| | |
| | |
Stat |
Members: 3645 Articles: 2'503'724 Articles rated: 2609
24 April 2024 |
|
| | | |
|
Article overview
| |
|
From Stellar Halos to Intracluster Light: the physics of the Intra-Halo Stellar Component in cosmological hydrodynamical simulations | Rodrigo Cañas
; Claudia del P. Lagos
; Pascal J. Elahi
; Chris Power
; Charlotte Welker
; Yohan Dubois
; Christophe Pichon
; | Date: |
8 Aug 2019 | Abstract: | We study the Intra-Halo Stellar Component (IHSC) of Milky Way-mass systems up
to galaxy clusters in the Horizon-AGN cosmological hydrodynamical simulation.
We identify the IHSC using an improved phase-space galaxy finder algorithm
which provides an adaptive, physically motivated and shape-independent
definition of this stellar component, that can be applied to halos of arbitrary
masses. We explore the IHSC mass fraction-total halo’s stellar mass,
$f_{M*,IHSC}-M*$, relation and the physical drivers of its scatter. We find
that on average the $f_{M*,IHSC}$ increases with $M_{*,tot}$, with the scatter
decreasing strongly with mass from 2 dex at $M_{*,tot}sim10^{11}M_odot$ to
0.3 dex at group masses. At high masses, $M_{*,tot}>10^{11.5}M_odot$,
$f_{M*,IHSC}$ increases with the number of substructures, and with the mass
ratio between the central galaxy and largest satellite, at fixed $M_{*,tot}$.
From mid-size groups and systems below $M_{*,tot}<10^{12}M_odot$, we find that
the central galaxy’s stellar rotation-to-dispersion velocity ratio, V/{sigma},
displays the strongest (anti)-correlation with $f_{M*,IHSC}$ at fixed
$M_{*,tot}$ of all the galaxy and halo properties explored, transitioning from
$f_{M*,IHSC}$<0.1% for high V/{sigma}, to $f_{M*,IHSC}sim5$% for low
V/{sigma} galaxies. By studying the $f_{M*,IHSC}$ temporal evolution, we find
that, in the former, mergers not always take place, but if they did, they
happened early (z>1), while the high $f_{M*,IHSC}$ population displays a much
more active merger history. In the case of massive groups and galaxy clusters,
$M_{*,tot}>10^{12}M_odot$, a fraction $f_{M*,IHSC}sim$10-20% is reached at
$zsim1$ and then they evolve across lines of constant $f_{M*,IHSC}$ modulo
some small perturbations. Because of the limited simulation’s volume, the
latter is only tentative and requires a larger sample of simulated galaxy
clusters to confirm. | Source: | arXiv, 1908.2945 | Services: | Forum | Review | PDF | Favorites |
|
|
No review found.
Did you like this article?
Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.
browser Mozilla/5.0 AppleWebKit/537.36 (KHTML, like Gecko; compatible; ClaudeBot/1.0; +claudebot@anthropic.com)
|
| |
|
|
|
| News, job offers and information for researchers and scientists:
| |