11 Management Plan

Fig. 9 presents an organisation diagram of the SEDI project listing the major activities with for each of them a leader and the institute who is taking responsibility of the successful completion of the task. We first describe the SEDI team and our plans for the overall coordination of the team and working groups. In the following sub-sections we detail the organization within each of the working groups.

11.1 The SEDI Team

The SEDI team was built with the ambition of gathering a dedicated and committed team of researchers with wide-ranging experience in all observational and theoretical areas of research and data processing relevant to the project. The co-Is together with experienced staff at participating institutions, including the post-docs we plan to hire, have the necessary expertise and workforce to successfully carry out the SEDI program in a timely manner. All co-Is and staff who will be involved in the preparation of SIRTF observations, data reduction and analsyis have worked and collaborated on similar tasks within the IRAS and ISO projects. The team members responsible for the gathering and reduction of the ancillary data set also have wide-ranging experience in what they commit. The Nagoya University routinely runs the Nanten millimeter telescope at Las Campanas. Joncas and Martin, who will be in charge of the H I DRAO observations, are active members of the Canadian Galactic Plane Survey consortium. F. Boulanger (PI) and the task leaders will constitute a Task Force that will remain in regular contact through regular conference calls to follow progress on all SEDI activities.

Co-Is will receive support from their institute and funding agencies. The IPAC funding request for american co-Is has been submitted for a total amount of 822 k$. The IAS/ENS team has submitted a funding request to the french Space Agency (CNES) for a total amount of 480 kEuros. Letters of endorsments have been sent to the SSC director. All institutions will provide significant work force beyond the project co-Is. Participating scientific associates with staff positions at the SEDI's institutes include: Coulais, Dartois, d'Hendecourt, Pineau des Forêts, Pérault, Rabasse at IAS/ENS, Gautier and Rho at IPAC/JPL, Gry and Prusti at Vilspa, Randich and Walmsley at Arcetri, Onishi at Nagoya and Kerton at DRAO.

Figure 9 SEDI organisation diagram. The names and institutes of the leaders of each task are in bold. The composition of working groups is given in a plain, smaller font.

Each institute has responsibility of a specific task. Major efforts on the team management and coordination will be around the SIRTF related activity. The team members working at the Vilspa ESA station will maintain a CVS data base where updated versions of all software, documents and data products at different levels of processing will be gathered and made available to all team members. A WEB site at Vilspa will also be maintained for distribution of project and scientific informations. Our SSC co-Is will greatly facilitate the necessary communication with SSC on pipeline developments, instrument and detector expertise. We will be granted sufficient travel money by our funding agencies to regularly visit SSC. One of the post-doc positions will be funded by the french space agency and will be partly based at IPAC. The travel money will also allow us to organize regular meetings and reviews at the working group and full consortium levels. This will serve to follow and stimulate the team progress on each task.

11.2 SIRTF observations and data reduction

The observation planning group will optimize the observing strategy and be responsible to deliver the MIPS and IRAC imaging AORs. They will also be responsible for selecting positions of the IRS and MIPS SED follow-up and deliver the corresponding AORs.Theis task is related to the science objectives, the data reduction schemes and the instrument expertise. The final observing strategy will optimize the data redundancy versus characteristics of memory effects in relation to the scientific goals but also progress in detector modeling integrated in the data reduction. This working group will thus include all relevant persons to ensure the best choice. Namely, the SSC instrument experts, the leaders of each SIRTF data reduction activity and the leaders of scientific topics.

The preparation of the SIRTF data products will be shared between a large group of co-Is in four different locations (IAS/ENS, Vilspa, Arcetri, IPAC). Each will have the responsibility of a specific part of the data processing/validation. Coordination between these four working groups is essential to the success of the proposal. The CVS data base will allow us to share up to date software developments. Further, the most challenging software development we plan to do, the modeling of detectors, will be under the sole IAS responsibility. All other software developments will either follow from the SSC pipeline or the existing ISO pipelines available at IAS and Vilspa. Coordination on software exchange and necessary adaptation will be greatly facilated by the fact that involved team members share a common experience on the ISO project

11.3 Ancillary data

The gathering and data reduction of the H I observations proposed here will fully benefit from the automatic procedures developped for the Canadian Galactic Plane Survey. The past achievments of Professor Fukui's team guarantees the successful completion of the CO observations. This team runs and has exclusive use of the 4m millimeter telescope they installed in 1996 at Las Campanas observatory. The optical observations rely on existing data reduction pipelines and experienced observers.

11.4 Scientific Analysis

The scientific analysis of the data will be organized around three themes: dust evolution, ISM structure and young stellar objects, coordinated by Anthony Jones, Edith Falgarone and Antonella Natta, respectively. Co-Is and scientific associates will participate in these groups according to their scientific interests. The activity of these groups will be stimulated by regular meetings. The teams will be sharing the modeling tools and expertise necessary for the data interpretation.

Previous

Next

Index