08:05:08 Good morning everyone. As our numbers rapidly increase. I'm just going to give you my, you know usual spiel to get us settled in to the morning and today is a very special morning.
08:05:23 It is the last keynote presentation of our workshop, it's kind of sad. And also, you know, a little bit of a relief maybe for those of you who are overwhelmed.
08:05:37 So, today's featured photo, at least one of our participants will recognize this photo. In fact, the one person will recognize it as the person who took it, who's here, I have verified.
08:05:51 If people want to guess who took this photo in the chat, you're welcome to was taken in Crater Lake, and 2013.
08:06:00 The photographer kicked the camera by mistake. During this long exposure. And that is what gives it this crazy ripple effect and looking at the stars shining through the dark tree trunks I think it's just absolutely beautiful.
08:06:19 If you look closely, almost in the center there, of those trees. You can see the Andromeda Galaxy for UM 31 aficionados and Marcus has Aurora, obviously, yes.
08:06:37 Aurora, our keynote speaker for today is actually an accomplished Astro photographer which I figured out, trying to hunt down some info for her, her bio and I was particularly impressed by this one, beautiful photograph.
08:06:48 Another beautiful photograph is the conference photo that we took on Tuesday. However, a few people dm to me and said oh I wasn't in the photo for whatever reason my video wasn't working it wasn't there blah blah blah.
08:07:02 They want to be in the photo. You'll get your chance. But I hope that you're studying this photo right now because you will be tested on this. And the question is, are you in this photo, or are you not in this photo.
08:07:15 That's it, that's all you need to know. Are you in this photo or are you not in this photo, hold that information in your head. Okay, you're going to need to hold that information in your head for the next 10 minutes, are you in this photo is the question.
08:07:28 Alright, study it carefully.
08:07:33 Alright, so tonight at 4:30pm, we have a social hour, and this is kind of like a way that we can celebrate our time together at the workshop, it's informal you don't need to download anything in advance details on Halo 21 socializing.
08:07:51 You know that it's going to be cool because of the very edgy way that room is spelled.
08:07:57 So it's an unfair structured video chat over drinks of any kind.
08:08:03 It's going to be awesome.
08:08:05 And, you know, I'm not going to go into detail the details of this are in Halo 21 General 12 of you have already filled out the Google Form, and I thank you from the bottom of my heart.
08:08:17 Thank you. Thank you. This kind of assessment is important. There's one non anonymous survey and one anonymous feedback form, both of them are absolutely essential.
08:08:25 Please do them. Please Please Please don't make me beg you Don't make me say this over and over again, head to Halo 21 general and see the details, there's links for both forms.
08:08:38 You just got to do it, and it's how you submit your mandatory activity reports so you won't get bugged, if you do it.
08:08:47 15 minutes or less. All right, more new results.
08:08:52 And just yesterday you Gong Chen posted a new video on KBSS using foreground and background galaxy pears to trace the structure and kinematics of the CGM h1 at redshift to amazing video.
08:09:05 These new results videos are still coming in, and I am just so pleased to be able to recommend them to you so please head over to Halo 21 new results, or go to our YouTube channel and watch these incredible videos that really are telling us about the
08:09:23 future of the CGM, and our ability to understand it.
08:09:29 Finally, I just want to point out that these are the photographs of the people who are frantically trying to prepare their debriefs for tomorrow. We'll hear from Halo 21 a mission Halo 21 new instruments in Halo 21 parametric model.
08:09:42 I know new instruments we had a roundtable discussion yesterday.
08:09:46 That was two hours it could have gone for four hours, it was absolutely amazing. It's not too late to head over to the slack channels and check out what's been going on.
08:09:55 Mark has been furiously preparing slides for the halo 21 parametric model.
08:10:01 Share back tomorrow it's sure to be very, very interesting.
08:10:06 I know that I have found myself in the position of having to defend all observers, he tried to put observers in the corner and Nobody puts observers in the corner, as far as I'm concerned.
08:10:19 All right. And finally, just want to plug emojis. For those of you who have not yet adopted them.
08:10:28 When we're not communicating in person. We're not in the same room we miss out on physical signals that suggest agreement approval connection, and warmth emojis are the fluid language of the internet and they will help us fill that void.
08:10:45 There aren't right or wrong ways to use emojis at nuance, add your own flair, can be found people if you want.
08:10:54 With that said, today's panel discussion is actually going to take place. Totally in emojis. All right, that's, that's a joke.
