1. ISEM (Infrared Spectrometer for ExoMars) O. Korablev (PI), A. Ivanov (PM) and the ISEM Team IKI - Space Research Institute, Moscow Vernadsky Institute of Geochemistry and Analytical Chemistry, Moscow NII MicroPriborov Guskova - Zelenograd Optical Box (OB) ISEM Electronic Box (EB) ISEM NII MicroPriborov

2. Science objectives of ISEM Search and study of OH/H 2 O-bearing minerals Geological investigation and study a composition of Martian surface materials (minerals and rocks) in the thin uppermost layer Identification and mapping of the distribution of all kind of aqueous alteration products on landing site Real-time assessment of surface composition in selected areas, in support of identifying and selection of the most promising drilling sites Studies of variations of the atmospheric dust properties and of the atmospheric gaseous composition (hampered by limited number of observation cycles)

3. NIR reflectance spectra of different Martian analogue materials Carbonates Spectral resolution ~2.5 nm (18-20 cm -1 ) Hydrated mineral spectra The variety of spectra of the single mineral type is due to different origins of samples => different impurities, microstructure, particle sizes this minerals probably were formed during hydrothermal processes Candidate of Martians background rocks Basalts of different contents Data source: CRISM spectral library

4. ISEM Team Science Team Oleg Korablev, Andrey Ivanov, Nadezhda Evdokimova, Anna Fedorova, Alexey Shapkin, Alexander Trokhimovky, Mikhail Gerasimov, Daniel Rodionov (PM) (IKI), Ruslan Kuzmin, Alexander Basilevsky (Vernadsky) Jean-Pierre Bibring MicrOmega Francois PouletMicrOmega Nicole Schmitz PanCam Andrew Griffiths PanCam Rolf Kilian (UT), Jessica Flahaut (VU UA), Francesca Esposito (NAI) Javier Martín-Torres (Luleå Univ) María-Paz Zorzano (CAB/INTA) Ozgur Karatekin (ROB) Ed Cloutis (U Winnipeg) Technical Team Alexander Stepanov, Andrei Titov, Nick Semena, Oleg Kozlov, Tatiana Kozlova, Nikita Vyazovetsky, Alexander Kiselev, Sergey Mantsevich, Vadim Arefiev, Michael Buntov (IKI), Yurii Kalinnikov (NII MicroPribor) PI: O. Korablev, IKI AOTF Yu. Kalinnikov, NII MicroPribor Thermal N Semena, IKI Electronics A. Titov, IKI Data interface and software: A. Stepanov, IKI Mechanics T. Kozlova, N. Viazovetski, IKI Project Manager: A. Ivanov, IKI Russian Payload Manager: D. Rodionov, IKI Science Team ExoMars

5. ISEM main parameters Electronic Box (EB) ISEM Optical Box (OB) ISEM Spectral range1.1-3.3 µm Field of view1° Optical point detectorInAs (Hamamatsu P10090-21), Two stage thermoelectrically cooled Ø1 mm Spectral resolution25 cm -1 Power consumption12 W Operating temperatures – 40… +20  С. Storage temperatures – 60 … +60  С (qualification down to -120) Output interfaceRS-422 Overall dimension50х160х66 mm (optical box) 80х84х55 mm (electronic box) Mass (estimation)0.6 kg (optical box) 0.5 kg (electronic box)

6. ISEM OB: 3D model and optical scheme

7. ISEM & PanCam Calibration target Mass budget estimation: total mass - 40g Dimensions: 67x76 mm 2x30mm ISEM calibration targets 6x18mm PanCam calibration targets ISEM calibration targets material (at the current moment): 1)Diffuser with reflectance coefficient near 100% in the 400-3000nm spectral range (opal glass or pyroceram) 2)Diffuser with known reflectance spectrum containing deep absorption areas both in visible and IR spectral region (WCT-2065) Targets 1 and 2 are for joint ISEM- PanCam calibrations 1 2 WCT-2065

8. Detector InAs Hamamatsu P10090-21

9. ISEM AOTF AOTF – Acousto-Optic Tunable Filter Incident light Passed light Diffracted light θBθB θDθD Qualification model of Lunar prototype 3D Model Laboratory model of Lunar prototype

10. Instrument accommodation. Optical box ISEM optical block –Spectral range 1.1-3.3 µm –FOV 1° HRC : high-resolution camera FOV 5°

11. ISEM – PanCam/HRC collaboration The optical axes of ISEM and HRC shall be aligned in the same direction within 1° and ISEM’s field of view shall be inside HRC’s field of view (from a distance of 2 meters). Verification of FOV co-alignment by observation of target in IR as well as in visible wavelength

12. Observation scenario Current scenario: one spectrum acquired together with each of 8 HRC images every 2 sols as per Reference Surface Mission, in all 16 spectra per Measurement Cycle. WAC HRC ISEM HRC ISEM

13. Status of Lunar prototype. Surface missions Luna-Globe (Luna 25) and Luna-Resource (Luna 27) planned for launch in 2018 and 2020 LIS (Lunar Infrared Spectrometer) Engineering Qualification Model More technical details in http://www.planetary-department- iki.ru/projects/future/luna/LIS_presentation_COSPAR_2014.pdf AOTF AOTF module LIS EQM. Qualification tests are planned in spring 2015Optical Box (OB) LIS TV camera 1 TV camera 2

14. LIS calibration

15. LIS Measurements The lamp spectrum Spectralon wavelength calibration standard (the red curve is the FTS spectrum) OSRAM calibration lampIntegrating sphere Optical Box

16. Thermovacuum test plan. ISEM team made first attempts to qualify most critical part of Lunar prototype (AOTF) with goal to achieve wider storage thermal range. First tests with laboratory model of Lunar prototype were carried out in April and July of 2013. Thermo-cycling with a number of AOTF prototypes is planned in Jan-Feb 2015. Roscosmos contract covering the production of few AOTF dummy prototypes dedicated for the termovacuum tests is under discussion. AOTF AOTF during thermovacuum tests in 2013

17. Status of Planetary Protection facilities. –IKI has no planetary protection experience. IKI has established the contract with experienced entity (medico-biological) to provide procedures required for ISEM Planetary protection and contamination control plan. The procedures were obtained and introduced in IKI at Quality Assurance level. –In June the ISEM team attended for the first time PP training in ESTEC –The next step will be provision of the necessary facilities for ISEM production, tests and package before delivery. This is a part of Roscosmos 2015 contract (in preparation). AOTF New laboratory facility