Presentation Transcript
Search for inspiraling black holes with the LIGO gravitational wave detectors : Search for inspiraling black holes with the LIGO gravitational wave detectors Alexander Dietz
Louisiana State University
Inspiral Working Group, LIGO Scientific Collaboration
Outline : Outline Analysis Pipeline
Injections & Templates
Background Estimate
LIGO Observatories : LIGO Observatories Hanford: two interferometers in same vacuum envelope (4km, 2km) Livingston: one interferometer (4km)
Inspiral and Merger of Compact Binaries : Inspiral and Merger of Compact Binaries Neutron Star
Component Masses of 1 to 3 MSUN
fISCO= 800 Hz
Use post-Newtonian waveform
Black Holes
Component Masses of >3MSUN
fISCO= 110 Hz
Use template (BCV) Buoanno, Chen, Vallisneri, PRD 67, 2003
Analysis Pipeline (S2) : Analysis Pipeline (S2) Vetoes/cuts L1 Vetoes/cuts Vetoes/cuts Event candidates
Injections : Injections Software injections
validate and tune the pipeline
quantify the sensitivity of the instruments
test how well the BCV templates can be used for recovering different waveforms and parameters
(PPN, Pade, EOB)
“Population”
Uniform in each component mass: 3 – 20 MSUN
Uniform in log10(distance): 1 kpc – 20 Mpc
Inspiral range : Inspiral range Inspiral range during S2: Up to 6 Mpc for L1
Neutron Star:
about 3Mpc L1 H1 H2
Background vs Injections : Background vs Injections Very clear distinction between:
Background triggers
Found injections
Background estimate : Background estimate Using combined statistic:
Conclusion : Conclusion Using ‘BCV’ templates to search for coalescences of binary black holes
Software injections done to tune pipeline, calculate efficiencies and test parameter recovery
Time slides are used for background estimations
Final results will be published soon
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