08:05:05 Good morning, everyone, it's 8:05am, on the dot and today is tutorial day, hope you're ready for what is clearly going to be a great day. All right, so I know this week is technically observation week, but I actually couldn't resist this graphic from 08:05:25 the illustrious tng collaboration, whose own Dylan Nelson is actually giving a tutorial today so it is relevant. This image shows a render of the gas velocity in the most massive redshift zero cluster in TMG 100, and it's at this intersection of cosmic 08:05:44 filaments, and I just think it's really beautiful. 08:05:48 Ok black is slow White is fast. Right. Alright so. Also of note, I'm going to encourage everybody to join the Slack channel Halo 21 week eight future. 08:06:01 There's also Halo 21 tutorials. I think one of the things we've established is that the halo 21 week eight future ABS is a kind of all purpose this week channel for writing your comments and questions about the tutorials and yeah so so use use that channel 08:06:18 for comments questions, and of course you'll have breakout rooms today for questions, just wanted to share with you this beautiful picture we took yesterday, of, of our workshop photo attempt. 08:06:34 These are most everybody who have their video enabled anyway it's posted in Halo 21 general, I think it's pretty beautiful, if you didn't make it into the photo were contemplating a way to maybe give you a second chance to get your photo included in our 08:06:48 our workshop picture. 08:06:50 All right. Um, also, another announcement is that on Thursday at 4:30pm, we are going to do a social activity. It's an unstructured unstructured video chat over drinks coffee. 08:07:08 If you are just waking up or, you know, tea or or wine or beer, whatever. It allows for spontaneous breakout rooms to occur between participants, you don't need to download any special software and you know just for an hour or so people can show up on 08:07:27 room and just kind of try to socialize so it's an experiment. Check out Halo 21 socializing for more details if you're interested in coming to that event. 08:07:37 All right, another announcement, and I just posted a link in Halo 21 General, I'll try to cross list it and announcements as well. it's really important that we get your feedback. 08:07:55 And we have tried to streamline this process for you so normally Kitt will ask you to generate a document called your activity report and upload a PDF to their site, they'll also ask you for an anonymous survey. 08:08:08 The organizers might have asked you for a Google form. Now we've actually worked with KGB to streamline this process for you so all you have to do is fill out this Google Form, enter in a couple sentences about your activity during the workshop, your 08:08:22 willingness to be involved in, maybe extending the impact if you're not interested that's fine you can say that too. And this can actually serve as submitting your mandatory KTP activity report, it's collecting email addresses. 08:08:35 There's also an anonymous survey that we would really appreciate you filling out so that the organizers and K GP can assess Halo 21 scientific success and make future programs better, honestly. 08:08:49 Both of these will take you 15 minutes or less and it's really important that you do them. So, so please, please, please do we would really appreciate it. 08:08:57 Thank you. 08:08:59 Okay. Just a couple more new results videos have been uploaded yesterday a new one by Danielle sir Eenie, and yeah these are high quality videos these images I'm showing you here from Brown rock hard shoes excellent video and CDs fantastic video, both 08:09:18 in the new results channel and now on our YouTube page, go ahead and check them out. These new results videos are just really fantastic. It's a great way to stay up to date on the relevant literature for CGM science. 08:09:34 We also have a couple of videos on new instruments. 08:09:37 We. These are also on our YouTube channel and then the halo 21 new instruments channel blue moons, news, and our guests have both made some very helpful informational videos. 08:09:49 Also today. Glenn Rudy, Carlos Vargas and I are hosting a, an after party for this feature channel this week, there's going to be an instrument Roundtable, and glad in particular has worked really hard to invite a number of relevant people that are building 08:10:07 new instruments planning to build new instruments to all get together and talk about the kind of functionalities of these instruments and what we're going to be able to do in the next decade. 08:10:17 I think it's going to be a really interesting and productive meeting. Quick, please. 08:10:24 Ironically, we don't have anyone to come talk about Lou voir. 08:10:28 So if you are on the live horror science team and you want to talk about Lou was amazing capabilities, please feel free to join the after party and plug blue bar as well. 08:10:39 There's details about the after party in the halo 21 new instruments channel. If this is something you want to join. Of course I also want to highlight that it's not too late to join the other feature conversations this week Halo 21 a mission, which is 08:10:55 very active right now and Halo 21 parametric model, which had a an after party yesterday so lots of good slides and activity in that channel. 