08:05:02 Alright, good morning, everyone, and welcome to day four of galaxy evolution week and Halo 21. 08:05:14 Today we have great Brian as our keynote speaker. 08:05:17 But I have some announcements first. 08:05:22 Here's our image of the day it's foggy today. 08:05:37 And we'll have one more tomorrow. 08:05:31 I think that's density temperature and medalist city. 08:05:35 Yeah, and we actually have a couple of this week. 08:05:40 Do results video when from Stephanie Tennyson, they did with our related to work with our keynote speaker, and one with Sarah Appleby with Romeo. And I, I recommend watching both I've actually haven't finished watching the second one, and I've been in 08:06:03 communication with Sarah so about other things so I can't wait for that. 08:06:11 Okay. I actually I want to make an announcement and this is something that organizers have developed. Next week is is a different format for Monday and I think it's going to be a lot more interactive instead of speak collaboration for the second hour, 08:06:30 we're going to talk about future observations of course next week is future observations week. And so, we want your help in articulating and communicating the particulars strengths and competence. 08:06:46 Geez, compliments Harry ness of different observation outcome from military observational approaches, obviously, somebody else wrote this and improve this from my initial version, and I'm reading it for the first time I went to, I we got seven inches 08:07:02 of snow here and I went for some seven mile run in addition to shoveling. So, and I'm paying for it now. 08:07:10 We got seven inches in Boulder. 08:07:13 Yep. 08:07:15 Mondays. 08:07:18 Our will session will feature opt in breakout rooms focusing. 08:07:25 I'm sorry I just went skiing I'm tired. Okay. 08:07:25 All right. Yeah, we got it we should talk later. Matt Yeah you're in Carbondale. 08:07:32 So, Monday the second hour session will feature opt in, breakout rooms focusing on diverse array of observational approaches, and each rooms task will be to identify and describe what the observational approach will review about the CGM and report key 08:07:49 strengths to the full group. So, this requires this exercise requires both experts involved, expert volunteers and eager participants. 08:08:00 This is much better written then my, my first version. 08:08:03 And please go to a new channel Halo 21 AVS domains to signal willingness to be one of our expert volunteers, just post your observational domain, or domains, so that people know that you will be joining the discussions. 08:08:19 And we have initially identified these different observational domains and they're pretty broad and there's nine of them absorption land studies and mission studies, X ray fast radio burst surnames they'll dovish radio and mission includes 20 ones the 08:08:38 meter co so a whole range polarization gravitational lensing and just infrared infrared is its own 08:08:50 domain. 08:08:51 Okay. 08:08:53 And, very important. 08:10:02 So without further ado, And after stumbling through a couple slides there, I am going to introduce our keynote speaker, Professor Greg Brian from Columbia. 08:10:13 And I also want to highlight our panel. 08:10:16 That will take over in the second hour Cameron Hummels Dylan Nelson married men and CJ Shen. 08:10:23 So Greg. 08:10:25 I will share my screen and let you share your screen. 08:10:57 So thank you. I'm. 08:11:01 I'm really putting this talk together was really have a lot of fun. 08:11:06 So, I was asked to talk about the gashes how gashes halos affect galaxy evolution. And I'll talk about little sit in the moment my own spin on that. but I've subtitled this the circle galactic Cathedral, in part because of that sort of almost religious 08:11:22 experience that I've had over the last six seven weeks, exploring the CGM with all of you. It's been an enormous privilege I've learned a huge amount. 08:11:34 And I have to give credit to our, our fearless leaders putting together this program we've done I think a fabulous job, 08:11:43 but also because I feel like this is it's sort of a big city, the, the, the galaxy is surrounded by the circle galactic medium and one can make all sorts of connections between cathedrals and. 08:11:59 But But finally, as you'll see the center point of what I'm going to talk about is, is around an idea that the market I sketched out on my, my, my whiteboard. 08:12:12 Probably 15 years ago, of a stained glass window, and you'll see in more detail, but But first of all, I just want to I want to be clear about how well I'm interpreting this question. 08:12:25 And really, it's not just how gashes failures that affect galaxies but vice versa as well how galaxies affect their circle galactic media. So, I mean, divide this up sort of into two parts, although it'll actually be multiple components. 08:12:41 But, but essentially looking at how the black hole affects certain galactic medium and how the supernova feedback, and stars effect there certain galactic medium so I I stole this. 08:12:57 Thank you to Cameron Hummels for this beautiful image and. 08:13:02 So, I'm going to try and phrase this in terms of this diagram so this is what I'm showing here is the cooling time as a function of the viral radius and Halo me. 08:13:18 So we go from, you know, some Milky Way. Guess galaxies up two clusters on the right, and then down here to our lowest 08:13:28 dwarf ultra faint galaxies, on the left. So this sort of spans the observable galactic systems, and we go from a radius of something little point one or via out to, to the video right yes and of course, that's all quite arbitrary but the point is to to 08:13:48 sketch out and this cooling time is computed. 