Miguel Mostafa

Penn State University

H-index: 99

North America-United States

About Miguel Mostafa

Miguel Mostafa, With an exceptional h-index of 99 and a recent h-index of 57 (since 2020), a distinguished researcher at Penn State University, specializes in the field of experimental particle astrophysics.

His recent articles reflect a diverse array of research interests and contributions to the field:

Exploring the Coronal Magnetic Field with Galactic Cosmic Rays: The Sun Shadow Observed by HAWC

The Giant Radio Array for Neutrino Detection experiment

Search for decaying dark matter in the Virgo cluster of galaxies with HAWC

Detailed Analysis of the TeV γ-Ray Sources 3HWC J1928+ 178, 3HWC J1930+ 188, and the New Source HAWC J1932+ 192

Search for Gamma-Ray and Neutrino Coincidences Using HAWC and ANTARES Data

Discovery of gamma rays from the quiescent Sun with HAWC

Expected performance of the AugerPrime Radio Detector

The high-altitude water cherenkov (HAWC) observatory in méxico: The primary detector

Miguel Mostafa Information

University	Penn State University
Position	Professor of Physics
Citations(all)	37282
Citations(since 2020)	15051
Cited By	26824
hIndex(all)	99
hIndex(since 2020)	57
i10Index(all)	277
i10Index(since 2020)	185
Email	Access Email
University Profile Page	Penn State University

Miguel Mostafa Skills & Research Interests

experimental particle astrophysics

Lorentz invariance violation (LIV) is often described by dispersion relations of the form E2 i= m2 i+ p2 i+ δi, nE2+n with delta different based on particle type i, with energy E, momentum p and rest mass m. Kinematics and energy thresholds of interactions are modified once the LIV terms become comparable to the squared masses of the particles involved. Thus, the strongest constraints on the LIV coefficients δi, n tend to come from the highest energies. At sufficiently high energies, photons produced by cosmic ray interactions as they propagate through the Universe could be subluminal and unattenuated over cosmological distances. Cosmic ray interactions can also be modified and lead to detectable fingerprints in the energy spectrum and mass composition observed on Earth. The data collected at the Pierre Auger Observatory are therefore possibly sensitive to both the electromagnetic and hadronic sectors of LIV …

A tau scenario application to a search for upward-going showers with the Fluorescence Detector of the Pierre Auger Observatory

Authors

Ioana Alexandra Caracas,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

The ANITA collaboration reported the observation of two up-going cosmic ray-like events that were observed in the first and third ANITA flights. The two events were reconstructed with moderately high elevation angles of 27.4◦±0.3◦ and 35.0◦±0.3◦, and their energies were initially reported to be 0.6±0.4 EeV and 0.56+ 0.3

Operations of the Pierre Auger Observatory

Authors

Rossella Caruso,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

The construction of the first stage of the Pierre Auger Observatory, designed for research of ultra-high energy cosmic rays, began in 2001 with a prototype system. The Observatory has been collecting data since early 2004 and was completed in 2008. The Observatory is situated at 1400 m above sea level near Malargüe,(Mendoza province) in western Argentina, covering a vast plain of 3000 km2, known as the Pampa Amarilla. The Observatory consists of a hybrid detector, in which there are 1660 water-Cherenkov stations, forming the Surface Detector (SD) and 27 peripheral atmospheric fluorescence telescopes, comprising the Fluorescence Detector (FD). Over time, the Auger Observatory has been enhanced with different R&D prototypes and is recently being to an important upgrade called AugerPrime. In the present contribution, the general operations of the SD and FD will be described. In particular the FD shift procedure-executable locally in Malargüe or remotely by teams in control rooms abroad within the Collaboration-and the newly SD shifts (operating since 2019) will be explained. Additionally, the SD and FD maintenance campaigns, as well as the data taking and data handling at a basic level, will be reported.37 th International Cosmic Ray Conference (ICRC 2021) July 12th–23rd, 2021

Event-by-event reconstruction of the shower maximum Xmax with the Surface Detector of the Pierre Auger Observatory using deep learning

Authors

Jonas Glombitza,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

Authors

AU Abeysekara,A Albert,R Alfaro,C Alvarez,JdD Álvarez Romero,JC Arteaga Velazquez,AB Kollamparambil,DO Rojas,HA Solares,R Babu,V Baghmanyan,AS Barber,J Becerra Gonzalez,E Belmont-Moreno,S BenZvi,D Berley,C Brisbois,KS Mora,T Capistrán,A Carramiñana,S Casanova,O Chaparro-Amaro,U Cotti,J Cotzomi,S Coutiño de León,E de la Fuente,CL de León,L Diaz,R Diaz Hernandez,JC Vélez,B Dingus,M Durocher,M DuVernois,R Ellsworth,K Engel,MC Hernández,J Fan,K Fang,M Fernandez Alonso,B Fick,H Fleischhack,JL Flores,NI Fraija,D Garcia Aguilar,JA Garcia-Gonzalez,JL García-Luna,G García-Torales,F Garfias,G Giacinti,H Goksu,MM González,JA Goodman,JP Harding,S Hernández Cadena,I Herzog,J Hinton,B Hona,D Huang,F Hueyotl-Zahuantitla,M Hui,B Humensky,P Hüntemeyer,A Iriarte,A Jardin-Blicq,H Jhee,V Joshi,D Kieda,GJ Kunde,S Kunwar,A Lara,J Lee,WH Lee,D Lennarz,H Leon Vargas,J Linnemann,AL Longinotti,R Lopez-Coto,G Luis-Raya,J Lundeen,K Malone,V Marandon,O Martinez,I Martinez Castellanos,H Martínez Huerta,J Martínez-Castro,J Matthews,J McEnery,P Miranda-Romagnoli,JA Soto,E Moreno Barbosa,M Mostafa,A Nayerhoda,L Nellen,M Newbold,MU Nisa,R Noriega-Papaqui,L Olivera-Nieto,N Omodei,A Peisker,Y Pérez Araujo,EG Pérez,CD Rho,C Rivière,D Rosa-Gonzalez,E Ruiz-Velasco,J Ryan,HI Salazar,F Salesa Greus,A Sandoval,M Schneider,H Schoorlemmer,J Serna-Franco,G Sinnis,AJ Smith,WR Springer,P Surajbali,I Taboada,M Tanner,K Tollefson,I Torres,R Torres Escobedo,R Turner,F Ureña-Mena,L Villaseñor,X Wang,IJ Watson,T Weisgarber,F Werner,E Willox,J Wood,G Yodh,A Zepeda,H Zhou,HAWC Collaboration

Published Date

2022/3

Monitoring the radio galaxy M87 with HAWC :: MPG.PuRe 日本語 Help Privacy Policy ポリシー/免責事項全文を含む詳細検索ブラウズホーム一時保存 (0)ツールアイテム詳細登録内容を編集ファイル形式で保存一時保存へ追加タグ情報を表示リリース履歴を表示詳細要約公開会議論文 Monitoring the radio galaxy M87 with HAWC MPS-Authors /persons/resource/persons30597 Hinton, J. Division Prof. Dr. James A. Hinton, MPI for Nuclear Physics, Max Planck Society; /persons/resource/persons135685 Werner, F. Division Prof. Dr. James A. Hinton, MPI for Nuclear Physics, Max Planck Society; External Resource There are no locators available Fulltext (restricted access) There are currently no full texts shared for your IP range. フルテキスト (公開) 公開されているフルテキストはありません付随資料 (公開) There is no public supplementary material available 引用 HAWC Collaboration, Abeysekara, AU, Albert, A., Alfaro, R., Alvarez, C.…

Arrival Directions of Cosmic Rays above 32 EeV from Phase One of the Pierre Auger Observatory

