UCL DEPT. OF SPACE & CLIMATE PHYSICS SOLAR & STELLAR PHYSICS GROUP Atomic Data for Astrophysics VOTADA VO Tools and Atomic Data for Astrophysics Giulio.

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UCL DEPT. OF SPACE & CLIMATE PHYSICS SOLAR & STELLAR PHYSICS GROUP Atomic Data for Astrophysics VOTADA VO Tools and Atomic Data for Astrophysics Giulio Del Zanna EUV image of solar coronal loops (TRACE)

ESAC March 2007 The VOTADA project aims at providing accurate atomic data for ions and derived products/tools for astrophysical applications within the Astrogrid (PPARC-UK) and VO. Collaboration: –Silvia Dalla (Univ. Manchester - Astrogrid) –Kevin Benson (UCL/MSSL - Astrogrid) –Peter Young (RAL, UK) –Helen Mason (Univ. of Cambridge, UK) Main user community: X-rays, EUV, UV Atomic data calculations – we need archives and standards for output results. -Iron Project, UK Rmax, APAP (Atomic Processes in Astrophys.Plasmas) network Atomic databases – we need standards and ways to propagate references to original work. -CHIANTI package, my contribution Tools: how we make tools to model observed spectra widely available?

ESAC March 2007 Line emission Del Zanna (1999) Black: observed solar spectrum (SOHO/CDS); blue: theoretical model spectrum

ESAC March 2007 In optically-thin plasmas, line intensities are proportional to (e.g. Fe XII): Obtain densities, temperatures and elemental abundances from spectra (and broad-band data). Create synthetic spectra to be compared to observed ones (requires links to instrument properties) Create synthetic broad-band images Calculate instrument response functions Calculate radiative losses Ion ab. YiEl. ab. Y

ESAC March 2007 Challenges ahead Soon (2008) we will have 1Tb/day of high-resolution narrow-band EUV images. Also, large amounts of atomic data. We need tools to handle large amounts of data. TRACE EUV images of the solar corona

ESAC March 2007 The CHIANTI package Collaboration between UK, US and Italy. Freely available and user-friendly. First release in 1996, most up-to-date and described with published papers. Provides all atomic data (homogeneous) and IDL programs necessary for modelling spectra from collisionally-ionised plasmas. Mostly stellar coronae, but also used for a wide range of astrophysical objects (Chandra, XMM-- Newton, FUSE, HST). Included in many other spectral codes such as: XSTAR, APED/ATOMDB XSPEC, ISIS, PINTofALE Over 800 citations

ESAC March 2007 CHIANTI atomic package Data, IDL programs, User Guides Link to references:

ESAC March 2007 CHIANTI data Currently, for each ion ascii files: fe_12.elvlcEnergy levels (theoretical, observed), level descriptions fe_12.wgfaTransition probabilities, gf values, theoretical, observed wavelengths fe_12.splupsspline fits to Maxwellian-averaged e- collision strengths CHIANTI emissivities are currently calculated for plasmas in ionization equilibrium, but non-equilibrium, non-Maxwellian plasmas will soon be included. Have photo-excitation but not photo-ionization. Building a database of radiative and dielectronic recombination rates, as well as collisional and photo-ionization rates / cross-sections  calculate time-dependent ionization

ESAC March 2007 CHIANTI, Astrogrid and the VO -CHIANTI data have been imported into a MySQL database. Tables: SpectralLines and LineEmissivities. Link to the VO: 1. using ESAC DAL Toolkit to install a SLAP server (DMMapper can translate from CHIANTI data model to Line data model) -Data will appear automatically in VOSpec, once registered. - in progress 2. by means of AstroGrid DSA software: user can build ADQL queries on the CHIANTI tables via Workbench. - Database tables include: wavelength, A-value, gf-value, configuration, nLSJ, observed, theoretical energy of upper and lower levels. Line emissivities in a grid of temperatures and densities. To do: Add tables of chemical abundances and ion fractions. Add continuum. Write workflows/scripts. IDL ? Python ?

ESAC March 2007 Spectral Lines table Result Result of query to spectral lines table via AstroGrid DSA:

ESAC March 2007 Emissivities table Table contains line emissivities calculated on a grid of temperatures and densities Results for Fe, for a query for log_density=5 and log_temperature=10 in wavelength range Angstrom:

ESAC March 2007 Benchmark (my own work) Transition probabilities - lifetimes (beam-foil spectroscopy) Line identifications and wavelengths using a wide range of laboratory and astrophysical spectra. Provide best estimates (empirically- adjusted) level energies and wavelengths. Uncertainties A lot of work is needed to revise/complete atomic data for the XUV. NIST data are incomplete. Del Zanna & Mason (2005)

ESAC March 2007 Questions What atomic data do users need ? How can we make atomic data available through the VO, have them used ‘properly’ and referenced ? My wish list: Provide multiple datasets of atomic data. Atomic data: excitation rates and cross-sections (APAP Network) ionization and recombination rates and cross-sections level energies and wavelengths transition probabilities Provide both theoretical and measured values; uncertainties. Have standard protocols to access atomic data. Provide general tools to measure physical parameters from observed spectra.