PSP QA for run 3469, rerun 157


Data reduced with photo v5_5_11

QA produced on Wed Nov 9 05:58:53 EST 2005 with photo version v5_5_11


Field Quality (nFields=149)
quality nOK nHOLE% HOLE
union 0 149 100.0*
col. 1 0 149 100.0*
col. 2 0 149 100.0*
col. 3 0 149 100.0*
col. 4 0 149 100.0*
col. 5 0 149 100.0*
col. 6 0 149 100.0*

*Red entries are triggered by the percentage of unacceptable fields exceeding
5 in any column, or 15 for the union of all columns.
PSP status plot


PSF width (FWHM arcsec) statistics for column 6, filter r:
Mean PSF width = 0.45
Median = 0.45, min = 0.45, max = 0.45
There are 0 fields ( 0.0%) with PSFwidth > 4.0 arcsec
This run is 149 fields long.
PSF width plot for all 30 chips
PSF width derivative plot for all 30 chips


Mean PSP status (0=OK)
bandugriz
col. 1 3.00 3.00 3.00 3.00 3.00
col. 2 3.00 3.00 3.00 3.00 3.00
col. 3 3.00 3.00 3.00 3.00 3.00
col. 4 3.00 3.00 3.00 3.00 3.00
col. 5 3.00 3.00 3.00 3.00 3.00
col. 6 3.00 3.00 3.00 3.00 3.00

PSP status plot

Mean N stars for estimating PSF
bandugriz
col. 1 0.0* 0.0* 0.0* 0.0* 0.0*
col. 2 0.0* 0.0* 0.0* 0.0* 0.0*
col. 3 0.0* 0.0* 0.0* 0.0* 0.0*
col. 4 0.0* 0.0* 0.0* 0.0* 0.0*
col. 5 0.0* 0.0* 0.0* 0.0* 0.0*
col. 6 0.0* 0.0* 0.0* 0.0* 0.0*

*Red entries are triggered by Nstars < 10
Number of stars used for estimating PSF

Mean m(aperture)-m(psf) Bias (mag)
bandugriz
col. 1 0.00 0.00 0.00 0.00 0.00
col. 2 0.00 0.00 0.00 0.00 0.00
col. 3 0.00 0.00 0.00 0.00 0.00
col. 4 0.00 0.00 0.00 0.00 0.00
col. 5 0.00 0.00 0.00 0.00 0.00
col. 6 0.00 0.00 0.00 0.00 0.00

Aperture Correction Bias plot

Mean m(aperture)-m(psf) Error (mag)
bandugriz
col. 1 1.00* 1.00* 1.00* 1.00* 1.00*
col. 2 1.00* 1.00* 1.00* 1.00* 1.00*
col. 3 1.00* 1.00* 1.00* 1.00* 1.00*
col. 4 1.00* 1.00* 1.00* 1.00* 1.00*
col. 5 1.00* 1.00* 1.00* 1.00* 1.00*
col. 6 1.00* 1.00* 1.00* 1.00* 1.00*

*Red entries are triggered by
apCorr Error > ( 0.15 0.10 0.10 0.10 0.15) mags in (u g r i z)
Aperture Correction Error plot
A few related auxiliary plots:
Aperture Correction Scatter (w/o bias contribution)
Power-law index for the outer PSF
Kolmogoroff exponents

Sky brightness* (mag/arsec2)
bandugriz
mean 18.11 18.24 17.23 16.45 15.14
max 18.16 18.28 17.32 16.60 15.31
min 18.04** 18.19** 17.11** 16.29** 14.94**
*Averaged over 6 columns

**Red entries are triggered by
min Sky < ( 21.2 21.0 20.0 19.2 18.0) mag in (u g r i z)
Sky brightness (in counts) plot
Sky brightness (in mag/arcsec2) plot
Sky derivative plot
Sky colors plot

Mean Sky Column offsets
bandugriz
col. 1 0.00 -0.69* 0.03 0.01 0.01
col. 2 -0.00 0.13 -0.01 -0.03 -0.04
col. 3 0.06 0.15* -0.02 -0.00 -0.03
col. 4 -0.07 0.14 -0.00 0.01 -0.03
col. 5 0.05 0.16* -0.00 0.01 0.06
col. 6 -0.04 0.11 0.01 0.00 0.04

*Red entries are triggered by abs(offset) > 0.15 mag


The noise is estimated from the width of the sky histogram, corrected
for the dark variance, and normalized by the Poisson value:
norm. spurious noise = sqrt[gain*(sigma_sky^2-dark_var)/sky]
Values significantly larger than 1 indicate the presence of spurious noise.

Spurious Noise (from sky quartiles)
bandugriz
col. 1 0.99 0.78 0.98 1.05 1.04
col. 2 0.89 1.00 1.02 1.02 1.06
col. 3 1.03 1.03 0.99 1.08 1.04
col. 4 0.93 1.05 1.06 1.04 1.02
col. 5 1.00 1.05 0.97 0.99 1.04
col. 6 1.01 1.04 1.04 1.07 1.01

Spurious Noise plot
Note that bright stars cause single-field spikes which are, for
different bands, aligned in the field number. A temporal increase
in noise can be traced in the r-i-u-z-g order (2 fields shift).


There are 75 warnings for this run.