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1. The Fluorescence Camera of the POEMMA-Balloon with Radio (PBR): Design and Scientific goals

Author

Battisti, Matteo, Eser, Johannes, Filippatos, George, Olinto, Angela, Osteria, Giuseppe, Parizot, Etienne, and Collaboration, JEM-EUSO

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The POEMMA-Balloon with Radio (PBR) is a proposed payload to fly on a NASA Super Pressure Balloon (SPB). It will act as a pathfinder of the Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) detector. PBR will consist of an innovative hybrid focal surface featuring a Fluorescence Camera (FC, based on Multi-Anode Photomultiplier Tubes [MAPMTs], 1.05 $\mu$s time resolution) and a Cherenkov Camera (based on SiPMs, 10 ns time resolution), both mounted on the same tiltable frame that can point from nadir up to 13$^\circ$ above the horizon. The FC's main scientific goal is to observe, for the first time, the fluorescence emission of Extensive Air Showers produced by Ultra-High Energy Cosmic Rays from sub-orbital altitudes. This measurement will validate the detection strategy for future space-based missions, such as POEMMA. As a secondary goal, the FC will perform a search for macroscopic dark matter through slowly evolving showers that will leave a signal similar to (but distinct from) a meteor. PBR targets a launch in 2027 as a payload of an ultra-long duration balloon flight with a duration of up to 100 days.

Published
2024
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2. The EUSO-SPB2 Fluorescence Telescope for the Detection of Ultra-High Energy Cosmic Rays

Author

Adams Jr., James H., Allard, Denis, Alldredge, Phillip, Anchordoqui, Luis, Anzalone, Anna, Battisti, Matteo, Belov, Alexander A., Bertaina, Mario, Bertone, Peter F., Blin-Bondil, Sylvie, Burton, Julia, Cafagna, Francesco S., Casolino, Marco, Černý, Karel, Christ, Mark J., Colalillo, Roberta, Crawford, Hank J., Creusot, Alexandre, Cummings, Austin, Diesing, Rebecca, Di Nola, Alessandro, Ebisuzaki, Toshikazu, Eser, Johannes, Ferrarese, Silvia, Filippatos, George, Finch, William W., Flaminio, Flavia, Fornaro, Claudio, Fuehne, Duncan, Fuglesang, Christer, Garg, Diksha, Golzio, Alessio, Guarino, Fausto, Guépin, Claire, Heibges, Tobias, Judd, Eleanor G., Klimov, Pavel A., Krizmanic, John F., Kungel, Viktoria, Kupari, Luke, Kuznetsov, Evgeny, Manfrin, Massimiliano, Marszal, Wlodzimierz, Matthews, John N., Mese, Marco, Meyer, Stephan S., Mignone, Marco, Miyamoto, Hiroko, Murashov, Alexey S., Nachtman, Jane M., Olinto, Angela V., Onel, Yasar, Osteria, Giuseppe, Panico, Beatrice, Parizot, Ètienne, Paul, Tom, Pech, Miroslav, Perfetto, Francesco, Piotrowski, Lech W., Plebaniak, Zbigniew, Posliguaaa, Jonatan, Prévôtb, Guillaume, Przybylakae, Marika, Reardona, Patrick, Reno, Mary Hall, Ricci, Marco, Sarazin, Fred, Schovánek, P., Scotti, Valentina, Shinozaki, Kenji, Soriano, Jorge F., Stillwell, Ben K., Szabelski, Jacek, Takizawa, Yoshiyuki, Trofimov, Daniil, Unel, Fredrik, Valore, Laura, Venters, Tonia M., Watts Jr., John, Wiencke, Lawrence, Wistrand, Hannah, and Young, Roy

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Extreme Universe Space Observatory on a Super Pressure Balloon 2 (EUSO-SPB2) flew on May 13$^{\text{th}}$ and 14$^{\text{th}}$ of 2023. Consisting of two novel optical telescopes, the payload utilized next-generation instrumentation for the observations of extensive air showers from near space. One instrument, the fluorescence telescope (FT) searched for Ultra-High Energy Cosmic Rays (UHECRs) by recording the atmosphere below the balloon in the near-UV with a 1~$\mu$s time resolution using 108 multi-anode photomultiplier tubes with a total of 6,912 channels. Validated by pre-flight measurements during a field campaign, the energy threshold was estimated around 2~EeV with an expected event rate of approximately 1 event per 10 hours of observation. Based on the limited time afloat, the expected number of UHECR observations throughout the flight is between 0 and 2. Consistent with this expectation, no UHECR candidate events have been found. The majority of events appear to be detector artifacts that were not rejected properly due to a shortened commissioning phase. Despite the earlier-than-expected termination of the flight, data were recorded which provide insights into the detectors stability in the near-space environment as well as the diffuse ultraviolet emissivity of the atmosphere, both of which are impactful to future experiments.

Published
2024

3. Infrared Cloud Monitoring with UCIRC2

Author

Diesing, Rebecca, Meyer, Stephan S., Eser, Johannes, Bukowski, Alexa, Miller, Alex, Apfel, Jake, Beck, Gerard, and Olinto, Angela V.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The second generation of the Extreme Universe Space Observatory on a Super Pressure Balloon (EUSO-SPB2) is a balloon instrument that searched for ultra high energy cosmic rays (UHECRs) with energies above 1 EeV and very high energy neutrinos with energies above 1 PeV. EUSO-SPB2 consists of two telescopes: a fluorescence telescope pointed downward for the detection of UHECRs and a Cherenkov telescope toward the limb for the detection of PeV-scale showers produced by neutrino-sourced tau decay (just below the limb) and by cosmic rays (just above the limb). Clouds inside the fields of view of these telescopes--particularly that of the fluorescence telescope--reduce EUSO-SPB2's geometric aperture. As such, cloud coverage and cloud-top altitude within the field of view of the fluorescence telescope must be monitored throughout data-taking. The University of Chicago Infrared Camera (UCIRC2) monitored these clouds using two infrared cameras centered at 10 and 12 $\mu$m. By capturing images at wavelengths spanning the cloud thermal emission peak, UCIRC2 measured cloud color-temperatures and thus cloud-top altitudes. In this contribution, we provide an overview of UCIRC2, including an update on its construction and performance. We also show first results from the flight., Comment: 10 pages, 7 figures, proceedings of the 38th International Cosmic Ray Conference (ICRC 2023). arXiv admin note: substantial text overlap with arXiv:2112.09618, arXiv:1909.02663

Published
2023

4. An end-to-end calibration of the Mini-EUSO detector in space

Author

Miyamoto, Hiroko, Battisti, Matteo, Barghini, Dario, Belov, Alexander, Bertaina, Mario, Bianciotto, Marta, Bisconti, Francesca, Blaksley, Carl, Blin, Sylvie, Bolmgren, Karl, Cambiè, Giorgio, Capel, Francesca, Casolino, Marco, Churilo, Igor, De La taille, Christophe, Ebisuzaki, Toshikazu, Eser, Johannes, Fenu, Francesco, Filippatos, Geroge, Franceschi, Massimo Alberto, Fuglesang, Christer, Golzio, Alessio, Gorodetzky, Philippe, Kajino, Fumioshi, Kasuga, Hiroshi, Klimov, Pavel, Kungel, Viktoria, Kuznetsov, Vladimir, Manfrin, Massimiliano, Marcelli, Laura, Mascetti, Gabriele, Marszał, Włodzimierz, Mignone, Marco, Murashov, Alexey, Napolitano, Tommaso, Ohmori, Hitoshi, Olinto, Angela, Parizot, Etienne, Picozza, Piergiorgio, Piotrowski, Lech Wiktor, Plebaniak, Zbigniew, Prévôt, Guillaume, Reali, Enzo, Ricci, Marco, Romoli, Giulia, Sakaki, Naoto, Sharakin, Sergei, Shinozaki, Kenji, Szabelski, Jacek, Takizawa, Yoshiyuki, Valentini, Giovanni, Vrabel, Michal, Wiencke, Lawrence, and MikhailZotov

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Mini-EUSO is a wide Field-of-View (FoV, 44$^{\circ}$) telescope currently in operation from a nadia-facing UV-transparent window in the Russian Zvezda module on the International Space Station (ISS). It is the first detector of the JEM-EUSO program deployed on the ISS, launched in August 2019. The main goal of Mini-EUSO is to measure the UV emissions from the ground and atmosphere, using an orbital platform. Mini-EUSO is mainly sensitive in the 290-430 nm bandwidth. Light is focused by a system of two Fresnel lenses of 25 cm diameter each on the Photo- Detector-Module (PDM), which consists of an array of 36 Multi-Anode Photomultiplier Tubes (MAPMTs), for a total of 2304 pixels working in photon counting mode, in three different time resolutions of 2.5 ${\mu}$s, 320 ${\mu}$s, 40.96 ms operation in parallel. In the longest time scale, the data is continuously acquired to monitor the UV emission of the Earth. It is best suited for the observation of ground sources and therefore has been used for the observational campaigns of the Mini-EUSO. In this contribution, we present the assembled UV flasher, the operation of the field campaign and the analysis of the obtained data. The result is compared with the overall efficiency computed from the expectations which takes into account the atmospheric attenuation and the parameterization of different effects such as the optics efficiency, the MAPMT detection efficiency, BG3 filter transmittance and the transparency of the ISS window.

Published
2023

5. POEMMA (Probe of Extreme Multi-Messenger Astrophysics) Roadmap Update

Author

Olinto, Angela V.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) was designed as a NASA Astrophysics probe-class mission to identify the sources of ultrahigh energy cosmic rays (UHECRs) and observe cosmic neutrinos from extremely energetic transient sources. POEMMA consists of two identical spacecraft flying in a loose formation at 525 km altitude oriented to view a common atmospheric volume and to provide full-sky coverage for both types of messengers. Each spacecraft hosts a wide field of view Schmidt telescope with a hybrid focal plane optimized to observe both the UV fluorescence signal from extensive air showers (EASs) and the optical Cherenkov signals from EASs. When in stereo close to nadir mode, POEMMA can measure the spectrum, composition, and full-sky distribution of the UHECRs above 20 EeV and be sensitive to UHE neutrinos. When pointing just below the Earth's limb, POEMMA will be sensitive to cosmic tau neutrinos above 20 PeV by observing the Cherenkov radiation of EASs produced by upward-moving tau decays, induced from tau neutrino interactions in the Earth. POEMMA is designed to quickly re-orient to follow a Target-of-Opportunity (ToO) neutrino transient from astrophysical sources with exceptional sensitivity to neutrinos from both short-duration transients, such as short-gamma-ray bursts (sGRBs), and long-duration sources, such as binary neutron star (BNS) mergers. Here we review the POEMMA mission and discuss the recent progress towards its technical readiness provided by the Mini-EUSO and EUSO-SPB2 missions and the forthcoming Terzina and POEMMA-Balloon-Radio missions, Comment: 12 pages, 5 figures, Proceeding 38th ICRC 2023 Nagoya, Japan. arXiv admin note: substantial text overlap with arXiv:1909.09466

Published
2023

6. Overview and First Results of EUSO-SPB2

Author

Eser, Johannes, Olinto, Angela V., and Wiencke, Lawrence

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Observing ultra-high energy cosmic rays (UHECR) and very high energy (VHE) neutrinos from space is a promising way to measure their extremely low fluxes by significantly increasing the observed volume. The Extreme Universe Space Observatory on a Super Pressure Balloon 2 (EUSO-SPB2), the next, most advanced pathfinder for such a mission, was launched May 13th 2023 from Wanaka New Zealand. The pioneering EUSO-SPB2 payload flew a Fluorescence Telescope (FT) with a PMT camera pointed in nadir to record fluorescence light from cosmic ray extensive air shower (EAS) with energies above 1 EeV, and a Cherenkov telescope (CT) with a silicon photomultiplier focal surface for observing Cherenkov emission of cosmic ray EAS with energies above 1 PeV with an above-the-limb geometry and of PeV-scale EAS initiated by neutrino-sourced tau decay. As the CT is a novel instrument, optical background measurements for space neutrino observation are an important goal of the mission. Any data collected during the mission will influence and improve the development of a space-based multi-messenger observatory such as the Probe of Extreme Multi-Messenger Astrophysics (POEMMA). We present an overview of the EUSO-SPB2 mission and its science goals and summarize results as available, from the 2023 flight., Comment: Proceeding 38th ICRC 2023 Nagoya, Japan

Published
2023
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7. Neutrino propagation through Earth: modeling uncertainties using nuPyProp

Author

Garg, Diksha, Reno, Mary Hall, Patel, Sameer, Ruestle, Alexander, Akaike, Yosui, Anchordoqui, Luis A., Bergman, Douglas R., Buckland, Isaac, Cummings, Austin L., Eser, Johannes, Garcia, Fred, Guépin, Claire, Heibges, Tobias, Ludwig, Andrew, Krizmanic, John F., Mackovjak, Simon, Mayotte, Eric, Mayotte, Sonja, Olinto, Angela V., Paul, Thomas C., Romero-Wolf, Andrés, Sarazin, Frédéric, Venters, Tonia M., Wiencke, Lawrence, and Wissel, Stephanie

Subjects
High Energy Physics - Phenomenology, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Using the Earth as a neutrino converter, tau neutrino fluxes from astrophysical point sources can be detected by tau-lepton-induced extensive air showers (EASs). Both muon neutrino and tau neutrino induced upward-going EAS signals can be detected by terrestrial, sub-orbital and satellite-based instruments. The sensitivity of these neutrino telescopes can be evaluated with the nuSpaceSim package, which includes the nuPyProp simulation package. The nuPyProp package propagates neutrinos ($\nu_\mu$, $\nu_\tau$) through the Earth to produce the corresponding charged leptons (muons and tau-leptons). We use nuPyProp to quantify the uncertainties from Earth density models, tau depolarization effects and photo-nuclear electromagnetic energy loss models in the charged lepton exit probabilities and their spectra. The largest uncertainties come from electromagnetic energy loss modeling, with as much as a 20-50% difference between the models. We compare nuPyProp results with other simulation package results., Comment: 9 pages, 6 figures, Proceedings for International Cosmic Ray Conference (ICRC) 2023

Published
2023

8. Neutrino propagation in the Earth and emerging charged leptons with $\texttt{nuPyProp}$

Author

Garg, Diksha, Patel, Sameer, Reno, Mary Hall, Reustle, Alexander, Akaike, Yosui, Anchordoqui, Luis A., Bergman, Douglas R., Buckland, Isaac, Cummings, Austin L., Eser, Johannes, Garcia, Fred, Guépin, Claire, Heibges, Tobias, Ludwig, Andrew, Krizmanic, John F., Mackovjak, Simon, Mayotte, Eric, Mayotte, Sonja, Olinto, Angela V., Paul, Thomas C., Romero-Wolf, Andrés, Sarazin, Frédéric, Venters, Tonia M., Wiencke, Lawrence, and Wissel, Stephanie

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
Abstract

Ultra-high-energy neutrinos serve as messengers of some of the highest energy astrophysical environments. Given that neutrinos are neutral and only interact via weak interactions, neutrinos can emerge from sources, traverse astronomical distances, and point back to their origins. Their weak interactions require large target volumes for neutrino detection. Using the Earth as a neutrino converter, terrestrial, sub-orbital, and satellite-based instruments are able to detect signals of neutrino-induced extensive air showers. In this paper, we describe the software code $\texttt{nuPyProp}$ that simulates tau neutrino and muon neutrino interactions in the Earth and predicts the spectrum of the $\tau$-lepton and muons that emerge. The $\texttt{nuPyProp}$ outputs are lookup tables of charged lepton exit probabilities and energies that can be used directly or as inputs to the $\texttt{nuSpaceSim}$ code designed to simulate optical and radio signals from extensive air showers induced by the emerging charged leptons. We describe the inputs to the code, demonstrate its flexibility and show selected results for $\tau$-lepton and muon exit probabilities and energy distributions. The $\texttt{nuPyProp}$ code is open source, available on Github., Comment: 42 pages, 21 figures, fixed typo in one of the author's name. Code available at https://github.com/NuSpaceSim/nupyprop

Published
2022
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9. Report of the Topical Group on Cosmic Probes of Fundamental Physics for for Snowmass 2021

