09:35:02 Okay everybody, welcome back. It looks like from from my view of the breakout rooms.
09:35:10 It looked like there were some very there must have been some very exciting conversation so, except for in the polarization room. It was such a sad room there was zero people in the polarization room, the entire time that we were talking.
09:35:25 This isn't to slander polarization as a future.
09:35:31 You know, Pathfinder for CGM science it's just started, probably reflective of our lack of expertise.
09:35:38 Hopefully you identified yourself or if you didn't decide in advance, go ahead just put your hands up, and I would love, because we only have nine rooms right and we have 25 minutes so it's really short right two to two to three minute kind of summary
09:36:03 of what happened in these rooms, and what you thought were kind of the most exciting constraints that you're going to be able to make on the CGM in the next in the next decade.
09:36:15 Alright so I'm seeing some hands already and I'll just go in the order in which they're raised and so we'll start with farty.
09:36:27 Thanks Jess so we had a discussion on gravitational lensing and identified a few areas that will be very interesting to pursue in the near future. So, one of which is saying.
09:36:45 These are scale lenses, especially for looking at the giant octet that are produced by gone gas is what has been learned spot is foreground lensing clusters.
09:36:58 So some of the things you mentioned was that could be done is to resolve the equivalent with special results the equivalent with absorption like magnesium to, as well as the kinematics on scales off easily.
09:37:21 10s of your parsecs around program galaxies, and this can be done with this.
09:37:17 Seeing limited data at essentially a beam sampling scale of plastic is probably useful in on the understanding the distribution of things like magnesium to on individual gas is a special distribution but also really understand kind of modeling the gas
09:37:38 flows, for example, you know, trying to model in terms of outflows or repeating this. And so this is something that Sebastian Lopez has done in the past couple of years and he has published I think two papers on two systems and, according to Sebastien,
09:37:53 we can really do kind of experiment with on the order of a couple of Dustin appliances for the next few years with 10 meter class telescopes and Instagram fix fields factor we have slightly so that seems to be something that we're very interested in the
09:38:09 near future.
09:38:11 Nothing that we discussed is using Lance quasars which is something that people have done for decades now, but right now. Another interesting thing to pursue is to look at the spatial distribution and the incidence of cool gas around this rap gasps things
09:38:28 which we thought that they don't show any progress but many of them do and this will be very interesting to partner with you to understand their business and their physical conditions.
09:38:42 Another thing that will be interesting, is to look at last questions and try to understand what the method was the mixing scale is in the hierarchy of CGM because you can try to see you know if you keep going to small scale so only can you understand
09:38:52 the cloud sizes of this absorbers but you can also try to understand. At what point, if you keep the progress with smaller scales along pair silence you actually stop seeing any variance in guess metal so they will tell us something about the physics
09:39:04 of the mixing in a CG and especially the mixing scale something we didn't really understand at the moment.
09:39:10 Excellent, thank you so much yeah there's tons of exciting stuff everybody, I apologize for the rudeness of the reaction, faster, but that's what I'm going to give you if you start going over two minutes.
09:39:21 Alright so let's move on quickly the next week guy, young Zhang.
09:39:27 Yeah, thank you. So, there was Claudia six homes markers, and also Michael stands in my room, and we talk about three things. First is in a centimeter meter we talked about like different tracers and seal.
09:39:42 For example, and there we realized that there are a lot of things can do with submillimeter, especially that you can eat really powerful can still resolve a lot of structures even a higher rushes, and a few things to identify or wine ratios for example
09:39:56 a mechanistic, and also the mass of all those molecular line tracers.
09:40:02 And then we move on to talk about a child. Each one is Michael is markers bring up this point out through that he can continue we can measure the magnetic field strength, and also the polarization.
09:40:13 This might be one of the few situations we mentioned polarization. So that is kind of exciting, and especially for stuff very near that this perhaps we can measure the mythology of the magnetic field.
09:40:25 This is something that might be interesting, and eventually we start to talk about each 121 centimeter initialize, and this will be really powerful with a lot of SK Pathfinders, which can result down to very small scales, but it does have a limitation
09:40:39 that it is very limited to nearby stuff like very low rushes, and it's powerful at resolving the structures of high velocity calls in a milky way down to.
