text:
Monty Hall, Host of 'Let's Make A Deal,' Dies at 96
Monty Hall, who co-created "Let's Make A Deal," which premiered in 1963 and has continued its successful run largely uninterrupted up to present day, has died.
Game show host Monty Hall.AP file
Sept. 30, 2017, 10:55 PM UTC / Updated Sept. 30, 2017, 10:55 PM UTC / Source: Variety
LOS ANGELES — Monty Hall, who co-created and hosted the game show "Let's Make A Deal," died as a result of heart failure Saturday in his home in Beverly Hills, Calif. He was 96.
"Let's Make a Deal" premiered in 1963 and has continued its successful run largely uninterrupted up to present day.
Hall hosted various game shows and other programs in his early career until he developed "Let's Make a Deal" with creative partner Stefan Hatos. The show became legendary for its audience members dressing up in outlandish costumes in order to attract Hall's attention in the hopes of being given the opportunity to win big.
Monty Hall arrives at the 40th Annual Daytime Emmy Awards on June 16, 2013, in Beverly Hills, CaliforniaRichard Shotwell / Invision/AP file
Hall and Hatos produced several other game shows under their production company through the '70s and '80s. Hall continued to host "Let's Make a Deal" for almost all of its 5,000 episodes, as it traversed from NBC, to ABC, and finally nighttime syndication. The show was revived by CBS in 2009 with host Wayne Brady, and continues to air.
The show became so popular in pop culture that it spawned "the Monty Hall Problem," a thought experiment in probability that involves three doors, two goats, and a prize.
Hall received a star on the Hollywood Walk of Fame in 1973, and, as a Canadian native, was named to the Order of Canada in 1988.
Born Monte Halparin, he was raised in an Orthodox Jewish family in Winnipeg, where he started his career in radio.
He is survived by three children: actress Joanna Gleason, who confirmed his death; TV exec Sharon Hall Kessler and TV producer Richard Hall; a brother and five grandchildren. His wife Marilyn died in June.


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Retour sur le discours poétique « The Soul of Corporations » lors de la soirée #IntFem du 29 Mars 2018 chez Deloitte après un panel de femmes inspirantes ! Découvrez le réseau International au Féminin.
"People Planet Purpose Profit "?
And bring souls into corporations in a world of cooperation as a human revolution.
We're all in this life, present, future together in the end.
I have another question for you: Who wants to be N°1?
Each is their uniqueness but united.
Change the world for good not for goods, unless they're common.
We can be part of the solution or be part of the pollution.
In harmony with nature as mankind may have now matured?
The post capitalism era we live in is a shot at humanism.
As a human symphony in the harmony of painting from Kandinsky.
Imagine we all say oui, imagine we can all be.
Imagine we might just win, imagine this can be real.
Imagine the role of your company is magic in its public utility.
Imagine your sense of purpose meets our future goals in this reality.
Imagine we build a peaceful world of harmony to live as one human family.
Where profit meets purpose and sky is the limit and the future is infinite!
Between Net Positive impact and Public Benefit as a global pact to bridge every gap.
On the dancefloor of our interdependence to choose our own zone of influence.
Your Human Potential Empowerment and your soul awareness enlightenment ?
Your contribution to our human evolution as a corporation?
Your common good retribution and share in our worldwide reconciliation?
The difference between cooperation and competition for a wider collaboration?
Your purpose and your horizon, your values and your higher mission ?
"Business + awareness of our souls = success + happiness for us all."?
To open the ways to new lights and new heights.
With one key word of life in a real world of light: "Solidarity" as an inspirational symbol.
And look at the future as one single soul in the dome of our home sweet home.
Actually don't be careful, be wonderful!
That's the balance. Thank you and…. Welcome.


text:
HomeInternet Security NewsOrganizations
ISPs Can Now Sell Your Web Browsing History Says Senate. Goodbye Privacy.
