High-resolution simulations of galaxy mergers: Resolving globular cluster formation

F. Bournaud; P. -A. Duc; E. Emsellem

doi:10.1111/j.1745-3933.2008.00511.x

Home/Archive/arXiv

arXiv · 0806.1386

High-resolution simulations of galaxy mergers: Resolving globular cluster formation

F. Bournaud·P. -A. Duc·E. Emsellem

View original source ↗Read source document ↗Export metadata ↓

Abstract

Massive star clusters observed in galaxy mergers are often suggested to be progenitors of globular clusters. To study this hypothesis, we performed the highest resolution simulation of a gas-rich galaxy merger so far. The formation of massive star clusters of 10^5 to 10^7 Mo, triggered by the galaxy interaction, is directly resolved in this model. We show that these clusters are tightly bound structures with little net rotation, due to evolve into compact long-lived stellar systems. Massive clusters formed in galaxy mergers are thus robust candidates for progenitors of long-lived globular clusters. The simulated cluster mass spectrum is consistent with theory and observations. Tidal dwarf galaxies of 10^8-9 Mo can form at the same time, and appear to be part of a different class of objects, being more extended and rotating.

Explore related subjects

astro-ph

Keep this discovery

BibTeX RIS

F. Bournaud, P. -A. Duc, E. Emsellem. 2008-06-09. High-resolution simulations of galaxy mergers: Resolving globular cluster formation. https://doi.org/10.1111/j.1745-3933.2008.00511.x

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2016

Black Stars and Gamma Ray Bursts

Stars that are collapsing toward forming a black hole but are frozen near the Schwarzschild horizon are termed "black stars". Collisions of black stars, in contrast to black hole collisions, may be sources of gamma ray bursts, whose basic parameters are estimated quite simply and are found to be consistent with observed gamma ray bursts. Black star gamma ray bursts should be preceded by gravitational wave emission similar to that from the coalescence of black holes.

astro-ph↗

arXiv2016

Kinematic Control of the Inertiality of ICRS Catalogs

We perform a kinematic analysis of the Hipparcos and TRC proper motions of stars by using a linear Ogorodnikov-Milne model. All of the distant (r more than 0.2 kpc) stars of the Hipparcos catalog have been found to rotate around the Galactic y axis with an angular velocity of -0.36 +/- 0.09 mas/year. One of the causes of this rotation may be an uncertainty in the lunisolar precession constant adopted when constructing the ICRS. In this case? the correction to the IAU (1976) lunisolar precession constant in longitude is shown to be -3.26 +/- 0.10 mas/yr. Based on the TRC catalog, we have determined the main Oort constants: A = 14.9 +/- 1.0 and B = -10.8 +/- 0.3 km/s/kpc. The component of the model that describes the rotation of all TRC stars around the Galactic y axis is nonzero for all magnitudes, My= -0.86 +/- 0.11 mas/yr.

astro-ph↗

arXiv2016

Astrometric Control of the Inertiality of the Hipparcos Catalog

Based on the most complete list of the results of an individual comparison of the proper motions for stars of various programs common to the Hipparcos catalog, each of which is an independent realization of the inertial reference frame with regard to stellar proper motions, we redetermined the vector $ω$ of residual rotation of the ICRS system relative to the extragalactic reference frame. The equatorial components of this vector were found to be the following: $ω_x = +0.04\pm 0.15$ mas yr$^{-1}$, $ω_y = +0.18\pm 0.12$ mas yr$^{-1}$, and $ω_z = -0.35\pm 0.09$ mas yr$^{-1}$.

astro-ph↗