Einstein Telescope: seismic and GGN...
Transcript of Einstein Telescope: seismic and GGN...
![Page 1: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/1.jpg)
Mark Beker, Nikhef Amsterdamon behalf of the ET design study teamGWADW 2010, Kyoto, Japan17 May 2010
Einstein Telescope: seismic and GGN studies
Tuesday, May 18, 2010
![Page 2: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/2.jpg)
Gravity gradient noise may limit Einstein Telescope sensitivity at low frequencies
2
Seismic noise spectrum - displacement
ASD
[m/rt
Hz]
Frequency [Hz]
GGN calculationsHigh/Low noise model
1e-12
1e-11
1e-10
1e-09
1e-08
1e-07
1e-06
1e-05
0.1 1 10
ET noise budget
10 0 10 1 10 210 26
10 25
10 24
10 23
10 22
10 21
10 20
10 19
Frequency [Hz]
Quantum noiseSeismic noiseNewtonian noiseCoating Brownian noiseCoating thermo-optic noiseSubstrate Brownian noiseExcess gasTotal noiseAdvanced VirgoET target
Strain
[1/
Hz]
Assumptions: - Surface detector - Isotropic body pressure waves - Seismic spectrum: (5 nm/ f2 )/√Hz
Saulson’s model prediction of GGNET-B requirement 0.1 nm/√HzET-C requirement (0.1 nm/ f2 )/√Hz
[S. Hild et. al. arXiv.org:0810.0604][P. R. Saulson, Phys. Rev. D, 30, 1984]
Tuesday, May 18, 2010
![Page 3: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/3.jpg)
Gravity gradient noise may limit Einstein Telescope sensitivity at low frequencies
2
Seismic noise spectrum - displacement
ASD
[m/rt
Hz]
Frequency [Hz]
GGN calculationsHigh/Low noise model
1e-12
1e-11
1e-10
1e-09
1e-08
1e-07
1e-06
1e-05
0.1 1 10
ET noise budget
10 0 10 1 10 210 26
10 25
10 24
10 23
10 22
10 21
10 20
10 19
Frequency [Hz]
Quantum noiseSeismic noiseNewtonian noiseCoating Brownian noiseCoating thermo-optic noiseSubstrate Brownian noiseExcess gasTotal noiseAdvanced VirgoET target
Strain
[1/
Hz]
Assumptions: - Surface detector - Isotropic body pressure waves - Seismic spectrum: (5 nm/ f2 )/√Hz
Saulson’s model prediction of GGNET-B requirement 0.1 nm/√HzET-C requirement (0.1 nm/ f2 )/√Hz
[S. Hild et. al. arXiv.org:0810.0604][P. R. Saulson, Phys. Rev. D, 30, 1984]
Tuesday, May 18, 2010
![Page 4: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/4.jpg)
Gravity gradient noise may limit Einstein Telescope sensitivity at low frequencies
2
Seismic noise spectrum - displacement
ASD
[m/rt
Hz]
Frequency [Hz]
GGN calculationsHigh/Low noise model
1e-12
1e-11
1e-10
1e-09
1e-08
1e-07
1e-06
1e-05
0.1 1 10
ET noise budget
10 0 10 1 10 210 26
10 25
10 24
10 23
10 22
10 21
10 20
10 19
Frequency [Hz]
Quantum noiseSeismic noiseNewtonian noiseCoating Brownian noiseCoating thermo-optic noiseSubstrate Brownian noiseExcess gasTotal noiseAdvanced VirgoET target
Strain
[1/
Hz]
Assumptions: - Surface detector - Isotropic body pressure waves - Seismic spectrum: (5 nm/ f2 )/√Hz
Saulson’s model prediction of GGNET-B requirement 0.1 nm/√HzET-C requirement (0.1 nm/ f2 )/√Hz
[S. Hild et. al. arXiv.org:0810.0604][P. R. Saulson, Phys. Rev. D, 30, 1984]
Tuesday, May 18, 2010
![Page 5: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/5.jpg)
ET sensitivity requirements corresponds to a seismic acceleration PSD of 3x10-17 (m2/s4) f4/Hz
3
PSD
[(m
2/s4
)/Hz]
Frequency [Hz]
ET-B requirementsHigh/Low noise model
1e-19 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e-10 1e-09
0.1 1 10
Seismic noise spectrum - acceleration
ASD
[m/H
z]
Frequency [Hz]
ET-B requirementsHigh/Low noise model
1e-12
1e-11
1e-10
1e-09
1e-08
1e-07
1e-06
1e-05
0.1 1 10
Seismic noise spectrum - displacement
Tuesday, May 18, 2010
![Page 6: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/6.jpg)
Can a suitably seismically quiet location be found to satisfy this requirement?