Author

Adhikari, Rana X., Anchordoqui, Luis A., Fang, Ke, Sathyaprakash, B. S., Tollefson, Kirsten, Lewis, Tiffany R., Engel, Kristi, Aboubrahim, Amin, Akarsu, Ozgur, Akrami, Yashar, Aloisio, Roberto, Batista, Rafael Alves, Ballardini, Mario, Ballmer, Stefan W., Bechtol, Ellen, Benisty, David, Berti, Emanuele, Birrer, Simon, Bonilla, Alexander, Brito, Richard, Bustamante, Mauricio, Caldwell, Robert, Cardoso, Vitor, Chakrabarti, Sukanya, Chen, Thomas Y., Cicoli, Michele, Clesse, Sebastien, Coleman, Alan, Cui, Yanou, Cusin, Giulia, Daylan, Tansu, Dienes, Keith R., Di Valentino, Eleonora, Dvorkin, Cora, Escamilla-Rivera, Celia, Farrar, Glennys R., Feng, Jonathan L., Frusciante, Noemi, Garcia-Bellido, Juan, Canal, Carlos Garcia, Garzelli, Maria Vittoria, Glombitza, Jonas, Golup, Geraldina, Gritsevich, Maria, Haiman, Zoltan, Haro, Jaume, Hazra, Dhiraj Kumar, Heavens, Alan, Holz, Daniel, Horandel, Jorg R., Ishak, Mustapha, Ivanov, Mikhail M., Joudaki, Shahab, Kampert, Karl-Heinz, Karwin, Christopher M., Keeley, Ryan, Klasen, Michael, Konoplich, Rostislav, Krizmanic, John F., Kumar, Suresh, L'Huillier, Benjamin, Levi, Noam, Mandic, Vuk, Marra, Valerio, Martins, C. J. A. P., Matarrese, Sabino, Mayotte, Eric, Mayotte, Sonja, Mersini-Houghton, Laura, Meyers, Joel, Miller, Andrew L., Mottola, Emil, Mukherjee, Suvodip, Murase, Kohta, Muzio, Marco Stein, Nath, Pran, Ng, Ken K. Y., No, Jose Miguel, Nunes, Rafael C., Olinto, Angela V., Pace, Francesco, Pan, Supriya, Bergliaffa, Santiago E. Perez, Pogosian, Levon, Read, Jocelyn, Reininghaus, Maximilian, Reno, Mary Hall, Riess, Adam G., Sakellariadou, Mairi, Sakharov, Alexander S., Salucci, Paolo, Santander, Marcos, Santos, Eva, Sarazin, Fred, Saridakis, Emmanuel N., Sciutto, Sergio J., Shafieloo, Arman, Shoemaker, David H., Sinha, Kuver, Soldin, Dennis, Soriano, Jorge F., Staicova, Denitsa, Sun, Ling, Steer, D. A., Thomas, Brooks, Tomsick, John A., Valera, Victor B., Vazquez, J. Alberto, Venters, Tonia M., Visinelli, Luca, Watson, Scott, Webb, John K., Weltman, Amanda, White, Graham, Wissel, Stephanie, Yadav, Anil Kumar, Yang, Fengwei, Yang, Weiqiang, Yunes, Nicolas, Yushkov, Alexey, and Zhang, Haocheng

Subjects
High Energy Physics - Phenomenology, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Cosmic Probes of Fundamental Physics take two primary forms: Very high energy particles (cosmic rays, neutrinos, and gamma rays) and gravitational waves. Already today, these probes give access to fundamental physics not available by any other means, helping elucidate the underlying theory that completes the Standard Model. The last decade has witnessed a revolution of exciting discoveries such as the detection of high-energy neutrinos and gravitational waves. The scope for major developments in the next decades is dramatic, as we detail in this report., Comment: Report of theTopical Group on Cosmic Probes of Fundamental Physics, for the U.S. decadal Particle Physics Planning Exercise (Snowmass 2021)

Published
2022

10. UCIRC2: EUSO-SPB2's Infrared Cloud Monitor

Author

Diesing, Rebecca, Bukowski, Alexa, Friedlander, Noah, Miller, Alex, Meyer, Stephan, and Olinto, Angela V.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The second generation of the Extreme Universe Space Observatory on a Super Pressure Balloon (EUSO-SPB2) is a balloon instrument for the detection of ultra high energy cosmic rays (UHECRs) with energies above 1 EeV and very high energy neutrinos with energies above 10 PeV. EUSO-SPB2 consists of two telescopes: a fluorescence telescope pointed downward for the detection of UHECRs and a Cherenkov telescope pointed towards the limb for the detection of tau lepton-induced showers produced by up-going tau neutrinos and background signals below the limb. Clouds inside the field of view of these telescopes reduce EUSO-SPB2's geometric aperture, in particular that of the fluorescence telescope. For this reason, cloud coverage and cloud-top altitude within the field of view of the fluorescence telescope must be monitored throughout data-taking. The University of Chicago Infrared Camera (UCIRC2) will monitor these clouds using two infrared cameras with response centered at wavelengths 10 and 12 microns. By capturing images at wavelengths spanning the cloud thermal emission peak, UCIRC2 will measure cloud color-temperatures and thus cloud-top altitudes. In this contribution, we provide an overview of UCIRC2, including an update on its construction and a discussion of the techniques used to calibrate the instrument., Comment: 12 pages, 5 figures, proceedings of the 37th International Cosmic Ray Conference (ICRC 2021). arXiv admin note: substantial text overlap with arXiv:1909.02663

Published
2021

11. EUSO-SPB2 Telescope Optics and Testing

Author

Kungel, Viktoria, Bachman, Randy, Brewster, Jerod, Dawes, Madeline, Desiato, Julianna, Eser, Johannes, Finch, William, Huelett, Lindsey, Olinto, Angela V., Pace, Justin, Pech, Miroslav, Reardon, Patrick, Schovanek, Petr, Wang, Chantal, and Wiencke, Lawrence

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Extreme Universe Space Observatory - Super Pressure Balloon (EUSO-SPB2) mission will fly two custom telescopes that feature Schmidt optics to measure \v{C}erenkov- and fluorescence-emission of extensive air-showers from cosmic rays at the PeV and EeV-scale, and search for tau-neutrinos. Both telescopes have 1-meter diameter apertures and UV/UV-visible sensitivity. The \v{C}erenkov telescope uses a bifocal mirror segment alignment, to distinguish between a direct cosmic ray that hits the camera versus the \v{C}erenkov light from outside the telescope. Telescope integration and laboratory calibration will be performed in Colorado. To estimate the point spread function and efficiency of the integrated telescopes, a test beam system that delivers a 1-meter diameter parallel beam of light is being fabricated. End-to-end tests of the fully integrated instruments will be carried out in a field campaign at dark sites in the Utah desert using cosmic rays, stars, and artificial light sources. Laser tracks have long been used to characterize the performance of fluorescence detectors in the field. For EUSO-SPB2 an improvement in the method that includes a correction for aerosol attenuation is anticipated by using a bi-dynamic Lidar configuration in which both the laser and the telescope are steerable. We plan to conduct these field tests in Fall 2021 and Spring 2022 to accommodate the scheduled launch of EUSO-SPB2 in 2023 from Wanaka, New Zealand.

Published
2021

12. Probing the properties of superheavy dark matter annihilating or decaying into neutrinos with ultra-high energy neutrino experiments

Author

Guépin, Claire, Aloisio, Roberto, Anchordoqui, Luis A., Cummings, Austin, Krizmanic, John F., Olinto, Angela V., Reno, Mary Hall, and Venters, Tonia M.

Subjects
High Energy Physics - Phenomenology, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The evidence for dark matter particles, $\chi$, is compelling based on Galactic to cosmological scale observations. Thus far, the promising weakly interacting massive particle scenario have eluded detection, motivating alternative models of dark matter. We consider scenarios involving superheavy dark matter (SHDM) that potentially can decay or annihilate to neutrinos and antineutrinos. In the mass range $m_\chi=10^7-10^{15}\,{\rm GeV}$, we evaluate the sensitivities of future observatories POEMMA and GRAND for indirect dark matter detection via the measurement of neutrino-induced extensive air showers (EAS), compute the Auger and ANITA limits using their last up-to-date sensitivities, and compare them with IceCube limits. We also show that the uncertainties related to the dark matter distribution in the Galactic halo have a large impact on the neutrino flux. We show that a ground-based radio detector such as GRAND can achieve high sensitivities due to its large effective area and high duty cycle. Space-based Cherenkov detectors such as POEMMA that measure the EAS optical Cherenkov signal have the advantage of full-sky coverage and rapid slewing, enabling an optimized SHDM observation strategy focusing on the Galactic Center. We show that increasing the field of view of the Cherenkov detectors can significantly enhance the sensitivity. Moreover, POEMMA's fluorescence observation mode that measures EAS above $20\,$EeV will achieve state-of-the-art sensitivity to SHDM properties at the highest mass scales., Comment: 8 pages, 4 figures, Proceedings of the 37th International Cosmic Ray Conference (ICRC 2021)

Published
2021

14. Monte Carlo simulations of neutrino and charged lepton propagation in the Earth with nuPyProp

Author

Patel, Sameer, Reno, Mary Hall, Akaike, Yosui, Anchordoqui, Luis, Bergman, Douglas, Buckland, Isaac, Cummings, Austin, Eser, Johannes, Guépin, Claire, Krizmanic, John F., Mackovjak, Simon, Olinto, Angela, Paul, Thomas, Reustle, Alex, Romero-Wolf, Andrew, Sarazin, Fred, Venters, Tonia, Wiencke, Lawrence, and Wissel, Stephanie

Subjects
High Energy Physics - Phenomenology
Abstract

An accurate modeling of neutrino flux attenuation and the distribution of leptons they produce in transit through the Earth is an essential component to determine neutrino flux sensitivities of underground, sub-orbital and space-based detectors. Through neutrino oscillations over cosmic distances, astrophysical neutrino sources are expected to produce nearly equal fluxes of electron, muon and tau neutrinos. Of particular interest are tau neutrinos that interact in the Earth at modest slant depths to produce $\tau$-leptons. Some $\tau$-leptons emerge from the Earth and decay in the atmosphere to produce extensive air showers. Future balloon-borne and satellite-based optical Cherenkov neutrino telescopes will be sensitive to upward air showers from tau neutrino induced $\tau$-lepton decays. We present nuPyProp, a python code that is part of the nuSpaceSim package. nuPyProp generates look-up tables for exit probabilities and energy distributions for $\nu_\tau\to \tau$ and $\nu_\mu\to \mu$ propagation in the Earth. This flexible code runs with either stochastic or continuous electromagnetic energy losses for the lepton transit through the Earth. Current neutrino cross section models and energy loss models are included along with templates for user input of other models. Results from nuPyProp are compared with other recent simulation packages for neutrino and charged lepton propagation. Sources of modeling uncertainties are described and quantified., Comment: 9 pages, 6 figures, PoS(ICRC2021)1203; for associated code, see https://github.com/NuSpaceSim/nupyprop

Published
2021
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15. Neutrino constraints on long-lived heavy dark sector particle decays in the Earth

Author

Reno, Mary Hall, Anchordoqui, Luis A., Bhattacharya, Atri, Cummings, Austin, Eser, Johannes, Guépin, Claire, Krizmanic, John F., Olinto, Angela V., Paul, Thomas, Sarcevic, Ina, and Venters, Tonia M.

Subjects
High Energy Physics - Phenomenology
Abstract

Recent theoretical work has explored dark matter accumulation in the Earth and its drift towards the center of the Earth that, for the current age of the Earth, does not necessarily result in a concentration of dark matter ($\chi$) in the Earth's core. We consider a scenario of long-lived ($\tau_\chi\sim 10^{28}$ s), super heavy ($m_\chi=10^7-10^{10}$ GeV) dark matter that decays via $\chi\to \nu_\tau \bar{\nu}_\tau$ or $\chi\to \nu_\mu \bar{\nu}_\mu$. We show that an IceCube-like detector over 10 years can constrain a dark matter density that mirrors the Earth's density or has a uniform density with density fraction $\epsilon_\rho$ combined with the partial decay width $B_{\chi\to \nu_\tau \bar{\nu}_\tau}\Gamma_\chi$ in the range of $(\epsilon_\rho/10^{-10}) B_{\chi\to \nu_\tau}\Gamma_\chi \lesssim 1.5\times 10^{-29}-1.5\times 10^{-28}$ s$^{-1}$. For $\chi\to \nu_\mu \bar{\nu}_\mu$, $m_\chi = 10^8-10^{10}$ GeV and $E_\mu>10^7$ GeV, the range of constraints is $(\epsilon_\rho/10^{-10}) B_{\chi\to \nu_\mu}\Gamma_\chi \lesssim 3\times 10^{-29}-7\times 10^{-28}$ s$^{-1}$., Comment: 12 pages, 9 figures, matching version accepted for publication in Physical Review D

Published
2021

16. Indirect dark matter searches at ultrahigh energy neutrino detectors

Author

Guépin, Claire, Aloisio, Roberto, Anchordoqui, Luis A., Cummings, Austin, Krizmanic, John F., Olinto, Angela V., Reno, Mary Hall, and Venters, Tonia M.

Subjects
High Energy Physics - Phenomenology, Astrophysics - High Energy Astrophysical Phenomena
Abstract

High to ultrahigh energy neutrino detectors can uniquely probe the properties of dark matter $\chi$ by searching for the secondary products produced through annihilation and/or decay processes. We evaluate the sensitivities to dark matter thermally averaged annihilation cross section $\langle\sigma v\rangle$ and partial decay width into neutrinos $\Gamma_{\chi\rightarrow\nu\bar{\nu}}$ (in the mass scale $10^7 \leq m_\chi/{\rm GeV} \leq 10^{15}$) for next generation observatories like POEMMA and GRAND. We show that in the range $ 10^7 \leq m_\chi/{\rm GeV} \leq 10^{11}$, space-based Cherenkov detectors like POEMMA have the advantage of full-sky coverage and rapid slewing, enabling an optimized dark matter observation strategy focusing on the Galactic center. We also show that ground-based radio detectors such as GRAND can achieve high sensitivities and high duty cycles in radio quiet areas. We compare the sensitivities of next generation neutrino experiments with existing constraints from IceCube and updated 90\% C.L. upper limits on $\langle\sigma v\rangle$ and $\Gamma_{\chi\rightarrow\nu\bar{\nu}}$ using results from the Pierre Auger Collaboration and ANITA. We show that in the range $ 10^7 \leq m_\chi/{\rm GeV} \leq 10^{11}$ POEMMA and GRAND10k will improve the neutrino sensitivity to particle dark matter by factors of 2 to 10 over existing limits, whereas GRAND200k will improve this sensitivity by two orders of magnitude. In the range $10^{11} \leq m_\chi/{\rm GeV} \leq 10^{15}$, POEMMA's fluorescence observation mode will achieve an unprecedented sensitivity to dark matter properties. Finally, we highlight the importance of the uncertainties related to the dark matter distribution in the Galactic halo, using the latest fit and estimates of the Galactic parameters., Comment: 28 pages, 8 figures, accepted to PRD

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

Author

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

Subjects
High Energy Physics - Phenomenology, 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., Comment: SNOWMASS 2021 LoI. Accepted for publication in Astroparticle Physics

Published
2021
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18. Prospects for macroscopic dark matter detection at space-based and suborbital experiments

Author

Anchordoqui, Luis A., Bertaina, Mario E., Casolino, Marco, Eser, Johannes, Krizmanic, John F., Olinto, Angela V., Otte, A. Nepomuk, Paul, Thomas C., Piotrowski, Lech W., Reno, Mary Hall, Sarazin, Fred, Shinozaki, Kenji, Soriano, Jorge F., Venters, Tonia M., and Wiencke, Lawrence

Subjects
High Energy Physics - Phenomenology, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We compare two different formalisms for modeling the energy deposition of macroscopically sized/massive quark nuggets (a.k.a. macros) in the Earth's atmosphere. We show that for a reference mass of 1 g, there is a discrepancy in the macro luminosity of about 14 orders of magnitude between the predictions of the two formalisms. Armed with our finding we estimate the sensitivity for macro detection at space-based (Mini-EUSO and POEMMA) and suborbital (EUSO-SPB2) experiments., Comment: 5 pages revtex, 3 figures

Published
2021
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19. EUSO-SPB2 sensitivity to macroscopic dark matter

Author

Paul, Thomas C., Reese, Sarah T., Anchordoqui, Luis A., Olinto, Angela V., and Chen, Thomas Y.

