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... 15. Galaxies Swan Leavitt’s Study of Cepheid Variables Leads to Measurement of Galactic Distances ...
... 15. Galaxies Swan Leavitt’s Study of Cepheid Variables Leads to Measurement of Galactic Distances ...
Galaxy Images - Institute of Physics
... which the galaxies reside (in the constellation Fornax), is just one-tenth the diameter of the full Moon (about the size of a grain of sand held at arms length) and is largely empty as seen with the naked eye. This is a "deep" core sample of the universe, cutting across billions of lightyears. The s ...
... which the galaxies reside (in the constellation Fornax), is just one-tenth the diameter of the full Moon (about the size of a grain of sand held at arms length) and is largely empty as seen with the naked eye. This is a "deep" core sample of the universe, cutting across billions of lightyears. The s ...
galaxy worksheet
... 1. The stars in an open cluster are young stars that all formed from the same __________. 2. Every star you can see from Earth with the unaided eye is part of the __________ Galaxy. 3. Our own galaxy is the type of galaxy called a(n) __________ galaxy. 4. The major galaxy closest to our own is the _ ...
... 1. The stars in an open cluster are young stars that all formed from the same __________. 2. Every star you can see from Earth with the unaided eye is part of the __________ Galaxy. 3. Our own galaxy is the type of galaxy called a(n) __________ galaxy. 4. The major galaxy closest to our own is the _ ...
PH607 – Galaxies
... stars and globular clusters. While the disk contains gas and dust obscuring the view in some wavelengths, the halo does not. Active star formation takes place in the disk (especially in the spiral arms, which represent areas of high density), but not in the halo. Open clusters also occur primarily i ...
... stars and globular clusters. While the disk contains gas and dust obscuring the view in some wavelengths, the halo does not. Active star formation takes place in the disk (especially in the spiral arms, which represent areas of high density), but not in the halo. Open clusters also occur primarily i ...
19 The Milky Way Galaxy
... 2. Observe objects at radio and infrared wavelengths to circumvent the problem of optical obscuration, and catalog their directions and distances. 3. Trace the orbital velocities of objects in different directions relative to our position. ...
... 2. Observe objects at radio and infrared wavelengths to circumvent the problem of optical obscuration, and catalog their directions and distances. 3. Trace the orbital velocities of objects in different directions relative to our position. ...
Galaxies Galaxies M81
... nucleus. Spirals are classified according to how tightly or loosely wound the arms are, and it turns out that the brightness of the central nucleus is correlated to the tightness of the arm. The galaxies M 104 (below) and M 51 (right) respectively show tightly and loosely wounds. Notice the effects ...
... nucleus. Spirals are classified according to how tightly or loosely wound the arms are, and it turns out that the brightness of the central nucleus is correlated to the tightness of the arm. The galaxies M 104 (below) and M 51 (right) respectively show tightly and loosely wounds. Notice the effects ...
charts_set_9
... Small fraction may be brown dwarfs, dead white dwarfs. Most likely it's a dark halo surrounding the Milky Way. ...
... Small fraction may be brown dwarfs, dead white dwarfs. Most likely it's a dark halo surrounding the Milky Way. ...
Unit 1
... fuzzy and diffuse, due to the vast separation between the Sun and the observed galaxy, as well as the separation between the stars of that galaxy! – The paleness of visible light from distant galaxies is called the surface brightness. ...
... fuzzy and diffuse, due to the vast separation between the Sun and the observed galaxy, as well as the separation between the stars of that galaxy! – The paleness of visible light from distant galaxies is called the surface brightness. ...
Integrative Studies 410 Our Place in the Universe
... distance ladder out as far as we can see Cepheids – about 50 million ly • In 1920 Hubble used this technique to measure the distance to Andromeda (about 2 million ly) • Works best for periodic variables ...
... distance ladder out as far as we can see Cepheids – about 50 million ly • In 1920 Hubble used this technique to measure the distance to Andromeda (about 2 million ly) • Works best for periodic variables ...
Chapter 31 Galaxies & the Universe
... The Shape of the Milky Way Astronomers have determined the shape of the Milky Way by using radio waves because they penetrate the interstellar gas and dust without being scattered or absorbed. ...
... The Shape of the Milky Way Astronomers have determined the shape of the Milky Way by using radio waves because they penetrate the interstellar gas and dust without being scattered or absorbed. ...
young science communicator`s competition
... and it seems that Shapley was right, the galaxy is indeed much bigger than expected and in fact, the sun is not at the centre of the galaxy, we seem to live quite far from it. [There is a stunned silence] SHAPLEY: So it seems we were both right. CURTIS: And both wrong. [The crowd cheers and sound f ...
... and it seems that Shapley was right, the galaxy is indeed much bigger than expected and in fact, the sun is not at the centre of the galaxy, we seem to live quite far from it. [There is a stunned silence] SHAPLEY: So it seems we were both right. CURTIS: And both wrong. [The crowd cheers and sound f ...
Our Galaxy, The Milky Way
... Pop. II: old stars in the bulge, halo, and globular clusters – Today, we distinguish between the old, metal-rich stars in the bulge, and old, metal-poor stars in the halo – Not clear whether the Pop. I is homogeneous: young thin disk, vs. intermediate-age thick disk ...
