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dc.contributor.authorNeha, S-
dc.contributor.authorMaheswar, G-
dc.contributor.authorSoam, A-
dc.contributor.authorLee, C. W-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Vol. 476, No. 4, pp.4442-4458en_US
dc.descriptionRestricted Accessen_US
dc.description.abstractWe made R-band polarization measurements of 234 stars towards the direction of the MBM 33-39 cloud complex. The distance of the MBM 33-39 complex was determined as 120 ± 10 pc using polarization results and near-infrared photometry from the 2MASS survey. The magnetic field geometry of the individual clouds inferred from our polarimetric results reveals that the field lines are in general consistent with the global magnetic field geometry of the region obtained from previous studies. This implies that the clouds in the complex are permeated by the interstellar magnetic field. Multi-wavelength polarization measurements of a few stars projected on to the complex suggest that the size of the dust grains in these clouds is similar to those found in the normal interstellar medium of the Milky Way. We studied a possible formation scenario of the MBM 33-39 complex by combining the polarization results from our study with those from the literature and by identifying the distribution of ionized, atomic and molecular (dust) components of material in the region.en_US
dc.publisherOxford University Press on behalf of the Royal Astronomical Societyen_US
dc.rights© Royal Astronomical Society-
dc.subjectISM: cloudsen_US
dc.subjectISM: individual objects: MBM 33-39en_US
dc.subjectISM: magnetic fieldsen_US
dc.titlePolarization of seven MBM clouds at high Galactic latitudeen_US
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