text:
Tagged: Trump
Israel Approves 1900 Settler Homes
On Sunday Israel approved the construction of over 1900 new illegal Jewish-only settlement units on Palestinian land. These settlements steal vital resources from Palestinians are completely off limits to those living under occupation in the West Bank
Last week, President Donald Trump issued an executive order conflating criticism of Israel on university campuses with antisemitism and threatening to cut off funding to institutions that allow campaigns in support of Palestinian human rights. The IMEU offers the following expert Q&A with attorney Dima Khalidi, founder and director of Palestine Legal and Cooperating Counsel with the Center for Constitutional Rights (CCR), explaining what the executive order consists of and the dangers it poses to human rights activism and free speech on campus.
Sebastian Cahill, the Daily Californian
UC Berkeley student group protests executive order on anti-Semitism
Last week Berkeley students rallied against Trump's executive order targeting critics of Israel, "As a Jewish person, it's important to speak out about issues like this because silencing Palestinians does nothing to keep me safe as a Jewish person..."
Nora Barrows-Friedman, Electronic Intifada
Trump appeases Israel lobby with executive order
Trump's executive order meets the demands of Israel lobby groups who wish to criminalize Palestine solidarity organizing – especially on US college campuses – by conflating criticism of Israel with anti-Jewish bigotry.
Trump wants to shoot asylum seekers in the legs
Trump's brutal fantasy is Gaza's wretched reality. Israeli snipers target the legs of Palestinians marching for their rights in Gaza. At least 6,392 Palestinians have been shot in their lower limbs by Israeli forces since March 2018, the start of the Great Return March.
Loveday Morris, The Washington Post
Kushner Presents Vision of a Middle East at Peace but No Details How to Get There
President Trump's adviser and son-in-law, Jared Kushner, presented a vision Tuesday of a new prosperity for the Middle East if peace could be achieved between Israelis and Palestinians but did not reveal how the White House plans to achieve such a political settlement.
Denied Entry to US, Palestinian Diplomat Hanan Ashrawi on US "Peace Plan" & Israeli Political Crisis
Israel will hold new elections after Prime Minister Benjamin Netanyahu failed to form a coalition government in six weeks of negotiations following the April 9 election. This marks the first time in Israeli history a prime minister-designate has failed to form a coalition government.
https://imeu.org/article/tag/Trump/
{/exp:tag:entries}


text:
Home › Sport › Motor Sport
Boyd revved up for glory bid after switch to Le Mans Cup
Title tilt: Wayne Boyd is confident of making title push
By Sammy Hamill
Wayne Boyd is staying with the United Autosports team for a third season but will move to the Michelin Le Mans Cup series.
https://www.belfasttelegraph.co.uk/sport/motor-sport/boyd-revved-up-for-glory-bid-after-switch-to-le-mans-cup-36656610.html
https://www.belfasttelegraph.co.uk/incoming/article36656749.ece/4193c/AUTOCROP/h342/wayneboyd.jpg
The former British Formula Ford champion has driven for the Anglo-American team in the European Le Mans championship for the past two years, piloting an LMP3 Ligier-Nissan to several podium finishes and victory at Portimao in Portugal at the end of last season.
But now he will switch to the Le Mans Cup which runs alongside the ELMS championship and will partner experienced amateur racer Richard Meins for the six round series which features LMP3 and GT3 cars.
Boyd will continue to drive a prototype LMP3 Ligier and sees the move to the Le Mans Cup as having benefits.
"I followed the Le Mans Cup races closely last year and although it's a really competitive series I'm confident we will be pushing for the championship," he said.
"I get on really well with Richard and he's a great driver so I'm looking forward to working with him.
"One of the benefits of the move is we will be challenging for outright race wins and won't have to be looking over our shoulders for the faster LMP2 cars like in the ELMS races.
"There will also be the opportunity to drive at Le Mans, not in the main 24-hour race but in the build-up event on the Saturday morning. Maybe I'll get the chance to drive in the big race sometime in the future."
The Cup races last two hours and will take place at Monza (Italy), Red Bull Ring (Austria), Le Castellet (France), Spa-Francorchamps (Belgium) and Portimao (Portugal).
Meanwhile Boyd's fellow Ulsterman Richard Lyons will continue with his long distance commute from Lisburn to the Far East to race in the Super GT championship in Japan.
The former Formula Nippon and Japanese GT500 champion is staying with the Hitostsuyama team for a fourth season driving a GT300 Audi R8 but will have a new partner, Ryuichiro Tomit.
Greer has sights on a surprise Down Rally double
By Sammy Hamill Jonny Greer surprised even himself when he won last year's Down Rally - and he will surely be equally shocked if he can repeat the performance this weekend.
British GP is set to move date to avoid clash with other big events
By Philip Duncan Next year's British Grand Prix is set to be moved, avoiding a direct clash with the Wimbledon men's singles final and football's Euro 2020 final at Wembley.
Jonathan Rea 'super satisfied' after strengthening World Superbike lead over arch-rival Bautista
Jonathan Rea missed out on another World Superbike treble at Laguna Seca but further strengthened his grip on the world championship lead.
Moffett closes in on National title with five wins out of six
By Sammy Hamill Josh Moffett has moved to within touching distance of adding the Irish National Rally Championship to the Tarmac and Forestry titles he won in 2018 with a start to finish victory in Sligo yesterday.

redpajama_set_name: RedPajamaCommonCrawl


I have an LG G4 mobile phone handset (bought as part of a contract August 2015).
Stupidly I had my photos split over an sd card and internal memory, with most of them on the internal phone memory (along with all my numbers saved to the phone too).
There are some really sentimental photos on there that I know aren't on my SD card, and am desperate to get them!
2 – how much would it be?
Windows failed to start. A recent hardware or software change may be to blame.
Then it moves to a screen saying Windows is loading files….
Then moves to a blue windows screen but is unresponsive.
The HDD is a Seagate Momentus 5400.6, 250GB.
My IT department have installed a new HDD in my laptop but as I hadn't backed up the old one for several weeks I would be interested in recovery if possible/cost effective.
Would appreciate email response initially as I cannot take calls at the moment.
I am based relatively local and could bring the HDD in on Wednesday.
Can you provide an indication of cost associated with the recovery and/or any guarantee offered?
I dropped my Seagate 2TB external hard-drive the other day and now it's not powering on at all. I'm not sure if the drive itself is scratched or if it's not able to power up. There's no light coming on when I plug the power in, so assumed it was a power problem.
Do you think you would be able to take a look at it if possible?
An email response would be better than a phonecall if possible, thank you.


text:
Andrea Levy
Contemporary Critical Perspectives
James David James
Andrea Levy has emerged as one of the most significant and popular voices in contemporary black British writing both in the UK and abroad. Drawing on a familial history of emigration, her critically-acclaimed novels - including the multiple award-winning Small Island - attempt to bring a variety of voices to the representation of black experience in post-war Britain. This book is the first of its kind to be devoted to Levy's work. Combining historical, theoretical and textual perspectives, the volume hosts a wide range of current critical approaches to Levy's fiction. With chapters written by leading established and emerging scholars, the book explores issues of literary form, diasporic literature and cultural value, the BBC TV adaptation of Small Island, while also shedding fresh light on Levy's critically neglected early works. The book also includes a new interview with Levy herself, a timeline of her life, chapter summaries, as well as guides to further reading and online resources, making this an essential companion to the writings of one of the most exciting voices in contemporary fiction.


text:
Sub-categories of "technology"
Sub-categories of "urban"
Filtering for technology (remove)
Filtering for urban (remove)
15 Results Found · Page 1 of 2 · Next Page
Opinion: Disruptive Technologies for Climate Action
2019/06 – United Nations University, Institute for Environment and Human Security (UNU-EHS); Press Release; Author(s): UNU-EHS
Details for "Opinion: Disruptive Technologies for Climate Action"
Opinion: « Le concept de "Smart City" n'est plus opérant »
2018 – Institut du développement durable et des relations internationales (IDDRI); Author(s): Mathieu Saujot, Thierry Marcou
Details for "Opinion: « Le concept de "Smart City" n'est plus opérant »"
Sources of Productivity Differentials in Manufacturing in Post-Transition Urban South-East Europe (PDF)
2017/11 – Economic Institute Zagreb (EIZ); EIZ-WP-1706; Author(s): Katarina Bačić, Ivana Rašić Bakarić and Sunčana Slijepčević
Details for "Sources of Productivity Differentials in Manufacturing in Post-Transition Urban South-East Europe (PDF)"
Community Development Planning: Success and Failure in the Extractive Sector
2017/02 – United Nations University World Institute for Development Economics Research (UNU-WIDER); Volume 2017, Issue 1; Author(s): Unu-Wider
Details for "Community Development Planning: Success and Failure in the Extractive Sector"
The Employment Dimension of Infrastructure Investments: A Guide for Employment Impact Assessment
2015/11 – International Labour Organization (ILO); Employment Working Paper No. 178; Author(s): Christoph Ernst; Steve Miller; Marc van Imschoot
Details for "The Employment Dimension of Infrastructure Investments: A Guide for Employment Impact Assessment"
Automatic Building Detection Using Oblique Imagery (pdf)
2013/04 - University of Twente - Faculty of Geo-Information Science and Earth Observation (ITC); Dissertation No.224; Author: Jing Xiao
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Innover et gouverner dans la ville numérique réelle
2018/04 – Institut du développement durable et des relations internationales (IDDRI); research paper; Author(s): Marine Albarede, et al.
Details for "Innover et gouverner dans la ville numérique réelle"
Technology and Cities: What Type of Development is Appropriate for Cities in the South
2012/09 - Ecole Polytechnique Federale de Lausanne (EPFL), Author(s): Bolay, J.-C. and Kern, A.-L.
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Technology and Cities: What Type of Development Is Appropriate for Cities of the South? (pdf)
2012/01 - Ecole Polytechnique Federale de Lausanne (EPFL), Author(s): Jean-Claude Bolay and Abigaı¨l Kern
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Emerging Realities in the European Space: Complexity, Mobility and Intercultural Dynamics
2011/09 - Center for International Relations and Development Studies (CIDOB); CIDOB Journal of Afers Internacionals, No. 95; Coordinator: Yolanda Onghena
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text:
\section{Introduction}

Recent studies have made great strides in inventorying molecular gas, the fuel for star formation, in galaxies during the peak epoch of cosmic star formation, redshift (z) $\sim$ 1-3, in an effort to determine the efficiency with which these galaxies convert their molecular gas reservoirs into stars \citep[e.g.,][]{Tacconi2010, Harris2012, Sharon2016, Harrington2018, Pavesi2018}. These surveys are complicated by the fact that hydrogen, whose lowest rotational transition takes $\sim$ 500 K to excite, is difficult to observe in cold molecular clouds, so that the easily-excited low-J rotational levels of carbon-monoxide (CO) are generally used as a proxy for molecular gas content. Under some interstellar medium (ISM) conditions however, appreciable amounts of molecular hydrogen are not accompanied by CO. These so-called ``CO-dark" molecular clouds are troublesome in that they cause galaxies containing them to appear very gas poor when employing CO-derived gas-mass estimates. Several possible explanations for these CO-dark molecular clouds exist, including low-metallicity gas present within the ISM of galaxies \citep[e.g.,][]{Maloney1988, Stacey1991} and highly-fractionated molecular clouds \citep[e.g.,][]{Storzer1997}. Here we investigate one such CO-dark galaxy, 3C 368 \citep[e.g.,][]{Evans1996, Lamarche2017}, which has an appreciable star-formation rate and seemingly very little molecular gas.

