Micr Omega Exo Mars JeanPierre Bibring Vincent Hamm

Micr. Omega / Exo. Mars Jean-Pierre Bibring Vincent Hamm Cédric Pilorget IAS Orsay, France and the Micr. Omega team bibring @ ias. u-psud. fr 10 th ESWT, Moscow, April 17, 2018

Exo. Mars: a unique mission ! Exo. Mars 2020 constitutes a totally unique science mission, with the capability to address questions which were not even raised when the mission was conceived and designed: in particular with the fundamental change of paradigm presently being built, with respect to the question of unicity of the Earth (what time/space scale ? ) and of the life it harbors. The mere question of “habitability” is severely challenged and re-visited, while programs to search for life beyond the solar system are decided.

Exo. Mars: a unique mission ! Exo. Mars 2020 constitutes a totally unique science mission, with the capability to address questions which were not even raised when the mission was conceived and designed: in particular with the fundamental change of paradigm presently being built, with respect to the question of unicity of the Earth (what time/space scale ? ) and of the life it harbors. The mere question of “habitability” is severely challenged and re-visited, while programs to search for life beyond the solar system are decided. Exo. Mars 2020 uniqueness resides in particular in its capability 1. to decipher the composition of Martian samples, deeply drilled, down their microscopic scale, sequentially by three instruments spatially coregistered; 2. to identify the sample context by a unique suite of instruments mounted on the rover, and 3. to explore a site known to have (uniquely in the entire solar system) preserved the witness of the processes which sequentially operated over the first billion years of its history, during which Mars (and Earth !) might have hosted an “habitable” environment.

Exo. Mars: a unique mission ! The Micr. Omega team (through OMEGA and CRISM primarily) has played a key role within the LSS process. The entire ESWT should be involved at least to endorse the final proposed selection (November 8 and 9).

Exo. Mars: a unique mission ! The Micr. Omega team (through OMEGA and CRISM primarily) has played a key role within the LSS process. The entire ESWT should be involved at least to endorse the final proposed selection (November 8 and 9). Exo. Mars 2020 is timely, to characterize samples with distinct (than NASA Mars 2020) means (e. g. down to its microscopic scale, from deep subsurface, well characterized…), thus offering to contribute to the sample selection Mars 2020 will perform in caching samples for MSR: cooperative activities between Exo. Mars 2020 and Mars 2020 are more than required. I made proposals in this direction at the recent MEPAG meeting, suggesting in particular an exchange of scientists between the two teams to envision coupled operations, scientific investigations, joined decisions on what samples to be cached etc… The reaction was… moderate… A pro-active decision from Exo. Mars, towards our Project Scientist, to interact with Mars 2020 Project Scientist, should be strongly encouraged at this ESWT.

Micr. Omega / Exo. Mars Goal Micr. Omega, within the ALD, shall characterize the structure and the composition (mineralogical and molecular) of each sample, at its grain scale (20 µm), over 5 x 5 mm 2 FOV, then guide targeting RLS and MOMA

Micr. Omega / Exo. Mars Goal 1. identify, by their composition, the distinct constituents of the samples

Micr. Omega / Exo. Mars Goal Region of Interest 1. identify, by their composition, the distinct constituents of the samples 2. automated identification/location of Ro. I to be analyzed by RLS/MOMA

Micr. Omega / Exo. Mars Goal Region of Interest 1. identify, by their composition, the distinct constituents of the samples 2. automated identification/location of Ro. I to be analyzed by RLS/MOMA unique joined science

Micr. Omega / Exo. Mars Goal 1. identify, by their composition, the distinct constituents of the samples 2. automated identification/location of Ro. I to be analyzed by RLS/MOMA 3. Quantify the abundance of all identified constituent

Micr. Omega / Exo. Mars Goal Micr. Omega, within the ALD, shall characterize the structure and the composition (mineralogical and molecular) of each sample, at its grain scale (20 µm), over 5 x 5 mm 2 FOV, then guide targeting RLS and MOMA Means (fully non destructive) ● Hyperspectral microscopic imagery, in the NIR aaaaa(0. 95 – 3. 7 µm), in up to 400 spectral channels ● Coupled 4 -color optical microscopy aaaaa(0. 5 to 0. 8 µm)

