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1. OffLine simulation and reconstruction software framework for the JEM-EUSO missions

Author

Paul, Thomas C.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Joint Experiment Missions for Extreme Universe Observatory comprises a collection of complementary missions dedicated to pioneering technologies and techniques for a future space-based multi-messenger observatory which will have sufficient sensitivity and exposure to measure properties of extremely rare ultra-high energy (E>50 EeV) cosmic rays and very high energy (E>100 PeV) neutrinos. Here we describe a general-purpose software framework designed to facilitate detailed simulation and reconstruction of events observed by the various missions using both detection of fluorescence and Cherenkov light produced when cosmic ray or neutrino-induced extensive air showers traverse Earth's atmosphere. The software builds on a framework developed by the Pierre Auger Collaboration. We describe the techniques used to organize contributions from numerous collaborators, manage an abundance of configuration information, and provide simple access to time-dependent detector and atmospheric information. We also explain how we support a multitude of computing platforms, provide fast installation and maintain the broad testing coverage required for stability of the large and heterogeneous code base. We provide a few examples of simulated and reconstructed data gathered by some of the JEM-EUSO missions, including the EUSO-SPB2 instrument., Comment: Update with acknowledgements and full author list arXiv admin note: text overlap with arXiv:2309.02577

Published
2023

2. 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

3. 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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4. 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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5. 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

6. Probing QCD approach to thermal equilibrium with ultrahigh energy cosmic rays

Author

Soriano, Jorge F., Anchordoqui, Luis A., Paul, Thomas C., and Weiler, Thomas J.

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

The Pierre Auger Collaboration has reported an excess in the number of muons of a few tens of percent over expectations computed using extrapolation of hadronic interaction models tuned to accommodate LHC data. Very recently, we proposed an explanation for the muon excess assuming the formation of a deconfined quark matter (fireball) state in central collisions of ultrarelativistic cosmic rays with air nuclei. At the first stage of its evolution the fireball contains gluons as well as $u$ and $d$ quarks. The very high baryochemical potential inhibits gluons from fragmenting into $u \bar u$ and $d \bar d$, and so they fragment predominantly into $s \bar s$ pairs. In the hadronization which follows this leads to the strong suppression of pions and hence photons, but allows heavy hadrons to be emitted carrying away strangeness. In this manner, the extreme imbalance of hadron to photon content provides a way to enhance the muon content of the air shower. In this communication we study theoretical systematics from hadronic interaction models used to describe the cascades of secondary particles produced in the fireball explosion. We study the predictions of one of the leading LHC-tuned models QGSJET II-04 considered in the Auger analysis., Comment: 7 pages LaTeX, 6 .pdf figures

Published
2018
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7. 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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8. 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

9. Estimating the contribution of Galactic sources to the diffuse neutrino flux

Author

Anchordoqui, Luis A., Goldberg, Haim, Paul, Thomas C., da Silva, Luiz H. M., and Vlcek, Brian J.

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

Motivated by recent IceCube observations we re-examine the idea that microquasars are high energy neutrino emitters. By stretching to the maximum the parameters of the Fermi engine we show that the nearby high-mass X-ray binary LS 5039 could accelerate protons up to above about 20 PeV. These highly relativistic protons could subsequently interact with the plasma producing neutrinos up to the maximum observed energies. After that we adopt the spatial density distribution of high-mass X-ray binaries obtained from the deep INTEGRAL Galactic plane survey and we assume LS 5039 typifies the microquasar population to demonstrate that these powerful compact sources could provide a dominant contribution to the diffuse neutrino flux recently observed by IceCube., Comment: Matching version to be published in PRD

Published
2014
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10. What IceCube data tell us about neutrino emission from star-forming galaxies (so far)

Author

Anchordoqui, Luis A., Paul, Thomas C., da Silva, Luiz H. M., Torres, Diego F., and Vlcek, Brian J.

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

Very recently, the IceCube Collaboration reported a flux of neutrinos in the energy range 50 TeV < E_\nu < 2 PeV, which departs from expectations from atmospheric background at the 5.7\sigma level. This flux is in remarkable agreement with the expected diffuse flux of neutrinos from starburst galaxies, and the 3 highest energy events have uncertainty contours encompassing some of such systems. These events, all of which have well-measured energies above 1 PeV, exhibit shower topologies, for which the angular resolution is about 15^\circ. Due to this angular uncertainty and the a posteriori nature of cuts used in our study it is not possible to assign a robust statistical significance to this association. Using muon tracks, which have angular resolution < 1^\circ, we compute the number of observations required to make a statistically significant statement, and show that in a few years of operation the upgraded IceCube detector should be able to confirm or refute this hypothesis. We also note that double bang topology rates constitute a possible discriminator among various astrophysical sources., Comment: Reference added, matching version to be published in PRD

Published
2014
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11. 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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12. Ergonomics Systems Mapping for Professional Responder Inter-operability in Chemical, Biological, Radiological and Nuclear Events

Author

Hancox, Graham, Hignett, Sue, Pillin, Hilary, Kintzios, Spyros, Silmäri, Jyri, Paul Thomas, C. L., Kacprzyk, Janusz, Series Editor, Pal, Nikhil R., Advisory Editor, Bello Perez, Rafael, Advisory Editor, Corchado, Emilio S., Advisory Editor, Hagras, Hani, Advisory Editor, Kóczy, László T., Advisory Editor, Kreinovich, Vladik, Advisory Editor, Lin, Chin-Teng, Advisory Editor, Lu, Jie, Advisory Editor, Melin, Patricia, Advisory Editor, Nedjah, Nadia, Advisory Editor, Nguyen, Ngoc Thanh, Advisory Editor, Wang, Jun, Advisory Editor, Bagnara, Sebastiano, editor, Tartaglia, Riccardo, editor, Albolino, Sara, editor, Alexander, Thomas, editor, and Fujita, Yushi, editor

Published
2019
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13. Cosmic Neutrino Pevatrons: A Brand New Pathway to Astronomy, Astrophysics, and Particle Physics

Author

Anchordoqui, Luis A., Barger, Vernon, Cholis, Ilias, Goldberg, Haim, Hooper, Dan, Kusenko, Alexander, Learned, John G., Marfatia, Danny, Pakvasa, Sandip, Paul, Thomas C., and Weiler, Thomas J.

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

The announcement by the IceCube Collaboration of the observation of 28 cosmic neutrino candidates has been greeted with a great deal of justified excitement. The data reported so far depart by 4.3\sigma from the expected atmospheric neutrino background, which raises the obvious question: "Where in the Cosmos are these neutrinos coming from?" We review the many possibilities which have been explored in the literature to address this question, including origins at either Galactic or extragalactic celestial objects. For completeness, we also briefly discuss new physics processes which may either explain or be constrained by IceCube data., Comment: This is a review article solicited for the inaugural edition of Journal of High Energy Astrophysics (JHEAp). Matching version accepted for publication

Published
2013
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14. Weinberg's Higgs portal confronting recent LUX and LHC results together with upper limits on B^+ and K^+ decay into invisibles

Author

Anchordoqui, Luis A., Denton, Peter B., Goldberg, Haim, Paul, Thomas C., da Silva, Luiz H. M., Vlcek, Brian J., and Weiler, Thomas J.