3C 368 was discovered as part of the Third Cambridge Radio Catalog \citep{Edge1959} and has come to be known as one of the archetypal Fanaroff-Riley class II (FR-II) galaxies. It is an interesting source, situated within the peak epoch of cosmic star-formation, forming stars at a rate of $\sim$ 350 $M_{\odot}$ yr$^{-1}$ \citep{Podigachoski2015}, and containing an active galactic nucleus (AGN) that has launched radio-emitting lobes which span $\sim$ 73 kpc \citep{Best1998}.

In \cite{Lamarche2017} we used both mid- and far-infrared (FIR) fine-structure line observations of 3C 368 to infer the age of the young stellar component present within the source, finding an age of $\sim$ 6.5 Myrs, consistent with that determined using a multi-component model for the observed UV-FIR spectral energy distribution (SED) \citep{Drouart2016}. We also presented a non-detection of the CO(2-1) line, constraining the CO luminosity to a level twelve times lower than expected in star-forming galaxies, based on standard ratios with the [C\,{\sc ii}] 158 $\micron$ line \citep[e.g.,][]{Stacey1991}, which we attributed to either a low-metallicity or highly-fractionated interstellar medium (ISM). In this follow-up paper, we present observations of the CO(4-3) and [C\,{\sc i}](1-0) 609 $\micron$ spectral lines, which emanate from molecular clouds and photo-dissociation regions (PDRs), respectively, as well as the dust continuum emission at 480.5\,GHz (rest-frame), in 3C 368, and show how these measurements help us to disentangle these two competing scenarios.

We assume a flat $\Lambda$CDM cosmology, with $\Omega_M$ = 0.27, $\Omega_\Lambda$ = 0.73, and H$_0$ = 71\,km\,s$^{-1}$\,Mpc$^{-1}$, throughout this paper \citep{Spergel2003}.

\section{Observations and Data Reduction}

\subsection{ALMA}

The CO(4-3) and [C\,{\sc i}] 609 $\micron$ lines were observed simultaneously in 3C 368, using the Atacama Large Millimeter/submillimeter Array (ALMA)\footnote{The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.} band-6 receivers. The observations were split into two separate execution blocks: the first conducted on June 3, 2016, with a precipitable water vapor (PWV) measurement of 1.24 mm and baselines up to 772 m, and the second conducted on August 20, 2016, with a PWV of 0.31 mm and baselines up to 1462 m. The total on-source integration time for these two observations was $\sim$ 1 hour and 40 minutes.

For both execution blocks, J1751+0939 (PKS 1749 +096) was used as the bandpass, flux, and phase calibrator. The data from the two execution blocks were reduced using the Common Astronomy Software Application (CASA)\footnote{https://casa.nrao.edu/} ALMA pipeline, version 38366 (C4 --- R2B), run in CASA version 4.7.0, and subsequently combined, imaged, and cleaned, using CASA version 4.7.2.

Imaging the CO(4-3) measurement set at a spectral resolution of 60 km s$^{-1}$, and employing a robust parameter of 0.5, we obtain an RMS sensitivity of 120 $\mu$Jy beam$^{-1}$ in each spectral channel, with a synthesized beam of size 0$\farcs$41 $\times$ 0$\farcs$31.

The [C\,{\sc i}] 609 $\micron$ measurement set was similarly imaged at 60 km s$^{-1}$ spectral resolution, employing a robust parameter value of 0.5. Here we obtain an RMS sensitivity of 130 $\mu$Jy beam$^{-1}$ in each spectral channel, with a synthesized beam of size 0$\farcs$39 $\times$ 0$\farcs$29.

A continuum image was created by combining the two line-free spectral windows present in the measurement set, for a total continuum bandwidth of $\sim$\,4\,GHz, centered at 225.5\,GHz (observed-frame). Imaging with a robust parameter value of 0.5, as was done for the line data, we obtain an RMS noise of 13 $\mu$Jy beam$^{-1}$, with a beam of size 0$\farcs$38 $\times$ 0$\farcs$29.

\section{Results and Discussion}

\subsection{Line and Continuum Fluxes}

Both the CO(4-3) and [C\,{\sc i}] 609 $\micron$ lines are well detected in our ALMA observations, emanating from the core component of 3C 368. A continuum-subtracted moment-zero map was created for each of the two spectral lines (see Figure 1), with the corresponding line fluxes determined by fitting a two-dimensional Gaussian to the emitting region of each moment-zero map. We obtain a CO(4-3) line flux of 1.08 $\pm$ 0.14 Jy km s$^{-1}$, or equivalently (7.8 $\pm$ 1.0) x 10$^{-21}$ W m$^{-2}$, and a [C\,{\sc i}] 609 $\micron$ line flux of 0.85 $\pm$ 0.09 Jy km s$^{-1}$, or equivalently (6.6 $\pm$ 0.7) x 10$^{-21}$ W m$^{-2}$ (see Table 1). These fluxes were verified by numerically integrating the spectra extracted from an aperture containing the core of 3C 368 (see Figure 3) and were found to be consistent within the quoted uncertainties.

The continuum in 3C 368 is resolved into three components in the 225.5\,GHz (observed-frame) map: the northern lobe at 226 $\pm$ 59 $\mu$Jy, the southern lobe at 128 $\pm$ 28 $\mu$Jy, and the core at 96 $\pm$ 21 $\mu$Jy (see Figure 2 and Table 1), where these flux densities were determined by fitting a two-dimensional Gaussian to each component in the continuum image. We note that continuum flux extended around the core component of 3C 368 at the same spatial scales as the [C\,{\sc i}] and CO emission could be resolved out at the resolution and sensitivity of our observations, making the quoted flux density from the core a lower limit on the true value.

\begin{figure*}
\gridline{\fig{3C368_CO43_mom0_contsub.png}{0.5\textwidth}{(a)}
          \fig{3C368_CI609_mom0_contsub.png}{0.5\textwidth}{(b)}
          }
\caption{(a) ALMA CO(4-3) moment-zero map showing the core component of 3C 368 at 0$\farcs$4 resolution. The CO-emitting source has a size of 0$\farcs$77 $\times$ 0$\farcs$46, deconvolved from the beam. (b) ALMA [C\,{\sc i}] 609 $\micron$ moment-zero map showing the same region of 3C 368 at 0$\farcs$4 resolution. The deconvolved [C\,{\sc i}]-emitting source size is 0$\farcs$43 $\times$ 0$\farcs$23.}
\end{figure*}

\begin{figure}
\plotone{3C368_cont_1256_map_with_Best_radio_contours.png}
\caption{ALMA 225.5\,GHz (observed-frame) continuum colormap of 3C 368 at 0$\farcs$4 resolution. The source is resolved into three components: a core, a northern lobe, and a southern lobe, co-spatial with those seen in 8.21 GHz (observed-frame) radio-continuum emission \citep[contour map;][]{Best1998}. The core component of 3C 368 is unresolved at this resolution and sensitivity.}
\end{figure}

\begin{figure}
\plotone{3C368_CO43_and_CI609um_contsub.pdf}
\caption{Continuum-subtracted ALMA spectra of both the CO(4-3) and [C\,{\sc i}] 609 $\micron$ lines extracted from the core component of 3C 368. v = 0 corresponds to z = 1.131.}
\end{figure}

\begin{deluxetable*}{ccccc}
\tablecaption{Spectral-line and continuum observations of 3C 368}
\tablecolumns{5}
\tablenum{1}
\tablehead{
\colhead{Observation} & \colhead{Core} & \colhead{N. Lobe} & \colhead{S. Lobe} & \colhead{Unit}\\
}
\startdata
CO(4-3) & 7.8\,$\pm$\,1.0 & - & - & F$_{obs}$\,($10^{-21}$\,W\,m$^{-2}$) \\
'' & 4.6\,$\pm$\,0.6 & - & - & L'\,(10$^{9}$\,K\,km\,s$^{-1}$\,pc$^2$) \\\relax
[C\,{\sc i}](1-0) & 6.6\,$\pm$\,0.7 & - & - & F$_{obs}$\,($10^{-21}$\,W\,m$^{-2}$) \\
'' & 3.2\,$\pm$\,0.3 & - & - & L'\,(10$^{9}$\,K\,km\,s$^{-1}$\,pc$^2$) \\
Continuum ($\nu_{obs}$ = 225.5\,GHz) & 96$\pm$21 & 226$\pm$59 & 128$\pm$28 & $S_{\nu, obs}$\,($\mu$Jy) \\
\enddata
\tablecomments{These flux and flux-density values were determined by fitting two-dimensional Gaussian profiles to the respective maps for each of the source components within 3C 368 (see the text).}
\end{deluxetable*}

\subsection{Continuum Science}

\subsubsection{Spectral Energy Distribution}
Using the ALMA continuum observations centered at 480.5\,GHz (rest-frame) presented here, together with our previous ALMA continuum measurements at 205 $\micron$ \citep[rest-frame;][]{Lamarche2017}, we can calculate the slope of the Rayleigh-Jeans power-law for the thermal dust continuum of 3C 368. This is particularly interesting in this case, since the core component of 3C 368, the star-forming galaxy, makes up the smallest contribution to the continuum flux at rest-frame 480.5\,GHz, the flux being dominated instead by the radio lobes. Hence, unresolved continuum measurements at mm/sub-mm wavelengths may have overestimated the flux from the core of 3C 368. We obtain a Rayleigh-Jeans power-law index, S$_\nu$ $\sim$ $\nu^\alpha$, of 3.7 $\pm$ 0.4, or equivalently a dust-emissivity $\beta$ value, S$_\nu$ $\sim$ $\nu^{2 + \beta}$, of 1.7 $\pm$ 0.4. This is consistent with the dust-emissivity $\beta$ value assumed in \cite{Podigachoski2015}, who used that value to derive an FIR luminosity of 2.0 $\times$ 10$^{12}$ $L_{\odot}$, which we used in our previous work and will adopt throughout this paper.