4
PSD
[(m
2/s4
)/Hz]
Frequency [Hz]
ET-B requirementsHigh/Low noise model
1e-19 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e-10 1e-09
0.1 1 10
Tuesday, May 18, 2010
![Page 7: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/7.jpg)
Seismic measurements have been done throughout Europe to classify underground locations
• 2 Trillium 240 seismometers• Broadband mHz - 30 Hz
• Hard-rock tile
• Insulation cover
• Data acquisition systems• LabView readout through 18 bit DAQ card
• Low noise amplifier
5Tuesday, May 18, 2010
![Page 8: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/8.jpg)
Seismic measurements have been done throughout Europe to classify underground locations
• 2 Trillium 240 seismometers• Broadband mHz - 30 Hz
• Hard-rock tile
• Insulation cover
• Data acquisition systems• LabView readout through 18 bit DAQ card
• Low noise amplifier
5Tuesday, May 18, 2010
![Page 9: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/9.jpg)
Seismic measurements have been done throughout Europe to classify underground locations
• 2 Trillium 240 seismometers• Broadband mHz - 30 Hz
• Hard-rock tile
• Insulation cover
• Data acquisition systems• LabView readout through 18 bit DAQ card
• Low noise amplifier
5Tuesday, May 18, 2010
![Page 10: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/10.jpg)
Seismic measurements have been done throughout Europe to classify underground locations
• 2 Trillium 240 seismometers• Broadband mHz - 30 Hz
• Hard-rock tile
• Insulation cover
• Data acquisition systems• LabView readout through 18 bit DAQ card
• Low noise amplifier
5Tuesday, May 18, 2010
![Page 11: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/11.jpg)
Seismic measurements have been done throughout Europe to classify underground locations
• 2 Trillium 240 seismometers• Broadband mHz - 30 Hz
• Hard-rock tile
• Insulation cover
• Data acquisition systems• LabView readout through 18 bit DAQ card
• Low noise amplifier
5Tuesday, May 18, 2010
![Page 12: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/12.jpg)
6
5/14/10 6:30 AMEinstein Telescope project - Google Maps
Page 1 of 5http://maps.google.com/maps/ms?f=q&source=s_q&hl=en&geocode=…5ff&ll=52.643063,18.017578&spn=29.791782,68.466797&z=4&pw=1
ETseismic locations0 views - PublicCreated on May 13 - Updated < 1 minute agoBy mbekerRate this map - Write a comment
SITE CHARACTERISTICS:- Decommissioned lead mine.- Local geology is andesite (wave speed equal to granite)
GYÖNGYÖSOROSZI MINE
Data collected from these sites
Measurements still to be carried out at these sites
Tuesday, May 18, 2010
![Page 13: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/13.jpg)
6
5/14/10 6:30 AMEinstein Telescope project - Google Maps
Page 1 of 5http://maps.google.com/maps/ms?f=q&source=s_q&hl=en&geocode=…5ff&ll=52.643063,18.017578&spn=29.791782,68.466797&z=4&pw=1
ETseismic locations0 views - PublicCreated on May 13 - Updated < 1 minute agoBy mbekerRate this map - Write a comment
SITE CHARACTERISTICS:- Decommissioned lead mine.- Local geology is andesite (wave speed equal to granite)
GYÖNGYÖSOROSZI MINE
Data collected from these sites
Measurements still to be carried out at these sites
Underground data available from these sites
Tuesday, May 18, 2010
![Page 14: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/14.jpg)
6
5/14/10 6:30 AMEinstein Telescope project - Google Maps
Page 1 of 5http://maps.google.com/maps/ms?f=q&source=s_q&hl=en&geocode=…5ff&ll=52.643063,18.017578&spn=29.791782,68.466797&z=4&pw=1
ETseismic locations0 views - PublicCreated on May 13 - Updated < 1 minute agoBy mbekerRate this map - Write a comment
