Confirmatory observations of newly discovered fainter NEO candidates
Some of new search facilities produce discoveries fainter than mag. 20 V
(1.8-m Spacewatch II, 1.2-m Palomar/NEAT) which need larger telescope
for confirmation and early follow-up.
1-m class telescope is also very suitable for confirmation
of very fast moving objects and our larger FOV enables to search
for NEO candidates having larger ephemeris uncertainty.
Recoveries of NEOs in the second opposition
For the determination of reliable orbits it is required to observe asteroids in
more oppositions. If observed arc in discovery apparition is long enough,
the chance for a recovery in next apparition is good. If the observed arc at single
opposition is not so good, we plan to search along the line of variation based on
data from Minor Planet Center databases (Marsden, Williams), Lowell Observatory
databases (Bowell, Koehn), and Klet Observatory databases (Tichy, Kocer)
Follow-up astrometry of poorly observed NEOs
It is necessary to observe newly discovered NEOs in longer arc during
the discovery opposition when they get fainter. A special attention is given
to "Virtual Impactors" and PHAs, target of future space missions
or radar observations. There is also need for some observational effort
at further oppositions.
On the other hand, it is necessary to find optimal observing strategy to maximize
orbit improvement of each asteroid.
Follow-up astrometry of other unusual objects, i.e. Centaurs, transneptunian objects
We plan to make follow-up astrometry of these objects, both in discovery opposition
and next apparitions. To obtain positions of brighter transneptunians, we
propose to use longer, several minutes exposures with magnitude limit about V = 22 mag..
Up to this limit there will be only some 10 - 20 brighter transneptunian objects from
more than 400 known, but considering the problem with securing adequate data for orbit
computation of these objects, follow-up astrometry at least of some of them will be useful.
Analysis of possible cometary activity of newly discovered bodies.
Search for new asteroids
Our primary goal is astrometric follow-up of unusual objects.
If observations will be planned effectively, there will be also time for searching.
We expect by our experience about one third of the whole observing time will be
devoted to searching. Moreover, all
CCD images will be processed not only for target objects, but also tested for possible
new objects. Regarding on effective field of view, observing time, limiting
magnitude of V = 22 mag. and existing models there is possibility to find several
hundreds of new objects per year. Obtained images will be processed with special
reference to fast moving objects and slowly moving objects.