The Curse of the Pharaohs is an expansion pack for the Ubisoft game Assassin's Creed Origins. It was released on March 13, 2018, and continues the story of the main game. The expansion takes place four years after the events of Origins and introduces a new storyline involving the revival of ancient Egyptian pharaohs. In this expansion, the protagonist Bayek arrives in a new region called Thebes, which is suffering from a plague of undead pharaohs. These pharaohs, known as the "Pharaoh's Shadows," have been brought back to life by a curse and wreak havoc upon the land. Bayek, along with his new ally and historian, Tahira, must uncover the origin of this curse and find a way to put an end to it.
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The move will increase broadcast signal coverage from 25,000 to 100,000 watts and 250,000 to 500,000 adults 35 from the South Carolina Georgia border to Asheville, NC, while covering parts of four South Carolina congressional districts and several North Carolina congressional districts. The move will increase broadcast signal coverage from 25,000 to 100,000 watts and 250,000 to 500,000 adults 35 from the South Carolina Georgia border to Asheville, NC, while covering parts of four South Carolina congressional districts and several North Carolina congressional districts.
Bayek, along with his new ally and historian, Tahira, must uncover the origin of this curse and find a way to put an end to it. The Curse of the Pharaohs brings a unique twist to the Assassin's Creed Origins gameplay by introducing a supernatural element. Players must navigate through haunted tombs, solve ancient puzzles, and battle formidable enemies, including mythical creatures like giant scorpions and Anubis warriors.
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MAGIC Collaboration
H. Abe 1 , S. Abe 1 , V. A. Acciari 2 , I. Agudo 3 , T. Aniello 4 , S. Ansoldi 5 ,45 , L. A. Antonelli 4 , A. Arbet Engels 6 , C. Arcaro 7 , M. Artero 8 , K. Asano 1 , D. Baack 9 , A. Babić 10 , A. Baquero 11 , U. Barres de Almeida 12 , J. A. Barrio 11 , I. Batković 7 , J. Baxter 1 , J. Becerra González 2 , W. Bednarek 13 , E. Bernardini 7 , M. Bernardos 3 , A. Berti 6 , J. Besenrieder 6 , W. Bhattacharyya 14 , C. Bigongiari 4 , A. Biland 15 , O. Blanch 8 , G. Bonnoli 4 , Ž. Bošnjak 10 , I. Burelli 5 , G. Busetto 7 , R. Carosi 16 , M. Carretero-Castrillo 17 , A. J. Castro-Tirado 3 , G. Ceribella 1 , Y. Chai 6 , A. Chilingarian 18 , S. Cikota 10 , E. Colombo 2 , J. L. Contreras 11 , J. Cortina 19 , S. Covino 4 , G. D'Amico 20 , V. D'Elia 4 , P. Da Vela 4 ,16 , F. Dazzi 4 , A. De Angelis 7 , B. De Lotto 5 , A. Del Popolo 21 , M. Delfino 8 ,47 , J. Delgado 8 ,47 , C. Delgado Mendez 19 , D. Depaoli 22 , F. Di Pierro 22 , L. Di Venere 23 , E. Do Souto Espiñeira 8 , D. Dominis Prester 24 , A. Donini 4 , D. Dorner 25 , M. Doro 7 , D. Elsaesser 9 , G. Emery 26 , J. Escudero 3 , V. Fallah Ramazani 27 ,48 , L. Fariña 8 , A. Fattorini 9 , L. Font 28 , C. Fruck 6 , S. Fukami 15 , Y. Fukazawa 29 , R. J. García López 2 , M. Garczarczyk 14 , S. Gasparyan 30 , M. Gaug 28 , J. G. Giesbrecht Paiva 12 , N. Giglietto 23 , F. Giordano 23 , P. Gliwny 13 , N. Godinović 31 , R. Grau 8 , D. Green 6 , J. G. Green 6 , D. Hadasch 1 , A. Hahn 6 , T. Hassan 19 , L. Heckmann 6 ,46 , J. Herrera 2 , D. Hrupec 32 , M. Hütten 1 , R. Imazawa 29 , T. Inada 1 , R. Iotov 25 , K. Ishio 13 , I. Jiménez Martínez 19 , J. Jormanainen 27 , D. Kerszberg 8 , Y. Kobayashi 1 , H. Kubo 1 , J. Kushida 33 , A. Lamastra 4 , D. Lelas 31 , F. Leone 4 , E. Lindfors 27 , L. Linhoff 9 , S. Lombardi 4 , F. Longo 5 ,50 , R. López-Coto 7 , M. López-Moya 11 , A. López-Oramas 2 , S. Loporchio 23 , A. Lorini 34 , E. Lyard 26 , B. Machado de Oliveira Fraga 12 , P. Majumdar 35 ,50 , M. Makariev 36 , G. Maneva 36 , N. Mang 9 , M. Manganaro 24 , S. Mangano 19 , K. Mannheim 25 , M. Mariotti 7 , M. Martínez 8 , A. Mas Aguilar 11 , D. Mazin 1 ,6 , S. Menchiari 34 , S. Mender 9 , S. Mićanović 24 , D. Miceli 7 , T. Miener 11 , J. M. Miranda 34 , R. Mirzoyan 6 , E. Molina 17 , H. A. Mondal 35 , A. Moralejo 8 , D. Morcuende 11 , V. Moreno 28 , T. Nakamori 37 , C. Nanci 4 , L. Nava 4 , V. Neustroev 38 , M. Nievas Rosillo 2 , C. Nigro 8 , K. Nilsson 27 , K. Nishijima 33 , T. Njoh Ekoume 2 , K. Noda 1 , S. Nozaki 6 , Y. Ohtani 1 , T. Oka 39 ,★ , A. Okumura 40 , J. Otero-Santos 2 , S. Paiano 4 , M. Palatiello 5 , D. Paneque 6 , R. Paoletti 34 , J. M. Paredes 17 , L. Pavletić 24 , M. Persic 5 , M. Pihet 6 , G. Pirola 6 , F. Podobnik 34 , P. G. Prada Moroni 16 , E. Prandini 7 , G. Principe 5 , C. Priyadarshi 8 , W. Rhode 9 , M. Ribó 17 , J. Rico 8 , C. Righi 4 , A. Rugliancich 16 , N. Sahakyan 30 , T. Saito 1 ,★ , S. Sakurai 1 , K. Satalecka 27 , F. G. Saturni 4 , B. Schleicher 25 , K. Schmidt 9 , F. Schmuckermaier 6 , J. L. Schubert 9 , T. Schweizer 6 , J. Sitarek 13 , V. Sliusar 26 , D. Sobczynska 13 , A. Spolon 7 , A. Stamerra 4 , J. Strišković 32 , D. Strom 6 , M. Strzys 1 ,★ , Y. Suda 29 , T. Surić 41 , H. Tajima 40 , M. Takahashi 40 , R. Takeishi 1 , F. Tavecchio 4 , P. Temnikov 36 , K. Terauchi 39 , T. Terzić 24 , M. Teshima 1 ,6 , L. Tosti 42 , S. Truzzi 34 , A. Tutone 4 , S. Ubach 28 , J. van Scherpenberg 6 , M. Vazquez Acosta 2 , S. Ventura 34 , V. Verguilov 36 , I. Viale 7 , C. F. Vigorito 22 , V. Vitale 43 , I. Vovk 1 , R. Walter 26 , M. Will 6 , C. Wunderlich 34 , T. Yamamoto 44 and D. Zarić 31
1 Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
2 Instituto de Astrofisica de Canarias and Dpto. de Astrofisica, Universidad de La Laguna, 38200 La Laguna, Tenerife, Spain
3 Instituto de Astrofisica de Andalucia-CSIC, Glorieta de la Astronomia s/n, 18008 Granada, Spain
4 National Institute for Astrophysics (INAF), 00136 Rome, Italy
5 Università di Udine and INFN Trieste, 33100 Udine, Italy
6 Max-Planck-Institut für Physik, 80805 München, Germany
7 Università di Padova and INFN, 35131 Padova, Italy
8 Institut de Fisica d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), 08193 Bellaterra (Barcelona), Spain
9 Technische Universität Dortmund, 44221 Dortmund, Germany
10 Croatian MAGIC Group: University of Zagreb, Faculty of Electrical Engineering and Computing (FER), 10000 Zagreb, Croatia
11 IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, 28040 Madrid, Spain
12 Centro Brasileiro de Pesquisas Físicas (CBPF), 22290-180 URCA, Rio de Janeiro (RJ), Brazil
13 University of Lodz, Faculty of Physics and Applied Informatics, Department of Astrophysics, 90-236 Lodz, Poland
14 Deutsches Elektronen-Synchrotron (DESY), 15738 Zeuthen, Germany
15 ETH Zürich, 8093 Zürich, Switzerland
16 Università di Pisa and INFN Pisa, 56126 Pisa, Italy
17 Universitat de Barcelona, ICCUB, IEEC-UB, 08028 Barcelona, Spain
18 Armenian MAGIC Group: A. Alikhanyan National Science Laboratory, 0036 Yerevan, Armenia
19 Centro de Investigaciones Energéticas, Medioambientales y Tecnologicas, 28040 Madrid, Spain
20 Department for Physics and Technology, University of Bergen, 5007 Bergen, Norway
21 INFN MAGIC Group: INFN Sezione di Catania and Dipartimento di Fisica e Astronomia, University of Catania, 95123 Catania, Italy
