LIGO- G040012-00-D Experimental Upper Limit from LIGO on the Gravitational Waves from GRB030329 Stan Whitcomb For the LIGO Scientific Collaboration Informal.

Slides:

Advertisements

Similar presentations

A walk through some statistic details of LSC results.

Advertisements

GWDAW9 – Annecy December 15-18, 2004 A. Di Credico Syracuse University LIGO-G Z 1 Gravitational wave burst vetoes in the LIGO S2 and S3 data analyses.

GWDAW-8 (December 17-20, 2003, Milwaukee, Wisconsin, USA) Search for burst gravitational waves with TAMA data Masaki Ando Department of Physics, University.

Pi of the Sky – preparation for GW Advance Detector Era Adam Zadrożny Wilga 2014.

Update on S5 Search for GRB and Gravitational Wave Burst Coincidence Isabel Leonor University of Oregon.

LIGO-G Z Coherent Coincident Analysis of LIGO Burst Candidates Laura Cadonati Massachusetts Institute of Technology LIGO Scientific Collaboration.

G Z April 2007 APS Meeting - DAP GGR Gravitational Wave AstronomyKeith Thorne Coincidence-based LIGO GW Burst Searches and Astrophysical Interpretation.

8/13/2004 Stefan Ballmer, MIT / LIGO Hanford G Directional Stochastic Search: a Gravitational Wave Radiometer Stefan Ballmer Massachusetts.

Paris, July 17, 2009 RECENT RESULTS OF THE IGEC2 COLLABORATION SEARCH FOR GRAVITATIONAL WAVE BURST Massimo Visco on behalf of the IGEC2 Collaboration.

Observing the Bursting Universe with LIGO: Status and Prospects Erik Katsavounidis LSC Burst Working Group 8 th GWDAW - UWM Dec 17-20, 2003.

S.Klimenko, G Z, December 21, 2006, GWDAW11 Coherent detection and reconstruction of burst events in S5 data S.Klimenko, University of Florida.

Search for gravitational-wave bursts associated with gamma-ray bursts using the LIGO detectors Soumya D. Mohanty On behalf of the LIGO Scientific Collaboration.

Status of LIGO Data Analysis Gabriela González Department of Physics and Astronomy Louisiana State University for the LIGO Scientific Collaboration Dec.

LIGO- G D Status of LIGO Stan Whitcomb ACIGA Workshop 21 April 2004.

Silvia Poggi - GW burst detection strategy in non-homogeneus networks Detection strategies for bursts in networks of non-homogeneus gravitational waves.

LIGO-G Z Peter Shawhan, for the LIGO Scientific Collaboration APS Meeting April 25, 2006 Search for Gravitational Wave Bursts in Data from the.

LIGO-G Z The AURIGA-LIGO Joint Burst Search L. Cadonati, G. Prodi, L. Baggio, S. Heng, W. Johnson, A. Mion, S. Poggi, A. Ortolan, F. Salemi, P.

The Analysis of Binary Inspiral Signals in LIGO Data Jun-Qi Guo Sept.25, 2007 Department of Physics and Astronomy The University of Mississippi LIGO Scientific.

GRBs & VIRGO C7 run Alessandra Corsi & E. Cuoco, F. Ricci.

Searching for Gravitational Waves with LIGO Andrés C. Rodríguez Louisiana State University on behalf of the LIGO Scientific Collaboration SACNAS

LIGO-G Z April 2006 APS meeting Igor Yakushin (LLO, Caltech) Search for Gravitational Wave Bursts in LIGO’s S5 run Igor Yakushin (LLO, Caltech)

Dec 16, 2005GWDAW-10, Brownsville Population Study of Gamma Ray Bursts S. D. Mohanty The University of Texas at Brownsville.

LIGO-G Z Results from LIGO's Second Search for Gravitational-Wave Bursts Patrick Sutton LIGO Laboratory, Caltech, for the LIGO Scientific Collaboration.

Gamma ray burst triggered searches in the S2, S3, S4 runs of LIGO Soumya D. Mohanty On behalf of the LIGO Science Collaboration.

Searching for Gravitational Waves from Binary Inspirals with LIGO Duncan Brown University of Wisconsin-Milwaukee for the LIGO Scientific Collaboration.

Searches for Compact Binary Coalescences in LIGO and Virgo data Gabriela González For the LIGO Scientific Collaboration and the Virgo Collaboration APS.

1 Status of Search for Compact Binary Coalescences During LIGO’s Fifth Science Run Drew Keppel 1 for the LIGO Scientific Collaboration 1 California Institute.

Searching for gravitational waves with LIGO detectors

LIGO- G D Gravitational Wave Observations with Interferometers: Results and Prospects Stan Whitcomb for the LIGO Scientific Collaboration 2 nd.

