PSP QA for run 4233, rerun 40

QA produced on Tue Nov 4 15:17:14 CST 2003 with photo version v5_4_26

	Field Quality (nFields=150)
quality	nOK	nHOLE	% HOLE
union	146	4	2.7
col. 1	147	3	2.0
col. 2	150	0	0.0
col. 3	149	1	0.7
col. 4	150	0	0.0
col. 5	150	0	0.0
col. 6	150	0	0.0

PSP status plot

PSF width (FWHM arcsec) statistics for column 6, filter r:
Mean PSF width = 1.66
Median = 1.63, min = 1.44, max = 2.11
There are 0 fields ( 0.0%) with PSFwidth > 4.0 arcsec
This run is 150 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	0.19	0.10	0.05	0.03	0.02
col. 2	0.13	0.06	0.03	0.06	0.01
col. 3	0.08	0.08	0.09	0.02	0.02
col. 4	0.08	0.06	0.04	0.04	0.04
col. 5	0.04	0.04	0.04	0.04	0.01
col. 6	0.10	0.06	0.01	0.02	0.02

PSP status plot

	Mean N stars for estimating PSF
band	u	g	r	i	z
col. 1	36.9	46.1	53.5	53.2	67.0
col. 2	43.3	45.8	52.4	49.7	65.1
col. 3	42.0	45.9	53.2	51.9	69.7
col. 4	46.0	46.4	52.0	50.7	67.8
col. 5	44.6	47.8	56.0	54.5	68.3
col. 6	46.9	47.1	61.3	59.0	72.6

Number of stars used for estimating PSF

	Mean m(aperture)-m(psf) Bias (mag)
band	u	g	r	i	z
col. 1	-0.06	-0.05	-0.05	-0.05	-0.06
col. 2	-0.06	-0.05	-0.05	-0.06	-0.06
col. 3	-0.05	-0.05	-0.05	-0.05	-0.06
col. 4	-0.05	-0.05	-0.05	-0.05	-0.06
col. 5	-0.05	-0.05	-0.04	-0.05	-0.06
col. 6	-0.06	-0.06	-0.05	-0.05	-0.06

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	0.01	0.02	0.02
col. 3	0.02	0.02	0.01	0.01	0.02
col. 4	0.02	0.02	0.01	0.01	0.02
col. 5	0.02	0.02	0.02	0.02	0.02
col. 6	0.02	0.02	0.01	0.02	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	22.03	21.70	20.64	19.80	18.56
max	22.05	21.78	20.69	19.88	18.66
min	22.00	21.63	20.59	19.74	18.47

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	-0.02	-0.00	-0.00	0.02
col. 2	0.01	-0.01	-0.01	-0.02	-0.06
col. 3	0.03	0.01	-0.02	0.02	-0.02
col. 4	0.01	-0.00	0.02	0.00	-0.01
col. 5	-0.02	0.01	0.00	0.00	0.02
col. 6	-0.03	0.01	0.01	0.00	0.04

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	0.95	1.03	1.00	1.10	1.05
col. 2	0.96	1.01	1.06	1.05	1.07
col. 3	1.01	1.05	0.99	1.09	1.04
col. 4	0.95	1.04	1.08	1.06	1.08
col. 5	1.00	1.08	0.99	1.01	1.04
col. 6	0.96	1.04	1.06	1.09	1.02

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).