- Though the old script had a duplication problem for GWF files (attachment 1), the new script didn't.
- Resent GWF files missed by the old script (attachment 2) were contained in cache files by the new script.
So changes in origin/ir1-upgrade branch was merged to origin/master. And then, I tried to deploy them to detchar account on Kashiwa cluster. But, even though it's a production environment, uncommitted changes exist and solving conflict will be required...
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k1ctr11 and 21@Mozumi hung up, I recovered them before this update.
Because NUC workstations freezes frequently, I set to periodically check whether the GUI is running properly on the NUCs (k1ctr11, 14, 15, 20, 21) same as monitor workstations. It may be able to recover problematic workstations automatically. (I'm not sure it works fine or not because I haven't identified a cause of this issue yet.) If checker script can be launched after the GUI hangs up, some kind of logs can be obtained at least.
k1ctr12@PSL is still link to 100Mbps (See also klog#36410).
Due to slow network speeds, the NFS mount timed out while the OS was booting up, so I had to mount NFS regions manually after the OS had started.
(Work on 13th)
[Hirata, Washimi, Takahashi]
This is a rapid report. Details will be reported later. We started assembling the new mirror. We found that the new mirror (85%) is thinner than the old mirror (70%). Measured thickness with vernier calipers was 7.9mm for the new mirror and 9.6mm for the old mirror at the edge marker. The thickness of the shims (#9 in Picture) was 1.5mm. Therefore, the flange (#5 in Picture) couldn't fix the mirror even if the shims were not used.
[Kimura and Yasui]
On March 13, we replaced the Q-mass for the IXC, whose filament had broken. (Photo 1)
As part of this replacement, we added a pressure gauge and a valve. (Phpoto 2)
After the replacement, we conducted a vacuum leak test, and the leak rate was found to be 1×10⁻¹² Pa·m³/s or less. (Photo 3)
Following the leak test, we are continuing to pump down the Q-mass connection piping.
We plan to open the valve between the Q-mass and the IXC on or after March 16 to connect the Q-mass to the IXC.
Old minute frames were removed on the storage for k1fw0.
Removed time segment is [1260000000, 1300000000)
These data is available on Kashiwa.
There was no undelivered data to Kashiwa in that time segment.
PoE doesn't seem to be enabled on the camera switch at the server room and I couldn't enable it because IP address of this switch is missing.
So I moved a2A5328-4gmPRO near the camera switch at the IOO0 rack on which PoE is enabled and a2A5328-4gmPRO came back online again (Fig.1).
But, I found that the switch at IOO0 rack and one at server room were only linked at 1G, contrary to what I had been told.
For this reason, I haven't yet done the test with the network which should have sufficient capability.
Anyway, both a2A5328-4gmPRO and acA4112-8gm are now online.
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In today's work, I understood the camera network configuration is completely chaos. IP address information on JGW wiki was not true for 3 of 6 network switches. I tried to do ping-search beyond L3 segment by using virtual NIC but 2 of 6 switches including the core switch at the server room are still missing. 2 of found 4 switches don't have a reachable route because the inconsistency between the physical and logical connections. A drastic reassessment is required.
As mentioned above, the link speed between the IOO0 and the server room is 1G though it should be 10G. According to my check, I couldn't find any reason why the link speed between IOO0 and the server room is limited as 1G on the switch at the IOO0 rack. So I'm doubting it comes from the settings on the core switch at the server room. But the core switch is still missing. So we need salvage it at first. Or using USB-RJ45 console cable if someone have...
Date: 2026/03/13
Member: Dan Chen, Misato Onishi
We performed our usual WSK calibration at UToyama.
The results look no problem.
Results
| Case | Alpha (Main Value) | Alpha (Uncertainty) |
| Front WSK, Back GSK | -0.910922 | 0.000075 |
| Front GSK, Back WSK | -0.908846 | 0.000225 |
Comparison with Previous Results
Comparing with previous results, no significant issues were found.
Attached graph is the result summary including the latest measured data.
