Short Gamma-Ray Bursts with Extended Emission

By Jay Norris, J. Bonnell. 2006

406 citations recorded by the source corpus.

The recent association of several short gamma-ray bursts (GRBs) with early-type galaxies with low star formation rates demonstrates that short bursts arise from a different progenitor mechanism than long bursts. However, since the duration distributions of the two classes overlap, membership is not always easily established. The picture is complicated by occasional softer, extended emission lasting tens of seconds after the initial spikelike emission comprising an otherwise short burst. Using the large BATSE sample with time-tagged event (TTE) data, we show that the fundamental defining characteristic of the short-burst class is that the initial spike exhibits negligible spectral evolution at energies above ~25 keV. The behavior is nearly ubiquitous for the 260 bursts with T90 < 2 s for which the BATSE TTE data type completely included the initial spike. We find this same signature—negligible spectral lag—for six Swift BAT short bursts and one HETE-2 short burst. We also analyze a small sample of "short" BATSE bursts—those with the most fluent, intense extended emission. The same lack of evolution on the pulse timescale obtains for the extended emission in the brighter bursts for which significant measurements can be made. We also show that the dynamic range in the ratio of peak intensities, spike:extended, is ~104. However, for our BATSE sample the total counts fluence of the extended component equals or exceeds that in the spike by a factor of several. A high Lorentz factor, ~500-1000, might explain the negligible lags.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/87cde667db72f05835fa015aa0f6f715758be1b0

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Bing Zhang
2. E. Berger
3. B. Metzger
4. Pawan Kumar
5. E. Nakar
6. E. Liang
7. E. Quataert
8. T. Piran

