1 00:00:01,020 --> 00:00:03,130 - [Tiffany] Yeah, sounds great, okay. 2 00:00:03,130 --> 00:00:04,470 - [Emily] So hi, everybody. 3 00:00:04,470 --> 00:00:05,630 My name is Emily Martin. 4 00:00:05,630 --> 00:00:08,320 And as Tiffany said, I'm a postdoc at UC Santa Cruz. 5 00:00:08,320 --> 00:00:10,230 And I spend most of my time 6 00:00:10,230 --> 00:00:12,570 thinking about building instruments. 7 00:00:12,570 --> 00:00:15,230 I also do some science looking at the atmospheres 8 00:00:15,230 --> 00:00:16,510 of cold brown dwarfs. 9 00:00:16,510 --> 00:00:19,430 And today I'll be talking to you about my new instrument 10 00:00:19,430 --> 00:00:21,080 called PEAS with the planet as 11 00:00:21,080 --> 00:00:23,620 exoplanet analog spectrograph. 12 00:00:23,620 --> 00:00:27,990 And before I get started, I'd like to acknowledge my 13 00:00:27,990 --> 00:00:30,510 collaborators, mostly here at UCSC. 14 00:00:30,510 --> 00:00:33,610 As well as acknowledge the support that we've received from 15 00:00:33,610 --> 00:00:35,890 the NSF from housing assignments, 16 00:00:35,890 --> 00:00:38,700 as well as from the observatories. 17 00:00:38,700 --> 00:00:39,573 Okay, next slide. 18 00:00:43,410 --> 00:00:47,810 So, we want to observe atmospheric dynamics, otherwise known 19 00:00:47,810 --> 00:00:49,950 as weather on exoplanets. 20 00:00:49,950 --> 00:00:53,690 We know from observations of objects in our Solar System, 21 00:00:53,690 --> 00:00:56,060 just how important atmospheric dynamics can be, 22 00:00:56,060 --> 00:00:57,600 as we've heard earlier today, 23 00:00:57,600 --> 00:01:02,240 regarding Venus and Io, as well as major storms that we know 24 00:01:02,240 --> 00:01:06,470 appear on the gas giants and ice giants in our Solar System 25 00:01:06,470 --> 00:01:11,470 that those storms and other kinds of dynamics can produce 26 00:01:13,040 --> 00:01:16,840 large time varying signatures in the kinds of observations 27 00:01:16,840 --> 00:01:17,673 that we can take. 28 00:01:17,673 --> 00:01:19,800 And so we know that this is going to affect the kinds of 29 00:01:19,800 --> 00:01:22,000 observations that we can take of exoplanets. 30 00:01:23,640 --> 00:01:27,170 And we have done have been many different theoretical 31 00:01:27,170 --> 00:01:31,460 studies to look at how various kinds of weather can appear 32 00:01:31,460 --> 00:01:33,620 in exoplanet atmospheres. 33 00:01:33,620 --> 00:01:36,210 For example, on the left, I'm showing a figure from 34 00:01:36,210 --> 00:01:41,210 Zhang and Showman 2014, in which, just by varying a small 35 00:01:41,280 --> 00:01:44,660 amount of the way that the heat coupled with the atmosphere, 36 00:01:44,660 --> 00:01:49,500 they were able to produce very different looking atmospheric 37 00:01:49,500 --> 00:01:52,340 dynamical properties, whether you've got a series of spots 38 00:01:52,340 --> 00:01:55,130 or whether you can end up with zonal bands, 39 00:01:55,130 --> 00:01:57,260 the structure is very different. 40 00:01:57,260 --> 00:01:59,760 We also have done atmospheric studies 41 00:01:59,760 --> 00:02:01,810 of hot Jupiter for example, 42 00:02:01,810 --> 00:02:05,743 and by observing different times of the phase curve. 43 00:02:07,060 --> 00:02:11,190 The authors for example, in Stevenson 2014, we're looking at 44 00:02:11,190 --> 00:02:16,030 WASP-43b, which is a hot Jupiter, and they were able to show 45 00:02:16,030 --> 00:02:20,270 extremely differing thermal structure depending on whether 46 00:02:20,270 --> 00:02:21,790 or not they were looking at the night side 47 00:02:21,790 --> 00:02:23,623 or the day side of the exoplanet. 