Search

Your search keyword '"Cherenkov counter"' showing total 217 results
Start Over Descriptor "Cherenkov counter"
217 results on '"Cherenkov counter"'

1. Electron Beam Monitor Based on Cherenkov Counter.

Author

Alekseev, V. I., Baskov, V. A., Dalkarov, O. D., Kol'zov, A. V., L'vov, A. I., Mamonov, I. A., Pavlyuchenko, L. N., and Polyansky, V. V.

Abstract

The design of a fast relativistic electron beam monitor based on a Cherenkov counter capable of determining the intensity in the range of 106–1011 electron/s is described. [ABSTRACT FROM AUTHOR]

Published
2019
Full Text
View/download PDF

2. Probing Dark Energy via Neutrino and Supernova Observatories

Author

Hall, Lawrence J.

Subjects
Physics of elementary particles and fields, dark energy, dark matter, antineutrino, cosmic radiation, cosmic radiation, flux, supernova, Cherenkov counter, water, Gadolinium, scintillation counter, liquid, argon, liquid, neutrino, mass, numerical calculations
Abstract

A novel method for extracting cosmological evolution parameters is proposed, using a probe other than light: future observations of the diffuse anti-neutrino flux emitted from core-collapse supernovae (SNe), combined with the SN rate extracted from future SN surveys. The relic SN neutrino differential flux can be extracted by using future neutrino detectors such as Gadolinium-enriched, megaton, water detectors or 100-kiloton detectors of liquid Argon or liquid scintillator. The core-collapse SN rate can be reconstructed from direct observation of SN explosions using future precision observatories. Our method, by itself, cannot compete with the accuracy of the optical-based measurements but may serve as an important consistency check as well as a source of complementary information. The proposal does not require construction of a dedicated experiment, but rather relies on future experiments proposed for other purposes.

Published
2008

4. Search for Ultraheavy Dark Matter from Observations of Dwarf Spheroidal Galaxies with VERITAS

Author

A. Acharyya, A. Archer, P. Bangale, J. T. Bartkoske, P. Batista, M. Baumgart, W. Benbow, J. H. Buckley, A. Falcone, Q. Feng, J. P. Finley, G. M. Foote, L. Fortson, A. Furniss, G. Gallagher, W. F. Hanlon, O. Hervet, J. Hoang, J. Holder, T. B. Humensky, W. Jin, P. Kaaret, M. Kertzman, M. Kherlakian, D. Kieda, T. K. Kleiner, N. Korzoun, F. Krennrich, M. J. Lang, M. Lundy, G. Maier, C. E McGrath, P. Moriarty, S. O’Brien, R. A. Ong, K. Pfrang, M. Pohl, E. Pueschel, J. Quinn, K. Ragan, P. T. Reynolds, E. Roache, N. L. Rodd, J. L. Ryan, I. Sadeh, L. Saha, M. Santander, G. H. Sembroski, R. Shang, M. Splettstoesser, D. Tak, J. V. Tucci, V. V. Vassiliev, and D. A. Williams

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), WIMP, VHE [gamma ray], FOS: Physical sciences, mass [dark matter], GeV, annihilation [dark matter], High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), TeV, fluctuation [background], composite, Particle Physics - Phenomenology, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, hep-ex, dark matter: mass, imaging, hep-ph, dark matter: annihilation, Astronomy and Astrophysics, observatory, High Energy Physics - Phenomenology, Cherenkov counter, gamma ray: VHE, Space and Planetary Science, astro-ph.CO, ddc:520, background: fluctuation, VERITAS, galaxy, Astrophysics - High Energy Astrophysical Phenomena, Particle Physics - Experiment, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The astrophysical journal / 1 945(2), 101 (2023). doi:10.3847/1538-4357/acbc7b, Dark matter is a key piece of the current cosmological scenario, with weakly interacting massive particles (WIMPs) a leading dark matter candidate. WIMPs have not been detected in their conventional parameter space (100 GeV ≲M $_{χ}$ ≲ 100 TeV), a mass range accessible with current Imaging Atmospheric Cherenkov Telescopes. As ultraheavy dark matter (UHDM; M $_{χ}$ ≳ 100 TeV) has been suggested as an underexplored alternative to the WIMP paradigm, we search for an indirect dark matter annihilation signal in a higher mass range (up to 30 PeV) with the VERITAS γ-ray observatory. With 216 hr of observations of four dwarf spheroidal galaxies, we perform an unbinned likelihood analysis. We find no evidence of a γ-ray signal from UHDM annihilation above the background fluctuation for any individual dwarf galaxy nor for a joint-fit analysis, and consequently constrain the velocity-weighted annihilation cross section of UHDM for dark matter particle masses between 1 TeV and 30 PeV. We additionally set constraints on the allowed radius of a composite UHDM particle., Published by Institute of Physics Publ., London

Published
2023

5. The PANDA Barrel DIRC.

Author

Dzhygadlo, R., Belias, A., Gerhardt, A., Lehmann, D., Peters, K., Schepers, G., Schwarz, C., Schwiening, J., Traxler, M., Wolf, Y., Schmitt, L., Böhm, M., Gumbert, K., Krauss, S., Lehmann, A., Miehling, D., Düren, M., Hayrapetyan, A., Köseoglu, I., and Schmidt, M.

Subjects
*CHERENKOV radiation, *FUSED silica, *MICROCHANNEL plates, *PANDAS, *PHOTOMULTIPLIERS, *CHERENKOV counters
Abstract

The PANDA experiment at the international accelerator Facility for Antiproton and Ion Research in Europe (FAIR), Darmstadt, Germany, will address fundamental questions of hadron physics using p ̄ p annihilations. Excellent Particle Identification (PID) over a large range of solid angles and particle momenta will be essential to meet the objectives of the rich physics program. Charged PID in the target region will be provided by a Barrel DIRC (Detection of Internally Reflected Cherenkov light) counter. The Barrel DIRC, covering the polar angle range of 22–140 degrees, will provide a π / K separation power of at least 3 standard deviations for charged particle momenta up to 3.5 GeV/c. The design of the Barrel DIRC features narrow radiator bars made from synthetic fused silica, an innovative multi-layer spherical lens focusing system, a prism-shaped synthetic fused silica expansion volume, and an array of lifetime-enhanced Microchannel Plate PMTs (MCP-PMTs) to detect the hit location and arrival time of the Cherenkov photons. Detailed Monte-Carlo simulations were performed, and reconstruction methods were developed to study the performance of the system. All critical aspects of the design and the performance were validated with system prototypes in a mixed hadron beam at the CERN PS. In 2020 the PANDA Barrel DIRC project advanced from the design stage to component fabrication. The series production of the fused silica bars was successfully completed in 2021 and delivery of the MCP-PMTs started in May 2022. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

6. Probing AGN variability with the Cherenkov Telescope Array

Author

Cangemi, F., Hovatta, T., Lindfors, E., Cerruti, M., Becerra-Gonzalez, J., Biteau, J., Boisson, C., Böttcher, M., de Gouveia Dal Pino, E., Dorner, D., Grolleron, G., Lenain, J.-P., Manganaro, M., Max-Moerbeck, W., Morris, P., Nilsson, K., Reis, L. Passos, Romano, P., Sergijenko, O., Tavecchio, F., Vercellone, S., Wagner, S., Zacharias, M., and Cherenkov Telescope Array Collaboration

Subjects
particle: acceleration, Cherenkov Telescope Array, electromagnetic, Cherenkov counter, accelerator, variability, spectral, imaging, TeV, AGN, GeV, sensitivity, jet: relativistic
Abstract

Relativistic jets launched by Active Galactic Nuclei are among the most powerful particle accelerators in the Universe. The emission over the entire electromagnetic spectrum of these relativistic jets can be extremely variable with scales of variability from less than few minutes up to several years. These variability patterns, which can be very complex, contain information about the acceleration processes of the particles and the area(s) of emission. Thanks to its sensitivity, five-to twenty-times better than the current generation of Imaging Atmospheric Cherenkov Telescopes depending on energy, the Cherenkov Telescope Array will be able to follow the emission from these objects with a very accurate time sampling and over a wide spectral coverage from 20 GeV to > 20 TeV and thus reveal the nature of the acceleration processes at work in these objects. We will show the first results of our lightcurve simulations and long-term behavior of AGN as will be observed by CTA, based on state-of-art particle acceleration models.

Published
2023
Full Text
View/download PDF

7. Limits on Neutrino Emission from GRB 221009A from MeV to PeV Using the IceCube Neutrino Observatory

Author

Abbasi, R., Ackermann, M., Adams, J., Agarwalla, S. K., Aggarwal, N., Aguilar, J. A., Ahlers, M., Alameddine, J. M., Amin, N. M., Andeen, K., Anton, G., Argüelles, C., Ashida, Y., Athanasiadou, S., Axani, S. N., Bai, X., Balagopal V., A., Baricevic, M., Barwick, S. W., Basu, V., Bay, R., Beatty, J. J., Becker, K.-H., Becker Tjus, J., Beise, J., Bellenghi, C., BenZvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bontempo, F., Book, J. Y., Borowka, J., Meneguolo, C. Boscolo, Böser, S., Botner, O., Böttcher, J., Bourbeau, E., Braun, J., Brinson, B., Brostean-Kaiser, J., Burley, R. T., Busse, R. S., Campana, M. A., Carloni, K., Carnie-Bronca, E. G., Chen, C., Chen, Z., Chirkin, D., Choi, S., Clark, B. A., Classen, L., Coleman, A., Collin, G. H., Connolly, A., Conrad, J. M., Coppin, P., Correa, P., Countryman, S., Cowen, D. F., Dappen, C., Dave, P., De Clercq, C., DeLaunay, J. J., Delgado López, D., Dembinski, H., Deoskar, K., Desai, A., Desiati, P., de Vries, K. D., de Wasseige, G., DeYoung, T., Diaz, A., Díaz-Vélez, J. C., Dittmer, M., Domi, A., Dujmovic, H., DuVernois, M. A., Ehrhardt, T., Eller, P., Engel, R., Erpenbeck, H., Evans, J., Evenson, P. A., Fan, K. L., Fazely, A. R., Fedynitch, A., Feigl, N., Fiedlschuster, S., Finley, C., Fischer, L., Fox, D., Franckowiak, A., Friedman, E., Fritz, A., Fürst, P., Gaisser, T. K., Gallagher, J., Ganster, E., Garcia, A., Garrappa, S., Gerhardt, L., Ghadimi, A., Glaser, C., Glauch, T., Glüsenkamp, T., Goehlke, N., Gonzalez, J. G., Goswami, S., Grant, D., Gray, S. J., Griffin, S., Griswold, S., Günther, C., Gutjahr, P., Haack, C., Hallgren, A., Halliday, R., Halve, L., Halzen, F., Hamdaoui, H., Ha Minh, M., Hanson, K., Hardin, J., Harnisch, A. A., Hatch, P., Haungs, A., Helbing, K., Hellrung, J., Henningsen, F., Heuermann, L., Hickford, S., Hidvegi, A., Hill, C., Hill, G. C., Hoffman, K. D., Hoshina, K., Hou, W., Huber, T., Hultqvist, K., Hünnefeld, M., Hussain, R., Hymon, K., In, S., Iovine, N., Ishihara, A., Jansson, M., Japaridze, G. S., Jeong, M., Jin, M., Jones, B. J. P., Kang, D., Kang, W., Kang, X., Kappes, A., Kappesser, D., Kardum, L., Karg, T., Karl, M., Karle, A., Katz, U., Kauer, M., Kelley, J. L., Kheirandish, A., Kin, K., Kiryluk, J., Klein, S. R., Kochocki, A., Koirala, R., Kolanoski, H., Kontrimas, T., Köpke, L., Kopper, C., Koskinen, D. J., Koundal, P., Kovacevich, M., Kowalski, M., Kozynets, T., Kruiswijk, K., Krupczak, E., Kumar, A., Kun, E., Kurahashi, N., Lad, N., Lagunas Gualda, C., Lamoureux, M., Larson, M. J., Lauber, F., Lazar, J. P., Lee, J. W., Leonard DeHolton, K., Leszczyńska, A., Lincetto, M., Liu, Q. R., Liubarska, M., Lohfink, E., Love, C., Lozano Mariscal, C. J., Lu, L., Lucarelli, F., Ludwig, A., Luszczak, W., Lyu, Y., Ma, W. Y., Madsen, J., Mahn, K. B. M., Makino, Y., Mancina, S., Sainte, W. Marie, Mariş, I. C., Marka, S., Marka, Z., Marsee, M., Martinez-Soler, I., Maruyama, R., Mayhew, F., McElroy, T., McNally, F., Mead, J. V., Meagher, K., Mechbal, S., Medina, A., Meier, M., Meighen-Berger, S., Merckx, Y., Merten, L., Micallef, J., Mockler, D., Montaruli, T., Moore, R. W., Morii, Y., Morse, R., Moulai, M., Mukherjee, T., Naab, R., Nagai, R., Naumann, U., Necker, J., Neumann, M., Niederhausen, H., Nisa, M. U., Noell, A., Nowicki, S. C., Pollmann, A. Obertacke, Oehler, M., Oeyen, B., Olivas, A., Orsoe, R., Osborn, J., O'Sullivan, E., Pandya, H., Park, N., Parker, G. K., Paudel, E. N., Paul, L., Pérez de los Heros, C., Peterson, J., Philippen, S., Pieper, S., Pizzuto, A., Plum, M., Popovych, Y., Rodriguez, M. Prado, Pries, B., Procter-Murphy, R., Przybylski, G. T., Raab, C., Rack-Helleis, J., Rawlins, K., Rechav, Z., Rehman, A., Reichherzer, P., Renzi, G., Resconi, E., Reusch, S., Rhode, W., Richman, M., Riedel, B., Roberts, E. J., Robertson, S., Rodan, S., Roellinghoff, G., Rongen, M., Rott, C., Ruhe, T., Ruohan, L., Ryckbosch, D., Safa, I., Saffer, J., Salazar-Gallegos, D., Sampathkumar, P., Herrera, S. E. Sanchez, Sandrock, A., Santander, M., Sarkar, S., Savelberg, J., Savina, P., Schaufel, M., Schieler, H., Schindler, S., Schlüter, B., Schmidt, T., Schneider, J., Schröder, F. G., Schumacher, L., Schwefer, G., Sclafani, S., Seckel, D., Seunarine, S., Sharma, A., Shefali, S., Shimizu, N., Silva, M., Skrzypek, B., Smithers, B., Snihur, R., Soedingrekso, J., Søgaard, A., Soldin, D., Sommani, G., Spannfellner, C., Spiczak, G. M., Spiering, C., Stamatikos, M., Stanev, T., Stein, R., Stezelberger, T., Stürwald, T., Stuttard, T., Sullivan, G. W., Taboada, I., Ter-Antonyan, S., Thompson, W. G., Thwaites, J., Tilav, S., Tollefson, K., Tönnis, C., Toscano, S., Tosi, D., Trettin, A., Tung, C. F., Turcotte, R., Twagirayezu, J. P., Ty, B., Unland Elorrieta, M. A., Upshaw, K., Valtonen-Mattila, N., Vandenbroucke, J., van Eijndhoven, N., Vannerom, D., van Santen, J., Vara, J., Veitch-Michaelis, J., Venugopal, M., Verpoest, S., Veske, D., Walck, C., Watson, T. B., Weaver, C., Weigel, P., Weindl, A., Weldert, J., Wendt, C., Werthebach, J., Weyrauch, M., Whitehorn, N., Wiebusch, C. H., Willey, N., Williams, D. R., Wolf, M., Wrede, G., Wulff, J., Xu, X. W., Yanez, J. P., Yildizci, E., Yoshida, S., Yu, F., Yu, S., Yuan, T., Zhang, Z., Zhelnin, P., and IceCube Collaboration

Subjects
background, gamma ray: burst, redshift, GLAST, neutrino: UHE, IceCube, observatory, Cherenkov counter, correlation, emission, TeV, Cherenkov, LHAASO
Abstract

Gamma-ray bursts (GRBs) have long been considered a possible source of high-energy neutrinos. While no correlations have yet been detected between high-energy neutrinos and GRBs, the recent observation of GRB 221009A—the brightest GRB observed by Fermi-GBM to date and the first one to be observed above an energy of 10 TeV—provides a unique opportunity to test for hadronic emission. In this paper, we leverage the wide energy range of the IceCube Neutrino Observatory to search for neutrinos from GRB 221009A. We find no significant deviation from background expectation across event samples ranging from MeV to PeV energies, placing stringent upper limits on the neutrino emission from this source.

