Volume 588, April 2016
|Number of page(s)||14|
|Section||Interstellar and circumstellar matter|
|Published online||16 March 2016|
Magnetic field geometry of an unusual cometary cloud Gal 110-13
1 Aryabhatta Research Institute of Observational Sciences (ARIES), 263002 Nainital, India
2 Pt. Ravishankar Shukla University, 492010 Raipur, India
3 Korea Astronomy & Space Science Institute (KASI), 776 Daedeokdae-ro, Yuseong-gu, Daejeon, Republic of Korea
4 University of Science Technology, 217 Gajungro, Yuseong-gu, 305-333 Daejeon, Republic of Korea
5 Indian Institute of Space Science and Technology (IIST), 695547 Trivandrum, India
Received: 28 June 2015
Accepted: 19 October 2015
Aims. We carried out optical polarimetry of an isolated cloud, Gal 110-13, to map the plane-of-the-sky magnetic field geometry. The main aim of the study is to understand the most plausible mechanism responsible for the unusual cometary shape of the cloud in the context of its magnetic field geometry.
Methods. When unpolarized starlight passes through the intervening interstellar dust grains that are aligned with their short axes parallel to the local magnetic field, it gets linearly polarized. The plane-of-the-sky magnetic field component can therefore be traced by doing polarization measurements of background stars projected on clouds. Because the light in the optical wavelength range is most efficiently polarized by the dust grains typically found in the outer layers of the molecular clouds, optical polarimetry enables us to trace the magnetic field geometry of the outer layers of the clouds.
Results. We made R-band polarization measurements of 207 stars in the direction of Gal 110-13. The distance of Gal 110-13 was determined as ~450 ± 80 pc using our polarization and 2MASS near-infrared data. The foreground interstellar contribution was removed from the observed polarization values by observing a number of stars located in the vicinity of Gal 110-13 which has Hipparcos parallax measurements. The plane-of-the-sky magnetic field lines are found to be well ordered and aligned with the elongated structure of Gal 110-13. Using structure function analysis, we estimated the strength of the plane-of-the-sky component of the magnetic field as ~25 μG.
Conclusions. Based on our results and comparing them with those from simulations, we conclude that compression by the ionization fronts from 10 Lac is the most plausible cause of the comet-like morphology of Gal 110-13 and of the initiation of subsequent star formation.
Key words: ISM: clouds / polarization / ISM: magnetic fields / ISM: individual objects: Gal 110-13
© ESO, 2016
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