研究者詳細 - 奥村　曉

論文 - 奥村　曉

分割表示 194 件中 1 - 20 件目／全件表示 >>

Development and quality control of PMT modules for the large-sized telescopes of the Cherenkov Telescope Array Observatory Open Access

Saito, T; Takahashi, M; Inome, Y; Abe, H; Artero, M; Blanch, O; González, JB; Fukami, S; Hadasch, D; Hanabata, Y; Hattori, Y; Llorente, JH; Ishio, K; Iwasaki, H; Katagiri, H; Kawamura, K; Kerszberg, D; Kimura, S; Kiyomoto, T; Kojima, T; Konno, Y; Kobayashi, Y; Koyama, S; Kubo, H; Kushida, J; López-Oramas, A; Masuda, S; Matsuoka, S; Mazin, D; Nakajima, D; Nakamori, T; Nagayoshi, T; Ninci, D; Nishijima, K; Nishiyama, G; Nogami, Y; Nozaki, S; Ogino, M; Ohoka, H; Oka, T; Ono, S; Okumura, A; Orito, R; Rugliancich, A; Sakurai, S; Sasaki, N; Sunada, Y; Suzuki, M; Tamura, K; Takeda, J; Terada, Y; Teshima, M; Tokanai, F; Tomono, Y; Tsujimoto, S; Tsukamoto, Y; Umetsu, Y; Yamamoto, T; Yoshida, T

NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT 1073 巻 2025年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment

The camera of the Large-Sized Telescopes (LSTs) of the Cherenkov Telescope Array Observatory (CTAO) consists of 1855 pixels that are grouped into 265 high-performance photomultiplier tube (PMT) modules. Each module comprises a seven-light-guide plate, seven PMT units, a slow control board, and a readout board with a trigger board. The requirements for the PMT modules include various aspects, such as photon detection efficiency, dynamic range, buffer depth, and test pulse functionality. We have developed a high-performance PMT module that fulfills all these requirements. Mass-production and quality control (QC) of modules for all four LSTs of the northern CTAO have been completed. Here we report on the technical details of each element of the module and its performance, together with the methods and results of QC measurements.

DOI： 10.1016/j.nima.2025.170229

Characterization of Markarian 421 during its most violent year: Multiwavelength variability and correlations Open Access

Abe K., Abe S., Abhir J., Abhishek A., Acciari V.A., Aguasca-Cabot A., Agudo I., Aniello T., Ansoldi S., Antonelli L.A., Arbet Engels A., Arcaro C., Asano K., Baack D., Babiäa A., Barres De Almeida U., Barrio J.A., Batkoviäa I., Bautista A., Baxter J., Becerra González J., Bednarek W., Bernardini E., Bernete J., Berti A., Besenrieder J., Bigongiari C., Biland A., Blanch O., Bonnoli G., Bošnjak , Bronzini E., Burelli I., Campoy-Ordaz A., Carosi R., Carretero-Castrillo M., Castro-Tirado A.J., Cerasole D., Ceribella G., Chai Y., Cifuentes A., Colombo E., Contreras J.L., Cortina J., Covino S., DâÂ€Â™ amico G., DâÂ€Â™ ammando F., DâÂ€Â™ elia V., Da Vela P., Dazzi F., De Angelis A., De Lotto B., De Menezes R., Delfino M., Delgado J., Delgado Mendez C., Di Pierro F., Di Tria R., Di Venere L., Dominis Prester D., Donini A., Dorner D., Doro M., Eisenberger L., Elsaesser D., Escudero J., Fariña L., Fattorini A., Foffano L., Font L., Fröse S., Fukami S., Fukazawa Y., García López R.J., Garczarczyk M., Gasparyan S., Gaug M., Giesbrecht Paiva J.G., Giglietto N., Giordano F., Gliwny P., Godinoviäa N., Gradetzke T., Grau R., Green D., Green J.G., Günther P., Hadasch D., Hahn A., Hassan T., Heckmann L., Herrera Llorente J., Hrupec D., Imazawa R., Ishio K., Jiménez Martínez I., Jormanainen J., Kankkunen S., Kayanoki T., Kerszberg D.

Astronomy and Astrophysics 694 巻 2025年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

Aims. Mrk 421 was in its most active state around early 2010, which led to the highest TeV gamma-ray flux ever recorded from any active galactic nuclei (AGN).We aim to characterize the multiwavelength behavior during this exceptional year for Mrk 421, and evaluate whether it is consistent with the picture derived with data from other less exceptional years. Methods. We investigated the period from November 5, 2009, (MJD 55140) until July 3, 2010, (MJD 55380) with extensive coverage from very-high-energy (VHE; E > 100 GeV) gamma rays to radio with MAGIC, VERITAS, Fermi-LAT, RXTE, Swift, GASP-WEBT, VLBA, and a variety of additional optical and radio telescopes. We characterized the variability by deriving fractional variabilities as well as power spectral densities (PSDs). In addition, we investigated images of the jet taken with VLBA and the correlation behavior among di_erent energy bands. Results. Mrk 421 was in widely di_erent states of activity throughout the campaign, ranging from a low-emission state to its highest VHE flux ever recorded. We find the strongest variability in X-rays and VHE gamma rays, and PSDs compatible with power-law functions with indices around 1.5. We observe strong correlations between X-rays and VHE gamma rays at zero time lag with varying characteristics depending on the exact energy band. We also report a marginally significant (_3_) positive correlation between high-energy (HE; E > 100 MeV) gamma rays and the ultraviolet band. We detected marginally significant (_3_) correlations between the HE and VHE gamma rays, and between HE gamma rays and the X-ray, that disappear when the large flare in February 2010 is excluded from the correlation study, hence indicating the exceptionality of this flaring event in comparison with the rest of the campaign. The 2010 violent activity of Mrk 421 also yielded the first ejection of features in the VLBA images of the jet of Mrk 421. Yet the large uncertainties in the ejection times of these unprecedented radio features prevent us from firmly associating them to the specific flares recorded during the 2010 campaign. We also show that the collected multi-instrument data are consistent with a scenario where the emission is dominated by two regions, a compact and extended zone, which could be considered as a simplified implementation of an energy-stratified jet as suggested by recent IXPE observations.

DOI： 10.1051/0004-6361/202451624

Time-dependent modelling of short-term variability in the TeV-blazar VER J0521+211 during the major flare in 2020

MAGIC Collaboration , Abe S., Abhir J., Abhishek A., Acciari V.A., Aguasca-Cabot A., Agudo I., Aniello T., Ansoldi S., Antonelli L.A., Arbet Engels A., Arcaro C., Artero M., Asano K., Baack D., Babić A., Barres De Almeida U., Barrio J.A., Batković I., Bautista A., Baxter J., Becerra González J., Bednarek W., Bernardini E., Bernete J., Berti A., Besenrieder J., Bigongiari C., Biland A., Blanch O., Bonnoli G., Bošnjak , Bronzini E., Burelli I., Campoy-Ordaz A., Carosi A., Carosi R., Carretero-Castrillo M., Castro-Tirado A.J., Cerasole D., Ceribella G., Chai Y., Cifuentes A., 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., De Menezes R., Delfino M., Delgado J., Delgado Mendez C., Di Pierro F., Di Tria R., Di Venere L., Dominis Prester D., Donini A., Dorner D., Doro M., Eisenberger L., Elsaesser D., Escudero J., Fariña L., Fattorini A., Foffano L., Font L., Fröse S., Fukami S., Fukazawa Y., García López R.J., Garczarczyk M., Gasparyan S., Gaug M., Giesbrecht Paiva J.G., Giglietto N., Giordano F., Gliwny P., Gradetzke T., Grau R., Green D., Green J.G., Günther P., Hadasch D., Hahn A., Hassan T., Heckmann L., Herrera Llorente J., Hrupec D., Imazawa R., Ishio K., Jiménez Martínez I., Jormanainen J., Kankkunen S., Kayanoki T., Kerszberg D.

Astronomy and Astrophysics 694 巻 2025年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

Self-repairing graphite protective layer has been discovered as a suitable protective layer in blast furnace (BF) hearth in recent years. In the current study, actual samples of self-repairing graphite protective layer taken from a commercial BF were analyzed in detail. The results revealed that the hot face of graphite protective layer exhibits a distinct white graphite luster, with large areas of graphite adhering to the surface. Along the direction of its formation, the sample displays a striped pattern with alternating layers. The graphite is strip-shaped, it is relatively coarse and unevenly distributed. The coarse graphite runs in the same direction, unlike graphite in molten iron which has no fixed direction in a chaotic state. The formation process of selfrepairing graphite protective layer can be concluded, graphite precipitates at the interface through heterogeneous nucleation. Crystal nuclei often preferentially adhere to the surface of these impurities to form, owing to the fact that the nucleation energy of heterogeneous nucleation is lower than that of homogeneous nucleation. Titanium is discovered during the observation of microscopic morphology of graphite protective layer, graphite protective layer is more robust due to the strengthening effect of titanium. Titanium strengthening mechanism of self-repairing graphite protective layer is summarized, the strengthening mechanism can be divided into four steps. TiC particles are dispersed around graphite, which reduces the difficulty of the orientation of flake graphite growth. The presence of TiC increases the growth rate of crystals. The four steps are cyclically performed, so the self-repairing graphite protective layer can precipitate layer by layer through titanium strengthening mechanism, which serves to protect the carbon brick in BF hearth.

