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all functions - l


             z = l2ll(x)  
    convert 2-by-dims 32 bit integer X to 64 bit integer  
    (only works if sizeof(long)=8)  
interpreted function, defined at i/idlsave.i   line 299  

struct l_frame {  
  float x_min, x_max, y_min, y_max;  
structure, defined at i/testb.i   line 884  

interpreted function, defined at i/demo3.i   line 78  

     Given the coefficients a(1:m+1) of the m'th degree  
     complex polynomial Sum(a(i)*x^(i-1)) and a guess x, returns a root.  
     See Numerical Recipes (Press, et. al., Cambridge Univ. Press 1988),  
     section 9.5.  
interpreted function, defined at i/zroots.i   line 70  

interpreted function, defined at i/demo2.i   line 158  

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

     returns the LCM (least common multiple) of A and B, which must  
     be one of the integer data types.  A and B may be conformable  
     arrays; the semantics of the lcm call are the same as any other  
     binary operation.  
     The absolute values of A and B are taken before the operation  
     commences; if either A or B is 0, the return value will be 0.  
interpreted function, defined at i/gcd.i   line 47  
SEE ALSO: gcd,   is_prime,   factorize  

   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/2-lambda0)  
             lambda0 : Cosmological constant, normalized to  
                       th closure density.  
interpreted function, defined at contrib/cosmo.i   line 104  
SEE ALSO: lumdist  

     Prints the legal details of Yorick's copyright, licensing,  
     and lack of warranty.  
interpreted function, defined at i0/std.i   line 88  
SEE ALSO: copyright,   warranty  

             legndr(l,m, x)  
     return the associated Legendre function Plm(x).  The X may  
     be an array (-1<=x<=1), but L and M (0<=M<=L) must be scalar  
     values.  For m=0, these are the Legendre polynomials Pl(x).  
     Relation of Plm(x) to Pl(x):  
       Plm(x) = (-1)^m (1-x^2)^(m/2) d^m/dx^m(Pl(x))  
     Relation of Plm(x) to spherical harmonics Ylm:  
       Ylm(theta,phi)= sqrt((2*l+1)(l-m)!/(4*pi*(l+m)!)) *  
                           Plm(cos(theta)) * exp(1i*m*phi)  
interpreted function, defined at i/legndr.i   line 12  
SEE ALSO: ylm_coef  

     print the Y_SITE/i/README file at the terminal.  
interpreted function, defined at i0/std.i   line 1667  

             light3, ambient=a_level,  
     Sets lighting properties for 3D shading effects.  
     A surface will be shaded according to its to its orientation  
     relative to the viewing direction.  
     The ambient level A_LEVEL is a light level (arbitrary units)  
     that is added to every surface independent of its orientation.  
     The diffuse level D_LEVEL is a light level which is proportional  
     to cos(theta), where theta is the angle between the surface  
     normal and the viewing direction, so that surfaces directly  
     facing the viewer are bright, while surfaces viewed edge on are  
     unlit (and surfaces facing away, if drawn, are shaded as if they  
     faced the viewer).  
     The specular level S_LEVEL is a light level proportional to a high  
     power spower=N of 1+cos(alpha), where alpha is the angle between  
     the specular reflection angle and the viewing direction.  The light  
     source for the calculation of alpha lies in the direction XYZ (a  
     3 element vector) in the viewer's coordinate system at infinite  
     distance.  You can have ns light sources by making S_LEVEL, N, and  
     XYZ (or any combination) be vectors of length ns (3-by-ns in the  
     case of XYZ).  (See source code for specular_hook function  
     definition if powers of 1+cos(alpha) aren't good enough for you.)  
     With no arguments, return to the default lighting.  
     light3, diffuse=.1, specular=1., sdir=[0,0,-1]  
       (dramatic "tail lighting" effect)  
     light3, diffuse=.5, specular=1., sdir=[1,.5,1]  
       (classic "over your right shoulder" lighting)  
     light3, ambient=.1,diffuse=.1,specular=1.,  
       (two light sources combining previous effects)  
interpreted function, defined at i/pl3d.i   line 262  
SEE ALSO: rot3,   save3,   restore3  

             lightwf, cmax  
     Sets the cmax= parameter interactively, assuming the current  
     3D display list contains the result of a previous plwf call.  
     This changes the color of the brightest surface in the picture.  
     The darkest surface color can be controlled using the ambient=  
     keyword to light3.  
interpreted function, defined at i/plwf.i   line 131  
SEE ALSO: plwf,   light3  

             limit3, xmin,xmax, ymin,ymax  
          or limit3, xmin,xmax, ymin,ymax, zmin,zmax  
     Set the 3D axis limits for use with the cage.  
     Use keyword aspect=[ax,ay,az] to set the aspect ratios of the  
     cage to ax:ay:az -- that is, the ratios of the lengths of the  
     cage axes will become ax:ay:az.  
interpreted function, defined at i/pl3d.i   line 181  
SEE ALSO: cage3,   range3,   plwf,   plwf,   orient3  

