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1. Wave function of the sexaquark or compact H-dibaryon

Author

Glennys R. Farrar and Nico Wintergerst

Subjects
Hadronic Spectroscopy, Structure and Interactions, Lattice QCD, Properties of Hadrons, Specific QCD Phenomenology, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract

Abstract We derive and explicitly display the internal wave function of a color-, flavor- and spin- singlet dibaryon composed of uuddss quarks in a spatially symmetric state, in the approximation of exact SU(3) flavor symmetry. This wavefunction shows that the often-used superposition of ΛΛ, NΞ and ΣΣ baryons, relevant for di-baryon molecules, accounts for only 1/5 of a spatially symmetric six-quark color-flavor-spin-singlet state, with the remaining 4/5 consisting of products of color-octet baryons. Using the correct wavefunction has important implications for calculations of the mass of the lowest-lying flavor-singlet dibaryon, as we illustrate using the Cornell potential. We also provide a compact representation of the state in terms of creation operators, and comment on the impact of not using the optimal operator in lattice studies of this system.

Published
2023
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2. Ultra-High-Energy Cosmic Rays Accelerated by Magnetically Dominated Turbulence

Author

Luca Comisso, Glennys R. Farrar, and Marco S. Muzio

Subjects
Particle astrophysics, High energy astrophysics, Cosmic rays, Plasma astrophysics, Plasma physics, Astrophysics, QB460-466
Abstract

Ultra-high-energy cosmic rays (UHECRs), particles characterized by energies exceeding 10 ^18 eV, are generally believed to be accelerated electromagnetically in high-energy astrophysical sources. One promising mechanism of UHECR acceleration is magnetized turbulence. We demonstrate from first principles, using fully kinetic particle-in-cell simulations, that magnetically dominated turbulence accelerates particles on a short timescale, producing a power-law energy distribution with a rigidity-dependent, sharply defined cutoff well approximated by the form ${f}_{\mathrm{cut}}\left(E,{E}_{\mathrm{cut}}\right)={\rm{sech}} \left[{(E/{E}_{\mathrm{cut}})}^{2}\right]$ . Particle escape from the turbulent accelerating region is energy dependent, with t _esc ∝ E ^− ^δ and δ ∼ 1/3. The resulting particle flux from the accelerator follows ${dN}/{dEdt}\propto {E}^{-s}{\rm{sech}} \left[{(E/{E}_{\mathrm{cut}})}^{2}\right]$ , with s ∼ 2.1. We fit the Pierre Auger Observatory’s spectrum and composition measurements, taking into account particle interactions between acceleration and detection, and show that the turbulence-associated energy cutoff is well supported by the data, with the best-fitting spectral index being $s={2.1}_{-0.13}^{+0.06}$ . Our first-principles results indicate that particle acceleration by magnetically dominated turbulence may constitute the physical mechanism responsible for UHECR acceleration.

Published
2024
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3. Where Did the Amaterasu Particle Come From?

Author

Michael Unger and Glennys R. Farrar

Subjects
Cosmic rays, Ultra-high-energy cosmic radiation, Milky Way magnetic fields, Cosmic ray astronomy, Astrophysics, QB460-466
Abstract

The Telescope Array Collaboration recently reported the detection of a cosmic-ray particle, “Amaterasu,” with an extremely high energy of 2.4 × 10 ^20 eV. Here we investigate its probable charge and the locus of its production. Interpreted as a primary iron nucleus or slightly stripped fragment, the event fits well within the existing paradigm for UHECR composition and spectrum. Using the most up-to-date modeling of the Galactic magnetic field strength and structure, and taking into account uncertainties, we identify the likely volume from which it originated. We estimate a localization uncertainty on the source direction of 6.6% of 4 π or 2726 deg ^2 . The uncertainty of magnetic deflections and the experimental energy uncertainties contribute about equally to the localization uncertainty. The maximum source distance is 8–50 Mpc, with the range reflecting the uncertainty on the energy assignment. We provide sky maps showing the localization region of the event and superimpose the location of galaxies of different types. There are no candidate sources among powerful radio galaxies. An origin in active galactic nuclei or star-forming galaxies is unlikely but cannot be completely ruled out without a more precise energy determination. The most straightforward option is that Amaterasu was created in a transient event in an otherwise undistinguished galaxy.

Published
2024
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4. The Large-scale Anisotropy and Flux (de)magnification of Ultrahigh-energy Cosmic Rays in the Galactic Magnetic Field

Author

Teresa Bister, Glennys R. Farrar, and Michael Unger

Subjects
Cosmic ray astronomy, Cosmic rays, Cosmic ray sources, Extragalactic magnetic fields, Milky Way magnetic fields, Ultra-high-energy cosmic radiation, Astrophysics, QB460-466
Abstract

We calculate the arrival direction distribution of ultrahigh-energy cosmic rays (UHECRs) with a new suite of models of the Galactic magnetic field (GMF), assuming sources follow the large-scale structure of the Universe. Compared to previous GMF models, the amplitude of the dipole component of the UHECR arrival flux is significantly reduced. We find that the reduction is due to the accidentally coinciding position of the peak of the extragalactic UHECR flux and the boundary of strong flux demagnification due to the GMF toward the central region of the Galaxy. This serendipitous sensitivity of UHECR anisotropies to the GMF model will be a powerful probe of the source distribution as well as Galactic and extragalactic magnetic fields. Demagnification by the GMF also impacts the visibility of some popular source candidates.

Published
2024
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5. Constraints on UHECR Sources and Extragalactic Magnetic Fields from Directional Anisotropies

Author

Teresa Bister and Glennys R. Farrar

Subjects
Cosmic ray astronomy, Cosmic ray sources, Ultra-high-energy cosmic radiation, Extragalactic magnetic fields, Milky Way magnetic fields, Cosmic anisotropy, Astrophysics, QB460-466
Abstract

A dipole anisotropy in ultra–high-energy cosmic ray (UHECR) arrival directions, of extragalactic origin, is now firmly established at energies E > 8 EeV. Furthermore, the UHECR angular power spectrum shows no power at smaller angular scales than the dipole, apart from hints of possible individual hot or warm spots for energy thresholds ≳40 EeV. Here we exploit the magnitude of the dipole and the limits on smaller-scale anisotropies to place constraints on two quantities: the extragalactic magnetic field (EGMF) and the number density of UHECR sources or the volumetric event rate if UHECR sources are transient. We also vary the bias between the extragalactic matter and the UHECR source densities, reflecting whether UHECR sources are preferentially found in over- or underdense regions, and find that little or no bias is favored. We follow Ding et al. (2021) in using the CosmicFlows-2 density distribution of the local universe as our baseline distribution of UHECR sources, but we improve and extend that work by employing an accurate and self-consistent treatment of interactions and energy losses during propagation. Deflections in the Galactic magnetic field are treated using either the full JF12 magnetic field model, with both random and coherent components, or just the coherent part, to bracket the impact of the GMF on the dipole anisotropy. This large-scale structure model gives good agreement with both the direction and magnitude of the measured dipole anisotropy and forms the basis for simulations of discrete sources and the inclusion of EGMF effects.

Published
2024
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6. The Coherent Magnetic Field of the Milky Way

Author

Michael Unger and Glennys R. Farrar

Subjects
Milky Way magnetic fields, Galaxy magnetic fields, Milky Way Galaxy physics, Cosmic rays, Cosmic ray astronomy, Astrophysics, QB460-466
Abstract

We present a suite of models of the coherent magnetic field of the Galaxy based on new divergence-free parametric functions describing the global structure of the field. The model parameters are fit to the latest full-sky Faraday rotation measures (RMs) of extragalactic sources and polarized synchrotron intensity (PI) maps from the Wilkinson Microwave Anisotropy Probe and Planck. We employ multiple models for the density of thermal and cosmic-ray electrons in the Galaxy, needed to predict the sky maps of RMs and PI for a given Galactic magnetic field (GMF) model. The robustness of the inferred properties of the GMF is gauged by studying many combinations of parametric field models and electron density models. We determine the pitch angle of the local magnetic field (11° ± 1°), explore the evidence for a grand-design spiral coherent magnetic field (inconclusive), determine the strength of the toroidal and poloidal magnetic halo fields below and above the disk (magnitudes the same for both hemispheres within ≈10%), set constraints on the half-height of the cosmic-ray diffusion volume (≥2.9 kpc), investigate the compatibility of RM- and PI-derived magnetic field strengths (compatible under certain assumptions), and check if the toroidal halo field could be created by the shear of the poloidal halo field due to the differential rotation of the Galaxy (possibly). A set of eight models is identified to help quantify the present uncertainties in the coherent GMF spanning different functional forms, data products, and auxiliary input. We present the corresponding sky maps of rates for axion–photon conversion in the Galaxy and deflections of ultrahigh-energy cosmic rays.

Published
2024
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7. Constraints on the Hosts of UHECR Accelerators

Author

Marco Stein Muzio and Glennys R. Farrar

Subjects
Ultra-high-energy cosmic radiation, Cosmic ray sources, Astrophysics, QB460-466
Abstract

Interactions of ultra-high-energy cosmic rays (UHECRs) in the surroundings of their accelerators can naturally explain the observed spectrum and composition of UHECRs, including the abundance of protons below the ankle. Here we show that astrophysical properties of the UHECR source environment such as the temperature, size, and magnetic field can be constrained by UHECR and neutrino data. Applying this to candidate sources with a simple structure shows that starburst galaxies are consistent with these constraints, but galaxy clusters are in tension with them. For multicomponent systems like active galactic nuclei and gamma-ray bursts, the results are indicative, but a customized analysis is needed for definitive conclusions.

Published
2023
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8. Hunting Super-heavy Dark Matter with Ultra-high Energy Photons

Author

Luis A Anchordoqui, Corinne Berat, Mario E Bertaina, Antonella Castellina, Olivier Deligny, Ralph Engel, Glennys R Farrar, Piera L Ghia, Dan Hooper, Oleg Kalashev, Mikhail Kuznetsov, Marcus Niechciol, Angela V Olinto, Philipp Papenbreer, Lorenzo Perrone, Julian Rautenberg, Andrés Romero-Wolf, Pierpaolo Savina, Jorge F Soriano, and Tonia M Venters

Subjects
Astrophysics
Abstract

At any epoch, particle physics must be open to completely unexpected discoveries, and that is reason enoughto extend the reach of searches for ultra-high energy (UHE) photons. The observation of a population ofphotons with energies𝐸 ≳100 EeVwould for example imply the existence of either a completely new physicalphenomena, or particle acceleration mechanisms heretofore never seen or imagined. But as we outline in thisLetter of Interest, there are also good arguments for super-heavy dark matter (SHDM) in a parameter rangesuch that it could be discovered via its decays to, in particular, UHE photons. Only ultra-high energy cosmic rayobservatories have capabilities to detect UHE photons. We first investigate how current and future observationscan probe and constrain SHDM models in important directions, and then outline some of the scenarios thatmotivate such searches. We also discuss connections between constraints on SHDM and on the parametervalues of cosmological models

Published
2021
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9. Probing hadronic interactions using the latest data measured by the Pierre Auger Observatory

