Elliptical galaxies
... •If the isophotes are not circularly symmetric, then the galaxy cannot be spherically symmetric, but it can still be axisymmetric. •In general the line of sight will be inclined at an angle with respect to the equatorial plane of an axisymmetric galaxy. •In that case, there are infinite de-projected ...
... •If the isophotes are not circularly symmetric, then the galaxy cannot be spherically symmetric, but it can still be axisymmetric. •In general the line of sight will be inclined at an angle with respect to the equatorial plane of an axisymmetric galaxy. •In that case, there are infinite de-projected ...
Introduction to Galaxies - West Jefferson Local Schools
... At the beginning of the 20th century, what we now call spiral galaxies were referred to as “spiral nebulae” and most astronomers believed them to be clouds of gas and stars associated with our own Milky Way. Edwin P. Hubble (1889-1953) ...
... At the beginning of the 20th century, what we now call spiral galaxies were referred to as “spiral nebulae” and most astronomers believed them to be clouds of gas and stars associated with our own Milky Way. Edwin P. Hubble (1889-1953) ...
normal and active - FirstLight Astro
... 1. What’s the difference between rich galaxy clusters and the poor ones? 2. What is the name of our local group of galaxies? 3. What major phenomenon is probably responsible for the shapes and sizes of galaxies? 4. What is galactic cannibalism? 5. What type of galaxy often results when one galaxy pa ...
... 1. What’s the difference between rich galaxy clusters and the poor ones? 2. What is the name of our local group of galaxies? 3. What major phenomenon is probably responsible for the shapes and sizes of galaxies? 4. What is galactic cannibalism? 5. What type of galaxy often results when one galaxy pa ...
the Local Group - Simon P Driver
... large distances, so don’t make up part of the total galaxy count for the Local Group • about half of known galaxies are in groups and clusters – these are dense enough to halt cosmological expansion locally, and so the galaxies remain bound to each other • the other half of galaxies are loosely s ...
... large distances, so don’t make up part of the total galaxy count for the Local Group • about half of known galaxies are in groups and clusters – these are dense enough to halt cosmological expansion locally, and so the galaxies remain bound to each other • the other half of galaxies are loosely s ...
The First Stars in the Universe
... universe of 13.7 billion years). Researchers will need better telescopes to see more distant objects dating from still earlier times. Cosmologists, however, can make deductions about the early universe based on the cosmic microwave background radiation, which was emitted about 400,000 years after th ...
... universe of 13.7 billion years). Researchers will need better telescopes to see more distant objects dating from still earlier times. Cosmologists, however, can make deductions about the early universe based on the cosmic microwave background radiation, which was emitted about 400,000 years after th ...
The Milky Way By
... Appearance from Earth • All the stars that the eye can distinguish in the night sky are part of the Milky Way Galaxy, but aside from these relatively nearby stars, the galaxy appears as a hazy band of white light arching around the entire celestial sphere. ...
... Appearance from Earth • All the stars that the eye can distinguish in the night sky are part of the Milky Way Galaxy, but aside from these relatively nearby stars, the galaxy appears as a hazy band of white light arching around the entire celestial sphere. ...
The Submillimeter Frontier: A Space Science Imperative
... • z ∼ 1000 – The decoupling of radiation from matter allows baryonic matter to cluster around the dark matter. The universe becomes transparent, leaving behind the microwave background radiation observed by COBE. We know the statistics of the density field at this time, and believe that a linear the ...
... • z ∼ 1000 – The decoupling of radiation from matter allows baryonic matter to cluster around the dark matter. The universe becomes transparent, leaving behind the microwave background radiation observed by COBE. We know the statistics of the density field at this time, and believe that a linear the ...
My Favorite Universe
... rotation has the effect of Àattening the system. This general Àattening is also seen in galaxies. In the Milky Way, for example, some stars reveal the skeleton of the sphere that originally existed, but the galaxy has Àattened out. Earth, too, is slightly bigger at the equator than at the poles, bec ...
... rotation has the effect of Àattening the system. This general Àattening is also seen in galaxies. In the Milky Way, for example, some stars reveal the skeleton of the sphere that originally existed, but the galaxy has Àattened out. Earth, too, is slightly bigger at the equator than at the poles, bec ...
