08:05:08 Good morning, everybody. It is 8:05am, and we are ready to get started with week two of our program fundamentals of gashes halos, and I don't know about you but I am feeling rather energized after last week we have a lot of exciting plenary events and 08:05:34 store this week which I will review just very briefly, But first I want to mention. 08:05:41 If you have not already, please go ahead and join the dedicated Slack channel for this week's discussions. And so it's not held 21, as I have written on this slide is Halo 21, of course, all of our channels begin to Halo 21. 08:05:59 And this one is Halo 21 week to multi-phase. And if you don't know how to find a Slack channel go ahead and find those three vertical dots next to the candles menu on your slack view, and then click Browse channels, and all of the handle channels beginning 08:06:19 Halo 21, you're welcome to join. 08:06:22 But this particular week we're going to use a dedicated channel Halo 21 week to multi-phase for slack discussions and more on that in a minute. 08:06:33 up today. We have a very exciting keynote speaker This is Professor Todd trip from UMass Amherst. 08:06:43 Sorry, Amherst, there's no h Amherst. 08:07:04 Ron mon borderline Dr. Sanjay for the current Dr. Gwen Rudy, along with Todd and moderated by myself and what I'm going to do as moderator is kind of interface between the Slack channel, the week to multi-phase Slack channel, and the panel and kind of 08:07:20 feed them questions that are generating some discussion from the slack page so please use that slack space what's nice about slack is it can preserve any discussions any questions. 08:07:34 Beyond this plenary session, you can thread, you can react with joy, or other emojis as you see fit. But before we do the keynote talk I just want to make a couple very exciting announcements. 08:07:52 First is that I have managed to secure jet city trivia which is a Seattle company that does pub trivia, obviously they're not doing pub trivia now they are running online virtual trivia nights and I have heard rave reviews from a number of my colleagues 08:08:08 at the University of Washington who have used this company to run their virtual trivia nights, they've agreed to host a halo 21 trivia night for us, for our entire workshop, and this will be Friday January 29 4pm pacific time it's a 90 minute event. 08:08:27 It's BYOB anybody living in your house with you, your cats, your kids, your spouse, welcome to join on your zoom screen, and I think it will be a really fun, kind of, I don't know camaraderie building team building event will play in teams on the trivia 08:08:47 night and it's it's just, it's not an adequate substitute for things like conference dinners and going out for drinks after a conference but it's something, and I'm really looking forward to it and so I hope that you'll all consider attending. 08:09:03 If you join the Slack channel Halo 21 dash socializing, that's where I'll post the zoom details. I'll send them by email ones. 08:09:15 But yeah, I'm really looking forward to that. 08:09:17 I also am very excited to announce that our YouTube channel for featuring four minute new results videos is up and running things, primarily to Cameron Hummels, who has posted not only a welcome video, but also a video telling you how to make a video, 08:09:38 it's very meta. 08:09:41 And, and there are already a few. 08:09:47 Beautiful, beautiful four minute videos that are on this YouTube channel so you know you've, you've already watched queens Gambit you watch that dumb movie with George Clooney who was an astronomer, you're sitting at your TV, you load up YouTube and you're 08:09:58 like what am I going to watch tonight fundamentals of gases Halo subscribe to this YouTube channel and you know you've got loads of new entertainment options at your fingertips. 08:10:11 And these are four minute videos, join the channel Halo 21 new results to see the videos that are uploaded. Sometimes people will post links to the accompanying papers and any discussion of these videos. 08:10:23 I really what I would love to see is, these if people watch these videos this week, incorporating some of these elements into maybe the discussions on Friday. 08:10:35 But this is this is a great new element of our asynchronous workshop and so the, the people who were able to get videos up last week I'd like to feature. 08:10:47 We've got Ezra Hutcher we've got Matt wild Hitesh dos Stephanie Whoa, and Sharon way posting a range of videos on a range of topics, and they're all absolutely excellent so I really highly encourage you to go four minutes I think is kind of the sweet 08:11:04 spot to in terms of like, it leaves you wanting more. But it gives you enough to really, to really appreciate the work. 08:11:13 Alright, so this week. We are also featuring two conversations, and you don't, you're not going to get the normal introduction like we'll do on Monday, but we'll hear from them on Friday, and that's Halo 21 SZ CGM and Halo 21 precipitation and, and they'll 08:11:33 be spotlighted on Friday. But if you're very if you're interested in precipitation. If you're interested in the sZ effect and it's a, you know, potentially transformative ability to study the circle galactic medium, join those channels participate in 08:11:50 the conversation, and we'll give an update on Friday and I know I'm also tutorials, speaking of precipitation. 08:12:00 Professor critique Sharma is going to give the first tutorial on Wednesday on precipitation will do a multi phase cloudy modeling tutorial immediately afterward will do a multi phase turbulent ASM analogies with the CGM tutorial, and then a synthetic 08:12:17 X ray observation tutorial. And so there are four tutorials on Wednesday. Again, these have staggered start times. They're all recorded and I also want to acknowledge you know we know that this is the day of the inauguration of the 46 you US president. 08:12:33 So for those of you who want to watch that in real time you can come back, watch the recorded tutorials, also after every tutorial there's a breakout that you can go and join a longer discussion. 08:12:46 Okay, so that's Wednesday, Thursday, I will have our second keynote speaker, Dr Drummond fielding from flat iron CCA, followed by the expert panel, featuring max Franchi Ivan Schneider critique Sharma and Jonathan Stern, so I really hope you can tune 08:13:03 in on Thursday. 08:13:06 And finally, I just want to run through a few quick slack tips, because we did look at your survey responses and notice that a number of you really self identify as slack newbies. 08:13:21 So a couple things to make your slack experience, enjoyable, and it one is to edit your profile that slack icon, like it's really hard to tell who's talking when you just see a bunch of little circles with like disembodied torsos update it put a picture 08:13:38 of your face you know this is one of the things we're interacting asynchronously it's really nice to see what the person you're interacting with looks like. 08:13:49 So, uh, so yeah or put a picture of a penguin or something but this is what people will identify with you your icon, edit your profile. You can also include your name pronunciation if it's not vs. 08:14:02 You can include your pronouns, you can include your affiliation. 08:14:06 You can also a knot in your profile that there's a separate menu to change your preferences for how you're getting notifications on slack. 08:14:17 All right, here we go this is you browse channels. join interesting channels. 08:14:23 Like I said, this week Halo 21 week two multi-phase but you can go ahead and browse and you can see there from my slack view there's Halo 21 Milky Way metal a city there's a million different channels that have already started. 