The PCMI directory 2013-2018
Information gathered by the PCMI science council Jer´ omeˆ Pety (IRAM, Grenoble & Obs. de Paris), Karine Demyk (IRAP, Toulouse), Jean-Hugues Fillion (LERMA, Paris) Arnaud Belloche (MPIfR, Bonn), Olivier Berne´ (IRAP, Toulouse) Ludovic Biennier (IPR, Rennes), Gregoire´ Danger (PIIM, Marseille), Alexandre Faure (IPAG, Grenoble), Fred´ eric´ Galliano (AIM-CEA, Paris) Pierre Gratier (LAB, Bordeaux), Jean-Claude Guillemin (ISCR, Rennes) Annie Hughes (IRAP, Toulouse), Eric Josselin (IRAP, Toulouse) Rosine Lallement (GEPI, Paris), Franc¸ois Levrier´ (LERMA, Paris) Franc¸ois Lique (LOMC, Le Havre), Laurent Margules,` (PhLAM, Lille) Dahbia Talbi (LUPM, Montpellier), Patrice Theule´ (PIIM, Marseille) Nathalie Ysard (IAS, Paris)
http://pcmi.cnrs.fr
16 June 2019 Version 1.0
1 Abstract This document gathers short descriptions of research teams and projects from the PCMI commu- nity. Its goals is to give a panorama of the community activities and skills, as of end of 2018. It completes the document “Physics and Chemistry of the Interstellar Medium: Review 2013-2018 & Prospective 2019-2024” available available at http://pcmi.cnrs.fr/IMG/pdf/pcmi-prospect-2019-2024.pdf, which highlights the main science strengths and the emerging activities of the PCMI community. Project and team forms were filled by the community following several calls via the pcmi newsletter. Each forms in- cludes the list of permanent members and technical staff, post-docs and PhD students, key research facilities and infrastructure, collaborations and provides the astrophysical context, goal and recent (< 5 years) highlighted work. The current state of these forms are gathered in the document and will be transformed as an online directory on the PCMI web site.
Contents
1 Teams 4 1.1 Astrophysics ...... 4 1.1.1 AMOR: Astrochimie Moleculaire´ et ORigine des systemes` planetaires,´ LAB . .5 1.1.2 Galactic Star Formation and ArTeMiS,´ AIM ...... 8 1.1.3 Jets et chocs, LERMA ...... 10 1.1.4 Star Formation, LAB ...... 13 1.1.5 ISM, LERMA ...... 16 1.1.6 NUAGES: earby Universe Agents of Galaxy Evolution Studies, AIM ...... 18 1.1.7 UV spectroscopy of interstellar and circumstellar matter, LAM ...... 21 1.2 Laboratory ...... 23 1.2.1 CMB: Cross Molecular Beams, ISM ...... 24 1.2.2 CRESU, ISM ...... 27 1.2.3 CORINT: Chimie Organique aux INTerfaces, IPR ...... 28 1.2.4 DESIRS beamline, SOLEIL ...... 30 1.2.5 ESPOIRS, IRAP ...... 34 1.2.6 Laboratory Astrophysics, IPR ...... 36 1.2.7 MASIR: ???, MONERIS ...... 38 1.2.8 Matrix team, ISM ...... 40 1.2.9 Astro, PIIM ...... 42 1.2.10 Reactivity on cold surfaces, RCS ...... 45 1.2.11 Spectroscopy for Radio Astronomy, IRAP ...... 47 1.2.12 Spectro Lille, PhLAM ...... 49 1.2.13 SPICES: Spins, Photons & ICES, LERMA ...... 51 1.2.14 SYSTEMAE-VUV, ISMO ...... 54 1.3 Theory ...... 57 1.3.1 Chimie theorique,´ MSME ...... 58 1.3.2 Structure and Reactivity in astrophysics ...... 63 1.3.3 Space Chemistries: from the ISM to the planet Earth, LCT ...... 65 1.3.4 Reactive processes, LOMC ...... 68 1.3.5 Theoretical Astrochemistry, LUPM ...... 70 1.3.6 PCMT, PhLAM ...... 72 1.3.7 Theory and simulations, LERMA ...... 75
2 2 Projects 77 2.1 3DICE: 3D Interstellar Chemo-physical Evolution ...... 78 2.2 ASAI: Astrochemical Surveys At IRAM ...... 80 2.3 BxB: Interstellar B-fields crossing inflation B-modes ...... 82 2.4 CADE: Centre d’Analyse de Donnees´ Etendues ...... 84 2.5 COCOON ...... 86 2.6 COMs: Complex Organic Molecules ...... 88 2.7 Formation des molecules´ organiques complexes dans le milieu interstellaire froid . . . . 90 2.8 COSMIDYN ...... 92 2.9 DustDist ...... 95 2.10 GALETTE: GALactic EnvironmenT in Three dimEnsions ...... 97 2.11 GCC: Galactic Cold Cores ...... 98 2.12 GENESIS: GENeration and Evolution of Structures in the ISm ...... 100 2.13 High-mass star formation and the origin of the IMF ...... 102 2.14 HYDRIDES ...... 106 2.15 Injection of stellar matter into the ISM ...... 108 2.16 KIDA, KInetic Database for Astrochemistry ...... 110 2.17 MIST: Molecules, Magnetic Fields, and Intermittency in Cosmic Turbulence ...... 111 2.18 Molecular complexity in high-mass protostars ...... 114 2.19 Nanocosmos ...... 117 2.20 ORION-B: Outstanding Radio-Imaging of OrioN-B ...... 119 2.21 ORISTARS ...... 121 2.22 PARCS ...... 123 2.23 PHANGS ...... 125 2.24 PILOT ...... 127 2.25 Radiative feedback from massive stars ...... 129 2.26 SICAL: Simulation d’Irradiation de Carbones Astrophysiques en Laboratoire ...... 131 2.27 THEMIS: The Heterogeneous dust Evolution Model for Interstellar Solids ...... 135 2.28 TRON: Tracing the Reservoirs Of Nitrogen ...... 137 2.29 VAMDC: Virtual Atomic and Molecular Data Center ...... 139
3 1 Teams
1.1 Astrophysics
4 Research Group: Astrochimie Moléculaire et ORigine des systèmes planétaires
Permanent staff: Edwige Chapillon (AA), Emmanuel Di Folco (AA), Anne Dutrey (DR1), Stéphane Guilloteau (DRCE2), Pierre Gratier (AA), Valentine Wakelam (DR2).
Technical staff: no PhD students (since 2010): Yann Boehler (2008/2011), Laura Reboussin (2012-2015), Maxime Ruaud (2013/2016), Jessica Pericaud (2013/2016), Sacha Gavino (2017). Thi Phuong Nguyen (2016/-) Post-docs (since 2010): Wasim Iqbal (2015/-) The PHD students and postdocs payed by the 3DICE ERC (PI V. Wakelam) are not mentioned here. See the 3DICE project sheet. Contact: [email protected]
Laboratory: Laboratoire d’Astrophysique de Bordeaux, UMR5804 Institution(s): UBX1 Website: http://astrophy.u-bordeaux.fr/
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: We are intensive users of the IRAM instruments (NOEMA, 30-m radiotelescope) and ALMA. We also develop tools in radiative transfer dedicated to molecular and dust disks (Diskfit) and in astro-chemistry (Nautilus).
Keywords: Interstellar medium, diffuse and molecular clouds, denses cores, protoplanetary disks, mo- lecular gas, dust evolution.
Astrophysical context and goals: Our team is composed of astro-chemists (around Nautilus (gas grain chemical code), KIDA (Kinetic Database for Astrochemistry) and ISA (Interstellar Abundances Database)), experts in interferometry (NOEMA, ALMA), imaging technics (Gildas) and astrostatistic, observers in mm/submm and in optical/NIR, and modelers (radiative transfer in disks) working on star formation. We are working on the various phases of the low-mass stellar formation, from cold clouds and pre-stellar dense cores to gas and dust disks found around low-mass young stars. We study both protostars environment (Class 0 & I) and pre-main sequence protoplanetary disks (Class II) and the final phase of disk dissipation (class III, debris disks). The ERC Starting Grant ERC 3DICE (obtained by Valentine Wakelam in 2013) is more focused on how the chemistry evolves from diffuse clouds of the interstellar medium to dense molecular clouds. We are regular users of the IRAM instruments (the 30-m radiotelescope and the interferometer NOEMA). We also use the interferometer ALMA (Atacama Large Millimetre Array). We are also deeply involved in the software GILDAS, a radioastronomy tool dedicated to the reduction and analysis of mm/submm data and implemented on many radiotelescopes. We are also regular users of the ESO NIR/optical instruments such as the VLT/I.
Collaborations: CID: Chemistry In Disks, an international collaboration with IRAM (V.Piétu, E.Chapillon, F.Gueth), the MPIA (Th.Henning, D.Semenov) and U.Gorty from Nasa-Ames (USA). Collaboration with Y-W.Tang and Paul Ho from ASIAA (Taipei, Taiwan) on the dynamics and physics of disks surrounding young low-mass multiple stars and Herbig Ae stars (https://www.asiaa.sinica.edu.tw/people/cv.php?i=ywtang). Collaboration with S.Wolf on dust disk properties and modeling (https://www.astrophysik.uni-kiel.de/en/staff/prof-dr-sebastian-wolf) Collaboration around several JWST projects dedicated to disks. We have recently (2016) started to collaborate with E.Pantin (CEA), E.Habard (IAS), A.Gusdorf (Obs. Paris) and T.Beck (STcSI, Baltimore, USA) in order to prepare JWST proposals. Collaboration with the OrionB Iram Large Program group Collaboration avec nos collègues de l’ISM à l’université de Bordeaux (Th.stoecklin, A.Bergeat, J.C.Loison).
Highlight: In between 2014 and 2018, we had several press-articles and press-releases, most of them were associated to ALMA results. First detailed image of the accreted CO gas inside the tidally truncated GG Tau A cavity. GG Tau A is a triple Tauri star: http://www.eso.org/public/france/news/eso1434/ Mesuring the dust temperature in the mid-plane of the TTauri disk around the Flying Saucer: https://www.eso.org/public/france/news/eso1604/ First image of the (CO) gas spirals inside the cavity of a forming-planet disk, orbiting around AB Auriga: http://www.insu.cnrs.fr/node/6702
Figure 1: AB Auriga observed with ALMA at 0.03” or 7 au. Red : Dust emission at 1. 3mm, Blue : integrated area of the CO J=2-1 emission. The CO spiral may be due to one or two planets. From Tang et al 2017.
Most significant publications (<5): New rate coefficients of CS in collision with para- and ortho-H2 and astrophysical implications, Denis-Alpizar et al 2018, MNRAS, 1112 The Flying Saucer: Tomography of the thermal and density gas structure of an edge-on protoplanetary disk, Dutrey et al 2017, AA, 607 Planet Formation in AB Aurigae: Imaging of the Inner Gaseous Spirals Observed inside the Dust Cavity, Tang et al 2017, ApJ, 840 The shadow of the Flying Saucer: A very low temperature for large dust grains, Guilloteau et al 2016, A&A, 586,L Dissecting the molecular structure of the Orion B cloud: insight from principal component analysis, Gratier et al 2017, A&A, 599, p. A100.
Link to full publication list: http://astrophy.u-bordeaux.fr/amor-astrochimie-moleculaire-et-origine-des-systemes- planetaires/ Press releases: voir plus haut Research Group: Galactic Star Formation and ArTéMiS
Permanent staff: Ph. André, A. Menshchikov, V. Revéret, A. Maury, F. Motte (until 2015) Technical staff: L. Rodriguez, M. Talvard, J. Le Pennec PhD students (since 2010): D. Arzoumanian, P. Palmeirim, B. Ladjelate, M. Gaudel, H. Ajeddig Post-docs (since 2010): V. Könyves, A. Roy, E. Ntormousi, A. Bracco, Y. Shimajiri, F. Schuller Contact: Philippe André ([email protected])
Laboratory: AIM (Lab. Astrophysique-Instrumentation-Modélisation de Paris Saclay) – UMR 7158 Institution(s): CEA, CNRS, Université Paris-Saclay, Université Paris-Diderot, Sorbonne Paris-Cité
Key Research Facilities, Infrastructure and Equipment: Herschel (SPIRE/PACS), ArTéMiS camera at APEX (developed and provided by the group), IRAM instruments, ALMA
Keywords: observations: submillimeter – Herschel and SPICA space missions – interstellar medium: structure – stars: formation – filaments – prestellar cores – protostars – magnetic fields
Astrophysical context and goals: Observational study of the link between the structure of the cold interstellar medium and the star formation process, in an effort to understand the global star formation efficiency in molecular clouds, the origin of the stellar initial mass function, the initial conditions and early stages of individual star/solar systems.
Collaborations: • LAM Marseille: A. Zavagno, D. Russeil • LAB Bordeaux: S. Bontemps • IAP Paris: H. Roussel • Cardiff Univ.: N. Peretto • UCLAN Preston: D. Ward-Thompson • Herschel Gould Belt Survey (HGBS) key project (http://gouldbelt-herschel.cea.fr) • CALYPSO IRAM PdBI large program (http://irfu.cea.fr/Projets/Calypso/Welcome.html) • ORISTARS (ERC AdG 2012-2018 – PI: André) • STARFICH (ANR 2012-2016 between AIM & LAB – PI: André AIM; co-I: Bontemps LAB) • SPICA consortium (pre-selected ESA M5 mission) – science/technical case for SPICA-POL
Highlight: Characterization of the filamentary structure in the massive star-forming complex NGC6334 with ArTéMiS. (Press Release: www.eso.org/public/ news/eso1341/) A discovery of our group as part of the Herschel N Gould Belt survey has been the finding that nearby molecular E filaments share a common inner width of about 0.1 pc (Arzoumanian+2011, 2019). This is at variance with the classical view that scale-free isothermal supersonic turbulence shapes the cold ISM and at the root of a proposed filamentary paradigm for star formation (André+2014). Using the new ArTéMiS submm camera developed by our group for APEX (open to the ESO and OSO communities since 2014) and providing a factor of ~3.5 higher resolution than Herschel at 350/450 µm, we could resolve the main filament in the high-mass star-forming region NGC6334 at d ~1.7 kpc and measured a width of 0.15 ± 0.05 pc all along the filament crest (André+2016). This result suggests that the 0.1 pc filamentary paradigm is not restricted to the Gould Belt and may well extend to the massive GMCs of the Galactic Plane.
Most significant publications (<5):
• From Filamentary Networks to Dense Cores in Molecular Clouds: Toward a New Paradigm for Star Formation, André, Ph., Di Francesco, J., Ward-Thompson et al. 2014, Protostars and Planets VI, p. 27-51 DOI: 10.2458/azu_uapress_9780816531240-ch002
• Characterizing filaments in regions of high-mass star formation: High-resolution submillimeter imaging of the massive star-forming complex NGC 6334 with ArTéMiS, André, Ph., Revéret, V., Könyves, V. et al. 2016, A&A, DOI: 10.1051/0004-6361/201628378
• Testing the universality of the star-formation efficiency in dense molecular gas, Shimajiri, Y., André, Ph., Braine, J. et al. 2017, A&A, DOI: 10.1051/0004-6361/201730633
• Characterizing the properties of nearby molecular filaments observed with Herschel, Arzoumanian, D., André, Ph., Könyves, V. et al. 2019, A&A, DOI: 10.1051/0004- 6361/201832725 • Characterizing young protostellar disks with the CALYPSO IRAM-PdBI survey: large Class 0 disks are rare, Maury, A., André, Ph., Testi, L. et al. 2019, A&A, DOI: 10.1051/0004-6361/201833537 Research Group: Jets et Chocs (LERMA)
Permanent staff (alphabetical order): Sylvie Cabrit, Maryvonne Gerin, Benjamin Godard, Antoine Gusdorf, Thibaut Lebertre, Pierre Lesaffre, Guillaume Pineau des Forêts (emeritus), A. Ciardi Technical staff: David Languignon PhD students (since 2010): Le Ngoc Tram (2015-2018), Benoit Tabone (2015-2018), Pierre Dell’Ova (2018-) Post-docs (since 2010): Antoine Gusdorf (2012-2016) Contact: [email protected], [email protected]
Laboratory: LERMA (Laboratoire d’Etudes de la Radiation et de la Matière en Astrophysique et Atmosphères), UMR 8112 Institution(s): Observatoire de Paris, Ecole Normale Supérieure, Sorbonne Université, PSL, CNRS Website: http://ism.obspm.fr/
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: We are extensive users of the top observing facilities in the submm and infrared ranges: the ground-based telescopes ALMA, PdBI-NOEMA, APEX ; the satellites Herschel and Spitzer, the stratospheric observatory SOFIA; We use our own MHD 1D shock code (originally developed by D. Flower & G. Pineau des Forêts), in which we include a wealth of thermo-chemical processes and develop several new applications (irradiated shocks, MHD disk winds, AGB envelopes) ; in the frame of our « tâches de service » we developed a public version and analysis tools accessible on the « Platform MIS & Jets ».
Keywords: shock waves, star formation, jets, outflows, AGB winds, supernova remnants, molecular clouds, stellar feedback
Astrophysical context and goals: Notre équipe étudie les jets et chocs moléculaires dans le milieu interstellaire (MIS), dans l’objectif de clarifier leur rôle (majeur) dans la formation stellaire, le cycle du MIS, et l’accélération des rayons cosmiques. Nos études se déclinent suivant différentes échelles: Nous nous intéressons à l’accélération des jets moléculaires magnétisés dans les protoétoiles, aux chocs associés aux flots bipolaires résultants, aux ejecta d’étoiles évoluées AGB, et à plus grande échelle aux chocs dans les restes de supernovae et les flots convergents et à la formation stellaire induite. Notre approche commune consiste à développer des outils numériques originaux où la magnéto/hydrodynamique du gaz est couplée avec une thermo-chimie détaillée hors équilibre; à calculer les signatures spectrales prédites pour divers modèles dans un large spectre d'espèces (H2, CO, H2O, SiO, C, C+, O, OH...), et à les comparer aux nouvelles observations multi-longueur d'onde de pointe en provenance des grands telescopes submm/infrarouges au sol (ALMA, NOEMA, IRAM-30m, APEX), dans la stratosphère (SOFIA), et dans l’espace (Herschel, Spitzer, et bientôt JWST...). Un effort particulier au cours de la période 2014-2018 a été consacré à l’exploitation des premières observations de jets protostellaires avec ALMA et SOFIA, à l’effet du rayonnement UV et X sur la thermo-chimie du choc, et aux prédictions de raies pour le JWST.
Experimental studies of the group: None
Collaborations: IPAG Grenoble: C. Dougados, J. Ferreira, B. Lefloch IRAM Grenoble: J. Pety, F. Gueth, C. Lefèvre Lyon: B. Commerçon (ENS) Vietnam: P. T. Nhung (USTH) Allemagne: R. Güsten, D. Riquelme (MPI Bonn) Espagne: J. Cernicharo and his team, A. Fuente (OAS) Italie: C. Codella, L. Podio, and their team (INAF) Mexique: A. Raga (UNAM) Chili: F. Louvet, D. Mardones, G. Garay (UMI-FCA), W. Dent (ALMA) USA: D. Neufeld (Johns Hopkins University), H. Arce (Yale)
Highlight: The study of the Cepheus E protostellar outflow. Back in 2012, we started a study of Cepheus E based on observations with SOFIA-GREAT. In this outflow driven by an intermediate-mass protostar, our velocity resolved spectra (Gomez-Ruiz, Gusdorf et al. 2012) showed features at low-, intermediate- and high-velocity (between 0 and 50, 50 and 100, and 100 and 140 km/s, see associated figure). In a second article (Lefloch, Gusdorf et al. 2015), we used PdBI data (see figure), and a wealth of CO spectra from single-dish telescopes (IRAM-30m, JCMT, Herschel, SOFIA) to interpret these first spectra, and show their association with the spatial structure of the outflow. In particular, our observations revealed the various shock structures (jet, bipolar cavity, and terminal bowshocks). We inferred the physical conditions in these components and showed that they were consistent with models of jet-driven outflows. We also interpreted the CO observations with non-stationary models of shocks of age consistent with the dynamical age of the source. In a third publication (Gusdorf et al. 2017), we 3 3 observed the emission of the OI P1 - P2 line at 63 µm with the SOFIA telescope, and showed that it was not compatible with our models of the jet component. We have obtained additional time to map the 2 2 emission from this line (and that of the CII P3/2 - P1/2 line at 158 µm) with SOFIA, and the observations are scheduled before the 15th of December, 2018 (our PhD student Pierre Dell’Ova will take this opportunity to fly on SOFIA). These observations will be combined with multiple-line observations of SO and SiO to better characterize the shock chemistry. On the modelling side, we are confident we will be able to use this source to benchmark the new models of self-irradiated shocks that are being developed in LERMA.
Figure. Observations of the Cepheus E protostellar outflow. Left: CO spectra (Jup = 1, 2, 3, 4, 5, 9, 12, 13, 14, 16) at BII position taken with the SOFIA, Herschel, JCMT and IRAM-30m telescopes. Right, top: CO (2-1) maps obtained with the PdBI telescope, revealing the association of the low-, intermediate-, and high-velocity gas with the outflow cavity, terminal shocks (HH 377), and jet. The BII and driving protostar’s positions are indicated by a red square and star. Right, bottom: the SOFIA OI spectrum at BII position, overlaid with the 2 spectra of the CO (16-15) and ∏1/2 3/2-1/2 OH (undetected). Most significant publications (<5): Nascent bipolar outflows associated with the first hydrostatic core candidates Barnard 1bN and 1bS, Gerin, M.; Pety, J.; Fuente, A.; Cernicharo, J.; Commerçon, B.; Marcelino, N., 2015 A&A 577, L2 2015A&A...577L...2G
ALMA discovery of a rotating SO/SO2 flow in HH212. A possible MHD disk wind? Ta bone, B.; Cabrit, S.; Bianchi, E.; Ferreira, J.; Pineau des Forêts, G.; Codella, C.; Gusdorf, A.; Gueth, F.; Podio, L.; Chapillon, E. 2017A&A...607L...6T Nature of shocks revealed by SOFIA [OI] observations in the Cep E protostellar outflow: A. Gusdorf, S. Anderl, B. Lefloch, et al. 2017, A&A 602, A8 2017A&A...602A...8G H2 emission from non-stationary magnetized bowshocks, T. Le Ngoc, P. Lesaffre, S. Cabrit, P. T. Nhung 2018MNRAS.473.1472T Models of irradiated molecular shocks : B. Godard, G. Pineau des Forêts, P. Lesaffre, A. Lehmann, A. Gusdorf, and E. Falgarone, 2018, A&A in press
Link to full publication list: 68 refereed papers between Jan 2014 and Sept 2018 (26 from Jan 2014-Sept 2015, 11 from Sept 2015-Sept 2016, 14 from Sept 2016-Sept 2017, 17 from Sept 2017-Sept 2018).
Press releases:
Les astronomes témoins d’une étape critique de la formation des étoiles
INSU : http://www.insu.cnrs.fr/node/5306
OBSPM : https://www.obspm.fr/lesastronomestemoinsdune.html Research Group: Star Formation group at LAB
Permanent staff: N. Brouillet, T. Csengeri, A. Baudry (Emerite), J. Braine, S. Bontemps, D. Despois, F. Herpin, T. Jacq. Technical staff: - PhD students (since 2010): Clément Druard (2010-2014); Sarah Fechtenbaum (2012-2015); Alizée Duthu (2013-2016); Jordan Molet (2016-); Lars Bonne (2017-). Post-docs (since 2010): A. Duarte-Cabral (2010-2012); Tzu-Cheng Peng (2011-2013); N. Schneider (2012-2015); A. Roy (2017-) Contact: Sylvain Bontemps, [email protected]
Laboratory: LAB (Laboratoire d’Astrophysique de Bordeaux) / UMR5804 Institution(s): CNRS and Universite de Bordeaux Website: http://astrophy.u-bordeaux.fr
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools:
Keywords: Star formation; High-mass Star Formation; Complex Organic Molecules; Structure of ISM; ISM in nearby galaxies; Astrochemistry; Evolved Stars; Magnetic field in evolved stars
Astrophysical context and goals: We study the earliest phases of high-mass star formation as well as the associated early chemical evolution with some emphasis on searching for rare complex organic molecules in these high-mass star precursors (mostly with ALMA and IRAM data). We also observationally approached the formation of dense structures (filaments, cores, clumps) leading to the formation of stars in nearby clouds (Herschel maps) but also in the inner galaxy (ATLASGAL and ALMA). Some aspects of these studies extend up to external galaxies in the local group where the effects of metallicity and of different physical conditions can be tested on (high-mass) star formation processes. We recently searched for low velocity shocks associated with filament formation with APEX and SOFIA and in preparation to SPICA. We have investigated the magnetic field in the extended atmospheres and envelopes of selected evolved stars using ALMA, APEX and the IRAM 30m. Also multi-transition water maser observations supported by new model predictions, enabled us to probe the physical conditions and kinematics of evolved stars.
Experimental studies of the group: None
Collaborations: Large programme ALMA ALMA-IMF (PI Motte, IPAG): IPAG, NRAO (US), National Astronomical Observatory of Japan, NAOJ Chile Observatory, Calan Observatory (Chile). SPARKS (ALMA programme; PI Csengeri): MPIfR Bonn, MPI Heidelberg. Complex Organic Molecules (PI Brouillet): Madrid, MPIfR Bonn. GENESIS (ANR France-Allemagne; PI Bontemps): Cologne University; INRIA Bordeaux; IPAG; LERMA; CASS San Diego (US); ITA/ZHA Heidelberg; ATN Canberra (Australia). SPICA consortium (ESA M5 selected mission in phase A): SRON Groningen (Pays-Bas); Japan; Italy; IRAP; CEA/AIM; … WISH, Herschel large programme (PI van Dishoeck): SRON Groningen (Pays-Bas), MPIfR-Bonn, Leiden University (Pays-Bas), Torun and Poznan University (Poland). HOBYS, Herschel large programme (PI Motte, Zavagno, Bontemps): CEA Saclay, IPAG, LAM, IFSI Rome (Italy), Cardiff (UK), Calgary University (Canada). M33@IRAM, large programme IRAM (PI Braine & Schuster): Arcetri (Italy), IRAM Grenoble, Alberta (Canada), Nanjing (Purple Mountain Observatory, China). Etoiles évoluées: IRAM, MPIfR-Bonn, Univ. of Manchester (UK), ESO (Garching by Munchen, Allemagne), Onsala Space Observatory
Highlight: High-mass stars form from supersonic motions. Thanks to the heterodyne instrument (HIFI) on Herschel and from unambiguous water line absorption features, our group has clearly demonstrated that the dense gas associated with the most massive, young clump of the Galaxy, W43-MM1, is highly dynamical and supersonic (collapse speed as large as ~3 km/s at 0.1 pc scale) (Jacq et al. 2016; Herpin et al. 2012). In parallel our group showed that this supersonic collapse originates from (relatively) large scale collapses (Duarte-Cabral et al. 2013; Csengeri et al. 2017; see also the Science letter of the LAB; April 2017; http://astrophy.u-bordeaux.fr/les-etoiles-massives-sont-la-consequence-deffondrements-a-grande-echel le/). These larger scale collapses would correspond to larger Jeans masses (lower average density) than is needed for low-mass star formation. We are therefore close to solve the long standing issue of the origin of the highest stellar masses and it is in the physics of the ISM that it has now to be hunt for to explain how, why and where such larger scale collapses can be initiated.
Most significant publications (<5):
Antifreeze in the hot core of Orion - Detection of ethylene glycol in Orion-KL, N. Brouillet, D. Despois, X.H. Lu, A. Baudry, et al. 2015, A&A, 576, 129. First detection of a THz water maser in NGC 7538-IRS1 with SOFIA and new 22 GHz e-MERLIN maps, F. Herpin, A. Baudry, A. Richards, et al. 2017, A&A, 606, 52. Properties and rotation of molecular clouds in M 33, J. Braine, E. Rosolowsky, P. Gratier, et al. 2018, A&A, 612, 51 Structure and kinematics of the clouds surrounding the Galactic mini-starburst W43 MM1, T. Jacq, J. Braine, F. Herpin, et al., 2016, A&A, 595, 66 The search for high-mass protostars with ALMA revealed up to kilo-parsec scales (SPARKS): I. Indication for a centrifugal barrier in the environment of a single high-mass envelope, T. Csengeri, S. Bontemps, F. Wyrowski, et al. 2018, A&A, arXiv:1804.06482
Link to full publication list: http://astrophy.u-bordeaux.fr/formation-stellaire/
Press releases: - « La tête de cheval vue par Herschel et Hubble », news INSU, 22 avril 2013 (http://www.insu.cnrs.fr/en/node/4346). - « Contrat rempli pour l’observatoire spatial Herschel », communiqué de presse de l’Université de Bordeaux, 2 mai 2013. - « ALMA révolutionne notre connaissance des étoiles évoluées », lettre science du LAB, 28 avril 2018 . - « Nuages moléculaires et formation stellaire », lettre science du LAB, 20 novembre 2017. - « Première détection d’un maser THz de l’eau dans l’infrarouge lointain », lettre science du LAB, 13 octobre 2017. - « Les étoiles massives sont la conséquence d’effondrements à grande échelle », lettre science du LAB, 26 avril 2017.
Liste des lettres science du LAB: http://astrophy.u-bordeaux.fr/actualites/ Research Group: ISM
Permanent staff: Emeric Bron , Maryvonne Gerin, Jacques Le Bourlot, Franck Le Petit, Evelyne Roueff, Technical staff: David Languignon PhD students (since 2010): * Jan Orkisz (2015-2018) - direction: M. Gerin et J. Pety * Emeric Bron (2011-2014) - direction: J. Le Bourlot et F. Le Petit * Gwendoline Stefan (2012-2016) - direction: P. Schilke et J. Le Bourlot Post-docs (since 2010): * Alan Heays (2016-2017) * Ronin Wu (2015-2017) * Emeric Bron (2014-2015) * Benjamin Godard (2012-2014) * Antoine Gusdorf (2011-2015) * Cecilia Pinto (2009-2012)
Contact: [email protected]
Laboratory: LERMA Institution(s): Observatoire de Paris, PSL, Sorbonne Université, ENS, CNRS Website: https://ism.obspm.fr
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: • Users of: observational facilities at all wavelengths, but mainly IRAM, ALMA and Herschel • Develop and provide: the Meudon PDR code.
Keywords: Astrochemistry, sub-millimeter observations, numerical models, radiative transfer, turbulence, Machine Learning methods, stochastic processes.
Astrophysical context and goals: The goal of the team is to develop new numerical methods to interpret observations and understand the physics and the chemistry of the interstellar medium. Some members of our team are also specialists of millimetre and sub-millimetre astronomy. Also, they have been very implied in Herschel observations as for example the study of hybrids in diffuse interstellar medium and in IRAM-30m large project OrioN-B. We develop and maintain some codes used by the community to interpret observations as the Meudon PDR code. A new axis of research of the team is to search for new statistical methods to analyse the mass of data produced both by instrumental facilities and numerical models. Among our main goals for the coming years : 1) we will develop an hydrodynamical-PDR code to interpret JWST observations and study the radiative feedback. 2) in the context of the OrioN-B project, we will search for new statistical methods to analyse large sets of hyper-spectral observations and understand the physics, chemistry and structure of Giant Molecular Clouds in Galactic and extragalactic conditions. 3) we will continue the development of our stochastic methods to simulate chemical processes on interstellar grains.
Collaborations: • France: IRAP (Toulouse), IPAG & IRAM (Grenoble), IAS (Orsay), CEA • Europe: Madrid, Köln, … • World: Japan, Israël, USA, …
Highlight: Formation of H2 in the interstellar medium A trademark, that is a result that well illustrate what the team or the project does). We developed a new stochastic method to simulate the formation of H2 on grains and its ortho-para conversion. Thanks to this new method we have been able to propose for the first time a consistent scenario to explain observations of H2 emission in PDRs (Ref: Bron et al. 2014 & 2016, A&A).
Most significant publications (<5): · Clustering the Orion B giant molecular cloud based on its molecular emission, Bron E, Daudon C., Pety J., Levrier F. et al. 2018, A&A, 10.1051/0004-6361/201731833 · Structure of photodissociation fronts in star-forming regions revealed by observations of high-J CO emission lines with Herschel, Joblin C., Bron E., Pinto C., et al., 2018, A&A accepted, 2018arXiv180103893J · Interstellar Hydrides, Gerin M., Neufeld D., Goicoechea J., 2016, ARA&A, 10.1146/annurev-astro-081915-023409 · Efficient ortho-para conversion of H2 on interstellar grain surface, Bron E., Le Petit F., Le Bourlot J., 2016, A&A, 10.1051/0004-6361/201527879 · Surface chemistry in the interstellar medium. II. H2 formation on dust with random temperature fluctuations, Bron E., Le Bourlot J., Le Petit F., 2014, A&A, 10.1051/0004-6361/201322101
Link to full publication list: http://adsabs.harvard.edu/cgi-bin/nph-abs_connect? db_key=AST&db_key=PRE&qform=AST&arxiv_sel=astro-ph&arxiv_sel=cond-mat&arxiv_sel=cs& arxiv_sel=gr-qc&arxiv_sel=hep-ex&arxiv_sel=hep-lat&arxiv_sel=hep-ph&arxiv_sel=hep-t h&arxiv_sel=math&arxiv_sel=math-ph&arxiv_sel=nlin&arxiv_sel=nucl-ex&arxiv_sel=nucl- th&arxiv_sel=physics&arxiv_sel=quant-ph&arxiv_sel=q-bio&sim_query=YES&ned_query=YES &adsobj_query=YES&aut_logic=OR&obj_logic=OR&author=Bron%2C+E.%0D%0ARoueff%2C+E.%0D %0ALe+Bourlot%2C+J.%0D%0AGerin%2C+M.%0D%0ALe+Petit %2C+F.&object=&start_mon=&start_year=&end_mon=&end_year=&ttl_logic=OR&title=&txt_lo gic=OR&text=&nr_to_return=500&start_nr=1&jou_pick=NO&ref_stems=&data_and=ALL&group_ and=ALL&start_entry_day=&start_entry_mon=&start_entry_year=&end_entry_day=&end_entr y_mon=&end_entry_year=&min_score=&sort=SCORE&data_type=SHORT&aut_syn=YES&ttl_syn=YE S&txt_syn=YES&aut_wt=1.0&obj_wt=1.0&ttl_wt=0.3&txt_wt=3.0&aut_wgt=YES&obj_wgt=YES&t tl_wgt=YES&txt_wgt=YES&ttl_sco=YES&txt_sco=YES&version=1.
