UV-to-Infrared laboratory spectroscopy facility

for planetary solids and surfaces

Trans-National Access – TNA

B. Schmitt (LPG), J. Helbert (IPR), B. Reynard (LST), L. d’Hendecourt (IAS)

Goals

• Planetary studies based on spectroscopic remote sensing and in-situ:

UV-Visible-IR spectroscopy and imaging spectroscopy of solids present at the surface or in the atmosphere (grains, aerosols, clouds) of solar system bodies.

• IR/Raman micro-spectroscopies for studies of extraterrestrial samples

Help scientists to prepare and analyze visible-infrared observations– ground or space based telescopes– exploration and in-orbit space missions– in-situ probe and rovers

Allow recording of laboratory spectra requisite for their analysis Sample caracterization (extraterrestrial, synthetic, …) Help development of space mission instruments : optical calibration

ObjectivesSpectroscopic facility

• Provide access to the planetary community to a complete and comprehensive set of laboratory spectroscopic tools to measure the spectroscopic properties – from the UV to the far-infrared – of natural, synthetic and technical solid samples and surfaces.

• Various instruments and techniques cover :

– The whole solar flux + planetary thermal ranges (0.3-2500 µm)

– Transmission spectroscopy– Emission spectroscopy– Reflection (bidirectional, diffuse and specular) spectroscopy– Micro-imaging infrared spectroscopy – Raman micro-spectroscopy and micro-imaging– Fluorescence micro-spectroscopy (LIF)

Research teams • Laboratoire de Planétologie de Grenoble

[LPG](CNRS-UJF, Grenoble, France)B. Schmitt & al.

• Laboratoire des Sciences de la Terre (ENS-Lyon, France)[LST]B. Reynard & al.

• Institute of Planetary Research (DLR-Berlin, Germany) [IPR]J. Helbert & al.

• Institut d’Astrophysique Spatiale (Univ. Paris, Orsay, France) [IAS]L. d’Hendecourt & al.

• + …

Instruments and techniques of facility

LPG : - Transmission spectroscopy (Vis to far-IR) at room temperatureat low temperature (> 10 K)

- Bidirectional reflection spectroscopy of surfaces (UV to mid-IR) - Micro-imaging spectroscopy (near- and mid-infrared) + ATR

IPR : - Thermal emission spectroscopy (1-50 μm) - Emission spectroscopy in vacuum and at temperatures up to 700K- Bi-conical diffuse reflection spectroscopy (Vis to mid-IR)

LST : - Raman micro-spectroscopy with visible excitations: at room and at high pressure and temperature, at low temperature (77 K)

- Raman micro-spectroscopy with UV excitations- Micro-imaging Raman spectroscopy with visible and UV excitations- Fluorescence spectroscopy with UV and visible excitations

IAS : - Transmission spectroscopy (Vis to Far-IR) at low temperature (> 10 K)- IR micro-spectrometry (Mid to Far-IR) on the synchrotron facility SOLEIL

- UV to Vis transmission spectroscopy of organic films- Spectro-fluorimetry of films and powders

Solid Materials that can be measured

• Ices, volatile molecules, hydrates, …• Organics: simple, macromolecular materials, polymers, • Rocks, minerals, salt, hydrated materials, …• Other compounds (Sulfur compounds, …)• Natural and Extraterrestrial samples (meteorites, IDP’s, …)• Optical components (windows, filters, reflectors, …)

• Different physical state and texture :– Compact (rock, ice, ..)– Powder (minerals, snow, …) : surface, – Thin films– Single grain, Monocrystals, polished thin section, …– Sample size : large (> 10 cm), medium (mm – cm), small (~10 µm)– Temperature : very low (10 K) to very high (700 K)

Transmission spectroscopy (0,4 – 200 µm)

Sampling- Thin films on windows- crystals growth in cells- powder in KBr pellets- diffuse reflectance (future attachment)

Side instruments :- Laser interferometry- UV an Vis irradiation- mass spectrometry (300 AMU)

Infrared spectrometer (FTS) with cryogenic optical system (10 - 350 K) under vacuum

Solids : - Ices, Organics, - Minerals, …- Optical materials, …

Bidirectional spectral reflectance (0,3 – 4,8 µm) of granular and compact surfaces

Variables :

- angles (i,e,a) : 0 - 80°

- Spectral range/resolution/

and sampling

- Temperature -40°C-20°C

- Environment chamber

-70°C – 200°C, atm.

