Teams in POE Network

Team 1: Imperial College (+Sussex, Cambridge, UCL, Athens)

Team 2: IfA, Edinburgh

Team 3: Padova (+SISSA, Bologna, RomeIII)

Team 4: MPE, Munich (+ AIP Potsdam, DLR Berlin)

Team 5: MPIA, Heidelberg (+Helsinki)

Team 6: IAP, Paris

Team 7: IAC, Tenerife (+Santander, Granada)

Team 8: Leiden (+Groningen)

The goals of the POE Network are:

1.To extend observations of the background to new wavelengths, particularly 90 and 200 microns, from a careful analysis of ISO data. To study and model extended sky foreground components, i.e. interplanetary dust cloud, galactic cirrus, intergalactic dust. These studies will contribute not only to our understanding of the extragalactic background radiation, but will also be important preparation for European space astronomy missions of the future like FIRST and PLANCK.

2.To survey extragalactic populations to deeper sensitivities at a wide range of wavelengths from radio to X-rays, and thereby to resolve a greater fraction of the background directly into discrete sources.

3.To make a direct connection between submm and far ir sources, on the one hand, and X-ray sources, on the other, using new surveys with the SAX, AXAF (=CHANDRA) and XMM satellites. The connection between the submm and X-ray background is seen as one of the key issues for the next decade. Radio surveys will also be of great value in unravelling the AGN contribution to the submm background.

4.To make detailed studies of source populations seen in the far ir, submm, radio and X-rays, for example: starburst, ultraluminous and hyperluminous infrared galaxies, Seyferts and quasars. To study the multi-wavelength spectral energy distributions (seds) of galaxies out to great distances and analyze the multi-component nature of these seds.

5.To carry out sophisticated theoretical modelling of the emission from extragalactic populations, using state-of-the-art radiative transfer codes to study the flow of radiation through dust, and the latest models for emission from accretion disks surrounding active galactic nuclei (AGN).

5.To carry out sophisticated theoretical modelling of the emission from extragalactic populations, using state-of-the-art radiative transfer codes to study the flow of radiation through dust, and the latest models for emission from accretion disks surrounding active galactic nuclei (AGN).

6.To model the star formation history, and the history of gas and dust, in galaxies, and understand the evolution of heavy elements, stars, starlight and stellar remnants in galaxies

7.To model the evolution of AGN, explore the predictions of unified models, and try to formulate the connection with galaxy formation and the star formation history in galaxies

8.To synthesize all the above knowledge and insights into comprehensive models for source counts and background radiation at all wavelengths from radio to x-rays.

The proposal submitted to the EC can be found here (password protected):

(proposal)

The minutes of the first POE consortium meeting on June 15th, 2000, can be found here:

(minutes)