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The contribution of N-rich stars to the Galactic stellar halo using APOGEE red giants | | Danny Horta
; J. Ted Mackereth
; Ricardo P. Schiavon
; Sten Hasselquist
; Jo Bovy
; Carlos Allende Prieto
; Timothy C. Beers
; Katia Cunha
; D. A. García-Hernández
; Shobhit S. Kisku
; Richard R. Lane
; Steven R. Majewski
; Andrew C. Mason
; David M. Nataf
; Alexandre Roman-Lopes
; Mathias Schultheis
; | | Date: |
3 Aug 2020 | | Abstract: | The contribution of dissolved globular clusters (GCs) to the stellar content
of the Galactic halo is a key constraint on models for GC formation and
destruction, and the mass assembly history of the Milky Way. Earlier results
from APOGEE pointed to a large contribution of destroyed GCs to the stellar
content of the inner halo, by as much as 25$\%$, which is an order of magnitude
larger than previous estimates for more distant regions of the halo. We set out
to measure the ratio between N-rich and normal halo field stars, as a function
of distance, by performing density modelling of halo field populations in
APOGEE DR16. Our results show that at 1.5 kpc from the Galactic Centre, N-rich
stars contribute a much higher 16$^{+12}_{-7}$$\%$ fraction to the total
stellar halo mass budget than the 2$^{+1}_{-0.7}$$\%$ ratio contributed at 15
kpc. Under the assumption that N-rich stars are former GC members that now
reside in the stellar halo field, and assuming the ratio between first-and
second-population GC stars being 1-to-2, we estimate a total contribution from
disrupted GC stars of the order of 24.7$^{+16}_{-10}$$\%$ at r = 1.5 kpc and
3$^{+1.5}_{-1}$$\%$ at r = 15 kpc. Furthermore, since our methodology compels
us to fit a density model to the stellar halo, we integrate such density within
a spherical shell from 1.5-20 kpc in radius, and find a total stellar mass
arising from dissolved and/or evaporated GCs of $M_{mathrm{GC,total}}$ =
10$^{+3.7}_{-2.5}$ $ imes$ 10$^{7}$ M$odot$. | | Source: | arXiv, 2008.01097 | | Services: | Forum | Review | PDF | Favorites | |
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