We have recorded spectra of iron-neon and iron-argon hollow cathode lamps in the region 1700Å -5 µm (59 000 -2000 cm −1 ), with Fourier transform (FT) spectrometers at the National Solar Observatory, Tucson, Arizona, U.S.A. and Imperial College, London, U.K., and with a high resolution grating spectrograph at the National Institute of Standards and Technology, Gaithersburg, U.S.A. The uncertainty of the strongest lines in the FT spectra is <0.002 cm −1 (0.2 mÅ at 3000Å; 8 mÅ at 2 µm ). Pressure and current-dependent shifts are <0.001 cm −1 for transitions between low lying levels, increasing to 0.006 cm −1 for transitions between the most highly excited levels. We report 28 new energy levels of Fe I and revised values of another 818 levels. We have identified 9501 lines as due to 9759 transitions in Fe I, and these are presented in the form of a new multiplet table and finding list. This compares with the ∼5500 lines due to 467 energy levels in the multiplet tables of Moore (1950, 1959). The biggest increase is in the near ultraviolet and near infra-red, and many of the new lines are present in the solar spectrum. Experimental log(gf) values are included where they are available. A further 125 unidentified lines due to Fe I are given. The tables are also available in computer-readable form.

We have measured the oscillator strength of the Ni I line at 6300.34Å, which is known to be blended with the forbidden [O I] λ6300 line, used for determination of the oxygen abundance in cool stars. We give also wavelengths of the two isotopic line components of 58 Ni and 60 Ni derived from the asymmetric laboratory line profile. These two line components of Ni I have to be considered when calculating a line profile of the 6300Å feature observed in stellar and solar spectra. We also discuss the labelling of the energy levels involved in the Ni I line, as level mixing makes the theoretical predictions uncertain.

We present the first ultraviolet and optical images of Car and its circumstellar Homunculus nebula, obtained with the Advanced Camera for Surveys/High Resolution Camera (ACS/HRC) on board the Hubble Space Telescope (HST ). Compared to those at visual wavelengths, UV images reveal excess emission 0B1-0B6 from the central source along the minor axis that may emanate from the outer parts of Car's nonspherical stellar wind, which dominates the UV flux from Car. The UV emission fills the cavity inside a dust torus measured from infrared (IR) data; within 0B2 of the star the UV emission projects a morphology reminiscent of the IR torus, but it is a factor of 10 smaller. This ''little torus'' seen in the UV may be related to the ''Little Homunculus'' discovered recently, signifying recurrent mass ejections with the same geometry. Finally, we reexamine the kinematics of nebular condensations near the star (Weigelt objects C and D) in HST images and spectra obtained over the past decade. We measure heliocentric velocities slower than previous estimates, and from proper motions we derive an ejection date of 1908 AE 12 yr, assuming linear motion. However, because of radiative acceleration, these objects may have been ejected earlier-perhaps during the 1890 outburst of Car.

The spectnrrn and term system of

We have discovered four extremely surprising emission lines of strontium in ejecta near g Carinae.