Descriptor: "dark matter: heavy" - Searchworks@Jio Institute Digital Library Search Results

16 results on '"dark matter: heavy"'

1. The B anomalies, the U 1 leptoquark and dark matter

Author: Geneviève Bélanger, Jacky Kumar, David London, Alexander Pukhov, and HEP, INSPIRE
Subjects: Nuclear and High Energy Physics, gauge boson, scale: TeV, dark matter: relic density, High Energy Physics::Phenomenology, Mathematics::Analysis of PDEs, anomaly, FOS: Physical sciences, dark matter: annihilation, singlet: scalar, leptoquark, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics - Phenomenology, dark matter: singlet, High Energy Physics - Phenomenology (hep-ph), dark matter: heavy, High Energy Physics::Experiment
Abstract: The present-day $B$-anomalies involving $b \to s \mu^+ \mu^-$ or $b \to c \tau^- {\bar\nu}$ transitions can all be explained with the addition of a vector $U_1$ leptoquark with a mass of $M_{U_1} \ge 1.8$ TeV. In the scalar singlet dark matter model (SSDMM), the DM is a scalar $S$ that couples to the Higgs via $\lambda_{hS} \, S^2|H|^2$. We update the fit to the data and find that the SSDMM is now viable only for $M_S \ge 1.6$ TeV. In this paper, we assume that the DM also couples to the $U_1$ via $\lambda_{U_1 S} \, S^2 \, U_{1\mu}^{\dagger} U^{\mu}_1$. In addition to leading to DM annihilation via $S S \to U_1 {\bar U}_1$, this coupling generates $SSgg$ and $SS\gamma\gamma$ couplings at one loop. Although naively divergent, these loop diagrams can be calculated under the assumption that the $U_1$ is a gauge boson of a group broken at the TeV scale. With this DM-$U_1$ coupling term, there are additional contributions to the various DM observables (relic density, direct and indirect detection). We find that the constraints on the SSDMM are relaxed for both heavy DM ($M_S \ge M_{U_1}$) and light DM ($M_S < M_{U_1}$)., Comment: 21 pages, 5 figures
Published: 2023

