Universe: Stars And Galaxies
6th Edition
ISBN: 9781319115098
Author: Roger Freedman, Robert Geller, William J. Kaufmann
Publisher: W. H. Freeman
expand_more
expand_more
format_list_bulleted
Concept explainers
Question
Chapter 6, Problem 43Q
To determine
The reason for image of the sky at the range of radiowaves in Figure (b) and the image of the sky at the range of radiowaves in Figure (d) to reveal the presence of cool gas in the Milky Way and whether one could infer the presence of this gas from the visible-light image in Figure (a).
Expert Solution & Answer
Want to see the full answer?
Check out a sample textbook solutionStudents have asked these similar questions
A)The star 58 Eridani is a feint but naked-eye star similar to the Sun. Suppose that you are observing this star in the night sky without a telescope. Ignoring any interstellar extinction or atmospheric absorption, approximately how many photons per second arrive at your retina? Show all steps in calculation .
B) The Mid-infared Instrument (MIRI , camera and spectrograph ) on the James Webb Space Telescope operates in the band 5-28 µm . For 58 Eridani , approximatley how many photons per second can be used by this instrument ? Assume that MIRI takes all the photons from the full JWST mirror . Show all steps in calcultation .
Describe breifly two or three other factors which play a role in determining the sensetivitu of an instrument such as MIRI ?
5=>
The wve n of h ē in H-dtem ca,
of ch e in H-dtom ia,
Us ing wave fns
6).Usina Ansbection, Find vallue of Q-no l ond ml ?
li).cebalting on this wave fr with z
iic) Exblain how it is that You
exbectation
wthout
Angular part of
fn with Iz
Find seult&me?
Cen detesmine
vallue of ohzular man stem 8queated
ofcater dioecthy, ?
1ging :20
e4-
Sinc
(sine
t sinto
%3D
263
Cas A SNR North Lobe
Chandra ACIS image
(M. Stage)
region of spectrum->
104
km/s (be sure to convert your answer to kilometers!)
(Enter a positive value--if you get a negative answer ignore the minus sign.)
1000
100
Combine counts / Ang./ (0.964324 sq. arcsec)
10
0.1
Cas A Ms Spectrum from 4362.5 4458.5, region size 0.964324 sq. arcsec
Mapangh
5
Silicon line
10
20
Wavelength (Angstroms)
The speed of the material ejected in a supernova can be measured by using the Doppler shift of the X-ray emission lines in its spectrum. The images above show real X ray data of the Cassiopeia A supernova remnant and a spectrum extracted from that data--you can see several emission lines
including the silicon line near 6.6 angstroms (0.66 nm).
If the emission line created by silicon normally has a wavelength of 0.6648 nm (nanometers), but is measured in the spectrum to have a wavelength of 0.6611 nm, how fast is the gas moving?
