The prevalence of pseudo-bulges in the Auriga simulations

Ignacio D. Gargiulo, Antonela Monachesi, Facundo A. Gómez, Robert J.J. Grand, Federico Marinacci, Rüdiger Pakmor, Simon D.M. White, Eric F. Bell, Francesca Fragkoudi, Patricia Tissera

Resultado de la investigación: Article

Resumen

We study the galactic bulges in the Auriga simulations, a suite of 30 cosmological magnetohydrodynamical zoom-in simulations of late-type galaxies in Milky Way sized dark matter haloes performed with the moving-mesh code AREPO. We aim to characterize bulge formation mechanisms in this large suite of galaxies simulated at high resolution in a fully cosmological context. The bulges of the Auriga galaxies show a large variety in their shapes, sizes, and formation histories. According to observational classification criteria, such as Sérsic index and degree of ordered rotation, the majority of the Auriga bulges can be classified as pseudo-bulges, while some of them can be seen as composite bulges with a classical component; however, none can be classified as a classical bulge. Auriga bulges show mostly an in situ origin, 21 per cent of them with a negligible accreted fraction (facc < 0.01). In general, their in situ component was centrally formed, with ∼75 per cent of the bulges forming most of their stars inside the bulge region at z = 0. Part of their in situ mass growth is rapid and is associated with the effects of mergers, while another part is more secular in origin. In 90 per cent of the Auriga bulges, the accreted bulge component originates from less than four satellites. We investigate the relation between the accreted stellar haloes and the bulges of the Auriga simulations. The total bulge mass shows no correlation with the accreted stellar halo mass, as in observations. However, the accreted mass of bulges tends to correlate with their respective accreted stellar halo mass.

Idioma originalEnglish
Páginas (desde-hasta)5742-5763
Número de páginas22
PublicaciónMonthly Notices of the Royal Astronomical Society
Volumen489
N.º4
DOI
EstadoPublished - 1 ene 2019

Huella dactilar

halos
simulation
galaxies
galactic bulge
formation mechanism
merger
mesh
dark matter
histories
stars
composite materials
high resolution
history
in situ

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Gargiulo, I. D., Monachesi, A., Gómez, F. A., Grand, R. J. J., Marinacci, F., Pakmor, R., ... Tissera, P. (2019). The prevalence of pseudo-bulges in the Auriga simulations. Monthly Notices of the Royal Astronomical Society, 489(4), 5742-5763. https://doi.org/10.1093/mnras/stz2536
Gargiulo, Ignacio D. ; Monachesi, Antonela ; Gómez, Facundo A. ; Grand, Robert J.J. ; Marinacci, Federico ; Pakmor, Rüdiger ; White, Simon D.M. ; Bell, Eric F. ; Fragkoudi, Francesca ; Tissera, Patricia. / The prevalence of pseudo-bulges in the Auriga simulations. En: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 489, N.º 4. pp. 5742-5763.
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abstract = "We study the galactic bulges in the Auriga simulations, a suite of 30 cosmological magnetohydrodynamical zoom-in simulations of late-type galaxies in Milky Way sized dark matter haloes performed with the moving-mesh code AREPO. We aim to characterize bulge formation mechanisms in this large suite of galaxies simulated at high resolution in a fully cosmological context. The bulges of the Auriga galaxies show a large variety in their shapes, sizes, and formation histories. According to observational classification criteria, such as S{\'e}rsic index and degree of ordered rotation, the majority of the Auriga bulges can be classified as pseudo-bulges, while some of them can be seen as composite bulges with a classical component; however, none can be classified as a classical bulge. Auriga bulges show mostly an in situ origin, 21 per cent of them with a negligible accreted fraction (facc < 0.01). In general, their in situ component was centrally formed, with ∼75 per cent of the bulges forming most of their stars inside the bulge region at z = 0. Part of their in situ mass growth is rapid and is associated with the effects of mergers, while another part is more secular in origin. In 90 per cent of the Auriga bulges, the accreted bulge component originates from less than four satellites. We investigate the relation between the accreted stellar haloes and the bulges of the Auriga simulations. The total bulge mass shows no correlation with the accreted stellar halo mass, as in observations. However, the accreted mass of bulges tends to correlate with their respective accreted stellar halo mass.",
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Gargiulo, ID, Monachesi, A, Gómez, FA, Grand, RJJ, Marinacci, F, Pakmor, R, White, SDM, Bell, EF, Fragkoudi, F & Tissera, P 2019, 'The prevalence of pseudo-bulges in the Auriga simulations', Monthly Notices of the Royal Astronomical Society, vol. 489, n.º 4, pp. 5742-5763. https://doi.org/10.1093/mnras/stz2536

The prevalence of pseudo-bulges in the Auriga simulations. / Gargiulo, Ignacio D.; Monachesi, Antonela; Gómez, Facundo A.; Grand, Robert J.J.; Marinacci, Federico; Pakmor, Rüdiger; White, Simon D.M.; Bell, Eric F.; Fragkoudi, Francesca; Tissera, Patricia.

