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The Einstein radius is the radius of an Einstein ring, and is a characteristic angle for gravitational lensing in general, as typical distances between images in gravitational lensing are of the order of the Einstein radius.

Derivation

In the following derivation of the Einstein radius, we will assume that all of mass M of the lensing galaxy L is concentrated in the center of the galaxy.

For a point mass the deflection can be calculated and is one of the classical tests of general relativity. For small angles α₁ the total deflection by a point mass M is given (see Schwarzschild metric) by

\alpha _{1}={\frac {4G}{c^{2}}}{\frac {M}{b_{1}}}

where

b₁ is the impact parameter (the distance of nearest approach of the lightbeam to the center of mass)

G is the gravitational constant,

c is the speed of light.

By noting that, for small angles and with the angle expressed in radians, the point of nearest approach b₁ at an angle θ₁ for the lens L on a distance d_L is given by b₁ = θ₁ d_L, we can re-express the bending angle α₁ as

\alpha _{1}(\theta _{1})={\frac {4G}{c^{2}}}{\frac {M}{\theta _{1}}}{\frac {1}{d_{\rm {L}}}}

(eq. 1)

If we set θ_S as the angle at which one would see the source without the lens (which is generally not observable), and θ₁ as the observed angle of the image of the source with respect to the lens, then one can see from the geometry of lensing (counting distances in the source plane) that the vertical distance spanned by the angle θ₁ at a distance d_S is the same as the sum of the two vertical distances θ_S d_S and α₁ d_LS. This gives the lens equation,

\theta _{1}\;d_{\rm {S}}=\theta _{\rm {S}}\;d_{\rm {S}}+\alpha _{1}\;d_{\rm {LS}}

,

which can be rearranged to give

\alpha _{1}(\theta _{1})={\frac {d_{\rm {S}}}{d_{\rm {LS}}}}(\theta _{1}-\theta _{\rm {S}})

(eq. 2)

By setting (eq. 1) equal to (eq. 2), and rearranging, we get

\theta _{1}-\theta _{\rm {S}}={\frac {4G}{c^{2}}}\;{\frac {M}{\theta _{1}}}\;{\frac {d_{\rm {LS}}}{d_{\rm {S}}d_{\rm {L}}}}

For a source right behind the lens, θ_S = 0, and the lens equation for a point mass gives a characteristic value for θ₁ that is called the Einstein radius, denoted θ_E. Putting θ_S = 0 and solving for θ₁ gives

\theta _{E}=\left({\frac {4GM}{c^{2}}}\;{\frac {d_{\rm {LS}}}{d_{\rm {L}}d_{\rm {S}}}}\right)^{1/2}

The Einstein radius for a point mass provides a convenient linear scale to make dimensionless lensing variables. In terms of the Einstein radius, the lens equation for a point mass becomes

\theta _{1}=\theta _{\rm {S}}+{\frac {\theta _{E}^{2}}{\theta _{1}}}

Substituting for the constants gives

\theta _{E}=\left({\frac {M}{10^{11.09}M_{\bigodot }}}\right)^{1/2}\left({\frac {d_{\rm {L}}d_{\rm {S}}/d_{\rm {LS}}}{\rm {Gpc}}}\right)^{-1/2}{\rm {arcsec}}

In the latter form, the mass is expressed in solar masses (M_☉ and the distances in Gigaparsec (Gpc). The Einstein radius most prominent for a lens typically halfway between the source and the observer.

For a dense cluster with mass M_c ≈ 10×10¹⁵ M_☉ at a distance of 1 Gigaparsec (1 Gpc) this radius could be as large as 100 arcsec (called macrolensing). For a Gravitational microlensing event (with masses of order 1 M_☉) search for at galactic distances (say d ~ 3 kpc), the typical Einstein radius would be of order milli-arcseconds. Consequently separate images in microlensing events are impossible to observe with current techniques.

The argument above can be extended for lenses which have a distributed mass, rather than a point mass, by using a different expression for the bend angle α. The positions θ_I(θ_S) of the images can then be calculated. For small deflections this mapping is one-to-one and consists of distortions of the observed positions which are invertible. This is called weak lensing. For large deflections one can have multiple images and a non-invertible mapping: this is called strong lensing. Note that in order for a distributed mass to result in an Einstein ring, it must be axially symmetric.

