A Redshift Determination for XRF 020903: First Spectroscopic Observations of an X‐Ray Flash

Söderberg, A. M.; Kulkarni, S. R.; Berger, E.; Fox, D. B.; Price, P. A.; Yost, S. A.; Hunt, Matthew P.; Frail, D. A.; Walker, R. C.; Hamuy, M.; Shectman, Stephen; Halpern, J. P.; Mirabal, N.

doi:10.1086/383082

Cited by 111 publications

(128 citation statements)

References 19 publications

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“…As observations accumulate, it is becoming clear that these two classes of phenomena share many properties, and both have afterglows with similar characteristics . This is a clue that both types of events may have a common origin and is supported by recent evidence that some XRFs are associated with supernovae (Soderberg et al 2004;Bersier et al 2005;Fynbo et al 2004). …”

Section: ) or As An "X-ray Rich Grb" (Xrr)supporting

confidence: 67%

“…Such a late break is not unexpected for an XRF. The few XRFs with known redshift (Soderberg et al 2004;Bersier et al 2005;Fynbo et al 2004) have a very low isotropic-energy release, and this may be at least in part accommodated if they have very wide jets. This picture is consistent with the result found by Frail et al (2001; see also Ghirlanda et al 2004), who found that low-energy GRBs tend to have wider opening angles.…”

Section: The X-ray Afterglow Light Curvementioning

confidence: 99%

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X-ray flare in XRF 050406: evidence for prolonged engine activity

Romano

Moretti

Banat

et al. 2006

AIP Conference Proceedings

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Abstract. We present observations of XRF 050406, the first burst detected by Swift showing a flare in its X-ray light curve. During this flare, which peaks at t peak ∼ 210 s after the BAT trigger, a flux variation of δF/F ∼ 6 in a very short time δt/t peak ≪ 1 was observed. Its measured fluence in the 0.2-10 keV band was ∼ 1.4 × 10 −8 erg cm −2 , which corresponds to 1-15% of the prompt fluence. We present indications of spectral variations during the flare. We argue that the producing mechanism is late internal shocks, which implies that the central engine is still active at 210 s, though with a reduced power with respect to the prompt emission. The X-ray light curve flattens to a very shallow slope with decay index of ∼ 0.5 after ∼ 4400 s, which also supports continued central engine activity at late times. This burst is classified as an X-ray flash, with a relatively low fluence (∼ 10 −7 erg cm −2 in the 15-350 keV band, E iso ∼ 10 51 erg), a soft spectrum (photon index 2.65), no significant flux above ∼ 50 keV and a peak energy E p < 15 keV. XRF 050406 is one of the first examples of a well-studied X-ray light curve of an XRF. We show that the main afterglow characteristics are qualitatively similar to those of normal GRBs. In particular, X-ray flares superimposed on a power-law light curve have now been seen in both XRFs and GRBs. This indicates that a similar mechanism may be at work for both kinds of events.

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Section: ) or As An "X-ray Rich Grb" (Xrr)supporting

confidence: 67%

Section: The X-ray Afterglow Light Curvementioning

confidence: 99%

X-ray flare in XRF 050406: evidence for prolonged engine activity

Romano

Moretti

Banat

et al. 2006

AIP Conference Proceedings

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“…Images are oriented with North up and East to the left, and the physical length scale for a one-arcsecond angular distance is indicated in each panel (except for GRB 051227); arrows point to the location of the burst where this is known to ∼pixel precision. Individual burst notes: GRB 030329 was the first classical long GRB to be associated with a well-observed spectroscopic supernova ; XRF 020903 was the first X-ray Flash event to yield a redshift measurement Soderberg et al (2004); GRB 050709 was the first short burst with optical afterglowindicated by the arrow -detected Fox et al (2005), Hjorth et al (2005b); GRB 050509B was the first short burst with detected afterglow ) GRB 051227 has a faint candidate host, of unknown redshift probably greater than 1, visible at the optical afterglow location; the spiral galaxy to the east has redshift z = 0.714 Foley et al (2005). Long-burst host images from Wainwright et al (2007); short-burst host images from Fox et al (2005) and this work.…”

Section: Host Galaxies Of Long Burstsmentioning

confidence: 99%

Gamma-Ray Bursts in theSwiftEra

Gehrels

Ramírez-Ruiz

Fox

2009

Annu. Rev. Astron. Astrophys.

585

474

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With its rapid-response capability and multiwavelength complement of instruments, the Swift satellite has transformed our physical understanding of γ-ray bursts (GRBs). Providing highquality observations of hundreds of bursts, and facilitating a wide range of follow-up observations within seconds of each event, Swift has revealed an unforeseen richness in observed burst properties, shed light on the nature of short-duration bursts, and helped realize the promise of GRBs as probes of the processes and environments of star formation out to the earliest cosmic epochs. These advances have opened new perspectives on the nature and properties of burst central engines, interactions with the burst environment from microparsec to gigaparsec scales, and the possibilities for nonphotonic signatures. Our understanding of these extreme cosmic sources has thus advanced substantially; yet, more than 40 years after their discovery, GRBs continue to present major challenges on both observational and theoretical fronts.

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“…The last of these predicts that there should also be short-duration X-ray flashers. The first host identification and redshift, (Soderberg et al 2004b), supports the small z p 0.25 total energy part of these relationships. Still, how can one not love the alternative, planet-planet collision scenario of Zhang & Sigurdsson (2003)?…”

Section: Gamma-ray Burstersmentioning

confidence: 67%