Zohair 0 Published: 25 March 2017 Updated: 30 March 2017
ISPs are now with advertisers. Time for advocacy groups to rise up to guard user privacy.
There was a time when the word ISP stood for Internet Service Provider.
Now it should be changed to something more relevant.
And more truthful.
ArsTechnica seems to have come up with just the right name.
From now on it seems like it wouldn't be far-fetched to call ISPs as Invading Subscriber Privacy companies.
Does the United States Senate even needs to get involved in this?
Perhaps they do.
Maybe they don't.
What we now know for sure is that they don't have a problem with ISPs selling your data.
How do we know that?
You only have to look at the voting that took place on March,23, 2017.
This might go down as an important day for future privacy-conscious generations, who knows.
Namely, the United States Senate voted to get rid of some certain broadband privacy rules and regulations which will impact the end-user in a big way.
Basically, the vote meant that ISPs would no longer be in need of consumer consent (explicit one!) before they move forward and sell (or share) web browsing data with advertisers.
ISPs can also help themselves to access your other private information and then sell those too, to, you know who.
Advertising companies along with every other kind of company that would want to use/buy consumer data.
Readers who have followed news related to privacy and ISPs invading it would know that the actual rules were official agreed upon back in October of 2016.
That was done by the Federal Communications Commission when it was lead by some Democrats.
As we know, not the Federal Communications Commission is under the rule of the Republican party.
And the Republican majority along with Republican in Congress have opposed the new rules as you probably would have figured out because of the Senate vote.
Needless to say, the Senate exercised its power given to it under the Congressional Review Act.
And essentially ensured that the Federal Communications Commission power of rulemaking would have no force or effect.
If it wasn't obvious enough already, the Senate vote will also, more or less, assure that the Federal Communications Commission is blocked from issuing similar regulations in the future as well.
To protect yourself against spying from government agencies as well as ISPs, you need the help of a VPN service.
A VPN service will encrypt your internet traffic and hence will protect your privacy and anonymity from all entities.
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Maybe Everything Isn't As Bad As It Seems.
Your internet service provider wants more from you than just monthly payments.
Of course one can't ignore the fact that The House (currently controlled by the Republicans) will also need to vote in favor of or against the new measures.
Only after that, the existing rules may or may not be eliminated on an official basis.
And then there is Donald Trump.
President Donald Trump can also move in, issue a veto and as a result preserve the existing privacy rules.
But will he do that?
Should we expect Donald Trump to safeguard the interests of consumers?
There should be no doubt about the fact that the trio of The House, Senate, and President Trump make a powerful foe/friend.
If President Trump and the House support the Senate's vote, then internet service providers will be free.
Free from seeking any kind of approval from customers before they share their web browsing record.
Add to that web browsing history and other types of private information as well.
With whom you ask?
You already know.
The hundreds and thousands of marketing agencies around the world.
Let's not forget advertising ones either.
What Was The Vote Count?
The Senate vote was, on official count, 50-48.
That should tell us that there was at least some form of resistance from members of the Senate against abolishing existing privacy rules.
Needless to say, the lawmakers in the country stayed true to their parties and voted unanimously along party lines.
Senator Ed Markey, a Democrat from Massachusetts, said after the Senate vote that president Trump might be outraged by the fake violations of his own privacy, but every American citizen should be alarmed by the very real violation of their privacy which will probably result from the Republican lead roll-back of existing broadband internet privacy protections.
This latest Senate measure against consumer internet privacy was introduced by Senator Jeff Flake, a Republican from Arizona, about two weeks ago.
Along with that, there were 23 other Republicans who co-sponsored the Senate measure.
So what did Flake want from all of this?
Apparently, he was trying to protect the consumers.
After the introduction of the new measure, he said that he was just trying to protect consumers from overreaching Internet regulation.
Let's not talk about how there should be from no to very little internet regulation.
Let's talk about Ajit Pai who is the current Chairman of Federal Communications Commission.
He recently argued that consumers and end-users will definitely get confused about privacy rules.
