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light_fills_the_universe.html
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light_fills_the_universe.html
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<!DOCTYPE html>
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<meta name="description" content="The site is intended as a free educational resource about the frontiers of galaxy formation." />
<meta name="keywords" content="background radiation, first light, early universe, cosmic dawn, first galaxies, first stars, population 3, cosmology" />
<meta name="author" content="Erika Hoffman" />
<title>Light Fills the Universe - Cosmic Dark to Cosmic Dawn</title>
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<a href="index.html"><h1 class="main-header">Cosmic Dark to Cosmic Dawn</h1></a>
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<li><a href="dark_ages.html">What happened during the <span class="bold">Dark Ages?</span></a></li>
<li class="current"><a href="cosmic_dawn_1.html">How did the <span class="bold">first stars</span> form?</a></li>
<li><a href="cosmic_dawn_2.html">How did the <span class="bold">first galaxies</span> form?</a></li>
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<a href="cosmic_dawn_1.html" class="cd_1_head">Era of the First Stars</a>
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<a href="first_black_holes.html" class="cd_1_cont">The First Black Holes</a>
<a href="light_fills_the_universe.html" class="cd_1_cont">Light Fills the Universe</a>
<a href="spin_flip.html" class="cd_1_cont">The Spin-Flip Backgound</a>
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<div class="page_title">LIGHT FILLS <br />THE UNIVERSE</div>
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Although the first stars formed in isolated gas clouds, the light they produced during their short lifetimes penetrated far into the Universe, affecting both the gas between the galaxies and other gas clumps attempting to form stars. In particular, ultraviolet radiation from these stars prevented primordial gas clouds from forming new stars: as the first stars formed, their radiation slowed down the formation of future generations. Meanwhile, X-rays from these stars' black hole remnants were absorbed by the hydrogen gas. The enormous energies of these X-rays heated the intergalactic gas, slowing down the formation of new clouds.
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<div class="img_cred">
A modern example of a star affecting other stars, but instead of just radiation, with an actual wave of gas.
<br />Image Credit: <a href="https://www.nasa.gov/mission_pages/spitzer/multimedia/pia16604.html" target="_blank" rel="noopener noreferrer">NASA/JPL-Caltech</a>
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<a href="first_black_holes.html">Previous: The First Black Holes </a>
<a href="spin_flip.html" style="float: right;">Next: The Spin-Flip Background </a>
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<h1>How does ultraviolet light affect the formation of the first stars?</h1>
<p>
Unlike clouds in the Milky Way, the first star-forming clouds were composed entirely of hydrogen and helium. In order to form stars, these clouds needed to condense to very high densities, which required them to cool to very low temperatures. In this kind of gas, such cooling could only happen after the formation of <i>molecular hydrogen</i> – two hydrogen atoms latched together. However, such molecules can be destroyed by ultraviolet light – which was likely produced in copious amounts by the very massive first stars.
</p>
<p class="img_cred_body">
Image: A cluster of newborn stars in NGC 7129, an <i>interstellar</i> (between stars) molecular cloud, picture obtained with the NASA Spitzer Space Telescope.
<br />Credit:<a href="https://images.nasa.gov/details-PIA05266" target="_blank" rel="noopener noreferrer">NASA/JPL/Caltech/Harvard-Smithsonian CfA</a>
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<h1>How do X-rays affect the temperature of the intergalactic gas?</h1>
<p>
X-rays are <i>photons</i> – particles of light – with extremely high energies. Because they are so energetic, they can travel through large swathes of the Universe before being fully absorbed by matter. But, as they travel, they collide with matter particles. An X-ray transfers some of its energy to the matter during each of these collisions, which then heats the gas. Without this process, the <i>intergalactic</i> gas - gas between galaxies - is very cold at early times, so even a small background is enough to change the gas temperature significantly.
</p>
<p class="img_cred_body">
Image: Galaxy cluster Abell 2125 as seen by the Chandra X-Ray Observatory, with several massive multimillion degree Celsius gas clouds.
