2018
DOI: 10.3847/1538-4357/aace60
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NICER and Fermi GBM Observations of the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124

Abstract: Swift J0243.6+6124 is a newly discovered Galactic Be/X-ray binary, revealed in late September 2017 in a giant outburst with a peak luminosity of 2 × 10 39 (d/7 kpc) 2 erg s −1 (0.

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Cited by 123 publications
(124 citation statements)
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“…The PF of > 50 % was detected at > ∼ 1 keV in NGC300 ULX1 and two observations of Swift J0243.6+6124 showed the PF of ≫ 50 %. In addition, it was reported that the PF depends on the photon energy (see e.g., Bachetti et al 2014;Wilson-Hodge et al 2018). The energy dependence of the PF and the high PF (≫ 50 %) might be resolved by the thermal and bulk Comptonization, which are not taken into account in the present study.…”
Section: Conclusion and Discussionmentioning
confidence: 75%
See 1 more Smart Citation
“…The PF of > 50 % was detected at > ∼ 1 keV in NGC300 ULX1 and two observations of Swift J0243.6+6124 showed the PF of ≫ 50 %. In addition, it was reported that the PF depends on the photon energy (see e.g., Bachetti et al 2014;Wilson-Hodge et al 2018). The energy dependence of the PF and the high PF (≫ 50 %) might be resolved by the thermal and bulk Comptonization, which are not taken into account in the present study.…”
Section: Conclusion and Discussionmentioning
confidence: 75%
“…This implies that the magnetic axis is not drastically misaligned with the rotation axis and that observer's viewing angle is relatively small in most ULXPs, since the sinusoidal pulse has been detected (see e.g., Bachetti et al 2014;Fürst et al 2016;Israel et al 2017aIsrael et al , 2017b). An exceptional object is Swift J0243.6+6124 of which the pulse has a secondary peak (Wilson-Hodge et al 2018). Thus, θ obs > 70 • or θB > 70 • might be realized in this object.…”
Section: Conclusion and Discussionmentioning
confidence: 97%
“…The expected counts λ j arise from folding a model for the jth source through the instrument response to predict the counts in bin i, including the effects of varying exposure. If these bins are taken to be so small that n i ∈ (0, 1), this becomes the "unbinned" likelihood (Tompkins 1999),…”
Section: General Formalismmentioning
confidence: 99%
“…Generally, the power spectrum is unchanged in regions where the window function is minimal (exposure variations washed out), but substantially improved near problematic frequencies. This approach is critical in the analysis of strongly pulsed sources; see, e.g., the analysis of an ultraluminous X-ray pulsar (Wilson-Hodge et al 2018).…”
Section: Pulse Profilesmentioning
confidence: 99%
“…The ULX population consists of several hundreds sources in nearby galaxies (e.g. , and they are usually extragalactic (although see Wilson-Hodge et al 2018), off-nuclear and point-like objects. Nowadays, they are believed to be mostly stellar mass BHs or neutron stars (NSs) accreting well above the Eddington limit rather than sub-Eddington accreting intermediate mass BHs (10 2 − 10 5 M ; e.g.…”
Section: Introductionmentioning
confidence: 99%