Authors

Pedro Abreu,Marco Aglietta,Justin M Albury,Ingomar Allekotte,K Almeida Cheminant,Alejandro Almela,Jaime Alvarez-Muñiz,R Alves Batista,J Ammerman Yebra,Gioacchino Alex Anastasi,Luis Anchordoqui,Belén Andrada,Sofia Andringa,Carla Aramo,PR Araújo Ferreira,Enrico Arnone,JC Arteaga Velázquez,H Asorey,Pedro Assis,Gualberto Avila,Emanuele Avocone,Alina Mihaela Badescu,Alena Bakalova,Alexandru Balaceanu,Felicia Barbato,Jose A Bellido,Corinne Berat,Mario Edoardo Bertaina,Gopal Bhatta,PL Biermann,Virginia Binet,Kathrin Bismark,Teresa Bister,Jonathan Biteau,Jiri Blazek,Carla Bleve,Johannes Blümer,Martina Boháčová,Denise Boncioli,Carla Bonifazi,L Bonneau Arbeletche,Nataliia Borodai,Ana Martina Botti,Jeffrey Brack,Thomas Bretz,PG Brichetto Orchera,Florian Lukas Briechle,Peter Buchholz,Antonio Bueno,Stijn Buitink,Mario Buscemi,Max Büsken,Karen S Caballero-Mora,Lorenzo Caccianiga,Fabrizia Canfora,Ioana Caracas,Rossella Caruso,Antonella Castellina,Fernando Catalani,Gabriella Cataldi,Lorenzo Cazon,Marcos Cerda,Jose Augusto Chinellato,Jiri Chudoba,Ladislav Chytka,Roger W Clay,AC Cobos Cerutti,Roberta Colalillo,Alan Coleman,Maria Rita Coluccia,Ruben Conceição,Antonio Condorelli,Giovanni Consolati,Fernando Contreras,Fabio Convenga,D Correia Dos Santos,CE Covault,Sergio Dasso,Kai Daumiller,Bruce R Dawson,Jarryd A Day,Rogerio M de Almeida,Joaquín de Jesús,Sijbrand J de Jong,JRT de Mello Neto,Ivan De Mitri,Jaime de Oliveira,Danelise de Oliveira Franco,Francesco de Palma,Vitor de Souza,Emanuele De Vito,Antonino Del Popolo,Mariano del Río,Olivier Deligny,Luca Deval,Armando Di Matteo,Madalina Dobre,Carola Dobrigkeit,Juan Carlos D’Olivo,LM Domingues Mendes,RC Dos Anjos,Maria Teresa Dova,Jan Ebr,Ralph Engel,Italo Epicoco,Martin Erdmann,Carlos O Escobar,Alberto Etchegoyen,Heino Falcke,John Farmer,Glennys Farrar,AC Fauth,Norberto Fazzini,Fridtjof Feldbusch,Francesco Fenu,Brian Fick,Juan Manuel Figueira,Andrej Filipčič,Thomas Fitoussi,Tomas Fodran,Toshihiro Fujii,Alan Fuster,Cristina Galea,Claudio Galelli,Beatriz García,Hartmut Gemmeke,Flavia Gesualdi,Alexandru Gherghel-Lascu,Piera Luisa Ghia,Ugo Giaccari,Marco Giammarchi,Jonas Glombitza,Fabian Gobbi,Fernando Gollan,Geraldina Golup,M Gómez Berisso,PF Gómez Vitale,Juan Pablo Gongora,Juan Manuel González,Nicolás González,Isabel Goos,Dariusz Góra,Alessio Gorgi,Marvin Gottowik,Trent D Grubb,F Guarino,GP Guedes,E Guido,S Hahn,P Hamal

Journal

The Astrophysical Journal

Published Date

2022/8/24

Cosmic rays are observed up to the astounding energies of more than 1020 eV, making them the most energetic particles known in the universe. However, the origin of these particles remains elusive. The search for the sources of ultra-high-energy cosmic rays (UHECRs), at energies above a few EeV (1 EeV≡ 1018 eV), is challenging since they are almost all charged particles and thus deflected by the magnetic fields permeating the interstellar, intra-halo, and intergalactic media (see, eg, Alves Batista et al. 2019, for an overview). These magnetic fields are difficult to study and their modeling is far from being complete. However, above a few tens of EeV, the deflections could be small enough for cosmic rays to retain some directional information on the position of their sources, at least for nuclei with a sufficiently small charge (eg, Erdmann et al. 2016; Farrar & Sutherland 2019). The cosmological volume within which …

A search for photons with energies above 2× 1017 eV using hybrid data from the low-energy extensions of the Pierre Auger Observatory

Authors

Pedro Abreu,Marco Aglietta,Justin M Albury,Ingomar Allekotte,K Almeida Cheminant,Alejandro Almela,Jaime Alvarez-Muñiz,R Alves Batista,J Ammerman Yebra,Gioacchino Alex Anastasi,Luis Anchordoqui,Belén Andrada,Sofia Andringa,Carla Aramo,PR Araújo Ferreira,Enrico Arnone,JC Arteaga Velázquez,H Asorey,Pedro Assis,Gualberto Avila,Emanuele Avocone,Alina Mihaela Badescu,Alena Bakalova,Alexandru Balaceanu,Felicia Barbato,Jose A Bellido,Corinne Berat,Mario Edoardo Bertaina,Gopal Bhatta,PL Biermann,Virginia Binet,Kathrin Bismark,Teresa Bister,Jonathan Biteau,Jiri Blazek,Carla Bleve,Johannes Blümer,Martina Boháčová,Denise Boncioli,Carla Bonifazi,L Bonneau Arbeletche,Nataliia Borodai,Ana Martina Botti,Jeffrey Brack,Thomas Bretz,PG Brichetto Orchera,Florian Lukas Briechle,Peter Buchholz,Antonio Bueno,Stijn Buitink,Mario Buscemi,Max Büsken,Karen S Caballero-Mora,Lorenzo Caccianiga,Fabrizia Canfora,Ioana Caracas,Rossella Caruso,Antonella Castellina,Fernando Catalani,Gabriella Cataldi,Lorenzo Cazon,Marcos Cerda,Jose Augusto Chinellato,Jiri Chudoba,Ladislav Chytka,Roger W Clay,AC Cobos Cerutti,Roberta Colalillo,Alan Coleman,Maria Rita Coluccia,Ruben Conceição,Antonio Condorelli,Giovanni Consolati,Fernando Contreras,Fabio Convenga,D Correia dos Santos,CE Covault,Sergio Dasso,Kai Daumiller,Bruce R Dawson,Jarryd A Day,Rogerio M de Almeida,Joaquín de Jesús,Sijbrand J de Jong,JRT de Mello Neto,Ivan De Mitri,Jaime de Oliveira,Danelise de Oliveira Franco,Francesco de Palma,Vitor de Souza,Emanuele De Vito,Antonino Del Popolo,Mariano del Río,Olivier Deligny,Luca Deval,Armando Di Matteo,Madalina Dobre,Carola Dobrigkeit,Juan Carlos D’Olivo,LM Domingues Mendes,RC Dos Anjos,Maria Teresa Dova,Jan Ebr,Ralph Engel,Italo Epicoco,Martin Erdmann,Carlos O Escobar,Alberto Etchegoyen,Heino Falcke,John Farmer,Glennys Farrar,AC Fauth,Norberto Fazzini,Fridtjof Feldbusch,Francesco Fenu,Brian Fick,Juan Manuel Figueira,Andrej Filipčič,Thomas Fitoussi,Tomas Fodran,Toshihiro Fujii,Alan Fuster,Cristina Galea,Claudio Galelli,Beatriz García,AL Garcia Vegas,Hartmut Gemmeke,Flavia Gesualdi,Alexandru Gherghel-Lascu,Piera Luisa Ghia,Ugo Giaccari,Marco Giammarchi,Jonas Glombitza,Fabian Gobbi,Fernando Gollan,Geraldina Golup,M Gómez Berisso,PF Gómez Vitale,Juan Pablo Gongora,Juan Manuel González,Nicolás González,Isabel Goos,Dariusz Góra,Alessio Gorgi,Marvin Gottowik,Trent D Grubb,F Guarino,GP Guedes,E Guido,S Hahn

Journal

The Astrophysical Journal

Published Date

2022/7/8

The recent observations of photons with energies of a few 1014 eV from decaying neutral pions, both from a direction coincident with a giant molecular cloud (HAWC J1825-134, Albert et al. 2021) and from the Galactic plane (Amenomori et al. 2021), provide evidence for an acceleration of cosmic rays to energies of several 1015 eV, and above, in the Galaxy. A dozen sources emitting photons with energies up to 1015 eV have even been reported (Cao et al. 2021a), and in at least one of them (LHAASO J2108+ 515, also in directional coincidence with a giant molecular cloud), these photons might have a hadronic origin (Cao et al. 2021b). Observations of these photons are key in probing the mechanisms of particle acceleration, completing the multi-messenger approach aimed at understanding the nonthermal processes producing cosmic rays. The detection of even higher-energy photons would be of considerable …

Downward terrestrial gamma-ray flashes at the Pierre Auger observatory?