          or limits, xmin, xmax, ymin, ymax,  
                     square=0/1, nice=0/1, restrict=0/1  
          or old_limits= limits()  
          or limits, old_limits  
     In the first form, restores all four plot limits to extreme values.  
     In the second form, sets the plot limits in the current coordinate  
     system to XMIN, XMAX, YMIN, YMAX, which may be nil or omitted to  
     leave the corresponding limit unchanged, a number to fix the  
     corresponding limit to a specified value, or the string "e" to  
     make the corresponding limit take on the extreme value of the  
     currently displayed data.  
     If present, the square keyword determines whether limits marked  
     as extreme values will be adjusted to force the x and y scales  
     to be equal (square=1) or not (square=0, the default).  
     If present, the nice keyword determines whether limits will be  
     adjusted to nice values (nice=1) or not (nice=0, the default).  
     There is a subtlety in the meaning of "extreme value" when one  
     or both of the limits on the OPPOSITE axis have fixed values --  
     does the "extreme value" of the data include points which  
     will not be plotted because their other coordinate lies outside  
     the fixed limit on the opposite axis (restrict=0, the default),  
     or not (restrict=1)?  
     If called as a function, limits returns an array of 5 doubles;  
     OLD_LIMITS(1:4) are the current xmin, xmax, ymin, and ymax,  
     and int(OLD_LIMITS(5)) is a set of flags indicating extreme  
     values and the square, nice, restrict, and log flags.  
     In the fourth form, OLD_LIMITS is as returned by a previous  
     limits call, to restore the limits to a previous state.  
     In an X window, the limits may also be adjusted interactively  
     with the mouse.  Drag left to zoom in and pan (click left to zoom  
     in on a point without moving it), drag middle to pan, and click  
     (and drag) right to zoom out (and pan).  If you click just above  
     or below the plot, these operations will be restricted to the  
     x-axis; if you click just to the left or right, the operations  
     are restricted to the y-axis.  A shift-left click, drag, and  
     release will expand the box you dragged over to fill the plot  
     (other popular software zooms with this paradigm).  If the  
     rubber band box is not visible with shift-left zooming, try  
     shift-middle or shift-right for alternate XOR masks.  Such  
     mouse-set limits are equivalent to a limits command specifying  
     all four limits EXCEPT that the unzoom command can revert to  
     the limits before a series of mouse zooms and pans.  
     The limits you set using the limits or range functions carry over  
     to the next plot -- that is, an fma operation does NOT reset the  
     limits to extreme values.  
builtin function, documented at i0/graph.i   line 715  
SEE ALSO: plsys,   range,   logxy,   zoom_factor,   unzoom,  
plg,   viewport  

     runs the Yorick equivalent of an old graphics performance test  
     used to compare PLAN, ALMA, and Basis with LTSS TMDS graphics.  
interpreted function, defined at i/testg.i   line 185  
SEE ALSO: testg,   grtest  

     returns natural log of the gamma function.  
     Error is less than 1e-13 for real part of z>=1.  
     Use lngamma if you know that all z>=1, or if you don't care much about  
     accuracy for z<1.  
interpreted function, defined at i/gamma.i   line 16  
SEE ALSO: lngamma,   bico,   beta  

     returns natural log of the gamma function.  
     Error is less than 1e-13 for real part of x>=1.  
     Use ln_gamma if some x<1.  
interpreted function, defined at i/gamma.i   line 37  
SEE ALSO: ln_gamma,   bico,   beta  

     returns the natural logarithm of its argument (inverse of exp).  
builtin function, documented at i0/std.i   line 613  
SEE ALSO: log1p,   log10,   exp,   asinh,   acosh,   atanh  

     returns the base 10 logarithm of its argument (inverse of 10^x).  
builtin function, documented at i0/std.i   line 619  
SEE ALSO: log,   exp,   asinh,   acosh,   atanh  

     return log(1+X) accurate to machine precision (even for X<<1)  
     from Goldberg, ACM Computing Surveys, Vol 23, No 1, March 1991,  
       apparently originally from HP-15C Advanced Functions Handbook  
interpreted function, defined at i0/std.i   line 637  
SEE ALSO: expm1,   log1p  

             logxy, xflag, yflag  
     sets the linear/log axis scaling flags for the current coordinate  
     system.  XFLAG and YFLAG may be nil or omitted to leave the  
     corresponding axis scaling unchanged, 0 to select linear scaling,  
     or 1 to select log scaling.  
builtin function, documented at i0/graph.i   line 785  
SEE ALSO: plsys,   limits,   range,   plg,   gridxy  

interpreted function, defined at i/kepler.i   line 474  

interpreted function, defined at i/kepler.i   line 481  

interpreted function, defined at i/ylmdec.i   line 357  

             files = lsdir(directory_name)  
          or files = lsdir(directory_name, subdirs)  
     List DIRECTORY_NAME.  The return value FILES is an array of  
     strings or nil; the order of the filenames is unspecified;  
     it does not contain "." or ".."; it does not contain the  
     names of subdirectories.  If SUBDIRS is given and is a simple  
     variable name, it is set to a list of subdirecotry names (or  
     nil if there are no subdirectories).  
     If DIRECTORY_NAME does not exist, the return value is the  
     integer 0 rather than nil.  
builtin function, documented at i0/std.i   line 1689  
SEE ALSO: cd,   mkdir,   rmdir,   get_cwd,   get_home  

   See IDL routine...  
     Calculate luminosity distance (in Mpc) of an object given its redshift   
     The luminosity distance in the Friedmann-Robertson-Walker 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  
     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);  
     xytitles,"z","Distance (Mpc)"  
interpreted function, defined at contrib/cosmo.i   line 162  
SEE ALSO: ldist