Arne Henden's collated datasets in SMSP fields

Last updated May 25, 1997

Arne Henden has created files with data from many different nights all combined together. At the moment, there is no documentation describing the information in detail, but I've tried to collect several of Arne's messages that describe them:

Note 1

My rule of thumb on these collated lists are:

1. no star with fewer than two detections is kept.
2. a detection is when two observations are within 10 arcsec of each other, and the observations are with different cameras.

This means that my lists will miss categories of objects; for example, those that are moving, and those where the cameras are not covering common regions of the sky. I've done this to be conservative. A better way to generate these collated lists would be to create them for the entire night's scan, rather than for the three smsp fields. The current software can handle an entire scan if it were uploaded that way.

Note 2

The lists are collated using my COLLATE program (the source is found under /pub/outgoing/aah/tass/sources/collate.f1), and consist of 3 lines/star, with mean RA/DEC and data for camera 1 on line 1, data for camera0 on line 2, and data for camera2 on line 3. The only objects that make the list are those where two or more cameras saw the same object, and where the coordinates agreed to within 10 arcsec radius. MG's collated data files have names like d_c_0547.744, where d=Gutzwiller, c=collated, and numerics are the jd and jdfraction for the earliest file processed in the collation.

Note 3: May 25, 1997

It has been cloudy at the 4m, so I've taken the time to revise (yet again) the difcal program, and upload new versions of fieldx.dif to our ftp server. The source for the new difcal is under /pub/outgoing/aah/tass/sources/difcal.f4. This version uses more comparison stars and has a header line for column identification. Each line contains a few new fields: sigV and sigI are the photometric errors based on the comparison stars (does not include the program object's photometric error); nc is the number of comparison stars used. A single iteration to reject discrepant comparison stars is performed.

I think these differential magnitudes are as good as we can do until we understand the individual photometric errors. However, at least some of the discrepant points have been cleaned up, so these new file versions should be easier to work with.