Published
2023
Full Text
View/download PDF

8. Study of the GeV to TeV morphology of the γ Cygni SNR (G 78.2+2.1) with MAGIC and Fermi-LAT - Evidence for cosmic ray escape

Author

Acciari, V. A., Ansoldi, S., Antonelli, L. A., Arbet Engels, A., Baack, D., Babić, A., Banerjee, B., Barres de Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Bellizzi, L., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bošnjak, Z., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S. M., Colin, U., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Depaoli, D., Di Pierro, F., Di Venere, L., Do Souto Espiñeira, E., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Ferrara, G., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., García López, R. J., Garczarczyk, Markus, Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Green, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Hütten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kajiwara, Y., Karjalainen, M., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Coto, R., López-Oramas, A., Loporchio, S., Machado de Oliveira Fraga, B., Masuda, S., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Mender, S., Mićanović, S., Miceli, D., Miener, T., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Nozaki, S., Ohtani, Y., Oka, T., Otero-Santos, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletić, L., Peñil, P., Peresano, M., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schleicher, B., Schmidt, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Spolon, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tosti, L., van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Ventura, S., Verguilov, V., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Zarić, D., authors, External, Celli, S., Morlino, G., and MAGIC Collaboration

Subjects
lifetime, model [emission], turbulence, diffusion, energy spectrum, acceleration: shock waves, imaging, GeV, MAGIC, GLAST, emission: model, energy dependence, inverse scattering method, Cherenkov counter, gamma ray, cosmic radiation: galaxy, supernova, ddc:520, galaxy [cosmic radiation], time dependence, TeV, shock waves [acceleration]
Abstract

Astronomy and astrophysics 670, A8 (2023). doi:10.1051/0004-6361/202038748, Context. Diffusive shock acceleration (DSA) is the most promising mechanism that accelerates Galactic cosmic rays (CRs) in the shocks of supernova remnants (SNRs). It is based on particles scattering caused by turbulence ahead and behind the shock. The turbulence upstream is supposedly generated by the CRs, but this process is not well understood. The dominant mechanism may depend on the evolutionary state of the shock and can be studied via the CRs escaping upstream into the interstellar medium (ISM).Aims. Previous observations of the γ Cygni SNR showed a difference in morphology between GeV and TeV energies. Since this SNR has the right age and is at the evolutionary stage for a significant fraction of CRs to escape, our aim is to understand γ-ray emission in the vicinity of the γ Cygni SNR.Methods. We observed the region of the γ Cygni SNR with the MAGIC Imaging Atmospheric Cherenkov telescopes between 2015 May and 2017 September recording 87 h of good-quality data. Additionally, we analysed Fermi-LAT data to study the energy dependence of the morphology as well as the energy spectrum in the GeV to TeV range. The energy spectra and morphology were compared against theoretical predictions, which include a detailed derivation of the CR escape process and their γ-ray generation.Results. The MAGIC and Fermi-LAT data allowed us to identify three emission regions that can be associated with the SNR and that dominate at different energies. Our hadronic emission model accounts well for the morphology and energy spectrum of all source components. It constrains the time-dependence of the maximum energy of the CRs at the shock, the time-dependence of the level of turbulence, and the diffusion coefficient immediately outside the SNR shock. While in agreement with the standard picture of DSA, the time-dependence of the maximum energy was found to be steeper than predicted, and the level of turbulence was found to change over the lifetime of the SNR.Key words: acceleration of particles / cosmic rays / gamma rays: general / gamma rays: ISM / ISM: clouds / ISM: supernova remnants★ Corresponding authors; e-mail: contact.magic@mpp.mpg.de, Published by EDP Sciences, Les Ulis

Published
2023

9. Validating Monte Carlo simulations for an analysis chain in H.E.S.S

Author

Leuschner, Fabian, Schäfer, Johannes, Steinmassl, Simon, Holch, Tim Lukas, Bernlöhr, Konrad, Funk, Stefan, Hinton, Jim, Ohm, Stefan, and Pühlhofer, Gerd

Subjects
numerical calculations, Monte Carlo, air, imaging, trigger, VHE, photon, energy, flux, Cherenkov counter, showers, electromagnetic, gamma ray, cosmic radiation, HESS, atmosphere, propagation, site, radiation, Cherenkov, showers, cascade, photon, primary
Abstract

Imaging Air Cherenkov Telescopes (IACTs) detect very high energetic (VHE) gamma rays. They observe the Cherenkov light emitted in electromagnetic shower cascades that gamma rays induce in the atmosphere. A precise reconstruction of the primary photon energy and the source flux depends heavily on accurate Monte Carlo (MC) simulations of the shower propagation and the detector response, and therefore also on adequate assumptions about the atmosphere at the site and time of a measurement. Here, we present the results of an extensive validation of the MC simulations for an analysis chain of the H.E.S.S. experiment with special focus on the recently installed FlashCam camera on the large 28 m telescope. One goal of this work was to create a flexible and easy-to-use framework to facilitate the detailed validation of MC simulations also for past and future phases of the H.E.S.S. experiment. Guided by the underlying physics, the detector simulation and the atmospheric transmission profiles were gradually improved until low level parameters such as cosmic ray (CR) trigger rates matched within a few percent between simulations and observational data. This led to instrument response functions (IRFs) with which the analysis of current H.E.S.S. data can ultimately be carried out within percent accuracy, substantially improving earlier simulations.

Published
2023
Full Text
View/download PDF

10. Analog signal processing for large area SiPM in Cherenkov telescope camera

Author

Shobha K. Rao, K.S. Gothe, S.S. Upadhya, N.K. Parmar, R.L. Deshmukh, B.B. Singh, Sandeep Kumar, M. Ranjan, A. Sarkar, S.R. Patel, and V.R. Chitnis

Subjects
Nuclear and High Energy Physics, topology, SiPM, ddc:530, photomultiplier, silicon, Instrumentation, Front-end, signal processing, analog, Preamplifier, photon, IACT, imaging, resolution, G-APD, detector, pixel, calibration, Cherenkov counter, photomultiplier, avalanche, gamma ray, atmosphere, amplifier, radiation, Cherenkov, Camera, performance
Abstract

Nuclear instruments & methods in physics research / A 1051, 168191 (2023). doi:10.1016/j.nima.2023.168191, We have developed a preamplifier which processes signals from large area pixel sensors each comprising a 4 × 4 array of SiPMs. These amplifiers constitute a front-end portion of 256 pixel camera for an Imaging Atmospheric Cherenkov Telescope (IACT). The camera would be mounted at the focal plane of the 4-m class telescope. The primary design objective of the camera is to detect the wide energy range of the celestial Gamma-rays by detecting the atmospheric Cherenkov photons produced by them in the atmosphere. The other important objective of the camera is to be able to resolve single photon response for accurate pixel gain calibration. There are several factors like large size sensor, long time response, single p.e. resolution, etc., which have led to a customized design of the preamplifier. We propose an original circuit topology to achieve the design goals. The paper describes the design features of the preamplifier and performance evaluation., Published by North-Holland Publ. Co., Amsterdam

Published
2023

11. The TAIGA experiment

Author

Tluczykont, M., Astapov, I. I., Awad, A. K., Bezyazeekov, P. A., Blank, M., Bonvech, E. A., Borodin, A. N., Bulan, A. V., Brückner, M., Budnev, N. M., Chiavassa, A., Chernov, D. V., Dyachok, A. N., Gafarov, A. R., Garmash, A. Yu., Grebenyuk, V. M., Gress, O. A., Gress, E., Gress, T. I., Grishin, O. G., Grinyuk, A. A., Horns, D., Ivanova, A. L., Kalmykov, N. N., Kindin, V. V., Kiryuhin, S. N., Kokoulin, R. P., Kompaniets, K. G., Korosteleva, E. E., Kozhin, V. A., Kravchenko, E. A., Kryukov, A. P., Kuzmichev, L. A., Lagutin, A. A., Lavrova, M., Lemeshev, E., Lubsandorzhiev, B. K., Lubsandorzhiev, N. B., Lukanov, A. D., Lukyantsev, D. S., Mirgazov, R. R., Mirzoyan, R., Monkhoev, R. D., Osipova, E. A., Pakhorukov, A. L., Pan, A., Pankov, L. V., Panov, A. D., Petrukhin, A. A., Podgrudkov, D. A., Poleschuk, V. A., Popova, E. G., Porelli, A., Postnikov, E. B., Prosin, V. V., Ptuskin, V. S., Pushnin, A. A., Raikin, R. I., Razumov, A. Y., Rubtsov, G. I., Ryabov, E. V., Sagan, Y. I., Samoliga, V. S., Satyshev, I., Semeney, Yu. A., Silaev, A. A., Sidorenkov, A. Yu., Skurikhin, A. V., Sokolov, A. V., Suvorkin, Y., Sveshnikova, L. G., Tabolenko, V. A., Tanaev, A. B., Tarashansky, B. A., Ternovoy, M., Tkachev, L. G., Ushakov, N., Vaidyanathan, A., Volchugov, P. A., Volkov, N. V., Voronin, D., Wischnewski, R., Yashin, I. I., Zagorodnikov, A. V., Zhurov, D. P., and TAIGA Collaboration

Subjects
showers, atmosphere, hybrid, air, Crab Nebula [Observations], resolution, Observations: Crab Nebula, beam, width, energy, low, wide-angle, Cherenkov counter, energy, high, gamma ray, cosmic radiation, experiments [Gamma-rays], charged particle, detector, radiation, Cherenkov, TeV, spectral, surface, muon, detector, Gamma-rays: experiments, detector, imaging
Abstract

The Sixteenth Marcel Grossmann Meeting On Recent Developments in Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories (In 4 Volumes) 16th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Astrophysics and Relativistic Field Theories, MG16, Online, Italy, 5 Jul 2021 - 9 Jul 2021; World Scientific Publishing 3324-3342 (2023). doi:10.1142/9789811269776_0274, The Tunka Advanced Instrument for Gamma-ray and cosmic ray Astrophysics (TAIGA) is a hybrid experiment for the measurement of Extensive Air Showers (EAS) with good spectral resolution in the TeV to PeV energy range. In this domain, the long-sought Pevatrons can be detected. Currently the hybrid TAIGA detector combines two wide angle shower front Cherenkov light sampling timing arrays (HiSCORE and Tunka-133), two 4m class, 10° aperture Imaging Air Cherenkov Telescopes (IACTs) and 240 m2 surface and underground charged particle detector stations. Our goal is to introduce a new hybrid reconstruction technique, combining the good angular and shower core resolution of HiSCORE with the gamma-hadron separation power of imaging telescopes. This approach allows to maximize the effective area and simultaneously to reach a good gamma-hadron separation at low energies (few TeV). At higher energies, muon detectors are planned to enhance gamma-hadron separation. During the commissioning phase of the first and second IACT, several sources were observed. First detections of known sources with the first telescope show the functionality of the TAIGA IACTs. Here, the status of the TAIGA experiment will be presented, along with first results from the current configuration., Published by World Scientific Publishing

Published
2023

15. Development of the ARICH monitor system for the Belle II experiment.

Author

Hataya, K., Adachi, I., Dolenec, R., Iori, S., Iwata, S., Kakuno, H., Kataura, R., Kawai, H., Kindo, H., Kobayashi, T., Korpar, S., Križan, P., Kumita, T., Mrvar, M., Nishida, S., Ogawa, K., Ogawa, S., Pestotnik, R., Šantelj, L., and Sumiyoshi, T.

Subjects
*CHERENKOV counters, *PHOTODETECTORS, *AEROGELS, *PHOTON scattering, *OPTICAL fibers
Abstract

The Belle II detector is under construction at KEK in Japan. In the forward endcap region of the Belle II detector, particle identification (PID) is performed by the Aerogel Ring Imaging Cherenkov (ARICH) counter composed of aerogel tiles and 144-channel Hybrid Avalanche Photo-Detectors (HAPDs). The photon detection efficiency of the photosensor is important for a stable operation of the ARICH. To examine the performance of the HAPDs periodically, a monitor system using scattered photons injected by optical fibers is being developed. In this paper, we report the test using the prototype monitor system and the tests with a partially built ARICH detector. [ABSTRACT FROM AUTHOR]

Published
2017
Full Text
View/download PDF

17. Study of the EUSO-SPB2 Photodetection Module

Author

Panico, B., Blin, S., Colalillo, R., Creusot, A., Flaminio, F., Mese, M., Osteria, G., Parizot, E., Perfetto, F., Prévôt, G., Scotti, V., Trofimov, D., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and JEM-EUSO

Subjects
observatory, pressure, Cherenkov counter, detector, cosmic radiation, background, Cherenkov, fluorescence, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], calibration, tracks, UHE
Abstract

International audience; The Extreme Universe Space Observatory Super Pressure Balloon 2 (EUSO-SPB2) is an approved NASA balloon mission that is planned to fly in 2023 fromWanaka, NZ with target duration of up to 100 days. It is a pathfinder for the Probe of Extreme Multi-Messenger Astrophysics (POEMMA), a candidate for a NASA Astrophysics probe-class mission. EUSO-SPB2 will consist of a Cherenkov telescope and a fluorescence telescope. The first is optimized for fast signals and is devoted to estimate the background sources for astrophysical neutrino observations; the second looks at the nadir to measure the fluorescence emission of Ultra High Energy Cosmic Rays (UHECRs).The long-duration flight will provide a large number of VHECR Cherenkov signals and UHECR fluorescence tracks. In this contribution we discuss the calibration with dedicated signal of thephotodetection module.

Published
2022

18. Neutrino tagging: a new tool for accelerator based neutrino experiments

Author

Mathieu Perrin-Terrin, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and ANR-19-CE31-0009,ENTER,Amélioration du tagging et de la reconstruction de l'énergie des neutrinos(2019)

Subjects
detector: technology, +muon-+neutrino%2Fmu%22">pi- --> muon- neutrino/mu, data analysis method, experimental methods, Physics - Instrumentation and Detectors, accelerator, Physics and Astronomy (miscellaneous), Cherenkov counter: water, Physics::Instrumentation and Detectors, water, pi: leptonic decay, FOS: Physical sciences, tagged beam, High Energy Physics - Experiment, neutrino: production, High Energy Physics - Experiment (hep-ex), neutrino, CP: violation, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], KM3NeT, Engineering (miscellaneous), detector, silicon, Instrumentation and Detectors (physics.ins-det), charged particle: decay, sensitivity, charged particle, asymmetry: CP, Cherenkov counter, CP, kinematics, technology, High Energy Physics::Experiment, production, violation, +muon%2B+neutrino%2Fmu%22">pi+ --> muon+ neutrino/mu, pi: particle identification, performance, experimental results
Abstract

This article describes a new experimental method for accelerator based neutrino experiments called neutrino tagging. The method consists in exploiting the neutrino production mechanism, the "Equation missing" decay, to kinematically reconstruct the neutrino properties from the decay incoming and outgoing charged particles. The reconstruction of these particles relies on the recent progress and on-going developments in silicon particle detector technology. A detailed description of the method and achievable key performances is presented, together with its potential benefits for short and long baseline experiments. Then, a novel configuration for long baseline experiments is discussed in which a tagged beam would be employed together with mega-ton scale natural deep water Cherenkov detectors. The coarseness of this type of detectors is overcome by the precision of the tagging and, conversely, the rate limitation imposed by the tagging is outweighed by the size of the detector. These mutual benefits result in an affordable design for next generations of long baseline experiments. The physics potential of such experiments is quantified using the Protvino to KM3NeT/ORCA setup as a case study for which an unprecedented sensitivity to the leptonic CP violation could be achieved.