DOI： 10.1051/0004-6361/202451378

Cosmic-ray acceleration and escape from supernova remnant W44 as probed by <i>Fermi</i>-LAT and MAGIC

Abe, S; Abhir, J; Abhishek, A; Acciari, VA; Aguasca-Cabot, A; Agudo, I; Aniello, T; Ansoldi, S; Antonelli, LA; Engels, AA; Arcaro, C; Asano, K; Babic, A; Baquero, A; de Almeida, UB; Barrio, JA; Batkovic, I; Bautista, A; Baxter, J; González, JB; Bednarek, W; Bernardini, E; Bernete, J; Berti, A; Besenrieder, J; Bigongiari, C; Biland, A; Blanch, O; Bonnoli, G; Bosnjak, Z; Bronzini, E; Burelli, I; Busetto, G; Campoy-Ordaz, A; Carosi, A; Carosi, R; Carretero-Castrillo, M; Castro-Tirado, AJ; Cerasole, D; Ceribella, G; Chai, Y; Chilingarian, A; Cifuentes, A; 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; de Menezes, R; Del Popolo, A; Delfino, M; Delgado, J; Mendez, CD; Di Pierro, F; Prester, DD; Donini, A; Dorner, D; Doro, M; Elsaesser, D; Emery, G; Escudero, J; Fariña, L; Fattorini, A; Foffano, L; Font, L; Fröse, S; Fukazawa, Y; López, RJG; Garczarczyk, M; Gasparyan, S; Gaug, M; Paiva, JGG; Giglietto, N; Gliwny, P; Godinovic, N; Gozzini, SR; Gradetzke, T; Grau, R; Green, JG; Günther, P; Hadasch, D; Hahn, A; Hassan, T; Heckmann, L; Herrera, J; Hrupec, D; Hütten, M; Imazawa, R; Ishio, K; Martínez, IJ; Jormanainen, J; Kayanoki, T; Kerszberg, D; Kluge, GW; Kobayashi, Y; Kouch, PM; Kubo, H; Kushida, J; Láinez, M; 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; 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; 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; Peresano, M; 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; Silvestri, G; 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; Temnikov, P; Terauchi, K; Terzic, T; Teshima, M; Truzzi, S; Tutone, A; Ubach, S; van Scherpenberg, J; Acosta, MV; Ventura, S; Viale, I; Vigorito, CF; Vitale, V; Vovk, I; Walter, R; Will, M; Wunderlich, C; Yamamoto, T; Di Tria, R; Di Venere, L; Giordano, F; Bissaldi, E; Green, D; Morlino, G

ASTRONOMY & ASTROPHYSICS 693 巻 2025年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

Context. The supernova remnant (SNR) W44 and its surroundings are a prime target for studying the acceleration of cosmic rays (CRs). Several previous studies established an extended gamma-ray emission that is set apart from the radio shell of W44. This emission is thought to originate from escaped high-energy CRs that interact with a surrounding dense molecular cloud complex. Aims. We present a detailed analysis of Fermi-LAT data with an emphasis on the spatial and spectral properties of W44 and its surroundings. We also report the results of the observations performed with the MAGIC telescopes of the northwestern region of W44. Finally, we present an interpretation model to explain the gamma-ray emission of the SNR and its surroundings. Methods. We first performed a detailed spatial analysis of 12 years of Fermi-LAT data at energies above 1 GeV, in order to exploit the better angular resolution, while we set a threshold of 100 MeV for the spectral analysis. We performed a likelihood analysis of 174 hours of MAGIC data above 130 GeV using the spatial information obtained with Fermi-LAT. Results. The combined spectra of Fermi-LAT and MAGIC, extending from 100 MeV to several TeV, were used to derive constraints on the escape of CRs. Using a time-dependent model to describe the particle acceleration and escape from the SNR, we show that the maximum energy of the accelerated particles has to be '40 GeV. However, our gamma-ray data suggest that a small number of lower-energy particles also needs to escape. We propose a novel model, the broken-shock scenario, to account for this effect and explain the gamma-ray emission.

DOI： 10.1051/0004-6361/202449748

Event reconstruction using pattern spectra and convolutional neural networks for the Cherenkov Telescope Array

Wilkinson M.H.F., Peletier R.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., Bernardos M.I.

Proceedings of Science 417 巻 2024年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Proceedings of Science

The Cherenkov Telescope Array (CTA) is the future observatory for ground-based imaging atmospheric Cherenkov 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 camera images that can be used as training data for convolutional neural networks (CNNs) to differentiate signals from background events and to determine the energy of the initial gamma-ray events. Pattern spectra are commonly used tools for image classification and provide the distributions of the sizes and shapes of features comprising an image. The application of pattern spectra on a CNN allows the selection of relevant combinations of features within an image. In this work, we generate pattern spectra from simulated gamma-ray images to train a CNN for signal-background separation and energy reconstruction for CTA. We compare our results to a CNN trained with CTA images and find that the pattern spectra-based analysis is computationally less expensive but not competitive with the purely CTA images-based analysis. Thus, we conclude that the CNN must rely on additional features in the CTA images not captured by the pattern spectra.

CTC and CT5TEA: An advanced multi-channel digitizer and trigger ASIC for imaging atmospheric Cherenkov telescopes Open Access

Schwab, B; Zink, A; Varner, G; Depaoli, D; Hinton, J; Liu, G; Okumura, A; Ross, D; Schäfer, J; Schoorlemmer, H; Tajima, H; Vandenbroucke, J; White, R; Watson, JJ; Zorn, J; Funk, S

NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT 1069 巻 2024年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment

We have developed a new set of Application-Specific Integrated Circuits (ASICs) of the TARGET family (CTC and CT5TEA), designed for the readout of signals from photosensors in cameras of Imaging Atmospheric Cherenkov Telescopes (IACTs) for ground-based gamma-ray astronomy. We present the performance and design details. Both ASICs feature 16 channels, with CTC being a Switched-Capacitor Array (SCA) sampler at 0.5 to 1 GSa/s with a 16,384 sample deep storage buffer, including the functionality to digitize full waveforms at arbitrary times. CT5TEA is its companion trigger ASIC (though may be used on its own), which provides trigger information for the analog sum of four (and 16) adjacent channels. Since sampling and triggering takes place in two separate ASICs, the noise due to interference from the SCA is suppressed, and allows a minimal trigger threshold of ≤ 2.5 mV (0.74 photo electrons (p.e.)) with a trigger noise of ≤ 0.5 mV (0.15 p.e.). For CTC, a maximal input voltage range from −0.5 V up to 1.7 V is achieved with an effective bit range of > 11.6 bits and a baseline noise of 0.7 mV. The cross-talk improved to ≤ 1% over the whole −3 dB bandwidth of 220 MHz and even down to 0.2% for 1.5 V pulses of 10 ns width. Not only is the performance presented, but a temperature-stable calibration routine for pulse mode operation is introduced and validated. The resolution is found to be ∼ 2.5% at 33.7 mV (10 p.e.) and ≤ 0.3% at 337 mV (100 p.e.) with an integrated non-linearity of < 1.6 mV. Developed for the Small-Sized Telescope (SST) and Schwarzschild-Couder Telescope (SCT) cameras of the Cherenkov Telescope Array Observatory (CTAO), CTC and CT5TEA are deployed for both prototypes and shall be integrated into the final versions.

DOI： 10.1016/j.nima.2024.169841

Constraints on VHE gamma-ray emission of flat spectrum radio quasars with the MAGIC telescopes Open Access

Abe, S; Abhir, J; Abhishek, A; Acciari, VA; Aguasca-Cabot, A; Agudo, ; Aniello, T; Ansoldi, S; Antonelli, LA; Engels, AA; Arcaro, C; Artero, M; Asano, K; Babic, A; Baquero, A; de Almeida, UB; Barrio, JA; Batkovic, ; Bautista, A; Baxter, J; González, JB; Bednarek, W; Bernardini, E; Bernete, J; Berti, A; Besenrieder, J; Bigongiari, C; Biland, A; Blanch, O; Bonnoli, G; Bosnjak, Z; Bronzini, E; Burelli, ; Busetto, G; Campoy-Ordaz, A; Carosi, A; Carosi, R; Carretero-Castrillo, M; Castro-Tirado, AJ; Cerasole, D; Ceribella, G; Chai, Y; Cifuentes, A; Colombo, E; Contreras, JL; Cortina, J; Covino, S; D'Amico, G; D'Ammando, F; D'Elia, ; Da Vela, P; Dazzi, F; De Angelis, A; De Lotto, B; de Menezes, R; Del Popolo, A; Delfino, M; Delgado, J; Mendez, CD; Di Pierro, F; Di Tria, R; 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; Fröse, S; Fukami, S; Fukazawa, Y; López, RJG; Garczarczyk, M; Gasparyan, S; Gaug, M; Paiva, JGG; Giglietto, N; Giordano, F; Gliwny, P; Godinovic, N; Gradetzke, T; Grau, R; Green, D; Green, JG; Günther, P; Hadasch, D; Hahn, A; Hassan, T; Heckmann, L; Herrera, J; Hrupec, D; Hutten, M; Imazawa, R; Ishio, K; Martínez, IJ; Jormanainen, J; Kayanoki, T; Kerszberg, D; Kobayashi, Y; Kouch, PM; Kubo, H; Kushida, J; Láinez, M; 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; 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, ; 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; Peresano, M; 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; Silvestri, G; Sitarek, J; Sliusar, ; Sobczynska, D; Spolon, A; Stamerra, A; Striskovic, J; Strom, D; Strzys, M; Suda, Y; Suutarinen, S; Tajima, H; Takahashi, M; Takeishi, R; Temnikov, P; Terauchi, K; Terzic, T; Teshima, M; Truzzi, S; Tutone, A; Ubach, S; van Scherpenberg, J; Acosta, MV; Ventura, S; Viale, ; Vigorito, CF; Vitale, V; Vovk, ; Walter, R; Will, M; Wunderlich, C; Yamamoto, T; Zywucka, N; Ramazani, VF; Buson, S; Ciprini, S

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 535 巻 ( 2 ) 頁： 1484 - 1506 2024年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

Flat spectrum radio quasars (FSRQs) constitute a class of jetted active galaxies characterized by a very luminous accretion disc, prominent and rapidly moving line-emitting cloud structures (broad-line region, BLR), and a surrounding dense dust structure known as dusty torus. The intense radiation field of the accretion disc strongly determines the observational properties of FSRQs. While hundreds of such sources have been detected at GeV energies, only a handful of them exhibit emission in the very-high-energy (VHE, E ≥ 100 GeV) range. This study presents the results and interpretation derived from a cumulative observation period of 174 h dedicated to nine FSRQs conducted with the Major Atmospheric Gamma-ray Imaging Cherenkov telescopes from 2008 to 2020. Our findings indicate no statistically significant (≥5σ) signal for any of the studied sources, resulting in upper limits on the emission within the VHE energy range. In two of the sources, we derived quite stringent constraints on the gamma-ray emission in the form of upper limits. Our analysis focuses on modelling the VHE emission of these two sources in search for hints of absorption signatures within the BLR radiation field. For these particular sources, constraints on the distance between the emission region and the central black hole are derived using a phenomenological model. Subsequently, these constraints are tested using a framework based on a leptonic model.

