08:05:02 All right. Hello everyone. Good morning, and welcome to week seven galaxy evolution week.
08:05:12 I hope everyone had a relaxing weekend.
08:05:18 I didn't I had an intense and cold weekend.
08:05:22 I think we are all taking time off from this and doing some, some good, some, a lot of outdoor activities.
08:05:32 But we're back to this week and we do have a full weekend started full week, as well as the weekend for me.
08:05:42 And I think you'll be, you'll see that we have some, you want to attend all the events so I'm going to point out the halo 21 week seven evolution Slack channel.
08:05:56 And then I'm going to show our introductory slide for how to get gashes payloads affect galaxy evolution and inspired by Cameron, I'm going to change the, the, the, the figure here the visual each day so please put your most beautiful and most inspiring
08:06:22 visuals from simulations maybe from observations as well.
08:06:27 On the beauty Slack channel, and will update this this is actually a galaxy from one of my simulations that was reimagined, in a way, showing the cool gas and kind of the brightness level, the hot gas in the colored scale.
08:06:52 And it also shows Dark Matter halos which I think is kind of cool this is part of a planetarium show that we, we did here at CU.
08:07:00 So I think this is a really interesting question.
08:07:06 the, you know, there's no galaxies is a huge field of course.
08:07:10 But to have a galaxy you need a gashes component, a gaseous Halo. And that comes first. So, I like the order of the question gashes how to gas use a halo effect galaxy evolution.
08:07:23 Because galaxies need gas to form of course we all know that but we really addressed that this week.
08:07:32 I mean, go on and go through a few announcements before we get to our featured conversations.
08:07:41 As we continue to update the YouTube channel thanks Cameron for doing all this, we have a lot of new results from last week and Mark gave updates throughout the week.
08:07:53 And there are nine videos from week six so this is continuing to get more and more.
08:08:02 More and more videos and more. Each week, especially, and I have a belief, to, to announce one from Natalie, Nicole Sanchez on, you know, showing some nice movies actually showing.
08:08:21 You know, the genetically modified simulations that she has worked on and it's very nice work, and also something that was talked a lot about last week was Cameron traps work on inflows and radial transport in deaths and we saw a lot of these videos last
08:08:37 week so I encourage you to check those out, and continue to update those and we'll post them and announce them throughout the week.
08:08:49 And I will also advertise our on the market. YouTube channel sub channel on there, and there are three videos on there as well, that have been announced.
08:09:05 Okay, I'm going to keep on going through announcements and trying to get to our featured conversations this week.
08:09:12 So, this week we have two. And we have Nick, take Leah and dice Kane a guy talking about synonyms Zelda but CGM and they actually had an after party last week.
08:09:29 So I will let them talk about their plans and if they plan to do an after party this week. And also we have the continuing ongoing conversation which is featured this week of Halo 21 quenching the role of gashes halos.
08:09:45 And that's led by Joe Birkhead and also dice K, and we will let them decide how to talk about their, their after yo scheduled their after parties I believe they have one for quenching scheduled for tomorrow.
08:10:03 So we'll get to that in a little bit but before we do that08:12:08 And of course we have a lot of events today.
08:12:11 This week.
08:12:13 Yes, we have our keynote speaker.
08:12:17 Professor crystal Martin talking tomorrow. She's a local for KTP, and she will give keynote number one with a panel that we can't fully assembled with Nicholas boo Shay, Sean Chen, Stephanie Whoa, and Zach half and I reverse those last two names I don't
08:12:39 know the alphabet but that's okay.
08:12:42 And then on Wednesday we have four tutorials, so it'd be very active I suggest you somehow watch all of them will have the usual breakout sessions.
08:12:55 I've ordered them in a way that, you know, interest kind of our, our parallel. And I think this works for everyone. And if you miss one if you go to a breakout room.
08:13:07 You can go back and watch the recordings of the session that you missed. So we have at least a pillow pitch talking about the effects of environment on the evolution of satellites, something we haven't talked much about but it's very relevant for this
08:13:22 week.
08:13:24 Chris how cool give a tutorial on the observational constraints on CGM cloud sizes.
08:13:32 JOHN, Jonathan Davis spelled Davies pronounced Davis. I'm a collaborator and close collaborator I learned that late.
08:13:41 Late To The Party.
08:13:43 You're talking about Baron clearing how halos are cleared of baryons, and I think there's a black hole in clear, for sure. And, sorry, the heady will talk about element abundance ratios in the CGM, and how you can determine them.
08:13:59 So, all very relevant talk tutorials this week.
