6,086 research outputs found
The status of music education in the public junior high schools of Massachusetts as of the year 1945-1955
Thesis (Ed.M.)--Boston Universit
Extending the halo mass resolution of -body simulations
We present a scheme to extend the halo mass resolution of N-body simulations
of the hierarchical clustering of dark matter. The method uses the density
field of the simulation to predict the number of sub-resolution dark matter
haloes expected in different regions. The technique requires as input the
abundance of haloes of a given mass and their average clustering, as expressed
through the linear and higher order bias factors. These quantities can be
computed analytically or, more accurately, derived from a higher resolution
simulation as done here. Our method can recover the abundance and clustering in
real- and redshift-space of haloes with mass below at to better than 10%. We demonstrate the
technique by applying it to an ensemble of 50 low resolution, large-volume
-body simulations to compute the correlation function and covariance matrix
of luminous red galaxies (LRGs). The limited resolution of the original
simulations results in them resolving just two thirds of the LRG population. We
extend the resolution of the simulations by a factor of 30 in halo mass in
order to recover all LRGs. With existing simulations it is possible to generate
a halo catalogue equivalent to that which would be obtained from a -body
simulation using more than 20 trillion particles; a direct simulation of this
size is likely to remain unachievable for many years. Using our method it is
now feasible to build the large numbers of high-resolution large volume mock
galaxy catalogues required to compute the covariance matrices necessary to
analyse upcoming galaxy surveys designed to probe dark energy.Comment: 11 pages, 7 Figure
Mycological Examination of Dust from Mouldy Hay Associated with Farmer's Lung Disease
RESP-473
The effect of gravitational-wave recoil on the demography of massive black holes
The coalescence of massive black hole (MBH) binaries following galaxy mergers
is one of the main sources of low-frequency gravitational radiation. A
higher-order relativistic phenomenon, the recoil as a result of the non-zero
net linear momentum carried away by gravitational waves, may have interesting
consequences for the demography of MBHs at the centers of galaxies. We study
the dynamics of recoiling MBHs and its observational consequences. The
``gravitational rocket'' may: i) deplete MBHs from late-type spirals, dwarf
galaxies, and stellar clusters; ii) produce off-nuclear quasars, including
unusual radio morphologies during the recoil of a radio-loud source; and iii)
give rise to a population of interstellar and intergalactic MBHs.Comment: emulateapj, 5 pages, 2 figures, to appear in the ApJ Letter
Cosmic Ray Production of Lithium-6 by Structure Formation Shocks in the Early Milky Way: A Fossil Record of Dissipative Processes during Galaxy Formation
While the abundances of Be and B observed in metal-poor halo stars are well
explained as resulting from spallation of CNO-enriched cosmic rays (CRs)
accelerated by supernova shocks, accounting for the observed Li in such
stars with supernova CRs is more problematic. Here we propose that
gravitational shocks induced by infalling and merging sub-Galactic clumps
during hierarchical structure formation of the Galaxy should dissipate enough
energy at early epochs, and CRs accelerated by such shocks can provide a
natural explanation of the observed Li. In clear constrast to supernovae,
structure formation shocks do not eject freshly synthesized CNO nor Fe, so that
the only effective production channel at low metallicity is
fusion, capable of generating sufficient Li with no accompanying Be or B
and no direct correspondence with Fe. Correlations between the Li abundance
and the kinematic properties of the halo stars may also be expected in this
scenario. Further, more extensive observations of Li in metal-poor halo
stars, e.g. by the Subaru HDS or VLT/UVES, may offer us an invaluable fossil
record of dissipative dynamical processes which occurred during the formation
of our Galaxy.Comment: Ap.J. in press; 6 pages, 1 figur
Epidemiological Study Designs: Traditional and Novel Approaches to Advance Life Course Health Development Research
Non-linear power spectra of dark and luminous matter in halo model of structure formation
The late stages of large-scale structure evolution are treated
semi-analytically within the framework of modified halo model. We suggest
simple yet accurate approximation for relating the non-linear amplitude to
linear one for spherical density perturbation. For halo concentration
parameter, , a new computation technique is proposed, which eliminates the
need of interim evaluation of the . Validity of the technique is
proved for CDM and WDM cosmologies. Also, the parameters for
Sheth-Tormen mass function are estimated. The modified and extended halo model
is applied for determination of non-linear power spectrum of dark matter, as
well as for galaxy power spectrum estimation. The semi-analytical techniques
for dark matter power spectrum are verified by comparison with data from
numerical simulations. Also, the predictions for the galaxy power spectra are
confronted with 'observed' data from PSCz and SDSS galaxy catalogs, good
accordance is found.Comment: 18 pages, 8 figures; major changes from the previous version;
accepted for publivation in Phys. Rev.
Flavor ordering of elliptic flows at high transverse momentum
Based on the quark coalescence model for the parton-to-hadron phase
transition in ultra-relativistic heavy ion collisions, we relate the elliptic
flow () of high \pt hadrons to that of high \pt quarks. For high \pt
hadrons produced from an isospin symmetric and quark-antiquark symmetric
partonic matter, magnitudes of their elliptic flows follow a flavor ordering as
if strange quarks have a
smaller elliptic flow than light quarks. The elliptic flows of high \pt
hadrons further follow a simple quark counting rule if strange quarks and light
quarks have same high \pt spectrum and coalescence probability.Comment: 4 pages, 1 figure, revte
Leading Order Calculation of Shear Viscosity in Hot Quantum Electrodynamics from Diagrammatic Methods
We compute the shear viscosity at leading order in hot Quantum
Electrodynamics. Starting from the Kubo relation for shear viscosity, we use
diagrammatic methods to write down the appropriate integral equations for
bosonic and fermionic effective vertices. We also show how Ward identities can
be used to put constraints on these integral equations. One of our main results
is an equation relating the kernels of the integral equations with functional
derivatives of the full self-energy; it is similar to what is obtained with
two-particle-irreducible effective action methods. However, since we use Ward
identities as our starting point, gauge invariance is preserved. Using these
constraints obtained from Ward identities and also power counting arguments, we
select the necessary diagrams that must be resummed at leading order. This
includes all non-collinear (corresponding to 2 to 2 scatterings) and collinear
(corresponding to 1+N to 2+N collinear scatterings) rungs responsible for the
Landau-Pomeranchuk-Migdal effect. We also show the equivalence between our
integral equations obtained from quantum field theory and the linearized
Boltzmann equations of Arnold, Moore and Yaffe obtained using effective kinetic
theory.Comment: 45 pages, 22 figures (note that figures 7 and 14 are downgraded in
resolution to keep this submission under 1000kb, zoom to see them correctly
- …