Ultra-High Energy Cosmic Rays Detected by Auger and AGASA:Corrections for Galactic Magnetic Field Deflections, Source Populations, and Arguments for Multiple-Components

TL;DR

This study refines the understanding of UHECR origins by modeling their deflections in Galactic magnetic fields, supporting radiogalaxies as potential sources and highlighting the complexity of cosmic ray compositions.

Contribution

It introduces detailed Monte Carlo simulations accounting for GMF uncertainties to better identify UHECR source populations and compositions.

Findings

Correlation between UHECRs and radiogalaxies is strengthened by GMF models.

Nearby radiogalaxies like CenA are likely sources of multiple UHECRs.

A significant portion of UHECRs could originate from extended radiogalaxies with specific magnetic field conditions.

Abstract

The origin and composition of Ultra-High Energy Cosmic Ray Events (UHECRs) are under debate. Here we improve constraints on the source population(s) and compositions of UHECRs by accounting for UHECR deflections within existing Galactic magnetic field models (GMFs). We used Monte Carlo simulations for UHECRs detected by the Pierre Auger Observatory and AGASA in order to determine their outside-the-Galaxy arrival directions, and compared these with Galactic and extragalactic sources. The simulations, which used UHECR compositions from protons to Iron and seven models of the ordered GMF, include uncertainties in the GMF and a turbulent magnetic field. The correlation between UHECRs and nearby extended radiogalaxies (Nagar & Matulich 2008) remains valid, even strengthened, within several GMF models. Both the nearest radiogalaxy CenA, and the nearest radio-extended BL Lac, CGCG 413-019, are likely sources of multiple UHECRs. The correlation appears to be linked to the presence of the extended radio source rather than a tracer of an underlying population. It is possible, but unlikely, that all UHECRs originate in the nearby radiogalaxy CenA. For light UHECRs about a third of UHECRs can be "matched" to nearby galaxies with extended radio jets. The remaining UHECRs could also be explained as originating in extended radiogalaxies if one has at least one of: a large UHECR mean free path, a high cluster and/or intergalactic magnetic field, a heavy composition for two-thirds of the detected UHECRs. Several UHECRs have trajectories which pass close to Galactic magnetars and/or microquasars. If extended radiogalaxies are, or trace, UHECR sources, the most consistent models for the ordered GMF are the BS-S and BS-A models; the GMF models of Sun et al. 2008 are acceptable if a dipole component is added.