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

We discuss a number of experimental constraints on Weinberg's Higgs portal model. In this framework, the standard model (SM) particle spectrum is extended to include one complex scalar field S and one Dirac fermion \psi. These new fields are singlets under the SM gauge group and are charged under a global U(1) symmetry. Breaking of this U(1) symmetry results in a massless Goldstone boson \alpha and a massive CP-even scalar r, and splits the Dirac fermion into two new mass-eigenstates \psi_\pm, corresponding to Majorana fermions. The interest on such a minimal SM extension is twofold. On the one hand, if the Goldstone bosons are in thermal equilibrium with SM particles until the era of muon annihilation their contribution to the effective number of neutrino species can explain the hints from cosmological observations of extra relativistic degrees of freedom at the epoch of last scattering. On the other hand, the lightest Majorana fermion \psi_- provides a plausible dark matter candidate. Mixing of r with the Higgs doublet \phi is characterized by the mass of hidden scalar m_h and the mixing angle \theta. We constrain this parameter space using a variety of experimental data, including heavy meson decays with missing energy, the invisible Higgs width, and direct dark matter searches. We show that different experimental results compress the allowed parameter space in complementary ways, covering a large range of \psi_- masses (5 GeV \alt m_- \alt 100 GeV). Though current results narrow the parameter space significantly (for the mass range of interest, \theta \alt 10^{-3} to 10^{-4}), there is still room for discovery (\alpha decoupling at the muon annihilation era requires \theta \agt 10^{-5} to 10^{-4}). In the near future, measurements from ATLAS, CMS, LHCb, NA62, XENON1T, LUX, and CDMSlite will probe nearly the full parameter space., Comment: Matching version accepted for publication in Physical Review D

Published
2013
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15. 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

16. 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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17. 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

18. SCROD: School Cosmic Ray Outreach Detector

Author

Gouchtchine, Evgueni, McCauley, Thomas P., Musienko, Yuri, Paul, Thomas C., Reucroft, Stephen, and Swain, John D.

Subjects
Astrophysics
Abstract

We report progress on applying technologies developed for LHC-era experiments to cosmic ray detection, using scintillating tiles with embedded wavelength-shifting fibers and avalanche photodiode readouts as parts of a robust, inexpensive cosmic air shower detector. We are planning to deploy such detectors in high schools as part of an outreach effort able to search for long-distance correlations between airshowers., Comment: To be published in the Proceedings of the 28th International Cosmic Ray Conference http://www.icrr.u-tokyo.ac.jp/icrc2003/

Published
2003

21. Neutrino propagation in the Earth and emerging charged leptons with nuPyProp

Author

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

Published
2023
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22. The Forward Physics Facility at the High-Luminosity LHC

