MODERN COSMOLOGY

(Axel Boer) #1
Simple lens models 391

forθ ≥0. Due to the axial symmetry it is enough to considerβ≥0. Since
m(θ)≥0 it follows thatθ≥β(forθ≥0). Instead of equation (14.34) we get


+(θ)= 2

∫θ

0

θ′dθ′k(θ′)ln

(


θ
θ′

)


, (14.55)


whereas the Fermat potential can be written as


(θ,β)=^12 (θ−β)^2 −+(θ). (14.56)

This way we get the lens equation (14.54) from


∂(θ,β)
∂θ

= 0. (14.57)


To get the Jacobi matrix we write:


α(θ)=

m(θ)
θ^2

θ (withθ=(θ 1 ,θ 2 )andθ=|θ|)

and thus


A=

(


10


01


)



m(θ)
θ^4

(


θ 22 −θ 12 − 2 θ 1 θ 2
− 2 θ 1 θ 2 θ 12 −θ 22

)



2 k(θ)
θ^2

(


θ 12 θ 1 θ 2
θ 1 θ 2 θ 22

)


, (14.58)


wherewemadeuseofm′(θ)= 2 θk(θ). The determinant of the Jacobi matrix is
given by


detA=

(


1 −


m
θ^2

)(


1 −


d

(m
θ

))


=


(


1 −


m
θ^2

)(


1 +


m
θ^2

− 2 k

)


. (14.59)


14.3.1.1 Tangential and radial critical curves


The critical curves (the points for which detA(θ)=0) are then circles of radius
θ. From equation (14.59) we see that there are two possible cases:


(1) θm 2 =1 : defined astangential critical curve;and
(2) ddθ(mθ)=1: defined asradial critical curve.

For case (1) one getsm/θ=θand thus from the lens equation (14.54) we
see thatβ=0 is the corresponding caustic, which reduces to a point. If the axial
symmetric gets only slightly perturbed this degeneracy is lifted.
We can look at the critical points on theθ 1 -axis withθ=(θ, 0 ),θ >0. Then


A= 1 −


m(θ)
θ^2

(


− 10


0 + 1


)



m′
θ

(


10


00


)


(14.60)


and this matrix must have an eigenvectorXwith eigenvalue zero. For symmetry
reasons, the vector must be either tangential,X=( 0 , 1 ), or normal,X=( 1 , 0 ),

Free download pdf