Abstract
The Lynx X-ray Grating Spectrograph (XGS) is responsible for providing high throughput and spectral resolution for soft x-ray energies. This instrument will help characterize the formation of galaxies and a large-scale structure in the universe. Such goals require large effective areas, >4000 cm2, and high resolving power, R > 5000, over much of the low-energy band, 0.2 to 2.0 keV. A concept design for the XGS using reflection gratings has the potential to achieve these requirements. The design uses achievable grating parameters, efficient packing of the grating array, and a compact detector layout. The concept is presented along with a detailed discussion of the considerations made in its determination.
Highlights
The main scientific contribution of the Lynx X-ray Grating Spectrograph (XGS) is to characterize the diffuse baryonic content in galactic halos and thereby inform formation models to help determine the drivers of galaxy and large-scale structure formation.[1,2] The Lynx XGS will observe 80 sight lines to bright active galactic nuclei (AGN) to reach 1-mÅ sensitivity for absorption lines of OVII and OVIII.[2]
This paper presents a reflection-grating-based concept for the Lynx XGS
Downloaded From: https://www.spiedigitallibrary.org/journals/Journal-of-Astronomical-Telescopes,Instruments,and-Systems on 08 Nov 2021 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use concepts baselined 40% diffraction efficiency for the gratings. These results show that this can be reached using blazed reflection gratings
Summary
The main scientific contribution of the Lynx X-ray Grating Spectrograph (XGS) is to characterize the diffuse baryonic content in galactic halos and thereby inform formation models to help determine the drivers of galaxy and large-scale structure formation.[1,2] The Lynx XGS will observe 80 sight lines to bright active galactic nuclei (AGN) to reach 1-mÅ sensitivity for absorption lines of OVII and OVIII.[2] This number of sight lines should characterize the halos of galaxies with mass 1012−13 MSun out to their virial radii and beyond for a redshift range of z 1⁄4 0 to 12 To accomplish this science goal, the XGS is required to achieve a spectral resolving power of 5000 (λ∕δλ) and an effective area of 4000 cm[2] over the energy range of 0.3 to 0.7 keV.
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