08:05:10 Alright, good morning, everyone. I'm noticing that the participants are rapidly increasing right around 805 now.
08:05:21 So, you figured out, our plan to delay by five minutes and of course everybody in science at immediate five now. So welcome, welcome to week eight Tuesday's keynote presentation.
08:05:35 So this week as advertised is about the prospect for new observations over the full electromagnetic spectrum to transform our view of the CGM over the next decade.
08:05:48 I just wanted to point out that you are invited and encouraged to join this week's dedicated Slack channel for discussions and more. I'll give you another word about that in a moment.
08:06:00 This week's Slack channel is Halo 21 dash week eight future jobs if you are new to slack newly joining us this week, just browse the channels and Slack, and head on down to Halo 21, anybody can join and that's where the bulk of the discussion is going
08:06:16 to take place today to these beautiful graphic is the McCarney galaxy from rookie at all 2019, which is data taken with Casey wi which, of course, our keynote speaker built so it's thematic this galaxy has a spectacular wind you can see here and oh two
08:06:36 and mission, which spans at by 100 kilo parsecs totally amazing and stunning so love this graphic. All right. Before we dive in a few announcements, as our participant number is rapidly still increasing today is zoom picture day, wow, I hope everybody
08:06:56 did their hair.
08:06:58 So after we break after Chris's keynote so Christmas keynote on sometime around nine will break for five minutes come back, take a group picture, and then dive right into the discussion.
08:07:06 This is a little experimental but we'll try to put it together in a collage, that includes everybody.
08:07:18 Okay, so another announcement is to join the halo 21 legacy channel.
08:07:24 If you're interested in various options that were floating around for how to extend the impact of this conference beyond this week. And finally, on Thursday at 430 pacific time.
08:07:38 We are going to be hosting a social hour on a platform called room. Are you me It's where all the cool kids are hanging out these days.
08:07:49 It doesn't involve installing any software, it's basically unstructured video chat. Bring a drink bring a coffee bring you know some wines and beer whatever you want.
08:08:00 It allows for spontaneous breakout rooms to occur.
08:08:04 And it all happens in your browser checkout Halo 21 socializing. For details, including the link to the room.
08:08:15 All right, and I just want to highlight that the new results are still pouring in.
08:08:21 Now featured on our YouTube channel, the fundamentals of gases halos.
08:08:25 The new results have been, I think one of the most successful aspects of this program, we've got now 56 high quality four minute videos describing new results.
08:08:36 And.
08:08:38 And so this week new this week Nikki Nielsen has uploaded to new videos recently, as well as brown rock hard to sweet Zhu Zhu Zhu Li, and Roland socket.
08:08:53 So check those out there not only posted in Halo 21 dash new results but they're also on our YouTube channel, which you can just stream and the evening with your feet up and a beer.
08:09:02 It's amazing. So go check them out. Now in addition to these new results videos we've also got some new instruments videos, and right now as of this moment we have two videos but I believe there are going to be more feature throughout this week which
08:09:19 I'll continue to try to advertise the two videos that exists right now on the new instruments playlist on YouTube, or in the new instruments channel are on artists by Randall Smith and blue moves, blue, Muse by Johann Ricard.
08:09:36 So check those out if you're interested in some of the new capabilities that are potentially coming online.
08:09:46 I don't know someday soon learn when watch the videos.
08:09:49 Okay, so let's see.
08:09:54 Slide stuff to advance advancing this week's featured conversations that we heard from yesterday, Halo 21 and mission. Halo 21 new instruments and Halo 21 parametric model I just wanted to let you know that there's a couple after parties scheduled I haven't
08:10:10 heard yet if Halo 21 and mission is scheduling and after party. These are separate zoom sessions, you run by the CO initiators and the zoom links are in the individual channels.
08:10:25 I know that the new instruments channel is having a new instrument roundtable discussion on Wednesday from 10am to 12pm Pacific. When will post the zoom details and Halo 21 new instruments.
08:10:39 If she hasn't already and Halo 21 parametric model has an after party today at 12pm Pacific so everybody is welcome to join these after parties, they're just different zoom links that you have to look out for.
08:10:53 All right. And my last comment before I quit blathering is on how I'm going to run the panel discussion and this is, this is my week, I'm the captain now, and I demand that you use emojis.
08:11:08 This is the future, everyone I know emojis might make you uncomfortable. Oh there for five year olds, but they're what we've got. And they turn out to be a useful tool.
