The Milky Way - The Independent School
... Dark Matter Adding “visible” mass in: • stars, • interstellar gas, • dust, …etc., we find that most of the mass is “invisible”! • The nature of this “dark matter” is not understood at this time. • Some ideas: brown dwarfs, small black holes, exotic elementary particles. ...
... Dark Matter Adding “visible” mass in: • stars, • interstellar gas, • dust, …etc., we find that most of the mass is “invisible”! • The nature of this “dark matter” is not understood at this time. • Some ideas: brown dwarfs, small black holes, exotic elementary particles. ...
the Local Group - Simon P Driver
... some Local Group galaxies, roughly to the same physical scale: ...
... some Local Group galaxies, roughly to the same physical scale: ...
Modern Telescopes and Ancient Skies
... of Galaxies The spectra of galaxies are shifted to the red: galaxies are moving away from us. The farther away a galaxy is, the faster it ...
... of Galaxies The spectra of galaxies are shifted to the red: galaxies are moving away from us. The farther away a galaxy is, the faster it ...
Lecture notes 18: Galaxies and galaxy clusters
... http://www.seds.org/ spider/ngc/ngc.cgi?n2841) number 30%. The former are presumed to be caused by quasistatic density waves, while the latter are caused by stochastic, self-propagating star formation. Both processes are probably active in most spiral galaxies. Elliptical Galaxies In contradiction t ...
... http://www.seds.org/ spider/ngc/ngc.cgi?n2841) number 30%. The former are presumed to be caused by quasistatic density waves, while the latter are caused by stochastic, self-propagating star formation. Both processes are probably active in most spiral galaxies. Elliptical Galaxies In contradiction t ...
Chap 16: Galaxies
... Dark Matter Adding “visible” mass in: • stars, • interstellar gas, • dust, …etc., we find that most of the mass is “invisible”! • The nature of this “dark matter” is not understood at this time. • Some ideas: brown dwarfs, small black holes, exotic elementary particles. ...
... Dark Matter Adding “visible” mass in: • stars, • interstellar gas, • dust, …etc., we find that most of the mass is “invisible”! • The nature of this “dark matter” is not understood at this time. • Some ideas: brown dwarfs, small black holes, exotic elementary particles. ...
Peculiar (Interacting) Galaxies
... formation, due to collisions between gas clouds. In addition • Gas which loses enough angular momentum during the encounter will fall into the center. (This is especially true if a bar is formed.) This can lead to strong nuclear starbursts. § M82 is currently forming a few M¤/year of stars (simila ...
... formation, due to collisions between gas clouds. In addition • Gas which loses enough angular momentum during the encounter will fall into the center. (This is especially true if a bar is formed.) This can lead to strong nuclear starbursts. § M82 is currently forming a few M¤/year of stars (simila ...
Seminar I: Tidal dwarf galaxies
... globe. Through one of your many collaborations, you happen to come across some of these new data (see Table 1). This includes the Hα emission-line equivalent width, the Hα/Hβ emission-line ratio and the K band flux of this galaxy. It is now up to you to analyze this information in order to extract a ...
... globe. Through one of your many collaborations, you happen to come across some of these new data (see Table 1). This includes the Hα emission-line equivalent width, the Hα/Hβ emission-line ratio and the K band flux of this galaxy. It is now up to you to analyze this information in order to extract a ...
PH607lec09-3gal1
... • Few E galaxies actually have flat luminosity profiles at small radii; instead, the profiles rise inward to the last measured point . • Cores may exhibit unusual kinematics; for example, about a quarter of all elliptical galaxies have cores which appear to counter-rotate with respect to the rest of ...
... • Few E galaxies actually have flat luminosity profiles at small radii; instead, the profiles rise inward to the last measured point . • Cores may exhibit unusual kinematics; for example, about a quarter of all elliptical galaxies have cores which appear to counter-rotate with respect to the rest of ...
PH607lec10-3gal1
... In types SBa and later the bar often connects to a spiral pattern extending to larger radii (e.g. NGC 1300). Viewed face-on, bars typically appear to have axial ratios of 2. The surface brightness within the bar is often fairly constant. Some bars appear to be ‘squared off’ at the ends. The true 3- ...
... In types SBa and later the bar often connects to a spiral pattern extending to larger radii (e.g. NGC 1300). Viewed face-on, bars typically appear to have axial ratios of 2. The surface brightness within the bar is often fairly constant. Some bars appear to be ‘squared off’ at the ends. The true 3- ...
AST1001.ch15
... What can you conclude from the fact that quasars usually have very large redshifts? A. B. C. D. ...
... What can you conclude from the fact that quasars usually have very large redshifts? A. B. C. D. ...
AST1001.ch15
... What can you conclude from the fact that quasars usually have very large redshifts? A. B. C. D. ...
... What can you conclude from the fact that quasars usually have very large redshifts? A. B. C. D. ...
8and10Dec_2014
... matter did not really exist; rather, everything was radiation or energy. Cosmologists call this time period the early universe. • When energy is converted into matter, antimatter is formed as well. • For a proton-antiproton pair to form, the temperature must be more than 1013 K! • Matter and antimat ...
... matter did not really exist; rather, everything was radiation or energy. Cosmologists call this time period the early universe. • When energy is converted into matter, antimatter is formed as well. • For a proton-antiproton pair to form, the temperature must be more than 1013 K! • Matter and antimat ...
Active Galaxies
... •Gas which loses enough angular momentum falls into the galaxy center bar formation funnels more gas inward violent star formation near center of disk and further out ...
... •Gas which loses enough angular momentum falls into the galaxy center bar formation funnels more gas inward violent star formation near center of disk and further out ...
