... The exact directions of the offsets are parallel to the rows and columns of the CCD on which the aperture is specified. ... It is often useful to explicitly specify the desired rotation of the WFPC2 field-of-view on the sky. ... Figure 7.8 shows the CCD orientation and aperture locations relative to the U3 axis. ... Obtain the Position Angle (PA) of the source axis on the sky, measured in the standard way, North through East. ... desired source angle in field-of-view measured CW from +U3 axis) . ...

... SCHED STANDARD OBSERVING BANDS ---------------------------------------------- Center BAND Frequency(1) Bandwidth '90cm' 330.49 0.0 '50cm' 610.98 0.0 '21cm' 1465.49 128.0 '21cm' 1435.49 64.0 '21cm' 1416.49 0.0 '18cm' 1658.49 0.0 (2) '18cm' 1653.99 0.0 (3) '13cm' 2295.49 0.0 '6cm' 4990.49 0.0 '4cm' 8415.49 0.0 '2cm' 15285.49 0.0 '1cm' 22235.49 0.0 '24ghz' 23800.49 0.0 '7mm' 43135.49 0.0 'sx' 2295.49 and 8415.49 0.0 ---------------------------------------------- 1. ... Most 18 cm observing. ...

Astronomy Discussion Forums . Forums: . ... Discussion Forums . ... Iridium Flare . Forum List | ... Post Message | ... Actually, you were right about Iridium flare. ... www.astronomy.net . About Astronomy Net | Advertise on Astronomy Net | ... Unless otherwise specified, web site content Copyright 1994-2016 John Huggins All Rights Reserved . Forum posts are Copyright their authors as specified in the heading above the post. "dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...

... Up: Description of program searchdup Previous: Program use . Input records are ordered per date of observation, and the list of known (observed) sources is cleared. Each record is compared in position to all the known sources. If the sky distance is less or equal to the specified one, the record is added to the list of observations for that source. If no known sources are within the specified radius, a new source is created, with the coordinates of the observation record. ...

Next: External Functions Up: Fitting of Data Previous: The Corrected Gauss--Newton . ... Basic functions are either defined in the system or defined by the user as external FORTRAN routines. ... Basic functions are specified by the name, the independent variable(s) and parameter(s), with optional guesses for the parameters, following the syntax: name(var1[, ];par1[, ]) [par1=value] . ... Parameters are defined by unique names after the semicolon in the function specification. ...

When entering Identification section user should open the file with observed positions of objects which are to be identified (the file may be first created). ... Format of observations must coincide with that of optic observations in which they are published by Minor Planet Center (observed position may be presented as “accurate” or “approximate” one): . ... observed right ascension (in hours, minutes, and seconds of time (“accurate position”) or in hours and minutes (“approximate position”) . ...

... Typically, an observation specified by an observer cannot be directly executed by an observatory. Observation specifications need to be configured so that they can be used by other components of the observatory. This paper motivates the need for configuration tools and describes a software architecture which supports configuring astronomical observations. ... This paper describes a system for preparing and configuring individual astronomical observations. ...

Allows you to specify a drift scan: motion at a constant velocity along a great circle. ... The path starts at the new object position (though the telescope actually intersects the path later, see Subtleties ). ... Note that the units are always /sec for both axes. ... The velocity along the path is 0.01 /sec. ... The path is assumed to start when you hit the Slew button (more precisely, when the TCC parses the command). However, it takes the telescope awhile to slew to meet the specified path. ...

... This routine is designed to read in the current correlator set-up, go to the chosen source, and then take data pointing directly at the specified source. This routine will automatically wait until you are on source before beginning to take data. ... Additionally, this routine allows you to take an ON/OFF calibration pair (one 10s scan with the noise diode on, followed by a 10s scan with the diode off), using the chosen noise diode configuration (see Section 1.6 . ...

Computer Ephemeris. Ephemeris for physical observations of the planets. Explanations. Each row of the table contains for date specified at 0h of Time Terrestrial Dynamical: . ... position angle of axis of planetary rotation (degrees) - 'P', . ... illumanated part of the disk - k, . ... position angle of disk point with minimal illumination (degrees), . longitude of central meridian of the disk (degrees) - 'merid1' - system I and so... phase correction (degrees). ...