Subjects
High Energy Physics - Phenomenology, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Macroscopic dark matter (or macro) provides a broad class of alternative candidates to particle dark matter. These candidates would transfer energy primarily through elastic scattering, and this linear energy deposition would produce observable signals if a macro were to traverse the atmosphere. We study the fluorescence emission produced by a macro passing through the atmosphere. We estimate the sensitivity of EUSO-SPB2 to constrain the two-dimensional parameter space ($\sigma$ vs. $M$), where $M$ is the macro mass and $\sigma$ its cross sectional area., Comment: To be published in the Proceedings of the 37th International Cosmic Ray Conference (ICRC 2012), Berlin, 12 -23 July 2021

Published
2021

20. The Case for Probe-class NASA Astrophysics Missions

Author

Elvis, Martin, Arenberg, Jon, Ballantyne, David, Bautz, Mark, Beichman, Charles, Booth, Jeffrey, Buckley, James, Burns, Jack O., Camp, Jordan, Conti, Alberto, Cooray, Asantha, Danchi, William, Delabrouille, Jacques, De Zotti, Gianfranco, Flauger, Raphael, Glenn, Jason, Grindlay, Jonathan, Hanany, Shaul, Hartmann, Dieter, Helou, George, Herranz, Diego, Hubmayr, Johannes, Johnson, Bradley R., Jones, William, Kasdin, N. Jeremy, Kouvoliotou, Chryssa, Kunze, Kerstin E., Lawrence, Charles, Lazio, Joseph, Lipscy, Sarah, Lillie, Charles F., Maccarone, Tom, Madsen, Kristin C., Mushotzky, Richard, Olinto, Angela, Plavchan, Peter, Pogosian, Levon, Ptak, Andrew, Ray, Paul, Rocha, Graca M., Scowen, Paul, Seager, Sara, Tinto, Massimo, Tomsick, John, Tucker, Gregory., Ulmer, Mel, Wang, Yun, and Wollack, Edward J.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Astrophysics spans an enormous range of questions on scales from individual planets to the entire cosmos. To address the richness of 21st century astrophysics requires a corresponding richness of telescopes spanning all bands and all messengers. Much scientific benefit comes from having the multi-wavelength capability available at the same time. Most of these bands,or measurement sensitivities, require space-based missions. Historically, NASA has addressed this need for breadth with a small number of flagship-class missions and a larger number of Explorer missions. While the Explorer program continues to flourish, there is a large gap between Explorers and strategic missions. A fortunate combination of new astrophysics technologies with new, high capacity, low dollar-per-kg to orbit launchers, and new satellite buses allow for cheaper missions with capabilities approaching strategic mission levels. NASA has recognized these developments by calling for Probe-class mission ideas for mission studies, spanning most of the electromagnetic spectrum from GeV gamma-rays to the far infrared, and the new messengers of neutrinos and ultra-high energy cosmic rays. The key insight from the Probes exercise is that order-of-magnitude advances in science performance metrics are possible across the board for initial total cost estimates in the range 500M-1B dollars., Comment: Submitted to the Astro2020 Decadal Survey call for Activities, Projects or State of the Profession Consideration (APC). 10 pages

Published
2020

21. UCIRC2: An Infrared Cloud Monitor for EUSO-SPB2

Author

Diesing, Rebecca, Durojaiye, Khadijat, Flannery, Seamus, Mehling, Kameron, Friedlander, Noah, Bukowski, Alexa, Donovan, Emily, Meyer, Stephan, and Olinto, Angela V.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We describe the design and implementation of the University of Chicago Infrared Camera 2 (UCIRC2) built for monitoring cloud coverage during the EUSO-SPB2 flight (the second generation of the Extreme Universe Space Observatory on a Super Pressure Balloon). UCIRC2 uses two infrared (IR) cameras centered on 10$\mu$m and 12$\mu$m wavelengths to capture images of the clouds beneath EUSO-SPB2 in two bands spanning the thermal emission peak. Taken every minute, the IR images allow the determination of the height and coverage of clouds between the telescope and the ground. We discuss the design and construction of UCIRC2, including the techniques and design principles that make the module temperature and vacuum resilient. Additionally, we delineate the image reconstruction process and the pixel by pixel temperature calibration procedure. This paper will posit design and implementation suggestions for future ultra-high energy space telescopes., Comment: 8 pages, 5 figures, proceedings of the 36th International Cosmic Ray Conference (ICRC 2019)

Published
2019

22. A new calculation of Earth-skimming very- and ultra-high energy tau neutrinos

Author

Reno, Mary Hall, Venters, Tonia M., Krizmanic, John F., Anchordoqui, Luis A., Guepin, Claire, and Olinto, Angela V.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Cosmic neutrinos above a PeV are produced either within astrophysical sources or when ultra-high energy cosmic rays interact in transit through the cosmic background radiation. Detection of these neutrinos will be essential for understanding cosmic ray acceleration, composition and source evolution. By using the Earth as a tau neutrino converter for upward-going extensive air showers from tau decays, balloon-borne and space-based instruments can take advantage of a large volume and mass of the terrestrial neutrino target. The theoretical inputs and uncertainties in determining the tau lepton exit probabilities and their translation to detection acceptance will be discussed in the context of a new calculation we have performed. We quantify the experimental detection capability based on our calculation, including using the Probe of Extreme Multi-Messenger Astrophysics (POEMMA) concept study response parameters for optical air Cherenkov detection. These case studies are used to illustrate the features and uncertainties in upward tau air shower detection., Comment: 8 pages, 3 figures, Proceedings of the 36th International Cosmic Ray Conference (ICRC 2019), held July 24th - August 1st, 2019 in Madison, WI, USA

Published
2019

23. Performance and science reach of POEMMA for ultrahigh-energy particles

Author

Anchordoqui, Luis A., Bergman, Douglas R., Bertaina, Mario E., Fenu, Francesco, Krizmanic, John F., Liberatore, Alessandro, Olinto, Angela V., Reno, Mary Hall, Sarazin, Fred, Shinozaki, Kenji, Soriano, Jorge F., Ulrich, Ralf, Unger, Michael, Venters, Tonia M., and Wiencke, Lawrence

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
Abstract

The Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) is a potential NASA Astrophysics Probe-class mission designed to observe ultra-high energy cosmic rays (UHECRs) and cosmic neutrinos from space. POEMMA will monitor colossal volumes of the Earth's atmosphere to detect extensive air showers (EASs) produced by extremely energetic cosmic messengers: UHECRs above 20 EeV over the full sky and cosmic neutrinos above 20 PeV. We focus most of this study on the impact of POEMMA for UHECR science by simulating the detector response and mission performance for EAS from UHECRs. We show that POEMMA will provide a significant increase in the statistics of observed UHECRs at the highest energies over the entire sky. POEMMA will be the first UHECR fluorescence detector deployed in space that will provide high-quality stereoscopic observations of the longitudinal development of air showers. Therefore, it will be able to provide event-by-event estimates of the calorimetric energy and nuclear mass of UHECRs. The particle physics in the interactions limits the interpretation of the shower maximum on an event by event basis. In contrast, the calorimetric energy measurement is significantly less sensitive to the different possible final states in the early interactions. We study the prospects to discover the origin and nature of UHECRs using expectations for measurements of the energy spectrum, the distribution of arrival direction, and the atmospheric column depth at which the EAS longitudinal development reaches maximum. We also explore supplementary science capabilities of POEMMA through its sensitivity to particle interactions at extreme energies and its ability to detect ultra-high energy neutrinos and photons produced by top-down models including cosmic strings and super-heavy dark matter particle decay in the halo of the Milky Way., Comment: 40 pages revtex, with 42 figures

Published
2019
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24. POEMMA's Target of Opportunity Sensitivity to Cosmic Neutrino Transient Sources

Author

Venters, Tonia M., Reno, Mary Hall, Krizmanic, John F., Anchordoqui, Luis A., Guépin, Claire, and Olinto, Angela V.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
Abstract

We investigate the capability of the Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) in performing Target-of-Opportunity (ToO) neutrino observations. POEMMA will detect tau neutrinos via Cherenkov radiation from their upward-moving extensive air showers. POEMMA will be able to quickly slew ($90^{\circ}$ in 500 s) to the direction of an astrophysical source, which in combination with its orbital speed will provide it with unparalleled capability to follow up transient alerts. We calculate POEMMA's transient sensitivity for two observational modes for its two satellites (ToO-stereo and ToO-dual) and investigate variations in neutrino sensitivity across the sky arising from POEMMA's orbit. We explore separate scenarios for long ($\sim 10^{6}$ s) and short ($\sim 10^3$ s) bursts, accounting for intrusion from the Sun and the Moon in long-duration scenarios. For long bursts, POEMMA will improve the average neutrino sensitivity above 300 PeV by up to a factor of 7 with respect to existing experiments (e.g., IceCube, ANTARES, and Pierre Auger), reaching the level of model predictions for neutrino fluences at these energies from several types of long-duration astrophysical transients (e.g., binary neutron star mergers and tidal disruption events). For short bursts in the optimal case, POEMMA will improve the sensitivity over existing experiments by at least an order of magnitude above 100 PeV. POEMMA's orbit and rapid slewing will provide access to the full celestial sky, including regions not accessible to ground-based experiments. Finally, we discuss the prospects for detecting neutrinos from candidate astrophysical neutrino sources in the nearby universe. Our results demonstrate that with its improved neutrino sensitivity at ultra-high energies and unique full-sky coverage, POEMMA will be an essential component in an expanding multi-messenger network., Comment: 39 pages (18.5 main + 20.5 appendices and references), 18 figures; submitted to Phys. Rev. D

Published
2019
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25. Open Questions in Cosmic-Ray Research at Ultrahigh Energies

Author

Batista, Rafael Alves, Biteau, Jonathan, Bustamante, Mauricio, Dolag, Klaus, Engel, Ralph, Fang, Ke, Kampert, Karl-Heinz, Kostunin, Dmitriy, Mostafa, Miguel, Murase, Kohta, Sigl, Günter, Oikonomou, Foteini, Olinto, Angela V., Panasyuk, Mikhail I., Taylor, Andrew, and Unger, Michael

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We review open questions and prospects for progress in ultrahigh-energy cosmic ray (UHECR) research, based on a series of discussions that took place during the `The High-Energy Universe: Gamma-Ray, Neutrino, and Cosmic-ray Astronomy' MIAPP workshop in 2018. Specifically, we overview open questions on the origin of the bulk of UHECRs, the UHECR mass composition, the origin of the end of the cosmic-ray spectrum, the transition from Galactic to extragalactic cosmic rays, the effect of magnetic fields on the trajectories of UHECRs, anisotropy expectations for specific astrophysical scenarios, hadronic interactions, and prospects for discovering neutral particles as well as new physics at ultrahigh energies. We also briefly present upcoming and proposed UHECR experiments and discuss their projected science reach., Comment: 47 pages, 17 figures, Review to appear in "Frontiers in Astronomy and Space Science" special issue, "Multi-Messenger Astrophysics: New Windows to the Universe"

Published
2019
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26. Astrophysics Uniquely Enabled by Observations of High-Energy Cosmic Neutrinos

Author

Ackermann, Markus, Ahlers, Markus, Anchordoqui, Luis, Bustamante, Mauricio, Connolly, Amy, Deaconu, Cosmin, Grant, Darren, Gorham, Peter, Halzen, Francis, Karle, Albrecht, Kotera, Kumiko, Kowalski, Marek, Mostafa, Miguel A., Murase, Kohta, Nelles, Anna, Olinto, Angela, Romero-Wolf, Andres, Vieregg, Abigail, and Wissel, Stephanie

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology
Abstract

High-energy cosmic neutrinos carry unique information about the most energetic non-thermal sources in the Universe. This white paper describes the outstanding astrophysics questions that neutrino astronomy can address in the coming decade. A companion white paper discusses how the observation of cosmic neutrinos can address open questions in fundamental physics. Detailed measurements of the diffuse neutrino flux, measurements of neutrinos from point sources, and multi-messenger observations with neutrinos will enable the discovery and characterization of the most energetic sources in the Universe., Comment: White paper for the Astro2020 US decadal survey. Companion paper: "Fundamental Physics with High-Energy Cosmic Neutrinos" (1903.04333). Corresponding Authors: Markus Ahlers, Albrecht Karle, Kohta Murase, Anna Nelles, Andres Romero-Wolf, Abigail Vieregg

Published
2019

27. Fundamental Physics with High-Energy Cosmic Neutrinos

Author

Ackermann, Markus, Ahlers, Markus, Anchordoqui, Luis, Bustamante, Mauricio, Connolly, Amy, Deaconu, Cosmin, Grant, Darren, Gorham, Peter, Halzen, Francis, Karle, Albrecht, Kotera, Kumiko, Kowalski, Marek, Mostafa, Miguel A., Murase, Kohta, Nelles, Anna, Olinto, Angela, Romero-Wolf, Andres, Vieregg, Abigail, and Wissel, Stephanie

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology
Abstract

High-energy cosmic neutrinos can reveal new fundamental particles and interactions, probing energy and distance scales far exceeding those accessible in the laboratory. This white paper describes the outstanding particle physics questions that high-energy cosmic neutrinos can address in the coming decade. A companion white paper discusses how the observation of cosmic neutrinos can address open questions in astrophysics. Tests of fundamental physics using high-energy cosmic neutrinos will be enabled by detailed measurements of their energy spectrum, arrival directions, flavor composition, and timing., Comment: White paper for the Astro2020 US decadal survey. Companion paper: "Astrophysics Uniquely Enabled by Observations of High-Energy Cosmic Neutrinos" (1903.04334). Corresponding Authors: Luis Anchordoqui, Mauricio Bustamante, Darren Grant, Andres Romero-Wolf, Abigail Vieregg, Stephanie Wissel

Published
2019

28. What is the nature and origin of the highest-energy particles in the universe?

Author

Sarazin, Fred, Anchordoqui, Luis, Beatty, James, Bergman, Douglas, Covault, Corbin, Farrar, Glennys, Krizmanic, John, Nitz, David, Olinto, Angela, Unger, Michael, Tinyakov, Peter, and Wiencke, Lawrence

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

This white paper was submitted to the US Astronomy and Astrophysics Decadal Survey (Astro2020) and defines the science questions to be answered in the next decade in the field of Ultra-High Energy Cosmic-Rays. Following a review of the recent experimental and theoretical advances in the field, the paper outlines strategies and requirements desirable for the design of future experiments., Comment: 5 pages, 3 figures

Published
2019

29. Geometrical Constraints of Observing Very High Energy Earth-Skimming Neutrinos from Space

Author

Guépin, Claire, Sarazin, Frédéric, Krizmanic, John, Loerincs, Jacqueline, Olinto, Angela, and Piccone, Ashley

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The detection of very-high-energy (VHE) neutrinos ($E_\nu \gtrsim 10$ PeV) is a challenge that future generations of experiments are being designed and constructed to address. One promising method relies on using the Earth as a neutrino target for indirect detection of skimming tau neutrinos interacting within the Earth and producing tau leptons that are able to escape and decay in the atmosphere. The tau decay produces upward-moving Extensive Air Showers (EASs). A space-based or suborbital instrument observing the ground near the Earth limb can search for the beamed Cherenkov signal produced by the up-going EAS resulting from the tau-lepton decay. In this paper, we derive the geometrical constraints for such an observation in general and for the specific case of the Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) mission currently under study, focusing on the Cherenkov signal detection. We show that, using reasonable orbital parameters, POEMMA can achieve full-sky coverage to search for potential neutrino sources over the length of its mission. We also show that follow-up of a transient Target-of-Opportunity (ToO), such as a flaring source, can be achieved within an orbit time scale depending on the source location on the celestial sphere and its relative position with respect to the Sun and the Moon., Comment: 18 pages, 13 figures, submitted to JCAP, comments welcome

Published
2018
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30. Ultrahigh-Energy Cosmic Ray Composition from the Distribution of Arrival Directions

Author

Anjos, Rita C. dos, Soriano, Jorge F., Anchordoqui, Luis A., Paul, Thomas C., Torres, Diego F., Krizmanic, John F., Paglione, Timothy A. D., Moncada, Roberto J., Sarazin, Frederic, Wiencke, Lawrence, and Olinto, Angela V.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The sources of ultrahigh-energy cosmic rays (UHECRs) have been difficult to catch. It was recently pointed out that while sources of UHECR protons exhibit anisotropy patterns that become denser and compressed with rising energy, nucleus-emitting-sources give rise to a cepa stratis (onion-like) structure with layers that become more distant from the source position with rising energy. The peculiar shape of the hot spots from nucleus-accelerators is steered by the competition between energy loss during propagation and deflection on the Galactic magnetic field (GMF). Here, we run a full-blown simulation study to accurately characterize the deflections of UHECR nuclei in the GMF. We show that while the cepa stratis structure provides a global description of anisotropy patterns produced by UHECR nuclei en route to Earth, the hot spots are elongated depending on their location in the sky due to the regular structure of the GMF. We demonstrate that with a high-statistics sample at the high-energy-end of the spectrum, like the one to be collected by NASA's POEMMA mission, the energy dependence of the hot-spot contours could become a useful observable to identify the nuclear composition of UHECRs. This new method to determine the nature of the particle species is complementary to those using observables of extensive air showers, and therefore is unaffected by the large systematic uncertainties of hadronic interaction models., Comment: Matching version published in PRD