08:14:05 Then Thursday we have our keynote by Professor Greg Brian, who will talk about more from a simulation and theoretical standpoint, how gashes halos affect galaxy evolution.
08:14:22 And this is a another great panel with our co organizer Cameron how most Dylan Nelson, Mary PacMan.
08:14:31 And we got staging Shen to join us she wanted to join us more but it's late where she is. So I'm glad that she will participate in their program this week.
08:14:43 Okay and then on Thursday at later in the day we have a social events. Another round of Jeopardy trivia.
08:14:53 Thanks Jess for finding us this is great it's a little bit early, and I encourage you to think of it as an early happy hour this week.
08:15:03 And we will have some new categories.
08:15:06 I was pushing for an international flair. And, you know, I think this will be an intense week, a lot of after parties.
08:15:17 A lot of activity so I'm going to declare Friday to be casual Friday and maybe we'll have a theme. And you can discuss that on Halo 21, I was inspired by break a band reports, dressing up and wearing a hat last week so maybe you'll be hats.
08:15:35 On Friday, so I'm going to take it easy as a moderator on Friday and maybe make it a more informal Friday or more easy for you Friday.
08:15:48 We are going to have speak collaboration, after our breakout session so I'm going to have our featured conversationalist prepare to share their slides, and I believe I don't know who's going first.
08:16:01 But I will invite them to speak up.
08:16:08 And as usual, we will have these, you know, guidelines for our speak collaboration. So, let me see what time it is, it's about nine 816.
08:16:19 So, if we are ready. are you ready for one of the featured conversations.
08:16:27 Yeah, I think those UK has a conflict at about 15 minutes to go first. Yes, that's why I rush to do it. Great, thank you. Okay.
08:17:02 So, basically you want to share your screen, it's probably best if you sharing the screen case I have to leave, I probably, if that's all right. Okay, okay, yeah let me just get that right I want to make sure you can share the screen.
08:17:06 Alright guys see my screen.
08:17:08 Great.
08:17:10 I'll let you go ahead and take over.
08:17:17 Right, so, NIR the featured conversationalists has been called us for the halo 21 sec GM extended atmospheres discussion this week.
08:17:31 Um, so what I thought I'd do was just spend at least two minutes. introducing the SEC just for those who aren't familiar, and then we'll go into some of the conversations that we've had already has been mentioned we had a after party last week that basically
08:17:46 arranged.
08:17:47 And then Daisuke is going to.
08:17:50 If we get there in time which we should.
08:17:53 He's going to outline certain sort of the questions we want to discuss this week, on, on the Slack channel as well as in the after party.
08:18:03 Right, so we do have a Slack channel it's been there since almost the first week, I believe, and there we've been discussing various things related to the Z.
08:18:13 For those who don't know what this you know it'll go into effect is well there's several singers Zelda which affects.
08:18:20 And what it is is we're using the CMD as a backlight and so as the CME photons, come towards us right they interact with free electrons along their on their journey to us, and some of the ways they interact well there's a, there's one effect where some
08:18:35 seem to be photons inverse competent up scatter of hot free electrons that's called the thermal cynical Don't you think that's the more I guess familiar, as the effect, it was detected way back in the 80s, and that's the amplitude of that effect is proportional
08:18:52 to the line of sight electron pressure which can also be interpreted as the integrated integrated thermal pressure along the line of sight which can also then turn into the thermal energy
08:19:07 that, then there's the kinematic or kinetic SC effect and this is the fact that free electrons had a peculiar velocity with respect to the CME, so they act like a movie mirror, and that gives the CME a Doppler boost right so this looks everybody's familiar
08:19:22 with the Doppler effect so if the free electrons happened to be moving towards us that's a blue shirt if they're moving away from us. That's a redshift and that's a slight change in the CSV temperature.
08:19:32 So these two combined effects right we have line of sight pressure line of sight momentum.
08:19:37 If you're able to split apart the momentum and have some estimator for the, for the velocity of those electrons then you have a measurement of the pressure, and you have a measurement of the density therefore you have full thermodynamic information on
08:19:50 these systems.
08:19:52 What's really neat is one, the kinetic energy looks identical at least the first order to the cosmic microwave background so it just looks like a black body with a slightly different temperature and the thermal se actually has this unique spectral distortion,
08:20:07 where you have a deficit of photons at low energy and access it high energy.
08:20:12 Okay, and this is this shape right here is unique to the thermal IC so if you measure your CB and various different bands which we do, you can in principle, separate out this particular thermal SC signal from the other signals, like dust, like the CFPB
08:20:31 like radio galaxies. So this is what we're doing these effects are particularly small.
