Limit on Supernova Emission in the Brightest Gamma-ray Burst, GRB 221009A

Shrestha, Manisha; Sand, David J.; Alexander, K. D.; Bostroem, K. Azalee; Hosseinzadeh, G.; Aghakhanloo, Mojgan; Vinkó, J.; Andrews, Jennifer E.; Jencson, J.; Lundquist, M.; Wyatt, S.; Howell, D. A.; McCully, C.; González, E. P.; Pellegrino, C.; Terreran, G.; Hiramatsu, D.; Newsome, Megan; Farah, Joseph; Smith, Nathan; Wheeler, J. C.; Martı́nez-Vázquez, C. E.; Carballo‐Bello, J. A.; Drlica-Wagner, A.; James, D. J.; Mutlu-Pakdil, Burçin; Stringfellow, Guy S.; Sakowska, J. D.; Noël, Noelia E. D.; Kuêhn, K.

doi:10.48550/arxiv.2302.03829

Cited by 4 publications

(9 citation statements)

References 58 publications

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“…Their data are in excellent agreement with ours, even though no image subtraction was undertaken. The z-filter data of Laskar et al (2023) and Shrestha et al (2023) are slightly brighter than ours after 8-10 days, which may suggest some host-galaxy contribution affects their measurements. The converted y filter from the HST data of Levan et al (2023) are fainter than ours by ∼0.3 mag at the respective epochs, which we attribute to the combined galaxy plus PSF fits of Levan et al (2023).…”

Section: Interpretation Of the Excess Flux As A Supernova Signaturecontrasting

confidence: 64%

“…We compare our r-and i-filter photometry with original data (not GCN values) in Laskar et al (2023), Shrestha et al (2023 and Levan et al (2023), three papers that suggest there is no strong evidence for an SN component in the data. Their data are in excellent agreement with ours, even though no image subtraction was undertaken.…”

Section: Interpretation Of the Excess Flux As A Supernova Signaturementioning

confidence: 97%

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The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

Fulton

Smartt

Rhodes

et al. 2023

ApJL

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We present extensive optical photometry of the afterglow of GRB 221009A. Our data cover 0.9–59.9 days from the time of Swift and Fermi gamma-ray burst (GRB) detections. Photometry in rizy-band filters was collected primarily with Pan-STARRS and supplemented by multiple 1–4 m imaging facilities. We analyzed the Swift X-ray data of the afterglow and found a single decline rate power law f(t) ∝ t −1.556±0.002 best describes the light curve. In addition to the high foreground Milky Way dust extinction along this line of sight, the data favor additional extinction to consistently model the optical to X-ray flux with optically thin synchrotron emission. We fit the X-ray-derived power law to the optical light curve and find good agreement with the measured data up to 5−6 days. Thereafter we find a flux excess in the riy bands that peaks in the observer frame at ∼20 days. This excess shares similar light-curve profiles to the Type Ic broad-lined supernovae SN 2016jca and SN 2017iuk once corrected for the GRB redshift of z = 0.151 and arbitrarily scaled. This may be representative of an SN emerging from the declining afterglow. We measure rest-frame absolute peak AB magnitudes of M g = −19.8 ± 0.6 and M r = − 19.4 ± 0.3 and M z = −20.1 ± 0.3. If this is an SN component, then Bayesian modeling of the excess flux would imply explosion parameters of M ej = 7.1 − 1.7 + 2.4 M ⊙, M Ni = 1.0 − 0.4 + 0.6 M ⊙, and v ej = 33,900 − 5700 + 5900 km s−1, for the ejecta mass, nickel mass, and ejecta velocity respectively, inferring an explosion energy of E kin ≃ 2.6–9.0 × 1052 erg.

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Section: Interpretation Of the Excess Flux As A Supernova Signaturecontrasting

confidence: 64%

Section: Interpretation Of the Excess Flux As A Supernova Signaturementioning

confidence: 97%

The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

Fulton

Smartt

Rhodes

et al. 2023

ApJL

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“…These relations provide decline indices of α 2 ∼ 1.675 and α 1 ∼ 1.425 and are similar to the observed afterglow decline rates at both X-ray and optical/NIR frequencies. This result is consistent with the "no observed SN" scenario described in Shrestha et al (2023), where the light curve is dominated by emission from the GRB afterglow only with no significant SN contribution, and consistent with the lack of any SN features in the spectra at >10 days.…”