Author

Feng, Jonathan L., Kling, Felix, Reno, Mary Hall, Rojo, Juan, Soldin, Dennis, Anchordoqui, Luis A., Boyd, Jamie, Ismail, Ahmed, Harland-Lang, Lucian, Kelly, Kevin J., Pandey, Vishvas, Trojanowski, Sebastian, Tsai, Yu-Dai, Alameddine, Jean-Marco, Araki, Takeshi, Ariga, Akitaka, Ariga, Tomoko, Asai, Kento, Bacchetta, Alessandro, Balazs, Kincso, Barr, Alan J., Battistin, Michele, Bian, Jianming, Bertone, Caterina, Bai, Weidong, Bakhti, Pouya, Balantekin, A. Baha, Barman, Basabendu, Batell, Brian, Bauer, Martin, Bauer, Brian, Becker, Mathias, Berlin, Asher, Bertuzzo, Enrico, Bhattacharya, Atri, Bonvini, Marco, Boogert, Stewart T., Boyarsky, Alexey, Bramante, Joseph, Brdar, Vedran, Carmona, Adrian, Casper, David W., Celiberto, Francesco Giovanni, Cerutti, Francesco, Chachamis, Grigorios, Chauhan, Garv, Citron, Matthew, Copello, Emanuele, Corso, Jean-Pierre, Darmé, Luc, d'Agnolo, Raffaele Tito, Darvishi, Neda, Das, Arindam, de Lellis, Giovanni, de Roeck, Albert, de Vries, Jordy, Dembinski, Hans P., Demidov, Sergey, Deniverville, Patrick, Denton, Peter B., Deppisch, Frank F., Dev, P.S. Bhupal, Di Crescenzo, Antonia, Dienes, Keith R., Diwan, Milind V., Dreiner, Herbi K., Du, Yong, Dutta, Bhaskar, Duwentäster, Pit, Elie, Lucie, Ellis, Sebastian A.R., Enberg, Rikard, Farzan, Yasaman, Fieg, Max, Foguel, Ana Luisa, Foldenauer, Patrick, Foroughi-Abari, Saeid, Fortin, Jean-François, Friedland, Alexander, Fuchs, Elina, Fucilla, Michael, Gallmeister, Kai, Garcia, Alfonso, García Canal, Carlos A., Garzelli, Maria Vittoria, Gauld, Rhorry, Ghosh, Sumit, Ghoshal, Anish, Gibson, Stephen, Giuli, Francesco, Gonçalves, Victor P., Gorbunov, Dmitry, Goswami, Srubabati, Grau, Silvia, Günther, Julian Y., Guzzi, Marco, Haas, Andrew, Hakulinen, Timo, Harris, Steven P., Harz, Julia, Herrera, Juan Carlos Helo, Hill, Christopher S., Hirsch, Martin, Hobbs, Timothy J., Höche, Stefan, Hryczuk, Andrzej, Huang, Fei, Inada, Tomohiro, Infantino, Angelo, Ismail, Ameen, Jacobsson, Richard, Jana, Sudip, Jeong, Yu Seon, Ježo, Tomas, Jho, Yongsoo, Jodłowski, Krzysztof, Lowski, Krzysztof Jod, Kalashnikov, Dmitry, Kärkkäinen, Timo J., Keppel, Cynthia, Kim, Jongkuk, Klasen, Michael, Klein, Spencer R., Ko, Pyungwon, Köhler, Dominik, Komatsu, Masahiro, Kovaˇrík, Karol, Kulkarni, Suchita, Kumar, Jason, Kumar, Karan, Kuo, Jui-Lin, Krauss, Frank, Kusina, Aleksander, Laletin, Maxim, Le Roux, Chiara, Lee, Seung J., Lee, Hye-Sung, Lefebvre, Helena, Li, Jinmian, Li, Shuailong, Li, Yichen, Liu, Wei, Liu, Zhen, Lonjon, Mickael, Lyu, Kun-Feng, Maciula, Rafal, Mammen Abraham, Roshan, Masouminia, Mohammad R., Mcfayden, Josh, Mikulenko, Oleksii, Mohammed, Mohammed M.A., Mohan, Kirtimaan A., Morfín, Jorge G., Mosel, Ulrich, Mosny, Martin, Muzakka, Khoirul F., Nadolsky, Pavel, Nakano, Toshiyuki, Nangia, Saurabh, Cornago, Angel Navascues, Nevay, Laurence J., Ninin, Pierre, Nocera, Emanuele R., Nomura, Takaaki, Nunes, Rui, Okada, Nobuchika, Olness, Fred, Osborne, John, Otono, Hidetoshi, Ovchynnikov, Maksym, Papa, Alessandro, Pei, Junle, Peon, Guillermo, Perez, Gilad, Pickering, Luke, Plätzer, Simon, Plestid, Ryan, Poddar, Tanmay Kumar, Quílez, Pablo, Rai, Mudit, Rajaee, Meshkat, Raut, Digesh, Reimitz, Peter, Resnati, Filippo, Rhode, Wolfgang, Richardson, Peter, Ritz, Adam, Rokujo, Hiroki, Roszkowski, Leszek, Ruhe, Tim, Ruiz, Richard, Sabate-Gilarte, Marta, Sandrock, Alexander, Sarcevic, Ina, Sarkar, Subir, Sato, Osamu, Scherb, Christiane, Schienbein, Ingo, Schulz, Holger, Schwaller, Pedro, Sciutto, Sergio J., Sengupta, Dipan, Shchutska, Lesya, Shimomura, Takashi, Silvetti, Federico, Sinha, Kuver, Sjöstrand, Torbjörn, Sobczyk, Jan T., Song, Huayang, Soriano, Jorge F., Soreq, Yotam, Stasto, Anna, Stuart, David, Su, Shufang, Su, Wei, Szczurek, Antoni, Tabrizi, Zahra, Takubo, Yosuke, Taoso, Marco, Thomas, Brooks, Thonet, Pierre, Tuckler, Douglas, Sabio Vera, Agustin, Vincke, Heinz, Vishnudath, K.N., Wang, Zeren Simon, Winkler, Martin W., Wu, Wenjie, Xie, Keping, Xu, Xun-Jie, You, Tevong, Yu, Ji-Young, Yu, Jiang-Hao, Zapp, Korinna, Zhang, Yongchao, Zhang, Yue, Zhou, Guanghui, Funchal, Renata Zukanovich, Abdul Khalek, Rabah, An, Di, Arakawa, Jason, Arduini, Gianluigi, Barman, Rahool Kumar, Beacom, John F., Bernlochner, Florian, Bishai, Mary, Boeckh, Tobias, Bortoletto, Daniela, Boveia, Antonio, Brenner, Lydia, Brodsky, Stanley J., Burgard, Carsten, Camargo-Molina, José Eliel, Carli, Tancredi, Chang, Spencer, Charitonidis, Nikolaos, Chen, Xin, Chen, Thomas Y., Chiang, Cheng-Wei, Coccaro, Andrea, Cohen, Timothy, Coleman, Alan, Conceição, Ruben, Cooper-Sarkar, Amanda, d'Onofrio, Monica, Davoudiasl, Hooman, Di Matteo, Armando, Di Valentino, Eleonora, Dmitrievsky, Sergey, Dobre, Radu, Doglioni, Caterina, Mendes, Luis M. Domingues, Dova, María Teresa, Duvernois, Michael A., Ekstedt, Andreas, Elsen, Eckhard, Escalante del Valle, Alberto, Essig, Rouven, Farrar, Glennys R., Fedynitch, Anatoli, Fellers, Deion, Firu, Elena, Galon, Iftah, Garcia Garcia, Isabel, da Silveira, Gustavo Gil, Giunti, Carlo, Gornushkin, Yury, Goldfarb, Steven, Goncalves, Dorival, Sevilla, Sergio Gonzalez, Gonzalez Suarez, Rebeca, Guler, A. Murat, Gwenlan, Claire, Gwilliam, Carl, Halzen, Francis, Han, Tao, Haungs, Andreas, Heeck, Julian, Hentschinski, Martin, Hsu, Shih-Chieh, Hu, Zhen, Huffman, B. Todd, Iacobucci, Giuseppe, Illana, Jose I., Insolia, Antonio, Ishak, Mustapha, Jaeckel, Joerg, Kabat, Daniel, Ken, Enrique Kajomovitz, Kanai, Takumi, Katori, Teppei, Khoze, Valery, Kotko, Piotr, Kribs, Graham D., Kuehn, Susanne, Kundu, Saumyen, Lee, Claire, Lek, Rafa L. Mase, Leszczynska, Agnieszka, Li, Lingfeng, Lie, Ki, Lillard, Benjamin, Lin, Huey-Wen, Lowette, Steven, Marfatia, Danny, López, Francisco Martínez, Masełek, Rafał, Masip, Manuel, Matchev, Konstantin, Mccauley, Thomas, Medina-Tanco, Gustavo, Menjo, Hiroaki, Miloi, Mˇadˇalina Mihaela, Miramonti, Lino, Mohlabeng, Gopolang, Moretti, Stefano, Moretti, Théo, Nath, Pran, Navarria, Francesco L., Neagu, Alina Tania, Nelles, Anna, Neuhaus, Friedemann, Nunez, Carlos, Ochoa-Ricoux, J. Pedro, Okui, Kazuaki, Olinto, Angela V., Onel, Yasar, de los Heros, Carlos Pérez, Pandini, Carlo, Pasechnik, Roman, Paul, Thomas C., Petersen, Brian A., Pierog, Tanguy, Plehn, Tilman, Plum, Matthias, Potamianos, Karolos, Preda, Titi, Prim, Markus, Queitsch-Maitland, Michaela, Reina, Laura, Reininghaus, Maximilian, Rizzo, Thomas G., Robens, Tania, Ruiz-Chóliz, Elisa, Schmieden, Kristof, Schnell, Gunar, Schott, Matthias, Schroeder, Frank G., Sfyrla, Anna, Shadmi, Yael, Shipsey, Ian, Shively, Savannah R., Shoemaker, Ian M., Vasina, Svetlana, Singh, Rajeev, Sousa, A., Muzio, Marco Stein, Stupak, John, Suarez, Indara, Tait, Tim M.P., Tata, Xerxes, Thottoli, Shafeeq Rahman, Toranosuke, Okumura, Torrence, Eric, Torres, Diego F., Trócsányi, Zoltán, Tricoli, Alessandro, Unger, Michael, Vázquez Sierra, Carlos, Valli, Mauro, Venters, Tonia, Verpoest, Stef, Vilela, Cristovao, Vormwald, Benedikt, Wang, Lian-Tao, Waterbury, Michael, Watts, Gordon, West, Stephen M., Xu, Tao, Yüksel, Emin, Yaeggy, Barbara, Yoon, Chun