1. technology and computing
2. software

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NSF 04-041
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0509690
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PHY - LIGO, OPERATIONS & ADVANC R&D
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Optical Simulations for Active Thermal Compensation at Advanced LIGO
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PI/PD DEPARTMENT
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1000 East Victoria Street
Department of Physics
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Carson, CA 90747
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REPRESENTATION IS REQUIRED FOR PROPER INTERPRETATION (GPG I.E.1)
High Degree
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PhD
1983
310-243-3438
[email protected]
PhD
1968
310-243-3783
[email protected]
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Kenneth S Ganezer
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Sam L Wiley
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Page 1 of 2
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Page 2 of 2
Optical Simulations for Active Thermal Compensation at Advanced LIGO
This three-year project will support the efforts of the CSUDH LIGO Scientific
Collaboration (LSC) subgroup. The major element and by far the highest priority of this
proposal are optical simulations for the development of active thermal compensation at
Advanced LIGO (A-LIGO). We will work closely with and be assisted by members of
the core optics and coatings and thermal compensation groups at Caltech LIGO
Laboratory, in particular by Dr. Phil Willems (see the letter of support in the Appendix to
this proposal) to formulate a carefully tested and optimal design for the active thermal
compensation system for A-LIGO. Our simulations will focus on the FFT full field
relaxation code and on a MATLAB and FEMLAB based finite element model recently
developed by Dr. Willems to simulate the effects of thermal lensing and thermal
expansion on individual optical elements.
We will also continue our on-going efforts on upgrading and maintaining the band
limited root mean square (BLRMS) seismic monitor software that is used for on-line data
acquisition and as a Figure of Merit in the control room at both LIGO sites (LIGO
Hanford Observatory and LIGO Livingston Observatory).
We will provide the only full field simulations presently available to the LSC for
interferometers with dual recycling (DR) using the DR version of the LIGO FFT code.
This project has five elements including addition of modulation sidebands (mod-sbs) to
the DR version of the FFT code, an investigation of thermal effects on the auto locking
system for A-LIGO with emphasis on the 9 MHz and 180 MHz mod sbs of A-LIGO,
studies of GW sideband extraction efficiency and performance in A-LIGO for various
tunings of the signal recycling cavity including signal recycling (SR), tuned SR, and the
resonant sideband extraction (RSE) limit, studies of thermoelastic deformations
including thermal expansion in A-LIGO, and the design of the active thermal
compensation system for A-LIGO.
Broader Impacts of This Project
This proposal will involve two CSUDH undergraduate students as well as two
physics faculty members. In addition to making an important scientific contribution to the
LSC our efforts will bring frontier research in one of the most promising new areas of
Physics and Astronomy to a minority institution and to the only public University in the
state of California that is a member of the LSC. This will complement, enhance, and
advance a strong research effort at the CSUDH Physics Department in particle
astrophysics, nuclear and particle physics, cosmic rays and in biomedical applications of
physics. In so doing it will provide an extraordinary research and educational experience
for CSUDH students and help to develop new educational programs in physics and
related disciplines.
TABLE OF CONTENTS
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Total No. of
Pages
Page No.*
(Optional)*
Cover Sheet for Proposal to the National Science Foundation
Project Summary
(not to exceed 1 page)
1
Table of Contents
1
Project Description (Including Results from Prior
NSF Support) (not to exceed 15 pages) (Exceed only if allowed by a
specific program announcement/solicitation or if approved in
advance by the appropriate NSF Assistant Director or designee)
15
References Cited
6
Biographical Sketches
(Not to exceed 2 pages each)
Budget
4
5
(Plus up to 3 pages of budget justification)
Current and Pending Support
2
Facilities, Equipment and Other Resources
2
Special Information/Supplementary Documentation
1
Appendix (List below. )
(Include only if allowed by a specific program announcement/
solicitation or if approved in advance by the appropriate NSF
Assistant Director or designee)
Appendix Items:
*Proposers may select any numbering mechanism for the proposal. The entire proposal however, must be paginated.
Complete both columns only if the proposal is numbered consecutively.
Optical Simulations for Active Thermal Compensation in Advanced LIGO
Introduction
This three-year project will support the research efforts of the CSUDH subgroup of the
LIGO Scientific Collaboration (LSC). We have been a member institution of the LSC and of the
LIGO-I and Advanced LIGO (A-LIGO) collaborations for over four years, having joined the
LSC in August 20001-2. In this project we will undertake optical simulations and calculations for
A-LIGO and participate in upcoming data and engineering runs during the proposed three-year
grant period, as required by the collaboration. This project will also support our continued
participation in the detector characterization group, in particular to upgrade and maintain the
software for the band limited seismic noise monitors (blrms) at LHO and LLO. One of the
investigators, Dr. Ganezer, is also a member of the Burst Source data analysis group, although no
funds are requested in this proposal for burst source analysis.
In the current decade a new generation of gravitational wave observatories will likely
bring about major advances in physics and astronomy through direct observation and
characterization of gravitational radiation3-6. The first of these instruments are the 2 Km and 4
Km Interferometer observatories (IFOs) at LIGO Hanford Observatory (LHO), and the 4 Km at
LIGO Livingston Observatory (LLO). During the last science run (S3), the strain sensitivity at
HLO was within a factor of the design specification of 10-21 at LHO for frequencies between
about 100 and 400 Hz and slightly worse for optimal data at LLO (acquired during the night
hours when seismic noise is minimal).
Engineering data was first taken by LIGO in 20017 and more than ten engineering runs
have been completed since then. The first LIGO science data run (S1) took place for two weeks
in 2002 and was followed by the E9 engineering run from January 24-27, 2003 and the S2
science run from February 14 through April 14, 2003. The CSUDH LIGO subgroup participated
in S2 by undertaking a total of 5 expert shifts and 8 training shifts at LHO and LLO (as required
for 2 full time equivalent scientists; FTEs). The E10 engineering and S3 runs took place from
October 17-24, 2003 and from October 31, 2003-January 5, 2004 respectively. The CSUDH
group undertook six expert shifts at LHO (2 FTEs) during S3. The E5 Engineering run took
place from October 22-24, 2004 and E11is scheduled to take place at LHO only from November
17-23. The S4 run will start sometime after January 2005 and will last for three months. During
S4 it is expected that sensitivities will be achieved at LHO and LLO that approach the 10-21
design levels.
S5 is tentatively scheduled for late 2006. Its duration will be as high as six months, and
will depend upon the sensitivity achieved in S4. LIGO-I data taking will conclude in 2007 to
make way for an upgrade to A-LIGO between 2006 and 2008. We plan to participate in all
LIGO-I and Advanced LIGO science runs. In the fall of 2004, NSF funding was tentatively
approved for an upgrade of the LIGO Interferometer Observatories (IFOs) to A-LIGO.
The data analysis groups have analyzed data from S1 for burst, inspiral, stochastic,
continuous and periodic sources and a series of articles on these analyses have been published812
. CSUDH had one author (K. Ganezer) on each of the S1 papers. We are currently participating
in burst analysis for S2 and S3. Sam Wiley has been added to the author list for LIGO papers on
S2, S3 and subsequent data runs; thus our subgroup now has two members who are authors on
LSC papers (K. Ganezer and S. Wiley). Some S2 articles are already under review or in
manuscript form13-14.
Rudiments of Optical Simulations for Thermal Compensation of Advanced LIGO
The level of success of LIGO hinges upon how well the project meets its planned strain
sensitivity of about 10-21 for LIGO-I and 10-22 for A-LIGO for gravitational waves of frequency
50-300 Hz. To achieve these specifications the performance of the interferometer must be
accurately modeled and residual sources of noise need to be understood. This requires
simulations that are as realistic as possible. Therefore an important task for the LSC is the
detailed optical modeling of the LIGO IFOs. These models must incorporate optical
imperfections including local and global deviations or deformations from the specified shapes
and from the nominal transmission and reflection coefficients. Imperfect optical elements
contribute significantly to noise by exciting higher order (than TEM00) modes and by increasing
shot noise due to loss of light from scattering out of the beam volume. Additional noise comes
from out-of-beam light that is scattered a second time back into the beam (through rescattering).
Since LIGO will probe new sensitivity levels with new technology, we cannot rely upon
previous data or simulations. Thus analytical and numerical models as well as prototypes are
pivotal to LIGO detector research and development. Several design issues and suggested
modifications for A-LIGO have recently arisen. By virtue of its high Q of 2 x 108, single-crystal
sapphire has low thermal Brownian noise in the gravitational wave (GW) frequency band of
greatest sensitivity (50-300Hz). Thus current plans for A-LIGO involve the use of Sapphire for
all of the test masses (the ITMs and ETMs). Fused silica optics (of Q= 3 x 107) will be used for
A-LIGO if high-quality Sapphire is not available for the relatively large (40kg) A-LIGO ITMs
and ETMs (see Figure-1) or if fused silica is shown to outperform Sapphire.
Our optical simulations to date have focused on the so-called FFT15 program, which
propagates light using Fast Fourier Transforms (from which the name is derived). The original
FFT code was written and applied to GW detectors for the first time by Jean-Yves Vinet of the
VIRGO collaboration. FFT has been applied to LIGO by several LSC members and was first
adapted by Brett Bochner to include realistically imperfect optics (from 1994-1998). Bochner
used FFT to set tolerances for imperfections for LIGO-I.
Sapphire and fused silica have quite different material properties, Sapphire having a
higher thermal conductivity (by a factor of 30), higher density and index of refraction, and larger
thermal expansion coefficient (by a factor of 10) compared to fused silica16. Recent theoretical
calculations indicate that the large thermal conductivity of Sapphire leads to significant levels of
thermo-elastic shot noise17-18. Our FFT simulation code cannot be used to model dynamic
phenomena such as thermal noise. Nonetheless the effects of thermal distortions such as thermal
lensing (“dn/dT” induced changes in the local index of refraction or simply thermorefractivity)
and thermal expansion can be studied using FFT and input phase maps for reflections from
optical surfaces and for transmission through substrates from measurements of real optics or
from a separate numerical calculation. In this proposal we put forward a plan to investigate
thermal lensing and thermal expansion using FFT, finite element models and real phase maps
when available.
In the past, we investigated the effects of imperfections in mirror shapes (resulting in
phase deformations) on IFO performance. A grid of 1.2 m x 1.2 m transverse dimensions and
256 pixel x 256 pixel square pixels of length 4.7 mm were used. Imperfections involving 1-100
pixels (4.6 mm-46 cm) are of small spatial scale (high spatial frequency) and can be simulated
using randomly deformed individual pixels or groups of pixels. Larger spatial scale
deformations, such as those greater than 1m (low spatial frequency) correspond to imperfections
in radii of curvature (ROC) of the optics (a typical ROC is 100 m or larger for A-LIGO) and can
be modeled using a smooth function such as a Zernicke polynomial. Small spatial scale (high
spatial frequency) imperfections tend to scatter significant light power out of the interferometer
and large spatial scale imperfections excite higher (than TEM00) spatial modes that remain in the
beam and corrupt resonating fields15. Tilts are modeled by directly rotating the optical axes in
each of the two transverse directions. Bochner found that tilts of less than about 1 µ-radian cause
insignificant degradation in interferometer performance15. Since LIGO-I and A-LIGO use an
auto-alignment control system that holds each optic in alignment to an accuracy of better than
10-8 radians15 tilts are not a significant problem.
FFT calculates the static electric fields on transverse grids in a LIGO-type Interferometer.
Fields are propagated using two-dimensional fast Fourier transforms and are relaxed within a
specified tolerance using an iterative technique. FFT calculates the basic fields and uses a
transverse grid of pixels (usually 256 x 256 pixels). It is assumed by FFT that nearly all of the
beam will be contained within a cone about the (beam) axis of half-angle θ that is small enough
that cos (θ) may be approximated by ½θ2. This “paraxial” assumption is equivalent to the nearfield (Fresnel) approximation.
A variety of optical imperfections can be modeled by FFT. These include15 misalignment
and mode-mismatch of the beam, finite mirror size effects including “clipping” and diffraction,
curvature distortions, mirror and beam splitter tilts, surface roughness, and substrate
inhomogeneities. FFT optimizes cavity lengths and the reflectivity of certain optics and includes
the effects of GW and modulation sidebands in A-LIGO and LIGO-I versions of the code
respectively. FFT makes microscopic adjustments to default lengths in order to satisfy various
resonance conditions.
