Stars, Galaxies, Superuniverses and the Urantia Book, by Frederick
... Given this number of galaxies and the total number of stars in the master universe, one can calculate that the average number of stars per galaxy is 4.4 x 1021 stars divided by 1.0 x 1011 galaxies or 4.4 x 1010 stars per galaxy (44 billion). The number of stars in our Milky Way galaxy is estimated t ...
... Given this number of galaxies and the total number of stars in the master universe, one can calculate that the average number of stars per galaxy is 4.4 x 1021 stars divided by 1.0 x 1011 galaxies or 4.4 x 1010 stars per galaxy (44 billion). The number of stars in our Milky Way galaxy is estimated t ...
Local Group Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mario L Mateo
... Galaxy. Various indirect indicators suggest that our Galaxy can be classified as an Sbc galaxy, intermediate between the properties described for M31 and M33. Some recent studies at radio, infrared and optical wavelengths also suggest that our Galaxy contains an elongated central bar composed of old ...
... Galaxy. Various indirect indicators suggest that our Galaxy can be classified as an Sbc galaxy, intermediate between the properties described for M31 and M33. Some recent studies at radio, infrared and optical wavelengths also suggest that our Galaxy contains an elongated central bar composed of old ...
A Spectroscopically Confirmed Excess of 24 micron Sources in a
... understanding the interplay between galaxy evolution and environment is to study galaxy groups because: 1) most galaxies in the local universe are in groups (e.g. Geller & Huchra 1983); and 2) hierarchical structure formation predicts that galaxy clusters assemble from the merger and accretion of sm ...
... understanding the interplay between galaxy evolution and environment is to study galaxy groups because: 1) most galaxies in the local universe are in groups (e.g. Geller & Huchra 1983); and 2) hierarchical structure formation predicts that galaxy clusters assemble from the merger and accretion of sm ...
Globular Clusters as Fossils of Galaxy Formation
... 1979; Larson 1988, 1992a). The surviving clusters would then have a peaked luminosity function even if cluster formation processes in the Galactic halo had initially produced objects with a mass function increasing monotonically toward smaller masses, like the mass function of the open clusters. Mor ...
... 1979; Larson 1988, 1992a). The surviving clusters would then have a peaked luminosity function even if cluster formation processes in the Galactic halo had initially produced objects with a mass function increasing monotonically toward smaller masses, like the mass function of the open clusters. Mor ...
Exploring Neutral Hydrogen and Galaxy Evolution with the SKA
... of the massive, H I -rich systems that will likely dominate the next-generation H I surveys with the SKA and its pathfinder telescopes. Taking advantage of the upgraded Westerbork receiver system, a Blind, Ultra-Deep H I Environmental Survey (BUDHIES) has been carried out to image two cosmic volumes ...
... of the massive, H I -rich systems that will likely dominate the next-generation H I surveys with the SKA and its pathfinder telescopes. Taking advantage of the upgraded Westerbork receiver system, a Blind, Ultra-Deep H I Environmental Survey (BUDHIES) has been carried out to image two cosmic volumes ...
Astronomical Picture of the Day
... The Orion Nebula (a) is a giant cloud of gas and dust in which new stars and planets are forming. It is located about 1,500 light-years from Earth, which means the light recorded in the photograph took about 1,500 years to reach us. Thus, we see it as it was about 1,500 years ago. Photograph (b) sho ...
... The Orion Nebula (a) is a giant cloud of gas and dust in which new stars and planets are forming. It is located about 1,500 light-years from Earth, which means the light recorded in the photograph took about 1,500 years to reach us. Thus, we see it as it was about 1,500 years ago. Photograph (b) sho ...
Chapter 15.3 Galaxy Evolution
... • Angular momentum may determine size of disk • Density of protogalactic cloud may determine how fast a galaxy forms • Collisions shape galaxies early on – Mergers of small objects make halo & bulge – Mergers of larger objects make elliptical galaxies • Relatively undisturbed galaxies can stil ...