We can also decompose the radio spectral energy distribution (SED) from the core of 3C 368 into thermal and nonthermal components, using our previous ALMA 230 GHz (rest-frame) continuum observations \citep{Lamarche2017}, together with radio continuum observations at 8.21 and 4.71 GHz (observed-frame) \citep{Best1998}, using an equation of the following form \citep[e.g.,][]{Condon1992, Klein2018}:

\begin{equation}
S_{total, r} = S_{th, 0, r} \bigg( \frac{\nu}{\nu_{0,r}} \bigg) ^{-0.1} + S_{nth, 0, r} \bigg( \frac{\nu}{\nu_{0,r}} \bigg) ^{-\alpha_{nth}}
\end{equation}

where $S_{th,0,r}$ and $S_{nth,0,r}$ are the (rest-frame) contributions to the total radio flux from the thermal and nonthermal components, respectively, at $\nu_{0,r}$ (rest-frame), and $\alpha_{nth}$ is the nonthermal power-law index. Adopting a $\nu_{0,r}$ value of 230 GHz and holding $\alpha_{nth}$ fixed at 0.7 \citep[e.g.,][]{ShuBook}, we fit for $S_{th,0,r}$ and $S_{nth,0,r}$. We find best-fit values of $S_{th,0,r}$ = 45 $\pm$ 18 $\mu$Jy and $S_{nth,0,r}$ = 4 $\pm$ 3 $\mu$Jy (see Figure 4).

We do not consider any contribution to this part of the SED from thermal dust emission, which, continuing the Rayleigh-Jeans power-law found above, would contribute only $\sim$ 5\% of the flux measured at 230\,GHz (rest-frame). Indeed, the continuum flux from the core of 3C 368 is observed to be brighter at rest-frame 230 GHz than at rest-frame 480.5\,GHz, indicating that the dominant emission mechanism at 230\,GHz is not thermal dust -- an inference made possible by the continuum observations presented here.

Beyond the core component of 3C 368, we note that the radio lobes have considerable emission even in the high-frequency observations presented here (rest-frame 480.5\,GHz). Between observed-frame 8.21 and 4.71 GHz, \cite{Best1998} find a spectral index, S$_\nu$ $\sim$ $\nu^\alpha$, of $\sim$ -1.5 for both the northern and southern radio lobes. While the flux densities at rest-frame 480.5\,GHz fall below the extrapolated power-law values, by factors of $\sim$ 1.4 and 2.3 for the northern and southern lobes, respectively, the fact that such energetic electrons are present within the radio-emitting lobes is noteworthy. While detailed modeling is beyond the scope of this paper, the observations presented here suggest that the radio-emitting lobes of 3C 368 are quite young \citep[e.g.,][]{Murgia1999}.

\begin{figure}
\plotone{3C368_radio_SED_decomposition_4_11_19.pdf}
\caption{Radio SED of the core component of 3C 368, decomposed into thermal (gold) and non-thermal (red) contributions. Data from \cite{Best1998} and \cite{Lamarche2017}.}
\end{figure}

\subsubsection{Metallicity From Free-Free Continuum and Far-IR Fine-Structure Lines}
Having determined that the radio SED of the star-forming core of 3C 368 is dominated by thermal free-free continuum at 230 GHz (rest-frame), we can estimate the gas-phase oxygen abundance in 3C 368 using our previous observations of the [O\,{\sc iii}] 52\,$\micron$ line \citep{Lamarche2017}.

The method for determining gas-phase absolute ionic abundances using fine-structure line emission and radio free-free continuum has been applied historically to galactic H\,{\sc ii} regions \citep[e.g.,][]{Herter1981, Rudolph1997} and more recently to high-redshift galaxies \citep[e.g.,][]{Lamarche2018}. This technique provides an alternative to optically-derived metallicities, which suffer both from uncertainties in the temperature structure of H\,{\sc ii} regions, as well as dust extinction of the line flux. Dust obscuration is important in the local Universe, especially in the more luminous star-forming galaxies, and becomes an increasingly important effect in the epoch of peak cosmic star formation, at redshift $\sim$ 1 -- 3. It can be shown that the abundance of ion X$^{i+}$, relative to hydrogen, is given by:

\begin{equation}
\frac{n_{X^{i+}}}{n_{H^+}} = \frac{F_\lambda}{S_{\nu,r}} \frac{4.21 \times 10^{-16} T_{4}^{-0.35} \nu_{9}^{-0.1}}{\epsilon_\lambda} \left( \frac{n_e}{n_p} \right)
\end{equation}

where $F_\lambda$ is the fine-structure line flux in units of erg s$^{-1}$ cm$^{-2}$, S$_{\nu,r}$ is the rest-frame radio free-free flux density at rest-frequency $\nu$ in units of Jy, T$_4$ is the electron temperature in units of 10$^4$ K, $\nu_9$ is the radio emission rest-frequency in units of GHz, n$_e$/n$_p$ is the electron to proton number density ratio, which accounts for the contribution of electrons from non-hydrogen atoms present in the H\,{\sc ii} regions, and $\epsilon_\lambda$ is the emissivity per unit volume of the fine-structure line at wavelength $\lambda$, given by:

\begin{equation}
\epsilon_\lambda = \frac{j_{ul}}{n_i n_e} = \frac{h \nu_{ul} A_{ul} n_u}{n_e n_i},
\end{equation}

where h is the Planck constant, A$_{ul}$ is the Einstein A coefficient for the line transition at frequency $\nu_{ul}$, 9.8 $\times$ 10$^{-5}$ s$^{-1}$ and 5785.9 GHz, respectively, for the [O\,{\sc iii}] 52\,$\micron$ line \citep{Carilli2013}, and the ratio of the level population in the upper state (n$_u$) to the total (n$_i$) is determined by detailed balance. Adopting the collisional coefficients of \cite{Palay2012}, and an H\,{\sc ii} region electron density of 1,000 cm$^{-3}$, as has been determined to be the case in 3C 368 \citep{Lamarche2017}, we calculate a value of $\epsilon_\lambda$ =  7.6 $\times$ 10$^{-22}$ erg s$^{-1}$ cm$^{3}$ for the [O\,{\sc iii}] 52\,$\micron$ line. We additionally assume n$_e$/n$_p$ = 1.05, which accounts for the electrons contributed from helium, and T$_4$ = 1, a typical value for H\,{\sc ii} regions.

Combining the total integrated [O\,{\sc iii}] 52\,$\micron$ line flux \citep[1.34 x 10$^{-17}$ W m$^{-2}$;][]{Lamarche2017} with the estimated free-free flux density at 230 GHz (rest-frame), and using Equation 2, we calculate [O$^{++}$/H] = 1 $\times$ 10$^{-4}$. Then, to determine the [O$^{++}$/O] ratio, and hence scale our ionic oxygen abundance to total oxygen abundance, an estimate for the hardness of the ambient radiation field within 3C 368 is required. Using the H\,{\sc ii} region models of \cite{Rubin1985}, we predicted that $\sim$ 84\% of the oxygen within the H\,{\sc ii} regions of 3C 368 is in the O$^{++}$ state \citep{Lamarche2017}. Using that ionization fraction here, we obtain an estimated [O/H] ratio of 1.2 $\times$ 10$^{-4}$, or $\sim$ 0.3 Z$_\odot$ \citep{Asplund2009}, within about a factor of two uncertainty, where this uncertainty is dominated by both the uncertainty in determining the free-free contribution to the radio SED and the uncertainty in the measured [O\,{\sc iii}] 52\,$\micron$ line flux.

This low-metallicity value is consistent with the results of \cite{Croxall2017}, who found empirically that the [C\,{\sc ii}] 158\,$\micron$ / [N\,{\sc ii}] 205\,$\micron$ line ratio is highly elevated in low-metallicity sources. In \cite{Lamarche2017} we found a lower-bound of [C\,{\sc ii}] 158\,$\micron$ / [N\,{\sc ii}] 205\,$\micron$  \textgreater\,60, which would indicate 12 + log(O/H) $\sim$ 8.1, or equivalently Z $\sim$ 0.25 Z$_\odot$, in the sample from \cite{Croxall2017}.

An alternative explanation for the radio emission emanating from the core component of 3C 368 is that it originates from the AGN itself. Strong synchrotron self-absorption can lead to AGN with flat radio spectra, such that the radio emission which we attribute to thermal free-free emission from extended star-forming H\,{\sc ii} regions may instead come from a compact AGN \citep[e.g.,][]{Roellig1986}. As a check on this possibility, we examine the radio/IR correlation, q$_{IR}$ \citep[e.g.,][]{Ivison2010}, where

\begin{equation}
q_{IR} \equiv log_{10} \Bigg( \frac{S_{IR}/(3.75\,\times\,10^{12}\,W\,m^{-2})}{S_{1.4\,GHz}/(W\,m^{-2}\,Hz^{-1})} \Bigg),
\end{equation}

S$_{IR}$ is the total integrated IR flux (rest-frame 8 -- 1000\,$\micron$) in units of W\,m$^{-2}$, and S$_{1.4\,GHz}$ is the flux density at 1.4 GHz in units of W\,m$^{-2}$\,Hz$^{-1}$. Extrapolating the SED-decomposed thermal contribution to the radio emission at rest-frame 230\,GHz (45\,$\mu$Jy) to the expected value at 1.4 GHz using a free-free power-law index of -0.1, and using the total FIR luminosity attributed to star formation in 3C 368 \citep[2.0 $\times$ 10$^{12}\,L_{\odot}$,][]{Podigachoski2015} to calculate S$_{IR}$, we obtain a value of q$_{IR}$ = 2.6. This value is within the range seen in star-forming galaxies \citep[e.g.,][]{Ivison2010}, suggesting that the attribution of the radio continuum to free-free emission in 3C 368 is appropriate.

