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IAUC 4225: 1986f; 1986I; CGSS 1175

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IAUC number

                                                  Circular No. 4225
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 617-495-7244/7440/7444

     J. Gibson reports his recovery of this comet with the 1.5-m
reflector and CCD at Palomar as follows:

         1986 UT             R.A. (1950.0) Decl.      m1

         June  9.45845      2 04.22      +25 21.2     18
              10.45079      2 06.14      +25 35.2
              11.45729      2 08.07      +25 50.3

The object is diffuse with central condensation and on June 9 had
a tail 1'-1'5 long in p.a. 260.  The position is in close
agreement with the prediction on MPC 10553 (elements on MPC 8273).

     W. S. Penhallow, Quonochontaug Observatory, has measured the
following precise position from a 20-min exposure with the 0.4-m
astrometric reflector on June 4: R.A. = 12h16m19s65, Decl. = +14deg41'23"4
(equinox 1950.0).

     W. Wenzel, Sonneberg Observatory, reports photographic
magnitude estimates by A. Jager: May 12.9 UT, [16.0; 26.9, 14.0.

     R. Kirshner and I. Wilson, Center for Astrophysics, report:
"Low-dispersion spectra (range 480-700 nm) obtained by E. Horine
and J. Peters using the Z machine on the Tillinghast 1.5-m
telescope at the Whipple Observatory indicate that the supernova in
NGC 4254 = M99 is of type II.  The FWHM of the HS emission line
was measured at ~ 9100 km/s (FWZM ~ 14 600 km/s) on June 7.  The
H-alpha profile is noticeably asymmetric toward the red."

CGSS 1175
     W. Wenzel, Sonneberg Observatory, telexes that A. Jager has
identified 16 maxima (brightest mpv = 9.8) of this object (IAUC
4221, 4224) on 300 Sonneberg sky-patrol plates since 1963, showing
that the object is a long-period variable with period ~ 1 yr.

     T. Iijima, Asiago Astrophysical Observatory, telexes that
spectra taken on June 8 show TiO absorption bands and emission lines
of H-alpha (very weak) H-beta, H-gamma (slightly stronger than H-beta)
and H-delta.  The object can therefore be classified as a Mira variable.

1986 June 13                   (4225)              Brian G. Marsden

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