Advanced search
Start date
(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Dynamical orbital classification of selected N-rich stars with Gaia Data Release 2 astrometry

Full text
Fernandez-Trincado, Jose G. [1] ; Chaves-Velasquez, Leonardo [2, 3] ; Perez-Villegas, Angeles [4] ; Vieira, Katherine [1] ; Moreno, Edmundo [5] ; Ortigoza-Urdaneta, Mario [1] ; Vega-Neme, Luis [6, 7]
Total Authors: 7
[1] Univ Atacama, Inst Astron & Ciencias Planetarias, Copayapu 485, Copiapo - Chile
[2] Univ Narino, Univ Narino Observ, Ave Panamer, Pasto, Narino - Colombia
[3] Univ Narino, Dept Fis, Torobajo Calle 18 Carrera 50, Pasto, Narino - Colombia
[4] Univ Sao Paulo, IAG, Rua Matao 1226, BR-05508900 Sao Paulo - Brazil
[5] Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 70264, Mexico City 04510, DF - Mexico
[6] Consejo Nacl Invest Cient & Tecn, Inst Astron Teor & Expt, Cordoba - Argentina
[7] Univ Nacl Cordoba, Observ Astron Cordoba, Cordoba - Argentina
Total Affiliations: 7
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 495, n. 4, p. 4113-4123, JUL 2020.
Web of Science Citations: 0

We have used the galaxy modelling algorithm GRAVPOT16, to explore the most probable orbital elements of a sample of 64 selected N-rich stars across the Milky Way. We use the newly measured proper motions from Gaia Data Release 2 with existing line-of-sight velocities from the second generation of the Apache Point Observatory Galactic Evolution Experiment (APOGEE-2) and spectrophotometric distance estimations from STARHORSE. We adopted a set of high-resolution particle simulations evolved in the same steady-state Galactic potential model with a bar, in order to identify the groups of N-rich stars that have a high probability of belonging to the bulge/bar, disc and stellar halo component. We find that the vast majority of the N-rich stars show typically maximum height from the Galactic plane below 3 kpc, and develop eccentric orbits (e > 0.5), which means that these stars appear to have bulge/bar-like and/or halo-like orbits. We also show that similar to 66 per cent of the selected N-rich stars currently reside in the inner Galaxy inside the corotation radius, whilst similar to 14 per cent are in halo-like orbits. Among the N-rich stars in the inner Galaxy, similar to 27 per cent share orbital properties in the boundary between bulge/bar and disc, depending on the bar pattern speeds. Our dynamical analysis also indicates that some of the N-rich stars are likely to be halo interlopers, which suggests that halo contamination is not insignificant within the bulge area. (AU)

FAPESP's process: 17/15893-1 - Globular cluster orbits of bulge: the formation and evolution of the Milky Way
Grantee:Maria de Los Angeles Perez Villegas
Support type: Scholarships in Brazil - Post-Doctorate