CSUDH EPRG, The 40m IFO, and Connections With Physics

1
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
2
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
3
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
4
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.

5
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.
6
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

7
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

8
Work So Far With FFT And Near Term Plans

• 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.

9
Perfect Optics
Results of 40m Single Recycling
Simulations Assumes perfect mirrors. See notes
following the table. (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)
10

• Notes
• 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.
• 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.
• finesse PiSqrtr1r2/(1-r1r2) where r1
  SqrtR_Mft and r2 Sqrt.999935 are amplitude
  reflectivities of mirrors at ends of FP cavity
  (equation 6.20 pp. 96 in Saulson's book).
• TauS is output of TauArm function in Bochner's
  Mathematica program.
• fpole 1/(4PiTauS)
• gamma is gammaNormSizeNormDensity in Bochner's
  Mathematica program. He also computes another
  parameter called gammaNormSizeNormDensityMclean
  which we did not record.
• h(f) is hDCNormSizeNormDensity in Bochner's
  Mathematica program. He also computes another
  parameter called hDCNormSizeNormDensityMclean
  which we did not record.
• 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.
• 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 in
  the second (sideband) fft.x run.

11
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.
12
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
13
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.
14
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.
15

• Three types of neutrino experiments using natural
  sources may provide useful
• Correlations with Gravity waves.
• Low Energy (30MeV or less) from Supernovae that
  are usually studied in conjunction with Solar
  Neutrinos.
• Studies of intermediate Energy (Elt 10 GeV)
  Neutrinos. These Experiments are designed for
  atmospheric neutrinos
• Studies of High Energy (Egt 10 GeV)
  Upward-Stopping or Through-Going Muon (or Tau)
  Neutrinos.

Super-Kamiokande Studies All Three Types of
Neutrinos
16
(No Transcript)
17
(No Transcript)
18
(No Transcript)
19
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
20
Supernovae are seen by optical observers and
occasionally, if nearby by neutrino telescopes
21
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
22
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 LIGO-SNEWS 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.
23
(No Transcript)
24
(No Transcript)
25

• The entry of LIGO into SNEWS has several
  complications
• Including.
• 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.

26
Summary

• As part of the LSC the CSUDH Elementary Particles
  and Relativity Group, CSUDH/ EPRG would work on
• Simulations for the upgraded 40m. In the near
  term involving the FFT program and in particular
  simulations of the advanced optical
  configurations.
• The Construction of the upgraded 40m.
• Correlating Neutrino and GW measurements. In
  particular correlations between Super-K and LIGO.
• 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.