M104: The Sombrero Galaxy
... This photogenic galaxy looks like a broad-brimmed Mexican hat floating in space. Appropriately called the Sombrero Galaxy, its catalogue name is Messier 104 (M104). Thick dust lanes make up the brim of the galaxy. The brim winds into the brilliant white crown, made up of a central bulge of older sta ...
... This photogenic galaxy looks like a broad-brimmed Mexican hat floating in space. Appropriately called the Sombrero Galaxy, its catalogue name is Messier 104 (M104). Thick dust lanes make up the brim of the galaxy. The brim winds into the brilliant white crown, made up of a central bulge of older sta ...
Dwarf Galaxies
... Tidal Dwarfs: •! Dwarf galaxies can form from the debris torn from more massive galaxies during interactions & mergers •! Do not contain dark matter •! May have high metallicities ...
... Tidal Dwarfs: •! Dwarf galaxies can form from the debris torn from more massive galaxies during interactions & mergers •! Do not contain dark matter •! May have high metallicities ...
Lecture 3 - University of Washington
... for grand design spirals. • The spiral arms are overdense regions which move around at a different speed than star: stars thus move in and out of the spiral arm • How these density waves are set up is unclear, but it may have to do with interactions. Once they are set up, they must last for a long e ...
... for grand design spirals. • The spiral arms are overdense regions which move around at a different speed than star: stars thus move in and out of the spiral arm • How these density waves are set up is unclear, but it may have to do with interactions. Once they are set up, they must last for a long e ...
ppt - UCL
... This image shows UV emission from the active nucleus of NGC 7469 (z=0.016317; bottom right), and also from inner spiral arms. These extend up to about 15’’ from the nucleus, and fainter arms can be observed further out at about 30’’. We also see (top left) UV emission from the non-interacting compan ...
... This image shows UV emission from the active nucleus of NGC 7469 (z=0.016317; bottom right), and also from inner spiral arms. These extend up to about 15’’ from the nucleus, and fainter arms can be observed further out at about 30’’. We also see (top left) UV emission from the non-interacting compan ...
Stars, Galaxies and Nebulae
... Star – the Sun Galaxy – Milky Way Galaxy Cluster – The Local Group ...
... Star – the Sun Galaxy – Milky Way Galaxy Cluster – The Local Group ...
PH607lec12-5gal3
... of gas Bar patterns are not static, they rotate with a pattern speed, but unlike spiral arms they are not density waves. Stars in the bar stay in the bar. The bar rotates as a unit in a rigidly rotating disk. The asymmetric gravitational forces of a disk allow gas to lose angular momentum (via shock ...
... of gas Bar patterns are not static, they rotate with a pattern speed, but unlike spiral arms they are not density waves. Stars in the bar stay in the bar. The bar rotates as a unit in a rigidly rotating disk. The asymmetric gravitational forces of a disk allow gas to lose angular momentum (via shock ...
Populations of Galaxies and their Formation at z < 7
... undergoing mergers. The transition from mergers to normal Hubble types occurs at about z~1.5. Calculations show that this picture is consistent with LBGs forming into modern Hubble types. 4. The source(s) of reionization are still unknown. The onset of galaxy formation is also not known with certain ...
... undergoing mergers. The transition from mergers to normal Hubble types occurs at about z~1.5. Calculations show that this picture is consistent with LBGs forming into modern Hubble types. 4. The source(s) of reionization are still unknown. The onset of galaxy formation is also not known with certain ...
PH607lec11-4gal2
... of gas Bar patterns are not static, they rotate with a pattern speed, but unlike spiral arms they are not density waves. Stars in the bar stay in the bar. The bar rotates as a unit in a rigidly rotating disk. The asymmetric gravitational forces of a disk allow gas to lose angular momentum (via shock ...
... of gas Bar patterns are not static, they rotate with a pattern speed, but unlike spiral arms they are not density waves. Stars in the bar stay in the bar. The bar rotates as a unit in a rigidly rotating disk. The asymmetric gravitational forces of a disk allow gas to lose angular momentum (via shock ...
Universe Power Point
... Universe began with a tremendous explosion. 13.7 billion years ago, all matter was compressed into one spot and expanded rapidly. They are still expanding today. ...
... Universe began with a tremendous explosion. 13.7 billion years ago, all matter was compressed into one spot and expanded rapidly. They are still expanding today. ...