09:40:50 I don't have the numbers in mind. Maybe 100, a few hundred percent probably and but it gets really hard. If you want to extend beyond the local volume in general.
09:41:01 And then finally, Michael stamp bring up a really important point which is a pipeline development which is something with Do not talk about at all in this conference.
09:41:08 But I do think it's important because we do have a lot of data, sitting there but we have not talked about how to best use the current data and how to best development pipeline to make sure that on the signals can bring to life.
09:41:20 So I think this is something valuable to talk about in addition to thinking about future missions.
09:41:26 That's all.
09:41:27 Perfect. Thank you, young I was well timed as well my timer didn't even go up you had 10 seconds left.
09:41:33 Okay, so the next hand that I see is Lee armas.
09:41:40 Okay thanks Jess so we we had a good discussion we opened up a little bit about sort of the basic diagnostic so the infrared. And if you consider from the infrared to the far infrared for the men and friends and farm Fred has sort of wealth of diagnostic
09:42:07 so we sort of went through those a little quickly, and it's very powerful because it sort of gives you the causes and effects for all the sort of processes that we've been talking about so we're able to measure not only the driving mechanisms and the
09:42:09 energy input but the effects that that energy input has on the ISS, and the CGM and that sort of interface between galaxies and the and their local CGM so there's heating, cooling diagnostics of the atomic gas.
09:42:21 You can measure outflows mass outflow rates, both and admission and absorption.
09:42:26 You can get direct traces of the dust and that's the small grains and the large grains. And those small grains those peaches are very, very fragile markers and that's very important of the interface between the photo nice region and the molecular clouds,
09:42:43 and you have access to all these lines of warm liquid or gas as well. So not only the sort of huge range of ionization of the atomic gas but this warm molecular gas which is exactly where the impact of the feedback is happening on the star forming gas
09:42:57 so if you want to talk about finding the sources of the energy input and you want to talk about the effects of the energy input on the star from it yes and quenching and what it's doing to that gas the infrared is the perfect place to look.
09:43:11 So we sort of went through all those diagnostics and we.
09:43:15 It gives you the energetics and it gives you the dynamics as well until we spent a little time at the end talking about sort of the exciting sort of future.
09:43:22 So there's a lot of effort going on to expand. If you use on large telescopes on the ground, there's there's work to get new generation of ao assisted by a fuse on Kak like lagger.
09:43:37 And then there's mere mouse, which is what Glenn was telling us about him and gentlemen, which is a much larger and non ao fed. If you in the infrared to study the sort of CGM on a much much larger scales hundred times when you can get with those hires.
09:43:52 And of course next year we're getting JWSD, so we're going to have near infrared and mid infrared if you choose to study the outflows and feedback and local galaxies and a high ratio.
09:44:09 that on Wednesday think as well. Wonderful, thank you so much, and it's incredibly exciting. Okay, so next hand Nic reid is Chad, who starred.
09:44:20 Yeah, well we had a nice conversation and the gamma ray room, and, you know, gamma rays as we discussed traces of cosmic rays so there you know if you're interested in cosmic rays for all the various applications they might have for the CGM You should
09:44:33 also be interested in gamma ray detections or non detections.
09:44:38 So one of the things we talked about was how we do have information from Fermi lat, which is still generating lots of data but what we get is gamma ray luminosity is for a number of galaxies one is, you know, we have information for high mass galaxy showing
09:44:57 showing us that cosmic rays are basically, you know, the calorie metric all the cosmic energy is lost to collisions and those collisions generate gamma is.
09:45:07 But there's more scatter at the low mass and for dwarf galaxies and we're hoping that we get more data points from for me or from next generation telescopes in the future, which would be very useful because that gives us a constraint on cosmic ray propagation
09:45:22 models and cosmic ray driven wind models.
09:45:26 So we're looking forward to that in the future.
09:45:29 We also talked about more specific to the CGM there's been some claims of a detection for gamma ray emission from Andromeda.