08:11:18 So, throw your pride away and get on the emoji train, think of them like hieroglyphics, they're a whole new efficient way to communicate, somebody's making a comment you like, you can't not enthusiastically at them, you know, and expect that they're going
08:11:31 to see your video you can't sneer at them when they trash your work. Instead, use an emoji. It's amazing. And what I'm going to do when I run the panel discussion is I'm going to look at the user submitted questions and comments and the ones that have
08:11:45 the most reactions to them, are the ones that I'm going to bring to the panel to discuss, so your emoji is kind of powerful. Okay, and the range of reactions available you can see here is immense.
08:11:59 Right. You can swear at someone, you can call someone a liar by giving them the Pinocchio emoji.
08:12:04 Or you can, you know, give them a heart when hundred. That's good.
08:12:09 Anyway, so, so please use emojis. Alright, and now, without further ado, I would like to introduce today's keynote speaker, Chris Martin.
08:12:21 He has over four decades of experience building space up and ground based instruments targeted at the dim matter of the CGM an idea. Of course he's responsible for bringing to fruition.
08:12:38 I think one of the most successful small explorer programs ever also fireball KZWIXZWIM probably has a number of exciting projects in the works. Maybe that he'll tell us about today.
08:12:47 After receiving his PhD in 1986 from UC Berkeley, he's authored many many papers from fact, it's hard to actually figure out exactly how many papers from ABS because he's confused with another giant in the field crystal Martin, who happens to be here
08:13:08 to on the panel so between them, they have over 1000 papers, it turns out, and also on the panel is Joe Birgit Chuck Seidel, and Sarah Tuttle, this is an absolutely incredible panel.
08:13:23 I can't wait for the discussion after the talk but. First up we have the talk, so I'm going to stop sharing and let Chris take the floor.
08:13:43 Hi everyone, this is a fantastic conference. It's too bad it's ending this week but hopefully we'll have a lot of fun in the last week.
08:13:53 So there's a huge amount of talk about I can't talk about everything so I'm not going to be talking very much about work done by a number of my distinguished colleagues, including Chuck, and all the work done by Muse online and off the halos and Q so
08:14:21 that I'm going to try to have a more forward looking picture of what may be possible with this, this technique. So many people are have worked with me on this for a very long time, and I can individually acknowledge them but here's a, here's a here's
08:14:30 a list.
08:14:32 So, the basic structure of this talk is to talk about why do a mission, some new and proposed instruments that will act as context what how we try to extract physical properties.
08:14:45 Some applications and I'll go through those more or less echoing the themes of the conference and then very briefly in future missions.
08:14:54 So, I've been thinking about this for a very long time. This is from a talk I gave predicable 2000, recognizing that the AGM and what I call the PGM the pre galactic medium is extremely fundamental for understanding how baryons forms structure in the
08:15:12 universe. And that both admission and absorption would be key to to tracing these phases of the universe.
08:15:19 And I was inspired as a graduate student by this paper by Lyman Spitzer, the idea that the galaxy had a Corona was an amazing idea to me and, you know, many of.
08:15:30 It's a beautiful paper if you go back and read it, it's one of those one of wonderful papers in which there's so much physics it's it's it's a joy to read.
08:15:41 So I like to think of it in terms of this paper by Blumenthal at all which I also was inspiring me as a graduate student, the formation of structure on the, on.
08:15:53 You look at over density look at temperature velocity mass, they're all on the same plane. And all of this, and and the dividing line is that cooling time equal to collapse time and solar or zero primordial medalist city.
08:16:11 And basically, you can put everything on this plane and show where galaxies form and show how the various phases of the, the matter this not in galaxies relates to that in this cosmic dissipation plane.
08:16:27 And in particular, halos, which at the time we call the pre galactic medium is fundamental, a fundamental stage in the formation and of course, ongoing evolution of galaxies.
08:16:41 Why study a mission, and of course you have to study a mission with absorption. And you would like to do it for all the phases, but I'm going to focus on up optical a mission.
08:16:52 And for me the most important is that you get global quantities like luminosity. Hopefully mass velocity dispersion size mass flux, if you can measure if you can measure it in and out, angular momentum.
08:17:06 And by measuring these global quantities you kind of minimize astrophysical noise.
08:17:11 You get information about density pressure, temperature, cooling and collapse timescales morphology, gas kinematics, and even, you can even do large scale structure mapping the two big questions are.