Mainly that there is another set of privacy rules for internet service providers and another set for technology behemoths like Facebook and Google.
Pai told lawmakers from the Democratic party that American consumers should not have to be lawyers or engineers.
And that they could not be expected to figure out if their information is protected or not.
More Democrats And Republicans Voice Their Opinion On The Senate Vote
Senator John Cornyn, a Republican from Texas, argued a couple of days ago that the existing privacy rules hurt job creators and stifled economic growth.
He also said that the Federal Communications Commission privacy rulemaking methodology was flawed.
Because it involved the government picking winners and losers.
He went a bit further and said that FCC's rulemaking was among the many harmful rules and regulations put forward by the Obama administration at the last moment.
Who Are The ISPs And What Do They Want?
Internet service providers want to invade your privacy.
A little while ago the answer to this question was pretty obvious to anyone not living under a rock.
ISPs were simply internet service providers.
They connect people to the vast world of the internet.
Many Democrats along with consumers advocates believe that this is starting to change.
And understandably, are furious about it.
During the floor debate a couple of days ago Markey said that the acronym ISP now stood for something else.
Something else like information sold for profit.
He also had another suggested acronym.
That ISPs stood for "invading subscriber privacy".
In other words, there is no room for Internet Service Provider as an acronym for ISPs.
But apart from that, Markey also raised a couple of valid points.
He said that the Senate vote was detrimental to progress.
Because the new Senate action would effectively allow broadband providers like,
to arrest any semblance of control away from the end user i.e the consumer.
After that these same broadband providers will relentlessly collect data on their users.
What Do ISPs Do With Your Collected Data
The final step is, of course, so sell that data to advertising companies.
So what kind of sensitive data/information are we talking about here?
Nothing serious.
Just private information like health records along with financial ones.
Markey also said that the type of information these ISPs would collect will also include information about children.
In a wider perspective, the ISPs want to draw a map of their users.
They want to know where users along with their families shop.
Of course, information about where the children go to school is also pretty valuable.
The ISPs will then sell this information to data brokers Markey said.
Markey ended his comment by saying that ISPs will not only sell user data to advertising companies.
No, they won't.
In fact, they are likely to sell user data to anyone who wants to make a profit off user data.
More Senator's Remarks
Will Donald Trump stop advertisers from exploiting user data?
Senator Bill Nelson, a Democrat from Florida, said that the potential consequences of the Senate vote could be significant.
He said that home broadband providers could easily know when a user woke up each day.
All an internet service provider had to do was to know the time each morning a user logged on to the internet to check the weather or something else like news in the morning.
ISPs could also track users through any other connected device in the user's home.
While debating during the Senate floor a couple of days ago, he also said that a provider might know immediately if the user was not feeling well assuming the user decided to peruse the internet like most of the people do today to get a quick check on their symptoms.
He further said that broadband internet provider could potentially know more about a user's health along with any reactions to an illness than the user might be willing to share with his/her doctor.
With so much information just sitting there waiting to be collected, ISPs can know a lot more about each of their users.
Senator Bill Nelson continued that pointed out that home broadband providers could also build a user profile about a user's listening and online viewing habits.
To top that up with more traction, mobile broadband providers could know how the user moved about during his/her day through information about the user's geolocation and internet activity through the user's mobile device.
All of this means that there is a ton of data that internet service providers want to get a hold of.
And then profit from.
What Do Consumers Want?
As you can probably imagine, consumers would not want their ISPs to sell their personal data to advertisers.
Not matter how philanthropic the intentions behind "selling data" may be.
Nelson further added that ISPs could potentially have landed on a gold mine of data which could be compared to the holy grail to speak.
He said that it was no wonder that internet broadband service providers wanted permission to sell user information.
Not only that, it seems that ISPs want to sell that information to the highest bidder without consumers knowledge.
Let's not even talk about consumer consent.
Furthermore, these internet service providers also want to collect and use information on their customers without providing any sort of transparency or accountability.
