IAUC 8854 (2007 July 11)
V5558 SAGITTARII
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R. W. Russell, D. K. Lynch, and R. Pearson, The Aerospace
Corporation; M. L. Sitko, University of Cincinnati and Space
Science Institute; H. B. Hammel, Space Science Institute; L.
Beerman, University of Cincinnnati; and W. Golisch, Infrared
Telescope Facility (IRTF), NASA, report on observations made of
V5558 Sgr (cf. IAUC 8832) using the IRTF (+ BASS) on July 9 UT.
The spectrum was smooth and featureless, roughly following a 2000-K
blackbody curve, although there were minor departures from a true
blackbody. If the object is a classical nova, then the F-type
spectrum (expected near peak brightness) is probably significantly
reddened. The narrowband [N] magnitude was approximately 2.0.
и
CBET 1006 : 20070719 : V5558 SAGITTARII
V5558 SAGITTARII
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T. Iijima, Astronomical Observatory of Padova, Asiago, writes that
the spectral evolution of V5558 Sgr has been monitored at Asiago
Observatory (CBET 934). Since its discovery on April 14, (IAUC 8832),
the luminosity of this object gradually increased (CBET 965, IAUC 8854),
with its maximum luminosity on July 9, and then a rather rapid fading
(
http://ooruri.kusastro.kyoto-u.ac.jp/pipermail/vsnet-alert/2007-July/001030.html).
The photometric evolution suggested that a drastic change
in the spectral features occurred. Spectra (range 350-600 nm; resolution
1000) taken on July 6.97 UT showed narrow, weak emissions of H_beta and Fe
II multiplets 42 and 49, accompanied by P-Cyg-type absorption components
blueshifted by about 400 km/s with respect to the emission features. The
higher numbers of the hydrogen Balmer series and the other metallic lines
were seen as pure absorptions. Also, Na I D and Ca II H and K were seen
as absorptions, and a weak trace of the Fraunhofer G band was detected.
On the contrary, the spectra (range 350-800 nm) taken on July 14.99 with
the same resolution showed broad (FWHM about 1000 km/s) emission lines of
H I, He I, and Fe II multiplets 27, 28, 37, 38, 42, 46, 48, 49, 55, 74,
etc. P-Cyg-type absorptions were seen only in Ca II H and K, of which
blueshifts were about 670 km/s. These spectral features are similar to
those of the extremely slow nova V723 Cas in the early decline stage
(Iijima 2006, A.Ap. 451, 563).
Вышел CBET 1010, но я пока до него не добрался
А вот тут полный список заслуг V5558 Sgr на сей день:
http://ooruri.kusastro.kyoto-u.ac.jp/pipermail/vsnet-recent/2007-July/058181.html