Published
2018
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31. White paper on EUSO-SPB2

Author

Adams Jr., James H., Anchordoqui, Luis A., Apple, Jeffrey A., Bertaina, Mario E., Christl, Mark J., Fenu, Francesco, Kuznetsov, Evgeny, Neronov, Andrii, Olinto, Angela V., Parizot, Etienne, Paul, Thomas C., Prevot, Guillaume, Reardon, Patrick, Vovk, Ievgen, Wiencke, Lawrence, and Young, Roy M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

EUSO-SPB2 is a second generation Extreme Universe Space Observatory (EUSO) on a Super-Pressure Balloon (SPB). This document describes the physics capabilities, the proposed technical design of the instruments, and the simulation and analysis software., Comment: References added

Published
2017

32. The NUSES space mission

Author

Trimarelli, Caterina, primary, Aloisio, Roberto, additional, Altomare, Altomare, additional, Barbato, Barbato, additional, Battiston, Battiston, additional, Bertania, Bertania, additional, Bissaldi, Bissaldi, additional, Boncioli, Boncioli, additional, Burmistrov, Burmistrov, additional, Cagnoli, Cagnoli, additional, Casolino, Casolino, additional, Cummings, Austin, additional, D'Ambrosio, Nicola, additional, De Mitri, Ivan, additional, De Robertis, Giuseppe, additional, De Santis, Cristian, additional, Di Giovanni, Adriano, additional, Di Salvo, Andrea, additional, Di Santo, Margherita, additional, Di Venere, Leonardo, additional, Eser, Johannes, additional, Fernandez Alonso, Mateo, additional, Fontanella, Giulio, additional, Fusco, Piergiorgio, additional, Garbolino, Sara, additional, Gargano, Fabio, additional, Giampaolo, Giampaolo, additional, Giliberti, Mario, additional, Guarino, Fausto, additional, Heller, Matthieu, additional, Iuppa, Roberto, additional, Krizmanic, John, additional, Lega, Alessandro, additional, Licciulli, Francesco, additional, Loparco, Loparco, additional, Lorusso, Leonarda, additional, Mariotti, Mosè, additional, Mazziotta, Nicola, additional, Mese, Marco, additional, Miyamoto, Hiroko, additional, Montaruli, Teresa, additional, Nagai, Adrii, additional, Nicolaidis, Riccardo, additional, Nozzoli, Nozzoli, additional, Olinto, Angela, additional, Orlandi, Donato, additional, Osteria, Giuseppe, additional, Palmieri, Piero, additional, Panico, Beatrice, additional, Panzarini, Giuliana, additional, Parenti, Andrea, additional, Perrone, Lorenzo, additional, Picozza, Piergiorgio, additional, Pillera, Roberta, additional, Rando, Riccardo, additional, Rinaldi, Marianna, additional, Rivetti, Angelo, additional, Rizi, Vicenzo, additional, Salamida, Francesco, additional, Santero Mormile, Edoardo, additional, Scherini, Viviana, additional, Scotti, Valentina, additional, Serini, Davide, additional, Siddique, Iqra, additional, Silveri, Leandro, additional, Smirnov, Aleksei, additional, Sparvoli, Roberta, additional, Tedesco, Silvia, additional, Wu, Libo, additional, Zuccon, Paolo, additional, and Zugravel, Stefan, additional

Published
2024
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33. Refined STACK-CNN for Meteor and Space Debris Detection in Highly Variable Backgrounds

Author

Olivi, Leonardo, primary, Montanaro, Antonio, additional, Bertaina, Mario Edoardo, additional, Coretti, Antonio Giulio, additional, Barghini, Dario, additional, Battisti, Matteo, additional, Belov, Alexander, additional, Bianciotto, Marta, additional, Bisconti, Francesca, additional, Blaksley, Carl, additional, Blin, Sylvie, additional, Bolmgren, Karl, additional, Cambié, Giorgio, additional, Capel, Francesca, additional, Casolino, Marco, additional, Churilo, Igor, additional, Crisconio, Marino, additional, Taille, Christophe De La, additional, Ebisuzaki, Toshikazu, additional, Eser, Johannes, additional, Fenu, Francesco, additional, Filippatos, George, additional, Franceschi, Massimo Alberto, additional, Fuglesang, Christer, additional, Golzio, Alessio, additional, Gorodetzky, Philippe, additional, Kajino, Fumiyoshi, additional, Kasuga, Hiroshi, additional, Klimov, Pavel, additional, Kungel, Viktoria, additional, Kuznetsov, Vladimir, additional, Manfrin, Massimiliano, additional, Marcelli, Laura, additional, Mascetti, Gabriele, additional, Marszał, Włodzimierz, additional, Mignone, Marco, additional, Miyamoto, Hiroko, additional, Murashov, Alexey, additional, Napolitano, Tommaso, additional, Ohmori, Hitoshi, additional, Olinto, Angela, additional, Parizot, Etienne, additional, Picozz, Piergiorgio, additional, Piotrowski, Lech Wiktor, additional, PlebaniakGuillaume, Zbigniew, additional, Prévôt, Guillaume, additional, Reali, Enzo, additional, Ricci, Marco, additional, RomoliGuillaume, Giulia, additional, Sakaki, Naoto, additional, Sharakin, Sergei, additional, Shinozaki, Kenji, additional, Szabelski, Jacek, additional, Takizawa, Yoshiyuki, additional, Vagelli, Valerio, additional, Valentini, Giovanni, additional, Vrabel, Michal, additional, Wiencke, Lawrence, additional, and Zotov, Mikhail, additional

Published
2024
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34. High-energy neutrinos from sources in clusters of galaxies

Author

Fang, Ke and Olinto, Angela V.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

High-energy cosmic rays can be accelerated in clusters of galaxies, by mega-parsec scale shocks induced by accretion of gas during the formation of large-scale structure, or by powerful sources harbored in clusters. Once accelerated, the highest energy particles leave the cluster via almost rectilinear trajectories, while lower energy ones can be confined by the cluster magnetic field up to cosmological time and interact with the intracluster gas. Using a realistic model of the baryon distribution and the turbulent magnetic field in clusters, we studied the propagation and hadronic interaction of high-energy protons in the intracluster medium. We report the cumulative cosmic ray and neutrino spectra generated by galaxy clusters including embedded sources, and demonstrate that clusters can contribute a significant fraction of the observed IceCube neutrinos above 30 TeV while remaining undetected in high-energy cosmic rays and $\gamma$ rays for reasonable choices of parameters and source scenarios., Comment: 9 pages, 3 figures, accepted for publication in ApJ

Published
2016
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35. Measurement of the Radiation Energy in the Radio Signal of Extensive Air Showers as a Universal Estimator of Cosmic-Ray Energy

Author

The Pierre Auger Collaboration, Aab, Alexander, Abreu, Pedro, Aglietta, Marco, Ahn, Eun-Joo, Samarai, Imen Al, Albuquerque, Ivone, Allekotte, Ingomar, Allison, Patrick, Almela, Alejandro, Castillo, Jesus Alvarez, Alvarez-Muñiz, Jaime, Batista, Rafael Alves, Ambrosio, Michelangelo, Aminaei, Amin, Anastasi, Gioacchino Alex, Anchordoqui, Luis, Andringa, Sofia, Aramo, Carla, Arqueros, Fernando, Arsene, Nicusor, Asorey, Hernán Gonzalo, Assis, Pedro, Aublin, Julien, Avila, Gualberto, Awal, Nafiun, Badescu, Alina Mihaela, Baus, Colin, Beatty, Jim, Becker, Karl Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter, Billoir, Pierre, Blaess, Simon G., Blanco, Alberto, Blanco, Miguel, Blazek, Jiri, Bleve, Carla, Blümer, Hans, Boháčová, Martina, Boncioli, Denise, Bonifazi, Carla, Borodai, Nataliia, Brack, Jeffrey, Brancus, Iliana, Bretz, Thomas, Bridgeman, Ariel, Brogueira, Pedro, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Caballero-Mora, Karen S., Caccianiga, Barbara, Caccianiga, Lorenzo, Candusso, Marina, Caramete, Laurentiu, Caruso, Rossella, Castellina, Antonella, Cataldi, Gabriella, Cazon, Lorenzo, Cester, Rosanna, Chavez, Alan G., Chiavassa, Andrea, Chinellato, Jose Augusto, Chudoba, Jiri, Cilmo, Marco, Clay, Roger W, Cocciolo, Giuseppe, Colalillo, Roberta, Coleman, Alan, Collica, Laura, Coluccia, Maria Rita, Conceição, Ruben, Contreras, Fernando, Cooper, Mathew J., Cordier, Alain, Coutu, Stephane, Covault, Corbin, Cronin, James, Dallier, Richard, Daniel, Bruno, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., de Almeida, Rogerio M., de Jong, Sijbrand J., De Mauro, Giuseppe, Neto, Joao de Mello, De Mitri, Ivan, de Oliveira, Jaime, de Souza, Vitor, del Peral, Luis, Deligny, Olivier, Dhital, Niraj, Di Giulio, Claudio, Di Matteo, Armando, Diaz, Johana Chirinos, Castro, Mary Lucia Díaz, Diogo, Francisco, Dobrigkeit, Carola, Docters, Wendy, D'Olivo, Juan Carlos, Dorofeev, Alexei, Hasankiadeh, Qader Dorosti, Anjos, Rita dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Erdmann, Martin, Erfani, Mona, Escobar, Carlos O., Espadanal, Joao, Etchegoyen, Alberto, Falcke, Heino, Fang, Ke, Farrar, Glennys, Fauth, Anderson, Fazzini, Norberto, Ferguson, Andrew P., Fick, Brian, Figueira, Juan Manuel, Filevich, Alberto, Filipčič, Andrej, Fratu, Octavian, Freire, Martín Miguel, Fujii, Toshihiro, García, Beatriz, Garcia-Gamez, Diego, Garcia-Pinto, Diego, Gate, Florian, Gemmeke, Hartmut, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, Giaccari, Ugo, Giammarchi, Marco, Giller, Maria, Głas, Dariusz, Glaser, Christian, Glass, Henry, Golup, Geraldina, Berisso, Mariano Gómez, Vitale, Primo F. Gómez, González, Nicolás, Gookin, Ben, Gordon, Jacob, Gorgi, Alessio, Gorham, Peter, Gouffon, Philippe, Griffith, Nathan, Grillo, Aurelio, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Hampel, Matías Rolf, Hansen, Patricia, Harari, Diego, Harrison, Thomas A., Hartmann, Sebastian, Harton, John, Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Heimann, Philipp, Herve, Alexander E., Hill, Gary C., Hojvat, Carlos, Hollon, Nicholas, Holt, Ewa, Homola, Piotr, Hörandel, Jörg, Horvath, Pavel, Hrabovský, Miroslav, Huber, Daniel, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Jandt, Ingolf, Jansen, Stefan, Jarne, Cecilia, Johnsen, Jeffrey A., Josebachuili, Mariela, Kääpä, Alex, Kambeitz, Olga, Kampert, Karl Heinz, Kasper, Peter, Katkov, Igor, Keilhauer, Bianca, Kemp, Ernesto, Kieckhafer, Roger, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Krause, Raphael, Krohm, Nicole, Kuempel, Daniel, Mezek, Gasper Kukec, Kunka, Norbert, Awad, Alaa Metwaly Kuotb, LaHurd, Danielle, Latronico, Luca, Lauer, Robert, Lauscher, Markus, Lautridou, Pascal, Coz, Sandra Le, Lebrun, Didier, Lebrun, Paul, de Oliveira, Marcelo Augusto Leigui, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Link, Katrin, Lopes, Luis, López, Rebeca, Casado, Aida López, Louedec, Karim, Lucero, Agustin, Malacari, Max, Mallamaci, Manuela, Maller, Jennifer, Mandat, Dusan, Mantsch, Paul, Mariazzi, Analisa, Marin, Vincent, Mariş, Ioana, Marsella, Giovanni, Martello, Daniele, Martinez, Humberto, Bravo, Oscar Martínez, Martraire, Diane, Meza, Jimmy Masías, Mathes, Hermann-Josef, Mathys, Sebastian, Matthews, James, Matthews, John, Matthiae, Giorgio, Maurizio, Daniela, Mayotte, Eric, Mazur, Peter, Medina, Carlos, Medina-Tanco, Gustavo, Meissner, Rebecca, Mello, Victor, Melo, Diego, Menshikov, Alexander, Messina, Stefano, Micheletti, Maria Isabel, Middendorf, Lukas, Minaya, Ignacio A., Miramonti, Lino, Mitrica, Bogdan, Molina-Bueno, Laura, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafá, Miguel, Moura, Celio A., Muller, Marcio Aparecido, Müller, Gero, Müller, Sarah, Navas, Sergio, Necesal, Petr, Nellen, Lukas, Nelles, Anna, Neuser, Jens, Nguyen, Phong H., Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Niemietz, Lukas, Niggemann, Tim, Nitz, Dave, Nosek, Dalibor, Novotny, Vladimir, Nožka, Lyberis, Núñez, Luis, Ochilo, Livingstone, Oikonomou, Foteini, Olinto, Angela, Pacheco, Noelia, Selmi-Dei, Daniel Pakk, Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Paul, Thomas, Pech, Miroslav, Pękala, Jan, Pelayo, Rodrigo, Pepe, Iuri, Perrone, Lorenzo, Petermann, Emily, Peters, Christine, Petrera, Sergio, Petrov, Yevgeniy, Phuntsok, Jamyang, Piegaia, Ricardo, Pierog, Tanguy, Pieroni, Pablo, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Plum, Matthias, Porcelli, Alessio, Porowski, Czeslaw, Prado, Raul Ribeiro, Privitera, Paolo, Prouza, Michael, Quel, Eduardo J, Querchfeld, Sven, Quinn, Sean, Rautenberg, Julian, Ravel, Olivier, Ravignani, Diego, Reinert, Darius, Revenu, Benoît, Ridky, Jan, Risse, Markus, Ristori, Pablo, Rizi, Vincenzo, de Carvalho, Washington Rodrigues, Rojo, Jorge Rubén Rodriguez, Rodríguez-Frías, Maria Dolores, Rogozin, Dmytro, Rosado, Jaime, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Saffi, Steven J., Saftoiu, Alexandra, Salazar, Humberto, Saleh, Ahmed, Greus, Francisco Salesa, Salina, Gaetano, Gomez, Jose Sanabria, Sánchez, Federico, Sanchez-Lucas, Patricia, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarkar, Biswaijt, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Scarso, Carlos, Schauer, Markus, Scherini, Viviana, Schieler, Harald, Schmidt, David, Scholten, Olaf, Schoorlemmer, Harm, Schovánek, Petr, Schröder, Frank G., Schulz, Alexander, Schulz, Johannes, Schumacher, Johannes, Sciutto, Sergio, Segreto, Alberto, Settimo, Mariangela, Shadkam, Amir, Shellard, Ronald C., Sigl, Guenter, Sima, Octavian, Śmiałkowski, Andrzej, Šmída, Radomir, Snow, Gregory, Sommers, Paul, Sonntag, Sebastian, Sorokin, J., Squartini, Ruben, Srivastava, Yogendra N., Stanca, Denis, Stanič, Samo, Stapleton, James, Stasielak, Jaroslaw, Stephan, Maurice, Stutz, Anne, Suarez, Federico, Durán, Mauricio Suarez, Suomijärvi, Tiina, Supanitsky, A. Daniel, Sutherland, Michael, Swain, John, Szadkowski, Zbigniew, Taborda, Oscar Alejandro, Tapia, Alex, Tepe, Andreas, Theodoro, Vanessa Menezes, Timmermans, Charles, Peixoto, Carlos J. Todero, Toma, Gabriel, Tomankova, Lenka, Tomé, Bernardo, Tonachini, Aurelio, Elipe, Guillermo Torralba, Machado, Diego Torres, Travnicek, Petr, Trini, Marta, Ulrich, Ralf, Unger, Michael, Urban, Martin, Galicia, Jose F. Valdés, Valiño, Ines, Valore, Laura, van Aar, Guus, van Bodegom, Patrick, Berg, Ad M. van den, van Velzen, Sjoert, van Vliet, Arjen, Varela, Enrique, Cárdenas, Bernardo Vargas, Varner, Gary, Vasquez, Rafael, Vázquez, Jose R., Vázquez, Ricardo, Veberič, Darko, Verzi, Valerio, Vicha, Jakub, Videla, Mariela, Villaseñor, Luis, Vlcek, Brian, Vorobiov, Serguei, Wahlberg, Hernan, Wainberg, Oscar, Walz, David, Watson, Alan, Weber, Marc, Weidenhaupt, Klaus, Weindl, Andreas, Welling, Christoph, Werner, Felix, Widom, Allan, Wiencke, Lawrence, Wilczyński, Henryk, Winchen, Tobias, Wittkowski, David, Wundheiler, Brian, Wykes, Sarka, Yang, Lili, Yapici, Tolga, Yushkov, Alexey, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, Zepeda, Arnulfo, Zimmermann, Benedikt, Ziolkowski, Michael, and Zuccarello, Francesca

