 Hello, everyone. Good morning. I'm Manami Sasaki. I'm from the Schnenwald Observatory in Bamberg, which is part of the Erlang Center for Astropharticle Physics of the University of Erlang-Nürnberg. And I have the pleasure today to speak to you about our newest mission, the X-ray telescope, erosita. And yeah, this is where you see a sketch here already provided by the DLR. So let me start by showing you this. Rosa was already mentioned by Professor Hofmann. This is the X-ray sky as we have known it for quite a long time since about the 1990s. You see the entire sky here in this map. You have the galactic plane in the center in the horizontal, in the horizontal, and then in the center you have the galactic center region. And you see the emission that we saw with the Rosa telescope, which you see here, in the very soft X-ray range below 2.4 kV. And this image is in three-color presentation. So what you see is the very soft, the softest X-rays in red. Then you have in green, the medium band around 1 kV and up to 2.4 kV. Then you see the harder sources in blue. And you realize a lot of emission is absorbed along the galactic plane because X-rays are very sensitive to interstellar absorption. But then you see a lot of hard sources along the galactic plane, those are neutron stars, black holes, and bright sources like supernova remnants. And then you see a lot of emission also above and below the galactic plane in particular, which are very soft in red. And I would like to quickly go through the sources that cause these emissions, especially in the galaxy, because this is what I would like to focus on X-ray sources in our Milky Way and in the nearby galaxies. So as you know, galaxies are made of stars and many of those are very massive stars. And very massive stars have strong UV photons. So they are hot, you have strong UV photons and strong stellar winds. So each of such a massive star during its lifetime will create a bubble around it because of the strong winds. And this is one example, the nice bubble nebula seen in the optical, that's a stellar bubble. And in the diagram on the right hand side, you see a standard model for explaining such a bubble. You see that the interior is very hot and it's thin with low density and is filled with thermal hot plasma. And this is the source of X-rays. While the swept up material around it, here you see an H2 region with a shell that emits in the optical. Then if you have many of those stars, like in a stellar cluster, where you typically find stars, then the combination of these stellar winds and also the Subanova explosion in the end, we create larger structures that we call superbubbles. And we are actually located in such a larger bubble, the local bubble inside. Therefore, that's the reason why we see this reddish emission around us below the plane, above the plane, below the plane, everywhere, because this is the hot gas that surrounds us. And if a galaxy evolves, of course, these things can happen many times due to the many generations of stars that you have in a galaxy. So in principle, you will also get larger structures, which we call supergine shells. So you have a combination of many H2 regions and superbubbles. And here again, you see in blue, the optical emission and the HR5 emission and the X-ray emission that fills the interior of such a superbubble. These two images are taken from the Large Magellanic Cloud. So this is the largest nearby galaxy, our satellite galaxy. And it's one of the, in principle, the best place to study emission coming from interstellar structures like this. Then if you have these stars, they will die in a supernova, as I mentioned before. And then they will create also interesting interstellar structures, which we call the supernova remnant. Here you see examples of the remnants of the supernova that have been detected by Tijokraha, Ioannes Kepler, and another one in the same region in the sky, the Kassiopaya A supernova remnant, which are only a few hundred years old. And you see they are very bright X-ray sources. And this is because the supernova explosion produces a strong shock. And this will ionize and heat the environment. Then also the ejector that is thrown out of the stars. And in these strong shock waves, also particles are saturated. That's why they are also very interesting high energy sources. Then here I wanted to show you another example of these combinations, what we actually do if we observe something like this. There's another supernova in the Large Magellanic Cloud where you nicely see the combination of everything. So this is an optical image, so in the narrow bands of H-alpha, but also the forbidden lines of S-alpha-2 and oxygen-3 combined in three colors. And as you see, it's a large structure filled with stellar clusters and associations marked here in white. And these are the stars that are powering these structures and heating and creating this emission nebula. And as you see, you already see a difference in color here and in this main structure. And this one looks different and that's because it is a supernova remnant. And one of the stars that belong to these associations must have already exploded. And you see it also nicely as a very bright object in X-rays. So on the right hand side, you see an X-ray image taking with XMM-muton, which is currently working very good to X-ray telescope. But on the other hand, you also see that there is interior emission. And this is this hot gas that I was talking about created by the stellar winds of the stars that are inside the supernova. So if you take again like a three-color image