Introduction to Galaxies - West Jefferson Local Schools
... able to measure the distance to the “Great Nebula in Andromeda” (M 31, previous slide) and found its distance to be much larger than the diameter of the Milky Way. This meant that M 31, and by extension other spiral nebulae, were galaxies in their own right, comparable to or even larger than the Mil ...
... able to measure the distance to the “Great Nebula in Andromeda” (M 31, previous slide) and found its distance to be much larger than the diameter of the Milky Way. This meant that M 31, and by extension other spiral nebulae, were galaxies in their own right, comparable to or even larger than the Mil ...
Notes on Integral Field Spectroscopy (IFS/3D) Sebastián F. Sánchez / IA-UNAM
... November 2012 DR2: Oct. 2014!!! ...
... November 2012 DR2: Oct. 2014!!! ...
Exploring The Universe
... • Quasars may be infant galaxies. • In 1960, a faint object was matched with a strong radio signal. This object was called a quasar. • quasar quasi-stellar radio sources; very luminous objects that produce energy at a high rate and that are thought to be the most distant objects in the universe • Ea ...
... • Quasars may be infant galaxies. • In 1960, a faint object was matched with a strong radio signal. This object was called a quasar. • quasar quasi-stellar radio sources; very luminous objects that produce energy at a high rate and that are thought to be the most distant objects in the universe • Ea ...
The Extragalactic Distance Database: Color–Magnitude Diagrams
... footprint of the observations used in our analysis is highlighted in yellow. The red boxes represent the footprint of another ACS observation of the galaxy. Footprints of observations other than those used for the production of the galaxy’s CMD often appear in these images, but those that are used a ...
... footprint of the observations used in our analysis is highlighted in yellow. The red boxes represent the footprint of another ACS observation of the galaxy. Footprints of observations other than those used for the production of the galaxy’s CMD often appear in these images, but those that are used a ...
Lecture notes 18: Galaxies and galaxy clusters
... 104 globular clusters. The mass to light ratio of these galaxies is also immense, 750 MS /LS , indicating large quantities of dark matter. • Normal elliptical galaxies are further seperated into giant elliptical (gE’s), ellipticals (E’s) and compact ellipticals (cE’s). Masses range 108 − 1013 MS , d ...
... 104 globular clusters. The mass to light ratio of these galaxies is also immense, 750 MS /LS , indicating large quantities of dark matter. • Normal elliptical galaxies are further seperated into giant elliptical (gE’s), ellipticals (E’s) and compact ellipticals (cE’s). Masses range 108 − 1013 MS , d ...
ppt document - FacStaff Home Page for CBU
... Way. By looking in the infrared (which is not scattered as much as visible light by the dust and gas), we see that we are not in the center of the disk, but somewhere away from the center. The approximate size of the Milky Way appears to be about 100,000 light years across and 2,000 light years thic ...
... Way. By looking in the infrared (which is not scattered as much as visible light by the dust and gas), we see that we are not in the center of the disk, but somewhere away from the center. The approximate size of the Milky Way appears to be about 100,000 light years across and 2,000 light years thic ...
Spiral Galaxies - Astronomy Centre
... • Spiral disks are relatively blue due to light from hot, massive, young stars • Elliptical galaxies are relatively red due to the dominant population of older, lower-mass stars ...
... • Spiral disks are relatively blue due to light from hot, massive, young stars • Elliptical galaxies are relatively red due to the dominant population of older, lower-mass stars ...
M101: The Pinwheel Galaxy
... class. Ask students to review the galaxy image on the front of the “M101: The Pinwheel Galaxy” lithograph and write down three questions they have about the galaxy in the image. Ask the students to read the information on the back of the “M101: The Pinwheel Galaxy” lithograph and check if any of the ...
... class. Ask students to review the galaxy image on the front of the “M101: The Pinwheel Galaxy” lithograph and write down three questions they have about the galaxy in the image. Ask the students to read the information on the back of the “M101: The Pinwheel Galaxy” lithograph and check if any of the ...
Quasars: Back to the Infant Universe
... Quasars appear extremely bright. Is this because they’re close to us or because they’re intrinsically luminous? What observations of quasars tell us they are small? What are Seyferts and Radio Galaxies? What is at the center of a galaxy that powers a quasar? Why are there few quasars close to us? Co ...