08:20:35 We have measured individual thermal and Connecticut see effects in galaxy clusters, but if you go down to sort of the massive galaxies to just regular galaxy scales, you tend to have to stack, or cross correlate to pull up the signals as they are, you
08:20:51 know, At least several orders of magnitude smaller than the than the fluctuations in the cosmic microwave background.
08:21:02 And these are extended what's really nice about the SEC is that you're not really sent Well, it's a pro and a con rated principle you really want to get down in there, and measure the, the thermodynamic properties inside the galaxies.
08:21:18 And that you, in principle can do with local galaxies or if we have really really large telescopes, but we're really the fraction limited here so at least with the current ground based experiments we have a better resolution one argument.
08:21:32 But we can prob, all the way up to several video radios so we can measure basically the transition of the IgM to the CGM, which is really nice in both density and pressure.
08:21:45 So just to give you an idea that's why we're calling it extended atmosphere is right where you know here's, here's a galaxy over here, and it's at the very very Center also potentially has some Dustin it, but you can see we measured the thermal I see
08:21:58 well beyond where the galaxy the extent of the stars and the galaxies.
08:22:04 So we had a discussion last week I'll let Daisuke mentioned mentioned this a little bit more, and there were several recent results that people presented on both the kinetic and thermal sZ.
08:22:16 We also had some talks about some theoretical modeling the various models people have, and as well as in frame properties of turbulence from the thermal se so if we if you can measure the pressure fluctuations you can infer something about the turbulence
08:22:30 in the CGM which is really cool and people have done this for the, the entire cluster medium.
08:22:36 So these are all there there's a video that basically posted on the Slack channel. Um, so you can all go if you missed it, you can go watch the video and watch some of the discussion, as well as the slides are linked actually to this slide deck so once
08:22:53 again I are done talking if you just continue on down to the slide deck. You can see all the slides from from that, that afterparty had last week.
08:23:02 So with that, I'm going to pass it off to dice okay who's going to tell us about what we want to talk about this week.
08:23:07 Great. Thank you Nick on so we'll follow up on the conversations that we started as a part of the kickoff after party last week, we're going to have a second one on tomorrow.
08:23:20 He says 20 a 18th both should be corrected the 23rd at 11:30am, to 12:30pm on the Pacific Time 230 to 330 on Eastern time. So here's a zoom link.
08:23:34 And the last week we talked, we had an overview brief overview of current sec measurements and ongoing modeling effort. So in the second after party we are planning to dig a little bit more dig our teeth into.
08:23:46 Some of these topics, discuss further about strengths and weaknesses of the SEC technique possible synergy with other probes. We want to discuss also about the future experiments.
08:24:00 What kind of science that we that can be enabled by using sec effectively in combination with some other multi wavelength probes.
08:24:07 We also want to start discussing more about how to make a specific forecast for different surveys different techniques, and some of the improvements in theoretical and computational modeling that needs to be done in order to develop the science case.
08:24:23 So that's going to be the main focus for the of the topic for the coming week. Our for tomorrow, and their minimum number of typos and instead of 11 to 12 I should I will correct this 1130 to 1230 tomorrow.
08:24:37 Okay, if you vote. Can we go to the next slide please.
08:24:41 So here are some of the, the questions and issues that we plan to discuss at the after party tomorrow.
08:24:51 This is similar and analogous is in part motivated by our conversations.
08:24:59 For the future observations that's coming up in the following week.
08:25:04 So last Friday we talked a little bit about what are some of the questions that we would like to address and discuss in order to define the science case.
08:25:15 That could be enabled with future survey, what are what are some of the parameters like mass redshift and radio range that are approved by different techniques and surveys.
08:25:26 We also want to talk about various ways of detecting sZ effect, such as the detail studies of individual objects to Varitek stacking and cross correlation techniques one are pros and cons of these different approaches.
08:25:41 In the process, we talked about number of systematic uncertainty facing sZ measurements, some of which has to do with how to do components separation, there are multiple sources in microwave sky that needs to be separated and distinguished using multi
08:25:54 frequency observations. So how can we actually do that, we need to think about how to do forward modeling and like things like dusty stuff I mean galaxies are extremely bright, and therefore, we are the potential potential contaminants for many of the
08:26:09 techniques of the of sZ pro constraints that we are expecting to get in the coming years. So we would want to discuss how to mitigate those systematic uncertainties.
08:26:21 With those future.
