3,492 research outputs found
A Sunyaev-Zel'dovich Effect Survey for High Redshift Clusters
Interferometric observations of the Sunyaev-Zel'dovich Effect (SZE) toward
clusters of galaxies provide sensitive cosmological probes. We present results
from 1 cm observations (at BIMA and OVRO) of a large, intermediate redshift
cluster sample. In addition, we describe a proposed, higher sensitivity array
which will enable us to survey large portions of the sky. Simulated
observations indicate that we will be able to survey one square degree of sky
per month to sufficient depth that we will detect all galaxy clusters more
massive than 2x10^{14} h^{-1}_{50}M_\odot, regardless of their redshift. We
describe the cluster yield and resulting cosmological constraints from such a
survey.Comment: 7 pages, 6 figures, latex, contribution to VLT Opening Symposiu
Imaging the Sunyaev-Zel'dovich Effect
We report on results of interferometric imaging of the Sunyaev-Zel'dovich
Effect (SZE) with the OVRO and BIMA mm-arrays. Using low-noise cm-wave
receivers on the arrays, we have obtained high quality images for 27 distant
galaxy clusters. We review the use of the SZE as a cosmological tool. Gas mass
fractions derived from the SZE data are given for 18 of the clusters, as well
as the implied constraint on the matter density of the universe, . We
find . A best guess for the matter
density obtained by assuming a reasonable value for the Hubble constant and
also by attempting to account for the baryons contained in the galaxies as well
as those lost during the cluster formation process gives .
We also give preliminary results for the Hubble constant. Lastly, the power for
investigating the high redshift universe with a non-targeted high sensitivity
SZE survey is discussed and an interferometric survey is proposed.Comment: 14 pages, 7 figures, latex, contribution to Nobel Symposium "Particle
Physics and the Universe" to appear in Physica Scripta and World Scientific,
eds L. Bergstrom, P. Carlson and C. Fransso
Substructure and halo density profiles in a Warm Dark Matter Cosmology
We performed a series of high-resolution simulations designed to study the
substructure of Milky Way-size galactic halos (host halos) and the density
profiles of halos in a warm dark matter (WDM) scenario with a non-vanishing
cosmological constant. The virial masses of the host halos range from 3.5 x
10^12 to 1.7 x 10^12 solar masses and they have more than 10^5 particles each.
A key feature of the WDM power spectrum is the free-streaming length R_f which
fixes an additional parameter for the model of structure formation. We analyze
the substructure of host halos using three R_f values: 0.2, 0.1, and 0.05 Mpc
and compare results to the predictions of the cold dark matter (CDM) model. We
find that guest halos (satellites) do form in the WDM scenario but are more
easily destroyed by dynamical friction and tidal disruption than their
counterparts in a CDM model. The small number of guest halos that we find
within the virial radii of host halos at z = 0 in the WDM models is the result
of a less efficient halo accretion and a higher satellite destruction rate.
Under the assumption that each guest halo hosts a luminous galaxy, we find that
the observed circular velocity function of satellites around the Milky Way and
Andromeda is well described by the R_f = 0.1 Mpc WDM model. In the R_f =
0.1-0.2 Mpc models, the surviving subhalos at z=0 have an average concentration
parameter c_1/5 which is approximately twice smaller than that of the
corresponding CDM subhalos. This difference, very likely, produces the higher
satellite destruction rate found in the WDM models. The density profile of host
halos is well described by the NFW fit whereas guest halos show a wide variety
of density profiles (abridged).Comment: Uses emulateapj.sty: 10 pages, 4 figures, ApJ accepted. Some changes
have been introduced as suggested by the referee: (1) the description of the
numerical simulations was sligthly modified to make it clearer, (2) the
ellipticities of the host halos are now measured, and (3) the discussion
section was divided in two subsections and enlarge
From Random to Regular: Variation in the Patterning of Retinal Mosaics
The various types of retinal neurons are each positioned at their respective
depths within the retina where they are believed to be assembled as orderly
mosaics, in which like-type neurons minimize proximity to one another. Two
common statistical analyses for assessing the spatial properties of retinal
mosaics include the nearest neighbor analysis, from which an index of their
"regularity" is commonly calculated, and the density recovery profile derived
from auto-correlation analysis, revealing the presence of an exclusion zone
indicative of anti-clustering. While each of the spatial statistics derived
from these analyses, the regularity index and the effective radius, can be
useful in characterizing such properties of orderly retinal mosaics, they are
rarely sufficient for conveying the natural variation in the self-spacing
behavior of different types of retinal neurons and the extent to which that
behavior generates uniform intercellular spacing across the mosaic. We consider
the strengths and limitations of different spatial statistical analyses for
assessing the patterning in retinal mosaics, highlighting a number of
misconceptions and their frequent misuse. Rather than being diagnostic criteria
for determining simply whether a population is "regular", they should be
treated as descriptive statistics that convey variation in the factors that
influence neuronal positioning. We subsequently apply multiple spatial
statistics to the analysis of eight different mosaics in the mouse retina,
demonstrating conspicuous variability in the degree of patterning present, from
essentially random to notably regular. This variability in patterning has both
a developmental as well as a functional significance, reflecting the rules
governing the positioning of different types of neurons as the architecture of
the retina is assembled (abstract truncated).Comment: 11 Figure
Target detection against narrow band noise backgrounds
AbstractWe studied the detectability of narrow band random noise targets embedded in narrow band random noise backgrounds as a function of differences in center frequency, spatial frequency bandwidth and orientation bandwidth between target and the immediately adjacent background. Unlike most target detection experiments the targets were not added to the background; they replaced the underlying background texture. Simulations showed that target detection probabilities could be accounted for by a simple transformation on the summed outputs of a two layer filter model similar to the complex channels model proposed by Graham, Beck and Sutter (Graham, N., Beck, J., & Sutter, A. (1992). Vision Research, 32, 719â743). Subsequently, the model was tested on the detection of camouflaged vehicle targets with encouraging results
Structure and Subhalo Population of Halos in a Self-Interacting Dark Matter Cosmology
We study the structure of Milky Way (MW)- and cluster-sized halos in a Lambda
Cold Dark Matter (CDM) cosmology with self-interacting (SI) dark particles. The
cross section per unit of particle mass has the form sigma =
sig_0(1/v_100)^alpha, where sig_0 is a constant in units of cm^2/gr and v_100
is the relative velocity in units of 100 km/s. Different values for sigma with
alpha= 0 or 1 were used. For small values of sigma = const. (sig_0<0.5), the
core density of the halos at z=0 is typically higher at a given mass for lower
values of sig_0 or, at a given sig_0, for lower masses. For values of sig_0 as
high as 3.0, the halos may undergo the gravothermal catastrophe before z=0.
