Orion arm

The most detailed v — l maps of the Milky Way are the Dame et al., 2001, observations of molecular gas using CO as a tracer. In this data set, we can clearly identify two different arms (with a ir/2 phase separation, i.e., probably part of an m = 4 set) The Carina arm which is located inwards to the solar galactic radius 11.. and the Perseus arm, externally located relative to Rq. The solar system is located in the Orion arm. We perform our analysis on the Sagittarius-Carina arm (Naoz and Shaviv 2004), which has the richest cluster data. 

As with any other spectral lines, radio lines exhibit Doppler shifts if the molecular gas is in motion. In Fig.7.30 velocity distributions are shown based on Doppler observations on OH, CH and HCHO lines observed in the direction of Cassiopeia A. The components around 45 km/s are due to clouds in the Perseus arm of our galaxy, while the components around 0 km/s are due to the Orion arm. While OH and HCHO appear in absorption, CH is seen in (weak maser) emission against the background source. 

Cation transport experiments were performed in a U-tube glass cell (2.0 cm, i.d.) as reported before. The carrier in CH Cl or CHCl (12 ml) was placed in the base of the U-tube, and two aqueous phases (5 ml, each) were placed in the arms of the U-tube, floating on the membrane phase. The membrane phase was stirred constantly with a magnetic stirrer. The transport rates were calculated from the initial rates of appearance of guest cations and cotransported anion (C10 ) into the receiving aqueous phase, which were determined by means of ion selective electrodes (Orion Model 92-32 for Ba 94-82 for Pb 95-12 for NH 93-19 for K 93-81 for C10 ). 

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