lassie: a marie curie training network on astrochemistry nigel mason centre for earth, planetary,...

LASSIE: A Marie Curie Training Network on Astrochemistry

http://www.u-cergy.fr/LERMA-LAMAP/LASSIE/

Nigel Mason Nigel Mason Centre for Earth, Planetary, Astronomy & Space

Research The Open University, UKThe Open University, UK

[email protected]@open.ac.uk

05th Jan 2006 Chemistry of Planets

• Project acronym: LASSIE• Project full title: LABORATORY ASTROCHEMICAL

SURFACE SCIENCE IN EUROPE

1 (Coordinator) Heriot-Watt University Prof Martin McCoustra2 Aarhus University 3 Paris Observatory OBSParis4 University of Münster5 Max-Plank-Gessellschaft6 National Institute forAstrophysics INAF7 Leiden University8 Chalmers University Chalmers9 University of Gothenburg10 University College London11 The Open University12 Queen’s University, Belfast13 Strathclyde University14 Graphic Science15 Gridcore AB Gridcore16 Hiden Analytical Ltd.17 Kore Technology Ltd.


LASSIE ITN

• The LASSIE Initial Training Network is;

• A large inclusive network that will allow interactions across the surface and solid state astrochemistry communities in Europe to be developed.

• Provides the necessary knowledge base and human resources to ensure that the past, present and future multibillion Euro support for observational astronomy is capable of being fully exploited by providing the necessary scientific support to allow astronomers to interpret their observations based on realistic and well-understood laboratory chemistry and physics.

• Provides a much needed infrastructure for developing a coherent programme of astrochemical research within the EU that will allow the ERA to compete more effectively globally.


LASSIE Science Programme aims

• To understand the formation and destruction of interstellar dust.

• To understand the formation of simple molecules, and hence icy mantles, on realistic models of (icy) dust grain surfaces.

• To understand the physical processes that result when an icy grain mantle is heated or irradiated with light, electrons or ions.

• To understand the chemical processes that result when an icy grain mantle is heated or irradiated with light, electrons or ions.

• To understand the role of these processes in observations of grains, ices and the molecules formed by the intermediary of grains and their icy mantles in the evolving Universe.


LASSIE 5 THEMES • Theme 1 - Formation of Grains, Small Molecules and

IcesLink to Eurogenesis ?? As A Tielens said === star death

•The mechanism of formation of interstellar dust grains from their initial condensation through to grain aggregate formation via grain-grain collisions (MPG, OU, UM).•The release of reaction energy into product translation, rotation and vibration in the heterogeneous formation of small molecules on model dust grain surfaces (AU, Chalmers, INAF, OBSParis, UCL,UM).•The rates of molecule and ice formation on dust grain surfaces, including studies of isotopic fractionation (AU, Chalmers, HWU, LUO, INAF, OBSParis, UCL).•The morphology of ices formed reactively on model grain surfaces (AU, Chalmers, HWU, INAF, OBSParis, UCL).•The infrared, optical and ultraviolet (UV) spectroscopy of ices formed reactively on model dust grain surfaces (Chalmers, HWU, LUO, OU, UCL).


LASSIE 5 THEMES

• Theme 2 - Physical Processes in and on Icy Grains

•Understanding the thermal desorption of simple ices, complex mixed ices and clathrates as observed in the cold, dense regions of the ISM associated with star formation (Chalmers, HWU, LUO, OBSParis,SU, UCL).•Understanding desorption of simples ices, complex mixed ices and clathrates induced through interaction with electromagnetic radiation (Chalmers, HWU, LUO, OU, SU, UM, UCL).•Understanding desorption of simple ices, complex mixed ices and clathrates induced via interaction with low energy electrons and models of cosmic rays (AU, Chalmers, HWU, INAF, OU, QUB).•Understanding the role of heat, electromagnetic radiation and cosmic rays in promoting changes in ice morphology (HWU, LUO, INAF, OBSParis, OU, UCL, SU).


