Comparison of N-body simulations to statistical observations of galaxy pairs

Roger E. Bartlett, Jane C. Charlton

Research output: Contribution to journalReview article

4 Citations (Scopus)

Abstract

N-body simulations were conducted of pairs of galaxies with a 3:1 mass ratio on parabolic orbits in order to quantify the effect of dynamical friction. The effects of varying the ratio of the dark matter halo size to the distance of closest approach were explored. Once the dark matter halos are fully overlapping the more massive simulated galaxies achieve a larger maximum separation after the first encounter, despite the increased dynamical friction caused by the more extended halos. Projected separation and radial velocity histograms were generated by "observing" the simulation results at various times and from various orientations. These histograms were compared with observations of galaxy pairs (Charlton & Salpeter 1991; Chengalur, Salpeter, & Terzian 1993) with the result that large halo radii (∼ 200-600 kpc) and wide distances of closest approach are generally favored. It is difficult to reconcile the small radial velocity differences that have been observed (median of ∼30 km s-1; Chengalur et al. 1993) with the simulations when we sample all parts of the orbits equally. Including an additional population of wide pairs that have just recently reached "turnabout" from the Hubble flow would lower the median velocity differences. Models suggest that additional data for pairs at intermediate separations should have a somewhat larger median velocity difference than the wide pairs. Very narrow pairs include galaxies that are interacting and whose gaseous components respond to forces other than gravity. If consistently small Δv are measured from neutral hydrogen velocities in a larger sample of narrow pairs, pressure forces and dissipation effects on the gaseous components could be responsible.

Original languageEnglish (US)
Pages (from-to)497-507
Number of pages11
JournalAstrophysical Journal
Volume449
Issue number2
DOIs
StatePublished - Aug 20 1995

Fingerprint

halos
galaxies
histograms
radial velocity
simulation
dark matter
histogram
friction
orbits
encounters
mass ratios
dissipation
gravitation
radii
comparison
hydrogen
gravity
effect

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

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abstract = "N-body simulations were conducted of pairs of galaxies with a 3:1 mass ratio on parabolic orbits in order to quantify the effect of dynamical friction. The effects of varying the ratio of the dark matter halo size to the distance of closest approach were explored. Once the dark matter halos are fully overlapping the more massive simulated galaxies achieve a larger maximum separation after the first encounter, despite the increased dynamical friction caused by the more extended halos. Projected separation and radial velocity histograms were generated by {"}observing{"} the simulation results at various times and from various orientations. These histograms were compared with observations of galaxy pairs (Charlton & Salpeter 1991; Chengalur, Salpeter, & Terzian 1993) with the result that large halo radii (∼ 200-600 kpc) and wide distances of closest approach are generally favored. It is difficult to reconcile the small radial velocity differences that have been observed (median of ∼30 km s-1; Chengalur et al. 1993) with the simulations when we sample all parts of the orbits equally. Including an additional population of wide pairs that have just recently reached {"}turnabout{"} from the Hubble flow would lower the median velocity differences. Models suggest that additional data for pairs at intermediate separations should have a somewhat larger median velocity difference than the wide pairs. Very narrow pairs include galaxies that are interacting and whose gaseous components respond to forces other than gravity. If consistently small Δv are measured from neutral hydrogen velocities in a larger sample of narrow pairs, pressure forces and dissipation effects on the gaseous components could be responsible.",
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Comparison of N-body simulations to statistical observations of galaxy pairs. / Bartlett, Roger E.; Charlton, Jane C.

In: Astrophysical Journal, Vol. 449, No. 2, 20.08.1995, p. 497-507.

Research output: Contribution to journalReview article

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