Chapter 6 Solutions
Universe: Stars And Galaxies
Ch. 6 - Prob. 1QCh. 6 - Prob. 2QCh. 6 - Prob. 3QCh. 6 - Prob. 4QCh. 6 - Prob. 5QCh. 6 - Prob. 6QCh. 6 - Prob. 7QCh. 6 - Prob. 8QCh. 6 - Prob. 9QCh. 6 - Prob. 10Q
Ch. 6 - Prob. 11QCh. 6 - Prob. 12QCh. 6 - Prob. 13QCh. 6 - Prob. 14QCh. 6 - Prob. 15QCh. 6 - Prob. 16QCh. 6 - Prob. 17QCh. 6 - Prob. 18QCh. 6 - Prob. 19QCh. 6 - Prob. 20QCh. 6 - Prob. 21QCh. 6 - Prob. 22QCh. 6 - Prob. 23QCh. 6 - Prob. 24QCh. 6 - Prob. 25QCh. 6 - Prob. 26QCh. 6 - Prob. 27QCh. 6 - Prob. 28QCh. 6 - Prob. 29QCh. 6 - Prob. 30QCh. 6 - Prob. 31QCh. 6 - Prob. 32QCh. 6 - Prob. 33QCh. 6 - Prob. 34QCh. 6 - Prob. 35QCh. 6 - Prob. 36QCh. 6 - Prob. 37QCh. 6 - Prob. 38QCh. 6 - Prob. 39QCh. 6 - Prob. 40QCh. 6 - Prob. 41QCh. 6 - Prob. 42QCh. 6 - Prob. 43QCh. 6 - Prob. 44QCh. 6 - Prob. 45Q
Knowledge Booster
Learn more about
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
- Cas A SNR North Lobe Chandra ACIS image (M. Stage) region of spectrum-> 10* km/s (be sure to convert your answer to kilometers!) (Enter a positive value--if you get a negative answer ignore the minus sign.) 1000 100 Combine counts / Ang./ (0.964324 sq. arcsec) 10 1 0.1 Cas A Ms Spectrum from 4362.5 4458.5, region size 0.964324 sq. arcsec Silicon line werden der 5 10 20 Wavelength (Angstroms) The speed of the material ejected in a supernova can be measured by using the Doppler shift of the X-ray emission lines in its spectrum. The images above show real X ray data of the Cassiopeia A supernova remnant and a spectrum extracted from that data--you can see several emission lines including the silicon line near 6.6 angstroms (0.66 nm). If the emission line created by silicon normally has a wavelength of 0.6648 nm (nanometers), but is measured in the spectrum to have a wavelength of 0.6599 nm, how fast is the gas moving?arrow_forwardI need urgent answers on the photo provided here pls. Thank you so much.arrow_forward5. The two images below show a portion of the Trifid Nebula. The image on the left was made with visible light, while the image on the right (shown to the same scale) is an infrared image from the Spitzer Space Telescope. Explain why the dark streaks in the visible-light image appear bright in the infrared image. (a) Reflection nebula, Dust lanes Emission nebula. R I 10 pc www V U X G (b) wwwwww R V U X Garrow_forward
- E A X X Math M Inbo b Last Class N Netf + Prob Logir M Inbo 4 Good #3 Grou Mail y! CVX EHL 4 fre ET Wha G neve docs.google.com/document/d/1UpdqZs7NIZ-YyjMagyW1hbk0T5S2ZUBluFm-OB5PACA/edit M AST1002001FALL2017PS7 ☆ Request edit access Share File Edit View Tools Help BINARY STARS 31 Problem 5. Binary star systems: Center of mass. (Palen, et. al. Chp. 10 1st Ed. Problem 65) d2 m, = 3m, The center of mass is where the fulcrum of a balance must be. m2 %3D dz = 3d, FIGURE 10.15 The center of mass of two objects is the "balance" point on a line joining the centers of two masses. Study Figure 10.15 in the text (1st ed.). Where would the center of mass be located if а) т — т? b) M¡ = 2m,? c) 2m2= 3m,? 11:50 PM e Type here to search 3/4/2021 + (8) IIarrow_forwardE A X M Inbo b Last Class N Netf + Prob Logir | X Math M Inbo Good #3 Mail y! CVX ET Wha 4 Grou EHL 4 fre G neve docs.google.com/document/d/1UpdqZs7NIZ-YyjMagyW1hbk0T5S2ZUBluFm-OB5PACA/edit M AST1002001FALL2017PS7 ☆ A Request edit access Share File Edit View Tools Help Problem 3. Brightness and Luminosity 31 The brightness or flux intensity of a star at an observer's location may be determined by measuring the rate at which its light enters the aperture of an observing instrument (this is referred to as photometry). We will call this "" (with units [Energy/time/Area] or [Watts/Area]). Imagine a sphere of radius, d (labeled "p" in the figure below), equal to the star's distance from the observer's location, at which the star is at the center (see the figure below). ALL of the star's light passes through the surface area of this sphere but only a small fraction passes through the instrument aperture. The fraction of the star's rate of light energy emission measured by the instrument is…arrow_forwarda) The