A Zoo of Galaxies - Portsmouth Research Portal
... fraction of the numbers of normal spirals” (at least in the photographic plates he used). In between the spirals and ellipticals was the (then hypothetical) S0, or lenticular type, which shows a disc, but no spiral arms. The small number of galaxies Hubble found not fitting this scheme were called “ ...
... fraction of the numbers of normal spirals” (at least in the photographic plates he used). In between the spirals and ellipticals was the (then hypothetical) S0, or lenticular type, which shows a disc, but no spiral arms. The small number of galaxies Hubble found not fitting this scheme were called “ ...
How different was the Universe at z=1?
... luminosity evolution since z=1. This study thus rules out the possibility that SB evolution of discs is caused by a significant size evolution. ...
... luminosity evolution since z=1. This study thus rules out the possibility that SB evolution of discs is caused by a significant size evolution. ...
The Thickness of Stellar Disks in Early
... that it is difficult to estimate other properties of the disk structure in this case, since all the material that is located in the equatorial plane is integrated along the line of sight. In early studies of the surface-brightness distributions in the optical (BV RI) in eight S0–Sd galaxies viewed edg ...
... that it is difficult to estimate other properties of the disk structure in this case, since all the material that is located in the equatorial plane is integrated along the line of sight. In early studies of the surface-brightness distributions in the optical (BV RI) in eight S0–Sd galaxies viewed edg ...
Gravitational Waves from Massive Black
... • Prior to reionization, cooling of gas inside darkmatter halos is limited by the gas cooling thresh-hold (104K for H). ...
... • Prior to reionization, cooling of gas inside darkmatter halos is limited by the gas cooling thresh-hold (104K for H). ...
Die Sonne im Röntgenlicht
... • Diffuse X-ray-emitting gas is strongly concentrated toward galactic disks and bulges (< 20 kpc). • Heating is mostly due to SNe. But the bulk of their energy is not detected in X-ray near galactic bulges/disks and is probably propagated into the halos. • Feedback from a galactic bulge likely plays ...
... • Diffuse X-ray-emitting gas is strongly concentrated toward galactic disks and bulges (< 20 kpc). • Heating is mostly due to SNe. But the bulk of their energy is not detected in X-ray near galactic bulges/disks and is probably propagated into the halos. • Feedback from a galactic bulge likely plays ...
The Mystery of the Giant Galactic Blobs
... Dokkum et al 2004) suggests that major star formation ceases in these massive systems very early in their assembly ...
... Dokkum et al 2004) suggests that major star formation ceases in these massive systems very early in their assembly ...
Chapter 15 Normal and Active Galaxies
... Milky Way, Andromeda, and M33. These and their satellites – about 45 galaxies in all – form the Local Group. Such a group of galaxies, held together by its own gravity, is called a galaxy cluster. ...
... Milky Way, Andromeda, and M33. These and their satellites – about 45 galaxies in all – form the Local Group. Such a group of galaxies, held together by its own gravity, is called a galaxy cluster. ...
Spectro-Morphology of Galaxies.
... (λ). Finally, in order to compare low and high-redshift galaxies, these parameters have to be robust against a degradation of spatial resolution and low signal-to-noise ratios (S/N ). For several years, a number of parameters have been proposed. Morgan (1958, 1959) originally used the index of light ...
... (λ). Finally, in order to compare low and high-redshift galaxies, these parameters have to be robust against a degradation of spatial resolution and low signal-to-noise ratios (S/N ). For several years, a number of parameters have been proposed. Morgan (1958, 1959) originally used the index of light ...
Read the paragraph on the left side of the book
... you have found the correct activity that matches the assignment Read the paragraph on the left side of the book. As you read, answer the questions below: ...
... you have found the correct activity that matches the assignment Read the paragraph on the left side of the book. As you read, answer the questions below: ...
A new view of galaxy evolution
... the universe is in a “dark” form that cannot be period. The critical aspect of this, however, is detected directly. The nature of this dark mat- that very little to no additional mass is added to ter, however, has a direct and perhaps primary a galaxy once it forms in the very early universe. role i ...
... the universe is in a “dark” form that cannot be period. The critical aspect of this, however, is detected directly. The nature of this dark mat- that very little to no additional mass is added to ter, however, has a direct and perhaps primary a galaxy once it forms in the very early universe. role i ...
Deep Sky Catalogues, the New Uranometria and Other Stories
... Clearly defined object classes and selection criteria. The „optical“ object classes should be contained: open and globular clusters, emission-, reflection- and dark nebulae, planetary nebulae, galaxies (including quasars) and clusters of galaxies. If there is a selection within a class, it must be b ...
... Clearly defined object classes and selection criteria. The „optical“ object classes should be contained: open and globular clusters, emission-, reflection- and dark nebulae, planetary nebulae, galaxies (including quasars) and clusters of galaxies. If there is a selection within a class, it must be b ...
Local Group Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mario L Mateo
... ‘island universes’ similar to our home galaxy, the MILKY WAY, he realized that a few of these external galaxies are considerably closer to us than any others. In 1936 he first coined the term ‘Local Group’ in his famous book The Realm of the Nebulae to identify our nearest galactic neighbors. More t ...
... ‘island universes’ similar to our home galaxy, the MILKY WAY, he realized that a few of these external galaxies are considerably closer to us than any others. In 1936 he first coined the term ‘Local Group’ in his famous book The Realm of the Nebulae to identify our nearest galactic neighbors. More t ...
What Drives the Stellar Mass Growth of Early-Type
... to observe these systems over a large redshift range in order to probe the physical mechanisms responsible for producing galaxies as observed at z = 0. However, it is simpler to observe galaxies in the nearby Universe compared to their counterparts at high redshift. This simple fact can introduce se ...