Sil, Yuan, Tianlu, Zgura, Ion Sorin, Groups, Snowmass Working, (Astro)-Particles Physics, Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Feng, Jonathan L, Kling, Felix, Reno, Mary Hall, Rojo, Juan, Soldin, Denni, Anchordoqui, Luis A, Boyd, Jamie, Ismail, Ahmed, Harland-Lang, Lucian, Kelly, Kevin J, Pandey, Vishva, Trojanowski, Sebastian, Tsai, Yu-Dai, Alameddine, Jean-Marco, Araki, Takeshi, Ariga, Akitaka, Ariga, Tomoko, Asai, Kento, Bacchetta, Alessandro, Balazs, Kincso, Barr, Alan J, Battistin, Michele, Bian, Jianming, Bertone, Caterina, Bai, Weidong, Bakhti, Pouya, Balantekin, A Baha, Barman, Basabendu, Batell, Brian, Bauer, Martin, Bauer, Brian, Becker, Mathia, Berlin, Asher, Bertuzzo, Enrico, Bhattacharya, Atri, Bonvini, Marco, Boogert, Stewart T, Boyarsky, Alexey, Bramante, Joseph, Brdar, Vedran, Carmona, Adrian, Casper, David W, Celiberto, Francesco Giovanni, Cerutti, Francesco, Chachamis, Grigorio, Chauhan, Garv, Citron, Matthew, Copello, Emanuele, Corso, Jean-Pierre, Darmé, Luc, D’Agnolo, Raffaele Tito, Darvishi, Neda, Das, Arindam, De Lellis, Giovanni, De Roeck, Albert, de Vries, Jordy, Dembinski, Hans P, Demidov, Sergey, Deniverville, Patrick, Denton, Peter B, Deppisch, Frank F, Dev, P S Bhupal, Di Crescenzo, Antonia, Dienes, Keith R, Diwan, Milind V, Dreiner, Herbi K, Du, Yong, Dutta, Bhaskar, Duwentäster, Pit, Elie, Lucie, Ellis, Sebastian A R, Enberg, Rikard, Farzan, Yasaman, Fieg, Max, Foguel, Ana Luisa, Foldenauer, Patrick, Foroughi-Abari, Saeid, Fortin, Jean-Françoi, Friedland, Alexander, Fuchs, Elina, Fucilla, Michael, Gallmeister, Kai, Garcia, Alfonso, García Canal, Carlos A, Garzelli, Maria Vittoria, Gauld, Rhorry, Ghosh, Sumit, Ghoshal, Anish, Gibson, Stephen, Giuli, Francesco, Gonçalves, Victor P, Gorbunov, Dmitry, Goswami, Srubabati, Grau, Silvia, Günther, Julian Y, Guzzi, Marco, Haas, Andrew, Hakulinen, Timo, Harris, Steven P, Harz, Julia, Helo Herrera, Juan Carlo, Hill, Christopher S, Hirsch, Martin, Hobbs, Timothy J, Höche, Stefan, Hryczuk, Andrzej, Huang, Fei, Inada, Tomohiro, Infantino, Angelo, Ismail, Ameen, Jacobsson, Richard, Jana, Sudip, Jeong, Yu Seon, Ježo, Toma, Jho, Yongsoo, Jodłowski, Krzysztof, Kalashnikov, Dmitry, Kärkkäinen, Timo J, Keppel, Cynthia, Kim, Jongkuk, Klasen, Michael, Klein, Spencer R, Ko, Pyungwon, Köhler, Dominik, Komatsu, Masahiro, Kovařík, Karol, Kulkarni, Suchita, Kumar, Jason, Kumar, Karan, Kuo, Jui-Lin, Krauss, Frank, Kusina, Aleksander, Laletin, Maxim, Le Roux, Chiara, Lee, Seung J, Lee, Hye-Sung, Lefebvre, Helena, Li, Jinmian, Li, Shuailong, Li, Yichen, Liu, Wei, Liu, Zhen, Lonjon, Mickael, Lyu, Kun-Feng, Maciula, Rafal, Abraham, Roshan Mammen, Masouminia, Mohammad R, Mcfayden, Josh, Mikulenko, Oleksii, Mohammed, Mohammed M A, Mohan, Kirtimaan A, Morfín, Jorge G, Mosel, Ulrich, Mosny, Martin, Muzakka, Khoirul F, Nadolsky, Pavel, Nakano, Toshiyuki, Nangia, Saurabh, Cornago, Angel Navascue, Nevay, Laurence J, Ninin, Pierre, Nocera, Emanuele R, Nomura, Takaaki, Nunes, Rui, Okada, Nobuchika, Olness, Fred, Osborne, John, Otono, Hidetoshi, Ovchynnikov, Maksym, Papa, Alessandro, Pei, Junle, Peon, Guillermo, Perez, Gilad, Pickering, Luke, Plätzer, Simon, Plestid, Ryan, Poddar, Tanmay Kumar, Quílez, Pablo, Rai, Mudit, Rajaee, Meshkat, Raut, Digesh, Reimitz, Peter, Resnati, Filippo, Rhode, Wolfgang, Richardson, Peter, Ritz, Adam, Rokujo, Hiroki, Roszkowski, Leszek, Ruhe, Tim, Ruiz, Richard, Sabate-Gilarte, Marta, Sandrock, Alexander, Sarcevic, Ina, Sarkar, Subir, Sato, Osamu, Scherb, Christiane, Schienbein, Ingo, Schulz, Holger, Schwaller, Pedro, Sciutto, Sergio J, Sengupta, Dipan, Shchutska, Lesya, Shimomura, Takashi, Silvetti, Federico, Sinha, Kuver, Sjöstrand, Torbjörn, Sobczyk, Jan T, Song, Huayang, Soriano, Jorge F, Soreq, Yotam, Stasto, Anna, Stuart, David, Su, Shufang, Su, Wei, Szczurek, Antoni, Tabrizi, Zahra, Takubo, Yosuke, Taoso, Marco, Thomas, Brook, Thonet, Pierre, Tuckler, Dougla, Sabio Vera, Agustin, Vincke, Heinz, Vishnudath, K N, Wang, Zeren Simon, Winkler, Martin W, Wu, Wenjie, Xie, Keping, Xu, Xun-Jie, You, Tevong, Yu, Ji-Young, Yu, Jiang-Hao, Zapp, Korinna, Zhang, Yongchao, Zhang, Yue, Zhou, Guanghui, Funchal, Renata Zukanovich, Khalek, Rabah Abdul, An, Di, Arakawa, Jason, Arduini, Gianluigi, Barman, Rahool Kumar, Beacom, John F, Bernlochner, Florian, Bishai, Mary, Boeckh, Tobia, Bortoletto, Daniela, Boveia, Antonio, Brenner, Lydia, Brodsky, Stanley J, Burgard, Carsten, Camargo-Molina, José Eliel, Carli, Tancredi, Chang, Spencer, Charitonidis, Nikolao, Chen, Xin, Chen, Thomas Y, Chiang, Cheng-Wei, Coccaro, Andrea, Cohen, Timothy, Coleman, Alan, Conceição, Ruben, Cooper-Sarkar, Amanda, D’Onofrio, Monica, Davoudiasl, Hooman, Di Matteo, Armando, Di Valentino, Eleonora, Dobre, Radu, Doglioni, Caterina, Domingues Mendes, Luis M, Dova, María Teresa, Duvernois, Michael A, Ekstedt, Andrea, Elsen, Eckhard, Escalante del Valle, Alberto, Essig, Rouven, Farrar, Glennys R, Fedynitch, Anatoli, Fellers, Deion, Firu, Elena, Galon, Iftah, Garcia, Isabel Garcia, Gil da Silveira, Gustavo, Giunti, Carlo, Goldfarb, Steven, Goncalves, Dorival, Sevilla, Sergio Gonzalez, Suarez, Rebeca Gonzalez, Guler, A Murat, Gwenlan, Claire, Gwilliam, Carl, Halzen, Franci, Han, Tao, Haungs, Andrea, Heeck, Julian, Hentschinski, Martin, Hsu, Shih-Chieh, Hu, Zhen, Huffman, B Todd, Iacobucci, Giuseppe, Illana, Jose I, Insolia, Antonio, Ishak, Mustapha, Jaeckel, Joerg, Kabat, Daniel, Ken, Enrique Kajomovitz, Kanai, Takumi, Katori, Teppei, Khoze, Valery, Kotko, Piotr, Kribs, Graham D, Kuehn, Susanne, Kundu, Saumyen, Lee, Claire, Leszczynska, Agnieszka, Li, Lingfeng, Lie, Ki, Lillard, Benjamin, Lin, Huey-Wen, Lowette, Steven, Marfatia, Danny, López, Francisco Martínez, Masełek, Rafał, Masip, Manuel, Matchev, Konstantin, Mccauley, Thoma, Medina-Tanco, Gustavo, Menjo, Hiroaki, Miloi, Mǎadǎlina Mihaela, Miramonti, Lino, Mohlabeng, Gopolang, Moretti, Stefano, Moretti, Théo, Nath, Pran, Navarria, Francesco L, Neagu, Alina Tania, Nelles, Anna, Neuhaus, Friedemann, Nunez, Carlo, Ochoa-Ricoux, J Pedro, Okui, Kazuaki, Olinto, Angela V, Onel, Yasar, Pérez de los Heros, Carlo, Pandini, Carlo, Pasechnik, Roman, Paul, Thomas C, Petersen, Brian A, Pierog, Tanguy, Plehn, Tilman, Plum, Matthia, Potamianos, Karolo, Preda, Titi, Prim, Marku, Queitsch-Maitland, Michaela, Reina, Laura, Reininghaus, Maximilian, Rizzo, Thomas G, Robens, Tania, Ruiz-Chóliz, Elisa, Schmieden, Kristof, Schnell, Gunar, Schott, Matthia, Schroeder, Frank G, Sfyrla, Anna, Shadmi, Yael, Shipsey, Ian, Shively, Savannah R, Shoemaker, Ian M, Singh, Rajeev, Sousa, A, Muzio, Marco Stein, Stupak, John, Suarez, Indara, Tait, Tim M P, Tata, Xerxe, Thottoli, Shafeeq Rahman, Toranosuke, Okumura, Torrence, Eric, Torres, Diego F, Trócsányi, Zoltán, Tricoli, Alessandro, Unger, Michael, Sierra, Carlos Vázquez, Valli, Mauro, Venters, Tonia, Verpoest, Stef, Vilela, Cristovao, Vormwald, Benedikt, Wang, Lian-Tao, Waterbury, Michael, Watts, Gordon, West, Stephen M, Xu, Tao, Yüksel, Emin, Yaeggy, Barbara, Yoon, Chun Sil, Yuan, Tianlu, and Zgura, Ion Sorin