Author

Caterina Trimarelli, Pedro Abreu, Marco Aglietta, Ingomar Allekotte, Kévin Almeida Cheminant, Alejandro Almela, Jaime Alvarez-Muniz, Juan Ammerman Yebra, Gioacchino Alex Anastasi, Luis A. Anchordoqui, Belén Andrada, Sofia Andringa, Carla Aramo, Paulo Ricardo Araújo Ferreira, Enrico Arnone, Juan Carlos Arteaga Velazquez, Hernán Gonzalo 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, Peter L. Biermann, Virginia Binet, Kathrin Bismark, Teresa Bister, Jonathan Biteau, Jiri Blazek, Carla Bleve, Johannes Blümer, Martina Bohacova, Denise Boncioli, Carla Bonifazi, Luan Bonneau Arbeletche, Nataliia Borodai, Jeffrey Brack, Thomas Bretz, P. Gabriel Brichetto Orchera, Florian Lukas Briechle, Peter Buchholz, Antonio Bueno, Stijn Buitink, Mario Buscemi, Max Büsken, Anthony Bwembya, Karen S. Caballero-Mora, Lorenzo Caccianiga, Ioana Caracas, Rossella Caruso, Antonella Castellina, Fernando Catalani, Gabriella Cataldi, Lorenzo Cazon, Marcos Cerda, Jose Augusto Chinellato, Jiří Chudoba, Ladislav Chytka, Roger W Clay, Agustín Cobos Cerutti, Roberta Colalillo, Alan Coleman, Maria Rita Coluccia, Rúben Conceição, Antonio Condorelli, Giovanni Consolati, Fernando Contreras, Fabio Convenga, Diego Correia dos Santos, Corbin Covault, Markus Cristinziani, Sergio Dasso, Kai Daumiller, Bruce R. Dawson, Jarryd A. Day, Rogerio M. de Almeida, Joaquin de Jesus, Sijbrand J. de Jong, João 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, Olivier Deligny, Luca Deval, Armando di Matteo, Madalina Dobre, Carola Dobrigkeit, Juan Carlos D'Olivo, Luis Miguel Domingues Mendes, Rita Cassia dos Anjos, Maria Teresa Dova, Jan Ebr, Mohamed Eman, Ralph Engel, Italo Epicoco, Martin Erdmann, Carlos O. Escobar, Alberto Etchegoyen, Heino Falcke, John Farmer, Glennys R. Farrar, Anderson Campos Fauth, Norberto Fazzini, Fridtjof Feldbusch, Francesco Fenu, Brian Fick, Juan Manuel Figueira, Andrej Filipcic, Thomas Fitoussi, Tomáš 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, Mariano Gómez Berisso, Primo F. Gómez Vitale, Juan Pablo Gongora, Juan Manuel González, Nicolas Martin Gonzalez, Isabel Goos, Dariusz Gora, Alessio Gorgi, Marvin Gottowik, Trent D. Grubb, Fausto Guarino, Germano Guedes, Eleonora Guido, Steffen Traugott Hahn, Petr Hamal, Matías Rolf Hampel, Patricia María Hansen, Diego Harari, Violet M. Harvey, Andreas Haungs, Thomas Hebbeker, Dieter Heck, Carlos Hojvat, Jörg R. Hörandel, Pavel Horvath, Miroslav Hrabovsky, Tim Huege, Antonio Insolia, Paula Gina Isar, Petr Janecek, Jeffrey A. Johnsen, Jakub Jurysek, Alex Kääpä, Karl-Heinz Kampert, Bianca Keilhauer, Abha Khakurdikar, Varada Varma Kizakke Covilakam, Hans Klages, Matthias Kleifges, Jonny Kleinfeller, Felix Knapp, Norbert Kunka, Bruno L. Lago, Niklas Langner, Marcelo Augusto Leigui de Oliveira, Vladimir Lenok, Antoine Letessier-Selvon, Isabelle Lhenry-Yvon, Domenico Lo Presti, Luis LOPES, Rebeca López, Lu Lu, Quentin Luce, Jon Paul Lundquist, Allan Machado Payeras, Giovanni Mancarella, Dusan Mandat, Bradley C. Manning, Julien Manshanden, Paul Mantsch, Sullivan Marafico, Federico Maria Mariani, Analisa Mariazzi, Ioana Maris, Giovanni Marsella, Daniele Martello, Sara Martinelli, Oscar Martínez Bravo, Miguel Alexandre Martins, Massimo Mastrodicasa, Hermann-Josef Mathes, James Matthews, Giorgio Matthiae, Eric William Mayotte, Sonja Mayotte, Peter Mazur, Gustavo Medina-Tanco, Diego Melo, Alexander Menshikov, Stanislav Michal, Maria Isabel Micheletti, Lino Miramonti, Silvia Mollerach, François Montanet, Leonel Morejon, Carlo Morello, Ana L. Müller, Katharine Mulrey, Roberto Mussa, Marco Stein Muzio, Wilson M. Namasaka, Alina Nasr-Esfahani, Lukas Nellen, Gabriela Nicora, Mihai Niculescu-Oglinzanu, Marcus Niechciol, Dave Nitz, Ian Norwood, Dalibor Nosek, Vladimír Novotný, Libor Nozka, Achille Nucita, Luis A. Nunez, Cainã Oliveira, Miroslav Palatka, Juan Pallotta, Gonzalo Parente, Alejandra Parra, Jannis Pawlowsky, Miroslav Pech, Jan Pękala, Rodrigo Pelayo, Edyvania Emily Pereira Martins, Johnnier Perez Armand, Carmina Pérez Bertolli, Lorenzo Perrone, Sergio Petrera, Camilla Petrucci, Tanguy Pierog, Mário Pimenta, Manuel Platino, Bjarni Pont, Mart Pothast, Paolo Privitera, Michael Prouza, Andrew Puyleart, Sven Querchfeld, Julian Rautenberg, Diego Ravignani, Maximilian Reininghaus, Jan Ridky, Felix Riehn, Markus Risse, Vincenzo Rizi, Washington Rodrigues de Carvalho, Jorge Rubén Rodriguez Rojo, Matías J. Roncoroni, Simone Rossoni, Markus Roth, Esteban Roulet, Adrian Rovero, Philip Ruehl, Alexandra Saftoiu, Mohit Saharan, Francesco Salamida, Humberto Ibarguen Salazar, Gaetano Salina, Jose Sanabria Gomez, Federico Andrés Sánchez, Edivaldo Moura Santos, Eva Santos, Fred Sarazin, Raul Sarmento, Ricardo Sato, Pierpaolo Savina, Christoph M. Schäfer, Viviana Scherini, Harald Schieler, Martin Schimassek, Michael Schimp, Felix Schlüter, David Schmidt, Olaf Scholten, Harm Schoorlemmer, Petr Schovanek, Frank G. Schröder, Josina Schulte, Tobias Schulz, Sergio J Sciutto, Marina Scornavacche, Alberto Segreto, Srijan Sehgal, Shima Ujjani Shivashankara, Guenter Sigl, Gaia Silli, Octavian Sima, Raluca Smau, Radomir Smida, Paul Sommers, Jorge F. Soriano, Ruben Squartini, Maximilian Stadelmaier, Denis Stanca, Samo Stanič, Jaroslaw Stasielak, Patrick Stassi, Maximilian Straub, Alexander Streich, Mauricio Suárez-Durán, Tristan Sudholz, Tiina Suomijarvi, A. Daniel Supanitsky, Zbigniew Szadkowski, Alex Tapia, Carla Taricco, Charles Timmermans, Olena Tkachenko, Petr Tobiska, Carlos J. Todero Peixoto, Bernardo Tomé, Zoé Torrès, Andres Travaini, Petr Travnicek, Matias Jorge Tueros, Ralf Ulrich, Michael Unger, Lukáš Vaclavek, Martin Vacula, Jose F. Valdés Galicia, Laura Valore, Enrique Varela, Adriana Vásquez-Ramírez, Darko Veberic, Cynthia Ventura, Indira D. Vergara Quispe, Valerio Verzi, Jakub Vicha, Jacco Vink, Serguei Vorobiov, Hernan Wahlberg, Clara Keiko Oliveira Watanabe, Alan Watson, Andreas Weindl, Lawrence Wiencke, Henryk Wilczyński, David Wittkowski, Brian Wundheiler, Alexey Yushkov, Orazio Zapparrata, Enrique Zas, Danilo Zavrtanik, Marko Zavrtanik, and Lukas Zehrer

Published
2022
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10. Constraining the origin of UHECRs and astrophysical neutrinos

Author

Marco Stein Muzio, Michael Unger, and Glennys R. Farrar

Subjects
Physics, Photon, Large Hadron Collider, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Phenomenology, Hadron, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic ray, Astrophysics, Spectral line, Coherence length, ddc:530, Ultrahigh energy, Neutrino
Abstract

We explore the possibility of a common origin of ultrahigh energy cosmic rays (UHECRs) and astrophysical neutrinos and further constrain sources which are consistent with this possibility. We show that the common origin hypothesis can be satisfied for the Sibyll2.3c hadronic interaction model but is difficult to accommodate for EPOS-LHC, showing that multimessenger analyses have the power to also constrain hadronic physics beyond LHC energies. We constrain properties of UHECR source environments (and potentially astrophysical neutrino sources), including their photon temperature, gas density, size, magnetic field strength and coherence length, using UHECR and neutrino spectra and composition. Our analysis represents a new type of information on UHECR sources, independent of the mechanism responsible for the UHECR acceleration.

Published
2022

11. A Uniformly Selected, Southern-Sky 6dF, Optical AGN Catalog

Author

Yan-Ping Chen, Ingyin Zaw, Glennys R. Farrar, and Sana Elgamal

Subjects
Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

We have constructed a catalog of active galactic nuclei (AGNs) with $z < 0.13$, based on optical spectroscopy, from the parent sample of galaxies in the 6dF galaxy survey (Final Release of 6dFGS), a census of the Southern hemisphere. This work is an extension of our all sky AGN catalog \citet [ZCF, here after]{ZCF19}. The ZCF is based on 43,533 galaxies with $\rm K_s \leq$ 11.75 ($z \leq 0.09$) in the 2MASS Redshift Survey (2MRS). The parent catalog of this work, the 6dF catalog, consists of 136,304 publicly available digital spectra for 125,071 galaxies with $\rm Dec \leq 0^\circ$ and $\rm K_s \leq 12.65$ (median $z = 0.053$). Our AGN catalog consists of 3109 broad line AGNs and 12,156 narrow line AGNs which satisfy the \citet{Kauffmann03} criteria, of which 3865 also satisfy the \citet{Kewley01} criteria. We also provide emission line widths, fluxes, flux errors, and signal-to-noise ratios of all the galaxies in our spectroscopic sample, allowing users to customize the selection criteria. In addition, we provide AGN likelihood for the rest of galaxies based on the availability and quality of their spectra. These likelihood values can be used for rigorous statistical analyses., 19 pages, 16 figures, accepted for publication in ApJS. arXiv admin note: text overlap with arXiv:1902.03799

Published
2021

13. Probing the environments surrounding ultrahigh energy cosmic ray accelerators and their implications for astrophysical neutrinos

Author

Marco Stein Muzio, Glennys R. Farrar, and Michael Unger

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), High Energy Physics - Phenomenology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We explore inferences on ultrahigh energy cosmic ray (UHECR) source environments -- constrained by the spectrum and composition of UHECRs and non-observation of extremely high energy neutrinos -- and their implications for the observed high energy astrophysical neutrino spectrum. We find acceleration mechanisms producing power-law CR spectra~$\propto E^{-2}$ are compatible with UHECR data, if CRs at high rigidities are in the quasi-ballistic diffusion regime as they escape their source environment. Both gas-dominated and photon-dominated source environments are able to account for UHECR observations, however photon-dominated sources give a better fit. Additionally, gas-dominated sources are in tension with current neutrino constraints. Accurate measurement of the neutrino flux at $\sim 10$ PeV will provide crucial information on the viability of gas-dominated sources, as well as whether diffusive shock acceleration is consistent with UHECR observations. We also show that UHECR sources are able to give a good fit to the high energy portion of the astrophysical neutrino spectrum, above $\sim$ PeV. This common origin of UHECRs and high energy astrophysical neutrinos is natural if air shower data is interpreted with the Sibyll2.3c hadronic interaction model, which gives the best-fit to UHECRs and astrophysical neutrinos in the same part of parameter space, but not for EPOS-LHC.

Published
2021

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

Author

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

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

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

Published
2021
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16. Hunting super-heavy dark matter with ultra-high energy photons

Author

Angela V. Olinto, Olivier Deligny, Marcus Niechciol, M. E. Bertaina, Glennys R. Farrar, Luis A. Anchordoqui, Philipp Papenbreer, Pierpaolo Savina, Andres Romero-Wolf, Dan Hooper, Julian Rautenberg, Piera Luisa Ghia, Jorge F. Soriano, Ralph Engel, Antonella Castellina, M. V. Kuznetsov, Tonia M. Venters, L. Perrone, Corinne Berat, Oleg Kalashev, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Anchordoqui, L. A., Berat, C., Bertaina, M. E., Castellina, A., Deligny, O., Engel, R., Farrar, G. R., Ghia, P. L., Hooper, D., Kalashev, O., Kuznetsov, M., Niechciol, M., Olinto, A. V., Papenbreer, P., Perrone, L., Rautenberg, J., Romero-Wolf, A., Savina, P., Soriano, J. F., and Venters, T. M.

Subjects
Photon, Astrophysics::High Energy Astrophysical Phenomena, Population, Dark matter, FOS: Physical sciences, Cosmic ray, Astrophysics, 01 natural sciences, 7. Clean energy, particle: acceleration, High Energy Physics - Phenomenology (hep-ph), Physical phenomena, cosmological model: parameter space, 0103 physical sciences, cosmic radiation: UHE, education, Superheavy dark matter, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Range (particle radiation), education.field_of_study, 010308 nuclear & particles physics, dark matter: mass, photon, Astronomy and Astrophysics, Particle acceleration, observatory, High Energy Physics - Phenomenology, High energy photon, Ultra-high energy photons, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract

At any epoch, particle physics must be open to completely unexpected discoveries, and that is reason enough to extend the reach of searches for ultra-high energy (UHE) photons. The observation of a population of photons with energies $E \gtrsim 100$ EeV would for example imply the existence of either a completely new physical phenomena, or particle acceleration mechanisms heretofore never seen or imagined. But as we outline in this Letter of Interest, there are also good arguments for super-heavy dark matter (SHDM) in a parameter range such that it could be discovered via its decays to, in particular, UHE photons. Only ultra-high energy cosmic ray observatories have capabilities to detect UHE photons. We first investigate how current and future observations can probe and constrain SHDM models in important directions, and then outline some of the scenarios that motivate such searches. We also discuss connections between constraints on SHDM and on the parameter values of cosmological models., SNOWMASS 2021 LoI. Accepted for publication in Astroparticle Physics

Published
2021
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17. Galaxy rotation curves disfavor traditional and self-interacting dark matter halos, preferring a disk component or Einasto function

Author

Glennys R. Farrar and Nicolas Loizeau

Subjects
Physics, Gravity (chemistry), Self-interacting dark matter, Dark matter, FOS: Physical sciences, Astronomy and Astrophysics, Function (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Modified Newtonian dynamics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo, Galaxy rotation curve, Astrophysics::Galaxy Astrophysics
Abstract

We use the galaxy rotation curves in the SPARC database to compare 9 different dark matter and modified gravity models on an equal footing, paying special attention to the stellar mass-to-light ratios. We compare three non-interacting dark matter models, a self interacting DM (SIDM) model, two hadronically interacting DM (HIDM) models, and three modified Newtonian dynamics type models: MOND, Radial Acceleration Relation (RAR) and a maximal-disk model. The models with DM-gas interactions generate a disky component in the dark matter, which significantly improves the fits to the rotation curves compared to all other models except an Einasto halo; the MOND-type models give significantly worse fits., We fixed a typo in eq A3, added fig 6 and updated fig 1 and fig 8 with two galaxy subsets of high and low inclinations

Published
2021

18. The Imprint of Large Scale Structure on the Ultra-High-Energy Cosmic Ray Sky

Author

Noemie Globus, Chen Ding, and Glennys R. Farrar

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Pierre Auger Observatory, Physics, Horizon, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Dipole anisotropy, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Universe, Magnetic field, Space and Planetary Science, Sky, Scale structure, Ultra-high-energy cosmic ray, Ultrahigh energy, Anisotropy, Astrophysics - High Energy Astrophysical Phenomena, media_common
Abstract

Ultra-high-energy cosmic rays (UHECRs) are atomic nuclei from space with vastly higher energies than any other particles ever observed. Their origin and chemical composition remain a mystery. As we show here, the large- and intermediate-angular-scale anisotropies observed by the Pierre Auger Observatory are a powerful tool for understanding the origin of UHECRs. Without specifying any particular production mechanism, but only postulating that the source distribution follows the matter distribution of the local Universe, a good accounting of the magnitude, direction and energy dependence of the dipole anisotropy at energies above $8 \times 10^{18}$ eV is obtained, after taking into account the impact of energy losses during propagation (the "GZK horizon"), diffusion in extragalactic magnetic field and deflections in the Galactic magnetic field (GMF). This is a major step toward the long-standing hope of using UHECR anisotropies to constrain UHECR composition and magnetic fields. The observed dipole anisotropy is incompatible with a pure proton composition in this scenario. With a more accurate treatment of energy losses, it should be possible to further constrain the cosmic-ray composition and properties of the extragalactic magnetic field, self-consistently improve the GMF model, and potentially expose individual UHECR sources., Accepted by the Astrophysical Journal Letters

Published
2021

19. Thermal production of sexaquarks in heavy-ion collisions

Author

Sonia Kabana, Ukraine, Coimbra, Larissa Bravina, Xiaoming Zhang, S. V. Kuleshov, Dubna, Hubei, Arkadiy Taranenko, Kyiv, Metrologichna str. B, Portugal, Casilla D, Oleksii Ivanytskyi, Max Born Pl. . Wroclaw, David Blaschke, Jinr Dubna, Avenida Republica, Santiago, Arica, V. V. Sagun, N Oslo, Chile, Moscow, Kashirskoe Shosse, CFisUC, Joliot-Curie Str., Ru Moscow, O. V. Vitiuk, Avenida España, B. E. Grinyuk, Glennys R. Farrar, Irina Potashnikova, Daicui Zhou, Pob Blindern, Poland, Departamento de Física, Lepton key Lab., Evgeny Zabrodin, Norway, Kyrill A. Bugaev, and Wuhan

Subjects
Physics, Quark, Nuclear and High Energy Physics, Work (thermodynamics), Particle physics, Large Hadron Collider, Age of the universe, Nuclear Theory, Hadron, Dark matter, High Energy Physics::Phenomenology, FOS: Physical sciences, Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Nuclear Theory (nucl-th), Neutron star, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Thermal, High Energy Physics::Experiment, Nuclear Experiment
Abstract

We present new results on the thermal production yield of a hypothetical state made of six quarks $uuddss$ assuming its production in heavy-ion collisions at the CERN LHC. A state with this quark content and mass low enough to be stable against decay in timescales of the order of the age of the Universe, has been hypothesized by one of us (G.F.) and has been discussed as a possible dark matter candidate. In this work we address for the first time the thermal production rate that can be expected for this state in heavy-ion collisions at colliders. For this estimate we use a thermal model which has been shown to describe accurately the production of hadrons and nuclei in heavy-ion collisions at LHC energy. This estimate is of great relevance for sexaquark searches at colliders as well as for its consideration as a dark matter candidate and for the composition of neutron stars., Comment: 11 pages, 2 figures

Published
2021
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20. Comment on 'Calorimetric Dark Matter Detection with Galactic Center Gas Clouds'

Author

Digvijay Wadekar, Glennys R. Farrar, Naomi McClure-Griffiths, and F. J. Lockman

Subjects
Physics, Radiative cooling, Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Galactic Center, Dark matter, General Physics and Astronomy, Astrophysics, 01 natural sciences, 0103 physical sciences, Heat transfer, Outflow, 010306 general physics, Astrophysics::Galaxy Astrophysics
Abstract

The paper "Calorimetric Dark Matter Detection with Galactic Center Gas Clouds" (Bhoonah et al. 2018) aims to derive limits on dark matter interactions by demanding that heat transfer due to DM interactions is less than that by astrophysical cooling, using clouds in the hot, high-velocity nuclear outflow wind of the Milky Way ($T_{wind} \sim 10^{6-7}$ K, $V_{wind} \sim$ 330 km/s). We argue that clouds in such an extreme environment cannot be assumed to be stable over the long timescales associated with their radiative cooling rates. Furthermore, Bhoonah et al. (2018) uses incorrect parameters for their clouds.

