Astronomical Spectroscopy & the Virtual Observatory - ESAC – March 23 rd 2007 Stefano Bianchi Matteo Guainazzi Isa Barbarisi Pedro Osuna Jesus Salgado

Guainazzi et al Predicted starburst contribution Actual soft X-ray luminosity Turner et al ASCA Soft X-ray excess in obscured AGN

NGC1068 Kinkhabwala et al XMM RGS Strong emission lines dominate No continuum => log(N H )<22.7

NGC1068 Kinkhabwala et al Detection of narrow Radiative Recombination Continua (RRC) => Low temperature gas => Photoionization (Liedhal et al. 1995) Diagnostic on triplets AND higher order series lines: confirm photoionization constraint <10% contribution from collisional plasma unveil the important role of resonant scattering (Band et al. 1990, Matt 1994, Krolik & Kriss 1995)

Can we do the same with low resolution? OVIII Kα OVII Kα OVII high orders RRCs

proudly announce all the type ≥ 1.5 AGNRGS We proudly announce the first catalogue of soft X-ray emission lines in a sample which includes all the type ≥ 1.5 AGN observed by the RGS CIELO-AGN [Catalogue of Ionized Emission Lines in Obscured-AGN] 66 objects ~ cgs OVIII Lyα detected in ~50% of the sample OVII triplet in ~40% Many other lines from O, Fe, C, Si, Mg, Ne, N detected in ~15% Guainazzi & Bianchi 2007

CIELO-AGN

Critical diagnostics RRCs are: Common Common (detected in 40% o.t.s.) Narrow Narrow (σ<10 eV) => Photoionization Strong higher order lines => Resonant scattering

Where is the gas? Circinus Smith & Wilson 2001 NGC4151 Yang et al NGC3393 – z= NGC1386 – z= Bianchi et al (+ 6 other objects)

What is the gas? The comparison between the Chandra and the HST images shows that the [OIII]/soft X-ray ratio is fairly constant along with the radius, up to hundreds of pc. Photoionization models reproduce this behavior if n e  r -β, with β=2 (i.e. constant ionization parameter). This is in agreement with NLR emission line ratios (e.g. Kraemer et al. ’00, Kraemer & Crenshaw ’00, Bradley et al. ’04, Collins et al. ‘05). Bianchi et al., 2007

What about the starburst contribution? HSTChandra 110 pc 3 pc In the immermost 110 pc: low luminosity AGN: L X ≈10 39 erg s -1 young stellar cluster: L X ≈6×10 38 erg s -1 NGC4303 Jiménez-Bailón et al NGC7130 Levenson et al. 2005

AGN -Total L O ≥10 40 erg s -1 -OVII/OVIII≥1 So… AGN or starburst? Empirical diagnostic diagram based on high resolution spectroscopy Guainazzi & Bianchi 2007 STARBURST

… of course this is too simple OVIII/OVII excess is NOT coincident with star formation regions! Bianchi et al., 2007 NGC7582

The VO Connection One needs: A Data Model, i.e. a standard abstract representation of the database structure A Data Access Protocol, i.e. standard rules to be followed by software designed to access line databases A Software Implementation capable of interfacing with other access protocols (spectra, images etc.) The process is close to be finalized: Relevant documents aiming at being promoted to formal recommendation at the next IVOA Interoperability Meeting The International Virtual Observatory Alliance started about 2 years ago a discussion on how to make line catalogues accessible in the VO context See J. Salgado’s Talk

Why is the Line Data Model appropriate for us? 1. It supports atomic and molecular “laboratory” databases as well as catalogue of observed lines (such as CIELO) 2. It is organized around the concept of line 3. It allows catalogue publishers to provide full characterization of the atomic/molecular state, the physical processes generating a line and the physical properties of the plasma where the line is emitted 4. Pilot implementation possible

CIELO VO implementation CIELO-AGN is the first astrophysical line catalogue compatible with the (draft) IVOA Line Data Model and accessible through the (draft) Simple Line Access Protocol (IVOA Line Data Model: Dubernet, Osuna et al., in prep.) (Simple Line Access Protocol: Salgado et al., in prep.)

Conclusions High-resolution spectroscopy IS fundamental to understand the physical properties of the gas in the AGN circumnuclear environment (as high- resolution imaging IS fundamental to unveil its true location) CIELO unveils a criterion to discriminate between AGN- and starburst-dominated sources on the basis of the OVII(f)/OVIII ratio In obscured AGN, CIELO unveils mounting evidence for Dominant role of AGN-photoionization, Important role of resonant scattering, Broadly constant ionisation parameter... on scales as large as a few hundreds parsec The VO is almost ready to be a tool for scientific investigation in this field. Stay tuned!