The IXPE view of GRB 221009A

Negro, Michela; Lalla, N. Di; Omodei, N.; Vereš, P.; Silvestri, Stefano; Manfreda, Alberto; Burns, E.; Baldini, Luca; Costa, E.; 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.; Marco, Alessandro Di; Puccetti, S.; Masanobu, Terashima,; Tiengo, A.; Viscolo, Domenico; Monaca, Fabio La; Latronico, L.; Matt, Giorgio; Perri, M.; Poutanen, Juri; Ratheesh, Ajay; Rogantini, Daniele; Slane, Patrick; Soffitta, P.; Lindfors, E.; Nilsson, K.; Kasikov, Anni; Marscher, A. P.; Tavecchio, F.; Gunji, Shuichi; Malacaria, C.; Paggi, A.; Yang, Yi-Jung; Zane, S.; Weisskopf, Martin C.; Agudo, I.; Antonelli, L. A.; Baumgartner, W. H.; Bellazzini, R.; Bianchi, S.; Bonino, R.; Brez, A.; Bucciantini, Niccol; Castellano, Simone; Cavazzuti, E.; Chen, Chien-Ting; Rosa, A. De; Monte, E. Del; Gesu, Laura Di; Donnarumma, I.; Doroshenko, V. T.; Dovčiak, Michal; Enoto, T.; Bachetti, Matteo; Bongiorno, Stephen D.; Capitanio, Fiamma; Ciprini, S.; Evangelista, Y.; Fabiani, Sergio; Ferrazzoli, Riccardo; Garcia, Javier A.; Hayashida, Kentaro; Heyl, Jeremy; Iwakiri, W.; Jorstad, Svetlana G.; Kaaret, Philip; Karas, Vladimír; Kislat, Fabian; Kitaguchi, Takao; Kolodziejczak, Jeffery J.; Krawczynski, H.; Maldera, S.; Marin, Frédéric; Marinucci, Andrea; Mitsuishi, Ikuyuki; Mizuno, T.; Ng, C. -Y.; Oppedisano, C.; Papitto, A.; Pavlov, G. G.; Peirson, Abel L.; Pesce-Rollins, Melissa; Petrucci, Pierre-Olivier; Ramsey, Brian D.; Rankin, John; Spandre, G.; Pilia, M.; Possenti, A.; Swartz, Douglas A.; Tamagawa, Toru; Taverna, Roberto; Tawara, Yuzuru; Tennant, Allyn F.; Thomas, N.; Tombesi, Francesco; Trois, A.; S., Tsygankov, Sergey; Turolla, R.; Vink, Jacco; Wu, Kinwah; Xie, Fei

doi:10.48550/arxiv.2301.01798

Cited by 6 publications

(10 citation statements)

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“…Right: evolution of peak flux and peak frequency from broken power-law fits to the radio SED at 50 GHz (Table 7). GRB 221009A is one of the brightest GRBs ever observed (Kennea et al 2022a;Veres et al 2022;Ursi et al 2022;Frederiks et al 2022;Iwakiri et al 2022;Kobayashi et al 2022;Negro et al 2023). While this is due in part to its proximity, GRB 221009A is also intrinsically among the most luminous known bursts at these wavelengths (Figure 7).…”

Section: Comparison To Other γ-Ray Burstsmentioning

confidence: 94%

The Radio to GeV Afterglow of GRB 221009A

Laskar

Alexander²,

Margutti

et al. 2023

ApJL

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GRB 221009A (z = 0.151) is one of the closest known long γ-ray bursts (GRBs). Its extreme brightness across all electromagnetic wavelengths provides an unprecedented opportunity to study a member of this still-mysterious class of transients in exquisite detail. We present multiwavelength observations of this extraordinary event, spanning 15 orders of magnitude in photon energy from radio to γ-rays. We find that the data can be partially explained by a forward shock (FS) from a highly collimated relativistic jet interacting with a low-density, wind-like medium. Under this model, the jet’s beaming-corrected kinetic energy (E K ∼ 4 × 1050 erg) is typical for the GRB population. The radio and millimeter data provide strong limiting constraints on the FS model, but require the presence of an additional emission component. From equipartition arguments, we find that the radio emission is likely produced by a small amount of mass (≲6 × 10−7 M ⊙) moving relativistically (Γ ≳ 9) with a large kinetic energy (≳1049 erg). However, the temporal evolution of this component does not follow prescriptions for synchrotron radiation from a single power-law distribution of electrons (e.g., in a reverse shock or two-component jet), or a thermal-electron population, perhaps suggesting that one of the standard assumptions of afterglow theory is violated. GRB 221009A will likely remain detectable with radio telescopes for years to come, providing a valuable opportunity to track the full lifecycle of a powerful relativistic jet.