Abstract
IO-chassis and the front-end computer for ITMX were replaced to new hardwares.Though a simple cabling check by DAC output was able to be done, we haven't checked LOCK_ACQUISITION state is reachable because of a large change in the room temperature of IXV.
These check can be done in tonight, weekend, or next Monday.
Details
A pair of V2 IO chassis and the front-end computer had been launched as k1iz1 without any connection to the circuits (klog#36129, klog#36183). They run stable in recent 1+ month. So we started to use them for ITMX.After stopping the old k1ix1 and V1 IO-chassis, all SCSI cables for AA inputs/AI outputs were moved from V1 to V2 IO-chassis. After then, the MAC address of the computer that had been operating as k1iz1 was re-registered to DHCP as k1ix1. As a quick check of front-end operation, we launched the new k1ix1 and we didn't find any issue on GDS and DAQ MEDM screens. Note that, RFM card installed in the new k1ix1 is signle-mode one. When we removed old k1ix1, it might be better to replace RFM card as multi-mode one. Using single-mode one for k1ix1 is no problem, but single-mode one can be used both long and short distance and it's useful for another place.
Finally, DB37 BO/BIO cables were also moved from V1 to V2 IO-chassis. After then we changed the guardian request but it IP control cannot be engaged probably because of large change (~2degC) in the room temperature of IXV. It seems come from our activity in long time. Checks with guardian will be able to be done after the room temperature will come back as same level before our work.
For this reason, please note the fact that the Guardian operation has not been verified though it's no problem to request some state to VIS_ITMX guardian.
SawadaH, Kimura, Uchiyama
Weekly vacuum system inspection found that TMP(#40) was stopped unexpectedly. We found the interlock system for TMP(#40) was turned off and this was the reason of why TMP(#40) was stopped.
Yesterday, we stopped TMP(#8) and the power breaker for TMP(#8) was turned off. Since the power cable of the interlock system for TMP(#40) was connected to the power breaker for TMP(#8) wrongly, the interlock system was also turned off.
We re-connected the power cable of the interlock system(#40) to the power breaker for TMP(#40) and then restarted TMP(#40).
Abstract:
Finesse measurements were conducted periodically in 2025, but the values between these measurements remain unknown.
We propose a method to estimate the finesse using linear fitting and subsequently calculate the multiplication of the amplitude reflectivities of the ITM and ETM.
Dividing the observation time into several segments to incorporate the time-dependent changes in finesse allows for a more accurate calculation of the transfer function, such as Eq. (20) in PhysRevD.104.062008.
Consequently, this enables a more accurate evaluation of the sensitivity to the axion-photon coupling.
Method:
The finesse of the linear cavity is given by
F = np.pi * np.sqrt(r_ITM * r_ETM) / (1 - r_ITM * r_ETM)
where r_ITM and r_ETM are the amplitude reflectivities of ITM and ETM, respectively.
By solving this equation as a quadratic for np.sqrt(r_ITM * r_ETM) and squaring the result, we obtain,
r_ITM * r_ETM = ((- np.pi + np.sqrt(np.pi**2 + 4 * F**2)) / (2 * F))**2
Therefore, the value of r_ITM * r_ETM can be determined by substituting the finesse value.
Results:
Using the above method, the value of r_ITM * r_ETM can be estimated from the finesse at a given GPS time.
For instance, by performing a linear fit on the finesse measured after 2025/02/28 15:00 UTC, the finesse at 2025/08/15 14:00 UTC can be estimated.
As shown in Fig.1, the blue and red dots are the updated finesse results (klog #36297).
Applying a linear fit to the finesse measured from GPS times 0.0 to 1.5e7 sec, we can obtain the fitting results for the finesse of the Xarm (F_x) and Yarm (F_y), indicated by the green and orange solid lines in Fig. 1, respectively.
The resulting fitting functions are as follows:
F_x = - 1.0336e-5 * (GPS - 1424790018) + 1413.7
F_y = - 6.2334e-6 * (GPS - 1424790018) + 1274.5
where GPS is the GPS time.