References

Chwolson, O (1924). "Über eine mögliche Form fiktiver Doppelsterne". Astronomische Nachrichten. 221 (20): 329–330. Bibcode:1924AN....221..329C. doi:10.1002/asna.19242212003. (The first paper to propose rings)
Einstein, Albert (1936). "Lens-like Action of a Star by the Deviation of Light in the Gravitational Field". Science. 84 (2188): 506–507. Bibcode:1936Sci....84..506E. doi:10.1126/science.84.2188.506. JSTOR 1663250. PMID 17769014. (The famous Einstein Ring paper)
Renn, Jurgen (1997). "The Origin of Gravitational Lensing: A Postscript to Einstein's 1936 Science paper". Science. 275 (5297): 184–186. Bibcode:1997Sci...275..184R. doi:10.1126/science.275.5297.184. PMID 8985006. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)

@@ Line 5: / Line 5: @@
 In the following derivation of the Einstein radius, we will assume that all of mass ''M'' of the lensing galaxy ''L'' is concentrated in the center of the galaxy.
-For a point mass the deflection can be calculated and is one of the classical [[tests of general relativity]]. For small angles ''α'' the total deflection by a point mass ''M'' is given (see [[Schwarzschild metric]]) by
+For a point mass the deflection can be calculated and is one of the classical [[tests of general relativity]]. For small angles ''α''<sub>1</sub> the total deflection by a point mass ''M'' is given (see [[Schwarzschild metric]]) by
-:<math>\alpha = \frac{4G}{c^2}\frac{M}{b}</math>
+:<math>\alpha_1 = \frac{4G}{c^2}\frac{M}{b_1}</math>
 where
-: ''b'' is the [[impact parameter]] (the distance of nearest approach of the lightbeam to the center of mass)
+: ''b''<sub>1</sub> is the [[impact parameter]] (the distance of nearest approach of the lightbeam to the center of mass)
 : ''G'' is the [[gravitational constant]],
 : ''c'' is the [[speed of light]].
-By noting that, for small angles and with the angle expressed in [[radian]]s, the point of nearest approach ''b'' at an angle ''θ'' for the lens ''L'' on a distance  ''d<sub>L</sub>'' is given by {{nowrap|''b'' {{=}} ''θ'' ''d<sub>L</sub>''}}, we can re-express the bending angle ''α'' as
+By noting that, for small angles and with the angle expressed in [[radian]]s, the point of nearest approach ''b''<sub>1</sub> at an angle ''θ''<sub>1</sub> for the lens ''L'' on a distance  ''d''<sub>L</sub> is given by {{nowrap|''b''<sub>1</sub> {{=}} ''θ''<sub>1</sub> ''d''<sub>L</sub>}}, we can re-express the bending angle ''α''<sub>1</sub> as
-:<math>\alpha(\theta) = \frac{4G}{c^2}\frac{M}{\theta}\frac{1}{d_L}</math> (eq. 1)
+:<math>\alpha_1(\theta_1) = \frac{4G}{c^2}\frac{M}{\theta_1}\frac{1}{d_{\rm L}}</math>   (eq. 1)
-If we set ''θ<sub>S</sub>'' as the angle at which one would see the source without the lens (which is generally not observable), and ''θ'' as the observed angle of the image of the source with respect to the lens, then one can see from the geometry of lensing (counting distances in the source plane) that the vertical distance spanned by the angle ''θ'' at a distance ''d<sub>S</sub>'' is the same as the sum of the two vertical distances {{nowrap|''θ<sub>S</sub>'' ''d<sub>S</sub>''}} and {{nowrap|''α'' ''d<sub>LS</sub>''}}. This gives the '''[[lens equation]]''',
+If we set ''θ''<sub>S</sub> as the angle at which one would see the source without the lens (which is generally not observable), and ''θ''<sub>1</sub> as the observed angle of the image of the source with respect to the lens, then one can see from the geometry of lensing (counting distances in the source plane) that the vertical distance spanned by the angle ''θ''<sub>1</sub> at a distance ''d''<sub>S</sub> is the same as the sum of the two vertical distances {{nowrap|''θ''<sub>S</sub> ''d''<sub>S</sub>}} and {{nowrap|''α''<sub>1</sub> ''d''<sub>LS</sub>}}. This gives the '''[[lens equation]]''',
-:<math>\theta \; d_S = \theta_S\; d_S + \alpha \; d_{LS}</math>,
+:<math>\theta_1 \; d_{\rm S} = \theta_{\rm S}\; d_{\rm S} + \alpha_1 \; d_{\rm LS}</math>,
 which can be rearranged to give
