TY - JOUR
T1 - Event rate for extreme mass ratio burst signals in the laser interferometer space antenna band
AU - Rubbo, Louis J.
AU - Holley-Bockelmann, Kelly
AU - Lee, Samuel Finn
N1 - Funding Information:
The authors are grateful to T. Bogdanovic, M. Freitag, P. Laguna, S. Larson, C. Miller, S. Sigurdsson, and D. Shoemaker for numerous helpful discussions on all aspects of this project. This work was supported by NASA NNG04GU99G, NASA NNG05GF71G, NSF PHY 00-99559 and the Center for Gravitational Wave Physics, which is funded by the National Science Foundation under cooperative agreement PHY 01-14375.
PY - 2006/9/20
Y1 - 2006/9/20
N2 - Stellar mass compact objects in short-period (P ≲ 103 s) orbits about a 104.5-107.5 M⊙ massive black hole (MBH) are thought to be a significant continuous-wave source of gravitational radiation for the ESA/NASA Laser Interferometer Space Antenna (LISA) gravitational wave detector. These extreme mass ratio inspiral sources began in long-period, nearly parabolic orbits that have multiple close encounters with the MBH. The gravitational radiation emitted during the close encounters may be detectable by LISA as a gravitational wave burst if the characteristic passage timescale is less than 105 s. Scaling a static, spherical model to the size and mass of the Milky Way bulge, we estimate an event rate of ∼15 yr-1 for such burst signals, detectable by LISA with signal-to-noise ratio greater than 5, originating in our Galaxy. When extended to include Virgo Cluster galaxies, our estimate increases to a gravitational wave burst rate of ∼18 yr-1. We conclude that these extreme mass ratio burst sources may be a steady and significant source of gravitational radiation in the LISA data streams.
AB - Stellar mass compact objects in short-period (P ≲ 103 s) orbits about a 104.5-107.5 M⊙ massive black hole (MBH) are thought to be a significant continuous-wave source of gravitational radiation for the ESA/NASA Laser Interferometer Space Antenna (LISA) gravitational wave detector. These extreme mass ratio inspiral sources began in long-period, nearly parabolic orbits that have multiple close encounters with the MBH. The gravitational radiation emitted during the close encounters may be detectable by LISA as a gravitational wave burst if the characteristic passage timescale is less than 105 s. Scaling a static, spherical model to the size and mass of the Milky Way bulge, we estimate an event rate of ∼15 yr-1 for such burst signals, detectable by LISA with signal-to-noise ratio greater than 5, originating in our Galaxy. When extended to include Virgo Cluster galaxies, our estimate increases to a gravitational wave burst rate of ∼18 yr-1. We conclude that these extreme mass ratio burst sources may be a steady and significant source of gravitational radiation in the LISA data streams.
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U2 - 10.1086/508326
DO - 10.1086/508326
M3 - Article
AN - SCOPUS:33751116802
SN - 0004-637X
VL - 649
SP - L25-L28
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1 II
ER -