48 00:02:25,420 --> 00:02:26,563 Okay, next slide. 49 00:02:28,230 --> 00:02:30,430 So we know that our own Solar System planets have weather 50 00:02:30,430 --> 00:02:33,260 we know that exoplanets are probably definitely 51 00:02:33,260 --> 00:02:34,730 going to have weather. 52 00:02:34,730 --> 00:02:38,100 However, the problem is that putting the context in which we 53 00:02:38,100 --> 00:02:42,390 understand our Solar System into a much more similar format 54 00:02:42,390 --> 00:02:45,600 to what we will observe with exoplanets is quite difficult. 55 00:02:45,600 --> 00:02:49,340 And that is illustrated largely here by what is basically 56 00:02:49,340 --> 00:02:50,730 an optics problem. 57 00:02:50,730 --> 00:02:53,370 So all of the planets in our Solar System 58 00:02:53,370 --> 00:02:55,370 are spatially resolved. 59 00:02:55,370 --> 00:02:58,570 Jupiter obviously is one of the largest ones 60 00:02:58,570 --> 00:03:02,500 in terms of spatial extent on the sky takes up about 61 00:03:02,500 --> 00:03:03,753 40 arc seconds. 62 00:03:04,660 --> 00:03:09,550 Whereas the closest by and easily observable directly image 63 00:03:09,550 --> 00:03:13,350 exoplanets, the entire systems as a whole take up of the 64 00:03:13,350 --> 00:03:15,100 order of arc seconds. 65 00:03:15,100 --> 00:03:18,770 And so whenever we take observations of exoplanets, 66 00:03:18,770 --> 00:03:20,440 we're looking at a single point of light 67 00:03:20,440 --> 00:03:22,570 that has been disk-integrated. 68 00:03:22,570 --> 00:03:26,250 And we have this just wealth of information and extremely 69 00:03:26,250 --> 00:03:31,250 high resolution information about Solar System planets. 70 00:03:31,270 --> 00:03:32,103 Next slide. 71 00:03:35,100 --> 00:03:38,450 So if we want to look at this from an observational problem, 72 00:03:38,450 --> 00:03:41,120 this is an example of what these two different systems 73 00:03:41,120 --> 00:03:44,460 would look like using NIRSPEC on Keck. 74 00:03:44,460 --> 00:03:47,920 And so if you were to try to take a spectrum of Jupiter 75 00:03:47,920 --> 00:03:50,550 with NIRSPEC, which has been done and I'll show a little bit 76 00:03:50,550 --> 00:03:55,550 in a little bit, it is impossible to get the entirety 77 00:03:56,100 --> 00:03:58,910 of Jupiter into the slit of NIRSPEC 78 00:03:58,910 --> 00:04:02,810 and therefore it's impossible to get a spectrum of Jupiter 79 00:04:02,810 --> 00:04:06,170 as a whole at one time, whereas if you were to put NIRSPEC 80 00:04:06,170 --> 00:04:09,470 behind AO, and use a coronagraph to block out the 81 00:04:09,470 --> 00:04:12,980 central starlight, you can actually get all of the light 82 00:04:12,980 --> 00:04:17,870 from, for example, the HR 8799 see planet down your slit. 83 00:04:17,870 --> 00:04:21,730 Most of these are very not these are not comparable 84 00:04:21,730 --> 00:04:23,653 observations that are being taken. 85 00:04:24,730 --> 00:04:25,563 Next slide. 86 00:04:27,440 --> 00:04:31,580 So, Gordy Berger and his team did this back in 2015, 87 00:04:31,580 --> 00:04:36,280 where they placed a slit at different locations on Jupiter. 88 00:04:36,280 --> 00:04:40,160 And the resulting spectra that they took in band 89 00:04:40,160 --> 00:04:42,740 vary widely depending on what portion 90 00:04:42,740 --> 00:04:44,820 of Jupiter they were looking at. 91 00:04:44,820 --> 00:04:47,450 And this is because there's a lot of interesting 92 00:04:47,450 --> 00:04:48,810 atmospheric dynamics happening. 