08:13:52 Assuming that the the profile looks a lot like an Fw profile with the density suppressed by the barrier fraction so that's one possible one one can, but but the broad picture is not debatable. 08:14:09 There's these regions where the cooling time is very long, and these regions where the cooling time is very short. 08:14:16 And that's going to influence how the circle galactic medium interacts with the galaxy of the center. So I'm going to take this diagram and I'm going to split it into pain. 08:14:30 So what I'm calling this the second galactic medium stained glass window. 08:14:36 So I'm going to start off with this phase, this region this pain. Over here, which I call the long cool. And this is the region for which the cooling time is is long, compared to the Hubble time. 08:14:52 so these are systems which, which, for which the the gas falls in hits the creation shock at the at the outer round the radius and the entropy is is enhanced. 08:15:06 And, and, and simply doesn't cool. 08:15:08 And so there's this is the simplest connection to the, to the host galaxy, there is no connection to those galaxy. And, and this is a plot showing the entropy profile for a set of Mr clusters SPH clusters, along with a fitting formula, which shows roughly 08:15:31 the entropy going as, as, as radius to the One Power so and and so I just want to show this because there's a lot of consensus This is the community, I think the simulation community has reproduced this particular result many times. 08:15:50 And indeed, if you can compare it to observations of the cluster, the entire cluster medium of courses, or the circuit galactic medium of clusters. I prefer to call it can be can actually be imaged out to large radius. 08:16:06 And so there's been a number of attempts to do that. 08:16:09 Here is one showing reasonable agreement with the X ray observation so this gives us some confidence that our overall picture of how gas inflow at least large masses is is correct. 08:16:25 But obviously, it's not that. 08:16:29 The connection is not very strong. So let's turn to the next page of this window, which I just, I simply called the Ag and regulation, we can come up with better than later. 08:16:41 And and you notice some, so it's goes down to about 10 to 12 solar masses I've tried to make that a little fuzzy because I'm not exactly sure where that boundary is. 08:16:50 But then I have this little also have this little cutout down here which I'll come back to in a little bit. 08:16:56 But I want to spend some time talking about this but not too much because this has been covered a number of, of, of, of tutorials, which I'll point out later so the. 08:17:12 So I take this nice plot. Actually, Mark, put it together it, but the data points come from paper by national sparring collaborators, and it shows the black hole mass as a function of the temperature the temperature the measure temperature of the of a 08:17:30 set of clusters. 08:17:33 Will down to groups and ellipticals as well. And it shows this very tight correlation. This is actually maybe one of the tightest correlations for the, for the black hole. 08:17:47 Galaxy connection. 08:17:50 And it shows that it falls along this line. If you take the black hole mass and you convert it to an available amount of energy. 08:18:03 Then you can compare it to the energy available for from from supernova which are given here, depending on how much to this just takes the halo mass converted to a stellar mass. 08:18:20 And then, depending on how much energy is available. 08:18:23 This these curves match. So, so one point. This This makes quite clearly is that supernova feedback alone is not sufficient to, to change the properties of the truth of what good medium. 08:18:36 We need he, but it also shows that there is this very tight correlation because the other thing, which should show in here is the stash blue line, which is just the, the energy of the circle galactic medium that's what that's what itself, and you see 08:18:51 indicating that, that the black holes are on a very deep level, the energy and input is, is, is deeply connected to the energy content of the circle galactic media. 08:19:06 So implying regulation. 08:19:09 So what is the form of that regulation. 08:19:12 Well, so, so one idea that's that's had a lot of talk is this idea of precipitation. I want to go into a lot of detail about this this originally. 08:19:22 This, this idea in various forms is quite old but there's this beautiful paper by Mike McCormick, and and shot and he quoted at demonstrating that in a, in a medium with thermal equilibrium, that it's unstable to precipitation if there's some if this 08:19:44 ratio of the schooling time to free full time is low some critical. 08:19:48 So a 08:19:51 number of groups have connected that idea to accretion up into supermassive black holes. 08:20:00 And the idea being that, that when precipitation occurs gas falls and condenses out cools condenses out falls into the black hole. Dry some bipolar those with high specific energy, which heat the CGM and return it to a state, so I can't resist showing 08:20:21 this, you want to lead. Did the simulation and produce this, this, this movie and set it to move it to the sound as well. I don't know if it actually comes through or not but anyway you can see the, the condensation which is occurring, and sometimes it 08:20:41 turns off, and there's a supermassive black hole right at the center this is about 80 kilo parsecs. 