We report on the Swift observations of the candidate supergiant fast X-ray transient (SFXT) IGR J16418-4532, which has an orbital period of ~3.7 d. Our monitoring, for a total of ~43 ks, spans over three orbits and represents the most intense and complete sampling along the orbital period of the light curve of this source. If one assumes a circular orbit, the X-ray emission from this source can be explained by accretion from a spherically symmetric clumpy wind from a blue supergiant, composed of clumps with different masses, ranging from ~5x10^16 g to 10^21g.
@article{arxiv.1209.5872,
title = {Swift monitoring of IGR J16418-4532},
author = {P. Esposito and P. Romano and V. Mangano and L. Ducci and S. Vercellone},
journal= {arXiv preprint arXiv:1209.5872},
year = {2015}
}
Comments
4 pages; Proceedings, 5th International Symposium on High-Energy Gamma-Ray Astronomy, (Gamma2012) Heidelberg, Germany, July 9-13th, 2012