93 00:04:48,810 --> 00:04:52,140 And so the spectrum that you observe is going to be 94 00:04:53,380 --> 00:04:55,590 broadly different depending on which part of the planet 95 00:04:55,590 --> 00:04:56,423 you're looking at. 96 00:04:56,423 --> 00:05:00,590 And so if we want to turn Jupiter into something that looks 97 00:05:00,590 --> 00:05:02,730 more like the exoplanets that we will observe, 98 00:05:02,730 --> 00:05:05,590 we're going to have to use some tricks to do that. 99 00:05:05,590 --> 00:05:10,270 Now, there was a team led by Theodora Karalidi, 100 00:05:10,270 --> 00:05:13,370 who looked at Jupiter with HST and they took 101 00:05:13,370 --> 00:05:18,260 broadband photometry as Jupiter rotated on the sky, 102 00:05:18,260 --> 00:05:20,940 and you can see that even then the broadband photometry 103 00:05:20,940 --> 00:05:23,803 of the planet changes significantly as it rotates. 104 00:05:25,531 --> 00:05:26,364 Next slide. 105 00:05:28,940 --> 00:05:31,100 So, there have been several missions, 106 00:05:31,100 --> 00:05:34,320 a few of which I've put up on the slide here that have 107 00:05:34,320 --> 00:05:36,180 attempted to look at Solar System planets 108 00:05:36,180 --> 00:05:38,690 to study them as exoplanets. 109 00:05:38,690 --> 00:05:41,870 So there was the NASA EPOXI mission which looked at Earth 110 00:05:41,870 --> 00:05:45,440 as an exoplanet and they were able to determine 111 00:05:46,350 --> 00:05:51,210 with pretty high certainty that Earth contains liquid water, 112 00:05:51,210 --> 00:05:55,373 and has also large surfaces of land. 113 00:05:56,430 --> 00:05:59,860 There was more in Mayorga paper from 2016 in which he was 114 00:05:59,860 --> 00:06:03,600 looking at phase curves of Jupiter and showing how Jupiter 115 00:06:03,600 --> 00:06:06,930 would look at different phases of its orbit, 116 00:06:06,930 --> 00:06:10,170 and thus how an exoplanet would look as well. 117 00:06:10,170 --> 00:06:13,090 And there was also Carl Sagan seminal work from 1993 118 00:06:13,090 --> 00:06:17,240 where he they turned Galileo around to look at Earth, 119 00:06:17,240 --> 00:06:20,700 the Pale Blue Dot, and using both radiometer is 120 00:06:20,700 --> 00:06:24,180 relative spectroscopy, we're also able to determine the 121 00:06:24,180 --> 00:06:28,990 spectroscopic, the atmospheric composition of Earth. 122 00:06:28,990 --> 00:06:31,130 However, all of these have been fairly 123 00:06:31,130 --> 00:06:33,290 serendipitous missions, and there has never been 124 00:06:33,290 --> 00:06:38,290 a dedicated mission to really look at spectroscopy 125 00:06:38,500 --> 00:06:40,960 of Solar System planets as if they were exoplanets. 126 00:06:40,960 --> 00:06:42,950 And so that is where PEAS comes in. 127 00:06:42,950 --> 00:06:43,783 Next slide. 128 00:06:46,140 --> 00:06:50,090 So PEAS is the planet of exoplanet analog spectrograph, 129 00:06:50,090 --> 00:06:52,550 and the major component of PEAS that really makes it 130 00:06:52,550 --> 00:06:57,550 different from any other any other instruments 131 00:06:57,970 --> 00:07:00,270 that have observed Solar System planets, as exoplanet 132 00:07:00,270 --> 00:07:01,960 is that we're going to use an object called 133 00:07:01,960 --> 00:07:03,360 an integrating sphere. 134 00:07:03,360 --> 00:07:08,280 That is, basically it's a small spherical object that has a 135 00:07:08,280 --> 00:07:11,670 very highly reflected, or highly reflective surface on the 136 00:07:11,670 --> 00:07:15,010 inside that bounces around the light very evenly. 