08:11:05 And they'll debrief us on Friday, with all the progress that they've made. 08:11:10 All right, and so today we have three absolutely excellent tutorials lined up for you. 08:11:17 First up, we've got Dr. Edmund Hodges clock, NASA scientist at Goddard, who will tell us about the X ray imaging and spectroscopy mission, aka the new Hitomi, which was focused on soft x rays. 08:11:31 So this is the future of CGM science, an exciting new capability, and then we will follow that up with maybe five to 10 minutes of questions depending on the time we'll take a break and then at 8:40am, Dylan Nelson himself will walk us through some online 08:11:49 tools for exploration and analysis of illustrious TMG simulation volumes, all of which are publicly available. These are tools that anybody can use. I'm very excited about this tutorial. 08:12:00 And, again, five minutes for kind of questions in the main room, there will be a breakout room devoted to to that particular tutorial. And then at 9:28am. 08:12:15 Nicholas de host will will give us a run through of some if you data, how to look at if you data particular Muse data. Nicholas is a professor at home to PC our university dog I totally can do have party so and yeah i think that this is a really interesting 08:12:33 juxtaposition of tutorials and especially given Chris Barnes talked yesterday, where he was suggesting we make, you know some processing capability to generate if you data from simulations, so. 08:12:45 So I think that this will be a really interesting eye opening tutorial. So without further ado, I'm going to stop sharing and hopefully admin is here to start our first tutorial. 08:13:16 Alright, so I see that there's actually a fair number of x rated people on this, on the participants list. So, if you're one of them prepare to be bored. 08:13:25 I am going to or you know feel free to pick as well. That's always welcome. 08:13:31 Yeah. Today I wanted to tell you a little bit about charisma which is just said the X ray imaging and spectroscopy mission. It is a Jackson that's a partnership with contributions from Isa and also Canada. 08:13:44 So we've already heard for the past seven weeks you know why hot gas is an important component of the CGM why it's important that we have x rays in order to study it. 08:13:55 And it's kind of embarrassing that we're still in this phase where we have. We really have not answered the big questions you know these are like these could be the big questions of life but especially for the CGM. 08:14:08 You know we'd like to know how much hot gas there is where it came from and what's going to happen to it, and prism is certainly not the instrument that is going to answer all of these questions but it will help to answer these questions, and it is like, 08:14:19 it is the next capability that we will have to do so. And if I had to summarize what prism will do for like all star galaxies. 08:14:30 Excuse me. 08:14:31 It would probably be, it'll it won't do very much for the extended CGM like beyond maybe 25 or 50 Calabar sex, but it will do some very interesting work closer to the desk. 08:14:44 So what is prison. 08:14:46 Well, it is two telescopes, with basically should have identical mirrors and practice will probably be, you know, slightly different data fabrication. 08:14:57 But there's two telescopes and two instruments, so the primary one is called resolve it is the micro color emitter that's what I'll be spending. Pretty much all of the rest of the time talking about but there is also a CCD detector. 08:15:10 That is collide and will be simultaneously observing. 08:15:14 So resolve is a is a quantum micro Keller emitter. So this is an idea that has been around in the infrared and implemented, but for a long time, but in the x rays, it's it's sort of in a holy grail for a long time to produce one of these things and fly 08:15:30 fly it and have it last more than, I don't know a few weeks. 08:15:35 The basic idea can be seen over here on the right. 08:15:39 I can't see my own cursor so I'm not going to bother with, but if you see this block where it says he capacity so there's a detector pad and a photon comes in and is absorbed in this detector pad. 08:15:53 And that heats it up. And when that happens, the, we can measure the temperature very sensitively, and that temperature rise is what is proportional to the energy of the incoming photon. 08:16:06 And that's how we measure the energy of the photon. So you can see in that graph, just to the left of that with this pulse. 08:16:16 Essentially we measure the pulse heights of incoming photons, and that's how we achieve a high resolution in a non dispersal spectrograph. 08:16:25 This requires things to be extremely cold because individual photons do not carry much energy. So there's a four or five stage cooler that cools down to about 50 million Kelvin and that's the operating temperature. 08:16:39 Interestingly, we can use both mechanical credit coolers as well as cryogenic murder to cool it down. So even though the credit Jen has a limited lifetime. 08:16:48 Prison kind of principle keep operating for long after the cryogenic has run out. 08:16:54 In terms of what the capabilities of this thing are the requirements are listed on the center I would ask you to focus on the Hitomi values because so far we are instrument testing. 