08:11:03 See I can't tell that you're laughing because nobody's using emojis but I assume you are laughing hysterically. Alright so, just kidding, but I do encourage you, thank you, Graham Thank you can't gosh you guys are.
08:11:18 All right, so, uh, but go ahead and use emojis, especially as reactions in the Slack channel, it's really going to help me guide the discussion and the direction that you want the panel discussion to go, it'll help me read your reactions, I can't do this,
08:11:30 we're not sitting in a room together emojis are great. I've also just heard that Ben and Aurora, have come up with an emoji that they want to symbolize X ray, and it's the skull, not the skull and bones which you can see on my frequently used emojis there
08:11:46 don't use that one that's like death, but the skull is the x ray symbol the plane skull and they're going to post that in the halo 21 week eight future of Slack channel.
08:11:59 All right. And finally, I am absolutely delighted to introduce our keynote speakers today we've got a double header, first up we're going to hear from Dr Aurora UNESCO.
08:12:11 She's an astrophysicist on the tenure track at restaurant, Netherlands Institute for Space Research and also an affiliate member of the academy Institute for physics and mathematics of the universe at the University of Tokyo in Japan.
08:12:24 In addition to her spectacular Astro photography, you may know, Aurora, as an expert in the physics of the hot plasma, and galaxy clusters.
08:12:33 Next up, we will hear from Nick Battaglia, a professor at Cornell University who specializes in the thermal and kinetic tonight we'll delve into effect and what it can tell us about galaxy evolution and cosmology.
08:12:48 He's directly involved with the Atacama cosmology telescope among many other projects, and with any luck, they'll both be finished around 9am, give or take, you know, I'm not strict about these things we'll take a quick break and then we'll have a thrilling
08:13:01 panel discussion, featuring Dr. Alexei Vic lemon, Rachel Somerville admin Hodges clock and Collin Hill and absolutely All Star lineup today, I cannot wait.
08:13:12 We're going to spend. Now, I told you there will be a test. So before I let Aurora take the reins here.

08:15:41 All right, week eight, everybody, uh, it's been really exciting I've been listening to this through the years of an X ray astronomer and I have a slogan of the conference that I would like to share with you and the slogan is hot is where it's at.
08:15:53 And by that I mean not only that most of the barriers that we are looking for are in the hot phase in the CGM, but also that is where most of the action is happening and I swear I came up with that before.
08:16:07 Chris Martin said the exact same thing. on Tuesday, so we agree.
08:16:11 And if you would like to understand and to know where all these baryons are and what they are doing, more importantly than that to probe this more than 10 to the six k phase you have two choices you have the choice of X rays either and absorption of Oriental
08:16:36 mission, and that's what I will be talking about, or you have the choice of the snaps although which if I am for that. Stay tuned for next talk just after my.
08:16:37 Okay. One thing that hasn't been stressed, to the extent that I would have liked to have seen it stress, though, in this conference is that if you go to the heart space.
08:16:46 The other thing that you learn is how everything connects and in week five from Busan I think we have seen this amazing plot of this intergalactic transfer, these are things that fly out of a galaxy and end up in another galaxy after having traveled to
08:17:03 the cosmic well. So we would really like to understand.
08:17:08 Also how all of these things connect so cluster of the outskirts of clusters of galaxies intergalactic our scale filaments and the CGM, these are all things that should equal us into should.
08:17:22 Why Why should be of equal interest to all of us who are in this room right now.
08:17:29 So, the holy grail of these the thing that is going to put the theories out of business or perhaps into business would be to create a map that tells us about the thermodynamics mentality and kinematics across this entire range of scales from CGM for feed
08:17:46 skills related to feedback, all the way out to the cosmic way. And as we've heard already on Tuesday. If you want the map, it's the easiest way to take picture of a lion as much as you can do it is through a mission so let's see how far emission studies
08:18:03 actually take us. Now for the people in the room who are not extra astronomers I got this question a couple of times what is it that we are actually looking for information in x rays.
08:18:14 What do things look like. So, here is a plot for three different temperatures of the gas so this is the spectral model. This is for a 10 to the eighth, Kelvin.
08:18:26 So this is a very hot cluster of galaxies about 10 kb.
08:18:30 This is standard a seven Kelvin so this is more like one kV either the outskirts of a cluster of galaxies will typically have this temperatures, or a typical galaxy group.
08:18:40 And here you have 10 to the six K, and that is I think what most people here are interested in.
