Central Bureau for Astronomical Telegrams

IAUC 7325: V1494 Aql; V382 Vel

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                                                  Circular No. 7325
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)


V1494 AQUILAE
     D. Moro, A. Pizzella, and U. Munari, Asiago Astrophysical
Observatory, write:  "Spectra (1 nm/pixel; range 340-950 nm) of
V1494 Aql (= N Aql 1999 No. 2) were obtained on Dec. 2.71 UT with
the Asiago 1.22-m telescope (+ Boller & Chivens CCD spectrograph).
The Balmer hydrogen series is in emission with a P-Cyg profile.
The H-alpha emission component has a 1300 km/s FWHM; the absorption
component is centered at -1850 km/s from the emission component.
Fe II multiplet 42 at 492, 502, and 517 nm, and O I 777-nm, are
visible in emission also with a P-Cyg profile."
     J. A. Mattei, AAVSO, reports an independent visual discovery
of this nova by Gary T. Nowak, Essex Junction, VT, with 7x35
binoculars on Dec. 1.958 UT at mag 5.6.  Additional m_v estimates:
Dec. 2.68, 4.2 (L. Kiss, Szeged, Hungary); 2.803, 4.1 (G. M. Hurst,
Basingstoke, England); 2.814, 4.2 (P. Schmeer, Bischmisheim,
Germany); 2.921, 3.7 (J. G. de S. Aguiar, Campinas, Brazil); 2.940,
4.3 (D. W. E. Green, Cambridge, MA); 2.956, 3.9 (R. Lourencon,
Jundiai, Brazil); 2.96, 4.1 (G. Seronik, Belmont, MA).


V382 VELORUM
     M. Orio, Turin Observatory and University of Wisconsin; A. N.
Parmar, European Space Agency; M. Capalbi, Italian Space Agency;
and L. Piro and T. Mineo, Consiglio Nazionale delle Ricerche,
report on behalf of the BeppoSAX team:  "BeppoSAX observed V382 Vel
(N Vel 1999) during Nov. 20.180-20.974 UT.  The nova has become a
supersoft luminous x-ray source.  The count rate was 0.097 +/-
0.002 counts/s in the two MECS instruments (1.6-10 keV) and 3.469
+/- 0.002 counts/s in the LECS instrument (0.1-10 keV).  The
spectrum is dominated by a blackbody-like component at about 40 eV
with unabsorbed flux about 1.5-2 x 10**-7 erg cm**-2 s**-1,
assuming a blackbody model and absorption around 2 x 10**21
atoms/cm**2.  At higher energy (1.0-10 keV), there is a harder
component that can be approximately modeled by emission from a
thermal plasma at kT about 1 keV and flux a few x 10**-12 erg
cm**-2 s**-1.  At a distance of 2000 pc (Della Valle et al. 1999,
IAUC 7193), the total bolometric luminosity is about 10**38 erg
cm**-2.  The x-ray spectrum has evolved dramatically since June
(Orio et al., IAUC 7196; Mukai and Ishida, IAUC 7205), and the
column of neutral hydrogen seems to have decreased by a factor of
10, due to thinning of the ejecta.  Further observations at x-ray
and other wavelength bands are encouraged."

                      (C) Copyright 1999 CBAT
1999 December 2                (7325)            Daniel W. E. Green

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