137 00:07:15,010 --> 00:07:18,310 So that whatever image you have going into the sphere, 138 00:07:18,310 --> 00:07:20,710 whatever, the light that comes out on the other side 139 00:07:20,710 --> 00:07:22,550 is very evenly mixed. 140 00:07:22,550 --> 00:07:25,120 And so I show an example here on the screen, 141 00:07:25,120 --> 00:07:29,090 where if you take an image of Jupiter from your telescope 142 00:07:29,090 --> 00:07:30,660 and put it into the integrating sphere, 143 00:07:30,660 --> 00:07:31,960 what do you get out on the other side 144 00:07:31,960 --> 00:07:34,170 is just a very smooth flat image. 145 00:07:34,170 --> 00:07:36,520 And so we're going to take the light from a telescope, 146 00:07:36,520 --> 00:07:37,830 put it through an integrating sphere, 147 00:07:37,830 --> 00:07:39,980 and then send that to a spectrograph. 148 00:07:39,980 --> 00:07:42,450 And PEAS will be observing all of the 149 00:07:42,450 --> 00:07:44,393 Solar System planets in this way. 150 00:07:45,470 --> 00:07:46,420 Next slide, please. 151 00:07:48,220 --> 00:07:51,240 So the basic broad concept of how PEAS works is that 152 00:07:51,240 --> 00:07:54,530 we're going to have a dedicated half meter telescope 153 00:07:54,530 --> 00:07:57,190 that will be observing all the Solar System planets. 154 00:07:57,190 --> 00:08:01,240 And then I've traced out the broad overview 155 00:08:01,240 --> 00:08:02,600 of the instrument layout. 156 00:08:02,600 --> 00:08:05,450 And so there will be a beam splitter that sends light to an 157 00:08:05,450 --> 00:08:09,400 imaging camera so that we can take simultaneous imaging 158 00:08:09,400 --> 00:08:12,740 and for that to also help with tracking. 159 00:08:12,740 --> 00:08:15,530 And then the majority of the light is actually going to be 160 00:08:15,530 --> 00:08:17,560 going into an integrating sphere where 161 00:08:17,560 --> 00:08:19,270 it will get disk-integrated. 162 00:08:19,270 --> 00:08:22,810 And then that light will be fed via fiber optic cable 163 00:08:22,810 --> 00:08:24,930 into an off the shelf spectrograph. 164 00:08:24,930 --> 00:08:27,300 So now I'm going to step through each of the components of 165 00:08:27,300 --> 00:08:30,460 PEAS and tell you a little bit about each of them. 166 00:08:30,460 --> 00:08:31,300 Next slide. 167 00:08:31,300 --> 00:08:32,290 Thanks. 168 00:08:32,290 --> 00:08:35,160 So our telescope is a Planewave RC-20. 169 00:08:35,160 --> 00:08:38,673 It's a half meter telescope with their fancy L500 mount. 170 00:08:40,190 --> 00:08:44,150 And these are really very solid telescopes that I think 171 00:08:44,150 --> 00:08:46,960 have been growing in popularity lately. 172 00:08:46,960 --> 00:08:48,970 We have the mount sitting in our shops that 173 00:08:48,970 --> 00:08:53,040 arrived literally the day before campus shut down for COVID. 174 00:08:53,040 --> 00:08:56,890 And the telescope should be arriving within about a month. 175 00:08:56,890 --> 00:09:01,300 It has very decent pointing accuracy and precision, 176 00:09:01,300 --> 00:09:03,460 and as well as tracking accuracy, 177 00:09:03,460 --> 00:09:06,930 and it comes complete with his own observing software, 178 00:09:06,930 --> 00:09:09,170 where you can basically align 179 00:09:09,170 --> 00:09:11,110 your telescope and get started observing 180 00:09:11,110 --> 00:09:12,270 within about five minutes. 181 00:09:12,270 --> 00:09:13,590 It's completely automated. 182 00:09:13,590 --> 00:09:14,783 It's really great. 183 00:09:15,820 --> 00:09:16,653 Next slide. 