Authors

Roberta Colalillo,Pedro Abreu,Marco Aglietta,Justin M Albury,Ingomar Allekotte,Alejandro Almela,Jaime Alvarez-Muniz,Rafael Alves Batista,Gioacchino Alex Anastasi,L Anchordoqui,Belén Andrada,Sofia Andringa,Carla Aramo,Paulo Ricardo Araújo Ferreira,Juan Carlos Arteaga Velazquez,H Asorey,Pedro Assis,Gualberto Avila,Alina Mihaela Badescu,Alena Bakalova,Alexandru Balaceanu,Felicia Barbato,Ricardo Jorge Barreira Luz,Karl-Heinz Becker,Jose A Bellido,Corinne Berat,Mario Edoardo Bertaina,Xavier Bertou,Peter L Biermann,Virginia Binet,Kathrin Bismark,Teresa Bister,Jonathan Biteau,Jiri Blazek,Carla Bleve,Martina Bohacova,Denise Boncioli,Carla Bonifazi,Luan Bonneau Arbeletche,Nataliia Borodai,Ana Martina Botti,Jeffrey Brack,Thomas Bretz,P Gabriel Brichetto Orchera,Florian Lukas Briechle,Peter Buchholz,Antonio Bueno,Stijn Buitink,Mario Buscemi,M Busken,Karen S Caballero-Mora,Lorenzo Caccianiga,Fabrizia Canfora,Ioana Caracas,Juan Miguel Carceller,Rossella Caruso,Antonella Castellina,Fernando Catalani,Gabriella Cataldi,Lorenzo Cazon,Marcos Cerda,Jose Augusto Chinellato,Jiří Chudoba,Ladislav Chytka,Roger W Clay,AC Cobos Cerutti,Alan Coleman,Maria Rita Coluccia,Rúben Conceição,Antonio Condorelli,Giovanni Consolati,Fernando Contreras,Fabio Convenga,Diego Correia dos Santos,CE Covault,Sergio Dasso,Kai Daumiller,Bruce R Dawson,Jarryd A Day,Rogerio M de Almeida,Joaquín de Jesús,Sijbrand J de Jong,Giuseppe De Mauro,JRT de Mello Neto,Ivan De Mitri,Jaime de Oliveira,Danelise de Oliveira Franco,Francesco de Palma,Vitor de Souza,Emanuele De Vito,Mariano del Río,Olivier Deligny,Luca Deval,Armando di Matteo,Carola Dobrigkeit,Juan Carlos D'Olivo,Luis Miguel Domingues Mendes,Rita Cassia dos Anjos,Diego dos Santos,Maria Teresa Dova,Jan Ebr,Ralph Engel,Italo Epicoco,Martin Erdmann,Carlos O Escobar,Alberto Etchegoyen,Heino Falcke,John Farmer,G Farrar,AC Fauth,Norberto Fazzini,Fridtjof Feldbusch,Francesco Fenu,Brian Fick,Juan Manuel Figueira,Andrej Filipcic,Thomas Fitoussi,Tomáš Fodran,Martín Miguel Freire,Toshihiro Fujii,Alan Fuster,Cristina Galea,Claudio Galelli,Beatriz García,Adrianna Luz García Vegas,Hartmut Gemmeke,Flavia Gesualdi,Alexandru Gherghel-Lascu,Piera Luisa Ghia,Ugo Giaccari,Marco Giammarchi,Jonas Glombitza,Fabian Gobbi,Fernando Gollan,Geraldina Golup,Mariano Gomez Berisso,Primo F Gomez Vitale,Juan Pablo Gongora,Juan Manuel González,N González,Isabel Goos,Dariusz Gora,Alessio Gorgi,Marvin Gottowik,Trent D Grubb,F Guarino,GP Guedes,Eleonora Guido,S Hahn,Petr Hamal

Journal

Pos proceedings of science

Published Date

2022

At the Pierre Auger Observatory, designed primarily to study ultra-high-energy cosmic rays, phenomena related to atmospheric electricity are also observed. Particularly, events have been detected with the surface detector, characterized by long-lasting signals (tens of microseconds) and event footprints much larger (up to 200 km2) than those produced by the highest energy cosmic rays. Moreover, some of them appear to be accompanied by smaller events occurring in the same area within about 1 ms and probably produced by the same phenomenon. A previously reported correlation with the World Wide Lightning Location Network, as well as the observation of very low-altitude clouds, confirm that such events are related to thunderstorms. An ad-hoc reconstruction points to high-energy particles being produced very close to the ground, suggesting that they originate from electrons accelerated to relativistic energies in strong electric fields inside low clouds, as is the case for terrestrial gamma-ray flashes above thunderstorms. A clear explanation of the observed phenomenon is hindered by two facts. One is that the rate of such events, detected serendipitously, is very small (less than 2 events/year) and decreases further after optimization of the surface detector trigger for low-energy shower-events. The second is that most events show a puzzling lack of signals in the central part of the footprint. We have studied in detail both effects and will present such studies here. We developed a strategy for a dedicated trigger to enhance the detection efficiency for these events associated with atmospheric-electricity events.

Monte Carlo simulations for the Pierre Auger Observatory using the VO auger grid resources

Authors

Eva Santos,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

Cosmic rays are mostly fully ionized atomic nuclei that permanently reach us from outside the Solar system. More than one century has passed since their discovery [1]. However, their nature, sources, and acceleration mechanisms are still largely unknown. The cosmic-ray spectrum can be relatively well described over an extensive energy range by a power-law whose spectral index slightly deviates from 3, showing remarkably very few distinctive features [2]. Whereas at sub-GeV energies, the mass composition of cosmic rays can be measured directly by balloon or space-borne experiments with isotope precision, and at multi-TeV with elemental precision [3, 4], significant uncertainties rapidly arise as soon as direct detections cease to be viable. Coincidently, around the same energy, the indirect detection of cosmic rays becomes feasible thanks to the many millions of particles generated in a cascading process that initiates from the interaction of the cosmic ray in the Earth’s atmosphere-a phenomenon called an extensive air shower. In the latter, the cosmic-ray energy and mass composition have to be derived indirectly from air shower and detector simulations.However, at the highest energies, full shower simulations become computationally prohibitive since the number of secondary particles produced in one extensive air shower, which scales linearly with the energy of the primary cosmic ray, exceeds 1010 at 1019 eV [5, 6]. These limitations were overcome by the development of thinning algorithms, which allow reducing the number of simulated particles with energies falling below a pre-defined threshold [7]. In this case, only a representative …

Update of the Offline Framework for AugerPrime

Authors

Lukas Nellen,Pedro Abreu,Marco Aglietta,Justin M Albury,Ingomar Allekotte,Alejandro Almela,Jaime Alvarez-Muniz,Rafael Alves Batista,Gioacchino Alex Anastasi,L Anchordoqui,Belén Andrada,Sofia Andringa,Carla Aramo,Paulo Ricardo Araújo Ferreira,Juan Carlos Arteaga Velazquez,H Asorey,Pedro Assis,Gualberto Avila,Alina Mihaela Badescu,Alena Bakalova,Alexandru Balaceanu,Felicia Barbato,Ricardo Jorge Bar-Reira Luz,Karl-Heinz Becker,Jose A Bellido,Corinne Berat,Mario Edoardo Bertaina,Xavier Bertou,Peter L Biermann,Virginia Binet,Kathrin Bismark,Teresa Bister,Jonathan Biteau,Jiri Blazek,Carla Bleve,Martina Bohacova,Denise Boncioli,Carla Bonifazi,Luan Bonneau Arbeletche,Nataliia Borodai,Ana Martina Botti,Jeffrey Brack,Thomas Bretz,PG Brichetto Orchera,FL Briechle,P Buchholz,A Bueno,S Buitink,M Buscemi,M Busken,KS Caballero-Mora,L Caccianiga,F Canfora,I Caracas,JM Carceller,R Caruso,A Castellina,F Catalani,G Cataldi,L Cazon,M Cerda,JA Chinellato,J Chudoba,L Chytka,RW Clay,AC Cobos Cerutti,R Colalillo,A Coleman,MR Coluccia,R Conceição,A Condorelli,G Consolati,F Contreras,F Convenga,D Correia dos Santos,CE Covault,S Dasso,K Daumiller,BR Dawson,JA Day,RM de Almeida,J de Jesús,SJ de Jong,G De Mauro,JRT de Mello Neto,I De Mitri,J de Oliveira,D de Oliveira Franco,F de Palma,V de Souza,E De Vito,M del Río,O Deligny,L Deval,A di Matteo,C Dobrigkeit,JC D'Olivo,LM Domingues Mendes,RC dos Anjos,D dos Santos,MT Dova,J Ebr,R Engel,I Epicoco,M Erdmann,CO Escobar,A Etchegoyen,H Falcke,J Farmer,G Farrar,AC Fauth,N Fazzini,F Feldbusch,F Fenu,B Fick,JM Figueira,A Filipcic,T Fitoussi,T Fodran,MM Freire,T Fujii,A Fuster,C Galea,C Galelli,B García,AL Garcia Vegas,H Gemmeke,F Gesualdi,A Gherghel-Lascu,PL Ghia,U Giaccari,M Giammarchi,J Glombitza,F Gobbi,F Gollan,G Golup,M Gomez Berisso,PF Gomez Vitale,JP Gongora,JM González,N González,I Goos,D Góra,A Gorgi,M Gottowik,TD Grubb,F Guarino,GP Guedes,Eleonora Guido,S Hahn

