UNIVERSE LL W/SAPLINGPLUS MULTI SEMESTER
11th Edition
ISBN: 9781319278670
Author: Freedman
Publisher: MAC HIGHER
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Chapter 23, Problem 18Q
To determine
The usefulness of Type Ia supernovae to find the distances to remote galaxies and also explain if they are applicable in finding the distance to any galaxy.
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Students have asked these similar questions
What is the redshift z of a galaxy 172 Mpc away from us?
Note: Assume a value of the Hubble constant of 71.1 km/s/Mpc
Round your answer to three decimal places.
Compute the gravitational energy of a pair of colliding galaxies , each of mass 10 Mo separated by a distance of 10 kpc and compare it with the energy requirements of a powerful radio source . What conclusion do you arrive at from such a comparison
A galaxy at redshift z has an infrared luminosity of LIR. What is the approximate star formation rate of the galaxy? Express your answer in solar masses per year, rounding to the nearest integer.
Values:
z = 0.3
LIR = 15.9
×
1
0
37
×10
37
W
Chapter 23 Solutions
UNIVERSE LL W/SAPLINGPLUS MULTI SEMESTER
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Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- Why are quasars generally so much more luminous (why do they put out so much more energy) than active galaxies?arrow_forwardWhat are the two best ways to measure the distance to a distant, isolated spiral galaxy, and how would it be measured?arrow_forwardWhat is the most useful standard bulb method for determining distances to galaxies?arrow_forward
- When comparing two isolated spiral galaxies that have the same apparent brightness, but rotate at different rates, what can you say about their relative luminosity?arrow_forwardGiven that only about 5% of the galaxies visible in the Hubble Deep Field are bright enough for astronomers to study spectroscopically, they need to make the most of the other 95%. One technique is to use their colors and apparent brightnesses to try to roughly estimate their redshift. How do you think the inaccuracy of this redshift estimation technique (compared to actually measuring the redshift from a spectrum) might affect our ability to make maps of large-scale structures such as the filaments and voids shown in Figure 28.21? Figure 28.21 Sloan Digital Sky Survey Map of the Large-Scale Structure of the Universe. This image shows slices from the SDSS map. The point at the center corresponds to the Milky Way and might say “You Are Here!” Points on the map moving outward from the center are farther away. The distance to the galaxies is indicated by their redshifts (following Hubble’s law), shown on the horizontal line going right from the center. The redshift z=/ , where is the difference between the observed wavelength and the wavelength emitted by a nonmoving source in the laboratory. Hour angle on the sky is shown around the circumference of the circular graph. The colors of the galaxies indicate the ages of their stars, with the redder color showing galaxies that are made of older stars. The outer circle is at a distance of two billion light-years from us. Note that red (older stars) galaxies are more strongly clustered than blue galaxies (young stars). The unmapped areas are where our view of the universe is obstructed by dust in our own Galaxy. (credit: modification of work by M. Blanton and the Sloan Digital Sky Survey)arrow_forwardDescribe the arguments supporting the idea that quasars are at the distances indicated by their redshifts.arrow_forward
- Why don’t any of the methods for establishing distances to galaxies, described in Galaxies (other than Hubble’s law itself), work for quasars?arrow_forwardCan an elliptical galaxy evolve into a spiral? Explain your answer. Can a spiral turn into an elliptical? How?arrow_forwardWhy can we not determine distances to galaxies by the same method used to measure the parallaxes of stars?arrow_forward
- Once again in this chapter, we see the use of Kepler’s third law to estimate the mass of supermassive black holes. In the case of NGC 4261, this chapter supplied the result of the calculation of the mass of the black hole in NGC 4261. In order to get this answer, astronomers had to measure the velocity of particles in the ring of dust and gas that surrounds the black hole. How high were these velocities? Turn Kepler’s third law around and use the information given in this chapter about the galaxy NGC 4261-the mass of the black hole at its center and the diameter of the surrounding ring of dust and gas-to calculate how long it would take a dust particle in the ring to complete a single orbit around the black hole. Assume that the only force acting on the dust particle is the gravitational force exerted by the black hole. Calculate the velocity of the dust particle in km/s.arrow_forwardDistances to local galaxies are determined by measuring the brightness of stars, called Cepheid variables, that can beobserved individually and that have absolute brightnesses at a standard distance that are well known. Explain how the measuredbrightness would vary with distance as compared with the absolute brightness.arrow_forwardA certain galaxy is observed to be receding from the Sun at a rate of 8000 km/sec. The distance to this Galaxy I measured independently and found to be 1.4 x 10 to the eighth power pc. Using these data , what is the value of the Hubble constant ?arrow_forward
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