in X-rays, you see it's very soft emission that you see in the interior and a little harder emission coming from this supernova remnant. And you also see that this outer part where you see this bright emission in optical H2 region also seems to absorb some of the X-rays because you don't see emission around here. And then there is another interesting structure that you see here. Here it's more obvious than there. There's some additional significant emission towards the north. And that's actually coinciding with the part of the H2 region where it seems to be broken. So it's not a nice circulation. And then if you compare it with the density distribution in this region by looking at the distribution of atomic hydrogen in the radio, you see there is a strong density gradient. And the position where you see this emission, this defined emission in X-ray coincides with an area in the H1 distribution where there is a hole. So in this image, white means a lot of emission, so a lot of atomic hydrogen, and black means less atomic hydrogen. So these stars have carved a region here in the distribution of gas because of their stellar winds and also supernova explosion. But since there is a density gradient, there was also some outflow in this direction, which we can see in X-rays. And these things happen a lot in the interstellar medium. And since we are sitting inside, it is difficult to observe such a thing inside our make-over. As you saw, the emission coming from the bubble around us, we only see a very diffuse emission everywhere in the sky. And in the LMC, you can study those in detail because you can look at the galactic disc. Another galaxy which is also very ideal for studying the interstellar medium is the next spiral galaxy, the closest spiral galaxy to us, the Andromeda Galaxy M31. And here you see it on the right-hand side in the optical, so you see the distribution of the star. And on the left-hand side, you see the emission only showing the extended emission in X-rays, also taking with XMMuton, we have performed a survey over the entire M31. And you see that especially in this part where we have a pronounced ring in the Andromeda nebula, we also have enhanced X-ray emission. But there's also emission filling the parts inside it, especially again bright where you have these dust strings and a lot of emission in the central region. So by looking at those emission in also nearby, other nearby galaxies, we can study the structure of the interstellar medium very well. So especially the hot phase of the interstellar medium, but comparing it with other observations like I showed you before, you will learn a lot about the structure of the interstellar medium. Now, here I wanted to show you another example, maybe most, many of you are familiar with, so this is again another region in the Large Magellanic Cloud, the Tarantula Nebula, we also call it the Cerdy Dorados region, which is a super giant H2 region. We don't have such a large region in our Milky Way, the next one would be in another nearby galaxy M33. So this is an H2 region that hosts a lot of very, very massive stars, will fly stars or stars, and the winds, the combination of those winds of those stars, they create this very large structure. And if you look at this region in your x-rays, you realize, yes, you see this, the Tarantula Nebula would be here. You see the brightest stars and stellar associations, stellar clusters inside here and also emitting x-rays in the thermal emission here. But then you also see this interesting region here on the right, which is a hard, so non-thermal x-ray source with a ring-like structure. That's the region which we call Cerdy Dorados, you see it here. And by now we know that it's a super bubble as well, but it behaves a little different than the oldest super bubbles we know. Or the other ones, as you saw, most of it show pronounced x-ray emission that comes from thermal plasma. Here again, you see the x-ray emission in three-color presentation, so everything that is blue is very hard. It's above 2 kV and below that you see a lot of thermal emission. On the right hand side, again, a three-color presentation of the optical image and in contrast the x-ray emission. And if you now take the spectra in x-rays, what you see is that in all these parts of this Cerdy Dorados, you see very dominant non-thermal emission. And how can you see that? For those that are not familiar with x-ray spectra, in this interior region where you have a lot of thermal emission, you see these bumps here in the spectra up to about 2 kV. These are non-the CCD resolution, energy resolution is not as good as, for example, in the optical. So you see them as like the emission lines of the ionized part species. So highly ionized, like oxygen, neon, magnesium, the elements that you encounter in interstellar you see as those bumps. So these are emission line features. And this is what you typically expect if you have thermal plasma at a higher temperature. But you have also additional emissions going up to higher energies. And this emission is non-thermal emission, which is shown seen as a power law. And that's what is dominating here. So you see hardly emission line features here, but you have these big bumps here that goes up to higher energies. And this is because the non-thermal emission is dominating. And here you see some signs of thermal emission, but that's not what is very bright in this, especially in this outer regions. So this super, sorry, the super bubble is known to be a very high energetic non-thermal super bubble. And it's the only one that we know of in the