115 research outputs found
Study of the winter 2005 Antarctica polar vortex
During winter and springtime, the flow above Antarctica at high altitude
(upper troposphere and stratosphere) is dominated by the presence of a vortex
centered above the continent. It lasts typically from August to November. This
vortex is characterized by a strong cyclonic jet centered above the polar high.
In a recent study of our group (Hagelin et al., 2008) of four different sites
in the Antarctic internal plateau (South Pole, Dome C, Dome A and Dome F), it
was made the hypothesis that the wind speed strength in the upper atmosphere
should be related to the distance of the site to the center of the Antarctic
polar vortex. This high altitude wind is very important from an astronomical
point of view since it might trigger the onset of the optical turbulence and
strongly affect other optical turbulence parameters. What we are interested in
here is to localize the position of the minimum value of the wind speed at high
altitude in order to confirm the hypothesis of Hagelin et al. (2008).Comment: 3rd ARENA conference, 11-15 May 2009 EAS Publication Serie
Mt. Graham: Optical turbulence vertical distribution at standard and high vertical resolution
A characterization of the optical turbulence vertical distribution and all
the main integrated astroclimatic parameters derived from the CN2 and the wind
speed profiles above Mt. Graham is presented. The statistic includes
measurements related to 43 nights done with a Generalized Scidar (GS) used in
standard configuration with a vertical resolution of ~1 km on the whole 20-22
km and with the new technique (HVR-GS) in the first kilometer. The latter
achieves a resolution of ~ 20-30 m in this region of the atmosphere.
Measurements done in different periods of the year permit us to provide a
seasonal variation analysis of the CN2. A discretized distribution of the
typical CN2 profiles useful for the Ground Layer Adaptive Optics (GLAO)
simulations is provided and a specific analysis for the LBT Laser Guide Star
system ARGOS case is done including the calculation of the 'gray zones' for J,
H and K bands. Mt. Graham confirms to be an excellent site with median values
of the seeing without dome contribution equal to 0.72", the isoplanatic angle
equal to 2.5" and the wavefront coherence time equal to 4.8 msec. We provide a
cumulative distribution of the percentage of turbulence developed below H*
where H* is included in the (0,1 km) range. We find that 50% of the whole
turbulence develops in the first 80 m from the ground. The turbulence
decreasing rate is very similar to what has been observed above Mauna Kea.Comment: 12 pages, 6 figures, Proc. SPIE Conference "Ground-based and Airborne
Telescopes III", 27 June 2010, San Diego, California, US
Optical turbulence vertical distribution with standard and high resolution at Mt. Graham
A characterization of the optical turbulence vertical distribution (Cn2
profiles) and all the main integrated astroclimatic parameters derived from the
Cn2 and the wind speed profiles above the site of the Large Binocular Telescope
(Mt. Graham, Arizona, US) is presented. The statistic includes measurements
related to 43 nights done with a Generalized Scidar (GS) used in standard
configuration with a vertical resolution Delta(H)~1 km on the whole 20 km and
with the new technique (HVR-GS) in the first kilometer. The latter achieves a
resolution Delta(H)~20-30 m in this region of the atmosphere. Measurements done
in different periods of the year permit us to provide a seasonal variation
analysis of the Cn2. A discretized distribution of Cn2 useful for the Ground
Layer Adaptive Optics (GLAO) simulations is provided and a specific analysis
for the LBT Laser Guide Star system ARGOS (running in GLAO configuration) case
is done including the calculation of the 'gray zones' for J, H and K bands. Mt.
Graham confirms to be an excellent site with median values of the seeing
without dome contribution epsilon = 0.72", the isoplanatic angle theta0 = 2.5"
and the wavefront coherence time tau0= 4.8 msec. We find that the optical
turbulence vertical distribution decreases in a much sharper way than what has
been believed so far in proximity of the ground above astronomical sites. We
find that 50% of the whole turbulence develops in the first 80+/-15 m from the
ground. We finally prove that the error in the normalization of the
scintillation that has been recently put in evidence in the principle of the GS
technique, affects these measurements with an absolutely negligible quantity
(0.04").Comment: 11 figures. MNRAS, accepte
Methodological Decisions in Undertaking Academic Integrity Policy Analysis: Considerations for Future Research
Purpose: The purpose of this article is to share details of the methodological decisions regarding data collection that a researcher or research team may want to consider when undertaking a policy analysis.
Methods: We have undertaken a meticulous documentation of our decision-making processes throughout the research design process.
Results: We provide narrative evidence of what worked for us as a collaborative research team.