08:17:25 Can we detect it and we now believe we can we have. And can we extract accurate physical parameters and that's something we're it's ongoing work, I would say.
08:17:38 But I want to put it in another term on an ancient plane two groups of astronomers worked tirelessly to identify a mysterious object. One group use the exquisitely sensitive measure method of absorption which allowed them to determine the statistical
08:17:54 distribution of various components of the object, given a large number of objects, it would finally be able to determine what it was.
08:18:01 The other group to use imaging imaging.
08:18:06 So, there's a simple reason to do imaging and that is, we can recognize what we're seeing more easily. And we can get global information about the objects
08:18:20 course when we're doing a mission probably looks more like that.
08:18:24 It's 10 tends to be very faint, and it tends to be hard to detect, but that's why we build instruments dedicated to do it.
08:18:33 An important point about the up is that it's tracing, not just the, the tend to the four degree phase, but all the way up to the 10 to the six degree phase, and there's a little bit of ambiguity in the literature, but I'm calling this the cold baryonic
08:18:47 halo around 10 to the fourth, and warm very warm baryonic Halo anything up to 10 to the six.
08:18:58 And in UV you can detect with the mission lies in particular the metal lines, all the way up to 10 to the six from collision eyes collision excited admission.
08:19:11 So here's a comparison by Return of the relative luminosity in the UV optical and X ray, and most of the luminosity comes out in the UV and that's an important point.
08:19:26 In a mission. And in particular, at low redshift, the halos show, for example for this simulation shows to the two components cold and warm but warm or warm hot, but the hot component is mostly below 10 to the six degrees Kelvin and that's important because
08:19:45 that is observable in the UV and particularly with nitrogen five, and oxygen six at lower hf the UV emission is both much brighter than the optical associated mission and the sky is 100 times faster so so looking in the space UV is extremely useful and
08:20:07 powerful in the low redshift.
08:20:08 So the methods methods we use of course our imaging spectroscopy, which is has been developing over the last five years to be very powerful new tool in particular with image slices.
08:20:23 and we need to do precision sky subtraction.
08:20:28 And we use a technique, originally developed by some back country, not in shuffle. And then, which works extremely well. And then in the UV we need very high efficiency detectors, which are being developed at JPL, for example, to get about 10 times the
08:20:46 efficiency of the galaxy detectors.
08:20:50 So, the basic idea is that here we have our beautiful Halo cartoon version, we can divide it up into components image them measure line profiles and in particular.
08:21:04 When we correct for radio transfer effects, we can determine inflow versus outflow.
08:21:11 And we can figure out how to measure mass, and I'll talk about that. And with kinematics bliss mass we can measure mass flux in and out.
08:21:23 Hopefully with empirical parameters that allow us to translate luminosity into mass.
08:21:30 So the program we have that I've been working with a Caltech with many collaborators is trying to span the entire width wavelength range from the epic of randomization with red channel case of bi through the blue channel down to riches to two for lyman
08:21:53 alpha. in the
08:21:52 stratospheric bloom payload fireball looks at point seven redshift dilemma an alpha.
08:22:00 And we're proposing an explorer, we would like to do an explorer called Halo which would do basically a UV version of case of UI from lyman alpha out to 25 or 2600 extras so the low redshift universe.
08:22:18 This all started when three graduate students and a postdoc built the Palomar cosmic web imager, which was first on Sky around 10 2012.
08:22:29 And it was really designed to do this very low surface brightness, a mission from the CGM in the IgM and and do precision sky subtracting using non shuffle.
08:22:44 That led to the cosmic imager, which was commissioned the blue channels commissioned in 2017, and it adds, all the benefits of the Keck telescope.
08:23:05 With to a much more flexible configuration you have small, medium and large slices, with a variety of great things that give you a variety of a spectrum resolutions, and again the non shuffle capability.
08:23:13 This shows the high resolution capability are close to 20,000, using the small slicer on a globular cluster.
08:23:24 And we're building the cosmic randomization map map are led by Matt. Matt is Jessica, and we're hoping to commission that next year.
08:23:33 And in particular, it should go out to almost 11,000 Nx rooms which will allow us to probe lime and alpha, close to the beginning of what we now believe is the epoch of revitalization.
08:23:46 It is always useful to compare Casey writing music, music on the sky First, we have a broader band pass but of course blues is, is, is has been proposed, and I'm sure will be built.
08:24:01 So there's a constant competition between these two great instruments.
