LIGO data analysis status Michael L in addition to ry LIGO Han as long as d Observatory as long as the LIGO Scientific Collaboration PAC19 Dec 12, 2005 LIGO Han as long as d Observatory } Einstein@home

LIGO data analysis status Michael L in addition to ry LIGO Han as long as d Observatory as long as the LIGO Scientific Collaboration PAC19 Dec 12, 2005 LIGO Han as long as d Observatory } Einstein@home

LIGO data analysis status Michael L in addition to ry LIGO Han as long as d Observatory as long as the LIGO Scientific Collaboration PAC19 Dec 12, 2005 LIGO Han as long as d Observatory } Einstein@home

Delsol, Christine, Contributing Travel Writer has reference to this Academic Journal, PHwiki organized this Journal LIGO data analysis status Michael L in addition to ry LIGO Han as long as d Observatory as long as the LIGO Scientific Collaboration PAC19 Dec 12, 2005 LIGO Han as long as d Observatory RX J1856.5-3754, neutron or strange quark star at d=117pc Credit: NASA/SAO/CXC/J.Drake et al. Overview Sources S2, S3, S4 results from the four search groups All searches: no detections yet S5 online Compact binary systems Neutron stars in addition to black holes Inspiral in addition to merger Probe internal structure, populations, in addition to spacetime geometry Supernovae, GRBs all-sky untriggered searches burst signals in coincidence with electromagnetic in addition to /or neutrino observations Stochastic background Cosmological relic Superposition of astrophysical sources Spinning neutron or quark stars Known compact spinning stars, LMXBs all-sky search as long as unknown objects (computing challenge) Astrophysical sources of gravitational waves

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Signal duration in addition to template Search groups LSC partitioned into four search groups 2 Co-chairs (one theory, one experimental) Mix of LIGO Lab in addition to LSC representation, theorists, phenomenologists in addition to experimentalists in each group Burst group ef as long as ts Expected wave as long as ms too numerous in addition to complicated to calculate as long as matched filter analysis Potential sources supernovae, astrophysical phenomenae that power GRBs mergers of compact objects cosmic string cusps in addition to kinks disruptions of neutron stars Search as long as untriggered bursts Triggers, vetoes, upper limits Injections of simulated wave as long as ms Multiple event trigger generator (ETG) investigations Search as long as triggered bursts Other work Cosmic string search Inspiral-burst-ringdown search LIGO-TAMA joint analysis of S2 LIGO-Virgo working group struck

S2 untriggered burst search bursts less than 1s, in b in addition to 100-1100Hz 9.98d of data analyzed – improved sensitivity of machine in addition to in analysis pipeline Event triggers generated on triple-coincidence data, followed up by “r-statistic” wave as long as m consistency test Background set by similar analysis with time-shifted data Set limit on rate of detectable gravitational wave bursts Test efficiency of pipeline to detect particular wave as long as ms: both ad hoc (gaussian, sine-gaussian) in addition to astrophysically-motivated wave as long as ms (core-collapse in addition to binary black hole) applied Set rate vs strength exclusion regions as long as these wave as long as ms S2 untriggered burst search S2 triggered burst search GRB 030329, confirmed supernova at z~0.17, or ~ 800Mpc away H1, H2 were in operation during S2. A targeted search resulted in no detection HETE

Stochastic group ef as long as ts Cosmological relic, or, summation of noise sources from astrophysical epoch Cross correlate detectors: uncorrelated noise integrates away while the signal to noise integrates up as the square root of time Make use of optimal filter, which includes overlap reduction function Searches include LHO-LLO H1-H2 LLO-Allegro WGW is the gravitational wave energy density per logarithmic frequency interval, divided by rc, the energy density required to close the universe S3 stochastic background results S3 Inspiral group ef as long as ts predicted BNS inspiral rates theoretical upper bound of 1/3 per year as long as LIGO S5 (Kalogera et. al, Ap J Lett 601, L179 (2004)) n.b. higher rates predicted as long as initial LIGO, based on identification of short GRBs as binary inspirals (astro-ph/0511254) predicted BBH inspiral rates theoretical upper bound of 1 per year as long as LIGO S5 Matched template analysis BNS BBH Primordial black holes High mass ratios, spin LIGO-Virgo LIGO-TAMA

