The IACOB project in a nutshell

The IACOB project aims to scientifically exploiting the IACOB spectroscopic database using state-of-the-art stellar atmosphere models, evolutionary codes, and techniques. Three main broad research lines are planned to be developed within this project:

Quantitative spectroscopic analysis of Galactic OB stars:

Aimed at investigating old-standing (and new) puzzling questions in the field of massive stars using the results from a homogeneous spectroscopic analysis of a large sample of Galactic OB stars. The outcome from the quantitative analysis of this unique dataset will also complement (and be complemented with) the astrometric and photometric observations which will be provided by the GAIA mission, and will be placed in a more broader context (in terms of metallicity) by considering the results from a similar analysis in OB stars in 30 Dor (LMC, Z=0.5Zsun) by the VLT/FLAMES Tarantula survey consortium. This research line will also make use of other available spectroscopic observations in other wavelength ranges. More information about this main research line can be found in WP3, WP4, and WP5.

Investigation of the macroturbulent broadening in OB stars and its possible pulsational origin:

Aimed at (a) characterizing the macroturbulent broadening along the life of massive stars in different metallicity environments, (b) investigating its connection with spectroscopic variability and stellar oscillations, (c) exploring this macroturbulent broadening as an alternative tool to identify and investigate pulsations in OB stars and d) studying the impact of stellar pulsations on the photospheric and wind structure, as well as the evolution of massive stars. This research line also aims at reinforcing already established synergies between the Massive Stars and the Asteroseismology communities. This research line is mainly developed in the framework of WP2.

Combined study of massive OB stars and HII regions:

Aimed at (a) investigating the agreement of presentday abundances as derived by means of stellar (B-type stars) and nebular (H II regions) spectroscopic studies, and (b) testing the ionizing spectral energy distributions predicted by state-of-the-art stellar atmosphere codes using nebular constraints. This research line will make use of stellar and nebular observations of selected candidates in the Milky Way compiled in the last years. This research line also aims at reinforcing already established synergies between the Massive Stars and the H II region communities. These two task are the main drivers of WP6

A global overview of the six working packages in which the IACOB project has been divided can be found here