Unfortunately, our 230\,GHz rest-frame ALMA observations \citep{Lamarche2017}, with a synthesized beam of size 3$\farcs$12 $\times$ 1$\farcs$81, do not resolve the core of 3C 368. We will propose for higher resolution continuum imaging with ALMA to test the theory of extended H\,{\sc ii} regions vs. compact AGN as the source for the high-frequency radio continuum in 3C 368, thereby supporting or disfavoring the low-metallicity hypothesis for the ISM within 3C 368.

\subsubsection{Comparison With Optically-Derived Metallicity}
The sub-solar oxygen abundance that we derive for 3C 368 using the [O\,{\sc iii}] 52\,$\micron$ line and radio free-free continuum can be compared to the same value derived using optical lines. Observations exist for 3C 368 in the [O\,{\sc iii}] 5007\,\AA, [O\,{\sc ii}] 3727\,\AA, and H$\delta$ lines, such that R$_{23}$ \citep[e.g.,][]{Pagel1979} can be calculated by assuming a scaling from H$\delta$ to H$\beta$, where

\begin{equation}
R_{23} \equiv \frac{[O II] \lambda 3727 + [O III] \lambda \lambda 4959,5007}{H\beta}.
\end{equation}

Adopting an [O\,{\sc iii}] 5007\,\AA\, line flux of 6.8 $\times$ 10$^{-18}$ W m$^{-2}$ \citep{Jackson1997}, an [O\,{\sc ii}] 3727\,\AA\, line flux of 5.9 $\times$ 10$^{-18}$ W m$^{-2}$ \citep{Best2000}, an H$\delta$ line flux of 2.8 $\times$ 10$^{-19}$ W m$^{-2}$ \citep{Best2000}, and assuming the theoretical scaling of H$\delta$/H$\beta$ = 0.26 \citep[Case-B recombination, e.g.,][]{AGN2}, we obtain an R$_{23}$ value of $\sim$ 12. This R$_{23}$ value indicates 12 + log(O/H) $\sim$ 8.3 \citep{Kewley2002}, or $\sim$ 0.4 Z$_\odot$ \citep{Asplund2009}, making it consistent with the FIR/radio-derived estimate.

\subsection{PDRs}

\subsubsection{PDR Parameters}

In \cite{Lamarche2017}, we modeled the photo-dissociation regions (PDRs) within 3C 368 utilizing the PDR Toolbox \citep{Pound2008, Kaufman2006}, together with detections of the [C\,{\sc ii}] 158 $\micron$ \citep{Stacey2010CII} and [O\,{\sc i}] 63 $\micron$ lines, as well as the modeled far-IR continuum luminosity \citep{Podigachoski2015}, obtaining best-fit parameters of G$_0$ $\sim$ 280 Habing units and n $\sim$ 7,500 cm$^{-3}$. Here we update the model to include the two newly-detected lines.

Including the CO(4-3) and [C\,{\sc i}] 609 $\micron$ lines, we obtain new best-fit values of G$_0$ $\sim$ 320 Habing units and n $\sim$ 3,200 cm$^{-3}$, with a PDR surface temperature of $\sim$ 200 K (see Figure 5). These PDR parameters are similar to those which we obtained previously, up to a decrease in the density, due to the detection significance of the CO(4-3) and [C\,{\sc i}] 609 $\micron$ lines, which tightly constrain that parameter. We again see that the [C\,{\sc ii}] emission is elevated relative to the CO emission, and now also relative to the [C\,{\sc i}] emission.

The penetration of far-UV photons capable of photodissociating CO and ionizing carbon is limited by dust extinction. Therefore, assuming dust content scales with metallicity, the CO-photodissociated surface of a molecular cloud becomes much larger relative to the shielded CO-emitting core in low-metallicity environments. In PDR models \citep[e.g.,][]{Kaufman2006}, [C\,{\sc i}] line emission arises from a thin transition region of neutral carbon that lies between the C$^+$ and CO regions. The [C\,{\sc ii}] line flux is therefore enhanced relative to both CO and [C\,{\sc i}] in these environments \citep[e.g.,][]{Maloney1988, Stacey1991}.

\begin{figure}
\plotone{3c368_pdr_5_17_19.pdf}
\caption{A plot of the best-fit PDR parameters in 3C 368, generated using the models of \cite{Pound2008} and \cite{Kaufman2006}. The fit favors PDRs with G$_0$ $\sim$ 320 Habing units and n $\sim$ 3,200 cm$^{-3}$.}
\end{figure}

\subsubsection{PDR Mass}

Using the calculated n, G$_0$, and PDR surface temperature values in 3C 368, we can estimate the PDR mass following \cite{Hailey-Dunsheath2010}:

\begin{equation}
\begin{split}
\frac{M_{PDR}}{M_\odot} = 0.77 \bigg( \frac{0.93 L_{[C\,\textrm{\sc ii}]}}{L_\odot} \bigg) \bigg( \frac{1.4 \times 10^{-4}}{X_{C^+}} \bigg) \\
\times \frac{1 + 2 \exp(\frac{-91 K}{T}) + \frac{n_{crit}}{n}}{2 \exp(\frac{-91 K}{T})},
\end{split}
\end{equation}

where $X_{C^+}$ is the abundance of C$^+$ per hydrogen atom, taken here to be $1.4 \times 10^{-4}$ \citep{Savage1996}, n$_{crit}$ is the critical density of the [C\,{\sc ii}] 158 $\micron$ transition \citep[2,800 cm$^{-3}$,][]{Stacey2011}, and assuming that $\sim$ 93\% of the [C\,{\sc ii}] emission originates within the PDRs of 3C 368 as we estimated in \cite{Lamarche2017}. We calculate a PDR gas mass of $\sim$ 1.7 $\times$ 10$^{10}$ $M_{\odot}$ in this source (see Table 2).

\subsubsection{Molecular-Gas Mass}

With detections of both the CO(4-3) and [C\,{\sc i}] 609 $\micron$ lines, the molecular-gas mass within 3C 368 can be estimated in three ways:

First, using the detection of the CO(4-3) line, we can estimate the molecular-gas mass by assuming a conversion factor back to CO(1-0) and then adopting an $\alpha_{CO}$ value. The measured CO(4-3) line flux of 1.08 $\pm$ 0.14 Jy km s$^{-1}$ equates to a value of L'$_{CO(4-3)}$ = 4.6 $\pm$ 0.6 $\times$ 10$^{9}$ K km s$^{-1}$ pc$^2$. Our previous non-detection of the CO(2-1) line with ALMA yields a 3$\sigma$ upper limit of L'$_{CO(2-1)}$ \textless  3.45 $\times$ 10$^{9}$ K km s$^{-1}$ pc$^2$ \citep{Lamarche2017}. This implies that r$_{43/21}$ \textgreater 1.3, so we use this excitation ratio to scale L'$_{CO(4-3)}$ back to L'$_{CO(1-0)}$. Taking an ultraluminous infrared galaxy (ULIRG) value of $\alpha_{CO}$ = 0.8 $M_{\odot}$(K km s$^{-1}$ pc$^2$)$^{-1}$ \citep[e.g.,][]{Bolatto2013}, we obtain a molecular-gas mass of 2.9 $\times$ 10$^{9}$ $M_{\odot}$.

If, instead, we calculate a value of $\alpha_{CO}$ based on the metallicity estimates from section 3.2, adopting the scaling of \cite{Glover2011} \citep[and see also][]{Bolatto2013}, we obtain $\alpha_{CO}$ $\sim$ 18 $M_{\odot}$(K km s$^{-1}$ pc$^2$)$^{-1}$. Adopting this larger value of $\alpha_{CO}$, and assuming the same super-thermal CO-excitation as above, we obtain a molecular mass of 6.4 $\times$ 10$^{10}$ $M_{\odot}$ (see Table 2). This metallicity-adjusted $\alpha_{CO}$-based molecular gas mass is $\sim$ 4x larger than the PDR gas mass estimated above, making the mass ratio consistent with that observed in other starburst galaxies \citep[e.g.,][]{Stacey1991}, lending further credibility to the low-metallicity explanation for the small CO luminosity in 3C 368.

The second method is based on a scaling of molecular gas mass with [C\,{\sc i}]-line luminosity -- which does not assume that the [C\,{\sc i}] line arises from a thin transition in the PDRs -- as indicated by the work of \cite{Papadopoulos2004Q10}. Following \cite{Bothwell2017}:

\begin{equation}
\begin{split}
M(H_2)^{[CI]} = 1375.8 D_{L}^{2} (1+z)^{-1} \left( \frac{X_{[CI]}}{10^{-5}} \right) ^{-1} \\
\times \left( \frac{A_{10}}{10^{-7} s^{-1}} \right) ^{-1} Q_{10}^{-1} S_{[CI]} \Delta v ,
\end{split}
\end{equation}

where D$_L$ is the luminosity distance in Mpc (7,735 in the case of 3C 368), X$_{[CI]}$ is the [C\,{\sc i}]/H$_2$ abundance ratio, taken here to be 3 $\times$ 10$^{-5}$ \citep[e.g.,][]{Weiss2003, Papadopoulos2004}, A$_{10}$ is the Einstein A coefficient, 7.93 $\times$ 10$^{-8}$ s$^{-1}$ \citep{Wiese1966}, Q$_{10}$ is the excitation parameter which depends on gas density, kinetic temperature and radiation field \citep[e.g.,][]{Papadopoulos2004Q10}, which we take to be 0.6 \citep{Bothwell2017}, and S$_{[CI]}$ $\Delta$v is the flux of the [C\,{\sc i}] 609 $\micron$ line in units of Jy km s$^{-1}$. We obtain a molecular-gas mass of 2.3 $\times$ 10$^{10}$ $M_{\odot}$. We note that this molecular-gas mass is $\sim$ 3x smaller than that derived using the metallicity-corrected $\alpha_{CO}$ method above. If we scale the [C\,{\sc i}]/H$_2$ abundance ratio, X$_{[CI]}$, by the sub-solar gas-phase metallicity estimated in section 3.2, Z $\sim$ 0.3 Z$_\odot$, we calculate an H$_2$ mass of 7.7 $\times$ 10$^{10}$ $M_{\odot}$. Boosting this mass by $\sim$ 20\% to account for the contribution from helium, which is already accounted for in the $\alpha_{CO}$-based method above, increases the mass estimate to 9.2 $\times$ 10$^{10}$ $M_{\odot}$, such that the two methods produce masses which differ by $\sim$ 30\%.