Press releases: Research Group: NUAGES (Nearby Universe Agents of Galaxy Evolution Studies)
Permanent staff: Frédéric Galliano, Vianney Lebouteiller, Suzanne Madden Technical staff: none PhD students (since 2010): Maud Galametz (2007-2010), Diane Cormier (2009-2012), Aurélie Rémy-Ruyer (2010-2013), Mélanie Chevance (2013-2016), Fiorella Polles (2014-2017), Antigone Lambert-Huygue (2017-) Post-docs (since 2010): Sacha Hony (2007-2013), Vianney Lebouteiller (2010-2013), Lynn Carlson (2011-2013), Ronin Wu (2011-2014), Min-Young Lee (2013-2017), Oskar Karczewski (2015-2017), Sophia Lianou (2015-2018), Maud Galametz (2016-), Diane Cormier (2017-) Contact: [email protected], [email protected], [email protected]
Laboratory: LFEMI (Laboratoire Formation d’Étoiles et Milieu Interstellaire), UMR AIM (7158) Institution(s): CEA, CNRS, Université Paris Diderot, Université Paris-Saclay Website: http://thesis.cormier.free.fr/WebGroup/
Key Research Facilities, Infrastructure and Equipment: we make extensive use of the following facilities: the IR/submm space telescopes Herschel, Spitzer and AKARI; the IR stratospheric observatory SOFIA; the ground-based submm-mm telescopes ALMA, IRAM and APEX. We have developed our own hierarchical Bayesian dust SED code, HerBIE. We are leading the Combined Atlas of Sources with Spitzer IRS Spectra (CASSIS).
Keywords: Interstellar medium; nearby galaxies; dwarf galaxies; Magellanic clouds; photoionisation; photodissociation regions; molecular gas; dust evolution.
Collaborations: DustPedia (FP7 european collaboration network; P.I. J. Davies): a definitive study of the dust properties in the nearby universe. We are leading the dust SED modelling of the whole 3000 galaxy sample. SAGE/HERITAGE (international consortium; P.I. M. Meixner): observations of the Magellanic clouds with Spitzer and Herschel. SYMPATICO (ANR between AIM and LERMA; P.I. S. Madden & F. Le Petit): multi-phase modelling of the ISM in nearby galaxies. EMPIRE (P.I. F. Bigiel): study of dense gas in nearby disk galaxies. EMPIRE (France-Japan PRC; P.I. F. Galliano & T. Onaka): study of PAH properties with AKARI and Spitzer spectroscopy. Spica consortium (P.I. P. Roelfsma): international team working of the science planification of the IR/submm satellite Spica (2025).
Goals: Understanding the heating, cooling and topology of the different gaseous phases across interstellar environments. Characterizing the grain properties of different galaxies, at different stages of their evolution, in order to constrain cosmic dust evolution. Providing accurate diagnostics of the physical conditions, based on a variety of interstellar tracers. Highlight: Unveiling the Impact of Massive Star Formation in Low-Metallicity environments
Understanding galaxy evolution requires understanding the impact of massive star formation on the interstellar medium (ISM). In particular, understanding the role of metallicity in the way stellar feedback shapes the ISM is crucial to interpret observations of distant galaxies, as the latter are expected to be on average less enriched in heavy elements than the Milky Way. To explore this effect, we have studied in detail the ISM properties in the massive star forming region 30Dor, in the Large Magellanic Cloud (LMC). This study is published as Chevance et al. (2016). We have combined spatially resolved tracers of the ionized, atomic and molecular gas as well as tracers of the dust to constrain the physical parameters that we have derived using the PhotoDissociation Region (PDR) code of Le Petit et al., (2006) and the dust SED model of Galliano et al. (2011). We have derived maps of the gaz pressure, the UV field density (Figure), the visual attenuation of the individual PDRs, AV, and their filling factor. Comparing the PDR modelled UV field with the stellar distribution, we could infer the 3D geometry of the region. Overall, our analysis shows that the ISM in 30Dor has a complex structure, with a porous medium permeated by hard photons, and numerous small PDR clumps.
Figure: Modelled pressure (cm-3.K; left) and UV field, GUV (in units of 1.6E-6 W/m2; right). The red circle shows the location of the super star cluser R136.
Most significant publications (<5): A Dust spectral energy distribution model with hierarchical Bayesian inference, Galliano, F., 2018, MNRAS, 476, 1445-1469. The Interstellar dust properties of nearby galaxies, Galliano, F., Galametz, M. and Jones, A.P., 2018, ARAA, in press. Neutral gas heating by X-rays in primitive galaxies: Infrared observations of the blue compact dwarf I Zw 18 with Herschel, Lebouteiller, V., Péquignot, D., Cormier, D., Madden, S.C., Pakull, M.W., Kunth, D., Galliano, F., Chevance, M., Heap, S.R., Lee, M.Y., Polles, F.L., 2017, A&A, 602, A45 A milestone toward understanding PDR properties in the extreme environment of LMC-30 Doradus, Chevance, M., Madden, S.C., Lebouteiller, V., Godard, B., Cormier, D., Galliano, F., Hony, S., Indebetouw, R., Le Bourlot, J., Lee, M.Y., Le Petit, F., Pellegrini, E., Roueff, E., Wu, R., 2016, A&A, 590, A36 The Herschel Dwarf Galaxy Survey. I. Properties of the low-metallicity ISM from PACS spectroscopy, Cormier, D., Madden, S.C., Lebouteiller, V., Abel, N., Hony, S., Galliano, F., Rémy-Ruyer, A., Bigiel, F., Baes, M., Boselli, A., Chevance, M., Cooray, A., De Looze, I., Doublier, V., Galametz, M., Hughes, A., Karczewski, O.L., Lee, M.Y, Lu, N., Spinoglio, L., 2015, A&A, 578, A53 Research Group: UV spectroscopy of interstellar and circumstellar matter
Permanent staff: Cecile Gry Technical staff: PhD students (since 2010): Post-docs (since 2010): Contact: [email protected]
Laboratory: Laboratoire d'Astrophysique de Marseille Institution(s): Aix-Marseille Université
Key Research Facilities, Infrastructure and Equipment: UV spectroscopy at high wavelength resolution, in particular STIS on HST.
Keywords: diffuse local ISM, ionization, structure, abundances, debris disks
Astrophysical context and goals: Study the diffuse ISM by detailed study of individual clouds in the nearby medium. Study of the cloud structure, the abundance distribution, the ionization, and the distribution of the different phases. Study of conditions (temperature, electron density, excitation mechanisms) in debris disks around stars by analysis of many metastable levels of metals.
Experimental studies of the group: UV spectroscopic observations Line profile fitting
Collaborations: Edward B. Jenkins, Princeton University Emmanuel Caux, Sandrine Bottinelli (IRAP Toulouse)
Highlight: Identification of a single Local Cloud surrounding the sun in all directions. We show that the cloud is deformed like a squashed balloon in its direction of motion. Metals are significantly depleted and there is an abundance gradient in the direction of the apex. In half of the sky, there is a secondary component compatible with a shock propagating toward the center of the cloud. Characterization of the conditions in the nearest interstellar cloud. By the analysis of the most complete UV and far UV spectrum ever obtained in one line of sight, we derive the physical conditions in the Local Cloud (T~7600 K, n(e) ~ 0.11 cm-3), the ionization fractions of 10 species (H+/H ~ 1/3), their depletion values ([S/H] ∼ −0.27), and the covering factor of the WIM in the line of sight (~13%), the rest of it being filled with X-ray emitting gas.
Most significant publications (<5): The interstellar cloud surrounding the Sun: a new perspective. Cecile Gry and Edward B. Jenkins 2014, A&A 567, A58, DOI: 10.1051/0004-6361/201323342. The nearby interstellar medium toward α Leo - UV observations and modeling of a warm cloud within hot gas. Cecile Gry and Edward B. Jenkins 2017, A&A 598, A31 DOI: 10.1051/0004-6361/201628987
1.2 Laboratory
23 Research Group: CMB team – COMEX group
Permanent staff: Astrid BERGEAT, Christian NAULIN Technical staff: Sébastien MORALES PhD students (since 2010): Simon CHEFDEVILLE Post-docs (since 2010): Contact: Astrid BERGEAT
Laboratory: Institut des Sciences Moléculaires, équipe COllisions Moléculaires en Milieux EXtrêmes (COMEX) Institution(s): Université de Bordeaux / CNRS Website: http://www.ism.u-bordeaux.fr/spip.php?article555
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: Crossed molecular beam experiment with variable beam crossing angle; Yag-Dye pulsed lasers; cryo-cooled pulsed molecular beam sources with discharge device (for metastable species generation), para-H2 conversion unit, time-of-flight mass spectrometer…
Keywords: Reactive and inelastic collision dynamics, kinetics, astrochemistry, molecular astrophysics, low temperatures, low energies, molecular energy transfer, state-to-state collisions.
Astrophysical context and goals: Physical Chemistry of atomic and molecular objects in the ISM: determination of cross-sections for reactive and inelastic collisions at low collision energies (corresponding to temperatures down to a few K): in conjunction with theoretical calculations, this allows one to provide modelers with rates of 3 reaction or collisional (de-)excitation for molecules (such as CO, O2, H2O…) and atoms (C P) with more abundant species (H2, He).
Experimental studies of the group: collision induced rotational excitation of H2O (D2O) by inelastic collisions with He, H2, D2 3 collision induced spin-orbit excitation of C( P0) by inelastic collisions with He, H2
collision induced rotational excitation of O2 by inelastic collisions with H2
collision induced rotational excitation of CO by inelastic collisions with He, H2, D2 1 reactivity of Sulfur atoms (S D) with H2 (D2, HD) 3 reactivity of Carbon atoms (C P) with small hydrocarbon molecules (C2H2, C2H4, C2H4)
Collaborations: François Lique group, LOMC, Le Havre, Alexandre Faure group, IPAG, Grenoble P. Honvault et G. Guillon, Université de Dijon Th. Stoecklin, ISM, Bordeaux International: Sebastiaan van de Meerakker group, Radboud University, Nijmegen (NLD) Piergiorgio Casavecchia, Dipartimento di Chimica, Biologia e Biotecnologie – Universita’ degli Studi di Perugia (ITA) Manuel Lara, Departamento de Química Física Aplicada, Facultad de Ciencias, Universidad Autónoma de Madrid, (ESP) Highlight: Experimental determination of state-to-state integral cross-sections of inelastic collisions. The first experimental determination of quantum resonances at low collision energy (or low temperature) for an inelastic process was performed on the rotational excitation of CO and O2 with H2 and He. These experimental results are a stringent test for theoretical calculations, which then can provide rate coefficient at low temperatures for astrochemistry.
Left: Cross-sections for the CO rotational transition 0→1 induced by para-H2 as function of collision energy. The experimental data is compared to the theoretical cross section convoluted with the experimental energy spread (from Chefdeville et al. 2015). Right: Cross-sections for the classically forbidden O2 rotational transition N=1, j= 0 → N=1, j= 1, induced by para-H2 as function of collision energy (from Chefdeville et al. 2013 & Lique et al. 2014).
Most significant publications (<5):
3 “Understanding the quantum nature of low-energy C( Pj) + He inelastic collisions”, Astrid Bergeat, Simon Chefdeville, Michel Costes, Sébastien B. Morales, Christian Naulin, Uzi Even, Jacek Kłos and François Lique, Nature Chemistry, 10 (2018) 519-522 ; DOI: 10.1038/s415570180030y “Observation of quantum dynamical resonances in near cold inelastic collisions of astrophysical molecules”, M. Costes and C. Naulin, Chemical Science, 7 (2016) 2462-2469; DOI: 10.1039/C5SC04557F
“Experimental and theoretical analysis of low-energy CO + H2 inelastic collisions”, S. Chefdeville, T. Stoecklin, C. Naulin, P. Jankowski, K. Szalewicz, A. Faure, M. Costes and A. Bergeat, Astrophys. J. Letters 799:L9 (2015); doi: 10.1088/2041-8205/799/1/L9
“Collisional excitation of O2 by H2 : On the validity of LTE models for interpreting O2 observations”, F. Lique, Y. Kalugina, S. Chefdeville, S. Y. T. van de Meerakker, M. Costes and C. Naulin, Astron. Astrophys. 567 (2014) A22; DOI: 10.1051/0004-6361/201423957
“Observation of Partial Wave Resonances in Low-Energy O2 – H2 Inelastic Collisions”, S. Chefdeville, Y. Kalugina, S. Y. T. van de Meerakker, C. Naulin, F. Lique, M. Costes, Science 341 (2013) 1094-1096; https://doi.org/10.1126/science.1241395
Link to full publication list: http://www.ism.u-bordeaux.fr/spip.php?article459
Press releases: http://www.ism.u-bordeaux.fr/spip.php?breve230 http://www.cnrs.fr/inc/communication/direct_labos/naulin.htm http://www.cnrs.fr/inc/communication/direct_labos/costes.html
Research Group: CRESU team – COMEX group
Permanent staff: Kevin HICKSON (DR2 CNRS) Technical staff: PhD students (since 2010): Julien DARANLOT, Dianailys NUNEZ-REYES Post-docs (since 2010): Cédric BRAY Contact: Kevin HICKSON [email protected] Laboratory: Institut des Sciences Moléculaires, équipe COllisions Moléculaires en Milieux EXtrêmes (COMEX)
Institution(s): Université de Bordeaux Website: https://www.ism.u-bordeaux.fr/spip.php?article355&lang=fr
Key Research Facilities, Infrastructure and Equipment: Supersonic flow (Laval nozzle) reactor; pulsed Nd:YAG lasers, dye lasers; microwave generators, rare gas tripling cells.
Keywords: astrochemistry, kinetics of gas-phase reactions; gas-phase quenching kinetics; low temperatures.
Astrophysical context and goals: Measurement of rate constants and product branching ratios at low temperature for astrochemically important reactions for use in modeling studies.
Experimental studies of the group: 4 Reactions of ground state atomic nitrogen, N( S), with radicals (OH, CN, CH, C2, C2N) 3 Reactions of ground state atomic carbon, C( P), with molecules CH3OH, H2O, NH3 Reactions of excited state atomic nitrogen, N(2D), with saturated and unsaturated hydrocarbons Reactions of excited state atomic oxygen, O(1D), with a wide range of molecules Reactions of excited state atomic carbon, C(1D), with a wide range of molecules
Collaborations: Pascal Larregaray, ISM Jean Christophe Loison, ISM Valentin Wakelam, LAB Tomás Gonzalez-Lezana, CSIC Madrid Yury Suleimanov The Cyprus Institute Wensheng Bian University of Chinese Academy of Sciences Hua Guo, University of New Mexico Research Group: CORINT
Permanent staff: Jean-Claude Guillemin (DR1 CNRS); Yann Trolez (MdC ENSCR). Technical staff: Jean-Paul Guégan (IR ENSCR), Sophie Rouen (IR ENSCR), Thomas Vives (AI CNRS). 10% of their time on the subject for each. PhD Student (since 2014): Nicolas Kerisit, Nour Jamal-Eddine (codirection), Javier Torres Escalona (codirection), Houda Gazzeh (9 months of internship) Contact: [email protected]
Laboratory: Chimie Organique aux Interfaces (CORINT, a team of the UMR 6226, Institut des Sciences Chimiques de Rennes). Website: https://iscr.univ-rennes1.fr/corint/
Context/astrophysic problematic Synthesis of Complex Organic Molecules, candidates for the Interstellar Medium Chemistry and photochemistry of detected compounds.
Key Research Facilities, Infrastructure and Equipment: The group is equipped or has access to a 400 MHz NMR spectrometer, Gas chromatographs with chiral columns, UV lamps, ovens with a temperature up to 1100°C, vacuum lines. Synthesis of kinetically unstable compounds can be generated in gas phase and directly introduced in spectrometers (millimetric, infra-red, photoelectron, …)
Keywords: Interstellar compounds, Astrochemistry, Organic Synthesis, Spectroscopic Characterization.
Experimental studies of the group: Looking for new interstellar compounds: Organic synthesis, Photochemistry. Prebiotic Chemistry. Sublimation for enantioenrichment.
Collaborations: Pr. Laurent Margulès, Dr. Roman Motienko, MdC, Millimeterwave Spectroscopy, Univ. Lille. Pr. José-Luis Alonso, Millimeterwave Spectroscopy, Univ. Valladolid, Spain. Dr. Luca Bizzocchi, Millimeterwave Spectroscopy, Max Planck Inst., Munich, Germany. Pr. Robert Kolos, Dr. Marcin Gronowski, MdC, Photochemistry in matrix, Infrared Spectroscopy, Inst. of Phys. Chem., Varsovie, Poland. Dr. Claudine Crépin, DR CNRS, Photochemistry in matrix, Infrared Spectroscopy, ISMO, Orsay. Dr. Ludovic Biennier and Dr. Sophie Carles, Kinetics on anions, IPR, Univ. Rennes. Dr. Christian Alcaraz, Kinetics on anions, Lab. Chimie Physique, Orsay. Pr. Lahouari Krim, Spectroscopie infrarouge. Hydrogen bombardment of compound in argon matrix and analysis by infrared spectroscopy, UPMC. Pr. Martin Schwell, VUV photoionization and dissociative photoionization, LISA, Créteil. Pr. Manuel Yanez and Pr. Otilia Mo, Theoretical calculations, UAM, Madrid, Spain. Dr. Ellinger, Yves, Dr. Pauzat, Françoise, DR1 Em. Theoretical Calculations, UPMC. Pr. José Cernicharo, Astrophysics, Madrid, Spain. Dr. Arnaud Belloche, Astrophysics, Max Planck Inst. Bonn, Germany.
Highligth: Two compounds have been detected in the Interstellar medium: the synthesis, the recording of the millimetric spectrum of methyl isocyanate (CH3-NCO) and methoxymethanol (CH3OCH2OH) allowed their detection in the ISM.
Figure. Detections of CH3OCH2OH indicated in red are overlaid on spectra of NGC 6334I toward MM1.
Most Significant publications. 1. B. A. McGuire, C. N. Shingledecker, E. R. Willis, A. M. Burkhardt, S. El-Abd, R. A. Motiyenko, C. L. Brogan, T. R. Hunter, L. Margulès, J.-C. Guillemin, R. T. Garrod, E. Herbst, A. J. Remijan, ALMA Detection of Interstellar Methoxymethanol (CH3OCH2OH) ApJ Lett., 851, L46 (2017). 2. N. Kerisit, C. Rouxel, S. Colombel-Rouen, L. Toupet, J.-C. Guillemin, Y. Trolez Synthesis, chemistry and photochemistry of methylcyanobutadiyne (MeC5N) in the context of space science, J. Org. Chem. 81, 3560-3567 (2016). 3. J. Cernicharo, Z. Kisiel, B. Tercero, L. Kolesniková, I.R. Medvedev, A. López, S. Fortman, M. Winnewisser, F. C. de Lucia, J. L. Alonso, and J.-C. Guillemin A rigorous detection of interstellar CH3NCO: an important missing species in astrochemical networks A&A, 587, L4 (2016). 4. C. Cabezas, C. Barrientos, A. Largo, J.-C. Guillemin, J. Cernicharo, I. Peña, and J. Alonso Generation and structural characterization of aluminum cyanoacetylide J. Chem. Phys. 141, 104305 (2014). 5. S. Carles, H. Møllendal, Y. Trolez, and J.-C. Guillemin Rotational spectrum of 4- methylcyanoallene (CH3CH=C=CH-CN), a chiral molecule of potential astrochemical interest A&A, 564, A82 (2014). Research Group: DESIRS
Permanent staff: Gustavo Garcia, Laurent Nahon, Nelson de Oliveira Technical staff: Jean-François Gil PhD students (since 2010): Maurice Tia, Iuliia Myrgorodska, Sarah Tigrine, Rim Hadidi, Abhyuday Chatterjee Post-docs (since 2010): François Gaie-Levrel, Barbara Cunha de Miranda, Steven Daly, Xiaofeng Tang, Dusan Bozanic, Helgi Hrodmarsson
Contact: [email protected]
Laboratory: Synchrotron SOLEIL Institution(s): Société civile (CNRS/CEA) Website: https://www.synchrotron-soleil.fr/fr/lignes-de-lumiere/desirs
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: • Intense, tunable, high resolution, variable polarization synchrotron radiation covering the VUV range (4-40 eV) • 2 permanent endstations: - The versatile molecular chamber SAPHIRS coupled to a double imaging electron/ion coincidence i2PEPICO spectrometer; sources of radicals (MW discharge coupled to a flow tube, pyrolysis), oven coupled to a molecular beam, effusive source, atomizer and aerodynamic lens for handling nanoparticles - The Fourier-Transform spectrometer (FTS) for high resolution absorption spectroscopy; sample environment chamber equipped with various-length closed cells, cold and heated open cell, DC and RF discharge cells (radicals and metastable states), molecular beam • 2 non-permanent set-ups connected to the monochromator branch - The ion trap for action spectroscopy on trap cations/anions with electro-spray and APPI sources - An in vacuum irradiation set-up with holders for thin films and cuvettes • experimental chambers brought by collaborator/users (CRESUSOL chamber with a Laval Nozzle for VUV PIMS as a probe of chemical reactivity at low temperatures)
Keywords: VUV source, high resolution absorption spectroscopy; electron/ion spectroscopy; molecular and electronic structures; gas phase photodynamics; gas phase reactivity; prebiotic chemistry and origin of life
Astrophysical context and goals: We are interested in VUV spectroscopy & photodynamics on a broad range of gas phase isolated samples, some of them relevant to PCMI (interstellar medium as well as planetary atmospheres) such as cold molecules, radicals, prebiotic species, chiral elementary bricks of life, clusters and nanoparticles, as well as on condensed matter samples such as thin films and interstellar ice analogs. Basically the DESIRS VUV photons in combination with our permanent and non-permanent endstations are used in an astrophysical context to: - study the molecular and electronic structures/dynamics of astrophysically-relevant objects - simulate in the lab photon-induced processes (especially at the Lyman radiation energy) - probe the products of astrophysically-relevant gas phase chemical reactions Experimental studies of the group: We describe briefly hereafter the main lines of research carried out either directly by our group or within close collaborations with the beamline user groups (the pure user group experiments in which we are not taking part are directly described when appropriate by the various PCMI teams description sheets. Same comment applies for the associated experiment CERISES group which has a dedicated description sheet).
Very high resolution absorption spectroscopy on (cold) molecules and radicals Photoelectron spectroscopy (PES) and state-selected ion fragmentation on cold molecules (including prebiotic species and PAHs), radicals, clusters Angle-Resolved PES on nanoparticles (including tholins) Asymmetric photochemistry in the condensed matter (thin films and ices) in relation to the origin of life homochirality Asymmetric photoionization of amino-acids in the gas phase (PECD) in relation to the origin of life homochirality ionization / fragmentation of trapped PAHs and fullerene cations VUV photochemistry in a gas phase photochemical reactor or on thin films Probe by i2PEPICO of room temperature radical-neutral reactions (with isomer sensitivity) Probe by mass spectrometry (VUV-PIMS) of low temperature radical-neutral reactions (CRESUSOL)
Collaborations: Wellesley College (USA), G. Stark et al. http://www.wellesley.edu/physics/people/faculty/stark Arizona Sate University (USA), J. Lyons et al., https://isearch.asu.edu/profile/2032452 Obs Meudon (LERMA) M. Eidelsberg, J.-L. Lemaire, A. Heays et al., https://lerma.obspm.fr LISA (Créteil), M. Schwell, O. Venot, Y. Benilan et al., http://www.lisa.univ-paris12.fr/fr/exobiologie-et-astrochimie ISMO (Orsay), B. Gans, S. Boyé-Peronne, P. Bréchignac et al., http://www.ismo.u-psud.fr/spip.php?rubrique28 Slacker lab for satrophysics (Leiden, NL), H. Linnartz et al., http://home.strw.leidenuniv.nl/~linnartz/ IRAP (Toulouse), C. Joblin et al., http://www.irap.omp.eu/recherche/groupes-thematiques/micmac ISM (Bordeaux), J.-C. Loison et al., http://www.ism.u-bordeaux1.fr/spip.php?rubrique10 LATMOS (Guyancourt), N. Carrasco et al., http://www.latmos.ipsl.fr/index.php/fr/activites-de-recherche/impec IAS (Orsay)/PIIM (Marseilles), L. Le Sergent dHendecourt, https://www.ias.u-psud.fr/fr/activites-de-recherche/astrochimie-et-origines Univ; Sophia Antipolis (Nice), U. Meierhenrich, C. Meinert, http://univ-cotedazur.fr/labs/icn/fr/equipes/APSM/page.html Aarhus University (Danmark), S. Hoffmann, http://pure.au.dk/portal/en/persons/id(5a53b491-0de4-481d-a3be-6649f619759a).html IPR (Rennes), S. Le Picard, I. Sims, L. Bennier et al., https://ipr.univ-rennes1.fr/labastro
Highlight: Correlation between structures and electronic properties in PAH clusters. The first experimental measurement of photoelectrons spectra of PAH clusters, have been obtained using the i2PEPICO technique available on. This data have been compared with the results of molecular simulations in which the effects of structure and temperature have been taken into account. In astrophysical environments, the PAHs would be produced by destruction (photoevaporation) of very small carbonaceous grains due to the effect of VUV photons. The work presented here constitutes a first step in the study of the process, the PAH clusters being considered as laboratory model systems of the very small cosmic carbonaceous grains. The ionisation properties of PAH clusters (relatively low ionisation energy and highly effective ionisation cross-section) imply that these species would largely be ionised in the environments where these PAHs are formed. Their evaporation properties will therefore differ in comparison with those of neutral clusters which have until now been considered as astrophysical models.
Figure: Change in the ionisation energy with size of pyrene (C16H10) clusters. The experimental values (black curve) are compared with the results of molecular simulations (colour curves). The vertical ionisation potential (green curve) has been calculated for the isomers of lowest energy, shown here for 5, 6 and 7 molecules. In these structures, the green molecules are those carrying the charge upon ionisation. At a finite temperature, typically 100 - 200 K in the experiment, the different isomers population must be taken into account in the simulations leading to the red and blue curves which are in very good agreement with the experimental curve. (from Joblin et al., J. Phys. Chem. Lett. 8, 3697 (2017)).
Most significant publications (<5): Hadidi, R., Bozanic, D. K., Garcia, G. A. & Nahon, L. Electron asymmetries in the photoionization of chiral molecules: possible astrophysical implications. Advances in Physics X, doi:10.1080/23746149.2018.1477530 (2018).
Carrasco, N., Tigrine, S., Gavilan, L., Nahon, L. & Gudipati, M. S. The evolution of Titan’s highaltitude aerosols under ultraviolet irradiation. Nature Astronomy, doi:10.1038/s4155001804397 (2018).
Heays, A. N. et al. Highresolution onephoton absorption spectroscopy of the D2Σ←X2Π system of radical OH and OD. J. Quant. Spectrosc. Radiat. Transfer 204, 1222, doi:10.1016/j.jqsrt.2017.08.021 (2018).
Joblin, C. et al. Size Effect in the Ionization Energy of PAH Clusters. J Phys Chem Lett 8, 36973702, doi:10.1021/acs.jpclett.7b01546 (2017). Gans, B. et al. Unveiling the Ionization Energy of the CN Radical. J Phys Chem Lett 8, 40384042, doi:10.1021/acs.jpclett.7b01853 (2017). Rouillé, G. et al. Dissociative Photoionization of Polycyclic Aromatic Hydrocarbon Molecules Carrying an Ethynyl Group. The Astrophysical Journal 810, 114, doi:10.1088/0004637x/810/2/114 (2015).
Modica, P. et al. Enantiomeric Excesses Induced in Amino Acids by Ultraviolet Circularly Polarized Light Irradiation of Extraterrestrial Ice Analogs: A Possible Source of Asymmetry for Prebiotic Chemistry. The Astrophysical Journal 788, 79, doi:10.1088/0004637x/788/1/79 (2014).
Meinert, C. et al. Photonenergy controlled symmetry breaking with circularlypolarized light. Angew. Chem.Int. Edit. 53, 210214 (2014).
Link to full publication list: https://www.synchrotron-soleil.fr/fr/publications?field_lignes_de_lumiere_tid=17
Press releases: https://www.synchrotron-soleil.fr/en/news/sunburn-titans-haze https://www.synchrotron-soleil.fr/en/news/ionization-potential-cyano-radical-and-implications-cn-catio n-chemistry-space https://www.synchrotron-soleil.fr/en/news/correlation-between-structures-and-electronic-properties-pah -clusters https://www.synchrotron-soleil.fr/en/news/photoionisation-cation-c60-buckminsterfullerene-molecule Research Group : ESPOIRs
Permanent staff : Karine Demyk, Claude Meny Technical staff : Anthony Bonnamy, Loïc Noguès PhD students : XingHeng Lu (2013 - 2016) Post-doc : Anne Coupeaud (2008 - 2011) Contact : [email protected]
Laboratory : Institut de Recherche en astrophysique et Planétologie. UMR 5277 (IRAP), http://www.irap.omp.eu/ Institutions : CNRS, Université de Toulouse, Observatoire MIdi-Pyrénées
Website : http://www.irap.omp.eu/observations/explabo/nanograins/espoirs
Key Research Facilities, Infrastructure and Equipment : The group is equipped with one experimental platform, including a cryogenics head (4K), a Fourier-Transform spectrometer equipped with tow sample compartments and sets of beamsplitters (Si, CaF2, KBr), sources (water-cooled Hg lamp, Tg lamp, globar) and detectors (room temperature and N2-cooled detectors in the FIR, MIR and NIR ranges and a He-free bolometer for the FIR). An environmental cell (hight temperature and high pressure) may be fitted into the spectrometer to study samples annealed up to 800C under controlled atmosphere.
Keywords : Experimental laboratory astrophysics, Cosmic dust ; solid-state science ; Temperature-induced processes; Vibrational Spectroscopy
Context : The ESPOIRs team provides fundamental data necessary to study cosmic dust. Circumstellar and interstellar dust plays a key role in the evolution of the ISM in Galaxies. Studying its composition and understanding its evolution along its life cycle is essential to improve our knowledge on star formation and on the ISM evolution.
Experimental studies of the group : • Spectroscopy of cosmic dust analogues (0.6 – 1000 µm) • Temperature dependence of the spectroscopic properties of dust analogues (10 K – 1173 K)
Collaborations : • UMET, Origine des matériaux du système solaire http://umet.univ- lille1.fr/Mineraux/index.php?lang=fr, H. Leroux, C. Depecker • LPCNO Nanostructure, http://lpcno.insa-toulouse.fr/spip.php?rubrique83&lang=fr, C. Nayral, F. Delpech • IAS, Physique du milieu interstellaire, https://www.ias.u-psud.fr/fr/activites-de- recherche/matiere-interstellaire-et-cosmologie/physique-du-milieu-interstellaire, A. Jones, N. Ysard, L. Verstraete • Synchrotron SOLEIL, AILES beamline, https://www.synchrotron-soleil.fr/fr/lignes-de- lumiere/ailes, P. Roy, J.-B. Brubach • Diamond Light source, http://www.diamond.ac.uk/Beamlines/Engineering-and- Environment/I11.html, S. Thompson • Institute of chemical engineering sciences, Nanothecnology / Advanced materials, http://www.iceht.forth.gr/about/ra1.html#amorphous, G. Papatheodorou Highlight : Cosmic dust models underestimate the silicate dust emissivity
Our new experimental measurements show that the emissivity of cosmic dust analogues is very different from the emissivity adopted in cosmic dust models. In the FIR, the spectral dependency is more complex than the often used power law and varies with the dust grain temperature. The emissivity is found to be 3 to 5 time higher than in dust models. These behaviours are related to the amorphous nature of the analogues, whatever their composition. It has strong implications for the study of the ISM and star formation since the enhanced emissivity of the analogues compared to the emissivity calculated by cosmic dust model implies that dust masses in interstellar clouds are overestimated by the models.
