z =
λ(obs)-λ(em)/λ(em)
v(rec) =
H(0)d
v(obs) =
H(0)d + v(pec)
r(t) =
a(t) x s
H(t) =
a(dot)/a
a^3(t)p(t) =
a^3(t(0))p(t(0)) = p(0)
Ω(t) =
p(t)/p(c)(t)
p(dot) + ∇ . (pv(v)) = - P/c^2 ∇ . v(v)
where RHS is the relativistic correction
p = p(0) + U/c^2
mass continuity
p(dot) + 3(p + P/c^2)H = 0
equation of state P(p) =
{Kp^5/3 adiabatic case
{Kp isothermal case
Visible stars in the Milky way p =
N(stars) x M(sun) / volume of Milky Way
Keplers third law
GM(gal)P^2 = 4π^2a^3
<v^2> =
<v(radial)^2> = 3σ^2
v^2(rot)/R =
GM/R^2
where M = 4/3 π p R^2