08:05:13 Good morning everyone. 08:05:15 We've got a great morning of tutorials on some really cool topics today. 08:05:26 And about things related in some way to outflows or also visualizations since this week is the, this week. 08:05:35 I also wanted to highlight this awesome image that is in the background here for, for our outflows week, produced by Evan Schneider. 08:05:49 The from the seagulls simulations using her choice code. Really amazing high resolution simulations, showing outflows into the CGM and the impact on the CGM so some great papers coming out of that, and Evan is also giving one of our tutorials today on 08:06:07 mass looting quick announcement. 08:07:29 Alright so today's tutorials. We have three awesome tutorials. 08:07:35 We will start off in a couple of moments with Joe Birgit talking about how to visualize the second galactic medium in your web browser using his new Cosmo of his tool. 08:07:49 And not just visualize but do some really cool data exploration of simulation data. 08:07:53 That gives you a lot of intuition for for how the CGM behaves. but I'll leave it to him to discuss that. 08:08:01 So, as well, I'll just go through all of them, our next one at 840 will be, as I mentioned given by Evan Schneider on mass loading in outflows, And then at 920, we will have one on absorption line profile fitting. 08:08:19 Primarily, Murray law will be giving that but then she'll, she'll get. 08:08:23 She'll be presenting one method or a couple of methods using some programs, and then other programs for doing this absorption line fitting will be provided by Joe, and by wrong one. 08:08:36 So, should be really cool. And as with all of our tutorials, we will have the tutorial itself recorded, and it will go on about 20 minutes or so. In the main zoom channel, and then we encourage people. 08:08:56 After that, before the next one has yet begun. If they have additional questions or discussion to go into the breakout room, that is designated associated with that particular tutorial, including the tutorial leader, the person who spoke, and then that 08:09:12 discussion can go on ad infinitum in the privacy of that breakout room, while the main channel continues on with the next tutorial. 08:09:23 And then one last quick announcement. There are a number of after parties going on this week, two of which are occurring today. 08:09:31 So at 12 noon, we will have an additional zoom discussion for people interested in cosmic rays it's being led by Chad bustard and Christophe Fromer so that should be pretty interesting and exciting I know I'm looking forward to it because of the, all 08:09:49 the that was discussed and left undiscussed from a couple of weeks ago. 08:09:55 And then following directly following that there will be an unrelated break at our after party on visualization led by Joe Burgett Stephanie Jonas and Dylan Nelson, and you can find links to the various zooms for these in their respective channels so 08:10:11 in Halo 21 cosmic rays and in Halo 21 visualization, and then tomorrow. Mark Voight has organized a, an after party at 11am Pacific so an hour after we finish this. 08:10:26 an hour after Tim Beckman's keynote and, and, and the subsequent discussion panel, and that after party will be on a gn. 08:10:36 So, if you'd be interesting. 08:10:39 But yeah, For now, let's move over to our tutorials. 08:10:44 Starting off with one from Joe. 08:10:53 Are you around you. Oh, there you are. 08:10:55 Yes, thank you. 08:10:59 Okay so yeah thanks camera and thanks to Jess Mark been all the organizers for putting together an incredible, incredible workshop here, and really making the most of this rather unexpected virtual venue, it's been it's been great and it will be great 08:11:18 for another three weeks, so it's my absolute pleasure to to present today and sort of a world premiere of sorts. Our project we've been working on for about the last year or so called Cosmo this. 08:11:35 And so how this will work. I'm going to demo the software. 08:11:40 And then we'll go into breakout rooms, I want to leave enough time to make sure and give plenty of time in the breakout room between this tutorial and, and Evans excellent tutorial i'm sure to come. 08:11:53 So please do. 08:11:56 Follow me into the breakout room. If you would like to accept what I believe will be an irresistible offer. 08:12:05 Okay so Cosmo is, this is, this is a project that I've been leading as I said over the past year or so. 08:12:14 And we've been fortunate to have an incredible team. 08:12:18 This is a truly interdisciplinary collaboration. 08:12:21 First, I'd like to highlight the our lead developer. David a remark who has really done so much of the heavy lifting. In terms of software development and researching visualization and rendering methods. 08:12:38 And so big thanks to him he's here today, and he will join us in the breakout room to answer any more technical questions you may have about the underlying software. 