Search for Gravitational Wave Transients. Florent Robinet On behalf of the LSC and Virgo Collaborations

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1 Search for Gravitational Wave Transients On behalf of the LSC and Virgo Collaborations 1

2 Gravitational Waves Gravitational waves = "ripples" in space time Weak field approximation : g = h h 1 Wave equation, speed c Solution with 2 d.o.f. : h= h+ hx Dimensionless amplitude given by h Black hole merger Signal strength: h rss= 2 2 h t h t dt x Production of gravitational waves R c 2 s v ℒ = G R c A good GW source : is compact and massive is asymmetric has a relativistic speed Lab production : h ~ Astrophysical sources : h ~

3 Gravitational Wave Sources Supernovae (asymmetric core bounce) Pulsars (asymmetric rotations, instabilities) Compact binary coalescence of neutron stars &/or black holes Cosmic strings The unexpected Stochastic background 3?

4 A Network of Detectors Virgo (3 km) LSC Virgo collaboration Full data sharing since May 2007 Common analyses and papers Common tools Livingston (4 km) Geo (600 m) Hanford (4&2 km) 4

5 A Network of Detectors SOURCE POINTING Source location within ~ tens of square degrees Serious candidates follow up (EM, neutrinos...) tvirgo SOURCE tlivingston GHOST thanford 5

6 A Network of Detectors Hanford sky coverage Antenna pattern 6

7 A Network of Detectors Livingstone sky coverage Antenna pattern 7

8 A Network of Detectors Virgo sky coverage Antenna pattern 8

9 A Network of Detectors Network sky coverage Antenna pattern 9

10 LIGO / Virgo Science Runs S commissioning 2005 S5 VSR1 Many Publications S6 Advanced Detectors VSR2 VSR3 VSR4? Analyses in progress Publications in preparation 10

11 LIGO / Virgo Science Runs S6 - VSR2 S5 - VSR1 11

12 Analysis Groups? Compact Binary Coalescence (CBC) Short Signals (Bursts) Continuous Waves Stochastic See C. Palomba's talk 12

13 Analysis Groups? Compact Binary Coalescence (CBC) Low Mass Short Signals (Bursts) High Mass All sky Multi-Messenger Astronomy GRB-triggered Parameter Estimation Inspiral-MergerRingdown (IMR) Supernovae SGR Flares Pulsars Glitches EM Follow-up Binary Mergers Cosmic Strings

14 CBC vs. Bursts Burst Signals Compact Binary Coalescence (CBC) The Signals Modeled signals Inspiral Merger Ringdown The Signals Short-duration signals (<1s) Modeled and unmodeled signals Large variety of sources The search Template search (selective) Waveform parameter estimation The search Robust signal detection methods Excess power (unmodeled) Template search (modeled) Science goals Detection Upper limits on GW emission Multi-messenger (EM, neutrino...) Parameter estimation Study gravity Study populations Study dense matter Study GRBs Science goals Detection Upper limits on GW emission Multi-messenger (EM, neutrino...) Parameter estimation Star equation of state Study populations 14

15 Analysis Methods COINCIDENT PIPELINE Data Detector 1 Triggers Coincidence Data Detector 2 Triggers Selection + Data Quality Significance? Data stream 15

16 Analysis Methods COINCIDENT PIPELINE Data Detector 1 Triggers Coincidence Data Detector 2 Triggers Data Detector 2 time-shifted wrt 1 Data stream Background stream 16 Selection + Data Quality Significance wrt background DETECTION? NO? Upper limits

17 Analysis Methods COINCIDENT PIPELINE UPPER LIMITS Signal injections Data Detector 1 Search efficiency Triggers Coincidence Data Detector 2 Triggers Data Detector 2 time-shifted wrt 1 Data stream Injection stream Background stream Selection + Data Quality Significance wrt background DETECTION? The number of detectors can be increased (up to 4) Various coincidence schemes: union of configurations Increasing the number of coincidences enables to be more selective (but less efficient) 17

18 Analysis Methods COHERENT PIPELINE UPPER LIMITS Signal injections Data Detector 1 Data Detector 2 Search efficiency Coherent combination Data Detector 2 time-shifted wrt 1 Triggers Selection + Data Quality Data stream Injection stream Background stream Significance wrt background DETECTION? The data of multiple detectors can be combined coherently Sky positions are scanned to take into account the time of arrival and the antenna pattern of each detectors 18

19 Analysis Methods: Template Searches Detector whitened Strain h(t) Noise + inspiral hardware injection Signal-to-noise ratio time serie: t 0 Sh h f f 2i f t e df S h f Template waveform Sensitivity An event is defined when t Threshold Given by the background estimation (+ additional clustering in time and frequency) This method is used for: CBC searches Pulsar ringdown search Cosmic string burst search A template bank covering the parameter space is slid over the data 19

20 Analysis Methods: Excess Power Searches Injected Inspiral Signal The time-frequency plane is tiled with pixels An event is defined when the energy of multiple pixels exceeds a given threshold This method is used for: 20 Most of the burst searches

21 Data Quality The noise of the detector displays a nongaussian behavior Transient glitches removal is crucial to improve the sensitivity of the searches Noise understanding for each detector have been performed for each science run Many glitch families have been understood Detection channel Magnetic sensor Example: Virgo, VSR2 Deadtime ~ 10% Removal efficiency ~ 80% (SNR>8) Specific vetoes based on auxiliary channels have been produced to remove specific glitch families Veto safety have been carefully checked (we don't want to flag real signals!) SNR 100