08:14:35 And you are absolutely welcome to join those channels and participate in the conversations and a couple other things for organizing your slack experience. 08:14:48 So do you see this little this little pin right here. If you click on that you'll get to see pinned pinned messages, and these are messages that are particularly important in Halo 21 week one Halo mass we pinned or Siobhan pinned her talk slides. 08:15:06 And then there are Megan's talk slides there and just like the key kind of things that you might want to scroll back to and find just for further reference. 08:15:15 That's access just by clicking on this pin here. Another thing that I want to highlight that we started doing really well during week one is threading. 08:15:24 Okay. And so, you know when makes a very salient comment about abundance patterns in the CGM, and then you can click down here to reply to just the thread and you would see the thread over on the side, you can react with. 08:15:40 Thank you so much. You're clapping or whatever so use emojis a thread University responses. 08:16:05 Even if you are next level, add your own emoji. Some people are adding these kind of bespoke emojis I think Joe Birgit added slime that had to be Joe Birgit somebody added a cool CGM graphic. 08:16:00 So, so, you know, you're welcome to do this and just make this experience on slack as meaningful as possible. 08:16:12 Okay, so now I am very pleased to introduce Professor Todd trip, and He is a professor at UMass Amherst since 2003, and I noticed that he has been publishing papers on UV spectra since 1990, his his first paper is using IUE data in 1990 and, and he has 08:16:40 been doing absolutely crucial work on the CGM since them for more than 30 years, and I am very happy to introduce him as our first keynote speaker this week. 08:16:56 Take it away, Tom. 08:17:00 Alright, actually see us. This is a little funny thing. 08:17:06 There we are. Can you see my screen. Okay. 08:17:10 All right, now I also want to turn on this little do Hickey here. 08:17:16 All right, super well I have to say. 08:17:19 This meeting is really neat. I mean don't get me wrong I I'd rather be in Santa Barbara than Western Massachusetts in the middle of mass, you know, January, but I'm quite impressed with what the meeting organizers have done with all sorts of interesting 08:17:35 conversations erupting online and virtual face to face conversations and videos and it's just been spectacular so I'd like to start by thanking the organizers for inviting me to participate in this workshop, which has been really fun. 08:17:52 And I've learned a lot. 08:17:53 So when I was thinking about how to put this talk together I was reminded of interview that Bill Moyers did with Jon Stewart, the famous Daily Show, and at the interview. 08:18:11 At the end, Stewart said well you know i just advanced the script. I have so many talented people around me, I just advanced the script and they take it from there. 08:18:17 So, that's kind of the attitude that I adopted with this talk was I'm just going to put up some things that I find interesting. And there's so many really interesting and creative people in this workshop that I expect you all. 08:18:32 We'll take it from there. 08:18:33 And probably my most important charge is to introduce this week's celebrity guests, which is of course German feeling fielding who will be doing the talk on Thursday. 08:18:45 German does great talks and is doing really interesting work so I'm just trying to sort of set the table for Drummond. And along those lines. I have a pretty talented team that I've been fortunate enough to work with now let's see why is that not advancing 08:19:01 my slides. 08:19:03 Here we go. 08:19:05 So I should give some of these folks credit I will try to put up the names of people on involved with specific papers, but I want to mention the Cosby team. 08:19:15 In particular, because they've really helped out with many parts of the work of my own that I'll be talking about. 08:19:22 Okay, so here's kind of a crude outline of what I want to try to talk about very generally first of all I'm going to make some kind of annoyingly dig deck tactic and sort of finger wagging comments about the importance of spectral resolution. 08:19:39 and then I'll try to do kind of a little whirlwind tour of different results related to multi-phase gas. 08:19:50 And my goal, if I succeed is to bring up some of the challenges that are emerging from observations and maybe share some information about the kind of constraints that observations might provide for testing, and all the exciting theory that's rapidly 08:20:08 developing in this field. 08:20:10 So I guess I feel like I don't really need to motivate this too much but I suppose I should a little bit. I think it's pretty easy to explain the big picture importance of the circle galactic medium and specifically multi phase gas. 08:20:28 You know, we can for example, think of the Mahler and Bullock paper. One of my colleagues in the theory group in my department has steam start to pour out of his ears. 08:20:39 Whenever I bring up this paper, but it was at UMass when he wrote this paper and I think he'd kind of viewed it as a sketch of the broad ideas and and that way it's a really nice paper. 08:20:51 And one of the main points I suppose that this paper makes is that if you want to explain a big problem, like the discrepancy between the observed galaxy luminosity function and expectations from CPM cosmology, well you know you can invoke. 08:21:10 You can invoke supernova feedback on the low mass and and you can invoke a gn feedback on the high mass and this is a little funky I suppose I need to swing this around here. 08:21:24 But. Alternatively, you could explain some of this as the way that gas cools, in a multi phase situation it's possible that much of the gas just as never able to cool and descend into the galaxy, so that it can fuel star formation. 08:21:42 So understanding exactly how gas cools and the physics that occurs as it descends into a galaxy is an important problem. 08:21:52 Now, even if you do prefer oh yeah and I guess just so I don't catch up from cats I'll make sure to put up one of his famous papers which is of course do Sean's wonderful paper on how galaxies get their gas and you know if you have cold the creation and 08:22:08 accretion and all sorts of things that's likely to be multi-phase as well. But even if you do want to use feedback of some sort to solve this problem you still have to understand how the outflows launched and how the mass and energy couples with the CGM 08:22:27 and the micro physics and there's just a lot of different interesting theoretical aspects that almost always involve multi-phase gas in a very fundamental way. 08:22:39 So, my purpose here is to just show you a random sampling of observations or, you know, observations that are interesting to me. 08:22:49 So, starting with what I know about. I'd like to just make a quick comment about how theorists are working with ultraviolet and optical absorption spectroscopy. 08:23:02 So what I've noticed is that many of the theory papers are trying to fit. For example, the cost halos data, which is total column densities particularly of oxygen six, and the circle galactic media of galaxies. 08:23:17 Know the comment that I'd like to make is that, that's a wonderful first step toward understanding the CGM, but there's a lot of information that's left behind. 08:23:27 If one is only working with these total column densities these things have complicated components structure and variety of ionization stages are detected in the various systems, and there's a lot more that we can do so so this is nice but I hope that 08:23:45 theorists will start to dig into the data, and look at some of the more detailed issues as well. And of course, along with this comes the responsibility for observers to explain the limitations of the data the noise the systematics and so on and so forth. 