The document proposes a test bench to conduct R&D for an Event Plane and Centrality Detector. Specifically, it will test different detector technologies including scintillator tiles with various pad geometries coupled to silicon photomultipliers. Cosmic ray and electron beam measurements are planned to characterize signal efficiency and timing resolution for different detector configurations. The goals are to optimize pad geometry, understand signal discrimination capabilities, and achieve the best timing resolution.
This document discusses using spectral corrections to better model PV performance. It presents an overview of how the spectral distribution of sunlight changes over the day and affects PV module performance. Models that account for the spectral response of modules and changing spectral irradiance can provide more accurate estimates of performance metrics like current and power output. The document shares results of analyzing spectral data that demonstrate variations in average module response under direct normal, diffuse horizontal, and global irradiance over the course of a day due to these spectral effects. Future work aims to refine estimates of air mass effects and integrate spectral modeling into broader PV modeling.
Testing the global grid of master events for waveform cross correlation with ...Ivan Kitov
Abstract
The Comprehensive Nuclear-Test-Ban Treaty’s verification regime requires uniform distribution of monitoring capabilities over the globe. The use of waveform cross correlation as a monitoring technique demands waveform templates from master events outside regions of natural seismicity and test sites. We populated aseismic areas with masters having synthetic templates for predefined sets (from 3 to 10) of primary array stations of the International Monitoring System. Previously, we tested the global set of master events and synthetic templates using IMS seismic data for February 12, 2013 and demonstrated excellent detection and location capability of the matched filter technique. In this study, we test the global grid of synthetic master events using seismic events from the Reviewed Event Bulletin. For detection, we use standard STA/LTA (SNR) procedure applied to the time series of cross correlation coefficient (CC). Phase association is based on SNR, CC, and arrival times. Azimuth and slowness estimates based f-k analysis cross correlation traces are used to reject false arrivals.
1. The document discusses using sky imagers for short-term solar forecasting, as traditional methods lack sufficient spatial and temporal resolution for small-scale applications.
2. The proposed sky imager forecast model involves 7 steps: image analysis, cloud detection, cloud projection, shadow projection, irradiance modeling, predicting cloud motion to generate forecasts, and PV power modeling.
3. Accurate cloud detection, projection, and shadow projection are challenging due to issues like cloud inhomogeneity, perspective errors with distance from camera, and sensitivity to errors in estimated cloud base height.
Exploring Sources of Uncertainties in Solar Resource Measurements
The presentation explored various sources of uncertainty in solar resource measurements, including calibration differences, spectral mismatch, and soiling effects. Calibration differences between manufacturers and outdoor methods provided irradiance differences up to 2% for pyranometers and 1% for pyrheliometers. Spectral mismatch contributed to spectral errors up to 1.6% and soiling reduced instrument output by 0.2-27% due to decreased transmittance. Quantifying uncertainty from multiple sources is essential for accurate solar resource assessment and project performance.
This document discusses improved methods for predicting the spectral impact on PV systems based on commonly available data. It presents a modified CREST model that uses the true spectral response rather than a useful fraction to better account for variations due to cloudy conditions. Evaluation shows this modified CREST-WUF model significantly outperforms existing models in predicting daily spectral impact factors for different module types. While this approach captures more variation than previous models, further work is still needed to fully characterize the relationship between site properties and spectral offset to enable general predictions of spectral impact.
The document discusses local and regional PV power forecasting based on PV measurements, satellite data, and numerical weather predictions. It summarizes a PV power prediction system that uses different data sources and models for various forecast horizons, from 15 minutes to 5 hours ahead. The system combines persistence forecasts, satellite-derived cloud motion forecasts, PV simulations using numerical weather predictions, and statistical models to improve forecast accuracy compared to individual models. Regional forecasts for Germany show lower errors than single site forecasts.
This document summarizes the results of a validation study of clear sky and all-weather solar irradiance models. It analyzed over 22 ground measurement sites in Europe and the Mediterranean over periods of up to 8 years. Key findings included:
- Hourly global irradiance models showed no bias and a standard deviation of 17-20%. Beam models had no bias and standard deviation of 34-50%.
- Daily models had no bias for global irradiance with a standard deviation of 8-12%, and no bias for beam with a standard deviation of 20-32%.
- Monthly models had negligible bias and standard deviations of 3-6% for global and 9-17% for beam irradiance.
This document discusses using satellite data to generate time series of spectrally resolved solar irradiance data for analyzing the impact of the solar spectrum on photovoltaic module performance. It describes the PVKLIMA project which uses a combination of atmospheric models, satellite imagery, and radiative transfer calculations to estimate spectral irradiance worldwide. Methods for speeding up the calculations and accounting for effects like clouds, aerosols, and module tilt angle are discussed. Future work includes further validation and expanding the method to additional geostationary satellites.
This document discusses using spectral corrections to better model PV performance. It presents an overview of how the spectral distribution of sunlight changes over the day and affects PV module performance. Models that account for the spectral response of modules and changing spectral irradiance can provide more accurate estimates of performance metrics like current and power output. The document shares results of analyzing spectral data that demonstrate variations in average module response under direct normal, diffuse horizontal, and global irradiance over the course of a day due to these spectral effects. Future work aims to refine estimates of air mass effects and integrate spectral modeling into broader PV modeling.
Testing the global grid of master events for waveform cross correlation with ...Ivan Kitov
Abstract
The Comprehensive Nuclear-Test-Ban Treaty’s verification regime requires uniform distribution of monitoring capabilities over the globe. The use of waveform cross correlation as a monitoring technique demands waveform templates from master events outside regions of natural seismicity and test sites. We populated aseismic areas with masters having synthetic templates for predefined sets (from 3 to 10) of primary array stations of the International Monitoring System. Previously, we tested the global set of master events and synthetic templates using IMS seismic data for February 12, 2013 and demonstrated excellent detection and location capability of the matched filter technique. In this study, we test the global grid of synthetic master events using seismic events from the Reviewed Event Bulletin. For detection, we use standard STA/LTA (SNR) procedure applied to the time series of cross correlation coefficient (CC). Phase association is based on SNR, CC, and arrival times. Azimuth and slowness estimates based f-k analysis cross correlation traces are used to reject false arrivals.
1. The document discusses using sky imagers for short-term solar forecasting, as traditional methods lack sufficient spatial and temporal resolution for small-scale applications.
