GRB 050509B: Constraints on Short Gamma-Ray Burst Models

Hjorth, J.; Sollerman, J.; Gorosabel, J.; Granot, Jonathan; Klose, S.; Kouveliotou, C.; Melinder, Jens; Ramírez-Ruiz, E.; Starling, R.; Thomsen, B.; Andersen, M. I.; Fynbo, J. P. U.; Jensen, B. L.; Vreeswijk, P. M.; Cerón, J. M. Castro; Jakobsson, P.; Levan, A. J.; Pedersen, K.; Rhoads, James E.; Tanvir, N. R.; Watson, Derrick G.; Wijers, R. A. M. J.

doi:10.1086/491733

Cited by 143 publications

(147 citation statements)

References 42 publications

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“…The data also rule out the existence of an early rebrightning in GRB 050509B [33] at 1.5 days in the restframe. Bright transient emission, dubbed a 'mini SN' [35,36], 'kilonova' [37] or 'macronova' [38], is expected to peak around the optical-UV range within a day or so with a semi-thermal spectrum [35].…”

Section: Supernova-less Gamma-ray Burstsmentioning

confidence: 55%

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The supernova–gamma-ray burst–jet connection

Hjorth

2013

Phil. Trans. R. Soc. A.

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The observed association between supernovae and gamma-ray bursts represents a cornerstone in our understanding of the nature of gamma-ray bursts. The collapsar model provides a theoretical framework for this connection. A key element is the launch of a bipolar jet (seen as a gamma-ray burst). The resulting hot cocoon disrupts the star, whereas the 56 Ni produced gives rise to radioactive heating of the ejecta, seen as a supernova. In this discussion paper, I summarize the observational status of the supernova–gamma-ray burst connection in the context of the ‘engine’ picture of jet-driven supernovae and highlight SN 2012bz/GRB 120422A—with its luminous supernova but intermediate high-energy luminosity—as a possible transition object between low-luminosity and jet gamma-ray bursts. The jet channel for supernova explosions may provide new insights into supernova explosions in general.

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Section: Supernova-less Gamma-ray Burstsmentioning

confidence: 55%

“…In figure 1, we have plotted the upper limits on the existence of supernovae accompanying GRB 050509B [33] and GRB 050709 [34]. These constrain any supernova to be about 100 times fainter than SN 1998bw at peak.…”

Section: Supernova-less Gamma-ray Burstsmentioning

confidence: 99%

The supernova–gamma-ray burst–jet connection

Hjorth

2013

Phil. Trans. R. Soc. A.

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“…However, this burst is known to be peculiar, being its optical emission dominated by a supernova component and not the afterglow (Campana et al 2006;Soderberg et al 2006; see also Thöne et al 2011). GRB 050509B an extremely faint short burst, most probably hosted by a giant elliptical galaxy at z = 0.22 (Hjorth et al 2005;Gehrels et al 2005;Castro-Tirado et al 2005) is the following dimmest limit. The least luminous burst with detection in the mm/submm range is GRB 041219A, which curiously was one of the longest and brightest GRBs detected, for which a redshift of z = 0.31 has been recently suggested (Götz et al 2011).…”

