TITLE: 07/01 Day Shift: 15:00-23:00 UTC (08:00-16:00 PST), all times posted in UTC
STATE of H1: Observing at 146Mpc
CURRENT ENVIRONMENT:
    SEI_ENV state: CALM
    Wind: 8mph Gusts, 5mph 5min avg
    Primary useism: 0.01 μm/s
    Secondary useism: 0.06 μm/s
QUICK SUMMARY:

Receiving a nicely locked H1 which has been locked 5.75hrs. 

Austin gave me a rundown of items to look out for with his lockloss experience:

1. X-arm PLL still was an issue (so may need to employ workarounds:  lower threshold & possibly reset Crystal Frequency
2. Sounds like Violins continue to get rung up after locklosses and result in ~1hr of waiting for the violins to damp down enough to allow one to engage OMC Whitening.
3. Hopefully there's no lockloss today!  *knock on wood*

Oh, and the winds have died but the high temperatures continue outside.

TITLE: 07/01 Owl Shift: 07:00-15:00 UTC (00:00-08:00 PST), all times posted in UTC
STATE of H1: Observing at 144Mpc
SHIFT SUMMARY:

- Lockloss @ 7:29

- Relocking - the ALS X PLL issue was still apparent - I set the RF minimum threshold to -30 and set the crystal frequency to 0 to reset the beatnote and that seemed to do the trick

• Subsequent lockloss due to the MC unlocking for unknown reasons

- 7:46 - incoming 5.8 EQ from Sri Lanka

- Rest of locking was automated, but did have to hold in OMC WHITENING to damp violins for just under an hour

- 9:31 - incoming 5.1 EQ from Kuril Islands

- Acquired NLN @ 9:31

- EX saturations @ 10:56/13:03/14:12

- 13:56 - incoming 4.8 EQ from Alaska

Leaving H1 to Corey with H1 in observing, going on 5:30 hours. Ground motion has settled from the EQs and all appears to be stable.

LOG:

No log for this shift.

H1 has been observing for 1:30 hours, following a lockloss, potentially due to local ground motion. There were a couple EQs that we were successfully able to ride out and ground/wind motion as a whole looks to be dwindling back down.

LOCKLOSS @ 7:29 - Potentially ground motion related, EX/EY is ~0.5 ur in the EQ bandwith and wind speeds are hovering around 30-35 mph sitewide.

TITLE: 07/01 Owl Shift: 07:00-15:00 UTC (00:00-08:00 PST), all times posted in UTC
STATE of H1: Observing at 141Mpc
CURRENT ENVIRONMENT:
    SEI_ENV state: CALM
    Wind: 28mph Gusts, 23mph 5min avg
    Primary useism: 0.07 μm/s
    Secondary useism: 0.08 μm/s
QUICK SUMMARY:

- H1 has been in observing for 9 hours

- End station ground motion in the EQ bandwith has been on the rise as is wind, will monitor both

- CDS/DMs ok

TITLE: 07/01 Eve Shift: 23:00-07:00 UTC (16:00-00:00 PST), all times posted in UTC
STATE of H1: Observing at 143Mpc
SHIFT SUMMARY:

An Earthquake from Argentina (5.3) rolled through around 4:12

Wind has been picking up even more and further increasing the arm ground motion. Gusts over 30mph from 05:30 and still as of 07:00

IX saturation at 05:17, EX at 06:11

                                                                                                                                                                                                              LOG:                                                                                                                                        

STATE of H1: Observing at 142Mpc

• No issues, everythings been stable
• The violins are coming down

(Jordan V., Gerardo M.)
The instrument air at X-End has been alarming, see entry here.  After looking at the trends for this channel, there is some noise/spikes noticeable for this particular channel, while the IFO was recovering from a lockloss, we vented the line but no change was noted on the signal, we will continue to look into this, for now we have raised the alarm level from 5 to 10 via probe, so this is not permanent change.  Perhaps a bad sensor or wire.

Looking at intensity noise in reflection of the interferometer allows us to measure the mode matching as well as the reflection coefficient.

The idea is that fluctuations above the cavity pole are promptly reflected by the interferometer, whereas the DC field will be resonant and have a reflectivity smaller than unity. In our case, where we are close to critically matched but still over-coupled, the reflected DC field also picks up a minus sign. Any field that is not mode matched will simply be prompt reflected and not acquire a minus sign. The later is true for both the fluctuations and the DC field.

