No kilonova detected from sub-solar GW candidate S251112cm, but coincident IIb supernova SN 2025adtq yields suggestive evidence for the superkilonova channel, though inconclusive after accounting for chance coincidence.
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4 Pith papers cite this work. Polarity classification is still indexing.
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A coordinated Rubin-DESI supernova survey could distinguish dynamical dark energy from Lambda CDM at over 5 sigma in one year using 2300 spectroscopically confirmed SNe Ia at low redshift.
EP260321a is identified as the faintest shock breakout X-ray transient associated with broad-lined Ic supernova SN 2026gzf, interpreted as originating from a mildly relativistic weak outflow choked inside the progenitor star.
GRB 260310A/SN 2026fgk is a spectroscopically confirmed Type Ic-BL supernova at z=0.153 with 0.4-0.6 times the luminosity of SN 1998bw, nickel mass 0.4-0.5 solar masses, ejected mass 4-6 solar masses, kinetic energy (3-8) x 10^51 erg, and located at a 15 kpc offset due to the host's extended light p
citing papers explorer
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Electromagnetic Follow-up of the Sub-Solar Mass Gravitational Wave Candidate S251112cm: Kilonova Constraints and a Coincident IIb Supernova
No kilonova detected from sub-solar GW candidate S251112cm, but coincident IIb supernova SN 2025adtq yields suggestive evidence for the superkilonova channel, though inconclusive after accounting for chance coincidence.
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EP260321a/SN 2026gzf: The Faintest Shock Breakout Associated with a Broad-Lined Supernova
EP260321a is identified as the faintest shock breakout X-ray transient associated with broad-lined Ic supernova SN 2026gzf, interpreted as originating from a mildly relativistic weak outflow choked inside the progenitor star.
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GRB 260310A/SN 2026fgk: Photometric and Spectroscopic Evolution of a Nearby GRB-Supernova and an Exceptionally Bright Afterglow at z=0.153
GRB 260310A/SN 2026fgk is a spectroscopically confirmed Type Ic-BL supernova at z=0.153 with 0.4-0.6 times the luminosity of SN 1998bw, nickel mass 0.4-0.5 solar masses, ejected mass 4-6 solar masses, kinetic energy (3-8) x 10^51 erg, and located at a 15 kpc offset due to the host's extended light p