In the Japanese fiscal year of 2023,
there are eleven courses that you can select,
A1 (Dr. Akiyama, March 2024)
A2 (Dr. Hattori, Summer 2023)
A3 (Dr. Hattori, Second semester)
A4 (Dr. Akiyama, Summer 2023)
N1 (Drs. Ishidoshiro and Miwa, November 2023)
N2 (Dr. Miwa, August - September 2023)
N3 (Dr. Kaneta, Second semester)
P1 (Dr. Ikeda, Second semester)
P3 (Dr. Ishidoshiro, February-March 2024)
P4 (Dr. Shimizu, Held in even-numbered financial years)
P5 (Drs. Ichikawa and Nakamura, Summer 2023)
P6 (Dr. Kishimoto, Summer 2023)
P7 (Dr. Ishidoshiro, Held in even-numbered financial years)
This class will give a basic overview on the main characteristics of the Geant4 Monte Carlo toolkit. Theoretical lessons will be coupled to practical exercises that will give the possibility to the student to move the first steps with the code, from the installation, to the run of a simple application.
GPPU prepares a laptop linux PC with geant4 installation.
Students will learn basic geant4 coding method (running geant4, geometry construction, primary particles definition, physics lists definition and scoring results) with lectures, write simple example codes by themselves, and analyzing the Monte Carlo results. Finally, students will make simple Monte Carlo simulation and present their simulation results. This class will help students to make and analyze their own Monte Carlo simulations.
[1] GEANT4 – a simulation toolkit: S. Agostinelli et al., Nuclear Instruments and Methods in Physics Research A, 506, 250-303 (2003).
[2] http://geant4.web.cern.ch/geant4/support/userdocuments.shtml
Superconducting detectors are extremely sensitive and have a wide variety of application from particle and nuclear physics to quantum measurement and biology. However, it is difficult to integrate into large arrays like a CCD camera. Kinetic Inductance Detectors (KIDs) provide a promising solution to produce the large array. Several KID arrays have been constructed for astronomical observations and TeraHertz imaging.
Research Center for Neutrino Science in Tohoku University is developing KID arrays for next generation dark matter and double-beta decay experiments. Using that facility, the students will learn basics of superconductor, electronics, cryocooler, digital signal processing, data acquisition system and data analysis from detector characterization and response measurements of cosmic rays and/or X rays.
[1] KID detector: P. K. Day et al., Nature 425, 817 (2003).
[2] KID detector: S. Doyle et al., J. Low Temp. Phys., 155, 530 (2008).
[3] Application example for elementary particle experiment: E. S. Battistelli et al., Eur. Phys. J. C 75 53 (2015).
[4] Application example for space observation: S. Oguri et al., J. Low Temp. Phys. 184, 786 (2016).
In this course, you will learn about single near-infrared photon detection, fiber-basedoptomechanics and the well-known strange phenomenon in quantum mechanics.
The ultimate goal of this project is to observe ‘wavefunction collapse’ of photonpolarization by decoherence of the entangled-photon. The equipments to be used are apolarization entangled 1550 nm photon Source, single-photon avalanche diode and fiberoptmechanics etc.In this year, we aim
1. to detect single 1550 nm-wavelength photonand.
2. construct a fiber-based polarization beam splitter and to confirm the entanglement oftwo photons from the source.
Microwave plays important roles in experimental particle physics. The most typical one is accelerator cavity and in recent years, microwave measurements themselves are the observables, such as CMB and dark matter search for axion/hidden photon. In this course, the students acquire basic knowledge of microwave and some measurement techniques through an experiment on a superconducting microwave cavity. The students also get knowledge on the super conductor.
Microwaves have been used in particle physics and astro-particle physics. One of the traditional examples is microwave accelerator cavity, and newer one is a experimental search for Axion, dark photons, etc. In this course, we will conduct basic experiments on a superconducting microwave cavity, which is used in the above two examples, and learn their principles and applications.
Microwave technology and particle physics
Basic of microwave and microwave cavity
Experimental setups (Vector Network Analyzer and Cryostat)
Transmission (S21) measurement of a superconducting cavity
Field-Programmable Gate Array (FPGA) is one of key components for digital signal processing in the experiments of particle and nuclear physics. For the development of FPGA circuits, knowledge of digital circuits and implementation methods to FPGA is required. This course focus to introduce the latter experience.