... to observe these systems over a large redshift range in order to probe the physical mechanisms responsible for producing galaxies as observed at z = 0. However, it is simpler to observe galaxies in the nearby Universe compared to their counterparts at high redshift. This simple fact can introduce se ...
Hubble Space Telescope Imaging of Post
... We hypothesis that the post-starburst quasar phase is a triggered event. We test the idea that PSQs are a phase in the life of all galaxies triggered by external dynamical events (e.g., mergers, tidal interactions) or whether they are a more heterogenous population in which multiple mechanisms can c ...
... We hypothesis that the post-starburst quasar phase is a triggered event. We test the idea that PSQs are a phase in the life of all galaxies triggered by external dynamical events (e.g., mergers, tidal interactions) or whether they are a more heterogenous population in which multiple mechanisms can c ...
THE INFLUENCE OF ENVIRONMENTAL EFFECTS ON GALAXY
... some galaxies that are traversing the cluster core for the rst time, and galaxies that appear in the cluster centre only in projection. Thus the statements made about cluster galaxies also constrain galaxies in the outer parts of clusters. Line strength indices measure essentially the same informat ...
... some galaxies that are traversing the cluster core for the rst time, and galaxies that appear in the cluster centre only in projection. Thus the statements made about cluster galaxies also constrain galaxies in the outer parts of clusters. Line strength indices measure essentially the same informat ...
PPT
... expensive in telescope time and in general these galaxies have not been detected in CO. • The nearest galaxies after SMC and LMC are ten times further away and we have been able to observe in CO (@10pc resolution) and continuum only a dozen of molecular cloud region in the ...
... expensive in telescope time and in general these galaxies have not been detected in CO. • The nearest galaxies after SMC and LMC are ten times further away and we have been able to observe in CO (@10pc resolution) and continuum only a dozen of molecular cloud region in the ...
Hubble`s Law Lab - The University of Texas at Austin
... Immediately after the Big Bang, the Universe began to expand, dragging all of the matter in the Universe along with it. Today it looks to us like every galaxy we can see is moving rapidly away from us (i.e., the light from the galaxy is “redshifted”). However, the galaxies we see today are not thems ...
... Immediately after the Big Bang, the Universe began to expand, dragging all of the matter in the Universe along with it. Today it looks to us like every galaxy we can see is moving rapidly away from us (i.e., the light from the galaxy is “redshifted”). However, the galaxies we see today are not thems ...
MOND as an alternative to dark matter: the Bullet
... BUT bullet => collisionless => BDM in the form of e.g. dense clumps of cold gas (Pfenniger & Combes 1994), present only in galaxy clusters? (but then, microlensing? X-ray emission from cloud-cloud annihilation?) + Why only in clusters and groups? BUT what about Abell 520? (Mahdavi et al. 2007) Effe ...
... BUT bullet => collisionless => BDM in the form of e.g. dense clumps of cold gas (Pfenniger & Combes 1994), present only in galaxy clusters? (but then, microlensing? X-ray emission from cloud-cloud annihilation?) + Why only in clusters and groups? BUT what about Abell 520? (Mahdavi et al. 2007) Effe ...
Lab 14 Galaxy Morphology
... which resembled pinwheels) were true galaxies–similar to the Milky Way in size and structure, but millions of light years from us. It was not until the 1920’s that the actual nature of galaxies was confirmed–they were true “Island Universes”, collections of millions and billions of stars. As you wil ...
... which resembled pinwheels) were true galaxies–similar to the Milky Way in size and structure, but millions of light years from us. It was not until the 1920’s that the actual nature of galaxies was confirmed–they were true “Island Universes”, collections of millions and billions of stars. As you wil ...
Epicycles… the short form. For lurid details, see [CO pp.1018-1030] φ
... Evidence showing density waves do occur. • Old, red stars show spiral density perturbation. • Molecular clouds form on inner edges of spiral arms. • HI gas flow shows discontinuity due to shocks at inner edges of spiral arms. • Bright young stars also in narrow arms. • Observed width ∆θ ~ t*(Ω - Ωp) ...
... Evidence showing density waves do occur. • Old, red stars show spiral density perturbation. • Molecular clouds form on inner edges of spiral arms. • HI gas flow shows discontinuity due to shocks at inner edges of spiral arms. • Bright young stars also in narrow arms. • Observed width ∆θ ~ t*(Ω - Ωp) ...
ch20
... The main difference between Sa, Sb and Sc galaxies is the relative amounts of gas and dust in them. The proportion of dust, gas and young stars increases from Sa to Sc galaxies. © 2014 Pearson Education, Inc. ...
... The main difference between Sa, Sb and Sc galaxies is the relative amounts of gas and dust in them. The proportion of dust, gas and young stars increases from Sa to Sc galaxies. © 2014 Pearson Education, Inc. ...
Module 11.1.1: Galaxies: Morphology and the Hubble Sequence
... S0's, which are galaxies that obviously had a disk but he couldn't see any spiral arms. Here's Sombrero galaxy, one of the famous examples. And indeed physically they are transitional in th ...
... S0's, which are galaxies that obviously had a disk but he couldn't see any spiral arms. Here's Sombrero galaxy, one of the famous examples. And indeed physically they are transitional in th ...
The oxygen abundance deficiency in irregular galaxies
... the gas outside the optical diameter can contain a significant part of the heavy elements produced by the stars and, therefore, can play an important role in the chemical evolution of the galaxy. Hunter & Gallagher (1985) have found that the presence or absence of extended HI envelopes does not appe ...
... the gas outside the optical diameter can contain a significant part of the heavy elements produced by the stars and, therefore, can play an important role in the chemical evolution of the galaxy. Hunter & Gallagher (1985) have found that the presence or absence of extended HI envelopes does not appe ...
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).