A very energetic supernova associated with the γ-ray burst of 29 March 2003

Hjorth, J.; Sollerman, J.; Møller, P.; Fynbo, J. P. U.; Woosley, S. E.; Kouveliotou, C.; Tanvir, N. R.; Greiner, J.; Andersen, M. I.; Castro-Tirado, A. J.; Cerón, J. M. Castro; Fruchter, A. S.; Gorosabel, J.; Jakobsson, P.; Kaper, L.; Klose, S.; Masetti, N.; Pedersen, H.; Pedersen, K.; Pian, E.; Palazzi, E.; Rhoads, James E.; Rol, E.; Heuvel, E. P. J. van den; Vreeswijk, P. M.; Watson, Derrick G.; Wijers, R. A. M. J.

doi:10.1038/nature01750

Cited by 1,436 publications

(1,351 citation statements)

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“…These are known as 'broad-line SNe Ic' (or SNe Ic BL), and a further subset of SNe Ic BL have been linked to long duration Gamma Ray Bursts (LGRBs, see e.g. Galama et al 1998;Hjorth et al 2003). From a theoretical viewpoint, historically SN progenitors have been separated into two classes.…”

Section: Introductionmentioning

confidence: 99%

Statistical Studies of Supernova Environments

Anderson

James

Habergham

et al. 2015

Publ. Astron. Soc. Aust.

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Mapping the diversity of supernovae (SNe) to progenitor properties is key to our understanding of stellar evolution and explosive stellar death. Investigations of the immediate environments of SNe allow statistical constraints to be made on progenitor properties such as mass and metallicity. Here we review the progress that has been made in this field. Pixel statistics using tracers of e.g. star formation within galaxies show intriguing differences in the explosion sites of, in particular SNe types II and Ibc (SNe II and SNe Ibc respectively), suggesting statistical differences in population ages. Of particular interest is that SNe Ic are significantly more associated with host galaxy Hα emission than SNe Ib, implying shorter lifetimes for the former. In addition, such studies have shown (unexpectedly) that the interacting SNe IIn do not explode in regions containing the most massive stars, which suggests that at least a significant fraction of their progenitors arise from the lower end of the core-collapse SN mass range. Host H ii region spectroscopy has been obtained for a significant number of core-collapse events, however definitive conclusions on differences between distinct SN types have to-date been elusive. Single stellar evolution models predict that the relative fraction of SNe Ibc to SNe II should increase with increasing metallicity, due to the dependence of mass-loss rates on progenitor metallicity. We present a meta-analysis of all current host H ii region oxygen abundances for CC SNe. It is concluded that the SN II to SN Ibc ratio shows little variation with oxygen abundance, with only a suggestion that the ratio increases in the lowest bin. Radial distributions of different SNe are discussed, where a central excess of SNe Ibc has been observed within disturbed galaxy systems, which is difficult to ascribe to metallicity or selection effects. Environment studies are also being undertaken for SNe Ia, where constraints can be made on the shortest delay times of progenitor systems. It is shown that 'redder' SNe Ia are more often found within star-forming regions. Environment studies are evolving to enable studies at higher spatial resolutions than previously possible, while in addition the advent of widefield integral field unit instruments allows galaxy-wide spectral analyses which will provide fruitful results to this field. Some example contemporary results are shown in that direction.

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Section: Introductionmentioning

confidence: 99%

Statistical Studies of Supernova Environments

Anderson

James

Habergham

et al. 2015

Publ. Astron. Soc. Aust.

