| Name: | Arijit Maiti |
| Affiliation: | Physical Research Laboratory |
| Conference ID : | ASI2024_536 |
| Title : | Performance Simulations of M-FOSC-EP instrument for Spectro-polarimetry with 2.5m PRL telescope |
| Authors : | Arijit Maiti, Mudit K. Srivastava, Bhavesh Kumar Mistry, Ankita Patel, Vaibhav Dixit, Arvind S. Rajpurohit, and Vipin Kumar |
| Authors Affiliation: | 1. Arijit Maiti, Mudit K. Srivastava, Bhavesh Kumar Mistry, Ankita Patel, Vaibhav Dixit, Arvind S. Rajpurohit (Physical Research Laboratory, Ahmedabad, 380009)
2. Vipin Kumar (University of Cologne) |
| Mode of Presentation: | Oral |
| Abstract Category : | Facilities, Technologies and Data science |
| Abstract : | Mt. Abu Faint Object Spectrograph and Camera – Echelle Polarimeter (M-FOSC-EP) is a two-channel multi-mode instrument currently being designed for 2.5m PRL telescope at Mt. Abu. M-FOSC-EP is designed to have two optical arms, (1.) the low-resolution arm (LRA) for low-resolution (R ~ 500-700) spectroscopy and filter-based imaging modes and (2.) an intermediate-resolution (R ~ 15000) Spectro-polarimetric arm using Echelle and cross-disperser gratings. The optical design of the instrument has been completed, the optical components are being procured and mechanical design is currently ongoing. To evaluate the expected performance of the instrument, a mathematical simulation model for its Spectro-polarimetry mode has been developed with the aim of optimizing the development process, observation methodology, and data reduction pipeline development. The instrument simulation code is developed in Python and incorporates various optical parameters (such as PSF, efficiency, dispersion, etc.) from the ZEMAX-based optical design model of the instrument. The algorithm takes the flux, degree of polarization, and angle of polarization as a function of the wavelength for an astrophysical object as input and produces raw CCD data frames which contain the echelle-cross dispersed spectra in multiple orders of two orthogonal polarized beams. These raw data frames also contain the effects of various instrumental noise sources (such as read-out noise, dark noise, etc.) in addition to the inherent photon noise of the source. These frames are then processed to retrieve the spectral and polarization information as a function of wavelength with corresponding errors. Multiple simulations are done to evaluate the noise characteristics of the instrument with respect to source magnitudes, integration time, etc. in terms of signal-to-noise ratio, polarization accuracy, etc. In this poster, we shall present the mathematical model and algorithm of these simulations along with the derived results. |