Including the total reflected power, one can then invert the equation and determine both mod matching and reflectivity. A note detailing the derivation can be found in LIGO-T2300249.

Using the values measured in alog 70982, we get

For this derivation we neglected to include the RF sidebands. Typically, they are small, but the note details how they can be included if the power is measured as function of the modulation index. The 75W interferometer wasn't thermalized yet, when the measurement was taken and we can expect an additional 1.2% of power increase in reflection. If we attribute all to mode mismatch, we would have a total of ~4.4% of the input power not mode matched.

The mode mismatch power is important for figuring out the impedance matching of the PRM, see alog 68451.

Closes FAMIS 17560, last checked in alog 70032

All plots look normal, as they did last time they were checked.

We are looking at the RIN measured by the reflection port of the interferometer and comparing it to the RIN of the input beam as measured by the ISS second loop detectors. For both 75W and 60W input we are measuring this transfer function using high frequency ISS noise injections.

One thing to notice is that the filter modules for LSC-REFL_A_RIN and LSC-REFL_B_RIN contain a calibration factor of 0.3055, which we removed from the measurements presented here.

We also used the calibration factor from alog 70979 to correct the ISS outer loop detector.

Finally, we derive the power reflection coefficient of the interferometer by dividing the observed power in reflection by the expected prompt reflection value. This is using scaling factors from the above alog.

For the 75W measurement the interferometer was not fully thermalized. We expect more like ~8.5% of the power to be reflected after a couple of hours locked.

Closes FAMIS 25588, previously checked in alog 70776

The outbuilding fans look fine. EY_FAN1_470_1 is the noisiest fan at about 0.3.

The CS fans looks fine, they all saw a glitch 3 days ago. MR_FAN5_170_1 is the noisiest fan at just under 0.4.

TITLE: 06/30 Day Shift: 15:00-23:00 UTC (08:00-16:00 PST), all times posted in UTC
STATE of H1: Observing at 146Mpc
CURRENT ENVIRONMENT:
    SEI_ENV state: CALM
    Wind: 25mph Gusts, 16mph 5min avg
    Primary useism: 0.03 μm/s
    Secondary useism: 0.06 μm/s
QUICK SUMMARY:

• CDS/VAC/Dust
• Winds picking up a little bit
• Motion at the arms is slightly elevated

TITLE: 06/30 Day Shift: 15:00-23:00 UTC (08:00-16:00 PST), all times posted in UTC
STATE of H1: Observing at 143Mpc
SHIFT SUMMARY:

Sheila was able to fix the issue with the EX PLL Beatnote by making adjustments to the ALSx laser.

LOCK #1:  1850-2221utc

• For this lock, held at LOCKING ARMS GREEN so Sheila could make adjustments to the ALSx laser to fix the EX PLL low beatnote (or FIBER_A_DEMOD_RFMON).  Once this was improved, took H1 to NOMINAL LOW NOISE and it almost made it there without intervention, BUT....
• H1 was stuck at OMC WHITENING due to rung up violins
• Oli and I then focused on damping violins.  Guardian thought the NOMINAL gains were a bit high, so we slowly brought up all gains to their NOMINAL values----this took about 1hr.
• Once the Violin Damping gains were all at their NOMINAL values, we made it to NLN, but within seconds there were DCPD saturations, rung-up violins, & some rung up PI modes---H1 was not happy!
• H1 did not like the extra gain of OMC WHITENING.
• TJ had us take the OMC_LOCK node from READY TO HANDOFF down to READY W NO WHITENING, and this removed gain from H1.  We then waited for violins to calm down for about 30min.
• OMC LOCK was then taken back to READY FOR HANDOFF once again.  This rung up violins up a little again, but after a few minutes we finally....
• 2221 Took H1 to OBSERVING (Violins were still a bit high, but have been slowly ringing down.)
• Since ALSx beatnote was fixed, for SDF, I needed to ACCEPT H1:ALS-X_FIBR_LOCK_BEAT_RFMIN original value of -10.0 (it was changed to -20.0 yesterday as a band-aid for the ALSx PLL issue.

LOG:

• 1545-1609 EY pump check (janos)
• 1722-1733 H2 Elec Room cleaning (kim)
• 1849 H1 lockloss (after 17hrs of lock)
  • Took this opportunity to hit "COEFF LOAD" button for LSC model on CDS Overview, at Dave's request. (This is due to a new filter [FM3] for MICH FF).  This filter isn't used, but it was a configuration change which showed up as a RED CFC box for LSC.
• 1855-1950 EX VAC checks (gerardo, jordan)
• 1925 ALSx Laser adjustments at EX (Sheila & a small crew)

Sheila, Naoki, Brina,

Took a look at what changed after powering down (alog 70497, alog 70687) and changing the OM2 settings (alog 70849), from the CAMERA_SERVO, it seems that the ETMX and BS were slightly affected by these changes, (shown in the images attached, the YAW/PIT1 refers to BS and YAW/PIT2 refers to ETMX).

When re-locking, ADS is ran until the error signal is small, then CAMERA_SERVO gets set, so we believe that the changes from the power and OM2 changed how ADS moves the setpoint.

Sheila, Corey, Brina, Lance, Genevieve, Oli

After the lockloss, we went to EX to adjust the ALS X laser current and temperature.  We found the settings at 1.874A, 25.06C, we left them at 1.889A, 25.17C.  

When we first looked at the beatnote on the agilent we could see that there were multiple beatnotes, and that the power was drifting back and forth between them, supporting the idea that the laser was mode hopping. We adjusted the current up and the temperature down until most of the power seemed to be stably in one beatnote, below 100MHz.  Then Corey was able to lock the PLL, and saw a beatnote strength of 4dBm and reset the threshold to it's normal value of -10dBm.  

The attached trend shows that in the last couple of hours, the beatnote has dropped down.  This may mean that we didn't move the current enough to completely avoid mode hopping.

Fri Jun 30 12:47:52 2023 INFO: Fill completed in 2min 52secs

Ran the fill again at 12:45 this afternoon, Gerardo confirmed it was a good fill curbside.

The trip temperatures have been reduced from -120C to -130C to see if this helps with the premature end-of-fills we have seen this week now that the outside temperatures are increasing.

For cross correlation with 60W, hot OM2, we removed squeezing for 1 hour.

start: 1372017274 (2023/6/28 19:54:16 UTC)
end:  1372021147 (2023/6/28 20:58:49 UTC)

Attached is a cross correlation plot for 20 minutes of no sqz time taken June 21st (70668) after first reducing the input power to 60W (366kW circulating power), this was before the LSC feedforward was retuned improving the sensitivity below 50Hz.  The first plot is in loop corrected mA, you can compare the correlated noise estimate by the cross correlation and by subtracting the shot noise.  At high frequencies the shot noise subtraction doesn't work well, I believe this is due to imperfections in how the DCPD sum mA channel is calibrated into actual mA.  At low frequencies the cross correlation is overestimating the DCPD sum PSD, this isn't due to an error in the OLG measurement. See alog 70453 for some information about checks of the cross correlation and this low frequency problem.  In mid frequencies the two methods seem to agree.  The second attachment is the same data calibrated into displacement, with a model of quantum raditation pressure noise included and subtracted from the two estimates. For this time the DARM OLG model from pyDARM was underestimating the OLG by 2% at 24Hz, so I've scaled it up by 2%.

The next set of attachments are the same two plots made for 2 hour of no sqz time from June 4th when the HAM7 ISI had a problem (70117), in DCPD mA and in displacement .  We don't have a DARM OLG measurement from this time, so we are just using the pyDARM model without any scaling.  

Plot 1 shows the dark noise in LSC-REFL_A_LF and REFL_B_LF (yellow/black), with 10W laser input with ISS second loop (red/blue) and w/o ISS second loop (magenta/cyan). The photocurrent in REFL_A and REFL_B was about 16mW each for the 10W measurements. It will turn to about 10mW in full lock. So, we are now about a factor 4 above dark noise.

Plot 2 shows the RIN of the 2 REFL PDs and their average, together with the ISS second loop sensors. The ISS inner and outer sensors have about 7-8mW of light each, so the measurements are limited by the shot noise of the inner PD. In full lock these sensors see about 60mW.