LIGO-G D Upper Limits on the Stochastic Background of Gravitational Waves from LIGO Vuk Mandic Einstein2005 Conference Paris, July

1 Laura Cadonati, MIT For the LIGO Scientific Collaboration APS meeting Tampa, FL April 16, 2005 LIGO Hanford ObservatoryLIGO Livingston Observatory New.

LIGO-G Z The Q Pipeline search for gravitational-wave bursts with LIGO Shourov K. Chatterji for the LIGO Scientific Collaboration APS Meeting.

S.Klimenko, G Z, December 2006, GWDAW11 Coherent detection and reconstruction of burst events in S5 data S.Klimenko, University of Florida for.

Search for Short-Duration GW Bursts Coincident with S2/S3/S4 Gamma-Ray Bursts S5 GRB-GWB Search: First Results Isabel Leonor (for External Triggers group)

This material is based upon work supported in part by National Science Foundation Award PHY May 30-31, 2003, LIGO G Z APS NW Section Meeting.

S.Klimenko, G Z, December 21, 2006, GWDAW11 Coherent detection and reconstruction of burst events in S5 data S.Klimenko, University of Florida.

LIGO-G v2 The Search For Continuous Gravitational Waves Gregory Mendell, LIGO Hanford Observatory on behalf of the LIGO Science Collaboration The.

Data Analysis Algorithm for GRB triggered Burst Search Soumya D. Mohanty Center for Gravitational Wave Astronomy University of Texas at Brownsville On.

LIGO-G Z GWDAW9 December 17, Search for Gravitational Wave Bursts in LIGO Science Run 2 Data John G. Zweizig LIGO / Caltech for the LIGO.

LIGO-G All-Sky Burst Search in the First Year of the LSC S5 Run Laura Cadonati, UMass Amherst For the LIGO Scientific Collaboration GWDAW Meeting,

Peter Shawhan The University of Maryland & The LIGO Scientific Collaboration Penn State CGWP Seminar March 27, 2007 LIGO-G Z Reaching for Gravitational.

LIGO-G Z Status of the LIGO-TAMA Joint Bursts Search Patrick Sutton LIGO Laboratory, Caltech, for the LIGO-TAMA Joint Working Group.

TAUP 2007, Sendai, September 12, 2007 IGEC2 COLLABORATION: A NETWORK OF RESONANT BAR DETECTORS SEARCHING FOR GRAVITATIONAL WAVES Massimo Visco on behalf.

LIGO-G Z TFClusters Tuning for the LIGO-TAMA Search Patrick Sutton LIGO-Caltech.

S5 First Epoch BNS Inspiral Results Drew Keppel 1 representing the Inspiral Group 1 California Institute of Technology Nov LSC Meeting MIT, 4 November.

GWDAW11 – Potsdam Results by the IGEC2 collaboration on 2005 data Gabriele Vedovato for the IGEC2 collaboration.

Igor Yakushin, December 2004, GWDAW-9 LIGO-G Z Status of the untriggered burst search in S3 LIGO data Igor Yakushin (LIGO Livingston Observatory)

LIGO-G Z Status of the LIGO-TAMA Joint Bursts Search Patrick Sutton LIGO Laboratory, Caltech, for the LIGO-TAMA Joint Working Group.

LIGO-G Z Peter Shawhan, for the LSC Burst Analysis Group LSC Observational Results Meeting November 4, 2006 The S4 LIGO All-Sky Burst Search.

LIGO- G D Results from the LIGO Science Runs Stan Whitcomb for the LIGO Scientific Collaboration Aspen Winter Conference on Gravitational Waves.

The first AURIGA-TAMA joint analysis proposal BAGGIO Lucio ICRR, University of Tokyo A Memorandum of Understanding between the AURIGA experiment and the.

Searching the LIGO data for coincidences with Gamma Ray Bursts Alexander Dietz Louisiana State University for the LIGO Scientific Collaboration LIGO-G Z.

LIGO-G Z The Q Pipeline search for gravitational-wave bursts with LIGO Shourov K. Chatterji for the LIGO Scientific Collaboration APS Meeting.

24 th Pacific Coast Gravity Meeting, Santa Barbara LIGO DCC Number: G Z 1 Search for gravitational waves from inspiraling high-mass (non-spinning)

Thomas Cokelaer for the LIGO Scientific Collaboration Cardiff University, U.K. APS April Meeting, Jacksonville, FL 16 April 2007, LIGO-G Z Search.

Detecting a Galactic Supernova with H2 or GEO

Searching for gravitational-wave transients with Advanced detectors

The Q Pipeline search for gravitational-wave bursts with LIGO

Analysis of LIGO S2 data for GWs from isolated pulsars

Igor Yakushin, LIGO Livingston Observatory

Searching for Gravitational-Wave Bursts (GWBs) associated with Gamma-Ray Bursts (GRBs) during the LIGO S5 run Isabel Leonor University of Oregon (for the.