08:20:50 And, and you can see that this system and does indeed balance heating and cooling effect you can show that more more rigorously. So there's a fair amount of evidence, this is actually occurring in 08:21:08 in nature. 08:21:10 So here's, here's some results showing a set of clusters observed of clusters, showing their, the ratio of their cooling time to freefall time. 08:21:23 These are the ones which have evidence for cold condensing gas, and these are ones which don't. 08:21:31 So this this condensation. 08:21:40 This right this precipitation mechanism seems to be operating. And it. And so what is what is its prediction. 08:21:44 In, the prediction is that, therefore the circle galactic medium should be in this critically precipitating state. 08:21:51 Of course, this might be episodic. 08:21:54 There might be outflows, which heat the gas and then the guests returns maybe to even to a cooling flow state for a brief period of time. 08:22:06 And then 08:22:09 the healing begins again. But in general, it makes this prediction that the gas density should be lower. So this is a plot of again actually taken by, you'll see mark so work features quite prominently in the number of places in this. 08:22:27 So this line is, is the is the prediction that just the NFW prediction, and then the black line here is the it's the critical precipitation prediction. 08:22:43 And so it nicely matches the observations and the other point you can see is that it decreases the amount of mass in the system decreases as you go to lower mass system, because they, 08:22:55 their, their precipitation requirement implies lower density, and therefore they require the black hole to heat them up and, and to remove and keep them in this state. 08:23:11 So, this is, this is I think nicely being found also in in cosmological simulations, so I won't go into a lot into a lot of details because this was covered. 08:23:37 Very nicely by john Davis's tutorial presentation yesterday, in which he showed these very same plots. 08:23:36 So we're just shows for for eagle and illustrious and I want to focus at the high mass end here. For now, showing that first of all that there is this decrease and in fact, this decreases is simple to understand. 08:23:54 It just comes in the precipitation picture anyway it just comes from the idea that actually even more generally, comes from the idea that, as you go down in math, more of the, of the gas is is at a cooling time, less than the, the age of the, the cluster, 08:24:13 and therefore it has to either be heated or can condense out and cool. 08:24:20 So you can make very simple predictions for this relationship, 08:24:26 just based on on atomic physics, plus cosmology, which, which produces curves which look much like this. 08:24:36 So, but this of course goes on to show more than that it shows that there's this correlation with. It shows that the that it is in fact the black hole, which is responsible that for this because it shows this correlation between the, the black hole excess 08:24:52 mass, the expert access black hole mass and the properties of the circle collective community. 08:24:58 So this is. 08:25:07 Then, and one can go beyond that and look at, at the correlation between the black hole mass, and we're between the and the circle gliding medium, but also the star formation profit. 08:25:16 So, so halos which have, which have less gas tend to have lower specific star formation so this is a clinching mechanism directly connects the properties of the circle galactic medium and and also even the morphology of the, The, the rotation rotation 08:25:44 of the desk. 08:25:46 So as I said I, I urge you to watch. 08:25:50 John's discussion, those results in more detail. 08:25:57 So, the tangy collaboration has also looked at this question. 08:26:03 So this is a paper by by singer and all that and Elisa has has mentioned, and it looks at this, this focus on the right hand side here, which goes across this the stellar mass so. 08:26:23 And up here is the is the is the corresponding Halo mass, and it shows that that as we move up here that the entropy of the gas increases. 08:26:34 And that's because, again, because this this gas has to would otherwise have cooled created under the black hole and beat heated up, but also it shows this correlation with the black hole. 08:26:52 Mass. 08:26:54 And the kinetic to thermal energy mode of the of the of the black hole feedback. 08:27:02 So, so this is showing that this is a nice 08:27:13 demonstration of the preventive aspect of the of this, this feedback. 08:27:18 There is also some interesting as it's interesting paper by, by, Erica Nelson, showing some evidence for an objective component as well. 08:27:31 It will be one of the interesting questions is what is the importance of these two kinds of mechanisms, the black hole. 08:27:40 Either ejects the gas in the disk to quench or it prevents it heats up the psychic medium and prevents is in full so these two different modes are quite interesting to look at. 08:27:55 So, with with graduate student at Columbia Brian Lou looked at this recently with a more calculation, exploring different modes of accretion. So one in which the accretion onto the black hole is dominated by torques and another where it's, it's driven, 08:28:18 just by the traditional bindi coil prescription. 