LASSIE 5 THEMES

• Theme 3 - Chemical Transformations in and on Icy Grains

• UV photon-induced chemical transformations (HWU, LUO, OU, UCL).

• Low energy electron-induced chemical transformations (AU, HWU, INAF, OU, UCL).

• VUV, XUV and X-ray photon- and cosmic ray-induced chemical transformations (AU, HWU, LUO,INAF, OU, UM, QUB

• Chemical transformations following atom, radical or thermal molecular ion bombardment (HWU, INAF, LUO, OBSParis,UCL).


LASSIE 5 THEMES • Theme 4 - Modelling the Gas-Grain Interaction

• Developing models of amorphous ices and dust grains (LUO, OBSParis, QUB, SU, UGOT).• Calculating IR and UV absorption spectra for water and adsorbates on and in crystalline and amorphous ices (HWU, UGOT).• Understanding the dynamics of photon-driven processes in amorphous ices, including photodesorption and photodissociation (HWU, LUO, OBSParis, UGOT).• Understanding molecular hydrogen and small molecule formation on silicates, carbonaceous, graphite and amorphous ice (AU, LUO, OBSParis, UGOT, QUB).• Understanding the hydrogenation and deuteration reactions of CO in various types of ice, particularly CH3OH formation (LUO, OBSParis, UGOT, QUB, SU).• Calculating diffusion and desorption rates of H atoms, O atoms and simple molecules on amorphous and crystalline ices of various compositions (OBSParis, UGOT).• Modelling coupled grain growth and chemistry under interstellar conditions (MPG).•Simulating the growth and evolution of water ice and other solids under interstellar conditions(LUO).


LASSIE 5 THEMES

• Large and small scale maps of infrared lines of H2 and deuterated species will be constructed to trace H2 formation on grain surfaces under different conditions (AU, OBSParis).

• An inventory of ices in different environments will be assembled using infrared spectroscopy from the Spitzer Space Telescope (INAF, LUO, UCL, SU).

• Constraints on ice formation will be obtained by ice mapping with the AKARI satellite (UCL, SU).

• A line survey of massive- and intermediate- star forming regions with the Submillimeter Array will be conducted in order to search for complex molecules, which may point to formation routes on grain surfaces (MPG, QUB).

•Theme 5 - Observations and Astronomical Models Involving Dust and Ices


LASSIE 5 THEMES

• A determination of the formation and lifecycle of water from gas to solid and back again will be performed by combining infrared spectroscopy of water ice with submillimeter spectroscopy of water gas from the Herschel Space Observatory (LUO, UCL, SU).

• A study of the formation and composition of silicate and carbonaceous grains in disks and envelopes around young and old stars will be undertaken using infrared spectroscopy (MPG, UCL).

• High spatial resolution IR spectroscopy of PDRs in nebulae and around stars will be recorded, looking at how the emission band strengths and relative intensities vary with distance from the exciting source as a diagnostic of PAH formation and excitation mechanisms (OBSParis, UCL).

• Modelling of the gas-grain chemistry in hot cores and disks using the new laboratory data and comparison with observations (UCL, LUO, MPG, OBSParis, QUB, UCL, SU).

•Theme 5 - Observations and Astronomical Models Involving Dust and Ices

The Interstellar Medium is rich in molecules… from the simplest molecule (H2)

to those necessary for the formation of life

Credit: R.Ruiterkamp

2 3 4 5 6 7 8 9 10 11H2 C3 c-C3H C5 C5H C6H CH3C3N CH3C4H CH3C5N? HC9N

AlF C2H l-C3H C4H l-H2C4 CH2CHCN HCOOCH3 CH3CH2CN (CH3)2CO

AlCl C2O C3N C4Si C2H4 CH3C2H CH3COOH (CH3)2O NH2CH2COOH ? 12C2 C2S C3O l-C3H2 CH3CN HC5N C7H CH3CH2OH C6H6

CH CH2 C3S c-C3H2 CH3NC NH2CH3 H2C6 HC7N

CH+ HCN C2H2 CH2CN CH3OH HCOCH3 CH2OHCHO C8H 13+

CN HCOCH2D+ ?