08:18:48 Two things very important that you should keep in mind throughout this stop. The first thing is we keep saying, Oh, you know, ambition depends on the square of the density.
08:18:59 This is true but in this picture actually ambition, also the flux also depends on the temperature, you can see the shape is changing, and it depends on the metal city, and Mother Nature has actually been a little bit kind to us in the sense that cooler
08:19:15 plasmas for a fixed asset the fixed mentality are actually brighter.
08:19:19 Okay.
08:19:20 The other thing you should keep in mind is that when you look at these very hot things most of what you're seeing in our mission is hydrogen that is most of the flux but when you look at cool things.
08:19:29 Most of what you're seeing is lines. Okay so, really important thing. What we are seeing in x rays for these very low temperature plasma is just the metals, if you care about hydrogen go to next talk.
08:19:42 Okay, there's a lot of fine, fine print here for you to look at, to look at later. But this is these are the spectra that we're, we're interested in. And now what kind of observational characteristics, do we need a telescope to have in order to reveal
08:19:56 these things.
08:19:58 I've picked out for important things that you want your telescope to have. There are many other things, but I don't want to make this plot very complicated.
08:20:09 So these things are effective area, things are very faint, you need a big mirror.
08:20:14 Grace, things are not only very faint but they're very big on the sky in some cases so you need a big mirror, and a big field of view you need a big survey speed spatial resolution.
08:20:25 You know, there are a lot of physical details that are interesting on very small scales that we also care about. And you want you care about the kinematic so you want to have a spectral resolving power so you can see the shifts and width of your emission
08:20:40 lines or absorption lines in exits. And so this is where we stand right now Chandra and XML. These are my units for each of these axes, and we'd like to push as far as we possibly can, along each of these axes that that we can so as many axes as far as
08:20:57 we can, at one time. So let's go the first push comes in this direction and it comes from your oz down the log axes doesn't do this figure, Justice arrows it ties about four times has a has a grace to those by four times that of XML.
08:21:16 And we've already seen in week four from Marcus's presentation.
08:21:20 What's that improvement of a factor of four can buy you in terms of mapping large scale emission from the Milky Way. And in terms of mapping large scale emission from the cosmic web in this very deep scan of April, 3319 3395.
08:21:38 Now the fully Rosita survey, all sky surveys underway. And one thing that I think you can look forward to is this proposal in a paper by Ben, which is that we can then take this all Sky Survey and we can pick out halos CGM halos weekend stack them and
08:21:56 then we can see what we might get. So here are the predictions in.
08:22:02 This is from ego and this is for from TMG of both for a high specific star formation low specific star formation, and then hi mass and Loma samples, and there are two important messages here I think the first important message is that we can detect these
08:22:18 things through stalking we can detect these things with your Zika out to a few times of parsing.
08:22:25 And the other thing is that you can start to see the difference between ego MTNG and maybe we can constrain which of these things, has a feedback prescription that fits, slightly better to the day.
08:22:38 Let's go in the next direction so next up on the launch pad is prism and this actually goes in the complete opposite direction, then you Rosita. So we have a very tiny grass.
08:22:51 But we have a very good spectral resolution and this is actually due to the technical limitation we are now using to, or we are using micro gallery image or pixels, and it's hard to have a very large right so if you want this resolution, the first thing
08:23:04 you have to do is start with a small field of view on a small number of pixels. All right, now this has a seven EV resolution.
08:23:13 It's actually optimized for hot things okay it will be great for clusters. For this, Iran 25 line you have a resulting power of 1000, but for these low energy lines maybe not necessarily that much if you want to know more details about prism, go to yesterday's
08:23:30 tutorial by.
08:23:33 I want to tell you three things that I'm excited about that.
08:23:38 Chris prism is going to do.
08:23:40 The first thing is my favorite object, all time and this is me. This is the BCG of the nearest cluster Virgo cluster. And we've seen in week four I believe from Dylan this beautiful simulations of how black holes were blowing metals, out of a galaxy at
08:23:57 24.8. Now, this is a well, not an equivalent of that but is a place where we actually are seeing the black hole transport metals blow metals, out of the center of the galaxy to large radio.
08:24:11 And here is an abundance map this is either an abundance measure with XM Newton. And you can see here this plume of hot a high Iran abundance material, and this plume happens to coincide with this big radio lobe, that is coming out of the black hole so
08:24:27 the radio lobe of the black hole is pushing or pulling actually I think metals out to larger API.
