Papers - TAJIMA, Hiroyasu

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

Acero F., Acharyya A., Adam R., Aguasca-Cabot A., Agudo I., Aguirre-Santaella A., Alfaro J., Aloisio R., Crespo N.Á., Batista R.A., Amati L., Amato E., Ambrosi G., Angüner E.O., Aramo C., Arcaro C., Armstrong T., Asano K., Ascasibar Y., Aschersleben J., Backes M., Baktash A., Balazs C., Balbo M., Ballet J., Larriva A.B., Martins V.B., de Almeida U.B., Barrio J.A., Bastieri D., Baxter J.R., Tjus J.B., Benbow W., Bernardos-Martín M.I., 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 R.A.C., 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 J.L., Costa A., Costantini H., Cristofari P., Crocker R., D'Amico G., D'Ammando F., De Angelis A., De Caprio V., de Gouveia Dal Pino E.M., de Ona Wilhelmi E., de Souza V., Delgado C., della Volpe D., Depaoli D., Di Girolamo T., Di Pierro F., Di Tria R., Di Venere L., Diebold S., Djuvsland J.I., Donini A., Doro M., Dos Anjos R.D.C., Dwarkadas V.V., Einecke S., Elsässer D., Emery G., Evoli C., Falceta-Goncalves D., Fedorova E., Fegan S.

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

Scopus

Multimessenger Characterization of Markarian 501 during Historically Low X-Ray and γ-Ray Activity Reviewed International coauthorship

Abe, H. et al.

  Vol. 266 ( 2 ) page： 37   2023.6

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DOI： 10.3847/1538-4365/acc181

AstroPix: CMOS pixels in space Reviewed

Steinhebel A.L., Caputo R., Fleischhack H., Striebig N., Jadhav M., Suda Y., Luz R., Violette D., Kierans C., Tajima H., Fukazawa Y., Leys R., Perić I., Metcalfe J., Negro M., Perkins J.S.

Proceedings of Science   Vol. 420   2023.5

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Space-based gamma-ray telescopes such as the Fermi Large Area Telescope have used single sided silicon strip detectors to measure the position of charged particles produced by incident gamma rays with high resolution. At energies in the Compton regime and below, two dimensional position information within a single detector is required. Double sided silicon strip detectors are one option; however, this technology is difficult to fabricate and large arrays are susceptible to noise. This work outlines the development and implementation of monolithic CMOS active pixel silicon sensors, AstroPix, for use in future gamma-ray telescopes. Based upon detectors designed using the HVCMOS process at the Karlsruhe Institute of Technology, AstroPix has the potential to maintain the high energy and angular resolution required of a medium-energy gamma-ray telescope while reducing noise with the dual detection-and-readout capabilities of a CMOS chip. The status of AstroPix development and testing as well as outlook for application in future telescopes is presented.

Scopus

Multiwavelength study of the galactic PeVatron candidate LHAASO J2108+5157 Reviewed International coauthorship

Abe, S. et al.

Astronomy & Astrophysics   Vol. 673   page： A75   2023.5

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DOI： 10.1051/0004-6361/202245086

The Fermi-LAT Lightcurve Repository Reviewed International coauthorship

Abdollahi, S. et al.

The Astrophysical Journal Supplement Series   Vol. 265 ( 2 ) page： 31   2023.4

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DOI： 10.3847/1538-4365/acbb6a

Studies of propagation mechanism of optical crosstalk in silicon photomultipliers Reviewed

Tajima H., Okumura A., Furuta K.

Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment   Vol. 1049   2023.4

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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  

Silicon photomultipliers (SiPMs) are now replacing photomultiplier tubes where low voltage operations, compactness, and cost per channel are important. However, optical crosstalk (OCT) is still one of the major disadvantages of SiPMs since it increases accidental triggers and degrades the accuracy of photon counting. Previously, we reported that OCTs can be suppressed by either thicker or no protection resin coating. Although no resin coating heavily suppresses OCTs, we still observe some OCTs at a few % levels. In this study, we have investigated the properties of OCTs and delayed OCTs for several types of SiPMs with different device sizes, cell sizes, and resin coating thickness. We observe that delayed OCTs have very similar properties compared with OCTs with no resin coating. Furthermore, we find that the sizable amount of delayed OCTs is overlapping with the original pulse and may be treated as OCTs when the delay is less than 8 ns in our analysis. Since the properties and rate of overlaps of delayed OCTs match those of OCTs with no resin coating, we conclude that the remaining OCTs for SiPMs with no coating can be fully explained by overlaps of delayed OCTs.

DOI： 10.1016/j.nima.2023.168029

Scopus

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

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

Scopus

The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope: Data Release 3 Reviewed

Ajello M., Baldini L., Ballet J., Bastieri D., Gonzalez J. Becerra, Bellazzini R., Berretta A., Bissaldi E., Bonino R., Brill A., Bruel P., Buson S., Caputo R., Caraveo P. A., Cheung C. C., Chiaro G., Cibrario N., Ciprini S., Crnogorcevic M., Cutini S., D'Ammando F., De Gaetano S., Di Lalla N., Di Venere L., Dominguez A., Ramazani V. Fallah, Ferrara E. C., Fiori A., Fukazawa Y., Funk S., Fusco P., Gammaldi V, Gargano F., Garrappa S., Gasparrini D., Giglietto N., Giordano F., Giroletti M., Green D., Grenier I. A., Guiriec S., Horan D., Hou X., Kayanoki T., Kuss M., Larsson S., Latronico L., Lewis T., Li J., Liodakis I, Longo F., Loparco F., Lott B., Lovellette M. N., Lubrano P., Madejski G. M., Maldera S., Manfreda A., Marti-Devesa G., Mazziotta M. N., Mereu I, Michelson P. F., Mirabal N., Mitthumsiri W., Mizuno T., Monzani M. E., Morselli A., Moskalenko I. V, Negro M., Ojha R., Orienti M., Orlando E., Ormes J. F., Pei Z., Pena-Herazo H., Persic M., Pesce-Rollins M., Petrosian V, Pillera R., Poon H., Porter T. A., Principe G., Raino S., Rando R., Rani B., Razzano M., Razzaque S., Reimer A., Reimer O., Scotton L., Serini D., Sgro C., Siskind E. J., Spandre G., Spinelli P., Suson D. J., Tajima H., Torres D. F., Valverde J., Yassin H., Zaharijas G.

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES   Vol. 263 ( 2 )   2022.12