Journal

POS PROCEEDINGS OF SCIENCE

Published Date

2022

Authors

Published Date

2022/3

Search for TeV decaying dark matter from the Virgo cluster of galaxies :: MPG.PuRe 日本語 Help Privacy Policy ポリシー/免責事項全文を含む詳細検索ブラウズホーム一時保存 (0)ツールアイテム詳細登録内容を編集ファイル形式で保存一時保存へ追加タグ情報を表示リリース履歴を表示詳細要約公開会議論文 Search for TeV decaying dark matter from the Virgo cluster of galaxies MPS-Authors /persons/resource/persons30597 Hinton, J. Division Prof. Dr. James A. Hinton, MPI for Nuclear Physics, Max Planck Society; /persons/resource/persons135685 Werner, F. Division Prof. Dr. James A. Hinton, MPI for Nuclear Physics, Max Planck Society; External Resource There are no locators available Fulltext (restricted access) There are currently no full texts shared for your IP range. フルテキスト (公開) 公開されているフルテキストはありません付随資料 (公開) There is no public supplementary material available 引用 HAWC …

Recent results from HAWC

Authors

Miguel Mostafa

Journal

44th COSPAR Scientific Assembly. Held 16-24 July

Published Date

2022/7

High energy gamma-ray observations are an essential probe of cosmic-ray acceleration mechanisms. The detection of the highest energy gamma rays and the shortest timescales of variability are the key to improve our understanding of the acceleration processes and the environment of the cosmic accelerators. The High Altitude Water Cherenkov (HAWC) experiment is a large field-of-view, multi-TeV, gamma-ray observatory continuously operating at 14,000 ft since March, 2015. The HAWC observatory has an order of magnitude better sensitivity, angular resolution, and background rejection than the previous generation of water-Cherenkov arrays. The improved performance allows us to discover TeV sources, to detect transient events, to study the Galactic diffuse emission at TeV energies, to measure or constrain the TeV spectra of GeV gamma-ray sources, and to search for Galactic Pevatrons. I will present the …

Search for spatial correlations of neutrinos with ultra-high-energy cosmic rays

Authors

Arnauld Albert,S Alves,Michel André,Marco Anghinolfi,S Ardid,J-J Aubert,J Aublin,Bruny Baret,S Basa,Bouchra Belhorma,Meriem Bendahman,Vincent Bertin,S Biagi,Matthias Bissinger,Jihad Boumaaza,M Bouta,MC Bouwhuis,H Brânzaş,R Bruijn,J Brunner,J Busto,B Caiffi,D Calvo,A Capone,L Caramete,J Carr,V Carretero,S Celli,M Chabab,TN Chau,R Cherkaoui El Moursli,T Chiarusi,M Circella,A Coleiro,R Coniglione,P Coyle,A Creusot,AF Díaz,C Distefano,I Di Palma,A Domi,C Donzaud,D Dornic,D Drouhin,T Eberl,T van Eeden,D van Eijk,N El Khayati,A Enzenhöfer,P Fermani,G Ferrara,F Filippini,L Fusco,Y Gatelet,P Gay,H Glotin,R Gozzini,R Gracia Ruiz,K Graf,C Guidi,S Hallmann,H van Haren,AJ Heijboer,Y Hello,JJ Hernández-Rey,J Hössl,J Hofestädt,F Huang,G Illuminati,CW James,B Jisse-Jung,M De Jong,P de Jong,M Kadler,O Kalekin,U Katz,NR Khan-Chowdhury,A Kouchner,I Kreykenbohm,V Kulikovskiy,R Lahmann,R Le Breton,S LeStum,D Lefèvre,E Leonora,G Levi,D Lopez-Coto,S Loucatos,L Maderer,J Manczak,M Marcelin,A Margiotta,A Marinelli,JA Martínez-Mora,B Martino,K Melis,P Migliozzi,A Moussa,R Muller,L Nauta,S Navas,E Nezri,BÓ Fearraigh,A Păun,GE Păvălaş,C Pellegrino,M Perrin-Terrin,V Pestel,P Piattelli,C Pieterse,C Poirè,V Popa,T Pradier,N Randazzo,D Real,S Reck,G Riccobene,A Romanov,A Sánchez-Losa,F Salesa Greus,DFE Samtleben,M Sanguineti,P Sapienza,J Schnabel,J Schumann,F Schüssler,J Seneca,M Spurio,Th Stolarczyk,M Taiuti,Y Tayalati,SJ Tingay,B Vallage,V Van Elewyck,F Versari,S Viola,D Vivolo,J Wilms,S Zavatarelli,A Zegarelli,JD Zornoza,J Zúñiga,R Abbasi,M Ackermann,J Adams,JA Aguilar,M Ahlers,M Ahrens,JM Alameddine,C Alispach

Journal

The Astrophysical Journal

Published Date

2022/8/3

Earth is continuously bombarded by high-energy cosmic rays, most of which are charged atomic nuclei (Particle Data Group et al. 2020). It is generally believed that cosmic rays with energies above 1 EeV (1018 eV), known as ultra-high-energy cosmic rays (UHECRs), mostly originate from extragalactic sources in the nearby universe. Based on the estimated magnitude of galactic magnetic fields (Nagano & Watson 2000), cosmic rays below this energy are believed to diffuse within their host galaxy, whereas cosmic rays above this energy escape from the galaxy. These assumptions are confirmed by the observation of large-scale anisotropies in the arrival directions of UHECRs above 8EeV with the excess flux directed from outside of our Galaxy (Aab et al. 2017). The two largest observatories for UHECRs are the Pierre Auger Observatory (Auger; The Pierre Auger Collaboration 2015) in Argentina in the Southern …

Performance of the 433 m surface array of the Pierre Auger Observatory

Authors

Gaia Silli,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

The detection of the cosmic-ray (CR) energy spectrum with surface detectors spans over six orders of magnitude in energy, from 1015 eV up to more than 1020 eV. It follows a power-law with a spectral index≃ 3 exhibiting five features identified by small deviations in the spectral index: the knee, the second knee, the ankle, the “instep”[1], and a suppression at the highest energies. Particularly, the second knee has been observed at∼ 1017 eV by several observatories as a steepening of the spectrum [2–6]. Its interpretation may be connected to the maximal energy of the accelerators in the Galaxy, considering that a gradual heavier composition has been observed at these energies [7], which is along the lines of the so-called Peters cycles [8]. The astrophysical interpretation of the acquired data is still delicate, mainly because the nature of the sources, the propagation effects, and the CR composition are strongly entwined. A signature of neutral particles such as photons and neutrinos around the second-knee may shed light on this problem, since they are not deflected by magnetic fields, thus providing valuable information about the acceleration processes in astrophysical objects.A more accurate understanding of the origin of the second knee may be possible if one observatory is capable of measuring all spectral features and the CR mass composition with a common energy scale. In this sense, the Pierre Auger Observatory extended its Surface Detector (SD) with the deployment of a433-m spaced triangular array (SD-433) of water-Cherenkov detectors (WCDs) to unveil the spectral region below 1017 eV. The installation of muon, radio, and …