08:24:06 They're there we are.
08:24:09 And I hope that we will be able to put an IQ on Ws on TMT.
08:24:16 The important point about that is that we'll have roughly the same field of use case of Vi with obviously nine times the collecting area, and it will be incredibly powerful.
08:24:26 Nine times faster than case and VI, and it will truly be able to map, not that not just CGM but IgM down to faint levels.
08:24:40 So the fireball balloon.
08:24:43 It is has been various configuration that started out as an animal field spectrograph is now a multi object spectrograph designed to look at halos of galaxies at redshift point seven is a huge cast of participants with major leadership from France, Columbia
08:25:04 University JPL, University of Arizona. Now, in particular, Carrie homely and Erica have them have been major leaders of this.
08:25:16 It flew.
08:25:19 This is some, some of the science the first Wide Field multi object UV imaging spectroscopy, with imaging constraints, online alpha mission and CGM and technology demonstration of these high efficiency detectors and the wide field up Imaging Spectrometer.
08:25:37 It flew in 2018.
08:25:40 The balloon had a hole in it and we had to fly during the full moon. So it was an engineering test but we got all the objects and the slits. And we're very optimistic about the next flight, working extremely well and be able to detect halos ratio point
08:25:57 seven.
08:26:01 What, what our true hope is a explorer called Halo, the galaxy Halo revolution explore the basic ideas to do something like case in view I only in the, in the space up from 1200 out to 2500 Nx drums.
08:26:21 And the number one goal would be to decode lyman alpha to actually use multi wavelength corollary surveys of nearby galaxies to understand the relationship between lyman alpha and the strong UV emission lines and physical parameters and then use that
08:26:36 to study galaxy k Halo co evolution.
08:26:40 And of course, explore the extended list of friends by the brightness even the universe. So there'll be more of that, as my tacos along.
08:26:50 How do we extract physical properties. I like to think with in terms of three levels of influence empirical tests like controlled experiments or looking for empirical scaling relationships model building.
08:27:07 That's me in a graduate student, and here's his model. And then what I call a bridge building between observations and simulations, and I'll give you an example of that as well.
08:27:20 So in the first category. I like to think that there will be because halos are relatively simple physical systems that there will be scaling laws, just like we have for much more complicated systems called galaxies, if only because there are conservation
08:27:35 laws which apply to both systems, and some analogies would be massive light ratios that have scaling relationships, something like a totally Fisher relation, dark Halo mass versus velocity dispersion and size, something like a fundamental plane maybe
08:27:54 something like a schmuck Canada law.
08:27:57 It's already been demonstrated that there are scaling laws between outflow velocity and specifics star formation rate, and so on.
08:28:06 This is aspirational, but I believe that this should be possible I mean that these may exist.
08:28:13 Here's an example.
08:28:15 Donald Sullivan did this amazing survey, using both Palomar and Keck have a number of Q so Natalie.
08:28:23 And one of the things we found this is just the images of them.
08:28:28 And one of the things we found is that there's a scaling relationship between the velocities version, the size and the source luminosity of objects around these quasars.
08:28:40 And you can show that you've just using the virile theorem again is mass light ratio goes as lemon alpha luminosity to the alphabet.
08:28:52 Then, then the luminosity would go as this power of the velocity Spurgeon radius and the fit gives you.
08:29:07 Consistent with alpha point two seven so massive luminosity ratio a week function of luminosity.
08:29:10 And if you look at the TNGS beautiful paper viral at all. The tng simulation of alignment alpha halos and scale the, for example, that the 50 kilowatts sex surface brightness in fact, the overall luminosity.
08:29:27 It has a similar kind of scaling relationship with Master light ratio. So that, that suggests, we're onto something, perhaps
08:29:37 model building, you really need a combination of some simple geometrical models radium transfer solutions. And of course cloudy and combining this with absorption and other information as available.
08:30:01 you can hopefully derive mass density, filling factor, temperature, and ionization from line ratios and use kinematic maps to constrain mass fluxes and other kinematic properties.
08:30:16 In particular, when you have externally illuminated gas in a quasar illuminated system for example, the radio transfer works out quite well as long as you're doing well some simple systems like extended rotating structures as we've been calling them,
08:30:34 where the velocity map measure from lemon alpha is comparable to the velocity and the gas.
08:30:40 Here's an example. This is a case where the lemon alpha is is from the emissivity in the Taurus it's a simple Taurus, showing that you can if you measure the actual velocity.
