ADASS XXII University of Illinois
November 4-8, 2012
ADASS2012 program header image

ADASS XXII Conference

Sunday Afternoon Tutorial

How the VO Gets Richer and Helps Solve Fundamental Problems of Extragalactic Astrophysics

Time/Location: Sunday Oct. 4, 15:00-17:00/Illinois Ballroom
Presenters: Zolotukhin, Ivan IRAP, Toulouse, France
Chilingarian, Igor Smithsonian Astrophysical Observatory
Abstract: see below

Special Note: Attendance is open, free of charge

Due to the late scheduling of this tutorial, we are opening up attendence to all interested ADASS attendees without charge. All those who paid for the tutorial at registration will be refunded.

Please let us of know of your interest!

If you are not already signed up for the tutorial but would like to attend, please submit your name here:


  

Abstract

This VO-Science tutorial may be interesting for those who are willing to learn cross-domain multi-discipline way of dealing with rich astronomical data through mature technological stack provided by the Virtual Observatory for the ultimate benefit of the scientific problems. General notion of VO concepts and technologies is a plus.

Our science case concerns stellar populations and the evolution of galaxies at low and intermediate redshifts. We will use the FUV-to-NIR SED catalogue of low and intermediate-redshift galaxies built from SDSS, UKIDSS, and GALEX data (whose construction was showcased in the ADASS XX tutorial) with resources available in data archives and the VO in order to study the galaxy evolution in different environments (groups, clusters, field) and to see how different galaxy properties vary across the cosmic web using three-dimensional visualisation of the large scale structure of the Universe. We will use recently developed IVOA standards (TAP, ObsCore, SIAPv2) to access large archives and automatically collect data of our interest. New science results will include: (a) a population of compact elliptical galaxies from their multi-colour properties; (b) the mass--metallicity relation of galaxies as a function of the environment richness/density; (c) gas versus stellar metallicity for starforming galaxies; (d) connection between stellar mass and X-ray luminosity in galaxy clusters using publicly available X-ray data.