In this course, we will use Xilinx Artix-7 FPGA with Vivado. The students are expected to install Vivado on their computers before the course. We do not recommend to use virtual machine.
The new photon sensor, MPPC, has many pixels of avalanche photo diode (APD) in the sensitive area and the MPPC signal is the sum of all fired APD. By operating each APD in the Geiger mode, MPPC can have an enough large gain to detect a single photon. The sensitive area of MPPC is rather small (typical size is 1 x 1 mm2). However, MPPC can be operated in the magnetic field and its cost is rather low. Therefore MPPC is one of the best photon sensors to read out fine segmented scintillation detectors such as scintillation fiber detector.
In this lecture, we obtain the skill to operate multi MPPCs by using the EASIROC board which was developed for this purpose. At first, we evaluate the basic performance and features of MPPC such as the relation between the operation voltage and signal gain. Then, we move to the readout of the scintillator hodoscope array with MPPC.
In this detector, a wave length shifting (WLS) fiber is embedded in the hole made on the surface of the scintillator. The scintillator hodoscope array consists of 128 scintillators with WLS fibers and has a layer configuration of 8 segments for X direction and 8 segments for Y direction. We try to read out the 128 channels of MPPCs with EASIROC board. As an advanced course, by making the special trigger with FPGA module, we try to measure the angular distribution of comic ray or the life time of the cosmic ray muon.
[1] 次世代光検出器Pixelated Photon Detector : 生出秀行、音野瑛俊、山下了、日本物理学会誌 第66巻第01号 p.20.
[2] A beam position fiber counter with scintillation fibers and multi-pixel photon counter for high intensity beam operation: R. Honda et al., Nucl. Inst. Meth A 787 157 (2015).
Recent high energy particle physics, like Large Hadron Collider (LHC) experiment at CERN, has a few hundred to a few thousand people in the collaboration. The tasks are separated to specialist, and it is difficult to underst and whole system (detectors, data acquisition, trigger,and analysis framework) by one person. On the other hand, the experimental physicist in elementary particle/nuclear physics filed should have an experience of construction of test bench for detector test. The knowledge will be requisite to design an experiment and to be a group leader. You will learn the following items in this course.
Construction of a test bench for detector test using cosmic ray.
Assembling of a plastic scintillator hodoscope and silicon photomultiplier (SiPM)
Performance test of timing resolution by cosmic ray.
We plan to analyze the Time-of-Flight (TOF) information from three hodoscopes to evaluate timing resolution. The data on VME module is a binary data and need to know how to treat those data on memory. Using a simple program written by C/C++, you will learn how to access VME memory. ROOT which is a framework for data processing and born at CERN will be used for analyses. SiPM is a solid-state photomultiplier comprised of a high-density matrix of Geiger mode-operated avalanche photodiodes. We had been used Photomultiplier tube (PMT) for the photon detection in many years. The normal PMT has a weakness in that it could not operate in a magnetic field. Because of silicon sensor, SiPM can be operated in a magnetic field. Additionally, SiPM has the advantage of being small.
Optical systems for observations of the universe are always affected by aberrations caused by various origins in the systems. Moreover, ground-based observations are affected by aberrations caused by fluctuation and turbulence in the atmosphere. Due to the aberrations, object images on a detector will be distorted from the ideal diffraction-limited pattern. Because observations of the universe are moving toward higher spatial resolution with larger lens/mirror/dish, understanding of the aberrations becomes more critical in the observations not only in the optical/visible wavelength, but also in the UV, IR, and mm wavelengths.
In this course, at first the relation between aberrations in an image and distortions in the optical wavefront is explained through Fourier optics as a lecture, then participants will conduct an optical experiment to measure the distorted optical wavefront. Obtained images are analyzed through your own C programs, and the distortion in the measured wavefront will be evaluated.
FIG. Examples of wavefront sensor images (left) and estimated optical wavefronts from the images (right). The sensor images are analyzed with your own code to estimate the distorted wavefront.