08:24:05 And I mean I think theory really demands that observers do this because a lot of interesting work is racing ahead and I sort of feel like we're getting behind a bit by not drilling down and working out some of the details that we can report from the observations. 08:24:25 So I want to try to get into that some of that today if I can. 08:24:30 So, one way to frame this perhaps is to just start with a simple question that Max and pain post is multi-phase gas cloudy or misty. 08:24:43 Now to start here my somewhat snarky and finger wagging comments. 08:24:50 People are very excited about the cosmic origin spectrograph and the data that it's producing and rightly so, because it's very good data and it's opened up a lot of windows for observing the universe using ultraviolet spectroscopy, but it does have its 08:25:07 limitations and I just want to make sure that those are on the table here. So, on the screen. I have actually an excellent cost spectrum that says signal to noise of 42 one per pixel So, so this is about as good as the data get from costs and you can 08:25:39 a couple of absorption lines here you see we have a silicon for absorption feature with, obviously multiple components and adjacent to that we have alignment alpha line from a different redshift and again we see well there's clearly several components in those absorption profiles. 08:25:42 absorption profiles. But we need to understand what we can learn from these data and what might be missing or not appreciated. 08:25:52 Now this is a little bit political I suppose, but I think it's fair to point out that if we were to use a current X ray spectrograph to look at the same absorption lines you would see something like this. 08:26:04 In fact, these are real data with about the resolution of current X ray spectrograph future X ray spectrograph will be better in terms of resolving power, but ultraviolet and optical spectroscopy will always be more orders of magnitude better than X ray 08:26:20 spectroscopy in terms of resolving power so we should bear that in mind you know we just need to understand what we can do and can't do with one type of instrument, or another. 08:26:29 But getting back to the cost data, you know, we might be interested in this so it conforms to numbers so we might say, but well let's compare it to the silicon to that we detect at the same redshift and we might take a particular interest in this component 08:26:43 over here, which seems to be lined up in these two ions of silicon and you know we could do what I like to do which is to convert the exponential absorption profile into a linear apparent column density profile where we just take the optical depth than 08:27:01 each pixel, and use it to calculate a column density. This is advantageous because then we can scale different profiles to see how their shapes compare and we can search for unresolved saturation and me, it needs to just very handy thing so I'm going 08:27:15 to show data like this quite a bit in this talk. So we might look at this and we might overlay the silicon to and so looking for and notice Oh, well this is a pretty nice component here. 08:27:28 The two components have the same centroid. They seem to have the same line with but you know it seems like it's co spatial gas so we can take the silicon to to Silicon for ratio and we can pull up your favorite ionization model and figure things out, 08:27:45 and this will just be swell. 08:27:48 But here's where some of the unpleasantness starts to emerge. I have actually observed this Quasar with a variety of instruments over the course of my career. 08:28:00 This is 818 21 plus 643. 08:28:03 And I've recently observed it with the E 148 mode of the Space Telescope Imaging Spectrograph, which provides a resolution of 2.5, kilometers per second. 08:28:15 So it's interesting to compare what we had previously with status at seven kilometers per second to what we get from costs, and so let me show that to you. 08:28:24 So the top panel here shows the costs silicon for profile and you can see the components and you know there's kind of a shoulder over here. 08:28:33 When we get a little better resolution with each 140 m mode we see well this shoulder here actually resolves into two components clearly and, and we can see a lot of other components structure at other velocities. 08:28:47 And then when we look at the same profile at two and a half kilometers per second. We see even sharper. 08:28:55 Little noisier this time because this is expensive and you can only get so much Hubble Space Telescope time but we see sharper profiles, and we can see that we'll be able to do a better job of measuring the component to component properties with this 08:29:09 high spectral resolution, but some of you out there might be saying, well, This middle panel is basically like what you get from Kak or the VI lt with Michelle spectrograph and then you know it's good enough. 08:29:22 And so yay tech winds were all said we don't need to worry about this business of higher spectral resolution. But let me show you some more of the data that we got with steps. 08:29:33 Okay, let's see how come that's not advancing There we go. So, that's the silicon for. You can also look at this this silicon to profile and compare it to what we saw at seven kilometers per second resolution. 08:29:48 So what you see is that a feature that basically look like one component, and then when you maybe there's there's sort of a little funky thing here but a lot of people would look at this and say oh it's just one component and fit it that way. 08:30:01 When you look at it with better resolution it resolves into five discrete components. And those are real. And we see them out in other species we see them and overlapping orders. 08:30:12 There's no doubt about the reality of those components so spectral resolution is important, and we need to bear this in mind when we're comparing things you know for example in cost data. 08:30:25 Alright. So, 08:30:28 for example, if we want to ask, Is this a shattering cloud, which is an idea that there is to become interested in lately. 08:30:39 Well, looking at it at seven kilometers per second, we might not really get a lot of insight about that, but when we see this with better spectral resolution it does start to look like something, one might expect. 08:30:52 In this theoretical situation. 08:30:56 Alright, so why is this important Well, let me push on and show something that pertains to the discussion that broke out over the weekend regarding medalists at in the circle galactic medium It was really has kind of an interesting conversation people 08:31:19 Well, yes it's pat you know the metal is city it's not meaningful. Who cares, you kids get off my lawn. But it's not just the middle Listen, there's a lot of diagnostics, in comparison of different ion so for example if we look at, at this particular 08:31:32 example, we see we have a couple of oxygen six components down here, one component lines up beautifully with very strong h1, and the other oxygen six component, which has more or less the same oxygen six component column density lines up with a much weaker, 08:31:52 and probably broader component. So there's a lot of stuff going on here from one component to another and understanding that it seems to me, is quite important for understanding the physics of the circle galactic medium. 