3.1 Radio Astronomy Research Results For much of PY 2010, radio
... An AGES objective is to investigate the number of low mass gas rich dwarf galaxies that reside around isolated galaxies and within galaxy groups, as hierarchical models of galaxy formation predict hundreds of dwarf companions for each giant galaxy. AGES typically finds only one or two new dwarf gala ...
... An AGES objective is to investigate the number of low mass gas rich dwarf galaxies that reside around isolated galaxies and within galaxy groups, as hierarchical models of galaxy formation predict hundreds of dwarf companions for each giant galaxy. AGES typically finds only one or two new dwarf gala ...
2011-GravLens
... Gravitational lenses can be used as gravitational telescopes. The concentrated light from objects seen behind gravitational lenses makes very faint objects appear brighter, larger and therefore more easily studied. One of the most distant object in the universe was discovered by the gravitational le ...
... Gravitational lenses can be used as gravitational telescopes. The concentrated light from objects seen behind gravitational lenses makes very faint objects appear brighter, larger and therefore more easily studied. One of the most distant object in the universe was discovered by the gravitational le ...
Molecular Gas in Galactic Environments Abstracts (Poster)
... that the Galactic diffuse ISM captured on the lines-of-sights are illuminated by ultraviolet radiation from distant massive stars. Molecular absorption studies should be more powerful in unveiling the chemistry in extragalactic sources. Secondly, we have detected various kinds of molecular emission ...
... that the Galactic diffuse ISM captured on the lines-of-sights are illuminated by ultraviolet radiation from distant massive stars. Molecular absorption studies should be more powerful in unveiling the chemistry in extragalactic sources. Secondly, we have detected various kinds of molecular emission ...
50 Annual ! th
... internet articles on light and optics, to tormenting my older brother and parents with theories and questions, my thirst for knowledge had no bounds. Naturally, my curiosity led me to pursue a degree in physics. But I soon came to learn that although lectures and tutorials are necessary, the secrets ...
... internet articles on light and optics, to tormenting my older brother and parents with theories and questions, my thirst for knowledge had no bounds. Naturally, my curiosity led me to pursue a degree in physics. But I soon came to learn that although lectures and tutorials are necessary, the secrets ...
Clusters as laboratories for the study of galaxy evolution
... “Clusters…are laboratories for the study of galaxy evolution and may become as useful as star clusters are in the study of stellar evolution” -- Dressler, 1984 Annual Reviews Back in 1984, (and still?) the prevalent view was that clusters were themselves agents that influenced the evolution of gala ...
... “Clusters…are laboratories for the study of galaxy evolution and may become as useful as star clusters are in the study of stellar evolution” -- Dressler, 1984 Annual Reviews Back in 1984, (and still?) the prevalent view was that clusters were themselves agents that influenced the evolution of gala ...
Super-solar Metal Abundances in Two Galaxies at ζ ∼ 3.57
... We report on the surprisingly high metallicity measured in two absorption systems at high redshift, detected in the Very Large Telescope spectrum of the afterglow of the gamma-ray burst GRB 090323. The two systems, at redshift z = 3.5673 and z = 3.5774 (separation ∆v ≈ 660 km s−1 ), are dominated by ...
... We report on the surprisingly high metallicity measured in two absorption systems at high redshift, detected in the Very Large Telescope spectrum of the afterglow of the gamma-ray burst GRB 090323. The two systems, at redshift z = 3.5673 and z = 3.5774 (separation ∆v ≈ 660 km s−1 ), are dominated by ...
Local Group Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mario L Mateo
... our own. These nearby systems also provide our clearest views of how galaxies interact with one another in the relatively small volume of space of the Local Group. The brightest members of the Local Group are so close to us that on a clear, dark night away from city lights it is possible to see them ...
... our own. These nearby systems also provide our clearest views of how galaxies interact with one another in the relatively small volume of space of the Local Group. The brightest members of the Local Group are so close to us that on a clear, dark night away from city lights it is possible to see them ...
