In the Japanese fiscal year of 2024,
there are eleven courses that you can select,
A1 (Dr. Akiyama, March 2025)
A2 (Dr. Hattori, Summer 2024)
A3 (Dr. Hattori, Second semester)
A4 (Dr. Akiyama, Summer 2024)
N1 (Drs. Ishidoshiro and Miwa, November 2024)
N2 (Dr. Miwa, Summer 2024)
N3 (Dr. Kaneta, Second semester)
P4 (Dr. Shimizu, Summmer 2024)
P5 (Drs. Ichikawa and Berns, Summer 2024)
P6 (Dr. Kishimoto, Summer 2024)
P7 (Dr. Ishidoshiro, Winter 2025)
The scintillation detection is a widely-used technique in foremost large-scale experiments in the world, relatively cost-effective and multipurpose, so there has been made ongoing efforts on various developments to improve the experimental sensitivities. Actually, a large liquid scintillator detector (KamLAND) has established a new world record in the neutrino mass sensitivity utilizing a unique low-background technique developed in Tohoku University.
In this experiment, you will learn the principal and the device design of the scintillation detection in lectures and experiments, and master the practical technique adaptable to the particle and nuclear physics experiments in the future. This course consists of lectures and experiments in 4 days, containing the following items, understanding of light-output and transfer mechanism, particle identification, measurement of neutron capture time, data acquisition and analysis.
[1] Measurement principle: Principle of liquid scintillation spectrometry, National Diagnostics (2004).
[2] Measurement of time constant, particle identification: Application example for elementary particle experiment: P. Lombardi et al., Nucl. Inst. Meth. A 701 133 (2013).
[3] Application plan for large neutrino experiment: M. Wurm et al., Astropart. Phys. 35, 685 (2012).
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 assemble single photon avalance diode (SPAD) for 1550 nm photon detection
2. to start up a polarization-entangled 1550 nm-photon source
3. construct a fiber-based polarization beam splitter and to confirm the entanglement of two photons from the source.
Technologies on superconductor and microwave technology are widely used in experiments on particle physics and astroparticle physics.
One example is microwave resonant cavities and superconducting magnets used in accelerators, where particles are accelerated in a microwave cavity and their trajectories are bent by a superconducting magnet.
In another example, the search for dark matter candidate particles called axions uses superconducting microwave detectors and powerful superconducting magnets.
However, while the applications of both superconducting and microwave technologies are expanding in the fields of elementary particles and atomic nuclei, it cannot be said that there are many opportunities to learn them.
This course provides opportunities to use them.
As mentioned above, microwave technology and superconducting technology are very important factors.
In this course, you will learn basic but practically important applications using a superconducting microwave cavity.
Microwave technology and particle physics
Basic of microwave and microwave cavity
Transmission (S21) measurement of a cavity
Simulation study on coupling between a cavity and a waveguide to feed microwave into cavity
In recent years, SoC (System on a Chip) that integrates FPGA and CPU has been used in a wide range of fields. Modern SoCs also include high-speed ADCs and DACs. These SoCs are used in radio astronomy, digital radio, quantum computer control, and so on. These developments require knowledge of AXI, DMA, Linux, etc., in addition to conventional FPGA development. Arbitrary waveform generation function and spectrum measurement on SoC are treated as examples.In this course, you will learn the basics of SoC, AXI and DMA handling. You will develop the code for data taking from front-end to a host computer. You are strongly recommended to get the FPGA training course 1 before getting this course.
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.
In this lecture, we aim to obtain knowledge and the experience of pixelated photon detectors (MPPC is the one of the pixelated photon detector produced by Hamamatsu photonics) which are widely used in the particle and nuclear experimental fields. We expect that students understand the basic features of MPPC and also learn how to operate multi MPPCs by operating multi MPPCs attached to a scintillator hodoscope.
A semiconductor photodetector, MPPC, consists of a large number of pixels of avalanche photo diode (APD) in the sensitive area. The MPPC signal is created as the sum of the fired APD pixels. By operating each APD in the Geiger mode, MPPC can have enough gain to detect 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, you will acquire the skills to operate multi MPPCs using the EASIROC board developed for this purpose. First, we evaluate the basic performance and features of MPPC such as the relation between the operation voltage and signal gain. Then, we proceed to read out the scintillator hodoscope array by MPPC. In this detector, wavelength-shifting (WLS) fibers are embedded in the holes drilled in 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 the X direction and 8 segments for the Y direction. We try to read out the 128 channels of MPPCs by EASIROC board. As an advanced course, we try to measure the angular distribution of comic ray or the lifetime 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.Measure 21 cm emission line (1.4204GHz at rest frame) from neutral hydrogen in the Galactic disk with radio spectroscopic measurement using hand made antenna and extract information of the Galactic rotation from the line features. Simultaneously, try to measure spectrum feature of the CMB
(its shape and possibly temperature).
2.Learn what the following simulators can do and get used to manipulate them.
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.
2-4. LightTools: ray tracing simulator for any kind of optical system.
Photo is the measurement system. Up to now, detection of 21 cm line has been confirmed
only toward the Cygnus constellation. I pointed the antenna toward Auriga and Orion but failed to detect although some broad band excess emission is seen. The Cygnus is available at early morning (for example 6 -4 AM April) and night (8-6 PM October). So if you are willing to perform observation during the comfortable season, I have to insist you come to university in out of working time. From November to March it is available at around 5 PM to 9 AM. You are able to perform observation during the working time. However, it is very cold and strong wind from the Zao makes you trouble. I strongly recommend you to choose some day during the comfortable season. Whether or not we are able to perform observation depends weather condition. So flexible respond on setting the date is required.
On the simulation, if you are willing to work on your research with some of these simulators, please let me know. You are able to get access right to manipulate them after the course under the condition that you follow the certain rules.
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 dataset. In the final part, hands-on session for deep learning application to handle large amount of image data will be made.
Textbook and References
[1] General background reading for inverse problems:"Discrete Inverse Problems -Insight and Algorithms", Per Chistain Hansen
Contact → Haruhiko Miyake
Office: Annex I-03 Rm. 121, Research Center for Neutrino Science, Tohoku University
Mail: miyake_at_awa.tohoku.ac.jp
Tel: 022-795-6727