The output of FFT contains grid-based maps of the real and imaginary parts of the
electric field and of the E-field intensity at all optical surfaces for the carrier and selected
sidebands. FFT simulations are used to calculate TEM00 power and power in each of a selected
number of higher order modes in the signal recycling and power recycling cavities (SRC and
PRC) and in each of the Fabry-Perot (FP) arms using a modal decomposition. It also calculates
the contrast defect, the strain sensitivity, and the signal to noise ratio at the output photodiode.
Other FFT output parameters include the finesse, storage time, cavity pole, power gain in
the FP arms, power in the carrier modes and sidebands, optimized recycling mirror reflectivity,
signal to noise ratio, and strain sensitivity for DC readout. In addition FFT can optimize the
Schnupp asymmetry15 and19, the difference in the lengths of the two arms of the recycling cavity
divided by two, the recycling mirror reflectivity, the modulation frequency, and the reflectivity
of the PRM.
There are several versions of the FFT program currently in use by the LSC. These include
single workstation codes for the LIGO-I power- recycling-only configuration (PR FFT) and for
the A-LIGO dual (power and signal) recycling setup (DR FFT) and versions to run on a parallel
machine under the MPI (message passing interface) architecture for the power-recycling (MPI
PR FFT) and dual-recycling (MPI DR FFT) configurations. The MPI DR version was developed
by CSUDH2 with the help of our LSC colleagues from the original paragon parallel architecture
of DR FFT used by Brett Bochner in his PhD thesis15.
A Schematic of A-LIGO with up-to-date specifications is given in Figure-1. A-LIGO is a
dual recycled FP interferometer with perpendicular arms, a power recycling mirror (PRM) at the
symmetric beamsplitter (BS) port (the bright port), a signal recycling mirror (SRM) at the
antisymmetric BS (dark) port, and input and output mode cleaners. Each of the FP arms is
formed from an input test mass (ITM) and an end test mass (ETM). Power recycling increases
light storage time and gain while signal recycling allows for an enhancement of the amount of
power in the GW sidebands.
Figure-1 gives the definitions of various lengths (L1 through L6) and electric fields (such
as Elas, and EFPinr for the entering beam and for the FP field on the reflective BS side
approaching the ITM respectively, that are used by FFT. A-LIGO and other dual recycled IFOs
(such as the Caltech 40m) may be operated in the Signal Recycling (SR or broadband SR), tuned
SR (narrow-band SR), and in the Resonant Sideband Extraction (RSE) limit modes. The SRC
extends from the ITMs (of both arms) to the SRM. In SR or tuned SR the SRC is set to antiresonance for the GW (signal) sidebands that are formed from beats between the carrier and the
signal. This results in a lower transmittance and increased storage time of the gravitational wave
signal20 and 21. The carrier power in the FP arms for A-LIGO is currently planned to be 850 kW
(not 680 kW as indicated in Fig.-1). These high power levels will require active thermal
compensation in the form of a heating ring or element or a scanning laser, as indicated in Fig.-1.
This proposal focuses on optical simulations that will guide the development and implementation
of the active thermal compensation efforts for A-LIGO.
In the next two to three years the major design features of A-LIGO will be determined.
Many difficult issues need to be resolved. A-LIGO will include Sapphire or fused Silica test
masses, 125 Watts of excitation power, and high FP and PRC gain equal to 770 and 14.3
respectively. The high levels of optical power circulating in the A-LIGO FP arms make thermal
distortions of the optics and thermal compensation important issues for A-LIGO22-24 and 64 that
will be tested at sites such as the Gingin High Power Test Facility (HPTF) in Western Australia
and the LIGO Advanced System Test Interferometer (LASTI) at MIT. Additional modeling,
particularly for GW sidebands in the SRC, is an important and yet to be completed component of
studies of thermal effects22 and 65. The full field DR FFT simulations that the CSUDH group is
undertaking can make a significant contribution to the understanding and management of ALIGO thermal effects.
Among the major thermal effects in A-LIGO are thermoelastic noise due to high frequency
(Brownian motion) fluctuations in mirror positions, thermal lensing in substrates due to local
changes in the index of refraction with temperature (sometimes called thermorefractivity or
dn/dT), and thermal expansion of the optical surfaces. The main consequence of these effects is
increased scattering in the interferometer, in particular in the PRC and SRC. Thermoelastic17 and
thermorefractive shot noise18 have undergone significant study by the LSC using the MELODY
(MATLAB based) program25. Since FFT models a static interferometer, it cannot simulate
thermoelastic noise, however it can model thermal lensing and thermal expansion.
Concerns have been raised about the high levels of circulating power in A-LIGO. Of
specific interest are parametric instabilities in the FP arms17, 18 and 26-30. The loss of TEM00 light
due to this phenomenon might limit the power circulating in the arms and may have discernable
effects even at low power above three kilowatts. The instability results from interference of the
natural mode of vibration of the arm cavity test masses with the optical resonance of the cavity.
Parametric oscillations may also result in instability of modulation sidebands. Thus the CSUDH
group was asked by the LIGO optics group to undertake a study of modulation sidebands for ALIGO. We plan to modify DR FFT to include modulation sidebands (SBs), a non-trivial yet
highly feasible endeavor given the use of modulation SBs in the LIGO-I version of FFT.
GW sideband and carrier degradation due to thermal effects in LIGO and A-LIGO have
been considered for more than 12 years31. Over the past two years experiments have been
undertaken at LHO that correct in part for thermal distortions in wave fronts due to transmission
through substrates as well as reflection. The technique reduces temperature asymmetries in the
optics in near real time through heating of low temperature regions to bring the optics to a
uniform temperature profile. This approach has been developed and tested over the past five
years, and is known as adaptive thermal correction. Presently the two leading options for thermal
compensation in A-LIGO involve a cylindrical nichrome heating ring or a scanning CO2 laser for
non-axisymmetric distortions16 and 32. These efforts are based on earlier work at MIT by Ryan
Lawrence and others33and 34.
We will study thermal effects in A-LIGO using MPI DR FFT. In particular, we will
investigate (broadband) SR, tuned SR, and the RSE limit in the presence of thermal effects and
possibly other imperfections such as surface roughness. A recent paper by Bochner21 considered
the RSE limit for A-LIGO and concluded that it is crucial to limit scattering losses in the high
finesse arms of A-LIGO for RSE to be viable. For thermal lensing and thermal expansion we
will undertake simulations using analytical expressions for the distorted fields23 and 25, the
MELODY program25, and a new finite element model from Caltech (described below) to
generate mirror phase maps with appropriate distortions due to thermally loaded mirrors, as input
to the FFT program. FFT will then be used to calculate the GW signal at the GW readout
including degradations due to thermal effects.
Several design changes have been recently suggested to increase the sensitivity of ALIGO by reducing thermal noise. These include the use of cork-shaped test masses, flat-topped
beams, and a large spot size. Such proposals have been tested to some extent using PR FFT27-28.
If these ideas are likely to be approved for A-LIGO we will study their influence on thermal
compensation using DR FFT, the only version of FFT, which includes the SRC and thus the
gravitational wave signal vis-à-vis gravitational wave sidebands. Calculations of thermal effects
in the SRC (including GW-sbs) have been noted by the LIGO thermal compensation group as an
important new avenue to pursue. A recent talk on optical compensation in A-LIGO22 that
includes the results of MELODY based modeling concluded, “More modeling is required to fully
set design requirements (particularly for SRM modes)”. The CSUDH group has been asked by
the LSC optics and core optics and coatings group to undertake FFT based calculations of
thermal effects in A-LIGO26 (also see the attached letter of support).
Figure-1: A Schematic of the Optics for Advanced LIGO.
Lengths in A-LIGO and LIGO-I are controlled using beats between the carrier and
sidebands and between sidebands of different frequencies. Dark port beam sensing photodiodes
are used for DC detection of possible gravitational wave signals. The control and data readout
scheme for A-LIGO includes two pairs of (positive and negative) phase-modulated sidebands
applied in series. All modulation sidebands are resonant in the PRC and non-resonant in the FP
arms and must pass through the output mode cleaner. The difference between the two
modulation frequencies is as high as possible to allow for maximum separation in frequency for
PRC and SRC control signals. The higher sideband frequency must be a harmonic (integer
multiple) of the lower frequency so that both sidebands will resonate in the PRC. The lower
modulation frequency was chosen to be 9 MHz, the fundamental frequency of the 8m-long PRC.
The higher modulation frequency is 180 MHz, the largest harmonic (n=20) of the fundamental
frequency that is practical given limitations on microwave modulation and detection
technologies.
The Schnupp asymmetry (length) is the difference between the distance from the
beamsplitter to the symmetric port (L2 =L+; see Figure-1) and the distance from the beamsplitter
to the asymmetric port (L3=L-). By convention L+ is always taken to be greater than L-. The
value of the Schnupp Asymmetry ((L+ - L-)/2= (L2 - L3)/2) is chosen so that the carrier is at a
dark fringe, the 180 MHz sidebands are bright, and the 9 MHz sidebands are nearly dark at the
asymmetric (beamsplitter) port. Since the 180 MHz sidebands are bright at the asymmetric port
and in the SRC (between the beam splitter and the asymmetric port), they are used to sense the
SRM. The 9 MHz sidebands are resonant in the PRC and nearly dark in the SRC, thus they are
used to sense the PRM. Beats between the carrier and the 9 MHz sidebands at the symmetric port
are used to sense and control L+. Beats at the asymmetric (beamsplitter) port between the carrier
and the 180 MHz sidebands are used to control L-. The lengths of the SRC, PRC, and the
Michelson arms are sensed using beats between the 9 MHz and 180 MHz sidebands.
Initial Results of Optical Simulations on Thermal Effects in A-LIGO and LIGO-I
In the past six months we have made some initial investigations into the effects of thermal
lensing on GW sidebands in A-LIGO and on modulation sidebands in the H4K as-built. These
FFT based simulations use phase maps generated by the finite element (FEMLAB) model of Phil
Willems that simulates the effects of light propagation through the heated ITM substrates.
In Figure-2a below we show the power as a function of frequency (the power spectrum) for a
tuning frequency of foptim = 250 Hz for the positive GW-sb (the dominant sideband for a positive
tuning) for perfect optics and for thermal lensing in the ITM substrates. As indicated by the
curve in yellow triangles, the frequency of maximum power (fmax) in the spectrum has been
shifted from about 250 Hz in the perfect case to about 50 Hz in the case of thermal lensing as
simulated by the FEMLAB phase maps. The peak (fmax) for the case of thermal lensing is much
broader, more asymmetric, and nearly washed out. Additional plots are provided in Figure 2a for
perfect mirrors with a radius of curvature (ROC) of the Signal Recycling Mirror (SRM) that has
been increased by factors of 5% and 10% in order to roughly approximate the effects of thermal
lensing through a “curvature mismatch”. The curve with 10% ROC increase does approximate
the effects of thermal lensing, since it has fmax shifted (from 250 Hz as in the perfect case) to
about 50 Hz and since it has an asymmetric highly broadened spectrum. Figure-2b demonstrates
how progressively higher proportions of curvature mismatch, gradually distort the GW-sb
frequency spectrum and shift fmax to lower frequencies. This figure includes the case of perfect
optics and 1 %, 3%, 5%, and 10% curvature mismatches. It is interesting that in both the case of
the highest ROC curvature mismatch (10%) and the case of the ITM thermal phase maps less
than half of the power in the +250 Hz GW-sb is in the TEM00 mode, 25% and 35% respectively,
while in the case of perfect optics nearly all power (more than 99.99%) is in the TEM00 mode.
This indicates that the thermal maps mimic a curvature mismatch between the beam and the
SRM.