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/1538-4365

Web of Science

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

Abe, H; Abe, S; Acciari, VA; 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, ; 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, ; Busetto, G; Carosi, R; Carretero-Castrillo, M; Ceribella, G; Chai, Y; Chilingarian, A; Cikota, S; Colombo, E; Contreras, JL; Cortina, J; Covino, S; D'Amico, G; D'Elia, ; 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; Ramazani, VF; Fariña, L; Fattorini, A; 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; Hoang, 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; Aguilar, AM; 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, ; Nakamori, T; Nanci, C; Nava, L; Neustroev, ; 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; Puljak, ; 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, ; 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, ; Vigorito, CF; Vitale, V; Vovk, ; Walter, R; Will, M; Wunderlich, C; Yamamoto, T; Zaric, D; Abdalla, H; Aharonian, F; Benkhali, FA; Angüner, EO; Ashkar, H; Backes, M; Baghmanyan, ; Martins, VB; Batzofin, R; Becherini, Y; Berge, D; Bernlöhr, K; Böttcher, M; Boisson, C; Bolmont, J; de Lavergne, MD; 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, OU; Cotter, G; Cristofari, P; Mbarubucyeye, JD; Devin, J; Djannati-Ataï, A; Dmytriiev, A; Egberts, K; Ernenwein, JP; Fiasson, A; de Clairfontaine, GF; Fontaine, G; Füssling, M; Funk, S; Gabici, S; Ghafourizadeh, S; Giavitto, G; Glawion, D; Glicenstein, JF; Goswami, P; Grolleron, G; Hinton, JA; Hörbe, M; Hoischen, C; Holch, TL; Holler, M; Horns, D; Huang, ZQ; Jamrozy, M; Jankowsky, F; Joshi, ; Jung-Richardt, ; Kasai, E; Katarzynski, K; Katz, U; Khélifi, B; Kluzniak, W; Komin, N; Kosack, K; Kostunin, D; Lang, RG; Le Stum, S; Lemière, A; Lemoine-Goumard, M; Lenain, JP; Leuschner, F; Lohse, T; Luashvili, A; Lypova, ; Mackey, J; Majumdar, J; Malyshev, D; Malyshev, D; Marandon, ; Marchegiani, P; Martí-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, AP; O'Brien, P; Ohm, S; Olivera-Nieto, L; Wilhelmi, ED; Ostrowski, M; Panny, S; Panter, M; Parsons, RD; Poireau, ; Prokhorov, DA; Prokoph, H; Pühlhofer, G; Punch, M; Quirrenbach, A; Reichherzer, P; Reimer, A; Reimer, O; Renaud, M; Rieger, F; Rowell, G; Rudak, B; Ricarte, HR; Ruiz-Velasco, E; Sahakian, ; Salzmann, H; Santangelo, A; Sasaki, M; Schäfer, J; Schüssler, F; Schutte, HM; Schwanke, U; Shapopi, JNS; Sol, H; Specovius, A; Spencer, S; Stawarz, L; Steenkamp, R; Steinmassl, S; Steppa, C; Sushch, ; 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, SJ; White, R; Wierzcholska, A; Wong, YW; Yusafzai, A; Zacharias, M; Zanin, R; Zargaryan, D; Zdziarski, AA; Zech, A; Zhu, SJ; Zouari, S; Zywucka, N; Acharyya, A; Adams, CB; Batista, P; Benbow, W; Capasso, M; Christiansen, JL; Chromey, AJ; Errando, M; Falcone, A; Feng, Q; Finley, JP; Foote, GM; Fortson, L; Furniss, A; Gent, A; Hanlon, WE; Hervet, O; Holder, J; Hona, B; Humensky, TB; Jin, W; Kaaret, P; Kertzman, M; Kherlakian, M; Kleiner, TK; Kumar, S; Lang, MJ; Lundy, M; Maier, G; McGrath, CE; Millis, J; Moriarty, P; Mukherjee, R; O'Brien, S; Ong, RA; Park, N; Patel, SR; Pfrang, K; Pohl, M; Pueschel, E; Quinn, J; Ragan, K; Reynolds, PT; Ribeiro, D; Roache, E; Ryan, JL; Sadeh, ; Saha, L; Santander, M; Sembroski, GH; Shang, R; Splettstoesser, M; Tak, D; Tucci, J; Weinstein, A; Williams, DA; Williamson, TJ; Bosch-Ramon, ; Celma, C; Linares, M; Russell, DM; 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

Web of Science

Scopus

All-sky Medium Energy Gamma-ray Observatory eXplorer mission concept Reviewed

Caputo Regina, Ajello Marco, Kierans Carolyn A., Perkins Jeremy S., Racusin Judith L., Baldini Luca, Baring Matthew G., Bissaldi Elisabetta, Burns Eric, Cannady Nicholas, Charles Eric, da Silva Rui M. Curado, Fang Ke, Fleischhack Henrike, Fryer Chris, Fukazawa Yasushi, Grove J. Eric, Hartmann Dieter, Howell Eric J., Jadhav Manoj, Karwin Christopher M., Kocevski Daniel, Kurahashi Naoko, Latronico Luca, Lewis Tiffany R., Leys Richard, Lien Amy, Marcotulli Lea, Martinez-Castellanos Israel, Mazziotta Mario Nicola, McEnery Julie, Metcalfe Jessica, Murase Kohta, Negro Michela, Parker Lucas, Phlips Bernard, Prescod-Weinstein Chanda, Razzaque Soebur, Shawhan Peter S., Sheng Yong, Shutt Tom A., Shy Daniel, Sleator Clio, Steinhebel Amanda L., Striebig Nicolas, Suda Yusuke, Tak Donggeun, Tajima Hiro, Valverde Janeth, Venters Tonia M., Wadiasingh Zorawar, Woolf Richard S., Wulf Eric A., Zhang Haocheng, Zoglauer Andreas

JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS   Vol. 8 ( 4 )   2022.10

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1117/1.JATIS.8.4.044003

Web of Science

Search for New Cosmic-Ray Acceleration Sites within the 4FGL Catalog Galactic Plane Sources Reviewed International coauthorship International journal

Abdollahi, S; Acero, F; Ackermann, M; Baldini, L; Ballet, J; Barbiellini, G; Bastieri, D; Bellazzini, R; Berenji, B; Berretta, A; Bissaldi, E; Blandford, RD; Bonino, R; Bruel, P; Buson, S; Cameron, RA; Caputo, R; Caraveo, PA; Castro, D; Chiaro, G; Cibrario, N; Ciprini, S; Coronado-Blázquez, J; Crnogorcevic, M; Cutini, S; D'Ammando, F; De Gaetano, S; Di Lalla, N; Dirirsa, F; Di Venere, L; Domínguez, A; Fegan, SJ; Fiori, A; Fleischhack, H; Franckowiak, A; Fukazawa, Y; Fusco, P; Gammaldi, V; Gargano, F; Gasparrini, D; Giacchino, F; Giglietto, N; Giordano, F; Giroletti, M; Glanzman, T; Green, D; Grenier, IA; Grondin, MH; Guiriec, S; Gustafsson, M; Harding, AK; Hays, E; Hewitt, JW; Horan, D; Hou, X; Jóhannesson, G; Kayanoki, T; Kerr, M; Kuss, M; Larsson, S; Latronico, L; Lemoine-Goumard, M; Li, J; Longo, F; Loparco, F; Lubrano, P; Maldera, S; Malyshev, D; Manfreda, A; Martí-Devesa, G; Mazziotta, MN; Mereu, I; Michelson, PF; Mirabal, N; Mitthumsiri, W; Mizuno, T; Monzani, ME; Morselli, A; Moskalenko, IV; Nuss, E; Omodei, N; Orienti, M; Orlando, E; Ormes, JF; Paneque, D; Pei, Z; Persic, M; Pesce-Rollins, M; Pillera, R; Poon, H; Porter, TA; Principe, G; Rainò, S; Rando, R; Rani, B; Razzano, M; Razzaque, S; Reimer, A; Reimer, O; Reposeur, T; Sánchez-Conde, M; Parkinson, PMS; Scotton, L; Serini, D; Sgrò, C; Siskind, EJ; Spandre, G; Spinelli, P; Sueoka, K; Suson, DJ; Tajima, H; Tak, D; Thayer, JB; Torres, DF; Troja, E; Valverde, J; Wadiasingh, Z; Wood, K; Zaharijas, G

ASTROPHYSICAL JOURNAL   Vol. 933 ( 2 )   2022.7

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/1538-4357/ac704f

Web of Science

Incremental Fermi Large Area Telescope Fourth Source Catalog Reviewed International coauthorship International journal