DOI： 10.1093/mnras/stae2313

Broadband multi-wavelength properties of M87 during the 2018 EHT campaign including a very high energy flaring episode

Algaba J.C., Baloković M., Chandra S., Cheong W.Y., Cui Y.Z., D'Ammando F., Falcone A.D., Ford N.M., Giroletti M., Goddi C., Gurwell M.A., Hada K., Haggard D., Jorstad S., Kaur A., Kawashima T., Kerby S., Kim J.Y., Kino M., Kravchenko E.V., Lee S.S., Lu R.S., Markoff S., Michail J., Neilsen J., Nowak M.A., Principe G., Ramakrishnan V., Ripperda B., Sasada M., Savchenko S.S., Sheridan C., Akiyama K., Alberdi A., Alef W., Anantua R., Asada K., Azulay R., Bach U., Baczko A.K., Ball D., Bandyopadhyay B., Barrett J., Bauböck M., Benson B.A., Bintley D., Lackburn L., Blundell R., Bouman K.L., Bower G.C., Boyce H., Bremer M., Brissenden R., Britzen S., Broderick A.E., Broguiere D., Bronzwaer T., Bustamante S., Carlstrom J.E., Chael A., Chan C.K., Chang D.O., Chatterjee K., Chatterjee S., Chen M.T., Chen Y., Cheng X., Cho I., Christian P., Conroy N.S., Conway J.E., Crawford T.M., Crew G.B., Cruz-Osorio A., Dahale R., Davelaar J., De Laurentis M., Deane R., Dempsey J., Desvignes G., Dexter J., Dhruv V., Dihingia I.K., Doeleman S.S., Dzib S.A., Eatough R.P., Emami R., Falcke H., Farah J., Fish V.L., Fomalont E., Ford H.A., Foschi M., Fraga-Encinas R., Freeman W.T., Friberg P., Fromm C.M., Fuentes A., Galison P., Gammie C.F.

Astronomy and Astrophysics 692 巻 2024年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

Context. The nearby elliptical galaxy M87 contains one of only two supermassive black holes whose emission surrounding the event horizon has been imaged by the Event Horizon Telescope (EHT). In 2018, more than two dozen multi-wavelength (MWL) facilities (from radio to γ-ray energies) took part in the second M87 EHT campaign. Aims. The goal of this extensive MWL campaign was to better understand the physics of the accreting black hole M87∗, the relationship between the inflow and inner jets, and the high-energy particle acceleration. Understanding the complex astrophysics is also a necessary first step towards performing further tests of general relativity. Methods. The MWL campaign took place in April 2018, overlapping with the EHT M87∗ observations. We present a new, contemporaneous spectral energy distribution (SED) ranging from radio to very high-energy (VHE) γ-rays as well as details of the individual observations and light curves. We also conducted phenomenological modelling to investigate the basic source properties. Results. We present the first VHE γ-ray flare from M87 detected since 2010. The flux above 350 GeV more than doubled within a period of ≈36 hours.We find that the X-ray flux is enhanced by about a factor of two compared to 2017, while the radio and millimetre core fluxes are consistent between 2017 and 2018. We detect evidence for a monotonically increasing jet position angle that corresponds to variations in the bright spot of the EHT image. Conclusions. Our results show the value of continued MWL monitoring together with precision imaging for addressing the origins of high-energy particle acceleration. While we cannot currently pinpoint the precise location where such acceleration takes place, the new VHE γ-ray flare already presents a challenge to simple one-zone leptonic emission model approaches, and it emphasises the need for combined image and spectral modelling.

DOI： 10.1051/0004-6361/202450497

A new method of reconstructing images of gamma-ray telescopes applied to the LST-1 of CTAO Open Access

Abe, K; Abe, S; Abhishek, A; Acero, F; Aguasca-Cabot, A; Agudo, I; Alispach, C; Crespo, NA; Ambrosino, D; Antonelli, LA; Aramo, C; Arbet-Engels, A; Arcaro, C; Asano, K; Aubert, P; Baktash, A; Balbo, M; Bamba, A; Larriva, AB; de Almeida, UB; Barrio, JA; Jiménez, LB; Batkovic, I; Baxter, J; González, JB; Bernardini, E; Medrano, JB; Berti, A; Bezshyiko, I; Bhattacharjee, P; Bigongiari, C; Bissaldi, E; Blanch, O; Bonnoli, G; Bordas, P; Borkowski, G; Brunelli, G; Bulgarelli, A; Burelli, I; Burmistrov, L; Buscemi, M; Cardillo, M; Caroff, S; Carosi, A; Carrasco, MS; Cassol, F; Castrejón, N; Cauz, D; Cerasole, D; Ceribella, G; Chai, Y; Cheng, K; Chiavassa, A; Chikawa, M; Chon, G; Chytka, L; Cicciari, GM; Cifuentes, A; Contreras, JL; Cortina, J; Costantini, H; Da Vela, P; Dalchenko, M; Dazzi, F; De Angelis, A; de Lavergne, MD; De Lotto, B; de Menezes, R; Del Burgo, R; Del Peral, L; 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; Eisenberger, L; Elsässer, D; Emery, G; Escudero, J; Ramazani, VF; Ferrarotto, F; Fiasson, A; Foffano, L; Coromina, LF; Fröse, S; Fukazawa, Y; López, RG; Gasbarra, C; Gasparrini, D; Geyer, D; Paiva, JG; Giglietto, N; Giordano, F; Gliwny, P; Godinovic, N; Grau, R; Green, D; Green, J; Gunji, S; Günther, P; Hackfeld, J; Hadasch, D; Hahn, A; Hassan, T; Hayashi, K; Heckmann, L; Heller, M; Llorente, JH; Hirotani, K; Hoffmann, D; Horns, D; Houles, J; Hrabovsky, M; Hrupec, D; Hui, D; Iarlori, M; Imazawa, R; Inada, T; Inome, Y; Inoue, S; Ioka, K; Iori, M; Iuliano, A; Martinez, IJ; Quiles, JJ; Jurysek, J; Kagaya, M; Kalashev, O; Karas, V; Katagiri, H; Kataoka, J; Kerszberg, D; Kobayashi, Y; Kohri, K; Kong, A; Kubo, H; Kushida, J; Lainez, M; Lamanna, G; Lamastra, A; Lemoigne, L; Linhoff, M; Longo, F; López-Coto, R; López-Oramas, A; Loporchio, S; Lorini, A; Bahilo, JL; Luciani, H; Luque-Escamilla, PL; Majumdar, P; Makariev, M; Mallamaci, M; Mandat, D; Manganaro, M; Manicò, G; Mannheim, K; Marchesi, S; Mariotti, M; Marquez, P; Marsella, G; Martí, J; Martinez, O; Martínez, G; Martínez, M; Mas-Aguilar, A; Maurin, G; Mazin, D; Méndez-Gallego, J; Guillen, EM; Micanovic, S; Miceli, D; Miener, T; Miranda, JM; Mirzoyan, R; Mizuno, T; Gonzalez, MM; Molina, E; Montaruli, T; Moralejo, A; Morcuende, D; Morselli, A; Moya, V; Muraishi, H; Nagataki, S; Nakamori, T; Neronov, A; Nickel, L; Rosillo, MN; Nikolic, L; Nishijima, K; Noda, K; Nosek, D; Novotny, V; Nozaki, S; Ohishi, M; Ohtani, Y; Oka, T; Okumura, A; Orito, R; Otero-Santos, J; Ottanelli, P; Owen, E; Palatiello, M; Paneque, D; Pantaleo, FR; Paoletti, R; Paredes, JM; Pech, M; Pecimotika, M; Peresano, M; Pfeifle, F; Pietropaolo, E; Pihet, M; Pirola, G; Plard, C; Podobnik, F; Pons, E; Prandini, E; Priyadarshi, C; Prouza, M; Rainò, S; Rando, R; Rhode, W; Ribó, M; Righi, C; Rizi, V; Fernandez, GR; Frías, MD; Ruina, A; Ruiz-Velasco, E; Saito, T; Sakurai, S; Sanchez, DA; Sano, H; Saric, T; Sato, Y; Saturni, FG; Savchenko, V; Schiavone, F; Schleicher, B; Schmuckermaier, F; Schubert, JL; Schussler, F; Schweizer, T; Arroyo, MS; Siegert, T; Sitarek, J; Sliusar, V; Striskovic, J; Strzys, M; Suda, Y; Tajima, H; Takahashi, H; Takahashi, M; Takata, J; Takeishi, R; Tam, PHT; Tanaka, SJ; Tateishi, D; Tavernier, T; Temnikov, P; Terada, Y; Terauchi, K; Terzic, T; Teshima, M; Tluczykont, M; Tokanai, F; Torres, DF; Travnicek, P; Tutone, A; Vacula, M; Vallania, P; van Scherpenberg, J; Acosta, MV; Ventura, S; Verna, G; Viale, I; Vigliano, A; Vigorito, CF; Visentin, E; Vitale, V; Voitsekhovskyi, V; Voutsinas, G; Vovk, I; Vuillaume, T; Walter, R; Wan, L; Will, M; Wójtowicz, J; Yamamoto, T; Yamazaki, R; Yeung, PKH; Yoshida, T; Yoshikoshi, T; Zhang, W; Zywucka, N

ASTRONOMY & ASTROPHYSICS 691 巻 2024年11月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

Context. Imaging atmospheric Cherenkov telescopes (IACTs) are used to observe very high-energy photons from the ground. Gamma rays are indirectly detected through the Cherenkov light emitted by the air showers they induce. The new generation of experiments, in particular the Cherenkov Telescope Array Observatory (CTAO), sets ambitious goals for discoveries of new gamma-ray sources and precise measurements of the already discovered ones. To achieve these goals, both hardware and data analysis must employ cutting-edge techniques. This also applies to the LST-1, the first IACT built for the CTAO, which is currently taking data on the Canary island of La Palma. Aims. This paper introduces a new event reconstruction technique for IACT data, aiming to improve the image reconstruction quality and the discrimination between the signal and the background from misidentified hadrons and electrons. Methods. The technique models the development of the extensive air shower signal, recorded as a waveform per pixel, seen by CTAO telescopes’ cameras. Model parameters are subsequently passed to random forest regressors and classifiers to extract information on the primary particle. Results. The new reconstruction was applied to simulated data and to data from observations of the Crab Nebula performed by the LST-1. The event reconstruction method presented here shows promising performance improvements. The angular and energy resolution, and the sensitivity, are improved by 10 to 20% over most of the energy range. At low energy, improvements reach up to 22%, 47%, and 50%, respectively. A future extension of the method to stereoscopic analysis for telescope arrays will be the next important step.