Subjects
Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, engineering, High Energy Physics - Experiment, Subatomär fysik, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), Subatomic Physics, CERN LHC Coll: upgrade, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Detectors and Experimental Techniques, quantum chromodynamics, nonperturbative, High Energy Astrophysical Phenomena (astro-ph.HE), neutrino, statistics, energy: high, new physics, new physics: search for, Physics, neutrino: statistics, neutrinos, Instrumentation and Detectors (physics.ins-det), ATLAS, High Energy Physics - Phenomenology, CERN LHC Coll, Large Hadron Collider, energy, high, astroparticle physics, vertex: primary, Astrophysics - High Energy Astrophysical Phenomena, numerical calculations: Monte Carlo, Particle Physics - Experiment, Forward Physics Facility, signature, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and Astronomy, p p: scattering, Nuclear and High Energy Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), quantum chromodynamics: nonperturbative, FOS: Physical sciences, dark matter, weak interaction, neutrino: energy, TeV, ddc:530, new particle searches, SDG 7 - Affordable and Clean Energy, Particle Physics - Phenomenology, scattering, Accelerators and Storage Rings, QCD, forward production, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], vertex, primary, p p: colliding beams, acceptance, new particle
Abstract

Acknowledgments We thank the participants of the FPF meetings and the Snowmass working groups for discussions that have contributed both directly and indirectly to this study. We gratefully acknowledge the invaluable support of the CERN Physics Beyond Colliders study group and the work of CERN technical teams related to civil engineering studies (SCE-DOD), safety discussions (HSE-OHS, HSE-RP, EP-DI-SO), integration (EN-ACE), and discussions on services (EN-CV, EN-EL, EN-AA) and simulations (SY-STI). The work by J Alameddine, W Rhode, T Ruhe, and A Sandrock has been supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation), Collaborative Research Center SFB 876 and SFB 1491. L A Anchordoqui is supported by the US National Science Foundation (NSF) Grant PHY-2112527. T Araki is supported by JP18H01210. A Ariga is supported by JSPS KAKENHI Grant JP20K23373 and the European Research Council (ERC) under the European Union's Horizon 2020 Research and Innovation Programme (Grant 101002690). T Ariga acknowledges support from JSPS KAKENHI Grant JP19H01909. K Asai is supported by JSPS KAKENHI Grant JP19J13812 and JP21K20365. A Bacchetta and F G Celiberto acknowledge support from the INFN/NINPHA project. P Bakhti and M Rajaee are supported by the National Research Foundation of Korea (NRF-2020R1I1A3072747). B Barman received funding from the Patrimonio Autónomo—Fondo Nacional de Financiamiento para la Ciencia, la Tecnología y la Innovación Francisco José de Caldas (MinCiencias—Colombia) Grant 80740-465-2020 and the European Union's Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie Grant Agreement No. 860881-HIDDeN. The work of B Batell is supported by the US Department of Energy (DOE) Grant DE–SC0007914. The work of A Berlin, T J Hobbs, S Hoeche, and J G Morfín was supported by the Fermi National Accelerator Laboratory (Fermilab), a US DOE, Office of Science, HEP User Facility. Fermilab is managed by Fermi Research Alliance, LLC (FRA), acting under Contract DE-AC02-07CH11359. M Becker, E Copello and J Harz acknowledge support from the DFG Emmy Noether Grant HA 8555/1-1. E Copello acknowledges also support from the DFG Collaborative Research Centre 'Neutrinos and Dark Matter in Astro- and Particle Physics' (SFB 1258). E Bertuzzo acknowledges financial support from FAPESP Contracts 2015/25884-4 and 2019/15149-6 and is indebted to the Theoretical Particle Physics and Cosmology group at King's College London for hospitality. The work of J Bian and W Wu is supported in part by US DOE Grant DE-SC0009920 and Heising-Simons Foundation Grant 2022-3319. The work of A Boyarsky and M Ovchynnikov is supported by the ERC under the European Union's Horizon 2020 Research and Innovation Programme (GA 694896). A Carmona acknowledges funding from the European Union's Horizon 2020 Research and Innovation Programme under the Marie Skłodowska-Curie Grant Agreement No. 754446 and UGR Research and Knowledge Transfer Found—Athenea3i. A Carmona also acknowledges partial support by the Ministry of Science and Innovation and SRA (10.13039/501100011033) Grant PID2019-106087GB-C22 and by the Junta de Andalucía Grant A-FQM-472-UGR20. F G Celiberto thanks the Università degli Studi di Pavia for the warm hospitality. The work of G Chachamis was supported by the Fundação para a Ciência e a Tecnologia (Portugal) under Project CERN/FIS-PAR/0024/2019 and Contract 'Investigador auxiliar FCT—Individual Call/03216/2017'. The work of M Citron and D Stuart is supported by US DOE Grant DE-SC0011702. The work of L Darme is supported by the European Union's Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie Grant Agreement 101028626. P B Denton acknowledges support from the US DOE Grant Contract DE-SC0012704. The work of P S Bhupal Dev was supported in part by the US DOE Grant DE-SC0017987. The research activities of K R Dienes were supported in part by the US DOE Grant DE-FG02-13ER41976/DE-SC0009913 and also by the US NSF through its employee IR/D program. M V Diwan acknowledges support from the US DOE Grant Contract DE-SC0012704. Y Du and J H Yu are supported in part by National Key Research and Development Program of China Grant 2020YFC2201501, and the National Science Foundation of China (NSFC) under Grants 12022514, 11875003 and 12047503, and CAS Project for Young Scientists in Basic Research YSBR-006, and the Key Research Program of the CAS Grant XDPB15. The work of B Dutta and S Ghosh are supported in part by the US DOE Grant DE-SC0010813. The work of S Ghosh is also supported in part by National Research Foundation of Korea (NRF)'s Grants, Grant 6N021413. Y Farzan has received financial support from Saramadan Contract ISEF/M/400279 as well as from the European Union's Horizon 2020 Research and Innovation Programme under the Marie Skłodowska-Curie Grant Agreement 860881-HIDDeN. The work of J L Feng is supported in part by US NSF Grants PHY-1915005 and PHY-2111427, Simons Investigator Award #376204, Simons Foundation Grant 623683, and Heising-Simons Foundation Grants 2019-1179 and 2020-1840. M Fieg is supported in part by US NSF Grant PHY-1915005 and by NSF Graduate Research Fellowship Award DGE-1839285. A L Foguel is supported by FAPESP Contract 2020/00174-2. The work of P Foldenauer is supported by the UKRI Future Leaders Fellowship DARKMAP. The work of S Foroughi-Abari and A Ritz is supported in part by NSERC, Canada. The work of J-F Fortin is supported in part by NSERC, Canada. A Friedland is supported by the US DOE Grant DE-AC02-76SF00515. E Fuchs acknowledges support by the DFG Germany's Excellence Strategy—EXC-2123 'QuantumFrontiers'—390837967. M Fucilla, M M A Mohammed, and A Papa acknowledge support from the INFN/QFT@COLLIDERS project. A Garcia acknowledges support from the European Union's H2020-MSCA Grant Agreement 101025085. C