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G070221 00

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Published on November 28, 2007

Author: VolteMort

Source: authorstream.com

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Search for Compact Binary Coalescences in LIGO’s Third and Fourth Science Runs:  Search for Compact Binary Coalescences in LIGO’s Third and Fourth Science Runs B.S. Sathyaprakash For the LIGO Scientific Collaboration (LSC) The LIGO Scientific Collaboration:  The LIGO Scientific Collaboration Sensitivity of LSC Interferometers:  Sensitivity of LSC Interferometers LIGO now at design sensitivity:  LIGO now at design sensitivity LLO 4 km – S1 (2002 09 07) LLO 4 km – S2 (2003 03 01) LHO 4 km – S3 (2004 01 04) LHO 4 km – S4 (2005.02.26) LHO 4 km – S5 (2006.01.02) LIGO SRD Goal, 4 km h(f) 1/Sqrt(Hz) Frequency (Hz) S5 Sensitivity:  S5 Sensitivity Gravitational wave network sensitivity:  Gravitational wave network sensitivity Frequency (Hz) Gravitational wave amplitude h (/Hz) LSC Searches:  LSC Searches Compact binary coalescences Binary neutron stars (BNS) Binary black holes (BBH) BH-NS binaries Stochastic background Primordial background Astrophysical background Continuous waves Rapidly spinning neutron stars or other objects Gravitational wave bursts Black hole collisions, supernovae, gamma-ray bursts Compact binary searches:  Compact binary searches Compact binary coalescences:  Compact binary coalescences Late-time dynamics of compact binaries is highly relativistic, dictated by non-linear general relativistic effects Post-Newtonian theory, which is used to model the evolution, is now known to O(v7) The shape and strength of the emitted radiation depend on many parameters of binary system: masses, spins, distance, orientation, sky location, … Waveform families:  Waveform families How reliable are the templates used in the search? Binary neutron stars coalesce well out of the detectors sensitive band – SNR is dominated by the early insprial part – pretty reliable signal models Binary black holes (of masses in the range 10-50 solar masses) coalesce in the most sensitive part of the detector, SNR has significant contribution from merger but we don’t (yet) use merger signal Searches reported in this talk use For binary neutron star and primordial black hole binary searches: Standard post-Newtonian templates at (v/c)4 post-Newtonian order For binary black holes: Phenomenological templates that have been shown to have a good overlap with most known waveform families (post-Newtonian families at various orders, effective one-body, P-approximants, etc.) Search parameter space:  Search parameter space BNS S1-S5 PBH S1-S5 Spin is important Detection templates S3-S5 “High mass ratio” Coming soon 1 3 10 0.1 Mass Mass 0.1 1 3 10 BBH Search S2-S5 Physical waveforms S5 Insp.-Burst-Ringdown S5 Binary Neutron Stars:  S3 search complete 0.09 yr of data ~3 Milky-Way like galaxies S4 search complete Preliminary results on slide 9 0.05 yr of data ~24 Milky-Way like galaxies Binary Neutron Stars Log (cumulative number of events) signal-to-noise ratio squared Rate < 47 per year per Milky-Way-like galaxy; 0.04 yr data, 1.27 Milky-Ways S2 Observational Result Phys. Rev. D. 72, 082001 (2005) Binary Black Holes:  Binary Black Holes signal-to-noise ratio squared Rate < 38 per year per Milky-Way-like galaxy S2 Observational Result Phys. Rev. D. 73, 062001 (2006) S3 search complete 0.09 yr of data 5 Milky-Way like galaxies for 5+5 Msuns S4 search complete Preliminary results on slide 9 0.05 yr of data 150 Milky-Way like galaxies for 5+5 Msuns Log| cum. no. of events | S4: Background Vs Foreground: Primordial Binary Black Holes (Preliminary):  S4: Background Vs Foreground: Primordial Binary Black Holes (Preliminary) S4: Background Vs Foreground: Binary Neutron Stars (Preliminary):  S4: Background Vs Foreground: Binary Neutron Stars (Preliminary) S4: Background Vs Foreground: Binary Black Holes (Preliminary):  S4: Background Vs Foreground: Binary Black Holes (Preliminary) S4 Preliminary Rate Upper Limits:  S4 Preliminary Rate Upper Limits Primordial BBH Binary neutron stars Binary black holes PBH (0.75/0.75 ): rate < 4.9 yr-1 L10-1 BNS (1.4/1.4 ): rate < 1.2 yr-1 L10-1 BBH (5.0/5.0 ): rate < 0.45 yr-1 L10-1 Binary Neutron Stars: S5 Search:  Distance to 1.4+1.4 Msun optimally oriented & located binary at SNR=8, in Mpc Binary Neutron Stars: S5 Search S2 Horizon Distance 1.5 Mpc S5 data is being analyzed Binary Black Holes: S5 Search:  Binary Black Holes: S5 Search binary neutron star horizon distance binary black hole horizon distance S5 data being analyzed Horizon distance (in Mpc) versus total mass (in M) for BBH Are we capable of detection?:  Are we capable of detection? Simulated signals Estimate background accidentals in time-slides Sample of S5 Data What to expect in the coming years:  What to expect in the coming years 2005-2007: S5 search About 1 year of triple coincident data Search at design sensitivity level Rates are probably about 0.2 per year for BNS 2007-2009: Initial detectors will be upgraded to enhanced interferometers GEO will provide coverage: sensitive to Galactic SN 2009-2011: Enhanced LIGO and VIRGO About 1 year of data at x 2 sensitivity (8 in volume) BNS rates are at few per year 2011-2013: GEO-HF GEO tuned to observe specifically in the high frequency regime 2013+: Advanced LIGO and VIRGO Several years of data at x 10 sensitivity (1000 in volume) Expect BNS rates of many per year to several per day

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