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ID Date Author Typeup Category Subject
  2354   Sat Dec 5 01:40:11 2009 KojiUpdateoplevsOplevs centered, IP_POS and IP_ANG centered

We restarted daqd and it did restored the problem
http://lhocds.ligo-wa.caltech.edu:8000/40m/Computer_Restart_Procedures#fb40m
Then restart the 'daqd' process:'telnet fb40m 8087', type "shutdown" at the prompt. The framebuilder will restart itself in ~20s.

 

It did not related to the problem, but we also cleaned the processes related to dtt, dataviewer by pkill

After that the alignment scripts started to work again. As a result, we got some misalignment of the oplevs.
I am going to come on Sunday
- Align the optics
- Align the oplevs again
- Take snapshots for the suspensions
- Align the IP_POS, IP_ANG
- Align the aux laser for the absolute length
- Align PSL table QPDs, and MCT QPD

  2357   Sat Dec 5 17:34:30 2009 robUpdateIOOfrequency noise problem

There's a large broadband increase in the MC_F spectrum.  I'm not totally sure it's real--it could be some weird bit-swapping thing.  I've tried soft reboots of c1susvme2 and c1iovme, which haven't helped.  In any case, it seems like this is preventing any locking success today.  Last night it was fine.

Attachment 1: mcf.png
mcf.png
  2358   Sat Dec 5 18:23:48 2009 KojiUpdateoplevsOplevs centered, IP_POS and IP_ANG centered

NOTE: HEPA is on at its full.

[[[OK]]] Align the suspended optics (by Rob)
[[[OK]]]
Align the oplevs again
[[[OK]]] Take snapshots for the suspensions/QPDs/IO QPDs/PZT strain gauges
[[[OK]]] Align the IP_POS, IP_ANG
[[[OK]]] Align the PSL table QPDs, the MC WFS QPDs, and the MCT QPD
[[[OK]]] Align the aux laser for the absolute length 


Alignment of the aux laser

o Go to only ITMX mode:
Save the alignment of the mirrors. Activate X-arm mode. Misalign ITMY and ETMX.

o Inject the aux beam:
Open the shutter of the aux NPRO. Turn the injection flipper on.

o Look at the faraday output:
There are several spots but only one was the right one. Confirm the alignment to the thorlabs PD. Connect the oscilloscope to the PD out with a 50Ohm termination.
Thanks to the Alberto's adjustment, the beat was already there at around 10MHz. After the PD adjustment, the DC was about 600mV, the beat amplitude was about 50mVpp.

o Adjust the aux beam alignment:
Adjust the alignment of the aux beam by the steering mirrors before the farady isolator. These only change the alignment of the aux beam independently from the IFO beam.
After the alignment, the beat amplitude of 100mVpp was obtained.

o Closing
Close the shutter of the NPRO. Turn off the flipper mirror. Restore the full alignment of the IFO.

Attachment 1: Screenshot_091205_1830.png
Screenshot_091205_1830.png
  2359   Sat Dec 5 22:31:52 2009 robUpdateIOOfrequency noise problem

Quote:

There's a large broadband increase in the MC_F spectrum.  I'm not totally sure it's real--it could be some weird bit-swapping thing.  I've tried soft reboots of c1susvme2 and c1iovme, which haven't helped.  In any case, it seems like this is preventing any locking success today.  Last night it was fine.

 Rebooting c1iovme (by keying off the crate, waiting 30 seconds, and then keying it back on and restarting) has resolved this.  The frequency noise is back to the 'usual' trace.

  2360   Mon Dec 7 09:38:05 2009 KojiUpdateVACVent started

Steve, Jenne, Koji

The PSL was blocked by the shutter and the manual block.
We started venting
at 9:30

09:30  25 torr
10:30 180 torr
11:00 230 torr

12:00 380 torr

13:00 520 torr
14:30 680 torr - Finish. It is already over pressured.

  2361   Mon Dec 7 18:18:55 2009 JenneUpdateCOCETMX drag wiped

[Koji, Jenne, Alberto, Steve, Bob]

ETMX has been drag wiped. 

Around 2:45pm, after the main IFO volume had come up to atmospheric pressure, we removed both doors to the ETMX chamber.  Regular procedures (wiping of O-rings with a dry, lint-free cloth, covering them with the light O-ring covers, etc.) were followed.  Koji took several photos of the optic, and the rest of the ETMX chamber before anything was touched. These will be posted to the 40m Picasa page.  Steve and Koji then deionized the optic.

Koji removed the bottom front earthquake stop, and clamped the optic with the remaining earthquake stops.

The clean syringes were prepared: These are all glass and metal (nothing else) medical syringes.  The size used was 100microliters.  Earlier today, we had prepared our solvents in small little beakers which had been baked over the weekend.  Brand new glass bottles of Acetone and Isopropyl Alcohol were opened, and poured into the small beakers.  To make sure we have enough, we have 3 ~10ml beakers of each Acetone and Isopropyl.

We started with Acetone.  The syringe was filled completely with acetone, then squirted onto a kimwipe.  This was repeated ~twice, to ensure the syringe was well rinsed.  Then the syringe was filled a little past the 100 microliter mark.  Koji held a piece of lens cleaning paper to ETMX and used an allen wrench underneath the optic to help guide the paper, and keep it near the optic (of course, the only thing in actual contact with the optic was the lens paper).  In one smooth shot, the plunger of the syringe was pressed all the way down.   (This is a bit tricky, especially when the syringe is totally full.  You have to squeeze it so the plunger moves fairly quickly down the barrel of the syringe to get a good arc of liquid.  The goal is to shoot all of the solvent to the same place on the lens paper, so that it makes a little circle of wetness on the paper which covers the coated part of the optic.  The amount of solvent used should be balanced between having too little, so that the paper is dry by the time it has been wiped all the way down, and too much such that there is still a residue of liquid on the optic after the paper has been removed.)  The target was to hit the optic just above the center mark (the oplev was on, so I went for just above the red oplev dot).  Immediately after applying the liquid onto the paper, Koji slowly and smoothly pulled down on the lens paper until it came off of the bottom of the optic.  The acetone was repeated, for a total of 2 acetone wipes.  Because acetone evaporates very quickly, more acetone is used than isopropyl.  The optimal amount turned out to be ~115 microliters of acetone.  It is hard to say exactly how much I had on the second wipe, because the syringe is not marked past 100 microliters.  On the first wipe, with about 105 microliters, the lens paper was too dry at the bottom of the optic.