LMC. And the next one that we know is, again, also in M31, 33. So in the other galaxy that components the microwave. So it's very, very rare case. And if you compare that in radio, it's, of course, it's a non-thermal source. It's very bright in X, then in radio, there you see an index map in a radio. And if you look at the the spectra in X rays, you can also confirm that it is most likely synchrotron emission that we see in X rays. And if you then combine the flux that we get from X rays down to radio, we can also get an estimate for the the energy of the electrons that are accelerated in this super bubble. And we get a number of about 80 terri electron volt. And this source is also one of the first sources that have been detected in the TV with HES. So many of you know, have seen this image before. So this is the X again, the XMM image. And here you see significant detection coming from in the TVs. And there was this, of course, discussion can that be get tonic or also some hydronic emission? And what would cause such an emission? So of course, it can be that there isn't, since there is active super bubble, there was maybe a young supernova remnant and when a supernova that went off recently will have a very strong shock. And as soon as it hits the wall, it can create such non-thermal emission. But maybe also the stars that are still there, they can also provide colliding shocks, acceleration in colliding shocks. And the last thing we did in the study of this super bubble is to look at it in X rays with Chandra, which has the highest spatial resolution. So we can resolve the filaments that you see the non-thermal filaments in the outer parts and get an idea of the profile. And assuming that this is limited by the advection of the accelerated particles, we can make an estimate of the magnetic fields. And it turns out this magnetic field estimate is rather low. So the dominant emission is most likely leptonic for this case. But this is, of course, not very surprising because you have this industrial structure that is already existent. And then if there is a strong shocks that runs inside it and hits the wall, you would expect such high energy emission. Now, I've now spoken about the most prominent cases in which you can see X-ray to very high energy emission in interstellar medium. But of course, we also have other interesting sources in the galaxies that can make X-ray emission like stars like our sun due to flares and the magnetic fields will be our bright X-ray sources. And also compact objects like white dwarf, neutron stars and black codes, especially if they are young and or if they are creating material like what is illustrated here in these images. If you have a neutron star or white dwarf or a black hole that is a creating matter, a lot of energy is released and you will see it as bright, see them as bright X-ray sources. So there are a lot of interesting sources in galaxies, but of course, even more so if you go outside the galaxies. So AGMs, the nuclear regions of active galaxies are very bright X-ray sources and they are so bright you can even look at the very, very far distances. And also the galaxy clusters. Now here I use what you see is an optical image of the coma cluster. So all these white points are distant galaxies. And if you look at the same position in X-rays again with a kind of a small survey performed with XMM mutant, here this green box is the same area as what you see in the optical. You see very bright diffuser emission that fills this interior, the central region of the galaxy cluster. So the intergalactic medium is very hot and is also a hot, yeah, thin plasma. So you will see a lot of thermal emission coming from the galaxy cluster. So by looking at those AGMs in the galaxy clusters, you can also study the entire universe because these are the objects that you can use to look at as far as possible. And this is also the reason why erosita was developed. So the idea was to study the entire X-ray scale to the furthest distances, but also the nearby sources. And as we said already, no, sorry, maybe I haven't, sorry, but erosita, the telescope that I want to want to talk about is a collaboration was produced in collaboration between German and German consortium and Russia. So it's a German X-ray telescope and is now located on a Russian spacecraft, the Spectrum Röntgen Gamma, and is supposed to do the an all-sky survey in the software now up to medium X-ray band. So we want to go up, we go up to 10 kilo electron volt. And it has a rather good spatial resolution and spectral resolution, which was not the case with Rosa back then. And here you see some comparison of the graphs, so it's the effective area of the telescope average over the freedom of view. Erosita is the red line and compared with the actual currently working X-ray telescope Chandra and X-ray mutant, or also Rosa PSPC. So comparing to Rosa, which did an Oscar survey, you see you have a very strong improvement in the sensitivity. And therefore, erosita will be able to study up to 100,000 galaxy clusters, millions of AGMs. So this is like the main science driver of the erosita mission to study the entire universe, especially focusing on studies of the dark meta-dark energy. But also we also want to do galactic X-ray studies. So we will study the physics of galactic X-ray sources. And this is what the main topic of this talk actually is. And another comparison between erosita and the other telescopes. So with X-ray mutant or Chandra, we have so far had had a very, very powerful telescopes with a very high sensitivity and good spatial and