Central Bureau for Astronomical Telegrams
IAUC 8529: V378 Ser, V2361 Cyg; C/2005 F3, C/2005 F4
The following International Astronomical Union Circular may be linked-to from your own Web pages, but must not otherwise be redistributed (see these notes on the conditions under which circulars are made available on our WWW site).
Read IAUC 8530
.dvi,
.ps or
.PDF format.
Circular No. 8529
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)
CBAT@CFA.HARVARD.EDU (science)
URL http://cfa-www.harvard.edu/iau/cbat.html ISSN 0081-0304
Phone 617-495-7440/7244/7444 (for emergency use only)
V378 SERPENTIS AND V2361 CYGNI
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
Read IAUC 8530
.dvi,
.ps or
.PDF format.
Our Web policy. Index to the CBAT/MPC/ICQ pages.
