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Current and future limits on the ALP-photon coupling (a) and ALP-electron coupling (b). The blue bands show the 1 and 2 sensitivities from the Monte Carlo runs and the blue solid line the median. The black solid line in figure (b) represents the XENON1T limit at 90% C.L. [31] and the dark grey box highlights roughly the best-fit parameter space from Ref. [32].
Contexts in source publication
Context 1
... as a black star, with mass = 7.1 keV and mixing angle sin 2 (2) = 7 × 10 −11 . We find that with an exposure time of = 2.5 ks, eROSITA will be sensitive to the 3.5 keV line and can even constrain the mixing angles up to nearly two orders of magnitude below the best-fit at = 7.1 keV. The sensitivity of eROSITA to the photon coupling is shown in Fig. 2a, where the best-fit for the 3.5 keV line is indicated by the black star. Even though recent work found no evidence for an unassociated X-ray line [8], in which the current X-ray limits are shown as the grey shaded area (see [8,[23][24][25][26][27][28][29]), eROSITA will be able to probe a region of the parameter space not yet excluded ...
Context 2
... we test if eROSITA will be able to probe the parameter space relevant for the observed XENON1T excess, which has been observed to be most prominent at ALP mass of = 2-3 keV and electron coupling ∼ 10 −13 . An anomaly-free ALP model is adopted, for which the expected sensitivity is presented in Fig. 2b. The excluded region based on X-ray observations are in grey, and indeed, we probe a parameter space not yet constrained [8,[23][24][25][26][27][28][29]. The expected sensitivity of Athena taken from Ref. [30] show comparable sensitivity, as shown as the red dashed dotted line. The black solid line shows the XENON1T limit at 90% CL ...
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Citations
... One way to test this scenario is to search for the fluxes of SM particles produced by the evaporation of PBHs. Limits from current data exclude the portion of parameter space in blue in fig. 3 Taken from [29]. Upper limits on the couplings of ALPs with photons from Fermi-LAT observations. ...
... For instance, a sterile neutrino can decay into an active neutrino and a photon, a process occurring through the mixing with active neutrinos. Prospects for detection with eROSITA have been presented in [29] (see also [35] for the prospects of X-ray telescopes for DM signals from dwarf spheroidal galaxies). This experiment covers the energy range 0.3-10 keV, and has an excellent energy resolution, an important requirement to look for line signals. ...
... This experiment covers the energy range 0.3-10 keV, and has an excellent energy resolution, an important requirement to look for line signals. Exploiting the full sky coverage of eROSITA, [29] focuses on signals from the galactic halo, considering latitudes |b| > 20 degrees. The sensitivity reach for sterile neutrinos is presented in fig. ...