08:32:07 Okay, so let me just make a few quick comments about what can happen if we're not careful with spectral resolution so here's the same profile. Here's what it looks like at cost spectral resolution with good signal to noise and you might say oh well, you 08:32:22 But what happens is that when you do that and you compare the results from the higher resolution data to the lower resolution data you find Well, the values can be off by a factor of two, even column densities in one component or another can be off by 08:32:45 a factor of two. So that's troubling X was saying well I don't think we can measure medalist at to a factor of two. Well, we might not be able to measure column density is to affect for two. 08:33:02 So that's even even worse situation and one has to think about these things now, it usually turns out that the total column densities. Some over these components are in agreement and, and the recordings at the different spectral resolution. 08:33:13 But here's some more insidious problem. Oh, I'm missing the slide. 08:33:18 Well, let me just speak the words this is very good data. If we were to look at, say just one exposure on this Quasar we'd have noisier data. And then this thing which you can kind of see well there's three components and noisier data. 08:33:35 It looks like it's just one component, and it will look like the centroid is different from the centroid of the each one, and we end up, reaching specious conclusions. 08:33:46 Okay, so now I want to push on to looking at multi phase gas in a couple of different situations and I would start want to start with gas in inflows. 08:33:58 So inflows are kind of hard to observe because oftentimes it's hard to determine if the gas is influencing or outlawing some situations you can be confident that it's influencing For example, this is a paper by Kate Rubin, where it's a down the barrel 08:34:15 observation of some galaxies where the kinematics of the absorption that's detected indicates that it's influenced, so that's quite nice. But galaxies or faint and sometimes there's limited information. 08:34:29 So in this case, Kate was able to get magnesium to an iron too. 08:34:34 Well, it's hard to work with just magnesium to an iron too I know lots of folks here love magnesium to. 08:34:41 But, this stuff is typically optically thin, there's a large ionization correction that's required magnesium can stick to dust there's a medalist at issue with only magnesium to it's hard to make a lot of progress on a lot of the questions that we're 08:34:58 interested in, so we can you know we'd like to be able to get more information. 08:35:03 So, Stephanie Whoa, and crystal Martin and her team have done some very nice work on evidence of influencing gas by looking at how magnesium to velocities compared to rotation curves of edge on galaxies, Chuck style had done this, some years ago, but 08:35:25 this team has really followed up and done a wonderful job of, of, sort of, understanding the extent of the influencing gas and its kinematics and, and it looks like there is either evidence of inflow or, you know, I read dropping rotation curve. 08:35:42 I highly recommend these papers and in fact Stephanie has a nice little video up for this workshop where she's commented that one has to be careful about looking at where the magnesium to is with respect to the minor access or the major access because 08:35:59 sometimes there's confusion from magnesium to that's actually affiliated with other galaxies so that's a nice little video, and it just illustrates how this workshop is really functioning in a wonderful way. 08:36:15 And, you know, various teams and groups have done this Dave bone has looked at multiple quasars behind NGC 1097 and his team also concludes that in absorption. 08:36:29 They see a much larger h1 disc, which seems to be rotating in the same sense as the 21 centimeter and the starlight in this galaxy, and yet there seems to be a requirement of an inflow component. 08:36:44 So there's a lot of literature on this and I apologize, I won't be able to mention everyone's literature, obviously but lots of great work going on. 08:36:52 But I think maybe the most interesting and informative place to learn about inflow is in our own backyard, because we clearly have some influencing objects. 08:37:05 We have a lot of detailed information. 08:37:08 So we have the high velocity clubs, we have the Magellanic stream. And in this case we can say without any doubt that these are multi phase entities. 08:37:19 This figure from sandbox at all, shows the 21 centimeter emission. 08:37:36 And contours are the you know the color scale. And then these little circles show detections of oxygen six absorption with the ultraviolet spectroscopic Explorer, and the color inside the circle indicates the velocity of the oxygen six absorption multiple 08:37:41 colors. Reflect multiple velocities and different components. And we can see that the oxygen six absorption. Overall, follows the kinematics of the 21 centimeter emission. 08:37:53 Even though the absorption is more extended than the emission that probably tells us that these high velocity clouds have ionized envelopes, which isn't too much of a surprise. 08:38:03 But we see a lot of things going on and it's not just oxygen six we detect a lot of different ions, when we look at quasars behind these high velocity clouds. 08:38:15 So I'd like to now talk just a little bit about some of my own research. 08:38:22 The high velocity community has a tendency to take this structure and snip out a big piece of it, and only live leave that kind of tip over here indicated and in high velocity cloud maps like this. 08:38:37 That's because this thing which is unfortunately referred to as the outer arm. 08:38:43 I think it can't possibly be affiliated with the true outer arm doesn't quite deviate from rotation velocities as much as the high velocity cloud people would like it to, but I have argued that these things are related. 08:39:02 For various reasons they have similar kinematics, they have similar medalists at ease. And they have similar distances so this outer arm thing was constrained a few years ago by later and how cou looked at a star at a distance of 15 killer parsecs and 08:39:17 clearly detected that structure and absorption and complex see up here has a similar distance from papers by Walker and Chris Tom and collaborators. So these things are at similar distances they're actually not that far away. 08:39:34 Here's the spectrum from Nicola and Chris, and you can see that the outer arm itself is quite nicely detected. It's interesting to note that there's an array of ions ranging from oxygen one up to carbon for that or cinematically aligned and then there's 08:39:49 also this high velocity part. 08:39:51 I had dubbed this to high velocity Ridge in the paper from 2003. This is also seen in 21 centimeter in mission. so it does appear that the high velocity rich I should say is in the complex see and also in the outer arm. 08:40:10 So the kinematics are similar for both of these structures so what I think is, these are some kind of inflow in the Milky Way. They're not that far they're probably now interacting with the is there decelerating so the high velocity Ridge might not have 08:40:27 They're decelerating so the high velocity Ridge might not have decelerated as much yet, and the lower velocity stuff is slowing down. And it's flowing into RISM and it gives us an interesting laboratory for looking at the physics of gas clouds interacting 08:40:41 with a more dense, I assume. 08:40:44 So recently I, as I said, observed this Quasar age 1821 plus 643 with this ultra high spectral resolution, with steps. 08:40:54 This cloud has some advantages over many Quasar absorbers its location is constrained. So, we have a pretty good idea about what the shape of the ionizing flux field and the intensity of the ionizing field will be we start when pointed out, we often don't 08:41:11 really know that in Quasar absorption studies. And so we have an ambiguity it's either. The ionizing photon density or it's the particle density or both and you can't really distinguish but it's sort of nice in this situation, because the, the ionization 08:41:28 is reasonably well condemned. 