Published
2022

20. Detection of extended TeV emission around the Geminga pulsar with H.E.S.S

Author

Michael Punch, Christo Venter, Christian Stegmann, Stefan Wagner, Andreas Zech, Yasunobu Uchiyama, M. Hörbe, L. Mohrmann, Hassan Abdalla, Albert Seyffert, Michael Backes, Laenita Lorraine Oberholzer, Dieter Horns, K. Nakashima, Tim Holch, K. Bernloehr, Naomi Tsuji, Heinrich J. Völk, Regis Terrier, Carlo Romoli, Gerard Fontaine, Tadayuki Takahashi, M. Fuessling, Hester Schutte, S. Steinmassl, Samuel Timothy Spencer, Sami Caroff, Victor Doroshenko, Frank M. Rieger, Clemens Hoischen, A. A. Zdziarski, P. T. O'Brien, Markus Holler, Q. Remy, Felix Jankowsky, Hannah Dalgleish, German Hermann, Paul Morris, Anne Lemiere, E. Kasai, Louis Du Plessis, Johann van der Walt, Martin Tluczykont, Dan Parsons, Anna Barnacka, D. Malyshev, Nukri Komin, Tom Armstrong, Felix Aharonian, Gilles Maurin, J. F. Glicenstein, David Sanchez, Krzysztof Katarzynski, Victor Barbosa Martins, Ira Jung, C. Arcaro, Sebastian Panny, Gianluca Giavitto, Angel Noel, Bruno Khelifi, Alison Mitchell, Santiago Pita, Werner Hofmann, Gašper Kukec Mezek, Atreyee Sinha, Emma Ona-Wilhelmi, Jonathan Mackey, Carlo van Rensburg, Gerd Puehlhofer, Lei Sun, Laura Olivera-Nieto, Hambeleleni Ndiyavala, Floriane Cangemi, A. Yusafzai, C. Levy, Alexandre Marcowith, Felix Werner, Thomas Lohse, Hend Yassin, Anton Dmytriiev, Manuel Meyer, Arnaud Mares, Manami Sasaki, Mathieu Naurois, Catherine Boisson, Jhilik Majumdar, N. Zywucka, Sumari Hattingh, Takaaki Tanaka, Gavin Rowell, Hector Rueda Ricarte, Mathieu Bony, Oguzhan Anguener, C. Moore, Riaan Steenkamp, Richard White, Kirsty Feijen, Heike Prokoph, Thomas Bylund, Rowan Batzofin, Andreas Zmija, Dorit Glawion, Samuel Zouari, Tomasz Bulik, Robert Brose, Andrea Santangelo, Jacco Vink, Michal Ostrowski, Anna Luashvili, Jacques Muller, Malgorzata Curlo, Marion Spir-Jacob, M. Lemoine-Goumard, Lente Dreyer, David Huber, J.-P. Lenain, Matthieu Renaud, Amid Nayerhoda, Hugh Spackman, Michael Kreter, Justine Devin, Sabrina Casanova, Anu Kundu, Stefan Klepser, V. Sahakian, G. Peron, Alessandro Montanari, Garret Cotter, Vikas Joshi, Zhiqiu Huang, T. Chand, Lott Frans, D. A. Prokhorov, K. Kosack, Sylvia Zhu, P. J. Meintjes, David Berge, Yves Gallant, Lukasz Stawarz, Stefan Ohm, Halim Ashkar, Fabian Leuschner, Jason John Watson, Davit Zargaryan, Arache Djannati-Ataï, Johannes Schaefer, S. J. Fegan, Andreas Quirrenbach, Gaëtan Fichet de Clairfontaine, Axel Donath, A. W. Chen, Stefan Funk, Alicja Wierzcholska, Guillem Marti'i-Devesa, P. Reichherzer, V. Poireau, Jimmy N.S. Shapopi, Jaqueline Catalano, Stefano Gabici, Ramin Marx, M. Panter, Michael Zacharias, Jim Hinton, Jean-Pierre Ernenwein, U. Katz, G. Lamanna, R. Konno, Isak Delberth Davids, Fabian Schüssler, A. Fiasson, Sabrina Einecke, Iryna Lypova, S. Sailer, Dmitry Khangulyan, Charles Thorpe-Morgan, Roberta Zanin, Emmanuel Moulin, Andrew Taylor, B. Rudak, Kathrin Egberts, Johannes Veh, J. Bolmont, Faical Ait-Benkhali, Kleopas Shiningayamwe, Jacek Niemiec, G. Vasileiadis, Monica Barnard, Yvonne Becherini, Denys Malyshev, Maria Haupt, Olaf Reimer, Edna Ruiz Velasco, Lenka Tomankova, Sébastien Le Stum, Thomas Murach, Christopher van Eldik, Rafal Moderski, Mohanraj Senniappan, Francois Brun, P. Vincent, Heiko Salzmann, Andreas Specovius, Yu Wun Wong, Vincent Marandon, Hannes Thiersen, Vardan Baghmanyan, Celine Armand, Dmitriy Kostunin, L. Giunti, Brian van Soelen, Thomas Tavernier, Markus Boettcher, Michelle Tsirou, M.-H. Grondin, Rachel Simoni, Anita Reimer, Constantin Steppa, Ullrich Schwanke, Jean Damascene Mbarubucyeye, Wlodek Kluzniak, Brian Reville, Connor Duffy, James Davies, R. J. Tuffs, B. Bi, Mischa Breuhaus, Pauline Chambery, Marek Jamrozy, Helene Sol, Paolo Marchegiani, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and H.E.S.S.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma rays, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, imaging, Astronomy, IACT, Cosmology, Tellurium compounds, Cherenkov counter, gamma ray: emission, Pulsar, HESS, Milagro, TeV, HESS - Abteilung Hinton, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, HAWC, Cosmic rays, Cherenkov radiation, pulsar
Abstract

Highly extended gamma-ray emission around the Geminga pulsar was discovered by Milagro and verified by HAWC. Despite many observations with Imaging Atmospheric Cherenkov Telescopes (IACTs), detection of gamma-ray emission on angular scales exceeding the IACT field-of-view has proven challenging. Recent developments in analysis techniques have enabled the detection of significant emission around Geminga in archival data with H.E.S.S.. In 2019, further data on the Geminga region were obtained with an adapted observation strategy. Following the announcement of the detection of significant TeV emission around Geminga in archival data, in this contribution we present the detection in an independent dataset. New analysis results will be presented, and emphasis given to the technical challenges involved in observations of highly extended gamma-ray emission with IACTs., PoS: Proceedings of Science, 395, ISSN:1824-8039, Proceedings of 37th International Cosmic Ray Conference

Published
2022

21. First observation of the cosmic ray shadow of the Moon and the Sun with KM3NeT/ORCA

Author

Aiello, S, Albert, A, Alves Garre, S, Aly, Z, Ambrosone, A, Ameli, F, Andre, M, Anghinolfi, M, Anguita, M, Ardid, M, Ardid, S, Aublin, J, Bagatelas, C, Bailly-Salins, L, Baret, B, Basegmez Du Pree, S, Becherini, Y, Bendahman, M, Benfenati, F, Berbee, E, Bertin, V, Biagi, S, Boettcher, M, Cabo, M. Bou, Boumaaza, J, Bouta, M, Bouwhuis, M, Bozza, C, Brânzas, H, Bruijn, R, Brunner, J, Bruno, R, Buis, E, Buompane, R, Busto, J, Caiffi, B, Calvo, D, Campion, S, Capone, A, Carenini, F, Carretero, V, Castaldi, P, Celli, S, Cerisy, L, Chabab, M, Chau, N, Chen, A, Cherkaoui El Moursli, R, Cherubini, S, Chiarella, V, Chiarusi, T, Circella, M, Cocimano, R, Coelho, J.A.B, Coleiro, A, Coniglione, R, Coyle, P, Creusot, A, Cruz, A, Cuttone, G, Dallier, R, Darras, Y, de Benedittis, A, de Martino, B, del Burgo, R, Di Palma, I, Dìaz, A.F, Diego-Tortosa, D, Distefano, C, Domi, A, Donzaud, C, Dornic, D, Dörr, M, Drakopoulou, E, Drouhin, D, Eberl, T, Eddyamoui, A, van Eeden, T, Eff, M, van Eijk, D, El Bojaddaini, I, El Hedri, S, Enzenhöfer, A, Espinosa, V, Ferrara, G, Filipovíc, M.D, Filippini, F, Fusco, L.A, Gabriel, J, Gal, T, García Méndez, J, Garcia Soto, A, Garufi, F, Gatius Oliver, C, Geißelbrecht, N, Gialanella, L, Giorgio, E, Girardi, A, Goos, I, Gozzini, S.R, Gracia, R, Graf, K, Guderian, D, Guidi, C, Guillon, B, Gutiérrez, M, Haegel, L, van Haren, H, Heijboer, A, Hekalo, A, Hennig, L, Hernández-Rey, J.J, Huang, F, Ibnsalih, W. Idrissi, Illuminati, G, James, C.W, Janezashvili, D, de Jong, M, de Jong, P, Jung, B.J, Kalaczynski, P, Kalekin, O, Katz, U.F, Khan Chowdhury, N.R, Kistauri, G, van der Knaap, F, Kooijman, P, Kouchner, A, Kulikovskiy, V, Labalme, M, Lahmann, R, Lakhal, A, Lamoureux, M, Larosa, G, Lastoria, C, Lazo, A, Le Breton, R, Le Stum, S, Lehaut, G, Leonora, E, Lessing, N, Levi, G, Liang, S, Lindsey Clark, M, Longhitano, F, Maderer, L, Majumdar, J, Manczak, J, Margiotta, A, Marinelli, A, Markou, C, Martin, L, Martínez-Mora, J.A, Martini, A, Marzaioli, F, Mastrodicasa, M, Mastroianni, S, Melis, K.W, Miccichè, S, Miele, G, Migliozzi, P, Migneco, E, Mijakowski, P, Mollo, C.M, Morales-Gallegos, L, Morley-Wong, C, Moussa, A, Muller, R, Musone, M.R, Musumeci, M, Nauta, L, Navas, S, Nicolau, C.A, Nkosi, B, Ó Fearraigh, B, Orlando, A, Oukacha, E, Palacios González, J, Papalashvili, G, Papaleo, R, Gomez, E.J. Pastor, Paun, A.M, Pavalas, G.E, Pellegrino, C, Peña Martínez, S, Perrin-Terrin, M, Perronnel, J, Pestel, V, Piattelli, P, Pisanti, O, Poirè, C, Popa, V, Pradier, T, Pulvirenti, S, Quéméner, G, Rahaman, U, Randazzo, N, Razzaque, S, Rea, I.C, Real, D, Reck, S, Riccobene, G, Robinson, J, Romanov, A, Salesa Greus, F, Samtleben, D.F.E, Sánchez Losa, A, Sanguineti, M, Santonastaso, C, Santonocito, D, Sapienza, P, Sathe, A, Schnabel, J, Schneider, M.F, Schumann, J, Schutte, H.M, Seneca, J, Sgura, I, Shanidze, R, Sharma, A, Simonelli, A, Sinopoulou, A, Smirnov, M.V, Spisso, B, Spurio, M, Stavropoulos, D, Stellacci, S.M, Taiuti, M, Tavzarashvili, K, Tayalati, Y, Tedjditi, H, Thiersen, H, Tsagkli, S, Tsourapis, V, Tzamariudaki, E, van Elewyck, V, Vannoye, G, Vasileiadis, G, Versari, F, Viola, S, Vivolo, D, Warnhofer, H, Wilms, J, de Wolf, E, Yepes-Ramirez, H, Yousfi, T, Zavatarelli, S, Zegarelli, A, Zito, D, Zornoza, J.D, Zúñiga, J, Zywucka, N, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de physique corpusculaire de Caen (LPCC), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique subatomique et des technologies associées (SUBATECH), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), KM3NeT, Aiello, S., Albert, A., Alves Garre, S., Aly, Z., Ambrosone, A., Ameli, F., Andre, M., Anghinolfi, M., Anguita, M., Ardid, M., Ardid, S., Aublin, J., Bagatelas, C., Bailly-Salins, L., Baret, B., Pree, S. B., Becherini, Y., Bendahman, M., Benfenati, F., Berbee, E., Bertin, V., Biagi, S., Boettcher, M., Cabo, M. B., Boumaaza, J., Bouta, M., Bouwhuis, M., Bozza, C., Branzas, H., Bruijn, R., Brunner, J., Bruno, R., Buis, E., Buompane, R., Busto, J., Caiffi, B., Calvo, D., Campion, S., Capone, A., Carenini, F., Carretero, V., Castaldi, P., Celli, S., Cerisy, L., Chabab, M., Chau, N., Chen, A., Moursli, R. C. E., Cherubini, S., Chiarella, V., Chiarusi, T., Circella, M., Cocimano, R., Coelho, J. A. B., Coleiro, A., Coniglione, R., Coyle, P., Creusot, A., Cruz, A., Cuttone, G., Dallier, R., Darras, Y., De Benedittis, A., De Martino, B., Burgo, R. D., Palma, I. D., Diaz, A. F., Diego-Tortosa, D., Distefano, C., Domi, A., Donzaud, C., Dornic, D., Dorr, M., Drakopoulou, E., Drouhin, D., Eberl, T., Eddyamoui, A., Eeden, T., Eff, M., Eijk, D., Bojaddaini, I. E., Hedri, S. E., Enzenhofer, A., Espinosa, V., Ferrara, G., Filipovic, M. D., Filippini, F., Fusco, L. A., Gabriel, J., Gal, T., Mendez, J. G., Soto, A. G., Garufi, F., Oliver, C. G., Geisselbrecht, N., Gialanella, L., Giorgio, E., Girardi, A., Goos, I., Gozzini, S. R., Gracia, R., Graf, K., Guderian, D., Guidi, C., Guillon, B., Gutierrez, M., Haegel, L., Haren, H., Heijboer, A., Hekalo, A., Hennig, L., Hernandez-Rey, J. J., Huang, F., Ibnsalih, W. I., Illuminati, G., James, C. W., Janezashvili, D., de Jong, M., de Jong, P., Jung, B. J., Kalaczynski, P., Kalekin, O., Katz, U. F., Chowdhury, N. R. K., Kistauri, G., Knaap, F., Kooijman, P., Kouchner, A., Kulikovskiy, V., Labalme, M., Lahmann, R., Lakhal, A., Lamoureux, M., Larosa, G., Lastoria, C., Lazo, A., Breton, R. L., Stum, S. L., Lehaut, G., Leonora, E., Lessing, N., Levi, G., Liang, S., Clark, M. L., Longhitano, F., Maderer, L., Majumdar, J., Manczak, J., Margiotta, A., Marinelli, A., Markou, C., Martin, L., Martinez-Mora, J. A., Martini, A., Marzaioli, F., Mastrodicasa, M., Mastroianni, S., Melis, K. W., Micciche, S., Miele, G., Migliozzi, P., Migneco, E., Mijakowski, P., Mollo, C. M., Morales-Gallegos, L., Morley-Wong, C., Moussa, A., Muller, R., Musone, M. R., Musumeci, M., Nauta, L., Navas, S., Nicolau, C. A., Nkosi, B., Fearraigh, B. O., Orlando, A., Oukacha, E., Gonzalez, J. P., Papalashvili, G., Papaleo, R., Pastor Gomez, E. J., Paun, A. M., Pavalas, G. E., Pellegrino, C., Pena Martinez, S., Perrin-Terrin, M., Perronnel, J., Pestel, V., Piattelli, P., Pisanti, O., Poire, C., Popa, V., Pradier, T., Pulvirenti, S., Quemener, G., Rahaman, U., Randazzo, N., Razzaque, S., Rea, I. C., Real, D., Reck, S., Riccobene, G., Robinson, J., Romanov, A., Greus, F. S., Samtleben, D. F. E., Losa, A. S., Sanguineti, M., Santonastaso, C., Santonocito, D., Sapienza, P., Sathe, A., Schnabel, J., Schneider, M. F., Schumann, J., Schutte, H. M., Seneca, J., Sgura, I., Shanidze, R., Sharma, A., Simonelli, A., Sinopoulou, A., Smirnov, M. V., Spisso, B., Spurio, M., Stavropoulos, D., Stellacci, S. M., Taiuti, M., Tavzarashvili, K., Tayalati, Y., Tedjditi, H., Thiersen, H., Tsagkli, S., Tsourapis, V., Tzamariudaki, E., Elewyck, V. V., Vannoye, G., Vasileiadis, G., Versari, F., Viola, S., Vivolo, D., Warnhofer, H., Wilms, J., de Wolf, E., Yepes-Ramirez, H., Yousfi, T., Zavatarelli, S., Zegarelli, A., Zito, D., Zornoza, J. D., Zuniga, J., Zywucka, N., Centre Tecnològic de Vilanova i la Geltrú, and Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques

Subjects
Astrofísica, Physics and Astronomy (miscellaneous), FOS: Physical sciences, Astrophysics, statistical analysis, muon, optical, detector: calibration, Neutrins, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Neutrinos, lunar, numerical calculations, Engineering (miscellaneous), KM3NeT, Monte Carlo, Instrumentation and Methods for Astrophysics (astro-ph.IM), Detectors òptics, High Energy Astrophysical Phenomena (astro-ph.HE), ANTARES, photomultiplier, background, Cherenkov radiation, Neutrino astrophysics, solar, flux, Cherenkov counter, angular resolution, cosmic radiation, shadowing, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, performance
Abstract

This article reports the first observation of the Moon and the Sun shadows in the sky distribution of cosmic-ray induced muons measured by the KM3NeT/ORCA detector. The analysed data-taking period spans from February 2020 to November 2021, when the detector had 6 Detection Units deployed at the bottom of the Mediterranean Sea, each composed of 18 Digital Optical Modules. The shadows induced by the Moon and the Sun were detected with a statistical significance of 4.2{\sigma} and 6.2{\sigma}, respectively, at their nominal position. This early result confirms the effectiveness of the detector calibration, in time, position and orientation and the accuracy of the event direction reconstruction. This also demonstrates the performance and the competitiveness of the detector in terms of pointing accuracy and angular resolution., Comment: 15 pages, 7 figures

Published
2022
Full Text
View/download PDF

22. SiPM-based camera for gamma-ray imaging air Cherenkov telescope

Author

Chernov, D., Bonvech, E., Fedorov, O., Gafarov, A., Garmash, A., Grebenyuk, V., Gress, O., Gress, T., Grishin, O., Grinyuk, A., Horns, D., Ivanova, A., Astapov, I., Kalmykov, N., Kazarina, Y., Kindin, V., Kiryuhin, S., Kokoulin, R., Kompaniets, K., Korosteleva, E., Kozhin, V., Kravchenko, E., Krykov, A., Bezyazeekov, P., Kuzmichev, L., Lagutin, A., Lemeshev, Yu., Lubsandorzhiev, B., Lubsandorzhiev, N., Mirgazov, R., Mirzoyan, R., Monkhoev, R., Osipova, E., Pakhorukov, A., Borodin, A., Pan, A., Pankov, L., Petrukhin, A., Podgrudkov, D., Poleschuk, V., Popescu, M., Popova, E., Porelli, Andrea, Postnikov, E., Prosin, V., Brueckner, M., Ptuskin, V., Pushnin, A., Raikin, R., Rubtsov, G., Rybov, E., Sagan, Y., Samoliga, V., Silaev, A., Sidorenkov, A., Budnev, N., Skurikhin, A., Slunecka, V., Sokolov, A., Suvorkin, Y., Sveshnikova, L., Tabolenko, V., Tanaev, A., Tarashansky, B., Ternovoy, L., Tkachev, L., Chernukh, D., Tluczykont, M., Ushakov, N., Vaidyanathan, A., Volchugov, P., Voronin, D., Vorobiov, V., Wischnewski, R., Yashin, I., Zagorodnikov, A., Zhurov, D., Chiavassa, A., and Dyachok, A.

