Review - LIGOajw/40m/40m_000516.pdf · Review of 40m upgrade go als The primary goal of the 40 m...
Transcript of Review - LIGOajw/40m/40m_000516.pdf · Review of 40m upgrade go als The primary goal of the 40 m...
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40m Upgrade Plans
� Review of 40m upgrade goals
� 40m infrastructure upgrade
� RSE con�guration - design considerations
� IFO optical con�guration
� RSE control scheme
� people, money, schedule
� problems and questions
http://www.ligo.caltech.edu/�ajw/40m 000516.pdf
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Review of 40m upgrade goals
� The primary goal of the 40 m upgrade
is to demonstrate a scheme for using
resonant sideband extraction (RSE),
in either broadband or tuned con�g,
appropriate for an optimal LIGO con�g
� RSE and DR have been demonstrated at
Garching 30m, and at table-top IFOs
� An RSE/DR con�g appropriate for LIGO
will be demonstrated at the Glasgow 10m
� For LIGO, need a full engineering prototype,
using LIGO electronics and control scheme.
This is the primary goal of the 40 m upgrade.
� Complements work at other R&D facilities:
{ 40m will focus on shot (phase, sensing) noise, high-f
{ LASTI: full-scale SEI,SUS prototyping; low-f
{ TNI: thermal noise; middle-f
{ ETF: Sagnac, high powered lasers
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Secondary 40m upgrade goals
Prototype \everything"?
� potentially, multiple pendula SUS
| this may be necessary, to extrapolate experience
gained at 40m to LIGO-II
� potentially, advanced SEI systems
| scaled down, of course. Cannot replace full-scale
testing at LASTI.
� potentially, thermal noise measurements
with maximized beam width (� at mirrors)
| a big, and challenging, diversion.
� LIGO-III: cryogenic TMs, QND, etc..
� physicist training
At the least, must prototype everything that has
large impact on electronics/control system,
for a meaningful full engineering test!
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40m infrastructure upgrade
� LIGO-like upgrade, during next 1-2 years:
{ building modi�cations, control room, electrical;
work to be completed by fall (???)
{ Active seismic isolators on TM stacks?
{ EPICS-based vacuum control system
(to be completed by summer)
{ LIGO-I PSL from Peter King (fall?)
{ 12 meter mode cleaner and MMT
(vacuum envelope, stack, exists)
{ 4" optics for IR running
{ 7th suspended optic (SM)
{ scaled (for 4" optics) suspensions
{ Output chamber for signal mirror
(chamber exists, seismic stack to be built)
{ full CDS control system: ISC, LSC, ASC, GDS
{ control scheme for all optics
{ strawman: frontal mod with M-Z IFO
� Ready to prototype an RSE scheme by 2002.
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Seismic noise
We have measured the seismic noise (V,H; day, night) at
the 40m lab:
100
101
102
10−16
10−14
10−12
10−10
10−8
10−6
10−4
Frequency (Hz)
Dis
plac
emen
t noi
se, m
/ rt
Hz
40m displacement noise
Starting GPS time:Wed Apr 12 02:17:43 2000 (and 0 usec)
Hanford IFO−Seis Floor−X Floor−Y Floor−Z Microphone
100
101
102
10−12
10−11
10−10
10−9
10−8
10−7
10−6
zrmsnite = 0.13 µm
zrmsday = 0.23 µm
nightday
100
101
102
10−10
10−9
10−8
10−7
10−6
10−5
vrmsnite = 1.64 µm/s
vrmsday = 3.13 µm/s
nightday
100
101
102
10−8
10−7
10−6
10−5
10−4
10−3
armsnite = 1929 µm/s2
armsday = 1809.59 µm/s2
nightday
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Stack transfer function
V,H transfer functions of the existing TM stacks:
100
101
102
10−4
10−3
10−2
10−1
100
101
102
Frequency (Hz)
Hor
izon
tal T
rans
fer
func
tion
40m displacement noise 12−Apr−2000 03:17:30 PDT −−− Horizontal
Seismic+Geo Shaker+AccelShaker+Geo Model
100
101
102
10−4
10−3
10−2
10−1
100
101
102
Frequency (Hz)
Ver
tical
Tra
nsfe
r fu
nctio
n
40m displacement noise 12−Apr−2000 03:17:30 PDT −−− Vertical
Seismic+Geo Shaker+AccelShaker+Geo Model
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Active seismic isolation?