08:30:55 Just the velocity mean, you can also measure higher moments dispersion skewed because it's etc.
08:31:00 But here's a case where you can measure the rotation velocity, and you can measure the presence of inflow is the usual sort of distortion of the spider diagram for rotation.
08:31:12 And that allows you to measure some simple parameters
08:31:18 to go the next level.
08:31:22 I think about numerical simulations versus observations with 3d mission cubes.
08:31:29 There's an enormous amount of information in both, but it's it's it's puzzling to try to bridge this gap.
08:31:38 So, I've been thinking about this a lot.
08:31:43 Ideally, we'd have a huge number of realizations in numerical simulations and we do in some sense because we have a lot of objects and we have many epics.
08:31:53 But ideally we would vary the physics.
08:31:57 We have our admission line data cubes.
08:32:02 And we want to forward model, the simulations into the instruments so these are case of UI simulations for modeled, and then use some sort of bridge modeling.
08:32:13 To connect these two. And I'll give you an example where we use the toy model, and I think it's possible to use also physical models, and even machine learning to determine what we can actually extract from these forward modeled as simulations.
08:32:30 So now I'm going to give you a few applications, they're going to follow the course of the this fantastic workshop.
08:32:37 Just touch upon each of these as possible examples.
08:32:42 By no means comprehensive or definitive.
08:32:46 So, Halo mass.
08:32:49 I love to think about the halos impact with this beautiful simple analytic model from today and then back in 2012.
08:33:02 Here's the IBM gas is always a creating.
08:33:06 And somehow, some of its forming stars but most of it isn't. And so the Halo is acting as a giant filtering machine, and their various filtering processes under way.
08:33:18 They distinguish gravity. That's very realized realization of the gas photo ionization for low mass halos quenching some mysterious process probably black holes and the interaction with the wind from the galaxy, and the CGM as processes which which prevent
08:33:39 the flow baryons from the IBM to the galaxy. And I've indicated here colors giving the different phases, cold, cold baryonic warm baryonic and hot baryonic.
08:33:52 So, if we can survey, the entire, what I call, galaxy HR diagram.
08:33:59 And I Halo would be able to do this at low redshift specific stuff star formation rate versus such stuff seller mass.
08:34:08 And look at different stages.
08:34:12 Galaxy evolution main sequence Green Valley transition galaxies and read sequence
08:34:18 that from that picture that I showed you before the debate picture.
08:34:23 You can imagine the mass dependence.
08:34:26 The dominant processes for low mass wins medium gravity and high mass quench, and one might expect that the ratio.
08:34:35 CBS to WBH would be low, high and low in three cases, and that the mass flux in the cold or warm would be preferentially out in an app, or low. In this case,
08:34:55 this is notional MIT also measuring Halo mass is it possible that we have this extended gas to actually measure Halo masses can automatically. Well we did that with the PC, and the flash survey.
08:35:09 O'Donnell, and the paper published last year, and we got a result, which was consistent with what we expect for the quasars hosted by halos have roughly 10 to 12.5 solar masses so that's that's encouraging you actually can inspire radio transfer and all
08:35:27 the other issues.
08:35:29 Use the kinematics to explore the halo mass.
08:35:34 Okay, multi-phase.
08:35:38 I want to make a point here that we can detect all the way up to 10 to the six. This shows various lines.
08:35:46 This is oh six, for example, as a funk, in occlusion is Halo relatively low mass in the baryons in the warm phase, but it is detectable in the UV by a by a mission like Halo.
08:36:04 And both, but oh six and nitrogen five, all the way out to 10 to the six.
08:36:15 And,
08:36:15 Of course, it's a mission in a lower temperature is detectable with different lines.
08:36:24 Carbon for in particular carbon three and line ratios allow you to extract both medalists the and the temperature of this face is multi-phase gas or determine whether it's a temperature distribution.
08:36:39 An example of that. In terms of ionization This is a paper that hopefully will come out in the next couple months, a quasar, the 2.5, where we detect an outflow with multiple lines.
08:36:56 And this is the radio integration of the spectrum, showing some large number of lines. And when you try to fit that two ionization parameters.
08:37:09 You really have to have a distribution of ionization parameters.
08:37:13 And the shows you the, the fit is is line and that observation.
08:37:19 Observe line ratios are the dots.
08:37:21 And this shows the distribution ization parameter you get and the distribution associated filling factors that come from that fit.
