Central Bureau for Astronomical Telegrams
IAUC 2713: N Sgr 1974
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Circular No. 2713
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Cable Address: SATELLITES, NEWYORK
Western Union: RAPID SATELLITE CAMBMASS
NOVA SAGITTARII 1974
Dr. D. P. Elias, Athens Observatory, sends the following precise
position: R.A. = 17h45m43s.84, Decl. = -18o44'39".8 (equinox 1950.0).
Nihondaira Obs. Circ. No. 583 gives a similar position (end figures
44s.13, 41".8), measured by T. Urata from an exposure by K. Tsuchiya
(Asahikawa).
Dr. W. Liller, Harvard College Observatory, reports that he
has examined at least one plate from every year from 1899 through
1953 and finds no evidence of a prior outburst brighter than mpg 11.
A. C. Gilmore, Carter Observatory; and W. S. G. Walker, Auckland
Observatory, communicate the following photoelectric observations,
obtained by G. Freeth using the Auckland 50-cm Cassegrain:
1974 UT V B - V U - B
Oct. 15.399 10.31 +1.00 -0.09
16.338 10.26 +1.00 -0.18
17.344 10.39 +0.98 -0.16
S. Wyckoff and E. M. Leibowitz, Wise Observatory, write:
"Image-tube spectrograms (dispersion 200 A/mm, range 3600-9000 A)
obtained with the 100-cm reflector on Oct. 16.7 and 17.7 UT indicate
that the nova is in the 'early decline' phase. The Balmer and
Fe II (multiplet 42) lines are the most outstanding emission features,
while beyond H-alpha the only prominent features are broad O I
emission lines centered at 7774 and 8446 A. All the Balmer, Fe II
and O I lines are flanked by their 'principal' and 'diffuse-enhanced'
absorption spectra, which are displaced by about -1500
and -2800 km/s, respectively, from the emission band centers."
F. Ciatti and L. Rosino, Asiago Astrophysical Observatory,
write: "A spectrum obtained on Oct. 18 using a grating spectrograph
(dispersion 120 A/mm) on the 122-cm telescope is characterized by
wide emission bands (halfwidth 1340 +/- 300 km/s) of H, N II, Fe II
(multiplets 42, 49, 74) and Na I; these are associated with P Cyg-type
absorptions and give an expansion velocity of 3200 +/- 200 km/s.
The presence of forbidden lines of N II and O I (6300, 6364 A) is
doubtful, precise identification being uncertain because of strong
night-sky lines arising from the low altitude of the object. It is
very likely that the nova is about 2.5 magnitudes below maximum,
near the Orion phase."
1974 November 7 (2713) Brian G. Marsden
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