text:
Fears About Cloud May Be Holding Organizations Back, Study Shows
Businesses are facing pressure to move to the cloud, but fear still holds some organizations back. Despite the fact that their competitors may be edging ahead of them, these businesses cling to outdated processes because it makes them feel safe. But is this the best course of action? A new study indicates that security hasn't proven as challenging for cloud-hosted businesses as their competitors might think.
The study, hosted by Internap Network Services Corporation, uncovered a big difference between expectations and reality when it comes to cloud computing. Those who are already using cloud technology, known as cloud wise, named concerns that were dramatically different from those who aren't using it, known as cloud wary.
Respondents were chosen from a variety of industries to show how cloud computing is impacting businesses serving customers in almost every type of enterprise. The study polled 250 decision makers for businesses that included healthcare organizations, software and internet, media and entertainment, and more.
Performance vs. Security
Cloud-wise organizations cited performance as the top challenge they face in working with cloud service providers. Of the respondents, 30 percent named performance as a key factor. This was especially true for those organizations hosting big data in the cloud. Nearly 60 percent of respondents said they'd run into performance challenges with their big data applications since contracting with cloud providers for the task.
Cloud-wary organizations, meanwhile, named security as a top concern. Of respondents who were hesitant to move toward the cloud, 40 percent said security was a problem. Yet among cloud-wise organizations, only 15 percent said they'd encountered security challenges in their cloud partnerships.
Unfounded Fears
The study posed questions about whether these fears may be unfounded. While some organizations have compliance and regulatory reasons to show caution in their technology solutions, the responses from cloud-wise organizations should allay those concerns.
"While a portion of cloud-wary are from security-conscious industries, such as financial services, healthcare and government, the majority may be overestimating security risks since performance and cost top the lists of actual problems encountered by the cloud wise," the report on the study states.
Cloud-Wary Dangers
The biggest danger cloud-wary organizations face is being left behind. Those organizations stated that they not only aren't currently using cloud solutions on a widespread basis, but they have no plans in the immediate future to do so. Unfounded fears may be holding these organizations back, forcing them to cling to outdated processes that slow them down.
One response that ignited concerns was that virtualization was a required part of cloud adoption. Virtualization isn't required for public clouds, yet 66 percent of those responding cited virtualization as a defining characteristic of cloud computing. The results show that education may help facilitate a greater move toward cloud adoption.
In addition to education, it's important that businesses choose a reliable vendor and have Service Level Agreements (SLAs) in place to ensure peak performance from the service provider they choose. As cloud-wary organizations see that businesses are successfully navigating the cloud without security issues, they'll begin to feel more confident about making the move.
Will The Cloud Continue Its Rise? Or Is It About To Deflate?


No wonder why Samus has not had a new game, because she just wants to take a break (By playing her past games). Well too bad, because she's gonna have to play in Smash Bros U and 3DS.
There is no puzzle without a solution!
How sticker star should've ended!
Sorry had to put in 1 more.


It lies in a cleft where Asia is literally splitting apart, the beginnings of a future ocean.
Geologists say Baikal today shows what the seaboards of North America, Africa and Europe looked like as they began to separate millions of years ago.
One of the world's oldest geographical features (formed 25 to 30 million years ago), magnificent Lake Baikal is the highlight of Eastern Siberia for many. Summer travellers enjoy gob-smacking vistas across waters of the deepest blue to soaring mountain ranges on the opposite shore; rarer winter visitors marvel at its powder-white surface, frozen steel-hard and scored with ice roads. Whether they swim in it, drink its water, skirt its southern tip by train, cycle or dog sled over it in winter or just admire it from 2000km of shoreline, most agree that Siberia doesn't get better than this.
Banana-shaped Baikal is 636km from north to south and up to 1637m deep, making it the world's deepest lake. In fact it's not a lake at all, but the world's future fifth ocean containing nearly one-fifth of the planet's unfrozen fresh water (more than North America's five Great Lakes combined). Despite some environmental concerns, it's pure enough to drink in most places but use common sense. Lake Baikal is one of the clearest and purest bodies of water. In a good day you could see 40 meters into the lake.
More than 5,000 feet deep (1637m) at its most profound, with another four-mile-thick layer of sediment further down, the lake's cold, oxygen-rich waters teem with bizarre life-forms. Lake Baikal is rich in biodiversity. It hosts more than 1,000 species of plants and 2,500 species of animals based on current knowledge, but the actual figures for both groups are believed to be significantly higher. More than 80% of the animals are endemic (found only at Lake Baikal). The Baikal seal or nerpa (Pusa sibirica) is found throughout Lake Baikal. It is one of only three entirely freshwater seal populations in the world, the other two being subspecies of ringed seal.
One of those is the seals' favourite food, the golomyanka, a pink, partly transparent fish which gives birth to live young. Geologists estimate that Lake Baikal formed somewhere 20-25 million years ago, during the Mesozoic.
Surrounded by mile-high snowcapped mountains, Lake Baikal still offers vistas of unmatched beauty. The mountains are still a haven for wild animals, and the small villages are still outposts of tranquillity and self-reliance in the remote Siberian taiga, as the forest is called. The cliff of Sagan-Zaba is one of the most beautiful places on the west coast of Lake Baikal. Situated 5 kilometres to the north-east of Cape Krestovskii in Pribaikalskiy National Park. Anyone who has travelled by kayak along the western coast of Baikal, remembers the moment when the Sagan-Zaba cliff came into sight from behind the promontory Khoboy-Khushun, 2-3 kilometres to the north-east, without fail. From a distance Sagan-Zaba looks majestically gloomy - a comb of massive leg-buttresses disappearing steeply into the water. Sagan-Zaba was given the status of Natural monument. Prehistoric rock paintings - petroglyphs on one of its faces - brought world-wide fame to the cliff. The drawings were executed in different epochs, going back to the bronze and late iron ages (two thousand years B.C. - one thousand years A.D.), that is, the oldest painting is some 4000 years old. The petroglyphs of Sagan-Zaba became known to science in 1881, thanks to the work of Nikolai Agapitov. Subsequently, they have been studied by many archaeological expeditions, some international. The rock paintings of Sagan-Zaba form a composition of figures of humans, and animals.
The lake, nicknamed "the Pearl of Siberia", drew investors from the tourist industry as energy revenues sparked an economic boom. Viktor Grigorov's Grand Baikal in Irkutsk is one of the investors, who planned to build three hotels, creating 570 jobs. In 2007, the Russian government declared the Baikal region a special economic zone. A popular resort in Listvyanka is home to the seven-story Hotel Mayak. At the northern part of the lake, Baikalplan (a German NGO) built together with Russians in 2009 the Frolikha Adventure Coastline Track, a 100-kilometer (62 mi)-long long-distance trail as example for a sustainable development of the region. Baikal was also declared a UNESCO World Heritage site in 1996.
From cattle feed to specialized food used by performance animals, Versele-Laga has a developed a wide range of animal and pet nutrition that answers the needs of breeders and competitors.


A Son of Two Countries is a story of struggle for education. Born in 1946 in Rwanda under Belgian colonial rule, the author recounts his early education in Rwanda and later as a refugee in Tanzania. He was naturalized as a Tanzanian citizen in 1980 while doing his undergraduate studies at the University of Dar es Salaam. As he struggled to get education, the author was also grappling with his refugee status, with all the challenges that it entailed.
The book gives insights into the contradictions of colonial and post-colonial education, as well as the author's reflections on education in Tanzania, given his long experience in the education sector in that country. Finally, we get some glimpses into the dual identity of the author as a Tanzanian citizen of Rwandan origin and how this shaped his relationship with the two countries he calls home. As he aptly puts it, "Rwanda gave me my heart; Tanzania gave me my brain. I find it difficult to choose between my heart and my brain".
Casmir M. Rubagumya (Ph.D., Lancaster) is professor of linguistics and Deputy Vice Chancellor (Academic) at St. John's University of Tanzania. Prior to his present post, he taught and held various leadership positions at the University of Dar es Salaam (1982- 2008) and the University of Dodoma (2008- 2013).


text:
Q: Are TCP Packets Received when Requested I have a server process running that listens on a port. I can establish the connection with this port, but when I try to send data, the client reports that data has been sent, while the server never receives it.
I am using WireShark to trace the data, and I can't find the data packet I sent, which means it was never received. So here's my question. Does this mean that:

*

*The packet has never reached the network adapter on the server side?
or,

*The server process never called the receiving API (recv() or equivalent)?
In other words, are TCP packets transmitted only when the receiving side calls the receiving API, or are they transmitted automatically whenever they are sent, and the receiving API only reads the buffered data?

redpajama_set_name: RedPajamaStackExchange


Many people have heard of THC, but a growing number of patients are seeking cannabis varieties high in CBD (cannabidiol), a non-psychoactive component of the plant potentially being used to treat a broad spectrum of ailments such as neuropathic pain, cancer, severe epilepsy, MS, arthritis, schizophrenia, anxiety, PTSD and sleep disorders. Because CBD does not cause a "high", it has the advantage of being a medicine with very few side effects. Until recently, the availability of high-CBD strains was quite scarce for medical users. However, Santa Cruz has since become a vital region for breeding newly discovered varietals of CBD-rich cannabis.
KindPeoples in Santa Cruz maintains one of the largest and most diverse cannabis seed banks in the state and actively supports our local community's unique culture of world class geneticists, cultivators and producers of cutting edge medicinal products. Our small coastal region produces a spectacular array of CBD medicines for cannabis patients ranging from topical ointments, oral sprays, capsules, tinctures, and baked goods, to oil concentrates, vaporizer pens and dried flowers. KindPeoples dedicates itself to ensuring the potency and safety of these CBD products through lab testing at SC Labs.
While CBD is itself nonpsychoactive, its effects can be greatly enhanced in combination with THC and we offer a wide selection of products featuring a variety of CBD:THC ratios. KindPeoples is enthusiastic about ground-breaking CBD medicine produced right here at home, products that have the potential to change how we treat certain ailments and which are at the forefront of a movement destined to reduce a medical patient's dependence on costly pharmaceutical drugs.
Tinctures and capsules are both highly effective and accessible methods of medicating. Alcohol-based tinctures are absorbed almost instantly for quick pain relief, and capsules can be easily digested for reliable, time-released dosages ranging from very low to very high. The purity of the medicine without any unnecessary ingredients make caps and tinctures an ideal solution for patients with dietary or digestive issues. See the Infused Menu for our full selection of CBD capsules and tinctures.
Cannabis-infused edibles go through a slow release process in the digestive system, so it can take an hour or two to feel the effects but the benefits are long-lasting. With dosages measured in milligrams of medicine, patients can easily find the CBD:THC ratio that works best for them in an assortment of delicious options, from chocolate bars and lemon drops to coconut oil, breath spray and tea. See the Infused Menu for our full selection of CBD-infused edibles.
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Concentrated CBD is one of the most potent forms of medicine. Whether vaporized through a pen or dripper or directly ingested (dabbing), concentrates can be used to effectively manage moderate to severe pain throughout the day. See the Concentrates Menu for our full selection of CBD concentrates.
CBD-rich flower is not typically as potent as other forms of the medicine, but the effects of smoking can be felt almost immediately as the CBD goes straight for the brain receptors. It can also be easily combined with strains rich in THC to provide a wide variety of additional benefits. See the Flowers Menu for our full selection of CBD-rich flowers.
Why not grow your own CBD medicine? We carry a huge selection of seeds and clones form respected breeders such as Medicine Man, Sohum, Midnight Farms and Medicinal Organics, including beloved CBD-rich strains like Harlequin, Cannatonic, ACDC, Pine-Tsu and many others. See the KindGenetics Menu for our full selection of CBD-rich seeds and clones.


text:
Richard Masere est un homme politique papou-néo-guinéen.