08:37:28 So by combining various line ratios you get you get constraints on the distribution of both ionization and filling factor identity.
08:37:39 Non thermal components. Well, I think it's very clear, we just look at this picture from G at all that you're going to see something different in a mission.
08:37:51 If they're cosmic rays or not.
08:37:54 And if the picture doesn't convince you.
08:38:07 The the distribution of temperature, and density is hugely different and in particular, very impactful on the emission from these halos. So, this is an important constraint will come from a mission observations.
08:38:15 The Milky Way. Well, this is where I started many years ago and with the inspiration of Stu Boyer who passed away last year due to coven related illness.
08:38:28 We flew this experiment in the space shuttle that detected from the Milky Way Halo carbon for a mission.
08:38:40 And
08:38:40 since then, fuse the same oh six and mission.
08:38:45 In many areas of the Halo and.
08:38:50 However, there has not been a lot of analysis of these, there's also the spear experiment which detected many lines.
08:39:02 And I think this all relates back to Joel's original paper. Another inspiration for me on the Galactic fountain.
08:39:11 And, and the transformation of gas from.
08:39:15 Perhaps condensing out of a hot Halo into, into intermediate temperature phases and condensing on onto the Milky Way.
08:39:26 Okay, outflows.
08:39:29 I showed the radio spectrum.
08:39:33 In the multi on his eyes, the multi component ionization spectrum of this key so outflow. Here's some images, we see it alignment alpha helium nitrogen five carbon for your the line profiles.
08:39:49 And we can show that radio transfer allows you to measure line moment velocity moments quite accurately. And one of the most amazing things about it it's a very clear by like Conal outflow which fits a quite well.
08:40:09 But you can in fact, with this case of data. Fit show that there has to be rotation in the outflow. So this is kind of a surprise. It's the kind of thing you get out of imaging, that in fact you have rotating gas and an outflow.
08:40:23 That means that angular momentum is actually being ejected, but itself, which is surprising.
08:40:30 And this shows the velocity map, and the velocity model.
08:40:35 It shows this behavior.
08:40:39 This is amazing paper that just just referred to the penny. When Starburst merger giant bubble outflow from with the diameter of 100 kilo parsecs Amazing, amazing object with taking the case of UI,
08:40:58 and again they extract a large number, not only large number physical parameters, but they can isolate to outflow episodes, which I think is going to be something that we're going to see more and more, that there are multiple starve ourselves with episodes
08:41:11 episodes that can be detected in the mission.
08:41:16 Of course this papers on women off the halos from Chuck and Don urban and they're working very hard to demonstrate to figure out what's going on in these star forming galaxies.
08:41:35 At high redshift, and there's a huge amount of information in alignment alpha profile. Some people say it's ready to transfer Sleiman alpha How can you figure out I say it's an opportunity because it actually gives you information that you don't get if
08:41:44 you have optically thin emission.
08:41:47 So, we can we can we can actually exploit this to learn more about the actual kinematic mythology of the systems, and physical origins.
08:42:19 This is an observation by case of UI, I'm sorry PCTBY the polymer cosmic imager of what Sebastian cantilupe calls the slug Nebula, we found that it had this very clear shear call it protein galactic disk we had this discussion and one of the previous
08:42:29 that it's not really a disc were trying to come up with a new name like extended. The creating rotating structure.
08:42:33 So here's a case where we use bridge modeling to figure out what this is, this is the veil model deco Severino showing. For example, the velocity distribution in this influencing gas employee and rotating, but it's obviously complex.
08:42:53 How do you compare this to observations.
08:42:57 Well, first of all, you get better data and this shows what happens when you go from piece of utilize to case of UI.
08:43:04 So just think about going from cases we lie to I FOSS.
08:43:09 But when I first saw that I said well this is this, how can we possibly fit this.
08:43:16 So this is what we do we, we first take a simulation do for modeling and use something called we call the multi filament inflow model. So it's just a successive increasing number of parameters where you have a linear radio flow, you have a single mode
08:43:33 of info or outflow. So it's an azimuth Lee modulated radial flow with either sign with one mode just like a sign mode or two modes, three modes, so on.
08:43:48 And then you calculate the cookie information criteria for that and see when it falls and when it falls to a low number you know you've, you've actually, perhaps measured something so here's a case where by going from pure rotation to rotation plus one
08:44:08 mode of MSI inflow you the ice goes down by a huge amount.