2. The proposed sky imager forecast model involves 7 steps: image analysis, cloud detection, cloud projection, shadow projection, irradiance modeling, predicting cloud motion to generate forecasts, and PV power modeling.
3. Accurate cloud detection, projection, and shadow projection are challenging due to issues like cloud inhomogeneity, perspective errors with distance from camera, and sensitivity to errors in estimated cloud base height.
Exploring Sources of Uncertainties in Solar Resource Measurements
The presentation explored various sources of uncertainty in solar resource measurements, including calibration differences, spectral mismatch, and soiling effects. Calibration differences between manufacturers and outdoor methods provided irradiance differences up to 2% for pyranometers and 1% for pyrheliometers. Spectral mismatch contributed to spectral errors up to 1.6% and soiling reduced instrument output by 0.2-27% due to decreased transmittance. Quantifying uncertainty from multiple sources is essential for accurate solar resource assessment and project performance.
This document discusses improved methods for predicting the spectral impact on PV systems based on commonly available data. It presents a modified CREST model that uses the true spectral response rather than a useful fraction to better account for variations due to cloudy conditions. Evaluation shows this modified CREST-WUF model significantly outperforms existing models in predicting daily spectral impact factors for different module types. While this approach captures more variation than previous models, further work is still needed to fully characterize the relationship between site properties and spectral offset to enable general predictions of spectral impact.
The document discusses local and regional PV power forecasting based on PV measurements, satellite data, and numerical weather predictions. It summarizes a PV power prediction system that uses different data sources and models for various forecast horizons, from 15 minutes to 5 hours ahead. The system combines persistence forecasts, satellite-derived cloud motion forecasts, PV simulations using numerical weather predictions, and statistical models to improve forecast accuracy compared to individual models. Regional forecasts for Germany show lower errors than single site forecasts.
This document summarizes the results of a validation study of clear sky and all-weather solar irradiance models. It analyzed over 22 ground measurement sites in Europe and the Mediterranean over periods of up to 8 years. Key findings included:
- Hourly global irradiance models showed no bias and a standard deviation of 17-20%. Beam models had no bias and standard deviation of 34-50%.
- Daily models had no bias for global irradiance with a standard deviation of 8-12%, and no bias for beam with a standard deviation of 20-32%.
- Monthly models had negligible bias and standard deviations of 3-6% for global and 9-17% for beam irradiance.
This document discusses using satellite data to generate time series of spectrally resolved solar irradiance data for analyzing the impact of the solar spectrum on photovoltaic module performance. It describes the PVKLIMA project which uses a combination of atmospheric models, satellite imagery, and radiative transfer calculations to estimate spectral irradiance worldwide. Methods for speeding up the calculations and accounting for effects like clouds, aerosols, and module tilt angle are discussed. Future work includes further validation and expanding the method to additional geostationary satellites.
1) The document presents a statistical model for describing small-scale ionospheric turbulence in radar data using power law functions.
2) It describes the Ionospheric Phase Statistics Simulator (IP-STATS) which uses parameters from a global ionospheric model to predict power spectra and simulate ionospheric phase screens.
3) Initial validation results show IP-STATS can accurately predict the variance and covariance of ionospheric phase signals observed in polar region radar data.
This document summarizes a presentation on estimating the influence of solar spectrum variations on PV performance using satellite-based spectral irradiance data. It describes methods for calculating spectral correction factors and module performance ratio given spectral response curves and spectrally resolved irradiance data. Maps of Europe show estimated annual spectral effects on c-Si, CdTe, a-Si tandem, and III-V multi-junction modules, with effects ranging from -3% to 3%. The analysis demonstrates how satellite data can be used to model large-scale spectral impacts, though results in some climates need validation.
This document describes a data analysis method to automatically detect energy losses from shadows on a partially shaded residential PV system using only production data. The method defines an error barrier between a benchmark PV system and the studied system. Times when the error exceeds the barrier are marked in red, otherwise green. Periods with high red concentrations indicate shadowing. Shadowed times are then analyzed daily to distinguish between shaded and unshaded days, and further analyze shadowing within expected shadow hours only on shaded days. The goal is to distinguish energy losses due to shadows from other faults using just production data from the inverter.
The document summarizes the development of satellite modeling for the National Solar Radiation Database (NSRDB) to provide accurate surface solar radiation data. It describes the evolution from empirical to physical models using satellite measurements and ancillary data as inputs to radiative transfer models. Validation shows the new 2005-2012 dataset has a mean bias error of less than 5% for GHI and DNI compared to surface measurements, though uncertainty remains for cloudy cases. Future work aims to improve the model with higher resolution data and better representation of aerosols and surfaces.
The document discusses the impact of spectral irradiance on the energy yield of different PV module technologies measured at test sites in various climates. Spectral response measurements showed variations between module types and locations. One year of spectral irradiance data from four test sites showed seasonal shifts from the AM1.5 standard spectrum. For c-Si modules, spectral effects had a minor impact on energy yield of up to 1.6% higher in Chennai. CdTe modules saw gains of up to 5.3% in Chennai due to their spectral response. While daily and seasonal shifts in spectrum compensated over the year for most modules, spectral irradiance was found to influence energy yield predictions, particularly for thin-film technologies
The document discusses modeling efforts for the James Webb Space Telescope (JWST). Preliminary analysis indicated traditional third-order effects could cause performance issues. This leads to large detailed models with millions of elements to model the composite tubes. Rapid analysis cycles are used to minimize differences between the model and baseline, but the large models and short cycle time create demanding multi-disciplinary analysis.
This document discusses the uncertainty of solar radiation data from the Solargis database. It describes how Solargis determines uncertainty ranges of ±4-8% for yearly global horizontal irradiation (GHI) and ±8-15% for direct normal irradiation (DNI). The total uncertainty is calculated based on contributions from various uncertainty drivers in the satellite input data and solar radiation models, including clouds, aerosols, water vapor, and terrain variability. Long-term GHI uncertainty can be reduced to ±2.5% by combining satellite data with ground measurements from monitoring stations.
1. The document discusses the author's past and planned work related to cosmic microwave background (CMB) research.
2. Previous work includes analyzing the effects of non-circular beams on CMB parameter estimation and tests for statistical isotropy violations. The author developed software tools for these areas.
3. Planned future work includes extending existing tools to analyze CMB polarization data, anisotropic lensing, and other anomalies, as well developing new capabilities for cosmological simulations and intensity mapping analyses.