SITE CHARACTERISTICS:- Decommissioned lead mine.- Local geology is andesite (wave speed equal to granite)
GYÖNGYÖSOROSZI MINE
Data collected from these sites
Measurements still to be carried out at these sites
5/16/10 10:52 AMInotani Station, Japan - Google Maps
Page 1 of 2http://maps.google.com/
Address
AND, Basarsoft, Geocentre Consulting, Mapabc, PPWK, Tele Atlas, Transnavicom, Europa Technologies, Google, INEGI, LeadDog Consulting, MapLink -
ETseismic locations
SITE CHARACTERISTICS:- Decommissioned lead mine.- Local geology is andesite (wave speed equal to granite)- Longest mine drift is approximately 3km.- Mine is at 330m depth.- Current seismic station is at approx 50m.- Local population density 75/km2 (Gyongyosoroszi 21.39km2)- Distance to sea or ocean is approximately 500km.SITE MEASUREMENTS:01/04/2010 UNTIL 07/04/2010Seismic info:https://workarea.et-gw.eu/et/general/public-slides/sites/Hungary.pdf
GYÖNGYÖSOROSZI MINE
View in Google Earth Print Send Link Get Directions My Maps
To see all the details that are visible on thescreen,use the "Print" link next to the map.
2 Seismometers in Homestake mine, SD
Underground data available from these sites
Tuesday, May 18, 2010
![Page 15: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/15.jpg)
6
5/14/10 6:30 AMEinstein Telescope project - Google Maps
Page 1 of 5http://maps.google.com/maps/ms?f=q&source=s_q&hl=en&geocode=…5ff&ll=52.643063,18.017578&spn=29.791782,68.466797&z=4&pw=1
ETseismic locations0 views - PublicCreated on May 13 - Updated < 1 minute agoBy mbekerRate this map - Write a comment
SITE CHARACTERISTICS:- Decommissioned lead mine.- Local geology is andesite (wave speed equal to granite)
GYÖNGYÖSOROSZI MINE
Data collected from these sites
Measurements still to be carried out at these sites
5/16/10 10:52 AMInotani Station, Japan - Google Maps
Page 1 of 2http://maps.google.com/
Address
AND, Basarsoft, Geocentre Consulting, Mapabc, PPWK, Tele Atlas, Transnavicom, Europa Technologies, Google, INEGI, LeadDog Consulting, MapLink -
ETseismic locations
SITE CHARACTERISTICS:- Decommissioned lead mine.- Local geology is andesite (wave speed equal to granite)- Longest mine drift is approximately 3km.- Mine is at 330m depth.- Current seismic station is at approx 50m.- Local population density 75/km2 (Gyongyosoroszi 21.39km2)- Distance to sea or ocean is approximately 500km.SITE MEASUREMENTS:01/04/2010 UNTIL 07/04/2010Seismic info:https://workarea.et-gw.eu/et/general/public-slides/sites/Hungary.pdf
GYÖNGYÖSOROSZI MINE
View in Google Earth Print Send Link Get Directions My Maps
To see all the details that are visible on thescreen,use the "Print" link next to the map.
2 Seismometers in Homestake mine, SD
5/16/10 10:57 AMInotani Station, Japan - Google Maps
Page 1 of 2http://maps.google.com/
Address
©2010 Google - Map data ©2010 AND, Europa Technologies, Geocentre Consulting, Mapabc, ZENRIN, SK M&C -
SITE CHARACTERISTICS:- Decommissioned salt mine (largest salt mine in Europe)- Local geology is andesite.- Already contains some large caverns.- Current depth of seismic station is unknown.- Depth of mine is at a few hundreds of metres.- Local population density is 180/km2 (Slanic 40km2).- Distance to sea or ocean is 300km.SITE MEASUREMENTS:08/04/2010 UNTIL 14/04/2010 Seismic info:https://workarea.et-gw.eu/et/general/public-slides/sites/Romania-SLANIC-PRAHOVA.pdf
Sl!nic
Baksan Neutrino Observatory
View in Google Earth Print Send Link Get Directions My Maps
To see all the details that are visible on thescreen,use the "Print" link next to the map.