We then switched to Isopropyl.  A new syringe was used, and again we rinsed it by filling it completely with isopropyl, and emptying it onto a kimwipe.  This was repeated at least twice.  We followed the same procedure for applying liquid to the optic and wiping the optic with the lens paper.  On the first try with isopropyl, we used 100 microliters, since that was the preferred amount for acetone.  Since isopropyl evaporates much slower than acetone, this was determined to be too much liquid.  On the second isopropyl wipe, I filled the syringe to 50 microliters, which was just about perfect.  The isopropyl wiping was done a total of 2 times.

After wiping, we replaced the front bottom earthquake stop, and released the optic from the other earthquake stops' clamping.  The OSEM values were checked against the values from the screenshots taken yesterday afternoon, and were found to be consistent.  Koji took more photos, all of which will be placed on the 40m Picasa page.

We visually inspected the optic, and we couldn't see anything on the optical surface of the mirror.  Koji said that he saw a few particulates on some horizontal surfaces in the chamber.  Since the optic seemed (at least to the level of human vision without a strong, focused light) to be free of particulates on the optical surface to start with, the suspense will have to remain until we button down, pump down, and try to lock the IFO to determine our new finesse, to see if the wiping helped any substantial amount. 

We replaced the regular, heavy door on the inner side of the ETMX chamber (the side closer to the CES building), and put only a light door on the outer side of the chamber (the side closer to the regular walkway down the arm).  We will look at the spectra of the OSEMS tomorrow, to confirm that none of the magnets are stuck.

We commence at ~9am tomorrow with ETMY.

LESSONS LEARNED:

The LED lights are awesome.  It's easy to use several lights to get lots of brightness (more than we've had in the past), and the chamber doesn't get hot.

We should get larger syringes for the acetone for the large optics.  It's challenging to smoothly operate the plunger of the syringe while it's so far out.  We should get 200 microliter syringes, so that for the acetone we only fill them about half way.  It was noticeably easier to apply the isopropyl when the syringe only had 50 microliters.

* It may be helpful to have a strong, focused optical light to inspect the surface of the mirror.  Rana says that Garilynn might have such an optical fiber light that we could borrow.

  2362   Mon Dec 7 19:02:22 2009 MottUpdateGeneralReflectivity Measurements

I have made some measurements of the R value for some coatings we are interested in.  The plots have statistical error bars from repeated measurements, but I would suspect that these do not dominate the noise, and would guess these should be trusted to plus or minus 5% or so.  They still should give some indication of how useful these coatings will be for the green light.  I plan to measure for the ITM as soon as possible, but with the venting and finals this may not be until late this week.

 

EDIT (12/9/09): I fixed the label on the y axis of the plots, and changed them to png format.

Attachment 1: Y1-45P_R.png
Y1-45P_R.png
Attachment 2: Y1-45S_R.png
Y1-45S_R.png
Attachment 3: Y1-50CC_R.png
Y1-50CC_R.png
  2363   Tue Dec 8 03:53:49 2009 kiwamuUpdateSUSFree swinging spectra of ETMX

In this night, I checked the free swinging spectra of ETMX to make sure nothing wrong with ETMX by the wiping.

Compared with the past (Aug.6 2008), the spectra of ETMX doesn't show significant change.

Successfully the wiping activity didn't change its configuration so much and didn't bring bad situations.

(bad situation means for example, the suspended components hit some others).

 

 The spectra of ETMX by DTT are attached. Also you can see the past spectra in Yoichi's entry.

Yoichi's data was taken during the air-pressure condition, so it's good for comparing.

Actually I compared those data by my eyes, because I could not get the past raw data somehow.

The resonant frequencies and their typical height changed a little bit, but I think those are not significant.

NOTE: In the figure, pitch and yaw modes (~0.57Hz and ~0.58Hz) look like having a smaller Q-factor than the past.

 

Attachment 1: ETMX_air.png
ETMX_air.png
  2364   Tue Dec 8 09:18:07 2009 JenneUpdateComputersA *great* way to start the day....

Opening of ETMY has been put on hold to deal with the computer situation.  Currently all front end computers are down.  The DAQ AWGs are flashing green, but everything else is red (fb40m is also green).  Anyhow, we'll deal with this, and open ETMY as soon as we can.

The computers take priority because we need them to tell us how the optics are doing while we're in the chambers, fitzing around.  We need to be sure we're not overly kicking up the suspensions. 

  2366   Tue Dec 8 13:03:26 2009 KojiUpdateCOCETMY drag wiped

Jenne, Kiwamu, Alberto, Steve, Bob, Koji

We wiped ETMY after recovery of the computer system. We take the lunch and resume at 14:00 for ITMX.
Detailed reports will follow.

  2367   Tue Dec 8 16:27:13 2009 JenneUpdateCOCITMX wiped

Jenne, Kiwamu, Koji, Alberto, Steve, Bob

ITMX was wiped without having to move it. 
After 'practice' this morning on ETMY, Kiwamu and I successfully wiped ITMX by leaning into the chamber to get at the front face. 

Most notable (other than the not moving it) was that inspection with the fiber light before touching showed many very small particles on the coated part of the optic (this is versus ETMY, where we saw very few, but larger particles).  The after-wiping fiber light inspection showed many, many fewer particles on the optical surface.  I have high hopes for lower optical loss here!

  2368   Tue Dec 8 23:13:32 2009 kiwamuUpdateSUSfree swinging spectra of ETMY and ITMX

The free swinging spectra of ETMY and ITMX were taken after today's wiping, in order to check the test masses.

These data were taken under the atmospheric pressure condition, as well as the spectra of ETMX taken yesterday.

Compared with the past (see Yoichi's  good summary in Aug.7 2008), there are no significant difference.

There are nothing wrong with the ETMY and ITMX successfully.

 --

By the way I found a trend, which can be seen in all of the data taken today and yesterday.

The resonances of pitch and yaw around 0.5Hz look like being damped, because their height from the floor become lower than the past.

I don't know what goes on, but it is interesting because you can see the trend in all of the data.

 

 

 

 

 

Attachment 1: SUS-ETMY.png
SUS-ETMY.png
Attachment 2: SUS-ITMX.png
SUS-ITMX.png
  2369   Wed Dec 9 00:23:28 2009 KojiUpdateSUSfree swinging spectra of ETMY and ITMX

Where is the plot for the trend?
It can be either something very important or just a daydream of you.
We can't say anything before we see the data.

We like to see it if you think this is interesting.

... Just a naive guess: Is it just because the seismic level got quiet in the night?

 

P.S.

You looks consistently confused some words like damping, Q, and peak height.

  • Q is defined by the transfer function of the system (= pendulum).
     
  • Damping (either active or passive) makes the Q lower.
     
