Central Bureau for Astronomical Telegrams
IAUC 3134: HEAO-1 POINTED Obs; MXB1706-43; SMC X-2 AND SMC X-3; ESO 113-IG 45; V Sge; 1977 UB (SLOW-MOVING OBJECT KOWAL)
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Read IAUC 3135
Circular No. 3134
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 Telex: 921428
Telephone: (617) 864-5758
HEAO-1 POINTED OBSERVATIONS
G. J. Fishman writes: "The HEAO-1 spacecraft is scheduled to
begin limited pointing operations on Nov. 16. The table below
lists the tentative dates for the objects indicated. All pointings
will be some time between 15h00m and 24h00m UT and nominally for
two orbits (~ 3 hours). During Nov. 16-18 the +y axis will be
pointed toward the objects, during Nov. 21-23 the -y axis. At
times other than pointing, the spacecraft will be in its normal
scanning mode with a period of ~ 35 min. The latest pointing information
may be obtained from one of the HEAO-1 investigators or
from Dr. Fishman at the address: Code SA, NASA Headquarters,
Washington, DC 20546, U.S.A. (telephone 202-755-3616)."
Nov. Obj. Remarks Nov. Obj. Remarks
16 SMC X-1 21 SMC X-1
17 Cyg X-1 Binary phase 0 22 Cyg A Strong radio source
18 A 754 Abell cluster 23 PSR 0833-45 Vela Pulsar
MXB1706-43
H. Marshall, F. Li and S. Rappaport, Massachusetts Institute
of Technology, report that the SAS-3 Group has observed five x-ray
bursts from a region of the sky ~ 0.3 square degrees in area, centered
at R.A. = 17h06m.8, Decl. = -43o24' (equinox 1950.0). This error box
is included in a region from which five bursts were previously reported
by Swank et al. (IAUC 3010). The times of the bursts were
as follows: Oct. 23d18h01m29s, 23d18h25m23s, 24d10h08m51s
24d13h32m51s and 25d02h02m34s UT. 3U 1705-44 is apparently excluded
as the source of the bursts.
SMC X-2 AND SMC X-3
J. van Paradijs, Massachusetts Institute of Technology; W.
Schlosser, Ruhr University; and M. Tarenghi, European Southern Observatory,
report that they have observed stars in the error box
for SMC X-2 (IAUC 3125) with the 60-cm Bochum telescope at E.S.O.
The star noted by Sanduleak and Philip (IAUC 3127) stands out because
of its high ultraviolet brightness. On Nov. 8.3 and 9.2 UT
it had V = 14.77, B-V = -0.06, U-B = -1.13. Although U was constant,
V and B seemed to fluctuate on a timescale of 30 min by +/-
0.06 and +/- 0.03, respectively. A 170-A/mm image-tube spectrogram
obtained with the 360-cm telescope shows absorption lines due to
H I, He I, N III, N IV, Si IV and the 4650 A C III-N III-O II blend.
N. Sanduleak, Warner and Swasey Observatory, reports that
using the same plate material described on IAUC 3127 (and noting
the correction to R.A.) he and A. G. D. Philip have found a
fourteenth-magnitude OB star within the error circle for SMC X-3. It is
identical with the emission-line star No. 198 in the survey by Lindsay
(1961, Astron. J. 66, 169, Fig. 2).
ESO 113-IG 45
R. M. West, European Southern Observatory, reports: "Spectroscopic,
photometric and photographic observations at La Silla of
the interacting galaxy ESO 113-IG 45 (R.A. = 1h21m51s.22, Decl. =
-59o03'58".9, equinox 1950.0) have shown that this object is basically
a Type 1 Seyfert spiral galaxy of diameter 75 kpc and at z =
0.845 with a bright (V = 13.23, B-V = +0.20, U-B = -0.95) quasar
(Mv = -24) in the center. It is probably associated with the x-ray
source 2A0120-591 = 4U 0106-59, the optical position being 0o.3
northeast of the x-ray position. X-ray and optical monitoring of
this unique object is highly desirable. The object was identified
as a Seyfert galaxy by Fairall (1977, Monthly Notices Roy. Astron.
Soc. 180, 391), who designated it as F-9."
V SAGITTAE
J. Patterson, McDonald Observatory, writes: "Photometry in
unfiltered light with the 91-cm reflector on June 26 and Oct. 19 reveals
the existence of coherent oscillations in the lightcurve of
this novalike variable. The fundamental period is 47s.7, but comparable
power is contained in the second harmonic (15s.9). The periods
and the amplitudes (0.003 magnitude) are the same on both
nights. This makes the existence of a white dwarf in the system
very likely and lends weight to the suggestion (IAUC 3049) that the
object is a promising candidate for x-ray and polarimetric study."
1977 UB (SLOW-MOVING OBJECT KOWAL)
C. Kowal, Hale Observatories, provides the following precise
positions measured from exposures by A. Dressler and R. Adams with
the 122-cm Schmidt telescope at Palomar (D. Richstone and T. Boroson
should have been mentioned on IAUC 3130 as assisting R. Green):
1977 UT R. A. (1950) Decl.
Nov. 9.24965 2 01 38.06 +11 46 26.8
10.19201 2 01 28.25 +11 45 28.5
Computations by B. G. Marsden and K. Aksnes, Center for Astrophysics,
show that a near-circular orbit solution (cf. IAUC 3130) is
still viable, but an ellipse of very high eccentricity is not.
1977 November 14 (3134) Brian G. Marsden
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