Energy spectrum of cosmic rays measured using the Pierre Auger Observatory

Authors

V Novotny,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,U Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

Authors

Ana Martina Botti,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

The first surface detector of the Pierre Auger Observatory [1] consisted of an array of about 1600 water-Cherenkov stations distributed in a triangular grid with 1500m spacing (SD-1500) covering a total area of 3000 km2. It was meant to detect cosmic rays with full efficiency at energies above 1018. 5 eV. After its completion, in 2008, two denser arrays with reduced spacings of 750 m (SD-750) and 433 m (SD-433) were deployed as a part of the Auger Muon and Infill for the Ground Array (AMIGA)[2] enhancement. The energy threshold of the surface detector was then extended to 1016. 5 eV. In addition, AMIGA is also aimed at obtaining direct measurements of the muonic component of air showers with an underground muon detector (UMD). The UMD consists of an array of scintillators associated with the water-Cherenkov detectors of the SD-750 and SD-433. At each grid position, three 10 m2 modules are buried at a depth of 2.3 m to shield them from the electromagnetic component of air showers [3]. Each module consists, in turn, of 64 scintillator strips with wavelength-shifting optical fiber coupled to an array of silicon photomultipliers (SiPMs)[4]. Pictures of a module commissioning are presented in Fig. 1: we show a module under construction (left) and deployment (middle), along with an image of a complete deployed station (right) just before being overburden with soil. The whole UMD array will have 73 positions, 219 modules, and over 14000 SiPMs. The deployment status, at the time of writing, is presented in Fig. 2 where we discriminate the positions shared with the SD-1500 (blue circles) and only AMIGA (gray circles for the SD-750 and red …

Analysis of a Sample of High-Energy Peaked BL Lac Objects with the HAWC Observatory

Authors

Erica Heller,Hugo Ayala,Miguel Mostafa,HAWC Team

Journal

APS April Meeting Abstracts

Published Date

2022/4

We identified candidate TeV emitters from a list of published High-Energy peaked BL Lac (HBL). We searched for very-high energy (VHE) gamma-ray emission from these objects using the six-year data set from the High Altitude Water Cherenkov (HAWC) Observatory. We established flux upper limits assuming extrapolated power laws for each source. We will present the results of our search in the VHE range as well as preliminary physical models of these sources using both X-ray and gamma-ray data.

The all-particle cosmic ray energy spectrum measured with HAWC

Authors

Journal

27th European Cosmic Ray Symposium

Published Date

2022/3

The all-particle cosmic ray energy spectrum measured with HAWC in the TeV region - NASA/ADS Now on home page ads icon ads Enable full ADS view NASA/ADS The all-particle cosmic ray energy spectrum measured with HAWC in the TeV region Morales-Soto, JA ; Arteaga-Velázquez, JC ; HAWC Collaboration Abstract Publication: 27th European Cosmic Ray Symposium Pub Date: 2023 Bibcode: 2023ecrs.confE..87M full text sources Publisher | © The SAO/NASA Astrophysics Data System adshelp[at]cfa.harvard.edu The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86A NASA logo Smithsonian logo Resources About ADS ADS Help What's New Careers@ADS Social @adsabs ADS Blog Project Switch to full ADS Is ADS down? (or is it just me...) Smithsonian Institution Smithsonian Privacy Notice Smithsonian Terms of Use Smithsonian …

Limits on the Diffuse Gamma-Ray Background above 10 TeV with HAWC

Authors

A Albert,R Alfaro,C Alvarez,JC Arteaga-Velázquez,D Avila Rojas,HA Solares,R Babu,E Belmont-Moreno,C Brisbois,KS Caballero-Mora,T Capistrán,A Carramiñana,S Casanova,O Chaparro-Amaro,U Cotti,J Cotzomi,S Coutiño de León,E De la Fuente,R Diaz Hernandez,BL Dingus,MA DuVernois,M Durocher,JC Díaz-Vélez,K Engel,C Espinoza,KL Fan,M Fernández Alonso,N Fraija,D Garcia,JA García-González,F Garfias,MM González,JA Goodman,JP Harding,S Hernandez,J Hinton,D Huang,F Hueyotl-Zahuantitla,P Hüntemeyer,A Iriarte,V Joshi,S Kaufmann,D Kieda,A Lara,WH Lee,H León Vargas,JT Linnemann,AL Longinotti,G Luis-Raya,K Malone,O Martinez,J Martínez-Castro,JA Matthews,P Miranda-Romagnoli,JA Morales-Soto,E Moreno,M Mostafá,A Nayerhoda,L Nellen,M Newbold,MU Nisa,R Noriega-Papaqui,N Omodei,A Peisker,Y Pérez Araujo,EG Pérez-Pérez,CD Rho,D Rosa-González,E Ruiz-Velasco,H Salazar,F Salesa Greus,A Sandoval,M Schneider,J Serna-Franco,AJ Smith,Y Son,RW Springer,O Tibolla,K Tollefson,I Torres,R Torres-Escobedo,R Turner,F Ureña-Mena,L Villaseñor,X Wang,E Willox,H Zhou,C de León,JD Álvarez,HAWC Collaboration

Journal

arXiv preprint arXiv:2209.08106

Published Date

2022/9/16

Authors

Eric Mayotte,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

The energy spectrum of ultra-high-energy cosmic rays, UHECRs, undergoes a hardening at 5EeV called the ankle [1]. Above this energy, the flux has long been thought to be primarily extragalactic in origin [2]. Observation confirmed this through the recent discovery of a dipole anisotropy in the arrival directions of UHECRs with energies slightly above the ankle (> 8EeV)[3]. This is further supported by evidence of anisotropies occurring near the flux suppression at around 40 EeV [4]. Above the ankle, the mass composition of UHECRs is also best described as consisting of a mix of light, intermediate and high-mass primaries [5, 6]. A mixed composition in turn implies that, at fixed energies, each species will undergo differing deflections in magnetic fields. Additionally, due to energy-loss effects which depend on primary mass and charge, at a fixed energy the horizon of each species, and therefore potentially their source distributions, differ [7]. These give rise to the possibility of mass dependent anisotropies in the UHECR flux. More specifically, simulation using both the Jansson-Farrar, JF12 [8], and the Pshirkov, Tinyakov and Kronberg, PTK11 [9], models of the Galactic Magnetic Field, GMF, have shown that around a rigidity of∼ 6EV, the propagation of UHECRs in the GMF transitions from diffusive to ballistic [10]. From this, it is clear that as energy increases, the lighter, less charged, components of the flux will reach this threshold first, and therefore can be expected to display some degree of their source anisotropy in their local arrival directions. The heavier species however, would maintain a more isotropic distribution until much higher energies …

Combined fit of the energy spectrum and mass composition across the ankle with the data measured at the Pierre Auger Observatory

Authors

T Bister,Pedro Abreu,Marco Aglietta,Justin M Albury,Ingomar Allekotte,Alejandro Almela,Jaime Alvarez-Muniz,Rafael Alves Batista,Gioacchino Alex Anastasi,L Anchordoqui,Belén Andrada,Sofia Andringa,Carla Aramo,Paulo Ricardo Araújo Ferreira,Juan Carlos Arteaga Velazquez,H Asorey,Pedro Assis,Gualberto Avila,Alina Mihaela Badescu,Alena Bakalova,Alexandru Balaceanu,Felicia Barbato,Ricardo Jorge Barreira Luz,Karl-Heinz Becker,Jose A Bellido,Corinne Berat,Mario Edoardo Bertaina,Xavier Bertou,Peter L Biermann,Virginia Binet,Kathrin Bismark,J Biteau,J Blazek,C Bleve,M Bohacova,D Boncioli,C Bonifazi,L Bonneau Arbeletche,N Borodai,AM Botti,J Brack,T Bretz,PG Brichetto Orchera,FL Briechle,P Buchholz,A Bueno,S Buitink,M Buscemi,M Busken,KS Caballero-Mora,L Caccianiga,F Canfora,I Caracas,JM Carceller,R Caruso,A Castellina,F Catalani,G Cataldi,L Cazon,M Cerda,JA Chinellato,J Chudoba,L Chytka,RW Clay,AC Cobos Cerutti,R Colalillo,A Coleman,MR Coluccia,R Conceicao,A Condorelli,G Consolati,F Contreras,F Convenga,D Correia dos Santos,CE Covault,S Dasso,K Daumiller,BR Dawson,JA Day,RM de Almeida,J de Jesus,SJ de Jong,G De Mauro,JRT de Mello Neto,I De Mitri,J de Oliveira,D de Oliveira Franco,F de Palma,V de Souza,E De Vito,M del Rio,O Deligny,L Deval,A di Matteo,C Dobrigkeit,JC D'Olivo,LM Domingues Mendes,RC dos Anjos,D dos Santos,MT Dova,J Ebr,R Engel,I Epicoco,M Erdmann,CO Escobar,A Etchegoyen,H Falcke,J Farmer,G Farrar,AC Fauth,N Fazzini,F Feldbusch,F Fenu,B Fick,JM Figueira,A Filipcic,T Fitoussi,T Fodran,MM Freire,T Fujii,A Fuster,C Galea,C Galelli,B Garcia,AL Garcia Vegas,H Gemmeke,F Gesualdi,A Gherghel-Lascu,PL Ghia,U Giaccari,M Giammarchi,J Glombitza,F Gobbi,F Gollan,G Golup,M Gomez Berisso,PF Gomez Vitale,JP Gongora,JM Gonzalez,N Gonzalez,I Goos,D Gora,A Gorgi,M Gottowik,TD Grubb,F Guarino,GP Guedes,E Guido,S Hahn,Petr Hamal

