PSP QA for run 4646, rerun 40

QA produced on Tue May 25 19:56:29 CDT 2004 with photo version v5_4_26

	Field Quality (nFields=380)
quality	nOK	nHOLE	% HOLE
union	380	0	0.0
col. 1	380	0	0.0
col. 2	380	0	0.0
col. 3	380	0	0.0
col. 4	380	0	0.0
col. 5	380	0	0.0
col. 6	380	0	0.0

PSP status plot

PSF width (FWHM arcsec) statistics for column 6, filter r:
Mean PSF width = 1.51
Median = 1.50, min = 1.38, max = 1.78
There are 0 fields ( 0.0%) with PSFwidth > 4.0 arcsec
This run is 380 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	0.28	0.06	0.01	0.01	0.00
col. 2	0.20	0.03	0.01	0.02	0.01
col. 3	0.17	0.03	0.02	0.03	0.03
col. 4	0.11	0.02	0.01	0.01	0.00
col. 5	0.17	0.03	0.00	0.01	0.01
col. 6	0.12	0.02	0.01	0.01	0.01

PSP status plot

	Mean N stars for estimating PSF
band	u	g	r	i	z
col. 1	27.9	43.7	47.5	47.7	55.6
col. 2	33.0	43.1	48.8	47.5	54.2
col. 3	30.2	42.5	49.2	47.4	55.2
col. 4	34.1	44.0	50.6	48.0	54.7
col. 5	31.6	44.7	54.8	52.3	56.0
col. 6	35.8	46.0	54.0	53.3	61.4

Number of stars used for estimating PSF

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

Aperture Correction Bias plot

	Mean m(aperture)-m(psf) Error (mag)
band	u	g	r	i	z
col. 1	0.02	0.02	0.01	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	0.01	0.01	0.01
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	22.25	22.11	21.18	20.25	18.95
max	22.38	22.15	21.22	20.38	19.12
min	22.07	21.95	21.14	20.11	18.77

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	-0.01	-0.02	-0.00	-0.00	0.01
col. 2	0.01	-0.00	0.00	-0.02	-0.04
col. 3	-0.01	-0.00	-0.04	0.00	-0.03
col. 4	0.01	0.00	0.01	0.02	-0.01
col. 5	0.03	0.02	0.02	0.00	0.04
col. 6	-0.04	0.00	0.00	0.00	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	1.02	1.05	0.99	1.11	1.03
col. 2	0.87	1.00	1.03	1.04	1.06
col. 3	0.97	1.05	0.99	1.08	1.04
col. 4	0.91	1.02	1.06	1.03	1.10
col. 5	1.11	1.07	0.97	1.01	1.04
col. 6	0.93	1.03	1.03	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).