ISS first loop was all over the place as was the diffracted power at the beginning of my shift.  A slight tweak in the less negative direction set it back to stable. Further adjustment got it back to ~7:5% diff power at 2.04V refsignal. Perhaps more attention can be given to ISS on a daily basis by the operator on shift until a better solution can be implemented. 

https://alog.ligo-wa.caltech.edu/aLOG/index.php?callRep=13781

Based on the TCSX central heating calibration (62.3 micro-diopters single-pass per Watt) and the calculated static lens of -80213m, we require:

+201mW of central heating on ITMX to correct this static lens.

Edited 31-Oct-2014: this isn't correct because of an error in the laser power calibration

Daniel, Dave

We have stopped the following CSD guardian nodes from running. They can be restarted at a future date if needed.

If we choose to restart these, they should be generically renamed (dropping the H1 in the name)

K. Venkateswara

I've attached ASD and coherence plots from 40k seconds of data from BRS/T240 and the super sensor from last night. Wind speeds were in the 5-10 mph range. This time, I showed the raw signals coming out from BRS and the T240 X instead of showing the output of the filters. I've also shown the ref. mirror and the output of the super-sensor.

BRS has much larger noise below 2-3 mHz, than the T240, even though the sensor noise appears to be much less. It was interesting to me that it had a similar shape as the ref. mirror output and there does appear to be some coherence between the two. Temperature is the usual suspect at these frequencies. A sensitive temperature sensor on the BRS platform would be useful in diagnosing this noise.

The current cdsutils installation (r361) has a new and improved NDS avg() function.  The previous version was buggy, was calculating the standard deviation incorrectly,  and had a clunky interface.  This new version fixes those issues:

fixes to standard deviation calculation

The standard deviation was previously being calculated incorrectly and the returned values were wrong (off by some unknown but kind of large factor).  The new version uses the python numpy.var() function to calculate the variance, from which the standard deviation is calculated.  It has been verified to be correct.

channel IFO prefixes no longer need to be specified

Previously, the avg() function required full channel names, with IFO prefixes.  This new version works like the ezca interface whereby the IFO prefix can be left off of the channel name.  This makes things much cleaner, and allows scripts to be portable.  E.g., instead of:

cdsutils.avg(2, IFO+':LSC-DARM_OUT')

just do:

cdsutils.avg(2, 'LSC-DARM_OUT')

new format for returned values

Probably the thing that's going to cause the most trouble is that the interface to the function has been fixed up.  Previously, the function was returning a dictionary of channel:avg key pairs.  This was very clunky to use.

The return value of the function now mirrors the input argument.  So for instance, if a single channel is requested, a single avg value is returned.  If a list of channels is requested, a list of average values is returned, in the same order as the input channel list.  So calls like:

avg = cdsutils.avg(2, 'LSC-DARM_OUT').values()[0]

can now just be:

avg = cdsutils.avg(2, 'LSC-DARM_OUT')

If the stddev option is provided, the output will be an (avg, stddev) tuple, or if multiple channels is requested, a list of such tuples, e.g.:

avg, stddev = cdsutils.avg(2, 'LSC-DARM_OUT', True)

I have fixed all calls to cdsutil.avg() that I could find in the USERAPPS/release.  I likely didn't catch everything, though, so be aware of the new interface and update your code appropriately.

After the recent upgrades, a couple of small bugs were identified in guardian and cdsutils, and new versions were pushed out:

• guardian r1102: fix bug is reload with NodeManagers, guardctrl allow restarting stopped nodes, new log viewer (see below)
• cdsutils r361: fix bugs in new avg() function (see followup log)

The new version have been pushed, and some of the guardian nodes have been restarted, but not all.  We should restart all nodes at the next opportunity.

New log viewer

I pushed out a new guardian node log viewing interface, so that you no longer need to ever type in a password when viewing logs.  This new interface can be used by using the new guardlog program that is now installed everywhere.  Just provide as arguments to the program the names of the nodes whose logs you would like to view, e.g.:

guardlog SEI_ITMY HPI_ITMY ISI_ITMY_ST1 ISI_ITMY_ST2

The logs of all specified nodes will be tailed, interleved as they are spit out, to the current terminal.  The GUARD medm control interfaces now use this log viewer as well.

tl;dr: A very lightweight "guardlog" server is now running on the guardian machine (h1guardian0), listening on port 5555.  Making a simple TCP connection to that port (with the guardlog client) will open up the interface and spit out the logs for the specified nodes.

J. Kissel

Another data point on the issue of IPC timing causing errors between the LSC model and QUAD models -- Stuart and I added 1 (one) RFM IPC sender to the LSC and 1 (one) RFM PC receiver to each of the ETM models for DARM-sensed, violin mode damping on Tuesday morning (see LHO aLOG 14657). This appears to have increased the ETM model's CPU_METER by ~1 [us], and made no change to the random-time computation time jumps up by as much as ~5-6 [us]. Surprisingly, it *decreased* the LSC model's average compute time by ~ 1 [us], but again also did not affect the timing jumps as high as an extra 7-9 [us].