08:28:22 What we found is, is that in both cases, there were some interesting differences, but the preventive nature in both case was the was the primary driver for the suppression of gas inflow so this shows the, the 08:28:39 decrease in the amount of gas which was flowing in in from redshift one to zero. 08:28:45 So this is how much the inflow decreased versus how much the outflow increase. So, in fact, mostly. So, so this is the sign of objective feedback outflows massive outflows driven by the supermassive black hole where this is a sign of preventive feedback 08:29:06 mostly gas, preventing from be flowing, flowing, flowing in. 08:29:13 So one of the key questions I think which we still don't know is how does this Ag and heating actually occur. So Dylan Nelson went through I thought a very nice job of talking about the various numerical algorithms which are physical algorithms which 08:29:28 are used in various simulations to inject energy into the, into the galaxy into the circle galactic medium or the galaxy. 08:29:40 And and 08:29:43 I think the. 08:29:47 So in particular how much of this, there is this a jet is it a wind. 08:29:55 Where does how does the heating actually occurs it's shocking is it mixing of hot bubbles. 08:30:00 So, here I just I think we don't know the answer to this. 08:30:05 I'm just throwing this up. This is Tony Sue. 08:30:09 Some recent work by by can be exploring many different models, I have to read this paper to get actually be able to read this. He did simulations of many different models with within the fire context but these are all idealized tend to the 14 solar mass 08:30:29 halos, and one of the coin some cosmic ray feedback which which was quite actually successful in quenching. 08:30:38 But one of the interesting things that came out of this is, is that the width of this cocoon so generically the jet drives. 08:30:48 Of course this bipolar outflow and produces a shocked cocoon, which, which can, depending on the energy density, the mass loading of the, of the AGM jet can either be quite elongated or quite round and so what we found, what can you found is that in order 08:31:14 to get suppressed cooling it needed to be relatively round, that if this jet was was too much like a drill, then the energy was deposited too far out and and cooling was not successful. 08:31:29 Of course, this may vary depending on different mass halos. So that's a natural next step to look but lots of other people have have looked at the impact of a GM jets. 08:31:42 And I think, including you only who looked at this and found it was primarily shocked at which did a number of many week shocks of this cocoon, passing out, which did the bulk of the healing. 08:31:57 But, but turbulence mixing cosmic rays are also all potential energy sources, I think this is a question we don't have the final answer to yet. 08:32:07 Okay, so that was a gn regulation. 08:32:11 Next I want to fill in this little gap down here, which is where type one a supernova heating can be important. 08:32:22 So, I, I want to look at briefly summarize one particular model for this type one a super nova heating. 08:32:34 But I want to just point out in general that there's been some nice work Daniel Wang, did some early work. 08:32:46 Looking at this point, because there's a. This, this range of masses for which type one a supernova heating can be important. 08:32:51 Right around 10 to the 13 solar masses. 08:32:54 For for halos galaxies. 08:32:59 Low masses. There's just not enough population of gold stars, and for halos of higher mass, the potential well is too deep for this to be have an important effect. 08:33:12 So type one a supernova. This is an estimate of, if you, if you take a population which is about 10. billion years old, and you take the energy input from that and you divided by the mass loss from stellar wins and other products, then you get a specific 08:33:32 energy, about 08:33:36 which is comparable to the specific energy of the CGM in this in this room. 08:33:43 And so, so this particular model that Mark has put out, just recently so I'm gonna move through this quite quickly in Halo 21 question which he goes through this and in considerably more detail, but very quickly. 08:33:57 The point is that, 08:34:00 that, that, of course, one crucial point is just this, this, this balance. 08:34:06 But if you, if you take the CGM entropy profile as some power law with radius. 08:34:16 Then and and require it to be an equilibrium with a with a wind, then the resulting enterprise profile has a has a form which which can be written in this like this. 08:34:31 And it started. So for which becomes steeper as the circular velocity increases. So that makes sense that low, low, circular velocity when the potential well is is narrow this specific energy dominates the gut and the wind just flows out. 08:34:52 Whereas, as its deep into it has to do more work. As far as the potential will deepens. It has do more work. And so the the entropy profile Stevens. So there's a critical profile such that 08:35:08 this balance occurs and and also that happens to be also the critical profile for which the to the cooling time to freefall time ratio is a constant. 08:35:23 So that makes this interesting regime right around. 08:35:26 So, so this power law of two thirds occurs right around a mass of about 10 to 13 or circuit or circular velocity of 330 kilometers per second or velocities version of about 240 coins. 