184 00:09:18,350 --> 00:09:20,750 The major component of our instrument is the 185 00:09:20,750 --> 00:09:21,980 integrating sphere itself. 186 00:09:21,980 --> 00:09:25,040 And we bought a one inch integrating sphere from a company 187 00:09:25,040 --> 00:09:26,313 called Spectral Products. 188 00:09:27,410 --> 00:09:31,950 Now integrating sphere, interestingly ends up costing you 189 00:09:31,950 --> 00:09:36,693 a lot in terms of throughput because you get an A omega cut. 190 00:09:38,060 --> 00:09:41,270 But basically what you want whenever you're trying to 191 00:09:41,270 --> 00:09:43,590 maximize the throughput through your integrating spheres, 192 00:09:43,590 --> 00:09:45,600 you want smaller port fractions. 193 00:09:45,600 --> 00:09:47,980 So that's like how big the entrance and exit holes are 194 00:09:47,980 --> 00:09:50,440 compared to the size of the sphere. 195 00:09:50,440 --> 00:09:52,720 Smaller sphere is better. 196 00:09:52,720 --> 00:09:53,980 And then you want to make sure that you have 197 00:09:53,980 --> 00:09:55,640 really good fiber coupling. 198 00:09:55,640 --> 00:09:58,190 And in this case, we actually were lucky in that we were 199 00:09:58,190 --> 00:10:01,800 able to get some leftover fibers from the mango projects 200 00:10:02,650 --> 00:10:05,950 that will basically turn this into 201 00:10:05,950 --> 00:10:07,970 a little kind of IFU. 202 00:10:07,970 --> 00:10:10,920 But basically just many fibers that we'll be able to feed 203 00:10:10,920 --> 00:10:14,260 from the integrating sphere into the spectrograph itself. 204 00:10:14,260 --> 00:10:15,640 And then the last thing is reflectance, 205 00:10:15,640 --> 00:10:18,720 which actually is quite good with this material called 206 00:10:18,720 --> 00:10:22,040 spectral line has extremely broad wavelengths coverage 207 00:10:22,040 --> 00:10:25,890 and you get about 99% reflectivity across the whole 208 00:10:25,890 --> 00:10:30,890 basically from the blue optical UV ish all the way out 209 00:10:31,940 --> 00:10:33,800 into the mid infrared. 210 00:10:33,800 --> 00:10:34,633 Next slide. 211 00:10:36,470 --> 00:10:38,680 So, the whole optical design of PEAS 212 00:10:38,680 --> 00:10:39,880 is actually quite simple. 213 00:10:39,880 --> 00:10:43,130 There are no powered optics, behind the telescope, 214 00:10:43,130 --> 00:10:44,480 just beam splitters. 215 00:10:44,480 --> 00:10:47,450 So on the left I'm showing the optical layout of the 216 00:10:47,450 --> 00:10:51,270 Planewave telescope, the primary and secondary mirrors. 217 00:10:51,270 --> 00:10:54,620 And then to the right of the line is basically 218 00:10:54,620 --> 00:10:56,750 the backplate of the telescope 219 00:10:56,750 --> 00:11:00,760 and after the first beam splitter is where we're going to 220 00:11:00,760 --> 00:11:04,750 send a small fraction of the light to an imager. 221 00:11:04,750 --> 00:11:07,460 And then we just use a series of compensating beam splitters 222 00:11:07,460 --> 00:11:10,980 afterwards to correct the optical quality before sending 223 00:11:10,980 --> 00:11:14,690 the remaining light into the integrating sphere. 224 00:11:14,690 --> 00:11:17,990 And as you can see, the whole thing is also fairly compact, 225 00:11:17,990 --> 00:11:20,940 because the telescope diameter itself is only a half meter. 226 00:11:21,930 --> 00:11:22,763 Next slide. 227 00:11:24,730 --> 00:11:27,470 So we're buying off the shelf spectrographs and cameras, 228 00:11:27,470 --> 00:11:28,540 they both been purchased, 229 00:11:28,540 --> 00:11:31,493 and the SBIG is sitting at home on my kitchen table. 