Central Bureau for Astronomical Telegrams
IAUC 6002: N Oph 1994
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Circular No. 6002
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)
NOVA OPHIUCHI 1994
R. M. Wagner, Ohio State University; K. M. Vandlandingham,
Arizona State University; and N. King, New Mexico State University,
report that optical spectra (range 367-723 nm, resolution 0.36 nm)
were obtained on June 4.31 UT with the 4.5-m Multiple Mirror
Telescope at the F. L. Whipple Observatory. The spectra exhibit
broad permitted emission lines due to the Balmer series of hydrogen
and Fe II superposed on a flat continuum. The FWHM of H-alpha and
H-beta emission is about 2500 km/s and the FWZI is about 5800 km/s.
The line profiles consist of at least four distinct components.
The spectra confirm the identification as a fast Fe II-class nova
in its early decline stage.
S. Benetti, European Southern Observatory (ESO), reports that
inspection of a preliminarily-reduced CCD spectrum (range 370-700
nm, resolution 1.2 nm) obtained on June 4.24 UT with ESO 3.6-m
telescope (+ EFOSC1) confirms that the object is a nova. The
spectrum is dominated by intense emission lines of hydrogen and Fe
II. The FWHM of H-alpha, H-beta, and H-gamma, corrected for the
instrumental resolution, is about 2500 km/s.
S. D. Van Dyk, University of California at Berkeley, obtained
a spectrum (range 470-720 nm, resolution 0.4 nm) of N Oph 1994 on
June 4 UT with the Kitt Peak 2.1-m reflector (+ Goldcam spectrograph).
G. S. Stringfellow (Penn State University) and A. V. Filippenko
(University of California at Berkeley) have examined the uncalibrated
spectrum; they report that broad emission lines are present, by far
the strongest being H-alpha. Prominent [O III] (495.9, 500.7 nm)
emission is evident, along with many weaker forbidden lines such as
[O I] at 630.0 and 636.4 nm. He I at 587.6 nm is narrower and
exhibits a P-Cyg profile. Structure is visible in most of the
emission lines, suggesting that the ejecta are clumpy. A spectrum
centered on H-alpha, obtained by G. E. Albright (University of
Virginia) at the coude feed telescope, confirms the presence of at
least four distinct components.
A. C. Gilmore reports the following preliminary photometry from
Mt. John (reference star from Cousins E746; uncertainty about 0.02
in each color except U-B, where the error may be 0.05): June 4.585
UT, V = 8.49, U-B = -0.25, B-V = +0.52, V-Rc = +0.66, V-Ic = +1.29.
Magnitude estimates from T-Max film from K. Kanatsu, Matsue,
Shimane, Japan: May 30.585 UT, [9.5; June 2.653, 7.5.
1994 June 4 (6002) Daniel W. E. Green
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