM172 microphones close together and measured there signal and coherence. They are plugged in to accelerometer channels.

Then I've suspended microphones around the MC - 2 at MC2, 2 at MC1,3 and 1 at PSL. The amplifier box is above STS readout box.

Microphone close to PSL gave a strong coherence with MC_F, as we already saw it using Blue Bird Microphone.

ACC_MC2_XY channels <=> MC2 microphones

ACC_MC1_XY channels <=> MC1,3 microphones

ACC_MC1_Z channel <=> PSL microphones

I fixed the problem Jamie pointed out in elog #6657 and #6659.

What I did:
1. Created the following template files in /opt/rtcds/userapps/trunk/sus/c1/medm/templates/ directry.

SUS_SINGLE_LOCKIN1.adl
SUS_SINGLE_LOCKIN2.adl
SUS_SINGLE_LOCKIN_INMTRX.adl
SUS_SINGLE_OPTLEV_SERVO.adl
SUS_SINGLE_PITCH.adl
SUS_SINGLE_POSITION.adl
SUS_SINGLE_SUSSIDE.adl
SUS_SINGLE_TO_COIL_MASTER.adl
SUS_SINGLE_COIL.adl
SUS_SINGLE_YAW.adl
SUS_SINGLE_INMATRIX_MASTER.adl
SUS_SINGLE_INPUT.adl
SUS_SINGLE_TO_COIL_X_X.adl
SUS_SINGLE_OPTLEV_IN.adl
SUS_SINGLE_OLMATRIX_MASTER.adl

To open these files, you have to define $(OPTIC) and $(DCU_ID).
For SUS_SINGLE_TO_COIL_X_X.adl, you also have to define $(FILTER_NUMBER), too. See SUS_SINGLE_TO_COIL_MASTER.adl.

2. Fixed the following screens so that they open SUS_SINGLE.adl.

C1SUS_WATCHDOGS.adl
C1IOO_MC_ALIGN.adl
C1IOO_WFS_MASTER.adl
C1IFO_ALIGN.adl

Now same as pianosa and rosalba.  I'll upgrade allegra on Friday.

I've created transmission error monitors in rfm, oaf, sus, lsc, scx, scy and ioo models. I tried to get data from every channel transmitted through PCIE and RFM. I also included some shared memory channels.

The medm screen is in the EF STATUS -> TEM. It shows 16384 for the channels that come from simulation plant. Others are 0, that's fine.

I just sat down in the control room, and discovered the PMC (and everything else) unlocked.  I relocked the PMC, but the MC wasn't coming back.  After a moment of looking around, I discovered that the WFS were on, and railing.  I ran the "turn WFS off" script, and the MC came back right away, and the WFS came on as they should.

We need to relook at the WFS script, or the MC down script, to make sure that any time the MC is unlocked, no matter why it unlocked, the WFS output is off and the filter histories are cleared.

Actually, it looks like we're not quite done here.  All the paths in the SUS_SINGLE screen need to be updated to reflect the move.  We should probably make a macro that points to /opt/rtcds/caltech/c1/screens, and update all the paths accordingly.

Hey, folks.  Please remember to commit all changes to the SVN in a timely manor.  If you don't, multiple commits will get lumped together and we won't have a good log of the changes we're making.  You might also end up just loosing all of your work.  SVN COMMIT when you're done!  But please don't commit broken or untested code.

pianosa:release 0> svn status | grep -v '^?'
M       cds/c1/models/c1rfm.mdl
M       sus/c1/models/c1mcs.mdl
M       sus/c1/models/c1scx.mdl
M       sus/c1/models/c1scy.mdl
M       isc/c1/models/c1lsc.mdl
M       isc/c1/models/c1pem.mdl
M       isc/c1/models/c1ioo.mdl
M       isc/c1/models/ADAPT_XFCODE_MCL.c
M       isc/c1/models/c1oaf.mdl
M       isc/c1/models/c1gcv.mdl
M       isc/common/medm/OAF_OVERVIEW.adl
M       isc/common/medm/OAF_DOF_BLRMS.adl
M       isc/common/medm/OAF_OVERVIEW_BAK.adl
M       isc/common/medm/OAF_ADAPTATION_MICH.adl
pianosa:release 0>

Very nice, Yuta!  Don't forget to commit your changes to the SVN.  I took the liberty of doing that for you.  I also tweaked the file a bit, so we don't have to specify IFO and SYS, since those aren't going to ever change.  So the arguments are now only: OPTIC=MC1,DCU_ID=36.  I updated the sitemap accordingly.

Yuta, if you could go ahead and modify the calls to these screens in other places that would be great.  The WATCHDOG, LSC_OVERVIEW, MC_ALIGN screens are ones that immediately come to mind.

And also feel free to make cool new ones.  We could try to make simplified version of the suspension screens now being used at the sites, which are quite nice.