Published
2020
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21. New physics searches with heavy-ion collisions at the CERN Large Hadron Collider

Author

Andrea Giammanco, Jan Heisig, David D'Enterria, John Jowett, Arttu Rajantie, Lucian Harland-Lang, Michele Lucente, Sonia Kabana, Jeremi Niedziela, Swagata Mukherjee, Guilherme Milhano, Roderik Bruce, Albert De Roeck, Marco Drewes, Glennys R. Farrar, Georgios Krintiras, Michael Korsmeier, V. A. Okorokov, Jan Hajer, Oliver Gould, Michaela Schaumann, Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), and Helsinki Institute of Physics

Subjects
Photon, heavy ion: scattering, Physics beyond the Standard Model, Hadron, Nuclear Theory, magnetic monopole, nucl-ex, 01 natural sciences, nucleon nucleon, new interaction, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Nuclear Experiment, heavy ions, quark gluon: plasma, Physics, Large Hadron Collider, new physics: search for, photon, quantum electrodynamics: noncommutative, hep-ph, Nuclear & Particles Physics, Pseudoscalar, 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics, LHC, beyond standard model, Nuclear and High Energy Physics, Particle physics, p p: scattering, interpretation of experiments: CERN LHC Coll, nucl-th, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], Dark matter, Magnetic monopole, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 114 Physical sciences, dark matter, 0103 physical sciences, ddc:530, 010306 general physics, peripheral, pseudoscalar, 010308 nuclear & particles physics, hep-ex, High Energy Physics::Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Quark–gluon plasma, nonlinear, particle: long-lived, new particle
Abstract

Journal of physics / G 47(6), 060501 (2020). doi:10.1088/1361-6471/ab7ff7, Published by IOP Publ., Bristol

Published
2020
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22. Progress towards characterizing ultrahigh energy cosmic ray sources

Author

Marco Stein Muzio, Michael Unger, and Glennys R. Farrar

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Pierre Auger Observatory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, Cosmic ray, Astrophysics, 01 natural sciences, Galaxy, Redshift, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Photodisintegration, Observatory, 0103 physical sciences, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use a multimessenger approach to constrain realistic mixed composition models of ultrahigh energy cosmic ray sources using the latest cosmic ray, neutrino, and gamma-ray data. We build on the successful Unger-Farrar-Anchordoqui 2015 (UFA15) model which explains the shape of the spectrum and its complex composition evolution via photodisintegration of accelerated nuclei in the photon field surrounding the source. We explore the constraints which can currently be placed on the redshift evolution of sources and the temperature of the photon field surrounding the sources. We show that a good fit is obtained to all data either with a source which accelerates a narrow range of nuclear masses or a Milky Way-like mix of nuclear compositions, but in the latter case the nearest source should be 30-50 Mpc away from the Milky Way in order to fit observations from the Pierre Auger Observatory. We also ask whether the data allow for a subdominant purely protonic component at UHE in addition to the primary UFA15 mixed composition component. We find that such a two-component model can significantly improve the fit to cosmic ray data while being compatible with current multimessenger data., Comment: Fixed 26% normalization error, conclusions remain unchanged

Published
2019
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23. On the origin of ultra-high energy cosmic ray anisotropy

Author

Glennys R. Farrar, Chen Ding, and Noemie Globus

Subjects
Physics, Dipole, Astrophysics::High Energy Astrophysical Phenomena, Quadrupole, Dipole anisotropy, Cosmic ray, Astrophysics, Cosmic variance, Ultra-high-energy cosmic ray, Anisotropy, Coherence length
Abstract

We show that the observed anisotropy of extragalactic ultra-high energy cosmic rays (UHECRs above 8 EeV) is well-described by treating sources as a continuous distribution following the local large-scale structure of matter (LSS). We assume homogeneous, rigidity-dependent diffusion in the extragalactic magnetic field (EGMF), taking its strength and coherence length as free parameters. We use high-resolution particle tracking ($\sim 1.8 \times 10^9$ trajectories) to treat the impact of the Galactic magnetic field (GMF), for rigidities (E/Z) from $10^{17.4}$--$10^{20}$ EV. We adopt the Jansson and Farrar (2012) model for the GMF, and consider values of the coherence length of the random component from 30--100 pc. We describe the composition and spectrum of UHECRs using both direct fits from Auger (2017) and the physically-based Muzio, Unger, Farrar (2019) model, and assess the impact of UHECR spectrum and composition uncertainties on predicted arrival direction anisotropies. Our model accounts for the magnitude and direction of the dipole anisotropy in the $>8$ EeV bin, as well as its evolution (in both magnitude and direction) in the 8-16, 16-32 and $>32$ EeV bins (although the dipole is not significant above 32 EeV due to the lack of statistics). The quadrupole is also in agreement with data. Our best fit parameters are $B_{\rm EGMF}\sim0.6$ nG, $\lambda_{\rm EGMF}\sim0.2$ Mpc and $\lambda_{\rm GMF}\sim75$ pc. We show that this result is robust against different dipole reconstruction methods (Rayleigh/K-inverse) and different hadronic interaction models (EPOS-LHC/Sybill 2.3). We note that in an alternative scenario where the dipole would be due to a few local sources, the effect of cosmic variance would dominate over the magnetic deflection and horizon effects, and the direction and magnitude of the anisotropy could not be predicted. We also note that a pure proton composition would not explain simultaneously the strength and direction of the dipole in this model.

Published
2019
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24. Constraints on UHECR sources and their environments, from fitting UHECR spectrum and composition, and neutrinos and gammas

Author

Glennys R. Farrar, Michael Unger, and Marco Stein Muzio

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Spectrum (functional analysis), Hadron, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astrophysics, Limiting, Neutrino, Event (particle physics), Auger
Abstract

We perform high-precision joint fitting of the ensemble of Auger extragalactic spectrum, composition, IceCube neutrino spectrum and upper limits, and Fermi-LAT diffuse gamma spectrum, to constrain the properties of UHECR sources, the source environments, source evolution and distance to nearest source. At present, the largest source of uncertainty comes from the LHC-tuned hadronic event generators, limiting the ability to derive decisive conclusions on all of the above topics. Nonetheless, interesting constraints on UHECR, neutrino and gamma ray sources can (and will) be presented.

Published
2019
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25. Developments in Modeling the Galactic Magnetic Field

Author

Michael Unger and Glennys R. Farrar

Subjects
Physics, Electron density, Random field, Astrophysics::High Energy Astrophysical Phenomena, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, CMB cold spot, Galaxy, Coherence length, Magnetic field, symbols.namesake, symbols, Planck, Astrophysics::Galaxy Astrophysics
Abstract

We present an improved 3D model of the strength and structure of the Galactic random field. The analysis uses the synchrotron intensity as measured by Planck, WMAP and Haslam et al. and the observed fluctuations of the rotation measures of extragalactic radio sources. As part of this modeling effort, we improve the separation of the various components of Galactic emission, the determination of the 3D cosmic ray electron density and spectrum, and the thermal electron distribution. This combined information allows us to constrain both the strength and coherence length of the random field. We also report developments in modeling the large scale coherent field of the Galaxy.

Published
2019
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26. Gas-rich dwarf galaxies as a new probe of dark matter interactions with ordinary matter

Author

Glennys R. Farrar and Digvijay Wadekar

Subjects
Physics, Photon, Radiative cooling, 010308 nuclear & particles physics, Scattering, Physics beyond the Standard Model, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Absorption (logic), Anomaly (physics), 010306 general physics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy
Abstract

We use observations of gas-rich dwarf galaxies to derive constraints on dark matter scattering with ordinary matter. We require that heating/cooling due to DM interacting with gas in the Leo T dwarf galaxy not exceed the ultra-low radiative cooling rate of the gas. This enables us to set $(i)$ stronger bounds than all the previous literature on ultra-light hidden photon DM for nearly all of the mass range $10^{-23}\lesssim m_\mathrm{DM} \lesssim 10^{-10}$ eV, $(ii)$ limits on sub-GeV millicharged DM which add to the constraints on the recent EDGES 21cm absorption anomaly, and $(iii)$ constraints on DM-baryon interactions directly at low relative velocities $v_\mathrm{rel}\sim 17$ km/s. Our study opens a new direction at using observations of gas-rich dwarf galaxies from previous, current and upcoming optical and 21cm surveys to probe physics beyond the standard model., 5+10 pages, 4+6 figures. Version appearing in PRD. Title and abstract revised to reflect the primary message of the paper. Minor changes to figures, conclusions unchanged. The code associated with this paper is available at https://github.com/JayWadekar/Gas_rich_dwarfs

Published
2019

27. Progress in the Global Modeling of the Galactic Magnetic Field

Author

Glennys R. Farrar and Michael Unger

Subjects
Astrophysics::High Energy Astrophysical Phenomena, QC1-999, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rotation, 01 natural sciences, symbols.namesake, 0103 physical sciences, ddc:530, Planck, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, CMB cold spot, Astrophysics - Astrophysics of Galaxies, Galaxy, Magnetic field, Synchrotron emission, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), symbols, Global modeling, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We discuss the global modeling of the properties of the Galactic Magnetic Field (GMF). Several improvements and variations of the model of the GMF from Jansson & Farrar (2012) (JF12) are investigated in an analysis constrained by all-sky rotation measures of extragalactic sources and polarized and unpolarized synchrotron emission data from WMAP and Planck. We present the impact of the investigated model variations on the propagation of ultrahigh-energy cosmic rays in the Galaxy., To appear in the proceedings of UHECR18

Published
2019

28. Constraints on Dark Matter with a moderately large and velocity-dependent DM-nucleon cross-section

Author

M. Shafi Mahdawi and Glennys R. Farrar

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, Lattice (group), FOS: Physical sciences, Electron, 01 natural sciences, Asymmetry, High Energy Physics - Experiment, Nuclear physics, Cross section (physics), High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Range (particle radiation), 010308 nuclear & particles physics, Astronomy and Astrophysics, High Energy Physics - Phenomenology, Anomaly (physics), Nucleon, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We derive constraints on a possible velocity-dependent DM-nucleon scattering cross section, for Dark Matter in the 10 MeV -- 100 GeV mass range, using the XQC, DAMIC, and CRESST 2017 Surface Run experiments. We report the limits on cross sections of the form $\sigma=\sigma_0\,v^n$, for a range of velocity dependencies with $n\in\{-4,-2,-1,0,1,2\}$. We point out the need to measure the efficiency with which nuclear recoil energy in the sub-keV range thermalizes, rather than being stored as Frenkel pairs in the semi-conductor lattice. The possibility of a significant inefficiency leaves open a considerable `hole' in the limits for mass in the $\sim$ 0.2 -- 2 GeV range, which XQC and CRESST can potentially fill when the thermalization efficiency is measured. We call attention to the asymmetry between a conventional lower limit cross section and the `upper-reach cross section' imposed by attenuation in an overburden -- an upper boundary being extremely sharp but quite insensitive to the statistics of the experiment. Considering the recent interest to use dark matter-baryon interaction with velocity dependence $n=-4$ to explain the EDGES 21 cm anomaly, we also derive the limits on milli-charged DM that scatters off protons and electrons under a Coulomb-like interaction. We find that much but not all of the region of interest for the EDGES anomaly can be excluded., Comment: 34 pages, 9 figures, 5 tables. v3: Matches version accepted to JCAP

Published
2018
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29. Magnetic deflections of ultra-high energy cosmic rays from Centaurus A

Author

Glennys R. Farrar, Azadeh Keivani, and Michael Sutherland

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Pierre Auger Observatory, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Centaurus A, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics, 01 natural sciences, Magnetic field, symbols.namesake, Rigidity (electromagnetism), 0103 physical sciences, Faraday effect, symbols, Substructure, Ultra-high-energy cosmic ray, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

We present the results of a study that simulates trajectories of ultra-high energy cosmic rays from Centaurus A to Earth, for particle rigidities from $E/Z = 2$ EV to 100 EV, i.e., covering the possibility of primary particles as heavy as Fe nuclei with energies exceeding 50 EeV. The Galactic magnetic field is modeled using the recent work of Jansson and Farrar (JF12) which fitted its parameters to match extragalactic Faraday rotation measures and WMAP7 synchrotron emission maps. We include the random component of the GMF using the JF12 3D model for $B_{\rm rand}(\vec{r})$ and explore the impact of different random realizations, coherence length and other features on cosmic ray deflections. Gross aspects of the arrival direction distribution such as mean deflection and the RMS dispersion depend mainly on rigidity and differ relatively little from one realization to another. However different realizations exhibit non-trivial substructure whose specific features vary considerably from one realization to another, especially for lower rigidities. At the lowest rigidity of 2 EV, the distribution is broad enough that it might be compatible with a scenario in which Cen A is the principle source of all UHECRs. No attempt is made here to formulate a robust test of this possibility, although some challenges to such a scenario are noted., 20 pages, 9 figures, 1 table; submitted to Astroparticle Physics

Published
2015
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30. 6-quark Dark Matter: viable + explains many observations

Author

Glennys R. Farrar

Subjects
Physics, Quark, Quantum chromodynamics, Big Bang nucleosynthesis, Dark matter, Scalar (mathematics), Hadron, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy rotation curve, Galaxy
Abstract

It is proposed that the relatively inert, highly symmetric, flavor singlet scalar hadron made of $uuddss$ quarks may have a mass $< 2 (m_p + m_e)$. This is consistent with QCD theory, and with existing accelerator and non-accelerator constraints. For mass in the 1.5-1.8 GeV range, the observed DM relic abundance and the observed DM to ordinary matter (OM) ratio are naturally explained. It freezes out before primordial nucleosynthesis and does not significantly impact primordial abundances, so the conventional argument that DM is non-baryonic does not apply. The interaction cross section between DM and the gas in the Galaxy is such that the dark matter in our local neighborhood is naturally co-rotating with the solar system, to a sufficient degree that DM does not have enough energy to be detected in XQC, the most sensitive DM experiment in this scenario. Its interaction with the gas in galactic disks provides the first (non-Mondian) explanation for the striking correlation in the small-scale structure of rotation curves and the inhomogeneous distribution of gas, and explains why most but not all galaxies exhibit such correlations. It naturally produces a dark matter disk as suggested by recent studies, and removes the inconsistencies of LCDM which motivated the idea of self-interacting DM (SIDM). Lab experiments to discover this particle are discussed.