Substituting the GPS time for 2025/08/15 14:00 UTC (black dashed line) into these functions, the estimated finesse values are as follows:
F_x = 1263.7
F_y = 1184.1
Furthermore, according to the procedure described in the above method, the estimated values of r_ITM * r_ETM for Xarm and Yarm are as follows:
r_ITMX * r_ETMX = 0.99752
r_ITMY * r_ETMY = 0.99735
By determining the values of r_ITM * r_ETM for each segment divided from the observation time and substituting them into the transfer function, we can calculate the sensitivity to the axion-photon coupling more accurately.
I measured the OMC PD dark noise wih several configurations.
Figure 1 shows the results (legend on the left top graph represents the setting of the measurement of each color plot).
Blue line (measured in 2025) and pink line (measured today) can be compared directly because the measurement setting of these two are the same.
Though the PDB spectrum was worse in the previous measurement (klog36277), the measured spectrum today seems good.
I'm not so sure why the PDB noise level was recovered.
This morning, I fund ETMY was tripped due to the watch dog of F2 GAS as shown in fig1
According to the seismometer signals, this trip seemed coincident with the earthquake (fig2).
So, I just recovered the ETMY from the tipped state.
[Kimura and Yasui]
On March 12, we switched the vacuum pumps in the central mirror chamber to ion pumps.
The TMP and dry pumps currently in operation are pumps #40 and #41 directly below the arm-side GV.
All other TMP and dry pumps in the central mirror room, including those on the 2nd floor, have been stopped.
The vacuum pumps at X-end 1F have also been switched to ion pumps.
Locations where the switch to ion pumps is not yet complete are the EXVs at X-end 2F and the EXVs at Y-end 1F and 2F.
The switch is scheduled for early next week.
[Takahashi, Hirata, Washimi]
We installed the FLDACCs in the pre-isolator.
- Set the attachment plates on the top table. Location is shown in Picture 1.
- Moved the assembled FLDACC units to the upper floor one by one (Picture 2), and removed the lower stopper, then put the unit on the attachment plate.
- Attached the counterweights to the proof mass along with the tuning results. Removed the protection covers temporarily during this work.
- Adjusted the tilt of the units (Picture 3).
- Removed three ballast rings of 8.3kg (Picture 4) and added one small ballast ring of 1.0kg to compensate for the additional weight of three units of 8.0kg.
- Installed the in-vacuum cables (Pictures 5 and 6). The Kapton cables from the units were connected to the PTFE cables from the feedthrough flange on the table.
- Connected the outer cables to the feedthrough flange with the flip cables (Picture 7). New flip cables were out of stock, so we used the old type cables.
- Checked the resistance of the coils in the FLDACC at the feedthrough flanges. Initially, the H3 1-6pin was disconnected due to a loose contact at the relay point.
H1 [Ω] H2 [Ω] H3[Ω] 1-6 47.3 47.2 53.0 2-7 55.2 55.2 62.5 3-8 5.5 5.1 4.9 - Checked the signals on the daiaggui. Measured the transfer functions (Picture 8).
We also examined the fluctuation of the current from the power supply to the circuit when the PRFPMI was flashing.
A rough diagram of the measurement setup is shown in fig. 1.
We connected three whitening filters (WF1, WF2, and WF3) to the external power supply (TEXIO DC power supply).
Between the +18 V from the power supply and the circuit (WF3), we inserted a 1-Ohm standard resistance to measure the current fluctuation to the circuit.
The data logger measured the voltage difference between the two edges of the resistance.
Figure 2 shows the time series data of the supply current to the circuit, and Figure 3 shows an enlarged view of Figure 2 from 190 to 200 seconds.
The red dashed line shows when we opened the laser shutter on the REFL WFS QPD path.
The green dashed line shows the time when we tuned the CARM/DARM offsets so that the PRFPMI flashes increased.
The current fluctuation becomes larger when the beam hits the QPDs and when the PRFPMI flashes increase.
