Central Bureau for Astronomical Telegrams
IAUC 7261: V382 Vel; 1999dk
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Circular No. 7261
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
BMARSDEN@CFA.HARVARD.EDU or DGREEN@CFA.HARVARD.EDU (science)
URL http://cfa-www.harvard.edu/iau/cbat.html ISSN 0081-0304
Phone 617-495-7244/7440/7444 (for emergency use only)
V382 VELORUM
S. N. Shore, Indiana University, South Bend; H. E. Bond and R.
Downes, Space Telescope Science Institute; S. Starrfield, Arizona
State University; R. D. Gehrz, University of Minnesota; J.
Krautter, Landessternwarte Heidelberg; and C. E. Woodward,
University of Wyoming, write: "We observed V382 Vel with the Hubble
Space Telescope's Imaging Spectrograph on June 21.6 and Aug. 29.2
UT, using the medium-resolution echelle gratings (E140M and E230M;
cf. IAUC 7192). Three exposures were obtained on each date,
centered at 142.5, 197.8, and 270.7 nm with resolutions of about
45 000 (E140M) and 30 000 (E230M). The June spectra displayed
saturated, sharp-blue-edged P-Cyg absorption on all resonance lines
with terminal velocities of order 5000 km/s for Al III 186.0-nm and
Si IV 140.0-nm. C IV 150.0-nm showed a profile consistent with a
linear velocity gradient. Weak iron-peak absorption was still
present. By the August observations, the nova had entered the
emission-line phase, and iron-peak absorption and P-Cyg profiles
had vanished. The following strong emission lines have been
detected: N V 124.0-nm, O I 130.4-nm, C II 133.4-nm, O V 137.1-nm,
Si IV 140.0-nm, N IV] 148.6-nm, C IV 155.0-nm, [Ne IV] 160.2-nm,
He II 164.0-nm, O III] 166.7-nm, Si II 181.6-nm, Al III 186.0-nm, C
II 232.1-nm, Al II 267.2-nm, Mg II 280.0-nm, and O III 304.0-nm. A
blend at 190.0 nm can be identified as Si III] and C III], with an
intensity ratio of about 0.3. All emission lines show structure
consistent with a flattened, ringlike shell with thickness-to-
radius ratio of about 0.5 and possibly asymmetric, higher-velocity,
diffuse emission (HWZI about 2000 km/s). Low-ionization species
such as Al II, Si III], and C III] show a strong knot at -1000
km/s, at the same velocity as the strongest Balmer line knot. Most
profiles show fine structure that is consistent with knots of the
sort detected in V1974 Cyg. A strong interstellar spectrum is
present, including Si IV and C IV, and the velocities reported on
IAUC 7192 are confirmed. The integrated flux from 119.0 to 312.0
nm was 3.0 x 10**-7 erg cm**-2 s**-1 on June 21.6 and 4.6 x 10**-8
erg cm**-2 s**-1 on Aug. 29.2, corrected for reddening of E(B-V) =
0.2. Continued monitoring at all wavelengths is urged. FUSE and
Chandra observations are currently being scheduled."
SUPERNOVA 1999dk IN UGC 1087
CCD V magnitudes from D. Hanzl, Brno, Czech Republic: Aug.
23.980 UT, 14.32 +/- 0.03; Sept. 4.952, 14.54 +/- 0.05; 9.935,
14.99 +/- 0.02; 12.963, 15.02 +/- 0.06.
(C) Copyright 1999 CBAT
1999 September 21 (7261) Daniel W. E. Green
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