Published
2017
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31. Detailed simulations of Fermi-LAT constraints on UHECR production scenarios

Author

Michael Unger, Marco Stein Muzio, and Glennys R. Farrar

Subjects
Physics, Extragalactic background light, Position (vector), Cascade, Photodisintegration, Flux, ddc:530, Production (computer science), Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

We have performed high-resolution simulations of the flux and spectrum of gammas detectable by Fermi-LAT, coming from UHECR-induced cascades, using the state-of-the-art (Gilmore) model of extragalactic background light, ELMAG to simulate the EM cascade (modified to work correctly for the Gilmore EBL) and CRPropa3 to simulate the production of EM secondaries from UHECR propagation. We examine the validity and limitations of the Liu et al. (2016) constraints, which found that we live in a local UHECR over-density. We also examine whether a model such as that of Unger, Farrar, and Anchordoqui (2015) -- which explains the full extragalactic CR spectrum and composition including the ankle, based on nuclear photodisintegration in the neighborhood surrounding the source -- satisfies the Fermi-LAT constraints, or requires Earth to be in an atypical position in the Universe as claimed by Liu et al. for pure proton primaries. We conclude that a mixed-composition scenario, like that of Unger, Farrar, and Anchordoqui, satisfies Fermi-LAT constraints evading any need for Earth to be in an atypical position in the Universe.

Published
2017
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32. Uncertainties in the Magnetic Field of the Milky Way

Author

Glennys R. Farrar and Michael Unger

Subjects
Field (physics), Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Measure (physics), FOS: Physical sciences, Astrophysics, Electron, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, symbols.namesake, law, 0103 physical sciences, Planck, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, CMB cold spot, Astrophysics - Astrophysics of Galaxies, Synchrotron, Magnetic field, Astrophysics of Galaxies (astro-ph.GA), symbols, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We improve on the model of the Galactic Magnetic Field (GMF) from Jansson \& Farrar (2012), which was constrained using all-sky rotation measures of extragalactic sources and polarized and unpolarized synchrotron emission data from WMAP. We have developed several alternative functional forms for the coherent and random components, used newer synchrotron products from Planck and WMAP and testes new models of the densities of thermal electrons and cosmic-ray electrons. The differences in the resultant GMF models, depending on which parameterization of the field, synchrotron product and electron densities are used, provides a measure of the uncertainty in our inference of the GMF. We discuss the impact of these uncertainties on charged-particle astronomy at ultra-high energies., 8 pages, 2 figures, to appear in the Proceedings of the 35th International Cosmic Ray Conference 10-20 July, 2017 Bexco, Busan, Korea

Published
2017

33. Deflections of UHECRs in the Galactic magnetic field

Author

Glennys R. Farrar and Michael Sutherland

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Random field, Isotropy, Galactic Center, FOS: Physical sciences, Centroid, Dipole anisotropy, Astronomy and Astrophysics, Celestial sphere, Coherence length, Magnetic field, Computational physics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report results of the first comprehensive, high resolution study of the deflections of UHECRs using a realistic model of the Galactic magnetic field and extending to sufficiently low rigidities, R = E/Z = 10^18 V, to describe Fe in the UHE energy range or the mixed composition reported by the Pierre Auger Collaboration at the energy of the observed dipole anisotropy. We use the Jansson-Farrar (JF12) model, which has both large scale coherent and a structured random components, and determine deflections for fifteen rigidities from 10^18.0 to 10^20.0 V, for L_coh = 30 pc and 100 pc. We check the sensitivity of UHECR deflections to the particular realization of the random field, for 3 rigidity values. For each rigidity and field model studied, the UHECR arrival direction distribution is determined for an arbitrary source direction, by inverting the trajectories of > 5 x 10^7 isotropic anti-CRs of the given rigidity. We present skyplots and tables characterizing the arrival directions, for representative 1 deg sources. Except at high rigidity, the pattern of multiple images is very complex and depends strongly on the coherence length and source direction. For almost all sources, average deflections grow rapidly as the rigidity falls below 10 EV and deflections commonly are greater than 90 deg. Magnification and demagnification can be strong at almost all rigidities, and varies significantly with source direction. Much of the extragalactic celestial sphere, behind and south of the Galactic Center, cannot be seen in UHECRs below 10 EV. The pattern of deflections obtained with the coherent field alone can be significantly different than with the complete field model, even as regards the position of the centroid, for some source directions and rigidities. Multiple images, sometimes very widely separated, are common for small coherence length, especially for low rigidity., 53 pp, many figures. Figures have been compressed to reduce file size; uncompressed figures available on request

Published
2019
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34. Evidence for a mixed mass composition at the 'ankle' in the cosmic-ray spectrum

Author

S. Stanič, Denis Stanca, J. A.J. Matthews, Xavier Bertou, M. L. Díaz Castro, C. Porowski, Jakub Vicha, Francesca Zuccarello, Pedro Assis, R. Sato, Jose Chinellato, I. Jandt, Hermann-Josef Mathes, M. Ziolkowski, Denise Boncioli, Markus Risse, Muller, F. Canfora, J. Blazek, A. Tonachini, Antonio Bueno, M. Josebachuili, J.D. Sanabria Gomez, Eric Mayotte, A. C. Rovero, J. Biteau, P.F. Gómez Vitale, G. A. Anastasi, Kai Daumiller, Alberto Filevich, Peter Hansen, John Matthews, Christian Sarmiento-Cano, Gualberto Avila, W. Rodrigues de Carvalho, Marco Torri, Nicolás González, M. Gómez Berisso, R. C. Shellard, Leigui de Oliveira, Paul M. Mantsch, Diego Ravignani, J. R. Vázquez, P. Sanchez-Lucas, S. Vorobiov, Ingomar Allekotte, F. Sánchez, J. W. Cronin, Lorenzo Cazon, Peter Buchholz, R. Piegaia, I. Al Samarai, Ivo Nicolas Naranjo, Antonio Insolia, A. Aab, L. Caramete, Alina Mihaela Badescu, P. Heimann, Anderson Fauth, M. Zavrtanik, G. Marsella, R. Ramos-Pollant, Valerio Pirronello, G. Torralba Elipe, O. Ravel, P. van Bodegom, Angela V. Olinto, C. Di Giulio, S. Navas, I.M. Brancus, H. Glass, Marco Aglietta, Johannes Schumacher, Joshua A. Gordon, Bruno Daniel, Corinne Berat, R. Krause, Gaia Silli, A. Filipčič, Foteini Oikonomou, G. S. Varner, Alessio Gorgi, Fred Sarazin, H. Gemmeke, Lukas Nellen, M. I. Micheletti, L. A. S. Pereira, Maria Giller, J. J. Masías Meza, C. J. Todero Peixoto, A.E. Herve, Octavian Sima, Nataliia Borodai, D. Mockler, Manuel Platino, E.M. Holt, B. Wundheiler, A. Fuster, Q. Hasankiadeh, A. Saleh, Jeffrey Brack, J. F. Valdés Galicia, Olaf Scholten, Ioana Codrina Maris, I. De Mitri, Dieter Heck, Martin Urban, Hans Klages, H. Nožka, A. Chiavassa, Maria-Teresa Dova, M. R. Hampel, O. A. Taborda, Carlos Hojvat, Miroslav Palatka, A. Menshikov, Diego Harari, B. Gookin, S. Müller, Carola Dobrigkeit, M. Schauer, Humberto Ibarguen Salazar, Ricardo Vázquez, Antoine Letessier-Selvon, Ernesto Kemp, R. Legumina, P. H. Nguyen, Lawrence Wiencke, B. Sarkar, Sarka Wykes, C. Morello, E. M. Santos, G. Kukec Mezek, L. Molina-Bueno, M. Plum, Z. Zong, David Walz, Harald Schieler, O. Kambeitz, Jeffrey A. Johnsen, Sven Querchfeld, L. Perrone, Marco Giammarchi, Bruce R. Dawson, S. Quinn, Christian Glaser, J. Espadanal, Octavian Fratu, M. E. Bertaina, Alan Watson, Mihai Niculescu-Oglinzanu, Jonny Kleinfeller, Sergio Sciutto, L. Ochilo, M. Mallamaci, Alberto Segreto, Nicusor Arsene, D. Rogozin, J. de Oliveira, R.R. Prado, Alejandro Almela, P. Billoir, Tim Huege, Ana Martina Botti, Belén Andrada, J. Alvarez Castillo, G. C. Hill, R.C. dos Anjos, Lukas Middendorf, D. Pakk Selmi-Dei, F. Diogo, G. De Mauro, Henryk Wilczyński, Ralph Engel, J. J. Beatty, Norbert Kunka, D. Nitz, Günter Sigl, Silvia Mollerach, A. Śmiałkowski, Jörg R. Hörandel, Sutherland, Julian Rautenberg, Peter L. Biermann, F. Montanet, L. Niemietz, R. M. de Almeida, L. Tomankova, Christine Peters, Radomir Smida, Alberto Etchegoyen, John L. Harton, Peter Gorham, T. Paul, Paolo Privitera, Federico Suarez, A. Schulz, D. Reinert, A. López Casado, G. Matthiae, Andreas Weindl, D. Garcia-Pinto, Paul Sommers, Petr Schovanek, A. Di Matteo, Charles Timmermans, Luis A. Nunez, A. Blanco, P. Gouffon, N. Krohm, D. Torres Machado, L. Collica, P. Abreu, Brian Fick, Zbigniew Szadkowski, Alberto Daniel Supanitsky, D. Melo, Julien Aublin, A. Shadkam, M. J. Cooper, Miguel Mostafá, Mário Pimenta, Gregory R Snow, Pablo Ristori, Miroslav Pech, P. H. Kasper, Carlos Medina, M. Settimo, R. Ulrich, Rodrigo Pelayo, Stijn Buitink, E. Varela, D. Yelos, Andrej Dundovic, Marcus Niechciol, D. Martello, Luis A. Anchordoqui, Pavel Horvath, Danilo Zavrtanik, Lorenzo Caccianiga, V. M. Theodoro, Paula Gina Isar, F. Salesa Greus, G. Cataldi, Florian Gaté, Michael Unger, S. Jansen, Gero Müller, P. W. Younk, Sofia Andringa, Eun-Joo Ahn, P. Lautridou, C. Scarso, Elton J. G. Santos, Jiri Chudoba, Markus Roth, G. van Aar, Dusan Mandat, Q. Luce, V. de Souza, Alex Kääpä, Maria Rita Coluccia, A. van Vliet, Tanguy Pierog, R. Cester, Gustavo Medina-Tanco, Miroslav Hrabovský, L. del Peral, Jaroslaw Stasielak, Andreas Haungs, Matthias Kleifges, V. Verzi, Philipp Papenbreer, Colin Baus, Glennys R. Farrar, David Schmidt, J. Sorokin, K. H. Becker, H. Martinez, A. G. Mariazzi, A. Kuotb Awad, S. G. Blaess, C. Aramo, Sergio Dasso, Tristan Sudholz, Fausto Guarino, Juan Pallotta, R. López, B. Tome, C. Bleve, Alexandru Balaceanu, Petr Travnicek, Rodríguez-Frías, V. Scherini, Arnulfo Zepeda, Eduardo Quel, David Wittkowski, Laura Valore, Martín Miguel Freire, Thomas Harrison, Benoît Revenu, Germano Guedes, Danielle LaHurd, Olivier Deligny, P. Pieroni, Alan Coleman, T. Hebbeker, Vincenzo Rizi, Trent D. Grubb, G. Rodriguez Fernandez, Benedikt Zimmermann, Rúben Conceição, Toshihiro Fujii, M. Ambrosio, L. Lopes, J. Debatin, O. Martínez Bravo, Dariusz Glas, Juan Manuel Figueira, F. Arqueros, Alexandra Saftoiu, Tim Niggemann, Roberta Colalillo, J. Hulsman, B. Mitrica, Hernán Asorey, Francesco Strafella, Martina Bohacova, Patrick Allison, Heino Falcke, Jaime Alvarez-Muñiz, Alexandru Gherghel-Lascu, I. Lhenry-Yvon, A. Lucero, Juan Carlos D'Olivo, O. Wainberg, A. Valbuena-Delgado, Esteban Roulet, T. Suomijärvi, Karl-Heinz Kampert, Antonella Castellina, Piera Luisa Ghia, V. Novotny, Rossella Caruso, S. Mathys, M. Erfani, John Swain, Thomas Bretz, Ruben Squartini, I. A. Minaya, Corbin Covault, Peter Mazur, J. Pȩkala, Geraldina Golup, Alexander Grillo, S. J. De Jong, Katrin Link, Lino Miramonti, Ugo Giaccari, A. Tepe, J. R. T. de Mello Neto, M. Prouza, J. Rodriguez Rojo, Bianca Keilhauer, A. G. Chavez, F.G. Schröder, Enrique Zas, Fernando Contreras, Jesús Peña-Rodríguez, A. Dorofeev, L. Villaseñor, A. Bridgeman, S. J. Saffi, Markus Lauscher, F. Pedreira, J. Phuntsok, Raul Sarmento, M. Suarez Durán, H. Wahlberg, A. Parra, G. Parente, M. Trini, Johannes Schulz, Florian Lukas Briechle, A. Cancio, B. Caccianiga, Alexey Yushkov, Max Malacari, Lili Yang, Luca Latronico, Piotr Homola, Alex Tapia, Tobias Winchen, P. Lebrun, Karen S. Caballero-Mora, Martin Erdmann, Carla Bonifazi, Beatriz García, Roger W Clay, Stefano D'Amico, Jose A. Bellido, Daniel Kuempel, S. Sonntag, Carlos Escobar, Jaime Rosado, R.M. Kieckhafer, B. Vargas Cárdenas, I. Valiño, J. Neuser, Ivone F. M. Albuquerque, Ke Fang, I. Katkov, Richard Dallier, Gaetano Salina, A.M. van den Berg, Darko Veberič, Jan Ridky, Marc Weber, M. Buscemi, D. Nosek, Jan Ebr, Sergio Petrera, S. Messina, S. Coutu, Norberto Fazzini, Aab, A., Abreu, P., Aglietta, M., Ahn, E. J., Al Samarai, I., Albuquerque, I. F. M., Allekotte, I., Allison, P., Almela, A., Alvarez Castillo, J., Alvarez Muñiz, J., Ambrosio, M., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Badescu, A. M., Balaceanu, A., Baus, C., Beatty, J. J., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Billoir, P., Biteau, J., Blaess, S. G., Blanco, A., Blazek, J., Bleve, Carla, Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Botti, A. M., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero Mora, K. S., Caccianiga, B., Caccianiga, L., Cancio, A., Canfora, F., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Cester, R., Chavez, A. G., Chiavassa, A., Chinellato, J. A., Chudoba, J., Clay, R. W., Colalillo, R., Coleman, A., Collica, L., Coluccia, MARIA RITA, Conceição, R., Contreras, F., Cooper, M. J., Coutu, S., Covault, C. E., Cronin, J., Dallier, R., D'Amico, Stefano, Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., de Jong, S. J., De Mauro, G., de Mello Neto, J. R. T., DE MITRI, Ivan, de Oliveira, J., de Souza, V., Debatin, J., del Peral, L., Deligny, O., Di Giulio, C., Di Matteo, A., Díaz Castro, M. L., Diogo, F., Dobrigkeit, C., D'Olivo, J. C., Dorofeev, A., dos Anjos, R. C., Dova, M. T., Dundovic, A., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Fang, K., Farrar, G., Fauth, A. C., Fazzini, N., Fick, B., Figueira, J. M., Filevich, A., Filipčič, A., Fratu, O., Freire, M. M., Fujii, T., Fuster, A., García, B., Garcia Pinto, D., Gaté, F., Gemmeke, H., Gherghel Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Glass, H., Golup, G., Gómez Berisso, M., Gómez Vitale, P. F., González, N., Gookin, B., Gordon, J., Gorgi, A., Gorham, P., Gouffon, P., Grillo, A. F., Grubb, T. D., Guarino, F., Guedes, G. P., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Harton, J. L., Hasankiadeh, Q., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hill, G. C., Hojvat, C., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Jandt, I., Jansen, S., Johnsen, J. A., Josebachuili, M., Kääpä, A., Kambeitz, O., Kampert, K. H., Kasper, P., Katkov, I., Keilhauer, B., Kemp, E., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Kukec Mezek, G., Kunka, N., Kuotb Awad, A., Lahurd, D., Latronico, L., Lauscher, M., Lautridou, P., Lebrun, P., Legumina, R., Leigui de Oliveira, M. A., Letessier Selvon, A., Lhenry Yvon, I., Link, K., Lopes, L., López, R., López Casado, A., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Mariş, I. C., Marsella, Giovanni, Martello, Daniele, Martinez, H., Martínez Bravo, O., Masías Meza, J. J., Mathes, H. J., Mathys, S., Matthews, J., Matthews, J. A. J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina, C., Medina Tanco, G., Melo, D., Menshikov, A., Messina, S., Micheletti, M. I., Middendorf, L., Minaya, I. A., Miramonti, L., Mitrica, B., Mockler, D., Molina Bueno, L., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Müller, G., Muller, M. A., Müller, S., Naranjo, I., Navas, S., Nellen, L., Neuser, J., Nguyen, P. H., Niculescu Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, H., Núñez, L. A., Ochilo, L., Oikonomou, F., Olinto, A., Pakk Selmi Dei, D., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pękala, J., Pelayo, R., Peña Rodriguez, J., Pereira, L. A. S., Perrone, Lorenzo, Peters, C., Petrera, S., Phuntsok, J., Piegaia, R., Pierog, T., Pieroni, P., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos Pollant, R., Rautenberg, J., Ravel, O., Ravignani, D., Reinert, D., Revenu, B., Ridky, J., Risse, M., Ristori, P., Rizi, V., Rodrigues de Carvalho, W., Rodriguez Fernandez, G., Rodriguez Rojo, J., Rodríguez Frías, M. D., Rogozin, D., Rosado, J., Roth, M., Roulet, E., Rovero, A. C., Saffi, S. J., Saftoiu, A., Salazar, H., Saleh, A., Salesa Greus, F., Salina, G., Sanabria Gomez, J. D., Sánchez, F., Sanchez Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarkar, B., Sarmento, R., Sarmiento Cano, C., Sato, R., Scarso, C., Schauer, M., Scherini, Viviana, Schieler, H., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Settimo, Mariangela, Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Śmiałkowski, A., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Sorokin, J., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Strafella, Francesco, Suarez, F., Suarez Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Sutherland, M. S., Swain, J., Szadkowski, Z., Taborda, O. A., Tapia, A., Tepe, A., Theodoro, V. M., Timmermans, C., Todero Peixoto, C. J., Tomankova, L., Tomé, B., Tonachini, A., Torralba Elipe, G., Torres Machado, D., Torri, M., Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Valbuena Delgado, A., Valdés Galicia, J. F., Valiño, I., Valore, L., van Aar, G., van Bodegom, P., van den Berg, A. M., van Vliet, A., Varela, E., Vargas Cárdenas, B., Varner, G., Vázquez, J. R., Vázquez, R. A., Veberič, D., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczyński, H., Winchen, T., Wittkowski, D., Wundheiler, B., Wykes, S., Yang, L., Yelos, D., Younk, P., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Bleve, C., Colalillo, Roberta, Coluccia, M. R., D'Amico, S., De Mitri, I., Guarino, Fausto, Marsella, G., Martello, D., Pȩkala, J., Perrone, L., Scherini, V., Settimo, M., Strafella, F., Valore, Laura, Physics, Astronomy and Astrophysics Research Group, Elementary Particle Physics, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), and Pierre Auger Collaboration

