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THE ASTRONOMER Electronic Circular No 948       1995 Apr 16 18.59UT
Ed:Guy M Hurst, 16,Westminster Close, Kempshott Rise,  Basingstoke,
Hants, RG22 4PP,England. Telephone/FAX(0256)471074 Int:+44256471074
INTERNET: GUY@TAHQ.DEMON.CO.UK             GMH at AST.STAR.RL.AC.UK
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UW PERSEI
This star, which is on the Recurrent Objects Programme, of the UK
Nova/Supernova Patrol, has been shrouded in mystery since its
discovery in outburst by Charles d'Esterre, of Tatsfield, Surrey in
1912 January.

The star was recorded on photographic plates and was reported to
reach a maximum of about magnitude 13.5. Although d'Esterre quoted
a position, Duerbeck (A Reference Catalogue and Atlas of Galactic
Novae, 1987) revised this based on the selection of the brightest
component of a 'three star blend' appearing on the Palomar Sky
Survey Plates when the star was at minimum.

Recently with valuable assistance from Martin Mobberley (Assistant
TA Editor), Pat Barber (BAA Office, London) and Peter Hingley (RAS,
London) the Editor found a copy of the original discovery plate
in the annexe of the Royal Astronomical Society rooms in London.

This was kindly measured by Stephen Boyle (Mill Hill) with
assistance from Ian Howarth (UCL). The result is shown below
together with a precessed position, calculated by the Editor using
software by Paul Leyland, for the Duerbeck candidate: A further
catalogued position is quoted from the Downes and Shara Atlas (PASP
Vol 105 No 684 [1993 Feb]).

RA  2h12m27.69s DEC +57o05'19.5"(2000) (Boyle, discovery plate)
RA  2h12m29.68s DEC +57o05'19.9"(2000) (Duerbeck precessed )
RA  2h12m29.59s DEC +57o05'19.7"(2000) (Downes & Shara Atlas)

Stephen Boyle reports the uncertainty in both coordinates is 1.5
arc seconds in the latest measure which in part is due to the scale
of the copy plate.

It is therefore not clear whether the brightest candidate proposed
by Duerbeck is the object when at minimum. It may be one of the
other two stars or even another fainter object in a similar line of
sight.

The Editor also obtained magnitude estimates using the discovery
plate. Using the TA sequence for UW Persei (reference [C], 941025),
the estimate was L-4 = 15.1. However a further estimate was also
made using the UV Persei TA sequence (reference [C], 940531) as
this field was also recorded on the same frame. This estimate
yielded K-4 = 14.7.
(The above is an extract from TA Vol 31 No 322 p286 [1995] ).


EASTER
I would like to take this opportunity of wishing all our readers
a very happy Easter.

Guy M Hurst