258 research outputs found
Keynote Address to the Atlas Conference: âInternational Business Disputes In An Era Of Receding Globalismâ
This is a transcript of the luncheon keynote address by Lord Peter Goldsmith at the Sixth Annual Conference of the Atlanta International Arbitration Society (AtlAS) on October 23, 2017.
Lord Peter Goldsmith QC, PC, is London Co-Managing Partner and Chair of European and Asian Litigation at Debevoise & Plimpton LLP. He joined the firm after serving as the UKâs Attorney General from 2001-2007, prior to which he was in private practice as one of the leading barristers in London.
Lord Goldsmith has a long practice in arbitration and in the interface between arbitration and litigation. He appears as counsel for leading cases in a number of jurisdictions and different arbitral institutions, including LCIA, ICC and SIAC and in ad hoc arbitrations. He is closely connected with the LCIA, ICC (for whom he co-chaired the task force on Arbitration for States and State entities), the HKIAC (of which he is Vice chairman), and SIAC. He also has been appointed or confirmed as arbitrator by LCIA, SIAC and the ICC, and is included in the international arbitration database of the Arbitration Center at the Institute of Modern Arbitration, Moscow.
Lord Goldsmith also co-chaired a Task Force on ICC arbitration involving States and State entities, which recommended changes to the ICC rules of arbitration to take account of special issues faced by States in ICC arbitrations. Lord Goldsmith has appeared in numerous cases in the House of Lords, the Privy Council and the Court of Appeal, as well as international and European courts and in the courts of a number of other jurisdictions.
Consistently acknowledged for his prominence, The American Lawyer states that â[he has] the advocacy skills of one of the finest barristers of his generation.â He is recommended as a leading lawyer in Chambers UK and Chambers Global for International Arbitration, Public International Law and Corporate Crime and Investigations. The guides have described him as âexceptionally accomplished,â âbreathtakingly persuasiveâ and âone of the great doyens of the English bar.â
Lord Goldsmith has a strong history and life-long support for pro bono assistance to bring legal expertise to the disadvantaged. As a young lawyer, he started a legal advice center in the East End of London and, later in his career, founded the Bar of England and Walesâ Pro Bono Unit, a nationwide charity providing the free legal services of thousands of barristers (of which he remains President), the Attorney Generalâs pro bono coordinating committees (which coordinates pro bono activity in England and Wales), and became first chair of the Access to Justice Foundation, a cross-profession initiative which raises money to support pro bono organisations across the country and is by statute the sole recipient of pro bono costs award (a role in which he continues).
Lord Goldsmith was a graduate in law from Cambridge University with double first class honours and a Masterâs from University College London. He was admitted to the Bar of England and Wales in 1972, Paris in 1997, Belize in 2010, St. Kitts and Nevis in 2010, New South Wales in 2010 and the British Virgin Islands in 2011. He is also a Registered Foreign Lawyer at the Singapore International Commercial Court
A Herschel/PACS Far Infrared Line Emission Survey of Local Luminous Infrared Galaxies
We present an analysis of [OI]63, [OIII]88, [NII]122 and [CII]158
far-infrared (FIR) fine-structure line observations obtained with
Herschel/PACS, for ~240 local luminous infrared galaxies (LIRGs) in the Great
Observatories All-sky LIRG Survey (GOALS). We find pronounced declines
-deficits- of line-to-FIR-continuum emission for [NII]122, [OI]63 and [CII]158
as a function of FIR color and infrared luminosity surface density,
. The median electron density of the ionized gas in LIRGs,
based on the [NII]122/[NII]205 ratio, is = 41 cm. We find
that the dispersion in the [CII]158 deficit of LIRGs is attributed to a varying
fractional contribution of photo-dissociation-regions (PDRs) to the observed
[CII]158 emission, f([CII]PDR) = [CII]PDR/[CII], which increases from ~60% to
~95% in the warmest LIRGs. The [OI]63/[CII]158PDR ratio is tightly correlated
with the PDR gas kinetic temperature in sources where [OI]63 is not
optically-thick or self-absorbed. For each galaxy, we derive the average PDR
hydrogen density, , and intensity of the interstellar radiation
field, in units of G, and find G/ ratios ~0.1-50 cm,
with ULIRGs populating the upper end of the distribution. There is a relation
between G/ and , showing a critical break at
