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New entries since:Wed Dec 31 16:00:00 1969
ID Date Author Type Categorydown Subject
  760   Tue Jul 29 21:04:55 2008 SharonUpdate OSEM's Power Spectrum
From 16:30 this afternoon
Attachment 1: ITMY2.JPEG
ITMY2.JPEG
Attachment 2: ITMY.JPEG
ITMY.JPEG
Attachment 3: ITMX2.JPEG
ITMX2.JPEG
Attachment 4: ITMX.JPEG
ITMX.JPEG
Attachment 5: ETMY2.JPEG
ETMY2.JPEG
Attachment 6: ETMY.JPEG
ETMY.JPEG
Attachment 7: ETMX2.JPEG
ETMX2.JPEG
Attachment 8: ETMX.JPEG
ETMX.JPEG
  765   Wed Jul 30 12:36:19 2008 SharonUpdate Weekly update
This week included many computer's issues. I tested Alex's new C code (the one that saves the FIR coefficients and restores them when you start running the code again). Seems there is an improvement in the adaptation time, but not a significant one (more details on the coming report). I had to recompile simulink and the FB whenever I wanted to find a solution for taking the record of those coefficients. This is so I could simulate the adaptive filter with a regular IIR filter and compare the two.
After Rob tried to help and it seems to be an impossible to a huge hassle mission, we thought of a different method to do this. I re-compiled the old simulink file and restored the .ini file and all should be back in place. Instead of finding the FIR coefficients, I am going to use one noise source in the adaptive filter, stop the adaptation (by setting mu and tau to 0), and put excitation instead of the noise signal. The transfer function I will get between the exc. and MC1_IN1 is the filter I am looking for.

Also seems that whenever I get the MC unstable, and the adaptive code stops itself, it doesn't come back. Setting the reset flag to a different number (anything other than 0) and pressing the reset button will get it working again, but the CPU will always flip and the ASS computer needed a restart. Still haven't found a problem in the C code, but that's the plan. Moreover, I want to change Alex's code, so that instead of starting from zero like in Matt's code, or starting from the old coefficients like in Alex's, it is going to calculate a Wiener Filter as the first set of coefficients. This will hopefully reduce the adaptation time.

I have also been working on my progress report, and stood in line for the MC... Still standing...
  814   Fri Aug 8 11:04:34 2008 SharonUpdate MCL Wiener filter
I took some old data from Rana and converted the units of the Weiner filter to m/m so to make the effect of the seismometer and accelerometers more obvious.

The data is in counts, and so to convert to m this is what I did:

%%% MC_L calibration
v_per_counts = 5/32768;
v_per_v = 3;
amp_per_N = 1/0.064;

%%% Accelerometers calibration
v_per_counts_acc = 61.045e-6;
g_per_v = 9.8/100;

%%% Seismometer calibration
v_per_counts_seis = 61.045e-6;
m_per_s_per_s_per_volt = 9.8/100;
m_per_v_per_s = 1/345;



for jj=1:6
hfmatm(:,jj)=hfmat(:,jj).*(v_per_counts.*v_per_v.*amp_per_N.*f)./(v_per_counts_acc*g_per_v); %%% accelerometers' data
end
hfmatm(:,7)=hfmat(:,7).*(v_per_counts.*v_per_v.*amp_per_N)./(v_per_counts_seis*m_per_v_per_s); %%% Seismometer data
Attachment 1: m_per_m.png
m_per_m.png
  841   Fri Aug 15 16:45:43 2008 SharonUpdate Converting from FIR to IIR
I have been looking into different techniques to convert from FIR to IIR. This is so we can see how effective the adaptive FIR filter is in comparison to an IIR one with fewer taps.
For now I tried 2 matlab functions: Prony and stmcb (which works on LMS method).
I used the FIR wiener code, MC1_X, (c1wino) and applied the FIR to IIR algorithm.
Seems like the stmcb one works a bit better, and that there isn't much effect for having 1000 and not 400 taps.

Will keep updating on more results I have, and hopefully have the MC in time to actually check this live.
Attachment 1: fir2iir50.png
fir2iir50.png
Attachment 2: fir2iir400.png
fir2iir400.png
Attachment 3: fir2iir1000.png
fir2iir1000.png
  850   Tue Aug 19 10:36:34 2008 SharonUpdate Calibrating accelerometers
I took apart the accelerometers near MC1 and MC2.
The 2 sets of 3 accelerometers are now covered by a box on the floor. Please try not to move them... I will place it all back once I am done calibrating.
  854   Tue Aug 19 17:00:19 2008 SharonUpdate Wiener TF calibration - update
This is an update for post 814

I added the calibration gains I got for the accelerometers (I realize I am just calibrating the accelerometers to themselves and this is not m/m exactly since we don't really know which accelerometer is doing exactly what we want it to do. However, since we are talking on relative small numbers, this shouldn't really change much).


