Chris Beaumont's IDL Library

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.pro files

This procedure converts from (a,d,v) sky coordinates to (x,y,z) pixel coordinates in a data cube.

The anneal class performs simulated annealing to maximize a fitness function.

This function returns the values of many different constants used in astrophysics.

This function appends a second array to a first one.

This function is similar to (and an extension of) built-in functions like indgen, findgen, etc.

This function calculates the inverse hyperbolic sine of one or more numbers.

This procedure is a simple routine to check assumptions during programming.

This function calculates the Planck function I_nu or I_lambda.

This function returns the probability density function of a Cauchy distribution, with median mu and width gamma, evaluated at x.

This function computes the covariance matrix for a set of multidimensional data.

This function both evaluates the IMF at given mass, and returns masses drawn at random from the IMF.

This procedure creates a smoothed map of the suface density of objects on the sky or in a plane.

Defines a simple IDL structure to represent a DS9-style region description.

This procedure calculates the empirical distribution function (edf) of a set of data, evaluated at each input data point.

This function calculates a variety of statistics to characterize the discrepancy between 1D data and a model for the distribution from which the data were drawn.

This program is a wrapper procedure to the extast routine in the IDL astronomy user's library.

This function computes, as a function of galactic coordinates, the angle between a vector pointing towards the galactic north pole and a vector pointing towards the North Celestial Pole.

Intersect returns the intersection of two 1D, interger-valued vectors.

This function determines whether a variable corresponds to a numeric data type.

This function calculates the near and far kinematic distances for a given galactic longitude and radial velocity.

This routine uses to do all of the work

Convert linux time (the number of seconds since UTC Jan 1 1970) to julian date (the number of days since Jan 1 4713 BC).

Evaluate the cumulative distribution function of a lognormal distribution.

The loopLister object class provides a standard way to provide status updates during long looping operations.

This function creates a blank image and fits header, based on input parameters describing the desired image size and orientation.

This class defines an interface for running Markov Chain Monte Carlo simulations.

mcmc_multi is a subclass of the mcmc class to create markov chain monte carlo simulations on multiple chains simultaneously.

This function returns the approximate main sequence lifetime as a function of stellar mass.

This function returns the number density of stars in the Milky Way, as a function of galactic coordinates.

Byte scales numbers so that non-finite values are zero, and finite values map from 1 - 255.

This procedure swaps out NANs in an array with another value.

nearestN takes takes a list of source locations and, for a list of test positions, returns the index of the n'th nearest source.

This function returns a structure of astrometry parameters parsed from a FITS header.

This function estimates the amount of reddening a star is seen through, based on its observed colors.

This function returns the various ASCII non-printing characters.

The otree class implements the oct tree data structure, used for calculating the potential energy of a system of point masses.

This function finds the unique parabola which fits three xy pairs.

This procedure creates plots of vector fields.

This function extracts a subregion from a 2 or 3-dimensional FITS image.

This function calculates the potential energy of a collection of point masses.

This function computes the potential energy of a mass distribution.

This function evaluates, or returns samples drawn at random from, a PieceWise Power Law distribution.

Returns the range (max - min) of an array

This function computes the rank of each element in a data set.

Shift the values associated by up to 5 variables

Returns the sign of x

This function translates between 'real' coordinates (eg, ra dec) to pixel coordinates in a fits file.

This class creates a smoothed sky map from an irregularly spaced set of measurements.

This procedure is a wrapper to skymap_smooth, which creates a smoothed map of some function sampled at discrete points on the sky.

This procuedure creates a smoothed map of some quantity sampled, with uncertainty, at irregualr points across the sky.

This class provides an array-based implementation of a stack.

This function removes the last section from a string

This function calculates the sum of very small numbers in a way that avoids computer underflow errors.

The procedure swaps two variables

This function converts a time length in seconds to a more readible string version of that number in years, days, minutes, and seconds

This function uses the trapezoidal rule to perform a running integration of tabulated data.

Blink between several images, without having to manually set up the plotting windows.

This function returns the union of two vectors.

This function computes an upper limit for the strength of a signal embedded in a sequence of noisy measurements.

These routines define a vector data type.

This procedure proivdes a mechanism to report messages of various priorities within programs.

Calculates the weighted mean of a set of measurements.

This function wraps one or more values into the range [0, range).

This procedure writes an array of ds9region structures (defined in the Beaumont IDL library) into a region file that ds9 undertands

This procedure is an extenion of (and a wrapper for) the xyad program in the astronomy user's library.

This function tags sources with IR excess based on their colors in Spitzer IRAC bands 1-4.