Five publications of the group: • Low-temperature MIR to submillimeter mass absorption coefficient of interstellar dust analogues. II. Mg and Fe-rich amorphous silicates, K. Demyk, C. Meny, H. Leroux, C. Depecker, J.-B. Brubach, P. Roy, C. Nayral, W.-S. Ojo, F. Delpech, 2017, A&A 606, A50, https://www.aanda.org/articles/aa/pdf/2017/10/aa30944-17.pdf • Low temperature MIR to submillimeter mass absorption coefficient of interstellar dust analogues. I. Mg-rich glassy silicates, K. Demyk, C. Meny, X,-H. Lu, G. Papatheodorou, M. Toplis, H. Leroux, C. Depecker, J.-B. Brubach, P. Roy, C. Nayral, W.-S. Ojo, F. Delpech, D. paradis, V. Gromov, 2017, A&A 600, A123, https://www.aanda.org/articles/aa/pdf/2017/04/aa29711-16.pdf • FIR and Submm Optical Properties of Astrophysically Relevant Minerals, K. Demyk, C/ Meny, H. Leroux, C. Depecker, C. Nayral, W.-S. Ojo, F. Delpech, J.-B. Brubach, P. Roy, 2013, Proceedings of The Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments (LCDU2013), https://pos.sissa.it/207/044/pdf • Low-temperature FIR and submillimetre mass absorption coefficient of interstellar silicate dust analogue, A. Coupeaud, K. Demyk, C. Meny, C. Nayral, F. Delpech, H. Leroux, C. Depecker, G. Creff, J.-B. Brubach, P. Roy, 2011, A&A 535, A124, https://www.aanda.org/articles/aa/pdf/2011/11/aa16945-11.pdf
Other publications: • Galactic cold cores. VI. Dust opacity spectral index, M. Juvela, K. Demyk, Y. Doi, A. Hughes, C. Lefèvre, D. Marshall, C. Meny, J. Montillaud, L. Pagani, D. Paradis, I. Ristorcelli, J. Malinen, L. Montier, R. Paladini, V.-M. Pelkonen, A. Rivera-Ingraham, 2015, A&A 584, A94, https://www.aanda.org/articles/aa/pdf/2015/12/aa25269-14.pdf • Modeling and predicting the shape of the far-infrared to submillimeter emission in ultra- compact HII regions and cold clumps, D. Paradis, C. Meny, A. Noriega-Crespo, R. Paladini, J.-P. Bernard, C. Bot, L. Cambrésy, K. Demyk, V. Gromov, A. Rivera-Ingraham, M. Veneziani, 2014, A&A 572, A37, https://www.aanda.org/articles/aa/pdf/2014/12/aa22566- 13.pdf • Modelling the dust emission from dense interstellar clouds: disentangling the effects of radiative transfer and dust properties, N. Ysard, M. Juvela, K. Demyk, V. Guillet, A. Abergel, J.-P. Bernard, J. Malinen, C. Mény, L. Montier, D. Paradis, I. Ristorcelli, L. Verstraete, 2012, A&A 542, A21, https://www.aanda.org/articles/aa/pdf/2012/06/aa18420- 11.pdf Research Group: Laboratory Astrophysics
Permanent staff: Le Picard Sébastien (coordinator), Benidar Abdessamad, Biennier Ludovic, Canosa André, Carles Sophie, Georges Robert, Sims Ian.
Technical staff: Courbe Jonathan, Thiévin Jonathan, Gallou Ewen, Dapp Alexandre, Biet Didier.
PhD students (since 2010): Gardez Aline, Roussel Vivien, Saidani Ghassen, Tizniti Meryem, Cheikh Sid Ely Sidaty, Suas-David Nicolas, Bourgalais, Jérémy, Jamal-Eddine Nour, Labiad Hamza, Durif Olivier, Fournier Martin
Post-docs (since 2010): Capron Mickael, Joalland Baptiste, Fournier Martin, Berteloite Coralie
Contact: Sébastien Le Picard
Laboratory: Institut de Physique de Rennes UMR CNRS 6251 Institution(s): Université Rennes 1 / CNRS Website: http:// ipr.univ-rennes1.fr
Key Research Facilities, Infrastructure and Equipment: CRESU reactors -Yag, Dye and Excimer pulsed Lasers - Mass spectrometers- CRDS- FTIR – High Enthalpy Source – Ion source – Flowing After Glow – Microwave Spectrometers
Keywords: Reaction dynamics, kinetics, spectroscopy, astrochemistry, molecular astrophysics, low temperatures, high temperatures, super and hypersonic flows.
Context: The Rennes group employs state of the art experimental techniques to understand the nature of molecules through their spectral signature, and their formation paths through their chemistry in astrophysical environments often characterized by extreme temperatures.
Experimental studies of the group: Low temperature ion-molecule and neutral- neutral reaction kinetics, low temperature collisional energy transfer, low temperature nucleation kinetics, low temperature chemical reaction branching ratio determination, dissociative recombination, high temperature infrared spectroscopy, infrared spectroscopy of transient species, spectroscopy of complex molecular systems and out-of-equilibrium
Collaborations: National: ENSCR ensc-rennes.fr/ - IPAG Grenoble ipag.osug.fr/ - LOMC Le Havre lomc.fr/ - ISM Bordeaux www.ism.u-bordeaux1.fr/ - SOLEIL St-Aubin www.synchrotron-soleil.fr/ - LIPhy Grenoble www-liphy.ujf-grenoble.fr/ - ICB Dijon icb.u-bourgogne.fr/ - IAS www.ias.u-psud.fr/ - GSMA Reims www.univ-reims.fr/gsma - PhLAM Lille www.phlam.univ-lille1.fr/ - MONARIS Paris www.monaris.cnrs.fr/
International: Unversity of Perugia, Department of Chemistry, Biology and Biotechnology (Italy) http://www.chm.unipg.it/ - University of Missouri, Dept. Chem. (USA) https://chemistry.missouri.edu/people/suits - Instituto de Ciencia de Materiales de Madrid (Spain) http://www.icmm.csic.es/ - University of Castilla-La Mancha, Departamento de Química Física, (Ciudad Real, Spain), https://www.uclm.es/departamentos/quimica-fisica - Université Libre de Bruxelles, Quantum Chemistry and Photophysics (Belgium) http://www.ulb.ac.be/cpm/ - Indian Institute of Science, Department of Inorganic and Physical Chemistry, Bangalore (India) http://ipc.iisc.ac.in/ - Argonne National Laboratory, Chemical Sciences and Engineering (USA), https://www.anl.gov/cse - NASA Ames Research Center, The Astrophysics and Astrochemistry Lab (Moffett Field, USA) http://www.astrochem.org/ - Lomonosov Moscow State University (Russia), http://www.msu.ru/en/ - University of West Virginia, Dept Chem (USA) https://www.wvu.edu/ Highlight: a better estimate of the mass of interstellar objects through the observation of HF
HF only occurs in space when a fluorine radical reacts with a H2 molecule. The Rennes team used the CRESU technique to measure the rate of the iconic HF formation reaction down to 11K. Computational chemists M. Alexander (Univ. of Maryland) and F. Lique (Univ. Le Havre) produced state-of-the-art quantum calculations. This combined work demonstrates, for the first time, that chemical reactions with barriers can have significant rates at temperatures as low as a few K. It also shows that first- principle quantum calculations of reaction rates at such low temperatures can be used for quantitative predictions. The amount of molecular hydrogen inferred from earlier observations of HF will have to be revised upwards. This work is a nice demonstration of how laboratory measurements of fundamental chemical processes can be critical to a proper understanding of the astrophysical universe.
The rate of the F + H2 reaction at very low temperatures, Meryem Tizniti, Sébastien D. Le Picard, François Lique, Coralie Berteloite, André Canosa, Millard H. Alexander, Ian R Sims, Nature Chemistry, 2014, 6 (2), pp.141-145. DOI : 10.1038/nchem.1835
Most significant publications (<5):
1 16 Nuclear Spin Symmetry Conservation in H2 O Investigated by Direct Absorption FTIR Spectroscopy of Water Vapor Cooled Down in Supersonic Expansion, Robert Georges, X. Michaut, A. Moudens, M. Goubet, O. Pirali, P. Soulard, P. Asselin, T. Huet, P. Roy, M. Fournier, A. Vigasin, Journal of Physical Chemistry A, 2017, 121 (40), pp.7455-7468. DOI : 10.1021/acs.jpca.7b06858
Low-Temperature Reactivity of C2n+1N- Anions with Polar Molecules, Baptiste Joalland, N. Jamal- Eddine, J. Kłos, F. Lique, Y. Trolez, J.-C. Guillemin, Sophie Carles, Ludovic Biennier, Journal of Physical Chemistry Letters, American Chemical Society, 2016, 7, pp.2957-2961. DOI : 10.1021/acs.jpclett.6b01191
Reactivity of OH and CH3OH between 22 and 64 K: Modelling the Gas Phase Production of CH3O in Barnard 1B, M. Antiñolo, M. Agúndez, Elena Jimenez, B. Ballesteros, André Canosa, Gisèle El Dib, J. Albaladejo, J. Cernicharo, Astrophysical Journal, American Astronomical Society, 2016, 823 (1), pp.25. DOI : 10.3847/0004-637X/823/1/25
Gas-phase infrared spectra of three compounds of astrochemical interest: vinyl, allenyl, and propargyl isocyanides., Abdessamad Benidar, Didier Bégué, Falk Richter, Claude Pouchan, Mohammed Lahcini, Jean-Claude Guillemin, ChemPhysChem, Wiley-VCH Verlag, 2015, 16 (4), pp.848-54. DOI : 10.1002/cphc.201402712
The rate of the F + H2 reaction at very low temperatures, Meryem Tizniti, Sébastien D. Le Picard, François Lique, Coralie Berteloite, André Canosa, Millard H. Alexander, Ian R Sims, Nature Chemistry, Nature Publishing Group, 2014, 6 (2), pp.141-145. DOI : 10.1038/nchem.1835
Link to full publication list: https://tinyurl.com/labastro-rennes-publications Research Group: CIRS-MASSIR Permanent staff: Mickaël guinet, David Jacquemart, Lahouari Krim Technical staff: Thierry Séropian, Mathilde Chaboud, Yann Berger, Gary Rose PhD students (since 2010): Claire Pirim (2008/2011), Prasad Joshi (2010/13), Nourry Sendres (2012/2015), Jonušas Mindaugas (20015/2018), Abraham Alejandro Vásquez Mencos (2015/2018), Killian Leroux (2018/2021) Contact: [email protected] Laboratory: Laboratoire MONARIS "de la Molécule aux Nano-objets : Réactivité, Interactions et Spectroscopies" Institution(s): Sorbonne université et CNRS Website: http://www.monaris.cnrs.fr/ Key Research Facilities, Infrastructure and Equipment: We are interested in the formation and characterization of complex organic molecules in solid phase and also in their evolutions at the solid-gas interface. The characterization of the solid phase reaction is carried out by IR spectroscopy while the desorbing species in the gas phase are analyzed by mass spectrometry, and they can also be characterized through high resolved infrared and terahertz spectroscopy. Our research in vibrational solid phase spectroscopy on the one hand and rotational and ro-vibrational gas phase spectroscopy on the other hand is based on three instrumental experimental setups using a high resolution IR spectrometer (10-3 cm-1) Brucker 125, a THz spectrometer (10-9 cm-1) designed and developed at MONARIS and the MASSIR setup for the solid phase reactivity (UHV 10 -10 mbar and cryogenic temperatures 3K). Keywords: VUV photolysis, Cryogenic temperatures, Interstellar ice analogs, Rare gas matrix isolation, Radicals, Atoms in ground and excited states, Plasma discharge, Solid and gas phase IR spectroscopy, THz spectroscopy, Mass spectrometry, Thermal processing. Astrophysical context and goals: - Formation of complex organic molecules in solid phase through atomic addition reactions and photochemical processing, and their evolutions at the solid-gas interface. - Links between laboratory experiment simulations and astronomical observations. Experimental studies of the group: Hydrogenation of CC and CO functional groups: CO + H, H2CO + H, CH3OCHO + H, 13 HC≡CCH2OH + H, HC≡CCHO + H, H2C=CH-CHO + H, H + O + C carbon grains,.... Radical reactions involving O, OH and NH radical and astrochemical species, NH3, CH4, H2O...
Solid phase chemistry of nitrogen atoms: N + N2, N + CO + H2O, N + CH4, N + CH3OH, N +
NH3, N + CH3CN. Solid state photo-induced reactions: CH3CN + HCOOH , NH3 + H2O, CH4 + H2O, NH3 + CH4 +
H2O. Collaborations: - Alexey Potapov, Max Planck Institute for Astronomy. - Jean-Claude Guillemin, Ecole Nationale Supérieure de Chimie de Rennes. - Manuel Yáñez and Al Mokhtar Lamsabhi, Universidad Autónoma de Madrid. - David Woon, University of Illinois. - Gianfranco Vidali, Syracuse University. Most significant publications (<5): Formation of ozone by solid state reactions, Lahouari Krim, Mindaguas Jonusas, Jean Louis Lemaire, Gianfranco Vidalia, 2018, PCCP, DOI: 10.1039/C8CP03020K Formation of doubly and triply bonded unsaturated compounds HCN, HNC, and CH2NH
via N + CH4 low-temperature solid state reaction: from molecular clouds to solar system objects, Alejandro Mencos, Lahouari Krim, 2018, MNRAS, DOI: 10.1093/mnras/sty609 Reduction of unsaturated compounds under interstellar conditions: chemoselective reduc- tion of C≡C and C=C bonds over C=O functional group, Mindaugas Jonusas Jean-Claude Guillemin Lahouari Krim, 2017, MNRAS, DOI: 10.1093/mnras/stx793 The Formation of Formaldehyde on Interstellar Carbonaceous Grain Analogs by O/H Atom Addition, Potapov Alexey, Jäger Cornelia, Henning Thomas, Jonusas Mindaugas, Krim Lahouari, 2017, Astrophys. J, DOI: 10.3847/1538-4357/AA85E8 The catalytic role of water in the photochemistry of ammonia ice: from diluted to concentrated phase, Mindaugas Jonusas, Lahouari Krim, 2017, MNRAS, DOI: 10.1093/mnras/stx1530 Research Group: Matrix team (Spectro Group at ISM Bordeaux)
Permanent staff: Joëlle Mascetti Technical staff: Christian Aupetit PhD students (since 2010): Post-docs (since 2010): Zohra Guennoun (2010), Jennifer Noble (2015-2016) Contact: [email protected]
Laboratory: Institut des Sciences Moléculaires UMR 5255 CNRS Institution(s): Université de Bordeaux Website: http://www.ism.u-bordeaux1.fr/spip.php?rubrique11
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: One experimental set-up with a cryogenic head (10K) and one home-made furnace for PAH and metal sublimation, one FTIR spectrometer Bruker V70V equipped with several sources, beamsplitters and detectors covering the NIR-MIR-FIR ranges, one UV-visible spectrometer Shimadzu, two irradiation lamps (Hg and Xe).
Keywords: Vibrational spectroscopy, UV-visible spectroscopy, matrix-isolation, PAH, water ice, iron, experimental laboratory astrophysics
Astrophysical context and goals: Chemistry of PAH in dense molecular clouds Depletion of iron in the gas phase of the ISM
Experimental studies of the group: PAH photo-oxidation in water ices and in argon matrices doped with water Organometallic chemistry of PAHs and water with iron
Collaborations: Dr Aude Simon, http://www.lcpq.ups-tlse.fr/spip.php?article1130 Prof. Céline Toubin, http://www.phlam.univ-lille1.fr/spip.php?article779 Dr Valérie Blanchet, http://www.celia.u-bordeaux1.fr/ Dr Christophe Jouvet, http://piim.univ-amu.fr/JOUVET-Christophe
Highlight:
Efficient photochemistry of coronene:water complexes. We recently demonstrated that small PAHs (such as pyrene or coronene) can easily undergo photoreactivity with small clusters of water rather than, as previously believed, uniquely in the presence of a water ice. This gives rise to the possibility of the formation of oxygenated PAH molecules (alcohols, ketones) in interstellar environments with low water abundances or onto grains in the absence of icy layers. Evolution of the FTIR spectrum of an irradiated coronene:water:argon matrix after irradiation times of one (blue), three (green) and eight (red) minutes. Photoproduct bands are observed at 1207, 1215 and 1221 cm-1.
Most significant publications (<5): Water Clusters in an Argon Matrix: Infrared Spectra from Molecular Dynamics Simulations with a Self-Consistent Charge Density Functional-Based Tight Binding/Force-Field Potential, A. Simon, C. Iftner, J. Mascetti, F. Spiegelman J. Phys. Chem. A 2015, 119, 2449-2467, DOI: 10.1021/jp508533k. Formation of coronene:water complexes: FTIR study in argon matrices and theoretical char- acterization, A. Simon, J. A. Noble, G. Rouaut, A. Moudens, C. Aupetit, C. Iftner and J. Mascetti, Phys. Chem. Chem. Phys. 2017, 19, 8516-8529, DOI: 10.1039/C6CP08559H
Photochemistry of Fe:H2O Adducts in Argon Matrices : A Combined Experimental and Theo- retical Study in the mid-IR and UV-Visible Regions, V. Deguin, J. Mascetti, A. Simon, N. Ben Amor, C. Aupetit, S. Latournerie, J. A. Noble, J. Phys. Chem. A 2018, 122, 529-542, DOI: 10.1021/acs.jpca.7b09681. Efficient photochemistry of coronene:water complexes, J. A. Noble, C. Jouvet, C. Aupetit, A. Moudens and J. Mascetti, Astron. Astrophys. 2017, 599, A124, DOI: 10.1051/0004-6361/201629613 Adsorption of PAHs on interstellar ice viewed by classical molecular dynamics, E. Michoulier, J. A. Noble, A. Simon, J. Mascetti, C. Toubin, PCCP 2018, 20, 8753-8764. DOI: 10.1039/C8CP00593A. Adsorption and ionisation energies of polycyclic aromatic hydrocarbons on water ice: compu- tational studies, E. Michoulier, N. Ben Amor, M. Rapacioli, J. A. Noble, J. Mascetti, C. Toubin and A. Simon, PCCP 2018, accepted manuscript, DOI: 10.1039/C8CP01175C.
Link to full publication list: http://www.ism.u-bordeaux.fr/spip.php?page=publications
Press releases: Research Group: ASTRO PIIM
Permanent staff: Fabien Borget, Thierry Chiavassa, Isabelle Couturier, Grégoire Danger, Fabrice Duvernay, Louis Le Sergeant d’Hendecourt, Nathalie Piétri, Patrice Theulé Technical staff: Gaël Roussin PhD students (since 2010): Jean-Baptiste Bossa, Teddy Butscher, Aurélien Fresneau, Florent Mispealer, Julie Mousay, Vassilissa Vinogradoff Post-docs (since 2010): Ninette Abu Mrad, Thomas Gautier, Jennifer Noble, Alexander Ruf Contact: [email protected]
Laboratory: Physique des Interactions Ioniques et Moléculaires Institution(s): Aix-Marseille University, CNRS Website: http://piim.univ-amu.fr/Equipe-ASTRO context/astrophysic problematic formation of Complex Organic Molecules in star forming regions astrochemical heritage from the dense ISM to planetary systems
Key Research Facilities, Infrastructure and Equipment: The group is equipped with 4 experimental set-ups: RING, AHIIA, MICMOC, CHARTS, each one of them including cryogenics heads (4K or 10 K), a Fourier-Transform Infra Red spectrometers equipped with different sources (water-cooled Hg lamp, Tg lamp, globar) and detectors (room temperature and N2-cooled detectors in the FIR, MIR and NIR ranges and a He-free bolometer for the FIR). An environmental cell (hight temperature and high pressure) may be fitted into the spectrometer to study samples annealed up to 800C under controlled atmosphere. Analytical systems such as GC-MS, GC-orbitrap and UHPLC-UV are also available for molecular characterization.
Keywords: Experimental laboratory astrophysics, solid-state chemistry, vibrational Spectroscopy, mass spectroscopy, Astrobiology, analytical chemistry
Experimental studies of the group: ice chemistry organic residue chemistry formation of complex organic molecules in space prebiotic chemistry: impact of exogenous organic matter in the emergence of life
Collaborations: Prof. Wolfram Sanders, http://www.ruhr-uni-bochum.de/oc2/wolfram_sander.html Dr Albert Rimola, http://grupsderecerca.uab.cat/getab/content/albert-rimola-i-gibert Dr Dahbia Talbi, http://www.lupm.univ-montp2.fr/ IPAG, http://ipag.osug.fr/ Dr Pauline Poinot IC2MP, Poitiers Dr Cornelia Meinert and Pr Uwe Meierhenrich, ICN, Nice Dr Rosario Brunetto and Zahia Djouadi, IAS, Paris Dr Olivier Mousis, LAM, Marseille
Highlight: (period: 2014-2018)
ESR spectroscopy in ice analogues
We recently demonstrated the possibility to use Electron Spin Resonance (ESR) spectroscopy to monitor open-shell molecules (radicals) chemistry at low-temperature in interstellar ice analogues. This technics is very promising to reveal atoms and radicals, which are involved in many elementary reactions of the solid-state chemical network, leading to the formation of interstellar complex organic molecules. This technique has enabled to infer which complex molecule is formed and which one not, under radical recombination. This shed light upon observation of complex molecules in different prestellar environments.
ESR spectrum of the VUV irradiation of CH3OH at 4 K. The experimental spectrum is compared with simulated spectra of CH3, HCO, CH2OH, CH3O radicals.
Most significant publications (<5): Formation mechanism of glycolaldehyde and ethylene glycol in astrophysical ices from • • HCO and CH2OH recombination: an experimental study, Butscher, T. et al. 2015, MNRAS, 10.1093/mnras/stv1706
Diffusion of molecules in the bulk of a low density amorphous ice from molecular dynamics simulations, Gesquière et al., 2015, PCCP, 10.1039/C5CP00558B
Radical-induced chemistry from VUV photolysis of interstellar ice analogues containing formaldehyde, Butscher et al., 2016, A&A, 10.1051/0004-6361/201628258
Radical recombination in interstellar ices, a not so simple mechanism, Butscher et al., 2017, PCCP, 10.1039/C6CP07024H
Reactivity in interstellar ice analogues: Role of the structural evolution, Ghesquière et al., 2018, A&A, 10.1051/0004-6361/201732288 The gaseous phase as a probe of the astrophysical solid phase chemistry. N. Abou Mrad, et al. The Astrophysical Journal, 2017, 846, 124. DOI : 10.3847/1538-4357/aa7cf0 Photo and thermochemical evolution of astrophysical ice analogs as a source of soluble and insoluble organic materials in Solar System minor bodies. P. de Marcellus, et al. Monthly Notices of the Royal Astronomical Society, 2017, 464, 114-120. DOI : 10.1093/mnras/stw2292
Other publications : http://piim.univ-amu.fr/Publications-456 Research Group: Reactivity on cold surfaces - LERMA
Permanent staff: F. Dulieu (PR), E.Congiu (MCF), (+ A. Moudens (MCF), V. Cobut) Technical staff: S. Baouche (IGR), S. Diana (I.E), F. Lachèvre (Tech). PhD students (since 2010): M. Accolla (2007-2010), M. Cherhouri (2007-2010), H. Mokrane (2007-2011),M. Minissale (2011-2014), H. Lemaître (2012-2015 (abandon)), T. Nguyen (2015-2018), A.S. Mohamed (2016-...), A. Sow (2016-...), M. Akel (2018-...) Post-docs (since 2010): K. Gaddallah (2018) Contact: [email protected]
Laboratory: LERMA (UMR 8112) Institution(s): Université de Cergy Pontoise, Sorbonne Université, Observatoire de Paris, ENS, PSL, CNRS Website: https://lerma.obspm.fr/spip.php?article48
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: 2 UHV Set-ups: FORMOLISM and VENUS. Keywords: Surface of grains, reactivity, desorption, diffusion. Astrophysical context and goals: How does evolve the molecular content at the surface of dust grains ? How is it coupled to the gas phase ?
Experimental studies of the group: Sticking and diffusion of H O and N atoms on ice, silicates and carbonaceous surfaces. Realistic desorption of mixed species. H2 formation and ortho to para conversion on grains. Chemical networks and others aspects (energetics) of the formation of molecules (H2O, CO2, H2CO, NH2OH, N2CHO, HNCO, CH2NC...)
Collaborations: C. Ceccarelli&P. Caselli (SOLIS); L. Pagani (LERMA); S. Morisset et al (ISMO); S. Cazaux (Delft U.), L. Kristensen (Copenhagen U. ), P. Theulé (Marseille U), JC Loison (Bordeaux)...
Highlight: Chemical desorption : How micron-sized dust particles determine the chemistry of our Universe. (see figure below) Most significant publications (<5): Minissale, M. et al., 2016. Dust as interstellar catalyst: I. Quantifying the chemical desorption process. Astronomy and Astrophysics, 585. Minissale, M., Congiu, E. & Dulieu, F., 2014. Oxygen diffusion and reactivity at low temperature on bare amorphous olivine-type silicate. The Journal of chemical physics, 140(7), p.074705. Available at: http://www.ncbi.nlm.nih.gov/pubmed/24559358 . Noble, J. a. et al., 2015. Hydrogenation at low temperatures does not always lead to saturation: the case of HNCO. Astronomy & Astrophysics, 576, p.A91. Available at: http://www.aanda.org/10.1051/0004-6361/201425403 . Dulieu, F., Minissale, M. & Bockelée-Morvan, D., 2017. Production of O2 through dismutation of H2O2 during water ice desorption: a key to understanding comet O2 abundances. Astronomy & Astrophysics, 597, p.A56. Available at: http://www.aanda.org/10.1051/0004-6361/201628445
Link to full publication list: https://www.u-cergy.fr/fr/laboratoires/lerma-cergy/liste-des-publications.html
Press releases: Research Group: Spectroscopy for Radio Astronomy - Toulouse
Permanent staff: Adam Walters Technical staff: PhD students (since 2010): Delong Liu (2015-); Aurélia Bouchez (2009-13) Post-docs (since 2010): Linh Nguyen (2011-2012) Contact: [email protected]
Laboratory: Institut de Recherche en Astrophysique et Planétologie. UMR 5277 (IRAP), Institution(s): Université de Toulouse 3, CNRS, OMP Website: http://www.irap.omp.eu/
Keywords: Rotational spectroscopy, microwave, terahertz, spectral analysis, laboratory astrophysics, complex organic molecules. Applications to radio-astronomy, ALMA, star-forming regions.
Astrophysical context and goals: To analyse laboratory spectra needed for the interpretation of spectral surveys of the interstellar medium in particular star-forming regions. To collaborate in radio-astronomical detection of newly characterized molecules. To make spectral data available, via databases, for astronomers.
Experimental studies of the group: Spectral measurements in the microwave and sub-millimetre bands taken at collaborating labs (mostly in Cologne).
Collaborations: Cologne Laboratory Astrophysics Group (Germany) - www.astro.uni-koeln.de/labastro. A. Belloche, Max Planck Institute for Radio Astronomy, Bonn (Germany) - www.mpifr-bonn.mpg.de/person/27759/765442.
Highlight: Laboratory spectroscopic study and astronomical detection of vibrationally excited n-propyl cyanide (n-PrCN). After analysis of the laboratory rotational spectra of 8 excited vibrational states of n-PrCN (4 for the anti conformer and 4 for the gauche) it was possible to identify all of them (Müller et al, 2016) in a spectral survey of the star forming region Sagittarius B2(N) taken using ALMA. As well as being an interesting spectroscopic problem (because of the vibrational coupling that may also serve to better determine the vibrational energy) there are several astrophysical interests. Firstly, this shows the sensitivity of ALMA in detecting many more types of molecular lines. Secondly, it is necessary to include in astrophysical modeling all the different lines of known species in order to look for new species in the remaining spectrum. Thirdly different types of transitions can be used to improve the physical and chemical models of the observed astrophysical object. For example, the emission caused by molecules in excited states may be used to infer the influence of (far-) infrared pumping.
This work followed on from the detection of isopropyl cyanide (i-PrCN) in the same object in 2014 by Belloche et al; the first branched molecule to be found in the ISM. Although we were not involved in the astrophysical detection cited we had previously participated in the laboratory analysis of the spectrum of isopropyl cyanide. The branched carbon structure of i-PrCN is a common feature in those molecules that are considered to be necessary for life – such as amino acids, adding weight to the search for the latter in star-forming regions. Recent and significant publications :
Laboratory spectroscopic study and astronomical detection of vibrationally excited n-propyl cyanide, H.S.P. Müller, A. Walters, N. Wehres, A. Belloche, O.H. Wilkins, D. Liu, R. Vicente, R.T. Garrod, K.M. Menten, F. Lewen, S. Schlemmer, Astron. Astrophys. 595 A87 26pp (2016). https://doi.org/10.1051/0004-6361/201629309 Exploring Molecular Complexity with ALMA (EMoCA): Alkanethiols and alkanols in Sagittarius B2(N2). H.S.P. Müller, A. Belloche, L-H. Xu, R.M. Lees, R.T. Garrod, A. Walters, J. van Wijngaarden, F. Lewen, S. Schlemmer, K.M. Menten, Astron. Astrophys., 587 A92 36 pp. (2016). https://doi.org/10.1051/0004-6361/201527470 Millimetre-wave spectrum of the singly deuterated isotopologues of anti-ethanol. A. Walters, M. Schäfer, M.H. Ordu, F. Lewen, S. Schlemmer, H.S.P. Müller, J. Mol. Spectrosc. 314, 6–12 (2015). https://doi.org/10.1016/j.jms.2015.05.005 The quest for complex molecules in space: Laboratory spectroscopy of n-butyl cyanide,
n-C4H9CN, in the millimeter wave region and astronomical search in Sagittarius B2(N). M.H. Ordu, H.S.P. Müller, A. Walters, M. Nuñez, F. Lewen, A. Belloche, K.M. Menten, S. Schlemmer, Astron. Astrophys. 541 A121 (2012). https://doi.org/10.1051/0004-6361/201118738 Rotational spectroscopy, dipole moment and 14N nuclear hyperfine structure of iso-propyl cyanide. H. S. P. Müller, A. Coutens, A. Walters, J-U. Grabow, S. Schlemmer, J. Mol. Spectrosc. 267, 100-107 (2011). https://doi.org/10.1016/j.jms.2011.02.011 Research Group: Spectro Lille
Permanent staff: S. Bailleux, F. L. Constantin, P. Dréan, M. Goubet, T. Huet, L. Margulès, R. Motiyenko, G. Wlodarczak Technical staff: PhD students (since 2010): S. Bteich, M. Chrayteh, I. Haykal, E. Neiman, A. Pienkina, O. Zakharenko Post-docs (since 2010): C. Bermudez Contact: [email protected]
Laboratory: Laboratoire PhLAM UMR CNRS 8523 Institution(s): Université de Lille – Faculté des Sciences et Technolgies Website: http://www.phlam.univ-lille1.fr/spip.php?article130
Key Research Facilities, Infrastructure and Equipment: * 2 supersonic jet beam Fourrier Transform Microwave Spectrometers (2-18 GHz) * 3 millimeter-submillimeter wave spectrometers: 1) inox cell, pyrex cell with avec in-situ pyrolysis, quartz and U.V. photolysis: from 75 to 1500 GHz based on two solid states frequency multiplication chains 2) Discharge cell (for radicals and ions): from 170 to 1100 GHz with solid states multipliers 3) Spectrometer with photomixing technique. It covers continuously the range 0.2-2 THz * High-performance computing cluster (~ 400 CPUs) with software relevant to molecular spectroscopy * High resolution FTIR spectrometer (20-4000 cm-1), coupled to (i) long pathlength cell or (ii) supersonic jet, on the AILES beamline at synchrotron facility SOLEIL (answer to call for proposal)
Keywords: Rotational spectroscopy, microwave, Terahertz, Laboratory astrophysics, Complex Organic Molecules, PAH
Experimental and theoretical studies of the group: • Complex Organic Molecules • Radicals, ions • PAH derivatives • Large amplitude motion • Variation and determination of fundamental constants
Collaborations: • P. Asselin, P. Soulard, Monaris Paris, http://www.monaris.cnrs.fr/fichiers/molecule_aux_agregats.html • A. Belloche, Max Planck Bonn (Allemagne), https://www.mpifr- bonn.mpg.de/person/27759/765442 • J. Cernicharo, CSIC Madrid (Espagne), https://nanocosmos.iff.csic.es/?page_id=27 • L. Coudert ISMO Orsay, http://www.ismo.u- psud.fr/spip.php?page=annuaire&id_individu=326 • R. Georges IPR Rennes, https://ipr.univ-rennes1.fr/interlocuteurs/robert-georges • V. Ilyushin, A. Alekseev, Kharkiv (Ukraine), http://quant.univer.kharkov.ua/en/sostav_en.htm • I. Kleiner, LISA Créteil, http://www.lisa.u-pec.fr/~kleiner/ • O. Pirali ISMO Orsay, http://www.ismo.u- psud.fr/spip.php?page=annuaire&id_individu=54 • H. Ozeki, Toho University (Japan) • T. Remijan, NRAO Charlottesville (USA), https://science.nrao.edu/about/scistaff • S. Schiller, University Düsseldorf, http://www.hhu.de/ • SOLEIL St-Aubin www.synchrotron-soleil.fr/
Highlight: Our recent works about hydroymethyl and methoxymethanol gave important information about astrochemistry models. • The non-detection of CH2OH (Bermudez et al., 2017, A&A, 598was a surprise, the upper limit to the column density of CH2OH of 1/1000 that of methanol. CH2OH was supposed to be major precursor of methanol in ISM. • The recent detection of methoxymethanol (B. A. Mc Guirre et al. 2018, ApJL, 851, 2) show it is ∼34 times less abundant than methanol (CH3OH), and significantly higher than predicted by astrochemical models
Most significant publications (<5): • Alma detection of interstellar methoxymethanol, B. A. Mc Guirre, C. N. Shingledecker, E. R. Willis et al. 2018, ApJL, 851, 2 10.3847/2041-8213/aaa0c3 • Rotational spectroscopy, tentative interstellar detection, and chemical modeling of N-methylformamide, A. Belloche, A. A. Meshcheryakov, R. T. Garrod et al. 2017, A&A, 601, A49, 10.1051/0004-6361/201629724 • Laboratory detection of the rotational-tunnelling spectrum of the hydroxymethyl radical, CH2OH, Bermudez et al 2017, A&A 598, A9, 10.1051/0004-6361/201629508 • Discovery of the ubiquitous cation NS+ in space confirmed by laboratory spectroscopy, Cernicharo et al 2018, ApJLett 853, 2, 10.3847/2041-8213/aaa83a • Sensitivity to proton-to-electron mass ratio variation from pairs of isotopic lithium hydride rotational and rovibrational transitions, F. L. Constantin 2015, J. Phys. B : At. Mol. Opt. Phys., 46 , art. no. 175006, 10.1088/0953-4075/48/17/175006
Link to full publication list: http://www.phlam.univ-lille1.fr/spip.php?article1163
Press releases: Research Group: Spins, Photons & Ices – SPICES – LERMA UMR 8112
Permanent staff: Xavier MICHAUT, Mathieu BERTIN, Géraldine FERAUD, Laurent PHILIPPE, Jean-Hugues FILLION Technical staff: Pascal Jeseck, Christian Rouillé, Patrick Marie-Jeanne PhD students (since 2010): Anica Lekic (2008-2012), Edith Fayolle (2009-2013), Micha Doronin (2012-2015), Rémi Dupuy (2016-), Thomas Putaud (2016-) Post-docs (since 2010): J Rakovsky (2013), A. Moudens (2011),A Gardez (2013), C. Romanzin (2010) Contact: [email protected]
Laboratory: Laboratoire d’Etudes du Rayonnement et de la matière en Astrophysique et Atmosphères. UMR 8112 du CNRS (LERMA). Institution(s): Observatoire de Paris & Sorbonne Université & CNRS Website: https://lerma.obspm.fr/spip.php?article47
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: The group is equipped with 2 experimental platforms, including 2 cryogenics heads (4K and 10 K), lasers (dye lasers, OPO), quadripolar mass spectrometers and high-resolution Fourier-Transform IR spectrometer. An Ultrahigh vacuum system dedicated to molecular processes at solid-gas interface is regularly coupled to the synchrotron SOLEIL facility (VUV DESIRS beamline & X SEXTANTS beamline) at St Aubin, France. Experiments with such a facility enable investigations of thermal and photon-induced desorption processes on thin condensed molecular layers.
