The IXPE View of GRB 221009A

Negro, Michela; Lalla, N. Di; Omodei, N.; Vereš, P.; Silvestri, S.; Manfreda, Alberto; Burns, E.; Baldini, Luca; Costa, E.; Ehlert, Steven R.; Kennea, J. A.; Liodakis, Ioannis; Marshall, Herman L.; Mereghetti, S.; Middei, R.; Muleri, Fabio; O’Dell, Stephen L.; Roberts, O. J.; Romani, Roger W.; Sgrò, C.; Masanobu, Terashima,; Tiengo, A.; Viscolo, Domenico; Marco, Alessandro Di; Monaca, Fabio La; Latronico, L.; Matt, Giorgio; Perri, M.; Puccetti, S.; Poutanen, Juri; Ratheesh, Ajay; Rogantini, Daniele; Slane, Patrick; Soffitta, P.; Lindfors, E.; Nilsson, K.; Kasikov, Anni; Marscher, A. P.; Tavecchio, F.; Cibrario, N.; Gunji, Shuichi; Malacaria, C.; Paggi, A.; Yang, Yi-Jung; Zane, S.; Weisskopf, Martin C.; Agudo, I.; Antonelli, L. A.; Bachetti, Matteo; Baumgartner, W. H.; Bellazzini, R.; Bianchi, S.; Bongiorno, Stephen D.; Bonino, R.; Brez, A.; Bucciantini, N.; Capitanio, Fiamma; Castellano, Simone; Cavazzuti, E.; Chen, Chien-Ting; Ciprini, S.; Rosa, A. De; Monte, E. Del; Gesu, Laura Di; Donnarumma, I.; Doroshenko, V.; Dovčiak, Michal; Enoto, T.; Evangelista, Y.; Fabiani, Sergio; Ferrazzoli, Riccardo; Garcia, J. Rodriguez; Hayashida, Kentaro; Heyl, Jeremy; Iwakiri, W.; Jorstad, S. G.; Kaaret, Philip; Karas, V.; Kislat, Fabian; Kitaguchi, Takao; Kolodziejczak, Jeffery J.; Krawczynski, H.; Maldera, S.; Marin, Frédéric; Marinucci, Andrea; Mitsuishi, Ikuyuki; Mizuno, T.; Ng, Chi-Yung; Oppedisano, C.; Papitto, A.; Pavlov, G. G.; Peirson, Abel L.; Pesce-Rollins, M.; Petrucci, Pierre-Olivier; Pilia, M.; Possenti, A.; Ramsey, Brian D.; Rankin, John; Spandre, G.; Swartz, Douglas A.; Tamagawa, Toru; Taverna, Roberto; Tawara, Yuzuru; Tennant, Allyn F.; Thomas, Nicholas E.; Tombesi, Francesco; Trois, A.; Tsygankov, Sergey S.; Turolla, R.; Vink, Jacco; Wu, Kinwah; Xie, Fei

doi:10.3847/2041-8213/acba17

Cited by 25 publications

(26 citation statements)

References 63 publications

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“…These authors reported the discovery of nine dust rings and derived the distances, with the most distant one lying at 3635 ± 36 pc, potentially already beyond the detection range of the RF09 method. Observations with IXPE (Negro et al 2023) confirm the most distant dust ring found by Swift at 3.75 ± 0.0375 kpc and report an even more distant dust curtain at 14.41 ± 0.865 kpc. Recently, Vasilopoulos et al (2023) reported a detailed analysis of Swift XRT data and also found evidence for dust out to 15 kpc (see Williams et al 2023 for further analysis), and XMM-Newton analysis of a total of 20 dust rings presented by Tiengo et al (2023) detects an even further dust curtain at ≈18.6 kpc.…”

Section: Extinction Selectionsupporting

confidence: 57%

“…This method results in a significantly lower extinction value (but is only valid out to 2-3 kpc) compared to the SF11 value. Taking into account the existence of dust at larger distances determined by X-ray measurements of dust rings (Negro et al 2023;Williams et al 2023;Vasilopoulos et al 2023), we proceed to discuss the reliability of these measurements and conduct our follow-up analysis using both correction methods for comparison.…”

Section: Discussionmentioning

confidence: 99%

“…The HXMT/LE flux measurements are not corrected for the dust echo scattering (see, for example, Negro et al 2023;Tiengo et al 2023;Williams et al 2023), since Insight-HXMT is a collimated telescope with a large FoV, e.g., 1°× 4°. It is thus not possible to easily remove the dust echo scattering flux contribution.…”

Section: Swift Xrt and Hxmt/le Afterglow Datamentioning

confidence: 99%

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GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

