215 research outputs found
Content Development of the Educational Interpreter Roles and Responsibilities Guiding Checklist
The purpose of this qualitative study was to extend development of the Educational Interpreter Roles and Responsibilities (EIRR) Guiding Checklist, which was designed to assist the Individualized Education Program (IEP) team in determining and documenting individualized roles and responsibilities of the educational interpreter, as appropriate to the needs of the student receiving such services and the qualifications of the interpreter as a related service provider. Literature indicates a long-standing state of confusion regarding the appropriate roles and responsibilities of the educational interpreter, as well as the need for more clear guidelines and procedures. The Checklist was initially designed by a certified teacher of the deaf who was experienced as an educational interpreter and supervised educational interpreters across a public-school d/Deaf and hard of hearing (DHH) program. To continue preliminary instrument development towards content validation, knowledge of laws and strategies related to DHH education were deemed critical. As such, seven certified teachers of DHH students, who had at least three years’ experience supervising, overseeing, and/or providing training to educational interpreters, provided extensive feedback regarding the Checklist. Content analysis was utilized to determine themes that emerged. Results indicated significant support regarding the need for the checklist, as well as contributions towards further development, thus concluding in 63 revisions. Next steps towards development and validation are presented
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The effects of an adolescent apprenticeship process in environmental education on the development of citizen participation characteristics in high school seniors.
Teaching Orientation and Mobility Skills to Students with Autism and Vision Impairment in Public Schools: A Data-Based Study
Two students with autism, vision impairment, and intellectual disability participated in an orientation and mobility (O&M) intervention to travel in school settings using their folding canes. A multiple-baseline across participants design to determine the effectiveness of the intervention was used. The dependent variable was time taken to travel the specified route. The independent variable was O&M training. Results indicated that both participants took less time to travel during the intervention compared to the baseline. Students with vision impairment and autism can be trained using systematic O&M training. The O&M specialists working with children with autism and vision impairment should collect data and make data-based decisions while providing O&M instruction
Dust-temperature of an isolated star-forming cloud: Herschel observations of the Bok globule CB244
We present Herschel observations of the isolated, low-mass star-forming Bok
globule CB244. It contains two cold sources, a low-mass Class 0 protostar and a
starless core, which is likely to be prestellar in nature, separated by 90
arcsec (~ 18000 AU). The Herschel data sample the peak of the Planck spectrum
for these sources, and are therefore ideal for dust-temperature and column
density modeling. With these data and a near-IR extinction map, the MIPS 70
micron mosaic, the SCUBA 850 micron map, and the IRAM 1.3 mm map, we model the
dust-temperature and column density of CB244 and present the first measured
dust-temperature map of an entire star-forming molecular cloud. We find that
the column-averaged dust-temperature near the protostar is ~ 17.7 K, while for
the starless core it is ~ 10.6K, and that the effect of external heating causes
the cloud dust-temperature to rise to ~ 17 K where the hydrogen column density
drops below 10^21 cm^-2. The total hydrogen mass of CB244 (assuming a distance
of 200 pc) is 15 +/- 5 M_sun. The mass of the protostellar core is 1.6 +/- 0.1
M_sun and the mass of the starless core is 5 +/- 2 M_sun, indicating that ~ 45%
of the mass in the globule is participating in the star-formation process.Comment: Accepted for A&A Herschel Special Issue; 5 pages, 2 figure
Herschel Observations of the W43 "mini-starburst"
Aims: To explore the infrared and radio properties of one of the closest
Galactic starburst regions. Methods: Images obtained with the Herschel Space
Observatory at wavelengths of 70, 160, 250, 350, and 500 microns using the PACS
and SPIRE arrays are analyzed and compared with radio continuum VLA data and 8
micron images from the Spitzer Space Telescope. The morphology of the
far-infrared emission is combined with radial velocity measurements of
millimeter and centimeter wavelength transitions to identify features likely to
be associated with the W43 complex. Results: The W43 star-forming complex is
resolved into a dense cluster of protostars, infrared dark clouds, and ridges
