The First<i>Swift</i>X‐Ray Flash: The Faint Afterglow of XRF 050215B

Levan, A. J.; Osborne, J. P.; Tanvir, N. R.; Page, K. L.; Rol, E.; Zhang, Bing; Goad, M. R.; O’Brien, P. T.; Priddey, R.; Bersier, D.; Burrows, D. N.; Chapman, R. W.; Fruchter, A. S.; Giommi, P.; Gehrels, N.; Hughes, Mark; Pak, S.; Simpson, Chris; Tagliaferri, G.; Vardoulaki, E.

doi:10.1086/506018

Cited by 12 publications

(12 citation statements)

References 67 publications

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“…At K ≈ 19.7 within an hour of the burst, this is considerably fainter than previous afterglow detections in NIR estimated at the same epoch. For example, the faint, red afterglow of GRB 050215B was also only seen in K , but would have been K ∼ 19 at 1 h based on extrapolating back the later time decay curve (Levan et al 2006b).…”

Section: Observationsmentioning

confidence: 99%

“…Note that error bars have been omitted for clarity. (Data taken from Blake et al 2005;Durig, McLarty & Manning 2005;Guidorzi et al 2005;Rykoff et al 2005;Sharapov et al 2005;Cenko & Fox 2006;Cenko et al 2006;Haislip et al 2006;Jakobsson et al 2006a;Levan et al 2006b;Oates et al 2006;Pandey et al 2006;Quimby et al 2006;Watson et al 2006;Yost et al 2006;Evans et al 2007;Guidorzi et al 2007;Huang et al 2007;Kann et al 2007;Rol, Tanvir & Kerr 2007). data can be accommodated with an overall shallower spectral slope. We note that a cooling break between the X-ray and optical/NIR should also produce a difference in their temporal decay slopes, but our constraint on α in the K band is not tight enough to make a meaningful test.…”

Section: The High-extinction Scenariomentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

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The extreme, red afterglow of GRB 060923A: distance or dust?

Tanvir

Levan

Rol

et al. 2008

Monthly Notices of the Royal Astronomical Society

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Gamma‐ray bursts (GRBs) are powerful probes of the early Universe, but locating and identifying very distant GRBs remain challenging. We report here the discovery of the K‐band afterglow of Swift GRB 060923A, imaged within the first hour post‐burst, and the faintest so far found. It was not detected in any bluer bands to deep limits, making it a candidate very high‐z burst (z≳ 11). However, our later‐time optical imaging and spectroscopy reveal a faint galaxy coincident with the GRB position which, if it is the host, implies a more moderate redshift (most likely z≲ 2.8) and therefore that dust is the likely cause of the very red‐afterglow colour. This being the case, it is one of the few instances so far found of a GRB afterglow with high‐dust extinction.

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Section: Observationsmentioning

confidence: 99%

Section: The High-extinction Scenariomentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

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The extreme, red afterglow of GRB 060923A: distance or dust?

Tanvir

Levan

Rol

et al. 2008

Monthly Notices of the Royal Astronomical Society

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“…Heise et al 2001;Kippen et al 2003;Sakamoto et al 2005); ii) host galaxy properties (e.g. Bloom et al 2003); iii) broadband afterglows as observed by Swift (Gehrels et al 2004 − XRFs 050215B, Levan et al 2006a;050315, Vaughan et al 2006;050406, Romano et al 2006; 050416A, Mangano et al 2006; 050714B, Levan et al 2006b;060218, Campana et al 2006b). The association of XRFs with supernovae of type Ib/c (e.g.…”

Section: Introductionmentioning

confidence: 99%

GRB 050822: detailed analysis of an XRF observed bySwift

Godet

Page

Osborne

et al. 2007

A&A

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We report on the temporal and spectral characteristics of the early X-ray emission from the GRB 050822 as observed by Swift. This burst is likely to be an XRF showing major X-ray flares in its XRT light-curve. The quality of the data allows a detailed spectral analysis of the early afterglow in the X-ray band. During the X-ray flares, a positive correlation between the count rate and the spectral hardness (i.e. the higher the count rate, the harder the spectrum) is clearly seen for the X-ray flares. This behaviour, similar to that seen for Gamma-ray pulses, indicates that the energy peak of the spectrum is in the XRT energy band and it moves towards lower energies with time. We show evidence for the possible detection of the emergence of the forward-shock emission, produced at a radius larger than 4 × 10 16 cm in the case of a CBM afterglow model (a formation region clearly different from that producing the prompt emission). Finally, we show that the null detection of a jet break up to T 0 + 4 × 10 6 s in the X-ray light curve of this XRF can be understood: i) if the jet seen on-axis is uniform with a large opening angle (θ > 20• ); or ii) if the jet is a structured Gaussian-like jet with the line-of-sight outside the bright Gaussian core.

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“…The spectrum was on the X-ray flasher end of the distribution of GRB spectra, which may or may not be an orientation effect (Granut et al 2005). SWIFT caught its very first X-ray flasher just as the year ran out (Levan et al 2006), and we may know more about these in a year or two.…”

Section: Gamma Ray Burstersmentioning

confidence: 99%

Astrophysics in 2006

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The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the universe) and others of which there are always many, like meteors and molecules, black holes and binaries.Comment: 244 pages, no figure

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The FirstSwiftX‐Ray Flash: The Faint Afterglow of XRF 050215B

Cited by 12 publications

References 67 publications

The extreme, red afterglow of GRB 060923A: distance or dust?

The extreme, red afterglow of GRB 060923A: distance or dust?

GRB 050822: detailed analysis of an XRF observed bySwift

Astrophysics in 2006

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