- Grain size, density, …

Materials

- Ices, minerals, salts, …

- Organic materials, …

- Geophysical materials,

- Technical materials …

Spectro-gonio Reflectometer - LPG

Instrumentation of the spectroscopy facility at IPR (DLR Berlin)

• Two Bruker FTIR spectrometers:

• Thermal emission spectroscopy• Wavelength coverage 1-50 µm• Planetary simulation chamber

• Vacuum capable• Temperature up to 700 K

• Bi-conical diffuse reflection spectroscopy

• Wavelength coverage 0.5-25 µm

• extended sample preparation capabilities • extensive collection of planetary analog

materials

Associated JRA project

• This TNA project is closely associated with a JRA project aimed at developing :

– The instruments, measurements and analysis techniques provided in this facility

– Spectroscopic data bases providing access to the whole community to spectra and products recorded with this facility.

Development of a UV-to-IR spectroscopy facility and

associated data bases of planetary solids and surfaces

Joint Research Activity – JRA

B. Schmitt (LPG), J. Helbert (IPR),

B. Reynard (LST), L. d’Hendecourt (IAS)

Objective 1

• Develop the capabilities of the facility

Expand :– our sampling techniques (micro-samples, …), – the conditions in which they can be measured

(temperature, pressure, observation geometry, polarization, …)

– the capabilities of our current instruments (spectral range, …).

Facility developmentInstruments developments :

• UV-Vis transmission spectroscopy • Bi-conical diffuse reflection under vacuum• in situ UV Raman micro-spectroscopy under high pressure and

temperature• Near to far infrared emission spectroscopy under vacuum and at high

temperatures• IR, UV-Vis transmission of organic films and molecular ices down to 10K• …

Methodology developments :

• Extraction of optical constants (from combined spectroscopies)• Emission and reflection spectra modeling• Spectro micro-images analysis (automated classification, identification,

quantification, …)

Objective 2 : Data Bases• Data bases requisite for the analysis of spectro-photometric

observations and extraterrestrial sample measurements.• Also of great help in the design of space mission

observation strategies.

Provide the planetary community with :

– several spectroscopic data bases (UV to far-infrared) of solids (compliant to Virtual observatory)

– a physical properties data base of solids (ices, organic molecules, extraterrestrial and synthetic organic matter, minerals, …).

to be merged in IDIS ?

Databases development• LPG :

– General frame of databases. – UV-to-IR transmission spectroscopy and optical constants – Bidirectional and diffuse reflection spectroscopy, – Micro-imaging infrared spectroscopy. – Physical properties of solids.

• LST : – Raman and Fluorescence database for meteoritic and planetary

analogue materials and hydrated glasses.

• IPR : – Near to mid-IR emissivity of planetary analog materials – Bi-conical diffuse reflection spectroscopy

• IAS : – Optical constants of organic materials (UV to far IR) – Emissivity of molecular ices in the submm.

Phase and temperature of H2O ice

STSP Database (LPG)Transmission spectroscopy – Optical constants

Berlin Emissivity Database (BED - IPR)

• Measurement of the emissivity of planetary analog materials

• Wavelength coverage : 6-23µm

(planned extension to 1-50 µm)

• Samples : 4 grain size fractions

(down to less than 25 µm)

• BED is highly complementary to existing databases (e.g. the ASU Spectral library)