Underground data available from these sites
Thanks to:Dr. Kazuaki KurodaDr. Uchiyama TakashiDr. Osamu MiyakawaDr. Shinji Miyoki
Tuesday, May 18, 2010
![Page 16: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/16.jpg)
6
5/14/10 6:30 AMEinstein Telescope project - Google Maps
Page 1 of 5http://maps.google.com/maps/ms?f=q&source=s_q&hl=en&geocode=…5ff&ll=52.643063,18.017578&spn=29.791782,68.466797&z=4&pw=1
ETseismic locations0 views - PublicCreated on May 13 - Updated < 1 minute agoBy mbekerRate this map - Write a comment
SITE CHARACTERISTICS:- Decommissioned lead mine.- Local geology is andesite (wave speed equal to granite)
GYÖNGYÖSOROSZI MINE
Data collected from these sites
Measurements still to be carried out at these sites
5/16/10 10:52 AMInotani Station, Japan - Google Maps
Page 1 of 2http://maps.google.com/
Address
AND, Basarsoft, Geocentre Consulting, Mapabc, PPWK, Tele Atlas, Transnavicom, Europa Technologies, Google, INEGI, LeadDog Consulting, MapLink -
ETseismic locations
SITE CHARACTERISTICS:- Decommissioned lead mine.- Local geology is andesite (wave speed equal to granite)- Longest mine drift is approximately 3km.- Mine is at 330m depth.- Current seismic station is at approx 50m.- Local population density 75/km2 (Gyongyosoroszi 21.39km2)- Distance to sea or ocean is approximately 500km.SITE MEASUREMENTS:01/04/2010 UNTIL 07/04/2010Seismic info:https://workarea.et-gw.eu/et/general/public-slides/sites/Hungary.pdf
GYÖNGYÖSOROSZI MINE
View in Google Earth Print Send Link Get Directions My Maps
To see all the details that are visible on thescreen,use the "Print" link next to the map.
2 Seismometers in Homestake mine, SD
5/16/10 10:57 AMInotani Station, Japan - Google Maps
Page 1 of 2http://maps.google.com/
Address
©2010 Google - Map data ©2010 AND, Europa Technologies, Geocentre Consulting, Mapabc, ZENRIN, SK M&C -
SITE CHARACTERISTICS:- Decommissioned salt mine (largest salt mine in Europe)- Local geology is andesite.- Already contains some large caverns.- Current depth of seismic station is unknown.- Depth of mine is at a few hundreds of metres.- Local population density is 180/km2 (Slanic 40km2).- Distance to sea or ocean is 300km.SITE MEASUREMENTS:08/04/2010 UNTIL 14/04/2010 Seismic info:https://workarea.et-gw.eu/et/general/public-slides/sites/Romania-SLANIC-PRAHOVA.pdf
Sl!nic
Baksan Neutrino Observatory
View in Google Earth Print Send Link Get Directions My Maps
To see all the details that are visible on thescreen,use the "Print" link next to the map.
Underground data available from these sites
Thanks to:Dr. Kazuaki KurodaDr. Uchiyama TakashiDr. Osamu MiyakawaDr. Shinji Miyoki
Surface seismic data from > 200 sites (Orfeus network)
Tuesday, May 18, 2010
![Page 17: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/17.jpg)
7
Characterization of sites is done using spectral variation plots of half hour averages
The Netherlands
Tuesday, May 18, 2010
![Page 18: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/18.jpg)
7
Characterization of sites is done using spectral variation plots of half hour averages
The NetherlandsSpain - Lab. Sub. Canfranc
Tuesday, May 18, 2010
![Page 19: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/19.jpg)
Locations in Hungary, France and Spain have shown to be within ET-B requirements > 2 Hz
8
1e-17
1e-16
1e-15
1e-14
1e-13
1e-12
1e-11
0.1 1 10Frequency [Hz]
Mode from half hour PSDs N
PSD
[m /s
/Hz
]2
4
RomaniaHolland
HungarySpain - LSC
France - LSMHigh/Low noise model
ET-B req.
