Simulating the shocks in the dissociative galaxy cluster Abell 1758N

R. E.G. Machado, R. Monteiro-Oliveira, G. B. Lima Neto, E. S. Cypriano

Resultado de la investigación: Article

11 Citas (Scopus)

Resumen

Major mergers between massive clusters have a profound effect in the intracluster gas, which may be used as a probe of the dynamics of structure formation at the high end of the mass function. An example of such a merger is observed at the northern component of Abell 1758, comprising two massive sub-clusters separated by approximately 750 kpc. One of the clusters exhibits an offset between the dark matter and the intracluster gas. We aim to determine whether it is possible to reproduce the specific morphological features of this cluster by means of a major merger. We perform dedicated SPH (smoothed particle hydrodynamics) N-body simulations in an attempt to simultaneously recover several observed features of Abell 1758, such as the X-ray morphology and the separation between the two peaks in the projected galaxy luminosity map. We propose a specific scenario for the off-axis collision of two massive clusters. This model adequately reproduces several observed features and suggests that Abell 1758 is seen approximately 0.4 Gyr after the first pericentric passage, and that the clusters are already approaching their maximum separation. This means that their relative velocity is as low as 380 km s-1. At the same time, the simulated model entails shock waves of ~4500 km s-1, which are currently undetected presumably due to the low-density medium. We explain the difference between these velocities and argue that the predicted shock fronts, while plausible, cannot be detected from currently available data.

Idioma originalEnglish
Páginas (desde-hasta)3309-3320
Número de páginas12
PublicaciónMonthly Notices of the Royal Astronomical Society
Volumen451
N.º3
DOI
EstadoPublished - 2015
Publicado de forma externa

Huella dactilar

merger
shock
galaxies
shock wave
gas
collision
hydrodynamics
probe
shock fronts
gases
simulation
shock waves
dark matter
luminosity
collisions
probes
x rays
particle
effect

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Machado, R. E. G., Monteiro-Oliveira, R., Lima Neto, G. B., & Cypriano, E. S. (2015). Simulating the shocks in the dissociative galaxy cluster Abell 1758N. Monthly Notices of the Royal Astronomical Society, 451(3), 3309-3320. https://doi.org/10.1093/mnras/stv1162
Machado, R. E.G. ; Monteiro-Oliveira, R. ; Lima Neto, G. B. ; Cypriano, E. S. / Simulating the shocks in the dissociative galaxy cluster Abell 1758N. En: Monthly Notices of the Royal Astronomical Society. 2015 ; Vol. 451, N.º 3. pp. 3309-3320.
@article{43e3e6c58ddb442595c2b8591c4f13b1,
title = "Simulating the shocks in the dissociative galaxy cluster Abell 1758N",
abstract = "Major mergers between massive clusters have a profound effect in the intracluster gas, which may be used as a probe of the dynamics of structure formation at the high end of the mass function. An example of such a merger is observed at the northern component of Abell 1758, comprising two massive sub-clusters separated by approximately 750 kpc. One of the clusters exhibits an offset between the dark matter and the intracluster gas. We aim to determine whether it is possible to reproduce the specific morphological features of this cluster by means of a major merger. We perform dedicated SPH (smoothed particle hydrodynamics) N-body simulations in an attempt to simultaneously recover several observed features of Abell 1758, such as the X-ray morphology and the separation between the two peaks in the projected galaxy luminosity map. We propose a specific scenario for the off-axis collision of two massive clusters. This model adequately reproduces several observed features and suggests that Abell 1758 is seen approximately 0.4 Gyr after the first pericentric passage, and that the clusters are already approaching their maximum separation. This means that their relative velocity is as low as 380 km s-1. At the same time, the simulated model entails shock waves of ~4500 km s-1, which are currently undetected presumably due to the low-density medium. We explain the difference between these velocities and argue that the predicted shock fronts, while plausible, cannot be detected from currently available data.",
keywords = "Galaxies: clusters: individual: A1758, Galaxies: clusters: intracluster medium, Methods: numerical",
author = "Machado, {R. E.G.} and R. Monteiro-Oliveira and {Lima Neto}, {G. B.} and Cypriano, {E. S.}",
year = "2015",
doi = "10.1093/mnras/stv1162",
language = "English",
volume = "451",
pages = "3309--3320",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "3",