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Nuclear and High Energy Physics, Proton, Pierre Auger Observatory, Cosmic Rays, Mass Composition, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Cosmic ray, Ankle, Cosmic rays, Mass composition, Astrophysics, 01 natural sciences, Auger, Observatory, 0103 physical sciences, ddc:530, High Energy Physics, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Cherenkov radiation, Ciencias Exactas, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Range (particle radiation), 010308 nuclear & particles physics, OBSERVATÓRIOS, Astrophysics::Instrumentation and Methods for Astrophysics, Física, lcsh:QC1-999, Physique atomique et nucléaire, Experimental High Energy Physics, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, lcsh:Physics
Abstract

We report a first measurement for ultrahigh energy cosmic rays of the correlation between the depth of shower maximum and the signal in the water Cherenkov stations of air-showers registered simultaneously by the fluorescence and the surface detectors of the Pierre Auger Observatory. Such a correlation measurement is a unique feature of a hybrid air-shower observatory with sensitivity to both the electromagnetic and muonic components. It allows an accurate determination of the spread of primary masses in the cosmic-ray flux. Up till now, constraints on the spread of primary masses have been dominated by systematic uncertainties. The present correlation measurement is not affected by systematics in the measurement of the depth of shower maximum or the signal in the water Cherenkov stations. The analysis relies on general characteristics of air showers and is thus robust also with respect to uncertainties in hadronic event generators. The observed correlation in the energy range around the ‘ankle’ at lg⁡(E/eV)=18.5–19.0 differs significantly from expectations for pure primary cosmic-ray compositions. A light composition made up of proton and helium only is equally inconsistent with observations. The data are explained well by a mixed composition including nuclei with mass A>4. Scenarios such as the proton dip model, with almost pure compositions, are thus disfavored as the sole explanation of the ultrahigh-energy cosmic-ray flux at Earth., 0, SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2016
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35. A Uniformly Selected, All-Sky Optical AGN Catalog for UHECR Correlation

Author

Glennys R. Farrar, Yanping Chen, and Ingyin Zaw

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, law.invention, Telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Redshift survey, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Optical spectra, Sky, Astrophysics of Galaxies (astro-ph.GA), Magnitude (astronomy), Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Studies discerning whether there is a significant correlation between UHECR arrival directions and optical AGN are hampered by the lack of a uniformly selected and complete all-sky optical AGN catalog. To remedy this, we are preparing such a catalog based on the 2MASS Redshift Survey (2MRS), a spectroscopic sample of $\sim 44,500$ galaxies complete to a K magnitude of 11.75 over 91% of the sky. We have analyzed the available optical spectra of these 2MRS galaxies ($\sim 80$% of the galaxies), in order to identify the AGN amongst them with uniform criteria. We present a first-stage release of the AGN catalog for the southern sky, based on spectra from the 6dF Galaxy survey and CTIO telescope. Providing a comparably uniform and complete catalog for the northern sky is more challenging because the spectra for the northern galaxies were taken with different instruments., 8 pages, 5 figures, Proceedings of The 34th International Cosmic Ray Conference

Published
2016
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37. Workshop on Stellar Tidal Disruption

Author

Glennys R. Farrar

Subjects
Swift, Physics, Spectral signature, Astrophysics::High Energy Astrophysical Phenomena, White dwarf, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Luminosity, law.invention, Black hole, Neutron star, Space and Planetary Science, law, Astrophysics::Solar and Stellar Astrophysics, Blazar, computer, Astrophysics::Galaxy Astrophysics, computer.programming_language, Flare
Abstract

The past year has seen major advances in the observational status of Stellar Tidal Disruption, with the discovery of two strong optical candidates in archived SDSS data and the real-time X-ray detection of Swift J1644+57, plus rapid radio and optical follow-up establishing it as a probable Tidal Disruption Flare (TDF) in “blazar mode”. These observations motivated a workshop devoted to discussion of such events and of the theory of their emission and flare rate. Observational contributions included a presentation of Swift J2058+05 (a possible second example of a TDF in blazar mode), reports on the late-time evolution and X-ray variability of the two Swift events, and a proposal that additional candidates may be evidenced by spectral signatures in SDSS. Theory presentations included models of radio emission, theory of light curves and the proposal that GRB101225A may be the Galactic tidal disruption of a neutron star, an interpretation of Swift J1644+57 as due to the disruption of a white dwarf instead of main-sequence star, calculation of the dependence of the TDF rate on the spin of the black hole, and analysis of the SDSS events, fitting their SEDs to profiles of thoretical emission from accretion disks and showing that their luminosity and rate are consistent with the proposal that TDEs can be responsible for UHECR acceleration.

Published
2011
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38. A Uniformly Selected, All-sky, Optical AGN Catalog

Author

Ingyin Zaw, Yanping Chen, and Glennys R. Farrar

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Continuum (design consultancy), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, 0103 physical sciences, Emission spectrum, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Line (formation), Physics, Astronomy and Astrophysics, Redshift survey, Astrophysics - Astrophysics of Galaxies, Universe, Galaxy, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA)
Abstract

We have constructed an all-sky catalog of optical AGNs with $z < 0.09$, based on optical spectroscopy, from the parent sample of galaxies in the 2MASS Redshift Survey (2MRS), a near-complete census of the nearby universe. Our catalog consists of 1929 broad line AGNs, and 6562 narrow line AGNs which satisfy the \citet{Kauffmann03} criteria, of which 3607 also satisfy the \citet{Kewley01} criteria. We also report emission line widths, fluxes, flux errors, and signal-to-noise ratios of all the galaxies in our spectroscopic sample, allowing users to customize the selection criteria. Although we uniformly processed the spectra of galaxies from a homogeneous parent sample, inhomogeneities persist due to the differences in the quality of the obtained spectra, taken with different instruments, and the unavailability of spectra for $\sim$20\% of the galaxies. We quantify how the differences in spectral quality affect not only the AGN detection rates but also broad line to narrow line AGN ratios. We find that the inhomogeneities primarily stem from the continuum signal-to-noise (S/N) in the spectra near the emission lines of interest. We fit for the AGN fraction as a function of continuum S/N and assign AGN likelihoods to galaxies which were not identified as AGNs using the available spectra. This correction results in a catalog suitable for statistical studies. This work also paves the way for a truly homogeneous and complete nearby AGN catalog by identifying galaxies whose AGN status needs to be verified with higher quality spectra, quantifying the spectral quality necessary to do so., 30 pages, 24 figures, 5 tables

Published
2019
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39. Testing the correlations between ultrahigh energy cosmic rays and the Veron-Cetty and Veron catalogue of quasars and active galactic nuclei

Author

Andreas A. Berlind, I. Zaw, and Glennys R. Farrar

Subjects
Physics, Pierre Auger Observatory, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Quasar, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Auger, Space and Planetary Science, Ultrahigh energy, Spectral line ratios, Astrophysics::Galaxy Astrophysics
Abstract

We investigate several aspects of the correlations reported by the Pierre Auger Observatory between the highest energy ultra-high energy cosmic rays (UHECRs) and galaxies in the Veron-Cetty Veron (VCV) catalogue of active galactic nuclei (AGNs). First, we quantify the extent of the inhomogeneity and impurity of the VCV catalogue. Second, we determine how the correlation between the highest energy Auger UHECRs and VCV galaxies is modified when only AGNs satisfying optical spectral line ratios, i.e. a very pure sample, are used. Finally, we measure the correlation between the published Auger UHECRs and the distribution of nearby galaxies. We find that the correlation between the arrival directions of published Auger UHECRs and the VCV AGNs is much stronger than the correlation with the random sets of galaxies drawn from nearby large-scale structure. This suggests that the correlation of the UHECRs with AGNs is not solely due to AGNs tracing the large-scale distribution of matter. We also find that once we take into account the heavy oversampling of the VCV catalogue in the Virgo region, the lack of UHECRs from that region is not incompatible with UHECRs having AGN sources.