Abdollahi, S; Acero, F; Baldini, L; Ballet, J; Bastieri, D; Bellazzini, R; Berenji, B; Berretta, A; Bissaldi, E; Blandford, RD; Bloom, E; Bonino, R; Brill, A; Britto, RJ; Bruel, P; Burnett, TH; Buson, S; Cameron, RA; Caputo, R; Caraveo, PA; Castro, D; Chaty, S; Cheung, CC; Chiaro, G; Cibrario, N; Ciprini, S; Coronado-Blázquez, J; Crnogorcevic, M; Cutini, S; D'Ammando, F; De Gaetano, S; Digel, SW; Di Lalla, N; Dirirsa, F; Di Venere, L; Domínguez, A; Ramazani, VF; Fegan, SJ; Ferrara, EC; Fiori, A; Fleischhack, H; Franckowiak, A; Fukazawa, Y; Funk, S; Fusco, P; Galanti, G; Gammaldi, V; Gargano, F; Garrappa, S; Gasparrini, D; Giacchino, F; Giglietto, N; Giordano, F; Giroletti, M; Glanzman, T; Green, D; Grenier, IA; Grondin, MH; Guillemot, L; Guiriec, S; Gustafsson, M; Harding, AK; Hays, E; Hewitt, JW; Horan, D; Hou, X; Jóhannesson, G; Karwin, C; Kayanoki, T; Kerr, M; Kuss, M; Landriu, D; Larsson, S; Latronico, L; Lemoine-Goumard, M; Li, J; Liodakis, I; Longo, F; Loparco, F; Lott, B; Lubrano, P; Maldera, S; Malyshev, D; Manfreda, A; Martí-Devesa, G; Mazziotta, MN; Mereu, I; Meyer, M; Michelson, PF; Mirabal, N; Mitthumsiri, W; Mizuno, T; Moiseev, AA; Monzani, ME; Morselli, A; Moskalenko, IV; Negro, M; Nuss, E; Omodei, N; Orienti, M; Orlando, E; Paneque, D; Pei, Z; Perkins, JS; Persic, M; Pesce-Rollins, M; Petrosian, V; Pillera, R; Poon, H; Porter, TA; Principe, G; Rainò, S; Rando, R; Rani, B; Razzano, M; Razzaque, S; Reimer, A; Reimer, O; Reposeur, T; Sánchez-Conde, M; Parkinson, PMS; Scotton, L; Serini, D; Sgrò, C; Siskind, EJ; Smith, DA; Spandre, G; Spinelli, P; Sueoka, K; Suson, DJ; Tajima, H; Tak, D; Thayer, JB; Thompson, DJ; Torres, DF; Troja, E; Valverde, J; Wood, K; Zaharijas, G

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES   Vol. 260 ( 2 )   2022.6

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/1538-4365/ac6751

Web of Science

Active Galactic Nuclei population studies with the Cherenkov Telescope Array Reviewed

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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Commissioning of the camera of the first Large Size Telescope of the Cherenkov Telescope Array Reviewed

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

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

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

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

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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Design and performance of the prototype Schwarzschild-Couder telescope camera Reviewed International coauthorship International journal

Adams, CB; Ambrosi, G; Ambrosio, M; Aramo, C; Arlen, T; Benbow, W; Bertucci, B; Bissaldi, E; Biteau, J; Bitossi, M; Boiano, A; Bonavolontà, C; Bose, R; Bouvier, A; Buscemi, M; Brill, A; Brown, AM; Buckley, JH; Canestrari, R; Capasso, M; Caprai, M; Coppi, P; Covault, CE; Depaoli, D; Di Venere, L; Errando, M; Fegan, S; Feng, Q; Fiandrini, E; Furniss, A; Garczarczyk, M; Gent, A; Giglietto, N; Giordano, F; Giro, E; Halliday, R; Hervet, O; Hughes, G; Incardona, S; Humensky, TB; Ionica, M; Jin, WD; Johnson, CA; Kieda, D; Krennrich, F; Kuznetsov, A; Lapington, J; Licciulli, F; Loporchio, S; Marsella, G; Masone, V; Meagher, K; Meures, T; Mode, BAW; Mognet, SAI; Mukherjee, R; Okumura, A; Pantaleo, FR; Paoletti, R; Di Pierro, F; Ribeiro, D; Riitano, L; Roache, E; Ross, D; Rousselle, J; Rugliancich, A; Santander, M; Schneider, M; Schoorlemmer, H; Shang, RY; Stevenson, B; Stiaccini, L; Tajima, H; Taylor, LP; Thornhill, J; Tosti, L; Tripodo, G; Vagelli, V; Valentino, M; Vandenbroucke, J; Vassiliev, VV; Wakely, SP; Watson, JJ; White, R; Wilcox, P; Williams, DA; Wood, M; Yu, P; Zink, A

