Ram pressure stripping in a galaxy formation model - I. A novel numerical approach

Tomás E. Tecce, Sofía A. Cora, Patricia B. Tissera, Mario G. Abadi, Claudia del P Lagos

Resultado de la investigación: Article

42 Citas (Scopus)

Resumen

We develop a new numerical approach to describe the action of ram pressure stripping (RPS) within a semi-analytic model of galaxy formation and evolution which works in combination with non-radiative hydrodynamical simulations of galaxy clusters. The new feature in our method is the use of the gas particles to obtain the kinematical and thermodynamical properties of the intragroup and intracluster medium (ICM). This allows a self-consistent estimation of the RPS experienced by satellite galaxies. We find that the ram pressure in the central regions of clusters increases approximately one order of magnitude between z= 1 and 0, consistent with the increase in the density of the ICM. The mean ram pressure experienced by galaxies within the virial radius increases with decreasing redshift. In clusters with virial masses Mvir≃ 1015 h-1 M, over 50 per cent of satellite galaxies have experienced ram pressures ~10-11 h-2 dyn cm-2 or higher for z≲ 0.5. In smaller clusters (Mvir≃ 1014 h-1 M) the mean ram pressures are approximately one order of magnitude lower at all redshifts. RPS has a strong effect on the cold gas content of galaxies for all cluster masses. At z= 0, over 70 per cent of satellite galaxies within the virial radius are completely depleted of cold gas. For the more massive clusters the fraction of depleted galaxies is already established at z≃ 1, whereas for the smaller clusters this fraction increases appreciably between z= 1 and 0. This indicates that the rate at which the cold gas is stripped depends on the virial mass of the host cluster. Compared to our new approach, the use of an analytic profile to describe the ICM results in an overestimation of the ram pressure larger than 50 per cent for z > 0.5.

Idioma originalEnglish
Páginas (desde-hasta)2008-2021
Número de páginas14
PublicaciónMonthly Notices of the Royal Astronomical Society
Volumen408
N.º4
DOI
EstadoPublished - nov 2010

Huella dactilar

ram
galactic evolution
stripping
galaxies
cold gas
gas
radii
profiles
gases

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Citar esto

Tecce, Tomás E. ; Cora, Sofía A. ; Tissera, Patricia B. ; Abadi, Mario G. ; Lagos, Claudia del P. / Ram pressure stripping in a galaxy formation model - I. A novel numerical approach. En: Monthly Notices of the Royal Astronomical Society. 2010 ; Vol. 408, N.º 4. pp. 2008-2021.
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Ram pressure stripping in a galaxy formation model - I. A novel numerical approach. / Tecce, Tomás E.; Cora, Sofía A.; Tissera, Patricia B.; Abadi, Mario G.; Lagos, Claudia del P.

En: Monthly Notices of the Royal Astronomical Society, Vol. 408, N.º 4, 11.2010, p. 2008-2021.

Resultado de la investigación: Article

TY - JOUR

T1 - Ram pressure stripping in a galaxy formation model - I. A novel numerical approach

AU - Tecce, Tomás E.

AU - Cora, Sofía A.

AU - Tissera, Patricia B.

AU - Abadi, Mario G.

AU - Lagos, Claudia del P

PY - 2010/11

Y1 - 2010/11

N2 - We develop a new numerical approach to describe the action of ram pressure stripping (RPS) within a semi-analytic model of galaxy formation and evolution which works in combination with non-radiative hydrodynamical simulations of galaxy clusters. The new feature in our method is the use of the gas particles to obtain the kinematical and thermodynamical properties of the intragroup and intracluster medium (ICM). This allows a self-consistent estimation of the RPS experienced by satellite galaxies. We find that the ram pressure in the central regions of clusters increases approximately one order of magnitude between z= 1 and 0, consistent with the increase in the density of the ICM. The mean ram pressure experienced by galaxies within the virial radius increases with decreasing redshift. In clusters with virial masses Mvir≃ 1015 h-1 M⊙, over 50 per cent of satellite galaxies have experienced ram pressures ~10-11 h-2 dyn cm-2 or higher for z≲ 0.5. In smaller clusters (Mvir≃ 1014 h-1 M⊙) the mean ram pressures are approximately one order of magnitude lower at all redshifts. RPS has a strong effect on the cold gas content of galaxies for all cluster masses. At z= 0, over 70 per cent of satellite galaxies within the virial radius are completely depleted of cold gas. For the more massive clusters the fraction of depleted galaxies is already established at z≃ 1, whereas for the smaller clusters this fraction increases appreciably between z= 1 and 0. This indicates that the rate at which the cold gas is stripped depends on the virial mass of the host cluster. Compared to our new approach, the use of an analytic profile to describe the ICM results in an overestimation of the ram pressure larger than 50 per cent for z > 0.5.

AB - We develop a new numerical approach to describe the action of ram pressure stripping (RPS) within a semi-analytic model of galaxy formation and evolution which works in combination with non-radiative hydrodynamical simulations of galaxy clusters. The new feature in our method is the use of the gas particles to obtain the kinematical and thermodynamical properties of the intragroup and intracluster medium (ICM). This allows a self-consistent estimation of the RPS experienced by satellite galaxies. We find that the ram pressure in the central regions of clusters increases approximately one order of magnitude between z= 1 and 0, consistent with the increase in the density of the ICM. The mean ram pressure experienced by galaxies within the virial radius increases with decreasing redshift. In clusters with virial masses Mvir≃ 1015 h-1 M⊙, over 50 per cent of satellite galaxies have experienced ram pressures ~10-11 h-2 dyn cm-2 or higher for z≲ 0.5. In smaller clusters (Mvir≃ 1014 h-1 M⊙) the mean ram pressures are approximately one order of magnitude lower at all redshifts. RPS has a strong effect on the cold gas content of galaxies for all cluster masses. At z= 0, over 70 per cent of satellite galaxies within the virial radius are completely depleted of cold gas. For the more massive clusters the fraction of depleted galaxies is already established at z≃ 1, whereas for the smaller clusters this fraction increases appreciably between z= 1 and 0. This indicates that the rate at which the cold gas is stripped depends on the virial mass of the host cluster. Compared to our new approach, the use of an analytic profile to describe the ICM results in an overestimation of the ram pressure larger than 50 per cent for z > 0.5.

KW - Galaxies: clusters: general

KW - Galaxies: clusters: intracluster medium

KW - Galaxies: evolution

KW - Galaxies: formation

KW - Intergalactic medium

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DO - 10.1111/j.1365-2966.2010.17262.x

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