The Cosmos & the Bible
... • Most cosmologists are working with varieties of this today, at least to the extent that our universe is finite in size and began with the big bang. • Many are apparently hoping that our universe is just a subset of an infinite, eternal universe, of which ours is just a transient bubble, but it is ...
... • Most cosmologists are working with varieties of this today, at least to the extent that our universe is finite in size and began with the big bang. • Many are apparently hoping that our universe is just a subset of an infinite, eternal universe, of which ours is just a transient bubble, but it is ...
PH607lec08
... • The dust lanes seen in E galaxies imply that the absorbing material is distributed in rings or disks. Dust lanes may be aligned with either the major or minor axes, or they may be warped. • E galaxies contain modest amounts of cool and warm gas, although not as much as is found in S galaxies. A fe ...
... • The dust lanes seen in E galaxies imply that the absorbing material is distributed in rings or disks. Dust lanes may be aligned with either the major or minor axes, or they may be warped. • E galaxies contain modest amounts of cool and warm gas, although not as much as is found in S galaxies. A fe ...
in search of antimatter in the universe
... constituent particles are at high energies, higher than the ionisation energy (energy required to remove an electron) of Positronium. This means that even if a positron and electron are close enough to form Positronium, they will not bind together4. On the other hand, if a jet were to collide with a ...
... constituent particles are at high energies, higher than the ionisation energy (energy required to remove an electron) of Positronium. This means that even if a positron and electron are close enough to form Positronium, they will not bind together4. On the other hand, if a jet were to collide with a ...
Extragalactic Distances from Planetary Nebulae
... stars. But they do have large numbers of 1 M stars. If some are in close binary systems which coalesce on the main sequence, the product may evolve into an [O III]-bright planetary. The ratio of bright planetaries to blue stragglers is about equal to the ratio of the objects’ lifetimes. Carrera et ...
... stars. But they do have large numbers of 1 M stars. If some are in close binary systems which coalesce on the main sequence, the product may evolve into an [O III]-bright planetary. The ratio of bright planetaries to blue stragglers is about equal to the ratio of the objects’ lifetimes. Carrera et ...
Module 11.1.1: Galaxies: Morphology and the Hubble Sequence
... doesn't have a lot of active star formation. And just like other spiral galaxies, these S0's, or lenticulars, because their shape resembles a lens, could also contain bars. [slide 10] Among the ...
... doesn't have a lot of active star formation. And just like other spiral galaxies, these S0's, or lenticulars, because their shape resembles a lens, could also contain bars. [slide 10] Among the ...
A Zoo of Galaxies - Cambridge University Press
... the first example of such a map based on actual astronomical data. By 1900 astronomers understood quite a lot more about the basic structure of our galaxy. The map made by Cornelius Easton in 1900 (Fig 3) was the first to show our galaxy as having spiral structures (Trimble 1995). Easton used pictures ...
... the first example of such a map based on actual astronomical data. By 1900 astronomers understood quite a lot more about the basic structure of our galaxy. The map made by Cornelius Easton in 1900 (Fig 3) was the first to show our galaxy as having spiral structures (Trimble 1995). Easton used pictures ...
mg_colloq - University of Massachusetts Amherst
... Residuals consistent with NORMAL surface density of intervening sources ...
... Residuals consistent with NORMAL surface density of intervening sources ...
File
... Two major theories about the origin of the Universe are the Big Bang and the Steady State theories. Some evidence supports both theories. Other evidence supports only one theory. By considering the evidence, discuss why one of these theories is preferred by most scientists. ...
... Two major theories about the origin of the Universe are the Big Bang and the Steady State theories. Some evidence supports both theories. Other evidence supports only one theory. By considering the evidence, discuss why one of these theories is preferred by most scientists. ...
Starburst Galaxies - Beck-Shop
... smaller regions each a few tens of light years across (∼10 pc) that have luminosities up to 100 million times that of the Sun. The energy emitted by the massive stars in these regions dominates the emission from the whole galaxy (Box 2.1) especially for the most energetic galaxies. Thirdly, the rate ...