CH4 CH3SH c-C2H4O HC11N

CO HCO+ HCCN HC3N HC3NH+ CH2CHOH PAHs

CO+ HCS+ HCNH+ HC2NC HC2CHO C60 C60 (Science (Science 2010)2010)

CP HOC+ HNCO HCOOH NH2CHO

CSi H2O HNCS H2CHN C5N

HCl H2S HOCO+ H2C2O

KCl HNC H2CO H2NCN

NH HNO H2CN HNC3

NO MgCN H2CS SiH4

NS MgNC H3O+ H2COH+

NaCl N2H+ NH3

OH N2O SiC3

PN NaCNSO OCSSO+ SO2

SiN c-SiC2SiO CO2

SiS NH2

CS H3+

HF SiCNSHFeO AlNCAlNC

>160 Interstellar Molecules>160 Interstellar Molecules

National Radio Astronomy Observatory

Formic Acid

Acetic Acid

Glycolaldehyde

Benzene

Cyanopolyynes

Glycine ?

http://www.cv.nrao.edu/~awootten/allmols.html


What chemistry can occur in such environments ?

• Temperatures are low … (As low as 10K)

• In the ISM the density is extremely low … so probability of collisions is low

• Hence it appears impossible to support chemistry !

But evidence shows there must be complex chemistry !



• At low temperatures there is little or no thermal/kinetic energy

• So chemistry must occur through barrierless• Reactions.

• Or

• Stimulated reactions ( e.g. photon assisted)



Ion-Molecule reactions are a typical example of a reaction that may have no activation barrier.

e.g. NH3+ + H2 NH4

+ + H

Ar+ + H2 ArH+ + H

He+ + H2 He + H+ + H

H2- + H H + H2 + e-

(Note anions as well as cations !)



However neutral – neutral reactions can also occur at low temperatures.

H2O + Cl HCl + O

F + D2 DF + D

Indeed the reaction rate may INCREASE as the temperature falls

It has been suggested that the increasing rate of these reactions as the temperature is lowered is related to the changing distribution of reagents over their rotational

levels as the temperature is lowered.

• Hence State Selective experiments are required


Supersonic crossed beam machine for radical-radical studies. CRESU (Cinétique de Réaction en Ecoulement Supersonique Uniforme)

to study neutral-neutral reactions and energy transfer processes in the

gas phase down to temperatures as low as ~10 K. (Rennes)



But such gas phase experiments can not explain all the chemistry in the ISM

E.g. the formation of H2 …. the most common molecule in the ISM can not be formed in the gas phase

Instead it is formed by reactions on DUST Surfaces !


Chemistry on Dust grains

• Some of these grains are covered with an icy mantle formed by freezing out of atoms/molecules from the gas phase

• Hence we need to explore ice chemistry !

•The ices in the mantle are bombarded with cosmic rays, Ions, solar UV, electrons.•Chemical modification occurs.

To pumping station

Continuous flow cryostat Ion gauge

Cryogen inlet via transfer line

Temperaturecontroller

Sources

E-gun

Synchrotron

Ion Source

Resistive heater

ThermocouplesMgF2/ZnSe

substrate

Copper sample mount

Detectors

- UV-VIS / FTIR detector

- Photomultiplier Tube

Sources- UV-VIS / FTIR

spectrometer- Synchrotron

• HV (UHV) chamber - Portable:– P~10-8 - 10-10 mbar

• Still > a million times higher than ISM!

• Temperature– Continuous flow LHe/LN2

cryostat• 12 K < T < 450 K

• Substrate– CaF2 / MgF2 (VUV) or ZnSe

(IR) window• transmission spectroscopy of

bulk ices

• Samples– deposited in situ by vapour

deposition– 0.1 – 1 m– Thick enough to ignore the

effects of the substrate– Looking at bulk ice reactions

Experiments at Synchrotron Facilities

UK Daresbury Aarhus Denmark

Recent results on astrochemical ice morphology (Theme 1)

• Study electronic state spectroscopy of molecules in the solid phase (photolysis).