Finally, we can use the dust mass calculated by multi-component SED modeling, along with a gas-to-dust ratio, $\delta_{GDR}$, to estimate the molecular-gas mass within 3C 368. Adopting an SED-modeled dust-mass of 1.4 $\times$ 10$^{8}$ $M_{\odot}$ \citep{Podigachoski2015} and a gas-to-dust ratio of 540, appropriate for Z $\sim$ 0.3 Z$_\odot$ \citep{Remy-Ruyer2014}, we obtain a molecular-gas mass of 7.6 $\times$ 10$^{10}$ $M_{\odot}$. Or, equivalently, if we use the CO-derived gas-mass together with the SED-modeled dust-mass, we obtain a value of $\delta_{GDR}$ = 464 (see Table 2). Since $\alpha_{CO}$ and $\delta_{GDR}$ scale differently with metallicity, the CO- and dust-derived gas masses are incompatible at solar metallicity, giving us more confidence that 3C 368 does indeed have sub-solar metallicity, and that our derived gas masses are robust.

The calculated molecular-gas mass implies that, at its current star-formation rate, $\sim$ 350 $M_{\odot}$ yr$^{-1}$ \citep{Podigachoski2015}, 3C 368 will deplete its supply of molecular gas in $\sim$ 170 Myrs. We can additionally calculate the gas fraction, f$_{gas} \equiv \frac{M_{gas}}{M_{gas} + M_{stars}}$, and the specific star-formation rate, sSFR $\equiv \frac{SFR}{M_{stars}}$, in 3C 368, finding values of $\sim$ 0.15 and $\sim$ 1 Gyr$^{-1}$, respectively (see Table 2). The calculated sSFR puts 3C 368 on the upper end of the galaxy main-sequence as defined by \cite{Genzel2015}, with SFR/SFR$_{MS}$ = 2.8, and the gas fraction lies exactly on the scaling with sSFR/sSFR$_{MS}$, stellar mass, and redshift found in \cite{Scoville2017}. Moreover, 3C 368 lies along the L'$_{[CI]}$ to L$_{IR}$ correlation found in other high-redshift main-sequence galaxies, however it is elevated in its L'$_{[CI]} / $L'$_{CO(2-1)}$ ratio, with a lower limit of 0.9, by a factor of $\sim$ 4.4 \citep{Valentino2018}. The models of \cite{Papadopoulos2018} find the [C\,{\sc i}](1-0)/CO(1-0) brightness ratio to be much larger than unity in low-metallicity or cosmic-ray-dominated regions, however, since we have only a modest lower limit on this ratio, we cannot draw any strong conclusions from it. When compared to a sample of low-metallicity high-redshift sources \citep{Coogan2019}, 3C 368 is observed to be similarly deficient in CO emission, and when compared to a sample of local luminous infrared galaxies (LIRGs) and spirals \citep{Liu2015}, it has a CO(4-3) flux which falls below that expected from the scaling with FIR luminosity, by a factor of $\sim$ 3.7.

\subsection{Dynamical Mass}

Since our ALMA observations of 3C 368 spatially resolve the source, we can additionally estimate the dynamical mass of the galaxy. Assuming a disk geometry and circular orbits:

\begin{equation}
M_{dyn} = \frac{v^2_{rot} r}{G},
\end{equation}

where v$_{rot}$ is the true rotational velocity of the disk, estimated from the observed velocity by correcting for the average inclination angle, $\langle$v$_{rot}$$\rangle$ $\sim$ $\frac{\pi}{2}$ v$_{obs}$ \citep[e.g.,][]{Erb2006}, r is the radius of the line-emitting region of the galaxy, and G is the universal gravitational constant.

We estimate the radius from two-dimensional Gaussian fits to the CO(4-3) moment-zero map (r = 0.5\,FWHM = 3.14 kpc). Similarly, we take the observed velocity to be half the full-width-half-maximum (FWHM) of the CO(4-3) line (v$_{obs}$ = 284 km s$^{-1}$). We obtain a dynamical mass of $\sim$ 1.5 $\times$ 10$^{11}$ $M_{\odot}$ (see Table 2). This dynamical mass estimate is $\sim$ 2x smaller than the estimated stellar mass within 3C 368 \citep[$\sim$ 3.6 $\times$ 10$^{11}$ M$_\odot$,][]{Best1998stellarmass}, a discrepancy that can be due to the effects of inclination angle and mass profile on the calculated dynamical mass.

\begin{deluxetable}{ccc}
\tablecaption{Physical Properties of 3C 368}
\tablecolumns{3}
\tablenum{2}
\tablehead{
\colhead{Property} & \colhead{Value} & \colhead{Reference}
}
\startdata
R.A. (J2000) & 18$^h$05$^m$06$^s$.40 & \cite{Best1998} \\
Dec. (J2000) & +11$^o$01'33".09 & \cite{Best1998} \\
z & 1.131 & \cite{Meisenheimer1992} \\
SFR & 350 $M_{\odot}$ yr$^{-1}$ & \cite{Podigachoski2015} \\
M$_*$ & 3.6 $\times$ 10$^{11}$ M$_\odot$ & \cite{Best1998stellarmass} \\
M$_{gas}$ & 6.4 $\times$ 10$^{10}$ $M_{\odot}$ & This Work \\
M$_{PDR}$ & 1.7 $\times$ 10$^{10}$ $M_{\odot}$ & This Work \\
M$_{dust}$ & 1.4 $\times$ 10$^{8}$ $M_{\odot}$ & \cite{Podigachoski2015} \\
M$_{dyn}$ & \textgreater 1.5 $\times$ 10$^{11}$ $M_{\odot}$ & This Work \\
$\delta_{GDR}$ & 464 & This Work \\
f$_{gas}$ & 0.15 & This Work \\
sSFR & 1 Gyr$^{-1}$ & This Work \\
SFR/SFR$_{MS}$ & 2.8 & This Work, \cite{Genzel2015} \\
$\tau_{Depletion}$ & 170 Myr & This Work \\
\enddata
\tablecomments{See the text for explanations of the physical properties presented in this work.}
\end{deluxetable}

\section{Conclusions}

We have presented detections of the CO(4-3) and [C\,{\sc i}] 609 $\micron$ spectral lines, as well as the rest-frame 480.5\,GHz dust continuum, in 3C 368, an FR-II type galaxy at redshift 1.131.

We have estimated the gas-phase metallicity in 3C 368 using two independent methods: (1) combining the observed [O\,{\sc iii}] 52\,$\micron$ fine-structure line flux with radio free-free continuum emission and (2) employing the optical [O\,{\sc iii}] 5007\,\AA\, and [O\,{\sc ii}] 3727\,\AA\, lines (R$_{23}$ technique). Both methods arrive at a consistent gas-phase metallicity of $\sim$ 0.3 Z$_\odot$.

We have calculated the molecular-gas mass within 3C 368 in three independent ways: (1) using the CO(4-3) line luminosity, gas excitation, and a metallicity-adjusted $\alpha_{CO}$ conversion factor, (2) scaling from the luminosity of the atomic carbon line, and (3) adopting a conversion factor from dust mass to molecular-gas mass. We find a consistent gas mass estimate of $\sim$ 6.4 $\times$ 10$^{10}$ $M_{\odot}$ across these three methods only when adopting a gas-phase metallicity of $\sim$ 0.3 Z$_\odot$.

Considering this molecular-gas mass, and a star-formation rate of $\sim$ 350 $M_{\odot}$ yr$^{-1}$ \citep{Podigachoski2015}, we deduce that 3C 368 has a molecular-gas depletion-time, $\tau_{Depletion}$, of $\sim$ 170 Myrs. We also calculate a gas fraction, f$_{gas}$, and specific star-formation rate, sSFR, adopting a stellar mass of $\sim$ 3.6 $\times$ 10$^{11}$ M$_\odot$ \citep{Best1998stellarmass}, of $\sim$ 0.15 and $\sim$ 1 Gyr$^{-1}$, respectively. The calculated sSFR puts 3C 368 on the upper end of the galaxy main-sequence, as defined by \cite{Genzel2015}, and the gas fraction lies exactly on the scaling with sSFR/sSFR$_{MS}$, stellar mass, and redshift found in \cite{Scoville2017}.

Further observations will allow us to determine whether 3C 368 does indeed have low gas-phase metallicity, if indeed free-free continuum emission dominates the radio spectrum at high frequencies, or whether the AGN is strongly contaminating the emission in those bands. In particular, we will propose for higher angular-resolution observations at rest-frame 230\,GHz to determine whether the radio continuum is extended, as should be the case if it originates from star-forming H\,{\sc ii} regions, or compact, as would be the case if it is of AGN origin.

\section*{Acknowledgments}

We thank the anonymous referee for the insightful comments and detailed suggestions that helped to improve this manuscript. C.L. acknowledges support from an NRAO Student Support Award, SOSPA3-011, and from NASA grant NNX17AF37G. D.B. acknowledges support from FONDECYT postdoctorado project 3170974.

This paper makes use of the following ALMA data: ADS/JAO.ALMA$\#$2015.1.00914.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.