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment
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 \pm 0.7 (stat) \pm 6.7 (sys) 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-principle 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., Comment: Replaced with published version. Added journal reference and DOI. Supplemental material in the ancillary files

Published
2016
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36. IceCube Constraints on Fast-Spinning Pulsars as High-Energy Neutrino Sources

Author

Fang, Ke, Kotera, Kumiko, Murase, Kohta, and Olinto, Angela V.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Relativistic winds of fast-spinning pulsars have been proposed as a potential site for cosmic-ray acceleration from very high energies (VHE) to ultrahigh energies (UHE). We re-examine conditions for high-energy neutrino production, considering the interaction of accelerated particles with baryons of the expanding supernova ejecta and the radiation fields in the wind nebula. We make use of the current IceCube sensitivity in diffusive high-energy neutrino background, in order to constrain the parameter space of the most extreme neutron stars as sources of VHE and UHE cosmic rays. We demonstrate that the current non-observation of $10^{18}$ eV neutrinos put stringent constraints on the pulsar scenario. For a given model, birthrates, ejecta mass and acceleration efficiency of the magnetar sources can be constrained. When we assume a proton cosmic ray composition and spherical supernovae ejecta, we find that the IceCube limits almost exclude their significant contribution to the observed UHE cosmic-ray flux. Furthermore, we consider scenarios where a fraction of cosmic rays can escape from jet-like structures piercing the ejecta, without significant interactions. Such scenarios would enable the production of UHE cosmic rays and help remove the tension between their EeV neutrino production and the observational data., Comment: 23 pages, 8 figures; published in JCAP04(2016)010

Published
2015
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37. Energy Estimation of Cosmic Rays with the Engineering Radio Array of the Pierre Auger Observatory

Author

The Pierre Auger Collaboration, Aab, Alexander, Abreu, Pedro, Aglietta, Marco, Ahn, Eun-Joo, Samarai, Imen Al, Albuquerque, Ivone, Allekotte, Ingomar, Allison, Patrick, Almela, Alejandro, Castillo, Jesus Alvarez, Alvarez-Muñiz, Jaime, Batista, Rafael Alves, Ambrosio, Michelangelo, Aminaei, Amin, Anastasi, Gioacchino Alex, Anchordoqui, Luis, Andringa, Sofia, Aramo, Carla, Arqueros, Fernando, Arsene, Nicusor, Asorey, Hernán Gonzalo, Assis, Pedro, Aublin, Julien, Avila, Gualberto, Awal, Nafiun, Badescu, Alina Mihaela, Baus, Colin, Beatty, Jim, Becker, Karl Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter, Billoir, Pierre, Blaess, Simon G., Blanco, Alberto, Blanco, Miguel, Blazek, Jiri, Bleve, Carla, Blümer, Hans, Boháčová, Martina, Boncioli, Denise, Bonifazi, Carla, Borodai, Nataliia, Brack, Jeffrey, Brancus, Iliana, Bretz, Thomas, Bridgeman, Ariel, Brogueira, Pedro, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Caballero-Mora, Karen S., Caccianiga, Barbara, Caccianiga, Lorenzo, Candusso, Marina, Caramete, Laurentiu, Caruso, Rossella, Castellina, Antonella, Cataldi, Gabriella, Cazon, Lorenzo, Cester, Rosanna, Chavez, Alan G., Chiavassa, Andrea, Chinellato, Jose Augusto, Chudoba, Jiri, Cilmo, Marco, Clay, Roger W, Cocciolo, Giuseppe, Colalillo, Roberta, Coleman, Alan, Collica, Laura, Coluccia, Maria Rita, Conceição, Ruben, Contreras, Fernando, Cooper, Mathew J., Cordier, Alain, Coutu, Stephane, Covault, Corbin, Cronin, James, Dallier, Richard, Daniel, Bruno, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., de Almeida, Rogerio M., de Jong, Sijbrand J., De Mauro, Giuseppe, Neto, Joao de Mello, De Mitri, Ivan, de Oliveira, Jaime, de Souza, Vitor, del Peral, Luis, Deligny, Olivier, Dhital, Niraj, Di Giulio, Claudio, Di Matteo, Armando, Diaz, Johana Chirinos, Castro, Mary Lucia Díaz, Diogo, Francisco, Dobrigkeit, Carola, Docters, Wendy, D'Olivo, Juan Carlos, Dorofeev, Alexei, Hasankiadeh, Qader Dorosti, Anjos, Rita dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Erdmann, Martin, Erfani, Mona, Escobar, Carlos O., Espadanal, Joao, Etchegoyen, Alberto, Falcke, Heino, Fang, Ke, Farrar, Glennys, Fauth, Anderson, Fazzini, Norberto, Ferguson, Andrew P., Fick, Brian, Figueira, Juan Manuel, Filevich, Alberto, Filipčič, Andrej, Fratu, Octavian, Freire, Martín Miguel, Fujii, Toshihiro, García, Beatriz, Garcia-Gamez, Diego, Garcia-Pinto, Diego, Gate, Florian, Gemmeke, Hartmut, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, Giaccari, Ugo, Giammarchi, Marco, Giller, Maria, Głas, Dariusz, Glaser, Christian, Glass, Henry, Golup, Geraldina, Berisso, Mariano Gómez, Vitale, Primo F. Gómez, González, Nicolás, Gookin, Ben, Gordon, Jacob, Gorgi, Alessio, Gorham, Peter, Gouffon, Philippe, Griffith, Nathan, Grillo, Aurelio, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Hampel, Matías Rolf, Hansen, Patricia, Harari, Diego, Harrison, Thomas A., Hartmann, Sebastian, Harton, John, Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Heimann, Philipp, Herve, Alexander E., Hill, Gary C., Hojvat, Carlos, Hollon, Nicholas, Holt, Ewa, Homola, Piotr, Hörandel, Jörg, Horvath, Pavel, Hrabovský, Miroslav, Huber, Daniel, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Jandt, Ingolf, Jansen, Stefan, Jarne, Cecilia, Johnsen, Jeffrey A., Josebachuili, Mariela, Kääpä, Alex, Kambeitz, Olga, Kampert, Karl Heinz, Kasper, Peter, Katkov, Igor, Keilhauer, Bianca, Kemp, Ernesto, Kieckhafer, Roger, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Krause, Raphael, Krohm, Nicole, Kuempel, Daniel, Mezek, Gasper Kukec, Kunka, Norbert, Awad, Alaa Metwaly Kuotb, LaHurd, Danielle, Latronico, Luca, Lauer, Robert, Lauscher, Markus, Lautridou, Pascal, Coz, Sandra Le, Lebrun, Didier, Lebrun, Paul, de Oliveira, Marcelo Augusto Leigui, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Link, Katrin, Lopes, Luis, López, Rebeca, Casado, Aida López, Louedec, Karim, Lucero, Agustin, Malacari, Max, Mallamaci, Manuela, Maller, Jennifer, Mandat, Dusan, Mantsch, Paul, Mariazzi, Analisa, Marin, Vincent, Mariş, Ioana, Marsella, Giovanni, Martello, Daniele, Martinez, Humberto, Bravo, Oscar Martínez, Martraire, Diane, Meza, Jimmy Masías, Mathes, Hermann-Josef, Mathys, Sebastian, Matthews, James, Matthews, John, Matthiae, Giorgio, Maurizio, Daniela, Mayotte, Eric, Mazur, Peter, Medina, Carlos, Medina-Tanco, Gustavo, Meissner, Rebecca, Mello, Victor, Melo, Diego, Menshikov, Alexander, Messina, Stefano, Micheletti, Maria Isabel, Middendorf, Lukas, Minaya, Ignacio A., Miramonti, Lino, Mitrica, Bogdan, Molina-Bueno, Laura, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafá, Miguel, Moura, Celio A., Muller, Marcio Aparecido, Müller, Gero, Müller, Sarah, Navas, Sergio, Necesal, Petr, Nellen, Lukas, Nelles, Anna, Neuser, Jens, Nguyen, Phong H., Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Niemietz, Lukas, Niggemann, Tim, Nitz, Dave, Nosek, Dalibor, Novotny, Vladimir, Nožka, Lyberis, Núñez, Luis, Ochilo, Livingstone, Oikonomou, Foteini, Olinto, Angela, Pacheco, Noelia, Selmi-Dei, Daniel Pakk, Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Paul, Thomas, Pech, Miroslav, Pękala, Jan, Pelayo, Rodrigo, Pepe, Iuri, Perrone, Lorenzo, Petermann, Emily, Peters, Christine, Petrera, Sergio, Petrov, Yevgeniy, Phuntsok, Jamyang, Piegaia, Ricardo, Pierog, Tanguy, Pieroni, Pablo, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Plum, Matthias, Porcelli, Alessio, Porowski, Czeslaw, Prado, Raul Ribeiro, Privitera, Paolo, Prouza, Michael, Quel, Eduardo J, Querchfeld, Sven, Quinn, Sean, Rautenberg, Julian, Ravel, Olivier, Ravignani, Diego, Reinert, Darius, Revenu, Benoît, Ridky, Jan, Risse, Markus, Ristori, Pablo, Rizi, Vincenzo, de Carvalho, Washington Rodrigues, Rojo, Jorge Rubén Rodriguez, Rodríguez-Frías, Maria Dolores, Rogozin, Dmytro, Rosado, Jaime, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Saffi, Steven J., Saftoiu, Alexandra, Salazar, Humberto, Saleh, Ahmed, Greus, Francisco Salesa, Salina, Gaetano, Gomez, Jose Sanabria, Sánchez, Federico, Sanchez-Lucas, Patricia, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarkar, Biswaijt, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Scarso, Carlos, Schauer, Markus, Scherini, Viviana, Schieler, Harald, Schmidt, David, Scholten, Olaf, Schoorlemmer, Harm, Schovánek, Petr, Schröder, Frank G., Schulz, Alexander, Schulz, Johannes, Schumacher, Johannes, Sciutto, Sergio, Segreto, Alberto, Settimo, Mariangela, Shadkam, Amir, Shellard, Ronald C., Sigl, Guenter, Sima, Octavian, Śmiałkowski, Andrzej, Šmída, Radomir, Snow, Gregory, Sommers, Paul, Sonntag, Sebastian, Sorokin, J., Squartini, Ruben, Srivastava, Yogendra N., Stanca, Denis, Stanič, Samo, Stapleton, James, Stasielak, Jaroslaw, Stephan, Maurice, Stutz, Anne, Suarez, Federico, Durán, Mauricio Suarez, Suomijärvi, Tiina, Supanitsky, A. Daniel, Sutherland, Michael, Swain, John, Szadkowski, Zbigniew, Taborda, Oscar Alejandro, Tapia, Alex, Tepe, Andreas, Theodoro, Vanessa Menezes, Tibolla, Omar, Timmermans, Charles, Peixoto, Carlos J. Todero, Toma, Gabriel, Tomankova, Lenka, Tomé, Bernardo, Tonachini, Aurelio, Elipe, Guillermo Torralba, Machado, Diego Torres, Travnicek, Petr, Trini, Marta, Ulrich, Ralf, Unger, Michael, Urban, Martin, Galicia, Jose F. Valdés, Valiño, Ines, Valore, Laura, van Aar, Guus, van Bodegom, Patrick, Berg, Ad M. van den, van Velzen, Sjoert, van Vliet, Arjen, Varela, Enrique, Cárdenas, Bernardo Vargas, Varner, Gary, Vasquez, Rafael, Vázquez, Jose R., Vázquez, Ricardo, Veberič, Darko, Verzi, Valerio, Vicha, Jakub, Videla, Mariela, Villaseñor, Luis, Vlcek, Brian, Vorobiov, Serguei, Wahlberg, Hernan, Wainberg, Oscar, Walz, David, Watson, Alan, Weber, Marc, Weidenhaupt, Klaus, Weindl, Andreas, Welling, Christoph, Werner, Felix, Widom, Allan, Wiencke, Lawrence, Wilczyński, Henryk, Winchen, Tobias, Wittkowski, David, Wundheiler, Brian, Wykes, Sarka, Yang, Lili, Yapici, Tolga, Yushkov, Alexey, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, Zepeda, Arnulfo, Zimmermann, Benedikt, Ziolkowski, Michael, and Zuccarello, Francesca

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Auger Engineering Radio Array (AERA) is part of the Pierre Auger Observatory and is used to detect the radio emission of cosmic-ray air showers. These observations are compared to the data of the surface detector stations of the Observatory, which provide well-calibrated information on the cosmic-ray energies and arrival directions. The response of the radio stations in the 30 to 80 MHz regime has been thoroughly calibrated to enable the reconstruction of the incoming electric field. For the latter, the energy deposit per area is determined from the radio pulses at each observer position and is interpolated using a two-dimensional function that takes into account signal asymmetries due to interference between the geomagnetic and charge-excess emission components. The spatial integral over the signal distribution gives a direct measurement of the energy transferred from the primary cosmic ray into radio emission in the AERA frequency range. We measure 15.8 MeV of radiation energy for a 1 EeV air shower arriving perpendicularly to the geomagnetic field. This radiation energy -- corrected for geometrical effects -- is used as a cosmic-ray energy estimator. Performing an absolute energy calibration against the surface-detector information, we observe that this radio-energy estimator scales quadratically with the cosmic-ray energy as expected for coherent emission. We find an energy resolution of the radio reconstruction of 22% for the data set and 17% for a high-quality subset containing only events with at least five radio stations with signal., Comment: Replaced with published version. Added journal reference and DOI

Published
2015
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38. An improved limit to the diffuse flux of ultra-high energy neutrinos from the Pierre Auger Observatory