08:41:32 Okay. So these are the data that I showed a few slides ago. So what can we do with these data. Well if we if I can show one of these apparent colon density comparisons, we see that the low and compare pretty nicely as we might expect, and we can look 08:41:46 at ratios in different components and use that in ionization models, but it's also interesting to compare the low ionization absorption to more highly ionized species so in these panels, black shows the silicon for, and then I compare it to various things 08:42:03 in the other panels silicon to carbon for oxygen six, and on the, on the right side it's just been a little bit to show the features more clearly so we can see for example on this component three and component for the silicon for the silicon two profiles 08:42:20 look quite similar in fact similar centroid and similar line with the two and a half kilometers per second resolution. 08:42:28 On the other hand, the carbon for recorded at the same resolution but with a little more noise, and the oxygen six with lower resolution but still 15 kilometers per second. 08:42:38 Do not show those peaks those clear components these things to be seemed to be smoother broader profiles. And yet, there's clearly a relationship between the oxygen six and the carbon form these lower ionization stages when the lower end stuff climbs 08:42:55 up, so too does the high iron absorption. 08:43:00 Okay, so what does, what does this mean why I think it's actually pretty interesting to explain how is it that the highly ionized species like oxygen six kinematic Lee correlated with lion ization stages, like so it can do they have no business being 08:43:19 together the ionization to the energy to destroy silicon to as far lower than the energy needed to create oxygen six. So, so what's going on. 08:43:31 Well, let's just look at some more details here we can run ionization models so I've done that here. And it looks like there might be a need for a little bit of depletion in this particular component because when I fit. 08:43:48 Say I try to fit everything as best I can I find there's too much sulfur to in the observations, so if I just the model, so that I get the software to write the purple here, then I would have the wrong amount of silicon to an iron to, well that can be 08:44:05 solved because silicon to an iron to stick to dust. And so maybe the silicon to an iron two are mildly depleted. 08:44:13 But looking at this, we also show the silicon for and black the carbon four and the oxygen six, and as I said, we don't expect these things to have anything to do with each other and yet the silicon for in particular has the same components structure 08:44:29 in this, in this component so what's happening. 08:44:33 Well, maybe it's something like what we talked about last week, where the, the gas is thoroughly broadened and the things like carbon for silicon for our broader than the so carbon foreign oxygen six are broader than the silicon for because of the different 08:44:52 masses. So I tried doing that and that works You can, of course, so if the carbon four and oxygen six or broader they'll be more smeared together and you'll get a broader profile. 08:45:03 So you can fit the data that way and you get fits that look just fine. But when you look at the ratio is it kind of falls apart so the red here is what I measure for Oxton six the blue is carbon for and the black is silicon for and this is the temperature 08:45:20 implied by this silicon Ford line with, and the ratios are all wrong, you could you could fiddle around with this but it's pretty much becomes unconstrained pretty quickly. 08:45:31 So I'm not sure that just invoking thermal broadening of the lore mass species works here. 08:45:39 So, what's happening. 08:45:42 Well it's interesting to look at what these ionization models and apply again the plan is in flux intensity is constrained so we get some constraints on the density. 08:45:54 That looks like the density and the log is something like minus point seven to minus point three total age column density about 10 to the 19. And so these things have a cloud thickness of 10 to 15 parsecs. 08:46:07 Now there are some systematic uncertainties, you know, the fox at all model of the flux coming out of the Milky Way has some uncertainties I haven't put all that in, but I think these give you a ballpark sense of the dimensions character of these little 08:46:24 little clouds. And so, a question for theorist is, does this look like shattering, or does this look like precipitation or turbulent mixing layers or whatever you like. 08:46:37 I know I think this is the kind of detail in the absorption data that I'd like to see theorists looking at more and more. And this might require simulation so Cameron's demonstration of how to use Trident might, you know that might turn out to be very 08:46:54 relevant. Okay, so maybe I should push on to some other things time is marching on multi-phase gas and outflows is much easier to observe and it scene and all sorts of places and of course everyone loves the poster child in 82, which is the cigar galaxy. 08:47:13 Now the exploding cigar galaxy it seen x rays we have dust detected with Spitzer there's molecular gas and the outflow. And of course the famous optical emission lines that revealed this by conical outflow in the first place. 08:47:28 So that's a pretty spectacular galaxy there's a lot of literature, I'm not going to talk about it too much but it's clearly multi-phase. When issue though is that emission goes as density square and it quickly becomes hard to detect and mission as the 08:47:43 density goes down so often these things, show us what's happening in the innermost CGM but we don't really know what happens is this stuff flows out, in a way, from the desk. 08:47:54 I would like to call out a paper that admin Hudgens cluck is put up that I think is a really nice paper on NGC, 3079 which is another beautiful example of filaments coming out of the center of the galaxy looking at this image from Jeroen festival, it 08:48:14 look like goes very far so fine whatever doesn't have much of an impact on the Galaxy, but what Edmund has shown in the recent papers that this by conical outflow actually extends out to 60 kilo parsecs so that makes it a lot more interesting. 08:48:30 And also there's some interesting indications of multi phase stuff going on the, the edge of the X ray wind is not the same as the edge of the foreign ultraviolet emission. 08:48:42 And so you know maybe this is a shell and you have x rays filling the cavity and blah blah blah blah blah. This seems like a really neat example of a by conical outflow. 08:48:54 Another example that people are loving these days. Thanks, he Rosita or the Fermi bubbles and I won't spend a lot of time on this but there is something that doesn't seem to be getting discussed which puzzles me, because people will put up these Fermi 08:49:09 bubbles and just start to talk about and measure them or even Rosita bubbles if you like the really the Fermi bubbles, excuse me, and what isn't getting discussed adequately i think is that this is the North Pole or spurt, which we've known about for 08:49:23 many decades and the North Pole or spur is seeing in polarization of starlight towards stars that are just a few hundred parsecs away. So there are spoilers per part, at least it seems to me is not that far away and so analysis of these, he Rosita bubbles 08:49:42 things should really make some effort to remove the North Polish bird, unless I'm mistaken about this somehow. 08:49:49 This might also be of interest I suppose to dispersion measure people because it's a security nearby thing and it might show up in dispersion measure maps, even though we didn't see it in the discussion last week. 08:50:02 I haven't calculated that maybe it's not a very strong signal. 