The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

redpajama_set_name: RedPajamaArXiv


Exercises for various aches and pains are described by our physiotherapists, and accompanied by illustrations from New Bodyworks, the most recent book by Francine St George.
How to Improve your Performance and Have an Injury-free Ski!
It took just one hailstorm in Sydney to get me itching to ski this season. Most of us ski just a few times each year, and don't get ourselves conditioned to ski. Try these easy ski-preparation exercises leading up to your ski holiday!
Start by preparing how you stand. Draw a mark on the centre of each kneecap and stand in front of a mirror. The mark should be directly above your second toe. Adjust your feet and knees until they are. Do a half squat, keeping the marks above your second toes, then stand back up.
Try lunging forward with one leg, keeping the mark above your second toe, then stand back up and repeat with the other leg.
Repeat each exercise 30 times, squatting lower and lunging a little further forward each time.
Practice will help you align your legs properly to ski, and get you holding an edge like a pro. If you are having difficulty with these exercises, it may mean you need the canting adjusted on your ski boots.
Step 2: How's your Balance?
Most skiers put too much weight on the back of the ski. Keeping your weight even from front to back will give you more control and a faster ride. It's great to practice weight-bearing on a balance board, bosu or duradisc.
Try this exercise on solid ground. Stand on one leg, hugging the other leg into your chest with both hands. Make sure that the centre of your kneecap is over your second toe. Get the weight on your toes the same as the weight on your heels. Once you feel steady, extend the leg and your arms behind you, keeping the weight even on toes and heels, then return to your starting position.
Progress to the Arabesque position, extending the leg straight behind you, with one arm extended in front. Then return to the starting position.
No sport uses Gluteus Medius as much as skiing. Good control of the hips includes having strong glute meds, and this is essential for your turns.
Stand side on to a wall, with your hands on your hips. Lift the knee closest to the wall. Pushing this knee into the wall will make the glutes contract on your standing leg. Maintain your alignment and balance throughout this exercise.
Hold for 10 seconds and repeat 8-10 times each side.
To progress this exercise further, try turning out the foot you are standing on, against the resistance of the floor.
Your quads are the workhorses of your skiing. You need strength and endurance in these muscles.
Stand with one leg on a step and the step the other down towards the floor in front of you. Stop before your foot actually hits the floor and return to your starting position.
Repeat 10-15 times and do 3 sets on each leg. Maintain your alignment and balance. Move to a higher step and add weights to progress this exercise when you're ready.
The fitter you are, the longer you will enjoy your day on the slopes. That chair ride up only lets you recover so much!
Running, skipping, cycling or using an elliptical trainer as often as you can – at least every second day – is the easiest way to improve your baseline fitness and endurance.
Start by standing feet together on the box, and stepping one leg sideways until it touches the ground, then return to both feet together on the box. Step to the other side. Repeat 30 times to each side, and keep your alignment and balance as you go.
Once you've mastered this exercise, keep your feet together and jump both feet to the floor on one side, then back onto the box, then both feet to the other side. Repeat 30 times on each side.
Increase the height of the box, and try jumping forward and back when you can.
Flexibility is particularly important when you are doing tricks or racing, and it is vital that you stretch any muscle that feels tight before and after your day on the slopes, especially as fatigue and the cold will make your muscles tighten up.
A good stretch for your calf muscles can be achieved by using a low wedge (an old cutting board against a brick or similar will do the job.) Angle the wedge down towards a wall, and stand with your back against the wall. Hold this position for 1-3 minutes with your legs straight (gastrocnemius), and then repeat with your legs a little bent to reach you r deeper calf muscles (soleus).
Your hip flexors will also need a good stretch after skiing. On your knees, lunge on leg forward with your pelvis tucked under, and then stretch the arm on that side over. Hold for 20 seconds, and repeat on both sides.
A simple quad stretch will also assist your muscle recovery after skiing. You can use a wall or table to support you. Stand up tall on one leg.
Bend the other leg and reach the foot up behind you. Hold onto your foot and try to keep your knees together. Hold for 20 seconds, and repeat on both sides.
If you follow these 5 guidelines, your performance will improve on the slopes this season, and you are much less likely to suffer injuries. Prevention is always better than cure! If you have any trouble with these exercises, or would like to improve your performance further, speak to your Physiotherapist.
At PPFC, our resident Skiing Physio is Alex Sherborne. Call to make an appointment with him on 02 9399 7399.
Ankle sprains: Why do I keep rolling my ankle? Exercises to stop it happening!
There are position receptors, "proprioceptors" located in your joints, ligaments and tendons. They sense where your body is positioned in space, sending this info to your brain.
With any injury, such as a rolled ankle, there is likely to be altered proprioception. Has your ankle ever felt vulnerable on uneven ground or with unexpected movements? Poor proprioception is why its common to suffer recurrent ankle sprains – the ankle stability muscles don't kick in when your ankle starts to roll.
By using unstable surfaces, we can retrain the stability muscles to function as they did pre-injury – or even better! That's why it is excellent for you to practice walking on uneven surfaces after an injury.
• Can you stand on one leg with your eyes closed? Try keeping your balance there for more than 10 seconds.
• Was this too easy? Stand on a rolled up towel to challenge your balance. Eventually you can add multitasking like throwing and catching a ball to this exercise.
In our gym, we use exercises on foam balance beams and the Bosu to retrain proprioception. A real challenge is walking on the beam with your eyes closed. Most of us are heavily reliant on vision for body awareness, and taking this away really works your other positional senses! The goal is to retrain your balance and co-ordination, as this will reduce your risk of re-injury.
For more tips on how to stop injury recurring, call 93997399 and request a consultation with Alla.
Needing some fun exercises to ease unwanted neck and shoulder aches and pains?
Our body does not like being in a sedentary postion for hours on end! Postural muscles fatigue and muscles that should be used for movement take over and tighten up. This in turn can cause tension on the nerves that run from our neck to our arms. Try to take regular breaks every hour or so and have fun with the following exercises!
We talk about gently winding up or tensioning up a nerve as the starting point for doing a nerve exercise. This means we position the body so the nerve is being slightly tensioned as it emerges from the spine and runs into a more distal area. We can then move either the limb, the back or the neck and this will begin to loosen the nerve. It is critical that you do not overstretch or force a nerve mobility exercise as this will cause pain. It is also important that if you feel pins and needles, or latent pain, then you need to ease back, as you are definitely overdoing it. In this case, consult your physiotherapist to find out how to do your nerve mobility work correctly.
Place your left hand onto your right shoulder. Tighten your right shoulder muscle by shrugging your shoulder. Now relax this muscle by altering the position of your right shoulder joint so that you can feel with your left hand that your right shoulder muscle is as relaxed as it can be. Try positioning your shoulder back and downwards, and then relaxing and softening your posture without slumping and this will usually help this muscle relax. Once you have learnt how to do this with your hand on your shoulder you can then do this whenever you feel yourself getting a little tense. Be sure to repeat this exercise on the opposite side – using the right hand on the left shoulder.
While sitting in a chair, take your hand out to the side of your body with your fingers facing upwards. Imagine there is a wall there and you are gently bending your elbow and almost straightening it while moving your hand towards and away from this imaginary wall. Keep your hand at about waistline level and then start to move your arm backwards slightly behind your body. If you feel tightness in your hand, this means you have tension in the nerves running from your neck into your forearms.
Now, turn your fingers downwards facing the ground with your palm still facing away from your body. Start with the elbow bent and then try to straighten it. Do this very gently with small oscillating movements. Be sure you expand the chest and pull the shoulders back and downwards for the exercise to be more effective.
This exercise is for tensioning the ulnar nerve which traverses the medial side of the elbow. Have fun with it! Make a circle with the tips of the thumbs and index fingers. Raise the arms and roll the other fingers towards you. Place the circles formed by the thumb and index fingers around the eyes and spread the fingers lengthways down the side of the face. Gently depress the shoulders and pull the shoulder blades together to achieve an effective stretch. Hold for 10–15 seconds. Great stretch if you are working at a computer and don't mind your colleagues' comments!


I have provided emergency room care for the past 6 years at a rural hospital and large metropolitan area hospital. I have also been involved in trauma for 6.5 years at a Level 1 Trauma Center in New Orleans. It is important to address patient needs and involve them in every aspect of his/her care. The patient's medical knowledge as a direct effect on his/her outcome and it is the provider's responsibility to ensure they have been educated appropriately.


Canada has earned its 22nd medal at the PyeongChang 2018 Winter Olympic Games in South Korea.
Canada lost to the USA 3-2 in a shootout and will settle for silver in women's hockey.
and then i was like nope, cannot watch the women. i had a feeling they would not win gold. that being said, they did win a medal and it's more than so many athletes can say; but i know it is disappointing to not be on top.
Like you, I watched all the big air and then realized I was zonked and wouldn't make it thought the hockey game. I think I drifted away seconds before the puck dropped.


