ISEM (Infrared Spectrometer for ExoMars)

O. Korablev (PI), A. Ivanov (PM) and the ISEM TeamIKI - Space Research Institute, MoscowVernadsky Institute of Geochemistry and Analytical Chemistry, MoscowNII MicroPriborov Guskova - Zelenograd

Optical Box (OB) ISEM Electronic Box (EB) ISEM

NII MicroPriborov

Science objectives of ISEM • Search and study of OH/H2O-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)

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

ISEM TeamScience TeamOleg 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 Poulet MicrOmegaNicole 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 TeamAlexander 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

ElectronicsA. Titov, IKI

Data interface and software:

A. Stepanov, IKI

MechanicsT. Kozlova,

N. Viazovetski, IKI

Project Manager: A. Ivanov, IKI

Russian Payload Manager:

D. Rodionov, IKI

Science Team

ExoMars

ISEM main parameters

Electronic Box (EB) ISEM

Optical Box (OB) ISEM

Spectral range 1.1-3.3 µm

Field of view 1°

Optical point detector InAs (Hamamatsu P10090-21), Two stage thermoelectrically cooled Ø1 mm

Spectral resolution 25 cm-1

Power consumption 12 W

Operating temperatures – 40… +20 С.

Storage temperatures – 60 … +60 С (qualification down to -120)

Output interface RS-422

Overall dimension 50х160х66 mm (optical box)80х84х55 mm (electronic box)

Mass (estimation) 0.6 kg (optical box) 0.5 kg (electronic box)

ISEM OB: 3D model and optical scheme

ISEM & PanCam Calibration target

Mass budget estimation: total mass - 40gDimensions: 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

2WCT-2065

ISEM AOTFAOTF – Acousto-Optic Tunable Filter

3

62

V

npM ij

A

lM

dPa 2

Incident light

Passed light

Diffracted

light

θB θD

2

Bsin

Qualification model of Lunar prototype

3D Model

Laboratory model of Lunar prototype

Instrument accommodation. Optical box

• ISEM optical block– Spectral range

1.1-3.3 µm– FOV 1°

• HRC: high-resolution camera

FOV 5°

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

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

HRCISEM

Status of Lunar prototype.• Surface missions Luna-Globe (Luna 25) and Luna-Resource (Luna 27)

planned for launch in 2018 and 2020LIS (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 2015 Optical Box (OB) LIS

TV camera 1

TV camera 2

LIS calibration

LIS Measurements

The lamp spectrum

Spectralon wavelength calibration standard (the red curve is the FTS

spectrum)

OSRAM calibration lamp Integrating sphere

Optical Box

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

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