08:24:34 And even though at these low energies, we don't have the power to resolve the width of individual lines. What I think we will be able to do is use the line shifts, and use the line shifts in order to see whether there is any line of sight component that
08:24:52 is associated with this metal uplift of the black hole and how fast these this actually happen.
08:25:01 The other thing that I wanted to point out because you know we are in the CGM workshop is, what is the lowest mass Halo that we are guaranteed to get time from Chris I'm so the lowest mass Halo in the Christian TV phase is NGC 4636.
08:25:17 This is a giant elliptical galaxy in the outskirts of the Virgo cluster, very very bright, beautiful science of interaction with the AGM.
08:25:27 And what we are hoping to do here, there is a hand from xmm Newton of resonance scattering, and this would indicate that the turbulent philosophies are very low, and we would like to confirm this hint and get that much better measurement of the turbulence,
08:25:41 that is associated with aging and feedback in this galaxy. And lastly, I will not belabor this because Edmund went into detail so please see his talk led to we've talked a lot about the mid to in this workshop, we will observe it with prism and we will,
08:25:57 we are looking for shifts of the magnesium lines silicon line independently of each other. See, these atoms are moving together or separately line broadening of the hot iron 25 line because that one is result.
08:26:11 We're looking for charge exchange and we're looking for the chemical composition of the wind object so lots of wonderful things.
08:26:18 Right.
08:26:32 So this is going to be the next five years, and I'm going to fast forward now to 10 years from now, and 10 years from now we're looking forward to Athena Athena will carry two instruments will have the few.
08:26:35 The few is here in blue and you see what the giant leap the Xi few is going to be compared to Chris and that is here in yellow.
08:26:51 And also, as you know will carry a Wide Field Imager and the Wide Field Imager is here in orange compared to your Rosita. So I think that will be better than the Rosetta and prism combined into one telescope, it's going to be absolutely amazing.
08:26:59 Now, again, this, the spectral resolution is optimized for hot clusters.
08:27:07 Okay.
08:27:08 And so in these podcasters you can measure kinematics to an amazing precision. And because now you have a much better spatial resolution and grasp, you finally have a true integral field unit.
08:27:24 So these are some models and predictions again our friend, I made the two here at the top, and the other you know favorite poster child purses cluster at the bottom.
08:27:34 These are x predicted X ray images, and for from every pixel that is about this size of this square here or this square here, you can get amazing spectra that will tell you about the dynamics and the chemical composition of these things.
08:27:51 This is amazing in nearby objects but also the capabilities that you have now will allow you to start the evolution, up to register one of the metal contents of the kinematics, and so on and so forth.
08:28:06 of these objects.
08:28:09 Now, Athena was actually not built on the science case of the CGM, and I dug and dug and dug for some predictions that would be able for me. Me to answer the question that I know that you guys have and the question is What colors do not do for the CGM
08:28:24 and how far into the CGM can we possibly got.
08:28:29 I didn't find a publication.
08:28:31 But I did find a participant of this workshop who happens to be next door to me in London, and who was kind enough to share with me a work in progress and made sure to tell me to tell you that this is preliminary and you should really take it with a grain
08:28:45 of salt.
08:28:47 So here we are. These are the little So, first of all, in color, the lines are predictions from the ego simulations for the brightness of some representative lines in x rays okay so this is all 789 10 and magnesium 12.
08:29:05 And so four different halos of different mass, you can see the, the median or the main predictions for the brightness of these lines.
08:29:14 Here you see the limits that you can get with Chris.
08:29:18 So with Chris I'm you can get down to flux of about this much.
08:29:22 And here you see the limits that you will get from the few, and the long and the short of this is that if you are interested in 10 to the 12. So, L star kind of halos with Xi few you can get to, again, a few times of kilo per sec.
08:29:39 If you really push it, you can go to maybe 100 but that's going to be quite difficult but this is for individual emission lines one by one and this is a five sigma limit.
08:29:52 So, if you combine detections in many different lines. You can go. I would say easily to 100 kilo per sec, but beyond that could be a little bit hard.
08:30:03 Okay, so that was Athena, I want to tell you there is one more mission on the horizon that I have been told is now an official project of the Chinese space agency.
08:30:16 And this is going to be amazing so Hobbs basically goes in this parameter space I was talking about, to a different
08:30:26 trade off the trade off is that helps has the exact same number or very similar number of pixels as a female, but instead of pushing for spatial resolution they have pushed for a very large survey speed.