09:45:39 This claim is a bit disputed and Susumu pointed us to a newer paper that states, a strong detection but only out to about a degree which is about 15 killer parsecs so we still don't have an unambiguous detection of gamma rays and the CGM, especially the
09:45:55 outer CGM of any galaxies.
09:45:57 And that would also be a wonderful constraint in the future.
09:46:02 We talked a bit about how there are other sources of cosmic rays out in the outer CGM one of which might be a termination shock which is also not been detected in any galaxies but might be detectable, not in gamma rays but maybe a next generation.
09:46:18 radio interferometer is like SK.
09:46:22 We talked a bit about how we would like to separate the CGM from the desk in terms of gamma rays but that's also very difficult.
09:46:29 And so I think we're looking forward to future gamma ray observations from things like CTA and SK, which will hopefully give us more information.
09:46:41 Awesome, thank you so much Chad had super cool to detect the termination shock and the CGM and gamma rays that would be incredible. Alright so, Jane Charlton has her hand up next.
09:46:56 Yeah. Okay, um, we talked about the interplay between having more targets.
09:47:05 More wavelength coverage, more higher resolution and higher signal to noise.
09:47:11 In terms of advancing knowledge from absorption one studies.
09:47:17 And in terms of having more targets, it's not just more targets of course but more targets behind in front or behind different kinds of objects.
09:47:31 And so with more targets and better statistics, we can measure covering fractions column densities of various elements and kinematics as the function of galaxy type star formation rate environment impact parameter and orientation, and really nail down
09:47:50 those properties statistically, the possibility of using foreground background galaxy pears and lensing as we just heard about would enhance the ability to understand things better.
09:48:06 In that way, then we also talked about. The other issue you know what can we pull from an individual spectrum, can we improve that we talked about how high a resolution would still benefit us and kind of came up with somewhere between 100,000 which probably
09:48:23 will be happening and 200,000 which we don't really see in the future would be useful and we had her said, Oh, you know anything in the next decade in the way of advances is going to be ground based rather than space based.
09:48:39 And then we talked about what can come from a single line of sight, measuring density temperature medalists at pressure and size.
09:48:51 Assuming clouds, along a given sight line, and how with higher resolution, we can compare the velocities in different ionization states, and we can really nail these properties recognizing that a statistical thing will average out a lot, because we know
09:49:10 there are different metals cities along the same slight line, and different processes contributing.
09:49:16 And so, you know, kind of a balance of the more detailed analysis, as well as the better statistics is kind of where our group felt that the progress will be made, anything to add to that Roman.
09:49:37 I think he's giving you the thumbs up so thank you, thank you so much Jane. Alright so next up we've got shall win.
09:49:42 Okay.
09:49:43 We are from the admission group, and we have a relatively large group with 13 to 14 members should I say their names include, I'll just read it quickly.
09:49:55 I think we can I think we can see them on the, on the list so don't waste your time with the names just head.
09:50:15 Okay, so I think we all agree that this is a very exciting time to be able to see diffuse so complicated gas emission.
09:50:11 That has been demonstrated by the reason why do integral few observations. And in terms of key observable is the general thinking is we are able right now to do this right now to measure the size of the line meeting structure and also a straightforward
09:50:29 measurement will be surface brightness profiles and a couple of with velocity measurement based on life enjoy on. So, we should be able in the region near future to determine the middle of city map, combining multiple line detections based on line ratios.
09:50:47 And we also realize, you know, recognize that there. There's a dichotomy between a little richer than high ratio of studies in high ratio of universe.
09:50:58 Nearly all observations are based on resonant line transitions and that has non negligible degeneracy between the underlying gas structure and those are the radiative transfer detail ready to transfer physics and low ratio, we can detect Nebula line missions
09:51:14 data. The interpretation or more straightforward we can determine on a station structure, density and also in the whole city, more robustly looking further into the future, the, the, the, the wish list is to be able to use the CGM as the accelerometer
09:51:34 to really look into the energy feedback, and the injection scale on different at different distances and also to measure cooling rate from these dense dense clouds, ideally we would like to see the 3d structure in terms of the geometry of the Cold.
