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IAUC 5829: NO 1993U, 1993V; YY Her; N Aql 1993

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                                                  Circular No. 5829
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)


NO SUPERNOVAE 1993U AND 1993V
     A. V. Filippenko, T. Matheson, and L. C. Ho, University of
California at Berkeley, report that fully calibrated CCD spectra
(range 320-1000 nm) obtained on June 28 UT with the Shane 3-m
reflector at Lick Observatory reveal that SNe 1993U and 1993V (cf.
IAUC 5818) are actually quasi-stellar objects (QSO).  SN 1993U has
a redshift of 0.591, based on the presence of broad (FWHM about
4000 km/s) emission lines of Mg II (279.8 nm), H-gamma, and H-beta
superposed on a blue continuum.  The emission-line redshift of the
adjacent galaxy is 0.107, and there is a foreground M star next to
it but diametrically opposite the QSO.  SN 1993V has a probable
redshift of 1.087, based on the presence of broad (FWHM about
10 000 km/s) Mg II (279.8 nm) superposed on a red continuum.  Weak
C III] (190.9 nm) might also be visible.  The redshift of the
adjacent galaxy is 0.108, measured from narrow emission lines.


YY HERCULIS
     M. Friedjung, Institut d'Astrophysique, Paris, communicates:
"As part of a programme with C. C. Huang (Purple Mountain Observatory)
involving observations of symbiotic stars between 810.0 and
870.0 nm, we have observed YY Her currently undergoing a bright
phase (see IAUC 5819).  The last observation made on 1993 June 30
can be compared with one made on 1992 June 15, all having been made
with the 1.93-m telescope of the Haute Provence Observatory (+
CARELEC spectrograph; dispersion 3.3 nm/mm).  The lines of the Ca
II triplet (of which the two shorter-wavelength ones at least were
in absorption in 1992) now appear in emission, resolved from the
nearby Paschen lines.  The fluxes of the latter in emission on both
dates, however, do not at first sight indicate very dramatic
changes since 1992."


NOVA AQUILAE 1993
     Further photoelectric photometry (cf. IAUC 5818):  June 23.197
UT, V = 10.65 +/- 0.02, B-V = +0.32 +/- 0.04 (D. H. Kaiser, Columbus,
IN); 24.93, V = 10.75 +/- 0.02, B-V = +0.37 +/- 0.03, U-B = -0.44
+/- 0.05 (D. Hanzl, N. Copernicus Observatory, Brno; comparison
star SAO 124317 = HD 178574); 26.05, V = 10.6 (H. Mikuz, Ljubljana,
Slovenia); 28.90, V = 11.8 (Mikuz); 30.90, V = 12.4 (Mikuz).


1993 July 12                   (5829)            Daniel W. E. Green

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