Abstract
Abstract One of the Roman Space Telescopes principal science objectives is to measure dark energy's equation-of-state using a strategic combination of imaging and spectroscopic surveys at high galactic latitude. Type Ia Supernovae survey requirements demand 0.3% photometric accuracy and calibration of key systematic effects. One of these is count rate dependent nonlinearity (CRNL) that if uncorrected affects the accuracy of SNe Ia distance measurements. Romans Relative Calibration System (RCS) enables on-orbit measurement and tracking of CRNL, through a direct illumination mode and a simultaneous lamp plus scene mode. We present results on the impact of CRNL calibration on the dark energy figure of merit (FoM), for a specific reduction of RCS capabilities. We examined many combinations of illumination and passbands, finding that only six meet the requirements. No RCS at all results in a factor of 5 degradation in the FoM.
Highlights
The Nancy Grace Roman Space Telescope is a NASA flagship mission described in the 2010 Decadal Survey to be a stage 4 dark energy mission
One of the Roman Space Telescopes principal science objectives is to measure dark energy's equation-of-state using a strategic combination of imaging and spectroscopic surveys at high galactic latitude
Type Ia Supernovae survey requirements demand 0.3% photometric accuracy and calibration of key systematic effects. One of these is count rate dependent nonlinearity (CRNL) that if uncorrected affects the accuracy of SNe Ia distance measurements
Summary
The Nancy Grace Roman Space Telescope is a NASA flagship mission described in the 2010 Decadal Survey to be a stage 4 dark energy mission. Provides light on every pixel of the focal plane array, for each filter, spanning a flux range equivalent to that between a 15th mag star and a 26th mag supernova With this method, the CRNL is determined by the ratios of any two illumination levels for each filter. In the absence of a CRNL correction, the galaxy shapes are undercorrected for the PSF, and the weak lensing signal amplitude will be underestimated In both cases, if the CRNL is not corrected for it will result in a FoM lower than that specified by the 2010 Decadal Survey, the mission will be not achieve one of its prime objectives, reducing it from a stage 4 dark energy mission to a stage 3.
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
