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IAUC 8324: V2574 Oph = Poss. N IN Oph; 2004bf, 2004bi

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                                                  Circular No. 8324
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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     N. N. Samus, Institute of Astronomy, Moscow, informs us that
the designation V2574 Oph has been given to this nova (cf. IAUC
8323).  Additional magnitudes of V2574 Oph:  Apr. 11.38 UT, [13.5:
(ASAS-3 image; via H. Yamaoka, Kyushu University); 14.780 and
14.785, 10.9 (K. Haseda, Aichi, Japan; photographic; prediscovery;
via Yamaoka); 14.782, 10.5 (Y. Nakamura, Mie, Japan; photographic;
independent discovery forwarded by J. Watanabe, National
Astronomical Observatory of Japan); 15.785, about 10.5 (A. Takao,
Kitakyushu, Japan; via Yamaoka); 16.146, 10.4 (P. Schmeer,
Bischmisheim, Germany; visual); 16.403, V = 10.29 (J. D. West,
Mulvane, KS); 16.409, B = 11.74 (West); 16.417, R_c = 9.52 (West);
16.803, 10.7 (A. Pearce, Nedlands, W. Australia; visual).  Yamaoka
adds that his measurement of the position of V2574 Oph from an R-
band CCD image taken by B. Monard on Apr. 16.144 yields R.A. =
17h38m45s.51, Decl. = -23o28'18".6 (equinox 2000.0; 95 UCAC2
reference stars).
     H. E. Bond, Space Telescope Science Institute; and F. Walter,
State University of New York at Stony Brook, report that
spectrograms (range 350-530 nm; resolution 0.4 nm) of V2574 Oph
were obtained by A. Pasten with the SMARTS Consortium 1.5-m
telescope at Cerro Tololo Interamerican Observatory on Apr. 16.25-
16.27 UT.  The spectrum resembles that of an F supergiant, with
strong absorption lines of Fe II and no obvious emission lines.
The absorption lines are blueshifted by about -410 km/s.  The
object thus appears to be a slow classical nova caught near
maximum light.

SUPERNOVAE 2004bf AND 2004bi
     T. Matheson, P. Challis, and R. Kirshner, Harvard-Smithsonian
Center for Astrophysics, write that a spectrogram of SN 2004bf (cf.
IAUC 8317), obtained by J. Huchra with the Mt. Hopkins 1.5-m
telescope on Apr. 13.42 UT, shows it to be a type-Ic supernova,
similar to SN 1987M (see Filippenko et al. 1990, A.J. 100, 1575).
The spectrum is reddened and shows a strong, narrow Na I D
absorption at the velocity of the host galaxy with an equivalent
width of 0.2 nm.  The dust maps of Schlegel et al. indicate a low
value for Galactic reddening of E(B-V) = 0.012.  A spectrum of SN
2004bi (cf. IAUC 8321), obtained by Huchra on Apr. 15.22, shows it
to be a type-Ic supernova.  The spectrum is similar to early
spectra of SN 1994I (Filippenko et al. 1995, Ap.J. 450, L11), but
there are some peculiarities.  An absorption near 625 nm (rest
wavelength) may be Si II (rest 635.5 nm), but it is unusually
strong compared to typical type-Ic supernovae.

                      (C) Copyright 2004 CBAT
2004 April 16                  (8324)            Daniel W. E. Green

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