Updated on 2024/04/19

写真a

 
OKUMURA Akira
 
Organization
Institute for Space-Earth Environmental Research Division for Cosmic Ray Research Lecturer
Graduate School
Graduate School of Science
Title
Lecturer

Degree 2

  1. 博士(理学) ( 2009.9   東京大学 ) 

  2. 修士(理学) ( 2005.3   東京大学 ) 

Research Interests 2

  1. ガンマ線天文学

  2. 宇宙線物理学

Research Areas 2

  1. Natural Science / Experimental studies related to particle-, nuclear-, cosmic ray and astro-physics

  2. Natural Science / Astronomy

Research History 9

  1. Nagoya University   Institute for Space-Earth Environmental Research   Lecturer

    2018.3

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    Country:Japan

  2. Nagoya University   Institute for Space-Earth Environmental Research   Associate Professor

    2015.10 - 2018.2

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    Country:Japan

  3. Max-Planck-Institut für Kernphysik   Guest Scientist

    2015.4 - 2016.3

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    Country:Germany

  4. University of Leicester   JSPS Fellow

    2013.4 - 2015.3

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    Country:United Kingdom

  5. Nagoya University   Solar-Terrestrial Environment Laboratory   Associate Professor

    2012.9 - 2015.9

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    Country:Japan

  6. Nagoya University, JSPS Fellow

    2011.10 - 2012.8

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    Country:Japan

  7. ISAS/JAXA, JSPS Fellow

    2010.4 - 2011.9

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    Country:Japan

  8. SLAC National Accelerator Laboratory, Visitting Researcher

    2010.4 - 2011.9

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    Country:United States

  9. The University of Tokyo, Project Researcher

    2009.10 - 2010.3

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    Country:Japan

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Education 3

  1. The University of Tokyo   Graduate School, Division of Science

    - 2009.9

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    Country: Japan

  2. The University of Tokyo   Graduate School, Division of Science

    2003.4 - 2005.3

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    Country: Japan

  3. The University of Tokyo   Faculty of Science

    1999.4 - 2003.3

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    Country: Japan

Professional Memberships 2

  1. 日本物理学会

  2. 日本天文学会

 

Papers 122

  1. Constraints on axion-like particles with the Perseus Galaxy Cluster with MAGIC

    Abe, H; Abe, S; Abhir, J; Acciari, VA; Agudo, I; Aniello, T; Ansoldi, S; Antonelli, LA; Engels, AA; Arcaro, C; Artero, M; Asano, K; Baack, D; Babic, A; Baquero, A; de Almeida, UB; Barrio, JA; Batkovic, I; Baxter, J; González, JB; Bednarek, W; Bernardini, E; Bernete, J; Berti, A; Besenrieder, J; Bigongiari, C; Biland, A; Blanch, O; Bonnoli, G; Bosnjak, Z; Burelli, I; Busetto, G; Campoy-Ordaz, A; Carosi, A; Carosi, R; Carretero-Castrillo, M; Castro-Tirado, AJ; Ceribella, G; Chai, Y; Cifuentes, A; Cikota, S; Colombo, E; Contreras, JL; Cortina, J; Covino, S; D'Amico, G; D'Elia, V; Da Vela, P; Dazzi, F; De Angelis, A; De Lotto, B; Del Popolo, A; Delgado, J; Mendez, CD; Depaoli, D; Di Pierro, F; Di Venere, L; Prester, DD; Donini, A; Dorner, D; Doro, M; Elsaesser, D; Emery, G; Escudero, J; Fariña, L; Fattorini, A; Foffano, L; Font, L; Fukami, S; Fukazawa, Y; López, RJG; Garczarczyk, M; Gasparyan, S; Gaug, M; Paiva, JGG; Giglietto, N; Giordano, F; Gliwny, P; Godinovic, N; Grau, R; Green, D; Green, JG; Hadasch, D; Hahn, A; Hassan, T; Heckmann, L; Herrera, J; Hrupec, D; Hütten, M; Imazawa, R; Inada, T; Iotov, R; Ishio, K; Martínez, IJ; Jormanainen, J; Kerszberg, D; Kluge, GW; Kobayashi, Y; Kouch, PM; Kubo, H; Kushida, J; Lezáun, ML; Lamastra, A; Leone, F; Lindfors, E; Linhoff, L; Lombardi, S; Longo, F; López-Coto, R; López-Moya, M; López-Oramas, A; Loporchio, S; Lorini, A; Fraga, BMD; Majumdar, P; Makariev, M; Maneva, G; Mang, N; Manganaro, M; Mangano, S; Mannheim, K; Mariotti, M; Martínez, M; Martínez-Chicharro, M; Mas-Aguilar, A; Mazin, D; Menchiari, S; Mender, S; Miceli, D; Miener, T; Miranda, JM; Mirzoyan, R; González, MM; Molina, E; Mondal, HA; Moralejo, A; Morcuende, D; Nakamori, T; Nanci, C; Nava, L; Neustroev, V; Nickel, L; Rosillo, MN; Nigro, C; Nikolic, L; Nilsson, K; Nishijima, K; Ekoume, TN; Noda, K; Nozaki, S; Ohtani, Y; Okumura, A; Otero-Santos, J; Paiano, S; Palatiello, M; Paneque, D; Paoletti, R; Paredes, JM; Pavlovic, D; Persic, M; Pihet, M; Pirola, G; Podobnik, F; Moroni, PGP; Prandini, E; Principe, G; Priyadarshi, C; Rhode, W; Ribó, M; Rico, J; Righi, C; Sahakyan, N; Saito, T; Satalecka, K; Saturni, FG; Schleicher, B; Schmidt, K; Schmuckermaier, F; Schubert, JL; Schweizer, T; Sciaccaluga, A; Sitarek, J; Sliusar, V; Sobczynska, D; Spolon, A; Stamerra, A; Striskovic, J; Strom, D; Strzys, M; Suda, Y; Suutarinen, S; Tajima, H; Takahashi, M; Takeishi, R; Tavecchio, F; Temnikov, P; Terauchi, K; Terzic, T; Teshima, M; Tosti, L; Truzzi, S; Tutone, A; Ubach, S; van Scherpenberg, J; Acosta, MV; Ventura, S; Verguilov, V; Viale, I; Vigorito, CF; Vitale, V; Vovk, I; Walter, R; Will, M; Yamamoto, T

    PHYSICS OF THE DARK UNIVERSE   Vol. 44   2024.5

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Physics of the Dark Universe  

    Axion-like particles (ALPs) are pseudo-Nambu–Goldstone bosons that emerge in various theories beyond the standard model. These particles can interact with high-energy photons in external magnetic fields, influencing the observed gamma-ray spectrum. This study analyzes 41.3 h of observational data from the Perseus Galaxy Cluster collected with the MAGIC telescopes. We focused on the spectra the radio galaxy in the center of the cluster: NGC 1275. By modeling the magnetic field surrounding this target, we searched for spectral indications of ALP presence. Despite finding no statistical evidence of ALP signatures, we were able to exclude ALP models in the sub-micro electronvolt range. Our analysis improved upon previous work by calculating the full likelihood and statistical coverage for all considered models across the parameter space. Consequently, we achieved the most stringent limits to date for ALP masses around 50 neV, with cross sections down to gaγ=3×10−12 GeV−1.

    DOI: 10.1016/j.dark.2024.101425

    Web of Science

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  2. The variability patterns of the TeV blazar PG 1553 + 113 from a decade of MAGIC and multiband observations

    Abe H., Abe S., Abhir J., Acciari V.A., Agudo I., Aniello T., Ansoldi S., Antonelli L.A., Arbet Engels A., Arcaro C., Artero M., Asano K., Baack D., Babić A., Baquero A., Barres de Almeida U., Batković I., Baxter J., Becerra González J., Bernardini E., Bernete J., Berti A., Besenrieder J., Bigongiari C., Biland A., Blanch O., Bonnoli G., Bošnjak , Burelli I., Busetto G., Campoy-Ordaz A., Carosi A., Carosi R., Carretero-Castrillo M., Castro-Tirado A.J., Chai Y., Cifuentes A., Cikota S., Colombo E., Contreras J.L., Cortina J., Covino S., D’Amico G., D’Elia V., Da Vela P., Dazzi F., De Angelis A., De Lotto B., Del Popolo A., Delfino M., Delgado J., Delgado Mendez C., Depaoli D., Di Pierro F., Di Venere L., Dominis Prester D., Donini A., Dorner D., Doro M., Elsaesser D., Emery G., Escudero J., Fariña L., Fattorini A., Foffano L., Font L., Fukami S., Fukazawa Y., García López R.J., Gasparyan S., Gaug M., Giesbrecht Paiva J.G., Giglietto N., Giordano F., Gliwny P., Grau R., Green J.G., Hadasch D., Hahn A., Heckmann L., Herrera J., Hovatta T., Hrupec D., Hütten M., Imazawa R., Inada T., Iotov R., Ishio K., Jimenez Martínez I., Jormanainen J., Kerszberg D., Kluge G.W., Kobayashi Y., Kouch P.M., Kubo H., Kushida J., Láinez Lezáun M., Lamastra A., Leone F., Lindfors E.

    Monthly Notices of the Royal Astronomical Society   Vol. 529 ( 4 ) page: 3894 - 3911   2024.4

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Monthly Notices of the Royal Astronomical Society  

    PG 1553 + 113 is one of the few blazars with a convincing quasi-periodic emission in the gamma-ray band. The source is also a very high energy (VHE; >100 GeV) gamma-ray emitter. To better understand its properties and identify the underlying physical processes driving its variability, the MAGIC Collaboration initiated a multiyear, multiwavelength monitoring campaign in 2015 involving the OVRO 40-m and Medicina radio telescopes, REM, KVA, and the MAGIC telescopes, Swift and Fermi satellites, and the WEBT network. The analysis presented in this paper uses data until 2017 and focuses on the characterization of the variability. The gamma-ray data show a (hint of a) periodic signal compatible with literature, but the X-ray and VHE gamma-ray data do not show statistical evidence for a periodic signal. In other bands, the data are compatible with the gamma-ray period, but with a relatively high p-value. The complex connection between the low- and high-energy emission and the non-monochromatic modulation and changes in flux suggests that a simple one-zone model is unable to explain all the variability. Instead, a model including a periodic component along with multiple emission zones is required.

    DOI: 10.1093/mnras/stae649

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  3. Silicon photomultipliers for the SST camera of the Cherenkov Telescope Array

    Depaoli, D; Lapington, J; Leach, S; Okumura, A; Sofia, I; Tajima, H

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   Vol. 1060   2024.3

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment  

    The Cherenkov Telescope Array Observatory (CTAO) will be the major global observatory for gamma-ray astronomy over the next decade and beyond. It will consist of two arrays of telescopes of different sizes, one for each hemisphere, and will be sensitive to gamma rays in the energy range from a few tens of GeV to hundreds of TeV. The Small-Sized Telescopes (SSTs) are a crucial component of the southern array, as they will extend the sensitivity of the observatory to the highest energies. Their focal plane will be equipped with 2048 Silicon Photomultiplier (SiPM) pixels, each one read independently by a state-of-the-art full waveform sampling readout. These solid-state sensors offer advantages over the traditional photomultiplier tubes, such as lower operating voltage, higher photon detection efficiency, and tolerance to bright illumination. In particular, they are the best choice for a small and compact camera such as the SST one. After a detailed comparative study, LVR3-type SiPMs from Hamamatsu Photonics were selected, with an active area of 6 mm × 6 mm, a microcell of 50 μm and without a protective coating, for optimum performance. The sensors demonstrated to have a higher photon detection efficiency and a lower crosstalk compared to the competitors, alongside a low dark count rate. In this contribution, we present the selection process and the latest measurements performed on the SiPMs mounted on the SST Camera module.

    DOI: 10.1016/j.nima.2023.169047

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  4. Multi-year characterisation of the broad-band emission from the intermittent extreme BL Lac 1ES 2344+514

    Abe, H; Abe, S; Acciari, VA; Agudo, I; Aniello, T; Ansoldi, S; Antonelli, LA; Engels, AA; Arcaro, C; Artero, M; Asano, K; Baack, D; Babic, A; Baquero, A; de Almeida, UB; Batkovic, I; Baxter, J; González, JB; Bernardini, E; Bernete, J; Berti, A; Besenrieder, J; Bigongiari, C; Biland, A; Blanch, O; Bonnoli, G; Bosnjak, Z; Burelli, I; Busetto, G; Campoy-Ordaz, A; Carosi, A; Carosi, R; Carretero-Castrillo, M; Castro-Tirado, AJ; Chai, Y; Cifuentes, A; Cikota, S; Colombo, E; Contreras, JL; Cortina, J; Covino, S; D'Amico, G; D'Ammando, F; D'Elia, V; Da Vela, P; Dazzi, F; De Angelis, A; De Lotto, B; Del Popolo, A; Delfino, M; Delgado, J; Mendez, CD; Depaoli, D; Di Pierro, F; Di Venere, L; Prester, DD; Dorner, D; Doro, M; Elsaesser, D; Emery, G; Escudero, J; Fariña, L; Fattorini, A; Foffano, L; Font, L; Fukami, S; Fukazawa, Y; López, RJG; Gasparyan, S; Gaug, M; Paiva, JGG; Giglietto, N; Giordano, F; Gliwny, P; Grau, R; Green, JG; Hadasch, D; Hahn, A; Heckmann, L; Herrera, J; Hrupec, D; Hütten, M; Imazawa, R; Inada, T; Iotov, R; Ishio, K; Martínez, IJ; Jormanainen, J; Kerszberg, D; Kluge, GW; Kobayashi, Y; Kouch, PM; Kubo, H; Kushida, J; Lezáun, ML; Lamastra, A; Leone, F; Lindfors, E; Linho, L; Lombardi, S; Longo, F; López-Moya, M; López-Oramas, A; Loporchio, S; Lorini, A; Fraga, BMD; Majumdar, P; Makariev, M; Maneva, G; Mang, N; Manganaro, M; Mariotti, M; Martínez, M; Martínez-Chicharro, M; Mas-Aguilar, A; Mazin, D; Menchiari, S; Mender, S; Miceli, D; Miener, T; Miranda, JM; Mirzoyan, R; González, MM; Molina, E; Mondal, HA; Moralejo, A; Morcuende, D; Nakamori, T; Nanci, C; Neustroev, V; Nigro, C; Nikolic, L; Nishijima, K; Ekoume, TN; Noda, K; Nozaki, S; Ohtani, Y; Okumura, A; Otero-Santos, J; Paiano, S; Palatiello, M; Paneque, D; Paoletti, R; Paredes, JM; Pavlovic, D; Persic, M; Pihet, M; Pirola, G; Podobnik, F; Moroni, PGP; Prandini, E; Principe, G; Priyadarshi, C; Rhode, W; Ribó, M; Rico, J; Righi, C; Sahakyan, N; Saito, T; Satalecka, K; Saturni, FG; Schleicher, B; Schmidt, K; Schmuckermaier, F; Schubert, JL; Schweizer, T; Sciaccaluga, A; Sitarek, J; Spolon, A; Stamerra, A; Striskovic, J; Strom, D; Suda, Y; Tajima, H; Takeishi, R; Tavecchio, F; Temnikov, P; Terauchi, K; Terzic, T; Teshima, M; Tosti, L; Truzzi, S; Tutone, A; Ubach, S; van Scherpenberg, J; Ventura, S; Verguilov, V; Viale, I; Vigorito, CF; Vitale, V; Walter, R; Wunderlich, C; Yamamoto, T; Perri, M; Verrecchia, F; Leto, C; Das, S; Chatterjee, R; Raiteri, CM; Villata, M; Semkov, E; Ibryamov, S; Bachev, R; Strigachev, A; Damljanovic, G; Vince, O; Jovanovic, MD; Stojanovic, M; Larionov, VM; Grishina, TS; Kopatskaya, EN; Larionova, EG; Morozova, DA; Savchenko, SS; Troitskiy, IS; Troitskaya, YV; Vasilyev, AA; Chen, WP; Hou, WJ; Lin, CS; Tsai, A; Jorstad, SG; Weaver, ZR; Acosta-Pulido, JA; Carnerero, MI; Carosati, D; Kurtanidze, SO; Kurtanidze, OM; Jordan, B; Ivanidze, RZ; Gazeas, K; Vrontaki, K; Hovatta, T; Liodakis, I; Readhead, ACS; Kiehlmann, S; Zheng, W; Filippenko, AV; Ramazani, VF

    ASTRONOMY & ASTROPHYSICS   Vol. 682   2024.2

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Astronomy and Astrophysics  

    Aims. The BL Lac 1ES 2344+514 is known for temporary extreme properties characterised by a shift of the synchrotron spectral energy distribution (SED) peak energy νsynch;p above 1 keV. While those extreme states have only been observed during high flux levels thus far, additional multi-year observing campaigns are required to achieve a coherent picture. Here, we report the longest investigation of the source from radio to very high energy (VHE) performed so far, focussing on a systematic characterisation of the intermittent extreme states. Methods.We organised a monitoring campaign covering a 3-year period from 2019 to 2021.Morethan ten instruments participated in the observations in order to cover the emission from radio to VHE. In particular, sensitive X-ray measurements by XMM-Newton, NuSTAR, and AstroSat took place simultaneously with multi-hour MAGIC observations, providing an unprecedented constraint of the two SED components for this blazar. Results. While our results confirm that 1ES 2344+514 typically exhibits νsynch;p > 1 keV during elevated flux periods, we also find periods where the extreme state coincides with low flux activity. A strong spectral variability thus happens in the quiescent state, and is likely caused by an increase in the electron acceleration efficiency without a change in the electron injection luminosity. On the other hand, we also report a strong X-ray flare (among the brightest for 1ES 2344+514) without a significant shift of νsynch;p. During this particular flare, the X-ray spectrum is among the softest of the campaign. It unveils complexity in the spectral evolution, where the common harder-when-brighter trend observed in BL Lacs is violated. By combining Swift-XRT and Swift-UVOT measurements during a low and hard X-ray state, we find an excess of the UV flux with respect to an extrapolation of the X-ray spectrum to lower energies. This UV excess implies that at least two regions significantly contribute to the infrared/optical/ultraviolet/X-ray emission. Using the simultaneous MAGIC, XMM-Newton, NuSTAR, and AstroSat observations, we argue that a region possibly associated with the 10 GHz radio core may explain such an excess. Finally, we investigate a VHE flare, showing an absence of simultaneous variability in the 0.3-2 keV band. Using time-dependent leptonic modelling, we show that this behaviour, in contradiction to single-zone scenarios, can instead be explained by a two-component model.

    DOI: 10.1051/0004-6361/202347845

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  5. MAGIC detection of GRB 201216C at z=1.1

    Abe, H; Abe, S; Acciari, VA; Aguda, ; Aniello, T; Ansoldi, S; Antonelli, LA; Engels, AA; Arcaro, C; Artero, M; Asano, K; Baack, D; Babic, A; Baquero, A; de Almeida, UB; Barrio, JA; Batkovic, I; Baxter, J; González, JB; Bednarek, W; Bernardini, E; Bernete, J; Berti, A; Besenrieder, J; Bigongiari, C; Biland, A; Blanch, O; Bonnoli, G; Bosnjak, Z; Burelli, I; Busetto, G; Campoy-Ordaz, A; Carosi, A; Carosi, R; Carretero-Castrillo, M; Castro-Tirado, AJ; Ceribella, G; Chai, Y; Cifuentes, A; Cikota, S; Colombo, E; Contreras, JL; Cortina, J; Covino, S; D'Amico, G; D'Elia, V; Da Vela, P; Dazzi, F; De Angelis, A; De Lotto, B; Del Popolo, A; Delfino, M; Delgado, J; Mendez, CD; Depaoli, D; Di Pierro, F; Di Venere, L; Prester, DD; Donini, A; Dorner, D; Doro, M; Elsaesser, D; Emery, G; Escudero, J; Fariña, L; Fattorini, A; Foffano, L; Font, L; Fukami, S; Fukazawa, Y; López, RJG; Garczarczyk, M; Gasparyan, S; Gaug, M; Paiva, JGG; Giglietto, N; Giordano, F; Gliwny, P; Godinovic, N; Grau, R; Green, D; Green, JG; Hadasch, D; Hahn, A; Hassan, T; Heckmann, L; Herrera, J; Hrupec, D; Hütten, M; Imazawa, R; Inada, T; Iotov, R; Ishio, K; Martínez, IJ; Jormanainen, J; Kerszberg, D; Kluge, GW; Kobayashi, Y; Kouch, PM; Kubo, H; Kushida, J; Lezáun, ML; Lamastra, A; Leone, F; Lindfors, E; Linhoff, L; Lombardi, S; Longo, F; López-Coto, R; López-Moya, M; López-Oramas, A; Loporchio, S; Lorini, A; Lyard, E; Fraga, BMD; Majumdar, P; Makariev, M; Maneva, G; Mang, N; Manganaro, M; Mangano, S; Mannheim, K; Mariotti, M; Martínez, M; Mas-Aguilar, A; Mazin, D; Menchiari, S; Mender, S; Micanovic, S; Miceli, D; Miener, T; Miranda, JM; Mirzoyan, R; González, MM; Molina, E; Mondal, HA; Moralejo, A; Morcuende, D; Nanci, C; Nava, L; Neustroev, V; Rosillo, MN; Nigro, C; Nikolic, L; Nilsson, K; Nishijima, K; Ekoume, TN; Noda, K; Nozaki, S; Ohtani, Y; Okumura, A; Otero-Santos, J; Paiano, S; Palatiello, M; Paneque, D; Paoletti, R; Paredes, JM; Pavletic, L; Pavlovic, D; Persic, M; Pihet, M; Pirola, G; Podobnik, F; Moroni, PGP; Prandini, E; Principe, G; Priyadarshi, C; Rhode, W; Ribó, M; Rico, J; Righi, C; Sahakyan, N; Saito, T; Satalecka, K; Saturni, FG; Schleicher, B; Schmidt, K; Schmuckermaier, F; Schubert, JL; Schweizer, T; Sciaccaluga, A; Sitarek, J; Sliusar, V; Sobczynska, D; Spolon, A; Stamerra, A; Striskovic, J; Strom, D; Strzys, M; Suda, Y; Suutarinen, S; Tajima, H; Takahashi, M; Takeishi, R; Tavecchio, F; Temnikov, P; Terauchi, K; Terzic, T; Teshima, M; Tosti, L; Truzzi, S; Tutone, A; Ubach, S; van Scherpenberg, J; Acosta, MV; Ventura, S; Verguilov, V; Viale, I; Vigorito, CF; Vitale, V; Vovk, I; Walter, R; Will, M; Yamamoto, T; Gomboc, A; Jordana-Mitjans, N; Melandri, A; Mundell, CG; Shrestha, M; Steele, IA

    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY   Vol. 527 ( 3 ) page: 5856 - 5867   2024.1

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Monthly Notices of the Royal Astronomical Society  

    Gamma-ray bursts (GRBs) are explosive transient events occurring at cosmological distances, releasing a large amount of energy as electromagnetic radiation over several energy bands. We report the detection of the long GRB 201216C by the MAGIC telescopes. The source is located at z = 1.1 and thus it is the farthest one detected at very high energies. The emission above 70 GeV of GRB 201216C is modelled together with multiwavelength data within a synchrotron and synchrotron self-Compton (SSC) scenario. We find that SSC can explain the broad-band data well from the optical to the very-high-energy band. For the late-time radio data, a different component is needed to account for the observed emission. Differently from previous GRBs detected in the very-high-energy range, the model for GRB 201216C strongly favours a wind-like medium. The model parameters have values similar to those found in past studies of the afterglows of GRBs detected up to GeV energies.

    DOI: 10.1093/mnras/stad2958

    Web of Science

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  6. Performance of the joint LST-1 and MAGIC observations evaluated with Crab Nebula data

    Abe, H; Abe, K; Abe, S; Acciari, VA; Aguasca-Cabot, A; Agudo, I; Crespo, NA; Aniello, T; Ansoldi, S; Antonelli, LA; Aramo, C; Arbet-Engels, A; Arcaro, C; Artero, M; Asano, K; Aubert, P; Baack, D; Babic, A; Baktash, A; Bamba, A; Larriva, AB; Baroncelli, L; de Almeida, UB; Barrio, JA; Batkovic, I; Baxter, J; González, JB; Bednarek, W; Bernardini, E; Bernardos, MI; Medrano, JB; Berti, A; Besenrieder, J; Bhattacharjee, P; Biederbeck, N; Bigongiari, C; Biland, A; Bissaldi, E; Blanch, O; Bonnoli, G; Bordas, P; Bosnjak, Z; Bulgarelli, A; Burelli, I; Burmistrov, L; Buscemi, M; Busetto, G; Ordaz, AC; Cardillo, M; Caroff, S; Carosi, A; Carosi, R; Carrasco, MS; Carretero-Castrillo, M; Cassol, F; Castro-Tirado, AJ; Cauz, D; Cerasole, D; Ceribella, G; Chai, Y; Cheng, K; Chiavassa, A; Chikawa, M; Chytka, L; Cifuentes, A; Cikota, S; Colombo, E; Contreras, JL; Cornelia, A; Cortina, J; Costantini, H; Covino, S; D'Amico, G; D'Elia, V; Da Vela, P; Dalchenko, M; Dazzi, F; De Angelis, A; de Lavergne, MD; De Lotto, B; De Lucia, M; de Menezes, R; Del Peral, L; Del Popolo, A; Deleglise, G; Delfino, M; Mendez, CD; Mengual, JD; della Volpe, D; Dellaiera, M; Depaoli, D; De Angelis, A; Di Piano, A; Di Pierro, F; Di Pilato, A; Di Tria, R; Di Venere, L; Dominik, RM; Prester, DD; Donini, A; Dorner, D; Doro, M; Díaz, C; Eisenberger, L; Elsässer, D; Emery, G; Escudero, J; Ramazani, VF; Fariña, L; Fattorini, A; Ferrara, G; Ferrarotto, F; Fiasson, A; Foffano, L; Font, L; Coromina, LF; Fröse, S; Fukami, S; Fukazawa, Y; López, RJG; Garcia, E; Garczarczyk, M; Gasbarra, C; Gasparrini, D; Gasparyan, S; Gaug, M; Geyer, D; Paiva, JGG; Giglietto, N; Giordano, F; Gliwny, P; Godinovic, N; Grau, R; Green, D; Green, JG; Gunji, S; Günther, P; Hackfeld, J; Hadasch, D; Hahn, A; Hashiyama, K; Hassan, T; Hayashi, K; Heckmann, L; Heller, M; Llorente, JH; Hirotani, K; Hoffmann, D; Horns, D; Houles, J; Hrabovsky, M; Hrupec, D; Hui, D; Hütten, M; Iarlori, M; Imazawa, R; Inada, T; Inome, Y; Ioka, K; Iori, M; Iotov, R; Ishio, K; Jacquemont, M; Martínez, IJ; Jobst, E; Jormanainen, J; Jurysek, J; Kagaya, M; Karas, V; Katagiri, H; Kataoka, J; Kerszberg, D; Kluge, GW; Kobayashi, Y; Kohri, K; Kong, A; Kouch, PM; Kubo, H; Kushida, J; Lainez, M; Lamanna, G; Lamastra, A; Le Flour, T; Leone, F; Lindfors, E; Linhoff, L; Linhoff, M; Lombardi, S; Longo, F; Loporchio, S; Lorini, A; Bahilo, JL; Luque-Escamilla, PL; Lyard, E; Lezáun, ML; López-Coto, R; López-Moya, M; López-Oramas, A; Fraga, BMD; Majumdar, P; Makariev, M; Mandat, D; Maneva, G; Manganaro, M; Mangano, S; Mang, N; Manicò, G; Mannheim, K; Mariotti, M; Marquez, P; Marsella, G; Martinez, O; Martínez, G; Martínez, M; Martí, J; Mas-Aguilar, A; Maurin, G; Mazin, D; Menchiari, S; Mender, S; Guillen, EM; Micanovic, S; Miceli, D; Miener, T; Miranda, JM; Mirzoyan, R; Mizuno, T; Micanovic, S; González, MM; Molina, E; Mondal, HA; Montaruli, T; Monteiro, I; Moralejo, A; Morcuende, D; Morselli, A; Moya, V; Muraishi, H; Murase, K; Nagataki, S; Nakamori, T; Nanci, C; Neronov, A; Neustroev, V; Nickel, L; Rosillo, MN; Nigro, C; Nikolic, L; Nilsson, K; Nishijima, K; Ekoume, TN; Noda, K; Nosek, D; Nozaki, S; Ohishi, M; Ohtani, Y; Oka, T; Okumura, A; Orito, R; Otero-Santos, J; Paiano, S; Palatiello, M; Paneque, D; Pantaleo, FR; Paoletti, R; Paredes, JM; Pavletic, L; Pech, M; Pecimotika, M; Peresano, M; Persic, M; Pfeiffle, F; Pietropaolo, E; Pihet, M; Pirola, G; Plard, C; Podobnik, F; Poireau, V; Polo, M; Pons, E; Moroni, PGP; Prandini, E; Prast, J; Principe, G; Priyadarshi, C; Prouza, M; Rando, R; Rhode, W; Ribó, M; Rico, J; Righi, C; Rizi, V; Fernandez, GR; Frías, MDR; Sahakyan, N; Saito, T; Sakurai, S; Sanchez, DA; Satalecka, K; Sato, M; Sato, Y; Saturni, FG; Savchenko, V; Schleicher, B; Schmidt, K; Schmuckermaier, F; Schubert, JL; Schussler, F; Schweizer, T; Sciaccaluga, A; Siegert, T; Silvia, R; Sitarek, J; Sliusar, V; Sobczynska, D; Spolon, A; Stamerra, A; Striskovic, J; Strom, D; Strzys, M; Suda, Y; Suutarinen, S; Saric, T; Tajima, H; Takahashi, H; Takahashi, M; Takata, J; Takeishi, R; Tam, PHT; Tanaka, SJ; Tateishi, D; Tavecchio, F; Temnikov, P; Terada, Y; Terauchi, K; Terzic, T; Teshima, M; Tluczykont, M; Tokanai, F; Torres, DF; Tosti, L; Travnicek, P; Truzzi, S; Tutone, A; Ubach, S; Vacula, M; Vallania, P; van Scherpenberg, J; Acosta, MV; Ventura, S; Verguilov, V; Viale, I; Vigliano, A; Vigorito, CF; Visentin, E; Vitale, V; Voutsinas, G; Vovk, I; Vuillaume, T; Acosta, M; Walter, R; Wei, Z; Will, M; Yamamoto, T; Yamazaki, R; Yoshida, T; Yoshikoshi, T; Zywucka, N

    ASTRONOMY & ASTROPHYSICS   Vol. 680   2023.12

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Astronomy and Astrophysics  

    Aims. Large-Sized Telescope 1 (LST-1), the prototype for the Large-Sized Telescope at the upcoming Cherenkov Telescope Array Observatory, is concluding its commissioning phase at the Observatorio del Roque de los Muchachos on the island of La Palma. The proximity of LST-1 to the two MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes makes it possible to carry out observations of the same gamma-ray events with both systems. Methods. We describe the joint LST-1+MAGIC analysis pipeline and used simultaneous Crab Nebula observations and Monte Carlo simulations to assess the performance of the three-telescope system. The addition of the LST-1 telescope allows for the recovery of events in which one of the MAGIC images is too dim to survive analysis quality cuts. Results. Thanks to the resulting increase in the collection area and stronger background rejection, we found a significant improvement in sensitivity, allowing for the detection of 30% weaker fluxes in the energy range between 200 GeV and 3 TeV. The spectrum of the Crab Nebula, reconstructed in the energy range between ∼60 GeV and ∼10 TeV, is in agreement with previous measurements.

