The Swift X-Ray Telescope

Burrows, D. N.; Hill, J. E.; Nousek, J. A.; Wells, A.; Chincarini, G.; Abbey, A. F.; Beardmore, A. P.; Bosworth, J.; Bräuninger, H.; Burkert, Wolfgang; Campana, S.; Capalbi, M.; Chang, Weijun; Citterio, O.; Freyberg, M. J.; Giommi, P.; Hartner, Gisela; Killough, Ronnie; Kittle, B.; Klar, Robert; Mangels, C.; McMeekin, M.; Miles, Broxton J.; Moretti, A.; Mori, Koji; Morris, D.; Mukerjee, K.; Osborne, J. P.; Short, A.; Tagliaferri, G.; Tamburelli, F.; Watson, D.; Willingale, R.; Zugger, Michael E.

doi:10.1117/12.504868

Cited by 92 publications

(51 citation statements)

References 17 publications

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“…Of these 32 novae, most were monitored with both the X-ray Telescope (XRT; Burrows et al, 2005) and the UV/Optical Telescope (UVOT; Roming et al, 2005), though in some cases the UV source was too bright for conventional photometry. Table 1 lists these novae, together with their outburst times from the literature.…”

Section: Swift Observations Of Supersoft Novaementioning

confidence: 99%

Neil Gehrels Swift Observatory studies of supersoft novae

Page

Beardmore

Osborne

2020

Advances in Space Research

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The rapid response capabilities of the Neil Gehrels Swift Observatory, together with the daily planning of its observing schedule, make it an ideal mission for following novae in the X-ray and UV bands, particularly during their early phases of rapid evolution and throughout the supersoft source interval. Many novae, both classical and recurrent, have been extensively monitored by Swift throughout their supersoft phase and later decline. We collect here results from observations of novae with outbursts which occurred between the start of 2006 and the end of 2017.

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Section: Swift Observations Of Supersoft Novaementioning

confidence: 99%

Neil Gehrels Swift Observatory studies of supersoft novae

Page

Beardmore

Osborne

2020

Advances in Space Research

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“…With the promptly slewing capability, the onboard X-ray Telescope (XRT; Burrows et al 2004) catches the very early X-rays following the prompt gamma-rays. The X-ray observations led to the identification of a canonical X-ray light curve, which is composed of four successive segments, i.e., an initial steep decay segment (with a decay slope 3 α 1 > 2), a shallow decay segment (α 2 < 0.75), a normal decay (α 3 ∼ 1), and a jet-like decay segment (α 4 > 1.5) (Tagliaferri et al 2005;Zhang et al 2006;Nousek et al 2006;O'Brien et al 2006).…”

Section: Introductionmentioning

confidence: 99%

A COMPREHENSIVE ANALYSIS OFSWIFT/X-RAY TELESCOPE DATA. IV. SINGLE POWER-LAW DECAYING LIGHT CURVES VERSUS CANONICAL LIGHT CURVES AND IMPLICATIONS FOR A UNIFIED ORIGIN OF X-RAYS

Liang

Lü

Hou

et al. 2009

ApJ

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By systematically analyzing the Swift/XRT light curves detected before 2009 July, we find 19 light curves that monotonously decay as a single power law (SPL) with an index of 1 ∼ 1.7 from tens (or hundreds) of seconds to ∼10 5 s post the gamma-ray burst (GRB) trigger. They are apparently different from the canonical light curves characterized by a shallow-to-normal decay transition. We compare the observations of the prompt gamma rays and the X-rays for these two samples of GRBs (SPL vs. canonical). No statistical difference is found in the prompt gamma-ray properties for the two samples. The X-ray properties of the two samples are also similar, although the SPL sample tends to have a slightly lower neutral hydrogen absorption column for the host galaxies and a slightly larger energy release compared with the canonical sample. The SPL X-ray Telescope (XRT) light curves in the burst frame gradually merge into a conflux, and their luminosities at 10 5 s are normally distributed at log L/ergs s −1 = 45.6 ± 0.5. The normal decay segment of the canonical XRT light curves has the same feature. Similar to the normal decay segment, the SPL light curves satisfy the closure relations and therefore can be roughly explained with external shock models. In the scenario that the X-rays are the afterglows of the GRB fireball, our results indicate that the shallow decay would be due to energy injection into the fireball and the total energy budget after injection for both samples of GRBs is comparable. More intriguing, we find that a prior X-ray emission model proposed by Yamazaki is more straightforward to interpret the observed XRT data. We show that the zero times (T 0 ) of the X-rays are 10 2 -10 5 s prior to the GRB trigger for the canonical sample, and satisfy a log-normal distribution. The negligible T 0 's of the SPL sample are consistent with being the tail of T 0 distributions at low end, suggesting that the SPL sample and the canonical sample may be from a same parent sample. Referenced to T 0 , the canonical XRT light curves well trace the SPL light curves. The T 0 's of the canonical light curves in our analysis are usually much larger than the offsets of the known precursors from the main GRBs. If the prior emission hypothesis is real, the X-ray emission is better interpreted within the external shock models based on the spectral and temporal indices of the X-rays. The lack of detection of a jet-like break in most XRT light curves implies that the opening angle of the prior emission jet would be usually large.

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“…The Burst Alert Telescope (BAT, Barthelmy et al 2005) measured a fluence of (4.0 ± 0.7 × 10 −7 ) erg cm −2 , with a peak photon flux of (0.4±0.1) cm −2 s −1 (15-150 keV, 90 per cent confidence errors). The enhanced X-Ray Telescope (XRT; Burrows et al 2004) position was ra. 09h 25m 33.08s, dec. 31 • 44 24.3 , with a 90 per cent error radius of 1.7 (Evans et al 2009) 1 .…”

Section: Observations Data Reduction and Resultsmentioning

confidence: 99%

The case for a high-redshift origin of GRB 100205A

Chrimes

Levan

Stanway

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The number of long gamma-ray bursts (GRBs) known to have occurred in the distant Universe (z > 5) is small (∼15), however these events provide a powerful way of probing star formation at the onset of galaxy evolution. In this paper, we present the case for GRB 100205A being a largely overlooked high-redshift event. While initially noted as a high-z candidate, this event and its host galaxy have not been explored in detail. By combining optical and near-infrared Gemini afterglow imaging (at t < 1.3 days since burst) with deep late-time limits on host emission from the Hubble Space Telescope, we show that the most likely scenario is that GRB 100205A arose in the range 4 < z < 8. GRB 100205A is an example of a burst whose afterglow, even at ∼ 1 hour post burst, could only be identified by 8-m class IR observations, and suggests that such observations of all optically dark bursts may be necessary to significantly enhance the number of high-redshift GRBs known.

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The Swift X-Ray Telescope

Cited by 92 publications

References 17 publications

Neil Gehrels Swift Observatory studies of supersoft novae

Neil Gehrels Swift Observatory studies of supersoft novae

A COMPREHENSIVE ANALYSIS OFSWIFT/X-RAY TELESCOPE DATA. IV. SINGLE POWER-LAW DECAYING LIGHT CURVES VERSUS CANONICAL LIGHT CURVES AND IMPLICATIONS FOR A UNIFIED ORIGIN OF X-RAYS

The case for a high-redshift origin of GRB 100205A

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