 is one of the best missions, and that seems like a good thing. But I think we can all agree that really, test has been secretly on a stellar activity, a stellar variability mission. And so I'm going to highlight some of the interesting astrophysics. And by highlight astrophysics, what I really mean is I'm going to play show and tell. Because the thing that's got me excited about test is that roughly every month, far faster than I can keep up with, a dump of 20,000 short cadence like hers shows up on my computer that I downloaded, and then I scratch my head and ponder how I'm going to look through them all. And really, I think test is arguably as impactful for stars as it is for exoplanets. So to show this great publication rate, which I just anticipate will continue to go up, like keep publishing. This is an amazing mission. And arguably, I mean, there's some other astrophysics, but really, come on, really, we're talking about stars. Like, there was a great website. I want to give a shout out in recognition of this great website that went up after sector 0, sector 1, excuse me, which was called Test Roulette. I think the URL was test.casino. I think, unfortunately, that website is down. So I don't know if Ben is able to buy the domain again or whatever. But this was a great website. And so this website, you could hit me. And it was like playing a slot machine in Vegas. And it would just bring up a new light curve. And then they added more buttons that, like, if you got a jackpot, I think it would tweet about it. And then there was one that it would, like, pretend to submit a paper to the archive if I found a planet. It was a great website. And it became a really useful, simple tool for people to just click through and explore light curves and really appreciate how dynamic and how interesting these light curves are. So I've been doing a similar thing occasionally on Tuesday. So I'm going to pretend it's Tuesday today. I've been doing a similar thing where I've just been doing, like, Twitter threads about, like, cool light curves. So every month or two, I'm like, let's just go click through a lot of light curves and just play show and tell about the things that get me excited. And that's what I want to do today. So this is how, this is my workflow, is I use the little icon view on my Mac. And I just look through thousands of light curves. It's a very efficient system, actually. It's a computer vision algorithm, whereby I look for things like this. And there's a lot of cool stuff in here. You could spend the whole talk, if this was an incredibly high-resolution projector, we could spend the whole talk just looking at this. There's so many cool, wiggly things here that should excite everyone in this audience, even the handful of planetary astronomers. So let's play a little show and tell. First thing that popped out to me, and I highlighted it here, sector one, this is, again, in the first days of the test primary mission. Abruptive variables, CVs, category variables, dwarf, no-bay, things that go bang, out of nowhere. This thing increased by, this is relative flux here, so 20, 22 times relative flux. I forget this has some, like, this is some name brand CV, which Paul Scoti's gonna be very disappointed that I don't remember the name of. But these are all known, dwarf, no-bay or outbursting CVs. These are incredible. And the likers, like we have from Kaplan and K2, are incredibly dynamic. There's amazing pulsations in variability and distinct changes as it goes through. These are different systems, I should say. The variability changes as they evolve. These are really, really neat events. There is an unbelievable number of what appeared to be rotating stars, star spots, fellow rotation. Sorry, there's all the kinds of colorful lines that's in my, these are literally just ripped out of my simple little pipeline of fitting loam-scarble periods to things. There's so many little periodic variables in this data set. Already, test has observed as many stars as Kepler has and we have a comparable number of rotating variables in the data set. So here's just a truly random subset of rotating variables. So for those who don't, instead of each kind of diagrams all the time, this is a dark spot, like a sun spot, on the surface of the star and as the star rotates, the spot rolls into the front of the star, makes it dimmer and then it's brighter as it rolls off and you get these quasi sinusoidal modulations. We can measure fundamental stellar properties, including rotation period and age perhaps with these. This is a really fascinating measure. Here actually, there's two, if you look really carefully, there's two periods in here. This was an amazing result from the Kepler mission that we've been working on in the K2 data where you can see the distribution, this is Gaia color and this is rotation period. It stars this angular momentum move upward in this diagram and so this is our sort of our age metric as they move upwards