PSP QA for run 6422, rerun 40

QA produced on Fri Nov 3 23:24:42 CST 2006 with photo version v5_4_28b

	Field Quality (nFields=128)
quality	nOK	nHOLE	% HOLE
union	128	0	0.0
col. 1	128	0	0.0
col. 2	128	0	0.0
col. 3	128	0	0.0
col. 4	128	0	0.0
col. 5	128	0	0.0
col. 6	128	0	0.0

PSP status plot

PSF width (FWHM arcsec) statistics for column 6, filter r:
Mean PSF width = 1.45
Median = 1.45, min = 1.33, max = 1.58
There are 0 fields ( 0.0%) with PSFwidth > 4.0 arcsec
This run is 128 fields long.
PSF width plot for all 30 chips
PSF width derivative plot for all 30 chips

	Mean PSP status (0=OK)
band	u	g	r	i	z
col. 1	0.46	0.03	0.01	0.01	0.02
col. 2	0.24	0.05	0.01	0.03	0.01
col. 3	0.33	0.01	0.00	0.02	0.00
col. 4	0.23	0.03	0.00	0.01	0.00
col. 5	0.26	0.00	0.00	0.00	0.00
col. 6	0.17	0.04	0.02	0.02	0.01

PSP status plot

	Mean N stars for estimating PSF
band	u	g	r	i	z
col. 1	15.5	35.3	40.7	40.1	45.8
col. 2	23.7	36.8	43.6	40.7	46.7
col. 3	18.2	38.1	46.2	42.4	50.7
col. 4	21.6	37.7	47.7	44.2	47.9
col. 5	20.7	37.0	49.3	47.3	48.9
col. 6	22.4	37.8	49.2	47.0	54.9

Number of stars used for estimating PSF

	Mean m(aperture)-m(psf) Bias (mag)
band	u	g	r	i	z
col. 1	-0.04	-0.03	-0.03	-0.04	-0.04
col. 2	-0.03	-0.03	-0.03	-0.04	-0.05
col. 3	-0.02	-0.03	-0.03	-0.03	-0.04
col. 4	-0.02	-0.03	-0.03	-0.03	-0.04
col. 5	-0.03	-0.03	-0.03	-0.03	-0.04
col. 6	-0.03	-0.03	-0.03	-0.04	-0.04

Aperture Correction Bias plot

	Mean m(aperture)-m(psf) Error (mag)
band	u	g	r	i	z
col. 1	0.02	0.02	0.02	0.02	0.02
col. 2	0.02	0.02	0.02	0.02	0.02
col. 3	0.02	0.02	0.01	0.02	0.02
col. 4	0.02	0.02	0.02	0.02	0.02
col. 5	0.02	0.02	0.01	0.02	0.02
col. 6	0.02	0.02	0.01	0.01	0.02

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

*Averaged over 6 columns

	Sky brightness* (mag/arsec2)
band	u	g	r	i	z
mean	22.35	22.11	21.11	20.42	19.23
max	22.39	22.14	21.14	20.48	19.31
min	22.28	21.99	21.07	20.36	19.14

Sky brightness (in counts) plot
Sky brightness (in mag/arcsec2) plot
Sky derivative plot
Sky colors plot

	Mean Sky Column offsets
band	u	g	r	i	z
col. 1	-0.00	0.01	0.01	0.00	0.01
col. 2	0.02	0.00	-0.01	-0.03	-0.06
col. 3	0.02	0.00	-0.02	0.01	-0.03
col. 4	0.01	0.00	0.01	0.02	-0.01
col. 5	-0.03	-0.02	-0.00	-0.01	0.03
col. 6	-0.02	0.00	0.01	0.02	0.05

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)
band	u	g	r	i	z
col. 1	1.01	1.03	0.99	1.08	1.04
col. 2	0.78	1.02	1.04	1.04	1.10
col. 3	0.99	1.01	0.96	1.09	1.06
col. 4	0.91	1.02	1.07	1.06	1.10
col. 5	1.01	1.05	0.95	1.02	1.04
col. 6	0.86	1.02	1.05	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).