08:50:06 But that doesn't reduce the interest in the Fermi bubbles and of course on the, on the southern side I have no explanation. It's just that I think the X ray emission might be faster than what it looks like when you just take a glance at this. 08:50:21 It does look like the Fermi bubbles are not as extended as the E Rosita bubbles, at least on the south side there. 08:50:30 So, these are interesting things in a variety of ways. Here's 21 centimeter emission from, I know what's going on with my I'm missing some of my references I'm sorry about that. 08:50:42 This is 21 centimeter mission and you see these little clumpy things and looking at these clumpy things in detail. 08:50:52 Molecular emission carbon monoxide and mission is also detected. So, these are multi phase aspects of this very nearby, or I'm sorry my references up here, these very, very nearby outflow that again is beneficial because we can study a lot of detail. 08:51:13 And, for example, we can use ultraviolet absorption spectroscopy, which is kind of do tomography of this nearby outflow. So this has been work led by Andy Fox and Robin mortally and their team wrong Mendez on the panel after this so maybe he can talk 08:51:29 about this further, but they actually see red shifted and blue shifted absorption, which I think is believed to be the front side and the backside of the show, and also the detection of the high velocity absorption or the non detection depends on the 08:51:46 location of the site line with respect to the Fermi bubble outside of the Fermi bubble, the absorption seems to go away. Inside the Fermi bubble. 08:51:56 There seems to be frequently detected absorption so this is kind of promising, and actually after this paper there were several more papers looking at the bubble on the southern side and so it's a nice set of work and I encourage people to check it out. 08:52:11 And maybe wrong men can talk about that more. Once again, we see this weird correlation of low ionization stages like carbon do with higher ionization stages, like carbon for in the Fermi bubble absorption lines. 08:52:27 So this is already showed up in two different places. That, to me suggests that there's something kind of interesting about it. 08:52:36 Now just quickly, our Milky Way. It has kind of a small town black hole in a small town outflow. If we look at something like Mercurial to 31 the nearest true Quasar, we see much more dramatic outflows and this is again a weird multi phase situation or 08:52:56 carrion to 31 is surrounded by an X ray emitting Nebula, which is roughly 50 by 50 kilo parsecs. And yet, Dave and Sylvain see sodium one absorption plowing into this stuff and 1000 to 1500 kilometers per second. 08:53:16 And that's not just from the nucleus. There's also a star cluster away from the nucleus that has the high velocity outflow. So this brings up a question for theorists. 08:53:27 How on earth does sodium one which has an ionization potential of only five electron volts survive at these crazy velocities plowing through X ray podcasts, I mean I just think it's a really interesting question maybe you all understand this already, 08:53:43 I mean I just think it's a really interesting question maybe you all understand this already, but it's an important clue about what goes on, and outflows. 08:53:47 Now I've worked on this a bit with this team, and we've been focused on the nuclear outflow of specifically the broad absorption line outflow we can see on the screen here that some of the iron to and magnesium, bal absorption features. 08:54:03 We looked at this with cost and the ultraviolet a few years back in order to of course study the strong ultraviolet broad absorption features. And we were astonished and perplexed, initially to find that there were no broad absorption features in the 08:54:19 ultraviolet very strong, bal features and the near ultraviolet and optical but in the far ultraviolet. They're gone. There's nothing there there's continuum but no be a outflow so what the heck. 08:54:33 Well, the explanation to this is seen by looking at the spectral energy distribution of Markarian to 31 in the optical and going into the near ultraviolet, it's very written and it's basically what people now color red Quasar. 08:54:51 But then, all of a sudden, the you know the ultraviolet makes a comeback. And it sort of becomes a somewhat more normal looking continuum from a quasar. 08:55:03 So what we think is happening is that the Bal outflow is dusty. 08:55:08 So we can't see into it. When we get too deep into the ultraviolet but we see it in the optical and near ultraviolet and so that's why the BA l absorption has disappeared. 08:55:19 And the far ultraviolet spectrum, and yet continuum sneaks through because there's some kind of pettiness or some way, that there, that the ultraviolet light from the central engine is able to sneak out and invade this dusty screen. 08:55:36 Now that one necessarily is not necessarily misty. We also looked at another Quasar but we're actually working on a whole bunch of these Bal quasars. And in this one, we were studying it because it had the usual famous big, fat, highly ionized Bal outflows. 08:55:56 And it was quite ordinary in 2011. And when we looked again to monitor whether there were changes in high on ba else, we found that thousands of new absorption lines had appeared in the spectrum, including many iron two lines bomber absorption lines helium 08:56:17 one absorption lines and it's important to note that the lower level. And these absorption lines is not met a stable it's, it's the lower level is connected to the ground state so it should be easy to deplete the electrons from the lower level and yet 08:56:31 we see these things, and absorption. 08:56:34 So we modeled this and basically it requires a huge density we require a density of at least 10 to seven per cubic centimeter. and for the sodium we actually found that we needed 10 to the 10 per cubic centimeter. 08:56:48 Now the stuff, partially covers the flux source and the partial covering depends on which ion we look at it ranges from point 044 sodium to about point five for the ultraviolet absorption lines. 08:57:03 And so we can place constraints on it so it's heterogeneous, and we can place constraints on its size it's pretty small thing. 08:57:21 It's always oh this, this is cool well just monitor it for years and see how it changes but it was not to be because within a couple of years it was gone again. So here we have something misty you all might be saying what the heck well this isn't certain galactic medium but a lot of folks are interested 08:57:29 medium but a lot of folks are interested in a gn feedback and. So here's an example of how we can start to look at the details of a gn feedback and that's actually pretty interesting. 08:57:39 Even if the density is maybe 15 orders of magnitude higher than what we see in the CGM perhaps physics is not exactly the same, but you know, whatever. 08:57:49 I just like to talk about stuff that's fascinating. Let's keep going. So, we see outflows and a lot of different situations here's Christina Montes paper on the post Star Wars galaxies and she found, magnesium, too. 08:58:05 And these things moving at 1000, to 2000 kilometers per second. Looking down the barrel. 08:58:09 So, the limitation of this was that you couldn't decide if it was just nuclear stuff or it had a more killer power sec galactic scale. 08:58:21 Sometimes, and this is happening more. The mission is seen with if use on large scales here's rep keys beautiful paper showing oxygen to a mission extending over 100 kilo parsecs, but often the densities are low, and we don't know what's going on on galactic 08:58:40 and certain galactic scales. So this is where Quasar absorption systems become rather handy because absorption is extremely sensitive when we can see that low density stuff, way out, and even into the intergalactic medium. 