Status of Virgo : Past, Present, Future
... Established in 2004, the VIRGO EGO Scientific Forum is composed of 47 research groups active in the European scientific community. A total of 18 fellowships with a two-year duration have been funded in Italy (7), Spain (3), France (2), Germany (2), Greece (1), Hungary (1), Poland (1) and UK (1). ...
... Established in 2004, the VIRGO EGO Scientific Forum is composed of 47 research groups active in the European scientific community. A total of 18 fellowships with a two-year duration have been funded in Italy (7), Spain (3), France (2), Germany (2), Greece (1), Hungary (1), Poland (1) and UK (1). ...
G050017-00
... The OMC of VIRGO is a small triangular monolithic cavity; The cavity is mounted in vacuum on a suspended bench; The bench is locally aligned The OMC is locked with thermal actuators; The OMC has worked satisfactory in the CITF and in VIRGO; The recycled VIRGO has been locked using the OMC transmissi ...
... The OMC of VIRGO is a small triangular monolithic cavity; The cavity is mounted in vacuum on a suspended bench; The bench is locally aligned The OMC is locked with thermal actuators; The OMC has worked satisfactory in the CITF and in VIRGO; The recycled VIRGO has been locked using the OMC transmissi ...
T1000311-v7 TMS Hazards Analysis - DCC
... Each team member should inspect to hid/her satisfaction the prospective part to be handled to determine if that part has a potentially hazardous sharp edge. Hands may also be pinched when assembling parts to one another, but this can be mitigated with proper attention to handling the parts. During t ...
... Each team member should inspect to hid/her satisfaction the prospective part to be handled to determine if that part has a potentially hazardous sharp edge. Hands may also be pinched when assembling parts to one another, but this can be mitigated with proper attention to handling the parts. During t ...
word version with changes tracked - DCC
... The petition process should be initiated before the paper is written, when possible, by contacting the P&P committee with an outline of the paper, a description of the data used and the results drawn. In some cases, the details of the writing may be needed for a final judgment. As a general guidelin ...
... The petition process should be initiated before the paper is written, when possible, by contacting the P&P committee with an outline of the paper, a description of the data used and the results drawn. In some cases, the details of the writing may be needed for a final judgment. As a general guidelin ...
Real-time earthquake warning for astronomical observatories
... suggest that earthquakes closer than 100 km are required to do the most damage, and we show why this is likely to be the case in section III. The Laser Interferometer Gravitational-wave Observatory (LIGO) [16], Virgo [17], and GEO600 [18] detectors are part of a network of gravitational-wave interf ...
... suggest that earthquakes closer than 100 km are required to do the most damage, and we show why this is likely to be the case in section III. The Laser Interferometer Gravitational-wave Observatory (LIGO) [16], Virgo [17], and GEO600 [18] detectors are part of a network of gravitational-wave interf ...
Resonantly-Enhanced Photon Regeneration
... • Resonant approach improves sensitivity to gaγγ by a factor of 300 or so. • It can reach 2 x 10-11 GeV-1 in 90 days of live time. • All the technology for such an experiment exists. – TeV magnets. – Laser, cavity, instrument control, and readout adopt technology proven in LIGO and LISA. ...
... • Resonant approach improves sensitivity to gaγγ by a factor of 300 or so. • It can reach 2 x 10-11 GeV-1 in 90 days of live time. • All the technology for such an experiment exists. – TeV magnets. – Laser, cavity, instrument control, and readout adopt technology proven in LIGO and LISA. ...
initial LIGO construction
... The scientific program for LIGO is both to test relativistic gravitation and to open the field of gravitational wave astrophysics. More precise tests of General Relativity (and competing theories) will be made. LIGO will enable the establishment of a brand new field of astronomy, using a completely ...
... The scientific program for LIGO is both to test relativistic gravitation and to open the field of gravitational wave astrophysics. More precise tests of General Relativity (and competing theories) will be made. LIGO will enable the establishment of a brand new field of astronomy, using a completely ...
slides ppt
... In the next weeks: reach LIGO sensitivity at high frequency Start collecting “Science” data this fall Soft transition towards long data taking periods for GW searches ...
... In the next weeks: reach LIGO sensitivity at high frequency Start collecting “Science” data this fall Soft transition towards long data taking periods for GW searches ...
3 Gravitational Waves from Binaries
... a single interferometer, by itself, from detecting with confidence shortduration gravitational-wave bursts (though it might be possible for a single interferometer to search for the periodic waves from known pulsars). The non-Gaussian noise can be removed by cross correlating two, or preferably thre ...