    DOI: 10.1051/0004-6361/202346927

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  7. Star tracking for pointing determination of Imaging Atmospheric Cherenkov Telescopes

    Abe, K; Abe, S; Aguasca-Cabot, A; Agudo, I; Crespo, NA; Antonelli, LA; Aramo, C; Arbet-Engels, A; Cornelia, A; Artero, M; Asano, K; Aubert, P; Baktash, A; Bamba, A; Larriva, AB; Baroncelli, L; de Almeida, UB; Barrio, JA; Batkovic, I; Baxter, J; Gonzalez, JB; Bernardini, E; Bernardos, M; Medrano, JB; Berti, A; Bhattacharjee, P; Biederbeck, N; Bigongiari, C; Bissaldi, E; Blanch, O; Bonnoli, G; Bordas, P; Bulgarelli, A; Burelli, ; Burmistrov, L; Buscemi, M; Cardillo, M; Caroff, S; Carosi, A; Cassol, F; Cauz, D; Ceribella, G; Chai, Y; Cheng, K; Chiavassa, A; Chikawa, M; Chytka, L; Cifuentes, A; Contreras, JL; Cortina, J; Costantini, H; Dalchenko, M; De Angelis, A; de Lavergne, MD; De Lotto, B; de Menezes, R; Deleglise, G; Delgado, C; Mengual, JD; della Volpe, D; Dellaiera, M; Di Piano, A; Di Pierro, F; Di Tria, R; Di Venere, L; Diaz, C; Dominik, RM; Prester, DD; Donini, A; Dorner, D; Doro, M; Elsässer, D; Emery, G; Escudero, J; Ramazani, VF; Ferrara, G; Ferrarotto, F; Fiasson, A; Coromina, LF; Fröse, S; Fukami, S; Fukazawa, Y; Garcia, E; Lopez, RG; Gasbarra, C; Gasparrini, D; Geyer, D; Paiva, JG; Giglietto, N; Giordano, F; Giro, E; Gliwny, P; Godinovic, N; Grau, R; Green, D; Green, J; Gunji, S; Guenther, P; Hackfeld, J; Hadasch, D; Hahn, A; Hashiyama, K; Hassan, T; Hayashi, K; Heckmann, L; Heller, M; Llorente, JH; Hirotani, K; Hoffmann, D; Horns, D; Houles, J; Hrabovsky, M; Hrupec, D; Hui, D; Hütten, M; Iarlori, M; Imazawa, R; Inada, T; Inome, Y; Ioka, K; Iori, M; Ishio, K; Jacquemont, M; Martinez, IJ; Jurysek, J; Kagaya, M; Karas, V; Katagiri, H; Kataoka, J; Kerszberg, D; Kobayashi, Y; Kohri, K; Kong, A; Kubo, H; Kushida, J; Lainez, M; Lamanna, G; Lamastra, A; Le Flour, T; Linhoff, M; Longo, F; Lopez-Coto, R; Lopez-Oramas, A; Loporchio, S; Lorini, A; Luque-Escamilla, PL; Majumdar, P; Makariev, M; Mandat, D; Manganaro, M; Manico, G; Mannheim, K; Mariotti, M; Marquez, P; Marsella, G; Marti, J; Martinez, O; Martinez, G; Martinez, M; Mas-Aguilar, A; Maurin, G; Mazin, D; Guillen, EM; Micanovic, S; Miceli, D; Miener, T; Miranda, JM; Mirzoyan, R; Mizuno, T; Gonzalez, MM; Molina, E; Montaruli, T; Monteiro, I; Moralejo, A; Morcuende, D; Morselli, A; Muraishi, H; Murase, K; Nagataki, S; Nakamori, T; Nickel, L; Nievas, M; Nishijima, K; Noda, K; Nosek, D; Nozaki, S; Ohishi, M; Ohtani, Y; Oka, T; Okumura, A; Orito, R; Otero-Santos, J; Palatiello, M; Paneque, D; Pantaleo, FR; Paoletti, R; Paredes, JM; Pech, M; Pecimotika, M; Peresano, M; Pfeiffle, F; Pietropaolo, E; Pirola, G; Plard, C; Podobnik, F; Poireau, ; Polo, M; Pons, E; Prandini, E; Prast, J; Principe, G; Priyadarshi, C; Prouza, M; Rando, R; Rhode, W; Ribo, M; Rizi, V; Fernandez, GR; Saito, T; Sakurai, S; Sanchez, DA; Saric, T; Sato, Y; Saturni, FG; Schleicher, B; Schmuckermaier, F; Schubert, JL; Schussler, F; Schweizer, T; Sato, M; Siegert, T; Silvia, R; Sitarek, J; Sliusar, V; Spolon, A; Striskovic, J; Strzys, M; Suda, Y; Tajima, H; Takahashi, H; Takahashi, M; Takata, J; Takeishi, R; Tam, PHT; Tanaka, SJ; Tateishi, D; Temnikov, P; Terada, Y; Terauchi, K; Terzic, T; Teshima, M; Tluczykont, M; Tokanai, F; Torres, DF; Travnicek, P; Truzzi, S; Tutone, A; Vacula, M; Vallania, P; van Scherpenberg, J; Acosta, MV; Viale, ; Vigliano, A; Vigorito, CF; Vitale, V; Voutsinas, G; Vovk, I; Vuillaume, T; Walter, R; Wei, Z; Will, M; Yamamoto, T; Yamazaki, R; Yoshida, T; Yoshikoshi, T; Zywucka, N

    ASTRONOMY & ASTROPHYSICS   Vol. 679   2023.11

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Astronomy and Astrophysics  

    We present a novel approach to the determination of the pointing of Imaging Atmospheric Cherenkov Telescopes (IACTs) using the trajectories of the stars in their camera s field of view. The method starts with the reconstruction of the star positions from the Cherenkov camera data, taking into account the point spread function of the telescope, to achieve a satisfying reconstruction accuracy of the pointing position. A simultaneous fit of all reconstructed star trajectories is then performed with the orthogonal distance regression (ODR) method. ODR allows us to correctly include the star position uncertainties and use the time as an independent variable. Having the time as an independent variable in the fit makes it better suitable for various star trajectories. This method can be applied to any IACT and requires neither specific hardware nor interface or special data-taking mode. In this paper, we use the Large-Sized Telescope (LST) data to validate it as a useful tool to improve the determination of the pointing direction during regular data taking. The simulation studies show that the accuracy and precision of the method are comparable with the design requirements on the pointing accuracy of the LST (=14''). With the typical LST event acquisition rate of 10 kHz, the method can achieve up to 50 Hz pointing monitoring rate, compared to O(1) Hz achievable with standard techniques. The application of the method to the LST prototype (LST-1) commissioning data shows the stable pointing performance of the telescope.

    DOI: 10.1051/0004-6361/202347128

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  8. Observations of the Crab Nebula and Pulsar with the Large-sized Telescope Prototype of the Cherenkov Telescope Array

    Abe, H; Abe, K; Abe, S; Aguasca-Cabot, A; Agudo, ; Crespo, NA; Antonelli, LA; Aramo, C; Arbet-Engels, A; Arcaro, C; Artero, M; Asano, K; Aubert, P; Baktash, A; Bamba, A; Larriva, AB; Baroncelli, L; de Almeida, UB; Barrio, JA; Batkovic, I; Baxter, J; González, JB; Bernardini, E; Bernardos, MI; Medrano, JB; Berti, A; Bhattacharjee, P; Biederbeck, N; Bigongiari, C; Bissaldi, E; Blanch, O; Bonnoli, G; Bordas, P; Borghese, A; Bulgarelli, A; Burelli, I; Buscemi, M; Cardillo, M; Caroff, S; Carosi, A; Cassol, F; Cauz, D; Ceribella, G; Chai, Y; Cheng, K; Chiavassa, A; Chikawa, M; Chytka, L; Cifuentes, A; Contreras, JL; Cortina, J; Costantini, H; D'Amico, G; Dalchenko, M; De Angelis, A; de Lavergne, MD; de Lotto, B; de Menezes, R; Deleglise, G; Delgado, C; Mengual, JD; della Volpe, D; Dellaiera, M; Depaoli, D; Di Piano, A; Di Pierro, F; Di Tria, R; Di Venere, L; Díaz, C; Dominik, RM; Prester, DD; Donini, A; Dorner, D; Doro, M; Elsässer, D; Emery, G; Escudero, J; Ramazani, VF; Ferrara, G; Ferrarotto, F; Fiasson, A; Coromina, LF; Fröse, S; Fukami, S; Fukazawa, Y; Garcia, E; López, RG; Gasbarra, C; Gasparrini, D; Geyer, F; Paiva, JG; Giglietto, N; Giordano, F; Giro, E; Gliwny, P; Godinovic, N; Grau, R; Green, D; Green, J; Gunji, S; Hackfeld, J; Hadasch, D; Hahn, A; Hashiyama, K; Hassan, T; Hayashi, K; Heckmann, L; Heller, M; Llorente, JH; Hirotani, K; Hoffmann, D; Horns, D; Houles, J; Hrabovsky, M; Hrupec, D; Hui, D; Hütten, M; Iarlori, M; Imazawa, R; Inada, T; Inome, Y; Ioka, K; Iori, M; Ishio, K; Iwamura, Y; Jacquemont, M; Martinez, IJ; Jurysek, J; Kagaya, M; Karas, V; Katagiri, H; Kataoka, J; Kerszberg, D; Kobayashi, Y; Kong, A; Kubo, H; Kushida, J; Lainez, M; Lamanna, G; Lamastra, A; Le Flour, T; Linhoff, M; Longo, F; López-Coto, R; López-Moya, M; López-Oramas, A; Loporchio, S; Lorini, A; Luque-Escamilla, PL; Majumdar, P; Makariev, M; Mandat, D; Manganaro, M; Manicò, G; Mannheim, K; Mariotti, M; Marquez, P; Marsella, G; Martí, J; Martinez, O; Martínez, G; Martínez, M; Marusevec, P; Mas-Aguilar, A; Maurin, G; Mazin, D; Guillen, EM; Micanovic, S; Miceli, D; Miener, T; Miranda, JM; Mirzoyan, R; Mizuno, T; Gonzalez, MM; Molina, E; Montaruli, T; Monteiro, I; Moralejo, A; Morcuende, D; Morselli, A; Mrakovcic, K; Murase, K; Nagai, A; Nagataki, S; Nakamori, T; Nickel, L; Nievas, M; Nishijima, K; Noda, K; Nosek, D; Nozaki, S; Ohishi, M; Ohtani, Y; Oka, T; Okazaki, N; Okumura, A; Orito, R; Otero-Santos, J; Palatiello, M; Paneque, D; Pantaleo, FR; Paoletti, R; Paredes, JM; Pech, M; Pecimotika, M; Peresano, M; Pérez, A; Pietropaolo, E; Pirola, G; Plard, C; Podobnik, F; Poireau, V; Polo, M; Pons, E; Prandini, E; Prast, J; Principe, G; Priyadarshi, C; Prouza, M; Rando, R; Rhode, W; Ribó, M; Rizi, V; Fernandez, GR; Ruíz, JE; Saito, T; Sakurai, S; Sanchez, DA; Saric, T; Sato, Y; Saturni, FG; Schleicher, B; Schmuckermaier, F; Schubert, JL; Schussler, F; Schweizer, T; Arroyo, MS; Silvia, R; Sitarek, J; Sliusar, V; Spolon, A; Striskovic, J; Strzys, M; Suda, Y; Sunada, Y; Tajima, H; Takahashi, H; Takahashi, M; Takata, J; Takeishi, R; Tam, PHT; Tanaka, SJ; Tateishi, D; Tejedor, LA; Temnikov, P; Terada, Y; Terauchi, K; Terzic, T; Teshima, M; Tluczykont, M; Tokanai, F; Torres, DF; Travnicek, P; Truzzi, S; Tutone, A; Uhlrich, G; Vacula, M; Vallania, P; van Scherpenberg, J; Acosta, MV; Verguilov, V; Viale, I; Vigliano, A; Vigorito, CF; Vitale, V; Voutsinas, G; Vovk, I; Vuillaume, T; Walter, R; Will, M; Yamamoto, T; Yamazaki, R; Yoshida, T; Yoshikoshi, T; Zywucka, N; Bernlöhr, K; Gueta, O; Kosack, K; Maier, G; Watson, J

    ASTROPHYSICAL JOURNAL   Vol. 956 ( 2 )   2023.10

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Astrophysical Journal  

    The Cherenkov Telescope Array (CTA) is a next-generation ground-based observatory for gamma-ray astronomy at very high energies. The Large-Sized Telescope prototype (LST-1) is located at the CTA-North site, on the Canary Island of La Palma. LSTs are designed to provide optimal performance in the lowest part of the energy range covered by CTA, down to ≃20 GeV. LST-1 started performing astronomical observations in 2019 November, during its commissioning phase, and it has been taking data ever since. We present the first LST-1 observations of the Crab Nebula, the standard candle of very-high-energy gamma-ray astronomy, and use them, together with simulations, to assess the performance of the telescope. LST-1 has reached the expected performance during its commissioning period—only a minor adjustment of the preexisting simulations was needed to match the telescope’s behavior. The energy threshold at trigger level is around 20 GeV, rising to ≃30 GeV after data analysis. Performance parameters depend strongly on energy, and on the strength of the gamma-ray selection cuts in the analysis: angular resolution ranges from 0.°12-0.°40, and energy resolution from 15%-50%. Flux sensitivity is around 1.1% of the Crab Nebula flux above 250 GeV for a 50 hr observation (12% for 30 minutes). The spectral energy distribution (in the 0.03-30 TeV range) and the light curve obtained for the Crab Nebula agree with previous measurements, considering statistical and systematic uncertainties. A clear periodic signal is also detected from the pulsar at the center of the Nebula.

    DOI: 10.3847/1538-4357/ace89d

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  9. Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants

    Acero, F; Acharyya, A; Adam, R; Aguasca-Cabot, A; Agudo, I; Aguirre-Santaella, A; Alfaro, J; Aloisio, R; Crespo, NA; Batista, RA; Amati, L; Amato, E; Ambrosi, G; Angüner, EO; Aramo, C; Arcaro, C; Armstrong, T; Asano, K; Ascasibar, Y; Aschersleben, J; Backes, M; Baktash, A; Balazs, C; Balbo, M; Ballet, J; Larriva, AB; Martins, VB; de Almeida, UB; Barrio, JA; Bastieri, D; Baxter, JR; Tjus, JB; Benbow, W; Bernardos-Martín, MI; Bernete, J; Berti, A; Bertucci, B; Beshley, V; Bhattacharjee, P; Bhattacharyya, S; Biland, A; Bissaldi, E; Biteau, J; Blanch, O; Bordas, P; Bottacini, E; Bregeon, J; Brose, R; Bucciantini, N; Bulgarelli, A; Capasso, M; Dolcetta, RAC; Caraveo, P; Cardillo, M; Carosi, R; Casanova, S; Cascone, E; Cassol, F; Catalani, F; Cerruti, M; Chadwick, P; Chaty, S; Chen, A; Chernyakova, M; Chiavassa, A; Chudoba, J; Coimbra-Araujo, C; Conforti, V; Contreras, JL; Costa, A; Costantini, H; Cristofari, P; Crocker, R; D'Amico, G; D'Ammando, F; De Angelis, A; De Caprio, V; Dal Pino, EMD; Wilhelmi, ED; de Souza, V; Delgado, C; della Volp, D; Depaoli, D; Di Girolamo, T; Di Pierro, F; Di Tria, R; Di Venere, L; Diebold, S; Djuvsland, JI; Donini, A; Doro, M; Dos Anjos, RDC; Dwarkadas, VV; Einecke, S; Elsässer, D; Emery, G; Evoli, C; Falceta-Goncalves, D; Fedorova, E; Fegan, S; Ferrand, G; Fiandrini, E; Filipovic, M; Fioretti, V; Fiori, M; Foffano, L; Fontaine, G; Fukami, S; Galanti, G; Galaz, G; Gammaldi, V; Gasbarra, C; Ghalumyan, A; Ghirlanda, G; Giarrusso, M; Giavitto, G; Giglietto, N; Giordano, F; Giroletti, M; Giuliani, A; Giunti, L; Godinovic, N; Coelho, JG; Gréaux, L; Green, D; Grondin, MH; Gueta, O; Gunji, S; Hassan, T; Heller, M; Hernández-Cadena, S; Hinton, J; Hnatyk, B; Hnatyk, R; Hoffmann, D; Hofmann, W; Holder, J; Horan, D; Horvath, P; Hrabovsky, M; Hrupec, D; Inada, T; Incardona, F; Inoue, S; Ishio, K; Jamrozy, M; Janecek, P; Martínez, IJ; Jin, W; Jung-Richardt, I; Jurysek, J; Kaaret, P; Karas, V; Katz, U; Kerszberg, D; Khélifi, B; Kieda, DB; Kissmann, R; Kleiner, T; Kluge, G; Kluzniak, W; Knödlseder, J; Kobayashi, Y; Kohri, K; Komin, N; Kornecki, P; Kubo, H; La Palombara, N; Láinez, M; Lamastra, A; Lapington, J; Lemoine-Goumard, M; Lenain, JP; Leone, F; Leto, G; Leuschner, F; Lindfors, E; Liodakis, I; Lohse, T; Lombardi, S; Longo, F; López-Coto, R; López-Moya, M; López-Oramas, A; Loporchio, S; Luque-Escamilla, PL; Macias, O; Mackey, J; Majumdar, P; Mandat, D; Manganaro, M; Manicò, G; Marconi, M; Martí, J; Martínez, G; Martinez, M; Martinez, O; Mello, AJTS; Menchiari, S; Meyer, DMA; Micanovic, S; Miceli, D; Miceli, M; Michalowski, J; Miener, T; Miranda, JM; Mitchell, A; Mode, B; Moderski, R; Mohrmann, L; Molina, E; Montaruli, T; Morcuende, D; Morlino, G; Morselli, A; Mosè, M; Moulin, E; Mukherjee, R; Munari, K; Murach, T; Nagai, A; Nagataki, S; Nemmen, R; Niemiec, J; Nieto, D; Rosillo, MN; Nikolajuk, M; Nishijima, K; Noda, K; Novosyadlyj, B; Nozaki, S; Ohishi, M; Ohm, S; Ohtani, Y; Okumura, A; Olmi, B; Ong, RA; Orienti, M; Orito, R; Orlandini, M; Orlando, E; Orlando, S; Ostrowski, M; Oya, I; Pantaleo, FR; Paredes, JM; Patricelli, B; Pecimotika, M; Peresano, M; Pérez-Romero, J; Persic, M; Petruk, O; Piano, G; Pietropaolo, E; Pirola, G; Pittori, C; Pohl, M; Ponti, G; Prandini, E; Principe, G; Priyadarshi, C; Pueschel, E; Pühlhofer, G; Pumo, ML; Quirrenbach, A; Rando, R; Razzaque, S; Reichherzer, P; Reimer, A; Reimer, O; Renaud, M; Reposeur, T; Ribó, M; Richtler, T; Rico, J; Rieger, F; Rigoselli, M; Riitano, L; Rizi, V; Roache, E; Romano, P; Romeo, G; Rosado, J; Rowell, G; Rudak, B; Sadeh, I; Safi-Harb, S; Saha, L; Sailer, S; Sánchez-Conde, M; Sarkar, S; Satalecka, K; Saturni, FG; Scherer, A; Schovánek, P; Schussler, F; Schwanke, U; Scuderi, S; Seglar-Arroyo, M; Sergijenko, O; Servillat, M; Shang, RY; Sharma, P; Siejkowski, H; Sliusar, V; Slowikowska, A; Sol, H; Specovius, A; Spencer, ST; Spengler, G; Stamerra, A; Stanic, S; Starecki, T; Starling, R; Stolarczyk, T; Pereira, LAS; Suda, Y; Suomijarvi, T; Sushch, I; Tajima, H; Tam, PHT; Tanaka, SJ; Tavecchio, F; Testa, V; Tian, W; Tibaldo, L; Torres, DF; Tothill, N; Vallage, B; Vallania, P; van Eldik, C; van Scherpenberg, J; Vandenbroucke, J; Acosta, MV; Vecchi, M; Vercellone, S; Verna, G; Viana, A; Vignatti, J; Vitale, V; Vodeb, V; Vorobiov, S; Vuillaume, T; Wagner, SJ; Walter, R; White, M; Wierzcholska, A; Will, M; Williams, D; Yang, L; Yoshida, T; Yoshikoshi, T; Zaharijas, G; Zampieri, L; Zavrtanik, D; Zavrtanik, M; Zhdanov, VI; Zivec, M

    ASTROPARTICLE PHYSICS   Vol. 150   2023.8

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Astroparticle Physics  

    The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3 PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The potential to search for hadronic PeVatrons with the Cherenkov Telescope Array (CTA) is assessed. The focus is on the usage of very high energy γ-ray spectral signatures for the identification of PeVatrons. Assuming that SNRs can accelerate CRs up to knee energies, the number of Galactic SNRs which can be identified as PeVatrons with CTA is estimated within a model for the evolution of SNRs. Additionally, the potential of a follow-up observation strategy under moonlight conditions for PeVatron searches is investigated. Statistical methods for the identification of PeVatrons are introduced, and realistic Monte-Carlo simulations of the response of the CTA observatory to the emission spectra from hadronic PeVatrons are performed. Based on simulations of a simplified model for the evolution for SNRs, the detection of a γ-ray signal from in average 9 Galactic PeVatron SNRs is expected to result from the scan of the Galactic plane with CTA after 10 h of exposure. CTA is also shown to have excellent potential to confirm these sources as PeVatrons in deep observations with O(100) hours of exposure per source.

    DOI: 10.1016/j.astropartphys.2023.102850

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  10. Sensitivity of the Cherenkov Telescope Array to TeV photon emission from the Large Magellanic Cloud

    Acharyya, A; Adam, R; Aguasca-Cabot, A; Agudo, I; Aguirre-Santaella, A; Alfaro, J; Aloisio, R; Batista, RA; Amato, E; Angüner, EO; Aramo, C; Arcaro, C; Asano, K; Aschersleben, J; Ashkar, H; Backes, M; Baktash, A; Balazs, C; Balbo, M; Ballet, J; Bamba, A; Larriva, AB; Martins, VB; de Almeida, UB; Barrio, JA; Bastieri, D; Batista, P; Batkovic, I; Baxter, JR; Gonzalez, JB; Tjus, JB; Benbow, W; Bernardini, E; Martín, MIB; Medrano, JB; Berti, A; Bertucci, B; Beshley, V; Bhattacharjee, P; Bhattacharyya, S; Bigongiari, C; Biland, A; Bissaldi, E; Bocchino, F; Bordas, P; Borkowski, J; Bottacini, E; Böttcher, M; Bradascio, F; Brown, AM; Bulgarelli, A; Burmistrov, L; Caroff, S; Carosi, A; Carquín, E; Casanova, S; Cascone, E; Cassol, F; Cerruti, M; Chadwick, P; Chaty, S; Chen, A; Chiavassa, A; Chytka, L; Conforti, V; Cortina, J; Costa, A; Costantini, H; Cotter, G; Crestan, S; Cristofari, P; D'Ammando, F; Dalchenko, M; Dazzi, F; De Angelis, A; De Caprio, V; Dal Pino, EMD; De Martino, D; de Naurois, M; de Souza, V; del Valle, MV; Giler, AGD; Delgado, C; della Volpe, D; Depaoli, D; Di Girolamo, T; Di Piano, A; Di Pierro, F; Di Tria, R; Di Venere, L; Diebold, S; Doro, M; Dumora, D; Dwarkadas, VV; Eckner, C; Egberts, K; Emery, G; Escudero, J; Falceta-Goncalves, D; Fedorova, E; Fegan, S; Feng, Q; Ferenc, D; Ferrand, G; Fiandrini, E; Filipovic, M; Fioretti, V; Foffano, L; Fontaine, G; Fukui, Y; Gaggero, D; Galanti, G; Galaz, G; Gallozzi, S; Gammaldi, V; Garczarczyk, M; Gasbarra, C; Gasparrini, D; Ghalumyan, A; Giarrusso, M; Giavitto, G; Giglietto, N; Giordano, F; Giuliani, A; Glicenstein, JF; Goldoni, P; Coelho, JG; Granot, J; Green, D; Green, JG; Grondin, MH; Gueta, O; Hadasch, D; Hamal, P; Hassan, T; Hayashi, K; Heller, M; Cadena, SH; Hiroshima, N; Hnatyk, B; Hnatyk, R; Hofmann, W; Holder, J; Holler, M; Horan, D; Horvath, P; Hrabovsky, M; Hütten, M; Iarlori, M; Inada, T; Incardona, F; Inoue, S; Iocco, F; Jamrozy, M; Jin, W; Jung-Richardt, I; Jurysek, J; Kantzas, D; Karas, V; Katagiri, H; Kerszberg, D; Knödlseder, J; Komin, N; Kornecki, P; Kosack, K; Kowal, G; Kubo, H; Lamastra, A; Lapington, J; Lemoine-Goumard, M; Lenain, JP; Leone, F; Leto, G; Leuschner, F; Lindfors, E; Lohse, T; Lombardi, S; Longo, F; López-Coto, R; López-Oramas, A; Loporchio, S; Luque-Escamilla, PL; Macias, O; Majumdar, P; Mandat, D; Mangano, S; Manicò, G; Mariotti, M; Marquez, P; Marsella, G; Martí, J; Martin, P; Martínez, M; Mazin, D; Menchiari, S; Meyer, DMA; Miceli, D; Miceli, M; Michalowski, J; Mitchell, A; Moderski, R; Mohrmann, L; Molero, M; Molina, E; Montaruli, T; Moralejo, A; Morcuende, D; Morselli, A; Moulin, E; Moya, V; Mukherjee, R; Munari, K; Muraczewski, A; Nagataki, S; Nakamori, T; Nayak, A; Niemiec, J; Nievas, M; Nikolajuk, M; Nishijima, K; Noda, K; Nosek, D; Novosyadlyj, B; Nozaki, S; Ohishi, M; Ohm, S; Okumura, A; Olmi, B; Ong, RA; Orienti, M; Orito, R; Orlandini, M; Orlando, E; Orlando, S; Ostrowski, M; Oya, I; Pagliaro, A; Palatka, M; Pantaleo, FR; Paoletti, R; Paredes, JM; Parmiggiani, N; Patricelli, B; Pech, M; Pecimotika, M; Persic, M; Petruk, O; Pierre, E; Pietropaolo, E; Pirola, G; Pohl, M; Prandini, E; Priyadarshi, C; Pühlhofer, G; Pumo, ML; Punch, M; Queiroz, FS; Quirrenbach, A; Rainò, S; Rando, R; Razzaque, S; Reimer, A; Reimer, O; Reposeur, T; Ribó, M; Richtler, T; Rico, J; Rieger, F; Rigoselli, M; Rizi, V; Roache, E; Fernandez, GR; Romano, P; Romeo, G; Rosado, J; de Leon, AR; Rudak, B; Rulten, C; Sadeh, I; Saito, T; Sanchez-Conde, M; Sano, H; Santangelo, A; Santos-Lima, R; Sarkar, S; Saturni, FG; Scherer, A; Schovanek, P; Schussler, F; Schwanke, U; Sergijenko, O; Servillat, M; Siejkowski, H; Siqueira, C; Spencer, S; Stamerra, A; Stanic, S; Steppa, C; Stolarczyk, T; Suda, Y; Tavernier, T; Teshima, M; Tibaldo, L; Torres, DF; Tothill, N; Vacula, M; Vallage, B; Vallania, P; van Eldik, C; Acosta, MV; Vecchi, M; Ventura, S; Vercellone, S; Viana, A; Vigorito, CF; Vink, J; Vitale, V; Vodeb, V; Vorobiov, S; Vuillaume, T; Wagner, SJ; Walter, R; White, M; Wierzcholska, A; Will, M; Yamazaki, R; Yang, L; Yoshikoshi, T; Zacharias, M; Zaharijas, G; Zavrtanik, D; Zavrtanik, M; Zdziarski, AA; Zhdanov, VI; Zietara, K; Zivec, M

    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY   Vol. 523 ( 4 ) page: 5353 - 5387   2023.6

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Monthly Notices of the Royal Astronomical Society  

    A deep survey of the Large Magellanic Cloud at ∼0.1-100 TeV photon energies with the Cherenkov Telescope Array is planned. We assess the detection prospects based on a model for the emission of the galaxy, comprising the four known TeV emitters, mock populations of sources, and interstellar emission on galactic scales. We also assess the detectability of 30 Doradus and SN 1987A, and the constraints that can be derived on the nature of dark matter. The survey will allow for fine spectral studies of N 157B, N 132D, LMC P3, and 30 Doradus C, and half a dozen other sources should be revealed, mainly pulsar-powered objects. The remnant from SN 1987A could be detected if it produces cosmic-ray nuclei with a flat power-law spectrum at high energies, or with a steeper index 2.3-2.4 pending a flux increase by a factor of >3-4 over ∼2015-2035. Large-scale interstellar emission remains mostly out of reach of the survey if its >10 GeV spectrum has a soft photon index ∼2.7, but degree-scale 0.1-10 TeV pion-decay emission could be detected if the cosmic-ray spectrum hardens above >100 GeV. The 30 Doradus star-forming region is detectable if acceleration efficiency is on the order of 1−10 per cent of the mechanical luminosity and diffusion is suppressed by two orders of magnitude within <100 pc. Finally, the survey could probe the canonical velocity-averaged cross-section for self-annihilation of weakly interacting massive particles for cuspy Navarro-Frenk-White profiles.

    DOI: 10.1093/mnras/stad1576

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  11. Multimessenger Characterization of Markarian 501 during Historically Low X-Ray and <i>γ</i>-Ray Activity

    Abé, H; Abé, S; Acciari, VA; Agudo, I; Aniello, T; Ansoldi, S; Antonelli, LA; Arbet-Engels, A; Arcaro, C; Artero, M; Asano, K; Baack, D; Babic, A; Baquero, A; de Almeida, UB; Barrio, JA; Batkovic, I; Baxter, J; González, JB; Bednarek, W; Bernardini, E; Bernardos, M; Berti, A; Besenrieder, J; Bhattacharyya, W; Bigongiari, C; Biland, A; Blanch, O; Bonnoli, G; Bosnjak, Z; Burelli, I; Busetto, G; Carosi, R; Carretero-Castrillo, M; Castro-Tirado, AJ; Ceribella, G; Chai, Y; Chilingarian, A; Cikota, S; Colombo, E; Contreras, JL; Cortina, J; Covino, S; D'Amico, G; D'Elia, V; Da Vela, P; Dazzi, F; De Angelis, A; De Lotto, B; Del Popolo, A; Delfino, M; Delgado, J; Mendez, CD; Depaoli, D; Di Pierro, F; Di Venere, L; Espiñeira, EDS; Prester, DD; Donini, A; Dorner, D; Doro, M; Elsaesser, D; Emery, G; Escudero, J; Ramazani, VF; Fariña, L; Fattorini, A; Foffano, L; Font, L; Fruck, C; Fukami, S; Fukazawa, Y; López, RJG; Garczarczyk, M; Gasparyan, S; Gaug, M; Paiva, JGG; Giglietto, N; Giordano, F; Gliwny, P; Godinovic, N; Grau, R; Green, D; Green, JG; Hadasch, D; Hahn, A; Hassan, T; Heckmann, L; Herrera, J; Hrupec, D; Hütten, M; Imazawa, R; Inada, T; Iotov, R; Ishio, K; Martínez, IJ; Jormanainen, J; Kerszberg, D; Kobayashi, Y; Kubo, H; Kushida, J; Lamastra, A; Lelas, D; Leone, F; Lindfors, E; Linhoff, L; Lombardi, S; Longo, F; López-Coto, R; López-Moya, M; López-Oramas, A; Loporchio, S; Lorini, A; Lyard, E; Fraga, BMD; Majumdar, P; Makariev, M; Maneva, G; Mang, N; Manganaro, M; Mangano, S; Mannheim, K; Mariotti, M; Martínez, M; Mas-Aguilar, A; Mazin, D; Menchiari, S; Mender, S; Micanovic, S; Miceli, D; Miener, T; Miranda, JM; Mirzoyan, R; Molina, E; Mondal, HA; Moralejo, A; Morcuende, D; Moreno, V; Nakamori, T; Nanci, C; Nava, L; Neustroev, V; Rosillo, MN; Nigro, C; Nilsson, K; Nishijima, K; Ekoume, TN; Noda, K; Nozaki, S; Ohtani, Y; Oka, T; Okumura, A; Otero-Santos, J; Paiano, S; Palatiello, M; Paneque, D; Paoletti, R; Paredes, JM; Pavletic, L; Persic, M; Pihet, M; Pirola, G; Podobnik, F; Moroni, PGP; Prandini, E; Principe, G; Priyadarshi, C; Rhode, W; Ribó, M; Rico, J; Righi, C; Rugliancich, A; Sahakyan, N; Saito, T; Sakurai, S; Satalecka, K; Saturni, FG; Schleicher, B; Schmidt, K; Schmuckermaier, F; Schubert, JL; Schweizer, T; Sitarek, J; Sliusar, V; Sobczynska, D; Spolon, A; Stamerra, A; Striskovic, J; Strom, D; Strzys, M; Suda, Y; Suric, T; Tajima, H; Takahashi, M; Takeishi, R; Tavecchio, F; Temnikov, P; Terauchi, K; Terzic, T; Teshima, M; Tosti, L; Truzzi, S; Tutone, A; Ubach, S; van Scherpenberg, J; Acosta, MV; Ventura, S; Verguilov, V; Viale, I; Vigorito, CF; Vitale, V; Vovk, I; Walter, R; Will, M; Wunderlich, C; Yamamoto, T; Zaric, D; Cerruti, M; Acosta-Pulido, JA; Apolonio, G; Bachev, R; Balokovic, M; Benítez, E; Björklund, I; Bozhilov, V; Brown, LF; Bugg, A; Carbonell, W; Carnerero, MI; Carosati, D; Casadio, C; Chamani, W; Chen, WP; Chigladze, RA; Damljanovic, G; Epps, K; Erkenov, A; Feige, M; Finke, J; Fuentes, A; Gazeas, K; Giroletti, M; Grishina, TS; Gupta, AC; Gurwell, MA; Heidemann, E; Hiriart, D; Hou, WJ; Hovatta, T; Ibryamov, S; Joner, MD; Jorstad, SG; Kania, J; Kiehlmann, S; Kimeridze, GN; Kopatskaya, EN; Kopp, M; Korte, M; Kotas, B; Koyama, S; Kramer, JA; Kunkel, L; Kurtanidze, SO; Kurtanidze, OM; Lähteenmäki, A; López, JM; Larionov, VM; Larionova, EG; Larionova, LV; Leto, C; Lorey, C; Mújica, R; Madejski, GM; Marchili, N; Marscher, AP; Minev, M; Modaressi, A; Morozova, DA; Mufakharov, T; Myserlis, I; Nikiforova, AA; Nikolashvili, MG; Ovcharov, E; Perri, M; Raiteri, CM; Readhead, ACS; Reimer, A; Reinhart, D; Righini, S; Rosenlehner, K; Sadun, AC; Savchenko, SS; Scherbantin, A; Schneider, L; Schoch, K; Seifert, D; Semkov, E; Sigua, LA; Singh, C; Sola, P; Sotnikova, Y; Spencer, M; Steineke, R; Stojanovic, M; Strigachev, A; Tornikoski, M; Traianou, E; Tramacere, A; Troitskaya, YV; Troitskiy, IS; Trump, JB; Tsai, A; Valcheva, A; Vasilyev, AA; Verrecchia, F; Villata, M; Vince, O; Vrontaki, K; Weaver, ZR; Zaharieva, E; Zottmann, N

    ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES   Vol. 266 ( 2 )   2023.6

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Astrophysical Journal, Supplement Series  

    We study the broadband emission of Mrk 501 using multiwavelength observations from 2017 to 2020 performed with a multitude of instruments, involving, among others, MAGIC, Fermi's Large Area Telescope (LAT), NuSTAR, Swift, GASP-WEBT, and the Owens Valley Radio Observatory. Mrk 501 showed an extremely low broadband activity, which may help to unravel its baseline emission. Nonetheless, significant flux variations are detected at all wave bands, with the highest occurring at X-rays and very-high-energy (VHE) 3-rays. A significant correlation (>3σ) between X-rays and VHE 3-rays is measured, supporting leptonic scenarios to explain the variable parts of the emission, also during low activity. This is further supported when we extend our data from 2008 to 2020, and identify, for the first time, significant correlations between the Swift X-Ray Telescope and Fermi-LAT. We additionally find correlations between high-energy 3-rays and radio, with the radio lagging by more than 100 days, placing the 3-ray emission zone upstream of the radio-bright regions in the jet. Furthermore, Mrk 501 showed a historically low activity in X-rays and VHE 3-rays from mid-2017 to mid-2019 with a stable VHE flux (>0.2 TeV) of 5% the emission of the Crab Nebula. The broadband spectral energy distribution (SED) of this 2 yr long low state, the potential baseline emission of Mrk 501, can be characterized with one-zone leptonic models, and with (lepto)-hadronic models fulfilling neutrino flux constraints from IceCube. We explore the time evolution of the SED toward the low state, revealing that the stable baseline emission may be ascribed to a standing shock, and the variable emission to an additional expanding or traveling shock.

