Galaxy cluster counts from eRASS1 plus weak lensing data set the tightest existing upper bounds on ultralight axion relic density Ω_a around 10^{-27} eV (Ω_a < 0.0035) and 10^{-26} eV (Ω_a < 0.0079) at 95% CL.
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3 Pith papers cite this work. Polarity classification is still indexing.
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Abeona is confirmed as a faint ~30 arcmin bilateral radio SNR shell with synchrotron polarization, flux density 1.5 Jy, and a spatially coincident 5.7-sigma GeV gamma-ray source.
Stacking analysis yields L-M slope 1.56, slightly steeper than self-similar, with X-ray detected clusters showing more centrally concentrated profiles than undetected ones.
citing papers explorer
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The SRG/eROSITA all-sky survey: Constraints on Ultra-light Axion Dark Matter through Galaxy Cluster Number Counts
Galaxy cluster counts from eRASS1 plus weak lensing data set the tightest existing upper bounds on ultralight axion relic density Ω_a around 10^{-27} eV (Ω_a < 0.0035) and 10^{-26} eV (Ω_a < 0.0079) at 95% CL.
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Radio detection of supernova remnant G310.7-5.4 with $\gamma$-ray counterpart: Abeona SNR
Abeona is confirmed as a faint ~30 arcmin bilateral radio SNR shell with synchrotron polarization, flux density 1.5 Jy, and a spatially coincident 5.7-sigma GeV gamma-ray source.
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The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray stacking analysis of Subaru's optically selected clusters spanning low richness regime
Stacking analysis yields L-M slope 1.56, slightly steeper than self-similar, with X-ray detected clusters showing more centrally concentrated profiles than undetected ones.