- Vanessa Bailey, she'll give us a Roman Update.

- Thank you very much, it's my audio coming in, okay?

- Yes, okay, you sure yes, we see that.

- Do you see the main slide or do I need to swap my displays?

- Yeah, I think you need to do that.

- Okay, how's this?

- Yeah, better.

- Okay, perfect.

- Thank you.

- Yeah, so thanks very much to the ExoPAG for inviting me to give this Roman Coronagraph Instrument Update today. It's been a while since you've heard from us on the Coronagraph, so there are some exciting new developments to report on. And of course I'm not just here showing my own work, but rather the work of large and talented and dedicated project teams and science teams that have been working on this project for last five years in the case of the science investigation teams and wanted to say a big thank you to both the Macintosh and the Turnbull Science Investigation Teams whose contracts have just recently been wrapping up, for all of their hard work and excellent contributions to the instrument over these past five and a half six years. And I'll talk a little bit at the end about ways that we're looking for science teams 2.0 and what that call will look like. So I'll spend a little bit of time giving me an introduction to the Coronagraph Instrument for folks who haven't thought about it in a while, present our timeline and our status, and then resources for the community for folks who want to learn more about the Coronagraph Instrument and talk very briefly about what the bit I can say, about the Roses 2022 call for the science teams 2.0 essentially. So we've been using these future flagship missions that the aim to image exo-Earths as a hypothetical motivation for the Coronagraph Instrument for some time, but now it's real, we were all absolutely thrilled at the Astro 2020 recommendations for this future flagship mission that that aims to not only image, but characterize an Earth-like planet. But there's a very large technological gap, indirect imaging between that goal and where we are today. So if you see here, oh, sorry, I think it may have swapped again, okay, hopefully that worked. If you see here, we have our usual direct imaging plot where we show projected separation on the sky and arc seconds and flux ratio with respect to the host star on the y-axis, the kinds of planets that we can directly image today in the infrared are these bright hot self luminous super Jupiters at the 10 to the minus five, 10 to the minus six contrasts, we're aiming at these feature flagships to get down to 10 to the minus 10 contrast in the visible and the Coronagraph Instrument is going to help us to bridge that gap. We have one reasonably loose requirement for giving the green light to launch, but our instrument design we believe is going to be much more capable than that minimum requirement, with three primary observing modes maybe just starting to skim the surface of the reflected light Jupiter distribution, the true Jupiter analogs for the first time. And you can get the data underlying this plot, as well as an exposure time calculator for your favorite point source target at the URLs and I'm showing here on the right. And with that performance, again, the EOS one panel in particular, it did endorse us to continue as a technology demonstrator for these future missions. So technologies that we're demonstrating, are a wafer and sensing and control, very precise way for in sensing and control for the first time in the space with the high actuator count deformable mirrors. So we're both sensing and doing precision correction to compensate for any residual scattered star light that makes it through our system. Even though we have these very advanced Coronagraph Masks that suppress the best majority of the starlight on their own, there are still some residuals that we need to correct for. Being able to do this Coronagraph Mask development on the rather challenging aperture that the Roman Telescope has shown us that it is possible to achieve high contrast on obscured apertures, but bearing out that it's not preferable and reinforcing why it's useful and what to choose an off-axis telescope design for one of these future missions. We're also for the first time in space proving out electronic multiplying CCDs for science observations. So we'll be looking at objects that are so faint that we'll be receiving individual photons from those planets on the seconds to maybe minutes timescales, so we really need to be able to capture and collect every single one of those photons and an EMCCDs can amplify the individual photons signals above the reed noise. And then modifying our post-processing algorithms to deal with that photon counted data as well. So we have still several observing modes within the instrument. Our one required mode, that's our bare minimum to get the green light to fly, is our narrow field of view imaging mode, the shortest wavelength, but we still have several additional modes on a best effort basis. We're focusing our efforts in particular on this 730 and 825 low resolution spectroscopy and "Wide field of view imaging it's 1.4 arc seconds radius field of view." Both of our imaging modes can be used in polarimetry mode as well. And then the main difference between the required mode and these best effort modes has to do with the level of ground testing. So we will have end to end performance testing certainly on the band one mode, but probably component testing and assembly level testing on these additional modes, but not the end to end performance testing due to our schedule and budget constraints. We're also going to have a lot of mass hardware that is officially not supported but will be flown, and if additional resources become