Calibration of LIGO data in the time domain X. Siemens, B. Allen, M. Hewitson, M. Landry.

Slides:

Advertisements

Similar presentations

LIGO-G v2 Recovering Burst Injections in LIGO S5 Data Alex Cole Data Analysis Meeting May 6, 2014.

Advertisements

Calibration of the gravitational wave signal in the LIGO detectors Gabriela Gonzalez (LSU), Mike Landry (LIGO-LHO), Patrick Sutton (PSU) with the calibration.

Spring LSC 2001 LIGO-G W E2 Amplitude Calibration of the Hanford Recombined 2km IFO Michael Landry, LIGO Hanford Observatory Luca Matone, Benoit.

Active Filters: concepts All input signals are composed of sinusoidal components of various frequencies, amplitudes and phases. If we are interested in.

Nonrecursive Digital Filters

Digital Filters. A/DComputerD/A x(t)x[n]y[n]y(t) Example:

1 BIEN425 – Lecture 13 By the end of the lecture, you should be able to: –Outline the general framework of designing an IIR filter using frequency transform.

ECE651 Digital Signal Processing I Digital IIR Filter Design.

So far We have introduced the Z transform

Digital Signal Processing – Chapter 11 Introduction to the Design of Discrete Filters Prof. Yasser Mostafa Kadah

Unit 9 IIR Filter Design 1. Introduction The ideal filter Constant gain of at least unity in the pass band Constant gain of zero in the stop band The.

LIGO-G D LIGO calibration during the S3 science run Michael Landry LIGO Hanford Observatory Justin Garofoli, Luca Matone, Hugh Radkins (LHO),

Calibration of data in the time domain (or how to generate 1800s long SFTs from time domain data) XS, Bruce Allen, Mike Landry, Soumya Mohanty, Malik Rachmanov,

Angular Noise in a Suspended Interferometer with DC Readout Royal Reinecke Co-Mentors: Alan Weinstein and Rana Adhikari.

LIGO- G060XXX-00-R E2E meeting, September How to design feedback filters? E2E meeting September 27, 2006 Osamu Miyakawa, Caltech.

Digital Filter Noise Why does the textbook tell us not to use direct form 2? LIGO-G v1 Matt Evans.

Use ofSiesta in VIRGO commissioning Lisa Barsotti University of Pisa – INFN Pisa For the Virgo collaboration Caltech, December 19th 2003.

1 Time-Domain Calibration Update Xavier Siemens, Mike Landry, Gaby Gonzalez, Brian O’Reilly, Martin Hewitson, Bruce Allen, Jolien Creighton.

LIGO Response to High Frequency Gravitational Waves Implications for Calibration Hunter Elliott Mentors: Rick Savage, Greg Mendell, Malik Rakhmanov.

Normalized Lowpass Filters “All-pole” lowpass filters, such as Butterworth and Chebyshev filters, have transfer functions of the form: Where N is the filter.

Calibration of TAMA300 in Time Domain Souichi TELADA, Daisuke TATSUMI, Tomomi AKUTSU, Masaki ANDO, Nobuyuki KANDA and the TAMA collaboration.

Over-Sampling and Multi-Rate DSP Systems

Sampling Theorem, frequency resolution & Aliasing The Sampling Theorem will be the single most important constraint you'll learn in computer-aided instrumentation.

EE513 Audio Signals and Systems Digital Signal Processing (Systems) Kevin D. Donohue Electrical and Computer Engineering University of Kentucky.

DSP. What is DSP? DSP: Digital Signal Processing---Using a digital process (e.g., a program running on a microprocessor) to modify a digital representation.

Ni.com Data Analysis: Time and Frequency Domain. ni.com Typical Data Acquisition System.

Hardware injection of continuous gravitational wave signals at GEO600 U. Weiland, G. Heinzel and the GEO600 team References P. Jaranowski, A. Królak, B.

S4/S5 Calibration The Calibration team G Z.

LIGO- G Z LSC ASIS Meeting LIGO Scientific Collaboration - University of Wisconsin - Milwaukee 1 S2 Hardware Pulsar Injections Bruce.

Searching for gravitational radiation from Scorpius X-1: Limits from the second LIGO science run Alberto Vecchio on behalf of the LIGO Scientific Collaboration.

LIGO-G I S5 calibration status Michael Landry LIGO Hanford Observatory for the LSC Calibration Committee LSC/Virgo Meeting May 22, 2007 Cascina,

6. Results The accompanying histograms show the empirical PDF of z for each interferometer (H1, H2 at Hanford, WA; L1 at Livingston, LA). The green areas.

LIGO-G Z GWDAW10, December 16, S3 Final Results Bruce Allen, for the LIGO Scientific Collaboration.

Unit-V DSP APPLICATIONS. UNIT V -SYLLABUS DSP APPLICATIONS Multirate signal processing: Decimation Interpolation Sampling rate conversion by a rational.

BIEN425 – Lecture 14 By the end of the lecture, you should be able to:

LIGO-G DM. Landry – Hanover LSC Meeting, August 18, 2003 LIGO S2 Calibration Michael Landry LIGO Hanford Observatory Representing the calibration.

Loïc Rolland LSC-Virgo, Orsay- June 11th Virgo ‘timing’ calibration Loïc Rolland Note: Timing calibration during VSR1 in the Virgo codifier (VIR-028A-08,

Control systems KON-C2004 Mechatronics Basics Tapio Lantela, Nov 5th, 2015.

Calibration in the Front End Controls Craig Cahillane LIGO Caltech SURF 2013 Mentors: Alan Weinstein, Jamie Rollins Presentation to Calibration Group 8/21/2013.

