350 research outputs found
Toward Fundamental Fairness in the Kangaroo Courtroom: The Due Process Case Against Statutes Presumptively Closing Juvenile Proceedings
Today\u27s juvenile courtroom functions quite differently than did its 1899 Chicago ancestor. During every decade since the 1960s, the juvenile court system has undergone a number of fundamental, structural changes. The most recent of these mega change[s] came during the 1990s, when a number of states abandoned their existing presumptive closure statutes and mandated that juvenile delinquency proceedings be held in the open for the press and the public to see.
The policy reviews of this development have been mixed. Some commentators criticize the recent trend, asserting that open proceedings enervate the juvenile system\u27s ultimate goal of rehabilitating wayward youths. Others laud the new openness, arguing that closure no longer serves the rehabilitative ethic, or that young offenders need to be held accountable to the body politic for their increasingly violent and adult-like wrongs against society. This Note also praises the trend toward openness, but it takes a different tack than do these commentators; it suggests, as the United States Supreme Court suggested in Oliver, that if a person\u27s liberty is at stake, public scrutiny is the only tolerably efficient check against potential abuse or malfunction of the adjudicative process. It argues that, aside from the states\u27 policy-based reasons for abandoning presumptive closure statutes, serious due process problems inhere in presumptive closure schemes. Thus, this Note does not concern itself with the states that have recently overturned their presumptive closure statutes; it instead turns its attention toward the nineteen jurisdictions that retain theirs.
This Note concludes that the nineteen remaining presumptive closure statutes are unconstitutional because they violate the Due Process Clause of the Fourteenth Amendment. The argument proceeds in two major Parts. Part I lays the necessary factual groundwork for the case against the statutes by describing how they affect today\u27s juvenile proceedings. Part II introduces and evaluates three separate-but related-constitutional challenges to the statutes. That is, it briefly acknowledges and rejects First Amendment and Sixth Amendment arguments, and it then raises a freestanding Fourteenth Amendment due process argument. Part II suggests that, while both the First and Sixth Amendment arguments could reasonably be brought to bear on presumptive closure statutes, only the freestanding due process claim has a strong chance of succeeding under existing Supreme Court jurisprudence. This Note concludes that the statutes are fundamentally unfair under that jurisprudence and can no longer withstand constitutional scrutiny
A Reanalysis of theUltraviolet Extinction from Interstellar Dust in the Large Magellanic Cloud
We have reanalyzed the Large Magellanic Cloud's (LMC) ultraviolet (UV)
extinction using data from the IUE final archive. Our new analysis takes
advantage of the improved signal--to--noise of the IUE NEWSIPS reduction, the
exclusion of stars with very low reddening, the careful selection of well
matched comparison stars, and an analysis of the effects of Galactic foreground
dust. Differences between the average extinction curves of the 30 Dor region
and the rest of the LMC are reduced compared to previous studies. We find that
there is a group of stars with very weak 2175 Ang. bumps that lie in or near
the region occupied by the supergiant shell, LMC 2, on the southeast side of 30
Dor. The average extinction curves inside and outside LMC 2 show a very
significant difference in 2175 Ang. bump strength, but their far--UV
extinctions are similar. While it is unclear whether or not the extinction
outside the LMC 2 region can be fit with the relation of Cardelli, Clayton and
Mathis (CCM), sightlines near LMC 2 cannot be fit with CCM due to their weak
2175 Ang. bumps. While the extinction properties seen in the LMC lie within the
range of properties seen in the Galaxy, the correlations of UV extinction
properties with environment seen in the Galaxy do not appear to hold in the
LMC.Comment: 29 pages, 10 figures, to be published in Ap
A programming and a modelling perspective on the evaluation of Java card implementations
Java Card Technology has provided a huge step forward in programming smart cards: from assembler to using a high level Object Oriented language. However, the authors have found some differences between the current Java Card version (2.1) and main stream Java that may restrict the benefits of using Java achievable in smartcard programming. In particular, efforts towards evaluating Java Card implementations at a high level of assurance may be hampered by the presence of these differences as well as by the complexity of the Java Card VM and API. The goal of the present paper is to detail the differences from a programming and a modelling point of view
Dust and Stellar Populations in the Large Magellanic Cloud
We present an analysis of line-of-sight extinction measurements obtained
using data from the Magellanic Clouds Photometric Survey, which provides
4-filter photometry for millions of stars in the Large Magellanic Cloud. We
find that visual extinctions are typically larger by several tenths of a
magnitude for stars with effective temperatures > 12000 K, than for stars with
effective temperatures between 5500 K and 6500 K. Several repercussions of this
population-dependent extinction are discussed. In particular, LMC distance
measurements that utilize old stellar populations (such as red clump stars),
but use extinctions derived from OB stars, may be biased low.