Subjects
History, family, hybrid, air, data acquisition, imaging, Computer Science Applications, Education, Cherenkov counter, wide-angle, star, analog-to-digital converter, gamma ray, power supply, ddc:530, photomultiplier, silicon, structure, control system, FPGA
Abstract

5th International Conference on Technology and Instrumentation in Particle Physics, TIPP 2021, Online, United States, 24 May 2021 - 28 May 2021; Journal of physics / Conference Series 2374(1), 012045 (2022). doi:10.1088/1742-6596/2374/1/012045, The current status of the equipment development for the new wide-angle gamma-ray imaging air Cherenkov telescope for TAIGA hybrid installation is presented. A front-end electronic and data acquisition system board based on the Zynq family Xilinx FPGA chips specially designed for this project have been produced and are being tested. A detailed description if presented for internal structure of the four main subsystems: four 8-channel 100 MHz ADCs, board’s control system, internal clock and synchronization system and the power supply system. Additionally, the current status of a small scale prototype telescope SIT consisting of 49 SiPM is presented. The telescope includes a digital camera for observing the stars and weather condition. The SIT-HiSCORE synchronization systems and the telemetry information collection had been tested., Published by IOP Publ., Bristol

Published
2022
Full Text
View/download PDF

23. Current and future $\gamma$-ray searches for dark-matter annihilation beyond the unitarity limit

Author

Tak, Donggeun, Baumgart, Matthew, Rodd, Nicholas L., and Pueschel, Elisa

Subjects
air, background, imaging, showers, GeV, VHE, cross section, geometrical, observatory, Cherenkov counter, unitarity, TeV, VERITAS, dark matter, annihilation, HAWC, signature, dark matter, mass
Abstract

For decades, searches for electroweak-scale dark matter (DM) have been performed without a definitive detection. This lack of success may hint that DM searches have focused on the wrong mass range. A proposed candidate beyond the canonical parameter space is ultra-heavy DM (UHDM). In this work, we consider indirect UHDM annihilation searches for masses between 30 TeV and 30 PeV, extending well beyond the unitarity limit at $\sim$100 TeV, and discuss the basic requirements for DM models in this regime. We explore the feasibility of detecting the annihilation signature, and the expected reach for UHDM with current and future Very-High-Energy (VHE; $>$ 100 GeV) $\gamma$-ray observatories. Specifically, we focus on three reference instruments: two Imaging Atmospheric Cherenkov Telescope arrays, modeled on VERITAS and CTA-North, and one Extended Air Shower array, motivated by HAWC. With reasonable assumptions on the instrument response functions and background rate, we find a set of UHDM parameters (mass and cross section) for which a $\gamma$-ray signature can be detected by the aforementioned observatories. We further compute the expected upper limits for each experiment. With realistic exposure times, the three instruments can probe DM across a wide mass range. At the lower end, it can still have a point-like cross section, while at higher masses the DM could have a geometric cross section, indicative of compositeness.

Published
2022
Full Text
View/download PDF

24. Search for Dark Matter Annihilation Signals in the H.E.S.S. Inner Galaxy Survey

Author

Abdalla, H., Aharonian, F., Becherini, Y., Rueda Ricarte, H., Ruiz-Velasco, E., Sahakian, V., Salzmann, H., Santangelo, A., Sasaki, M., Schüssler, F., Schutte, H. M., Schwanke, U., Senniappan, M., Berge, D., Shapopi, J. N. S., Sol, H., Specovius, A., Spencer, S., Stawarz, L., Stegmann, C., Steinmassl, S., Steppa, C., Takahashi, T., Tanaka, T., Bernlöhr, K., Terrier, R., Thorpe-Morgan, C., Tluczykont, M., Tsirou, M., Tsuji, N., Uchiyama, Y., van Eldik, C., Veh, J., Vink, J., Wagner, S. J., Bi, B., White, R., Wierzcholska, A., Wong, Yu Wun, Zacharias, M., Zargaryan, D., Zdziarski, A. A., Zech, A., Zhu, S. J., Zouari, S., Zywucka, N., Böttcher, M., H. E. S. S. Collaboration, Bolmont, J., de Bony de Lavergne, M., Brose, R., Brun, F., Cangemi, F., Benkhali, F. Ait, Caroff, S., Cerruti, M., Chand, T., Chen, A., Cotter, G., Damascene Mbarubucyeye, J., Devin, J., Djannati-Ataï, A., Dmytriiev, A., Doroshenko, V., Angüner, E. O., Egberts, K., Fiasson, A., Fichet de Clairfontaine, G., Fontaine, G., Funk, S., Gabici, S., Giavitto, G., Glawion, D., Glicenstein, J. F., Grondin, M.-H., Armand, C., Hinton, J. A., Hofmann, W., Holch, T. L., Holler, M., Horns, D., Huang, Zhiqiu, Jamrozy, M., Jankowsky, F., Kasai, E., Katarzynski, K., Ashkar, H., Katz, U., Khélifi, B., Klúzniak, W., Komin, Nu., Kosack, K., Kostunin, D., Lamanna, G., Lemoine-Goumard, M., Lenain, J.-P., Leuschner, F., Backes, M., Lohse, T., Luashvili, A., Lypova, I., Mackey, J., Malyshev, D., Marandon, V., Marchegiani, P., Martí-Devesa, G., Marx, R., Baghmanyan, V., Maurin, G., Meyer, M., Mitchell, A., Moderski, R., Montanari, A., Moulin, E., Muller, J., de Naurois, M., Niemiec, J., Noel, A. Priyana, Barbosa Martins, V., Ohm, S., Olivera-Nieto, L., de Ona Wilhelmi, Emma Maria, Ostrowski, M., Panny, S., Panter, M., Parsons, R. D., Peron, G., Poireau, V., Prokoph, H., Batzofin, R., Pühlhofer, G., Punch, M., Quirrenbach, A., Reichherzer, P., Reimer, A., Reimer, O., Renaud, M., Rieger, F., Rowell, G., Rudak, B., Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), H.E.S.S., High Energy Astrophys. & Astropart. Phys (API, FNWI), and H.E.S.S. Collaboration

Subjects
General Physics and Astronomy, FOS: Physical sciences, mass [dark matter], dark matter: density, GeV, annihilation [dark matter], VHE, cross section: annihilation, HESS, TeV, ddc:530, High Energy Astrophysical Phenomena (astro-ph.HE), dark matter: mass, density [dark matter], central region, dark matter: annihilation, Navarro-Frenk-White profile, annihilation [cross section], Cherenkov counter, gamma ray, HESS - Abteilung Hinton, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], signature
Abstract

Physical review letters 129(11), 111101 (2022). doi:10.1103/PhysRevLett.129.111101, The central region of the Milky Way is one of the foremost locations to look for dark matter (DM) signatures. We report the first results on a search for DM particle annihilation signals using new observations from an unprecedented $γ$-ray survey of the Galactic Center (GC) region, i.e., the Inner Galaxy Survey, at very high energies (≳100 GeV) performed with the H.E.S.S. array of five ground-based Cherenkov telescopes. No significant $γ$-ray excess is found in the search region of the 2014–2020 dataset and a profile likelihood ratio analysis is carried out to set exclusion limits on the annihilation cross section $⟨σv⟩$. Assuming Einasto and Navarro-Frenk-White (NFW) DM density profiles at the GC, these constraints are the strongest obtained so far in the TeV DM mass range. For the Einasto profile, the constraints reach $⟨σv⟩$ values of 3.7×10$^{-26}$ cm$^3$ s$^{-1}$ for 1.5 TeV DM mass in the W$^+$W$^-$ annihilation channel, and 1.2×10$^{-26}$ cm$^3$ s$^{-1}$ for 0.7 TeV DM mass in the $τ^+τ^-$ annihilation channel. With the H.E.S.S. Inner Galaxy Survey, ground-based $γ$-ray observations thus probe $⟨σv⟩$ values expected from thermal-relic annihilating TeV DM particles., Published by APS, College Park, Md.

Published
2022
Full Text
View/download PDF

25. Mirror production for the Cherenkov telescopes of the ASTRI mini-array and the MST project for the Cherenkov Telescope Array

Author

Nicola La Palombara, Giorgia Sironi, Enrico Giro, Salvatore Scuderi, Rodolfo Canestrari, Simone Iovenitti, Markus Garczarczyk, Maria Krause, Sebastian Diebold, Rachele Millul, Fabio Marioni, Nadia Missaglia, Matteo Redaelli, Giuseppe Valsecchi, Fabio Zocchi, Adelfio Zanoni, Giovanni Pareschi, ITA, and DEU

Subjects
Cherenkov Telescope Array, cold-slumping technology, Spherical lenses, FOS: Physical sciences, quality: monitoring, fabrication, hot-slumpìing technology, quality assurance, Reflectivity, monitoring [quality], Atmospheric Cherenkov telescopes, ddc:530, Solids, ASTRI, mirror, Instrumentation and Methods for Astrophysics (astro-ph.IM), Instrumentation, activity report, CTA, Mechanical Engineering, Glasses, coating, Astronomy and Astrophysics, Point spread functions, Electronic, Optical and Magnetic Materials, Mirrors, Cherenkov counter, Space and Planetary Science, Control and Systems Engineering, dual mirror, Astrophysics - Instrumentation and Methods for Astrophysics, performance, Telescopes, Aluminum
Abstract

SPIE Optical Engineering + Applications, San Diego, United States, 11 Aug 2019 - 15 Aug 2019; Journal of astronomical telescopes, instruments, and systems 8, 014005 (2022). doi:10.1117/1.JATIS.8.1.014005, The Cherenkov Telescope Array (CTA) is the next ground-based γ-ray observatory in the TeV γ-ray spectral region operating with the Imaging Atmospheric Cherenkov Technique. It is based on almost 70 telescopes of different class diameters - LST, MST and SST of 23, 12, and 4 m, respectively - to be installed in two sites in the two hemispheres (at La Palma, Canary Islands, and near Paranal, Chile). Several thousands of reflecting mirror tiles larger than 1 m$^2$ will be produced for realizing the segmented primary mirrors of a so large number of telescopes. Almost in parallel, the ASTRI Mini-Array (MA) is being implemented in Tenerife (Canary Islands), composed of nine 4 m diameter dual-mirror Cherenkov telescopes (very similar to the SSTs). We completed the mirror production for all nine telescopes of the ASTRI MA and two MST telescopes (400 segments in total) using the cold glass slumping replication technology. The results related to the quality achieved with a so large-scale production are presented, also discussing the adopted testing methods and approaches. They will be very useful for the adoption and optimization of the quality assurance process for the huge production (almost 3000 m$^2$ of reflecting surface) of the MST and SST CTA telescopes., Published by SPIE, [Bellingham, Wash.]

Published
2022

26. Hybrid cosmic ray measurements using the IceAct telescopes in coincidence with the IceCube and IceTop detectors

Author

Bretz, T., Do, G., Hewitt, J. W., Maslowski, F., Paul, L., Plum, M., Rehbein, F., Johannes Schäfer, Schaufel, M., Zink, A., Abbasi, R., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Alispach, C., Alves, A. A., Amin, N. M., An, R., Andeen, K., Anderson, T., Anton, G., Argüelles, C., Ashida, Y., Axani, S., Bai, X., Balagopal, A. V., Barbano, A., Barwick, S. W., Bastian, B., Basu, V., Baur, S., Bay, R., Beatty, J. J., Becker, K. -H, Becker Tjus, J., Bellenghi, C., Benzvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Boddenberg, M., Bontempo, F., Borowka, J., Böser, S., Botner, O., Böttcher, J., Bourbeau, E., Bradascio, F., Braun, J., Bron, S., Brostean-Kaiser, J., Browne, S., Burgman, A., Burley, R. T., Busse, R. S., Campana, M. A., Carnie-Bronca, E. G., Chen, C., Chirkin, D., Choi, K., Clark, B. A., Clark, K., Classen, L., Coleman, A., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dappen, C., Dave, P., Clercq, C., Delaunay, J. J., Dembinski, H., Deoskar, K., Ridder, S., Desai, A., Desiati, P., Vries, K. D., Wasseige, G., With, M., Deyoung, T., Dharani, S., Diaz, A., Díaz-Vélez, J. C., Dittmer, M., Dujmovic, H., Dunkman, M., Duvernois, M. A., Dvorak, E., Ehrhardt, T., Eller, P., Engel, R., Erpenbeck, H., Evans, J., Evenson, P. A., Fan, K. L., Fazely, A. R., Fiedlschuster, S., Fienberg, A. T., Filimonov, K., Finley, C., Fischer, L., Fox, D., Franckowiak, A., Friedman, E., Fritz, A., Fürst, P., Gaisser, T. K., Gallagher, J., Ganster, E., Garcia, A., Garrappa, S., Gerhardt, L., Ghadimi, A., Glaser, C., Glauch, T., Glüsenkamp, T., Goldschmidt, A., Gonzalez, J. G., Goswami, S., Grant, D., Grégoire, T., Griswold, S., Gündüz, M., Günther, C., Haack, C., Hallgren, A., Halliday, R., Halve, L., Halzen, F., Ha Minh, M., Hanson, K., Hardin, J., Harnisch, A. A., Haungs, A., Hauser, S., Hebecker, D., Helbing, K., Henningsen, F., Hettinger, E. C., Hickford, S., Hignight, J., Hill, C., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Huber, T., Hultqvist, K., Hünnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jansson, M., Japaridze, G. S., Jeong, M., Jones, B. J. P., Kang, D., Kang, W., Kang, X., Kappes, A., Kappesser, D., Karg, T., Karl, M., Karle, A., Katz, U., Kauer, M., Kellermann, M., Kelley, J. L., Kheirandish, A., Kin, K., Kintscher, T., Kiryluk, J., Klein, S. R., Koirala, R., Kolanoski, H., Kontrimas, T., Köpke, L., Kopper, C., Kopper, S., Koskinen, D. J., Koundal, P., Kovacevich, M., Kowalski, M., Kozynets, T., Kun, E., Kurahashi, N., Lad, N., Lagunas Gualda, C., Lanfranchi, J. L., Larson, M. J., Lauber, F., Lazar, J. P., Lee, J. W., Leonard, K., Leszczyńska, A., Li, Y., Lincetto, M., Liu, Q. R., Liubarska, M., Lohfink, E., Lozano Mariscal, C. J., Lu, L., Lucarelli, F., Ludwig, A., Luszczak, W., Lyu, Y., Ma, W. Y., Madsen, J., Mahn, K. B. M., Makino, Y., Mancina, S., Mariş, I. C., Maruyama, R., Mase, K., Mcelroy, T., Mcnally, F., Mead, J. V., Meagher, K., Medina, A., Meier, M., Meighen-Berger, S., Micallef, J., Mockler, D., Montaruli, T., Moore, R. W., Morse, R., Moulai, M., Naab, R., Nagai, R., Naumann, U., Necker, J., Nguyên, L. V., Niederhausen, H., Nisa, M. U., Nowicki, S. C., Nygren, D. R., Obertacke Pollmann, A., Oehler, M., Olivas, A., O’sullivan, E., Pandya, H., Pankova, D. V., Park, N., Parker, G. K., Paudel, E. N., Pérez Los Heros, C., Peters, L., Peterson, J., Philippen, S., Pieloth, D., Pieper, S., Pittermann, M., Pizzuto, A., Popovych, Y., Porcelli, A., Prado Rodriguez, M., Price, P. B., Pries, B., Przybylski, G. T., Raab, C., Raissi, A., Rameez, M., Rawlins, K., Rea, I. C., Rehman, A., Reichherzer, P., Reimann, R., Renzi, G., Resconi, E., Reusch, S., Rhode, W., Richman, M., Riedel, B., Roberts, E. J., Robertson, S., Roellinghoff, G., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk Cantu, D., Safa, I., Saffer, J., Sanchez Herrera, S. E., Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Scharf, M., Schieler, H., Schindler, S., Schlunder, P., Schmidt, T., Schneider, A., Schneider, J., Schröder, F. G., Schumacher, L., Schwefer, G., Sclafani, S., Seckel, D., Seunarine, S., Sharma, A., Shefali, S., Silva, M., Skrzypek, B., Smithers, B., Snihur, R., Soedingrekso, J., Soldin, D., Spannfellner, C., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stürwald, T., Stuttard, T., Sullivan, G. W., Taboada, I., Tenholt, F., Ter-Antonyan, S., Tilav, S., Tischbein, F., Tollefson, K., Tomankova, L., Tönnis, C., Toscano, S., Tosi, D., Trettin, A., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Twagirayezu, J. P., Ty, B., Unland Elorrieta, M. A., Valtonen-Mattila, N., Vandenbroucke, J., Eijndhoven, N., Vannerom, D., Santen, J., Verpoest, S., Vraeghe, M., Walck, C., Watson, T. B., Weaver, C., Weigel, P., Weindl, A., Weiss, M. J., Weldert, J., Wendt, C., Werthebach, J., Weyrauch, M., Whitehorn, N., Wiebusch, C. H., Williams, D. R., Wolf, M., Woschnagg, K., Wrede, G., Wulff, J., Xu, X. W., Xu, Y., Yanez, J. P., Yoshida, S., Yu, S., Yuan, T., and Zhang, Z.

