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IAUC 8529: V378 Ser, V2361 Cyg; C/2005 F3, C/2005 F4

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                                                  Circular No. 8529
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
Phone 617-495-7440/7244/7444 (for emergency use only)

     D. Gaggero, I. Martire, R. Poggiani, V. Puccetti, S. N. Shore,
and E. Tognelli, Department of Physics, University of Pisa; and S.
Bernabei, Osservatorio Astrofisica, Bologna, and Istituto Nazionale
di Astrofisica (INAF), report 0.4-1.0-micron observations of V378
Ser and V2361 Cyg using the Loiano 1.52-m telescope (+ BFOSC grism
spectrograph) of the Bologna Observatory/INAF during Apr. 29.8-May
2.2 UT (at resolutions of 700 and 900).  V378 Ser (IAUC 8505)
showed weak H_alpha P-Cyg absorption (H_beta and H_gamma indicate a
Balmer progression in emission intensity, while the velocity of the
minimum of each of the three Balmer absorption troughs was -2200
km/s); stronger absorption is seen for Paschen 10-13, and weak
emission appears at C I 908.5- and 940.6-nm and O I 777.3- and
844.2-nm but with similar velocities.  No He II or O II is observed.
Strong P-Cyg absorption is detected for He I 587.5-nm at -1500 km/s
and also for Fe II (42, 48, 49).  The spectrum resembles those of
the nova in the Large Magellanic Cloud 1988 No. 1 and V443 Sct at
two weeks after maximum -- consistent with the ejecta being in the
pre-nebular phase (no change observed in line profile or intensity
during the 3 days of observation).  The spectrum is developing
relatively slowly for the observed optical velocities.  V2361 Cyg
(IAUC 8483) displays strong emission at H_alpha with principal
asymmetric peaks at -700 km/s (weaker) and +705 km/s, and a still-
weaker third peak at -200 km/s (FWHM = 2200 km/s and FWZI = 4500
km/s for the entire profile); O I 844.2-nm shows the same peak
velocities and intensities as that of the H_alpha emission (FWHM =
2000 km/s and FWZI 3800 km/s); the Paschen series has similar
widths; and other emission lines (e.g., [O III] 436.3-, 495.9-,
and 500.7-nm; He I 587.5-nm; O I 777.3, 844.2 nm; N I 821.6-nm;
and Mg II 823.2-nm) show symmetric peaks at the same peak
velocities.  The H_alpha/H_beta intensity ratio is consistent with
the high reported reddening (IAUC 8524).  Both novae resemble
CO-type outbursts.

COMETS C/2005 F3 AND C/2005 F4 (SOHO)}
     Additional diffuse Kreutz sungrazers (cf. IAUC} 8527); C/2005
F3 had no tail (too faint for photometry, but at mag about 8),
while C/2005 F4 had a possible hint of a tail and reached mag about
6.5 at 7.1 solar radii (Mar. 28.842 UT).

 Comet       2005 UT       R.A.(2000)Decl.  Inst.  F    MPEC
 C/2005 F3   Mar. 28.017   0 35.5  + 2 17    C2    MM   2005-J25
 C/2005 F4        28.429   0 44.9  + 2 08    C3/2  HS   2005-J25

                      (C) Copyright 2005 CBAT
2005 May 16                    (8529)            Daniel W. E. Green

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