 Yesterday I swapped in new He/Ne laser with output power 3.5 mW  The return spot on qpd is large ~6mm in diameter and 20,500 counts

The spot size reduction require similar layout as ETMX oplev.

I've started to create channels and an medm screen to monitor the errors that occur during the transmission through the RFM model. The screen will show the amount of lost data per second for each channel.

Not all channels are ready yet. For created channels, number of errors is 0, this is good.

Background:
 We need more organized MEDM screens. Let's use macro.

What I did:
1. Edited /opt/rtcds/userapps/trunk/sus/c1/medm/templates/SUS_SINGLE.adl using replacements below;

sed -i s/#IFO#SUS_#PART_NAME#/'$(IFO)$(SYS)_$(OPTIC)'/g SUS_SINGLE.adl
sed -i s/#IFO#SUS#_#PART_NAME#/'$(IFO)$(SYS)_$(OPTIC)'/g SUS_SINGLE.adl
sed -i s/#IFO#:FEC-#DCU_ID#/'$(IFO):FEC-$(DCU_ID)'/g SUS_SINGLE.adl
sed -i s/#CHANNEL#/'$(IFO):$(SYS)-$(OPTIC)'/g SUS_SINGLE.adl
sed -i s/#PART_NAME#/'$(OPTIC)'/g SUS_SINGLE.adl

2. Edited sitemap.adl so that they open SUS_SINGLE.adl with arguments like
    IFO=C1,SYS=SUS,OPTIC=MC1,DCU_ID=36
instead of opening ./c1mcs/C1SUS_MC1.adl.

3. I also fixed white blocks in the LOCKIN part.

Result:
  Now you don't have to generate every suspension screens. Just edit SUS_SIGNLE.adl.

Things to do:
 - fix every other MEDM screens which open suspension screens, so that they open SUS_SINGLE.adl
 - make SUS_SINGLE.adl more cool

I rebooted rossa and the X sever has stalled.

I locked the PMC and the MC followed instantly.

I've soldered EM172 microphones to BNC connectors to get data from them.

Then I've build an amplifier for them. The circuit is

I've build 6 such circuits inside 1 box. It needs +15 V to A3 and GND to A2. A1 power channel is not used.

LISO model for this scheme was created and simulation results were compared to measurement of each channel

Measured noise curve (green) is the SR785 own noise.

 The uncoated bi-concave lens was replaced by AR coated one: KBC 037 -100 AR.14 resulting 35% count increase on qpd

 The typical sign of a dying gas laser is that it glows for a few minutes only. The power supplies are fine.

Two new  JDS - Uniphase 1103P lasers ( NT64-104 )  arriving on Monday, May 21

 Aluminum posts and SS clamps for green glass traps in vacuum will be out of the shops by June 6, 2012 the latest

Guralp 1  is on the south side of IOO chamber

 This is totally cool!  You can see that the OSEM lights are almost entirely gone in the subtracted image.

Can you switch to trying with one of the *TM*F cameras?  (ITMXF, ITMYF, ETMYF, ETMXF)  They tend to have more background, so there should be a more dramatic subtraction.  Den or Suresh should be able to lock one of the arms for you.

I acquired 2 raw frames of MC2 using "/users/mjenson/sensoray/sdk_2253_1.2.2_linux/capture -n -s 720x480 -f 1", one while the laser was off the mode cleaner and another while it was on:

I then used "/users/mjenson/sensoray/sdk_2253_1.2.2_linux/imsub/display-image.py" to generate bitmaps of the raw images, which I then subtracted using the Python Imaging Library to generate a new image:

It doesn't look all that different, but the first image didn't have that much lit up in it to begin with. I should be able to write a script that does all of this without needing to generate new files in between acquisition and subtraction.

ETMX sus damping restored

ETMY sus damping restored.

I've compared offline Wiener filtering with online static + adaptive filtering for MC_F with GUR1_XYZ and GUR2_XYZ as witness signals

Note: online filter works up to 32 Hz (AI filter at 32 Hz is used). There is no subtraction up from this frequency, just MC_F was measured in different times for online and offline filtering. This difference in MC_F in frequency range 20-100 Hz showed up again as before with microphone testing.  One can see it in 1 minute. Smth is noisy.

Reasons why online filter is worse then offline:

1. FIR -> IIR conversion produces error. Now I'm using VECTFIT approximation with 16 poles (splitting into 2 filter banks), this not enough. I tried to use 50 and split them into 5 filter banks, but this scheme is not working: zpk -> sos conversion produces error and the result filter works completely wrong.

2. Actuator TF. VECTFIT works very good here - we have only 1 resonance. However, it should be measured precisely.

3. Account for AA and AI filters that rotate the phase at 1-10 Hz by ~ 10 degrees.