1. LIGO- G030081-00-Z AJW, Caltech, LIGO Project1 Hardware Burst Injections in E9  S2 Alan Weinstein, Caltech Laura Cadonati, MIT Shourov Chatterjee, MIT Sergei Klimenko, UFla Igor Yakushin, LIGO-LLO LSC meeting, 3/18/03

2. LIGO- G030081-00-Z AJW, Caltech, LIGO Project2 Goals of the Burst Injections  test our understanding of the entire signal chain from »GDS excitation point  »displacements of test masses  »data logged in LSC-AS_Q and related DM and common mode channels  »entire burst search analysis chain.  In particular, we need a quantitative comparison between signals injected into the IFO and signals injected into the datastream in software (in LDAS), to validate the efficiency calculation.  Verify that we detect HW injected signals with SNR as expected »Detection confidence  Test our understanding of the dependence on source direction and polarization.

3. LIGO- G030081-00-Z AJW, Caltech, LIGO Project3 Injecting signals The multiawgstream and SIStr facilities developed by I. Leonor, P. Shawhan, D. Sigg are used to inject series of signals into the LSC-ETMX_EXC, and LSC-ETMY_EXC, or DARM_CTRL_EXC channels of the three interferometers. The injections during S1, E9 and S2 were/are coordinated by M. Landry, P. Shawhan, S. Marka Many thanks to all the developers for this immensely important and useful facility!

4. LIGO- G030081-00-Z AJW, Caltech, LIGO Project4 Original (ambitious) program: Burst_z and Burst_ang Burst_z scan, into DARM or ETMX-ETMY:  inject sine-Gaussians into all 6 end test masses, with durations of ~ 1 second, spaced 40 seconds apart.  Scan 8 logarithmically-spaced central frequencies from 100 - 2000 Hz.  Scan ~6 amplitudes from 1 to 100 times the nominal calibrated strain sensitivity at that central frequency.  These 48 bursts should thus take 32 minutes. Burst_ang scan, exciting both DARM and CARM, with IFO-IFO delays:  Choose one central frequency and relatively large amplitude, and scan over 100 source directions and polarizations (5 in cos , 5 in , 4 in  ; all with respect to the mean of the LHO/LLO zenith and orientation). This should take 67 minutes.

5. LIGO- G030081-00-Z AJW, Caltech, LIGO Project5 Waveforms, amplitudes  Short, narrow-bandwidth signals (sine-Gaussians) provide the most direct and useful interpretation of IFO and data analysis responses. We envision a "swept-sine calibration" of sine-Gaussians of varying frequency, spanning the LIGO band of interest.  Signal amplitudes should span the range from "barely detectable" to "large, but not so large as to excite a non-linear response". The IFO strain sensitivity varies over the frequency range of interest, so the amplitudes should vary as well.  Signals are injected using the GDS excitation engine, which accepts 16384-Hz time series in units of counts to the coil driver. The frequency dependence of the test mass response must be taken into account.  Each sine-Gaussian has Q ~ 9; total duration ~ Q/f 0 Frequency f 0 (Hz) Duration (msec) 100 90 153 58 235 38 361 25 554 16 850 11 1304 7 2000 4.5 Time from segment start t 0 (sec) 20406080100120140160

6. LIGO- G030081-00-Z AJW, Caltech, LIGO Project6 Ad-hoc signals: (Sine)-Gaussians These have no astrophysical significance; But are well-defined in terms of waveform, duration, bandwidth, amplitude SG 554, Q = 9

7. LIGO- G030081-00-Z AJW, Caltech, LIGO Project7 Schedule of Signal Injections During the S2 Run Feb 14 2:48 CST, 0:48 PST # Feb 18 23:00 CST, 21:00 PST Feb 23 16:00 CST, 14:00 PST Feb 25 18:00 CST, 16:00 PST * Mar 2 14:00 CST, 12:00 PST Mar 3 12:00 CST, 10:00 PST Mar 7 2:00 CST, 0:00 PST Mar 12 20:00 CST, 18:00 PST Mar 15 24:00 CST, 22:00 PST * Mar 19 23:00 CST, 21:00 PST Mar 23 3:00 CST, 1:00 PST Mar 25 22:00 CST, 20:00 PST Mar 28 20:00 CST, 18:00 PST * Apr 2 10:00 CST, 8:00 PST Apr 5 4:00 CST, 2:00 PST Apr 9 24:00 CST, 22:00 PST * Apr 11 22:00 CDT, 20:00 PDT * inserted during the run to make up for lost opportunities (sometimes the interferometers were just out of lock and injection was pointless or partial) # The injection time was determined just before the injection S, Marka, P. Shawhan, I. Leonor

