Aspen 
Maroon Bells / Gravitational Waves / Link to Aspen Center for Physics Aspen 
Maroon Bells / Gravitational Waves / Link to Aspen Center for Physics Aspen 
Maroon Bells / Gravitational Waves / Link to Aspen Center for Physics Aspen 
Maroon Bells / Gravitational Waves / Link to Aspen Center for Physics Aspen 
Maroon Bells / Gravitational Waves / Link to Aspen Center for Physics Aspen 
Maroon Bells / Gravitational Waves / Link to Aspen Center for Physics Aspen 
Maroon Bells / Gravitational Waves / Link to Aspen Center for Physics Aspen 
Maroon Bells / Gravitational Waves / Link to Aspen Center for Physics Aspen 
Maroon Bells / Gravitational Waves / Link to Aspen Center for Physics Aspen 
Maroon Bells / Gravitational Waves / Link to Aspen Center for Physics
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        MOTIVATION

The space-based gravitational radiation detector, LISA, will be sensitive to gravitational radiation in the frequency range from 10-5 to 1 Hz. Astrophysical sources in this range include compact binaries and black holes with a variety of masses.

Artist's concept of the LISA mission.
Artist's concept of the Laser Interferometer Space Antenna (LISA) mission.

The detection of gravitational radiation and the mapping of spacetime in the strong field regime is an important goal of LISA. It is equally important to use this radiation to shed light on the source astrophysics.

The goal of this workshop is to bring together members of the astrophysics community, the gravitational wave detector community, and the data analysis community to stimulate discussions and understanding of the astrophysics that can be done using gravitational radiation. Hundreds of events are expected to be detected per year, many at high signal-to-noise. In addition, thousands of identifiable continuous sources are expect to be present in the data. Finally, millions of stellar mass binaries in the galaxy will contribute to a confusion-limited foreground. Thus, LISA is like a gravitational wave telescope. In order to maximize the science potential of the data gathered by this telescope, it is important to get these three communities interacting as soon as possible. Potential LISA sources can be grouped in three general classes -- massive black hole binaries, extreme mass ratio inspirals, and intermediate/stellar mass compact object binaries. Each class of source presents unique issues involving detection, source simulation, and population synthesis.

The workshop will address these issues by focusing on each particular class of gravitational source each week. We hope to have the following schedule:

Week 1: Massive black hole binary inspiral
Week 2: Extreme mass ratio inspiral
Week 3: Stellar mass binaries and foregrounds

Since the main purpose of the workshop is to foster discussion between the relevant communities, we anticipate starting each week with two or three talks by relevant astrophysicists, source simulators, and data analysts to focus the discussions. At the end of the week we would hope for two or three talks addressing progress or ideas for new directions. The remainder of the time will be reserved for interaction and informal discussions.

LISA orbit highlighting 1 particular spacecraft over a year
 LISA orbit highlighting 1 particular spacecraft over a year

The LISA mission is planned for a 2013 launch with technology demonstration missions (LTP and ST7) planned for the LISA Pathfinder mission in 2007. LISA has been scheduled as the next major mission in the "Beyond Einstein" roadmap for NASA, and work is progressing on the LISA Pathfinder mission. It is important that techniques for tying the astrophysics of sources with data analysis be developed soon to maximize the science that can be done with LISA. It is expected that this workshop will further the discussions between the astrophysics, source simulation, and gravitational wave data analysis communities.

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    ORGANIZERS

    Matt Benacquista (Montana State University-Billings)
    Sam Finn (Penn State University)
    Vicky Kalogera (Northwestern University)
    Alberto Vecchio (University of Birmingham, UK)


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