The Metaverse and Oncology McWilliam, A.; Scarfe, P.
Clinical oncology (Royal College of Radiologists (Great Britain)),
January 2023, 2023-01-00, 20230101, Letnik:
35, Številka:
1
Journal Article
The aim of this study was to find out about attitudes toward inclusion and benefits perceived by families with children enrolled in schools attended by students with ASD at different educational ...stages (from kindergarten to high school). 323 families of classmates of students with ASD from different educational stages of 16 mainstream schools participated. The analysis of the attitudes, perceived benefits, relationship with the teacher, and relationship with the school was carried out through questionnaires. The results show positive attitudes toward the inclusive education of students with ASD in all families, but especially among families of children with SEN. All the families identified the benefit of inclusion. Attitudes are related to collaboration with the school and satisfaction with teachers.
The GIRAFFE Inner Bulge Survey (GIBS) Zoccali, M; Vasquez, S; Gonzalez, O A ...
Astronomy and astrophysics (Berlin),
3/2017, Letnik:
599
Journal Article
Recenzirano
Odprti dostop
Context. Several recent studies have demonstrated that the Galactic bulge hosts two components with different mean metallicities, and possibly different spatial distribution and kinematics. As a ...consequence, both the metallicity distribution and the radial velocity of bulge stars vary across different lines of sight. Aims. We present here the metallicity distribution function of red clump stars in 26 fields spread across a wide area of the bulge, with special emphasis on fields close to Galactic plane, at latitudes b= -2degrees and b= -1degrees, that have not been explored before. Methods. This paper includes new metallicities from a sample of approximately 5000 K giant stars, observed at spectral resolution R~ 6500, in the Calcium II Triplet region. These represent the main dataset from the GIRAFFE Inner Bulge Survey. As part of the same survey we have previously published results for a sample of approximately 600 K giant stars, at latitude b~ -4degrees, derived from higher resolution spectra (R= 22 500). Results. The combined sample allows us to trace and characterize the metal poor and metal rich bulge populations down to the inner bulge. We present a density map for each of the two components. Contrary to expectations from previous works, we found the metal poor population to be more centrally concentrated than the metal rich one, and with a more axisymmetric spatial distribution. The metal rich population, on the other hand, is arranged in a boxy distribution, consistent with an edge-on bar. By coupling metallicities and radial velocities we show that the metal poor population has a velocity dispersion that varies rather mildly with latitude. On the contrary, the metal rich population has a low velocity dispersion far from the plane (b= -8.5degrees), yet has a steeper gradient with latitude, becoming higher than the metal poor one in the innermost field (b= -1degrees). Conclusions. This work provides new observational constraints on the actual chemodynamical properties of the Galactic bulge, that will help discrimination between different formation models.
As an initial step toward improving the outcomes of learners with disabilities, special educators have formulated guidelines for identifying evidence-based practices. We describe the Council of ...Exceptional Children’s new set of standards for identifying evidence-based practices in special education and how they (a) were systematically vetted by expert special education researchers through a Delphi study, (b) demonstrated adequate inter-rater reliability in a pilot study, (c) delineate specific criteria in many areas and provide flexibility to tailor other criteria, (d) provide an integrated set of standards for classifying the evidence base of practices based on findings from both group comparison and single-subject studies, and (e) can be applied by independent special education researchers. We conclude by noting limitations to the standards, briefly comparing these new standards with other evidence-based practice standards, and providing recommendations for future research and for refining the standards.
