The Functional Vision for Communication Questionnaire (FVC-Q):Exploring Parental Report of Non-Speaking Children's Fixation Skills Using a Structured History-Taking Approach

This paper explores whether a structured history-taking tool yields useful descriptions of children’s looking skills. Parents of 32 children referred to a specialist communication clinic reported their child’s looking skills using the Functional Vision for Communication Questionnaire (FVC-Q), providing descriptions of single object fixation, fixation shifts between objects and fixation shifts from object to person. Descriptions were compared with clinical assessment. 24/32 children were reported to have some limitation in fixation. Limitation was subsequently seen in 30/32 children. Parental report and assessment agreed fully in 23/32 (72%). The largest area of discrepancy was object-person fixation shifts, with five children not observed to show this behavior despite its being reported. Findings indicate a structured questionnaire yields description of fixations, which correspond well with clinical assessment. Descriptions supported discussion between parents and clinicians. It is proposed that the FVC-Q is a valuable tool in supporting clinicians in eliciting information about fixation skills

The Functional Vision for Communication Questionnaire (FVC-Q):Exploring Parental Report of Non-Speaking Children's Fixation Skills Using a Structured History-Taking Approach

This paper explores whether a structured history-taking tool yields useful descriptions of children’s looking skills. Parents of 32 children referred to a specialist communication clinic reported their child’s looking skills using the Functional Vision for Communication Questionnaire (FVC-Q), providing descriptions of single object fixation, fixation shifts between objects and fixation shifts from object to person. Descriptions were compared with clinical assessment. 24/32 children were reported to have some limitation in fixation. Limitation was subsequently seen in 30/32 children. Parental report and assessment agreed fully in 23/32 (72%). The largest area of discrepancy was object-person fixation shifts, with five children not observed to show this behavior despite its being reported. Findings indicate a structured questionnaire yields description of fixations, which correspond well with clinical assessment. Descriptions supported discussion between parents and clinicians. It is proposed that the FVC-Q is a valuable tool in supporting clinicians in eliciting information about fixation skills

A Measurement of the Temperature-Density Relation in the Intergalactic Medium Using a New Lyman-alpha Absorption Line Fitting Method

The evolution of the temperature in the intergalactic medium is related to the reionization of hydrogen and helium, and has important consequences for our understanding of the Lya forest and of galaxy formation in gravitational models of large-scale structure. We measure the temperature-density relation of intergalactic gas from Lya forest observations of eight quasar spectra with high resolution and signal-to-noise ratio, using a new line fitting technique to obtain a lower cutoff of the distribution of line widths from which the temperature is derived. We carefully test the accuracy of this technique to recover the gas temperature with a hydrodynamic simulation. The temperature at redshift z=(3.9, 3.0, 2.4) is best determined at densities slightly above the mean: T_star=(20200\pm2700, 20200\pm1300, 22600\pm1900)K (statistical error bars) for gas density (in units of the mean density) Delta_star=(1.42\pm0.08, 1.37\pm0.11, 1.66\pm0.11). The power-law index of the temperature-density relation, defined by T=T_star(Delta/Delta_star)^{gamma-1}, is gamma-1= (0.43\pm0.45, 0.29\pm0.30, 0.52\pm0.14) for the same three redshifts. The temperature at the fixed over-density Delta=1.4 is T_1.4=(20100\pm2800, 20300\pm1400, 20700\pm1900)K. These temperatures are higher than expected for photoionized gas in ionization equilibrium with a cosmic background, and can be explained by a gradual additional heating due to on-going HeII reionization. The measurement of the temperature reduces one source of uncertainty in the lower limit to the baryon density implied by the observed mean flux decrement. We find that the temperature cannot be reliably measured for under-dense gas, because the velocities due to expansion always dominate the widths of the corresponding weak lines.Comment: submitted to Ap

Prospectus, November 28, 1979

STARCASTLE\u27 FEATURED IN FIRST PRESENTING SHOW; Week in Review: Across the globe, In the nation, Around the state; Salt of the Earth : controversial film at PC; Iranians air grievances against Shah; Briefs: Board summary listed, Women Forum meets Sat.; Letters to the Editor: Letter reasons vs. Nolen\u27s logic, Voter writes to reveal real Kennedy opinion; Campus Question: How would you handle Irainian situation?; Classifieds; NFL playoffs make blurry pic; Sports shorts; Cobras split games, play at home Fri.; Winter survival tips can keep you alive; Reviews: After big talk, \u27Tusk\u27 gets low grade, \u27Keep the Fire\u27 keeps Loggins\u27 formula; Transfer students need financial aids transcripthttps://spark.parkland.edu/prospectus_1979/1002/thumbnail.jp

