Dust and gas absorption in the High Mass X-ray Binary IGR J16318−4848

• Published in: Astronomy and astrophysics (Berlin) Vol. 641; no. na; p. A65
• Main Authors: Furst, Felix, Pottschmidt, Katja, Kühnel, Matthias Bissinger né, Hell, Natalie, Psadaraki, Ioanna
• Format: Journal Article
• Language: English
• Published: Goddard Space Flight Center EDP Sciences 15.09.2020
• Subjects: Absorbers; Absorption; Astronomy; ASTRONOMY AND ASTROPHYSICS; Astrophysics; circumstellar matter; Density; Dust; Emission analysis; Emission spectra; Empirical analysis; extinction; Fluorescence; Fluxes; Gas absorption; Grain size distribution; individual x-rays; Ionization; Mathematical models; Modelling; Monte Carlo simulation; Olivine; Optical thickness; Particle size distribution; Photoionization; Radiative transfer; X ray binaries; X ray spectra; X ray stars; XMM (spacecraft)
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/202038317

Context. With an absorption column density on the order of 10(exp 24)per sq. cm, IGR J16318-4848 is one of the most extreme cases of a highly obscured High Mass X-ray Binary. Besides the overall continuum absorption, the source spectrum exhibits a strong iron and nickel fluorescence line complex at 6.4 keV. Previous empirical modeling of these features and comparison with radiative transfer simulations raised questions about the structure and covering fraction of the absorber and the profile of the fluorescence lines. Aims. We aim at a self-consistent description of the continuum absorption, the absorption edges and the fluorescent lines to constrain properties of the absorbing material, such as ionization structure and geometry. We further investigate the effects of dust absorption on the observed spectra and the possibility of fluorescent emission from dust grains. Methods. We use XMM-Newton and NuSTAR spectra to first constrain empirically the incident continuum and fluorescence lines. Next, we use XSTAR to construct a customized photoionization model where we vary the ionization parameter, column density, and covering fraction. In a third step, we model the absorption and fluorescence in a dusty olivine absorber and employ both, a simple analytical model for the fluorescent line emission and Monte Carlo radiative transfer, spectral shapes and line fluxes that are very close to the data are generated. Results. Our empirical spectral modeling is in agreement with previous works. Our second model, the single gas absorber does not describe the observational data. In particular, irrespective of the ionization state or column density of the absorber, a much higher covering fraction than previously estimated is needed to produce the strong fluorescence lines and the large continuum absorption. A dusty, spherical absorber (modeled as consisting of olivine dust, although the nature of dust cannot be constrained) is well able to produce the observed continuum absorption and edges. Conclusions. A dense, dusty absorber in the direct vicinity of the source consisting of dust offers a consistent description of both the strong continuum absorption and the strong emission features in the X-ray spectrum of IGR J16318􀀀4848. In particular, for low optical depth of individual grains the dust will contribute significantly to the fluorescent emission, which is the case for typical densities and grain size distribution models.