Journal

Pos proceedings of science

Published Date

2022

The combined fit of the measured energy spectrum and distribution of depths of shower maximum of ultra-high-energy cosmic rays is known to constrain the parameters of astrophysical scenarios with homogeneous source distributions. Further measurements show that the cosmic-ray arrival directions agree better with the directions and fluxes of catalogs of starburst galaxies and active galactic nuclei than with isotropy. Here, we present a novel combination of both analyses. For that, a three-dimensional universe model containing a nearby source population and a homogeneous background source distribution is built, and its parameters are adapted using a combined fit of the energy spectrum, depth of shower maximum distribution and energy-dependent arrival directions. The model takes into account a symmetric magnetic field blurring, source evolution and interactions during propagation. We use simulated data, which resemble measurements of the Pierre Auger Observatory, to evaluate the method’s sensitivity. With this, we are able to verify that the source parameters as well as the fraction of events from the nearby source population and the size of the magnetic field blurring are determined correctly, and that the data is described by the fitted model including the catalog sources with their respective fluxes and three-dimensional positions. We demonstrate that by combining all three measurements we reach the sensitivity necessary to discriminate between the catalogs of starburst galaxies and active galactic nuclei.

Study of the morphology of the region surrounding eHWC J1850+ 001

Authors

Journal

37th International Cosmic Ray Conference.

Published Date

2022/1

The VHE source eHWC J1850+ 001 was identified to emit significant flux above 50 TeV and was fit with a Gaussian extent of 0.37◦±0.16◦[1]. However, in the region surrounding eHWC J1850+ 001, significant emission has been observed at lower energies in the High Energy Stereoscopic System (HESS) Galactic Plane Survey (hereafter HGPS) and previous catalogs from the High Altitude Water Cherenkov (HAWC) Collaboration [2–4]. Unlike the HGPS, the 2HWC and 3HWC did not provide a detailed description of the morphology and spectrum of the region, instead using a more simplistic search for isolated sources, both point-like and extended [2, 3]. The 3HWC search found four sources in the region, with the HGPS reporting three. With the context of this high energy detection, and multiple sources in the region at lower energies in those catalogs, a detailed investigation of the region testing the likelihood of different models is needed to better interpret the HAWC data.

Studying High-Mass Microquasars with HAWC

Authors

Journal

Proceedings of Science

Published Date

2022

High-mass microquasars (HMMQs) are powerful particle accelerators, but their mechanism of the high-energy emission is poorly understood. To date, only a handful of these particle engines have ever been observed to emit gamma-ray photons and are thus potential TeV gamma-ray emitters. In this work, we study four HMMQs, namely, LS 5039, Cyg X-1, Cyg X-3, and SS 433 using the data from the High Altitude Water Cherenkov (HAWC) observatory. We perform time dependent analyses on each HMMQ to look for any periodic variations in their flux. We produce light curves using the HAWC daily maps from which we generate Lomb-Scargle periodograms. By analysing the significance of the periodogram peaks, we assess whether or not HAWC is sensitive to orbitally modulating TeV gamma-ray flux in the four HMMQs.

Large-scale and multipolar anisotropies of cosmic rays detected at the Pierre Auger Observatory with energies above 4 EeV

Authors

RM Almeida,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

Ultra-high energy cosmic rays (UHECR) are particles with energies above 1 EeV that hit our atmosphere coming from space. Their origin remains an open question in physics and astrophysics. The study of anisotropies in the arrival directions of UHECR as a function of energy is a very important element to unveil their sources. In particular, together with the analysis of features in the energy spectrum and information about the mass composition of these high-energy particles, it can help to understand their acceleration mechanisms at their sources and how they propagate up to Earth. Since the majority of UHECR are charged particles, they are deflected along with their propagation on magnetic field regions. The poor knowledge about the magnitude of the galactic and extragalactic magnetic fields and chemical composition of the cosmic rays makes the identification of such sources a very difficult task. Large-scale anisotropies such as dipolar or quadrupolar patterns in the flux of UHECR are expected in the case of diffusive or quasi-rectilinear propagation from an anisotropic distribution of sources or diffusive propagation from the closest extragalactic source (s). Even for a pure dipole gradient at the entrance of the Galaxy, magnetic deflections are expected to give rise to higher-order multipoles, although with small amplitude [1]. Moreover, the cosmic-ray flux could be also affected by random configurations of point sources and magnetic deflections, showing the relevance of extending the search to larger multipoles. We reconstruct the dipolar and quadrupolar components through a combined Fourier analysis of the event rate in right ascension and …

Authors

Journal

Proceedings of Science

Published Date

2022/3

In addition to dense regions of dark matter, such as galaxy clusters and dwarf galaxies, dark matter annihilation and decay are also expected to have a nearly isotropic distribution across the sky. This isotropic component is less model-dependent than the flux from isolated dark matter targets, and would produce galactic contributions to the Diffuse Gamma-Ray Background (DGRB). With its continuous monitoring of the gamma-ray sky from a few hundred GeV to several hundred TeV and its wide field-of-view, the High Altitude Water Cherenkov (HAWC) observatory is well-suited to search for dark matter contributions in the DGRB. In this work, 535 days of HAWC data and Monte Carlo simulations were studied to set limits on annihilating or decaying diffuse dark matter at TeV energies. With this data, we consider both leptonic and hadronic dark matter channels and are able to constrain dark matter up to masses> 100 TeV.

Constraints on the very high energy gamma-ray emission from short GRBs with HAWC

Authors

A Albert,R Alfaro,C Alvarez,JC Arteaga-Velázquez,KP Arunbabu,D Avila Rojas,HA Ayala Solares,R Babu,E Belmont-Moreno,C Brisbois,KS Caballero-Mora,T Capistrán,A Carramiñana,S Casanova,O Chaparro-Amaro,U Cotti,J Cotzomi,S Coutiño De León,C De León,E De la Fuente,R Diaz Hernandez,S Dichiara,BL Dingus,MA DuVernois,M Durocher,JC Díaz-Vélez,K Engel,C Espinoza,KL Fan,N Fraija,A Galván-Gámez,JA García-González,F Garfias,MM González,JA Goodman,JP Harding,S Hernandez,B Hona,D Huang,F Hueyotl-Zahuantitla,TB Humensky,P Hüntemeyer,A Iriarte,V Joshi,S Kaufmann,A Lara,WH Lee,H León Vargas,JT Linnemann,AL Longinotti,G Luis-Raya,K Malone,SS Marinelli,O Martinez,J Martínez-Castro,JA Matthews,P Miranda-Romagnoli,JA Morales-Soto,E Moreno,M Mostafá,A Nayerhoda,L Nellen,M Newbold,R Noriega-Papaqui,A Peisker,Y Pérez Araujo,EG Pérez-Pérez,Z Ren,CD Rho,D Rosa-González,M Rosenberg,JR Sacahui,H Salazar,F Salesa Greus,A Sandoval,J Serna-Franco,AJ Smith,RW Springer,P Surajbali,O Tibolla,K Tollefson,I Torres,R Torres-Escobedo,R Turner,L Villaseñor,X Wang,E Willox,A Zepeda,H Zhou,HAWC COLLABORATION