08:17:05 We are basically replicating all of the performance benchmarks they had told me hit. So the energy resolution is going to be about five vv, the energy scale accuracy is certainly going to be better than TV. 08:17:21 The field of views about three minutes so not especially large, and the angular resolution is a little over one argument which means that the the resolution is not like Chandra, this is, this is a much courser imagery. 08:17:36 And then the creation mode lifetime is between three to four years but as I said beyond that, you'll be able to continue using it, it just can operate with slightly lower efficiency. 08:17:48 The other instrument is called extends the CCD to maturity for chips with a 38 documented field of view. So, you can see from this inset, which represents the 35 active pixels of the resolve detector that the the field of view of resolve is a really small 08:18:08 fraction of the field of extend so the idea is that extend sort of tells you what you're looking at and how much light is being scattered into your field of view for resolve etc. 08:18:18 And there's other science you can do with it, but it's not a new capability. So we're going to focus on the lunar calendar. 08:18:26 So I thought that, for the sake of people who are not as familiar with X ray astronomy, it would be worth just briefly reviewing the different types of common X ray spectrograph so I know there are other types out there but these are probably the types 08:18:39 are going to be hearing in the most about. So there are CDs or similar detectors there's great things. And then there's micro kilometers. And then the X ray astronomy world, the incoming event rate the incoming photon rate for pretty much any source is 08:18:57 low enough that you can detect individual photons. 08:19:02 And so for CCD is what you can do is, is the photon will hit the CCD, it will liberate electrons from the semiconductor and then that will create a charge cloud or current cloud. 08:19:18 And, and that is going to the size of that is going to correspond to a pulse or the voltage spike. And then you can measure the energy from the size of that. 08:19:32 Now, that, that allows you to have emerging spectroscopy like we have on Chandra xmm, but it is relatively low resolution. So most of the data that, that you see from x ray astronomy is in fact this type of imaging spectroscopy. 08:19:47 Chandra and xmm both have greetings. 08:19:50 They also can detect individual photons and dispersed individual photons. 08:19:55 They have lower throughput and the CDs. 08:19:58 And in this case you get higher resolution because of course as you all know you disperse the light, and you're able to achieve higher resolution. And as you also know the greetings of constant wavelength resolution which means that you have higher resolution 08:20:11 for lower energies, 08:20:14 the micro color amateurs are kind of like the very complimentary to the greetings, the energy as we just discussed as measured from a temperature spike in the detector, you can get even higher resolution by creating something called a transition of sensor, 08:20:27 which at the end it will have where you basically keep the, the, the detector material just to the edge of super conductivity. So, when a photon is absorbed the resistance spikes, and you can measure the energy more accurately than with prism. 08:20:42 And in any case the the principle of the color emitter is that you have constant energy resolution, which means that you have higher resolution at high energy. 08:20:49 So really, in order to have high resolution spectroscopy across the X ray band. What you want is a combination of creating some micro kilometres, but crucially, the micro kilometer since it's non discursive, it means that you can actually build them if 08:21:03 you and that is that is what Islam Islam that is what Athena will be. 08:21:07 And this is great for a lot of surface brightness submission, for obvious reasons. 08:21:12 So these are simulations of the same simulated source it's not a real source, but I just put in a thermal occasionally. I am nice plasma model and pretended to observe it with these three different instruments so Chandra, is this instrument the CCD the. 08:21:33 xmm grading and then prism. And what you can see is both the effect of resolution, and also the different collecting areas of the different telescopes. 08:21:43 So the blue line is Chandra, and you can see that a low resolution at the CCD resolution. All of these lines just get smeared into a bump. And this is this bump is what we use in most of most of the time to measure things like temperatures and densities. 08:21:58 So you can see that it will be much more powerful, to have higher resolution, and what you can also see from the black line which is the RGS is that over this baton pass you can actually see the resolution get better as you go to lower energies and down 08:22:12 and oxygen seven, it's very clear. I mean this is the exact same spectrum so it's very clear that the instrumental profile of resolve is worse than ours wider than the RGS dotted oxygen seven, but up at neon nine it's not quite so bad and if you were 08:22:27 to go up to say to kV then prison would start to win. So if we look at a higher temperature plasma. So this is now a 4k TV plasma, about 46 million degrees observed with the great things now we can't use XMMRGS because it only goes up to about two kV. 08:22:47 So I have instead simulated the Chandra high energy transmission grading. 