LERMA UMR8112

Laboratoire d’Études du Rayonnement et de la Matière en Astrophysique et Atmosphères



Accueil > en > Research > Molecules in the Universe > Molecular Spectroscopy Experiments > High resolution VUV spectroscopy of interstellar molecules

High resolution VUV spectroscopy of interstellar molecules

par Christian Balança, Mathieu Bertin - publié le , mis à jour le

Members

M. Eidelsberg (voluntary researcher), M. Glass-Maujean (Prof. emeritus), A.-M. Vasserot (Ass. Prof.), S. Leach (voluntary researcher), J.-L. Lemaire (voluntary researcher), W-Ü L. Tchang-Brillet (Prof.), C. Blaess (tech.), N. Champion (engineer)

Context

The huge improvements of observational data supplied by new generation of space and ground-based telescope, increase, for their interpretation, the need for highly accurate laboratory data. The group has expertise in high resolution studies of electronic spectra of small molecules, which occur in the vacuum ultraviolet (VUV) range. High resolution is necessary for determination of energy levels of these quantum systems, for probing their fundamental radiative properties, and for photodynamics studies.

Complementary laboratory techniques are involved, including mass spectrometry and ionic dissociation channels. Emission studies are carried out using the 10-meter vacuum spectrograph (resolution R=150000) of the Meudon Observatory.

Absorption studies are performed at synchrotron facilities, either on the SOLEIL-DESIRS beamline using the Fourier Transform Spectrometer (R=350000) or at BESSY (R=100000). Wavelengths with a precision better than 10-7 are obtained, as well as absorption cross-sections and predissociation and/or ionization widths.

The interpretation of experimental spectra is closely related to theoretical calculations based on ab initio potentials and coupling operator.

Current studies

The species under study are of interest to a variety of astrophysical environments.

  • H2/HD/D2 : we are conducting experimental and theoretical investigations of the complex line spectra of the most abundant molecule of the Univers and of its isotopologues, which show strong non adiabatic perturbations. H2 and HD lines are candidats for probing possible cosmological variation of the fundamental constant mass ratio mu= mp/me. These studies participate to the enrichment of the MOLAT database.
  • CO : The CO molecule is a tracer for H2 and gives rise to a rich photochemistry in the ISM. We are conducting exhaustive study of Rydberg series in CO and in its isotopologues, including the Rydberg-valence predissociating interactions, which are isotopically dependent.
  • Molecules relevant to exobiology : Recent investigation of formamide and its methyl derivatives, diacetylene, cyanoacetylene and dicyanoacetylene, by absorption studies and electron-ion coincidence technique in the far UV. /Measurement, through CN radical interstellar UV absorption spectra, of the cosmic background radiation temperature. /Study of the part played by VUV radiation in exoplanets. /Testing the validity of published values of the heat of formation for neutral and ionic molecules.

Collaborations

Mourad Roudjane, Wim Ubachs (VU Amsterdam), Christian Jungen (LAC Orsay), I. Haar, A. Ehresmann (Kassel), Steve Federman (Univ. of Toledo, Ohio) and Glenn Stark (Wellesley College, Massachussets), Martin Schwell (LISA, Crêteil), H. Baumgärtel (Berlin)

Séminaires à venir

Vendredi 17 janvier 2020, 14h00
Salle de l'atelier, Paris
The role of feedback- and accretion-driven turbulence in galaxy build-up
Pierre GUILLARD
IAP
résumé :
Cosmological models describe accurately the growth of large scale, dark matter-dominated, structures, but largely fail to reproduce the baryon content and physical properties of galaxies. Why? Essentially because the build-up of galaxies is regulated by a complex interplay between gravitational collapse, galaxy merging and feedback related to AGN and star formation, for which we still miss a robust theory. The energy released by these processes has to dissipate for gas to cool, condense, and form stars. How gas cools is thus a key to understand galaxy formation and why it such an inefficient process. In this seminar, I will discuss a few examples where turbulence driven by gas accretion, feedback, and galaxy interactions, which is largely ignored in models of galaxy formation, and captured in current simulations only over a limited range of scales, may have a major impact on galaxy and halos properties.

 
Vendredi 24 janvier 2020, 14h00
Salle de l'atelier, Paris
The accretion-ejection connection in planet-forming disks. New perspectives from high angular resolution observations
Benoît TABONE
Leiden
 
Vendredi 7 février 2020, 14h00
Salle de l'atelier, Paris
Redistribution of angular momentum from core to disk scales in Class 0 stars
Mathilde GAUDEL
LERMA
 
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