Keywords: Experimental laboratory astrophysics, Ices; surface science; Photon-induced processes; Nuclear spin conversion; Temperature-induced processes.
Astrophysical context and goals: Understanding the origin of small organic molecules in cold and highly irradiated regions of the inter- stellar medium Interpretation of ortho-to-para ratio in photon-dominated region and in cometary atmospheres
Experimental studies of the group:
Nuclear Spin Conversion dynamics at low temperatures in solids and at surfaces UV and X-ray photodesorption from cold surfaces Temperature-Programmed-Desorption of molecular ices
Collaborations: -Laboratoire de Chimie Théorique (SU, Paris) : A. Markovits et al. http://www.lct.jussieu.fr/ -European Organization for Nuclear Research (CERN), Surfaces & Coatings Group , Technology Department V. Baglin et al. https://home.cern/about/engineering/vacuum-empty-interstellar-space -Laboratoire de Chimie-Physique d’Orsay : C. Romanzin http://www.lcp.u-psud.fr/spip.php?rubrique83 -Observatoire de Leiden : H. Linnartz et al https://www.universiteitleiden.nl/en/research/research-facilities/science/sackler-laboratory-for-astrophysics -University of Manchester : Sven Khoeler https://www2.mmu.ac.uk/sste/ -Laboratoire MONARIS « De la Molécule aux Nano-Objets : Réactivités, Interactions et Spectroscopies (SU, Paris) : P. Asselin, B. Tremblay, P. Soulard http://www.monaris.cnrs.fr/ -Institut de Physique de Rennes : R. Georges et al https://ipr.univ-rennes1.fr/ - Laboratoire de physique des Lasers, Atomes et molécules : équipe théorique M. Monnerville, C. Toubin et al. http://www.phlam.univ-lille1.fr/spip.php?article127 - Laboratoire de physique des Lasers, Atomes et molécules : équipe expérimentale M. Goubet, T. Huet http://www.phlam.univ-lille1.fr/spip.php?article731 -Institut des Sciences Moléculaires d’Orsay : O. Pirali ; A. Lafosse http://www.ismo.u-psud.fr/ -Ligne Infrarouge AILES du synchrotron SOLEIL : P. Roy https://www.synchrotron-soleil.fr/fr/lignes-de-lumiere/ailes - Université de Sherbrooke, P. Ayotte et al. https://www.usherbrooke.ca/sciences/personnel/chimie/professeurs/professeurs/patrick-ayotte/
Highlight (period 2014-2018): X-ray Photodesorption of water ice
Photodesorption induced by soft X-rays photons has been investigated with the SPICES instrument installed at the national synchrotron facility SOLEIL. Ions and neutral particles desorption from amorphous solid water has been investigated at 15 K and 90 K. Desorption yields of neutral species were for the first time measured experimentally. In particular, photodesorption of intact H2O has been found two orders of magnitude higher than the desorption of H+, the most abundant ion, which should affect significantly the gas-to-ice ratio in X-ray irradiated regions of the interstellar medium such as the surface of propotoplanetary disks (paper recently accepted for publication in nature Astronomy)
Most significant publications (<5): Robert Georges, Xavier Michaut, Audrey Moudens, Manuel Goubet, Olivier Pirali, Pascale Soulard, Pierre Asselin, Thérèse Huet, Pascale Roy, Martin Fournier, and Andrey Vigasin Nuclear Spin Symmetry Conservation in 1 16 H2 O Investigated by Direct Absorption FTIR Spectroscopy of Water Vapor Cooled Down in Supersonic Expansion J. Phys. Chem. A 121, 7455-7468 (2017) Turgeon P.-A., Vermette J., Alexandrowicz G., Peperstraete Y., Philippe L., Bertin M., Fillion J.-H., Michaut X. & Ayotte P. Confinement Effects on the Nuclear Spin Isomer Conversion of H2O Journal of Physical Chemistry A 121, 1571-1576 (2017)
Dupuy R., Bertin M., Féraud G., Michaut X., Jeseck P., Doronin M., Philippe L., Romanzin C., & Fillion J.-H.Spectrally-resolved UV photodesorption of CH4 in pure and layered ices Astronomy & Astrophysics 603, A61 (2017)
Bertin M., Doronin, M., Michaut X., Philippe L., Fillion J.-H., Markovits A., Pauzat F., Ellinger Y. & Guillemin J.-C. Nitrile versus isonitrile adsorption at interstellar grains surfaces. II. Carbonaceous aromatic surfaces Astronomy & Astrophysics (2017)
M. Bertin, C. Romanzin, M. Doronin, L. Philippe, N. Ligterinks, H. Linnartz, X. Michaut, & J.-H. Fillion, UV photodesorption of methanol in pure and CO-rich ices: desorption rates of the intact molecule and of the photofragments, The Astrophysical Journal Letters 817 (2016), L12
Link to full publication list: https://lerma.obspm.fr/spip.php?article154 Research Group: SMAE_VUV
Permanent staff: S. Boyé-Péronne, B. Gans Technical staff: PhD students (since 2010): N. Lamarre, O. Harper Post-docs (since 2010): aucun Contact: [email protected], [email protected]
Laboratory: Institut des Sciences Moléculaires d’Orsay Institution(s): CNRS, Université Paris Sud, Université Paris Saclay Website: http://www.ismo.u-psud.fr
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: Nanosecond pulsed lasers (from IR to VUV), mass spectrometer, photoelectron spectrometer, molecular beam, radical sources (discharge, pyrolysis, flow tube,…)
Keywords: Photoelectron, photoion, high-resolution VUV laser, synchrotron radiation, radical, rovibronic spectroscopy, astrophysical media.
Astrophysical context and goals: The VUV irradiation (λ < 200 nm) of the gas phase leads to different kind of relaxation processes which produce very reactive species (radicals and ions). This irradiation is thus one of the primary steps of the complex photochemistry which occurs in astrophysical media (molecular clouds, planetary atmospheres, coma of comets). Our research is thus mainly focused on the processes linked to the VUV irradiation (absorption, photodissociation, ionization or dissociative ionization) of molecules and radicals of astrophysical interest.
Experimental studies of the group: Measurements of data for photochemical models (absorption and ionization cross sections, branching ratios, ionization thresholds,…) Rovibronic spectroscopy of cations: photoelectron spectroscopy (with lasers or synchrotron) of molecules and free radicals
Collaborations: J.-C. Loison, ISM, VUV spectroscopy of radicals S. Pratt, Argonne National Laboratory, VUV spectroscopy of hydrocarbons and radicals DESIRS beamline of SOLEIL, VUV spectroscopy of radicals J.-C. Guillemin, molecular synthesis J. Liévin, ULB, ab initio calculations Highlight: Unveiling the Ionization Energy of the CN Radical. Photoionization transitions of the CN radical have been measured for the first time using a flow-tube reactor and the DELICIOUS III spectrometer of the DESIRS beamline at SOLEIL. ( GANS et al. JPCL, 8 , 4038 (2017), actualités SOLEIL) Most significant publications (<5): High-resolution one-photon absorption spectroscopy of the D 2Σ− ← X 2Π system of radical OH and OD, A.N. Heays, N. de Oliveira, B. Gans, K. Ito, S. Boyé-Péronne, S. Douin, K.M. Hickson, L. Nahon, J.C. Loison, 2018, Journal of Quantitative Spectroscopy & Radiative Trans- fer, doi: 10.1016/j.jqsrt.2017.08.021 Unveiling the Ionization Energy of the CN Radical, B. Gans, S. Boyé-Péronne, G. A. Garcia, A. Röder, D. Schleier, P. Halvick, and J.-C. Loison, 2017 The Journal of Physical Chemistry Letters, doi: 10.1021/acs.jpclett.7b01853 + Experimental and ab initio characterization of HC3N vibronic structure. II. High- resolu- tion VUV PFI-ZEKE spectroscopy, B. Gans, N. Lamarre, M. Broquier, J. Liévin, and S. Boyé-Péronne, 2016, The Journal of Chemical Physics, doi: 10.1063/1.4972018 Photolysis of methane revisited at 121.6 nm and at 118.2 nm: quantum yields of the prima- ry products, measured by mass spectrometry, B. Gans, S. Boyé-Péronne, M. Broquier, M. Delsaut, S. Douin, C. E. Fellows, P. Halvick, J.-C. Loison, R. R. Lucchese, and D. Gauyacq, 2011, Physical Chemistry Chemical Physics , doi: 10.1039/c0cp02627a
Link to full publication list: http://www.ismo.u-psud.fr/spip.php?article1878
Press releases: Actualités du synchrotron SOLEIL: Potentiel d’ionisation du radical cyano et implications pour la chimie du cation CN+ dans l’espace Link : https://www.synchrotron-soleil.fr/fr/actualites/potentiel-dionisation-du-radical-cyano-et-implications-p our-la-chimie-du-cation-cn-dans 1.3 Theory
57 Research Group: Chimie Théorique Permanent staff: Majdi Hochlaf, Roberto Linguerri, Halima Mouhib et Gilberte Chambaud Technical staff: - PhD students (since 2010): Yosra Ajili (2011-2014), Mohamed Achref Gannouni (2011-2014), Yosra Tabai (2011-2015), Ayad Bellili (2013-2017), Tarek Trabelsi (2013-2016), Khaled Mahjoubi (2013-2016), Onsi Sghaier (2013-2018), Sameh Nasri (2013-2016), Tarek Ayari (2013-2017), Asma Sanaa Zaag (2013-2017), Mohamed Cheraki (since 2016), Imen Derbeli (since 2018). Post-docs (since 2010): Mohamed Achref Gannouni (2015-2016), Tarek Trabelsi (since 2016) Contact: [email protected]
Laboratory: Modelisation Simulation et Modélisation Multi Echelle (MSME) – UMR 8208 Institution(s): U. Paris-Est Marne-La-Vallée Website: http://msme.u-pem.fr
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: • Small clusters • Software: Hibridon, MOLSCAT, MOLPRO, GAUSSIAN, CP2K, VASP • Home made code for studying the nuclear motions of molecules and their spectroscopy (rovibronic, electronic, …)
Keywords: Laboratory astrophysics, astrochemistry, interstellar medium, spectroscopies, synchrotron radiation based spectroscopies
Astrophysical context and goals: • Spectroscopic (vibrational, rotational, electronic, photoelectronic) characterization of molecules and clusters and in interaction with substrats (surfaces or aggregates or matrices). • Determination of the chemical mechanisms and explanation of the complexity in the ISM • Reactive and non-reactive collisions under the astrophysical ISM conditions
Experimental studies of the group: Synchrotron photoelectron spectroscopy of prebiotic molecules Unimolecular decomposition of molecules after XUV photoionization Microwave spectroscopies of complex molecules
Collaborations: M. Schwell, I. Kleiner, L. Nguyen, Y. Bénilan, N. Fray, M.-C. Gazeau, Université Paris-Est Créteil (France) T. Stoecklin, P. Halvick, Université de Bordeaux (France) A. Faure, Observatoire de Grenoble (France) F. Lique, Université du Havre (France) G. A. Garcia, L. Nahon, Synchrotron Soleil (France) C. Puzzarini, University of Bologna (Italy) Y. Ajili, Ben Yaglane, K. Hammami, D. Ben Abdallah, N. E. Jaidane, Faculté des Sciences de Tunis (Tunisie) K.-C. Lau, City University of Hong Kong (Chine) J. S. Francisco, University of Nebraska (USA) C.-Y. Ng, W. Jackson, University of Davis in California (USA) O. Denis-Alpizar, Universidad Autónoma De Chile (Chili) M. Mogren Al Mogren, King Saud University (Saudi Arabia)
Highlight: Toward the computations of accurate spectroscopic, thermochemical and dynamical properties of astrophysical relevant molecular systems. Full understanding of the spectroscopy and the dynamical behavior of molecular systems of astrophysical interest, either strongly or weakly bound needs, at first glance, the full exploration of their global multidimensional potential energy surfaces (PESs). These species can be in their electronic ground and/or electronically excited states. These PESs should cover the molecular regions where (meta)stable isomers can be located, the regions of the potential barriers (isomerization) and the asymptotic regions leading to fragmentation. These PESs should be mapped using accurate ab initio post Hartree–Fock methodologies after considering effects beyond the Born–Oppenheimer (BO) approximation such as relativistic, nonadiabatic and quantum electrodynamic (QED) effects. In the last decade, we developed composite schemes based on the use of explicitly correlated methods. These schemes are viewed as the method of choice for effective and accurate predictions, for the mapping of multi-dimensional PESs and for the determination of the rotational, vibrational and energetic properties of medium-sized molecular species and of their thermochemical properties.
Most significant publications (<5): Y. Ajili, K. Hammami, N. E. Jaidane, M. Lanza, Y. N. Kalugina, F. Lique and M. Hochlaf. "On the accu- racy of explicitly correlated methods to generate potential energy surfaces for scattering calculations and clustering: application to the HCl–He complex". Phys. Chem. Chem. Phys. 15, 10062 (2013). Invited ar- ticle: Themed issue Spectroscopy and dynamics of medium-sized molecules and clusters: Theory, experiment and applications. M. Schwell and M. Hochlaf. "Photoionization spectroscopy of nucleobases and analogues in the gas phase using synchrotron radiation as excitation light source". Photoinduced phenomenain nucleic acids I: Nucleobases in the gas phase and in solvants. Edited by M. Barbatti, A. C. Borin and S. Ullrich, Book Series: Topics in Current Chemistry 355, 155 (2015). Invited revue. Y. Song, H. Gao, Y. Chung Chang, D. Hammoutène, H. Ndome, M. Hochlaf, W. M. Jackson and C. Y. Ng. "Quantum-State-Dependence of Product Branching Ratios in Vacuum Ultraviolet Photodissociation of N2". ApJ 819, 23 (2016). T. Stoecklin, P. Halvick, M. A. Gannouni, M. Hochlaf, S. Kotochigova and E. R. Hudson. "Explanation of efficient quenching of vibrational motion with ultracold atoms". Nature Communications 7, 11234 (2016). M. Hochlaf. "Advances in spectroscopy and dynamics of small and medium sized molecules and clus- ters". Phys. Chem. Chem. Phys. 19, 21236 (2017). Invited perspective Link to full publication list: http://msme.u-pem.fr/equipe-chimie-theorique/ct/hochlaf-majdi/ Press releases: http://www.cnrs.fr/inc/communication/direct_labos/poisson.htm http://www.insu.cnrs.fr/node/4409 http://www.cnrs.fr/inc/communication/direct_labos/stoecklin.htm http://iramis.cea.fr/Phocea/Vie_des_labos/Ast/ast.php?t=fait_marquant&id_ast=2702 Couvertures et Faits Marquants
PCCP back cover : Inside cover: Catalysis PCCP front cover : J. Phys. Chem. A front Phys. Chem. Chem. Science and Phys. Chem. Chem. cover : DOI: Phys. 18, 30205 Technology, 2017, 7 Phys. 15, 9949 (2013). 10.1021/acs.jpca.5b12135 (2016). (10), pp.2012.
PCCP front cover : PCCP back cover : Phys. Inside Cover Phys. Chem. Chem. Chem. Chem. Phys. 19, ChemPhysChem. Phys. 19, 8152 (2017). 21236 (2017). 2017, 18(14), 1855-1859.
M. Briant, L. Poisson, M. Hochlaf, P. de Pujo, M.-A. Gaveau et B. Soep. "Ar2 Photoelectron Spectroscopy Mediated by Autoionizing States". Phys. Rev. Letters 109, 193401 (2012). Fait marquant UPEM, CEA, CNRS et Synchrotron Soleil. http://www.cnrs.fr/inc/communication/direct_labos/poisson.htm
C. Sanloup, S. A. Bonev, M. Hochlaf et H. E. Maynard-Casely. "Reactivity of Xenon with Ice at Planetary Conditions". Phys. Rev. Letters 110, 265501 (2013). Fait marquant UPEM, CNRS et Synchrotron ESRF. http://www.insu.cnrs.fr/node/4409 A. Trabattoni, M. Klinker, J. González-Vázquez, C. Liu, G. Sansone, R. Linguerri, M. Hochlaf, J. Klei, M. J. J. Vrakking, F. Martín, M. Nisoli et F. Calegari. "Mapping the dissociative ionization dynamics of molecular nitrogen with attosecond time resolution". Phys. Rev. X 5, 041053 (2015). Fait marquant UPEM et CNRS. http://www.cnrs.fr/inc/communication/direct_labos/hochlaf.htm
T. Stoecklin, P. Halvick, M. A. Gannouni, M. Hochlaf, S. Kotochigova et E. R. Hudson. "Explanation of efficient quenching of vibrational motion with ultracold atoms". Nature Communications 7, 11234 (2016). Fait marquant UPEM, U. Bordeaux et CNRS. http://www.cnrs.fr/inc/communication/direct_labos/stoecklin.htm
Z. Chen, K.-C. Lau, G. A. Garcia, L. Nahon, D. K. Božanić, L. Poisson, M. Mogren Al-Mogren, M. Schwell, J. S. Francisco, A. Bellili et M. Hochlaf*. "Identifying cytosine-specific isomers via high-accuracy single photon ionization". J. Am. Chem. Soc. 138, 16596 (2016). Communication. Fait marquant Synchrotron SOLEIL et CEA. http://iramis.cea.fr/Phocea/Vie_des_labos/Ast/ast.php? t=fait_marquant&id_ast=2702 Research Group: Structure and Reactivity in astrophysics
Permanent staff: F. Aguillon, S. Morisset, N. Rougeau, D. Teillet-Billy (retired in 2017) Contact: [email protected]
Laboratory: ISMO Institution(s): Université Paris-Sud, CNRS Website: http://www.ismo.u-psud.fr
Key Research Facilities, Infrastructure and Equipment: Cluster for calculations
Keywords: PAH (Polycyclic Aromatic Hydrocarbons) reactivity : hydrogenation or oxygenation of PAH and PAH cation; H2 formation mechanisms; Addition mechanisms; Fragmentation channels.
Astrophysical context and goals: In the interstellar medium (ISM), molecules such as OH, H2 or more complex molecules are known to be form on interstellar dust grains or on smaller structures such as PAH. The objective is to study the reactivity of PAH with H or O atoms. The competition between the H or O addition, the abstraction of H2 or OH and the fragmentation channels are studied.
Collaborations: S. Cazaux (Delft University) F. Dulieu (LERMA) D. Pelaez-Ruiz (PHLAM)
Highlight: Sequence of complete hydrogenation of coronene cation
Most significant publications (<5): "H2 formation on interstellar dust grains: the viewpoints of theory, experiments, models and observations", V. Wakelam, E. Bron, S. Cazaux, F. Dulieu, C. Gry, P. Guillard, E. Habart, L. Hornekaer, S. Morisset, G. Nyman, V. Pirronello, S.D. Price, V. Valdivia, G. Vidali, N. Watanabe; Molecular Astrophysics, 2017, 9, 1-36 "Influence of a graphene surface on the first steps of the hydrogenation of a coronene molecule", S. Morisset, N. Rougeau, D. Teillet Billy, Chem. Phys. Lett., 2017, 679, 225 “The sequence to hydrogenate coronene cations: A journey guided by magic numbers.”, S. Cazaux, L. Boschman, N. Rougeau, G. Reitsma, R. Hoekstra, D. Teillet Billy, S. Morisset, M. Spaans, and T. Schlatholter, Scientific Reports, 2016, 6 19835
Link to full publication list: http://www.ismo.u-psud.fr/spip.php?rubrique238
Research Group: Space Chemistries: from the ISM to the planet Earth
Permanent staf: Alexis Markovits, Isabelle Fourré, Olivier Parisel, François Volatron, Franck Fuster, Françoise Pauzat, Yves Ellinger Technical staf: Marie-France Couret, Antoine Loret PhD students (since 2010): Gaël Marloie (2008-2011), Amélie Pernet (2010-2013), Eléonore Zicler (2011-2014), Mikhail Doronin (2012-2015), Ozge Ozgurel (2014-2017) Contact: [email protected] Laboratory: Laboratoire de Chimie théorique (LCT), UMR 7616. Institution(s): Sorbonne Université/CNRS Website: http://www.lct.jussieu.fr
Astrophysical context and goals The molecular data necessary for astrochemical models are provided by chemical computations altogether with molecular experiments. The interstellar molecules having interacted with dust or grains (covered with ices or bare according the environment) throughout their history, gas phase chemistry, solid phase chemistry and catalysis chemistry are to be considered. Using quantum chemistry methods, and implementing gas phase modeling and solid modeling, we investigate reactive and non-reactive processes, mainly aiming at: Help for detection of molecules in the ISM Prebiotic chemistry: origin of Chirality and synthesis of prebiotic species Understanding and rationalizing adsorption/desorption of molecules on interstellar surfaces Reactivity with and within water ices.
Keywords: Computational astrochemistry, electronic structure calculations, gas phase reactivity, solid gas interactions, reactivity in ices, exobiology.
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools Computing facilities: JARVIS-BETA (1200 processors owned by the laboratory, out of which 200 are devoted to the group). Free access to ~1000 processors of JARVIS-ALPHA owned by the IP2CT federation the laboratory belongs to. Numerical tools: Apart some house codes, the codes available in the laboratory are, for ab initio electronic calculations GAMESS, ALCHEMY, MOLPRO, GAUSSIAN, CRYSTAL, VASP, for Molecular Dynamic simulations PINY, QUANTUM EXPRESSO, VENUS.
Collaborations Laboratoire d’Etudes du Rayonnement et de la matière en Astrophysique et Atmosphères (Sorbonne Université et Observatoire de Paris, CNRS, Paris): Jean-Hugues Fillion and Mathieu Bertin https://lerma.obspm.fr/spip.php?article47 Institut des sciences Chimiques de Rennes (Université de Rennes, CNRS, Rennes) : Jean-Claude Guillemin https://iscr.univ-rennes1.fr/corint/-322 Laboratoire d’Astrophysique de Marseille (Aix-Marseille Université, Marseille) : Olivier Mousis https://www.lam.fr Institut Lumière Matière (Université Claude Bernard Lyon 1, CNRS) : Marie-Christine Bacchus-Montabonnel http://ilm.univ-lyon1.fr/index.php Institut des sciences moléculaires (Université de Bordeaux, CNRS, Bordeaux) : Thierry Stoecklin http://www.ism.u-bordeaux.fr/spip.php?rubrique71 Institut de Planétologie et d’Astrophysique de Grenoble (Université de Grenoble Alpes, CNRS) Cecillia Ceccarelli http://ipag.osug.fr/ Computational Chemistry group (Universidad de Valladolid, Spain): Pilar Redondo http://albergueweb1.uva.es/ccg/group.html Center for Astrophysics and Planetary Science, Cornell University (Ithaca, USA): Jonathan Lunine http://astro.cornell.edu/ccaps.html Department of Space Research, Southwest Research Institute, (San Antonio, TX, USA): Alexis Bouquet, Kathlyn Mandt , Adienn Luspay-Kuti https://www.swri.org/ Institut de mineralogie, physique des matériaux et cosmologie, (MNHN et Sorbonne Université) : B. Zanda http://www.impmc.upmc.fr/fr/index.html
Highlight
Observations of O2 in comet 67/P by the Rosetta mission raised multiple questions still under debate. We proposed a full scenario on chemical grounds: going from the in-depth irradiation of the icy interstellar grains in the ISM by cosmic rays creating latent tracks
where the irradiation fragments H, OH,O can recombine to form O2 encapsulated in cavities inside the ice. Using “first principle“ solid
state quantum simulations we were able to show that O2 and even
O2 dimers are stable in the ice until they are co-released with their
neighbor H2O molecules by erosion of the comet surface. From our simulations we could also deduce the ratio between the correlated
emissions of O2 and H2O, in accordance with the observations.
Alerte presse CNRS INSU (2 Juin 2016) « origine de l’oxygène de la comète -7P/Churyumov-Gerasi- menko dévoilée » http://www.insu.cnrs.fr/node/5842
Latest most significant publications On the gas-phase formation of the HCO radical: accurate quantum study of the H plus CO radiative association :Stoecklin, T. ; Halvick, P. ; Yu, HG ; Nyman, G.; Ellinger, Y.; MNRAS, 475,2, 2545-2552 (2018) DOI: 10.1093/mnras/stx3348 Nitrile versus isonitrile adsorption at interstellar grains surfaces II. Carbonaceous aromatic surfaces M. Guillemin. Astron. Astrophys., 608, A50 (2017). http://dx.doi.org/10.1051/0004-6361/201731144 Nitrile versus isonitrile adsorption at interstellar grains surfaces.I. Hydroxylated surfaces Bertin, M.; Doronin, M.; Fillion J.-H.; Michaut, X.; Philippe, L.; Lattelais, M.; Markovits, A.; Pauzat, F.; Ellinger, Y.; Guillemin, J.-C. Astron. Astrophys., 598, A18 (2017). DOI: 10.1051/0004-6361/201629394 Origin of molecular oxygen in comet 67P/Churyumov-Gerasimenko : Mousis, O.; Ronnet, T.; Brugger, B.; Ozgurel, O.; Pauzat, F.; Ellinger, Y.; Maggiolo, R.; Wurz, P.; Vernazza, P.; Lunine, J. I.; Luspay-Kuti, A.; Mandt, K. E.; Altwegg, K.; Bieler, A.; Markovits, A.; Rubin, M.; ApJ. Lett., 823, L41 (2016). DOI: 10.3847/2041-8205/823/2/L41 About the detection of urea in the interstellar medium: the energetic aspect: Fourre, I. ; Rosset, L.; Chevreau, H.; Ellinger, Y.; Astron. Astrophys., 589, A18 (2016). DOI: 10.1051/0004-6361/201527537 The composition of the protosolar disk and the formation conditions for comets: Willacy, K.; Alexander, C.; Ali-Dib, M.; Ceccarelli, C.; Charnley, S.B.; Doronin, M.; Ellinger, Y.; Gast, P.; Gibb, E.; Milam, S.N.; Mousis, O.; Pauzat, F.; Tornow, C.; Wirström, E.S.; Zicler E.; Space Sci. Rev., 197, 151 (2015). DOI : 10.1007/s11214-015-0167-6 Link to full publication list: http://www.lct.jussieu.fr
Research Group: Reactive processes
Permanent staff: François Lique, Fabien Dumouchel, Ioan Schneider Technical staff: - PhD students (since 2010): Sebastien Niyonzima (2010-2013), Mathieu Lanza (2011-2014), Mario Hernandez Vera (2012-2014), Nezha Bouhafs (2014-2017), Ragav Ramachandran (since 2016), Abdillah Aboulanziz (since 2017) Post-docs (since 2010): Yulia Kalugina (2011-2013), Janos Zsolt Mezei (2011-2016), Sidaty Cheikh Sid Ely, Kyle Walker (2015-2017), Fidel Batista Romero (2017), Vincenzo Laporta (since 2017), Jérôme Loreau (2017-2018), Nezha Bouhafs (since 2017). Contact: [email protected]
Laboratory: Laboratoire Ondes et Milieux Complexes (LOMC) – UMR6294 Institution(s): Université Le Havre Normandie Website: http://www.lomc.fr
Key Research Facilities, Infrastructure and Equipment: • Small clusters • Software: Hibridon, MOLSCAT, MOLPRO • Home made code for studying the inelastic and reactive collisions
Keywords: Laboratory astrophysics, astrochemistry, interstellar medium
Astrophysical context: • Modelling of the observations provided by terrestrial and space-based observatories • Determination of the most accurate census of the molecular content and complexity in the ISM • Formation and destruction of interstellar molecules (including the complex cones)
Studies of the group: - • Inelastic collisions between interstellar molecules/ions and H2/He/H/e • Chemical reactivity (bimolecular reaction and dissociative recombination) • Spectroscopy
Collaborations: • N. Feautrier, C. Balança, F. Dayou, L. Pagani, E. Roueff, M. Gérin, Observatoire de Paris (France) • T. Stoecklin, P. Halvick, C. Naulin, A. Bergeat, Université de Bordeaux (France) • M. Hochlaf, Université Paris Est Marne la Vallée (France) • A. Faure, C. Rist, C. Ceccarelli, A. Bacman, P. Hily-Blant, Observatoire de Grenoble (France) • P. Honvault, Université de Dijon (France) • I. R. Sims, S. D. Le Picard, L. Biennier, S. Carles, R. Georges, Université de Rennes (France) • M. H. Alexander, J. Klos, Universiy of Maryland (USA) • P. J. Dagdigian, Johns Hopkins University, Baltimore (USA) • R. Dawes, Missouri University of Science and Technology (USA) • S. Y. T. van de Meerakker, D. H. Parker, Nijmegen University (Netherlands) • O. Roncero, J. Cernicharo, M. Agundez, CSIC, Madrid (Spain) • D. Talbi, Y. Scribano, Université de Montpellier (France) • L. Pagani, E. Roueff, M. Gérin, B. Godard, Observatoire de Meudon (France) • F. F. S. van de Tak, University of Groningen (Netherlands) • C. Coppola, Bari University (Italy) • O. Dulieu, Université Paris 11 (France)
Highlight: Toward the convergence of theory and experiments in scattering studies Collisional rate coefficients are required for accurate determination of the physical conditions in interstellar molecular clouds. We have been able to compute highly accurate data for inelastic collisions implying interstellar molecules and the most abundant collisional partners in the ISM. The theoretical calculations were able to reproduce the details seen in the experiments as can be seen in the Fig. 1, where theoretical excitation cross-sections of O2 by H2 perfectly match with the experimental data. Such agreement shows that we can now be really confident in the accuracy of nowadays calculations and that the present molecular data allow making the most of the observations provided by nowadays terrestrial and space-based observatories.
10 (a) ) 2
(a.u.) (b) (nm exp
0,1 th 5 ICS
ICS (c)
0 0,0 0 5 10 15 20 25 -1 Relative translational energy (cm ) Fig. 1: O2(N=1, j=0)+p-H2 → O2(N=1, j=1)+p-H2:
Fig. 1. CollisionalExperiments energy (open dependence circles); of theorythe integral (solid cross line) sections for O2 excitation (N = 1, j =
Most significant publications0) → (N: = 1, j = 1). Experimental data with para-H2 (open circles); theoretical ICSs convoluted Spin-orbit relaxation of O(3P ) induced by collisions with He, H and H F. Lique, J. Kłos, M. H. • with the experimentalj collision energy spread (solid line). 2, Alexander, S. D. Le Picard and P. J. Dagdigian, 2018, MNRAS 474, 2313 • An efficient statistical method to compute molecular collisional rate coefficients, J. Loreau, F. Lique and A. Faure, 2018, ApJL 853, L5 • The rotational excitation of the HCN and HNC molecules by H2 revisited, M. Hernandez Vera, F. Lique, F. Dumouchel, P. Hily-Blant and A. Faure, 2018, MNRAS 468, 1084 (2017) - • Inelastic Rate Coefficients for Collisions of C6H with H2 and He, K. M. Walker, F. Lique, F.
Dumouchel and R.10 Dawes, 2017, MNRAS 466, 831 • A theoretical study of the dissociative recombination of SH+ with electrons through the 2Π states
of SH, D. O. Kashinski, (a.u.) D. Talbi, A. P. Hickman, O. E. Di Nallo, F. Colboc, K. Chakrabarti, I. F. Schneider and J.exp Zs. Mezei, 2017, J. Chem. Phys. 146, 204109 ICS 5
Press releases: http://www.insu.cnrs.fr/node/8262 http://www.cnrs.fr/inp/IMG/pdf/14_02_masse-objets-interstellaires.pdf http://www.cnrs.fr/insis/recherche/prix/2016/01/francois0 -lique.htm 5 10 15 20 -1 Relative translational energy (cm )
Fig. 2. Collisional energy dependence of the integral cross sections for O2 excitation (N = 1, j =
0) → (N = 1, j = 1). Experimental data with para-H2 (open circles) and normal-H2 (open
triangles).