Subjects
detector: performance, Physics::Instrumentation and Detectors, air, Astrophysics::High Energy Astrophysical Phenomena, pole, Cosmic ray, Coincidence, IceCube Neutrino Observatory, law.invention, Telescope, energy: threshold, Silicon photomultiplier, surface [IceCube], law, pixel, Cherenkov [radiation], site, TeV, photomultiplier: silicon, ddc:530, Cherenkov radiation, Physics, hybrid, performance [detector], Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, imaging, showers, IceCube: surface, threshold [energy], radiation: Cherenkov, observatory, Cherenkov counter, cosmic radiation, atmosphere, silicon [photomultiplier], Neutrino, statistical
Abstract

37th International Cosmic Ray Conference, ICRC 2021, Berlin, Germany, 15 Jul 2021 - 22 Jul 2021; Proceedings of Science 395, 276 (2022). doi:10.22323/1.395.0276 special issue: "37th International Cosmic Ray Conference : ICRC2021 : 12-23 July 2021 : Berlin, Germany - Online / Editorial Board: Alexander Kappes, Institut für Kernphysik, Westfälische Wilhelms-Universität Münster, D-48149 Münster, Germany ; Bianca Keilhauer, Karlsruhe Institute of Technology, Institute for Astroparticle Physics (IAP)", Published by SISSA, Trieste

Published
2022

27. Muon detection in electron-positron annihilation for muon collider studies

Author

N. Amapane, M. Antonelli, F. Anulli, G. Ballerini, L. Bandiera, N. Bartosik, M. Bauce, A. Bertolin, C. Biino, O.R. Blanco-García, M. Boscolo, C. Brizzolari, A. Cappati, F. Casaburo, M. Casarsa, G. Cavoto, G. Cesarini, F. Collamati, G. Cotto, C. Curatolo, R. Di Nardo, F. Gonella, S. Hoh, M. Iafrati, F. Iacoangeli, B. Kiani, R. Li Voti, D. Lucchesi, V. Mascagna, A. Paccagnella, N. Pastrone, J. Pazzini, M. Pelliccioni, B. Ponzio, M. Prest, M. Ricci, S. Rosati, R. Rossin, M. Rotondo, O. Sans Planell, L. Sestini, M. Soldani, A. Triossi, E. Vallazza, S. Ventura, M. Zanetti, Institut Pluridisciplinaire Hubert Curien (IPHC), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, CERN Lab, Physics::Instrumentation and Detectors, tungsten, muon collider, muon detection, FOS: Physical sciences, muon: particle identification, electron positron: annihilation, Muon Collider, muon: storage ring, 7. Clean energy, 01 natural sciences, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Detectors and Experimental Techniques, 010306 general physics, physics.ins-det, Instrumentation, activity report, 010308 nuclear & particles physics, Cherenkov detectors, Instrumentation and Detectors (physics.ins-det), muon: production, Cherenkov counter, Physics::Accelerator Physics, High Energy Physics::Experiment, performance
Abstract

The investigation of the energy frontier in physics requires novel concepts for future colliders. The idea of a muon collider is very appealing since it would allow to study particle collisions at up to tens of TeV energy, while offering a cleaner experimental environment with respect to hadronic colliders. One key element in the muon collider design is the low-emittance muon production. Recently, the Low EMittance Muon Accelerator (LEMMA) collaboration has explored the muon pair production close to its kinematic threshold by annihilating 45 GeV positrons with electrons in a low Z material target. In this configuration, muons are emerging from the target with a naturally low-emittance. In this paper we describe the performance of a system, to study this production mechanism, that consists in several segmented absorbers with alternating active layers composed of fast Cherenkov detectors together with a muon identification technique based on this detector. Passive layers were made of tungsten. We collected data corresponding to muon and electron beams produced at the H2 line in the North Area of the European Organization for Nuclear Research (CERN) in September 2018. The investigation of the energy frontier in physics requires novel concepts for future colliders. The idea of a muon collider is very appealing since it would allow to study particle collisions at up to tens of TeV energy, while offering a cleaner experimental environment with respect to hadronic colliders. One key element in the muon collider design is the low-emittance muon production. Recently,the Low EMittance Muon Accelerator (LEMMA) collaboration has explored the muon pair production close to its kinematic threshold by annihilating 45 GeV positrons with electrons in a low Z material target. In this configuration, muons are emerging from the target with a naturally low-emittance. In this paper we describe the performance of a system, to study this production mechanism, that consists in several segmented absorbers with alternating active layers composed of fast Cherenkov detectors together with a muon identification technique based on this detector. Passive layers were made of tungsten. We collected data corresponding to muon and electron beams produced at the H2 line in the North Area of the European Organization for Nuclear Research (CERN) in September 2018.

Published
2022

28. Towards the ultimate reach of current Imaging Atmospheric Cherenkov Telescopes to TeV Dark Matter

Author

Montanari, Alessandro, Moulin, Emmanuel, Rodd, Nicholas L., HEP, INSPIRE, Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay

Subjects
Cherenkov Telescope Array, ANTARES, scale: TeV, relic density, background, Wino, halo, imaging, neutrino: final state, sensitivity, observatory, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Cherenkov counter, annihilation, gamma ray, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], mass: thermal, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Higgsino: dark matter
Abstract

International audience; Indirect detection opens a unique window for probing thermal dark matter (DM): the same annihilation process that determined the relic abundance in the early Universe drives the present day astrophysical signal. While TeV-scale particles weakly coupled to the Standard Model face undoubted challenges from decades of null searches, the scenario remains compelling, and simple realizations such as Higgsino DM remain largely unexplored. The fate of such scenarios could be determined by gamma-ray observations of the centre of the Milky Way with Imaging Atmospheric Cherenkov Telescopes (IACTs). We consider the ultimate sensitivity of current IACTs to a broad range of TeV-scale DM candidates - including specific ones such as the Wino, Higgsino, and Quintuplet. To do so, we use realistic mock H.E.S.S.-like observations of the inner Milky Way halo, and provide a careful assessment of the impact of recent Milky Way mass modeling, instrumental and astrophysical background uncertainties in the Galactic Center region, and the theoretical uncertainty on the predicted signal. We find that the dominant systematic for IACT searches in the inner Galaxy is the unknown distribution of DM in that region, however, beyond this the searches are currently statistically dominated indicating a continued benefit from more observations. For two-body final states at $1~{\rm TeV}$, we find a H.E.S.S.-like observatory is sensitive to $\langle \sigma v \rangle \sim 3 \times 10^{-26}-4 \times 10^{-25}~{\rm cm}^3{\rm s}^{-1}$, except for neutrino final states, although we find results competitive with ANTARES. In addition, the thermal masses for the Wino and Quintuplet can be probed; the Higgsino continues to be out of reach by at least a factor of a few. Our conclusions are also directly relevant to the next generation Cherenkov Telescope Array, which remains well positioned to be the discovery instrument for thermal DM.

Published
2022

29. toise: a framework to describe the performance of high-energy neutrino detectors

Author

Santen, Jakob van, Clark, Brian A., Halliday, Rob, Hallmann, Steffen, and Nelles, Anna

Subjects
detector: performance, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, energy resolution, FOS: Physical sciences, programming, Software architectures (event data models, frameworks and databases), ddc:530, ddc:610, detector [neutrino], Monte Carlo, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Mathematical Physics, radio wave, performance [detector], sensitivity, flux, neutrino: detector, Cherenkov counter, angular resolution, Analysis and statistical methods, High Energy Physics::Experiment, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Journal of Instrumentation 17(08), T08009 (2022). doi:10.1088/1748-0221/17/08/T08009, Neutrinos offer a unique window to the distant, high-energy universe. Several next-generation instruments are being designed and proposed to characterize the flux of TeV–EeV neutrinos. The projected physics reach of the detectors is often quantified with simulation studies. However, a complete Monte Carlo estimate of detector performance is costly from a computational perspective, restricting the number of detector configurations considered when designing the instruments. In this paper, we present a new Python-based software framework, toise, which forecasts the performance of a high-energy neutrino detector using parameterizations of the detector performance, such as the effective areas, angular and energy resolutions, etc. The framework can be used to forecast performance of a variety of physics analyses, including sensitivities to diffuse fluxes of neutrinos and sensitivity to both transient and steady state point sources. This parameterized approach reduces the need for extensive simulation studies in order to estimate detector performance, and allows the user to study the influence of single performance metrics, like the angular resolution, in isolation. The framework is designed to allow for multiple detector components, each with different responses and exposure times, and supports paramterization of both optical- and radio-Cherenkov (Askaryan) neutrino telescopes. In the paper, we describe the mathematical concepts behind toise and introduce the reader to the use of the framework., Published by Inst. of Physics, London

Published
2022
Full Text
View/download PDF

30. Cosmic-Ray Studies with the Surface Instrumentation of IceCube

Author

Haungs, A., Abbasi, R., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Alispach, C., Alves, A. A., Amin, N. M., An, R., Andeen, K., Anderson, T., Anton, G., Argüelles, C., Ashida, Y., Axani, S., Bai, X., Balagopal, A. V., Barbano, A., Barwick, S. W., Bastian, B., Basu, V., Baur, S., Bay, R., Beatty, J. J., Becker, K. -H, Becker Tjus, J., Bellenghi, C., Benzvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Boddenberg, M., Bontempo, F., Borowka, J., Böser, S., Botner, O., Böttcher, J., Bourbeau, E., Bradascio, F., Braun, J., Bron, S., Brostean-Kaiser, J., Browne, S., Burgman, A., Burley, R. T., Busse, R. S., Campana, M. A., Carnie-Bronca, E. G., Chen, C., Chirkin, D., Choi, K., Clark, B. A., Clark, K., Classen, L., Coleman, A., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dappen, C., Dave, P., Clercq, C., Delaunay, J. J., Dembinski, H., Deoskar, K., Ridder, S., Desai, A., Desiati, P., Vries, K. D., Wasseige, G., With, M., Deyoung, T., Dharani, S., Diaz, A., Díaz-Vélez, J. C., Dittmer, M., Dujmovic, H., Dunkman, M., Duvernois, M. A., Dvorak, E., Ehrhardt, T., Eller, P., Engel, R., Erpenbeck, H., Evans, J., Evenson, P. A., Fan, K. L., Fazely, A. R., Fiedlschuster, S., Fienberg, A. T., Filimonov, K., Finley, C., Fischer, L., Fox, D., Franckowiak, A., Friedman, E., Fritz, A., Fürst, P., Gaisser, T. K., Gallagher, J., Ganster, E., Garcia, A., Garrappa, S., Gerhardt, L., Ghadimi, A., Glaser, C., Glauch, T., Glüsenkamp, T., Goldschmidt, A., Gonzalez, J. G., Goswami, S., Grant, D., Grégoire, T., Griswold, S., Gündüz, M., Günther, C., Haack, C., Hallgren, A., Halliday, R., Halve, L., Halzen, F., Ha Minh, M., Hanson, K., Hardin, J., Harnisch, A. A., Hauser, S., Hebecker, D., Helbing, K., Henningsen, F., Hettinger, E. C., Hickford, S., Hignight, J., Hill, C., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Huber, T., Hultqvist, K., Hünnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jansson, M., Japaridze, G. S., Jeong, M., Jones, B. J. P., Kang, D., Kang, W., Kang, X., Kappes, A., Kappesser, D., Karg, T., Karl, M., Karle, A., Katz, U., Kauer, M., Kellermann, M., Kelley, J. L., Kheirandish, A., Kin, K., Kintscher, T., Kiryluk, J., Klein, S. R., Koirala, R., Kolanoski, H., Kontrimas, T., Köpke, L., Kopper, C., Kopper, S., Koskinen, D. J., Koundal, P., Kovacevich, M., Kowalski, M., Kozynets, T., Kun, E., Kurahashi, N., Lad, N., Lagunas Gualda, C., Lanfranchi, J. L., Larson, M. J., Lauber, F., Lazar, J. P., Lee, J. W., Leonard, K., Leszczyńska, A., Li, Y., Lincetto, M., Liu, Q. R., Liubarska, M., Lohfink, E., Lozano Mariscal, C. J., Lu, L., Lucarelli, F., Ludwig, A., Luszczak, W., Lyu, Y., Ma, W. Y., Madsen, J., Mahn, K. B. M., Makino, Y., Mancina, S., Mariş, I. C., Maruyama, R., Mase, K., Mcelroy, T., Mcnally, F., Mead, J. V., Meagher, K., Medina, A., Meier, M., Meighen-Berger, S., Micallef, J., Mockler, D., Teresa Montaruli, Moore, R. W., Morse, R., Moulai, M., Naab, R., Nagai, R., Naumann, U., Necker, J., Nguyên, L. V., Niederhausen, H., Nisa, M. U., Nowicki, S. C., Nygren, D. R., Obertacke Pollmann, A., Oehler, M., Olivas, A., O’sullivan, E., Pandya, H., Pankova, D. V., Park, N., Parker, G. K., Paudel, E. N., Paul, L., Pérez Los Heros, C., Peters, L., Peterson, J., Philippen, S., Pieloth, D., Pieper, S., Pittermann, M., Pizzuto, A., Plum, M., Popovych, Y., Porcelli, A., Prado Rodriguez, M., Price, P. B., Pries, B., Przybylski, G. T., Raab, C., Raissi, A., Rameez, M., Rawlins, K., Rea, I. C., Rehman, A., Reichherzer, P., Reimann, R., Renzi, G., Resconi, E., Reusch, S., Rhode, W., Richman, M., Riedel, B., Roberts, E. J., Robertson, S., Roellinghoff, G., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk Cantu, D., Safa, I., Saffer, J., Sanchez Herrera, S. E., Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Scharf, M., Schaufel, M., Schieler, H., Schindler, S., Schlunder, P., Schmidt, T., Schneider, A., Schneider, J., Schröder, F. G., Schumacher, L., Schwefer, G., Sclafani, S., Seckel, D., Seunarine, S., Sharma, A., Shefali, S., Silva, M., Skrzypek, B., Smithers, B., Snihur, R., Soedingrekso, J., Soldin, D., Spannfellner, C., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stürwald, T., Stuttard, T., Sullivan, G. W., Taboada, I., Tenholt, F., Ter-Antonyan, S., Tilav, S., Tischbein, F., Tollefson, K., Tomankova, L., Tönnis, C., Toscano, S., Tosi, D., Trettin, A., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Twagirayezu, J. P., Ty, B., Unland Elorrieta, M. A., Valtonen-Mattila, N., Vandenbroucke, J., Eijndhoven, N., Vannerom, D., Santen, J., Verpoest, S., Vraeghe, M., Walck, C., Watson, T. B., Weaver, C., Weigel, P., Weindl, A., Weiss, M. J., Weldert, J., Wendt, C., Werthebach, J., Weyrauch, M., Whitehorn, N., Wiebusch, C. H., Williams, D. R., Wolf, M., Woschnagg, K., Wrede, G., Wulff, J., Xu, X. W., Xu, Y., Yanez, J. P., Yoshida, S., Yu, S., Yuan, T., and Zhang, Z.

