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http://hdl.handle.net/2289/6255Full metadata record
| DC Field | Value | Language |
|---|---|---|
| dc.contributor.author | Aasi, J. | - |
| dc.contributor.author | Abbott, B.P. | - |
| dc.contributor.author | Abbott, R. | - |
| dc.contributor.author | Iyer, B.R. | - |
| dc.contributor.author | LIGO Scientific Collaboration and Virgo Collaboration | - |
| dc.contributor.author | +250 Co authors | - |
| dc.date.accessioned | 2015-07-28T09:49:56Z | - |
| dc.date.available | 2015-07-28T09:49:56Z | - |
| dc.date.issued | 2015-04-09 | - |
| dc.identifier.citation | Classical and Quantum Gravity, 2015, Vol.32, p074001 | en |
| dc.identifier.issn | 0264-9381 | - |
| dc.identifier.issn | 1361-6382 (online) | - |
| dc.identifier.uri | http://hdl.handle.net/2289/6255 | - |
| dc.description | Restricted Access. An open-access version is available at arXiv.org (one of the alternative locations) | en |
| dc.description.abstract | The Advanced LIGO gravitational wave detectors are second-generation instruments designed and built for the two LIGO observatories in Hanford, WA and Livingston, LA, USA. The two instruments are identical in design, and are specialized versions of a Michelson interferometer with 4 km long arms. As in Initial LIGO, Fabry–Perot cavities are used in the arms to increase the interaction time with a gravitational wave, and power recycling is used to increase the effective laser power. Signal recycling has been added in Advanced LIGO to improve the frequency response. In the most sensitive frequency region around 100 Hz, the design strain sensitivity is a factor of 10 better than Initial LIGO. In addition, the low frequency end of the sensitivity band is moved from 40 Hz down to 10 Hz. All interferometer components have been replaced with improved technologies to achieve this sensitivity gain. Much better seismic isolation and test mass suspensions are responsible for the gains at lower frequencies. Higher laser power, larger test masses and improved mirror coatings lead to the improved sensitivity at mid and high frequencies. Data collecting runs with these new instruments are planned to begin in mid-2015. | en |
| dc.language.iso | en | en |
| dc.publisher | IOP Publishing Ltd. | en |
| dc.relation.uri | http://arxiv.org/abs/1411.4547 | en |
| dc.relation.uri | http://dx.doi.org/10.1088/0264-9381/32/7/074001 | en |
| dc.relation.uri | http://adsabs.harvard.edu/abs/2015CQGra..32g4001T | en |
| dc.rights | 2015 IOP Publishing Ltd. | en |
| dc.title | Advanced LIGO | en |
| dc.type | Article | en |
| Appears in Collections: | Research Papers (TP) | |
Files in This Item:
| File | Description | Size | Format | |
|---|---|---|---|---|
| 2015_CQG_32_7_074001.pdf Restricted Access | Restricted Access | 4.73 MB | Adobe PDF | View/Open Request a copy |
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