I also added another missing gain for the seismometer. Rana has previously installed a 4300 ohm resistor in the seismometer, which changed the gain to 4300/(4300+5000) = 0.46 (this is from the manual). Moreover, there is a gain of 100 on the SR560. This comes up to an extra gain of 46, meaning multiplying the seismometer's counts by 1/46.
Attachment 1: m_per_m.png
m_per_m.png
  855   Tue Aug 19 17:15:34 2008 SharonUpdate MEDM
I plugged in the gains I got for the accelerometers in the accelerometers' filters in the PEM screen of the adaptive filter
  863   Wed Aug 20 17:02:01 2008 SharonUpdate More FIR to IIR
I tested another method for converting from FIR to IIR other than the 2 mentioned in post 841.
I got this one from Yoichi, called poles fitting, you can read about it more if you want at: http://www.rssd.esa.int/SP/LISAPATHFINDER/docs/Data_Analysis/DA_Six/Heinzel.pdf.

Seems it's not doing much good for us though.

I am attaching a PDF file with the plots, which have N=50,100,600,1000, respectivaly.
Attachment 1: polefit1.pdf
polefit1.pdf polefit1.pdf polefit1.pdf polefit1.pdf
  870   Fri Aug 22 13:58:39 2008 SharonSummary Trend of the Wiener TF
In order to understand if we really need an adaptive filter, I used old data of MC_L and the accelerometers and seismometer to see if the Wiener (ideal) TF between MC_L and the others really changes all the time.
Two tests I made:
  • Compare the TF after different segments of time, starting from the same point. Meaning, measuring the TF after 5,10,15,20... minutes, looking when and if the TF stablizes (stops changing).
  • Compare the TF between same-length segments, from different times. Meaning, comparing for example 2 segments of 10 minutes taken from different times.

Results:
  • As you can see in the attached PDF, the changes start being minor after 200,000 data points, which correspont to 200,000/256 s, which is approximately 13 minutes.
    If you look at the PDF file, it is arranged from shorter times to longer in the order of: 3, 6, 13, 26 and 39 minutes.

  • As expected, the TF between different segmants of the same length is not completely the same. Again, you can look at the attached PDF.
    Sorry the titles are the same. Each 2 consecutive pages represent the same length of segment in different times. The order of segment's lengths is: 3, 13, 26 and 39 minutes

How do I explain what's going on?

Since the Wiener filter finds the correlation matrix between the data and the noise signals, it will maintain some kind of familiar shape when we don't add a significant amount of unusual data. I am assuming that if I had looked at longer time periods, we could see a more significant change in the TF in time. When looking at different times, the average noise is likely to be different which can explain the change in the correlation matrix and the TF.

To sum up

I think we should give adaptive filtering a go.
Attachment 1: Same_start_time1.pdf
Same_start_time1.pdf Same_start_time1.pdf Same_start_time1.pdf Same_start_time1.pdf Same_start_time1.pdf
Attachment 2: same_length.pdf
same_length.pdf same_length.pdf same_length.pdf same_length.pdf same_length.pdf same_length.pdf same_length.pdf same_length.pdf
  916   Wed Sep 3 18:45:01 2008 AlbertoConfiguration PD3 gain
Alberto, Yoichi,

We found that the PD3 servo was unstable with a gain of 1, so we switched it to 0.5
  1442   Mon Mar 30 12:29:17 2009 YoichiConfiguration MC1 glitches not seen during the weekend
The attached is the MC trend for the past 12 hours.
There is no MC1 glitches in the OSEM signals. Moreover, the total amplitude of the drift is smaller than it used to be (now the amplitude is less than 100 but it used to be a few hundreds).
There still is a small step in the OSEM signals at around 6AM this morning, but the amount of the jump is very insignificant.
The cause of the glitch in the TMP1, DRUM1 and APTEMP (LL, UL and UR coils respectively) at 7AM is not known.
Since the MC1 has been behaving OK during the weekend, I removed the probes from the MC1 coil driver board and locked the MC.
Hopefully the replacement of the broken connector fixed the problem, but I'm not sure.
Attachment 1: MC_drift.pdf
MC_drift.pdf
  1556   Thu May 7 17:59:23 2009 AlbertoConfiguration MC WFS
This afternoon the MC could not get locked.
I first checked the Osems values at the MC mirrors and compared them to the trend of the last few hours. That showed that the alignment of the mirrors had slightly changed. I then brought each mirror back to its old alignment state.
 
That let the LSC loop lock the MC, although the reflected power was still high (1.5V) and the WFS control wouldn't engage.
 
Since earlier during the day I was working on the AS table, it is possible that I inadvertently hit the MC REFL beam splitter misaligning the beam to the MC WFS.
To exclude that there was a problem in the suspensions, before touching the WFS, I checked that the cables at the MC's ends and those going to the ADC in the rack were well pushed in.
 
Then I proceeded in centering the beam on both the WFS, balancing the power over the QPDs.
 
In the end the MC could lock again properly.
 
  1739   Mon Jul 13 16:59:10 2009 ZachUpdate GigE Phase Camera

Today, I moved the router from on top of the PSL into the control room in order to perform dark field tests on the GC650 (which I also moved).  The GC750 along with the lens that was on it and the mount it was on has been lent to Ricardo's lab for the time being.  I successfully triggered the GC650 externally and I also characterized the average electronic noise.  For exposure times less than 1 microsecond, the average noise contribution appears to be a constant 15 on a 12-bit scale.