spectral resolution. The only disadvantage is that the field of use are smaller than compared to the moon. Here in this image, you see it's in the arc minute range. While the erosita has a field of view of one degree, and it can do these scanning observations. So that's the reason why we can do an Oscar survey, which is just not possible with X-ray telescopes like X-ray mutant or Chandra. And we can also study larger fields. So we can do deep observations of large sky fields. And here you see erosita before it was launched. So this was assembled at the MPE in Garching. Erosita consists of seven telescopes. So you see the telescope module here. One of it here with the nested shells for the X-ray optics. This is the instrument in the focal point where you have the CCD detector with the filter with. And so this is the front view. This would be the back view. So you see the instrument electronics in here. And this was ready to be... So it was a very long preparation until it was ready to be launched. And then finally at the end of 2016, it could be then prepared for to be shipped to Russia, where then it was mounted on the spacecraft. So here you see the plane that brought it from Munich to Moscow in January 2017. And then in Moscow it went to Lavochkin, which is the company that produced the satellite. Here you see erosita together with ART-XC, which is another X-ray telescope from the Russian collaboration, which is a hard X-ray telescope mounted on spectrum. And it went through a lot of testing. And then finally in mid 2019, the Spectrum-Rentgen Gamma was ready to be launched. So it was then brought to Baikonur. And here you see how it is now mounted on top of the proton M rocket in erosita again at XC with the navigator platform. And it is now moved out to the launch pad. And here the first launch was supposed to be in June. And you see some colleagues here from MPE and other participating institutes. That's Peter Predil, who has been the PI of the erosita project for a very long time. And as you might know, he was now succeeded by Andrea Meloni. But on this day, there were some technical issues. So Spectrum-Rentgen Gamma could not be launched. And it was shifted by three weeks. And finally, July 13, this was the good day. Erosita onboard Spectrum-Rentgen Gamma, along with ART-XC, was launched successfully. And this was more or less two years ago. And ever since, it is taking a lot of nice data. So in the first month, we had the calibration and performance verification phase after the telescope was commissioned. And half a year later, after the launch, we started with the first all-sky survey. And you should know that we are one all-sky survey. One scan of the entire sky takes half a year. And we are going to make eight of such scans. Therefore, the entire, the full all-sky survey will take four years. And we are in the middle of it. So we have finished three scans, those three all-sky surveys. Now, we are in eras four right now. And we will continue. And some of you might have also heard that a couple of months ago, we released the first data of erosita. So these are the data that were taken during this calibration and performance verification phase. And this was called the early data release. So we released the data plus some publications reporting on the results of the analysis of this data. And here, this is just a summary of what we released. So you see, we have all the data that are available taking from the first month. We also have the science analysis system, ESAS, which was also made public at the same time. And some online documentation. So if you are interested in looking at the erasita data, you should go to this webpage hosted by the Max Planck Institute for Extraterrestrial Physics. And you can take a look at these nice data. Right. Here now, in the rest of the time, I would like to show you some results that we have obtained. So as I said, we are going to make eight surveys of the entire sky and what you see now is an image created only after the first survey. So this is the entire sky comparable to what you've seen from Rosa, the first slide that I showed. And you already realize that you see much more structures in here. You see a lot of point sources. So this is due to the much better spatial resolution. And you recognize all these structures that you have seen before, but in a much better or finer structures. And in each of these regions, you can also take spectra like similar to the resolution that I showed before, similar to what you have for XMM Newton. So now you can go and study the entire X-ray sky also in taking spectra. And when you look at this image, there is one striking thing that you realize. And you have realized it as well also looking at Rosa. So this is this one structure here, which we call the North Polar Spur. And in the beginning, this has been discussed to be the part in which this local bubble in which we are located. And I talked about it. So this is this large super bubble in which the solar system is located inside. And this local bubble has a neighboring bubble, which is called the Loop 1 bubble, and it's merging. And one explanation for this ring like large, huge ring like structure in the scene in the sky is that we see the rim of these two bubbles where they meet. Of course, this is not ruled out yet, but there are also other ways to explain it. Here in this image, what is also now striking is that you don't have only a large bubble here, but you clearly start seeing this bubble also in the southern part of this X-ray sky, which was existing in Rosa's image, but was not so