230 00:11:33,200 --> 00:11:37,090 And so we have an SBIG STF-8300 imager, which is 231 00:11:39,546 --> 00:11:43,040 fairly decent quality off the shelf imager that you can get 232 00:11:43,040 --> 00:11:48,040 for not too expensive, and it has decent optical coverage 233 00:11:48,940 --> 00:11:51,940 from about 350 to 900 nanometers. 234 00:11:51,940 --> 00:11:53,930 And it's actually got way more detector real estate 235 00:11:53,930 --> 00:11:56,080 than we actually need for this project 236 00:11:56,080 --> 00:11:59,980 but we're not upset about that. 237 00:11:59,980 --> 00:12:03,350 And then the spectrograph that we just recently got our 238 00:12:03,350 --> 00:12:08,040 purchase order and for is an ANDOR Kymera 328-i. 239 00:12:08,040 --> 00:12:13,040 And so we did some significant amount of testing again 240 00:12:13,140 --> 00:12:17,020 from my kitchen table during the COVID crisis of making sure 241 00:12:17,020 --> 00:12:20,200 that the spectrograph would be sensitive enough to detect 242 00:12:20,200 --> 00:12:23,200 the signals of Jupiter and Venus for example. 243 00:12:23,200 --> 00:12:28,200 And these off the shelf spectrographs actually pretty good 244 00:12:28,900 --> 00:12:30,190 for what you get. 245 00:12:30,190 --> 00:12:33,190 So there's a grading chart inside the spectrograph 246 00:12:33,190 --> 00:12:37,540 that can hold up to for grading from Richardson. 247 00:12:37,540 --> 00:12:40,960 We got protective silver coating on all of our optics 248 00:12:40,960 --> 00:12:43,260 and it has an adjustable slit. 249 00:12:43,260 --> 00:12:45,820 And then we also bought an iDUS 420 imager 250 00:12:45,820 --> 00:12:47,170 to go on the back end. 251 00:12:47,170 --> 00:12:50,660 And this is a 256 by 1024 array that 252 00:12:50,660 --> 00:12:53,600 has extremely good quality especially in the red which is 253 00:12:53,600 --> 00:12:56,120 where we would expect some of the most interesting science 254 00:12:56,120 --> 00:13:01,120 to be done in terms of Solar System spectroscopy. 255 00:13:01,690 --> 00:13:02,523 Next slide. 256 00:13:03,830 --> 00:13:07,580 - [Tiffany] Emily just to interrupt, for the 13 minute mark. 257 00:13:07,580 --> 00:13:08,570 - [Emily] Thank you. 258 00:13:08,570 --> 00:13:09,450 - [Tiffany] Thank you. 259 00:13:09,450 --> 00:13:10,570 - [Emily] So this is what PEAS 260 00:13:10,570 --> 00:13:11,600 is going to look like to scale. 261 00:13:11,600 --> 00:13:15,180 That's a picture of me during the NIRSPEC upgrade on Keck. 262 00:13:15,180 --> 00:13:17,890 And I'm about five foot three tall. 263 00:13:17,890 --> 00:13:21,470 And so PEAS is going to ride around on a cart. 264 00:13:21,470 --> 00:13:25,310 And every all of the optics are going to mount 265 00:13:25,310 --> 00:13:26,640 to the back end of the telescope 266 00:13:26,640 --> 00:13:28,550 and have room to move around with the telescope, 267 00:13:28,550 --> 00:13:30,530 I've excluded some points. 268 00:13:30,530 --> 00:13:33,560 And then sitting next to the telescope cart, there will be a 269 00:13:33,560 --> 00:13:36,970 computer cart that will hold the laptop which runs the 270 00:13:36,970 --> 00:13:39,110 telescope software, the imager 271 00:13:39,110 --> 00:13:40,760 and the spectrograph software. 272 00:13:40,760 --> 00:13:42,420 And the spectrograph will also be sitting 273 00:13:42,420 --> 00:13:45,950 on the computer cart and connected via fiber optic cable 274 00:13:45,950 --> 00:13:47,493 to the integrating sphere. 275 00:13:48,730 --> 00:13:49,563 Next slide. 276 00:13:51,160 --> 00:13:54,910 PEAS will live inside the dome of the Shane Telescope 277 00:13:54,910 --> 00:13:56,350 at Lick Observatory. 278 00:13:56,350 --> 00:13:58,460 And then every night that we're observing, we're going to 279 00:13:58,460 --> 00:14:01,190 wheel it out into the parking lot to the east. 280 00:14:01,190 --> 00:14:04,378 And then you can see the little PEAS logo, which is where 281 00:14:04,378 --> 00:14:06,600 we're hoping to be observing from. 282 00:14:06,600 --> 00:14:09,730 And we are very grateful to all of the staff 283 00:14:09,730 --> 00:14:11,690 at Lick Observatory, who are also excited about having 284 00:14:11,690 --> 00:14:14,173 a new project coming out there. 285 00:14:15,550 --> 00:14:17,930 And we are hopefully going to be getting on Sky sometime 286 00:14:17,930 --> 00:14:21,410 this winter, but I'll get into the timeline in a little bit. 287 00:14:21,410 --> 00:14:22,360 Next slide, please. 288 00:14:25,594 --> 00:14:28,590 So the major science mission, we have actually a lot of 289 00:14:28,590 --> 00:14:30,600 goals that we'd like to accomplish. 290 00:14:30,600 --> 00:14:31,820 So we'll walk through each of these. 291 00:14:31,820 --> 00:14:35,930 We'd like to measure atmospheric composition of all of the 292 00:14:35,930 --> 00:14:38,060 Solar System planets, and we want to compare those 293 00:14:38,060 --> 00:14:41,390 to in situ, or flyby measurements that have been taken of 294 00:14:41,390 --> 00:14:43,700 all of the Solar System planets. 295 00:14:43,700 --> 00:14:47,370 We'd also like to produce a 2D surface maps of Venus, Mars, 296 00:14:47,370 --> 00:14:49,170 Jupiter, Saturn, Uranus and Neptune. 297 00:14:50,290 --> 00:14:53,950 So these would be 2D surface maps that we are reproducing 298 00:14:53,950 --> 00:14:56,670 from the spectroscopy itself, basically verifying 299 00:14:56,670 --> 00:14:57,933 our ability to do that. 300 00:14:58,950 --> 00:15:02,200 Produce fiducial measurements that will be used to plan 301 00:15:02,200 --> 00:15:05,050 future instruments that are designed 302 00:15:05,050 --> 00:15:06,920 to look at exoplanet missions. 303 00:15:06,920 --> 00:15:10,820 So we're really expecting that the kinds of measurements 304 00:15:10,820 --> 00:15:12,690 that we take are going to tell us whether or not 305 00:15:12,690 --> 00:15:15,430 what we've been doing as far as characterizing exoplanets 306 00:15:15,430 --> 00:15:18,070 is right or whether we've been completely off base. 307 00:15:18,070 --> 00:15:21,910 And hopefully be able to tell the HabEx/LUVOIR 308 00:15:21,910 --> 00:15:25,100 and all the extremely large telescope instruments. 309 00:15:25,100 --> 00:15:26,970 This is the wavelength range you need to be looking at 310 00:15:26,970 --> 00:15:30,583 if you want to find different kinds of molecules, et cetera. 311 00:15:31,920 --> 00:15:33,530 More long term, we'd like to be looking at 312 00:15:33,530 --> 00:15:36,060 Time-Series Observations to explore variability 313 00:15:36,060 --> 00:15:37,110 and weather patterns. 314 00:15:38,140 --> 00:15:40,540 Kind of a stretch goal for us would be to study planetary 315 00:15:40,540 --> 00:15:43,130 seismology of the Solar System planets. 316 00:15:43,130 --> 00:15:45,980 And then of course, we want to produce an atlas of 317 00:15:45,980 --> 00:15:49,130 Solar System planets spectra that basically is going to 318 00:15:49,130 --> 00:15:53,250 serve as a really solid comparison to all the ground truth 319 00:15:53,250 --> 00:15:56,560 information that we have the Solar System planets. 