14 research outputs found
Contribution to the T2K experiment at J-PARC, Tokai Design, assembly and installation of the SMRD modules (2008-2009)
No full textThe SMRD detectors (counters) of the T2K experiment are assembled into bigger units called modules. The final design of the modules was elaborated in the Division of Scientific Equipment and Infrastructure Construction (DAI) of the H.Niewodniczański Institute of Nuclear Physics Polish Academy of Sciences (IFJ PAN) in Krakow, Poland. The methods of the module assembly and stabilization inside the T2K magnet were also worked out. Installation procedures of the modules including cable handling were proposed as well. All elements and tools for the assembly, stabilization and installation of 440 SMRD modules had been produced in Poland in 2008. The SMRD modules had been assembled at J-PARC in Tokai and then installed in the T2K experiment in 2009
207. Próba oceny „węzła wartownika” w raku odbytnicy metodą barwnikową
No full textZałożenia i cel pracyCelem badania była próba oznaczania węzła „wartownika” (WW) w raku odbytnicy i ocena wpływu wyniku badania histopatologicznego tego węzła na określenie stopnia zaawansowania klinicznego.Materiał i metodykaDo oceny WW użyto metody opisanej przez Saha i wsp. Błękit metylenowy w ilości 1 ml podawano podśluzówkowo poniżej guza uwidocznionego za pomocą anoskopu. Po otwarciu jamy brzusznej i nacięciu blaszek otrzewnej ściennej miednicy wyszukiwano wybarwionych naczyń i węzłów, które przesyłano w osobnym pojemnik do Zakł. Anat. Pat.WynikiW okresie od czerwca 2002 do czerwca 2003 w Klinice Chirurgii Onkologicznej leczono 17 chorych z rakiem odbytnicy. Do badania kwalifikowano chorych, u których w badaniach USG i TK nie stwierdzono powiększonych regionalnych węzłów chłonnych i przerzutów do wątroby. Węzeł „wartownik” uwidoczniono u 12/17 chorych (70%). W badanej grupie chorych „węzeł wartownik” (3/17) był jedynym węzłem zawierającym przerzuty raka. U dwóch chorych (2/17) przerzuty raka stwierdzono w innych niż „węzeł wartownik” regionalnych węzłach chłonnych. U pozostałych chorych stan „węzła wartownika” (7/12) był identyczny, jak w pozostałych regionalnych węzłach chłonnych.WnioskiUzyskane wyniki badania węzła „wartownika” w raku odbytnicy wymagają dalszych badań w celu ustalenia przydatności tej metody do diagnostyki regionalnych węzłów chłonnych. W przypadku raka odbytnicy metodą bardziej wiarygodną wydaje się być technika barwnikowo-izotopowa
Ocena duktoskopii jako nowej metody diagnostycznej w chorobach piersi na podstawie doświadczeń własnych i danych z piśmiennictwa
No full textNew approach to the conceptual design of STUMM: A module dedicated to the monitoring of neutron and gamma radiation fields generated in IFMIF-DONES
No full textInternational Fusion Materials Irradiation Facility — DEMOsingle bondOriented Neutron Source (IFMIF-DONES) is a planned powerful neutron source, which will generate an intense flux of neutrons (up to ∼1015n/s/cm2) with a fusion-relevant energy spectrum. It will be an accelerator source based on deuteron beam - lithium target reactions. The engineering design of IFMIF-DONES is elaborated in the frame of the Early Neutron Source work package of the EUROfusion consortium. The facility will be dedicated to the irradiation of suitable structural materials planned for the construction of future fusion reactors such as DEMO (Demonstration Fusion Power Plant). Start-up Monitoring Module (STUMM) is designed to monitor radiation and thermal conditions during the commissioning phase of IFMIF-DONES, characterize the produced neutron flux and validate neutronic modeling of the facility. The conceptual design of STUMM is prepared by a team of physicists and engineers from the Institute of Nuclear Physics Polish Academy of Sciences (IFJ PAN) and the National Centre for Nuclear Research (NCBJ), Poland. This paper presents the concept of STUMM, the proposed design of the module, and selected measuring systems
Author Correction: A MHz-repetition-rate hard X-ray free-electron laser driven by a superconducting linear accelerator
No full textThe SMRD subdetector at the T2K near detector station
No full textThe T2K long-baseline neutrino oscillation experiment is running in Japan. The primary goals of the T2K are measurement of the mixing angle 13, and precise measurements of the mixing angle 23 and of the mass difference m2 23. The installation of the near detector complex was completed and first data were already registered. This article presents operation of the Side Muon Range Detector, a component of the Off-Axis near detector. Detector concept and implementation are presented, followed by a description of cosmic muon track reconstruction algorithm and finally current status
Observation of the Crab Nebula with the Single-Mirror Small-Size Telescope stereoscopic system at low altitude