DOI： 10.1051/0004-6361/202450889

Standardised formats and open-source analysis tools for the MAGIC telescopes data Open Access

Abe, S; Abhir, J; Abhishek, A; Acciari, VA; Aguasca-Cabot, A; Agudo, I; Aniello, T; Ansoldi, S; Antonelli, LA; Engels, AA; Arcaro, C; Artero, M; Asano, K; Babic, A; de Almeida, UB; Barrio, JA; Batkovic, I; Bautista, A; Baxter, J; González, JB; Bednarek, W; Bernardini, E; Bernete, J; Berti, A; Besenrieder, J; Bigongiari, C; Biland, A; Blanch, O; Bonnoli, G; Bosnjak, Z; Bronzini, E; Burelli, I; Busetto, G; Campoy-Ordaz, A; Carosi, A; Carosi, R; Carretero-Castrillo, M; Castro-Tirado, AJ; Cerasole, D; Ceribella, G; Chai, Y; Cifuentes, A; 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; de Menezes, R; Delfino, M; Delgado, J; Di Pierro, F; Di Tria, R; Di Venere, L; Prester, DD; Donini, A; Dorner, D; Doro, M; Elsaesser, D; Escudero, J; Fariña, L; Fattorini, A; Foffano, L; Font, L; Fröse, S; Fukami, S; Fukazawa, Y; López, RJG; Garczarczyk, M; Gasparyan, S; Gaug, M; Paiva, JGG; Giglietto, N; Giordano, F; Gliwny, P; Gradetzke, T; Grau, R; Green, D; Green, JG; Günther, P; Hadasch, D; Hahn, A; Hassan, T; Heckmann, L; Llorente, JH; Hrupec, D; Hütten, M; Imazawa, R; Ishio, K; Martínez, IJ; Jormanainen, J; Kayanoki, T; Kerszberg, D; Kluge, GW; Kobayashi, Y; Kouch, PM; Kubo, H; Kushida, J; Láinez, M; Lamastra, A; Leone, F; Lindfors, E; 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; 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; Neustroev, V; Nickel, L; Rosillo, MN; Nigro, C; Nikolic, L; Nishijima, K; Ekoume, TN; Noda, K; Nozaki, S; Ohtani, Y; Okumura, A; Otero-Santos, J; Paiano, S; Paneque, D; Paoletti, R; Paredes, JM; Peresano, M; 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; Saturni, FG; Schmidt, K; Schmuckermaier, F; Schubert, JL; Schweizer, T; Sciaccaluga, A; Silvestri, G; 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; Temnikov, P; Terauchi, K; Terzic, T; Teshima, M; Truzzi, S; Tutone, A; Ubach, S; van Scherpenberg, J; Acosta, MV; Ventura, S; Viale, I; Vigorito, CF; Vitale, V; Vovk, I; Walter, R; Will, M; Wunderlich, C; Yamamoto, T; Jouvin, L; Linhoff, L; Linhoff, M

JOURNAL OF HIGH ENERGY ASTROPHYSICS 44 巻頁： 266 - 278 2024年11月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Journal of High Energy Astrophysics

Instruments for gamma-ray astronomy at Very High Energies (E>100GeV) have traditionally derived their scientific results through proprietary data and software. Data standardisation has become a prominent issue in this field both as a requirement for the dissemination of data from the next generation of gamma-ray observatories and as an effective solution to realise public data legacies of current-generation instruments. Specifications for a standardised gamma-ray data format have been proposed as a community effort and have already been successfully adopted by several instruments. We present the first production of standardised data from the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes. We converted 166h of observations from different sources and validated their analysis with the open-source software Gammapy. We consider six data sets representing different scientific and technical analysis cases and compare the results obtained analysing the standardised data with open-source software against those produced with the MAGIC proprietary data and software. Aiming at a systematic production of MAGIC data in this standardised format, we also present the implementation of a database-driven pipeline automatically performing the MAGIC data reduction from the calibrated down to the standardised data level. In all the cases selected for the validation, we obtain results compatible with the MAGIC proprietary software, both for the manual and for the automatic data productions. Part of the validation data set is also made publicly available, thus representing the first large public release of MAGIC data. This effort and this first data release represent a technical milestone toward the realisation of a public MAGIC data legacy.

DOI： 10.1016/j.jheap.2024.09.011

A detailed study of the very high-energy Crab pulsar emission with the LST-1 Open Access

Abe, K; Abe, S; Abhishek, A; Acero, F; 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, ; Baxter, J; Gonzailez, JB; Bernardini, E; Medrano, JB; Berti, A; Bhattacharjee, P; Bigongiari, C; Bissaldi, E; Blanch, O; Bonnoli, G; Bordas, P; Brunelli, G; Bulgarelli, A; Burelli, ; Burmistrov, L; Buscemi, M; Cardillo, M; Caroff, S; Carosi, A; Carrasco, MS; Cassol, F; Castrejón, N; Cauz, D; Cerasole, D; Ceribella, G; Chai, Y; Cheng, K; Chiavassa, A; Chikawa, M; Chon, G; Chytka, L; Cicciari, GM; Cifuentes, A; Contreras, JL; Cortina, J; Costantini, H; Da Vela, P; Dalchenko, M; Dazzi, F; De Angelis, A; de Lavergne, MD; De Lotto, B; de Menezes, R; Del Peral, L; 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; Eisenberger, L; Elsässer, D; Emery, G; Escudero, J; Ramazani, VF; Ferrarotto, F; Fiasson, A; Foffano, L; Coromina, LF; Fröse, S; Fukazawa, Y; López, RG; Gasbarra, C; Gasparrini, D; Gavira, L; Geyer, D; Paiva, JG; Giglietto, N; Giordano, F; Gliwny, P; Godinovic, N; Grau, R; Green, D; Green, J; Gunji, S; Günther, P; Hackfeld, J; Hadasch, D; Hahn, A; Hassan, T; Hayashi, K; Heckmann, L; Heller, M; Llorente, JH; Hirotani, K; Hoffmann, D; Horns, D; Houles, J; Hrabovsky, M; Hrupec, D; Hui, D; Iarlori, M; Imazawa, R; Inada, T; Inome, Y; Ioka, K; Iori, M; Martinez, IJ; Quiles, JJ; Jurysek, J; Kagaya, M; Karas, ; Katagiri, H; Kataoka, J; Kerszberg, D; Kobayashi, Y; Kohri, K; Kong, A; Kubo, H; Kushida, J; Lainez, M; Lamanna, G; Lamastra, A; Lemoigne, L; Linhoff, M; Longo, F; López-Coto, R; López-Moya, M; López-Oramas, A; Loporchio, S; Lorini, A; Bahilo, JL; Luque-Escamilla, PL; Majumdar, P; Makariev, M; Mallamaci, M; Mandat, D; Manganaro, M; Manicò, G; Mannheim, K; Marchesi, S; Mariotti, M; Marquez, P; Marsella, G; Martí, J; Martinez, O; Martínez, G; Martínez, 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; Moralejo, A; Morcuende, D; Morselli, A; Moya, ; Muraishi, H; Nagataki, S; Nakamori, T; Neronov, A; Nickel, L; Rosillo, MN; Nikolic, L; Nishijima, K; Noda, K; Nosek, D; Novotny, ; Nozaki, S; Ohishi, M; Ohtani, Y; Oka, T; Okumura, A; Orito, R; Otero-Santos, J; Ottanelli, P; Owen, E; Palatiello, M; Paneque, D; Pantaleo, FR; Paoletti, R; Paredes, JM; Pech, M; Pecimotika, M; Peresano, M; Pfeiffle, F; Pietropaolo, E; Pihet, M; Pirola, G; Plard, C; Podobnik, F; Pons, E; Prandini, E; Priyadarshi, C; Prouza, M; Rando, R; Rhode, W; Ribó, M; Righi, C; Rizi, ; Fernandez, GR; Frias, MDR; Saito, T; Sakurai, S; Sanchez, DA; Sano, H; Saric, T; Sato, Y; Saturni, FG; Savchenko, ; Schiavone, F; Schleicher, B; Schmuckermaier, F; Schubert, JL; Schussler, F; Schweizer, T; Arroyo, MS; Siegert, T; Silvia, R; Sitarek, J; Sliusar, ; Striskovic, J; Strzys, M; Suda, Y; Tajima, H; Takahashi, H; Takahashi, M; Takata, J; Takeishi, R; Tam, PHT; Tanaka, SJ; Tateishi, D; Tavernier, T; 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; Verna, G; Viale, ; Vigliano, A; Vigorito, CF; Visentin, E; Vitale, V; Voitsekhovskyi, V; Voutsinas, G; Vovk, ; Vuillaume, T; Walter, R; Wan, L; Will, M; Yamamoto, T; Yamazaki, R; Yeung, PKH; Yoshida, T; Yoshikoshi, T; Zhang, W; Zywucka, N

ASTRONOMY & ASTROPHYSICS 690 巻 2024年10月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

Context. To date, three pulsars have been firmly detected by imaging atmospheric Cherenkov telescopes (IACTs). Two of them reached the TeV energy range, challenging models of very high-energy (VHE) emission in pulsars. More precise observations are needed to better characterize pulsar emission at these energies. The LST-1 is the prototype of the large-sized telescopes, which will be part of the Cherenkov Telescope Array Observatory (CTAO). Its improved performance over previous IACTs makes it well suited for studying pulsars. Aims. In this work we study the Crab pulsar emission with the LST-1, improving upon and complementing the results from other telescopes. Crab pulsar observations can also be used to characterize the potential of the LST-1 to study other pulsars and detect new ones. Methods. We analyzed a total of ~103 hours of gamma-ray observations of the Crab pulsar conducted with the LST-1 in the period from September 2020 to January 2023. The observations were carried out at zenith angles of less than 50 degrees. To characterize the Crab pulsar emission over a broader energy range, a new analysis of the Fermi/LAT data, including ~14 years of observations, was also performed. Results. The Crab pulsar phaseogram, long-term light curve, and phase-resolved spectra are reconstructed with the LST-1 from 20 GeV to 450 GeV for the first peak and up to 700 GeV for the second peak The pulsed emission is detected with a significance level of 15.2σ. The two characteristic emission peaks of the Crab pulsar are clearly detected (> 10σ), as is the so-called bridge emission between them (5.7σ). We find that both peaks are described well by power laws, with spectral indices of ~3.44 and ~3.03, respectively. The joint analysis of Fermi/LAT and LST-1 data shows a good agreement between the two instruments in their overlapping energy range. The detailed results obtained from the first observations of the Crab pulsar with the LST-1 show the potential that CTAO will have to study this type of source.

