![Galaxy5](http://s1.studyres.com/store/data/006138968_1-e20ce4ebe9370ed28ed48120392e61bb-300x300.png)
Galaxy5
... stars retained their orbits and made the halo of the Galaxy. • The gas collided and sunk to the center. The Milky Way was built up piece-meal in this fashion. • Today, galaxy interactions between the primary spiral galaxy and its satellites are much less frequent, because there are few satellites re ...
... stars retained their orbits and made the halo of the Galaxy. • The gas collided and sunk to the center. The Milky Way was built up piece-meal in this fashion. • Today, galaxy interactions between the primary spiral galaxy and its satellites are much less frequent, because there are few satellites re ...
Document
... contained) in the distant past was very high; ● the temperature falls as the universe expands and so does the temperature of the radiation in the universe; ...
... contained) in the distant past was very high; ● the temperature falls as the universe expands and so does the temperature of the radiation in the universe; ...
The Hubble Redshift Distance Relation
... that the Universe itself is expanding. At first glance, it may appear that since everything appears to be moving away from us, that we must be located at the center of the Universe, but this is not the case. As we will discover in this lab, we are not in some preferred location in our Universe. In t ...
... that the Universe itself is expanding. At first glance, it may appear that since everything appears to be moving away from us, that we must be located at the center of the Universe, but this is not the case. As we will discover in this lab, we are not in some preferred location in our Universe. In t ...
Chapter 18 Notes - Valdosta State University
... The Life Cycle of High-Mass Stars The birth of a high mass star occurs the same way as the birth of a low mass star. The difference is in the way they end their lives as stars. A high mass star can end its life as a supernova. A nova occurs when a nuclear explosion occurs on the surface of a white d ...
... The Life Cycle of High-Mass Stars The birth of a high mass star occurs the same way as the birth of a low mass star. The difference is in the way they end their lives as stars. A high mass star can end its life as a supernova. A nova occurs when a nuclear explosion occurs on the surface of a white d ...
Astro 13 Galaxies & Cosmology LECTURE 1 28 Mar 2001 D. Koo
... Lensed position 2) See its gravitational effects on nearby companion stars. Normal Star Black Hole Astronomers have found two handfuls of good candidates, but for many, we cannot exclude other “Dark” objects, such as neutron stars. ...
... Lensed position 2) See its gravitational effects on nearby companion stars. Normal Star Black Hole Astronomers have found two handfuls of good candidates, but for many, we cannot exclude other “Dark” objects, such as neutron stars. ...
Sizing Up The Universe
... motions of the stars into the future, we can see a convergence point in the sky where they are headed. The direction to this point tells us the ratio of the radial to the tangential velocities of the stars in the cluster. By measuring the radial velocities of the stars, we can figure out their tange ...
... motions of the stars into the future, we can see a convergence point in the sky where they are headed. The direction to this point tells us the ratio of the radial to the tangential velocities of the stars in the cluster. By measuring the radial velocities of the stars, we can figure out their tange ...
Chapter 19. Mapping the Universe from Herschel to Sloan
... stars. Galaxies were giant collections of stars, gas and dust and to understand how matter was distributed through space, we had to focus on their distribution. Since faint galaxies could be seen right to the limit of the largest telescopes, it became clear that the Universe was much larger than we ...
... stars. Galaxies were giant collections of stars, gas and dust and to understand how matter was distributed through space, we had to focus on their distribution. Since faint galaxies could be seen right to the limit of the largest telescopes, it became clear that the Universe was much larger than we ...
Galaxies
... In 1923 Edwin Hubble measured the brightness of a pulsating variable star in the Andromeda galaxy, M31. The rate at which the variable star pulsed was linked to its actual brightness so he could estimate how far away it was. He discovered it was way outside the Milky Way. He then applied these measu ...
... In 1923 Edwin Hubble measured the brightness of a pulsating variable star in the Andromeda galaxy, M31. The rate at which the variable star pulsed was linked to its actual brightness so he could estimate how far away it was. He discovered it was way outside the Milky Way. He then applied these measu ...
Lab 9
... How accurate were you? Is the criterion or criteria you used a good way to find galaxy distances? ...
... How accurate were you? Is the criterion or criteria you used a good way to find galaxy distances? ...
Earth_Universe04
... Accounts for galaxies moving away from us Universe was once confined to a "ball" that was • Supermassive • Dense • Hot ...
... Accounts for galaxies moving away from us Universe was once confined to a "ball" that was • Supermassive • Dense • Hot ...
file - University of California San Diego
... "So we want to know, how much helium is left in intergalactic space? In quasars? What was the primordial amount?" Looking at a quasar with a redshift of four, for instance, corresponds to looking back 10 billion years in time to the period shortly after the Big Bang. 3. The spectra of intermediate r ...