• VUV and IR spectroscopy of ice morphology.

• Experiments performed in transmission mode.

VUV Spectrum of water ice <90K

Note : Blue shift in the solid phase

0.0E+00

2.0E-18

4.0E-18

6.0E-18

8.0E-18

1.0E-17

1.2E-17

1.4E-17

1.6E-17

1.8E-17

2.0E-17

6.0 6.5 7.0 7.5 8.0 8.5 9.0 9.5 10.0 10.5

Photon Energy / eV

Cro

ss S

ectio

n

/ cm2

VUV Spectrum of carbon dioxide ice <90K Note : Blue shift in the solid phase

0.0E+00

2.0E-19

4.0E-19

6.0E-19

8.0E-19

1.0E-18

1.2E-18

1.4E-18

6.5 7 7.5 8 8.5 9 9.5 10 10.5

Photon Energy / eV

Cro

ss S

ectio

n / c

m2

Comparison of gas and solid phase Methylamine

Note absence of low lying bands in solid phase

Energy (eV)

5 6 7 8 9 10 11

Cro

ss S

ectio

n (

cm

2 )

0

1e-18

2e-18

3e-18

4e-18

5e-18

6e-18

7e-18

Gas PhaseSolid Phase

Some ‘first’ conclusions

• Can not use gas phase data to predict position of electronic bands in the ice phase.

• Some electronic states are ‘missing’ in solid phase spectra.

• Cross sections ( hence photodissociation rates) change from gas to solid.

SO2 Morphology and temperature

• ‘Fast’ deposition at 25 KNo vibrational structure

Indicates amorphous ice

• Annealed to/deposited at 90 Kvibrational structure &

evidence of Davydov splitting Indicates crystalline ice

• Slow’ deposition at 25 KWeak vibrational structure

evidence of some degree of crystallinity !

SO2

• Conclusions • Rate of deposition is important in

determining ice morphology.

• May form mixed amorphous/crystalline ice.

• Crystallinity is not always a signature oftemperature or thermal history !

Ammonia gas vs solid (25K)

Ammonia Different T

The band at 194 nm is indicative of

‘exciton’ formation

Ammonia ice in the IR

• 1060 cm-1 peak is evidence of crystalline structure.

• 1070 cm-1 peak is due to amorphous ice.

• The 1100 cm-1 peak indicative of exciton measure of grain boudaries

85

90

95

100

10001050110011501200

NH3 dep. 75K

NH3 ann. 75K

Wavenumber (cm-1

)

Tra

nsm

itta

nce

0

1

2

3

140 160 180 200 220

0

1

2

3

140 160 180 200 220

0

1

2

3

140 160 180 200 220

0.00

0.01

0.02

0.03

0.04

1000105011001150

0.00

0.02

0.04

0.06

0.08

1000105011001150

0.00

0.02

0.04

0.06

0.08

0.10

1000105011001150

0.00

0.05

0.10

0.15

0.20

0.25

1000105011001150

Wavenumber / cm-10

1

2

3

140 160 180 200 220

Wavelength / nm

Deposited at 25 K

Annealed to >65 K

Deposited >65 K

Deposited at >90 K

Amorphous: Disordered structure, thermodynamically unstable

Semi/polycrystalline: More ordered structure with crystallite & amorphous mix, thermodynamically stable

Polycrystalline: many small crystallites, large number of grain boundaries, thermodynamically stable

Crystalline: Large crystallites, few grain boundaries, thermodynamically stable

Ammonia

• Both UV and IR show features that are characteristic of exciton formation

• Complex ice morphology formation of regions of crystalline ice in an ‘amorphos sea’

• Crystallites

• Structure is random/statistical. Each sample is different ! Depends on deposition time.

