Please use this identifier to cite or link to this item:
Full metadata record
DC FieldValueLanguage
dc.contributor.authorRamya, M. Anche-
dc.contributor.authorAnupama, G. C-
dc.contributor.authorSriram, S-
dc.contributor.authorSankarasubramanian, K-
dc.contributor.authorSkidmore, W-
dc.identifier.citationProceedings of the SPIE, Vol10703, pp. 107034K-1- 107034K-12en_US
dc.descriptionRestricted Accessen_US
dc.description.abstractThe Thirty Meter Telescope (TMT) is a future generation telescope proposed to be located in Mauna Kea, Hawaii or in La Palma in the Canary Islands. The telescope will have a segmented primary and an inclined tertiary mirror. The segmentation of the primary mirror and the inclination in the tertiary mirror can introduce significant polarization aberrations. Typically, the polarization aberrations, introduced due to the mirror coating and the high incident angles cause small modifications to the Point Spread Function (PSF). Here, we perform the polarization ray tracing for TMT using the optical design software Zemax for different input polarizations for a point source (on-axis). We calculate the diattenuation and retardance aberration maps for all the three mirrors of TMT. The coating induced astigmatism obtained from the retardance of the primary and secondary mirror is found to be of the order of 0.048 radians, whereas, the polarization induced tilt by the retardance of the tertiary mirror is in the order of 0.29 radians. The Jones pupil maps are estimated at two of the instrument ports, Wide Field Optical Spectrograph (WFOS) and Narrow Field Infrared Adaptive Optics System (NFIRAOS).The Amplitude Response Matrix (ARM) estimated at the WFOS port show the presence of ghost PSF's. The magnitude of the ghost PSF components is of the order of 2.5 x 10-5 at 1μm at WFOS port. The ARM and the Point Spread Matrix (PSM) are estimated at the focus of the NFIRAOS instrument. The Stokes PSF is shown for horizontal and vertical polarization as inputs. The Huygen's point spread function obtained from Zemax shows the variations in FWHM for unpolarized and polarized inputs. These estimations would help in the design aspects of a high contrast imaging instrument for the TMT in the future.en_US
dc.publisherSPIE--The International Society for Optical Engineeringen_US
dc.rights© SPIE--The International Society for Optical Engineering-
dc.subjectInstrumental polarizationen_US
dc.subjectPoint spread functionen_US
dc.subjectPolarization aberrationsen_US
dc.subjectJones Pupil mapen_US
dc.subjectPoint spread matrixen_US
dc.subjectThirty Meter Telescopeen_US
dc.titleEstimation of polarization aberrations and its effect on the point spread function of the Thirty Meter Telescopeen_US
Appears in Collections:IIAP Publications

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