Please use this identifier to cite or link to this item:
Full metadata record
DC FieldValueLanguage
dc.contributor.authorRamya, M. Anche-
dc.identifier.citationPh.D. Thesis, University of Calcutta, Calcuttaen_US
dc.descriptionThesis Supervisor Prof. Anupama G Cen_US
dc.description.abstractPolarimetric observations of celestial objects reveal information regarding magnetic field, scattered dust and planetary atmosphere. The degree of polarization, which is of interest to astronomers, ranges from 10 -5 to a few tens of percent. A potential problem in carrying out polarimetry in astronomy is the polarization introduced by the telescope and instrument optics to the incoming light. Hence, it is necessary to estimate the polarization effects for any telescope prior to the design of a polarimeter. We have developed a polarization model to estimate the polarization effects from the telescope optics of one of the next generation large telescopes, the Thirty Meter Telescope (TMT). Analysis has been carried out to study the effects of the segments of the primary mirror of TMT and to understand their impact on instrumental polarization and crosstalk. The dependence of polarization effects on the field of view and zenith angle of the telescope at different instrument ports of the TMT has been determined. Polarization aberrations due to telescope optics have been estimated for the adaptive optics system to ascertain their effect on the final PSF of the telescope. This is useful in the design of second generation instruments for TMT with high contrast and high spatial resolution capabilities. We also propose a design technique for the mitigation of the polarization effects due to the telescope optics in future polarimetric instruments. The polarization ray tracing algorithm which was used to develop the polarization model for TMT was also used to develop a polarization model for the Multi-Application Solar Telescope (MAST). The results of the analytical model were veri ed experimentally to understand the deviations between the model and the observations. The Stokes parameters were measured for different input polarizations at the wavelength of 6173 A using an imaging spectro-polarimeter. A fairly good match is seen between the model and the observed Mueller matrix elements. Finally, for an understanding of the science requirements, we have studied the polarimetric properties of a few nova systems as a case study. The studies were conducted using linear polarization data obtained with imaging and photopolarimeters available on the existing 1-2 m class telescopes.en_US
dc.publisherIndian Institute of Astrophysicsen_US
dc.rights© Indian Institute of Astrophysics-
dc.subjectInstrumental polarizationen_US
dc.subjectThirty Meter Telescopeen_US
dc.titleDetermination of polarimetric capabilities of astronomical telescopesen_US
Appears in Collections:IIAP Ph.D.Theses

Files in This Item:
File Description SizeFormat 
Determination of polarimetric capabilities of astronomical telescopes.pdf7.01 MBAdobe PDFView/Open

Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.