Biographie
Il obtient un diplôme de gestion des ressources humaines de l' à Madang en 2003. Il travaille pour la branche océanienne de la maison de commerce japonaise Toyota Tsusho avant d'entrer en politique, et aux élections législatives de 2017 il est élu député d' au Parlement national, avec l'étiquette du Parti de l'alliance nationale.

Après son élection, il devient membre du parti Congrès national populaire, au pouvoir. Il change ensuite d'affiliation en cours de législature et rejoint le Parti de notre développement. En mai 2021, le Premier ministre James Marape le nomme ministre adjoint au bureau du Premier ministre, chargé de la gestion des investissements étrangers. Le mois suivant, il devient ministre adjoint à l'Agriculture, auprès du ministre John Simon. Cette même année, il quitte le Parti de notre développement et devient membre du Parti des Verts de Papouasie-Nouvelle-Guinée, devenant ainsi le premier député de ce parti. Aux élections de 2022, c'est avec cette étiquette et dans la circonscription de Popondetta qu'il est réélu député.

Références

Personnalité politique papouasienne
Personnalité liée à l'écologie politique

redpajama_set_name: RedPajamaWikipedia


text:
\section{Introduction}

Seyfert's Sextet (a.k.a \object{HCG 79}) is one of the most compact and isolated galaxy aggregates in the local Universe\footnote{$v_r\sim4400\ \rm{km\ s^{-1}}$ (\citealt{durbala}) implies $D\sim60\ \rm{Mpc}$ for H$_0=73\ \rm{km\ s^{-1} Mpc^{-1}}$. At the distance of the group 1' is equivalent to 17.1 kpc} (\citealt{hickson82}, \citealt{sulentic87}, \citealt{iovino}).
The group involves four accordant redshift galaxies (H79abcd) plus what we interpret as
a largely dissolved remnant galaxy H79f, which some would call a tidal tail (see Fig. \ref{fig:1}-left for the optical image and labeling). A background galaxy H79e appears projected within the boundaries of the group ($v_r\sim19809\ \rm{km\ s^{-1}}$).
Basic properties of the galaxies are listed in Table \ref{tab:1}.
In the context of evolution of galaxy aggregates, a group of early-type galaxies embedded in a stellar halo must represent an evolved system while groups containing mostly late-type galaxies should be in earlier evolutionary phases (\citealt{Mulchaey}).
Multiwavelength observations of HCG 79 support the hypothesis that it is a highly evolved system probably still growing by occasional infall of late-type neighbors. This must be a very slow process because HCG 79 has few neighbors to accrete within several Mpc (\citealt{durbala}, D08 hereafter).
The extreme compactness of Seyfert's Sextet (the group diameter is $\sim 1.3$ arcmin, $\sim 23$ kpc),
the low velocity dispersion ($\sigma_v\leq 200$ km/s), the number of early-type members (3 out of 5, Table \ref{tab:1}), the fraction of total light in a diffuse optical component ($\sim 40-50\%$), the star formation suppression and the lack of a high luminosity AGN suggest that it should be at a late evolutionary stage.
Some of these features are also observed in other evolved compact groups, which show an X-ray luminosity L$_X\gtrsim5\times10^{41}$ erg s$^{-1}$\  (e.g. HCG 15, 51, 42, 62, 92; \citealt{rasmussen}, \citealt{sun}, \citealt{finoguenov}, \citealt{morita}, \citealt{trinchieri03,trinchieri05}). Another clue that HCG 79 is relatively old and evolved comes from the sizes and luminosities of its early-type members. They are too bright for their sizes, consistent with stripped spiral bulges. This was demonstrated by comparing sizes and luminosities of HCG 79 members with the bulges of typical spirals in the HCG 79 neighborhood (D08).
In the context of galaxy structure evolution, groups are expected to become more prominent in the X-ray band as they grow older, therefore in this scenario it would be reasonable to expect a strong diffuse and relaxed X-ray component associated with HCG 79.

VLA maps (\citealt{verdes}) suggested that HCG 79 is gas deficient in HI, although the expected HI content itself is somewhat uncertain, due to the uncertainties on the morphology of its original members. Subsequently, however, single-dish GBT observations detected an extended, very low surface brightness HI component (\citealt{borth}) missed by the higher resolution VLA map, better reconciling the amount of neutral HI gas with expectations.
At the same time, a search for additional gas, hidden in a hot component, motivated us to ask for deep \textit{Chandra} observations of this system, which we are now presenting here.

\begin{table}
\caption{Properties of the member galaxies of Seyfert's Sextet and discordant galaxy H79e.}
\label{tab:1}
\centering
\begin{tabular}{cccccc}\hline
\small{HCG 79} & v$_r$ & Type & D$_{r}$ & L$_{r}$ & L$_{X}$\\
\small{ } & (km s$^{-1}$) &  & (kpc)&\ ($10^9$ L$_\odot$) & erg s$^{-1}$\ \\ \hline
a & 4292 & E3 & 8.1 & 7.9 &$2.6\times10^{39}$\\
b & 4446 & S0 & 6.5 & 8.7 &$1.9\times10^{39}$\\
c & 4146 & S0 & 5.3 & 3.5 & $< 1\times10^{39}$\\
d & 4503 & Sd & 7.6 & 1.4 &$3.5\times10^{39}$\\
e & 19809 & Sc & -- & -- & --\\
f & 4095 & remnant & 5.1 & 0.7 & --\\\hline
\end{tabular}
\begin{list}{}{}
 \item[ ]{\textbf{Notes.} $D_r$ is the semimajor axis of the last concentric isophote in the \textit{r} band. Data taken from \cite{durbala}. L$_{X}$ in the (0.5-5) keV energy band from this paper, see section 2.4.}
\end{list}
\end{table}

\cite{pildis} reported an X-ray detection of HCG 79 at 2.6 $\sigma$ level with ROSAT/PSPC in the soft energy band (0.1-2.4) keV. The observation yielded only $28.4\pm11.1$ net counts which, considering the relatively poor PSPC resolution, could not be properly attributed to the different components of HCG 79. \cite{nishiura} subsequently used the ROSAT data and estimated a soft X-ray luminosity of L$_X\sim2-3\times10^{40}$ erg s$^{-1}$\  for the group.
They further suggested that, while the ROSAT data did not resolve the emission, it was nonetheless indicative of the presence of a soft X-ray halo morphologically similar to the diffuse optical light.

In this work, we present a detailed analysis of a pointed \textit{Chandra} observation of HCG 79. The observation was requested in order to separate the individual galaxy contribution from that of the diffuse group emission, and to study the X-ray morphology and spectral characteristics of the different components. We discuss Seyfert's Sextet in the context of other compact groups and their evolution.
The structure of the paper is as follows: in Section 2 we present the X-ray data of Seyfert's Sextet obtained with \textit{Chandra}, in Section 3 we describe the main properties of the background cluster we detect with this data, in Section 4 we summarize our results.

\section{Data Analysis and Results}
HCG 79 was observed with \textit{Chandra}'s back-illuminated CCD S3 (ACIS-S in imaging configuration) on May 20, 2010 for a total of 70 ks, observation ID 11261. The basic X-ray data reduction was based on the \textquotedblleft CIAO science threads\textquotedblright\  given on the \textit{Chandra} X-Ray Center (CXC) Web site\footnote{{http://cxc.harvard.edu/ciao/}}.
We also used \textquotedblleft Sherpa\textquotedblright\ \footnote{http://cxc.harvard.edu/sherpa/index.html}, the \textquotedblleft funtools\textquotedblright\ tasks, ds9 and corollary software\footnote{{http://hea-www.harvard.edu/RD/index.html}}. For the spectral analysis we used XSPEC\footnote{{http://heasarc.nasa.gov/xanadu/xspec/}} 12.6.0.
No background ``flares'' affected the observations, therefore the useful exposure time is 70.0 ks.
All quantities are derived from the event file in the broad energy band (0.5-5.0) keV chosen to maximize the signal.

\subsection{X-ray Images}

\begin{figure*}
\resizebox{\hsize}{!}{\includegraphics{Fig1_left.ps}
\includegraphics{Fig1_right.ps}}
\caption{\textit{Left}: optical image of the Seyfert's Sextet from the HST archival image [WFPC2, F555W filter] with (0.5-5) keV X-ray contours superimposed; the contours are logarithmically spaced and the first displayed is at $0.29 \times 10^{-5}$ ct s$^{-1}$ pix$^{-1}$. The original Hickson labeling of the galaxies is indicated. \textit{Right}: raw smoothed \textit{Chandra} image with optical contours of HCG 79 and brighter sources overlaid.}
\label{fig:1}
\end{figure*}

The X-ray emission in the HCG 79 region was imaged by smoothing the 0.5 to 5 keV \textit{Chandra} data using
the \texttt{csmooth} routine with a Gaussian filter adopting 3$\sigma$ as the minimum significant signal
within the kernel on an image binned at $\sim$1''/pix. Fig.~\ref{fig:1} shows the resulting image in the region of interest: in the left panel we show the X-ray contours superposed on the optical image and in the right one we show the smoothed X-ray image with optical contours from the HST archive.  X-ray emission can be identified from: a) individual sources connected with the optical galaxies (e.g H79abde, see Table~\ref{tab:100}), b) some diffuse emission between the galaxies in HCG 79, and c) a strong extended source NW of the group and likely associated with a  background cluster of galaxies. Our goal in this study is to properly separate the different components and quantify the emission from the group.
We therefore produced an X-ray image of the pure extended component, shown in Fig. \ref{fig:2}-left, which we  obtained ``refilling"  all point sources detected (see Section 2.2) with the emission from neighboring regions [CIAO's tool: \texttt{dmfilth}]. The X-ray contours of the diffuse emission were then compared to the optical diffuse halo of HCG 79, shown in  Fig. \ref{fig:2}-right (adapted from D08).