... Quasars appear extremely bright. Is this because they’re close to us or because they’re intrinsically luminous? What observations of quasars tell us they are small? What are Seyferts and Radio Galaxies? What is at the center of a galaxy that powers a quasar? Why are there few quasars close to us? Co ...
Dark Matter: Observational Constraints Properties of Dark Matter:
... Where Doesn’t Dark Matter Exist? • Star Clusters (open and globular) ...
... Where Doesn’t Dark Matter Exist? • Star Clusters (open and globular) ...
Lecture 16
... How do we observe the life histories of galaxies? – Deep observations of the universe are showing us the history of galaxies because we are seeing galaxies as they were at different ages How did galaxies form? – Our best models for galaxy formation assume that gravity made galaxies out of regions ...
... How do we observe the life histories of galaxies? – Deep observations of the universe are showing us the history of galaxies because we are seeing galaxies as they were at different ages How did galaxies form? – Our best models for galaxy formation assume that gravity made galaxies out of regions ...
Planets and Moons - Fraser Heights Chess Club
... grand spiral arms and sweeping cosmic dust lanes with a scale comparable to the Milky Way. Hinting at a disorderly past, a remarkable dust lane runs straight through the disk, below and right of the galactic center, contrary to M81's other prominent spiral features. The errant dust lane may be the l ...
... grand spiral arms and sweeping cosmic dust lanes with a scale comparable to the Milky Way. Hinting at a disorderly past, a remarkable dust lane runs straight through the disk, below and right of the galactic center, contrary to M81's other prominent spiral features. The errant dust lane may be the l ...
Document
... astronomers can carry out look-back studies to assess empirically when and how galaxies formed. The distant universe became a prominent field of astronomical research during the final decade of the twentieth century. At that time the Lyman break technique in combination with the new generation of 8- ...
... astronomers can carry out look-back studies to assess empirically when and how galaxies formed. The distant universe became a prominent field of astronomical research during the final decade of the twentieth century. At that time the Lyman break technique in combination with the new generation of 8- ...
Why Aren`t All Galaxies Barred?
... It is this aspect wh ich makes calculation of the orbits of stars in a galaxy so much more complicated than those of the planets in the solar system, even though the relevant laws of physics are identical. One way, although not the only way, to study the behaviour of such galaxies, is to programme ...
... It is this aspect wh ich makes calculation of the orbits of stars in a galaxy so much more complicated than those of the planets in the solar system, even though the relevant laws of physics are identical. One way, although not the only way, to study the behaviour of such galaxies, is to programme ...
harvest09b - NMSU Astronomy
... Clear causal connection of “strong” CIV absorbers seen in QSO spectra with galaxies; I.e., C IV traces metal enriched gas in vicinity (80 kpc proper) of galaxies O VI absorption and z=3 galaxies For N(OVI) > 1013.5 cm-2, the OVI absorber temperatures, kinematics, and rate of ...
... Clear causal connection of “strong” CIV absorbers seen in QSO spectra with galaxies; I.e., C IV traces metal enriched gas in vicinity (80 kpc proper) of galaxies O VI absorption and z=3 galaxies For N(OVI) > 1013.5 cm-2, the OVI absorber temperatures, kinematics, and rate of ...
Here
... Hence the stellar populations characteristics of E galaxies must be derived from the integrated colors and spectra. As we saw before, the spectra of an E galaxy resembles that of a K giant star. E galaxies appear generally red: •very few stars made in the last 1-2 Gyr (recall that after 1 Gyr, only ...
... Hence the stellar populations characteristics of E galaxies must be derived from the integrated colors and spectra. As we saw before, the spectra of an E galaxy resembles that of a K giant star. E galaxies appear generally red: •very few stars made in the last 1-2 Gyr (recall that after 1 Gyr, only ...
file - University of California San Diego
... The University of California, San Diego team will devote much of its observing time to quasars, the most distant and energetic objects in the universe. The goal is to try to understand the nature and evolution of these enigmatic objects that are as compact as our solar system yet as bright as 100 tr ...
... The University of California, San Diego team will devote much of its observing time to quasars, the most distant and energetic objects in the universe. The goal is to try to understand the nature and evolution of these enigmatic objects that are as compact as our solar system yet as bright as 100 tr ...
Chapter 20. Galaxies
... of some AGNS is no more than, say, 1 AU, but was as powerful as an entire galaxy! Today, we understand that only a black hole, which can convert gravitational potential energy of infalling gas to radiation, is capable of such efficient energy generation on such a small scale! An extreme example of t ...
