Relativistic ejecta from X-ray flash XRF 060218 and the rate of cosmic explosions

Söderberg, A. M.; Kulkarni, S. R.; Nakar, Ehud; Berger, E.; Cameron, P. B.; Fox, D. B.; Frail, D. A.; Gal‐Yam, A.; Sari, Re’em; Cenko, S. Bradley; Kasliwal, M. M.; Chevalier, Roger A.; Piran, Tsvi; Price, P. A.; Schmidt, B.; Pooley, G. G.; Moon, D. S.; Penprase, B. E.; Ofek, E. O.; Rau, A.; Gehrels, N.; Nousek, J. A.; Burrows, D. N.; Persson, S. E.; McCarthy, P. J.

doi:10.1038/nature05087

Cited by 509 publications

(805 citation statements)

References 28 publications

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“…The motivation for this work is, on the one hand, to assess the ability of the magnetar model in reproducing 4 There is no evidence for strong collimation in the class of lowluminosity GRBs (see e.g., Soderberg et al 2006). Some SNe Ic-BL show evidence for mildly relativistic ejecta (SN 2009bb, Soderberg et al 2010SN 2012ap, Margutti et al 2014, Chakraborti et al 2015.…”

Section: Introductionmentioning

confidence: 99%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

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Broad-lined type Ic supernovae (SNe Ic-BL) are peculiar stellar explosions that distinguish themselves from ordinary SNe. Some SNe Ic-BL are associated with long-duration ( 2 s) gamma-ray bursts (GRBs). Black holes and magnetars are two types of compact objects that are hypothesized to be central engines of GRBs. In spite of decades of investigations, no direct evidence for the formation of black holes or magnetars has been found for GRBs so far. Here we report the finding that the early peak (t 50 days) and late-time (t 300 days) slow decay displayed in the light curves of both SNe 1998bw (associated with GRB 980425) and 2002ap (not GRB-associated) can be attributed to magnetar spin-down with initial rotation period P 0 ∼ 20 ms, while the intermediate-time (50 t 300 days) exponential decline is caused by radioactive decay of 56 Ni. The connection between the early peak and late-time slow decline in the light curves is unexpected in alternative models. We thus suggest that GRB 980425 and SN 2002ap were powered by magnetars.

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Section: Introductionmentioning

confidence: 99%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

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“…Figure 8 shows the expected areal densities of extragalactic radio transients brighter than 0.1 mJy within given distances. The areal densities of type Ibc supernovae(SNe Ibc; Berger et al 2003;Soderberg et al 2006b), low-luminosity GRBs(LLGRB; Soderberg et al 2006a;Barniol Duran et al 2015), and tidal disruption events(TDEs) without strong jets Holoien et al 2015;van Velzen et al 2016) are so small that it will be quite rare to detect them as false positive transients. Although off-axis long GRBs(LGRBs; van Eerten et al 2010; Ghirlanda et al 2014) and tidal disruption events with strong jets (TDE(jet); Burrows et al 2011;Zauderer et al 2011;Berger et al 2012) can be false positive transients, they will be identified earlier through their optical counterparts or can be filtered by identifying their host galaxies since the typical distance of these events is far beyond the detectable distance of the GW networks.…”

