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Conference Paper

The Mock LISA Data Challenges: from Challenge 1B to Challenge 3

MPS-Authors
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Babak,  Stanislav
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

Porter,  Edward K.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

Gair,  Jonathan
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons40534

Prix,  Reinhard
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

Wen,  Linqing
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons4293

Whelan,  John T.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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cqg8_18_184026.pdf
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Citation

Babak, S., Baker, J. G., Benacquista, M. J., Cornish, N. J., Crowder, J., Larson, S. L., et al. (2008). The Mock LISA Data Challenges: from Challenge 1B to Challenge 3. Classical and Quantum Gravity, 25(18): 184026. doi:10.1088/0264-9381/25/18/184026.


Cite as: https://hdl.handle.net/11858/00-001M-0000-0013-1339-5
Abstract
The Mock LISA Data Challenges are a programme to demonstrate and encourage the development of LISA data-analysis capabilities, tools and techniques. At the time of this workshop, three rounds of challenges had been completed, and the next was about to start. In this paper we provide a critical analysis of the entries to the latest completed round, Challenge 1B. The entries confirm the consolidation of a range of data-analysis techniques for galactic and massive-black-hole binaries, and they include the first convincing examples of detection and parameter estimation of extreme-mass-ratio inspiral sources. In this paper we also introduce the next round, Challenge 3. Its data sets feature more realistic waveform models (e. g., galactic binaries may now chirp, and massive-black-hole binaries may precess due to spin interactions), as well as new source classes (bursts from cosmic strings, isotropic stochastic backgrounds) and more complicated nonsymmetric instrument noise.