We present our detailed spectroscopic analysis of the chemical composition of four red giant stars in the halo globular cluster NGC 6426. We obtained high-resolution spectra using the Magellan2/MIKE ...spectrograph, from which we derived equivalent widths and subsequently computed abundances of 24 species of 22 chemical elements. For the purpose of measuring equivalent widths, we developed a new semi-automated tool, called EWCODE. We report a mean Fe content of Fe/H =−2.34 ± 0.05 dex (stat.) in accordance with previous studies. At a mean α-abundance of (Mg, Si, Ca)/3 Fe = 0.39 ± 0.03 dex, NGC 6426 falls on the trend drawn by the Milky Way halo and other globular clusters at comparably low metallicities. The distribution of the lighter α-elements as well as the enhanced ratio Zn/Fe = 0.39 dex could originate from hypernova enrichment of the pre-cluster medium. We find tentative evidence for a spread in the elements Mg, Si, and Zn, indicating an enrichment scenario, where ejecta of evolved massive stars of a slightly older population have polluted a newly born younger one. The heavy element abundances in this cluster fit well into the picture of metal-poor globular clusters, which in that respect appear to be remarkably homogeneous. The pattern of the neutron-capture elements heavier than Zn points toward an enrichment history governed by the r-process with little, if any, sign of s-process contributions. This finding is supported by the striking similarity of our program stars to the metal-poor field star HD 108317.
Early intervention is a system of services designed to strengthen child outcomes and build family capacity. One approach of service provision is the Routines-Based Model which implements ...adult-learning practices wherein service providers and caregivers partner to build family-mediated interventions for children. Owing to COVID-19 and the benefits of telepractice, more and more service providers are likely to incorporate a telepractice modality into service provision. Because the Routines-Based Model uses family consultation, these home-visiting practices translate well to telepractice. In addition to consultation techniques, however, service providers must use technology advantageously to ensure effective communication practices. This article discusses technology uses in telepractice that can be incorporated in the Routines-Based Model, Tele-Routines-Based Home Visits, and examples of Tele-Routines-Based Home Visits.
The GIRAFFE Inner Bulge Survey (GIBS) Zoccali, M; Gonzalez, O A; Vasquez, S ...
Astronomy and astrophysics (Berlin),
2/2014, Letnik:
562
Journal Article
Recenzirano
Odprti dostop
The Galactic bulge is a massive, old component of the Milky Way. It is known to host a bar, and it has recently been demonstrated to have a pronounced boxy/peanut structure in its outer region. ...Several independent studies suggest the presence of more than one stellar populations in the bulge, with different origins and a relative fraction changing across the bulge area. This is the first of a series of papers presenting the results of the Giraffe Inner Bulge Survey, carried out at the ESO-VLT with the multifibre spectrograph FLAMES. In total we present here radial velocities for 6392 red clump stars. We derive a radial velocity, and velocity dispersion map of the Milky Way bulge, useful to be compared with similar maps of external bulges, and to infer the expected velocities and dispersion at any line of sight. Finally, we find strong evidence for a velocity dispersion peak at (0, -1) and (0, -2), possibly indicative of a high density peak in the central ~250 pc of the bulge.
Context. M 75 is a relatively young globular cluster (GC) found at 15 kpc from the Galactic centre at the transition region between the inner and outer Milky Way halos. Aims. Our aims are to perform ...a comprehensive abundance study of a variety of chemical elements in this GC such as to investigate its chemical enrichment history in terms of early star formation, and to search for any multiple populations. Methods. We have obtained high resolution spectroscopy with the MIKE instrument at the Magellan telescope for 16 red giant stars. Their membership within the GC is confirmed from radial velocity measurements. Our chemical abundance analysis is performed via equivalent width measurements and spectral synthesis, assuming local thermodynamic equilibrium. Results. We present the first comprehensive abundance study of M 75 to date. The cluster is metal-rich (Fe/H = −1.16 ± 0.02 dex, α/Fe = +0.30 ± 0.02 dex), and shows a marginal spread in Fe/H of 0.07 dex, typical of most GCs of similar luminosity. A moderately extended O-Na anticorrelation is clearly visible, likely showing three generations of stars, formed on a short timescale. Additionally the two most Na-rich stars are also Ba-enhanced by 0.4 and 0.6 dex, respectively, indicative of pollution by lower mass (M ~ 4−5 M⊙) asymptotic giant branch stars. The overall n-capture element pattern is compatible with predominant r-process enrichment, which is rarely the case in GCs of such a high metallicity.
