Background

As the coolest of the DOVs, PG 0122+200 is believed to have its cooling dominated by neturino emssions (a factor of ~2.5x that of photon emission). Our goal therefore, of PG 0122 observations, is to aid in determining a Pdot (or rate of period change) to learn more about the details of the neutrino emssions.

For more information, consult the full PG0122 Scientific Justification.

Observing Instructions

A sample lightcurve is shown in the figure at the bottom of this page.

Control Center: The Xcov 18 control center is at Iowa State University's International Institute of Theoretical and Applied Physics (IITAP).

Contacting the Control Center: Consult the Phone Contact List for information on phone, fax, and email for the control center. See the Xcov18 People List for contact information for the other Xcov18 active sites.

Time Check: Please do a clock time check each night before taking data and verify your time with HQ at the beginning of the run, and as often during the run as possible. HQ will have an accurate clock available for phone clock checks. We had many problems with time during Xcov17, so please, check the time before each run!

Data Transfer: There are two ways to send your data and logs at the end of each night.

1. By anonymous ftp to: wet.physics.iastate.edu
   If you use the ftp option, load your data into the "wet/incoming/xcov18/" directory.
   
   
2. Via e-mail to: wet@wet.physics.iastate.edu
   
   We will be reducing the data as fast as they come in, and we'll contact you promptly if we have any questions about, or problems with, the data you send.
   
   In case the IITAP mail/ftp servers go down, there is an emergency email address for use in contacting the control center: wet@iastate.edu.

Observing Logs: We ask that you send a copy of your observation log along with the data, at the same time if you can.

Run start: Please start your run on an integral multiple of ten seconds (times ending in "0"). Check the computer clock just before the start of a run, synchronizing with your master clock to within 0.1 sec if possible.

Integration time: Use 10 seconds integration time for PMT-based systems. Those with CCDs will have to use their judgement (and/or confer with HQ) to obtain the appropriate balance between signal to noise, cycle time, and duty time.

Filters: Use NO filter in all channels. If you are using a blue-sensitive CCD, also please use no filter unless you have a CuSO4 filter available, in which case please contact us at HQ.

Guide star: We have not selected any standard comparison stars for PG 0122. Please pick your own isolated star and send us your ch2 offsets and telescope plate scale so we can verify exactly which star was observed.

Sky calibration: Observers with 3-channel photometers should record sky in all three channels near the beginning and possibly the end of each run to permit accurate cross calibration. Observers with 2 channel photometers should take sky by moving the telescope. We have sometimes in the past used the channel 2 verniers to measure channel 2 sky (only) but we find this is not really reliable. Try to take sky as often as needed, at least once per 1/2 hour, for 3 - 5 good sky points; more are not needed and cause unwanted data gaps in the light curve of the target star.

Apertures: Please use the smallest aperture consistent with getting data of good quality (e.g. no visible loss of light to the edge of the aperture). A general rule of thumb is to use an aperture approximately 8-10 times the diameter of the seeing disk. (An aperture too small can lead to light loss out the edges; one too large adds additional sky noise and possibly opens the field up to nearby contaminating stars.) Record the size of the aperture (in arcsec) in your observing log.

Good luck to each of you.

Click on the plot to download a gzipped postscript version.

Sample PG 0122 Lightcurve.