The Connection between Gamma-Ray Bursts and Extremely Metal-poor Stars: Black Hole-forming Supernovae with Relativistic Jets

Tominaga, Nozomu; Maeda, Keiichi; Umeda, Hideyuki; Nomoto, Ken’ichi; Tanaka, Masaomi; Iwamoto, Nobuyuki; Suzuki, Tomoharu; Mazzali, P. A.

doi:10.1086/513193

Cited by 127 publications

(153 citation statements)

References 38 publications

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“…Our observations argue against a significant non-axisymmetric supernova, such as one in which much of the explosion energy is channelled into a jet, since this would entrain and eject material from the core region. Any appreciable jet would lower [Mg/Fe] below that observed 11 .…”

mentioning

confidence: 71%

A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3

Keller

Bessell

Frebel

et al. 2014

Nature

355

401

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The element abundance ratios of four low-mass stars with extremely low metallicities indicate that the gas out of which the stars formed was enriched in each case by at most a few, and potentially only one low-energy, supernova 1,2,3,4 . Such supernovae yield large quantities of light elements such as carbon but very little iron. The dominance of lowenergy supernovae is surprising, because it has been expected that the first stars were extremely massive, and that they disintegrated in pair-instability explosions that would rapidly enrich galaxies in iron 5 . What has remained unclear is the yield of iron from the first supernovae, because hitherto no star is unambiguously interpreted as encapsulating the yield of a single supernova. Here we report the optical spectrum of SMSS J031300.36-670839.3, which shows no evidence of iron (with an upper limit of 10 -7.1 times solar abundance). Based on a comparison of its abundance pattern with those of models, we conclude that the star was seeded with material from a single supernova with an original mass of ~60 M  (and that the supernova left behind a black hole). Taken together with the previously mentioned low-metallicity stars, we conclude that low-energy supernovae were

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mentioning

confidence: 71%

A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3

Keller

Bessell

Frebel

et al. 2014

Nature

355

401

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“…These galaxies are of late type, lie at relatively low redshifts and present a moderate level of star formation activity. The absence of brightening in the late optical light curve of GRB 071227 rules against an association with a bright core collapse SN, though the limit M B > −15 on the peak absolute magnitude cannot exclude the presence of a core-collapse explosion characterized by low energy and very little content of 56 Ni in the ejecta (Della Valle et al 2006;Tominaga et al 2007). The offsets between the afterglows and the centers of their host galaxies may suggest that these short GRBs originated from the merging of double compact objects system likely of "primordial" origin.…”

Section: Discussionmentioning

confidence: 99%

The optical afterglows and host galaxies of three short/hard gamma-ray bursts

D’Avanzo¹,

Malesani

Covino³

et al. 2009

A&A

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Context. Our knowledge of short gamma-ray bursts (GRBs) has significatively improved in the Swift era. Rapid multiband observations from the largest ground-based observatories led to the discovery of the optical afterglows and host galaxies of these events. In spite of these advancements, the number of short GRBs with secure detections in the optical is still fairly small. Short GRBs are commonly thought to originate from the merging of double compact object binaries but direct evidence for this scenario is still missing. Aims. Optical observations of short GRBs allow us to measure redshifts, firmly identify host galaxies, characterize their properties, and accurately localize GRBs within them. Multiwavelength observations of GRB afterglows provide useful information on the emission mechanisms at work. These are all key issues that allow one to discriminate among different models of these elusive events. Methods. We carried out photometric observations of the short/hard GRB 051227, GRB 061006, and GRB 071227 with the ESO-VLT starting from several hours after the explosion down to the host galaxy level several days later. For GRB 061006 and GRB 071227 we also obtained spectroscopic observations of the host galaxy. We compared the results obtained from our optical observations with the available X-ray data of these bursts. Results. For all the three above bursts, we discovered optical afterglows and firmly identified their host galaxies. About half a day after the burst, the optical afterglows of GRB 051227 and GRB 061006 present a decay significatly steeper than in the X-rays. In the case of GRB 051227, the optical decay is so steep that it likely indicates different emission mechanisms in the two wavelength ranges. The three hosts are blue star forming galaxies at moderate redshifts and with metallicities comparable to the Solar one. The projected offsets of the optical afterglows from their host galaxy center span a wide range, but all afterglows lie within the light of their hosts and present evidence for local absorption in their X-ray spectra. We discuss our findings in light of the current models of short GRB progenitors.

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“…3.11). The origin of the other two bursts (GRB 060505 and GRB 060614) remains controversial: they have been argued to be linked to the explosions of massive stars that produce very little radioactive nickel and thus no radioactivity-driven SN emission (Fynbo et al 2006;Della Valle et al 2006a;Gal-Yam et al 2006;Thöne et al 2008;McBreen et al 2008;Tominaga et al 2007;Fryer et al 2006Fryer et al , 2007, whereas other indicators point to an origin in merging compact objects despite their longer duration, which would naturally not be accompanied by SN emission (Gehrels et al 2006;Zhang et al 2007;Ofek et al 2007;Kann et al 2008;Krimm et al 2009). …”

Section: Fig 12mentioning

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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The Connection between Gamma-Ray Bursts and Extremely Metal-poor Stars: Black Hole-forming Supernovae with Relativistic Jets

Cited by 127 publications

References 38 publications

A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3

A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3

The optical afterglows and host galaxies of three short/hard gamma-ray bursts

Searching for differences inSwift’s intermediate GRBs

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