269 research outputs found
Investigating the physics and environment of lyman limit systems in cosmological simulations
In this work, I investigate the properties of Lyman limit systems (LLSs)
using state-of-the-art zoom-in cosmological galaxy formation simulations with
on the fly radiative transfer, which includes both the cosmic UV background
(UVB) and local stellar sources. I compare the simulation results to
observations of the incidence frequency of LLSs and the HI column density
distribution function over the redshift range and find good agreement.
I explore the connection between LLSs and their host halos and find that LLSs
reside in halos with a wide range of halo masses with a nearly constant
covering fraction within a virial radius. Over the range , I find that
more than half of the LLSs reside in halos with ,
indicating that absorption line studies of LLSs can probe these low-mass
galaxies which H-based star formation models predict to have very little
star formation. I study the physical state of individual LLSs and test a simple
model (Schaye 2001) which encapsulates many of their properties. I confirm that
LLSs have a characteristic absorption length given by the Jeans length and that
they are in photoionization equilibrium at low column densities. Finally, I
investigate the self-shielding of LLSs to the UVB and explore how the
non-sphericity of LLSs affects the photoionization rate at a given . I find that at , LLSs have an optical depth of unity at a
column density of and that this is the column
density which characterizes the onset of self-shielding.This work was supported in part
by the NSF grant AST-0908063, and by the NASA grant NNX-
09AJ54G. The simulations used in this work have been performed
on the Joint Fermilab - KICP Supercomputing Cluster, supported
by grants from Fermilab, Kavli Institute for Cosmological Physics,
and the University of Chicago.This is the final version. It was first published by OUP at http://mnras.oxfordjournals.org/content/451/1/904.abstract?sid=5f7e04bf-6176-4b8f-bc81-ae4f70107d18
A Magellanic origin for the Virgo substructure
Iorio et al. (2018) mapped out the Milky Way halo using a sample of RR Lyrae
stars drawn from a cross-match of Gaia with 2MASS. We investigate the
significant residual in their model which we constrain to lie at Galactocentric
radii and extend over of the
sky. A counterpart of this structure exists in both the Catalina Real Time
Survey and the sample of RR Lyrae variables identified in Pan-STARRS by
Hernitschek et al. (2016), demonstrating that this structure is not caused by
the spatial inhomogeneity of Gaia. The structure is likely the Virgo Stellar
Stream and/or Virgo Over-Density. We show the structure is aligned with the
Magellanic Stream and suggest that it is either debris from a disrupted dwarf
galaxy that was a member of the Vast Polar Structure or that it is SMC debris
from a tidal interaction of the SMC and LMC ago. If the
latter then the sub-structure in Virgo may have a Magellanic origin.Comment: 9 pages, 7 figures, accepted to MNRAS 31/10/201
Cultural Transmission of Work-Welfare Attitudes and the Intergenerational Correlation in Welfare Receipt
This paper considers the potential for the cultural transmission of attitudes toward work, welfare, and individual responsibility to explain the intergenerational correlation in welfare receipt. Specifically, we investigate whether 18-year olds’ views about social benefits and the drivers of social inequality depend on their families’ welfare histories. We begin by incorporating welfare receipt into a theoretical model of the cultural transmission of work-welfare attitudes across generations. Consistent with the predictions of our model, we find that young people’s attitudes towards work and welfare are shaped by socialization within their families. Young people are more likely to oppose generous social benefits and adopt an internal view of social inequality if their mothers support these views, if their mothers were employed while they were growing up, and if their families never received welfare. These results are consistent with —though do not definitively establish— the existence of an intergenerational welfare culture.cultural transmission, attitudes, intergenerational welfare receipt
Stray, swing and scatter: Angular momentum evolution of orbits and streams in aspherical potentials
In aspherical potentials orbital planes continuously evolve. The
gravitational torques impel the angular momentum vector to precess, that is to
slowly stray around the symmetry axis, and nutate, i.e. swing up and down
periodically in the perpendicular direction. This familiar orbital pole motion
- if detected and measured - can reveal the shape of the underlying
gravitational potential, the quantity only crudely gauged in the Galaxy so far.
