The Fornax3D project

(F3D)

Using the superb capabilities of MUSE@VLT, the F3D provides detailed high-resolution maps of the line-of-sight kinematics, line strengths of the stars, ionised gas for the 31 brightest galaxies (mB < 15 mag) inside the virial radius of the Fornax cluster 

Therefore, the F3D galaxies is a complete sample in morphology, stellar masses and radial distribution. 

The MUSE mosaics allow to map the stellar kinematics and stellar populations for the ETGs at larger radii, about two times more extended than the previous integral-field data of Scott et al. (2014) and more than 1–2 Re covered by the long-slit data of Bedregal et al. (2006). 

I am the co-PI of the F3D project (other co-PI is M. Sarzi). My major role in F3D was to provide the survey design, in terms of sample selection, MUSE pointings and depths, data analysis. 

I am leading the study of the structure and stellar population of the ETGs in the sample. This could be considered as a “follow-up” of the FDS study on the same sample based on the light and colour distribution analysed for each galaxy. 

Results were recently published in Iodice et al. (2019). For the present research project, I plan to derive the metallicity gradients out to the regions of the stellar halo in the massive ETGs at the centre of the cluster, to be compared with the theoretical predictions. Preliminary results on this topic, derived by combining FDS with F3D data, suggested that the massive members in the high-density region of the cluster have a higher fraction of accreted material that dominates most the galaxy structure. In these galaxies, the outskirts are more metal poor (−0.4 ≤ [M/H] ≤ 0 dex) than the central in-situ dominated parts (see Iodice et al. 2019).