The document discusses the development of an energy-based parameter for photovoltaic classification by the PhotoClass consortium. The consortium aims to define a new metric based on the annual energy yield of photovoltaic modules under real-world conditions, rather than just peak power. This will provide a more accurate assessment of module performance and energy generation. The PhotoClass work plan includes modelling to calculate energy yields, characterizing reference devices, detector characterization, source characterization, and developing standards. The goal is to establish a standardized energy rating that supports the renewable energy industry and implementation of EU directives.
The System Advisor Model (SAM) is a free software tool that calculates the energy production and financial metrics of renewable energy projects. Recent updates include improved photovoltaic, battery storage, and shading models, as well as expanded international weather data, utility rate structures, and a software development kit. Future enhancements will include direct links to additional international weather data, inverters with multiple inputs, and open sourcing the PV and battery models.
Explanation of very simple methods for atmospheric corrections and an example adapted from a paper of the Dept. of Thermodynamics, University of Valencia, Spain.
This document describes three atmospheric correction algorithms for the Geostationary Ocean Color Imager (GOCI): the Standard NASA algorithm, the Spectral Shape Matching Method (SSMM), and the Sun-Glint Correction Algorithm (SGCA). It outlines the processing steps for each algorithm, including radiometric calibration, removal of Rayleigh and aerosol scattering, and derivation of remote sensing reflectance. Validation results show SSMM and SGCA provide reasonable matches to NASA standard processing of MODIS data, though all three GOCI algorithms could be improved by updating aerosol and ocean models. The document concludes the algorithms capture the essential ocean color measurement but would benefit from further refinement.
The document discusses upcoming changes to international standards for classifying radiometers. It outlines the motivation for revising ISO 9060 and developing new ASTM classification standards. Key proposed updates include adding new classes for fast response sensors and spectrally flat sensors to better accommodate modern instrument technologies. Other topics cover revising definitions of spectral selectivity, allowing corrected instrument signals to determine classification, and defining shading structures for diffuse irradiance measurements. The presentation seeks feedback on the draft standards and identifies remaining open issues to resolve.
This document presents results from a lattice QCD calculation of the proton isovector scalar charge (gs) at two light quark masses. The calculation uses domain-wall fermions and Iwasaki gauge actions on a 323x64 lattice with a spacing of 0.144 fm. Ratios of three-point to two-point correlation functions are formed and fit to a plateau to extract gs. Values of gs are obtained for quark masses of 0.0042 and 0.001, and all-mode averaging is used for the lighter mass. Chiral perturbation theory will be used to extrapolate gs to the physical quark mass. Preliminary results for gs at the unphysical quark masses are reported in lattice units.
This document describes a lattice QCD computation of the proton isovector scalar charge (gs) at two unphysical quark masses. Jackknife statistics and all-mode averaging techniques are used to calculate correlation functions from Monte Carlo simulations, which are then fitted and extrapolated to obtain gs at the physical quark mass. Results show the unrenormalized values of gs computed at quark masses of 0.0042 and 0.0015, with the goal of constraining gs through precise theoretical calculations needed to interpret experimental measurements.
1) The document presents a statistical model for describing small-scale ionospheric turbulence in radar data using power law functions.
2) It describes the Ionospheric Phase Statistics Simulator (IP-STATS) which uses parameters from a global ionospheric model to predict power spectra and simulate ionospheric phase screens.
3) Initial validation results show IP-STATS can accurately predict the variance and covariance of ionospheric phase signals observed in polar region radar data.
This document summarizes a presentation on estimating the influence of solar spectrum variations on PV performance using satellite-based spectral irradiance data. It describes methods for calculating spectral correction factors and module performance ratio given spectral response curves and spectrally resolved irradiance data. Maps of Europe show estimated annual spectral effects on c-Si, CdTe, a-Si tandem, and III-V multi-junction modules, with effects ranging from -3% to 3%. The analysis demonstrates how satellite data can be used to model large-scale spectral impacts, though results in some climates need validation.
This document describes a data analysis method to automatically detect energy losses from shadows on a partially shaded residential PV system using only production data. The method defines an error barrier between a benchmark PV system and the studied system. Times when the error exceeds the barrier are marked in red, otherwise green. Periods with high red concentrations indicate shadowing. Shadowed times are then analyzed daily to distinguish between shaded and unshaded days, and further analyze shadowing within expected shadow hours only on shaded days. The goal is to distinguish energy losses due to shadows from other faults using just production data from the inverter.
The document summarizes the development of satellite modeling for the National Solar Radiation Database (NSRDB) to provide accurate surface solar radiation data. It describes the evolution from empirical to physical models using satellite measurements and ancillary data as inputs to radiative transfer models. Validation shows the new 2005-2012 dataset has a mean bias error of less than 5% for GHI and DNI compared to surface measurements, though uncertainty remains for cloudy cases. Future work aims to improve the model with higher resolution data and better representation of aerosols and surfaces.
The document discusses the impact of spectral irradiance on the energy yield of different PV module technologies measured at test sites in various climates. Spectral response measurements showed variations between module types and locations. One year of spectral irradiance data from four test sites showed seasonal shifts from the AM1.5 standard spectrum. For c-Si modules, spectral effects had a minor impact on energy yield of up to 1.6% higher in Chennai. CdTe modules saw gains of up to 5.3% in Chennai due to their spectral response. While daily and seasonal shifts in spectrum compensated over the year for most modules, spectral irradiance was found to influence energy yield predictions, particularly for thin-film technologies
The document discusses modeling efforts for the James Webb Space Telescope (JWST). Preliminary analysis indicated traditional third-order effects could cause performance issues. This leads to large detailed models with millions of elements to model the composite tubes. Rapid analysis cycles are used to minimize differences between the model and baseline, but the large models and short cycle time create demanding multi-disciplinary analysis.
This document discusses the uncertainty of solar radiation data from the Solargis database. It describes how Solargis determines uncertainty ranges of ±4-8% for yearly global horizontal irradiation (GHI) and ±8-15% for direct normal irradiation (DNI). The total uncertainty is calculated based on contributions from various uncertainty drivers in the satellite input data and solar radiation models, including clouds, aerosols, water vapor, and terrain variability. Long-term GHI uncertainty can be reduced to ±2.5% by combining satellite data with ground measurements from monitoring stations.
1. The document discusses the author's past and planned work related to cosmic microwave background (CMB) research.
2. Previous work includes analyzing the effects of non-circular beams on CMB parameter estimation and tests for statistical isotropy violations. The author developed software tools for these areas.