Канн

Agayeva

Aivazyan

et al. 2023

ApJL

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Object GRB 221009A is the brightest gamma-ray burst (GRB) detected in more than 50 yr of study. In this paper, we present observations in the X-ray and optical domains obtained by the GRANDMA Collaboration and the Insight Collaboration. We study the optical afterglow with empirical fitting using the GRANDMA+HXMT-LE data sets augmented with data from the literature up to 60 days. We then model numerically using a Bayesian approach, and we find that the GRB afterglow, extinguished by a large dust column, is most likely behind a combination of a large Milky Way dust column and moderate low-metallicity dust in the host galaxy. Using the GRANDMA+HXMT-LE+XRT data set, we find that the simplest model, where the observed afterglow is produced by synchrotron radiation at the forward external shock during the deceleration of a top-hat relativistic jet by a uniform medium, fits the multiwavelength observations only moderately well, with a tension between the observed temporal and spectral evolution. This tension is confirmed when using the augmented data set. We find that the consideration of a jet structure (Gaussian or power law), the inclusion of synchrotron self-Compton emission, or the presence of an underlying supernova do not improve the predictions. Placed in the global context of GRB optical afterglows, we find that the afterglow of GRB 221009A is luminous but not extraordinarily so, highlighting that some aspects of this GRB do not deviate from the global known sample despite its extreme energetics and the peculiar afterglow evolution.

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Section: Extinction Selectionsupporting

confidence: 57%

Section: Discussionmentioning

confidence: 99%

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GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

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Agayeva

Aivazyan

et al. 2023

ApJL

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“…We find the total fluence = (9.47 ± 0.07) × 10 −2 erg cm −2 and E γ,iso = (1.01 ± 0.007) × 10 55 erg. Assuming an opening angle of 2° (Negro et al 2023), the beaming corrected energy is = ǵ E 6.1 ( ) q 10 2 j 51 2 erg. We obtain the isotropic-equivalent luminosity by integrating the spectrum in the t 0 + 230.8 s to t 0 + 231.8 s interval.…”

Section: Energeticsmentioning

confidence: 99%

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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“…, where n 0 is the medium number density, η γ is the radiative efficiency of the prompt phase, and t jet is measured in days. Although extensive multiwavelength follow-up of GRB 221009A did not reveal an apparent achromatic break in the afterglow light curve, a number of θ jet estimates are reported, ranging from 0°.7 to >10°.7 (An et al 2023;Kann et al 2023;Negro et al 2023;O'Connor et al 2023;Williams et al 2023), which, assuming typical η γ = 0.2 and n 0 = 1 cm −3 , imply E K from ∼5 × 10 51 to ∼5 × 10 53 and even higher.…”

Section: Collimation-corrected Energy and Central Enginementioning

confidence: 99%

Properties of the Extremely Energetic GRB 221009A from Konus-WIND and SRG/ART-XC Observations

Frederiks

Svinkin

Lysenko

et al. 2023

ApJL

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We report on Konus-WIND (KW) and Mikhail Pavlinsky Astronomical Roentgen Telescope – X-ray Concentrator (ART-XC) observations and analysis of a nearby GRB 221009A, the brightest γ-ray burst (GRB) detected by KW for >28 yr of observations. The prompt, pulsed phase of the burst emission lasts for ∼600 s and is followed by a steady power-law decay lasting for more than 25 ks. From the analysis of the KW and ART-XC light curves and the KW spectral data, we derive time-averaged spectral peak energy of the burst E p ≈ 2.6 MeV, E p at the brightest emission peak ≈ 3.0 MeV, the total 20 keV–10 MeV energy fluence of ≈0.22 erg cm−2, and the peak energy flux in the same band of ≈0.031 erg cm−2 s−1. The enormous observed fluence and peak flux imply, at redshift z = 0.151, huge values of isotropic energy release E iso ≈ 1.2 × 1055 erg (or ≳6.5 solar rest mass) and isotropic peak luminosity L iso ≈ 3.4 × 1054 erg s−1 (64 ms scale), making GRB 221009A the most energetic and one of the most luminous bursts observed since the beginning of the GRB cosmological era in 1997. The isotropic energetics of the burst fit nicely both “Amati” and “Yonetoku” hardness–intensity correlations for >300 KW long GRBs, implying that GRB 221009A is most likely a very hard, super-energetic version of a “normal” long GRB.

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The IXPE View of GRB 221009A

Cited by 25 publications

References 63 publications

GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

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

Properties of the Extremely Energetic GRB 221009A from Konus-WIND and SRG/ART-XC Observations

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