and lose angular momentum. We can see interesting structures in here in Kepler and K2. There's hints of structure here at the rapid rotating end. Now these slower rotators are gonna be a big challenge because Tesla only observes these stars for notionally 27 days or so. That's not really hard. The sun rotates at 25 days. That becomes really difficult to measure. But there's some hope. There's pulsators. I only found one in the one folder of images that I was looking at but there's a ton of pulsating light here so this is probably some kind of RL library or something. This is an amazing variable. There's gonna be a whole bunch of interesting long-term blotch to RL library that we're gonna see that are gonna be really fun. And there are so, so many eclipsing binaries and I know this is particularly the bane of the other half of the test mission was people who wanna study the planets because these things tend to show up of looking like really big planets. But they're amazing and there's so much fundamental classical astrophysics we can do with the pulsing binaries. Now you see that there's often the data gap here in the middle of the test data. There are always data gap here in the middle of the sector and you get these funny cases where you get very strange looking light curves like this looks like a Batman logo or something that's missing the primary transit. So a little bit of care has to be taken when you're trying to discover pulsing binaries here. But I mean I look at this and I just freak out because it's an amazing variety of possibilities. Like this little feature here is little bump between this extremely eccentric pulsing binary. This is some like a heartbeat start kind of activity where it's tidily exciting it. Here's one that probably would get a mistake in off hand for a transient planet. Look how long this eclipses. This eclipses like three days long. This is amazing and it's a flat bottom eclipse. This is a really cool system. I think there's a possibility here with tests, perfect, given the nearly all sky coverage to have the first like complete census of eclipsing binaries out to 20, 30 days over the whole sky. I think that's a huge opportunity. And there's opportunities really cool. Talk to Jessica Burkey here for me, Doug, about cool methods to classify these things with fancy statistics and machine learning techniques. Here's one that I found the other day that looks like it's a heartbeat start. I remember when Bill Wells showed one of the first of these at the Kepler, from the Kepler science meetings, he said, ah, I must have my magnitudes wrong. This must be an eclipse and it's not. It's an eclipsing binary, but it's the high of execution every time the two stars get close to each other. These are amazing systems. And we have these zones of continuous feeling or nearly continuous feeling where we have the opportunity to look for very long period systems. And I think this is where we'll even surpass or eclipse if you will, the Kepler mission in terms of looking for very long period variables. So there's great opportunities here for long term studies of variable. And it really goes on and on and on. Massive stars, evolved stars, O and D stars, they all vary. Flare stars, of course, they go pop all the time. There's a huge number of flare stars and young stars in the test data that I'm excited to talk to you about at Nauseam. Here's a good example of what tests Kepler 1. The same star observed in Kepler and then we observed it again in TESS, obviously not continuously. We can do statistics and the statistics line up. And the society, right? There's fun overlap things we can do with this data set. Blah, blah, blah. We can talk about this, okay? The conclusion is, TESS really is one of the most powerful astrophysics missions. Like its precursor, like its predecessor, just Kepler and K2. TESS is going to change what we know about the nearby and bright stars in our galaxy. And I think it's going to unlock or solve puzzles or whatever the symbol I'm trying to elicit here is. It's going to solve a lot of mysteries. And of course, that means whenever we're probing a new frame of space, it's going to open up all my ones. Thank you. Two seconds to spare, so I get one question and then I can scratch my head. Hi, you mentioned before that there is a citizen science project looking for planets. Is any of this information incorporated into the citizen science project and how can citizen scientists discover variable stars, pulsars, pulsating stars? I'm going to ask Andrea to answer this. I don't know. That's a great question. I believe that they do have categories that they classify other variables. I'm not sure exactly which categories they are. Is there anyone here who can collect hunters? Well, I will note that in the one mission, Voyage of the Star was discovered by amateur astronomers. So I wonder how many truly fascinating things TESS will discover, not by most people in this room. Jim, again?