Published
2010
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40. Dependence of Optical Active Galactic Nuclei Identification on Stellar Population Models

Author

Yanping Chen, Ingyin Zaw, and Glennys R. Farrar

Subjects
Physics, Active galactic nucleus, Stellar population, 010308 nuclear & particles physics, Metallicity, Doubly ionized oxygen, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Spectral line, Luminosity, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010303 astronomy & astrophysics, Line (formation)
Abstract

We have conducted a study to quantify the systematic differences resulting from using different stellar population models in optical spectroscopic identification of type II AGN. We examined the different AGN detection fractions of 7069 nearby galaxies (z = 10^40 erg s-1 and increasing to ~ 50% for L[OIII]5007, 21 pages, 20 figures, 1 table; accepted for publication in The Astrophysical Journal

Published
2018
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41. CORRELATIONS BETWEEN ULTRAHIGH ENERGY COSMIC RAYS AND INFRARED-LUMINOUS GALAXIES

Author

Glennys R. Farrar, Andreas A. Berlind, and Ingyin Zaw

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Pierre Auger Observatory, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Horizon, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Luminosity, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Ultrahigh energy, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

We confirm the UHECR horizon established by the Pierre Auger Observatory using the heterogeneous Veron-Cetty Veron (VCV) catalog of AGNs, by performing a redshift-angle-IR luminosity scan using PSCz galaxies having infrared luminosity greater than 10^{10}L_sun. The strongest correlation -- for z < 0.016, psi = 2.1 deg, and L_ir > 10^{10.5}L_sun -- arises in fewer than 0.3% of scans with isotropic source directions. When we apply a penalty for using the UHECR energy threshold that was tuned to maximize the correlation with VCV, the significance degrades to 1.1%. Since the PSCz catalog is complete and volume-limited for these parameters, this suggests that the UHECR horizon discovered by the Pierre Auger Observatory is not an artifact of the incompleteness and other idiosyncrasies of the VCV catalog. The strength of the correlation between UHECRs and the nearby highest-IR-luminosity PSCz galaxies is stronger than in about 90% percent of trials with scrambled luminosity assignments for the PSCz galaxies. If confirmed by future data, this result would indicate that the sources of UHECRs are more strongly associated with luminous IR galaxies than with ordinary, lower IR luminosity galaxies., 4 pages, 3 figures. Replaced with accepted version

Published
2010
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42. GALAXIES CORRELATING WITH ULTRA-HIGH ENERGY COSMIC RAYS

Author

Ingyin Zaw, Jenny E. Greene, and Glennys R. Farrar

Subjects
Physics, Pierre Auger Observatory, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Luminosity, law.invention, Space and Planetary Science, law, Astrophysics::Solar and Stellar Astrophysics, Ultra-high-energy cosmic ray, Astrophysics::Galaxy Astrophysics, Flare
Abstract

The Pierre Auger Observatory reports that 20 of the 27 highest energy cosmic rays have arrival directions within 3.2 deg of a nearby galaxy in the Veron-Cetty & Veron Catalog of Quasars and Active Galactic Nuclei (12th Ed.), with ~5 of the correlations expected by chance. In this paper we examine the correlated galaxies to gain insight into the possible UHECR sources. We find that 14 of the 21 correlated VCV galaxies are AGNs and we determine their bolometric luminosities. The remaining 7 are primarily star-forming galaxies. The bolometric luminosities of the correlated AGNs are all greater than 5 x 10^{42} erg/s, which may explain the absence of UHECRs from the Virgo region in spite of the large number of VCV galaxies in Virgo, since most of the VCV galaxies in the Virgo region are low luminosity AGNs. Interestingly, the bolometric luminosities of most of the AGNs are significantly lower than required to satisfy the minimum condition for UHECR acceleration in a continuous jet. If a UHECR-AGN correlation is substantiated with further statistics, our results lend support to the recently proposed ``giant AGN flare" mechanism for UHECR acceleration., 13 pages, 3 figures, to be submitted to ApJ

Published
2009
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43. Measurement of the radiation energy in the radio signal of extensive air showers as a universal estimator of cosmic-ray energy

