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

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

Members of CSUDH EPRG

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 calculateSix parameters as a function of RITM any one of whichCan be used to drive design. Our results of full FFT relaxationCalculation are consistent with simple analytical calculations2. We will do similar calculations for the dual recycling Upgraded 40m configuration. Have fixed minor problemsWith DR FFT code from repository3. Fred Jenet has done most of work to set up SR FFT toRun 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. DifferentExecutables will be compiled under different cpp options.

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)

Perfect Optics

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 in the second (sideband) fft.x run.

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, OutputChambers, 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 opticalComponents, M-Z IFO sideband, and possiblyLIGO II SUS and SEI will be used.Also a hardware prototype for LIGO-II RSE willBe 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 commisionAt CSUDH then install at 40m such as Pockels Cells

Connections Between Neutrinos and Gravity Waves

Gravity Waves and Neutrinos have similarities inThat they tell yield information about hard to study regionsOf space and time like Stellar Cores and the early Universe(through Relic Neutrinos and Gravity Waves). BothTypes of radiation travel from a source to an observer withLittle attenuation, scattering, or bending; and thus maintainInformation on the source. Both have been touted asOpening 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 rangedWhile 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) Upward-Stopping 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 upWith the help of others A LIGO software proposal and reportThat outlines how LIGO might receive join SNEWSAs both an alarm sender and receiver; “Entry ofLIGO into SNEWS and initiative for further cooperative agreements”

SNEWS is designed to provide advance notice to opticalObservatories and “Amateur Astronomers” that the EM signal fromA Supernova will arrive soon. The system is running in test modeAt Super-K and after the September SNEWS board meetingWill become fully operational. The CSUDH group would like to followThrough on the plan in the proposal working closely with Szabi MarkaAnd 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 partnershipNeutrinos in particular SN neutrinos measured by Super-K offer The best pointing accuracy for early warning or refined analysis forSupernovae, especially in the early phases of GW Astronomy.This is because Neutrino detectors are triggered and have multipleParticle like events that point well to the source ( 2-5 degreeAccuracy 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. ThereIs currently a great uncertainty in the precise form and strength of anSN (type II or type Ia) GW signal. Arnaud et. al.Has applied a collection of SN gw waveform envelopes and 9 differentTypes 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 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.

The entry of LIGO into SNEWS has several complicationsIncluding.1. Issues of Confidentiality and of the Independence ofCollaborations and Credit for discovery2. 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.