Journal

The Astrophysical Journal

Published Date

2022/9/8

Many gamma-ray bursts (GRBs) have been observed from radio wavelengths, and a few at very high energies (VHEs,> 100 GeV). The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is well suited to study transient phenomena at VHEs owing to its large field of view and duty cycle. These features allow for searches of VHE emission and can probe different model assumptions of duration and spectra. In this paper, we use data collected by HAWC between 2014 December and 2020 May to search for emission in the energy range from 80 to 800 GeV coming from a sample of 47 short GRBs that triggered the Fermi, Swift, and Konus satellites during this period. This analysis is optimized to search for delayed and extended VHE emission within the first 20 s of each burst. We find no evidence of VHE emission, either simultaneous or delayed, with respect to the prompt emission. Upper limits (90 …

VizieR Online Data Catalog: The 2HWC HAWC Observatory gamma-ray cat.(Abeysekara+, 2017)

Authors

AU Abeysekara,A Albert,R Alfaro,C Alvarez,JD Alvarez,R Arceo,JC Arteaga-Velazquez,HA Ayala Solares,AS Barber,B Baughman,N Bautista-Elivar,J Becerra Gonzalez,A Becerril,E Belmont-Moreno,SY Benzvi,D Berley,A Bernal,J Braun,C Brisbois,KS Caballero-Mora,T Capistran,A Carraminana,S Casanova,M Castillo,U Cotti,J Cotzomi,S Coutino de Leon,E de La Fuente,C de Leon,R Diaz Hernandez,BL Dingus,MA Duvernois,JC Diaz-Velez,RW Ellsworth,K Engel,DW Fiorino,N Fraija,JA Garcia-Gonzalez,F Garfias,M Gerhardt,A Gonzalez Munoz,MM Gonzalez,JA Goodman,Z Hampel-Arias,JP Harding,S Hernandez,A Hernandez-Almada,J Hinton,CM Hui,P Huntemeyer,A Iriarte,A Jardin-Blicq,V Joshi,S Kaufmann,D Kieda,A Lara,RJ Lauer,WH Lee,D Lennarz,H Leon Vargas,JT Linnemann,AL Longinotti,G Luis Raya,R Luna-Garcia,R Lopez-Coto,K Malone,SS Marinelli,O Martinez,SI Martinez-Castellano,J Martinez-Castro,H Martinez-Huerta,JA Matthews,P Miranda-Romagnoli,E Moreno,M Mostafa,L Nellen,M Newbold,MU Nisa,R Noriega-Papaqui,R Pelayo,J Pretz,EG Perez-Perez,Z Ren,CD Rho,C Riviere,D Rosa-Gonzalez,M Rosenberg,E Ruiz-Velasco,H Salazar,F Salesa Greus,A Sandoval,M Schneider,H Schoorlemmer,G Sinnis,AJ Smith,RW Springer,P Surajbali,I Taboada,O Tibolla,K Tollefson,I Torres,TN Ukwatta,G Vianello,L Villasenor,T Weisgarber,S Westerhoff,IG Wisher,J Wood,T Yapici,PW Younk,A Zepeda,H Zhou

Journal

VizieR Online Data Catalog

Published Date

2022/8

The High-Altitude Water Cherenkov (HAWC) detector is located in central Mexico at 18 59'41" N, 97 18'30.6" W and an elevation of 4100m asl The instrument comprises of 300 identical water Cherenkov detectors (WCDs). The angular resolution of the HAWC instrument varies with the event size (number of hit photomultiplier tubes (PMTs)). It ranges from~ 0.2 (68% containment) for large events events hitting almost all the PMTs, to~ 1.0 for events near the analysis threshold.

Satellite Data for Atmospheric Monitoring at the Pierre Auger Observatory

Authors

Andrew Puyleart,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

Figure 1: A map of the Pierre Auger Observatory. Water-Cherenkov stations of the surface detector are seen as black dots and the field of view of the fluorescence detector stations are indicated by the blue lines. The high-elevation extension of the fluorescence detector, HEAT, is also seen in orange. The Xtreme and Central Laser Facilities are labelled in red. The balloon launch site and engineering array are also labelled.

Characterizing gamma-ray sources with HAL (HAWC Accelerated likelihood) and 3ML

Authors

Anushka Udara Abeysekara,A Albert,R Alfaro,C Alvarez,J d Álvarez Romero,JR Camacho,JC Arteaga Velazquez,AB Kollamparambil,Avila Rojas,HA Ayala Solares,R Babu,V Baghmanyan,AS Barber,J Becerra Gonzalez,E Belmont-Moreno,S BenZvi,D Berley,C Brisbois,KS Caballero Mora,T Capistrán,A Carramiñana,S Casanova,O Chaparro-Amaro,U Cotti,J Cotzomi,S Coutiño de Leon,E de la Fuente,CL de León,L Diaz,R Diaz Hernandez,JC Díaz Vélez,B Dingus,M Durocher,M DuVernois,R Ellsworth,K Engel,Espinoza Hernández,J Fan,K Fang,M Fernandez Alonso,B Fick,H Fleischhack,JL Flores,NI Fraija,D Garcia Aguilar,JA Garcia-Gonzalez,JL García-Luna,G García-Torales,F Garfias,G Giacinti,H Goksu,MM González,JA Goodman,JP Harding,S Hernández Cadena,I Herzog,J Hinton,B Hona,D Huang,F Hueyotl-Zahuantitla,M Hui,B Humensky,P Hüntemeyer,A Iriarte,A Jardin-Blicq,H Jhee,V Joshi,D Kieda,GJ Kunde,S Kunwar,A Lara,J Lee,WH Lee,D Lennarz,H Leon Vargas,J Linnemann,AL Longinotti,R Lopez-Coto,G Luis-Raya,J Lundeen,K Malone,V Marandon,O Martinez,I Martinez Castellanos,H Martínez Huerta,J Martínez-Castro,J Matthews,J McEnery,P Miranda-Romagnoli,JA Morales Soto,E Moreno Barbosa,M Mostafa,A Nayerhoda,L Nellen,M Newbold,MU Nisa,R Noriega-Papaqui,L Olivera-Nieto,N Omodei,A Peisker,Y Pérez Araujo,EG Pérez Pérez,CD Rho,C Rivière,D Rosa-Gonzalez,E Ruiz-Velasco,J Ryan,HI Salazar,F Salesa Greus,A Sandoval,M Schneider,H Schoorlemmer,J Serna-Franco,G Sinnis,AJ Smith,WR Springer,P Surajbali,I Taboada,M Tanner,K Tollefson,I Torres,R Torres Escobedo,R Turner,F Ureña-Mena,L Villaseñor,X Wang,IJ Watson,T Weisgarber,F Werner,E Willox,J Wood,G Yodh,A Zepeda,H Zhou

Journal

37th International Cosmic Ray Conference.

Published Date

2022/1

The Multi-Mission Maximum Likelihood (3ML) framework enables multiwavelength data analysis in a statistically consistent way across a wide range of energies [1]. Combined with the 3ML affiliated astromodels package allows the arbitrary definition of one or more sources and their spectra in a flexible way that enables multisource fits to be performed with relative ease. 3ML has plugins for many instruments: HAWC, Fermi-LAT, Swift XRT, all OGIP compliant instruments, POLAR, VERITAS, INTEGRAL/SPI, and KONUS. These allow for an analysis to incorporate information from a wide range of energies so that the best understanding of a source or region in the sky can be reached.The use of 3ML has been ubiquitous within HAWC for several years. The HAWC plugin for 3ML was originally developed as an internal software tool that was largely inaccessible to those outside the collaboration. However the 3ML framework was heavily embedded in important HAWC analyses [2]. Giacomo Vianello was a HAWC member and wrote the original code for HAWC Accelerated Likelihood (HAL).

