Universe Eighth Edition Universe Roger A. Freedman William J. Kaufmann III CHAPTER 24 Galaxies Galaxies

Chapter 24 and 26 online quizzes due Thursday 12/9 Skip Chapter 27 Final Exam – Monday 12/13, 5:30-7:30 PM The final will cover chapters 23, 24 and 26 only, same format as Exams 1-3 Last HW!

How did Edwin Hubble show that M31 in Andromeda is a distant galaxy and not part of the Milky Way? A.By measuring the distance to M31 using Cepheid variables. B.By measuring the distance to M31 using RR Lyrae variables. C.By precisely measuring the parallax of M31. D.By observing a nova in M31. E.By observing a supernova in M31. Q24.7

How did Edwin Hubble show that M31 in Andromeda is a distant galaxy and not part of the Milky Way? A.By measuring the distance to M31 using Cepheid variables. B.By measuring the distance to M31 using RR Lyrae variables. C.By precisely measuring the parallax of M31. D.By observing a nova in M31. E.By observing a supernova in M31. A24.7

Which of the following best describes the Hubble law in its simplest form? A.The recessional velocity of a galaxy is proportional to its distance from us. B.The recessional velocity of a galaxy is inversely proportional to its distance from us. C.The brightness of a galaxy is proportional to its distance from us. D.The brightness of a galaxy is inversely proportional to its distance from us. E.The brightness of a galaxy is inversely proportional to its color. Q24.10

Which of the following best describes the Hubble law in its simplest form? A.The recessional velocity of a galaxy is proportional to its distance from us. B.The recessional velocity of a galaxy is inversely proportional to its distance from us. C.The brightness of a galaxy is proportional to its distance from us. D.The brightness of a galaxy is inversely proportional to its distance from us. E.The brightness of a galaxy is inversely proportional to its color. A24.10

In which of the following types of galaxies would you be least likely to find a newly-formed star? A.Elliptical B.Spiral C.Irregular D.Misleading question — newly-formed stars can be found in ellipticals, spirals, and irregulars Q24.8

In which of the following types of galaxies would you be least likely to find a newly-formed star? A.Elliptical B.Spiral C.Irregular D.Misleading question — newly-formed stars can be found in ellipticals, spirals, and irregulars A24.8

Key Ideas The Hubble Classification: Galaxies can be grouped into four major categories: spirals, barred spirals, ellipticals, and irregulars. The Hubble Classification: Galaxies can be grouped into four major categories: spirals, barred spirals, ellipticals, and irregulars. The disks of spiral and barred spiral galaxies are sites of active star formation. The disks of spiral and barred spiral galaxies are sites of active star formation. Elliptical galaxies are nearly devoid of interstellar gas and dust, and so star formation is severely inhibited. Elliptical galaxies are nearly devoid of interstellar gas and dust, and so star formation is severely inhibited. Lenticular galaxies are intermediate between spiral and elliptical galaxies. Lenticular galaxies are intermediate between spiral and elliptical galaxies. Irregular galaxies have ill-defined, asymmetrical shapes. They are often found associated with other galaxies. Irregular galaxies have ill-defined, asymmetrical shapes. They are often found associated with other galaxies.

Key Ideas Distance to Galaxies: Standard candles, such as Cepheid variables and the most luminous supergiants, globular clusters, H II regions, and supernovae in a galaxy, are used in estimating intergalactic distances. Distance to Galaxies: Standard candles, such as Cepheid variables and the most luminous supergiants, globular clusters, H II regions, and supernovae in a galaxy, are used in estimating intergalactic distances. The Tully-Fisher relation, which correlates the width of the 21-cm line of hydrogen in a spiral galaxy with its luminosity, can also be used for determining distance. A method that can be used for elliptical galaxies is the fundamental plane, which relates the galaxy’s size to its surface brightness distribution and to the motions of its stars. The Tully-Fisher relation, which correlates the width of the 21-cm line of hydrogen in a spiral galaxy with its luminosity, can also be used for determining distance. A method that can be used for elliptical galaxies is the fundamental plane, which relates the galaxy’s size to its surface brightness distribution and to the motions of its stars.