... smaller regions each a few tens of light years across (∼10 pc) that have luminosities up to 100 million times that of the Sun. The energy emitted by the massive stars in these regions dominates the emission from the whole galaxy (Box 2.1) especially for the most energetic galaxies. Thirdly, the rate ...
The National Centre for Radio Astrophysics
... energies reach maximum, during the free-expansion phase or during the Sedov stage? How do cosmic rays escape from a SNR, what is the dynamics of escape, i.e. how the maximum energy evolves with time? What is the primary particle population producing the gamma-ray emission? The first two questions ar ...
... energies reach maximum, during the free-expansion phase or during the Sedov stage? How do cosmic rays escape from a SNR, what is the dynamics of escape, i.e. how the maximum energy evolves with time? What is the primary particle population producing the gamma-ray emission? The first two questions ar ...
A Map of the Universe
... picture, at a scale of 1/108 , shows the entire Earth. The 14th picture, at a scale of 1/1014 , shows the entire Solar system. The 18th picture, at a scale of 1/1018 , includes α Centauri, The 22nd picture, at a scale of 1/1022 shows all of the Milky Way Galaxy. The 26th and last picture in the sequ ...
... picture, at a scale of 1/108 , shows the entire Earth. The 14th picture, at a scale of 1/1014 , shows the entire Solar system. The 18th picture, at a scale of 1/1018 , includes α Centauri, The 22nd picture, at a scale of 1/1022 shows all of the Milky Way Galaxy. The 26th and last picture in the sequ ...
bars and secular evolution
... that SB(s) galaxies have weaker bars. Observational indication that bar is actually stronger for the SB(s) galaxies Examples of galaxies that might have slow, medium and fast pattern speeds (give various numbers and locations of resonances) slow pattern speed <=> nuclear rings, medium pattern speed ...
... that SB(s) galaxies have weaker bars. Observational indication that bar is actually stronger for the SB(s) galaxies Examples of galaxies that might have slow, medium and fast pattern speeds (give various numbers and locations of resonances) slow pattern speed <=> nuclear rings, medium pattern speed ...
AR2013 - Vatican Observatory
... already-existing stellar databases and archived data available, such as from HST, SDSS, Spitzer, GALEX, Kepler, and soon-to-be available GAIA data (just to name a few) with future observational projects with telescopes (such as VATT). Asteroseismology: The Kepler and CoRot missions have provided a ...
... already-existing stellar databases and archived data available, such as from HST, SDSS, Spitzer, GALEX, Kepler, and soon-to-be available GAIA data (just to name a few) with future observational projects with telescopes (such as VATT). Asteroseismology: The Kepler and CoRot missions have provided a ...
Emission from dust in galaxies: Metallicity dependence
... region (Osterbrock 1989). Thus, during the resonant scatterings in an H ii region, all the Lyα photons are assumed to be absorbed by grains in IHK00, which this paper is based on. If the dust-to-gas ratio is significantly smaller than the Galactic value, the dust grains might not efficiently absorb ...
... region (Osterbrock 1989). Thus, during the resonant scatterings in an H ii region, all the Lyα photons are assumed to be absorbed by grains in IHK00, which this paper is based on. If the dust-to-gas ratio is significantly smaller than the Galactic value, the dust grains might not efficiently absorb ...
Next Generation VLA Science White Paper
... previous capabilities and it is a stunning tool to study dust emission, excited gas, and active regions. Though still revolutionary at ν ∼ 70–115 GHz, ALMA in its current (nearly final) form would still require ∼ 15 hours to produce a 100 CO map of a nearby galaxy (σ = 0.2 K, ∆v = 5 km s−1 ). To wor ...
... previous capabilities and it is a stunning tool to study dust emission, excited gas, and active regions. Though still revolutionary at ν ∼ 70–115 GHz, ALMA in its current (nearly final) form would still require ∼ 15 hours to produce a 100 CO map of a nearby galaxy (σ = 0.2 K, ∆v = 5 km s−1 ). To wor ...