  • The peak height of the resonance in the spectrum dy is determined by the disturbance dx and the transfer function H (=y/x).

dy = H dx

As the damping makes the Q lower, the peak height also gets lowered by the damping.
But if the disturbance gets smaller, the peak height can become small even without any change of the damping and the Q.

Quote:

By the way I found a trend, which can be seen in all of the data taken today and yesterday.

The resonances of pitch and yaw around 0.5Hz look like being damped, because their height from the floor become lower than the past.

I don't know what goes on, but it is interesting because you can see the trend in all of the data.

 

  2370   Wed Dec 9 09:07:32 2009 steveUpdatePEMhigh seismic activity

The construction activity is shaking the tables in the control room.  The compactor- large remote controlled jackhammer is in the bottom of the 16-17 ft deep hole 15 ft east of ITMY in CES bay. The suspensions  are holding OK. PRM, MC1 and MC3 are effected mostly.

Attachment 1: seis24d.png
seis24d.png
Attachment 2: seis4h.png
seis4h.png
Attachment 3: P1050833.JPG
P1050833.JPG
Attachment 4: P1050836.JPG
P1050836.JPG
  2371   Wed Dec 9 10:53:41 2009 josephbUpdateCamerasCamera client wasn't able to talk to server on port 5010, reboot fixed it.

I finally got around to taking a look at the digital camera setup today.  Rob had complained the client had stopped working on Rosalba.

After looking at the code start up and not complain, yet not produce any window output, it looks like it was a network problem.  I tried rebooting Rosalba, but that didn't fix anything.

Using netstat -an, I looked for the port 5010 on both rosalba and ottavia, since that is the port that was being used by the camera.  Ottavia was saying there were 6 established connections after Rosalba had rebooted (rosalba is 131.215.113.103).  I can only presume 6 instances of the camera code had somehow shutdown in such a way they had not closed the connection.

[root@ottavia controls]#netstat -an | grep 5010
tcp        0      0 0.0.0.0:5010                0.0.0.0:*                   LISTEN     
tcp        0      0 131.215.113.97:5010         131.215.113.103:57366       ESTABLISHED
tcp        0      0 131.215.113.97:5010         131.215.113.103:58417       ESTABLISHED
tcp        1      0 131.215.113.97:46459        131.215.113.97:5010         CLOSE_WAIT 
tcp        0      0 131.215.113.97:5010         131.215.113.103:57211       ESTABLISHED
tcp        0      0 131.215.113.97:5010         131.215.113.103:57300       ESTABLISHED
tcp        0      0 131.215.113.97:5010         131.215.113.103:57299       ESTABLISHED
tcp        0      0 131.215.113.97:5010         131.215.113.103:57315       ESTABLISHED

 

I switched the code to use port 5022 which worked fine.  However, I'm not sure what would have caused the original connection closure failures, as I test several close methods (including the kill command on the server end used by the medm screen), and none seemed to generate this broken connection state.  I rebooted Ottavia, and this seemed to fix the connections, and allowed port 5010 to work.  I also tried creating 10 connections, which all seem to run fine simultaneously.  So its not someone overloading that port with too many connections which caused the problem.  Its like the the port stopped working somehow, which froze the connection status, but how or why I don't know at this point.

  2372   Wed Dec 9 17:51:03 2009 kiwamuUpdateSUSwatchdogs

Please do not touch the watchdogs for all SUSs except for MCs,

because I am going to measure the free swinging spectra for ITMs, ETMs, BS, PRM, SRM tonight.

Today, it is good chance to summarize those data under atmospheric pressure.

thank you.

 

  2373   Wed Dec 9 18:01:06 2009 KojiUpdateCOCWiping finished

[Kiwamu, Jenne, Alberto, Steve, Bob, Koji]

We finished wiping of four test masses without any trouble. ITMY looked little bit dusty, but not as much as ITMX did.
We confirmed the surface of the ITMX again as we worked at vertex a lot today. It still looked clean.

We closed the light doors. The suspensions are left free tonight in order to check their behavior.
Tomorrow morning from 9AM, we will replace the door to the heavy ones.

  2374   Wed Dec 9 21:09:28 2009 kiwamuUpdateSUSRe: free swinging spectra of ETMY and ITMX

Okay, now the data are attached. At that time I just wanted to say like the follower.

- - -

In the free-swinging spectra around ~0.5Hz, you can see the two resonances, which come from pitch and yaw mode of the pendulum.

Note that, the vertical and the horizontal axis are adjusted to be the same for the two plots in the figure .

And I found that

* the floor levels are almost the same (the factor of about 1.5 or something like that) compared to the past.

* however the peak heights for two resonances are several 10 times smaller than the past.

* this tendency are shown in all of the data (ITMX, ETMX, ETMY).

If such variation of the peak heights is cased by the seismic activity, it means the seismic level change by several 10 times. It sounds large to me.
 

Quote:

Where is the plot for the trend?
It can be either something very important or just a daydream of you.
We can't say anything before we see the data.

Quote:

By the way I found a trend, which can be seen in all of the data taken today and yesterday.

The resonances of pitch and yaw around 0.5Hz look like being damped, because their height from the floor become lower than the past.

I don't know what goes on, but it is interesting because you can see the trend in all of the data.

 

 

Attachment 1: Pitch-Yaw_modes.png
Pitch-Yaw_modes.png
  2375   Thu Dec 10 00:46:15 2009 KojiUpdateSUSRe: free swinging spectra of ETMY and ITMX

Well, I get the point now. It could be either seismic or change in the suspension Q.

The pendulum memorizes its own state for a period of ~ Q T_pend. (T_pend is the period of the pendulum)
If the pendulum Q is very high (>104), once the pendulum is excited, the effect of the excitation can last many hours.

On the other hand, in our current case, we turned on the damping once, and then turned off the damping.
Again it takes ~Q T_pend to be excited. 

In those cases, the peak height is not yet before in equilibrium, and can be higher or lower than expected. 

So, my suggestion is:
Track the peak height along the long time scale (~10hrs) and compare between the previous one and the current one.
This may indicate whether it is equilibrium or not, and where the equilibrium is.

Quote:

If such variation of the peak heights is cased by the seismic activity, it means the seismic level change by several 10 times. It sounds large to me.

 

  2376   Thu Dec 10 08:40:12 2009 AlbertoUpdateComputersFronte-ends down

I found all the front-ends, except for C1SUSVME1 and C0DCU1 down this morning. DAQAWG shows up green on the C0DAQ_DETAIL screen but it is on a "bad" satus.

I'll go for a big boot fest.

