|Proposer||(19714) Tonis Eenmae (email@example.com) obscode: ETOA|
|Assigned To||(3663) Dirk Terrell|
|Date Submitted||Oct. 10, 2017|
Dear AAVSO team,
We have previous photometric observations of this system from VARMAS survey (from 2011-2015, first results in https://arxiv.org/abs/1611.02452) showing that Be star in the system is very active, it has frequent large-amplitude optical outbursts (so called phase changes of disc build-up and break-down) - amplitudes in V and I filters 0.3 and 0.6 magnitudes, respectively. To be able to properly interpret X-ray observations and optical spectroscopy of such rapidly changing system, reasonably dense time-series of optical flux measurements would be very much needed.
We would like to ask monitoring of that system in B,V,R,I filters with cadence ca 2x per week till the end of the season (probably up to Christmas 2017, when object is above airmass 2), with targeted SNR=300...500 (from Poisson statistics!). If it is appropriate from amount of data viewpoint, 3 exposures per filter would be most useful. Magnitude estimates according to Simbad and VSX are B=13.1, V=12.0, R=10.6, I=9.7, it is known that the region is rather reddened by the dust. System is not expected to become dimmer, only brighter up to 1 magnitude.
If it is possible (from the AAVSOnet load point of view) to increase cadence of observations in +-1 week surrounding predicted periastron time to one observation per two days, it would even more useful.
|Target||RA (H.HH)||Dec (D.DD)||Magnitude||Telescope||Observation Frequency||Expiration Date||Proprietary Term|
|MT91 213||20.536981||41.45678||13.2–9.6||—||—||—||6 Months|
Comments on this proposal are closed.