A simple empirical redshift indicator for gamma-ray bursts

Atteia, J. L.

doi:10.1051/0004-6361:20030958

Cited by 92 publications

(117 citation statements)

References 27 publications

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“…It is important to mention here that this error is a statistical one, while the systematic error is much bigger (Atteia 2003;Pelangeon et al 2006;Pelangeon 2008), of a factor of ∼1.5, i.e., z = 0.9 +0.45 −0.3 . This result agrees with the redshift range found from the Amati relation for episode 2 and is also consistent with the upper limit determined with method 1.…”

Section: Methods 3: Empirical Methods For the Pseudo-redshiftmentioning

confidence: 90%

“…From a sample of 17 GRBs with known redshift reported in Atteia (2003) we compute the theoretical evolution of X with the redshift z, that is X = f (z). Then we invert the relation to derive a pseudo-redshift from the value of X.…”

Section: Methods 3: Empirical Methods For the Pseudo-redshiftmentioning

confidence: 99%

“…It is interesting, as a rough estimate, that if one were to assume that the two sources, GRB 101023 and GRB 090618 had not only the same morphology but also the same energy E iso , one would infer z = 1 for the cosmological redshift of GRB 101023. A main result of this article is that, assuming the validity of the Amati relation (see Amati et al 2009, and references therein) and Atteia criteria (Atteia 2003), it is possible to theoretically derive an expected cosmological redshift z = 0.9 ± 0.084(stat.) ± 0.2(sys.)…”

Section: Introductionmentioning

confidence: 94%

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Evidence for a proto-black hole and a double astrophysical component in GRB 101023

Penacchioni

Ruffini

Izzo

et al. 2012

A&A

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Context. It has been recently shown that GRB 090618, observed by AGILE, Coronas Photon, Fermi, Konus, Suzaku, and Swift, is composed of two very different components: episode 1, lasting 50 s, shows a thermal plus power-law spectrum with a characteristic temperature evolving in time as a power law; episode 2 (the remaining 100 s) is a canonical long GRB. We have associated episode 1 to the progenitor of a collapsing bare core leading to the formation of a black hole: what was defined as a "proto black hole" Aims. In precise analogy with GRB 090618 we aim to analyze the 89 s of the emission of GRB 101023, observed by Fermi, Gemini, Konus and Swift, to see if there are two different episodes: the first one presenting a characteristic black-body temperature evolving in time as a broken power law, and the second one consistent with a canonical GRB. Methods. To obtain information on the spectra, we analyzed the data provided by the GBM detector onboard the Fermi satellite, and we used the heasoft package XSPEC and RMFIT to obtain their spectral distribution. We also used the numerical code GRBsim to simulate the emission in the context of the fireshell scenario for episode 2. Results. We confirm that the first episode can be well fit by a black body plus power-law spectral model. The temperature changes with time following a broken power law, and the photon index of the power-law component presents a soft-to-hard evolution. We estimate that the radius of this source increases with time with a velocity of 1.5 × 10 4 km s −1 . The second episode appears to be a canonical GRB. By using the Amati and the Atteia relations, we determined the cosmological redshift, z ∼ 0.9±0.084(stat.)±0.2(sys.). The results of GRB 090618 are compared and contrasted with the results of GRB 101023. Particularly striking is the scaling law of the soft X-ray component of the afterglow. Conclusions. We identify GRB 090618 and GRB 101023 with a new family of GRBs related to a single core collapse and presenting two astrophysical components: a first one related to the proto-black hole prior to the process of gravitational collapse (episode 1), and a second one, which is the canonical GRB (episode 2) emitted during the formation of the black hole. For the first time we are witnessing the process of a black hole formation from the instants preceding the gravitational collapse up to the GRB emission. This analysis indicates progress towards developing a GRB distance indicator based on understanding the P-GRB and the prompt emission, as well as the soft X-ray behavior of the late afterglow.

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Section: Methods 3: Empirical Methods For the Pseudo-redshiftmentioning

confidence: 90%

Section: Methods 3: Empirical Methods For the Pseudo-redshiftmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 94%

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Evidence for a proto-black hole and a double astrophysical component in GRB 101023

Penacchioni

Ruffini

Izzo

et al. 2012

A&A

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“…Neither the time history, nor the spectrum, nor the intensity of this event was exceptional in any way. Atteia (2003) has proposed a simple redshift estimator based on the photon flux, energy spectrum, and duration of a GRB. Using this method, we obtain z % 0:8, with a statistical uncertainty of about 50%.…”