8. LIGO- G030081-00-Z AJW, Caltech, LIGO Project8 Actually done and analyzed (so far): DATEETMx-ETMyETMxETMy Feb 13 (pre-S2) 13 (H1,L1)8 (H1,L1) Feb 17--3 (H1,L1) Feb 25--3 (H1,H2,L1) Mar 2--3 (H1) Mar 7--3 (H1,L1) Groups of 8 SG’s, varying amplitudes. Intra-run injections subject to IFO availability.

9. LIGO- G030081-00-Z AJW, Caltech, LIGO Project9 Signal amplitudes The waveform files have a peak amplitude (at 0.5 secs) of 1. You can read off the ETMx and ETMy signals, peak amplitude in counts. So: |ETMx-ETMy| (in counts)  (~1 nm / ct) (DC calibration, approximate, varies from ~0.5-1.0)  (0.744/f0)^2 (pendulum response, where f0 is central SG frequency) / 4000 m (or 2000 m for H2) will give you a peak amplitude in strain. # Time Cfg Waveform file ETMX ETMY hpeak (strain) 729154547.000000 1 wfsg100Q9.dat 0.0107060 -0.0104160 3.0e-19 729154567.000000 1 wfsg153Q9.dat 0.0312080 -0.0303660 3.7e-19 729154587.000000 1 wfsg235Q9.dat 0.0227440 -0.0221300 1.1e-19 729154607.000000 1 wfsg361Q9.dat 0.0663000 -0.0645080 1.4e-19 729154627.000000 1 wfsg554Q9.dat 0.1932700 -0.1880460 1.7e-19 729154647.000000 1 wfsg850Q9.dat 0.5634020 -0.5481760 2.1e-19 729154667.000000 1 wfsg1304Q9.dat 6.5694940 -6.3919400 1.1e-18 729154687.000000 1 wfsg2000Q9.dat 19.1507320 -18.6331460 1.3e-18

10. LIGO- G030081-00-Z AJW, Caltech, LIGO Project10 SG injections: frequencies, amplitudes SG central frequencies f 0 are color-coded Closed circles are detected bursts; Open circles are undetected (H1)

11. LIGO- G030081-00-Z AJW, Caltech, LIGO Project11 Analysis  Data were analyzed through the standard Burst pipeline  Pre-filtering in datacond, including 100 Hz HPF and whitening »For the first few injection runs, HPF 150 Hz and S1 whitening  Then, data from each IFO were passed through tfclusters and slope ETG’s  Each ETG returns triggers with start_time and trigger strength  tfclusters also returns a central frequency  Time resolution: »tfclusters uses time bins of 1/8 second, start_time is quantized in those units (125 msec) »Slope is expected to give < 50 msec resolution

12. LIGO- G030081-00-Z AJW, Caltech, LIGO Project12 Trigger power (tfclusters) Feb 13 injections Before frequency consistency cutAfter frequency consistency cut L. Cadonati

13. LIGO- G030081-00-Z AJW, Caltech, LIGO Project13 TFCLUSTERS central frequency vs injected frequency The red, off diagonal events are the ones rejected by the frequency cut (background noise). The blue, off diagonal events have large bandwidth, covering the injected frequency, thus pass the frequency cut.

14. LIGO- G030081-00-Z AJW, Caltech, LIGO Project14 Timing accuracy Injection peaks at 0.5 secs, starts ~10’s of msec before then Tfclusters (left) is quantized in bins of 1/8 sec. Slope (right) peak is 10 msec before 0.5 sec.

15. LIGO- G030081-00-Z AJW, Caltech, LIGO Project15 ETG strength ~ xrms 2 There’s a lot of scatter, but most injections indeed show strength ~ xrms 2 Don’t compare the different colors; they’re different frequencies, and the IFOs have different sensitivities. The black dots are at 100 Hz, and we hpf’ed at 150 Hz! Still, a lot of signals were not found – under investigation!

