Gamma-Ray Burst Formation Rate Inferred from the Spectral Peak Energy-Peak Luminosity Relation

By D. Yonetoku, T. Murakami, T. Nakamura, R. Yamazaki, A. Inoue, K. University, Kyoto University, O. University. 2003

608 citations recorded by the source corpus.

We estimate a gamma-ray burst (GRB) formation rate based on the new relation between the spectral peak energy (Ep) and the peak luminosity. The new relation is derived by combining the data of Ep and the peak luminosities by BeppoSAX and BATSE, and it looks considerably tighter and more reliable than the relations suggested by the previous works. Using the new Ep-luminosity relation, we estimate redshifts of the 689 GRBs without known distances in the BATSE catalog and derive a GRB formation rate as a function of the redshift. For the redshift range of 0 ≤ z ≤ 2, the GRB formation rate increases and is well correlated with the star formation rate, while it keeps constant toward z ~ 12. We also discuss the luminosity function and the redshift dependence of the intrinsic luminosity (luminosity evolution).

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a7c7dce0b6281a3d8b852dc05ce5a6aa0060c47a

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In Astronomy and Astrophysics

1. Bing Zhang
2. Pawan Kumar
3. E. Berger
4. B. Metzger
5. E. Liang
6. Binbin Zhang
7. E. Quataert
8. L. Amati

Citations in the corpus

• The THESEUS space mission concept: science case, design and expected performances (2017, methodology): “By using the spectral peak energy - radiated energy (or luminosity) correlation Ep,i - Eiso (Amati et al., 2002; Yonetoku et al., 2004), the luminosity at the end of the plateau emission and its rest frame duration correlation (Dainotti et al., 2008) and the fundamental plane relation, an extension ”
• Gamma-Ray Bursts in the Swift Era (2007, background): “A related relation is Ep ∝ L 1/2 p,iso (Yonetoku et al. 2004, see also Wei & Gao 2003), whereLp,iso is the isotropic peak luminosity.”
• THE INTERNAL-COLLISION-INDUCED MAGNETIC RECONNECTION AND TURBULENCE (ICMART) MODEL OF GAMMA-RAY BURSTS (2010, background): “Wei, D. M., & Gao, W. H. 2003, MNRAS, 345, 743.”
• A RADIO-SELECTED SAMPLE OF GAMMA-RAY BURST AFTERGLOWS (2011, unknown): “…2004; (48) Soderberg et al. 2005; (49) Soderberg et al. 2006a; (50) Soderberg et al. 2006b; (51) Tanvir et al. 2010a; (52) Tanvir et al. 2009; (53) Yonetoku et al. 2004; (54) http://www.raunvis.hi.is/∼pja/GRBsample.html; (55) http://gcn.gsfc.nasa.gov/integral_grbs.html; (56)…”
• A Cosmology-Independent Calibration of Gamma-Ray Burst Luminosity Relations and the Hubble Diagram (2008, background): “…spectral energy ((EisoEp) relation (i.e., the so-called Amati relation, Amati et al. 2002), the collimation-corrected energy-peak spectral energy (Eγ-Ep) relation (i.e., the so-called Ghirlanda et al. 2004a), theL-Ep relation (Schaefer 2003a; Yonetoku et al. 2004), and two multi-variable relations.”
• 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): “(9) into Ep ∝ L1/2γ,iso ∝ E 1/2 γ,iso by taking the trivial proportionality L ∝ Lγ,iso ∝ Eγ,iso.”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “general, a positive correlation between E p;zand E ;isoseems real, although the scatter may be wide. Similarly, a positive correlation between E p;z and L ;p;iso has been reported (Wei and Gao, 2003; Yonetoku et al., 2004); where L ;p;iso is the isotropic gamma-ray luminosity of a burst at its peak ”
• THE COSMIC RATE, LUMINOSITY FUNCTION, AND INTRINSIC CORRELATIONS OF LONG GAMMA-RAY BURSTS (2009, background): “Notably, some of these works (e.g., Lloyd-Ronning et al. 2002; Yonetoku et al. 2004), using hazard statistics (Lynden-Bell 1971; Efron & Petrosian 1992; Petrosian 1993; Maloney & Petrosian 1999), also found evidence for potential strong luminosity evolution, parameterized as L ∝ (1+z)a, with a in…”
• Extremely energetic Fermi Gamma-Ray Bursts obey spectral energy correlations (2009, unknown): “E iso correlation, it was pointed out that E p , i also correlates with other GRB intensity indicators, such as the peak luminosity, L p , iso , (Yonetoku et al. 2004; Ghirlanda et al. 2005b) or the average luminosity, L iso , (Lamb et al. 2004; Ghirlanda et al. 2009).”
• The Ep,i–Eiso correlation in gamma-ray bursts: updated observational status, re-analysis and main implications (2006, background): “Finally, the relevance of the Ep,i – Eiso correlation for the GRB field stimulated several similar studies, which led to the discovery of correlations of Ep,i with other GRB intensity indicators like the average isotropic equivalent luminosity Liso (Lamb, Donaghy & Graziani 2004, 2005) and the peak ”
• A COMPLETE SAMPLE OF BRIGHT SWIFT LONG GAMMA-RAY BURSTS. I. SAMPLE PRESENTATION, LUMINOSITY FUNCTION AND EVOLUTION (2011, background): “In order to broadly estimate the peak energy of the spectrum, Ep, for a given L, we assumed the validity of the correlation between Ep and L (Yonetoku et al. 2004; Ghirlanda et al. 2005, Nava et al. 2011).”
• A COMPREHENSIVE ANALYSIS OF FERMI GAMMA-RAY BURST DATA. I. SPECTRAL COMPONENTS AND THE POSSIBLE PHYSICAL ORIGINS OF LAT/GBM GRBs (2010, methodology): “For time-integrated spectra, it was found that Ep is positively correlated with the isotropic gamma-ray energy and the isotropic peak gamma-ray luminosity (Amati et al. 2002; Wei & Gao 2003; Yonetoku et al. 2004).”
• Short versus long gamma-ray bursts: spectra, energetics, and luminosities (2009, background): “Long bursts follow some empirical correlations involving the (isotropic) energeticsEiso (Amati et al. 2002) and/or peak luminosityLiso (Yonetoku et al. 2004), and the rest–frame peak energyEpeak.”