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Extracting Galaxy Merger Timescales II: A new fitting formula | | Rhys J. J. Poulton
; Chris Power
; Aaron S. G. Robotham
; Pascal J. Elahi
; Claudia del P. Lagos
; | | Date: |
Sat, 17 Oct 2020 13:20:29 GMT (1829kb,D) | | Abstract: | Predicting the merger timescale ($ au_{
m merge}$) of merging dark matter
halos, based on their orbital parameters and the structural properties of their
hosts, is a fundamental problem in gravitational dynamics that has important
consequences for our understanding of cosmological structure formation and
galaxy formation. Previous models predicting $ au_{
m merge}$ have shown
varying degrees of success when compared to the results of cosmological
$N$-body simulations. We build on this previous work and propose a new model
for $ au_{
m merge}$ that draws on insights derived from these simulations.
We find that published predictions can provide reasonable estimates for
$ au_{
m merge}$ based on orbital properties at infall, but tend to
underpredict $ au_{
m merge}$ inside the host virial radius ($R_{200}$)
because tidal stripping is neglected, and overpredict it outside $R_{200}$
because the host mass is underestimated. Furthermore, we find that models that
account for orbital angular momentum via the circular radius $R_{
m circ}$
underpredict (overpredict) $ au_{
m merge}$ for bound (unbound) systems. By
fitting for the dependence of $ au_{
m merge}$ on various orbital and host
halo properties,we derive an improved model for $ au_{
m merge}$ that can be
applied to a merging halo at any point in its orbit. Finally, we discuss
briefly the implications of our new model for $ au_{
m merge}$ for
semi-analytical galaxy formation modelling. | | Source: | arXiv, 2010.08786 | | Services: | Forum | Review | PDF | Favorites | |
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