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“…LGRBs have been associated to supernovae (Galama et al 1999;Stanek et al 2003;Hjorth et al 2003;Matheson et al 2003), all of which lacked any hydrogen or helium lines and so were of the type-Ib/c (e.g., Filippenko 1997). In combination with the fact that any outer hydrogen layer of the star would stop the LGRB escaping (MacFadyen & Woosley 1999), means that the hydrogen envelope of the progenitor has to be lost before it undergoes gravitational collapse.…”

Section: Manymentioning

confidence: 99%

“…The association of LGRBs with the death of massive stars (Galama et al 1999;Stanek et al 2003;Hjorth et al 2003;Matheson et al 2003) facilitates their use as star formation tracers and their naturally luminous nature would complement or even surpass conventional methods at high redshift. However, before this connection can be used routinely and robustly, the way in which they trace one another must be known accurately.…”

Section: Manymentioning

confidence: 99%

The First Billion Years project: gamma-ray bursts at z > 5

Elliott

Khochfar

Greiner

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Long gamma-ray burst's (LGRB's) association to the death of massive stars suggest they could be used to probe the cosmic star formation history (CSFH) with high accuracy, due to their high luminosities. We utilise cosmological simulations from the First Billion Years project to investigate the biases between the CSFH and the LGRB rate at z > 5, assuming various different models and constraints on the progenitors of LGRBs. We populate LGRBs using a selection based on environmental properties and demonstrate that the LGRB rate should trace the CSFH to high redshifts. The measured LGRB rate suggests that LGRBs have opening angles of θ jet = 0.1 • , although the degeneracy with the progenitor model cannot rule out an underlying bias. We demonstrate that proxies that relate the LGRB rate with global LGRB host properties do not reflect the underlying LGRB environment, and are in fact a result of the host galaxy's spatial properties, such that LGRBs can exist in galaxies of solar metallicity. However, we find a class of host galaxies that have low stellar mass and are metal-rich, and that their metallicity dispersions would not allow low-metallicity environments. Detection of hosts with this set of properties would directly reflect the progenitor's environment. We predict that 10% of LGRBs per year are associated with this set of galaxies that would have forbidden line emission that could be detected by instruments on the James Webb Space Telescope. Such a discovery would place strong constraints on the collapsar model and suggest other avenues to be investigated.

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“…Several observational evidences point toward this hypothesis. At low redshift, the association between the GRBs and massive star progenitors is well established by (i) Type Ic supernovae (SNe) identified at the positions of GRB events (Hjorth et al 2003;Mirabal et al 2006) and (ii) the location of GRBs in Wolf-Rayet galaxies (Hammer et al 2006). At high redshift, the connection between GRBs and star-forming regions is inferred by (i) GRBs found in blue galaxies with nebular lines indicative of on-going star formation (Le Floc'h et al 2003;Prochaska et al 2004) and (ii) GRBs observed within a few kpc from the weighted flux centroid of their host (Fruchter et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Probing the Interstellar Medium and Stellar Environments of Long-Duration GRBs

2007

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Abstract.We review the properties of the gas surrounding high-redshift gamma-ray bursts (GRBs) assessed through the analysis of damped Lyman-alpha systems (DLAs) identified in their afterglow spectra. These GRB-DLAs are characterized by large H I column densities with a median of N (H I) = 10 21. 7 cm −2 , no molecular gas signatures, metallicities ranging from 1/100 to nearly solar with a median exceeding 1/10 solar, and no anomalous abundance patterns. The detection of the atomic Mg lines and the time-variability of the fine-structure lines demonstrates that the majority of the neutral gas along the GRB sightlines is located between 50 pc and a few kpc from the GRB. This implies that this gas is presumably associated with the ambient interstellar medium of the host galaxy and that the derived properties from low-ionization lines do not directly constrain the local environment of the GRB progenitor. The highly ionized gas, traced by N V lines, which could result from a pre-existing H II region produced by the GRB progenitor and neighboring OB stars, appears on the other hand to be very local to the GRB at about 10 pc, yielding a snapshot of the medium's physical conditions at this radius.

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A very energetic supernova associated with the γ-ray burst of 29 March 2003

Cited by 1,436 publications

References 25 publications

Statistical Studies of Supernova Environments

Statistical Studies of Supernova Environments

The First Billion Years project: gamma-ray bursts at z > 5

Probing the Interstellar Medium and Stellar Environments of Long-Duration GRBs

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