Subjects
Physics::Instrumentation and Detectors, Cherenkov detector, air, Astrophysics::High Energy Astrophysical Phenomena, Instrumentation, ice, pole, FOS: Physical sciences, Cosmic ray, law.invention, surface [IceCube], surface [detector], law, muon, TeV, ddc:530, enhancement, Cherenkov radiation, scintillation counter, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Scintillation, showers: atmosphere, detector: surface, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Electromagnetic signal, IceCube: surface, Cherenkov counter, electromagnetic, cosmic radiation, statistics, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, atmosphere [showers]
Abstract

IceCube is a cubic-kilometer Cherenkov detector installed in deep ice at the geographic South Pole. IceCube's surface array, IceTop, measures the electromagnetic signal and mainly low-energy muons from extensive air showers above several 100 TeV primary energy, with shower bundles and high-energy muons detected by the in-ice detector IceCube. In combination, the in-ice detector and IceTop provide unique opportunities to study cosmic rays in detail with large statistics. This contribution summarizes recent results from these studies. In addition, the IceCube-Upgrade will include a considerable enhancement of the surface detector through the installation of scintillation detectors and radio antennas and possibly small air-Cherenkov telescopes. We will discuss the results of the prototype detectors installed at the South Pole and the prospects of this enhancement as well as the surface array planned for IceCube-Gen2., Comment: Presented at the 37th International Cosmic Ray Conference (ICRC 2021). See arXiv:2107.06966 for all IceCube contributions

Published
2022
Full Text
View/download PDF

31. Combined searches for dark matter in dwarf spheroidal galaxies observed with the MAGIC telescopes, including new data from Coma Berenices and Draco

Author

MAGIC Collaboration, Acciari, V., Ansoldi, S., Antonelli, L., Arbet Engels, A., Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., Barres de Almeida, U., Barrio, J., Batković, I., Becerra González, J., Bednarek, W., Bellizzi, L., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bökenkamp, H., Bonnoli, G., Bošnjak, Ž., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S., Colombo, E., Contreras, J., Cortina, J., Covino, S., D'Amico, G., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., 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., Fallah Ramazani, V., Fattorini, A., Fonseca, M., Font, L., Fruck, C., Fukami, S., García López, R., Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Green, J., Green, D., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., Hütten, M., Inada, T., Ishio, K., Iwamura, Y., Jiménez, I., Jormanainen, J., Jouvin, L., Karjalainen, M., 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., Machado de Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Menchiari, S., Mender, S., Mićanović, S., Miceli, D., Miener, T., Miranda, J., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J., Pavletić, L., Peñil, P., Persic, M., Pihet, M., Prada Moroni, P., Prandini, E., Priyadarshi, C., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Saturni, F., Schleicher, B., Schmidt, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Spolon, A., Stamerra, A., Strišković, J., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Takeishi, R., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Ventura, S., Verguilov, V., Vigorito, C., Vitale, V., Vovk, I., Will, M., Wunderlich, C., Zarić, D., Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), MAGIC, Département de Physique des Particules (ex SPP) (DPP), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Academy of Finland, German Research Foundation, European Commission, Ministerio de Economía y Competitividad (España), and Japan Society for the Promotion of Science

Subjects
Astrophysics and Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Dark Matter, Indirect searches, Gamma Rays, Dwarf spheroidal galaxies, Imaging Atmospheric Cherenkov, Telescopes, 01 natural sciences, WIMP: annihilation, Imaging Atmospheric Cherenkov Telescopes, 0103 physical sciences, TeV, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, 010308 nuclear & particles physics, imaging, Dark Matter Indirect searches Gamma Rays Dwarf spheroidal galaxies Imaging Atmospheric Cherenkov Telescopes, Astronomy and Astrophysics, dark matter: annihilation, sensitivity, MAGIC, gamma ray: emission, Cherenkov counter, Space and Planetary Science, quality, Física nuclear, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

T.M. Collaboration, V.A. Acciari, S. Ansoldi et al., Milky Way dwarf spheroidal galaxies (dSphs) are among the best candidates to search for signals of dark matter annihilation with Imaging Atmospheric Cherenkov Telescopes, given their high mass-to-light ratios and the fact that they are free of astrophysical gamma-ray emitting sources. Since 2011, MAGIC has performed a multi-year observation program in search for Weakly Interacting Massive Particles (WIMPs) in dSphs. Results on the observations of Segue 1 and Ursa Major II dSphs have already been published and include some of the most stringent upper limits (ULs) on the velocity- averaged cross-section ⟨σannv⟩ of WIMP annihilation from observations of dSphs. In this work, we report on the analyses of 52.1 h of data of Draco dSph and 49.5 h of Coma Berenices dSph observed with the MAGIC telescopes in 2018 and in 2019 respectively. No hint of a signal has been detected from either of these targets and new constraints on the ⟨σannv⟩ of WIMP candidates have been derived. In order to improve the sensitivity of the search and reduce the effect of the systematic uncertainties due to the J-factor estimates, we have combined the data of all dSphs observed with the MAGIC telescopes. Using 354.3 h of dSphs good quality data, 95% CL ULs on ⟨σannv⟩ have been obtained for 9 annihilation channels. For most of the channels, these results reach values of the order of 10−24 cm3/s at ∼1 TeV and are the most stringent limits obtained with the MAGIC telescopes so far., he financial support of the German BMBF, MPG and HGF; the Italian INFN and INAF; the Swiss National Fund SNF; the ERDF under the Spanish Ministerio de Ciencia e Innovación (MICINN) (PID2019-104114RB-C31, PID2019-104114RB-C32, PID2019-104114RB-C33, PID2019-105510GB-C31, PID2019-107847RB-C41, PID2019-107847RB-C42, PID2019-107988GB-C22); the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-400/18.12.2020 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia ‘‘Severo Ochoa’’ (SEV-2016-0588, CEX2019-000920-S), the Unidad de Excelencia ‘‘María de Maeztu’’ (CEX2019-000918-M, MDM-2015-0509-18-2) and by the CERCA program of the Generalitat de Catalunya; by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02; by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3; the Polish National Research Centre grant UMO- 2016/22/M/ST9/00382; and by the Brazilian MCTIC, CNPq and FAPERJ. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 754510.

Published
2022

35. A tidal disruption event coincident with a high-energy neutrino

Author

Yuhan Yao, Eric C. Bellm, V. Brinnel, Anna Franckowiak, Tomas Ahumada, Mansi M. Kasliwal, Mickael Rigault, Erica Hammerstein, Leo Singer, César Rojas-Bravo, Ashish Mahabal, Albert K. H. Kong, Patrick A. Woudt, Jesper Sollerman, Ariel Goobar, Maayane T. Soumagnac, Andrew Drake, Charlotte Ward, Avishay Gal-Yam, George Helou, Kirsty Taggart, Jannis Necker, Thomas Kupfer, Ryan J. Foley, Markus Böttcher, S. Garrappa, Itai Sfaradi, Assaf Horesh, Frank J. Masci, Tiara Hung, Simeon Reusch, Sjoert van Velzen, Daniel Stern, Rob Fender, Ben Rusholme, Russ R. Laher, J. V. Santen, Igor Andreoni, Hector P. Rodriguez, Suvi Gezari, Marek Kowalski, Michael Bietenholz, V. Zach Golkhou, Justin Belicki, Daniel A. Perley, Michael Feeney, Michael W. Coughlin, Rick Burruss, Sara Frederick, James Miller-Jones, Virginia Cunningham, David L. Shupe, Robert Stein, Glennys R. Farrar, Charles D. Kilpatrick, S. Bradley Cenko, Jakob Nordin, Matthew J. Graham, Laboratoire de Physique de Clermont (LPC), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA)

Subjects
electron, 010504 meteorology & atmospheric sciences, neutrino: energy: high, Energy flux, Flux, photon: thermal, Astrophysics, pi: production, 01 natural sciences, Astrophysics - high energy astrophysical phenomena, neutrino: flux, IceCube, particle: acceleration, ultraviolet, black hole, p: accelerator, site, optical, energy: flux, 010303 astronomy & astrophysics, QB, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), radio wave, education.field_of_study, COSMIC cancer database, cross section, p p, black body, Neutrino, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Population, interaction, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, GLAST, jet: relativistic, neutrino: production, X-ray, Tidal disruption event, bolometer, neutrino: spectrum, 0103 physical sciences, cosmic radiation: UHE, education, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Photosphere, synchrotron radiation, Astronomy and Astrophysics, Doppler effect, Cherenkov counter, electromagnetic, gamma ray, 13. Climate action, star: mass, neutrino: oscillation, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Cosmic neutrinos provide a unique window into the otherwise-hidden mechanism of particle acceleration in astrophysical objects. A flux of high-energy neutrinos was discovered in 2013, and the IceCube Collaboration recently reported the likely association of one high-energy neutrino with a flare from the relativistic jet of an active galaxy pointed towards the Earth. However a combined analysis of many similar active galaxies revealed no excess from the broader population, leaving the vast majority of the cosmic neutrino flux unexplained. Here we present the likely association of a radio-emitting tidal disruption event, AT2019dsg, with a second high-energy neutrino. AT2019dsg was identified as part of our systematic search for optical counterparts to high-energy neutrinos with the Zwicky Transient Facility. The probability of finding any coincident radio-emitting tidal disruption event by chance is 0.5%, while the probability of finding one as bright in bolometric energy flux as AT2019dsg is 0.2%. Our electromagnetic observations can be explained through a multi-zone model, with radio analysis revealing a central engine, embedded in a UV photosphere, that powers an extended synchrotron-emitting outflow. This provides an ideal site for PeV neutrino production. Assuming that the association is genuine, our observations suggest that tidal disruption events with mildly-relativistic outflows contribute to the cosmic neutrino flux., Comment: Title and text modified during journal review. Version accepted for publication in Nature Astronomy

Published
2021

36. Nuclearite search with ANTARES

Author

G. E. Păvălaş, M. Bouta, Yahya Tayalati, J. Brunner, A. Moussa, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and ANTARES

Subjects
Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, nonrelativistic, Particle tracking detectors, 0103 physical sciences, Cherenkov, 14. Life underwater, Neutrino detectors, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), matter: strangeness, Mathematical Physics, black body: radiation, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), quark: matter, radiation: emission, ANTARES, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Trigger detectors, neutrino: detector, Cherenkov counter, Partickle tracking detectors (Solid-state detectors), High Energy Physics::Experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The ANTARES detector is a Cherenkov underwater neutrino telescope operating in the Mediterranean Sea. Its construction was completed in 2008. Even though optimised for the search of cosmic neutrinos, this telescope is also sensitive to nuclearites (massive nuggets of strange quark matter) trough the black body radiation emitted along their path. We discuss here the possible detection of non-relativistic down-going nuclearites with the ANTARES telescope and present the results of an analysis using data collected from 2009 till 2017., 5 pages, 5 figures, VLVNT2021

Published
2021

37. The H.E.S.S. Gravitational Wave Rapid Follow-up Program during O2 and O3

Author

Fabian Schüssler, Francois Brun, Patrick Reichherzer, S. Ohm, Halim Ashkar, Monica Seglar Arroyo, Sylvia Zhu, Ruslan Konno, Heike Prokoph, M. Füßling, Sylvia J. Zhu, Clemens Hoischen, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy de Physique des Particules (LAPP), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)

Subjects
data analysis method, neutron star: binary, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, VHE [gamma ray], FOS: Physical sciences, burst [gamma ray], absorption: effect, Field of view, binary [neutron star], effect [absorption], gamma ray: burst, 01 natural sciences, emission [gravitational radiation], binary: coalescence, HESS, 0103 physical sciences, Astronomical interferometer, binary [black hole], ddc:530, High Energy Stereoscopic System, LIGO, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gravitational wave, Astronomy, Galaxy, Afterglow, Cherenkov counter, VIRGO, gamma ray: VHE, black hole: binary, Sky, gravitational radiation: emission, galaxy, gravitational radiation: localization, coalescence [binary], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], localization [gravitational radiation]
Abstract

37th International Cosmic Ray Conference, ICRC 2021, Berlin, online, Germany, 12 Jul 2021 - 23 Jul 2021; Proceedings of Science / International School for Advanced Studies (ICRC2021), 936 (2021). doi:10.22323/1.395.0936, Since 2015, the direct detection of Gravitational Waves (GWs) became possible with ground-based interferometers like LIGO and Virgo. GWs became the center of attention of the astronomical community and electromagnetic observatories took a particular interest in follow-up observations of such events. The main setback of these observations is the poor localization of GW events. In fact, GW localization uncertainties can span tens to hundreds of deg$^2$ the sky even with the advanced configurations of current GW interferometers. In this contribution, we present five follow-up strategies developed for the High Energy Stereoscopic System (H.E.S.S.) and assess their performances. We show how a 2D and 3D galaxy targeted search approach exploiting the integral probability inside the instruments field of view are best suited for medium field of view instruments like H.E.S.S. We also develop an automatic response scheme within the H.E.S.S. Transient Follow-up system that is optimized for fast response and is capable of responding promptly to all kind of GW alerts. GW events are filtered by the developed scheme and prompt and afterglow observations are automatically scheduled. The H.E.S.S. response latency to prompt alerts is measured to be less than 1 minute. With this continually optimized GW response scheme, H.E.S.S. scheduled several GW follow-up observations during the second and third LIGO/Virgo observation runs., Published by SISSA, Trieste

Published
2021

38. The first cross-calibration of Imaging Atmospheric Cherenkov Telescopes with a UAV-based airborne calibration platform

Author

Anthony M. Brown, Mathieu De Naurois, Jacques Muller, Laboratoire Leprince-Ringuet (LLR), and Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)

Subjects
Cherenkov Telescope Array, Astrophysics::High Energy Astrophysical Phenomena, measurement methods, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, IACT, calibration, 7. Clean energy, law.invention, Telescope, Wavelength, Cherenkov counter, law, HESS, Calibration, Environmental science, Sensitivity (control systems), detector: efficiency, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Energy (signal processing), Cherenkov radiation, performance, Remote sensing
Abstract

International audience; The Cherenkov Telescope Array (CTA) aims to have unprecedented accuracy and sensitivity, affording us the ability to understand the mysteries of the high energy universe. This unprecedented accuracy forces us to improve current calibration procedures, or indeed pioneer new techniques, to ensure the envisaged CTA performance. CTA will infer the energy of the gamma-rays it detects from the amount of Cherenkov radiation it observes. As such, the optical efficiency of the telescopes needs to be monitored, and its wavelength dependent degradation, which might be different for different telescope types, needs to be determined. Based on the results of a feasibility study, a novel cross-calibration method with an unmanned aerial vehicle (UAV) was tested on the H.E.S.S. telescope array, leading to the first cross-calibration of an Imaging Atmospheric Cherenkov Telescope (IACT) array with a single light source. In this talk, we present the cross-calibration results from a first test campaign in which we determine the relative optical efficiencies of the four HESS-I telescopes by successfully recording light from the UAV-mounted nanosecond pulsed UV light source simultaneously in all four telescopes. In addition, we show that the UAV data can be used to monitor the pointing accuracy at the level of at least tens of arcseconds and we give an outlook on other potential use cases of UAVs such as the monitoring of the atmospheric state.