10 Research Team: Stellar Astrophysics Research Group: Theoretical Astrochemistry
Permanent staff: Dahbia TALBI and Yohann SCRIBANO PhD students Pierre Ghesquiere (2012-2015), Duncan Bossion (2016-2019) Contact: [email protected], [email protected] Laboratory: Laboratoire Univers et Particules de Montpellier – UM5299 Institutions : CNRS and Université de Montpellier Website : http://www.lupm.univ-montp2.fr/
Astrophysical context Astrochemists and astrophysicist need molecular data. These data are required both to detect molecules and to produce robust astrochemical models. We use methods of theoretical chemistry (electronic and nuclear dynamic) to provide such data, contributing to the enrichment of the data bases for the astronomical community (the Kinetic Data Base for Astrochemistry KIDA and the Ro-vibrational collision excitation database BASECOL). Our studies of the reactive and non-reactive gas-phase molecular processes are undertaken for a large domain of temperature to cover the physical conditions from the present day solar system to the early stages of star formation. We investigate the chemistry catalyzed by the interstellar ices (taking into account both diffusion and reactivity). We also study the vibrational spectroscopy of molecules in gas-phase and in confined environments (like in cavities of some ices structures).
Keywords: Interstellar and Early universe chemistry, electronic structure calculations, quantum and classical reaction dynamics, molecular dynamics, molecular spectroscopy.
Key Research Facilities, Infrastructure, Equipment and Numerical tools: HPC resources of [TGCC/CINES/IDRIS], HPC resources of the University of Montpellier. Codes for ab initio electronic structure calculations (GAMESS, MOLPRO, GAUSSIAN, CRYSTAL) for Molecular Dynamic simulations (GROMACS, CP2K ) for Nuclear Dynamic treatments (MCTDH, ABC, PVSCF, CONVIV) and others developed house codes)
Collaborations Eric Herbst: University of Virginia (USA) Peet Hickman: University of Lehigh (USA) David Kashinski: West Point Military Academy (USA) Amir Karton: Scholl of molecular Sciences (Australia) David Benoit : Hull University (UK) Bill Poirier : Texas-Tech University (USA) Steve Ndengue : University of Missouri (USA) Tomas Gonzalez Lezana : CSIC Madrid (Spain) David Lauvergnat : LCP, Université d’Orsay (France) Pascal Honvault : ICB, Université de Dijon (France) Alexandre Faure : IPAG, Université de Grenoble (France) Fabien Gatti : ISMO, Université d’Orsay (France) Ioan Schneider, François Lique: LOMC, Université du Havre (France) Jean-Christophe Loison : ISM, Université de Bordeaux (France) Valentine Wakelam : Observatoire de Bordeaux (France) Patrice Theulé, Thierry Chiavassa : PIIM, Université de Provence (France Highlight
The diffusion and the reactivity of molecules inside interstellar ices are important processes to take into account to understand the molecular complexity observed in space. Using method of theoretical chemistry we have outlined the importance of bulk diffusion in interstellar ices. We have also demonstrated the catalytic role of these ices in the formation of ammonium carbamate and carbamic acid from CO2 and NH3.
Highlight 2015 of the national HPC ressources GENCI : au cœurs des glaces de l’espace
Latest most significant publications On the inclusion of a diagonal Born-Oppenheimer correction in the reduced dimensional treatment of the H2O--para-H2 complex Y. Scribano and A. Faure Journal of Chemical Physics 146, 226102 (2017) A theoretical study of the dissociative recombination of electrons with SH+ through the 2 P states of SH D. O. Kashinski, D. Talbi, A. P. Hickman I. F. Schneider O. E. Di Nallo F. Colboc, Chakrabarti and J. Zs. Mezei Journal of Chemical Physics 146, 204109 (2017) Diffusion of molecules in the bulk of a low density amorphous ice from molecular dynamics simulations Ghesquiere P., Mineva T., Talbi D., Theulé P., Noble J. A., Chiavassa T. Physical Chemistry Chemical Physics 17, 11455 (2015) + A new potential energy surface for the collisional excitation of N2H by H2 A. Spiefiedel, M.L. Senent, Y. Kalugina, Y. Scribano, C. Balanca, F. Lique, N. Feautrier Journal of Chemical Physics 143, 024301 (2015) Kinetics of the NH3 and CO2 solid-state reaction at low temperature J. A. Noble, P. Theule, F. Duvernay, G. Danger, T. Chiavassa, P. Ghesquiere,T. Mineva and D. Talbi Phys. Chem. Chem. Phys. 16, 23604 (2014)
Research Group: PCMT Group Permanent staff: M. Monnerville, D. Duflot, C. Toubin, D. Pelaez
PhD students (since 2010): A. Rivero-Santamaria () P. Peters (2009-2012) (ANR FORCOMS) E. Michoulier (2014-2018) (ANR PARCS) Post-docs (since 2010): Contact: [email protected]
Laboratory: Laboratoire de Physique des Lasers, Atomes et Molécules (PHLAM), UMR CNRS 8523 Institution(s): Université de Lille Website: http://www.phlam.univ-lille1.fr
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: Computational facilities with a local cluster. Development of codes for classical and quantum dynamics. Expert in the use of open source programs (Gromacs, …) or standard quantum chemistry/electronic structure codes (Gaussian, Molpro, Gamess, Cfour,…)
Expertise in ice modeling and in c ex
Keywords: collisions, recative collision, photodissociation, molecular dynamics, quantum dynamics, ice surfaces, adsorption, rate constant,
Astrophysical context and goals: Heterogeneous processes at ice surfaces in dense molecular clouds Collisions and reaction rates/ branching ratios calculations.
Theoretical studies of the group: - Adsorption, ionization and spectroscopy of PAH molecules on ice surfaces (ANR PARCS) - Determination of adsorption energies of radicals on ice surfaces (PCMI project 2018) - Desorption of molecules from interstellar ices (CO ices) (PCMI project 2018) - Rate constant for reactive collisions - Photodissociation cross section
Collaborations: Aude Simon (LCQP) Joëlle Mascetti (ISM) Jean-Christophe Loison (ISM) Jean-Hugues Fillion & Mathieu Bertin (LERMA) Fabrice Dayou (Observatoire de Meudon) Pascal Larregaray (ISM Bordeaux) Laurent Bonnet (ISM Bordeaux)
Highlight: Our expertise on ice surfaces modeling has been exploited in the PARCS project (2014-2018). The originality of this project was to propose pioneering joint theoretical and experimental treatments (J. Mascetti, ISM) of these reactions. The theoretical study implied the elaboration of a multiscale-multimethod approach that uses techniques mastered in the PCMT and LCPQ (Toulouse) group with various levels of sophistication and efficiency (MD, DFTB, ab-initio methods…). The collaboration has been particularly successful with a shared PhD and the following outcomes: i) a rigorous force field parametrization transferable to any PAH and in a broader extent to any other system, ii) prediction from classical MD of adsorption energies for PAHs of various sizes on crystalline and amorphous ices, iii) estimation from a DFTB/MM approach of the ionization energies of PAH on ice (a precursor stage to reactivity) and iv) DFTB/MM calculation of the IR spectra of the PAH adsorbed on ice and comparison with the experimental ones. The other project related to the astrophysics theme is the determination of accurate kinetic data as cross sections and thermal rate constants of interstellar reactive collisions to be integrated in astrophysical models. In the past few years, we have developed and improved our homemade quasi-classical trajectories (QCT) and time dependent wave-packet (TDWP) codes in order to study the dynamics of the Si(3P) + OH(X2Π) → SiO(X1Σ+) + H(2S) reaction. This process which is the major formation pathways of interstellar SiO in gas phase is very difficult to handle experimentally due to the presence of two radicals highly reactive. Theoretical calculations are then the only alternatives to obtain data for this kind of reactions. This collaboration with the Lerma group (Meudon), the InsTEC (La Habana, Cuba) and Alejandro Rivero Santamaria’s (postdoc) has been particularly successful in producing highly accurate classical and quantum results such as: has been particularly successful to produce high accurate classical and quantum results such as: i) integral cross sections and state selected (v = 0, j = 0-15) rate constants for the temperature range 10 − 500 K, ii) thermal rate constants in the same temperature range, and iii) rovibrational energy distributions of the SiO product.
At very low temperatures (< 20 K) which are characteristic of cold and dense regions of the interstellar medium (ISM), thermal desorption of all molecules except H2 is negligible. This mechanism cannot explain the existence of molecules like CO, CO2 etc … in this medium. Among several processes, vacuum ultraviolet (VUV) photodesorption from interstellar ice mantles has been proposed as an important desorption pathway to produce this kind of molecules particularly in the surface layers of protoplanetary disks. Recent laboratory studies have shown that the photodesorption rate could vary by several orders of magnitude depending on the nature of molecules as well as the composition of ices involved. The role of X photodesorption in this chemistry is also pointed out. Deriving strength of our experience and skills on i)- force-fields construction, ii)- classical simulations of photodissociation processes on ice and of our iii)- collaboration with experimentalists as J.-H. Fillon, M. Bertin (LERMA) experts in these photodesorption experiments, we propose to model the photodesorption of pure (CO, N2, …) as well as binary (CO/N2, …) ices using classical molecular dynamics calculations. These simulations require several steps: i) the construction of force-fields describing ground and excited states of the ice by means of electronic structure calculation data and their fit by analytical forms ii) the development of specific classical codes. The comparison between theoretical and experimental results will provide significant insights in the molecular mechanisms involved in these processes (project supported by PCMI in 2018).
Most significant publications (<5): [1] V. Taquet, P. S. Peters, C. Kahane, C. Ceccarelli, A. Lopez-Sepulcre, C. Toubin, D. Duflot, and L. Wiesenfeld. “Water ice deuteration: a tracer of the chemical history of protostars". In: Astron. Astrophys. 550 (2013), A127. doi: 10.1051/0004-6361/201220084.
[2] P. S. Peters, D. Duflot, L. Wiesenfeld, and C. Toubin. “The H + CO → HCO reaction studied by ab initio benchmark calculations". In: J. Chem. Phys. 139.16 (2013), p. 164310. doi: 10.1063/1.4826171 [3] A. Rivero Santamaría, F. Dayou, J. Rubayo-Soneira, and M. Monnerville. “Time-Depen- dent Quantum Wave Packet Study of the Si + OH → SiO + H Reaction: Cross Sections and Rate Constants". In: J. Phys. Chem. A 121.8 (2017), pp. 1675-1685. doi: 10.1021/acs. jpca.7b00174.
[4] S. Douix, D. Duflot, D. Cubaynes, J.-M. Bizau, and A. Giuliani. “Photoionization of the Buckminsterfullerene Cation". In: J. Phys. Chem. Lett. 8.1 (2017). PMID: 28052677, pp. 7-12. doi: 10.1021/acs. jpclett.6b02558
[5] E. Michoulier, J. A. Noble, A. Simon, J. Mascetti, C. Toubin. ”Adsorption of PAHs on inter- stellar ice viewed by classical molecular dynamics”, Phys. Chem. Chem. Phys., 2018, 20, 8753-8764, doi: 10.1039/C8CP00593A. Research Group: Theory and simulations
Permanent staff: Fabrice Dayou, Christian Balança, Marie-Lise Dubernet, Lydia Tchang-Brillet, Nicole Feautrier, Annie Spielfiedel (passed away in 2016) Technical staff: Carlo Maria Zwolf, Yaye Awa Ba, Nicolas Moreau, Norbert Champion, Christophe Blaess PhD students (since 2010): Ichraf Oueslati (2011-2015), Ghofrane Werfelli (2016) Post-docs (since 2010): Contact: [email protected]
Laboratory: Laboratoire d’Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères (LERMA) - UMR 8112 Institution(s): Observatoire Paris & Sorbonne Université Website: https://lerma.obspm.fr/spip.php?rubrique43
Key Research Facilities, Infrastructure and Equipment: • Computing resources of IDRIS and Paris Observatory. • Softwares for ab initio electronic structure calculations (MOLPRO, GAUSSIAN) and inelastic collisions (MOLSCAT). Home made codes (PES fitting, reactivity, photodissociation). • High resolution VUV spectrograph.
Keywords: Astrochemistry, interstellar medium, electronic structure calculations, inelastic collisions, gas-phase reactivity, spectroscopy.
Astrophysical context and goals: Rate coefficients for the collisional excitation of molecules by He/H2 are determined for a wide range of temperatures for the modelling of spectral lines originating from the ISM under non-LTE conditions. Reaction rate coefficients (for chemical and photo-induced processes) serve to improve astrochemical models.
Experimental studies of the group: High resolution VUV emission spectra of small molecules (H2, CO,.., and isotopologues) and atomic ions.
Collaborations: • M. Monnerville, D. Duflot (PhLAM, Lille) • A. Faure, L. Wiesenfield (IPAG, Grenoble) • F. Lique, F. Dumouchel (LOMC, Le Havre) • P. Honvault, B. Bussery-Honvault (ICB, Dijon) • S. Le Picard, J.-M. Launay (IPR, rennes) • T. Stoecklin, P. Larregaray, L. Bonnet (ISM, Bordeaux) • J. Cernicharo, M.-L. Senent (CSIC, Madrid, Spain) • M. Lara, M. Paniagua (Univ. Autonoma, Madrid, Spain) • F. Najar, D. Ben Abdallah (LSAMA, Univ. Tunis, Tunisia) • B. Kerkeni, I. Oueslati (LPMC, Univ. Tunis, Tunisia) • W. Ubachs (Univ. Amsterdam, Amsterdam, Netherlands) • D. Savin (Univ. Columbia, New York, USA)
Highlight: Rate coefficients for the collisional excitation of SiO by H2 The SiO molecule is mostly detected in regions associated with warm, dense, and shocked gas. The SiO emission lines are commonly used as tracers of molecular outflows surrounding star-forming regions. The radiative transfer modelling of spectral lines can provide valuable information on the SiO abundance and the physical properties of the emitting regions. Under non-LTE conditions, a proper modelling requires the knowledge of the rate coefficients for the collisional excitation mechanisms of the SiO ro-vibrational levels. We recently determined accurate rate coefficients for the rotational excitation of SiO by para-H2 and ortho-H2 species, employing state-of-the-art quantum methods. State- to-state rate coefficients were obtained for the first 21 rotational levels of SiO for temperatures up to 300K. Higher temperatures were also considered using approximated approaches to treat the rotational excitation of SiO by H2 (up to 1000K) and the ro-vibrational excitation of SiO by He (up to 6000K).
3 10-10
20 → 19 )
-1 -10 .s
3 2 10 20 → 19 2 → 1
2 → 1 1 → 0 Rate coefficient (cm 10-10 1 → 0 -11 SiO/para-H SiO/ortho-H 9 10 2 2 8 10-11 0 50 100 150 200 250 300 0 50 100 150 200 250 300 Temperature (K) Temperature (K)
Most significant publications (<5):
• Rotationally inelastic collisions of SiO with H2, C. Balança, F. Dayou, A. Faure, L. Wiesenfeld, N. feautrier, MNRAS, 479, 2692 (2018)
• Theoretical study of HCN-water interaction: five dimensional potential energy surfaces , E. Quintas-Sanchez, M.L. Dubernet, Phys. Chem. Chem. Phys., 6849, 19 (2017)
• Time-dependent quantum wave packet study of the Si+OH -> SiO+H reaction: cross sections and rate constants, A. Rivero-Santamaria, F. Dayou, J. Rubayo-Soneira, M. Monnerville, J. Phys. Chem. A, 121, 1675 (2017)
• Collisional excitation of sulfur dioxide by molecular hydrogen in warm molecular clouds, C. Balança, A. Spielfiedel, N Feautrier, MNRAS, 460, 3766 (2016)
• Quantum scattering study of the abstraction reaction of H atoms from tetramethylsilane, I. Oueslati, B. Kerkeni, W.-U L. Tchang-Brillet, N. Feautrier, Chem. Phys. Lett., 624, 29 (2015)
Link to full publication list: https://lerma.obspm.fr/spip.php?article153 2 Projects
77 Project: 3D Interstellar Chemo-physical Evolution
Timeframe: 2013-2018
Staff: Contacts: Valentine Wakelam ([email protected]). Permanent staff in France: PI: Valentine Wakelam (LAB, CNRS), Pierre Gratier (LAB, CNAP), Franck Hersant (LAB, researcher CNRS), Jean-Christophe Loison (ISM, researcher CNRS) Permanent staff in other countries: Ian Bonnell (Prof., University of Saint Andrews, UK) PhD students (since 2010): Laura Reboussin (2012-2015, LAB, astronomer), Maxime Ruaud (2013-2016, LAB, astronomer), Thomas Vidal (2015 – 2018, LAB, astronomer) Post-docs (since 2010): Liton Majumdar (2014-2017, LAB, astronomer), Wasim Iqbal (2016 – 2018, astronomer), Audrey Coutens (2017 – , astronomer) Other : Benjamin Pavone (engineer, 2013-2016), Christophe Cossou (2014, LAB, engineer)
Website: http://perso.astrophy.u-bordeaux.fr/VWakelam/3DICE/Home.html
Goals: Study the chemical evolution of the interstellar medium in a continuous and consistent way from the diffuse medium to the early disk formation.
Methods: We have been working on the physico-chemical data to be included in astrochemical models (reviewing the available data + computing/measuring some data). In addition, we have been using dynamical physical structure with our gas-grain model to compute the chemical evolution during the formation of cold cores using large-scale physical structures computed with galactic SPH simulations. Using these various cloud compositions, we are currently computing the 3D protostellar (and young disk) chemical composition with 1D and 3D physical structures computed with RHD and RMHD simulations.
Highlight: Influence of galactic arm scale dynamics on the molecular composition of the cold and dense ISM. I. Observed abundance gradients in dense clouds (Ruaud et al. 2018)
Keywords: astrochemistry, astrochemical models, molecules, star formation, cold cores, protostars
Most significant publications (< 5): Influence of galactic arm scale dynamics on the molecular composition of the cold and dense ISM. I. Observed abundance gradients in dense clouds, Ruaud, M.; Wakelam, V.; Gratier, P.; Bonnell, I. A. (2018) Astronomy & Astrophysics, Volume 611, id.A96, 14 pp. A new look at sulphur chemistry in hot cores and corinos Vidal, Thomas H. G.; Wakelam, Valentine (2018) Monthly Notices of the Royal Astronomical Society, Volume 474, Issue 4, p.5575-5587 A New Reference Chemical Composition for TMC-1 Gratier, P.; Majumdar, L.; Ohishi, M.; Roueff, E.; Loison, J. C.; Hickson, K. M.; Wakelam, V. (2016) The Astrophysical Journal Supplement Series, Volume 225, Issue 2, article id. 25, 10 pp. Gas and grain chemical composition in cold cores as predicted by the Nautilus three-phase model Ruaud, Maxime; Wakelam, Valentine; Hersant, Franck (2016) Monthly Notices of the Royal Astronomical Society, Volume 459, Issue 4, p.3756-3767 Link to full publication list: http://perso.astrophy.u-bordeaux.fr/VWakelam/3DICE/Publications.html
Press releases: Title and html link.
Related projects: Title and html link.
Instruments and Tools: Nautilus gas-grain model given upon request for the moment. KIDA (Kinetics Database for Astrochemistry): http://kida.obs.u-bordeaux1.fr ISA (Interstellar Abundance Database): http://isa.obs.u-bordeaux1.fr Project: ASAI
Timeframe: 2013-2018
Staff: Contacts: Bertrand Lefloch ([email protected]) Permanent staff in France: Cecilia Ceccarelli, Claudine Kahane, A. Lopez-Sepulcre (IPAG, astronomer), C. Vastel, E. Caux (IRAP, astronomer), E. Roueff (LERMA, astronomer) Permanent staff in other countries: Rafael Bachiller, Mario Tafalla, Asuncion Fuente (OAN, Espagne, astronomer), Jose Cernicharo, Nuria Marcelino (CSIC, Espagne, astronomer), Claudio Codella, Linda Podio (O. Arcetri, Italie, astronomer), Nami Sakai, Satoshi Yamamoto (U. Tokyo, Japon, astronomer), S. Viti (UCL, UK, astronomer) PhD students (since 2010): Juan Ospina-Zamudio (2016-2018), (IPAG, astronomer), Eleonora Bianchi (2015-2017, O. Arcetri, Italie, astronomer), Kento Yoshida (U. Tokyo, Japon, astronomer), J. Holdship (2014-2017, UCL, astronomer) Post-docs (since 2010): Linda Podio (2013-2014, IPAG, astronomer); A. Lopez-Sepulcre (IPAG, U. Tokyo, 2013-2015, astronomer); A. Gomez-Ruiz (O. Arcetri, 2014-2015, astronomer); E. Mendoza (2014-2016; USP, Brazil; astronomer)
Website: http://www.oan.es/asai;
Goals: The goal of the Large Program ”Astrochemical Surveys At IRAM” (ASAI) is to investigate the emergence and the evolution of molecular complexity in the early stages of low-mass star formation.
Methods: the goals are obtained by carrying out unbiased millimeter line surveys between 80 and 272 GHz of a sample of ten template sources, which fully cover the first stages of the formation process of solar-type stars, from prestellar cores to the late protostellar phase.
Highlight: Detection of prebiotic molecules in a protostellar shock region.
Despite a rather low elemental abundance, phosphorus is one of the main biogenic elements, present in all life forms on Earth. As such, phosphorus-bearing compounds, in particular molecules containing bonds between phosphorus and oxygen (P-O), play a key role in many biochemical and metabolic processes in living systems. However, searches for phosphorous compounds were unsuccessful towards solar-type star-forming regions, and only one line of PN was tentatively detected towards L1157-B1 until now. These are the first firm detections of phosphorous compounds in a star-forming region of solar type stars. The emission of these species is restricted to the shocked region L1157-B1; no emission was detected towards the position of the protostar L1157-mm itself, and a search of PH3 was unsuccessful in both positions. (Lefloch et al. 2016)
Keywords: astrochemistry – star formation - jets and outflows – molecular abundances
Most significant publications (< 5): Astrochemical evolution along star formation: Overview of the IRAM Large Program ASAI, Lefloch, B. et al., 2018, MNRAS, 10.1093/mnras/sty937, https://arxiv.org/abs/1803.10292 L1157-B1, a factory of complex organic molecules in a solar-type star-forming region, Lefloch B., et al., 2017, MNRAS, 469, L73, 10.1093/mnrasl/slx050 Phosphorus-bearing molecules in solar-type star-forming regions: first PO detection, Lefloch B., et al. 2016, MNRAS, 462, 3937, 10.1093/mnras/stw1918 The Origin of Complex Organic Molecules in Prestellar Cores,
Vastel. C., et al., 2014, ApJ, 795, L2, 10.1088/2041-8205/795/1/L2 Link to full publication list: http://www.
Press releases: http://www.iram-institute.org/EN/news/2017/143.html http://www.iram-institute.org/EN/news/2015/113.html
Related projects: Seeds Of Life In Space (SOLIS) (PIs: C. Ceccarelli, IPAG, France; P. Caselli, MPE, Germany)
Instruments and Tools: IRAM Project: BxB (Interstellar B-fields crossing inflation B-modes)
Timeframe: 2017-2021
Staff: Contacts: François Boulanger ([email protected]) and Katia Ferrière ([email protected]). Permanent staff in France:
LERMA & ENS Paris : Erwan Allys (Agrégé préparateur), Edith Falgarone (DR), François Levrier (MdC), Pierre Lesaffre (CR), Stéphane Mallat (Professeur)
IRAP Toulouse : Jonathan Aumont (CR), Anthony Banday (DR), Jean-Philippe Bernard (DR), Ludovic Montier (IR), Isabelle Ristorcelli (CR)
APC : Josquin Errard (CR), Radek Stompor (DR)
CEA/AIM Saclay : Patrick Hennebelle (Ingénieur CEA), Douglas Marshall (MdC), Marc-An- toine Miville-Deschênes (DR)
LAL Orsay : Jérémy Neveu (MdC), Matthieu Tristram (CR)
IAS Orsay : Julien Grain (CR), Vincent Guillet (MdC)
GEPI, Meudon : Rosine Lallement (DR)
Permanent staff in other countries: Marijke Haverkorn (Radboud University, Netherlands, Professor) Vibor Jelic (Ruđer Bošković Institute, Croatia, Professor). PhD students (since 2010): Cedric Cooling (2016-2019, AIM). Post-docs (since 2010): Marta Alves (2017-2019, Radboud University).
Website: http://bxb.lra.ens.fr/
Goals: With Planck data, the study of interstellar magnetic fields has become inter-connected to a paramount objective of observational cosmology: the quest for curl-like B-mode polarization of the cosmic microwave background (CMB), an expected signature of primordial gravitational waves. Set within this research context, the ANR BxB project has three ambitious goals involving inter-disciplinary collaborations. Combining observations of the magnetized ISM (stellar and dust polarization, synchrotron emission and Faraday rotation), applied mathematics, state-of-the-art numerical simulations, and theoretical modelling, we are working towards (1) the first 3D model of the ordered magnetic field from the Sun to the Galactic halo, (2) a statistical description of the Galactic magnetized interstellar medium, and (3) physically motivated simulations of the dust foreground to CMB polarization needed to optimize component separation and reliably quantify uncertainties in the search for primordial B-modes.
Methods: The BxB work plan innovates and supersedes state-of-the-art research in three research directions. (i) We are extending the 3D information on the nearby ISM derived from stellar observations, including Gaia astrometry, to the modelling of the Galactic magnetic field. (ii) We are introducing a novel approach in the analysis of data and of numerical simulations that captures the hierarchy of coherent, anisotropic structures characterizing the magnetized ISM. (iii) We are building a statistical model, which will allow us to link the astrophysics of polarized Galactic foregrounds to the quest for primordial CMB B-modes.
Highlight: BxB is an ANR research project that started in October 2017. It is a follow-up of the MISTIC ERC project, focused on the analysis of Planck dust polarization data, which opened this new research interface between Galactic astrophysics and cosmology.
Keywords: Magnetic fields - Interstellar medium – Turbulence – Numerical simulations – Statistics
First BxB publications: The Local Bubble: a magnetic veil to our Galaxy. Alves, M. I. R.; Boulanger, F.; Ferrière, K. and Montier, L. 2018 A&A 611, L5. On the statistics of the polarized submillimetre emission maps from thermal dust in the turbulent, magnetized, diffuse ISM. Levrier, F.; Neveu, J.; Falgarone, E.; Boulanger, F.; Bracco, A.; Ghosh, T. and Vansyngel, F., 2018 A&A in press, arXiv: 1802.08725 Planck intermediate results. LIV. Polarized dust foregrounds. Planck Collaboration, 2018 Submitted to A&A, arXiv: 1801.04945 Link to full publication list: http://bxb.lra.ens.fr/
Related projects: MIST (Molecules, Magnetic Fields, and Intermittency in Cosmic Turbulence), http://mist.lra.ens.fr
Instruments and Tools: Data from Planck, LOFAR and Gaia MHD Simulations of the multiphase turbulent ISM and of dissipative structures Project: CADE (Centre d’Analyse de Données Etendues)
Timeframe: 2012 — ongoing. Certified Service d’Observation since 2016.
Staff: • Contacts: Deborah Paradis ([email protected]) • Permanent staff in France: Jean-Michel Glorian (IRAP, engineer), Jean-Philippe Bernard (IRAP, astronomer), Annie Hughes (IRAP, astronomer) • CDD: Antoine Goutenoir (6 months in 2015, 2 months in 2016), Gabriel Foënard (2 months in 2018) • Collaborators: Pierre Fernique (CDS, engineer), Thomas Boch (CDS, engineer), Caroline Bot (CDS, astronomer), Mark Allen (CDS, astronomer)
Website: http://cade.irap.omp.eu
Goals: CADE is a service to the astronomical community dedicated to the analysis of extended emission. CADE provides astronomical data production in the HEALPix format, data archiving and diffusion to the community (data are VO-compatible through the HiPS format), as well as tools dedicated to the analysis of all-sky maps. The service includes the drizzling software library (drizzlib), which reprojects data from HEALPix to local WCS, and a web interface of the drizzlib (drizzweb).
Methods: The ingestion tool is based on the drizzling library, and uses a strategy where the surface of pixel intersection is computed. This method allows fast ingestion and guarantees the photometric accuracy of the transformation with minimal data loss during the transformation from a local WCS FITS map to HEALPix and vice-versa.
Highlight: A reference service for extended emission. CADE is undeniably used by the community with more than 1.2 Terabytes of downloads per year. The HEALPix database has been extensively used in the framework of the Planck and Herschel collaborations, and is the only database that provides uncertainty maps, which are essential to perform accurate scientific analyses. CADE is an important HiPS producer for the CDS (used by Aladin), that are also mirrored by ESA to be visible in the ESASky tool. The drizzlib/drizzweb are unique tools (developed in IDL and Python) that ensure flux conservation. The CADE service has been crucial to derive the gains and offsets in the Herschel maps by comparison with the Planck data. For instance, the effort led by the CADE team allowed the first data release of the Hi-GAL project (Molinari et al. 2016). Below are some example images of HEALPix maps produced by CADE. Keywords: HEALPix – database – tools – extended emission
Most significant publications (< 5): • Dark gas in the solar neighborhood from extinction data (appendix), Paradis, D., Dobashi, K., Shimoikura, T., et al., al. 2012, A&A, 543, 103 • Hierarchical progressive surveys. Multi-resolution HEALPix data structures for astronomical images, catalogues, and 3-dimensional data cubes, Fernique, P., Allen, M. G., Boch, T. et al., 2015, Instrumentation and Methods for Astrophysics, • Planck intermediate results. XXIII. Galactic plane emission components derived from Planck with ancillary data, Planck Collaboration, 2015, A&A, 580, 13
Link to full publication list: http://cade.irap.omp.eu/dokuwiki/doku.php?id=publications
Related projects: • OV-GSO (https://ov-gso.irap.omp.eu) • DustEM Wrapper (http://dustemwrap.irap.omp.eu/)
Tools: • Drizzlib (http://cade.irap.omp.eu/dokuwiki/doku.php?id=software) • Drizzweb (http://drizzweb.irap.omp.eu/) • Aladin et AladinLite (http://aladin.u-strasbg.fr/) • ESASky (http://sky.esa.int/) • HEALPix (http://healpix.sourceforge.net/) Project: COCOON
Timeframe: 2014-2022
Staff: Contacts: Laurent Pagani ([email protected]) and Shih-Ping Lai ([email protected]). Permanent staff in France: ◦ Laurent Pagani (LERMA, OP, astronomer). ◦ Pierre Lesaffre (LERMA, ENS, astronomer) ◦ François Dulieu (LERMA, UCP, astronomer) ◦ Vincent Guillet (IAS, astronomer) Permanent staff in other countries: ◦ Shih-Ping Lai (Institute of Astronomy, NTHU, Taiwan, astronomer) ◦ Sheng-Yuan Liu (ASIAA, Taiwan, astronomer) ◦ Hiroyuki Hirashita (ASIAA, Taiwan, astronomer) PhD students (since 2010): ◦ Nguyen Hoang Phuong Thanh (2015-2018, LERMA, UCP, astronomer). ◦ Ren-Shiang Sun (2015-?, NTHU, Taiwan, astronomer) ◦ Sheng-Jun Lin (2016-2020, NTHU, Taiwan, astronomer) Post-docs (since 2010): ◦ Charlène Lefèvre (post-doc à l’IRAM, astronomer, collaboratrice du projet)
Website: not yet opened
Goals: Study the 3D structure of a handful of starless clouds in Taurus and Scorpion/Rho Oph, determine the dust properties (size distribution, composition), the cold core deuteration and depletion profiles, and the core ages from all three time dependent phenomena (grain growth, deuteration, and depletion). Comparison between the different clouds will help understand the first steps of low mass star formation and the type of collapse (slow or fast) driving the formation of the cores. Differential depletion of CO and N2 is a by-product of this work. It will be better characterized in the clouds and investigated in the lab.
+ Methods: model the 3D cloud density and temperature structure by combining N2H radiative transfer modeling with dust NIR/MIR absorption and scattering (cloudshine, coreshine) modelling and dust FIR/mm emission modelling (and get dust properties in parallel). Model the abundance of deuterated + + + species (N2D , DCO , H2D ) through a time- and spin-dependent deuteration chemical model. Model the growth of the grains with time. Laboratory works in interstellar conditions of vacuum and tempe-rature to explore CO and N2 ice interactions.
Highlight: Grains grow beyond 1 µm in size to efficiently scatter light at λ = 8 µm (Lefèvre et al. 2016). In an attempt to use extinction image at λ = 8 µm of L183 to model the cloud column density with high spatial resolution, we have found that limiting the extinction to absorption of background light asin previous works was leading to an incoherent result when compared with other maps of the same source. Consistency was retrieved by modeling the scattering effect of grains at this wavelength. Though this scattering effect does not appear in emission, unlike the coreshine effect seen at 3-5 µm, it is nevertheless present and compensates 50% of the absorption. We have found that fractal grains of equivalent size of 4 µm were necessary in the center of the cloud to fit the observations. Only Min et al. (2016) grains fit our needs but they are naked grains (no ices) and contain pure magnesium silicates which are too emissive at long wavelengths (in accordance with Demyk et al. results). New grains, derived from Min’s work but including ices and iron will be calculated with our new grain modeling code, SIGMA, presently under development (Lefèvre et al., in prep.). Keywords: prestellar cores, deuteration, grain growth, coreshine, depletion, core age
Most significant publications (< 5): Lefèvre, C., Pagani, L. Min, M., Poteet, C., Whittet, D., 2016, A&A, 585, L4,On the importance of scattering at 8 μm: Brighter than you think Pagani, L., Lefèvre, C., Juvela, M., et al., 2015, A&A, 574, L5,Can we trace very cold dust from its emission alone? Lefèvre, C., Pagani, L., Juvela, M., Paladini, R., et al., 2014, A&A, 572, A20,Dust properties inside molecular clouds from coreshine modeling and observations Pagani, L., Lesaffre, P., M. Jorfi, P. Honvault, T. González-Lezana, and A. Faure, 2013, A&A, 551, A38, Ortho-H2 and the age of prestellar cores
Pagani, L., Bourgoin, A., Lique, F., 2012, A&A, 548, L4, A method to measure CO and N2 depletion profiles inside prestellar cores
Link to full publication list: to be included in the website to come.