08:44:14 That's the simulation run through Ford Model case of UI, and then this is one of our galaxies near Quasar illuminated galaxies and again you see the same thing, here's, here's the MSI for and the data.
08:44:31 Here's the second, the slug nebula.
08:44:33 Simple rotation MSI for in the data, so it works quite well.
08:44:38 This is a less massive system. It requires fewer modes, this is more massive system requires more modes.
08:44:45 But it's extremely significant and shows.
08:44:48 And the fact that that happens with the simulation. Well, tends to show that these, we might be seeing the same thing and though the simulations and the observations.
08:44:59 And when you do that you can actually calculate masses mass flexes and so on. And the system, the mass flux you get is, is comparable to that of the star formation of this central galaxy.
08:45:11 In those cases, so that's encouraging.
08:45:16 Okay angular momentum. This is something you can measure with a mission projected angular momentum in the plane in the sky.
08:45:24 You can look at just simple object sheer the same objects I showed you before Quasar illuminated.
08:45:30 Some sort of gas cloud.
08:45:32 This is the distribution of sheer and we do find, we went in search for other objects like these standard rotating structures. And we found a distribution of shares but there are an order of 20 sources that have very high shear.
08:45:49 You can measure the anger momentum parameter of the gas, and this is the distribution you get and this is the log normal Halo lambda, a distribution for halos anger momentum and seems to seem to fit.
08:46:09 There may even be some what I call spin orbit coupling the sources, you can compare the source angular momentum to the angular momentum of the whole system.
08:46:20 And there seems to be an access of sources that have their angle and either aligned or anti aligned with that of the overall system. And the fact that they could be anti line could just be the orientation ambiguity.
08:46:36 So that's, that's an interesting possibility that you can only get from imaging. Okay, a redshift dependence.
08:46:49 This is, I like to think of all these kinds of observations as controlled experiments will be very one parameter.
08:46:57 Halo mass star formation rate redshift okay so this is this is a huge variation, everything changes, low and high redshift galaxy sighs star formation rate specific star formation rate, angle event and quenching Halo size Halo density filament size, with
08:47:17 respect to Halo
08:47:20 galaxies hosting quasars, etc.
08:47:26 Here is a prediction for the CGM at low redshift and I and HL permission by lock worst, they're trying to observe it with the, with the
08:47:40 dragon fly narrowband version.
08:47:45 And we've been doing some observations with case of Vy to try to detect a child but since we don't have a UV satellite yet.
08:47:56 This has been led by Zara and Lynn.
08:47:59 And here's a case where we're observing fairly bright massive galaxies i star formation right.
08:48:09 And this shows, we're seeing a mission.
08:48:13 It's noisy, but in fact there's a, there appears to be a large enhancement at a very greater than 100 kilo parsecs, which is quite amazing and the overall mission levels are comparable to those same by Lacoste.
08:48:30 And the velocity of components for example the last version seems to be rising in this outer enhancement. very interesting observation.
08:48:41 Hopefully this will be published the next couple months.
08:48:46 And I just want to show the halo field of view again compared to that KCBI of course we have to mosaic this to get out to even partial of the ways for a variable radius, with Halo field of view, We get a lot more, all at once.
08:49:02 So galaxy Halo evolution.
08:49:14 And the halo mission.
08:49:11 As I said, the first goal is to basically learn how to extract physical parameters from lyman alpha and the other strong up lines.
08:49:21 And then, by surveying galaxies over the galaxy HR diagram, make connections between the halo properties and the galaxy properties in order to probe galaxy helical evolution, so that the multiple surveys, a reference survey would do basically go one,
08:49:40 looking at for example all the costs, galaxies.
08:49:45 Looking at Black Holes both active and not active.
08:49:53 So, this is my mental picture. Here's the galaxy HR diagram and we get a large number of galaxies, spanning all these parameters.
08:50:05 And we correlate those with the halo properties that we measure in a mission.
08:50:14 And in terms of cartoons. The goal would be to try to explain the bearing on conversion efficiency curve.
08:50:24 The equilibrium, that's occurring on the star forming main sequence, which may be some sort of balance between inflows outflows and star formation the galaxy show that the mass middle middle Felicity where they relationship is is connected to outflows
08:50:49 and try to show how the CGM is responsible.
08:50:55 The distribution of cold gas that can be created is responsible for the fall in the cosmic star formation. Right.
