2007CBET.1039....1K

L. Kiss, University of Sydney; and K. Sarneczky, University of Szeged, report that optical spectra (0.05 nm/pixel, ranges 400-500 and 580-680 nm) of V5558 Sgr (cf. IAUC 8832; CBETs 1006, 1010) were obtained on Aug. 18.56 UT (during the second major rebrightening of this slow nova) with the Siding Spring 2.3-m telescope (+ DBS CCD spectrograph). The hydrogen Balmer lines show emission profiles with broad wings (FWZI approximately 3000-3500 km/s) and distinct narrow central components (FWZI approximately 600-700 km/s), separated by P-Cyg-like absorptions at about -300 km/s. Similarly complex line profiles are seen for the numerous Fe II emission lines, most notably for the Fe II (27, 28), (37, 38), and (42) multiplets in the blue range and the Fe II (74) triplet in the red range. The Na I D doublet has multiple absorption components, suggesting both complex velocity structure in the intervening clouds and strong interstellar extinction. This nova has continued to slowly brighten, as indicated by the following visual magnitude estimates (cf. CBET 1006): July 18.888 UT, 8.6 (M. Lehky, Hradec Kralove, Czech Republic); 18.903, 8.4 (K. Hornoch, Vohancice, Czech Republic); 20.864, 8.7 (Lehky); 21.870, 8.4 (Hornoch); 21.885, 8.4 (Lehky); 22.875, 8.2 (Hornoch); 22.885, 8.3 (Lehky); 23.888, 8.2 (Hornoch); 23.935, 8.4 (A. P. Correia, Esposende, Portugal); 24.925, 8.2 (Hornoch); 25.896, 8.1 (Lehky); 26.877, 8.1 (Hornoch); 26.882, 8.1 (Lehky); 27.872, 8.0 (Hornoch); 30.874, 8.5 (Hornoch); 31.885, 8.6 (Hornoch); Aug. 1.835, 8.7 (Hornoch); 1.854, 8.6 (Lehky); 3.876, 8.6 (Hornoch); 4.894, 8.7 (Hornoch); 4.916, 8.6 (Lehky); 5.842, 8.6 (Hornoch); 5.916, 8.7 (Lehky); 6.838, 8.7 (Hornoch); 6.916, 8.7 (Lehky); 9.809, 8.6 (T. Scarmato, Calabria, Italy); 10.922, 7.6 (Scarmato); 11.840, 7.3 (Scarmato); 12.829, 7.4 (Scarmato); 13.827, 7.9 (Scarmato); 14.808, 7.6 (Scarmato); 14.882, 7.8 (Lehky); 15.863, 7.4 (Scarmato); 16.803, 7.9 (Scarmato).