The upgrade of the Pierre auger observatory with the scintillator surface detector

Authors

G Cataldi,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

The upgrade [1, 2] of the Auger Observatory [3] follows from a decade of discovery and a recognition that shower-by-shower measurements of cosmic ray mass-related properties are essential to advance the field further [4]. The main scientific aspects motivating the upgrade are the lack of information on the primary mass composition at the highest energies, the observation that the averaged mass tends to increase at the highest energies complicating the anisotropy search, and the discrepancies among the hadronic interaction models predictions and the measured shower parameters. The upgrade consists of new plastic scintillator detectors (SSD) on top of the Water Cherenkov Detector (WCD) of the Surface Detector array (SD), an additional small photomultiplier (sPMT) installed in the WCD for the extension of the dynamic range, and new SD electronics provided by an Upgraded Unified Board (UUB)[5]. Additionally, an underground muon detector [6] is going to be deployed beside each WCD in the 750m region of the Observatory to provide direct muon measurements. The upgrade will also be complemented by extending the measurements of the existing fluorescence detector [7] into periods of higher night-sky background to increase their duty cycle. Finally, based on the Auger Radio Engineering Array (AERA) experience and results, a radio detector is also included on top of every WCD to improve the measurement of the inclined showers since the SSDs are mostly sensitive to the vertical ones [8, 9]. In March 2019, the first 77 SSDs deployed had been equipped with photomultiplier tubes and put into data acquisition using an adapted …

Outreach activities at the Pierre Auger Observatory

Authors

Karen Salomé Caballero-Mora,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,U Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

Authors

Viviana Scherini,R Alves Batista,F Canfora,SJ de Jong,G De Mauro,H Falcke,T Fodran,C Galea,UG Giaccari,J Hörandel,AR Khakurdikar,BBT Pont,MR Pothast,C Timmermans

Published Date

2022

The Pierre Auger Collaboration has recently released 10% of the data recorded using the world’s largest cosmic ray detector [1, 2]. The Observatory Open Data are released under the (CC BY-SA 4.0) International License. All datasets have a unique DOI that you are requested to cite in any applications or publications. The current release should be cited as: Pierre Auger Collaboration (2021), Auger Open Data release 1-2021, DOI: 1. 5281/zenodo. 4487613. Data from the Observatory come from a variety of instruments and take many forms, starting from raw experimental data, through reconstructed data and datasets of higher level generated by analysis workflows all the way to data presented in scientific publications. These data were made available publicly with the expectation that they will be used by a wide and diverse community including professional and citizen-scientists and for educational and outreach initiatives. While the Collaboration has released data in a similar manner for over a decade, the present release is much wider with regard to both the quantity and type of data, making them suitable both for educational purposes and for scientific research.The rich harvest of the Pierre Auger Collaboration covers different and complementary fields of research. The main focus, the nature and origin of ultra-high energy cosmic rays (UHECR), relies on measurements of the energy spectrum and mass composition of the primaries, carried out with unprecedented precision, on multi-messenger studies and on extensive searches for anisotropy at both large and intermediate angular scales. Interactions of primary cosmic rays in the atmosphere …

The TeV Sun Rises: Discovery of Gamma rays from the Quiescent Sun with HAWC

Authors

A Albert,R Alfaro,C Alvarez,JC Arteaga-Velazquez,D Avila Rojas,HA Solares,R Babu,E Belmont-Moreno,C Brisbois,KS Caballero-Mora,T Capistran,A Carraminana,S Casanova,O Chaparro-Amaro,U Cotti,J Cotzomi,S Coutino de Leon,E De la Fuente,R Diaz Hernandez,BL Dingus,MA DuVernois,M Durocher,JC Diaz-Velez,RW Ellsworth,K Engel,C Espinoza,KL Fan,K Fang,M Fernandez Alonso,H Fleischhack,N Fraija,JA Garcia-Gonzalez,F Garfia,MM Gonzalez,JA Goodman,JP Harding,S Hernandez,J Hinton,D Huang,F Hueyotl-Zahuantitla,P Huntemeyer,A Iriarte,V Joshi,S Kaufmann,J Lee,JT Linnemann,AL Longinotti,G Luis-Raya,K Malone,O Martinez,J Martinez-Castro,JA Matthews,P Miranda-Romagnoli,JA Morales-Soto,E Moreno,M Mostafa,A Nayerhoda,L Nellen,MU Nisa,R Noriega-Papaqui,L Olivera-Nieto,N Omodei,Y Pérez Araujo,EG Perez-Perez,CD Rho,D Rosa-Gonzalez,E Ruiz-Velasco,H Salazar,D Salazar-Gallegos,A Sandoval,M Schneider,J Serna-Franco,AJ Smith,Y Son,RW Springer,O Tibolla,K Tollefson,I Torres,R Torres-Escobedo,R Turner,F Urena-Mena,X Wang,IJ Watson,E Willox,S Yun-Cárcamo,H Zhou,C de León,JF Beacom,T Linden,KCY Ng,AHG Peter,B Zhou

Journal

arXiv preprint arXiv:2212.00815

Published Date

2022/12/1

We report the first detection of a TeV gamma-ray flux from the solar disk (6.3), based on 6.1 years of data from the High Altitude Water Cherenkov (HAWC) observatory. The 0.5--2.6 TeV spectrum is well fit by a power law, dN/dE = , with TeV cm s and . The flux shows a strong indication of anticorrelation with solar activity. These results extend the bright, hard GeV emission from the disk observed with Fermi-LAT, seemingly due to hadronic Galactic cosmic rays showering on nuclei in the solar atmosphere. However, current theoretical models are unable to explain the details of how solar magnetic fields shape these interactions. HAWC's TeV detection thus deepens the mysteries of the solar-disk emission.

Multimessenger NuEM Alerts with AMON

Authors

Journal

Proceedings of Science

Published Date

2022/3

The Astrophysical Multimessenger Observatory Network (AMON), has developed a real-time multi-messenger alert system. The system performs coincidence analyses of datasets from gamma-ray and neutrino detectors, making the Neutrino-Electromagnetic (NuEM) alert channel. For these analyses, AMON takes advantage of sub-threshold events, ie, events that by themselves are not significant in the individual detectors. The main purpose of this channel is to search for gamma-ray counterparts of neutrino events. We will describe the different analyses that make-up this channel and present a selection of recent results.

A measurement of the proton plus helium spectrum of cosmic rays in the TeV region with HAWC

Authors

A Albert,R Alfaro,C Alvarez,JR Camacho,JC Arteaga-Velázquez,KP Arunbabu,D Avila Rojas,HA Solares,E Belmont-Moreno,C Brisbois,KS Caballero-Mora,T Capistrán,A Carramiñana,S Casanova,U Cotti,J Cotzomi,E De la Fuente,R Diaz Hernandez,MA DuVernois,M Durocher,JC Díaz-Vélez,C Espinoza,N Fraija,JA García-González,F Garfias,MM González,JA Goodman,JP Harding,B Hona,D Huang,F Hueyotl-Zahuantitla,P Hüntemeyer,A Iriarte,V Joshi,D Kieda,GJ Kunde,A Lara,WH Lee,H León Vargas,JT Linnemann,AL Longinotti,G Luis-Raya,K Malone,O Martinez,J Martínez-Castro,JA Matthews,P Miranda-Romagnoli,JA Morales-Soto,E Moreno,M Mostafá,A Nayerhoda,L Nellen,M Newbold,R Noriega-Papaqui,N Omodei,EG Pérez-Pérez,CD Rho,D Rosa-González,H Salazar,F Salesa Greus,A Sandoval,J Serna-Franco,AJ Smith,RW Springer,K Tollefson,I Torres,R Torres-Escobedo,F Ureña-Mena,L Villaseñor,X Wang,E Willox,H Zhou,C de León,JD Álvarez,GB Yodh,A Zepeda,HAWC Collaboration

Journal

arXiv preprint arXiv:2208.13350

Published Date

2022/8/29

HAWC is an air-shower detector designed to study TeV gamma and cosmic rays. The observatory is composed of a array of water Cherenkov tanks ( deep x diameter) with photomultipliers (PMT) each. The instrument registers the number of hit PMTs, the timing information and the total charge at the PMTs during the event. From these data, shower observables such as the arrival direction, the core position at ground, the lateral age and the primary energy are estimated. In this work, we study the distribution of the shower age vs the primary energy of a sample of shower data collected by HAWC from June 2015 to June 2019 and employ a shower-age cut based on predictions of QGSJET-II-04 to separate a subsample of events dominated by H and He primaries. Using these data and a dedicated analysis, we reconstruct the cosmic ray spectrum of H+He from to TeV, which shows the presence of a softening at around TeV with a statistical significance of .

See List of Professors in Miguel Mostafa University(Penn State University)