Positive GWSB Power vs Frequency
40
35
35
30
30
25
10% Mirror Mismatch
5% Mirror Mismatch
Thermal Lensing
Perfect Mirrors
20
15
GW Power x E-09
GW Power x E-09
Positive GWSB Power vs Frequency
40
25
15
10
10
5
5
0
10% Mirror Mismatch
5% Mirror Mismatch
3% Mirror Mismatch
1% Mirror Mismatch
Perfect Mirrors
20
0
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250
Frequency (hz)
300
350
400
450
0
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350
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Frequency (hz)
Figure 2. The effects of thermal lensing for foptim = 250 Hz on the positive (dominant) sideband; Fig. 2a (left)
compares perfect optics with of thermal lensing simulated by the Willems FEMLAB model and with ROC
mismatches of the SRM with the beam while Fig. 2b (right) shows the perfect optics case and how (ROC) curvature
mismatches of the SRM can approximately mimic the effects of thermal lensing. Fig. 2b contains curvature
mismatches of 1, 3, 5 and 10 %.
In Figure-3a below the residual phase (compared to resonance) is plotted as a function of
frequency for the cases considered in Figure-2, perfect optics, thermal lensing of the ITM
substrates using the FEMLAB model, and curvature mistaches of 1, 3, 5, and 10 %, for an SRC
tuning frequency of foptim = 250 Hz. The curve for 10% mismatch indicates that the SRC exhibits
broadband behavior becoming nearly degenerate for a range of GW–sb frequencies from 0 to
+400 Hz. Figure-3b contains an intensity map and intensity profile for the +250 Hz GW-sb in
the A-LIGO SRC with Sapphire optics. These plots were made using thermal maps for
transmissions through the ITMs generated by the FEMLAB model and an SRC tuning with foptim
= + 250 Hz. The secondary peaks (the “horns”) in the intensity profile indicate the presence of
higher order modes, and indeed a modal analysis (using 256 modes) shows that 75% of the
power in the + 250 Hz GW-sb for this case is in modes other than TEM00. This type of modal
composition and profile for sideband power is indicative of a significant effective curvature
mismatch and in agreement with the results of Figure-2 which indicate that thermal phase maps
(from the FEM model) cause an effective beam ROC mismatch (with the optics of the SRC) that
is similar to that expected from an increase in the ROC of the SRM of 10%.
Plus GWSB Phase vs Frequency
6.00E-01
SB Phase From Resonance (rad)
5.00E-01
4.00E-01
Thermal Lensing
Perfect Mirrors
10% Mirror Mismatch
1% Mirror Mismatch
3% Mirror Mismatch
5% Mirror Mismatch
3.00E-01
2.00E-01
1.00E-01
0.00E+00
0
50
100
150
200
250
300
350
400
450
-1.00E-01
Frequency (hz)
Figure-3a (left). GW-sb residual phases compared to resonance for an SRC tuning of foptim = 250 Hz as a function
of sideband frequency for the cases of figure 2 ; perfect optics, thermal phase maps for the ITM substrates, and SRC
beam curvature mismatches of 1, 3, 5, and 10 %. Figure-3b (right). An intensity map and profile for the +250 Hz
dominant GW- sb for the case of foptim = 250 Hz with thermal maps from the Willem’s FEMLAB model used for
transmission through the ITMs (units are arbitrary).
As a prelude to our studies of thermal effects in A-LIGO, we performed FFT simulations
of the positive and negative 24.482 kHz modulation sidebands for the (LIGO-I) LHO-4K IFO
(H4K) in its as-built configuration including reflection phasemaps of the as-built ITMs and PRM
that were compiled using interferograms. We also modeled phases acquired from transmission
through the heated ITM substrates using (transmission) thermal maps based on the Willems FEM
model and also looked at the perfect case. Thus, our LIGO-I simulations of modulation
sidebands included a perfect configuration as well as cases with measured (as-built) reflection
phases only and those with FEM thermal phases only.
The H4K and other LIGO-I IFOs (the H2K and the L4K) were built with ROCs designed
to take into account thermal lensing at full laser power, thus the as-built ROC of the H4K SRM
is 14.4 km, significantly larger than it would be if there were no lensing. Since the H4K has been
operating lower laser power than its 6 W specification there is less heating at the H4K then
anticipated and the SRM ROC is not optimally matched to the beam ROC.
Thermal maps from the FEMLAB model were used for transmission through the
substrates of the ITMs in order to take into account ITM lensing in our H4K simulations of
modulation sidebands. In a test at the H4K, W. Kells and P. Fritschel heated both ITMs by
putting the IFO into lock and letting it reach thermal equilibrium before taking the arms out of
lock by misaligning the ETMs35. A “cooling curve” was obtained by keeping the PRC in lock
and measuring the modulation sideband gain (GSB) as a function of time since arm lock was
broken. Kells concluded from the cooling curve that the current less than optimal power mode
(the cool mode) of operation of the H4K (as well as the other LIGO-I IFOs) at significantly less
excitation power than the design specifications, GSB is significantly lower than its design value35.
A plot of GSB versus power in the SRC was obtained by d’Ambrosio using FFT simulations36
that agrees in peak GSB and in shape with our results given below in Fig.-5.
Our FFT as-built results for the H4K with reflection phase maps (and no additional
thermal maps) are in agreement with previous simulations made by Kells and Bhawal that were
used to confirm the presence of significant thermal effects at the as-built H4K35. Since the H4K
currently operates at less excitation power than its design specifications FFT as-built simulations
by the CSUDH group and by Kells and Bhawal and d’Ambrosio yield 24 kHz modulation
sideband powers that are below design specifications.
Our and earlier as-built FFT simulations found that modulation sidebands contained
significant proportions of higher order modes in the PRC due to mode mismatch at the PRM.
These results are outlined in Figure-4, which contains intensity maps and profiles of the +24 kHz
modulation sideband at the PRM (moving towards the beamsplitter) for moderate and strong
thermal lensing in the ITM substrates. For moderate deformations, Fig. 5a and a corresponding
modal decomposition show that most of the mod-sb power is in the TEM00 mode. Figure-5b
demonstrates that a significant fraction of the + 24 kHz mod-sb power in the PRC can be in
higher order modes due to thermally induced mode mismatch in analogy to the thermal effects
for GW sidebands in the A-LIGO SRC outlined in Figs. 2 and 3.
We subsequently added phase maps from the FEMLAB model to simulate thermal
lensing due to transmission through the ITM substrates to our H4K simulations and used the asbuilt 14.4Km ROC for the PRM, without as-built reflection phases. As a result of the inclusion
of the FEMLAB ITM phasemaps, the modulation side band power increased from 7.5 W
(without thermal phases) to 12 W. This increase indicates that a realistic thermal model, in
particular the FEMLAB model of Willems and its ITM transmission maps, can account for at
least some of the thermal lensing in the H4K, and suggests that transmission through the ITM
substrates is a major source of lensing in LIGO-I, as one might expect.
Figure-4a (left). Here we plot the intensity for the +24 kHz modulation sideband in the LIGO-I H4K IFO at the
SRM with as-built reflection phases and moderate ITM thermal transmission phasemaps from the Willems
FEMLAB model. Figure-4b (right). A similar plot is given here with phasemaps representing relatively strong
thermal lensing.
We also simulated the effects of thermal lensing by varying the ROC of the PRM in FFT
to lower values than the cold value (of 14.4 km). In Figure-5a we plot the modulation sideband
gain (G), a parameter that is equivalent to mod-sb power in the PRC per Watt of excitation, as a
function of ROC of the PRM. Our results agree well with those of d’Ambrosio36 and
qualitatively with an earlier work by Kells35, who used similar approaches of varying the ROC to
mimic thermal lensing. All models find the peak gain at an ROC of about 9.7 Km. Our
calculation yields a (relative) peak gain of about 40 in agreement with d’Ambrosio35. The gain
(G) of the TEM00 mode and the total gain are plotted as functions of the PRM ROC in Figure-5b.
Near 9.7 Km, for the ROC of peak G, nearly all power is in the TEM00 mode. For the lowest and
highest ROC in Fig-5, 8 Km and 14 Km respectively, the TEM00 contribution to G falls off to
50% and 40% respectively of the peak G. Thus there is a significant mode mismatch when the
PRM ROC is set far from its optimal value.
SB Gain vs PRC Curvature
SB Gain vs PRC Curvature
50
50
SB PRC Gain
Too Mode Power
40
30
30
SB Gain
SB Gain
40
20
20
10
10
0
8000
10000
12000
ROC of Power Recyling Mirror
14000
16000
0
8000
10000
12000
14000
16000
ROC of Power Recyling Mirror
Figure-5a (left). A plot of the modulation sideband (SB) gain (G), which equals SB power per Watt of excitation
power, versus PRM ROC for our H4K as-built FFT calculations. Peak gain occurs at an ROC of about 9.7 km.
Figure -5b (right). The TEM00 component of the mod-sb gain (G) and total mod-sb gain (G) versus PRM ROC for
our as-built FFT simulations.
Optical Simulations of Thermal Effects for A-LIGO
We will use a FEMLAB based finite element model that calculates phase deformations
due to thermally generated inhomogeneities in absorption and in the index of refraction, that has
been recently developed by Phil Willems of Caltech-LIGO16 and that builds upon a previous
finite element model of MIT23. Phase maps for reflection and substrate transmission (if needed)
at each of the optical surfaces will be generated by the thermal model (of Willems) and used as
input for FFT in order to simulate thermal-lensing and thermal expansion in A-LIGO.
We have already performed simulations using phase maps from Willems’s finite element
model of the carrier and of the gravitational wave sidebands for Sapphire optics and the current
A-LIGO configuration. Our results indicate that thermal lensing due to the ITMs alone does not
cause significant loss of power or excitation of higher than TEM00 modes for the carrier.
However the GW sidebands are significantly affected, with about two-thirds of the power in
higher order modes, which is likely due to mode mismatch of the heated optics. When we
perform calculations using perfect optics with the radius of curvature (ROC) altered by 5-10%
from the nominal ROC we can mimic to a large extent the effects of thermal lensing on the GW
sidebands.
The main focus of our optical simulations will be a study thermal effects and thermal
compensation in A-LIGO. These efforts will be partitioned into several phases. We are currently
investigating thermal lensing for Sapphire as well as Fused Silica optics, to compare the relative
merits of these two possible materials for the A-LIGO test masses. Our initial results with GW
sidebands suggest that there may be problems with the auto-locking actuator system due to loss
of power and aberrations in the modulation sidebands and that there could be significant loss of
power in the GW sidebands. So the first phase of this proposal will involve studies of thermal
effects and auto-locking at A-LIGO using modulation sidebands. Our initial simulations of
thermal lensing in the ITMs indicate that a narrow band tuning of the SRC to 250 Hz can have its
resonance washed out and can behave as if it were tuned to be broadband and thus degenerate to
a range of GW frequencies and result is significantly reduced power in the TEM00 mode for GWsb power. We expect similar thermally induced aberrations for the modulation sidebands that
may cause problems for length sensing and control. This stage of our project will done in parallel
with stage-5 (described below), in which modulation sidebands will be added by to the A-LIGO
version of the FFT code.
Since modulation sidebands are only required to provide a signal of sufficient power that
they can be used to control IFO degrees of freedom, it is thought that their modal structure is less
important than GW sidebands whose spectrum contains crucial information on the GW signal.
Nonetheless there is a current A-LIGO specification that modulation power in the PRC must not
saturate below 120 W16. If sapphire test masses are used in A-LIGO with a minimal absorption
of 30 ppm/cm and current specifications for the test masses, thermal compensation will have to
reduce this loss by a factor of 5.516, something which was easily realizable in laboratory tests
undertaken by Ryan Lawrence16, 24 and 34. If absorption in Sapphire test masses is found to be a
factor of 3 higher then losses must be reduced by a factor of 68 to reach the A-LIGO criterion on
modulation power saturation, at the limit of the compensation ability demonstrated by
Lawrence16. This is a compelling argument in favor of studying modulation sidebands in ALIGO using FFT and FEMLAB thermal phases.
The second phase of our project will focus on a study of the GW sideband extraction
efficiency and how it relates to detector performance in A-LIGO. This will involve computations
of the Amplitude (or Intensity) spectra for various tunings of the SRC. Thermal aberrations of
the GW sidebands and possibly to the modulation sidebands could dramatically reduce detector
efficiency. In this phase, GW-sb powers will be used to compute shot noise, which will be added
to seismic, and suspension noise to compute sensitivity versus frequency curves for broadband
and narrow band SR tunings. We will also study RSE tunings of the A-LIGO SRC, which should
significantly decrease thermal effects on the optics and GW-sbs. Thermal lensing and thermal
expansion will be included using thermal phase maps for the transmission through the ITMs and
through the bean splitter calculated using a finite element model (FEM). This will involve adding
thermal expansion to the FEMLAB model and thermal effects to the beamsplitter, which will be
done by Phil Willems of Caltech in consultation with our group. As indicated by our initial
studies, thermal effects might significantly diminish the detection efficiency for GW-sbs in ALIGO.