08:35:48 So, so the idea in a nutshell if we is, is that right around this, this critical point of about 240 kilometers per second, where the curves, the profiles are all critical, or, or somewhat above that, then we have this, We have this two phase kind of this 08:36:13 this, there's there's. If the outer CGM pressure is is low. Then, the solution is allowed, such that the cooling balance of heating and air this this wind is ghost stable. 08:36:32 And, however, that deposits mass at large radius, or there can be accretion, and that drives up the, the outer pressure. 08:36:42 And so, eventually, that other pressures boundary condition is high enough here that the disc profile. 08:36:50 No longer can balance. 08:36:53 And then the gas accrete onto the circuit but the black hole the center and heats up. The CGM, which then the outer CGM the jet submitted to narrow thingies gets out heats up the CGM decreases that math, the density out there decreases the pressure. 08:37:16 And you return back to the state. So this is a cyclical process in which the black hole operates as a valve. 08:37:25 And this the type one a supernova either effectively Staveley sweep out the material or they don't. 08:37:32 And this operates most effectively at higher, higher mass. 08:37:42 And, and above, so this. 08:37:45 I just I'm focusing just here on this picture on the right for this critical velocities version. and above. And, and this just is a depiction of this idea that this odor CGM is heated by ag periodic AGN jets, and they're controlled by the. 08:38:12 This, this type one is sweeping energy wind type on a driven when. 08:38:21 So, so, then so there's other possible ways in which, of course, what's the type on a hidden can can play a role. 08:38:30 But I want to get into. 08:38:36 into this fourth pain what I call the core collapse supernova regulation things region so down it at masses below 10 to the 12 so the masses are so, 08:38:49 And 08:38:52 where the energy and put it for the CGM has to come from, from supernova. Well, we're at least can come from supernovas was there, there may be an AGM contribution as well. 08:39:06 But I'll assume that's that's mine, Of course, 08:39:11 as it's been noted a few times before, for gas for for halos this mass and below the, the shock. 08:39:25 The cooling, time is very short emphasized in the first diagram showing the cooling times, and and therefore 08:39:38 Birnbaum and Dekel showed that the shock actually the spherical case doesn't even for that it's unstable below. 08:39:47 This, this crucial mass and this, and in the absence of any feedback, then the, the, the gas flows in and is largely cold and and and do Shanda done a nice job of talking about all of the, the recent results on on called filament free flow. 08:40:08 So, 08:40:09 so I want to focus instead on on this, the regulation part. 08:40:15 Certain regulation of the of the of the CGM and and so I want to highlight here is a pair of simulations done by Drummond fielding a few years ago, which looked at Hilo mass here these are two different simulations time it goes down from top to the bottom. 08:40:37 They're both for 10 to the 11 solar mass halos on the, the only difference here is the mass loading of the, of the week. 08:40:46 So here on the left, the mass loading is high, there's a ratio of of five in for the wind ejection to the star formation rate and just to be clear, these are simulations, which essentially cut out the very center. 08:41:04 So there's no attempt to model the galaxy itself, any get in Guinea gas which creates on to the center is injected back with a certain amount of mass certain amount of energy and a certain loading fact. 08:41:22 So, 08:41:22 so it's loading factor is quite high, than these winds are our very own dominated. And so cool rapidly so you can see an outflow here which is quite cold. 08:41:33 And then in the end. Essentially what you just what you get is 08:41:49 On the other hand, if the, 08:41:52 If the Maslin factor is low, so that specific energy of the outflows high, then you can produce it, a shock and hotter gas. Now, in this case I mean so on the left here I showed the Drummond shows the 08:42:11 shock radius as a function of the veal radius and and so you can see that this this plays a key role in whether the hot Halo with setup. 08:42:21 And so you can see that this this plays a key role in whether the hot Halo is set up. Now to be clear in the even in this case on the right. You didn't find as much evidence for for this kind of precipitation picture that we talked about the flow here 08:42:33 is still very chaotic with, and the pressure support is, is, is significant. As Cassie lock house, showed by analyzing things them simulations later, is the, the dominated by by turbulent motions of the gas and not by the thermal pressure. 08:42:55 Although, I think this is still an open question the energy of these of these winds is still not that high the specific energy. 08:43:05 There's more specific energy which could be injected which is available from. 08:43:10 So, but the point here is that it shows some key question, if we want to understand the, the properties of the circle galactic medium in these low mess objects, then we need to be able to answer this question. 08:43:26 So, does are the outflows high in specific energy or low mass loading or or vice versa. And this turns out to be a critical question, because, as I just showed it. 08:43:43 It determines what is the thermodynamic properties of the circuit galactic meeting and Dylan I thought, also did a beautiful job of talking about particular within the context of tg work of the, of the outflows of properties of the outflows and those 08:44:01 simulation. 