    DOI: 10.3847/1538-4365/acc181

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  12. Multiwavelength study of the galactic PeVatron candidate LHAASO J2108+5157

    Abe, S; Aguasca-Cabot, A; Agudo, I; Crespo, NA; Antonelli, LA; Aramo, C; Arbet-Engels, A; Artero, M; Asano, K; Aubert, P; Baktash, A; Bamba, A; Larriva, AB; Baroncelli, L; de Almeida, UB; Barrio, JA; Batkovic, I; Baxter, J; González, JB; Bernardini, E; Bernardos, MI; Medrano, JB; Berti, A; Bhattacharjee, P; Biederbeck, N; Bigongiari, C; Bissaldi, E; Blanch, O; Bordas, P; Buisson, C; Bulgarelli, A; Burelli, I; Buscemi, M; Cardillo, M; Caroff, S; Carosi, A; Cassol, F; Cauz, D; Ceribella, G; Chai, Y; Cheng, K; Chiavassa, A; Chikawa, M; Chytka, L; Cifuentes, A; Contreras, JL; Cortina, J; Costantini, H; D'Amico, G; Dalchenko, M; De Angelis, A; de Lavergne, MD; De Lotto, B; de Menezes, R; Deleglise, G; Delgado, C; Mengual, JD; della Volpe, D; Dellaiera, M; Di Piano, A; Di Pierro, F; Di Tria, R; Di Venere, L; Díaz, C; Dominik, RM; Prester, DD; Donini, A; Dorner, D; Doro, M; Elsässer, D; Emery, G; Escudero, J; Ramazani, VF; Ferrara, G; Fiasson, A; Coromina, LF; Fröse, S; Fukami, S; Fukazawa, Y; Garcia, E; López, RG; Gasparrini, D; Geyer, D; Paiva, JG; Giglietto, N; Giordano, F; Giro, E; Gliwny, P; Godinovic, N; Grau, R; Green, D; Green, J; Gunji, S; Hackfeld, J; Hadasch, D; Hahn, A; Hashiyama, K; Hassan, T; Hayashi, K; Heckmann, L; Heller, M; Llorente, JH; Hirotani, K; Hoffmann, D; Horns, D; Houles, J; Hrabovsky, M; Hrupec, D; Hui, D; Hütten, M; Imazawa, R; Inada, T; Inome, Y; Ioka, K; Iori, M; Ishio, K; Iwamura, Y; Jacquemont, M; Martinez, IJ; Jurysek, J; Kagaya, M; Karas, V; Katagiri, H; Kataoka, J; Kerszberg, D; Kobayashi, Y; Kong, A; Kubo, H; Kushida, J; Lainez, M; Lamanna, G; Lamastra, A; Le Flour, T; Linhoff, M; Longo, F; López-Coto, R; López-Moya, M; López-Oramas, A; Loporchio, S; Lorini, A; Luque-Escamilla, PL; Majumdar, P; Makariev, M; Mandat, D; Manganaro, M; Manicò, G; Mannheim, K; Mariotti, M; Marquez, P; Marsella, G; Martí, J; Martinez, O; Martínez, G; Martínez, M; Marusevec, P; Mas-Aguilar, A; Maurin, G; Mazin, D; Guillen, EM; Micanovic, S; Miceli, D; Miener, T; Miranda, JM; Mirzoyan, R; Mizuno, T; Gonzalez, MM; Molina, E; Montaruli, T; Monteiro, I; Moralejo, A; Morcuende, D; Morselli, A; Mrakovcic, K; Murase, K; Nagai, A; Nakamori, T; Nickel, L; Nievas, M; Nishijima, K; Noda, K; Nosek, D; Nozaki, S; Ohishi, M; Ohtani, Y; Okazaki, N; Okumura, A; Orito, R; Otero-Santos, J; Palatiello, M; Paneque, D; Pantaleo, FR; Paoletti, R; Paredes, JM; Pavletic, L; Pech, M; Pecimotika, M; Pietropaolo, E; Pirola, G; Podobnik, F; Poireau, V; Polo, M; Pons, E; Prandini, E; Prast, J; Priyadarshi, C; Prouza, M; Rando, R; Rhode, W; Ribó, M; Rizi, V; Fernandez, GR; Saito, T; Sakurai, S; Sanchez, DA; Saric, T; Saturni, FG; Scherpenberg, J; Schleicher, B; Schmuckermaier, F; Schubert, JL; Schussler, F; Schweizer, T; Arroyo, MS; Sitarek, J; Sliusar, V; Spolon, A; Striskovic, J; Strzys, M; Suda, Y; Sunada, Y; Tajima, H; Takahashi, M; Takahashi, H; Takata, J; Takeishi, R; Tam, PHT; Tanaka, SJ; Tateishi, D; Temnikov, P; Terada, Y; Terauchi, K; Terzic, T; Teshima, M; Tluczykont, M; Tokanai, F; Torres, DF; Travnicek, P; Truzzi, S; Tutone, A; Uhlrich, G; Vacula, M; Acosta, MV; Verguilov, V; Viale, I; Vigliano, A; Vigorito, CF; Vitale, V; Voutsinas, G; Vovk, I; Vuillaume, T; Walter, R; Will, M; Yamamoto, T; Yamazaki, R; Yoshida, T; Yoshikoshi, T; Zywucka, N; Balbo, M; Eckert, D; Tramacere, A

    ASTRONOMY & ASTROPHYSICS   Vol. 673   2023.5

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Astronomy and Astrophysics  

    Context. Several new ultrahigh-energy (UHE) γ-ray sources have recently been discovered by the Large High Altitude Air Shower Observatory (LHAASO) collaboration. These represent a step forward in the search for the so-called Galactic PeVatrons, the enigmatic sources of the Galactic cosmic rays up to PeV energies. However, it has been shown that multi-TeV γ-ray emission does not necessarily prove the existence of a hadronic accelerator in the source; indeed this emission could also be explained as inverse Compton scattering from electrons in a radiation-dominated environment. A clear distinction between the two major emission mechanisms would only be made possible by taking into account multi-wavelength data and detailed morphology of the source. Aims. We aim to understand the nature of the unidentified source LHAASO J2108+5157, which is one of the few known UHE sources with no very high-energy (VHE) counterpart. Methods. We observed LHAASO J2108+5157 in the X-ray band with XMM-Newton in 2021 for a total of 3.8 hours and at TeV energies with the Large-Sized Telescope prototype (LST-1), yielding 49 hours of good-quality data. In addition, we analyzed 12 years of Fermi-LAT data, to better constrain emission of its high-energy (HE) counterpart 4FGL J2108.0+5155. We used naima and jetset software packages to examine the leptonic and hadronic scenario of the multi-wavelength emission of the source. Results. We found an excess (3.7σ) in the LST-1 data at energies E > 3 TeV. Further analysis of the whole LST-1 energy range, assuming a point-like source, resulted in a hint (2.2σ) of hard emission, which can be described with a single power law with a photon index of Σ = 1.6 ± 0.2 the range of 0.3 - 100 TeV. We did not find any significant extended emission that could be related to a supernova remnant (SNR) or pulsar wind nebula (PWN) in the XMM-Newton data, which puts strong constraints on possible synchrotron emission of relativistic electrons. We revealed a new potential hard source in Fermi-LAT data with a significance of 4σ and a photon index of Σ = 1.9 ± 0.2, which is not spatially correlated with LHAASO J2108+5157, but including it in the source model we were able to improve spectral representation of the HE counterpart 4FGL J2108.0+5155. Conclusions. The LST-1 and LHAASO observations can be explained as inverse Compton-dominated leptonic emission of relativistic electrons with a cutoff energy of 100-30+70 TeV. The low magnetic field in the source imposed by the X-ray upper limits on synchrotron emission is compatible with a hypothesis of a PWN or a TeV halo. Furthermore, the spectral properties of the HE counterpart are consistent with a Geminga-like pulsar, which would be able to power the VHE-UHE emission. Nevertheless, the lack of a pulsar in the neighborhood of the UHE source is a challenge to the PWN/TeV-halo scenario. The UHE γ rays can also be explained as π0 decay-dominated hadronic emission due to interaction of relativistic protons with one of the two known molecular clouds in the direction of the source. Indeed, the hard spectrum in the LST-1 band is compatible with protons escaping a shock around a middle-aged SNR because of their high low-energy cut-off, but the origin of the HE γ-ray emission remains an open question.

    DOI: 10.1051/0004-6361/202245086

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  13. MAGIC observations provide compelling evidence of hadronic multi-TeV emission from the putative PeVatron SNR G106.3+2.7

    Abe H., Abe S., Acciari V.A., Agudo I., Aniello T., Ansoldi S., Antonelli L.A., Arbet Engels A., Arcaro C., Artero M., Asano K., Baack D., Babić A., Baquero A., Barres De Almeida U., Barrio J.A., Batković I., Baxter J., Becerra González J., Bednarek W., Bernardini E., Bernardos M., Berti A., Besenrieder J., Bhattacharyya W., Bigongiari C., Biland A., Blanch O., Bonnoli G., Bošnjak , Burelli I., Busetto G., Carosi R., Carretero-Castrillo M., Castro-Tirado A.J., Ceribella G., Chai Y., Chilingarian A., Cikota S., Colombo E., Contreras J.L., Cortina J., Covino S., D'Amico G., D'Elia V., Da Vela P., Dazzi F., De Angelis A., De Lotto B., Del Popolo A., Delfino M., Delgado J., Delgado Mendez C., Depaoli D., Di Pierro F., Di Venere L., Do Souto Espiñeira E., Dominis Prester D., Donini A., Dorner D., Doro M., Elsaesser D., Emery G., Escudero J., Fallah Ramazani V., Fariña L., Fattorini A., Font L., Fruck C., Fukami S., Fukazawa Y., García López R.J., Garczarczyk M., Gasparyan S., Gaug M., Giesbrecht Paiva J.G., Giglietto N., Giordano F., Gliwny P., Godinović N., Grau R., Green D., Green J.G., Hadasch D., Hahn A., Hassan T., Heckmann L., Herrera J., Hrupec D., Hütten M., Imazawa R., Inada T., Iotov R., Ishio K., Jiménez Martínez I., Jormanainen J., Kerszberg D., Kobayashi Y., Kubo H., Kushida J.

    Astronomy and Astrophysics   Vol. 671   2023.3

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Astronomy and Astrophysics  

    Context. Certain types of supernova remnants (SNRs) in our Galaxy are assumed to be PeVatrons, capable of accelerating cosmic rays (CRs) to ∼ PeV energies. However, conclusive observational evidence for this has not yet been found. The SNR G106.3+2.7, detected at 1- 100 TeV energies by different γ-ray facilities, is one of the most promising PeVatron candidates. This SNR has a cometary shape, which can be divided into a head and a tail region with different physical conditions. However, in which region the 100 TeV emission is produced has not yet been identified because of the limited position accuracy and/or angular resolution of existing observational data. Additionally, it remains unclear as to whether the origin of the γ-ray emission is leptonic or hadronic. Aims. With the better angular resolution provided by new MAGIC data compared to earlier γ-ray datasets, we aim to reveal the acceleration site of PeV particles and the emission mechanism by resolving the SNR G106.3+2.7 with 0.1 resolution at TeV energies. Methods. We observed the SNR G106.3+2.7 using the MAGIC telescopes for 121.7 h in total - after quality cuts - between May 2017 and August 2019. The analysis energy threshold is ∼0.2 TeV, and the angular resolution is 0.07-0.1. We examined the γ-ray spectra of different parts of the emission, whilst benefitting from the unprecedented statistics and angular resolution at these energies provided by our new data. We also used measurements at other wavelengths such as radio, X-rays, GeV γ-rays, and 10 TeV γ-rays to model the emission mechanism precisely. Results. We detect extended γ-ray emission spatially coincident with the radio continuum emission at the head and tail of SNR G106.3+2.7. The fact that we detect a significant γ-ray emission with energies above 6.0 TeV from only the tail region suggests that the emissions above 10 TeV detected with air shower experiments (Milagro, HAWC, Tibet ASγ and LHAASO) are emitted only from the SNR tail. Under this assumption, the multi-wavelength spectrum of the head region can be explained with either hadronic or leptonic models, while the leptonic model for the tail region is in contradiction with the emission above 10 TeV and X-rays. In contrast, the hadronic model could reproduce the observed spectrum at the tail by assuming a proton spectrum with a cutoff energy of ∼1 PeV for that region. Such high-energy emission in this middle-aged SNR (4-10 kyr) can be explained by considering a scenario where protons escaping from the SNR in the past interact with surrounding dense gases at present. Conclusions. The γ-ray emission region detected with the MAGIC telescopes in the SNR G106.3+2.7 is extended and spatially coincident with the radio continuum morphology. The multi-wavelength spectrum of the emission from the tail region suggests proton acceleration up to ∼PeV, while the emission mechanism of the head region could either be hadronic or leptonic.

    DOI: 10.1051/0004-6361/202244931

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  14. Gamma-ray observations of MAXI J1820+070 during the 2018 outburst

    Abe H., Abe S., Acciari V. A., Aniello T., Ansoldi S., Antonelli L. A., Engels A. Arbet, Arcaro C., Artero M., Asano K., Baack D., Babic A., Baquero A., de Almeida U. Barres, Barrio J. A., Batkovic I, Baxter J., Gonzalez J. Becerra, Bednarek W., Bernardini E., Bernardos M., Berti A., Besenrieder J., Bhattacharyya W., Bigongiari C., Biland A., Blanch O., Bonnoli G., Bosnjak Z., Burelli I, Busetto G., Carosi R., Carretero-Castrillo M., Ceribella G., Chai Y., Chilingarian A., Cikota S., Colombo E., Contreras J. L., Cortina J., Covino S., D'Amico G., D'Elia V, Da Vela P., Dazzi F., De Angelis A., De Lotto B., Del Popolo A., Delfino M., Delgado J., Mendez C. Delgado, Depaoli D., Di Pierro F., Di Venere L., Prester D. Dominis, Donini A., Dorner D., Doro M., Elsaesser D., Emery G., Ramazani V. Fallah, Farina L., Fattorini A., Font L., Fruck C., Fukami S., Fukazawa Y., Lopez R. J. Garcia, Garczarczyk M., Gasparyan S., Gaug M., Paiva J. G. Giesbrecht, Giglietto N., Giordano F., Gliwny P., Godinovic N., Grau R., Green D., Green J. G., Hadasch D., Hahn A., Hassan T., Heckmann L., Herrera J., Hoang J., Hrupec D., Hutten M., Imazawa R., Inada T., Iotov R., Ishio K., Martinez I. Jimenez, Jormanainen J., Kerszberg D., Kobayashi Y., Kubo H., Kushida J., Lamastra A., Lelas D., Leone F., Lindfors E., Linhoff L., Lombardi S., Longo F., Lopez-Coto R., Lopez-Moya M., Lopez-Oramas A., Loporchio S., Lorini A., Lyard E., Fraga B. Machado de Oliveira, Majumdar P., Makariev M., Maneva G., Mang N., Manganaro M., Mangano S., Mannheim K., Mariotti M., Martinez M., Aguilar A. Mas, Mazin D., Menchiari S., Mender S., Micanovic S., Miceli D., Miener T., Miranda J. M., Mirzoyan R., Molina E., Mondal H. A., Moralejo A., Morcuende D., Moreno V, Nakamori T., Nanci C., Nava L., Neustroev V, Rosillo M. Nievas, Nigro C., Nilsson K., Nishijima K., Ekoume T. Njoh, Noda K., Nozaki S., Ohtani Y., Oka T., Okumura A., Otero-Santos J., Paiano S., Palatiello M., Paneque D., Paoletti R., Paredes J. M., Pavletic L., Persic M., Pihet M., Pirola G., Podobnik F., Moroni P. G. Prada, Prandini E., Principe G., Priyadarshi C., Puljak I, Rhode W., Ribo M., Rico J., Righi C., Rugliancich A., Sahakyan N., Saito T., Sakurai S., Satalecka K., Saturni F. G., Schleicher B., Schmidt K., Schmuckermaier F., Schubert J. L., Schweizer T., Sitarek J., Sliusar V, Sobczynska D., Spolon A., Stamerra A., Striskovic J., Strom D., Strzys M., Suda Y., Suric T., Tajima H., Takahashi M., Takeishi R., Tavecchio F., Temnikov P., Terauchi K., Terzic T., Teshima M., Tosti L., Truzzi S., Tutone A., Ubach S., van Scherpenberg J., Acosta M. Vazquez, Ventura S., Verguilov V., Viale I, Vigorito C. F., Vitale V., Vovk I, Walter R., Will M., Wunderlich C., Yamamoto T., Zaric D., Abdalla H., Aharonian F., Benkhali F. Ait, Anguner E. O., Ashkar H., Backes M., Baghmanyan V, Martins V. Barbosa, Batzofin R., Becherini Y., Berge D., Bernloehr K., Bottcher M., Boisson C., Bolmont J., de Lavergne M. de Bony, Bradascio F., Breuhaus M., Brose R., Brun F., Bulik T., Bylund T., Cangemi F., Caroff S., Casanova S., Cerruti M., Chand T., Chandra S., Chen A., Chibueze O. U., Cotter G., Cristofari P., Mbarubucyeye J. Damascene, Devin J., Djannati-Atai A., Dmytriiev A., Egberts K., Ernenwein J-P, Fiasson A., de Clairfontaine G. Fichet, Fontaine G., Fuessling M., Funk S., Gabici S., Ghafourizadeh S., Giavitto G., Glawion D., Glicenstein J. F., Goswami P., Grolleron G., Hinton J. A., Horbe M., Hoischen C., Holch T. L., Holler M., Horns D., Huang Zhiqiu, Jamrozy M., Jankowsky F., Joshi V, Jung-Richardt I, Kasai E., Katarzynski K., Katz U., Khelifi B., Kluzniak W., Komin Nu, Kosack K., Kostunin D., Lang R. G., Le Stum S., Lemiere A., Lemoine-Goumard M., Lenain J-P, Leuschner F., Lohse T., Luashvili A., Lypova I, Mackey J., Majumdar J., Malyshev D., Malyshev D., Marandon V, Marchegiani P., Marti-Devesa G., Marx R., Maurin G., Meyer M., Mitchell A., Moderski R., Mohrmann L., Montanari A., Moulin E., Muller J., Murach T., Nakashima K., de Naurois M., Nayerhoda A., Niemiec J., Noel A. Pniyana, O'Brien P., Ohm S., Olivera-Nieto L., Wilhelmi E. de Ona, Ostrowski M., Panny S., Panter M., Parsons R. D., Poireau V, Prokhorov D. A., Prokoph H., Puehlhofer G., Punch M., Quirrenbach A., Reichherzer P., Reimer A., Reimer O., Renaud M., Rieger F., Rowell G., Rudak B., Ricarte H. Rueda, Ruiz-Velasco E., Sahakian V, Salzmann H., Santangelo A., Sasaki M., Schaefer J., Schussler F., Schutte H. M., Schwanke U., Shapopi J. N. S., Sol H., Specovius A., Spencer S., Stawarz L., Steenkamp R., Steinmassl S., Steppa C., Sushch I, Suzuki H., Takahashi T., Tanaka T., Thorpe-Morgan C., Tluczykont M., Tomankova L., Tsuji N., Uchiyama Y., van Eldik C., van Soelen B., Vecchi M., Veh J., Venter C., Vink J., Wagner S. J., White R., Wierzcholska A., Wong Yu Wun, Yusafzai A., Zacharias M., Zanin R., Zargaryan D., Zdziarski A. A., Zech A., Zhu S. J., Zouari S., Zywucka N., Acharyya A., Adams C. B., Batista P., Benbow W., Capasso M., Christiansen J. L., Chromey A. J., Errando M., Falcone A., Feng Q., Finley J. P., Foote G. M., Fortson L., Furniss A., Gent A., Hanlon W. E., Hervet O., Holder J., Hona B., Humensky T. B., Jin W., Kaaret P., Kertzman M., Kherlakian M., Kleiner T. K., Kumar S., Lang M. J., Lundy M., Maier G., McGrath C. E., Millis J., Moriarty P., Mukherjee R., O'Brien S., Ong R. A., Park N., Patel S. R., Pfrang K., Pohl M., Pueschel E., Quinn J., Ragan K., Reynolds P. T., Ribeiro D., Roache E., Ryan J. L., Sadeh I, Saha L., Santander M., Sembroski G. H., Shang R., Splettstoesser M., Tak D., Tucci J. V, Weinstein A., Williams D. A., Williamson T. J., Bosch-Ramon V, Celma C., Linares M., Russell D. M., Sala G.

    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY   Vol. 517 ( 4 ) page: 4736 - 4751   2022.12

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Monthly Notices of the Royal Astronomical Society  

    MAXI J1820+070 is a low-mass X-ray binary with a black hole (BH) as a compact object. This binary underwent an exceptionally bright X-ray outburst from 2018 March to October, showing evidence of a non-thermal particle population through its radio emission during this whole period. The combined results of 59.5 h of observations of the MAXI J1820+070 outburst with the H.E.S.S., MAGIC and VERITAS experiments at energies above 200 GeV are presented, together with Fermi-LAT data between 0.1 and 500 GeV, and multiwavelength observations from radio to X-rays. Gamma-ray emission is not detected from MAXI J1820+070, but the obtained upper limits and the multiwavelength data allow us to put meaningful constraints on the source properties under reasonable assumptions regarding the non-thermal particle population and the jet synchrotron spectrum. In particular, it is possible to show that, if a high-energy (HE) gamma-ray emitting region is present during the hard state of the source, its predicted flux should be at most a factor of 20 below the obtained Fermi-LAT upper limits, and closer to them for magnetic fields significantly below equipartition. During the state transitions, under the plausible assumption that electrons are accelerated up to ∼500 GeV, the multiwavelength data and the gamma-ray upper limits lead consistently to the conclusion that a potential HE and very-HE gamma-ray emitting region should be located at a distance from the BH ranging between 1011 and 1013 cm. Similar outbursts from low-mass X-ray binaries might be detectable in the near future with upcoming instruments such as CTA.

    DOI: 10.1093/mnras/stac2686

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  15. Active Galactic Nuclei population studies with the Cherenkov Telescope Array

    Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D., Bernardini E., Bernardos M.I., Bernlöhr K., Berti A.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) observatory is the next generation of ground-based imaging atmospheric Cherenkov telescopes (IACTs). Building on the strengths of current IACTs, CTA is designed to achieve an order of magnitude improvement in sensitivity, with unprecedented angular and energy resolution. CTA will also increase the energy reach of IACTs, observing photons in the energy range from 20 GeV to beyond 100 TeV. These advances in performance will see CTA heralding in a new era for high-energy astrophysics, with the emphasis shifting from source discovery, to population studies and precision measurements. In this talk we discuss CTA’s ability to conduct source population studies of γ-ray bright active galactic nuclei and how this ability will enhance our understanding on the redshift evolution of this dominant γ-ray source class.

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  16. Physics Performance of the Large-Sized Telescope prototype of the Cherenkov Telescope Array

    Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Artero M., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Becerra González J., Bernardos M.I., Berti A., Biederbeck N., Bigongiari C., Blanch O., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Carosi A., Cassol F., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., Dalchenko M., De Angelis A., de Bony de Lavergne M., Deleglise G., Delgado C., Delgado Mengual J., della Volpe D., Depaoli D., Di Pierro F., Di Venere L., Díaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsässer D., Emery G., Escudero J., Fiasson A., Foffano L., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Giglietto N., Giordano F., Gliwny P., Godinovic N., Green D., Grespan P., Gunji S., Hackfeld J., Hadasch D., Hahn A., Hassan T., Hayashi K., Heckmann L., Heller M., Herrera Llorente J., Hirotani K., Hoffmann D., Horns D., Houles J., Hrabovsky M., Hrupec D., Hui D., Hütten M., Inada T., Inome Y., Iori M., Ishio K., Iwamura Y., Jacquemont M., Jimenez Martinez I., Jouvin L., Jurysek J.

    Proceedings of Science   Vol. 395   2022.3

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    The Large-Sized Telescope (LST) prototype of the future Cherenkov Telescope Array (CTA) is located at the Northern site of CTA, on the Canary Island of La Palma. It is designed to provide optimal performance in the lowest part of the energy range covered by CTA, observing gamma rays down to energies of tens of GeV. The LST prototype started performing astronomical observations in November 2019 during the commissioning of the telescope and it has been taking data since then. In this contribution, we will present the tuning of the characteristics of the telescope in the Monte Carlo (MC) simulations to describe the data obtained, the estimation of its angular and energy resolution, and an evaluation of its sensitivity, both with simulations and with observations of the Crab Nebula.

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  17. Performance of the Cherenkov Telescope Array in the presence of clouds

    Pecimotika M., Adamczyk K., Prester D.D., Gueta O., Hrupec D., Maier G., Mićanović S., Pavletić L., Sitarek J., Sobczyńska D., Szanecki M., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) is the future ground-based observatory for gamma-ray astronomy at very high energies. The atmosphere is an integral part of every Cherenkov telescope. Different atmospheric conditions, such as clouds, can reduce the fraction of Cherenkov photons produced in air showers that reach ground-based telescopes, which may affect the performance. Decreased sensitivity of the telescopes may lead to misconstructed energies and spectra. This study presents the impact of various atmospheric conditions on CTA performance. The atmospheric transmission in a cloudy atmosphere in the wavelength range from 203 nm to 1000 nm was simulated for different cloud bases and different optical depths using the MODerate resolution atmospheric TRANsmission (MODTRAN) code. MODTRAN output files were used as inputs for generic Monte Carlo simulations. The analysis was performed using the MAGIC Analysis and Reconstruction Software (MARS) adapted for CTA. As expected, the effects of clouds are most evident at low energies, near the energy threshold. Even in the presence of dense clouds, high-energy gamma rays may still trigger the telescopes if the first interaction occurs lower in the atmosphere, below the cloud base. A method to analyze very high-energy data obtained in the presence of clouds is presented. The systematic uncertainties of the method are evaluated. These studies help to gain more precise knowledge about the CTA response to cloudy conditions and give insights on how to proceed with data obtained in such conditions. This may prove crucial for alert-based observations and time-critical studies of transient phenomena.

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  18. Performance of a proposed event-type based analysis for the Cherenkov Telescope Array

    Hassan T., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D., Bernardini E., Bernardos M.I., Bernlöhr K.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) will be the next-generation observatory in the field of very-high-energy (20 GeV to 300 TeV) gamma-ray astroparticle physics. Classically, data analysis in the field maximizes sensitivity by applying quality cuts on the data acquired. These cuts, optimized using Monte Carlo simulations, select higher quality events from the initial dataset. Subsequent steps of the analysis typically use the surviving events to calculate one set of instrument response functions (IRFs). An alternative approach is the use of event types, as implemented in experiments such as the Fermi-LAT. In this approach, events are divided into sub-samples based on their reconstruction quality, and a set of IRFs is calculated for each sub-sample. The sub-samples are then combined in a joint analysis, treating them as independent observations. This leads to an improvement in performance parameters such as sensitivity, angular and energy resolution. Data loss is reduced since lower quality events are included in the analysis as well, rather than discarded. In this study, machine learning methods will be used to classify events according to their expected angular reconstruction quality. We will report the impact on CTA high-level performance when applying such an event-type classification, compared to the classical procedure.

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  19. Monte Carlo Simulations and Validation of NectarCAM, a Medium Sized Telescope Camera for CTA

    Armstrong T.P., Costantini H., Glicenstein J.F., Lenain J.P., Schwanke U., Tavernier T., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R.

    Proceedings of Science   Vol. 395   2022.3

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    The upcoming Cherenkov Telescope Array (CTA) ground-based gamma-ray observatory will open up our view of the very high energy Universe, offering an improvement in sensitivity of 5-10 times that of previous experiments. NectarCAM is one of the proposed cameras for the Medium-Sized Telescopes (MST) which have been designed to cover the core energy range of CTA, from 100 GeV to 10 TeV. The final camera will be capable of GHz sampling and provide a field of view of 8 degrees with its 265 modules of 7 photomultiplier each (for a total of 1855 pixels). In order to validate the performance of NectarCAM, a partially-equipped prototype has been constructed consisting of only the inner 61-modules. It has so far undergone testing at the integration test-bench facility in CEA Paris-Saclay (France) and on a prototype of the MST structure in Adlershof (Germany). To characterize the performance of the prototype, Monte Carlo simulations were conducted using a detailed model of the 61 module camera in the CORSIKA/sim_telarray framework. This contribution provides an overview of this work including the comparison of trigger and readout performance on test-bench data and trigger and image parameterization performance during on-sky measurements.

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  20. Monitoring the pointing of the prototype LST-1 using star reconstruction in the Cherenkov camera

    Foffano L., Carosi A., Dalchenko M., Heller M., Della Volpe D., Montaruli T., Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Artero M., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Becerra González J., Bernardos M.I., Berti A., Biederbeck N., Bigongiari C., Blanch O., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Cassol F., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., De Angelis A., de Bony de Lavergne M., Deleglise G., Delgado C., Delgado Mengual J., Depaoli D., Di Pierro F., Di Venere L., Díaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsässer D., Emery G., Escudero J., Fiasson A., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Giglietto N., Giordano F., Gliwny P., Godinovic N., Green D., Grespan P., Gunji S., Hackfeld J., Hadasch D., Hahn A., Hassan T., Hayashi K., Heckmann L., Herrera Llorente J., Hirotani K., Hoffmann D., Horns D., Houles J., Hrabovsky M., Hrupec D., Hui D., Hütten M., Inada T., Inome Y., Iori M., Ishio K., Iwamura Y., Jacquemont M., Jimenez Martinez I., Jouvin L.

    Proceedings of Science   Vol. 395   2022.3

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    The first Large-Sized Telescope (LST-1) proposed for the forthcoming Cherenkov Telescope Array (CTA) has started to operate in 2019 in La Palma. The large structure of LST-1 - with a 23 m mirror dish diameter - imposes a strict control of its deformations that could affect the pointing accuracy and its overall performance. According to CTA specifications that are conceived to resolve e.g. the fine structure of galactic sources, the LST post-calibration pointing accuracy should be better than 14 arcseconds. To fulfill this requirement, the telescope pointing precision is monitored with two dedicated CCD cameras located at the dish center. The analysis of their images allows us to disentangle different systematic deformations of the structure. In this work, we investigate a complementary approach that offers the possibility to monitor the pointing of the telescope during the acquisition of sky data. After properly cleaning the events from the Cherenkov showers, the reconstructed positions of the stars imaged in the camera field of view are compared to their nominal expected positions in catalogues. This provides a direct measurement of the telescope pointing, that can be used to cross-check the other methods and as a real-time monitoring of the optical properties of the telescope and of the pointing corrections applied by the bending models. Additionally, this method benefits from not relying on specific hardware or dedicated observations. In this contribution we will illustrate this analysis and show results based on simulations of LST-1.

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  21. HAWC J2227+610: a potential PeVatron candidate for the CTA in the northern hemisphere

    Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D., Bernardini E., Bernardos M.I., Bernlöhr K., Berti A.

    Proceedings of Science   Vol. 395   2022.3

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    Recent observations of the gamma-ray source HAWC J2227+610 by Tibet AS+MD and LHAASO confirm the special interest of this source as a galactic PeVatron candidate in the northern hemisphere. HAWC J2227+610 emits Very High Energy (VHE) gamma-rays up to 500 TeV, from a region coincident with molecular clouds and significantly displaced from the nearby pulsar J2229+6114. Even if this morphology favours an hadronic origin, both leptonic or hadronic models can describe the current VHE gamma-ray emission. The morphology of the source is not well constrained by the present measurements and a better characterisation would greatly help the understanding of the underlying particle acceleration mechanisms. The Cherenkov Telescope Array (CTA) will be the future most sensitive Imaging Atmospheric Cherenkov Telescope and, thanks to its unprecedented angular resolution, could contribute to better constrain the nature of this source. The present work investigates the potentiality of CTA to study the morphology and the spectrum of HAWC J2227+610. For this aim, the source is simulated assuming the hadronic model proposed by the Tibet AS+MD collaboration, recently fitted on multi-wavelength data, and two spatial templates associated to the source nearby molecular clouds. Different CTA layouts and observation times are considered. A 3D map based analysis shows that CTA is able to significantly detect the extension of the source and to attribute higher detection significance to the simulated molecular cloud template compared to the alternative one. CTA data does not allow to disentangle the hadronic and the leptonic emission models. However, it permits to correctly reproduce the simulated parent proton spectrum characterized by a ∼ 500 TeV cutoff.

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  22. First follow-up of transient events with the CTA Large Size Telescope prototype

    Kobayshi Y., Sanchez D., Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Artero M., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Becerra González J., Bernardos M.I., Berti A., Biederbeck N., Bigongiari C., Blanch O., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Carosi A., Cassol F., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., Dalchenko M., De Angelis A., de Bony de Lavergne M., Deleglise G., Delgado C., Delgado Mengual J., della Volpe D., Depaoli D., Di Pierro F., Di Venere L., Díaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsässer D., Emery G., Escudero J., Fiasson A., Foffano L., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Giglietto N., Giordano F., Gliwny P., Godinovic N., Green D., Grespan P., Gunji S., Hackfeld J., Hadasch D., Hahn A., Hassan T., Hayashi K., Heckmann L., Heller M., Herrera Llorente J., Hirotani K., Hoffmann D., Horns D., Houles J., Hrabovsky M., Hrupec D., Hui D., Hütten M., Inada T., Inome Y., Iori M., Ishio K., Iwamura Y., Jacquemont M., Jimenez Martinez I.

    Proceedings of Science   Vol. 395   2022.3

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    The recent detection of a very high energy (VHE) emission from Gamma-Ray Bursts (GRBs) above 100 GeV performed by the MAGIC and H.E.S.S. collaborations, has represented a significant, long-awaited result for the VHE astrophysics community. Although these results' scientific impact has not yet been fully exploited, the possibility to detect VHE gamma-ray signals from GRBs has always been considered crucial for clarifying the poorly known physics of these objects. Furthermore, the discovery of high-energy neutrinos and gravitational waves associated with astrophysical sources have definitively opened the era of multi-messenger astrophysics, providing unique insights into the physics of extreme cosmic accelerators. In the near future, the Cherenkov Telescope Array (CTA) will play a major role in these observations. Within this framework, the Large Size Telescopes (LSTs) will be the instruments best suited to significantly impact on short time-scale transients follow-up thanks to their fast slewing and large effective area. The observations of the early emission phase of a wide range of transient events with good sensitivity below 100 GeV will allow us to open new opportunities for time-domain astrophysics in an energy range not affected by selective absorption processes typical of other wavelengths. In this contribution, we will report about the observational program and first transients follow-up observations performed by the LST-1 telescope currently in its commissioning phase on La Palma, Canary Islands, the CTA northern hemisphere site.

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  23. Exploring the population of Galactic very-high-energy γ-ray sources

    Steppa C., Egberts K., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D., Bernardini E., Bernardos M.I.

    Proceedings of Science   Vol. 395   2022.3

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    At very high energies (VHE), the emission of γ rays is dominated by discrete sources. Due to the limited resolution and sensitivity of current-generation instruments, only a small fraction of the total Galactic population of VHE γ-ray sources has been detected significantly. The larger part of the population can be expected to contribute as a diffuse signal alongside emission originating from propagating cosmic rays. Without quantifying the source population, it is not possible to disentangle these two components. Based on the H.E.S.S. Galactic plane survey, a numerical approach has been taken to develop a model of the population of Galactic VHE γ-ray sources, which is shown to account accurately for the observational bias. We present estimates of the absolute number of sources in the Galactic Plane and their contribution to the total VHE γ-ray emission for five different spatial source distributions. Prospects for CTA and its ability to constrain the model are discussed. Finally, first results of an extension of our modelling approach using machine learning to extract more information from the available data set are presented.

