But… If the temperature is constant, the local CMB consists of a series of increasingly redshifted Blackbody curves and so the final result will not be ‘perfect’
So, at what redshift were they ‘touching’ - assuming expansion?
dN/dZ = 6600 Z = 29
Or 46x109 years!
I was expecting it to be sort of a cut-and-dried 'constant' all the way from high-z; I wasn't actually expecting it to indicate (in a non-static interpretation) a slowdown effect in the more recent past, rather opposite what would be expected in an expanding universe. (Do I have that right? cf. the graph on p.13 of the presentation)
The Doppler parameter table was pretty interesting, but I must ask: why are the error bars so large? Why is it so hard to measure b properly?
I was having a bit of trouble understanding that. Do you mean to say that the scale of this effect would be representative of the 'inhomogeneities' of the CMB? How would we know?
Doesn't mainstream cosmology have some means of normalizing redshifts such that z -> infinite as t -> (13.7 Gya)?
This is very interesting piece of work, Lyndon.
Redshift -> infinity when v -> c. That follows from relativistic Doppler effect, see Wikipedia's article on redshift. But of course, when dealing with mainstream cosmology, you should use BB theory's cosmological redshift equation.
But it is more complicated than that. If z -> infinity dz does too. But dN ->0 so what is dN/dz then? Ergo, what is zero divided by infinity?I was just extrapolating back. Perhaps i need to go by size of universe at different z's? I will look into it.
And yet the H1 clouds have increasing redshifts but are, on average, equally spaced in this region. How do we explain that?
I use redshift as a distance indicator. If its about 1 billion year per z = 1 now then we should be able to extrapolate back and find the age to the end of inflation. They use inflation, i don't. my estimate is an underestimate.
seem to get a good fit with their simulation and observations
Dave et al (1999) have explained that this break is due to a steep decline of the ionizing background intensity from z =1 to 0. Thus, we assume a break at z=1 in the functional form of f(z).
We take the evolution of j directly from HM who calculated the intensity based solely on the observed quasar population at various epochs.
The intensity of the UV background drops at z <2 because of the declining quasar population so that the lower recombination rate at low redshifts is countered by a lower photoionization rate.
we conclude that the decrease of the weaker lines is decelerated in the phase z = 1 − 2, turning into a nearly flat evolution for z -> 0, without showing any hint for a sharp break in the evolution.
Janknecht et al. said:
we conclude that the decrease of the weaker lines is decelerated in the phase z = 1 − 2, turning into a nearly flat evolution for z -> 0, without showing any hint for a sharp break in the evolution.
Powered by mwForum 2.15.0 © 1999-2008 Markus Wichitill