The Line Emission Mapper (LEM) probe mission concept
conference contribution
posted on 2024-12-13, 10:14 authored by Ralph P Kraft, Akos Bogdan, John Zuhone, JS Adams, JD Alvarado-Gomez, C Argiroffi, M Ayromlou, M Azadi, Simon R Bandler, M Barbera, A Bhardwaj, V Biffi, D Bodewits, E Boettcher, B Branham, J Burchett, D Burke, Jenna Cann, Jennifer CarterJennifer Carter, D Castro, P Chakraborty, K-W Chan, S Chen, E Churazov, K Coderre, MF Corcoran, Renata S Cumbee, SV DePalo, K Dolag, M Donahue, WB Doriese, Jeremy Drake, William Dunn, Megan E Eckart, D Eckert, S Ettori, Y Ezoe, CH Feldman, E Flaccomio, W Forman, Massimiliano Galeazzi, Amy Gall, Cecilia Garraffo, M Gonzalez, N Grosso, J Hartley, N Hell, L Hernquist, Edmund Hodges-Kluck, J Houston, S Hull, N Islam, P Janas, F Jennings, C Jones, Philip E Kaaret, H Kanner, M Karovska, V Kashyap, P Kavanagh, Richard L Kelley, Ildar Khabibullin, Caroline A Kilbourne, C-G Kim, D Koutroumpa, O Kovacs, K Kuntz, S-H Lee, Maurice A Leutenegger, T Linn, S Lotti, M Markevitch, K Martin, L May, D McCammon, S McEntee, S Mei, Francois Mernier, M Miceli, J Miller, M Mirakhor, K Monsch, Y Naze, D Nelson, A Nordt, Anna Ogorzalek, J Olsen, S Orlando, E Osborne, L Oskinova, Daniel J Patnaude, Ryan Pfeifle, C Pinto, Paul P Plucinsky, G Ponti, D Porquet, Frederick S Porter, D Prele, S Ramm, S Randall, E Rasia, Markus Rau, S Richardson, K Sakai, A Sarkar, G Schellenberger, S Sciortino, J Schaye, A Simionescu, S Smith, M Sobolewska, James Steiner, J Stern, Yuanyuan Su, M Sun, Nhut Truong, E Ursino, M Valentini, S Veilleux, S Vladutescu-Zopp, M Vogelsberger, N Wakeham, S Walker, QD Wang, B Wargelin, Kimberly Weaver, J Werk, N Werner, S Wolk, C Zhang, WW Zhang, Irina ZhuravlevaThe Line Emission Mapper (LEM) is a Probe mission concept developed in response to NASA's Astrophysics Probe Explorer (APEX) Announcement of Opportunity. LEM has a single science instrument composed of a large-area, wide-field X-ray optic and a microcalorimeter X-ray imaging spectrometer in the focal plane. LEM is optimized to observe low-surface-brightness diffuse X-ray emission over a 30′ equivalent diameter field of view with 1.3 and 2.5 eV spectral resolution in the 0.2 − 2.0 keV band. Our primary scientific objective is to map the thermal, kinetic, and elemental properties of the diffuse gas in the extended X-ray halos of galaxies, the outskirts of galaxy clusters, the filamentary structures between these clusters, the Milky Way star-formation regions, the Galactic halo, and supernova remnants in the Milky Way and Local Group. The combination of a wide-field optic with 18′′ angular resolution end-to-end and a microcalorimeter array with 1.3 eV spectral resolution in a 5′ × 5′ inner array (2.5 eV outside of that) offers unprecedented sensitivity to extended low-surface-brightness X-ray emission. This allows us to study feedback processes, gas dynamics, and metal enrichment over seven orders of magnitude in spatial scales, from parsecs to tens of megaparsecs. LEM will spend approximately 11% of its five-year prime science mission performing an All-Sky Survey, the first all-sky X-ray survey at high spectral resolution. The remainder of the five-year science mission will be divided between directed science (30%) and competed General Observer science (70%). LEM and the NewAthena/XIFU are highly complementary, with LEM's optimization for soft X-rays, large FOV, 1.3 eV spectral resolution, and large grasp balancing the NewAthena/X-IFU's broadband sensitivity, large effective area, and unprecedented spectral resolving power at 6 keV. In this presentation, we will provide an overview of the mission architecture, the directed science driving the mission design, and the broad scope these capabilities offer to the entire astrophysics community.
History
Author affiliation
College of Science & Engineering Physics & AstronomySource
Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray. 16-22 JUNE 2024Version
- AM (Accepted Manuscript)