320 00:15:56,560 --> 00:15:57,393 Next slide. 321 00:15:59,580 --> 00:16:02,360 So the timeline got pushed back a little bit, unfortunately 322 00:16:02,360 --> 00:16:04,780 due to COVID, but we're not too far away 323 00:16:04,780 --> 00:16:06,360 from where we were originally. 324 00:16:06,360 --> 00:16:09,210 So the design hat is in the process of being finalized 325 00:16:09,210 --> 00:16:11,170 and will be finalized over the summer. 326 00:16:11,170 --> 00:16:15,210 And all of our hardware should be in hand by the fall. 327 00:16:15,210 --> 00:16:18,400 And then we will be assembling and testing that as we 328 00:16:18,400 --> 00:16:21,840 are able to in the lab here at UC Santa Cruz. 329 00:16:21,840 --> 00:16:25,610 And then we'll start commissioning, hopefully this winter. 330 00:16:25,610 --> 00:16:28,260 After that, we'll have approximately a year to do 331 00:16:28,260 --> 00:16:31,060 our initial Solar System Atlas observations, 332 00:16:31,060 --> 00:16:33,070 and maybe six months into that we'll start 333 00:16:33,070 --> 00:16:35,293 with our Time-Series Observation. 334 00:16:36,410 --> 00:16:37,303 Next slide. 335 00:16:38,790 --> 00:16:42,000 So I really just wanted to finish up by saying that PEAS is 336 00:16:42,000 --> 00:16:45,260 a mission for the whole exoplanet and planetary community. 337 00:16:45,260 --> 00:16:46,810 And we would really love to get 338 00:16:46,810 --> 00:16:48,740 more people involved in this. 339 00:16:48,740 --> 00:16:51,620 We are going to be making our data 340 00:16:51,620 --> 00:16:54,040 publicly available to the community. 341 00:16:54,040 --> 00:16:57,910 And so if you have any excitement about doing cool science 342 00:16:57,910 --> 00:17:00,870 with disk-integrated spectra of Solar System planets, 343 00:17:00,870 --> 00:17:02,010 please reach out to me. 344 00:17:02,010 --> 00:17:05,080 And also PEAS of a modular design, 345 00:17:05,080 --> 00:17:08,470 and is quite easy to modify or add things to it. 346 00:17:08,470 --> 00:17:10,820 And so if you have any ideas about things 347 00:17:10,820 --> 00:17:13,933 that you'd like to try, please get in touch. 348 00:17:15,890 --> 00:17:16,723 Thank you. 349 00:17:18,050 --> 00:17:18,883 - [Tiffany] Thanks, Emily. 350 00:17:18,883 --> 00:17:21,770 Yeah, sends out a free talk really exciting stuff. 351 00:17:21,770 --> 00:17:23,650 I don't see any questions currently. 352 00:17:23,650 --> 00:17:26,113 So I'll just have a quick one as we transition. 353 00:17:27,070 --> 00:17:29,080 A question I asked earlier in fact. 354 00:17:29,080 --> 00:17:32,530 Have you considered submitting a some sort of white paper 355 00:17:32,530 --> 00:17:35,662 to describe the PEAS instrument for the Planetary Decadal? 356 00:17:35,662 --> 00:17:38,380 Because I see quite a few synergies there obviously. 357 00:17:38,380 --> 00:17:39,213 (laughs) 358 00:17:39,213 --> 00:17:40,150 - [Emily] I had not considered writing white paper, 359 00:17:40,150 --> 00:17:41,490 but that's a very good idea. 360 00:17:41,490 --> 00:17:45,730 I was at the exoplanets in our backyard conference in 361 00:17:45,730 --> 00:17:48,920 February and that was really fantastic to get to interface 362 00:17:48,920 --> 00:17:50,360 with all the planetary people 363 00:17:50,360 --> 00:17:52,160 and I definitely learned a lot. 364 00:17:52,160 --> 00:17:53,930 - [Tiffany] Yeah, yeah, I think it'd be good to get the idea 365 00:17:53,930 --> 00:17:55,770 out there and see what other applications 366 00:17:55,770 --> 00:17:57,620 you know might be possible with PEAS.