... epframes (epframes-8.87.1) [xmmsas_20080701_1801-8.0.0] . ... epframes reads a raw event list of a single CCD and exposure from an EPIC PN ODF ([ 1 ]) . ... The auxiliary, main periodic housekeeping and spacecraft time correlation files corresponding to the selected EPIC PN raw event list are needed for the computation of event time tags. epframes flags events with faulty coordinates or times in a FLAG column. ... The PHA values are the event raw amplitudes corrected for column offsets. ...

Next: Power Law fit to Up: Spectral Analysis Previous: Error Determination . With PROS2.3 all fitting is performed using Poisson statistics , rather than Gaussian, so that results will be correct even for small counts ( ) in some channels. Power Law fit to a Point Source . Raymond Model . Two-Temperature Raymond Model . Limiting Energy Channels Input to the Fit . Multiple Data Sets . ... Fit a source with a small number of net counts . Inspection of results . ...

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Pulkovo NEO Page . ... EPOS Software Package . ... EPOS ( E phemeris P rogram for O bjects of the S olar system) is the Windows PC application for study and ephemeris support of observations of the Solar system objects. ... It controls the part of common data and transfers the control to one of the programs that solve the restricted set of tasks. ... So with the EPOS software package one can calculate the accurate ephemerides for many objects and get the quick illustration of their motion as well. ...

adjustable array . The array in a subprogram has a variable dimension just as in Fortran 77 through that both the array name and the dimension (all dimensions) are dummy arguments. ... Array sections can be used here instead of arrays. array function . ... An array in a subprogram which is not local and has a certain data type and a certain rank. ... Each Fortran program has to consist of exactly one main program and and any number of subroutines, functions, modules and BLOCK DATA program units. ...

OptInt PmWiki : Pm Wiki / Page List Templates . ... template first:) . ... template last ...:) sections to specify output for the first or last page in the list or a group. ... template]] (:template defaults order=name:) (:template first:) Pages ordered by group (:template first {=$Group}:) Pages in group [[{=$Group}/]] (:template each:) * [[{=$FullName}]] (:template last {=$Group}:) {=$Group} contains {$$GroupPageCount} pages. (:template last:) {$$PageCount} pages total. [[#templateend]] . ...

RTT150 . ... This search system is designed for generating the necessary information on series of pointings (observations of each source consist of sets of exposures with different filters and sometimes with different exposure times) for observed sources. Search results appear at the separate page as a table with the following data: . DATE - real (not evening!) observations date (in YYYY-MM-DD format); . ... Bin - minimal CCD binning mode (may vary during the observations); . ...

Stellarium 0.12.3 . ... Classes . ... ClassљList . ... TuiNodeActivate Class Reference . ... voidљ . ... TuiNodeActivate (const QString &text, QObject *receiver, const char *method, TuiNode *parent=NULL, TuiNode *prev=NULL) . Create a TuiNodeActivate node. ... virtual TuiNodeResponse љ . handleKey (int key) . ... TuiNode (const QString &text, TuiNode *parent=NULL, TuiNode *prev=NULL) . ... virtual TuiNode *љ . ... virtual voidљ . ... Contains the numbers of the parent nodes in the hierarchy. ...

... In order to realize the optimal scientific return from the VLT, ESO has undertaken to develop an end-to-end data flow system from proposal entry to science archive. The VLT Data Flow System (DFS) is being designed and implemented by the DFS Group (ESO Internal access only) in collaboration with VLT Division and Instrumentation Division . ... VLT Control System Interface . ... OBs are the quantum of data that flows within the DFS, collecting state, data and status information as they flow. ...

... public class WindowManager . ... This class consists of static methods used to manage ImageJ's windows. ... static void . ... Adds the specified window to the Window menu. static boolean . ... Returns a reference to the active image or null if there isn't one. static ImageWindow . ... Makes the image contained in the specified window the active image. static void . ... Returns the first image that has the specified title or null if it is not found. public static void addWindow (java.awt.Frame win) ....