OK.

So on behalf of the 6T team, I would

like to present you some details about the 6T implementation

of the Athena WFI instrument, for which we will perform

some simulations in the next practical sessions.

So Athena, the Advanced Telescope for High-Energy

Astrophysics, is an X-ray observatory mission

selected by ESA as the second L-class mission

within the Cosmic Vision Program and will

be launched in the early 2030s.

And Athena will address fundamental questions

like, how does ordinary matter assemble

into the large-scale structures that we see today,

and how do black holes grow and shape the universe?

And for this, Athena will be equipped with a 12-meter focal

length telescope with a mirror that's

based on silicon poor-optics technology.

And this mirror can then focus X-rays

onto either one of two focal plane instruments, the right

field imager and the X-ray integral field unit.

The WFI enables imaging and spectroscopy

over a large field of view, about 40 times 40 arc minutes,

with an energy resolution of 170 electron volts at 7 keV.

And the X-ray view provides spatially-resolved high

resolution spectroscopy with a field of view

of 5 arc minutes and an energy resolution of 2.5 electron

volts up to 7 keV.

And in this talk, I would like to focus on the WFI instrument.

So the WFI combines two sensors, a large detector array that's

divided into four quadrants and a separate smaller fast

detector that's optimized to observe

the brightest sources and which is also mounted,

defocused by default. The WFI uses sensors

based on depleted P-channel field effect transistors,

DEPFET, active pixel technology, which

have an energy resolution of 170 electron volts at 7 keV.

And the small fast detector provides high count rate

capabilities up to 10 KREB.

And here is an example simulation

of the WFI of the galactic center.

And for comparison, also an image

of an X-ray view simulation of the central region, which

also illustrates the different field of views of the two

instruments nicely.

And here's another example of the Chandra DEEPFIELD south,

which we will also recreate in the next practical session.

And you can also see the gaps between the four chips here,

which can be filled by an appropriate dithering pattern

during the observation, as shown here.

And this is also something that we