S2 binary neutron star search No detection. Simulations from up to 1.5 Mpc away were “detected” in S2. Effective distance of sources considered, in addition to cumulative number of galaxies searched as long as in S2. S2 binary neutron star search False alarm coincident triggers, in addition to simulated injections Rate < 47 per year per Milky Way-like galaxy Triggers generated when event passes SNR cut Chisquare test applied Intersite coincidence Continuous waves search group ef as long as ts Known pulsar Coherent time-domain method Target known isolated in addition to binary neutron stars Pulsar timing provided by Jodrell Bank Pulsar Group Markhov-Chain Monte Carlo method Incoherent methods Multiple methods (Powerflux, Stackslide, Hough) to test robustness in addition to make crosschecks All-sky searches in addition to quick passing of data Incoherent step in heirarchical search Coherent frequency-domain (“F-statistic”) searches Search as long as LMXBs Isolated all-sky, wide-parameter searches Best as long as blind search Coherent step in heirarchical search Einstein@home: distributed computing ef as long as t S3, S4 time-domain preliminary results as long as known neutron stars Closest to spin-down upper limit Crab pulsar ~ 2.5 times greater than spin-down (fgw = 59.6 Hz, dist = 2.0 kpc) h0 = 3.5x10-24, e = 1.9x10-3 Assumes I = 1038 kgm2 Best limit on e: one pulsar below 1x10-6 Crab pulsar NASA/CXC/SAO Pulsar timing : Jodrell Bank Pulsar Group S2 Hough trans as long as m search Semi-coherent method Wide-parameter space 200-400Hz, one spindown parameter Hough trans as long as m is applied to find pattern produced by Doppler shift in addition to spindown of gravitational wave signal to the time-frequency plane of the data 95% confidence upper limits on h0, over whole sky in addition to different spindown values in 1Hz b in addition to s are shown Outliers: known instrument artifacts, or, not in triple coincidence GEO-600 Hannover LIGO Han as long as d LIGO Livingston Current search point Current search coordinates Known pulsars Known supernovae remenants User name User’s total credits Machine’s total credits Team name Current work % complete } Einstein@home Final S3 analysis results Data: 60 10-hour stretches of the best H1 data Post-processing step on centralized server: find points in sky in addition to frequency that exceed threshold in many of the sixty ten-hour segments analyzed 50-1500 Hz b in addition to shows no evidence of strong pulsar signals in sensitive part of the sky, apart from the hardware in addition to software injections. There is nothing “in our backyard”. Outliers are consistent with instrumental lines. All significant artifacts away from r.n=0 are ruled out by follow-up studies. WITH INJECTIONS WITHOUT INJECTIONS Instrument artifacts Some instrument lines permanent features, others can be mitigated, e.g. violin resonances in addition to 1Hz lines, respectively S4 Einstein@home search notches both classes of lines S2, S3 analysis papers Upper Limits on Gravitational Wave Bursts in LIGO’s Second Science Run, Phys Rev D 72, 062001 (2005) A Search as long as Gravitational Waves Associated with the Gamma Ray Burst GRB030329 Using the LIGO Detectors, Phys Rev D 72, 042002 (2005) Upper Limits from the LIGO in addition to TAMA detectors on the rate of gravitational-wave bursts, gr-qc/0507081, accepted as long as publication in Phys Rev D Upper limits on a stochastic background of gravitational waves, Phys Rev Lett 95, 221101 (2005) Search as long as gravitational waves from galactic in addition to extra–galactic binary neutron stars, Phys Rev D 72, 082001 (2005) Search as long as Gravitational Waves from primordial black hole binary coalescences in the galactic halo, Phys Rev D 72, 082002 (2005) Search as long as gravitational waves from binary black hole inspirals in LIGO data, gr-qc/0509129, submitted to PRD Limits on Gravitational-Wave Emission from Selected Pulsars Using LIGO Data, B. Abbot et al., LIGO Scientific Collaboration; M. Kramer in addition to A. G. Lyne, Phys Rev Lett 94, 181103 (12 May 2005) First all-sky upper limits from LIGO on the strength of periodic gravitational waves using the Hough trans as long as m, Phys Rev D 72, 102004 (2005) To be submitted to gr-qc on the near horizon: S2 joint LIGO-TAMA search as long as binary neutron stars, in addition to , S2 coherent wide-parameter search as long as gravitational waves: all-sky in addition to Sco X-1 Plus! Many technical papers on techniques, status etc. S5 S5 analyses online or near-online Precision calibration in place: S5 V1 quality as good or better than the S4 V4 (final) calibration h(t) to be produced online Stochastic in addition to CW searches fast-tracked (weeks-months), burst in addition to inspiral searches in true real time Stochastic search Accumulated sensitivity calculated weekly Fast-track H1-L1 search CW search Fast-track time-domain search as long as known objects, update monthly Incoherent searches to scan weekly as long as new line artifacts, in addition to make blind, all-sky searches on months of data Goal: deep, wide-b in addition to , blind search, heirarchical employing Einstein@home S5 Burst search Fast track triggered searches, in addition to high-threshold searches as long as gold-plated events. Deeper searches offline. Realtime injections. Inspiral search Fast track BNS in addition to BBH searches. Realtime triggers in control room (10m). Coincidence, chi-square later (2h). Realtime injections Delsol, Christine San Francisco Chronicle Contributing Travel Writer

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