240 research outputs found
The accreted stellar halo as a window on halo assembly in L* galaxies
Theory and observations agree that the accreted stellar halos (ASHs) of Milky
Way-like galaxies display significant scatter. I take advantage of this
stochasticity to invert the link between halo assembly history (HAH) and ASH,
using mock ASHs corresponding to 750 CDM HAHs, sharing a final virial
mass of . Hosts with poor/rich ASHs assemble
following orthogonal growth-patterns. Hosts with rich ASHs experience accretion
events (AEs) with high virial mass ratios (HVMRs, ) at
, in a phase of fast growth. This maximizes
the accreted stellar mass under the condition these satellites are disrupted by
. At similar times, hosts with poor ASHs grow slowly through minor
mergers, with only very recent HVMR AEs: this results in a globally more
abundant satellite population and in distinctive surviving massive satellites
(stellar mass ). Several properties of the Milky
Way are in agreement with the predictions of this framework for hosts with
poor, concentrated ASHs, including: i) the recent infall of Sagittarius and
Magellanic Clouds, ii) the likely higher-than-average concentration of its dark
halo, iii) the signatures of fast chemical enrichment of a sizable fraction of
its halo stellar populations.Comment: accepted version, minor change
Giant cold satellites from low-concentration haloes
The dwarf satellite galaxies of the Milky Way Crater II and Antlia II have
uncommonly low dynamical mass densities, due to their large size and low
velocity dispersion. Previous work have failed to identify formation scenarios
within the CDM framework and have invoked cored dark matter haloes,
processed by tides. I show that the tidal evolution of CDM NFW haloes
is richer than previously recognised: tidal heating causes the innermost
regions of haloes that fall short of the mass-concentration relation to expand
significantly, resulting in the formation of giant, kinematically cold
satellites like Crater II and Antlia II. Furthermore, while the satellite is
reaching apocenter, extra-tidal material can cause an even more inflated
appearance. When present, as likely for the larger Antlia II, nominally unbound
material can be recognised thanks to its somewhat hotter kinematics and
line-of-sight velocity gradient. Contrary to other formation scenarios, Crater
II and Antlia II may well have experienced very little mass loss, as in fact
hinted by their observed metallicity. If indeed a satellite of NGC1052, tidal
evolution of a low-concentration halo may similarly have led to the formation
of NGC1052-DF2.Comment: MNRAS Letters submitted, comments welcom
Deadly dark matter cusps vs faint and extended star clusters: Eridanus II and Andromeda XXV
The recent detection of two faint and extended star clusters in the central
regions of two Local Group dwarf galaxies, Eridanus II and Andromeda XXV,
raises the question of whether clusters with such low densities can survive the
tidal field of cold dark matter haloes with central density cusps. Using both
analytic arguments and a suite of collisionless N-body simulations, I show that
these clusters are extremely fragile and quickly disrupted in the presence of
central cusps with . Furthermore, the
scenario in which the clusters where originally more massive and sank to the
center of the halo requires extreme fine tuning and does not naturally
reproduce the observed systems. In turn, these clusters are long lived in cored
haloes, whose central regions are safe shelters for . The
only viable scenario for hosts that have preserved their primoridal cusp to the
present time is that the clusters formed at rest at the bottom of the
potential, which is easily tested by measurement of the clusters proper
velocity within the host. This offers means to readily probe the central
density profile of two dwarf galaxies as faint as
and , in which stellar feedback is unlikely to be
effective.Comment: accepted versio
On feathers, bifurcations and shells: the dynamics of tidal streams across the mass scale
I present an organic description of the regimes of collisionless tidal
streams and define the orderings between the physical quantities that shape
their morphology. Three fundamental dichotomies are identified in the form of
dimensionless inequalities. These govern i) the speed of the stream's growth,
ii) its internal coherence, iii) its thickness or opening angles. The
mechanisms that regulate such main properties are analysed. The slope of the
host's density profile influences the speed of the stream's growth, in both
length and width, as steeper profiles enhance differential streaming. Internal
coherence is the requirement for the appearance of substructure in tidal
debris, and I concentrate on the `feathering' typical of GC streams.
Overdensities are associated with minima in the relative streaming velocity of
the stream members. For streams with high circularity, these are caused by the
epicyclic oscillations of stars; however, for highly non-circular progenitor's
orbits, substructure is caused by the oscillating differences in energy and
actions with which material is shed at different orbital phases of the
progenitor. This modulation results in different streaming speeds: the
streakline of material shed between two successive apocentric passages is
folded along its length, pulled at its centre by the faster streaming of
particles released near pericenter, which are therefore more widely scattered.