Transitional disks and their origins: an infrared spectroscopic survey of Orion A

Transitional disks are protoplanetary disks around young stars, with inner holes or gaps which are surrounded by optically thick outer, and often inner, disks. Here we present observations of 62 new transitional disks in the Orion A star-forming region. These were identified using the \textit{Spitzer Space Telescope}'s Infrared Spectrograph and followed up with determinations of stellar and accretion parameters using the Infrared Telescope Facility's SpeX. We combine these new observations with our previous results on transitional disks in Taurus, Chamaeleon I, Ophiuchus and Perseus, and with archival X-ray observations. This produces a sample of 105 transitional disks of "cluster" age 3 Myr or less, by far the largest hitherto assembled. We use this sample to search for trends between the radial structure in the disks and many other system properties, in order to place constraints on the possible origins of transitional disks. We see a clear progression of host star accretion rate and the different disk morphologies. We confirm that transitional disks with complete central clearings have median accretion rates an order of magnitude smaller than radially continuous disks of the same population. Pre-transitional disks --- those objects with gaps that separate inner and outer disks --- have median accretion rates intermediate between the two. Our results from the search for statistically significant trends, especially related to $\dot{M}$, strongly support that in both cases the gaps are far more likely to be due to the gravitational influence of Jovian planets or brown dwarfs orbiting within the gaps, than to any of the photoevaporative, turbulent or grain-growth processes that can lead to disk dissipation. We also find that the fraction of Class II YSOs which are transitional disks is large, 0.1-0.2, especially in the youngest associations.Comment: 96 pages, 25 figures, resubmitted to Ap

Student Housing Overview: Assessing Issues and Potential Options

report: 59 pp.; ill., digital file.This report sets out for the administration of the University of Winnipeg some of the contexts, considerations and principles necessary when undertaking any future housing-oriented development. The report provides general support for the proposition that – given demonstrated need for affordable and accessible housing in the neighbourhoods surrounding the University of Winnipeg – some kind of mixed-use development – incorporating affordable, accessible housing for a range of household types, as well as other services that would cater to both the student body and residents and organizations of the surrounding communities – would be beneficial to the university and be consistent with both the surrounding community as well as its overall strategic plan.University of Winnipeg. The report concludes with very general recommendation

Prospectus, December 1, 1983

SKETCHES TELL STORIES; News Digest; Boisso - striving to improve; PC Happenings: Cabin Fever, Holiday play; Students keep candy on hand; Club Notes; Crime and drug abuse never to lower to 1950-69 level; Treat hypothermia; Artists will be able to display art on video; Question: What did you think of \u27The Day After\u27?; Fellow students sharing their talents during \u27Celebrate the Arts Week\u27; Classified; PC grad to Texas; \u27Rear Window\u27 first of Hitchcock re-releases; Rock and Roll with \u27the Kid\u27; King trips with \u27Pet\u27; Free theater offered to students; Police attracts fans from all over; Parkland edges Spoon River; IOC shoots past Cobras; Composite Athletic Schedule; Fast Freddy Contesthttps://spark.parkland.edu/prospectus_1983/1002/thumbnail.jp

The Metallicity and Dust Content of HVC 287.5+22.5+240: Evidence for a Magellanic Clouds Origin

We estimate the abundances of S and Fe in the high velocity cloud HVC 287.5+22.5+240, which has a velocity of +240 km/s with respect to the local standard of rest and is in the Galactic direction l~287, b~23. The measurements are based on UV absorption lines of these elements in the Hubble Space Telescope spectrum of NGC 3783, a background Seyfert galaxy, as well as new H I 21-cm interferometric data taken with the Australia Telescope. We find S/H=0.25+/-0.07 and Fe/H=0.033+/-0.006 solar, with S/Fe=7.6+/-2.2 times the solar ratio. The S/H value provides an accurate measure of the chemical enrichment level in the HVC, while the super-solar S/Fe ratio clearly indicates the presence of dust, which depletes the gas-phase abundance of Fe. The metallicity and depletion information obtained here, coupled with the velocity and the position of the HVC in the sky, strongly suggest that the HVC originated from the Magellanic Clouds. It is likely (though not necessary) that the same process(es) that generated the Magellanic Stream is also responsible for HVC 287.5+22.5+240.Comment: AASTEX, 3 postscript figures, AJ, 1998, Jan issu