Erratum: “The<i>Swift</i>Gamma‐Ray Burst Mission” (ApJ, 611, 1005 [2004])

Gehrels, N.; Chincarini, G.; Giommi, P.; Mason, K. O.; Nousek, J. A.; Wells, A.; White, N. E.; Barthelmy, S. D.; Burrows, D. N.; Cominsky, L.; Hurley, K.; Marshall, F. E.; Mészáros, P.; Roming, P. W. A.; Angelini, L.; Barbier, L.; Belloni, T.; Boyd, Patricia T.; Campana, S.; Caraveo, P. A.; Chester, M. M.; Citterio, O.; Cline, T. L.; Cropper, Mark; Cummings, J. R.; Dean, Anthony J.; Feigelson, E. D.; Fenimore, E. E.; Frail, D. A.; Fruchter, A. S.; Garmire, G. P.; Gendreau, Keith C.; Ghisellini, G.; Greiner, J.; Hill, J. E.; Hunsberger, S.; Krimm, H. A.; Kulkarni, S. R.; Kumar, Parveen; Lebrun, F.; Lloyd-Ronning, Nicole M.; Markwardt, C. B.; Mattson, B. J.; Mushotzky, R. F.; Norris, J. P.; Paczyński, B.; Palmer, D. M.; Park, H.-S.; Parsons, A.; Paul, Jacques; Rees, M. J.; Reynolds, C. S.; Rhoads, James E.; Sasseen, T.; Schaefer, Bradley E.; Short, Alexander T.; Smale, A. P.; Smith, I. A.; Stella, L.; Still, M.; Tagliaferri, G.; Takahashi, T.; Tashiro, M.; Townsley, Leisa K.; Tueller, J.; Turner, Martin; Vietri, M.; Voges, W.; Ward, Michael J.; Willingale, R.; Zerbi, F. M.; Zhang, W. W.

doi:10.1086/427409

Cited by 46 publications

(37 citation statements)

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“…The Swift satellite (Gehrels et al 2005) observed the location of iPTF17cw on two epochs, beginning at 13:48 UT on 2017 January 13, and 00:35 UT on 2017 January 18. These observations were obtained as part of our approved target of opportunity program ( Table 4).…”

Section: X-ray Observationsmentioning

confidence: 99%

iPTF17cw: An Engine-driven Supernova Candidate Discovered Independent of a Gamma-Ray Trigger

Corsi

Cenko

Kasliwal

et al. 2017

ApJ

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We present the discovery, classification, and radio-to-X-ray follow-up observations of iPTF17cw, a broad-lined (BL) type Ic supernova (SN) discovered by the intermediate Palomar Transient Factory (iPTF). Although it is unrelated to the gravitational wave trigger, this SN was discovered as a happy by-product of the extensive observational campaign dedicated to the follow-up of Advanced LIGO event GW 170104. The spectroscopic properties and inferred peak bolometric luminosity of iPTF17cw are most similar to the gamma-ray-burst (GRB)-associated SN, SN 1998bw, while the shape of the r-band light curve is most similar to that of the relativistic SN, SN 2009bb. Karl G. Jansky Very Large Array (VLA) observations of the iPTF17cw field reveal a radio counterpart ≈10 times less luminous than SN 1998bw, and with a peak radio luminosity comparable to that of SN 2006aj/ GRB 060218 and SN 2010bh/GRB 100316D. Our radio observations of iPTF17cw imply a relativistically expanding outflow. However, further late-time observations with the VLA in its most extended configuration are needed to confirm fading of the iPTF17cw radio counterpart at all frequencies. X-ray observations carried out with Chandra reveal the presence of an X-ray counterpart with a luminosity similar to that of SN 2010bh/ GRB 100316D. Searching the Fermi catalog for possible γ-rays reveals that GRB 161228B is spatially and temporally compatible with iPTF17cw. The similarity to SN 1998bw and SN 2009bb, the radio and X-ray detections, and the potential association with GRB 161228B all point to iPTF17cw being a new candidate member of the rare sample of optically discovered engine-driven BL-Ic SNe associated with relativistic ejecta.

