Churazov, E.E.ChurazovKhabibullin, I.I.KhabibullinPONTI, GABRIELEGABRIELEPONTISunyaev, R.R.Sunyaev2020-12-302020-12-3020170035-8711http://hdl.handle.net/20.500.12386/29373We use a model of the molecular gas distribution within ∼100 pc from the centre of the Milky Way (Kruijssen, Dale & Longmore) to simulate time evolution and polarization properties of the reflected X-ray emission, associated with the past outbursts from Sgr A*. While this model is too simple to describe the complexity of the true gas distribution, it illustrates the importance and power of long-term observations of the reflected emission. We show that the variable part of X-ray emission observed by Chandra and XMM-Newton from prominent molecular clouds is well described by a pure reflection model, providing strong support of the reflection scenario. While the identification of Sgr A* as a primary source for this reflected emission is already a very appealing hypothesis, a decisive test of this model can be provided by future X-ray polarimetric observations, which will allow placing constraints on the location of the primary source. In addition, X-ray polarimeters (like, e.g. XIPE) have sufficient sensitivity to constrain the line-of-sight positions of molecular complexes, removing major uncertainty in the model.STAMPAenArticle10.1093/mnras/stx4432-s2.0-85017225677000398419200013https://academic.oup.com/mnras/article/468/1/165/30454012017MNRAS.468..165CFIS/05 - ASTRONOMIA E ASTROFISICA