Published
2021

39. Search for enhanced TeV gamma ray emission from Giant Molecular Clouds using H.E.S.S

Author

Abdalla, H., Aharonian, F., Ait Benkhali, F., Angüner, E. O., Arcaro, C., Armand, C., Armstrong, T., Ashkar, H., Backes, M., Baghmanyan, V., Barbosa Martins, V., Barnacka, A., Barnard, M., Batzofin, R., Becherini, Y., Berge, D., Bernlöhr, K., Bi, B., Böttcher, M., Boisson, C., Bolmont, J., Bony Lavergne, M., Breuhaus, M., Brose, R., Brun, F., Bulik, T., Bylund, T., Cangemi, F., Caroff, S., Casanova, S., Catalano, J., Chambery, P., Chand, T., Chen, A., Cotter, G., Curyło, M., Dalgleish, H., Damascene Mbarubucyeye, J., Davids, I. D., Davies, J., Devin, J., Djannati-Ataï, A., Dmytriiev, A., Donath, A., Doroshenko, V., Dreyer, L., Du Plessis, L., Duffy, C., Egberts, K., Einecke, S., Ernenwein, J. -P, Fegan, S., Feijen, K., Fiasson, A., Fichet Clairfontaine, G., Fontaine, G., Lott, F., Füßling, M., Funk, S., Gabici, S., Gallant, Y. A., Giavitto, G., Giunti, L., Glawion, D., Glicenstein, J. F., Grondin, M. -H, Hattingh, S., Haupt, M., Hermann, G., Hinton, J. A., Hofmann, W., Hoischen, C., Holch, T. L., Holler, M., Horns, D., Huang, Z., Huber, D., Hörbe, M., Jamrozy, M., Jankowsky, F., Joshi, V., Jung-Richardt, I., Kasai, E., Katarzyński, K., Katz, U., Khangulyan, D., Khélifi, B., Klepser, S., Kluźniak, W., Komin, Nu, Konno, R., Kosack, K., Kostunin, D., Kreter, M., Kukec Mezek, G., Kundu, A., Lamanna, G., Le Stum, S., Lemière, A., Lemoine-Goumard, M., Lenain, J. -P, Leuschner, F., Levy, C., Lohse, T., Luashvili, A., Lypova, I., Mackey, J., Majumdar, J., Malyshev, D., Marandon, V., Marchegiani, P., Marcowith, A., Mares, A., Martí-Devesa, G., Marx, R., Maurin, G., Meintjes, P. J., Meyer, M., Mitchell, A., Moderski, R., Mohrmann, L., Montanari, A., Moore, C., Morris, P., Moulin, E., Muller, J., Murach, T., Nakashima, K., Naurois, M., Nayerhoda, A., Ndiyavala, H., Niemiec, J., Priyana Noel, A., O Brien, P., Oberholzer, L., Ohm, S., Olivera-Nieto, L., Ona Wilhelmi, E., Ostrowski, M., Panny, S., Panter, M., Parsons, R. D., Peron, G., Pita, S., Poireau, V., Prokhorov, D. A., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Reichherzer, P., Reimer, A., Reimer, O., Remy, Q., Renaud, M., Reville, B., Rieger, F., Romoli, C., Rowell, G., Rudak, B., Rueda Ricarte, H., Ruiz-Velasco, E., Sahakian, V., Sailer, S., Salzmann, H., Sanchez, D. A., Santangelo, A., Sasaki, M., Johannes Schäfer, Schutte, H. M., Schwanke, U., Schüssler, F., Senniappan, M., Seyffert, A. S., Shapopi, J. N. S., Shiningayamwe, K., Simoni, R., Sinha, A., Sol, H., Spackman, H., Specovius, A., Spencer, S., Spir-Jacob, M., Stawarz, Ł., Steenkamp, R., Stegmann, C., Steinmassl, S., Steppa, C., Sun, L., Takahashi, T., Tanaka, T., Tavernier, T., Taylor, A. M., Terrier, R., Thiersen, J. H. E., Thorpe-Morgan, C., Tluczykont, M., Tomankova, L., Tsirou, M., Tsuji, N., Tuffs, R., Uchiyama, Y., Walt, D. J., Eldik, C., Rensburg, C., Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Vincent, P., Vink, J., Völk, H. J., Wagner, S. J., Watson, J., Werner, F., White, R., Wierzcholska, A., Wong, Y. W., Yassin, H., Yusafzai, A., Zacharias, M., Zanin, R., Zargaryan, D., Zdziarski, A. A., Zech, A., Zhu, S. J., Zmija, A., Zouari, S., Żywucka, N., Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), HESS, for the H.E.S.S. collaboration, and H.E.S.S.

Subjects
dimension: 3, accelerator, Astrophysics::High Energy Astrophysical Phenomena, Hadron, FOS: Physical sciences, Neutral pions, Cosmic ray, cosmic radiation: density, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cherenkov counter: atmosphere, 7. Clean energy, Dense gas, Imaging atmospheric Cherenkov telescopes, Clouds, Cosmology, Gamma rays, Cosmic ray interactions, diffuse emission, Giant molecular clouds, Ray density, TeV gamma-ray emission, VHE, Pion, TRACER, gas, HESS, TeV, cloud, matter: density, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Molecular cloud, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, model: hadronic, Galaxy, background: hadronic, Cherenkov counter, gamma ray: emission, 13. Climate action, cosmic radiation: galaxy, HESS - Abteilung Hinton, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Cosmic Ray (CR) interactions with the dense gas inside Giant Molecular Clouds (GMCs) produce neutral pions, which in turn decay into gamma rays. Thus, the gamma ray emission from GMCs is a direct tracer of the cosmic ray density and the matter density inside the clouds. Detection of enhanced TeV emission from GMCs, i.e., an emission significantly larger than what is expected from the average Galactic cosmic rays illuminating the cloud, can imply a variation in the local cosmic ray density, due to, for example, the presence of a recent accelerator in proximity to the cloud. Such gamma-ray observations can be crucial in probing the cosmic ray distribution across our Galaxy, but are complicated to perform with present generation Imaging Atmospheric Cherenkov Telescopes (IACTs). These studies require differentiating between the strong cosmic-ray induced background, the large scale diffuse emission, and the emission from the clouds, which is difficult to the small field of view of present generation IACTs. In this contribution, we use H.E.S.S. data collected over 16 years to search for TeV emission from GMCs in the inner molecular galacto-centric ring of our Galaxy. We implement a 3D FoV likelihood technique, and simultaneously model the hadronic background, the galactic diffuse emission and the emission expected from known VHE sources to probe for excess TeV gamma ray emission from GMCs., PoS: Proceedings of Science, 395, ISSN:1824-8039, Proceedings of 37th International Cosmic Ray Conference

Published
2021

40. Search for relativistic magnetic monopoles with ten years of the ANTARES detector data

Author

J. Brunner, J. Boumaaza, Abdelilah Moussa, Yahya Tayalati, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and ANTARES

Subjects
media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, magnetic monopole, Magnetic monopole, FOS: Physical sciences, magnetic field: galaxy, 01 natural sciences, symmetry breaking, High Energy Physics - Experiment, law.invention, photon: velocity, Telescope, Nuclear physics, High Energy Physics - Experiment (hep-ex), law, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Grand Unified Theory, Cherenkov, Symmetry breaking, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, numerical calculations, Instrumentation, Mathematical Physics, Cherenkov radiation, activity report, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, energy: high, ANTARES, 010308 nuclear & particles physics, Computer Science::Information Retrieval, Detector, Universe, Magnetic field, neutrino: detector, grand unified theory, Cherenkov counter, Speed of light, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], experimental results
Abstract

The presented study is an updated search for Magnetic Monopoles (MMs) using data taken with the ANTARES neutrino telescope over a period of 10 years (January 2008 to December 2017). In accordance with some Grand Unification Theories (GUT), MMs were created during the phase of symmetry breaking in the early Universe, and accelerated by inter-galactic magnetic fields. As a consequence of their high energy, they could cross the Earth and emit a significant signal in a Cherenkov-based telescope like ANTARES, for appropriate mass and velocity ranges. This analysis a new simulation of MMs taking into account the Kasama, Yang and Goldhaber (KYG) model for their cross section with matter. The results obtained for relativistic magnetic monopoles with β = v/c ⩾ 0.817, where v is the magnetic monopole velocity and c the speed of light in vacuum, are presented.

Published
2021

41. Fast simulation of Time-of-Flight detectors at the LHC

Author

Tom Sykora, Olivier Rousselle, Laboratoire Kastler Brossel (LKB [Collège de France]), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution))

Subjects
Cherenkov detector, Physics::Instrumentation and Detectors, QC1-999, Geant4, 02 engineering and technology, 01 natural sciences, programming, law.invention, 010309 optics, Optics, Python/Numba, law, 0103 physical sciences, numerical methods, 0202 electrical engineering, electronic engineering, information engineering, [INFO]Computer Science [cs], Nuclear Experiment, numerical calculations, Physics, 020203 distributed computing, Large Hadron Collider, business.industry, background, Detector, time-of-flight counter, ATLAS, HEP, Time of flight, Cherenkov counter, GEANT, business, performance
Abstract

International audience; The modelling of Cherenkov based detectors is traditionally done using Geant4 toolkit. In this work, we present another method based on Python programming language and Numba high performance compiler to speed up the simulation. As an example we take one of the Forward Proton Detectors at the CERN LHC - ATLAS Forward Proton (AFP) Time-of-Flight, which is used to reduce the background from multiple proton-proton collisions in soft and hard diffiractive events. We describe the technical details of the fast Cherenkov model of photon generation and transportation through the optical part of the ToF detector. The fast simulation is revealed to be about 200 times faster than the corresponding Geant4 simulation, and provides similar results concerning length and time distributions of photons. The study is meant as the first step in a construction of a building kit allowing creation of a fast simulation of an arbitrary shaped optical part of detectors.Key words: Geant4 / Python/Numba / HEP / Cherenkov detector

Published
2021

42. The GlueX DIRC detector.

Author

Barbosa, F., Bessuille, J., Chudakov, E., Dzhygadlo, R., Fanelli, C., Frye, J., Hardin, J., Kelsey, J., Patsyuk, M., Schwarz, C., Schwiening, J., Stevens, J., Shepherd, M., Whitlatch, T., and Williams, M.

Subjects
*CHERENKOV counters, *PHOTONS, *PROTOTYPES, *PARTICLES (Nuclear physics), *NUCLEAR counters
Abstract

The GlueX DIRC (Detection of Internally Reflected Cherenkov light) detector is being developed to upgrade the particle identification capabilities in the forward region of the GlueX experiment at Jefferson Lab. The GlueX DIRC will utilize four existing decommissioned BaBar DIRC bar boxes, which will be oriented to form a plane roughly 4 m away from the fixed target of the experiment. A new photon camera has been designed that is based on the SuperB FDIRC prototype. The full GlueX DIRC system will consist of two such cameras, with the first planned to be built and installed in 2017. We present the current status of the design and R&D, along with the future plans of the GlueX DIRC detector. [ABSTRACT FROM AUTHOR]

Published
2017
Full Text
View/download PDF

43. VHE gamma-ray observation of Crab Nebula with HAGAR telescope array

Author

S. S. Upadhya, Pijushpani Bhattacharjee, S. K. Rao, K. S. Gothe, G. C. Anupama, R. Srinivasan, P. R. Vishwanath, A. Shukla, T. P. Prabhu, R. J. Britto, B. K. Nagesh, B. S. Acharya, Lab Saha, Atreyee Sinha, B. B. Singh, V. R. Chitnis, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Cosmic ray, Cherenkov telescopes, cosmic background radiation, 01 natural sciences, law.invention, Telescope, law, VHE γ-rays, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Cherenkov radiation, Analysis method, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Crab nebula, photon, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Astronomy and Astrophysics, flux, Cherenkov counter, Crab Nebula, gamma ray: VHE, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, performance
Abstract

HAGAR is a system of seven Non-imaging Atmospheric Cherenkov Telescopes located at Hanle in the Ladakh region of the Indian Himalayas at an altitude of 4270 meters {\it amsl}. Since 2008, we have observed the Crab Nebula to assess the performance of the HAGAR telescopes. We describe the analysis technique for the estimation of $\gamma$-ray signal amidst cosmic ray background. The consolidated results spanning nine years of the Crab nebula observations show long term performance of the HAGAR telescopes. Based on about 219 hours of data, we report the detection of $\gamma$-rays from the Crab Nebula at a significance level of about 20$\sigma$, corresponding to a time averaged flux of (1.64$\pm$0.09) $\times10^{-10}$ photons cm$^{-2}$ sec$^{-1}$ above 230 GeV. Also, we perform a detailed study of possible systematic effects in our analysis method on data taken with the HAGAR telescopes., Comment: Accepted for publication in experimental astronomy

Published
2019

44. The PANDA Barrel DIRC detector.

Author

Hoek, M., Dzhygadlo, R., Gerhardt, A., Götzen, K., Hohler, R., Kalicy, G., Kumawat, H., Lehmann, D., Lewandowski, B., Patsyuk, M., Peters, K., Schepers, G., Schmitt, L., Schwarz, C., Schwiening, J., Traxler, M., Zühlsdorf, M., Dodokhov, V. Kh., Britting, A., and Eyrich, W.

Subjects
*PARTICLE detectors, *CHERENKOV counters, *IONS, *ANTIPROTONIC molecules, *PHOTON detectors
Abstract

The PANDA experiment at the new Facility for Antiproton and Ion Research in Europe (FAIR) at GSI, Darmstadt, will study fundamental questions of hadron physics and QCD using high-intensity cooled antiproton beams with momenta between 1.5 and 15 GeV/ c . Efficient Particle Identification for a wide momentum range and the full solid angle is required for reconstructing the various physics channels of the PANDA program. Hadronic Particle Identification in the barrel region of the detector will be provided by a DIRC counter. The design is based on the successful BABAR DIRC with important improvements, such as focusing optics and fast photon timing. Several of these improvements, including different radiator geometries and optics, were tested in particle beams at GSI and at CERN. The evolution of the conceptual design of the PANDA Barrel DIRC and the performance of complex prototypes in test beam campaigns will be discussed. [ABSTRACT FROM AUTHOR]

Published
2014
Full Text
View/download PDF

45. Deep-learning based reconstruction of the shower maximum $X_{max}$ using the water-Cherenkov detectors of the Pierre Auger Observatory

Author

Aab, Alexander, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Mu��iz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis, Andrada, Bel��n, Andringa, Sofia, Aramo, Carla, Ara��jo Ferreira, Paulo Ricardo, Arteaga Vel��zquez, Juan Carlos, Asorey, Hern��n Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter, Bister, Teresa Karolin, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Boh����ov��, Martina, Boncioli, Denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Choi, Koun, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agust��n, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Concei����o, Ruben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., de Almeida, Rogerio M., de Jes��s, Joaqu��n, de Jong, Sijbrand J., De Mauro, Giuseppe, de Mello Neto, J. R. T., De Mitri, Ivan, de Oliveira, Jaime, de Oliveira Franco, Danelise, de Palma, Francesco, de Souza, Vitor, De Vito, Emanuele, del R��o, Mariano, Deligny, Olivier, Di Matteo, Armando, Dobrigkeit, Carola, D'Olivo, Juan Carlos, dos Anjos, Rita, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys, Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filip��i��, Andrej, Fodran, Tomas, Freire, Mart��n Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, Garc��a, Beatriz, Garcia Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, Giaccari, Ugo, Giammarchi, Marco, Giller, Maria, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, G��mez Berisso, Mariano, G��mez Vitale, Primo F., Gongora, Juan Pablo, Gonz��lez, Juan Manuel, Gonz��lez, Nicol��s, Goos, Isabel, G��ra, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Mat��as Rolf, Hansen, Patricia, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, H��randel, J��rg, Horvath, Pavel, Hrabovsk��, Miroslav, Huege, Tim, Hulsman, Johannes, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Jurysek, Jakub, K����p��, Alex, Kampert, Karl-Heinz, Keilhauer, Bianca, Kemp, Julian, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, K��pke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas Uwe, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, Lopes, Luis, L��pez, Rebeca, Lu, Lu, Luce, Quentin, Lucero, Agustin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Mari��, Ioana, Marsella, Giovanni, Martello, Daniele, Martinez, Humberto, Mart��nez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, Fran��ois, Morello, Carlo, Mostaf��, Miguel, M��ller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotny, Vladimir, No��ka, Libor, Nucita, Achille, N����ez, Luis, Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pech, Miroslav, Pedreira, Francisco, P��kala, Jan, Pelayo, Rodrigo, Pe��a-Rodriguez, Jes��s, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, P��rez Bertolli, Carmina, Perlin, Mat��as, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, M��rio, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rub��n, Roncoroni, Mat��as J., Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saffi, Steven J., Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto, Salina, Gaetano, Sanabria Gomez, Jose, S��nchez, Federico, Moura Santos, Edivaldo, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Sch��fer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schl��ter, Felix, Schmidt, David, Scholten, Olaf, Schov��nek, Petr, Schr��der, Frank G., Schr��der, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, ��m��da, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stani��, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Su��rez-Dur��n, Mauricio, Sudholz, Tristan, Suomij��rvi, Tiina, Supanitsky, A. Daniel, ��up��k, Jan, Szadkowski, Zbigniew, Taboada, Alvaro, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tom��, Bernardo, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Trini, Marta, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Luk����, Vacula, Martin, Vald��s Galicia, Jose F., Valore, Laura, Varela, Enrique, Varma KC, Varada, V��squez-Ram��rez, Adriana, Veberi��, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczy��ski, Henryk, Winchen, Tobias, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, Zehrer, Lukas, and Zepeda, Arnulfo

Subjects
showers: energy, interaction: model, showers: atmosphere, air, detector: surface, neural network, Large detector systems for particle and astroparticle physics, Pattern recognition, cluster finding, calibration and fitting methods, Data analysis, resolution, calibration, Auger, detector: fluorescence, observatory, Particle identification methods, Cherenkov counter, cosmic radiation: UHE, nucleus: mass spectrum, structure, network: performance, showers: longitudinal
Abstract

27 Seiten : Illustrationen, Diagramme (2021).

Published
2021
Full Text
View/download PDF

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

Author

Christopher Eckner, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and CTA Consortium

Subjects
Cherenkov Telescope Array, WIMP, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, GLAST, thermal, cross section: annihilation, Observatory, TeV, Cherenkov radiation, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), background, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, dark matter: annihilation, sensitivity, observatory, gamma ray: emission, Cherenkov counter, angular resolution, Sky, Weakly interacting massive particles, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract

High-energy gamma rays are promising tools to constrain or reveal the nature of dark matter, in particular Weakly Interacting Massive Particles. Being well into its pre-construction phase, the Cherenkov Telescope Array (CTA) will soon probe the sky in the 20 GeV - 300 TeV energy range. Thanks to its improved energy and angular resolutions as well as significantly larger effective area when compared to the current generation of Cherenkov telescopes, CTA is expected to probe heavier dark matter, with unprecedented sensitivity, reaching the thermal annihilation cross-section at ~1 TeV. This talk will summarise the planned dark matter search strategies with CTA, focusing on the signal from the Galactic centre. As observed with the Fermi LAT at lower energies, this region is rather complex and CTA will be the first ground-based observatory sensitive to the large scale diffuse astrophysical emission from that region. We report on the collaboration effort to study the impact of such extended astrophysical backgrounds on the dark matter search, based on Fermi-LAT data in order to guide our observational strategies, taking into account various sources of systematic uncertainty., Comment: Proceedings of the 37th International Cosmic Ray Conference (ICRC2021), Berlin, Germany; PoS (ICRC2021) 998; 23 pages: full CTA author list starting on page 10

Published
2021
Full Text
View/download PDF

47. Tunka-Rex Virtual Observatory

Author

Tunka-REX Collaboration, Lenok, Vladimir, Kopylova, O., Wochele, D., Polgart, F., Golovachev, S., Sotnikov, V., Sotnikova, E., Bezyazeekov, P. A., Budnev, N., Fedorov, O., Gress, O., Grishin, O., Haungs, A., Huege, T., Kazarina, Y., Kleifges, M., Korosteleva, E., Kostunin, D., Kuzmichev, L., Lenok, V., Lubsandorzhiev, N., Malakhov, S., Marshalkina, T., Monkhoev, R., Osipova, E., Pakhorukov, A., Pankov, L., Prosin, V., Schröder, F. G., Shipilov, D., and Zagorodnikov, A.