Section: Implications For Afterglow Modelssupporting

confidence: 91%

“…Similarly, for ν < ν c , then β = (p − 1)/2, and for β = 0.3 we find a consistent p = 1.6. However, the steep temporal decline of the afterglow (where F ν (t) ∝ ν − β t − α ), with α ∼ 1.67 at X-ray frequencies (Williams et al 2023), and α ∼ 1.44 at optical/NIR (Shrestha et al 2023) is not consistent with the expected decline rate, given these spectral regimes and p < 2 using standard closure relations. To resolve this, we invoke a very early jet break without significant lateral spreading, that steepens the temporal index by three-fourths, and the temporal index for an ISM medium with p < 2 is then (Gao et al 2013)…”

Section: Implications For Afterglow Modelsmentioning

confidence: 83%

“…Despite these challenges, observations to date have yielded a rich data set across the electromagnetic spectrum (e.g., Fulton et al 2023;Kann et al 2023;Laskar et al 2023;O'Connor et al 2023;Shrestha et al 2023;Williams et al 2023). These data paint a complex picture of a burst with multiple components not readily subsumed within standard afterglow models.…”

Section: Introductionmentioning

confidence: 99%

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The First JWST Spectrum of a GRB Afterglow: No Bright Supernova in Observations of the Brightest GRB of all Time, GRB 221009A

Levan

Lamb

Schneider

et al. 2023

ApJL

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We present James Webb Space Telescope (JWST) and Hubble Space Telescope (HST) observations of the afterglow of GRB 221009A, the brightest gamma-ray burst (GRB) ever observed. This includes the first mid-IR spectra of any GRB, obtained with JWST/Near Infrared Spectrograph (0.6–5.5 micron) and Mid-Infrared Instrument (5–12 micron), 12 days after the burst. Assuming that the intrinsic spectral slope is a single power law, with F ν ∝ ν −β , we obtain β ≈ 0.35, modified by substantial dust extinction with A V = 4.9. This suggests extinction above the notional Galactic value, possibly due to patchy extinction within the Milky Way or dust in the GRB host galaxy. It further implies that the X-ray and optical/IR regimes are not on the same segment of the synchrotron spectrum of the afterglow. If the cooling break lies between the X-ray and optical/IR, then the temporal decay rates would only match a post-jet-break model, with electron index p < 2, and with the jet expanding into a uniform ISM medium. The shape of the JWST spectrum is near-identical in the optical/near-IR to X-SHOOTER spectroscopy obtained at 0.5 days and to later time observations with HST. The lack of spectral evolution suggests that any accompanying supernova (SN) is either substantially fainter or bluer than SN 1998bw, the proto-type GRB-SN. Our HST observations also reveal a disk-like host galaxy, viewed close to edge-on, that further complicates the isolation of any SN component. The host galaxy appears rather typical among long-GRB hosts and suggests that the extreme properties of GRB 221009A are not directly tied to its galaxy-scale environment.

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JWST detection of heavy neutron capture elements in a compact object merger

Levan,

Gompertz,

Salafia

et al. 2023

Preprint

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The mergers of binary compact objects such as neutron stars and black holes are of central interest to several areas of astrophysics, including as the progenitors of gamma-ray bursts (GRBs), sources of high-frequency gravitational waves and likely production sites for heavy element nucleosynthesis via rapid neutron capture (the r-process). These heavy elements include some of great geophysical, biological and cultural importance, such as thorium, iodine, and gold. Here we present observations of the exceptionally bright gamma-ray burst GRB230307A. We show that GRB 230307A belongs to the class of long-duration gamma-ray bursts associated with compact object mergers, and contains a kilonova similar to AT2017gfo, associated with the gravitational-wave merger GW170817. We obtained James Webb Space Telescope mid-infrared (mid-IR) imaging and spectroscopy 29 & 61 days after the burst. The spectroscopy shows an emission line at 2.1 microns which we interpret as tellurium (atomic mass A=130), and a very red source, emitting most of its light in the mid-IR due to the production of lanthanides. These observations demonstrate that nucleosynthesis in GRBs can create r-process elements across a broad atomic mass range and play a central role in heavy element nucleosynthesis across the Universe.

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Limit on Supernova Emission in the Brightest Gamma-ray Burst, GRB 221009A

Cited by 4 publications

References 58 publications

The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

The First JWST Spectrum of a GRB Afterglow: No Bright Supernova in Observations of the Brightest GRB of all Time, GRB 221009A

JWST detection of heavy neutron capture elements in a compact object merger

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