08:30:39 So this is by far the highest grasp mission, that is a microcosm with our so you can study you can serve a big parts of the sky with the resolution of a micro calorie answer and Junko here has a very nice plot that shows you why it's important to do that,
08:31:03 because the line emission from the CGM. It's very important to have this resolution to disentangle it from emission lines from our own galaxy so I think for the CGM at very very low redshift This mission is going to be the thing to watch out for.
08:31:17 Right now we're getting into, you know a little bit less certain terrain. We are all of it, awaiting the results of the 2020 Cato survey. And actually, we I haven't heard axis mentioned at all in the future observations channel on slack this week and
08:31:34 we should talk about it.
08:31:36 Because access is actually could be quite exciting for the CGM.
08:31:40 The main points of axis is, it's the of all of the images I've talked about so far axis is the first one that actually has Chandra resolution. Everything else would have worse resolution that Chandra that we're talking about so far.
08:31:55 And it will have by far the lowest detector background detector background was not one of my five things because I didn't want to burden you with it, but detector background is very important for pushing things to very low surface brightness.
08:32:15 So the goal of axis is to push things to 50 to 100 times fainter things, then the limit of Chandra, so if you want faint the mission, you should be paying paying attention to this proposal.
08:32:24 And the thing that is on everybody's radar that we have been talking about these links. And so this is proposed for 2036 links has again, kind of like Athena, it has two main.
08:32:37 Well, I started one I will talk about in a minute but two main things on board.
08:32:42 One is a micro calorie meter. There's actually two flavors or three flavors but let me talk about two flavors of this micro cut calories are one is the is the main array of the micro gallery matter and that is this purple seeing here, the really exciting
08:32:57 stuff for CGM science, though, is the ultra high resolution sub array of this micro kilometer and that is the yellow square over here, and that would finally finally put us into the resolving power of more than 2000 at, oh eight.
08:33:18 Okay, at the lines that are bright, in the case of the CGM the dominant emission lines of the CGM, so we can finally do dynamics of the CGM in especially resolve way with this ultra high resolution submarine.
08:33:34 And then the high definition X ray imager. This is a CCD so it doesn't have great spectral resolution, but it will have the spatial resolution of Chandra, with of course a much larger affected area and service be.
08:33:49 There's I don't have time to tell you how many amazing amazing things things is going to do but hopefully Alex a reclaiming will be with us today and he's on the panel so please direct your questions to him.
08:34:02 What I want to leave you with in terms of the emission where I want to conclude, is this plot. And this is a product of collaboration initiated during this character up workshop and so we've been discussing this with Ben john and Natasha, and the credit
08:34:19 goes to band for producing this wonderful cloth that compares the same simulated Halo as it would be observed by Chandra Rosita Athena Whitefield imager and links, HDXI, and this is a 10 to 12.4 So log of em 228 am 200 is 10 to 12.4.
08:34:41 And the Reggie point or one and all of these are 100 kilo second observation is if you're not an extra astronomer This is about one day of time and this is how our view of the CGM and that mission is going to evolve over the next sort of 1520 years.
08:35:00 Now, even though we are getting you really further out in radius, you can see all these beautiful details. Nevertheless, we are all aware that eventually a mission gets to faint.
08:35:12 And if you really want to push to video read the eye of these halos, you probably also need to do absorption so let me spend the last five minutes of the talk telling you a little bit about what we do in absorption.
08:35:25 So, again introduction where we are right now.
08:35:30 Is this side of the plot. So, these are observations of bright X ray points sources with the XML neuter RTS.
08:35:38 And these are oh seven absorption lines from our own galaxy, okay this is milk, milk you absorption. And basically, these are about one week of staring at the single point source and in one week of staring at a single point source you can get a log n
08:35:57 o seven have about 60.
08:36:00 of about 60. And that's what no seven of 16 looks like when you look at it for a week now where we would like to be is more like maybe 15, so these are again predictions from Natasha for this is also been in absorption from ego.
08:36:19 And if you want to look at the veil radius of attend to the 12 solar mass Halo, you need to be around here okay so 10 to 15, if you want to look at more than a single line, if you want to catch not only have seven, but some of the next three brightest
08:36:34 ones.