... Pop. II: old stars in the bulge, halo, and globular clusters – Today, we distinguish between the old, metal-rich stars in the bulge, and old, metal-poor stars in the halo – Not clear whether the Pop. I is homogeneous: young thin disk, vs. intermediate-age thick disk ...
Galaxy5
... • Today the mergers are less frequent and usually not as much material. But when they happen they can produce AGN. • When the material is all accreted by the black hole, the nucleus becomes normal once again. ...
... • Today the mergers are less frequent and usually not as much material. But when they happen they can produce AGN. • When the material is all accreted by the black hole, the nucleus becomes normal once again. ...
Galaxies - senwiki
... that nothing, not even light, can escape. -Why? Black holes have extremely strong gravitational pulls. They can pull in stars and accumulate the mass of the stars. -Where are black holes located? Astronomers believe that each galaxy contains at least one supermassive black hole at its centre. ...
... that nothing, not even light, can escape. -Why? Black holes have extremely strong gravitational pulls. They can pull in stars and accumulate the mass of the stars. -Where are black holes located? Astronomers believe that each galaxy contains at least one supermassive black hole at its centre. ...
Chapter 12 Quiz, Nov. 28, 2012, Astro 162, Section 4 12-1
... The O and B stars formed in the spiral arms explode as supernovae before they emerge from the arms. Therefore, these stars are not found between the arms of spiral galaxies. 12-33. Describe the Sun’s motion through our Galaxy. About how long is one orbit? An elliptical orbit, with the Sun oscillatin ...
... The O and B stars formed in the spiral arms explode as supernovae before they emerge from the arms. Therefore, these stars are not found between the arms of spiral galaxies. 12-33. Describe the Sun’s motion through our Galaxy. About how long is one orbit? An elliptical orbit, with the Sun oscillatin ...
Hubble`s Classification of Galaxies (PDF version)
... Hubble now set out to derive distances to as many of the nebulae (now called ‘galaxies’) as he could. (He did this using Cepheids where possible, but also by other means.) He noted that the nebulae do not all look the same. What sorts of galaxies exist? Can they be classified in some useful way? Wha ...
... Hubble now set out to derive distances to as many of the nebulae (now called ‘galaxies’) as he could. (He did this using Cepheids where possible, but also by other means.) He noted that the nebulae do not all look the same. What sorts of galaxies exist? Can they be classified in some useful way? Wha ...
Universe ppt - Killeen ISD
... Spectrograph – breaks the light from an object into colors and photographs the resulting spectrum; this allows astronomers to identify the chemical composition and temperature of a star; each element has a unique set of lines on a spectrum ...
... Spectrograph – breaks the light from an object into colors and photographs the resulting spectrum; this allows astronomers to identify the chemical composition and temperature of a star; each element has a unique set of lines on a spectrum ...
Milky Way thin disk
... Since bars are dynamical states of a disk, we do not need a separate stellar population for the bulge; the bar is part of the inner disk Many galactic astronomers still say ‘bulge’ which is confusing ...
... Since bars are dynamical states of a disk, we do not need a separate stellar population for the bulge; the bar is part of the inner disk Many galactic astronomers still say ‘bulge’ which is confusing ...
Andromeda Galaxy
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The Andromeda Galaxy (/ænˈdrɒmɨdə/), also known as Messier 31, M31, or NGC 224, is a spiral galaxy approximately 780 kiloparsecs (2.5 million light-years) from Earth. It is the nearest major galaxy to the Milky Way and was often referred to as the Great Andromeda Nebula in older texts. It received its name from the area of the sky in which it appears, the constellation of Andromeda, which was named after the mythological princess Andromeda. Being approximately 220,000 light years across, it is the largest galaxy of the Local Group, which also contains the Milky Way, the Triangulum Galaxy, and about 44 other smaller galaxies.The Andromeda Galaxy is the most massive galaxy in the Local Group as well. Despite earlier findings that suggested that the Milky Way contains more dark matter and could be the most massive in the grouping, the 2006 observations by the Spitzer Space Telescope revealed that Andromeda contains one trillion (1012) stars: at least twice the number of stars in the Milky Way, which is estimated to be 200–400 billion.The Andromeda Galaxy is estimated to be 1.5×1012 solar masses, while the mass of the Milky Way is estimated to be 8.5×1011 solar masses. In comparison, a 2009 study estimated that the Milky Way and M31 are about equal in mass, while a 2006 study put the mass of the Milky Way at ~80% of the mass of the Andromeda Galaxy. The Milky Way and Andromeda are expected to collide in 3.75 billion years, eventually merging to form a giant elliptical galaxy or perhaps a large disk galaxy.At 3.4, the apparent magnitude of the Andromeda Galaxy is one of the brightest of any of the Messier objects, making it visible to the naked eye on moonless nights even when viewed from areas with moderate light pollution. Although it appears more than six times as wide as the full Moon when photographed through a larger telescope, only the brighter central region is visible to the naked eye or when viewed using binoculars or a small telescope and would it hence appear to be but another star.