Recovering<i>Swift</i>-XRT energy resolution through CCD charge trap mapping

Pagani, C.; Beardmore, A. P.; Abbey, A. F.; Mountford, C. J.; Osborne, J. P.; Capalbi, M.; Perri, M.; Angelini, L.; Burrows, D. N.; Campana, S.; Cusumano, G.; Evans, P. A.; Kennea, J. A.; Moretti, A.; Page, K. L.; Starling, R. L. C.

doi:10.1051/0004-6361/201117660

Cited by 16 publications

(20 citation statements)

References 26 publications

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“…However, these appear to be due to a calibration artifact unrecognized at the time, namely charge trapping (Pagani et al 2011). The spectral fits to XRT data shown in Figures 2 for BFF and 3 for F2 do not show any evidence of excess emission near 6.4 keV.…”

Section: Discussionmentioning

confidence: 82%

A VERY BRIGHT, VERY HOT, AND VERY LONG FLARING EVENT FROM THE M DWARF BINARY SYSTEM DG CVn

Osten¹,

Kowalski

Drake³

et al. 2016

ApJ

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On 2014 April 23, the Swift satellite responded to a hard X-ray transient detected by its Burst Alert Telescope, which turned out to be a stellar flare from a nearby, young M dwarf binary DGCVn. We utilize observations at X-ray, UV, optical, and radio wavelengths to infer the properties of two large flares. The X-ray spectrum of the primary outburst can be described over the 0.3-100 keV bandpass by either a single very high-temperature plasma or a nonthermal thick-target bremsstrahlung model, and we rule out the nonthermal model based on energetic grounds. The temperatures were the highest seen spectroscopically in a stellar flare, at T X of 290 MK. The first event was followed by a comparably energetic event almost a day later. We constrain the photospheric area involved in each of the two flares to be >10 20 cm 2 , and find evidence from flux ratios in the second event of contributions to the white light flare emission in addition to the usual hot, T∼10 4 K blackbody emission seen in the impulsive phase of flares. The radiated energy in X-rays and white light reveal these events to be the two most energetic X-ray flares observed from an M dwarf, with X-ray radiated energies in the 0.3-10 keV bandpass of 4×10 35 and 9×10 35 erg, and optical flare energies at E V of 2.8×10 34 and 5.2×10 34 erg, respectively. The results presented here should be integrated into updated modeling of the astrophysical impact of large stellar flares on close-in exoplanetary atmospheres.

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Section: Discussionmentioning

confidence: 82%

A VERY BRIGHT, VERY HOT, AND VERY LONG FLARING EVENT FROM THE M DWARF BINARY SYSTEM DG CVn

Osten¹,

Kowalski

Drake³

et al. 2016

ApJ

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“…Soon afterwards Pagani et al (2011) found the position of the new source at RA (J2000): 18h 22m 18.00s Dec (J2000): -16d 04 ′ 26.8 ′′ , with 1.8 arcsec radius of uncertainty (90% confidence). Subsequently, the source was followed by virtually all the current generation of Xray satellites.…”

Section: Swift J18223-1606mentioning

confidence: 98%

The outburst decay of the low magnetic field magnetar SWIFT J1822.3−1606: phase-resolved analysis and evidence for a variable cyclotron feature

Castillo

Israel

Tiengo

et al. 2016

Mon. Not. R. Astron. Soc.

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“…= −16 • 04 26. 8 (Pagani et al 2011) and the best available spacecraft attitude file. Events were then reduced to the solar-system barycenter using the above source position.…”

Section: Swift Observationsmentioning

confidence: 99%

The Long-Term Post-Outburst Spin Down and Flux Relaxation of Magnetar Swift J1822.3–1606

Scholz

Kaspi

Cumming

2014

ApJ

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The magnetar Swift J1822.3−1606 entered an outburst phase in 2011 July. Previous X-ray studies of its post-outburst rotational evolution yielded inconsistent measurements of the spin-inferred magnetic field. Here we present the timing behavior and flux relaxation from over two years of Swift, RXTE, and Chandra observations following the outburst. We find that the ambiguity in previous timing solutions was due to enhanced spin down that resembles an exponential recovery following a glitch at the outburst onset. After fitting out the effects of the recovery, we measure a long-term spin-down rate ofν = (−3.0 ± 0.3) × 10 −16 s −2 which implies a dipolar magnetic field of 1.35 × 10 13 G, lower than all previous estimates for this source. We also consider the post-outburst flux evolution, and fit it with both empirical and crustal cooling models. We discuss the flux relaxation in the context of both crustal cooling and magnetospheric relaxation models.

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RecoveringSwift-XRT energy resolution through CCD charge trap mapping

Cited by 16 publications

References 26 publications

A VERY BRIGHT, VERY HOT, AND VERY LONG FLARING EVENT FROM THE M DWARF BINARY SYSTEM DG CVn

A VERY BRIGHT, VERY HOT, AND VERY LONG FLARING EVENT FROM THE M DWARF BINARY SYSTEM DG CVn

The outburst decay of the low magnetic field magnetar SWIFT J1822.3−1606: phase-resolved analysis and evidence for a variable cyclotron feature

The Long-Term Post-Outburst Spin Down and Flux Relaxation of Magnetar Swift J1822.3–1606

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