... "So we want to know, how much helium is left in intergalactic space? In quasars? What was the primordial amount?" Looking at a quasar with a redshift of four, for instance, corresponds to looking back 10 billion years in time to the period shortly after the Big Bang. 3. The spectra of intermediate r ...
E1 Introduction to the universe
... down a little bit but it is not strong enough to bring the expansion to a halt. A low density universe. A closed Universe is one that is brought to a stop and then collapses back on itself( "big crunch"). The force of gravity is enough to bring the expansion to an end. A high density universe. A fla ...
... down a little bit but it is not strong enough to bring the expansion to a halt. A low density universe. A closed Universe is one that is brought to a stop and then collapses back on itself( "big crunch"). The force of gravity is enough to bring the expansion to an end. A high density universe. A fla ...
Exercise 8
... How accurate were you? Is the criterion or criteria you used a good way to find galaxy distances? ...
... How accurate were you? Is the criterion or criteria you used a good way to find galaxy distances? ...
Extension worksheet – Topic 6 - Cambridge Resources for the IB
... the temperature of the star (obtained form its spectrum) and the stellar type so the HR can be used to find luminosity. ...
... the temperature of the star (obtained form its spectrum) and the stellar type so the HR can be used to find luminosity. ...
TF_final3 - Arecibo Observatory
... i in infrared. The TullyFisher relation states that the bigger the galaxy is, the faster it rotates. The faster the galaxy rotates, the wider is the emission line in velocity. Also, the bigger the galaxy, the more is its luminosity. TullyFisher relation shows that for normal galaxies, the velocity w ...
... i in infrared. The TullyFisher relation states that the bigger the galaxy is, the faster it rotates. The faster the galaxy rotates, the wider is the emission line in velocity. Also, the bigger the galaxy, the more is its luminosity. TullyFisher relation shows that for normal galaxies, the velocity w ...
Search For Dark Matters Essay Research Paper
... The way in which dark matter reveals its presence to us is through the gravitational effect it exerts on luminous matter in the universe. (\”Luminous\” matter is the matter we can see with our telescopes.) The most obvious example of the gravitational effects of dark matter can be observed when look ...
... The way in which dark matter reveals its presence to us is through the gravitational effect it exerts on luminous matter in the universe. (\”Luminous\” matter is the matter we can see with our telescopes.) The most obvious example of the gravitational effects of dark matter can be observed when look ...
Questions - Clever Teach
... supported the Big Bang theory. This should then be coupled with an understanding of the significance of another observation; cosmic microwave background radiation. Candidates were not asked to describe the Big Bang or Steady State theories in detail and many candidates devoted a large part of their ...
... supported the Big Bang theory. This should then be coupled with an understanding of the significance of another observation; cosmic microwave background radiation. Candidates were not asked to describe the Big Bang or Steady State theories in detail and many candidates devoted a large part of their ...
Electromagnetic Waves - Flipped Out Science with Mrs. Thomas!
... whether the object is moving towards the viewer or away from the viewer. If the object is moving towards the viewer, they are compressed into shorter wavelengths. If the object is moving away from the viewer, the waves are stretched out, making the wavelengths longer. In visible light, the light app ...
... whether the object is moving towards the viewer or away from the viewer. If the object is moving towards the viewer, they are compressed into shorter wavelengths. If the object is moving away from the viewer, the waves are stretched out, making the wavelengths longer. In visible light, the light app ...
High School Science Essential Curriculum - Astronomy
... Galaxies including elliptical galaxies, spiral galaxies, barred-spiral galaxies, and irregular galaxies. c. Discuss active galaxies that do not conform to the original Hubble Classification System, including radio galaxies, Seyfert galaxies, and quasars. UNIT VII: Cosmology Goal 1. ...
... Galaxies including elliptical galaxies, spiral galaxies, barred-spiral galaxies, and irregular galaxies. c. Discuss active galaxies that do not conform to the original Hubble Classification System, including radio galaxies, Seyfert galaxies, and quasars. UNIT VII: Cosmology Goal 1. ...
solution - Evergreen Archives
... We live in a "flat" universe with a decelerating rate of expansion. We live in an open universe with a constant rate of expansion given by Hubble’s law. We live in a "flat" universe with an accelerating rate of expansion. 28. The recently estimated density of radiation and matter in the universe (in ...
