Transcript G000245-00 - DCC

CSUDH/ EPRG, The 40m IFO,
and Connections With  Physics
New LSC Group;
Cal. State U. Dominguez Hills
Elem. Part. & Relativity Group
LIGO-G000245-00-D
Members of CSUDH EPRG
Kenneth S. Ganezer Dept. of Physics (Super-K, IMB)
William E. Keig
Dept. of Physics (Super-K )
Samuel L. Wiley
Dept. of Physics
George A. Jennings Dept. of Mathematics
CSUDH EPRG and Med.Apps. Of Physics; Funding
NSF PHY 9208472. Solar Neutrinos at IMB; Past
NSF PHY 9514150. Solar Neutrinos and Nucleon Decay S-K; Current
NSF PHY 0071656. Neutrino Oscillations and Astronomy and Nucleon
Decay at S-K; 7/01- 7-04; Approved; Postdoc Needed.
NIH Current funding for Medical Imaging Design; 4/99-4/01
NIH S06 GM 08156-22; Pending (highly likely); New Med. Imaging
Tech using -rays and CZT; start 4/01- 4/05
California State University Dominguez Hills
8500 on-campus students.
3000 students in off-campus nursing program.
Wide Spectrum of Student groups; 58% females, average age of undergrads is 29 years.
Ethnicity is about 30% Caucasian American, 30% African American, 25% Hispanic American, and 15%.
Asian American.
8-14 Physics Majors (undergrads).
2.25 Bachelors Degrees per year.
No CSUDH Physics Grad Program; But we Supervise MS Students from Nearby CSU, Long Beach.
Caltech and CSUDH are on opposite ends o f Harbor (110) Freeway ; We are near the Southwest end of 110.
Background in Non-Newtonian Gravity
K. Ganezer, “ The Consistency of the Constraint and Field
Algebras in Minimal Supergravity Theory”, Nucl. Phys.
B, 176, 216-220, (1980).
G. Jennings, “Geometry for Teachers including Relativity”,
Springer Verlag, 1994.
Possible CSUDH/ EPRG LIGO Projects
• Simulations for Upgraded 40m IFO Including Imperfect Optics and
Resonant Sideband Extraction
• Help in Construction of Upgraded 40m IFO
• Connections between Neutrinos and Gravity Waves
• Gravity Waves and Supernovas; the LIGO-SNEWS connection
Simulations for Upgraded 40m
IFO
Simulations using FFT code (of Bochner and others)
And Possibly Other Programs (E2E)
40m Configuration with Imperfect Optics for
•1.Dual Recycling
•2. Imperfect Optics
•3. Wavefront Healing
•4. RSE; Broadband and Narrowband (tuned)
•Eventually simulate control and sensing
•And LIGO III Optical Systems
Work So Far With FFT And Near Term Plans
1. We have run the single recycling FFT mode to calculate
Six parameters as a function of RITM any one of which
Can be used to drive design. Our results of full FFT relaxation
Calculation are consistent with simple analytical calculations
2. We will do similar calculations for the dual recycling
Upgraded 40m configuration. Have fixed minor problems
With DR FFT code from repository
3. Fred Jenet has done most of work to set up SR FFT to
Run under MPI, industry standard parallel architecture.
We will modify DR FFT to run under MPI and make any
Modifications needed to run SR FFT under MPI.
4. Will take 4 versions of FFT; single workstation and MPI
SR and DR versions and set up as single code. Different
Executables will be compiled under different cpp options.
Results of 40m Single Recycling Simulations
Assumes perfect mirrors.
See notes following the table.
Perfect Optics
(In the table "power" = "gain" since laser power = 1.0 nominally in fft.x simulations)
R_Mft = Intensity reflectivity of interior FP mirrors Mft and Mft
T_Mft = Intensity transmittivity of interior FP mirrors
finesse = finesse
TauS = storage time
fpole = cavity pole freq.
