Why do Auger and Telescope Array spectra differ above 3 * 10^19 eV? · revision history

Revision 2

Accepted · core change · record

Changes against revision 1:

Title · changed
Revision 1: Why do Auger and Telescope Array spectra differ above $3e19\,\mathrm{eV}$?
Revision 2: Why do Auger and Telescope Array spectra differ above $3 \times 10^{19}\,\mathrm{eV}$?
Plain
The two largest cosmic-ray observatories, one in each hemisphere, disagree on how many particles arrive at the very highest energies.
Precise · changed · core
Revision 1: After cross-calibration of energy scales, the Telescope Array flux above $\sim 3e19\ \mathrm{eV}$ and its suppression energy remain higher than those of the Pierre Auger Observatory. Determine whether the residual difference is instrumental (energy-scale nonlinearity, aperture, atmospheric corrections) or a real dependence on sky direction that would imply a nearby source in the northern sky. Answer: yes or no for a direction-dependent flux, with significance after systematics, evaluated in the declination band seen by both.
Revision 2: After cross-calibration of energy scales, the Telescope Array flux above $\sim 3 \times 10^{19}\ \mathrm{eV}$ and its suppression energy remain higher than those of the Pierre Auger Observatory. Determine whether the residual difference is instrumental (energy-scale nonlinearity, aperture, atmospheric corrections) or a real dependence on sky direction that would imply a nearby source in the northern sky. Answer: yes or no for a direction-dependent flux, with significance after systematics, evaluated in the declination band seen by both.
Settled by
Measurements in the common declination band with identical detector types at both sites, such as Auger-type surface stations operated at the Telescope Array site.
Kind
well-posed
Answer type
yes-no
References
(empty)
Literature status
contested
Status note
(empty)
Posed since
(empty)

Decisions