\begin{figure*}
\resizebox{\hsize}{!}{\includegraphics[scale=0.32]{Fig2_left.ps}
\includegraphics[scale=0.32]{Fig2_right.ps}}
\caption{\textit{Left}: raw smoothed X-ray image of the Sextet and its surrounding region with point sources subtracted. \textit{Right}: B+R image of HCG 79 with its optical luminous halo adapted from D08. X-ray contours of the pure diffuse hot emission are superimposed on the optical image; the contours are logarithmically spaced and the first is displayed at $0.21 \times 10^{-5}$ ct s$^{-1}$ pix$^{-1}$.}
\label{fig:2}
\end{figure*}

\subsection{Discrete X-ray sources}

\begin{table*}
\caption{Positions, net counts, fluxes and luminosities of the sources detected within and around HCG 79.}
\label{tab:100}
\centering
\begin{tabular}{ccccccl}\hline
\small{Source} & RA(J2000) & Dec(J2000) & Net Counts& $f_{x}$ (0.5-5 keV) & $L_{X}$ & Notes\\
\small{Number} & (hh mm ss) & ($^\circ$ ' '' ) & &erg cm$^{-2}$ s$^{-1}$ & erg s$^{-1}$&\\ \hline\hline
1 & 15 59 10.974 & +20 45 45.11 & $8.9\pm3.3$ & $6.9\times10^{-16}$ & $3.2\times10^{38}$ & H79c\\
2 & 15 59 11.200 & +20 45 17.07 & $26.0\pm5.2$ & $2.0\times10^{-15}$ & $9.5\times10^{38}$ & H79a\\
3 & 15 59 11.856 & +20 44 54.11 & $63.4\pm8.0$ & $4.9\times10^{-15}$ & $2.3\times10^{39}$ & H79d\\
4 & 15 59 11.857 & +20 44 48.58 & $9.4\pm3.3$ & $7.3\times10^{-16}$ & $3.4\times10^{38}$ & H79d\\
5 & 15 59 12.564 & +20 45 48.02 & $38.5\pm6.5$ & $3.0\times10^{-15}$ & $1.4\times10^{39}$ & H79b\\\hline
6 & 15 59 04.430 & +20 45 27.37 & $9.5\pm3.2$ & $7.4\times10^{-16}$ & -- &\\
7 & 15 59 10.345 & +20 46 19.50 & $45.5\pm6.9$ & $3.5\times10^{-15}$ & -- & \tiny{FIRST}\\
8 & 15 59 11.695 & +20 45 09.47 & $9.3\pm3.2$ & $7.2\times10^{-16}$ & -- & \tiny{SDSS }\\
9 & 15 59 12.778 & +20 45 12.70 & $7.3\pm3.0$ & $5.7\times10^{-16}$ & -- &\\
10 & 15 59 13.215 & +20 45 39.34 & $14.6\pm4.0$ & $1.1\times10^{-15}$ & -- & near H79e\\\hline
\end{tabular}
\begin{list}{}{}
\item[ ]{\textbf{Notes.} Flux $f_x$ in the broad energy band (0.5-5) keV is calculated assuming a fixed power law with index $\Gamma=1.7$ and Galactic line-of-sight absorption. Counts from the detection algorithm.}
\end{list}
\end{table*}

We employed a source detection algorithm from the CIAO package (\texttt{wavdetect}) on a section of
the (0.5-5) keV band image that includes HCG 79 and surroundings (a box of size $8'\times8'$).
We used \textit{ds9} to examine all obvious contaminating sources. Several discrete X-ray sources are found within and near HCG 79 and five of them appear to be connected with the galaxies in the group. Only one discrete source was
identified in the strong diffuse emission NW of HCG 79. It corresponds to a radio detection
(see Table~\ref{tab:100}, source \#7) and on the high resolution version of the public HST WFPC2 image
it is spatially coincident with a pair of apparently interacting galaxies, one of which shows a remarkably blue
disk or optical jets. It may belong to the background cluster as discussed in \cite{palma} but no redshift is available.
Table 2 lists the discrete sources found together with their optical counterparts within HCG 79 whenever available
or with other identifications from the literature. We report their positions, net counts and
uncertainties (as estimated by the detection algorithm) and the (0.5-5.0) keV flux obtained
assuming a constant conversion factor of $7.8\times10^{-17}$  erg cm$^{-2}$ s$^{-1}$ counts$^{-1}$
(corresponding to a power law with $\Gamma=1.7$ and Galactic line-of-sight absorption
$N_{H}=3.8\times10^{20}$ cm$^{-2}$, \citealt{kalberla}). Luminosities are derived
assuming $D=60.4$ Mpc only for sources associated with HCG 79, since no redshift is available
for the other sources. Background source \# 10 in Table~\ref{tab:100} is located near H79e but it does not coincide with the galaxy nucleus.
The X-ray sources associated with the galaxies show (0.5-5) keV luminosities in the range of $\sim10^{38}-10^{39}$ erg s$^{-1}$\ , which are typical of bright sources found in normal galaxies (see review by \citealt{fabbiano06}).
H79a and H79b show evidence for nuclear activity at radio, MIR and optical wavelengths with H79a a bone fide AGN and H79b a minor merger (D08); the X-ray sources associated with these two galaxies, even if coincident with the nuclear position, are at best very low luminosity AGN.

\subsection{Searching for diffuse emission in Seyfert's Sextet}
\begin{figure}
  \includegraphics[scale=0.40]{Fig3.ps}
\caption{\textit{Chandra} image in the (0.5-5) keV energy band. Regions used to derive the radial profile: solid/black for SE region (90 deg to 180 deg counter clockwise from N), dashed/red for the other three quadrants. Black slanted line traces the S3 chip border. Circles indicate detected point-like sources. The color version is available on line.}
  \label{fig:3}
  \end{figure}
In order to quantify the amount and distribution of the diffuse emission associated with Seyfert's Sextet we must first estimate
the contribution from the strong source to the NW of it, which is likely
related to the cluster of galaxies identified by \cite{palma}.
The center of this X-ray emission is consistent with a galaxy well resolved by HST which could very well be the cluster cD.
We produced two radial profiles centered on the peak of the cluster emission (RA = $15^{h} 59^{m}{09.54}^{s}$, $\delta=+20^{\circ}46^{'}{02.82}^{''}$), one taken in the SE quadrant (90 deg to 180 deg counter clockwise from N) where HCG 79 is located and a second in the complementary 270 deg azimuthal region contained in the S3 chip, shown in Fig. \ref{fig:3}. Only a small fraction of the outer annuli falls outside the S3 chip, which we have not included in the area considered.
Point sources were removed using circles with radius $1''\div3''$ following source sizes derived by wavdetect. The profiles are plotted in Fig. \ref{fig:4}-left. Their comparison indicates a clear excess of
counts in the SE quadrant particularly in the radial range 40''$\div$80'' which corresponds to the region
of the group.
Since the excess emission sits on top of the emission from the cluster which extends out to r$\gtrsim80'' $ (see Fig. \ref{fig:4}-left) we need to include it in our estimate of the background for the group. We have therefore assumed that the emission from the cluster is azimuthally symmetric around its center and estimated the background from the annular region at the same distance from the cluster center as HCG 79 in the azimuthal sectors clockwise E to S (dashed in Fig. \ref{fig:3}). This includes also the instrumental and sky background in the field.

We tried to obtain a radial profile of the diffuse group emission to better study its spatial distribution, but the presence of the strong source to the NW together with the weakness of the emission from the group prevented us from finding an obvious X-ray peak on which we could center the profile. Therefore we chose to centre the radial distribution on the optical diffuse halo first discussed by \cite{darocha05} (see also Fig. \ref{fig:2}-right). In Fig. \ref{fig:4}-right we show the resulting radial profile. The background for each annulus of the profile was estimated taking into account the emission from the cluster as discussed above. We can see that the profile does not peak at the center of the optical halo but has a stronger emission at a radius of 15''$\div$35''.

Fig. \ref{fig:2}-left shows the most useful representation that we could obtain by generating an X-ray image with
all discrete sources subtracted. This suggests that the diffuse emission in HCG 79 involves two separate components: 1) the region of galaxy H79a and 2) the region of galaxy H79b and its surroundings, of about 100 counts each. Part of the latter emission might be due to the background source near H79e. This extended emission could be regarded as a halo component specific to those galaxies or the candidate for diffuse X-ray substructure in HCG 79. With the limited statistics and the complexity of the field, it is unlikely that we can resolve the issue at this time. The presence of the background galaxy H79e represents an additional source of noise to our analysis, since in spite of it being further away, it could still contribute: for instance a reasonable luminosity of $\sim10^{40}$ erg s$^{-1}$\  would contribute $\sim 10$ net counts, and a moderate starburst could give a higher contribution.

\begin{figure*}
\resizebox{\hsize}{!}{\includegraphics[scale=0.32]{Fig4_left.ps}
\includegraphics[scale=0.32]{Fig4_right.ps}}
\caption{\textit{Left}: radial profiles of the total emission centered on the peak of the cluster's emission.The regions used for the profiles are shown in Fig.\ref{fig:3}. Black/filled symbols refer to the SE quadrant (black solid line in Fig.\ref{fig:3}), red/open symbols refer to the complementary 270 deg region (red dashed line in Fig.\ref{fig:3}). \textit{Right}: radial profile of HCG 79 centered at (RA = $15^{h} 59^{m}{11.9}^{s}$, $\delta=+20^{\circ}45^{'}{31.0}^{''}$) the center of the optical halo (\citealt{darocha05}).}
\label{fig:4}
\end{figure*}
In order to better quantify the extended group emission we compared the X-ray surface brightness of 3 regions chosen to separate the galaxy contribution from the intragroup medium (IGM) one (see Fig. \ref{fig:5}).
The (20''/70'') inner/outer radii are dictated by the evidence of an excess emission and are selected to include almost all of the group galaxies. Point sources were removed using circles with radius $1''\div3''$ and correspond to the sources listed in Tab. \ref{tab:100}. We find marginal evidence that the region between the galaxies  (central sector considered) shows a lower surface brightness than (S$_{B}=0.028\pm0.017\ \rm{cnts/arcsec^2}$ compared to S$_{B}=0.050\pm0.011\ \rm{cnts/arcsec^2}$) confirming the impression given in Fig. \ref{fig:1} and suggesting very little emission in the intergalactic intragroup region.

\begin{figure}
\includegraphics[scale=0.44]{Fig5.ps}
\caption{Regions used to estimate the emission of HCG 79 relative to its members are shown on the HST image (see text). The first wedge subtends an angle from 78 deg to 120 deg, the second one from 120 deg to 143 deg, the third one from 143 deg to 189 deg counter clockwise from N.}
\label{fig:5}
\end{figure}

 \begin{figure*}
 \resizebox{\hsize}{!}{\includegraphics[angle=-90]{Fig6_left.ps}
 \includegraphics[angle=-90]{Fig6_right.ps}}
\caption{Spectral distribution for the emission compared to spectral models. The spectrum includes the contribution from H79a, H79b and H79d and excludes the other point sources. Spectral models used: \textit{Left}: APEC and Power Law. \textit{Right}: APEC, Power Law and Gaussian at E$\sim 2.4$ keV.}
 \label{fig:6}
 \end{figure*}

\subsection{Spectral Analysis}
We used the \texttt{specextract} script in CIAO, appropriate for extended sources, to create the spectral matrices and data files for the XSPEC analysis.
In order to improve the signal to noise of our data, we chose to bin the spectra using a minimum of 25 total counts per bin. This is a good compromise between increasing the statistical significance of each spectral bin and having a sufficient number of bins. We used the $\chi^2_{\nu}$ statistics to estimate the goodness of fit.
The Galactic hydrogen column density in the model spectra was fixed at the line of sight value determined from radio surveys ($N_{H}=3.8\times10^{20}$ cm$^{-2}$, \citealt{kalberla}). For the APEC model we used abundances tabulated in \cite{anders}.

