Central Bureau for Astronomical Telegrams
IAUC 8370: 2004da; V5113 Sgr, V2574 Oph; PSR 0833-45
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Circular No. 8370
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)
SUPERNOVA 2004da IN NGC 6901
T. Boles, Coddenham, England, reports the discovery of an
apparent supernova (mag 15.2) on unfiltered CCD images taken on
July 6.099 and 7.031 UT with a 0.35-m reflector. The new object is
located at R.A. = 20h22m21s.24, Decl. = +6o25'50".3, which is
approximately 5".4 west and 2".3 north of the center of NGC 6901.
SN 2004da is not present on Boles' images from May 5 (limiting mag
19.5) and June 14, and it is not present on Digitized Sky Survey
red (1990 Aug. 19) or blue (1988 July 8) plates.
V5113 SAGITTARII AND V2574 OPHIUCHI
Further to IAUC 8368, R. J. Rudy, D. K. Lynch, S. Mazuk, C. C.
Venturini, R. C. Puetter, and R. B. Perry report 0.4-2.5-micron
NIRIS spectroscopy of V5113 Sgr on June 24.06 UT, approximately 9
months after outburst (cf. IAUC 8204, 8206). This Fe II-type nova
has reached moderately high excitation, displaying strong He II
lines as well as the coronal lines [S VIII] 0.9911-micron and [Si
VI] 1.9641-microns. The unidentified novae lines at 1.1114, 1.1900,
1.5545, and 2.0996 microns were also present. The nebular [O III]
lines were very strong, as was the [S III] feature at 0.9532 micron.
The continuum shows a sharp rise beyond 2 microns, indicative of
hot dust.
Puetter, Rudy, Lynch, Mazuk, Venturini, and Perry add that
their NIRIS observations of V2574 Oph (cf. IAUC 8323, 8324) on June
23.4 UT show that the nova is still in its low-excitation phase,
showing lines of C I, N I, and Fe II. No He II or coronal lines
are seen. The Balmer, Paschen, and Bracket lines are strong, as
are the Lyman_beta-fluoresced O I lines at 0.8446 and 1.1287
microns. The lines are approximately gaussian in shape but are
asymmetric near their peaks (FWHM approximately 1500 km/s). The
slow development of this nova suggests that continued monitoring
should be possible for several years.
PSR 0833-45
R. Dodson, Institute of Space and Astronautical Science; S.
Buchner, Hartebeesthoek Radio Astronomy Observatory (HartRAO); B.
Reid and D. Lewis, University of Tasmania; and C. Flanagan,
Johannesburg Planetarium, report observing a sudden spin-up
("glitch") in the Vela pulsar (cf. IAUC 7347) on July 7.09 UT.
Preliminary model fitting gives a fractional decrease of 2.1 x
10**-6 in the rotation period. The jump was first detected by the
HartRAO 26-m telescope and observed at three frequencies (635.034,
990.25, and 1390.64 MHz) with the Mount Pleasant 14-m dish.
(C) Copyright 2004 CBAT
2004 July 7 (8370) Daniel W. E. Green
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