Studies in chemical processing of astrochemical ices

Ices may be processed by UV light or cosmic rays in the ISM

On planetary surfaces interaction with ions from the planetary magnetosphere

e.g. Moons of Jupiter and Saturn


Ion Interactions with Planetary Surfaces

Nature 373, 677 - 679 (1995)

Detection of an oxygen atmosphere on Jupiter's moon EuropaD. T. Hall, D. F. Strobel, P. D. Feldman, M. A. McGrath & H. A. Weaver

EUROPA, the second large satellite out from Jupiter, is roughly the size of Earth's Moon, but unlike the Moon, it has water ice on its surface1. ……..…………. Here we report the detection of atomic oxygen emission from Europa, which we interpret as being produced by the simultaneous dissociation and excitation of atmospheric O2 by

electrons from Jupiter's magnetosphere. Europa's molecular oxygen atmosphere is very tenuous, with a surface pressure about 10-11 that of the Earth's atmosphere at sea level.

Nature 388, 45 - 47 (1997)

Detection of ozone on Saturn's satellites Rhea and Dione K. S. NOLL, T. L. ROUSH, D. P. CRUIKSHANK, R. E. JOHNSON & Y. J. PENDLETON

The satellites Rhea and Dione orbit within the magnetosphere of Saturn, where they are exposed to particle irradiation from trapped ions. A similar situation applies to the galilean moons Europa, Ganymede and Callisto, which reside within Jupiter's radiation belts. All of these satellites have surfaces rich in water ice1, 2……. …………… Here we report the identification of O3 in spectra of the

saturnian satellites Rhea and Dione. The presence of trapped O3 is

thus no longer unique to Ganymede, suggesting that special circumstances may not be required for its production.

Nature 292, 38 - 39 (02 July 1981)

Evidence for sulphur implantation in Europa's UV absorption bandArthur L. Lane, Robert M. Nelson & Dennis L. Matson

The International Ultraviolet Explorer (IUE) spacecraft has obtained observations of the galilean satellites over the past 2 years ……………………… We report here the discovery of an absorption feature at 280 nm in Europa's reflection spectrum. Observations with the IUE show that this absorption is strongest on Europa's trailing hemisphere (central longitude 270°). We identify the feature as an SO2 absorption band and hypothesize that SO2 may

form when energetic jovian magnetospheric sulphur ions are injected into Europa's water-ice surface.


Ion v Photon irradiation

• Photoabsorption of a photon interact with single target (selection rules)

– Dissociation, ionisation, excitation– Secondary electrons

• Penetration depth depends on the optical properties of the material

• Ions interact with many atoms/molecules along the ion tracks

– Dissociation, ionisation, excitation– Dislocations– Primary, secondary… knock-on

particles– Secondary, tertiary… electrons– Sputtering– Implantation (reactive species)

• Penetration depth depends on the ion energy and mass and the stopping power of the ice


Experiments performed at ECRIS QUB

• 9.0 – 10.5 GHz Electron Cyclotron Resonance Ion Source at QUB


Results: FTIR Spectroscopy

13CO2

dOH

Redshift and broadening of the H2O O-H stretching band


Proton irradiation of H2O:CO2

H2O

H2O

H2CO3

H2CO3

H2CO3

CO

CO3

CO2

H2O

H2O

H2CO3

H2CO3

H2CO3

CO

CO2

No CO3

100 keV H+

5 keV H+

Stability and Reactivity of Ozone in Astrochemical Ices

Bio-signaturesMolecules that can be used to detect life elsewhere – exoplanets

>> Ozone (O3)

>> Nitrous oxide (N2O)

These molecules are selected from the planet that already supports organic life form… EARTH !.

Why Ozone?

• Essential component of any atmosphere capable of sustaining life

• Strong evidence that the planet can support life - if not the existence of life itself

• Identified in planetary, satellites surfaces. Ozone chemistry is possible in these ices.

• DARWIN mission --- Biomarker?

Ozone from oxides of nitrogen

• Ozone produced from the irradiation of solid oxides of nitrogen, like N2O and NO2.