3. Planned future work includes extending existing tools to analyze CMB polarization data, anisotropic lensing, and other anomalies, as well developing new capabilities for cosmological simulations and intensity mapping analyses.
The document discusses the development of an energy-based parameter for photovoltaic classification by the PhotoClass consortium. The consortium aims to define a new metric based on the annual energy yield of photovoltaic modules under real-world conditions, rather than just peak power. This will provide a more accurate assessment of module performance and energy generation. The PhotoClass work plan includes modelling to calculate energy yields, characterizing reference devices, detector characterization, source characterization, and developing standards. The goal is to establish a standardized energy rating that supports the renewable energy industry and implementation of EU directives.
The System Advisor Model (SAM) is a free software tool that calculates the energy production and financial metrics of renewable energy projects. Recent updates include improved photovoltaic, battery storage, and shading models, as well as expanded international weather data, utility rate structures, and a software development kit. Future enhancements will include direct links to additional international weather data, inverters with multiple inputs, and open sourcing the PV and battery models.
Explanation of very simple methods for atmospheric corrections and an example adapted from a paper of the Dept. of Thermodynamics, University of Valencia, Spain.
This document describes three atmospheric correction algorithms for the Geostationary Ocean Color Imager (GOCI): the Standard NASA algorithm, the Spectral Shape Matching Method (SSMM), and the Sun-Glint Correction Algorithm (SGCA). It outlines the processing steps for each algorithm, including radiometric calibration, removal of Rayleigh and aerosol scattering, and derivation of remote sensing reflectance. Validation results show SSMM and SGCA provide reasonable matches to NASA standard processing of MODIS data, though all three GOCI algorithms could be improved by updating aerosol and ocean models. The document concludes the algorithms capture the essential ocean color measurement but would benefit from further refinement.
The document discusses upcoming changes to international standards for classifying radiometers. It outlines the motivation for revising ISO 9060 and developing new ASTM classification standards. Key proposed updates include adding new classes for fast response sensors and spectrally flat sensors to better accommodate modern instrument technologies. Other topics cover revising definitions of spectral selectivity, allowing corrected instrument signals to determine classification, and defining shading structures for diffuse irradiance measurements. The presentation seeks feedback on the draft standards and identifies remaining open issues to resolve.
This document presents results from a lattice QCD calculation of the proton isovector scalar charge (gs) at two light quark masses. The calculation uses domain-wall fermions and Iwasaki gauge actions on a 323x64 lattice with a spacing of 0.144 fm. Ratios of three-point to two-point correlation functions are formed and fit to a plateau to extract gs. Values of gs are obtained for quark masses of 0.0042 and 0.001, and all-mode averaging is used for the lighter mass. Chiral perturbation theory will be used to extrapolate gs to the physical quark mass. Preliminary results for gs at the unphysical quark masses are reported in lattice units.
This document describes a lattice QCD computation of the proton isovector scalar charge (gs) at two unphysical quark masses. Jackknife statistics and all-mode averaging techniques are used to calculate correlation functions from Monte Carlo simulations, which are then fitted and extrapolated to obtain gs at the physical quark mass. Results show the unrenormalized values of gs computed at quark masses of 0.0042 and 0.0015, with the goal of constraining gs through precise theoretical calculations needed to interpret experimental measurements.
This document discusses two projects related to the Upsilon meson. The first estimates the systematic uncertainty associated with Upsilon polarization measurements at the LHC due to detector acceptance effects. The second analyzes Upsilon yields from STAR data at RHIC to compare to recent CMS findings of a correlation between Upsilon production and event activity measures. While STAR sees a less pronounced correlation possibly due to lower statistics, both detectors aim to better understand Upsilon properties to reveal characteristics of the quark-gluon plasma.
The document provides an overview of the SPHENIX Clusterizer algorithm used at CMS. It describes the island algorithm which clusters calorimeter towers starting from the highest energy seed tower and moving in φ and η directions until an energy rise or hole is found. Simple checks are performed using single particle events to evaluate the number and energy of clusters compared to the generated particle properties. Further work is planned to characterize shower shapes and evaluate performance on more complex events.
The island algorithm is a photon clusterization method used in the sPHENIX detector upgrade. It identifies photon clusters by starting from energy towers above a threshold and grouping adjacent towers. For single particle simulations, it closely reconstructs particle energies. It performs better than a simple 5x5 clusterizer which can overestimate energies. While it reliably clusters electrons, photons and pions, more testing is needed with complex events before full implementation.
This document summarizes a research project that involves building a toy model of particle collisions using C++ and ROOT. The model simulates collisions by sampling probability distributions measured in real collisions. It generates particles and assigns them properties like momentum and angle. It also models physical processes like jet production and elliptic flow. The goal is to study how properties of particles like jets are affected by a quark-gluon plasma and vice versa. The model allows tuning parameters to learn about collision interactions and switch physics processes on or off.
This document provides an overview of a toy model for simulating particle collisions. It describes sampling particle data from experimental measurements to generate events. A jet finding algorithm is used to cluster particles into jets using FastJet. The current status indicates particle generation works as expected but jet finding results appear buggy. Next steps involve analyzing jet distributions and performance of the jet finder on simulated events without embedded jets. Possible extensions include jet fragmentation.
This document summarizes research on characterizing crosstalk in dense Geiger-mode avalanche photodiode arrays. The researchers measured crosstalk probability (PCT) using different experimental setups and calculation methods. Key findings include:
1) PCT decreases with increasing pixel distance and decreases with lower bias voltages.
2) PCT increases with higher pixel capacitance, extrapolating to a value of 0.05% for a capacitance of 100fF.
3) PCT decay time was measured to be a few microseconds to investigate crosstalk origins.
The document describes the development of an automatic MATLAB-based tool for measuring beam emittance at the Idaho Accelerator Center. An optical transition radiation screen and camera were installed to capture beam images during a quadrupole scan. MATLAB codes were developed to extract beam sizes from the images, perform a polynomial fit to determine emittance, and control the scan automatically via EPICS and MATLAB Channel Access. The tool was tested by measuring the emittance of the HRRL accelerator, reducing measurement time and error compared to manual methods.
