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| == LCGT Bandwidth Study 2011 == | == LCGT Bandwidth Study 2011 (new design with 22cm mirrors) == 1st meeting: 2011 9/9 2pm-4pm [[http://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/DocDB/ShowDocument?docid=590|slides]]<<BR>> 2nd meeting: 2011 9/22 10am-12pm [[http://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=599|slides]]<<BR>> === Scope of the meeting === It has recently turned out that the largest S-axis Sapphire available right now is not as large as 25cm in diameter but 22cm.<<BR>> And the measured absorption of a Sapphire substrate is not as low as 20ppm/cm but 50-70ppm/cm.<<BR>> It should be also noted that the economic situation is not so good that we cannot expect too much on an additional large budget<<BR>> within the next few years, and also that it takes three years or more to provide 4 Sapphire mirrors, which means we should<<BR>> make it in mind that the mirrors we are ordering will be the one we use in 2017. === 1st meeting reference === * 25W injection <<BR>> . [[attachment:25Wcontour.pdf|IR vs Finesse/Rs]]<<BR>> [[attachment:25Wplot.pdf|Spectrum with 25W]]<<BR>> [[attachment:25Wspectra.pdf|Spectra with 25/50/75W]]<<BR>> * 50W injection <<BR>> . [[attachment:50Wcontour.pdf|IR vs Finesse/Rs]]<<BR>> [[attachment:50Wplot.pdf|Spectrum with 50W]]<<BR>> [[attachment:50Wspectra.pdf|Spectra with 25/50/75W]]<<BR>> * 75W injection <<BR>> . [[attachment:75Wcontour.pdf|IR vs Finesse/Rs]]<<BR>> [[attachment:75Wplot.pdf|Spectrum with 75W]]<<BR>> [[attachment:75Wspectra.pdf|Spectra with 25/50/75W]]<<BR>> The input power refers the level of absorption; if the total absorption is high we can inject only 25W while the default is 75W.<<BR>> Here the power recycling gain is set 11, i.e. the power on the BS is 275W, 550W, 825W, for 25, 50, 75W, respectively. * Preliminary cryogenic setup with 1.2W heat and point-scattering effect (It seems that we can inject 75W into <<BR>> the interferometer, allowing the mirror temperature to be 23.5K instead of 20K). . [[attachment:newconfig.pdf|file]]<<BR>> === Influence on the detection of high frequency gravitational waves === * GWs from supernovae [[attachment:hayama09092011.pdf|FILE]] === Minutes of the first meeting === * [[http://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=600|Minutes]]<<BR>> === 2nd meeting reference === * Slides are [[http://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=599|here]]<<BR>> * Data sets are [[attachment:ToTagoshisan.txt|here]].<<BR>> |
LCGT Bandwidth Study 2011 (new design with 22cm mirrors)
1st meeting: 2011 9/9 2pm-4pm slides
2nd meeting: 2011 9/22 10am-12pm slides
Scope of the meeting
It has recently turned out that the largest S-axis Sapphire available right now is not as large as 25cm in diameter but 22cm.
And the measured absorption of a Sapphire substrate is not as low as 20ppm/cm but 50-70ppm/cm.
It should be also noted that the economic situation is not so good that we cannot expect too much on an additional large budget
within the next few years, and also that it takes three years or more to provide 4 Sapphire mirrors, which means we should
make it in mind that the mirrors we are ordering will be the one we use in 2017.
1st meeting reference
25W injection
50W injection
75W injection
The input power refers the level of absorption; if the total absorption is high we can inject only 25W while the default is 75W.
Here the power recycling gain is set 11, i.e. the power on the BS is 275W, 550W, 825W, for 25, 50, 75W, respectively.
Preliminary cryogenic setup with 1.2W heat and point-scattering effect (It seems that we can inject 75W into
the interferometer, allowing the mirror temperature to be 23.5K instead of 20K).
Influence on the detection of high frequency gravitational waves
GWs from supernovae FILE
Minutes of the first meeting