We analyzed the spectral data of the Sextet in a slightly smaller region than described above, with inner and outer radii of 40$''$ and 70$''$ to obtain a better S/N (see the region showed in Fig.~\ref{fig:5}); moreover, in order to include H79d as well, we added a box that contains this galaxy rather than expanding the wedge to a larger radius which would add a large portion of the annulus with no emission. We did not try to include H79c due to the high contribution of the cluster in that region. We also considered the counts of the X-ray point sources associated to the optical galaxies H79a, H79b and H79d (which contribute $\sim 137$ net counts), but we have excluded  the point sources unrelated to HCG 79. The background was taken in a region complementary to the region of HCG 79 emission that includes the cluster emission as explained above (see also Fig. ~\ref{fig:3}).
The spectral analysis was based on $316.0\pm23.4$ net counts, consistent with those estimated from the excess in Fig. \ref{fig:4}, given the different extraction regions and the presence of the emission from the point sources.

Although the quality of the data is such that a single power law can reasonably represent the data (albeit a power law with a very steep index $\Gamma=3.0$), we chose to use a combination of a thin plasma and power law to account for the different components expected to be present: a diffuse ISM/IGM and discrete sources/AGN in the galaxies. When fitting the X-ray spectrum of the source, we found that we could not constrain well the photon index of the assumed power-law component. This component however was necessary to account for emission at high energy. Thus we fixed the photon index at 1.7 and we fitted only the temperature and the two normalizations.
With a fixed abundance at $50\%$ of the solar value, we found an X-ray temperature of kT=(0.3$\pm$0.2) keV and $\chi^2_{\nu}=1.6$ for 23 d.o.f. (Fig. \ref{fig:6}-left).

The high value of $\chi^2_{\nu}$ is primarily due to an excess emission at $E\sim2$ keV, and to a lesser degree to an  excess around 4 keV. We know from the analysis of the \textit{Chandra} background (http://cxc.harvard.edu/contrib/maxim/bg) that there is an Au line contributing at $\sim 2.2$ keV, while no obvious equivalent is visible at 4-5 keV. Before dismissing the $\sim 2$ keV feature as due to a faulty background subtraction, we looked at the 2-3 keV spectral region in different areas of the detector.  We found, for example, that the excess is more prominent in the area around H79a, relative to the area around H79d. We also noticed that different background areas yield different levels of excess emission around $\sim2-2.5$ keV, from no excess to a recognizable bump.  We also looked at the possibility of contribution from one of the detected sources, which we include in the overall spectra.  We concluded that the excess is most likely due to fluctuations in the background and we resolved to model it with a Gaussian line, with peak energy at $\sim 2.4$ keV, which reduces the  $\chi^2_{\nu}$ value to a more reasonable value $\chi^2_{\nu}=1.0$ for 20 d.o.f. (Fig. \ref{fig:6}-right).

With the inclusion of the Gaussian line to account for the Au line, the best fit temperature is (0.4$\pm0.2$) keV.  The corresponding unabsorbed flux and  luminosity for the plasma component are $f_X\sim 4.3 \times 10^{-15}$ erg cm$^{-2}$ s$^{-1}$, $L_X\sim 2.0\times 10^{39}$ erg s$^{-1}$\ . The  power law component contributes  $f_X\sim 2.0\times 10^{-14}$ erg cm$^{-2}$ s$^{-1}$ and  $L_X\sim 9.6\times 10^{39}$ erg s$^{-1}$\ . This value is entirely consistent with the integrated X-ray luminosity expected from the low mass X-ray binary component
present in the sum of all galaxies, derived from the L$_X$(LMXB)/L$_{B}$ relation of \cite{kim}.

Using the spectral information obtained from the whole source, we estimated the luminosity that we can attribute to individual galaxy. For each galaxy we assumed an elliptical region with major axis from Table 5 of D08, corresponding to the last concentric isophote in the SDSS \textit{g} band. We chose local background regions near each galaxy, which should include the contributions from the instrument, the cluster and any diffuse emission from the group. The results are reported in the last column of Table \ref{tab:1}, where the L$_X$ corresponds to the total excess above the surrounding emission inclusive of point sources if inside the ellipse. Note that in Table \ref{tab:100}, the luminosity L$_X$ refers only to the point sources found from the detection algorithm. As expected, the sum of the contributions from the galaxies is more than 70\% of the total emission detected.

\section{The background cluster source}
\begin{figure*}
\includegraphics[width=8cm]{Fig7_left.ps}
\vskip -8.0truecm
\hskip 8truecm
\includegraphics[angle=-90,width=9cm]{Fig7_right.ps}
\vskip 0.1truecm
\caption{\textit{Left}: net radial profile centered on the peak of the cluster emission (red open symbols). The solid line represents the best fit obtained with a $\beta$ model with $\beta\sim0.7$ and $r_c\sim25.5''$. \textit{Right}: spectral distribution of the cluster's emission. The spectrum contains about $573.7\pm38.6$ net counts, binned to have at least 18 net counts in each spectral bin. Spectral model is APEC, the fit gives $\chi^2_{\nu}=0.5$ for 26 d.o.f.}
\label{fig:7}
\end{figure*}

In order to better investigate its nature, we have also analyzed the emission from the source to the NW, which we attribute to a background cluster. We have produced a radial profile centered on the NW X-ray peak (Fig. \ref{fig:7}-left). We used concentric annuli with outermost radius of $\sim90''$. We estimated the background in a concentric annulus with inner/outer radii of 100$''$/130$''$ excluding the SE region containing the group.
We fitted this profile with a $\beta$-model distribution ($S(R)=S_0[1+(R/r_c)^2]^{-3\beta+0.5}$), traditionally used to describe the surface brightness profiles of clusters and groups of galaxies (e.g. \citealt{jones84}), plotted in Fig. \ref{fig:7}-left. The best fit parameters obtained are: $\beta=0.7 \pm0.2$ and $r_c=25 \pm 8$ arcsec, corresponding to a size of 109.31 kpc (if we assume the redshift $z=0.3$ as the lower limit estimated by \citealt{palma}).

The X-ray spectrum for the NW source and relative background were extracted from a circle of 65'' radius centered on the cluster's peak, but excluding a SE box at the position of the group, and the adjacent annulus, with $80''<r<130''$ respectively. The spectrum contains $573.7\pm38.6$ net counts (Fig. \ref{fig:7}-right). To obtain a
reasonable statistical significance and no negative bins in the energy range considered, we chose to bin the data to have 18 net counts per bin.

We assumed a thin plasma model (APEC) with the abundance fixed at 50\% of the solar value and a Galactic hydrogen column density ($N_{H}=3.8\times10^{20}$ cm$^{-2}$, \citealt{kalberla}). The fit gives $\chi^2_{\nu}=0.5$ for 26 d.o.f..
Given the limited quality of the data, we could only derive a temperature kT$\sim6$ keV ($\gtrsim$3 keV), which corresponds to an  unabsorbed flux $f_X \sim5.52  \times 10^{-14}$ erg cm$^{-2}$ s$^{-1}$. Assuming photometric redshift $z=0.3$ (the lower limit reported by \citealt{palma}) and  kT$\sim6$ keV we found a luminosity of $L_X\sim 1.5\times 10^{43}$ erg s$^{-1}$\  in the (0.5-5) keV band.
Assuming that the source is spherically symmetric, we can correct for the missing area due to the presence of the group and estimate that the total luminosity from the cluster amounts to $L_X\sim 2\times 10^{43}$ erg s$^{-1}$\  in the (0.5-5) keV band.
The parameters found are consistent with a low luminosity cluster of galaxies (e.g. \citealt{pacaud07}, \citealt{sarazin86}), but we need more detailed information on this source to draw firm conclusions on its nature.

\section{Discussion and Conclusions}
X-ray observations of HCG 79 show that the field is rather complex with an X-ray bright background galaxy cluster accounting for most of the detected
emission. The excellent quality of the \textit{Chandra} data enables us to separate emission from HCG 79 and the cluster with reasonable confidence.
We find the group to be extremely deficient in X-ray emission: the total (0.5-5) keV luminosity originating from HCG 79 is $L_X\sim 1.2\times10^{40}$ erg s$^{-1}$\ , of which only $L_X\sim 2.0\times 10^{39}$ erg s$^{-1}$\  can be ascribed to a gaseous component. Most of the detected counts appear to be associated with individual galaxies (primarily H79a to the W and H79b and its surroundings to the E, cf. Table \ref{tab:1} and Fig. \ref{fig:2}-left) and therefore it is unlikely that we have detected ``bona-fide'' diffuse group emission. The reality of any diffuse emission of course depends upon our assumption that the background cluster source is relaxed without any subcluster emission on the side towards HCG 79. The discontinuity between the low inferred temperature of the emission from HCG 79 and the hot background cluster source adds support to the plausibility of our assumption.

The weakness of any diffuse emission from the intergalactic medium has significant implications for our understanding of compact group evolution.
Theoretical models predict the coalescence of compact groups into a single object (\citealt{governato}; \citealt{atha}), possibly a fossil elliptical, which should be characterized by significant X-ray emission (Jones et al. 2003). Most current models assume that groups coalesce by major merging. Instead the detailed study of HCG 79 (D08) points toward a slow and quiet dissolution process rather than coalescence by major merging, in line with the model by \cite{atha} which indicates that groups embedded in a massive dark matter halo can persist much longer.