as prominent as you can see here. So just marking it again, so you see the northern part, the North Polar Spur, but here you also see some emission here, very faint emission in the south. We now call it the erosita bubble. So here you see the image the entire sky without the point sources, only in the range between 0.6 to 1 kiloelectron, where this emission coming from the erosita bubbles are most prominent. And as you see, you clearly see this ring like the arc here, up here, and also below here. And of course, if you see that, you realize that it must be somehow associated to the Fermi bubbles that were detected a while ago. So here now you see an overlay between the erosita image and the Fermi image. And you see this in the inner part, you clearly see the Fermi bubbles, and they are surrounded, seem to be surrounded by the erosita bubbles. So how can you explain it? Of course, it can be still the rim of our nearby local bubble, but it can also in addition be caused by some outflow from the galactic center. So what you have is you have this outflow causing a hot galactic wind and will cause shocks and you will see the inner more energetic part as in Fermi bubbles. But then the shock medium in the halo will be visible still in x-rays, and that's why we see it in erosita. And as I said, we can now take also spectra, and from that we can derive the surface brightness, temperatures, abundances, and make an estimate calculations of the creation of such bubbles. Shortly after we published these results, there were several other people working on that. And in this case, by software in Kataoka, it was also shown that not only do their calculations support this idea of a galactic center outflow, but they also find a crater in the galactic disc in the distribution of the gold gas or the atomic hydrogen and the molecular gas, where you see kind of the base of this outflow. Now I would want to move out of the galaxy again to the Large Magellanic Cloud. Maybe you are now tired of hearing it, but as it is the best place to look at extended structures in the galaxy, here you see the Large Magellanic Cloud. In the optical we see a lot of emission coming from the stars. Then if you take again only the narrow band emission line images in the optical H4 oxygen-3 and silicon cell 4-2, sorry, then you start seeing all these emission nebulae here, you see the Tarantula nebulae. And that's typically because you have this partly ionized worm interstellar medium. And if you look at it in X-rays, this is what it looks like. It's an image taken with erosita fine with the other telescopes like XMM Newton. We have been trying to cover the entire LMC, but it's really difficult with the small field of view. With erosita, it's done in one go. You have a lot of diffuser emission, and here you see again the Tarantula nebulae or the Seltidora to C. So we had performed long observations in this region, so this part around the Tarantula nebulae was our first light of erosita. And here you see the Supanova remnant N132D, which is the brightest Supanova remnant in the Large Magellanic Cloud, and also a nice calibration source, because it has a lot of emission lines. Therefore, these regions have been observed very deeply with long exposures in the beginning. So this is these data we already analyzed before the early data release, and mainly focusing on the diffuser emission. So like here, for example, you can remove all the point sources and do some spectrum analysis in these regions. And what you see again, so for example in the Seltidora, just typically you have this, as I said, this thermal emission, you see a lot of emission lines here. Also, if you look in regions between these prominent sources, you see a lot of emission coming from the intestinal medium. But if you go into the interior of the Seltidora or in the Seltidora, you also see this additional non-thermal component. So this was the initial study of the intestinal plasma performed in the LMC. And you can also compare the distribution of this hot face with the warm face, as I said before, this is again the optical image. And what you realize is that there is a lot of emission everywhere coming from this diffuser emission, but then it looks greenish here. And this is because again, I'm used, I have used the three color presentation. So this is a soft X-rays. And here some soft X-rays seems to be to be absorbed by something that is also in agreement with the distribution of the warm ionized gas. So there seems to be a lot of also cooler material in front of the material that is emitting X-rays. So what you can do is you take all these spectra, as I said before, in these small regions and do spectral analysis. And not only you can study the properties of the emission, the emitting plasma, but you can also study absorption because X-rays are easily absorbed. And you can derive the column density. And this is shown here. So this image on the left is the column density obtained from the spectral analysis of each of these regions. And if you now compare that to the measured column density from the atomic gas on the right hand side, you clearly see there is a nice agreement. So these contours are taken from here and over plotted here. So now what it looks like, what we can do with erosita due to this spatial and thanks to the spatial and the spectral resolution, we can do X some really analysis also not only of the emission that comes from X-ray sources, but also the absorption of material that lies between us. So in principle, what we can do is something like what you do at the doctor if you go and make an