of warm dust heated by massive stars. The 4 brightest compact sources with L >
1.5 x 10^4 Lsun embedded within the Z-shaped ridge of bright dust emission in
W43 remain single at 4" (0.1 pc) resolution. These objects, likely to be
massive protostars or compact clusters in early stages of evolution are
embedded in clumps with masses of 10^3 to 10^4 Msun, but contribute only 2% to
the 3.6 x 10^6 Lsun far-IR luminosity of W43 measured in a 16 by 16 pc box. The
total mass of gas derived from the far-IR dust emission inside this region is
~10^6 Msun. Cometary dust clouds, compact 6 cm radio sources, and warm dust
mark the locations of older populations of massive stars. Energy release has
created a cavity blowing-out below the Galactic plane. Compression of molecular
gas in the plane by the older HII region near G30.684-0.260 and the bipolar
structure of the resulting younger W43 HII region may have triggered the
current mini-star burst.Comment: 5 pages, 3 figures, accepted for A&A Special Issu
BLAST: The Mass Function, Lifetimes, and Properties of Intermediate Mass Cores from a 50 Square Degree Submillimeter Galactic Survey in Vela (l = ~265)
We present first results from an unbiased 50 deg^2 submillimeter Galactic
survey at 250, 350, and 500 micron from the 2006 flight of the Balloon-borne
Large Aperture Submillimeter Telescope (BLAST). The map has resolution ranging
from 36 arcsec to 60 arcsec in the three submillimeter bands spanning the
thermal emission peak of cold starless cores. We determine the temperature,
luminosity, and mass of more than one thousand compact sources in a range of
evolutionary stages and an unbiased statistical characterization of the
population. From comparison with C^(18)O data, we find the dust opacity per gas
mass, kappa r = 0.16 cm^2 g^(-1) at 250 micron, for cold clumps. We find that
2% of the mass of the molecular gas over this diverse region is in cores colder
than 14 K, and that the mass function for these cold cores is consistent with a
power law with index alpha = -3.22 +/- 0.14 over the mass range 14 M_sun < M <
80 M_sun. Additionally, we infer a mass-dependent cold core lifetime of t_c(M)
= 4E6 (M/20 M_sun)^(-0.9) years - longer than what has been found in previous
surveys of either low or high mass cores, and significantly longer than free
fall or likely turbulent decay times. This implies some form of non-thermal
support for cold cores during this early stage of star formation.Comment: Accepted for publication in the Astrophysical Journal. Maps available
at http://blastexperiment.info
Determination of the far-infrared dust opacity in a prestellar core
Context. Mass estimates of interstellar clouds from far-infrared and submillimetre mappings depend on the assumed dust absorption cross-section for radiation at those wavelengths.
Aims: The aim is to determine the far-IR dust absorption cross-section in a starless, dense core located in Corona Australis. The value is needed for determining of the core mass and other physical properties. It can also have a bearing on the evolutionary stage of the core.
Methods: We correlated near-infrared stellar H - Ks colour excesses of background stars from NTT/SOFI with the far-IR optical depth map, τFIR, derived from Herschel 160, 250, 350, and 500 μm data. The Herschel maps were also used to construct a model for the cloud to examine the effect of temperature gradients on the estimated optical depths and dust absorption cross-sections.
Results: A linear correlation is seen between the colour H - Ks and τFIR up to high extinctions (AV ~ 25). The correlation translates to the average extinction ratio A250 μm/AJ = 0.0014 ± 0.0002, assuming a standard near-infrared extinction law and a dust emissivity index β = 2. Using an empirical NH/AJ ratio we obtain an average absorption cross-section per H nucleus of σH250 μm = (1.8 ± 0.3) × 10-25 cm H-atom, corresponding to a cross-section per unit mass of gas κ250 μmg = 0.08 ± 0.01 cm g. The cloud model, however, suggests that owing to the bias caused by temperature changes along the line-of-sight, these values underestimate the true cross-sections by up to 40% near the centre of the core. Assuming that the model describes the effect of the temperature variation on τFIR correctly, we find that the relationship between H - Ks and τFIR agrees with the recently determined relationship between σH and NH in Orion A.
Conclusions: The derived far-IR cross-section agrees with previous determinations in molecular clouds with moderate column densities, and is not particularly large compared with some other cold cores. We suggest that this is connected to the core not being very dense (the central density is likely to be ~105 cm), and judging from previous molecular line data, it appears to be at an early stage of chemical evolution
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