Losses of GW power in the SRC of as little as .1% due to absorption, scattering, or
production of higher order modes have been shown by three different models to cause a
significant decrease in binary inspiral range of 5%16 (decreasing detection rates by 14%). Thus
detailed modeling of GW sidebands in A-LIGO with FFT, as well as with MELODY have been
called essential16.
Thermo-elastic deformations in A-LIGO using FFT and the FEMLAB model (of
Willems), is the topic of the third phase of this project. The high power of about 850 kW
circulating in the arms may cause the High Reflectivity (HR) surfaces of all four test masses (the
ITMs and ETMs) to be deformed resulting in changes in the mode size and shape, and
composition including excitation of higher order modes. Changes in modal size result in
distortions that can likely be corrected by adjusting the beam ROC, however changes in modal
shape will have more complicated effects on the optics that will not be cylindrically symmetric
and thus require use of FFT. These asymmetric effects are difficult to simulate using the
FEMLAB thermal model, but nonetheless tractable. It will likely take a multi-step iterative
approach alternating between FFT and FEMLAB modeling to perform these simulations.
The fourth step of this project will focus on modeling and designing thermal
compensators to be built for and installed in A-LIGO. The only way that a reliable compensation
system can be designed is through asymmetric simulations such as those afforded by the FFT
program with appropriate phasemaps to simulate thermal lensing and expansion for the
FEMLAB model. Thus our FFT simulations will guide the hardware design of the compensators.
Our efforts in phases 1-3 on the Auto-locking system, GW-sb extraction efficiency, and optical
deformation in the FP arms will be essential elements in the design and testing of the
compensator system. A central issue will be the type of compensation system, and the two
leading choices at the moment are an external thermal heating element, or a scanning laser based
heating system.
A fifth phase will be the addition of RF sidebands to the DR FFT program, to be
completed early in the project, within the first six months. Since the CSUDH group has
experience with both modulation and GW sidebands through FFT simulations for LIGO-I and ALIGO respectively we have the background to complete this task. The result of these efforts will
be the first full field FFT simulation that includes all sidebands available to the LSC. In addition
a single FFT program will be available that include both the LIGO-I, power recycling only
configuration, as well as the A-LIGO dual (power and signal) recycled configurations. The
addition and propagation of two pairs of modulation sidebands (at 9 MHz and 180 MHz) to the
DR FFT program will complicate the relaxation procedure for FFT somewhat, but will is highly
feasible given the success of modulation sideband simulations in the LIGO-I version of FFT.
Data Characterization Efforts for LIGO-I
One year ago, Dr. Ganezer took over responsibility for maintenance of the band limited RMS
on-line seismic DMT (data monitoring tool) seismic monitors, referred to as “seismic blrms”.
The monitors37 are run by a single program formulated by Ed Daw (formerly of LSU) based on a
template by John Zweizig37, and use IIR filters for band limiting. Seismic blrms is among the
main diagnostic tools for determination of data quality, a so-called figure of merit (FOM) whose
results are projected on the walls of the LIGO control rooms. This FOM is consulted by
scientists and observatory staff in on-line data taking in near real time as well as by those
performing data analysis off-line. We have made simple improvements in the program to find
and label in the plotted minute trends loses of (1 second) data frames in the DMT data due to
various hardware or software problems or to stoppage of lock. An updated version of the blrms
software was tested successfully before and during the E11 engineering run and is planned for
use during the upcoming S4 data run.
Roles of Individuals
The CSUDH LIGO subgroup includes Dr. Kenneth Ganezer, Professor of Physics and
Dr. Samuel L. Wiley, Professor Emeritus of Physics. In spite of a lack of external or reliable
internal funding for LIGO at CSUDH, one undergraduate student and one student from our oncampus high school, in a program sponsored by the Southern California Academy of Sciences
(SCAS), have worked during the past year at CSUDH on our LIGO research. Prof. Ganezer and
Prof. Wiley plan to spend 35% and 50% of their time respectively on our LIGO research. The
two undergraduate students requested can work up to 50% time during the Semester and 100%
time during the summer and winter breaks. In practice, students work about 35% time during the
semester and about 65% time during the breaks, and by not working the full-allotted time might
allow for an additional student to be hired.
All CSUDH LIGO investigators including the undergraduate students will participate in
all studies described in this proposal. Ganezer will focus on optical simulations and software
development for the optical simulations. Wiley will focus on optical simulations and analytical
calculations. Ganezer will maintain the blrms software, a much lower priority than the optical
simulations, but nonetheless a significant contribution to the LSC. The work on the seismic
monitors may be particularly suited for the students because it involves real time data that is
available through the web, does not require advanced computer or physics skills, can be done
remotely, and is closely associated with hardware.
Timeline
Our studies of thermal effects and auto-locking will begin in the first year, and will take
six months to complete. The addition of RF sidebands to the DR FFT program will be
undertaken and completed in the first year. Studies of the GW extraction efficiency will be
started during the first year and take about six months to complete, and this activity may
continue with into part of the second year. Our studies of thermo-elastic deformations in the FP
arms will begin at the end of the first year and be completed by the end of the second year.
These efforts will depend to some extent upon our colleagues at Caltech incorporating thermoelastic effects into the current finite element optical codes.
Our efforts at modeling and designing the thermal compensators will be undertaken
throughout the entire three years, although a focus on these efforts will not occur into earlier
tasks are finished. During the first year with the help of considerable input form the Caltech
group thermal compensation schematics of the layout and components of compensation systems
shall be formulated based on the ring, scanning laser and other approaches. There will be some
computer and analytical modeling of thermal effects during this period, which will involve a
study of the performance and relative merits of the different compensation schemes.
Modeling and design of the thermal compensation system will be the focus of the second and
third year. Data from the various test sites such as MIT LASTI, Gingin, and the H4K
compensation system will be used as input to our efforts. A choice will be made of the design
scheme and its major elements by the end of the second year. The third year will focus on the
formulation of a detailed final design for the thermal compensation system. The third year will
also involve detailed studies of the performance of GW and modulation (RF) sidebands as well
as A-LIGO in general in the context of the newly designed thermal compensation system.
Our efforts on the blrms seismic (figure of merit) monitor software will continue throughout
all three years. We will continue to modify and upgrade the software as needed by the LSC. We
have already added time marking of data loss segments, a technique that was tested before and
during the E11 engineering runs. In the near future we plan to eliminate or mark minute trends
with elevated seismic signals due to filter ring-down. In the future additional DMT channels may
be monitored and modifications to the IIR filters may be made as needed by the LSC.
Dr. Wiley has contributed significantly to FFT computations and to analytical models that we
have presented at LSC meetings38-39. Ganezer and Wiley are members of the LSC Core Optics
and Coatings and Laser and Electro-Optics working groups. Ganezer is a member of the Burst
Source data analysis and detector characterization group, although not directly involved in burst
analysis. The CSUDH LIGO subgroup has contributed in the past to attempts to correlate GW
signals with neutrino bursts40-42.
This proposal includes a request for faculty travel to attend LSC meetings and to
participate in scientific monitoring shifts that are required of all LSC members and attendance at
and participation in LSC meetings, which now number four per year. The shift work is to support
the overall LIGO-I effort in achieving high detector sensitivity and high data quality. Each
LIGO-I group is expected to assist in the staffing of scientific monitoring shifts during organized
data runs. The staffing of these shifts is notable for both its importance and the travel burden it
places on scientists. The quota is based upon the FTE fraction devoted to LIGO-I. For CSUDH
with 2 FTEs for LIGO-I this amounts to up to 24 work-shifts per year in the upcoming three
years (assuming a maximum of 8 months per year of data runs).
Broader Impact of the Proposed Activities
Prior to 1990, there had been no sustained research effort in the CSUDH physics
department for many years. Since that time, we have developed a research group in particle and
nuclear physics, particle-astrophysics, and biomedical applications of physics that presently
includes two regular faculty members and two postdoctoral scholars.
CSUDH is a state institution with 8850 on-campus full time equivalent students (FTES).
Default teaching loads are 12 units per semester, a relatively high instructional commitment. Our
12-unit teaching load is equivalent to 4 three-hour lectures or six three-hour laboratory courses.
Currently the Biology Department has the only graduate program in the natural sciences. At
present there are four full-time physics faculty members including, Dr. Kenneth S. Ganezer
(Professor and Chair), Dr. James E. Hill (Assistant Professor), Dr James Imai (Professor) and Dr.
Alice Newman (Professor). We are currently recruiting for a new tenure track faculty member to
fill the position vacated earlier this year by Dr. Brendan Crill, an experimental cosmologist who
left after two years on the CSUDH faculty to become a staff scientist at Caltech (IPAC).
As a result of external funding, we have had two postdoctoral scholars, Dr. Miodrag
Krmar who worked on our NIH funded research in biomedical physics from April 2002 – May
2004, and Dr. Alberto Gago who worked on our NSF funded research in particle physics from
September 2001 – August 2002. Currently, we are recruiting two new postdoctoral scholars in
particle and biomedical physics respectively.
Our research has benefited the department and institution greatly. It has helped to
increase the number of physics majors at CSUDH from only eight in 1998 to 14 at present,
helped to justify the recent hiring (in 2002) of one new faculty member (Dr. Hill) and the ongoing tenure track faculty recruitment, and has improved the infrastructure and institutional
support for research at CSUDH. With the addition in 2002 of Dr. Hill, an experimental
elementary particle physicist, the physics department had established a significant effort in
particle astrophysics that includes gravity waves (LIGO), cosmic rays (CHICOS), and
accelerator based neutrino physics (Super-K, K2K, JPARC-SK). Support for this proposal will
help to further our efforts in particle-astrophysics and will help us to reach a critical mass of
researchers and research programs. The two investigators on this proposal have worked for more
than four years to establish CSUDH as the only public institution in California in the LSC, in
spite of high teaching loads, minimal state and institutional support, and an on-going state budget
crisis that has reduced total enrollment at CSUDH by 10%.
Dr. Ganezer heads a NIH funded project to develop new medical imaging and other
diagnostic technology as well as biophysical models for bone, involving human subjects at
nearby Harbor-UCLA Medical Center. Through these efforts the research infrastructure at
CSUDH has grown to include two full time research physicists, computing support for research,
and efforts to establish a machine shop.
Dr. Ganezer has received NSF funding for research in particle physics since 1992 and
NIH funding for research in biomedical physics since 1998. From 1993-1996 the physics
department had a NSF ILI award to partly equip an instructional advanced laboratory in nuclear
and particle physics and a modern physics laboratory for physics majors that were motivated in
part by our particle physics research46. This advanced laboratory has been taught for three of the
last four years and the modern physics laboratory taught for about 5 out of 10 years using the
equipment from this grant. An application for an MS in physics degree program has been
circulated to our administration that is justified in part by our strengths in research. This
semester, a concentration within the CSUDH physics major in electrical engineering (EE), is
being established. An agreement has been signed with CSU Fullerton (CSUF) in which students
in the EE concentration would take 58 units at CSUDH and 14 units at CSUF to complete their
CSUDH Physics BS (with an EE concentration) and thereby qualify for admission to an MS in
EE at CSUF.
There are many educational spin-offs from our research including the availability of liquid
nitrogen (LN2), x-ray sources and solid state (HPGe, CdTe, and NaI) detectors, state of the art
digitizing oscilloscopes, software such as MATLAB and LABVIEW, and LINUX/ UNIX based
computing. Over the past two years, a laboratory for LINUX-based computing was established in
the physics department for student as well as faculty research.
In July 2003, we obtained funding from the NIH for a Beowulf-type LINUX cluster for
the departments of Chemistry and Physics and a device for high-resolution non-contact
ultrasound imaging. We hope to use the Beowulf cluster in the optical simulations proposed here.
