Bose, APS-Denver, 2008/05/04 Estimating the parameters of coalescing black hole binaries (non-spinning) using ground-based detectors Sukanta Bose Washington.

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Presentation transcript:

Bose, APS-Denver, 2008/05/04 Estimating the parameters of coalescing black hole binaries (non-spinning) using ground-based detectors Sukanta Bose Washington State University, Pullman Based on a paper by Ajith, SB, Phys. Rev. D 79, (2009), arXiv: (Supported in part by NSF grants PHY & PHY ) In collaboration with P. Ajith (Caltech/AEI) LIGO-G v1

Bose, APS-Denver, 2008/05/04 Coalescing binary signals in earth-based detectors The 3 Phases in a Binary’s Life… …lasting up to several minutes AdLIGO can detect these sources with a total mass of up to several hundred solar masses. [Figure: Courtesy of Kip Thorne]

Bose, APS-Denver, 2008/05/04 NR-based hybrid waveforms [P. Ajith et al, PRD ’08]

Bose, APS-Denver, 2008/05/04 Astrophysical reach Effects of waveform extensions (data analysis): »Better template match, –Lower false-alarms / background, Greater signal-to-noise ratio (SNR). Event rates & source “variety”: Both will increase Parameter estimation: »Can we determine both component masses? »Any improvements in measuring sky-localization, wave polarization, and distance? Provide impetus for other studies: Do IMBHs really exist? Can such binaries have electromagnetic counterparts?

Bose, APS-Denver, 2008/05/04 Rate estimates Radio observations confirm existence of neutron star binaries: » Hulse-Taylor pulsar » J (both neutron stars are visible as pulsars) Stellar population modelers estimate an upper bound on BNS rates of ~ 1 in a few to several LIGO-I sensitivity Rates for black hole binary coalescences much more uncertain »Population synthesis studies suggest a likely rate of around 0.01 / 0.1 / 30 per year in LIGO-I / eLIGO / AdLIGO for stellar mass BBHs [O'Shaughnessy et al., Astrophys. J. 633, 1076 (2005), astro-ph/ ] »IMBH binaries: the plausible rates for LIGOI / AdLIGO detectors are 10−4 / 0.1 per year [J. M. Fregeau et al., ibid. 646, L135 (2006), astro-ph/ ] »Stellar-mass BHs merging with IMBHs (the so called intermediate-mass-ratio inspirals): plausible event rates for LIGOI / AdLIGO are 10−3 / 10 per year [ I. Mandel et al., arXiv: ]

Bose, APS-Denver, 2008/05/04 Noise PSDs & SNRs The source effective distance is taken to be 100Mpc, except for AdLIGO and AdVirgo, where it is taken as 1Gpc.

Bose, APS-Denver, 2008/05/04 Single IFO (AdLIGO) parameter accuracies (effective distance fixed at 1Gpc)

Bose, APS-Denver, 2008/05/04 Single IFO (AdLIGO) parameter accuracies (SNR fixed to 10)

Bose, APS-Denver, 2008/05/04 Single IFO (eLIGO) parameter accuracies (SNR fixed to 10) The overlap function obtained by running a template bank across twelve different target (simulated) signals.

Bose, APS-Denver, 2008/05/04 Comparing Fisher calculations with Monte Carlo simulations (SNR = 10)

Bose, APS-Denver, 2008/05/04 Comparing Fisher calculations with Monte Carlo simulations SNR 

Bose, APS-Denver, 2008/05/04 Network observations: SNR in an AdLIGO- AdLIGO-AdVirgo network ( Gpc, orientation-averaged)

Bose, APS-Denver, 2008/05/04 Sky-position accuracy in an AdLIGO- AdLIGO-AdVirgo network ( Gpc, orientation-averaged)

Bose, APS-Denver, 2008/05/04 Distance accuracy in an AdLIGO-AdLIGO- AdVirgo network ( Gpc, orientation-averaged)

Bose, APS-Denver, 2008/05/04 Sky-position: Multi-IFO (H1-L1-V1) accuracy 1Gpc; observed in advanced detectors) Inspiral-only accuracies shown in black. Complete-waveform accuracies shown in red. Top row: A Msun system  Bottom row: A Msun system 

Bose, APS-Denver, 2008/05/04 Sky-position: Multi-IFO (H1-L1-V1) accuracy 1Gpc; observed in advanced detectors) Inspiral-only accuracies shown in black. Complete-waveform accuracies shown in red. Top row: A Msun system  Bottom row: A Msun system 

Bose, APS-Denver, 2008/05/04 Summary of parameter accuracies (in advanced detectors) SNR= %2.58%0.68%1.2% %0.26%0.22%0.81% SNR= % % % % Single detector estimates: AdLIGO-AdLIGO-AdVirgo estimates: