Nova Sagittarii 1992

M. Della Valle and O. Hainaut, European Southern Observatory; and L. Wisotski, Hamburg Observatory, report: "Preliminary analysis of a spectrum (range 390-690 nm, resolution about 2 nm), obtained with the 3.6-m telescope (+ EFOSC) at La Silla on Feb. 15.4, shows this object to be a nova. The spectrum is characterized by emission lines of H I, Fe II (mult. 42), N II (mult. 3), and Na I (589 nm). The FWZI of H-alpha and H-beta are about 5000 km/s. No clear evidence for P-Cyg absorption was observed. Photometry by C. Nitschelm (Geneva Observatory) with the 0.70-m Swiss telescope: Feb. 15.4, V = 8.5 +/- 0.1. Photometry by G. Cutispoto (Catagna Observatory) with the ESO 0.50-m telescope: Feb. 15.4, V = 8.66 +/- 0.03, B-V = +0.90 +/- 0.05, U-B = +0.05 +/- 0.07, V-R = +0.75 +/- 0.05, V-I = +1.60 +/- 0.05; Feb. 16.5: V = 8.93, B-V = +0.78, U-B = -0.05, V-R = +0.75, V-I = +1.60; Feb. 17.4, V = 9.12, B-V = +0.72, U-B = -0.10, V-R = +0.75, V-I = +1.60 (same errors)." G. Stringfellow and T. E. Harrison, Mt. Stromlo Observatory, report: "Infrared spectroscopy (J, H, and K bands) of Nova Sgr 1992 on Feb. 15.7 UT revealed weak, broad lines of H I (Br-gamma, Br10 to Br13, Pa-beta, Pa-gamma). There was no evidence for He I emission. However, weak emission from O I at 1.13 microns was present." R. H. McNaught, Anglo-Australian Observatory, reports that N Sgr 1992 has increased in brightness by more than 10 magnitudes. The nearest star to the earlier reported position (IAUC 5452) on the ESO B survey is a star of mag 18-19, of no obvious color, situated at R.A. = 18h06m28s.68, Decl. = -25 52'32".1 (equinox 1950.0; uncertainty 0".3 in R.A., 0".2 in Decl.). On the SERC J survey, there is a blend of stars around mag 20 at the nominal position. Magnitude estimate from P. Camilleri, Cobram, Victoria: Feb. 15.724 UT, 9.4.