Section: Observationsmentioning

confidence: 99%

Multiwavelength Studies of the Optically Dark Gamma‐Ray Burst 001025A

Pedersen

Hurley

Hjorth

et al. 2006

ApJ

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We identify the fading X-ray afterglow of GRB 001025A from XMM-Newton observations obtained 1.9-2.3 days, 2 yr, and 2.5 yr after the burst. The nondetection of an optical counterpart to an upper limit of R ¼ 25:5, 1.20 days after the burst, makes GRB 001025A a ''dark'' burst. Based on the X-ray afterglow spectral properties of GRB 001025A, we argue that some bursts appear optically dark because their afterglow is faint and their cooling frequency is close to the X-ray band. This interpretation is applicable to several of the few other dark bursts where the X-ray spectral index has been measured. The X-ray afterglow flux of GRB 001025A is an order of magnitude lower than for typical longduration gamma-ray bursts. The spectrum of the X-ray afterglow can be fitted with an absorbed synchrotron emission model, an absorbed thermal plasma model, or a combination thereof. For the latter, an extrapolation to optical wavelengths can be reconciled with the R-band upper limit on the afterglow, without invoking any optical circumburst absorption, provided the cooling frequency is close to the X-ray band. Alternatively, if the X-ray afterglow is due to synchrotron emission only, 7 mag of extinction in the observed R-band is required to meet the R-band upper limit, making GRB 001025A much more obscured than bursts with detected optical afterglows. Based on the column density of X-ray-absorbing circumburst matter, an SMC gas-to-dust ratio is insufficient to produce this amount of extinction. The X-ray tail of the prompt emission enters a steep temporal decay excluding that the tail of the prompt emission is the onset of the afterglow. To within the astrometric uncertainty, this afterglow was coincident with an extended object, seen in a deep VLT R-band image, which we identify as the likely host galaxy of GRB 001025A.

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“…Band & Preece 2005;Ghirlanda et al 2005;Nakar & Piran 2005;Sakamoto et al 2006;Butler et al 2007;Cabrera et al 2007;Schaefer & Collazzi 2007;Butler et al 2009;Firmani et al 2009;Krimm et al 2009;Butler et al 2010;Shahmoradi & Nemiroff 2011;Collazzi et al 2012;Kocevski 2012;Goldstein 2012). Despite these discussions, the E pi -E iso relation was quickly proposed as a tool to infer GRB redshifts (Atteia 2003), to constrain the physics of the prompt emission (Eichler & Levinson 2004;Rees & Mészáros 2005) and the geometry of GRB jets (Lamb et al 2005;Toma et al 2005), and to standardize GRBs, in much the same way as the Phillips relation was used to standardize SNe Ia (Phillips 1993). This last approach aims at constructing standard candles with GRBs and at using them to constrain the cosmological parameters (e.g.…”

Section: Introductionmentioning

confidence: 99%

TheE_peak–E_isorelation revisited withFermiGRBs

Heussaff

Atteia

Zolnierowski

2013

A&A

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Aims. We used a sample of gamma-ray bursts (GRBs) detected by Fermi and Swift to reanalyze the correlation discovered by Amati et al. (2002, A&A, 390, 81) between E pi , the peak energy of the prompt GRB emission, and E iso , the energy released by the GRB assuming isotropic emission. This correlation has been disputed by various authors, and our aim is to assess whether it is an intrinsic GRB property or the consequence of selection effects. Methods. We constructed a sample of Fermi GRBs with homogeneous selection criteria, and we studied their distribution in the E pi -E iso plane. Our sample is made of 43 GRBs with a redshift and 243 GRBs without a redshift. We show that GRBs with a redshift follow a broad E pi -E iso relation, while GRBs without a redshift show several outliers. We use these samples to discuss the impact of selection effects associated with GRB detection and with redshift measurement. Results. We find that the E pi -E iso relation is partly due to intrinsic GRB properties and partly due to selection effects. The lower right boundary of the E pi -E iso relation stems from a true lack of luminous GRBs with low E pi . In contrast, the upper left boundary is attributed to selection effects acting against the detection GRBs with low E iso and large E pi that appear to have a lower signal-to-noise ratio. In addition, we demonstrate that GRBs with and without a redshift follow different distributions in the E pi -E iso plane. GRBs with a redshift are concentrated near the lower right boundary of the E pi -E iso relation. This suggests that it is easier to measure the redshift of GRBs close to the lower E pi -E iso boundary and that GRBs with a redshift follow the Amati relation better than the general population. In this context, we attribute the controversy about the reality of the Amati relation to the complex nature of this relation resulting from the combination of a true physical boundary and biases favoring the detection and the measurement of the redshift of GRBs located close to this boundary.

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A simple empirical redshift indicator for gamma-ray bursts

Cited by 92 publications

References 27 publications

Evidence for a proto-black hole and a double astrophysical component in GRB 101023

Evidence for a proto-black hole and a double astrophysical component in GRB 101023

Multiwavelength Studies of the Optically Dark Gamma‐Ray Burst 001025A

TheE_peak–E_isorelation revisited withFermiGRBs

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A simple empirical redshift indicator for gamma-ray bursts

Cited by 92 publications

References 27 publications

Evidence for a proto-black hole and a double astrophysical component in GRB 101023

Evidence for a proto-black hole and a double astrophysical component in GRB 101023

Multiwavelength Studies of the Optically Dark Gamma‐Ray Burst 001025A

TheEpeak–Eisorelation revisited withFermiGRBs

Contact Info

Product

Resources

About

TheE_peak–E_isorelation revisited withFermiGRBs