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Here is a drawing of a very large universe as seen from earth, which is at the center of the circle, and the circle represents our “telescopic sphere of visibility”, the radius of which increases every time we build a new larger telescope. Of course, we see no end to the universe and no outer “edge”. Note that we would see galaxies moving away from us in any direction we look, and observers on the other nearby galaxies would see basically the same thing. (Disregard the square sides to my drawing of part of the overall universe.): http://i32.tinypic.com/20z4lnc.jpg So, we are in the center of our "sphere of visibility", but that's about all we know so far. Here is what we should see if we were out near an outer “edge” of a spherical universe. We would see fewer distant galaxies in one direction of our telescopic viewing, much like we see fewer stars in our own galaxy, when we look in the direction away from the center of our own galaxy. If we could ever see a sudden absence of very distant galaxies in one direction of view, but plenty of galaxies in all other directions, then that could indicate that we are close to an outer “edge” of a spherical universe. http://i29.tinypic.com/2inviu.jpg Our problem has always been that we can’t see far enough into our universe to be able to tell if it has an “outer edge” or not. Edited to add: And this poor fellow of the 16th Century is in the same situation we are still in.... wanting to look beyond and outside our limited sphere of visibiltiy. http://i29.tinypic.com/24q93bs.jpg |
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What is thought to be causing this limited sphere of visibility? Is it that we don't yet have powerful enough telescopes to pick up the fainter light signatures? A time constraint? Also, how do we know that the universe is 46 billion LY in radius if we can only see 13.7 billion years?
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The limit of our sphere of visibility is strictly due to the limits of the sizes of our present telescopes. For example, Galileo’s first telescope couldn’t see very deep into space and even nearby galaxies were dim and tiny. Newton’s reflector was better but it was still a small telescope. Later 50-inch telescopes were invented that could see further and deeper, then the 100 inch telescope, the 200 inch, then Hubble. And our earth’s own atmosphere blurs images of tiny objects such as distant galaxies. That’s why Hubble was put up above the atmosphere. But it was limited in size too because of the limited size of the Space Shuttle that carried it into space. New plans are in the works to build bigger space telescopes that have several mirror parts that can be carried by the Shuttle, and then opened up into a much wider compound-mirror telescope for deeper field viewing. Also, long exposure times are needed to register images of the most faint and distant galaxies. The last deep-field Hubble photos of galaxies required many days of exposure time, and a lot of technical coordination is required to aim the telescope in the same direction for many days as it continues to move as it orbits the earth. |
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That, I don't know. I think the radius is calculated by complex math formulas.
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ETA: Sorry, misread that. But kinda touched on the answer.. Sam5 did too. The expansion rate of the Universe (Wiki for Hubble) is how we determine the size, even though we can only see a smaller percentage of the Universe visibly. |
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(VCM = very common misunderstanding, in case you were wondering.)
__________________
Chris Hillman Read these PF posts. Avoid Wikipedia--- except for these versions. Read this and this suggested sticky. When asked for advice, I always say: never take advice! Last edited by Chris Hillman; 17-July-2008 at 06:02 AM. Reason: moo! |
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I had typed up two replies to that and ended up closing the page out twice ![]() Those are nice easy reading with simple descriptions. |
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