W 4.2: Scientific Cases and Input Data
WP 4.2 produces simulated data or provides real data (for PIONIER, LINC-Nirvana and Vega) in a common file format. These data will serve as inputs for testing and comparing the algorithms and, later, for training end users of the image reconstruction software. At least part of these data files will be made available to the partners in the early stages of the project (about T0+6m) to allow for algorithm developments. According to the science cases of the instruments, synthetic brightness distributions of astrophysical objects will be computed for a number of relevant cases, e.g. circumstellar and AGN environments (jets, dust and protoplanetary disks, clumpy environments, etc.). These models will serve to simulate realistic data for GRAVITY MATISSE and LINC-Nirvana. However, for thorough testing of the algorithms, nothing replaces real data so sample datasets will be obtained from existing instruments such as PIONIER, Vega/CHARA and, (after late 2014), LINC-Nirvana. These data files will follow astronomical standards and use the FITS-based format expected by the image reconstruction software: OI-FITS for the interferometric data and multi-dimensional FITS for the images. For the simulated data files, in order to establish the performance of the image reconstruction methods, the specific brightness distribution (x,y,lambda) of the true object will also be delivered. A scientific document based on published papers will be written and provided to WP4.3 to describe the conventions used for the data format and the specific characteristics of the data generated by different instruments. We expect that, as it will take into account the characteristics of the new instruments for the first time, this document will be useful to propose a revised OI-FITS standard to the community.
A clumpy AGN torus (model by Schartmann et al., 2008, A&A 482, 67) reconstructed by BSMEM algorithm from synthetic 6-telescope MROI data (Young et al., 2011, conf. "Resolving the future of astronomy with long-baseline interferometry", Socorro).
The Mira-type star Chi Cygni at several epochs. Images reconstructed with the MiRA algorithm from IOTA data (Lacour et al., 2007, A&A 707, 632).
