Central Bureau for Astronomical Telegrams
IAUC 5516: 1992i; HV Vir; N Cyg 1992
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Circular No. 5516
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Telephone 617-495-7244/7440/7444 (for emergency use only)
TWX 710-320-6842 ASTROGRAM CAM EASYLINK 62794505
MARSDEN@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)
COMET BRADFIELD (1992i)
R. H. McNaught, Anglo-Australian Observatory, reports the
following additional precise positions from Uppsala Southern Schmidt
telescope films:
1992 UT R.A. (2000) Decl.
May 5.80220 0 37 46.30 -15 41 35.4
5.80454 0 37 47.26 -15 41 35.0
Total visual magnitude estimates: May 5.77 UT, 9.4 (G. Garradd,
Tamworth, N.S.W., 0.25-m reflector); 5.80, 9.3 (D. Seargent, The
Entrance, N.S.W., 25x100 binoculars; 3' coma).
HV VIRGINIS
P. Szkody and D. Ingram, University of Washington, report:
"Time-resolved CCD photometry of the very-large-outburst-amplitude
dwarf nova HV Vir on Apr. 30.34-30.42 and on May 1.20-1.25 and
1.34-1.42 UT with the 1.8-m ARC telescope indicate superhumps of
0.2 mag amplitude and period of 84.1 +/- 0.4 min. The V magnitude
was about 13.4 and indicates that the object is declining from
outburst. Since the superhump period is a few percent longer than the
orbital period, HV Vir increases the correlation of large-outburst
amplitude with orbital periods below the period gap for high galactic
latitude dwarf novae (Howell and Szkody 1990, Ap.J. 356, 623);
11 of the 12 with known orbital periods are now below the gap."
Visual magnitude estimates (cf. IAUC 5504): Apr. 24.86 UT,
12.7 (P. Schmeer, Bischmisheim, Germany); 25.88, 13.0 (O.
Midtskogen, Tranby, Norway); 26.02, 12.9 (H. Dahle, Oslo, Norway);
28.07, 13.0: (J. E. Bortle, Stormville, NY); 29.90, 13.3 (Dahle);
30.88, 13.6 (Schmeer).
NOVA CYGNI 1992
R. J. Ivison and M. K. Bang, Lancashire Polytechnic; and M. F.
Bode, Liverpool Polytechnic, report the detection of Nova Cyg 1992
with the 15-m James Clerk Maxwell Telescope, Mauna Kea, on Apr.
25.6 UT. Measured continuum flux densities were 1.43, 0.83, 0.77,
and 0.53 Jy at 0.8, 1.1, 1.3, and 2.0 mm, respectively. A 3-sigma
upper limit of 4.0 Jy was obtained at 0.45 mm. Uranus and W75N
were the primary and secondary calibrators. These data suggest a
10-fold rise in the 1.3-mm flux density over a period of little
more than a month (IAUC 5476).
1992 May 7 (5516) Daniel W. E. Green
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