I will present a brief overview of the eROSITA science program, with particular emphasis on the all-sky survey, and describe how the eROSITA X-ray data can be used to open up new discovery spaces across several areas of high-energy astrophysics.
The seven eROSITA cameras are a further development of the PN-camera on ESA's XMM-Newton satellite. The eROSITA camera concept and design are explained, and the development is described. Its key component is the silicon PN-CCD detector, which was custom-developed for the eROSITA project. The most important scientific parameters are the energy, spatial, and time resolution, as well as the...
The eROSITA ground operations comprise the areas of mission planning, telescope operation, and data reception, the operation of the data processing pipeline, and the creation of tools for data access and interactive data analysis. All these activities take place at and are the responsibility of MPE.
Since its launch, eROSITA spent almost 1,000 days in nominal operations. During this time, the...
We will guide the attendees through measuring the properties of clusters of galaxies. The session will focus on fitting images of clusters of galaxies with MBProj2D to obtain profiles of their physical properties, such as density and gas mass. This will include extracting images, setting up a model, fitting it, and interpreting the results. We will also cover the extraction and fitting of...
White dwarfs are the final state of stellar evolution of main-sequence stars with masses from about 0.1 to 10 solar masses. After the hydrogen-fusing period, the star expands to a red giant, and helium fuses to carbon and oxygen in its core. Depending on its mass, no further fusion is possible, and the red giant sheds its outer layers so that the core is exposed. The mass of these remnants is...
During the hands-on session, we will learn how to create spectra of point sources and diffuse emission from the X-ray photons collected by eROSITA. Then, we will extract some physical properties of white dwarfs and diffuse emission by fitting the spectra with physical models. During the session, there will be plenty of space to ask questions.
During this session, we will discuss all the facts that may undermine the correct identification of the multiwavelength counterparts to X-ray sources, such as X-ray catalog properties, ancillary data characteristics, and type of X-ray sources (Galactic, extragalactic).