-:<math>\alpha(\theta) = \frac{d_S}{d_{LS}} (\theta - \theta_S)</math> (eq. 2)
+:<math>\alpha_1(\theta_1) = \frac{d_{\rm S}}{d_{\rm LS}} (\theta_1 - \theta_{\rm S})</math>   (eq. 2)
 By setting (eq. 1) equal to (eq. 2), and rearranging, we get
-:<math>\theta-\theta_S = \frac{4G}{c^2} \; \frac{M}{\theta} \; \frac{d_{LS}}{d_S d_L}</math>
+:<math>\theta_1-\theta_{\rm S} = \frac{4G}{c^2} \; \frac{M}{\theta_1} \; \frac{d_{\rm LS}}{d_{\rm S} d_{\rm L}}</math>
-For a source right behind the lens, {{nowrap|''θ<sub>S</sub>'' {{=}} 0}}, and the lens equation for a point mass gives a characteristic value for ''θ'' that is called the '''Einstein radius''', denoted ''θ<sub>E</sub>''. Putting {{nowrap|''θ<sub>S</sub>'' {{=}} 0}} and solving for ''θ'' gives
+For a source right behind the lens, {{nowrap|''θ''<sub>S</sub> {{=}} 0}}, and the lens equation for a point mass gives a characteristic value for ''θ''<sub>1</sub> that is called the '''Einstein radius''', denoted ''θ''<sub>E</sub>. Putting {{nowrap|''θ''<sub>S</sub> {{=}} 0}} and solving for ''θ''<sub>1</sub> gives
-:<math>\theta_E = \left(\frac{4GM}{c^2}\;\frac{d_{LS}}{d_L d_S}\right)^{1/2}</math>
+:<math>\theta_E = \left(\frac{4GM}{c^2}\;\frac{d_{\rm LS}}{d_{\rm L} d_{\rm S}}\right)^{1/2}</math>
 The Einstein radius for a point mass provides a convenient linear scale to make dimensionless lensing variables. In terms of the Einstein radius, the lens equation for a point mass becomes
-:<math>\theta = \theta_S + \frac{\theta^2_E}{\theta}</math>
+:<math>\theta_1 = \theta_{\rm S} + \frac{\theta_E^2}{\theta_1}</math>
 Substituting for the constants gives
-:<math>\theta_E = \left(\frac{M}{10^{11.09} M_{\bigodot}}\right)^{1/2} \left(\frac{d_L d_S/ d_{LS}}{Gpc}\right)^{-1/2}  arcsec</math>
+:<math>\theta_E = \left(\frac{M}{10^{11.09} M_{\bigodot}}\right)^{1/2} \left(\frac{d_{\rm L} d_{\rm S}/ d_{\rm LS}}{\rm{Gpc}}\right)^{-1/2} \rm{arcsec}</math>
 In the latter form, the mass is expressed in [[solar mass]]es (M<sub>☉</sub> and the distances in Giga[[parsec]] (Gpc). The Einstein radius most prominent for a lens typically halfway between the source and the observer.
 For a dense cluster with mass {{nowrap|M<sub>c</sub> ≈ {{val|10|e=15|u=M<sub>☉</sub>}}}} at a distance of 1 Gigaparsec (1 Gpc) this radius could be as large as 100 arcsec (called '''[[macrolensing]]'''). For a [[Gravitational microlensing]] event (with masses of order {{val|1|u=M<sub>☉</sub>}}) search for at galactic distances (say {{nowrap|''d'' ~ {{val|3|u=kpc}}}}), the typical Einstein radius would be of order milli-arcseconds. Consequently separate images in microlensing events are impossible to observe with current techniques.
-The argument above can be extended for lenses which have a distributed mass, rather than a point mass, by using a different expression for the bend angle α. The positions ''θ<sub>I</sub>''(''θ<sub>S</sub>'')'' of the images can then be calculated. For small deflections this mapping is one-to-one and consists of distortions of the observed positions which are invertible. This is called '''[[weak lensing]]'''. For large deflections one can have multiple images and a non-invertible mapping: this is called '''[[strong lensing]]'''. Note that in order for a distributed mass to result in an Einstein ring, it must be axially symmetric.
+The argument above can be extended for lenses which have a distributed mass, rather than a point mass, by using a different expression for the bend angle α. The positions ''θ''<sub>I</sub>(''θ''<sub>S</sub>) of the images can then be calculated. For small deflections this mapping is one-to-one and consists of distortions of the observed positions which are invertible. This is called '''[[weak lensing]]'''. For large deflections one can have multiple images and a non-invertible mapping: this is called '''[[strong lensing]]'''. Note that in order for a distributed mass to result in an Einstein ring, it must be axially symmetric.
 == References ==

Revision as of 11:15, 1 February 2013

Derivation

References

See also