Author

The Pierre Auger Collaboration, Aab, Alexander, Abreu, Pedro, Aglietta, Marco, Ahn, Eun-Joo, Samarai, Imen Al, Albuquerque, Ivone, Allekotte, Ingomar, Allison, Patrick, Almela, Alejandro, Castillo, Jesus Alvarez, Alvarez-Muñiz, Jaime, Batista, Rafael Alves, Ambrosio, Michelangelo, Aminaei, Amin, Anchordoqui, Luis, Andringa, Sofia, Aramo, Carla, Aranda, Victor Manuel, Arqueros, Fernando, Arsene, Nicusor, Asorey, Hernán Gonzalo, Assis, Pedro, Aublin, Julien, Ave, Maximo, Avenier, Michel, Avila, Gualberto, Awal, Nafiun, Badescu, Alina Mihaela, Barber, Kerri B, Bäuml, Julia, Baus, Colin, Beatty, Jim, Becker, Karl Heinz, Bellido, Jose A, Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter, Billoir, Pierre, Blaess, Simon G, Blanco, Alberto, Blanco, Miguel, Bleve, Carla, Blümer, Hans, Boháčová, Martina, Boncioli, Denise, Bonifazi, Carla, Borodai, Nataliia, Brack, Jeffrey, Brancus, Iliana, Bridgeman, Ariel, Brogueira, Pedro, Brown, William C, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Caballero-Mora, Karen S, Caccianiga, Barbara, Caccianiga, Lorenzo, Candusso, Marina, Caramete, Laurentiu, Caruso, Rossella, Castellina, Antonella, Cataldi, Gabriella, Cazon, Lorenzo, Cester, Rosanna, Chavez, Alan G, Chiavassa, Andrea, Chinellato, Jose Augusto, Chudoba, Jiri, Cilmo, Marco, Clay, Roger W, Cocciolo, Giuseppe, Colalillo, Roberta, Coleman, Alan, Collica, Laura, Coluccia, Maria Rita, Conceição, Ruben, Contreras, Fernando, Cooper, Mathew J, Cordier, Alain, Coutu, Stephane, Covault, Corbin, Cronin, James, Dallier, Richard, Daniel, Bruno, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R, de Almeida, Rogerio M, de Jong, Sijbrand J, De Mauro, Giuseppe, Neto, Joao de Mello, De Mitri, Ivan, de Oliveira, Jaime, de Souza, Vitor, del Peral, Luis, Deligny, Olivier, Dembinski, Hans, Dhital, Niraj, Di Giulio, Claudio, Di Matteo, Armando, Diaz, Johana Chirinos, Castro, Mary Lucia Díaz, Diogo, Francisco, Dobrigkeit, Carola, Docters, Wendy, D'Olivo, Juan Carlos, Dorofeev, Alexei, Hasankiadeh, Qader Dorosti, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Erdmann, Martin, Erfani, Mona, Escobar, Carlos O, Espadanal, Joao, Etchegoyen, Alberto, Falcke, Heino, Fang, Ke, Farrar, Glennys, Fauth, Anderson, Fazzini, Norberto, Ferguson, Andrew P, Fernandes, Mateus, Fick, Brian, Figueira, Juan Manuel, Filevich, Alberto, Filipčič, Andrej, Fox, Brendan, Fratu, Octavian, Freire, Martín Miguel, Fuchs, Benjamin, Fujii, Toshihiro, García, Beatriz, Garcia-Pinto, Diego, Gate, Florian, Gemmeke, Hartmut, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, Giaccari, Ugo, Giammarchi, Marco, Giller, Maria, Głas, Dariusz, Glaser, Christian, Glass, Henry, Golup, Geraldina, Berisso, Mariano Gómez, Vitale, Primo F Gómez, González, Nicolás, Gookin, Ben, Gordon, Jacob, Gorgi, Alessio, Gorham, Peter, Gouffon, Philippe, Griffith, Nathan, Grillo, Aurelio, Grubb, Trent D, Guardincerri, Yann, Guarino, Fausto, Guedes, Germano, Hampel, Matías Rolf, Hansen, Patricia, Harari, Diego, Harrison, Thomas A, Hartmann, Sebastian, Harton, John, Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Heimann, Philipp, Herve, Alexander E, Hill, Gary C, Hojvat, Carlos, Hollon, Nicholas, Holt, Ewa, Homola, Piotr, Hörandel, Jörg, Horvath, Pavel, Hrabovský, Miroslav, Huber, Daniel, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Jandt, Ingolf, Jansen, Stefan, Jarne, Cecilia, Johnsen, Jeffrey A, Josebachuili, Mariela, Kääpä, Alex, Kambeitz, Olga, Kampert, Karl Heinz, Kasper, Peter, Katkov, Igor, Kégl, Balazs, Keilhauer, Bianca, Keivani, Azadeh, Kemp, Ernesto, Kieckhafer, Roger, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Krause, Raphael, Krohm, Nicole, Krömer, Oliver, Kuempel, Daniel, Kunka, Norbert, LaHurd, Danielle, Latronico, Luca, Lauer, Robert, Lauscher, Markus, Lautridou, Pascal, Coz, Sandra Le, Lebrun, Didier, Lebrun, Paul, de Oliveira, Marcelo Augusto Leigui, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Link, Katrin, Lopes, Luis, López, Rebeca, Casado, Aida López, Louedec, Karim, Lu, Lu, Lucero, Agustin, Malacari, Max, Maldera, Simone, Mallamaci, Manuela, Maller, Jennifer, Mandat, Dusan, Mantsch, Paul, Mariazzi, Analisa, Marin, Vincent, Mariş, Ioana, Marsella, Giovanni, Martello, Daniele, Martin, Lilian, Martinez, Humberto, Bravo, Oscar Martínez, Martraire, Diane, Meza, Jimmy Masías, Mathes, Hermann-Josef, Mathys, Sebastian, Matthews, James, Matthews, John, Matthiae, Giorgio, Maurel, Detlef, Maurizio, Daniela, Mayotte, Eric, Mazur, Peter, Medina, Carlos, Medina-Tanco, Gustavo, Meissner, Rebecca, Mello, Victor, Melo, Diego, Menshikov, Alexander, Messina, Stefano, Meyhandan, Rishi, Micheletti, Maria Isabel, Middendorf, Lukas, Minaya, Ignacio A, Miramonti, Lino, Mitrica, Bogdan, Molina-Bueno, Laura, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafá, Miguel, Moura, Celio A, Muller, Marcio Aparecido, Müller, Gero, Müller, Sarah, Mussa, Roberto, Navarra, Gianni, Navarro, Jose Luis, Navas, Sergio, Necesal, Petr, Nellen, Lukas, Nelles, Anna, Neuser, Jens, Nguyen, Phong H, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Niemietz, Lukas, Niggemann, Tim, Nitz, Dave, Nosek, Dalibor, Novotny, Vladimir, Nožka, Lyberis, Ochilo, Livingstone, Oikonomou, Foteini, Olinto, Angela, Pacheco, Noelia, Selmi-Dei, Daniel Pakk, Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Paul, Thomas, Pech, Miroslav, Pękala, Jan, Pelayo, Rodrigo, Pepe, Iuri, Perrone, Lorenzo, Petermann, Emily, Peters, Christine, Petrera, Sergio, Petrov, Yevgeniy, Phuntsok, Jamyang, Piegaia, Ricardo, Pierog, Tanguy, Pieroni, Pablo, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Plum, Matthias, Porcelli, Alessio, Porowski, Czeslaw, Prado, Raul Ribeiro, Privitera, Paolo, Prouza, Michael, Purrello, Victor, Quel, Eduardo J, Querchfeld, Sven, Quinn, Sean, Rautenberg, Julian, Ravel, Olivier, Ravignani, Diego, Revenu, Benoît, Ridky, Jan, Riggi, Simone, Risse, Markus, Ristori, Pablo, Rizi, Vincenzo, de Carvalho, Washington Rodrigues, Fernandez, Gonzalo Rodriguez, Rojo, Jorge Rubén Rodriguez, Rodríguez-Frías, Maria Dolores, Rogozin, Dmytro, Rosado, Jaime, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Saffi, Steven J, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto, Saleh, Ahmed, Greus, Francisco Salesa, Salina, Gaetano, Sánchez, Federico, Sanchez-Lucas, Patricia, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarkar, Biswaijt, Sarmento, Raul, Sato, Ricardo, Scarso, Carlos, Schauer, Markus, Scherini, Viviana, Schieler, Harald, Schiffer, Peter, Schmidt, David, Scholten, Olaf, Schoorlemmer, Harm, Schovánek, Petr, Schröder, Frank G, Schulz, Alexander, Schulz, Johannes, Schumacher, Johannes, Sciutto, Sergio, Segreto, Alberto, Settimo, Mariangela, Shadkam, Amir, Shellard, Ronald C, Sidelnik, Iván, Sigl, Guenter, Sima, Octavian, Śmiałkowski, Andrzej, Šmída, Radomir, Snow, Gregory, Sommers, Paul, Sorokin, J, Squartini, Ruben, Srivastava, Yogendra N, Stanca, Denis, Stanič, Samo, Stapleton, James, Stasielak, Jaroslaw, Stephan, Maurice, Stutz, Anne, Suarez, Federico, Suomijärvi, Tiina, Supanitsky, A Daniel, Sutherland, Michael, Swain, John, Szadkowski, Zbigniew, Taborda, Oscar Alejandro, Tapia, Alex, Tepe, Andreas, Theodoro, Vanessa Menezes, Tiffenberg, Javier, Timmermans, Charles, Peixoto, Carlos J Todero, Toma, Gabriel, Tomankova, Lenka, Tomé, Bernardo, Tonachini, Aurelio, Elipe, Guillermo Torralba, Machado, Diego Torres, Travnicek, Petr, Ulrich, Ralf, Unger, Michael, Urban, Martin, Galicia, Jose F Valdés, Valiño, Ines, Valore, Laura, van Aar, Guus, van Bodegom, Patrick, Berg, Ad M van den, van Velzen, Sjoert, van Vliet, Arjen, Varela, Enrique, Cárdenas, Bernardo Vargas, Varner, Gary, Vasquez, Rafael, Vázquez, Jose R, Vázquez, Ricardo, Veberič, Darko, Verzi, Valerio, Vicha, Jakub, Videla, Mariela, Villaseñor, Luis, Vlcek, Brian, Vorobiov, Serguei, Wahlberg, Hernan, Wainberg, Oscar, Walz, David, Watson, Alan, Weber, Marc, Weidenhaupt, Klaus, Weindl, Andreas, Werner, Felix, Widom, Allan, Wiencke, Lawrence, Wilczyński, Henryk, Winchen, Tobias, Wittkowski, David, Wundheiler, Brian, Wykes, Sarka, Yang, Lili, Yapici, Tolga, Yushkov, Alexey, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, Zepeda, Arnulfo, Zhu, Yue, Zimmermann, Benedikt, Ziolkowski, Michael, and Zuccarello, Francesca

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Neutrinos in the cosmic ray flux with energies near 1 EeV and above are detectable with the Surface Detector array of the Pierre Auger Observatory. We report here on searches through Auger data from 1 January 2004 until 20 June 2013. No neutrino candidates were found, yielding a limit to the diffuse flux of ultra-high energy neutrinos that challenges the Waxman-Bahcall bound predictions. Neutrino identification is attempted using the broad time-structure of the signals expected in the SD stations, and is efficiently done for neutrinos of all flavors interacting in the atmosphere at large zenith angles, as well as for "Earth-skimming" neutrino interactions in the case of tau neutrinos. In this paper the searches for downward-going neutrinos in the zenith angle bins $60^\circ-75^\circ$ and $75^\circ-90^\circ$ as well as for upward-going neutrinos, are combined to give a single limit. The $90\%$ C.L. single-flavor limit to the diffuse flux of ultra-high energy neutrinos with an $E^{-2}$ spectrum in the energy range $1.0 \times 10^{17}$ eV - $2.5 \times 10^{19}$ eV is $E_\nu^2 dN_\nu/dE_\nu < 6.4 \times 10^{-9}~ {\rm GeV~ cm^{-2}~ s^{-1}~ sr^{-1}}$., Comment: Replaced with published version. Added journal reference and DOI

Published
2015
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39. Measurement of the cosmic ray spectrum above $4{\times}10^{18}$ eV using inclined events detected with the Pierre Auger Observatory

Author

The Pierre Auger Collaboration, Aab, Alexander, Abreu, Pedro, Aglietta, Marco, Ahn, Eun-Joo, Samarai, Imen Al, Albuquerque, Ivone, Allekotte, Ingomar, Allison, Patrick, Almela, Alejandro, Castillo, Jesus Alvarez, Alvarez-Muñiz, Jaime, Batista, Rafael Alves, Ambrosio, Michelangelo, Aminaei, Amin, Anchordoqui, Luis, Andringa, Sofia, Aramo, Carla, Aranda, Victor Manuel, Arqueros, Fernando, Arsene, Nicusor, Asorey, Hernán Gonzalo, Assis, Pedro, Aublin, Julien, Ave, Maximo, Avenier, Michel, Avila, Gualberto, Awal, Nafiun, Badescu, Alina Mihaela, Barber, Kerri B, Bäuml, Julia, Baus, Colin, Beatty, Jim, Becker, Karl Heinz, Bellido, Jose A, Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter, Billoir, Pierre, Blaess, Simon G, Blanco, Alberto, Blanco, Miguel, Bleve, Carla, Blümer, Hans, Boháčová, Martina, Boncioli, Denise, Bonifazi, Carla, Borodai, Nataliia, Brack, Jeffrey, Brancus, Iliana, Bridgeman, Ariel, Brogueira, Pedro, Brown, William C, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Caballero-Mora, Karen S, Caccianiga, Barbara, Caccianiga, Lorenzo, Candusso, Marina, Caramete, Laurentiu, Caruso, Rossella, Castellina, Antonella, Cataldi, Gabriella, Cazon, Lorenzo, Cester, Rosanna, Chavez, Alan G, Chiavassa, Andrea, Chinellato, Jose Augusto, Chudoba, Jiri, Cilmo, Marco, Clay, Roger W, Cocciolo, Giuseppe, Colalillo, Roberta, Coleman, Alan, Collica, Laura, Coluccia, Maria Rita, Conceição, Ruben, Contreras, Fernando, Cooper, Mathew J, Cordier, Alain, Coutu, Stephane, Covault, Corbin, Cronin, James, Dallier, Richard, Daniel, Bruno, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R, de Almeida, Rogerio M, de Jong, Sijbrand J, De Mauro, Giuseppe, Neto, Joao de Mello, De Mitri, Ivan, de Oliveira, Jaime, de Souza, Vitor, del Peral, Luis, Deligny, Olivier, Dembinski, Hans, Dhital, Niraj, Di Giulio, Claudio, Di Matteo, Armando, Diaz, Johana Chirinos, Castro, Mary Lucia Díaz, Diogo, Francisco, Dobrigkeit, Carola, Docters, Wendy, D'Olivo, Juan Carlos, Dorofeev, Alexei, Hasankiadeh, Qader Dorosti, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Erdmann, Martin, Erfani, Mona, Escobar, Carlos O, Espadanal, Joao, Etchegoyen, Alberto, Falcke, Heino, Fang, Ke, Farrar, Glennys, Fauth, Anderson, Fazzini, Norberto, Ferguson, Andrew P, Fernandes, Mateus, Fick, Brian, Figueira, Juan Manuel, Filevich, Alberto, Filipčič, Andrej, Fox, Brendan, Fratu, Octavian, Freire, Martín Miguel, Fuchs, Benjamin, Fujii, Toshihiro, García, Beatriz, Garcia-Pinto, Diego, Gate, Florian, Gemmeke, Hartmut, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, Giaccari, Ugo, Giammarchi, Marco, Giller, Maria, Głas, Dariusz, Glaser, Christian, Glass, Henry, Golup, Geraldina, Berisso, Mariano Gómez, Vitale, Primo F Gómez, González, Nicolás, Gookin, Ben, Gordon, Jacob, Gorgi, Alessio, Gorham, Peter, Gouffon, Philippe, Griffith, Nathan, Grillo, Aurelio, Grubb, Trent D, Guarino, Fausto, Guedes, Germano, Hampel, Matías Rolf, Hansen, Patricia, Harari, Diego, Harrison, Thomas A, Hartmann, Sebastian, Harton, John, Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Heimann, Philipp, Herve, Alexander E, Hill, Gary C, Hojvat, Carlos, Hollon, Nicholas, Holt, Ewa, Homola, Piotr, Hörandel, Jörg, Horvath, Pavel, Hrabovský, Miroslav, Huber, Daniel, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Jandt, Ingolf, Jansen, Stefan, Jarne, Cecilia, Johnsen, Jeffrey A, Josebachuili, Mariela, Kääpä, Alex, Kambeitz, Olga, Kampert, Karl Heinz, Kasper, Peter, Katkov, Igor, Kégl, Balazs, Keilhauer, Bianca, Keivani, Azadeh, Kemp, Ernesto, Kieckhafer, Roger, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Krause, Raphael, Krohm, Nicole, Krömer, Oliver, Kuempel, Daniel, Kunka, Norbert, LaHurd, Danielle, Latronico, Luca, Lauer, Robert, Lauscher, Markus, Lautridou, Pascal, Coz, Sandra Le, Lebrun, Didier, Lebrun, Paul, de Oliveira, Marcelo Augusto Leigui, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Link, Katrin, Lopes, Luis, López, Rebeca, Casado, Aida López, Louedec, Karim, Lu, Lu, Lucero, Agustin, Malacari, Max, Maldera, Simone, Mallamaci, Manuela, Maller, Jennifer, Mandat, Dusan, Mantsch, Paul, Mariazzi, Analisa, Marin, Vincent, Mariş, Ioana, Marsella, Giovanni, Martello, Daniele, Martin, Lilian, Martinez, Humberto, Bravo, Oscar Martínez, Martraire, Diane, Meza, Jimmy Masías, Mathes, Hermann-Josef, Mathys, Sebastian, Matthews, James, Matthews, John, Matthiae, Giorgio, Maurel, Detlef, Maurizio, Daniela, Mayotte, Eric, Mazur, Peter, Medina, Carlos, Medina-Tanco, Gustavo, Meissner, Rebecca, Mello, Victor, Melo, Diego, Menshikov, Alexander, Messina, Stefano, Meyhandan, Rishi, Micheletti, Maria Isabel, Middendorf, Lukas, Minaya, Ignacio A, Miramonti, Lino, Mitrica, Bogdan, Molina-Bueno, Laura, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafá, Miguel, Moura, Celio A, Muller, Marcio Aparecido, Müller, Gero, Müller, Sarah, Mussa, Roberto, Navarra, Gianni, Navas, Sergio, Necesal, Petr, Nellen, Lukas, Nelles, Anna, Neuser, Jens, Newton, David, Nguyen, Phong H, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Niemietz, Lukas, Niggemann, Tim, Nitz, Dave, Nosek, Dalibor, Novotny, Vladimir, Nožka, Lyberis, Ochilo, Livingstone, Oikonomou, Foteini, Olinto, Angela, Olmos-Gilbaja, Victor, Pacheco, Noelia, Selmi-Dei, Daniel Pakk, Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Paul, Thomas, Pech, Miroslav, Pękala, Jan, Pelayo, Rodrigo, Pepe, Iuri, Perrone, Lorenzo, Petermann, Emily, Peters, Christine, Petrera, Sergio, Petrov, Yevgeniy, Phuntsok, Jamyang, Piegaia, Ricardo, Pierog, Tanguy, Pieroni, Pablo, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Plum, Matthias, Porcelli, Alessio, Porowski, Czeslaw, Prado, Raul Ribeiro, Privitera, Paolo, Prouza, Michael, Purrello, Victor, Quel, Eduardo J, Querchfeld, Sven, Quinn, Sean, Rautenberg, Julian, Ravel, Olivier, Ravignani, Diego, Revenu, Benoît, Ridky, Jan, Riggi, Simone, Risse, Markus, Ristori, Pablo, Rizi, Vincenzo, de Carvalho, Washington Rodrigues, Fernandez, Gonzalo Rodriguez, Rojo, Jorge Rubén Rodriguez, Rodríguez-Frías, Maria Dolores, Rogozin, Dmytro, Rosado, Jaime, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Saffi, Steven J, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto, Saleh, Ahmed, Greus, Francisco Salesa, Salina, Gaetano, Sánchez, Federico, Sanchez-Lucas, Patricia, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarkar, Biswaijt, Sarmento, Raul, Sato, Ricardo, Scarso, Carlos, Schauer, Markus, Scherini, Viviana, Schieler, Harald, Schiffer, Peter, Schmidt, David, Scholten, Olaf, Schoorlemmer, Harm, Schovánek, Petr, Schröder, Frank G, Schulz, Alexander, Schulz, Johannes, Schumacher, Johannes, Sciutto, Sergio, Segreto, Alberto, Settimo, Mariangela, Shadkam, Amir, Shellard, Ronald C, Sidelnik, Iván, Sigl, Guenter, Sima, Octavian, Śmiałkowski, Andrzej, Šmída, Radomir, Snow, Gregory, Sommers, Paul, Sorokin, J, Squartini, Ruben, Srivastava, Yogendra N, Stanca, Denis, Stanič, Samo, Stapleton, James, Stasielak, Jaroslaw, Stephan, Maurice, Stutz, Anne, Suarez, Federico, Suomijärvi, Tiina, Supanitsky, A Daniel, Sutherland, Michael, Swain, John, Szadkowski, Zbigniew, Taborda, Oscar Alejandro, Tapia, Alex, Tepe, Andreas, Theodoro, Vanessa Menezes, Timmermans, Charles, Peixoto, Carlos J Todero, Toma, Gabriel, Tomankova, Lenka, Tomé, Bernardo, Tonachini, Aurelio, Elipe, Guillermo Torralba, Machado, Diego Torres, Travnicek, Petr, Ulrich, Ralf, Unger, Michael, Urban, Martin, Galicia, Jose F Valdés, Valiño, Ines, Valore, Laura, van Aar, Guus, van Bodegom, Patrick, Berg, Ad M van den, van Velzen, Sjoert, van Vliet, Arjen, Varela, Enrique, Cárdenas, Bernardo Vargas, Varner, Gary, Vasquez, Rafael, Vázquez, Jose R, Vázquez, Ricardo, Veberič, Darko, Verzi, Valerio, Vicha, Jakub, Videla, Mariela, Villaseñor, Luis, Vlcek, Brian, Vorobiov, Serguei, Wahlberg, Hernan, Wainberg, Oscar, Walz, David, Watson, Alan, Weber, Marc, Weidenhaupt, Klaus, Weindl, Andreas, Werner, Felix, Widom, Allan, Wiencke, Lawrence, Wilczyński, Henryk, Winchen, Tobias, Wittkowski, David, Wundheiler, Brian, Wykes, Sarka, Yang, Lili, Yapici, Tolga, Yushkov, Alexey, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, Zepeda, Arnulfo, Zhu, Yue, Zimmermann, Benedikt, Ziolkowski, Michael, and Zuccarello, Francesca