08:44:03 So, so I want to actually focus on something, try to answer this question in a slightly different way, which is to focus down on even smaller skills. 08:44:13 So, 08:44:16 the problem with cosmological simulations of courses that they can't resolve the individual supernova set off tailored blast waves, and so have to make some sort of approximation for understanding the feedback from all of these, these supernova explosions. 08:44:31 So this is just said going, his chin goo Kim's beautiful Tiger a simulation results in which they can resolve this. 08:44:45 And, and can can only see the, the driving of individual outflow. so this is shows many different properties, what I want to focus on is the temperature of this gas is, there's a lot of hot gas which is flowing out. 08:45:04 Notice it, it's the it's the hot component which is the high outflow velocities and the colder component as as generally actually info. 08:45:14 So these are very useful to understand the outflows of course the weakness here is that they don't go beyond a few killer parsecs, and they also don't have the global geometry. 08:45:26 So diving into those simulations into a little bit more detail. So here's one, this is 08:45:37 set up to mimic the Milky Way at about a four kilo per sec somewhat more star forming than our local region. 08:45:48 And, and this shows the outflows as the function of times right click to the time axis here. 08:46:02 But this is, this is a border Giga here so this is the red shows the outflow of the cold component. 08:46:21 And you can see it's undergoing a galactic founding flows out and gets to about a killer Prosecco so and then comes back down. On the other hand, the hot component flows out and escapes, in fact it's, it leaves it more than the escape velocity and and 08:46:36 this just shows that so this paper changers paper has has many beautiful results and looking at a wide range of different box conditions. And here's one that I just pulled out which just shows the mass loading factor of the cold gas. 08:46:50 The intermediate temperature gas and the high gas, and you can see that one of the really interesting results is that the mass slogan factor of these calculations is actually quite low. 08:47:01 and it is decreasing with height. 08:47:04 So now, since dropping below point one in these cases. 08:47:11 On the other hand, the energy. 08:47:14 If I would show a similar plot for the, the energy lovely factor. It's dominated by the hot actual show results, which later but and is constant. 08:47:25 So, this is interesting result. 08:47:30 So, 08:47:55 Evan Schneider, so this this beautiful, beautiful 3d image I won't show that's been shown before from the seagulls calculation which 08:47:48 has similar high resolution, but has the, the geometry of the other of the full system, and this produces a similar result, the outflow massive flow is dominated by the hot component. 08:48:04 And as is the energy and the, the mass outflow in the cold component is dropping at larger radius. 08:48:11 So, these are high specific energy outflows. 08:48:16 The cold, there is a cold component definitely very interesting, but in detail it seems to be getting in trained a small radius transported outwards and then mixed back into the hot medium at large ratings. 08:48:31 So this tell is telling us something about the basic dynamics of the outflow. 08:48:49 So Amelie collected together a set of results from a wide range of these toolbox calculations, many workers, using many different codes Amr codes. 08:48:56 fixed grid codes SPH codes. 08:49:00 And, and found as long as you had very high resolution, this basic outflow result seem to hold that most of the energy came out in the form of the heart, and not the cold in fact Dylan, I think showed, very similar results for tng 08:49:22 and and these match the specific this seemed to match the X ray properties observed in in some of these outflows. 08:49:33 In fact, the things like MADT seem to show very high energy civilization efficiencies and are producing very high specific energy of 08:49:48 the. 08:49:50 I won't go into a lot of detail about this but the the hot outflows also carry metals. 08:49:57 So here's a. 08:50:01 Again this compilation from from meals paper, which shows the correlation between the energy loading factor, and the middle loading fact. 08:50:08 So that's, again an indication that these outflows are really coming straight from the supernova. 08:50:17 Okay. So, given all that. What can we say about the CGM galaxy connection. 08:50:25 Well, we don't have an answer for giving you some, some reason to think that the outflows may be high specific energy. 08:50:34 But I think we don't yet know we hit those simulations I showed you before, don't cover the full parameter space that are that are required to understand this. 08:50:46 So, so we can have a few different ways of thinking about this one is that the CGM is heated up is largely hot, not to say that there's not cooled phase. 08:51:02 In fact, in a hot pressure supported medium, we naturally arrive back to this gas precipitation picture I talked about before. 