SMART IDEA Applications

(This page is adapted from the ISAP WWW page "GUI Buttons" with all relevant acknowledgements.)

Running IDEA Applications

To run an Application on data first select the relevant data by using the right mouse key to draw a region on the SMART IDEA window display box.

If the "Mouse" selection is set to "OFF" the "Applications" window (above) will appear and an Application can be selected.
If a particular application has already been selected from the "Mouse" drop-down menu then that one is applied to the selected data.

Data Return

With the exception of "CANCEL" and "MAKE-AAR" the new data returned from your selected application will be merged with the remaining portion of your PRIME AAR.

This may result in the loss of some data tags. eg. In "Average" you will lose most of the tags. The averaged/merged data will have the WAVE, FLUX, STDEV, ORDER and FLAG tags.
(If you average across the orders the ORDER tag will also be lost.) If you select the whole AAR (ie. plot the whole AAR and draw a box that encompasses all the data points)

the new data returned after the Application will be the new PRIME AAR.

Data Present Boxes

At the top of the "Applications" window are 4 boxes listing the data selected for processing :

• Orders Present
• Slit Pos Present
• BCDs Present
• Modules Present

IDEA Applications

FIX STDEV :

Please see Fix StDev |

MASK :

Sets the FLAG TAG so that this data is ignored in subsequent operations.

Some functions (eg. "Normalize") ignore the masked data when calculating the normalization factor but then apply the factor to all the data.
(ie.masked and unmasked)

To view the MASKED data set "Show Masked" to "ON" on the IDEA Plot Style Preferences window. MASKED data can be UNMASKED or ZAPPED. |

TIPPEX :

Replaces the selected flux data with an interpolated value. For a full description see  Tippex?. |

UNMASK :

Re-Sets the FLAG TAG on any previously MASKED data so that it is now included in the analysis. |

ZAP :

Removes the selected data from the prime AAR. You cannot select the whole PRIME AAR as there would be no data left! |

ZAP ASSOC :

If you plot several BCD's for a given order you sometimes see a poorly behaved BCD(s) for an order that you would like to delete.

If you select a portion of this bad data with the right mouse button you can delete all the associated data.

Associated data has the same value for a given tag e.g. Order:0 Slit Pos:1 Module:0, BCD:37,

or if you had selected data from two detectors it could be Order:0,1 Slit Pos:1 Module:0 BCD:4,37 etc. |

ZAP MASKED :

This will remove any masked data from the selected portion of the PRIME AAR.

You must include some unmasked data points as the routine will not allow you to remove all your selected data points. |

NORM (CONST, NOWEIGHT) :

Please see Norm(Const, NoWeight) |

NORM (CONST, WEIGHT) :

Please see Norm(Const, Weight) |

NORM (REF, NOWEIGHT) :

The data selected using the right mouse button is multiplied by a value so that the mean is equal to the mean value of the reference spectrum

(see MAKE REFERENCE). |

NORM (REF, WEIGHT) :

The data selected using the right mouse button is multiplied by a value so that the mean is equal to the mean value of the reference spectrum
(see MAKE REFERENCE). The data are weighted by 1/(stdev^2). |

REBIN AND DEFINE SCALE :

Please see Rebin |

REBIN TO REFERENCE SCALE :

Please see Rebin to Reference |

SMOOTH :

Please see Smooth |

ARITHM :

Arithm consists of a pulldown menu with 13 operations that can be performed on the flux values (i.e. y-values) of the sub-set of data that you have just selected
from your PRIME AAR. If you click on any of the first 7 options a pop-up text window will appear that will prompt you to enter a constant.

• + Add a constant
• - Subtract a constant
• * Multiply by a constant
• / Divide by a constant
• Sigma clipping - kappa*sigma outliers will be masked
• Clip Above - remove all data above a constant
• Clip Below - remove all data  below a constant
• 1/y - invert the AAR as 1/y
• Sqrt - returns the square root
• Exp - returns the natural exponential
• Exp10 - returns the exponential
• Log - returns the natural log
• Log10 -returns the log to the base 10

|

ARITHM2(REF) :

This Application allows arithmetic operations between the current prime spectra and a reference spectra.
It is greyed out unless a reference spectra has been designated.
To designate a spectra as a reference use the "Make Reference" application described below
or the "Use as Reference Data Set" option on the IDEA Stored Data Sets window.
A full description of how to use "Arithm2(Ref) is at Arithm2(Ref)". |

CLIPPING :

Please see Clip |

AVERAGE :

Please see Average |

BLACKBODY FIT :

Please see Blackbody |

LINE FIT :

Please see Line Fit |

PHOTOMETRY :

Please see Photometry |

ZODIACAL LIGHT :

This gives a modeled value for all wavelengths in a spectra.
The model reads the RA, DEC, day of year, and UT of the observation from the aar file header and computes a line of sight
through the modeled zodiacal dust cloud.
For a more detailed description, please see Zodiacal. |

|SHIFT : | This Application is intended ONLY for use with ISO LWS data.
Attempting to use it for IRS data will display a pop-up box with the warning message : "SHIFT is not allowed for IRS Aots". Click "OK" to continue.
This routine will normalize a single BCD to a given order by comparing overlapping wavelength regions.
The flux values for the "good" order will remain unchanged.
Flux values (and stdev) for the other orders will each be multiplied by a computed constant to adjust it to the good order.
This computed constant is ratio between the weighted means in the overlap region.
This process will ripple through all orders until they have all been corrected. (See : sap_shift.pro?.)
Note : This can alter the slope of the order.
Extra care should be taken if you are averaging data that contains a line which has been detected in two orders (due to the overlap in wavelength coverage).

1. Select the "good" order or "preserve mean". The preserve mean option will shift in such a way that the mean flux of the entire AAR is not changed
2. Select the "correction type" :
   • "scaling" for multiplicative adjustments
   • "offset" for additive adjustments
   • "LWS Dark Correction" for LWS 01 observations. An additive correction is done by finding a value = C/RSRF to correct one detector to the next.
3. Select the "weighting" :
   • "weighted" (to weight fluxes by 1/stdev**2)
   • "unweighted" (to treat all fluxes equally)
4. Press "OK" to perform the operation and return the result to the main window. (Or press "Cancel" if you have changed your mind.)

|

XSHIFT :

Please see X Shift |

XSHIFT(REF) :

Please see X Shift(Ref) |

MAKE AAR :

Please see Make AAR |

MAKE REFERENCE :

A copy of the selected data becomes the REFERENCE AAR. Any AAR can be made reference.
When you make an AAR the reference it replaces any previous reference data set.
This is the same as the "Use as Reference Data Set" option on the IDEA Stored Data Sets window.

Once set a reference data set can be in applications requiring one, eg. NORM(REF, NO WEIGHT/WEIGHT), XSHIFT(REF). |

OPLOT DATA TO REF :

Please see Oplot Data to Ref |

SELECTION INFO :

Please see Selection Info |

CANCEL :

Quits the Application window without changing the PRIME AAR. |