text:
Greg Kot
FKA Twigs danced past her past into a new sound
By Greg Kot
Singer FKA Twigs. (David Burton)
After two drowsy EPs, FKA Twigs arrived this year with her first full-length album, "LP1" (Young Turks), an immersive shadow world of eerie soundscapes, disruptive noise and insinuating melody. It showcases an artist with an ability to create an entire planet of sound all her own between the headphones.
Twigs, born Tahliah Barnett 26 years ago in rural Gloucestershire, England, took a jagged path to the creation of one of the year's most distinctive albums.
"When I was younger, I had conversations with friends about wanting to create something different," she says. "Every young musician probably thinks that. But it's difficult to do, because there are only so many words, notes, melodies, songs. But as soon as I stopped thinking and started feeling, it worked. I didn't realize it till I was done."
Barnett spent years studying dancing and initially made her mark as a background dancer in videos for established artists such as Kylie Minogue, Ed Sheeran and most notably Jessie J, with quirky, scene-stealing appearances in "Do it Like a Dude" and "Price Tag."
"In school I had a tough time fitting in and dancing was my way of being in my own element," she says. "As a teenager, I became a bit disillusioned with it. Even with competitions, I'd win, but still there would be tears. I knew I wanted to get out of the countryside, and the summer before I left for London, I got a boyfriend and started hanging out in places I shouldn't be. I started going to this club with a big Jamaican community, and it opened things up for me. I'm half Jamaican, and I really felt at home being around these amazing West Indian musicians and rockers. I started singing hooks on rapper's songs, I would sing a little chorus, and people encouraged me to write my own songs. I spent my whole teenage life trying to get to London and go to dance school, but when I got there, I couldn't wait to get to the clubs on weekends. I knew I wanted to make music."
Her mission shifted: Find a way to pay her bills so she could focus on her new obsession. She put her dancing talents to work, in videos for artists whose music she might not even like, and as part of the cabaret scene in London. "I immersed myself in this world full of crazy acts with stilts, bows and arrows, Russian gymnasts, drag queens, a really bizarre I-am-divine lifestyle. It was full of weird, creative people who never ever would get a break, but made this a thing. I would become this character — Betty Boop crossed with Jessica Rabbit – and toss wine in people's faces. So I was this androgynous girl with piercings in people's videos, and this other character in the cabaret, wearing heels, blinking about and being naughty."
Meanwhile, Barnett taught herself to play instruments and shape songs with assists from several producers.
"I love learning, and I learn quickly," she says. "When I was doing the record, if I realized I was a little bit good at something, it made me want to do more. If it had too much of them (the producers) in the music, I would feel disconnected. I never let anyone write any one melodic note or one lyric. It can be confusing as a songwriter if you write every melody or lyric and someone else is playing piano or synth. I want to be that involved in production, directing. If I can do it, I want to do it. If I can learn, I will learn. Sometimes people show you things and it's about ego. But I'm not stupid. Being a gal, people can be a bit patronizing. 'Oh, look at you using the computer.' They would never say that to a boy. And I don't let them do it to me."
Barnett's hands-on approach came with a price. That's when she came across Thomas Wyatt's poem "I Find No Peace," and the line, "I love another, and thus I hate myself," which became the unofficial subtitle of an album about longing and loneliness.
"It was near the end of the album and I was really confused about everything going on," she says. "I'd been out and I came home, really drunk. My flat mate was out. I remember coming in, the TV was on, all the lights off, and the presenter on this BBC program was reading that Wyatt poem. And I thought, 'That's my life at this moment.' You can apply it to everything. You love dancing so much, work so hard, but you hate yourself because you feel uncomfortable expressing yourself that way. Or you love making music, and you can't figure out this computer, everything is going wrong, even on a good day, the ghost in the computer is not working, it breaks down, and you lose your work. And you hate yourself in that moment. You can be with someone, and love someone, but they bring out the worst in you, you become jealous and insecure, and you start to hate yourself. That swing and balance between love and hate – I realized that's what my record was about."
As she was wrapping up "LP1," she acknowledges feeling let down, a bit adrift. "I was so in it, so emotionally tied to what was going on, so many ups and downs," she says. "Emotionally it was the most exhausting thing I've ever done in my life. I tell friends now who have doubts about something they've just finished, 'It's OK not to know whether it's any good or not. You should feel tormented. Three months later you'll like it.' I'm finally starting to enjoy my record. That torment of finishing a record is finally leaving me."
Also worth hearing
Bob Dylan: At 73, Dylan still looks for new ways to sing his most iconic songs, in part because his voice sometimes sounds like it just got roughed up in the alley behind the stage. He's focusing on newer material on this current tour, though on any night he's liable to veer off script, which keeps everyone -- including his excellent band -- on their toes. 8 p.m. Saturday-Monday at Cadillac Palace, 151 Randolph St., $52.50, $86.50, $142.50; ticketmaster.com
Sonny Knight: After debuting as a teenager a half-century ago, Sonny Knight's future looked bright. But it wasn't until this year that the 66-year-old Minneapolis singer got the opportunity to record his debut album, "I'm Still Here," (Secret Stash) and it's a doozy of hard-driving soul. 7:30 p.m. Sunday at Space, Evanston, Ill., $15 and $25; evanstonspace.com
Greg Kot co-hosts "Sound Opinions" at 8 p.m. Fridays and 11 a.m. Saturdays on WBEZ (FM-91.5).
greg@gregkot.com
Latest Greg Kot
Commentary: Grammys' diversity blindspot shows no signs of clearing up
Torres album review: 'Silver Tongue' turns a relationship inside out
Grammy preview: Will the sound of the new — Lizzo, Billie Eilish, Lil Nas X, Rosalia — have staying power?
Beach Slang album review: James Alex doubles down on his Replacements love
Lollapalooza's Charlie Jones leaves fest producer C3, no immediate changes anticipated
Twitter @gregkot
When: 9 p.m. Nov. 13
Where: Metro,3730 N. Clark St.
Tickets: $19 and $21; metrochicago.com


Mr. Lamrani previously worked as an intern with the U.N. Office on Drugs and Crime, where he was assigned to the Afghanistan desk. He was raised in Morocco and is a native speaker of Arabic and French. He has lived and worked in Europe, the United States and Thailand.
The U.S. has said it will soon begin pulling its forces from Afghanistan. But apart from the Taliban, few will be happy -- including Washington's biggest regional adversaries.
The United States is debating the organizational future of the new Space Force, but the bigger question centers on the future of war beyond the planet's frontiers.
Regional hotspots like Iran and North Korea have pulled Washington away from its main concerns: China and Russia.
The rise of disruptive weapons technology and the decline of long-standing arms control agreements will raise the stakes as the United States works to boost its defenses against China and Russia.
Stratfor Deputy Editor Lynn Wise talks about the recent Islamic State attack on the Deir el-Zour air base in Syria. Though the Islamic State has lost much of its territorial control in Syria, it was able to successfully infiltrate the base and inflict considerable damage.
During the Cold War, the United States became an expert in the concept of nuclear deterrence. But this isn't the 20th century, and North Korea is no Soviet Union.
Senior Military Analyst Omar Lamrani and South Asia Analyst Faisel Pervaiz discuss geography's role in the standoff between Chinese and Indian forces along the Line of Actual Control.
As the fight against the Islamic State winds down, a new and deadly conflict is threatening to erupt in Syria's war-torn east.
In a progressively multilateral world, the growing threat of weapons proliferation is a constant specter. Given the rapidly shifting landscape, the focus of arms control efforts will increasingly turn toward efforts at containing the spread of technology and weapons rather than the more difficult task of negotiating great-power deployment and use.
Turkey is no stranger to tumultuous times. As the Republic of Turkey and as the Ottoman Empire before that, the country has weathered foreign invasion, military coups and civil strife. Today, Turkey has found itself once again in a trying time.
Space is becoming more congested, contested and competitive. As technology advances and more countries jostle for advantage, the risk of orbital battles -- a global threat -- grows. The United States is pushing to bolster its capabilities and is preparing for a potential conflict.


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Home » The Branch » Branch History
The branch started as an informal activity when some youths started to train together. It was Bengt Amnehagen who was the one who was the acting instructor at the time. Bengt had received some training under Roy Colegate sensei, and participated in some training camp in Shorinji Kempo. In the autumn of 1983 he gathered some school friends who began training under his direction in a relatively informal setting.
Already in the autumn of 1983 Pontus Liljequist began, Pontus later become the shibu-chō in Stockholms Studenter Shibu, and Pelle Svensson to train with Bengt. Anders Pettersson and Åke Olsson began training in January 1984, Mikael Sjödin was also practising during this time. Mikael has not been active for many years although he made occasional short comebacks over the years. Pelle has had some periods of rest from the practice, but since a number of years he is a regular member of the branch. Peter Malmberg also trained with us in the beginning, but after a year he began to train Taekwondo, where he is now 5 dan and the driving force of the club Samurang Taekwondo.
Pictures by Pelle Svensson, from about 1985.
Since no one was high enough graded to formally lead an official Shorinji Kempo branch all kenshi were registered as members of Bromma shibu, under the guidance of Roy Colegate sensei.
As often as possible everyone went to Stockholm (a little over 300 km away and about 3.5 hours drive) to train and the club also organised weekend training camps in Karlstad, often a few times per semester, with instructors from Stockholm and Visby (which at this time were the only places where there was official Shorinji Kempo branches). Roy sensei came often, but the branch also received a lot of help from Leif Larsson sensei, at the time shibu-chō i Visby shibu.
In 1987 Kawahara Tomokazu sensei, kenshi from Rakutō dōin and at this time 4 dan seikenshi but currently 6 dan junhanshi, spent almost a year in Sweden. During this time he lived in Visby, but also came on visit to Karlstad and taught at weekend camps. This was the branch's first direct contact with Rakutō dōin.
Kawahara Tomokazu-sensei together with Anders when Kawahara-sensei visited Karlstad 1987.
Next year Morikawa Kazuhito came to Sweden, although he lived primarily in Visby, he also spent a full month in Karlstad. Morikawa Kazuhito sensei is the oldest son of Morikawa Zeoh sensei and was at this time 4 dan seikenshi, he is now 7 dan seihanshi. The help we got from Morikawa Kazuhito sensei was a real boost for the club.
Morikawa Kazuhito-sensei with Anders to the left and Åke to the right, when they held a demonstration in Karlstad 1988.
In September 1989, Anders Pettersson and Åke Olsson graded to shōkenshi 2 dan during an international training camp at the Shorinji Kempo Hombu (headquarters) in Japan. This was the first time that members from Karlstad was in Japan and visited Hombu, during the same trip some time was also spent in Kyoto to train in Rakutō dōin.
Swedish kenshi in front of niōmon (the niō gate) at Hombu in 1989. At the front stands Shimura sensei and Fujii sensei, Anders is in the far left while Åke is directly behind Shimura sensei.
After returning from Japan all the application documents was filled out and submitted to headquarters in Japan and during the spring of 1990 Shorinji Kempo Karlstad Shibu was officially registered in the World Shorinji Kempo Organization as a Shorinji Kempo shibu (branch). In the same period the branch also became a member of the Swedish Budo Federation (now called Swedish Budo & Martial Arts Federation, SB & K). Anders became the shibu-chō and Åke became the fuku shibu-chō, Roy sensei served as kantoku (coach) and was responsible for all gradings, etc. It is necessary to have a kantoku if the shibu-chō have a lower rank than 3 dan.
In 1992 Anders Pettersson lived 3 months in Kyoto and received instructions from Morikawa Zeoh sensei in Rakutō dōin. In September 1993 it was again time for a Kokusai Taikai (international Taikai) and Anders and Åke graded to chūkenshi 3 dan at Hombu. In doing so they became independent and were able to grade the members of Karlstad on their own.
Swedish kenshi in Hombu dōin in 1993. At the front sits Arai sensei, Kawashima sensei and Yamasaki sensei, directly behind them are Åke and Anders. At the far right in the back row is Pontus Liljequist.
In 1995 the branch had a guest instructor for about 6 months when Kawashima Hiroshi, a kenshi from Rakutō dōin that at this time was 4 dan seikenshi and now is 6 dan junhanshi, lived with us in Karlstad. Anders got to know Kawashima Hiroshi sensei during the time he lived in Kyoto, and when Kawashima sensei finished university, it was a good opportunity to get out and travel a bit.
Ever since the first contact in the late 1980s, the branch has maintained contact with Rakutō dōin and when travellin to Japan Rakutō dōin is always visited. Sweden and we in Karlstad has also received regular visits by Morikawa Zeoh sensei or his sons and students over the years.