Author

Alaa Kuotb Awad, Benoît Revenu, James Matthews, Alexandra Saftoiu, Alberto Filevich, Peter Hansen, Ivan De Mitri, I. Lhenry-Yvon, John Matthews, Peter Buchholz, Philipp Papenbreer, Petr Travnicek, H. Wahlberg, A. Nelles, R. Piegaia, I.M. Brancus, Alan Coleman, T. Hebbeker, Trent D. Grubb, D. Huber, Marco Aglietta, Eun-Joo Ahn, S. Vorobiov, K. Weidenhaupt, E.M. Holt, B. Wundheiler, A. Saleh, A. Parra, R. J. Lauer, Juan Manuel Figueira, S. Jansen, Bruno Daniel, Maria-Teresa Dova, Foteini Oikonomou, M. R. Hampel, Peter Mazur, J. Sorokin, Marcelo Augusto Leigui de Oliveira, Sarka Wykes, R. Meissner, Octavian Fratu, G. Parente, M. Trini, Roberta Colalillo, O. Wainberg, C. Bleve, P. Pieroni, S. Müller, Vincenzo Rizi, Nicusor Arsene, Julian Rautenberg, V. B. B. Mello, K. H. Becker, A. G. Mariazzi, Eric Mayotte, Jeffrey A. Johnsen, Sven Querchfeld, L. Perrone, R. C. Shellard, W. Docters, Carlos Hojvat, Ernesto Kemp, Xavier Bertou, Luis del Peral, Ugo Giaccari, Henryk Wilczyński, J. J. Beatty, Norbert Kunka, D. Nitz, Silvia Mollerach, D. Lebrun, S. Quinn, Sjoert van Velzen, Primo F. Gómez Vitale, R. Sato, S. Coutu, Norberto Fazzini, Antonio Bueno, Antonio Insolia, M. Josebachuili, Gualberto Avila, Ingomar Allekotte, G. Matthiae, Angela V. Olinto, O. Kambeitz, M. Ambrosio, Eva Santos, R. Krause, Jose Sanabria Gomez, M. Zavrtanik, Fred Sarazin, Lukas Nellen, B. Caccianiga, Julien Aublin, A. Shadkam, Amin Aminaei, Rafael Alves Batista, Jakub Vicha, Pedro Assis, Radomir Smida, Diego Harari, B. Gookin, P. H. Nguyen, Alberto Etchegoyen, Darius Reinert, Lorenzo Caccianiga, V. M. Theodoro, Tobias Winchen, D. Martello, Karen S. Caballero-Mora, Michael Unger, D. Melo, Luca Latronico, Guenter Sigl, D. Garcia-Pinto, Alessio Gorgi, Paul Sommers, A. Blanco, M. J. Cooper, S. Stanič, Carlos Medina, Tanguy Pierog, Mariano Gómez Berisso, D. Rogozin, Alejandro Almela, E. M. Santos, P. Heimann, Florian Gaté, J. R. Vázquez, Carla Bonifazi, Bernardo Vargas Cárdenas, A. C. Rovero, B. Tome, Marco Giammarchi, D. Garcia-Gamez, J. W. H. Gordon, Jose A. Bellido, L. Niemietz, S. Hartmann, Martin Erdmann, Jan Pękala, Hans Klages, A. Chiavassa, P. Sanchez-Lucas, Vitor de Souza, Bruce R. Dawson, Tim Huege, Carola Dobrigkeit, M. Plum, P. Abreu, Miguel Mostafá, C. Porowski, S. Sonntag, Markus Risse, Christian Sarmiento-Cano, B. Vlcek, Dariusz Glas, Diego Ravignani, O. A. Taborda, M. Settimo, M. Blanco, Mário Pimenta, Gregory R Snow, Pablo Ristori, P. H. Kasper, Gaetano Salina, Maria Rita Coluccia, Yogendra N. Srivastava, Alan Watson, Glennys R. Farrar, C. Jarne, A. Śmiałkowski, Andreas Weindl, Jaime Rosado, R. Cester, Alina Mihaela Badescu, F. Sánchez, N. Awal, Beatriz García, Jeffrey Brack, Olaf Scholten, Humberto Ibarguen Salazar, J. W. Cronin, Harald Schieler, Antoine Letessier-Selvon, C. Aramo, B. Mitrica, Heino Falcke, Nicolás González, Mihai Niculescu-Oglinzanu, Jonny Kleinfeller, K. Louedec, Arnulfo Zepeda, Armando di Matteo, G. Cocciolo, Roger W Clay, R. López, M. Mallamaci, F. G. Schröder, Mary Lucia Díaz Castro, Denise Boncioli, Jiri Chudoba, P. Lebrun, Alex Kääpä, Alberto Segreto, G. Toma, Benedikt Zimmermann, Rúben Conceição, R. Vasquez, Dusan Mandat, Colin Baus, Darko Veberič, D. Martraire, Oscar Martínez Bravo, Miroslav Hrabovský, T. Yapici, Alexey Yushkov, G. A. Anastasi, Pascal Lautridou, W. R. Carvalho, Dieter Heck, Martin Urban, G. S. Varner, Nataliia Borodai, Toshihiro Fujii, A. Menshikov, C. Morello, Jaroslaw Stasielak, Luis A. Anchordoqui, Markus Roth, N. Griffith, S. G. Blaess, Niraj Dhital, Jörg R. Hörandel, Thomas Harrison, Jaime de Oliveira, I. Valiño, H. Blümer, Max Malacari, Lili Yang, Laura Valore, L. Lopes, Lukas Middendorf, Corinne Berat, Piotr Homola, Lawrence Wiencke, Fausto Guarino, A. Filipčič, A. Aab, Johannes Schumacher, J. Neuser, Alex Tapia, Christine Peters, Ad M. van den Berg, Juan Pallotta, S. Le Coz, Jaime Alvarez-Muñiz, Alexandru Gherghel-Lascu, Mauricio Suaréz Durán, Petr Schovanek, L. Caramete, Rita dos Anjos, João de Mello Neto, H. Gemmeke, Peter L. Biermann, Sergio Sciutto, L. Ochilo, T. Suomijärvi, Karl-Heinz Kampert, Antonella Castellina, M. I. Micheletti, Federico Suarez, A. Schulz, J. Stapleton, L. Molina-Bueno, Q. Hasankiadeh, L. Tomankova, F. Arqueros, P. Necesal, Daniel Pakk Selmi-Dei, Imen Al Samarai, Martina Bohacova, David Walz, Johannes Schulz, Ruben Squartini, Paolo Privitera, F. Diogo, Juan Carlos D'Olivo, Patrick van Bodegom, Esteban Roulet, Patrick Allison, I. A. Minaya, Hernán Asorey, John Swain, Thomas Bretz, R.R. Prado, Harm Schoorlemmer, John L. Harton, T. Paul, A. Lucero, Jan Ridky, Marc Weber, F. Werner, Katrin Link, Denis Stanca, Guus van Aar, D. Maurizio, A. P. Ferguson, Corbin Covault, Y. Petrov, Geraldina Golup, Alexander Grillo, Zbigniew Szadkowski, Alessio Porcelli, J. C. Diaz, Rodrigo Pelayo, Stijn Buitink, N. Hollon, Olivier Ravel, C. A. Moura, Jose F. Valdés Galicia, Brian Fick, Lino Miramonti, Luis A. Nunez, M. Buscemi, C. Scarso, C. Welling, Marcus Niechciol, V. Novotny, Arjen van Vliet, A. Stutz, E. Varela, Rossella Caruso, S. Mathys, M. Erfani, Eduardo Quel, Henry Glass, Michael Sutherland, Francisco Salesa Greus, Guillermo Torralba Elipe, Piera Luisa Ghia, I. Jandt, Octavian Sima, Manuel Platino, M. D. Rodríguez-Frías, M. Schauer, N. Pacheco, Tim Niggemann, D. Nosek, Jan Ebr, V. Scherini, Jimmy Masías Meza, M. Candusso, Peter Gorham, Valerio Pirronello, Charles Timmermans, L. Collica, Sergio Petrera, Paul M. Mantsch, Miroslav Palatka, Jesus Alvarez Castillo, J. Blazek, Gustavo Medina-Tanco, Anderson Fauth, Vincent Marin, Rogerio M. de Almeida, M. E. Bertaina, B. Sarkar, Christian Glaser, S. Messina, Claudio Di Giulio, L. Nožka, J. Espadanal, Diego Torres Machado, Paula Gina Isar, Pedro Brogueira, G. Cataldi, Sergio Dasso, Martín Miguel Freire, P. Billoir, Aida López Casado, Carlos J. Todero Peixoto, G. Marsella, Daniel Kuempel, Carlos Escobar, R.M. Kieckhafer, Iuri Muniz Pepe, Maria Giller, Hermann-Josef Mathes, A. Cordier, Ivone F. M. Albuquerque, Ke Fang, Gašper Kukec Mezek, I. Katkov, Richard Dallier, Francesca Zuccarello, Kai Daumiller, Maurice Stephan, M. Ziolkowski, A. Tonachini, A.E. Herve, F. Montanet, J. Maller, V. Verzi, David Schmidt, S. Sánchez Navas, Jose Chinellato, Lorenzo Cazon, Ioana Codrina Maris, Ricardo Vázquez, Giuseppe De Mauro, G. C. Hill, Ralph Engel, Andreas Haungs, M. Videla, A. Daniel Supanitsky, Matthias Kleifges, H. Martinez, David Wittkowski, Germano Guedes, Danielle LaHurd, Olivier Deligny, Marcio Aparecido Muller, A. Dorofeev, L. Villaseñor, Marco Cilmo, Jorge Rubén Rodriguez Rojo, A. Bridgeman, E. Petermann, S. J. Saffi, Markus Lauscher, J. Phuntsok, Raul Sarmento, M. Prouza, Bianca Keilhauer, A. G. Chavez, Enrique Zas, Sijbrand J. de Jong, Fernando Contreras, N. Krohm, Miroslav Pech, R. Ulrich, Pavel Horvath, P. Gouffon, Allan Widom, Danilo Zavrtanik, Gero Müller, Sofia Andringa, A. Tepe, Research unit Nuclear & Hadron Physics, Research unit Astroparticle Physics, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), Institut de Physique Nucléaire d'Orsay (IPNO), Pierre Auger Collaboration, ANR-11-IDEX-0004,SUPER,Sorbonne Universités à Paris pour l'Enseignement et la Recherche(2011), European Project: 328826,EC:FP7:PEOPLE,FP7-PEOPLE-2012-IEF,AUGER2FUTURE(2013), European Project: 246806,EC:FP7:PEOPLE,FP7-PEOPLE-2009-IRSES,EPLANET(2011), Aab, A., Abreu, P., Aglietta, M., Ahn, E. J., Al Samarai, I., Albuquerque, I. F. M., Allekotte, I., Allison, P., Almela, A., Alvarez Castillo, J., Alvarez Muñiz, J., Alves Batista, R., Ambrosio, M., Aminaei, A., Anastasi, G. A., Anchordoqui, L., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Awal, N., Badescu, A. M., Baus, C., Beatty, J. J., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Billoir, P., Blaess, S. G., Blanco, A., Blanco, M., Blazek, J., Bleve, C., Blümer, H., Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Brogueira, P., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero Mora, K. S., Caccianiga, B., Caccianiga, L., Candusso, M., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Cester, R., Chavez, A. G., Chiavassa, A., Chinellato, J. A., Chudoba, J., Cilmo, M., Clay, R. W., Cocciolo, G., Colalillo, Roberta, Coleman, A., Collica, L., Coluccia, M. R., Conceição, R., Contreras, F., Cooper, M. J., Cordier, A., Coutu, S., Covault, C. E., Cronin, J., Dallier, R., Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., De Almeida, R. M., De Jong, S. J., De Mauro, G., De Mello Neto, J. R. T., De Mitri, I., De Oliveira, J., De Souza, V., Del Peral, L., Deligny, O., Dhital, N., Di Giulio, C., Di Matteo, A., Diaz, J. C., Díaz Castro, M. L., Diogo, F., Dobrigkeit, C., Docters, W., D'Olivo, J. C., Dorofeev, A., Dorosti Hasankiadeh, Q., Dos Anjos, R. C., Dova, M. T., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Fang, K., Farrar, G., Fauth, A. C., Fazzini, N., Ferguson, A. P., Fick, B., Figueira, J. M., Filevich, A., Filipčič, A., Fratu, O., Freire, M. M., Fujii, T., García, B., Garcia Gamez, D., Garcia Pinto, D., Gate, F., Gemmeke, H., Gherghel Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Glass, H., Golup, G., Gómez Berisso, M., Gómez Vitale, P. F., González, N., Gookin, B., Gordon, J., Gorgi, A., Gorham, P., Gouffon, P., Griffith, N., Grillo, A. F., Grubb, T. D., Guarino, Fausto, Guedes, G. P., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Hartmann, S., Harton, J. L., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hill, G. C., Hojvat, C., Hollon, N., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huber, D., Huege, T., Insolia, A., Isar, P. G., Jandt, I., Jansen, S., Jarne, C., Johnsen, J. A., Josebachuili, M., Kääpä, A., Kambeitz, O., Kampert, K. H., Kasper, P., Katkov, I., Keilhauer, B., Kemp, E., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Kukec Mezek, G., Kunka, N., Kuotb Awad, A. W., Lahurd, D., Latronico, L., Lauer, R., Lauscher, M., Lautridou, P., Le Coz, S., Lebrun, D., Lebrun, P., Leigui De Oliveira, M. A., Letessier Selvon, A., Lhenry Yvon, I., Link, K., Lopes, L., López, R., López Casado, A., Louedec, K., Lucero, A., Malacari, M., Mallamaci, M., Maller, J., Mandat, D., Mantsch, P., Mariazzi, A. G., Marin, V., Mariş, I. C., Marsella, G., Martello, D., Martinez, H., Martínez Bravo, O., Martraire, D., Masías Meza, J. J., Mathes, H. J., Mathys, S., Matthews, J., Matthews, J. A. J., Matthiae, G., Maurizio, D., Mayotte, E., Mazur, P. O., Medina, C., Medina Tanco, G., Meissner, R., Mello, V. B. B., Melo, D., Menshikov, A., Messina, S., Micheletti, M. I., Middendorf, L., Minaya, I. A., Miramonti, L., Mitrica, B., Molina Bueno, L., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Moura, C. A., Muller, M. A., Müller, G., Müller, S., Navas, S., Necesal, P., Nellen, L., Nelles, A., Neuser, J., Nguyen, P. H., Niculescu Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, L., Núñez, L. A., Ochilo, L., Oikonomou, F., Olinto, A., Pacheco, N., Pakk Selmi Dei, D., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pkala, J., Pelayo, R., Pepe, I. M., Perrone, L., Petermann, E., Peters, C., Petrera, S., Petrov, Y., Phuntsok, J., Piegaia, R., Pierog, T., Pieroni, P., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porcelli, A., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Rautenberg, J., Ravel, O., Ravignani, D., Reinert, D., Revenu, B., Ridky, J., Risse, M., Ristori, P., Rizi, V., Rodrigues De Carvalho, W., Rodriguez Rojo, J., Rodríguez Frías, M. D., Rogozin, D., Rosado, J., Roth, M., Roulet, E., Rovero, A. C., Saffi, S. J., Saftoiu, A., Salazar, H., Saleh, A., Salesa Greus, F., Salina, G., Sanabria Gomez, J. D., Sánchez, F., Sanchez Lucas, P., Santos, E., Santos, E. M., Sarazin, F., Sarkar, B., Sarmento, R., Sarmiento Cano, C., Sato, R., Scarso, C., Schauer, M., Scherini, V., Schieler, H., Schmidt, D., Scholten, O., Schoorlemmer, H., Schovánek, P., Schröder, F. G., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Settimo, M., Shadkam, A., Shellard, R. C., Sigl, G., Sima, O., Śmiałkowski, A., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Sorokin, J., Squartini, R., Srivastava, Y. N., Stanca, D., Stanič, S., Stapleton, J., Stasielak, J., Stephan, M., Stutz, A., Suarez, F., Suarez Durán, M., Suomijärvi, T., Supanitsky, A. D., Sutherland, M. S., Swain, J., Szadkowski, Z., Taborda, O. A., Tapia, A., Tepe, A., Theodoro, V. M., Timmermans, C., Todero Peixoto, C. J., Toma, G., Tomankova, L., Tomé, B., Tonachini, A., Torralba Elipe, G., Torres Machado, D., Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Valdés Galicia, J. F., Valiño, I., Valore, Laura, Van Aar, G., Van Bodegom, P., Van Den Berg, A. M., Van Velzen, S., Van Vliet, A., Varela, E., Vargas Cárdenas, B., Varner, G., Vasquez, R., Vázquez, J. R., Vázquez, R. A., Veberič, D., Verzi, V., Vicha, J., Videla, M., Villaseñor, L., Vlcek, B., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weidenhaupt, K., Weindl, A., Welling, C., Werner, F., Widom, A., Wiencke, L., Wilczyński, H., Winchen, T., Wittkowski, D., Wundheiler, B., Wykes, S., Yang, L., Yapici, T., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zuccarello, F., Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Aab A, Abreu P, Aglietta M, Ahn E J, Al Samarai I, Albuquerque I F M, Allekotte I, Allison P, Almela A, Alvarez Castillo J, Alvarez-Muñiz J, Alves Batista R, Ambrosio M, Aminaei A, Anastasi G A, Anchordoqui L, Andringa S, Aramo C, Arqueros F, Arsene N, Asorey H, Assis P, Aublin J, Avila G, Awal N, Badescu A M, Baus C, Beatty J J, Becker K H, Bellido J A, Berat C, Bertaina M E, Bertou X, Biermann P L, Billoir P, Blaess S G, Blanco A, Blanco M, Blazek J, Bleve C, Blümer H, Boháčová M, Boncioli D, Bonifazi C, Borodai N, Brack J, Brancus I, Bretz T, Bridgeman A, Brogueira P, Buchholz P, Bueno A, Buitink S, Buscemi M, Caballero-Mora K S, Caccianiga B, Caccianiga L, Candusso M, Caramete L, Caruso R, Castellina A, Cataldi G, Cazon L, Cester R, Chavez A G, Chiavassa A, Chinellato J A, Chudoba J, Cilmo M, Clay R W, Cocciolo G, Colalillo R, Coleman A, Collica L, Coluccia M R, Conceição R, Contreras F, Cooper M J, Cordier A, Coutu S, Covault C E, Cronin J, Dallier R, Daniel B, Dasso S, Daumiller K, Dawson B R, de Almeida R M, de Jong S J, De Mauro G, de Mello Neto J R T, De Mitri I, de Oliveira J, de Souza V, Del Peral L, Deligny O, Dhital N, Di Giulio C, Di Matteo A, Diaz J C, Díaz Castro M L, Diogo F, Dobrigkeit C, Docters W, D'Olivo J C, Dorofeev A, Dorosti Hasankiadeh Q, Dos Anjos R C, Dova M T, Ebr J, Engel R, Erdmann M, Erfani M, Escobar C O, Espadanal J, Etchegoyen A, Falcke H, Fang K, Farrar G, Fauth A C, Fazzini N, Ferguson A P, Fick B, Figueira J M, Filevich A, Filipčič A, Fratu O, Freire M M, Fujii T, García B, Garcia-Gamez D, Garcia-Pinto D, Gate F, Gemmeke H, Gherghel-Lascu A, Ghia P L, Giaccari U, Giammarchi M, Giller M, Głas D, Glaser C, Glass H, Golup G, Gómez Berisso M, Gómez Vitale P F, González N, Gookin B, Gordon J, Gorgi A, Gorham P, Gouffon P, Griffith N, Grillo A F, Grubb T D, Guarino F, Guedes G P, Hampel M R, Hansen P, Harari D, Harrison T A, Hartmann S, Harton J L, Haungs A, Hebbeker T, Heck D, Heimann P, Herve A E, Hill G C, Hojvat C, Hollon N, Holt E, Homola P, Hörandel J R, Horvath P, Hrabovský M, Huber D, Huege T, Insolia A, Isar P G, Jandt I, Jansen S, Jarne C, Johnsen J A, Josebachuili M, Kääpä A, Kambeitz O, Kampert K H, Kasper P, Katkov I, Keilhauer B, Kemp E, Kieckhafer R M, Klages H O, Kleifges M, Kleinfeller J, Krause R, Krohm N, Kuempel D, Kukec Mezek G, Kunka N, Kuotb Awad A W, Lahurd D, Latronico L, Lauer R, Lauscher M, Lautridou P, Le Coz S, Lebrun D, Lebrun P, Leigui de Oliveira M A, Letessier-Selvon A, Lhenry-Yvon I, Link K, Lopes L, López R, López Casado A, Louedec K, Lucero A, Malacari M, Mallamaci M, Maller J, Mandat D, Mantsch P, Mariazzi A G, Marin V, Mariş I C, Marsella G, Martello D, Martinez H, Martínez Bravo O, Martraire D, Masías Meza J J, Mathes H J, Mathys S, Matthews J, Matthews J A J, Matthiae G, Maurizio D, Mayotte E, Mazur P O, Medina C, Medina-Tanco G, Meissner R, Mello V B B, Melo D, Menshikov A, Messina S, Micheletti M I, Middendorf L, Minaya I A, Miramonti L, Mitrica B, Molina-Bueno L, Mollerach S, Montanet F, Morello C, Mostafá M, Moura C A, Muller M A, Müller G, Müller S, Navas S, Necesal P, Nellen L, Nelles A, Neuser J, Nguyen P H, Niculescu-Oglinzanu M, Niechciol M, Niemietz L, Niggemann T, Nitz D, Nosek D, Novotny V, Nožka L, Núñez L A, Ochilo L, Oikonomou F, Olinto A, Pacheco N, Pakk Selmi-Dei D, Palatka M, Pallotta J, Papenbreer P, Parente G, Parra A, Paul T, Pech M, Pȩkala J, Pelayo R, Pepe I M, Perrone L, Petermann E, Peters C, Petrera S, Petrov Y, Phuntsok J, Piegaia R, Pierog T, Pieroni P, Pimenta M, Pirronello V, Platino M, Plum M, Porcelli A, Porowski C, Prado R R, Privitera P, Prouza M, Quel E J, Querchfeld S, Quinn S, Rautenberg J, Ravel O, Ravignani D, Reinert D, Revenu B, Ridky J, Risse M, Ristori P, Rizi V, Rodrigues de Carvalho W, Rodriguez Rojo J, Rodríguez-Frías M D, Rogozin D, Rosado J, Roth M, Roulet E, Rovero A C, Saffi S J, Saftoiu A, Salazar H, Saleh A, Salesa Greus F, Salina G, Sanabria Gomez J D, Sánchez F, Sanchez-Lucas P, Santos E, Santos E M, Sarazin F, Sarkar B, Sarmento R, Sarmiento-Cano C, Sato R, Scarso C, Schauer M, Scherini V, Schieler H, Schmidt D, Scholten O, Schoorlemmer H, Schovánek P, Schröder F G, Schulz A, Schulz J, Schumacher J, Sciutto S J, Segreto A, Settimo M, Shadkam A, Shellard R C, Sigl G, Sima O, Śmiałkowski A, Šmída R, Snow G R, Sommers P, Sonntag S, Sorokin J, Squartini R, Srivastava Y N, Stanca D, Stanič S, Stapleton J, Stasielak J, Stephan M, Stutz A, Suarez F, Suarez Durán M, Suomijärvi T, Supanitsky A D, Sutherland M S, Swain J, Szadkowski Z, Taborda O A, Tapia A, Tepe A, Theodoro V M, Timmermans C, Todero Peixoto C J, Toma G, Tomankova L, Tomé B, Tonachini A, Torralba Elipe G, Torres Machado D, Travnicek P, Trini M, Ulrich R, Unger M, Urban M, Valdés Galicia J F, Valiño I, Valore L, van Aar G, van Bodegom P, van den Berg A M, van Velzen S, van Vliet A, Varela E, Vargas Cárdenas B, Varner G, Vasquez R, Vázquez J R, Vázquez R A, Veberič D, Verzi V, Vicha J, Videla M, Villaseñor L, Vlcek B, Vorobiov S, Wahlberg H, Wainberg O, Walz D, Watson A A, Weber M, Weidenhaupt K, Weindl A, Welling C, Werner F, Widom A, Wiencke L, Wilczyński H, Winchen T, Wittkowski D, Wundheiler B, Wykes S, Yang L, Yapici T, Yushkov A, Zas E, Zavrtanik D, Zavrtanik M, Zepeda A, Zimmermann B, Ziolkowski M, Zuccarello F, Aab, A, Abreu, P, Aglietta, M, Ahn, E. J, Al Samarai, I, Albuquerque, I. F. M, Allekotte, I, Allison, P, Almela, A, Alvarez Castillo, J, Alvarez Muñiz, J, Alves Batista, R, Ambrosio, M, Aminaei, A, Anastasi, G. A, Anchordoqui, L, Andringa, S, Aramo, C, Arqueros, F, Arsene, N, Asorey, H, Assis, P, Aublin, J, Avila, G, Awal, N, Badescu, A. M, Baus, C, Beatty, J. J, Becker, K. H, Bellido, J. A, Berat, C, Bertaina, M. E, Bertou, X, Biermann, P. L, Billoir, P, Blaess, S. G, Blanco, A, Blanco, M, Blazek, J, Bleve, Carla, Blümer, H, Boháčová, M, Boncioli, D, Bonifazi, C, Borodai, N, Brack, J, Brancus, I, Bretz, T, Bridgeman, A, Brogueira, P, Buchholz, P, Bueno, A, Buitink, S, Buscemi, M, Caballero Mora, K. S, Caccianiga, B, Caccianiga, L, Candusso, M, Caramete, L, Caruso, R, Castellina, A, Cataldi, G, Cazon, L, Cester, R, Chavez, A. G, Chiavassa, A, Chinellato, J. A, Chudoba, J, Cilmo, M, Clay, R. W, Cocciolo, G, Colalillo, R, Coleman, A, Collica, L, Coluccia, MARIA RITA, Conceição, R, Contreras, F, Cooper, M. J, Cordier, A, Coutu, S, Covault, C. E, Cronin, J, Dallier, R, Daniel, B, Dasso, S, Daumiller, K, Dawson, B. R, de Almeida, R. M, de Jong, S. J, De Mauro, G, de Mello Neto, J. R. T, DE MITRI, Ivan, de Oliveira, J, de Souza, V, Del Peral, L, Deligny, O, Dhital, N, Di Giulio, C, Di Matteo, A, Diaz, J. C, Díaz Castro, M. L, Diogo, F, Dobrigkeit, C, Docters, W, D'Olivo, J. C, Dorofeev, A, Dorosti Hasankiadeh, Q, Dos Anjos, R. C, Dova, M. T, Ebr, J, Engel, R, Erdmann, M, Erfani, M, Escobar, C. O, Espadanal, J, Etchegoyen, A, Falcke, H, Fang, K, Farrar, G, Fauth, A. C, Fazzini, N, Ferguson, A. P, Fick, B, Figueira, J. M, Filevich, A, Filipčič, A, Fratu, O, Freire, M. M, Fujii, T, García, B, Garcia Gamez, D, Garcia Pinto, D, Gate, F, Gemmeke, H, Gherghel Lascu, A, Ghia, P. L, Giaccari, U, Giammarchi, M, Giller, M, Głas, D, Glaser, C, Glass, H, Golup, G, Gómez Berisso, M, Gómez Vitale, P. F, González, N, Gookin, B, Gordon, J, Gorgi, A, Gorham, P, Gouffon, P, Griffith, N, Grillo, A. F, Grubb, T. D, Guarino, F, Guedes, G. P, Hampel, M. R, Hansen, P, Harari, D, Harrison, T. A, Hartmann, S, Harton, J. L, Haungs, A, Hebbeker, T, Heck, D, Heimann, P, Herve, A. E, Hill, G. C, Hojvat, C, Hollon, N, Holt, E, Homola, P, Hörandel, J. R, Horvath, P, Hrabovský, M, Huber, D, Huege, T, Insolia, A, Isar, P. G, Jandt, I, Jansen, S, Jarne, C, Johnsen, J. A, Josebachuili, M, Kääpä, A, Kambeitz, O, Kampert, K. H, Kasper, P, Katkov, I, Keilhauer, B, Kemp, E, Kieckhafer, R. M, Klages, H. O, Kleifges, M, Kleinfeller, J, Krause, R, Krohm, N, Kuempel, D, Kukec Mezek, G, Kunka, N, Kuotb Awad, A. W, Lahurd, D, Latronico, L, Lauer, R, Lauscher, M, Lautridou, P, Le Coz, S, Lebrun, D, Lebrun, P, Leigui de Oliveira, M. A, Letessier Selvon, A, Lhenry Yvon, I, Link, K, Lopes, L, López, R, López Casado, A, Louedec, K, Lucero, A, Malacari, M, Mallamaci, M, Maller, J, Mandat, D, Mantsch, P, Mariazzi, A. G, Marin, V, Mariş, I. C, Marsella, Giovanni, Martello, Daniele, Martinez, H, Martínez Bravo, O, Martraire, D, Masías Meza, J. J, Mathes, H. J, Mathys, S, Matthews, J, Matthews, J. A. J, Matthiae, G, Maurizio, D, Mayotte, E, Mazur, P. O, Medina, C, Medina Tanco, G, Meissner, R, Mello, V. B. B, Melo, D, Menshikov, A, Messina, S, Micheletti, M. I, Middendorf, L, Minaya, I. A, Miramonti, L, Mitrica, B, Molina Bueno, L, Mollerach, S, Montanet, F, Morello, C, Mostafá, M, Moura, C. A, Muller, M. A, Müller, G, Müller, S, Navas, S, Necesal, P, Nellen, L, Nelles, A, Neuser, J, Nguyen, P. H, Niculescu Oglinzanu, M, Niechciol, M, Niemietz, L, Niggemann, T, Nitz, D, Nosek, D, Novotny, V, Nožka, L, Núñez, L. A, Ochilo, L, Oikonomou, F, Olinto, A, Pacheco, N, Pakk Selmi Dei, D, Palatka, M, Pallotta, J, Papenbreer, P, Parente, G, Parra, A, Paul, T, Pech, M, Pȩkala, J, Pelayo, R, Pepe, I. M, Perrone, Lorenzo, Petermann, E, Peters, C, Petrera, S, Petrov, Y, Phuntsok, J, Piegaia, R, Pierog, T, Pieroni, P, Pimenta, M, Pirronello, V, Platino, M, Plum, M, Porcelli, A, Porowski, C, Prado, R. R, Privitera, P, Prouza, M, Quel, E. J, Querchfeld, S, Quinn, S, Rautenberg, J, Ravel, O, Ravignani, D, Reinert, D, Revenu, B, Ridky, J, Risse, M, Ristori, P, Rizi, V, Rodrigues de Carvalho, W, Rodriguez Rojo, J, Rodríguez Frías, M. D, Rogozin, D, Rosado, J, Roth, M, Roulet, E, Rovero, A. C, Saffi, S. J, Saftoiu, A, Salazar, H, Saleh, A, Salesa Greus, F, Salina, G, Sanabria Gomez, J. D, Sánchez, F, Sanchez Lucas, P, Santos, E, Santos, E. M, Sarazin, F, Sarkar, B, Sarmento, R, Sarmiento Cano, C, Sato, R, Scarso, C, Schauer, M, Scherini, V, Schieler, H, Schmidt, D, Scholten, O, Schoorlemmer, H, Schovánek, P, Schröder, F. G, Schulz, A, Schulz, J, Schumacher, J, Sciutto, S. J, Segreto, A, Settimo, M, Shadkam, A, Shellard, R. C, Sigl, G, Sima, O, Śmiałkowski, A, Šmída, R, Snow, G. R, Sommers, P, Sonntag, S, Sorokin, J, Squartini, R, Srivastava, Y. N, Stanca, D, Stanič, S, Stapleton, J, Stasielak, J, Stephan, M, Stutz, A, Suarez, F, Suarez Durán, M, Suomijärvi, T, Supanitsky, A. D, Sutherland, M. S, Swain, J, Szadkowski, Z, Taborda, O. A, Tapia, A, Tepe, A, Theodoro, V. M, Timmermans, C, Todero Peixoto, C. J, Toma, G, Tomankova, L, Tomé, B, Tonachini, A, Torralba Elipe, G, Torres Machado, D, Travnicek, P, Trini, M, Ulrich, R, Unger, M, Urban, M, Valdés Galicia, J. F, Valiño, I, Valore, L, van Aar, G, van Bodegom, P, van den Berg, A. M, van Velzen, S, van Vliet, A, Varela, E, Vargas Cárdenas, B, Varner, G, Vasquez, R, Vázquez, J. R, Vázquez, R. A, Veberič, D, Verzi, V, Vicha, J, Videla, M, Villaseñor, L, Vlcek, B, Vorobiov, S, Wahlberg, H, Wainberg, O, Walz, D, Watson, A. A, Weber, M, Weidenhaupt, K, Weindl, A, Welling, C, Werner, F, Widom, A, Wiencke, L, Wilczyński, H, Winchen, T, Wittkowski, D, Wundheiler, B, Wykes, S, Yang, L, Yapici, T, Yushkov, A, Zas, E, Zavrtanik, D, Zavrtanik, M, Zepeda, A, Zimmermann, B, Ziolkowski, M, Elementary Particle Physics, and Physics