... • Angular momentum may determine size of disk • Density of protogalactic cloud may determine how fast a galaxy forms • Collisions shape galaxies early on – Mergers of small objects make halo & bulge – Mergers of larger objects make elliptical galaxies • Relatively undisturbed galaxies can stil ...
Next Generation VLA Science White Paper
... bulk tracers of interstellar gas — tools like the Hi or low-J CO lines. These lines will remain essential to understand where the gas is, but they reveal comparatively little about the conditions within the gas. Detailed spectroscopic work on small regions (e.g., galactic nuclei, Galactic cores) has ...
... bulk tracers of interstellar gas — tools like the Hi or low-J CO lines. These lines will remain essential to understand where the gas is, but they reveal comparatively little about the conditions within the gas. Detailed spectroscopic work on small regions (e.g., galactic nuclei, Galactic cores) has ...
On the Spiral Structure of the Milky Way Galaxy
... Data on other galaxies are known to demonstrate that HI superclouds, giant molecular clouds (GMCs) and young stars genetically related to them, and HII regions are located along spiral arms and often concentrated in giant star and gas complexes [5, 6]. The complexes in the spiral arms related to the ...
... Data on other galaxies are known to demonstrate that HI superclouds, giant molecular clouds (GMCs) and young stars genetically related to them, and HII regions are located along spiral arms and often concentrated in giant star and gas complexes [5, 6]. The complexes in the spiral arms related to the ...
AGN surveys to study galaxy evolution along cosmic times
... “The observed line intensities [....] in NGC1068 and 4151 closely resemble the line intensities of the planetary nebula NGC7027” and “The hydrogen lines in NGC4151 and 7469 are of unusual interest, being composed of relatively narrow cores (1100 km/sec wide) superposed on very wide wings (7500 km/se ...
... “The observed line intensities [....] in NGC1068 and 4151 closely resemble the line intensities of the planetary nebula NGC7027” and “The hydrogen lines in NGC4151 and 7469 are of unusual interest, being composed of relatively narrow cores (1100 km/sec wide) superposed on very wide wings (7500 km/se ...
Plotting the Rotation Curve of M31
... Measure the peak frequencies of the hydrogen spectra. Is this part of the galaxy approaching us or moving away from us? Answer: the spectra show higher frequencies than the rest value (1420.406 MHz) which indicates they are blueshifted and that they were taken from the approaching limb of M31. Your ...
... Measure the peak frequencies of the hydrogen spectra. Is this part of the galaxy approaching us or moving away from us? Answer: the spectra show higher frequencies than the rest value (1420.406 MHz) which indicates they are blueshifted and that they were taken from the approaching limb of M31. Your ...
1 Introduction - Wiley-VCH
... of galaxies. A typical example is illustrated in Figure 1.5 which shows the image of the interacting system M51 observed at different wavelengths, from the X-ray (Figure 1.5a) to the 21 cm HI radio line (Figure 1.5l). The distribution of the old stellar population, as traced by the near-infrared ima ...
... of galaxies. A typical example is illustrated in Figure 1.5 which shows the image of the interacting system M51 observed at different wavelengths, from the X-ray (Figure 1.5a) to the 21 cm HI radio line (Figure 1.5l). The distribution of the old stellar population, as traced by the near-infrared ima ...
The Milky Way disk
... mechanism, like for instance streaming motions. The same Oort formulae cannot be used outside the solar ring, and other independent distance indicators have to be adopted. Besides this, other limitations are that our galaxy is filled with HI, and apparently inter-arm regions have the same physical s ...
... mechanism, like for instance streaming motions. The same Oort formulae cannot be used outside the solar ring, and other independent distance indicators have to be adopted. Besides this, other limitations are that our galaxy is filled with HI, and apparently inter-arm regions have the same physical s ...
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.