<i>HETE</i>Observations of the Gamma‐Ray Burst GRB 030329: Evidence for an Underlying Soft X‐Ray Component

Vanderspek, R.; Sakamoto, T.; Barraud, C.; Tamagawa, Toru; Graziani, C.; Suzuki, M.; Shirasaki, Y.; Prigozhin, G.; Villaseñor, J.; Jernigan, J. G.; Crew, G. B.; Atteia, J. L.; Hurley, K.; Kawai, N.; Lamb, D. Q.; Ricker, G.; Woosley, S. E.; Butler, Nathaniel R.; Doty, J.; Dullighan, A.; Donaghy, T.; Fenimore, E. E.; Galassi, M.; Matsuoka, M.; Takagishi, K.; Torii, K.; Yoshida, A.; Boër, M.; Dezalay, J. P.; Olive, J. F.; Braga, J.; Manchanda, R. K.; Pizzichini, G.

doi:10.1086/423923

Cited by 64 publications

(53 citation statements)

References 22 publications

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“…This is also the case of GRB 130427A (the rightmost point in Figs. 2 and 5) that is one of the few nearby energetic GRBs (like GRB 030329 detected by Hete-2 at z = 0.17, Vanderspek et al 2004). GRB 130427A is at redshift z = 0.34, the value of V/V max for this GRB, V/V max = 0.003, indicates that there is a 10% chance observing this GRB so close among 30 similar bursts at higher redshift.…”

Section: Intrinsic Propertiesmentioning

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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Section: Intrinsic Propertiesmentioning

confidence: 99%

TheE_peak–E_isorelation revisited withFermiGRBs

Heussaff

Atteia

Zolnierowski

2013

A&A

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“…GRB 030329 was detected with the FREGATE detector (8Y 400 keV) on board the High-Energy Transient Explorer (HETE-2) on 2003 March 29 at 11 : 37:14 UT (Vanderspek et al 2004; also Fig. 3).…”

Section: Grb 030329mentioning

confidence: 99%

Prompt and Afterglow Emission Properties of Gamma-Ray Bursts with Spectroscopically Identified Supernovae

Kaneko¹,

Ramirez-Ruiz²,

Granot³

et al. 2006

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We present a detailed spectral analysis of the prompt and afterglow emission of four nearby long-soft gamma-ray bursts (GRBs 980425, 030329, 031203, and 060218) that were spectroscopically found to be associated with Type Ic supernovae and compare them to the general GRB population. For each event, we investigate the spectral and luminosity evolution and estimate the total energy budget based on broadband observations. The observational inventory for these events has become rich enough to allow estimates of their energy content in relativistic and subrelativistic form. The result is a global portrait of the effects of the physical processes responsible for producing long-soft GRBs. In particular, we find that the values of the energy released in mildly relativistic outflows appears to have a significantly smaller scatter than those found in highly relativistic ejecta. This is consistent with a picture in which the energy released inside the progenitor star is roughly standard, while the fraction of that energy that ends up in highly relativistic ejecta outside the star can vary dramatically between different events.

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“…Figure 1: Some properties of prompt GRB emission. Upper left: Light-curve of the bright GRB 030329 in the range 7-400 keV [78]. Upper right: νFν energy spectrum of GRB 100724B [29].…”

Section: Prompt Emissionmentioning

confidence: 99%

Gamma-Ray Bursts: Frontier astrophysics with the most extreme cosmic explosions

Atteia¹

2016

Proceedings of Frontier Research in Astrophysics — PoS(FRAPWS2014)

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This paper presents the main properties of Gamma-ray bursts (GRBs) and their connection with various topics of modern astrophysics. The future of the field is also addressed with a detailed presentation of the SVOM Sino-French mission and its scientific objectives. Keywords: Gamma-ray bursts, Cosmology, Gravity waves PoS(FRAPWS2014)026Gamma-Ray Bursts Jean-Luc Atteia Gamma-ray burstsGamma-ray bursts (GRBs) are powerful cosmic explosions produced at the end of the life of some massive stars, but also when two compact stars in a binary system merge after the dissipation of the angular momentum by gravitational waves. In both cases, the catastrophic event results in the birth of a fast rotating compact object (a black hole or a magnetar) which expels transient but very powerful relativistic jets in two opposite directions. If, by chance, one of these jets is directed towards the Earth, we observe a bright gamma-ray transient (the prompt GRB), which is followed by quickly fading afterglow emission at longer wavelengths (from X-rays to visible and radio). 1 While the brightness of GRBs allows their detection out to very large distances (up to redshift z = 8.3 for GRB 090423 [66,73]), we only detect the GRBs which emit a jet towards the Earth. Assuming an average opening angle of GRBs jets of a few degrees, the fraction of detectable GRBs amounts to 0.1 to 1%. This paper is divided into two parts. Section 1 provides a brief overview of the GRB phenomenon including some frontier topics that may interest the participants of this conference. Section 2 contains a brief description of the instruments and the scientific objectives of the future GRB mission SVOM, that will perpetuate GRB detection after Swift. The reader interested in getting a complete view of the field and its recent advances is invited to read the reviews listed in the bibliography [22,87,23,9,38,49]. The reader interested in an overview of the discoveries that have led to the solution of the so-called GRB mystery is invited to read the books of Vedrenne & Atteia [80] and of Kouveliotou, Wijers & Woosley [36]. Prompt emissionGRBs are transient events whose temporal evolution is divided into two steps: the prompt GRB and the afterglow. Figure 1 shows the main properties of the prompt GRB emission in hard X-rays: the light-curve of the bright nearby GRB 030329 at redshift z=0.17; the νFν spectrum of GRB 100724B peaking around E peak ∼ 500 keV; the isotropic distribution of GRBs on the sky [6], and the duration histogram which shows two peaks suggesting the existence of two classes, respectively called short and long GRBs. High-energy satellites play an essential role in the detection and classification of GRBs. The Large Area Detectors of BATSE, which have worked more than 9 years have shown that about 1000 GRBs cross the solar system each year (hereafter we call these bursts "classical GRBs", in contrast with X-Ray Flashes or low-luminosity GRBs described below). Since then, instruments like BeppoSAX WFC and HETE-2 WXM have extended GRB detection to soft ...

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HETEObservations of the Gamma‐Ray Burst GRB 030329: Evidence for an Underlying Soft X‐Ray Component

Cited by 64 publications

References 22 publications

TheE_peak–E_isorelation revisited withFermiGRBs

TheE_peak–E_isorelation revisited withFermiGRBs

Prompt and Afterglow Emission Properties of Gamma-Ray Bursts with Spectroscopically Identified Supernovae

Gamma-Ray Bursts: Frontier astrophysics with the most extreme cosmic explosions

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HETEObservations of the Gamma‐Ray Burst GRB 030329: Evidence for an Underlying Soft X‐Ray Component

Cited by 64 publications

References 22 publications

TheEpeak–Eisorelation revisited withFermiGRBs

TheEpeak–Eisorelation revisited withFermiGRBs

Prompt and Afterglow Emission Properties of Gamma-Ray Bursts with Spectroscopically Identified Supernovae

Gamma-Ray Bursts: Frontier astrophysics with the most extreme cosmic explosions

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TheE_peak–E_isorelation revisited withFermiGRBs

TheE_peak–E_isorelation revisited withFermiGRBs