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  24. Development of an advanced SiPM camera for the Large Size Telescope of the Cherenkov Telescope Array Observatory

    Bellato M., Bergnoli A., Bernasconi E., Biland A., Charbon E., Corti D., Gascón D., Gómez S., Ziȩtara K., Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Artero M., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Becerra González J., Bernardos M.I., Berti A., Biederbeck N., Bigongiari C., Blanch O., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Carosi A., Cassol F., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., Dalchenko M., De Angelis A., de Bony de Lavergne M., Deleglise G., Delgado C., Delgado Mengual J., della Volpe D., Depaoli D., Di Pierro F., Di Venere L., Díaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsässer D., Emery G., Escudero J., Fiasson A., Foffano L., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Giglietto N., Giordano F., Gliwny P., Godinovic N., Green D., Grespan P., Gunji S., Hackfeld J., Hadasch D., Hahn A., Hassan T., Hayashi K., Heckmann L., Heller M., Herrera Llorente J., Hirotani K., Hoffmann D., Horns D., Houles J., Hrabovsky M., Hrupec D., Hui D., Hütten M.

    Proceedings of Science   Vol. 395   2022.3

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    Silicon photomultipliers (SiPMs) have become the baseline choice for cameras of the small-sized telescopes (SSTs) of the Cherenkov Telescope Array (CTA). On the other hand, SiPMs are relatively new to the field and covering large surfaces and operating at high data rates still are challenges to outperform photomultipliers (PMTs). The higher sensitivity in the near infra-red and longer signals compared to PMTs result in higher night sky background rate for SiPMs. However, the robustness of the SiPMs represents a unique opportunity to ensure long-term operation with low maintenance and better duty cycle than PMTs. The proposed camera for large size telescopes will feature 0.05◦ pixels, low power and fast front-end electronics and a fully digital readout. In this work, we present the status of dedicated simulations and data analysis for the performance estimation. The design features and the different strategies identified, so far, to tackle the demanding requirements and the improved performance are described.

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  25. Detection of the Crab Nebula by the prototype Schwarzschild-Couder Telescope

    Adams C.B., Ambrosi G., Ambrosio M., Aramo C., Batista P.I., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolontà C., Bose R., Brill A., Brown A.M., Buckley J.H., Cameron R.A., Canestrari R., Capasso M., Caprai M., Covault C.E., Depaoli D., Di Venere L., Errando M., Fegan S., Feng Q., Fiandrini E., Furniss A., Gent A., Giglietto N., Giordano F., Giro E., Halliday R., Hervet O., Holder J., Humensky T.B., Incardona S., Ionica M., Jin W., Kieda D., Licciulli F., Loporchio S., Marsella G., Masone V., Meagher K., Meures T., Mode B.A.W., Mognet S.A.I., Mukherjee R., Okumura A., Otte N., Pantaleo F.R., Paoletti R., Pareschi G., Di Pierro F., Pueschel E., Ribeiro D., Riitano L., Roache E., Rousselle J., Rugliancich A., Santander M., Shang R., Stiaccini L., Tajima H., Taylor L.P., Tosti L., Tovmassian G., Tripodo G., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V.V., Williams D.A., Zink A.

    Proceedings of Science   Vol. 395   2022.3

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    The Schwarzschild-Couder Telescope (SCT) is a medium-sized telescope technology proposed for the Cherenkov Telescope Array. It uses a novel dual-mirror optical design that removes comatic aberrations across its entire field of view. The SCT camera employs high-resolution silicon photomultiplier (SiPM) sensors with a pixel size of 4 arcminutes. A prototype SCT (pSCT) has been constructed at the Fred Lawrence Whipple Observatory in Arizona, USA. An observing campaign in 2020, with a partial camera of 1600 pixels (2.7 degrees by 2.7 degrees field of view) resulted in detection of the Crab Nebula at 8.6 sigma statistical significance. Work on the pSCT camera and optical system is ongoing to improve performance and prepare for an upcoming camera upgrade. The pSCT camera upgrade will replace the current camera modules with improved SiPMs and readout electronics and will expand the camera to its full design field of view of 8 degrees in diameter (11,328 pixels). The fully upgraded pSCT will enable next-generation very-high-energy gamma-ray astrophysics through excellent background rejection and angular resolution. In this presentation we describe first results from the successful operation of the pSCT and future plans.

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  26. Detection methods for the Cherenkov Telescope Array at very-short exposure times

    Di Piano A., Bulgarelli A., Fioretti V., Baroncelli L., Parmiggiani N., Longo F., Stamerra A., López-Oramas A., Stratta G., De Cesare G., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) will be the next generation ground-based observatory for very-high-energy (VHE) gamma-ray astronomy, with the deployment of tens of highly sensitive and fast-reacting Cherenkov telescopes. It will cover a wide energy range (20 GeV - 300 TeV) with unprecedented sensitivity. To maximize the scientific return, the observatory will be provided with an online software system that will perform the first analysis of scientific data in real-time. This study investigates the precision and accuracy of available science tools and analysis techniques for the short-term detection of gamma-ray sources, in terms of sky localization, detection significance and, if significant detection is achieved, a first estimation of the integral photon flux. The scope is to evaluate the feasibility of the algorithms' implementation in the real-time analysis of CTA. In this contribution we present a general overview of the methods and some of the results for the test case of the short-term detection of a gamma-ray burst afterglow, as the VHE counterpart of a gravitational wave event.

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  27. Design and performance of the prototype Schwarzschild-Couder Telescope camera

    Taylor L.P., Adams C.B., Ambrosi G., Ambrosio M., Aramo C., Batista P.I., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolontà C., Bose R., Brill A., Brown A.M., Buckley J.H., Cameron R.A., Capasso M., Caprai M., Covault C.E., Depaoli D., Di Venere L., Errando M., Fegan S., Feng Q., Fiandrini E., Furniss A., Gent A., Giglietto N., Giordano F., Halliday R., Hervet O., Humensky T.B., Incardona S., Ionica M., Jin W., Kieda D., Licciulli F., Loporchio S., Marsella G., Masone V., Meagher K., Meures T., Mode B.A.W., Mognet S.A.I., Mukherjee R., Okumura A., Otte N., Pantaleo F.R., Paoletti R., Pareschi G., Di Pierro F., Pueschel E., Ribeiro D., Riitano L., Roache E., Ross D., Rousselle J., Rugliancich A., Santander M., Shang R., Stiaccini L., Tajima H., Taylor L.P., Tosti L., Tovmassian G., Tripodo G., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V.V., Watson J.J., White R., Williams D.A., Zink A.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) is the next-generation ground-based observatory for very-high-energy gamma-ray astronomy. An innovative 9.7 m aperture, dual-mirror Schwarzschild-Couder Telescope (SCT) design is a candidate design for CTA Medium-Sized Telescopes. A prototype SCT (pSCT) has been constructed at the Fred Lawrence Whipple Observatory in Arizona, USA. Its camera is currently partially instrumented with 1600 pixels covering a field of view of 2.7 degrees square. The small plate scale of the optical system allows densely packed silicon photomultipliers to be used, which combined with high-density trigger and waveform readout electronics enable the high-resolution camera. The camera's electronics are capable of imaging air shower development at a rate of one billion samples per second. We describe the commissioning and performance of the pSCT camera, including trigger and waveform readout performance, calibration, and absolute GPS time stamping. We also present the upgrade to the camera, which is currently underway. The upgrade will fully populate the focal plane, increasing the field of view to 8 degree diameter, and lower the front-end electronics noise, enabling a lower trigger threshold and improved reconstruction and background rejection.

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  28. Deep-learning-driven event reconstruction applied to simulated data from a single Large-Sized Telescope of CTA

    Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Artero M., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Becerra González J., Bernardos M.I., Berti A., Biederbeck N., Bigongiari C., Blanch O., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Carosi A., Cassol F., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., Dalchenko M., De Angelis A., de Bony de Lavergne M., Deleglise G., Delgado C., Delgado Mengual J., della Volpe D., Depaoli D., Di Pierro F., Di Venere L., Díaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsässer D., Emery G., Escudero J., Fiasson A., Foffano L., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Giglietto N., Giordano F., Gliwny P., Godinovic N., Green D., Grespan P., Gunji S., Hackfeld J., Hadasch D., Hahn A., Hassan T., Hayashi K., Heckmann L., Heller M., Herrera Llorente J., Hirotani K., Hoffmann D., Horns D., Houles J., Hrabovsky M., Hrupec D., Hui D., Hütten M., Inada T., Inome Y., Iori M., Ishio K., Iwamura Y., Jacquemont M., Jimenez Martinez I., Jouvin L., Jurysek J.

    Proceedings of Science   Vol. 395   2022.3

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    When very-high-energy gamma rays interact high in the Earth's atmosphere, they produce cascades of particles that induce flashes of Cherenkov light. Imaging Atmospheric Cherenkov Telescopes (IACTs) detect these flashes and convert them into shower images that can be analyzed to extract the properties of the primary gamma ray. The dominant background for IACTs is comprised of air shower images produced by cosmic hadrons, with typical noise-to-signal ratios of several orders of magnitude. The standard technique adopted to differentiate between images initiated by gamma rays and those initiated by hadrons is based on classical machine learning algorithms, such as Random Forests, that operate on a set of handcrafted parameters extracted from the images. Likewise, the inference of the energy and the arrival direction of the primary gamma ray is performed using those parameters. State-of-the-art deep learning techniques based on convolutional neural networks (CNNs) have the potential to enhance the event reconstruction performance, since they are able to autonomously extract features from raw images, exploiting the pixel-wise information washed out during the parametrization process. Here we present the results obtained by applying deep learning techniques to the reconstruction of Monte Carlo simulated events from a single, next-generation IACT, the Large-Sized Telescope (LST) of the Cherenkov Telescope Array (CTA). We use CNNs to separate the gamma-ray-induced events from hadronic events and to reconstruct the properties of the former, comparing their performance to the standard reconstruction technique. Three independent implementations of CNN-based event reconstruction models have been utilized in this work, producing consistent results.

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  29. Cross-calibration and combined analysis of the CTA-LST prototype and the MAGIC telescopes

    Ohtani Y., Berti A., Depaoli D., Di Pierro F., Green D., Heckmann L., Hütten M., Inada T., López-Coto R., Medina E., Moralejo A., Morcuende D., Pirola G., Strzys M., Suda Y., Vovk I., Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Artero M., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Becerra González J., Bernardos M.I., Biederbeck N., Bigongiari C., Blanch O., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Carosi A., Cassol F., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., Dalchenko M., De Angelis A., de Bony de Lavergne M., Deleglise G., Delgado C., Delgado Mengual J., della Volpe D., Di Venere L., Díaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsässer D., Emery G., Escudero J., Fiasson A., Foffano L., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Giglietto N., Giordano F., Gliwny P., Godinovic N., Grespan P., Gunji S., Hackfeld J., Hadasch D., Hahn A., Hassan T., Hayashi K., Heller M., Herrera Llorente J., Hirotani K., Hoffmann D., Horns D., Houles J., Hrabovsky M., Hrupec D.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) will be the next generation gamma-ray observatory, which will consist of three kinds of telescopes of different sizes. Among those, the Large Size Telescope (LST) will be the most sensitive in the low energy range starting from 20 GeV. The prototype LST (LST-1) proposed for CTA was inaugurated in October 2018 in the northern hemisphere site, La Palma (Spain), and is currently in its commissioning phase. MAGIC is a system of two gamma-ray Cherenkov telescopes of the current generation, located approximately 100 m away from LST-1, that have been operating in stereoscopic mode since 2009. Since LST-1 and MAGIC can observe the same air shower events, we can compare the brightness of showers, estimated energies of gamma rays, and other parameters event by event, which can be used to cross-calibrate the telescopes. Ultimately, by performing combined analyses of the events triggering the three telescopes, we can reconstruct the shower geometry more accurately, leading to better energy and angular resolutions, and a better discrimination of the background showers initiated by cosmic rays. For that purpose, as part of the commissioning of LST-1, we performed joint observations of established gamma-ray sources with LST-1 and MAGIC. Also, we have developed Monte Carlo simulations for such joint observations and an analysis pipeline which finds event coincidence in the offline analysis based on their timestamps. In this work, we present the first detection of an astronomical source, the Crab Nebula, with combined observation of LST-1 and MAGIC. Moreover, we show results of the inter-telescope cross-calibration obtained using Crab Nebula data taken during joint observations with LST-1 and MAGIC.

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  30. Commissioning of the camera of the first Large Size Telescope of the Cherenkov Telescope Array

    Saito T., Delgado C., Blanch O., Artero M., Barrio J.A., Cassol F., Diaz C., Hadasch D., Hoffmann D., Houles J., Inome Y., Iori M., Jouvin L., Kerszberg D., Kobayashi Y., Kubo H., Martinez G., Mazin D., Moretti E., Nakamori T., Nozaki S., Oka T., Okumura A., Palatiello M., Polo M., Prast J., Sakurai S., Sunada Y., Takahashi M., Takeishi R., Tejedor L.A., Yamamoto T., Yoshida T., Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Batkovic I., Becerra González J., Bernardos M.I., Berti A., Biederbeck N., Bigongiari C., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Carosi A., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., Dalchenko M., De Angelis A., de Bony de Lavergne M., Deleglise G., Delgado Mengual J., della Volpe D., Depaoli D., Di Pierro F., Di Venere L., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsässer D., Emery G., Escudero J., Fiasson A., Foffano L., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Giglietto N., Giordano F., Gliwny P., Godinovic N., Green D.

    Proceedings of Science   Vol. 395   2022.3

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    The first Large Size Telescope (LST-1) of the Cherenkov Telescope Array has been operational since October 2018 at La Palma, Spain. We report on the results obtained during the camera commissioning. The noise level of the readout is determined as a 0.2 p.e. level. The gain of PMTs are well equalized within 2% variation, using the calibration flash system. The effect of the night sky background on the signal readout noise as well as the PMT gain estimation are also well evaluated. Trigger thresholds are optimized for the lowest possible gamma-ray energy threshold and the trigger distribution synchronization has been achieved within 1 ns precision. Automatic rate control realizes the stable observation with 1.5% rate variation over 3 hours. The performance of the novel DAQ system demonstrates a less than 10% dead time for 15 kHz trigger rate even with sophisticated online data correction.

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  31. Camera Calibration of the CTA-LST prototype

    Kobayashi Y., Okumura A., Cassol F., Katagiri H., Sitarek J., Gliwny P., Nozaki S., Nogami Y., Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Artero M., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Becerra Gonzalez J., Bernardos M.I., Berti A., Biederbeck N., Bigongiari C., Blanch O., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Carosi A., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., Dalchenko M., De Angelis A., de Bony de Lavergne M., Deleglise G., Delgado C., Delgado Mengual J., della Volpe D., Depaoli D., Di Pierro F., Di Venere L., Daaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsaasser D., Emery G., Escudero J., Fiasson A., Foffano L., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia Lapez R., Giglietto N., Giordano F., Godinovic N., Green D., Grespan P., Gunji S., Hackfeld J., Hadasch D., Hahn A., Hassan T., Hayashi K., Heckmann L., Heller M., Herrera Llorente J., Hirotani K., Hoffmann D., Horns D., Houles J., Hrabovsky M., Hrupec D., Hui D., HÃŒtten M., Inada T., Inome Y., Iori M.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) is the next-generation gamma-ray observatory that is expected to reach one order of magnitude better sensitivity than that of current telescope arrays. The Large-Sized Telescopes (LSTs) have an essential role in extending the energy range down to 20 GeV. The prototype LST (LST-1) proposed for CTA was built in La Palma, the northern site of CTA, in 2018. LST-1 is currently in its commissioning phase and moving towards scientific observations. The LST-1 camera consists of 1855 photomultiplier tubes (PMTs) which are sensitive to Cherenkov light. PMT signals are recorded as waveforms sampled at 1 GHz rate with Domino Ring Sampler version 4 (DRS4) chips. Fast sampling is essential to achieve a low energy threshold by minimizing the integration of background light from the night sky. Absolute charge calibration can be performed by the so-called F-factor method, which allows calibration constants to be monitored even during observations. A calibration pipeline of the camera readout has been developed as part of the LST analysis chain. The pipeline performs DRS4 pedestal and timing corrections, as well as the extraction and calibration of charge and time of pulses for subsequent higher-level analysis. The performance of each calibration step is examined, and especially charge and time resolution of the camera readout are evaluated and compared to CTA requirements. We report on the current status of the calibration pipeline, including the performance of each step through to signal reconstruction, and the consistency with Monte Carlo simulations.

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  32. Application of pattern spectra and convolutional neural networks to the analysis of simulated Cherenkov Telescope Array data

    Aschersleben J., Peletier R.F., Vecchi M., Wilkinson M.H.F., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D., Bernardini E.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) will be the next generation gamma-ray observatory and will be the major global instrument for very-high-energy astronomy over the next decade, offering 5 − 10 × better flux sensitivity than current generation gamma-ray telescopes. Each telescope will provide a snapshot of gamma-ray induced particle showers by capturing the induced Cherenkov emission at ground level. The simulation of such events provides images that can be used as training data for convolutional neural networks (CNNs) to determine the energy of the initial gamma rays. Compared to other state-of-the-art algorithms, analyses based on CNNs promise to further enhance the performance to be achieved by CTA. Pattern spectra are commonly used tools for image classification and provide the distributions of the shapes and sizes of various objects comprising an image. The use of relatively shallow CNNs on pattern spectra would automatically select relevant combinations of features within an image, taking advantage of the 2D nature of pattern spectra. In this work, we generate pattern spectra from simulated gamma-ray events instead of using the raw images themselves in order to train our CNN for energy reconstruction. This is different from other relevant learning and feature selection methods that have been tried in the past. Thereby, we aim to obtain a significantly faster and less computationally intensive algorithm, with minimal loss of performance.

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  33. Analysis of the Cherenkov Telescope Array first Large-Sized Telescope real data using convolutional neural networks

    Vuillaume T., Jacquemont M., de Bony de Lavergne M., Sanchez D.A., Poireau V., Maurin G., Benoit A., Lambert P., Lamanna G., Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Artero M., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Becerra González J., Bernardos M.I., Berti A., Biederbeck N., Bigongiari C., Blanch O., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Carosi A., Cassol F., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., Dalchenko M., De Angelis A., Deleglise G., Delgado C., Delgado Mengual J., della Volpe D., Depaoli D., Di Pierro F., Di Venere L., Díaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsässer D., Emery G., Escudero J., Fiasson A., Foffano L., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Giglietto N., Giordano F., Gliwny P., Godinovic N., Green D., Grespan P., Gunji S., Hackfeld J., Hadasch D., Hahn A., Hassan T., Hayashi K., Heckmann L., Heller M., Herrera Llorente J., Hirotani K., Hoffmann D., Horns D., Houles J., Hrabovsky M., Hrupec D., Hui D., Hütten M., Inada T.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) is the future ground-based gamma-ray observatory and will be composed of two arrays of imaging atmospheric Cherenkov telescopes (IACTs) located in the Northern and Southern hemispheres respectively. The first CTA prototype telescope built on-site, the Large-Sized Telescope (LST-1), is under commissioning in La Palma and has already taken data on numerous known sources. IACTs detect the faint flash of Cherenkov light indirectly produced after a very energetic gamma-ray photon has interacted with the atmosphere and generated an atmospheric shower. Reconstruction of the characteristics of the primary photons is usually done using a parameterization up to the third order of the light distribution of the images. In order to go beyond this classical method, new approaches are being developed using state-of-the-art methods based on convolutional neural networks (CNN) to reconstruct the properties of each event (incoming direction, energy and particle type) directly from the telescope images. While promising, these methods are notoriously difficult to apply to real data due to differences (such as different levels of night sky background) between Monte Carlo (MC) data used to train the network and real data. The GammaLearn project, based on these CNN approaches, has already shown an increase in sensitivity on MC simulations for LST-1 as well as a lower energy threshold. This work applies the GammaLearn network to real data acquired by LST-1 and compares the results to the classical approach that uses random forests trained on extracted image parameters. The improvements on the background rejection, event direction, and energy reconstruction are discussed in this contribution.

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  34. Prospects for Galactic transient sources detection with the Cherenkov Telescope Array

    López-Oramas A., Bulgarelli A., Chaty S., Chernyakova M., Gnatyk R., Hnatyk B., Kantzas D., Markoff S., McKeague S., Mereghetti S., Mestre E., di Piano A., Romano P., Sadeh I., Sergijenko O., Sidoli L., Spolon A., de Ona Wilhelmi E., Piano G., Zampieri L., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D.

    Proceedings of Science   Vol. 395   2022.3

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    Several types of Galactic sources, like magnetars, microquasars, novae or pulsar wind nebulae flares, display transient emission in the X-ray band. Some of these sources have also shown emission at MeV-GeV energies. However, none of these Galactic transients have ever been detected in the very-high-energy (VHE; E>100 GeV) regime by any Imaging Air Cherenkov Telescope (IACT). The Galactic Transient task force is a part of the Transient Working group of the Cherenkov Telescope Array (CTA) Consortium. The task force investigates the prospects of detecting the VHE counterpart of such sources, as well as their study following Target of Opportunity (ToO) observations. In this contribution, we will show some of the results of exploring the capabilities of CTA to detect and observe Galactic transients; we assume different array configurations and observing strategies.

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  35. The Small-Sized Telescopes for the Southern Site of the Cherenkov Telescope Array

    Amans J.P., Berge D., Bonanno G., Bose R.B., Brown A.M., Buckley J.H., Chadwick P.M., Conte F., Cotter G., De Frondat F., De Simone N., Dournaux J.L., Duffy C.A., Einecke S., Fasola G., Funk S., Giavitto G., Hinton J.A., Huet J.M., La Palombara N., Lapington J.S., Laporte P., Leach S.A., Leto G., Lloyd S., Lombardi S., Nayak A., Okumura A., Pareschi G., Prokoph H., Rébert E., Ross D., Rowell G., Scuderi S., Sol H., Spencer S., Tajima H., Trois A., Vercellone S., Vink J., Watson J.J., White R., Zech A.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) will use three telescope sizes to efficiently detect cosmic gamma rays in the energy range from several tens of GeV to hundreds of TeV. The Small-Sized Telescopes (SSTs) will form the largest section of the array, covering an area of many square kilometres on the CTA southern site in Paranal, Chile. Up to 70 SSTs will be implemented by an international consortium of institutes and teams as an in-kind contribution to the CTA Observatory. The SSTs will provide unprecedented sensitivity to gamma rays above 1 TeV and the highest angular resolution of any instrument above the hard X-ray band. CTA has recently finalised the technology that will be used for the SSTs: the telescopes will be a dual-reflector design with a primary reflector of 4 m diameter, equipped with an SiPM-based camera with full waveform readout from ∼2000 channels covering a ∼9° field of view. The Schwarzschild-Couder optical configuration leads to a small plate-scale, and consequently a compact, cost-efficient camera. In this contribution, we describe the experience gained operating telescope and camera prototypes during the CTA preparatory phase, and the development of the final SST design.

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  36. The Cherenkov Telescope Array: layout, design and performance

    Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D., Bernardini E., Bernardos M.I., Bernlöhr K., Berti A.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) will be the next generation very-high-energy gamma-ray observatory. CTA is expected to provide substantial improvement in accuracy and sensitivity with respect to existing instruments thanks to a tenfold increase in the number of telescopes and their state-of-the-art design. Detailed Monte Carlo simulations are used to further optimise the number of telescopes and the array layout, and to estimate the observatory performance using updated models of the selected telescope designs. These studies are presented in this contribution for the two CTA stations located on the island of La Palma (Spain) and near Paranal (Chile) and for different operation and observation conditions.

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  37. The Cherenkov Telescope Array transient and multi-messenger program

    Carosi A., López-Oramas A., Longo F., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D., Bernardini E.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) is a next generation ground-based very-high-energy gamma-ray observatory that will allow for observations in the >10 GeV range with unprecedented photon statistics and sensitivity. This will enable the investigation of the yet-marginally explored physics of short-time-scale transient events. CTA will thus become an invaluable instrument for the study of the physics of the most extreme and violent objects and their interactions with the surrounding environment. The CTA Transient program includes follow-up observations of a wide range of multi-wavelength and multi-messenger alerts, ranging from compact galactic binary systems to extragalactic events such as gamma-ray bursts (GRBs), core-collapse supernovae and bright AGN flares. In recent years, the first firm detection of GRBs by current Cherenkov telescope collaborations, the proven connection between gravitational waves and short GRBs, as well as the possible neutrino-blazar association with TXS 0506+056 have shown the importance of coordinated follow-up observations triggered by these different cosmic signals in the framework of the birth of multi-messenger astrophysics. In the next years, CTA will play a major role in these types of observations by taking advantage of its fast slewing (especially for the CTA Large Size Telescopes), large effective area and good sensitivity, opening new opportunities for time-domain astrophysics in an energy range not affected by selective absorption processes typical of other wavelengths. In this contribution we highlight the common approach adopted by the CTA Transients physics working group to perform the study of transient sources in the very-high-energy regime.

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  38. Status and results of the prototype LST of CTA

    Mazin D., Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Artero M., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Becerra González J., Bernardos M.I., Berti A., Biederbeck N., Bigongiari C., Blanch O., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Carosi A., Cassol F., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., Dalchenko M., De Angelis A., de Bony de Lavergne M., Deleglise G., Delgado C., Delgado Mengual J., della Volpe D., Depaoli D., Di Pierro F., Di Venere L., Díaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsässer D., Emery G., Escudero J., Fiasson A., Foffano L., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Giglietto N., Giordano F., Gliwny P., Godinovic N., Green D., Grespan P., Gunji S., Hackfeld J., Hadasch D., Hahn A., Hassan T., Hayashi K., Heckmann L., Heller M., Herrera Llorente J., Hirotani K., Hoffmann D., Horns D., Houles J., Hrabovsky M., Hrupec D., Hui D., Hütten M., Inada T., Inome Y., Iori M., Ishio K., Iwamura Y., Jacquemont M., Jimenez Martinez I., Jouvin L.

    Proceedings of Science   Vol. 395   2022.3

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    The Large-Sized Telescopes (LSTs) of Cherenkov Telescope Array (CTA) are designed for gamma-ray studies focusing on low energy threshold, high flux sensitivity, rapid telescope repositioning speed and a large field of view. Once the CTA array is complete, the LSTs will be dominating the CTA performance between 20 GeV and 150 GeV. During most of the CTA Observatory construction phase, however, the LSTs will be dominating the array performance until several TeVs. In this presentation we will report on the status of the LST-1 telescope inaugurated in La Palma, Canary islands, Spain in 2018. We will show the progress of the telescope commissioning, compare the expectations with the achieved performance, and give a glance of the first physics results.

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  39. Southern African Large Telescope Spectroscopy of BL Lacs for the CTA project

    Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D., Bernardini E., Bernardos M.I., Bernlöhr K., Berti A.

    Proceedings of Science   Vol. 395   2022.3

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    In the last two decades, very-high-energy gamma-ray astronomy has reached maturity: over 200 sources have been detected, both Galactic and extragalactic, by ground-based experiments. At present, Active Galactic Nuclei (AGN) make up about 40% of the more than 200 sources detected at very high energies with ground-based telescopes, the majority of which are blazars, i.e. their jets are closely aligned with the line of sight to Earth and three quarters of which are classified as high-frequency peaked BL Lac objects. One challenge to studies of the cosmological evolution of BL Lacs is the difficulty of obtaining redshifts from their nearly featureless, continuum-dominated spectra. It is expected that a significant fraction of the AGN to be detected with the future Cherenkov Telescope Array (CTA) observatory will have no spectroscopic redshifts, compromising the reliability of BL Lac population studies, particularly of their cosmic evolution. We started an effort in 2019 to measure the redshifts of a large fraction of the AGN that are likely to be detected with CTA, using the Southern African Large Telescope (SALT). In this contribution, we present two results from an on-going SALT program focused on the determination of BL Lac object redshifts that will be relevant for the CTA observatory.

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  40. Sensitivity of the Cherenkov Telescope Array to emission from the gamma-ray counterparts of neutrino events

    Sergijenko O., Brown A.M., Fiorillo D.F.G., de León A.R., Satalecka K., Tung C.F., Reimann R., Glauch T., Taboada I., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W.

    Proceedings of Science   Vol. 395   2022.3

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    We investigate the possibility of detection of the VHE gamma-ray counterparts to the neutrino astrophysical sources within the Neutrino Target of Opportunity (NToO) program of CTA using the populations simulated by the FIRESONG software to resemble the diffuse astrophysical neutrino flux measured by IceCube. We derive the detection probability for different zenith angles and geomagnetic field configurations. The difference in detectability of sources between CTA-North and CTA-South for the average geomagnetic field is not substantial. We investigate the effect of a higher night-sky background and the preliminary CTA Alpha layout on the detection probability.

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  41. Sensitivity of the Cherenkov Telescope Array to a dark matter signal from the Galactic centre

    Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D., Bernardini E., Bernardos M.I., Bernlöhr K., Berti A.

    Proceedings of Science   Vol. 395   2022.3

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    High-energy gamma rays are promising tools to constrain or reveal the nature of dark matter, in particular Weakly Interacting Massive Particles. Being well into its pre-construction phase, the Cherenkov Telescope Array (CTA) will soon probe the sky in the 20 GeV - 300 TeV energy range. Thanks to its improved energy and angular resolutions as well as significantly larger effective area when compared to the current generation of Cherenkov telescopes, CTA is expected to probe heavier dark matter, with unprecedented sensitivity, reaching the thermal annihilation cross-section at 1 TeV. This talk will summarise the planned dark matter search strategies with CTA, focusing on the signal from the Galactic centre. As observed with the Fermi LAT at lower energies, this region is rather complex and CTA will be the first ground-based observatory sensitive to the large scale diffuse astrophysical emission from that region. We report on the collaboration effort to study the impact of such extended astrophysical backgrounds on the dark matter search, based on Fermi-LAT data in order to guide our observational strategies, taking into account various sources of systematic uncertainty.

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  42. Sensitivity of CTA to gamma-ray emission from the Perseus galaxy cluster

    Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D., Bernardini E., Bernardos M.I., Bernlöhr K., Berti A.

    Proceedings of Science   Vol. 395   2022.3

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    In these proceedings we summarize the current status of the study of the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse gamma-ray emission from the Perseus galaxy cluster. Gamma-ray emission is expected in galaxy clusters both from interactions of cosmic rays (CR) with the intra-cluster medium, or as a product of annihilation or decay of dark matter (DM) particles in case they are weakly interactive massive particles (WIMPs). The observation of Perseus constitutes one of the Key Science Projects to be carried out by the CTA Consortium. In this contribution, we focus on the DM-induced component of the flux. Our DM modelling includes the substructures we expect in the main halo which will boost the annihilation signal significantly. We adopt an ON/OFF observation strategy and simulate the expected gamma-ray signals. Finally we compute the expected CTA sensitivity using a likelihood maximization analysis including the most recent CTA instrument response functions. In absence of signal, we show that CTA will allow us to provide stringent and competitive constraints on TeV DM, especially for the case of DM decay.

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  43. Searching for very-high-energy electromagnetic counterparts to gravitational-wave events with the Cherenkov Telescope Array

    Patricelli B., Carosi A., Nava L., Seglar-Arroyo M., Schüssler F., Stamerra A., Adelfio A., Ashkar H., Bulgarelli A., Di Girolamo T., Di Piano A., Gasparetto T., Green J., Longo F., Agudo I., Berti A., Bissaldi E., Cella G., Circiello A., Covino S., Ghirlanda G., Humensky B., Inoue S., Lefaucheur J., Filipovic M., Razzano M., Ribeiro D., Sergijenko O., Stratta G., Vergani S., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A.

    Proceedings of Science   Vol. 395   2022.3

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    The detection of electromagnetic (EM) emission following the gravitational wave (GW) event GW170817 opened the era of multi-messenger astronomy with GWs and provided the first direct evidence that at least a fraction of binary neutron star (BNS) mergers are progenitors of short Gamma-Ray Bursts (GRBs). GRBs are also expected to emit very-high energy (VHE, > 100 GeV) photons, as proven by the recent MAGIC and H.E.S.S. observations. One of the challenges for future multi-messenger observations will be the detection of such VHE emission from GRBs in association with GWs. In the next years, the Cherenkov Telescope Array (CTA) will be a key instrument for the EM follow-up of GW events in the VHE range, owing to its unprecedented sensitivity, rapid response, and capability to monitor a large sky area via scan-mode operation. We present the CTA GW follow-up program, with a focus on the searches for short GRBs possibly associated with BNS mergers. We investigate the possible observational strategies and we outline the prospects for the detection of VHE EM counterparts to transient GW events.

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  44. ROBAST 3

    Okumura A.

    Proceedings of Science   Vol. 395   2022.3

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    The ROOT-based simulator for ray tracing (ROBAST) is an open-source C++ library to simulate various types of cosmic-ray (CR) and gamma-ray telescopes. It is used in multiple purposes in all the different telescope designs of the Cherenkov Telescope Array and is a promising tool for use in other future projects in optics simulations. We have released ROBAST 3 that supports interference calculations in multilayer coating in addition to geometrical optics. Here, we present its new functionality and several recent applications in future CR telescopes.

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  45. Reconstruction of stereoscopic CTA events using deep learning with CTLearn

    Miener T., Nieto D., Brill A., Spencer S., Contreras J.L., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA), conceived as an array of tens of imaging atmospheric Cherenkov telescopes (IACTs), is an international project for a next-generation ground-based gamma-ray observatory, aiming to improve on the sensitivity of current-generation instruments a factor of five to ten and provide energy coverage from 20 GeV to more than 300 TeV. Arrays of IACTs probe the very-high-energy gamma-ray sky. Their working principle consists of the simultaneous observation of air showers initiated by the interaction of very-high-energy gamma rays and cosmic rays with the atmosphere. Cherenkov photons induced by a given shower are focused onto the camera plane of the telescopes in the array, producing a multi-stereoscopic record of the event. This image contains the longitudinal development of the air shower, together with its spatial, temporal, and calorimetric information. The properties of the originating very-high-energy particle (type, energy, and incoming direction) can be inferred from those images by reconstructing the full event using machine learning techniques. In this contribution, we present a purely deep-learning driven, full-event reconstruction of simulated, stereoscopic IACT events using CTLearn. CTLearn is a package that includes modules for loading and manipulating IACT data and for running deep learning models, using pixel-wise camera data as input.