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

Author: Abdalla, H., Abe, H., Abe, S., Abusleme, A., Acero, F., Acharyya, A., Acín Portella, V., Ackley, K., Adam, R., Adams, C., Adhikari, S. S., Aguado-Ruesga, I., Agudo, I., Aguilera, R., Aguirre-Santaella, A., Aharonian, F., Alberdi, A., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Alves Batista, R., Amans, J. -P, Amati, L., Amato, E., Ambrogi, L., Ambrosi, G., Ambrosio, M., Ammendola, R., Anderson, J., Anduze, M., Angüner, E. O., Antonelli, L. A., Antonuccio, V., Antoranz, P., Anutarawiramkul, R., Aragunde Gutierrez, J., Aramo, C., Araudo, A., Araya, M., Arbet-Engels, A., Arcaro, C., Arendt, V., Armand, C., Armstrong, T., Arqueros, F., Arrabito, L., Arsioli, B., Artero, M., Asano, K., Ascasíbar, Y., Aschersleben, J., Ashley, M., Attinà, P., Aubert, P., Singh, C. B., Baack, D., Babic, A., Backes, M., Baena, V., Bajtlik, S., Baktash, A., Balazs, C., Balbo, M., Ballester, O., Ballet, J., Balmaverde, B., Bamba, A., Bandiera, R., Baquero Larriva, A., Barai, P., Barbier, C., Barbosa Martins, V., Barcelo, M., Barkov, M., Barnard, M., Baroncelli, L., Barres Almeida, U., Barrio, J. A., Bastieri, D., Batista, P. I., Batkovic, I., Bauer, C., Bautista-González, R., Baxter, J., Becciani, U., Becerra González, J., Becherini, Y., Beck, G., Becker Tjus, J., Bednarek, W., Belfiore, A., Bellizzi, L., Belmont, R., Benbow, W., Berge, D., Bernardini, E., Bernardos, M. I., Bernlöhr, K., Berti, A., Berton, M., Bertucci, B., Beshley, V., Bhatt, N., Bhattacharyya, S., Bhattacharyya, W., Bi, B., Bicknell, G., Biederbeck, N., Bigongiari, C., Biland, A., Bird, R., Bissaldi, E., Biteau, J., Bitossi, M., Blanch, O., Blank, M., Blazek, J., Bobin, J., Boccato, C., Bocchino, F., Boehm, C., Bohacova, M., Boisson, C., Boix, J., Bolle, J. -P, Bolmont, J., Bonanno, G., Bonavolontà, C., Bonneau Arbeletche, L., Bonnoli, G., Bordas, P., Borkowski, J., Bórquez, S., Bose, R., Bose, D., Bosnjak, Z., Bottacini, E., Böttcher, M., Botticella, M. T., Boutonnet, C., Bouyjou, F., Bozhilov, V., Bozzo, E., Brahimi, L., Braiding, C., Brau-Nogué, S., Breen, S., Bregeon, J., Breuhaus, M., Brill, A., Brisken, W., Brocato, E., Brown, A. M., Brügge, K., Brun, P., Brun, F., Brunetti, L., Brunetti, G., Bruno, P., Bruno, A., Bruzzese, A., Bucciantini, N., Buckley, J., Bühler, R., Bulgarelli, A., Bulik, T., Bünning, M., Bunse, M., Burton, M., Burtovoi, A., Buscemi, M., Buschjäger, S., Busetto, G., Buss, J., Byrum, K., Caccianiga, A., Cadoux, F., Calanducci, A., Calderón, C., Calvo Tovar, J., Cameron, R., Campaña, P., Canestrari, R., Cangemi, F., Cantlay, B., Capalbi, M., Capasso, M., Cappi, M., Caproni, A., Capuzzo-Dolcetta, R., Caraveo, P., Cárdenas, V., Cardiel, L., Cardillo, M., Carlile, C., Caroff, S., Carosi, R., Carosi, A., Carquín, E., Carrère, M., Casandjian, J. -M, Casanova, S., Cascone, E., Cassol, F., Castro-Tirado, A. J., Catalani, F., Catalano, O., Cauz, D., Ceccanti, A., Celestino Silva, C., Celli, S., Cerny, K., Cerruti, M., Chabanne, E., Chadwick, P., Chai, Y., Chambery, P., Champion, C., Chandra, S., Chaty, S., Chen, A., Cheng, K., Chernyakova, M., Chiaro, G., Chiavassa, A., Chikawa, M., Chitnis, V. R., Chudoba, J., Chytka, L., Cikota, S., Circiello, A., Clark, P., Çolak, M., Colombo, E., Colome, J., Colonges, S., Comastri, A., Compagnino, A., Conforti, V., Congiu, E., Coniglione, R., Conrad, J., Conte, F., Contreras, J. L., Coppi, P., Cornat, R., Coronado-Blazquez, J., Cortina, J., Costa, A., Costantini, H., Cotter, G., Courty, B., Covino, S., Crestan, S., Cristofari, P., Crocker, R., Croston, J., Cubuk, K., Cuevas, O., Cui, X., Cusumano, G., Cutini, S., D’aì, A., D’amico, G., D’ammando, F., D’avanzo, P., Da Vela, P., Dadina, M., Dai, S., Dalchenko, M., Dall’ Ora, M., Daniel, M. K., Dauguet, J., Davids, I., Davies, J., Dawson, B., Angelis, A., Araújo Carvalho, A. E., Bony Lavergne, M., Caprio, V., Cesare, G., Frondat, F., Gouveia Dal Pino, E. M., La Calle, I., Lotto, B., Luca, A., Martino, D., Menezes, R. M., Naurois, M., Oña Wilhelmi, E., Palma, F., Persio, F., Simone, N., Souza, V., Del Santo, M., Del Valle, M. V., Delagnes, E., Deleglise, G., Delfino Reznicek, M., Delgado, C., Delgado Giler, A. G., Delgado Mengual, J., Della Ceca, R., Della Valle, M., Della Volpe, D., Depaoli, D., Depouez, D., Devin, J., Di Girolamo, T., Di Giulio, C., Di Piano, A., Di Pierro, F., Di Venere, L., Díaz, C., Díaz-Bahamondes, C., Dib, C., Diebold, S., Digel, S., Dima, R., Djannati-Ataï, A., Djuvsland, J., Dmytriiev, A., Docher, K., Domínguez, A., Dominis Prester, D., Donath, A., Donini, A., Dorner, D., Doro, M., Dos Anjos, R. D. C., Dournaux, J. -L, Downes, T., Drake, G., Drass, H., Dravins, D., Duangchan, C., Duara, A., Dubus, G., Ducci, L., Duffy, C., Dumora, D., Dundas Morå, K., Durkalec, A., Dwarkadas, V. V., Ebr, J., Eckner, C., Eder, J., Ederoclite, A., Edy, E., Egberts, K., Einecke, S., Eisch, J., Eleftheriadis, C., Elsässer, D., Emery, G., Emmanoulopoulos, D., Ernenwein, J. -P, Errando, M., Escarate, P., Escudero, J., Espinoza, C., Ettori, S., Eungwanichayapant, A., Evans, P., Evoli, C., Fairbairn, M., Falceta-Goncalves, D., Falcone, A., Fallah Ramazani, V., Falomo, R., Farakos, K., Fasola, G., Fattorini, A., Favre, Y., Fedora, R., Fedorova, E., Fegan, S., Feijen, K., Feng, Q., Ferrand, G., Ferrara, G., Ferreira, O., Fesquet, M., Fiandrini, E., Fiasson, A., Filipovic, M., Fink, D., Finley, J. P., Fioretti, V., Fiorillo, D. F. G., Fiorini, M., Flis, S., Flores, H., Foffano, L., Föhr, C., Fonseca, M. V., Font, L., Fontaine, G., Fornieri, O., Fortin, P., Fortson, L., Fouque, N., Fournier, A., Fraga, B., Franceschini, A., Franco, F. J., Franco Ordovas, A., Freixas Coromina, L., Fresnillo, L., Fruck, C., Fugazza, D., Fujikawa, Y., Fujita, Y., Fukami, S., Fukazawa, Y., Fukui, Y., Fulla, D., Funk, S., Furniss, A., Gabella, O., Gabici, S., Gaggero, D., Galanti, G., Galaz, G., Galdemard, P., Gallant, Y., Galloway, D., Gallozzi, S., Gammaldi, V., Garcia, R., Garcia, E., García, E., Garcia López, R., Garczarczyk, M., Gargano, F., Gargano, C., Garozzo, S., Gascon, D., Gasparetto, T., Gasparrini, D., Gasparyan, H., Gaug, M., Geffroy, N., Gent, A., Germani, S., Gesa, L., Ghalumyan, A., Ghedina, A., Ghirlanda, G., Gianotti, F., Giarrusso, S., Giarrusso, M., Giavitto, G., Giebels, B., Giglietto, N., Gika, V., Gillardo, F., Gimenes, R., Giordano, F., Giovannini, G., Giro, E., Giroletti, M., Giuliani, A., Giunti, L., Gjaja, M., Glicenstein, J. -F, Gliwny, P., Godinovic, N., Göksu, H., Goldoni, P., Gómez, J. L., Gómez-Vargas, G., González, M. M., González, J. M., Gothe, K. S., Götz, D., Goulart Coelho, J., Gourgouliatos, K., Grabarczyk, T., Graciani, R., Grandi, P., Grasseau, G., Grasso, D., Green, A. J., Green, D., Green, J., Greenshaw, T., Grenier, I., Grespan, P., Grillo, A., Grondin, M. -H, Grube, J., Guarino, V., Guest, B., Gueta, O., Gündüz, M., Gunji, S., Gusdorf, A., Gyuk, G., Hackfeld, J., Hadasch, D., Haga, J., Hagge, L., Hahn, A., Hajlaoui, J. E., Hakobyan, H., Halim, A., Hamal, P., Hanlon, W., Hara, S., Harada, Y., Hardcastle, M. J., Harvey, M., Hashiyama, K., Hassan Collado, T., Haubold, T., Haupt, A., Hautmann, U. A., Havelka, M., Hayashi, K., Hayashida, M., He, H., Heckmann, L., Heller, M., Helo, J. C., Henault, F., Henri, G., Hermann, G., Hermel, R., Hernández Cadena, S., Herrera Llorente, J., Herrero, A., Hervet, O., Hinton, J., Hiramatsu, A., Hiroshima, N., Hirotani, K., Hnatyk, B., Hnatyk, R., Hoang, J. K., Hoffmann, D., Hofmann, W., Hoischen, C., Holder, J., Holler, M., Hona, B., Horan, D., Hörandel, J., Horns, D., Horvath, P., Houles, J., Hovatta, T., Hrabovsky, M., Hrupec, D., Huang, Y., Huet, J. -M, Hughes, G., Hui, D., Hull, G., Humensky, T. B., Hütten, M., Iaria, R., Iarlori, M., Illa, J. M., Imazawa, R., Impiombato, D., Inada, T., Incardona, F., Ingallinera, A., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Insolia, A., Iocco, F., Ioka, K., Ionica, M., Iori, M., Iovenitti, S., Iriarte, A., Ishio, K., Ishizaki, W., Iwamura, Y., Jablonski, C., Jacquemier, J., Jacquemont, M., Jamrozy, M., Janecek, P., Jankowsky, F., Jardin-Blicq, A., Jarnot, C., Jean, P., Jiménez Martínez, I., Jin, W., Jocou, L., Jordana, N., Josselin, M., Jouvin, L., Jung-Richardt, I., Junqueira, F. J. P. A., Juramy-Gilles, C., Jurysek, J., Kaaret, P., Kadowaki, L. H. S., Kagaya, M., Kalekin, O., Kankanyan, R., Kantzas, D., Karas, V., Karastergiou, A., Karkar, S., Kasai, E., Kasperek, J., Katagiri, H., Kataoka, J., Katarzyński, K., Katsuda, S., Katz, U., Kawanaka, N., Kazanas, D., Kerszberg, D., Khélifi, B., Kherlakian, M. C., Kian, T. P., Kieda, D. B., Kihm, T., Kim, S., Kimeswenger, S., Kisaka, S., Kissmann, R., Kleijwegt, R., Kleiner, T., Kluge, G., Kluźniak, W., Knapp, J., Knödlseder, J., Kobakhidze, A., Kobayashi, Y., Koch, B., Kocot, J., Kohri, K., Kokkotas, K., Komin, N., Kong, A., Kosack, K., Kowal, G., Krack, F., Krause, M., Krennrich, F., Krumholz, M., Kubo, H., Kudryavtsev, V., Kunwar, S., Kuroda, Y., Kushida, J., Kushwaha, P., La Barbera, A., La Palombara, N., La Parola, V., La Rosa, G., Lahmann, R., Lamanna, G., Lamastra, A., Landoni, M., Landriu, D., Lang, R. G., Lapington, J., Laporte, P., Lason, P., Lasuik, J., Lazendic-Galloway, J., Le Flour, T., Le Sidaner, P., Leach, S., Leckngam, A., Lee, S. -H, Lee, W. H., Lee, S., Leigui Oliveira, M. A., Lemière, A., Lemoine-Goumard, M., Lenain, J. -P, Leone, F., Leray, V., Leto, G., Leuschner, F., Levy, C., Lindemann, R., Lindfors, E., Linhoff, L., Liodakis, I., Lipniacka, A., Lloyd, S., Lobo, M., Lohse, T., Lombardi, S., Longo, F., Lopez, A., López, M., López-Coto, R., Loporchio, S., Louis, F., Louys, M., Lucarelli, F., Lucchesi, D., Ludwig Boudi, H., Luque-Escamilla, P. L., Lyard, E., Maccarone, M. C., Maccarone, T., Mach, E., Maciejewski, A. J., Mackey, J., Madejski, G. M., Maeght, P., Maggio, C., Maier, G., Majczyna, A., Majumdar, P., Makariev, M., Mallamaci, M., Malta Nunes Almeida, R., Maltezos, S., Malyshev, D., Mandat, D., Maneva, G., Manganaro, M., Manicò, G., Manigot, P., Mannheim, K., Maragos, N., Marano, D., Marconi, M., Marcowith, A., Marculewicz, M., Marčun, B., Marín, J., Marinello, N., Marinos, P., Mariotti, M., Markoff, S., Marquez, P., Marsella, G., Martí, J., Martin, J. -M, Martin, P., Martinez, O., Martínez, M., Martínez, G., Martínez, O., Martínez-Huerta, H., Marty, C., Marx, R., Masetti, N., Massimino, P., Mastichiadis, A., Matsumoto, H., Matthews, N., Maurin, G., Max-Moerbeck, W., Maxted, N., Mazin, D., Mazziotta, M. N., Mazzola, S. M., Mbarubucyeye, J. D., Mc Comb, L., Mchardy, I., Mckeague, S., Mcmuldroch, S., Medina, E., Medina Miranda, D., Melandri, A., Melioli, C., Melkumyan, D., Menchiari, S., Mender, S., Mereghetti, S., Merino Arévalo, G., Mestre, E., Meunier, J. -L, Meures, T., Meyer, M., Micanovic, S., Miceli, M., Michailidis, M., Michałowski, J., Miener, T., Mievre, I., Miller, J., Minaya, I. A., Mineo, T., Minev, M., Miranda, J. M., Mirzoyan, R., Mitchell, A., Mizuno, T., Mode, B., Moderski, R., Mohrmann, L., Molina, E., Molinari, E., Teresa Montaruli, Monteiro, I., Moore, C., Moralejo, A., Morcuende-Parrilla, D., Moretti, E., Morganti, L., Mori, K., Moriarty, P., Morik, K., Morlino, G., Morris, P., Morselli, A., Mosshammer, K., Moya, P., Mukherjee, R., Muller, J., Mundell, C., Mundet, J., Murach, T., Muraczewski, A., Muraishi, H., Murase, K., Musella, I., Musumarra, A., Nagai, A., Nagar, N., Nagataki, S., Naito, T., Nakamori, T., Nakashima, K., Nakayama, K., Nakhjiri, N., Naletto, G., Naumann, D., Nava, L., Navarro, R., Nawaz, M. A., Ndiyavala, H., Neise, D., Nellen, L., Nemmen, R., Newbold, M., Neyroud, N., Ngernphat, K., Nguyen Trung, T., Nicastro, L., Nickel, L., Niemiec, J., Nieto, D., Nievas, M., Nigro, C., Nikołajuk, M., Ninci, D., Nishijima, K., Noda, K., Nogami, Y., Nolan, S., Nomura, R., Norris, R., Nosek, D., Nöthe, M., Novosyadlyj, B., Novotny, V., Nozaki, S., Nunio, F., O’brien, P., Obara, K., Oger, R., Ohira, Y., Ohishi, M., Ohm, S., Ohtani, Y., Oka, T., Okazaki, N., Okumura, A., Olive, J. -F, Oliver, C., Olivera, G., Olmi, B., Ong, R. A., Orienti, M., Orito, R., Orlandini, M., Orlando, S., Orlando, E., Osborne, J. P., Ostrowski, M., Otte, N., Ovcharov, E., Owen, E., Oya, I., Ozieblo, A., Padovani, M., Pagano, I., Pagliaro, A., Paizis, A., Palatiello, M., Palatka, M., Palazzi, E., Panazol, J. -L, Paneque, D., Panes, B., Panny, S., Pantaleo, F. R., Panter, M., Paoletti, R., Paolillo, M., Papitto, A., Paravac, A., Paredes, J. M., Pareschi, G., Park, N., Parmiggiani, N., Parsons, R. D., Paśko, P., Patel, S., Patricelli, B., Pauletta, G., Pavletić, L., Pavy, S., Pe’er, A., Pech, M., Pecimotika, M., Pellegriti, M. G., Peñil Del Campo, P., Penno, M., Pepato, A., Perard, S., Perennes, C., Peres, G., Peresano, M., Pérez-Aguilera, A., Pérez-Romero, J., Pérez-Torres, M. A., Perri, M., Persic, M., Petrera, S., Petrucci, P. -O, Petruk, O., Peyaud, B., Pfrang, K., Pian, E., Piano, G., Piatteli, P., Pietropaolo, E., Pillera, R., Pilszyk, B., Pimentel, D., Pintore, F., Pio García, C., Pirola, G., Piron, F., Pisarski, A., Pita, S., Pohl, M., Poireau, V., Poledrelli, P., Pollo, A., Polo, M., Pongkitivanichkul, C., Porthault, J., Powell, J., Pozo, D., Prado, R. R., Prandini, E., Prasit, P., Prast, J., Pressard, K., Principe, G., Priyadarshi, C., Produit, N., Prokhorov, D., Prokoph, H., Prouza, M., Przybilski, H., Pueschel, E., Pühlhofer, G., Puljak, I., Pumo, M. L., Punch, M., Queiroz, F., Quinn, J., Quirrenbach, A., Rainò, S., Rajda, P. J., Rando, R., Razzaque, S., Rebert, E., Recchia, S., Reichherzer, P., Reimer, O., Reimer, A., Reisenegger, A., Remy, Q., Renaud, M., Reposeur, T., Reville, B., Reymond, J. -M, Reynolds, J., Rhode, W., Ribeiro, D., Ribó, M., Richards, G., Richtler, T., Rico, J., Rieger, F., Riitano, L., Ripepi, V., Riquelme, M., Riquelme, D., Rivoire, S., Rizi, V., Roache, E., Röben, B., Roche, M., Rodriguez, J., Rodriguez Fernandez, G., Rodriguez Ramirez, J. C., Rodríguez Vázquez, J. J., Roepke, F., Rojas, G., Romanato, L., Romano, P., Romeo, G., Romero Lobato, F., Romoli, C., Roncadelli, M., Ronda, S., Rosado, J., Rosales Leon, A., Rowell, G., Rudak, B., Rugliancich, A., Ruíz Del Mazo, J. E., Rujopakarn, W., Rulten, C., Russell, C., Russo, F., Sadeh, I., Sæther Hatlen, E., Safi-Harb, S., Saha, L., Saha, P., Sahakian, V., Sailer, S., Saito, T., Sakaki, N., Sakurai, S., Salesa