Here we demonstrate that the debris poles of stellar tidal streams show a very
similar straying and swinging behavior, and give analytic expressions to link
the amplitude and the frequency of the pole evolution to the flattening of the
dark matter distribution. While these results are derived for near-circular
orbits, we show they are also valid for eccentric orbits. Most importantly, we
explain how the differential orbital plane precession leads to the broadening
of the stream and show that streams on polar orbits ought to scatter faster. We
provide expressions for the stream width evolution as a function of the
axisymmetric potential flattening and the angle from the symmetry plane and
prove that our models are in good agreement with streams produced in N-body
simulations. Interestingly, the same intuition applies to streams whose
progenitors are on short or long-axis loops in a triaxial potential. Finally,
we present a compilation of the Galactic cold stream data, and discuss how the
simple picture developed here, along with stream modelling, can be used to
constrain the symmetry axes and flattening of the Milky Way.The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement no. 308024. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science.This is the final version of the article. It first appeared from Oxford University Press via http://dx.doi.org/10.1093/mnras/stw140
Revealing the tidal scars of the Small Magellanic Cloud
Due to their close proximity, the Large and Small Magellanic Clouds (SMC/LMC)
provide natural laboratories for understanding how galaxies form and evolve.
With the goal of determining the structure and dynamical state of the SMC, we
present new spectroscopic data for 3000 SMC red giant branch stars
observed using the AAOmega spectrograph at the Anglo-Australian Telescope. We
complement our data with further spectroscopic measurements from previous
studies that used the same instrumental configuration and proper motions from
the \textit{Gaia} Data Release 2 catalogue. Analysing the photometric and
stellar kinematic data, we find that the SMC centre of mass presents a
conspicuous offset from the velocity centre of its associated \mbox{H\,{\sc
i}} gas, suggesting that the SMC gas is likely to be far from dynamical
equilibrium. Furthermore, we find evidence that the SMC is currently undergoing
tidal disruption by the LMC within 2\,kpc of the centre of the SMC, and
possibly all the way in to the very core. This is evidenced by a net outward
motion of stars from the SMC centre along the direction towards the LMC and
apparent tangential anisotropy at all radii. The latter is expected if the SMC
is undergoing significiant tidal stripping, as we demonstrate using a suite of
-body simulations of the SMC/LMC system disrupting around the Milky Way.
These results suggest that dynamical models for the SMC that assume a steady
state will need to be revisited.Comment: Revised version submitted to MNRAS after referee report, 18 pages, 18
figure
Galaxy halo expansions: a new biorthogonal family of potential-density pairs
Efficient expansions of the gravitational field of (dark) haloes have two
main uses in the modelling of galaxies: first, they provide a compact
representation of numerically-constructed (or real) cosmological haloes,
incorporating the effects of triaxiality, lopsidedness or other distortion.
Secondly, they provide the basis functions for self-consistent field expansion
algorithms used in the evolution of -body systems. We present a new family
of biorthogonal potential-density pairs constructed using the Hankel transform
of the Laguerre polynomials. The lowest-order density basis functions are
double-power-law profiles cusped like at small
radii with asymptotic density fall-off like .
Here, is a parameter satisfying . The family therefore
spans the range of inner density cusps found in numerical simulations, but has
much shallower -- and hence more realistic -- outer slopes than the
corresponding members of the only previously-known family deduced by Zhao
(1996) and exemplified by Hernquist & Ostriker (1992). When , the
lowest-order density profile has an inner density cusp of
and an outer density slope of , similar to the famous
Navarro, Frenk & White (1997) model. For this reason, we demonstrate that our
new expansion provides a more accurate representation of flattened NFW haloes
than the competing Hernquist-Ostriker expansion. We utilize our new expansion
by analysing a suite of numerically-constructed haloes and providing the
distributions of the expansion coefficients.JLS and EJL acknowledge the support of the STFC
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