08:51:12 Another possibility though is that these the loading factors of the winter are high and the CGM, especially as we get to these lower mess he listens relatively cold is in fact supported by, 08:51:24 by, by some sort of turbulent Lake process and the clouds are really juggled or rejected, rather than in some sort of equilibrium state in which case, what's really important here. 08:51:37 These two states are these two processes are quite interesting because in a the crucial thing is the cooling which controls the structure, and the accretion and hence the star formation, whereas be. 08:51:52 It's really the physics of the winds, which control the CGM property. And then finally, I won't really unfortunately don't have time to go into cosmic rays. 08:52:03 But there's been lots of nice work by a wide variety of groups, looking at this and and in this case the cosmic realm. 08:52:13 The cause of the CGM is in the extreme case in which its cosmic rate pressures supported. It can be cold in in regions, but still pressure support, I think, 08:52:28 a nice simple picture, 08:52:32 explaining this picture is, is, sort of, this, this, this situation is still needs to be worked on. 08:52:43 So I will say if it is in fact precipitation and regulated by a supernova. 08:52:49 Then, then there is this nice prediction prediction, simple model. 08:52:59 Mark put together a few years back, in which, if you if you just take the simple idea that this requirement of the precipitation requirement applies to low density halos then remarkably, because the cooling rate is the, that is the CGM mass divided by 08:53:19 the cooling time, and the CGM s depends on the cooling time, then the creation rate ends up being inversely proportional to the, to the cooling rate. 08:53:31 And so, paradoxically, the faster the cooling. 08:53:35 The more effective the cooling, the less master is too cool. And so the less star formation. 08:53:41 And so this is a comparison between a compilation of galaxy mass fractions, versus this this prediction, assuming this, the precipitation picture. 08:53:56 OK, so the. 08:54:01 If the to better understand the in the flow of mass from the circuit collecting from the galaxy and full mass momentum and energy from the galaxy into the circle galactic medium. 08:54:16 It's useful to go into the simulations to measure. 08:54:21 So, so Dylan talked about some of this. 08:54:25 This is an upcoming paper by barrage Pandya, who was looking at the fire simulations and trying to characterize all of these loading factors in two places one out of the galaxy so out of the ASM and into the CGM, and to it, out of into and out of the 08:54:47 CGM from the circuit, collecting it. So I'm going to focus first of all on mostly on this region. 08:54:55 The outflows between the galaxy in the circle galactic medium. 08:54:59 So I'll just quickly show this movie, which is one of the fire halos This is attend to the 12 solar mass hell fire Halo. 08:55:10 You're so it seemed this outer line is the barrel radius. And this is a zoomed up resumed in region in which you see the, the outflows and the inflows and basically what I want to point out here is that many of the outflows are hot, but not all of them 08:55:25 in fire. Some of the outflows are actually cold and this characterizes that this is a phase diagram of the outflow in material and you can see much of it as it's hot, but there is a component, which is going out. 08:55:37 Cool. 08:55:38 And then this is correlating it with the star formation rate. And this is a radio view of the inflow and outflow. 08:55:45 So, so there's lots of interesting results from this. 08:55:51 I want to pull out two things. One is that is, it's just a characterization of the mass loading factor in the fire simulations, 08:56:00 as a function of the stellar mass as others have pointed out, I think, more tough, analyze a similar set of simulations. 08:56:09 This work does tries to do a look and improve job by removing gas that is not going to make it out to the circle galactic medium, by doing a cut on the brewery parameter. 08:56:24 But for the Mass Effect of the results are quite similar. And the mass is carried partially in the hot phase, or the high mass halos almost all in the hot phase for low mass surveillance halos it's low in the, in the warmer face, but keep in mind that 08:56:39 the temperature of these, these guys down here is actually close to 25. So part of this is just the fact that these flows are the variable temperature, as I'll show you in a little bit. 08:56:52 And then the other thing. 08:56:54 So, one can also look at momentum and metals, but the thing I want to pull out here is the energy loading factor, which shows how much energy is actually getting out of the, of the halo into the, into the circuit into the circuit galactic medium. 08:57:10 And this is it depends. Depends on redshift and on Halo. 08:57:17 But generally, interesting enough at at a higher redshift when the outflows are burst here, and it's lower, lower masses, the energy flowing out is higher, and and is comparable to the energy available in the supernova weeks in some cases, at least that 08:57:33 early time. 08:57:36 And as promised. This energy is carried largely by those hot fixes. 08:57:44 So, 08:57:47 finally, I want to turn to the lowest mass Halo so I'm almost at a time just good because I'm almost out of other things to talk about here. 08:57:57 This these, these these very low mass halos which have very low temperatures. And I can't resist throwing this in. If you go to the very lowest mass halos that one can imagine forming stars on population three objects that they also have a certain galactic 08:58:17 medium. 08:58:18 So, this is a calculation of a 10 to the six solar mass Halo average of 20 So one has to make it redshift adjustment so it has a virile temperature, less of a few thousand degrees. 