ArmCarr00 = Carrier TEM00 power in inline FP cavity
AsymCarr00 = Carrier TEM00 power at antisymmetric beamsplitter port
AsymCarr = total carrier power at antisymmetric beamsplitter port
PrcSB00 = Sideband TEM00 power in power recycling cavity
AsymSB00 = Sideband TEM00 power at antisymmetric beamsplitter port
AsymSB = Total Sideband power at antisymmetric beamsplitter port
R_MRec = Optimum intensity reflectivity of power recycling mirror
1-C = contrast defect
Lasymm = Schnupp asymmetry
gamma = Optimum modulation depth? (see note 6)
h(f) = Strain sensitivity at DC? (see note 7)
Notes
1.
R_Mft is set independently for each simulation. Except for R_Mft = R_Mfr and the initial
reflectivity of Mrec all other reflectivities in the ligo.dat file are the same in all simulations:
Mbs = .49995, Mtback = Mrback = .999935. Base REF side losses are Mrec = Mft = Mfr =
Mtback = Mrback = 5.0e-5 and Mbs = 1.0e-4.
2.
T_Mft, PrcCarr00 - AsymCarr and R_MRec are taken from the fft.x output files
40m_perf_carr.out. PrcSB00 - AsymSB and Lasym are taken from the fft.x output files
40m_perf_sb.out.
3.
finesse = Pi*Sqrt[r1*r2]/(1-r1*r2) where r1 = Sqrt[R_Mft] and r2 = Sqrt[.999935] are
amplitude reflectivities of mirrors at ends of FP cavity (equation 6.20 pp. 96 in Saulson's
book).
4.
TauS is output of TauArm function in Bochner's Mathematica program.
5.
fpole = 1/(4*Pi*TauS)
6.
gamma is gammaNormSizeNormDensity in Bochner's Mathematica program. He also
computes another parameter called gammaNormSizeNormDensityMclean which we did not
record.
7.
h(f) is hDCNormSizeNormDensity in Bochner's Mathematica program. He also computes
another parameter called hDCNormSizeNormDensityMclean which we did not record.
8.
Laser power was nominally set at 1.0 watt for all fft.x simulation runs (following Bochner's
instructions) and changed to 6.0 watt (the value in 40m_design.ps) for calculating TauS, fp,
1-C, gamma, and h(f) in Bochner's Mathematica post-processing routine.
9.
FP arm lengths and reflectivity of Mrec were optimized simultaneously in the first (carrier)
fft.x run. Laser moculation frequency (not reported here) and Lassym were both optimized
Graph of transmittivity v.s.
finesse, TauS, fpole, ArmCarr00,
PrcCarr00, h(f).
Abscissa has TITM
Ordinate contains the following
With various units
1. Finesse in Purple
2. S = storage time in ms in
Green.
3. Fpole-arm in Hz in Red.
4. Carrier TEM00 gain in in-line
FP arm in Dark Blue.
5. Carrier TEM00 gain in PRC
in Bright Blue
6. Strain (h(f)) multiplied by
1024 in Black.
Our Role in Construction of Upgraded 40m IFO
In near future New Vacuum System, Output
Chambers, PSL, 12m suspended mass mode cleaner,
4” optics, CDS control system will be installed.
In longer term new Output chamber for signal mirror,
SM optics suspension, control strategy for all optical
Components, M-Z IFO sideband, and possibly
LIGO II SUS and SEI will be used.
Also a hardware prototype for LIGO-II RSE will
Be ready for testing by 2002
We Will participate in planning and carrying out the construction.
Would like to find some small part of 40 m we could commision
At CSUDH then install at 40m such as Pockels Cells
Connections Between Neutrinos and Gravity Waves
Gravity Waves and Neutrinos have similarities in
That they tell yield information about hard to study regions
Of space and time like Stellar Cores and the early Universe
(through Relic Neutrinos and Gravity Waves). Both
Types of radiation travel from a source to an observer with
Little attenuation, scattering, or bending; and thus maintain
Information on the source. Both have been touted as
Opening op a new field of Astronomy.
On the other hand complimentary roles are played
By neutrinos and gravity waves. Gravitons have large
Wavelengths but neutrinos have extremely small de Broglie
Wavelengths. Gravitons are a force carrying gauge Boson
while neutrinos are particles that interact through the weak
(and gravitational Force). The weak force is short ranged
While gravity is long ranged.
In the past we have helped with the old 40 m and to make
Seismic Transfer function and noise measurements for the
upgraded 40m. We are interested in active seismic isolation
techniques like STASIS.