09:51:56 Cold face. And those are the feeling factor of dense clumps. We also have one theorists in the group that help bridge the gap between observation and simulations to really provide the validation and verification of the structure we, the 3d structure of
09:52:13 CO streams and how that set feeding to the galaxy in the center of the Halo. So I think that I should also mention that there are quite a few. Okay, speed up, I just want to mention that there are many new instrument concept that you addition to near
09:52:30 mouth we hear about We also heard about full boss from toolbar shit, that's been planned for tech.
09:52:37 Thank you so much, that was, that was great.
09:52:40 Yeah, you guys had I think by far the most popular room, if that says anything about the future of CGM observations.
09:52:49 Okay, so next up, Greg. Right.
09:52:55 Right. Yes.
09:52:56 So, so we were in the Sundance elbow which effects room. And we had a small but excellent group.
09:53:06 And I'm particular we had Nick, Taylor who's was able to answer all of our questions.
09:53:12 So, FC, of course, has the promise of percent level density and pressure profiles for halos have potentially down to tend to the 12 solar masses out to several times already, so we did we thought that was really important.
09:53:34 And there are there are constraints, out there now and more coming soon with things like Simon's Observatory, CBS for see cat prime.
09:53:46 These instruments will improve the resolution, and also provide more frequency coverage for proof separation.
09:53:57 And, as well as sensitivity.
09:53:59 So, some of the interesting questions that could be tackled. For example, the revolved around, particularly the sensitivity of density and pressure.
09:54:09 large radius in the sec measurements.
09:54:13 So, so it's particularly good at measuring for example the AGN feedback thermo see in particular is like a calorie remember this point was made before but really, because of the long cooling time of the podcast at large radius.
09:54:35 It bears a memory of all of the energy and put into the heart,
09:54:35 and could be combined with other pressure sensitive probes like a mission or absorption.
09:54:43 To get a better probe of the can to help us. The SEC pressure measurements then to constrain
09:54:53 to help feed into things like emission and absorption probes.
09:54:59 Nothing we talked about was the fact that the Kinect Cassie effect is sensitive to velocities and so your potential to measure the rotation of halos their, their motion in a variety of ways.
09:55:13 And maybe talk to a little bit about combining that with.
09:55:17 If you measurements of the galaxy to see the the connection between the rotation of the Halo, and the galaxy.
09:55:25 Of course one of the issues with this is that these measurements are that particular for the low mass halos. They come from stacking many galaxies. And so one of the things that's required as is, is good surveys, which go down to low mass of galaxies
09:55:41 which cover large, which which have many galaxies per degree per minute.
09:55:50 So So highlighted the need for improved survey.
09:55:55 And then there was also some discussion about instruments which could focus, which had smaller higher resolution but smaller, smaller area, and so would maybe be good for combining with the larger survey.
09:56:10 Thank you Greg that's good, that's your time.
09:56:13 All right.
09:56:14 But this is great, I'm noticing a theme and that like combining multiple you know observational domains will obviously lead to the best constraints, and that's wonderful.
09:56:27 All right, then you are up next. Okay, thank you, Jess Yes, the X ray group I think had the most people 18 people. And maybe that's because of half of all baryons are at least 10 the pipe Calvin we've known that for you know since like Chen and debate
09:56:44 20 years ago, integrating over gas and halos, whether it be CGM ICM anything in between. Most periods are above 10 of the five cup and probably above 10 to six Calvin the average temperature of Baron in the local universe is 10 to the six Calvin.
09:56:59 So our group is, you know, comprises both emission and absorption of this massive reservoir of baryons, and those complimentary complement each other.
09:57:09 One inner Halo one outer Halo more so we we had Randall Smith and a lot of extra absorption people, and we were talking about throughput versus spectral resolution of extra gruesome spectrometers about Hitomi extremism.
09:57:43 in the future future missions will be able to resolve the vo 100 kilometers per second, archives specifically will prob 30 lines of sight to get about 100 or seven detections and other a lot of other metals as well. So, we wanted to know how would you
09:57:46 be CGM style like cost halos like plot of column density as a function of radius, for, for galaxies, look in the X ray and we need to make this plot for future missions.