star 58 Eridani is a feint but naked-eye star similar to the Sun. Suppose that you are observing this star in the night sky without a telescope. Ignoring any interstellar extinction or atmospheric absorption, approximately how many photons per second arrive at your retina? Show all steps in your calculation. Look up any required information about the star using Wikipedia. Use sensible approximations so your calculation is straightforward. For example you could consider only the region of the spectrum where the photon flux peaks. b) The Mid-Infrared Instrument (MIRI, camera and spectrograph) on the James Webb Space Telescope operates in the band 5 – 28 µm. For 58 Eridani, approximately how many photons per second can be used by this instrument? Assume that MIRI takes all the photons from the full JWST mirror. Show all steps in your calculation. Describe briefly two or three other factors which play a role in determining the sensitivity of an instrument such as MIRI?arrow_forward
- Background: Design and completely analyze an optical system to measure how fast the Sun is spinning,based on the Doppler shift between the west side of the sun (always turning toward us atvelocity v1) and the east side (turning away from us, also at velocity v1). It turns out the Sun hasvery sharp emission lines at a wavelength of λ = 630.0 nm. You may ignore Earth’s rotation andatmosphere.You’ll need at least 2 parts in your optical system. First, you’ll need to gather (maybe focus,maybe magnify?) the light from only the outer edge of the sun—no more than 5% of itsdiameter as seen from Earth. Be sure your system blocks out the rest of the sun when taking ameasurement of one side or the other. Second, you’ll need to very precisely and accuratelyseparate the sun’s spectrum into different wavelengths so you can measure the difference inwavelength caused by the Doppler shifts. You can use any combination of any optical elementswe have discussed in class: lenses, mirrors, pinholes,…arrow_forwardDon’t worry about the K - images. Just focus on the figure 1 providedarrow_forwardIm studying this laboratory example and I can not figure out where the 30mA came from? An explanation would be great~arrow_forward
- . How are we able to determine the chemical composition and temperature of any visible object? ite often advertisements appear for telescopes that extol their aluating telescopes? enifviarrow_forwardLongs Van aw rejtoug] - consider a liquid mixture of components 1,2, 3, 4. The excess Gibbo energies of all the binaries, formed by these components obey relations of the formi Aijxjxj G₁₁ RT where Alj is the const characteristic of the i-j binary. Desire an expression for the co-efficient of component-I in the quaternary solution. وعاد سامانه . NL = enemical Engg Thermodyamies Question Torture TA gif croftrum svedo sitarrow_forwardExplain what is an excitation table?arrow_forward
arrow_back_ios
SEE MORE QUESTIONS
arrow_forward_ios
Recommended textbooks for you
- Stars and GalaxiesPhysicsISBN:9781305120785Author:Michael A. Seeds, Dana BackmanPublisher:Cengage LearningHorizons: Exploring the Universe (MindTap Course ...PhysicsISBN:9781305960961Author:Michael A. Seeds, Dana BackmanPublisher:Cengage LearningStars and Galaxies (MindTap Course List)PhysicsISBN:9781337399944Author:Michael A. SeedsPublisher:Cengage Learning
- Foundations of Astronomy (MindTap Course List)PhysicsISBN:9781337399920Author:Michael A. Seeds, Dana BackmanPublisher:Cengage Learning
Stars and Galaxies
Physics
ISBN:9781305120785
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
Horizons: Exploring the Universe (MindTap Course ...
Physics
ISBN:9781305960961
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
Stars and Galaxies (MindTap Course List)
Physics
ISBN:9781337399944
Author:Michael A. Seeds
Publisher:Cengage Learning
Foundations of Astronomy (MindTap Course List)
Physics
ISBN:9781337399920
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
General Relativity: The Curvature of Spacetime; Author: Professor Dave Explains;https://www.youtube.com/watch?v=R7V3koyL7Mc;License: Standard YouTube License, CC-BY