Fig. 10: Comparison of the radial [Fe/H] gradient (∂[Fe/H]/∂Rguide, in terms of guiding-centre radius Rguide) and the corresponding [Fe/H] dispersion (σ[Fe/H]) around the gradient in this work, with the results from LAMOST and APOGEE.
From: Potential impact of the Sagittarius dwarf galaxy on the formation of young O-rich stars
The uncertainties (error bars) in each panel are derived using MCMC (Markov Chain Monte Carlo) fitting, employing the Python code emcee69. a, b The black lines in each panel represent the result of this work, using the GALAH subgiant and MSTO stars; the blue and green lines represent the results from the LAMOST data (LAMOST DR7 subgiant sample from Xiang & Rix 202218) and literature (based on APOGEE DR17 red giant sample from Anders et al. 202330), respectively. The grey-shaded area marks the age interval in which we expect to see signatures from the Gaia Sausage/Enceladus (GSE) merger event. Source data are provided as a Source Data file.
