Proceedings of the Workshop
"The Magellanic Clouds and Other Dwarf Galaxies"
of the Bonn/Bochum-Graduiertenkolleg

Spatial distribution of halo high velocity clouds towards the LMC

Bernhard Wierig and Klaas S. de Boer

Sternwarte der Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany

Received 14th March 1998
Abstract. IUE high dispersion spectra of 18 Large Magellanic Cloud stars have been analysed with the aim of mapping the Si II column density in the galactic halo gas towards the LMC. Sample Si II spectra in velocity space are presented which confirm, with their general appearance, earlier results. Low ion stage lines exhibit a component structure with strong features near ∼60 km s-1 and ∼130 km s-1. For these intermediate and high velocity clouds' column densities can be derived. Using H I column densities as reference the abundance of Si II in the galactic halo is estimated. Maps showing the Si II column densities in the two clouds towards the LMC are presented.

1. Introduction

In 1981, Savage and de Boer presented a study of interstellar absorption features toward 6 LMC stars. They found that the low ions like Si II or Fe II exhibit a component structure with strong features near ∼+60 km s-1 and ∼+130 km s-1. Column densities were given for galactic and LMC absorption structures, but only for one star (HD 36402) column densities for the galactic intermediate and high velocity components were given separately (see Savage & de Boer 1981 and references therein).

Since that time many more LMC stars have been observed with the IUE and all the high dispersion spectra have been reprocessed by the IUE observatories with new reduction software. This motivated us to investigate the halo absorption structures in as many LMC star spectra as possible in order to map the Si II column density in these clouds in front of the LMC.

2. Method of analysis

The radial velocity of the LMC of ∼+275 km s-1 (Westerlund 1997) produces a separation of galactic and extragalactic interstellar absorption features which is convenient for the analysis of distinct halo structures. The IUE spectra have been transformed into intensity vs. velocity plots in order to facilitate this analysis and allow for a distinction between intermediate (40 - 100 km s-1) and high velocity (100 - 170 km s-1) components. The resolution of the spectra (λ/Δλ∼1.2·104) is 20 - 25 km s-1 in velocity space.

Inspection of all absorption lines on a given line of sight allows to decide whether a certain spectral structure is a true absorption or not. The equivalent widths are measured by fitting trapezoidal profiles to the absorption structures. Column densities are obtained from a curve-of-growth analysis. Whenever possible, an attempt has been made to obtain column densities for the intermediate and high velocity structures separately. A comparison with H I column densities leads to an estimate of the abundances of Si II in the halo.

3. Results

Si II shows two distinct absorption structures in the galactic halo near ∼60 km s-1 and ∼125 km s-1, which confirms earlier results of Savage & de Boer 1981 (see Fig. 1a, 2a; velocities are given in km s-1 LSR).

Si II column densities in the HVC tend to be higher than those in the IVC (see Fig. 1b, 2b; column densities are given in cm-2). Comparison with H I column densities from McGee & Newton 1986 and McGee et al. 1983 shows that abundances range from -4.65 to -3.1 for the IVC and -4.56 to -2.6 for the HVC.

Assuming a solar abundance of -4.45 (de Boer et al. 1987), we note that Si II appears to be overabundant. However, the values are based on N (H I) from 21 cm. Since the resolution of the Parkes telescope is rather limited (half-power beam width ∼15 arcmin), the columns sampled in Si II and H I most likely do not refer to the same gas.

[Click here to see Figs. 1 and 2!]

4. Discussion

Our results are consistent with those of Savage & de Boer (1981) and McGee et al. (1983). Further UV observations with higher sensitivity are desirable to obtain a denser grid of background light sources. Thus, one could account even better for small-scale variations in column densities.

References


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First version: 22ndJune,1998
Last update: 30thSeptember,1998

Jochen M. Braun   &   Tom Richtler
 (E-Mail: jbraun|richtler@astro.uni-bonn.de)