available sometime down the line could be used. I like to think of these a little bit like, this disbar five Coronagraph and that it wasn't initially supported as an observing mode, but enthusiastic community members came along and commissioned it later when more resources were available. If you wanna see more about these contributed modes, the hardware for which was contributed by the Exoplanet Exploration Program, you can see this paper here by AJ Riggs. And when all of this comes together, although we're technically a tech demo, we might as well look at the most scientifically interesting targets that we can, while we're proving out all of these technologies, the best way to prove the way for future exoplanetary system imaging missions is to image exoplanetary systems. So we can image these self luminous young super Jupiters at shorter wavelengths. We can potentially, take the very first reflected light images of a true Jupiter analog cold old mature of orbiting a sun-like star at a Jupiter like orbital separation, and broadly distinguished between cloudy versus clear atmospheres based on albedos and colors. We can have access to these low surface brightness discs with better and less ambiguous morphology measurements than we can get from the ground, because the ground often relies on angular differential imaging, which causes some high-pass artifacts or relies only on polar metric differential imaging which then is only sensitive of course to the polarized fraction of the light that's emitted. And lastly, we might also be able to break some new ground in terms of taking the first image and visible light of an exozodi system. And this is rather important because these future missions are going to need to know what the dust populations look like in the habitable zones to be assured that they will be able to see that Earth orbiting this nearby sun-like star, and that it won't be enshrouded in too much dust. So there have been infrared observations, other NASA funded observatories, but the extrapolation to visible is at this point model dependent and NCGI could potentially provide some very useful information. So some updates on our timeline, since the last time we spoke at ExoPAG, we've passed our critical design review as of April, 2021. And we're now planning instrument delivery to payload integration and test at the end of 2023. This is a few months delayed, due to understandable COVID impacts, and as well our launch for Roman as a mission has been delayed by to late 2026 as our goal, we have an agency commitment of no later than May, 2027, but we're planning to late 2026 at this point, like with JW, there will be a commissioning phase, immediately following launch, and we'll do we have about 450 hours of initial instrument checkout during that commissioning phase, but the real fun is going to begin about 90 days after launch with the start of the technology demonstration phase for the Coronagraph, where notionally we have about 2200 hours of observing time spread over the next year and a half of that mission. So about three months of time, for dedicated Coronagraph observations means that we really have an opportunity to conduct a number of exciting observations of interesting systems while proving out the technology. And if we're performing sufficiently well, that the community and NASA think that that were compelling, Roman is not gonna turn off that launch plus 21 months. And so the majority of the remainder of the next five years will be spent on community surveys and geo and GI programs with the wide field instrument, the other instrument on the Roman Space Telescope. But there's a small amount of time that we think having your mind order of magnitude 10% maybe might be accessible to the Coronagraph, if the community thinks it's compelling and if there are additional resources, but really this part of the mission is not guaranteed is not currently funded, but it is a question we often get what could the Coronagraph do during the remainder of the mission? I wanted to address that, there we go. And so I mentioned that we're well into build integration and test, and so we have a lot of flight hardware on hand, I'm showing just a few different components here. A couple of the things that I wanted to highlight, are electrical deploying CCDs, so we have three of those chips in hand now from Teledyne and they're undergoing performance testing at JPL. Preliminary indications are that they're looking good and we'll know more soon. We have completed the fabrication of their housing, and that has an important function of shielding the detector from radiation damage. And when you're trying to count individual photons as they come in, that radiation damage causes charge traps, which can eat the photons before they're ever sent to the readout, and so we want to minimize that radiation damage. And so we have a housing thankfully, that we were able to preserve material from our original five-year lifetime design before we became a tech demo. So we don't think that 21 months in a day, radiation is going to kill their detector. So I'm pleased that the housing has been coming along well. We also have various flight electronics boards that have been coming in, are spectroscopy and polarimetry prisons being fabricated, doing final acceptance testing now. One of the major technical milestones that you might remember from last ExoPAG presentation was the maturation for flight of the deformable mirrors. They had a long lab heritage by not flight heritage, and so the electronics interconnect problems have been solved and they've all it's reached TRL six a bit more than a year ago, and in fact, we have good flight candidates in the lab right now being assembled.