09:57:56 X ray mission detections are, you know, detectors are always if us, and we need to talk about the different types of detectors out there because you know CCD type detectors like a CSI on Chandra
09:58:13 epic on XM give you I think on our 50 to 100 EV resolution for energies of point 322 KV. Somebody can correct me on that. However, in the future, ultra micro color color images on links and others can go down 2.3 EV if you think about like 500 600 EV
09:58:37 where a lot of these lines arise from. So can you detect Elster he lives in a mission. Well, thanks could, but probably out 2.5 rb or in long integrations of 10 to 12 solar mass halos you know further out and more massive objects, near term missions,
09:58:50 can pipe probe out to several 10s of killer parsecs Ege Rosita etc.
09:58:55 and something we want to, you know, emphasize is x rays give you thermodynamics medalist, temperature, maybe density, which is a great compliment cherry probe to Mr B's and se, which give you density and pressure, and from this together you can derive
09:59:12 hot gas cooling rates, nothing that's it.
09:59:17 Sorry I just invented a new sound effects. When you're done, I'm going to be like
09:59:24 Dropbox.
09:59:26 Thank you so much Ben Yeah, I forgot actually the X ray room was the most popular room which then hopefully pointed out might be reflected of reflective of the berry on distribution and the CGM knows.
09:59:38 All right, last but not least, Cameron's going to close us out with a summary of the FRV room. Excellent. Yeah, so I'm fast radio bursts.
09:59:47 We had a smallest group but very, very active discussion. And much like the last couple of probes that were mentioned this and yet still dovish effect and x rays were primarily probing the hotter components of the CGM and the AGM as well, so fast radio
10:00:04 bursts right now are the instruments that are online are able to detect a few per day, and have some localization of those on the sky but generally just being able to detect them and to get the various observational components, but not necessarily localize
10:00:21 them super well, whereas in the next 10 years, there's a number of different instruments that are coming online that will be nominally detecting on the order of 50 to 100 of these per day and then also localizing them to arc second or milli second in
10:00:36 some case locations on the sky, which provides you essentially the same kind of precision that you get from from absorption line studies of quasars in the movie and optical, so.
10:00:47 But to answer the primary question for this group, what kind of constraints does it put on the quantities that we care about in the circle galactic medium that the two, the two major things that you get when you detect a fast radio first from a distant
10:01:01 object or the dispersion measure and the rotation measure of the, of the, of the radio waves along that line of sight path.
10:01:10 The dispersion measure for for people who are more comfortable with things from UV and optical absorption mind studies is effectively the column density of free electrons along that path.
10:01:24 It's not broken up like it isn't a spectrum, but it's just the aggregate free electron column density, but that tells you something really important about the hot nominally the hot component of the gas, because it can help reveal things like the missing
10:01:35 baryons that primarily may be in this in this in this free electronic content, and provides a lot of complementarity to absorption line studies which are primarily looking at, at low ions and intermediate ion so so cooler gas, And in addition to that.
10:01:52 The other thing is the rotation measure, which is like, sorry I'll go faster, the rotation measure, which is effectively the magnetic field waited column density of free electrons.
10:02:03 So, that gives you something that very few of the other observational techniques give you in terms of of what's the magnetic field strength along that line of sight, especially if it intervenes with a with a galactic Halo along that line of sight.
10:02:18 And there are additional things like scattering that may be able to provide information about the clustering of the CGM but but I'd say dispersion measure and rotation measure the main things that we get so that gives you free electron content and magnetic
10:02:33 field strength.
10:02:36 I didn't hear the fog horn that's because you were blathering.
10:02:47 All right, everybody. Thank you so much. It's 10am.
10:02:47 Pacific time at least wherever you are, it's too after the hour, it's time to wrap up what was I think an incredibly exciting discussion. Thank you so much everybody for participating.
10:02:58 I know that throughout the entire week we're going to be able to incorporate elements of this and the various discussions that are happening, we'll revisit.
10:03:08 All of these observational domains and the physical parameters we're trying to constrain on Friday. But in the meantime, can't wait to see you tomorrow for Chris Martin's talk, and the panel discussion to follow.