DOI： 10.1051/0004-6361/202450059

Prospects for a survey of the galactic plane with the Cherenkov Telescope Array

Abe, S; Abhir, J; Abhishek, A; Acero, F; Acharyya, A; Adam, R; Aguasca-Cabot, A; Agudo, I; Aguirre-Santaella, A; Alfaro, J; Alvarez-Crespo, N; Batista, RA; Amans, JP; Amato, E; Ambrosi, G; Ambrosino, F; Angüner, EO; Aramo, C; Arcaro, C; Arrabito, L; Asano, K; Ascasíbar, Y; Aschersleben, J; Stuani, LA; Backes, M; Balazs, C; Balbo, M; Ballet, J; Larriva, AB; Martins, VB; de Almeida, UB; Barrio, JA; Batkovic, I; Batzofin, R; Baxter, J; González, JB; Beck, G; Beiske, L; Belmont, R; Benbow, W; Bernardini, E; Bernete, J; Bernlöhr, K; Berti, A; Bertucci, B; Beshley, V; Bhattacharjee, P; Bhattacharyya, S; Bi, B; Biederbeck, N; Biland, A; Bissaldi, E; Biteau, J; Blanch, O; Blazek, J; Bocchino, F; Boisson, C; Bolmont, J; Arbeletche, LB; Bonnoli, G; Bonollo, A; Bordas, P; Bosnjak, Z; Bottacini, E; Braiding, C; Bronzini, E; Brose, R; Brown, AM; Brun, F; Brunelli, G; Bucciantini, N; Bulgarelli, A; Burelli, I; Burmistrov, L; Burton, M; Burtovoi, A; Bylund, T; Calisse, PG; Campoy-Ordaz, A; Cantlay, BK; Caproni, A; Capuzzo-Dolcetta, R; Caraveo, P; Caroff, S; Carosi, A; Carosi, R; Carquin, E; Carrasco, MS; Cascone, E; Cassol, F; Castrejon, N; Castro-Tirado, AJ; Cerasole, D; Cerruti, M; Chadwick, PM; Chambery, P; Chaty, S; Chen, AW; Chernyakova, M; Chiavassa, A; Chytka, L; Cifuentes, A; Araujo, CHC; Conforti, V; Conte, F; Contreras, JL; Cortina, J; Costa, A; Costantini, H; Cotter, G; Crestan, S; Cristofari, P; Cuevas, O; Curtis-Ginsberg, Z; D'Aì, A; D'Amico, G; D'Ammando, F; Dadina, M; Dalchenko, M; David, L; Dazzi, F; de Lavergne, MD; De Caprio, V; Laadim, FD; Dal Pino, EMD; De Lotto, B; De Lucia, M; de Martino, D; de Menezes, R; de Naurois, M; Wilhelmi, ED; de Souza, V; del Peral, L; Giler, AGD; Delgado, C; Dell'aiera, M; Della Valle, M; della Volpe, D; Depaoli, D; Di Girolamo, T; Di Piano, A; Di Pierro, F; Di Tria, R; Di Venere, L; Díaz, C; Diebold, S; Dinesh, A; Djannati-Ataï, A; Djuvsland, J; Domínguez, A; Dominik, RM; Donini, A; Dörner, J; Doro, M; dos Anjos, RDC; Dournaux, JL; Duangchan, C; Dubos, C; Dubus, G; Duffy, S; Dumora, D; Dwarkadas, VV; Ebr, J; Eckner, C; Egberts, K; Einecke, S; Elsässer, D; Emery, G; Errando, M; Escanuela, C; Escarate, P; Godoy, ME; Escudero, J; Esposito, P; Evoli, C; Falceta-Goncalves, D; Fattorini, A; Fegan, S; Feijen, K; Feng, Q; Ferrand, G; Ferrarotto, F; Fiandrini, E; Fiasson, A; Filipovic, M; Fioretti, V; Fiori, M; Flores, H; Foffano, L; Guiteras, LF; Fontaine, G; Fröse, S; Fukazawa, Y; Fukui, Y; Funk, S; Furniss, A; Gaggero, D; Galanti, G; Galaz, G; Gallant, YA; Gallozzi, S; Gammaldi, V; Garczarczyk, M; Gasbarra, C; Gasparrini, D; Gaug, M; Ghalumyan, A; Giarrusso, M; Giesbrecht, J; Giglietto, N; Giordano, F; Giuffrida, R; Giuliani, A; Glicenstein, JF; Glombitza, J; Godinovic, N; Goldoni, P; González, JM; Coelho, JG; Granot, J; Grasso, D; Grau, R; Gréaux, L; Green, D; Green, JG; Greenshaw, T; Grenier, I; Grolleron, G; Grondin, MH; Gueta, O; Gunji, S; Hackfeld, J; Hadasch, D; Hanlon, W; Hara, S; Harvey, VM; Hassan, T; Hayashi, K; Heckmann, L; Heller, M; Hermann, G; Cadena, SH; Hervet, O; Hinton, J; Hiroshima, N; Hnatyk, B; Hnatyk, R; Hofmann, W; Holder, J; Holler, M; Horan, D; Horvath, P; Hovatta, T; Hrabovsky, M; Iarlori, M; Inada, T; Incardona, F; Inoue, S; Iocco, F; Iori, M; Jamrozy, M; Janecek, P; Jankowsky, F; Jarnot, C; Jean, P; Martínez, IJ; Jin, W; Juramy-Gilles, C; Jurysek, J; Kagaya, M; Kalekin, O; Kantzas, D; Karas, V; Katagiri, H; Kataoka, J; Kaufmann, S; Kazanas, D; Kerszberg, D; Khélifi, B; Kieda, DB; Kissmann, R; Kleiner, T; Kluge, G; Kluzniak, W; Knödlseder, J; Kobayashi, Y; Kohri, K; Komin, N; Kornecki, P; Kosack, K; Kostunin, D; Kowal, G; Kubo, H; Kushida, J; La Barbera, A; La Palombara, N; Láinez, M; Lamastra, A; Lapington, J; Laporte, P; Lazarevic, S; Lazendic-Galloway, J; Lemoine-Goumard, M; Lenain, JP; Leone, F; Leto, G; Leuschner, F; Lindfors, E; Linhoff, M; Liodakis, I; Lombardi, S; Longo, F; López-Coto, R; López-Moya, M; López-Oramas, A; Loporchio, S; Bahilo, JL; Lucarelli, F; Luque-Escamilla, PL; Lyard, E; Macias, O; Mackey, J; Maier, G; Malyshev, D; Mandat, D; Manicò, G; Marcowith, A; Marinos, P; Mariotti, M; Markoff, S; Marquez, P; Marsella, G; Martí, J; Martin, P; Martínez, GA; Martínez, M; Martinez, O; Marty, C; Mas-Aguilar, A; Mastropietro, M; Maurin, G; Mazin, D; McKeague, S; Mello, AJTS; Menchiari, S; Mereghetti, S; Mestre, E; Meunier, JL; Meyer, DMA; Miceli, D; Miceli, M; Michailidis, M; Michalowski, J; Miener, T; Miranda, JM; Mitchell, A; Mizuno, T; Moderski, R; Mohrmann, L; Molero, M; Molfese, C; Molina, E; Montaruli, T; Moralejo, A; Morcuende, D; Morik, K; Morlino, G; Morselli, A; Moulin, E; Zamanillo, VM; Mukherjee, R; Munari, K; Murach, T; Muraczewski, A; Muraishi, H; Nagataki, S; Nakamori, T; Nemmen, R; Nickel, L; Niemiec, J; Nieto, D; Rosillo, MN; Nikolajuk, M; Nikolic, L; Noda, K; Nosek, D; Novosyadlyj, B; Novotny, V; Nozaki, S; Ohishi, M; Ohtani, Y; Okumura, A; Olive, JF; Olmi, B; Ong, RA; Orienti, M; Orito, R; Orlandini, M; Orlando, E; Orlando, S; Ostrowski, M; Oya, I; Pagano, I; Pagliaro, A; Palatiello, M; Panebianco, G; Paneque, D; Pantaleo, FR; Paoletti, R; Paredes, JM; Parmiggiani, N; Patel, SR; Patricelli, B; Pavlovic, D; Pech, M; Pecimotika, M; Peresano, M; Pérez-Romero, J; Pérez-Torres, MA; Peron, G; Persic, M; Petrucci, PO; Petruk, O; Piano, G; Pierre, E; Pietropaolo, E; Pihet, M; Pintore, F; Pittori, C; Plard, C; Podobnik, F; Pohl, M; Pons, E; Ponti, G; Prandini, E; Principe, G; Priyadarshi, C; Produit, N; Prokhorov, D; Pueschel, E; Pühlhofer, G; Pumo, ML; Punch, M; Queiroz, F; Quirrenbach, A; Rando, R; Ravel, T; Razzaque, S; Regeard, M; Reichherzer, P; Reimer, A; Reimer, O; Remy, Q; Renaud, M; Reposeur, T; Rhode, W; Ribeiro, D; Ribó, M; Richtler, T; Rico, J; Rieger, F; Rigoselli, M; Rizi, V; Roache, E; Fernandez, GR; Rodríguez-Vázquez, JJ; Romano, P; Romeo, G; Rosado, J; de Leon, AR; Rowell, G; Rudak, B; Ruiter, AJ; Rulten, CB; Russo, F; Sadeh, I; Saha, L; Saito, T; Salzmann, H; Sánchez-Conde, M; Sangiorgi, P; Sano, H; Santander, M; Santangelo, A; Santos-Lima, R; Sapienza, V; Saric, T; Sarkar, S; Saturni, FG; Scherer, A; Schiavone, F; Schipani, P; Schleicher, B; Schovanek, P; Schubert, JL; Schussler, F; Schwanke, U; Schwefer, G; Arroyo, MS; Seitenzahl, I; Sergijenko, O; Servillat, M; Sguera, V; Sharma, P; Siejkowski, H; Siqueira, C; Sizun, P; Sliusar, V; Slowikowska, A; Sol, H; Spencer, ST; Spiga, D; Stamerra, A; Stanic, S; Starling, R; Stawarz, L; Steinmassl, S; Steppa, C; Stolarczyk, T; Suda, Y; Suomijärvi, T; Tajima, H; Takeishi, R; Tanaka, SJ; Tavecchio, F; Tavernier, T; Terada, Y; Terrier, R; Teshima, M; Tian, WW; Tibaldo, L; Tibolla, O; Torradeflot, F; Torres, DF; Tothill, N; Toussenel, F; Touzard, V; Travnicek, P; Tripodo, G; Trois, A; Tsiahina, A; Tutone, A; Umana, G; Vaclavek, L; Vacula, M; Vallania, P; van Eldik, C; Vassiliev, V; Acosta, MLV; Vecchi, M; Ventura, S; Vercellone, S; Verna, G; Viana, A; Viaux, N; Vigliano, A; Vignatti, J; Vigorito, CF; Villanueva, J; Vink, J; Vitale, V; Vodeb, V; Voisin, V; Vorobiov, S; Voutsinas, G; Vovk, I; Vuillaume, T; Waegebaert, V; Wagner, SJ; Walter, R; Wechakama, M; White, R; Wierzcholska, A; Williams, DA; Wohlleben, F; Yamazaki, R; Yang, L; Yoshida, T; Yoshikoshi, T; Zacharias, M; Zaharijas, G; Zampieri, L; Zanin, R; Zavrtanik, D; Zavrtanik, M; Zdziarski, AA; Zech, A; Zhdanov, VI; Zietara, K; Zivec, M; Zuriaga-Puig, J; Luque, PD; Guillemot, L; Smith, DA