During the eighteen-year period from 1986 to 2004, 42 Physics BS or BA degrees were
awarded by CSUDH. Funding for physics research has helped to keep the numbers of physics
majors and BS degrees higher than it would otherwise be, and has improved the quality of
education in the physics department. This is evidenced by several recent manuscripts and
presentations47-63 by our research group that involved student authors or student participation in
our funded research.
A large proportion of current physics majors are under-represented minorities, 62.5%
total, with 50% Hispanic American and 12.5% African American in 2001. Our campus
enrollment includes 63.3% females. The ethnic distribution of undergraduate and graduate
students at CSUDH is 31 % Hispanic American, 30% African American, 25% Caucasian
American, and 12 % Asian and Pacific Islander American. We supervised a physics MS student,
an African American male, from our sister institution CSU Long Beach43 with a thesis based on
our particle physics research, and two MS Biology students from CSUDH on theses with our
Medical Physics research, one an Asian American male44 and one an Hispanic-American
female45.
In Table-1 below we summarize the educational or vocational pursuits of our alumni,
directly after graduation to the best of our knowledge, for the past 18 years from 1986-2004. We
have been successful in placing and encouraging our students to pursue graduate degrees. Most
go on to graduate programs in physics, math, engineering, or related fields (45%) or to
technology related positions in private industry (47%). A much smaller, but significant
proportion of our students (8%), take jobs in teaching (8%) at the K-12 or college level, with
most finding positions at the high school level.
Table-1 – Placement Categories for Physics Students from 1986-1987 through 2003-2004
Placement Category
Industry
Graduate School
K-12/College
Teaching
TOTAL
Number
18
17
3
38
Percentage (%)
47.4
44.7
7.9
100
These proportions have remained somewhat constant over the past five years, with about 45% of
our graduates pursuing positions in industry, about 45% going on to graduate studies in physics
related fields, and about 10% taking jobs in K-12 education.
Literature Cited
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Gravitational Wave Bursts”, Phys. Rev. D, 102001, 1-21, May (2004), also
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of Periodic Gravitational Waves from PSR J1939 + 2134 Using the First Science Data from the
GEO 600 and LIGO Detectors”, Phys. Rev. D, 69, 082004, 1-16, April (2004) and grqc/0308050.
12. The LIGO Scientific Collaboration (B. Abbott et al.), “Detector Description and Performance
for the First Coincidence Observations between LIGO and GEO”, Nuclear Instruments and
Methods in Physics Res., A 517, 154-179, March (2004), and gr-qc/0308043
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Emission from Selected Pulsars Using LIGO Data”, submitted to Physical Review Letters, and
gr-qc/0410007, October 2004, (2004).
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Realistically Imperfect Optics”, Gen. Rel. Grav., 35, 1029-1057, and astro-ph/0306133, June
(2003).
22. R. Lawrence and D. Ottaway, “Thermal Compensation Update”, LIGO G020502-00-R,
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23. R. Lawrence, “A Thermo-Mechanical Core Optic Finite Element Model”, LIGO T02000100-R, March 2002, (2002).
24. R. Lawrence, M. Zucker, P. Fritschel, P. Marfuta, and D. Shoemaker, “Adaptive Thermal
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25. R. G. Beausoleil, MELODY/MATLAB Object-Oriented Model of Gravitational-Wave
Interferometers using MATLAB, LIGO G010301-00-Z, (2001).
26. V. B. Braginsky, S. E. Stringin, and S. P. Vyatchanin, “ Parametric Oscillatory Instability in
a Fabry-Perot (FP) Interferometer”, gr-qc/0107079 v2, (2001).
27. V. B. Braginsky, E. d’Ambrosio, R. O’Shaughnessy, S. E. Strigin, K. Thorne, and S. P.
Vyatchanin, “ Reducing Thermoelastic Noise by Reshaping the Light Beams and Test Masses”,
Proceedings of the 7th LSC Meeting, Baton Rouge LA, March 2001, LIGO G010151-00-R,
http://www.ligo.caltech.edu, (2001).
28. E. d’Ambrosio, “Study of the Behavior of an Interferometer with Non-Spherical Mirrors,
Proceedings of the 8th LSC Meeting, Hanford WA, August 2001, LIGO G010297-00-D,
http://www.ligo.caltech.edu, (2001).
29. E D’ Ambrosio and W. Kells, “Considerations on Parametric Instability in Fabry-Perot
Interferometer “, LIGO P020025-00-D, February 2002.
30. E. D’ Ambrosio, W. Kells, and S. P. Vyachanin, “Recommendations on the Program of
Researches on the Parametric Oscillatory Instability in Power Recycled LIGO Interferometer”,
LIGO T020194-00-D, December, 2002.
31. W. Winkler, K. Danzmann, A. Rüdiger, and R. Schilling, “Heating by Optical Absorption
and the Performance of Interferometric Gravitational-Wave Detectors”, Physical Review A, 44
(11), 7022-7036, December (1991).
32. D. Ottaway, K. Mason, S. Ballmer, C. Vorick, G. Moreno, and D. Sigg, “Thermal
Compensation at LHO” , LIGO-G040172-00-Z, March 2004 LSC meeting, retrieved from
http://www.ligo.caltech.edu/docs/G/G040172-00/G040172-00.ppt#1.
33. R. Lawrence and D. Ottaway, “Thermal Compensation Update”, LIGO-G020502-00-R,
October (2002).
34. R. C. Lawrence, “Active Wavefront Correction in Laser Interferometric Gravitational Wave
Detectors”, PhD thesis (MIT), LIGO-P030001-00-R, February (2003).
35. W. P. Kells, “The Thermal Lens in LIGO-I”, LIGO-G030021-00-D, talk at the Aspen Winter
Conference on Gravitational Waves and GWADW, February 2003 (2003).
36. E. D’Ambrosio, “My Personal Interpretation of Thermal Lensing, LIGO T030047-00-D,
March (2003).
37. E. J. Daw, J. A. Giame, D. Lormand, M. Lubinski, and J. Zweizig, “ Long Term Study of the
Seismic Environment at LIGO”, Classical and Quantum Gravity, 21, (2004), 2255-2273, and grqc 0403046, (2004).
38. K. Ganezer, G. Jennings and S. Wiley, “First DR FFT Results on Advanced LIGO Using
Perfect and Imperfect Optics”, LIGO G020086-00-Z, talk by K. Ganezer at the LSC meeting
March 20-23 2002 at Livingston LA, March 2002.
39. K. Ganezer, G. Jennings, and S. Wiley, “New FFT Simulations for Advanced LIGO and the
40m ”, LIGO G020353-00-Z, talk by K. Ganezer at the August 2002 LSC meeting at Hanford
LIGO Observatory, 2002.
40. B. Barish, K. Ganezer, A. Lazzarini, S. Marka, B. Mours, P. Saulson, and J. Zweizig,
Proposal to the LSC for Entry of LIGO into the Supernova Early Warning System (SNEWS) and
Prototype Development of A Real Time LIGO Supernova Alert, LIGO G000313-00-D, (2000).
41. K. Scholberg, SNEWS: The Supernova Early Warning System, preprint astro-ph/9911359,
Nov. 1999. A. Habig, SNEWS: A Neutrino Early Warning System for Galactic SN II, Dec. 1999.
The SNEWS web page, http://hep.bu.edu/~snnet, (1999).
42. K. Ganezer, “Update on Neutrino/ Gravity Wave Correlations with a Focus on SNEWS/
LIGO-I”, LIGO G020354-00-Z, talk at the August 2002 LSC meeting at Hanford LIGO
Observatory, August 2002.
43. M. D. Campbell, M. S. in Physics thesis CSU Long Beach, “Measurement of Beryllium-11
Production Due to Spallation of Oxygen-16 Nuclei in Super-Kamiokande”, unpublished. August
1999, (1999).
44. J. N. Yano, “Correlation Analysis of the Speed and Attenuation of Ultrasonic Pulses with
Physical and Radiological Parameters as an Assessment for Bone Strength and Quality”, M. S.
thesis, CSU, Dominguez Hills, Spring 1997, University Microfilms, Ann Arbor, Michigan, UMI
number 1384243, (1997).
45. K. L. Hurst, “Ultrasound Analysis of Cortical Bone Model: New Method for Early Detection
of Osteoporosis,” MS thesis, CSU Dominguez Hills, summer 2003, University Microfilms, Ann
Arbor Michigan, (2003).
46. K. S. Ganezer, W. E. Keig, and A. F. Shor, "A Simple High Efficiency Cherenkov Counter",
IEEE Transactions on Nuclear Science, 41, 336-342, (1994).
47. K. Ganezer, K. Mack, and A. Gago, “A New Super-K Neutron-Antineutron Oscillation
Analysis”, Super-Kamiokande Collaboration Meeting, Kailua Hawaii, October 2001.
48. A. Gago, K. Ganezer, and K. Mack, “Neutron-Antineutron Oscillation results from SuperK”, Super-Kamiokande Collaboration Meeting, Toyama Japan, April 2002.
49. K. Ganezer, “Searches for Neutron Antineutron Oscillations at Super-Kamiokande”,
http://www.iucf.indiana.edu/Seminars/NNBAR/program.php, talk at International Workshop on
Neutron-Antineutron Search with Ultracold Neutrons at Indiana University Cyclotron Facility,
Bloomington Indiana, September 2002.
50. K. Ganezer, K. Hurst, S. Shukla, R. Sinow, and M. Bhardwaj, “Initial Studies of NonContact Ultrasound for Osteoporosis and Bone Imaging,” American Association of Physicists in
Medicine (AAPM) 44th Annual Meeting, Oral Presentation MO-D-519-3, Montreal Quebec,
Canada, July 2002, and Medical Physics, 29 (6), 1292, June 2002.
51. K. Ganezer, K. Hurst, M. Krmar, S. Shukla, and C. Tran, “ A New Thomson (Coherent) to
Compton Scattering System for Bone Assessment and Imaging”, American Association of
Physicists in Medicine (AAPM) 44th Annual Meeting, (Works in Progress) Poster Presentation
SU-GG-WIP-EXH-11, Montreal Quebec, Canada, July 2002.
52. M. Krmar (CSUDH), G. Pantelic, and Z. Djurcic, “ Endpoint Energy of Therapy
Accelerators: Determination and Control by Activation Technique”, American Association of
Physicists in Medicine (AAPM) 44th Annual Meeting, Poster Presentation SU-DD-EXH-09,
Montreal Quebec, Canada, July 2002, Medical Physics, 29 (6), 1200, July 2002.
53. M. Krmar, K. Ganezer, and S. Shukla, “ How to avoid the limitations of DEXA: The
introduction of x-ray spectroscopy in diagnostic absorptiometry”, Abstract Submitted to the
American Association of Physicists in Medicine (AAPM) 45th Annual Meeting, August 2003 in
San Diego, CA, Oral Presentation TU-C25A-08, Medical Physics, 30 (6), 1391, June (2003)
54. M. Krmar, K. Ganezer, and S. Shukla, “A new radiological method for the determination of
trabecular bone mineral density (TBMD) in-vivo”, Abstract Submitted to the American
Association of Physicists in Medicine (AAPM) 45th Annual Meeting, August 2003,in San Diego,
CA, Poster Presentation PO-I-21, Medical Physics, 30 (6), 1463, June (2003).
55. K. Ganezer, K. Hurst, M. Krmar, and S. Shukla “Ultrasound Attenuation, Attenuation
Spectra, and Speed in Cortical Bone; New Measurements and Models”, Abstract Submitted to
the American Association of Physicists in Medicine (AAPM) 45th Annual Meeting, August 2003
in San Diego CA, Oral Presentation MO-D23A-3, Medical Physics, 30 (6), 1366, June (2003).
56.M. Krmar, S. Shukla, P. Kristonovic, and K. Ganezer, “Bone Densitometry Using X-ray
Spectra”, Medical Physics manuscript 03-261, June 2003, currently under revision for
resubmission to Medical Physics.
57. M. Krmar, S. Shukla, and K. Ganezer, “Using CdTe for End-Point Energy Determination in
Diagnostic Radiology”, Medical Physics manuscript 03-298, July 2003, currently under revision
for resubmission to Medical Physics.
58. K. Ganezer, K. Hurst, M. Krmar, and S. Shukla, “Quantitative Ultrasound in Cortical Bone”,
to be submitted to Medical Physics, October, 2003.