Helbert et al. 2006Maturilli et al. 2006

Example data from the BED

Data from BED and Maturilli, Helbert et al. 2005

Budget TNA

per year 5 years

• Post-Doc (4 x 6 months x 2-5 years) 4 x 18 k€ 305 k€

• Operating costs (20% = 7-20 kE/instrument/y) 120 k€ 600 k€

• Travel costs (participating teams) 20 k€ 100 k€

TOTAL : 200 k€ 1005 k€

Budgetper year 5

years

• Post-Doc (4 x 6 months x 2-5 years): 4 x 18 k€ 305 k€ • Engineer technical/computer (5 years): 36 k€ 180 k€ • Operating/equipment costs (databases): 20 k€ 100 k€

• Equipment/development (facility): 500 k€• Operating costs (7-20 kE/instrument/year) 120 k€ 600 k€

• Travel costs (between participating teams) 30 k€ 150 k€

TOTAL : 365 k€ 1835 k€

IR emissivity lab – example of current projects

•Berlin Emissivity Database (BED) for planetary analog materials

•Support of MarsExpress PFS, Rosetta and VenusExpress VIRTIS data analysis by supporting lab measurements

•Study on the effect of dust loading on a radiator for long living lander missions

•Support of the development of MERTIS on BepiColombo by definition and measurement of Mercury analog materials

A set of analog materials for Mercury

Helbert et al. 2006

Internalnumber

Mineral Size separates (microns)

Locality Subclass, group, formula

MA 1 Andesine-Labradorite(An47-52)

0-25, 25-63, 63-125, 125-250

Madagascar Tectosilicate, plagioclase feldspar (Ca,Na)(Al,Si)AlSi2O8

MA 2 Oligoclase 0-25, 25-63, 63-125, 125-250

Iveland, Norway Tectosilicate, plagioclase feldspar Na(Ca)AlSi3O8

MA 3 Anorthite 0-25, 25-63, 63-125, 125-250

Miyake, Japan

Tectosilicate, plagioclase feldspar CaAl2Si2O8

MA 4 Orthoclase 0-25, 25-63, 63-125, 125-250

Froland, Norway Tectosilicate, potassium feldspar KAlSi3O8

MA 5 Enstatite En85 0-25, 25-63, 63-125, 125-250

Bamble, Norway Inosilicate,orthopyroxene (Mg,Fe)SiO3

MA 6 Diopside 0-25, 25-63, 63-125, 125-250

Otter Lake, Quebec, Canada Inosilicate, clinopyroxene Ca(Mg,Fe)Si2O6

MA 7 Forsterite Fo90 0-25, 25-63, 63-125, 125-250

San Carlos, Arizona, USA Nesosilicate, olivine (Mg,Fe)2SiO4

MA 8 Sulfur 0-25, 25-63, 63-125, 125-250

Agrigento, Sicily, Italy Element, non-metal, S

MA 9 Apollo 16 soil sample 62231

0-1000 Descartes highlands,southeast rim of Buster crater

Mature lunar soil

• A set of analog materials for Mercury is already part of the BED

• We are currently small standard sets of analog materials for Mars, Moon to be include in the BED

The Planetary Emissivity Laboratory (PEL)• The Planetary Emissivity Laboratory allows

measuring the emissivity of planetary analog materials in the wavelength range from 1-50 µm

• very high sensitivity in the NIR and MIR range - ideally suited to study fine grained materials

• The spectrometer can be evacuated to remove the effects of atmosphere

• emissivity chamber (developed at DLR) working with dry air purging is used

• replaced by a “real” planetary simulation chamber (PSC)

will allow measurments under vacuum and for sample temperatures up to 700K

• The facility is capable of providing measurements on analog materials for a widerange of planetary bodies and space craft instruments

ASU

PEL NIR+MIR

PEL FIR

Sketch of the Planetary Simulation Chamber

Hot Blackbody with adjustable T

Cold Blackbody (LN2) and cold shield

Optical port for FT spec

Chamber access

Sample cup with Tc

Parabolic mirror

Cooper cold shield (LN2)

Stepper motor for mirror drive

•Allows measurement under vacuum

•Samples can be heated up to 700K

•Thermal gradients can be introduced in the sample