Greus, F., Salina, G., Salzmann, H., Sanchez, D., Sánchez-Conde, M., Sandaker, H., Sandoval, A., Sangiorgi, P., Sanguillon, M., Sano, H., Santander, M., Santangelo, A., Santos, E. M., Santos-Lima, R., Sanuy, A., Sapozhnikov, L., Saric, T., Sarkar, S., Sasaki, H., Sasaki, N., Satalecka, K., Sato, Y., Saturni, F. G., Sawada, M., Sawangwit, U., Schaefer, J., Scherer, A., Scherpenberg, J., Schipani, P., Schleicher, B., Schmoll, J., Schneider, M., Schoorlemmer, H., Schovanek, P., Schussler, F., Schwab, B., Schwanke, U., Schwarz, J., Schweizer, T., Sciacca, E., Scuderi, S., Seglar Arroyo, M., Segreto, A., Seitenzahl, I., Semikoz, D., Sergijenko, O., Serna Franco, J. E., Servillat, M., Seweryn, K., Sguera, V., Shalchi, A., Shang, R. Y., Sharma, P., Shellard, R. C., Sidoli, L., Sieiro, J., Siejkowski, H., Silk, J., Sillanpää, A., Singh, B. B., Singh, K. K., Sinha, A., Siqueira, C., Sironi, G., Sitarek, J., Sizun, P., Sliusar, V., Slowikowska, A., Sobczyńska, D., Sobrinho, R. W., Sol, H., Sottile, G., Spackman, H., Specovius, A., Spencer, S., Spengler, G., Spiga, D., Spolon, A., Springer, W., Stamerra, A., Stanič, S., Starling, R., Stawarz, Ł., Steenkamp, R., Stefanik, S., Stegmann, C., Steiner, A., Steinmassl, S., Stella, C., Steppa, C., Sternberger, R., Sterzel, M., Stevens, C., Stevenson, B., Stolarczyk, T., Stratta, G., Straumann, U., Strišković, J., Strzys, M., Stuik, R., Suchenek, M., Suda, Y., Sunada, Y., Suomijarvi, T., Suric, T., Sutcliffe, P., Suzuki, H., Świerk, P., Szepieniec, T., Tacchini, A., Tachihara, K., Tagliaferri, G., Tajima, H., Tajima, N., Tak, D., Takahashi, K., Takahashi, H., Takahashi, M., Takata, J., Takeishi, R., Tam, T., Tanaka, M., Tanaka, T., Tanaka, S., Tateishi, D., Tavani, M., Tavecchio, F., Tavernier, T., Taylor, L., Taylor, A., Tejedor, L. A., Temnikov, P., Terada, Y., Terauchi, K., Terrazas, J. C., Terrier, R., Terzic, T., Teshima, M., Testa, V., Thibaut, D., Thocquenne, F., Tian, W., Tibaldo, L., Tiengo, A., Tiziani, D., Tluczykont, M., Todero Peixoto, C. J., Tokanai, F., Toma, K., Tomankova, L., Tomastik, J., Tonev, D., Tornikoski, M., Torres, D. F., Torresi, E., Tosti, G., Tosti, L., Totani, T., Tothill, N., Toussenel, F., Tovmassian, G., Travnicek, P., Trichard, C., Trifoglio, M., Trois, A., Truzzi, S., Tsiahina, A., Tsuru, T., Turk, B., Tutone, A., Uchiyama, Y., Umana, G., Utayarat, P., Vaclavek, L., Vacula, M., Vagelli, V., Vagnetti, F., Vakili, F., Valdivia, J. A., Valentino, M., Valio, A., Vallage, B., Vallania, P., Valverde Quispe, J. V., Den Berg, A. M., Driel, W., Eldik, C., Rensburg, C., Soelen, B., Vandenbroucke, J., Vanderwalt, J., Vasileiadis, G., Vassiliev, V., Vázquez Acosta, M., Vecchi, M., Vega, A., Veh, J., Veitch, P., Venault, P., Venter, C., Ventura, S., Vercellone, S., Vergani, S., Verguilov, V., Verna, G., Vernetto, S., Verzi, V., Vettolani, G. P., Veyssiere, C., Viale, I., Viana, A., Viaux, N., Vicha, J., Vignatti, J., Vigorito, C. F., Villanueva, J., Vink, J., Vitale, V., Vittorini, V., Vodeb, V., Voelk, H., Vogel, N., Voisin, V., Vorobiov, S., Vovk, I., Vrastil, M., Vuillaume, T., Wagner, S. J., Wagner, R., Wagner, P., Wakazono, K., Wakely, S. P., Walter, R., Ward, M., Warren, D., Watson, J., Webb, N., Wechakama, M., Wegner, P., Weinstein, A., Weniger, C., Werner, F., Wetteskind, H., White, M., White, R., Wierzcholska, A., Wiesand, S., Wijers, R., Wilkinson, M., Will, M., Williams, D. A., Williams, J., Williamson, T., Wolter, A., Wong, Y. W., Wood, M., Wunderlich, C., Yamamoto, T., Yamamoto, H., Yamane, Y., Yamazaki, R., Yanagita, S., Yang, L., Yoo, S., Yoshida, T., Yoshikoshi, T., Yu, P., Yusafzai, A., Zacharias, M., Zaharijas, G., Zaldivar, B., Zampieri, L., Zanmar Sanchez, R., Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zenin, A., Zerwekh, A., Zhdanov, V. 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O., Antonelli, L. A., Aramo, C., Araudo, A., Armstrong, T., Arqueros, F., Asano, K., Ascas??bar, Y., Ashley, M., Balazs, C., Ballester, O., Baquero Larriva, A., Barbosa Martins, V., Barkov, M., Barres de Almeida, U., Barrio, J. A., Bastieri, D., Becerra, J., Beck, G., Becker Tjus, J., Benbow, W., Benito, M., Berge, D., Bernardini, E., Bernl??hr, K., Berti, A., Bertucci, B., Beshley, V., Biasuzzi, B., Biland, A., Bissaldi, E., Biteau, J., Blanch, O., Blazek, J., Bocchino, F., Boisson, C., Bonneau Arbeletche, L., Bordas, P., Bosnjak, Z., Bottacini, E., Bozhilov, V., Bregeon, J., Brill, A., Bringmann, T., Brown, A. 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B., H??tten, M., Iarlori, M., Inada, T., Inoue, S., Iocco, F., Iori, M., Jamrozy, M., Janecek, P., Jin, W., Jouvin, L., Jurysek, J., Karukes, E., Katarzy??ski, K., Kazanas, D., Kerszberg, D., Kherlakian, M. C., Kissmann, R., Kn??dlseder, J., Kobayashi, Y., Kohri, K., Komin, N., Kubo, H., Kushida, J., Lamanna, G., Lapington, J., Laporte, P., Leigui de Oliveira, M. A., Lenain, J., Leone, F., Leto, G., Lindfors, E., Lohse, T., Lombardi, S., Longo, F., Lopez, A., L??pez, M., L??pez-Coto, R., Loporchio, S., Luque-Escamilla, P. L., Mach, E., Maggio, C., Maier, G., Mallamaci, M., Malta Nunes de Almeida, R., Mandat, D., Manganaro, M., Mangano, S., Manic??, G., Marculewicz, M., Mariotti, M., Markoff, S., Marquez, P., Mart??, J., Martinez, O., Mart??nez, M., Mart??nez, G., Mart??nez-Huerta, H., Maurin, G., Mazin, D., Mbarubucyeye, J. D., Medina Miranda, D., Meyer, M., Miceli, M., Miener, T., Minev, M., Miranda, J. 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L., Queiroz, F., Quirrenbach, A., Rain??, S., Rando, R., Razzaque, S., Recchia, S., Reimer, O., Reisenegger, A., Renier, Y., Rhode, W., Ribeiro, D., Rib??, M., Richtler, T., Rico, J., Rieger, F., Rinchiuso, L., Rizi, V., Rodriguez, J., Rodriguez Fernandez, G., Rodriguez Ramirez, J. C., Rojas, G., Romano, P., Romeo, G., Rosado, J., Rowell, G., Rudak, B., Russo, F., Sadeh, I., S??ther Hatlen, E., Safi-Harb, S., Salesa Greus, F., Salina, G., Sanchez, D., S??nchez-Conde, M., Sangiorgi, P., Sano, H., Santander, M., Santos, E. M., Santos-Lima, R., Sanuy, A., Sarkar, S., Saturni, F. G., Sawangwit, U., Schussler, F., Schwanke, U., Sciacca, E., Scuderi, S., Seglar-Arroyo, M., Sergijenko, O., Servillat, M., Seweryn, K., Shalchi, A., Sharma, P., Shellard, R. C., Siejkowski, H., Silk, J., Siqueira, C., Sliusar, V., S??owikowska, A., Sokolenko, A., Sol, H., Spencer, S., Stamerra, A., Stani??, S., Starling, R., Stolarczyk, T., Straumann, U., Stri??kovi??, J., Suda, Y., Suomijarvi, T., wierk, P., Tavecchio, F., Taylor, L., Tejedor, L. A., Teshima, M., Testa, V., Tibaldo, L., Todero Peixoto, C. J., Tokanai, F., Tonev, D., Tosti, G., Tosti, L., Tothill, N., Truzzi, S., Travnicek, P., Vagelli, V., Vallage, B., Vallania, P., van Eldik, C., Vandenbroucke, J., Varner, G. S., Vassiliev, V., V??zquez Acosta, M., Vecchi, M., Ventura, S., Vercellone, S., Vergani, S., Verna, G., Viana, A., Vigorito, C. F., Vink, J., Vitale, V., Vorobiov, S., Vovk, I., Vuillaume, T., Wagner, S. J., Walter, R., Watson, J., Weniger, C., White, R., White, M., Wiemann, R., Wierzcholska, A., Will, M., Williams, D. A., Wischnewski, R., Yanagita, S., Yang, L., Yoshikoshi, T., Zacharias, M., Zaharijas, G., Zakaria, A. A., Zampieri, L., Zanin, R., Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. I., ivec, M., ITA, USA, GBR, FRA, DEU, ESP, AUT, BEL, BRA, HRV, DNK, JPN, IRL, NLD, POL, SVN, CHE, High Energy Astrophys. & Astropart. Phys (API, FNWI), GRAPPA (ITFA, IoP, FNWI), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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 des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Iocco, Fabio, Anguner, E. O., Ascasibar, Y., Bernlohr, K., Colak, M., D'Ai, A., de Angelis, A., de Caprio, V., de Cassia dos Anjos, R., de Lotto, B., de Martino, D., de Ona Wilhelmi, E., de Palma, F., Dominguez, A., Elsasser, D., Gonzalez, M. M., Hernandez Cadena, S., Horandel, J., Hutten, M., Katarzynski, K., Knodlseder, J., Lopez, M., Lopez-Coto, R., Manico, G., Marti, J., Martinez, M., Martinez, G., Martinez-Huerta, H., Nikolajuk, M., Pavletic, L., Perez-Romero, J., Puhlhofer, G., Raino, S., Ribo, M., Saether Hatlen, E., Sanchez-Conde, M., Slowikowska, A., Stanic, S., Striskovic, J., Swierk, P., Vazquez Acosta, M., Zivec, M., Consortium, The CTA, Acharyya A., Adam R., Adams C., Agudo I., Aguirre-Santaella A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Alves Batista R., Amati L., Ambrosi G., Anguner E.O., Antonelli L.A., Aramo C., Araudo A., Armstrong T., Arqueros F., Asano K., Ascasibar Y., Ashley M., Balazs C., Ballester O., Baquero Larriva A., Barbosa Martins V., Barkov M., Barres de Almeida U., Barrio J.A., Bastieri D., Becerra J., Beck G., Becker Tjus J., Benbow W., Benito M., Berge D., Bernardini E., Bernlohr K., Berti A., Bertucci B., Beshley V., Biasuzzi B., Biland A., Bissaldi E., Biteau J., Blanch O., Blazek J., Bocchino F., Boisson C., Bonneau Arbeletche L., Bordas P., Bosnjak Z., Bottacini E., Bozhilov V., Bregeon J., Brill A., Bringmann T., Brown A.M., Brun P., Brun F., Bruno P., Bulgarelli A., Burton M., Burtovoi A., Buscemi M., Cameron R., Capasso M., Caproni A., Capuzzo-Dolcetta R., Caraveo P., Carosi R., Carosi A., Casanova S., Cascone E., Cassol F., Catalani F., Cauz D., Cerruti M., Chadwick P., Chaty S., Chen A., Chernyakova M., Chiaro G., Chiavassa A., Chikawa M., Chudoba J., Colak M., Conforti V., Coniglione R., Conte F., Contreras J.L., Coronado-Blazquez J., Costa A., Costantini H., Cotter G., Cristofari P., D'Ai A., D'Ammando F., Damone L.A., Daniel M.K., Dazzi F., de Angelis A., de Caprio V., de Cassia dos Anjos R., de Gouveia Dal Pino E.M., de Lotto B., de Martino D., de Ona Wilhelmi E., de Palma F., de Souza V., Delgado C., Delgado Giler A.G., della Volpe D., Depaoli D., Di Girolamo T., Di Pierro F., Di Venere L., Diebold S., Dmytriiev A., Dominguez A., Donini A., Doro M., Ebr J., Eckner C., Edwards T.D.P., Ekoume T.R.N., Elsasser D., Evoli C., Falceta-Goncalves D., Fedorova E., Fegan S., Feng Q., Ferrand G., Ferrara G., Fiandrini E., Fiasson A., Filipovic M., Fioretti V., Fiori M., Foffano L., Fontaine G., Fornieri O., Franco F.J., Fukami S., Fukui Y., Gaggero D., Galaz G., Gammaldi V., Garcia E., Garczarczyk M., Gascon D., Gent A., Ghalumyan A., Gianotti F., Giarrusso M., Giavitto G., Giglietto N., Giordano F., Giuliani A., Glicenstein J., Gnatyk R., Goldoni P., Gonzalez M.M., Gourgouliatos K., Granot J., Grasso D., Green J., Grillo A., Gueta O., Gunji S., Halim A., Hassan T., Heller M., Hernandez Cadena S., Hiroshima N., Hnatyk B., Hofmann W., Holder J., Horan D., Horandel J., Horvath P., Hovatta T., Hrabovsky M., Hrupec D., Hughes G., Humensky T.B., Hutten M., Iarlori M., Inada T., Inoue S., Iocco F., Iori M., Jamrozy M., Janecek P., Jin W., Jouvin L., Jurysek J., Karukes E., Katarzynski K., Kazanas D., Kerszberg D., Kherlakian M.C., Kissmann R., Knodlseder J., Kobayashi Y., Kohri K., Komin N., Kubo H., Kushida J., Lamanna G., Lapington J., Laporte P., Leigui de Oliveira M.A., Lenain J., Leone F., Leto G., Lindfors E., Lohse T., Lombardi S., Longo F., Lopez A., Lopez M., Lopez-Coto R., Loporchio S., Luque-Escamilla P.L., Mach E., Maggio C., Maier G., Mallamaci M., Malta Nunes de Almeida R., Mandat D., Manganaro M., Mangano S., Manico G., Marculewicz M., Mariotti M., Markoff S., Marquez P., Marti J., Martinez O., Martinez M., Martinez G., Martinez-Huerta H., Maurin G., Mazin D., Mbarubucyeye J.D., Medina Miranda D., Meyer M., Miceli M., Miener T., Minev M., Miranda J.M., Mirzoyan R., Mizuno T., Mode B., Moderski R., Mohrmann L., Molina E., Montaruli T., Moralejo A., Morcuende-Parrilla D., Morselli A., Mukherjee R., Mundell C., Nagai A., Nakamori T., Nemmen R., Niemiec J., Nieto D., Nikolajuk M., Ninci D., Noda K., Nosek D., Nozaki S., Ohira Y., Ohishi M., Ohtani Y., Oka T., Okumura A., Ong R.A., Orienti M., Orito R., Orlandini M., Orlando S., Orlando E., Ostrowski M., Oya I., Pagano I., Pagliaro A., Palatiello M., Pantaleo F.R., Paredes J.M., Pareschi G., Parmiggiani N., Patricelli B., Pavletic L., Pe'Er A., Pecimotika M., Perez-Romero J., Persic M., Petruk O., Pfrang K., Piano G., Piatteli P., Pietropaolo E., Pillera R., Pilszyk B., Pintore F., Pohl M., Poireau V., Prado R.R., Prandini E., Prast J., Principe G., Prokoph H., Prouza M., Przybilski H., Puhlhofer G., Pumo M.L., Queiroz F., Quirrenbach A., Raino S., Rando R., Razzaque S., Recchia S., Reimer O., Reisenegger A., Renier Y., Rhode W., Ribeiro D., Ribo M., Richtler T., Rico J., Rieger F., Rinchiuso L., Rizi V., Rodriguez J., Rodriguez Fernandez G., Rodriguez Ramirez J.C., Rojas G., Romano P., Romeo G., Rosado J., Rowell G., Rudak B., Russo F., Sadeh I., Saether Hatlen E., Safi-Harb S., Salesa Greus F., Salina G., Sanchez D., Sanchez-Conde M., Sangiorgi P., Sano H., Santander M., Santos E.M., Santos-Lima R., Sanuy A., Sarkar S., Saturni F.G., Sawangwit U., Schussler F., Schwanke U., Sciacca E., Scuderi S., Seglar-Arroyo M., Sergijenko O., Servillat M., Seweryn K., Shalchi A., Sharma P., Shellard R.C., Siejkowski H., Silk J., Siqueira C., Sliusar V., Slowikowska A., Sokolenko A., Sol H., Spencer S., Stamerra A., Stanic S., Starling R., Stolarczyk T., Straumann U., Striskovic J., Suda Y., Suomijarvi T., Swierk P., Tavecchio F., Taylor L., Tejedor L.A., Teshima M., Testa V., Tibaldo L., Todero Peixoto C.J., Tokanai F., Tonev D., Tosti G., Tosti L., Tothill N., Truzzi S., Travnicek P., Vagelli V., Vallage B., Vallania P., van Eldik C., Vandenbroucke J., Varner G.S., Vassiliev V., Vazquez Acosta M., Vecchi M., Ventura S., Vercellone S., Vergani S., Verna G., Viana A., Vigorito C.F., Vink J., Vitale V., Vorobiov S., Vovk I., Vuillaume T., Wagner S.J., Walter R., Watson J., Weniger C., White R., White M., Wiemann R., Wierzcholska A., Will M., Williams D.A., Wischnewski R., Yanagita S., Yang L., Yoshikoshi T., Zacharias M., Zaharijas G., Zakaria A.A., Zampieri L., Zanin R., Zaric D., Zavrtanik M., Zavrtanik D., Zdziarski A.A., Zech A., Zechlin H., Zhdanov V.I., and Zivec M.
