Deliverables

Objective: We will determine the optimal methods of detecting substructure in both dust/molecular gas maps (including radial velocity information for the gas), as well as in the stellar component of young clusters.

• D1.1 – Substructure Techniques
  Report on optimal substructure techniques for stellar, gas and combined samples. KO+12m.
• D1.2 – Substructure Software Package
  Packaged software to public website, and other repositories if new or adapted. KO+12m
• D1.3 – Subcluster Catalogue
  Catalogue of subclusters. KO+30mth.
• D1.4 – Molecular Core and Clump Catalogue
  Catalogue of compact and extended molecular cloud components. KO+36mth.

Objective: We will  determine the best statistical methods for comparing observations and simulations, and for characterising the degree of clustering present in both dust/gas and stars.  We will also determine the best techniques for comparing the gas and stars in both density and kinematics.

• D2.1 – Mass Segregation Methodology
  Report (and paper) on optimal method for detecting mass segregation in young clusters. KO+18mths.
• D2.2 – Clustering Statistics Report
  Report on comparison of different clustering statistics for examining the environmental dependence of clustering in a wider sense. KO+24mths
• D2.3 – Clustering Software Package
  Publication of software tools for clustering. KO+36mths.

Objective: The Cardiff node will cover the main theoretical underpinning of this network. Cardiff have extensive expertise in modelling the physics of the ISM (e.g. Glover & Clark 2012a; Clark et al. 2012a, b; Clark et al. 2013; Clark & Glover 2015) and the formation and evolution of clusters (Clark et al. 2005, 2008, 2011; Bonnell et al. 2011; Dopcke et al. 2013). Grenoble also have previous experience in using N-body codes to follow the evolution of open clusters. They will adopt an oversight role to ensure the simulations are delivered in a form which can be turned into catalogues similar to the observational data. This work-package will cover 2 broad topics: Identify which physical processes lead to clustered versus distributed star formation to determine whether we can use 6D stellar information (e.g. from Gaia) to trace the ‘birth sites’ of stars in the field. Each of the these topics explores a different phase of the star formation process: the first focuses on the early stages of assembly and the second on the dynamical evolution and disruption. These topics are described in more detail further down. The comparison of models from Cardiff and Grenoble will also allow us to test how different N-body codes perform in terms of following the evolution of clusters as the gas disperses.

• D3.1 – Report on Required Simulations
  Document the suite of simulations that study star formation under different conditions in the ISM KO+10 Months
• D3.2 – Report on Available N-body Simulations
  Document the suite of N-body simulations, some of which will be based on the output from the gas-ISM simulations. This will also include those that study the effects of gas on the dynamics and the presence of ejected tight multiple systems KO+12 Months
• D3.3 – Report on Object Catalogue from Simulation Data
  Document the post processing of the simulation data, via radiative transfer (RT), that allows it to be compared directly with the observational data, together with necessary metadata for cataloguing KO+20 Months
• D3.4 – Simulation Data Release
  Upload and document the simulation data (including the data products, such as the RT post-processing) on the online servers, to allow public access. KO+24 Months.

Objective: This Work Package  deals with the creation of the necessary software tools in order to handle the algorithms for statistical analysis of combined Gaia, Herschel and other data for  young star  clusters and the visualization of the results of the analysis. The software package will consist of a Virtual Infrastructure that will contain the algorithm plus accompanying software, Client/Server systems to interact with it, Client/Server access to the Gaia and other external, if needed, Archives, and Client/Server systems for the 3D visualization of the analysis results.

• D4.1 – Virtualization Study Report
  Report of virtualization technology study and viability KO+6 m
• D4.2 – Virtual machine test report
  VM Testing and validation reports KO+32m
• D4.3 – GAIA data centre integration report
  Report of Gaia data center integration study KO+36m
• D4.4 – DEAVI report
  DEAVI Test and Validation Report KO+36m
• D4.5 – RISEA architecture report
  RISEA System Design & Analysis on Standards Report KO+6m
• D4.6 – Gaia data architecture report
  Study Report on Gaia frameworks and architecture KO+6m
• D4.7 – RISEA Software Library
  Release of RISEA Software libraries KO+24m
• D4.8 – RISEA Testing Validation Report
  RISEA Testing and validation Report KO+24m
• D4.9 – Vizualisation Server Data Resampling Study
  Report on the Data Resampling Study KO+12m
• D4.10 – Visualization Server Documentation
  Data Visualization Server Documentation KO+36m
• D4.11 – Visualization Client Verification Report
  Data Visualization Client testing, validation and verification report KO+24m
• D4.12 – Visualization Client Documentation
  Data Visualization Client Documentation KO+36m
• D4.13 – Software Quality Assurance Plan
  Software Quality Assurance Plan (SQAP) KO+6m
• D4.14 – Revised SQAP
  Revised SQAP KO+12
• D4.15 – Revised SQAP v2
  Revised SQAP KO+24
• D4.16 – Revised SQAP v3
  Revised SQAP KO+36
• D4.17 – Revised SQAP v4
  Revised SQAP KO+42
• D4.18 – Final Software Release
  System Documentation KO+42m
• D4.19 – Full Software Documentation Release
  Full public release of all software KO+42m

Objective: Observational studies of heavily embedded clusters.  We will acquire data relevant to two issues:  high spatial resolution sub-mm molecular gas maps and near infrared spectroscopic observations of embedded stars to determine radial velocities.

• D5.1 – Additional Observational Data Requirements
  Report on any telescope applications required, with relevant facilities, in order to complete and extend the project.  KO+ 1 year, and if required 6mths thereafter.

Objective: Disseminate our results quickly and widely to the astronomical community, and where sensible to the wider scientific and statistical community. Promote wider public awareness about the project’s results (data products, simulations, software, 3D visualisation tools).

• D6.1 – Public Project Website
  Public website.  To be updated at regular intervals by all nodes.
  KO+6mths.
• D6.2 – Documentation for Schools
  Documentation for the schools package. KO+24mths
• D6.3 – Outreach Activities Report
  Report on dissemination and communication activities, including updated publication lists, media appearances, links to outreach events etc. To be kept as a public web document.  To be updated regularly by all nodes. KO+3mths for initial version.
• D6.4 – Full Report on Outreach and Communication Activities
  Final report on dissemination and communication activities. The final version of D6.3 will be encapsulated as a formal report. KO+42mths.
• D6.5 – Outreach Activities Update v1
  Outreach activities update KO+12
• D6.6 – Outreach Activities Update v2
  Outreach activities update 2 KO+27

Objective: Produce a full data management plan, and update it as the project progresses. Ensure the integrity of all central storage, and document the structure fully. Provide description of all metadata associated with the project.

• D7.1 – Data Management Plan v 1
  Initial Data Management Plan KO+6m
• D7.2 – Archive User Verification Report
  Data archive user verification report KO+36m
• D7.3 – Completed Data Management Plan 
  Final DMP KO+42m
• D7.4 – Data Archive Documentation
  Final documentation of structure of data archive KO+42m

Objective: Ensure a proper and effective management of the consortium and its relationship with the Commission.

• D8.1 – End of Year 1 Review
  End of year 1 review KO+12
• D8.2 – End of Year 2 Review
  End of year 2 review KO+27
• D8.3 – Final Review
  Final review KO+42