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

A measurement of the cosmic-ray spectrum for energies exceeding $4{\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\times}10^{18}$ eV, the "ankle", the flux can be described by a power law $E^{-\gamma}$ with index $\gamma=2.70 \pm 0.02 \,\text{(stat)} \pm 0.1\,\text{(sys)}$ followed by a smooth suppression region. For the energy ($E_\text{s}$) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find $E_\text{s}=(5.12\pm0.25\,\text{(stat)}^{+1.0}_{-1.2}\,\text{(sys)}){\times}10^{19}$ eV., Comment: Replaced with published version. Added journal reference and DOI

Published
2015
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40. Implications of Mini-EUSO measurements for a space-based observation of UHECRs

Author

Bertaina Mario Edoardo, Barghini Dario, Battisti Matteo, Belov Alexander, Bianciotto Marta, Bisconti Francesca, Blaksley Carl, Blin Sylvie, Bolmgren Karl, Cambiè Giorgio, Capel Francesca, Casolino Marco, Churilo Igor, Crisconio Marino, De La Taille Christophe, Ebisuzaki Toshikazu, Eser Johannes, Fenu Francesco, Filippatos George, Franceschi Massimo Alberto, Fuglesang Christer, Golzio Alessio, Gorodetzky Philippe, Kajino Fumiyoshi, Kasuga Hiroshi, Klimov Pavel, Kungel Viktoria, Kuznetsov Vladimir, Manfrin Massimiliano, Marcelli Laura, Mascetti Gabriele, Marszał Włodzimierz, Mignone Marco, Miyamoto Hiroko, Murashov Alexey, Napolitano Tommaso, Ohmori Hitoshi, Olinto Angela, Parizot Etienne, Picozza Piergiorgio, Piotrowski Lech Wiktor, Plebaniak Zbigniew, Prévôt Guillaume, Reali Enzo, Ricci Marco, Romoli Giulia, Sakaki Naoto, Sharakin Sergei, Shinozaki Kenji, Szabelski Jacek, Takizawa Yoshiyuki, Valentini Giovanni, Vrabel Michal, Wiencke Lawrence, and Zotov Mikhail

Subjects
Physics, QC1-999
Abstract

Mini-EUSO is the first mission of the JEM-EUSO program on board the International Space Station. It was launched in 2019 and it is currently located in the Russian section (Zvezda module) of the station and viewing our planet from a nadir-facing UV-transparent window. The instrument is based on the concept of the original JEM-EUSO mission and consists of an optical system employing two Fresnel lenses and a focal surface composed of 36 Multi-Anode Photomultiplier tubes, 64 channels each, for a total of 2304 channels with single photon counting sensitivity and an overall field of view of 44° × 44°. Mini-EUSO can map the night-time Earth in the near UV range (predominantly between 290 nm and 430 nm), with a spatial resolution of about 6.3 km and different temporal resolutions of 2.5 µ, 320 µs and 41 ms. Mini-EUSO observations are extremely important to better assess the potential of a space-based detector in studying Ultra-High Energy Cosmic Rays (UHECRs) such as K-EUSO and POEMMA. In this contribution we focus the attention on UV measurements, the observation of clouds and of certain categories of events that Mini-EUSO triggers with the shortest temporal resolution. We place them in the context of UHECR observations from space, namely the estimation of exposure and sensitivity to Extensive Air Showers.

Published
2023
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41. The JEM-EUSO Program for UHECR Studies from Space

Author

Parizot Etienne, Casolino Marco, Picozza Piergiorgio, Ebisuzaki Toshikazu, Bertaina Mario Edoardo, Fuglesang Christer, Haungs Andreas, Kajino Fumiyoshi, Klimov Pavel, Olinto Angela, Ricci Marco, Sagawa Hiroyuki, Szabelski Jacek, and Wiencke Lawrence

Subjects
Physics, QC1-999
Abstract

To take up the challenge of understanding the origin of the ultra-high-energy cosmic rays (UHECRs), new observational means appear necessary. The JEM-EUSO Collaboration has undertaken to open the space road to UHECR studies. For more than a decade, it has been developing a realistic program to measure the UHECRs from space with unprecedented aperture, together with complementary scientific objectives in a broader multidisciplinary context. Several intermediate missions have already been completed (on the ground: EUSO-TA; under stratospheric ballons: EUSO-Balloon and EUSO-SPB1; in space: TUS, and on-board the ISS: MINI-EUSO), and others are in preparation for flight (EUSO-SPB2), under review (K-EUSO: currently on hold), or proposed for the next decade (POEMMA). We report on the general status of the JEM-EUSO program, underlining that its technology has now reached operational maturity, and is ready for actual cosmic-ray shower detection from above.

Published
2023
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42. EUSO-SPB2: A balloon experiment for UHECR and VHE neutrino observation

Author

Cummings Austin, Eser Johannes, Filippatos George, Olinto Angela, Venters Tonia, and Wiencke Lawrence

Subjects
Physics, QC1-999
Abstract

The Extreme Universe Space Observatory on a Super Pressure Balloon 2 (EUSO-SPB2) experiment will make new measurements from suborbital space as a precursor for future space missions that will address the challenge of the extremely low fluxes of ultra-high energy cosmic rays (UHECR) and very high energy (VHE) neutrinos. The EUSO-SPB2 detector is comprised of two 1m diameter aperture telescopes. The Fluorescence Telescope (FT) will point in nadir and will record fluorescence light from cosmic ray EAS with energies above 1 EeV in its field of view of 36 by 12 degrees. The Cherenkov Telescope (CT) features a silicon photomultiplier focal surface with a field of view of 12 by 6 degrees. The CT will switch between two observation modes: one which points the CT above the limb to measure the Cherenkov emission of cosmic ray EAS with energies above 1 PeV and one which points the CT below the limb to record the Cherenkov emission produced by PeV scale EAS initiated by neutrino-sourced tau decay. As it is the first time such an instrument has been flown, one of the priorities of the CT will be the study of the optical background for observing neutrinos in this way. EUSO-SPB2 is undergoing the final integration steps for launch on a NASA super pressure balloon payload in the spring of 2023 from Wanaka NZ. The CT was field-tested in March 2022 and the FT in August - September 2022. The data collected during the EUSO-SPB2 mission will be essential to advancing the development of a space-based multi-messenger observatory such as the Probe of Extreme Multi-Messenger Astrophysics (POEMMA). In this contribution, we discuss the EUSO-SPB2 science goals, the instruments, the expected performance and the current status.

Published
2023
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43. An end-to-end in-flight calibration of Mini-EUSO detector

Author

Miyamoto Hiroko, Battisti Matteo, Barghini Dario, Belov Alexander, Bertaina Mario, Bianciotto Marta, Bisconti Francesca, Blaksley Carl, Blin Sylvie, Bolmgren Karl, Cambiè Giorgio, Capel Francesca, Casolino Marco, Churilo Igor, Crisconio Marino, De La Taille Christophe, Ebisuzaki Toshikazu, Eser Johannes, Fenu Francesco, Filippatos George, Franceschi Massimo Alberto, Fuglesang Christer, Golzio Alessio, Gorodetzky Philippe, Kajino Fumiyoshi, Kasuga Hiroshi, Klimov Pavel, Kungel Viktoria, Kuznetsov Vladimir, Manfrin Massimiliano, Marcelli Laura, Mascetti Gabriele, Marszał Włodzimierz, Mignone Marco, Murashov Alexey, Napolitano Tommaso, Ohmori Hitoshi, Olinto Angela, Parizot Etienne, Picozza Piergiorgio, Piotrowski Lech Wiktor, Plebaniak Zbigniew, Prévôt Guillaume, Reali Enzo, Ricci Marco, Romoli Giulia, Sakaki Naoto, Sharakin Sergei, Shinozaki Kenji, Szabelski Jacek, Takizawa Yoshiyuki, Valentini Giovanni, Vrabel Michal, Wincke Lawrence, and Zotov Mikhail

Subjects
Physics, QC1-999
Abstract

Mini-EUSO is a wide Field-of-View (FoV, 44°) telescope currently in operation from a nadir-facing UV-transparent window in the Russian Zvezda module on the International Space Station (ISS). It is the first detector of the JEM-EUSO program deployed on the ISS, launched in August 2019. The main goal of Mini-EUSO is to measure the UV emissions from the ground and atmosphere, using an orbital platform. Mini-EUSO is mainly sensitive in the 290–430 nm bandwidth. Light is focused by a system of two Fresnel lenses of 25 cm diameter each on the Photo-Detector-Module (PDM), which consists of an array of 36 Multi-Anode Photomultiplier Tubes (MAPMTs), arranged in blocks of 2 × 2 called Elementary Cells (ECs), for a total of 2304 pixels working in photon counting mode, in three different time resolutions of 2.5 µs (defined as 1 Gate Time Unit, GTU), 320 µs and 40.96 ms operating in parallel. In the longest time scale, the data is continuously acquired to monitor the UV emission of the Earth. It is best suited for the observation of ground sources and therefore has been used for the observational campaigns of the ground-based UV flasher in order to perform an end-to-end calibration of Mini-EUSO. In this contribution, the assembled UV flasher, the operation of the field campaign and the analysis of the obtained data are presented. The result is compared with the overall effi ciency computed from the expectations which takes into account the atmospheric attenuation and the parametrisation of different effects such as the optics effi ciency, the MAPMT detection effi ciency, BG3 filter transmittance and the transparency of the ISS window.

Published
2023
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44. Is the Ultra-High Energy Cosmic-Ray Excess Observed by the Telescope Array Correlated with IceCube Neutrinos?