  2378   Thu Dec 10 08:50:33 2009 AlbertoUpdateComputersFronte-ends down

Quote:

I found all the front-ends, except for C1SUSVME1 and C0DCU1 down this morning. DAQAWG shows up green on the C0DAQ_DETAIL screen but it is on a "bad" satus.

I'll go for a big boot fest.

Since I wanted to single out the faulting system when these situations occur, I tried to reboot the computers one by one.

1) I reset the RFM Network by pushing the reset button on the bypass switch on the 1Y7 rack. Then I tried to bring C1SOSVME up by power-cycling and restarting it as in the procedure in the wiki. I repeated a second time but it didn't work. At some point of the restarting process I get the error message "No response from EPICS".
2) I also tried rebooting only C1DCUEPICS but it didn't work: I kept having the same response when restarting C1SOSVME
3) I tried to reboot C0DAQCTRL and C1DCU1 by power cycling their crate; power-cycled and restarted C1SOSVME. Nada. Same response from C1SOSVME.
4) I restarted the framebuilder;  power-cycled and restarted C1SOSVME. Nothing. Same response from C1SOSVME.
5) I restarted the framebuilder, then rebooted C0DAQCTRL and C1DCU, then power-cycled and restarted C1SOSVME. Niente. Same response from C1SOSVME.
 
Then I did the so called "Nuclear Option", the only solution that so far has proven to work in these circumstances. I executed the steps in the order they are listed, waiting for each step to be completed before passing to the next one.
0) Switch off: the frame builder, the C0DAQCTRL and C1DCU crate, C1DCUEPICS
1) turn on the frame builder
2) reset of the RFM Network switch on 1Y7 (although, it's not sure whether this step is really necessary; but it's costless)
3) turn on C1DCUEPICS
4) turn on the C0DAQCTRL and C1DCU crate
5) power-cycle and restart the single front-ends
6) burt-restore all the snapshots
 
When I tried to restart C1SOSVME by power-cycling it I still got the same response: "No response from EPICS". But I then reset C1SUSVME1 and C1SUSVME2 I was able to restart C1SOSVME.
 
It turned out that while I was checking the efficacy of the steps of the Grand Reboot to single out the crucial one, I was getting fooled by C1SOSVME's status. C1SOSVME was stuck, hanging on C1SUSVME1 and C1SUSVME2.
 
So the Nuclear option is still unproven as the only working procedure. It might be not necessary.
 
Maybe restating BOTH RFM switches, the one in 1Y7 and the one in 1Y6, would be sufficient. Or maybe just power-cycling the C0DAQCTRL and C1DCU1 is sufficient. This has to be confirmed next time we incur on the same problem.
  2379   Thu Dec 10 09:51:06 2009 robUpdatePSLRCPID settings not saved

Koji, Jenne, Rob

 

We found that the RCPID servo "setpoint" was not in the relevant saverestore.req file, and so when c1psl got rebooted earlier this week, this setting was left at zero.  Thus, the RC got a bit chilly over the last few days.  This channel has been added. 

 

Also, RCPID channels have been added (manually) to conlog_channels. 

  2381   Thu Dec 10 09:56:32 2009 KojiUpdatePSLRCPID settings not saved

Note: The set point C1:PSL-FSS_RCPID_SETPOINT is 37.0 on C1PSL_FSS_RCPID.adl.

Now the temp is recovering with its full speed. At some point we have to restore the value of the FSS SLOW DC as the temp change drag it up.

Quote:

Koji, Jenne, Rob

We found that the RCPID servo "setpoint" was not in the relevant saverestore.req file, and so when c1psl got rebooted earlier this week, this setting was left at zero.  Thus, the RC got a bit chilly over the last few days.  This channel has been added. 

Also, RCPID channels have been added (manually) to conlog_channels. 

 

Attachment 1: RC_TEMP.png
RC_TEMP.png
  2382   Thu Dec 10 10:01:16 2009 JenneUpdateComputersFronte-ends down

All the front ends are back up.  

Quote:

Quote:

I found all the front-ends, except for C1SUSVME1 and C0DCU1 down this morning. DAQAWG shows up green on the C0DAQ_DETAIL screen but it is on a "bad" satus.

I'll go for a big boot fest.

Since I wanted to understand once for all what's the faulting system when these situations occur, I tried to reboot the computers one by one.

1) I reset the RFM Network by pushing the reset button on the bypass switch on the 1Y7 rack. Then I tried to bring C1SOSVME up by power-cycling and restarting it as in the procedure in the wiki. I repeated a second time but it didn't work. At some point of the restarting process I get the error message "No response from EPICS".
2) I also tried rebooting only C1DCUEPICS but it didn't work: I kept having the same response when restarting C1SOSVME
3) I tried to reboot C0DAQCTRL and C1DCU1 by power cycling their crate; power-cycled and restarted C1SOSVME. Nada. Same response from C1SOSVME.
4) I restarted the framebuilder;  power-cycled and restarted C1SOSVME. Nothing. Same response from C1SOSVME.
5) I restarted the framebuilder, then rebooted C0DAQCTRL and C1DCU, then power-cycled and restarted C1SOSVME. Niente. Same response from C1SOSVME.
 
The following is the so called "Nuclear Option", the only solution that so far has proven to work in these circumstances. Execute the following steps in the order they are listed, waiting for each step to be completed before passing to the next one.
0) Switch off: the frame builder, the C0DAQCTRL and C1DCU crate, C1DCUEPICS
1) turn on the frame builder
2) reset of the RFM Network switch on 1Y7 (although, it's not sure whether this step is really necessary; but it's costless)
3) turn on C1DCUEPICS
4) turn on the C0DAQCTRL and C1DCU crate
 
One other possibility remains to be explored to avoid the Nuclear Option. And that is to just try to reset both RFM Network switches: the one in 1Y7 and the one in 1Y6.

 

  2383   Thu Dec 10 10:31:18 2009 JenneUpdateComputersFronte-ends down

Quote:

All the front ends are back up.  

Quote:

Quote:

I found all the front-ends, except for C1SUSVME1 and C0DCU1 down this morning. DAQAWG shows up green on the C0DAQ_DETAIL screen but it is on a "bad" satus.

I'll go for a big boot fest.

Since I wanted to understand once for all what's the faulting system when these situations occur, I tried to reboot the computers one by one.

