% @(#)analysroma.hlq 17.1.1.1 (ESO-IPG) 01/25/02 17:17:45 \rightpage \se SECTION./ROMAFOT \es\co ANALYSE/ROMAFOT 07-AUG-1989 RHW \oc\su ANALYSE/ROMAFOT frame [cat_tab] [int_tab] [sigma,sat] INPUT\ MODE\ select all stars within selected subfields; OUTPUT\ MODE\ check at the results of the fit operation and select \us\pu Purpose: In INPUT MODE select all stars within selected subfields; \\ In OUTPUT MODE, look at the results of the fit operation and to select the results for final registration \up\sy Syntax: ANALYSE/ROMAFOT frame [cat_tab] [int_tab] [sigma,sat] \ys\pa frame = input frame \ap\pa cat_tab = catalogue table containing the information about the objects selected manually by SEARCH/ROMAFOT or automatically by FIND/ROMAFOT. An existing catalogue table is needed in INPUT MODE. Default is the name of the frame extended with `CAT'. \ap\pa int_tab = intermediate table which will contain trial values for position, location and size of holes, intensity within the subfield of all marked stars, the subfield's size and position and background level. After the fit, trial values will be substituted by the computed parameters. An existing intermediate table is needed in OUTPUT MODE. Default is the name of the frame extended with `INT'. \ap\pa sigma,sat = Enter the sigma of the PSF and the saturation level above which the pixels are ignored. Default values are displayed. \ap\no Note: The command is the central part of the ROMAFOT package to reduce stellar photometry data and has two functions. Which input tables are needed depends on which of the modes the user selects. In INPUT MODE the command needs at least two files: the IMAGE FRAME and the CATALOGUE TABLE (containing the selected stars and created by SEARCH/ROMAFOT or FIND/ROMAFOT).\\ In this mode the initial coordinates are read from the catalogue table. The subfield around the star is found in the frame and is displayed. The user then marks all stars within the subfield. The intensity and position of all marked stars within the subfield together with the subfield size and background level is written to the intermediate table. Position and size of holes to ignore given regions in the subframe are also stored in the intermediate table. The intermediate table can serve also as input table, although this use is limited. In OUTPUT MODE the command also needs two files: the IMAGE FRAME and the intermediate table (to read the computed parameters, and created by the command SELECT/ROMAFOT or by SORT/ROMAFOT).\\ In this mode for all the fitted subfield the program reads the image frame for the original subfield, the intermediate table for the calculated fits and displays the original subfield with the calculated fit. Together with the image, several parameters are displayed on the terminal: in particular, starting from the fourth row, five figures are reported in each row. These figures are the intensity, the local coordinates, the sigma and the fitting flag, respectively, for each object in the window. In the first row the star name is reported. In the second row one finds the record number of the intermediate table, the coordinates of the window in the image frame, the dimensions of the window in X and Y, and a flag for the fit. Finally, in the third row one finds the three parameters of the plane fitted to the sky background. \on \no Note: The commands has many function in it each of which are activated by pressing a key stroke (each function has one key stroke). During execution some of these functions will ask the user for input interactively. Below a list is given with the valid key stroke and the corresponding function of the commands and the interactive input required. For more extensive description of the interactive treatment of the data the user is refered to The MIDAS User' Guide, Volume 2, Chapter 5. A __switch between colour map and contour map display\\ B __enter scale factor for intensity projections (data on disk not affected)\\ C __enter the component to delete\\ D __enter the INTERMEDIATE TABLE record to display (OUTPUT mode)\\ E __make a hole of given radius at cursor position\\ F __FINISH\\ G __enter the hole to restore\\ H __display this help information\\ I __add a component at cursor position (trial-height is the local maximum)\\ J __add a component at cursor position (trial-height must be entered)\\ K __coordinates and pixel-value at cursor position appear on the screen\\ L __level above which the background at vertical cursor position appears on screen\\ M __enter the CATALOGUE TABLE to display an object\\ N __enter the INTERMEDIATE TABLE to display (INPUT mode)\\ P __enter identification of a component; all other components will be disabled for display or registration\\ Q __restore P\\ R __enter DELTA_X,DELTA_Y to reduce the subframe\\ S __enter DELTA_X,DELTA_Y to move the subframe\\ T __enter identification of a component: it will be disabled for display and registration. Restore with T(-n)\\ U __enter factor for the zero of colour scale (current 0)\\ V __close old files and open new ones\\ W __enter slope of the colour scale (larger than 0.0)\\ X __display isophotes\\ Y __enter factor (less than 1.) to get isophotes at arbitrary threshold\\ Z __enter "0" to display components already considered; "1" to be informed\\ 4 __OUTPUT mode. Objects to examine: (A)ll, (M)anual or (S)elective, enter A, M or S to select one of the three modes. If (S)elective examine only special subarrays: No conv., height above ..., more than ... iterations\\ 5 __INPUT mode. Objects to examine: (A)ll, (M)anual or (S)elective, enter A, M or S to select one of the three modes. If (S)elective examine only special subarrays: not grouped by WINDOW; height above ...\\ 6 __enable smoothing of the displayed subframe. Data on disk will not be affected\\ 7 __enable integral of the fitted subframe to be displayed\\ bar_repeat last display (with new parameters)\\ / __enter new default window size\\ - __enable/disable hole reporting\\ ? __enable/disable multiple registration of components\\ @ __enter `R' to replace one component with the next input (using `I' or `J'); enter `A' to append\\ For more information the user is referred to The MIDAS User's Guide, Volume 2, Chapter 5. \on\exs Examples: \ex ANALYSE/ROMAFOT GCLUST ? GCLINT Execute the command on the frame GCLUST using the intermediate table GCLUSTCAT. If the catalogue table does not exist the command assumes that the user wants to look at the fitted results (OUTPUT mode). \xe\ex ANALYSE/ROMAFOT GCLUSTER GCLCAT GCLINT Execute the command on the frame GCLUSTER using the catalogue table GCLCAT and the intermediate table GCLINT. If the catalogue table GCLCAT (e.g. created by FIND/ROMAFOT) exists the user can (INPUT mode) have a look at the windows stored in the catalogue table. After finishing the intermediate table will contain all program stars with the trial values, with dimensions and shapes. The data can be processed by the command FIT/ROMAFOT. \xe \sxe