Calculation of the phases of injected pulsars from the servo loop

Slides:

Advertisements

Similar presentations

RECOVERING HARDWARE INJECTIONS IN LIGO S5 DATA Ashley Disbrow Carnegie Mellon University Roy Williams, Michele Vallisneri, Jonah Kanner LIGO SURF 2013.

Advertisements

LIGO-G v2 Form F v1 Advanced LIGO1 SCATTERED LIGHT CONTROL in ADVANCED LIGO Michael Smith LIGO Laboratory Caltech, Pasadena, CA.

LIGO- G Z Optimally Combining the Hanford Interferometer Strain Channels Albert Lazzarini LIGO Laboratory Caltech S. Bose, P. Fritschel, M. McHugh,

1 LIGO-G Z Penn State / LIGO Scientific Collaboration 2003 March 18 Calibration Testing Patrick Sutton, with Michael Landry, Gabriela Gonzalez,

1 ILIAS WG1 meeting, Hannover, Alignment electronics noise budget ● Sources of electronic noise ● C7 electronic noise ● Electronic noise for.

Calculation of and. Wanted independent method to calculate calibration factors to use in search codes. XS, Jolien Creighton, Mike Landry.

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

Fourier Transforms on Simulated Pulsar Data Gamma-ray Large Area Space Telescope.

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,

LIGO-G ZM. Landry – LHO LSC Meeting, November 11, 2003 CW search group S2 status report Michael Landry LIGO Hanford Observatory and the Continuous.

Calibration Accuracy of LIGO Interferometers Brian O’Reilly LIGO Livingston Observatory Rana Adikhari (MIT), Peter Fritschel (MIT), Gabriela Gonzalez(LSU),

Phase Difference = Phase Difference = 0.05.

S3: Timescale for calibration factors At the frequency of the calibration line: Using this and going around the loop we obtain: Implemented in LAL/LALapps.

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

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

LSC Meeting, 17 March 2004 Shawhan, Marka, et al.LIGO-G E Summary of E10 / S3 Hardware Signal Injections Peter Shawhan, Szabolcs Márka, Bruce.

RF Synchronization Activity at SPARC A.Gallo and D. Alesini, M. Bellaveglia, R. Boni, G. Di Pirro, A. Drago, A.Ghigo P. Baldini, L. Cacciotti, M. Scampati,

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

Takanori Sekiguchi External Review Alignment control servo for type-B/type-Bp (OpLev/WFS) 1 T. Sekiguchi.

Optical Gyroscopes for Ground Tilt Sensing in Advanced LIGO The need for low frequency tilt sensing The optics in Advanced LIGO’s suspensions must be very.

European Gravitational Observatory12/12/2005 WG1 Hannover 1 Mode Matching of the Fabry-Perrot cavities Julien Marque.

Displacement calibration techniques for the LIGO detectors Evan Goetz (University of Michigan)‏ for the LIGO Scientific Collaboration April 2008 APS meeting.

Phase Noise and Oscillators Stephen Powell. What is an Oscillator?  Produces a signal at a particular frequency  They are everywhere! watches, radios,

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.

10/06/2003LSC WIDE COLLOQUIUM1 LSC Pulsar Group and P Shawhan, S Marka, and S Koranda presented by B Allen, R Dupuis, N Christensen, and X Siemens S2 Hardware.

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

LSC ASIS Meeting LIGO Scientific Collaboration - University of Wisconsin - Milwaukee LIGO-G Z E10/S3 Hardware Pulsar Injections Bruce.

Networks in Engineering A network consists of a set of interconnected components that deliver a predictable output to a given set of inputs. Function InputOutput.

3/21/06G D S4/S5 Calibration Status Brian O’Reilly For the Calibration Committee LSC March 2006 Brian O’Reilly For the Calibration Committee LSC.

Graphing Trig Functions Review Whiteboard Activity.

S3 and S4 pulsars injections Graham Woan, University of Glasgow, For Matt Pitkin Réjean Dupuis PULG … LIGO-G Z.

