Central Bureau for Astronomical Telegrams
IAUC 5007: V3890 Sgr
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Circular No. 5007
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Telephone 617-495-7244/7440/7444 (for emergency use only)
TWX 710-320-6842 ASTROGRAM CAM EASYLINK 62794505
MARSDEN or GREEN@CFA.BITNET MARSDEN or GREEN@CFAPS2.SPAN
V3890 SAGITTARII
E. P. Belserene, Maria Mitchell Observatory, reports the
following measurement of N Sgr 1962 = V3890 Sgr from a plate exposed
1962 June 3.2 UT (cf. Dinerstein and Hoffleit 1973, IBVS 845):
R.A. = 18h27m39s.97, Decl. = -24 03'15".9 (equinox 1950.0; estimated
uncertainty +/- 2" in each coordinate). This suggests that the
star(s) measured by Duerbeck (1987, Space Sci. Rev. 45, 123) and by
Williams (1983, Ap.J. Suppl. 53, 523) is (are) not V3890 Sgr. This
agrees with remarks by several observers (including Kato et al.,
below) that the object now in outburst lies southwest of the
Duerbeck and Williams positions.
T. Kato, T. Djamaluddin, R. Hirata, and M. Saito, Kyoto University,
report: "We observed V3890 Sgr with the CCD camera attached
to the Ouda 0.60-m reflector on Apr. 30.8 UT, and obtained V about
9.3. The position of the present nova coincides with a mag 17 star
on the POSS O plate located 6" west and 10" south of the Williams
(ibid.) candidate. The magnitude on Duerbeck's SERC-J finding chart
is about 14, suggesting an unreported outburst."
T. Harrison and J. Johnson, Mount Stromlo Observatory; and J.
Spyromilio, Anglo-Australian Observatory, communicate: "J, H, K,
and L' spectra of V3890 Sgr were obtained on May 4, 5, and 6 using
the cooled grating spectrometer (CIGS) on the 2.3-m reflector at
Siding Spring. The spectral resolution was 500. The spectra show
strong Paschen-beta and Paschen-gamma, as well as Brackett-alpha and
Br-gamma and Brackett10 through Brackett14, in emission. Pfund-
gamma was also detected. The line ratios are consistent with a
'Case B' hydrogen recombination spectrum (Hummer and Storey 1987,
M.N.R.A.S. 224, 801). He 1083.0-nm and 2058.0-nm were also detected
to be strong in emission. There was no evidence for P-Cyg profiles
in either of the helium lines. The emission lines are broad with
FWHM around 1000 km/s. In contrast to V745 Sco, no absorption was
detected from the first overtone of CO (cf. IAUC 4885)."
A. F. Jones, Stoke, New Zealand, writes that he has monitored
this object since 1988 Jan., but failed to detect the star on 61
nights prior to its current outburst (cf. IAUC 5002). Further
visual magnitude estimates: Apr. 20.68 UT, [13: (Jones); May 3.18,
9.8 (A. Pereira, Linda-a-Velha, Portugal); 4.18, 9.9 (Pereira);
5.17, 10.3 (Pereira); 5.89, 9.7 (A. Pearce, Scarborough, W.A.);
6.17, 9.7 (Pereira); 6.87, 9.8 (Pearce); 7.11, 9.0 (A. Boattini,
Monte Senario, Italy).
1990 May 9 (5007) Daniel W. E. Green
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