Since the current spike from the power supply is less than 100 ms (which corresponds to several tens of Hz), the DC power supply must supply not only DC current, but also an AC current of ~1 A to the circuit in total because there are ten or more whitening filters for the REFL PDs/QPDs.
We are unsure whether these values can be supplied by the DC power supply in the computer room, which is far from the DGS rack. However, one possibility of the IR-GR coupling is due to the DC power supply's poor performance at high frequencies.
In any case, we need to discuss how to address the GR-IR coupling issue, as we would require an additional 10 A power supply near the ALS/IOO racks if we were to replace all the WFs for the REFL PDs/QPDs.
We found unused whitening filter (s1909741) was in BS rack. We removed it from the rack and used for the investigation in klog36538. Today, we brought it back to Mozumi circuit room.
Ushiba, Tanaka
## Abstract
Similarly with the PD case in klog36550, We succeeded in solving the couplilng issue when the beam was on REFL QPDs by replacing the power supply.
## What we did
At first, we recovered the shutter for REFL QPDs with the almost same procedure in klog36514. Then, When LSC_LOCK was in FIND_IR_RESONANCES, we opened the shutter so that the reflection beam hit on QPDs. After that, we aligned PRM manually. Figure 1 shows the time series of f DARM error/feedback and PRM guardian state from MISALIGNED_FOR_LOCK_ACQ(2300) to LOCK_ACQUISITION(2000). As PRM alignment got better, DARM signal got noisier. At last, ALS_DARM lock was lost due to the TM actuator saturation. This situation is the almost same as the one in klog31299. So we tried to solve issue by changing the power supply for QPD whitening filters.
Next, we measured DARM spectra in some different situations. Fig. 2 shows the DARM error spectra when IR beam was flushing in FIND_IR_RESONANCES. Blue lines shows the reference when IR flash amount was very low because PRM misalgined and Black lines shows the noisy reference when IR flash amount was very high because PRM aligned. Also, green lines shows the reference of yesterday's last result.
Brown shows the spectrum when the shutter for REFL QPDs was opend but all of QPD whitening filters were turned off. It seems to be the same level as green lines. Therefore, other circuits in the QPD path, ex. IQ demodulaters, did not contaminated the noise to DARM loops.
Magenta shows the spectrum when we turned on the only whitening filter for REFL QPD1 RF17. Then, DARM spectrum got noisy. This is the same situation as the PDA one. So, we changed the power supply to an independent one. Orange line in Fig.2 shows the result after changing the power supply. The noise level got quieter and got the same level as the brown one. This indicates that separating the power supply is valid for reducing the coupling.
Therefore, we need to change the power supplies for all of QPD whitening filters or to modify the current buffer in the circuits. .
This also indicates that we can use REFL QPDs during the lock acquisition term.
## Note
- Above 20 Hz, the brown, green, and orange spectra is slightly larger than the most slient one (blue). This indicates the power supplies for other circuits, ex. PD interfaces, may also be changed.
- Sorry, we completely forgot to turning on the other whitening filters (QPD1 RF45, QPD2, QPD3, QPD4). we need to turn on them before starting ASC commissioing.
We also examined the fluctuation of the current from the power supply to the circuit when the PRFPMI was flashing.
A rough diagram of the measurement setup is shown in fig. 1.
We connected three whitening filters (WF1, WF2, and WF3) to the external power supply (TEXIO DC power supply).
Between the +18 V from the power supply and the circuit (WF3), we inserted a 1-Ohm standard resistance to measure the current fluctuation to the circuit.
The data logger measured the voltage difference between the two edges of the resistance.
Figure 2 shows the time series data of the supply current to the circuit, and Figure 3 shows an enlarged view of Figure 2 from 190 to 200 seconds.
The red dashed line shows when we opened the laser shutter on the REFL WFS QPD path.
The green dashed line shows the time when we tuned the CARM/DARM offsets so that the PRFPMI flashes increased.
The current fluctuation becomes larger when the beam hits the QPDs and when the PRFPMI flashes increase.