1) I reset the RFM Network by pushing the reset button on the bypass switch on the 1Y7 rack. Then I tried to bring C1SOSVME up by power-cycling and restarting it as in the procedure in the wiki. I repeated a second time but it didn't work. At some point of the restarting process I get the error message "No response from EPICS".
2) I also tried rebooting only C1DCUEPICS but it didn't work: I kept having the same response when restarting C1SOSVME
3) I tried to reboot C0DAQCTRL and C1DCU1 by power cycling their crate; power-cycled and restarted C1SOSVME. Nada. Same response from C1SOSVME.
4) I restarted the framebuilder;  power-cycled and restarted C1SOSVME. Nothing. Same response from C1SOSVME.
5) I restarted the framebuilder, then rebooted C0DAQCTRL and C1DCU, then power-cycled and restarted C1SOSVME. Niente. Same response from C1SOSVME.
 
The following is the so called "Nuclear Option", the only solution that so far has proven to work in these circumstances. Execute the following steps in the order they are listed, waiting for each step to be completed before passing to the next one.
0) Switch off: the frame builder, the C0DAQCTRL and C1DCU crate, C1DCUEPICS
1) turn on the frame builder
2) reset of the RFM Network switch on 1Y7 (although, it's not sure whether this step is really necessary; but it's costless)
3) turn on C1DCUEPICS
4) turn on the C0DAQCTRL and C1DCU crate
 
One other possibility remains to be explored to avoid the Nuclear Option. And that is to just try to reset both RFM Network switches: the one in 1Y7 and the one in 1Y6.

 

 I burtrestored all the snapshots to Dec 9 2009 at 18:00.

  2385   Thu Dec 10 13:13:08 2009 JenneUpdateComputersfb40m backup restarted

The frame builder was power cycled during the morning bootfest.  I have restarted the backup script once more.

  2386   Thu Dec 10 13:50:02 2009 JenneUpdateVACAll doors on, ready to pump

[Everybody:  Alberto, Kiwamu, Joe, Koji, Steve, Bob, Jenne]

The last heavy door was put on after lunch.  We're now ready to pump.

  2387   Thu Dec 10 15:18:55 2009 JenneUpdateVACseisBLRMS

last 20 days - including the pounding from next door

Attachment 1: Untitled.png
Untitled.png
  2388   Thu Dec 10 16:51:35 2009 steveUpdateVACpumpdown will start tomorrow morning

The vacuum system is at 760 torr  All chambers with doors on and their annuloses are pumped down.

PSL output shutter is still closed. We are fully prepared to star slow pump down tomorrow.

The plan is to reach 1 torr ~ in 6 hrs  without a creating a sand storm.

  2391   Thu Dec 10 17:13:36 2009 kiwamuUpdateSUSFree swiging spectra under the atmospheric pressure

The free swinging spectra of ITMs, ETMs, BS, PRM and SRM were measured last night in order to make sure that nothing wrong have happened by the wiping.

I think there are nothing wrong with ITMs, ETMs, BS, PRM and SRM successfully.

For the comparison, Yoichi's figure in his elog entry of Aug.7 2008 is good, but in his figure somehow PRM spectrum doesn't look correct.

Anyway, compared with his past data, there are no significant changes in the spectra. For PRM which has no counterpart to compare with, its shape of spectra looks similar to any other spectra. So I think PRM is also OK. The measured spectra are attached below.

Indeed the current data are still showing smaller peak height for their pitch and yaw modes (roughly factor of 10 ).
 
Attachment 1: summary_freeswing.pdf
summary_freeswing.pdf summary_freeswing.pdf summary_freeswing.pdf summary_freeswing.pdf summary_freeswing.pdf summary_freeswing.pdf summary_freeswing.pdf
  2392   Thu Dec 10 18:27:48 2009 MottUpdateGeneralUpdated R & T Measurements

Attached are updated plots of the T&R Measurements for a variety of mirrors, and diagrams for the setup used to make the measurements.

T is plotted for the 1064 nm measurement, since these mirrors are highly reflective at 1064, and either R or R&T are plotted for the 532 nm measurement, depending on how larger the R signal is.

As with the previous set of plots, the error bars here are purely statistical, and there are certainly other sources of error not accounted for in these plots.  In general, the T measurement was quite stable, and the additional errors
are probably not enormous, perhaps a few percent.

The mirrors are:

Y1-1037-00.50CC

Y1-2037-45S

Y1-2037-45P

Y1S-1025-0

Y1S-1025-45

 

Attachment 1: Y1S-0.png
Y1S-0.png
Attachment 2: Y1S-45.png
Y1S-45.png
Attachment 3: Y45P.png
Y45P.png
Attachment 4: Y45S.png
Y45S.png
Attachment 5: Y150CC.png
Y150CC.png
Attachment 6: Setup.png
Setup.png
  2401   Fri Dec 11 17:36:37 2009 kiwamuUpdateGeneralIFO restoring plan

Alberto, Jenne, Kiwamu

 

We together will lead the IFO restoring and the following is our plan.

- - - - -|- - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -

#.0     |  measuring the free swinging spectra                     (weekend by kiwamu)   DONE

#.1     |  turn ON the PZTs for steering mirror and so on.         (Dec.14 Mon.) DONE

#. 1            |    lock around PSL  DONE

#.2     |  deal with mechanical shutter                            (Dec.14 Mon.)DONE

#.3     |  lock MCs                                                (Dec.14 Mon.)DONE

#.4     |  align the IFO                                           (Dec.15 Tue.)DONE

#.5     |  lock full IFO                                           (Dec.15 Tue.)DONE

- - - - -|- - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -

 

Thank you.

  2405   Sun Dec 13 17:43:10 2009 kiwamuUpdateSUSfree swinging spectra (vacuum)

The free swinging spectra of ITMs, ETMs, BS, PRM and SRM were measured under the vacuum-condition. The attachment are measured spectra.

It looks there are nothing wrong because no significant difference appear from the past data and the current data (under atmosperic pressure).

So everything is going well.

Attachment 1: summary_FreeSwinging_vacuum.pdf
summary_FreeSwinging_vacuum.pdf summary_FreeSwinging_vacuum.pdf summary_FreeSwinging_vacuum.pdf summary_FreeSwinging_vacuum.pdf summary_FreeSwinging_vacuum.pdf summary_FreeSwinging_vacuum.pdf summary_FreeSwinging_vacuum.pdf
  2410   Mon Dec 14 12:13:52 2009 JenneUpdateTreasureWe are *ROCKSTARS* ! IFO is back up

[Jenne, Kiwamu, Koji]

We got the IFO back up and running!  After all of our aligning, we even managed to get both arms locked simultaneously.  Basically, we are awesome. 

 This morning, we did the following:

*  Turned on the PZT High voltages for both the steering mirrors and the OMC.  (For the steering mirrors, turn on the power, then hit "close loop" on each.  For the OMC, hit Output ON/OFF).

