Summary:

Jason worked on the PSL DBB in the morning and various commissioning activities have been going on during the day.  Have had it at DC Read Out for last few hours during the afternoon for ISS work.

If winds pick up, Jim asked Commissioners to give him a call to take the End Station ISIs to a certain state.

H1 Locking Notes:

After a lockloss, there were some FSS issues (resolved by toggling Autolocker).  Kiwamu also noticed an oscillation with the ISS Diffracted Power (on the plot on the ISS medm, the max/min/mean signals are all separated from each other by quite a bit).  To remedy this,

• Click on the "Manual Mode" button in the AUTOLOCK box.  
• Click the "ON" button (which turns off the INTegrator), and wait for oscillation to go away.
• Click the "ON+INT" to reenable the INTegrator.

Day's Activities

• 9:25 PSL Rotation Stage work; LSC PWR Scale changed from 1.8 to 50 during this measurement (Nutsinee)
• 9:30 DBB PSL work (Jason)
• ~9:45 H1 PSL trips & Jason begins recovery.
• ~10:30 PSL Rotation Stage measurement re-started (Nutsinee)
• 12:33 Measuring cable runs in the LVEA (Fil)
• 12:45 Large group of 3rd graders from Captain Gray Elementary visits the Control Room en masse
• 12:56 Checking PSL 3rd Loop electronics; multiple visits (Kiwamu)
• 13:11 CP3 overfill (Chandra)
• 14:00 ISS 3rd Loop work with H1 in DC Read Out (Kiwamu, Evan)
• 14:21 VAC rack photo-taking (Fil)
• ~15:00 Yakima Community College Tour on-site 

Since the new 64k to 16k decimation filter of RCG3.0.X has about 12us smaller delay for duotone, I changed two duotone scripts:

/ligo/svncommon/CalSVN/aligocalibration/trunk/Common/MatlabTools/timing/scienceFrameDuotone.m and scienceFrameDuotoneStat.m.

If you specify gps time larger than 1144501217 (Apr/12/2016 13:00:00 UTC) for L1, or 1146322817 (May/03/2016 15:00:00 UTC) for H1, the new decimation filter is used to assess the expected delay in ADC.

For O1 data (first attachment), the old scripts (left) and the new one (right) generate the same results except a negligible offset of 0.047us (first attachment). The difference comes from the fact that the decimation delay was hard coded in the old script.

I also confirmed that the scripts generate correct timing information that is consistent with that of O1 (second attachment right).

Ross, Tega 

We have been using the new h1omcpi and h1susetmxpi models to look at mechanical modes  in OMC DCPD which should be related to parmatetric instabilities. Only the OMC DCPDA is used as subtracting the A and B signals seemed to remove the lines from our spectrum i.e. they must be completely in phase with each other. This signal is being used instead of the QPD transmission signal as it has a much higher SNR for these modes.

Starting in the 64kHz h1omcpi model, the signal (H1:OMC-PI_DOWNCONV_DEMOD_SIG_IN1) is first down converted to DC using a local oscillator set at the frequency of the particular mechanical mode. The I and Q phase signals are then passed via PCIE to the 16kHz h1omc model where they are low passed with a 64Hz corner frequency, multiplexed and sent across to the 16kHz h1pemex model using RFM. The signals are then demuxed and sent to the 64kHz h1susetmxpi model. At this point these signals are low passed again to avoid imaging  and then upconverted back to the frequency of the mode. The I and Q phase signals are then summed which effectively leaves the original signal with a bandpass due to the lowpassed signal being upconverted (H1:SUS-ETMX_PI_OMC_UC1). We are then able to use our linetracking tool iwave to track the particular line you are interested in (H1:SUS-ETMX_PI_MODE_OUT). 

This was process was used to track a selection of lines around 15000 Hz which should be related to some of the mechanical modes. The hope is that we can now use the iwave tracked signals to damp these modes using ESD assuming we know what lines relate to each test mass. 

Quick conclusion:

Bad news: The further away the rotation stage has to travel, the less accurate the measured requested power becomes.

Good news: The uncertainty is within 1-3%.