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Section: Comparison To Other γ-Ray Burstsmentioning

confidence: 94%

The Radio to GeV Afterglow of GRB 221009A

Laskar

Alexander²,

Margutti

et al. 2023

ApJL

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“…Other key observations include the first observations of the prompt and afterglow polarization from the same burst (Negro et al 2023), the (somewhat) surprising (Murase et al 2022) lack of neutrinos (Abbasi et al 2023), and the first disruptive target of opportunity from an out-of-cycle proposal of JWST (Levan et al 2023; also the first JWST observation of a GRB afterglow ever).…”

Section: Introductionmentioning

confidence: 99%

GRB 221009A: The BOAT

Burns

Svinkin

Fenimore

et al. 2023

ApJL

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GRB 221009A has been referred to as the brightest of all time (BOAT). We investigate the veracity of this statement by comparing it with a half century of prompt gamma-ray burst observations. This burst is the brightest ever detected by the measures of peak flux and fluence. Unexpectedly, GRB 221009A has the highest isotropic-equivalent total energy ever identified, while the peak luminosity is at the ∼99th percentile of the known distribution. We explore how such a burst can be powered and discuss potential implications for ultralong and high-redshift gamma-ray bursts. By geometric extrapolation of the total fluence and peak flux distributions, GRB 221009A appears to be a once-in-10,000-year event. Thus, it is almost certainly not the BOAT over all of cosmic history; it may be the brightest gamma-ray burst since human civilization began.

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“…Analysis of the GRB 221009A dust-scattering rings were also reported by Vasilopoulos et al (2023) and Williams et al (2023), who used Swift/XRT, and by Negro et al (2023), who used IXPE data. Swift/XRT could already image the X-ray rings about 1 day after the GRB, making possible the discovery of dust clouds at distances smaller than 300 pc (Vasilopoulos et al 2023), which formed X-ray rings that were already outside the EPIC field of view during XMM-Newton observations.…”

Section: Discussionmentioning

confidence: 90%

“…A 1-10 keV fluence of (1.6-6.1) × 10 −4 erg cm −2 was instead estimated from the analysis of the dust rings observed with IXPE, which allowed Negro et al (2023) to derive limits on the X-ray polarization of GRB 221009A. During the IXPE observations, the rings produced by dust closer than 2 kpc were outside the field of view, and due to the limited angular resolution and collecting area, only two rings corresponding to broad dust distributions centered at 3.75 and 14.41 kpc could be identified.…”

Section: Discussionmentioning

confidence: 99%

“…During the IXPE observations, the rings produced by dust closer than 2 kpc were outside the field of view, and due to the limited angular resolution and collecting area, only two rings corresponding to broad dust distributions centered at 3.75 and 14.41 kpc could be identified. The GRB fluence was then reconstructed using the Draine (2003) model, assuming that all the optical extinction at distances greater than 3 kpc is due to two narrow dust layers at such distances (Negro et al 2023). As demonstrated by the complex dust distribution unveiled by our analysis of the XMM-Newton data, this is an overestimate of the quantity of dust in these dust layers, leading to a lower estimate of the GRB fluence.…”

Section: Discussionmentioning

confidence: 99%

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The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo

Tiengo

Pintore

Beatrice

et al. 2023

ApJL

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GRB 221009A is the brightest gamma-ray burst (GRB) ever detected that has occurred at low Galactic latitude. Owing to this exceptional combination, its prompt X-ray emission could be detected for weeks in the form of expanding X-ray rings produced by scattering in Galactic dust clouds. We report on the analysis of 20 rings, generated by dust at distances ranging from 0.3 to 18.6 kpc, detected during two X‐ray Multi Mirror (XMM)-Newton observations performed about 2 and 5 days after the GRB. By fitting the spectra of the rings with different models for the dust composition and grain size distribution, we reconstructed the spectrum of the GRB prompt emission in the 0.7–4 keV energy range as an absorbed power law with photon index Γ = 1–1.4 and absorption in the host galaxy N H,z = (4.1–5.3) × 1021 cm−2. Taking into account the systematic uncertainties regarding the column density of dust contained in the clouds producing the rings, the 0.5–5 keV fluence of GRB 221009A can be constrained between 10−3 and 7 × 10−3 erg cm−2. Both the fluence and the photon index indicate the presence of a possible soft excess with respect to the extrapolation of the main GRB peak observed at higher energies.

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The IXPE view of GRB 221009A

Cited by 6 publications

References 0 publications

The Radio to GeV Afterglow of GRB 221009A

The Radio to GeV Afterglow of GRB 221009A

GRB 221009A: The BOAT

The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo

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