*  Looked at the PZT strain gauges, to confirm that the PZTs came back to where they had been.  (Look at the snapshot of C1ASC_PZT_Al)

*  Locked all components of the PSL (This had already been done.)

*  Removed beam dump which was blocking the PSL, and opened the PSL mechanical shutter.  Light into the IFO!

*  Locked the Mode Cleaner.  The auto-locker handled this with no problem.

*  Confirm that light is going through the Faraday.  (Look at the TV sitting on top of MC13 tank...it shows the Faraday, and we're hitting the input of the Faraday pretty much dead-on).

*  Look at IP_ANG and IP_POS.  Adjust the steering mirrors slightly to zero the X&Y readings on IP_ANG.  This did not change the PZTs by very much, so that's good.

*  Align all of the Core Optics to their OpLev positions.

*  On the IFO_Align screen, save these positions.

*  Run the IFO_Configure scripts, in the usual order.  (Xarm, Yarm, PRM, DRM).  Save the appropriate optics' positions after running the alignment scripts.  We ended up running each alignment script twice, because there was some residual misalignment after the first iteration, which we could see in the signal as viewed on DataViewer (Either TRX, TRY, or SPOB, for those respective DoFs).

*  Restore Full IFO.

*  Watch the beauty of both arms and the central cavity snapping together all by themselves!  In the attached screenshot, notice that TRX and TRY are both ~0.5, and SPOB and AS166Q are high.  Yay!

Conclusions: 

*  The wiping may have helped.  While aligning X and Y separately, TRX got as high as ~1.08, and TRY got as high as 0.98  This seems to be a little bit higher than it was previously.

*  Since everything locked up in pretty short order, and the free swinging spectra (as measured by Kiwamu in elog 2405) looks good, we didn't break anything while we were in the chambers last week.  Excellent.

*  We are now ready for a finesse measurement to tell us more quantitatively how we did with the wiping last week.

 

Attachment 1: Jenne14Dec09_IFOlocked.png
Jenne14Dec09_IFOlocked.png
  2411   Mon Dec 14 13:08:33 2009 KojiUpdateTreasureLOCKSTARS

Good job guys. What I did was saying "I don't know", "Maybe", and "Ants...".

Now you can proceed to measurements for the visibility and the cavity pole! 

Quote:

[Jenne, Kiwamu, Koji]

We got the IFO back up and running!  After all of our aligning, we even managed to get both arms locked simultaneously.  

  2412   Mon Dec 14 13:17:33 2009 robUpdateTreasureWe are *ROCKSTARS* ! IFO is back up

 

 

Attachment 1: two-thumbs-up.jpeg
two-thumbs-up.jpeg
  2413   Mon Dec 14 14:16:14 2009 AlbertoUpdateTreasureLOCKSTARS

Quote:

Good job guys. What I did was saying "I don't know", "Maybe", and "Ants...".

Now you can proceed to measurements for the visibility and the cavity pole! 

Quote:

[Jenne, Kiwamu, Koji]

We got the IFO back up and running!  After all of our aligning, we even managed to get both arms locked simultaneously.  

 I'm going to do it right now.

  2414   Mon Dec 14 15:18:18 2009 JenneUpdatelorearmLoss script ran....results confidential

I ran the armLoss script for both Xarm and Yarm.  The results are confidential, pending the completion of Alberto's cavity pole/finesse measurement due to the 'bet' as to what the new losses are after the drag wiping.

If you're the kind of person who likes to look at their Chrismas presents, the log files with the results are in the usual place for this script: /scripts/LSC/loss-ARM-GPStime.log  (loss-Y-944865071.log and loss-X-944865946.log)

  2415   Mon Dec 14 19:33:04 2009 AlbertoUpdateGeneralArm Cavity Poles measured again after cleaning the optics last week

Last week we vented and we cleaned the main optics of the arm cavities.

I measured the frequency of the cavity poles for both the arm cavities to see how they changed (see previous elog entry 2226). These the results:

fp_X = 1616 +/- 14 Hz

fp_Y = 1590 +/- 4 Hz

The error is the statistical error that I got with the Matlab NonLinearLeastSquare fitting function.
 
I calculated the cavity pole frequencies by measuring the transfer function between a photodiode located at the end of the arms (either X or Y) and another photodiode placed after the mode cleaner. Both diodes where Thorlabs PDA255.
(Last time, I had measured that the pair of diode had a flat calibration).
 
With the SR785 I measured the transfer function by exciting the OMC_ISS_EXC input cable.
For both arms I set to 1V the excitation amplitude. I repeated the measurements for different excitation amplitudes without observing any changes.
I then fitted the data with the NonLinearLeastSquare function of matlab. The script I wrote to do that is attached to this entry in a compressed file.
The files also contains the PDF with the output plots and the data from both set of measurements performed before and after the cleaning.
The data is commented in a file called measurements.log.
 
In the end I disabled again the test switch on the ISS MEDM screen.
I disconnected the excitation cable from the OMC_ISS_EXC input cable.
I removed the photodiode that measured the Mode Cleaner transmission from the PSL clearing the way for the beam to get back to its path to the RFAM photodiode.
Attachment 1: XarmTF01_fit.pdf
XarmTF01_fit.pdf
Attachment 2: YarmTF01_fit.pdf
YarmTF01_fit.pdf
Attachment 3: ArmCavityFinesseMeasurment.tar.gz
  2416   Mon Dec 14 22:32:56 2009 KojiUpdateGeneralArm cavity loss ~ result

I like to ask someone to review the calculation on the wiki.

In the calculation, the round trip loss and the front mirror T are the unknown variables.
The end mirror T of 10ppm was assumed. (End mirror T)+(Round trip loss) is almost invariant, and T_end does not change the other results much.

