WEBVTT FILE 1 00:00:00.166 --> 00:00:05.105 Music 2 00:00:05.205 --> 00:00:09.442 The James Webb Space Telescope is exploring the universe 3 00:00:09.809 --> 00:00:13.480 and it's revealed sights humanity has never seen. 4 00:00:13.580 --> 00:00:17.017 Music 5 00:00:17.050 --> 00:00:21.554 So the goals of the first images were to showcase the impressive 6 00:00:21.554 --> 00:00:26.226 capabilities of JWST to the public and to the astronomical community 7 00:00:26.226 --> 00:00:27.127 at large. 8 00:00:27.127 --> 00:00:31.364 And the subsequent images have been taken more for specific science questions 9 00:00:31.364 --> 00:00:34.501 that have been asked by the various groups in the astronomical community. 10 00:00:34.768 --> 00:00:38.104 And so those pictures are much more tied to specific science questions. 11 00:00:38.605 --> 00:00:39.873 And still, they're beautiful. 12 00:00:41.274 --> 00:00:43.676 The JWST mission has taken a long time to get here. 13 00:00:43.676 --> 00:00:45.979 It's been 20, 25 years in production, 14 00:00:46.513 --> 00:00:49.549 and so it's been a lot of effort by a lot of people, 15 00:00:49.549 --> 00:00:53.319 including myself, over a decade and a half myself on the mission. 16 00:00:53.620 --> 00:00:54.988 And so to actually get to the point 17 00:00:54.988 --> 00:00:59.059 where we get to see the pictures, the fruits of all that work was really, 18 00:00:59.526 --> 00:01:02.262 really amazing for me to finally see that come through. 19 00:01:02.429 --> 00:01:04.264 And they were just so spectacular. 20 00:01:04.264 --> 00:01:05.832 It was excellent. 21 00:01:05.832 --> 00:01:08.468 It paid back all that effort and more for me. 22 00:01:09.269 --> 00:01:13.339 So for a team of scientists to get time to actually observe with Webb, 23 00:01:13.740 --> 00:01:15.909 the first thing they need to do is write a proposal. 24 00:01:16.376 --> 00:01:19.846 And so that proposal is a text, but it also comes 25 00:01:19.846 --> 00:01:23.183 with what they want to do, what targets they want to observe, 26 00:01:23.583 --> 00:01:27.787 and which instruments they want to use on JWST and which modes. 27 00:01:27.787 --> 00:01:31.658 And so then that gets put together and submitted, submits here to the Institute. 28 00:01:31.658 --> 00:01:34.294 But then the Institute convenes a panel of experts 29 00:01:34.494 --> 00:01:37.063 from outside the Institute for us all astronomers. 30 00:01:37.430 --> 00:01:40.633 And then they get to rank they look at all the proposals 31 00:01:40.633 --> 00:01:43.903 in a specific area and then rank them, and the top ranked proposals 32 00:01:44.170 --> 00:01:47.240 then get forwarded to actually take their observations. 33 00:01:48.675 --> 00:01:51.544 When a science team is awarded time to work with Webb. 34 00:01:52.011 --> 00:01:55.849 They start by using a special software to set the required parameters 35 00:01:56.015 --> 00:01:58.017 for the telescope to conduct their science. 36 00:01:58.918 --> 00:02:01.754 The software allow scientists to use different modes 37 00:02:01.754 --> 00:02:04.791 on Webb's instruments to achieve their scientific objectives. 38 00:02:05.992 --> 00:02:09.162 When it's time for the observation, the code instructs the telescope 39 00:02:09.229 --> 00:02:12.966 to locate the target object and capture several images of it. 40 00:02:13.199 --> 00:02:17.670 Light from the target object is processed through the instruments and the raw data 41 00:02:17.670 --> 00:02:21.441 the science team requires is stored onto Webb's onboard hard drive. 42 00:02:22.075 --> 00:02:25.845 Once the team's data is collected, their data and images are transmitted 43 00:02:25.845 --> 00:02:26.446 to Earth 44 00:02:26.446 --> 00:02:29.983 from Webb to NASA's Deep Space Network ground stations, 45 00:02:29.983 --> 00:02:34.087 where their data gets routed directly to the Space Telescope Science Institute. 46 00:02:34.888 --> 00:02:37.423 Once we get the data here in Baltimore at the Institute, 47 00:02:37.724 --> 00:02:39.559 then we run it through our pipeline. 48 00:02:39.559 --> 00:02:42.962 That is a series of steps that removes the artifacts 49 00:02:43.029 --> 00:02:45.732 from the instrument or the detectors that we know about, 50 00:02:45.999 --> 00:02:48.401 because we've taken extensive calibration observations 51 00:02:48.735 --> 00:02:52.205 and we now produce these cleaned images that are just about the 52 00:02:52.205 --> 00:02:54.174 astrophysical source we're interested in. 53 00:02:54.174 --> 00:02:57.010 And then the all those images go into an archive here 54 00:02:57.010 --> 00:03:00.547 at the Institute that's then available to the proposers 55 00:03:01.781 --> 00:03:04.417 that they can then download it and start doing their science on it. 56 00:03:04.951 --> 00:03:08.621 So if we're going to produce a color image out of the observations, 57 00:03:08.621 --> 00:03:12.225 then we take we've taken multiple images in different filters. 58 00:03:12.692 --> 00:03:15.461 And then those after they've been processed through 59 00:03:15.461 --> 00:03:17.297 and removed all the instrumental artifacts, 60 00:03:17.297 --> 00:03:21.401 then we pass them along to the experts in our public outreach office 61 00:03:21.734 --> 00:03:26.706 that then turn them into the really sensational color images that we all love. 62 00:03:27.740 --> 00:03:30.743 When you're processing any sort of astronomical image, 63 00:03:31.211 --> 00:03:33.780 those images are taken through different filters. 64 00:03:33.780 --> 00:03:37.050 So the light's captured through different filters and it starts out grayscale. 65 00:03:37.283 --> 00:03:40.220 And then so you actually get color information 66 00:03:40.220 --> 00:03:43.923 from taking the light in those filters, and then you assign colors afterwards 67 00:03:43.923 --> 00:03:46.159 like an image processor will assign colors. 68 00:03:46.326 --> 00:03:48.795 And we do this typically what we call chromatic ordering, 69 00:03:48.795 --> 00:03:51.164 which just means that the shortest wavelengths gets assigned. 70 00:03:51.164 --> 00:03:54.934 The blue color in between it's green, and then the longest wavelength 71 00:03:54.934 --> 00:03:56.269 gets assigned the red color. 72 00:03:56.269 --> 00:03:59.973 And then we additively combine those together to get our full color image. 73 00:04:00.073 --> 00:04:03.109 The reason we want to color the images is because there's actually more 74 00:04:03.109 --> 00:04:04.477 that you can get, more information 75 00:04:04.477 --> 00:04:06.579 that you can get from the image if you see it in color. 76 00:04:06.879 --> 00:04:09.649 If you're looking at a galaxy in optical light, 77 00:04:10.049 --> 00:04:12.318 we expect that they're going to be star forming regions 78 00:04:12.318 --> 00:04:14.887 and they're going to show up as these bright blue regions. 79 00:04:14.887 --> 00:04:18.758 And then if there's hydrogen gas around them, that will show up as bright red. 80 00:04:19.259 --> 00:04:22.028 And so if we can apply the color to the different filters 81 00:04:22.028 --> 00:04:25.164 and make an image in color, you can actually just see that right away. 82 00:04:25.164 --> 00:04:27.433 And you learn something new from the image by seeing it in color. 83 00:04:28.167 --> 00:04:31.537 Webb's imagery and science are revolutionary. 84 00:04:32.438 --> 00:04:36.209 It's challenging our theories of the universe and generating more 85 00:04:36.209 --> 00:04:37.910 questions we need to answer. 86 00:04:37.910 --> 00:04:45.718 Music