Context. The evolution of C and O abundances in the Milky Way can impose strong constraints on stellar nucleosynthesis and help in understanding the formation and evolution of our Galaxy. Aims. The ...aim of this paper is to review the measured C and O abundances in the disk and bulge of the Galaxy and compare the results to predictions of Galactic chemical evolution models. Methods. We adopt two successful chemical evolution models for the bulge and the disk, respectively. They assume the same nucleosynthesis prescriptions but different histories of star formation. Results. The data show a clear distinction between the trend of C/O in the thick and thin Galactic disks, while the thick disk and bulge trends are indistinguishable with a large (>0.5 dex) increase in the C/O ratio in the range from -0.1 to +0.4 dex for O/H. In our models we consider yields from massive stars with and without the inclusion of metallicity-dependent stellar winds. The observed increase in the C/O with metallicity in the bulge and thick disk lies between the predictions utilizing mass-loss rates of Maeder and Meynet & Maeder. A model without metallicity-dependent yields completely fails to match the observations. Thus, the relative increase in carbon abundance at high metallicity appears to come from metallicity-dependent stellar winds in massive stars. These results also explain the steep decline of the O/Fe ratio with Fe/H in the Galactic bulge, while the Mg/Fe ratio is enhanced at all Fe/H. Conclusions. We conclude that data and models are consistent with a rapid bulge and thick disk formation timescales, and with metallicity-dependent yields for C and O. The observed too high C/O ratios at low metallicity in the bulge may stem from an unaccounted source of carbon: very fast rotating metal poor stars, or metal-poor binary systems whose envelopes were stripped by Roche lobe overflow.
Purpose
Due to the electron return effect (ERE) during magnetic resonance imaging guided radiotherapy (MRIgRT), rectal gas during pelvic treatments can result in hot spots of over‐dosage in the ...rectal wall. Determining the clinical impact of this effect on rectal toxicity requires estimation of the amount and mobility (and stability) of rectal gas during treatment. We therefore investigated the amount of rectal gas and local inter‐ and intra‐fractional changes of rectal gas in pelvic cancer patients.
Methods
To estimate the volume of gas present at treatment planning, the rectal gas contents in the planning computed tomography (CT) scans of 124 bladder, 70 cervical and 2180 prostate cancer patients were calculated.
To estimate inter‐ and intra‐fractional variations in rectal gas, 174 and 131 T2‐w MRIs for six cervical and eleven bladder cancer patients were used. These scans were acquired during four scan‐sessions (~20–25 min each) at various time‐points. Additionally, 258 T2‐w MRIs of the first five prostate cancer patients treated using MRIgRT at our center, acquired during each fraction, were analyzed. Rectums were delineated on all scans.
The area of gas within the rectum delineations was identified on each MRI slice using thresholding techniques. The area of gas on each slice of the rectum was used to calculate the inter‐ and intra‐fractional group mean, systematic and random variations along the length of the rectum.
The cumulative dose perturbation as a result of the gas was estimated. Two approaches were explored: accounting or not accounting for the gas at the start of the scan‐session.
Results
Intra‐fractional variations in rectal gas are small compared to the absolute volume of rectal gas detected for all patient groups. That is, rectal gas is likely to remain stable for periods of 20–25 min. Larger volumes of gas and larger variations in gas volume were observed in bladder cancer patients compared with cervical and prostate cancer patients.
For all patients, local cumulative dose perturbations per beam over an entire treatment in the order of 60 % were estimated when gas had not been accounted for in the daily adaption. The calculated dose perturbation over the whole treatment was dramatically reduced in all patients when accounting for the gas in the daily set‐up image.
Conclusion
Rectal gas in pelvic cancer patients is likely to remain stable over the course of an MRIgRT fraction, and also likely to reappear in the same location in multiple fractions, and can therefore result in clinically relevant over‐dosage in the rectal wall. The over‐dosage is reduced when accounting for gas in the daily adaption.
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