[1] General background: “OPTICS”, Hecht
[2] Fourier optics: “Introduction to Fourier Optics”, Goodman
[3] Wavefront measurements: “Principles of Adaptive Optics”, Tyson
[4] Adaptive optics application to the astronomy: “Adaptive Optics for Astronomy”, Davies, R., and Kasper, M. 2012, ARA&A, 50, 305
MP-FTS is a broad band absolute spectrometer which has played important role in wide field of astronomy, cosmology and calibrating detector systems in the wave bands longer than far infrared wave bands.
The FIRAS instrument mounted on COBE satellite[3] is one of the most famous applications of MP-FTS.
It measured spectrum of the cosmic microwave background (CMB) radiation and showed that it follows the perfect black body spectrum with temperature of 2.725K.
This result has confirmed that our universe has been evolved following the description of the standard big band theory.
A photo of the MP-FTS which is used in this experiment is shown in right panel.
MP-FTS does not lose value and is still active in observational astronomy and cosmology fields.
In this course, the application of the MP-FTS to the measurements of the frequency dependence of complex dielectric constants of samples against millimeter wave at room temperature and liquid Nitrogen temperature is experienced.
Millimeter wave high sensitive bolometer with Nitrogen Trans Doped Germanium (NTD-Ge) semiconductor thermistor is used as detector.
A photo of inside of detector cryostat, which is wet dwar, is shown in left panel. Scenery of the measurement is shown in right panel.
An example of the sample measurement auto-correlation fringe is shown in left panel.
An example Obtained frequency dependence of the transmittance of a sample against millimeter waves is shown in right panel.
Beat signals found in the fringe and sinusoidal pattern found in the transmittance are caused by Fabry-Perot intereference effect.
By fitting the transmittance, refractive index and absorption coefficient, that is real and imaginary part of dielectric constant, are obtained. Textbook and References
[1] MP-FTS: Martin,D.H. and Puplett,E., Infrared Phys., 10, 105 (1969).
[2] Detector: G.H.Rieke, Detection of light, Cambridge Univ. Press, 1994.
[3] Application example for cosmology: J.C.Mathor et al., ApJ, 420, 439 (1994).
[4] Optics: M.Born and E.Wolf, Principles of Optics, Sections 1 and 7 (1974).
Following are the goals of the study.
1.Fundamental of sky temperature measurement at microwave (11GHz) and measure 21 cm
emission line from neutral hydrogen in Galactic disk with spectroscopic measurement in 1-2 GHz.
2.Become able to use one of following simulation methods to treat electromagnetic wave transportation.
2-1. CST: Obtain the beam pattern and other optical features of the system which has the comparable size of the wavelength of the EM wave based on Physical Optics.
2-2. GRASP: Obtain the beam pattern of the optical system for which the size of the system is much larger than the wavelength of the EM wave based on Quasi Optics.
2-3. Sonnet: high frequency electromagnetic wave transportation simulation code for 2 dimensional system.
At the first and second day, thema 1 measurement is performed.
Following days simulation from one of thema listed in thema 2 is performed. Textbook and References
With the spread of CPUs with multi cores and GPUs with many cores, parallel computing has become a popular means of speeding up scientific calculations. With the development of the fast and many elements measurement systems, amount of data necessary to be reduced exponentially growing for various scientific experiments. The increase of the amount of data also increase the size of the problem needs to be solved. Furthermore, more complicated calculations are applied to the massive data to reflect the details of the real experiments. In order to reduce such large amount of raw data and apply more sophisticated analysis in a realistic time scale, parallel computing has been a cost effective choice.
In this lecture, the background of the parallel computing is introduced, then the parallel computing methods with multi core CPUs and GPGPUs are discussed. For the parallel computing with multi-core CPU and GPGPU, coding with OpenMP and CUDA environments are explained, respectively. After testing the programming environment, two topics are discussed as the application of the parallel computing: 1) analyzing image data, and 2) solving inverse problem with large number of datase
Textbook and References
[1] General background reading for inverse problems:"Discrete Inverse Problems -Insight and Algorithms", Per Chistain Hansen
Contact → Hideyoshi Ozaki
Office: Annex I-03 Rm. 121, Research Center for Neutrino Science, Tohoku University
Mail: ozaki_at_awa.tohoku.ac.jp
Tel: 022-795-6727
