Lecture 13 Local group chapter 4 of S+G
... irregulars with low mass; most are satellites of MW, M31 or M33 The gravitational interaction between these systems is complex but the local group is apparently bound. Major advantages – close and bright- all nearby enough that individual stars can be well measured as well as HI, H2, IR, x-ray sourc ...
... irregulars with low mass; most are satellites of MW, M31 or M33 The gravitational interaction between these systems is complex but the local group is apparently bound. Major advantages – close and bright- all nearby enough that individual stars can be well measured as well as HI, H2, IR, x-ray sourc ...
Chapter 16
... 2. The center portion was the first to become dense enough for stars to form. Dense pockets in orbit around the center became globular clusters. 3. The initial cloud had some rotation, and as it contracted it spun faster. The rotating matter formed into a disk. 4. Density waves formed in the Galaxy’ ...
... 2. The center portion was the first to become dense enough for stars to form. Dense pockets in orbit around the center became globular clusters. 3. The initial cloud had some rotation, and as it contracted it spun faster. The rotating matter formed into a disk. 4. Density waves formed in the Galaxy’ ...
Paper - Astrophysics - University of Oxford
... 2.1. Formation of stars across the Universe When did stars form? To answer this basic question we can make use of the fact that every star must eventually die. Indeed the more massive stars die in spectacular supernova explosions that can outshine a whole galaxy. With an ELT these explosions can be ...
... 2.1. Formation of stars across the Universe When did stars form? To answer this basic question we can make use of the fact that every star must eventually die. Indeed the more massive stars die in spectacular supernova explosions that can outshine a whole galaxy. With an ELT these explosions can be ...
ies la arboleda – centro tic - plurilingüe
... (A)- The universe was contained in a single point in space. All of the matter and energy of space was then contained at this point. What existed prior to this event is completely unknown. About 13.73 billion years (13.730.000.000 years) ago a tremendous explosion started the expansion of the univers ...
... (A)- The universe was contained in a single point in space. All of the matter and energy of space was then contained at this point. What existed prior to this event is completely unknown. About 13.73 billion years (13.730.000.000 years) ago a tremendous explosion started the expansion of the univers ...
The Marathon
... The next seventeen objects are all galaxies and are part of the Coma-Virgo cluster. All the galaxies (with the exception of M104) are all very close together. You might think that's a good thing, since you won't have to swing your telescope all over the sky. What makes this part of the marathon diff ...
... The next seventeen objects are all galaxies and are part of the Coma-Virgo cluster. All the galaxies (with the exception of M104) are all very close together. You might think that's a good thing, since you won't have to swing your telescope all over the sky. What makes this part of the marathon diff ...
Andromeda Galaxy www.AssignmentPoint.com The Andromeda
... Way- as well as the significant Doppler shift that he had observed of Andromeda. In 1922 Ernst Öpik presented a method to estimate the distance of M31 using the measured velocities of its stars. His result placed the Andromeda Nebula far outside our galaxy at a distance of about 450,000 parsecs (1,5 ...
... Way- as well as the significant Doppler shift that he had observed of Andromeda. In 1922 Ernst Öpik presented a method to estimate the distance of M31 using the measured velocities of its stars. His result placed the Andromeda Nebula far outside our galaxy at a distance of about 450,000 parsecs (1,5 ...
Integrated Science
... Size and Mass Once astronomers know a star’s temperature and absolute brightness, they can estimate its diameter and then calculate its volume. The masses of many stars can be determined by observing the gravitational interaction of stars that occur in pairs. For most stars, there is a relationship ...
... Size and Mass Once astronomers know a star’s temperature and absolute brightness, they can estimate its diameter and then calculate its volume. The masses of many stars can be determined by observing the gravitational interaction of stars that occur in pairs. For most stars, there is a relationship ...