Subjects: Cherenkov Telescope Array, MATÉRIA ESCURA, scale: TeV, Astronomy, atmosphere [Cherenkov counter], dark matter experiment, Dark matter theory, energy resolution, Gamma ray experiments, Particle, Astrophysics, cosmic background radiation, 01 natural sciences, 7. Clean energy, High Energy Physics - Phenomenology (hep-ph), benchmark, WIMP, HESS, energy: flux, TeV [scale], relativistic [charged particle], gamma ray experiment, MAGIC (telescope), Monte Carlo, Event reconstruction, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Contraction, spatial distribution, track data analysis, density [dark matter], Clumpy, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, High Energy Physics - Phenomenology, dark matter experiments, dark matter theory, gamma ray experiments, galaxy morphology, Dark matter experiments, Física nuclear, VERITAS, Astrophysics - High Energy Astrophysical Phenomena, Simulations, noise, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, satellite, Cosmic background radiation, FOS: Physical sciences, Annihilation, dark matter: density, Astrophysics::Cosmology and Extragalactic Astrophysics, Cherenkov counter: atmosphere, heavy [dark matter], annihilation [dark matter], GLAST, Galaxy morphology, cosmic radiation [p], 0103 physical sciences, Cherenkov [radiation], Candidates, ddc:530, AGN, Cherenkov radiation, Radiative Processes, thermal [cross section], 010308 nuclear & particles physics, Física, dark matter: annihilation, Gamma-Ray Signals, dark matter, Galactic Center, TeV gamma-ray astronomy, Astronomy and Astrophysics, Mass, radiation: Cherenkov, sensitivity, MAGIC, Galaxy, Astronomía, dark matter: heavy, gamma ray, p: cosmic radiation, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], correlation, charged particle: relativistic, flux [energy], galaxy, supersymmetry, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cross section: thermal
Abstract: Full list of authors: Acharyya, A.; Adam, R.; Adams, C.; Agudo, I.; Aguirre-Santaella, A.; Alfaro, R.; Alfaro, J.; Alispach, C.; Aloisio, R.; Alves Batista, R.; Amati, L.; Ambrosi, G.; Angüner, E. O.; Antonelli, L. A.; Aramo, C.; Araudo, A.; Armstrong, T.; Arqueros, F.; Asano, K.; Ascasíbar, Y. Ashley, M.; Balazs, C.; Ballester, O.; Baquero Larriva, A.; Barbosa Martins, V.; Barkov, M.; Barres de Almeida, U.; Barrio, J. A.; Bastieri, D.; Becerra, J.; Beck, G.; Becker Tjus, J.; Benbow, W.; Benito, M.; Berge, D.; Bernardini, E.; Bernlöhr, K.; Berti, A.; Bertucci, B.; Beshley, V.; Biasuzzi, B.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Blazek, J.; Bocchino, F.; Boisson, C.; Bonneau Arbeletche, L.; Bordas, P.; Bosnjak, Z.; Bottacini, E.; Bozhilov, V.; Bregeon, J.; Brill, A.; Bringmann, T.; Brown, A. M.; Brun, P.; Brun, F.; Bruno, P.; Bulgarelli, A.; Burton, M.; Burtovoi, A.; Buscemi, M.; Cameron, R.; Capasso, M.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Carosi, R.; Carosi, A.; Casanova, S.; Cascone, E.; Cassol, F.; Catalani, F.; Cauz, D.; Cerruti, M.; Chadwick, P.; Chaty, S.; Chen, A.; Chernyakova, M.; Chiaro, G.; Chiavassa, A.; Chikawa, M.; Chudoba, J.; Çolak, M.; Conforti, V.; Coniglione, R.; Conte, F.; Contreras, J. L.; Coronado-Blazquez, J.; Costa, A.; Costantini, H.; Cotter, G.; Cristofari, P.; D'Aimath, A.; D'Ammando, F.; Damone, L. A.; Daniel, M. K.; Dazzi, F.; De Angelis, A.; De Caprio, V.; de Cássia dos Anjos, R.; de Gouveia Dal Pino, E. M.; De Lotto, B.; De Martino, D.; de Oña Wilhelmi, E.; De Palma, F.; de Souza, V.; Delgado, C.; Delgado Giler, A. G.; della Volpe, D.; Depaoli, D.; Di Girolamo, T.; Di Pierro, F.; Di Venere, L.; Diebold, S.; Dmytriiev, A.; Domínguez, A.; Donini, A.; Doro, M.; Ebr, J.; Eckner, C.; Edwards, T. D. P.; Ekoume, T. R. N.; Elsässer, D.; Evoli, C.; Falceta-Goncalves, D.; Fedorova, E.; Fegan, S.; Feng, Q.; Ferrand, G.; Ferrara, G.; Fiandrini, E.; Fiasson, A.; Filipovic, M.; Fioretti, V.; Fiori, M.; Foffano, L.; Fontaine, G.; Fornieri, O.; Franco, F. J.; Fukami, S.; Fukui, Y.; Gaggero, D.; Galaz, G.; Gammaldi, V.; Garcia, E.; Garczarczyk, M.; Gascon, D.; Gent, A.; Ghalumyan, A.; Gianotti, F.; Giarrusso, M.; Giavitto, G.; Giglietto, N.; Giordano, F.; Giuliani, A.; Glicenstein, J.; Gnatyk, R.; Goldoni, P.; González, M. M.; Gourgouliatos, K.; Granot, J.; Grasso, D.; Green, J.; Grillo, A.; Gueta, O.; Gunji, S.; Halim, A.; Hassan, T.; Heller, M.; Hernández Cadena, S.; Hiroshima, N.; Hnatyk, B.; Hofmann, W.; Holder, J.; Horan, D.; Hörandel, J.; Horvath, P.; Hovatta, T.; Hrabovsky, M.; Hrupec, D.; Hughes, G.; Humensky, T. B.; Hütten, M.; Iarlori, M.; Inada, T.; Inoue, S.; Iocco, F.; Iori, M.; Jamrozy, M.; Janecek, P.; Jin, W.; Jouvin, L.; Jurysek, J.; Karukes, E.; Katarzyński, K.; Kazanas, D.; Kerszberg, D.; Kherlakian, M. C.; Kissmann, R.; Knödlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kubo, H.; Kushida, J.; Lamanna, G.; Lapington, J.; Laporte, P.; Leigui de Oliveira, M. A.; Lenain, J.; Leone, F.; Leto, G.; Lindfors, E.; Lohse, T.; Lombardi, S.; Longo, F.; Lopez, A.; López, M.; López-Coto, R.; Loporchio, S.; Luque-Escamilla, P. L.; Mach, E.; Maggio, C.; Maier, G.; Mallamaci, M.; Malta Nunes de Almeida, R.; Mandat, D.; Manganaro, M.; Mangano, S.; Manicò, G.; Marculewicz, M.; Mariotti, M.; Markoff, S.; Marquez, P.; Martí, J.; Martinez, O.; Martínez, M.; Martínez, G.; Martínez-Huerta, H.; Maurin, G.; Mazin, D.; Mbarubucyeye, J. D.; Medina Miranda, D.; Meyer, M.; Miceli, M.; Miener, T.; Minev, M.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Mode, B.; Moderski, R.; Mohrmann, L.; Molina, E.; Montaruli, T.; Moralejo, A.; Morcuende-Parrilla, D.; Morselli, A.; Mukherjee, R.; Mundell, C.; Nagai, A.; Nakamori, T.; Nemmen, R.; Niemiec, J.; Nieto, D.; Nikołajuk, M.; Ninci, D.; Noda, K.; Nosek, D.; Nozaki, S.; Ohira, Y.; Ohishi, M.; Ohtani, Y.; Oka, T.; Okumura, A.; Ong, R. A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, S.; Orlando, E.; Ostrowski, M.; Oya, I.; Pagano, I.; Pagliaro, A.; Palatiello, M.; Pantaleo, F. R.; Paredes, J. M.; Pareschi, G.; Parmiggiani, N.; Patricelli, B.; Pavletić, L.; Pe'er, A.; Pecimotika, M.; Pérez-Romero, J.; Persic, M.; Petruk, O.; Pfrang, K.; Piano, G.; Piatteli, P.; Pietropaolo, E.; Pillera, R.; Pilszyk, B.; Pintore, F.; Pohl, M.; Poireau, V.; Prado, R. R.; Prandini, E.; Prast, J.; Principe, G.; Prokoph, H.; Prouza, M.; Przybilski, H.; Pühlhofer, G.; Pumo, M. L.; Queiroz, F.; Quirrenbach, A.; Rainò, S.; Rando, R.; Razzaque, S.; Recchia, S.; Reimer, O.; Reisenegger, A.; Renier, Y.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richtler, T.; Rico, J.; Rieger, F.; Rinchiuso, L.; Rizi, V.; Rodriguez, J.; Rodriguez Fernandez, G.; Rodriguez Ramirez, J. C.; Rojas, G.; Romano, P.; Romeo, G.; Rosado, J.; Rowell, G.; Rudak, B.; Russo, F.; Sadeh, I.; Sæther Hatlen, E.; Safi-Harb, S.; Salesa Greus, F.; Salina, G.; Sanchez, D.; Sánchez-Conde, M.; Sangiorgi, P.; Sano, H.; Santander, M.; Santos, E. M.; Santos-Lima, R.; Sanuy, A.; Sarkar, S.; Saturni, F. G.; Sawangwit, U.; Schussler, F.; Schwanke, U.; Sciacca, E.; Scuderi, S.; Seglar-Arroyo, M.; Sergijenko, O.; Servillat, M.; Seweryn, K.; Shalchi, A.; Sharma, P.; Shellard, R. C.; Siejkowski, H.; Silk, J.; Siqueira, C.; Sliusar, V.; Słowikowska, A.; Sokolenko, A.; Sol, H.; Spencer, S.; Stamerra, A.; Stanič, S.; Starling, R.; Stolarczyk, T.; Straumann, U.; Strišković, J.; Suda, Y.; Suomijarvi, T.; Świerk, P.; Tavecchio, F.; Taylor, L.; Tejedor, L. A.; Teshima, M.; Testa, V.; Tibaldo, L.; Todero Peixoto, C. J.; Tokanai, F.; Tonev, D.; Tosti, G.; Tosti, L.; Tothill, N.; Truzzi, S.; Travnicek, P.; Vagelli, V.; Vallage, B.; Vallania, P.; van Eldik, C.; Vandenbroucke, J.; Varner, G. S.; Vassiliev, V.; Vázquez Acosta, M.; Vecchi, M.; Ventura, S.; Vercellone, S.; Vergani, S.; Verna, G.; Viana, A.; Vigorito, C. F.; Vink, J.; Vitale, V.; Vorobiov, S.; Vovk, I.; Vuillaume, T.; Wagner, S. J.; Walter, R.; Watson, J.; Weniger, C.; White, R.; White, M.; Wiemann, R.; Wierzcholska, A.; Will, M.; Williams, D. A.; Wischnewski, R.; Yanagita, S.; Yang, L.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zakaria, A. A.; Zampieri, L.; Zanin, R.; Zaric, D.; Zavrtanik, M.; Zavrtanik, D.; Zdziarski, A. A.; Zech, A.; Zechlin, H.; Zhdanov, V. I.; Živec, M.-- This is an open access article published by IOP Publishing Ltd on behalf of Sissa Medialab. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI., We provide an updated assessment of the power of the Cherenkov Telescope Array (CTA) to search for thermally produced dark matter at the TeV scale, via the associated gamma-ray signal from pair-annihilating dark matter particles in the region around the Galactic centre. We find that CTA will open a new window of discovery potential, significantly extending the range of robustly testable models given a standard cuspy profile of the dark matter density distribution. Importantly, even for a cored profile, the projected sensitivity of CTA will be sufficient to probe various well-motivated models of thermally produced dark matter at the TeV scale. This is due to CTA's unprecedented sensitivity, angular and energy resolutions, and the planned observational strategy. The survey of the inner Galaxy will cover a much larger region than corresponding previous observational campaigns with imaging atmospheric Cherenkov telescopes. CTA will map with unprecedented precision the large-scale diffuse emission in high-energy gamma rays, constituting a background for dark matter searches for which we adopt state-of-the-art models based on current data. Throughout our analysis, we use up-to-date event reconstruction Monte Carlo tools developed by the CTA consortium, and pay special attention to quantifying the level of instrumental systematic uncertainties, as well as background template systematic errors, required to probe thermally produced dark matter at these energies. © 2021 The Author(s)., We gratefully acknowledge financial support from the following agencies and organisations: State Committee of Science of Armenia, Armenia; The Australian Research Council, Astronomy Australia Ltd, The University of Adelaide, Australian National University, Monash University, The University of New South Wales, The University of Sydney, Western Sydney University, Australia; Federal Ministry of Education, Science and Research, and Innsbruck University, Austria; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Fundacao de Amparo a Pesquisa do Estado do Rio de Janeiro (FAPERJ), Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), Ministry of Science, Technology, Innovations and Communications (MCTIC), and Instituto Serrapilheira, Brasil; Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018, Bulgaria; The Natural Sciences and Engineering Research Council of Canada and the Canadian Space Agency, Canada; CONICYT-Chile grants CATA AFB 170002, ANID PIA/APOYO AFB 180002, ACT 1406, FONDECYT-Chile grants, 1161463, 1170171, 1190886, 1171421, 1170345, 1201582, Gemini-ANID 32180007, Chile; Croatian Science Foundation, Rudjer Boskovic Institute, University of Osijek, University of Rijeka, University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture, University of Zagreb, Faculty of Electrical Engineering and Computing, Croatia; Ministry of Education, Youth and Sports, MEYS LM2015046, LM2018105, LTT17006, EU/MEYS CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/18_046/0016007 and CZ.02.1.01/0.0/0.0/16_019/0000754, Czech Republic; Academy of Finland (grant nr.317636, 320045, 317383 and 320085), Finland; Ministry of Higher Education and Research, CNRS-INSU and CNRS-IN2P3, CEA-Irfu, ANR, Regional Council Ile de France, Labex ENIGMASS, OSUG2020, P2IO and OCEVU, France; Max Planck Society, BMBF, DESY, Helmholtz Association, Germany; Department of Atomic Energy, Department of Science and Technology, India; Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare (INFN), MIUR, Istituto Nazionale di Astrofisica (INAF-OABRERA) Grant Fondazione Cariplo/Regione Lombardia ID 2014-1980/RST_ERC, Italy; ICRR, University of Tokyo, JSPS, MEXT, Japan; Netherlands Research School for Astronomy (NOVA), Netherlands Organization for Scientific Research (NWO), Netherlands; University of Oslo, Norway; Ministry of Science and Higher Education, DIR/WK/2017/12, the National Centre for Research and Development and the National Science Centre, UMO-2016/22/M/ST9/00583, Poland; Slovenian Research Agency, grants P1-0031, P1-0385, I0-0033, J1-9146, J1-1700, N1-0111, and the Young Researcher program, Slovenia; South African Department of Science and Technology and National Research Foundation through the South African Gamma-Ray Astronomy Programme, South Africa; The Spanish Ministry of Science and Innovation and the Spanish Research State Agency (AEI) through grants AYA2016-79724-C4-1-P, AYA2016-80889-P, AYA2016-76012-C3-1-P, BES-2016-076342, ESP2017-87055-C2-1-P, FPA2017-82729-C6-1-R, FPA2017-82729-C6-2-R, FPA2017-82729-C6-3-R, FPA2017-82729-C6-4-R, FPA2017-82729-C6-5-R, FPA2017-82729-C6-6-R, PGC2018-095161-B-I00, PGC2018-095512-B-I00; the \Centro de Excelencia Severo Ochoa"program through grants no. SEV-2015-0548, SEV-2016-0597, SEV-2016-0588, SEV-2017-0709; the "Unidad de Excelencia Maria de Maeztu" program through grant no. MDM-2015-0509; the "Ramon y Cajal" programme through grants RYC-2013-14511, RyC-2013-14660, RYC-2017-22665; and the MultiDark Consolider Network FPA2017-90566-REDC. Atraccion de Talento contract no. 2016-T1/TIC-1542 granted by the Comunidad de Madrid; the "Postdoctoral Junior Leader Fellowship" programme from La Caixa Banking Foundation, grants no. LCF/BQ/LI18/11630014 and LCF/BQ/PI18/11630012; the "Programa Operativo" FEDER2014-2020, Consejeria de Economia y Conocimiento de la Junta de Andalucia (ref. 1257737), PAIDI 2020 (ref. P18-FR-1580), and Universidad de Jaen; the Spanish AEI EQC2018-005094-P FEDER 2014-2020; the European Union's "Horizon 2020" research and innovation programme under Marie Sklodowska-Curie grant agreement no. 665919; and the ESCAPE project with grant no. GA:824064, Spain; Swedish Research Council, Royal Physiographic Society of Lund, Royal Swedish Academy of Sciences, The Swedish National Infrastructure for Computing (SNIC) at Lunarc (Lund), Sweden; State Secretariat for Education, Research and Innovation (SERI) and Swiss National Science Foundation (SNSF), Switzerland; Durham University, Leverhulme Trust, Liverpool University, University of Leicester, University of Oxford, Royal Society, Science and Technology Facilities Council, U.K.; U.S. National Science Foundation, U.S. Department of Energy, Argonne National Laboratory, Barnard College, University of California, University of Chicago, Columbia University, Georgia Institute of Technology, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI program), Iowa State University, the Smithsonian Institution, Washington University McDonnell Center for the Space Sciences, The University of Wisconsin and the Wisconsin Alumni Research Foundation, U.S.A. The research leading to these results has received funding from the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreements No 262053 and No 317446. This project is receiving funding from the European Union's Horizon 2020 research and innovation programs under agreement No 676134.
Published: 2022

