2,254 research outputs found
Litigation in 2050: A Backward-Forward, Topsy-Turvy Look at Dispute Resolutions
Litigation in 2050: A Backward, Forward, Topsy-Tury Look at Dispute Resolutions was originally comissioned by the American Bar Association Center for Professional Responsibility. Along with two companion pieces reflecting varying perspectives on the same subject, it was presented as part of the Seventeenth Annual Conference on Professional Responsibility, presented at Scottsdale, Arizona, June 6-9, 1991. It appears here with the permission of the American Bar Association
Ethics Bureau at Yale: Combining Pro Bono Professional Responsibility Advice with Ethics Education
The SCUBA 8-mJy survey - I: Sub-millimetre maps, sources and number counts
We present maps, source lists, and number counts from the largest, unbiassed,
extragalactic sub-mm survey so far undertaken with the SCUBA camera on the
JCMT. Our maps cover 260 sq. arcmin, to a noise level S(850)=2.5 mJy/beam. We
have reduced the data using both SURF, and our own pipeline which produces
zero-footprint maps and noise images. The uncorrelated noise maps produced by
the latter approach have allowed application of a maximum-likelihood method to
measure the statistical significance of each peak, leading to properly
quantified flux-density errors for all potential sources. We detect 19 sources
with S/N > 4, 38 with S/N > 3.5, and 72 with S/N > 3. To assess completeness
and the impact of source confusion we have applied our source extraction
algorithm to a series of simulated images. The result is a new estimate of the
sub-mm source counts in the flux-density range S(850)=5-15mJy, which we compare
with other estimates, and with model predictions. Our estimate of the
cumulative source count at S(850) > 8 mJy is 320 (+80,-100) per square degree.
Assuming that the majority of sources have z > 1.5, the co-moving number
density of high-z galaxies forming stars at a rate >1000 solar masses per year
is 10^-5 per Mpc^3, with only a weak dependence on the precise redshift
distribution. This number density corresponds to that of massive ellipticals
with L > 3-4 L* at low redshift and is also the same as the co-moving number
density of comparably massive, passively-evolving objects in the redshift band
1<z<2 inferred from recent surveys of extremely red objects. Thus the bright
sub-mm sources can plausibly account for the formation of all present-day
massive ellipticals. Improved z constraints, and a proper measurement of sub-mm
clustering can refine or refute this picture.Comment: Minor revisions. 27 pages, 13 figures. Higher resolution versions of
Figs 5,6,7 and 8 are available from the autho
The SCUBA 8-mJy survey - II: Multiwavelength analysis of bright sub-mm sources
We present the results of a multi-wavelength study of the 19 most significant
sub-mm sources detected in the SCUBA 8-mJy survey. As described in Scott et al.
(2001), this survey covers ~260 arcmin^2 using the sub-millimetre camera SCUBA,
to a limiting source detection limit S(850um) ~ 8 mJy. One advantage of this
relatively bright flux-density limit is that accurate astrometric positions are
potentially achievable for every source using existing radio and/or mm-wave
interferometers. However, an associated advantage is that SED-based redshift
constraints should be more powerful than in fainter sub-mm surveys. Here we
therefore exploit the parallel SCUBA 450um data, in combination with existing
radio and ISO data at longer and shorter wavelengths to set constraints on the
redshift of each source. We also analyse new and existing optical and
near-infrared imaging of our SCUBA survey fields to select potential
identifications consistent with these constraints. Our derived SED-based
redshift constraints, and the lack of statistically significant associations
with even moderately bright galaxies allow us to conclude that all 19 sources
lie at z > 1, and at least half of them apparently lie at z > 2.Comment: 14 pages (including 30 figures and 4 tables) accepted by MNRAS.
Figure 1 and 2 and a higher quality version of the full paper are available
at http://astro.ic.ac.uk/~mfox
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