Search for gravitational wave ringdowns from perturbed black holes in LIGO S4 data
Name
Abbott-2009-Search for gravitati.pdf
Size
1.3 MB
Format
Adobe PDF
Checksum (MD5)
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Author(s)
Wipf, Christopher C.
Weiss, Rainer
Waldman, Samuel J.
Stein, Leo Chaim
Stein, Andrew J.
Smith, Nicolas de Mateo
Shapiro, B.
Sarin, P.
Markowitz, Jared John
Katsavounidis, Erotokritos
Date Issued
September 2009
Journal
Physical Review D
Publisher
American Physical Society
Citation
The LIGO Scientic Collaboration et al. “Search for gravitational wave ringdowns from perturbed black holes in LIGO S4 data.” Physical Review D 80.6 (2009): 062001. © 2009 The American Physical Society
Version
Final published version
Abstract
According to general relativity a perturbed black hole will settle to a stationary configuration by the emission of gravitational radiation. Such a perturbation will occur, for example, in the coalescence of a black hole binary, following their inspiral and subsequent merger. At late times the waveform is a superposition of quasinormal modes, which we refer to as the ringdown. The dominant mode is expected to be the fundamental mode, l=m=2. Since this is a well-known waveform, matched filtering can be implemented to search for this signal using LIGO data. We present a search for gravitational waves from black hole ringdowns in the fourth LIGO science run S4, during which LIGO was sensitive to the dominant mode of perturbed black holes with masses in the range of 10M[subscript ⊙] to 500M[subscript ⊙], the regime of intermediate-mass black holes, to distances up to 300 Mpc. We present a search for gravitational waves from black hole ringdowns using data from S4. No gravitational wave candidates were found; we place a 90%-confidence upper limit on the rate of ringdowns from black holes with mass between 85M[subscript ⊙] and 390M[subscript ⊙] in the local universe, assuming a uniform distribution of sources, of 3.2×10[superscript -5] yr[superscript -1] Mpc[superscript -3]=1.6×10[superscript -3] yr[superscript -1]L10[superscript -1],where L[subscript 10] is 10[superscript 10] times the solar blue-light luminosity.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
http://dx.doi.org/10.1103/PhysRevD.80.062001