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  46. Reconstruction of extensive air shower images of the first Large Size Telescope prototype of CTA using a novel likelihood technique

    Emery G., Alispach C., Dalchenko M., Foffano L., Heller M., Montaruli T., Abe H., Aguasca A., Agudo I., Antonelli L.A., Aramo C., Armstrong T., Artero M., Asano K., Ashkar H., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Becerra González J., Bernardos M.I., Berti A., Biederbeck N., Bigongiari C., Blanch O., Bonnoli G., Bordas P., Bose D., Bulgarelli A., Burelli I., Buscemi M., Cardillo M., Caroff S., Carosi A., Cassol F., Cerruti M., Chai Y., Cheng K., Chikawa M., Chytka L., Contreras J.L., Cortina J., Costantini H., De Angelis A., de Bony de Lavergne M., Deleglise G., Delgado C., Delgado Mengual J., della Volpe D., Depaoli D., Di Pierro F., Di Venere L., Díaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Elsässer D., Escudero J., Fiasson A., Fonseca M.V., Freixas Coromina L., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Giglietto N., Giordano F., Gliwny P., Godinovic N., Green D., Grespan P., Gunji S., Hackfeld J., Hadasch D., Hahn A., Hassan T., Hayashi K., Heckmann L., Herrera Llorente J., Hirotani K., Hoffmann D., Horns D., Houles J., Hrabovsky M., Hrupec D., Hui D., Hütten M., Inada T., Inome Y., Iori M., Ishio K., Iwamura Y., Jacquemont M., Jimenez Martinez I.

    Proceedings of Science   Vol. 395   2022.3

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    Ground-based gamma-ray astronomy aims at reconstructing the energy and direction of gamma rays from the extensive air showers they initiate in the atmosphere. Imaging Atmospheric Cherenkov Telescopes (IACT) collect the Cherenkov light induced by secondary charged particles in extensive air showers (EAS), creating an image of the shower in a camera positioned in the focal plane of optical systems. This image is used to evaluate the type, energy and arrival direction of the primary particle that initiated the shower. This contribution shows the results of a novel reconstruction method based on likelihood maximization. The novelty with respect to previous likelihood reconstruction methods lies in the definition of a likelihood per single camera pixel, accounting not only for the total measured charge, but also for its development over time. This leads to more precise reconstruction of shower images. The method is applied to observations of the Crab Nebula acquired with the Large Size Telescope prototype (LST-1) deployed at the northern site of the Cherenkov Telescope Array.

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  47. Prototype Schwarzschild-Couder Telescope for the Cherenkov Telescope Array: Commissioning the Optical System

    Ribeiro D., Adams C.B., Ambrosi G., Ambrosio M., Aramo C., Batista P.I., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolontà C., Bose R., Brill A., Buckley J.H., Cameron R.A., Canestrari R., Capasso M., Caprai M., Covault C.E., Depaoli D., Di Venere L., Errando M., Fegan S., Feng Q., Fiandrini E., Furniss A., Gent A., Giglietto N., Giordano F., Giro E., Halliday R., Hervet O., Humensky T.B., Incardona S., Ionica M., Jin W., Kieda D., Licciulli F., Loporchio S., Marsella G., Masone V., Meagher K., Meures T., Mode B.A.W., Mognet S.A.I., Mukherjee R., Nieto D., Okumura A., Otte N., Pantaleo F.R., Paoletti R., Pareschi G., Di Pierro F., Pueschel E., Riitano L., Roache E., Rousselle J., Rugliancich A., Santander M., Shang R., Stiaccini L., Taylor L.P., Tosti L., Tovmassian G., Tripodo G., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V.V., Williams D.A., Yu P.

    Proceedings of Science   Vol. 395   2022.3

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    A prototype Schwarzschild-Couder Telescope (pSCT) has been constructed at the Fred Lawrence Whipple Observatory as a candidate for the medium-sized telescopes of the Cherenkov Telescope Array Observatory (CTAO). CTAO is currently entering early construction phase of the project and once completed it will vastly improve very high energy gamma-ray detection component in multiwavelength and multi-messenger observations due to significantly improved sensitivity, angular resolution and field of view comparing to the current generation of the ground-based gamma-ray observatories H.E.S.S., MAGIC and VERITAS. The pSCT uses a dual aspheric mirror design with a 9.7 m primary mirror and 5.4 m secondary mirror, both of which are segmented. The Schwarzschild-Couder (SC) optical system (OS) selected for the prototype telescope achieves wide field of view of 8 degrees and simultaneously reduces the focal plane plate scale allowing an unprecedented compact (0.78m diameter) implementation of the high-resolution camera (6mm/0.067deg per imaging pixel with 11, 328 pixels) based on the silicon photo-multipliers (SiPMs). The OS of the telescope is designed to eliminate spherical and comatic aberrations and minimize astigmatism to radically improve off-axis imaging and consequently angular resolution across all the field of view with respect to the conventional single-mirror telescopes. Fast and high imaging resolution OS of the pSCT comes with the challenging submillimeter-precision custom alignment system, which was successfully demonstrated with an on-axis point spread function (PSF) of 2.9 arcmin prior to the first-light detection of the Crab Nebula in 2020. Ongoing commissioning activities aim to meet the on-axis PSF design goal of 2.6 arcmin, verify the off-axis performance of the pSCT OS, and develop techniques to maintain alignment stability over telescope structural deformations from pointing and temperature variations. In this contribution, we report on the commissioning status, the optical alignment procedures adopted for segmented OS, and alignment progress to verify and validate design requirements.

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  48. Prototype Open Event Reconstruction Pipeline for the Cherenkov Telescope Array

    Nöthe M., Kosack K., Nickel L., Peresano M., Abdalla H., Abe H., Abe S., Abusleme A., Acero F., Acharyya A., Acín Portella V., Ackley K., Adam R., Adams C., Adhikari S.S., Aguado-Ruesga I., Agudo I., Aguilera R., Aguirre-Santaella A., Aharonian F., Alberdi A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amans J.P., Amati L., Amato E., Ambrogi L., Ambrosi G., Ambrosio M., Ammendola R., Anderson J., Anduze M., Angüner E.O., Antonelli L.A., Antonuccio V., Antoranz P., Anutarawiramkul R., Aragunde Gutierrez J., Aramo C., Araudo A., Araya M., Arbet-Engels A., Arcaro C., Arendt V., Armand C., Armstrong T., Arqueros F., Arrabito L., Arsioli B., Artero M., Asano K., Ascasíbar Y., Aschersleben J., Ashley M., Attinà P., Aubert P., Singh C.B., Baack D., Babic A., Backes M., Baena V., Bajtlik S., Baktash A., Balazs C., Balbo M., Ballester O., Ballet J., Balmaverde B., Bamba A., Bandiera R., Baquero Larriva A., Barai P., Barbier C., Barbosa Martins V., Barcelo M., Barkov M., Barnard M., Baroncelli L., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Bauer C., Bautista-González R., Baxter J., Becciani U., Becerra González J., Becherini Y., Beck G., Becker Tjus J., Bednarek W., Belfiore A., Bellizzi L., Belmont R., Benbow W., Berge D.

    Proceedings of Science   Vol. 395   2022.3

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    The Cherenkov Telescope Array (CTA) is the next-generation gamma-ray observatory currently under construction. It will improve over the current generation of imaging atmospheric Cherenkov telescopes (IACTs) by a factor of five to ten in sensitivity and it will be able to observe the whole sky from a combination of two sites: a northern site in La Palma, Spain, and a southern one in Paranal, Chile. CTA will also be the first open gamma-ray observatory. Accordingly, the data analysis pipeline is developed as open-source software. The event reconstruction pipeline accepts raw data of the telescopes and processes it to produce suitable input for the higher-level science tools. Its primary tasks include reconstructing the physical properties of each recorded shower and providing the corresponding instrument response functions. ctapipe is a framework providing algorithms and tools to facilitate raw data calibration, image extraction, image parameterization and event reconstruction. Its main focus is currently the analysis of simulated data but it has also been successfully applied for the analysis of data obtained with the first CTA prototype telescopes, such as the Large-Sized Telescope 1 (LST-1). pyirf is a library to calculate IACT instrument response functions, needed to obtain physics results like spectra and light curves, from the reconstructed event lists. Building on these two, protopipe is a prototype for the event reconstruction pipeline for CTA. Recent developments in these software packages will be presented.

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  49. Design and performance of the prototype Schwarzschild-Couder telescope camera

    Adams Colin B., Ambrosi Giovanni, Ambrosio Michelangelo, Aramo Carla, Arlen Timothy, Benbow Wystan, Bertucci Bruna, Bissaldi Elisabetta, Biteau Jonathan, Bitossi Massimiliano, Boiano Alfonso, Bonavolonta Carmela, Bose Richard, Bouvier Aurelien, Buscemi Mario, Brill Aryeh, Brown Anthony M., Buckley James H., Canestrari Rodolfo, Capasso Massimo, Caprai Mirco, Coppi Paolo, Covault Corbin E., Depaoli Davide, Di Venere Leonardo, Errando Manel, Fegan Stephan, Feng Qi, Fiandrini Emanuele, Furniss Amy, Garczarczyk Markus, Gent Alasdair, Giglietto Nicola, Giordano Francesco, Giro Enrico, Halliday Robert, Hervet Olivier, Hughes Gareth, Incardona Simone, Humensky Thomas B., Ionica Maria, Jin Weidong, Johnson Caitlin A., Kieda David, Krennrich Frank, Kuznetsov Andrey, Lapington Jon, Licciulli Francesco, Loporchio Serena, Marsella Giovanni, Masone Vincenzo, Meagher Kevin, Meures Thomas, Mode Brent A. W., Mognet Samuel A. I, Mukherjee Reshmi, Okumura Akira, Pantaleo Francesca R., Paoletti Riccardo, Di Pierro Federico, Ribeiro Deivid, Riitano Luca, Roache Emmet, Ross Duncan, Rousselle Julien, Rugliancich Andrea, Santander Marcos, Schneider Michael, Schoorlemmer Harm, Shang Ruo-Yu, Stevenson Brandon, Stiaccini Leonardo, Tajima Hiroyasu, Taylor Leslie P., Thornhill Julian, Tosti Luca, Tripodo Giovanni, Vagelli Valerio, Valentino Massimo, Vandenbroucke Justin, Vassiliev Vladimir V., Wakely Scott P., Watson Jason J., White Richard, Wilcox Patrick, Williams David A., Wood Matthew, Yu Peter, Zink Adrian

    JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS   Vol. 8 ( 1 )   2022.1

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Journal of Astronomical Telescopes, Instruments, and Systems  

    The prototype Schwarzschild-Couder Telescope (pSCT) is a candidate for a medium-sized telescope in the Cherenkov Telescope Array. The pSCT is based on a dual-mirror optics design that reduces the plate scale and allows for the use of silicon photomultipliers as photodetectors. The prototype pSCT camera currently has only the central sector instrumented with 25 camera modules (1600 pixels), providing a 2.68-deg field of view (FoV). The camera electronics are based on custom TARGET (TeV array readout with GSa/s sampling and event trigger) application-specific integrated circuits. Field programmable gate arrays sample incoming signals at a gigasample per second. A single backplane provides camera-wide triggers. An upgrade of the pSCT camera that will fully populate the focal plane is in progress. This will increase the number of pixels to 11,328, the number of backplanes to 9, and the FoV to 8.04 deg. Here, we give a detailed description of the pSCT camera, including the basic concept, mechanical design, detectors, electronics, current status, and first light.

    DOI: 10.1117/1.JATIS.8.1.014007

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  50. The Small-Sized Telescope of CTAO

    Tagliaferri G., Antonelli A., Arnesen T., Aschersleben J., Attina P., Balbo M., Bang S., Barcelo M., Baryshev A., Bellassai G., Berge D., Bicknell C., Bigongiari C., Bonnoli G., Bouley F., Brown A., Bulgarelli A., Cappi M., Caraveo P., Caschera S., Chadwick P., Conte F., Cotter G., Cristofari P., De Frondat F., Dal Pino E. De Gouveia, De Simone N., Depaoli D., Dournaux J-L, Duffy C., Einecke S., Fermino C., Funk S., Gargano C., Giavitto G., Giuliani A., Greenshaw T., Hinton J., Huet J-M, Iovenitti S., La Palombara N., Lapington J., Laporte P., Leach S., Lessio L., Leto G., Lloyd S., Lucarelli F., Lombardi S., Macchi A., Martinetti E., Micciche A., Millul R., Mineo T., Mitsunari T., Nayak A., Nicotra G., Okumura A., Pareschi G., Penno M., Prokoph H., Rebert E., Righi C., Rulten C., Russo F., Sanchez R. Zanmar, Saturni F. G., Schaefer J., Schwab B., Scuderi S., Sironi G., Sliusar V, Sol H., Spencer S., Stamerra A., Tajima H., Tavecchio F., Tosti G., Trois A., Vecchi M., Vercellone S., Vink J., Walter R., Watson J., White R., Zanin R., Zampieri L., Zech A., Zink A.

    GROUND-BASED AND AIRBORNE TELESCOPES IX   Vol. 12182   2022

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    The Cherenkov Telescope Array Observatory (CTAO) consists of three types of telescopes: large-sized (LST), mediumsized (MST), and small-sized (SST), distributed in two observing sites (North and South). For the CTA South "Alpha Configuration"the construction and installation of 37 (+5) SST telescopes (a number that could increase up to 70 in future upgrades) are planned. The SSTs are developed by an international consortium of institutes that will provide them as an in-kind contribution to CTAO. The SSTs rely on a Schwarzschild-Couder-like dual-mirror polynomial optical design, with a primary mirror of 4 m diameter, and are equipped with a focal plane camera based on SiPM detectors covering a field of view of ∼9°. The current SST concept was validated by developing the prototype dual-mirror ASTRI-Horn Cherenkov telescope and the CHEC-S SiPM focal plane camera. In this contribution, we will present an overview of the SST key technologies, the current status of the SST project, and the planned schedule.

    DOI: 10.1117/12.2627956

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  51. Camera design and performance of the prototype Schwarzschild-Couder Telescope for the Cherenkov Telescope Array

    Adams C., Ambrosi G., Ambrosio M., Aramo C., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolontá C., Bose R., Brill A., Buckley J.H., Caprai M., Di Venere L., Feng Q., Fiandrini E., Giglietto N., Giordano F., Hervet O., Hughes G., Humensky T.B., Ionica M., Jin W., Kaaret P., Kieda D., Kim B., Licciulli F., Loporchio S., Masone V., Meures T., Mode B.A.W., Mukherjee R., Pantaleo F.R., Okumura A., Petrashyk A., Powell J., Paoletti R., Ribeiro D., Rugliancich A., Santander M., Shang R., Stevenson B., Stiaccini L., Taylor L.P., Tosti L., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V., Wilcox P., Williams D.A.

    Proceedings of Science   Vol. 358   2021.7

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    The Schwarzschild-Couder Telescope (SCT) is a candidate technology for a medium-sized telescope within the Cherenkov Telescope Array, the next generation ground based observatory for very high energy gamma ray astronomy. The SCT uses a novel two-mirror design and is expected to yield improvements in field of view and image resolution compared to traditional Cherenkov telescopes based on single-mirror-dish optics. To match the improved optical resolution, challenging requirements of high channel count and density at low power consumption must be overcome by the camera. The prototype camera, currently commissioned and tested on the prototype SCT, has been developed based on millimeter scale SiPM pixels and a custom high density digitizer ASIC, TARGET, to provide 1600 pixels spanning a 2.7 degree field of view while being able to sample nanosecond photon pulses. It is mechanically designed to allow for an upgrade to 11,328 pixels covering a field of view of 8 degrees and demonstrating the full potential of the technology. The camera was installed on the telescope in 2018. We will present its design and performance including first light data.

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  52. Development and operations of INFN optical modules for the SCT Telescope camera proposed for the Cherenkov Telescope Array Observatory

    Adams C., Ambrosi G., Ambrosio M., Aramo C., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolontà C., Bose R., Brill A., Buckley J.H., Caprai M., Covault C.E., Di Venere L., Feng Q., Fiandrini E., Gent A., Giglietto N., Giordano F., Halliday R., Hervet O., Hughes G., Humensky T.B., Ionica M., Jin W., Kaaret P., Kieda D., Kim B., Licciulli F., Loporchio S., Masone V., Meures T., Mode B.A.W., Mukherjee R., Okumura A., Otte N., Pantaleo F.R., Paoletti R., Petrashyk A., Powell J., Powell K., Ribeiro D., Rugliancich A., Santander M., Shang R., Stevenson B., Stiaccini L., Taylor L.P., Tosti L., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V., Wilcox P., Williams D.A.

    Proceedings of Science   Vol. 358   2021.7

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Proceedings of Science  

    The Schwarzschild-Couder Telescope (SCT) is a proposal for the Medium Size Telescopes of the Cherenkov Telescope Array. Its concept is based on a two-mirror optical system designed to improve the telescope field of view and image resolution with respect to the single mirror Davies-Cotton solution. The SCT camera is planned to be instrumented with 177 photodetection modules, each composed of 64 Silicon Photomultiplier (SiPM) pixels. The third generation of 6×6 mm2 high density NUV SiPMs (NUV-HD3) produced by Fondazione Bruno Kessler (FBK) in collaboration with INFN has been used to equip optical units to be integrated on the upgrade of the camera of the SCT prototype (pSCT). Each optical unit is composed of an array of 16 NUV-HD3 SiPMs coupled with the front-end electronics, which is designed for full-waveform nanosecond readout and digitization using the TARGET-7 ASIC. Several optical units have been assembled and tested in the laboratories of INFN and have been integrated on the camera of the pSCT telescope, that is currently operating at the Fred Lawrence Whipple Observatory. In this contribution we report on the development, assembly and calibration of the optical units that are currently taking data on the pSCT camera.

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  53. Prototype Schwarzschild-Couder Telescope for the Cherenkov Telescope Array: Commissioning Status of the Optical System

    Adams C., Ambrosi G., Ambrosio M., Aramo C., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolontà C., Bose R., Brill A., Buckley J.H., Caprai M., Covault C.E., Di Venere L., Fegan S., Feng Q., Fiandrini E., Gent A., Giglietto N., Giordano F., Halliday R., Hervet O., Hughes G., Humensky T.B., Ionica M., Jin W., Kaaret P., Kieda D., Kim B., Licciulli F., Loporchio S., Masone V., Meures T., Mode B.A.W., Mukherjee R., Okumura A., Otte N., Pantaleo F.R., Paoletti R., Petrashyk A., Powell J., Powell K., Ribeiro D., Rousselle J., Rugliancich A., Santander M., Shang R., Stevenson B., Stiaccini L., Taylor L.P., Tosti L., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V., Wilcox P., Williams D.A.

    Proceedings of Science   Vol. 358   2021.7

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Proceedings of Science  

    The Cherenkov Telescope Array (CTA), with more than 100 telescopes, will be the largest ever ground-based gamma-ray observatory and is expected to greatly improve on both gamma-ray detection sensitivity and energy coverage compared to current-generation detectors. The 9.7-m Schwarzschild-Couder telescope (SCT) is one of the two candidates for the medium size telescope (MST) design for CTA. The novel aplanatic dual-mirror SCT design offers a wide field-of-view with a compact plate scale, allowing for a large number of camera pixels that improves the angular resolution and reduce the night sky background noise per pixel compared to the traditional single-mirror Davies-Cotton (DC) design of ground-based gamma-ray telescopes. The production, installation, and the alignment of the segmented aspherical mirrors are the main challenges for the realization of the SCT optical system. In this contribution, we report on the commissioning status, the alignment procedures, and initial alignment results during the initial commissioning phase of the optical system of the prototype SCT.

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  54. Using Muon Rings for the Optical Throughput Calibration of the Cherenkov Telescope Array

    Gaug M., Fegan S., Mitchell A., Maccarone M.C., Mineo T., Okumura A.

    Proceedings of Science   Vol. 358   2021.7

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Proceedings of Science  

    Muon ring images observed with Imaging Atmospheric Cherenkov Telescopes (IACTs) provide a powerful means to calibrate the optical throughput of IACTs and monitor their optical point spread function. We investigate whether muons ring images can be used as the primary optical throughput calibration method for the telescopes of the future Cherenkov Telescope Array (CTA) and find several additional systematic effects in comparison to previous works. To ensure that the method achieves the accuracy required by CTA, these systematic effects need to be taken into account and minor modifications to the hardware and analysis are necessary. We derive analytic estimates for the expected muon data rates to be used for optical throughput calibration, monitoring of the optical point spread function, with achievable statistical and systematic uncertainties, and explore the potential of muon ring images as a secondary method of camera pixel flat-fielding.

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  55. Upgrading the Prototype Schwarzschild-Couder Telescope Camera to a Wide-Field, High-Resolution Instrument

    Adams C., Ambrosi G., Ambrosio M., Aramo C., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolontà C., Bose R., Brill A., Buckley J.H., Caprai M., Covault C.E., Di Venere L., Feng Q., Fiandrini E., Gent A., Giglietto N., Giordano F., Halliday R., Hervet O., Hughes G., Humensky T.B., Ionica M., Jin W., Kaaret P., Kieda D., Kim B., Licciulli F., Loporchio S., Masone V., Meures T., Mode B.A.W., Mukherjee R., Okumura A., Otte N., Pantaleo F.R., Paoletti R., Petrashyk A., Powell J., Powell K., Ribeiro D., Rugliancich A., Santander M., Shang R., Stevenson B., Stiaccini L., Taylor L.P., Tosti L., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V., Wilcox P., Williams D.A.

    Proceedings of Science   Vol. 358   2021.7

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Proceedings of Science  

    The Schwarzschild-Couder Telescope (SCT) is a candidate technology for a medium-sized telescope within the Cherenkov Telescope Array. It is expected to yield substantial improvements in field of view and image resolution compared to traditional telescopes based on Davies-Cotton optics. To match the improved optical resolution, challenging requirements of high channel count and density at low power consumption have to be met by the camera. An initial prototype camera, with 1600 pixels spanning a 2.7◦ field of view, was installed on the prototype SCT in 2018. A project is now underway to upgrade the camera by increasing its pixel count and field of view by factors of 7 and 3, respectively (to 11,328 pixels and 8.0◦). At the same time, the electronics design is being improved in order to lower the gamma-ray energy threshold and thereby provide an instrument especially well-suited for scientific studies related to extended sources and multimessenger astronomy.

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  56. The calibration of the first Large-Sized Telescope of the Cherenkov Telescope Array

    Sakurai S., Depaoli D., López-Coto R., Becerra González J., Berti A., Blanch O., Cassol F., Chiavassa A., Corti D., De Angelis A., Delgado C., Díaz C., Di Pierro F., Di Venere L., Doro M., Fernández-Barral A., Giordano F., Griffiths S., Hadasch D., Inome Y., Jouvin L., Kerszberg D., Kubo H., López-Oramas A., Mallamaci M., Mariotti M., Martínez G., Masuda S., Mazin D., Moralejo A., Moretti E., Nagayoshi T., Ninci D., Nogués L., Nozaki S., Okumura A., Paoletti R., Penil P., Pillera R., Pio C., Rando R., Rotondo F., Rugliancich A., Saito T., Sunada Y., Suzuki M., Takahashi M., Tejedor L.A., Vallania P., Vigorito C., Yamamoto T., Yoshida T.

    Proceedings of Science   Vol. 358   2021.7

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    Language:English   Publishing type:Research paper (scientific journal)   Publisher:Proceedings of Science  

    The Cherenkov Telescope Array (CTA) represents the next generation of very high-energy gamma-ray observatory, which will provide broad coverage of gamma rays from 20 GeV to 300 TeV with unprecedented sensitivity. CTA will employ three different sizes of telescopes, and the Large-Sized Telescopes (LSTs) of 23-m diameter dish will provide the sensitivity in the lowest energies down to 20 GeV. The first LST prototype has been inaugurated in October 2018 at La Palma (Canary Islands, Spain) and has entered the commissioning phase. The camera of the LST consists of 265 PMT modules. Each module is equipped with seven high-quantum-efficiency Photomultiplier Tubes (PMTs), a slow control board, and a readout board. Ensuring high uniformity and precise characterization of the camera is the key aspects leading to the best performance and low systematic uncertainty of the LST cameras. Therefore, prior to the installation on site, we performed a quality check of all PMT modules. Moreover, the absolute calibration of light throughput is essential to reconstruct the amount of light received by the telescope. The amount of light is affected by the atmosphere, by the telescope optical system and camera, and can be calibrated using the ring-shaped images produced by cosmic-ray muons. In this contribution, we will show the results of off-site quality control of PMT modules and on-site calibration using muon rings. We will also highlight the status of the development of Silicon Photomultiplier modules that could be considered as a replacement of PMT modules for further improvement of the camera.

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  57. Detection of the Crab Nebula with the 9.7 m prototype Schwarzschild-Couder telescope

    Adams C. B., Alfaro R., Ambrosi G., Ambrosio M., Aramo C., Arlen T., Batista P. I, Benbow W., Bertucci B., Bissaldi E., Biteau J., Bitossi M., Boiano A., Bonavolonta C., Bose R., Bouvier A., Brill A., Brown A. M., Buckley J. H., Byrum K., Cameron R. A., Canestrari R., Capasso M., Caprai M., Covault C. E., Depaoli D., Errando M., Fegan S., Feng Q., Fiandrini E., Foote G., Fortin P., Funk S., Furniss A., Garfias F., Gent A., Giglietto N., Giordano F., Giro E., Gonzalez M. M., Guarino V, Halliday R., Hervet O., Holder J., Hughes G., Humensky T. B., Ionica M., Iriarte A., Jin W., Johnson C. A., Kaaret P., Kieda D., Kim B., Kuznetsov A., Lapington J. S., Licciulli F., Loporchio S., Masone V, Meagher K., Meures T., Mode B. A. W., Mognet S. A. I, Mukherjee R., Nguyen T., Nieto D., Okumura A., Otte N., La Palombara N., Pantaleo F. R., Paoletti R., Pareschi G., Petrashyk A., Di Pierro F., Pueschel E., Reynolds P. T., Ribeiro D., Richards G., Roache E., Ross D., Rousselle J., Rugliancich A., Ruiz-Diaz-Soto J., Santander M., Schlenstedt S., Schneider M., Scuderi S., Shang R., Sironi G., Stevenson B., Stiaccini L., Tajima H., Taylor L. P., Thornhill J., Tosti L., Tovmassian G., Vagelli V., Valentinoa M., Vandenbroucke J., Vassiliev V. V., Di Venere L., Wakely S. P., Watson J. J., White R., Wilcoxa P., Williams D. A., Wood M., Yu P., Zink A.

    ASTROPARTICLE PHYSICS   Vol. 128   2021.3

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    Publishing type:Research paper (scientific journal)   Publisher:Astroparticle Physics  

    DOI: 10.1016/j.astropartphys.2021.102562

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  58. Sensitivity of the Cherenkov Telescope Array to a dark matter signal from the Galactic centre

    Acharyya A., Adam R., Adams C., Agudo I, Aguirre-Santaella A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Batista R. Alves, Amati L., Ambrosi G., Anguner E. O., Antonelli L. A., Aramo C., Araudo A., Armstrong T., Arqueros F., Asano K., Ascasibar Y., Ashley M., Balazs C., Ballester O., Baquero Larriva A., Martins V. Barbosa, Barkov M., de Almeida U. Barres, Barrio J. A., Bastieri D., Becerra J., Beck G., Tjus J. Becker, Benbow W., Benito M., Berge D., Bernardini E., Bernloehr K., Berti A., Bertucci B., Beshley V, Biasuzzi B., Biland A., Bissaldi E., Biteau J., Blanch O., Blazek J., Bocchino F., Boisson C., Arbeletche L. Bonneau, Bordas P., Bosnjak Z., Bottacini E., Bozhilov V, Bregeon J., Brill A., Bringmann T., Brown A. M., Brun P., Brun F., Bruno P., Bulgarelli A., Burton M., Burtovoi A., Buscemi M., Cameron R., Capasso M., Caproni A., Capuzzo-Dolcetta R., Caraveo P., Carosi R., Carosi A., Casanova S., Cascone E., Cassol F., Catalani F., Cauz D., Cerruti M., Chadwick P., Chaty S., Chen A., Chernyakova M., Chiaro G., Chiavassa A., Chikawa M., Chudoba J., Colak M., Conforti V, Coniglione R., Conte F., Contreras J. L., Coronado-Blazquez J., Costa A., Costantini H., Cotter G., Cristofari P., D'Ai A., D'Ammando A., Damone L. A., Daniel M. K., Dazzi F., De Angelis A., De Caprio V, dos Anjos R. de Cassia, de Gouveia Dal Pino E. M., De Lotto B., De Martino D., Wilhelmi E. de Ona, De Palma F., de Souza V, Delgado C., Delgado Giler A. G., della Volpe D., Depaoli D., Di Girolamo T., Di Pierro F., Di Venere L., Diebold S., Dmytriiev A., Dominguez A., Donini A., Doro M., Ebr J., Eckner C., Edwards T. D. P., Ekoume T. R. N., Elsaesser D., Evoli C., Falceta-Goncalves D., Fedorova E., Fegan S., Feng Q., Ferrand G., Ferrara G., Fiandrini E., Fiasson A., Filipovic M., Fioretti V, Fiori M., Foffano L., Fontaine G., Fornieri O., Franco F. J., Fukami S., Fukui Y., Gaggero D., Galaz G., Gammaldi V, Garcia E., Garczarczyk M., Gascon D., Gent A., Ghalumyan A., Gianotti F., Giarrusso M., Giavitto G., Giglietto N., Giordano F., Giuliani A., Glicenstein J., Gnatyk R., Goldoni P., Gonzalez M. M., Gourgouliatos K., Granot J., Grasso D., Green J., Grillo A., Gueta O., Gunji S., Halim A., Hassan T., Heller M., Hernandez Cadena S., Hiroshima N., Hnatyk B., Hofmann W., Holder J., Horan D., Horandel J., Horvath P., Hovatta T., Hrabovsky M., Hrupec D., Hughes G., Humensky T. B., Huetten M., Iarlori M., Inada T., Inoue S., Iocco F., Iori M., Jamrozy M., Janecek P., Jin W., Jouvin L., Jurysek J., Karukes E., Katarzynski K., Kazanas D., Kerszberg D., Kherlakian M. C., Kissmann R., Knodlseder J., Kobayashi Y., Kohri K., Komin N., Kubo H., Kushida J., Lamanna G., Lapington J., Laporte P., Leigui de Oliveira M. A., Lenain J., Leone F., Leto G., Lindfors E., Lohse T., Lombardi S., Longo F., Lopez A., Lopez M., Lopez-Coto R., Loporchio S., Luque-Escamilla P. L., Mach E., Maggio C., Maier G., Mallamaci M., Nunes de Almeida R. Malta, Mandat D., Manganaro M., Mangano S., Manico G., Marculewicz M., Mariotti M., Markoff S., Marquez P., Marti J., Martinez O., Martinez M., Martinez G., Martinez-Huerta H., Maurin G., Mazin D., Mbarubucyeye J. D., Miranda D. Medina, Meyer M., Miceli M., Miener T., Minev M., Miranda J. M., Mirzoyan R., Mizuno T., Mode B., Moderski R., Mohrmann L., Molina E., Montaruli T., Moralejo A., Morcuende-Parrilla D., Morselli A., Mukherjee R., Mundell C., Nagai A., Nakamori T., Nemmen R., Niemiec J., Nieto D., Nikolajuk M., Ninci D., Noda K., Nosek D., Nozaki S., Ohira Y., Ohishi M., Ohtani Y., Oka T., Okumura A., Ong R. A., Orienti M., Orito R., Orlandini M., Orlando S., Orlando E., Ostrowski M., Oya I, Pagano I, Pagliaro A., Palatiello M., Pantaleo F. R., Paredes J. M., Pareschi G., Parmiggiani N., Patricelli B., Pavletic L., Pe'er A., Pecimotika M., Perez-Romero J., Persic M., Petruk O., Pfrang K., Piano G., Piatteli P., Pietropaolo E., Pillera R., Pilszyk B., Pintore F., Pohl M., Poireau V, Prado R. R., Prandini E., Prast J., Principe G., Prokoph H., Prouza M., Przybilski H., Puhlhofer G., Pumo M. L., Queiroz F., Quirrenbach A., Raino S., Rando R., Razzaque S., Recchia S., Reimer O., Reisenegger A., Renier Y., Rhode W., Ribeiro D., Ribo M., Richtler T., Rico J., Rieger F., Rinchiuso L., Rizi V, Rodriguez J., Fernandez G. Rodriguez, Rodriguez Ramirez J. C., Rojas G., Romano P., Romeo G., Rosado J., Rowell G., Rudak B., Russo F., Sadeh I, Hatlen E. Saether, Safi-Harb S., Greus F. Salesa, Salina G., Sanchez D., Sanchez-Conde M., Sangiorgi P., Sano H., Santander M., Santos E. M., Santos-Lima R., Sanuy A., Sarkar S., Saturni F. G., Sawangwit U., Schussler F., Schwanke U., Sciacca E., Scuderi S., Seglar-Arroyo M., Sergijenko O., Servillat M., Seweryn K., Shalchi A., Sharma P., Shellard R. C., Siejkowski H., Silk J., Siqueira C., Sliusar V, Sokolenko A., Sol H., Spencer S., Stamerra A., Stanic S., Starling R., Stolarczyk T., Straumann U., Striskovic J., Suda Y., Suomijarvi T., Swierk P., Tavecchio F., Taylor L., Tejedor L. A., Teshima M., Testa V, Tibaldo L., Todero Peixoto C. J., Tokanai F., Tonev D., Tosti G., Tosti L., Tothill N., Truzzi S., Travnicek P., Vagelli V., Vallage B., Vallania P., van Eldik C., Vandenbroucke J., Varner G. S., Vassiliev V., Vazquez Acosta M., Vecchi M., Ventura S., Vercellone S., Vergani S., Verna G., Viana A., Vigorito C. F., Vink J., Vitale V., Vorobiov S., Vovk I, Vuillaume T., Wagner S. J., Walter R., Watson J., Weniger C., White R., White M., Wiemann R., Wierzcholska A., Will M., Williams D. A., Wischnewski R., Yanagita S., Yang L., Yoshikoshi T., Zacharias M., Zaharijas G., Zakaria A. A., Zampieri L., Zanin R., Zaric D., Zavrtanik M., Zavrtanik D., Zdziarski A. A., Zech A., Zechlin H., Zhdanov V. I, Zivec M.

    JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS   Vol. 2021 ( 1 )   2021.1

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    Publishing type:Research paper (scientific journal)   Publisher:Journal of Cosmology and Astroparticle Physics  

    DOI: 10.1088/1475-7516/2021/01/057

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  59. Technical and scientific performance of the prototype Schwarzschild-Couder Telescope for CTA

    Adams C.B., Ambrosi G., Ambrosio M., Aramo C., Batista P.I., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolontà C., Bose R., Brill A., Brown A.M., Buckley J.H., Canestrari R., Capasso M., Caprai M., Covault C.E., Depaoli D., Di Venere L., Errando M., Fegan S., Feng Q., Fiandrini E., Furniss A., Gent A., Giglietto N., Giordano F., Giro E., Halliday R., Hervet O., Holder J., Humensky T.B., Incardona S., Ionica M., Jin W., Kieda D., Licciulli F., Loporchio S., Marsella G., Masone V., Meagher K., Meures T., Mode B.A.W., Mognet S.A.I., Mukherjee R., Nieto D., Okumura A., Otte N., Pantaleo F.R., Paoletti R., Pareschi G., Di Pierro F., Pueschel E., Ribeiro D., Riitano L., Roache E., Ross D., Rousselle J., Rugliancich A., Santander M., Shang R., Stiaccini L., Tajima H., Taylor L.P., Tosti L., Tovmassian G., Tripodo G., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V.V., Watson J.J., White R., Williams D.A., Yu P., Zink A.

    Proceedings of SPIE - The International Society for Optical Engineering   Vol. 11820   2021

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    The Cherenkov Telescope Array (CTA) is the next-generation ground-based observatory for very-high-energy gamma rays. One candidate design for CTA’s medium-sized telescopes consists of the Schwarzschild-Couder Telescope (SCT), featuring innovative dual-mirror optics. The SCT project has built and is currently operating a 9.7-m prototype SCT (pSCT) at the Fred Lawrence Whipple Observatory (FLWO); such optical design enables the use of a compact camera with state-of-the art silicon photomultiplier detectors. A partially-equipped camera has recently successfully detected the Crab Nebula with a statistical significance of 8.6 standard deviations. A funded upgrade of the pSCT focal plane sensors and electronics is currently ongoing, which will bring the total number of channels from 1600 to 11328 and the telescope field of view from about 2.7◦ to 8◦. In this work, we will describe the technical and scientific performance of the pSCT.

    DOI: 10.1117/12.2594580

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  60. Status of the development of NUV SiPMs for INFN optical modules for the SCT medium sized telescope proposed for the CTA observatory

    Adams C., Ambrosi G., Ambrosio M., Aramo C., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolonta C., Bose R., Brill A., Buckley J. H., Caprai M., Covault C. E., Di Venere L., Feng Q., Fiandrini E., Gent A., Giglietto N., Giordano F., Halliday R., Hervet O., Hughes G., Humensky T. B., Ionica M., Jin W., Kaaret P., Kieda D., Kim B., Licciulli F., Loporchio S., Masone V., Meures T., Mode B. A. W., Mukherjeek R., Okumura A., Otte N., Pantaleo F. R., Paoletti R., Petrashyk A., Powell J., Powell K., Riberio D., Rouselle J., Rugliancich A., Santander M., Shang R., Stevenson B., Stiaccini L., Taylor L. P., Tosti L., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V., Wilcox P., Williams D. A.

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   Vol. 982   2020.12

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    Publishing type:Research paper (scientific journal)   Publisher:Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment  

    DOI: 10.1016/j.nima.2020.164486

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  61. Study of the Cosmic Rays and Interstellar Medium in Local HI Clouds Using Fermi-LAT Gamma-Ray Observations

    Mizuno T., Abdollahi S., Fukui Y., Hayashi K., Koyama T., Okumura A., Tajima H., Yamamoto H.

    ASTROPHYSICAL JOURNAL   Vol. 890 ( 2 )   2020.2

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    Publishing type:Research paper (scientific journal)   Publisher:Astrophysical Journal  

    DOI: 10.3847/1538-4357/ab6a99

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  62. Front-end electronics of the Compact High Energy Camera

    Leach S. A., Lapington J. S., Ross D., Thornhill J., Duffy C., Funk S., Zink A., Jankowsky D., White R., Zorn J., Tibaldo L., Varner G., Okumura A., Tajima H., Watson J.

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   Vol. 952   2020.2

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    Publishing type:Research paper (scientific journal)   Publisher:Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment  

    DOI: 10.1016/j.nima.2018.12.061

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  63. Alignment of the optical system of the 9.7-m prototype Schwarzchild-Coulder Telescope

    Adams C.

    Proceedings of SPIE - The International Society for Optical Engineering   Vol. 11445   2020

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    DOI: 10.1117/12.2564653

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  64. Design and production of segment mirrors for the Large-Sized Telescopes of the Cherenkov Telescope Array

    Inada T.

    Proceedings of SPIE - The International Society for Optical Engineering   Vol. 11451   2020

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    DOI: 10.1117/12.2562111

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  65. Verification of the Optical System of the 9.7-m Prototype Schwarzschild-Couder Telescope

    Adams C., Alfaro R., Ambrosi G., Ambrosio M., Aramo C., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolonta C., Bose R., Brill A., Buckley J. H., Byrum K., Cameron R. A., Capasso M., Caprai M., Covault C. E., Di Venere L., Fegan S., Feng Q., Fiandrini E., Furniss A., Garczarczyk M., Garfias F., Gent A., Giglietto N., Giordano F., Gonzalez M. M., Halliday R., Hervet O., Hughes G., Humensky T. B., Ionica M., Iriarte A., Jin W., Kaarat P., Kieda D., Kim B., Licciulli F., Limon M., Loporchio S., Masone V, Meures T., Mode B. A. W., Mukherjee R., Nieto D., Okumura A., Otte N., La Palombara N., Pantaleo F. R., Paoletti R., Pareschi G., Petrashyk A., Powell J., Powell K., Ribeiro D., Roache E., Rousselle J., Rugliancich A., Ruiz-Diaz-Soto J., Santander M., Schlenstedt S., Scuderi S., Shang R., Sironi G., Stevenson B., Stiaccini L., Taylor L. P., Tosti L., Tovmassian G., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V. V., Wakely S. P., Wilcox P., Williams D. A., Yu P.

    OPTICAL SYSTEM ALIGNMENT, TOLERANCING, AND VERIFICATION XIII   Vol. 11488   2020

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    DOI: 10.1117/12.2568134

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  66. Calibration and performance of the readout system based on switched capacitor arrays for the Large-Sized Telescope of the Cherenkov Telescope Array

    Seiya Nozaki, Kyosuke Awai, Aya Bamba, Juan Abel Barrio, Maria Isabel Bernardos, Oscar Blanch, Joan Boix, Franca Cassol, Yuuki Choushi, Carlos Delgado, Carlos Diaz, Nadia Fouque, Lluis Freixas, Pawel Gliwny, Shuichi Gunji, Daniela Hadasch, Dirk Hoffmann, Julien Houles, Yusuke Inome, Yuki Iwamura, Lea Jouvin, Hideaki Katagiri, Kiomei Kawamura, Daniel Kerszberg, Yusuke Konno, Hidetoshi Kubo, Junko Kushida, Yukiho Kobayashi, Ruben Lopez, Gustavo Martinez, Shu Masuda, Daniel Mazin, Abelardo Moralejo, Elena Moretti, Tsutomu Nagayoshi, Takeshi Nakamori, Kyoshi Nishijima, Yuto Nogami, Leyre Nogués, Hideyuki Ohoka, Tomohiko Oka, Nao Okazaki, Akira Okumura, Reiko Orito, Jean-Luc Panazol, Riccardo Paoletti, Cristobal Pio, Miguel Polo, Julie Prast, Takayuki Saito, Shunsuke Sakurai, Julian Sitarek, Yuji Sunada, Megumi Suzuki, Mitsunari Takahashi, Kenji Tamura, Manobu Tanaka, Luis Angel Tejedor, Yukikatsu Terada, Masahiro Teshima, Yusuke Tsukamoto, Tokonatsu Yamamoto

    Ground-based and Airborne Instrumentation for Astronomy VIII   Vol. 11447   page: 114470H   2020

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    DOI: 10.1117/12.2560018

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  67. CTA report 161: Cross-calibration of the CTA-LST1 and the MAGIC telescopes

    Ohtani Y., Orito R., Kajiwara Y., Katagiri H., Kushida J., Kubo H., Gunji S., Kobayashi Y., Saito T., Sakaki N., Sakurai S., Abe H., Zenin A., Takahashi Mari, Takahashi Mitsunari, Tateishi D., Chikawa M., Choshi Y., Teshima M., Nakamori T., Nabatame Y., Nishijima K., Inada T., Nogami Y., Nozaki S., Nomura R., Harada Y., Fukami S., Fujihara C., Furuta T., Yamamoto T., Yoshikoshi T., Yoshida T., Imagawa K., for the CTA-Japan, Iwamura Y., Ohishi M., Oka T., Ogata T., Okumura A.

    Meeting Abstracts of the Physical Society of Japan   Vol. 75   page: 441 - 441   2020

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    DOI: 10.11316/jpsgaiyo.75.1.0_441

  68. CTA Report 159: General Report

    Kubo Hidetoshi, Teshima Masahiro, Totani Tomonori, Asano Katsuaki, Abe Hyuga, Awai Kyosuke, Ioka Kunihito, Ishio Kazuma, Ishizaki Wataru, Inada Tomohiro, Inoue Susumu, Inoue Tsuyoshi, Inoue Yoshiyuki, Inome Yusuke, Imagawa Kaname, Iwamura Yuki, Warren Donald, Uchiyama Yasunobu, Ohishi Michiko, Ohoka Hideyuki, Ohtani Yoshiki, Ohira Yutaka, Oka Tomohiko, Okazaki Nao, Ogata Tomoyuki, Okumura Akira, Obara Kotaro, Orito Reiko, Kagaya Mika, Kajiwara Yuki, Kataoka Jun, Katagiri Hideaki, Katsukura Daisuke, Katsuda Satoru, Khalikov Emil, Kawashima Shotaro, Kawanaka Norita, Kawamura Kiomei, Kisaka Shota, Cui Xiaohong, Kushida Junko, Kuroda Yusuke, Gunji Shuichi, Kohri Kazunori, Kobayashi Yukiho, Kong Albert K. H., Saito Takayuki, Sakaki Naoto, Sakurai Shunsuke, Sano Hidetoshi, Sawada Makoto, Shibata Toru, Dzhatdoev Timur, Suzuki Megumi, Suzuki Hiromasa, Suda Yusuke, Strzys Marcel, Sunada Yuji, Zenin Anatolii, Takata Jumpei, Takahashi Mari, Takahashi Keitaro, Takahashi Hiromitsu, Takahashi Mitsunari, Tajima Hiroyasu, Tachihara Kengo, Tateishi Dai, Tanaka Shuta, Tanaka Takaaki, Tanaka Manobu, Tam Thomas P. H., Tamura Kenji, Cheng K. S., Chikawa Michiyuki, Choushi Yuuki, Tsukamoto Yusuke, Tsujimoto Shimpei, Tsuru Takeshi, Tian Wenwu, Terada Yukikatsu, Toma Kenji, Tokanai Fuyuki, Naito Tsuguya, Nagataki Shigehiro, Nakamura Yuki, Nakamori Takeshi, Nakayama Kazunori, Nabatame Yasuyuki, Nishijima Kyoshi, Nogami Yuto, Nozaki Seiya, Noda Koji, Nomura Ryosuke, Barkov Maxim, Hadasch Daniela, Hayakawa Takahiro, Hayashi Kohei, Hayashi Katsuhiro, Hayashida Masaaki, Hara Satoshi, Harada Yoshiki, Bamba Aya, Hiroshima Nagisa, Hirotani Kouichi, Hui David C. Y., Ferrand Gilles, Fukazawa Yasushi, Fukami Satoshi, Fukui Yasuo, Fujikawa Yui, Fujita Yutaka, Fujihara Chikako, Furuta Tomoya, He Haoning, Vovk Ievgen, Majumdar Pratik, Mazin Daniel, Matsumoto Hironori, Mizuno Tsunefumi, Muraishi Hiroshi, Murase Kohta, Mori Koji, Yanagita Shohei, Yamazaki Ryo, Yamane Yumiko, Yamamoto Tokonatsu, Yamamoto Hiroaki, Yoshikoshi Takanori, Yoshida Atsumasa, Yoshida Tatsuo, Lee Shiu-Hang (Herman)

    Meeting Abstracts of the Physical Society of Japan   Vol. 75.1   page: 439 - 439   2020

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    DOI: 10.11316/jpsgaiyo.75.1.0_439

  69. CTA Report 162: CTA-LST1 camera calibration

    Kobayashi Y., Oka T., Okazaki N., Ogata T., Okumura A., Orito R., Kajiwara Y., Katagiri H., Kushida J., Kubo H., Gunji S., Abe H., Saito T., Sakaki N., Sakurai S., Suzuki M., Sunada Y., Zenin A., Takahashi Mari, Takahashi Mitsunari, Tateishi D., Tanaka M., Inada T., Tamura K., Chikawa M., Choshi Y., Teshima M., Terada Y., Tokanai F., Nakamori T., Nabatame Y., Nishijima K., Nogami Y., Inome Y., Nozaki S., Noda K., Nomura R., Hadasch D., Harada Y., Fukami S., Fujihara C., Furuta T., Mazin D., Yamamoto T., Imagawa K., Yoshikoshi T., Yoshida T., for the CTA-Japan Consortium, Iwamura Y., Ohishi M., Ohoka H., Ohtani Y.

    Meeting Abstracts of the Physical Society of Japan   Vol. 75   page: 471 - 471   2020

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    DOI: 10.11316/jpsgaiyo.75.1.0_471

  70. CTA Report 160: Status of the mono analysis for the LST proposed for CTA

    Nozaki S., Okumura A., Orito R., Kajiwara Y., Katagiri H., Kushida J., Kubo H., Gunji S., Kobayashi S., Saito T., Sakaki N., Abe H., Sakurai S., Zenin A., Takahashi Mari, Takahashi Mitsunari, Tateishi D., Chikawa M., Choshi Y., Teshima M., Nakamori T., Nabatame Y., Inada T., Nishijima K., Nogami Y., Nomura R., Harada Y., Fukami S., Fujihara C., Furuta T., Yamamoto T., Yoshikoshi T., Yoshida T., Imagawa K., the CTA-Japan Consortium, Iwamura Y., Ohishi M., Ohtani Y., Oka T., Ogata T.

    Meeting Abstracts of the Physical Society of Japan   Vol. 75   page: 440 - 440   2020

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:The Physical Society of Japan  

    DOI: 10.11316/jpsgaiyo.75.1.0_440

  71. Fermi-LAT γ-Ray Study of the Interstellar Medium and Cosmic Rays in the Chamaeleon Molecular Cloud Complex: A Look at the Dark Gas as Optically Thick H i Reviewed

    H. Sano, Katsuhiro Hayashi, Tsunefumi Mizuno, Yasuo Fukui, Ryuji Okamoto, Hiroaki Yamamoto, Naoya Hidaka, Akira Okumura, Hiroyasu Tajima, Hidetoshi Sano

    The Astrophysical Journal   Vol. 884 ( 2 )   2019.10

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    We report a Fermi-LAT $\gamma$-ray analysis for the Chamaeleon<br />
    molecular-cloud complex using a total column density (NH) model based on the<br />
    dust optical depth at 353 GHz ($\tau_{353}$) with the Planck thermal dust<br />
    emission model. Gamma rays with energy from 250 MeV to 100 GeV are fitted with<br />
    the NH model as a function of $\tau_{353}$, NH $\propto$<br />
    $\tau_{353}^{1/\alpha}$ ($\alpha$ $\geq$ 1.0), to explicitly take into account<br />
    a possible nonlinear $\tau_{353}$/NH ratio. We found that a nonlinear relation,<br />
    $\alpha$$\sim$1.4, gives the best fit to the $\gamma$-ray data. This nonlinear<br />
    relation may indicate dust evolution effects across the different gas phases.<br />
    Using the best-fit NH model, we derived the CO-to-H2 conversion factor (XCO)<br />
    and gas mass, taking into account uncertainties of the NH model. The value of<br />
    XCO is found to be (0.63-0.76) $\times$10$^{20}$ cm$^{-2}$ K$^{-1}$ km$^{-1}$<br />
    s, which is consistent with that of a recent $\gamma$-ray study of the<br />
    Chamaeleon region. The total gas mass is estimated to be (6.0-7.3) $\times$<br />
    10$^{4}$ Msun, of which the mass of additional gas not traced by standard HI or<br />
    CO line surveys is 20-40%. The additional gas amounts to 30-60% of the gas mass<br />
    estimated in the case of optically thin HI and has 5-7 times greater mass than<br />
    the molecular gas traced by CO. Possible origins of the additional gas are<br />
    discussed based on scenarios of optically thick HI and CO-dark H2. We also<br />
    derived the $\gamma$-ray emissivity spectrum, which is consistent with the<br />
    local HI emissivity derived from LAT data within the systematic uncertainty of<br />
    $\sim$20%

    DOI: 10.3847/1538-4357/ab4351

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    arXiv

  72. Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout

    Acharyya A

    Astroparticle Physics   Vol. 111   page: 35 - 53   2019.9

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    DOI: 10.1016/j.astropartphys.2019.04.001

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  73. Using Muon Rings for the Calibration of the Cherenkov Telescope Array: A Systematic Review of the Method and Its Potential Accuracy

    Gaug M., Fegan S., Mitchell A. M. W., Maccarone M. C., Mineo T., Okumura A.

    ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES   Vol. 243 ( 1 )   2019.7

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    Publishing type:Research paper (scientific journal)   Publisher:Astrophysical Journal, Supplement Series  

    DOI: 10.3847/1538-4365/ab2123

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  74. Prototype schwarzschild-couder telescope for the cherenkov telescope array: Commissioning status of the optical system

    Adams C.

    Proceedings of Science   Vol. 358   2019

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    Publishing type:Research paper (scientific journal)   Publisher:Proceedings of Science  

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  75. Introduction to CTA Science

    Acharya B. S., Agudo I., Al Samarai I., Alfaro R., Alfaro J., Alispach C., Batista R. Alves, Amans J. -P., Amato E., Ambrosi G., Antolini E., Antonelli L. A., Aramo C., Araya M., Armstrong T., Arqueros F., Arrabito L., Asano K., Ashley M., Backes M., Balazs C., Balbo M., Ballester O., Ballet J., Bamba A., Barkov M., Barres de Almeida U., Barrio J. A., Bastieri D., Becherini Y., Belfiore A., Benbow W., Berge D., Bernardini E., Bernardini M. G., Bernardos M., Bernloehr K., Bertucci B., Biasuzzi B., Bigongiari C., Biland A., Bissaldi E., Biteau J., Blanch O., Blazek J., Boisson C., Bolmont J., Bonanno G., Bonardi A., Bonavolonta C., Bonnoli G., Bosnjak Z., Bottcher M., Braiding C., Bregeon J., Brill A., Brown A. M., Brun P., Brunetti G., Buanes T., Buckley J., Bugaev V., Buehler R., Bulgarelli A., Bulik T., Burton M., Burtovoi A., Busetto G., Canestrari R., Capalbi M., Capitanio F., Caproni A., Caraveo P., Cardenas V., Carlile C., Carosi R., Carquin E., Carr J., Casanova S., Cascone E., Catalani F., Catalano O., Cauz D., Cerruti M., Chadwick P., Chaty S., Chaves R. C. G., Chen A., Chen X., Chernyakova M., Chikawa M., Christov A., Chudoba J., Cieslar M., Coco V., Colafrancesco S., Colin P., Conforti V., Connaughton V., Conrad J., Contreras J. L., Cortina J., Costa A., Costantini H., Cotter G., Covino S., Crocker R., Cuadra J., Cuevas O., Cumani P., D'Ai A., D'Ammando F., D'Avanzo P., D'Urso D., Daniel M., Davids I., Dawson B., Dazzi F., De Angelis A., de Cassia dos Anjos R., De Cesare G., De Franco A., De Gouveia Dal Pino E. M., de la Calle I., Lopez R. de los Reyes, De Lotto B., De Luca A., De Lucia M., de Naurois M., de Ona Wilhelmi E., De Palma F., De Persio F., de Souza V., Deil C., Del Santo M., Delgado C., della Volpe D., Di Girolamo T., Di Pierro F., Di Venere L., Diaz C., Dib C., Diebold S., Djannati-Atai A., Dominguez A., Prester D. Dominis, Dorner D., Doro M., Drass H., Dravins D., Dubus G., Dwarkadas V. V., Ebr J., Eckner C., Egberts K., Einecke S., Ekoume T. R. N., Elsaesser D., Ernenwein J. -P., Espinoza C., Evoli C., Fairbairn M., Falceta-Goncalves D., Falcone A., Farnier C., Fasola G., Fedorova E., Fegan S., Fernandez-Alonso M., Fernandez-Barral A., Ferrand G., Fesquet M., Filipovic M., Fioretti V., Fontaine G., Fornasa M., Fortson L., Freixas Coromina L., Fruck C., Fujita Y., Fukazawa Y., Funk S., Fuessling M., Gabici S., Gadola A., Gallant Y., Garcia B., Garcia Lopez R., Garczarczyk M., Gaskins J., Gasparetto T., Gaug M., Gerard L., Giavitto G., Giglietto N., Giommi P., Giordano F., Giro E., Giroletti M., Giuliani A., Glicenstein J. -F., Gnatyk R., Godinovic N., Goldoni P., Gomez-Vargas G., Gonzalez M. M., Gonzalez J. M., Gotz D., Graham J., Grandi P., Granot J., Green A. J., Greenshaw T., Griffiths S., Gunji S., Hadasch D., Hara S., Hardcastle M. J., Hassan T., Hayashi K., Hayashida M., Heller M., Helo J. C., Hermann G., Hinton J., Hnatyk B., Hofmann W., Holder J., Horan D., Horandel J., Horns D., Horvath P., Hovatta T., Hrabovsky M., Hrupec D., Humensky T. B., Huetten M., Iarlori M., Inada T., Inome Y., Inoue S., Inoue T., Inoue Y., Iocco F., Ioka K., Iori M., Ishio K., Iwamura Y., Jamrozy M., Janecek P., Jankowsky D., Jean P., Jung-Richardt I., Jurysek J., Kaaret P., Karkar S., Katagiri H., Katz U., Kawanaka N., Kazanas D., Khelifi B., Kieda D. B., Kimeswenger S., Kimura S., Kisaka S., Knapp J., Knodlseder J., Koch B., Kohri K., Komin N., Kosack K., Kraus M., Krause M., Krauss F., Kubo H., Mezek G. Kukec, Kuroda H., Kushida J., La Palombara N., Lamanna G., Lang R. G., Lapington J., Le Blanc O., Leach S., Lees J. -P., Lefaucheur J., Leigui de Oliveira M. A., Lenain J. -P., Lico R., Limon M., Lindfors E., Lohse T., Lombardi S., Longo F., Lopez M., Lopez-Coto R., Lu C. -C., Lucarelli F., Luque-Escamilla P. L., Lyard E., Maccarone M. C., Maier G., Majumdar P., Malaguti G., Mandat D., Maneva G., Manganaro M., Mangano S., Marcowith A., Marin J., Markoff S., Marti J., Martin P., Martinez M., Martinez G., Masetti N., Masuda S., Maurin G., Maxted N., Mazin D., Medina C., Melandri A., Mereghetti S., Meyer M., Minaya I. A., Mirabal N., Mirzoyan R., Mitchell A., Mizuno T., Moderski R., Mohammed M., Mohrmann L., Montaruli T., Moralejo A., Morcuende-Parrilla D., Mori K., Morlino G., Morris P., Morselli A., Moulin E., Mukherjee R., Mundell C., Murach T., Muraishi H., Murase K., Nagai A., Nagataki S., Nagayoshi T., Naito T., Nakamori T., Nakamura Y., Niemiec J., Nieto D., Nikolajuk M., Nishijima K., Noda K., Nosek D., Novosyadlyj B., Nozaki S., O'Brien P., Oakes L., Ohira Y., Ohishi M., Ohm S., Okazaki N., Okumura A., Ong R. A., Orienti M., Orito R., Osborne J. P., Ostrowski M., Otte N., Oya I., Padovani M., Paizis A., Palatiello M., Palatka M., Paoletti R., Paredes J. M., Pareschi G., Parsons R. D., Pe'er A., Pech M., Pedaletti G., Perri M., Persic M., Petrashyk A., Petrucci P., Petruk O., Peyaud B., Pfeifer M., Piano G., Pisarski A., Pita S., Pohl M., Polo M., Pozo D., Prandini E., Prast J., Principe G., Prokhorov D., Prokoph H., Prouza M., Puehlhofer G., Punch M., Puerckhauer S., Queiroz F., Quirrenbach A., Raino S., Razzaque S., Reimer O., Reimer A., Reisenegger A., Renaud M., Rezaeian A. H., Rhode W., Ribeiro D., Ribo M., Richtler T., Rico J., Rieger F., Riquelme M., Rivoire S., Rizi V., Rodriguez J., Fernandez G. Rodriguez, Rodriguez Vazquez J. J., Rojas G., Romano P., Romeo G., Rosado J., Rovero A. C., Rowell G., Rudak B., Rugliancich A., Rulten C., Sadeh I., Safi-Harb S., Saito T., Sakaki N., Sakurai S., Salina G., Sanchez-Conde M., Sandaker H., Sandoval A., Sangiorgi P., Sanguillon M., Sano H., Santander M., Sarkar S., Satalecka K., Saturni F. G., Schioppa E. J., Schlenstedt S., Schneider M., Schoorlemmer H., Schovanek P., Schulz A., Schussler F., Schwanke U., Sciacca E., Scuderi S., Seitenzahl I., Semikoz D., Sergijenko O., Servillat M., Shalchi A., Shellard R. C., Sidoli L., Siejkowski H., Sillanpaa A., Sironi G., Sitarek J., Sliusar V., Slowikowska A., Sol H., Stamerra A., Stanic S., Starling R., Stawarz L., Stefanik S., Stephan M., Stolarczyk T., Stratta G., Straumann U., Suomijarvi T., Supanitsky A. D., Tagliaferri G., Tajima H., Tavani M., Tavecchio F., Tavernet J. -P., Tayabaly K., Tejedor L. A., Temnikov P., Terada Y., Terrier R., Terzic T., Teshima M., Testa V., Thoudam S., Tian W., Tibaldo L., Tluczykont M., Todero Peixoto C. J., Tokanai F., Tomastik J., Tonev D., Tornikoski M., Torres D. F., Torresi E., Tosti G., Tothill N., Tovmassian G., Travnicek P., Trichard C., Trifoglio M., Pujadas I. Troyano, Tsujimoto S., Umana G., Vagelli V., Vagnetti F., Valentino M., Vallania P., Valore L., van Eldik C., Vandenbroucke J., Varner G. S., Vasileiadis G., Vassiliev V., Vazquez Acosta M., Vecchi M., Vega A., Vercellone S., Veres P., Vergani S., Verzi V., Vettolani G. P., Viana A., Vigorito C., Villanueva J., Voelk H., Vollhardt A., Vorobiov S., Vrastil M., Vuillaume T., Wagner S. J., Wagner R., Walter R., Ward J. E., Warren D., Watson J. J., Werner F., White M., White R., Wierzcholska A., Wilcox P., Will M., Williams D. A., Wischnewski R., Wood M., Yamamoto T., Yamazaki R., Yanagita S., Yang L., Yoshida T., Yoshiike S., Yoshikoshi T., Zacharias M., Zaharijas G., Zampieri L., Zandanel F., Zanin R., Zavrtanik M., Zavrtanik D., Zdziarski A. A., Zech A., Zechlin H., Zhdanov V. I., Ziegler A., Zorn J.

    SCIENCE WITH THE CHERENKOV TELESCOPE ARRAY     page: 1 - +   2019

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  76. Development and operations of INFN optical modules for the SCT telescope camera proposed for the Cherenkov Telescope Array Observatory

    Adams C.

    Proceedings of Science   Vol. 358   2019

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  77. Characterization and assembly of near-ultraviolet SiPMs for the Schwarzschild-Couder medium-size telescope proposed for the CTA Observatory

    Adams C., Ambrosi G., Ambrosio M., Aramo C., Benbow W., Bertucci B., Bissaldi E., Bitossi M., Boiano A., Bonavolonta C., Bose R., Brill A., Buckley J. H., Caprai M., Covault C. E., Di Venere L., Feng Q., Fiandrini E., Gent A., Giglietto N., Giordano F., Halliday R., Hervet O., Hughes G., Humensky T. B., Ionica M., Jin W., Kaaret P., Kieda D., Kim B., Licciulli F., Loporchio S., Masone V., Meures T., Mode B. A. W., Mukherjee R., Okumura A., Otte N., Pantaleo F. R., Paoletti R., Petrashyk A., Powell J., Powell K., Ribeiro D., Rousselle J., Rugliancich A., Santander M., Shang R., Stevenson B., Stiaccini L., Taylor L. P., Tosti L., Vagelli V., Valentino M., Vandenbroucke J., Vassiliev V., Wilcox P., Williams D. A.

    HARD X-RAY, GAMMA-RAY, AND NEUTRON DETECTOR PHYSICS XXI   Vol. 11114   2019

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    DOI: 10.1117/12.2530617

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  78. Camera design and performance of the prototype schwarzschild-couder telescope for the Cherenkov Telescope Array

    Adams C.

    Proceedings of Science   Vol. 358   2019

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  79. The calibration of the first large-sized telescope of the Cherenkov telescope array

    Sakurai S.

    Proceedings of Science   Vol. 358   2019

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  80. Using muon rings for the optical throughput calibration of the Cherenkov Telescope array

    Gaug M.

    Proceedings of Science   Vol. 358   2019

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  81. Upgrading the prototype Schwarzschild-Couder telescope camera to a wide-field, high-resolution instrument

    Adams C.

    Proceedings of Science   Vol. 358   2019

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  82. CTA Report 156: Evaluation of effect of uncertainty in hadronic interaction models on the estimation of CTA sensitivity

    Ohishi Michiko, Arbeletche Luan, Souza Vitor de, Maier Gernot, Bernloehr Konrad, Moralejo Abelardo, Bregeon Johan, Arrabito Luisa, Yoshikoshi Takanori, Iwamura Yuki, Ohtani Yoshiki, Ogata Tomoyuki, Okumura Akira, Orito Reiko, Katagiri Hideaki, Kushida Junko, Gunji Shuichi, Kobayashi Yukiho, Saito Takayuki, Sakaki Naoto, Sakurai Shunsuke, Zenin Anatolii, Chikawa Michiyuki, Nakamori Takeshi, Nishijima Kyoshi, Miura Chika, Nozaki Seiya, Fukami Satoshi, Fujihara Chikako, Furuta Tomoya, Yoshida Tatsuo, the CTA-Japan Consortium

    Meeting Abstracts of the Physical Society of Japan   Vol. 74.2 ( 0 ) page: 359 - 359   2019

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    DOI: 10.11316/jpsgaiyo.74.2.0_359

    CiNii Research

  83. CTA Report 150: Commissioning test of the focal plane camera of the first CTA Large-Sized Telescope.

    Nozaki S., Kajiwara Y., Katagiri H., Kushida J., Kimura S., Kubo H., Gunji S., Koyama S., Saito T., Sakurai S., Sawada M., Inada T., Suzuki M., Sunada Y., Takahashi M., Takahara H., Tanaka M., Tamura K., Choushi Y., Tujimoto S., Teshima M., Terada Y., Inome Y., Tokanai F., Nakamori T., Nagayoshi T., Nishijima K., Nishiyama G., Noda K., Hayashida M., Bamba A., Hirako J., Fukami S., Iwamura Y., Furuta T., Masuda S., Yamamoto T., Yoshida T., Hadasch Daniela, Mazin Daniel, the CTA-Japan consortium, Ikeno M., Uchida T., Ohoka H., Okazaki N., Oka T., Okumura A., Orito R.

    Meeting Abstracts of the Physical Society of Japan   Vol. 74   page: 559 - 559   2019

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    DOI: 10.11316/jpsgaiyo.74.1.0_559

  84. CTA Report 149: Development of analysis software for CTA LST-1

    Iwamura Yuki, Kubo Hidetoshi, Gunji Shuichi, Kobayashi Yukiho, Saito Takayuki, Sakaki Naoto, Sakurai Shunsuke, Sasai Yoshinori, Sunada Yuji, Takahashi Tomoya, Taneda Yuki, Inada Tomohiro, Chikawa Michiyuki, Choushi Yuuki, Teshima Masahiro, Terada Yukikatsu, Nakamori Takeshi, Nishijima Kyoshi, Nozaki Seiya, Noda Koji, Hayashida Masaaki, Hiroshima Nagisa, Ohishi Michiko, Fukami Satoshi, Fujihara Chikako, Miura Chika, Yamamoto Tokonatsu, Yoshikoshi Takanori, Yoshida Tatsuo, Ri Ken, Zenin Anatolii, the CTA-Japan Consortium, Ohtani Yoshiki, Okumura Akira, Orito Reiko, Katagiri Hideaki, Kamimoto Takumi, Kushida Junko

    Meeting Abstracts of the Physical Society of Japan   Vol. 74   page: 558 - 558   2019

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    DOI: 10.11316/jpsgaiyo.74.1.0_558

  85. CTA Report 148: A Monte Carlo simulation study using muon events of Large Size Telescope

    Ri Ken, Gunji Shuichi, Saito Takayuki, Sakaki Naoto, Sasai Yoshinori, Takahashi Tomoya, Taneda Yuki, Nakamori Takeshi, Nishijima Kyoshi, Miura Chika, Yoshikoshi Takanori, Fujihara Chikako, Yoshida Tatsuo, Zenin Anatolii, the CTA-Japan Consortium, Chikawa Michiyuki, Ohishi Michiko, Okumura Akira, Orito Reiko, Katagiri Hideaki, Kamimoto Takumi, Kushida Junko

    Meeting Abstracts of the Physical Society of Japan   Vol. 74   page: 557 - 557   2019

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    DOI: 10.11316/jpsgaiyo.74.1.0_557

  86. CTA Report 157: Measurement of timing response performance of photomultiplier tube used for CTA large sized telescope

    Sunada Yuji, Katagiri Hideaki, Kushida Junko, Kubo Hidetoshi, Gunji Shuichi, Kobayashi Yukiho, Saito Takayuki, Sakurai Shunsuke, Suzuki Megumi, Takahashi Mitsunari, Tanaka Manobu, Inome Yusuke, Tamura Kenji, Choushi Yuuki, Teshima Masahiro, Terada Yukikatsu, Tokanai Fuyuki, Nakamori Takeshi, Nagayoshi Tsutomu, Nishijima Kyoshi, Nogami Yuto, Nozaki Seiya, Iwamura Yuki, Noda Koji, Hadasch Daniela, Hayashida Masaaki, Bamba Aya, Hirako Joe, Furuta Tomoya, Mazin Daniel, Masuda Shu, Yamamoto Tokonatsu, Yoshida Tatsuo, Ohoka Hideyuki, Ikeno Masahiro, Uchida Tomohisa, Oka Tomohiko, Okazaki Nao, Okumura Akira, Orito Reiko, Kajiwara Yuki

    Meeting Abstracts of the Physical Society of Japan   Vol. 74   page: 360 - 360   2019

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    DOI: 10.11316/jpsgaiyo.74.2.0_360

  87. Evaluation of silicon photomultipliers for dual-mirror Small-Sized Telescopes of Cherenkov Telescope Array

    Asano A, Berge D, Bonanno G, Bryan M, Gebhardt B, Grillo A, Hidaka N, Kachru P, Lapington J, Leach S, Nakamura Y, Okumura A, Romeo G, Ross D, Stephan M, Tajima H, Timpanaro M. C, White R, Yamane N, Zink A

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   Vol. 912   page: 177 - 181   2018.12

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    DOI: 10.1016/j.nima.2017.11.017

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  88. Characterisation and testing of CHEC-M-A camera prototype for the small-sized telescopes of the Cherenkov telescope array

    Zorn J., White R., Watson J. J., Armstrong T. P., Balzer A., Barcelo M., Berge D., Bose R., Brown A. M., Bryan M., Chadwick P. M., Clark P., Costantini H., Cotter G., Dangeon L., Daniel M., De Franco A., Deiml P., Fasola G., Funk S., Gebyehu M., Gironnet J., Graham J. A., Greenshaw T., Hinton J. A., Kraus M., Lapington J. S., Laporte P., Leach S. A., Le Blanc O., Malouf A., Molyneux P., Moore P., Prokoph H., Okumura A., Ross D., Rowell G., Sapozhnikov L., Schoorlemmer H., Sol H., Stephan M., Tajima H., Tibaldo L., Varner G., Zink A.

