Central Bureau for Astronomical Telegrams
IAUC 7027: XTE J1946+274; NGC 7582; DRACONID METEORS 1998
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Circular No. 7027
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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XTE J1946+274
R. M. Hjellming, National Radio Astronomy Observatory (NRAO);
and A. J. Mioduszewski, Joint Institute for VLBI in Europe and NRAO,
report: "Very Large Array observations on Oct. 7.02 UT reveal a
5-mJy radio source at 1.49 GHz inside the error region for the
transient x-ray pulsar XTE J1946+274 reported by Takeshima et al.
(IAUC 7016; see also Smith et al., IAUC 7014). This radio source
has a position R.A. = 19h45m31s.75, Decl. = +27o21'38".0 (equinox
2000.0; 2" uncertainty). Since it was at < 1 mJy at 4.9 GHz on
Oct. 7.02, and it was not detected at 1.49 GHz with upper limits of
1 and 2 mJy on Sept. 21 and 27, respectively, this may indicate
that we have detected the early rise of an optically thick radio
source. The radio source was also not present in a 1995 May 16
NVSS survey image at 1.4 GHz with a limit of about 2 mJy. Further
radio observations are needed to confirm variability, particularly
since it is unusual for a transient x-ray pulsar to exhibit
detectable radio continuum emission."
NGC 7582
J. P. Halpern, L. E. Kay, and K. M. Leighly, Columbia
University, write: "We obtained spectropolarimetry (range 390-750
nm; 0.3-nm resolution) of the Seyfert-2 galaxy NGC 7582 on June 20
using the Cerro Tololo 4-m telescope. In a 24-min exposure, we do
not see the broad Balmer lines detected by Joguet et al. (IAUC
7024) on July 11, in either direct or polarized flux. If the
emergence of this transient broad-line emission was caused either
by the removal of absorbing material at a velocity of 25~000 km/s
(the reported FWZI of the lines), or by the tidal disruption of a
star with such a relative velocity, the 21-day interval sets an
upper limit of 4.5 x 10E15 cm on the size of the emission-line
region on July 11."
DRACONID METEORS 1998
Numerous reports have been received of meteor activity coming
from the Draconid/Giacobinid radiant, with a visual peak of around
40-50 meteors/hr seen around Oct. 8.56 UT (S. Yoshida and D. Ito in
Japan). Peaks near 100/hr were detected with a high-density video
camera around Oct. 8.5 by J. Watanabe at the Dodaira Observatory,
and a similar peak time and rates were detected via forward-
scattered radio echoes by K. Suzuki (Aichi, Japan) and by E. P. Bus
(Groningen, The Netherlands). Backscattering radar echoes by J.
Borovicka, P. Prida, and P. Pecina (Ondrejov Observatory) showed
high activity perhaps peaking as late as Oct. 8.6.
(C) Copyright 1998 CBAT
1998 October 9 (7027) Daniel W. E. Green
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