HCG 79 is a very compact group with member galaxies too luminous for their small sizes (D08). These ``compact'' galaxies are embedded in an optical halo that contributes 50$\%$ of the total group light. Based on the inferred mass of this diffuse halo, its color, the isolation of the group, and the size/luminosity similarity of group members to bulges of spirals in the neighborhood, D08 proposed that current members are remnants of larger galaxies embedded in their own debris halo. If this interpretation is correct, then the major challenge connected with this group is to explain the small amount of hot gas that it contains.

\cite{verdes} has argued that HCG 79 is also deficient in cold gas based on VLA observations of the HI content. Subsequent single-dish GBT data (\citealt{borth}) has reduced the evidence of cold gas deficiency in HCG 79 if estimated based upon current galaxy morphologies. The total HI mass (4.3$\times$10$^9$ M$_{\odot}$, \citealt{borth}) associated with the group is typical of a single spiral galaxy, and at least 2$\times$10$^9$ M$_{\odot}$ is coincident with H79d (D08). The low surface brightness component found with single dish observations might be the remnant of an earlier stripping event. The expected HI content in HCG 79 is uncertain, as also suggested by \cite{verdes} and D08, due to the uncertain morphologies of HCG 79 members when they first entered the system. If we assume, as suggested in D08, that at least some of the current early-type members entered the group as spirals then we would infer a much higher gas deficiency. On the contrary HCG 79 is a HI-normal system if the intruders were passive spiral galaxies (galaxies with a spiral morphology and lack of star-formation activity; \citealt{dressler}, \citealt{poggianti}). \cite{bundy} show that these passive galaxies tend to be Sa-Sb types, more abundant at low mass, and presumably gas poor; they might not be as rare as inferred by \cite{goto}.

In order to evaluate the peculiarity of HCG 79 we searched for other compact groups where diffuse optical halos have been measured and for which X-ray data is also available. We found four compact groups: HCG 15, HCG 51, HCG 90, HCG 92, with available X-ray observations. All four are bona fide compact groups possessing n$>$ 4 accordant redshift members and clear signs of dynamical evolution. We use the diffuse optical halo light fraction as a chronometer to rank the groups by age -- groups with a larger halo light fraction should be older.

The first comparison is with the well studied Stephan's Quintet (HCG 92); both typify evolved compact groups. Their significant diffuse light fractions leave little doubt that they are physical aggregates with Stephan's Quintet younger (and more massive) than Seyfert's Sextet.
\object{HCG 92} is less relaxed and contains a lower diffuse light fraction ($\sim30$\%) (\citealt{moles}). Two spirals in Stephan's Quintet are in the process of transformation from spiral into lenticular galaxies and the presence of a high velocity intruder produces a large scale shock confirmed by \textit{Chandra} and XMM-Newton observations (\citealt{trinchieri03,trinchieri05}). Separating shocked and diffuse X-ray components enabled \cite{trinchieri05} to estimate the luminosity of the diffuse (non-shocked) X-ray component in HCG 92: $L_X\sim5\times10^{41}$ erg s$^{-1}$\  (0.5-2 keV; \citealt{trinchieri05}). Although not particularly X-ray luminous, this value is two orders of magnitude larger than the extremely low X-ray luminosity of HCG 79.

Another group of possible relevance involves \object{HCG 90} which consists of a core of three bright galaxies (two ellipticals and a disturbed disk galaxy) surrounded by an extended loose group. The contribution of the diffuse light to the total light is of the order of $\sim 45 \%$ L$_{tot}$, close to HCG 92 and 79. Low luminosity diffuse X-ray emission was reported by \cite{white} who discussed the observed lack of hot gas in terms of expectations from the dynamical state of the system and the evidence for a large reservoir of diffuse optical light. It is interesting to note that, in analogy to what is observed in HCG 79, the X-ray emission in HCG 90 is predominantly concentrated on the galaxies of the group (see Fig. 10 of \citealt{white}). Unfortunately the analogy breaks down there because the luminosity of the gaseous component in HCG 90, $L_X\sim1.6\times10^{41}$ erg s$^{-1}$\  is two orders of magnitude higher than in HCG 79.

The other two groups considered, \object{HCG 15} and \object{HCG 51}, show smaller percentages of diffuse light,  $\sim 20$\% and $\sim30$\% respectively (\citealt{darocha08}). These smaller values would point to dynamically younger systems and hence to smaller fractions of stripped gas. In both cases the intragroup medium content is significantly higher than in HCG 79, L$_X\sim3.2\times10^{41}$ erg s$^{-1}$\  for HCG 15 (\citealt{rasmussen}) and L$_X\sim3.0\times10^{42}$ erg s$^{-1}$\  for HCG 51 (\citealt{sun}).

All the above examples involve systems more massive than HCG 79. Although the velocity dispersion based on a small number of galaxies is a poor indicator of the size of the group potential well, the total luminosities (in stars) and the total masses inferred for these systems are 1-2 order of magnitude larger than estimated for HCG 79 (M$_{tot}\sim3\times10^{11}$ M$_{\odot}$, \citealt{nishiura}). If we then consider that a significantly smaller mass system might not be able to produce enough hot gas and retain it, we could separate issues and consider that the deficit of hot gas in HCG 79
might not be related to its evolution, but simply to its shallow potential and low mass. Had it been possible to have a reliable measure of the total mass of the system we would have tested this hypothesis. At the present time however we notice that the total optical luminosity, HI mass and total X-ray luminosity (in gas and in ``binaries'') are all consistent with what is expected from a normal galaxy. If the final fate of compact groups is in the formation of a single galaxy, then Seyfert's Sextet is likely to become a relatively isolated, normal [rather than giant] galaxy.

\begin{acknowledgements}
S.T., G.T. and A.W. acknowledge financial support from the Italian Space Agency ASI under contract ASI-INAF agreement I/009/10/0. M.R. acknowledges financial support from contract P-82389 from CONACYT and IN102309 from DGAPA-UNAM.

\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


The Greek philosopher Zeno of Elea posed several philosophical arguments that have become collectively known as Zeno's paradoxes. One such argument is known as Zeno's arrow paradox; the simplistic explanation of which is that in order for motion to occur an object must change its location, like an arrow flying to its target, yet at any instantaneous moment the arrow is motionless, and since, as Zeno posed, time is composed of a sequence of many such duration-less instants, then motion of the arrow is impossible. This paradox is actually highly salient to an understanding of the fundamental nature of motion and time, and hence the fundamentals of physics.
Zeno's paradox has found its way into the lexicon of quantum mechanics in a class of phenomena known as quantum Zeno dynamics. As the name would indicate, quantum Zeno effects have to do with time evolution of a system, often with effects that are paradoxically counter to what is normally observed in quantum experimentation. For instance, frequent measurements of a quantum system can in fact arrest its evolution, delaying its decay -- even going so far as to decouple a system from its decohering environment. This is the opposite of what "measurements", or interactions with the environment are normally thought to do in quantum mechanics theory.
In quantum Zeno dynamics, the decoherence rate of a quantum state can be either increased or decreased by how the system is coupled to the environment. When the time evolution or decay of a quantum state is frozen, it is referred to as the Zeno effect. An increased decay rate is known as the anti-Zeno effect, because instead of "freezing" the state of the quantum system in time, it accelerates its time evolution. Frequent measurements will alter how a quantum state, such as a qubit, will interact with the environment, essentially allowing control of quantum evolution with tunable environmental interactions.
Certain schemes of coupling a quantum system with the environment are referred to as "quasi-measurements", as the interaction with the environment does not necessarily transmit information about the state of the quantum system – highlighting that the effect is not necessarily antithetical to the normal description of environmental decoherence in quantum theory.
in the June 14, 2017, issue of Physical Review Letters physicists describe the observation of quasi-measurements producing quantum Zeno effects. Their protocol used a qubit uniquely coupled to a thermal bath to produce both enhanced and diminished decay times. Researchers were able to show that by changing the frequency and type of interaction of the qubit with a noise-source they could arrest the evolution of the system, such that the qubit did not decohere or decay, or they could accelerate the decay.
Does the Zeno effect have relevance beyond quantum computing?
In addition to potential implications and applications in quantum computing, Resonance Science Foundation researchers are taking notice in the results because of potential implications in understanding the finely ordered and coherent state of the biological system. Just as quantum measurements are being utilized to stabilize the fragile state of the artificial qubit, similar mechanisms may be involved in stabilizing quantum states, natural qubits, in the biological system.
For instance, the quantum Zeno effect can be considered in evaluating how theories involving non-classical information processing dynamics in a strongly interacting environment like the cell may in fact be occurring. Information processing that may involve quantum correlation (entanglement) or nonlocal interaction have largely been summarily dismissed because of the presumed high amount of noise of the biological system.
Such a presumption, however, may be problematic or largely erroneous because the molecular structures of the biological system are in a highly ordered arrangement and are comprised of novel forms of matter that have been exquisitely fine-tuned by natural selection over billions of years. It is no stretch of the imagination that novel molecular forms that optimally capitalize on nature's intrinsic properties, such as quantum informational dynamics, will have an immediate selective advantage – highly improved efficiency of photosynthesis and metabolism, greater environmental sensitivity, memory, responsiveness, and perhaps greater cognitive capabilities.
As such, biomolecules may not be comparable to the "simple matter" -- often times individual quanta like free photons and electrons -- used in experimentation where non-classical quantum phenomena are observed. The biological supramolecular assemblies of the cell are a special state of matter. And the large numbers of interacting units and their frequent interaction may in fact enable a certain degree of increased "quantumness" instead of being the primary source of decoherence as is naively assumed.
For instance, there are relatively new developments in quantum mechanics such as quantum discord, where the "quantumness" of correlations can be variable and present in certain mixed separable states – that is to say, quantum correlations that exist but that are not necessarily entanglement. In terms of the relatively high temperature of the biological system, a condition that is supposed to inhibit strong coherence, it has been shown that for a qubit pair in contact with a normally decohering environment, like a heat bath, the strength of correlations can actually increase with increasing temperature.
This brings us to the quantum Zeno effect, where measurements made in rapid succession can actually prolong the quantum coherency of a state. This is quite the paradoxical situation, because measurements are supposed to be the agents of decoherence and decay of quantum states, yet here increased interaction can do the opposite. Leading to the question of whether the frequent interactivity / communication of components of the supramolecular assemblies of the biological system may work to prolong and enhance the lifetime of strongly coupled and coherent states.
Relevant supramolecular assemblies include the plasma membrane, mitochondria, DNA, and microtubules. Mitochondria and microtubules are significant in that they can theoretically function as quantum electrodynamic cavities, where interactions between light, atomically ordered water, and electron dipole moments can form quantum coherent states for intra- and inter-cellular dissipation-less solitonic energy transfer and quantum teleportation.
Mitochondria and microtubules, in close association, form dendritic networks in which coherent photon emission can be channeled through the cell. Coherent photons modulate the electronic properties of biomolecules, a QED-like mechanism that can be used to holographically store information as well as initiate physicochemical responses in the cellular system. This system is referred to as the holographic information network of the mitochondrial reticular matrix.
Intercellular networks are formed by gap junctions and tunneling nanotubes, the latter of which contain filamentous mitochondria and microtubules that can connect multiple cells, enabling gestalt information transmission and processing. Quantum coherence and nonlocal phenomena can enable the cellular information system to perform massively parallel processing, enabling remarkable organizational synergy and unified orchestration of function.
As explained in the manuscript the Unified Spacememory Network by Nassim Haramein et alia, nonlocality is a result of spacetime geometry, such that entanglement is the manifestation of multiply-connected spacetime architecture, i.e. a Planckian micro-wromhole network, or quantum spacetime foam. This multiply-connected geometry represents a kind of hyperspace, comprised of information resulting from the quasi-instantaneous communicativity of all spacetime frames across spatial and temporal domains. The interaction across this transtemporal, nonlocal connectivity network is one way in which memory, recorded in the entanglement connectivity patterns, is produced. Hence the moniker, spacememory network.
This has important implications for considerations of entanglement and other quantum processes of nonlocality in the biological system. Specifically, entanglement necessarily results from the underlying spacetime geometry – therefore any such process interlaces functions of the biological system with the informational manifold of the spacememory network. A possibly important dynamic that, theoretically, would be intricately and inextricably involved in processes of evolution, development, sentience and memory of the living system.
Experiments that advance our understanding of quantum entanglement and other phenomena involving nonlocality, like the testing of quantum Zeno dynamics with qubit stability, are important for developing a deeper understanding of how nature may be utilizing quantum dynamics, particularly in the biological system. While theoretical considerations of quantum coherence, entanglement, and other nonlocal phenomena in the living organism remain relatively controversial, the true test of these ideas will be to conduct experiments aimed at observing just such phenomena. Resonance Science Foundation researchers are designing experimental protocols to do exactly that, so that soon they will be able to experimentally test whether or not the entanglement and information exchange with the nonlocal spacememory network is in fact supported observationally and empirically.


