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    Please use this identifier to cite or link to this item: http://ir.lib.ncu.edu.tw/handle/987654321/50844


    Title: A multiwavelength polarimetric study towards the open cluster NGC 1893
    Authors: Eswaraiah,C;Pandey,AK;Maheswar,G;Medhi,BJ;Pandey,JC;Ojha,DK;Chen,WP
    Contributors: 天文研究所
    Keywords: OPTICAL POLARIZATION OBSERVATIONS;MAIN-SEQUENCE STARS;WAVELENGTH DEPENDENCE;INTERSTELLAR GRAINS;MAXIMUM POLARIZATION;OB ASSOCIATIONS;REGION;EXTINCTION;PHOTOMETRY;NGC-1893
    Date: 2011
    Issue Date: 2012-03-27 18:11:18 (UTC+8)
    Publisher: 國立中央大學
    Abstract: We present multiwavelength linear polarimetric observations for 44 stars of the NGC 1893 young open cluster region along with V-band polarimetric observations of stars of four other open clusters located between l similar to 160 degrees and 175 degrees. We found evidence for the presence of two dust layers located at a distance of similar to 170 and similar to 360 pc. The dust layers produce a polarization P(V) similar to 2.2 per cent. It is evident from the clusters studied in this work that, in the Galactic longitude range from l similar to 160 degrees to 175 degrees and within the Galactic plane (vertical bar b vertical bar < 2 degrees), the polarization angles remain almost constant, with a mean of similar to 163 degrees and a dispersion of 6 degrees. The small dispersion in polarization angle could be due to the presence of a uniform dust layer beyond 1 kpc. Present observations reveal that in the case of NGC 1893, the foreground two dust layers, in addition to the intracluster medium, seem to be responsible for the polarization effects. It is also found that towards the direction of NGC 1893, the dust layer that exists between 2 and 3 kpc has a negligible contribution towards the total observed polarization. The weighted mean for percentage of polarization (P(max)) and the wavelength at maximum polarization (lambda(max)) are found to be 2.59 +/- 0.02 per cent and 0.55 +/- 0.01 mu m, respectively. The estimated mean value of lambda(max) indicates that the average size of the dust grains within the cluster is similar to that in the general interstellar medium. The spatial variation of the polarization is found to decrease towards the outer region of the cluster. In this work, we support the notion, as has already been shown in previous studies, that polarimetry, in combination with the (U - B)-(B - V) colour-colour diagram, is a useful tool for identifying non-members in a cluster.
    Relation: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
    Appears in Collections:[天文研究所] 期刊論文

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