Background: We have recently discovered that the young star V1490Cyg  (20:50:53.6 +44:21:01, situated in the Pelican Nebula IC5070) is periodically occulted by material in its circumstellar disk(*). Our  light-curves indicate a period of about 32days, and the obscuration's are comparable to UX-Ori type eclipses.

      We will be conducting a 1.5 month, high cadence, multi-wavelengths optical monitoring campaign (in BVRI) of this source to map out in high resolution the azimuthal distribution of the material in the disk around this young star. Our campaign will run from 01.08.2018 to 15.09.2018 and we will use three 'observatories':

      i) Daily observations with the LCO (in particular the 1m telescope at the McDonald Observatory (longitude ~104deg West). This also includes spectroscopy of the source every 5 days.

      ii) Daily observations with the University of Kent's Beacon Observatory (longitude ~1deg East).

      iii) The observations will be supported by UK amateur astronomers who work with us already as part of our HOYS-CAPS(**) citizen science project and are distributed across the entire UK.

      We estimate that the optimal cadence to fully map the azimuthal distribution of material in this object is about 6-8hrs.

      Observations: We request CCD or DSLR observations of the target as often as possible and in as many optical filters as are available. In particular we would like BVRI observations, but U and Halpha are welcome as well if the equipment is available and the object can be detected.

      The brightness of the object outside occultation's is: B~16.4, V~15.3,  R~14.3, I~13.3; During the occultation's the object will be up to 1.5mag fainter in all filters. Thus, all the observations should be deep enough to detect the target star at all states with good signal to noise, as we do not know the exact behaviour of the object during this period.

      All images should be dark and flat-field corrected. The field of view should be large enough to ensure a sufficient number of comparison stars is available to perform an accurate relative photometric calibration.

      Please stack individual images taken in the same filter per night for an improved signal to noise before submission, but only if they are taken no further apart than 2hrs. Images taken over a longer duration should be stacked separately.

      Data Submission: As this object is in IC5070, and thus part of our HOYS-CAPS citizen science project, the reduced images should be submitted in FITS format via our web-upload system (***). Once they are processed the photometry of all the stars in the images will be available immediately publically via our web interface.

      To ensure accurate processing, the FITS header should contain information of the filter used, the total exposure time of the stacked images and the mid-point of the integrations in each stack.

      In case of any questions please contact the PI at df@star.kent.ac.uk or use the HOYS-CAPS facebook group(****)

      (*)    http://adsabs.harvard.edu/abs/2018RNAAS...2b..61F
      (**)   http://astro.kent.ac.uk/~df/hoyscaps/index.html
      (***)  http://astro.kent.ac.uk/HOYS-CAPS/
      (****) https://www.facebook.com/groups/342831266192555/