08:58:52 So I'd like to make a few comments about a survey that I've been leading for a few years, called the cost absorption absorption survey of Barry on Carver's or Cosmo. 08:59:12 And the idea of this was to access all of the wonderful diagnostics, that nature, provided. But then quite mysteriously hid in the deep ultraviolet so there are all kinds of resonance transitions of all kinds of metals and ions but most of them are in 08:59:31 far ultraviolet below 912 extremes where we can't see them in the interstellar medium because of the hydrogen. But the trick to play, is that if we look at a redshift and absorption system then all this stuff gets red shifted into the observable band. 08:59:41 So we've been working on this and we detect all things we'd hope to detect some of them are in Quasar outflow type stuff and some of them are in foreground certain galactic halos. 08:59:53 We looked at nine quasars with redshift ranging 2.9 to 1.5 signal noise 20 to 50 per Razzle cost gives us you know 1520 kilometers per second resolution we also got dear ultraviolet spectra with costs and justice, that's very important for line identifications 09:00:11 and often the oxygen six is red shifted into that band, and we obtained Keck hi Reza shell spectrum. So, the data, look like this, and I hope you can see this normally we're kind of stuck working with these species and maybe we got silicon to in carbon 09:00:29 to Silicon form carbon for as is kind of kind of meager. But as we go deeper into the ultraviolet, we see that more and more ions and species are detected. 09:00:41 These are all lines that are detected in a single absorption system, and the spectrum of this equation RPG 1630 plus 377. 09:00:51 I think I've identified more than 8000 lines in this single spectrum from the cosmos survey. So I think this is a wonderful archive, for Quasar absorption line people to use for years and years to come. 09:01:05 We I don't know I think we've written a dozen papers or something that use these data and we're continuing to work on it as hard as we can. 09:01:13 You get often lineman limit systems you get coverage of lineman series so you can get excellent h1 measurements in addition to the metals, it's really very powerful data. 09:01:25 So, what do we learn. I don't know why it's sometimes stops advancing. Here we are. So, we're also doing a galaxy redshift survey, much like what we heard about last week and Costco has led this part, along with just work, our host, and many other people. 09:01:48 Christopher Wilmer played an important role here Joe virgin I mean lots of folks have been helping out with the survey. So here we see the different galaxy. 09:01:59 Red shifts with the impact parameter, and the redshift along the x axis. We also adopted a wedding cake strategy we use the heck prospect with its 300 fibers to get the brighter lower redshift stuff we use Sloan Of course, and then we use the most on 09:02:16 tech to go deeper, and narrower. 09:02:19 And I think we got something like 5900 galaxy read shifts. 09:02:24 At this point, and that's published purchase good old 2019. So, we can make statements about the six covering fraction, extending to very large impact parameters we measured the oh six galaxy cross correlation function so there's a lot of information 09:02:41 on how oh six absorbers cluster with galaxies. So I'm not going to spend too much time on that paper, I see time is marching on I want to make a few more comments. 09:02:51 We also provided the first survey of neon eight absorption in certain galactic halos so this is a paper that was led by Joe Burgett. 09:03:03 And what we found is that when we have a galaxy, close to the site line at a redshift that brings neon ate into our band pass, we typically do detect neon a at least within one or two very old radio at larger impact parameters, we don't detect neonates 09:03:23 so the neon he seems to have a similar behavior to oxygen six and other ions that we know and love. This is not all of our neonates detections This is just the neon eight that's affiliated with galaxies. 09:03:38 So this is a paper also came out in 2019, supposedly it's an appt j letter but it seems to be 40 or 50 pages long somehow so go and take a look at it. 09:03:48 There's a lot of information in this ft letter to virtue is very good at writing fJ letters that are far, far longer than they're supposed to be so you talked to him about how you how you do that trick I don't quite get it. 09:04:00 My update letters have always been four pages, Joe. 09:04:04 All right, well anyway. 09:04:07 There's something interesting about this cosmic data. So here's an example here's one of the galaxies, we've got a spectroscopic redshift it's 100 Kayla parsecs from the quasar and projection. 09:04:20 We see all kinds of lines so it's great. We've got the h1 linemen series lions, you got me on a song for five so for for. So for three carbon for carbon three nitrogen for nitrogen the, you know, all these different islands that we'd hope to find and 09:04:36 here the ionization potentials for these things. 09:04:40 It's really weird. 09:04:43 You know, you need you need say 50 Evie, to get rid of some of the lower ionization stages in a 270 EV to make neon eight. 09:04:54 And yet these things are lined up beautifully. 09:04:57 Oh, this is a, here's the oxygen six, I should probably just have this one figure in here. Anyway, if we look at these apparent column density profiles again. 09:05:07 You see, weird just weird, the centroid, and the line widths to whatever you can get with 15 kilometers per second resolution which is a few kilometers per second, seem to be the same for things ranging from h1 to oxygen three to nitrogen for so for five 09:05:26 and beyond eight. 09:05:29 We talked last week about whether this stuff is turbulent Lee broadened, whatever that means, or thermals abroad and in this case, it's really hard to, it's not thermal abroad, because you can look at things with different masses and they seem to have 09:05:44 the same line widths. 09:05:46 So what's going on. Here's another example that I'd like to show actually my collaborators take bets on how long it will be for me to actually put this slide and because I always show it, but it never gets old. 09:06:01 Just doesn't actually I I'm working on some malware code, what I intend to do is set up this malware so that all astronomy talks will show this slide at some random time so if you see this slide pop into your talk, bizarrely while you'll know what happened 09:06:15 and. 09:06:16 Just don't tell the FBI. Anyway, this, this one here's the quasar and Jake Charlton and Chris Churchill and their group have worked on this too, with ground based data. 09:06:27 There's galaxy about 70 QO parsecs from the sideline. It seems to be a face on galaxy I don't know if you go so far to say it's a spiral galaxy but it sure looks like its face on it has magnesium to absorption spread over 1500 kilometers per second. 09:06:44 So some of this stuff is probably escaping. 09:06:49 It's quite different from what we heard about last week, but again that's just magnesium to it's hard to work with that. 09:06:56 Maybe just to sort of be speculative maybe this is some kind of outflow. And on one side we happen to intercept the outflow where there's more stuff happening on the other side, maybe we just dip off a bit more boring region so we only see a little bit 09:07:11 of the absorption. 09:07:13 Even if you just focus on this part, it probably got some escaping stuff in it. 09:07:19 Now here's the great part. Oh, that's annoying. 