Tuesday, May 18, 2010
![Page 20: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/20.jpg)
Locations in Hungary, France and Spain have shown to be within ET-B requirements > 2 Hz
8
1e-17
1e-16
1e-15
1e-14
1e-13
1e-12
1e-11
0.1 1 10Frequency [Hz]
Mode from half hour PSDs N
PSD
[m /s
/Hz]
24
RomaniaHolland
HungarySpain - LSC
France - LSMHigh/Low noise model
ET-B req.
Error bars indicate 90 and 10%
occurrence levels
Tuesday, May 18, 2010
![Page 21: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/21.jpg)
Locations in Hungary, France and Spain have shown to be within ET-B requirements > 2 Hz
8
10 m2000 m200 m400 m800 m
Depth
1e-17
1e-16
1e-15
1e-14
1e-13
1e-12
1e-11
0.1 1 10Frequency [Hz]
Mode from half hour PSDs N
PSD
[m /s
/Hz]
24
RomaniaHolland
HungarySpain - LSC
France - LSMHigh/Low noise model
ET-B req.
Error bars indicate 90 and 10%
occurrence levels
Tuesday, May 18, 2010
![Page 22: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/22.jpg)
Locations in Hungary, France and Spain have shown to be within ET-B requirements > 2 Hz
8
10 m2000 m200 m400 m800 m
Depth
1e-17
1e-16
1e-15
1e-14
1e-13
1e-12
1e-11
0.1 1 10Frequency [Hz]
Mode from half hour PSDs N
PSD
[m /s
/Hz]
24
RomaniaHolland
HungarySpain - LSC
France - LSMHigh/Low noise model
ET-B req.
Error bars indicate 90 and 10%
occurrence levels
Romania was a working salt mine
Tuesday, May 18, 2010
![Page 23: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/23.jpg)
SuSa Mo
9
Seismic noise at 1 - 20 Hz is dominated by anthropogenic activity
Earthquake, Solomon Islands, Magnitude 6.8 Mining blast
Tuesday, May 18, 2010
![Page 24: Einstein Telescope: seismic and GGN studiesgw.icrr.u-tokyo.ac.jp/gwadw2010/program/2010_GWADW_Beker.pdf · Mark Beker, Nikhef Amsterdam on behalf of the ET design study team GWADW](https://reader036.fdocuments.net/reader036/viewer/2022081405/5f0b35cf7e708231d42f63e8/html5/thumbnails/24.jpg)
SuSa Mo
9
Seismic noise at 1 - 20 Hz is dominated by anthropogenic activity
Earthquake, Solomon Islands, Magnitude 6.8 Mining blast
Spectrogram Slanic salt mine Romania
Tuesday, May 18, 2010
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Given that underground seismicity is achievable, what about the contribution of surface waves to GGN?
10
ET-B
ET-C
[G. Cella et. al. Class.Quan.Grav 2010]
Frequency [Hz]
Strain / √H
z
Tuesday, May 18, 2010
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Given that underground seismicity is achievable, what about the contribution of surface waves to GGN?
• G. Cella (ET workshop 2009)• Propagating surface wave modes only (distant sources)
• Significant reductions with depth
• Smaller wavelength = higher reductions
10
ET-B
ET-C
[G. Cella et. al. Class.Quan.Grav 2010]
Frequency [Hz]
Strain / √H
z
Tuesday, May 18, 2010
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Given that underground seismicity is achievable, what about the contribution of surface waves to GGN?
• G. Cella (ET workshop 2009)• Propagating surface wave modes only (distant sources)
• Significant reductions with depth
• Smaller wavelength = higher reductions
10
Surface
ET-B
ET-C
[G. Cella et. al. Class.Quan.Grav 2010]
Frequency [Hz]
Strain / √H
z
Tuesday, May 18, 2010
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Given that underground seismicity is achievable, what about the contribution of surface waves to GGN?