22 INFN MAGIC Group: INFN Sezione di Torino and Università degli Studi di Torino, 10125 Torino, Italy
23 INFN MAGIC Group: INFN Sezione di Bari and Dipartimento Interateneo di Fisica dell'Università e del Politecnico di Bari, 70125 Bari, Italy
24 Croatian MAGIC Group: University of Rijeka, Faculty of Physics, 51000 Rijeka, Croatia
25 Universität Würzburg, 97074 Würzburg, Germany
26 University of Geneva, Chemin d'Ecogia 16, 1290 Versoix, Switzerland
27 Finnish MAGIC Group: Finnish Centre for Astronomy with ESO, University of Turku, 20014 Turku, Finland
28 Departament de Fisica, and CERES-IEEC, Universitat Autönoma de Barcelona, 08193 Bellaterra, Spain
29 Japanese MAGIC Group: Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 739-8526 Hiroshima, Japan
30 Armenian MAGIC Group: ICRANet-Armenia, 0019 Yerevan, Armenia
31 Croatian MAGIC Group: University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture (FESB), 21000 Split, Croatia
32 Croatian MAGIC Group: Josip Juraj Strossmayer University of Osijek, Department of Physics, 31000 Osijek, Croatia
33 Japanese MAGIC Group: Department of Physics, Tokai University, Hiratsuka, 259-1292 Kanagawa, Japan
34 Università di Siena and INFN Pisa, 53100 Siena, Italy
35 Saha Institute of Nuclear Physics, A CI of Homi Bhabha National Institute, Kolkata 700064, West Bengal, India
36 Inst. for Nucl. Research and Nucl. Energy, Bulgarian Academy of Sciences, 1784 Sofia, Bulgaria
37 Japanese MAGIC Group: Department of Physics, Yamagata University, Yamagata 990-8560, Japan
38 Finnish MAGIC Group: Space Physics and Astronomy Research Unit, University of Oulu, 90014 Oulu, Finland
39 Japanese MAGIC Group: Department of Physics, Kyoto University, 606-8502 Kyoto, Japan
40 Japanese MAGIC Group: Institute for Space-Earth Environmental Research and Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, 464-6801 Nagoya, Japan
41 Croatian MAGIC Group: Ruđer Bošković Institute, 10000 Zagreb, Croatia
42 INFN MAGIC Group: INFN Sezione di Perugia, 06123 Perugia, Italy
43 INFN MAGIC Group: INFN Roma Tor Vergata, 00133 Roma, Italy
44 Japanese MAGIC Group: Department of Physics, Konan University, Kobe, Hyogo 658-8501, Japan
45 International Center for Relativistic Astrophysics (ICRA), Rome, Italy
46 Port d'Informacio Cientifica (PIC), 08193 Bellaterra (Barcelona), Spain
47 Ruhr-Universität Bochum, Fakultät für Physik und Astronomie, Astronomisches Institut (AIRUB), 44801 Bochum, Germany
48 University of Innsbruck, Institute for Astro- and Particle Physics, University of Innsbruck, A-6020 Innsbruck, Austria
49 Dipartimento di Fisica, Università di Trieste, 34127 Trieste, Italy
50 University of Lodz, Faculty of Physics and Applied Informatics, Department of Astrophysics, 90-236 Lodz, Poland
Received: 9 September 2022
Accepted: 11 November 2022
Context. Certain types of supernova remnants (SNRs) in our Galaxy are assumed to be PeVatrons, capable of accelerating cosmic rays (CRs) to ~ PeV energies. However, conclusive observational evidence for this has not yet been found. The SNR G106.3+2.7, detected at 1–100 TeV energies by different γ-ray facilities, is one of the most promising PeVatron candidates. This SNR has a cometary shape, which can be divided into a head and a tail region with different physical conditions. However, in which region the 100 TeV emission is produced has not yet been identified because of the limited position accuracy and/or angular resolution of existing observational data. Additionally, it remains unclear as to whether the origin of the γ-ray emission is leptonic or hadronic.