I attach a 7 day, minute trend. The only discrete jump in the trend is when the models were restarted around 2014-10-28 14:15 UTC (or Tuesday 2014-10-28 07:15 PDT).

I noticed that the DARM Error damping display on the QUAD MEDM Overview screen was showing the incorrect channel information. So I substituted them for the correct channels (H1:SUS-ITMY_L2_DAMP_MODE1_OUTPUT, H1:SUS-ITMY_L2_DAMP_MODE2_OUTPUT etc.) and committed the fixed screen to the userapps svn, as follows:-

/opt/rtcds/userapps/release/sus/common/medm/quad/
M        SUS_CUST_QUAD_OVERVIEW.adl

This will need to be svn'd up at LLO too.

Between approximately 10:07 AM PT and 10:16 AM PT the network upstream of LHO had some routing changes or outage that caused a temporary loss of connectivity to the Internet past PNNL/ESnet.

Bubba, John,

In order to compensate for the cooler weather we have turned on two LVEA heaters at ~ 09:40 local

HC1A  is  set to 15ma (two stages) - it appears that the first stage is open circuit.

HC2b is set to 9ma (one stage).

There will be a minor impact on LVEA temperatures.

At Peter Fritschel's request, I have extracted lists of science and commissioning channels, as a follow-up to the frame rate studies ( see aLOG 14718 ).  I modified my existing script to extract the names (see attached scichannels_script.txt).  As a reminder 'acquire=1' means commissioning only, 'acquire=3' means science and commissioning frames.

The list of science frame channels is 'h1_sci_channels.txt'.  The list of commissioning frame-only channels is 'h1_comm_channels.txt'.  Each list has a channel and its rate.

Kyle Ryan, R. Weiss
Running the ionizer on purge gas air solves the problem of unequal positive and negative
ion currents in the gas being used to discharge the test masses. The oxygen which has
known negative ion states provides the bulk of the negative ions. The ionizer was run for
2 hours with sampled + and - ion currents of 1.5e-9 Amps ( a factor of 100 more in the ion 
stream). Optical HR coating test samples and some VITON pieces were placed in the ion stream
to determine if the chemically reactive oxygen ions and ozone formed in the ionizer do damage. The
optical samples will be sent to Caltech for absorption tests.

The purge air system was turned off at 7:10PM last night.

The 4.5 hour heating test last night on ITMX was successful. The initial thermal lens transient is shown in the attached plot.

The thermal lens forms relatively rapidly in response to the CO2 heating. Then it decays at the same rate when the heating is turned off. Once again, Physics works.

When the offset in the spherical power at t = 0s is accounted for, the thermal lens magnitude is approximately 80 micro-diopters (double-passed) for 680mW of applied CO2 laser power.

Further analysis on the shape and centering of the lens is pending ...

(The noise in the HWS measurement in the last half hour is coming from SUS injections into ITMX).

model restarts logged for Wed 29/Oct/2014
2014_10_29 10:31 h1fw1

unexpected restart of h1fw1

Posting some more details on the parameter changes from the model fitting of H1SR2 discussed in 10124.

Some plots showing measured M3 length to pitch coupling against this model and the original model are also attached. The coherence is pretty poor in this data, so it is difficult to draw concolusions on which model is the better predictor of this coupling.

Parameters  |      units        |         old model       |        H1SR2 fit         |      difference       |      percent difference


 'I1x'   | kgm^2    [   0.0213]    [   0.01994]    [ -0.0013599]    '-6.38%'  

 'I1y'   | kgm^2    [   0.0025]    [ 0.0027219]    [ 0.00022193]    '8.88%'   

 'I1z'   | kgm^2    [   0.0216]    [  0.020356]    [ -0.0012436]    '-5.76%'  

 'm2'    | kg       [    2.983]    [     2.985]    [      0.002]    '0.067%'  

 'I2x'   | kgm^2    [  0.00889]    [ 0.0084199]    [-0.00047015]    '-5.29%'  

 'I2y'   | kgm^2    [  0.00531]    [ 0.0050135]    [-0.00029646]    '-5.58%'  

 'I2z'   | kgm^2    [  0.00635]    [ 0.0064319]    [ 8.1928e-05]    '1.29%'   

 'I3x'   | kgm^2    [  0.00832]    [ 0.0080117]    [-0.00030834]    '-3.71%'  

 'I3y'   | kgm^2    [   0.0054]    [ 0.0051465]    [-0.00025352]    '-4.69%'  

 'I3z'   | kgm^2    [  0.00557]    [ 0.0053901]    [-0.00017987]    '-3.23%'  

 'l1'    |  m       [    0.295]    [   0.30057]    [  0.0055655]    '1.89%'   

 'l2'    |  m       [    0.167]    [   0.17123]    [  0.0042327]    '2.53%'   

 'l3'    |  m       [     0.22]    [   0.22142]    [  0.0014169]    '0.644%'   

 'kc1'   | N/m      [    179.8]    [    182.45]    [     2.6509]    '1.47%'   

 'kc2'   | N/m      [   219.33]    [     212.9]    [    -6.4336]    '-2.93%'  

 'd4'    |  m       [    0.001]    [-0.0006798]    [ -0.0016798]    '-168%'   

 'flex1' |  m       [0.0019381]    [ 0.0019382]    [ 1.0483e-07]    '0.00541%'

Chris, Evan

We have implemented pitch damping by feeding the SR3 oplev back onto M2.