Micr. Omega / Exo. Mars instrument concept cryocooler 2 D VIS-NIR imaging array Source source AOTF imaging optics UCZ Cal target sample UCZ window

Micr. Omega / Exo. Mars instrument concept cryocooler 2 D VIS-NIR imaging array Source source AOTF imaging optics UCZ Cal target sample up to 400 contiguous spectral images, scanned over (covering) the 0. 95 – 3. 7 µm range UCZ window

Micr. Omega / Exo. Mars instrument concept cryocooler 2 D VIS-NIR imaging array Source source AOTF 4 VIS LEDs UCZ Cal target imaging optics sample UCZ window

OFP AM sample in "refillable" container E M. B ILLU UCZ TOP PANNEL Electronics AOTF All subunits (illumination, VIS/NIR detection, active cooling, power conversion, proximity electronics, digital electronics) integrated in a single 2 kg unit (!) instrument concept Detector + Cryocooler Micr. Omega / Exo. Mars Imag. Opt. UCZ TOP PANNEL " fixed" Cal. target

OFP AM E M. B ILLU UCZ TOP PANNEL Electronics AOTF All subunits (illumination, VIS/NIR detection, active cooling, power conversion, proximity electronics, digital electronics) integrated in a single 2 kg unit (!) instrument concept Detector + Cryocooler Micr. Omega / Exo. Mars Imag. Opt. UCZ TOP PANNEL Micr. Omega specific UCZ target sample in "refillable" container " fixed" Cal. target

Micr. Omega / Exo. Mars Development Status ● EQM, fully FM representative, weighted, tested (vibration/thermal/PP/EMI/EMC/shocks), ready to be delivered September 2015; delivery date Prime-driven shifted to mid-March 2017 (need date 26/04/2017 at Micr. Omega CDR), then to May/June/July 2017: delivery done (03/07/17), but still not integrated (mid-May 2018 ? ). ● FM and FS CTs, fully cleaned, delivered to TAS-I in hermetic overpressurized container, still awaiting being integrated in FM UCZ (June 2018 ? ) ● FM, fully tested, calibrated, cleaned (PP included), awaiting delivery based on need date (July 2018 ? ? ? ) ● FS, being integrated, towards a potential delivery, supposedly a dedicated FS strategy is defined, at least at ALD level…

Micr. Omega / Exo. Mars Development Status unit status date at present STM delivered 04/02/2015 ? ? ? EQM CTs delivered 20/07/2016 within QM ALD UCZ EQM unit delivered 03/07/2017 TAS-I shelf delivered 09/03/2018 TAS-I shelf to be delivered pending need date PP cleaned, more test FS CTs delivered 09/03/2018 TAS-I shelf FS unit to be delivered ? pending need date ! being integrated FM CTs • EQM CTs FM unit

Micr. Omega / Exo. Mars Development Status unit status date at present STM delivered 04/02/2015 ? ? ? EQM CTs delivered 20/07/2016 within QM ALD UCZ EQM unit delivered 03/07/2017 TAS-I shelf delivered 09/03/2018 TAS-I shelf to be delivered pending need date PP cleaned, more test FS CTs delivered 09/03/2018 TAS-I shelf FS unit to be delivered ? pending need date ! being integrated FM CTs • EQM CTs FM unit FM and FS are integrated and tested almost in parallel FM first quality validation tests performed successfully (next slides) FM was STERADed successfully yesterday FM will enter mechanical acceptance next week, followed by TVAC FM will then enter an extended phase of calibration, until delivery

Micr. Omega / Exo. Mars Development Status unit status date at present STM delivered 04/02/2015 ? ? ? EQM CTs delivered 20/07/2016 within QM ALD UCZ EQM unit delivered 03/07/2017 TAS-I shelf delivered 09/03/2018 TAS-I shelf to be delivered pending need date PP cleaned, more test FS CTs delivered 09/03/2018 TAS-I shelf FS unit to be delivered ? pending need date ! being integrated FM CTs • EQM CTs FM unit The recent DG (to Space Agencies heads) blame on P/L, targeted as (sole) responsible for delays and overcost, is (felt) truly scandalous. Fingerpointing the “wanted murder”, as if one had decided that the mission cannot be timely achieved, is not the optimized way to create a spirit of co-responsible partnership, towards jointly elaborating the best workaround solutions for the success of Exo. Mars.

