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

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)

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

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  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 = 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). • TauS is output of TauArm function in Bochner's Mathematica program. • fpole = 1/(4*Pi*TauS) • 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 (E< 10 GeV) Neutrinos. These Experiments are designed for atmospheric neutrinos • Studies of High Energy (E> 10 GeV) Upward-Stopping or Through-Going Muon (or Tau) Neutrinos. Super-Kamiokande Studies All Three Types of Neutrinos

  16. 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

  17. Supernovae are seen by optical observers and occasionally, if nearby by neutrino telescopes

  18. 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

  19. 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.

  20. 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.

  21. 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.

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