MODELING THE CALIBRATED RESPONSE OF THE ADVANCED LIGO DETECTORS Luke Burks 2013 LIGO Caltech SURF Mentors: Alan Weinstein, Jameson Rollins Final Presentation.

Martin Hewitson and the GEO team Measuring gravitational waves with GEO600.

Digital Signal Processing

S.Klimenko, LSC, August 2004, G Z BurstMon S.Klimenko, A.Sazonov University of Florida l motivation & documentation l description & results l.

ECE 8443 – Pattern Recognition EE 3512 – Signals: Continuous and Discrete Objectives: FIR Filters Design of Ideal Lowpass Filters Filter Design Example.

LIGO-G Z March 2007, LSC meeting, Osamu Miyakawa 1 Osamu Miyakawa Hiroaki Yamamoto March 21, 2006 LSC meeting Modeling of AdLIGO arm lock acquisition.

G52IIP, School of Computer Science, University of Nottingham 1 Image Transforms Basic idea Input Image, I(x,y) (spatial domain) Mathematical Transformation.

ALLEGRO GWDAW-9, Annecy 16 December, Generating time domain strain data (h(t)) for the ALLEGRO resonant detector or calibration of ALLEGRO data.

DISP 2003 Lecture 5 – Part 1 Digital Filters 1 Frequency Response Difference Equations FIR versus IIR FIR Filters Properties and Design Philippe Baudrenghien,

Martin Hewitson and the GEO team Measuring gravitational waves with GEO600.

Calibration and the status of the photon calibrators Evan Goetz University of Michigan with Peter Kalmus (Columbia U.) & Rick Savage (LHO) 17 October 2006.

Calibration in the Front End Controls Craig Cahillane Luke Burks LIGO Caltech SURF 2013 Mentors: Alan Weinstein, Jamie Rollins Presentation to Calibration.

Time domain simulation for a FP cavity with AdLIGO parameters on E2E

Time domain simulation for a FP cavity with AdLIGO parameters on E2E

(Some) noise hunting issues at Virgo

Echivalarea sistemelor analogice cu sisteme digitale

Noise issues – Potentiometer signal from the electronic card

Calibration of data in the time domain (or how to generate 1800s long SFTs from time domain data) XS, Bruce Allen, Mike Landry, Soumya Mohanty, Malik.

Jordi Burguet-Castell for the Calibration Team

Homodyne readout of an interferometer with Signal Recycling

Chapter 8 Design of Infinite Impulse Response (IIR) Digital Filter

ECET 350 Education for Service/tutorialrank.com

Calibration of TAMA300 in Time Domain

Broad-band CW searches in LIGO and GEO S2 and S3 data

Broad-band CW searches in LIGO and GEO S2 and S3 data

LIGO Scientific Collaboration, UW - Milwaukee

Broad-band CW searches in LIGO and GEO S2 and S3 data

Optimal on-line time-domain calibration of the

Simulating the Advanced LIGO Interferometer Using the Real Control Code Juan F. Castillo.

Calculation of the phases of injected pulsars from the servo loop

Presentation transcript:

Calibration of LIGO data in the time domain X. Siemens, B. Allen, M. Hewitson, M. Landry

-So far LIGO data has been calibrated in the frequency domain. -For the S1 analysis 60s Fourier transforms were used. The change in the response of the instrument was computed every minute. -For the S2 analysis the pulsar working group decided to use 1800s long Fourier transforms to take advantage of the speed of FFT. -GEO has been producing h(t) and we can adapt their method to calibrate our data.

We reconstruct the strain from the residual and control motions: [Mohanty and Rakhmanov, August 2003 LSC Meeting] High frequencyLow frequency [R. Adhikari et al. LIGO-T D]

Need to construct digital filters for the inverse sensing function, the servo, and the actuation function Sensing function -cavity pole at 84.8 Hz [Inverse of pole is unstable: Stabilise it by adding a zero at 100 kHz and filter up-sampled (by a factor of 16) Q through it] -anti-aliasing 8 th order elliptic filter at 7.5KHz [Has zeros on imaginary axis which need to be moved off; Inverse rises sharply at 7.5 kHz: low-pass at 6kHz with high order BW filter] -a pole at 100kHz [We ignore it] -electronics gain Have implemented time domain calibration for S2/H1. Have digitised the modified sensing function using a bi-linear transformation at 16384*16Hz

Response of digital filter (blue) vs. official sensing function (red): Have digitised the modified sensing function using a bi-linear transformation at 16384*16Hz.

Servo nd order digital filters [problems with first filter: a double pole at 0Hz which we moved to 1.6Hz] Response of modified servo (blue) vs. actual servo (red):

Actuation function nd order digital filters (7 for x-arm, 6 for y-arm), pendulum transfer function, anti-imaging 4 th order elliptic filter at 7.5kHz, time delay Pade filter, snubber Analog part of this filter was digitised using a bilinear transformation at 16384Hz Hz m/count Response of digitised actuation (blue) vs. official actuation (red): Actuation makes no difference at high frequencies!

Signal Processing Pipeline:

Comparison of Fourier transform of time domain calibrated data (blue) with data calibrated in the frequency domain (red). ~1Hz band around 1000Hz at 1/60 Hz: Wrap-around

Around 630Hz: Around 112Hz:

Conclusions -All elements of pipeline are in place -Code has been parallelized (under condor) and full S2/H1 dataset is calibrated on Medusa (UWM) in a few hours. The output is 16s frames. -Still need filters for H2 and L1. -Will keep working on filter and pipeline optimization.