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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The Small-Sized Telescope of CTAO Reviewed

Tagliaferri, G; Antonelli, A; Arnesen, T; Aschersleben, J; Attinà, 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, ED; De Simone, N; Depaoli, D; Dournaux, JL; Duffy, C; Einecke, S; Fermino, C; Funk, S; Gargano, C; Giavitto, G; Giuliani, A; Greenshaw, T; Hinton, J; Huet, JM; 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; Miccichè, 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, RZ; Saturni, FG; 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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DOI： 10.1117/12.2627956

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SOlar Neutron and Gamma-ray Spectroscopy Mission (SONGS) Reviewed

Yamaoka, K; Tajima, H; Miyata, K; Usami, M; Watabe, T; Matsushita, K; Ito, K; Nakazawa, K; Masuda, S; Tani, K; Arai, M; Hatori, S; Kume, K; Mizushima, S; Takahashi, H; Watanabe, K

SPACE TELESCOPES AND INSTRUMENTATION 2022: ULTRAVIOLET TO GAMMA RAY   Vol. 12181   2022

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Language：English   Publishing type：Research paper (scientific journal)   Publisher：Proceedings of SPIE - The International Society for Optical Engineering  

The SOlar Neutron and Gamma-ray Spectroscopy (SONGS) mission is a 3U cubesat dedicated for detecting neutrons and gamma-rays associated with intense solar flares. Solar neutron observations have not been in progress because ground-based observations are affected by attenuation in the Earth atmosphere, and there is no dedicated mission in space at present. Hence, we are now developing in collaboration between science and engineering people at universities, and preparing for launch around 2024 during the next solar maximum. The SONGS carries a novel radiation detector which consists of multi-layered plastic scintillator bars and GAGG(Ce) scintillator array so that it can determine energies for both neutrons and gamma-rays. In total 704 signals from Silicon photo-multipliers (SiPMs) are processed by 45 ASICs with very low power consumption, and realized within limited resources. In this presentation, we will describe scientific motivation, mission and instrument overview, and results from the bread-board model (BBM).

DOI： 10.1117/12.2629131

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AstroPix: Novel monolithic active pixel silicon sensors for future gamma-ray telescopes Reviewed

Steinhebel, AL; Fleischhack, H; Striebig, N; Jadhav, M; Suda, Y; Luz, R; Kierans, C; Caputo, R; Tajima, H; Leys, R; Peric, I; Metcalfe, J; Perkins, JS

SPACE TELESCOPES AND INSTRUMENTATION 2022: ULTRAVIOLET TO GAMMA RAY   Vol. 12181   2022

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Language：English   Publishing type：Research paper (scientific journal)   Publisher：Proceedings of SPIE - The International Society for Optical Engineering  

Space-based γ-ray telescopes such as the Fermi Large Area Telescope have used single sided silicon strip detectors to track secondary charged particles produced by primary γ-rays with high resolution. At the lower energies targeted by keV-MeV telescopes, two dimensional position information within a single detector is required for event reconstruction - especially in the Compton regime. This work describes the development of monolithic CMOS active pixel silicon sensors – AstroPix – as a novel technology for use in future γ-ray telescopes. Based upon sensors (ATLASPix) designed for use in the ATLAS detector at the Large Hadron Collider, AstroPix has the potential to maintain high performance while reducing noise with low power consumption. This is achieved with the dual detection and readout capabilities in each CMOS pixel. The status of AstroPix development and testing, as well as outlook for future testing and application, will be presented.

DOI： 10.1117/12.2630405

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