Central Bureau for Astronomical Telegrams
IAUC 2216: N Ser 1970; 1970a
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Circular No. 2216
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 SERPENTIS 1970
The following position has been measured at the Tokyo
Astronomical Observatory from a 50-cm Schmidt plate (f = 100 cm):
R.A. (1950) Decl.
18 28 16.36 + 2 34 41.5
Comparison of this plate with the Palomar Sky Survey prints
suggested five possible candidates for identification, their blue
magnitudes ranging from 14.3 to 19.4, and their red magnitudes from
11.2 to 15.9. Mr. T. Seki, Kochi, provides a position differing
from the above by -0.18s, +1.3".
Mr. H. Kosai, Tokyo Observatory, has measured the following
magnitudes from panchromatic plates (without filter) taken by M.
Honda with his Fujinar camera (f = 21 cm, f/4.5):
1970 UT Mag.
Feb. 12.85347 >10.5
13.86007 6.8
The following photoelectric observations have been made by
E. Ichimura, M. Shimizu and E. Watanabe at the Okayama station of
the Tokyo Observatory. These results are preliminary ones.
1970 UT V B - V U - B Note
Feb. 16.86 4.88 +0.84 +0.33
17.84 4.56 +0.96 +0.53
18.84 4.6 +1.1 +0.9 through clouds
Also at the Okayama station, coude spectrograms (10 A/mm) of
the photographic region were obtained by K. Nariai and Y. Yamashita.
At the Dodaira station, prism spectrograms (60 A/mm at H-gamma) of the
photographic and visual regions were obtained by M. Kiyokawa and
S. Kikuchi. On Feb. 16.8 UT the spectrum had the general appearance
of that of an F-type supergiant, with strong absorption lines
of H, Ca II, Fe II, O I, C I and many other ionized metals. The
radial velocity was approximately -500 km/s. Emission components
were also found for some lines between H-alpha and H-beta and for the
Ca II lines. Spectrograms on the following nights show the gradual
decrease in intensity of the absorption lines, accompanied by
broadening. Emission components are increasing in intensity. On Feb.
18.8 UT new diffuse absorption components with larger violet
displacements were visible for the Ca II lines (H and K).
The following visual magnitude estimates have been reported:
1970 UT mV Observer 1970 UT mV Observer
Feb. 15.8 4.9 Kanno Feb. 20.38 4.4 Sweetsir
15.85 4.9 Sugano 20.44 4.8 Lowder
16.8 <4.5 Honda 20.45 5.0 Pilcher
16.83 4.5 Kosai 20.49 4.7 Hodson
16.87 4.9 Seki 21.38 4.6 Mayer
17.8 4.5 Honda 21.38 4.8 Sweetsir
17.83 4.2 Kosai 21.38 4.6 Simmons
17.87 4.7 Seki 21.4 4.8 Rosebrugh
18.4 5.2 Peltier 21.44 4.9 Lowder
18.46 4.5 Lowder 22.36 5.1 Simmons
18.8 4.5 Honda 22.42 4.5 Sweetsir
18.83 3.9 Kosai 22.5 4.8 Rosebrugh
18.85 4.8 Seki 23.5 4.8 "
19.4 5.0 Hurless
Kanno, M. Honda and H. Kosai. Communicated by Tokyo Observatory.
M. Sugano (Akashi, Japan). Communicated by T. Urata.
T. Seki (Kochi Observatory).
L. C. Peltier, C. Hurless, R. Sweetsir, R. Hodson, E. Mayer, K.
Simmons and D. Rosebrugh. Communicated by Margaret Mayall.
W. M. Lowder (Scarsdale, N.Y.). Communicated by J. Ashbrook.
F. Pilcher (Jacksonville, Illinois).
COMET DAIDO-FUJIKAWA (1970a)
Further precise positions have been reported as follows:
1970 UT R.A. (1950) Decl. Observer
Feb. 6.22402 19 51 26.97 - 2 51 45.3 Milet
6.22956 19 51 29.18 - 2 52 11.7 "
6.23024 19 51 29.39 - 2 52 12.0 "
8.85556 20 13 07.54 - 6 26 49.7 Kurosaki
9.87789 20 23 01.49 - 8 01 29.3 Seki
B. Milet (Nice Observatory). Type I tail about 20' long.
T. Kurosaki (Utsunomiya). f = 500 mm, f/5 camera. Long. = -9h19m41.7s,
10**7 Dxy = -343, 10**7 Dz = -252. Measurer: T. Urata.
T. Seki (Kochi Observatory). Correction to IAUC 2215.
1970 February 26 (2216) Brian G. Marsden
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