7 citations · 10 across the 6 of their papers we have counts for
6 papers
The metal-poor tail of the APOGEE survey II. Spectral analysis of Mg and Si in very metal-poor APOGEE spectra
M. Montelius, A. Angrilli Muglia, E. Starkenburg +9
H-band spectra contain very limited spectral information for stars at the most metal-poor tail ( Fe/H < -2.5) because the available Fe lines in FGK stars in this wavelength range a…
The metal-poor tail of the APOGEE survey I. Uncovering [Fe/H] < -2.5 stars from the inner Galaxy to the Magellanic Clouds
M. Montelius, E. Starkenburg, H. Woudenberg +9
In the search for metal-poor stars, large spectroscopic surveys are an invaluable tool. However, the spectra of metal-poor stars can be difficult to analyse because of the relative…
A Pristine-UNIONS view on the Galaxy: Kinematics of the distant spur feature of the Sagittarius stream traced by Blue Horizontal Branch stars
M. Bayer, E. Starkenburg, G. F. Thomas +14
Providing a detailed picture of the Sagittarius (Sgr) stream offers important constraints on the build-up of the Galactic halo as well as its gravitational potential at large radii…
The Pristine survey. XXVI. Chemical abundances of subgiant stars of the extremelymetal-poor stream C-19
P. Bonifacio, E. Caffau, P. François +17
Context: The C-19 stellar stream is the most metal-poor stream known to date. While its width and velocity dispersion indicate a dwarf galaxy origin, its metallicity spread and abu…
HR-GO I: Comprehensive NLTE abundance analysis of the Cetus stream
T. M. Sitnova, Z. Yuan, T. Matsuno +8
Dwarf galaxy streams encode vast amounts of information essential to understanding early galaxy formation and nucleosynthesis channels. Due to the variation in the timescales of st…
The Pristine survey -- XXII. A serendipitous discovery of an extremely Li-rich very metal-poor giant and a new method of Li/Li isotope measurement
T. M. Sitnova, T. Matsuno, Z. Yuan +5
We report the serendipitous discovery of a very metal-poor (VMP) Li-rich giant star ( = 469080 K, log g = 1.340.13, [Fe/H] = 0.07). We analyse the…