... of some AGNS is no more than, say, 1 AU, but was as powerful as an entire galaxy! Today, we understand that only a black hole, which can convert gravitational potential energy of infalling gas to radiation, is capable of such efficient energy generation on such a small scale! An extreme example of t ...
Elliptical galaxies
... •If the distribution function f (r, v) is known, and all stars were the same, we could derive the spectrum of the galaxy. •In practice, one makes a guess for the f(r, vz), which depends on a few parameters, and fixes those in order to reproduce the observed spectrum. ...
... •If the distribution function f (r, v) is known, and all stars were the same, we could derive the spectrum of the galaxy. •In practice, one makes a guess for the f(r, vz), which depends on a few parameters, and fixes those in order to reproduce the observed spectrum. ...
astro704_final - Department of Physics and Astronomy
... Smooths out the cusp on a timescale of only ~100 Myr using only moderate (~10 km/s) random bulk motions induced by SNe Requires recognition that gas distribution in progenitor galaxy disks is clumpy Suggests that NFW density profile is not appropriate choice for Cole et al.’s CDM merger trees, at le ...
... Smooths out the cusp on a timescale of only ~100 Myr using only moderate (~10 km/s) random bulk motions induced by SNe Requires recognition that gas distribution in progenitor galaxy disks is clumpy Suggests that NFW density profile is not appropriate choice for Cole et al.’s CDM merger trees, at le ...
PH607 – Galaxies
... 7.2 Clusters of Galaxies Clusters are systems a few Mpc across, typically containing at least 50-100 luminous galaxies within the central 1 Mpc Clusters are gravitationally bound Clusters are filled with hot X-ray gas Only ~20% of galaxies live in clusters, most live in groups or in the “fi ...
... 7.2 Clusters of Galaxies Clusters are systems a few Mpc across, typically containing at least 50-100 luminous galaxies within the central 1 Mpc Clusters are gravitationally bound Clusters are filled with hot X-ray gas Only ~20% of galaxies live in clusters, most live in groups or in the “fi ...
SCIN 293-PL-New Course
... Objective 1: Evaluate the lives of galaxies from formation to star production and evolution by collision with other galaxies. Lesson 1: Galactic Evolution Topic 1: The Milky Way Galaxy Topic 2: Formation of Galaxies Topic 3: Active Galactic Nuclei Topic Mastery: Based on the Hubble tuning fork comp ...
... Objective 1: Evaluate the lives of galaxies from formation to star production and evolution by collision with other galaxies. Lesson 1: Galactic Evolution Topic 1: The Milky Way Galaxy Topic 2: Formation of Galaxies Topic 3: Active Galactic Nuclei Topic Mastery: Based on the Hubble tuning fork comp ...
1 Introduction - Wiley-VCH
... (Figure 1.5a) to the 21 cm HI radio line (Figure 1.5l). The distribution of the old stellar population, as traced by the near-infrared image at 3.6 μm obtained by the Spitzer space mission, is relatively smooth. Old stars are the dominant stellar population in the companion NGC 5195, an early-type g ...
... (Figure 1.5a) to the 21 cm HI radio line (Figure 1.5l). The distribution of the old stellar population, as traced by the near-infrared image at 3.6 μm obtained by the Spitzer space mission, is relatively smooth. Old stars are the dominant stellar population in the companion NGC 5195, an early-type g ...
Beyond the Solar System By Patti Hutchison ANSWER THE
... As a galaxy, the Milky Way is actually a giant. Its diameter is about 100,000 light years. A light year is the distance that light travels in one year. A light year is about 9.5 trillion kilometers or about 6 trillion miles. Our solar system is about 4.6 billion years old. Our sun is a young star. S ...
... As a galaxy, the Milky Way is actually a giant. Its diameter is about 100,000 light years. A light year is the distance that light travels in one year. A light year is about 9.5 trillion kilometers or about 6 trillion miles. Our solar system is about 4.6 billion years old. Our sun is a young star. S ...
Pea galaxy
A Pea galaxy, also referred to as a Pea or Green Pea, might be a type of Luminous Blue Compact Galaxy which is undergoing very high rates of star formation. Pea galaxies are so-named because of their small size and greenish appearance in the images taken by the Sloan Digital Sky Survey (SDSS).Pea Galaxies were first discovered in 2007 by the volunteer users within the forum section of the online astronomy project Galaxy Zoo (GZ).