The document examines the effect of microcell size on the timing performance of silicon photomultipliers (SiPMs) for time-of-flight positron emission tomography (TOF-PET) imaging. Coincidence timing resolution measurements were performed using Hamamatsu 3x3 mm2 SiPMs with 25, 50, and 100 um microcells. While a larger microcell size provides benefits like higher photon detection efficiency, devices with larger microcells also exhibited higher dark count rates which degraded timing resolution. However, incorporating a high pass filter to reduce the impact of dark counts allowed the 100 um device to achieve better timing resolution than the 50 um device. Nonetheless, the 50 um microcell size remains preferable for TO
IRJET- Compressed Sensing based Modified Orthogonal Matching Pursuit in DTTV ...IRJET Journal
This document discusses a modified orthogonal matching pursuit algorithm used for channel estimation in digital terrestrial television systems. It proposes using compressed sensing based channel estimation at the receiver to eliminate sparse information. Thresholding is used to remove noise from the channel estimation and improve signal quality. Simulation results show that bit error rate decreases when the received signal power from different transmitters is almost equal.
This document provides an introduction to analyzing signals in the time, frequency, and modal domains. It discusses:
1) The time domain directly records how a parameter varies over time, while the frequency domain represents a signal as the sum of its sine wave components.
2) Analyzing signals in the frequency domain can make it easier to detect small signals masked by large ones, as components are separated. Instruments like dynamic signal analyzers are useful for frequency domain analysis.
3) Examples show that a sine wave has a single frequency component, while square waves and transients have multiple components. The spectrum of an impulse is flat, containing all frequencies.
This document compares the use of commercially available X5R and Y5V ceramic capacitors as alternatives to lead zirconate titanate (PZT) for nanoactuators. It finds that the Y5V capacitors provide the highest displacement per volt at 17.4 ppm/V, followed by the X5R capacitors at 7.64 ppm/V, while the PZT material provides 6.02 ppm/V. Additionally, the Y5V capacitors require only 11% of the maximum voltage needed for the PZT material. Therefore, the Y5V capacitors provide a cheaper and lead-free alternative to PZT for applications requiring high displacement at low voltages.
Cetc11 - Wireless Magnetic Based Sensor System For Vehicles ClassificationNokia Networks
This paper presents a full pre-industrial prototype implementation of an innovative system capable to
detects vehicles and classify them. This work study the architecture of a full autonomous road sensor
network that count and classify passing vehicles, reducing the impact of conventional wired systems in
roads, by dramatically reducing their installation and operational costs. The power supply can be supported
either by solar harvest or by none rechargeable batteries. For communications the IEEE 802.15.4 with
ZigBee on top are used to transmit digitalized vehicle’s magnetic analogue signatures up to a vehicles
classification server. This information is acquired using a magnetometer translating in voltage the variation
of the natural magnetic field of the earth caused by ferromagnetic components of a vehicle passing over the
sensor. Results show clearly that it is possible to distinguish vehicles magnetic signatures per model and
class even at different speeds.
Design and implementation of microstrip rotman lens for ISM band applicationsjournalBEEI
This work presents the design and implementation of Rotman lens as a beam steering device for Industrial, Scientific, and Medical (ISM) applications. 2.45 GHz is considered as a center frequency design with (2-6) GHz frequency bandwidth. The beam steering is examined to cover ±21o scan angle with maximum main lobe magnitude 10.1 dBi, rectangular patch antennas are used as radiation elements to beam the output far field. The work is extended to compare between the tapered line which is used for matching between 50-Ω ports and lens cavity. CST microwave simulation studio results show that the rectangular taper line can yield 2 dB return loss less than linear taper line with a little bit shifting in responses for same input and load impedance.
MODELING STUDY OF LASER BEAM SCATTERING BY DEFECTS ON SEMICONDUCTOR WAFERSjmicro
Accurate modeling of light scattering from nanometer scale defects on Silicon wafersiscritical for enabling
increasingly shrinking semiconductor technology nodes of the future. Yet, such modeling of defect
scattering remains unsolved since existing modeling techniques fail to account for complex defect and
wafer geometries. Here, we present results of laser beam scattering from spherical and ellipsoidal
particles located on the surface of a silicon wafer. A commercially available electromagnetic field solver
(HFSS) was deployed on a multiprocessor cluster to obtain results with previously unknown accuracy
down to light scattering intensity of -170 dB. We compute three dimensional scattering patterns of silicon
nanospheres located on a semiconductor wafer for both perpendicular and parallel polarization and show
the effect of sphere size on scattering. We further computer scattering patterns of nanometer scale
ellipsoidal particles having different orientation angles and unveil the effects of ellipsoidal orientation on
scattering.
This is research work carried out by Dr. Preeta sharan and her student Kavya Ullal. It was live streaming international conference. The organizer appreciated her work at the end of the show.
Backtracking Search Optimization for Collaborative Beamforming in Wireless Se...TELKOMNIKA JOURNAL
Due to energy limitation and constraint in communication capabilities, the undesirable high
battery power consumption has become one of the major issues in wireless sensor network (WSN).
Therefore, a collaborative beamforming (CB) method was introduced with the aim to improve the radiation
beampattern in order to compensate the power consumption. A CB is a technique which can increase the
sensor node gain and performance by aiming at the desired objectives through intelligent capabilities. The
sensor nodes were located randomly in WSN environment. The nodes were designed to cooperate among
each other and act as a collaborative antenna array. The configuration of the collaborative nodes was
modeled in circular array formation. The position of array nodes was determined by obtaining the optimum
parameters pertaining to the antenna array which implemented by using Backtracking Search Optimization
Algorithm (BSA). The parameter considered in the project was the side-lobe level minimization. It was
observed that, the suppression of side-lobe level for BSA was better compared to the radiation
beampattern obtained for conventional uniform circular array.
Channel Overlapping Between IMT-Advanced Users and Fixed Satellite ServiceEECJOURNAL
This document summarizes a research paper that proposes a new algorithm to mitigate interference between IMT-Advanced base stations and fixed satellite services. The algorithm aims to form nulls in the radiation pattern of base stations towards satellites by extracting null directions using MUSIC algorithm and controlling handover. It studies two mobile users moving around a satellite and simulates calculating the shortest separation distance after identifying critical points. Results show the algorithm can enable good coexistence and spectrum sharing between the different wireless services in the C-band frequency range.