Key Ideas The Hubble Law: There is a simple linear relationship between the distance from the Earth to a remote galaxy and the redshift of that galaxy (which is a measure of the speed with which it is receding from us). This relationship is the Hubble law, v = H 0 d. The Hubble Law: There is a simple linear relationship between the distance from the Earth to a remote galaxy and the redshift of that galaxy (which is a measure of the speed with which it is receding from us). This relationship is the Hubble law, v = H 0 d. The value of the Hubble constant, H 0, is not known with certainty but is close to 73 km/s/Mpc. The value of the Hubble constant, H 0, is not known with certainty but is close to 73 km/s/Mpc.

Key Ideas Clusters and Superclusters: Galaxies are grouped into clusters rather than being scattered randomly throughout the universe. Clusters and Superclusters: Galaxies are grouped into clusters rather than being scattered randomly throughout the universe. A rich cluster contains hundreds or even thousands of galaxies; a poor cluster, often called a group, may contain only a few dozen. A rich cluster contains hundreds or even thousands of galaxies; a poor cluster, often called a group, may contain only a few dozen. A regular cluster has a nearly spherical shape with a central concentration of galaxies; in an irregular cluster, galaxies are distributed asymmetrically. A regular cluster has a nearly spherical shape with a central concentration of galaxies; in an irregular cluster, galaxies are distributed asymmetrically.

Key Ideas Our Galaxy is a member of a poor, irregular cluster called the Local Group. Our Galaxy is a member of a poor, irregular cluster called the Local Group. Rich, regular clusters contain mostly elliptical and lenticular galaxies; irregular clusters contain spiral, barred spiral, and irregular galaxies along with ellipticals. Rich, regular clusters contain mostly elliptical and lenticular galaxies; irregular clusters contain spiral, barred spiral, and irregular galaxies along with ellipticals. Giant elliptical galaxies are often found near the centers of rich clusters. Giant elliptical galaxies are often found near the centers of rich clusters.

Key Ideas Galactic Collisions and Mergers: When two galaxies collide, their stars pass each other, but their interstellar media collide violently, either stripping the gas and dust from the galaxies or triggering prolific star formation. Galactic Collisions and Mergers: When two galaxies collide, their stars pass each other, but their interstellar media collide violently, either stripping the gas and dust from the galaxies or triggering prolific star formation. The gravitational effects during a galactic collision can throw stars out of their galaxies into intergalactic space. The gravitational effects during a galactic collision can throw stars out of their galaxies into intergalactic space. Galactic mergers may occur; a large galaxy in a rich cluster may tend to grow steadily through galactic cannibalism, perhaps producing in the process a giant elliptical galaxy. Galactic mergers may occur; a large galaxy in a rich cluster may tend to grow steadily through galactic cannibalism, perhaps producing in the process a giant elliptical galaxy.

Key Ideas The Dark-Matter Problem: The luminous mass of a cluster of galaxies is not large enough to account for the observed motions of the galaxies; a large amount of unobserved mass must also be present. This situation is called the dark-matter problem. The Dark-Matter Problem: The luminous mass of a cluster of galaxies is not large enough to account for the observed motions of the galaxies; a large amount of unobserved mass must also be present. This situation is called the dark-matter problem. Hot intergalactic gases in rich clusters account for a small part of the unobserved mass. These gases are detected by their X-ray emission. The remaining unobserved mass is probably in the form of dark-matter halos that surround the galaxies in these clusters. Hot intergalactic gases in rich clusters account for a small part of the unobserved mass. These gases are detected by their X-ray emission. The remaining unobserved mass is probably in the form of dark-matter halos that surround the galaxies in these clusters. Gravitational lensing of remote galaxies by a foreground cluster enables astronomers to glean information about the distribution of dark matter in the foreground cluster. Gravitational lensing of remote galaxies by a foreground cluster enables astronomers to glean information about the distribution of dark matter in the foreground cluster.

Key Ideas Formation and Evolution of Galaxies: Observations indicate that galaxies arose from mergers of several smaller gas clouds. Formation and Evolution of Galaxies: Observations indicate that galaxies arose from mergers of several smaller gas clouds. Whether a protogalaxy evolves into a spiral galaxy or an elliptical galaxy depends on its initial rate of star formation. Whether a protogalaxy evolves into a spiral galaxy or an elliptical galaxy depends on its initial rate of star formation.