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/