3. Phenomenology of the Dark Matter sector in the Two Higgs Doublet Model with Complex Scalar Singlet extension

Author: Dutta, Juhi, Moortgat-Pick, Gudrid, and Schreiber, Merle
Subjects: flavor, dark matter, heavy, dark matter: mass, High Energy Physics::Phenomenology, gravitational radiation, Higgs particle: doublet: 2, singlet: scalar, Astrophysics::Cosmology and Extragalactic Astrophysics, baryogenesis, singlet, scalar, doublet, benchmark, dark matter: heavy, CERN LHC Coll: upgrade, ddc:530, CERN LHC Coll, upgrade, dark matter: scalar, dark matter, scalar, dark matter, mass
Abstract: 41st International Conference on High Energy physics, ICHEP2022, Bologna, Italy; Proceedings of Science / International School for Advanced Studies (ICHEP2022), 265 (2023). doi:10.22323/1.414.0265, Extensions of the Two Higgs Doublet model with a complex scalar singlet (2HDMS) may accommodate all current experimental constraints and are highly motivated candidates for Beyond Standard Model Physics. In this work, we focus on the phenomenology of the 2HDMS with the complex scalar singlet as the dark matter candidate. We study variations of dark matter observables with respect to the model parameters and present representative benchmark points allowed by existing experimental constraints from dark matter, flavour physics and collider searches. Further, we discuss the discovery potential of observing such scenarios at future colliders., Published by SISSA, Trieste
Published: 2022
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4. First implications of Tibet AS$_\gamma$ data for heavy dark matter