• G. Cella (ET workshop 2009)• Propagating surface wave modes only (distant sources)
• Significant reductions with depth
• Smaller wavelength = higher reductions
10
Surface-10 m
ET-B
ET-C
[G. Cella et. al. Class.Quan.Grav 2010]
Frequency [Hz]
Strain / √H
z
Tuesday, May 18, 2010
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Given that underground seismicity is achievable, what about the contribution of surface waves to GGN?
• G. Cella (ET workshop 2009)• Propagating surface wave modes only (distant sources)
• Significant reductions with depth
• Smaller wavelength = higher reductions
10
Surface-10 m-50 m
ET-B
ET-C
[G. Cella et. al. Class.Quan.Grav 2010]
Frequency [Hz]
Strain / √H
z
Tuesday, May 18, 2010
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Given that underground seismicity is achievable, what about the contribution of surface waves to GGN?
• G. Cella (ET workshop 2009)• Propagating surface wave modes only (distant sources)
• Significant reductions with depth
• Smaller wavelength = higher reductions
10
Surface-10 m-50 m-100 m
ET-B
ET-C
[G. Cella et. al. Class.Quan.Grav 2010]
Frequency [Hz]
Strain / √H
z
Tuesday, May 18, 2010
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Given that underground seismicity is achievable, what about the contribution of surface waves to GGN?
• G. Cella (ET workshop 2009)• Propagating surface wave modes only (distant sources)
• Significant reductions with depth
• Smaller wavelength = higher reductions
10
Surface-10 m-50 m-100 m-150 m
ET-B
ET-C
[G. Cella et. al. Class.Quan.Grav 2010]
Frequency [Hz]
Strain / √H
z
Tuesday, May 18, 2010
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Given that underground seismicity is achievable, what about the contribution of surface waves to GGN?
• G. Cella (ET workshop 2009)• Propagating surface wave modes only (distant sources)
• Significant reductions with depth
• Smaller wavelength = higher reductions
• Still left with self-generated local noise sources
• Local impulse excitations don’t profit from a reduction in depth
• Prediction and subtraction methods
10
Surface-10 m-50 m-100 m-150 m
ET-B
ET-C
[G. Cella et. al. Class.Quan.Grav 2010]
Frequency [Hz]
Strain / √H
z
Tuesday, May 18, 2010
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Finite element models can be used to get a better understanding of local source effects
• FE models have been shown to accurately reproduce seismic surface and body waves from an excitation
• Investigate surface / body wave effects• FE models can be developed to include inhomogeneities and complex geologies
• Used to test GGN subtraction algorithms
11Tuesday, May 18, 2010
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GGN simulations done on homogeneous media show strong contributions from local sources
12
5e-14
1e-13
1.5e-13
2e-13
2.5e-13
3e-13
3.5e-13
4e-13
0 0.5 1 1.5 2
Max
imum
acc
eler
atio
n [m
/s2 ]
Depth, z/cP
1e-17
1e-16
1e-15
1e-14
1e-13
1e-12
0.1 1 10
Ampl
itude
Spe
ctru
m [m
/s2 ]
Frequency [Hz]
z/cP = 0z/cP = 0.5
z/cP = 1z/cP = 1.5
-1e-13
-5e-14
0
5e-14
1e-13
0 1 2 3 4 5 6
Time [s]
z/cP=1.5
TotalSurface
Bulk
-1e-13
-5e-14
0
5e-14
1e-13
1.5e-13
2e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
Time [s]
z/cP=1 m
-4e-13
-3e-13
-2e-13
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
z/cP=0.5 m
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
QS2Clay3 z/cP=0 m
5e-14
1e-13
1.5e-13
2e-13
2.5e-13
3e-13
3.5e-13
4e-13
0 0.5 1 1.5 2
Max
imum
acc