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Tag Archives: 99c
IN THE COMPANY OF THE DEAD 99c #SALE (Dark Fantasy) + Monday Morsel
For a limited time only, you can pick up my dark epic fantasy, In the Company of the Dead, for 99c–catch up now before Book 2 is released!
The woman stood observing the spectacle. Though the soldier had struck the ground mere feet from her and was already on his feet, moving towards her, her face reflected only a resigned calmness.
The man reached for her with his free hand. Time oozed with the slowness of poured honey.
"No!" Lyram choked the word into a strangled gasp, and broke into an unsteady run.
One step. The girl brought one long-fingered white hand up in a gesture of—what? Supplication? Forestalling? Defence even.
Two steps.
The soldier seized her by the wrist. With her other hand, she reached out and touched the boiled leather plate over his chest.
Three steps.
The sword dropped from the soldier's fingers. In one fluid motion, he crumpled at the knees and fell face-first into the knee-high grass.
Time snapped back to normal, and Lyram skidded to a stop over the motionless soldier.
The fallen man didn't move a muscle. Dropping to one knee, Lyram reached for the man's neck, seeking a pulse—but he stopped before touching him. The skin was blue with such intense cold that it chilled his fingers where they hovered several inches short of contact. He let his hand drop back to his side.
A shadow darkened the dim, rainy haze of the morning and he glanced up. A colourless face loomed over him, alabaster skin, midnight hair made all the darker by contrast, and eyes so black the pupils could barely be distinguished. What he'd taken for a homespun peasant dress was instead the billowing black robe of a priestess of Ahura.
She met his gaze with a chill that should have left snowflakes in the air, and he shivered, despite the hot, sweaty aftermath of battle. This close, there was nothing of Zaheva in her stern face.
"That was not necessary," she said, speaking Ahlleyn with the same lilting accent as Zaheva.
"Forgive me, Sister," he answered in Tembran, a reflex response to the familiar accent of his wife, and her eyes flickered a fraction in surprise. Backing off, he sketched a bow. When he straightened and met her gaze again, the skin around her eyes tightened with suppressed emotion.
Though she couldn't be more than a dragon's heartbeat past twenty, if that, she wore the gravitas of a much older woman. She clutched a long, thin package, wrapped and tied round with knotted cords. At one end, the wrappings were torn open, and she was working to loosen the knots, her hands blocking his view of the object inside.
"I am Ellaeva," she said in Ahlleyn, despite his use of her own language, and extended a hand.
The name didn't so much ring bells as send them tolling in alarm. He knew it. Everyone knew it. Ciotach an Bhais they called her in Ahlleyn, behind her back at least. The Left Hand of Death. In other lands she was known more simply as the Death Priestess. Ahura had many priestesses dedicated to death, but only one Death Priestess.
His gaze dropped to the dead man. Well, that explained that.
Shaking her hand, particularly over the corpse of a man slain by her touch, held all the appeal of the gallows, but he met her gaze squarely and took her hand.
Only a fool crosses a god, but Ellaeva and Lyram will do anything to get what they want.
Chosen as a five-year-old orphan to be the Left Hand of Death, Ellaeva has nothing to call her own—nothing except a desire to avenge her slaughtered parents. Her duties leave her no time to pursue the man responsible, until both her work and revenge lead to the same place—the lonely castle where Lyram Aharris is serving out his exile after the murder of his wife.
Lyram is third in line for the throne, and when the castle is unexpectedly besieged, he fears his prince means to remove him from contention for the crown permanently. Ellaeva's arrival brings hope, until she reveals she has not come for the siege, but instead she hunts the castle for a hidden necromancer dedicated to the dark god of decay.
Within their stone prison, Ellaeva and Lyram must fight to save themselves from political machinations and clashing gods. But as the siege lengthens, the greatest threat comes from an unexpected quarter.
Praise for IN THE COMPANY OF THE DEAD
"Some of the most notable fantasy authors create powerful reads with slower beginnings that lead up to a crescendo of gripping action – such as this story… Much like the acclaimed fantasy writer Patrick Rothfuss's productions, In the Company of the Dead evolves slowly for the first few chapters… perfect for the fantasy fan seeking depth, who appreciates a slow build-up before the fiery action begins. Such an audience will find this perfectly fits the definition of an epic saga: sweeping, complex, and ultimately engrossing." ~ D.Donovan, Senior Reviewer, Midwest Book Review
"Ballintyne's deep characterizations make you feel for the people she's created, root for their endeavors, and gasp at their tribulations… The prose is wonderfully evocative and the plot has good twists and is well-paced… an engrossing read, a good choice for fantasy fans who like a meaty storyline." ~ Readers' Favorite
"If you're a fan of epic fantasy with a romantic twist along the lines of Game of Thrones and The Lord of the Rings, I think you'll enjoy this book… I definitely see this as a book that the more you read it, the more you'll glean from it. If you're looking for a hefty, deep, complex fantasy novel, definitely check this book out." ~ Nebula of Books
Monday Morsel
And now a brief excerpt from the sequel, On the Edge of Death.
"Perhaps, then, my company will make it all the more pleasurable." The duchess favoured him with a bright smile, and a muscle in Lyram's cheek jumped spasmodically as he ground his teeth.
First Drault, and now Narrawen. Well, he could not gainsay the prince, although he would appeal to Alagondar, for what good it might do him, but by Ahura's blade, he could stop Narrawen. "You'll do no such thing. We have reports of some upheaval in the region. I'm not convinced we should be risking his highness, but we'll certainly not be risking the stability of a duchy at the same time."
She gave him a wide-eyed look, still standing in the doorway and blocking Everard and Ellaeva's departure, and her eyes flickered significantly to the priestess. "Surely you wouldn't force me to stay here and gossip."
And that simply, she had him. His shoulders slumped. Either he brought her along, or she'd accidentally reveal Ellaeva's identity. The more who knew the truth, the greater the risk someone would slip up at the border or inside Jerrek, and he certainly couldn't risk Drault finding out.
"Why do you even want to come?"
Narrawen stepped closer, touching his cheek with one gloved hand. "Lyram, dear, if I keep letting you run away from me, I'll never get you to marry me."
About On the Edge of Death – Book 2 in The Sundered Oath
All the Left Hand of Death wants is something to call her own, but is the price too high?
Ellaeva, the fated avatar of the death goddess, is desperate to track down her missing family but the trail is decades old. Instead, she discovers her battered and bloodied sister priestesses driven across the Jerreki border on pain of death. Ellaeva must turn aside from her personal quest to investigate the murders, only to find her parents have been taken into the heart of the conflict.
Lyram Aharris, favoured son of the royal line of Ahlleyn, is the only living person she trusts to help her infiltrate the enemy stronghold and uproot the horror they find there, but their chequered past threatens the mission. Accompanying him is his crown prince, the one man Lyram wants dead above all others.
Now Ellaeva must face down the darkness in her soul before a dark god is brought into the world.
At the boundary of life and death, all oaths will be tested.


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OMV hit by Greenpeace protests in New Zealand
Austrian oil company OMV has been under attack by Greenpeace activists in New Zealand at two separate occasions. First, the protesters boarded OMV's supply vessel at a port in Timaru and then moved the protests in front of OMV's offices in Plymouth.
Source: Greenpeace New Zealand
Activists spent three days this week protesting in front of OMV's Plymouth offices. This protest was preceded by an occupation of OMV's support vessel Skandi Atlantic in late November.
Namely, 30 people, including a team of Greenpeace climbers, on November 24 climbed aboard the support vessel for OMV's oil rig and some locked themselves to the ship to stop it from leaving the port.
According to Greenpeace, the Bahamas-flagged Skandi Atlantic was preparing to leave the Port of Timaru and travel north to meet an oil rig commissioned by OMV, now stationed off the coast of Taranaki.
Greenpeace climate and energy campaigner, Amanda Larsson, said: "By occupying OMV's henchboat, we're delaying the monster rig from drilling for new oil in the middle of a climate emergency."
Larsson added: "People are over it. We're over companies being allowed to search for new oil to burn in the middle of a climate emergency, threatening the lives of millions of people. At every turn, OMV can expect us to be all over them."
After 50 hours of occupying the support vessel in Timaru to prevent it from leaving the port, the last 10 protesters were forcibly removed by the police on Tuesday, November 26. However, Greenpeace did not stop there. The environmentalist organization then announced its intentions to continue the protest in front of OMV's offices in Plymouth.
Larsson said in a statement on November 26: "This resistance is only set to continue. Next week, hundreds of people from around the country are gearing up to take part in a Climate Uprising mobilization in New Plymouth, where this vessel is heading and OMV has its Taranaki Headquarters."
Following the end of protests on the support vessel, a group of people who had been occupying the vessel in the Port of Timaru raced north to New Plymouth – the destination of the boat and OMV's Taranaki base.
Plymouth protest
On Monday, December 2 protesters formed a human barricade around OMV's offices in Taranaki – shutting it down. The activists called on OMV to leave New Zealand.
The three-day occupation of OMV headquarters in New Plymouth wrapped up on Wednesday. Greenpeace claimed that at least 300 of the oil giant's staff were forced to stay away from the office during the protest.
However, the activists have left OMV a parting gift. They've installed an outdoor pop-up museum in OMV's front car park, full of artifacts from the oil industry's past.
Greenpeace stated that OMV is about to begin drilling for new oil and gas off Taranaki, and has plans to move into the untouched, deep seas of the Great South Basin off Dunedin afterward.
Larsson said: "We are encouraging OMV executives to help New Zealanders make oil history by surrendering their permits to drill in New Zealand waters. We can always find a place for it in our oil museum."
According to information on OMV's New Zealand website, the company's exploration team is actively working towards a drilling campaign in the Taranaki basin in 2019/2020 aiming to grow OMV's and New Zealand's reserves through new discoveries. This exploration drilling campaign is supported by the acquisition of the largest seismic survey ever acquired in the Taranaki Basin.
In addition, the company is committed to drill one exploration well in the Great South Basin, which is required to be drilled by July 2021.
Shell wins court order
Over in Europe, Shell last week won a court order against Greenpeace aimed at preventing environmentalists from boarding the company's oil installations in the North Sea.
In October 2019, Greenpeace protested on the Shell-operated Brent field in the North Sea against the company's plans to leave parts of old oil structures with 11,000 tonnes of oil in the North Sea.
Following the protest, Shell sought an order from the Edinburgh court to ban protests near the company's platforms. The judge concluded that since the installations were private property, Shell had a legal right to stop the climate activists from accessing them.
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Posted on December 6, 2019 with tags Greenpeace, New Zealand, OMV.
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