59. R. D. McKeown, J. Gao, M. B. Larson, C. Zheng, R. Seki,
A. Shoup, G. B. Yodh, C. Jillings, K. Ganezer, J. Hill, W. E. Keig, and J. Sepikas (Caltech,
Kellogg Lab & Cal State, Northridge & UC, Irvine & Cal State, Dominguez Hills), “CHICOS:
Status and Prospects”, Proceedings of the International Cosmic Ray Conference 2003, Kyoto,
Japan, July 31 2003 – 7 August 2003, Edited by T. Kajita, Y. Asaoka, A. Kawachi, Y.
Matsubara, M. Sasaki. Tokyo, Univ. Acad. Pr., Frontiers in Science series, 41, 493-496, (2003).
60. M. Krmar, K. Ganezer, G. Pantelić, P. Krstonošić*, “The Endpoint Energy for Medical
Linear Accelerators used in Radiation Therapy”, accepted for publication in Nuclear
Instruments and Methods in Physics Research A, 532/533, 533-537, October (2004).
61. M. Krmar, S. Shukla, and K. Ganezer, “New Possibilities for the CCSR Technique”, Oral
presentation at the 46th Annual AAPM Meeting, July 2004 in Pittsburg PA , and Medical
Physics, 31 (6), 1748, June (2004).
62. M. Krmar, S. Shukla, and K. Ganezer, “Bone Densitometry Using X-ray Spectra”, Oral
presentation at the 46th Annual AAPM Meeting, July 2004 in Pittsburg PA, Medical Physics, 31
(6), 1747, June (2004).
63. K. Ganezer, K. Hurst, M. Krmar, D. Nunez*, and S. Shukla “Contact and Air-Coupled (NonContact) Ultrasonic Attenuation and Speed for Quantitative Measurements and Imaging of Bone
In-Vivo”, Oral presentation at the 46th Annual AAPM Meeting, July 2004 in Pittsburg PA, Oral
Presentation, Medical Physics, 31 (6), 1747, June (2004).
64. D. Rietze, “Test Mass Substrate Material Selection for Advanced LIGO: An Update from the
Optics Working Group”, talk by D. Reitze at the August 2004 LSC meeting at Hanford LIGO
Observatory, 2005, LIGO G040321-00-R, retrieved from
http://www.ligo.caltech.edu/docs/G/G040321-00/G040321-00.pdf, (2004).
65. The LIGO Scientific Collaboration (B. Abbott et al.), “The Advanced LIGO Proposal”,
LIGO M030023-00M.
Kenneth S. Ganezer
Professor of Physics, Department of Physics
California State University, Dominguez Hills
1000 East Victoria Street, Carson, CA 90747
(310) 243-3438, FAX (310) 243-2593
[email protected]
___________________________________________________________
EDUCATION
University of California, Berkeley, B.A., Mathematics, June 1974
University of California, Los Angeles, M.S., Physics, June 1976
University of California, Los Angeles, Ph.D., Physics, March 1983
APPOINTMENTS
2001-present Professor, Physics, California State University, Dominguez Hills
1995-2001: Associate Professor, Physics, California State University, Dominguez Hills
1990-1995: Assistant Professor, Physics, California State University, Dominguez Hills
1987-1990:
Senior Physicist, Pacific Sierra Research Corporation, Los Angeles, Ca.
1986-1987:
Member of the Research Staff, Arete Associates, Sherman Oaks, Ca.
1986:
Postdoctoral Scholar, UCLA, Department of Radiological Sciences
1983-1986:
Assistant Research Physicist, University of California, Irvine
1983:
Adjunct Assistant Professor and Assistant Research Physicist, UCLA
RELATED PUBLICATIONS
The LIGO Scientific Collaboration (B. Abbott et al), “Analysis of LIGO Data for
Stochastic Gravitational Waves”, FERMILAB-PUB-03-416, gr-qc/0312088, Physical
Review D (Phys. Rev. D), 69, 122001, 1-24, June (2004).
The LIGO Scientific Collaboration (B. Abbott et Al.), “Analysis of LIGO Data for
Gravitational Waves from Binary Neutron Stars”, gr-qc/0308069, Physical Review D, 69,
122001, 1-16, June (2004).
The LIGO Scientific Collaboration (B. Abbott et al.), “First Upper Limits from LIGO on
Gravitational Wave Bursts”, Phys. Rev. D, 102001, 1-21, May (2004), also
Class.Quant.Grav.21:S677-S684, (2004), and gr-qc/0312056 (e-print archive at
xxx.lanl.gov).
The LIGO Scientific Collaboration (B. Abbott et Al.), “Setting Upper Limits on the
Strength of Periodic Gravitational Waves from PSR J1939 + 2134 Using the First
Science Data from the GEO 600 and LIGO Detectors”, Phys. Rev. D, 69, 082004, 1-16,
April (2004) and gr-qc/0308050.
The LIGO Scientific Collaboration (B. Abbott et al.), “Detector Description and
Performance for the First Coincidence Observations Between LIGO and GEO”, Nuclear
Instruments and Methods in Physics Res., A 517, 154-179, March (2004), and grqc/0308043.
OTHER SIGNIFICANT (CLOSELY RELATED) PUBLICATIONS
Super-Kamiokande Collaboration (Y. Ashie et al.), “Evidence for an Oscillatory
Signature in Atmospheric Neutrino Oscillation”,Physical Review Letters, 93,
101801,September (2004), also hep-ex/0404034.
The Super Kamiokande Collaboration (D. W. Liu et al.), Limits on The Neutrino
Magnetic Moment Using 1496 Days of Super-Kamiokande-I Solar Neutrino Data, Phys.
Rev. Lett., 93, 021802, and hep-ex/0402015, (2004).
Super-Kamiokande Collaboration (S. Desai et al.), “Search for dark matter WIMPs using
upward through-going muons in Super-Kamiokande”, Accepted for publication Phys.
Rev. D, September (2004), also hep-ex/0404025.
Super-Kamiokande Collaboration (M. Smy et al.), “Precise Measurement of the Solar
Neutrino Day/Night and Seasonal Variation in Super-Kamiokande I”, submitted to Phys.
Rev. D Rapid Communications (hep-ex/030911), September 2003.
Super-Kamiokande Collaboration (M. Smy et al.), “Precise Measurement of the Solar
Neutrino Day/Night and Seasonal Variation in Super-Kamiokande-I”, Phys. Rev. D
Rapid Communications, 011104, also hep-ex/030911, September (2003).
Super-Kamiokande Collaboration (J. Yoo et al.), “A Search for Periodic Modulations of
the Solar Neutrino Flux in Super-Kamiokande-I”, Phys. Rev. D, 68,092002, (2003), also
hep-ex/0307070.
The Super-Kamiokande Collaboration (Y. Gando et al.), “Search for anti-electron
neutrinos from the sun at Super-Kamiokande I”, Physical Review, Letters, 90, 171302,
hep-ex/0212067, March (2003).
The Super-Kamiokande Collaboration (M. Malek et al.), "Search for Supernova Relic
Neutrinos at Super-Kamiokande", by the Super-Kamiokande Collaboration, Physical
Review Letters, 90 (6), 061101-1 – 061101-6, hep-ex/0209028, February (2003).
R. Bionta et. Al., “Observation of a Neutrino Burst in Coincidence with Supernova
1987A in the Large Magellanic Cloud,” Phys. Rev. Lett., 58, 1494-1496, (1987)
K.S. Ganezer, “The Consistency of the Constraint and Transformation Algebras in
Supergravity Theory”, Nucl. Phys. B, 176, 216-220, (1980)
GRADUATE AND POST-GRADUATE ADVISORS
Graduate Student and Postdoctoral Advisors (respectively): George Igo, UCLA,
Frederick Reines, University of California, Irvine, and Moses Greenfield, UCLA.
POSTDOCTORAL ADVISEES
Alberto M. Gago, California State University, Dominguez Hills (Particle Physics)
Miodrag Krmar, California State University Dominguez Hills (Medical Physics)
GRADUATE ADVISEES
Mel Campbell, California State University, Long Beach.
Keyvan Benham, California State University, Dominguez Hills.
Craig Harmon, California State University, Long Beach.
James Yano, California State University, Dominguez Hills.
Katherine Hurst, California State University, Dominguez Hills
LONG TERM COLLABORATORS
W. Kropp, H. Sobel, D. Kielszewska, M. Vagins, M. Smy, D. Casper, University of California
Irvine, A. Weinstein, B. Barish, S. Marka, W. Kells, E. d’Ambrosio, P. Willems CalTech, J.
Learned, S. Matsuno University of Hawaii, L. Sulak, E. Kearns Boston University, J. Hill, M.
Krmar, W. Keig, G. Jennings, S. Willey California State University, Dominguez Hills.
Sam L. Wiley
Professor of Physics, Emeritus
Department of Physics
California State University, Dominguez Hills
1000 East Victoria Street
Carson, CA 90747
(310) 243-3438, FAX (310) 243-2593
[email protected]
___________________________________________________________
EDUCATION
B.S. Physics and Mathematics, Capital University, (With Honors) 1959.
Ph.D. Physics, The Ohio State University, 1968.
APPOINTMENTS
1997-Present
1993-1997
1990-1993
1979-1990
1978-1979
1973-1978
1976-1997
1972-1976
1968-1972
1964-1967
Professor (Emeritus), Physics Department, California State University, Dominguez Hills
Vice President, Academic Affairs, California State University, Dominguez Hills
Associate Vice President, California State University, Dominguez Hills
Dean, School of Science, Mathematics and Technology, California State University,
Dominguez Hills
Director, Computer Center, California State University, Dominguez Hills
Chair, Physics Department, California State University, Dominguez Hills
Professor, Physics Department, California State University, Dominguez Hills
Associate Professor, California State University, Dominguez Hills
Assistant Professor, California State University, Dominguez Hills
Instructor, Physics Department, Capital University
RELATED PUBLICATIONS
1. K. Ganezer, G. Jennings and S. Wiley, “First DR FFT Results on Advanced
LIGO Using Perfect and Imperfect Optics”, LIGO G020086-00-Z, talk by K.
Ganezer at the LSC meeting March 20-23 2002 at Livingston LA, March
2002.
2. K. Ganezer, G. Jennings, and S. Wiley, “New FFT Simulations for Advanced
LIGO and the 40m ”, LIGO G020353-00-Z, talk by K. Ganezer at the August
2002 LSC meeting in Hanford WA, 2002.
3.
The LIGO Scientific Collaboration (B. Abbott et al.), “Limits on
Gravitational Wave Emission from Selected Pulsars Using LIGO Data”,
submitted to Physical Review Letters, and gr-qc/0410007, October 2004,
(2004).
4.
The LIGO Scientific Collaboration (B. Abbott et al.), “Upper Limits on
Gravitational Wave Bursts in LIGO’s Second Science Run”, to be submitted
to Physical Review D, and LIGO-P040040-00-R, October 2004, (2004)
COLLABORATORS
K. Ganezer, and G. Jennings, California State University, Dominguez Hills.
GRADUATE AND POST-GRADUATE ADVISORS
Dr. Chin-Ping Yang, Professor of Physics (emeritus), The Ohio State University.
SUMMARY
YEAR 1
PROPOSAL BUDGET
FOR NSF USE ONLY
PROPOSAL NO.
DURATION (months)
Proposed Granted
AWARD NO.
ORGANIZATION
California State University-Dominguez Hills
PRINCIPAL INVESTIGATOR / PROJECT DIRECTOR
Kenneth S Ganezer
A. SENIOR PERSONNEL: PI/PD, Co-PI’s, Faculty and Other Senior Associates
(List each separately with title, A.7. show number in brackets)
NSF Funded
Person-months
CAL
ACAD
1. Kenneth S Ganezer - Professor
0.00 0.00
2. Sam L Wiley - Professor
0.00 0.00
3.
4.
5.
6. ( 0 ) OTHERS (LIST INDIVIDUALLY ON BUDGET JUSTIFICATION PAGE)
0.00 0.00
7. ( 2 ) TOTAL SENIOR PERSONNEL (1 - 6)
0.00 0.00
B. OTHER PERSONNEL (SHOW NUMBERS IN BRACKETS)
1. ( 0 ) POST DOCTORAL ASSOCIATES
0.00 0.00
2. ( 0 ) OTHER PROFESSIONALS (TECHNICIAN, PROGRAMMER, ETC.)
