Central Bureau for Astronomical Telegrams
IAUC 2892: V1500 Cyg; AO 0235+164; PG 2337+12
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Circular No. 2892
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Cable Address: SATELLITES, NEWYORK
Western Union: RAPID SATELLITE CAMBMASS
V1500 CYGNI
P. C. Gregory and W. H. McCutcheon, Physics Department,
University of British Columbia, report that observations on Dec. 15.75
UT with the Algonquin 46-m radio telescope gave a flux density of
35 +/- 6 mJy at a frequency of 10.5 GHz.
P. Tempesti, Collurania Observatory, writes that the amplitude
of the short-period variations in the V magnitude (cf. IAUC 2834,
2842) had decreased to 0.03 on Oct. 2. The various observations
indicated that the period varied between 0.137 and 0.141 day.
AO 0235+164
W. Liller, Center for Astrophysics, Harvard and Smithsonian
Observatories, reports that L. J. Eachus has made a careful survey
of this eruptive BL Lac-type object (cf. IAUC 2867), using plates
in the Harvard collection. She finds only one definite outburst,
in 1939-40, when the star reached B ~ 15.8 and remained brighter
than B = 17 for more than 100 days but less than a year.
PG 2337+12
J. Kristian, Hale Observatories, reports that R. F. Green
noted this high-latitude object with ultraviolet excess (R.A. =
23h37m50s, Decl. = +12o21'.0, equinox 1950.0) near magnitude 13.5 on
1973 July 2 and on the Palomar Sky Survey (1951 Aug. 10). Multi-channel
spectrophotometry by J. L. Greenstein on 1974 Aug. 9 classified
it as DAs (Gr 336) and gave V = 13.12; the hydrogen lines were
very weak. Green's photoelectric measurements show it at y = 13.32
on 1974 Oct. 14, but recently it was at y = 15.87 and 15.52, on
1975 Nov. 10 and 11, respectively; there was an increase of +0.40
in the 1975 b-y color. On 1975 Nov. 26 Greenstein and A.
Boksenberg, using the image photon-counting system of University
College, London, at the Hale reflector, found apparent changes in
hydrogen-line profiles on a half-hour timescale. A variable central
emission is found in a weak H-gamma line about 60 A wide. H-delta is in
absorption and sharper. The present spectrum resembles that of the
recurrent nova WZ Sge. PG 2337+12 is unusual in the weakness of
its lines and in having remained bright for so long. A photometric
history would be valuable, and it might also be interesting to
examine existing x-ray data for a source at the position.
1975 December 29 (2892) Brian G. Marsden
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