08:12:49 Oscar elec, who is, I should mentioned david Abramoff is a graduate student in the computational media department at UC Santa Cruz Oscar elec is a postdoc at UC Santa Cruz in the same department, and he has been credibly valuable as a resource that he's 08:13:06 an expert and graphics rendering in 3d printing. 08:13:11 Angus Forbes who heads up the creative coding lab in the computational media departments at UC Santa Cruz, who joined us on Monday will be joining us for The after visualization after party today. 08:13:25 And lastly, our very own Cameron Hummels who without whom this would really not have been able to be where it is today so a big thanks to Cameron for being a incredible resource for all things, Trident and YT, both of which Cosmo is heavily relies on. 08:13:48 So, key question, what is Cosmo Cosmo is. And just so you notice a teaser images of Cosmo is from Cosmo is here on each of these pages Cosmo is is a web based interactive visualization and analysis tool. 08:14:07 And essentially what we're doing with Cosmo is is serving up. 08:14:12 For now, cosmological hydrodynamic dynamical simulation data, and I say for now, we are looking to to move into the realm of zoom ins and such, currently implemented are a couple of volumes from the eagle simulation, and we will soon incorporate fire, 08:14:32 as well as illustrious tng, and hopefully more custom events will be released to the public as not only an analysis tool, access to the web, but also all the underlying software will be open source. 08:14:50 And so, realistically, this is probably looking at second quarter of this year, but everyone here today will get a chance to check it out. And so, who is the Cosmo of his audience that is you, your research collaborators your students. 08:15:06 Your neighbors, your family. This is really intended to be intended for mass consumption. So, hopefully, a little bit of everyone can get something out of it. 08:15:20 And just some of the technical details. 08:15:23 What makes cosmos is run well there's basically two parts, there is what happens when the web browser. So this is using JavaScript libraries to render in a 3d environment in two different ways through volumetric rendering, in which we project the gas 08:15:41 and dark matter from a simulation, with customizable capacity color mapping, etc. 08:15:49 and also particle data. 08:15:51 When we visualize these particles, which would be stars and black holes within galaxies. And all of this is customizable on the fly on the back end we have tried it running on top of it, of course, with Amazon Web Services cloud computing. 08:16:08 So this is handling. Some of the more computationally intensive tasks that really we wouldn't want to offload to a web browser such as generating synthetic spectra through Trident and doing the line of sight. 08:16:23 Physical attribute mapping is, we'll see later. 08:16:29 So just some of the motivation for you, why we wanted to undertake this this project. And so, What I have here is sort of a workflow of how one might use simulation data, say as an observer, as I primarily am you know there's there's all this great simulation 08:16:48 data, there's been a lot of tools such as YT trend, and many others that individual groups have developed for their own site for their own simulation data. 08:17:01 And so, in terms of actually using these data, to, to, to bring them to bear on our observational results to try to glean scientific insight, it's it's really not quite as straightforward, a process, at least, I found to do that. 08:17:23 So, in addition to acquiring whatever simulation data set, you might want to compare to be it. 08:17:28 Many of these cosmological boxes that have been released to the public like Eagle Lester's TMG. 08:17:37 There are independently sort of tools to to to analyze those, such as such as Trident for example if I want to compare some of my HST cos spectra to those that would result from, from the models. 08:17:55 So it's sort of a convoluted process to come out in the end. 08:18:09 For basically lay user. So we wanted to encapsulate a lot of these analysis data acquisition pieces of the, of the workflow into sort of one unified environment. 08:18:15 And that is what Cosmo is all about. 08:18:17 So the idea here is, one can go straight to straight to Cosmo biz. 08:18:27 Explore manipulate the cosmological simulation, and then get out some physical attributes, or even synthetic data that can then be directly compared to observations. 08:18:38 So, I know what you're thinking. So I'll sounds great. 