eler
atio
n [m
/s2 ]
Depth, z/cP
1e-17
1e-16
1e-15
1e-14
1e-13
1e-12
0.1 1 10
Ampl
itude
Spe
ctru
m [m
/s2 ]
Frequency [Hz]
z/cP = 0z/cP = 0.5
z/cP = 1z/cP = 1.5
-1e-13
-5e-14
0
5e-14
1e-13
0 1 2 3 4 5 6
Time [s]
z/cP=1.5
TotalSurface
Bulk
-1e-13
-5e-14
0
5e-14
1e-13
1.5e-13
2e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
Time [s]
z/cP=1 m
-4e-13
-3e-13
-2e-13
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
z/cP=0.5 m
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
QS2Clay3 z/cP=0 m
z = 0 m
z = 800 m = λP
Tuesday, May 18, 2010
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GGN simulations done on homogeneous media show strong contributions from local sources
12
Rayleigh wave arrives at surface detector
S-wave arrives at sub-ter. detector
5e-14
1e-13
1.5e-13
2e-13
2.5e-13
3e-13
3.5e-13
4e-13
0 0.5 1 1.5 2
Max
imum
acc
eler
atio
n [m
/s2 ]
Depth, z/cP
1e-17
1e-16
1e-15
1e-14
1e-13
1e-12
0.1 1 10
Ampl
itude
Spe
ctru
m [m
/s2 ]
Frequency [Hz]
z/cP = 0z/cP = 0.5
z/cP = 1z/cP = 1.5
-1e-13
-5e-14
0
5e-14
1e-13
0 1 2 3 4 5 6
Time [s]
z/cP=1.5
TotalSurface
Bulk
-1e-13
-5e-14
0
5e-14
1e-13
1.5e-13
2e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
Time [s]
z/cP=1 m
-4e-13
-3e-13
-2e-13
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
z/cP=0.5 m
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
QS2Clay3 z/cP=0 m
5e-14
1e-13
1.5e-13
2e-13
2.5e-13
3e-13
3.5e-13
4e-13
0 0.5 1 1.5 2
Max
imum
acc
eler
atio
n [m
/s2 ]
Depth, z/cP
1e-17
1e-16
1e-15
1e-14
1e-13
1e-12
0.1 1 10
Ampl
itude
Spe
ctru
m [m
/s2 ]
Frequency [Hz]
z/cP = 0z/cP = 0.5
z/cP = 1z/cP = 1.5
-1e-13
-5e-14
0
5e-14
1e-13
0 1 2 3 4 5 6
Time [s]
z/cP=1.5
TotalSurface
Bulk
-1e-13
-5e-14
0
5e-14
1e-13
1.5e-13
2e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
Time [s]
z/cP=1 m
-4e-13
-3e-13
-2e-13
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
z/cP=0.5 m
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
QS2Clay3 z/cP=0 m
z = 0 m
z = 800 m = λP
Tuesday, May 18, 2010
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GGN simulations done on homogeneous media show strong contributions from local sources
12
Rayleigh wave arrives at surface detector
S-wave arrives at sub-ter. detector
5e-14
1e-13
1.5e-13
2e-13
2.5e-13
3e-13
3.5e-13
4e-13
0 0.5 1 1.5 2
Max
imum
acc
eler
atio
n [m
/s2 ]
Depth, z/cP
1e-17
1e-16
1e-15
1e-14
1e-13
1e-12
0.1 1 10
Ampl
itude
Spe
ctru
m [m
/s2 ]
Frequency [Hz]
z/cP = 0z/cP = 0.5
z/cP = 1z/cP = 1.5
-1e-13
-5e-14
0
5e-14
1e-13
0 1 2 3 4 5 6
Time [s]
z/cP=1.5
TotalSurface
Bulk
-1e-13
-5e-14
0
5e-14
1e-13
1.5e-13
2e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
Time [s]
z/cP=1 m
-4e-13
-3e-13
-2e-13
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
z/cP=0.5 m
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
QS2Clay3 z/cP=0 m
5e-14
1e-13
1.5e-13
2e-13
2.5e-13
3e-13
3.5e-13
4e-13
0 0.5 1 1.5 2
Max
imum
acc
eler
atio
n [m
/s2 ]
Depth, z/cP
1e-17
1e-16
1e-15
1e-14
1e-13
1e-12
0.1 1 10
Ampl
itude
Spe
ctru
m [m
/s2 ]
Frequency [Hz]
z/cP = 0z/cP = 0.5
z/cP = 1z/cP = 1.5
-1e-13
-5e-14
0
5e-14
1e-13
0 1 2 3 4 5 6
Time [s]
z/cP=1.5
TotalSurface
Bulk
-1e-13
-5e-14
0
5e-14
1e-13
1.5e-13
2e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
Time [s]
z/cP=1 m
-4e-13
-3e-13
-2e-13
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
z/cP=0.5 m
-1e-13
0
1e-13
2e-13
3e-13
4e-13
0 1 2 3 4 5 6
Acce
lera
tion
[m/s
2 ]
QS2Clay3 z/cP=0 m
z = 0 m
z = 800 m = λP
Tuesday, May 18, 2010
