GRB 050911

A black hole-neutron star merger or a naked GRB

K. L. Page, A. R. King, A. J. Levan, P. T. O'Brien, J. P. Osborne, S. D. Barthelmy, A. P. Beardmore, David Nelson Burrows, S. Campana, N. Gehrels, J. Graham, M. R. Goad, O. Godet, Y. Kaneko, Jamie A. Kennea, C. B. Markwardt, D. E. Reichart, T. Sakamoto, N. R. Tanvir

Research output: Contribution to journalArticle

30 Citations (Scopus)

Abstract

GRB 050911, discovered by the Swift Burst Alert Telescope, was not seen 4.6 hr later by the Swift X-ray Telescope, making it one of the very few X-ray nondetections of a gamma-ray burst (GRB) afterglow at early times. The γ-ray light curve shows at least three peaks, the first two of which (∼To - 0.8 and To + 0.2 s, where To is the trigger time) were short, each lasting 0.5 s. This was followed by later emission 10-20 s postburst. The upper limit on the unabsorbed X-ray flux was 1.7 × 10-14 ergs cm-2 s-1 (integrating 46 ks of data taken between September 11 and 18), indicating that the decay must have been rapid. All but one of the long bursts detected by Swift were above this limit at ∼4.6 hr, whereas the afterglows of short bursts became undetectable more rapidly. Deep observations with Gemini also revealed no optical afterglow 12 hr after the burst, down to r = 24.0 (5 σ limit). We speculate that GRB 050911 may have been formed through a compact object (black hole-neutron star) merger, with the later outbursts due to a longer disk lifetime linked to a large mass ratio between the merging objects. Alternatively, the burst may have occurred in a low-density environment, leading to a weak, or nonexistent, forward shock - the so-called "naked GRB" model.

Original languageEnglish (US)
JournalAstrophysical Journal
Volume637
Issue number1 II
DOIs
StatePublished - Jan 20 2006

Fingerprint

gamma ray bursts
merger
neutron stars
bursts
afterglows
outburst
erg
telescopes
x rays
mass ratios
light curve
rays
actuators
shock
life (durability)
decay

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Page, K. L., King, A. R., Levan, A. J., O'Brien, P. T., Osborne, J. P., Barthelmy, S. D., ... Tanvir, N. R. (2006). GRB 050911: A black hole-neutron star merger or a naked GRB. Astrophysical Journal, 637(1 II). https://doi.org/10.1086/500430
Page, K. L. ; King, A. R. ; Levan, A. J. ; O'Brien, P. T. ; Osborne, J. P. ; Barthelmy, S. D. ; Beardmore, A. P. ; Burrows, David Nelson ; Campana, S. ; Gehrels, N. ; Graham, J. ; Goad, M. R. ; Godet, O. ; Kaneko, Y. ; Kennea, Jamie A. ; Markwardt, C. B. ; Reichart, D. E. ; Sakamoto, T. ; Tanvir, N. R. / GRB 050911 : A black hole-neutron star merger or a naked GRB. In: Astrophysical Journal. 2006 ; Vol. 637, No. 1 II.
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abstract = "GRB 050911, discovered by the Swift Burst Alert Telescope, was not seen 4.6 hr later by the Swift X-ray Telescope, making it one of the very few X-ray nondetections of a gamma-ray burst (GRB) afterglow at early times. The γ-ray light curve shows at least three peaks, the first two of which (∼To - 0.8 and To + 0.2 s, where To is the trigger time) were short, each lasting 0.5 s. This was followed by later emission 10-20 s postburst. The upper limit on the unabsorbed X-ray flux was 1.7 × 10-14 ergs cm-2 s-1 (integrating 46 ks of data taken between September 11 and 18), indicating that the decay must have been rapid. All but one of the long bursts detected by Swift were above this limit at ∼4.6 hr, whereas the afterglows of short bursts became undetectable more rapidly. Deep observations with Gemini also revealed no optical afterglow 12 hr after the burst, down to r = 24.0 (5 σ limit). We speculate that GRB 050911 may have been formed through a compact object (black hole-neutron star) merger, with the later outbursts due to a longer disk lifetime linked to a large mass ratio between the merging objects. Alternatively, the burst may have occurred in a low-density environment, leading to a weak, or nonexistent, forward shock - the so-called {"}naked GRB{"} model.",
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Page, KL, King, AR, Levan, AJ, O'Brien, PT, Osborne, JP, Barthelmy, SD, Beardmore, AP, Burrows, DN, Campana, S, Gehrels, N, Graham, J, Goad, MR, Godet, O, Kaneko, Y, Kennea, JA, Markwardt, CB, Reichart, DE, Sakamoto, T & Tanvir, NR 2006, 'GRB 050911: A black hole-neutron star merger or a naked GRB', Astrophysical Journal, vol. 637, no. 1 II. https://doi.org/10.1086/500430