The document summarizes Satadru Das' summer internship exploring quantum technologies at IIT Madras from May to July 2019. It discusses three approaches to building an optical Ising machine using optical parametric oscillators. It also covers several quantum key distribution protocols including BB84, DPS-QKD and E91. Finally, it describes experiments performed on fiber optic communication systems, including characterization of WDM components, fiber Bragg gratings, optical time domain reflectometry and more. The internship provided an opportunity for Satadru to learn about active research in quantum computing, communication and related fiber optic experiments.
MODELING STUDY OF LASER BEAM SCATTERING BY DEFECTS ON SEMICONDUCTOR WAFERSjmicro
Accurate modeling of light scattering from nanometer scale defects on Silicon wafersiscritical for enabling
increasingly shrinking semiconductor technology nodes of the future. Yet, such modeling of defect
scattering remains unsolved since existing modeling techniques fail to account for complex defect and
wafer geometries. Here, we present results of laser beam scattering from spherical and ellipsoidal
particles located on the surface of a silicon wafer. A commercially available electromagnetic field solver
(HFSS) was deployed on a multiprocessor cluster to obtain results with previously unknown accuracy
down to light scattering intensity of -170 dB. We compute three dimensional scattering patterns of silicon
nanospheres located on a semiconductor wafer for both perpendicular and parallel polarization and show
the effect of sphere size on scattering. We further computer scattering patterns of nanometer scale
ellipsoidal particles having different orientation angles and unveil the effects of ellipsoidal orientation on
scattering.
This document summarizes the design and testing of a photonic gas sensor using a silicon strip waveguide to detect carbon dioxide (CO2). Finite element simulations were used to design a strip waveguide with a high evanescent field ratio to enable gas absorption sensing. The sensor was experimentally tested and could detect CO2 concentrations as low as 5000 parts per million, the workplace exposure limit. Measurements matched predictions from the Beer-Lambert law for light absorption, demonstrating the sensor's potential for quantitative gas detection.
The document discusses using MCNP simulations to design a fast neutron spectrometer to measure neutron backgrounds in dark matter detectors. It describes how MCNP simulations were used to simulate different detector geometries containing scintillator cells to evaluate which configuration detected the highest percentage of neutrons. PTRAC files recorded energy deposition information to allow calculation of expected light output. Simulations also informed the design of a neutron shielding container containing an optimized mixture of steel and paraffin wax that increased neutron attenuation by a factor of 105 compared to no shielding.
This document reports on the development of an analytic model to calculate skyshine radiation doses from radioactive waste stores. Skyshine occurs when radiation reflects off the atmosphere back towards the ground. The analytic model is compared to results from Monte Carlo N-Particle (MCNP) simulations, which are considered the standard approach. The analytic model underestimated potential skyshine doses compared to MCNP, ranging from 43.4 to 188.1 times lower. This difference is mainly attributed to the analytic model not accurately accounting for scattering events in the concrete roof and air. The report concludes the analytic model is not suitable for radioactive waste store design without improvements to model scattering.
1. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
Event-Plane and Centrality Detector
Test Bench Proposal
Brandon McKinzie, Michael Lomnitz, Alexander Schmah
March 25, 2015
1. Motivation / Background
A test bench will be constructed to begin research and development for an Event Plane and Centrality
Detector (EPD) for Beam Energy Scan (BES) II. The EPD serves the following purposes: event plane recon-
struction for heavy-ion flow measurements, centrality determination by particle multiplicity measurement,
trigger detection for “good” reactions within a certain z-vertex range. It will be the main upgrade for the
Beam Energy Scan Phase II program. As written in section four of the EPD proposal, the result of the
overall R&D program should be answers to the following questions:
1. What is the optimal pad geometry for different radii?
2. Are waveshifters needed and if yes, how do we install them?
3. What is the optimal connection between SiPM and scintillator?
4. Can multiple hits be distinguished, and what kind of ADC is needed?
5. What timing resolution can we achieve with the setup?
6. How will the radiation damage influence the measurement?
At present, we are most interested in questions 1, 4, and 5. We associate optimal pad geometry with high
detection efficiencies and clear signal shape. The results of tests related to pad geometry should then
include efficiencies and signal shapes for each different proposed tile, as discussed in the Equipment section.
As far as hit discrimination, we are less concerned with individual pulse heights and more interested in a
charge-integration technique. This is because simultaneous hits on a tile will travel different distances to
the ADC, and an integration method would provide a better representation of the incident hits. Finally, the
timing resolution is dependent on the dead times of each detector element and how they interact. We hope
to find a setup that optimizes this timing resolution for fast data collection.
In order to answer these questions, we plan to construct a test bench with the proposed detector technology
and conduct cosmic ray measurements. The final stage of the R&D will be building a prototype of two
fully equipped sectors with about 16 channels each. We expect to have a construction proposal ready at the
end of 2015. The final apparatus has to be ready in 2018 with a partial commissioning in 2017.
1
2. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
2. Measurements of Interest
As stated in the EPD proposal, we need to check which silicon photomultiplier’s (SiPM) performance is
sufficient for our purpose. Presently, we will be conducting measurements using Hamamatsu S12572 and
S13360 series multi-pixel photon counters (MPPC). We are interested in the following SiPM measurements:
• Efficiency for single m.i.p. hits
• Uniformity of pulse area and efficiency as a function of poisition of hit on a scintillator
• Pulse shapes for m.i.p.’s
• Gain vs bias voltage
• Timing resolution
• Dark noise characteristics
• Temperature stability
Overall, we want to see how the Megatile - WLS Plastic - SiPM setup will perform via cosmic ray
measurements. We hope to trigger on an incident cosmic ray with the setup, measure the signal, then
measure the same ray again as it exits the apparatus for timing measurements. We hope to see fast
triggering and fast decay time from the scintillator.
2.1 Cosmic Ray Measurements
See Figure 5 and the Procedure section for a rough idea of the proposed setup. Essentially, we place
our detector in between two trigger paddles built from the same scintillator/WLS fiber/SiPM technology.
Cosmics incident on the paddles will trigger data acquisition from the detector placed in the middle. The
size of the triggers will be made small (about 2x2 cm) in comparison to the detector. The distance between
the detector and both paddles will be made large to improve timing resolution. The most important initial
measurement is confirmation of electric signals from the SiPM to the ADC at a rate typical of cosmic
ray measurements. In the case of the BEMC cosmic measurements, the trigger rate associated with the
coincidence signal of two muon-counters was 0.15 Hz and the ADC gate was 100 ns. Figure 1a shows a
BEMC plot of the ADC pulse height spectrum from cosmic muons for tile/fiber assemblies. To obtain light
yield information, the spectra were fitted with a Gaussian function. Since we are using a similar setup as
the BEMC, we expect to measure similar pulse spectra, with expected differences arising from different
trigger sizes/rates.