08:22:53 The, the, the iron 25 complex that you see here is now not really very well resolved by by the gender grading, and instead. 08:23:06 You really win by going to the micro Keller amateur with prism. 08:23:11 That was a simulated data set. This is the real thing this is the spectrum of the Hitomi of the person is cluster with autonomy. And what you can see is that they were able to measure the Doppler broadening and measure the turbulent velocity within the 08:23:29 person is cluster, because it's wider than the Tomi response which is shown there and purple. 08:23:35 So this is what five EV resolution looks like you know the iron kale full lines. 08:23:43 So I guess it's worth reviewing, just for the people who are not familiar with this history, how we got here and why it is that, like we talked about to tell me and now we're talking about tourism. 08:23:54 So, a long time ago, there was this idea to put a calendar in space and extra calorie butter. And one of the first serious considerations of that was for Chandra, back when it was called Xf there was there was sort of two components to that the imaging 08:24:12 and the spectroscopy. 08:24:14 They separated them out and ultimately only the imaging One Flew and that's that's what we know is Chandra. So, the, the spectroscopy capability was then picked up by Japan, and in around 2000 they launched Astro he. 08:24:28 But as you can see from this image on the left. 08:24:32 It failed to reach orbit. So after we failed, but they tried again. 08:24:39 Several years later with us for me to which was called Sudoku, she's okay did manage to reach orbit and that was just fine. But the kilometer needed helium cryo cooling and, unfortunately, shortly after launch the colon all vented, and so they were no 08:24:59 longer able to use the micro kilometer on board Cissokho, and I started became a very productive imaging instrument. 08:25:07 But, you know, there was still. We're still waiting to get the micro kilometer data so the next attempt was Astro he had told me, and for Hitomi they actually added to the back, a hard X ray imager, which is that boom that you can see extending out the 08:25:23 back. And the reason that you'd want to do that is because when observing things like AGN it's really nice to have both the soft and the hard component observed simultaneously. 08:25:34 So he told me he had a similar but better spectrograph from Amazon Cissokho, and it performed beautifully. And so that's where we got the wonderful Perseus data from, as well as a shorter observations of a couple other astronomical objects. 08:25:51 Unfortunately, There was a mishap as you probably know, and to tell me more or less fun itself out of control and the solar panels snapped off and the boom snapped off, and the mission was lost. 08:26:02 So prism is the next attempt. And I think this tells you that this is hard to do, but we're very optimistic that the President was going to launch and not have problems and perform well and launches expected around, 2022, or 2023. 08:26:22 Alright so this is going to be sort of a little detour. because this is a tutorial into the methods of X ray astronomy, there's obviously a lot of them so I'm just going to very briefly go over how we do this for hot gas, the quantity is that we would 08:26:36 like to know are the mass the temperature the medalists at the velocity, maybe a couple others that you can think of. 08:26:43 So for occasionally ionized plasma we call the thermal plasma. And this is just using the APEC model from from Adam dB. 08:26:53 The, the temperature can be measured by the, the different ions that are present with the lines from the different ions that are present. So, this equation at the bottom, where the flux is proportional to the what's called emissivity times the emission 08:27:08 measure the mission measures the amount of stuff. 08:27:11 And so that's how we can measure the density if we can constrain that. But to do that, we also have to constrain this emissivity, which is a function of both the temperature and the middle of the city. 08:27:21 So, from the temperature, we get from for example if you look at the top right, you can see the oxygen ion fraction as a function of temperature. So if you see that you have more oxygen seven than oxygen eight. 08:27:33 The blue shaded region is sort of the X ray band. Then, then you would know that you have a cooler plasma. So, you can do this type of thing for a number of different species. 08:27:44 And by comparing the the strength of the different lines, you are able to constrain the temperature which we do by fitting, what we call a global fitting over the whole band pass and seeing what what ions are present. 08:27:56 And then from the ratio of the middle st ratio of the lines to the continuum, we can measure the, the elemental abundances. 08:28:07 In practice, this doesn't look all that pretty, especially at CCD resolution. 