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The brightest GRB ever detected: GRB 221009A as a highly luminous event at z = 0.151
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abstract
Context: The extreme luminosity of gamma-ray bursts (GRBs) makes them powerful beacons for studies of the distant Universe. The most luminous bursts are typically detected at moderate/high redshift, where the volume for seeing such rare events is maximized and the star-formation activity is greater than at z = 0. For distant events, not all observations are feasible, such as at TeV energies. Aims: Here we present a spectroscopic redshift measurement for the exceptional GRB 221009A, the brightest GRB observed to date with emission extending well into the TeV regime. Methods: We used the X-shooter spectrograph at the ESO Very Large Telescope (VLT) to obtain simultaneous optical to near-IR spectroscopy of the burst afterglow 0.5 days after the explosion. Results: The spectra exhibit both absorption and emission lines from material in a host galaxy at z = 0.151. Thus GRB 221009A was a relatively nearby burst with a luminosity distance of 745 Mpc. Its host galaxy properties (star-formation rate and metallicity) are consistent with those of LGRB hosts at low redshift. This redshift measurement yields information on the energy of the burst. The inferred isotropic energy release, $E_{\rm iso} > 5 \times 10^{54}$ erg, lies at the high end of the distribution, making GRB 221009A one of the nearest and also most energetic GRBs observed to date. We estimate that such a combination (nearby as well as intrinsically bright) occurs between once every few decades to once per millennium.
Forward citations
Cited by 10 Pith papers
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Accretion Regimes of Neutrino-Cooled Flows onto Black Holes
A 1D relativistic disk model charts the accretion regimes of neutrino-cooled flows and predicts r-process outflows up to black hole masses of about 3000 solar masses.
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Late-time HST and JWST Observations of GRB 221009A: Evidence for a Break in the Light Curve at 50 Days
Late-time HST and JWST photometry of GRB 221009A provides evidence for a break in the afterglow light curve at about 50 days, a blue excess component, and a supernova no brighter than 1.5 times SN 1998bw.
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Extreme value distribution for gamma-ray-burst prompt data -- How unexpected was the BOAT event?
Using generalized extreme value fits to 30-day maxima from Fermi-GBM and BATSE, the fluence and peak flux of GRB 221009A are extreme outliers, with median return periods of about 1000 years and 140 years respectively.
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The optical constants and grain sizes of interstellar dust measured directly using the dust scattered x-ray halo of GRB 221009A
Using the fading X-ray rings of GRB 221009A, the authors infer the complex refractive index and grain size distribution of Milky Way dust, finding a maximum grain radius of 0.24 micrometers and an iron mass fraction of 35%.
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Insight-HXMT observations of the extremely bright GRB 221009A
Insight-HXMT's ME and LE telescopes, detecting secondary particles rather than direct gamma rays, recovered the main burst light curve of GRB 221009A and measured a minimum variability timescale of 0.10 s.
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Carpet-3 detection of a photon-like air shower with estimated primary energy above 100 TeV in a spatial and temporal coincidence with GRB 221009A
Carpet-3 reports a photon-like air shower with estimated energy around 300 TeV arriving from the direction of GRB 221009A about 75 minutes after the trigger, with a coincidence probability of about 0.9 percent.
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Polarization of impulsive relativistic jets propagating in a stratified medium
Stratified external media reduce and slow the temporal evolution of afterglow polarization in impulsive jets, with the polarization peak near the geometrical light-curve break.
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TeV Afterglow of BOAT GRB without Jet Break
A magnetized, thick ejecta with an inverted circumstellar density profile can reproduce GRB 221009A's TeV light curve without invoking an early jet break.
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GRB 221009A and the Apparently Most Energetic Gamma-Ray Bursts
Using 185 energetic gamma-ray bursts, the authors confirm a cutoff near Eiso = 4×10^54 erg that is not invalidated by GRB 221009A.
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