STACIS isolator pedestals (roughly $120K)
For robust IFO lock, need mirror horizontal vrms � �=s
�lock ��=2
vthrP (v < vthr); vthr ' 1�=s
100
101
102
10−16
10−14
10−12
10−10
10−8
10−6
10−4
vrmsfloor = 1.64 µm/s
vrmsmirr = 0.43 µm/s
vrmsSTACIS = 0.27 µm/s
Frequency (Hz)
velo
city
noi
se p
ower
spe
ctru
m, µ
m/s
/ rt
Hz
40m displacement noise 12−Apr−2000 03:17:30 PDT
vrms
, floor v
rms, mirror
vrms
, STACIS
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Resonant Sideband Extraction(RSE) Config
South
East Arm
ArmL1
l 3
l 2l 1
PSL
RM
L2
RF 12m MC
APD PPDSPD
BS
SM
A power-recycled Michelson IFO with Fabry-Perot arms,
with a signal recycling mirror (SM) for resonant sideband
extraction (RSE).
� LSC/AIC group is evaluating di�erent control schemes.
� Key parameters depend on what is chosen:
{ TITM , TSM , LSRC , LPRC
{ Method for applying sidebands to beam
� Hope to have a workable scheme by fall
� May have to fold SRC!!
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Will it fit?
150
cm
Output chamber
Beam splitter
25 cm
Recycling mirror
Signal mirror
For broadband operation (�cs = 0, worst case),
need � 178 cm. Have only � 150 cm!
May be limited in available tune,
or may have to fold the SRC optical path.
More careful optimizations and drawings are in the works
(Mike Smith).
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Fundamental noise at 40m
101
102
103
104
10−22
10−21
10−20
10−19
10−18
10−17
10−16
40m strain sensitivity
stra
in s
ensi
tivity
(1/
rtH
z)
Frequency (Hz)
TITM
TPRM
TSRM
Gprc
Garm
fpol
0.030 0.000 0.176 10 131 9516
Seismic
FSilica Thermal
Suspension
RSE, tuned
Radiation pressure
40m RSE total
� Thermoelastic, photothermal noise are negligible
� Suspension noise may be trouble with 3" optics
� Q (F-Si) = 2� 106. Dominates from 100{3KHz!
� May need to turn laser power down
to expose shot noise over thermal;
� Alternatively, live with thermal noise;
don't bother to expose shot noise;
focus on controls problem
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People
� Currently: Two physicists (Weinstein, Ugolini),
one master tech (Vass)
� MUST make heavy use of LIGO engineers:
{ building modi�cations: Fred Asiri
{ Output chamber stack: Fred Asiri
{ active isolators?: Larry Jones
{ PSL-I: Peter King, Rich Abbott
{ optics: Garilynn Billingsley
{ single ! multiple pendula: Janeen Romie
{ optical layout, ba�ing: Mike Smith
{ CDS (ISC, LSC, ASC): Jay Heefner, Rolf Bork,
new hire
� Expect to hire another controls engineer/postdoc
� MUST involve more postdocs, grad students,
undergrads
� MUST involve LSC personnel
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Summer REU's
� Lisa Goggin, University College, Cork:
12 meter mode cleaner
� Jitesh Chauhan, Leicester U:
Global Diagnostics System
� Brian Kappus, Harvey Mudd:
Wavefront sensing
� Ted Jou, Caltech:
RSE modelling; Twiddle/Finesse ! E2E
� Ivica Stevanovic, Belgrade U:
multiple pendulum modelling
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Schedule, Milestone Fantasy
� 3q2000
{ lab building repairs and mods
{ LIGO IR PSL
{ Construction of new Output chamber, stack
{ Bakeout? Active isolators?
� 4q2000
{ Review of optical design consistent with RSE/DR
{ Development of control system
� 2q2001
{ LIGO-like suspensions, controllers, optics in place
{ LIGO-like CDS: ISC, LSC, ASC, WFS systems
{ LIGO-like diagnostics, DAQS software
{ Review of SM control scheme
(broad-band and detuned)
� 2002
{ Prototype installation complete.
{ Initial shakedown complete.
{ Ready to prototype an RSE scheme.
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Problems and questions
� Do we need to bake out the vacuum envelope?
� Should we rebuild the seismic stacks,
replacing sti�-but-well-damped viton
(contaminating the vacuum at a low level?)
with soft but-poorly-damped metal springs?
� Should we consider employing
advanced (scaled down) SEI systems?
� should we consider prototyping advanced SUS systems
(multiple pendula, electrostatic control)?
� Is the \simple" control scheme developed by Mason
adequate for LIGO-II?
� How can we implement it? M-Z? fRF2 = 100 MHz?
� Modulation in vacuum or air? Before/after MC?
� where will we get the physicists and eng. support?
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