Dissociation pathwayN2O N2 + O (1D or 3P) NO2 NO + O Formation pathway O + O O2

O + O2 O3

e- irradiation of N2O

0 15 30 45 60 75 900.00E+000

1.00E+015

2.00E+015

3.00E+015

4.00E+015

5.00E+015

6.00E+015

7.00E+015

Co

lum

n d

en

sity

, cm

-2

Time, min

O3

>> Steady ozone growth

>> No dissociation or reduction

>> Less dose -- less NxOy molecules

Will there be any change with the higher dose irradiation?

Presence of N2O5 in N2O ice

1950 1900 1850 1800 1750 1700 1650 1600 1550

0.0000

0.0025

0.0050

0.0075

0.0100

0.0125

0.0150

0.0175

0.0200

0.0225

?

**

N2O

3 [NO2 ]

2

c - N2O

2

t - N2O

2

N2O

5

N2O

NO2

Ab

sorb

an

ce

Wavenumber, cm-1

How are the other new molecules produced?

Reactions for N2O ice

N2O+ O(1D) (NO)2

NO + O NO2

2NO2 + O3 N2O5 + O2

Will it be the same for an NO2 ice?

Conclusion

• Ozone is highly stable in a pure oxygen ice.

• No reaction or significant amount of dissociation in a CO2 ice.

• But in the presence of oxides of nitrogen, ozone that is produced reacts with NxOy molecules.

Implications

• Ozone that is produced by the action of energetic particles in astrochemical ices take part in reactions as observed in the Earth’s stratosphere.

• Therefore ozone not only acts as a biomarker but also an active reactant in the icy surfaces similar to Earth’s troposphere/stratosphere.

Questions for Astrochemistry

• Spectral analysis of ices is a useful tool for identifying ice morphology both in the IR and UV. So need more spectroscopic studies of ices under ISM conditions

• Experimentally it is vital that different experiments are calibrated against one another such that the morphology of the ices used are compatible.


• We need a data base of astro-ice spectra to be assembled similar to the large database of gas phase photo-absorption cross sections assembled by the atmospheric community.

• Different temperatures, deposition times and for different substrates


• The mimic of ‘realistic’ astrochemical conditions within the laboratory environment must be addressed.

• Time scales – is our slow deposition still too fast ?

So…….• Can we model ice growth in the ISM ?• Look at statistical pattern (e.g. run model many

times to provide ‘average’ of ice morphologies)


• Chemical reactions and their rates

depends on surface morphology

• Parameters such as ion charge state,

incident energy and secondary electron

production are equally important


• To date have used large bulk ice samples whereas in the ISM dust grains only a few microns in size.

• How is the physics and chemistry influenced by the surface area to volume ratio?

Dust grain chemistry

• Build an ultrasonic trap

• Within which we can suspend ice covered dust particles

• Study spectral characteristics and coalescence properties

Ultrasonic dust trap

Transducer

Thermocouple

Gas dosing

Reflector

Vacuum

Cold inner chamber

He atmosphere Transducer

Thermocouple

Gas dosing

Reflector

Vacuum

Cold inner chamber

He atmosphere

Study of Ice morphology in ultrasonic trap

• Studies of ice morphology and grain accretion

– Use of ultrasonic trap for IR spectra of ice/dust surfaces

Transducer

Reflector

Soot + ice

Smaller particles revolving around and sticking to larger soot + ice disc

“Sticky Ice Grains Aid Planet Formation: Unusual Properties Of Cryogenic Water Ice”, H. Wang et al, The Astrophysical Journal, 620:1027-1032, (2005)

Soot and ice agglomerates formed and suspended in an ultrasound field

• Grain sticking planitesimal building planet formation

IR spectra of volcanic ash

Absorbance of low silicate percentage volcanic ash (approx 50%)

