3.5) The PIA Astrophysical Applications

The main Astrophysical Applications window is a menu called via Buffers -> Astrophysical Work in the PIA Top Window.

This chapter describes the PIA Astrophysical Applications Window shown in Figure 1 and its items.

FIGURE 1: The PIA Astrophysical Applications Window 

3.5.1) Applications using several measurements as input:

By all the Astrophysical Applications options, except by Spectro-Photometry and Mapping (on which the further reduction is performed on a per measurement basis), several measurements are chosen to be combined. The desired measurements will be selected using the by-now familiar measurement selection window, as for plotting and reducing data at the various stages of reduction.

From every measurement several variables are calculated yielding a value per variable per measurement.
The main calculated variables are flux and surface brightness per measurement, accompanied by filter, aperture, polarizer, etc. In the case of a C100 / C200 measurement, fluxes are obtained by integrating over the full array and surface brightnesses are obtained by averaging over the array.
In the case of C100 or C200 measurements, a choice of detector pixels to be used is given. The selected pixels are then taken to obtain full fluxes and brightnesses from the array. Please note that at this stage a PSF correction is first applied by data from these detectors.

Also the possibility of colour corrections is offered, by a menu with several source spectrum alternatives: black-body spectrum (with a choice of temperature of the BB), power-law spectrum (with a choice of its index) and modified BB spectra with emissivity proportional to nu and nu squared. If one of the colour corrections is chosen, the calculated factors from folding source spectrum and filter curve correct the data. The factors used are presented to the user in a text window.
 
 
 
 
 

FIGURE 1b: Colour correction widget

Multi-Filter Photometry (for point or extended sources)

FIGURE 2: Multi-filter plot 

Multi-Aperture Photometry (for point or extended sources)

Spectro Photometry

FIGURE 3: PIA Spectro-photometry main window 

From the Process -> Fit spectrum option a menu for fitting combinations of several functions to the spectrum can be activated, shown in Fig. 4. This program is an adaptation for PIA from an original package kindly offered to us by the ISO-SWS instrument dedicated team. A description of this menu is given in the next section (3.5.2) PIA Spectrum Multi-Fit Facility.

FIGURE 4: PIA multi-fitting package 

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FIGURE 5: Fit results window 

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Mapping

Polarimetry

Show and Correlate Mean Values

Summary and Print Values (text or table format)

FIGURE 6: Example of a Summary and Print Values list

Write multiple measurements FITS (Super-FITS)

FIGURE 7: Selection GUI for the multiple FITS writing option.
 

At the top, the default filename is shown.  Edit the directory and filename as necessary.  The default name (for an example, May121659_AAP.FITS) contains the month, date, hour and minute respectively.

The following variables can be selected or deselected to be contained in the FITS binary table.

• "Meas. ID (Det - TDT - Meas. number)" : All the selected measurements are consectively numbered for identification purpose within the FITS binary table.  This variable which contains the detector, TDT, and measurement number information is written to the primary header with a keyword, "MEASID" followed by the corresponding number assigned to it.  For example, the third measurement you selected will have "3" assigned to it, and you'll see its information next to the keyword "MEASID3" in the header.
• "Pixel number"
• "Aperture_Y in arcsec (zero means a circular aperture)"
• "Aperture_Z in arcsec (diameter if Aperture_Y is zero)"
• "Wavelength in um"
• "Uncertainty in wavelength in um" : In the cases of the PHT-C and PHT-P, the know values are given, and for PHT-S, it is half the difference between each pixel wavelength.
• "Mean flux in Jy" : This corresponds to MNFL in phtiaap structure.
• "Mean flux uncertainty in Jy" : This corresponds to MNFU in phtiaap structure.
• "Median flux in Jy" : This corresponds to MDFL in phtiaap structure.
• "Mean brightness in MJy/sr" : This corresponds to MNBR in phtiaap structure.
• "Mean brightness uncertainty in MJy/sr" : This corresponds to MNBU in phtiaap structure.
• "Median brightness in MJy/sr" : This corresponds to MDBR in phtiaap structure.
• "Raster point ID in Y"
• "Raster point ID in Z"
• "Declination in degrees"
• "Right Ascension in degrees"
• "Roll Angle in degrees"
• "Flag"