24.1 Hubble`s Galaxy Classification
... Elliptical galaxies have no spiral arms and no disk. They come in many sizes, from giant ellipticals of trillions of stars, down to dwarf ellipticals of less than a million stars. Ellipticals also contain very little, if any, cool gas and dust, and they show no evidence of ongoing star formation. Ma ...
... Elliptical galaxies have no spiral arms and no disk. They come in many sizes, from giant ellipticals of trillions of stars, down to dwarf ellipticals of less than a million stars. Ellipticals also contain very little, if any, cool gas and dust, and they show no evidence of ongoing star formation. Ma ...
Velocity Field in the Local Volume
... The deviations from the pure Hubble expansion can be expected due to gravitational action of nearby groups, as well as by Virgocentric and Great Attractor flows. We used simple spherically symmetric model to estimate influence of nearby groups on kinematic of the Local Volume. This method allows us ...
... The deviations from the pure Hubble expansion can be expected due to gravitational action of nearby groups, as well as by Virgocentric and Great Attractor flows. We used simple spherically symmetric model to estimate influence of nearby groups on kinematic of the Local Volume. This method allows us ...
Galaxies
... The discrepancy is even larger in galaxy clusters, which need 10 to 100 times more mass. The total needed is more than the sum of the dark matter associated with each galaxy. ...
... The discrepancy is even larger in galaxy clusters, which need 10 to 100 times more mass. The total needed is more than the sum of the dark matter associated with each galaxy. ...
Christian Marinoni
... geometry and energy content of the Universe Clusters relatively simple objects. Evolution of massive cluster abundance determined by gravity. ...
... geometry and energy content of the Universe Clusters relatively simple objects. Evolution of massive cluster abundance determined by gravity. ...
Student Reading
... An irregular galaxy is neither a spiral nor an elliptical. Irregular galaxies tend to be smaller objects without definite shape, and they typically have very hot newer stars mixed in with lots of gas and dust. These galaxies often have active regions of star formation. Sometimes their irregular shap ...
... An irregular galaxy is neither a spiral nor an elliptical. Irregular galaxies tend to be smaller objects without definite shape, and they typically have very hot newer stars mixed in with lots of gas and dust. These galaxies often have active regions of star formation. Sometimes their irregular shap ...
PH607lec10-4gal2
... of gas Bar patterns are not static, they rotate with a pattern speed, but unlike spiral arms they are not density waves. Stars in the bar stay in the bar. The bar rotates as a unit in a rigidly rotating disk. The asymmetric gravitational forces of a disk allow gas to lose angular momentum (via shock ...
... of gas Bar patterns are not static, they rotate with a pattern speed, but unlike spiral arms they are not density waves. Stars in the bar stay in the bar. The bar rotates as a unit in a rigidly rotating disk. The asymmetric gravitational forces of a disk allow gas to lose angular momentum (via shock ...
9 Dwarf Galaxies
... of gas Bar patterns are not static, they rotate with a pattern speed, but unlike spiral arms they are not density waves. Stars in the bar stay in the bar. The bar rotates as a unit in a rigidly rotating disk. The asymmetric gravitational forces of a disk allow gas to lose angular momentum (via shock ...
... of gas Bar patterns are not static, they rotate with a pattern speed, but unlike spiral arms they are not density waves. Stars in the bar stay in the bar. The bar rotates as a unit in a rigidly rotating disk. The asymmetric gravitational forces of a disk allow gas to lose angular momentum (via shock ...
Early Star-Forming Galaxies
... stars cannot be seen in visible light because they are buried inside dense clouds of molecular hydrogen that are laced with dust. Previous observations by ground-based telescopes made at submillimeter wavelengths found only a few massive galaxies within the epoch of interest. Researchers calculated ...
... stars cannot be seen in visible light because they are buried inside dense clouds of molecular hydrogen that are laced with dust. Previous observations by ground-based telescopes made at submillimeter wavelengths found only a few massive galaxies within the epoch of interest. Researchers calculated ...
Clusters
... it is currently thought that the very large amounts of expected cooling are in reality much smaller, as there is little evidence for cool X-ray emitting gas in many of these systems = the cooling flow problem theories for why there is little evidence of cooling include ◦ heating by the central AGN p ...
... it is currently thought that the very large amounts of expected cooling are in reality much smaller, as there is little evidence for cool X-ray emitting gas in many of these systems = the cooling flow problem theories for why there is little evidence of cooling include ◦ heating by the central AGN p ...