Author: Esmaili, Arman, Serpico, Pasquale D., Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), and Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)
Subjects: showers: atmosphere, air, background, shower detector, Astrophysics::High Energy Astrophysical Phenomena, photon, Astrophysics::Instrumentation and Methods for Astrophysics, sensitivity, boson: massive, IceCube, boson: final state, High Energy Physics - Phenomenology, gamma ray: emission, benchmark, dark matter: heavy, cosmic radiation: galaxy, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], spectral, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract: Extensive air shower detectors of gamma rays in the sub-PeV energy region provide a new and relatively unexplored window for dark matter searches. Here we derive some implications of the recently published Tibet AS$_\gamma$ data for decaying dark matter candidates. The available spectral information is already useful in obtaining competitive constraints, surpassing existing limits above 10 PeV mass for hadronic or massive boson final states. This is particularly true if accounting for a benchmark astrophysical background of Galactic cosmic rays in the (0.1-1) PeV range. By relying on the arrival distribution of the photons, we show that significantly better sensitivity can be attained, comparable or better than IceCube also for most leptonic final states. Full data exploitation requires however further information disclosure., Comment: 5 pages, 2 figures. v2: more decay channels included, minor clarifications added, matches the version published in PRD Letters
Published: 2021

5. Heavy dark matter through the dilaton portal

Author: Benjamin Fuks, Seung Joo Lee, Mark D. Goodsell, Manuel Utsch, Dong Woo Kang, Pyungwon Ko, Laboratoire de Physique Théorique et Hautes Energies (LPTHE), and Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear and High Energy Physics, Particle physics, Dark matter, Scalar (mathematics), gluon: scattering, FOS: Physical sciences, dark matter: density, dark matter: production, 01 natural sciences, effective field theory, High Energy Physics - Phenomenology (hep-ph), dilaton: coupling, fermion: Majorana, 0103 physical sciences, CERN LHC Coll: upgrade, Effective field theory, mixing, invariance: gauge, FCC, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, 010306 general physics, Phenomenological Models, Physics, dark matter: vector, Unitarity, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Gluon, coupling: Higgs, High Energy Physics - Phenomenology, dark matter: heavy, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Higgs boson, field theory: vector, lcsh:QC770-798, Dilaton, direct detection, unitarity: constraint, Majorana fermion
Abstract: We re-examine current and future constraints on a heavy dilaton coupled to a simple dark sector consisting of a Majorana fermion or a St\"uckelberg vector field. We include three different treatments of dilaton-Higgs mixing, paying particular attention to a gauge-invariant formulation of the model. Moreover, we also invite readers to re-examine effective field theories of vector dark matter, which we show are missing important terms. Along with the latest Higgs coupling data, heavy scalar search results, and dark matter density/direct detection constraints, we study the LHC bounds on the model and estimate the prospects of dark matter production at the future HL-LHC and 100 TeV FCC colliders. We additionally compute novel perturbative unitarity constraints involving vector dark matter, dilaton and gluon scattering., Comment: 18 pages, 10 figures
Published: 2020
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6. Equilibrium axisymmetric halo model for the Milky Way and its implications for direct and indirect dark matter searches

Author: Mihael Petač, Laboratoire Univers et Particules de Montpellier (LUPM), and Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Milky Way, Dark matter, FOS: Physical sciences, Astrophysics, dark matter: density, 01 natural sciences, Bayesian, flux: time dependence, symmetry: axial, anisotropy: velocity, High Energy Physics - Experiment, dark matter: coupling, High Energy Physics - Experiment (hep-ex), phase space, High Energy Physics - Phenomenology (hep-ph), near detector, 0103 physical sciences, conservation law, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Sensitivity (control systems), 010306 general physics, halo: rotation, Physics, 010308 nuclear & particles physics, dark matter: mass, Galactic Center, scattering: operator, Relative velocity, Coupling (probability), sensitivity, Astrophysics - Astrophysics of Galaxies, Baryon, High Energy Physics - Phenomenology, modulation, halo: model, annihilation, dark matter: heavy, kinematics, Astrophysics of Galaxies (astro-ph.GA), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], direct detection, Halo, dark matter: velocity, galaxy, velocity dependence, numerical calculations: Monte Carlo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract: We for the first time provide self-consistent axisymmetric phase-space distribution models for the Milky Way's dark matter (DM) halo which are carefully matched against the latest kinematic measurements through Bayesian analysis. By using broad priors on the individual galactic components, we derive conservative estimates for the astrophysical factors entering the interpretation of direct and indirect DM searches. While the resulting DM density profiles are in good agreement with previous studies, implying $\rho_\odot \approx 10^{-2} \, M_\odot / \mathrm{pc}^3$, the presence of baryonic disc leads to significant differences in the local DM velocity distribution in comparison with the standard halo model. For direct detection, this implies roughly 30% stronger cross-section limits at DM masses near detectors maximum sensitivity and up to an order of magnitude weaker limits at the lower end of the mass range. Furthermore, by performing Monte-Carlo simulations for the upcoming DARWIN and DarkSide-20k experiments, we demonstrate that upon successful detection of heavy DM with coupling just below the current limits, the carefully constructed axisymmetric models can eliminate bias and reduce uncertainties by more then 50% in the reconstructed DM coupling and mass, but also help in a more reliable determination of the scattering operator. Furthermore, the velocity anisotropies induced by the baryonic disc can lead to significantly larger annual modulation amplitude and sizable differences in the directional distribution of the expected DM-induced events. For indirect searches, we provide the differential $J$-factors and compute several moments of the relative velocity distribution that are needed for predicting the rate of velocity-dependent annihilations. However, we find that accurate predictions are still hindered by large uncertainties regarding the DM distribution near the galactic center., Comment: Article consists of 44 pages, 15 figures. We additionally provide the tabulated values of astrophysical factors (in total 18 files) obtained in this work
Published: 2020

7. Hunting for heavy Dark Matter in the Galactic Center with ground-based Cherenkov telescopes

Author: Nicholas L. Rodd, Lucia Rinchiuso, Tracy R. Slatyer, Emmanuel Moulin, 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
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), scale: TeV, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Wino, FOS: Physical sciences, photon: spectrum, Astrophysics, dark matter: density, 7. Clean energy, WIMP: dark matter, thermal, High Energy Physics - Phenomenology (hep-ph), WIMP, HESS, Cherenkov radiation, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, Annihilation, background, photon: annihilation, Galactic Center, Electroweak interaction, scale: electroweak interaction, dark matter: annihilation, Cherenkov Telescope Array, sensitivity, Universe, High Energy Physics - Phenomenology, Cherenkov counter, dark matter: heavy, gamma ray, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A TeV scale electroweak particle is a well motivated candidate for the dark matter (DM) of our Universe. Yet such a particle may only be detectable using indirect detection instruments sensitive to TeV-scale gamma rays that can result from dark matter annihilations. We present a mock analysis of the sensitivity for the present ground-based Cherenkov telescope array H.E.S.S. (High Energy Spectroscopic System) to detect TeV scale DM in the Galactic Center region. The work combines next-to-leading-logarithmic order calculations for the annihilation photon spectrum, as well as a comprehensive treatment of detector effects and expected backgrounds. Forecast limits on the sensitivity of H.E.S.S. have been derived across the important TeV mass range, assuming different DM density profiles and focusing on the canonical WIMP dark matter candidate Wino.These limits test our present and future ability to probe the predicted thermal cross section for some of the most promising DM candidates that could be discovered in the coming decade., Comment: 7 pages, 4 figures, 36th International Cosmic Ray Conference
Published: 2019

8. Gamma-ray counterpart of the IceCube neutrinos

Author: M. Kachelrieß, Dmitri Semikoz, Andrii Neronov, 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 de Paris (UP), Observatoire de Paris, 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: History, media_common.quotation_subject, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, halo, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, neutrino: flux, Education, IceCube, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science Applications, dark matter: heavy, Sky, gamma ray, cosmic radiation: galaxy, spectral, High Energy Physics::Experiment, Halo, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract: A γ-ray excess at high Galactic latitudes starting at energies 300 GeV was recently discovered in the data of the Fermi telescope. The multi-TeV γ-ray emission found has spectral characteristics at both low and high Galactic latitudes compatible with those of the IceCube neutrinos in the same sky regions. This suggests that these γ-rays are the counterpart of the IceCube neutrino signal, implying that a sizeable part of the IceCube neutrino flux originates from the Milky Way. The diffuse neutrino and γ-ray signal at high Galactic latitudes may originate either from a nearby cosmic ray "PeVatron" cosmic ray source, an extended Galactic cosmic ray halo or from decays of heavy dark matter particles. Content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
Published: 2019

9. Latest results on dark matter searches with H.E.S.S

Author: Rinchiuso, Lucia, Collaboration, H. E. S. S., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and H.E.S.S.
Subjects: High energy, Milky Way, QC1-999, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, satellite, FOS: Physical sciences, dark matter: signature, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, cross section: annihilation, HESS, 0103 physical sciences, 010306 general physics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, Annihilation, 010308 nuclear & particles physics, dark matter: annihilation, Cherenkov counter, gamma ray: VHE, dark matter: heavy, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The nature of Dark Matter (DM) is one of the most debated questions of contemporary physics. Ground-based arrays of Cherenkov telescopes such as the High Energy Spectroscopic System (H.E.S.S.) search for DM signatures through the detection of Very-High-Energy (VHE, $E > 100$ GeV) gamma-rays. DM particles could self-annihilate in dense environments producing VHE $\gamma$-rays in the final states that could be eventually detected by H.E.S.S.. The H.E.S.S. observation strategy for DM search focuses towards the Galactic Centre (GC) region and nearby dwarf galaxy satellites of the Milky Way. The GC dataset provides the most stringent constraints on the DM annihilation cross section in the mass range 300 GeV - 70 TeV. Searches have been carried out towards classical and ultra-faint dwarf galaxies to test specific heavy DM models. The latest results towards the GC and dwarf galaxies are shown., Comment: 4 pages, 3 figures, conference proceeding
Published: 2018