Galaxies
... Astronomers are finding more and more evidence to show that galaxies collide, interact, and merge. In fact, collisions among galaxies may dominate their evolution. Arp 148 is the staggering aftermath of an encounter between two galaxies, resulting in a ring-shaped galaxy and a long-tailed companion. ...
... Astronomers are finding more and more evidence to show that galaxies collide, interact, and merge. In fact, collisions among galaxies may dominate their evolution. Arp 148 is the staggering aftermath of an encounter between two galaxies, resulting in a ring-shaped galaxy and a long-tailed companion. ...
No Slide Title
... radio surveys but their visible image looked faint and star like and were called Quasi Stellar Radio Sources or Quasars for short. ...
... radio surveys but their visible image looked faint and star like and were called Quasi Stellar Radio Sources or Quasars for short. ...
Galaxies
... leftovers. He named them “irregulars.” • Irregular galaxies are galaxies that do not fit into any other class. • As their name suggests, their shape is irregular. • The gravity of large spiral galaxies may be distorting the shape of these galaxies. ...
... leftovers. He named them “irregulars.” • Irregular galaxies are galaxies that do not fit into any other class. • As their name suggests, their shape is irregular. • The gravity of large spiral galaxies may be distorting the shape of these galaxies. ...
Galaxy Morphology Classification - CS229
... validation (CV) are shown in table I. The best performing algorithm was the random forest with 67% accuracy. The random forest confusion matrix for a subsample of our data is shown in table II. A random forest is a classifier consisting of a collection of treestructured classifiers {h(x, Θk ), k = 1 ...
... validation (CV) are shown in table I. The best performing algorithm was the random forest with 67% accuracy. The random forest confusion matrix for a subsample of our data is shown in table II. A random forest is a classifier consisting of a collection of treestructured classifiers {h(x, Θk ), k = 1 ...
Dust Reprocessing In Astrophysics
... – Complex problem, need to explain how dust grains are produces and destroyed (Dwek 98, Morgan & Edmunds 2003). – The main ways in which dust grains can be produced are in the stellar outflow of stars such as AGBs and supernova and also by being built up in the ISM. – Processes which lead to their d ...
... – Complex problem, need to explain how dust grains are produces and destroyed (Dwek 98, Morgan & Edmunds 2003). – The main ways in which dust grains can be produced are in the stellar outflow of stars such as AGBs and supernova and also by being built up in the ISM. – Processes which lead to their d ...
Cosmic Castaways Scene Chart
... Galaxies do not exist alone. They are found in groups, held together by the same gravity that keeps their stars in orbit. Our Milky Way lies in a small galaxy group known as the Local Group, which contains a handful of large galaxies, and dozens of small galaxies. As galaxies move within galaxy grou ...
... Galaxies do not exist alone. They are found in groups, held together by the same gravity that keeps their stars in orbit. Our Milky Way lies in a small galaxy group known as the Local Group, which contains a handful of large galaxies, and dozens of small galaxies. As galaxies move within galaxy grou ...
The Big Bang
... • galaxies were much smaller than they are today (factors of 3 to 20 smaller) and almost all are badly disturbed/lumpy • there were far fewer galaxies in the universe than there are today, and the farther back you go (beyond 7 billion years), the fewer you find ...
... • galaxies were much smaller than they are today (factors of 3 to 20 smaller) and almost all are badly disturbed/lumpy • there were far fewer galaxies in the universe than there are today, and the farther back you go (beyond 7 billion years), the fewer you find ...
Introduction to Galaxies - West Jefferson Local Schools
... •Disk + spiral arms + bulge (usually) •Subtype a b c defined by 3 criteria: •Bulge/disk luminosity ratio •Sa: B/D>1 Sc: B/D<0.2 •Spiral pitch angle •Sa: tightly wound arms Sc: loosely wound arms •Degree of resolution into knots, HII regions, etc. ...
... •Disk + spiral arms + bulge (usually) •Subtype a b c defined by 3 criteria: •Bulge/disk luminosity ratio •Sa: B/D>1 Sc: B/D<0.2 •Spiral pitch angle •Sa: tightly wound arms Sc: loosely wound arms •Degree of resolution into knots, HII regions, etc. ...
talk
... • The disk-averaged Schmidt law in galaxies is rooted in a local relationship that persists to scales of <500 pc • In M51 the SF density is tightly coupled to the local H2 surface density, and not with HI density • A kinematic star formation law does not seem to extend as well to local scales • The ...
... • The disk-averaged Schmidt law in galaxies is rooted in a local relationship that persists to scales of <500 pc • In M51 the SF density is tightly coupled to the local H2 surface density, and not with HI density • A kinematic star formation law does not seem to extend as well to local scales • The ...
DOC - Cool Cosmos
... continually running out of fuel and dying. But in galaxies with enough raw material to make new stars, a young population of stars will replace the dying ones. However, if enough time passes and a galaxy converts all of its available gas into stars and then the stars die out, at that point the galax ...
... continually running out of fuel and dying. But in galaxies with enough raw material to make new stars, a young population of stars will replace the dying ones. However, if enough time passes and a galaxy converts all of its available gas into stars and then the stars die out, at that point the galax ...
Disk Galaxies in the Magneticum Pathfinder Simulations
... to properly resolve dwarf galaxies. Fig. 1 shows some typical disk galaxies formed in this simulation. 3.1. The Classification of Galaxies We successfully reproduce a population of disk as well as spheroidal galaxies due to the improvements in the numerical methods as well as the included prescripti ...
... to properly resolve dwarf galaxies. Fig. 1 shows some typical disk galaxies formed in this simulation. 3.1. The Classification of Galaxies We successfully reproduce a population of disk as well as spheroidal galaxies due to the improvements in the numerical methods as well as the included prescripti ...
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 ...
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).