Implications: Understanding the decisions we made throughout our research design and implementation may help other research teams, particularly those working as virtual collaborations and/or those undertaking academic integrity policy analysis
Deep Near-Infrared Imaging of a Field in the Outer Disk of M82 with the ALTAIR Adaptive Optics System on Gemini North
Deep H and K' images, recorded with the ALTAIR adaptive optics system and
NIRI imager on Gemini North, are used to probe the red stellar content in a
field with a projected distance of 1 kpc above the disk plane of the starburst
galaxy M82. The data have an angular resolution of 0.08 arcsec FWHM, and
individual AGB and RGB stars are resolved. The AGB extends to at least 1.7 mag
in K above the RGB-tip, which occurs at K = 21.7. The relative numbers of
bright AGB stars and RGB stars are consistent with stellar evolution models,
and one of the brightest AGB stars has an H-K color and K brightness that is
consistent with it being a C star. The brightnesses of the AGB stars suggest
that they formed during intermediate epochs, possibily after the last major
interaction with M81. Therefore, star formation in M82 during intermediate
epochs may not have been restricted to the plane of the disk.Comment: 16 pages of text plus 7 postscript figures; to appear in the PAS
Book Reviews
BOOK REVIEWS Poverty amidst affluence: Britain and the United States, Vic George and Irving Howards, Aldershot,England, Edward Elgar Publishers, 1991, Reviewed by James Midgley Separate societies: Poverty and inequality in American cities. William W. Goldsmith and Edward J. Blakely,Philadelphia, Temple University Press, 1992, Reviewed by James Midgley The new politics of poverty: The non-working poor in America Lawrence M. Mead, New York, Basic Books, 1992, Reviewed by James Midgley The End of Equality. Mickey Kaus. New York: Basic Books, 1992, Reviewed by David Stoesz The Moral Construction of Poverty: Welfare Reform in America. Joel F. handler and Yeheskel HasenfeldNewbury Park: Sage Publications, 1991, Reviewed by Howard Jacob Karger The Dispossessed: American Underclasses from the Civil War to the Present. Jacqueline Jones, New York: Basic Books, 1992, Reviewed by Henry J. D\u27Souza. 213 Poor Women and Their Families: Hard Working Charity Cases. Beverly Stadum, Albany, New York, State University of New York Press, 1992, Reviewed by Leslie Leighninger From Middle Income to Poor: Downward mobility Among Displaced Steelworkers. Allisojn Zippay, New York, Praeger, 1992, Reviewed by Joel Bla
Interventions for Challenging Behaviours of Students with Autism Spectrum Disorders and Developmental Disabilities: A Synthesis Paper
This synthesis paper summarizes research literature addressing challenging be-haviours in children and youth with autism spectrum disorders and developmental disabilities in school settings. We conducted a comprehensive literature review to identify relevant peer-reviewed articles published between the years 2000 and 2011. The methodological quality of all studies was screened following a stan-dard quality assessment checklist. Intervention effects were assessed quantitatively. Results of quality analysis and intervention effectiveness were in-tegrated to identify interventions with strong support and evidence of effectiveness. We discuss results in terms of implications for intervention choice and implementation in school settings, limitations, and directions for future re-search
Comparison of the atmosphere above the South Pole, Dome C and Dome A: first attempt
The atmospheric properties above three sites (Dome C, Dome A and the South
Pole) on the Internal Antarctic Plateau are investigated for astronomical
applications using the monthly median of the analyses from ECMWF (the European
Centre for Medium-Range Weather Forecasts). Radiosoundings extended on a yearly
time scale at the South Pole and Dome C are used to quantify the reliability of
the ECMWF analyses in the free atmosphere as well as in the boundary and
surface layers, and to characterize the median wind speed in the first 100 m
above the two sites. Thermodynamic instability properties in the free
atmosphere above the three sites are quantified with monthly median values of
the Richardson number. We find that the probability to trigger thermodynamic
instabilities above 100 m is smaller on the Internal Antarctic Plateau than on
mid-latitude sites. In spite of the generally more stable atmospheric
conditions of the Antarctic sites compared to mid-latitude sites, Dome C shows
worse thermodynamic instability conditions than those predicted above the South
Pole and Dome A above 100 m. A rank of the Antarctic sites done with respect to
the strength of the wind speed in the free atmosphere (ECMWF analyses) as well
as the wind shear in the surface layer (radiosoundings) is presented.Comment: Accepted for publishing in MNRAS. 14 pages, 10 figures. The
definitive version is available at http://www.blackwell-synergy.co
Galactic interstellar 18O/17O ratios - a radial gradient?
(Abridged) Our aim is to determine 18O/17O abundance ratios across the entire
Galaxy. These provide a measure of the amount of enrichment by high-mass versus
intermediate-mass stars. Such ratios, derived from the C18O and C17O J=1-0
lines alone, may be affected by systematic errors. Therefore, the C18O and C17O
(1-0), (2-1), and (3-2), as well as the 13CO (1-0) and (2-1) lines, were
observed towards 18 prominent galactic targets (a total of 25 positions). The
combined dataset was analysed with an LVG model, accounting for optical depth
effects. The data cover galactocentric radii R between 0.1 and 16.9 kpc (solar
circle at 8.5 kpc). Near the centre of the Galaxy, 18O/17O = 2.88 +/- 0.11. For
the galactic disc out to an R of ca. 10 kpc, 18O/17O = 4.16 +/- 0.09. At ca. R
= 16.5 kpc, 18O/17O = 5.03 +/- 0.46. Assuming that 18O is synthesised
predominantly in high-mass stars (M > 8 Msun), while C17O is mainly a product
of lower-mass stars, the ratio from the inner Galaxy indicates a dominance of
CNO-hydrogen burning products that is also apparent in the C- and N-isotope
ratios. The high 18O/17O value of the solar system (5.5) relative to that of
the ambient ISM suggests contamination by nearby high-mass stars during its
formation. High values in the metal-poor environment of the outer Galaxy are
not matched by the low values observed towards the even more metal-poor LMC.
Apparently, the outer Galaxy cannot be considered as an intermediate
environment between the solar neighbourhood and the ISM of small metal-poor
galaxies. The apparent 18O/17O gradient along the galactic disc and the
discrepancy between outer disc and LMC isotope ratios may be explained by
different ages of the respective stellar populations.Comment: Accepted by Astron. & Astroph.; 10 pages + 4 pages on-line material
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