Intrinsic spectra and energetics of BeppoSAX Gamma-Ray Bursts with known redshifts

By L. Amati, Federico Frontera, M. Tavani, J. I. Zand, A. Antonelli, E. Costa, M. Feroci, C. Guidorzi, J. Heise, N. Masetti and 6 more. 2002

1,061 citations recorded by the source corpus.

We present the main results of a study of spectral and energetics properties of twelve gamma-ray bursts (GRBs) with redshift estimates. All GRBs in our sample were detected by BeppoSAX in a broad energy range (2-700 keV). From the redshift estimates and the good-quality BeppoSAX time-integrated spectra we deduce the main properties of GRBs in their cosmological rest frames. All spectra in our sample are satisfactorily represented by the Band model, with no significant soft X-ray excesses or spectral absorptions. We find a positive correlation between the estimated total (isotropic) energies in the 1-10 000 keV energy range (Erad) and redshifts z. Interestingly, more luminous GRBs are characterized also by larger peak energies Ep so f theirEF(E) spectra. Furthermore, more distant GRBs appear to be systematically harder in the X-ray band compared to GRBs with lower redshifts. We discuss how selection and data truncation eects could bias our results and give possible explanations for the correlations that we found.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fb135ddd815150b975450e294e52ccbd2a4eeeb5

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In Astronomy and Astrophysics

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

In Instrumentation

1. Bing Zhang
2. P. Hopkins
3. E. Liang
4. Pawan Kumar
5. L. Hernquist
6. L. Amati
7. E. Quataert
8. Brant Robertson

Citations in the corpus

• 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).”
• Extremely energetic Fermi Gamma-Ray Bursts obey spectral energy correlations (2009, neutral): “…with their uncertainties, the redshift, with its uncertainty, provided by GROND, and by integrating the cosmological rest-frame spectrum in the commonly adopted 1 keV − 10 MeV energy band (Amati et al. 2002; Amati 2006a), we derive E iso = (3.8 ± 0.8) × 10 54 erg, and E p , i = 2646 ± 566 keV.”
• An Analysis of Gamma-Ray Burst Spectral Break Models (2002, background): “Indeed, such a correlation has been seen in the BeppoSAX bursts with known redshifts (Amati et al. 2002).”
• Did a gamma-ray burst initiate the late Ordovician mass extinction? (2003, methodology): “LloydRooning et a1 (2000) deduce a slightly larger number, about 6 x analysis of 220 BATSE GRB with redshifts estimated from a luminosity-variability relation.”
• On the Evolution of the Hubble Constant with the SNe Ia Pantheon Sample and Baryon Acoustic Oscillations: A Feasibility Study for GRB-Cosmology in 2030 (2022, background): “We here stress that this work can be also preparatory to the work of future application of GRBs as cosmological tools together with SNe Ia and Baryon Acoustic Oscillations (BAOs) through well-established correlations among the prompt variables, such as: the Amati relation [20], which connects the pe”
• OBSERVATIONS OF THE NAKED-EYE GRB 080319B: IMPLICATIONS OF NATURE'S BRIGHTEST EXPLOSION (2008, background): “The restframe isotropic-equivalent energy release is Eiso = 1.3 × 1054 erg in the standard source frame 1–104 keV band (Amati et al. 2002; Bloom et al. 2001).”
• A Cosmology-Independent Calibration of Gamma-Ray Burst Luminosity Relations and the Hubble Diagram (2008, background): “…& Ramirez-Ruiz 2000; Reichart et al. 2001), the isotropic energy-peak 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…”
• Quantum-gravity analysis of gamma-ray bursts using wavelets (2002, background): “By now, redshifts have been measured for about 20 bursts (see for example Norris et al. 2000; http://www.aip.de/ ˜jcg/grbrsh.html; Amati et al. 2002 and references therein).”
• Signatures of Extragalactic Dust in Pre-Swift GRB Afterglows (2005, background): “Fynbo et al. (2004) find tentative evidence for a low redshift (although the host galaxy would be very faint), and Butler et al. (2005a) find a preferred z ¼ 0:4 from the Amati relation (Amati et al. 2002).”
• THE COSMIC RATE, LUMINOSITY FUNCTION, AND INTRINSIC CORRELATIONS OF LONG GAMMA-RAY BURSTS (2009, neutral): “…tantalizing pre-Swift correlations between the host-frame characteristics of GRBs (e.g., Lloyd, Petrosian, & Mallozzi 2000; Fenimore & Ramirez-Ruiz 2000; Norris, Marani, & Bonnell 2000; Schaeffer 2003; Amati et al. 2002; Lamb et al. 2004; Ghirlanda, Ghisellini, & Lazzati 2004; Firmani et al. 2006).”
• Short versus long gamma-ray bursts: spectra, energetics, and luminosities (2009, background): “If the GRB redshift is known, from the bolometric fluence one can derive the isotropic equivalent energy, which was found to be correlated with the rest–frame peak energy (Amati et al. 2002, and Amati 2006).”
• A Comprehensive Analysis of Swift XRT Data. II. Diverse Physical Origins of the Shallow Decay Segment (2007, background): “This suggests that the apparent Ej,γ − E ′ p relation by assuming a jet origin of tb (Willingale et al. 2007) is likely a manifestation of the Amati-relation.”
• THE THIRD SWIFT BURST ALERT TELESCOPE GAMMA-RAY BURST CATALOG (2015, methodology): “…1,rest 2,rest band,rest rest rest 1,rest 2,rest rest rest rest 1,rest 2,rest rest rest rest rest rest 1,rest 2,rest 1,rest 2,rest 1,rest 2,rest ( ) Sband,rest corresponds to the ò a bEN E E A dE, , , ,1 10000 0( ) in the original equation in Amati et al. (2002).”
• JET BREAKS AND ENERGETICS OF Swift GAMMA-RAY BURST X-RAY AFTERGLOWS (2008, methodology): “…of the spectrum and integrate it over the desired energy range, correcting for the distance and redshift (k-correction) effects using the method of Amati et al. (2002) Eγ,iso = 4πD2L (1 + z) ∫ 10 MeV/(1+z) 1 keV/(1+z) E F (E) dE (A1) where F (E) is the functional form of the spectrum, and DL is…”
• Gamma-Ray Burst Formation Rate Inferred from the Spectral Peak Energy-Peak Luminosity Relation (2003, methodology): “The k-correction factors (kc) are estimated by the same method used by Amati et al. (2002), are consistent with the ones of Bloom et al. (2001), and do not exceed 2.”