AVO Science Telecon: Oct. 23, 03 present: MA Mark Allen TB Thomas Boch LC Laurent Cambresy PF Pepi Fabbiano FG Francoise Genova ML Marco Leoni TP Timo Prusti AR Anita Richards PR Piero Rosati NW Nicholas Walton chair: PP Paolo Padovani minutes: MD Markus Dolensky, revised by PP action items: PP contact Alberto Salama concerning accessibility of ISO images/spectra (there is SIA for XMM images; is the same true for ISO images?) AR flow diagram for galactic scenario PP flow diagram for extragalactic scenario The flow diagrams include input/output data (instrument,format,readily available or pre-cooked files,...) MD to enquire about http access of HST spectra at ST-ECF [ALL] next telecon: Oct 29, 2003, 4 pm CET --- +[LC+AR+TP] write down ideas for a galactic case +[PP+PR] write down ideas for extragalactic case +[MD] prepare wiki page for SWG +[PP] contact SWG and point them to the wiki page +[ALL] next telecon: Oct 23, 2003, 4pm CET --- notes: AR summary of galactic case: http://www.euro-vo.org/twiki/bin/view/Avo/GalacticScenario http access to ISO spectra not certain by January, XMM should be ok evolved star case, suggested by Alberto Salama, is one scenario too much PP will talk to him to thank him for his help and enquire about accessibility of ISO spectra; we will store "extra" scenarios on the Twiki pages Q: What about ESO data? A: For extragalactic case there are reduced spectra and images available. In general there are lots of 'raw' data but not reduced data, as far as we know, for the Galactic scenario. HST data? We need to check on http accessibility of HST spectra from the ST-ECF archive SEDs: Major issue is to get the zero points to compute fluxes plus image registration and PSF matching (see below) Worries about data access: 1. We need to know which data products we want to access 2. Then we can contact the archives and specify interface *********** PP summary of extragalactic case: http://www.euro-vo.org/twiki/bin/view/Avo/ExtragalacticScenario PR reservations: computation of redshift on-the-fly (photo-z) is difficult; images in different bands and/or taken with different instruments need to be registered on the same astrometric solution; plus, the different PSF have to be matched, i.e. aperture corrections have to be made, to obtain meaningful colours. No tools are available to do this on-the-fly. One solution adopted by the GOODS team is to degrade the ACS data to match them with the ISAAC data. Moreover, automated classification difficult, as it requires to know the redshift to identify the lines. Again, people have tools to do this but none is available for on-the-fly classification. Very unlikely that we can have this sort of tools ready by the demo but it's something to keep in mind for the long term. Object classification will be done manually. PP suggested using the fx/fo - Lx correlation found by Fiore et al. (2003) as a way to estimate (roughly) the X-ray power for type 2 sources. Debate on how 'far' the AVO prototype can go realistically MD remarks that there are use cases for individual parts of VO infrastructure; Philippe Prugniel has offered some tools for the demo. PP will circulate his email. 60 - 70 potential type 2 QSO candidates for Northern + Southern fields