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS 2024 巻 ( 10 ) 2024年10月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Journal of Cosmology and Astroparticle Physics

Approximately one hundred sources of very-high-energy (VHE) gamma rays are known in the Milky Way, detected with a combination of targeted observations and surveys. A survey of the entire Galactic Plane in the energy range from a few tens of GeV to a few hundred TeV has been proposed as a Key Science Project for the upcoming Cherenkov Telescope Array Observatory (CTAO). This article presents the status of the studies towards the Galactic Plane Survey (GPS). We build and make publicly available a sky model that combines data from recent observations of known gamma-ray emitters with state-of-the-art physically-driven models of synthetic populations of the three main classes of established Galactic VHE sources (pulsar wind nebulae, young and interacting supernova remnants, and compact binary systems), as well as of interstellar emission from cosmic-ray interactions in the Milky Way. We also perform an optimisation of the observation strategy (pointing pattern and scheduling) based on recent estimations of the instrument performance. We use the improved sky model and observation strategy to simulate GPS data corresponding to a total observation time of 1620 hours spread over ten years. Data are then analysed using the methods and software tools under development for real data. Under our model assumptions and for the realisation considered, we show that the GPS has the potential to increase the number of known Galactic VHE emitters by almost a factor of five. This corresponds to the detection of more than two hundred pulsar wind nebulae and a few tens of supernova remnants at average integral fluxes one order of magnitude lower than in the existing sample above 1 TeV, therefore opening the possibility to perform unprecedented population studies. The GPS also has the potential to provide new VHE detections of binary systems and pulsars, to confirm the existence of a hypothetical population of gamma-ray pulsars with an additional TeV emission component, and to detect bright sources capable of accelerating particles to PeV energies (PeVatrons). Furthermore, the GPS will constitute a pathfinder for deeper follow-up observations of these source classes. Finally, we show that we can extract from GPS data an estimate of the contribution to diffuse emission from unresolved sources, and that there are good prospects of detecting interstellar emission and statistically distinguishing different scenarios. Thus, a survey of the entire Galactic plane carried out from both hemispheres with CTAO will ensure a transformational advance in our knowledge of Galactic VHE source populations and interstellar emission.

DOI： 10.1088/1475-7516/2024/10/081

Prospects for γ-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array Open Access

Abe, K; Abe, S; Acero, F; Acharyya, A; Adam, R; Aguasca-Cabot, A; Agudo, I; Aguirre-Santaella, A; Alfaro, J; Alfaro, R; Alvarez-Crespo, N; Batista, RA; Amans, JP; Amato, E; Angüner, EO; Antonelli, LA; Aramo, C; Araya, M; Arcaro, C; Arrabito, L; Asano, K; Ascasíbar, Y; Aschersleben, J; Ashkar, H; Stuani, LA; Baack, D; Backes, M; Baktash, A; Balazs, C; Balbo, M; Ballester, O; Larriva, AB; Martins, VB; de Almeida, UB; Barrio, JA; Batista, PI; Batkovic, I; Batzofin, R; Baxter, J; González, JB; Beck, G; Tjus, JB; Benbow, W; Medrano, JB; Bernlöhr, K; Berti, A; Bertucci, B; Beshley, V; Bhattacharjee, P; Bhattacharyya, S; Bi, B; Biederbeck, N; Biland, A; Bissaldi, E; Biteau, J; Blanch, O; Blazek, J; Boisson, C; Bolmont, J; Bordas, P; Bosnjak, Z; Bottacini, E; Bradascio, F; Braiding, C; Bronzini, E; Brose, R; Brown, AM; Brun, F; Brunetti, G; Bucciantini, N; Bulgarelli, A; Burelli, I; Burmistrov, L; Burton, M; Bylund, T; Calisse, PG; Campoy-Ordaz, A; Cantlay, BK; Capalbi, M; Caproni, A; Capuzzo-Dolcetta, R; Caraveo, P; Caroff, S; Carosi, R; Carquin, E; Carrasco, MS; Cascone, E; Cassol, F; Castro-Tirado, AJ; Cerasole, D; Cerruti, M; Chadwick, P; Chaty, S; Chen, AW; Chernyakova, M; Chiavassa, A; Chudoba, J; Chytka, L; Cifuentes, A; Araujo, CHC; Conforti, V; Conte, F; Contreras, JL; Cortina, J; Costa, A; Costantini, H; Cotter, G; Cristofari, P; Cuevas, O; Curtis-Ginsberg, Z; D'Amico, G; D'Ammando, F; Dalchenko, M; Dazzi, F; de Lavergne, MD; De Caprio, V; Laadim, FDF; Dal Pino, EMD; De Lotto, B; De Lucia, M; De Martino, D; De Menezes, R; de Naurois, M; De Simone, N; De Souza, V; del Valle, MV; Delagnes, E; Giler, AGD; Delgado, C; Dell'aiera, M; della Volpe, D; Depaoli, D; Di Girolamo, T; Di Piano, A; Di Pierro, F; Di Tria, R; Di Venere, L; Diebold, S; Djannati-Ataï, A; Djuvsland, J; Dominik, RM; Donini, A; Dorner, D; Dörner, J; Doro, M; dos Anjos, RDC; Dournaux, JL; Duangchan, C; Dubos, C; Dumora, D; Dwarkadas, VV; Ebr, J; Eckner, C; Egberts, K; Einecke, S; Elsässer, D; Emery, G; Godoy, ME; Escudero, J; Esposito, P; Ettori, S; Evoli, C; Falceta-Goncalves, D; Ramazani, VF; Fattorini, A; Faure, A; Fedorova, E; Fegan, S; Feijen, K; Feng, Q; Ferrand, G; Ferrarotto, F; Fiandrini, E; Fiasson, A; Filipovic, M; Fioretti, V; Foffano, L; Guiteras, LF; Fontaine, G; Fröse, S; Fukazawa, Y; Fukui, Y; Gaggero, D; Galanti, G; Gallozzi, S; Gammaldi, V; Garczarczyk, M; Gasbarra, C; Gasparrini, D; Gaug, M; Ghalumyan, A; Gianotti, F; Giarrusso, M; Giesbrecht, J; Giglietto, N; Giordano, F; Glicenstein, JF; Göksu, H; Goldoni, P; González, JM; González, MM; Coelho, JG; Granot, J; Grau, R; Gréaux, L; Green, D; Green, JG; Grenier, I; Grolleron, G; Grube, J; Gueta, O; Hackfeld, J; Hadasch, D; Hamal, P; Hanlon, W; Hara, S; Harvey, VM; Hassan, T; Heckmann, L; Heller, M; Cadena, SH; Hervet, O; Hie, J; Hiroshima, N; Hnatyk, B; Hnatyk, R; Hoang, J; Hoffmann, D; Hofmann, W; Holder, J; Horan, D; Horvath, P; Hrupec, D; Hütten, M; Iarlori, M; Inada, T; Incardona, F; Inoue, S; Iocco, F; Iori, M; Jamrozy, M; Janecek, P; Jankowsky, F; Jarnot, C; Jean, P; Martínez, IJ; Jin, W; Juramy-Gilles, C; Jurysek, J; Kagaya, M; Kantzas, D; Karas, V; Katagiri, H; Kataoka, J; Kaufmann, S; Kerszberg, D; Khélifi, B; Kissmann, R; Kleiner, T; Kluge, G; Kluzniak, W; Knödlseder, J; Kobayashi, Y; Kohri, K; Komin, N; Kornecki, P; Kosack, K; Kowal, G; Kubo, H; Kushida, J; La Barbera, A; La Palombara, N; Láinez, M; Lamastra, A; Lapington, J; Laporte, P; Lazarevic, S; Leitgeb, F; Lemoine-Goumard, M; Lenain, JP; Leone, F; Leto, G; Leuschner, F; Lindfors, E; Linhoff, M; Liodakis, I; Lombardi, S; Longo, F; López-Coto, R; López-Moya, M; López-Oramas, A; Loporchio, S; Luque-Escamilla, PL; Macias, O; Mackey, J; Majumdar, P; Malyshev, D; Mandat, D; Manganaro, M; Manicò, G; Mariotti, M; Markoff, S; Márquez, I; Marquez, P; Marsella, G; Martínez, GA; Martínez, M; Martinez, O; Marty, C; Mas-Aguilar, A; Mastropietro, M; Maurin, G; Mazin, D; Melkumyan, D; Mello, AJTS; Meunier, JL; Meyer, DMA; Meyer, M; Miceli, D; Michailidis, M; Michalowski, J; Miener, T; Miranda, JM; Mitchell, A; Mizote, M; Mizuno, T; Moderski, R; Molero, M; Molfese, C; Molina, E; Montaruli, T; Morcuende, D; Morik, K; Morlino, G; Morselli, A; Moulin, E; Zamanillo, VM; Munari, K; Murach, T; Muraczewski, A; Muraishi, H; Nagataki, S; Nakamori, T; Nemmen, R; Neyroud, N; Nickel, L; Niemiec, J; Nieto, D; Rosillo, MN; Nikolajuk, M; Nishijima, K; Noda, K; Nosek, D; Novotny, V; Nozaki, S; O'Brien, P; Ohishi, M; Ohtani, Y; Okumura, A; Olive, JF; Olmi, B; Ong, RA; Orienti, M; Orito, R; Orlandini, M; Orlando, E; Ostrowski, M; Oya, I; Pagliaro, A; Palatiello, M; Panebianco, G; Paneque, D; Pantaleo, FR; Paoletti, R; Paredes, JM; Parmiggiani, N; Patel, SR; Patricelli, B; Pavlovic, D; Pech, M; Pecimotika, M; Pensec, U; Peresano, M; Pérez-Romero, J; Peron, G; Persic, M; Petrucci, PO; Petruk, O; Piano, G; Pierre, E; Pietropaolo, E; Pintore, F; Pirola, G; Pita, S; Plard, C; Podobnik, F; Pohl, M; Polo, M; Pons, E; Ponti, G; Prandini, E; Prast, J; Principe, G; Priyadarshi, C; Produit, N; Pueschel, E; Pühlhofer, G; Pumo, ML; Punch, M; Queiroz, F; Quirrenbach, A; Rainò, S; Rando, R; Razzaque, S; Recchia, S; Regeard, M; Reichherzer, P; Reimer, A; Reimer, O; Reisenegger, A; Rhode, W; Ribeiro, D; Ribó, M; Richtler, T; Rico, J; Rieger, F; Righi, C; Riitano, L; Rizi, V; Roache, E; Fernandez, GR; Rodríguez-Vázquez, JJ; Romano, P; Romeo, G; Rosado, J; de Leon, AR; Rowell, G; Rudak, B; Rulten, CB; Russo, F; Sadeh, I; Saha, L; Saito, T; Salzmann, H; Sanchez, D; Sánchez-Conde, M; Sangiorgi, P; Sano, H; Santander, M; Santangelo, A; Santos-Lima, R; Sanuy, A; Saric, T; Sarkar, A; Sarkar, S; Satalecka, K; Saturni, FG; Savchenko, V; Scherer, A; Schipani, P; Schleicher, B; Schubert, JL; Schussler, F; Schwanke, U; Schwefer, G; Arroyo, MS; Seiji, S; Semikoz, D; Sergijenko, O; Servillat, M; Sguera, V; Shang, RY; Sharma, P; Siejkowski, H; Sinha, A; Siqueira, C; Sliusar, V; Slowikowska, A; Sol, H; Specovius, A; Spencer, ST; Spiga, D; Stamerra, A; Stanic, S; Starecki, T; Starling, R; Stawarz, L; Steppa, C; Stolarczyk, T; Striskovic, J; Suda, Y; Suomijärvi, T; Tajima, H; Tak, D; Takahashi, M; Takeishi, R; Tanaka, SJ; Tavernier, T; Tejedor, LA; Terauchi, K; Terrier, R; Teshima, M; Tian, WW; Tibaldo, L; Tibolla, O; Torradeflot, F; Torres, DF; Torresi, E; Tosti, G; Tosti, L; Tothill, N; Toussenel, F; Touzard, V; Tramacere, A; Travnicek, P; Tripodo, G; Truzzi, S; Tsiahina, A; Tutone, A; Vacula, M; Vallage, B; Vallania, P; van Eldik, C; van Scherpenberg, J; Vandenbroucke, J; Vassiliev, V; Acosta, MV; Vecchi, M; Ventura, S; Vercellone, S; Verna, G; Viana, A; Viaux, N; Vigliano, A; Vigorito, CF; Vitale, V; Vodeb, V; Voisin, V; Vorobiov, S; Voutsinas, G; Vovk, I; Vuillaume, T; Wagner, SJ; Walter, R; Wechakama, M; White, R; Wierzcholska, A; Will, M; Williams, DA; Wohlleben, F; Wolter, A; Yamamoto, T; Yamazaki, R; Yoshida, T; Yoshikoshi, T; Zacharias, M; Zaharijas, G; Zavrtanik, D; Zavrtanik, M; Zdziarski, AA; Zech, A; Zhdanov, VI; Zivec, M; Zuriaga-Puig, J; Luque, PD