10. Earth scattering of superheavy dark matter: Updated constraints from detectors old and new

Author: Bradley J. Kavanagh, Laboratoire de Physique Théorique et Hautes Energies (LPTHE), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and IoP (FNWI)
Subjects: Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, FOS: Physical sciences, Parameter space, 7. Clean energy, 01 natural sciences, Gravitation, particle: massive, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, CRESST, nucleus: scattering, surface, inflation, atmosphere: effect, 010306 general physics, capture, Nuclear Experiment, Nuclear scattering, Physics, Annihilation, 010308 nuclear & particles physics, Scattering, shielding, dark matter: mass, Detector, High Energy Physics - Phenomenology, Formalism (philosophy of mathematics), annihilation, dark matter: heavy, gravitation, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], direct detection, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], up: mass, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Direct searches for Dark Matter (DM) are continuously improving, probing down to lower and lower DM-nucleon interaction cross sections. For strongly-interacting massive particle (SIMP) Dark Matter, however, the accessible cross section is bounded from above due to the stopping effect of the atmosphere, Earth and detector shielding. We present a careful calculation of the SIMP signal rate, focusing on super-heavy DM ($m_\chi \gtrsim 10^5 \,\,\mathrm{GeV}$) for which the standard nuclear-stopping formalism is applicable, and provide code for implementing this calculation numerically. With recent results from the low-threshold CRESST 2017 surface run, we improve the maximum cross section reach of direct detection searches by a factor of around 5000, for DM masses up to $10^8 \,\,\mathrm{GeV}$. A reanalysis of the longer-exposure, sub-surface CDMS-I results (published in 2002) improves the previous cross section reach by two orders of magnitude, for masses up to $10^{15} \,\,\mathrm{GeV}$. Along with complementary constraints from SIMP capture and annihilation in the Earth and Sun, these improved limits from direct nuclear scattering searches close a number of windows in the SIMP parameter space in the mass range $10^6$ GeV to $10^{13}$ GeV, of particular interest for heavy DM produced gravitationally at the end of inflation., Comment: 12 pages, 7 figures. Code available at https://github.com/bradkav/verne . Comments welcome. v2: Fixed references and minor typos, corrected "$\nu$-cleus" to "CRESST 2017 surface run". v3: Added Appendix A with explicit expressions and coordinate system. v4: Added discussion of variance in final DM speed. Version published in PRD
Published: 2018

11. Multi-messenger gamma-ray counterpart of the IceCube neutrino signal

Author: Andrii Neronov, M. Kachelrieß, Dmitri Semikoz, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), AstroParticule et Cosmologie (APC (UMR_7164)), 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, 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), 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 de Paris (UP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: gamma ray: background, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, gamma ray: energy spectrum, neutrino: flux, GLAST, IceCube, High Energy Physics - Phenomenology (hep-ph), KASCADE, 0103 physical sciences, supernova, gamma ray: flux, 010303 astronomy & astrophysics, KM3NeT, attenuation, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, ANTARES, 010308 nuclear & particles physics, dark matter: decay, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, suppression, Galaxy, messenger, Supernova, High Energy Physics - Phenomenology, dark matter: heavy, 13. Climate action, cosmic radiation, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics::Experiment, galaxy, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: A signal of high-energy extraterrestrial neutrinos from unknown source(s) was recently discovered by the IceCube experiment. Neutrinos are always produced together with $\ensuremath{\gamma}$-rays, but the $\ensuremath{\gamma}$-ray flux from extragalactic sources is suppressed due to attenuation in the intergalactic medium. We report the discovery of a $\ensuremath{\gamma}$-ray excess at high galactic latitudes starting at energies 300 GeV in the data of the Fermi telescope. We show that the multi-TeV $\ensuremath{\gamma}$-ray diffuse emission has spectral characteristics at both low and high galactic latitudes compatible with those of the IceCube high neutrino signal in the same sky regions. This suggests that these $\ensuremath{\gamma}$-rays are the counterpart of the IceCube neutrino signal, implying that a sizable part of the IceCube neutrino flux originates from the Milky Way. We argue that the diffuse neutrino and $\ensuremath{\gamma}$-ray signal at high galactic latitudes originates either from previously unknown nearby cosmic ray ``PeVatron'' source(s), an extended galactic cosmic ray halo or from decays of heavy dark matter particles.
Published: 2018

12. Gravitino and Polonyi production in supergravity

Author: Maxim Yu. Khlopov, Andrea Addazi, Sergei V. Ketov, 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: High Energy Physics - Theory, Physics and Astronomy (miscellaneous), 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics::Theory, High Energy Physics - Phenomenology (hep-ph), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Supergravity, Supersymmetry, High Energy Physics - Phenomenology, gravitino: production, Higgs boson, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], gauge field theory: U(1), Gravitino, Astrophysics - High Energy Astrophysical Phenomena, inflaton: decay, гравитирующие тела, Particle physics, nucleosynthesis: big bang, FOS: Physical sciences, lcsh:Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, supersymmetry: spontaneous symmetry breaking, supergravity: 1, Supermultiplet, 0103 physical sciences, lcsh:QB460-466, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, 010306 general physics, Engineering (miscellaneous), Inflation (cosmology), полоний, супергравитация, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Inflaton, superfield: chiral, High Energy Physics - Theory (hep-th), dark matter: heavy, Supersymmetric gauge theory, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], lcsh:QC770-798, High Energy Physics::Experiment, Starobinsky model, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We study production of gravitino and Polonyi particles in the minimal Starobinsky-Polonyi $\mathcal{N}=1$ supergravity with inflaton belonging to a massive vector supermultiplet. Our model has only one free parameter given by the scale of spontaneous SUSY breaking triggered by Polonyi chiral superfield. The vector supermultiplet generically enters the action non-minimally, via an arbitrary real function. This functon is chosen to generate the inflaton scalar potential of the Starobinsky model. Our supergravity model can be reformulated as an abelian supersymmetric gauge theory with the vector gauge superfield coupled to two (Higgs and Polonyi) chiral superfields interacting with supergravity, where the $U(1)$ gauge symmetry is spontaneously broken. We find that Polonyi and gravitino particles are efficiently produced during inflation. After inflation, perturbative decay of inflaton also produces Polonyi particles that rapidly decay into gravitinos. As a result, a coherent picture of inflation and dark matter emerges, where the abundance of produced gravitinos after inflation fits the CMB constraints as a Super Heavy Dark Matter (SHDM) candidate. Our scenario avoids the notorous gravitino and Polonyi problems with the Big Bang Nucleosynthesis (BBN) and DM overproduction., Comment: Version published in in Eur.Phys.J. C78 (2018) no.8, 642
Published: 2018

13. Emergence of the mass discrepancy-acceleration relation from dark matter-baryon interactions

Author: Benoit Famaey, Justin Khoury, Riccardo Penco, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg ( ObAS ), Université de Strasbourg ( UNISTRA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], galaxy: model, Dark matter, FOS: Physical sciences, feedback, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: direct detection, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Gravitation, galaxy: formation, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Galaxy cluster, Physics, density, Number density, 010308 nuclear & particles physics, Astronomy and Astrophysics, dark matter: exchange, Astrophysics - Astrophysics of Galaxies, Galaxy, Elastic collision, Baryon, baryon, High Energy Physics - Phenomenology, dark matter: heavy, gravitation, density dependence, Astrophysics of Galaxies (astro-ph.GA), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy: cluster, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], energy: exchange, velocity dependence, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The observed tightness of the mass discrepancy-acceleration relation (MDAR) poses a fine-tuning challenge to current models of galaxy formation. We propose that this relation could arise from collisional interactions between baryons and dark matter (DM) particles, without the need for modification of gravity or ad hoc feedback processes. We assume that these interactions satisfy the following three conditions: (i) the relaxation time of DM particles is comparable to the dynamical time in disk galaxies; (ii) DM exchanges energy with baryons due to elastic collisions; (iii) the product between the baryon-DM cross section and the typical energy exchanged in a collision is inversely proportional to the DM number density. We present an example of a particle physics model that gives a DM-baryon cross section with the desired density and velocity dependence. Direct detection constraints require our DM particles to be either very light ($m << m_b$) or very heavy ($m >> m_b$), corresponding respectively to heating and cooling of DM by baryons. In both cases, our mechanism applies and an equilibrium configuration can in principle be reached. Here, we focus on the heavy DM/cooling case as it is technically simpler. Under these assumptions, we find that rotationally-supported disk galaxies could naturally settle to equilibrium configurations satisfying a MDAR at all radii without invoking finely tuned feedback processes. We also discuss issues related to the small scale clumpiness of baryons, as well as predictions for pressure-supported systems. We argue in particular that galaxy clusters do not follow the MDAR despite being DM-dominated because they have not reached their equilibrium configuration. Finally, we revisit existing phenomenological, astrophysical and cosmological constraints on baryon-DM interactions in light of the unusual density dependence of the cross section., 64 pages, 8 figures, matches the published version
Published: 2018

14. Discovery of a new extragalactic source population of energetic particles

Author: Anthony M. Brown, Thomas Lacroix, P. M. Chadwick, J. A. Graham, Joseph Silk, Céline Bœhm, 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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 ), Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Active galactic nucleus, lepton, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Population, Dark matter, Centaurus A, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, VHE, GLAST, jet: relativistic, dark matter: halo, Millisecond pulsar, 0103 physical sciences, black hole, AGN, education, 010303 astronomy & astrophysics, enhancement, Astrophysics::Galaxy Astrophysics, pulsar, energy: low, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Spectral index, 010308 nuclear & particles physics, galaxy: radio wave, Astronomy, hadronic component, Dark matter halo, gamma ray: emission, dark matter: heavy, cosmic radiation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Lepton
Abstract: We report the discovery of a statistically significant hardening in the Fermi-LAT $\gamma$-ray spectrum of Centaurus A's core, with the spectral index hardening from $\Gamma_{1}=2.73 \pm 0.02$ to $\Gamma_{1}=2.29 \pm 0.07$ at a break energy of ($2.6 \pm 0.3$) GeV. Using a likelihood analysis, we find no evidence for flux variability in Cen A's core lightcurve above or below the spectral break when considering the entire 8 year period. Interestingly, however, the first $\sim3.5$ years of the low energy lightcurve shows evidence of flux variability at the $\sim3.5 \sigma$ confidence level. To understand the origin of this spectral break, we assume that the low energy component below the break feature originates from leptons in Centaurus A's radio jet and we investigate the possibility that the high energy component above the spectral break is due to an additional source of very high energy particles near the core of Cen A. We show for the first time that the observed $\gamma$-ray spectrum of an Active Galactic Nucleus is compatible with either a very large localized enhancement (referred to as a spike) in the dark matter halo profile or a population of millisecond pulsars. Our work constitutes the first robust indication that new $\gamma$-ray production mechanisms can explain the emission from active galaxies and could provide tantalizing first evidence for the clustering of heavy dark matter particles around black holes., Comment: 8 pages, 10 figures. Final version selected as an editor's suggestion and published in Phys. Rev. D. Updated version includes an additional reference that was missing from the final published version
Published: 2016

15. Connecting the new H.E.S.S. diffuse emission at the Galactic center with the Fermi GeV excess: a combination of millisecond pulsars and heavy dark matter?