08:26:35 sec measurements forthcoming sec measurements we will then want to think also about some of the sciences that can be enabled by those measurements and here are the list of things that we've discussed so far about CGM measurements and what kind of constraints
08:26:38 that we might be able to to obtain using sZ effect. And of course how we can actually combine sZ effect with other wave rings and what are some of the sweet spots in terms of Halo mass redshift range and radio range that can be enabled by combining sZ
08:26:53 for with other groups.
08:26:55 We would also then want to discuss about the theoretical challenges and also simulation that are needed in order to refine the predictions and the also think about the simple man possibly Uber CGM model that can be used to interpret multi wavelength observation,
08:27:14 as well as making forecast for future surveys.
08:27:31 So there's that. And then last but not least, we would then want to think about what whether we actually need a new instruments, such as high resolution sZ spatial spectral imaging capabilities with large field of view, such as CMVHD, unless they are
08:27:37 these are proposed missions that are under consideration for future ground based opposite telescopes. And how many frequency bands are needed in order to mitigate all of these systematic uncertainties so we have a loaded questions.
08:27:50 We know we just had from the first after party we had, we got a glimpse of where we are now, but there are so much more we could do over the next few years to decades to come.
08:28:02 So we'd like to unpack some of these questions and we'll think about how best to organize in order to, to come up with some specific idea on directions and possible project that we can actually pursued together as a part of the halo 21 workshop, so I'll
08:28:17 stop here.
08:28:20 Okay, thank you, thank you guys Hey everyone, thanks for doing that in your like up against I think you have to teach, like on the half hour so you have Yes, minutes to spare.
08:28:32 Great job.
08:28:41 turn it over, I think Joe is going to talk now and I think we are going to have two concurrent after or no, not concurred two consecutive after parties tomorrow and Joe will confirm or deny that rumor.
08:28:56 Yeah, and hopefully you can see my first slide here.
08:29:02 Hello. Well, yes.
08:29:06 Okay, or Joe. All right.
08:29:09 So, yeah, I'm here this morning to introduce our conversation group Halo 21 quenching.
08:29:16 So, this in the background here is a breathtaking image, to me, an image of the four next cluster, which is very much, not what you might visualize for the prototypical galaxy cluster.
08:29:32 But I think dice k had this kind of environment in mind.
08:29:37 Whatever we we sort of conceived this this conversation group.
08:29:44 And, and we did so with a subtext of galaxy quenching and massive halos and the cosmic web.
08:29:50 So, before next cluster is very much a dynamic environment that is in an active state of evolution, far from far from things are far from being over in terms of the impact this environment is having on the galaxies within.
08:30:09 So you see lots of star forming galaxies in this cluster, in addition to the the more red and dead population that you might find dominating more massive clusters.
08:30:23 And so, however, a point that, you know, I think we've sort of refined our mission statement, a little bit, and come back to this in a bit but if we could refine you know so what we, what do we mean in in massive halos.
08:30:38 And I'll come back to this in a bit but if we could refine you know so what we, what do we mean in in massive halos. And so this is, you know, I would say Halo masses host Halo mass ranges, greater than 10 to the 12 solar masses. So this includes the environments of Milky
08:30:50 Way type galaxies in the dwarf population in our local group.
08:30:56 Through galaxy groups, and all the way to galaxy clusters.
08:31:01 So, what do gaseous halos have to do with all of this, So this is maybe something that looks a little bit more like the prototypical galaxy cluster, being completely dominated by by quenched red and dead galaxies.
08:31:17 And so really in terms of the galaxy. evolution that's going on within this environment, the circle galactic media very much as the point of contact mediating environmental impacts on on galaxies.
08:31:38 And so I just show here. This is the h1 covering fraction around the CGM of individual galaxies within various environments so from a purple to green to red.
08:31:48 We're moving from field galaxies into group environments, and then into cluster environments and we see a clear suppression in the CGM h1 contents of galaxies, as we move into denser and denser environments.
08:32:03 So perhaps this is an important piece of the puzzle in terms of drawing the connection.
08:32:10 Physically, between galaxies, their evolution in their environment. So, you know, we want to bear in mind that within this as as Nick and dissected just nicely illustrated that the hot atmospheres in you know around galaxies around galaxy clusters.
08:32:30 So this is presumably filled with, you know, a very hot intra cluster medium.