<br />Credit: <a href="https://images.nasa.gov/details-0401555" target="_blank" rel="noopener noreferrer">MSFC</a>
</p>
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<div class="in_text_image_left_5" style="background-image:url('images/UV_buildup_snapshot.png');"></div>
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<h1>How do "radiation backgrounds" of ultraviolet light and X-rays build up over time?</h1>
<p>
Because the first stars were so massive, they were also extremely hot, which in turn made them powerful ultraviolet sources. As these stars formed, they flooded the Universe with ultraviolet light, building up a background that subsequent generations of stars had to overcome. Meanwhile, when these stars died (and perhaps through other processes as well), black holes formed. If these black holes encountered clouds of gas, their strong gravity would suck the clouds in – but not before the clouds underwent intense heating, allowing them to produce X-rays. Because the X-rays could travel so far through the Universe, an X-ray background likely built up early in the Universe’s history.
</p>
<p class="img_cred_body">
Image: A computer simulation of the heating of the Universe by X-rays. Orange regions are near black holes emitting X-rays, where heating is strong, while blue regions remain cold.
<br />Credit: <a href="http://homepage.sns.it/mesinger/DexM___21cmFAST.html" target="_blank" rel="noopener noreferrer">Andrei Mesinger</a>
</p>
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<div class="in_text_image_right_7" style="background-image: url('images/tadpole.jpg'); background-size:140%;"></div>
<div class="text_left_7" style="">
<h1>How do these radiation backgrounds affect the growth of stars and galaxies?</h1>
<p>
As the first generations of stars form, ultraviolet light builds up in the Universe – making it more difficult for later stars to form! If the background were absent, star formation would proceed very rapidly, as more and more star-forming clouds formed. But the background slows this process down, because so many of the clouds are unable to cool in the presence of the ultraviolet light. Meanwhile, if black holes form and grow at this early time, an X-ray background also builds up. This heats the Universe, which makes it harder for clouds to form as well. Of course, we have not yet observed this era, so the strength of these <i>feedback</i> processes are currently unknown. The ultraviolet and X-ray backgrounds are in fact key targets of forthcoming observations, because they would tell us the overall rate at which stars and black holes form during the Cosmic Dawn.
</p>
<p class="img_cred_body">
Image: IRAS 20324+4057, aka "the Tadpole," is gas and dust surrounding multiple protostars, and the intense blue glow is caused by nearby stars' ultraviolet radiation, which also sculpts its tail into a long, wiggly shape.
<br />Credit: <a href="https://images.nasa.gov/details-PIA18168" target="_blank" rel="noopener noreferrer"> NASA/JPL-Caltech/ESA, the Hubble Heritage Team STScI/AURA and IPHAS</a>
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<h1>Which telescopes are trying to observe this?</h1>
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<div class="tiny_text">The James Webb Space Telescope</div>
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<div class="tiny_text">The Hydrogen Epoch of Reionization Array (HERA)</div>
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<div class="telescope_title"><h3><a href="radio_telescopes.html">Radio Telescopes</a></h3></div>
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<p>Although these ultraviolet and X-ray backgrounds are crucial for understanding the earliest generations of galaxies, they are extraordinarily faint by the time they reach us today. Fortunately, they can be detected indirectly through the <a href="spin_flip.html"> 21-cm line.</a></p>
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<h2><a href="glossary.html">Vocab</a></h2>
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<li>Ultraviolet </li>
<li>X-ray </li>
<li>Primordial Gas </li>
<li>Intergalactic</li>
<li>Hydrogen Gas </li>
<li>Milky Way </li>
<li>Black Hole </li>
<li>Interstellar (Medium)</li>
<li>Feedback</li>
<li>Galaxy Cluster</li>
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<a href="first_black_holes.html">Previous: The First Black Holes </a>
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<li><a href=""></a> </li> There currently is not much information on the web about this, but when we find more resources we will add them here!
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<div class="mission"><span class="bold">Our Mission:</span> <br />The site is intended as a free educational resource about the frontiers of galaxy formation.</div>
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<span class="bold">Creation and Funding:</span>
<br />Content and supervision by Professor Steven Furlanetto, website design by Erika Hoffman, funding and support from NASA NESS, NSF, & UCLA Physics and Astronomy.
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