Galaxy interactions - collisions Many stars are thrown out into space
... Galaxy evolution in color and luminosity This is NOT an HR diagram – we are not plotting individual stars, but whole galaxies Galaxies can go from “blue cloud” to “red sequence” by undergoing collisions, or through “gas stripping” ...
... Galaxy evolution in color and luminosity This is NOT an HR diagram – we are not plotting individual stars, but whole galaxies Galaxies can go from “blue cloud” to “red sequence” by undergoing collisions, or through “gas stripping” ...
normal and active - FirstLight Astro
... 1. Which galaxy type varies the most in size? 2. Which can be enormously bigger than our galaxy? 3. Which make up the tiniest group overall? 4. What “stuff” is making the whole process of knowing galactic properties more difficult? ...
... 1. Which galaxy type varies the most in size? 2. Which can be enormously bigger than our galaxy? 3. Which make up the tiniest group overall? 4. What “stuff” is making the whole process of knowing galactic properties more difficult? ...
- Lorentz Center
... (effectively passively evolving) m < m*+1.5 Additional k-correction for non-red sequence galaxies as a function of observed color Final distribution is close to stellar-mass limited ...
... (effectively passively evolving) m < m*+1.5 Additional k-correction for non-red sequence galaxies as a function of observed color Final distribution is close to stellar-mass limited ...
Lecture 10
... radiation: relativistic electrons spiraling in B-field • QSO model + unification scheme for Quasars, Blazars, and Radio galaxies • QSOs in the Universe: z > 0.3 => common in early Universe then died out ...
... radiation: relativistic electrons spiraling in B-field • QSO model + unification scheme for Quasars, Blazars, and Radio galaxies • QSOs in the Universe: z > 0.3 => common in early Universe then died out ...
Astronomy Library wk 8.cwk (WP)
... However, there are scientific rationale for the HDF as well: With such a deep exposure one can see very distant galaxies. Examining such galaxies allows us to, in essence, look backwards in time. In fact, they are so far away we can see back a significant fraction of the way to the beginning of the ...
... However, there are scientific rationale for the HDF as well: With such a deep exposure one can see very distant galaxies. Examining such galaxies allows us to, in essence, look backwards in time. In fact, they are so far away we can see back a significant fraction of the way to the beginning of the ...
Atlas of Peculiar Galaxies
The Atlas of Peculiar Galaxies is a catalog of peculiar galaxies produced by Halton Arp. A total of 338 galaxies are presented in the atlas, which was originally published in 1966 by the California Institute of Technology.The primary goal of the catalog was to present photographs of examples of the different kinds of peculiar structures found among nearby galaxies. Arp realized that the reason why galaxies formed into spiral or elliptical shapes was not well understood. He perceived peculiar galaxies as small ""experiments"" that astronomers could use to understand the physical processes that distort spiral or elliptical galaxies. With this atlas, astronomers had a sample of peculiar galaxies that they could study in more detail. The atlas does not present a complete overview of every peculiar galaxy in the sky but instead provides examples of the different phenomena as observed in nearby galaxies.Because little was known at the time of publication about the physical processes that caused the different shapes, the galaxies in the atlas are sorted based on their appearance. Objects 1–101 are individual peculiar spiral galaxies or spiral galaxies that apparently have small companions. Objects 102–145 are elliptical and elliptical-like galaxies. Individual or groups of galaxies with neither elliptical nor spiral shapes are listed as objects 146–268. Objects 269–327 are double galaxies. Finally, objects that simply do not fit into any of the above categories are listed as objects 332–338. Most objects are best known by their other designations, but a few galaxies are best known by their Arp numbers (such as Arp 220).Today, the physical processes that lead to the peculiarities seen in the Arp atlas are now well understood. A large number of the objects are interacting galaxies, including M51 (Arp 85), Arp 220, and the Antennae Galaxies (NGC 4038/NGC 4039, or Arp 244). A few of the galaxies are simply dwarf galaxies that do not have enough mass to produce enough gravity to allow the galaxies to form any cohesive structure. NGC 1569 (Arp 210) is an example of one of the dwarf galaxies in the atlas. A few other galaxies are radio galaxies. These objects contain active galactic nuclei that produce powerful jets of gas called radio jets. The atlas includes the nearby radio galaxies M87 (Arp 152) and Centaurus A (Arp 153).