1,605 research outputs found
Obstacles to Success of Students with Autism Spectrum Disorder in General Education Settings
The purpose of this study was to survey teacher opinions of 14 potential obstacles to teaching in general education classes attended by students with autism spectrum disorder (ASD). The anonymous participant responses were received from 16 elementary school teachers, 60 middle school teachers, and 131 high school teachers. Participants completed a questionnaire in which they rated 14 items. Rating data were uploaded to STATA data analysis software. The Kruskal-Wallis (K-W) statistic was used to analyze and interpret the data. Results identified items that significantly discriminated among teachers of the three grade levels and show a difference in the perceptions of teachers at different grade levels for some obstacles. Teachers at the elementary school level generally perceived greater obstacles than teachers at the middle school level, who perceived greater obstacles than those at the high school level. The results can be considered by educators and service providers when identifying professional development topics and resources to assist educators and service providers in the provision of instruction to maximize the potential for academic and social success for students with ASD in general education settings
Void Statistics in Large Galaxy Redshift Surveys: Does Halo Occupation of Field Galaxies Depend on Environment?
We use measurements of the projected galaxy correlation function w_p and
galaxy void statistics to test whether the galaxy content of halos of fixed
mass is systematically different in low density environments. We present new
measurements of the void probability function (VPF) and underdensity
probability function (UPF) from Data Release Four of the Sloan Digital Sky
Survey, as well as new measurements of the VPF from the full data release of
the Two-Degree Field Galaxy Redshift Survey. We compare these measurements to
predictions calculated from models of the Halo Occupation Distribution (HOD)
that are constrained to match both w_p and the space density of galaxies. The
standard implementation of the HOD assumes that galaxy occupation depends on
halo mass only, and is independent of local environment. For luminosity-defined
samples, we find that the standard HOD prediction is a good match to the
observations, and the data exclude models in which galaxy formation efficiency
is reduced in low-density environments. More remarkably, we find that the void
statistics of red and blue galaxies (at L ~ 0.4L_*) are perfectly predicted by
standard HOD models matched to the correlation function of these samples,
ruling out "assembly bias" models in which galaxy color is correlated with
large-scale environment at fixed halo mass. We conclude that the luminosity and
color of field galaxies are determined predominantly by the mass of the halo in
which they reside and have little direct dependence on the environment in which
the host halo formed. In broader terms, our results show that the sizes and
emptiness of voids found in the distribution of L > 0.2L_* galaxies are in
excellent agreement with the predictions of a standard cosmological model with
a simple connection between galaxies and dark matter halos. (abridged)Comment: 20 emulateapj pages, 9 figures. submitted to Ap
The DEEP2 Galaxy Redshift Survey: Probing the Evolution of Dark Matter Halos around Isolated Galaxies at z ~ 1
Using the first 25% of DEEP2 Redshift Survey data, we probe the line-of-sight
velocity dispersion profile for isolated galaxies with absolute B-band
magnitude -22<M_B-5log(h)<-21 at z=0.7-1.0, using satellite galaxies as
luminous tracers of the underlying velocity distribution. Measuring the
velocity dispersion beyond a galactocentric radius of ~200 kpc/h (physical)
permits us to determine the total mass, including dark matter, around these
bright galaxies. We find a line-of-sight velocity dispersion (sigma_los) of
162^{+44}_{-30} km/s at ~110 kpc/h, 136^{+26}_{-20} km/s at ~230 kpc/h, and
150^{+55}_{-38} km/s at ~320 kpc/h. Assuming an NFW model for the dark matter
density profile, this corresponds to a mass within r_{200} of
M_200=5.5^{+2.5}_{-2.0} x 10^12 M_Sun/h for our sample of satellite hosts with
mean luminosity ~2.5L*. Roughly $~60% of these host galaxies have early-type
spectra and are red in restframe (U-B) color, consistent with the overall DEEP2
sample in the same luminosity and redshift range. The halo mass determined for
DEEP2 host galaxies is consistent with that measured in the Sloan Digital Sky
Survey for host galaxies within a similar luminosity range relative to M*_B.
