Describes how XPA access points can be added to X Toolkit (Xt) programs. ... Thus, in order to add XPA access points to the standard Xt event loop, the following routine should be called before entering the loop: int XPAXtAddInput(XtAppContext app, XPA xpa) . The XPAAddAddInput() routine will add XPA access points to the Xt event loop by making calls to the standard XtAppAddInput() routine. ... If the xpa argument is NULL, then all active XPA access points are added to the loop. ...

... Chapter 4: Solar System Targets > 4.2 Target Identification . ... The following information is required to identify and classify each target. ... For example, separate targets should be defined if you plan to take spectra of several different surface features on a planet, or if you plan to observe the same feature with different timing constraints. ... Description . PLANET . If the target is the center of a planet, enter PLANET followed by its name (e.g., PLANET JUPITER , PLANET SATURN ). ...

... The parameter pgdev allows the user to specify a pgplot device, but, in contrast to the pgplot standard, the file name should not be included, but instead supplied via the parameter plotfile . ... To write a colour postscript file called op.ps: pgdev=/cps plotfile=op.ps . However note that at present, if a colour postscript device ( pgdev = `/cps'), a fits file ( pgdev = `/fits') or a ppm file ( pgdev = `/ppm') are selected, the task in fact bypasses pgplot and writes the postscript file directly. ...

... Though Flint knows the interface definitions (i.e. number, type and intent of each argument) of standard FORTRAN functions, it is desirable for users to build and use a file (or files) describing the interfaces to their own library. ... The format is: flint -o file .. ... While these interface definitions could be input along with normal source files, preceding the interface file with the -l (library) switch has the advantage that the source of this file does not appear in the listing file. ...

Next: Saving the Data Up: The Reduction Session Previous: Flat Field correction . In the scheme described in the previous Section, the correction for the blaze function and for the chromatic response is done using standard stars. When the input data sets do not include standard stars it is possible to correct for the blaze function using a model of this effect as described in Chapter . ... where input is the raw image, . command MERGE/ECHELLE output name order1,order2 NOAPPEND . ...

. This is the CIMA alternative drift map menu: . The following is the on-line help page for alternative drift map: . You can return to the main CIMA page by clicking here .

The database contains references to the papers, data files and links to the Internet resources related to measurements and calculations of the optical constants in the wavelength interval from X-rays to radio domain. ... References to some useful books and reviews on the subject (e.g. the classical handbooks edited by E.D.Palik) and links to Internet collections of optical constants and personal WWW pages with related software were also placed in the database. You have arrived at our welcome page. ...

... fudge factors for nroff and troff .if n \{\ . ... IX Title "xpaxt n" .TH xpaxt n "June 7, 2012" "version 2.1.14" "SAORD Documentation" .SH "NAME" \&\fBXPAXt: the XPA Interface to Xt (X Windows)\fR .SH "SYNOPSIS" .IX Header "SYNOPSIS" Describes how \s-1XPA\s0 access points can be added to X Toolkit (Xt) programs. ... If the xpa argument is \s-1NULL\s0, then all active \s-1XPA\s0 access points are added to the loop. If xpa is not \s-1NULL\s0, then only the specified access point is added. ...