En: Monthly Notices of the Royal Astronomical Society, Vol. 489, N.º 4, 01.01.2019, p. 5742-5763.

Resultado de la investigación: Article

TY - JOUR

T1 - The prevalence of pseudo-bulges in the Auriga simulations

AU - Gargiulo, Ignacio D.

AU - Monachesi, Antonela

AU - Gómez, Facundo A.

AU - Grand, Robert J.J.

AU - Marinacci, Federico

AU - Pakmor, Rüdiger

AU - White, Simon D.M.

AU - Bell, Eric F.

AU - Fragkoudi, Francesca

AU - Tissera, Patricia

PY - 2019/1/1

Y1 - 2019/1/1

N2 - We study the galactic bulges in the Auriga simulations, a suite of 30 cosmological magnetohydrodynamical zoom-in simulations of late-type galaxies in Milky Way sized dark matter haloes performed with the moving-mesh code AREPO. We aim to characterize bulge formation mechanisms in this large suite of galaxies simulated at high resolution in a fully cosmological context. The bulges of the Auriga galaxies show a large variety in their shapes, sizes, and formation histories. According to observational classification criteria, such as Sérsic index and degree of ordered rotation, the majority of the Auriga bulges can be classified as pseudo-bulges, while some of them can be seen as composite bulges with a classical component; however, none can be classified as a classical bulge. Auriga bulges show mostly an in situ origin, 21 per cent of them with a negligible accreted fraction (facc < 0.01). In general, their in situ component was centrally formed, with ∼75 per cent of the bulges forming most of their stars inside the bulge region at z = 0. Part of their in situ mass growth is rapid and is associated with the effects of mergers, while another part is more secular in origin. In 90 per cent of the Auriga bulges, the accreted bulge component originates from less than four satellites. We investigate the relation between the accreted stellar haloes and the bulges of the Auriga simulations. The total bulge mass shows no correlation with the accreted stellar halo mass, as in observations. However, the accreted mass of bulges tends to correlate with their respective accreted stellar halo mass.

AB - We study the galactic bulges in the Auriga simulations, a suite of 30 cosmological magnetohydrodynamical zoom-in simulations of late-type galaxies in Milky Way sized dark matter haloes performed with the moving-mesh code AREPO. We aim to characterize bulge formation mechanisms in this large suite of galaxies simulated at high resolution in a fully cosmological context. The bulges of the Auriga galaxies show a large variety in their shapes, sizes, and formation histories. According to observational classification criteria, such as Sérsic index and degree of ordered rotation, the majority of the Auriga bulges can be classified as pseudo-bulges, while some of them can be seen as composite bulges with a classical component; however, none can be classified as a classical bulge. Auriga bulges show mostly an in situ origin, 21 per cent of them with a negligible accreted fraction (facc < 0.01). In general, their in situ component was centrally formed, with ∼75 per cent of the bulges forming most of their stars inside the bulge region at z = 0. Part of their in situ mass growth is rapid and is associated with the effects of mergers, while another part is more secular in origin. In 90 per cent of the Auriga bulges, the accreted bulge component originates from less than four satellites. We investigate the relation between the accreted stellar haloes and the bulges of the Auriga simulations. The total bulge mass shows no correlation with the accreted stellar halo mass, as in observations. However, the accreted mass of bulges tends to correlate with their respective accreted stellar halo mass.

KW - Galaxies: bulges

KW - Galaxies: formation

KW - Methods: numerical

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DO - 10.1093/mnras/stz2536

M3 - Article

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JO - Monthly Notices of the Royal Astronomical Society

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Gargiulo ID, Monachesi A, Gómez FA, Grand RJJ, Marinacci F, Pakmor R y otros. The prevalence of pseudo-bulges in the Auriga simulations. Monthly Notices of the Royal Astronomical Society. 2019 ene 1;489(4):5742-5763. https://doi.org/10.1093/mnras/stz2536