This comparison is insensitive to the assumed halo mass profile, and implies an
increase in the dynamical mass-to-light ratio (M_200/L_B) of isolated galaxies
which host satellites by a factor of ~2.5 from z ~ 1 to z ~ 0. Our results are
consistent with scenarios in which galaxies populate dark matter halos
similarly from z ~ 0 to z ~ 1, except for ~1 magnitude of evolution in the
luminosity of all galaxies.Comment: 8 pages, 5 figures, ApJ accepte
The DEEP2 Galaxy Redshift Survey: The Evolution of Void Statistics from z~1 to z~0
We present measurements of the void probability function (VPF) at z~1 using
data from the DEEP2 Redshift Survey and its evolution to z~0 using data from
the Sloan Digital Sky Survey (SDSS). We measure the VPF as a function of galaxy
color and luminosity in both surveys and find that it mimics trends displayed
in the two-point correlation function, ; namely that samples of brighter,
red galaxies have larger voids (i.e. are more strongly clustered) than fainter,
blue galaxies. We also clearly detect evolution in the VPF with cosmic time,
with voids being larger in comoving units at z~0. We find that the reduced VPF
matches the predictions of a `negative binomial' model for galaxies of all
colors, luminosities, and redshifts studied. This model lacks a physical
motivation, but produces a simple analytic prediction for sources of any number
density and integrated two-point correlation function, \bar{\xi}. This implies
that differences in the VPF across different galaxy populations are consistent
with being due entirely to differences in the population number density and
\bar{\xi}. The robust result that all galaxy populations follow the negative
binomial model appears to be due to primarily to the clustering of dark matter
halos. The reduced VPF is insensitive to changes in the parameters of the halo
occupation distribution, in the sense that halo models with the same \bar{\xi}
will produce the same VPF. For the wide range of galaxies studied, the VPF
therefore does not appear to provide useful constraints on galaxy evolution
models that cannot be gleaned from studies of \bar{\xi} alone. (abridged)Comment: 17 pages, 15 figures, ApJ accepte
NIMBUS: The Near-Infrared Multi-Band Ultraprecise Spectroimager for SOFIA
We present a new and innovative near-infrared multi-band ultraprecise
spectroimager (NIMBUS) for SOFIA. This design is capable of characterizing a
large sample of extrasolar planet atmospheres by measuring elemental and
molecular abundances during primary transit and occultation. This wide-field
spectroimager would also provide new insights into Trans-Neptunian Objects
(TNO), Solar System occultations, brown dwarf atmospheres, carbon chemistry in
globular clusters, chemical gradients in nearby galaxies, and galaxy
photometric redshifts. NIMBUS would be the premier ultraprecise spectroimager
by taking advantage of the SOFIA observatory and state of the art infrared
technologies.
This optical design splits the beam into eight separate spectral bandpasses,
centered around key molecular bands from 1 to 4 microns. Each spectral channel
has a wide field of view for simultaneous observations of a reference star that
can decorrelate time-variable atmospheric and optical assembly effects,
allowing the instrument to achieve ultraprecise calibration for imaging and
photometry for a wide variety of astrophysical sources. NIMBUS produces the
same data products as a low-resolution integral field spectrograph over a large
spectral bandpass, but this design obviates many of the problems that preclude
high-precision measurements with traditional slit and integral field
spectrographs. This instrument concept is currently not funded for development.Comment: 14 pages, 9 figures, SPIE Astronomical Telescopes and Instrumentation
201
The DEEP2 Galaxy Redshift Survey: The Voronoi-Delaunay Method Catalog of Galaxy Groups
We present a public catalog of galaxy groups constructed from the spectroscopic sample of galaxies in the fourth data release from the Deep Extragalactic Evolutionary Probe 2 (DEEP2) Galaxy Redshift Survey, including the Extended Groth Strip (EGS). The catalog contains 1165 groups with two or more members in the EGS over the redshift range 0 0.6 in the rest of DEEP2. Twenty-five percent of EGS galaxies and fourteen percent of high-z DEEP2 galaxies are assigned to galaxy groups. The groups were detected using the Voronoi-Delaunay method (VDM) after it has been optimized on mock DEEP2 catalogs following similar methods to those employed in Gerke et al. In the optimization effort, we have taken particular care to ensure that the mock catalogs resemble the data as closely as possible, and we have fine-tuned our methods separately on mocks constructed for the EGS and the rest of DEEP2. We have also probed the effect of the assumed cosmology on our inferred group-finding efficiency by performing our optimization on three different mock catalogs with different background cosmologies, finding large differences in the group-finding success we can achieve for these different mocks. Using the mock catalog whose background cosmology is most consistent with current data, we estimate that the DEEP2 group catalog is 72% complete and 61% pure (74% and 67% for the EGS) and that the group finder correctly classifies 70% of galaxies that truly belong to groups, with an additional 46% of interloper galaxies contaminating the catalog (66% and 43% for the EGS). We also confirm that the VDM catalog reconstructs the abundance of galaxy groups with velocity dispersions above ~300 km s^(–1) to an accuracy better than the sample variance, and this successful reconstruction is not strongly dependent on cosmology. This makes the DEEP2 group catalog a promising probe of the growth of cosmic structure that can potentially be used for cosmological tests
The Density Profiles of Massive, Relaxed Galaxy Clusters. II. Separating Luminous and Dark Matter in Cluster Cores