... a single interferometer, by itself, from detecting with confidence shortduration gravitational-wave bursts (though it might be possible for a single interferometer to search for the periodic waves from known pulsars). The non-Gaussian noise can be removed by cross correlating two, or preferably thre ...
T1000700-v2 Transmon Telescope Mirror Test Procedure
... Fax (626) 304-9834 E-mail: [email protected] ...
... Fax (626) 304-9834 E-mail: [email protected] ...
G060098-01 - DCC
... Need to monitor the input beam position/orientation into the PRM, e.g. partially transmitting optics and cameras IO wants 3 beams (one is REFL) from Faraday Isolator -- tells about polarization state of beam into & back from RM IO beams: 2 MC, 1 Input, could bring laser intensity stabilization ...
... Need to monitor the input beam position/orientation into the PRM, e.g. partially transmitting optics and cameras IO wants 3 beams (one is REFL) from Faraday Isolator -- tells about polarization state of beam into & back from RM IO beams: 2 MC, 1 Input, could bring laser intensity stabilization ...
T060269-01 - DCC - LIGO Document Control Center Portal
... Figure 5.2 Incremental transmitted power as a function of motor drive count to be used to send a control signal to the rotational motorized stage controller. Note that the x-axis is units of 104 counts. _______________________________________________________________________ 36 Figure 5.3 Power in W ...
... Figure 5.2 Incremental transmitted power as a function of motor drive count to be used to send a control signal to the rotational motorized stage controller. Note that the x-axis is units of 104 counts. _______________________________________________________________________ 36 Figure 5.3 Power in W ...
J.Marque: Mode matching of the Virgo FP cavities
... telescope in order to match the mode parameters of the input beam (waist size, distance to waist) to the cavity eigenmodes (radius of curvature of the mirrors of the cavity, length of the cavity). o This action can be performed by adjusting the position of the various optical elements of the telesco ...
... telescope in order to match the mode parameters of the input beam (waist size, distance to waist) to the cavity eigenmodes (radius of curvature of the mirrors of the cavity, length of the cavity). o This action can be performed by adjusting the position of the various optical elements of the telesco ...
T1000179-v18_aLIGO_HWS_optical_layouts - DCC
... The HWS will have a band-pass filter, (790nm 10nm) or (840nm 10nm) mounted directly in front of it. This will be used filter out ambient light and any residual 1064nm radiation. This will need to be tilted vertically by ~ 10 mrad to prevent any 1064nm reflections back into the signalrecycling ca ...
... The HWS will have a band-pass filter, (790nm 10nm) or (840nm 10nm) mounted directly in front of it. This will be used filter out ambient light and any residual 1064nm radiation. This will need to be tilted vertically by ~ 10 mrad to prevent any 1064nm reflections back into the signalrecycling ca ...
Document
... identify and subtract the signal in its detection band from every merging neutron star and black hole binary in the universe. It will also extend LISA’s scientific program of measuring wavesfrom the merging of intermediate-mass black holes at any redshift, and will refine the mapping of space-time a ...
... identify and subtract the signal in its detection band from every merging neutron star and black hole binary in the universe. It will also extend LISA’s scientific program of measuring wavesfrom the merging of intermediate-mass black holes at any redshift, and will refine the mapping of space-time a ...
LIGO-T0900407-v4 - DCC - LIGO Document Control Center Portal
... There are a number of sources that can change the ROC of the input beam: 1. IMC Substrate thermal lensing in IMC3 2. PMMT1 ROC tolerance or positioning error 3. FI thermal compensation 4. PMMT2 ROC tolerance or positioning error Out of these, we showed that the ROC tolerances or positioning errors i ...
... There are a number of sources that can change the ROC of the input beam: 1. IMC Substrate thermal lensing in IMC3 2. PMMT1 ROC tolerance or positioning error 3. FI thermal compensation 4. PMMT2 ROC tolerance or positioning error Out of these, we showed that the ROC tolerances or positioning errors i ...
M060056-07 - LIGO dcc - LIGO Scientific Collaboration
... The basic optical configuration is a power-recycled and signal-recycled Michelson interferometer with Fabry-Perot “transducers” in the arms; see Figure 2.. Using the initial LIGO design as a point of departure, Advanced LIGO requires the addition of a signal-recycling mirror at the output “dark” por ...
... The basic optical configuration is a power-recycled and signal-recycled Michelson interferometer with Fabry-Perot “transducers” in the arms; see Figure 2.. Using the initial LIGO design as a point of departure, Advanced LIGO requires the addition of a signal-recycling mirror at the output “dark” por ...