A García Canal and S J Sciutto acknowledge support from CONICET and ANPCyT M V Garzelli acknowledges support the from German BMBF Contract 05H21GUCCA. V P Goncalves was partially financed by the Brazilian funding agencies CNPq, CAPES, FAPERGS and INCT-FNA (Process Number 464898/2014-5). S Goswami acknowledges the J C Bose Fellowship (JCB/2020/000011) of Science and Engineering Research Board of Department of Science and Technology, Government of India. The work of M Guzzi is supported by US NSF Grant PHY-2112025. L Harland-Lang thanks the Science and Technology Facilities Council (STFC) for support via Grant Award ST/L000377/1. The work of S P Harris is supported by the US DOE Grant DE-FG02-00ER41132 as well as the US NSF Grant PHY-1430152 (JINA Center for the Evolution of the Elements). J C Helo acknowledge support from Grant ANID FONDECYT-Chile 1201673 and ANID—Millennium Science Initiative Program ICN2019-044. The work of M Hirsch is supported by the Spanish Grants PID2020-113775GB-I00 (AEI/10.13039/501100011033) and PROMETEO/2018/165 (Generalitat Valenciana). The work of A Hryczuk and M Laletin is supported by the National Science Centre, Poland, research Grant 2018/31/D/ST2/00813. The research activities of F Huang are supported by the International Postdoctoral Exchange Fellowship Program and in part by US NSF Grant PHY-1915005. A Ismail is supported by NSERC (Reference Number 557763) and by US NSF Grant PHY-2014071. Y S Jeong acknowledges support from the National Research Foundation of Korea (NRF) grant funded by the Korea government through Ministry of Science and ICT Grant 2021R1A2C1009296. K Jodlowski and L Roszkowski are supported by the National Science Centre, Poland, research Grant 2015/18/A/ST2/00748. S R Klein is supported in part by the US NSF Grant PHY-1307472 and the US DOE Contract DE-AC-76SF00098. F Kling and P Quílez are supported by the DFG under Germany's Excellence Strategy—EXC 2121 Quantum Universe—390833306. P Ko is supported in part by KIAS Individual Grant PG021403 and by National Research Foundation of Korea (NRF) Grant NRF-2019R1A2C3005009. S Kulkarni is supported by the Austrian Science Fund Elise-Richter Grant V592-N27. The work of J Kumar is supported in part by US DOE Grant DE-SC0010504. J-L Kuo is supported by US NSF Theoretical Physics Program, Grant PHY-1915005. The work of C Le Roux and K Zapp is part of a project that has received funding from the ERC under the European Union's Horizon 2020 Research and Innovation Programme (Grant Agreement 803183, collectiveQCD). The work of H-S Lee was supported in part by the National Research Foundation of Korea (NRF-2021R1A2C2009718). S J Lee was supported by the Samsung Science and Technology Foundation. Ji Li is supported by the National Natural Science Foundation of China Grant 11905149. K-F Lyu and Z Liu are supported in part by the US DOE Grant DE-SC0022345. The work of R Maciula and A Szczurek was partially supported by the Polish National Science Centre under Grant 2018/31/B/ST2/03537. R Mammen Abraham and A Ismail acknowledge support from the US DOE Grant DE-SC0016013. M R Masouminia is supported by the UK Science and Technology Facilities Council (Grant ST/P001246/1). The work of J McFayden was supported by the Royal Society Fellowship Grant URF R1 201519. The work of O Mikulenko is supported by the NWO Physics Vrij Programme 'The Hidden Universe of Weakly Inter-acting Particles' with Project Number 680.92.18.03 (NWO Vrije Programma), which is (partly) financed by the Dutch Research Council (NWO). P Nadolsky and F Olness acknowledge support through US DOE Grant DE-SC0010129. E R Nocera thanks the STFC for support by the Grant Awards ST/P000630/1and ST/T000600/1. The work of N Okada is supported by the US DOE Grant DE-SC0012447. V Pandey acknowledges the support from US DOE Grant DE-SC0009824. The work of D Raut is supported by the US DOE Grant DE-SC0013880. P Reimitz acknowledges financial support from FAPESP Contract 2020/10004-7. M H Reno is supported in part by US DOE Grant DE-SC-0010113. The work of J Rojo is partly supported by the Dutch Research Council (NWO). L Roszkowski and S Trojanowski are supported by the grant 'AstroCeNT: Particle Astrophysics Science and Technology Centre' carried out within the International Research Agendas programme of the Foundation for Polish Science financed by the European Union under the European Regional Development Fund. S Trojanowski is also supported in part by the Polish Ministry of Science and Higher Education through its scholarship for young and outstanding scientists (Decision No. 1190/E-78/STYP/14/2019). S Trojanowski is also supported in part from the European Union's Horizon 2020 Research and Innovation Programme under Grant Agreement No. 952480 (DarkWave 24 project). I Sarcevic is supported by US DOE Grant DOE DE-SC-0009913. The work of L Shchutska is supported by the ERC under the European Union's Horizon 2020 Research and Innovation Programme (GA 758316). The work of T Shimomura is supported by JSPS KAKENHI Grants JP18H01210, JP18K03651, and MEXT KAKENHI Grant JP18H05543. The work of K Sinha is supported in part by US DOE Grant DE-SC0009956. The work of T Sjöstrand is supported by the Swedish Research Council, Contract 2016-05996. J T Sobczyk acknowledges support from NCN Grant UMO-2021/41/B/ST2/02778. D Soldin acknowledges support from the US NSF Grant PHY-1913607. H Song is supported by the International Postdoctoral Exchange Fellowship Program. Y Soreq is supported by grants from the NSF-BSF, BSF, the ISF and by the Azrieli foundation. A Stasto acknowledges support from US DOE Grant DE-SC-0002145. S Su is supported by the US DOE Grant DE-FG02-13ER41976/DE-SC0009913. W Su is supported by a KIAS Individual Grant (PG084201) at Korea Institute for Advanced Study. Y Takubo is supported by JP20K04004. M Taoso acknowledges support from the INFN Grant 'LINDARK', the research grant 'The Dark Universe: A Synergic Multimessenger Approach 2017X7X85' funded by MIUR, and the project 'Theoretical Astroparticle Physics (TAsP)' funded by the INFN. The research activities of B Thomas are supported in part by US NSF Grant PHY-2014104. The work of Y-D Tsai is supported in part by US NSF Grant PHY-1915005. The work of A Sabio Vera has been supported by the Spanish Research Agency (Agencia Estatal de Investigación) through the Grant IFT Centro de Excelencia Severo Ochoa SEV-2016-0597, by the Spanish Government Grant FPA2016-78022-P and from the European Union's Horizon 2020 Research and Innovation Programme under Grant Agreement 824093. The work of Yongchao Zhang is supported by the National Natural Science Foundation of China Grant 12175039, the 2021 Jiangsu Shuangchuang (Mass Innovation and Entrepreneurship) Talent Program JSSCBS20210144, and the 'Fundamental Research Funds for the Central Universities'. Yue Zhang is supported by the Arthur B McDonald Canadian Astroparticle Physics Research Institute. R Zukanovich Funchal is partially supported by Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) and Conselho Nacional de Ciência e Tecnologia (CNPq). The opinions and conclusions expressed herein are those of the authors and do not represent any funding agencies., High energy collisions at