CINESPA | Centro de Investigaciones Espaciales

The program * xfglenses* (Linux Version) needs the *XForms*, the *Mesa Libraries (OpenGL)* and the *Image Library.*

An old SGI version is also available: *gllenses*

Now, the source code is available *xfglenses.zip*

**Paper**

American Journal of Physics (February 2001 -- Volume 69, Issue 2, pp. 218-222)

ArXiv version of this paper.

**JLenses**

The Java version of XFGLenses, *JLenses* is now available. This new version was written by Hugo Solís Sánchez at the University of Costa Rica. A paper about it will appear soon. The source code is also available on request.

**Keeton's Interface**

An interface for Keeton's programs *gravlens* and lensmodel is almost ready. You also need *XForms* to run it.

**XFGLenses: The Control Panel**

The Control Panel interface has the following items:

Model Menu (22 models, see below)

Source Menu (Filled Circle, Coloured Rings and Image File)

Source Positioner

Three counters, two for source positioning (X, Y) and one for adjusting the pixel resolution (N)

Buttons (Model Parameters, Image Window, Image File, OBIP, Track, Source, Images, Smooth, Grid, Ray Plot, CC / Caustic (not yet), Roots, Fitting (final phase), R_E, Contour, Help, Save, Inversion, Light Curve (not yet), Time Delay, Exit)

Sliders (if a model is chosen, then the corresponding sliders appears)

The user can click the Image Window button to see the visualization.

**Model Menu**

When this menu is clicked with the mouse, one gets a list of models. If one chooses one model, then the required sliders appear on the control panel. The model menu has the following models:

Chang Refsdal,

Double Plane Lens,

Transparent Sphere,

Singular Isothermal Sphere (SIS),

Nonsingular Isothermal Sphere (NIS),

Elliptical Model (SEF Book),

King Model,

Truncated King Model,

Hubble Model,

De Vaucouleur Model,

Spiral Model,

Multipole Lens,

Rotation Lens (Ibañez),

Uniform Ring (SEF Book),

Second Order Schwarzschild,

Elliptic SIS,

Elliptic NIS,

Elliptic King,

Elliptic Hubble,

Elliptic Plummer (not yet),

Kassiola-Kovner and,

Barkana

**Source Menu**

There are three sources:

Filled Circle

Coloured Rings

Image File

You can load any image using the File button.

**Source Positioners**

For positioning the source there are two possibilities:

Source Positioner and

Two counters (X, Y) for fine positioning

**Input Fields**

With the input fields one can position the observed images of a real gravitational lens. The images are then represented through circles. One can also try to fit it by means of parameter variations of a chosen model.

**Buttons**

Seventeen buttons are available:

Image Window : When clicking this button the Image Window appears.

Model Parameters : To disappear the sliders

Source : To visualize the source

Images : To visualize the images

Smooth : To smooth the lens images

Ray Plot : To show the Ray Plot

R_E : To dipect the Eintein Ring

Image File : To load an image File

OBIP : To show the observed image positions of the browser by means of circles

Save : To save the model images using gimp

Grid : To visualize the grid

Help

Exit

**Image Window**

On this window all events are interactively shown

**OBIP**

By cliking this button, the user get a window to enter the image positions and the number of images of the Lens System.

Add : To add an observed image position on the browser

Replace: To replace an observed image position on the browser

Remove : to remove an observed image position on the browser

Clear : To clear the observed image positions

Add : To draw concentric circles that represent the lens images

Browser : The information about the position of the images appears in it.

**Sliders**

The parameters of the chosen model are adjusted be means of these sliders. There are six sliders which all models have:

E : Length scale

Theta: To rotate (X, Y) coordinates

Gamma: Shear of the macrolens

Sigma: Constant surface mass density of the macrolens

Phi : Shear angle

R : Radius of the source

**The Chang Refsdal Model**

For this model there are no additional sliders.