}

Machado, REG, Monteiro-Oliveira, R, Lima Neto, GB & Cypriano, ES 2015, 'Simulating the shocks in the dissociative galaxy cluster Abell 1758N', Monthly Notices of the Royal Astronomical Society, vol. 451, n.º 3, pp. 3309-3320. https://doi.org/10.1093/mnras/stv1162

Simulating the shocks in the dissociative galaxy cluster Abell 1758N. / Machado, R. E.G.; Monteiro-Oliveira, R.; Lima Neto, G. B.; Cypriano, E. S.

En: Monthly Notices of the Royal Astronomical Society, Vol. 451, N.º 3, 2015, p. 3309-3320.

Resultado de la investigación: Article

TY - JOUR

T1 - Simulating the shocks in the dissociative galaxy cluster Abell 1758N

AU - Machado, R. E.G.

AU - Monteiro-Oliveira, R.

AU - Lima Neto, G. B.

AU - Cypriano, E. S.

PY - 2015

Y1 - 2015

N2 - Major mergers between massive clusters have a profound effect in the intracluster gas, which may be used as a probe of the dynamics of structure formation at the high end of the mass function. An example of such a merger is observed at the northern component of Abell 1758, comprising two massive sub-clusters separated by approximately 750 kpc. One of the clusters exhibits an offset between the dark matter and the intracluster gas. We aim to determine whether it is possible to reproduce the specific morphological features of this cluster by means of a major merger. We perform dedicated SPH (smoothed particle hydrodynamics) N-body simulations in an attempt to simultaneously recover several observed features of Abell 1758, such as the X-ray morphology and the separation between the two peaks in the projected galaxy luminosity map. We propose a specific scenario for the off-axis collision of two massive clusters. This model adequately reproduces several observed features and suggests that Abell 1758 is seen approximately 0.4 Gyr after the first pericentric passage, and that the clusters are already approaching their maximum separation. This means that their relative velocity is as low as 380 km s-1. At the same time, the simulated model entails shock waves of ~4500 km s-1, which are currently undetected presumably due to the low-density medium. We explain the difference between these velocities and argue that the predicted shock fronts, while plausible, cannot be detected from currently available data.

AB - Major mergers between massive clusters have a profound effect in the intracluster gas, which may be used as a probe of the dynamics of structure formation at the high end of the mass function. An example of such a merger is observed at the northern component of Abell 1758, comprising two massive sub-clusters separated by approximately 750 kpc. One of the clusters exhibits an offset between the dark matter and the intracluster gas. We aim to determine whether it is possible to reproduce the specific morphological features of this cluster by means of a major merger. We perform dedicated SPH (smoothed particle hydrodynamics) N-body simulations in an attempt to simultaneously recover several observed features of Abell 1758, such as the X-ray morphology and the separation between the two peaks in the projected galaxy luminosity map. We propose a specific scenario for the off-axis collision of two massive clusters. This model adequately reproduces several observed features and suggests that Abell 1758 is seen approximately 0.4 Gyr after the first pericentric passage, and that the clusters are already approaching their maximum separation. This means that their relative velocity is as low as 380 km s-1. At the same time, the simulated model entails shock waves of ~4500 km s-1, which are currently undetected presumably due to the low-density medium. We explain the difference between these velocities and argue that the predicted shock fronts, while plausible, cannot be detected from currently available data.

KW - Galaxies: clusters: individual: A1758

KW - Galaxies: clusters: intracluster medium

KW - Methods: numerical

UR - http://www.scopus.com/inward/record.url?scp=84942155894&partnerID=8YFLogxK

U2 - 10.1093/mnras/stv1162

DO - 10.1093/mnras/stv1162

M3 - Article

AN - SCOPUS:84942155894

VL - 451

SP - 3309

EP - 3320

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -