1 00:00:00,000 --> 00:00:10,158 [Music] 2 00:00:10,158 --> 00:00:12,586 Hello, my name is Marjorie Decleir. 3 00:00:12,586 --> 00:00:14,439 Hi, I'm Alberto Noriega-Crespo. 4 00:00:14,439 --> 00:00:16,667 Hi, my name is Paul Scowen. 5 00:00:16,667 --> 00:00:18,992 Hello, I am Jesus Toala. 6 00:00:24,600 --> 00:00:29,640 So the Eagle Nebula is a very big  star-forming region and it is full   7 00:00:29,640 --> 00:00:34,341 of dust and gas, and in these clouds stars  are continuously being formed. 8 00:00:34,341 --> 00:00:40,800 So triggered star formation is a mechanism by which star  formation self-propagates across a galaxy. 9 00:00:40,800 --> 00:00:47,700 The idea is that you make a series of stars  in one particular location; that causes this   10 00:00:47,700 --> 00:00:52,560 ionized cavity that we recognize as a nebula, of which the Eagle Nebula is a good example. 11 00:00:52,560 --> 00:00:58,560 The ionizing radiation that comes off those  central stars blows a bubble, that's   12 00:00:58,560 --> 00:01:05,400 really what the cavity of a nebula is, and as  that bubble grows it collapses and compresses   13 00:01:05,400 --> 00:01:13,320 the material outside the wall of that cavity, and the material there, the gas and dust, is then   14 00:01:13,320 --> 00:01:19,234 compressed and collapses under gravity to form  a second generation of stars and planets. 15 00:01:24,900 --> 00:01:32,220 One of the features that one sees at optical wavelengths in the large view is that really the dust is present and forms 16 00:01:32,220 --> 00:01:38,800 the shape of an eagle in the outer part, and  it's illuminated by the newborn starts, some of them are very hot. 17 00:01:38,800 --> 00:01:47,241 In the near-infrared you're seeing the stars themselves, you're seeing heat of the light that's being emitted by them, 18 00:01:47,241 --> 00:01:51,639 and you're seeing where those stars are relative to the walls of the nebula. 19 00:01:51,639 --> 00:01:57,600 So in the infrared image what we can  see is that the dust emits light and depending on   20 00:01:57,600 --> 00:02:04,200 the temperature of the dust particles, it will emit  at shorter infrared wavelengths or longer infrared wavelengths. 21 00:02:04,200 --> 00:02:09,300 Also people notice in particularly when  you go to longer wavelengths, is that you don't see   22 00:02:09,300 --> 00:02:16,080 as many sources. The stars themselves have a chaff  of their emission, in particular when they're very young they're   23 00:02:16,080 --> 00:02:20,351 very blue, and so they essentially disappear  because essentially there are not emitting.   24 00:02:20,351 --> 00:02:26,820 You get to see some other sources and indeed  probably many of the sources are cooler, older   25 00:02:26,820 --> 00:02:28,881 and may not belong to the cluster itself. 26 00:02:28,881 --> 00:02:32,760 In the x-rays, we see the hottest contribution of the gas 27 00:02:32,760 --> 00:02:37,320 which is produced by the stellar winds  from the most massive stars in the region. 28 00:02:38,760 --> 00:02:42,840 My favorite thing about the Eagle Nebula is  the fact that we can use multi-instrument   29 00:02:42,840 --> 00:02:48,480 observations to characterize the origins  of stars. Multi-wavelength observations   30 00:02:48,480 --> 00:02:55,740 help us peer into a phenomenon with different  glasses, in this case, stellar nurseries. 31 00:03:01,380 --> 00:03:07,301 The Pillars of Creation is a collection of filaments  that are located at the heart of the Eagle Nebula. 32 00:03:07,301 --> 00:03:13,320 This was formed as a result of the impact of the most massive stars in the nebula. 33 00:03:13,320 --> 00:03:19,080 These stars have winds and strong UV light  that evaporates the initial configuration of   34 00:03:19,080 --> 00:03:26,375 the nebula from which they were born. As a result, the pillars point towards the location of these massive stars. 35 00:03:26,375 --> 00:03:31,145 The name "Creation" comes from the  fact that there are lots and lots of stars being   36 00:03:31,145 --> 00:03:37,980 formed continuously out of the dust and gas clouds, and so this is very interesting because when we   37 00:03:37,980 --> 00:03:43,620 study this image we can learn a lot about  how stars are being formed in these clouds. 38 00:03:50,420 --> 00:03:55,993 In the Hubble images themselves, we don't penetrate  the columns, we don't see the stars. 39 00:03:55,993 --> 00:04:01,689 We see the surroundings and we see them illuminated,  perhaps some of the edges we can see some of the protostars. 40 00:04:01,689 --> 00:04:07,020 Infrared images like the ones from JWST, we begin to see not only the dust  41 00:04:07,020 --> 00:04:12,855 but also we can see the protostars and  we can see through some of the columns, 42 00:04:12,855 --> 00:04:15,400 and we can see where they are being born. 43 00:04:15,900 --> 00:04:20,640 In the MIRI images, this filter was chosen specifically to 44 00:04:20,640 --> 00:04:25,030 probe a particle that we call polycyclic aromatic  hydrocarbons. 45 00:04:25,030 --> 00:04:33,634 These specific dust particles will emit light and that's why you can see that parts of these dust clouds are now shining. 46 00:04:34,145 --> 00:04:42,480 In the x-ray you're going to see a rather different story. Most of the nebulosity that you see in the   47 00:04:42,480 --> 00:04:48,780 visible and in the infrared disappears altogether  and all you see is the bright emission coming   48 00:04:48,780 --> 00:04:54,720 from those few massive stars kicking out all  of the radiation that lights up the nebula in   49 00:04:54,720 --> 00:04:59,460 the visible in the infrared, but in the x-ray all  you see is the stars and that's pretty much it. 50 00:05:01,837 --> 00:05:06,180 What strikes me the most of the James Webb images is the details  51 00:05:06,180 --> 00:05:09,420 There is no comparison with previous  infrared missions in terms of   52 00:05:09,420 --> 00:05:13,320 sharpness and fine detail disclosed  by the James Webb Space Telescope. 53 00:05:20,143 --> 00:05:23,573 Have you ever wanted to make your own astronomy image? 54 00:05:24,148 --> 00:05:26,905 Tell us about the colors you choose. 55 00:05:27,307 --> 00:05:30,134 Were they scientific, artistic or both? 56 00:05:30,994 --> 00:05:32,712 We want to see what you've done!