  1797   Mon Jul 27 14:43:34 2009 ChrisUpdate Photodetectors

I found two ThorLabs PDA55 Si photodetectors that says detect visible light from DC to 10MHz that I'm going to use from now on.  I don't know how low of a frequency they will actually be good to.

  1907   Fri Aug 14 18:33:02 2009 ClaraUpdate Record of Accelerometer and Seismometer Movements

Rather than make a new elog post every time I move something, I'm going to just keep updating this Google spreadsheet, which ought to republish every time I change it. It's already got everything I've done for the past week-ish. The spreadsheet can be accessed here, as a website, or here, as a pdf. I will still post something nightly so that you don't have to search for this post, but I wanted to be able to provide more-or-less real-time information on where things are without carpet-bombing the elog.

  2984   Tue May 25 17:04:37 2010 KevinUpdate Beam Profile After Mode Cleaner

I fit the data from the beam profile that Jenne measured on 5/21/2010. The distances are measured from halfway between MC1 and MC3 to the beam scanner. The fits give the following where w0 is the waist size and z0 is the distance from the waist to halfway between MC1 and MC3.

For the horizontal profile:

reduced chi^2 = 0.88

z0 = (1 ± 29) mm

w0 = (1.51 ± 0.01) mm

For the vertical profile:

reduced chi^2 = 0.94

z0 = (673 ± 28) mm

w0 = (1.59 ± 0.01) mm

I calculated the radius of curvature of MC2 using these values of w0:

horizontal: (16.89 ± 0.06) m

vertical:   (17.66 ± 0.07) m

For this calculation, I used the value of (13.546 ± .0005) m for the length of the mode cleaner measured on 6/10/2009. The specification for the radius of curvature of MC2 is (18.4 ± 0.1) m.

In the following plots, the blue curve is the fit to the vertical beam radius, the purple curve is the fit to the horizontal beam radius, * denotes a data point from the vertical data, and + denotes a data point from the horizontal data.

Attachment 1: mcfit.png
mcfit.png
Attachment 2: mcerrors.png
mcerrors.png
  3027   Tue Jun 1 18:39:59 2010 NancyUpdate Lead spheres for the seismographs

 

the lead spheres that were placed below the granite slab have been flattened by hammering to have lesser degree of wobbling of the slab.

the height of each piece, and the flatness of their surfaces was checked by placing another slab over them and checking by the spirit level.

P6010170.JPG

P6010166.JPG

P6010164.JPG

 

  3168   Wed Jul 7 12:45:00 2010 nancyUpdate Weekly Update

Wednesday after the meeting - Started report, learnt mode cleaner locking from Kiwamu and Rana, saw how to move optics on the tables with Rana and kiwamu.

Thursday - Made the report

Tuesday - report.

Today - am trying locking the MC with kiwamu's help to see the WFS signals and also to start characterizing the QPD.

  3560   Sun Sep 12 23:02:53 2010 valeraUpdate PMC mode matching

Kiwamu and I found that the first lens in the PMC mode matching telescope was mislabeled. It is supposed to be PLCX-25.4-77.3-C and was labeled as such but in fact it was PLCX-25.4-103.0-C. This is why the PMC mode matching was bad. We swapped the lens for the correct one and got the PMC visibility of 82%. The attached plot shows the beam scans before and after the PMC. The data were taken with the wrong lens. The ABCD model shown in the plot uses the lens that was there at the time - PLCX-25.4-103.0-C. The model for the PMC is just the waist of 0.371 mm at the nominal location. The snap shot of the ABCD file is attached. The calculation includes the KTP for FI and LiNb for EOM with 4 cm length. The distances are as measured on the table.

Attachment 1: pmc.pdf
pmc.pdf
Attachment 2: pmc-abcd.tiff
  3561   Sun Sep 12 23:16:52 2010 valeraUpdate FSS mode matching

The attached plot shows the beam scans of the beam leaking from the back mirror of the PMC to the BS cube that first turns the S-pol beam 90 deg to the AOM and then transmits the AOM double passed and polarization rotated P-pol beam to the reference cavity. The beam from the PMC is mode matched to the AOM using a single lens f=229 mm. The ABCD file is attached. The data were taken with VCO control voltage at 5 V. We then reduced the voltage to 4 V to reduce the astigmatism. Tara has the data for the beam scan in this configuration in his notebook.

The beam from AOM is mode matched to the reference cavity using a single lens f=286.5 mm. The ABCD file is attached.

Attachment 1: fss.pdf
fss.pdf
Attachment 2: fssaom-abcd.tiff
Attachment 3: fssrc-abcd.tiff
  3562   Mon Sep 13 00:19:32 2010 ranaUpdate VCO Driver Output power v. slider control voltage

I measured the RF power output of the VCO Driver box as a function of slider value. I measured using the Gigatronics Handheld power meter and connected to the AOM side of the cable after the white Pasternak DC block.

