Central Bureau for Astronomical Telegrams
IAUC 2826: N Cyg 1975
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Read IAUC 2827
Circular No. 2826
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
NOVA CYGNI 1975
Word of M. Honda's discovery of this nova was received from K.
Osawa, Director of the Tokyo Astronomical Observatory, by cablegram
last Friday afternoon; it was relayed by cablegram, telegram and
telephone to various observatories and individuals around the world
at that time. Unfortunately, a long holiday weekend in the U.S.
has delayed the production of this Circular.
Among the many hundred independent discoveries that must have
been made of the nova during the 24 hours following its rise to
naked-eye brightness are the following: Aug. 29.48 UT, m_v = 3.0
(Kentaro Osada, Yamaguchi, Japan); 29.57, 3.0 (Minoru Honda, Kurashiki,
Japan); 29.64, 2.7 (Shigeru Ito, Japan); 29.67, 2.5 (30 persons,
Nihon University Astronomical Study Group); 29.78, 3.0 (N.
Hashimoto, Japan); 29.8, - (S. Yu. Shugarov, Sternberg Astronomical
Institute); 29.81, 2 (L. Kohoutek et al., Hamburg Observatory);
29.81, 2.5 (G. Richter and W. Gotz, Sonneberg Observatory); 29.83,
2.6 (J. Lefevre, Brussels, Belgium); 29.83, 3 (Y. Shefer, Tel Aviv,
Israel); 29.83, - (Baranowski and Garbacz, Poland); 29.84, 3-3.5
(Schroeder, Norway); 29.9, 3 (J. W. Schippers et al., The Netherlands);
29.9, 2.5 (E. Madlow, Berlin, Germany); 29.9, - (M. Schnitz
and M. Durkefalden, Hannover, Germany); 29.9, 2.5 (R. Callus, The
Hague, The Netherlands); 29.9, 2 (Deterwagne, Antwerp, Belgium);
29.92, 2.8 (M. H. Marx and H. J. Trumpp, Stuttgart, Germany); 30.04,
2.2 (R. Jones et al., Statesville, North Carolina); 30.05, 2 (K.
Cernis, Vilnius, U.S.S.R.); 30.05, 2.3 (P. Garnavich, Bowie, Maryland);
30.06, 2 (D. Lemay, Rimouski, Quebec); 30.06, 1-2 (E. J.
Seykora and A. C. Thompson, Greenville, North Carolina); 30.07, 2.5
(J. L. Kuhns, Thunderbolt, Georgia); 30.07, 2.0 (G. W. Kelley,
Glade Springs, Virginia); 30.08, 2 (G. Kirby, Granite Falls, North
Carolina); 30.08, 2.4 (J. F. Stone, Stillwater, Oklahoma); 30.09, 2
(E. F. Dodds, Mussle Shoals, Alabama); 30.09, 2 (R. Johnson, Lincoln,
Nebraska); 30.1, 2.5 (D. Duke et al., Coral Gables, Florida);
30.10, - (H. L. Miller, Norfolk, Virginia); 30.10, 1.7 (T. W.
Edwards, Columbia, Missouri); 30.10, - (A. Lockett, Los Alamos, New
Mexico); 30.1, - (R. Maim, Los Altos, California); 30.1, - (J.
Cannon, Minot, North Dakota); 30.11, 2.0 (W. Gates and J. Prentice,
Albuquerque, New Mexico); 30.1, 2.5 (D. Wallace, Arecibo Ionospheric
Observatory); 30.12, 2.3 (P. Maloney, Mountain View, California);
30.12, 2.0 (A. R. Upgren, Margate, New Jersey); 30.1, 2 (W. G.
Dillon, Springfield, Virginia); 30.1, 2 (R. Gunnerson, Aurora,
Colorado); 30.13, 2-2.5 (C. Richardson et al., Lynchburg, Virginia);
30.15, 2.0 (R. H. Stanton, La Canada, California); 30.15, 2 (F.
King, Camarillo, California); 30.15, 2.0 (R. A. Keen, Boulder, Colorado);
30.16, 2.2 (H. Povenmire, Homestead, Florida); 30.2, 2.1 (D.
Fellers, Topeka, Kansas); 30.2, - (D. Tallant et al., Houston, Texas);
30.21, 2 (C. Tyson, San Mateo, California); 30.21, 2.3 (R.
Sampson et al., Calgary, Alberta); 30.21, - (J. Weisberg, Iowa City,
Iowa); 30.2, 2 (M. D. Decaria, Salt Lake City, Utah); 30.23, 2.1 (D.
Machholz, Concord, California); 30.2, 2.5 (J. W. Wooten, De Funiak
Springs, Florida); 30.27, 1.9 (J. Rather and E. Conquest, Torrance,
California); 30.28, 2.2 (E. B. Hickson, Asheboro, North Carolina);
30.29, 2 (D. Lightfoot, Tulsa, Oklahoma); 30.32, 2.5 (A. Howell,
Colorado Springs, Colorado); 30.33, 2.5 (L. Kemble and P. Bergbusch,
Lumsden, Saskatoon); 30.41, 1.5 (D. Wallentine, Albuquerque, New
Mexico); 30.48, 2 (S. Cooperman, North Hollywood, California).
The following precise position has been reported by C. de
Vegt, U. K. Gehuch and L. Kohoutek, Hamburg observatory: R.A. =
21h09m52s.85, Decl. = +47o56'41".3 (equinox 1950.0); it is a preliminary
result, with 0".3 m.e., obtained using the 23-cm astrograph and five
AGK3 reference stars. H. Debehogne, Royal Observatory, Uccle, has
also reported a precise position, the end figures being 52s.86, 40".5.
The following prediscovery observations have been reported:
Aug. 12 UT, m_pg = 16 (N. N. Samus, Sternberg Astronomical Institute,
Southern station); 28.059, m_pv > 9.6 (P. Garnavich, Bowie, Maryland,
Tri-X film); 29.052, m_pv = 7.5 (Garnavich). Samus remarks that
there is no trace of the object on the blue Palomar Sky Survey
print. De Vegt et al. also remark that there is no star brighter
than magnitude 20 (red) or magnitude 21 (blue) on the Palomar Sky
Survey prints at the position of the nova. They add: "There is
only a weak structure, which could be considered as a star of about
magnitude 21, within 1" of our position for the nova. The nova
lies about 4" southeast of a star of magnitude 19 and about 9" east
of a star of about magnitude 16. The present brightness of the
object implies an amplitude of at least 19 magnitudes, which suggests
that the object might be a supernova."
The following photoelectric magnitude observations have been
reported: Aug. 29.8167 UT, V = 2.55, B-V = +0.35 (D. Ya. Martynov,
Sternberg Astronomical Institute); 30.0470, V = 2.26, B-V = +0.45
(Martynov); 30.96, V = 1.79, B-V = +0.58 (P. Tempesti, Collurania
Observatory; comparison star epsilon Cyg).
Infrared magnitudes by V. I. Shenavrin, Sternberg Astronomical
Institute, on Aug. 29.87 UT: 2.02 at 1.3 um, 1.79 at 2.2 um.
C. R. Purton, York University; and P. Clark, Carleton University,
report that a search for radio emission, using the 46-m telescope
at Algonquin Radio Observatory on Aug. 31 UT, yielded an
upper limit of 0.01 Jy at a frequency of 10.6 GHz.
1975 September 2 (2826) Brian G. Marsden
Read IAUC 2827
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