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... 3. Does not appear to be a large population of HI clouds with no optical counterparts. 4. Dwarf (mainly dE/dSph) galaxies with red colours found in large numbers in the cluster. They are gas poor, but are they stripped of their gas? 5. Low numbers of dwarf (dI) galaxies with blue colours and gas ric ...
... 3. Does not appear to be a large population of HI clouds with no optical counterparts. 4. Dwarf (mainly dE/dSph) galaxies with red colours found in large numbers in the cluster. They are gas poor, but are they stripped of their gas? 5. Low numbers of dwarf (dI) galaxies with blue colours and gas ric ...
Galaxies - Physics
... What are the spiral and elliptical nebulae? • No individual stars are visible, even in largest telescopes • Some have spiral structure, as if spinning rapidly • Visible amount of rotation over a few decades? • Continuous spectra • Hypothesis 1: Swirling clouds of fluid, possibly forming new solar s ...
... What are the spiral and elliptical nebulae? • No individual stars are visible, even in largest telescopes • Some have spiral structure, as if spinning rapidly • Visible amount of rotation over a few decades? • Continuous spectra • Hypothesis 1: Swirling clouds of fluid, possibly forming new solar s ...
galaxy worksheet
... 2. Every star you can see from Earth with the unaided eye is part of the __________ Galaxy. 3. Our own galaxy is the type of galaxy called a(n) __________ galaxy. 4. The major galaxy closest to our own is the __________ Galaxy. 5. A spiral galaxy has a rotating disk of stars and dust with several __ ...
... 2. Every star you can see from Earth with the unaided eye is part of the __________ Galaxy. 3. Our own galaxy is the type of galaxy called a(n) __________ galaxy. 4. The major galaxy closest to our own is the __________ Galaxy. 5. A spiral galaxy has a rotating disk of stars and dust with several __ ...
Abstract Observations Numerical Setup Results
... Simon Karl, Thorsten Naab - University Observatory Munich ...
... Simon Karl, Thorsten Naab - University Observatory Munich ...
Highligh in Physics 2005
... defined as A =A (|k|;Qh,a,b,d,h). Here k and n are the dimensionless wavenumber and Doppler-shifted frequency,Qh is the well known axisymmetric stability parameter,a function of the dimensionless wavenumber k. The other parameters have been set to the following values: a=0.1, b=0.1, Qh=Qcrit≈1.14. a ...
... defined as A =A (|k|;Qh,a,b,d,h). Here k and n are the dimensionless wavenumber and Doppler-shifted frequency,Qh is the well known axisymmetric stability parameter,a function of the dimensionless wavenumber k. The other parameters have been set to the following values: a=0.1, b=0.1, Qh=Qcrit≈1.14. a ...
8and10Dec_2014
... mostly older Pop II stars – Contain very high temperature, very low density clouds of gas that cannot condense into stars. ...
... mostly older Pop II stars – Contain very high temperature, very low density clouds of gas that cannot condense into stars. ...
X-ray observations of the hot CGM of nearby disk galaxies
... X-ray emitting CGM is substantially greater. • The emission is observed from low-mass galaxies for which little hot CGM is expected from the accretion. • The X-ray-emitting gas is apparently enriched by the stellar feedback of different types of galaxies. Thus the emission most likely traces the f ...
... X-ray emitting CGM is substantially greater. • The emission is observed from low-mass galaxies for which little hot CGM is expected from the accretion. • The X-ray-emitting gas is apparently enriched by the stellar feedback of different types of galaxies. Thus the emission most likely traces the f ...
Driving downsizing with galaxy groups
... dominated by groups) Simple strangulation models may still work well, if the instantaneous assumption is ...
... dominated by groups) Simple strangulation models may still work well, if the instantaneous assumption is ...
Lecture 8: The distance ladder
... Hubble’s law and distances • the most fundamental method is to use the redshift to estimate the distances to faint galaxies: • Hubble’s law is v = H0 d – so measure v and use H0 is ≈ 70 km s-1 Mpc-1 – NB this only works if the motion is cosmological, not within the Local Group, for example! • ...
... Hubble’s law and distances • the most fundamental method is to use the redshift to estimate the distances to faint galaxies: • Hubble’s law is v = H0 d – so measure v and use H0 is ≈ 70 km s-1 Mpc-1 – NB this only works if the motion is cosmological, not within the Local Group, for example! • ...
Astronomy Library wk 8.cwk (WP)
... With lighter elements, this contraction led to fusion of the spent fuel, but this is impossible with iron. Any nuclear reaction involving iron takes energy. ...
... With lighter elements, this contraction led to fusion of the spent fuel, but this is impossible with iron. Any nuclear reaction involving iron takes energy. ...
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. ...
Modern Telescopes and Ancient Skies
... The closest star to our Sun is Proxima Centauri, about 4 light years distant. ...
... The closest star to our Sun is Proxima Centauri, about 4 light years distant. ...
Galaxies - University of Iowa Astrophysics
... How big is the Universe? • Spiral nebulae were identified not long after development of the telescope around 1600 • In the 1600’s, it was suggested that spiral nebula are separate galaxies so far away that the stars blur together, but most people thought they were clouds of gas • The question wasn’ ...
... How big is the Universe? • Spiral nebulae were identified not long after development of the telescope around 1600 • In the 1600’s, it was suggested that spiral nebula are separate galaxies so far away that the stars blur together, but most people thought they were clouds of gas • The question wasn’ ...
Universe Power Point
... The further away the galaxy , the faster the galaxy is moving away from us. ...
... The further away the galaxy , the faster the galaxy is moving away from us. ...
Chapter 25 Beyond Our Solar System
... violent explosion from which the universe continues to expand, evolve, and cool • The big bang theory states that at one time, the entire universe was confined to a dense, hot, supermassive ball. Then, about 13.7 billion years ago, a violent explosion occurred, hurling this material in all direction ...
... violent explosion from which the universe continues to expand, evolve, and cool • The big bang theory states that at one time, the entire universe was confined to a dense, hot, supermassive ball. Then, about 13.7 billion years ago, a violent explosion occurred, hurling this material in all direction ...
A - 4 - Subaru Telescope
... Not all galaxies look pretty and symmetric. When they do not, astronomers use the term “irregular" to describe them. IC 10 is one such galaxy. Astronomers study it in order to understand how stars evolve. IC 10 is also a member of a cluster of galaxies called the Local Group, which includes the Milk ...
... Not all galaxies look pretty and symmetric. When they do not, astronomers use the term “irregular" to describe them. IC 10 is one such galaxy. Astronomers study it in order to understand how stars evolve. IC 10 is also a member of a cluster of galaxies called the Local Group, which includes the Milk ...
Homework sheet 12 - Egyptian Language School
... by number of stars 2. There are many different colors of stars. Which characteristic determines the color of a star? temperature size and shape actual brightness distance from Earth Page 1 of 2 ...
... by number of stars 2. There are many different colors of stars. Which characteristic determines the color of a star? temperature size and shape actual brightness distance from Earth Page 1 of 2 ...
Stars, Galaxies and Nebulae
... Name Street, City, Postal Code Continent Planet – Earth Star – the Sun Galaxy – Milky Way Galaxy Cluster – The Local Group ...
... Name Street, City, Postal Code Continent Planet – Earth Star – the Sun Galaxy – Milky Way Galaxy Cluster – The Local Group ...
1.5 The Big Bang - Animated Science
... …we’re looking at light that was made when the universe was young… …and if we study the light it tells us that the atoms of the early universe were… ...
... …we’re looking at light that was made when the universe was young… …and if we study the light it tells us that the atoms of the early universe were… ...
2010–2015 Edusmart Answer Key for The Universe
... A star’s brightness, or luminosity, depends on how far away it is from Earth and how much energy it puts out in a given time. ...
... A star’s brightness, or luminosity, depends on how far away it is from Earth and how much energy it puts out in a given time. ...
Coma Cluster of Galaxies Activity
... Using what you’ve learned, write a hypothesis that might explain why we see the morphology-density effect. In other words, why do we see more elliptical and lenticular galaxies in clusters and more spiral galaxies in the field? Remember that galaxies change and evolve over time, and these galaxies h ...
... Using what you’ve learned, write a hypothesis that might explain why we see the morphology-density effect. In other words, why do we see more elliptical and lenticular galaxies in clusters and more spiral galaxies in the field? Remember that galaxies change and evolve over time, and these galaxies h ...
What the UV SED Tells us About Stellar Populations and
... • Stellar mass ~ 108 M☉, so halo mass (Mstar + Mgas + DM) must be >109 M☉ • High SFR (10-100 M☉ per year) • Large (negative) b suggests incomplete absorption of stellar ionizing radiation ➙ HI envelope is perforated, thin, or non existent ...
... • Stellar mass ~ 108 M☉, so halo mass (Mstar + Mgas + DM) must be >109 M☉ • High SFR (10-100 M☉ per year) • Large (negative) b suggests incomplete absorption of stellar ionizing radiation ➙ HI envelope is perforated, thin, or non existent ...
The Universe is Expanding – Galactic Redshift
... n=3 (2nd excited state) n=2 (1st excited state) ...
... n=3 (2nd excited state) n=2 (1st excited state) ...
Seyfert galaxy
Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei (very luminous, distant and bright sources of electromagnetic radiation) with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.Seyfert galaxies account for about 10% of all galaxies and are some of the most intensely studied objects in astronomy, as they are thought to be powered by the same phenomena that occur in quasars, although they are closer and less luminous than quasars. These galaxies have supermassive black holes at their centers which are surrounded by accretion discs of in-falling material. The accretion discs are believed to be the source of the observed ultraviolet radiation. Ultraviolet emission and absorption lines provide the best diagnostics for the composition of the surrounding material.Seen in visible light, most Seyfert galaxies look like normal spiral galaxies, but when studied under other wavelengths, it becomes clear that the luminosity of their cores is of comparable intensity to the luminosity of whole galaxies the size of the Milky Way.Seyfert galaxies are named after Carl Seyfert, who first described this class in 1943.