... We live in a "flat" universe with a decelerating rate of expansion. We live in an open universe with a constant rate of expansion given by Hubble’s law. We live in a "flat" universe with an accelerating rate of expansion. 28. The recently estimated density of radiation and matter in the universe (in ...
ppt
... few galaxies (1-2 Mpc). Even Hubble Space Telescope cannot find Cepheids beyond the Virgo cluster (16 Mpc). Beyond 1-2Mpc, Hubble used… ...
... few galaxies (1-2 Mpc). Even Hubble Space Telescope cannot find Cepheids beyond the Virgo cluster (16 Mpc). Beyond 1-2Mpc, Hubble used… ...
Chapter 27 Quasars, Active Galaxies, and Gamma
... • Early radio telescopes found radio emission from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like stars. ...
... • Early radio telescopes found radio emission from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like stars. ...
Description
... star formation and evolution, solar system formation and planetary motion, as well as the cosmological principles for predicting the future of our universe. The content materials will be introduced at a conceptual and qualitative level, although some algebraic mathematics will be applied. There is n ...
... star formation and evolution, solar system formation and planetary motion, as well as the cosmological principles for predicting the future of our universe. The content materials will be introduced at a conceptual and qualitative level, although some algebraic mathematics will be applied. There is n ...
Motion in the Sky & Getting to know the Sky
... About 30 galaxies in total, dominated by two large spiral galaxies (Milky Way and M31); remaining galaxies are “dwarf” galaxies. Local Group is about 2.5x106 ly = 2.5 Mly in diameter. Milky Way and M31 are approaching each other at a relative speed of about 300 km/s. ...
... About 30 galaxies in total, dominated by two large spiral galaxies (Milky Way and M31); remaining galaxies are “dwarf” galaxies. Local Group is about 2.5x106 ly = 2.5 Mly in diameter. Milky Way and M31 are approaching each other at a relative speed of about 300 km/s. ...
Olbers` Paradox - NMSU Astronomy
... stars were too far away to be seen individually the collective flux of light from all the stars would cause the night sky to glow. The first person to realise this was Johannes Kepler, who with brilliant intuition noted that the relative darkness of the night sky is of huge cosmological significanc ...
... stars were too far away to be seen individually the collective flux of light from all the stars would cause the night sky to glow. The first person to realise this was Johannes Kepler, who with brilliant intuition noted that the relative darkness of the night sky is of huge cosmological significanc ...
Observable universe
![](https://commons.wikimedia.org/wiki/Special:FilePath/Observable_Universe_with_Measurements_01.png?width=300)
The observable universe consists of the galaxies and other matter that can, in principle, be observed from Earth at the present time because light and other signals from these objects has had time to reach the Earth since the beginning of the cosmological expansion. Assuming the universe is isotropic, the distance to the edge of the observable universe is roughly the same in every direction. That is, the observable universe is a spherical volume (a ball) centered on the observer. Every location in the Universe has its own observable universe, which may or may not overlap with the one centered on Earth.The word observable used in this sense does not depend on whether modern technology actually permits detection of radiation from an object in this region (or indeed on whether there is any radiation to detect). It simply indicates that it is possible in principle for light or other signals from the object to reach an observer on Earth. In practice, we can see light only from as far back as the time of photon decoupling in the recombination epoch. That is when particles were first able to emit photons that were not quickly re-absorbed by other particles. Before then, the Universe was filled with a plasma that was opaque to photons.The surface of last scattering is the collection of points in space at the exact distance that photons from the time of photon decoupling just reach us today. These are the photons we detect today as cosmic microwave background radiation (CMBR). However, with future technology, it may be possible to observe the still older relic neutrino background, or even more distant events via gravitational waves (which also should move at the speed of light). Sometimes astrophysicists distinguish between the visible universe, which includes only signals emitted since recombination—and the observable universe, which includes signals since the beginning of the cosmological expansion (the Big Bang in traditional cosmology, the end of the inflationary epoch in modern cosmology). According to calculations, the comoving distance (current proper distance) to particles from the CMBR, which represent the radius of the visible universe, is about 14.0 billion parsecs (about 45.7 billion light years), while the comoving distance to the edge of the observable universe is about 14.3 billion parsecs (about 46.6 billion light years), about 2% larger.The best estimate of the age of the universe as of 2015 is 7010137990000000000♠13.799±0.021 billion years but due to the expansion of space humans are observing objects that were originally much closer but are now considerably farther away (as defined in terms of cosmological proper distance, which is equal to the comoving distance at the present time) than a static 13.8 billion light-years distance. It is estimated that the diameter of the observable universe is about 28 gigaparsecs (91 billion light-years, 8.8×1026 metres or 5.5×1023 miles), putting the edge of the observable universe at about 46–47 billion light-years away.