08:36:47 Then, oh a neon 10 and I run 17, you would need to go even below 10 to the 15 okay so that's our goal, 10 times but how are you going to get 10 times better with current instrumentation, the only thing you can do is stalking, again, and I want to show
08:36:53 you this very nice result from cobalt and collaborators and what they did is they use the Chandra le tg spectrum, and they looked at this guy, you know, telephone number age something and they know that there are 17 lyman alpha absorbers within a certain
08:37:12 distance of these points or that we're looking at an X ray So what they did is they took the observed spectrum with Chandra, and they blue shifted it 17 different times to the corresponding graduates of those 17 lyman alpha absorbers, and they stack the
08:37:27 the spectrum, 17 times well, different parts of the spectrum 17 times, and they report about the three sigma detection of oh seven absorption.
08:37:38 That is what you see here, and that corresponds to lock and observant of 15. So we are where we want to be but in a stock not an individual systems.
08:37:49 If you want to do better for individual line detection not for a stack, you need new thoughts. And here is a cheat sheet for the new toys that I think are are on the, on the horizon.
08:38:01 And let me explain the axes here so here is the resolving for power and I'm plotting this for rest frame oh eight.
08:38:11 For restaurant Oh, oh seven you should probably move the the white the circles a little bit more to that.
08:38:19 Um, so, what we have here in red, our micro color emitters in blue or white are great things.
08:38:29 And the solid symbols are approved and the empty symbols are proposed missions and hear what you are seeing is the figure of merit for week line detection so this is how efficient.
08:38:50 How much more efficient one of these missions is compared to the other ones if what you are looking for is, we now you want to be over here, right, because we don't.
08:38:54 So, the higher you are on this axis, the more efficient you are at just finding the line say hey there's a line here.
08:39:03 But you also want to measure dynamics from this.
08:39:08 You also want to measure dynamic strongest line.
08:39:11 Okay, so if you want to easily resolve 100 kilometer per second line broadening you need to be in the green regime.
08:39:19 So this is where things stand. You know, this will be available so you can stare at it later.
08:39:25 Let me give you some numbers for these proposed future missions, but they can do for you.
08:39:33 We've heard the Randall say several times that our course is planning to probe in a two year mission 30 lines of sight to get 100 or seven detections down to 3 million strong so this is basically the outer part of a star Halo.
08:39:51 If you look at a phoenix I feel we have two objectives, the first objective is to find out well when filaments but honestly, this could just as well be the CGM, you know absorption.
08:40:03 150 detections towards be Alex and 50 detection Stuart's bright Jeremy after glow so that gives you 200 detections of these emission lines.
08:40:13 And the other objective which is very interesting is that towards these Jeremy after glows. Once the afterglow has faded away you can stare at it and you can detect the same gas also in absorption so that would be very cool.
08:40:25 And then we have links and links will observe at the goal is to observe at AGM to characterize the hot halos beyond the variable radius in 30 galaxies, with a mass around the again I'll start so these are the number of detection is that you might expect.
08:40:44 This is really beautiful cloth from the links concept study report that you can also stare at.
08:40:51 And so the limits for links are this black contour over here.
08:40:57 So, out to this country you can detect absorption lines and that is going to be of course, really amazing.
08:41:05 One plug slide for a really crazy thought that proposal that I submitted to the Aesop 2054 So I'm now taking us, not 20 by 30 or 40 years into the future, which is this proposal to have it all.
08:41:23 Okay, so to have really huge effective area really good spatial resolution excellent spectral resolution for these low emission lines, and a million calorie myth or pixels so millions Paxos for this detector.
08:41:41 Millions Paxos for this detector. And what we would like to do is to do a survey in a mission and in the survey. The survey will be sensitive enough to go to the rural radius of an all star Halo as part of the survey that will cover thousand square degrees.
08:41:54 And the other really crazy thing that you can do is that you can detect things in absorption, but not an absorption against point sources but in absorption against the cosmic web.
08:42:06 Sorry, against the X ray background. Okay, so you can take any point source out of the X ray background you have a bunch of points sources in our field of view, no matter what, you can stack all of them, and you will be detecting absorption from the cosmic
08:42:20 web at the same time as emission really crazy thoughts for the far future so I'm out of time so I want to leave you with my summary and my summary is a compilation of all these ranges of parameter space that we are hoping to probe in the near future.
08:42:37 And what I would like to see in the discussion after that is, we have this huge parameter space opening up, I think we should be prepared for surprises.
08:42:47 And I would like us to discuss what we think those surprises might be. So thank you very much.
08:42:57 Thank you so much Aurora, I'm so much to be inspired by right now that was absolutely excellent.