Slightly more details:

• The first set of measurement I ran the random walk script to let the RS rotate between -25.4 and -19 degree (roughly 0 W and 3 W) 100 times. The result yields ~1% deviation at 3W.
• The second set of measurement I ran the same code to let the RS rotate between -25.4, -19, -7, and 20 degree (which correspond roughly to 0 W, 3 W, 20 W, and 55 W) 66 times (people needs the IFO back and this RS measurement is taking forever). The result yields 2-3% deviation of the mean. 
• Both measurement overlapped at 0W.
• ISS and FSS was locked during the time of measurement, IMC was left unlocked so it doesn't kick FSS. ISS integrator was off according to Jason. ISC_LOCK and LASER_PWR guardian nodes were paused.

Richard changed PID settings on CP 5 & 6 today. Current settings:

CP5
Gain: 7
Integral: 460
Set Pt: 90

CP6
Gain: 6
Integral: 360
Set Pt: 88

Set points are set lower than nominal 92% so PID experiments can continue Monday.

1:30pm local

1/2 turn open on LLCV bypass --> took 33:17 min. to overfill CP3. 

Raised LLCV from 20% to 21%.

Kiwamu, Darkhan,

We updated the ETMY L1 stage (UIM) compensation filters FM2, FM3, FM4, FM7, FM8, FM9 of ETMY_L1_ESDOUTF_{UL,LL,UR,LR} with zeros and poles more accurately fitted to the most recent measurements by Jeff K. from ER8 (LHO alogs 20846, 21283). We have not updated the acquisition circuit zero-pole pair, because the measurements do not include the response of this circuit (for details see LHO alog 21142).

We've also updated the ETMY L2 stage (PUM) compenstation filters FM1, FM2, FM3, FM6, FM7, FM8 of ETMY_L2_ESDOUTF_{UL,LL,UR,LR} to their fitted values (LHO alogs 20846, 21232).

Python scritps were used to load new vailes into the Foton file, the scripts are based on Kiwamu's script for updating filter in the L3 stage (ESD) (LHO alog 27150). The scripts are committed to CalSVN at

Runs/PreER9/H1/Scripts/SUS/setH1SUSETMY_UIMDriver_compensations.py
Runs/PreER9/H1/Scripts/SUS/setH1SUSETMY_PUMDriver_compensations.py

Notes for CAL FOLKS:

• UIM and PUM filter replicas in CAL-CS model have not been updated accordingly at the moment;
• The extra compensations (for imperfect front-end filters) in the Matlab DARM calibration model are not necessary anymore, must be removed from the model.

I checked the output of the HWS vs the expected thermal lens from the online simulation code. The results are posted below. As you can see the time series agree very well with each other, certainly within the error bars of the HWS measurement ... at least just looking in dataviewer. (I rescaled the time series from diopters into micro-diopters and reset the HWS value to match the SIM value at t=0).

The HWS measurement is double-passed through the lens and while the simulation predicts the single-pass value: hence a factor of 2 difference between them.

The HWSY data is extremely noisy and shows almost no correlation with the simluation data.

The circulation fan on the staging building chiller is broken. The bearing support on the drive side has fractured due to metal fatigue. The circulation fan on this unit has been an ongoing issue for some time because of a poor design originally. I have removed the fan and the part of the housing that supports the above mentioned bearing.
This fan typically runs continually to ensure a positive pressure in the staging building. I have the booster fan running so there is still adequate positive pressure in the building. The AAON unit is running and keeping the building at a reasonable temperature given the current outdoor conditions.

One of the two condenser fans has also stopped operating.

This chiller only affects the assembly area and the upstairs area excluding the mezzanine lab.  

Tega, Ross, Dave:

We rebuilt and restarted h1susitmpi and h1susetmxpi models. They now use the iwave light function in IWAVE.c to see if some CPU time can be recovered.  We found that h1susitmpi is still running long (12-17uS) when the code is unbypassed for all 16 nodes. Tega is looking to see if parts can be removed from the model, and we'll also test this on a faster computer on the DTS.

I made a new version of the Matlab iopdownsamplingfilters.m script for use by the calibration group to apply the RCGv3.0.2 digital AA filter. The new file for use is stored at:

/ligo/svncommon/CalSVN/aligocalibration/trunk/Runs/O2/DARMmodel/Scripts/iopdownsamplingfilters.m

Minor adjustments were made to the h1dustlvea EPICS database file to try to solve some oddities in the raw count channels.  The h1dustlvea IOC was restarted several times, we are done for now and it should run over the weekend.

Also killed the h1dustpsl IOC as it's no longer connected to dust monitors.  The PSL dust monitors were connected to the LVEA network last week, and are now controlled by the h1dustlvea IOC.