the High-Luminosity Large Hadron Collider (LHC) produce a large number of particles along the beam collision axis, outside of the acceptance of existing LHC experiments. The proposed Forward Physics Facility (FPF), to be located several hundred meters from the ATLAS interaction point and shielded by concrete and rock, will host a suite of experiments to probe standard model (SM) processes and search for physics beyond the standard model (BSM). In this report, we review the status of the civil engineering plans and the experiments to explore the diverse physics signals that can be uniquely probed in the forward region. FPF experiments will be sensitive to a broad range of BSM physics through searches for new particle scattering or decay signatures and deviations from SM expectations in high statistics analyses with TeV neutrinos in this low-background environment. High statistics neutrino detection will also provide valuable data for fundamental topics in perturbative and non-perturbative QCD and in weak interactions. Experiments at the FPF will enable synergies between forward particle production at the LHC and astroparticle physics to be exploited. We report here on these physics topics, on infrastructure, detector, and simulation studies, and on future directions to realize the FPF's physics potential., German Research Foundation (DFG) SFB 876 SFB 1491, National Science Foundation (NSF) PHY2112527, Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research (KAKENHI) JP18H01210 JSPS KAKENHI JP20K23373 JP19H01909 JSPS KAKENHI JP19J13812 JP21K20365 JSPS KAKENHI JP18K03651, European Research Council (ERC) 101002690, National Research Foundation of Korea NRF-2020R1I1A3072747, Patrimonio Autónomo-Fondo Nacional de Financiamiento para la Ciencia Tecnología y la Innovación Francisco José de Caldas (MinCiencias-Colombia) 80740-465-2020, European Commission Joint Research Centre 860881-HIDDeN European Union's Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie Grant 754446, United States Department of Energy (DOE) DE-SC0007914, Fermi National Accelerator Laboratory (Fermilab), a US DOE, Office of Science, HEP User Facility, Fermi Research Alliance, LLC (FRA) DE-AC02-07CH11359, German Research Foundation (DFG) HA 8555/1-1, DFG Collaborative Research Centre 'Neutrinos and Dark Matter in Astro-and Particle Physics' SFB 1258, Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) 2015/25884-4 2019/15149-6, United States Department of Energy (DOE) DE-SC0009920, Heising-Simons Foundation 2022-3319 2019-1179 2020-1840, ERC under the European Union's Horizon 2020 Research and Innovation Programme 694896 803183, UGR Research and Knowledge Transfer Found-Athenea3i, Ministry of Science and Innovation, Spain (MICINN) Spanish Government, SRA Grant PID2019-106087GB-C22, Junta de Andalucía A-FQM-472-UGR20, Fundacao para a Ciencia e a Tecnologia (FCT) CERN/FIS-PAR/0024/2019 03216/2017, United States Department of Energy (DOE) DE-SC0011702 DE-SC0017987 DE-FG02-13ER41976/DE-SC0009913 DE-SC0012704 DE-SC0010813 DE-AC02-76SF00515 DE-FG02-00ER41132 DE-AC-76SF00098 DE-SC0010504 DE-SC0022345 DE-SC0010129, US NSF through its employee IR/D program, National Key Research and Development Program of China 2020YFC2201501, National Natural Science Foundation of China (NSFC) 12022514 11875003 12047503, CAS Project for Young Scientists in Basic Research YSBR-006, Key Research Program of the CAS XDPB15, National Research Foundation of Korea (NRF)'s Grants 6N021413, Saramadan Contract ISEF/M/400279, National Science Foundation (NSF) PHY-1915005 PHY-2111427 PHY1430152 PHY-2014071 PHY-1307472 PHY-2014104, Simons Investigator Award 376204, Simons Foundation 623683, National Science Foundation (NSF) DGE-1839285, FAPESP Contract 2020/00174-2, UKRI Future Leaders Fellowship DARKMAP, Natural Sciences and Engineering Research Council of Canada (NSERC), German Research Foundation (DFG) EXC-2123 390837967, INFN/QFT@COLLIDERS project, European Union's H2020-MSCA Grant Agreement 101025085, Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET), ANPCyT, Federal Ministry of Education & Research (BMBF) 05H21GUCCA, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ), Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES), Fundacao de Amparo a Ciencia e Tecnologia do Estado do Rio Grande do Sul (FAPERGS), INCT-FNA 464898/2014-5, J C Bose Fellowship of Science and Engineering Research Board of Department of Science and Technology, Government of India JCB/2020/000011, National Science Foundation (NSF) PHY-2112025, UK Research & Innovation (UKRI) Science & Technology Facilities Council (STFC) Science and Technology Development Fund (STDF) ST/L000377/1, Grant ANID FONDECYT-Chile 1201673, ANID-Millennium Science Initiative Program ICN2019-044, Spanish Grant (AEI) PID2020-113775GBI00, Center for Forestry Research & Experimentation (CIEF) PROMETEO/2018/165, National Science Centre, Poland 2018/31/D/ST2/00813, International Postdoctoral Exchange Fellowship Program, KIAS Individual Grant PG021403, National Research Foundation of Korea NRF-2019R1A2C3005009, Austrian Science Fund Elise-Richter Grant V592-N27, US NSF Theoretical Physics Program PHY-1915005, Samsung, National Natural Science Foundation of China (NSFC) 11905149, Polish National Science Centre 2018/31/B/ST2/03537, UK Research & Innovation (UKRI) Science & Technology Facilities Council (STFC) ST/P001246/1, Royal Society of London URF R1 201519, Netherlands Organization for Scientific Research (NWO) 680.92.18.03 Physics Vrij Programme .The Hidden Universe of Weakly Inter-acting Particles' - Dutch Research Council (NWO), UK Research & Innovation (UKRI) Science & Technology Facilities Council (STFC) ST/T000600/1 ST/P000630/1, Netherlands Organization for Scientific Research (NWO), European Union under the European Regional Development Fund, Polish Ministry of Science and Higher Education through its scholarship for young and outstanding scientists 1190/E-78/STYP/14/2019, European Commission 952480, ERC under the European Union 758316, Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research (KAKENHI) JP18H05543 MEXT KAKENHI, Swedish Research Council 2016-05996, NCN UMO-2021/41/B/ST2/02778, NSF-BSF, US-Israel Binational Science Foundation, Israel Science Foundation, Azrieli foundation, KIAS Individual Grant at Korea Institute for Advanced Study PG084201, Istituto Nazionale di Fisica Nucleare (INFN), Ministry of Education, Universities and Research (MIUR) 2017X7X85', Spanish Government SEV-2016-0597 Spanish Research Agency (Agencia Estatal de Investigacion) through the Grant IFT Centro de Excelencia Severo Ochoa FPA2016-78022-P, European Union's Horizon 2020 Research and Innovation Programme 824093, National Natural Science Foundation of China (NSFC) 12175039, 2021 Jiangsu Shuangchuang (Mass Innovation and Entrepreneurship) Talent Program JSSCBS20210144, Fundamental Research Funds for the Central Universities, Arthur B McDonald Canadian Astroparticle Physics Research Institute, Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), United States Department of Energy (DOE) DE-SC0012447 DE-SC0009824 DE-SC0013880 :The US DOE DE-SC-0010113 DOE DE-SC-0009913 US DOE DE-SC0009956 DE-FG02-13ER41976/DESC0009913 US DOE JP20K04004

