SMA detected a 6.9 mJy source at 1.3 mm from GRB 260127A 12.6 minutes post-trigger with a 2.7 arcsec offset from the optical position; no emission was seen 1.9 days later, implying a decline at least as steep as t to the -0.5.
Title resolution pending
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
fields
astro-ph.HE 3years
2026 3verdicts
UNVERDICTED 3representative citing papers
The GeV emission zone in Cygnus X-3 is too large and magnetized too weakly to accelerate protons to PeV energies, so the PeV gamma rays must originate from a more compact inner region with rapid magnetic field dissipation.
The counterjet dominates PeV photon production in Cyg X-3 due to longer interaction paths through the donor star's wind at low inclination.
citing papers explorer
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Rapid-response 1.3 mm Observations of GRB 260127A with the Submillimeter Array
SMA detected a 6.9 mJy source at 1.3 mm from GRB 260127A 12.6 minutes post-trigger with a 2.7 arcsec offset from the optical position; no emission was seen 1.9 days later, implying a decline at least as steep as t to the -0.5.
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Constraining the PeV gamma-ray emission zone of Cygnus X-3 with contemporaneous GeV timing and spectral observations
The GeV emission zone in Cygnus X-3 is too large and magnetized too weakly to accelerate protons to PeV energies, so the PeV gamma rays must originate from a more compact inner region with rapid magnetic field dissipation.
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The counterjet dominates the production of PeV photons from Cyg X-3
The counterjet dominates PeV photon production in Cyg X-3 due to longer interaction paths through the donor star's wind at low inclination.