Browsing by Author "Pandey, S. K."

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    BVR photometry of a newly identified RS CVn binary star HD 61396
    (2011-07-06) Barway, Sudhanshu; Pandey, S. K.
    BVR photometry of a recently identified RS CVn binary star HD 61396, carried out during 2001, is presented. The new photometry reveal significant evolution in the shape and amplitude of light curve when compared with those reported earlier by Padmakar et al.(2000). The traditional two-starspot model has been used to obtain the spot parameters from the observed light curve. Changes in the spot area and their location on the stellar surface are discernible from the extracted parameters from the new photometry.
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    Dust and gas in nearby early-type galaxies
    (2011-11-22) Kulkarni, Samridhi; Pandey, S. K.
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    HD 52452: New BVRI photometry
    (2012-07-06) Barway, Sudhanshu; Pandey, S. K.
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    New BVR photometry of six prominent RS CVn Binaries
    (2015-03-01) Padmakar; Pandey, S. K.
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    Properties of dust in early-type galaxies
    (2006-11-12) Patil, M. K.; Pandey, S. K.; Sahu, D. K.; et al.
    We report optical extinction properties of dust for a sample of 26 early-type galaxies based on the analysis of their multicolour CCD observations. The wavelength dependence of dust extinction for these galaxies is determined and the extinction curves are found to run parallel to the Galactic extinction curve, which implies that the properties of dust in the extragalactic environment are quite similar to those of the Milky Way. For the sample galaxies, value of the parameter RV, the ratio of total extinction in V band to selective extinction in B & V bands, lies in the range 2.03 - 3.46 with an average of 3.02, compared to its canonical value of 3.1 for the Milky Way. A dependence of RV on dust morphology of the host galaxy is also noticed in the sense that galaxies with a well defined dust lane show tendency to have smaller RV values compared to the galaxies with disturbed dust morphology. The dust content of these galaxies estimated using total optical extinction is found to lie in the range 104 to 106 M⊙, an order of magnitude smaller than those derived from IRAS flux densities, indicating that a significant fraction of dust intermixed with stars remains undetected by the optical method. We examine the relationship between dust mass derived from IRAS flux and the X-ray luminosity of the host galaxies.The issue of the origin of dust in early-type galaxies is also discussed.