A Sensitive Search for Supernova Emission Associated with the Extremely Energetic and Nearby GRB 221009A

Srinivasaragavan, Gokul P.; O’Connor, B.; Cenko, S. Bradley; Dittmann, Alexander J.; Yang, S.; Sollerman, J.; Anupama, G. C.; Barway, Sudhanshu; Bhalerao, V.; Kumar, Harsh; Swain, Vishwajeet; Hammerstein, Erica; Isiah, Holt,; Anand, S.; Andreoni, Igor; Coughlin, M. W.; Dichiara, S.; Gal‐Yam, A.; Miller, M. Coleman; Soon, J.; Soria, Roberto; Durbak, J. M.; Gillanders, J.; Laha, Sibasish; Moore, Anna; Ragosta, Fabio; Troja, E.

doi:10.3847/2041-8213/accf97

“…With the triggering pulse having thermally dominant spectral properties, a clear and distinct start time, a derived emitting shell radius consistent with that of a Wolf-Rayet progenitor star, along with the discovery of the associated supernova SN 2022xiw (de Ugarte Postigo et al 2022a;Fulton et al 2023;Maiorano et al 2022;Srinivasaragavan et al 2023), GRB 221009A is likely the result of a massive core-collapse supernova progenitor. Although the beam-corrected E γ value of ( ) q 6.1 10 2 j 51 2 erg from Section 8 is within the maximum energy release limit for a magnetar progenitor (∼3 × 10 52 erg; Usov 1992), this progenitor source is unlikely.…”

Section: Central Enginementioning

confidence: 87%

Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow

Lesage¹,

Veres²,

Briggs³

et al. 2023

ApJL

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We report the discovery of GRB 221009A, the highest flux gamma-ray burst (GRB) ever observed by the Fermi Gamma-ray Burst Monitor (Fermi-GBM). This GRB has continuous prompt emission lasting more than 600 s, which smoothly transitions to afterglow emission visible in the Fermi-GBM energy range (8 keV–40 MeV), and total energetics higher than any other burst in the Fermi-GBM sample. By using a variety of new and existing analysis techniques we probe the spectral and temporal evolution of GRB 221009A. We find no emission prior to the Fermi-GBM trigger time (t 0; 2022 October 9 at 13:16:59.99 UTC), indicating that this is the time of prompt emission onset. The triggering pulse exhibits distinct spectral and temporal properties suggestive of the thermal, photospheric emission of shock breakout, with significant emission up to ∼15 MeV. We characterize the onset of external shock at t 0 + 600 s and find evidence of a plateau region in the early-afterglow phase, which transitions to a slope consistent with Swift-XRT afterglow measurements. We place the total energetics of GRB 221009A in context with the rest of the Fermi-GBM sample and find that this GRB has the highest total isotropic-equivalent energy (E γ,iso = 1.0 × 1055 erg) and second highest isotropic-equivalent luminosity (L γ,iso = 9.9 × 1053 erg s–1) based on its redshift of z = 0.151. These extreme energetics are what allowed us to observe the continuously emitting central engine of Fermi-GBM from the beginning of the prompt emission phase through the onset of early afterglow.

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“…Furthermore, in order to account for systematic uncertainties due to combining data from multiple telescopes (s-corrections; Stritzinger et al 2002), we numerically optimize the likelihood function assuming that the reported errors actually underestimate the true uncertainty. We do this using the same method as Srinivasaragavan et al (2023), by introducing an error-stretching factor β in the fitting procedure to represent the s-correction.…”

Section: Sn1998bw Obsmentioning

confidence: 99%

“…An SN is not always detected for nearby LGRBs (Della Valle et al 2006;Fynbo et al 2006;Gal-Yam et al 2006;Tanga et al 2018), and the physical link between LGRBs and their associated SN is also not clear. Studies of the brightest GRB of all time, GRB 221009A (Frederiks et al 2023a;Lesage et al 2023b;Burns et al 2023;Kann et al 2023;Laskar et al 2023;LHAASO Collaboration et al 2023;Malesani et al 2023;O'Connor et al 2023;Williams et al 2023), have shown that its associated SN has a peak luminosity consistent with those of the rest of the GRB-SN population (Levan et al 2023b;Blanchard et al 2023;Fulton et al 2023;Kann et al 2023;Shrestha et al 2023;Srinivasaragavan et al 2023), despite the GRB being more luminous by orders of magnitude. On the other hand, SN 1998bw associated with GRB 0980425 was a very nearby (z = 0.0085; Iwamoto et al 1998;Patat et al 2001;Clocchiatti et al 2011) and relatively luminous SN with a derived nickel mass (M Ni ) powering the SN as high as 0.9 M e (Sollerman et al 2000).…”

