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Interstellar Medium in the M43 Nebula

Gnaciński P.

Acta Astronomica

2009

Vol. 59, No. 3

325--334

We present a list of interstellar absorption lines in the direction of HD 37061 in the M43 nebula. Some of the absorption lines arise from atomic excited levels that are uncommon in interstellar clouds. The excited levels of FeII are populated by fluorescence. We found a large number of H2 molecular absorption lines arising from vibrationally excited levels. The ortho/para H2 ratio is equal to 2.7. The H2 rotational temperature of vibrational levels 1-5 exceeds 2000 K.

Composition of the Interstellar Medium

Gnaciński P., Krogulec M.

Acta Astronomica

2006

Vol. 56, No. 4

373--384

We present an analysis of the FeII, GeII, MgI, MgII, SI, SII, SiII and ZnII interstellar lines for 63 stars. Column density of MgII, SII, SiII and ZnII is well correlated with distance. However, the column density - distance relation should be used with care for the estimation of the distance to OB stars. For stars with large f(H2) this relation can lead to a large overestimation of the distance. The column densities of MgII, SiII and GeII (our largest samples of data) normalized to their total hydrogen column densities decrease with interstellar reddening E(B-V) as expected for elements that are incorporated into dust grains. The GeII abundance (GeII/H) is lower in dense molecular clouds. The abundances of all analyzed elements are generally lower than their Solar System values.