text:
Primary Source Spotlight: Tokamahamon
Photo: Part of the Nemasket Trail in Plymouth MA
When it comes to early Plymouth Colony there are many well-known names that show up in history books: Bradford, Massasoit, Brewster, Squanto. However there are a multitude of lesser known people who played important roles in Plymouth Colony's beginning. Today we will explore one such person, Tokamahamon.
There is much that is unknown about Tokamahamon, especially his personal life. We do not know things like how old he was, or whether he was married had children etc. We are however able to piece together from the primary sources a picture of an important person, who during the first few years of Plymouth Colony, seems to have performed a similar role as Squanto and Hobomok.
The first mention of Tokamahamon by name is during Edward Winslow and Stephen Hopkins' journey to Pokanoket to visit Massasoit. While there, Massasoit requested to retain Squanto there for a time "…and appointing another, called Tokamahamon, in his [Squanto] place, whom we had found faithful before and after upon all occasions" (Mourt's Relation 67). Thus Tokamahamon was appointed by Massasoit himself to assist the pilgrims. From this appointment we can infer that Tokamahamon had an understanding of English in some capacity and that Massasoit trusted him enough to serve as a representative.
Tokamahamon's role as an interpreter, similar to both Squanto and Hobomok, is brought up again when the colonists travel to Nauset to retrieve John Billington Jr. When they set out they take along "…Squanto, our interpreter, the other Tokamahamon, a special friend" (Mourt's 69). During the voyage they encountered some Nauset people gathering lobsters and "…sent our two interpreters [Squanto & Tokamahamon] to speak with them…" (Mourt's 69).
Tokamahamon is mentioned as serving a diplomatic role similar to Squanto and Hobomok as well. When Plymouth hears that Corbitant, the leader of Nemasket, is upset and trying to draw people away from Massasoit it is mentioned that he was "storming at the peace between Nauset, Cummaquid, and us, and at Squanto the worker of it; also at Tokamahamon, and one Hobomok…" (Mourt's 73). When he heard of this "Tokamahamon went to him [Corbitant]" (Mourt's 73) to seemingly try his hand at diplomacy with Corbitant. Later, when the colonists, led by Capt. Standish, raided Nemasket to avenge Squanto whom they, incorrectly, heard had been killed; once again Tokamahamon assisted for "In this hurley-burly we discharged two pieces at random, which much terrified all the inhabitants, except Squanto and Tokamahamon, who, though they knew not our end in coming, yet assured them in our honesty, that we would not hurt them." (Mourt's 75).
The last mention of Tokamahamon in the primary sources is in 1622, when a messenger arrives from the Narragansett "who was sent by Conanacus, their chief sachim or king, accompanied with one Tokamahamon" (Good News from New England, Winslow 8) Bradford not only recognized Tokamahamon to be friendly, despite traveling with a messenger carrying a challenge, they asked his opinion on the matter. His "answer was sparingly to this effect, that he [Tokamahamon] could not certainly tell us, but he thought they [Narragansett] were enemies to us" (Winslow 8). Further, when the Narragansett messenger wished Tokamahamon to return with him the result was "The weather being violent, he [Tokamahamon] used many words to persuade him to stay longer, but could not. Whereupon he left him, and said he was with his friends, and would not take a journey in such extremity." (Winslow 9).
After 1622, Tokamahamon stopped showing up in Plymouth sources. Whether this means he moved on to other areas, passed away, or the colonists simply stopped referring to him by name, we may never know. However despite this, his contributions in the first few years are just as influential as some of the other more well-known names and should not be forgotten to history.
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Nothing is more American that Country Music. Whether they are working on their next broken heart, throwing it into overdrive on a Friday night, reminiscing about lost youth,or taking a trip to church, they hit at the heart of everyone in small town America. Case is proud to introduce the inaugural family of quality Brooks & Dunn knives featuring laser-embellished Smooth Natural Bone handles with the recognizable Brooks and Dunn steer head logo.


Deli and cheese shop to open this spring.
A cheese shop, deli and small grocery store all-in-one is coming to Northside's Hamilton Avenue business district.
Morsel and Nosh is a "career 2.0" for Michael Heerkens, a former IT professional, who is opening the shop with his husband Mark Dreibelbis.
The store, at 4183 Hamilton, is the brick and mortar version of Heerkens' catering company. He said they like to entertain with small bites, putting out cheese and meats, olives, nuts and bread, as an easy way to feed a gathering.
Heerkens supplies a few local bars and restaurants with cheese and meat trays. He made a Kentucky beer cheese for Urban Artifact and puts together plates for Tilly's and Higher Gravity.
That's the inspiration for what they'll stock at Morsel and Nosh.
A cheese case will hold cheese of all kinds: regional, local, American and imported, along with salamis and other kinds of charcuterie. The shelves will be stocked with olive oil, crackers, balsamic vinegar, Marcona almonds and other such accompaniments.
Northsiders told him they really wanted a deli on Hamilton, so the store will also have a deli with meats sliced to order, homemade pate, potato and macaroni salad, hummus, baba ganoush, tabouli, and other salads.
Everything will be prepared to go, there is no seating.
The store will open this spring if all goes as planned.


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Italian Archbishop Stresses Importance of LGBT Ministry
October 21, 2018 /2 Comments/in Parish Life & Pastoral Care, Politics & Human Rights, Synod on Youth 2018 /by Francis DeBernardo, Editor
The cover of the Italian translation of Fr. James Martin's "Building a Bridge"
At Thursday's synod press briefing, one of the featured speakers was Archbishop Matteo Zuppi of Bologna, Italy. As far as LGBT issues go, Zuppi is probably best known for writing the preface to Un ponte da costruire, the Italian translation of Fr. James Martin's book, Building a Bridge, about improving the relationship between LGBT people and the Catholic Church.
Zuppi, who is known as the "Italian Bergoglio," spoke eloquently about the church as a "communion." He described this idea of communion as antidote to "clericalism and nationalism" which seek to exclude people and close doors. "The Church speaks to everyone and with everyone. No one is to be left out," he said. His talk was one of the moving descriptions of Pope Francis' new approach to pastoral ministry that I have heard hear at the synod so far.
During the question period, I decided to ask him for his impressions on how LGBT topics are being received within the synod. So, I posed this question:
"In your preface to the Italian version of Fr. James Martin's book on improving relationships between the LGBT community and the Catholic Church, you wrote:
'These teachings [about sensitivity, compassion, and respect for LGBT people] have not been followed up with a commensurate pastoral program—one that doesn't simply restrict itself to the cold application of doctrinal guidelines, but instead transforms them into a journey of accompaniment.'
"During your time in the synod, have you seen any bishops moving towards being open to this model of accompaniment for LGBT people or are they still holding on to the cold application of doctrinal guidelines?"
Because of translation problems, I'm not sure that he understood the precise question I was asking, but he did offer a response:
Archbishop Matteo Zuppi
"I believe that pastoral ministry for homosexual people is an important topic. There are different sensitivities, and we must also consider different situations on the basis of geographical areas. It is not viewed the same in the West as it is in Africa. It is not just a new issue. This is borne out by the fact that the group of Catholic homosexuals from Bologna is more than thirty years old. In my opinion, it is a pastoral question, and as such I believe it should be treated: when it becomes ideological it becomes more complex and it is better to leave it aside "
Zuppi's reference to this issue as "important" and his recognition that people have been calling for LGBT pastoral ministry for a long while is good to hear. I understand, too, his acknowledgement that different cultures approach the question from different perspectives and histories. But, I fear that this acknowledgement can sometimes be an excuse to do nothing. Yes, LGBT ministry will look different in Africa or Asia from how it look in the U.S. For that matter, LGBT ministry will look different in Los Angeles from what it does in New York City, Peoria, Houston, Cleveland, and dozens of smaller U.S. cities. But isn't it the responsibility of Catholic leaders everywhere to teach the importance of "respect, compassion, and sensitivity" as the Catechism instructs. Yes, the model of ministry may be different, but the message should be the same.
Similarly, I would hope that church leaders would sensitively respect that cultures around the globe view lesbian/gay relationships and gender identity differently. Marriage equality is a reality in the West. So, why are married lesbian and gay people fired from church jobs, shunned at some parishes, and treated differently by church leaders from other married couples? Respecting cultural norms should work both ways, whether the norm is progressive or traditionalist.
I also agree, mostly, with Zuppi's approach to LGBT issues as pastoral, and not ideological. But, where does pastoral end and ideology begin, or vice versa? Drawing that line will always be a matter of prudential judgement. For some the difference between pastoral and ideological is similar to the difference between spiritual and political. But that doesn't always hold up well from a Catholic perspective. Protecting people's human and civil rights should always be a part of pastoral ministry. Focusing simply on the spiritual is not sufficient for a full gospel response.
—Francis DeBernardo, New Ways Ministry, October 21, 2018
Tags: Archbishop Matteo Zuppi, Building a Bridge, Catholic, James Martin, LGBT, Synod on Youth, Un ponte da costruire, youth synod
https://i1.wp.com/www.newwaysministry.org/wp-content/uploads/2018/10/Synod-Default.png?fit=1080%2C1080&ssl=1 1080 1080 Francis DeBernardo, Editor https://www.newwaysministry.org/wp-content/uploads/2017/09/logo_nwm-1.png Francis DeBernardo, Editor2018-10-21 01:00:042018-10-19 07:50:35Italian Archbishop Stresses Importance of LGBT Ministry
John Montague says:
Thanks to Frank DeBernardo for devoting his energy to being a voice for us gay Catholics. This is who a prophet looks like in this century.
Deacon Thimas Smith says:
This discussion deinds me of the current Presidential Nightmare we face as a nation. While so many complacently dismiss "politics" as a sore subject, they are also dismissing ethics. Jesus' ethics surely motivated His politics. Similarly, our ideology should strongly influence our pastoral approach. Standing by silently witnessing GLBT Catholics suffer spiritual abuse and rejection is similar to allowing empoverished Americans to be deprived of healthcare. So, while our leaders remain reluctant to speak out publicly and challenge the anti-gay terrorist activities threatening our Church for fear of opening the "pandora's box" of ideology, this shameful pastoral crisis continues. Yes, the USCCB needs to act like Jesus and stand with us "in the circle" as He did with the woman unjustly accused of sin, not on the outskirts, silently blending in with the accusers.
Question for Synod: How Can Bishops Learn to Be Listeners? Gay Pastoral Minister Resigns Because of Fear for His Safety


