To obtain the polarization due to the dust grains that are
present in the cloud, it is essential to subtract the polarization due to those that are present
foreground to the cloud. The polarization vectors of foreground subtracted 186 stars are
over-plotted on the WISE 12m image as shown in Fig. 1. The mean values of P% after
the subtraction of the fore- ground interstellar polarization is obtained as 1.5 %. The mean
value of P is found to be 40 which is considered as the mean direction of the plane of the
sky component of magnetic eld in Gal 110-13. Based on far-infrared, HI and CO data of
the region, Odenwald et al. (1992) proposed cloud-cloud collision scenario to be the most
preferred mechanism responsible for the formation of Gal 110-13. They suggested that the
Gal 110-13 was formed as a result of the interaction between two HI clouds moving across
the line of sight and having velocity components of ô€€€8 and ô€€€6 km sô€€€1. They also suggested
that the southern part compared to the northern part is in an advanced stage which resulted
in it being predominantly molecular. According to Odenwald et al. (1992), based on HI
observations, collided clouds have traveled across the line of sight in the northeastô€€€southwest
direction. But the current magnetic eld geometry is almost perpendicular to the proposed
direction of the interaction of the clouds. Also, the simulations show that irrespective of the
initial eld conguration, in both parallel and perpendicular cases the eld distribution after
the shock interaction was found to be chaotic especially on the large scales (Marinho et al.,
2001). However, the observed magnetic eld lines from polarization are found to be uniformly
distributed contrary to the results from the simulations.
Lee and Chen (2007) have considered either a supernova explosion or ionization fronts from
a massive star in the vicinity of Gal 110-13 as alternate mechanism that might have caused
its cometary shape.