Context. Elements heavier than Li are produced in the interiors of stars. However, for many elements the exact production sites and the timescales on which they are dispersed into the interstellar medium are unknown. Having a clear picture on the origins of the elements is important for our ability to trace and understand the formation and chemical evolution of the Milky Way and its stellar populations. Aims. The aim of this study is to investigate the origin and evolution of Sc, V, Mn, and Co for a homogeneous and statistically significant sample of stars probing the different populations of the Milky Way, in particular the thin and thick disks. Methods. Using high-resolution spectra obtained with the MIKE, FEROS, SOFIN, FIES, UVES, and HA...
We have derived elemental abundances of O, Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Co, Ni as well as for...
Aims. Following our solar work, we perform NLTE calculations of the Mn abundance for fourteen stars ...
For the first time, we present an extensive study of stars with individual non-LTE (NLTE) abundances...
Context. Elements heavier than Li are produced in the interiors of stars. However, for man...
Context.The formation scenario of the Galactic thick disk is an unresolved problem. Chemical abunda...
Aims. We have used FLAMES (the Fibre Large Array Multi Element Spectrograph) at the VLT-UT2 telescop...
Context.Manganese is an iron-peak element and although the nucleosynthesis path that leads to its f...
Context. Elements heavier than iron are produced through neutron-capture processes in the different ...
Context. Manganese is an iron-peak element and although the nucleosynthesis path that leads to its f...
We have used FLAMES (the Fibre Large Array Multi Element Spectrograph) at the VLT-UT2 telescope to o...
The abundance ratios of manganese to iron in late-type stars across a wide metallicity range place t...
Context. Elements heavier than iron are produced through neutron-capture processes in the different ...
Context. The formation and evolution of the Galactic bulge and the Milky Way is still a debated subj...
Context. The pattern of chemical abundance ratios in stellar populations of the Milky Way is a finge...
We have derived elemental abundances of O, Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Co, Ni as well as for...
We have derived elemental abundances of O, Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Co, Ni as well as for...
Aims. Following our solar work, we perform NLTE calculations of the Mn abundance for fourteen stars ...
For the first time, we present an extensive study of stars with individual non-LTE (NLTE) abundances...
Context. Elements heavier than Li are produced in the interiors of stars. However, for man...
Context.The formation scenario of the Galactic thick disk is an unresolved problem. Chemical abunda...
Aims. We have used FLAMES (the Fibre Large Array Multi Element Spectrograph) at the VLT-UT2 telescop...
Context.Manganese is an iron-peak element and although the nucleosynthesis path that leads to its f...
Context. Elements heavier than iron are produced through neutron-capture processes in the different ...
Context. Manganese is an iron-peak element and although the nucleosynthesis path that leads to its f...
We have used FLAMES (the Fibre Large Array Multi Element Spectrograph) at the VLT-UT2 telescope to o...
The abundance ratios of manganese to iron in late-type stars across a wide metallicity range place t...
Context. Elements heavier than iron are produced through neutron-capture processes in the different ...
Context. The formation and evolution of the Galactic bulge and the Milky Way is still a debated subj...
Context. The pattern of chemical abundance ratios in stellar populations of the Milky Way is a finge...
We have derived elemental abundances of O, Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Co, Ni as well as for...
We have derived elemental abundances of O, Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Co, Ni as well as for...
Aims. Following our solar work, we perform NLTE calculations of the Mn abundance for fourteen stars ...
For the first time, we present an extensive study of stars with individual non-LTE (NLTE) abundances...