PSP QA for run 5867, rerun 40

QA produced on Sat Nov 26 21:46:23 CST 2005 with photo version v5_4_28

	Field Quality (nFields=235)
quality	nOK	nHOLE	% HOLE
union	230	5	2.1
col. 1	233	2	0.9
col. 2	234	1	0.4
col. 3	235	0	0.0
col. 4	234	1	0.4
col. 5	233	2	0.9
col. 6	235	0	0.0

PSP status plot

PSF width (FWHM arcsec) statistics for column 6, filter r:
Mean PSF width = 1.85
Median = 1.81, min = 1.35, max = 2.63
There are 0 fields ( 0.0%) with PSFwidth > 4.0 arcsec
This run is 235 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	0.37	0.20	0.07	0.05	0.01
col. 2	0.28	0.08	0.09	0.10	0.03
col. 3	0.28	0.13	0.05	0.05	0.01
col. 4	0.17	0.16	0.05	0.06	0.03
col. 5	0.26	0.12	0.08	0.10	0.02
col. 6	0.25	0.14	0.03	0.05	0.01

PSP status plot

	Mean N stars for estimating PSF
band	u	g	r	i	z
col. 1	30.1	36.5	42.1	41.3	55.0
col. 2	34.2	36.9	42.8	41.7	53.1
col. 3	32.2	37.2	45.4	41.8	55.6
col. 4	34.8	36.9	44.8	41.0	56.2
col. 5	31.5	38.3	43.4	42.0	52.0
col. 6	35.4	38.0	48.1	44.1	58.2

Number of stars used for estimating PSF

	Mean m(aperture)-m(psf) Bias (mag)
band	u	g	r	i	z
col. 1	-0.08	-0.07	-0.07	-0.07	-0.07
col. 2	-0.08	-0.07	-0.07	-0.07	-0.07
col. 3	-0.07	-0.07	-0.06	-0.07	-0.07
col. 4	-0.07	-0.07	-0.06	-0.07	-0.07
col. 5	-0.07	-0.07	-0.07	-0.07	-0.07
col. 6	-0.08	-0.07	-0.07	-0.07	-0.08

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	0.01	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	22.16	21.80	20.75	20.09	18.97
max	22.22	21.97	20.87	20.23	19.12
min	21.84	21.14	20.54	19.89	18.86

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	-0.04	-0.02	-0.01
col. 2	-0.02	0.00	0.01	-0.01	-0.04
col. 3	-0.01	-0.01	0.00	-0.00	-0.03
col. 4	0.02	-0.00	0.02	0.02	-0.02
col. 5	0.04	0.03	0.01	0.02	0.07
col. 6	-0.04	-0.00	-0.00	-0.01	0.03

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	1.05	1.01	1.00	1.08	1.03
col. 2	0.83	1.02	1.04	1.04	1.07
col. 3	1.00	1.05	1.00	1.08	1.03
col. 4	0.92	1.04	1.08	1.05	1.08
col. 5	1.02	1.07	0.99	1.01	1.04
col. 6	0.88	1.02	1.05	1.07	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).