Session of pointing monitoring the 20-25 of July 2007 <<BR>>
We check the evolution of the of the flux of the  pointing sources used for the bolometer
observations.

<<TableOfContents>>


=== Summary ===
We observed the pointing sources doing a pointing and an Onf-Off
measurements in most of the cases.

   * 100 pointing sources observed and usable for the analysis
   * 6 sources are found to be too faint (<100 mJy): J0121+044, J0750+827, J1056+702, J1628-143, J1909+486 J1628-143, J2106+216
   * 16 observations of primary and secondary calibrators were done: Uranus, K3-50A, MWC349, LKHALF234, G34.3, CW-LEO, G10.62, NGC7538, G45.1



=== Pointing status ===

The plot below shows the '''azimuth''' (blue) and '''elevation''' (red) corrections. 

{{attachment:pointingCorr20-25.06.07.png}}


From that pointing session, a new pointing model was derived by JP and implemented. The parameters P2 and P7 (offsets) were changed.



=== Flux ===

The pointing sources are normally radio-galaxies. They can present strong variation of their radio continuum flux. The goal of this monitoring session was to check the current flux of a sub-sample of pointing sources and flag the sources with a millimetric flux too low. In the current system the Xephem is written if the flux is larger than 100 mJy. The pointing source list for Xephem has been written to follow the update of the flux measurements. <<BR>>
Here is the list of the sources with a  measured flux > 100 mJy and < 150 mJy: <<BR>>
J1333-198 <<BR>> 
J2106+216 <<BR>>
J1638-143 <<BR>>
J2138-247 <<BR>>
J2007+661 <<BR>>

The new fluxes have been automatically added to the database.

=== Conclusions ===

   * The 1 mm flux of about 100 sources was measured down to ~50 mJy with the bolometer Mambo2.
   * The updated flux has  allowed to give an updated picture of the pointing source flux. It allowed to update the XEphem files used for the observations with the updated flux.
   * Still '''1611 radio sources''' in the DB have an unknown flux.
   * A very precise pointing model was obtained thanks to  the large sample observed.
   * One or two similar sessions per year would allow to have an updated list of flux for the bolometer pointing source and may increase the number of new detected radio sources, especially in the sky area with a low density of pointing sources.