Author: Joseph Silk, Thomas Lacroix, Emmanuel Moulin, Celine Boehm, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Département de Physique des Particules (ex SPP) (DPP), 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-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / 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 Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Université Montpellier 2 - Sciences et Techniques ( UM2 ), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Département de Physique des Particules (ex SPP) ( DPP ), 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-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 Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: electron, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, magnetic field, Astrophysics, Electron, dark matter: density, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, thermal, High Energy Physics - Phenomenology (hep-ph), Pulsar, Millisecond pulsar, HESS, muon, 0103 physical sciences, emission, black hole, Diffusion (business), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, pulsar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Muon, cross section, 010308 nuclear & particles physics, Galactic Center, diffusion, Astrophysics - Astrophysics of Galaxies, Magnetic field, High Energy Physics - Phenomenology, dark matter: heavy, 13. Climate action, gamma ray, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Astrophysics of Galaxies (astro-ph.GA), spectral, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The H.E.S.S. collaboration has reported a high-energy spherically symmetric diffuse gamma-ray emission in the inner 50 pc of the Milky Way, up to ~ 50 TeV. Here we propose a leptonic model which provides an alternative to the hadronic scenario presented by the H.E.S.S. collaboration, and connects the newly reported TeV emission to the Fermi-LAT Galactic center GeV excess. Our model relies on a combination of inverse Compton emission from a population of millisecond pulsars---which can account for the GeV excess---and a supermassive black hole-induced spike of heavy (~ 60 TeV) dark matter particles annihilating into electrons with a sub-thermal cross-section. With an up-to-date interstellar radiation field, as well as a standard magnetic field and diffusion set-up, our model accounts for the spectral morphology of the detected emission. Moreover, we show that the dark matter induced emission reproduces the spatial morphology of the H.E.S.S. signal above ~ 10 TeV, while we obtain a slightly more extended component from pulsars at lower energies, which could be used as a prediction for future H.E.S.S. observations., Comment: 7 pages, 3 figures; matches version published in Phys. Rev. D
Published: 2016
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16. A Search for Neutrinos from Decaying Dark Matter in Galaxy Clusters and Galaxies with IceCube

Author: IceCube Collaboration, Abbasi, Rasha, An, Rui, Fischer, Leander, Fox, Derek B., Franckowiak, Anna, Friedman, Elizabeth, Fritz, Alexander, Fürst, Philipp, Gaisser, T. K., Gallagher, Jay, Ganster, Erik, Garcia, Alfonso, Andeen, Karen, Garrappa, Simone, Gerhardt, L., Ghadimi, Ava, Glaser, Christian, Glauch, Theo, Glusenkamp, Thorsten, Goldschmidt, A., Gonzalez, Javier, Goswami, Sreetama, Grant, Darren, Anderson, Tyler, Grégoire, Timothée, Griswold, Spencer, Gunduz, Mehmet, Günther, Christoph, Haack, Christian, Hallgren, Allan, Halliday, R., Halve, Lasse Yannik, Halzen, F., Ha Minh, Martin, Anton, Gisela, Hanson, Kael, Hardin, John, Harnisch, Alexander A., Haungs, Andreas, Hauser, Simon, Hebecker, Dustin, Helbing, K., Henningsen, Felix, Hettinger, Emma C., Hickford, Stephanie, Arguelles, Carlos, Hignight, Joshua, Hill, Colton, Hill, G. C., Hoffman, Kara, Hoffmann, Ruth, Hoinka, Tobias, Hokanson-Fasig, Benjamin, Hoshina, K., Huang, Feifei, Huber, Matthias, Ashida, Yosuke, Huber, Thomas, Hultqvist, Klas, Hunnefeld, Mirco, Hussain, Raamis, In, Seongjin, Iovine, Nadège, Ishihara, Aya, Jansson, Matti, Japaridze, George, Jeong, Minjin, Axani, Spencer, Jones, Ben, Kang, Donghwa, Kang, Woosik, Kang, Xinyue, Kappes, Alexander, Kappesser, David, Karg, Timo, Karl, Martina, Karle, A., Katz, U., Bai, Xinhua, Kauer, M., Kellermann, Moritz, Kelley, J. L., Kheirandish, Ali, Kin, Ken'ichi, Kintscher, Thomas, Kiryluk, Joanna, Klein, Spencer, Koirala, Ramesh, Kolanoski, Hermann, Balagopal V., Aswathi, Kontrimas, Tomas, Kopke, Lutz, Kopper, Claudio, Kopper, Sandro, Koskinen, D. J., Koundal, Paras, Kovacevich, Michael, Kowalski, Marek, Kozynets, Tetiana, Kun, Emma, Barbano, Anastasia Maria, Kurahashi, Naoko, Lad, Neha, Lagunas Gualda, Cristina, Lanfranchi, Justin, Larson, M. J., Lauber, Frederik Hermann, Lazar, Jeffrey, Lee, Jiwoong, Leonard, Kayla, Leszczyńska, Agnieszka, Ackermann, Markus, Barwick, S. W., Li, Yijia, Lincetto, Massimiliano, Liu, Qinrui, Liubarska, Maria, Lohfink, Elisa, Lozano Mariscal, Cristian Jesus, Lu, Lu, Lucarelli, Francesco, Ludwig, Andrew, Luszczak, William, Bastian, Benjamin, Lyu, Yang, Ma, Wing Yan, Madsen, James, Mahn, Kendall, Makino, Yuya, Mancina, Sarah, Maris, Ioana Codrina, Maruyama, Reina H., Mase, K., McElroy, Thomas, Basu, Vedant, McNally, Frank, Mead, James Vincent, Meagher, K., Medina, Andres, Meier, Maximilian, Meighen-Berger, Stephan, Micallef, Jessie, Mockler, Daniela, Montaruli, Teresa, Moore, Roger, Baur, Sebastian, Morse, R., Moulai, Marjon, Naab, Richard, Nagai, Ryo, Naumann, Uwe, Necker, Jannis, Nguyen, Le Viet, Niederhausen, Hans, Nisa, Mehr, Nowicki, Sarah, Bay, R. C., Nygren, Dave, Obertacke Pollmann, Anna, Oehler, Marie, Olivas, A., O'Sullivan, Erin, Pandya, Hershal, Pankova, Daria, Park, Nahee, Parker, Grant, Paudel, Ek Narayan, Beatty, J. J., Paul, Larissa, Perez de los Heros, Carlos, Peters, Lilly, Peterson, Josh, Philippen, Saskia, Pieloth, Damian, Pieper, Sarah, Pittermann, Martin, Pizzuto, A., Plum, M., Becker, K. H., Popovych, Yuiry, Porcelli, Alessio, Prado Rodriguez, Maria, Price, P. Buford, Pries, Brandom, Przybylski, Gerald, Raab, Christoph, Raissi, Amirreza, Rameez, Mohamed, Rawlins, K., Becker Tjus, Julia, Rea, Immacolata Carmen, Rehman, Abdul, Reichherzer, Patrick, Reimann, René, Renzi, Giovanni, Resconi, Elisa, Reusch, Simeon, Rhode, Wolfgang, Richman, Mike, Riedel, Benedikt, Bellenghi, Chiara, Roberts, Ella, Robertson, Sally, Roellinghoff, Gerrit, Rongen, Martin, Rott, Carsten, Ruhe, Tim, Ryckbosch, Dirk, Rysewyk Cantu, Devyn, Safa, Ibrahim, Saffer, Julian, BenZvi, Segev, Sanchez Herrera, Sebastian, Sandrock, Alexander, Sandroos, Joakim, Santander, Marcos, Sarkar, Subir, Sarkar, Sourav, Satalecka, Konstancja, Scharf, Maximilian Karl, Schaufel, Merlin, Schieler, Harald, Adams, Jenni, Berley, D., Schindler, Sebastian, Schlunder, P., Schmidt, Torsten, Schneider, Austin, Schneider, Judith, Schröder, Frank G., Schumacher, Lisa Johanna, Schwefer, Georg, Sclafani, Steve, Seckel, D., Bernardini, Elisa, Seunarine, Surujhdeo, Sharma, Ankur, Shefali, Shefali, Silva, Manuel, Skrzypek, Barbara, Smithers, Ben, Snihur, Robert, Soedingrekso, Jan, Soldin, Dennis, Spannfellner, Christian, Besson, D. Z., Spiczak, Glenn, Spiering, Christian, Stachurska, Juliana, Stamatikos, Michael, Stanev, T., Stein, Robert, Stettner, Jöran Benjamin, Steuer, A., Stezelberger, T., Sturwald, Timo, Binder, Gary, Stuttard, Thomas, Sullivan, G. W., Taboada, I., Tenholt, Frederik, Ter-Antonyan, Samvel, Tilav, S., Tischbein, Franziska, Tollefson, Kirsten, Tomankova, Lenka, Tönnis, Christoph, Bindig, Daniel, Toscano, Simona, Tosi, Delia, Trettin, Alexander, Tselengidou, Maria, Tung, Chunfai, Turcati, Andrea, Turcotte, Roxanne, Turley, Colin, Twagirayezu, Jean Pierre, Ty, Bunheng, Blaufuss, E., Unland Elorrieta, Martin, Valtonen-Mattila, Nora, Vandenbroucke, Justin, van Eijndhoven, Nick, Vannerom, David, van Santen, Jakob, Verpoest, Stef, Vraeghe, Matthias, Walck, C., Watson, Timothyblake, Blot, Summer, Weaver, Chris, Weigel, Philip, Weindl, Andreas, Weiss, Matthew, Weldert, Jan, Wendt, Chris, Werthebach, Johannes, Weyrauch, Mark, Whitehorn, Nathan, Wiebusch, Christopher, Boddenberg, Matthias, Williams, Dawn, Wolf, Martin, Woschnagg, Kurt, Wrede, Gerrit, Wulff, Johan, Xu, Xianwu, Xu, Yiqian, Yanez, Juan Pablo, Yoshida, S., Yu, Shiqi, Bontempo, Federico, Yuan, Tianlu, Zhang, Zelong, Borowka, Jürgen, Aguilar, Juanan, Boser, S., Botner, Olga, Böttcher, Jakob, Bourbeau, Etienne, Bradascio, Federica, Braun, J., Bron, Stephanie, Brostean-Kaiser, Jannes, Browne, Sally-Ann, Burgman, Alexander, Ahlers, M., Burley, Ryan, Busse, Raffaela, Campana, Michael, Carnie-Bronca, Erin, Chen, Chujie, Chirkin, Dmitry, Choi, Koun, Clark, Brian, Clark, Kenneth, Classen, Lew, Ahrens, Maryon, Coleman, Alan, Collin, Gabriel, Conrad, J. M., Coppin, Paul, Correa, Pablo, Cowen, D. F., Cross, R., Dappen, Christian, Dave, Pranav, DE CLERCQ, Catherine, Alispach, Cyril Martin, DeLaunay, James, Dembinski, Hans, Deoskar, Kunal, De Ridder, Sam, Desai, Abhishek, Desiati, Paolo, de Vries, Krijn, de Wasseige, Gwenhaël, De With, Meike, DeYoung, Tyce, Alves Junior, Antonio Augusto, Dharani, Sukeerthi, Diaz, Alejandro, Diaz-Velez, Juan Carlos, Dittmer, Markus, Dujmovic, Hrvoje, Dunkman, Matt, DuVernois, Michael, Dvorak, Emily, Ehrhardt, Thomas, Eller, Philipp, Amin, Najia Moureen Binte, Engel, Ralph, Erpenbeck, Hannah, Evans, John, Evenson, P. A., Fan, Kwok Lung, Fazely, A. R., Fiedlschuster, Sebastian, Fienberg, Aaron, Filimonov, Kirill, and Finley, Chad
Subjects: decay [dark matter], Dark matter, pole, Astrophysics, mass [dark matter], heavy [dark matter], IceCube, cluster [galaxy], TeV, ddc:530, detector [neutrino], Galaxy cluster, Physics, lifetime, dark matter: mass, dark matter: decay, sensitivity, Galaxy, observatory, neutrino: detector, dark matter: heavy, galaxy: cluster, Neutrino
Abstract: 37th International Cosmic Ray Conference, ICRC 2021, Berlin, Germany, 15 Jul 2021 - 22 Jul 2021; Proceedings of Science 395, 506 (2022). doi:10.22323/1.395.0506 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

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16 results on '"dark matter: heavy"'

1. The B anomalies, the U 1 leptoquark and dark matter

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

3. Phenomenology of the Dark Matter sector in the Two Higgs Doublet Model with Complex Scalar Singlet extension

4. First implications of Tibet AS$_\gamma$ data for heavy dark matter

5. Heavy dark matter through the dilaton portal

6. Equilibrium axisymmetric halo model for the Milky Way and its implications for direct and indirect dark matter searches

7. Hunting for heavy Dark Matter in the Galactic Center with ground-based Cherenkov telescopes

8. Gamma-ray counterpart of the IceCube neutrinos

9. Latest results on dark matter searches with H.E.S.S

10. Earth scattering of superheavy dark matter: Updated constraints from detectors old and new

11. Multi-messenger gamma-ray counterpart of the IceCube neutrino signal

12. Gravitino and Polonyi production in supergravity

13. Emergence of the mass discrepancy-acceleration relation from dark matter-baryon interactions

14. Discovery of a new extragalactic source population of energetic particles

15. Connecting the new H.E.S.S. diffuse emission at the Galactic center with the Fermi GeV excess: a combination of millisecond pulsars and heavy dark matter?

16. A Search for Neutrinos from Decaying Dark Matter in Galaxy Clusters and Galaxies with IceCube

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16 results on '"dark matter: heavy"'

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