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   Vol. 904   page: 44-63   2018.10

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    DOI: 10.1016/j.nima.2018.06.078

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  89. Final characterisation and design of the Gamma-ray Cherenkov Telescope (GCT) for the Cherenkov Telescope Array

    Le Blanc O, Fasola G, Huet J. M, White R, Dmytriiev A, Sol H, Zech A, Abchiche A, Amans J. P, Armstrong T. P, Barcelo M, Berge D, Brown A. M, Buchholtz G, Chadwick P. M, Clark P, Cotter G, Dangeon L, De Frondat F, Deiml P, Dournaux J. L, Duffy C, Einecke S, Flis S, Funk S, Giavitto G, Gironnet J, Graham J. A, Greenshaw T, Hinton J. A, Jegouzo I, Kraus M, Lapington J. S, Laporte P, Leach S. A, Lloyd S, Minaya I. A, Morier R, Okumura A, Prokoph H, Ross D., R

    GROUND-BASED AND AIRBORNE TELESCOPES VII   Vol. 10700   2018

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    DOI: 10.1117/12.2313158

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  90. CTA Project 130: General Report

    Teshima Masahiro, Kubo Hidetoshi, Totani Tomonori, Consortium for, the CTA-Japan

    Meeting Abstracts of the Physical Society of Japan   Vol. 73 ( 0 ) page: 412-412 - 412   2018

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    DOI: 10.11316/jpsgaiyo.73.1.0_412

  91. CTA Report 139: General Report

    Kubo Hidetoshi, Inoue Tsuyoshi, Fukami Satoshi, Fukui Yasuo, Fujita Yutaka, Fujihara Chikako, He Haoning, Majumdar Pratik, Mazin Daniel, Masuda Shu, Matsumoto Hironori, Miura Chika, Inoue Yoshiyuki, Mizuno Tsunefumi, Muraishi Hiroshi, Murase Kohta, Mori Koji, Yanagita Shohei, Yamazaki Ryo, Yamamoto Tokonatsu, Yamamoto Hiroaki, Yoshiike Satoshi, Yoshikoshi Takanori, Inome Yusuke, Yoshida Atsumasa, Yoshida Tatsuo, Ri Ken, Lee Shiu-Hang (Herman), Iwamura Yuki, Warren Donald, Uchiyama Yasunobu, Ohishi Michiko, Ohoka Hideyuki, Ohira Yutaka, Okazaki Nao, Teshima Masahiro, Okumura Akira, Orito Reiko, Kagaya Mika, Kakuwa Jun, Kataoka Jun, Katagiri Hideaki, Katsukura Daisuke, Katsuda Satoru, Kato Sho, Kamimoto Takumi, Totani Tomonori, Kawanaka Norita, Kisaka Shota, Kimura Souichiro, Cui Xiaohong, Kushida Junko, Kumon Taku, Kuroda Hayato, Gunji Shuichi, Kohri Kazunori, Koyama Shu, Asano Akira, Kong Albert K. H., Saito Takayuki, Sakaki Naoto, Sakurai Shunsuke, Sasai Yoshinori, Sano Hidetoshi, Sawada Makoto, Shibata Toru, Dzhatdoev Timur, Suzuki Megumi, Asano Katsuaki, Sunada Yuji, Sekizaki Haruhito, Zenin Anatolii, Takata Jumpei, Takahashi Keitaro, Takahashi Tomoya, Takahashi Hiromitsu, Takahashi Mitsunari, Takahara Hiro, Tajima Hiroyasu, Ioka Kunihito, Tachihara Kengo, Tanaka Shuta, Tanaka Takaaki, Tanaka Manobu, Tanaka Yasuyuki, Taneda Yuuki, Tam Thomas P. H., Cheng K. S., Chikawa Michiyuki, Tsujimoto Shimpei, Ishio Kazuma, Tsuru Takeshi, Tian Wenwu, Terada Yukikatsu, Toma Kenji, Tokanai Fuyuki, Naito Tsuguya, Nakajima Daisuke, Nagataki Shigehiro, Nakamura Yuki, Nakamori Takeshi, Inada Tomohiro, Nakayama Kazunori, Nagayoshi Tsutomu, Nishijima Kyoshi, Nishiyama Gaku, Nozaki Seiya, Noda Koji, Barkov Maxim, Hadasch Daniela, Hayakawa Takahiro, Hayashi Katsuhiro, Inoue Susumu, Hayashida Masaaki, Hara Satoshi, Bamba Aya, Hidaka Naoya, Hirako Joe, Hiroshima Nagisa, Hirotani Kouichi, Hui David C. Y., Ferrand Gilles, Fukazawa Yasushi

    Meeting Abstracts of the Physical Society of Japan   Vol. 73 ( 0 ) page: 188 - 188   2018

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    DOI: 10.11316/jpsgaiyo.73.2.0_188

  92. CTA report 140: A Monte Carlo simulation study on gamma-ray like proton events in CTA and dependence on hadronic interaction models

    Ohishi Michiko, Sasai Yoshinori, Takahashi Tomoya, Taneda Yuki, Chikawa Michiyuki, Nakamori Takeshi, Nishijima Kyoshi, Fujiwara Chikako, Miura Chika, Yoshikoshi Takanori, Yoshida Tatsuo, Okumura Akira, Ri Ken, Zenin Anatolii, the CTA-Japan Consortium, Orito Reiko, Katagiri Hideaki, Kamimoto Takumi, Kushida Junko, Gunji Shuichi, Saito Takayuki, Sakaki Naoto

    Meeting Abstracts of the Physical Society of Japan   Vol. 73   page: 189 - 189   2018

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    DOI: 10.11316/jpsgaiyo.73.2.0_189

  93. CTA report 132: A simulation study on CTA performance for the measurement of electron/positron spectrum in TeV region(III)

    Ohishi Michiko, Sasai Yoshinori, Takahashi Tomoya, Taneda Yuki, Chikawa Michiyuki, Nakamori Takeshi, Nishijina Kyoshi, Miura Chika, Yoshikoshi Takanori, Yoshida Tatsuo, Ri Ken, Okumura Akira, the CTA-Japan Consortium, Orito Reiko, Katagiri Hideaki, Kamimoto Takumi, Kushida Junko, Gunji Shuichi, Saito Takayuki, Sakaki Naoto

    Meeting Abstracts of the Physical Society of Japan   Vol. 73   page: 487 - 487   2018

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    DOI: 10.11316/jpsgaiyo.73.1.0_487

  94. CTA Report 131: Monte Carlo performance studies of the Cherenkov Telescope Array under moonlight

    Miura Chika, Sakaki Naoto, Sasai Yoshinori, Takahashi Tomoya, Taneda Yuki, Chikawa Michiyuki, Nakamori Takeshi, Nishijima Kyoshi, Yoshikoshi Takanori, Yoshida Tatsuo, Ri Ken, Ohishi Michiko, the CTA-Japan Consortium, Okumura Akira, Orito Reiko, Katagiri Hideaki, Kamimoto Takumi, Kushida Junko, Gunji Shuichi, Saito Takayuki

    Meeting Abstracts of the Physical Society of Japan   Vol. 73   page: 413 - 413   2018

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    DOI: 10.11316/jpsgaiyo.73.1.0_413

  95. CTA report 143: Evaluation of the sensitivity of the Small-Sized Telescopes under moonlight

    Sasai Yoshinori, Sakaki Naoto, Takahashi Tomoya, Tajima Hiroyasu, Taneda Yuki, Chikawa Michiyuki, Nakamura Yuki, Nakamori Takeshi, Nishijina Kyoshi, Fujihara Chikako, Miura Chika, Ohishi Michiko, Yoshikoshi Takanori, Yoshida Tatsuo, Ri Ken, Zenin Anatolii, the CTA-Japan Consortium, Okumura Akira, Orito Reiko, Katagiri Hideaki, Kamimoto Takumi, Kushida Junko, Gunji Shuichi, Saito Takayuki

    Meeting Abstracts of the Physical Society of Japan   Vol. 73   page: 192 - 192   2018

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    DOI: 10.11316/jpsgaiyo.73.2.0_192

  96. CTA Report 141: Monte Carlo performance studies of the Cherenkov Telescope Array under moonlight (II)

    Miura Chika, Sakaki Naoto, Sasai Yoshinori, Takahashi Tomoya, Taneda Yuki, Chikawa Michiyuki, Nakamori Takeshi, Nishijima Kyoshi, Fujihara Chikako, Yoshikoshi Takanori, Yoshida Tatsuo, Ohishi Michiko, Ri Ken, Zenin Anatolii, the CTA-Japan Consortium, Okumura Akira, Orito Reiko, Katagiri Hideaki, Kamimoto Takumi, Kushida Junko, Gunji Shuichi, Saito Takayuki

    Meeting Abstracts of the Physical Society of Japan   Vol. 73   page: 190 - 190   2018

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    DOI: 10.11316/jpsgaiyo.73.2.0_190

  97. CTA report 135: Optimization of the trigger performance for the Small-Sized Telescope

    Sasai Yoshinori, Sakaki Naoto, Takahashi Tomoya, Taneda Yuki, Chikawa Michiyuki, Nakamori Takeshi, Nishijina Kyoshi, Miura Chika, Yoshikoshi Takanori, Yoshida Tatsuo, Ri Ken, Ohishi Michiko, the CTA-Japan Consortium, Okumura Akira, Orito Reiko, Katagiri Hideaki, Kamimoto Takumi, Kushida Junko, Gunji Shuichi, Saito Takayuki

    Meeting Abstracts of the Physical Society of Japan   Vol. 73   page: 418 - 418   2018

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    DOI: 10.11316/jpsgaiyo.73.1.0_418

  98. The GCT camera for the Cherenkov Telescope Array

    Lapington J. S., Abchiche A., Allan D., Amans J. -P., Armstrong T. P., Balzer A., Berge D., Boisson C., Bousquet J. -J., Bose R., Brown A. M., Bryan M., Buchholtz G., Buckley J., Chadwick P. M., Costantini H., Cotter G., Daniel M. K., De Franco A., De Frondat F., Dournaux J. -L., Dumas D., Ernenwein J. -P., Fasola G., Funk S., Gironnet J., Graham J. A., Greenshaw T., Hervet O., Hidaka N., Hinton J. A., Huet J. -M., Jankowsky D., Jegouzo I., Jogler T., Kawashima T., Kraus M., Laporte P., Leach S., Lefaucheur J., Markoff S., Melse T., Minaya I. A., Mohrmann L., Molyneux P., Moore P., Nolan S. J., Okumura A., Osborne J. P., Parsons R. D., Rosen S., Ross D., Rowell G., Rulten C. B., Sato Y., Sayede F., Schmoll J., Schoorlemmer H., Servillat M., Sol H., Stamatescu V., Stephan M., Stuik R., Sykes J., Tajima H., Thornhill J., Tibaldo L., Trichard C., Varner G., Vink J., Watson J. J., White R., Yamane N., Zech A., Zink A., Zorn J.

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   Vol. 876   page: 1-4   2017.12

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    DOI: 10.1016/j.nima.2016.12.010

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  99. Prototyping hexagonal light concentrators using high-reflectance specular films for the Large-Sized Telescopes of the Cherenkov Telescope Array Reviewed

    A. Okumura, et al.

    Journal of Instrumentation   Vol. 12   page: P12008   2017.12

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    DOI: 10.1088/1748-0221/12/12/P12008

  100. Prototyping hexagonal light concentrators using high-reflectance specular films for the Large-Sized Telescopes of the Cherenkov Telescope Array

    Okumura A., Dang T. V., Ono S., Tanaka S., Hayashida M., Hinton J., Katagiri H., Noda K., Teshima M., Yamamoto T., Yoshida T.

    JOURNAL OF INSTRUMENTATION   Vol. 12   2017.12

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    DOI: 10.1088/1748-0221/12/12/P12008

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  101. TARGET 5: A new multi-channel digitizer with triggering capabilities for gamma-ray atmospheric Cherenkov telescopes

    Albert A., Funk S., Katagiri H., Kawashima T., Murphy M., Okumura A., Quagliani R., Sapozhnikov L., Shigenaka A., Tajima H., Tibaldo L., Vandenbroucke J., Varner G., Wu T.

    ASTROPARTICLE PHYSICS   Vol. 92   page: 49-61   2017.6

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    DOI: 10.1016/j.astropartphys.2017.05.003

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  102. Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7-3946

    Acero F., Aloisio R., Amans J., Amato E., Antonelli L. A., Aramo C., Armstrong T., Arqueros F., Asano K., Ashley M., Backes M., Balazs C., Balzer A., Bamba A., Barkov M., Barrio J. A., Benbow W., Bernloehr K., Beshley V., Bigongiari C., Biland A., Bilinsky A., Bissaldi E., Biteau J., Blanch O., Blasi P., Blazek J., Boisson C., Bonanno G., Bonardi A., Bonavolonta C., Bonnoli G., Braiding C., Brau-Nogue S., Bregeon J., Brown A. M., Bugaev V., Bulgarelli A., Bulik T., Burton M., Burtovoi A., Busetto G., Bottcher M., Cameron R., Capalbi M., Caproni A., Caraveo P., Carosi R., Cascone E., Cerruti M., Chaty S., Chen A., Chen X., Chernyakova M., Chikawa M., Chudoba J., Cohen-Tanugi J., Colafrancesco S., Conforti V., Contreras J. L., Costa A., Cotter G., Covino S., Covone G., Cumani P., Cusumano G., D'Ammando F., D'Urso D., Daniel M., Dazzi F., De Angelis A., De Cesare G., De Franco A., De Frondat F., Dal Pino E. M. de Gouveia, De Lisio C., Lopez R. de los Reyes, De Lotto B., de Naurois M., De Palma F., Del Santo M., Delgado C., della Volpe D., Di Girolamo T., Di Giulio C., Di Pierro F., Di Venere L., Doro M., Dournaux J., Dumas D., Dwarkadas V., Diaz C., Ebr J., Egberts K., Einecke S., Elsaesser D., Eschbach S., Falceta-Goncalves D., Fasola G., Fedorova E., Fernandez-Barral A., Ferrand G., Fesquet M., Fiandrini E., Fiasson A., Filipovic M. D., Fioretti V., Font L., Fontaine G., Franco F. J., Freixas Coromina L., Fujita Y., Fukui Y., Funk S., Forster A., Gadola A., Lopez R. Garcia, Garczarczyk M., Giglietto N., Giordano F., Giuliani A., Glicenstein J., Gnatyk R., Goldoni P., Grabarczyk T., Graciani R., Graham J., Grandi P., Granot J., Green A. J., Griffiths S., Gunji S., Hakobyan H., Hara S., Hassan T., Hayashida M., Heller M., Helo J. C., Hinton J., Hnatyk B., Huet J., Huetten M., Humensky T. B., Hussein M., Horandel J., Ikeno Y., Inada T., Inome Y., Inoue S., Inoue T., Inoue Y., Ioka K., Iori M., Jacquemier J., Janecek P., Jankowsky D., Jung I., Kaaret P., Katagiri H., Kimeswenger S., Kimura S., Knodlseder J., Koch B., Kocot J., Kohri K., Komin N., Konno Y., Kosack K., Koyama S., Kraus M., Kubo H., Mezek G. Kukec, Kushida J., La Palombara N., Lalik K., Lamanna G., Landt H., Lapington J., Laporte P., Lee S., Lees J., Lefaucheur J., Lenain J. -P., Leto G., Lindfors E., Lohse T., Lombardi S., Longo F., Lopez M., Lucarelli F., Luque-Escamilla P. L., Lopez-Coto R., Maccarone M. C., Maier G., Malaguti G., Mandat D., Maneva G., Mangano S., Marcowith A., Marti J., Martinez M., Martinez G., Masuda S., Maurin G., Maxted N., Melioli C., Mineo T., Mirabal N., Mizuno T., Moderski R., Mohammed M., Montaruli T., Moralejo A., Mori K., Morlino G., Morselli A., Moulin E., Mukherjee R., Mundell C., Muraishi H., Murase K., Nagataki S., Nagayoshi T., Naito T., Nakajima D., Nakamori T., Nemmen R., Niemiec J., Nieto D., Nievas-Rosillo M., Nikolajuk M., Nishijima K., Noda K., Nogues L., Nosek D., Novosyadlyj B., Nozaki S., Ohira Y., Ohishi M., Ohm S., Okumura A., Ong R. A., Orito R., Orlati A., Ostrowski M., Oya I., Padovani M., Palacio J., Palatka M., Paredes J. M., Pavy S., Pe'er A., Persic M., Petrucci P., Petruk O., Pisarski A., Pohl M., Porcelli A., Prandini E., Prast J., Principe G., Prouza M., Pueschel E., Puelhofer G., Quirrenbach A., Rameez M., Reimer O., Renaud M., Ribo M., Rico J., Rizi V., Rodriguez J., Fernandez G. Rodriguez, Rodriguez Vazquez J. J., Romano P., Romeo G., Rosado J., Rousselle J., Rowell G., Rudak B., Sadeh I., Safi-Harb S., Saito T., Sakaki N., Sanchez D., Sangiorgi P., Sano H., Santander M., Sarkar S., Sawada M., Schioppa E. J., Schoorlemmer H., Schovanek P., Schussler F., Sergijenko O., Servillat M., Shalchi A., Shellard R. C., Siejkowski H., Sillanpaa A., Simone D., Sliusar V., Sol H., Stanic S., Starling R., Stawarz L., Stefanik S., Stephan M., Stolarczyk T., Szanecki M., Szepieniec T., Tagliaferri G., Tajima H., Takahashi M., Takeda J., Tanaka M., Tanaka S., Tejedor L. A., Telezhinsky I., Temnikov P., Terada Y., Tescaro D., Teshima M., Testa V., Thoudam S., Tokanai F., Torres D. F., Torresi E., Tosti G., Townsley C., Travnicek P., Trichard C., Trifoglio M., Tsujimoto S., Vagelli V., Vallania P., Valore L., van Driel W., van Eldik C., Vandenbroucke J., Vassiliev V., Vecchi M., Vercellone S., Vergani S., Vigorito C., Vorobiov S., Vrastil M., Vazquez Acosta M. L., Wagner S. J., Wagner R., Wakely S. P., Walter R., Ward J. E., Watson J. J., Weinstein A., White M., White R., Wierzcholska A., Wilcox P., Williams D. A., Wischnewski R., Wojcik P., Yamamoto T., Yamamoto H., Yamazaki R., Yanagita S., Yang L., Yoshida T., Yoshida M., Yoshiike S., Yoshikoshi T., Zacharias M., Zampieri L., Zanin R., Zavrtanik M., Zavrtanik D., Zdziarski A., Zech A., Zechlin H., Zhdanov V., Ziegler A., Zorn J.

    ASTROPHYSICAL JOURNAL   Vol. 840 ( 2 )   2017.5

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    DOI: 10.3847/1538-4357/aa6d67

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  103. Operating performance of the gamma-ray Cherenkov telescope: An end-to-end Schwarzschild-Couder telescope prototype for the Cherenkov Telescope Array

    Dournaux J. L., De Franco A., Laporte P., White R., Greenshaw T., Sol H., Abchiche A., Allan D., Amans J. P., Armstrong T. P., Balzer A., Berge D., Boisson C., Bousquet J. J., Brown A. M., Bryan M., Buchholtz G., Chadwick P. M., Costantini H., Cotter G., Daniel M., De Frondat F., Dumas D., Ernenwein J. P., Fasola G., Funk S., Gaudemard J., Graham J. A., Gironnet J., Hervet O., Hidaka N., Hinton J. A., Huet J. M., Jegouzo I., Jogler T., Kawashima T., Kraus M., Lapington J. S., Lefaucheur J., Markoff S., Melse T., Morhrmann L., Molnyeux P., Nolan S. J., Okumura A., Parsons R. D., Ross D., Rowell G., Sato Y., Sayede F., Schmoll J., Schoorlemmer H., Servillat M., Stamatescu V., Stephan M., Stuik R., Sykes J., Tajima H., Thornhill J., Tibaldo L., Trichard C., Vinkh J., Watson J., Yamane N., Zech A., Zink A.

    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT   Vol. 845   page: 355-358   2017.2

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    DOI: 10.1016/j.nima.2016.05.059

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  104. TARGET 5: a new multi-channel digitizer with triggering capabilities for gamma-ray atmospheric Cherenkov telescopes Reviewed

    A. Albert, S. Funk, T. Kawashima, M. Murphy, A. Okumura, R. Quagliani, L. Sapozhnikov, H. Tajima, L. Tibaldo, J. Vandenbroucke, G. Varner, T. Wu

    Astroparticle Physics   Vol. 92   page: 49-61   2017

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    DOI: 10.1016/j.astropartphys.2017.05.003

  105. Inauguration and First Light of the GCT-M Prototype for the Cherenkov Telescope Array

    J. J. Watson, A. De Franco, A. Abchiche, D. Allan, J. -P. Amans, T. P. Armstrong, A. Balzer, D. Berge, C. Boisson, J. -J. Bousquet, A. M. Brown, M. Bryan, G. Buchholtz, P. M. Chadwick, H. Costantini, G. Cotter, M. K. Daniel, F. De Frondat, J. -L. Dournaux, D. Dumas, J. -P. Ernenwein, G. Fasola, S. Funk, J. Gironnet, J. A. Graham, T. Greenshaw, O. Hervet, N. Hidaka, J. A. Hinton, J. -M. Huet, I. Jegouzo, T. Jogler, M. Kraus, J. S. Lapington, P. Laporte, J. Lefaucheur, S. Markoff, T. Melse, L. Mohrmann, P. Molyneux, S. J. Nolan, A. Okumura, J. P. Osborne, R. D. Parsons, S. Rosen, D. Ross, G. Rowell, C. B. Rulten, Y. Sato, F. Sayede, J. Schmoll, H. Schoorlemmer, M. Servillat, H. Sol, V. Stamatescu, M. Stephan, R. Stuik, J. Sykes, H. Tajima, J. Thornhill, L. Tibaldo, C. Trichard, J. Vink, R. White, N. Yamane, A. Zech, A. Zink, J. Zorn

    HIGH ENERGY GAMMA-RAY ASTRONOMY   Vol. 1792   2017

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    The Gamma-ray Cherenkov Telescope (GCT) is a candidate for the Small Size Telescopes (SSTs) of the Cherenkov Telescope Array (CTA). Its purpose is to extend the sensitivity of CTA to gamma-ray energies reaching 300 TeV. Its dual-mirror optical design and curved focal plane enables the use of a compact camera of 0.4 m diameter, while achieving a field of view of above 8 degrees. Through the use of the digitising TARGET ASICs, the Cherenkov flash is sampled once per nanosecond continuously and then digitised when triggering conditions are met within the analogue outputs of the photosensors. Entire waveforms (typically covering 96 ns) for all 2048 pixels are then stored for analysis, allowing for a broad spectrum of investigations to be performed on the data. Two prototypes of the GCT camera are under development, with differing photosensors: Multi -Anode Photomultipliers (MAPMs) and Silicon Photomultipliers (SiPMs). During November 2015, the GCT MAPM (GCT-M) prototype camera was integrated onto the GCT structure at the Observatoire de Paris-Meudon, where it observed the first Cherenkov light detected by a prototype instrument for CTA.

    DOI: 10.1063/1.4969027

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  106. TARGET: A Digitizing And Trigger ASIC For The Cherenkov Telescope Array

    S. Funk, D. Jankowsky, H. Katagiri, M. Kraus, A. Okumura, H. Schoorlemmer, A. Shigenaka, H. Tajima, L. Tibaldo, G. Varner, A. Zink, J. Zorn

    HIGH ENERGY GAMMA-RAY ASTRONOMY   Vol. 1792   2017

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    The future ground-based gamma-ray observatory Cherenkov Telescope Array (CTA) will feature multiple types of imaging atmospheric Cherenkov telescopes, each with thousands of pixels. To be affordable, camera concepts for these telescopes have to feature low cost per channel and at the same time meet the requirements for CTA in order to achieve the desired scientific goals. We present the concept of the TeV Array Readout Electronics with GSa/s sampling and Event Trigger (TARGET) Application Specific Circuit (ASIC), envisaged to be used in the cameras of various CTA telescopes, e. g. the Gamma-ray Cherenkov Telescope (GCT), a proposed 2-Mirror Small-Sized Telescope, and the Schwarzschild-Couder Telescope (SCT), a proposed Medium-Sized Telescope. In the latest version of this readout concept the sampling and trigger parts are split into dedicated ASICs, TARGET C and T5TEA, both providing 16 parallel input channels. TARGET C features a tunable sampling rate (usually 1 GSa/s), a 16k sample deep buffer for each channel and on-demand digitization and transmission of waveforms with typical spans of similar to 100 ns. The trigger ASIC, T5TEA, provides 4 low voltage differential signal (LVDS) trigger outputs and can generate a pedestal voltage independently for each channel. Trigger signals are generated by T5TEA based on the analog sum of the input in four independent groups of four adjacent channels and compared to a threshold set by the user. Thus, T5TEA generates four LVDS trigger outputs, as well as 16 pedestal voltages fed to TARGET C independently for each channel. We show preliminary results of the characterization and testing of TARGET C and T5TEA.

    DOI: 10.1063/1.4969033

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  107. The Gamma-ray Cherenkov Telescope for the Cherenkov Telescope Array

    L. Tibaldo, A. Abchiche, D. Allan, J. -P. Amans, T. P. Armstrong, A. Balzer, D. Bergey, C. Boisson, J. -J. Bousquet, A. M. Brown, M. Bryan, G. Buchholtz, P. M. Chadwick, H. Costantini, G. Cotter, M. K. Daniels, A. De Franco, F. De Frondat, J. -L. Dournaux, D. Dumas, J. -P. Ernenwein, G. Fasola, S. Funk, J. Gironnet, J. A. Graham, T. Greenshaws, O. Hervet, N. Hidaka, J. A. Hintoni, J. -M. Huet, D. Jankowsky, I. Jegouzo, T. Jogler, M. Kraus, J. S. Lapington, P. Laporte, J. Lefaucheur, S. Markoff, T. Melse, L. Mohrmann, P. Molyneux, S. J. Nolan, A. Okumura, J. P. Osborne, R. D. Parsons, S. Rosen, D. Ross, G. Rowell, C. B. Rulten, Y. Sato, F. Sayede, J. Schmoll, H. Schoorlemmer, M. Servillat, H. Sol, V. Stamatescu, M. Stephan, R. Stuik, J. Sykes, H. Tajima, J. Thornhill, C. Trichard, J. Vink, J. J. Watson, R. White, N. Yamane, A. Zech, A. Zink, J. Zorn

    HIGH ENERGY GAMMA-RAY ASTRONOMY   Vol. 1792   2017

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    The Cherenkov Telescope Array (CTA) is a forthcoming ground-based observatory for very-high-energy gamma rays. CTA will consist of two arrays of imaging atmospheric Cherenkov telescopes in the Northern and Southern hemispheres, and will combine telescopes of different types to achieve unprecedented performance and energy coverage. The Gamma-ray Cherenkov Telescope (GCT) is one of the small-sized telescopes proposed for CTA to explore the energy range from a few TeV to hundreds of TeV with a field of view greater than or similar to 8 degrees and angular resolution of a few arcminutes. The GCT design features dual-mirror SchwarzschildCouder optics and a compact camera based on densely-pixelated photodetectors as well as custom electronics. In this contribution we provide an overview of the GCT project with focus on prototype development and testing that is currently ongoing. We present results obtained during the first on-telescope campaign in late 2015 at the Observatoire de Paris-Meudon, during which we recorded the first Cherenkov images from atmospheric showers with the GCT multi-anode photomultiplier camera prototype. We also discuss the development of a second GCT camera prototype with silicon photomultipliers as photosensors, and plans toward a contribution to the realisation of CTA.

    DOI: 10.1063/1.4969025

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  108. Study of Interstellar Medium and Cosmic Rays in MBM 53-55 Molecular Clouds and the Pegasus Loop using Fermi-LAT Gamma-ray Observations

    Mizuno T, Abdollahi S, Fukui Y, Hayashi K, Okumura A, Tajima H, Yamamoto H

    Meeting Abstracts of the Physical Society of Japan   Vol. 72 ( 0 ) page: 461-461 - 461   2017

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    DOI: 10.11316/jpsgaiyo.72.1.0_461

  109. Improvement of scintillator's reflector toward the improvement of the performance for Compton scattering type polarimeter

    Saito Yo, Gunji Shuichi, Nakamori Takeshi, Okumura Akira, Nakazawa Kazuhiro, Kurosawa Shunsuke, Watanabe Naoki, Karube Atsuhito

    Meeting Abstracts of the Physical Society of Japan   Vol. 72 ( 0 ) page: 414-414 - 414   2017

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    DOI: 10.11316/jpsgaiyo.72.2.0_414

  110. CTA Report 124: A simulation study of CTA performance for measurement of electron/positron spectrum in TeV region(II)

    Ohishi Michiko, Nishijima Kyoshi, Miura Chika, Yoshikoshi Takanori, Yoshida Tatsuo, Ri Ken, the CTA-Japan, Inada Tomohiro, Okumura Akira, Katagiri Hideaki, Kushida Junko, Gunji Shuichi, Saito Takayuki, Sakaki Naoto, Chikawa Michiyuki

    Meeting Abstracts of the Physical Society of Japan   Vol. 72   page: 356 - 356   2017

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    DOI: 10.11316/jpsgaiyo.72.2.0_356

  111. Simulating the optical performance of a small-sized telescope with secondary optics for the Cherenkov Telescope Array Reviewed

    Cameron Rulten, Andreas Zech, Akira Okumura, Philippe Laporte, Jürgen Schmoll

    Astroparticle Physics   Vol. 82   page: 36-48   2016.5

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    DOI: 10.1016/j.astropartphys.2016.05.002

  112. ROBAST: Development of a ROOT-based ray-tracing library for cosmic-ray telescopes and its applications in the Cherenkov Telescope Array Reviewed

    Akira Okumura, Koji Noda, Cameron Rulten

    Astroparticle Physics     2015.12

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    DOI: 10.1016/j.astropartphys.2015.12.003

  113. Prototyping of Hexagonal Light Concentrators for the Large-Sized Telescopes of the Cherenkov Telescope Array

    Akira Okumura, Sakiya Ono, Syunya Tanaka, Masaaki Hayashidad, Hideaki Katagiri, Tatsuo Yoshida

    Proceedings of the 34th International Cosmic Ray Conference (ICRC2015)     page: 951   2015

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  114. ROBAST: Development of a Non-sequential Ray-tracing Simulation Library and its Applications in the Cherenkov Telescope Array

    A. Okumura, K. Noda, C. Rulten

    Proceedings of the 34th International Cosmic Ray Conference (ICRC2015)     page: 941   2015

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  115. Inferred Cosmic‐Ray Spectrum from Fermi Large Area Telescope γ‐Ray Observations of Earth's Limb

    M. Ackermann, M. Ajello, A. Albert, A. Allafort, L. Baldini, G. Barbiellini, D. Bastieri, K. Bechtol, R. Bellazzini, R. D. Blandford, E. D. Bloom, E. Bonamente, E. Bottacini, A. Bouvier, T. J. Brandt, M. Brigida, P. Bruel, R. Buehler, S. Buson, G. A. Caliandro, R. A. Cameron, P. A. Caraveo, C. Cecchi, E. Charles, R. C. G. Chaves, A. Chekhtman, J. Chiang, G. Chiaro, S. Ciprini, R. Claus, J. Cohen‐Tanugi, J. Conrad, S. Cutini, M. Dalton, F. D’Ammando, A. de Angelis, F. de Palma, C. D. Dermer, S. W. Digel, L. Di Venere, E. do Couto e Silva, P. S. Drell, A. Drlica‐ Wagner, C. Favuzzi, S. J. Fegan, E. C. Ferrara, W. B. Focke, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, D. Gasparrini, S. Germani, N. Giglietto, F. Giordano, M. Giroletti, T. Glanzman, G. Godfrey, G. A. Gomez‐Vargas, I. A. Grenier, J. E. Grove, S. Guiriec, M. Gustafsson, D. Hadasch, Y. Hanabata, A. K. Harding, M. Hayashida, K. Hayashi, J. W. Hewitt, D. Horan, X. Hou, R. E. Hughes, Y. Inoue, M. S. Jackson, T. Jogler, G. Jóhannesson, A. S. Johnson, T. Kamae, T. Kawano, J. Knödlseder, M. Kuss, J. Lande, S. Larsson, L. Latronico, F. Longo, F. Loparco, M. N. Lovellette, P. Lubrano, M. Mayer, M. N. Mazziotta, J. E. McEnery, J. Mehault, P. F. Michelson, W. Mitthumsiri, T. Mizuno, A. A. Moiseev, C. Monte, M. E. Monzani, A. Morselli, I. V. Moskalenko,§ S. Murgia, R. Nemmen, E. Nuss, T. Ohsugi, A. Okumura, M. Orienti, E. Orlando, J. F. Ormes, D. Paneque, J. H. Panetta, J. S. Perkins, M. Pesce‐Rollins, F. Piron, G. Pivato, T. A. Porter, S. Rainò, R. Rando, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, S. Ritz, M. Roth, M. Schaal, A. Schulz, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, A. W. Strong, H. Takahashi, Y. Takeuchi, J. G. Thayer, J. B. Thayer, D. J. Thompson, L. Tibaldo, M. Tinivella, D. F. Torres, G. Tosti, E. Troja, V. Tronconi, T. L. Usher, J. Vandenbroucke, V. Vasileiou, G. Vianello, V. Vitale, M. Werner, B. L. Winer, K. S. Wood, M. Wood, and Z. Yang

      Vol. 112   page: 151103   2014

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  116. Geometry dependence of the light collection efficiency of BGO crystal scintillators read out by avalanche photo diodes Reviewed

    M. Sasano, et al.

    Nuclear Instruments and Methods in Physics Research A   Vol. 715   page: 105-111   2013.3

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    DOI: 10.1016/j.nima.2013.03.022

  117. Optimization of the collection efficiency of a hexagonal light collector using quadratic and cubic Bézier curves Reviewed

    Akira Okumura

    Astroparticle Physics   Vol. 38   page: 18-24   2012.9

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  118. Gamma-Ray Observations of the Orion Molecular Clouds with the Fermi Large Area Telescope Reviewed

    M. Ackermann, M. Ajello, A. Allafort, E. Antolini, L. Baldini, J. Ballet, G. Barbiellini, D. Bastieri, K. Bechtol, R. Bellazzini, B. Berenji, R. D. Blandford, E. D. Bloom, E. Bonamente, A. W. Borgland, E. Bottacini, T. J. Brandt, J. Bregeon, M. Brigida, P. Bruel, R. Buehler, S. Buson, G. A. Caliandro, R. A. Cameron, P. A. Caraveo, C. Cecchi, A. Chekhtman, J. Chiang, S. Ciprini, R. Claus, J. Cohen-Tanugi, J. Conrad, F. D'Ammando, A. de Angelis, F. de Palma, C. D. Dermer, E. do Couto e Silva, P. S. Drell, A. Drlica-Wagner, T. Enoto, L. Falletti, C. Favuzzi, S. J. Fegan, E. C. Ferrara, W. B. Focke, Y. Fukazawa, Y. Fukui, P. Fusco, F. Gargano, D. Gasparrini, S. Germani, N. Giglietto, F. Giordano, M. Giroletti, T. Glanzman, G. Godfrey, S. Guiriec, D. Hadasch, Y. Hanabata, A. K. Harding, M. Hayashida, K. Hayashi, D. Horan, X. Hou, R. E. Hughes, M. S. Jackson, G. Jóhannesson, A. S. Johnson, T. Kamae, H. Katagiri, J. Kataoka, M. Kerr, J. Knödlseder, M. Kuss, J. Lande, S. Larsson, S.-H. Lee, F. Longo, F. Loparco, M. N. Lovellette, P. Lubrano, K. Makishima, M. N. Mazziotta, J. Mehault, W. Mitthumsiri, A. A. Moiseev, C. Monte, M. E. Monzani, A. Morselli, I. V. Moskalenko, S. Murgia, T. Nakamori, M. Naumann-Godo, S. Nishino, J. P. Norris, E. Nuss, M. Ohno, T. Ohsugi, A. Okumura, M. Orienti, E. Orlando, J. F. Ormes, M. Ozaki, D. Paneque, J. H. Panetta, D. Parent, V. Pelassa, M. Pesce-Rollins, M. Pierbattista, F. Piron, G. Pivato, T. A. Porter, S. Rainò, M. Razzano, A. Reimer, O. Reimer, M. Roth, H. F.-W. Sadrozinski, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, A. W. Strong, H. Takahashi, T. Takahashi, T. Tanaka, J. G. Thayer, J. B. Thayer, O. Tibolla, M. Tinivella, D. F. Torres, A. Tramacere, E. Troja, Y. Uchiyama, T. L. Usher, J. Vandenbroucke, V. Vasileiou, G. Vianello, V. Vitale, A. P. Waite, P. Wang, B. L. Winer, K. S. Wood, Z. Yang, S. Zimmer

    The Astrophysical Journal   Vol. 756 ( 1 ) page: 4   2012.9

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  119. TARGET: A multi-channel digitizer chip for very-high-energy gamma-ray telescopes Reviewed

    K. Bechtol, S. Funk, A. Okumura, L.L. Ruckman, A. Simons, H. Tajima, J. Vandenbroucke, G.S. Varner

    Astroparticle Physics   Vol. 36 ( 1 ) page: 156-165   2012.7

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  120. Design concepts for the Cherenkov Telescope Array CTA: an advanced facility for ground-based high-energy gamma-ray astronomy Reviewed

    Actis, M. et al.

