Cassiopeia A (Cas A) is the youngest known galactic core-collapse supernova remnant (SNR) and is perhaps the best-studied SNR in X-rays. Cas A was observed at two different locations by XRISM, the X-Ray Imaging and Spectroscopy Mission, for more than a total of 350 ks. This rich dataset has revealed unprecedented details in elemental abundances, their dynamics, and plasma properties. In this...
We present an in-house developed tool for synthesizing high-resolution thermal X-ray spectra from three-dimensional magneto-hydrodynamic (MHD) simulations of supernova remnants (SNR). Our approach translates directly the physical quantities predicted by MHD models, such as temperature, density, ionization timescale, and velocity fields, into observable spectra for current and future...
Since the advent of high-resolution X-ray imaging with modern CCD detectors, multi-band images of bright supernova remnants (SNRs) have stunned us with their beauty. While the spectral properties of such SNRs have been studied in detail with complex models, the spatial morphologies are frequently described qualitatively, but not quantified.
In this talk, I will discuss the potential of...
I report on preliminary results from a collaborative project between the Supernova Remnants and Cosmic Ray Group, the Observatory of Complex Systems Group, and the Quantum Theory Group at the University of Palermo.
By adopting different dendrogram-based techniques, we developed a tool to quantitatively measure the similarities among different narrow-band images of a supernova remnant and of...
The Cluster HEritage project with XMM-Newton - Mass Assembly and Thermodynamics at the Endpoint of structure formation (CHEX-MATE) is a multi-year Heritage program focused on studying 118 galaxy clusters, identified as the ultimate products of structure formation. This extensive analysis, encompassing over 6 Msec of XMM-Newton data, recently concluded with the application of a...
Ever since X-ray observatories have started to probe the Universe, one of the objectives has been to classify the observed sources. Indeed, the X-ray sky is extremely diverse, with emission coming from stellar atmospheres, to super-massive black holes, up to galaxy clusters. It remains challenging to conduct extensive studies of all the detected sources due to the considerable volume of data...
In a simple cold dark matter scenario, galaxy clusters are formed by hierarchical gravitational collapse of the dominant dark matter component. To the first order, this process is self-similar and scale-free. However, it is known that the thermodynamic properties of the hot gas deviate from those predicted by simple self-similar models, presumably due to the influence of non-gravitational...
We present a simulation framework developed to evaluate the capability of the NewAthena mission, but easily adaptable to other missions as well, to detect and characterize diffuse X-ray emission, focusing on reproducing realistic instrument performance and consolidated X-ray analysis tools.
Synthetic observations were generated starting from map simulations, which were converted into mock...
Spectral analysis of X-ray emission from ejecta in supernova remnants (SNRs) is hampered by the low spectral resolution of CCD detectors, which typically creates a degeneracy between the best-fit values of chemical abundances and the plasma emission measure. The combined contribution of shocked ambient medium and ejecta to the emerging X-ray emission further complicates the determination of...
Fitting models to X-ray spectra is a fundamental technique to infer information about the hot and energetic universe. Finding credible parameter ranges for a given spectral model and dataset(s) however is not a simple task. In this workshop, we will first present the recommended practices for fitting models to X-ray spectra, including an overview of the instrumentation response, the linear...
SUSHI is a new algorithm for fitting the spatial distribution of spectral parameters within extended X-ray emitting structures. In this talk, I will present two examples of the implementation of SUSHI to pulsar wind nebulae and AGN jets. Not only does SUSHI identify trends that were previously hidden, it also defines regions of particular interest. In this way, it allows us to investigate the...