Set 2: Nature of Galaxies
... • History: as late as the early 1920’s it was not known that the “spiral nebula” were galaxies like ours • Debate between Shapley (galactic objects) and Curtis (extragalactic, or galaxies) in 1920 highlighted the difficulties distances in astrophysics difficult to measure - Shapley’s inferences base ...
... • History: as late as the early 1920’s it was not known that the “spiral nebula” were galaxies like ours • Debate between Shapley (galactic objects) and Curtis (extragalactic, or galaxies) in 1920 highlighted the difficulties distances in astrophysics difficult to measure - Shapley’s inferences base ...
Galaxies have different sizes and shapes.
... The disk of the Milky Way measures The Milky Way is about 100,000 light-years in diameter. more than 100,000 light-years in diameter. The bulge of densely packed stars at the center is located about 26,000 light-years from the Sun. A large but very faint layer of stars surrounds the disk and bulge. ...
... The disk of the Milky Way measures The Milky Way is about 100,000 light-years in diameter. more than 100,000 light-years in diameter. The bulge of densely packed stars at the center is located about 26,000 light-years from the Sun. A large but very faint layer of stars surrounds the disk and bulge. ...
Supermassive Black Holes and the Growth of Galaxies
... Despite this exciting progress, theoretical models have still faced some fundamental problems. Of these, perhaps the most troubling is the near-universal prediction that massive galaxies should be able to continually accrete new gas that cools and falls from the cosmic web into their large dark matt ...
... Despite this exciting progress, theoretical models have still faced some fundamental problems. Of these, perhaps the most troubling is the near-universal prediction that massive galaxies should be able to continually accrete new gas that cools and falls from the cosmic web into their large dark matt ...
Quiz 2 Lecture 12
... a. Ring galaxies can be produced by head-on collisions between galaxies. b. The ratio of the number of elliptical to spiral galaxies remains constant over time. c. The Magellanic Clouds may eventually be "cannibalized" by our Galaxy. d. The shape of a galaxy can be influenced by collision with anoth ...
... a. Ring galaxies can be produced by head-on collisions between galaxies. b. The ratio of the number of elliptical to spiral galaxies remains constant over time. c. The Magellanic Clouds may eventually be "cannibalized" by our Galaxy. d. The shape of a galaxy can be influenced by collision with anoth ...
Chapter 26: Stars, Galaxies, and the Universe Stars
... Stars are made mostly of hydrogen and helium. These are both very lightweight gases. However, there is so much hydrogen and helium in a star that the weight of these gases is enormous. In the center of a star, the pressure is great enough to heat the gases and cause nuclear fusion reactions. In a nu ...
... Stars are made mostly of hydrogen and helium. These are both very lightweight gases. However, there is so much hydrogen and helium in a star that the weight of these gases is enormous. In the center of a star, the pressure is great enough to heat the gases and cause nuclear fusion reactions. In a nu ...
Lecture notes 18: Galaxies and galaxy clusters
... Gravitational lenses and dark matter. Galactic cluster dynamics show that there is a great amount of dark matter: there is not enough luminous matter, even when considering the very hot intergalactic gas clouds, to bind galaxies together. Another method of assessing the mass of galaxy clusters is by ...
... Gravitational lenses and dark matter. Galactic cluster dynamics show that there is a great amount of dark matter: there is not enough luminous matter, even when considering the very hot intergalactic gas clouds, to bind galaxies together. Another method of assessing the mass of galaxy clusters is by ...
Here
... Ripples and shells have also been detected in S0 and Sa galaxies. Since in early-type galaxies they are detected because of the smooth profile of the underlying galaxy, it is not clear whether this is an universal phenomenon also present in later-type galaxies but difficult to detect there. ...
... Ripples and shells have also been detected in S0 and Sa galaxies. Since in early-type galaxies they are detected because of the smooth profile of the underlying galaxy, it is not clear whether this is an universal phenomenon also present in later-type galaxies but difficult to detect there. ...
Chap 16: Galaxies
... light years away. Why are we able to see Andromeda galaxy (M31) which is about 2.54 million light years away without aid when the night sky is clear? A: Surely we can’t see a star which is 2.54 million light years from us, but obviously Andromeda galaxy itself isn’t a star but is made up of a great ...
... light years away. Why are we able to see Andromeda galaxy (M31) which is about 2.54 million light years away without aid when the night sky is clear? A: Surely we can’t see a star which is 2.54 million light years from us, but obviously Andromeda galaxy itself isn’t a star but is made up of a great ...