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Section: X-ray Observationsmentioning

confidence: 99%

iPTF17cw: An Engine-driven Supernova Candidate Discovered Independent of a Gamma-Ray Trigger

Corsi

Cenko

Kasliwal

et al. 2017

ApJ

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“…NASA's Swift satellite (Gehrels et al 2004(Gehrels et al , 2005 was launched as a Medium Explorer mission in 2004. Its scientific payload consists of the Burst Alert Telescope (BAT, Barthelmy et al 2005), the X-ray Telescope (XRT, Burrows et al 2005), and the Ultraviolet/Optical Telescope (UVOT, Roming et al 2005).…”

Section: Swiftmentioning

confidence: 99%

Looking at A 0535+26 at low luminosities with NuSTAR

Ballhausen

Pottschmidt

Fürst

et al. 2017

A&A

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We report on two NuSTAR observations of the high-mass X-ray binary A 0535+26 taken toward the end of its normal 2015 outburst at very low 3-50 keV luminosities of ∼1.4 × 10 36 erg s −1 and ∼5 × 10 35 erg s −1 , which are complemented by nine Swift observations. The data clearly confirm indications seen in earlier data that the source's spectral shape softens as it becomes fainter. The smooth, exponential rollover at high energies present in the first observation evolves to a much more abrupt steepening of the spectrum at 20-30 keV. The continuum evolution can be well described with emission from a magnetized accretion column, modeled using the compmag model modified by an additional Gaussian emission component for the fainter observation. Between the two observations, the optical depth changes from 0.75 ± 0.04 to 0.56−0.04 , the electron temperature remains constant, and there is an indication that the column decreases in radius. Since the energy resolved pulse profiles remain virtually unchanged in shape between the two observations, the emission properties of the accretion column, however, reflect the same accretion regime. This conclusion is also confirmed by our result that the energy of the cyclotron resonant scattering feature (CRSF) at ∼45 keV is independent of the luminosity, implying that the magnetic field in the region in which the observed radiation is produced is the same in both observations. Finally, we also constrain the evolution of the continuum parameters with rotational phase of the neutron star. The width of the CRSF could only be constrained for the brighter observation. Based on Monte-Carlo simulations of CRSF formation in single accretion columns, its pulse phase dependence supports a simplified fan beam emission pattern. The evolution of the CRSF width is very similar to that of the CRSF depth, which is, however, in disagreement with expectations.

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“…The detection of the high-flux state at VHE by VERITAS triggered X-ray and UV observations by the Swift satellite (Gehrels et al 2005), which observed 1ES 1727+502 on May 7 and May 8, 2013 (MJD 56419 and 56420) for a total live time of 6.8 ks. The X-Ray Telescope (XRT, Burrows et al 2005) performed observations in windowed-timing mode, where only the 200 central columns of the detector are read, improving the time resolution of the instrument (see Cusumano et al 2012).…”

Section: Swift-xrtmentioning

confidence: 99%

VERITAS detection of gamma-ray flaring activity from the BL Lac object 1ES1727+502 during bright moonlight observations

Cerruti¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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During moonlit nights, observations with ground-based Cherenkov telescopes at very high energies (VHE, E > 100 GeV) are constrained since the photomultiplier tubes (PMTs) in the telescope camera are extremely sensitive to the background moonlight. Observations with the VERITAS telescopes in the standard configuration are performed only with a moon illumination less than 35% of full moon. Since 2012, the VERITAS collaboration has implemented a new observing mode under bright moonlight, by either reducing the voltage applied to the PMTs (reduced-high-voltage configuration, RHV), or by utilizing UV-transparent filters. While these operating modes result in lower sensitivity and increased energy thresholds, the extension of the available observing time is useful for monitoring variable sources such as blazars and sources requiring spectral measurements at the highest energies. In this paper we report the detection of γ-ray flaring activity from the BL Lac object 1ES 1727+502 during RHV observations. This detection represents the first evidence of VHE variability from this blazar. The integral flux is (1.1 ± 0.2) × 10 −11 cm −2 s −1 above 250 GeV, which is about five times higher than the low-flux state. The detection triggered additional VERITAS observations during standard dark-time. Multiwavelength observations with the FLWO 48" telescope, and the Swift and Fermi satellites are presented and used to produce the first spectral energy distribution (SED) of this object during γ-ray flaring activity. The SED is then fitted with a standard synchrotron-self-Compton model, placing constraints on the properties of the emitting region and of the acceleration mechanism at the origin of the relativistic particle population in the jet.

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Erratum: “TheSwiftGamma‐Ray Burst Mission” (ApJ, 611, 1005 [2004])

Cited by 46 publications

References 0 publications

iPTF17cw: An Engine-driven Supernova Candidate Discovered Independent of a Gamma-Ray Trigger

iPTF17cw: An Engine-driven Supernova Candidate Discovered Independent of a Gamma-Ray Trigger

Looking at A 0535+26 at low luminosities with NuSTAR

VERITAS detection of gamma-ray flaring activity from the BL Lac object 1ES1727+502 during bright moonlight observations

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