Central Bureau for Astronomical Telegrams
IAUC 2720: N Sgr 1974; BINARY PULSAR; SU Tau; 1973g; 1973f
The following International Astronomical Union Circular may be linked-to from your own Web pages, but must not otherwise be redistributed (see these notes on the conditions under which circulars are made available on our WWW site).
Read IAUC 2721
Circular No. 2720
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 SAGITTARII 1974
The following visual magnitude estimates have been reported:
Oct. 16.39 UT, 9.5 (A. F. Jones, Nelson, New Zealand); 17.0, 9.6
(E. Mayer, Barberton, Ohio); 20.0, 9.6 (P. Morrison, Lexington,
Mass.); 20.79, 9.2 (Young, Shanklin and Burch, University of Cambridge);
22.0, 9.7 (Mayer); 22.71, 9.9 (D. P. Elias, Athens); 23.72,
9.8 (Elias); 27.0, 9.8 (Mayer); 28.0, 9.7 (Morrison); Nov. 2.04,
9.4 (K. Simmons, Jacksonville, Florida).
N. Vidal, Mount Stromlo and Siding Spring Observatories,
writes: "Image-tube spectra taken with the 190-cm telescope (200 A/mm)
on Nov. 7.44 UT show the Balmer lines from H-alpha to H-epsilon, Fe II
(multiplet 42) and Na I 5892 A, with broad emission lines flanked
shortward by two systems of absorption lines. The positions of the
emission lines (distorted) are a few hundred km/s shifted to the
red. The two systems of Balmer absorptions show velocities of
-3330 +/- 100 and -1650 +/- 100 km/s. The Fe II systems show -3160 +/-
50 and -1200 +/- 35 km/s, and Na I shows -3050 +/- 35 and -1130 +/- 35
km/s. A broad emission blend (halfwidth ~ 90 A) appears at 4640 A
and is flanked by two absorptions. Emission lines of O I are conspicuous
at 6100-6400 A. An unidentified strong line (with a core)
is found at about 5625 A. This overall picture seems to indicate
that the nova is in its final stages of the early decline in which
the 'Orion spectrum' and the '4640 A stage' exist together."
BINARY PULSAR
C. Papaliolios and C. Pennypacker, Department of Physics,
Harvard University; and C. Canizares and J. McClintock, Center for
Space Research, Massachusetts Institute of Technology, report the
absence of a 59-ms optical pulsar near the binary pulsar discovered
by Taylor and Hulse (IAUC 2704). Using the Harvard 155-cm telescope,
a 29"-diameter aperture was placed at 24 locations to cover
completely an area 104" (east-west) by 116" (north-south) centered
at R.A. = 19h13m13s, Decl. = +16o00'05" (equinox 1950.0). Data were
recorded for 5 min at each location and were subsequently Fourier
analyzed to search for a periodic signal. A magnitude limit of
about 18.5 can be set for the optical pulsar (~ 10-percent duty
cycle assumed). In a separate but similar search with a 2'-diameter
aperture a magnitude limit of about 17.5 can be set for an optical
pulsar within a 4' diameter circle centered on the same location.
The candidate suggested by Bernacca and Ciatti (IAUC 2714) is at the
center of both searched areas and is thus ruled out.
SU TAURI
Mrs. Janet Mattei, Director of the American Association of
Variable Star Observers, communicates the following visual magnitude
estimates: Oct. 5.28 UT, 14.4 (E. Mayer, Barberton, Ohio);
11.21, 13.9 (Mayer); 22.19, 12.8 (Mayer); Nov. 14.2, 12.6 (G.
Kelley, Glade Spring, Virginia); 18.2, 12.0 (R. Annal, Barstow,
California). These confirm the rise reported by C. Scovil (IAUC
2707). Mrs. Mattei adds that the star has been fluctuating
between magnitudes 14.5 and 15.5 for the past year.
PERIODIC COMET REINMUTH 2 (1973g)
The following precise positions, by T. Seki (Geisei), are from
Orient. Astron. Assoc. Comet Bull. No. 93:
1974 UT R. A. (1950) Decl. m1
Oct. 13.68264 3 36 59.86 +30 15 24.8 15.5
23.69097 3 30 38.62 +30 05 45.4 16
COMET KOHOUTEK (1973f)
Mrs. G. R. Kastel', Institute for Theoretical Astronomy,
Leningrad, communicates the following precise positions, obtained by
N. S. Chernykh at the Crimean Astrophysical Observatory. Measurer:
L. I. Chernykh. Reduced at I.T.A.
1973/74 UT R. A. (1950) Decl.
Dec. 12.15489 15 03 43.09 -24 39 57.0
Jan. 4.65074 20 16 36.03 -16 07 04.5
5.64861 20 28 32.68 -15 19 06.9
11.65170 21 39 10.89 -10 01 30.1
14.69124 22 14 00.17 - 7 04 51.8
15.72278 22 25 32.05 - 6 04 07.5
19.66812 23 07 40.52 - 2 15 37.9
30.71690 0 43 22.18 + 6 23 13.4
30.72170 0 43 24.26 + 6 23 22.9
Feb. 10.71507 1 47 53.82 +11 34 08.0
10.72135 1 47 55.54 +11 34 15.4
12.72175 1 57 14.77 +12 14 48.7
12.75299 1 57 23.08 +12 15 25.1
14.70617 2 05 55.32 +12 51 28.7
14.73603 2 06 02.91 +12 52 02.0
15.76498 2 10 20.35 +13 09 41.8
15.77259 2 10 22.38 +13 09 50.2
18.71600 2 21 57.39 +13 56 16.1
18.73441 2 22 01.58 +13 56 32.1
1974 November 21 (2720) Brian G. Marsden
Read IAUC 2721
Our Web policy. Index to the CBAT/MPC/ICQ pages.