Since the current spike from the power supply is less than 100 ms (which corresponds to several tens of Hz), the DC power supply must supply not only DC current, but also an AC current of ~1 A to the circuit in total because there are ten or more whitening filters for the REFL PDs/QPDs.
We are unsure whether these values can be supplied by the DC power supply in the computer room, which is far from the DGS rack. However, one possibility of the IR-GR coupling is due to the DC power supply's poor performance at high frequencies.
In any case, we need to discuss how to address the GR-IR coupling issue, as we would require an additional 10 A power supply near the ALS/IOO racks if we were to replace all the WFs for the REFL PDs/QPDs.
>Moreover, we found that the REFL HWP before PDA1 and PDA2 was not functioning, so we will restore it.
In this morning, this issue was somehow resolved without any actions.
So, if the similar issue will be found, please let us know.
Please note that Hyades-2 has only a single volume for storing both full and trend data. As a result, the disk usage values for full and trend data are shown as the same value on the MEDM screen.
> Please note that we confirmed that the current drawn from the independent power supply approximately doubled (~1.4 A for +18 V and ~0.8 A for −18 V) after connecting the two boards.
> Correspondingly, the current meter in the computer room showed a reduction of more than 1 A.
Photo. 1 and 2 show the current values on +18 V power supply before and after changing the power supply for the whitening filters. You can see the current reduction before and after the power supply change.
This was a question about the PSL table that was suggested I post here.
Robert Schofield saw the presentation on beam jitter at LVK and wanted to ask if the legs of the PSL table had been grouted. He said he had discussed this with some people from KAGRA a few years ago and wanted to ask if there had been any further discussion about this.
LIGO grouted its PSL during the initial LIGO phase and it reduced PSL table coupling to ground motion. It involves glueing the table legs to the floor with a cement called hydrostone. It can apparently be done without moving the table as you build a dam for the cement around the leg and just pour it in situ.
[Takahashi.R, Washimi, Hirata]
We confirmed that IRM damper works well. After that, we locked suspention again.
1. Release suspention
BF, IRM, IM, RM and TM are released. IP and Topfilter were locked.
2. Check IRM damper position
Fortunately, IRM damper position looks almost same as before releasing suspention.
3. Check motion of IRM damper
First, we tried to check the damper motion, but it seemed that the damper was not working.
Takahashi-san inspected the area outside the SRM rack and found that the cross‑cable used between the feedthrough and the D‑sub cable was not appropriate.
After we replaced the cross‑cable, Takahashi-san confirmed that the IRM damper was working properly using the OSEM signal.
4. Transfer function
Takahashi-san will report later.
5. Lock the suspention
BF, IRM, IM, RM, TM were locked again.
6. Fasten feedthrough flange
We tighten feedthrough flange bolts(K-4-2). 10Nm→15Nm, 2times.
Today's photo is here: https://www.dropbox.com/scl/fo/ljozph0rohm3n46sp2ewj/ACaU31NZxhAETiqBB0v-Ras?rlkey=akuabdr9t2kroq02a5ae85t08&st=wy6asdyg&dl=0
*Sorry, I don't have any information about the relation of the pins and the coil wire-winding directions now. I will ask Takahashi-san.
We performed the tapping test with monitoring the IMC REFL WFS signals.
10 : 56 - 11:20 (JST)
All results can be seen in attached pdf file and I will make the summary page in notion soon.
Quick comments;
M7 mirror 372 Hz
M18 right mirror 150 Hz
M13 mirror 320 and 480 Hz
M17 mirror 214, 340 and 715 Hz
EOM various peaks
M19 mirror 368 and 395 Hz, various peaks
Periscope various peaks
M18 337 and 355 Hz and above 800 Hz
Note ;
We should perform to all mirrors for main path.
We should set blue spectrum, not p and y, but during tapping(red) and silent(blue, reference) since we can easily get the information of the excitation frequency.
I have performed an overall test the these check scripts: link
I did not find any issue on the scripts, but there are many issues on the test data.
We need the reconstructed data made by updated offline pipeline.