English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse
  1. View item / 
  2. Item Summary

Item

ITEM ACTIONSEXPORT
Add to Basket
  Local TagsRelease HistoryDetailsSummary

Released
Journal Article

NIHAO XVI: the properties and evolution of kinematically selected discs, bulges, and stellar haloes

MPS-Authors

Obreja,  Aura
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Dutton,  Aaron A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Macciò,  Andrea V.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Moster,  Benjamin
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Buck,  Tobias
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

van den Ven,  Glenn
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wang,  Liang
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Stinson,  Gregory S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zhu,  Ling
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.4424O
(Any fulltext)

Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Obreja, A., Dutton, A. A., Macciò, A. V., Moster, B., Buck, T., van den Ven, G., et al. (2019). NIHAO XVI: the properties and evolution of kinematically selected discs, bulges, and stellar haloes. Monthly Notices of the Royal Astronomical Society, 487, 4424-4456.


Cite as: https://hdl.handle.net/21.11116/0000-0005-D034-5
Abstract
We use 25 simulated galaxies from the NIHAO project to define and characterize a variety of kinematic stellar structures: thin and thick discs, large-scale single discs, classical and pseudo-bulges, spheroids, inner discs, and stellar haloes. These structures have masses, spins, shapes, and rotational support in good agreement with theoretical expectations and observational data. Above a dark matter halo mass of 2.5× 10^ 11 M_{\odot }, all galaxies have a classical bulge and 70 per cent have a thin and thick disc. The kinematic (thin) discs follow a power-law relation between angular momentum and stellar mass J_*=3.4M_*^{1.26± 0.06}, in very good agreement with the prediction based on the empirical stellar-to-halo-mass relation in the same mass range, and show a strong correlation between maximum `observed' rotation velocity and dark matter halo circular velocity v_c=6.4v_max^{0.64± 0.04}. Tracing back in time these structures' progenitors, we find all of them to lose a fraction 1 - fj of their maximum angular momentum. Thin discs are significantly better at retaining their high- redshift spins (fj ̃ 0.70) than thick ones (fj ̃ 0.40). Stellar haloes have their progenitor baryons assembled the latest (z1/2 ̃ 1.1) and over the longest time-scales (τ ̃ 6.2 Gyr), and have the smallest fraction of stars born in situ (fin situ = 0.35 ± 0.14). All other structures have 1.5 ≲ z1/2 ≲ 3, τ = 4 ± 2 Gyr, and fin situ ≳ 0.9.