Central Bureau for Astronomical Telegrams
IAUC 2714: SN IN NGC 7343; 1974b; BINARY PULSAR
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Read IAUC 2715
Circular No. 2714
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
SUPERNOVA IN NGC 7343
A. Bianchini, F. Ciatti and L. Rosino, Asiago Astrophysical
Observatory, write: "Spectrograms of the supernova were obtained on
Oct. 16-18 with the prism spectrograph attached to the 182-cm reflector
(dispersion 210 A/mm at H-gamma), using the Westinghouse image
tube. The spectrum is that of a type I supernova, characterized by
the strong absorption feature near 6150 A, and by the presence of
broad emission bands at about 6500, 5900, 5750, 5250, 4930 and
4620 A. The overall behavior of the spectrum indicates that maximum
was reached from 10 to 20 days earlier. Schmidt plates of Sept.
11-12 do not show any star brighter than magnitude 17 at the position
of the supernova. On Oct. 12 the magnitudes were estimated as
B = 15.75, V = 15.90."
COMET BRADFIELD (1974b)
The following precise positions have been reported:
1974 UT R. A. (1950) Decl. Observer
Feb. 24.42431 0 19 40.53 -29 23 49.3 Herald
27.41745 0 31 34.96 -27 44 54.6 "
27.43669 0 31 39.42 -27 44 16.8 "
Mar. 1.44167 0 39 52.58 -26 26 26.8 "
2.42639 0 43 58.84 -25 44 02.1 "
2.43212 0 44 00.25 -25 43 44.0 "
4.41667 0 52 21.81 -24 09 25.6 "
27.78344 2 13 35.21 +19 14 41.2 Korhonen
27.80662 2 13 37.79 +19 18 28.9 "
28.80421 2 15 24.31 +22 02 58.4 "
28.81616 2 15 25.56 +22 04 58.8 "
31.78533 2 19 52.59 +30 07 08.6 Niemi
31.81565 2 19 55.09 +30 11 57.6 "
Apr. 3.83845 2 23 19.66 +37 55 27.6 Korhonen
9.84104 2 27 45.43 +51 10 28.7 Snare
9.84974 2 27 45.65 +51 11 31.2 "
18.85545 2 31 37.41 +65 50 23.9 Korhonen
18.87698 2 31 38.12 +65 52 09.2 "
18.88274 2 31 37.59 +65 52 34.2 Snare
18.89830 2 31 38.08 +65 53 48.2 "
22.87772 2 33 20.65 +70 50 56.9 Korhonen
22.88466 2 33 20.85 +70 51 24.5 "
24.99719 2 34 26.89 +73 12 42.9 Snare
25.00396 2 34 27.16 +73 13 12.4 "
25.84333 2 34 55.98 +74 06 41.7 Korhonen
25.85774 2 34 56.79 +74 07 35.9 "
May 2.90428 2 41 32.49 +80 47 47.0 Lehtinen
10.89042 3 13 57.0 +87 05 26.3 "
10.93069 3 14 27.2 +87 07 11.0 "
12.91403 3 58 42.4 +88 29 49.2 "
12.97375 4 01 19.3 +88 32 09.0 "
13.91681 5 09 38.7 +89 06 34.4 "
13.93208 5 11 30.1 +89 07 04.0 "
D. Herald (Barton, near Canberra). Improved measurements of the
observations mentioned on IAUC 2647 and 2661.
T. Korhonen, A. Niemi and J. Lehtinen (Astronomical-Optical Institute,
Turku, Tuorla Station). Communicated by L. Oterma.
M.-A. Snare (Astronomical-Optical Institute, Turku, Kevola Station)
Long. = -1h31m00s (correction to IAUC 2661).
BINARY PULSAR
W. Liller, Harvard College Observatory, reports that he has
examined several plates from every year from 1891 through 1953 and
finds no evidence of a nova, supernova or other kind of variable
object with mpg <= 11 within 10' of the binary pulsar discovered by
Taylor and Hulse (IAUC 2704). No object with a proper motion > 0".1
per year brighter than mpg = 16 was found in this same area.
P. L. Bernacca and F. Ciatti, Asiago Astrophysical Observatory,
report that a suspected optical pulsar, of magnitude 13.5,
has been discovered at R.A. = 19h13m12s, Decl. = +16o00' (equinox 1950.0),
which is within the improved error box of the radio pulsar. A 20"
diaphragm was used. The central star is a close visual pair. They
add that further observations should be made synchronized with the
59-ms pulsar period.
R. St. John and V. H. Regener, Department of Physics and Astronomy,
University of New Mexico, report that an attempt to photograph
the binary pulsar with the Capilla Peak 61-cm reflector produced
negative results. Eight 30- to 60-min exposures were made on
Oct. 15 and 16 through a rotating shutter synchronized to the
apparent pulsar period. The period was corrected for Doppler shift
using heliocentric orbital information on the binary furnished
privately by J. H. Taylor. After shifting the phase of the shutter
180o between pairs of plates, each pair was then visually scanned
for changes in the intensity of all stars to magnitude 17. Candidates
were later checked for optical pulses by counting photoelectrons
with a synchronized multiscalar.
1974 November 12 (2714) Brian G. Marsden
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