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IAUC 3813: SNe; NGC 4151; Corrs

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                                                  Circular No. 3813
Central Bureau for Astronomical Telegrams
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
TWX 710-320-6842 ASTROGRAM CAM     Telephone 617-864-5758

     E. P. Aksenov, Sternberg Astronomical Institute, relays a
report from Lyutyj to the effect that Doroshenko and Tsvetkov have
discovered supernovae in NGC 6217 and NGC 4051, respectively,
presumably both at the Sternberg Crimean Station.  The supernova in
NGC 6217 was of mpg 15.1 on May 11.02 UT and is 4" east, 12" south
of the nucleus.   That in NGC 4051 was of mpg 15.0 on May 12.00 UT
and is 21" east, 50" south of the nucleus.  The supernova in NGC
4051 was independently detected by J. Kielkopf, R. Brashaer, A.
Goldstein and R. Gabart on a single photograph taken at the
University of Louisville's Moore Observatory on May 11; mpg was given
as 13.5, and the offset from the nucleus 23" east, 53" south.

NGC 4151
     H. Schulz, J. Fried and H. Hippelein, Max-Planck-Institut fur
Astronomie, Heidelberg, report: " A pronounced narrow depression in
the blue wing of broad-line H-alpha in the Seyfert galaxy NGC 4151
appeared on a 5-min reticon spectrum taken on Mar. 30 with the
2.2-m telescope at Calar Alto.  The deepest point of the depression
lies 1200 km/s to the blue of narrow-line H-alpha.  The presence
of the feature is confirmed by an uncalibrated photographic
image-tube spectrum taken on May 3, although the broad emission
wings might have become stronger in the mean time.  The feature is
most probably related to the transient blueshifted Balmer absorption
detected by Anderson and Kraft (1969, Ap.J. 158, 859), but it
is of unprecedented strength on the reticon spectrum.  Since the
behavior of these absorptions with time could provide unique
kinematic and spatial information about the active nucleus (cf.
Ferland and Mushotzky 1982, Ap.J. 262, 564), we urge further
spectroscopic observations before the object moves into daylight.
However, only high signal-to-noise observations with good resolution
(better than 0.3 nm) and simultaneous photometric monitoring
of the continuum are useful."

IAUC 3801 and 3804.  For  G. Bothum  read  G. Bothun.
IAUC 3806, Another  Millisecond  Pulsar,  line  5.  For  19h53m25s7
   read  19h53m26s7.
IAUC 3810, line 17 from foot.  For  May 8-12  read  May 9-12.

1983 May 18                    (3813)              Brian G. Marsden

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