Eventually, we want to know the efficiency/light yield as a function of the hit position. However, in order to
reduce the time needed to conduct the initial measurements, we will first measure the detection efficiency
on a limited region. In other words, we want to know what fraction of triggered particles are measured by
the detector. After this measurement is complete, it can be used as a baseline reference for more precise
measurements using either an electron beam (see next subsection) or further cosmic measurements of finer
position resolution. This depends on the accessibility of an electron source during the measurement stage.
2
3. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
(a) The ADC pulse height spectrum from cosmic muons
for tile tile/fiber assemblies from documentation on the
BEMC prototyping stages. Data corresponds to about
3000 events at an unspecified point of measurement.
(b) Fluxes of nuclei of the primary cosmic radiation in par-
ticles per energy-per-nucleus are plotted vs energy-per-
nucleus. Figure Credit: P. Boyle and D. Muller [3].
The trigger scintillators above and below the tile will be made small compared to the tile. By doing
this, we know roughly where the cosmic ray struck the detector and can record the light yield informa-
tion for a given tile region. Figure 1b shows that, for particles with energy on the order of 1 GeV, the
rate of arrival is about 1,000 m−2s−1. However, this is rate of arrival at the top of the atmosphere. For the
vertical flux of cosmic rays at ground-level, experimentalists use I = 1 cm−2min−1 for horizontal detectors[3].
Using this information and relevant tile quantities, we can estimate how long it should take to measure 500
cosmics for a given trigger scintillator size. The proposed tiles are 12 cm x 12 cm, so a reasonable resolution
in hit position would be 2 cm x 2 cm trigger scintillators. Therefore, the time required to detect 500 cosmics
is
t =
500counts
4cm2
1count
cm2min
= 2 hr 5 min
So, depending on the solid-angle acceptance of incident cosmics on the trigger, we expect a collection of
500 cosmics to take about 2 hours.
2.2 Electron Gun Measurements
With a radiation source, we can determine which groove geometry exhibits optimal light collection. This
would likely be done by scanning over the tiles with a Sr-90 source to give a relative light yield from
different positions on the tiles. With plots of hit detection as a function of source position, one for each
3
4. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
groove geometry, one could compare light yields/efficiencies scanned over the entire tile.
An advantage of the chosen SiPMs is low crosstalk. This means that a given detecting pixel is less likely
to affect other nearby pixels or cause them to produce pulses separate from output pulses. We can take
advantage of this characteristic in radiation source measurements because we know (roughly) where the
detected particles are originating and, on average, their energy. Using this information, we can measure
whether or not the SiPM output accurately reflects the strength of the input beam. In other words, should
we measure more signal than expected, this is indicative of noise complications/interactions between the
detector elements. Such measurements would have to take into account other factors, such as the level
of SiPM dark count, which is the rate of registered counts without any incident light [1]. The chosen
SiPMs are rated for a typical dark counts of 1000 kcps (S12572), 90 kcps (S13360-1350CS), and 500 kcps
(S13360-3050CS). Thus, by conducting these measurements, we can obtain a better understanding of the
overall signal-to-noise ratio in our setup and how it varies depending on the chosen SiPM.
3. Equipment
The EJ-200 Plastic Scintillator [4], Wavelength Shifting Plastics, and S12572 MPPC have been chosen for
the proposed detector technology. The EJ-200 Plastic Scintillator has long optical attenuation length
and fast timing. The scintillator tiles will either (a) contain WLS fibers which absorb the scintillator light
and emit it isotropically at longer wavelengths, or (b) be directly coupled to an attached SiPM (no WLS fiber).
The WLS fibers will be installed into grooves on the surface of the tiles and fed out into the SiPMs. We
recognize the time-spread induced by the WLS fiber in the larger tiles, but this level of time precision is
not needed for the larger tiles. This is because there will be a far narrower time spread in the smaller and
more central tiles. The degree of time spread is dependent on the chosen geometry of grooves into the tiles.
The geometry is to be determined during this phase of R&D. The three primary geometries of interest are
shown in Figure 3. We will be ordering the EJ-200 scintillating plastic with dimensions 28cm x 28cm and
widths of 0.5 cm, 1.0 cm, and 2.0 cm. These large tiles will be cut down to three smaller tiles of dimensions
12 cm x 12 cm and the remaining tile material will be further cut down to experiment with smaller tile
geometries. The milling for the proposed groove geometries will be done in the LBL machine shop.
The lines on the tiles indicate where the WLS fibers are to be inserted into a groove. A side-view of the
proposed U-shaped grooves is shown below in Figure 7, specifically for the straight-groove design. The
shape and depth of the groove is the same for all three shown designs. Another possible groove shape of
interest involved the upper edges curling into each other more, resembling an upside-down Ω. Once the
WLS fibers are installed into these grooves, they will be sealed in with optical glue.
When installed, the individual tiles in a given sector will be physically connected, separated only by a
4
5. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
90% depth groove-cut, as shown in Figures 2 and 6. Reflective paint will be applied to the side of these
tile-edge grooves, and the grooves themselves will be filled with epoxy. These “separation” grooves, as
used in the BEMC, optically isolate the tiles from each other while maintaining mechanical robustness of
the tiles. Since scintillated photons may reflect off the bottom 10% of the un-milled tile underneath the
groove, we need to measure and account for any possible crosstalk between the tiles (i.e. one scintillation
from one tiling affecting an adjacent tile). A more complete list of proposed tile geometries is shown at the
end of this report in Figure 6.
