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% @(#)integrstar.hlq 19.1 (ESO-IPG) 02/25/03 13:19:17
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%++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
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%.COPYRIGHT (c) 1990 European Southern Observatory
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%.KEYWORDS MIDAS, help files, INTEGRATE/STAR
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%.PURPOSE On-line help file for the command: INTEGRATE/STAR
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%.VERSION 1.0 31-JUL-1990 : Creation, RHW
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%----------------------------------------------------------------
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INTEGRATE/STAR 31-JUL-1990 RHW
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INTEGRATE/STAR [in_specs] [out_tab] [parameters] [mode]
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computes flux, radius and background of stars previously centered
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Computes flux, radius and background of stars previously centered
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INTEGRATE/STAR [in_specs] [out_table] [parameters] [mode]
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in_specs = input specifications. Can be CURSOR, if the objects
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are interactively chosen with the display cursor, or
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frame,table if the objects are defined in a table. In
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the latter case no image display/window is required.
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The table should have two columns labeled X_COORD and
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Y_COORD. It can be created by the commands GET/GCURSOR
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and GET/CURSOR. Default input is CURSOR.
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out_table = output table if you want to store the results in a
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table. The table will contain: x, y, flux, magnitude,
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and background in the columns :X_COORD, :Y_COORD,
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:FLUX, :BGSB, and :MAG. Default no output table will
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be created, and results appear on the screen.
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parameters = radius,step,ref_magnitude (defaulted to 20,1,0), where
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radius is the maximum radius in pixels of the aperture;
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step is the step in pixels between 2 annuli;
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ref_magnitude is the magnitude of the reference star.
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mode = AUTO or INTERACTIVE; only applicable if in_spec is
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given frame,table as input. default INTERACTIVE. In
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the interactive mode the graphics display/window
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Note: The command computes the (stellar) object magnitude according to
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the following receipe. The algorithm is based on determination
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of the parameters in a single line through the (stellar) object,
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not on a two-dimenional approch.\\
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1. First, the image pixel values are sorted and put in a table,
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running from low to high values.\\
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2. From the lowest 4 values in this table a first order average
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sky background and standard deviation (sigma) is computed;\\
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3. Then, the algorithm looks for the table value which falls
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between sky average and average + sigma/2;\\
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4. Depending where in the table this value is found the average
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sky value and sigma are adjusted to determine the final values;\\
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5. The radius of the object is then computed considering only
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those points above sky average + 6*sigma.\\
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Because the one-dimensional approch results obtained from less
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than 10 pixel values should be considered to be unreliable. In most
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case a error message will be given.
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Compute interactively the fluxes in frame loaded using the image
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and graphics display. The command will run in INTERACTIVE mode.
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INTEGR/STAR rfot,rfotpos rfotout 5,1,0 AUTO
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Use columns :X_COORD and :Y_XCOORD of the table rfotpos (e.g.
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created by GET/CURSOR) to define the centers of the objects for
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which the fluxes are to be computed. The results will be stored in
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the table rfotout. The command runs in automatic mode and uses
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non-default values for the radius, step, and reference magnitude.