M060056-08 - DCC - LIGO Document Control Center Portal
... LIGO M060056-08-M 2. Sensitivity and Reference Design Configuration The Advanced LIGO interferometer design allows tuning and optimization of the sensitivity both to best search for specific astrophysical gravitational-wave signatures and to accommodate instrumental limitations. To define the goal ...
... LIGO M060056-08-M 2. Sensitivity and Reference Design Configuration The Advanced LIGO interferometer design allows tuning and optimization of the sensitivity both to best search for specific astrophysical gravitational-wave signatures and to accommodate instrumental limitations. To define the goal ...
Stable Operation of a 300-m Laser Interferometer with Sufficient
... has the ability to detect GW events within our galaxy, though such events are expected to be very rare. In order to increase the detection probability for GW events farther away from our galaxy, we are improving the detector sensitivity and stability further. Almost all of the noise sources which li ...
... has the ability to detect GW events within our galaxy, though such events are expected to be very rare. In order to increase the detection probability for GW events farther away from our galaxy, we are improving the detector sensitivity and stability further. Almost all of the noise sources which li ...
No Slide Title
... Much better event reconstruction » Source location in the sky » Reconstruction of polarization components » Reconstruction of amplitude at source and determination of source distance (BNS) ...
... Much better event reconstruction » Source location in the sky » Reconstruction of polarization components » Reconstruction of amplitude at source and determination of source distance (BNS) ...
ET: Einstein Telescope
... • The target of the four Working Groups in the ET project is to try to transform these (and many other) ideas in a coherent conceptual design • It is an huge job for a restricted set of persons • ET is an emerging facility for the whole Europe and we don’t want to limit the contribution to the found ...
... • The target of the four Working Groups in the ET project is to try to transform these (and many other) ideas in a coherent conceptual design • It is an huge job for a restricted set of persons • ET is an emerging facility for the whole Europe and we don’t want to limit the contribution to the found ...
Thermal_Compensator_System_CDD_01 - LIGO
... The positions of the thermal compensators and optical sensors are indicated schematically in Figure 1. The phase cameras monitoring pickoff ports of the main interferometer beam are not shown. The main thermal compensation of homogeneous absorption in the optics will use carbon dioxide laser project ...
... The positions of the thermal compensators and optical sensors are indicated schematically in Figure 1. The phase cameras monitoring pickoff ports of the main interferometer beam are not shown. The main thermal compensation of homogeneous absorption in the optics will use carbon dioxide laser project ...
SEI Structure Development - LIGO
... look at the cost book detail, the individual cost items have the same contingency value, even though we listed whether the estimate is a vendor quote or an engineering estimate. This is because the risk factors were evaluated at the activity level, not at the individual cost item. ...
... look at the cost book detail, the individual cost items have the same contingency value, even though we listed whether the estimate is a vendor quote or an engineering estimate. This is because the risk factors were evaluated at the activity level, not at the individual cost item. ...
G030086-00 - DCC
... What do I gather from globular cluster and galaxy observations • The only electromagnetically visible BH are those accreting from companion star • Why so many are visible? • Frequent Encounters of binaries with singles tie and tighten up the bigger guy and fling out the smaller guy (s.m. size ones) ...
... What do I gather from globular cluster and galaxy observations • The only electromagnetically visible BH are those accreting from companion star • Why so many are visible? • Frequent Encounters of binaries with singles tie and tighten up the bigger guy and fling out the smaller guy (s.m. size ones) ...
LIGO
LIGO, which stands for the Laser Interferometer Gravitational-Wave Observatory, is a large-scale physics experiment aiming to directly detect gravitational waves. Cofounded in 1992 by Kip Thorne and Ronald Drever of Caltech and Rainer Weiss of MIT, LIGO is a joint project between scientists at MIT, Caltech, and many other colleges and universities. It is sponsored by the National Science Foundation (NSF). At the cost of $620 million, it is the largest and most ambitious project ever funded by the NSF.Observations at LIGO began in 2002, ended in 2010, and no gravitational waves have been reported. The original detectors were disassembled and were replaced by improved versions known as ""Advanced LIGO"". As of February 2015, two such advanced detectors (one in Livingston, Louisiana and the other in Hanford, Washington) have been brought into engineering mode. On September 18, 2015, Advanced LIGO became fully operational and began formal science operations at twice the sensitivity of the initial LIGO interferometers.