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all functions  l
lbs

lbs
returns linear b spline
in 1,2,3,4 D
EXAMPLE
> lbs([1.,0.5,0,0.5,1])
[0,0.5,1,0.5,0]
interpreted function, defined at ./histon.i line 6

SEE ALSO:


ldist

ldist(z,q0=,lambda0=)
Compute the term to integrate to compute the luminosity
distance. z can be a VECTOR of values.
KEYWORDS: q0 : Deceleration parameter,numeric scalar
a*(a'')/(a')^2 (Omega_m/2lambda0)
lambda0 : Cosmological constant, normalized to
th closure density.
interpreted function, defined at ./cosmo.i line 104

SEE ALSO:

lumdist

lumdist

lumdist(z,h0=,k=,lambda0=,Omega_m=,q0=,silent=)
See IDL routine...
PURPOSE:
Calculate luminosity distance (in Mpc) of an object given its redshift
EXPLANATION:
The luminosity distance in the FriedmannRobertsonWalker model is
taken from Caroll, Press, and Turner (1992, ARAA, 30, 499), p. 511
Uses a closed form (Mattig equation) to compute the distance when the
cosmological constant is zero. Otherwise integrates the function using
simpson_cosmo.
EXAMPLE:
Plot the distance of a galaxy in Mpc as a function of redshift out
to z = 5.0, assuming the default cosmology (Omega_m=0.3, Lambda = 0.7,
H0 = 70 km/s/Mpc)
z = span(0,5,50);
plg,lumdist(z),z;
xytitles,"z","Distance (Mpc)"
interpreted function, defined at ./cosmo.i line 162

SEE ALSO:

ldist