Subjects
radio wave, showers: atmosphere, air, UHE [cosmic radiation], resolution, FOS: Physical sciences, programming, observatory, Cherenkov counter, optical [detector], interface, ddc:530, cosmic radiation: UHE, detector: optical, ddc:620, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Engineering & allied operations, atmosphere [showers]
Abstract

37th International Cosmic Ray Conference, ICRC 2021, Berlin, online, Germany, 12 Jul 2021 - 23 Jul 2021; Proceedings of Science / International School for Advanced Studies (ICRC2021), 421 (2021). doi:10.22323/1.395.0421, Tunka-Rex (Tunka Radio Extension) was a detector for ultra-high energy cosmic rays measuring radio emission for air showers in the frequency band of 30-80 MHz, operating in 2010s. It provided an experimental proof that sparse radio arrays can be a cost-effective technique to measure the depth of shower maximum with resolutions competitive to optical detectors. After the decommissioning of Tunka-Rex, as last phase of its lifecycle and following the FAIR (Findability ��� Accessibility ��� Interoperability ��� Reuse) principles, we publish the data and software under free licenses in the frame of the TRVO (Tunka-Rex Virtual Observatory), which is hosted at KIT under the partnership with the KCDC and GRADLCI projects. We present the main features of TRVO, its interface and give an overview of projects, which benefit from its open software and data., Published by SISSA, Trieste

Published
2021

48. A muon-track reconstruction exploiting stochastic losses for large-scale Cherenkov detectors

Author

Abbasi, R., Ackermann, Markus, Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Alispach, C., Alves, A. A., Amin, N. M., An, R., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Arg��elles, C., Axani, S., Bai, X., Balagopal V., A., Barbano, A., Barwick, S. W., Bastian-Querner, Benjamin, Basu, V., Baur, S., Bay, R., Beatty, J. J., Becker, K.-H., Becker Tjus, J., Bellenghi, C., BenZvi, S., Berley, D., Bernardini, Elisa, Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Borowka, J., B��ser, S., Botner, O., B��ttcher, J., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Bron, S., Brostean-Kaiser, J., Browne, S., Burgman, A., Busse, R. S., Campana, M. A., Chen, C., Chirkin, D., Choi, K., Clark, B. A., Clark, K., Classen, L., Coleman, A., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., De Clercq, C., DeLaunay, J. J., Dembinski, H., Deoskar, K., De Ridder, S., Desai, A., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Dharani, S., Diaz, A., D��az-V��lez, J. C., Dujmovic, H., Dunkman, M., DuVernois, M. A., Dvorak, E., Ehrhardt, T., Eller, P., Engel, R., Erpenbeck, H., Evans, J., Evenson, P. A., Fahey, S., Fazely, A. R., Fiedlschuster, S., Fienberg, A. T., Filimonov, K., Finley, C., Fischer, Leander, Fox, D., Franckowiak, A., Friedman, E., Fritz, A., F��rst, P., K. Gaisser, T., Gallagher, J., Ganster, E., Garrappa, S., Gerhardt, L., Ghadimi, A., Glaser, C., Glauch, T., Gl��senkamp, T., Goldschmidt, A., Gonzalez, J. G., Goswami, S., Grant, D., Gr��goire, T., Griffith, Z., Griswold, S., G��nd��z, M., G��nther, C., Haack, C., Hallgren, A., Halliday, R., Halve, L., Halzen, F., Ha Minh, M., Hanson, K., Hardin, J., Harnisch, A. A., Haungs, A., Hauser, S., Hebecker, D., Helbing, K., Henningsen, F., Hettinger, E. C., Hickford, S., Hignight, J., Hill, C., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Huber, T., Hultqvist, K., H��nnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jansson, M., Japaridze, G. S., Jeong, M., Jones, B. J. P., Joppe, R., Kang, D., Kang, W., Kang, X., Kappes, A., Kappesser, D., Karg, T., Karl, M., Karle, A., Katz, U., Kauer, M., Kellermann, M., Kelley, J. L., Kheirandish, A., Kin, K., Kintscher, T., Kiryluk, J., Klein, S. R., Koirala, R., Kolanoski, H., K��pke, L., Kopper, C., Kopper, S., Koskinen, D. J., Koundal, P., Kovacevich, M., Kowalski, Marek, Krings, K., Kurahashi, N., Kyriacou, A., Lagunas Gualda, C., Lanfranchi, J. L., Larson, M. J., Lauber, F., Lazar, J. P., Lee, J. W., Leonard, K., Leszczy��ska, A., Li, Y., Liu, Q. R., Lohfink, E., Lozano Mariscal, C. J., Lu, L., Lucarelli, F., Ludwig, A., Luszczak, W., Lyu, Y., Ma, Wing Yan, Madsen, J., Mahn, K. B. M., Makino, Y., Mancina, S., Mari��, I. C., Maruyama, R., Mase, K., McNally, F., Meagher, K., Medina, A., Meier, M., Meighen-Berger, S., Merz, J., Micallef, J., Mockler, D., Montaruli, T., Moore, R. W., Morse, R., Moulai, M., Naab, R., Nagai, R., Naumann, U., Necker, J., Nguy���n, L. V., Niederhausen, H., Nisa, M. U., Nowicki, S. C., Nygren, D. R., Obertacke Pollmann, A., Oehler, M., Olivas, A., O'Sullivan, E., Pandya, H., Pankova, D. V., Park, N., Parker, G. K., Paudel, E. N., Paul, L., P��rez de los Heros, C., Philippen, S., Pieloth, D., Pieper, S., Pizzuto, A., Plum, M., Popovych, Y., Porcelli, A., Prado Rodriguez, M., Price, P. B., Pries, B., Przybylski, G. T., Raab, C., Raissi, A., Rameez, M., Rawlins, K., Rea, I. C., Rehman, A., Reimann, R., Renzi, G., Resconi, E., Reusch, S., Rhode, W., Richman, M., Riedel, B., Robertson, S., Roellinghoff, G., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk Cantu, D., Safa, I., Saffer, J., Sanchez Herrera, S. E., Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Scharf, M., Schaufel, M., Schieler, H., Schlunder, P., Schmidt, T., Schneider, A., Schneider, J., Schr��der, F. G., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Sharma, A., Shefali, S., Silva, M., Skrzypek, B., Smithers, B., Snihur, R., Soedingrekso, J., Soldin, D., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stein, Robert, Stettner, J., Steuer, A., Stezelberger, T., St��rwald, T., Stuttard, T., Sullivan, G. W., Taboada, I., Tenholt, F., Ter-Antonyan, S., Tilav, S., Tischbein, F., Tollefson, K., Tomankova, L., T��nnis, C., Toscano, S., Tosi, D., Trettin, A., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Twagirayezu, J. P., Ty, B., Unland Elorrieta, M. A., Valtonen-Mattila, N., Vandenbroucke, J., van Eijk, D., van Eijndhoven, N., Vannerom, D., van Santen, J., Verpoest, S., Vraeghe, M., Walck, C., Wallace, A., Watson, T. B., Weaver, C., Weigel, P., Weindl, A., Weiss, M. J., Weldert, J., Wendt, C., Werthebach, J., Weyrauch, M., Whelan, B. J., Whitehorn, N., Wiebusch, C. H., Williams, D. R., Wolf, M., Woschnagg, K., Wrede, G., Wulff, J., Xu, X. W., Xu, Y., Yanez, J. P., Yoshida, S., Yuan, T., Zhang, Z., and Icecube Collaboration

Subjects
secondary [muon], data analysis method, cosmic radiation [neutrino], charge: current, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, ice, Data analysis, muon: particle identification, FOS: Physical sciences, High Energy Physics - Experiment, IceCube, High Energy Physics - Experiment (hep-ex), muon: tracks, current [charge], Cherenkov [radiation], ddc:530, stochastic, Neutrino detectors, ddc:610, Instrumentation and Methods for Astrophysics (astro-ph.IM), particle identification [muon], muon: secondary, photomultiplier, muon: energy loss, Physics, nucleus, photon, Cherenkov detectors, Astrophysics::Instrumentation and Methods for Astrophysics, parametrization, showers, radiation: Cherenkov, energy loss [muon], Cherenkov counter, angular resolution, neutrino: cosmic radiation, High Energy Physics::Experiment, tracks [muon], Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Journal of Instrumentation 16(08), P08034 (2021). doi:10.1088/1748-0221/16/08/P08034, IceCube is a cubic-kilometer Cherenkov telescope operating at the South Pole. The main goal of IceCube is the detection of astrophysical neutrinos and the identification of their sources. High-energy muon neutrinos are observed via the secondary muons produced in charge current interactions with nuclei in the ice. Currently, the best performing muon track directional reconstruction is based on a maximum likelihood method using the arrival time distribution of Cherenkov photons registered by the experiment's photomultipliers. A known systematic shortcoming of the prevailing method is to assume a continuous energy loss along the muon track. However at energies >1 TeV the light yield from muons is dominated by stochastic showers. This paper discusses a generalized ansatz where the expected arrival time distribution is parametrized by a stochastic muon energy loss pattern. This more realistic parametrization of the loss profile leads to an improvement of the muon angular resolution of up to 20% for through-going tracks and up to a factor 2 for starting tracks over existing algorithms. Additionally, the procedure to estimate the directional reconstruction uncertainty has been improved to be more robust against numerical errors., Published by Inst. of Physics, London

Published
2021

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

Author

Pecimotika, Mario, Adamczykc, Katarzyna, Szanecki, Michał, Array, Cherenkov Telescope, Prester, Dijana Dominis, Gueta, Orel, Hrupec, Dario, Maier, Gernot, Mićanović, Saša, Pavletić, Lovro, Sitarek, Julian, Sobczyńska, Dorota, API (FNWI), High Energy Astrophys. & Astropart. Phys (API, FNWI), and GRAPPA (ITFA, IoP, FNWI)

Subjects
Cherenkov Telescope Array, energy resolution, law.invention, energy: threshold, Observatory, law, HESS, optical, cloud, MAGIC (telescope), energy: low, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), MODTRAN, photon, Astrophysics::Instrumentation and Methods for Astrophysics, Mars Exploration Program, Monte Carlo [numerical calculations], threshold [energy], observatory, Astrophysics::Earth and Planetary Astrophysics, numerical calculations: Monte Carlo, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, performance, atmosphere [showers], data analysis method, sensitivity [detector], air, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, programming, VHE, Atmosphere, Telescope, Cherenkov [radiation], low [energy], ddc:530, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, Remote sensing, showers: atmosphere, Cherenkov telescopes, clouds, CTA, MODTRAN, Monte Carlo simulations, background, resolution, trigger, radiation: Cherenkov, MAGIC, detector: sensitivity, Cherenkov counter, angular resolution, gamma ray
Abstract

37th International Cosmic Ray Conference, ICRC 2021, Berlin, online, Germany, 12 Jul 2021 - 23 Jul 2021; Proceedings of Science / International School for Advanced Studies (ICRC2021), 773 (2021). doi:10.22323/1.395.0773, The Cherenkov Telescope Array (CTA) is the future ground-based observatory for gamma-ray astronomy at very high energies. The atmosphere is an integral part of every Cherenkov telescope. Different atmospheric conditions, such as clouds, can reduce the fraction of Cherenkov photons produced in air showers that reach ground-based telescopes, which may affect the performance. Decreased sensitivity of the telescopes may lead to misconstructed energies and spectra. This study presents the impact of various atmospheric conditions on CTA performance. The atmospheric transmission in a cloudy atmosphere in the wavelength range from 203 nm to 1000 nm was simulated for different cloud bases and different optical depths using the MODerate resolution atmospheric TRANsmission (MODTRAN) code. MODTRAN output files were used as inputs for generic Monte Carlo simulations. The analysis was performed using the MAGIC Analysis and Reconstruction Software (MARS) adapted for CTA. As expected, the effects of clouds are most evident at low energies, near the energy threshold. Even in the presence of dense clouds, high-energy gamma rays may still trigger the telescopes if the first interaction occurs lower in the atmosphere, below the cloud base. A method to analyze very high-energy data obtained in the presence of clouds is presented. The systematic uncertainties of the method are evaluated. These studies help to gain more precise knowledge about the CTA response to cloudy conditions and give insights on how to proceed with data obtained in such conditions. This may prove crucial for alert-based observations and time-critical studies of transient phenomena., Published by SISSA, Trieste

Published
2021

50. The Crab nebula variability at short time-scales with the Cherenkov telescope array

Author

Dmitry Khangulyan, Diego F. Torres, E. de Oña Wilhelmi, Enrique Mestre, Fabio Acero, Roberta Zanin, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Alexander von Humboldt Foundation, Japan Society for the Promotion of Science, and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Cherenkov Telescope Array, model [emission], threshold [detector], Astrophysics, GeV, detectors -stars, 01 natural sciences, law.invention, energy: threshold, law, Astrophysics::Solar and Stellar Astrophysics, individual, flare, 010303 astronomy & astrophysics, detectors [Instrumentation], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), instrumentation, Nebula, energy: high, Astrophysics::Instrumentation and Methods for Astrophysics, threshold [energy], flare [Stars], detector: threshold, Supernova, gamma ray: emission, supernovae: individual: Crab Nebula, high [energy], Spectral energy distribution, individual: Crab Nebula [Supernovae], stars: flare, Crab Nebula -stars, Astrophysics - High Energy Astrophysical Phenomena, Flare, supernovae, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, determinant, GLAST, emission: model, emission [gamma ray], 0103 physical sciences, TeV, 010306 general physics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, instrumentation: detectors, Astronomy and Astrophysics, Crab Nebula, Cherenkov counter, 13. Climate action, Space and Planetary Science, ddc:520, spectral, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract

Monthly notices of the Royal Astronomical Society 509(1), 337 - 346 (2020). doi:10.1093/mnras/staa3599, Since 2009, several rapid and bright flares have been observed at high energies (>100 MeV) from the direction of the Crab Nebula. Several hypotheses have been put forward to explain this phenomenon, but the origin is still unclear. The detection of counterparts at higher energies with the next generation of Cherenkov telescopes will be determinant to constrain the underlying emission mechanisms. We aim at studying the capability of the Cherenkov Telescope Array (CTA) to explore the physics behind the flares, by performing simulations of the Crab Nebula spectral energy distribution, both in flaring and steady state, for different parameters related to the physical conditions in the nebula. In particular, we explore the data recorded by Fermi during two particular flares that occurred in 2011 and 2013. The expected GeV and TeV gamma-ray emission is derived using different radiation models. The resulting emission is convoluted with the CTA response and tested for detection, obtaining an exclusion region for the space of parameters that rule the different flare emission models. Our simulations show different scenarios that may be favourable for achieving the detection of the flares in Crab with CTA, in different regimes of energy. In particular, we find that observations with low sub-100 GeV energy threshold telescopes could provide the most model-constraining results., Published by Oxford Univ. Press, Oxford

Published
2021

Catalog

Books, media, physical & digital resources
See catalog results