0

0.05

0.1

0.15

0.2

0.25

0.3

0.35

0.4

7.0E+02 1.7E+03 2.7E+03 3.7E+03 4.7E+03 5.7E+03 6.7E+03

wavenumber

Ab

sorb

ance

<32

<32

32-45

45-63

63-90

IR spectrum of water ice particles in trap see change from crystal to amorphous on particle surface

H2O spectrum - Temperature Profile

0.00

0.05

0.10

0.15

0.20

0.25

0.30

0.35

0.40

2600280030003200340036003800

Wavenumber (cm-1)

Abso

rban

ce

90K150K200KSoot+ice approx200 K

Other linked EU programmes

• ESF COST Action CM0805 The Chemical Cosmos

www.cost.esf.org

European Cooperation in the field of Scientific and Technical Research

COST is supported by the EU RTD Framework Programme

ESF provides the COST Office through an EC contract

The Chemical Cosmos: Understanding Chemistry in Astronomical Environments

CM0805Start date: 17/04/2009End date: 16/04/2013

Nigel J Mason Chair The Open University / UK [email protected]

Beverley Bishop Administrator The Open University [email protected]

mailto:[email protected]

www.cost.esf.org

European Cooperation in the field of Scientific and Technical Research



22 countries:Austria

BelgiumCzech Republic

Denmark FinlandFrance

GermanyHungary

IcelandIreland

Italy Latvia

NetherlandsPoland

PortugalSerbia

SlovakiaSpain

Sweden United Kingdom

22 COST countries

Malta /Norway --- IntentionSLOVENIA ASKS to join

Chemical Cosmos-Partners



Scientific context and objectives

• The main objective of this Action is to study chemical processes relevant to the physical conditions encountered in the interstellar medium, and on the surface and in the atmospheres of planetary bodies.

• The Action aims to provide new insights into the dynamics of the chemical reactions leading to molecular synthesis under such conditions and reveal how these are influenced by the ambient temperature and pressure.

• Special attention will also be given to the study of the novel surface chemistry prevalent on interstellar medium dust grains and planetary surfaces.

• The Action also aims to combine such laboratory data with complementary chemical models to allow a fuller interpretation of observational data.



Organised in 3 Working groups

• Working group 1; Radical- and Ion-induced reactions in the interstellar medium (Gas phase chemistry) Wolf Geppert Stockholm

• Working group 2;. Heterogeneous and ice chemistry (Surface chemistry) Maria Palumbo Catania

• Working group 3;. Chemistry of planetary atmospheres (Models and observations ) exoplanets Christian Muller Brussels



VAMDC

• A database of Atomic and molecular data for applications including astronomy.

• Http://www.vamdc.org/

VAMDC - Brussels - Nov 08

KEY VAMDC OUTCOMES

Develop or/and extend standards for interoperability of AM resources

Implementation of 17 selected databases Compatibility with existing extraction tools

Create a safe environment where latest AM data can be easily published (even small sets)

Linking producers and users

KEY BENEFITS

Uniform access, i.e. saving time with format of data, tools development

Increase level of scientific analysis of ground/space missions or experiments good standardisation

implies Documentation allows cross-matching

of different sets of AM data

allows wide access to the latest published AM data

Europlanet

Framework VII Research Infrastructure

http://www.europlanet-ri.eu/

6 million Euros 4 years from 01/01/2009

27 partners (plus other CNRS partners !)

Coordinator M Blanc (CNRS) Toulouse


Provides access to facilities across EU

Including analytical (isotope facilities)

-- including those that did star dust analysis.

and

• The IDIS database


Also comprises of:

• Scientific workshops and Exchanges

•Outreach (Public engagement – Media service)

•European Planetary Science Congress (EPSC)


So finally…..

• Eurogenesis is welcome new programme in astronomy/astochemistry

• Explore links and collaborations

• [email protected]

lassie: a marie curie training network on astrochemistry nigel mason centre for earth, planetary,...

Documents

grain aggregate formation

icy grain mantle

graingrain collisions

formation of grains

model dust grain surfaces

model grain surfaces

formation of simple

ice formation