0.00 0.00
3. ( 0 ) GRADUATE STUDENTS
4. ( 2 ) UNDERGRADUATE STUDENTS
5. ( 0 ) SECRETARIAL - CLERICAL (IF CHARGED DIRECTLY)
6. ( 0 ) OTHER
TOTAL SALARIES AND WAGES (A + B)
C. FRINGE BENEFITS (IF CHARGED AS DIRECT COSTS)
TOTAL SALARIES, WAGES AND FRINGE BENEFITS (A + B + C)
D. EQUIPMENT (LIST ITEM AND DOLLAR AMOUNT FOR EACH ITEM EXCEEDING $5,000.)
TOTAL EQUIPMENT
E. TRAVEL
1. DOMESTIC (INCL. CANADA, MEXICO AND U.S. POSSESSIONS)
2. FOREIGN
F. PARTICIPANT SUPPORT COSTS
0
1. STIPENDS
$
0
2. TRAVEL
0
3. SUBSISTENCE
0
4. OTHER
TOTAL NUMBER OF PARTICIPANTS
(
0)
G. OTHER DIRECT COSTS
1. MATERIALS AND SUPPLIES
2. PUBLICATION COSTS/DOCUMENTATION/DISSEMINATION
3. CONSULTANT SERVICES
4. COMPUTER SERVICES
5. SUBAWARDS
6. OTHER
TOTAL OTHER DIRECT COSTS
H. TOTAL DIRECT COSTS (A THROUGH G)
I. INDIRECT COSTS (F&A)(SPECIFY RATE AND BASE)
TOTAL PARTICIPANT COSTS
SUMR
1.00 $
1.00
Funds
Requested By
proposer
Funds
granted by NSF
(if different)
9,163 $
2,086
0.00
2.00
0
11,249
0.00
0.00
0
0
0
13,500
0
0
24,749
3,217
27,966
0
15,383
0
0
2,000
0
0
0
0
0
2,000
45,349
MTDC (Rate: 38.0000, Base: 45349)
TOTAL INDIRECT COSTS (F&A)
17,233
J. TOTAL DIRECT AND INDIRECT COSTS (H + I)
62,582
K. RESIDUAL FUNDS (IF FOR FURTHER SUPPORT OF CURRENT PROJECTS SEE GPG II.C.6.j.)
0
L. AMOUNT OF THIS REQUEST (J) OR (J MINUS K)
$
62,582 $
M. COST SHARING PROPOSED LEVEL $
AGREED LEVEL IF DIFFERENT $
Not Shown
PI/PD NAME
FOR NSF USE ONLY
INDIRECT COST RATE VERIFICATION
Kenneth S Ganezer
Date Checked
Date Of Rate Sheet
Initials - ORG
ORG. REP. NAME*
Raymond Riznyk
1 *ELECTRONIC SIGNATURES REQUIRED FOR REVISED BUDGET
SUMMARY
YEAR 2
PROPOSAL BUDGET
FOR NSF USE ONLY
PROPOSAL NO.
DURATION (months)
Proposed Granted
AWARD NO.
ORGANIZATION
California State University-Dominguez Hills
PRINCIPAL INVESTIGATOR / PROJECT DIRECTOR
Kenneth S Ganezer
A. SENIOR PERSONNEL: PI/PD, Co-PI’s, Faculty and Other Senior Associates
(List each separately with title, A.7. show number in brackets)
NSF Funded
Person-months
CAL
ACAD
1. Kenneth S Ganezer - Professor
0.00 0.00
2. Sam L Wiley - Professor.
0.00 0.00
3.
4.
5.
6. ( 0 ) OTHERS (LIST INDIVIDUALLY ON BUDGET JUSTIFICATION PAGE)
0.00 0.00
7. ( 2 ) TOTAL SENIOR PERSONNEL (1 - 6)
0.00 0.00
B. OTHER PERSONNEL (SHOW NUMBERS IN BRACKETS)
1. ( 0 ) POST DOCTORAL ASSOCIATES
0.00 0.00
2. ( 0 ) OTHER PROFESSIONALS (TECHNICIAN, PROGRAMMER, ETC.)
0.00 0.00
3. ( 0 ) GRADUATE STUDENTS
4. ( 2 ) UNDERGRADUATE STUDENTS
5. ( 0 ) SECRETARIAL - CLERICAL (IF CHARGED DIRECTLY)
6. ( 0 ) OTHER
TOTAL SALARIES AND WAGES (A + B)
C. FRINGE BENEFITS (IF CHARGED AS DIRECT COSTS)
TOTAL SALARIES, WAGES AND FRINGE BENEFITS (A + B + C)
D. EQUIPMENT (LIST ITEM AND DOLLAR AMOUNT FOR EACH ITEM EXCEEDING $5,000.)
TOTAL EQUIPMENT
E. TRAVEL
1. DOMESTIC (INCL. CANADA, MEXICO AND U.S. POSSESSIONS)
2. FOREIGN
F. PARTICIPANT SUPPORT COSTS
0
1. STIPENDS
$
0
2. TRAVEL
0
3. SUBSISTENCE
0
4. OTHER
TOTAL NUMBER OF PARTICIPANTS
(
0)
G. OTHER DIRECT COSTS
1. MATERIALS AND SUPPLIES
2. PUBLICATION COSTS/DOCUMENTATION/DISSEMINATION
3. CONSULTANT SERVICES
4. COMPUTER SERVICES
5. SUBAWARDS
6. OTHER
TOTAL OTHER DIRECT COSTS
H. TOTAL DIRECT COSTS (A THROUGH G)
I. INDIRECT COSTS (F&A)(SPECIFY RATE AND BASE)
TOTAL PARTICIPANT COSTS
SUMR
1.00 $
1.00
Funds
Requested By
proposer
Funds
granted by NSF
(if different)
9,438 $
2,149
0.00
2.00
0
11,587
0.00
0.00
0
0
0
13,500
0
0
25,087
3,261
28,348
0
15,383
0
0
2,000
0
0
0
0
0
2,000
45,731
MTDC (Rate: 38.0000, Base: 45731)
TOTAL INDIRECT COSTS (F&A)
17,378
J. TOTAL DIRECT AND INDIRECT COSTS (H + I)
63,109
K. RESIDUAL FUNDS (IF FOR FURTHER SUPPORT OF CURRENT PROJECTS SEE GPG II.C.6.j.)
0
L. AMOUNT OF THIS REQUEST (J) OR (J MINUS K)
$
63,109 $
M. COST SHARING PROPOSED LEVEL $
AGREED LEVEL IF DIFFERENT $
Not Shown
PI/PD NAME
FOR NSF USE ONLY
INDIRECT COST RATE VERIFICATION
Kenneth S Ganezer
Date Checked
Date Of Rate Sheet
Initials - ORG
ORG. REP. NAME*
Raymond Riznyk
2 *ELECTRONIC SIGNATURES REQUIRED FOR REVISED BUDGET
SUMMARY
YEAR 3
PROPOSAL BUDGET
FOR NSF USE ONLY
PROPOSAL NO.
DURATION (months)
Proposed Granted
AWARD NO.
ORGANIZATION
California State University-Dominguez Hills
PRINCIPAL INVESTIGATOR / PROJECT DIRECTOR
Kenneth S Ganezer
A. SENIOR PERSONNEL: PI/PD, Co-PI’s, Faculty and Other Senior Associates
(List each separately with title, A.7. show number in brackets)
NSF Funded
Person-months
CAL
ACAD
1. Kenneth S Ganezer - Professor
0.00 0.00
2. Sam L Wiley - Professor
0.00 0.00
3.
4.
5.
6. ( 0 ) OTHERS (LIST INDIVIDUALLY ON BUDGET JUSTIFICATION PAGE)
0.00 0.00
7. ( 2 ) TOTAL SENIOR PERSONNEL (1 - 6)
0.00 0.00
B. OTHER PERSONNEL (SHOW NUMBERS IN BRACKETS)
1. ( 0 ) POST DOCTORAL ASSOCIATES
12.00 0.00
2. ( 0 ) OTHER PROFESSIONALS (TECHNICIAN, PROGRAMMER, ETC.)
0.00 0.00
3. ( 0 ) GRADUATE STUDENTS
4. ( 2 ) UNDERGRADUATE STUDENTS
5. ( 0 ) SECRETARIAL - CLERICAL (IF CHARGED DIRECTLY)
6. ( 0 ) OTHER
TOTAL SALARIES AND WAGES (A + B)
C. FRINGE BENEFITS (IF CHARGED AS DIRECT COSTS)
TOTAL SALARIES, WAGES AND FRINGE BENEFITS (A + B + C)
D. EQUIPMENT (LIST ITEM AND DOLLAR AMOUNT FOR EACH ITEM EXCEEDING $5,000.)
TOTAL EQUIPMENT
E. TRAVEL
1. DOMESTIC (INCL. CANADA, MEXICO AND U.S. POSSESSIONS)
2. FOREIGN
F. PARTICIPANT SUPPORT COSTS
0
1. STIPENDS
$
0
2. TRAVEL
0
3. SUBSISTENCE
0
4. OTHER
TOTAL NUMBER OF PARTICIPANTS
(
0)
G. OTHER DIRECT COSTS
1. MATERIALS AND SUPPLIES
2. PUBLICATION COSTS/DOCUMENTATION/DISSEMINATION
3. CONSULTANT SERVICES
4. COMPUTER SERVICES
5. SUBAWARDS
6. OTHER
TOTAL OTHER DIRECT COSTS
H. TOTAL DIRECT COSTS (A THROUGH G)
I. INDIRECT COSTS (F&A)(SPECIFY RATE AND BASE)
TOTAL PARTICIPANT COSTS
SUMR
1.00 $
1.00
Funds
Requested By
proposer
Funds
granted by NSF
(if different)
9,721 $
2,213
0.00
2.00
0
11,934
0.00
0.00
0
0
0
13,500
0
0
25,434
3,306
28,740
0
15,383
0
0
2,000
0
0
0
0
0
2,000
46,123
MTDC (Rate: 38.0000, Base: 46123)
TOTAL INDIRECT COSTS (F&A)
17,527
J. TOTAL DIRECT AND INDIRECT COSTS (H + I)
63,650
K. RESIDUAL FUNDS (IF FOR FURTHER SUPPORT OF CURRENT PROJECTS SEE GPG II.C.6.j.)
0
L. AMOUNT OF THIS REQUEST (J) OR (J MINUS K)
$
63,650 $
M. COST SHARING PROPOSED LEVEL $
AGREED LEVEL IF DIFFERENT $
Not Shown
PI/PD NAME
FOR NSF USE ONLY
INDIRECT COST RATE VERIFICATION
Kenneth S Ganezer
Date Checked
Date Of Rate Sheet
Initials - ORG
ORG. REP. NAME*
Raymond Riznyk
3 *ELECTRONIC SIGNATURES REQUIRED FOR REVISED BUDGET
SUMMARY
Cumulative
FOR NSF USE ONLY
PROPOSAL BUDGET
ORGANIZATION
PROPOSAL NO.
California State University-Dominguez Hills
PRINCIPAL INVESTIGATOR / PROJECT DIRECTOR
DURATION (months)
Proposed Granted
AWARD NO.
Kenneth S Ganezer
A. SENIOR PERSONNEL: PI/PD, Co-PI’s, Faculty and Other Senior Associates
(List each separately with title, A.7. show number in brackets)
NSF Funded
Person-months
CAL
ACAD
1. Kenneth S Ganezer - Professor
0.00 0.00
2. Sam L Wiley - Professor
0.00 0.00
3.
4.
5.
6. (
) OTHERS (LIST INDIVIDUALLY ON BUDGET JUSTIFICATION PAGE)
0.00 0.00
7. ( 2 ) TOTAL SENIOR PERSONNEL (1 - 6)
0.00 0.00
B. OTHER PERSONNEL (SHOW NUMBERS IN BRACKETS)
1. ( 0 ) POST DOCTORAL ASSOCIATES
12.00 0.00
2. ( 0 ) OTHER PROFESSIONALS (TECHNICIAN, PROGRAMMER, ETC.)