1 Introduction - Wiley-VCH
... The contribution of these multifrequency surveys to the study of galaxy evolution is invaluable, since it simultaneously provides us with information on the different components of any extragalactic object (see Table 1.1 for a summary). The modern instrumentation now in our hands enables us to measu ...
... The contribution of these multifrequency surveys to the study of galaxy evolution is invaluable, since it simultaneously provides us with information on the different components of any extragalactic object (see Table 1.1 for a summary). The modern instrumentation now in our hands enables us to measu ...
Lecture 16
... – Our best models for galaxy formation assume that gravity made galaxies out of regions of the early universe that were slightly denser than their surroundings. The gas collapsed to form galaxies. Galaxies continue to cannibalize smaller galaxies and draw in gas as the evolve. What determines the m ...
... – Our best models for galaxy formation assume that gravity made galaxies out of regions of the early universe that were slightly denser than their surroundings. The gas collapsed to form galaxies. Galaxies continue to cannibalize smaller galaxies and draw in gas as the evolve. What determines the m ...
pompton lakes high school - Pompton Lakes School District
... Lab: Spectroscopes – What is the rainbow? How electromagnetic types of do the spectra of different gases compare with the radiation are: Gamma electromagnetic Sun’s spectrum? rays, X-rays, radiation? How Ultraviolet light, are they related to visible light, Infrared one another? How light, Micro wav ...
... Lab: Spectroscopes – What is the rainbow? How electromagnetic types of do the spectra of different gases compare with the radiation are: Gamma electromagnetic Sun’s spectrum? rays, X-rays, radiation? How Ultraviolet light, are they related to visible light, Infrared one another? How light, Micro wav ...
pompton lakes high school - Pompton Lakes School District
... Lab: Spectroscopes – What is the rainbow? How electromagnetic types of do the spectra of different gases compare with the radiation are: Gamma electromagnetic Sun’s spectrum? rays, X-rays, radiation? How Ultraviolet light, are they related to visible light, Infrared one another? How light, Micro wav ...
... Lab: Spectroscopes – What is the rainbow? How electromagnetic types of do the spectra of different gases compare with the radiation are: Gamma electromagnetic Sun’s spectrum? rays, X-rays, radiation? How Ultraviolet light, are they related to visible light, Infrared one another? How light, Micro wav ...
DTU 8e Chap 17 Quasars and Other Active Galaxies
... speed of 5% of the speed of light. According to the Hubble law, Cygnus A is therefore 635 million light-years from Earth. Because Cygnus A is one of the brightest radio sources in the sky, this remote galaxy’s energy output must be enormous. (b) An X-ray image of Cygnus A taken by the Chandra X-ray ...
... speed of 5% of the speed of light. According to the Hubble law, Cygnus A is therefore 635 million light-years from Earth. Because Cygnus A is one of the brightest radio sources in the sky, this remote galaxy’s energy output must be enormous. (b) An X-ray image of Cygnus A taken by the Chandra X-ray ...
Curriculum Vitae - Centre for Astrophysics and Supercomputing
... September 2008 – MPA Cosmology Seminar, Max-Planck-Institute for Astrophysics, Germany November 2007 – Seminar at the Center for Astrophysics of the University of Porto, Portugal ...
... September 2008 – MPA Cosmology Seminar, Max-Planck-Institute for Astrophysics, Germany November 2007 – Seminar at the Center for Astrophysics of the University of Porto, Portugal ...
SIMULATIONS
... Comparison to observations of local galaxy samples are encouraging, particularly remarkable for PAH features Detailed analysis of parameter space from literature gives consistent results ...
... Comparison to observations of local galaxy samples are encouraging, particularly remarkable for PAH features Detailed analysis of parameter space from literature gives consistent results ...
Spectroscopy Applications - Astrophysics and
... Moving one step closer to finding the fingerprints of life in a habitable planet beyond the solar system, astronomers have for the first time detected carbon dioxide in the atmosphere of a planet that orbits a star other than the sun Fall 2008 ...
... Moving one step closer to finding the fingerprints of life in a habitable planet beyond the solar system, astronomers have for the first time detected carbon dioxide in the atmosphere of a planet that orbits a star other than the sun Fall 2008 ...
Observable universe
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.