New LOFAR radio data and X-ray modeling indicate the extended source is thermal ICM emission from a massive merging galaxy cluster, unrelated to 1LHAASO J0343+5254u.
Title resolution pending
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
citation-role summary
background 1
citation-polarity summary
fields
astro-ph.HE 5years
2026 5roles
background 1polarities
background 1representative citing papers
A neutrino flare in GB6 J1542+6129 precedes gamma-ray and radio activity by about one year, indicating upstream neutrino production near the AGN central engine.
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.
Several nearby AGN ultra-fast outflows are predicted to produce detectable very-high-energy gamma rays via shock-accelerated protons, visible to CTAO even if invisible to Fermi-LAT.
Fermi-LAT variability analysis of jetted AGNs finds mean damping timescales of ~100 days, greater amplitudes in FSRQs than BL Lacs, emission regions at 2-4.5 R_DT but 123-295 R_BLR, and correlations with luminosities, loudness, black hole mass, and Eddington ratio.
citing papers explorer
-
Multi-wavelength insights into the pulsar wind nebula candidate near 1LHAASO J0343+5254u: an obscured merging galaxy cluster?
New LOFAR radio data and X-ray modeling indicate the extended source is thermal ICM emission from a massive merging galaxy cluster, unrelated to 1LHAASO J0343+5254u.
-
Upstream neutrino production and delayed jet emission in the blazar GB6 J1542+6129
A neutrino flare in GB6 J1542+6129 precedes gamma-ray and radio activity by about one year, indicating upstream neutrino production near the AGN central engine.
-
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.
-
Very High Energy Gamma Rays from Ultra Fast Outflows
Several nearby AGN ultra-fast outflows are predicted to produce detectable very-high-energy gamma rays via shock-accelerated protons, visible to CTAO even if invisible to Fermi-LAT.
-
Characterizing the origins of gamma-ray variability of the jetted active galactic nuclei observed with the Fermi-LAT
Fermi-LAT variability analysis of jetted AGNs finds mean damping timescales of ~100 days, greater amplitudes in FSRQs than BL Lacs, emission regions at 2-4.5 R_DT but 123-295 R_BLR, and correlations with luminosities, loudness, black hole mass, and Eddington ratio.