Supermassive Black Holes in Inactive Galaxies Encyclopedia of Astronomy & Astrophysics eaa.iop.org
... that M31 contains a central dark mass M• ≃ 3 × 107M⊙. The possible effects of velocity anisotropy have been checked and provide no escape. Furthermore, the asymmetry provides an almost independent check of the BH mass, as follows. The top panel of figure 3 shows the HST image at the same scale as an ...
... that M31 contains a central dark mass M• ≃ 3 × 107M⊙. The possible effects of velocity anisotropy have been checked and provide no escape. Furthermore, the asymmetry provides an almost independent check of the BH mass, as follows. The top panel of figure 3 shows the HST image at the same scale as an ...
talk.wyse - Johns Hopkins University
... ΛCDM cosmology extremely successful on large scales. Galaxies are the scales on which one must see the nature of dark matter & galaxy formation astrophysics Ostriker & Steinhardt 03 ...
... ΛCDM cosmology extremely successful on large scales. Galaxies are the scales on which one must see the nature of dark matter & galaxy formation astrophysics Ostriker & Steinhardt 03 ...
Gilmore
... Apparently dark-matter dominated ~ 10km/s, 10 < M/L < 100 Metal-poor, all contain very old stars; but ...
... Apparently dark-matter dominated ~ 10km/s, 10 < M/L < 100 Metal-poor, all contain very old stars; but ...
So What All Is Out There, Anyway?
... vast areas of space where there are very few stars, and once you finally get big enough you see that most of the stars are grouped together in a large, flat disk with long arms reaching out into space in a spiral. This beautiful collection of stars, star clusters, and nebulas, is slowly rotating. At ...
... vast areas of space where there are very few stars, and once you finally get big enough you see that most of the stars are grouped together in a large, flat disk with long arms reaching out into space in a spiral. This beautiful collection of stars, star clusters, and nebulas, is slowly rotating. At ...
The Milky Way`s Spiral Arms
... and gas to slow down near the arm • This compresses the interstellar clouds, triggering the formation of stars • The entire arm pattern rotates around the Milky Way once every 500 million years ...
... and gas to slow down near the arm • This compresses the interstellar clouds, triggering the formation of stars • The entire arm pattern rotates around the Milky Way once every 500 million years ...
Section 4 Formation of the Universe Chapter 19
... • A galaxy is a collection of stars, dust, and gas held together by gravity. ...
... • A galaxy is a collection of stars, dust, and gas held together by gravity. ...
Extremely Large Telescopes
... Evolution of Galaxies: Assembly of galaxy haloes • Map evolution dark matter from 1
... Evolution of Galaxies: Assembly of galaxy haloes • Map evolution dark matter from 1
Multiple Choice, continued Stars, Galaxies, and the Universe
... Today, we know that Copernicus was right: the stars are very far from Earth. In fact, stars are so distant that a new unit of length—the light-year—was created to measure their distance. A light-year is a unit of length equal to the distance that light travels through space in 1 year. Because the sp ...
... Today, we know that Copernicus was right: the stars are very far from Earth. In fact, stars are so distant that a new unit of length—the light-year—was created to measure their distance. A light-year is a unit of length equal to the distance that light travels through space in 1 year. Because the sp ...
Birth, Age and the Future of the Universe
... divide this distance by the recession velocity. The result is nothing else but the expansion age of the ...
... divide this distance by the recession velocity. The result is nothing else but the expansion age of the ...
Beyond Our Solar System
... – The sun is a fairly typical star, and it seems to be located in a fairly average neighborhood in the universe. – Although there are many billions of stars like the sun, none is close enough to be visible in the diagram— which shows an area only 11,000 AU in diameter. ...
... – The sun is a fairly typical star, and it seems to be located in a fairly average neighborhood in the universe. – Although there are many billions of stars like the sun, none is close enough to be visible in the diagram— which shows an area only 11,000 AU in diameter. ...
Galaxy Formation and Evolution
... In currently popular cosmologies we usually consider a Universe consisting of three main components. In addition to the ‘baryonic’ matter, the protons, neutrons and electrons that make up the visible Universe, astronomers have found various indications for the presence of dark matter and dark energy ...