~ 5 x 10 Lsun/kpc. Below , G/ remains constant, ~0.32 cm, and variations
in are driven by the number density of star-forming regions
within a galaxy, with no change in their PDR properties. Above , G/ increases rapidly with ,
signaling a departure from the typical PDR conditions found in normal
star-forming galaxies towards more intense/harder radiation fields and compact
geometries typical of starbursting sources.Comment: 23 pages, 12 figures. Submitted to ApJ, including 2nd round of
referee comments. Data tables can be found at: http://goals.ipac.caltech.edu/
and will also appear on the electronic version of the journa
The CHESS chemical Herschel surveys of star forming regions: Peering into the protostellar shock L1157-B1. I. Shock chemical complexity
We present the first results of the unbiased survey of the L1157-B1 bow
shock, obtained with HIFI in the framework of the key program Chemical Herschel
surveys of star forming regions (CHESS). The L1157 outflow is driven by a
low-mass Class 0 protostar and is considered the prototype of the so-called
chemically active outflows. The bright blue-shifted bow shock B1 is the ideal
laboratory for studying the link between the hot (around 1000-2000 K) component
traced by H2 IR-emission and the cold (around 10-20 K) swept-up material. The
main aim is to trace the warm gas chemically enriched by the passage of a shock
and to infer the excitation conditions in L1157-B1. A total of 27 lines are
identified in the 555-636 GHz region, down to an average 3 sigma level of 30
mK. The emission is dominated by CO(5-4) and H2O(110-101) transitions, as
discussed by Lefloch et al. (2010). Here we report on the identification of
lines from NH3, H2CO, CH3OH, CS, HCN, and HCO+. The comparison between the
profiles produced by molecules released from dust mantles (NH3, H2CO, CH3OH)
and that of H2O is consistent with a scenario in which water is also formed in
the gas-phase in high-temperature regions where sputtering or grain-grain
collisions are not efficient. The high excitation range of the observed tracers
allows us to infer, for the first time for these species, the existence of a
warm (> 200 K) gas component coexisting in the B1 bow structure with the cold
and hot gas detected from ground
Nitrogen hydrides in the cold envelope of IRAS16293-2422
Nitrogen is the fifth most abundant element in the Universe, yet the
gas-phase chemistry of N-bearing species remains poorly understood. Nitrogen
hydrides are key molecules of nitrogen chemistry. Their abundance ratios place
strong constraints on the production pathways and reaction rates of
nitrogen-bearing molecules. We observed the class 0 protostar IRAS16293-2422
with the heterodyne instrument HIFI, covering most of the frequency range from
0.48 to 1.78~THz at high spectral resolution. The hyperfine structure of the
amidogen radical o-NH2 is resolved and seen in absorption against the continuum
of the protostar. Several transitions of ammonia from 1.2 to 1.8~THz are also
seen in absorption. These lines trace the low-density envelope of the
protostar. Column densities and abundances are estimated for each hydride. We
find that NH:NH2:NH3=5:1:300. {Dark clouds chemical models predict steady-state
abundances of NH2 and NH3 in reasonable agreement with the present
observations, whilst that of NH is underpredicted by more than one order of
magnitude, even using updated kinetic rates. Additional modelling of the
nitrogen gas-phase chemistry in dark-cloud conditions is necessary before
having recourse to heterogen processes
Herschel observations of extra-ordinary sources: Detecting spiral arm clouds by CH absorption lines
We have observed CH absorption lines ()
against the continuum source Sgr~B2(M) using the \textit{Herschel}/HIFI
instrument. With the high spectral resolution and wide velocity coverage
provided by HIFI, 31 CH absorption features with different radial velocities
and line widths are detected and identified. The narrower line width and lower
column density clouds show `spiral arm' cloud characteristics, while the
absorption component with the broadest line width and highest column density
corresponds to the gas from the Sgr~B2 envelope. The observations show that
each `spiral arm' harbors multiple velocity components, indicating that the
clouds are not uniform and that they have internal structure. This
line-of-sight through almost the entire Galaxy offers unique possibilities to
study the basic chemistry of simple molecules in diffuse clouds, as a variety
of different cloud classes are sampled simultaneously. We find that the linear
relationship between CH and H column densities found at lower by UV
observations does not continue into the range of higher visual extinction.
