Data Product Codes

PUNCH data products are organized into data processing levels from Level 0 (raw camera data) to Level 3 (calibrated science data). Within and across levels distinct data products and calibration files are marked with a unique identifying product code. For data in the spacecraft frame, each spacecraft is marked with a unique numeral identity - 1,2,3 for each WFI, or 4 for NFI.

Data Product Codes

Level	Code	Description
0	PM1, PM2, PM3, PM4, PZ1, PZ2, PZ3, PZ4, PP1, PP2, PP3, PP4, CR1, CR2, CR3, CR4	Standard polarization (PM for -60 degree, PZ for 0 degree, PP for +60 degree polarization) and clear (CR) images
0	PX1, PX2, PX3, PX4	Science images in a nonstandard polarization state or when the filter wheel packet is stale
1	PM1, PM2, PM3, PM4, PZ1, PZ2, PZ3, PZ4, PP1, PP2, PP3, PP4, CR1, CR2, CR3, CR4	Standard polarization (PM for -60 degree, PZ for 0 degree, PP for +60 degree polarization) and clear (CR) images (photometrically calibrated)
2	PTM	Polarized science mosaics (Trefoil) in output coordinates, resolved into MZP polarization triplets, and uncertainty layer
2	CTM	Clear science mosaics (Trefoil) in output coordinates, resolved into image and uncertainty layer
2	PNN	Polarized NFI images in output coordinates, resolved into MZP polarization triplets, and uncertainty layer
2	CNN	Clear NFI images in output coordinates, resolved into image, and uncertainty layer
Q	CNN	QuickPUNCH NFI images
Q	CTM	QuickPUNCH Mosaic images (5.4–80 Rsun)
L	CNN	Quicklook Clear NFI images
L	PNN	Quicklook Polarized NFI images
L	CTM	Quicklook Clear Mosaic images
L	PTM	Quicklook Polarized Mosaic images
3	CAM	Clear low-noise science mosaic, bkg-sub & resolved into B & uncertainty layer
3	PAN	Polarized low-noise NFI science image, bkg-sub & resolved into B, pB, & uncertainty layer
3	CAN	Clear low-noise NFI science image, bkg-sub & resolved into B & uncertainty layer
3	PIM	Polarized science mosaics (trefoils), with F-corona subtraction, without starfield subtraction, and still in the MZP system
3	CIM	Clear science mosaics (trefoils), with F-corona subtraction and without starfield subtraction
3	PTM	Polarized K PUNCH science mosaics (Trefoil), bkg-sub & resolved into B, pB, & uncertainty layer
3	CTM	Clear K science mosaics (Trefoil), bkg-sub & resolved into B & uncertainty layer
3	PNN	Polarized K NFI science image, bkg-sub & resolved into B, pB, & uncertainty layer
3	CNN	Clear K NFI science image, bkg-sub & resolved into B & uncertainty layer
3	VAM	Mosaic derived wind velocity maps: 1440 pos. angles at various altitudes
3	PAM	Polarized low-noise science mosaic, bkg-sub & resolved into B, pB, & uncertainty layer

Calibration Product Codes

Level	Code	Description
0	DK1, DK2, DK3, DK4, DY1, DY2, DY3, DY4	Polarizer in dark position, used for calibration; stim lamp off (DK) or on (DY)
0	OV1, OV2, OV3, OV4	CCD over-scan images
0	XI1, XI2, XI3, XI4	Experimental image (no set parameters; variable crop)
1	BD1, BD2, BD3, BD4	Deficient pixel (boolean) map
1	DS1, DS2, DS3, DS4	Optical distortion models
1	FQ1, FQ2, FQ3, FQ4	Flat-field parameters (quartic polynomial coefficients), by pixel
1	GM1, GM2, GM3, GM4, GZ1, GZ2, GZ3, GZ4, GP1, GP2, GP3, GP4, GR1, GR2, GR3, GR4	Vignetting functions for the standard polarization (GM, GZ, GP) and clear (GR) states
1	LM1, LM2, LM3, LM4, LZ1, LZ2, LZ3, LZ4, LP1, LP2, LP3, LP4, LR1, LR2, LR3, LR4	Outlier limits used for image rejection, saved as NumPy format instead of FITS
1	MS1, MS2, MS3, MS4	Mask files to define where image is undefined for each satellite
1	QR1, QR2, QR3, QR4	Intermediate level-1 processing necessary for QuickPUNCH
1	SM1, SM2, SM3, SM4, SZ1, SZ2, SZ3, SZ4, SP1, SP2, SP3, SP4, SR1, SR2, SR3, SR4	Instrumental additive stray light model for the standard polarization (SM, SZ, SP) and clear (SR) states
1	TM1, TM2, TM3, TM4, TZ1, TZ2, TZ3, TZ4, TP1, TP2, TP3, TP4, TR1, TR2, TR3, TR4	Dynamic instrumental additive stray light model for the standard polarization (TM, TZ, TP) and clear (TR) states
1	XM1, XM2, XM3, XM4, XZ1, XZ2, XZ3, XZ4, XP1, XP2, XP3, XP4, XR1, XR2, XR3, XR4	Result of the “L1 early” pipeline stage, an input to dynamic stray light model generation.
1	YM1, YM2, YM3, YM4, YZ1, YZ2, YZ3, YZ4, YP1, YP2, YP3, YP4, YR1, YR2, YR3, YR4	Result of the “L1 middle” pipeline stage, an input to static stray light model generation.
1	RM1, RM2, RM3, RM4, RZ1, RZ2, RZ3, RZ4, RP1, RP2, RP3, RP4, RC1, RC2, RC3, RC4	Point Spread Function (PSF) model for the standard polarization and clear states
Q	CFN	QuickPUNCH NFI images F corona model
Q	CFM	QuickPUNCH Mosaic images (5.4–80 Rsun) F corona model
3	PFM	Polarized mosaic F corona model, resolved into MZP pol. triplets, and uncertainty layer
3	CFM	Clear mosaic F corona model, resolved into image and uncertainty layer
3	PFN	Polarized NFI F-corona model, resolved into MZP pol. triplets, and uncertainty layer
3	CFN	Clear NFI F-corona model, resolved into image and uncertainty layer
3	PSM	Polarized mosaic stellar model, resolved into MZP pol. triplets, and uncertainty layer
3	CSM	Clear mosaic stellar model, resolved into image and uncertainty layer
3	PSN	Polarized NFI stellar model, resolved into MZP pol. triplets, and uncertainty layer
3	CSN	Clear NFI stellar model, resolved into image and uncertainty layer