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THE ASTRONOMER Electronic Circular No 960       1995 May 24 06.28UT
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
Further to the announcement on E948, Stephen Boyle, Mill Hill
Observatory, UK has, at the request of the Editor, carried out a
further investigation of possible candidates on the Palomar
Sky Survey. He reports as follows:

I have measured the position of the star identified as UW Per on
your TA/AAVSO/Duerbeck charts/photos.  This measurement was made
from a positive contact plate I exposed under a Palomar II
reproduction on film.

The position I obtained was:
   RA(2000.0) = 2h 12m 29s.63    Dec(2000.0) = +57d 5' 19''.5

This is in good agreement with the positions obtained by Duerbeck
and also Downes & Shara (cf E948-Editor).

It seems likely, however, that it is not correct to identify this
star as UW Per. In addition to the disagreement with my measurement
of the d'Esterre plate, the original candidate has identical
brightness on the Palomar I (1954) and Palomar II (1990) images.

The latter suggests (but, I appreciate, does not prove
conclusively) that this star is not an eruptive variable.

I have not yet found a convincing candidate for UW Per at minimum
brightness from the Palomar II image but research continues.

Editor:
If the star is a dwarf nova, it evidently has outbursts at very
long intervals. It is therefore likely that the amplitude will be
large, possibly seven magnitudes or more. Given the maximum
magnitude I reported on E948, it is quite possible that the star
may be magnitude 22 or fainter at minimum.

Guy M Hurst