Measuring the cosmological parameters with the Ep,i–Eiso correlation of gamma-ray bursts

By L. Amati, C. Guidorzi, Federico Frontera, M. Della Valle, F. Finelli, R. Landi, Enrico Montanari. 2008

330 citations recorded by the source corpus.

We have used the E p,i -E iso correlation of gamma-ray bursts (GRBs) to measure the cosmological parameter Ω M . By adopting a maximum likelihood approach which allows us to correctly quantify the extrinsic (i.e. non-Poissonian) scatter of the correlation, we constrain (for a flat universe) Ω M to 0.04-0.40 (68 per cent confidence level), with a best-fitting value of Ω M ∼ 0.15, and exclude Ω M = 1 at >99.9 per cent confidence level. If we release the assumption of a flat universe, we still find evidence for a low value of Ω M (0.04-0.50 at 68 per cent confidence level) and a weak dependence of the dispersion of the E p,i -E iso correlation on Ω Λ (with an upper limit of Ω Λ ∼ 1.15 at 90 per cent confidence level). Our approach makes no assumptions on the E p,i -E iso correlation and it does not use other calibrators to set the 'zero' point of the relation, therefore our treatment of the data is not affected by circularity and the results are independent of those derived via Type Ia supernovae (or other cosmological probes). Unlike other multi-parameters correlations, our analysis grounds on only two parameters, then including a larger number (a factor of ∼3) of GRBs and being less affected by systematics. Simulations based on realistic extrapolations of ongoing (and future) GRB experiments (e.g. Swift, Konus-Wind, GLAST) show that: (i) the uncertainties on cosmological parameters can be significantly decreased and (ii) future data will allow us to get clues on the 'dark energy' evolution.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b28474347df8381812dfd456d0567c86a9c35695

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Bing Zhang
2. E. Berger
3. Pawan Kumar
4. B. Metzger
5. Xuefeng Wu
6. D. Burrows
7. Raffaella Margutti
8. L. Amati

Citations in the corpus

• THE COSMIC RATE, LUMINOSITY FUNCTION, AND INTRINSIC CORRELATIONS OF LONG GAMMA-RAY BURSTS (2009, background): “However, the correlation is not a narrow log-log relation (e.g., Amati et al. 2008), and its observed appearance (more like an inequality) is strongly detector-dependent.”
• The prompt-afterglow connection in gamma-ray bursts: a comprehensive statistical analysis of Swift X-ray light curves (2012, background): “• Epk: rest-frame peak energy of the νFν spectrum during the prompt γ-ray emission from Amati et al. (2008).”
• Extremely energetic Fermi Gamma-Ray Bursts obey spectral energy correlations (2009, unknown): “E iso plane is very close to the best-fit power-law obtained for a sample of 70 long GRBs considered by Amati et al. (2008).”
• A PHOTOMETRIC REDSHIFT OF z ∼ 9.4 FOR GRB 090429B (2011, background): “A second line of evidence comes from observed high-energy correlations seen in many GRBs, in particular, in the relation between the peak energy of the νFν spectrum (Ep) and the burst isotropic energy (Amati et al. 2008).”
• COSMOLOGICAL IMPLICATIONS OF FAST RADIO BURST/GAMMA-RAY BURST ASSOCIATIONS (2013, methodology): “We apply the so-called Amati relation (Amati et al. 2002, 2008; Capozziello & Izzo 2010) log Eγ,iso erg = A+ γ log Ep,z keV (16) to estimate the redshifts of the two GRBs.”
• A new method for estimating the bolometric properties of Ibc supernovae (2013, unknown): “(1) Zhang et al. (2012), (2) Savaglio et al. (2009), (3) Amati et al. (2008), (4) Wiersema et al. (2007), (5) Levesque et al. (2010), (6) Sollerman et al. (2007), (7) Grupe et al. (2007), (8) Margutti et al. (2008), (9) Ghirlanda et al. (2010), (10) Page et al. (2011), (11) Troja et al. (2012),…”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “milar to the one obtained using the Ghirlanda relation. Later, Amati and collaborators suggested that the Amati-relation can also be used for the purpose of constraining cosmological parameters (e.g. Amati et al., 2008); see Amati and Valle (2013) for a review. We would like to point out two serious”