08:28:11 This is what are called folded spectra so these are the, this is the to add some instruments looking at the exact same thing. And the reason they look different, is because the, the effect of area of the collecting area as a function of energy is different 08:28:27 for the two instruments and the spectral resolution is also a little different. 08:28:31 And you might ask, Well, why can't we just unfold us you know why can't we take this and go back to something that looks like this. And the reason is that when an X ray is absorbed it has a chance of being detected at the energy that it actually has or 08:28:44 at any lower energy. And that's because, as it's absorbed some of the energy can be lost some of it can like scatter out as an electron into a neighboring pixel or something like that. 08:28:54 And because of that, it's actually very hard to invert the spectrum to get back to what we know is the truth. So what we do is what's called forward fitting, where we. 08:29:08 And we've heard a lot about this already in this meeting. So we generate a testimonial similarly the observation using that the telescope model, and then compare to the observed data. 08:29:17 Another thing that you'll probably hear a lot about is, these helium like ions, and these can be used to diagnose the density and temperature within a certain regime, without having to fit the whole spectrum. 08:29:29 And that has to do with just the properties of the so called tripled of lines of the resonance center combination and forbidden lines. So for example the forbidden transition. 08:29:39 It takes longer to decay so it can be suppressed if electrons that are sitting at that level are being conditionally depopulated because you have high density and charge exchange can also results in a high forbidden to resonance ratio so if you are interested 08:29:52 in getting involved in extra astronomy. 08:29:56 With President it would be worth learning about the helium like triplets for velocity. 08:30:02 In terms of direct measurement so I think that right now for bulk flows at least, pretty much all we can do is use Doppler shifts and resonance absorption lines, and the Milky Way is currently the only place where we can really directly measure the kinematics 08:30:15 and indirect measurements are possible in a few galaxies, but this is something we're coming artists will will really help. So this is an RDS spectrum mmm RGS spectrum of Markarian for 21 which is an extremely bright blazer. 08:30:38 And what you can see is that referenced, then the inside is the reference to the laboratory wavelength but recalibrate from this bright star Capella. There's a Doppler shift so you can do that for different lines across the sky. 08:30:43 But with prison will be able to do much better. 08:30:48 So, Crystal was really good for clusters. 08:30:52 I think that, you know, you've probably heard about all of the stuff that micro color emitters can do for clusters much more than anything else because that's some of the most spectacular work. 08:31:02 So these are simulations done by Aurora, who contributed this to the prism science white paper which you can find on the archive and prism is going to be able to measure, like the dynamics of cluster mergers measure precise masses freezing clusters and 08:31:18 cosmology, and determine how Ag and feedback heats the ICM and mixes the metals into it. So if you're interested in clusters and I know that many of you are prism is going to be absolutely fantastic for that. 08:31:30 The question though is that I wanted to get at is how does it. How does it do for all star CGM science and since just had encouraged us to use emojis. 08:31:39 I tried to do this. 08:31:41 And I think what you can see is like on the left, the instruments that we have Chandra and XML and now you Rosita are really not very good for all star CGM science, they're good for some things, especially at higher Halo masses but but for Milky Way size 08:31:58 galaxies, other than perhaps the Milky Way itself. 08:32:01 They're really not all that spectacular artists, this is not really a advertisement for artists but archives is designed to, to look at the CGM and so of course over on the right you can see that it would be just fantastic for CGM science Christian was 08:32:16 not built to look at the CGM and all star galaxies. So, there are some things that it will do. There are things that will make breakthroughs. 08:32:25 But as I said it's going to generally be closer to the galaxy. 08:32:29 But I think that there's one thing in particular that you should be very excited about with prism for smaller galaxies is understanding outflows, and the role of hot gas and these outflows. 08:32:43 So, with the remaining time I just wanted to go briefly through the three sort of case studies that are at least adjacent to the type of science that we've been talking about it this meeting. 08:32:51 So these would be a galactic wind, the temperature structure of the hot ISS, and resonant scattering. 08:32:57 So, the pot on the left is very familiar to all of you. And we've seen something like this and pretty much every talk and this conference. 08:33:06 But the point is that stellar feedback is not to be a driver of galaxy evolution, and it's likely unbalanced more important than ag ends in terms of number of galaxies and it's a way to enrich the AGM hi redshift. 