PIA Checklist for Chopped Data

PIA v6.3 Checklist for Chopped Data             IPAC, aew 5 August 1997, v. 2.1
(extracted from PIA manual, but not produced by the PHT team)

ERD window (Do FCS first, then astronomical data)

Correction	Nonlinearity
Selection	Discard Readouts
Correction	Read-out Deglitching
Data		Save 
Process Meas.	Fit Ramps, 1st Order Poly

SRD window

Correction	Deglitching
Correction	Dark Current Subtr
Data		Save to PIA Internal file
Process		No drift handling

SCP Window 

Process		Responsivity Calculation
Accept as actual response the least noisy of average or median for FCS1 
*or* FCS2, save print file
Data		Save as PIA Internal file

Now select the astronomical data measurement instead of FCS measurement and 
repeat earlier steps for astronomical data measurement.

ERD window

Correction	Nonlinearity
Selection	Discard Readouts
Correction	Read-out Deglitching
 (if "number of readouts is too low", use "test processing" to reduce number)
Data		Save 
Process Meas.	Fit Ramps, 1st Order Poly

SRD window

Correction	Deglitching
Correction	Dark Current Subtr
Data		Save to PIA Internal file
Process		No drift handling

SCP window

(Correction	Vignetting causes  "divide by zero" error, so skip this step)
Process		Background subtraction within measurement

Background Subtraction Window

Choose defaults for chopper steps for source and background,
namely source="c" and Background="I" by clicking "ok"
Click "", 
Click "Subtracted Measurement --> buffer"
"quit" background subtraction window
Data		Load (select subtracted measurement)
(You have now loaded the background-subtracted measurement into SCP window)
Process		Power Calibration with Actual Response

SPD Window

Process		Extract Flux Density
Assign Astronomical Coordinates
Data		Save PIA Internal file *or* fits file
Print Flux values

Now open "Astrophysical Work" buffer, choose Multifilter Photometry.  The
resulting flux density has been summed over all pixels and adjusted
for the fraction of the PSF falling on the array.  The uncertainties
include both the noise in the astronomical data measurement and the
uncertainty in the responsivity.