Three types of neutrino experiments using natural
sources may provide useful
Correlations with Gravity waves.
1. Low Energy (30MeV or less) from Supernovae that
are usually studied in conjunction with Solar
Neutrinos.
2. Studies of intermediate Energy (E< 10 GeV)
Neutrinos. These Experiments are designed for
atmospheric neutrinos
3. Studies of High Energy (E> 10 GeV) UpwardStopping or Through-Going Muon (or Tau)
Neutrinos.
Super-Kamiokande Studies All Three Types of Neutrinos
The LIGO-SNEWS (Supernova Early Warning System) Connection
K. Ganezer and Szabi Marka (CalaTech) have written up
With the help of others A LIGO software proposal and report
That outlines how LIGO might receive join SNEWS
As both an alarm sender and receiver; “Entry of
LIGO into SNEWS and initiative for further cooperative agreements”
SNEWS is designed to provide advance notice to optical
Observatories and “Amateur Astronomers” that the EM signal from
A Supernova will arrive soon. The system is running in test mode
At Super-K and after the September SNEWS board meeting
Will become fully operational. The CSUDH group would like to follow
Through on the plan in the proposal working closely with Szabi Marka
And with the help of other members of the LSC
Supernovae are seen by optical observers and occasionally, if nearby by neutrino telescopes
The SNEWS initiative arises in part from a natural partnership
Neutrinos in particular SN neutrinos measured by Super-K offer
The best pointing accuracy for early warning or refined analysis for
Supernovae, especially in the early phases of GW Astronomy.
This is because Neutrino detectors are triggered and have multiple
Particle like events that point well to the source ( 2-5 degree
Accuracy for Super_Ka galactic supernova (per Beacom and
Vogel (1999)) using neutrino-electron elastic scattering.
GW detectors need verification from neutrino experiments
Distinguish a real signal from possible unknown noise sources
(until noise sources are better understood) as well as for pointing.
Eventually GW detectors will have a much longer range
(50 Mpc to the Virgo Cluster and further) for SNs. There
Is currently a great uncertainty in the precise form and strength of an
SN (type II or type Ia) GW signal. Arnaud et. al.
Has applied a collection of SN gw waveform envelopes and 9 different
Types of filters to create a near real-time SN trigger for VIRGO
Szabi Marka and K. Ganezer plan to use the extensive
Base of LSC burst signature work to construct an
On-line SN trigger system that would work in near- real
time at could be used to send an alarm to SNEWS.
Please see the SNEWS web page and the LIGOSNEWS web page. We believe that this will take about
a year. The trigger will also allow us to determine
accurate upper limits on SN GW signals and on SN
Occurrence rates. We hope to later apply these ideas to
other burst sources. It is notable that the few GRBs that
have optical counterparts are at distances in excess of
300 Mpc. However perhaps continuous GR sources
Mostly in the Milky including the nearby Gould Belt
May have interesting GW signals.
The entry of LIGO into SNEWS has several complications
Including.
1. Issues of Confidentiality and of the Independence of
Collaborations and Credit for discovery
2. False Alarms and credibility of collaborations and
Experiments. This is greatly reduced when coincidences
are used since detector specific noise sources are
highly unlikely to produce coincidences of two or more
detectors. Indeed coincidences among gravity wave
detectors is a technique that has been proposed before
to verify detections and to diminish false alarms.
3. A near real time supenova alarm will be difficult
because matched filters are not available for SNs; but
The VIRGO (Arnaud et. Al.) technique is promising.
4. Early GW detectors may not have as large a range as
existing neutrino detectors (Super-K can detect an SN
as far away as Andromeda with high efficiency.
Summary
As part of the LSC the CSUDH Elementary Particles and
Relativity Group, CSUDH/ EPRG would work on
1. Simulations for the upgraded 40m. In the near term
involving the FFT program and in particular simulations of
the advanced optical configurations.
2. The Construction of the upgraded 40m.
3. Correlating Neutrino and GW measurements. In particular
correlations between Super-K and LIGO.
4. Entry of LIGO into SNEWS and on-line detection of GW
bursts from SNs and other sources. Also work on other
cooperative agreements involving LIGO.