Flight Details: Nice flight. An early morning departure. Not a long wait for takeoff. Nice clear flight with a few strong winds. A hard landing and had to perform a go round as I was too high on initial approach.


You're there to travel out of Denver, but the trip from DIA ticket counters to Concourse C could be regarded as a journey itself at this, the largest American airport by size.
Little did we know, Denver International Airport takes up more space than a few major American cities.
DIA posted a photo comparing its size to Manhattan, San Francisco and Miami. Denver's hub takes up 53-square-miles of space, or 34,000 acres.
Twenty-five airlines, six runways, three concourses -- other airports may hold more but there's room to grow. DIA wrote on Facebook that the current structure was designed to allow for expansion. The goal is 12 runways in the future.
The airport was dubbed the nation's fifth busiest overall by Airports Council International this year. It comes as no surprise that DIA served a record number of passengers in November. Officials are still calculating December data.


The children's commissioners for England, Wales and Northern Ireland have expressed concern at the number of boys using anabolic steroids for cosmetic reasons.
The commissioners said they believed that social media was putting pressure on children to try to achieve what they believed was an ideal body shape.
Experts who work with users of image and performance enhancing drugs (IPEDs) have reported that boys as young as 13 are using steroids.
Social media is seen to pile pressure on children over their body shape and there is also a concern that it makes it easy for them to source IPEDs.
The children's commissioner for England, Anne Longfield, said: "I'd be very concerned with any young person using steroids to enhance the way they look. The real solution is to tackle early on issues around body image and the desire of some young people on social media desperate to match celebrities' images.
Sally Holland, the children's commissioner for Wales, said her office had co-produced a pack for secondary schools encouraging young people to challenge stereotypes about appearance.
"There is a consistent pressure on young people to look and behave in a certain way; a pressure that is often amplified and perpetuated by social media," she said.
"We need all young people to know that there is no definition of 'perfect' and that individuality is to be celebrated.
Koulla Yiasouma, Northern Ireland commissioner for children and young people, said: "It's important to educate young people on how they can keep fit and nourish their bodies in a healthy way.
The Guardian has revealed that up to 1 million people in the UK may be taking IPEDs, the majority for aesthetic rather than sporting reasons.
A particular concern among health officials is teenagers and young twenty-somethings using the drugs when their bodies are still developing. There are real worries they may suffer serious health problems in 10 or 20 years as a result.
Hickmott said those using steroids ranged from talented athletes who wanted to boost their performances to others who simply wanted a honed body to – in their eyes – look good during nights out or on the beach.
He said: "We've got all the pressures of social media saying: 'this is what a young man should look like'. In films, in TV, everyone is ripped and young people think there can't be much harm in it.


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Trowers, an international law firm with over 160 partners, is the latest firm to optimize support for its internal and external clients by opting to convert its BigHand Voice licenses to the full BigHand Workflow Management Solution.
BigHand Workflow Management is a task delegation solution that allows work to be automatically routed to the right support staff at the right cost to the firm and monitored throughout the process. Output reports can be used by management for visibility of key metrics like work type, volume, capacity and utilization to allow firms to make data-driven decisions around staffing, training and performance.
Kate Kirkham, Head of Secretarial Services comments, "I was impressed with the visibility of workloads and reporting capabilities that BigHand Workflow Management offers to management. With the technology in place, we'll be able to see what our teams are working on, and report on key areas like utilization to make more informed business decisions in future."
The forward-thinking firm had already restructured its support teams prior to the pandemic, and benefits from Legal PAs who help oversee and delegate the legal tasks coming from the lawyers, as well as Team Assistants who look after most of the administration work, and a centralized Document Production Centre for all legal document tasks.
Kate continues, "Our lawyers don't want to have to think about who the right person is to complete a task, and soon they won't have to thanks to BigHand. The solution ensures the right resource completes the right work, at the right time and efficiency of cost to the firm. We're increasing our mobility licenses too, which will allow our lawyers to delegate tasks easily, regardless of location. It helps that they are used to using BigHand for dictation too, so training requirements are minimal."
The firm experienced a boost of productivity during lockdown, with support team assistants and PAs able to assist with some tasks outside of their regional remit. BigHand Workflow Management will help to improve the manual processes and accuracy to track team and individual workloads which can be time consuming for support team management.
Kate explains, "We want to encourage our support teams to continue to pick up tasks for different regions, and with BigHand we gain full visibility and can easily move work around wherever needed to enhance turnaround times and optimize service delivery for our lawyers and in turn, for our clients."
Kate Kirkham
Head of Secretarial Services , Trowers & Hamlins
I was impressed with the visibility of workloads and reporting capabilities that BigHand Workflow Management offers to management. With the technology in place, we'll be able to see what our teams are working on, and report on key areas like utilization to make more informed business decisions in future.
Remote Working is a Permanent Reality for Law Firms, Finds ALA Change Management Poll and Expert Webinar Panel
#Legal #Advanced Workflow #News #North America #Workflow Management


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Are full-time Medical Devices contracts a thing of the past?
Are full-time contracts becoming a thing of the past? Matthew Moulton of Real Staffing's Medical Device contract team, has seen a growing trend of QA and RA contractors taking on multiple shorter-hours contracts, instead of the typical full-time hour contracts. With this growing trend, we look at what could be driving this change.
How have Medical Device contractors operated before?
Typically most contractors still work similar hours to full-time employees by taking on five days per week, eight hours per day work. However, Matthew has seen a rise in contractors taking on less lengthy contracts, to work with multiple clients. As we enter an age where candidates are taking more consideration of their roles than just salary, companies in the Medical Device industry are having to become more flexible in their job offerings to attract the best talent.
What are the benefits of having multiple contracts?
It's widely reported that work/life flexibility is an important factor in new roles, which is why the approach to taking on multiple contracts is so attractive. With some roles offering only a few hours per week to work on internal processes and compliances, this has allowed contractors in the Medical Device Regulatory and Quality industry to create their own varied working week. This flexibility can also help increase income for these contractors. With companies competing for talent within this space, this gives candidates the advantage to have a lot more control over their hourly rates.
The introduction of MDR has only helped increase the demand for additional contractors to work on contingency plans, which usually is best suited to contract positions. It's evident that some of these roles are being filled with contractors who also work elsewhere throughout the week. Some of these roles can be done remotely which is also an attractive benefit to contractors who seek a better work/life balance. Matthew has noticed a recent rise in the popularity of these types of roles, explaining; 'since the introduction of MDR within Medical Device companies, over 20% of my placements in the last 12 months have been with contractors who are also undertaking additional contract work, on top of their current roles'. As well as the additional salary and flexibility benefits, by adopting this way of working contractors will also fall outside of IR35, as they would no longer equate to the same working patterns as a full-time employee.
How can Real Staffing help support working with multiple contracts?
After years of experience recruiting into the Medical Device industry, Matthew has been actively seeking candidates who are open to the opportunity of a short-term contract alongside their current role.
In the last 12 months he's seen a rise in job vacancies for shorter-term hours and is seeking new people to fill these new contracts. His experience in recruiting for these roles has also given him a deeper insight into the new IR35 regulations coming into effect within the private sector, which has been invaluable information for the contractors who work with him.
Get in touch with Matthew Moulton if you have a spare 6-16 hours per week and are open to new opportunities around your current role.
How will hiring contingent workers in a GMP-regulated environment impact your organisation today?
The gig economy has gained in popularity today as the workforce continues to embrace th...
Are there more opportunities in South Korea's medical scene following the government's ₩500b investment?
Yonhap News has recently announced that South Korea has pledged to commit ₩500 billion ...
IR35 changes - "doing nothing is not an option"
From April 2020, all UK companies with more than 50 employees and more than £10.2 milli...
Does no industry experience mean zero experience?
With an aging population and one of the world's lowest birth rates, Japan's local talen...


