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Spectral Line Access

Paris Observatory and ESA/ESAC ML Dubernet, P. Osuna, M. Guanazzi, J. Salgado, E. Roueff MLD acknowledges support from VO-France, MDA project (F. Genova), Paris Observatory. Spectral Line Access. Project Overview (1). Access Atomic/Molecular DB starting with line lists

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Spectral Line Access

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  1. Paris Observatory and ESA/ESAC ML Dubernet, P. Osuna, M. Guanazzi, J. Salgado, E. Roueff MLD acknowledges support from VO-France, MDA project (F. Genova), Paris Observatory Spectral Line Access

  2. Project Overview (1) Access Atomic/Molecular DB startingwith line lists Theoretical (measured or calculated) DB Observed line lists DB Necessary to access complementary information in order to interpret spectra or model astrophysical media: excitation rate coefficients, etc.. Clients: stronger evolution towards public software packages for spectral analysis and on line codes for astro. Simulation Shared, structured, complete and documented access to AM DB Standardisation O/I, queries, ressources ID

  3. Overview (2) • Numerous DB are available • Atomic lines: NIST DBs, Kurucz's CD-ROM, Atomic Line List of P. Van Hoof, TOPbase, Kelly Atomic Line DB, VALD, MCHF/MCDHF Collection, D.R.E.A.M, KAERI AMODS • Molecular Lines: JPL Spectroscopic DB, CDMS, HITRAN, GEISA, NIST • Other DB: IEAE, NIFS, CHIANTI, UMIST, BASECOL, small compilations • Observed databases: ATOMDB, NIST, ... • Identification of Pbs • Different DB have similar datasets • DB have different levels of update • Lengthy to identify origin of datasets, find all relevant description of data • Useful data for a single astrophysical application are dispersed in various DB • No homogeneous description of data

  4. Access to Lines: Data Model Based on fundamental physics, current databases and needs in astrophysics Current DM is centered around line for atom and molecules: electronic, vibrational, rotational transitions (couplings) Allows for identification of Chemical Species Level -->Quantum State-->Quantum numbers Origin and modification of Line Can be used to model other processes involving transitions because a line corresponds to a transition between two levels Could be extended to nuclear physics

  5. H(3p2P03/2)---> H(1s 2S1/2) + hv

  6. Quantum Number: coupling N2H+ : rotationN, 3 nuclearSpinI level characterized with a single state |NF1F2F> N+I1= F1; F1+I2=F2; F2+I3 = F QuantumNumber : I1 name = nuclearSpinI type = nuclear spin of outer nitrogen origin = pure intValue = 1 QuantumNumber : F2 name = intermediateAngularMomentumF type = intermediate angular momentum origin = N + nuclearspinI (nuclear spin of outer nitrogen) + nuclearspinI (nuclear spin of inner nitrogen) value = 0

  7. DM : general transition model Each time a species undergoes a transition, it can be modeled by a Line DM A transition is modeled by Before .... Oups Something happens! ... After Light – Matter Interaction : bound-bound A(j) + hv ---> A(j') A(j') ---> A(j) + hv

  8. DM : general transition modelLight-Matter : bound-continuum Radiative recombinaison (Z, N-1)[level.of.Z(N-1)] + e ---> (Z, N)[level.of.Z(N)] + hv InitialElement = ChemicalElement IonizationStage = -1 (comparatively to N) Z is specified full atomic symbol is specified (see DM) FinalElement = ChemicalElement IonizationStage = 0 (comparatively to N) Z is specified full atomic symbol is specified (see DM)

  9. Excitation : A(i) + B(k) --> A(j) + B(l) TargetLine = Line : A initialElement=finalElement InitialLevel = i ; finalLevel = j PerturberLine = Line : B Other attributes specific to excitation Temperature Rate coefficients Reaction : AB(i) + C(k) --> A(j) +BC(l) Reactant = (1 to *) Line: AB, C InitialChemical: AB or C InitialLevel_species : i FinalLevel_species : none FinalChemical: none Products = (1 to *) Line: A, BC Reverse identification DM : general transition modelMatter – Matter Interaction

  10. DM document: Current status • Draft currently being written up • All attributes are carefully described following exact theoretical definitions • Most quantum numbers are described • In particular, most of the well known coupling cases

  11. DM : missing Provenance Observations : see characterization Measured Data : instrument and parameters Calculated sets : VOTheory Various steps in getting final data, ex : Method Hamiltonian (parameters, approximations), basis sets Algorithms Fitting functions: parameters, function, error Etc...

  12. Access : Query Parameters • Opened question for Line Access : SLAP : Simple Line Access Protocol • By wavelength_min, _max, _mid • By species: Fe I, H20, ... • By type of transition (E1, M1, E2) • By type of levels (vibration, rotation, ..) • Combined with associated processes • Would we allow search of other processes independently of lines ?

  13. Access to Lines: SLAP What information do we retrieve from a service implementing SLAP? Wavelength : mandatory Initial/Final ChemicalElement : should Name or atomicSymbol/formula : should Initial/Final Level : should QuantumState : should energy, statWeight : should Einstein A : should Optional : everything else

  14. Access to Lines: questions • Registry parameters? • Wavelength range • Keywords = energies, atoms or molecules, processes • Practically how should we proceed ? • Some DB will implement VO, otherwise create VO providers • Create Web Services and vizualization tools with filters

  15. Milestones : 2005-2006 • 1rst Draft « Atomic and Molecular Lines Data Model » : July 2005 • Agree on SLAP : July 2005 • Get inputs from community : until Sept. 05 • Implement simple prototype : Next Interop. • Extend DM: Provenance, .. Queries : 2006

  16. KAERI: Y.-J. Rhee ATOMDB: N. Brickhouse D. Schwenke J. Tennyson A bunch of french spectroscopists J. Aboudarham (solar) B. Plez (stars) J. Cernicharo (ISM) F. Valdes (calibration package) Contacted peoplePhysicists, Databases, Astronomers • GEISA: N. Husson-Jacquinet • HITRAN: L. Rothman • CDMS: S. Schlemmer • JPL: J. Pearson • UMIST: T. Millar • CHIANTI: P. Young • DREAM: P. Quinet • TOPBase: C. Zeippen • NIST: F. Lovas, Y. Ralchenko • NIFS: T. Kato • IEAE: B. Clark

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