08:18:43 You're going to need people to use this thing right the the audience is me. So, if you're a big fan of the judge, like I am, three words come to mind, why not me. 08:18:57 Well, everyone here is invited to become a beta tester to help steer development in the future of cosmos is so we just invite you to please complete just about a 30 minute user study on your experience with Cosmo because because this will really help 08:19:16 not only steer the development, but this is a visualization project and so we really want to research the human human data interaction piece of all this. 08:19:28 So also join the new Slack channel that I have created called Halo, 21 Cosmo is, and we can talk all about Cosmo is there, share some interesting results, maybe you found with it, and so on. 08:19:44 So, without further ado, 08:19:55 switch over here. 08:20:03 Okay so, whenever you load up cosmos is, this is essentially what you are going to see. 08:20:18 So this is the eagle 12 megabytes per second box. 08:20:24 And we have a number of attributes that are visualized here. 08:20:29 There is gas dark matter and stars. As I mentioned in this slide. So previously. 08:20:43 Now we're left only with the gas layer. 08:20:48 And I realized the video might be a little choppy so I'm just going to optimize here. 08:20:54 You stop sharing. 08:20:57 We go. 08:20:59 Okay so, um, so as I was saying we can turn on and off each of these layers within within Cosmo is and 08:21:09 turned off dark matter, turn off gas. 08:21:12 And here we just have the stars from the individual galaxies 08:21:22 can turn on just the dark matter so you can see the cosmic web filaments and such, and just the dark matter distribution. 08:21:31 And this is just gas as I was saying, so you can already kind of see some interesting, interesting phenomena that have been going on. 08:21:40 Over the course of the evolution of this boxes is a redshift zero. 08:21:43 So, can already sort of see some interesting things that will actually investigate a little bit more detail here in a bit. 08:21:52 So, I just want to walk through the interface of Cosmo this and and demonstrate some of the features that we have here so I'm going to focus mostly on the guests, so you'll see me, turn off, dark matter for for the majority of this demonstration. 08:22:14 So here we just have the gas layer, as I mentioned, this is the 12 megabytes sec box of Eagle. 08:22:26 And 08:22:26 I want to now just use the data selection tool here and just kind of focus on some various regions of the simulation, but turned on the axes helper, so you can probably see down in the corners along the box. 08:22:44 We have the color coding corresponding to various axes here so I can slice the data. 08:22:57 Look at a particular region just slicing along these axes color coded above the respective sliders for each axis. So, can kind of zoom in on individual region. 08:23:11 So, this is, this is sort of the courses grid resolution. This is what you'll see when you first open up the application. 08:23:20 This is only a 64 cube box so a fairly course resolution. 08:23:25 And we net we have under the hood here a couple, three actually resolution levels, per, per simulation volume. So this is now that same volume we were looking at. 08:23:42 Slice from from the big 12 megabytes a box. Now just focusing in on a couple of galaxies here, apparently has some, some nice super bubble action in their CGM. 08:23:52 So, I'm going back to our Layers panel. I would customize the visualization a little bit. So, so, color coded here is, is the temperature of the gas, and I have color range picked here about 3.2 to 3.7 K, up to 6.75 Kelvin, where the red or values, the 08:24:27 rhetoric colors are corresponding to the hotter, hotter temperatures. 08:24:23 And I have the all gasp below 3.7 Calvin. 08:24:29 To 3.7 clipped out so can see a little bit of difference there just focusing in on the temperature range for about 10 of the four on hotter. 08:24:39 So, I visualized temperature, or a color coded temperature, but we can also look at the other attributes. This is the middle of the city 08:24:51 in the same environment. 08:24:54 So you can see a lot of interesting substructure that's actually quite different than that we see in the, in the temperature entropy. 08:25:06 Now go back and look at the full volume. 08:25:22 Some interesting structure, a long shot friends and such, with the, with the interview data. 08:25:31 Um, okay so let's now focus on a specific region of parameter space so now I'm going to just focus on the so called warm hot medium so this would be about 10 to the five Kelvin, to, to the six Kelvin. 08:25:54 So I can clip out everything that is below and above this temperature. So, so you can see a lot of the hot gas that sort of in the 08:26:15 on the hot gas that's right in the center of the halo has now been 08:26:13 is now missing. 08:26:19 Turn off the dark matter, get a better view here. 08:26:27 Okay, so let's go back and view the full range here. 08:26:44 We'll go back to the course resolution so it's kind of demonstrate a workflow, one might, one might use when, when interacting with software. 08:26:57 We go back to the full volume so they said this is the this is the courses resolution. And this loads, very quickly, and enables you to get a nice overview it's obviously not quite as much quite as much structure, as, as you would see in the higher resolutions. 