Micr. Omega / Exo. Mars Development Status The Industry has a key responsibility in this “contractually-based” behavior, treating P/L as customers, contrasting with the spirit of partnership key for such missions. The demonstration that Exo. Mars cannot be achieved timely is a (unexpected dream) gift offered to those searching to transfer such optional programs to EU.

Micr. Omega / Exo. Mars Development Status The Industry has a key responsibility in this “contractually-based” behavior, treating P/L as customers, contrasting with the spirit of partnership key for such missions. The demonstration that Exo. Mars cannot be achieved timely is a (unexpected dream) gift offered to those searching to transfer such optional programs to EU. We, scientists, have indeed a responsibility in the severe delays triggered by severe technical issues: the (scientifically required) level of performances at mission start was non realistic, and should have been descoped, when it became obvious that it was not achievable. ESA should not have followed Industry interest to maintain them (thus asking for more time (and money!) to solve them. Years ago already some of us proposed to sit and address this issue, in three directions: 1. accept/decide to get at Mars with the system and P/L as is, even with a descoped level of performances (e. g. at UCZ level !); 2. re-shuffle the EQM/FM/FS AIT plans for a 2020 launch, and reprioritize their sequencing. Was never accepted but : still on the table !

Micr. Omega / Exo. Mars A few preliminary FM results

Micr. Omega / Exo. Mars A few preliminary FM results Micr. Omega spectrum (20 x 20 pixels 2 = 400 x 400 mm 2) (not fully calibrated yet and measurement performed at T°=26°C !!) Reference spectrum (without window)

weathered alkali olivine basalt from Painted Hills (Oregon) ~ 1. 5 cm

weathered alkali olivine basalt from Painted Hills (Oregon) albedo map (1. 3 µm) ~ 1. 5 cm

weathered alkali olivine basalt from Painted Hills (Oregon) ~ 1. 5 cm albedo map (1. 3 µm) Mean Micr. Omega spectrum

weathered alkali olivine basalt from Painted Hills (Oregon) albedo map (1. 3 µm) olivine map 1. 4 c c 1. 04 ~ 1. 5 cm

weathered alkali olivine basalt from Painted Hills (Oregon) albedo map (1. 3 µm) ~ 1. 5 cm olivine map 1. 4 c c 1. 04 5 x 5 px Micr. Omega spectrum 1 µm olivine band

weathered alkali olivine basalt from Painted Hills (Oregon) albedo map (1. 3 µm) olivine map 1. 4 c c 1. 04 hydration map (1. 9 µm) c ~ 1. 5 cm

weathered alkali olivine basalt from Painted Hills (Oregon) albedo map (1. 3 µm) olivine map 1. 4 c c 1. 04 hydration map (1. 9 µm) c 0. 1 0. 4 ~ 1. 5 cm

weathered alkali olivine basalt from Painted Hills (Oregon) albedo map (1. 3 µm) ~ 1. 5 cm olivine map 1. 4 c c 1. 04 5 x 5 px Micr. Omega spectrum hydration map (1. 9 µm) c 1, 9 & 1, 4 µm hydration bands 0. 1 0. 4

weathered alkali olivine basalt from Painted Hills (Oregon) ~ 1. 5 cm olivine map albedo map (1. 3 µm) 1. 4 c c 1. 04 5 x 5 px Micr. Omega spectrum hydration map (1. 9 µm) carbonate map c carbonates bands 0. 1 0. 4 0. 01 0. 4

weathered alkali olivine basalt from Painted Hills (Oregon) olivine map albedo map (1. 3 µm) 1. 4 c c 1. 04 hydration map (1. 9 µm) carbonate map c 0. 1 0. 4 0. 01 0. 4 ~ 1. 5 cm

weathered alkali olivine basalt from Painted Hills (Oregon) ~ 1. 5 cm olivine map albedo map (1. 3 µm) 1. 4 c c 1. 04 hydration map (1. 9 µm) carbonate map On top of the identification and location of all constituents, we shall perform the modelled quantification of the abundances c 0. 1 0. 4 0. 01 0. 4