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Setting the stage
GWADW2010, Kyoto
Francesco Fidecaro
Pisa
GWADW2010 - Kyoto
Recent progress in gravitational
wave research
• With input from
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Rana Adhikari
Matt Evans
Hartmut Grote
Kazuaki Kuroda
David Shoemaker
Didier Verkindt
Stefano Vitale
Work of many
Data taking by current detectors (S6/VSR2) and analysis of large datasets
Network of interferometers in coincidence <-> em and n observatories
Theoretical study of sources
A new promising entry: Pulsar timing (not covered this time)
Ongoing projects for Advanced Detectors and space
Cryogeny, thermal noise, mechanical noise, underground-> third generation
Endless spiral: Research, development, construction, tests, measurements,
models, simulation
GWADW2010 - Kyoto
Analysis of 6 months of coincidence
data between LHO, LLO and Virgo
• Data quality: the noise curve is the beginning of the story, not the end!
Virgo Omega
triggers in 107
seconds
1 s coincidence -> 10 ev
GWADW2010
- Kyoto Triples?
O(104) SNR>8
triggers
-> 0.01 ev
10 nrad rms
https://pub3.ego-gw.it/itf/tds/file.php?callFile=VIR-0123A-10.pdf
GWADW2010 - Kyoto
GWADW2010 - Kyoto
Signalled by
Jay Marx
GWADW2010 - Kyoto
Direct and indirect origins for
strong contributions to noise
• In random order:
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Large beams
High intensity
Thermal effects
Position, angular noise (rms)
Optical design
Poor or missing error signals
Beam halo, stray, diffused light
Creep and the like
• End up in different approaches (all will be working, with trade offs)
• It is a little bit like having to choose between…
GWADW2010 - Kyoto
GWADW2010 - Kyoto
GWADW2010 - Kyoto
ALIA
ASTROD-GW
DECIGO
Current launch date 2012 Q1
GWADW2010 - Kyoto
Light and heat
• Compensation of thermal distortions: significant
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complication introduced (TCS, managing higher
modes)
Can we go around high light intensity?
• Warm mirrors and suspensions have thermal noise
– The direct way: cool them (CLIO, LCGT, …)
– Or reduce internal dissipation
– Or both
• In any case, need to address material properties
• New ideas?
GWADW2010 - Kyoto
Alignment
• Longitudinal noise is not the end of the
story
• Angular control comes in, becomes more
difficult with high power and broad beams
• Engineered-in since the beginning?
GWADW2010 - Kyoto
Simulation after first generation
• Now is a Must have
• Optical, frequency domain, time domain
• We know better how to ask questions
aiming at lock acquisition, noise coupling
• Need to introduce imperfections, which
ones?
• How to simulate non stationarity?
GWADW2010 - Kyoto
Entering the advanced detector era
• Long run
• Not only knowledge but also skills to be acquired and
maintained:
– Teaching the art
– Managing these bright minds
– Thinking
• Built-in reliability:
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hw and core sw at the same level
Cleanliness
QC
Prototype and test as much as possible
• Manage centrifugal forces:
– Missing real astrophysical data
– New detector instead of routine construction and debugging
GWADW2010 - Kyoto
Squeezed states of light
• “As a positive thing one might see that
squeezing may arrive earlier than anticipated in
the past” Hartmut Grote
• Be prepared...
GWADW2010 - Kyoto
Photo Courtesy H. Grote
GWADW2010 - Kyoto
A stimulating program
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Expertise is building, experience accumulates
Experiments are made
Codes are run
Third generation takes shape
Progress is made on all fronts, our detectors will
be better than ever
Thank you Syd and convenors for putting it
together, and our warmest wishes!
But there was a starter: Kamioka mountain
GWADW2010 - Kyoto
CLIO/KS tour: very interesting
LCGT is planned to be built
underground at Kamioka, where
the prototype CLIO detector is
placed.
Location of ＣＬＩＯ／LCGT
Effort headed by the Director of
ICRR Takaaki Kajita.
GWADW2010 - Kyoto