Subjects
Ciencias Físicas, Astronomy, General Physics and Astronomy, ultra-high energy cosmic rays, Astrophysics, 01 natural sciences, High Energy Physics - Experiment, purl.org/becyt/ford/1 [https], High Energy Physics - Experiment (hep-ex), CODALEMA, Observatory, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Range (particle radiation), Radio detector, TUNKA-REX, Settore FIS/01 - Fisica Sperimentale, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Radio Technique, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, radio emission, CIENCIAS NATURALES Y EXACTAS, Radio wave, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Physics and Astronomy (all), 0103 physical sciences, extensive air showers, High Energy Physics, ultra-high energy cosmic rays, extensive air showers, radio emission, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cosmic rays, Pierre Auger Observatory, 010308 nuclear & particles physics, Radiant energy, Física, LOFAR, purl.org/becyt/ford/1.3 [https], ASTROFÍSICA, SIMULATIONS, Computational physics, Astronomía, COREAS, Experimental High Energy Physics, ARRAY, EMISSION, SIMULATIONS, LOFAR, EMISSION
Abstract

We measure the energy emitted by extensive air showers in the form of radio emission in the frequency range from 30 to 80 MHz. Exploiting the accurate energy scale of the Pierre Auger Observatory, we obtain a radiation energy of 15.8±0.7(stat)±6.7(syst) MeV for cosmic rays with an energy of 1 EeV arriving perpendicularly to a geomagnetic field of 0.24 G, scaling quadratically with the cosmic-ray energy. A comparison with predictions from state-of-the-art first-principles calculations shows agreement with our measurement. The radiation energy provides direct access to the calorimetric energy in the electromagnetic cascade of extensive air showers. Comparison with our result thus allows the direct calibration of any cosmic-ray radio detector against the well-established energy scale of the Pierre Auger Observatory., La lista completa de autores que integran el documento puede consultarse en el archivo, Instituto de Física La Plata

Published
2016
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44. The speed of the ‘bullet’ in the merging galaxy cluster 1E0657−56

Author

Volker Springel and Glennys R. Farrar

Subjects
Physics, Shock (fluid dynamics), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Mass ratio, Cosmology, symbols.namesake, Gravitational lens, Mach number, Space and Planetary Science, symbols, Bow shock (aerodynamics), Astrophysics::Galaxy Astrophysics, Galaxy cluster, Line (formation)
Abstract

Deep Chandra exposures of the hot galaxy cluster 1E0657-56 have revealed that the cluster is observed shortly after the first core-passage of a massive infalling subcluster, which is preceded by a prominent bow shock with Mach number M~3. The inferred shock velocity of ~4700 km/s has been commonly interpreted as the velocity of the `bullet' subcluster itself. This velocity is unexpectedly high in the LCDM cosmology, which may require non-trivial modifications in the dark sector to be accommodated if taken at face value. Here we present explicit hydrodynamical toy models of galaxy cluster mergers which very well reproduce the observed dynamical state of 1E0657-56 and the mass models inferred from gravitational lensing observations. However, despite a shock speed of 4500 km/s, the subcluster's mass centroid is moving only with 2600 km/s in the rest frame of the system. The difference arises in part due to a gravitationally induced inflow velocity of the gas ahead of the shock, which amounts to ~1100 km/s for our assumed 10:1 mass ratio of the merger. A second effect is that the shock front moves faster than the subcluster itself. A generic LCDM collision model, where a bullet subcluster with concentration c=7.2 merges with a parent cluster with concentration c=3 on a zero-energy orbit, reproduces all the main observational features seen in 1E0657-56 with good accuracy, suggesting that 1E0657-56 is well in line with expectations from standard cosmological models. In theories with an additional 5th-force in the dark sector, the subcluster can be accelerated beyond the velocity reached in LCDM, and the spatial offset between the X-ray peak and the mass centroid of the subcluster can be significantly enlarged. (abridged)

Published
2007
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45. The Galactic Magnetic Field and UHECR Optics

Author

N. Awal, Michael Sutherland, Deepak Khurana, and Glennys R. Farrar

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Field (physics), Field line, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Magnetic field, Rigidity (electromagnetism), Astrophysics of Galaxies (astro-ph.GA), Scale structure, Halo, Diffusion (business), Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

A good model of the Galactic magnetic field is crucial for estimating the Galactic contribution in dark matter and CMB-cosmology studies, determining the sources of UHECRs, and also modeling the transport of Galactic CRs since the halo field provides an important escape route for by diffusion along its field lines. We briefly review the observational foundations of the Jansson-Farrar 2012 model for the large scale structure of the GMF, underscoring the robust evidence for a N-to-S directed, spiraling halo field. New results on the lensing effect of the GMF on UHECRs are presented, displaying multiple images and dramatic magnification and demagnification that varies with source direction and CR rigidity., Oral Contribution to ICRC 2015

Published
2015

46. Foreground and Source of a Cluster of Ultra-High-Energy Cosmic Rays

Author

Andreas A. Berlind, David W. Hogg, and Glennys R. Farrar

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Space and Planetary Science, Sky, Ultra-high-energy cosmic ray, Ultrahigh energy, Astrophysics::Galaxy Astrophysics, Galaxy cluster, media_common
Abstract

We investigate the origin of a nearly pointlike cluster of 5 ultrahigh energy cosmic rays at RA ~169.2deg and dec ~56.8deg, using Sloan Digital Sky Survey and other data. No particular source candidates are found near the estimated source direction, but the direction is exceptional in having a likely merging pair of galaxy clusters at 140/h Mpc, with an unusually low foreground density. Large scale shocks or another product of the merging galaxy clusters may accelerate the UHECRs, or the merging galaxy clusters may be coincidental and the UHECRs may be accelerated in a rare event of an unexceptional progenitor. Low magnetic deflections in the foreground void may explain why this is the only identified pointlike cluster of so many UHECRs., 5 pp

Published
2006
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47. Late arriving particles in cosmic ray air showers and determination of UHECR energies by AGASA

Author

H. J. Drescher and Glennys R. Farrar

Subjects
Physics, Energy loss, Air shower, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Nucleon, Arrival time
Abstract

We give the first detailed study of the arrival time distribution of nucleons in UHECR air showers. We analyze in detail the influence of late arriving particles on the energy determination of the AGASA experiment, as well as how the arrival time distribution changes with distance from shower core. Our calculations are consistent with experimental observations of the AGASA group. Crucial to obtaining agreement, is the correct implementation of the energy loss for low-energy protons. We confirm AGASA’s estimation of the error in their energy determination associated with late-arriving particles, assuming primary protons.

Published
2005
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48. Dominant contributions to lateral distribution functions in ultra-high energy cosmic ray air showers

Author

Glennys R. Farrar and H. J. Drescher

Subjects
Physics, Muon, Meson, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Hadron, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Electron, Nuclear physics, High Energy Physics - Phenomenology, Superposition principle, High Energy Physics - Phenomenology (hep-ph), Distribution function, High Energy Physics::Experiment, Ultra-high-energy cosmic ray
Abstract

In hadron induced air showers of highest energies (E> 1e18 eV), the lateral distribution functions of electrons and muons are a superposition of many separate electromagnetic sub-showers, initiated by meson decay at different altitudes and energies. The lateral distribution function is the primary tool for reconstructing the energy of the primary in a UHE cosmic ray shower, so understanding it in detail is a prerequisite for having confidence in the energy determination. We analyze in this paper the dominant contributions to the ground level lateral distribution functions, as a function of the altitude and energy at which the sub-showers are initiated. Far from the core, the dominant contribution to the density of electrons comes from sub-showers initiated at low altitudes and low energies (E, 19 pages, 21 figures

Published
2003
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49. [Untitled]

Author

Glennys R. Farrar

Subjects
Physics, Quantum chromodynamics, Particle physics, Cold dark matter, Physics and Astronomy (miscellaneous), General Mathematics, Dark matter, Stability (probability)
Abstract

Particle physics arguments suggest that the H-dibaryon—a state consisting of two u, two d, and two s quarks—may have a mass ≈ 1.5 ± 0.2 MeV, and that r H≲ $${1 \over 4}$$ r N. Remarkably, the observed stability of nuclei and other experimental limits do not exclude this scenario at present, as discussed here. If they are present in sufficient abundance, relic H's would be the cold dark matter. Tests of this scenario are discussed.

Published
2003
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50. The Galactic magnetic field and its lensing of ultrahigh energy and Galactic cosmic rays

Author

Glennys R. Farrar

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar System, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Magnetic field, Galactic halo, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Ultrahigh energy, Diffusion (business), Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

It has long been recognized that magnetic fields play an important role in many astrophysical environments, yet the strength and structure of magnetic fields beyond our solar system have been at best only qualitatively constrained. The Galactic magnetic field in particular is crucial for modeling the transport of Galactic CRs, for calculating the background to dark matter and CMB-cosmology studies, and for determining the sources of UHECRs. This report gives a brief overview of recent major advances in our understanding of the Galactic magnetic field (GMF) and its lensing of Galactic and ultrahigh energy cosmic rays., Comment: Invited talk at the Focus Meeting on Scale Free Phenomena at the Honolulu IAU, Aug. 2015. arXiv admin note: substantial text overlap with arXiv:1508.04530

Published
2015
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