Central Bureau for Astronomical Telegrams
IAUC 5427: N Pup 1991; omicron Cet; 1991g1
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Read IAUC 5428
Circular No. 5427
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Telephone 617-495-7244/7440/7444 (for emergency use only)
TWX 710-320-6842 ASTROGRAM CAM EASYLINK 62794505
MARSDEN or GREEN@CFA.BITNET MARSDEN or GREEN@CFAPS2.SPAN
NOVA PUPPIS 1991
M. Della Valle, European Southern Observatory; K. Reinsch,
Institut fur Astronomie und Astrophysik, Technische Universitat Berlin;
and H. Thomas, Max-Planck-Institut fur Astrophysik, report: "
Spectrograms (range 350-680 nm, resolution about 1 nm) obtained on Jan.
9.1 UT with the ESO/MPI 2.2-m telescope (+ EFOSC) at La Silla,
confirm this to be a nova. The analysis of the spectra finds strong
Balmer emission lines (up to H11) superimposed on a relatively weak
continuum. The presence of deep P-Cyg absorption lines of the
'principal' and 'diffuse-enhanced' systems suggests that this nova
is during its early decline. The maximum expansion velocity deduced
from the minimum of the P-Cyg absorptions is about 3000 km/s. Other
prominent features are at 418, 424, 430, 441 (Fe II mult. 27), 455,
458 (Fe II mult. 38), 493, 503, 519 (Fe II mult. 42), and 589 nm (Na
I) and at 568-576 nm (N II/O I/[N II] blend). H-alpha appears split
in two components, with the blue maximum stronger than the red one.
R. Rampazzo, Osservatorio di Brera, Milan, reports the following
photometric observations, obtained on Jan. 9.3 with the 0.90-m
telescope at La Silla: V = 8.40 +/- 0.02, B = 9.12 +/- 0.03."
omicron CETI
E. Gerard and G. Bourgois, Observatoire de Paris-Meudon,
communicate: "Following the campaign initiated by Karovska and Guinan
(IAUC 5043 and 5151), we detected OH radio emission from Mira (
omicron Cet) with the Nancay radio telescope and have monitored the
1665-MHz line since 1990 November with a velocity resolution of 0.07
km/s. The OH feature is centered at 46 km/s LSR, with total width
1.5 km/s, and shows strong circular polarization. The radio light
curve appears periodic and the next maximum is expected between 1992
early February and early May (near light minimum), with peak flux
density between 0.7 Jy (left hand circular) and 1.5 Jy (right hand
circular). Radio observations of OH (polarimetry and/or interferometry)
and other maser lines would be useful to understand the
peculiar nature of the prototype Mira variable."
COMET ZANOTTA-BREWINGTON (1991g1)
Total visual magnitude estimates by H. Mikuz, Ljubljana,
Yugoslavia (20x60 binoculars): 1991 Dec. 28.74 UT, 9.6; 1992
Jan. 2.73, 9.5; 6.75, 9.2.
1992 January 9 (5427) Daniel W. E. Green
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