22 CBC Searches BNS BBH BHNS S5/VSR1 data have been analyzed and results are published "Realistic" observable BNS coalescence rate ~ 0.02 per year (large uncertainty) S6/VSR2-3 analyses are in progress Preliminary results are released See T. Dent's talk 22

23 CBC: Low Mass Search Description of the search: No Detection Non-spinning templates Post-Newtonian up to the innermost stable orbit Mass region 2 < M < 35 Msun total Phys. Rev. D 82(2010) BNS/BBH Upper limits NS/BH Upper limits 23

24 CBC: High Mass Searches High-Mass Effective One Body (EOB) waveforms Inspiral-Merger-Ringdown is covered No spin Mass region 25 < M < 100 Msun total Uncertainty on the waveforms LIGO only search (Virgo is not sensitive enough for High mass systems) arxiv: Ringdown search In progress for S5 LIGO only search Mass region 75 < MBH < 750 Msun Spin is included The ringdown contains most of the GW energy More reliable waveforms

25 CBC & Burst Signals: GRB Triggered Searches Powerful bursts of highly energetic gamma rays Two populations: short and long duration Short: possibly produced by the merging of binary objects CBC colored search Long: possibly produced by violent stellar collapse (hypernovae) Number of Bursts Long-duration Short-duration GRBs GRBs 60 Use mainly Swift and Fermi triggers to get a source location a timing and sometimes a distance Background reduction Better sensitivity 40 During S5/VSR1 137 GRBs were analyzed by the burst coherent pipeline (short and long). See M. Was's talk T90 (seconds) 22 GRBs were analyzed by a CBC pipeline. See N. Christensen's talk 25

26 CBC & Burst Signals: GRB Triggered Searches GRB Short and hard GRB detected by 4 satellites in Feb in direction of the Andromeda galaxy The binary merger scenario is excluded with a 99% confidence level! Astrophys. J. 681(2008) 1419 Inspiral Exclusion Zone 25% 50% 75% 90% 26 99%

27 Burst Signals: All-Sky Search Upper limit (sine-gaussian) Description of the search Multiple Algorithms Broad-band frequency search Coincident and coherent searches Very large variety of waveforms Robustness Rate (90% C.L.) vs. frequency (EGW = Msunc2) No detection With a 90% confidence level, the rate of burst signals with 50 < f < 2048 Hz is lower than 2 events per year 1e-2 yr-1 Mpc-3 ~8e-7 yr-1 Mpc-3 Phys. Rev. D 81(2010) f(hz) 1000

28 Burst Signals: Neutron Stars 2006/08/12: timing glitch observed in the radio emission of the Vela pulsar Quasi-normal mode oscillations GW Both Hanford detectors were up at that time Ringdown signal is searched No detection Upper limits on GW energy released by monoharmonic modes Phys. Rev. D83(2011) Soft Gamma Repeaters (SGR) / Anomalous X-ray Pulsars (AXP) Neutron stars powered by extreme magnetic fields (magnetars) SGR SGR SGR SGR SGR AXP 1E magnetars have been analyzed by a dedicated pipeline (excess power) arxiv:

29 Burst Signals: Cosmic String Cusps When 2 cosmic string segments meet they can reconnect and produce loops. The main mechanism for the loop to loose its energy is to radiate gravitationally. GW radiation is the most promising signature to detect cosmic strings. GW Points of the string can acquire a large Lorentz boost and form a "cusp" GW burst GW Well-modeled signal Template burst search Dedicated pipeline Upper limits on the cosmic string parameter space: S5 Projection Gμ: String tension S4 ε: loop size parameter p: reconnection probability Phys Rev D 80(2009) Gμ

30 Online Searches Hanford h(t) Livingstone Virgo h(t) Low latency searches took place during S6 / VSR2-3 for both CBC and burst searches h(t) Central Location h(t) CBC pipeline MBTA event h(t) Burst pipeline Omega h(t) Burst pipeline Coherent Waveburst event event Candidate Database ~ 30 min Most significant events were sent to telescopes / satellites (14 events for S6/VSR2-3) Sky localization is performed with a resolution of ~tens of square degrees for events at threshold Image analysis is performed within the collaboration Most significant Candidate selection See M. Branchesi's talk Swift Zadko ROTSE

31 S6/VSR2-3 Science Run Improved sensitivity ~ 200 days of live-time with at least 2 detectors up Big challenge: run analyses online 3 pipelines were running (2 bursts + 1 CBC) The data quality was performed with low latency (< 1 min) EM follow-up by partner telescopes Offline analyses are in progress (some results are released) Analyses pipelines and data quality tools have been improved for a better sensitivity Blind hardware injection challenge was successful (we detected it with great confidence). See T. Dent's talk 31

32 Preparation for Advanced Detectors Era Sensitivity improvement by a factor 10 This translates into a detection rate up to 40 neutron star binary events per year Science should resume in 2015 Design sensitivity achieved by 2019 What are we going to do in the meantime? Virgo might run this summer (VSR4) along with the GEO detector Similar sensitivity at high frequency This run could be of some interest for external triggered searches Then GEO will run alone in astrowatch mode during the construction of Adv. detectors ( ) Some mock data runs are planned to test and improve our searches A lot of work is required to optimize the EM-followup procedures 32

33 Summary - Conclusions A large variety of physical results have been produced from the LIGO-Virgo data There is no detection yet but upper limits can be used to constrain astrophysical models The first generation of detectors is close to the end. Analysis pipeline have greatly improved over the last years to perform optimized and sensitive searches on GW data Data quality is a great challenge. Multiple tools have been developed to reject noise events efficiently. GW astronomy is on its way: online searches, Multi-messengers, EM followup Now, the big challenge is to be fully ready for the Advanced Detectors Era 33

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