Issue |
A&A
Volume 690, October 2024
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Article Number | C2 | |
Number of page(s) | 3 | |
Section | Letters to the Editor | |
DOI | https://doi.org/10.1051/0004-6361/202451843e | |
Published online | 04 October 2024 |
Letters to the Editor
The dispersion of the Ep, i–Liso correlation of long gamma-ray bursts is partially due to assembling different sources (Corrigendum)
1
Department of Physics and Earth Science, University of Ferrara, Via Saragat 1, I-44122 Ferrara, Italy
2
INFN – Sezione di Ferrara, Via Saragat 1, 44122 Ferrara, Italy
3
INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Piero Gobetti 101, 40129 Bologna, Italy
Key words: methods: data analysis / methods: statistical / gamma-ray burst: general / errata / addenda
We found a mistake in the code used to compute the parameters m, q, and σint of the Ep, i–Liso and Ep, i–Lcoll correlations reported in Tables 1, 2, and 3. We verified to see whether the essence of our results remains unaffected, and in fact the statistical evidence of our conclusions is even stronger than what was reported in the Letter.
For each burst in the sample, we recomputed the aforementioned parameters and provide the correct values in Tables 1, 2, and 3, which are meant to replace those reported in the Letter. We also provide the amended version of Fig. 1. Not only do the general conclusions that we found remain valid, but the main result shown in Sect. 3.1 improved. In fact, with reference to that section, the statistical significance goes from 4.2 (Pt = 2.69 × 10−5) to 5.9σ (Gaussian,Pt = 4.55 × 10−9).
Sample of GRBs with redshift z, jet half-opening angle θj – both in the homogeneous interstellar medium (ISM) and wind profile (W) –, the Lorentz factor Γ0, and the minimum variability timescale (MVT).
Best-fit parameters of the Ep, i–L correlation (90% confidence) for the overall sample 𝒮 and for the sub-samples 𝒮(ISM) and 𝒮(W) of time-resolved spectra of GRBs with available information on and on , respectively.
Best-fit parameters of the Ep, i–Liso correlation (90% confidence) of the GRBs with the highest S/N obtained including BGO data with a better viewing angle (mBGO, qBGO, and σint, BGO using the Band function; mCPL, qCPL, and σint, CPL using the CPL model) and NaI alone (m, q, and σint).
Fig. 1. Top panel: Time-resolved Ep, i–Liso relation for the overall sample 𝒮. Bottom panel: Collimation-corrected Ep, i–Lcoll relation for the subset 𝒮(ISM) of GRBs with available information on . In both panels the best-fit model along with the 1-σint, t region (shaded area) is shown, while median uncertainties along both axes are shown in the top left. |
Referring to Sect. 3.3, we provide here the correct values of the parameters of GRB 090102: , , and .
References
- Camisasca, A. E., Guidorzi, C., Amati, L., et al. 2023, A&A, 671, A112 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
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© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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All Tables
Sample of GRBs with redshift z, jet half-opening angle θj – both in the homogeneous interstellar medium (ISM) and wind profile (W) –, the Lorentz factor Γ0, and the minimum variability timescale (MVT).
Best-fit parameters of the Ep, i–L correlation (90% confidence) for the overall sample 𝒮 and for the sub-samples 𝒮(ISM) and 𝒮(W) of time-resolved spectra of GRBs with available information on and on , respectively.
Best-fit parameters of the Ep, i–Liso correlation (90% confidence) of the GRBs with the highest S/N obtained including BGO data with a better viewing angle (mBGO, qBGO, and σint, BGO using the Band function; mCPL, qCPL, and σint, CPL using the CPL model) and NaI alone (m, q, and σint).
All Figures
Fig. 1. Top panel: Time-resolved Ep, i–Liso relation for the overall sample 𝒮. Bottom panel: Collimation-corrected Ep, i–Lcoll relation for the subset 𝒮(ISM) of GRBs with available information on . In both panels the best-fit model along with the 1-σint, t region (shaded area) is shown, while median uncertainties along both axes are shown in the top left. |
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In the text |
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