0.00 0.00
3. ( 0 ) GRADUATE STUDENTS
4. ( 6 ) UNDERGRADUATE STUDENTS
5. ( 0 ) SECRETARIAL - CLERICAL (IF CHARGED DIRECTLY)
6. ( 0 ) OTHER
TOTAL SALARIES AND WAGES (A + B)
C. FRINGE BENEFITS (IF CHARGED AS DIRECT COSTS)
TOTAL SALARIES, WAGES AND FRINGE BENEFITS (A + B + C)
D. EQUIPMENT (LIST ITEM AND DOLLAR AMOUNT FOR EACH ITEM EXCEEDING $5,000.)
TOTAL EQUIPMENT
E. TRAVEL
1. DOMESTIC (INCL. CANADA, MEXICO AND U.S. POSSESSIONS)
2. FOREIGN
F. PARTICIPANT SUPPORT COSTS
0
1. STIPENDS
$
0
2. TRAVEL
0
3. SUBSISTENCE
0
4. OTHER
TOTAL NUMBER OF PARTICIPANTS
(
0)
G. OTHER DIRECT COSTS
1. MATERIALS AND SUPPLIES
2. PUBLICATION COSTS/DOCUMENTATION/DISSEMINATION
3. CONSULTANT SERVICES
4. COMPUTER SERVICES
5. SUBAWARDS
6. OTHER
TOTAL OTHER DIRECT COSTS
H. TOTAL DIRECT COSTS (A THROUGH G)
I. INDIRECT COSTS (F&A)(SPECIFY RATE AND BASE)
TOTAL PARTICIPANT COSTS
SUMR
Funds
Requested By
proposer
Funds
granted by NSF
(if different)
3.00 $
3.00
28,322 $
6,448
0.00
6.00
0
34,770
0.00
0.00
0
0
0
40,500
0
0
75,270
9,784
85,054
0
46,149
0
0
6,000
0
0
0
0
0
6,000
137,203
TOTAL INDIRECT COSTS (F&A)
52,138
J. TOTAL DIRECT AND INDIRECT COSTS (H + I)
189,341
K. RESIDUAL FUNDS (IF FOR FURTHER SUPPORT OF CURRENT PROJECTS SEE GPG II.C.6.j.)
0
L. AMOUNT OF THIS REQUEST (J) OR (J MINUS K)
$
189,341 $
M. COST SHARING PROPOSED LEVEL $
AGREED LEVEL IF DIFFERENT $
Not Shown
PI/PD NAME
FOR NSF USE ONLY
INDIRECT COST RATE VERIFICATION
Kenneth S Ganezer
Date Checked
Date Of Rate Sheet
Initials - ORG
ORG. REP. NAME*
Raymond Riznyk
C *ELECTRONIC SIGNATURES REQUIRED FOR REVISED BUDGET
Budget Justification Page
Senior Personnel:
All salaries are based on current levels with a projected 3% increase per year.
PI Kenneth Ganezer: 1 month summer salary each year
Year 1: $9,163
Year 2: $9,438
Year 3: $9,721
Co-PI Sam Wiley: 1.0 summer month each year
Year 1: $2086
Year 2: $2149
Year 3: $2213
Other Personnel
2 undergraduate students each $9/hour for 15 hours for 50 weeks per year.
Year 1: $13,500
Year 2: $13,500
Year 3: $13,500
Fringe Benefits
Summer faculty and student employee benefits are charged as direct costs at 13% of salary
and wages.
Travel
Two (2) trips per year of 10 days each for 2 peoiple to Ligo Livingson for shiftwork.
Airfare @$415/person/trip x 2 people x 2 trips = $1,660
Car rental $300/trip x 2 trips = $600
lodging @$75/night/person x 2 people x 10 nights x 2 trips = $3,000
Per diem @$46/day/person x 2 people x 10 days x 2 trips = $1,840
Two (2) trips per year of 10 days each for 2 peoiple to Hanford, WA for shiftwork.
Airfare @$275/person/trip x 2 people x 2 trips = $1,100
Car rental $300/trip x 2 trips = $600
lodging @$75/night/person x 2 people x 10 nights x 2 trips = $3,000
Per diem @$46/day/person x 2 people x 10 days x 2 trips = $1,840
Travel for undergraduate studnets to LIGO sites (LHO & LLO) and to meetings.
Airfare @ $500 x 2 = $1,000
Per Diem @$46/day x 2 students x 4 days = $368
Lodging @$125/day (share room) x 3 days = $375
Other Direct Costs
Materials and Supplies
Paper goods and consumables @$2000/year
Current and Pending Support
(See GPG Section II.C.2.h for guidance on information to include on this form.)
The following information should be provided for each investigator and other senior personnel. Failure to provide this information may delay consideration of this proposal.
Other agencies (including NSF) to which this proposal has been/will be submitted.
Investigator: Kenneth Ganezer
Support:
Current
Pending
Submission Planned in Near Future
*Transfer of Support
Project/Proposal Title: Neutrino Mixing, Baryon Number Non-Conservation, and
Neutrino Astrophysics at SuperKamiokande and JPARC-SK
NSF
Source of Support:
Total Award Amount: $
0 Total Award Period Covered: 07/01/04 - 06/30/07
Location of Project:
California State University Dominguez Hills
Person-Months Per Year Committed to the Project. Cal:0.00
Acad: 0.00 Sumr: 1.00
Support:
Current
Pending
Submission Planned in Near Future
*Transfer of Support
Project/Proposal Title: Optical Simulations, Burst Source Analysis, and 40m
Participation by the CSUDH LIGO Subgroup
NSF
Source of Support:
Total Award Amount: $
0 Total Award Period Covered: 07/01/05 - 06/30/08
Location of Project:
California State University Dominguez Hills
Person-Months Per Year Committed to the Project. Cal:0.00
Acad: 0.00 Sumr: 1.00
Support:
Current
Pending
Submission Planned in Near Future
*Transfer of Support
Project/Proposal Title: Bone Properties and Risks from New Technologies and a
Composite Material Model
NIH
Source of Support:
Total Award Amount: $
900,000 Total Award Period Covered: 07/01/01 - 06/30/05
Location of Project:
California State University Dominguez Hills
Person-Months Per Year Committed to the Project. Cal:0.00
Acad: 5.50 Sumr: 0.00
Support:
Current
Pending
Submission Planned in Near Future
*Transfer of Support
Project/Proposal Title: New Quantitative Studies of Bone and Applications
NIH
Source of Support:
Total Award Amount: $
0 Total Award Period Covered: 06/01/05 - 05/31/09
Location of Project:
CSUDH
Person-Months Per Year Committed to the Project. Cal:0.00
Acad: 4.80 Sumr: 0.00
Support:
Current
Pending
Submission Planned in Near Future
*Transfer of Support
Project/Proposal Title: Bone Densitometry Using a New Radiological Method
NIH
Source of Support:
Total Award Amount: $
0 Total Award Period Covered: 03/01/05 - 09/01/05
Location of Project:
CSUDH
Person-Months Per Year Committed to the Project. Cal:0.00
Acad: 0.50 Summ: 0.00
*If this project has previously been funded by another agency, please list and furnish information for immediately preceding funding period.
Page G-1
USE ADDITIONAL SHEETS AS NECESSARY
Current and Pending Support
(See GPG Section II.C.2.h for guidance on information to include on this form.)
The following information should be provided for each investigator and other senior personnel. Failure to provide this information may delay consideration of this proposal.
Other agencies (including NSF) to which this proposal has been/will be submitted.
Investigator: Sam Wiley
Support:
Current
Pending
Submission Planned in Near Future
*Transfer of Support
Project/Proposal Title: Optical Simulations, Burst Source Analysis, and 40m
Participation by the CSUDH LIGO Subgroup
NSF
Source of Support:
Total Award Amount: $
0 Total Award Period Covered: 07/01/05 - 06/30/08
Location of Project:
California State University Dominguez Hills
Person-Months Per Year Committed to the Project. Cal:0.00
Acad: 0.00 Sumr: 1.00
Support:
Current
Pending
Submission Planned in Near Future
*Transfer of Support
Project/Proposal Title:
Source of Support:
Total Award Amount: $
Total Award Period Covered:
Location of Project:
Person-Months Per Year Committed to the Project. Cal:
Acad:
Support:
Current
Pending
Submission Planned in Near Future
Sumr:
*Transfer of Support
Project/Proposal Title:
Source of Support:
Total Award Amount: $
Total Award Period Covered:
Location of Project:
Person-Months Per Year Committed to the Project. Cal:
Acad:
Support:
Current
Pending
Submission Planned in Near Future
Sumr:
*Transfer of Support
Project/Proposal Title:
Source of Support:
Total Award Amount: $
Total Award Period Covered:
Location of Project:
Person-Months Per Year Committed to the Project. Cal:
Acad:
Support:
Current
Pending
Submission Planned in Near Future
Sumr:
*Transfer of Support
Project/Proposal Title:
Source of Support:
Total Award Amount: $
Total Award Period Covered:
Location of Project:
Person-Months Per Year Committed to the Project. Cal:
Acad:
Summ:
*If this project has previously been funded by another agency, please list and furnish information for immediately preceding funding period.
Page G-2
USE ADDITIONAL SHEETS AS NECESSARY
FACILITIES, EQUIPMENT & OTHER RESOURCES
FACILITIES: Identify the facilities to be used at each performance site listed and, as appropriate, indicate their capacities, pertinent
capabilities, relative proximity, and extent of availability to the project. Use "Other" to describe the facilities at any other performance
sites listed and at sites for field studies. USE additional pages as necessary.
Laboratory:
Room NSM C-207A is used as a computer laboratory with desk space for
students. NSM C207B is an electromagnetically screened room containing
electronic equipment, including PMTs, that will be used as an eleconics
and optics laboratory.
Clinical:
Not applicable
Animal:
Not applicable
Computer:
The laboratory contains a DEC Alphastation 500 running TRU 64, 4 Pentium
III pcs, 8 Pentium IVs running LINUX, with DLT tape drive. It also
contains an HP 2100 and HP 4550 laserjet printers and various ultrasound
sources and transducers. We will install a 16-node Beowulf cluster in the
Office:
The PI has a private office in NSM C-201. There is desk space for
students in rooms C-207A and C-207B.
Other:
The investigators have up-to-date LINUX pcs in their offices.
MAJOR EQUIPMENT: List the most important items available for this project and, as appropriate identifying the location and pertinent
capabilities of each.
A Hewlett-Packard 3561A Dynamic Signal analyzer (Fourier Analyzer),
several HP oscilloscopes, and a Stanford Research Systems DS345
Syntehsized Fundtion generator are available in NSM C-207B. Specialized
ultrasound transducers and excitation sources are available for use in
medical imaging research. Also a noncontact ultrasound imaging and
analsis system in EAC 108. There is also an X-ray lab with nuclear
detectors located in NSM C-207A.
OTHER RESOURCES: Provide any information describing the other resources available for the project. Identify support services
such as consultant, secretarial, machine shop, and electronics shop, and the extent to which they will be available for the project.
Include an explanation of any consortium/contractual arrangements with other organizations.
The PI and students often use the computer and laboratory facilties of the
University of California, Irvine at SuperK Observatory Experimental High
Energy Physics group and of the Caltech Physics Department and the Caltech
Advanced Computer Research Center. The PI has collaborated closely with
the Univ. of Calif., Irvine, since 1983; he is a visiting researcher in
the UCI Dept. of Physics and Astronomy and a Clinical Professor of
Radiology at UCLA. The PI is a founding member of the U.S.
FACILITIES, EQUIPMENT & OTHER RESOURCES
Continuation Page:
LABORATORY FACILITIES (continued):
COMPUTER FACILITIES (continued):
chemistry department for use by chemistry and physics in the next few
months.
MAJOR EQUIPMENT (continued):
OTHER RESOURCES (continued):
Super-Kamiokande group and has been a member of the IMB collaboration
since 1983 and is a collaboartion council member of the LIGO scientific
collaboration. Super-Kamiokande is one of the two most important UC
Irvine high energy physics group projects. LIGO is a major national
project. LIGO obervatories at Hanford and Livingston are run by Caltech
and MIT for the LIGO Scientific Collabortion.
NSF FORM 1363 (10/99)