* at low power levels, I believe the waveform is too crappy to get an accurate reading - that's probably why it looks non-monotonic.

* the meter has a sticker label on it saying 'max +20 dBm'. I went above +20 dBm, but I wonder if maybe the thing isn't linear up there...

Attachment 1: vco.png
vco.png
  3579   Wed Sep 15 19:29:13 2010 valeraSummary PSL power budget
 Location  Power (mW)
 NPRO - after HWP  252
 Rejected by input FI polarizer  38
 After output FI polarizer  175
 Into PMC  164
 PMC reflected  37
 PMC transmitted  71
 PMC leakage  1.5
 After PMC TRANS PD/Camera BS

 1.2

 After RefCav EOM  1.1
 Into RefCav  0.3

 Notes:

- NPRO injection current 1.0 A

- PMC losses ~32%

- FSS AOM diffraction efficiency ~52%

  3580   Fri Sep 17 01:36:14 2010 valeraUpdate PMC line width

The attached plots show the PMC cavity line width measurement with 1 mW and 160 mW into the PMC. The two curves on each plot are the PMC transmitted power and the ramp of the fast input of the NPRO. The two measurements are consistent within errors - a few %. The PMC line width  3.5 ms (FWHM) x 4 V / 20 ms (slope of the ramp) x 1.1 MHz / V (NPRO fast actuator calibration from Innolight spec sheet) = 0.77 MHz.

Here is the output of the calculation using Malik Rakhmanov code:

 

modematching =  8.4121e-01

transmission1 =   2.4341e-03

transmission2 =   2.4341e-03

transmission3 =   5.1280e-05

averageLosses =  6.1963e-04

visibility =  7.7439e-01

Here are the inputs for the calculation in the param.m:

 

fw = 0.77e6;                % width of resonance (FWHM) in Hz

Plas = 0.164;                % power into the PMC in W

 

% the following number refer to the in-lock cavity state

 

Pref = 0.037;                % reflected power in W

Ptr = 0.0712;                 % transmitted power in W

Pleak = 0.0015;              % power leaking from back of PMC in W

 

 

Attachment 1: TEK00009.PNG
TEK00009.PNG
Attachment 2: TEK00010.PNG
TEK00010.PNG
  3897   Thu Nov 11 15:27:43 2010 valera, steveConfiguration ISS AOM installed

 We installed the ISS AOM in the PSL. The AOM was placed right after the EOM. The beam diameter is ~600 um at the AOM. The AOM aperture is 3 mm.

We monitored the beam size by scanning the leakage beam through the turning mirror after the AOM. The beam diameter changed from 525 um to 515 um at a fixed point. We decided that the AOM thermal lensing is not large enough to require a  new scan of the mode going into the PMC and we can proceed with PMC mode matching using the scan that was taken without the AOM (to be posted).

  4317   Thu Feb 17 22:51:04 2011 josephb, valeraSummary dither alignment model

We made a model for the dither angular stabilization system c1ass.mdl. The attached file shows the diagram.

The idea is to dither a combination of 6 optics (ETMs, ITMs, PZTs) at different frequencies and demodulate three PDs (TRX, TRY, REFL11I). Then form the DOFs from demodulted signals, filter, and send each DOF to a combination of optics.

This is enough to get started with arm cavities alignment (we may need to add the BS for the Y arm). More optics and PD can be added as they become available and/or needed.

The DAC for the fast PZT  are not connected and have to be commissioned.

Attachment 1: ass-model.png
ass-model.png
  4335   Tue Feb 22 00:18:47 2011 valeraConfiguration c1ioo and c1ass work and related fb crashes/restarts

I have been editing and reloading the c1ioo model last two days. I have restarted the frame builder several times. After one of the restarts on Sunday evening the fb started having problems which initially showed up as dtt reporting synchronization error. This morning Kiwamu and I tried to restart the fb again and it stopped working all together. We called Joe and he fixed the fb problem by fixing the time stamps (Joe will add details to describe the fix when he sees this elog).

The following changes were made to c1ioo model:

- The angular dither lockins were added for each optics to do the beam spot centering on MC mirrors. The MCL signal is demodulated digitally at 3 pitch and 3 yaw frequencies. (The MCL signal was reconnected to the first input of the ADC interface board).

- The outputs of the lockins go through the sensing matrix, DOF filters, and control matrix to the MC1,2,3 SUS-MC1(2,3)_ASCPIT(YAW) filter inputs where they sum with dither signals (CLOCK output of the oscillators).

- The MCL_TEST_FILT was removed

The arm cavity dither alignment (c1ass) status:

- The demodulated signals were minimized by moving the ETMX/ITMX optic biases and simultaneously keeping the arm buildup (TRX) high by using the BS and PZT2. The minimization of the TRX demodulated signals has not been successful for some reason.

- The next step is to close the servo loops REFL11I demodulated signals -> TMs and TRX demodulated signals -> combination of BS and PZTs.