When alpha = 1, the core density of cluster- and MW-sized halos is similar.
Using sigma = 0.5-1.0x(1/v_100), our predictions agree with the central
densities and the core scaling laws of halos both inferred from the
observations of dwarf and LSB galaxies and clusters of galaxies. The cumulative
Vmax-functions of subhalos in MW-sized halos with (sig_0,alpha) = (0.1,0.0),
(0.5,0.0) and (0.5,1.0) agree roughly with observations (luminous satellites)
for Vmax > 30 km/s, while at Vmax = 20 km/s the functions are a factor 5-8
higher, similar to the CDM predictions. The halos with SI have slightly more
specific angular momentum at a given mass shell and are rounder than their CDM
counterparts. We conclude that the introduction of SI particles with sigma
\propto 1/v_100 may remedy the cuspy core problem of the CDM cosmogony, while
the subhalo population number remains similar to that of the CDM halos.Comment: To appear in ApJ, December 20, 2002. We added plots showing the
evolution of the heat capacity profile for halos in the core expansion and
gravothermal catastrophe phases. Minor changes in the text were introduce
Words are Malleable: Computing Semantic Shifts in Political and Media Discourse
Recently, researchers started to pay attention to the detection of temporal
shifts in the meaning of words. However, most (if not all) of these approaches
restricted their efforts to uncovering change over time, thus neglecting other
valuable dimensions such as social or political variability. We propose an
approach for detecting semantic shifts between different viewpoints--broadly
defined as a set of texts that share a specific metadata feature, which can be
a time-period, but also a social entity such as a political party. For each
viewpoint, we learn a semantic space in which each word is represented as a low
dimensional neural embedded vector. The challenge is to compare the meaning of
a word in one space to its meaning in another space and measure the size of the
semantic shifts. We compare the effectiveness of a measure based on optimal
transformations between the two spaces with a measure based on the similarity
of the neighbors of the word in the respective spaces. Our experiments
demonstrate that the combination of these two performs best. We show that the
semantic shifts not only occur over time, but also along different viewpoints
in a short period of time. For evaluation, we demonstrate how this approach
captures meaningful semantic shifts and can help improve other tasks such as
the contrastive viewpoint summarization and ideology detection (measured as
classification accuracy) in political texts. We also show that the two laws of
semantic change which were empirically shown to hold for temporal shifts also
hold for shifts across viewpoints. These laws state that frequent words are
less likely to shift meaning while words with many senses are more likely to do
so.Comment: In Proceedings of the 26th ACM International on Conference on
Information and Knowledge Management (CIKM2017
Turbulent dissipation in the ISM: the coexistence of forced and decaying regimes and implications for galaxy formation and evolution
We discuss the dissipation of turbulent kinetic energy Ek in the global ISM
by means of 2-D, MHD, non-isothermal simulations in the presence of model
radiative heating and cooling. We argue that dissipation in 2D is
representative of that in three dimensions as long as it is dominated by shocks
rather than by a turbulent cascade. Energy is injected at a few isolated sites
in space, over relatively small scales, and over short time periods. This leads
to the coexistence of forced and decaying regimes in the same flow. We find
that the ISM-like flow dissipates its turbulent energy rapidly. In simulations
with forcing, the input parameters are the radius l_f of the forcing region,
the total kinetic energy e_k each source deposits into the flow, and the rate
of formation of those regions, sfr_OB. The global dissipation time t_d depends
mainly on l_f. In terms of measurable properties of the ISM, t_d >= Sigma_g
u_rms^2/(e_k sfr_OB), where Sigma_g is the average gas surface density and
u_rms is the rms velocity dispersion. For the solar neighborhood, t_d >=
1.5x10^7 yr. The global dissipation time is consistently smaller than the
crossing time of the largest energy-containing scales. In decaying simulations,
Ek decreases with time as t^-n, where n~0.8-0.9. This suggests a decay with
distance d as Ek\propto d^{-2n/(2-n)} in the mixed forced+decaying case. If
applicable to the vertical direction, our results support models of galaxy
evolution in which stellar energy injection provides significant support for
the gas disk thickness, but not models of galaxy formation in which this energy
injection is supposed to reheat an intra-halo medium at distances of up to
10-20 times the optical galaxy size, as the dissipation occurs on distances
comparable to the disk height.Comment: 23 pages, including figures. To appear in ApJ. Abstract abridge
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