Each WLS fiber will be fed to a SiPM, which in our case will be a general-purpose Multi-Pixel Photon
Counter (MPPC)(Hamamatsu S12572 or S13360). MPPCs require low voltages and exhibit high gain, high
photon detection efficiency, and high-speed response. They have excellent time-resolution (250 ps FWHM)
and a wide spectral response range (320-900 nm). In addition, they have the advantage of being immune
to magnetic fields and resistant to mechanical shocks. Such properties make these MPPCs promising
technology for the EPD. As shown in Figure 4, the S12572 series has a photon detection efficiency of 35%
for incident photons with λ = 450 nm, the peak sensitivity wavelength of the SiPMs.1
The peak emission wavelength of the Y11 WLS fibers, which will be incident on the SiPMs, is rated at 476
nm. This is roughly a 5.6% difference. The SiPMs have a photon detection efficiency of 35% at the peak
sensitivity wavelength of 450 nm, so we expect to see near-peak photon detection efficiencies from the WLS
fibers to the SiPMs. The chosen scintillator is also well-matched with the Y11 WLS fiber. The scintillator
Figure 2: (From BEMC Technical Design Report) Upper photo shows separation grooves between tiles with σ shaped
grooves for WLS fibers in the scintillators. Lower photo shows shows the opposite side of the fiber-routing
layer, with wavelength-shifting fibers routed through undulating channels, from which they enter the σ
grooves in each tile.
1For more SiPM specs, see Ref. [5]
5
6. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
Figure 3: Different proposed tile / WLS designs. All tiles are 12x12 cm. The four-line grooves are each 2.4 cm apart.
6
7. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
(a) EJ-200 Scintillator (b) Y11 WLS Fiber (darkest line)
(c) Hamamatsu SiPM MPPC (detec-
tion efficiency)
Figure 4: Emission/Absorption spectra for detector components.
has a peak emission of 425 nm and the Y11 has peak absorption at 430 nm. Figure 4 illustrates, from
left-to-right, how likely a photon is to be emitted by the scintillator, absorbed by the Y11 WLS fiber, emitted
from the fiber, and finally detected by the SiPM.
Summary of Materials
The full list of materials to be ordered is as follows:
Material Size Quantity
EJ-200 Plastic Scintillator 28x28 cm tile ; 0.5 cm thick 3
EJ-200 Plastic Scintillator 28x28 cm tile ; 1 cm thick 3
Y-11 WLS Fibers 1 mm 6 meters
Y-11 WLS Fibers 0.5 mm 6 meters
Hamamatsu MPPC S12572 3x3 mm 3
Hamamatsu MPPC S13360-1350CS(3050CS) 1.3x1.3 mm (3x3 mm) 3
Driver Circuit for MPPC C12332 n/a 3
Oscilloscope n/a 1
5V Power Source n/a 3
As for more general lab equipment/accessories, we have ordered optical glue, but we may need optically
opaque epoxy if possible. We have ordered reflective paint and optical grease. Finally, We will need a
mechanical structure to support the three scintillators (2 triggers, 1 detector) and mylar wrapping to cover
the plastics.
7
8. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
4. Procedure
We plan on conducting cosmic ray tests using a similar setup as shown in Figure 5. However, our setup
will have notable differences. Namely, we won’t be using any lead plates, we plan on triggering with
two SiPM arrangements above and below our detector, and we will be sequentially testing the three WLS
groove geometries discussed earlier instead of the straight fiber setup in Figure 5. All measurements
will first be carried out on the sigma tile geometry. Then, after these first test results are analyzed, the
proposed building procedure and design will be finer-tuned for all subsequent tests. This approach is more
time-efficient than building and assembling all the design setups at once before understanding the details
of how a single test run may operate.
Figure 5: Cosmic muon telescope used in the prototyping stage of the BEMC.
Whether or not we will trigger with the proposed detector prototype itself or, rather, a previously verified
PMT arrangement has yet to be determined. Regardless, the decision to place the triggers above and
below the detector is for accurate hit determination and analysis. For example, if the top and bottom
triggers detect a signal but the prototype detector in the middle does not, this is indicative of a problem
in the middle detector, and we can correct for this error more quickly. In addition, by changing the size
and/or position of the two triggers, we can determine light collection efficiencies as a function of position,
as discussed in the Measurements section. Geant4 simulations have also been made for the proposed
detector and will serve as a means of comparison for the measurements. The results of these light collection
tests will play a major role in determining which WLS fiber/groove geometries will be employed in the EPD.
After all cosmic data is collected, analyses will be performed to provide estimates for levels of crosstalk,
SiPM detection efficiencies, signal peak-to-noise ratios, luminosities, etc. After the cosmic measurements,
additional tests may be conducted with an radiation source. This would provide another method of
determining which groove geometry (straight, sigma, or spiral) is associated with optimum light collection.
8
9. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
In terms of results, we want to obtain detector efficiencies, for small trigger cross sections, as a function of
discriminator setting. Plots indicating the detector’s time resolution are also desirable, but the statistics
afforded by cosmic/radiation source measurements with an oscilloscope will limit the tightness of bounds
for confidence levels on time resolution. We also hope to obtain plots of dark count/crosstalk for the SiPMs
as well as the full detector apparatus.
We estimate it will take about 4 - 5 weeks to obtain all the necessary materials. After that, it should take
another week for the machine shop to mill the grooves into the scintillating tiles. Then another week or two
will be needed to setup the test bench/equipment in a suitable area. We can then conduct basic functionality
and preliminary cosmic tests on the equipment to ensure all components are operating as expected, which
should take about another week or two. From there we can take the proposed position-dependent hit
measurements. The data collection and analysis process for these measurements should take approximately
4 weeks. In summation, this phase of R&D should be near completion in (using conservative end of
estimates) 14 weeks.
9
10. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
Additional Figures
Figure 6: Various proposed tile-WLS-SiPM geometries. All tiles shown are 1 cm thick. The same designs will also be
tested with 0.5 cm tiles. The trapezoidal figures are 1.25 cm at the base, and 2.8 cm at the top. In the middle
of each trapezoidal figure is a 90% depth cut, leaving 0.1 cm of scintillating material between. The designs in
the center indicate where a SiPM may be attached should we couple the SiPM directly to a scintillating tile.
The lower two designs will likely not be tested due to the very small fiber bending radius needed, but are
shown for reference/completeness.
10
11. Event-Plane and Centrality Detector • R&D Plans • February - March 2015
Figure 7: A side-view on a straight-groove tile design.
References
[1] Photon Counting. http://www.rp-photonics.com/photon_counting.html
[2] BEMC Technical Design Report. https://drupal.star.bnl.gov/STAR/subsys/bemc/documents
[3] Physical Review D Particles, Fields, Gravitation, and Cosmology. Ridge, NY: American Physical Society, July
2012. 305 - 306. Print.
[4] EJ-200 Homepage. http://www.eljentechnology.com/index.php/component/content/article/31-
general/48-ej-200
[5] Hamamatsu MPPC Data Sheet. http://www.hamamatsu.com/jp/en/S12572-050P.html
11