Arm cavity loss measurement (Dec. 14, 2009)

X Arm:
  • Arm visibility (given): 0.897 +/- 0.005 (20 pts) (2.5%UP!!)
  • Cut off freq (given): 1616 +/- 14 [Hz] (2.1%UP!!)
  • Finesse (derived): 1206 +/- 10 (2.1%UP!!)
  • Round Trip loss (estimated): 127 +/- 6 [ppm] (28%DOWN!!)
  • Front Mirror T (estimated): 0.00506 +/- 0.00004
Y Arm:
  • Arm visibility (given): 0.893 +/- 0.004 (20 pts) (2.1%UP!!)
  • Cut off freq (given): 1590 +/- 4 [Hz] (8.2%UP!!)
  • Finesse (derived): 1220 +/- 3 (8.2%UP!!)
  • Round Trip loss (estimated): 131 +/- 6 [ppm] (37%DOWN!!)
  • Front Mirror T (estimated): 0.00500 +/- 0.00001 

Previous measurement (Oct 07, 2009 & Nov 10, 2009)

X Arm:  

  • Arm visibility (given): 0.875 +/- 0.005 (34 pts)
  • Cut off freq (given): 1650 +/- 70 [Hz]
     
  • Finesse (derived): 1181 +/- 50
  • Round Trip loss (estimated): 162 +/- 10 [ppm]
  • Front Mirror T (estimated): 0.0051 +/- 0.0002

Y Arm: 

  • Arm visibility (given): 0.869 +/- 0.006 (26 pts)
  • Cut off freq (given): 1720 +/- 70 [Hz]
     
  • Finesse (derived): 1128 +/- 46
  • Round Trip loss (estimated): 179 +/- 12 [ppm]
  • Front Mirror T (estimated): 0.0054 +/- 0.0002
  2417   Tue Dec 15 00:02:10 2009 ranaUpdatePEMNoise of the Ranger SS-1 Seismometer

I wanted to see what the noise of the Ranger seismometer should be. I used LISO and file ranger.fil (in our LISO SVN) to calculate the voltage noise referred to the input. In this model, we represent the EMF from the moving magnet in the coil as a voltage source at 'nin' which drives the coil impedance. This is the same approach that Brian Lantz uses in his noise modeling of the GS-13 (PDF is on our Ranger wiki page).

In the simulation, I used the OP27 as a placeholder for the SR560 that we use (I don't know the current noise of the SR560). To do this, I use the new 'inputnoise' feature in LISO (its in the README, but not in the manual).

You can see that we would be limited by the input current noise of the OP27. So we would do a lot better if we used an FET based readout amp like the AD743 (or equivalent) or even better using the new multi-FET readout circuit that Rich Abbott has developed. Clearly, its also silly to have a load resistance in there - I put it in because the manual says to do it, but all it does is damp the mass and reduce the size of the signal.

#  Noise sim for the Ranger SS-1 seismometer
#
#                            \
#                           | \            
#           n2- - - ----  - |  \          
#            |    |         | op1>-- n4 - r4 -- no
#           Rg   RL     n3- |  /     |           
#       n1 - |    |     |   | /      |                
#           Lg    |     |    /       |                        
#            |    |     | - - - R2 - -                    
#           nin  gnd   R1 
#                       |
#                      gnd

We previously measured the Ranger's self noise by locking it down.

The 1/f^3 noise that we see below 1 Hz is roughly consistent with the noise model: to get from my plot into meters you have to multiply by:

(1 + f)^2

----------

340 * f^2

P.S. Secret PDF handshake: You can make your non-compliant applications like LISO or DTT produce a thumbnailing PDF by using Acrobat to open the file and export it as PDF/A.

In the second attachment, I have used an OPA827 (new low-noise FET input amp from TI) as the readout amplifier. This seems like a good choice - main drawback is that Digikey backordered my OPA827s by 19 weeks!

Attachment 1: rangerx.pdf
rangerx.pdf
Attachment 2: ranger827.pdf
ranger827.pdf
  2418   Tue Dec 15 05:29:31 2009 AlbertoUpdateGeneralArm Cavity Poles measured again after cleaning the optics last week

 

 The Y arm cavity pole moved down by 130 Hz, whereas the X arm moved by only 34 Hz. I wonder if that is because Kiwamu spent much more time on cleaning ITMY than on any other optic.

  2419   Tue Dec 15 17:16:22 2009 KojiUpdateGeneralTable distance measurements

During the vent we have tried to measure the distances of the optical tables for BS-ITMX and BS-ITMY.
We need to take into account the difference between the AutoCAD drawing and the reality.

X direction distance of the table center for BS and ITMX:
84.086" (= 2135.8mm)
(This is 84.0000" in AutoCAD drawing)

Y direction distance of the table center for BS and ITMX:
83.9685" (= 2132.8mm)
(This is 83.5397" in AutoCAD drawing)

We used two scales attached each other in order to measure the distance of the certain holes on the tables.

We got more numbers that were estimated from several separated measurements.
I think they were not so accurate, but just as a record, I also put the figure as an attachment 2.

Attachment 1: Table_distance_by_metal_scale.pdf
Table_distance_by_metal_scale.pdf
Attachment 2: Table_distance_by_chambers.pdf
Table_distance_by_chambers.pdf
  2420   Tue Dec 15 21:39:34 2009 AlbertoUpdateABSLbrief summary of this afternoon's measurements
I took measurements of the open loop gain of the AbsL PLL with the old Universal PDH Box.
I Also measured the filter shape of both the new and the old PDH box.
I'm going to plot the results in a nice form tomorrow morning.
For who's interested, the PLL UGF was at 10KHz.
 
I can't lock the PLL with the new PDH box. Measuring its filter's shape, as suggested by Koji, I found out that it differs from the old one. That despite the fact that the two boxes should share the same circuit schematic. O,r at least, that is what it looks like from the schematics in the DCC.
I need to understand whether that is intentional and, if that was the case, what kind of use  Rich Abbott designed it for.
 
Tomorrow I'm going to post in the elog the filter's transfer functions too.
 
Before leaving the lab I closed the auxiliary laser's mechanical shutter.
  2421   Wed Dec 16 11:21:20 2009 AlbertoUpdateABSLUniversal PDH Box Servo Filters
Yesterday I measured the shape of the servo filter of both the old and the new Universal PDH boxes.
Here they are compared.

NewandOlfFilterTF.png

The way the filter's transfer function has been measured is by a swept sine between the "SERVO INPUT" and the "PIEZO DRIVE OUTPUT" connection on the box front panel. The spectrum analyzer used for the measurement is the SR785 and the source amplitude is set at 0.1V.

The two transfer functions are clearly different. In particular the old one looks like a simple integrator, whereas the new one already includes some sort of boost.

That probably explains why the new one is unable to lock the PLL. Indeed what the PLL needs, at least to acquire lock, is an 1/f filter.

I thought the two boxes were almost identical, at least in the filter shapes. Also the two schematics available in the DCC coincide.

Attachment 1: NewandOlfFilterTF.png
NewandOlfFilterTF.png
  2422   Wed Dec 16 11:46:25 2009 AlbertoUpdateABSLAbsl PLL Open Loop Gain

Yesterday I measured the Open Loop Gain of the PLL in the absolute length experiment. The servo I used was that of the old Universal PDH box.

The OLG looks like this:

OldBoxOLTF.png

The UGF is at 10 KHz.

