Universe: Stars And Galaxies
Universe: Stars And Galaxies
6th Edition
ISBN: 9781319115098
Author: Roger Freedman, Robert Geller, William J. Kaufmann
Publisher: W. H. Freeman
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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).

Universe: Stars And Galaxies, Chapter 6, Problem 43Q

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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?
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