Aims. With the better angular resolution provided by new MAGIC data compared to earlier γ-ray datasets, we aim to reveal the acceleration site of PeV particles and the emission mechanism by resolving the SNR G106.3+2.7 with 0.1° resolution at TeV energies.
Methods. We observed the SNR G106.3+2.7 using the MAGIC telescopes for 121.7 h in total – after quality cuts – between May 2017 and August 2019. The analysis energy threshold is ~0.2 TeV, and the angular resolution is 0.07−0.1°. We examined the γ-ray spectra of different parts of the emission, whilst benefitting from the unprecedented statistics and angular resolution at these energies provided by our new data. We also used measurements at other wavelengths such as radio, X-rays, GeV γ-rays, and 10 TeV γ-rays to model the emission mechanism precisely.
Results. We detect extended γ-ray emission spatially coincident with the radio continuum emission at the head and tail of SNR G106.3+2.7. The fact that we detect a significant γ-ray emission with energies above 6.0 TeV from only the tail region suggests that the emissions above 10 TeV detected with air shower experiments (Milagro, HAWC, Tibet ASγ and LHAASO) are emitted only from the SNR tail. Under this assumption, the multi-wavelength spectrum of the head region can be explained with either hadronic or leptonic models, while the leptonic model for the tail region is in contradiction with the emission above 10 TeV and X-rays. In contrast, the hadronic model could reproduce the observed spectrum at the tail by assuming a proton spectrum with a cutoff energy of ~1 PeV for that region. Such high-energy emission in this middle-aged SNR (4−10 kyr) can be explained by considering a scenario where protons escaping from the SNR in the past interact with surrounding dense gases at present.
Conclusions. The γ-ray emission region detected with the MAGIC telescopes in the SNR G106.3+2.7 is extended and spatially coincident with the radio continuum morphology. The multi-wavelength spectrum of the emission from the tail region suggests proton acceleration up to ~PeV, while the emission mechanism of the head region could either be hadronic or leptonic.
Key words: acceleration of particles / cosmic rays / gamma rays: general / gamma rays: ISM / ISM: clouds / ISM: supernova remnants
Corresponding authors: T. Oka, T. Saito, M. Strzys; e-mail: [email protected]
The expansion also introduces new weapons, outfits, and abilities for Bayek, allowing players to further customize their gameplay experience. The storyline of the expansion delves deep into ancient Egyptian mythology, with references to famous pharaohs such as Ramses the Great and Tutankhamun. Players will explore famous landmarks like the Valley of the Kings and the city of Thebes, all meticulously recreated in stunning detail. The Curse of the Pharaohs is praised for its rich and immersive gameplay experience. It offers players a substantial amount of content, with new quests, side missions, and activities to engage in. The expansion also expands on the leveling system of the main game, allowing players to reach a maximum level of 55. Overall, the Curse of the Pharaohs expansion pack brings a fresh and exciting addition to Assassin's Creed Origins. It offers a captivating storyline, challenging gameplay, and an opportunity to explore the mystical side of ancient Egypt. Whether you are a fan of the main game or simply intrigued by Egyptian mythology, this expansion is definitely worth a try..
Reviews for "AC Origins: Curse of the Pharaohs - A Love Letter to Egyptian Culture"
1. John - 2 stars - I was really excited for the Curse of the Pharaohs DLC for Assassin's Creed Origins, but I ended up being extremely disappointed. The new region of Thebes looked great, but the storyline was lacking and felt disjointed. The quests felt repetitive, and I quickly lost interest in the expansion. Additionally, the gameplay mechanics felt buggy and unpolished. Overall, I don't think the Curse of the Pharaohs DLC added much value to the base game and I wouldn't recommend it.
2. Sarah - 1 star - I love the Assassin's Creed series, but Curse of the Pharaohs was a major letdown for me. The DLC was extremely glitchy, with frequent crashes and gameplay issues. The new enemies in the expansion were frustratingly difficult, and I often found myself dying repeatedly. The main storyline felt rushed and poorly executed, leaving me feeling unsatisfied with the overall experience. I was really hoping for a great addition to the game, but Curse of the Pharaohs fell flat for me.
3. Mike - 2 stars - I've been a fan of Assassin's Creed Origins, but I was disappointed by Curse of the Pharaohs. The DLC was visually stunning, with beautiful Egyptian landscapes and detailed designs. However, the gameplay felt repetitive, and the quests lacked depth and variety. The addition of mythical creatures was interesting, but they often felt out of place in the historical setting of the game. I was hoping for a more engaging storyline and more meaningful interactions, but unfortunately, Curse of the Pharaohs didn't deliver on those fronts.