Press releases: A new window for the observation of dust growth in molecular clouds https://www.obspm.fr/a-new-window-for-the-observation-of-dust-growth.html?lang=en Dense cores inside interstellar clouds do shine: a widespread phenomenon https://www.obspm.fr/dense-cores-inside-interstellar-clouds-do-shine-a.html?lang=en
Related projects: SPARX, https://sparx.tiara.sinica.edu.tw/code/
Instruments and Tools: VENUS and FORMOLISM lab experiments Radio telescopes (GBT, JCMT, APEX, 30-m, spectrometers + bolometers at 0.85, 1.2, & 2.0 mm) Optical/NIR telescopes (VISTA, CFHT) Satellites (Spitzer, Herschel, Akari, Planck) Radiative transfer codes (CRT, line radiative codes including SPARX, LIME) Chemical codes (modified NAHOON, modified NAUTILUS, dynamical model) Research Group: COMs
Permanent staff: Laurent Wiesenfeld, Alexandre Faure, C. Rist, C. Ceccarelli, Y. Scribano, Majdi Hochlaf Technical staff: None PhD students (since 2010): Emna Sahnoun and Malek Ben Khalifa (Tunis) Post-docs (since 2010): Helena Massó, Fabien Daniel Contact: Laurent Wiesenfeld ([email protected]) Laboratory: IPAG Institution(s): Université Grenoble Alpes Website: http://www.
Key Research Facilities, Infrastructure, Equipment, and Numerical Tools: CIMENT grid of computers, Observatoire de Grenoble MOLPRO quantum chemistry program MOLSCAT quantum scattering code + homegrown codes. Keywords: Complex Organic Molecules, water, rotational quenching, quantum chemistry, quantum scattering Astrophysical context and goals: Quantitative modeling of COMs and water in the interstellar medium and in Young Stellar Objects Hershel WiFi observations, multiwavelengths observations from GHz (Green Bank) to THz (ALMA)
Experimental and theoretical studies of the group: Rotational quenching coefficients of H2CO, HCOOCH3, HNCO, HC3N, HCO+ (all finished and published) NH2CH, l- and c-C3H2 (in progress) Water isotopomers (HDO,D2O), theory modeling and scattering experiments Water excitation, experiments
Collaborations: D. Parker, A van der Avoird (U Nijmegen) F. Lique (U Le Havre) J Cernicharo (CSIC) K Hammami (U. El Manar, Tunis) K. Szalewicz (U Delaware) A. Remijan (NRAO) A. Coutens, C. Vastel, E Caux(Obs. Toulouse)
Highlight: Knowing the collision rate allows to predict masing effects for heavy COMs. In a paper written in collaboration with astronomers from NRAO, we were able to show that the emission/absorption intensities of most low-lying transitions (observed by the Green Bank telescope) are very far from equilibrium, some being even weakly masing. This comes about because of the large variation of optical and collisional rates for the various the transition observed (ref 4 below). Strong non LTE effects are also observed for HNCO, in a forthcoming work in coll. with E. Caux.
Most significant publications (<5): 1. van der Waals interaction of HNCO and H-2: Potential Energy Surface and Rotational Energy Transfer 2018 Sahnoun E, Wiesenfeld L et al., J Phys Chem A, DOI: 10.1021/acs.jpca.8b00150.
2. Collisional excitation of HC3N by para- and ortho-H-2, 2016 Faure, Lique, Wiesenfeld MNRAS, DOI: 10.1093/mnras/stw1156
3. Collision energy dependence of statetostate differential cross sections for rotationally inelastic scattering of H2O by He, 2017, Sarma et al. PCCP , DOI: 10.1039/c6cp06495g
4. Weak Maser Emission Of Methyl Formate Toward Sagittarius B2(N) In The Green Bank Telescope Primos Survey Faure A., Remijan, AJ et al. 2014, ApJ, DOI: 10.1088/0004-637X/783/2/72
Link to full publication list: http://www.
Press releases: Project: Formation des molécules organiques complexes dans le milieu interstellaire froid
Timeframe: 2014-2021
Staff: Contacts: Aurore Bacmann ([email protected]) Permanent staff in France: Alexandre Faure (IPAG), Eric Quirico (IPAG), Sébastien Le Picard (IPR), Ian Sims (IPR), André Canosa (IPR), Patrice Theulé (PIIM) PhD students (since 2010): Enrique Garcia (2014-2017).
Collaborators: - Philippe Boduch (CIMAP Caen) - François Lique (LOMC Le Havre) - Elena Jiménez (Universidad Castilla La Mancha)
Goals: Complex organic “terrestrial”molecules were believed to be hot core tracers, since they were found in the hot regions (>100 K) surrounding young stars. The detection of these molecules in cold (10 K) prestellar cores has cast doubts on the previously accepted warm chemistry scenarios that had been put forward to account for the presence of these species in hot cores. The aim of this project is to constrain chemical pathways for complex molecules in the cold interstellar medium to account quantitatively for their abundances.
Methods: The project relies on close interactions between observations and laboratory experiments in order to derive quantitative data. Observations target samples of prestellar cores in the complex organic molecules commonly detected in hot cores, using state-of-the-art facilities like the IRAM 30m telescope or the Green Bank Telescope. Molecular abundances are determined using multi-transition radiative transfer modelling, requiring the use of collisional coefficients. Elementary processes (molecular formation, destruction or desorption) are modelled using the newest reaction rates / desorption efficiencies measured in the laboratory and confronted to observational results.
Highlight: Gas phase formation pathways for precursor radicals. By determining the abundances of important precursor radicals HCO and CH3O of complex organic molecules in a sample of prestellar cores, we have found that the relative ratios of HCO, H2CO, CH3O and CH3OH are similar in all the sources (Bacmann & Faure 2016). We have shown that the derived abundances are consistent with a gas phase formation of these radicals, either via ion-molecule chemistry or neutral-neutral reactions such as H2CO + OH HCO+H2O, which new CRESU experiments have shown to accelerate towards low temperatures (e.g. Ocaña et al. 2017). We were able to identify important reactions to be studied in the laboratory.
Keywords: Interstellar medium, Star Formation, Molecular Emission
Most significant publications (< 5): The origin of gas-phase HCO and CH3O radicals in prestellar cores, Bacmann, A. & Faure, A. 2016, A&A, 587, A130, DOI: 10.1051/0004-6361/201526198 Detection of protonated formaldehyde in the prestellar core L1689B, Bacmann, A. García- García E., & Faure, A. 2016, A&A, 588, L8, DOI: 10.1051/00046361/201628280 Is the Gas phase OH + H2CO reaction a source of HCO in interstellar cold dark clouds? A kinetic, dynamic, and modeling study Ocaña, A.J., Jiménez, E., Ballesteros, B., Canosa, A., Antiñolo, M., et al. 2017, ApJ, 850, 28, DOI: 10.3847/1538-4357/aa93d9
Instruments and Tools: IRAM 30m telescope (http://www.iram-institute.org) Green Bank Telescope (http://greenbankobservatory.org/gbt-observers/) CRESU apparatus (Institut de Physique de Rennes, Universidad Castilla la Mancha) GANIL (https://www.ganil-spiral2.eu/) Project: COSMIDYN
Timeframe: 2016-2020
Staff: Contacts: Alexandre Marcowith ([email protected]) and Benoit Commerçon ([email protected]). Permanent staff in France: Benoit Commerçon (ENS Lyon, CR), Yohan Dubois (IAP, CR), Alexandre Marcowith (LUPM, DR) PhD students (since 2010): Loann Brahimi (2017-2020, LUPM).
Goals: Investigate the dynamical effects of Cosmic Rays at intermediary galactic scales.
Methods: This project is almost numerical. It uses the magnetohydrodynamic (MHD) code RAMSES upgraded with a module treating Cosmic Rays as a fluid (multi-fluid simulations). The Cosmic Ray fluid energy equation is treated to account for multiple physical effects: diffusion, streaming, sources of Cosmic Rays. The original (quite unique actually) aspect developed by the team is the possibility to adapt the Cosmic Ray diffusion coefficient to the amplitude of the local Cosmic ray gradient in the simulation grid. This allows us to treat reduced Cosmic ray diffusion due to the Cosmic Ray self-generation of magnetic perturbations by the streaming instability. This implies to develop a proper treatment of Cosmic Ray streaming terms.
Highlight: Effect of Cosmic Rays over magnetized interstellar turbulence at intermediary galactic scales. The study has two steps. The first step, which is now completed and is the subject of a publication in preparation in Astronomy & Astrophysics is a parametric study of the combined statistics of warm and cold interstellar medium phases including Cosmic rays. In this first study, Cosmic Rays have an imposed unique diffusion coefficient defined over the simulation grid. We investigate the conditions under which the magnetized turbulence, which develops in these two phases, is modified by the Cosmic Ray pressure. We find that the critical diffusion coefficient is usually 2-3 orders of magnitude below the standard Cosmic ray diffusion coefficient deduced from direct observations (see figure). We discuss the possibility to reach such low diffusion coefficients invoking recent theories of interstellar turbulence. Figure: Probability distribution function of the gas density and temperature and Cosmic Ray energy density for different Cosmic Ray diffusion coefficients. A clear bifurcation is seen below a coefficient value of 10 26 cm2/s where Cosmic Rays are fully coupled with the gas.
In a second step, we will complement this first study with an investigation of the effect of self-generated turbulence over interstellar turbulence dynamics. This requires implementing a diffusion coefficient scaled over the local Cosmic Ray gradient to mimic the effect of the streaming instability and to implement a term, which accounts of the drift of the particles with their scattering centers. Both terms require substantial numerical developments that are part of a PhD thesis work.
Keywords: Cosmic rays – Interstellar turbulence – Gravitational collapse – Star formation.
Most significant publications (< 5): B. Commerçon, A.Marcowith, Y. Dubois, A&A, 2018, en preparation.
Related projects: Projet de Yohan.
Instruments and Tools: MHD code RAMSES http://irfu.cea.fr/Phocea/Vie_des_labos/Ast/ast_sstechnique.php? id_ast=904 Project: DustDist
Timeframe: 2015-2022
Staff: Contacts: Francois-Xavier Désert ([email protected]) Permanent staff in France: Francois-Xavier Désert (IPAG, astronomer, UGA), Nicolas Ponthieu (IPAG, CR, CNRS), Frédérique Motte (IPAG, DR, CNRS), Aurore Bacmann (IPAG, Adj.Astronomer, UGA), Juan Macias-Perez (LPSC, DR, CNRS), Pierre Hily-Blant (IPAG, MCF, UGA), Isabelle Ristorcelli (IRAP, DR, CNRS). Permanent staff in other countries: Nicolas Peretto (Assistant Professor, Cardiff University).
Website:
Goals: Establish the Dust spectral and spatial Distribution in the (sub)mm domain around diffuse and star-forming regions
Methods: Use Planck, Herschel, Scuba2, Atlasgal, and NIKA2 data in merged maps.
Highlight: DustDist. Bracco et al (2017) have analyzed how the dust emission spectrum can change within a small region of the interstellar medium. We want to generalize this kind of analysis to different regions.
Keywords: Dust, Interstellar, Emission
Most significant publications (< 5): Probing changes of dust properties along a chain of solar-type prestellar and protostellar cores in Taurus with NIKA, Bracco et al., A&A 604, A52 (2017), DOI: 10.1051/0004-6361/201731117 Press releases:
Related projects: NIKA2 large programs
Instruments and Tools: NIKA2 instrument GALETTE
Timeframe: 2016-2021
Staff: ● Contacts: Douglas Marshall (Associate professor, Université Paris Diderot douglas.- [email protected]) & Julien Montillaud (Associate professor, Université de Franche-Comté, [email protected]) ● Permanent staff in France: Laurent Cambresy (Obs. Strasbourg, astronomer) & Annie Robin (Obs. Besancon, DR) ● Permanent staff in other countries: Mika Juvela (University of Helsinki, professor) ● PhD students (since 2017) : David Cornu (Université de Franche-Comté) ● Post docs (since 2016) : Heddy Arab(2016-2018, Strasbourg) & Veli-Matti Pelkonen (2016-present, Helsinki, Barcelona)
Goals: We aim to produce maps of the Milky Way, in three dimensions, that describe: 1. The differential extinction as a function of distance: dAv/ds, 2. The density field of interstellar matter: nH(x,y,z), 3. The excitation of the dust grains per grain population: TDUST(pop; x,y,z), 4. The interstellar radiation field from the far-ultraviolet to the far-infrared: I_nu(x,y,z,nu).
Methods: Our methodology can be separated into two main elements: the extinction map and the adjustment of the dust emission. The extinction code that we are using is called MACHETE (MArkov CHain Extinction in Three dimEnsions, Marshall et al., in prep.). It uses an affine invariant Markov chain Monte Carlo (MCMC) Ensemble sampler to determine the most likely 3D line of sight extinction. The Galactic mOdeL of stellar and dust EMission (GOLEM) is a code under development at the Institute UTINAM (Montillaud et al., in prep.) which combines 1. the BGM to compute the intrinsic stellar emission in the Galaxy in 3D, 2. the CRT code (Juvela and Padoan 2005) to compute the 3D radiative transfer of stellar light through the ISM and obtain the ISRF at any point of the Galaxy, and 3. the DustEM code (Compiègne et al. 2011) to derive the SED of dust emission.
Highlight: - MACHETE was benchmarked against concurrent tools, revealing competitive perfor- mances with the unique asset to simultaneously measure the width of the log-normal distribution of dust extinction. From these measurements, we derived maps of Mach number that characterise the dynamical state of interstellar clouds. - Using GOLEM, we showed that the sub-cell (fractal) structure of the ISM and the spatial variations in stellar populations throughout the Galaxy play major roles in the prediction of the Galactic mid-IR emission. We showed that neglecting these aspects can lead to overestimate the abundance of PAHs by ~50%. Project: 'Galactic Cold Cores : Study of the Early stages of Star formation: filaments and dense cores properties'
Timeframe: started in 2010
Staff: Contacts: Isabelle Ristorcelli ([email protected]) and Mika Juvela (Helsinki). Permanent staff in France: Jean-Philippe Bernard (IRAP), Karine Demyk (IRAP), Edith Falgarone (ENS), Katia Ferrière (IRAP), Vincent Guillet (IAS), Annie Hughes (IRAP), Francois Levrier (ENS), Douglas Marshall (AIM), Claude Mény (IRAP), Ludovic Montier (IRAP), Julien Montillaud (UTINAM), Frédérique Motte (IPAG), Laurent Pagani (LERMA), Déborah Paradis (IRAP), Charlotte Vastel (IRAP), Nathalie Ysard (IAS), Annie Zavagno (LAM) Permanent staff in other countries: Yasuo Doi (Japan), Viktor Toth (Budapest University), Peregrine McGehee (IPAC, USA), Paolo Padoan (Barlecona University), Roberta Paladini (IPAC), Derek Ward- Thomson (UCLAN, Preston), Katherine Pattle (UCLAN, Preston). PhD students (since 2010): Dana Alina (2011-2015, IRAP), Jean-Sébastien Carrière (since 2018, IRAP), Gabor Marton (Budapest University), Erika Verebelyi (Budapest University), David Cornu (since 2016, UTINAM), Mika Saajasto (since 2015, Helsinki University). Post-docs (since 2010): Dana Alina (since 2015, Astana Nazarbayev University), Douglas Marshall (2010-2012, IRAP), Alana Rivera-Ingraham (2012-2014, IRAP), Johanna Malinen (University of Cologne since 2016), Julien Montillaud (2011 - 2013, Helsinki University), Elisabetta Micelotta (Helsinki University since 2016), Veli-Matti Pelkonen (Helsinki University), Nathalie Ysard (2009-2011, Helsinki University), Orsolya Feher (Budapest University), Sarolta Zahorecz (Budapest University) .
Website: http://www.interstellarmedium.org/Besancon2018/ https://wiki.helsinki.fi/display/PlanckHerschel/The+Cold+Cores
Goals: study the initial conditions of star formation by characterizing the physical properties of dense cores in the different environments of the Galaxy and investigating what are the processes generating their formation or controlling their evolution. For this purpose, it is needed to study the properties of dense structures (cores, clumps and their environment) and analyze the interplay between gravity, turbulence, and magnetic fields at different scales. As a tracer of dense matter (mass and density) and of the magnetic fields lines, dust emission properties and their evolution toward dense medium are also critical to characterize, both in intensity and polarization.
Methods: The Planck all-sky survey has allowed us to build the catalogue of Galactic cold clumps 'PGCC', and we are now working on a large number of molecular and continuum follow-ups from ground-based and space telescopes (Herschel, PILOT, IRAM-30m, Onsala, Apex, Effelsberg, and soon NIKA2, NOEMA, BLAST-pol, JWST). Both statistical studies and detailed analysis on individual fields (cores and environments) are performed on the basis of these observations. These observational results are compared to MHD simulations and predictions from dust models. The Galactic Cold Cores project has recently been extended to the TOPSCOPE collaboration (PI: Tie Liu, KASI) and its dedicated PGCC follow-ups (SCUBA2 legacy survey of 1000 clumps, SCUBA-pol, TRAO, ALMA). Highlight: Planck and Herschel catalogues of cold cores and clumps: We have built the first all-sky catalogue of Galactic Cold Clumps (Planck collaboration XXVIII, 2016), a fraction of which has been studied in detail with our Herschel follow-up. The sources, often embedded in filamentary structures, cover a broad range in physical properties and correspond to different evolutionary stages in the star formation process, from quiescent starless clumps and nearby cores to young protostellar objects (Montillaud et al. 2015). Link with the environment large-scale properties: Our statistical studies of nearby filaments show that their properties depend on their environment density, with the precursors of star-forming filaments evolving coevally with their environment (Rivera-Ingraham et al. 2016, 2017). Detailed analysis of intertwined filaments in Monoceros OB1 has evidenced a connection between the filament dynamics and the global evolution of the large-scale cloud (Montillaud et al. 2019). In parallel, our results confirm a strong interplay between interstellar magnetic fields and filaments during their formation and evolution (Malinen et al. 2016, Alina et al. 2019).
Keywords: star formation, ISM dense structures, pre-stellar cores, magnetic fields, polarization, ISM dust properties
Most significant publications (< 5): ‘Planck 2015 results. XXVIII.The Planck Catalogue of Galactic Cold Clumps’ Planck Collaboration 2016, A&A 594, A28, DOI: 10.1051/0004-6361/201525819 'Galactic Cold cores IV: Cold submillimeter sources: catalogue and statistical analysis', Montillaud J., Juvela, Rivera-Ingraham et al. 2015, A&A 584, A92, DOI: 10.1051/0004- 6361/201424063 'Statistical analysis of the interplay between interstellar magnetic fields and filaments hosting Planck Galactic cold clumps', Alina D., Ristorcelli I., Montier L. et al. 2019, MNRAS 485, doi:10.1093/mnras/stz508 'Galactic cold cores VIII. Filament formation and evolution: Filament properties in context with evolutionary models', Rivera-Ingraham A., Ristorcelli I., Juvela M. et al., 3017, A&A 601, A94, DOI: 10.1051/0004-6361/201628552 'Galactic cold cores V. Dust opacity', 2015, Juvela M., Ristorcelli I., Marshall D.J. et al., 2015, A&A 584, A93, DOI: 10.1051/0004-6361/201423788 Project: GENeration and Evolution of Structures in the ISm - GENESIS
Timeframe: 2017-2020
Staff: Contacts: Sylvain Bontemps ([email protected]) and Nicola Schneider ([email protected]). Permanent staff in France: Sylvain Bontemps (LAB, astronomer), Hussein Yahia (INRIA Bordeaux, Computing science), Nicolas Brodu (INRIA Bordeaux, Computing science), Fabrice Herpin (LAB, astronomer), Jonathan Braine (LAB, astronomer), Antoine Gursdorf (LERMA, astronomer), Nathalie Brouillet (LAB, astronomer), Thierry Jacq (LAB, astronomer), Pascal Tremblin (CEA Saclay, astronomer), Timea Csengeri (LAB, astronomer), Frederique Motte (IPAG, astronomer). Permanent staff in other countries: Robert Simon (Univ. of Cologne, astronomer), Volker Ossenkopf (Univ. of Cologne, astronomer), Markus Roellig (Univ. of Cologne, astronomer), Ralf Klessen (ITA/ZAH Heidelberg, astronomer), Simon Glover (ITA/ZAH Heidelberg, astronomer), Paul Clark (Institute of Astronomy Cardiff, astronomer), Nicolas Peretto (Institute of Astronomy Cardiff, astronomer), Alexei Kritsuk (CASS San Diego), Phil Myers (CfA Harvard). PhD students (since 2010): Lars Bonne (LAB, 2017-). Post-docs (since 2010): Nicola Schneider (Univ. of Cologne), Arabindo Roy (LAB), Guillaume Attuel (INRIA Bordeaux), Ana Duarte-Cabral (Institute of Astronomy Cardiff).
Website: https://www.astro.uni-koeln.de/GENESIS
Goals: The objective of this research project is to better understand the structure and evolution of molecular clouds in the interstellar medium (ISM) and to link cloud structure with star-formation.
Methods: For that, far-infrared observations of dust (Herschel) and cooling lines (SOFIA) are combined with ground-based submillimetre observations of molecular lines (IRAM and APEX). Dedicated tools will be used and developed to analyse the maps and compared to simulations in order to disentangle the underlying physical processes such as gravity, turbulence, magnetic fields and radiation. An innovative approach is to combine the competence of the members of the Cologne KOSMA group in structure identification methods and SOFIA with the expertise of the Bordeaux LAB star formation group in Herschel and spectro-imaging maps, and the Bordeaux GeoStat team of the INRIA institute who are experts in nonlinear methods and multi-fractal analysis of images and complex systems. This project is also seen as a preparation for the science case of SPICA, CCAT-prime and Origins projects and may also contribute to the HSTDM (High Sensitivity Terahertz Detection Module) science (2m telescope close to the chinese orbital station).
Highlight: First promising results: Excess of warm emission associated with Musca filament. Using APEX/FLASH we obtained maps of CO3-2 and 4-3 across the crest of the Musca filament and detected a CO emission made of two velocity components, one associated with the cold dense gas of the crest and an additional component which corresponds to warm and relatively dense gas (100 K and 3x103 cm-3 from RADEX modeling). We interpret this warm gas as shocked gas due to low velocity accretion shocks at the surface of the filament (Bonne et al. in prep). If confirmed it would strongly support the dynamical view for the formation of dense filaments, and would reject the quasi-static view based on pressure confinement. Keywords: ISM structure and physics; star formation; dense filaments; dense cores/clumps; turbulence; shocks; ISM cooling
Most significant publications (< 5): New project, no “strong” publication yet.
Link to full publication list: https://hera.ph1.uni-koeln.de/~nschneid/publications.html Press releases: None. Related projects: SPICA (ESA M5) Origins (NASA decadal) CCAT-prime HSTDM Instruments and Tools: Herschel images, SOFIA, APEX, ALMA, multi-fractal analysis tools. Project: High-mass star formation and the origin of the IMF
Timeframe: 2015-2020
Staff: Contacts: Frédérique Motte ([email protected]). Permanent staff in France: ◦ Sylvain Bontemps, Timea Csengeri, Nathalie Brouillet, Fabrice Herpin (LAB, astronomers); ◦ Estelle Moraux, Isabelle Joncour, and Nicolas Ponthieu (IPAG, astronomers); ◦ Pierre Didelon, Patrick Hennebelle, and Matthias Gonzalez (AIM, astronomers); ◦ Antoine Gusdorf and Pierre Lesaffre (LERMA, astronomers); ◦ Annie Zavagno and Delphine Russeil (LAM, astronomers). Staff in other countries: ◦ Fabien Louvet (Univ. of Chile, Chile, astronomer); ◦ Nicolas Peretto and Kenneth Marsh (Cardiff Univ., astronomers) ◦ HOBYS and ALMA-IMF consortia. PhD students (since 2010): ◦ 2017-2020: Lars Bonne (LAB, astronomer); ◦ 2016-2019: Thomas Nony (IPAG, astronomer), Aina Andrianasolo (IPAG, astronomer), and Jordan Molet (LAB, astronomer); ◦ 2011-2015: Jérémy Tigé (LAM, astronomer); ◦ 2011-2014: Fabien Louvet (AIM, astronomer); ◦ 2009-2012: Quang Nguyen Luong (AIM, astronomer). Post-docs (since 2010): ◦ Jean-François Robitaille (2018-2019, IPAG, astronomer); ◦ Arabindo Roy (2017-2019, LAM, astronomer); ◦ Nicola schneider (2010-2015, first AIM then LAB, astronomer); ◦ Tracy Hill (2010-2013, AIM, astronomer); ◦ M. Hennemann (2010-2013, AIM, astronomer).
Websites: http://hobys-herschel.cea.fr et http://ipag.osug.fr/~mottef
Goals: o Build a coherent picture of high-mass star formation, using a combined observational and theoretical approach. o Revisit the origin of the mass distribution stars, the Initial Mass Function (IMF), by investigating to which extent environmental effects do matter, using a combined observational and theoretical approach.
Methods: o Use Herschel, ALMA, NOEMA, and IRAM 30m (EMIR and soon NIKA2) data. o Extract compact cores and filaments/ridges from the ISM, measure their mass, follow gas inflows toward filaments/ridges and cores, constrain the magnetic field strength and topology. o Compare observational constraints to theoretical models and numerical simulations. o Define evolutionary sequences of ISM structures (cores and filaments/ridges) to constrain star formation and the origin of the IMF.
Highlight: The unexpectedly large proportion of high-mass star-forming cores in a Galactic mini-starburst, Motte, F., Nony, Louvet, F., et al., Nature Astronomy, 50 (2018). Understanding the processes that determine the stellar initial mass function (IMF) is a critical unsolved problem, with profound implications for many areas of astrophysics. In molecular clouds, stars are formed in cores—gas condensations sufficiently dense that gravitational collapse converts a large fraction of their mass into a star or small clutch of stars. In nearby star-formation regions, the core mass function (CMF) is strikingly similar to the IMF, suggesting that the shape of the IMF may simply be inherited from the CMF. Here, we present 1.3 mm observations, obtained with the Atacama Large Millimeter/submillimeter Array telescope, of the active star-formation region W43-MM1, which may be more representative of the Galactic-arm regions where most stars form. The unprecedented resolution of these observations reveals a statistically robust CMF at high masses, with a slope that is markedly shallower than the IMF. This seriously challenges our understanding of the origin of the IMF.
Keywords: Interstellar Medium – Star formation – Initial Mass Function
Most significant publications (< 5): The unexpectedly large proportion of high-mass star-forming cores in a Galactic mini-starburst, Motte, F., Nony, Louvet, F., et al., Nature Astronomy, 50 (2018) 10.1038/s41550-018-0452-x High-Mass Star and Massive Cluster Formation in the Milky Way, Motte, F., Bontemps, S., Louvet, F., ARA&A 56 (2018) 10.1146/annurev-astro-091916-055235 Cluster-formation in the Rosette molecular cloud at the junctions of filaments, Schneider, N., Csengeri, T., Hennemann, M. et al., A&A 518, L77 (2012) 10.1051/0004-6361/201118566 Initial highlights of the HOBYS key program, the Herschel imaging survey of OB young stellar objects, Motte, F., Zavagno, A., Bontemps, S. et al., A&A 518, L77 (2010) 10.1051/0004-6361/201014690 Fragmentation and mass segregation in the massive dense cores of Cygnus X, Bontemps, S., Motte, F., Csengeri, T., Schneider, N., A&A 524, 18 (2010) 10.1051/0004-6361/200913286
Link to full publication list:
Press releases: Les lois de la naissance des étoiles remises en question, http://www2.cnrs.fr/presse/communique/5577.htm https://www.univ-grenoble-alpes.fr/fr/acces-direct/actualites/a-la-une/a-la-une-recherche/l es-lois-de-la-naissance-des-etoiles-remises-en-question-343970.kjsp http://www.cea.fr/presse/pages/actualites-communiques/sciences-de-la-matiere/les-lois-nai ssance-etoiles-remises-en-question.aspx https://www.obspm.fr/les-lois-de-la-naissance-des.html
Related projects: Herschel/HOBYS key program: http://hobys-herschel.cea.fr IRAM/W43-HERO large program: http://www.iram-institute.org/EN/content-page-292-7-158-240-292-0.html ALMA/ALMA-IMF large program NIKA2 large program GASTON
Instruments and Tools: Instruments: ALMA, NOEMA, Herschel and soon JWST Tools used: Getsources (Men’shchikov et al. 2012), PPMAP (Marsh et al. 2015), MnG-seg (Robitaille et al. 2014) http://sapm.qc.ca/%C3%A9lement-de-flux/lois-de-naissance-des-%C3%A9toiles-remises-en-question Research Group: HYDRIDES (ANR project 2013-2017)
Permanent staff: Aurore Bacmann, Astrid Bergeat, Michel Costes, Cecilia Ceccarelli, Fabien Dumouchel, Alexandre Faure, Philippe Halvick, Pierre Hily-Blant, Sébastien Le Picard, François Lique, Sébastien Maret, Christian Naulin, Claire Rist, Ioan Schneider, Ian Sims, Thierry Stoecklin, Laurent Wiesenfeld Technical staff: Didier Biet, Jonathan Courbe, Ewen Gallou, Jacques Sorieux, Daniel Travers PhD students (since 2010): Nezha Bouhafs, Simon Chefdeville, Labiad Hamza, Mario Hernandez- Vera, Mathieu Lanza, Romane Le Gal Post-docs (since 2010): Otoniel Alpizar, Fabien Daniel, Martin Fournier, Yulia Kalugina Contact: [email protected]
Laboratories: Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut des Sciences Moléculaires (ISM), Laboratoire Ondes et Milieux Complexes (LOMC), Institut de Phydique de Rennes (IPR) Institution(s): CNRS, Université Grenoble Alpes, Université de Bordeaux, Université Le Havre Normandie, Université de Rennes Website: http://ipag.osug.fr/Hydrides/
Key Research Facilities, Infrastructure and Equipment: Mésocentre CIMENT (Grenoble), mésocentre MCIA (Bordeaux), crossed molecular beam apparatus (Bordeaux), CRESU apparatus (Rennes)
Keywords: molecular energy transfer; state-to-state collisions; chemical pumping
Experimental and theoretical studies of the group: • Rotational energy transfer (cross sections and rate coefficients) • Quantum state-to-state collisions (inelastic and reactive) • Spectral-line radiative transfer calculations
Astrophysical context: • Excitation and chemistry of hydrides in the interstellar medium (molecular clouds, prestellar cores, photon-dominated regions) • Submillimeter (Herschel, SOFIA, ALMA) and centimeter (Effelsberg) observations
Collaborations: • M.H. Alexander, J. Klos, University of Maryland (USA) • D. Carty, Department of Chemistry, Durham (UK) • P. Caselli, J. Harju, Max-Planck-Institut für extraterrestrische Physik, Garching (Germany) • P. Dagdigian, Johns Hopkins University, Baltimore (USA) • M. Gérin, Observatoire de Paris • P. Honvault, Université de Dijon • O. Roncero, C.S.I.C., Madrid (Spain) • J. Tennyson, University College London (UK) • F. van der Tak, SRON Netherlands Institute for Space Research, Groningen (The Netherlands)
Highlights: • State-to-state chemistry of reactive ions. We have quantitatively reproduced, for the first time, the emission spectrum of CH+ as measured by Herschel satellite in photodissociation regions (Orion bar and NGC 7027). This was possible thanks to high-accuracy quantum calculations for + + 2 + + - the formation, excitation and destruction of CH via C ( P) +H2, CH + H and CH + e collisions (see Faure et al. 2017).
Comparison between our emission model for CH+(j®j-1) and Herschel observations towards the Orion bar (from Faure et al. 2017).
Most significant publications (<5): • State-to-state chemistry and rotational excitation of CH+ in photon-dominated regions Faure, A. et al. (2017) MNRAS 469 612 • Collisional excitation of NH3 by atomic and molecular hydrogen Bouhafs, N. et al. (2017) MNRAS 470 2204 • Rotational energy transfer in collisions between CO and Ar at temperatures from 293 to 30 K Mertens, L. A. et al. (2017) Chem. Phys. Lett. 683 521 • Experimental and theoretical analysis of low-energy CO+H2 inelastic collisions Chefdeville, S. et al. (2015) Astrophys. J. Lett., 799, L9 • Ortho-Para Selection Rules in the Gas-phase Chemistry of Interstellar Ammonia Faure, A. et al. (2013) Astrophys. J. Lett. 770 L2
Link to full publication list: http://ipag.osug.fr/Hydrides/publications.shtml
Press releases: http://ipag.osug.fr/Hydrides/links.shtml Project: Injection of stellar matter into the ISM
Timeframe: 2019-2024
Staff: Contact: Thibaut Le Bertre ([email protected]) Permanent staff in France: Thibaut Le Bertre, Jan Martin Winters (IRAM) Permanent staff in other countries: Lynn Matthews (MIT-Haystack: astronomer), P.T. Nhung (VNSC: astronomer), D.T. Hoai (VNSC: astronomer), PhD students (since 2010): D.T. Hoai (2012-2015, LERMA, astronomer). Post-docs (since 2010): P.T. Nhung (2013-2014, LERMA, astronomer).