Population-dependent extinction affects the interpretation of color-magnitude
diagrams and results in an effective absorption law that is steeper than that
intrinsic to the dust for unresolved stellar systems. We further explore the
relation between the stellar populations and dust by comparing our extinction
map to the 100mu image of the region and identifying potential heating sources
of the dust. We conclude that 100mu flux should be used with caution as a star
formation tracer, particularly for studies of star formation within galaxies.
Finally, we reproduce the observed extinction variation between the hot and
cold stellar populations with a simple model of the distribution of the stars
and dust where the scaleheight of the cooler stars is >> than that of the dust
(which is twice that of the OB stars). (Abridged Abstract)Comment: Accepted for publication in AJ (scheduled for Dec. 1999). 31 pgs
(including Figures
Ultraviolet Imaging Polarimetry of the Large Magellanic Cloud. II. Models
Motivated by new sounding-rocket wide-field polarimetric images of the Large
Magellanic Cloud, we have used a three-dimensional Monte Carlo radiation
transfer code to investigate the escape of near-ultraviolet photons from young
stellar associations embedded within a disk of dusty material (i.e. a galaxy).
As photons propagate through the disk, they may be scattered or absorbed by
dust. Scattered photons are polarized and tracked until they escape to be
observed; absorbed photons heat the dust, which radiates isotropically in the
far-infrared, where the galaxy is optically thin. The code produces four output
images: near- UV and far-IR flux, and near-UV images in the linear Stokes
parameters Q and U. From these images we construct simulated UV polarization
maps of the LMC. We use these maps to place constraints on the star + dust
geometry of the LMC and the optical properties of its dust grains. By tuning
the model input parameters to produce maps that match the observed polarization
maps, we derive information about the inclination of the LMC disk to the plane
of the sky, and about the scattering phase function g. We compute a grid of
models with i = 28 deg., 36 deg., and 45 deg., and g = 0.64, 0.70, 0.77, 0.83,
and 0.90. The model which best reproduces the observed polarization maps has i
= 36 +2/-5 degrees and g ~0.7. Because of the low signal-to-noise in the data,
we cannot place firm constraints on the value of g. The highly inclined models
do not match the observed centro-symmetric polarization patterns around bright
OB associations, or the distribution of polarization values. Our models
approximately reproduce the observed ultraviolet photopolarimetry of the
western side of the LMC; however, the output images depend on many input
parameters and are nonunique.Comment: Accepted to AJ. 20 pages, 7 figure
Lightcurves of Type Ia Supernovae from Near the Time of Explosion
We present a set of 11 type Ia supernova (SN Ia) lightcurves with dense,
pre-maximum sampling. These supernovae (SNe), in galaxies behind the Large
Magellanic Cloud (LMC), were discovered by the SuperMACHO survey. The SNe span
a redshift range of z = 0.11 - 0.35. Our lightcurves contain some of the
earliest pre-maximum observations of SNe Ia to date. We also give a functional
model that describes the SN Ia lightcurve shape (in our VR-band). Our function
uses the "expanding fireball" model of Goldhaber et al. (1998) to describe the
rising lightcurve immediately after explosion but constrains it to smoothly
join the remainder of the lightcurve. We fit this model to a composite observed
VR-band lightcurve of three SNe between redshifts of 0.135 to 0.165. These SNe
have not been K-corrected or adjusted to account for reddening. In this
