CaltechAUTHORS
  A Caltech Library Service

Searching for periodic sources with LIGO

Brady, Patrick R. and Creighton, Teviet and Cutler, Curt and Schutz, Bernard F. (1998) Searching for periodic sources with LIGO. Physical Review D, 57 (4). pp. 2101-2116. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:BRAprd98b

[img]
Preview
PDF - Published Version
See Usage Policy.

413Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:BRAprd98b

Abstract

We investigate the computational requirements for all-sky, all-frequency searches for gravitational waves from spinning neutron stars, using archived data from interferometric gravitational wave detectors such as LIGO. These sources are expected to be weak, so the optimal strategy involves coherent accumulation of signal-to-noise using Fourier transforms of long stretches of data (months to years). Earth-motion-induced Doppler shifts, and intrinsic pulsar spindown, will reduce the narrow-band signal-to-noise by spreading power across many frequency bins; therefore, it is necessary to correct for these effects before performing the Fourier transform. The corrections can be implemented by a parametrized model, in which one does a search over a discrete set of parameter values (points in the parameter space of corrections). We define a metric on this parameter space, which can be used to determine the optimal spacing between points in a search; the metric is used to compute the number of independent parameter-space points Np that must be searched, as a function of observation time T. This method accounts automatically for correlations between the spindown and Doppler corrections. The number Np(T) depends on the maximum gravitational wave frequency and the minimum spindown age τ=f/ḟ that the search can detect. The signal-to-noise ratio required, in order to have 99% confidence of a detection, also depends on Np(T). We find that for an all-sky, all-frequency search lasting T=10^7 s, this detection threshold is hc≈(4–5)h3/yr, where h3/yr is the corresponding 99% confidence threshold if one knows in advance the pulsar position and spin period. We define a coherent search, over some data stream of length T, to be one where we apply a correction, followed by a fast Fourier transform of the data, for every independent point in the parameter space. Given realistic limits on computing power, and assuming that data analysis proceeds at the same rate as data acquisition (e.g., 10 days of data gets analyzed in ∼10 days), we can place limitations on how much data can be searched coherently. In an all-sky search for pulsars having gravity-wave frequencies f<~200 Hz and spindown ages τ>~1000 yr, one can coherently search ∼18 days of data on a teraflops computer. In contrast, a teraflops computer can only perform a ∼0.8-day coherent search for pulsars with frequencies f<~1 kHz and spindown ages as low as 40 yr. In addition to all-sky searches we consider coherent directed searches, where one knows in advance the source position but not the period. (Nearby supernova remnants and the galactic center are obvious places to look.) We show that for such a search, one gains a factor of ∼10 in observation time over the case of an all-sky search, given a 1 Tflops computer. The enormous computational burden involved in coherent searches indicates the need for alternative data analysis strategies. As an example we briefly discuss the implementation of a simple hierarchical search in the last section of the paper. Further work is required to determine the optimal approach.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1103/PhysRevD.57.2101DOIUNSPECIFIED
http://link.aps.org/abstract/PRD/v57/p2101PublisherUNSPECIFIED
Additional Information:© 1998 The American Physical Society. (Received 27 February 1997, published 12 January 1998) P.R.B. and T.C. wish to thank Kip Thorne for suggesting that we work on this problem; we are extremely grateful to him for his encouragement and suggestions. P.R.B. and T.C. also thank Bruce Allen, Kent Blackburn, Jolien Creighton, Sam Finn, Scott Hughes, Ben Owen, Massimo Tinto, and Alan Wiseman for useful discussions. This work was supported in part by NSF grant PHY-9424337. P.R.B. is grateful to the Sherman Fairchild Foundation for financial support. B.F.S. wishes to thank Gareth Jones, Andrez Krolak, Andrew Lyne, and David Nicolson for useful conversations. C.C. thanks Lee Lindblom for helpful discussions; C.C.’s work was supported in part by NSF grant PHY-9507686 and by a grant from the Alfred P. Sloan Foundation.
Group:TAPIR
Funders:
Funding AgencyGrant Number
National Science FoundationPHY-9424337
Sherman Fairchild FoundationUNSPECIFIED
National Science FoundationPHY-9507686
Alfred P. Sloan FoundationUNSPECIFIED
Record Number:CaltechAUTHORS:BRAprd98b
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:BRAprd98b
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:12435
Collection:CaltechAUTHORS
Deposited By: Archive Administrator
Deposited On:26 Nov 2008 19:26
Last Modified:26 Dec 2012 10:31

Repository Staff Only: item control page