There, the curve flattens, which probably means that CH is depleted in the
denser cores of these clouds.Comment: Accepted for publication in A&A, HIFI Special Issu
Reversal of infall in SgrB2(M) revealed by Herschel/HIFI observations of HCN lines at THz frequencies
To investigate the accretion and feedback processes in massive star
formation, we analyze the shapes of emission lines from hot molecular cores,
whose asymmetries trace infall and expansion motions. The high-mass star
forming region SgrB2(M) was observed with Herschel/HIFI (HEXOS key project) in
various lines of HCN and its isotopologues, complemented by APEX data. The
observations are compared to spherically symmetric, centrally heated models
with density power-law gradient and different velocity fields (infall or
infall+expansion), using the radiative transfer code RATRAN. The HCN line
profiles are asymmetric, with the emission peak shifting from blue to red with
increasing J and decreasing line opacity (HCN to HCN). This is most
evident in the HCN 12--11 line at 1062 GHz. These line shapes are reproduced by
a model whose velocity field changes from infall in the outer part to expansion
in the inner part. The qualitative reproduction of the HCN lines suggests that
infall dominates in the colder, outer regions, but expansion dominates in the
warmer, inner regions. We are thus witnessing the onset of feedback in massive
star formation, starting to reverse the infall and finally disrupting the whole
molecular cloud. To obtain our result, the THz lines uniquely covered by HIFI
were critically important.Comment: A&A, HIFI special issue, accepte
Nitrogen hydrides in interstellar gas: Herschel/HIFI observations towards G10.6-0.4 (W31C)
The HIFI instrument on board the Herschel Space Observatory has been used to
observe interstellar nitrogen hydrides along the sight-line towards G10.6-0.4
in order to improve our understanding of the interstellar chemistry of
nitrogen. We report observations of absorption in NH N=1-0, J=2-1 and ortho-NH2
1_1,1-0_0,0. We also observed ortho-NH3 1_0-0_0, and 2_0-1_0, para-NH3 2_1-1_1,
and searched unsuccessfully for NH+. All detections show emission and
absorption associated directly with the hot-core source itself as well as
absorption by foreground material over a wide range of velocities. All spectra
show similar, non-saturated, absorption features, which we attribute to diffuse
molecular gas. Total column densities over the velocity range 11-54 km/s are
estimated. The similar profiles suggest fairly uniform abundances relative to
hydrogen, approximately 6*10^-9, 3*10^-9, and 3*10^-9 for NH, NH2, and NH3,
respectively. These abundances are discussed with reference to models of
gas-phase and surface chemistry.Comment: 5 pages, 3 figures, 2 online pages with 2 figures. Accepted for
publication in A&A July 6 (Herschel/HIFI special issue
Herschel observations of deuterated water towards Sgr B2(M)
Observations of HDO are an important complement for studies of water, because
they give strong constraints on the formation processes -- grain surfaces
versus energetic process in the gas phase, e.g. in shocks. The HIFI
observations of multiple transitions of HDO in Sgr~B2(M) presented here allow
the determination of the HDO abundance throughout the envelope, which has not
been possible before with ground-based observations only. The abundance
structure has been modeled with the spherical Monte Carlo radiative transfer
code RATRAN, which also takes radiative pumping by continuum emission from dust
into account. The modeling reveals that the abundance of HDO rises steeply with
temperature from a low abundance () in the outer envelope
at temperatures below 100~K through a medium abundance () in
the inner envelope/outer core, at temperatures between 100 and 200~K, and
finally a high abundance () at temperatures above 200~K in
the hot core.Comment: A&A HIFI special issue, accepte
Herschel observations of extra-ordinary sources: Detection of Hydrogen Fluoride in absorption towards Orion~KL
We report a detection of the fundamental rotational transition of hydrogen
fluoride in absorption towards Orion KL using Herschel/HIFI. After the removal
of contaminating features associated with common molecules ("weeds"), the HF
spectrum shows a P-Cygni profile, with weak redshifted emission and strong
blue-shifted absorption, associated with the low-velocity molecular outflow. We
derive an estimate of 2.9 x 10^13 cm^-2 for the HF column density responsible
for the broad absorption component. Using our best estimate of the H2 column
density within the low-velocity molecular outflow, we obtain a lower limit of
~1.6 x 10^-10 for the HF abundance relative to hydrogen nuclei, corresponding
to 0.6% of the solar abundance of fluorine. This value is close to that
inferred from previous ISO observations of HF J=2--1 absorption towards Sgr B2,
but is in sharp contrast to the lower limit of 6 x 10^-9 derived by Neufeld et
al. (2010) for cold, foreground clouds on the line of sight towards G10.6-0.4.Comment: 5 pages, 3 figures, paper to be published in the Herschel special
issue of A&A letter
Herschel observations of EXtra-Ordinary Sources: The Terahertz spectrum of Orion KL seen at high spectral resolution
We present the first high spectral resolution observations of Orion KL in the
frequency ranges 1573.4 - 1702.8 GHz (band 6b) and 1788.4 - 1906.8 GHz (band
7b) obtained using the HIFI instrument on board the Herschel Space Observatory.
We characterize the main emission lines found in the spectrum, which primarily
arise from a range of components associated with Orion KL including the hot
core, but also see widespread emission from components associated with
molecular outflows traced by H2O, SO2, and OH. We find that the density of
observed emission lines is significantly diminished in these bands compared to
lower frequency Herschel/HIFI bands.Comment: Accepted for publication in the Herschel HIFI special issue of
Astronomy and Astrophysics Letters, 5 pages, 3 figure
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