When the stream is coherent enough, this mechanism is potentially capable of
generating a bimodal profile in the density distributions of the longer wraps
of more massive progenitors, which I dub `bifurcations'. The conditions for
internal coherence are explored and I comment on the cases of Palomar 5,
Willman 1, the Anticenter and Sagittarius' streams. Analytical methods are
accompanied by numerical experiments, performed using a purposely built
generative model, also presented here.Comment: 18 pages, submitted to MNRA
The virial mass distribution of ultra-diffuse galaxies in clusters and groups
We use the observed abundances of ultra-diffuse galaxies (UDGs) in clusters
and groups and \Lambda CDM subhalo mass functions to put constraints on the
distribution {of present-day halo masses of satellite} UDGs. If all of the most
massive subhaloes in the cluster host a UDG, UDGs occupy all subhaloes with
\log M_{sub}/M_\odot\gtrsim11. For a model in which the efficiency of UDG
formation is higher around some characteristic halo mass, higher fractions of
massive UDGs require larger spreads in the UDG mass distribution. In a cluster
with a virial mass of 10^{15}M_\odot, the 90% upper limit for the fraction of
UDGs with \log M_{sub}/M_\odot>12 is 7%, occupying 70% of all cluster subhaloes
above the same mass. To reproduce the observed abundances, however, the mass
distribution of satellite UDGs has to be broad, with >30% having \log
M_{sub}/M_\odot<10.9. This strongly supports that UDGs are part of a continuous
distribution in which a majority are hosted by low mass haloes. The abundance
of satellite UDGs may fall short of the linear relation with the cluster/group
mass M_{host} in low-mass hosts, \log M_{host}/M_\odot\sim 12. Characterising
these deviations -- or the lack thereof -- will allow for stringent constraints
on the UDG virial mass distribution.Comment: matches accepted versio
Contributions to the accreted stellar halo: an atlas of stellar deposition
The accreted component of stellar halos is composed of the contributions of
several satellites, falling onto their host with their different masses, at
different times, on different orbits. This work uses a suite of idealised,
collisionless N-body simulations of minor mergers and a particle tagging
technique to understand how these different ingredients shape each contribution
to the accreted halo, in both density and kinematics. I find that more massive
satellites deposit their stars deeper into the gravitational potential of the
host, with a clear segregation enforced by dynamical friction. Earlier
accretion events contribute more to the inner regions of the halo; more
concentrated subhaloes sink deeper through increased dynamical friction. The
orbital circularity of the progenitor at infall is only important for low-mass
satellites: dynamical friction efficiently radialises the most massive minor
mergers erasing the imprint of the infall orbit for satellite-to-host virial
mass ratios . The kinematics of the stars contributed by each
satellite is also ordered with satellite mass: low-mass satellites contribute
fast-moving populations, in both ordered rotation and radial velocity
dispersion. In turn, contributions by massive satellites have lower velocity
dispersion and lose their angular momentum to dynamical friction, resulting in
a strong radial anisotropy.Comment: 15 pages, accepted version, discussion extende
The core size of the Fornax dwarf Spheroidal
We exploit the detection of three distinct stellar subpopulations in the red
giant branch of the Fornax dwarf Spheroidal to probe its density distribution.
This allows us to resolve directly the evolution with radius of the dark matter
mass profile. We find that a cored dark matter halo provides a perfect fit to
the data, being consistent with all three stellar populations well within
1-sigma, and for the first time we are able to put constraints on the core size
of such a halo. With respect to previous work, we do not strengthen the
statistical exclusion of a dark matter cusp in Fornax, but we find that
Navarro-Frenk-White haloes would be required to have unrealistically large
scale radii in order to be compatible with the data, hence low values of the
concentration parameter. We are then forced to conclude that the Fornax dwarf
Spheroidal sits within a dark matter halo having a constant density core, with
a core size of between 0.6 and 1.8 kpc.Comment: MNRAS Letters, submitte
Galaxies with Shells in the Illustris Simulation: Metallicity Signatures
Stellar shells are low surface brightness arcs of overdense stellar regions,
extending to large galactocentric distances. In a companion study, we
identified 39 shell galaxies in a sample of 220 massive ellipticals
() from the
Illustris cosmological simulation. We used stellar history catalogs to trace
the history of each individual star particle inside the shell substructures,
and we found that shells in high-mass galaxies form through mergers with
massive satellites (stellar mass ratios ).
Using the same sample of shell galaxies, the current study extends the stellar
history catalogs in order to investigate the metallicity of stellar shells
around massive galaxies. Our results indicate that outer shells are often times
more metal-rich than the surrounding stellar material in a galaxy's halo. For a
galaxy with two different satellites forming shells, we find a
significant difference in the metallicity of the shells produced by each
progenitor. We also find that shell galaxies have higher mass-weighted
logarithmic metallicities ([Z/H]) at -
compared to galaxies without shells. Our results indicate that observations
comparing the metallicities of stars in tidal features, such as shells, to the
average metallicities in the stellar halo can provide information about the
assembly histories of galaxies.Comment: 15 pages, 5 figures. Article published in a special issue of MDPI
Galaxies after the conference "On the Origin (and Evolution) of Baryonic
Galaxy Halos", Galapagos Islands, 201
Formation and Incidence of Shell Galaxies in the Illustris Simulation
Shells are low surface brightness tidal debris that appear as interleaved
caustics with large opening angles, often situated on both sides of the galaxy
center. In this paper, we study the incidence and formation processes of shell
galaxies in the cosmological gravity+hydrodynamics Illustris simulation. We
identify shells at redshift z=0 using stellar surface density maps, and we use
stellar history catalogs to trace the birth, trajectory and progenitors of each
individual star particle contributing to the tidal feature. Out of a sample of
the 220 most massive galaxies in Illustris
(),
of the galaxies exhibit shells. This fraction increases with
increasing mass cut: higher mass galaxies are more likely to have stellar
shells. Furthermore, the fraction of massive galaxies that exhibit shells
decreases with increasing redshift. We find that shell galaxies observed at
redshift form preferentially through relatively major mergers
(1:10 in stellar mass ratio). Progenitors are accreted on low angular
momentum orbits, in a preferred time-window between 4 and 8 Gyrs ago. Our
study indicates that, due to dynamical friction, more massive satellites are
allowed to probe a wider range of impact parameters at accretion time, while
small companions need almost purely radial infall trajectories in order to
produce shells. We also find a number of special cases, as a consequence of the
additional complexity introduced by the cosmological setting. These include
galaxies with multiple shell-forming progenitors, satellite-of-satellites also
forming shells, or satellites that fail to produce shells due to multiple major
mergers happening in quick succession.Comment: 27 pages, 18 figures. Accepted for publication in MNRAS (new figures
3 and D1 + additional minor changes to match accepted version
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