08:58:36 And what you see is that it actually has a nice circle galactic medium This is a zoom in, here's but here's this hot, medium, and the center is cooling. 08:58:47 So here's the thing, this is a zoom in six parsecs and then even smaller. 08:58:53 And what's interesting here is that this really does form a cooler classic cooling flow 08:59:02 Jonathan stern stern has has developed some nice some nice models this this really is just flowing in the compression time is equal to the freefall time and gases is actually fairly stable and and so this is a classic, who we flow situation. 08:59:23 And so, this is a classic, who we flow situation. So for once you introduce metals. 08:59:29 Then things of course get more complicated and you go to higher slightly higher mass, then think back again becomes important. 08:59:36 So, I just want to highlight this work. In this context, one one thing that came out of this work that the garage led so this is a another paper which came out recently, comparing the fire calculations to semi elec models. 08:59:54 And again, there's lots of interesting results, but the key one I want to point out is that the for 10 to 12 so mF halos both the semantic model and, and fire predicted similar CGM masses. 09:00:08 But the SAM under predicted drastically. 09:00:12 So this is Rachel Somerville semiotic model drastically under predicted the amount of circle galactic medium. 09:00:23 And, and this was interesting because what it's doing it, what it was doing is, it was just using this very short cooling times and assuming that the gas at the cool very rapidly under the galaxy, and therefore required very strong objection. 09:00:40 And 09:00:43 out. 09:00:44 But the other thing that was happening is that the, the fire simulations predicted, much lower mass inflow rates at the odor at the virile radius so you remember I drew those two circles one. 09:01:05 The is m. at point one virile radius, but the other out of the bureau radius. And this shows the mass in flow rate as a function of time. 09:01:11 For these various different halos so the red is the high mass halos, but I want to focus here on the low mass halos the tend to the 12 ones those those. 09:01:22 The fire inflow rates were down by a factor of 10 from the simple prediction that the the berry on inflow rated the viewer radius is the barrier infraction times the dark matter accretion rate, which is what similar models, almost always take. 09:01:43 And so this required the SAM to work extra hard on these limits he wants to check. 09:01:49 So, so one thing I made the interest of time actually I'll skip over this and just show you the movie. 09:01:55 So this is the same thing I showed before, but now for attended the tensile a mess Halo and. And what you can see is that these guys produce shocks which go way out beyond the bureau ratings and the heat gas, many times the bureau radius. 09:02:16 and so they really completely control their own surroundings, that what that means that they set their own inflow rate, which is much lower than what you would like we predict. 09:02:27 So these produce some. So this outflow. 09:02:31 For these low mass halos really changes the properties of the circle of the intro into intergalactic medium will be on the view, and that causes the info for rate to drop substantial. 09:02:49 And actually, let me, I will. So these are just some simulations done by an undergraduate at Columbia. And I just want to emphasize that for halos have around 10 to the 10 solar masses that we're finding that the temperatures of the circle galactic medium 09:03:08 are actually around the temperature. 09:03:11 Not even though the video temperature is about 100,000 degrees. So, not too far from the peak of the creature. 09:03:21 and. And so, the density is much lower. 09:03:25 But the cooling time is still quite long. 09:03:29 For these systems. 09:03:31 What is controlling the CGM properties in these very low mass halos well in the inner regions, actually maybe precipitation, we've got gas around this critical factor of 10. 09:03:41 But in the outer CGM it's clearly not, not, at least not in the simulations, something else, is, is keeping this gas, rather than it's not in the critical precipitation balance. 09:03:55 So there's lots of interesting possibilities photo and ization cloud density contrast is low. 09:04:03 I completely skip angular momentum because crystal Martin did such a great job of that. And I'm going to completely skip satellites. Because, and Elisa did a fabulous job of that and when. 09:04:15 So thank you to both of them for making my job a lot easier. 09:04:20 And I'm just going to stop and leave you with rather than summaries question. 09:04:41 And what is the process which really sets the disconnection. Is it, is there some simple like precipitation some simple model which which controls the, the structure or is it something, is it just simply that the outflows ar, ar, ar, ar throwing out a 09:05:05 a lot of math. So, thank you. And I'll stop there. 09:05:11 Okay. 09:05:12 Thank you Greg. 09:05:14 That was has a very comprehensive 09:05:18 keynote, and I like those questions at the end I took a screenshot of, in fact, we are going to take a will take us. Come back at 10 912. 09:05:32 We need a better six or seven minute break. 09:05:36 And I encourage everyone to go to Halo 21 week seven evolution to not just ask questions, we got a few there, but also to vote on them and see what you would like to discuss, so we'll see you here back here in about six minutes.