Central Bureau for Astronomical Telegrams
IAUC 2272: N Sct 1970; CH Cyg; 1970g; 1969a
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Circular No. 2272
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 SCUTI 1970
Prof. M. Huruhata, Director of the Tokyo Astronomical Observatory,
cables the following correction to the position by H. Kosai
reported on IAUC 2270. The pre-nova has been identified on the
Palomar charts: blue magnitude 18.6, red magnitude 16.6.
R. A. (1950) Decl.
18 42 59.99 - 8 36 14.0
Prof. Huruhata also sends the following magnitudes, obtained
by comparison with Epsilon Scuti (V = 4.88, B - V = +1.12, U - B = +.91),
with the 91-cm reflector at Okayama station of TAO.
1970 UT V B - V U - B Observer
Aug. 3.65 * 8.3 +.74 -.01 Watanabe
5.55 * 8.4 +.62 Takahashi
9.55 8.7 +.57 -.24 "
10.51 9.0 +.56 -.23 "
* Correction to IAUC 2270
E. Watanabe, Tokyo Astronomical Observatory.
K. Takahashi, Wakayama University.
Marcia J. Keyes writes that approximately 700 plates taken
with the 7.5-inch Cooke triplet at the Maria Mitchell Observatory,
Nantucket, from J.D. 2421871 to 2440483, were examined for earlier
appearances of Nova Scuti 1970. It did not appear on any of the
plates. The average plate limit was about magnitude 15.2 with a
significant number of plates reaching 15.7 and a few going below
16.0. A magnitude of 8.0 on J.D.2440808 (1970 Aug. 9-10) was derived
from a plate using the S.A.O. Star Catalog visual magnitudes.
J. Smolinski and J. Grygar, Dominion Astrophysical Observatory,
write that three spectrographic plates were taken 1970 August 12
and 13 at dispersions 15 and 41 A/mm, covering the range from 3500 A
to 6600 A, with the 183-cm and 120-cm telescopes.
About 20 lines of H I, Fe II, Ca II and possibly Na I were
identified and interstellar components of Ca II H and K are rather
strong. Broad emissions (35A to 45A) each with a very weak blue-shifted
absorption component resemble the P Cygni profiles of the
second type (see J. B. Hutchings, Publ. of the D.A.O. 13, No. 16,
1970). The broad emissions are frequently overlapped by several
(three to five) sharp emission components. The average heliocentric
velocity of the absorptions is -1120 km/s. No significant
difference in velocities between hydrogen and metallic lines was
found.
CH CYGNI
Mr. C. Y. Shao, Harvard College Observatory, reports: Photoelectric
observations of the symbiotic star CH Cyg at Agassiz Station
by J. Goguen, M. Mattei and C. Y. Shao show that its rapid,
irregular light fluctuations, previously amounting to 0.7 mag. in
the ultraviolet (Wallerstein, The Observatory, 88, 111, 1968),
gradually diminished during the past few months. Measures in July
and August 1970 indicate that the rapid variation has completely
disappeared. The star has become 0.8 mag. brighter in V, but 0.8
mag. fainter in U since last March. Its magnitudes on 13 Aug.
1970 were approximately U = 9.6, B = 8.6 and V = 6.9; thus B-V
and U-B now closely resemble those of a normal M6 III giant.
COMET ABE (1970g)
The following precise positions have been reported
1970 UT R. A. (1950) Decl. Mag. Observer
July 10.07689 2 19 17.34 +25 57 26.6 Waterfield
26.97663 2 17 58.96 +34 50 54.1 Mrkos
27.97613 2 17 31.13 +35 31 46.0 "
28.03725 2 17 29.36 +35 34 19.1 "
28.96608 2 16 59.72 +36 13 36.8 "
29.00764 2 16 58.14 +36 15 21.4 Waterfield
29.04763 2 16 57.15 +36 17 10.0 Sykes
29.06017 2 16 56.43 +36 17 39.8 Mrkos
Aug. 3.79757 2 12 15.76 +40 51 8.2 Seki
8.98496 2 4 36.01 +45 55 50.1 6.5 Waterfield
R. L. Waterfield (Woolston Observatory)
A. Mrkos (Klet Observatory)
D. E. Sykes (Woolston Observatory) Communicated by Waterfield.
T. Seki (Kochi Observatory)
PERIODIC COMET FAYE (1969a)
V. Ionescu, Bucharest Observatory, communicates the following
precise position obtained there by C. Cristescu.
1969 UT R. A. (1950) Decl.
Nov. 14.91901 5 31 42.43 + 8 33 41.9
1970 August 19 (2272) Richard B. Southworth
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