**The Double Plane Lens**

This model has the following additional sliders:

m1 : Point mass in the first lens plane

m2 : Point mass in the second lens plane

Beta: distance between both lens planes

x1 : X position component of the mass m1

y1 : Y position component of the mass m1

x2 : X position component of the mass m2

y2 : Y position component of the mass m2

**The Singular Isothermal Sphere**

For this model there is only one additional slider:

Kappa: mass exponent

**The Non Singular Isothermal Sphere**

This model contains the following additional slider:

C : The core radius

Kappa: Constant central mass density

**The Transparent Sphere**

This model has the following additional slider:

C: The sphere radius

**The Elliptical Model**

For this model there are following additional sliders:

C : Core radius of the lens

Epsilon: Lens ellipticity

Alpha : Lens softness

Kappa : Constant central mass density

**The Galactical Profiles**

Following galactical model are available:

King Model

Truncated King Model

Hubble Model

De Vaucouleur Model

Spiralmodel

These models contain one additional slider (except the Truncated King Model):

Kappa: Constant central mass density

For the Truncated King Model there are two additional sliders:

C : The tidal radius of the lens

Kappa: Constant central mass density

**Multipole Lens**

For this model there are following additional sliders:

dx: X dipole moment component vector

dy: Y dipole moment component vector

q1: Component Q11 of the quadrupole moment tensor (Q11 + Q22 = 0)

q2: Component Q12 of the quadrupole moment tensor (Q12 = Q21)

**Rotational Lens**

This model has two additional sliders:

Sx: X angular momentum component

Sy: Y angular momentum component

**The Uniform Ring**

This model has three additional sliders:

Ri : The inner radius of the ring

Ro : The outer radius of the ring

Kappa: Constant surface mass density

**Second Order Schwarschild**

This model has one additional slider:

K: This parameter represents the term that appears in the GL equation if we consider the second order expansion of the Schwarzschild metric

**Elliptic SIS**

This model has two additional sliders:

Epsilon3: Lens ellipticity

Kappa : Constant surface mass density

**Elliptic King**

This model has three additional sliders:

C : Core radius of the lens

Epsilon2: Lens ellipticity

Kappa : Constant surface mass density

**Elliptic Hubble**

This model has three additional sliders:

C : Core radius of the lens

Epsilon2: Lens ellipticity

Kappa : Constant surface mass density

**Elliptic NIS**

This model has three additional sliders:

C : Core radius of the lens

Epsilon2: Lens ellipticity

Kappa : Constant surface mass density

**Elliptic Plummer**

This model has three additional sliders:

C : Core radius of the lens

Epsilon2: Lens ellipticity

Kappa : Constant surface mass density

**The Kassiola Kovner Model**

This model has four additional sliders:

C : Core radius of the lens

Kappa : Constant surface mass density

Q3 : Lens ellipticity

Thetai: Inclination angle

**The Navarro Frenk White Model**

This model has one additional sliders:

Kappa: Constant surface mass density

**The Barkana Model**

This model has four additional sliders:

C : Core radius of the lens

Kappa : Constant surface mass density

Epsilon2: Lens ellipticity

Alpha : Lens softness

**Internet Subroutines**

- Contouring: Translation from Fortran into C of *Aramini's* contouring program. We do not use his C version.

- Brent : Translation from Fortran into C of the program *554* of Netlib/Toms.

- Simplex: This algorithm is used to optimize.

**References**

P. Schneider, J. Ehlers and E. E. Falco, Gravitational Lenses (SEF Book), Springer Verlag, 1992.

J. Huchra, Galactic Structure and Evolution, in R. Meyers, Encyclopedia of Astronomy and Astrophysics, 203-219, Academic Press, 1989.

J. Lawrence, Focusing of Gravitational Radiation by Interior Gravitational Fields, Nuovo Cimento, 6B, 225-235, 1971.

Coments and suggestions to: frutos@fisica.ucr.ac.cr or frutto@tat.physik.uni-tuebingen.de

Last version on 16 February 2008.