Website:
Goals:
During the next years we will exploit CO data obtained with NOEMA and ALMA in order to study in detail the morpho-kinematics of circumstellar environments around mass losing evolved stars. In parti- cular we want to investigate the deviations from spherical symmatry, and to constrain the acceleration of outflows. We plan also to map, in the HI line at 21 cm, AGB and RSG outer shells and their turbulent trails at much higher resolution and sensitivity than previously using VLA, MeerKAT and FAST, with the aim of revealing how stellar matter is injected into the ISM. New thermo-chemical models of stellar winds will be developed at LERMA and ENS (P. Lesaffre) in close collaboration with our Vietnamese colleagues, and applied to ALMA/NOEMA spectroscopic maps.
Methods: Observations in CO (ALMA, NOEMA) and HI (VLA) lines, and modeling
Highlight: HI tail of RS Cnc. (attached : RSCnc_colormom0.gif) Caption : HI tail associated with the mass-losing AGB star RS Cnc (VLA; Hoai et al. 2014). The star is moving to the southeast. The tail has a length of ~0.6 pc.
Keywords: Asymptotic Giant Branch stars, Red Supergiants, circumstellar shells, mass loss
Most significant publications (< 5):
“The multi-scale environment of RS Cancri from CO and HI observations”, Hoai et al. (2014, A&A, 565, A54)
“Modelling the HI 21-cm line profile from circumstellar shells around red giants”, Hoai et al. (2015, MNRAS, 449, 2386) “Discovery of a shell of neutral atomic hydrogen surrounding the carbon star IRC+10216”, Matthews et al. (2015, MNRAS, 449, 220) “12CO emission from EP Aquarii: Another example of an axi-symmetric AGB wind ?”, Nhung et al. (2015, A&A, 583, A64) Link to full publication list: http://www.
Press releases: Title and html link.
Related projects: Title and html link.
Instruments and Tools: NOEMA, ALMA, VLA, MeerKAT, FAST Project: KInetic Database for Astrochemistry
Timeframe: 2009 -
Staff: Contacts: Valentine Wakelam ([email protected]) and Pierre Gratier ([email protected]). Permanent staff in France: Valentine Wakelam ([email protected]), Pierre Gratier ([email protected]), Jean-Christophe Loison ([email protected] + other French KIDA experts (http://kida.obs.u-bordeaux1.fr/contact.html). Permanent staff in other countries: KIDA experts from other countries (http://kida.obs.u-bordeaux1.fr/contact.html). Others (since 2010): Benjamin Pavone (2009 - 2013, LAB, engineer).
Website: http://kida.obs.u-bordeaux1.fr/
Goals: Provide formatted and commented kinetic data for astrochemical studies, i.e. gas-phase chemical reactions with associated partial rate coefficients, binding and diffusion energies for physisorbed species on various surfaces, surface reactions with activation energies. In addition to KIDA, and linked with it, we provide a database of chemical abundances observed in various regions of the interstellar medium (ISA). We also maintain a monthly newsletter sharing the recently accepted publications in astrochemistry (ACN).
Highlight: Several subsets of gas-phase chemical reactions are made available for astrochemical studies (kida.uva.2011, kida.uva.2014)
Keywords: astrochemistry, molecules, chemical reactions, rate coefficient, abundances.
Most significant publications (< 5): Reaction Networks for Interstellar Chemical Modelling: Improvements and Challenges Wakelam et al. 2010, Space Science Reviews, Volume 156, Issue 1-4, pp. 13-72, 10.1007/s11214-010-9712-5 A KInetic Database for Astrochemistry (KIDA) Wakelam et al. (2012) The Astrophysical Journal Supplement, Volume 199, Issue 1, article id. 21, 10 pp., 10.1088/0067-0049/199/1/21 The 2014 KIDA Network for Interstellar Chemistry Wakelam et al. (2015) The Astrophysical Journal Supplement Series, Volume 217, Issue 2, article id. 20, 7 pp. 10.1088/0067-0049/217/2/20
Instruments and Tools: KIDA http://kida.obs.u-bordeaux1.fr/ ISA http://isa.obs.u-bordeaux1.fr/ ACN http://acn.obs.u-bordeaux1.fr/ Project: MIST (Molecules, Magnetic Fields, and Intermittency in Cosmic Turbulence)
Timeframe: 2017-2022
Staff: • Contacts: Edith Falgarone ([email protected]). • Permanent staff in France: François Boulanger (LERMA, astronomer), Edith Falgarone (LERMA, astronomer, emeritus), Benjamin Godard (LERMA, astronomer), Pierre Hily-Blant (IPAG, astronomer), Pierre Lesaffre (LERMA, astronomer), François Levrier (LERMA, astronomer), Guillaume Pineau des Forêts (LERMA, astronomer, emeritus) • Permanent staff in other countries: N/A. • PhD students (since 2010): Thibaud Richard (2018-2021, LERMA) • Post-docs (since 2010): Andrew Lehmann (2017-2019, LERMA, astronomer), Alba Vidal Garcia (2018-2020, LERMA, astronomer).
Website: http://mist.lra.ens.fr
Goals: The discovery of molecules in the early universe is a challenging providence. Molecules unveil the truly cold universe in which stars form and their rich versatility provides unique diagnostics to unravel the “relative importance of purely gravitational effects and gas dynamical effects involving dissipation and radiative cooling”, recognized 40 years ago by White and Rees to be a central issue in theories of galaxy formation. Molecules also reveal that cosmic turbulence is far less dissipative than predicted by cosmological simulations, with a broad equipartition in a vast variety of media between the thermal energy of the hottest phases and the turbulent energy of the coldest. Our project focuses on the physics of turbulent dissipation, and its link to the emergence of molecules, in the magnetized compressible medium where gravitational instability develops to form stars and seed galaxies in the early universe.
Methods: The MIST project builds on a fundamental property of turbulence, its space-time intermittency: dissipation occurs in bursts. Our team fosters strong interactions between three main research axes: (1) observations of the chemical and thermal markers of turbulent dissipation in the high-redshift and local universe, (2) statistical analyses of the magnetic and velocity fields in samples of unprecedented size and sensitivity to study the non-Gaussian signatures of turbulent dissipation, and (3) numerical experiments dedicated to (a) the space-time structures of turbulent dissipation and the formation of molecules in their wake, and (b) the split of the energy trails between hot/thermal and cold/turbulent phases. This project benefits from the prodigious capabilities of the ALMA and NOEMA interferometers and the Planck satellite data on polarized Galactic foregrounds. The JWST, whose launch is postponed to 2019, should be another asset.
Highlight: Chemistry driven by turbulent dissipation, bridging theory and observations As this is a starting project, it has not yet produced results. However, it is based on a number of findings by our group, which are worthy to present. One of our assets is the careful control of dissipation, whether it is numerical or physical, whether it is viscous, resistive or ambipolar (see Momferratos+2014). We also have a great expertise in the coupling between chemistry and magneto-hydrodynamics, which allowed us to compare our models to observations and show the impact of turbulence dissipation on molecular chemistry (Godard+2014). Finally, our recent observations reveal for the first time the molecular dynamics in high-z galaxies (Falgarone+2017). One of our ambitions is to understand dissipation to the point where we are able to produce sub-grid models which will greatly help interpret the presence of molecules in such extremely turbulent media. We may not succeed, but even if we fail we are very likely to discover new alleys on the energy trail.
Simulations of a pc-scale field (5123): (Left) Extrema of dissipation due to viscosity (blue), resistivity (green) and ion-neutral friction (red) in a non-ideal incompressible MHD turbulence simulation (Momferratos et al. 2014). Contours show the largest increments of observables: line centroid velocity, Stokes parameters Q and U and polarization direction. (Right) Compressible MHD turbulence with viscous (green), ohmic (red) and numerical dissipations (blue) (Lesaffre et al. in prep.)
Keywords: Molecules - Magnetic fields - Interstellar medium - Turbulence - Chemistry - Intermittency - Numerical simulations - Statistics
Most significant publications (< 5): • E. Falgarone et al. (2017) Nature, 548, 430 • B. Godard ; E. Falgarone ; G. Pineau des Forêts (2014) A&A, 570, 27 • G. Momferratos ; P. Lesaffre ; E. Falgarone ; G. Pineau des Forêts (2014) MNRAS, 444, 86
Link to full publication list: N/A
Press releases: https://www.eso.org/public/news/eso1727/ https://public.nrao.edu/news/2017almaturbulentstarburst/
Related projects: • BxB (Interstellar B-fields crossing inflation B-modes) (http://bxb.lra.ens.fr)
Instruments and Tools: • ALMA Observatory (http://www.almaobservatory.org/en/home/) • NOEMA Interferometer (http://iram-institute.org/EN/noema-project.php) • JWST (https://www.jwst.nasa.gov) • トトロ (Totoro) computing cluster hosted by MesoPSL (http://www.mesopsl.fr) Project: Molecular complexity in high-mass protostars
Timeframe: 2017-2023
Staff: Contacts: Nathalie Brouillet ([email protected]) and Timea Csengeri ([email protected]). Permanent staff in France: Sylvain Bontemps (LAB, astronomer), Nathalie Brouillet (LAB, astronomer), Benoît Commerçon (ENS-Lyon, astronomer), Timea Csengeri (LAB, astronomer), Didier Despois (LAB, astronomer), Frédérique Motte (IPAG, astronomer), Valentine Wakelam (LAB, astronomer). Permanent staff in other countries: Arnaud Belloche (MPIfR, DE, astronomer), Karl Menten(MPIfR, DE, astronomer), Holger Müller (U. Cologne, DE, astronomer), Alvaro Sanchez-Monge (U. Cologne, DE, astronomer), Friedrich Wyrowski (MPIfR, DE, astronomer). PhD students (since 2010): Sarah Fechtenbaum (2012-2015), Jordan Molet (2016-2019), Laure Bouscasse (2017-), a new PhD as part of the Bordeaux Idex Junior Chair“C-Origins”(PI Csengeri) starting in 2019. Post-docs (since 2010): Tzu-Cheng Peng (2011-2013); a 3 year post-doc as part of the Bordeaux Idex Junior Chair “C-Origins”(PI Csengeri) starting in 2019.
Website: None
Goals: Probe the origins of complex organic molecules (COMs) during the formation of high-mass stars (dust surface versus gas phase after desorption). Investigate a possible new type of targets, the early hot cores, to search for the rarest COMs. Help to understand the origin of rare COMs in reference sources SgrB2 and Orion BN/KL as they are both made of hot cores associated with high-mass star formation.
Methods: Unbiased spectral surveys with IRAM 30m when possible (nearby single sources) and ALMA/NOEMA spectral surveys for more distant sources.
Highlight: Witnessing the formation of hot cores. Hot cores, such as SgrB2 and Orion BN/KL, are prime targets to search for organic compounds related to our cosmic origins. We here investigate young high-mass protostars which are the precursors of hot cores, and contains so-called early hot cores. A significant effort of our group to acquire ALMA data towards the richest protoclusters of the Galaxy has been rewarded with 3 individual programs (among which one is an ALMA large program, ALMA-IMF) allowing us to get spectral coverage at high spatial resolution for ~ 300 high-mass protostars at different evolutionary stages [see right part of the Figure below for 3 such high-mass protostars in the richest protocluster of the galactic disk, W43-MM1]. The recent highlight related to the formation of chemically rich hot cores was obtained for the young high-mass protostar G328.25-0.53 at 2.5 kpc. We found that its nascent hot core is actually made of two spots associated with accretion shocks (seen in v=1 methanol lines with ALMA) at the centrifugal barrier of an inner keplerian disk (Csengeri et al. 2018) [see left part of the Figure below]. Keywords: COMs; High-mass star formation; hot cores
Most significant publications (< 5): The search for high-mass protostars with ALMA revealed up to kilo-parsec scales (SPARKS): I. Indication for a centrifugal barrier in the environment of a single high-mass envelope, T. Csengeri, S. Bontemps, F. Wyrowski, A. Belloche, K. M. Menten, et al. 2018, A&A in press. The unexpectedly large proportion of high-mass star-forming cores in a Galactic mini-starburst, Motte, F.; Nony, T.; Louvet, F.; Marsh, K. A.; Bontemps, S., et al. 2018, Nature 04/2018. Unbiased spectral survey of CygX-N63: nascent hot core and pristine gas for high-mass star formation, S. Fechtenbaum, S. Bontemps, T. Csengeri, A. Belloche, F. Herpin, et al. 2017, A&A submitted, in revision. Antifreeze in the hot core of Orion - Detection of ethylene glycol in Orion-KL, N. Brouillet, D. Despois, X.H. Lu, A. Baudry, et al. 2015, A&A, 576, 129. Link to full publication list: None. Press releases: None. Related projects: SPARKS (PI T. Csengeri) ALMA-IMF (PI F. Motte) Instruments and Tools: ALMA. Project: Nanocosmos
Timeframe: 2014-2020
Staff: • Contacts: Christine Joblin ([email protected]) • Permanent staff in France: CNRS/Université de Toulouse IRAP/Research team: C. Joblin, H. Sabbah (IRAP/LCAR), K. Demyk, O. Berné IRAP/Engineer team: A. Bonnamy (OMP), L. Noguèz, D. Murat, O. Coeur-Joly LCAR-IRSAMC/Research team: P. Moretto-Capelle, S. Zamith LCPQ-IRSAMC/Research team: A. Simon, M. Rapacioli, F. Spiegleman LAPLACE/Research team: K. Makasheva, R. Clergeraux • Permanent staff in other countries: co-PIs of the Nanocosmos ERC Synergy project: J. Cernicharo (IFF-CSIC, Spain, Professor), J.-A. Martín-Gago (ICMM-CSIC, Spain, Professor), Associate IRAP Scientist; G. Mulas (Astronomer, OAC-INAF, Italy). • PhD students (since 2010): S. Rodriguez Castillo (2015-2017, IRAP/LCPQ), R. Bérard (2016- 2019, IRAP/LAPLACE), M. Carlos (2016-2019, IRAP/LCAR), S. Foschino (2017-2020, IRAP). • Post-docs (since 2010): P. Pilleri (2014-2017, IRAP), J. Zhen (2015, IRAP), L. Dontot (2015 & 2018, IRAP/LCPQ), M. Ji (2016-2018, IRAP), S. Chakraborty (2016-2018, IRAP), P. Jusko (2017-2019, IRAP), F. Mastrorocco (2019, IRAP).
Website: https://nanocosmos.iff.csic.es/
Goals: The objective of the Nanocosmos ERC Synergy project "Gas and dust from stars to the laboratory: exploring the Nanocosmos" is to combine astronomical observations, modelling, and top-level experiments to produce stardust analogues in the laboratory and identify the key species and steps that govern the formation of these nanograins and their evolution in different environments. This is an ERC Synergy project that involves two PIs in Madrid and one PI at CNRS/Université de Toulouse.
Methods: The project comprises different aspects including observations with ALMA of the dust formation zone in evolved stars, the development of new millimeter receivers, a large effort in laboratory astrophysics, as well as chemical modeling and quantum chemistry calculations. Four major innovative experimental setups have been developed, two in Madrid (Stardust and Gas Cell) and two in Toulouse (AROMA and PIRENEA 2). In the Stardust machine, new types of cosmic dust analogues are created by combining three magnetrons for the production of atoms. Astrophysical processes such as infrared heating in the environment of AGB stars and gas-grain chemistry at low temperatures can also be investigated. In AROMA, the coupling of efficient ion production and transmission to ion trapping and in-flight mass spectrometry leads to unique features in terms of detection and characterization of the molecular content of these dust analogues. With PIRENEA 2, we have designed a unique machine to study the physical and chemical properties of dust analogues in cosmic conditions. Similarly to PIRENEA, it is based on a cryogenic FT-ICR cell to mimic the isolation conditions in interstellar space. Nanograins of cosmic interest can be produced with a laser vaporisation cluster source and a molecular aggregation source with the possibility to thermalize the formed species. Finally, the Gas Cell is a new chemical reactor that was built to follow the evolution of molecular mixtures of astrophysical interest under ultraviolet radiation. The changes in gas composition are recorded by collecting the gas radio emission with very sensitive receivers that are the subject of on-going developments. The same radio receivers are to be used at the 40-m IGN telescope to make a census of the molecular content of evolved stars.
Highlight: The diversity of cosmic C-species investigated by AROMA Carbon-rich cosmic dust analogues have been produced in the Stardust machine but also using plasma reactors (LAPLACE) and the laser vaporization aggregation source (LVAP/PIRENEA 2) at IRAP/LCAR. We demonstrated the potential of AROMA to analyze the intimate molecular content of these particles and tell us about their formation and growth histories. Hundreds of peaks were identified in the mass spectra with notable discrepancies across the different types of samples. These differences can be used to trace the chemical history of each sample and are not a bias of our analysis. A double bound-equivalent (DBE) method is applied to sort the detected carbonaceous molecules into families of compounds. The DBE is representative of the unsaturation level of the molecules and thus corresponds to a direct measure of their aromaticity. The performed analysis reveals in addition of polycyclic aromatic hydrocarbons, the presence of other populations such as mixed aromatic-aliphatic species, carbon clusters and fullerenes. An internal database is being developed to cross linking the species and family of species detected in the different samples. On-going experiments indicate a similar diversity in meteorite samples, which opens perspectives to trace the origin of this extraterrestrial matter.
Keywords: astrochemistry, laboratory astrophysics, cosmic dust, polycyclic aromatic hydrocarbons, dust formation, dust processing, infrared spectroscopy, mass spectrometry
Most significant publications (< 5): • Investigating the importance of edge-structure in the loss of H/H2 of PAH cations: the case of dibenzopyrene isomers, Rodriguez Castillo, S., Simon, A., Joblin, C., IJMS 429 (2018), 189-197, DOI: 10.1016/j.ijms.2017.09.013 • Anharmonic vibrational spectroscopy of PAHs, Mulas, G., Falvo, C., Cassam-Chenaï, P., Joblin, C., JCP 149 (2018), 144102, 16pp., DOI: 10.1063/1.5050087 • Detection of Buckminsterfullerene emission in the diffuse interstellar medium, Berné, O., Cox, N. L. J., Mulas, G., Joblin, C., A&A 605 (2017), id.L1, 6 pp, DOI: 10.1051/0004- 6361/201630325 • Identification of PAH Isomeric Structure in Cosmic Dust Analogs: The AROMA Setup, Sabbah, H., Bonnamy, A., Papanastasiou, D., Cernicharo, J., Martín-Gago, J.-A., Joblin, C., ApJ 843 (2017), id. 34, 8 pp., DOI: 10.3847/1538-4357/aa73dd • Link to full publication list: https://nanocosmos.iff.csic.es/
Conferences and major outreach operations: • Energetic processing of large molecules and interstellar dust : Nanocosmos and EPoLM-3 meetings (Toulouse, 12-16/06/2017), https://epolm3-nanocosm.sciencesconf.org/ • European Conference on Laboratory Astrophysics- ECLA 2016 : Gas on the Rocks (Madrid, 21-25/11/2016), www.ecla2016.com • ERC comics Estrella, https://www.erccomics.com/comics/estrella, https://lejournal.cnrs.fr/articles/bulles-de-science • NANOCOSMOS documentary: "Un viaje a lo pequeño", https://nanocosmos.iff.csic.es
Related projects: • Innovative Training Network EUROPAH, PhD student: G. Wenzel (2017-2020, IRAP) Project: ORION-B (Outstanding Radio-Imaging of OrioN-B)
Timeframe: 2013-2021
Staff: Contacts: Jérôme Pety ([email protected]) and Maryvonne Gerin ([email protected]). Permanent staff in France: Sébastien Bardeau (IRAM, software engineer), Maryvonne Gerin (LERMA, astronomer), Pierre Gratier (LAB, astronomer), Annie Hughes (IRAP, astronomer), David Languignon (software engineer), Franck Le Petit (LERMA, astronomer), François Levrier (LERMA, astronomer), Jérôme Pety (IRAM, astronomer), Evelyne Roueff (LERMA, astronomer, emeritus), Pascal Tremblin (CEA, astronomer). Permanent staff in other countries: Javier Goicoechea (CSIC, Spain, astronomer), Viviana Guzman (PUC, Chile, astronomer), Harvey Liszt (NRAO, USA, astronomer), Karin Oberg (Harvard, USA, astronomer), Nicolas Peretto (Cardiff Univ., UK, astronomer). PhD students (since 2010): Jan Orkisz (2015-2018, IRAM, astronomer). Post-docs (since 2010): Emeric Bron (2014-2018, CSIC, Spain, astronomer), Pierre Gratier (2013-2016, LAB, astronomer), Viviana Guzman (2013-2018, Harvard, USA, and then JAO, Chile).
Website: http://www.iram-institute.org/~pety/ORION-B/
Goals: Molecular line intensities and their ratios are commonly used to determine the properties of Galactic and extra-galactic clouds and their star-forming regions. To fully exploit the broad band capabilities of the new generation (sub-)millimeter receivers, which turns every observation nearly into a line survey, detailed bench-marking of available and new line diagnostics is required. We aim to characterize the physical and chemical properties of Orion B in relation to its star forming activity, and establish it as a local template for interpreting Galactic and extra-galactic molecular line observations.
Methods: The ORION-B project currently uses the IRAM-30m/EMIR 3mm receiver to image a field of 5 square degrees, located near the southern edge of the Orion B molecular cloud, including the Horsehead nebula, NGC 2023, and NGC 2024. A total frequency bandwidth of 40 GHz is observed with a spectral resolution of 195 kHz (0.6 km s-1), a typical spatial resolution of 26'' (i.e., 50 mpc or 104 AU at the Orion B distance of 400 pc), and a typical sensitivity of 0.1 K. We succeeded to image the J=1-0 line of the CO isotopologues as well as the strongest 3mm lines of HCO+, HCN, HNC, CN, + CCH, c-C3H2, CS, SO, N2H , SiO, CH3OH, H2CO, and many other weaker features. We aim at adapting statistical methods and machine learning tools to finely characterize the structure, chemistry and dynamics of this particular GMC, and identify new molecular diagnostics that could be used in a wide variety of regions.
Highlight: Characterizing the physics and chemistry of a Giant Molecular Cloud from its molecular emission Using the Mean-Shift clustering algorithm, Bron et al. (2017) have been able to separate the different physical environments on the basis of a restricted sample of molecular line intensities. Key factors for the matter evolution like its density or its UV illumination can be approximately retrieved without any additional information with the well-known method of Principal Component Analysis (Gratier et al. 2017).
Keywords: Orion B – Giant Molecular Clouds – Interstellar Medium – Galaxies – Star formation – Molecular emission – Statistics – Machine learning – Wide-Field Imaging – Wide-Bandwidth imaging – Hyper-Spectral Imaging
Most significant publications (< 5): Clustering the Orion B giant molecular cloud based on its molecular emission, Bron et al. 2018, A&A, 610, 12, doi:10.1051/0004-6361/201731833 Dissecting the molecular structure of the Orion B cloud: Insight from Principal Component Analysis, Gratier et al. 2017, A&A, 599, 100, doi:10.1051/0004-6361/201629847 Turbulence and star formation efficiency in molecular clouds: solenoidal versus compressive motions in Orion B, Orkisz et al. 2017, A&A, 599, 99, doi:10.1051/0004-6361/201629220 The anatomy of the Orion B Giant Molecular Cloud: A local template for studies of nearby galaxies, Pety et al. 2017, A&A, 599, 98, doi:10.1051/0004-6361/201629862 Link to full publication list: https://www.researchgate.net/project/ORION-B-The-Anatomy-of-a-Giant-Molecular-Cloud
Press releases: Beyond the appearances: The anatomy of the Orion Jedi revealed by radio-astronomy. Le nuage d'Orion radiographié comme jamais.
Related projects: SCHISM: Structure and Chemistry of the Inter-Stellar Medium. Horsehead WHISPER: Wideband High-resolution. Iram-30 m Surveys at two Positions with Emir Receivers PHANGS: Physics at High Angular resolution in Nearby GalaxieS
Instruments and Tools: IRAM-30m telescope (http://www.iram-institute.org/EN/30-meter-telescope.php) Meudon PDR code (https://ism.obspm.fr/) Project: ORISTARS
Timeframe: 2012-2018 Staff: • Contacts: Philippe André ([email protected]). • Permanent staff in France: Philippe André (CEA/AIM, astronomer), Alexander Menshchikov (CEA/AIM, astronomer), Anaëlle Maury (CEA/AIM, astronomer) • Permanent staff in other countries: Nicolas Peretto (Cardiff University, UK, astronomer). • PhD students (since 2010): Doris Arzoumanian (2009-2012, AIM, astronomer), Pedro Palmeirim (2010-2013, AIM, astronomer), B. Ladjelate (2014-2017, AIM, astronomer) • Post-docs (since 2010): Vera Könyves (2012-2017, AIM & IAS, astronomer), Arabindo Roy (2012-2017, AIM, astronomer), Evangelia Ntormousi (2012-2017, AIM, astronomer), Andrea Bracco (2015-2017, AIM, astronomer), Yoshito Shimajiri (2013-2019, AIM, astronomer)
Website: http://irfu.cea.fr/Phocea/Vie_des_labos/Ast/ast_technique.php?id_ast=3627
Goals: On the research front, the ERC AdG project ORISTARS aimed to study the origin of molecular filaments, the fragmentation of filaments into prestellar cores and its possible link to the origin of the core mass function (CMF) and stellar initial mass function (IMF), and the rotational sub-fragmentation of prestellar cores into binary protostars and the formation of protostellar disks. On the instrumental front, the project aimed to equip the new generation millimeter continuum camera of the IRAM 30m telescope (NIKA-2) with a Polarization Channel, with the ultimate goal of probing magnetic fields.
Methods: Confronting millimeter/submillimeter observations of nearby molecular clouds with numerical simulations and helping to develop new relevant instrumentation on mm/submm telescopes.
Highlight: Consolidation of a filamentary paradigm for solar-type star formation and opening of a polarization channel on the NIKA2 camera to probe the role of magnetic fields. Detailed analysis of the results from the Herschel Gould Belt survey (e.g. Könyves+2015) have led to very significant advances in our understanding of the link between the structure of the cold ISM IRAM30m + NIKA 1.2mm and the star formation process. Overall, the Herschel results support a filamentary paradigm for solar-type star formation in two main steps: first, multiple large-scale compressions of interstellar material in supersonic MHD flows generates a cobweb of ~0.1 pc–wide molecular filaments; second, the densest filaments fragment into prestellar cores by gravitational instability above the critical line mass of nearly isothermal gas cylinders (e.g. André+2014). This paradigm has the merit that it can account for the “base” of the CMF/IMF and possibly the Salpeter power law at the high-mass end as well (Roy+2015). It differs from the classical “gravo-turbulent” fragmentation picture in that it relies on the unique properties of filamentary geometry. One of the next steps will be to clarify the role of magnetic fields in the fragmentation of molecular filaments and the formation of prestellar cores on scales < 0.1 pc. This cannot be done with Planck polarization data due to insufficient resolution but will become possible in the coming years with NIKA2-Pol, the polarization channel opened up by the ORISTARS project on the NIKA2 camera at the IRAM 30m telescope.
Keywords: stars: formation, ISM: clouds, ISM: filaments, ISM: structure, submm, magnetic fields
Most significant publications (< 5):
• From Filamentary Networks to Dense Cores in Molecular Clouds: Toward a New Paradigm for Star Formation, André, Ph., Di Francesco, J., Ward-Thompson et al. 2014, Protostars and Planets VI, p. 27-51 DOI: 10.2458/azu_uapress_9780816531240-ch002
• Herschel view of the Taurus B211 filament & striations: evidence of filamentary growth?, Palmeirim, P., André, Ph., Kirk, J. et al. 2013, A&A DOI: 10.1051/0004-6361/201220500
• A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey, Könyves, V., André, Ph., Menshchikov, A. et al. 2015, A&A DOI: 10.1051/0004-6361/201525861
• Possible link between the power spectrum of interstellar filaments and the origin of the prestellar core mass function, Roy, A., André, Ph., Arzoumanian, D. et al. 2015, A&A DOI: 10.1051/0004-6361/201526431
• Probing changes of dust properties along a chain of solar-type prestellar and protostellar cores in Taurus with NIKA, Bracco, A., Palmeirim, P., André, Ph. et al. 2017, A&A DOI: 10.1051/0004-6361/201731117
Related projects: • STARFICH ANR (2012-2016) • Herschel Gould Belt Survey - http://gouldbelt-herschel.cea.fr • IRAM Large Program CALYPSO - http://irfu.cea.fr/Projets/Calypso/Welcome.html and http://www.iram-institute.org/EN/content-page-317-7-158-240-317-0.html
Instruments and Tools: • NIKA2 camera on IRAM 30m telescope: http://ipag.osug.fr/nika2/Welcome.html • ArTéMiS camera on APEX 12m telescope: - http://www.apex- telescope.org/instruments/pi/artemis/ and http://irfu.cea.fr/Phocea/Vie_des_labos/Ast/ast_technique.php?id_ast=1020 • Database of column density maps and dense core catalogs from Herschel Gould Belt survey results: http://gouldbelt-herschel.cea.fr/archives
Project: PARCS (ANR 13-BS08-005)
Timeframe: 2014-2017
Staff: Contacts: Joëlle Mascetti (ISM, Bordeaux) ([email protected]) Permanent staff in France: Aude Simon (LCPQ, Toulouse), Céline Toubin (PhLAM, Lille). PhD students (since 2010): Eric Michoulier (2015-2017, PhLAM & LCPQ). Post-docs (since 2010): Jennifer Noble (2015-2016, ISM).
Website: http://www.lcpq.ups-tlse.fr/anr-parcs/
Goals: The ambition of the PARCS project was to bring new elements for the understanding of AIBs and DIBs assignments through the study of: (1) the photo-reactions of PAHs embedded in or trapped on water ice and (2) the reactions of PAHs with iron atoms. The originality of this project was to propose pioneering joint theoretical and experimental treatments of these reactions.
Methods: In the experimental part, the challenging novelty was the study of ternary PAH/Fe/H2O systems at cryogenic temperatures, that has been made possible using matrix isolation spectroscopy techniques, together with a specially designed furnace fixed to a cryostat, allowing co-deposition of Fe and PAH, and of two spectrometers, allowing to run both IR and UV spectroscopy on the same sample. The theoretical study implied the elaboration of a multiscale-multimethod approach that uses some of the best current available techniques with various levels of sophistication and efficiency: DFTB, MD-DFTB, PI-MD-DFTB, ab-initio methods CASPT2, …
Highlight: Efficient photochemistry of PAH:water and Fe:water complexes We have described: - The effects of the environment (argon matrix, water ice) on the geometry/energetics/IR spectra of water aggregates and on their complexes with PAHs - The efficient photochemistry of PAH:water complexes and PAH oxidation under soft UV-irradiation, whereas this reaction was supposed to occur only in water ices subject- ed to VUV radiation - The evolution of the IR spectra and the variation of the ionization potentials of PAHs when adsorbed on water ice surfaces of different structures (amorphous or crystalline) - The effect of the water ice structure (amorphous or crystalline) on the efficiency of the photo-oxidation of PAHs - The efficient photochemistry of Fe:water complexes with the formation of iron-bearing molecules and the production of hydrogen. We have also produced new theoretical developments concerning i) force fields transferable to any PAH, ii) prediction of adsorption energies for large PAHs, and iii) implementation of new methods in quantum chemistry and molecular dynamics codes. Adsorption of coronene on interstellar water ice viewed by molecular dynamics.
Keywords: PAHs, water ice, matrix isolation spectroscopy, DFTB, molecular dynamics, metadynamics
Most significant publications (< 5): Formation of coronene:water complexes: FTIR study in argon matrices and theoretical char- acterization, A. Simon, J. A. Noble, G. Rouaut, A. Moudens, C. Aupetit, C. Iftner and J. Mascetti, Phys. Chem. Chem. Phys. 2017, 19, 8516-8529, DOI: 10.1039/C6CP08559H
Photochemistry of Fe:H2O Adducts in Argon Matrices : A Combined Experimental and Theo- retical Study in the mid-IR and UV-Visible Regions, V. Deguin, J. Mascetti, A. Simon, N. Ben Amor, C. Aupetit, S. Latournerie, J. A. Noble, J. Phys. Chem. A 2018, 122, 529-542, DOI: 10.1021/acs.jpca.7b09681. Efficient photochemistry of coronene:water complexes, J. A. Noble, C. Jouvet, C. Aupetit, A. Moudens and J. Mascetti, Astron. Astrophys. 2017, 599, A124, DOI: 10.1051/0004-6361/201629613 Adsorption of PAHs on interstellar ice viewed by classical molecular dynamics, E. Michoulier, J. A. Noble, A. Simon, J. Mascetti, C. Toubin, PCCP 2018, 20, 8753-8764. DOI: 10.1039/C8CP00593A. Adsorption and ionisation energies of polycyclic aromatic hydrocarbons on water ice: compu- tational studies, E. Michoulier, N. Ben Amor, M. Rapacioli, J. A. Noble, J. Mascetti, C. Toubin and A. Simon, PCCP 2018, accepted manuscript, DOI: 10.1039/C8CP01175C.
Link to full publication list: http://www.lcpq.ups-tlse.fr/anr-parcs/pages/publi.html
Press releases: Title and html link.
Related projects: Title and html link.