redshift range, the observed VR-band most closely matches the rest frame
V-band. Using the best fit to our functional description of the lightcurve, we
find the time between explosion and observed VR-band maximum to be
17.6+-1.3(stat)+-0.07(sys) rest-frame days for a SN Ia with a VR-band Delta
m_{-10} of 0.52mag. For the redshifts sampled, the observed VR-band
time-of-maximum brightness should be the same as the rest-frame V-band maximum
to within 1.1 rest-frame days.Comment: 35 pages, 18 figures, 15 tables; Higher quality PDF available at
http://ctiokw.ctio.noao.edu/~sm/sm/SNrise/index.html; AJ accepte
Background risk of breast cancer and the association between physical activity and mammographic density
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by/4.0
The effects of dust in simple environments: Large Magellanic Cloud HII regions
We investigate the effects of dust on Large Magellanic Cloud (LMC) HII region
spectral energy distributions using arcminute-resolution far-ultraviolet (FUV),
H-alpha, far-infrared (FIR), and radio images. Widely-used indicators of the
amount of light lost to dust (attenuation) at H-alpha and in the FUV correlate
with each other, although often with substantial scatter. There are two
interesting systematic discrepancies. First, H-alpha attenuations estimated
from the Balmer decrement are lower than those estimated from the
H-alpha-to-thermal radio luminosity ratio. Our data, at this stage, cannot
unambiguously identify the source of this discrepancy. Second, the attenuation
at 1500 angstroms and UV spectral slope, beta, correlate, although the slope
and scatter are substantially different from the correlation first derived for
starbursting galaxies by Calzetti et al. Combining our result with those of
Meurer et al. for ultra-luminous infrared galaxies and Calzetti et al. for
starbursting galaxies, we conclude that no single relation between beta and
1500 angstrom attenuation is applicable to all star-forming systems.Comment: 15 pages; 11 embedded postscript figures; 1 GIF figure; to appear in
ApJ on 20 January 2002, vol. 565, no. 1. Section 5.1 (the discussion of the
discrepancies between Balmer-derived and Radio-derived H alpha attenuations)
has changed considerably to take into account small number statistics for
high-mass stars in the model HII region IMFs. The abstract and conclusions
have been modifie
X-Rays from Superbubbles in the Large Magellanic Cloud. V. The H II Complex N11
The large H II complex N11 in the Large Magellanic Cloud contains OB
associations at several different stages in their life histories. We have
obtained ROSAT PSPC and HRI X-ray observations, Curtis Schmidt CCD images,
echelle spectra in H-alpha and [N II] lines, and IUE interstellar absorption
line observations of this region. The central bubble of N11 has an X-ray
luminosity a factor of only 3-7 brighter than predicted for an
energy-conserving superbubble, making this the first detection of X-ray
emission from a superbubble without a strong X-ray excess. The region N11B
contains an extremely young OB association analogous to the central association
of the Carina nebula, apparently still embedded in its natal molecular cloud.
We find that N11B emits diffuse X-ray emission, probably powered by stellar
winds. Finally, we compare the tight cluster HD32228 in N11 to R136 in 30 Dor.
The latter is a strong X-ray source, while the former is not detected, showing
that strong X-ray emission from compact objects is not a universal property of
such tight clusters.Comment: submitted to ApJ 1 April 1997, uses aasms4.sty, 20 pages, 10 figures
(figure 3 is color; figures 1a and 4 are gifs; original postscript available
from
http://www.mpia-hd.mpg.de/MPIA/Projects/THEORY/maclow/papers/n11/n11.htm
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