... In currently popular cosmologies we usually consider a Universe consisting of three main components. In addition to the ‘baryonic’ matter, the protons, neutrons and electrons that make up the visible Universe, astronomers have found various indications for the presence of dark matter and dark energy ...
Galaxies (and stars) in the far infrared: results from the AKARI All
... Supply of metals to the interstellar space II: final life stages of stars The death of light stars : planetary nebulae (PNe) Stars with masses similar to the Sun run out the hydrogen in the core, change their equilibrium structure and expand, and become cool huge stars (red giant branch stars: RGBs ...
... Supply of metals to the interstellar space II: final life stages of stars The death of light stars : planetary nebulae (PNe) Stars with masses similar to the Sun run out the hydrogen in the core, change their equilibrium structure and expand, and become cool huge stars (red giant branch stars: RGBs ...
Contents - Classroom Complete Press
... 2. Circle the word TRUE if the statement is TRUE FALSE if it is FALSE. ...
... 2. Circle the word TRUE if the statement is TRUE FALSE if it is FALSE. ...
Measuring the masses of clusters
... –! In densest regions, gas may cool and sink toward the cluster center as a “cooling flow” –! Unlikely that all of it has escaped from galaxies, some must be around from cluster formation process. It is heated via shocks as the gas falls into the cluster potential –! But some metals, must be from st ...
... –! In densest regions, gas may cool and sink toward the cluster center as a “cooling flow” –! Unlikely that all of it has escaped from galaxies, some must be around from cluster formation process. It is heated via shocks as the gas falls into the cluster potential –! But some metals, must be from st ...
ASTR2100 - Saint Mary's University | Astronomy & Physics
... the distance to the Andromeda Nebula using Cepheid variables. Somewhat less well-known is Lindblad’s 1926 development of a mathematical model for Galactic rotation. Lindblad’s model was developed further in 1927-28 by Oort, who demonstrated its applicability to the radial velocity data for stars. Fi ...
... the distance to the Andromeda Nebula using Cepheid variables. Somewhat less well-known is Lindblad’s 1926 development of a mathematical model for Galactic rotation. Lindblad’s model was developed further in 1927-28 by Oort, who demonstrated its applicability to the radial velocity data for stars. Fi ...
AJAstroProject
... • The pictures will appear before the data and then a smaller image will be included with the data on the next slide. ...
... • The pictures will appear before the data and then a smaller image will be included with the data on the next slide. ...
Galaxy
.jpg?width=300)
A galaxy is a gravitationally bound system of stars, stellar remnants, interstellar gas and dust, and dark matter. The word galaxy is derived from the Greek galaxias (γαλαξίας), literally ""milky"", a reference to the Milky Way. Galaxies range in size from dwarfs with just a few thousand (103) stars to giants with one hundred trillion (1014) stars, each orbiting their galaxy's own center of mass. Galaxies are categorized according to their visual morphology, including elliptical, spiral, and irregular. Many galaxies are thought to have black holes at their active centers. The Milky Way's central black hole, known as Sagittarius A*, has a mass four million times greater than our own Sun. As of July 2015, EGSY8p7 is the oldest and most distant galaxy with a light travel distance of 13.2 billion light-years from Earth, and observed as it existed 570 million years after the Big Bang. Previously, as of May 2015, EGS-zs8-1 was the most distant known galaxy, estimated to have a light travel distance of 13.1 billion light-years away and to have 15% of the mass of the Milky Way.Approximately 170 billion (1.7 × 1011) to 200 billion (2.0 × 1011) galaxies exist in the observable universe. Most of the galaxies are 1,000 to 100,000 parsecs in diameter and usually separated by distances on the order of millions of parsecs (or megaparsecs). The space between galaxies is filled with a tenuous gas with an average density less than one atom per cubic meter. The majority of galaxies are gravitationally organized into associations known as galaxy groups, clusters, and superclusters. At the largest scale, these associations are generally arranged into sheets and filaments that are surrounded by immense voids.