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13
Clay:λP = 800 mλS = 462 mρ = 2000 kg/m3ν = 0.25
Limestone:λP = 2200 mλS = 1270 mρ = 2500 kg/m3ν = 0.25
Harmonic excitations only benefit from small reduction factors
Tuesday, May 18, 2010
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13
Clay:λP = 800 mλS = 462 mρ = 2000 kg/m3ν = 0.25
Limestone:λP = 2200 mλS = 1270 mρ = 2500 kg/m3ν = 0.25
Harmonic excitations only benefit from small reduction factors
Tuesday, May 18, 2010
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13
Clay:λP = 800 mλS = 462 mρ = 2000 kg/m3ν = 0.25
Limestone:λP = 2200 mλS = 1270 mρ = 2500 kg/m3ν = 0.25
0.1
1
100 1000
Redu
ction
facto
r
Depth [m]
Clay 1Hz FEA/FitClay 4Hz FEA/Fit
Granite 1Hz FEA/FitGranite 4Hz FEA/Fit
GGN re
duction factor
Depth [m]
GGNmax(z)/GGNmax(0)GGN at depth / GGN at surface
λP=800 m λP=2200 m
Harmonic excitations only benefit from small reduction factors
100 1000
1
0.1
LimestoneClay
Tuesday, May 18, 2010
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Adaptive filter algorithms can be used to predict and subtract GGN
• Use secondary sensors to measure the density perturbations around the detector.
• Create models that estimatethe sensor to test mass impulse responses.
• Use adaptive filter techniques to estimate and reduce GGN
14
NewtonianNoise TFhnn
x(n) d(n) e(n)
e(n) = d(n) -
!+
-
Update algorithm
Digital filtersystemw
d(n)^
d(n)^"w
Seismic signalNewtonian
noise
Estimated Newtonian
noise
GW signal
Tuesday, May 18, 2010
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GGN due to harmonic local source is used to test filter effectiveness
15
0
0
1 2 3 4 5 6Time [s]
Finite Element Analysis GGN - Harmonic excitation
GGNxExcitation
Loca
l acc
elerat
ion am
plitud
e [Ar
b. Un
its]
Tuesday, May 18, 2010
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GGN due to harmonic local source is used to test filter effectiveness
15
0
0
1 2 3 4 5 6Time [s]
Finite Element Analysis GGN - Harmonic excitation
GGNxExcitation
Loca
l acc
elerat
ion am
plitud
e [Ar
b. Un
its]
Tuesday, May 18, 2010
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Results of simple filtering algorithm show a reduction of 1.5 orders of magnitude
16
Time domain performance of the Wiener filter
GGN !xfiltered estimateSubracted channel
Loca
l acc
elerat
ion am
plitud
e [Ar
b. Un
its]
0 1 2 3 4 5 6Time [s]
Tuesday, May 18, 2010
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Future work
• Seismic measurements
• Finish preliminary characterization of sites in Europe
• Data analysis
• FE GGN models
• Multiple uncorrelated sources
• Various geologies
• Cavity size and shape
• GGN filtering
• Optimizing filter coefficients
• Determine requirements for seismic array (seismometer density and positions)
17Tuesday, May 18, 2010
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Conclusions
• The ET-B seismic noise requirement can be obtained at various locations in Europe.
• ET-C requirement will be more challenging
• Surface wave effects reduce with depth• Local excitations will still be a source of GGN• Finite element models used to better understand these effects
• Can be reduced using adaptive filtering techniques
• Care must be taken when considering placement of infrastructure (advice committee)
18Tuesday, May 18, 2010
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19Tuesday, May 18, 2010
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20Tuesday, May 18, 2010