The MC dither alignment (c1ioo) status:

- The demodulated signals were obtained and sensing matrix (MCs -> lockin outputs) was measured for pitch dof.

- The inversion of the matrix is in progress.

- The additional c1ass and c1ioo medm screens and up and down scripts are being made.

  4339   Tue Feb 22 23:11:42 2011 valeraUpdate new medm screens: C1ASS.adl and C1MCASS.adl
Attachment 1: C1MCASS.jpeg
C1MCASS.jpeg
Attachment 2: C1ASS.jpeg
C1ASS.jpeg
  4345   Wed Feb 23 16:34:42 2011 valeraConfiguration pmc lens staged

I put the PMC last mode matching lens (one between the steering mirrors) on a translation stage to facilitate the PMC mode matching.

Currently 4% of incident power is reflected by the PMC. But the reflected beam does not look "very professional" on the camera to Rana - meaning there is too much TEM20 (bulls eye) mode in the reflected beam.

I locked the  PMC  on bulls eye mode and measured  the ratio of the TEM20/TEM00 in transmission to be 1.3%. Thus the PMC mode matching is ~99% and the incident beam HOM content is ~3%.

While working on the PMC I found that the source of PMC "blinking" is not the frequency control signal from MC to the laser (the MC servo was turned off) but possibly some oscillation which could be affected even by a small change of the pump current 2.10 A to 2.08 A. I showed this behaviour to Kiwamu and we decided to leave the the current at 2.08 A for now where things look stable and investigate later.

Attachment 1: PMCrefl.JPG
PMCrefl.JPG
Attachment 2: P1070438.JPG
P1070438.JPG
Attachment 3: P1070439.JPG
P1070439.JPG
  4625   Wed May 4 13:51:51 2011 valeraConfiguration Intermittent MC3 UL PD signal

The attached plot shows the 30 day trend of the MC3 UL PD signal. The signal dropped to zero at some point but now it is close to the level it was a few weeks ago. There still could be a problem with the cable.

The rest of the MC1,2,3 PD signals looked ok.

Attachment 1: mc3ulpdmon.pdf
mc3ulpdmon.pdf
  4627   Wed May 4 15:22:39 2011 kiwamuUpdate Re: Intermittent MC3 UL PD signal

I went push all the possible connectors for the MC3 shadow sensors including the SCSIs, flat cables and satellite box.

Also I put screws on them so that they won't become loose any more.

As a result UL_PDMON dropped from 0.6 V to 0.490 V and it becomes stable so far.

I didn't strain relief the cables but we must do it at some point before going into the full locking test.

Quote from #4625

The attached plot shows the 30 day trend of the MC3 UL PD signal. The signal dropped to zero at some point but now it is close to the level it was a few weeks ago. There still could be a problem with the cable.

The rest of the MC1,2,3 PD signals looked ok.

 

  4959   Mon Jul 11 10:10:31 2011 IshwitaConfiguration AA board

The AA board shown in attachment 1 will be used in the seismometer hardware setup. A cartoon of this setup is shown in attachment 2.

BNC connectors are required for the seismometer breakout boxes. So the four-pin LEMO connectors present in the AA board were removed and panel mount BNC connectors were soldered to it. Red and blue colored wires were used to connect the BNC connectors to the board. Red wire connects the center of the BNC connector to a point on the board and that connection leads to the third leg (+IN) of the IC U### and the blue wire connects the shield of the BNC connector to the second leg (-IN) of the IC U###.

All the connections (including BNC to the AA board and in the AA board to all the filters) were tested using a multimeter by the beeping method and it was found that channel 10 (marked as C10) had a wrong connection from the point where the red wire (+ve) was connected to the third leg (+IN) of IC U91  and channel 32 (marked as C32) had opposite connections meaning the blue wire is connected to the third leg (+IN) of IC U311 and red wire is connected to the second leg (-IN) of IC U311.

Attachment 1: P7080305.JPG
P7080305.JPG
Attachment 2: seismometers.png
seismometers.png
  4999   Wed Jul 20 11:42:47 2011 Ishwita, ManuelUpdate Weekly summary
  • We gave a white-board presentation on derivation of formula for optimum Wiener filter coefficients and wrote a latex document for the same. relevant elog entry
  • We enjoyed drilling the cover of the AA board and fixing it.
  • The AA board was fixed on rack 1X7 with Jenne's help. relevant elog entry
  • We tried writing a simulation for the transfer function of the stacks in Matlab. Once we get some satisfying results, we will post it on the elog.
  • We started reading the book 'Digital Signal Processing - Alan V. Oppenheim / Ronald W. Schafer' and are still reading it. We also tried watching lecture videos on z-transform...
  5015   Thu Jul 21 23:36:51 2011 JennyUpdate Fitting beam waist with MATLAB

I am starting work on the PSL table at the 40m. My goal is to lock the laser coming from the nearby table to the FP cavity and get a measurement of the response to a temperature step on the surrounding can.