16. LIGO- G030081-00-Z AJW, Caltech, LIGO Project16 H1 – L1 cross-correlation Filtered AS_Q data streams 554 Hz SG at hrms ~ 2e-20 Injected in H1 and L1 simultaneously Correlation coefficient and confidence L. Cadonati

17. LIGO- G030081-00-Z AJW, Caltech, LIGO Project17 Intra-run injections and stability A much more limited set of injections are being done throughout S1. Oops! Used different pre-filtering for the 3/7/03 injections! Need to run with the new filters on all injections; trying to get the data and filters all available at one ldas…

18. LIGO- G030081-00-Z AJW, Caltech, LIGO Project18 Comparison with SW injections Comparison currently only available for latest round of intra- run injections into H1. Solid points = HW Open diamonds = SW Find 45 o line connecting points and diamonds of same color (f 0 )? That’s qualitative evidence that HW and SW injections with same (nominal) xrms are found by tfclusters with same strength. Much more work, statistics, etc, required to establish this quantitatively!

19. LIGO- G030081-00-Z AJW, Caltech, LIGO Project19 Results from WaveBurst  WaveBurst DSO (S. Klimenko, I. Yakushin) cross-correlates data streams from 2 detectors in wavelet basis.  Run on H1 and H2 detectors, using the 23 groups of 8 SG bursts from Feb 13, 2003  Biorthogonal wavelet of 16 th order was used  WaveBurst TF resolution of 1/32 sec x 16 Hz

20. LIGO- G030081-00-Z AJW, Caltech, LIGO Project20 Central frequency from WaveBurst

21. LIGO- G030081-00-Z AJW, Caltech, LIGO Project21 WaveBurst power

22. LIGO- G030081-00-Z AJW, Caltech, LIGO Project22 Central time of WaveBurst cluster

23. LIGO- G030081-00-Z AJW, Caltech, LIGO Project23 Summary  HW Burst injections, pre-S2 and during S2, are a powerful tool for honing algorithms, building confidence in detection ability, monitoring detection stability, finding problems  Confirms ability to detect bursts at ~ expected level  Comparison of HW and SW injections: qualitatively, in the right ballpark  Failure to detect some signals with tfclusters is under investigation

24. LIGO- G030081-00-Z AJW, Caltech, LIGO Project24 Signal sent to GDS system The signal that is sent to each of the ETMs by the GDS system is a product of factors:  A waveform with units of strain, sampled at 16384 Hz, is input to the system.  The peak strain amplitude can be scaled to a desired value.  This is multiplied by the arm length (2000 m for H2 and 4000 m for L1), and by “antenna pattern” factors (for the two ETMs in each of the 3 interferometers) corresponding to a particular source direction and polarization.  From the calibration 6, we know how many DAC counts, G, correspond to a motion of 1 nm, at frequencies much below the pendulum frequency (f p = 0.74 Hz). G is typically on the order of 1 nm/count.  Since sine-Gaussians are narrow band, with central frequency f c, there is a factor of (f c / f p ) 2 to account for the pendulum response to force from the GDS- controlled coil actuators. (more complicated filtering would be required for broad-band signals).  Relative delays between the three interferometers are calculated based on the source direction (on the order of msec).

