For Expanding Universe, with look back times to where Universe was noticeably different (density and...
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Transcript of For Expanding Universe, with look back times to where Universe was noticeably different (density and...
• For Expanding Universe, with look back times to where Universe was noticeably different (density and expansion rate),
• Will see effects of expansion and D will be complex
• D will depend on 1+z, and m
• Make observations of D versus 1+z
• Fit curves based on different amounts to and m
• Extract the best fit • Never proves a model• Demonstrates a model is consistent (or not) with observations
• SNe are bright so can see far enough away to see effects of change in expansion rate of universe
• SNe Ia are “easy” to calibrate
Take case of where D is simple
D = velocity/(Hubble “Constant”) ; D = V/H
• H is a measure of expansion rate, higher H higher expansion. H0 = expansion rate now
• H0 is what we measure out to z = about 0.1
• for z in this range z = V/c where c = speed of light => z <=> V
• If universe has been slowing down in expansion
• Means higher H in past.
• For a given H0 and m we infer how fast the slow down =>
• H0 <=> m
• H0 and m give D
• But suppose in last billion years expansion has speeded up?
• Then H0 we see is higher than the value we should be using => we calculate D too low
• => calculate expected F too high, F = L/4D2
• When we look, find SNe Ia fainter than expected if m were 1
• m low (0.2) is better, but
• Still not good because D versus 1+z is complex due to acceleration ()
Positive means fainter
SNe Ia fainter than expected
velocity
Sub from all and the result re-plotted below
• Need to calibrate several effects seen
• SNe people have done a very thorough job
• One of “coolest” things is they see affect of “time dilation” (cf. Book pages 174-177)
• Things moving faster appear to have slower moving clocks
• If we take 1+z to be a relative velocity with respect to us, we get the right answer for the SN light versus time!
• Special relativity works; the model all hangs together
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More sample light curves
• Fig.1: UBVRI and Bolometric Light Curves of SN 1994D, from Vacca & Leibundgut (1996). Solid lines are the best fits of the model to the data; residuals are plotted below each panel. Dashed lines are the commonly used templates for Type Ia light curves.
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