Limit on intergalactic magnetic field from ultra-high-energy cosmic ray hotspot in Perseus-Pisces region

Neronov, A.; Semikoz, D.; Kalashev, O.

doi:10.48550/arxiv.2112.08202

Cited by 4 publications

(5 citation statements)

References 35 publications

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“…If the data collected in the next decade corroborate the existence of hot spots in the UHECR sky, then their location and angular extend will provide important insights on the GMF and IGMF, as demonstrated in studies using the current indications for these intermediate-scale anisotropies, see e.g., Refs. [525][526][527].…”

Section: Insights Into Magnetic Fields From Future Uhecr Observationsmentioning

confidence: 99%

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Coleman,

Eser,

Mayotte

et al. 2022

Preprint

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Pin down the shower energy observable to use μ as a composition-only Reduce hadronic uncertainties interaction model E threshold (TBD) Other messengers Galactic * μ / em separation † * depending on analysis progress † depending on detector configuration• At least one next-generation experiment needs to be able to make high-precision measurements to explore new particle physics and measure particle rigidity on an event-by-event basis. Of the planned next-generation experiments, GCOS is the best positioned to meet this recommendation.• As a complementary effort, experiments with sufficient exposure ( 5 × 10 5 km 2 sr yr) are needed to search for Lorentz-invariance violation (LIV), SHDM, and other BSM physics at the Cosmic and Energy Frontiers, and to identify UHECR sources at the highest energies.• Full-sky coverage with low cross-hemisphere systematic uncertainties is critical for astrophysical studies. To this end, next generation experiments should be space-based or multi-site. Common sites between experiments are encouraged.• Based on the productive results from inter-collaboration and inter-disciplinary work, we recommend the continued progress/formation of joint analyses between experiments and with other intersecting fields of research (e.g., magnetic fields).• The UHECR community should continue its efforts to advance diversity, equity, inclusion, and accessibility. It also needs to take steps to reduce its environmental impacts and improve open access to its data to reduce the scientific gap between countries.vi

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Section: Insights Into Magnetic Fields From Future Uhecr Observationsmentioning

confidence: 99%

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Coleman,

Eser,

Mayotte

et al. 2022

Preprint

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“…The magnetic field can be additionally constrained from above by observations of ultra-high-energy cosmic rays (UHECR) sources. Recent observations of UHECR from the Perseus-Pisces supercluster [80] allowed for the first time to put an upper limit on the primordial magnetic field in the voids of the LSS [81]. Finally, the upper bounds from Faraday rotation measurements [79] are shown in Fig.…”

Section: Constraints On the Magnetic Field Amplitude And Characterist...mentioning

confidence: 92%

“…The blue line shows the expected sensitivity of CTA [53]. At larger scales, the upper bound from Faraday rotation (FR) is shown [79], and the blue shaded region indicates the observations of UHECR from the Perseus-Pisces supercluster [80,81]. Note that the latter constraints refer to present time magnetic field strength and characteristic scale, and they have been cut to avoid intersecting the evolutionary paths from the QCD phase transition up to recombination in the plot, for clarity.…”

Section: Constraints On the Magnetic Field Amplitude And Characterist...mentioning

confidence: 99%

Gravitational wave signal from primordial magnetic fields in the Pulsar Timing Array frequency band

Pol,

Caprini,

Neronov

et al. 2022

Preprint

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“…Upper limits at the 10 −9 G level come from a variety of CMB observations (see Table 1 of [58]). More stringent upper limits of 10 −10 G come from UHECR correlations with the Perseus-Pisces supercluster [59] and even 5 × 10 −11 G from nonobservation of small-scale baryonic density fluctuations [58]. Here, we assume that EGMF are smaller than 10 −11 G in the voids and neglect their influence on GZK photons.…”

Section: Icecubementioning

confidence: 99%

Upper Limit on the Diffuse Radio Background from GZK Photon Observation

2022

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Here, we point out that an observation of ultrahigh energy cosmic ray (UHECR) photons, “GZK photons”, could provide an upper limit on the level of the extragalactic radio background, depending on the level of UHECR proton primaries (to be determined after a few years of data taking by the Pierre Auger Observatory upgrade AugerPrime). We also update our 2005 prediction of the range of GZK photon fluxes expected from proton primaries.

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Limit on intergalactic magnetic field from ultra-high-energy cosmic ray hotspot in Perseus-Pisces region

Cited by 4 publications

References 35 publications

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Gravitational wave signal from primordial magnetic fields in the Pulsar Timing Array frequency band

Upper Limit on the Diffuse Radio Background from GZK Photon Observation

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