08:51:06 And so, in terms of observable and conversion factors, we do the reference survey to measure these empirical conversion factors and some of course with the functions.
08:51:18 And then hopefully measure.
08:51:22 Cold bear Kayla mass.
08:51:25 Both inflow and outflow mass and mass flux angular momentum dark Hello mass and warm very on a Kayla mass over this HR diagram with a knife galaxies in each region to make a statistically significant measurement.
08:51:45 Here's an example of how this was done.
08:51:51 Here's an alpha galaxy.
08:51:54 Above the main sequence.
08:51:56 With this beautiful mag magnesium to mission and virtual at all.
08:52:04 Did this beautiful conversion of the optically thick admission into physical parameters showing the large outflow flux in this in this what looks like an isotopic outflow with case of UI.
08:52:20 And this may even be able to see this post post when post a star from a new episode, this is a case where there's,
08:52:32 perhaps, perhaps extension galaxy, plus a galaxy, showing what looks like the relic New Relic wind.
08:52:41 Okay, finally I think it's very important.
08:52:45 I've added a few topics that we had more more weeks in this conference. I think the CGM IGN connection is extremely important.
08:52:55 And all I can say about this is here's this beautiful picture from the illustrious simulation, the paper but viral, showing alignment off and emission and showing in fact you can see the connection of these halos with the filaments of the cosmic web.
08:53:11 Okay, what's the future.
08:53:16 I promise that I will retire after all of these fly.
08:53:21 Of course we heard about Astra looks like a great mission to look at oh six and thereby galaxies.
08:53:27 We would like to do an emerald field.
08:53:31 Mid x Halo, but we might also be able to do a long duration balloon. That does it just a point seven.
08:53:41 If the kale survey decides we need probes then I would propose a probe, which has both integral field spectroscopy and multi audio spectroscopy over the UV.
08:53:53 And, of course, in the future. And of course there are many other ideas as well.
08:53:58 there may be an eight to 16 meter UV optical telescope, but it's not going to be in the next 10 years I can say that, maybe 90 in the next 20, and high red ship redshift of course we're about to have a fully equipped case of Vi with red and blue channel,
08:54:19 and had sex is under construction or almost question I'm not sure.
08:54:24 Blue music blues will be extremely powerful.
08:54:28 I don't know what the status is but I imagine it's going to be funded.
08:54:35 I would like to see and I focus on w SOS, I think that's going to be extremely powerful.
08:54:40 And one can imagine a dedicated Whitefield optical clinical field spectrograph with ultra large field of view and precision sky subtraction.
08:54:53 So, a mission like Halo needs broad community support, and would be a perfect complement to an extra mission like artists so this is the community that would be interested scientifically.
08:55:06 And
08:55:09 I think it's important to remember this, when you talk to your grandmother or funding.
08:55:17 Funding people, NASA people like in the elevator you have 10 seconds to make a case. Most of the matter of universes and halos, and maybe most of the action.
08:55:30 Determining galaxy evolution is in halos as well. And we've been spending a lot of time doing galaxies. But, as this conference has pointed out the potential for understanding what's going on with galaxies instruction formation.
08:55:50 By studying halos is incredibly powerful.
08:55:54 If you do an atheist search for galaxy plus evolution you get 56,000 papers 3 million citations.
08:56:02 So, I think that I'm preaching to the choir but I, it's time to try something new.
08:56:09 And there's there's a hope that halos are they Deus Ex Mako galaxies, which is a plot device whereby a seemingly unsolvable problem in the story is suddenly abruptly resolved by an expected unlikely occurrence, bringing the tale to a happy ending.
08:56:25 Maybe that will be the case.
08:56:29 And I just want to end by thanking everyone who participated in this conference and thanking the organizers for inviting me and for their incredible work.
08:56:40 I think they're, they're amazing group, and I think they deserve.
08:56:45 halos. So, thank you.
08:56:53 Sounds like we all deserve Halo.
08:56:56 Okay, so thank you so much Chris that was a great talk inspirational I think a lot of us are now filled with ideas for the future.
08:57:08 How about we hold on to those ideas. Let's come back at 905 for our picture, where then we will go right into the panel discussion but until 905 so that's eight minutes from now, you know, do your hair, make sure you look good.
08:57:23 And then also, head on to the slack, ask questions react to the questions that are already there using your emojis. And, and, yeah, we'll see you at 905 pacific time so five after the hour.
08:57:55 thanks again Chris for a great talk.