Coherent detection and reconstruction

Background estimation in searches for binary inspiral

Search for the gravity wave signature of GRB030329/SN2003dh

The arrival of Gravitational Waves and the EEE network:

Status of LIGO Patrick J. Sutton LIGO-Caltech

Search for the gravity wave signature of GRB030329/SN2003dh

Searching for GRB-GWB coincidence during LIGO science runs

Status and Plans for the LIGO-TAMA Joint Data Analysis

with coherent WaveBurst pipeline

Presentation transcript:

LIGO- G D Experimental Upper Limit from LIGO on the Gravitational Waves from GRB Stan Whitcomb For the LIGO Scientific Collaboration Informal Lunch Seminar MIT 30 January 2004 Software Signal Injection Special thanks to Szabi Marka

LIGO- G D MIT Lunch Seminar 2 LIGO Observatories

LIGO- G D MIT Lunch Seminar 3 Transition to Full Operation Commissioning Science Runs S1 (papers “in press”) 17 Days (Aug-Sep 2002) S2 (this talk) 59 Days (Feb- Apr 2003) S3 (even better) 70 Days (Oct 03 – Jan 04)

LIGO- G D MIT Lunch Seminar 4 GRBs during S2 Both Hanford detectors operating for GRB030329

LIGO- G D MIT Lunch Seminar 5 Relative delay between gravity wave and GRB predicted to be small Signal region to cover most predictions Known direction Optical counterpart located LIGO antenna factor identified LIGO arrival times are known Source distance is known z= (d~800Mpc) Unknown waveform/duration Signal region and GRB trigger “Signal” region +60 seconds -120 seconds

LIGO- G D MIT Lunch Seminar 6 Correlation Analysis h rss 2 = 0

LIGO- G D MIT Lunch Seminar 7 Event Identification - Simulated Signal Color coding: “Number of variances above mean” Event strength [ES] calculation: Average value of the “optimal” pixels

LIGO- G D MIT Lunch Seminar 8 Analysis Flow Chart Noise event Spectrum DataExternal Trigger Adaptive pre - conditioning Correlation detection algorithm Signal regionBackground regionSimulations Efficiency Measurements Upper limits Candidates Inject Simulated Signals Threshold Largest event Threshold

LIGO- G D MIT Lunch Seminar 9 Based on ~15 ks of H1 & H2 coincident data around the GRB “signal region” Estimated False Rate: events in 180s Spectrum of Noise Events Note: Preliminary ! Evidence for some correlated noise bursts between detectors?

LIGO- G D MIT Lunch Seminar 10 Sensitivity Determination Noise examples “Huge” Sine-Gaussian F = 361Hz, Q = 8.9 h RSS ~ 6x [1/  Hz] Optimal integration Time [ ~ms ] Integration length [ ms, uneven steps ] Optimal integration “Small” Sine-Gaussian F = 361Hz, Q = 8.9 h RSS ~ 3x [1/  Hz] (~ detection threshold)

LIGO- G D MIT Lunch Seminar 11 Detection Efficiency at Fixed False Alarm Rate Calibration known within ~10% Detection efficiencies obtained for threshold corresponding to ~4 x Hz false alarm rate (<10% probability of noise event in 180 sec) H1/H2 noise curves reflect levels around GRB Symbols: 50% detection efficiency points Lines: 90% detection efficiency boundaries Note: Preliminary !

LIGO- G D MIT Lunch Seminar 12 Threshold for <10% false alarm probability Events Within the Signal Region The signal region seems to be “relatively quiet” when compared to the neighboring regions No event was detected with strength above the pre-determined threshold It is an upper limit result Note: Preliminary !

LIGO- G D MIT Lunch Seminar 13 For an observation (or limit) made at a luminosity distance d from a source Observed Limit on h rss Relates to GW Energy h rss 2

LIGO- G D MIT Lunch Seminar 14 H1-H2 only Antenna attenuation factor ~0.37 (assuming optimal polarization) z =  d  800Mpc For narrowband GWs near minimum of noise curve (simulated with Q  Hz sine-Gaussian), obtain 90% efficiency h RSS < 5  [1/  Hz]  E GW < 125 M  (1 / 0.37)  340 M  Example: Estimating E GW for GRB Note: Preliminary ! ~ ~

LIGO- G D MIT Lunch Seminar 15 Summary and Prospects for Future Searches Executed a sensitive, cross-correlation based search for gravitational wave bursts around GRB Sensitivity (depending on frequency) h RSS < few x [1/  Hz] »Current limit of some hundreds of M  in GWs »Detector improvement: both detectors, factor of 10 – 30 (in h rss ) between S2 and final sensitivity (depending on frequency…)  improvement of 100 – 300 in E GW »Beaming factor: estimate for every GRB detected, 100 to 500 “missed” -- reasonable for one year of observation might give 10 times closer event (cf. SN1998bw at ~ 40 Mpc)  another factor of 100 in E GW »More detectors, better location in antenna pattern, better discrimination against noise events…. »very realistic chance to set a sub-solar mass limit in the near future