Instruments and Tools: deMonNano code (http://demon-nano.ups-tlse.fr) Project: PHANGS (Physics at High Angular resolution in Nearby GalaxieS)
Timeframe: 2016-2023
Staff: · Contacts: Annie Hughes ([email protected]) and Jérôme Pety ([email protected]). · Permanent staff in France: Annie Hughes (IRAP, astronomer), Jérôme Pety (IRAP, astronomer), Eric Emsellem (ESO, astronomer) · Permanent staff in other countries: Eva Schinnerer (MPIA, Germany, astronomer), Adam Leroy (OSU, USA, astronomer), Guillermo Blanc (U. Chile, Chile, astronomer), Antonio Usero (OAN), Diederik Kruijssen (ARI, Germany, astronomer), Erik Rosolowsky (U. Alberta, Canada, astronomer), Karin Sandstrom (UCSD, USA, astronomer), Patricia Sanchez Blazquez (PUC, Spain, astronomer), Andres Escala (U. Chile, Chile, astronomer), Miguel Querejeta (OAN, Spain, astronomer), Janice Lee (STScI, USA, astronomer) · PhD students (since 2010): · Post-docs working in France (since 2010): Cinthya Herrera (2015- present, IRAM, astronomer), Diane Cormier (2018 - present)
Website: http://www.phangs.org
Goals: We aim to understand the interplay of the small-scale physics of gas and star formation with galactic structure and galaxy evolution by obtaining the first comprehensive view of the chemo- dynamical evolution of the star formation process across a representative sample of normal star- forming main sequence galaxies in the local Universe. We use observations of ~80 nearby galaxies to understand how physics near the “cloud” scale are affected by galaxy-scale conditions, how they affect still smaller scale processes, and how these influence the evolution of whole galaxies.
Methods: For 30 years, our observational understanding of extragalactic star formation has been built on individual case studies and low resolution surveys of small galaxy samples. PHANGS is leading three flagship observing programmes with ALMA, VLT/MUSE and HST to move the field into the era of big surveys. With 75 hours of ALMA 12m observations, PHANGS is imaging CO(2-1) at 1” resolution across the disks of all massive (log M_star > 9.75 M_sun) star-forming galaxies in the local volume (d<17 Mpc). This will yield >100,000 giant molecular clouds spread across a sample of galaxies and environments that is truly representative of star formation in the current epoch. The complementary PHANGS MUSE and PHANGS HST programmes are conducting matched high resolution observations to measure diagnostics of star formation, HII region and young stellar cluster properties, chemical mixing and enrichment, stellar populations, and star formation feedback. NOEMA and MaNGA are being used to obtain matching quality surveys for key northern targets.
A key parameter for almost all theories of star formation is the gas volume density, which is primarily accessible to extragalactic observers via multi-line mm-wave spectroscopy. Due to the faintness of so- called ‘high density tracers’ (typically 30x fainter than CO), previous extragalactic millimetre line surveys have mostly targeted active galaxies (starbursts, AGN) and bright galactic nuclei. With the improved sensitivity and wide bandwidth of new receivers (such as EMIR on the IRAM 30m), another important observational effort by PHANGS is to use the information from wideband, multi-line millimetre surveys to characterise the gas density distribution across the disks of normal star-forming galaxies. Highlight: Using new ALMA observations obtained as part of the PHANGS ALMA Large Programme, Sun et al (2018) have characterised the cloud-scale properties and structure of the molecular interstellar medium across 30000 independent sightlines in 15 nearby galaxies. Contrary to the notion of ‘universal GMCs’, the molecular gas properties in this pilot sample show a clear dependence on host galaxy properties, such that the velocity dispersion and mass surface density of the molecular gas each vary by several orders of magnitude among the different systems. However, the cloud-scale virial parameter, i.e. the ratio of kinetic to self-gravitational potential energy of the molecular gas, shows only small variations from galaxy to galaxy, suggesting that most molecular gas structures at ~100pc spatial scales in our target galaxies are close to energy equipartition.
Keywords: Interstellar Medium – Galaxies – Star formation – Galaxy Evolution — Giant Molecular Clouds – Star Formation Feedback
Most significant publications (< 5): · Do Spectroscopic Dense Gas Fractions Track Molecular Cloud Surface Densities? Gallagher et al. 2018, ApJ Letter, arXiv:1811.07940 · A 50 pc Scale View of Star Formation Efficiency across NGC 628 Kreckel et al. 2018, ApJ Let- ter, 863, L21 · Star Formation Efficiency per Free-fall Time in nearby Galaxies Utomo et al. 2018, ApJ Letter, 861, L18 · Cloud-scale molecular gas properties in 15 nearby galaxies Sun et al. 2018, ApJ, 860, 172 (see youtube video) · A model for the Onset of Self-gravitation and Star Formation in Molecular Gas Governed by Galactic Forces: I. Cloud-scale Gas Motions Meidt et al. 2018, ApJ, 854, 100
Link to full publication list: https://sites.google.com/view/phangs/publications Press releases:
Related projects: · PAWS: The PdBI Arcsecond Whirlpool Survey · EMPIRE: EMIR Multiline Probe of the ISM Regulating Galaxy Evolution · HERACLES: HERA CO-Line Extragalactic Survey · MUSTANG: Multi-scale Star Formation across Nascent Galaxies · OrionB (http://iram.fr/~pety/ORION-B/)
Instruments and Tools: · ALMA (http://www.almaobservatory.org) · IRAM: NOEMA and 30m telescope (http://www.iram.fr/) · MUSE (http://muse-vlt.eu/science/) · HST (https://www.nasa.gov/mission_pages/hubble/main/index.html) Project: the PILOT balloon-borne instrument
Timeframe: 2009-2020
Staff: • Contacts: Jean-Philippe Bernard ([email protected]) • Permanent staff in France (non exhaustive): Jean-Philippe Bernard (IRAP, CNRS, PI), Jonathan Aumont (IRAP, CNRS), Jean-Pierre Dubois (IAS, engineer), Jean Evrard (CNES, engineer, Chef de Projet), Annie Hughes (IRAP, astronomer), Yuying Longval (IAS, engineer), Bruno Maffei (IAS, Professor), Johan Montel (CNES, engineer), Baptiste Mot (IRAP, engineer, Chef de Projet), François Pajot (IRAP, CNRS), Isabelle Ristorcelli (IRAP, CNRS), Louis Rodriguez (CEA, engineer)
• Permanent staff in other countries (non exhaustive): Paolo deBernardis (LaSapienza, Italy, astronomer), Sylvia Masi (LaSapienza, Italy, astronomer), Peter Ade (Cardiff University, UK, astronomer), Carole Tucker (Cardiff University, UK, astronomer), Giorgio Savini (UCLO , UK), Jan Tauber (ESTEC, Netherlands, astronomer) • PhD students (since 2010): Ruka Misawa (2012-2016, IRAP, astronomer), Gabriel Foënard (2015-2018, IRAP, astronomer). • Post-docs (since 2010): Annie Hughes (2016-2017, IRAP, astronomer), Anna Mangilli (2017- 2019, IRAP, astronomer).
Website: http://pilot.irap.omp.eu
Goals: PILOT is a balloon-borne experiment observing the polarization of dust emission at 240 microns. The goal of these measurements is to determine the geometry of the magnetic field and the nature of dust grain through their magnetic properties.
Methods: PILOT has a large instantaneous field of view of almost 1 square degree and an angular resolution of 2.2’. The experiment is designed to map large regions of the sky with high sensitivity using large format multiplexed bolometer arrays, from an altitude of 40 km, above most of the atmospheric absorption.
Highlight: Geometry of the magnetic field in the Galactic Central Molecular Zone. The PILOT experiment has recently measured the orientation of the magnetic field over the central molecular zone of our Galaxy. The field appears extremely organized, with a tilt angle of 22° clockwise with respect to the galactic plane, and possibly very intense. The figure shows the intensity map (color) and magnetic field sky orientation (striations) observed with PILOT at 240 microns.
Keywords: balloon experiment, dust emission, polarization, magnetic field
Most significant publications (< 5): • Geometry of the magnetic field in the Central Molecular Zone, as measured by PILOT, Mangilli et al 2019, submitted to A&A, arXiv:1901.06196v1 • PILOT balloon-borne experiment in-flight performance, Mangilli et al. 2019, accepted in experimental Astronomy, arXiv:180405645M • PILOT: a balloon-borne experiment to measure the polarized FIR emission of dust grains in the interstellar medium, Bernard et al. 2016, ExA, 42 199 Link to full publication list: see http://pilot.irap.omp.eu
Press releases: • http://www.cite-espace.com/actualites-spatiales/pilot-un-ballon-pour-le-cosmos • http://www.ambafrance-ca.org/CNES-s-PILOT-telescope-completes-first-successful-balloon- flight-over-Canada • http://www.parlonspeuparlonscience.com/spip.php?article111 • https://pilot.cnes.fr/fr/deuxieme-vol-pilot-en-australie-un-atterrissage-en-douceur-limage-du- lacher-plus-de-33-heures-plus
Related projects: • COPILOT Project: Radiative feedback from massive stars
Timeframe: 2017-2025
Staff: Contacts: Olivier Berné ([email protected]) and Emilie Habart ([email protected]). Permanents in France: Alain Abergel (IAS, professor), Emanuel Dartois (ISMO, researcher) Permanents in other countries: See full list here : http://jwst-ism.org/?page_id=29 PhD students (since 2010): to come Post-docs (since 2010): to come
Website: http://www.jwst-ism.org
Goals: The James Webb Space telescope (NASA/ESA/CSA) will be launched in 2019. During the first months of operations, 500 hours of director’s time has been allocated to 13 “Early Release Science” programs. The goals of these programs will be 1) to provide first-look public data to a wide community as soon as possible after launch, 2) to test the instruments and observing modes, 3) to help prepare the community for the open time proposals. Our program, which has been accepted, concerns observations of photodissociation regions and is coordinated by an international “Core team” of 20 scientists and supported by more than 100 “science collaborators“ . The PI team is composed of Olivier Berné, Emilie Harbart, and Els. Peeters. More information on the scientific objective is given in the rationale.
Methods: Massive stars disrupt their natal molecular cloud material by dissociating molecules, ionizing atoms and molecules, and heating the gas and dust. These processes drive the evolution of interstellar matter in our Galaxy and throughout the Universe from the era of vigorous star formation at redshifts of 1-3, to the present day. Much of this interaction occurs in Photo-Dissociation Regions (PDRs) where far-ultraviolet photons of these stars create a largely neutral, but warm region of gas and dust. PDR emission dominates the IR spectra of star- forming galaxies and also provides a unique tool to study in detail the physical and chemical processes that are relevant for most of the mass in inter- and circumstellar media including diffuse clouds, protoplanetary disk – and molecular cloud surfaces, globules, planetary nebulae, and starburst galaxies. With this project we will provide template datasets designed to identify key PDR characteristics in JWST spectra in order to guide the preparation of Cycle 2 proposals on star-forming regions in our Galaxy and beyond. We plan to obtain the first spatially resolved, high spectral resolution IR observations of a PDR using NIRCam, NIRSpec and MIRI. These data will test widely used theoretical models and extend them into the JWST era. We have engaged the broader community as exemplified by the supporting large international team. We will assist the community interested in JWST observations of PDRs through science-enabling products that will guide observational planning and allow fast data analysis. We will train the community through telecons and dedicated workshops. Highlight:
Coming soon
Keywords:
Photodissociation regions, JWST, interstellar medium, infrared spectroscopy.
Most significant publications (< 5): Coming soon
Link to full publication list: http://www.
Press releases: Announcement of selection of ERS programs: https://jwst.stsci.edu/news-events/news/News %20items/selections-made-for-the-jwst-directors-discretionary-early-release-science-program
CNRS press release : http://www.cnrs.fr/midi-pyrenees/actualites/article/communique-de-presse-jwst-un-regard-inedi t-sur-la-matiere-interstellaire-a-l CSIC press release : http://www.icmm.csic.es/mag/index.php/2017/11/13/time-for-the-cycle-1-of-the-jwst/
Related projects:
Instruments and Tools: JWST Meudon PDR core Project: SICAL (Simulation d’Irradiation de Carbones Astrophysiques en Laboratoire)
Timeframe: 2011-
Staff: Contacts: Emmanuel Dartois ([email protected]) and Marin Chabot ([email protected]). Permanent staff in France: Karine Béroff (ISMO), Marin Chabot (IPNO), Emmanuel Dartois (ISMO), Thomas Pino (ISMO), Marie Godard (CSNSM) Permanent staff in other countries: Markus Bender (GSI, Germany), Daniel Severin (GSI, Germany), C. Trautmann (GSI, Germany) PhD students (since 2010): Marie Godard (2009-2011, IAS) Aurélie Jallat (2013-2015, IPNO) Post-docs (since 2010): Ivan Alata (2014-2015, IAS)
Goals: - Probe experimentally the chemical paths induced by radiation such as UV or ions (Cosmic Rays), for the synthesis of new materials and for their adequacy with the radiative environments encountered in interstellar space. - Interpret the astrophysical observables in the light of the analogues produced and species released upon interaction with the radiative environments. - Analysis of synthetic laboratory analogues relevant for the development of spectral fingerprints related to their underlying structural organization. - Produce quantitative measurements (cross section) of the processes for an implementation in models used by the astrophysical community.
Methods: Simulations of the ISM solid phases and their evolution can be performed in the laboratory. These, through different methods of analysis, shed light on the complex interactions between physical and chemical processes acting in the diffuse interstellar medium. The diffuse medium contains VUV photons and high-energy particles, cosmic rays, that will have common and different energy deposition behaviors. VUV (~10 eV) photons dissociate chemical bonds as well as high-energy ions that can also ionize the material locally. Our team produces analogues to the material, in particular carbonaceous, observed in the diffuse Galactic environments (SICAL, Nanograins, PRIMALE experiments). We expose them to laboratory simulated UV sources and Cosmic Rays sources on particles accelerators (GSI, Darmstadt, Germany; Tandem, Orsay, France). The determination of the efficiencies of the processes serves the astrophysical community and the modeling of the interstellar medium evolution.
Highlight: Cosmic rays irradiation of interstellar dust analogues: Small carbonaceous species release The laboratory simulations and measurements of processes induced by radiations observed in space allow constraining their importance. The objective of these studies is to provide data on the evolution of the interstellar material, to understand its further evolution and provide constraints for modelers of astrophysical environments. Interstellar dust grain particles are immersed in vacuum ultraviolet (VUV) and cosmic ray (high energy particles) radiation environments influencing their physicochemical composition. Owing to the energetic ionizing interactions, carbonaceous dust particles release fragments that have direct impact on the gas phase chemistry. The exposure of carbonaceous dust analogues to cosmic rays is simulated in the laboratory by irradiating films of hydrogenated amorphous carbon interstellar analogues with energetic ions. New species formed and released into the gas phase are explored.
Fig 1: View of the experimental setup configuration used to study irradiation of interstellar dust analogues at GSI. The M branch equipped with an FTIR spectrometer, QMS and cryogenic high vacuum sample chamber is coupled to the GSI UNILAC delivering swift heavy ion beams.
For these experimental simulations, thin hydrogenated amorphous carbon films (called a-C:H), astrophysical analogues giving rise to a widespread astronomical spectroscopic signature observed at 3.4 μm in the diffuse medium of galaxies, were irradiated with gold (950 MeV), xenon (630 MeV), and carbon (43 MeV) ions at the GSI UNILAC accelerator (see Fig 1 for a view of the experimental setup). The evolution of the dust analogues was monitored in situ as a function of fluence at 40, 100, and 300K. Effects on the solid phase are studied by means of infrared spectroscopy complemented by simultaneously recording mass spectrometry of species released into the gas phase. Specific species produced and released under the ion beam are analyzed.
The main radiolysis product is H2, participating in the dehydrogenation of the a-C:H in an astrophysical context. These irradiations also show that the production of numerous small hydrocarbons (CxHy ; x = {1, 4}) is efficient with swift heavy ions (see Fig. 2), and increases over the H2 production with the deposited energy.
The cross sections derived from the experiments for the interaction with swift heavy ions were implemented in an astrophysical model showing that the effect of CR irradiations are important in intermediate to dense regions where the high-energy CR component penetrates much deeper with respect to the external UV field. The CR reaches at depth equilibrium with an induced secondary UV field, produced by cosmic ray interaction with H2 (See Fig.3). Fig 2: QMS time integrated signal for a-C:H sample irradiated with 132Xe21+ (orange bars) at 300 K. The best model species fits contributing to the QMS signal are shown in blue. The labels above mark the positions where residual contaminant gases could contribute.
Fig 3: CH bond destruction timescale associated with Galactic cosmic rays (GCR) irradiation as a function of different assumption on the low-energy GCR ions spectrum (through an E0 parameter). The colored area gives the error bar obtained from the reported measurements uncertainties on the cross section. The corresponding ionization rate calculated is reported on the opposite axis. The observed interstellar ionization rates for dense clouds and mean values for diffuse clouds are shown with dashed lines.
The production of these carbonaceous species will contribute to eroding the a-C:H dust grains. The extent of this process will depend on the hydrogen content of the interstellar dust grains. If the hydrogen content is high, either intrinsically or via hydrogenation by interaction with the ambient hydrogen gas, the production of small volatile carbonaceous species is efficient, and leads to the complete destruction of the grains while the species released enrich the gas phase chemistry. We expect that this efficiency will decrease if the hydrogen content gets much lower and that the grains will eventually convert into a polyaromatic structure. The species released during experiments simulating the cosmic ray ions, starting with less hydrogenated, more polyaromatic interstellar analogues, will be further investigated using dedicated forthcoming experiments.
Keywords: Astrochemistry, Cosmic rays, Interstellar dust, Laboratory astrophysics
Most significant publications (< 5): Swift heavy ion irradiation of interstellar dust analogues. Small carbonaceous species released by cosmic rays. Dartois, E., Chabot, M., Pino, T., Béroff, K., Godard, M., Severin, D., Bender, M., Trautmann, C. 2017, Astronomy and Astrophysics 599, A130. DOI:10.1051/0004-6361/201629646 Vacuum ultraviolet of hydrogenated amorphous carbons. II. Small hydrocarbons production in Photon Dominated Regions. Alata, I., Jallat, A., Gavilan, L., Chabot, M., Cruz-Diaz, G.~A., Munoz Caro, G.~M., Béroff, K., Dartois, E., 2015, Astronomy and Astrophysics 584, A123. DOI:10.1051/0004-6361/201526368
Ion irradiation of carbonaceous interstellar analogues. Effects of cosmic rays on the 3.4 m interstellar absorption band. Godard, M., and 10 colleagues 2011, Astronomy and Astrophysics 529, A146. DOI:10.1051/0004-6361/201016228 Link to full publication list: http://www.
Press releases: https://www.ias.u-psud.fr/fr/content/une-simulation-exp%C3%A9rimentale-de-l %E2%80%99%C3%A9jection-d%E2%80%99esp%C3%A8ces-carbon %C3%A9es-par-les-grains
Related projects: Title and html link.
Instruments and Tools: SICAL Nanograins PRIMALE GSI (https://www.gsi.de/) Tandem (ipnwww.in2p3.fr/Tandem) Project: THEMIS (The Heterogeneous dust Evolution Model for Interstellar Solids)
Timeframe: 2012-
Staff: Contacts: A.P. Jones ([email protected]) and N. Ysard ([email protected] psud.fr). Permanent staff in France: K. Demyk (IRAP), V. Guillet (IAS), A.P Jones (IAS), L. Verstraete (IAS), N. Ysard (IAS) PhD students (since 2010): M. Bocchio (2012-2014), T. Boutéraon (2016-2019), L. Fanciullo (2012-2015), E. Micelotta (2008-2009), T. Schirmer (2017-2020) Post-docs (since 2010): M. Bocchio (2015), M. Köhler (2010-2015), , E. Micelotta (2013- 2015), G. Wagle (2012, IAS)
Website: https://www.ias.u-psud.fr/themis
Goals: THEMIS is a global approach to ISM dust modelling, the goal of which is to provide a self- consistent dust model from the most diffuse ISM regions to dense molecular clouds.
Methods: THEMIS is anchored to the laboratory-measured properties of ISM dust analogues: namely, amorphous hydrocarbons and amorphous silicates. A key element of the THEMIS framework is a self- consistent treatment of the evolution of the dust material properties as they react to the local radiation field intensity and hardness and to the gas density and dynamics. Detailed optical property calculations are performed using the Discrete Dipole Approximation (DDA).
Highlight: Dust evolution from diffuse to dense clouds explained within the THEMIS framework THEMIS includes the effects of dust evolution in the denser regions of the ISM (Köhler et al. 2015). The model is consistent with the dust scattering properties needed to explain observations of cloud- shine and core-shine (Jones et al. 2016; Ysard et al. 2016). Thus, the THEMIS modelling approach encompasses, and indeed requires, rather wide variations in the composition and size distribution from region to region within the ISM (gas accretion, grain-grain coagulation).
Albedos for diffuse-ISM type dust (CM) Cloudshine radial profiles of the TMC- and for coagulated grains without 1N cloud measured by Malinen et al. (AMM) and with ice mantles (AMMI). (2013) in the J (blue), H (black), and K (pink) bands. Circles of the same colours show the THEMIS fit to these data. Keywords: cosmic dust – solid state physics – dust evolution – amorphous hydrocarbons
Most significant publications (< 5): The global dust modelling framework THEMIS, Jones et al. 2017, A&A, https://arxiv.org/pdf/1703.00775.pdf Dust evolution in the transition towards the denser ISM: impact on dust temperature, opacity and spectral index, Köhler et al. 2015, A&A, https://arxiv.org/pdf/1506.01533v1.pdf Dust variations in the diffuse interstellar medium: constraints on Milky Way dust from Planck-HFI observations, Ysard et al. 2015, A&A, https://arxiv.org/pdf/1503.07435v2.pdf The evolution of amorphous hydrocarbons in the ISM: dust modelling from a new vantage point, Jones et al. 2013, A&A, https://arxiv.org/pdf/1411.6293v1.pdf Link to full publication list: https://www.ias.u-psud.fr/themis/THEMIS_papers.html
Related projects: DustEM, a modelling tool for dust emission and extinction https://www.ias.u-psud.fr/DUSTEM/ DustPedia, a definitive study of cosmic dust in the local universe http://dustpedia.com/ ESPOIRS, étude spectroscopique des propriétés optiques dans l’IR et le submm d’analogues de grains interstellaires http://www.irap.omp.eu/observations/explabo/nanograins/espoirs
Numerical Tools: eRCN (extended Random Covalent Network) and DG (Defective Graphite) models https://arxiv.org/abs/1511.01673 DDA (Discrete Dipole Approximation) http://ddscat.wikidot.com/ DustEM https://www.ias.u-psud.fr/DUSTEM/ Project: TRON — Tracing the Reservoirs Of Nitrogen
Timeframe: 2013-2021
Staff: Contacts: Pierre Hily-Blant ([email protected]) Permanent staff in France: Alexandre Faure (IPAG, CNRS), Claire Rist (IPAG, MdC), Thierry Forveille (IPAG, Astronome), E. Quirico (IPAG, PR), L. Bonal (IPAG, Astronome Adj.), P. Beck (IPAG, MdC), G. Pineau des Forêts (LERMA, Emerite), E. Falgarone (LERMA, Emerite), P. Lesaffre (LERMA, CNRS), F. Lique (Univ. Le Havre, PR) Permanent staff in other countries: J. Kastner (RIT, USA), D. Flower (Univ. of Durham, UK), C. Qi (CfA, USA) PhD students (since 2010): R. Le Gal (2011-2014), V. Magalhaes de Souza (2014-2017), J. Bublitz (RIT/IPAG, USA/France, 2018-2021) Post-docs (since 2010): F. Daniel (2014-2017), R. Le Gal (CfA, USA, post-doc), V. Magalhaes de Souza (IRAM, post-doc)
Website: http://www.
Goals: Follow the trail of volatile nitrogen, from interstellar clouds to planets.
Methods: spectral line and continuum observations (ALMA, IRAM, X-ray, etc); radiative transfer modeling; steady-state and time-dependent chemical modeling of collapsing cores and disks;
Highlight:
Keywords:
Most significant publications (< 5): Modelling the molecular composition and nuclear-spin chemistryof collapsing pre-stellar sources, P Hily-Blant A Faure C Rist G Pineau des Forêts D R Flower, 2018, MNRAS, https://doi.org/10.1093/mnras/sty881 Abundance of HCN and its C and N isotopologues in L1498, Magalhaes, Victor S.; Hily-Blant, Pierre; Faure, Alexandre; Hernandez-Vera, Mario; Lique, Francois, 2018, A&A, Direct evidence of multiple reservoirs of volatile nitrogen in a protosolar nebula analogue, Hily-Blant, P.; Magalhaes, V.; Kastner, J.; Faure, A.; Forveille, T.; Qi, C., 2017, A&A, doi:10.1051/0004-6361/201730524 Interstellar chemistry of nitrogen hydrides in dark clouds, Le Gal, R.; Hily-Blant, P.; Faure, A.; Pineau des Forêts, G.; Rist, C.; Maret, S., 2014, A&A, 10.1051/0004-6361/201322386 Link to full publication list: http://www.
Related projects: HYDRIDES (P.I. Faure) Exploring Planet Formation in the Nearest Known Protoplanetary Disks (P.I. Kastner) MIST (P.I. Falgarone)
Instruments and Tools: ALMA IRAM ESO/Sphere, Gemini/GPI Chandra Project: Virtual Atomic and Molecular Data Center (VAMDC) - http://www.vamdc.eu
Timeframe: Starting date : 2009 - continuing
Staff: • Contacts: Marie Lise Dubernet ([email protected], Chair of VAMDC Consortium) • Permanent staff in France: Carlo Maria Zwölf ([email protected], executive Director), Nicolas Moreau ([email protected], co-chair of the technical board), Yaye Awa Ba ([email protected]) + please see at http://www.vamdc.eu/ for other french partners. • Permanent staff in other countries: please the VAMDC partners at http://www.vamdc.eu/ • Engineers (since 2010): Misha Doronin (2010-2012, LPMAA-now LERMA, engineer), L. Nenadovic (2009-2011, LPMAA-now LERMA, engineer) • Post-docs (since 2010): Christian Hill (2009-2012, UCL, theoretician), T. Marquart (2009- 2012, Uppsala University, engineer), C. Endres (2009-2012, Cologne University, laboratory), K. Smith (2009-2011, Queen's University Belfast, theoretician/engineer),
Website: http://www.vamdc.eu
Goals: At present Paris Observatory is the legal representative of the VAMDC Consortium.
The "Virtual Atomic and Molecular Data Centre Consortium" (VAMDC Consortium, http://www.vamdc.eu) [1] is a worldwide consortium which federates Atomic and Molecular databases through an e-science infrastructure and an organisation to support this activity (http://www.vamdc.org/structure/how-to-join-us/). The inter- connected databases handle data that are used for the interpretation of astronomical spectra and for the modelling in media of many fields of astrophysics, for atmospheric physics, plasmas, fusion, radiation damage. The VAMDC consortium members are in Europe, in Russia, in Serbia, and associated members (providing databases within VAMDC but without signing the MoU) are in the USA and in Japan, and we support inclusion of an Indian A.&M. database working the India Association of Physics.
The current VAMDC e-infrastructure interconnects about 30 atomic and molecular databases that cover atomic and molecular spectroscopy and processes. VAMDC offers a common entry point to all connected databases through the VAMDC portal (https://portal.vamdc.eu) and VAMDC develops also standalone tools in order to retrieve and handle the data, the SPECTCOL tool [2] is an example (http://www.vamdc.eu/software). VAMDC provides also software [3] and support in order to include new databases within the VAMDC e-infrastructure. One feature of VAMDC e-infrastructure is the constrained environment for the description of data, in particular the VAMDC-XSAMS, a standard XML file (XML Schema for Atomic Molecular and SolidData) (https://standards.vamdc.eu/dataModel/vamdcxsams/index.html\#vamdcxsamslanguage-index), and other standardized protocols (http://www.vamdc.eu/standards) that ensure a higher quality for the distribution of data. Our recent publication [1] provides details about VAMDC- XSAMS and about the main databases included in the VAMDC e-infrastructure. Relevant publications to the text above : [1] Dubernet et al (VAMDC consortium), The Virtual Atomic and Molecular Data Centre (VAMDC) Consortium. Journal of Physics B: Atomic, Molecular and Optical Physics 299 2016, 49, 074003. doi:10.1088/ 0953-4075/49/7/074003. [2] Dubernet, M.L.; Nenadovic, L. SPECTCOL: Spectroscopic and Collisional Data Retrieval. Astrophysics 301 Source Code Library, record ascl:1111.005, 2011, p. 11005. [3] Regandell, S.; Marquart, T.; Piskunov, N. Inside a VAMDC data node - putting standards into practical 304 software. Physica Scripta 2018, 93, 035001, [arXiv:astro-ph.IM/1803.09217]. doi:10.1088/1402- 4896/aaa268.
Methods: VAMDC has been designed to include further A+M databases and networks pathways by which common policies may be developed for an open science version of VAMDC that will extend its availability to new audiences such as schools, students, citizens and industry. Thus VAMDC is an ideal e-infrastructure to deliver a fit-for-purpose and sustainable service through the European Open Science Cloud (EOSC) hub that can satisfy the evolving needs of the A&M scientific community. VAMDC has a track record of stimulating the design and prototyping of novel innovative digital services that deliver a user oriented open science approach to a range of topics from astrophysics to radiotherapy. It covers all aspects of the research data cycle (from data production to publication, curation, preservation and reuse), and is now able to exploit new scientific data-related developments such as Machine learning and AI.
Highlight:
Since the foundation of the VAMDC Consortium, the consortium has implemented its excellence roadmap focused on coordination with other e-infrastructures, developing links with existing data- networks and disseminating the VAMDC facilities and protocols in the international research community:
l Research Data Alliance: The Authentication Authorisation and Accounting strategy developed during SUP@VAMDC has inspired, through VAMDC’s leading role in the Federation Identity Management Interest Group of the Research Data Alliance, the Federation Identity Management for Research Collaboration White-Paper (DOI: 10.5281/zenodo.1296031) which became an RDA supporting output. l Open Science : VAMDC has played a leading role in the Group of European Experts in RDA (GEDE-RDA, https://www.rd-alliance.org/groups/gede-group-european-data-experts- rda), where it is promoting, fostering and driving discussions to create a consensus on hot- topics common to various European Research Infrastructure. After focusing on usage of persistent identifiers for research data (https://zenodo.org/record/1116189) it is focusing on best practices for data citation, FAIR digital objects and blockchains technology as tools for research infrastructures. l Query Store : VAMDC became an early pilot for the RDA-recommendation from Data- Citation Working Group. During the year 2017, as subcontractors of RDA-EU3 project, it implemented the RDA Data-Citation and Scholix recommendations. VAMDC adoption stories are having great impact (https://rd- alliance.org/sites/default/files/VAMDC_adoption%20story.pdf) and it is working with the main scientific editors for integration of our data-citation facilities into the paper-submission workflow. l BASECOL and SPECTCOL tools : BASECOL (database of inelastic collisional rate coefficient) has been included in VAMDC. The SPECTCOL tool allows to combine spectroscopic data from the JPL/CDMS database (or any set of molecular spectroscopic data in the VAMDC format) with the collisional data from BASECOL in order to produce combined sets of data able to be introduced directly the users tools (users being the PCMI community) l IVOA : VAMDC is collaborating with the IVOA (International Virtual Observatory Alliance) on an update of their standards dedicated to atomic and molecular data. This collaboration aims at a convergence between IVOA and VAMDC standards in order to achieve interoperability between their respective services.
Keywords: open science, interoperability, open data, atoms, molecules, quality, e-infrastructure
Most significant publications (< 5): Ø The Virtual Atomic and Molecular Data Centre (VAMDC) Consortium, Dubernet et al (VAMDC consortium), Journal of Physics B: Atomic, Molecular and Optical Physics 299 2016, 49, 074003. doi:10.1088/ 0953-4075/49/7/074003. Ø The VAMDC Portal as a major enabler of atomic and molecular data citation, N. Moreau, C.M. Zwölf, Y.A. Ba, C. Richard, V. Boudon, M.L. Dubernet, (2018) Galaxies 2018, 6, 105; doi:10.3390/galaxies6040105 (Open Access) Ø Implementing in the VAMDC the New Paradigms for Data Citation from the Research Data Alliance. Data Science Journal, Zwölf, C.M., Moreau, N., Ba, Y.-A. and Dubernet, M.-L., 2019., 18(1), p.4. DOI: http://doi.org/10.5334/dsj-2019-004 Ø SPECTCOL: Spectroscopic and Collisional Data Retrieval, Dubernet, M.L.; Nenadovic, L. Astrophysics 301 Source Code Library, record ascl:1111.005, 2011, p. 11005. Ø BASECOL2012: A Collisional Database Repository and Web Service within VAMDC, M.L. Dubernet et al, A.&A., 2013, 553, p A50
Link to full publication list: no such list is available. would need to be done as there are
Related projects: • The team has coordinated the 2 following projects : VAMDC and SUP@VAMDC. VAMDC was supported by EU in the framework of the FP7 "Research Infrastructures - INFRA-2008-1.2.2 - Scientific Data Infrastructures" initiative. It started on the 1rst of July for a duration of 42 months. SUP@VAMDC is supported by EU in the framework of the "Research Infrastructures - FP7 - INFRA-2012-3.3 - Scientific Data Infrastructures" initiative from 01/12/2012 to 30/11/2014. • In 2016 the team has been sub-contracted by the Research Data Alliance in order to implement the RDA citation recommendation and created the Query Store
Tools: • see all products at http://www.vamdc.eu/research/ • http://species.vamdc.eu • https://portal.vamdc.eu