09:07:24 That figure is not supposed to be in front. Well, it's fine. We here's the line in series lines flux both the line series we've got excellent h1 constraints and we see all these different metals So there we go. 09:07:38 And they're all lined up it's just nuts, the centuries of the line what's very similar for things ranging from magnesium to up to neon eight, you know, and so I'm just going to zip through this we did some goofy things show modeling came up with masses 09:07:55 and outflow rates and there's sort of interesting. I don't know how much stock to put in that model and it's not really what I want to talk about, but I'll just flash those numbers up it's probably an interesting outflow. 09:08:06 But here's, here's another one of these plots again and just looking at different things compared to carbon to. You see this extraordinary correspondence that the Keck magnesium to data has higher spectral resolution but you know you can see the same 09:08:21 features, recalling the discussion at the beginning of this talk in higher resolution data. 09:08:28 So this is another, I think, important question for theorists. How on earth do we get these really disparate ionization stages to line up and track each other so precisely at these high velocities over a large velocity range. 09:08:47 And, you know, you might accuse me of, oh no I'm missing a slide again No way. 09:08:55 I'm not sure what happened. 09:08:57 Well, it's fine. You might accuse me of cherry picking the Cosby data, and only showing the juicy examples but it's actually not the case this is very commonly observed in Cosby data, where if we look at something like carbon for each one oxygen for an 09:09:16 oxygen six, we find there, they're beautifully lined up. Now sometimes the line with two different, but the centuries, often are extraordinarily well aligned. 09:09:28 But we should recall my little goofy lecture at the beginning. That doesn't mean that these things are code spatial. 09:09:39 In fact, thank you just. 09:09:42 They probably not co spatial and I think the phase structure the component structure is just lost at cost resolution. But clearly, there's a relationship. 09:09:51 That's the point I've been trying to make all these years and understanding that relationship is important. And, well, I don't know, maybe it's cloud shattering maybe it's precipitation maybe it's cool gas that forums and the outflows. 09:10:08 There's lots of great theorist here we can talk about these things and so I just want to put the question out there. Now I know I have to finish up so let me just quickly advertise a paper that graduate student working with me has just finished, which 09:10:21 is really the only way to handle all these different ions, with the this unresolved and indistinguishable phase structure, I think, which is to take a Bayesian approach, and just explore parameters base. 09:10:39 Probably with forward modeling if you can computationally hack it and and see what the constraints on the parameters are in that way. So Carlos put out this paper and it's on Astro pH we're going to hear more about this I think from Jane tomorrow her 09:10:54 team has also done similar work and I and I. There's also let me advertise one of these videos. So there's a lot of information so I'm not going to get into this in too much detail and I'm out of time anyway. 09:11:08 But there's a number of important priors and different parameters that we can explore we can explore the you know the density the relative abundances that were discussed. 09:11:19 We can add hot gas, we can do a lot of different things. 09:11:24 One of the important priors I should mention is we put a prior on the cloud sighs that's partly motivated by Michael Roberts great work from years ago, showing that the things like carbon for just not that big. 09:11:38 So, we're not, I'm not I shouldn't say compelled by models that require a very large very metal enriched cloud. We can vary the shape of the UV flux do lots of things so let me show you some results. 09:11:53 So for the oxygen six. 09:12:06 The Basie and models really prefer a hot face and no by the way we can put in multiple phases we find a single phase just doesn't happen, that's no surprise, but we've it's valid it's helpful to show you can rule out a single phase. 09:12:11 Typically we require at least three phases. And for oxygen six and neon eight we, the models tend to prefer hot gas. 09:12:20 The models also to tend to prefer an ionizing flux field that is softer and brighter than heart muddle. 09:12:28 And this is maybe what people wanted me to say most of all I've sort of waited until the last possible moment, which is that we can look at the pressures in these different phases, with all these different ions and metals, and we can ask, are these things 09:12:44 in pressure balance, do they have the same pressures and therefore seem like they might be in thermal pressure equilibrium, or do they have very different pressures and this is a problem that just raised with her, her big costs a little paper from 2014 09:13:00 where she showed that the pressures are much lower than what you might expect from say the monitoring Bullock bottle. 09:13:08 So we even put in a prior to try to force the models to find pressure equilibrium. 09:13:14 And here's what we found. I can't believe it I don't know what's going on here. 09:13:18 Well, I'll just tell you the answer is, if we only allow photo ionized phases. Then we cannot find pressure equilibrium, typically and that's shown in this top panel that and it's no surprise the highly ionized gas has to have a low density there's not 09:13:35 that many ionized flux photons that can make oxygen six. So the density has to be low so the but the temperature is more or less the same it's borderline is so that the oxygen six phase has a low pressure but the more the ionization phases have higher 09:13:51 pressure so they're not in pressure equilibrium. But if we allow some sort of heating that makes some of the phases hotter than we can find pressure equilibrium solutions, I should say, thermal pressure equilibrium, because we don't put in non thermal 09:14:10 pressure sources. So, let me skip ahead. I'll just quickly show something I think I've shown everyone before with this high resolution spectroscopy with just we can also look at the oxygen six absorbers that are regifted, and we find that they to resolve 09:14:30 into multiple components. And this is bad news. The components are narrow. And so the gas is cool, let me know we can put an upper limit on the temperature. 09:14:40 And so for this one, the upper limits are 20,010 thousand Kelvin. So, we shouldn't have any oxygen six there. If it's crucially ionized so it's sort of runs against what Basie and studies seem to indicate some people will argue that this photo ionized. 09:14:57 I don't think it is, it just you have to have these big absorbers. 09:15:02 That doesn't work for me. 09:15:04 I think maybe there's some physics, that's missing, I think, yeah, maybe the stuff cools more rapidly than it recombined and it's just an overall nice state. 09:15:14 So that's another question for theorists, so let me go ahead and put up some sort of goofy conclusions and. And I will say thank you once again for your time and for the opportunity to participate in this wonderful workshop. 09:15:32 OK, so I guess we take a break now. 09:15:34 Thank you. Thank you, Todd. That was great. It was a lot of this is a very beautiful, Misty 09:15:45 information a lot of fodder for the discussion, there's a lot happening right below 21 week to multi-phase, and so I encourage you to go there. Let's take five minutes we'll come back here at 920. 09:16:01 When our expert panel will convene. I have been monitoring closely Halo 21 week two multi-phase. I'm already looking at a few comments that I definitely want to bring up to the panel, but please type some comments there. 09:16:14 And, and I'll make sure to feed them to the expert panel. All right, take five See you in five minutes, 920.