- Vanessa you have two minutes.

- Thanks, and the Coronagraph Masks, we have all of the mass fabricated for the hybrid Leo, that one required mode for the best effort modes the shape pupil mode that's partially complete. So each one of these modes has multiple different people playing and focal plane masks. Some of those are complete, but you have to have all of them for the mode to work. All four of the shape pupil masks themselves, are printed on a single substrate both those baseline and the contributed ones, which makes manufacturing with 100% yield a bit more difficult. So those are being fabricated right now, the need by date is in February. So it's gonna be down to the wire, but we think we have a plan, for completing fabrication of those, and have a high probability of getting, one good flight candidate in these next fab runs over the next month. But we'll be able to say more in February and March about those and progress on those as well. And so lastly, I wanted to briefly speak about the community participation program. So I mentioned to you at the beginning that the round one science teams, their contracts have recently run out, and we are going to be competing for a community participation program. So we don't have a geo or GI program, with the Coronagraph Instrument, but rather the way that the community interacts with the observatory is really to become integrated with the project team through this community participation program. So this'll be coming out in Roses 2022, we'll be looking for topical areas like target selection, image simulations, data analysis, potentially wave functions and control alternative research, I don't have a definitive list now, that's gonna come out in the Roses 2022 call along with guidelines for timing and funding. But just wanted to make you aware that this is coming and hopefully towards the beginning of the 2022 Roses period. And lastly, basically here the main takeaway point is if you want to learn more about the Coronagraph Instrument, we have a number of different resources prepared by both the project and by the science investigation teams, and you can find out things project prepared on this Roman IPAC site, and as well the science investigation teams each have prepared their own extensive sites with their resources. And they'll soon be a one-stop-shop page on the Roman IPAC site. And so in summary, the Coronagraph Instrument exists as a tech demo for these future missions that want to image exoplanets and the best way to prove out these technologies, is to image planets and discs around your by stars. In my opinion, in our opinion, we are well into build and test with delivery less than two years from now, to payload, integration and test, and the community can find a lot more information on the Roman IPAC website, and thanks for much.

- Hey, thank you very much. Let's provide a virtual round of applause to our speaker. And currently there are no questions on the, oh, there's one. Where does imaging young stars protoplanetary disc, is this things from older stars the breeze disk fit in the CGI plans of your outline?

- Yeah, so what I showed in that, let's see. So I focused primarily in this slide on debris discs and that's because we are more limited to bright targets for performance reasons are nominal host star V magnitude limit is officially a V mega five, internally for planning purposes, we're bookkeeping down to VF6, VF7, I feel fairly confident we're gonna be able to exceed our host star magnitude requirement that has to do with our ability to keep a very fast tip tilt loop locked, having a photons for that that kilohertz tip tilt loop to correct for telescope jitter and keep it very high contrast. So in the initial stages of the tech demo, I imagine we're going to be focusing on the brighter stars, V brighter than seven. If we end up knocking out all of those initial tests and requirements very quickly, I think trying out our performance on fainter stars is something that's absolutely very interesting. In particular, we do have a narrow band engineering filter that we use for wavelength calibration but have also placed it at H-alpha. So that could be one of these potential additional modes that we don't say at this point we're officially supporting, but if we end up with some extra time in that tech demo phase, I would be very interested in trying to commission those.

- Okay, I think we can move on, I don't see any new other questions. Let's thank our speaker again and move on to the next one.