I have to mode match the beam to the cavity. Specifically, I have to mode match to the beam coming from the PMC through the EOM to the polarizing beam splitter. Yesterday David and I measured the beam width at various distances (from a particular lens through which the beam traveled), and I fit that data using MATLAB to find the beam's waist size and location. However, I'm not convinced that the fit is any good, since we only took measurements at five spots and they had large error bars.

 

z (mm) 2w_vert (mm) 2w_horiz (mm)
180 4.68 3.38
230 4.64 3.49
305 4.68 3.47
370 5.1 3.81
510 5.5 4.17

Here is the fit I obtained using fminsearch. The horizontal beam width measurements were smaller than the vertical width measurements, suggesting that the incoming beam was elliptical. I fit the data for each set of measurements separately and got two waist locations. The red trace is the fit for the horizontal width and the blue represents the vertical width of the beam. Averaging the two fitted waist locations and sizes gives

vert z_0= -1760 mm (waist location)

horiz z_0= -1540 mm (waist location)

vert w_0 = 0.286 mm (waist size)

horiz  w_0 = 0.275 mm (waist size)

avg z_0= -1650 mm

avg w_0 = 0.281 mm

 

twobeamfit2.jpg

Here is the code I used:

I defined the function spotsize.m and then made a function gaussbeam.m that called it with input parameters and returned the least squares error. I then wrote another function twobeamfits.m that ran fminsearch to minimize the least squares error and made the above plot. I've pasted the code below.

spotsize

function omega = spotsize(z_0, w_0, z)
lambda=0.001064;
omega=w_0*(1+(lambda*(z-z_0)/(pi*w_0^2)).^2).^(1/2);

 

gaussbeam

function sse = gaussbeam(params,xvals,yvals)

%This f'n takes as its inputs
%three parameters (w_0, z_0, and lambda),
%a vector of x-values (distances),
%and an associated vector of y-values (spotsizes),


%It then generates a vector of fitted y-values by applying
%an exponential approach function (single pole), with the given parameters,
%to the x-values.

%It then returns the sum of the squares of the entries of the difference
%between the fitted y-vector and the actual y-vector

z_0=params(1);
w_0=params(2);
fityvals=spotsize(z_0, w_0, xvals);

error=(fityvals - yvals);% .*xvals;
% sse stands for sum of squares error
sse=sum(error.^2);

 

twobeamfits

function [outputs] = twobeamfits(guesses, dists, vert, horiz)


%This f'n takes as its inputs
%two starting guess parameters (w_0 and z_0),
%a vector of distances (x-values),
%and two associated vectors of measured beam radii,

%the radius measured along the vertical axis

%and the radius measured along a horizontal axis (y-values).

%It then calls the gaussbeam f'n for each set of y-values and minimizes its output (sum of squares error)
%using the fminsearch f'n. It outputs the fit parameters it settles on.

%It then plots the input data, the fitted curves, and the residuals


fminopts=optimset('TolFun',1e-6,'MaxIter', 100000);
vertparams=fminsearch(@gaussbeam,guesses,fminopts,dists,vert);
fitvert=spotsize(vertparams(1), vertparams(2), dists);
resid1=(vert-fitvert)./vert;
spoterror=[.1, .1, .1, .1, .1]; %uncertainties, all in mm

fminopts=optimset('TolFun',1e-6,'MaxIter', 100000);
horizparams=fminsearch(@gaussbeam,guesses,fminopts,dists,horiz);
fithoriz=spotsize(horizparams(1), horizparams(2), dists);
resid2=(horiz-fithoriz)./horiz;


points=linspace(-2000,1000,1000);
figure(1)
hold off
clf
subplot(2,1,1)
hold on
errorbar(dists, vert, spoterror, 'x')
grid
errorbar(dists, horiz, spoterror, 'r*');
plot(points,spotsize(vertparams(1), vertparams(2), points));
plot(points,spotsize(horizparams(1), horizparams(2), points),'r');
xlabel('Distance z (mm)')
title('Gaussian Beam Fits')
ylabel('Spotsize w (mm)')
legend('Vertical Spotsize','Horizontal Spotsize','Vertical Fit',...
    'Horizontal Fit','Location','SouthEast')
hold off

subplot(2,1,2)
plot(dists,resid1,'x')
hold on
plot(dists,resid2,'r*');
xlabel('Distance (z)')
title('Residuals')
ylabel('Fractional Difference')
legend('Vertical Fit Residuals','Horizontal Fit Residuals',...
    'Location','SouthEast')
grid

outputs=[vertparams horizparams];

 

 

 

Later on I may repeat some measurements and try to gain more certainty in my fit. In the mean time I will use this beam profile for mode matching. 

 

  6282   Wed Feb 15 11:34:01 2012 steveUpdate under the shouth end optical table

I added an U channel based bottom shelf at the south end today.

Attachment 1: P1080535.JPG
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  6571   Thu Apr 26 09:22:17 2012 steveUpdate under the east end optical table

Quote:

I added an U channel based bottom shelf at the south end today.

 I'm working on similar shelf at ETMY.  Precondition: NPRO in bypass mode, heater for doubling in bypass........since power outage?  Optical level servo turned off.......