1 Frequency Noise in Virgo by Matt Evans. 2 The Actors  Noise Sources  Input Mode Cleaner length noise  Sensing noise on IMC lock  Frequency Servo.

LIGO-G Z LIGO’s Thermal Noise Interferometer Progress and Status Eric D. Black, Kenneth G. Libbrecht, and Shanti Rao (Caltech) Seiji Kawamura.

LIGO-G Z S5 calibration: time dependent coefficients  Myungkee Sung, Gabriela González, Mike Landry, Brian O’Reilly, Xavier Siemens,…

Review of the LIGO S4 data search for GW bursts from cosmic superstrings - Review committee: Chris Messenger, Richard O'Shaughnessy, M.Alessandra Papa.

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

Review production of 30min calibrated SFTs well under way (see talks by V.Dergachev., X. Siemens in ASIS/DetChar). Also expect calibrated h(t) in the next.

Pcal actuation of the TST stage of the DARM servo loop

Electric Circuits Fall, 2014

RF Synchronization Activity

Introduction to control system

402.5 MHz Debunching in the Ring

A study of Arm Length Stabilization in KAGRA

Fiber Optic Gyroscope Systems Design

Overview of E10 / S3 Hardware Injections

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.

S2/S3 calibration Gabriela González, Louisiana State University Plus

2012 סיכום מפגש 2 שלב המשכי תהליך חזוני-אסטרטגי של המועצה העליונה של הפיזיותרפיה בישראל.

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

Frequency Noise in Virgo

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

Line tracking methods used in LineMon

First look at Injection of Burst Waveforms prior to S1

Modules Produced With Low Rint Sensors

Religious threats to Elizabeth

h(t): are you experienced?

Inspiral Hardware Injections

S2 Bilinear Couplings Study

ALLEGRO calibration for the LLO-ALLEGRO stochastic analysis

John Zweizig LIGO/Caltech

Optimal on-line time-domain calibration of the

Unit 3 Review (Calculator)

S3 Performance of the LIGO Interferometers as Measured by SenseMonitor

Calibration: S2 update, S3 preliminaries

MC radiation pressure effects

Review 1+3= 4 7+3= = 5 7+4= = = 6 7+6= = = 7+7+7=

Calculate 9 x 81 = x 3 3 x 3 x 3 x 3 3 x 3 x 3 x 3 x 3 x 3 x =

Presentation transcript:

Calculation of the phases of injected pulsars from the servo loop X. Siemens, B. Allen, M. Landry LIGO-G040177-00-Z The phases of the injections can be determined from the functions that make up the servo loop

Servo loop with injection points The actuation function: negative During S2 the pulsar signals were injected into M. During S3 into L.

If we ignore contributions from external noise and go around the loop: Injection point M is the simplest because injected signals are seen by entire actuation. If we ignore contributions from external noise and go around the loop: Expect phase of injected signal to be shifted by the phase of the actuation function as well as an overall factor of h=Calibrated AS_Q Expected signal

Injection point L is more involved because injected signals see only part of the actuation function. Once again we ignore contributions from external noise and go around the loop: Also expect phase of injected signal to be shifted by the phase of the actuation function as well as an overall factor of ! Calibrated AS_Q Expected signal

Some results S2: S3: Strongest Weakest expected (measured) Signal 1 H1 102o (100o) 102o (98o) H2 100o (98o) 99o (100o) L1 94o(84o +/- 15o) 93o (86o+/-10o) S3: expected (measured) Pulsar 4 Pulsar 3 Pulsar 2 Pulsar 1 Pulsar 0 H1 108o (105o) 302o (303o) 164o (105o) 338o (354o) 112o (126o) H2 100o (102o) 303o (301o) 163o (122o) 331o (312o) 117o (234o) L1 279o (98o) 122o (276o) 240o (117o) 151o (144o) 52o (---) Strongest Weakest

Conclusions We can predict phases of injected CW signals as seen in a calibrated AS_Q from models of the servo loop. We know how to account for actuation in future injections. - Injection phases of pulsars agree well with prediction for S2 and S3 (except for L1) … Problem with calibration functions?