Central Bureau for Astronomical Telegrams
IAUC 2712: N Sgr 1974; R Aqr; BINARY PULSAR
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Read IAUC 2713
Circular No. 2712
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. 9.47 UT, 9.5 (Y. Kuwano, Hita, Japan); 13.02, 9.2 (M. Mattei,
Littleton, Mass.); 13.44, 9.3 (D. Herald, Canberra, Australia);
13.8, 9.7 (K. Locher, Wetzikon, Switzerland); 13.99, 9.4 (J. Bortle,
Stormville, New York); 15.04, 9.5 (K. Simmons, Jacksonville,
Florida); 16.03, 9.0 (C. Sherrod, North Little Rock, Arkansas);
16.75, 10.0 (Locher); 16.99, 9.3 (E. Mayer, Barberton, Ohio); 17.08,
9.5 (P. Maley, Houston, Texas); 18.0, 9.5 (Bortle); 18.08, 8.9
(Sherrod); 22.0, 9.8 (Bortle); 22.04, 9.4 (Mayer); 23.0, 10.0
(Bortle).
R AQUARII
Dr. K. Serkowski, Lunar and Planetary Laboratory, reports: "The
following polarization was observed for R Aqr on Oct. 14 UT
with the 154-cm reflector. The star is now near minimum light (V =
11.5, U = 12.0). Further observations, in particular spectroscopic
ones, would be desirable during the next few weeks."
lambda_eff P (%) & m.e. theta lambda_eff P (%) & m.e. theta
0.345 um 19.0 +/- 0.9 108o 0.66 um 2.14 +/- 0.03 34o
0.365 um 6.8 +/- 0.2 109 0.88 um 2.25 +/- 0.02 31
0.45 um 0.5 +/- 0.1 3 0.96 um 2.21 +/- 0.02 35
0.53 um 1.79 +/- 0.07 20
BINARY PULSAR
B. Margon and A. Davidsen, Space Sciences Laboratory, University
of California at Berkeley; and K. Mason and P. Sanford,
Mullard Space Science Laboratory, University College, London, report
that they have searched unsuccessfully for x-ray emission
from the binary radio pulsar reported by Taylor and Hulse (IAUC
2704). One hour of observations, obtained around Oct. 12.29 UT
with the 1-3 A detector aboard OAO Copernicus, yielded an upper
limit of 1.0 x 10**-10 erg cm**-2 s**-1. This is a factor of 16 weaker
than the pulsed component of the Crab Nebula at the same
energies.
1974 October 24 (2712) Brian G. Marsden
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