Central Bureau for Astronomical Telegrams
IAUC 6065: 1994Y; LT Del
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Circular No. 6065
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@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)
SUPERNOVA 1994Y IN NGC 5371
A. Clocchiatti, R. Garcia-Lopez, E. S. Barker, W. Wren, and J.
C. Wheeler, University of Texas, report: "A fully-reduced spectrogram
(range 380-640 nm, resolution 1.3 nm) of SN 1994Y, obtained on
Aug. 27.15 UT at the 2.7-m telescope of McDonald Observatory, shows
the lines of the Balmer series and Na D in emission superimposed on
a blue continuum. In the low-S/N spectrum, the emission lines do
not show a P-Cyg absorption counterpart with the possible exception
of Na D, but consist of a narrow core and a broad base, both centered
at the velocity of NGC 5371. The FWHM of the broader components
implies an expansion velocity of about 2600 km/s, while the
FWZI implies a maximum expansion of about 7000 km/s. SN 1994Y
apparently belongs to the 'Seyfert 1' subclass of type-II supernovae
(Filippenko 1989, A.J. 97, 726), called type-IIn by Schlegel (1990,
MNRAS 244, 269). Continuous monitoring of this event is strongly
recommended."
X. J. Jiang, W. Liu, and J. Y. Hu, Beijing Observatory, communicate:
"A spectrogram (range 450-700 nm, resolution 0.53 nm/pixel)
of SN 1994Y has been obtained using the 2.2-m telescope at Beijing
Observatory, Xinglong, on Aug. 25. The spectrum shows strong Balmer
emission, confirming it to be a type-II supernova. The wavelengths
of the H-alpha and H-beta emission lines coincide with the radial
velocity of the host galaxy NGC 5371 (2550 km/s). The emission
lines are narrow compared with normal type-II supernovae; the FWHM
of H-alpha and H-beta are about 1200 km/s. Another dominating wide
emission feature peaks at 592.9 nm, possibly due to He I (587.6 nm)
and Na I (589.3 nm). A feature at 673.0 nm is from He I (667.8 nm).
The spectrum is similar to that of SN 1994W, but without narrow
absorption features at the blue side of the Balmer emission lines."
A. Boattini and M. Tombelli, Florence, provide an accurate
position for this object: R.A. = 13h53m30s.57, Decl. =
+40o42'32".8 (equinox 1950.0).
LT DELPHINI
R. Passuello and S. Saccavino, Associazione Friulana di
Astronomia e Meteorologia (AFAM), Udine; and U. Munari, Asiago
Astrophysical Observatory, report their photometry of this symbiotic
star, obtained with the AFAM 0.45-m telescope on Aug. 26.9 UT: V =
12.22, B-V = +0.56, U-B = -0.74 (+/- 0.05 mag in all colors).
Comparison with archival data collected on 1990 June 23, when the star
was at V = 13.13, B-V = +1.26, U-B = -0.48 (Munari et al. 1992,
A.Ap. Suppl. 93, 383), suggests that this star is currently
undergoing an unexpected bright phase.
1994 August 29 (6065) Daniel W. E. Green
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