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Download Astronomy 275 Lecture Notes, Spring 2009 by Edward L. Wright, Phd, UCLA PDF

By Edward L. Wright, Phd, UCLA

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We can also ask a very different question: for a source with fixed comoving distance, how does the redshift vary with observation time? In this case the emission time varies as a function of the observation time to satisfy the light speed constraint. In principle this is a way to directly measure the deceleration parameter of the Universe (Loeb, 1998 astro-ph/9802122). In order to calculate the rate at which observed redshifts for comoving objects will change, we need to carry Eqn(32) to the next higher order, and in this order we need to use a(te + ∆te ) = a(te )(1 + H(te )∆te + .

Data. 44 Since there are a large number of supernovae a plot showing all of the data points is not very informative, because the errorbars cover the graph with black ink. So it is easier to see the effect and the differences between models in a plot like Fig 15 which uses binned normal points and subtracts a fiducial model from the DM values. 1 Redshift z 1 Fig. — Distance modulus vs. redshift for high redshift Type Ia supernovae. Data are taken from the Union catalog published by Kowalski et al.

Redshift for high redshift Type Ia supernovae. Data have been binned into normal points and only the difference between the distance modulus and an empty Universe are shown. 87. The differences between models are clear on this plot. 48 10. Number Counts One kind of cosmological observation is the number versus flux law, N(S). We can compute the expected N(S) law for various cosmological models using the distances dA and dL . The physical volume of the shell between redshift z and z + dz is given by the surface area of the sphere which is 4πdA (z)2 times the thickness of the shell which is (cdt/dz)dz.

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