Author

Fang, Ke, Fujii, Toshihiro, Linden, Tim, and Olinto, Angela V.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Telescope Array (TA) has observed a statistically significant excess in cosmic-rays with energies above 57 EeV in a region of approximately 1150 square degrees centered on coordinates (R.A. = 146.7, Dec. = 43.2). We note that the location of this excess correlates with two of the 28 extraterrestrial neutrinos recently observed by IceCube. The overlap between the two IceCube neutrinos and the TA excess is statistically significant at the 2$\sigma$ level. Furthermore, the spectrum and intensity of the IceCube neutrinos is consistent with a single source which would also produce the TA excess. Finally, we discuss possible source classes with the correct characteristics to explain the cosmic-ray and neutrino fluxes with a single source., Comment: 7 pages, 4 figures, accepted for publication in the Astrophysical Journal

Published
2014
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45. Large Scale Anisotropy of Cosmic Rays and Directional Neutrino Signals from Galactic Sources

Author

Anchordoqui, Luis A., Goldberg, Haim, Olinto, Angela V., Paul, Thomas C., Vlcek, Brian J., and Weiler, Thomas J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We investigate the neutrino - cosmic ray connection for sources in the Galaxy in terms of two observables: the shape of the energy spectrum and the distribution of arrival directions. We also study the associated gamma ray emission from these sources., Comment: Proceedings of the 2nd Cosmic Ray Anisotropy Workshop, 26-28 September 2013, Madison, Wisconsin. To appear in IOP Conference Series

Published
2014
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46. Testing the Newborn Pulsar Origin of Ultrahigh Energy Cosmic Rays with EeV Neutrinos

Author

Fang, Ke, Kotera, Kumiko, Murase, Kohta, and Olinto, Angela V.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Fast-spinning newborn pulsars are intriguing candidate sources of ultrahigh energy cosmic rays (UHECRs). The acceleration of particles with a given composition in a fraction of the extragalactic pulsar population can give a consistent explanation for the measurements of the Auger Observatory. We calculate the associated diffuse neutrino flux produced while particles cross the supernova ejecta surrounding the stars. We show that in the minimal pulsar scenario that are compatible with the UHECR data, the effective optical depth to hadronuclear interactions is larger than unity at ultrahigh energies. Thus, even in the most pessimistic case, one expects energy fluxes of $\sim 0.1 - 1 \,\rm EeV$ neutrinos that should be detectable with IceCube or Askaryan Radio Array within a decade., Comment: 7 pages, 3 figures, combined published paper and appended erratum. Fig.3 has been corrected

Published
2013
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47. Roadmap for Ultra-High Energy Cosmic Ray Physics and Astronomy (whitepaper for Snowmass 2013)

Author

Anchordoqui, Luis A., Farrar, Glennys R., Krizmanic, John F., Matthews, Jim, Mitchell, John W., Nitz, Dave, Olinto, Angela V., Paul, Thomas C., Sokolsky, Pierre, Thomson, Gordon B., and Weiler, Thomas J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
Abstract

We summarize the remarkable recent progress in ultra-high energy cosmic ray physics and astronomy enabled by the current generation of cosmic ray observatories. We discuss the primary objectives for future measurements and describe the plans for near-term enhancements of existing experiments as well as the next generation of observatories., Comment: 7 revtex pages, 1 figure (v2 author added, references added)

Published
2013

48. The Pierre Auger Observatory: Contributions to the 33rd International Cosmic Ray Conference (ICRC 2013)

Author

The Pierre Auger Collaboration, Aab, Alexander, Abreu, Pedro, Aglietta, Marco, Ahlers, Markus, Ahn, Eun-Joo, Albuquerque, Ivone, Allekotte, Ingomar, Allen, Jeff, Allison, Patrick, Almela, Alejandro, Castillo, Jesus Alvarez, Alvarez-Muñiz, Jaime, Batista, Rafael Alves, Ambrosio, Michelangelo, Aminaei, Amin, Anchordoqui, Luis, Andringa, Sofia, Antičić, Tome, Aramo, Carla, Arqueros, Fernando, Asorey, Hernán Gonzalo, Assis, Pedro, Aublin, Julien, Ave, Maximo, Avenier, Michel, Avila, Gualberto, Badescu, Alina Mihaela, Barber, Kerri B., Bardenet, Remi, Bäuml, Julia, Baus, Colin, Beatty, Jim, Becker, Karl Heinz, Bellido, Jose A., BenZvi, Segev, Berat, Corinne, Bertou, Xavier, Biermann, Peter, Billoir, Pierre, Blanco, Francisco, Blanco, Miguel, Bleve, Carla, Blümer, Hans, Boháčová, Martina, Boncioli, Denise, Bonifazi, Carla, Bonino, Raffaella, Borodai, Nataliia, Brack, Jeffrey, Brancus, Iliana, Brogueira, Pedro, Brown, William C., Buchholz, Peter, Bueno, Antonio, Buscemi, Mario, Caballero-Mora, Karen S., Caccianiga, Barbara, Caccianiga, Lorenzo, Candusso, Marina, Caramete, Laurentiu, Caruso, Rossella, Castellina, Antonella, Cataldi, Gabriella, Cazon, Lorenzo, Cester, Rosanna, Cheng, Shih-Ho, Chiavassa, Andrea, Chinellato, Jose Augusto, Chudoba, Jiri, Cilmo, Marco, Clay, Roger W, Cocciolo, Giuseppe, Colalillo, Roberta, Collica, Laura, Coluccia, Maria Rita, Conceição, Ruben, Contreras, Fernando, Cooper, Mathew J., Coutu, Stephane, Covault, Corbin, Criss, Adrienne, Cronin, James, Curutiu, Alex, Dallier, Richard, Daniel, Bruno, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., de Almeida, Rogerio M., De Domenico, Manlio, de Jong, Sijbrand J., De La Vega, Gonzalo, Junior, Walter J. M. de Mello, Neto, Joao de Mello, De Mitri, Ivan, de Souza, Vitor, de Vries, Krijn, del Peral, Luis, Deligny, Olivier, Dembinski, Hans, Dhital, Niraj, Di Giulio, Claudio, Di Matteo, Armando, Diaz, Johana Chirinos, Castro, Mary Lucia Díaz, Diep, Pham Ngoc, Diogo, Francisco, Dobrigkeit, Carola, Docters, Wendy, D'Olivo, Juan Carlos, Dong, Pham Ngoc, Dorofeev, Alexei, Anjos, Joao dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Erdmann, Martin, Escobar, Carlos O., Espadanal, Joao, Etchegoyen, Alberto, Luis, Pedro Facal San, Falcke, Heino, Fang, Ke, Farrar, Glennys, Fauth, Anderson, Fazzini, Norberto, Ferguson, Andrew P., Fick, Brian, Figueira, Juan Manuel, Filevich, Alberto, Filipčič, Andrej, Foerster, Nadine, Fox, Brendan, Fracchiolla, Claudia, Fraenkel, Eric Daniel, Fratu, Octavian, Fröhlich, Uwe, Fuchs, Benjamin, Gaior, Romain, Gamarra, Rodolfo Federico, Gambetta, Silvia, García, Beatriz, Roca, Sayri Tupac Garcia, Garcia-Gamez, Diego, Garcia-Pinto, Diego, Garilli, Gianpaolo, Bravo, Alberto Gascon, Gemmeke, Hartmut, Ghia, Piera Luisa, Giammarchi, Marco, Giller, Maria, Gitto, Javier, Glaser, Christian, Glass, Henry, Albarracin, Flavia Gomez, Berisso, Mariano Gómez, Vitale, Primo F. Gómez, Gonçalves, Patrícia, Gonzalez, Javier G., Gookin, Ben, Gorgi, Alessio, Gorham, Peter, Gouffon, Philippe, Grebe, Stefan, Griffith, Nathan, Grillo, Aurelio, Grubb, Trent D., Guardincerri, Yann, Guarino, Fausto, Guedes, Germano, Hansen, Patricia, Harari, Diego, Harrison, Thomas A., Harton, John, Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Herve, Alexander E., Hill, Gary C., Hojvat, Carlos, Hollon, Nicholas, Holt, Ewa, Homola, Piotr, Hörandel, Joerg, Horvath, Pavel, Hrabovský, Miroslav, Huber, Daniel, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Jansen, Stefan, Jarne, Cecilia, Josebachuili, Mariela, Kadija, Krešo, Kambeitz, Olga, Kampert, Karl Heinz, Karhan, Pavel, Kasper, Peter, Katkov, Igor, Kégl, Balazs, Keilhauer, Bianca, Keivani, Azadeh, Kemp, Ernesto, Kieckhafer, Roger, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Knapp, Johannes, Krause, Raphael, Krohm, Nicole, Krömer, Oliver, Kruppke-Hansen, Daniel, Kuempel, Daniel, Kunka, Norbert, La Rosa, Giovanni, LaHurd, Danielle, Latronico, Luca, Lauer, Robert, Lauscher, Markus, Lautridou, Pascal, Coz, Sandra Le, Leão, Milton, Lebrun, Paul, Lebrun, Didier, de Oliveira, Marcelo Augusto Leigui, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Link, Katrin, López, Rebeca, Agüera, Angeles Lopez, Louedec, Karim, Bahilo, Julio Lozano, Lu, Lu, Lucero, Agustin, Ludwig, Marianne, Lyberis, Haris, Maccarone, Maria Concetta, Malacari, Max, Maldera, Simone, Maller, Jennifer, Mandat, Dusan, Mantsch, Paul, Mariazzi, Analisa, Marin, Vincent, Mariş, Ioana, Falcon, Hugo R. Marquez, Marsella, Giovanni, Martello, Daniele, Martin, Lilian, Martinez, Humberto, Bravo, Oscar Martínez, Martraire, Diane, Meza, Jimmy Masías, Mathes, Hermann-Josef, Matthews, James, Matthews, John A. J., Matthiae, Giorgio, Maurel, Detlef, Maurizio, Daniela, Mayotte, Eric, Mazur, Peter, Medina, Carlos, Medina-Tanco, Gustavo, Melissas, Maximilien, Melo, Diego, Menichetti, Ezio, Menshikov, Alexander, Messina, Stefano, Meyhandan, Rishi, Mićanović, Saša, Micheletti, Maria Isabel, Middendorf, Lukas, Minaya, Ignacio A., Miramonti, Lino, Mitrica, Bogdan, Molina-Bueno, Laura, Mollerach, Silvia, Monasor, Maria, Ragaigne, Delphine Monnier, Montanet, François, Morales, Benjamin, Morello, Carlo, Moreno, Juan Cruz, Mostafá, Miguel, Moura, Celio A., Muller, Marcio Aparecido, Müller, Gero, Münchmeyer, Moritz, Mussa, Roberto, Navarra, Gianni, Navarro, Jose Luis, Navas, Sergio, Necesal, Petr, Nellen, Lukas, Nelles, Anna, Neuser, Jens, Nhung, Pham Thi Tuyet, Niechciol, Marcus, Niemietz, Lukas, Niggemann, Tim, Nitz, Dave, Nosek, Dalibor, Nožka, Libor, Oehlschläger, Juergen, Olinto, Angela, Oliveira, Micael, Ortiz, Montserrat, Pacheco, Noelia, Selmi-Dei, Daniel Pakk, Palatka, Miroslav, Pallotta, Juan, Palmieri, Nunzia, Parente, Gonzalo, Parra, Alejandra, Pastor, Sergio, Paul, Thomas, Pech, Miroslav, Pękala, Jan, Pelayo, Rodrigo, Pepe, Iuri, Perrone, Lorenzo, Pesce, Roberto, Petermann, Emily, Petrera, Sergio, Petrolini, Alessandro, Petrov, Yevgeniy, Piegaia, Ricardo, Pierog, Tanguy, Pieroni, Pablo, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Plum, Matthias, Pontz, Michael, Porcelli, Alessio, Preda, Titi, Privitera, Paolo, Prouza, Michael, Quel, Eduardo J, Querchfeld, Sven, Quinn, Sean, Rautenberg, Julian, Ravel, Olivier, Ravignani, Diego, Revenu, Benoît, Ridky, Jan, Riggi, Simone, Risse, Markus, Ristori, Pablo, Rivera, Hugo M., Rizi, Vincenzo, Roberts, Jonathan, de Carvalho, Washington Rodrigues, Cabo, Iago Rodriguez, Fernandez, Gonzalo Rodriguez, Martino, Julio Rodriguez, Rojo, Jorge Rubén Rodriguez, Rodríguez-Frías, Maria Dolores, Ros, Germán, Rosado, Jaime, Rossler, Tomas, Roth, Markus, Rouillé-d'Orfeuil, Benjamin, Roulet, Esteban, Rovero, Adrian, Rühle, Christoph, Saffi, Steven J., Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto, Greus, Francisco Salesa, Salina, Gaetano, Sánchez, Federico, Sanchez-Lucas, Patricia, Santo, Catarina E., Santos, Eva, Santos, Edivaldo Moura, Sarazin, Fred, Sarkar, Biswaijt, Sarmento, Raul, Sato, Ricardo, Scharf, Nils, Scherini, Viviana, Schieler, Harald, Schiffer, Peter, Schmidt, Adrian, Scholten, Olaf, Schoorlemmer, Harm, Schovánek, Petr, Schröder, Frank G., Schulz, Alexander, Schulz, Johannes, Sciutto, Sergio, Scuderi, Mario, Segreto, Alberto, Settimo, Mariangela, Shadkam, Amir, Shellard, Ronald C., Sidelnik, Iván, Sigl, Guenter, Sima, Octavian, Śmiałkowski, Andrzej, Šmída, Radomir, Snow, Gregory, Sommers, Paul, Sorokin, J., Spinka, Hal, Squartini, Ruben, Srivastava, Yogendra N., Stanič, Samo, Stapleton, James, Stasielak, Jaroslaw, Stephan, Maurice, Straub, Marcel, Stutz, Anne, Suarez, Federico, Suomijärvi, Tiina, Supanitsky, A. Daniel, Šuša, Tatjana, Sutherland, Michael, Swain, John, Szadkowski, Zbigniew, Szuba, Marek, Tapia, Alex, Tartare, Mathieu, Taşcău, Oana, Thao, Nguyen Thi, Tiffenberg, Javier, Timmermans, Charles, Tkaczyk, Wieslaw, Peixoto, Carlos J. Todero, Toma, Gabriel, Tomankova, Lenka, Tomé, Bernardo, Tonachini, Aurelio, Elipe, Guillermo Torralba, Machado, Diego Torres, Travnicek, Petr, Tridapalli, Diogo, Trovato, Enrica, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Galicia, Jose F. Valdés, Valiño, Ines, Valore, Laura, van Aar, Guus, Berg, Ad M. van den, van Velzen, Sjoert, van Vliet, Arjen, Varela, Enrique, Cárdenas, Bernardo Vargas, Varner, Gary, Vázquez, Jose R., Vázquez, Ricardo, Veberič, Darko, Verzi, Valerio, Vicha, Jakub, Videla, Mariela, Villaseñor, Luis, Wahlberg, Hernan, Wahrlich, Philip, Wainberg, Oscar, Walz, David, Watson, Alan, Weber, Marc, Weidenhaupt, Klaus, Weindl, Andreas, Werner, Felix, Westerhoff, Stefan, Whelan, Ben J., Widom, Allan, Wieczorek, Grzegorz, Wiencke, Lawrence, Wilczyńska, Barbara, Wilczyński, Henryk, Will, Martin, Williams, Christopher, Winchen, Tobias, Wundheiler, Brian, Wykes, Sarka, Yamamoto, Tokonatsu, Yapici, Tolga, Younk, Patrick, Yuan, Guofeng, Yushkov, Alexey, Zamorano, Bruno, Zarza, Gabriel, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, Zaw, Ingyin, Zepeda, Arnulfo, Zhou, Jing, Zhu, Yue, Silva, Marcelo Zimbres, and Ziolkowski, Michael

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Contributions of the Pierre Auger Collaboration to the 33rd International Cosmic Ray Conference, Rio de Janeiro, Brazil, July 2013, Comment: Contributions to the 33rd International Cosmic Ray Conference, Rio de Janeiro, Brazil, July 2013

Published
2013

49. Pinning down the cosmic ray source mechanism with new IceCube data

Author

Anchordoqui, Luis A., Goldberg, Haim, Lynch, Morgan H., Olinto, Angela V., Paul, Thomas C., and Weiler, Thomas J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
Abstract

Very recently the IceCube Collaboration has reported an observation of 28 neutrino candidates with energies between 50 TeV and 2 PeV, constituting a 4.1$\sigma$ excess compared to the atmospheric background. In this article we investigate the compatibility between the data and a hypothesized unbroken power-law neutrino spectrum for various values of spectral index \Gamma >= 2. We show that \Gamma ~ 2.3 is consistent at the ~ 1.5$\sigma$ level with the observed events up to 2 PeV and to the null observation of events at higher energies. We then assume that the sources of this unbroken spectrum are Galactic, and deduce (i) an energy-transfer fraction from parent protons to pions, and (ii) a way of discriminating among models which have been put forth to explain the "knee" and "ankle" features of the cosmic ray spectrum. Future IceCube data will test the unbroken power law hypothesis and provide a multi-messenger approach to explaining features of the cosmic ray spectrum, including the transition from Galactic to extragalactic dominance., Comment: Matching version to be published in Physical Review D

Published
2013
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50. Sensitivity of JEM-EUSO to Ensemble Fluctuations in the Ultra-High Energy Cosmic Ray Flux

Author

Ahlers, Markus, Anchordoqui, Luis A., Olinto, Angela V., Paul, Thomas C., and Taylor, Andrew M.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics, High Energy Physics - Phenomenology
Abstract

The flux of ultra-high energy (UHE) cosmic rays (CRs) depends on the cosmic distribution of their sources. Data from CR observations are yet inconclusive about their exact location or distribution, but provide a measure for the average local density of these emitters. Due to the discreteness of the emitters the flux is expected to show ensemble fluctuations on top of the statistical variations, a reflection of the cosmic variance. This effect is strongest for the most energetic cosmic rays due to the limited propagation distance in the cosmic radiation background and is hence a local phenomenon. In this work we study the sensitivity of the JEM-EUSO space mission to ensemble fluctuations on the assumption of uniform distribution of sources, with local source density \sim 10^{-5} Mpc^{-3}. We show that in 3 years of observation JEM-EUSO will be able to probe ensemble fluctuations if the nearest sources are at 3 Mpc, and that after 10 years orbiting the Earth, this pathfinder mission will become sensitive to ensemble fluctuations if the nearest sources are 10 Mpc away. The study of spectral fluctuations from the local source distributions are complementary to but independent of cosmic ray anisotropy studies., Comment: To be published in Proceedings of the 33rd International Cosmic Ray Conference (ICRC2013), Rio de Janeiro, Brazil, 2-9 July, 2013. Paper Id: 239

Published
2013

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