Section: False Positives: Extragalactic Radio Transients and Variablesmentioning

confidence: 99%

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Hotokezaka

Nissanke

Hallinan

et al. 2016

ApJ

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113

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Mergers of binary neutron stars and black hole-neutron star binaries produce gravitational-wave(GW) emission and outflows with significant kinetic energies. These outflows result in radio emissions through synchrotron radiation. We explore the detectability of these synchrotron-generated radio signals by follow-up observations of GW merger events lacking a detection of electromagnetic counterparts in other wavelengths. We model radio light curves arising from (i) sub-relativistic merger ejecta and (ii) ultra-relativistic jets. The former produce radio remnants on timescales of a few years and the latter produce γ-ray bursts in the direction of the jet and orphan-radio afterglows extending over wider angles on timescales of weeks. Based on the derived light curves, we suggest an optimized survey at 1.4 GHz with five epochs separated by a logarithmic time interval. We estimate the detectability of the radio counterparts of simulated GW-merger events to be detected by advanced LIGO and Virgo by current and future radio facilities. The detectable distances for these GW merger events could be as high as 1 Gpc. Around 20%-60% of the long-lasting radio remnants will be detectable in the case of the moderate kinetic energy of 3 10 50 · erg and a circum-merger density of -0.1 cm 3 or larger, while 5%-20% of the orphan-radio afterglows with kinetic energy of 10 48 erg will be detectable. The detection likelihood increases if one focuses on the well-localizable GW events. We discuss the background noise due to radio fluxes of host galaxies and false positives arising from extragalactic radio transients and variable activegalacticnuclei, and we show that the quiet radio transient sky is of great advantage when searching for the radio counterparts.

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“…Angular and energetic properties suggest that brief engines (with T inj < T breakout , either due to short T inj or large θ 0 ) represent excellent models to explain the debated llGRBs. In particular, brief engines' jets display two of llGRBs peculiar, and hard to explain, features: 1) an estimated llGRBs rate ~100 times higher than that of GRBs [3,4,5] and, 2) a potentially energetic SN emission ~ 10 51-52 erg [6] (as most of these failed jets' are not well collimated and expands with sub-relativistic velocities). These two features only arise from brief engines.…”

Section: Resultsmentioning

confidence: 99%

“…llGRBs and their contrast to classical GRBs, present a challenge to the traditional collapsar model. Apart from being several orders of magnitude softer than typical GRBs, llGRBs show: 1) Huge rates, ~100 times than typical GRBs: ~220 Gpc -3 yr -1 [9], ~110 Gpc -3 yr -1 [10], ~260 Gpc -3 yr -1 [11], a rate of llGRBs/GRBs ~ 300 -1000 [12], ~325 Gpc -3 yr -1 [5] and, ~380 Gpc -3 yr -1 [13] (the rate of GRB is ~1 Gpc-3 yr-1). 2) Strong and clear SN connection, in contrast with the typically SN-less GRBs.…”

Section: Introductionmentioning

confidence: 99%

“…Our results show that the expanding jet's hydrodynamical properties significantly differ, in particular outflow collimation and relativistic acceleration. The implication of this is that brief engines (with T inj < T breakout , either due to a short T inj or to a large θ 0 ) represent excellent systems to explain the debated low-luminosity GRBs (llGRBs), displaying two of llGRBs peculiar features: i) the estimated llGRBs rate at least about 100 times higher than that of GRBs [3,4,5], and ii) potentially energetic SN emission [6]. We find that these two features only arise from brief engines.…”

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confidence: 99%

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Failed Collapsar Jets to Explain Low Luminosity GRB Properties

Hamidani¹,

Umeda²,

Takahashi³

2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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Using the collapsar scenario for long GRBs [1], we present series of numerical simulations to investigate properties of expanding jets, driven by engines deploying the same total energy (10 52 erg), differently. We include a wide range of engine durations (T inj ), from 0.1 to 100 sec, as well as different initial opening angles (θ 0 ) for the deployed energy. We employ an AMR 2D special relativistic hydrodynamical code, using a 25 solar mass Wolf-Rayet star as the progenitor [2]. We analyze the effect of the engine duration on the jet's hydrodynamic properties, and discuss the implications on GRB and SN emissions. Our results show that the expanding jet's hydrodynamical properties significantly differ, in particular outflow collimation and relativistic acceleration. The implication of this is that brief engines (with T inj < T breakout , either due to a short T inj or to a large θ 0 ) represent excellent systems to explain the debated low-luminosity GRBs (llGRBs), displaying two of llGRBs peculiar features: i) the estimated llGRBs rate at least about 100 times higher than that of GRBs [3,4,5], and ii) potentially energetic SN emission [6]. We find that these two features only arise from brief engines. The conclusion is that brief engines dominate collapsars, at least at low redshift.

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Relativistic ejecta from X-ray flash XRF 060218 and the rate of cosmic explosions

Cited by 509 publications

References 28 publications

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Failed Collapsar Jets to Explain Low Luminosity GRB Properties

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