  2423   Wed Dec 16 11:55:47 2009 ranaUpdateABSLUniversal PDH Box Servo Filters

 

 To me, they both look stable. I guess that the phase has to go to -180 deg to be unstable.

Why does the magnitude go flat at high frequencies? That doesn't seem like 1/f.

How about a diagram of what inputs and outputs are being measured and what the gain knob and boost switch settings are?

  2424   Wed Dec 16 20:29:08 2009 ranaUpdateCOCETM Coating study

This plot shows the Transmission for 532 and 1064 nm as a function of the thickness of the SiO2 layer.

i.e. the thickness is constrained so that the optical thickness of the SiO2 and Ta2O5 pair is always 1/2 of a wavelength.

The top layer of the mirror is also fixed in this plot to be 1/2 wave.

This plot shows the result for 17 pairs. For 16 pairs, we are unable to get as low as 15 ppm for the 1064 nm transmission.

Attachment 1: layerfrac.png
layerfrac.png
  2425   Thu Dec 17 02:57:08 2009 JenneUpdateWienerFilteringL1 DARM Static Wiener Filtered data

This is perhaps best put in the LLO elog, but I'm not yet a 'person' there, so I can't write to their elog (yet another thing for the eternal to-do list).  So for now, we're putting things here...

This isn't totally finalized, but I do want to get what I have posted before I hop on a plane in the morning.  Mostly it just needs more time to run, to make the plot longer.  Hopefully I'll be able to edit this in the morning and have a longer-duration plot. 

What's plotted:

This spectrogram shows the amplitude spectra of L1:LSC-DARM_CTRL, after being subtracted via a Static Wiener Filter.  Each spectra is normalized by the very first one, which was created from the same data that was used to determine the Wiener Filter.  The X-axis is time.  The Y-axis is frequency, and the Color/Z-axis is amplitude in dB.  I'm only looking at Science Mode time, so other times when the IFO isn't in science mode, I plot a black stripe to fill in the plot.  The start time of the plot is 83675598, which is Jul 08 2006 06:33:04 UTC. 

Why?

The idea is to see that the filter does equally well a long time after it was created, as when it was initially made.  This will help tell us how often it is useful to recompute the Wiener filters.  Less often is nice, because redoing the Wiener filters may also include remeasuring the high precision transfer functions...if the filter isn't working as well anymore it may be because the transfer function has changed ever so slightly. 

How the plot is created / the background story:

I use one hour of DARM_CTRL data and the following seismometer channels to create an optimal Wiener Filter (pem indicates L0:PEM- , sei indicates L1:SEI- , and lsc indicates L1:LSC- ) :

chans = {[pem 'EX_SEISX'],...
         [pem 'EX_SEISY'],...
         [pem 'EX_SEISZ'],...
         [pem 'EY_SEISX'],...
         [pem 'EY_SEISY'],...
         [pem 'EY_SEISZ'],...
         [pem 'LVEA_SEISX'],...
         [pem 'LVEA_SEISY'],...
         [pem 'LVEA_SEISZ'],...
         [sei 'LVEA_STS2_X'],...
         [sei 'LVEA_STS2_Y'],...
         [sei 'LVEA_STS2_Z'],...
         [sei 'ETMX_STS2_X'],...
         [sei 'ETMX_STS2_Y'],...
         [sei 'ETMX_STS2_Z'],...
         [sei 'ETMY_STS2_X'],...
         [sei 'ETMY_STS2_Y'],...
         [sei 'ETMY_STS2_Z'],...
         [lsc 'DARM_CTRL']};

I then apply this one filter to ten minute chunks of science mode data, for some long period of time.  The game plan is to have a month long plot, but it takes a while to fetch all of the data in separate 10min intervals (~45sec per iteration, times ~3000 iterations), so this plot isn't a full month.  Even if I don't get a chance to plot a full month by Thursday morning, it'll go up here within the next few days. The particular times chosen have the most science mode data within a 30 day period.  I can easily run the code for some other time, if there is a known time (or season) which might be more interesting.  For the spectrogram plot, I then normalize each amplitude spectra by the first one, which comes from the first ten minutes in the hour which was used to make the filter.  This makes it easier to see how the filter's efficacy changes over time.

The analogous analysis for Hanford is in the 40m elog: 1606.  The Hanford stuff in the elog has some cool BLRMS plots also, but I'm not sure that they're so helpful when I only have a few days of L1 data so far.  I'll do those and add them later.

Conclusions:

I can't really say anything yet about the long-term efficacy of a Wiener Filter for LLO yet, since my code hasn't finished filtering my one month of S5 L1 data.  It definitely looks like (so far) that there was a big seismic event around the (arbitrarily defined) 'Day 4'. 

Attachment 1: L1darmCompPlot_17Dec2009_4daysLong.png
L1darmCompPlot_17Dec2009_4daysLong.png
  2426   Thu Dec 17 07:47:29 2009 JenneUpdateWienerFilteringL1 DARM Static Wiener Filtered data

This surface plot is the same as the previous one, with a little more data than I had previously. 

This time around, I also include the "BLRMS" plots for this data.  The first one takes each residual and normalizes it by the DARM_CTRL signal at that time, separates the spectra into bands, and integrates underneath the spectra within that band.  The second one is the raw DARM_CTRL signal's spectra at each time, and integrates under the spectra for each band, and the third BLRMS plot does the same thing for the residuals.  Unfortunately, these plots don't have the same handy black stripe during time which I don't analyze that the spectrogram utilizes.

From the second BLRMS plot we can see that the large red splotch in the spectrogram is due to higher noise in the DARM spectrum, and that (by looking at the Ratio BLRMS plot) the Wiener filter still does a pretty good job during this time.  I expect that for later times when the seismic (or something) event is gone, the Wiener filter will continue performing almost as well as it had been initially.

Again, once the script finishes applying the filter to the many ten minute chunks (the huge time drain is the data fetching, so this shouldn't be a limiting factor for using Wiener filters online), I'll post a final plot.

Attachment 1: L1darmComp_17Dec2009_6day_residualsNormSurfacePlot.png
L1darmComp_17Dec2009_6day_residualsNormSurfacePlot.png
Attachment 2: L1darmComp_17Dec2009_6day_ratioBLRMS.png
L1darmComp_17Dec2009_6day_ratioBLRMS.png
Attachment 3: L1darmComp_17Dec2009_6day_rawBLRMS.png
L1darmComp_17Dec2009_6day_rawBLRMS.png
Attachment 4: L1darmComp_17Dec2009_6day_residualsBLRMS.png
L1darmComp_17Dec2009_6day_residualsBLRMS.png
ELOG V3.1.3-