1,425 research outputs found
Spatially valid proprioceptive cues improve the detection of a visual stimulus
Vision and proprioception are the main sensory modalities that convey hand location and direction of movement. Fusion of these sensory signals into a single robust percept is now well documented. However, it is not known whether these modalities also interact in the spatial allocation of attention, which has been demonstrated for other modality pairings. The aim of this study was to test whether proprioceptive signals can spatially cue a visual target to improve its detection. Participants were instructed to use a planar manipulandum in a forward reaching action and determine during this movement whether a near-threshold visual target appeared at either of two lateral positions. The target presentation was followed by a masking stimulus, which made its possible location unambiguous, but not its presence. Proprioceptive cues were given by applying a brief lateral force to the participant’s arm, either in the same direction (validly cued) or in the opposite direction (invalidly cued) to the on-screen location of the mask. The d′ detection rate of the target increased when the direction of proprioceptive stimulus was compatible with the location of the visual target compared to when it was incompatible. These results suggest that proprioception influences the allocation of attention in visual spac
The Dynamical Status of the Cluster of Galaxies 1E0657-56
We present the results of a new spectroscopic and photometric survey of the
hot X-ray cluster 1E0657-56, at z=0.296. We determine the presence of a low
velocity dispersion subcluster, which is offset from the main cluster position
by 0.7 Mpc and about 600 km/s. We determine the virial masses and total
luminosities of the cluster and its subcluster, and solve for the two-body
dynamical model. With additional constraints from the results of the analysis
of the cluster X-ray emission by Markevitch et al. (2001), we find that the
subcluster passed through the cluster centre about 0.15 Gyr ago. Taken at face
value the mass of the subcluster is typical of a loose group. It is however
difficult to establish the pre-merger mass of the colliding system. We provide
tentative evidence that the subcluster is in fact the remnant core of a
moderately massive cluster, stripped by the collision with 1E0657-56. The main
cluster dynamics does not seem to have suffered from this collision. On the
contrary, the cluster X-ray properties seem to have been significantly
affected. We also discuss the effect of the subcluster collision in relation to
starburst events and the cluster radio halo.Comment: Accepted for publication on A&
Distances to Galactic high-velocity clouds. Complex C
We report the first determination of a distance bracket for the high-velocity
cloud (HVC) complex C. Combined with previous measurements showing that this
cloud has a metallicity of 0.15 times solar, these results provide ample
evidence that complex C traces the continuing accretion of intergalactic gas
falling onto the Milky Way. Accounting for both neutral and ionized hydrogen as
well as He, the distance bracket implies a mass of 3-14x10^6 M_sun, and the
complex represents a mass inflow of 0.1-0.25 M_sun/yr. We base our distance
bracket on the detection of CaII absorption in the spectrum of the blue
horizontal branch star SDSS J120404.78+623345.6, in combination with a
significant non-detection toward the BHB star BS 16034-0114. These results set
a strong distance bracket of 3.7-11.2 kpc on the distance to complex C. A more
weakly supported lower limit of 6.7 kpc may be derived from the spectrum of the
BHB star BS 16079-0017.Comment: Accepted for publication in ApJ Letter
The complex structure of Abell 2345: a galaxy cluster with non-symmetric radio relics
We aim to obtain new insights into the internal dynamics of the cluster Abell
2345. This cluster exhibits two non-symmetric radio relics well studied through
recent, deep radio data. Our analysis is based on redshift data for 125
galaxies acquired at the Telescopio Nazionale Galileo and on new photometric
data acquired at the Isaac Newton Telescope. We also use ROSAT/HRI archival
X-ray data. We combine galaxy velocities and positions to select 98 cluster
galaxies and analyze the internal dynamics of the cluster. We estimate a mean
redshift =0.1789 and a LOS velocity dispersion \sigma ~ 1070 km/s. The
two-dimensional galaxy distribution reveals the presence of three significant
peaks within a region of ~ 1 Mpc (the E, NW, and SW peaks). The spectroscopic
catalog confirms the presence of these three clumps. The total mass of the
cluster is very uncertain: M~ 2 10^15 solar masses. The E clump well coincides
with the main mass peak as recovered from the weak gravitational lensing
analysis and is off-set to the east from the BCG by ~ 1.3 arcmin. The ROSAT
X-ray data also show a very complex structure, mainly elongated in the E-W
direction, with two (likely three) peaks in the surface brightness
distribution, which, however, are off-set from the position of the peaks in the
galaxy density. The observed phenomenology agrees with the hypothesis that we
are looking at a complex cluster merger occurring along two directions: a major
merger along the ~ E-W direction (having a component along the LOS) and a minor
merger in the western cluster regions along the ~ N-S direction, roughly
parallel to the plane of the sky.Comment: 27 pages, 11 figures and 3 tables. Accepted for publication on
Astronomy and Astrophysic
Kinematics of Metal-Poor Stars in the Galaxy. III. Formation of the Stellar Halo and Thick Disk as Revealed from a Large Sample of Non-Kinematically Selected Stars
(Abbreviated) We present a detailed analysis of the space motions of 1203
solar-neighborhood stars with metal abundances [Fe/H] <= -0.6, on the basis of
a recently revised and supplemented catalog of metal-poor stars selected