Published
2023
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25. Prospects for macroscopic dark matter detection at space-based and suborbital experiments

Author

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

Published
2021
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26. Monte Carlo simulations of neutrino and charged lepton propagation in the Earth with nuPyProp

Author

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

Published
2021
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30. POEMMA: Probe Of Extreme Multi-Messenger Astrophysics

Author

Olinto, Angela V., primary, Adams, James H., additional, Aloisio, Roberto, additional, Anchordoqui, Luis A., additional, Bergman, Doug R., additional, Bertaina, Mario E., additional, Bertone, Peter, additional, Christl, Mark J., additional, Csorna, Steven E., additional, Eser, Johannes, additional, Fenu, Francesco, additional, Hays, Elizabeth A., additional, Hunter, Stanley D., additional, Judd, Eleanor, additional, Jun, Insoo, additional, Krizmanic, John, additional, Kuznetsov, Evgeny, additional, Martinez-Sierra, L. M., additional, mastafa, malek, additional, Matthews, John N., additional, McEnery, Julie, additional, Mitchell, John W., additional, Neronov, Andrii, additional, Otte, A. Nepomuk, additional, Parizot, Etienne, additional, Paul, Thomas C., additional, Perkins, Jeremy S., additional, Prévôt, Guillaume, additional, Reardon, Patrick, additional, Reno, Mary Hall, additional, Sarazin, Frederic, additional, Shinozaki, Kenji, additional, Stecker, Floyd, additional, Streitmatter, Robert, additional, Wiencke, Lawrence, additional, and Young, Roy M., additional

Published
2017
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42. Non-invasive metabolomic analysis of breath using differential mobility spectrometry in patients with chronic obstructive pulmonary disease and healthy smokers

Author

Basanta, Maria, primary, Jarvis, Roger M., additional, Xu, Yun, additional, Blackburn, Gavin, additional, Tal-Singer, Ruth, additional, Woodcock, Ashley, additional, Singh, Dave, additional, Goodacre, Royston, additional, Paul Thomas, C. L., additional, and Fowler, Stephen J., additional

Published
2010
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45. Spatial variations in the microbial community structure and diversity of the human foot is associated with the production of odorous volatiles.

Author

Stevens, Deborah, Cornmell, Robert, Taylor, David, Grimshaw, Sally G., Riazanskaia, Svetlana, Arnold, David S., Fernstad, Sara Johansson, Smith, Adrian M., Heaney, Liam M., Reynolds, James C., Paul Thomas, C. L., and Harker, Mark

Subjects
SPATIAL variation, STAPHYLOCOCCUS, BACTERIAL growth, BACTERIAL colonies, BACTERIAL cultures, BACTERIAL population, ISOVALERIC acid
Abstract

The human foot provides an ideal environment for the colonization and growth of bacteria and subsequently is a body site associated with the liberation of odour. This study aimed to enumerate and spatially map bacterial populations' resident across the foot to understand any association with odour production. Culture-based analysis confirmed that Staphylococci were present in higher numbers than aerobic corynebacteria and Gram-positive aerobic cocci, with all species being present at much higher levels on the plantar sites compared to dorsal sites. Microbiomic analysis supported these findings demonstrating that Staphylococcus spp. were dominant across different foot sites and comprised almost the entire bacterial population on the plantar surface. The levels of volatile fatty acids, including the key foot odour compound isovaleric acid, that contribute tofoot odour were significantly increased at the plantar skin site compared to the dorsal surface. The fact that isovaleric acid was not detected on the dorsal surface but was present on the plantar surface is probably attributable to the high numbers of Staphylococcus spp. residing at this site. Variations in the spatial distribution of these microbes appear to be responsible for the localized production of odour across the foot. [ABSTRACT FROM AUTHOR]

Published
2015
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50. Photochemistry of refractive index structures in poly(methyl methacrylate) by femtosecond laser irradiation

Author

Baum, Alexandra, Scully, Patricia J., Basanta, Maria, Paul Thomas, C. L., Fielden, Peter R., Goddard, Nicholas J., Perrie, Walter, and Chalker, Paul R.

Abstract

Femtosecond, subablation threshold photomodification of poly(methyl methacrylate) (PMMA) at 387nm is explored to enable fabrication of optical components. Volatile fragment analysis (thermal desorption gas chromatography-mass spectrometry) and molecular weight distribution monitoring (size exclusion chromatography) suggest photochemical modification, involving direct cleavage of the polymer backbone and propagation via chain unzipping under formation of monomers, similar to the pyrolytic degradation of PMMA. Waveguides were produced in undoped, clinical-grade PMMA, showing an increased refractive index in the laser focal region (Δn_max=4×10^−3).

Published
2007

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