In the Japanese fiscal year of 2019,
there are nine courses that you can select,
A1 (Dr. Akiyama, Early March 2020)
A2 (Dr. Hattori, July 22-25 2019)
N1 (Drs. Ishidoshiro and Miwa, Early November 2019)
N2 (Dr. Miwa, Early September 2019)
N3 (Dr. Kaneta, Late July - Early August, or September 2019, or February 2020)
N4 (Dr. Matsuda, October - December 2019)
P1 (Dr. Ikeda, February - March 2020)
P3 (Dr. Ishidoshiro, Late February 2020)
P4 (Dr. Shimizu, Late September 2019)
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. Kinitic 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, students will learn superconducting detectors, especially KID detectors, and their wide application. We hope that the students will propose in future the new experiments using superconducting detectors based on this experience.
[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).
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).
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.
[1] Textbook: http://openit.kek.jp/training/2016/fpga/docs/OpenIt_FTC_preparation.pdf
[2] Reference: http://openit.kek.jp/training/2016/fpga/docs/OFTC_ref_note.pdf
The latest version will be announced.
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 understand whole system (detectors, data acquisition, trigger, and analysis frame work) 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.
(1) Construction of a test bench for detector test using cosmic-ray.
(2) Assembling of Multi-gap Resistive Plate Chamber (MRPC) and performance study by cosmic-ray and electron/positron beam.
We plant to use plastic scintillation counters and to analyze data 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.
MRPC is a kind of gaseous ionization detector and developed as a Time-Of-Flight (TOF) detector. It consists of print circuit boards, glass plates, and fishing line as a spacer. You will make MRPC by yourself and investigate its timing resolution and efficiency by cosmic-ray and electron/positron beam.
The recent references are proceedings of “3th Workshop on Resistive Plate Chambers and Related Detectors (RPC2016)” http://iopscience.iop.org/journal/1748-0221/page/extraproc54.
The basic information of MRPC can be found the web page of ALICE experiments: http://aliceinfo.cern.ch/Public/en/Chapter2/Chap2_TOF.html. Also you can find a link to “Technical Design report” in that web page to know detailed information of ALICE-MRPC, https://edms.cern.ch/document/460192/1
Tohoku University has a good environment to study experimental nuclear physics because there are various accelerators in the campus.
K=110 MeV AVF cyclotron in CYRIC offers you an opportunity to learn the basic knowledge and the skills.
In this course, after taking some lectures to learn principles of the accelerator (ECR ion source, AVF cyclotron), detectors (DSSD, IC, Scintillator), and data acquisition system (VME, ROOT, C/C++), you will participate in an experiment, the purpose of which is searching for new alpha cluster states in excited states of nuclei.
By analyzing the scattering data, you will experience the extraction of the physical quantities. In addition, you may find a new cluster state.
FIG.1: AVF cyclotron.FIG.2: ECR ion source.FIG.3: Experimental setup.
[1] Sector focusing cyclotrons: J. R. Richardson, Progress in Nuclear Techniques and Instrumentation, North-Holland Publishing Co. (1965).
[2] Radiation Detection and Measurement: Glenn F. Knoll, Wiley (2000).
[3] http://www.cyric.tohoku.ac.jp/kenkyu/kasoku.html
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).