without kinematic bias (Beers et al. 2000). This sample, having available
proper motions, radial velocities, and distance estimates for stars with a wide
range of metal abundances, is by far the largest such catalog to be assembled
to date. Unlike essentially all previous kinematically selected catalogs, the
metal-poor stars in our sample exhibit a diverse distribution of orbital
eccentricities, e, with no apparent correlation between [Fe/H] and e. This
demonstrates, clearly and convincingly, that the evidence offered by Eggen,
Lynden-Bell, and Sandage (1962) for a rapid collapse of the Galaxy, an apparent
correlation between the orbital eccentricity of halo stars with metallicity, is
basically the result of their proper-motion selection bias. However, even in
our non-kinematically selected sample, we have identified a small concentration
of high-e stars at [Fe/H] = -1.7, which may originate, in part, from infalling
gas during the early formation of the Galaxy. The implications of our results
for the formation of the Galaxy are also discussed, in particular in the
context of the currently favored CDM theory of hierarchical galaxy formation.Comment: 51 pages, including 17 figures, to appear in AJ (June 2000), full
paper with all figures embedded available at
http://pluto.mtk.nao.ac.jp/people/chiba/preprint/halo5
The Origin of the Bifurcation in the Sagittarius Stream
The latest Sloan Digital Sky Survey data reveal a prominent bifurcation in
the distribution of debris of the Sagittarius dwarf spheroidal (Sgr) beginning
at a right ascension of roughly 190 degrees. Two branches of the stream (A and
B) persist at roughly the same heliocentric distance over at least 50 degrees
of arc. There is also evidence for a more distant structure (C) well behind the
A branch. This paper provides the first explanation for the bifurcation. It is
caused by the projection of the young leading (A) and old trailing (B) tidal
arms of the Sgr, whilst the old leading arm (C) lies well behind A. This
explanation is only possible if the halo is close to spherical, as the angular
difference between the branches is a measure of the precession of the orbital
plane.Comment: ApJ, in pres
A dynamical and kinematical model of the Galactic stellar halo and possible implications for galaxy formation scenarios
We re-analyse the kinematics of the system of blue horizontal branch field
(BHBF) stars in the Galactic halo (in particular the outer halo), fitting the
kinematics with the model of radial and tangential velocity dispersions in the
halo as a function of galactocentric distance r proposed by Sommer-Larsen,
Flynn & Christensen (1994), using a much larger sample (almost 700) of BHBF
stars. The basic result is that the character of the stellar halo velocity
ellipsoid changes markedly from radial anisotropy at the sun to tangential
anisotropy in the outer parts of the Galactic halo (r greater than approx 20
kpc). Specifically, the radial component of the stellar halo's velocity
ellipsoid decreases fairly rapidly beyond the solar circle, from approx 140 +/-
10 km/s at the sun, to an asymptotic value of 89 +/- 19 km/s at large r. The
rapid decrease in the radial velocity dispersion is matched by an increase in
the tangential velocity dispersion, with increasing r.
Our results may indicate that the Galaxy formed hierarchically (partly or
fully) through merging of smaller subsystems - the 'bottom-up' galaxy formation
scenario, which for quite a while has been favoured by most theorists and
recently also has been given some observational credibility by HST observations
of a potential group of small galaxies, at high redshift, possibly in the
process of merging to a larger galaxy (Pascarelle et al 1996).Comment: Latex, 16 pages. 2 postscript figures. Submitted to the Astrophysical
Journal. also available at http://astro.utu.fi/~cflynn/outerhalo.htm
Internal dynamics of the galaxy cluster Abell 545
Diffuse radio emission in galaxy clusters, and their connection with cluster
mergers, are still debated. We seek to explore the internal dynamics of the
radio halo cluster Abell 545. This cluster is also peculiar for hosting in its
center a very bright, red, diffuse intracluster light due to an old, stellar
population, so bright to be named as "star pile". Our analysis is based on
redshift data for 110 galaxies. We identify 95 cluster members and analyze the
cluster internal dynamics by combining galaxy velocities and positions. We also
use both photometric and X-ray data. We estimate the cluster redshift,
z=0.1580, a velocity dispersion of 1200 km/s, and ICM temperature kT_X~8 keV.
Our optical and X-ray analyses detect substructures. Optical data reveal three
main galaxy clumps (center, NNW, and NE), and possibly a fourth clump at South.
There is not a dominant galaxy and the four brightest galaxies avoid the
cluster core (>~0.4h distant from the cluster center) and are >~1500 km/s far
from the mean cluster velocity. The analysis of the X-ray surface brightness
distribution provides us evidence of a disturbed dynamical phase. Located in
the star pile region there is the brightest galaxies of the cluster core (CBCG)
and a very compact elliptical galaxy. We show that the star pile has a similar
redshift to that of the CBCG. Both the star pile and the CBCG are at rest in
the cluster rest frame. The emerging picture of Abell 545 is that of a massive,
M(R<1.6 h_70^-1 Mpc)=1.1-1.8x10^15 h_70^-1 Msun, very complex cluster with
merging occurring along two directions. A545 gives another proof in the favor
of the connection between cluster merger and extended, diffuse radio emission.
The star pile, likely due to the process of a brightest galaxy forming in the
cluster core. A545 represents a textbook cluster where to study the
simultaneous formation of a galaxy system and its brightest galaxy.Comment: 16 pages, 11 figures and 2 tables. Accepted in A&
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