08:27:18 But you can quickly through go between the 12 week apart six boxes we were just on to the 25 megabytes per sec. 08:27:27 Just a second to load here. 08:27:36 Turn off dark matter. 08:27:42 Take another look at the entropy. So you really see some nice shock fronts. Along the CGM and IBM. 08:28:00 Go back to the 12 for a sec. 08:28:03 And I mentioned that 08:28:11 sort of highlighted these couple of galaxies here earlier. 08:28:39 Fake clear evidence of some past feedback activity. 08:28:42 Let's come in a little bit higher resolution. 08:28:46 So you can see a little bit more substructure. 08:28:50 This is not only in the, in the temperature of course but these other values but let's crank up the resolution even further and do a little bit more in depth study on this particular this particular system 08:29:10 should take about between 30 seconds in a minute to load from the web, I'm running this locally here. So, just to mitigate any issues well continuously. 08:29:26 We're slipping all simultaneous simultaneously running zoom. Okay so here you see even more substructure and the temperature. But I want to get a little bit more quantitative with the analysis. 08:29:36 And so it can draw skewer anywhere through here so let's just go right through this bubble area 08:29:49 and request, some, some data along the line of sight. So this is all generated on the back end with Trident, and YT trading is is taking the physical conditions of the gas along the line of sight. 08:30:05 And not only returning those but also going to provide us some, some eye on data. 08:30:14 Okay, here we are. So now you see the temperature structure along the line of sight. I'm going from sort of the cool phases out in the AGM here. As we enter the CGM in this in this bubble area we get to the hotter regime, until around two to the six Calvin, 08:30:33 and then going back into the cooler phases. Once we leave the CGM. So, this is temperature you can look at a number of a number of quantities inter be medalist medalists at. 08:30:46 So this is about a 10th solar, for the most part, quite a bit of relatively metal poor gas. 08:30:55 Actually in in this bubble. And then we can get my own column densities. So, as a fairly low h one column density through this line of sight, have a number smorgasbord of ions here. 08:31:11 Carbon three. 08:31:16 I like neon eight quite a bit so you can see the column density in each cell along the line of sight and then the cumulative calm density of that particular species. 08:31:26 So, oxygen six we like oxygen six. 08:31:30 We also like oxygen seven oxygen eight. So, basically any of these ions, you can get a cumulative comments as well as see the distribution of that particular ion along the line of sight. 08:31:49 We'll go ahead and draw another skewer between these two between these two bubbles. 08:31:54 Get this data. 08:32:15 And you can see the two temperature peaks, where we are going through the the bubble region, the outflow. 08:32:24 The region of the past outflow from one galaxy to the next. So, Lots of fun, one can have here can go back in and since we have this higher resolution of the volumetric rendering. 08:32:38 Take a look at the middle of city. 08:32:49 See the middle of city structure, the morphology of the middle of the distribution is actually quite different temperature distribution which I find to be interesting. 08:32:58 Okay. So, with that, I do want to save some room to step into the breakout rooms. 08:33:04 Like I was saying. Everyone here is invited to, to be a beta tester. 08:33:13 Everyone, as long as you complete the user study, help us out on the development side as well as from the visualization standpoint, HCI standpoint. So please join me in the breakout room there I will actually give you the IP where you can go on and you 08:33:28 can play with the tool, and we can get started on the user study, if you like, but that. Thank you. 08:33:37 Awesome. That was super great Joe really could be a game changer for a lot of people in terms of how they interact with the simulation data and how they prob it. 08:33:50 There are a number of questions that were raised in the chat, as well as Drummond has his hand raised. But I think, for the purposes of making sure, Evan. 08:34:00 Evan gets a chance to do everything in six minutes for her presentation, we will move, Joe, and Angus and David, and everyone who's interested in talking about this awesome tool to a breakout room. 08:34:16 So if you go into the breakout rooms, you can click Cosmo, I believe, recall though that we will start Evans presentation in at 846 minutes or so. 08:34:28 So, it's a trade off the presentations are recorded the breakout rooms are not, if that helps your decisions. 08:34:38 But yeah, super great Joe. 08:34:41 Really cool work 08:34:46 tutorial day is tough Evan. 08:34:58 So yeah well our five minutes or so if people need to take a break, and we will start Evans presentation in five minutes at 840.