    Experimental Astronomy   Vol. 32 ( 3 ) page: 193-316   2011.11

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  121. Development of an ASIC for Dual Mirror Telescopes of the Cherenkov Telescope Array

    Justin Vandenbroucke, Keith Bechtol, Stefan Funk, Akira Okumura, Hiro Tajima, Gary Varner

    Proceedings of the 32nd International Cosmic Ray Conference   Vol. 9   page: 161-164   2011

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  122. Development of Non-sequential Ray-tracing Software for Cosmic-ray Telescopes

    Akira Okumura, Masaaki Hayashida, Hideaki Katagiri, Takayuki Saito, Vladimir Vassiliev

    Proceedings of the 32nd International Cosmic Ray Conference   Vol. 9   page: 210-213   2011

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MISC 16

  1. CTA大口径望遠鏡初号機のカメラの較正と試験観測

    齋藤隆之, 猪目祐介, 岩村由樹, 大岡秀行, 岡崎奈緒, 小林志鳳, 櫻井駿介, 高橋光成, 手嶋政廣, HADASCH Daniela, MAZIN Daniel, 岡知彦, 梶原侑貴, 窪秀利, 野崎誠也, 平子丈, 増田周, 奥村曉, 折戸玲子, 片桐秀明, 鈴木萌, 野上優人, 吉田龍生, 櫛田淳子, 西嶋恭司, 古田智也, 郡司修一, 門叶冬樹, 中森健之, 砂田裕志, 寺田幸功, 永吉勤, 田中真伸, 田村謙治, 町支勇貴, 山本常夏, 林田将明, 馬場彩, 池野正弘, 内田智久

    日本天文学会年会講演予稿集   Vol. 2019   page: 236   2019.8

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  2. CTA報告151:CTA大口径望遠鏡初号機におけるカメラ集光器の量産と性能評価

    鈴木萌, 山本常夏, 吉田龍生, 稲田知大, 猪目祐介, 岩村由樹, 大岡秀行, 岡崎奈緒, 岡知彦, 奥村曉, 折戸玲子, 梶原侑貴, 片桐秀明, 櫛田淳子, 木村颯一朗, 窪秀利, 郡司修一, 小山志勇, 齋藤隆之, 櫻井駿介, 澤田真理, 砂田裕志, 高橋光成, 田中真伸, 田村謙治, 町支勇貴, 辻本晋平, 手嶋政廣, 手嶋政廣, 寺田幸功, 門叶冬樹, 中森健之, 永吉勤, 西嶋恭司, 西山楽, 野崎誠也, 林田将明, 馬場彩, 平子丈, 深見哲志, 古田智也, 増田周, HADASCH Daniela, MAZIN Daniel

    日本物理学会講演概要集(CD-ROM)   Vol. 74 ( 1 ) page: ROMBUNNO.17aK105‐8   2019.3

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  3. CTA Project 155: Status Report

    Teshima Masahiro, Kubo Hidetoshi, Totani Tomonori, Asano Katsuaki, Ioka Kunihito, Ishio Kazuma, Inada Tomohiro, Inoue Susumu, Inoue Tsuyoshi, Inoue Yoshiyuki, Inome Yusuke, Iwamura Yuki, Warren Donald, Uchiyama Yasunobu, Ohishi Michiko, Ohoka Hideyuki, Ohtani Yoshiki, Ohira Yutaka, Oka Tomohiko, Okazaki Nao, Ogata Tomoyuki, Okumura Akira, Orito Reiko, Kagaya Mika, Kajiwara Yuki, Kataoka Jun, Katagiri Hideaki, Katsukura Daisuke, Katsuda Satoru, Khalikov Emil, Kawanaka Norita, Kisaka Shota, Cui Xiaohong, Kushida Junko, Gunji Shuichi, Kohri Kazunori, Kobayashi Yukiho, Kong Albert K. H., Saito Takayuki, Sakaki Naoto, Sakurai Shunsuke, Sano Hidetoshi, Sawada Makoto, Shibata Toru, Dzhatdoev Timur, Suzuki Megumi, Suzuki Hiromasa, Suda Yusuke, Sunada Yuji, Zenin Anatolii, Takata Jumpei, Takahashi Keitaro, Takahashi Hiromitsu, Takahashi Mitsunari, Tajima Hiroyasu, Tachihara Kengo, Tanaka Shuta, Tanaka Takaaki, Tanaka Manobu, Tam Thomas P. H., Tamura Kenji, Cheng K. S., Chikawa Michiyuki, Choushi Yuuki, Tsujimoto Shimpei, Tsuru Takeshi, Tian Wenwu, Terada Yukikatsu, Toma Kenji, Tokanai Fuyuki, Naito Tsuguya, Nagataki Shigehiro, Nakamura Yuki, Nakamori Takeshi, Nakayama Kazunori, Nishijima Kyoshi, Nozaki Seiya, Noda Koji, Barkov Maxim, Hadasch Daniela, Hayakawa Takahiro, Hayashi Katsuhiro, Hayashida Masaaki, Hara Satoshi, Bamba Aya, Hidaka Naoya, Hiroshima Nagisa, Hirotani Kouichi, Hui David C. Y., Ferrand Gilles, Fukazawa Yasushi, Fukami Satoshi, Fukui Yasuo, Fujita Yutaka, Fujihara Chikako, Furuta Tomoya, He Haoning, Majumdar Pratik, Mazin Daniel, Matsumoto Hironori, Mizuno Tsunefumi, Muraish Hiroshi, Murase Kohta, Mori Koji, Yanagita Shohei, Yamazaki Ryo, Yamane Yumiko, Yamamoto Tokonatsu, Yamamoto Hiroaki, Yoshikoshi Takanori, Yoshida Atsumasa, Yoshida Tatsuo, Lee Shiu-Hang (Herman)

    Meeting Abstracts of the Physical Society of Japan   Vol. 74.2   page: 358 - 358   2019

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    DOI: 10.11316/jpsgaiyo.74.2.0_358

  4. CTA Report 147: General Report

    Kubo Hidetoshi, Teshima Masahiro, Totani Tomonori, Asano Katsuaki, Asano Akira, Ioka Kunihito, Ishio Kazuma, Inada Tomohiro, Inoue Susumu, Inoue Tsuyoshi, Inoue Yoshiyuki, Inome Yusuke, Iwamura Yuki, Warren Donald, Uchiyama Yasunobu, Ohishi Michiko, Ohoka Hideyuki, Ohtani Yoshiki, Ohira Yutaka, Oka Tomohiko, Okazaki Nao, Ogata Tomoyuki, Okumura Akira, Orito Reiko, Kagaya Mika, Kajiwara Yuki, Kataoka Jun, Katagiri Hideaki, Katsukura Daisuke, Katsuda Satoru, Kamimoto Takumi, Khalikov Emil, Kawanaka Norita, Kisaka Shota, Cui Xiaohong, Kushida Junko, Kumon Taku, Gunji Shuichi, Kohri Kazunori, Kobayashi Yukiho, Kong Albert K. H., Saito Takayuki, Sakaki Naoto, Sakurai Shunsuke, Sasai Yoshinori, Sano Hidetoshi, Sawada Makoto, Shibata Toru, Dzhatdoev Timur, Suzuki Megumi, Suda Yusuke, Sunada Yuji, Sekizaki Haruhito, Zenin Anatolii, Takata Jumpei, Takahashi Keitaro, Takahashi Tomoya, Takahashi Hiromitsu, Takahashi Mitsunari, Tajima Norio, Tajima Hiroyasu, Tachihara Kengo, Tanaka Shuta, Tanaka Takaaki, Tanaka Manobu, Taneda Yuuki, Tam Thomas P. H., Tamura Kenji, Cheng K. S., Chikawa Michiyuki, Choushi Yuuki, Tsujimoto Shimpei, Tsuru Takeshi, Tian Wenwu, Terada Yukikatsu, Toma Kenji, Tokanai Fuyuki, Naito Tsuguya, Nagataki Shigehiro, Nakamura Yuki, Nakamori Takeshi, Nakayama Kazunori, Nagayoshi Tsutomu, Nishijima Kyoshi, Nozaki Seiya, Noda Koji, Barkov Maxim, Hadasch Daniela, Hayakawa Takahiro, Hayashi Katsuhiro, Hayashida Masaaki, Hara Satoshi, Bamba Aya, Hidaka Naoya, Hirako Joe, Hiroshima Nagisa, Hirotani Kouichi, Hui David C. Y., Ferrand Gilles, Fukazawa Yasushi, Fukami Satoshi, Fukui Yasuo, Fujita Yutaka, Fujihara Chikako, Furuta Tomoya, He Haoning, Majumdar Pratik, Mazin Daniel, Masuda Shu, Matsumoto Hironori, Miura Chika, Mizuno Tsunefumi, Muraishi Hiroshi, Murase Kohta, Mori Koji, Yanagita Shohei, Yamazaki Ryo, Yamane Yumiko, Yamamoto Tokonatsu, Yamamoto Hiroaki, Yoshiike Satoshi, Yoshikoshi Takanori, Yoshid Atsumasa, Yoshida Tatsuo, Ri Ken, Lee Shiu-Hang (Herman)

    Meeting Abstracts of the Physical Society of Japan   Vol. 74.1   page: 556 - 556   2019

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    DOI: 10.11316/jpsgaiyo.74.1.0_556

  5. CTA報告142:CTA大口径望遠鏡初号機の焦点面カメラ統合試験(II)

    砂田裕志, 稲田知大, 猪目祐介, 岩村由樹, 大岡秀行, 岡崎奈緒, 奥村曉, 折戸玲子, 片岡淳, 片桐秀明, 櫛田淳子, 木村颯一朗, 窪秀利, 郡司修一, 小山志勇, 齋藤隆之, 櫻井駿介, 澤田真理, 鈴木萌, 高橋光成, 高原大, 田中真伸, 辻本晋平, 手嶋政廣, 手嶋政廣, 寺田幸功, 門叶冬樹, 中嶋大輔, 中森健之, 永吉勤, 西嶋恭司, 西山楽, 野崎誠也, 林田将明, 馬場彩, 平子丈, 深見哲志, 増田周, 山本常夏, 吉田龍生, HADASCH Daniela, MAZIN Daniel

    日本物理学会講演概要集(CD-ROM)   Vol. 73 ( 2 ) page: ROMBUNNO.16pS36‐8   2018.9

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  6. CTA大口径望遠鏡初号機のカメラ最終試験報告

    櫻井駿介, 稲田知大, 猪目祐介, 岩村由樹, 大岡秀行, 岡崎奈緒, 齋藤隆之, 澤田真理, 高橋光成, 手嶋政廣, 中嶋大輔, 深見哲志, HADASCH Daniela, MAZIN Daniel, 奥村曉, 折戸玲子, 片岡淳, 片桐秀明, 鈴木萌, 吉田龍生, 窪秀利, 今野裕介, 野崎誠也, 平子丈, 増田周, 木村颯一郎, 櫛田淳子, 辻本晋平, 西島恭司, 郡司修一, 門叶冬樹, 中森健之, 小山志勇, 砂田裕志, 寺田幸功, 永吉勤, 西山楽, 馬場彩, 高原大, 林田将明, 山本常夏, 池野正弘, 内田智久, 田中真伸

    日本天文学会年会講演予稿集   Vol. 2018   page: 229   2018.8

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  7. CTA報告133:CTA大口径望遠鏡初号機の焦点面カメラ統合試験

    野崎誠也, 稲田知大, 猪目祐介, 岩村由樹, 大岡秀行, 奥村曉, 岡崎奈緒, 折戸玲子, 片岡淳, 片桐秀明, 加藤翔, 木村颯一朗, 櫛田淳子, 窪秀利, 郡司修一, 小山志勇, 今野裕介, 齋藤隆之, 櫻井駿介, 澤田真理, 砂田裕志, 高橋光成, 高原大, 田中真伸, 辻本晋平, 手嶋政廣, 手嶋政廣, 寺田幸功, 門叶冬樹, 中嶋大輔, 中森健之, 永吉勤, 西嶋恭司, 西山楽, 林田将明, 馬場彩, 平子丈, 深見哲志, 増田周, 山本常夏, 吉田龍生, HADASCH Daniela, MAZIN Daniel, 池野正弘, 池野正弘, 内田智久, 内田智久

    日本物理学会講演概要集(CD-ROM)   Vol. 73 ( 1 ) page: ROMBUNNO.22aK307‐9   2018.3

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  8. CTA報告134:CTA大口径望遠鏡搭載光電子増倍管の経年変化の研究

    櫻井駿介, 永吉勤, 稲田知大, 猪目祐介, 岩村由樹, 大岡秀行, 奥村曉, 岡崎奈緒, 折戸玲子, 片岡淳, 片桐秀明, 木村颯一朗, 櫛田淳子, 窪秀利, 郡司修一, 小山志勇, 今野裕介, 齋藤隆之, 澤田真理, 砂田裕志, 高橋光成, 辻本晋平, 手嶋政廣, 手嶋政廣, 寺田幸功, 門叶冬樹, 中嶋大輔, 中森健之, 西嶋恭司, 西山楽, 野崎誠也, 林田将明, 馬場彩, 平子丈, 深見哲志, 増田周, 山本常夏, 吉田龍生, HADASCH Daniela, MAZIN Daniel, MAZIN Daniel

    日本物理学会講演概要集(CD-ROM)   Vol. 73 ( 1 ) page: ROMBUNNO.22aK307‐10   2018.3

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  9. CTA大口径望遠鏡初号機の焦点面カメラ統合試験

    平子丈, 窪秀利, 今野裕介, 野崎誠也, 増田周, 稲田知大, 岩村由樹, 大岡秀行, 岡崎奈緒, 齋藤隆之, 櫻井駿介, 高橋光成, 手嶋政廣, 中嶋大輔, 林田将明, 深見哲志, HADASCH Daniela, MAZIN Daniel, 猪目祐介, 高原大, 山本常夏, 奥村曉, 折戸玲子, 片桐秀明, 吉田龍生, 木村颯一朗, 櫛田淳子, 辻本晋平, 西嶋恭司, 郡司修一, 門叶冬樹, 中森健之, 小山志勇, 砂田裕志, 寺田幸功, 永吉勤, 西山楽, 馬場彩, 片岡淳, 澤田真理, 池野正弘, 田中真伸

    日本天文学会年会講演予稿集   Vol. 2018   page: 237   2018.2

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  10. CTA報告123:全体報告

    窪秀利, 手嶋政廣, 手嶋政廣, 戸谷友則, 浅野勝晃, 朝野彰, 井岡邦仁, 石尾一馬, 石尾一馬, 稲田知大, 井上進, 井上剛志, 井上芳幸, 猪目祐介, 岩村由樹, WARREN Donald, 内山泰伸, 大石理子, 大岡秀行, 大平豊, 岡崎奈緒, 奥村曉, 折戸玲子, 加賀谷美佳, 格和純, 片岡淳, 片桐秀明, 勝倉大輔, 勝田哲, 加藤翔, 神本匠, 川中宣太, 木坂将大, 木村颯一朗, CUI Xiaohong, 櫛田淳子, 久門拓, 黒田隼人, 郡司修一, 郡和範, 小山志勇, KONG Albert K. H, 齋藤隆之, 榊直人, 櫻井駿介, 佐々井義矩, 佐野栄俊, 澤田真理, 柴田徹, DZHATDOEV Timur, 砂田裕志, 関崎晴仁, 高田順平, 高橋慶太郎, 高橋知也, 高橋弘充, 高橋光成, 田島宏康, 立原研悟, 田中周太, 田中孝明, 田中真伸, 田中康之, 種田裕貴, TAM Thomas P. H, CHENG K. S, 千川道幸, 辻本晋平, 鶴剛, TIAN Wenwu, 寺田幸功, 當真賢二, 門叶冬樹, 内藤統也, 中嶋大輔, 長瀧重博, 中村裕樹, 中森健之, 中山和則, 永吉勤, 西嶋恭司, 西山楽, 野崎誠也, 野田浩司, BARKOV Maxim, HADASCH Daniela, 早川貴敬, 林克洋, 林田将明, 原敏, 馬場彩, 日高直哉, 平子丈, 廣島渚, 廣島渚, 広谷幸一, HUI David C. Y, FERRAND Gilles, 深沢泰司, 深見哲志, 福井康雄, 藤田裕, HE Haoning, MAJUMDAR Pratik, MAZIN Daniel, 増田周, 松本浩典, 三浦知佳, 水野恒史, 村石浩, 村瀬孔大, 森浩二, 柳田昭平, 山崎了, 山本常夏, 山本宏昭, 吉池智史, 吉越貴紀, 吉田篤正, 吉田龍生

    日本物理学会講演概要集(CD-ROM)   Vol. 72 ( 2 ) page: ROMBUNNO.13aU32‐1   2017.9

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  11. CTA報告126:CTA大口径望遠鏡焦点面検出器の改良と較正

    砂田裕志, 池野正弘, 池野正弘, 稲田知大, 猪目祐介, 岩村由樹, 内田智久, 内田智久, 大岡秀行, 奥村曉, 岡崎奈緒, 折戸玲子, 片岡淳, 片桐秀明, 木村颯一朗, 櫛田淳子, 窪秀利, 郡司修一, 小山志勇, 今野裕介, 齋藤隆之, 澤田真理, 櫻井駿介, 高橋光成, 田中真伸, 田中真伸, 辻本晋平, 手嶋政廣, 手嶋政廣, 寺田幸功, 門叶冬樹, 中嶋大輔, 中森健之, 永吉勤, 西嶋恭司, 西山楽, 野崎誠也, 林田将明, 馬場彩, 平子丈, 深見哲志, 増田周, 山本常夏, 吉田龍生, HADASCH Daniela, MAZIN Daniel

    日本物理学会講演概要集(CD-ROM)   Vol. 72 ( 2 ) page: ROMBUNNO.13aU32‐11   2017.9

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  12. CTA報告125:CTA大口径望遠鏡初号機の焦点面検出器建設状況

    櫻井駿介, 池野正弘, 池野正弘, 稲田知大, 猪目祐介, 岩村由樹, 内田智久, 内田智久, 大岡秀行, 奥村曉, 岡崎奈緒, 折戸玲子, 片岡淳, 片桐秀明, 木村颯一朗, 櫛田淳子, 窪秀利, 郡司修一, 小山志勇, 今野裕介, 齋藤隆之, 澤田真理, 砂田裕志, 高橋光成, 田中真伸, 田中真伸, 辻本晋平, 手嶋政廣, 手嶋政廣, 寺田幸功, 門叶冬樹, 中嶋大輔, 中森健之, 永吉勤, 西嶋恭司, 西山楽, 野崎誠也, 林田将明, 馬場彩, 平子丈, 深見哲志, 増田周, 山本常夏, 吉田龍生, HADASCH Daniela, MAZIN Daniel

    日本物理学会講演概要集(CD-ROM)   Vol. 72 ( 2 ) page: ROMBUNNO.13aU32‐10   2017.9

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  13. CTA大口径望遠鏡初号機カメラの建設状況

    平子丈, 窪秀利, 今野裕介, 野崎誠也, 増田周, 稲田知大, 岩村由樹, 大岡秀行, 岡崎奈緒, 齋藤隆之, 櫻井駿介, 高橋光成, 手嶋政廣, 中嶋大輔, 林田将明, 深見哲志, HADASCH Daniela, MAZIN Daniel, 猪目祐介, 山本常夏, 奥村曉, 折戸玲子, 片桐秀明, 吉田龍生, 木村颯一朗, 櫛田淳子, 辻本晋平, 西嶋恭司, 郡司修一, 門叶冬樹, 中森健之, 小川志勇, 砂田裕志, 寺田幸功, 永吉勤, 西山楽, 馬場彩, 片岡淳, 澤田真理, 池野正弘, 内田智久, 田中真伸

    日本天文学会年会講演予稿集   Vol. 2017   page: 255   2017.8

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  14. 将来の硬X線・ガンマ線衛星に向けたシンチレータ反射材の改良

    清野愛海, 奥田和史, 中澤知洋, 奥村曉, 郡司修一, 牧島一夫

    日本天文学会年会講演予稿集   Vol. 2017   page: 242   2017.8

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  15. CTA報告 119:CTA大口径望遠鏡初号機の焦点面カメラのシステム統合試験

    中嶋大輔, 猪目祐介, 大岡秀行, 奥村曉, 折戸玲子, 片桐秀明, 岸田柊, 木村颯一朗, 窪秀利, 櫛田淳子, 郡司修一, 今野裕介, 齋藤隆之, 齋藤隆之, 櫻井駿介, 高橋光成, 武田淳希, 谷川俊介, TAN Dang Viet, 辻本晋平, 手嶋政廣, 手嶋政廣, 寺田幸功, 門叶冬樹, 中森健之, 永吉勤, 西嶋恭司, 西山楽, 野崎誠也, 林田将明, 馬場彩, 増田周, 山本常夏, 吉田龍生, 吉田麻佑, MAZIN Daniel, HADASCH Daniela

    日本物理学会講演概要集(CD-ROM)   Vol. 72 ( 1 ) page: ROMBUNNO.18pK21‐8   2017.3

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  16. CTA報告117:全体報告

    手嶋政廣, 手嶋政廣, 窪秀利, 戸谷友則, 朝野彰, 浅野勝晃, 井岡邦仁, 池野祐平, 石尾一馬, 石尾一馬, 稲田知大, 井上進, 井上剛志, 井上芳幸, 猪目祐介, 岩村由樹, WARREN Donald, 内山泰伸, 梅津陽平, 大石理子, 大岡秀行, 大平豊, 岡崎奈緒, 奥村曉, 折戸玲子, 加賀谷美佳, 格和純, 片岡淳, 片桐秀明, 加藤翔, 川中宣太, 木坂将大, 岸田柊, 木村颯一朗, CUI Xiaohong, 櫛田淳子, 黒田隼人, 郡司修一, 郡和範, 小山志勇, KONG Albert K. H, 今野裕介, 齋藤隆之, 榊直人, 櫻井駿介, 佐藤雄太, 佐野栄俊, 澤田真理, 重中茜, 柴田徹, 高田順平, 高橋慶太郎, 高橋弘充, 高橋光成, 高見将太, 武田淳希, 田島宏康, 立原研悟, 田中周太, 田中孝明, 田中真伸, 田中康之, 谷川俊介, TAM Thomas P. H, TAN Dang Viet, CHENG K. S, 千川道幸, 辻本晋平, 鶴剛, TIAN Wenwu, 寺田幸功, 當真賢二, 門叶冬樹, 友野弥生, 内藤統也, 中嶋大輔, 長瀧重博, 中村裕樹, 中森健之, 中山和則, 永吉勤, 西嶋恭司, 西山楽, 野崎誠也, 野田浩司, BARKOV Maxim, HADASCH Daniela, 早川貴敬, 林克洋, 林田将明, 原敏, 馬場彩, 日高直哉, 平井亘, 廣島渚, 廣島渚, 広谷幸一, HUI DavidC. Y, FERRAND Gilles, 深沢泰司, 深見哲志, 福井康雄, 藤田裕, HE Haoning, MAJUMDAR Pratik, MAZIN Daniel, 増田周, 松本浩典, 水野恒史, 村石浩, 村瀬孔大, 本橋大輔, 森浩二, 柳田昭平, 山崎了, 山根暢仁, 山本常夏, 山本宏昭, 吉池智史, 吉越貴紀

    日本物理学会講演概要集(CD-ROM)   Vol. 72 ( 1 ) page: ROMBUNNO.18aS11‐5   2017.3

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Presentations 4

  1. Final characterisation and design of the Gamma-ray Cherenkov Telescope (GCT) for the Cherenkov Telescope Array

    Le Blanc O.

    Proceedings of SPIE - The International Society for Optical Engineering 

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    Event date: 2018.1

    Language:English   Presentation type:Oral presentation (general)  

    DOI: 10.1117/12.2313158

    Scopus

  2. Inauguration and first light of the GCT-M prototype for the Cherenkov telescope array

    Watson J.

    AIP Conference Proceedings 

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    Event date: 2017.1

    Language:English   Presentation type:Oral presentation (general)  

    DOI: 10.1063/1.4969027

    Scopus

  3. The gamma-ray Cherenkov telescope for the Cherenkov telescope array

    Tibaldo L.

    AIP Conference Proceedings 

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    Event date: 2017.1

    Language:English   Presentation type:Oral presentation (general)  

    DOI: 10.1063/1.4969025

    Scopus

  4. TARGET: A digitizing and trigger ASIC for the Cherenkov telescope array

    Funk S.

    AIP Conference Proceedings 

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    Event date: 2017.1

    Language:English   Presentation type:Oral presentation (general)  

    DOI: 10.1063/1.4969033

    Scopus

KAKENHI (Grants-in-Aid for Scientific Research) 14

  1. 多粒子宇宙観測技術の開発による新たな「眼」の獲得

    Grant number:23H04897  2023.4 - 2028.3

    科学研究費助成事業  学術変革領域研究(A)

    奥村 曉

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    Authorship:Principal investigator 

    Grant amount:\112710000 ( Direct Cost: \86700000 、 Indirect Cost:\26010000 )

  2. The creation of multimessenger astrophysics

    Grant number:23H04891  2023.4 - 2028.3

    Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research  Grant-in-Aid for Transformative Research Areas (A)

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    Authorship:Coinvestigator(s) 

  3. Comprehensive Understanding of Galactic and Extragalactic Cosmic-ray Acceleration by Exploring Gamma-ray Observations beyond 100 TeV

    Grant number:20H01916  2020.4 - 2023.3

    Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research Grant-in-Aid for Scientific Research (B)  Grant-in-Aid for Scientific Research (B)

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    Authorship:Principal investigator 

    Grant amount:\17550000 ( Direct Cost: \13500000 、 Indirect Cost:\4050000 )

  4. Improving the gamma-ray detection sensitivity of the Cherenkov Telescope Array to discover dark matter and Galactic PeVatrons

    Grant number:18KK0384  2019 - 2021

    Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research Fund for the Promotion of Joint International Research (Fostering Joint International Research (A))  Fund for the Promotion of Joint International Research (Fostering Joint International Research (A))

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    Authorship:Principal investigator 

    Grant amount:\15600000 ( Direct Cost: \12000000 、 Indirect Cost:\3600000 )

  5. 銀河内PeVatron探査のための地上ガンマ線望遠鏡の開発

    2017.4 - 2019.3

    科学研究費補助金  若手研究(A)

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    Authorship:Principal investigator 

  6. Development of Ground-based Gamma-ray Telescopes for Galactic PeVatron Search

    Grant number:17H04838  2017.4 - 2019.3

    Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research Grant-in-Aid for Young Scientists (A)  Grant-in-Aid for Young Scientists (A)

    Okumura Akira

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    Authorship:Principal investigator  Grant type:Competitive

    Grant amount:\25610000 ( Direct Cost: \19700000 、 Indirect Cost:\5910000 )

    In this research we achieved two main results for the Cherenkov Telescope Array (CTA) project, the next-generation ground-based gamma-ray observatory, to be built in 2020s. The first result is the successful completion of our prototype CTA camera with 2048 silicon photomultiplier camera pixels for the CTA small-sized telescopes. It was installed on a CTA prototype telescope in Italy, and its first light was achieved in 2019. The second result is gamma-ray detection of the Crab Nebula with another CTA prototype camera and telescope for the medium-sized telescopes, that use similar technologies but with a larger mirror diameter. These results are important milestones proving that our camera and telescope designs are viable for CTA.

  7. Developing an aspherical lens array system to halve the production cost of large-area silicon photomultiplier arrays

    Grant number:16K13801  2016.4 - 2018.3

    Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research Grant-in-Aid for Challenging Exploratory Research  Grant-in-Aid for Challenging Exploratory Research

    Okumura Akira

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    Authorship:Principal investigator 

    Grant amount:\3510000 ( Direct Cost: \2700000 、 Indirect Cost:\810000 )

    We have developed a UV-transparent lens array system to improve the effective photodetection efficiency of multi-pixel silicon photomultiplier (SiPM) arrays. Array type SiPMs currently available in the market have dead area between adjacent pixels, resulting in about 15% photon loss. Putting a lens array on the SiPM surface can guide photons from the dead area to the sensitive area, enabling us to improve the gamma-ray detection efficiency of ground-based gamma-ray telescopes or to reduce the production cost of photodetectors. Our prototype lens array showed improvement of photodetection efficiency by 10 to 20% in the angle-of-incidence range of 0 to 70 degrees.

  8. 大面積の半導体光検出器アレイの製造費用を半額にする非球面レンズアレイの開発

    2016.4 - 2017.3

    科学研究費補助金  挑戦的萌芽研究

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    Authorship:Principal investigator 

  9. 大面積の半導体光検出器アレイの製造費用を半額にする非球面レンズアレイの開発

    2016.4 - 2017.3

    科学研究費助成事業  挑戦的萌芽研究

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    Grant type:Competitive

  10. Improving the sensitivity of the next-generation gamma-ray observatory CTA with higher collection efficiency of atmospheric Cherenkov photons

    Grant number:25707017  2013.4 - 2018.3

    Japan Society for the Promotion of Science  Grants-in-Aid for Scientific Research Grant-in-Aid for Young Scientists (A)  Grant-in-Aid for Young Scientists (A)

    Okumura Akira

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    Authorship:Principal investigator 

    Grant amount:\22490000 ( Direct Cost: \17300000 、 Indirect Cost:\5190000 )

    We have developed a prototype hexagonal light concentrator for the Large-Sized Telescopes of the Cherenkov Telescope Array. To maximize the photodetection efficiency of the focal-plane camera pixels for atmospheric Cherenkov photons and to lower the energy threshold, a specular film with a very high reflectance of 92-99% has been developed to cover the inner surfaces of the light concentrators. The prototype has a relative anode sensitivity (which can be roughly regarded as collection efficiency) of about 95 to 105% at the most important angles of incidence.

  11. 大気チェレンコフ光の収集効率改善による次世代ガンマ線望遠鏡CTAの高感度化

    2013.4 - 2017.3

    科学研究費補助金  若手研究(A)

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    Authorship:Principal investigator 

  12. 大気チェレンコフ光の収集効率改善による次世代ガンマ線望遠鏡CTAの高感度化

    2013.4 - 2017.3

    日本学術振興会  科学研究費助成事業  若手研究(A)

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    Grant type:Competitive

  13. CTA大口径望遠鏡アクティブ・ミラー制御(AMC)システムの開発

    2013.4 - 2016.3

    科学研究費補助金  基盤研究(B)

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    Authorship:Coinvestigator(s) 

  14. 世界最高の角度分解能を持つ光学望遠鏡の実現

    2013.4 - 2015.3

    科学研究費補助金  挑戦的萌芽研究

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    Authorship:Principal investigator 

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Industrial property rights 1

  1. 光学製品及び集光器

    奥村曉, 西本圭司, 井上知晶

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    Application no:特願2021-031974  Date applied:2021

 

Teaching Experience (On-campus) 2

  1. 先端物理学特論

    2020

  2. 物理実験学

    2020