Section: Redshift Distribution and Luminositiesmentioning

confidence: 98%

Pre-ALMA observations of GRBs in the mm/submm range

Postigo

Lundgren

Martín

et al. 2012

A&A

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Context. Gamma-ray bursts (GRBs) generate an afterglow emission that can be detected from radio to X-rays during days, or even weeks after the initial explosion. The peak of this emission crosses the millimeter and submillimeter range during the first hours to days, making their study in this range crucial for constraining the models. Observations have been limited until now due to the low sensitivity of the observatories in this range. This situation will be greatly improved with the start of scientific operations of the Atacama Large Millimeter/submillimeter Array (ALMA). Aims. In this work we do a statistical analysis of the complete sample of mm/submm observations of GRB afterglows obtained before the beginning of scientific operations at ALMA. Methods. We present observations of 11 GRB afterglows obtained from the Atacama Pathfinder Experiment (APEX) and the SubMillimeter Array (SMA), as well as the first detection of a GRB with ALMA, still in the commissioning phase, and put them into context with a catalogue of all the observations that have been published until now in the spectral range that is covered by ALMA.Results. The catalogue of mm/submm observations collected here is the largest to date and is composed of 102 GRBs, of which 88 have afterglow observations, whereas the rest are host galaxy searches. With our programmes, we contributed with data of 11 GRBs and the discovery of 2 submm counterparts. In total, the full sample, including data from the literature, has 22 afterglow detections with redshifts ranging from 0.168 to 8.2. GRBs have been detected in mm/submm wavelengths with peak luminosities spanning 2.5 orders of magnitude, the most luminous reaching 10 33 erg s −1 Hz −1 . We observe a correlation between the X-ray brightness at 0.5 days and the mm/submm peak brightness. Finally we give a rough estimate of the distribution of peak flux densities of GRB afterglows, based on the current mm/submm sample. Conclusions. Observations in the mm/submm bands have been shown to be crucial for our understanding of the physics of GRBs, but have until now been limited by the sensitivity of the observatories. With the start of the operations at ALMA, the sensitivity has improved by more than an order of magnitude, opening a new era in the study of GRB afterglows and their host galaxies. Our estimates predict that, once completed, ALMA will detect up to ∼98% of the afterglows if observed during the passage of the peak synchrotron emission.

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“…There are a variety of objects capable of generating the fireball: collapsars (Woosley 1993;Paczyński 1998), neutron star -neutron star mergers (Paczynski 1990), neutron star -black hole mergers (Narayan et al 1992), or white dwarf -black hole mergers Chattopadhyay et al 2007;King et al 2007). The most widely accepted idea is that long GRBs are generated by collapsars (characterised by the presence of a core-collapse supernova, Galama et al 1998;Castro-Tirado & Gorosabel 1999;Hjorth et al 2003;Stanek et al 2003;Malesani et al 2004;Pian et al 2006), while short bursts are the result of compact binary mergers (with no supernova component, Gehrels et al 2005;Hjorth et al 2005a;Barthelmy et al 2005;Berger et al 2005c;Fong et al 2010). Specific studies of the progenitors of the intermediate class based on afterglow observations have not yet been done.…”

Section: Introductionmentioning

confidence: 99%

Searching for differences inSwift’s intermediate GRBs

Postigo

Horváth²,

Vereš

et al. 2010

A&A

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Context. Gamma-ray bursts are usually classified in terms their high-energy emission into either short-duration or long-duration bursts, which presumably reflect two different types of progenitors. However, it has been shown on statistical grounds that a third, intermediate population is needed in this classification scheme, although an extensive study of the properties of this class has so far not been performed. The large amount of follow-up studies generated during the Swift era allows us to have a sufficient sample to attempt a study of this third population through the properties of their prompt emission and their afterglows. Aims. To understand the differences of the intermediate population, we study a sample of GRBs observed by Swift during its first four years of operation. The sample contains only bursts with measured redshifts since these data help us to derive intrinsic properties. Methods. We search for differences in the properties of the three groups of bursts, which we quantify using a Kolmogorov-Smirnov test whenever possible. Results. Intermediate bursts are found to be less energetic and have dimmer afterglows than long GRBs, especially when considering the X-ray light curves, which are on average one order of magnitude fainter than long bursts. There is a less significant trend in the redshift distribution that places intermediate bursts closer than long bursts. Except for this, intermediate bursts show similar properties to long bursts. In particular, they follow the E peak versus E iso correlation and have, on average, positive spectral lags with a distribution similar to that of long bursts. As for long GRBs, they normally have an associated supernova, although some intermediate bursts have been found to contain no supernova component. Conclusions. This study shows that intermediate bursts differ from short bursts, but exhibit no significant differences from long bursts apart from their lower brightness. We suggest that the physical difference between intermediate and long bursts could be explained by being produced by similar progenitors, of the former being the ejecta thin shells and the latter thick shells.

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GRB 050509B: Constraints on Short Gamma-Ray Burst Models

Cited by 143 publications

References 42 publications

The supernova–gamma-ray burst–jet connection

The supernova–gamma-ray burst–jet connection

Pre-ALMA observations of GRBs in the mm/submm range

Searching for differences inSwift’s intermediate GRBs

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