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS 2024 巻 ( 10 ) 2024年10月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Journal of Cosmology and Astroparticle Physics

Galaxy clusters are expected to be both dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster’s formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at γ-ray energies and are predicted to be sources of large-scale γ-ray emission due to hadronic interactions in the intracluster medium (ICM). In this paper, we estimate the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse γ-ray emission from the Perseus galaxy cluster. We first perform a detailed spatial and spectral modelling of the expected signal for both the DM and the CRp components. For each case, we compute the expected CTA sensitivity accounting for the CTA instrument response functions. The CTA observing strategy of the Perseus cluster is also discussed. In the absence of a diffuse signal (non-detection), CTA should constrain the CRp to thermal energy ratio X500 within the characteristic radius R500 down to about X500 < 3 × 10−3, for a spatial CRp distribution that follows the thermal gas and a CRp spectral index αCRp = 2.3. Under the optimistic assumption of a pure hadronic origin of the Perseus radio mini-halo and depending on the assumed magnetic field profile, CTA should measure αCRp down to about ∆αCRp ≃ 0.1 and the CRp spatial distribution with 10% precision, respectively. Regarding DM, CTA should improve the current ground-based γ-ray DM limits from clusters observations on the velocity-averaged annihilation cross-section by a factor of up to ∼ 5, depending on the modelling of DM halo substructure. In the case of decay of DM particles, CTA will explore a new region of the parameter space, reaching models with τχ > 1027 s for DM masses above 1 TeV. These constraints will provide unprecedented sensitivity to the physics of both CRp acceleration and transport at cluster scale and to TeV DM particle models, especially in the decay scenario.

DOI： 10.1088/1475-7516/2024/10/004

A survey to evaluate diversity, equity and inclusion in large collaborations

van Scherpenberg J., Heckmann L., Strišković J., Berti A., Dorner D., Elsaesser D., Green J., Manganaro M., Satalecka K., 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., Barrio J.A., Batković I., Baxter J., Becerra González J., Bednarek W., Bernardini E., Bernardos M., Bernete J., 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., Ceribella G., Chai Y., Chilingarian A., 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., Doro M., Emery G., Escudero J., Fariña L., Fattorini A., Foffano L., Font L., Fröse S., 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., Herrera J., Hrupec D., Hütten M., Imazawa R.

Proceedings of Science 444 巻 2024年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Proceedings of Science

In 2020, the MAGIC collaboration started an initiative to improve diversity, equity and inclusion (DEI) in the collaboration. One of the major actions undertaken by this initiative was a survey which was distributed among all MAGIC members with the goal of getting a clear picture of the status quo and to identify potential problems or opportunities concerning DEI related topics. Two surveys have since been performed - one in December 2020 and one in June 2022 - covering questions related to demographics, working conditions, recognition, harassment, bullying and discrimination. In this contribution, we present the questionnaire and strategy used to run these surveys. Additionally, we describe the impact the survey had within the collaboration and which actions have been taken as a direct consequence of the survey results.

Development of a blue-mirror multilayer coating on light concentrators for future SiPM cameras

Okumura A., Haga J., Inoue C., Nishimoto K., Furuta K., Tajima H.

Proceedings of Science 444 巻 2024年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Proceedings of Science

Silicon photomultipliers (SiPMs) have a few advantages over conventional photomultiplier tubes (PMTs) used in imaging atmospheric Cherenkov telescopes. The first notable characteristic is their higher photon detection efficiency (PDE) of up to about 60%, which is roughly 1.2–1.5 times better than that of PMTs in the 300–450 nm range, enabling us to lower the energy threshold of gamma-ray observations and increase the photon statistics. The second advantage is that SiPMs are chemically stable after exposure to long and bright illumination, while PMTs can cause gain and quantum efficiency degradation after the same exposure. Therefore, the use of SiPMs under bright or full moon conditions may extend the total observation time in the highest energy coverage region of individual telescopes. However, the SiPM PDE is too high in wavelengths longer than 500 nm; hence, the signal-to-noise ratio (S/N) of the Cherenkov signal over the night-sky background (NSB) is not necessarily superb. This is because the Cherenkov signal is dominant over the wavelength of 300–500 nm, while the NSB is brighter in the region of 550 nm or longer. To improve the S/N with minimal and cost-effective additional hardware, we have developed multilayer coating designs with only 8 layers and applied them to the specular surfaces of light concentrators. The layers were designed to reflect more photons in the 300–500 nm range but fewer in 550–800 nm. Using a prototype light concentrator fabricated with the novel multilayer design, we demonstrated that a SiPM array exhibits ∼50% better photon collection efficiency at 403 nm than that obtained with PMTs, agreeing with the result of a ray-tracing simulation. The efficiency measured at 830 nm was also successfully reduced by 30–50%.

Detection of the 2021 Outburst of RS Ophiuchi with the LST-1

Kobayashi Y., Aguasca-Cabot A., Bernardos Martín M.I., Green D., López-Coto R., Abe K., Abe S., Agudo I., Alvarez Crespo N., Antonelli L.A., Aramo C., Arbet-Engels A., Arcaro C., Artero M., Asano K., Aubert P., Baktash A., Bamba A., Baquero Larriva A., Baroncelli L., Barres de Almeida U., Barrio J.A., Batkovic I., Baxter J., Becerra González J., Bernardini E., Bernardos M.I., Bernete Medrano J., Berti A., Bhattacharjee P., Biederbeck N., Bigongiari C., Bissaldi E., Blanch O., Bonnoli G., Bordas P., Bulgarelli A., Burelli I., Burmistrov L., Buscemi M., Cardillo M., Caroff S., Carosi A., Carrasco M.S., Cassol F., Cauz D., Cerasole D., Ceribella G., Chai Y., Cheng K., Chiavassa A., Chikawa M., Chytka L., Cifuentes A., Contreras J.L., Cortina J., Costantini H., Dalchenko M., Dazzi F., De Angelis A., de Bony de Lavergne M., De Lotto B., De Lucia M., de Menezes R., Del Peral L., Deleglise G., Delgado C., Delgado Mengual J., della Volpe D., Dellaiera M., Di Piano A., Di Pierro F., Di Pilato A., Di Tria R., Di Venere L., Díaz C., Dominik R.M., Dominis Prester D., Donini A., Dorner D., Doro M., Eisenberger L., Elsässer D., Emery G., Escudero J., Fallah Ramazani V., Ferrara G., Ferrarotto F., Fiasson A., Foffano L., Freixas Coromina L., Fröse S., Fukami S., Fukazawa Y., Garcia E., Garcia López R., Gasbarra C., Gasparrini D., Geyer D.

Proceedings of Science 444 巻 2024年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Proceedings of Science

Novae are luminous explosions in close binaries which host a white dwarf and a companion donor star. They are triggered by a thermonuclear runaway when the white dwarf accretes a critical amount of matter from the secondary. Though novae are established as high-energy gamma-ray emitters through observations by the Fermi Large Area Telescope (LAT), the origin of the gamma-ray emission, whether it is hadronic or leptonic, had been under intense debate until very recently. RS Ophiuchi (RS Oph) is a well-known recurrent symbiotic nova with a recurrence time scale of 15 years. The most recent outburst of RS Oph in 2021 brought the first detection of very-high-energy (VHE) gamma rays from a nova ever. The first Large-Sized Telescope prototype (LST-1) of the Cherenkov Telescope Array observed this historic event along with H.E.S.S. and MAGIC. The LST-1 observations in the first days after the burst onset show a clear VHE gamma-ray signal from RS Oph. The low energy threshold of LST-1 allows us to reconstruct the RS Oph gamma-ray spectrum down to ∼30 GeV, providing the best connection of the VHE gamma-ray data to the Fermi LAT energy range. The results from the analysis of the LST-1 observations are consistent with those obtained with H.E.S.S. and MAGIC, and also support a hadronic origin for the observed gamma-ray fluxes. In this contribution, we will present the analysis results of the LST-1 observations of the 2021 outburst of RS Oph.

