On the night of August 29, 2001 UT, Matt Aggleton and Michael Richmond used the RIT Observatory's 10-inch Meade LX200 telescope to monitor WZ Sge. All exposures were taken without the focal reducer, through a V-band filter, onto an SBIG ST-8 CCD camera. Each exposure was 10 seconds long. Due to the design of the SBIG software, the time of each exposure is accurate only to +/- 1 second. The field of view was about 17 by 12 arcminutes; a typical example is shown below (North is up, East to the left):
We subtracted dark current from the images and divided by a median twilight sky flatfield. We ran software to detect all stars more than 4 sigma above the sky, then measured the light from each star within a circular aperture of radius 6.6 arcseconds.
The night was good: no clouds, but a bright waxing gibbous moon.
We gathered about 700 images of the field. We fed all raw instrumental magnitudes of 109 stars into a program which implemented Honeycutt's inhomogeneous ensemble photometry technique. The solution gave most weight to the stars marked "A" and "B" in the chart above. The standard deviation from the mean magnitudes in the solution are shown below, as a function of differential magnitude.
The solution placed the mean magnitude of stars "A" = GSC 1612.1830 = HD 191083 and "B" = HD 351517 as follows:
star mean stdev
A 0.0 0.005
B 0.983 0.007
We used star "B" as a check star to detect errors due to clouds or poor images (which clearly were present in the entire night's run). We discarded any image in which star "B" differed from its mean magnitude by more than +/- 3 times its standard deviation.
The final result is 697 measurements of WZ Sge, over a period of 5 hours. Here is the light curve:
You can download an ASCII text file with the measurements:
The file has some comments at the top, followed by data lines with 4 numbers per line, like this:
Jul_27.06510 2117.56510 2117.56977 0.046
The columns are:
Last modified 8/30/2001 by MWR.