image of your hand or whatever, and you get information about the hand. Now we can do that also with this X-ray telescope. What we also studied in this new data is all the supernova remnants, which we find in this area. So as I said, there is one N132D, but there are also a lot of known supernova remnants, bright sources. On the right hand side, you see the radio image because supernova remnants are also very bright sources in radio. And we also could confirm a new supernova remnants. Here you see this is for visualization. We used a mask so the data is cut here, but there is additional data also here next to it and you see it here. So here we confirmed a new supernova remnants, which was detected in the optical and can now be confirmed as well in X-rays. So we will be searching for new supernova remnants in the Magellanic clouds, but also in the galaxy. And we are sure that we will be finding a lot of new interesting sources. Then 1987A, or maybe let me go back. You can see supernova 1987A here as this bright source. This is an interesting source that is now developing from a supernova to a supernova remnant. Here you see the change of the spectrum from X-ray Newton, which we have been covering all the time. So you see that especially this hot component is getting brighter. You see this black dotted line. And that's because the shock wave of this supernova, which was for a long time interacting with this equatorial ring around the progenitor, now has most likely left this ring and is now expanding in the H2 region in the circumstance data medium. And we can confirm that with erosita. So this is the erosita spectrum, the latest erosita spectrum compared to X-ray Newton spectrum. And they are in very good agreement. And if you look at the light curve for the different energy bands, erosita confirms that at the software energies, it levels down, but the hotter component of the outer shock base keeps increasing. Then, as I said, N132D, our calibration source, we are looking at it very regularly. So this is an image of the region and zoom in on the supernova remnant from the very first data. And here you see the spectrum. You can clearly see this bright oxygen lines, iron lines, neon lines. And this is the reason why it is also used as a calibration source, especially for this for the spectral resolution. So we are analyzing this data, and we have so much data from N132D, we have to see how we are going to publish them. Then I wanted to talk about structure seen in our microweaded carina nebula. So it's a very, also a very bright H2 region. You might have seen that before. It's also bright in infrared, which you see here in the lower panel, taking with all wires. And it's famous because it hosts the Eta Carina Wolf-Rayier system. It's a colliding wind binary. It's a very high energetic source. And this is the image taking with erosita. So you see clearly again in three color presentations, so red is soft, blue is hard. And all these massive stars emit hard x-rays, and then the shock region around it, higher energies, greenish. And then in the outer parts, you see the softer x-ray emission from the shock tot, hot plasma. So we are currently analyzing these emission and also looking for indications of non-thermal emission may be coming from the accelerated particles. Then what else do we see? Of course, this is the most striking thing that you see if you're interested in the extended emission. This is the Vila Supanova Remnant. Here you see a zoom in onto this point. So this is the Vila Supanova Remnant, again in three color presentation. You see the Vila parts are here in blue, the neutron star with the pulse of wind nebula. Then you have the additional Supanova Remnant, which we call Vila Junior. You have here this nice non-thermal shape. So this is a completely non-thermal Supanova Remnant with NCCO. Then nearby you have Papis A. So you see this nice bright thing. This is another Supanova Remnant seen in projection and into this direction. And you see, so this is again a three color presentation using different color scales. You see very nice filamentary structures. You can also see the neutron star inside it. And we are now doing a detailed spectral analysis of this emission, and we are also studying the ejecta in the Supanova Remnant. Then another interesting source that was found in this IRAS data is this new Supanova Remnant, which is called the Ho Inga Supanova Remnant. It is also confirmed in radio. The blue emission is radio and in X-rays we see this filling red emission. So this is in principle, this is the first Supanova Remnant we newly identified in our Milky Way based on IRAS data. And I'm sure there will be many more. And this brings me also ready to the end of my talk. Now I just wanted to make some, give you some outlook to what you can be expecting. So we are now currently working on all these data. And especially we have a new research unit in the core institutes of EROSETA, so which is MPE, ASS, and then Tubing and Humboldt and Potsdam, funded by the DFG, especially on the study of galactic sources. And a big part of this research unit will be working on the interstellar structures like this and the entire background and the entire interstellar medium in the Milky Way, but also Supanova Remnants and especially also in the study of the Magellanic Clouds because they are nearby and as I said, you can also the small Magellanic Cloud, which I didn't mention, but there is a lot of data where we can study all these type of sources. Yes, that's the end of my talk. Thank you very much and I'm happy to take questions.