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redpajama_set_name: RedPajamaGithub


Rockville, Md. (January 24, 2019)—Lower-than-normal zinc levels may contribute to high blood pressure (hypertension) by altering the way the kidneys handle sodium. The study is published ahead of print in the American Journal of Physiology—Renal Physiology.
Zinc deficiency is common in people with chronic illnesses such as type 2 diabetes and chronic kidney disease. People with low zinc levels are also at a higher risk for hypertension. The way in which the kidneys either excrete sodium into the urine or reabsorb it into the body—specifically through a pathway called the sodium chloride cotransporter (NCC)—also plays a role in blood pressure control. Less sodium in the urine typically corresponds with higher blood pressure. Recent research has suggested that zinc may help regulate proteins that in turn regulate the NCC, but a direct link between zinc-deficiency-induced hypertension has not been examined.
Researchers compared male mice with zinc deficiency to healthy controls with normal zinc levels. The zinc-deficient mice developed high blood pressure and a corresponding decrease in urinary sodium excretion. The control group did not experience the same changes. A small group of the zinc-deficient mice were fed a zinc-rich diet partway through the study. Once the animals' zinc reached adequate levels, blood pressure began to drop and urinary sodium levels increased. "These significant findings demonstrate that enhanced renal [sodium] reabsorption plays a critical role in [zinc-deficiency]-induced hypertension," the research team wrote.
"Understanding the specific mechanisms by which [zinc deficiency] contributes to [blood pressure] dysregulation may have an important effect on the treatment of hypertension in chronic disease settings," the researchers added.
Read the full article, "Zinc deficiency induces hypertension by promoting renal sodium reabsorption," published ahead of print in the American Journal of Physiology—Renal Physiology.
Released February 9, 2016 - Most clinical studies have shown that renal denervation—a procedure that disrupts the nerves in the kidneys and prevents them from relaying signals—can treat drug-resistant hypertension, although a number have shown the procedure to be ineffective. A new study in American Journal of Physiology—Regulatory, Integrative and Comparative Physiology supports that renal denervation can treat hypertension and suggests that failures may be due to incomplete procedure. This research is highlighted as one of this month's "best of the best" as part of the American Physiological Society's APSselect program.
The Down Side of Your Sweet and Salty Addiction: Rapid Onset High Blood Pressure?
Released April 5, 2016 - High levels of fructose similar to amounts consumed within the American diet may predispose individuals to fast-onset, salt-sensitive hypertension, according to New research presented at the Experimental Biology 2016 meeting in San Diego.
Released August 12, 2017 - Automatic blood pressure devices are often used to assess blood pressure levels at home and in the clinic. But these automatic devices are prone to significant errors, sometimes leading to the prescription of blood pressure-lowering medications to patients who don't actually need them. Researchers at the Jerusalem College of Technology and the Shaare Zedek Medical Center in Israel have developed a method to more accurately measure systolic blood pressure. They will present their findings at the Cardiovascular Aging: New Frontiers and Old Friends conference in Westminster, Colo.


Laboratory Analysts Certification - Georgia Water and Wastewater Institute, Inc.
To obtain a Water Laboratory Analyst Certification or a Wastewater Laboratory Analyst Certification, applicants must take the appropriate course work, obtain the required amount of experience, pass the Georgia state exam, and then apply for their license. To help with this process, we've compiled information on each of these steps.
To obtain a Laboratory Analysts Certification, please follow these five steps.
The type of laboratory analyst certification required is simply determined by the type of laboratory work that the analyst performs. In Georgia, all those performing water analyses on drinking water samples should obtain a Water Laboratory Analyst certification, and all those performing analyses on wastewater samples should obtain a Wastewater Laboratory Analyst certification.
According to GA Board Rulesa 750-3.04, the applicant "must have completed the required course work prior to taking the examination and provide proof of completion of course work when they submit their application for certification to the Board." The course work requirements for each license are listed below, as well as the GWWI course that will satisfy that requirement.
*The required course work can be bypassed if the candidate holds an Associate's Degree or higher in Biology, Environmental Science, Chemistry, or an equivalent degree. For other types of the degrees, the Board may evaluate, on a case by case basis, post-secondary education to determine satisfaction of the course work requirements.


In many ways, the name Alastair Borthwick conjures up many thoughts to those familiar with his works. For some, he is remembered as a broadcaster who introduced radio listeners to mountaineering. To others, his name immediately brings to mind his many literary works, all of which have him regarded as one of the greatest Scottish writers of his generation. But no matter what memories people have of the man who passed away in 2003, it is clear Alastair Borthwick was considered a pioneer in many areas.
Starting his literary career at age 16 by dropping out of high school and taking a copytaker position with the Evening Times, he edited a variety of columns and was responsible for compiling the paper's crossword puzzle. However, it was his introduction to the paper's Open Air page that began his love affair with mountaineering. Discovering he quickly had a passion for the activity, he spent many days traversing the nearby mountains. Ultimately, his experiences were brought to life through a 15-minute radio show, and eventually his famed literary work Always A Little Further, which while published in 1939 has yet to ever be out of print.
Along with his mountaineering adventures, Alastair Borthwick also wrote of his experiences as an infantryman during World World II. Reaching the rank of Captain, he also served as a battalion intelligence officer in such areas of the world as North Africa and Western Europe. In one of his most exciting adventures during the war, he led a group of 600 men on a nighttime mission behind German enemy lines, eventually overtaking a group of enemy soldiers.
Using his experiences during the war, Alastair Borthwick published a second book titled Sans Peur in 1946. Noted for its excellent writing and graphic details of what war was like for an infantryman, the book was given worldwide acclaim and excellent reviews by literary critics.
Considered a Renaissance man by many in today's modern Scotland, Alastair Borthwick will always be remembered for his ability to speak and write about mountaineering, war, and other topics in ways few others could ever imagine.


From IH 10 westward via Anthony to Texas/New Mexico State Line, a distance of approximately 1.9 miles. (El Paso County) Extended eastward approximately 1.2 miles from US 80 to IH 10.
From Texas/New Mexico State Line, eastward to SH 20 in Anthony, and from another point on SH 20 in Anthony, eastward to IH 10, a total distance of approximately 2.2 miles. (El Paso County) Redescribed to include break in route at SH 20 (Formerly US 80).


Alexion Pharmaceuticals, a clinical stage biopharmaceutical company focusing on the development of life-transforming therapies for patients with devastating and rare diseases, recently announced positive results from a phase 3 study of their second generation of Soliris® (ALXN1210), for the treatment of PNH. The press release announcing these results can be read here.
According to the news release, the study showed that PNH patients can be effectively and safely switched from treatment with Soliris® (eculizumab) every two weeks to treatment with ALXN1210 every eight weeks; providing a treatment schedule that would be significantly more convenient for patients. The study held included clinical trial sites in Edmonton and Toronto, Canada.
After reaching out to the company for an update, the Canadian Association of PNH Patients has learned that Alexion Pharmaceuticals has submitted ALXN1210 for regulatory approval in Canada and expects a decision in the second half of 2019.


The Rio has been a fan-favorite among Kia customers for many years, but none of the past models have ever been as well-rounded as the 2018 edition. This next-generation Rio has received numerous upgrades and a full redesign for the 2018 production year. Starting with the foundation, the 2018 Rio has a longer wheelbase, longer body and wider platform than its predecessors. As a result, it also provides passengers with more comfort and space, which make the ride even better than it was previously. Of course, that's just the beginning of what makes the 2018 Rio the best one yet.
An excellent choice for passengers and drivers alike, the 2018 Kia Rio isn't just great for riding in, it's also fun to drive! This enhanced experience begins with its new engine, a 1.6-liter athlete that pumps out 130 horsepower and 119 pound-feet of torque. The peppy engine is sure to get the adrenaline flowing, but the interior of the Rio is where the magic happens. All-new, more modern, and undeniably more comfortable, the inside of the 2018 Kia Rio has more technology, better seats, and a wide variety of improvements across the board. Of course, the best way to experience all of this in person. Want to get behind the wheel of a 2018 Kia Rio? Fill out the included form and schedule a test drive today!


Preacher: John Van Meerbeke (39), Zachary Siggins (7), Stephen Payson (1), John Mallin (1), Kyle Brown (1).
Series: Sola Power (5), (12), Consider Jesus (32).
Galatians 4:4-5 (Part of the series).
Preached by John Van Meerbeke on December 24, 2017 (Living Hope).
Preached by Stephen Payson on December 17, 2017 (Living Hope).
Consider Jesus: 48. "But you have come to Mount Zion"
Hebrews 12:18-24 (Part of the Consider Jesus series).
Preached by John Van Meerbeke on December 10, 2017 (Living Hope).
Consider Jesus: 47. "Obtain the grace of God"
Hebrews 12:12-17 (Part of the Consider Jesus series).
Preached by John Van Meerbeke on December 3, 2017 (Living Hope).
Consider Jesus: 46. "The peaceful fruit of righteousness"
Hebrews 12:7-11 (Part of the Consider Jesus series).
Preached by John Van Meerbeke on November 26, 2017 (Living Hope).
Consider Jesus: 45. ...so that you may not grow weary of fainthearted"
Hebrews 12:3-6 (Part of the Consider Jesus series).
Preached by John Van Meerbeke on November 19, 2017 (Living Hope).
Consider Jesus: 44. "Commended through their Faith"
Hebrews 12:1-2 (Part of the Consider Jesus series).
Preached by John Van Meerbeke on November 12, 2017 (Living Hope).
Malachi 1:1-5 (Part of the series).
Preached by Zachary Siggins on November 5, 2017 (Living Hope).
Isaiah 42:1-9 (Part of the Sola Power series).
Preached by John Van Meerbeke on October 29, 2017 (Living Hope).
2 Timothy 3:10-17 (Part of the Sola Power series).
Preached by John Van Meerbeke on October 22, 2017 (Living Hope).


With the Israeli general elections coming up soon, here's everything you need to know.
1. Why are there so many political parties?
Israeli society is very diverse, and the political parties represent all the different ideological, ethnic, and religious populations. Israel also allows representation in the Knesset to any party which clears the 3.25-percent threshold in the elections.
The advantage of this is that minorities in Israel are adequately represented in the Knesset (the parliament). However, representation comes at a price in terms of political stability, since larger parties must negotiate with a number of smaller parties to form a coalition government, which could cause a conflict of interest down the line.
2. How do you build a coalition?
In Israel, the president appoints a member of the Knesset to try to form a majority coalition (at least 61 out of the 120 mandates). The president usually appoints the leader of the party with the most votes, although it's not mandatory. The leader of the party then joins with other political parties to create a majority government.
3. What are the main parties?
4. How do Israeli politics affect my life?
a. Expense of living, or in Hebrew: יוקר המחייה (yoh-ker hah-meech-yah). Politics play a huge role in the economy, imports and exports, taxes, real estate, et cetera.
b. Breaking up large monopolies to allow small businesses to succeed. Currently the media, telecommunications, dairy products, and other industries are controlled by a few large corporations. This allows them to control prices and market supply, which isn't always in the people's best interest.
c. Role of religion in day-to-day life. There are a number of topics constantly being discussed in Israeli society regarding the role of religion in society. For example, businesses are not allowed to open on שבת (Saturday), and the חרדי (orthodox) population isn't required to complete the obligatory national service.
5. What are the criminal charges against Netanyahu, and how will they affect the elections?
There are three criminal accounts against Bibi for corruption and bribery.
In the first case, known as Case 1000, Netanyahu is charged with receiving bribes. Netanyahu allegedly received gifts from overseas billionaires totaling 1 million shekels, including cigars, champagne, jewelry and more. In exchange for the gifts, investigators say Netanyahu tried to advance a tax break which would have benefited the businessmen.
In Case 2000, Netanyahu allegedly requested more favorable coverage from the media company Yedioth Ahronoth, in exchange for limiting circulation of their top rival Israel HaYom.
In the third case, known as Case 4000, Netanyahu faces charges of receiving bribery of 1 billion shekels from Walla News in exchange for favorable media coverage. While Bibi received the bribes, he was serving as Prime Minister and as the minister of communications.
The elections will take place Tuesday, April 9, 2019.