The Collimation-corrected Gamma-Ray Burst Energies Correlate with the Peak Energy of Their νFν Spectrum

By G. Ghirlanda, G. Ghisellini, D. Lazzati. 2004

500 citations recorded by the source corpus.

We consider all bursts with known redshift and νFν peak energy, E. For a good fraction of them an estimate of the jet opening angle is available from the achromatic break of their afterglow light curve. This allows the derivation of the collimation-corrected energy of the bursts, Eγ. The distribution of the values of Eγ is more spread out than in previous findings, covering about 2 orders of magnitude. We find a surprisingly tight correlation between Eγ and the source frame Epeak: E(1 + z) ∝ E. This correlation can shed light on the still uncertain radiation processes for the prompt GRB emission. More importantly, if the small scatter of this newly found correlation could be confirmed by forthcoming data, it would be possible to use it for cosmological purposes.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/db44bd3b3e60f137ea94cd4ca7f257b3079772f6

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In Astronomy and Astrophysics

1. Bing Zhang
2. Pawan Kumar
3. E. Berger
4. E. Liang
5. A. Filippenko
6. Binbin Zhang
7. L. Amati
8. R. Kirshner

In Nuclear and High Energy Physics

1. Bing Zhang
2. Pawan Kumar
3. L. Amati
4. E. Berger
5. F. Ryde
6. E. Liang
7. A. Filippenko
8. B. Leibundgut

Citations in the corpus

• Gamma-ray bursts in the comoving frame (2011, background): “However, though somehow speculative, we can deriveθj for the 32 GRBs of our sample assuming theEpeak − Eγ correlation in the H case (Ghirlanda et al. 2004) or in the W (Nava et al. 2006).”
• A complete sample of bright Swift long gamma-ray bursts: testing the spectral-energy correlations (2011, background): “…strongly correlates with (i) the isotropic energyEiso (Amati relation, Amati et al. 2002), (ii) the isotropic peak luminosity Liso (Yonetoku relation, Yonetoku et al. 2004) and (iii) the collimation– corrected energyEγ (Ghirlanda relation, Ghirlanda et al. 2004b; see also Liang & Zhang 2005).”
• Gamma-Ray Bursts in the Swift Era (2007, methodology): “Starting with the assumption of constant energy reservoir of all events (as derived by Frail et al. 2001; Bloom et al. 2003 - but not confirmed by more systematic observations by Swift, e.g., Willingale et al. 2006; Burrows 2006; Zhang 2007), they drew the conclusion that GRBs have a typical opening”
• The physics of gamma-ray bursts & relativistic jets (2014, methodology): “The correlation (Ghirlanda relation), in its original form (Ghirlanda et al., 2004a), reads Ep,z 100 keV ' 4.8 ( Eγ 1051erg )0.7 , (105) which was claimed to be tighter than the Amati relation.”
• A RADIO-SELECTED SAMPLE OF GAMMA-RAY BURST AFTERGLOWS (2011, unknown): “…Frail et al. 2000; (17) Frail et al. 2001; (18) Frail et al. 2006; (19) Frontera et al. 2009; (20) Fynbo et al. 2009; (21) Gehrels et al. 2008; (22) Ghirlanda et al. 2004; (23) Ghirlanda et al. 2010; (24) Gorosabel et al. 2005; (25) Graham et al. 2009; (26)…”
• A time - luminosity correlation for Gamma - Ray Bursts in the X - rays (2008, unknown): “Previous attempts along this road are represented by the Eiso − Epeak (Amati et al. 2002), Eγ − Epeak (Ghirlanda et al. 2004; Ghirlanda et al. 2006), L−Epeak (Schaefer 2003), L − τlag (Norris et al. 2000), L − V (Fenimore & Ramirez - Ruiz 2000; Riechart et al. 2001), L− τRT .”
• A Comprehensive Analysis of Swift XRT Data. II. Diverse Physical Origins of the Shallow Decay Segment (2007, result): “9 If t′b,opt is interpreted as a jet break, then the relation is similar to the Ghirlanda-relation (Ghirlanda et al. 2004).”
• A DECADE OF SHORT-DURATION GAMMA-RAY BURST BROADBAND AFTERGLOWS: ENERGETICS, CIRCUMBURST DENSITIES, AND JET OPENING ANGLES (2015, methodology): “…we collect opening angle measurements for 265 long GRBs, including 17 events with limits (Frail et al. 2001; Berger et al. 2003; Bloom et al. 2003; Ghirlanda et al. 2004; Friedman & Bloom 2005; Racusin et al. 2009; Cenko et al. 2010, 2011; Filgas et al. 2011; Goldstein et al. 2011; Ryan et al.…”
• Scrutinizing Exotic Cosmological Models Using ESSENCE Supernova Data Combined with Other Cosmological Probes (2007, methodology): “We have, for example, chosen to omit any information from distant gamma-ray bursts (Ghirlanda et al. 2004) since such data are rather controversial (Mörtsell & Sollerman 2005; Friedman & Bloom 2005).”
• A Comprehensive Analysis of Swift XRT Data. III. Jet Break Candidates in X-Ray and Optical Afterglow Light Curves (2007, methodology): “This correlation was taken as a potential standard candle to perform cosmographic studies (e.g., Dai et al. 2004; Ghirlanda et al. 2004a).”
• DISCERNING THE PHYSICAL ORIGINS OF COSMOLOGICAL GAMMA-RAY BURSTS BASED ON MULTIPLE OBSERVATIONAL CRITERIA: THE CASES OF z = 6.7 GRB 080913, z = 8.2 GRB 090423, AND SOME SHORT/HARD GRBs (2009, background): “When the optical afterglow light curve temporal break (topt) is included, a tighter correlation involving Ep and Eγ,iso is obtained (Ghirlanda et al. 2004; Liang & Zhang 2005) for some long duration GRBs.”
• The Ep,i–Eiso correlation in gamma-ray bursts: updated observational status, re-analysis and main implications (2006, methodology): “In addition, the Ep,i – Eγ and Ep,i – Eiso – tb correlations, given their low dispersion, have been used for the estimate of cosmological parameters, e.g., Ghirlanda et al. (2004); Dai, Liang & Xu (2004); Liang & Zhang (2005); Xu, Dai & Liang (2005), in a way similar to that used with type Ia SNe .”
• The Proto-Magnetar Model for Gamma-Ray Bursts (2010, unknown): “…energy Eiso, Epeak ∝ E 0.4 iso (Amati et al. 2002) with the correlation Epeak ∝ E 0.7 γ between Epeak and the beaming-corrected energy Eγ = fbEiso (Ghirlanda et al. 2004), we obtain the empirical relationship (cf. Nava et al. 2006) fb ≈ 2× 10 −3 ( Eγ 1051 ergs )−3/4 ; θj ≈ 3.3 ◦ ( Eγ 1051…”
• Gamma-ray burst afterglows (2006, background): “– Ghirlanda relation: Ghirlanda et al. (2004) found that the beaming-corrected gamma-ray energy is not constant, but is related to the rest-frame spectral peak energy (E p ) through E p ∝ E 2/3 γ,j .”
• THE FERMI GBM GAMMA-RAY BURST SPECTRAL CATALOG: THE FIRST TWO YEARS (2012, background): “Many correlative studies in the field of GRB global properties studies rely on only two very distinct representative spectra (Amati et al. 2002; Ghirlanda et al. 2004; Yonetoku et al. 2004).”