Background: We (the HOYS-CAPS project team) 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 obscurations 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 occultations is: B~16.4, V~15.3,
R~14.3, I~13.3; During the occultations 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 behavior 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 seperately.

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/

\/ \/
(oo) (oo)
'Life is what happens to us when we're making other plans.'
Dr Dirk Froebrich
Senior Lecturer for Astronomy and Astrophysics
Director of Undergraduate Studies
Director of the Beacon Observatory
Centre for Astrophysics & Planetary Science
School of Physical Sciences, Ingram Building, Room 117
The University of Kent
Canterbury CT2 7NH, U.K.

telephone: 00-44-(0)1227-827346
email: df@star.kent.ac.uk
www: http://astro.kent.ac.uk/~df/
office hours: on appointment only

In Association with Amazon.co.uk