U-channel based shelf in place.  Oplev servo is back on at 11:15am    The table may moved.  The oplev return is missing the quad by a few milimeter.

  6878   Wed Jun 27 11:27:49 2012 LizUpdate First Week Update!

This week, the other SURF students and I got acquainted with the caltech campus, LIGO 40m lab and the expectations of the SURF program.  We went to a lot of safety meetings and lectures that established a framework for the jobs we will be doing over the course of the summer.  I went on several tours of the 40m interferometer (one each with Jenne, Jamie and Steve) to get an overview of the layout and specifics of the setup.  I read parts of R. Ward and A. Parameswaran's theses and Saulson's book in order to prepare myself and gain a broader understanding of the purpose of LIGO.

I also began working in Python this week, primarily graphing PSDs of data from the C1:SUS-ETMY_SENSOR_LR, C1:SUS-ETMY_SENSOR_LL, C1:SUS-ETMY_SENSOR_UR, and C1:SUS-ETMY_SENSOR_UL channels.  I will eventually be using Python to generate the plots for the summary pages, so this is good practice.  The code that I have been working on can be found in /users/elizabeth.davison/script5.py.  Additionally, I have been going through the G1 summary pages and attempting to understand the plots available on them and the code that is available.

My plans for the upcoming week begin with modifying my code and potentially calibrating the channel data so that it is in units of length instead of counts.  I will also access the code from the G1 pages and go over it in depth, hopefully gaining insight into the structure of the website.

  7164   Mon Aug 13 19:29:10 2012 ManasaSummary Ringdown measurements

I tried to make ringdown measurements at the IMC using the DC falling edge as the trigger. Input to the MC was switched off by changing the polarity of the MC servo. But it does not seem to give the needed data as there seem to be several DC falling edges as soon as the polarity is switched. We should think about a better trigger or try to setup data recording from the oscilloscope seamlessly.

Also an ethernet cable has been connected to the router from the oscilloscope at the MC trans, but has not been set up to record data yet.

  7256   Thu Aug 23 12:17:39 2012 ManasaUpdate IMC Ringdown

The ringdown measurements are in progress. But it seems that the MC mirrors are getting kicked everytime the cavity is unlocked by either changing the frequency at the MC servo or by shutting down the input to the MC. This means what we've been observing is not the ringdown of the IMC alone. Attached are MC sus sensor data and the observed ringdown on the oscilloscope.  I think we need to find a way to unlock the cavity without the mirrors getting kicked....in which case we should think about including an AOM or using a fast shutter before the IMC.

P.S. The origin of the ripples at the end of the ringdown still are of unknown origin. As of now, I don't think it is because of the mirrors moving but something else that should figured out.

Attachment 1: mozilla.pdf
mozilla.pdf
Attachment 2: MC_sus.pdf
MC_sus.pdf
  7257   Thu Aug 23 15:35:33 2012 ranaUpdate IMC Ringdown

 

 It is HIGHLY unlikely that the IMC mirrors are having any effect on the ringdown. The ringdowns take ~20 usec to happen. The mirrors are 0.25 kg and you can calculate that its very hard to get enough force to move them any appreciable distance in that time.

  7260   Thu Aug 23 17:51:25 2012 ManasaUpdate IMC Ringdown

Quote:

 

 It is HIGHLY unlikely that the IMC mirrors are having any effect on the ringdown. The ringdowns take ~20 usec to happen. The mirrors are 0.25 kg and you can calculate that its very hard to get enough force to move them any appreciable distance in that time.

The huge kick observed in the MC sus sensors seem to last for ~10usec; almost matching the observed ringdown decay time. We should find a way to record the ringdown and the MC sus sensor data simultaneously to know when the mirrors are exactly moving during the measurement process. It could also be that the moving mirrors were responsible for the ripples observed later during the ringdown as well.

* How fast do the WFS respond to the frequency switching (time taken by WFS to turn off)? I think this information will help in narrowing down the many possible explanations to a few.

  7317   Thu Aug 30 12:01:27 2012 janosch, Manasa,SteveUpdate ETMX

We have done some work at ETMX today. We installed the baffle and placed two mirrors on the table.

The baffle position/orientation still needs to be checked more thoroughly to make sure that the beam will pass through the center of the baffle hole.

One of the two mirrors will stay on the table as pickoff. The other is only temporarily installed for alignment purposes. Later today we will shoot a laser into the chamber that will reflect off one of these mirrors towards the center of ITMX, then go back to the pickoff mirror next to ETMX and hopefully make it through the viewport.

To place the pickoff mirror, we had to move the "cable rack" next to ETMX a few inches towards the back of the table.

  7319   Thu Aug 30 17:03:32 2012 janosch, Manasa, SteveUpdate ETMX

The baffle has been moved away from ETMX towards the edge of the table (in fact, it is a little beyond the edge). It is also rotated so that its long edge is horizontal. In this way it was possible to center the baffle hole with respect to the optical axis, but also make it possible that the camera looks over the baffle.