Detecting and characterizing pulsar halos with the Cherenkov Telescope Array Observatory

Eckner C., Abe K., Abe S., Acharyya A., Adam R., Aguasca-Cabot A., Agudo I., Alfaro J., Alvarez-Crespo N., Alves Batista R., Amans J.P., Amato E., Ambrosino F., Angüner E.O., Antonelli L.A., Aramo C., Arcaro C., Arrabito L., Asano K., Aschersleben J., Ashkar H., Augusto Stuani L., Baack D., Backes M., Balazs C., Balbo M., Baquero Larriva A., Barbosa Martins V., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Batzofin R., Baxter J., Beck G., Becker Tjus J., Beiske L., Belardinelli D., Benbow W., Bernardini E., Bernete Medrano J., Bernlöhr K., Berti A., Beshley V., Bhattacharjee P., Bhattacharyya S., Bi B., Biederbeck N., Biland A., Bissaldi E., Blanch O., Blazek J., Boisson C., Bolmont J., Bonnoli G., Bordas P., Bosnjak Z., Bradascio F., Braiding C., Bronzini E., Brose R., Brown A.M., Brun F., Brunelli G., Bulgarelli A., Burelli I., Burmistrov L., Burton M., Bylund T., Calisse P.G., Campoy-Ordaz A., Cantlay B.K., Capalbi M., Caproni A., Capuzzo-Dolcetta R., Carlile C., Caroff S., Carosi A., Carosi R., Carrasco M.S., Cascone E., Cassol F., Castrejon N., Catalani F., Cerasole D., Cerruti M., Chaty S., Chen A.W., Chernyakova M., Chiavassa A., Chudoba J., Coimbra Araujo C.H., Conforti V., Conte F., Contreras J.L., Cossou C., Costa A., Costantini H., Cristofari P.

Proceedings of Science 444 巻 2024年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Proceedings of Science

The recently identified source class of pulsar halos may be populated and bright enough at TeV energies to constitute a large fraction of the sources that will be observed with the Cherenkov Telescope Array (CTA), especially in the context of the planned Galactic Plane Survey (GPS). In this study, we examine the prospects offered by CTA for the detection and characterization of such objects. CTA will cover energies from 20 GeV to 300 TeV, bridging the ranges already probed with the Fermi Large Area Telescope and High Altitude Water Cherenkov Observatory, and will also have a better angular resolution than the latter instruments, thus providing a complementary look at the phenomenon. From simple models for individual pulsar halos and their population in the Milky Way, we examine under which conditions such sources can be detected and studied from the GPS observations. In the framework of a full spatial-spectral likelihood analysis, using the most recent estimates for the instrument response function and prototypes for the science tools, we derive the spectral and morphological sensitivity of the CTA GPS to the specific intensity distribution of pulsar halos. From these, we quantify the physical parameters for which pulsar halos can be detected, identified, and characterized, and what fraction of the Galactic population could be accessible. We also discuss the effect of interstellar emission and data analysis systematics on these prospects.

Defining the data legacy of the MAGIC telescopes: adopting a standardised data format and open-source analysis tools

Nigro C., 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., Barrio J.A., Batković I., Baxter J., Becerra González J., Bednarek W., Bernardini E., Bernardos M., 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., Ceribella G., Chai Y., Chilingarian A., 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., Fröse S., 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.

Proceedings of Science 444 巻 2024年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Proceedings of Science

Very-high-energy (VHE, E > 100 GeV) gamma-ray telescopes have traditionally conducted science with proprietary data and software. After two decades of operations, they have accumulated thousands of hours of observations whose full scientific exploitation cannot be accomplished by the restricted group of scientists operating these instruments. The advent of a new generation of open gamma-ray observatories and, at the same time, the forthcoming end of their scientific operations, call for the realisation of public archives of their observations. With the objective to facilitate the exchange and dissemination of data from current- and next-generation gamma-ray instruments, the "Data formats for gamma-ray astronomy" (GADF) initiative was formed to provide an open and standardised format for gamma-ray astronomical data. In this contribution, we present the effort to produce data of the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes in this standardised format. A total of 150 hours of observations of different sources were converted to the GADF format and then validated by analysing them with the open-source software Gammapy and comparing the results obtained against those produced with the MAGIC proprietary software, MARS. The effort to standardise and validate the MAGIC data in an open and shared format constitute the first fundamental milestone towards the realisation of its public data legacy.

Dark matter searches in dwarf spheroidal galaxies with the Cherenkov Telescope Array

Saturni F.G., Doro M., Morselli A., Rodríguez-Fernández G., Abe K., Abe S., Acharyya A., Adam R., Aguasca-Cabot A., Agudo I., Alfaro J., Alvarez-Crespo N., Alves Batista R., Amans J.P., Amato E., Ambrosino F., Angüner E.O., Antonelli L.A., Aramo C., Arcaro C., Arrabito L., Asano K., Aschersleben J., Ashkar H., Augusto Stuani L., Baack D., Backes M., Balazs C., Balbo M., Baquero Larriva A., Barbosa Martins V., Barres de Almeida U., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Batzofin R., Baxter J., Beck G., Becker Tjus J., Beiske L., Belardinelli D., Benbow W., Bernardini E., Bernete Medrano J., Bernlöhr K., Berti A., Beshley V., Bhattacharjee P., Bhattacharyya S., Bi B., Biederbeck N., Biland A., Bissaldi E., Blanch O., Blazek J., Boisson C., Bolmont J., Bonnoli G., Bordas P., Bosnjak Z., Bradascio F., Braiding C., Bronzini E., Brose R., Brown A.M., Brun F., Brunelli G., Bulgarelli A., Burelli I., Burmistrov L., Burton M., Bylund T., Calisse P.G., Campoy-Ordaz A., Cantlay B.K., Capalbi M., Caproni A., Capuzzo-Dolcetta R., Carlile C., Caroff S., Carosi A., Carosi R., Carrasco M.S., Cascone E., Cassol F., Castrejon N., Catalani F., Cerasole D., Cerruti M., Chaty S., Chen A.W., Chernyakova M., Chiavassa A., Chudoba J., Coimbra Araujo C.H., Conforti V., Conte F., Contreras J.L., Cossou C.

Proceedings of Science 444 巻 2024年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Proceedings of Science

Dark matter (DM) is one of the major components in the Universe. However, at present its existence is still only inferred through indirect astronomical observations. DM particles can annihilate or decay, producing final-state Standard Model pairs that subsequently annihilate into high-energy γrays. The dwarf spheroidal galaxies (dSphs) in the Milky Way DM halo have long been considered optimal targets to search for annihilating DM signatures in GeV-to-TeV γ-ray spectra due to their high DM densities (hence high astrophysical factors), as well as the expected absence of intrinsic γ-ray emission of astrophysical origin. For such targets, it is important to compute the amount of DM in their halos in a consistent way to optimize the γ-ray data analysis. Such estimates directly affect the observability of DM signals in dSphs, as well as the DM constraints that can be derived in case of null detection. In this contribution, we present the results on the sensitivity of the Cherenkov Telescope Array (CTA) for DM annihilation and decay searches using planned observations of the Milky Way dSphs. We select the most promising targets among all presently known dwarf satellites, providing new determinations of their expected DM signal. This study shows an improvement of approximately an order of magnitude in sensitivity compared to current searches in similar targets. We also discuss the results in terms of cuspy and cored DM models, and investigate the sensitivity obtained by the combination of observations from different dSphs. Finally, we explore the optimal strategies for CTA observations of dSphs.

Ctapipe - Prototype Open Event Reconstruction Pipeline for the Cherenkov Telescope Array

Linhoff M., Beiske L., Biederbeck N., Fröse S., Kosack K., Nickel L., Abe K., Abe S., Acharyya A., Adam R., Aguasca-Cabot A., Agudo I., Alfaro J., Alvarez-Crespo N., Alves Batista R., Amans J.P., Amato E., Ambrosino F., Angüner E.O., Antonelli L.A., Aramo C., Arcaro C., Arrabito L., Asano K., Aschersleben J., Ashkar H., Augusto Stuani L., Baack D., Backes M., Balazs C., Balbo M., Baquero Larriva A., Barbosa Martins V., de Almeida U.B., Barrio J.A., Bastieri D., Batista P.I., Batkovic I., Batzofin R., Baxter J., Beck G., Becker Tjus J., Belardinelli D., Benbow W., Bernardini E., Bernete Medrano J., Bernlöhr K., Berti A., Beshley V., Bhattacharjee P., Bhattacharyya S., Bi B., Biland A., Bissaldi E., Blanch O., Blazek J., Boisson C., Bolmont J., Bonnoli G., Bordas P., Bosnjak Z., Bradascio F., Braiding C., Bronzini E., Brose R., Brown A.M., Brun F., Brunelli G., Bulgarelli A., Burelli I., Burmistrov L., Burton M., Bylund T., Calisse P.G., Campoy-Ordaz A., Cantlay B.K., Capalbi M., Caproni A., Capuzzo-Dolcetta R., Carlile C., Caroff S., Carosi A., Carosi R., Carrasco M.S., Cascone E., Cassol F., Castrejon N., Catalani F., Cerasole D., Cerruti M., Chaty S., Chen A.W., Chernyakova M., Chiavassa A., Chudoba J., Coimbra Araujo C.H., Conforti V., Conte F.

Proceedings of Science 444 巻 2024年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Proceedings of Science

The Cherenkov Telescope Array Observatory (CTAO) is the next-generation ground-based 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. CTAO will also be the first open ground-based gamma-ray observatory. Accordingly, the CTAO data processing pipeline is developed as open-source software and ctapipe will be a core package therein. 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 air shower and providing the corresponding instrument response functions. ctapipe is a python framework providing algorithms and command-line tools to facilitate raw data calibration, image extraction, image parametrization and event reconstruction. Its current main focus is the analysis of simulated data but it has also been successfully applied for the analysis of data obtained with the CTA prototype telescopes, and first science results have now been obtained by the LST-1 collaboration using ctapipe. A plugin system also allows the processing of nonCTA data. Recent updates, including event reconstruction using machine learning and a new plugin system as well as the roadmap towards a 1.0 release will be presented.

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