GRB 050911 : A black hole-neutron star merger or a naked GRB. / Page, K. L.; King, A. R.; Levan, A. J.; O'Brien, P. T.; Osborne, J. P.; Barthelmy, S. D.; Beardmore, A. P.; Burrows, David Nelson; Campana, S.; Gehrels, N.; Graham, J.; Goad, M. R.; Godet, O.; Kaneko, Y.; Kennea, Jamie A.; Markwardt, C. B.; Reichart, D. E.; Sakamoto, T.; Tanvir, N. R.

In: Astrophysical Journal, Vol. 637, No. 1 II, 20.01.2006.

Research output: Contribution to journalArticle

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T2 - A black hole-neutron star merger or a naked GRB

AU - Page, K. L.

AU - King, A. R.

AU - Levan, A. J.

AU - O'Brien, P. T.

AU - Osborne, J. P.

AU - Barthelmy, S. D.

AU - Beardmore, A. P.

AU - Burrows, David Nelson

AU - Campana, S.

AU - Gehrels, N.

AU - Graham, J.

AU - Goad, M. R.

AU - Godet, O.

AU - Kaneko, Y.

AU - Kennea, Jamie A.

AU - Markwardt, C. B.

AU - Reichart, D. E.

AU - Sakamoto, T.

AU - Tanvir, N. R.

PY - 2006/1/20

Y1 - 2006/1/20

N2 - GRB 050911, discovered by the Swift Burst Alert Telescope, was not seen 4.6 hr later by the Swift X-ray Telescope, making it one of the very few X-ray nondetections of a gamma-ray burst (GRB) afterglow at early times. The γ-ray light curve shows at least three peaks, the first two of which (∼To - 0.8 and To + 0.2 s, where To is the trigger time) were short, each lasting 0.5 s. This was followed by later emission 10-20 s postburst. The upper limit on the unabsorbed X-ray flux was 1.7 × 10-14 ergs cm-2 s-1 (integrating 46 ks of data taken between September 11 and 18), indicating that the decay must have been rapid. All but one of the long bursts detected by Swift were above this limit at ∼4.6 hr, whereas the afterglows of short bursts became undetectable more rapidly. Deep observations with Gemini also revealed no optical afterglow 12 hr after the burst, down to r = 24.0 (5 σ limit). We speculate that GRB 050911 may have been formed through a compact object (black hole-neutron star) merger, with the later outbursts due to a longer disk lifetime linked to a large mass ratio between the merging objects. Alternatively, the burst may have occurred in a low-density environment, leading to a weak, or nonexistent, forward shock - the so-called "naked GRB" model.

AB - GRB 050911, discovered by the Swift Burst Alert Telescope, was not seen 4.6 hr later by the Swift X-ray Telescope, making it one of the very few X-ray nondetections of a gamma-ray burst (GRB) afterglow at early times. The γ-ray light curve shows at least three peaks, the first two of which (∼To - 0.8 and To + 0.2 s, where To is the trigger time) were short, each lasting 0.5 s. This was followed by later emission 10-20 s postburst. The upper limit on the unabsorbed X-ray flux was 1.7 × 10-14 ergs cm-2 s-1 (integrating 46 ks of data taken between September 11 and 18), indicating that the decay must have been rapid. All but one of the long bursts detected by Swift were above this limit at ∼4.6 hr, whereas the afterglows of short bursts became undetectable more rapidly. Deep observations with Gemini also revealed no optical afterglow 12 hr after the burst, down to r = 24.0 (5 σ limit). We speculate that GRB 050911 may have been formed through a compact object (black hole-neutron star) merger, with the later outbursts due to a longer disk lifetime linked to a large mass ratio between the merging objects. Alternatively, the burst may have occurred in a low-density environment, leading to a weak, or nonexistent, forward shock - the so-called "naked GRB" model.

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Page KL, King AR, Levan AJ, O'Brien PT, Osborne JP, Barthelmy SD et al. GRB 050911: A black hole-neutron star merger or a naked GRB. Astrophysical Journal. 2006 Jan 20;637(1 II). https://doi.org/10.1086/500430