Section: Introductionmentioning

confidence: 99%

“…Photometrically, a characteristic supernova (SN) "bump" arises in the afterglow light curve (LC) within 10-20 days, as the afterglow fades. Over 40 LGRBs with this characteristic bump have been discovered (see, e.g., Hjorth 2013;Cano et al 2017a;Melandri et al 2019;Hu et al 2021;Kumar et al 2022a;Rossi et al 2022;Blanchard et al 2023;Srinivasaragavan et al 2023) and are known as GRB-SNe. Spectroscopic observations of these SNe have revealed that almost all (SN 2011kl associated with GRB 111209A was a superluminous SN; Greiner et al 2015;Kann et al 2019) are broad-line Type Ic SNe (Type Ic-BL; Woosley & Bloom 2006); they lack hydrogen and helium lines in their optical spectra and have broad lines corresponding to ejecta velocities higher than those seen in normal Type Ic explosions.…”

Section: Introductionmentioning

confidence: 99%

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Characterizing the Ordinary Broad-line Type Ic SN 2023pel from the Energetic GRB 230812B

Srinivasaragavan,

Swain,

O’Connor

et al. 2024

ApJL

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1

0

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We report observations of the optical counterpart of the long gamma-ray burst (GRB) GRB 230812B and its associated supernova (SN) SN 2023pel. The proximity (z = 0.36) and high energy (E γ,iso ∼ 1053 erg) make it an important event to study as a probe of the connection between massive star core collapse and relativistic jet formation. With a phenomenological power-law model for the optical afterglow, we find a late-time flattening consistent with the presence of an associated SN. SN 2023pel has an absolute peak r-band magnitude of M r = −19.46 ± 0.18 mag (about as bright as SN 1998bw) and evolves on quicker timescales. Using a radioactive heating model, we derive a nickel mass powering the SN of M Ni = 0.38 ± 0.01 M ⊙ and a peak bolometric luminosity of L bol ∼ 1.3 × 1043 erg s−1. We confirm SN 2023pel’s classification as a broad-line Type Ic SN with a spectrum taken 15.5 days after its peak in the r band and derive a photospheric expansion velocity of v ph = 11,300 ± 1600 km s−1 at that phase. Extrapolating this velocity to the time of maximum light, we derive the ejecta mass M ej = 1.0 ± 0.6 M ⊙ and kinetic energy E KE = 1.3 − 1.2 + 3.3 × 10 51 erg . We find that GRB 230812B/SN 2023pel has SN properties that are mostly consistent with the overall GRB-SN population. The lack of correlations found in the GRB-SN population between SN brightness and E γ,iso for their associated GRBs across a broad range of 7 orders of magnitude provides further evidence that the central engine powering the relativistic ejecta is not coupled to the SN powering mechanism in GRB-SN systems.

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“…That paper (S. Yang et al 2023, in preparation) contains an analysis of the objects that are used here to demonstrate the capabilities of HAFFET, and is hereafter referred to as Paper I. We have also estimated the luminosities for ZTF SNe Ic-BL using HAFFET in Corsi et al (2023), Srinivasaragavan et al (2023), and Anand et al (2023).…”

Section: Introductionmentioning

confidence: 99%

HAFFET: Hybrid Analytic Flux FittEr for Transients

Yang,

Sollerman

2023

ApJS

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The progenitors for many types of supernovae (SNe) are still unknown, and an approach to diagnose their physical origins is to investigate the light-curve brightness and shape of a large set of SNe. However, it is often difficult to compare and contrast the existing sample studies due to differences in their approaches and assumptions, for example, in how to eliminate host galaxy extinction, and this might lead to systematic errors when comparing the results. We therefore introduce the Hybrid Analytic Flux FittEr for Transients (HAFFET), a Python-based software package that can be applied to download photometric and spectroscopic data for transients from open online sources, derive bolometric light curves, and fit them to semianalytical models for estimation of their physical parameters. In a companion study, we have investigated a large collection of SNe Ib and Ic observed with the Zwicky Transient Facility (ZTF) with HAFFET, and here we detail the methodology and the software package to encourage more users. As large-scale surveys such as ZTF and LSST continue to discover increasing numbers of transients, tools such as HAFFET will be critical for enabling rapid comparison of models against data in statistically consistent, comparable, and reproducible ways. Additionally, HAFFET is created with a graphical user interface mode, which we hope will boost the efficiency and make the usage much easier (https://github.com/saberyoung/HAFFET).

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A Sensitive Search for Supernova Emission Associated with the Extremely Energetic and Nearby GRB 221009A

Cited by 11 publications

References 52 publications

Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow

Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow

Characterizing the Ordinary Broad-line Type Ic SN 2023pel from the Energetic GRB 230812B

HAFFET: Hybrid Analytic Flux FittEr for Transients

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