| NSF Org: |
PHY Division Of Physics |
| Recipient: |
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| Initial Amendment Date: | October 29, 2007 |
| Latest Amendment Date: | October 5, 2009 |
| Award Number: | 0653582 |
| Award Instrument: | Continuing Grant |
| Program Manager: |
Pedro Marronetti
pmarrone@nsf.gov (703)292-7372 PHY Division Of Physics MPS Directorate for Mathematical and Physical Sciences |
| Start Date: | November 1, 2007 |
| End Date: | October 31, 2011 (Estimated) |
| Total Intended Award Amount: | $450,000.00 |
| Total Awarded Amount to Date: | $450,000.00 |
| Funds Obligated to Date: |
FY 2009 = $150,000.00 FY 2010 = $150,000.00 |
| History of Investigator: |
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| Recipient Sponsored Research Office: |
1523 UNION RD RM 207 GAINESVILLE FL US 32611-1941 (352)392-3516 |
| Sponsor Congressional District: |
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| Primary Place of Performance: |
1523 UNION RD RM 207 GAINESVILLE FL US 32611-1941 |
| Primary Place of
Performance Congressional District: |
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| Unique Entity Identifier (UEI): |
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| Parent UEI: |
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| NSF Program(s): | LIGO RESEARCH SUPPORT |
| Primary Program Source: |
01000910DB NSF RESEARCH & RELATED ACTIVIT 01001011DB NSF RESEARCH & RELATED ACTIVIT |
| Program Reference Code(s): |
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| Program Element Code(s): |
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| Award Agency Code: | 4900 |
| Fund Agency Code: | 4900 |
| Assistance Listing Number(s): | 47.049 |
ABSTRACT
Future interferometric gravitational wave detectors such as enhanced LIGO and Advanced LIGO will only reach their fundamental sensitivity limits if significant technical problems can be solved first. Many laser power related problems can be reduced significantly by using adaptive mode matching techniques and employing a new optical configuration known as a stable recycling cavity. The interaction of these techniques and configuration changes on other subsystems will be studied in this research effort. Advanced interferometric detectors also depend on improved sensors and improved modulation techniques. These technologies will be developed beyond the current state of the art.
During the commissioning of the LIGO detectors unexpected problems were discovered and in many cases non-optimal solutions where used to mitigate the problems. These often improvised solutions are sufficient for LIGO but will not be sufficient in future detectors like Advanced LIGO. New solutions have been developed for Advanced LIGO but their broad impact on the entire instrument may not be fully understood. New technologies have to be developed or older technologies have to be improved to ensure the success of future gravitational wave detectors. These technology developments are also a chance for new students and postdocs to participate in and contribute to this very exciting and still expanding scientific area.
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