I also uncommented TCS related lines in DOWN (Ln 417, 418) and COIL_DRIVERS (ln 2755, Ln 2756)

During the wind storms this week I collected data with a second STS at locations around the BRS and the GND STS that gets corrected for tilt, ranging from a huddle between the two STSs at 47cm apart to a maximum separation of 550 cm. For each location I found a period of the storm during which the average over 1664 seconds was close to 17 MPH. The figures show data only for these 17 MPH periods. I checked that in addition to averages within ½ MPH of 17, the extremes for each period were within a few MPH of each other.   

Figure 1 shows the coherences between the two STSs (top plot) as well as the spectra when the movable one was closest or furthest from the wall (bottom plot). Orange, red, blue, black and thin black traces are for increasing separation. The coherence tends to drop with distance and drops as low as 0.75 at the two sites at 2.08 and 2.54 meters, blue and black. The spectra in the lower plot show that the tilt near the wall (dotted thick black) is more than twice the tilt only 2.54 m away (black). The thin black dotted line is for the furthest location from the wall, near the far pier of the BSC, and its tilt is about half of that at the BRS. The trend for greater tilts at sites closer to the wall is consistent. A better location for the BRS and the BRS-corrected STS might have been on the opposite side of the beam tube from the wall.

The top plot of figure 2 shows coherence between the BRS and each of the two seismometers. The best coherence that I got was for the red site, as close as possible and centered on the BRS. This red dotted coherence is better than the solid red coherence for the GND STS, taken at the same time. The coherence near the bases of the near and far piers was remarkably poor. This may explain why using the BRS to correct the chamber rather than the seismometer, such as BRS RX to ISI RX, would not be very successful.

The bottom plot of figure 2 shows the coherence between the Z-axes of the GND STS and the moveable STS. I include this because the effect of tilt on the Z axis is much less than on the horizontal axes so it tends to show the coherence lengths for the real displacements that we want to subtract using a seismometer. At 2.5 m from the GND seismometer, the coherence is down to 0.5 from about 0.3 to 1 Hz. This is also the case at the far blue piers on the opposite side at about 5 m away.  It is unlikely that even the corrected GND STS helps much in this frequency band. Just as we are in the near field region for wind induced tilt, we are also in the near field region for wind induced vibration. The chamber and walls are only about 3 m from the wall that is bending according to the pressure distribution outside the building and the bending scale is meters.

For 1-5, ISI was set to off-line, HPI was nominal except that sensor correction was turned off. For 6, ISI was back on set for normal IFO operation

1) Huddled, igloos touching, 47 cm +Y of GND 5/6 3:00 to 5/7 00:00; 1664 seconds starting at 14:32:17,  6-26 MPH, ave 17 MPH

2) Huddled rotated by 10 degrees  5/7 04:00 to 5/7 16:00; 1664 seconds starting 5/7 at 15:02:17,  7-25 MPH, ave 17 MPH

3) Across BRS from GND and 20 cm -Y to center on Y of BRS, 133 cm distance, had to recenter so 5/7 19:00 -  5/8 23:50; 1664 seconds starting 5/8 20:56:17   4-32 MPH, ave 17 MPH OR 5/8 14:32:17 6-27 ave 17 MPH

4) Near -Y, +X leg of BSC10, +190 Y of GND, 208 total, 11:00 5/9 UTC to 15:00 5/9 UTC, if drift in Y-axis is OK, the start time could be extended back until 5/9 at 2:00 UTC; 1664 seconds starting 5/9 4:10:17, 4-37 MPH, ave 17 MPH

5) about 30 cm from edge of slab, 254 cm distance from GND, all in +X 16:00 5/9 UTC to 5/10 0:00:00; 1664 seconds starting 5/9 16:30:00, 5-30 MPH, ave 17 MPH

6) Near far (+Y, -X) BSC pier, +510 cm Y total 550 cm distance from GND. Start time 5/11 5:00; 1664 seconds 5/13 15:12:57,  7-31 MPH, ave 17 MPH

Robert & Hugh

H1 was available for commissioning this morning, and had tried to attempt locking, but had issues with the FSS (as noted by Kiwamu below).

Current H1 tasks:

1. DBB work on PSL (but other work could continue)
2. PSL Rotation Stage (Nutsinee) on the order of 45min
3. ISS High Power tests after Nutsinee measurement
4. --->H1 tripped off around 9:45 & Jason is currently working on bringing it back.  Once the PSL is back, DBB & Rotation Stage work will be on deck again.