08:33:19 But we still don't know what the driving mechanism for the winds are like we had the outflows week we heard a lot about epileptic wins and then in the non verbal week we heard a lot about cosmic rays. 08:33:31 And I think that we still don't really have a clear answer for the role of hot gas is it mostly along for the ride or is it really the driver and how much mass is taken out what does the math loading even mean right we had a tutorial about that early 08:33:45 on. 08:33:47 So our goal is to measure the mass energy and mental content of the hot component and determine really how important it is. So one of the best places to do this is mad to which is shown here on the right the prototypical Starburst. 08:34:00 And so this is what the data looks like and Chandra. So this is the green is the resolve field of view overlaid on to add to the left image is showing the soft mission, and on the right panel shows a very narrow band, highlighting that there is diffuse 08:34:20 iron 25 emission as well in the center. 08:34:24 And there's also some bright point sources but the diffuse iron 25 is about 40% of the total admission of that band which means we stand a chance of seeing it. 08:34:36 So, you know, if we were to measure the velocity and the soft bound. 08:34:42 Then, you know, we can use some of these other these lines to measure the velocity and the overall Nebula, and prism is going to do a very good job at that. 08:34:53 So we're going to be able to constrain velocities, a line of sight velocity, and velocity width in in this Nebula, but we're also going to be able to do it in the very nucleus, and this is really exciting because this is the hot gas the very hot gas that 08:35:07 we think actually drives the wind. 08:35:12 So if we're able to measure a very high velocity in the nucleus from the, the iron 25 or 26, then we will know that there's a lot of kinetic energy there and then probably is an important driver. 08:35:25 The next case study and probably the lesson I'll get to before the breakout room is the temperature structure of the hotline. 08:35:32 only measure one or two temperature models and those little show that's that's very much not adequate. And so what we want to do is use the lines from multiple species to construct a temperature distribution. 08:35:55 Much like has been done and stellar crony. 08:35:58 So this plot here just shows the, the results for measured temperatures for to temperature best fit models as a function of the variable temperature for that Halo mass and you can see that pretty much like all halos have the same temperatures and, and 08:36:15 in fact this is generally true that you can take the same temperature model and fit it to most galaxies on the Chandra archive. 08:36:22 And these temperatures really don't mean anything, or at least not very reliable other low side for admission measure distributions with different shapes when viewed at low resolution. 08:36:31 And this leads to systematic uncertainties on the pressure of up to like 500%. So there are external constraints that may reduce that. But we'd really like to know the true temperature structure. 08:36:41 I'm just going to skip past the resonance scattering to let you know about this important result which is that we now have the guaranteed time targets announced, so if you go to this website which I'll post on the slack later. 08:36:58 You can see the targets which have been selected priority a will be observed priority see maybe observed. And there's actually an opportunity for you to get involved. 08:37:07 There's going to be a call for proposals to join target teams for a priority targets so each target is going to doesn't have it now but it will list of the proposed science, as well as the the possible needs that team has, so he will propose to individual 08:37:22 targets, and then selection will be made by anonymous peer review. And then the guest scientists would be assigned to the target teams in advance of launch, and basically add money to cover salary travel and publication charges. 08:37:35 But this is a good way to get involved with prism early on, we're not only looking for extra astronomers there there's definitely room for theorists and multi wavelength observers to join the team. 08:37:46 So with that, I'm just going to leave this up, I talked about what Christian could do for CGM Jason science but Islam Islam Observatory, you many of you are interested in many different things, because it was good for a whole bunch of stuff. 08:37:59 So I look forward to talking more about that on the breakout room. 08:38:08 Thank you, Adam and that was amazing. I am very excited for for this. So, I have just opened up the breakout rooms, and that should be pretty obvious which one is which the. 08:38:24 You say it, you say XRISM right. 08:38:26 We call it prism. 08:38:29 Okay, Chris them. 08:38:32 We will, it will be renamed on lunch. So, you know, don't get too attached the name. 08:38:37 All right, well there's a XRISM room, and that's the room you go to if you want to talk more about prism. And let's take a two minute break and then exactly 8:40am, I'm going to ask Dylan. 08:38:48 To begin, so, Edmund if you can head over to your breakout room and Dylan if you want to start sharing your slides if you if you have them. You are welcome to do so and we'll start an exactly one minute, from now.