We used the HLTS model susPR3model.mat in NbSVN/aligonoisebudget/trunk/DRMI/L1/TransferFunctions to get a simplified, two-resonance model of the M2 pitch →M3 pitch plant:

• First resonance: f0 = 0.8 Hz, Q = 125
• Second resonance: f0 = 3.6 Hz, Q = 251
• (Also a small resonant wiggle aroung 0.6 Hz, but it doesn't seem to be so important.)

Then we added the following filters to foton:

• zpk([0],[100],1,"n")
• zpk([],[50;50;50],1,"n")
• zpk([0.045+i*3.6;0.045-i*3.6],[],1,"n")
• zpk([0.03;0.7],[0.141421+i*0.141421;0.141421-i*0.141421],1,"n")gain(0.525002)
• ellip("LowPass",4,2,40,15)

In the attached screenshot, you can see the expected OLTF (in foton) and the measured OLTF (in DTT).

Also in the attached screenshot, you can also see some spectra. Blue is no damping, Green is the existing M3 damping, and red is the new M2 damping. Brown is the control signal for the M2 damping. Evidently, amount of suppression is about the same for the two loops.

We suspect that the bump at 2.5 Hz or so (not to be confused with the suspension resonance at 3.6 Hz) is gain peaking in the loop. Some more optimization may be necessary. Additionally, we need to consider how much noise is being injected into the motion of PR3. We tried for a little while, but realized that (a) we need to get the calibration from counts to newton-meters in order to make sense of the control spectrum, and (b) we haven't yet formulated a noise requirement that the oplev loop must meet.

As requested by the seismic team,  I ran the script to configure the ETMX ISI to a test configuration at around 1:47:00 in UTC or 18:47:00 in PDT. I am leaving it in this configuration.

Alexa, Kiwamu,

In response to Keita's alog about the PR2 baffle, we took a peek at the PR2 baffle by opening some of the viewports on HAM3 and HAM2 spool.

Conclusions:

• The aperture hole on the baffle looks centered.
• The baffle in front of PR2 looks the right one.

(PR2 baffle check out)

We opened up a viewport on the East side of HAM3 which the leftmost one with an illuminator attached on. This was the only available viewport to open up. We removed the illuminator and looked at the baffle through the viewport. We confirmed that there was no cross bar structure on the side of the baffle unit as shown in the DCC document (D1000328). We could not see the top part of the baffle where it supposed to have a cross bar structure. We took some pictures and I attach them to this entry.

(Peek at the aperture position)

Then we tried a different zooming in the PR2 digital camera in order to have a better view so that we can determine if the aperture hole is in the middle of the baffle unit or not. With a help of flash light illuminating the PR2 baffle from the HAM2 East side viewport, we could clearly see the edge on both right and left sides of the unit as well as the edge of the aperture. It looked like the hole is centered with respect to the right and left edges of the unit. We took several pictures of it via the digital camera so that one can evaluate the position later if necessary.

(MC2 scraper baffle check out)

Then we opened up another viewport on the West side of HAM3 in order to see both MC2 and PR2 baffles. Though, the MC2 baffle was completely occulting the PR2 baffle and therefore we could not see it. We could still confirm that the MC2 baffle has a cross bar structure on the side as shown in the design document (D1000327).

[Jeff K, Stuart A]

Following work yesterday preparing QUAD model updates (see LHO aLOG entry 14645), we convened early this morning to rebuild, install and restart models. 

A detailed log of our activities follows:-

- Bring down the IMC to DOWN state via Guardian (no change to LSC model)
- Bring down QUADs to SAFE state via Guardian
- Bring down SEI to OFFLINE state via Guardian  
- Capture new safe BURT snapshots for h1lsc, h1susetmx, h1susetmy, h1susitmx and h1susitmx
- Made all QUADs
- Installed all QUADs
- Restarted all QUADs
- Svn-up updated QUAD MEDM screens
- Untripped all Watchdogs
- Restore QUAD alignments
- Restore SEIs to FULLY_ISOLATED via Guardian 
- Restore IMC to LOCKED via Guardian
- DAQ process restart at 14:29 (UTC)
- Update other SUS MEDM screens (see LLO aLOG entry 15004) 
- Cleaned errant IPC issues with diag reset on GDS TP screen
- Committed new safe BURT snapshots to svn

Summary of benefits:

This now makes damping of violin, bounce and roll modes possible via the the L2 (PUM) stage of all QUADs using DARM error. Other benefits include: ESD linearization, providing infrastructure for remote ESD activation and deactivation. Also, old Guardian infrastructure has been removed from the model and MEDM screen, with new Guardian embedded mini control-panel replacing them in the QUAD Overview MEDM screen (as well as for other Suspensions too)

This closes-out WP#4915.