Citations in the corpus

• Short-Duration Gamma-Ray Bursts (2013, background): “Another difference between short and long GRBs is evident in the distribution of spectral lags, which are generally∼> 0 s for long GRBs (i.e., they exhibit a hard to soft evolution), while they are∼ 0 s (±20 ms) for short GRBs (Norris & Bonnell 2006; Norris, Gehrels & Scargle 2011).”
• THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. II. TYPE I GRB VERSUS TYPE II GRB OPTICAL AFTERGLOWS (2008, background): “Norris & Bonnell (2006) propose that a strong indicator for a merger-population event is a negligible spectral lag between different energy bands, i.e. Type I GRBs do not follow a lag-luminosity correlation (Norris et al. 2000).”
• WHAT IS THE MOST PROMISING ELECTROMAGNETIC COUNTERPART OF A NEUTRON STAR BINARY MERGER? (2011, background): “A mystery associated with SGRBs is that ∼ 1/4 − 1/2 are followed by variable X-ray emission with a fluence comparable to, or in excess of the initial burst (e.g., Norris & Bonnell 2006; Perley et al. 2009).”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “Short GRBs do not show significant spectral lags [430].”
• An Ordinary Short Gamma-Ray Burst with Extraordinary Implications: Fermi-GBM Detection of GRB 170817A (2017, background): “Limits on Extended Emission 19 Since the launch of Swift BAT, a class of short GRBs with softer extended emission has been discovered (Norris & Bonnell 2006), with a signature short, hard spike typical of short GRBs followed by a weaker long, soft tail extending from a few seconds to more than a…”
• DISCERNING THE PHYSICAL ORIGINS OF COSMOLOGICAL GAMMA-RAY BURSTS BASED ON MULTIPLE OBSERVATIONAL CRITERIA: THE CASES OF z = 6.7 GRB 080913, z = 8.2 GRB 090423, AND SOME SHORT/HARD GRBs (2009, background): “More importantly, several strong Type I GRB candidates (e.g. GRB 050724) are not short, but have softer, extended emission (Villasenor et al. 2005; Barthelmy et al. 2005a; Norris & Bonnell 2006).”
• Gamma-Ray Bursts in the Swift Era (2007, methodology): “Extended emission following short GRBs has been seen in about 1/3 of the sample in Table 1 (Norris & Bonnell 2006).”
• A time - luminosity correlation for Gamma - Ray Bursts in the X - rays (2008, background): “Indeed, the existence of an intermediated class of GRBs have also been studied (Norris & Bonnell (2006); Bernardini et al. (2007)).”
• Short versus long gamma-ray bursts: spectra, energetics, and luminosities (2009, background): “It was known from BATSE and Hete–II (Norris & Bonnell 2006; Donaghy et al. 2006) that the short hard spikes can be followed by dim, very long–duration emission (referred to as “extended emission”).”
• Optical and X-ray emission from stable millisecond magnetars formed from the merger of binary neutron stars (2013, background): “This includes bright X-ray flaring on timescales∼ 10-100 seconds after the initial spike (e.g., Norris & Bonnell 2006; Bostancı et al. 2013), which could be powered by jetted emission from a collimated magnetar outflow (Metzger et al. 2008; Bucciantini et al. 2012; Gompertz et al. 2013), a process…”
• THE THIRD SWIFT BURST ALERT TELESCOPE GAMMA-RAY BURST CATALOG (2015, background): “Short GRBs with extended emissions have raised special interests among the GRB community, partially due to their mixed characteristics between the short and long bursts (e.g., Gehrels et al. 2006; Norris & Bonnell 2006; Troja et al. 2008; Kaneko et al. 2015).”
• Making a Short Gamma-Ray Burst from a Long One: Implications for the Nature of GRB 060614 (2006, background): “From the prompt emission analysis, GRB 060614 has very small spectral lags (Gehrels et al. 2006), being consistent with the property of typical short GRBs (Yi et al. 2005; Norris & Bonnell 2006).”
• RELATIVISTIC SHOCK BREAKOUTS—A VARIETY OF GAMMA-RAY FLARES: FROM LOW-LUMINOSITY GAMMA-RAY BURSTS TO TYPE Ia SUPERNOVAE (2011, background): “Nevertheless, it is worth looking for an initial hard spike in nearby GRBs. Interestingly, there is a sub-sample of BATSE GRBs that show an initial short hard spikes followed by a softer burst (Norris & Bonnell 2006).”
• Short GRBs with Extended Emission from Magnetar Birth: Jet Formation and Collimation (2011, background): “Such events cannot be too common because the fraction of short GRBs with observed EE is already rather large (Norris & Bonnell 2006).”
• FERMI OBSERVATIONS OF GRB 090510: A SHORT–HARD GAMMA-RAY BURST WITH AN ADDITIONAL, HARD POWER-LAW COMPONENT FROM 10 keV TO GeV ENERGIES (2010, background): “By contrast, short duration GRBs typically show no evidence for lags between different energy ranges below 1MeV (Norris & Bonnell 2006).”
• The Ep,i–Eiso correlation in gamma-ray bursts: updated observational status, re-analysis and main implications (2006, background): “Thus the Ep,i – Eiso plane may be a powerful tool under this respect, especially when combined e.g with the lack of spectral lag and spectral evolution which seems to characterize short GRBs (Norris & Bonnell 2006).”
• The Proto-Magnetar Model for Gamma-Ray Bursts (2010, background): “…mysteries associated with shortduration GRBs is that ∼> 1/4 are followed by a ‘tail’ of emission (usually soft X-rays) starting ∼ 10 seconds after the GRB and lasting for ∼ 30− 100 seconds (Norris & Bonnell 2006; Gehrels et al. 2006; Gal-Yam et al. 2006; Perley et al. 2009; Norris et al. 2010).”
• GRB 080503: IMPLICATIONS OF A NAKED SHORT GAMMA-RAY BURST DOMINATED BY EXTENDED EMISSION (2008, background): “While lag can vary between pulses in a GRB (Hakkila et al. 2008) and short pulses typically have short lags, even very short pulses in canonical long GRBs have been observed to have nonnegligible lags (Norris & Bonnell 2006).”