08:32:36 And then, you know what, I'm kind of plotting here is would be the the the gaseous contents of halos surrounding each of the galaxies within the galaxy cluster So, so I think this is, this is potentially an important, important mechanism that we would
08:32:54 like to know more about and we are sort of in early days, trying to understand this relationship. And we're really I think what led to us refining our mass regime, where we want to think about environmental effects and quenching in halos comes from this
08:33:14 work that Mary Putman showed earlier on in the workshop, and also at one of our two after parties we've had. So this is showing that as a satellite galaxies location within the local group is very much correlated with whether or not the galaxy galaxy
08:33:37 has a gas supply remaining in it. So, these are all non detections the open symbols here you see at small group centric radius.
08:33:47 For the Milky Way satellites.
08:33:51 And so, some key questions that that I think we've, we've sort of decided on and are converging on pursuing in this group.
08:34:01 How are gaseous halos and star formation related so I've talked about disruptive method mechanisms but there may very well be some constructive mechanisms to as seen in this beautiful jellyfish galaxy here where we see star formation occurring in the,
08:34:18 in this room pressure strip tail.
08:34:22 What are the dominant quenching mechanisms. Now, this is likely to various assumption of host Halo mass. What switching galaxies in massive say Tim is a 13 so our mascot.
08:34:35 Halo mass galaxies might be very different than what's happening a galaxy clusters, as a function of galaxy satellite mass, the more massive Milky Way dwarf satellites for example seem to be able to hold on to their gas supplies, which is presumably going
08:34:54 TO to affect their ability to continue forming stars state of satellite info, the relationship of weather satellite is sort of newly falling into a more massive Halo, for example, or whether it's more mature dynamical state.
08:35:14 And then lastly, the dynamical state of the group and cluster environment, as a whole, we, we find that more dynamically relaxed environments tend to have higher intra cluster medium for example.
08:35:30 So, so what is the role here.
08:35:34 Perhaps a precursor to all of this, what is a quince galaxy differing different definitions, certainly exists.
08:35:44 And then lastly, what are the observational indicators of, of any of these points that have raised, thus far.
08:35:53 So I think, over the next week, and two weeks, perhaps, you know, we really like to drive towards this final point, so that we can you know make some progress in this in this field.
08:36:10 So one thing we haven't yet really talked about, and I would personally like to like to hear from some of you, your thoughts on this but this is our team's cosmic web reconstruction scheme, showing the, the large scale structure, fitted from, from the
08:36:29 slum Digital Sky Survey from spectroscopic galaxies out to about a redshift of one so you know what is the impact of large scale structure on gaseous halos and therefore, the galaxies that reside within.
08:36:43 So this is just one result from Coronado con at all, 2018, showing that as a function of filaments centric distance galaxies tend to be redder towards the spines of filaments, and in their h1 contents, at least in the discs of galaxies, those tend to
08:37:02 be more h1 deficient towards the central regions of filaments so yeah we really haven't kind of gotten into the large scale structure aspect of this, which I hope we can.
08:37:16 And lastly I'll just advertise our after party tomorrow.
08:37:21 That's Tuesday, February 23 at 10:30am. Pacific time so that'll leave about a half hour break between our keynote session tomorrow, which I'm very much looking forward to, and our Halo 21 quenching after party.
08:37:36 So thank you and hope to see you tomorrow. Look for a lot more updates in the, in the Slack channel.
08:37:43 Great, thank you Joe, and we will make all those announcements in the, you know, in the tutorial section in the tutorial Slack channel. I also want to remind people that the staircase
08:38:02 talk today. The information that link for that is in announcements as well as general.
08:38:09 Looks like we will have an active day tomorrow, two consecutive after parties, 1030 and 1130.
08:38:19 And I'm going to definitely attend both.
08:38:38 So, Mondays are for the latter half after we do the introduction of the featured conversations, is we do speak collaboration, and I am going to we're going about, about to have a coffee break here just for like five minutes, or just a quick break and
08:38:45 then start speak collaboration but before I do that, I'm just going to share kind of the the you know the reasons why we do speak collaboration, it is to mimic.
08:38:58 You know what we can't do in a in person conferences, it's like having an extended coffee break and mingling and talking one on one with people so let me share our speed collaboration.
08:39:14 Slide.
08:39:16 And I'll just leave this up.
08:39:18 You know, this is for, you know, we definitely want people to participate.
08:39:25 You know, end of PhD and beyond.
08:39:28 And we highly recommend that you enable your video and we'll have five rounds today.
08:39:37 So, given that it is about 839.
08:39:43 Let's take a little bit of a break. I'm going to get us some coffee.
08:39:48 And some breakfast I haven't eaten yet.
08:39:50 And then be joined here at 45 after. So see you in five minutes.