No full textThe Single-Mirror Small-Size Telescope (SST-1M) stereoscopic system is composed of two Imaging Atmospheric Cherenkov Telescopes (IACTs) designed to deliver optimal performance for gamma-ray astronomy in the multi-TeV energy range. It features a 4-m diameter tessellated mirror dish and an innovative SiPM-based camera. Its optical system features a 4-m diameter spherical mirror dish based on the Davies-Cotton design, maintaining a good image quality over a large field of view (FoV), while minimizing optical aberrations. In 2022, two SST-1M telescopes were installed at the Ondřejov Observatory, Czech Republic at an altitude of 510 meters above sea level, collecting data for commissioning and astronomical observations since then. We present the first SST-1M observations of the Crab Nebula, conducted between September 2023 and March 2024 in both mono and stereoscopic modes. During this observation period, 46 hours for the SST-1M-1 and 52 hours for the SST-1M-2 were collected (of which 33 hours were in stereoscopic mode). In this work, we used the Crab Nebula observation to validate the expected performance of the instrument, as evaluated by Monte Carlo (MC) simulations that were carefully tuned to account for instrumental and atmospheric effects. We determined that the energy threshold at the analysis level for the zenith angles below 30° is 1 TeV for mono mode and 1.3 TeV for stereo mode. The energy and angular resolutions were approximately 20% and 0.18° for mono mode and 10% and 0.10° for stereo mode, respectively. We present an off-axis performance assessment of the instrument and a detailed study of the systematic uncertainties. The full simulation results for the telescope and its camera are compared to the data for the first time, enabling a deeper understanding of the SST-1M array performance.Key words: instrumentation: detectors / methods: data analysis / gamma rays: general / ISM: individual objects: Crab Nebul
Observation of the Crab Nebula with the Single-Mirror Small-Size Telescope stereoscopic system at low altitude
No full textThe Single-Mirror Small-Size Telescope (SST-1M) stereoscopic system is composed of two Imaging Atmospheric Cherenkov Telescopes (IACTs) designed to deliver optimal performance for gamma-ray astronomy in the multi-TeV energy range. It features a 4-m diameter tessellated mirror dish and an innovative SiPM-based camera. Its optical system features a 4-m diameter spherical mirror dish based on the Davies-Cotton design, maintaining a good image quality over a large field of view (FoV), while minimizing optical aberrations. In 2022, two SST-1M telescopes were installed at the Ondřejov Observatory, Czech Republic at an altitude of 510 meters above sea level, collecting data for commissioning and astronomical observations since then. We present the first SST-1M observations of the Crab Nebula, conducted between September 2023 and March 2024 in both mono and stereoscopic modes. During this observation period, 46 hours for the SST-1M-1 and 52 hours for the SST-1M-2 were collected (of which 33 hours were in stereoscopic mode). In this work, we used the Crab Nebula observation to validate the expected performance of the instrument, as evaluated by Monte Carlo (MC) simulations that were carefully tuned to account for instrumental and atmospheric effects. We determined that the energy threshold at the analysis level for the zenith angles below 30° is 1 TeV for mono mode and 1.3 TeV for stereo mode. The energy and angular resolutions were approximately 20% and 0.18° for mono mode and 10% and 0.10° for stereo mode, respectively. We present an off-axis performance assessment of the instrument and a detailed study of the systematic uncertainties. The full simulation results for the telescope and its camera are compared to the data for the first time, enabling a deeper understanding of the SST-1M array performance.</p
The SST-1M imaging atmospheric Cherenkov telescope for gamma-ray astrophysics
No full textThe SST-1M is a Small-Sized Telescope (SST) designed to provide a cost-effective and high-performance solution for gamma-ray astrophysics, particularly for energies beyond a few TeV. The goal is to integrate this telescope into an array of similar instruments, leveraging its lightweight design, earthquake resistance, and established Davies-Cotton configuration. Additionally, its optical system is designed to function without a protective dome, allowing it to withstand the harsh atmospheric conditions typical of mountain environments above 2000 m. The SST-1M utilizes a fully digitizing camera system based on silicon photomultipliers (SiPMs). This camera is capable of digitizing all signals from the UV-optical light detectors, allowing for the implementation of various triggers and data analysis methods. We detail the process of designing, prototyping, and validating this system, ensuring that it meets the stringent requirements for gamma-ray detection and performance. An SST-1M stereo system is currently operational and collecting data at the Ondřejov observatory in the Czech Republic, situated at 500 m. Preliminary results from this system are promising. A forthcoming paper will provide a comprehensive analysis of the performance of the telescopes in detecting gamma rays and operating under real-world conditions
Calibration and operation of SiPM-based cameras for gamma-ray astronomy in presence of high night-sky light
No full text