25. LIGO- G030081-00-Z AJW, Caltech, LIGO Project25 Driver files for injections BURST_Z #T_off filename H2_DELAY M_ETMX M_ETMY L1_DELAY M_ETMX M_ETMY H1_DELAY M_ETMX M_ETMY # (s) (s) (s) (s) 40 wf100.dat 1.0000 0.0544 -0.0536 1.0000 0.0275 -0.0291 1.0000 0.0516 -0.0452 80 wf153.dat 1.0000 0.0640 -0.0630 1.0000 0.0647 -0.0686 1.0000 0.1215 -0.1063 120 wf235.dat 1.0000 0.0753 -0.0742 1.0000 0.0761 -0.0807 1.0000 0.2859 -0.2502 160 wf361.dat 1.0000 0.0354 -0.0349 1.0000 0.0716 -0.0760 1.0000 0.6729 -0.5888 200 wf554.dat 1.0000 0.0417 -0.0411 1.0000 0.0674 -0.0715 1.0000 1.5837 -1.3858 240 wf850.dat 1.0000 0.0981 -0.0967 1.0000 0.1587 -0.1683 1.0000 3.7274 -3.2614 280 wf1304.dat 1.0000 0.2310 -0.2275 1.0000 0.4670 -0.4952 1.0000 17.5450 -15.3519 320 wf2000.dat 1.0000 0.5436 -0.5355 1.0000 1.9783 -2.0979 1.0000 61.9395 -54.1970 360 wf100.dat 1.0000 0.2718 -0.2678 1.0000 0.1374 -0.1457 1.0000 0.2581 -0.2258 400 wf153.dat 1.0000 0.3199 -0.3151 1.0000 0.3233 -0.3429 1.0000 0.6074 -0.5315 … BURST_ANG #T_off filename H2_DELAY M_ETMX M_ETMY L1_DELAY M_ETMX M_ETMY H1_DELAY M_ETMX M_ETMY # (s) (s) (s) (s) 40 wf850.dat 0.0000 1.8795 -1.9080 -0.0000 -3.1329 3.2244 0.0000 71.3846 -64.3627 80 wf850.dat -0.0038 0.7602 -1.8054 0.0038 -2.3396 0.2829 -0.0038 28.8713 -60.9012 120 wf850.dat -0.0038 0.4389 -1.2321 0.0038 -0.9553 0.1659 -0.0038 16.6688 -41.5612 160 wf850.dat -0.0038 0.0000 -0.3286 0.0038 0.6849 0.0045 -0.0038 0.0000 -11.0849 200 wf850.dat -0.0043 1.0065 -1.2559 0.0043 -0.9788 0.6367 -0.0043 38.2277 -42.3656 240 wf850.dat -0.0043 0.7087 -0.4360 0.0043 0.4348 0.7272 -0.0043 26.9171 -14.7080 280 wf850.dat -0.0043 0.2210 0.5007 0.0043 1.7320 0.6229 -0.0043 8.3941 16.8906 320 wf850.dat -0.0043 -0.3259 1.3033 0.0043 2.5650 0.3516 -0.0043 -12.3781 43.9634 360 wf850.dat -0.0042 1.3805 -0.6045 0.0042 -0.0302 1.5366 -0.0042 52.4316 -20.3904

26. LIGO- G030081-00-Z AJW, Caltech, LIGO Project26 First look at 8/17/02 injections into L1:LSC-DARM_CTRL_EXC  Beginning with 360 seconds of injections (one every 40 seconds) with scale factors 7.5 and 30  Command: darm_z_burst 713668660 1  Can we see the signals in the time series?  Can we see the signals in spectrograms?  Can the burst search DSOs see the signals?  Do we quantitatively understand the amplitude of the signals? Do they compare well with software injections into the data stream in LDAS?

27. LIGO- G030081-00-Z AJW, Caltech, LIGO Project27 Can we see the signals in the time series?  Surely not, given the very large low frequency noise.  But we can zoom in, A LOT. (eg, zoom in on 235 Hz SG at 121 seconds after start).  Or, we can HP filter the data. (eg, 10 th order Butterworth at 120 Hz) 235 Hz wiggle here!

28. LIGO- G030081-00-Z AJW, Caltech, LIGO Project28 Can we see the signals in the spectrogram?  Surely not, unless you really zoom in.  But this shows that it’s a pretty quiet stretch of data.

29. LIGO- G030081-00-Z AJW, Caltech, LIGO Project29 Zoom in on the spectrogram 100 Hz at 41 sec153 Hz at 81 sec235 Hz at 121 sec 361 Hz at 161 sec 554 Hz at 201 sec 2000 Hz at 321 sec

30. LIGO- G030081-00-Z AJW, Caltech, LIGO Project30 Can we see it in tfclusters?  tfclusters (J. Sylvestre) is one of our well-tested burst search algorithms, running in LDAS as a wrapperAPI DSO  It calculates excess power in pixels in the t-f plane, then looks for clusters of such pixels.  It generates a list of triggers, with start_time, burst power, central frequency, bandwidth, duration.

31. LIGO- G030081-00-Z AJW, Caltech, LIGO Project31 tfclusters triggers Triggers in time with injected bursts are indicated in red For scale factor 7.5, we find bursts above 150 Hz with large SNR Trigger “power” scales like (30/7.5) 2 as expected scale factor 30 scale factor 7.5 10015323536155485013042000

32. LIGO- G030081-00-Z AJW, Caltech, LIGO Project32 Amplitude  The real point of all this is to “cross-calibrate” hardware vs software injections, testing our understanding of all the gain factors.  First check: injections into LLO with scale factors differing by factor 4, show up in tfclusters with “power” differing by ~ 4 2. OK!  This work is in progress.