We present stellar and dark matter (DM) density profiles for a sample of
seven massive, relaxed galaxy clusters derived from strong and weak
gravitational lensing and resolved stellar kinematic observations within the
centrally-located brightest cluster galaxies (BCGs). In Paper I of the series,
we demonstrated that the total density profile derived from these data, which
span 3 decades in radius, is consistent with numerical DM-only simulations at
radii >~ 5-10 kpc, despite the significant contribution of stellar material in
the core. Here we decompose the inner mass profiles of these clusters into
stellar and dark components. Parametrizing the DM density profile as a power
law rho_DM ~ r^{-\beta} on small scales, we find a mean slope = 0.50 +-
0.10 (random) +0.14-0.13 (systematic). Alternatively, cored Navarro-Frenk-White
(NFW) profiles with = 1.14 +- 0.13 (random) +0.14-0.22
(systematic) provide an equally good description. These density profiles are
significantly shallower than canonical NFW models at radii <~ 30 kpc,
comparable to the effective radii of the BCGs. The inner DM profile is
correlated with the distribution of stars in the BCG, suggesting a connection
between the inner halo and the assembly of stars in the central galaxy. The
stellar mass-to-light ratio inferred from lensing and stellar dynamics is
consistent with that inferred using stellar population synthesis models if a
Salpeter initial mass function is adopted. We compare these results to theories
describing the interaction between baryons and DM in cluster cores, including
adiabatic contraction models and the possible effects of galaxy mergers and
active galactic nucleus feedback, and evaluate possible signatures of
alternative DM candidates.Comment: Updated to matched the published version in Ap
Voreloxin Is an Anticancer Quinolone Derivative that Intercalates DNA and Poisons Topoisomerase II
Topoisomerase II is critical for DNA replication, transcription and chromosome segregation and is a well validated target of anti-neoplastic drugs including the anthracyclines and epipodophyllotoxins. However, these drugs are limited by common tumor resistance mechanisms and side-effect profiles. Novel topoisomerase II-targeting agents may benefit patients who prove resistant to currently available topoisomerase II-targeting drugs or encounter unacceptable toxicities. Voreloxin is an anticancer quinolone derivative, a chemical scaffold not used previously for cancer treatment. Voreloxin is completing Phase 2 clinical trials in acute myeloid leukemia and platinum-resistant ovarian cancer. This study defined voreloxin's anticancer mechanism of action as a critical component of rational clinical development informed by translational research.Biochemical and cell-based studies established that voreloxin intercalates DNA and poisons topoisomerase II, causing DNA double-strand breaks, G2 arrest, and apoptosis. Voreloxin is differentiated both structurally and mechanistically from other topoisomerase II poisons currently in use as chemotherapeutics. In cell-based studies, voreloxin poisoned topoisomerase II and caused dose-dependent, site-selective DNA fragmentation analogous to that of quinolone antibacterials in prokaryotes; in contrast etoposide, the nonintercalating epipodophyllotoxin topoisomerase II poison, caused extensive DNA fragmentation. Etoposide's activity was highly dependent on topoisomerase II while voreloxin and the intercalating anthracycline topoisomerase II poison, doxorubicin, had comparable dependence on this enzyme for inducing G2 arrest. Mechanistic interrogation with voreloxin analogs revealed that intercalation is required for voreloxin's activity; a nonintercalating analog did not inhibit proliferation or induce G2 arrest, while an analog with enhanced intercalation was 9.5-fold more potent.As a first-in-class anticancer quinolone derivative, voreloxin is a toposiomerase II-targeting agent with a unique mechanistic signature. A detailed understanding of voreloxin's molecular mechanism, in combination with its evolving clinical profile, may advance our understanding of structure-activity relationships to develop safer and more effective topoisomerase II-targeted therapies for the treatment of cancer
Stellar populations of barred quiescent galaxies
International audienceSelecting centrally quiescent galaxies from the Sloan Digital Sky Survey (SDSS) to create high signal-to-noise ratio (greater than or similar to 100 angstrom(-1)) stacked spectra with minimal emission-line contamination, we accurately and precisely model the central stellar populations of barred and unbarred quiescent disk galaxies. By splitting our sample by redshift, we can use the fixed size of the SDSS fiber to model the stellar populations at different radii within galaxies. At 0.02 \textless z \textless 0.04, the SDSS fiber radius corresponds to approximate to 1 kpc, which is the typical half-light radii of both classical bulges and disky pseudobulges. Assuming that the SDSS fiber primarily covers the bulges at these redshifts, our analysis shows that there are no significant differences in the stellar populations, i.e., stellar age, [Fe/H], [Mg/Fe], and [N/Fe], of the bulges of barred versus unbarred quiescent disk galaxies. Modeling the stellar populations at different redshift intervals from z = 0.020 to z = 0.085 at fixed stellar masses produces an estimate of the stellar population gradients out to about half the typical effective radius of our sample, assuming null evolution over this approximate to 1 Gyr epoch. We find that there are no noticeable differences in the slopes of the azimuthally averaged gradients of barred versus unbarred quiescent disk galaxies. These results suggest that bars are not a strong influence on the chemical evolution of quiescent disk galaxies
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