We have tried to get an alignment beam from view port -> ETMX pick-off ->ITMX-> back to EX. This work was pretty much unsuccessful though. We could see the green laser scattering around ITMX, but there was no good way to know when the beam hit ITMX. So tomorrow we will find a better way to check where the beam is hitting at ITMX and finish the alignment of the scattering pick-off mirror.

  7326   Fri Aug 31 10:16:02 2012 janosch, SteveUpdate ETMX, scattering preps

The alignment of the pick-off mirror near ETMX is done. Everything turned out to be easy once we realized that there is no sense getting the alignment laser (going through viewport to pick-off to ITMX) back to ETMX. It is only necessary to hit ITMX somehow, since this makes sure that there is one scattered beam that will make it from ITMX to pick-off through viewport.

After the auxiliary optic (that we never used in the end) was removed again, we levelled the optical table.

So in the current setup, we can have small-angle scattering measurements on ITMX and large-angle scattering measurements on ETMX.

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Attachment 2: IMG_1608b.jpg
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  7352   Thu Sep 6 17:11:40 2012 janosch, Manasa, SteveUpdate pick-off and baffle at ETMY

We have installed the pick-off mirror at the ETMY table for the small-angle scattering measurement on ITMY. As we had already done for the X arm pick-off, the pick-off mirror at ETMY was aligned shooting a green laser normally through the viewport on the pick-off and steering it onto ITMY.

A baffle was also installed at a distance of about 30cm from ETMY near the edge of the table.

  7356   Fri Sep 7 00:08:10 2012 janoschMetaphysics baffle clipping loss

With a curvature radius of about 57m for the ETMs, flat ITMs at the beam waist, and using 39m for the arm lengths, one finds that the beam radius at the ETMs is about 5.3mm. The clipping power loss of a 5.3mm beam through a 20mm radius baffle hole would be less than a ppm of a ppm if the beam was perfectly centered. If the baffle hole had 15mm radius, the clipping loss would be 0.01ppm. If the baffle hole had 10mm radius, the loss would be 810ppm. The loss values are calculated using the formula of the  "Gaussian beam" Wikipedia article, "Power through an aperture" section. So I did not check if that one is ok.

  7363   Fri Sep 7 15:58:29 2012 Rijuparna ChakrabortyUpdate cavitymode scan

 IMC transmission photodiode has been aligned.

  7366   Fri Sep 7 17:37:16 2012 JenneUpdate cavitymode scan

Quote:

 IMC transmission photodiode has been aligned.

 Which PD?  The 'regular' DC one, or the newer one?  Why did it need realigning?  What mirrors did you touch to do the alignment?

Did you do anything else in the last 3 days?  I want to see ALL the gory details, because it can help people doing future measurements, or help us debug if something is wrong with the interferometer later.

MORE WORDS! Thanks.

  7368   Sat Sep 8 00:15:57 2012 Rijuparna ChakrabortyUpdate cavitymode scan

Quote:

Quote:

 IMC transmission photodiode has been aligned.

 Which PD?  The 'regular' DC one, or the newer one?  Why did it need realigning?  What mirrors did you touch to do the alignment?

Did you do anything else in the last 3 days?  I want to see ALL the gory details, because it can help people doing future measurements, or help us debug if something is wrong with the interferometer later.

MORE WORDS! Thanks.

 No, not the "regular DC one", the "newer one"  along with the controls of the corresponding mirror only i touched.

It needed to be realigned cause last week when we fitted a longer cable there, which may reach the network analyzer, it got misaligned since it got touched.

No other component in that box except that PD and the corresponding mirror controls I touched.

For my last 2 days work, I feel my last elog is reliable.

Today other than doing this, I checked for the higher order modes of the cavity, misaligning one of the MC mirror though the software only. I didn't mention it in my elog cause although I saw the presence of the higher order modes I didn't record it, so I can not upload any picture in support of such a statement.

Thanks

  7376   Wed Sep 12 19:26:08 2012 Rijuparna ChakrabortyUpdate cavitymode scan

 Summary: Recorded the presence of higher order modes in IMC

What I did: Misaligned the flat mirror MC1 by small amount in both pitch and yaw (it was needed to be done cause at the beginning of the experiment no higher order modes were present)  and scanned the cavity for frequency-range 32MHz to 45MHz.

I found the presence of higher order modes around 36.7MHz (1st order)  and 40.6MHz (2nd order) along with two other strong modes near 35MHz and 42.5MHz.

 

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  7486   Thu Oct 4 23:01:49 2012 RijuparnaConfiguration cavitymode scan

 Here I am attaching the schematic diagram of the experimental set-up for IMC cavitymode scanning. A 30- 45MHz scanning signal generated by Agilent 4395A network analyzer enters EOM, which in turn modulates the laser beam entering IMC. The cavity response can be verified from reflected/transmitted beam.

I worked with the reflected beam last days. But I got no clue about the percentage of  reflected light reaching the photodiode and also the photodiode response. I would like to measure the power reaching photodiode and also would like to perform the test with transmitted beam - on wednesday if possible.

 

Attachment 1: diagram1.pdf
diagram1.pdf
ELOG V3.1.3-