Note:  SEI would like to have a locked H1 (DC Readout?) for some measurements at some point.

New SEI configuration nodes (ISI_ETMX_ST1_CONF and ISI_ETMY_ST1_CONF)  are now available from the GRD Overview as well as the the H1 Blend page under O-1 on the sitemap.

These nodes will control the configuration of the blends and sensor correction for the end stations. The states try to describe both the engaged blend filter as well as the sensor correction being used:

Blend_Quite_90_SC_BRS - Uses the BRS tilt-corrected sensor correction with the Quite_90 blends. The Quite_90s are the best blends we have for high winds, but do not do as well with the useism as the 45s. Using the BRS tilt corrected signal for SC helps with the wind as well as long as the BRS does not get rung up from the wind.

Blend_Quite_90_SC_None - Quite_90 blends with no SC filters enabled. Also could be used as a good all-around configuration, but not as good in the wind as the previous.

Blend_Quite_90_SC_useism - Quite_90 blends with the sei_notch filter in the WNR bank enabled for SC. The configuration for both high wind and useism. Since the Quite_90s can handle wind but not useism very well, the addition of this SC is meant to help when we have conditions with both wind and useism.

Blend_Quite_45_SC_None -  Uses the 45Mhz blends with no SC filters enabled. The 45mHz blends perform much better in high useism conditions, but do not do well with wind.

Blend_Quite_45_SC_useism - Uses the 45mHz blends with the sei_notch filter in the WNR bank enabled for SC. This may help with the useism a bit more, or it may make it a touch worse. More testing is needed.

(Disclaimer: As testing progresses these states may change and the use of the states may also need some re-evaluation in the future.)

These nodes can turn ON and OFF the BRS SC  by going into and out of the Blend_Quite_90_SC_BRS state. This node will also notify if the BRS damper is on, and then an operator should inform an SEI team member or switch out of a configuration that uses it. It will not automatically turn OFF the BRS SC if the damper turns on! (maybe in the future, but not yet). It will be the job of the operator or SEI team member to take action.

A few notes:

• These states may change as newer, better configurations are made.
• The INIT state is currently a WIP, but I will hopfully have it working consistently soon.
• These nodes manage the BRS_STAT node which reports what state the BRS is in. I would like to remove the BRS_STAT nodes in the future, but not yet.
• Probably more that I'm forgetting

I attached a shot of the Guardian Overview with these new nodes, the updated H1 blend page, as well as the Ops Overview that now have a BRS SC Active/Inactive light.

The attached plot has the EndY and EndX Drift monitor signals for 45 days.  The drift mon represents the reflected image on the linear PD of the BRS Beam DC position.

The bottom graph has the EndX Drift which is relatively stable(compared to BRSY) showing the daily fluctuations and trends up.  Maybe these are warming periods?

The middle graph has the entire invacuum period of the BRSY showing this downward trend is definitely slowing.

The upper graph is the EndY from ~3 May when we rebalanced the beam to a time where I've extrapolated the slope (only about 6 days) out to a drift level when we'll need to balance again.  We expect the drift to slowly ease and I've probably overestimated the slope.  The limit is +-16000 so we should be okay into early  next month.

Corey, Kiwamu,

FSS does not lock on its own as reported Cheryl (27108). In addition, this morning we found that the range of the temperature scan was not good at all so that the autolocker was not finding a 00 mode at all. We have changed the range from [-0.025 K, 0.00 K] to [0.00 K, 0.025 K]. This improved the situation, but the FSS autolocker still keep failing the acquisition.

As Cheryl reported, disabling autolocker actually catches a 00 mode successfully for some reason. Having the autolocker enabled does not acquire a resonance, but rather kicks the servo out of resonance. We than guessed that this may be due to a loo-low oscillation threshold releasing the control loop unnecessarily, and pulled up the threshold from 1 V to 2 V. This setting acquired a resonance once for the first trial, but in the later trials, it never acquired a resonance.

The FSS autolocker needs a more thorough investigation.

It looks like we need to do something about the triple coil drivers that we switch in lock, especially PRM M3.  We have lost lock a good fraction of the times that we have tried to switch in the last month or so.  Screenshot is attached, I also filed an FRS ticket hoping that someone might make an attempt to tune the delays while people are in the PSL tomorrow morning.  FRS ticket #5489 

I forgot to de-energize the Pfeiffer turbo controller sitting on the floor -> someone from the Vacuum group can do this the next time they are in the LVEA.