Who Will Hold Internet Service Providers Accountable?
The fact is, most of the consumers in the United States of America don't have a lot of choices when it comes to internet service providers.
At least that is what Senator Ron Wyden, a Democrat from Oregon, thinks.
He told reporters that consumers might be in a bit of a bother in the coming months and years.
Because consumers might be left without any choice.
He said that users would either give up their web browsing history for an internet provider to sell to the highest bidder or have no connection to the internet at all.
Of course, most of the consumers would go with the former.
Moreover, Wyden said that the Federal Communications Commission rules did not stop internet service providers from making a lot of money from customer data.
The current rules simply state that internet service providers simply have to inform the user/consumer about how their user data is utilized.
After that, they only have to get the customer's consent and then sell the most sensitive kind of data to someone who offers them money.
Advocacy Groups Could Play An Important Role
Perhaps the only positive aspect about this whole Senate vote thing is advocacy group activity.
About four days ago, advocacy groups such as,
Demand Progress
managed to get 90,000 petitions and then delivered them to the Congress.
The petitions were mainly about saving user broadband privacy.
The Only Problem Advocacy Groups Have Is That They Aren't Fighting Senate Alone
Internet service providers are just one of the players who are trying to force senators to get rid of privacy rules.
Let's not forget advertising lobby groups as well.
They also want senators to kill any rule that may protect user privacy and data.
One of such groups goes by the name of NCTA- The Internet and Television Association.
It recently came out with a statement and said that the association appreciated the Senate vote that was held a couple of days ago.
The statement further read that Senate's action to repeal unwarranted Federal Communication Commission rules which basically denied consumers regular privacy protection while they were online.
The cable lobby group also said that current FCC rules violated competitive neutrality.
Finishing up the statement, the group, pointed out that the cable industry remained committed to offering high-quality services that protected the privacy and online security of the personal information of their customers.
How Do ISPs Sell Your Data And How To Stop Them
The Only B.VPN Review You Want To Read Right Now

redpajama_set_name: RedPajamaCommonCrawl


text:
University of Texas at Austin Social Work Professor Chosen to Lead Juvenile Justice Task Force
Dr. David Springer, professor of social work at The University of Texas at Austin, has been asked by the Texas Youth Commission (TYC) to chair a blue ribbon task force charged with defining a new juvenile correctional rehabilitation system.
AUSTIN, Texas—Dr. David Springer, professor of social work at The University of Texas at Austin, has been asked by the Texas Youth Commission (TYC) to chair a blue ribbon task force charged with defining a new juvenile correctional rehabilitation system.
The "Transforming Juvenile Justice in Texas: A Framework for Action" task force, which includes juvenile justice experts from around the country, will meet May 21-22 on the university campus.
"In his role as chairman, Dr. Springer has worked to identify key panelists, is assisting us in inviting other state and national practitioners to make presentations to the panel and ultimately will provide us with a document that will identify the goals, objectives and possible activities to be implemented," said Ed Owens, acting executive director of the TYC.
The scope of the task force's charge has been expanded to include recommendations about reforming the entire juvenile justice system in Texas.
"It is impossible to discuss TYC facilities as if they exist in silos," said Springer. "While what happened at TYC is extremely unfortunate and tragic, it also presents a unique opportunity for the state of Texas."
The TYC was created to care for, treat and educate the state's most serious and chronic juvenile offenders. In March, the Texas governor placed the TYC under conservatorship to guide reform of the agency's correctional and rehabilitative systems following reports of sexual abuse of youth.
The task force will look at two questions: If it could re-design health care, treatment and case management at TYC correctional facilities, what would it look like? If it could re-design the juvenile justice system in Texas, what would it look like?
Springer, associate dean for academic affairs in the School of Social Work and a University Distinguished Teaching Professor, specializes in adolescent health, juvenile justice and substance abuse, and mental health treatment for juvenile delinquents.
A list of task force members can be found online.
For more information contact: Nancy Neff, The University of Texas at Austin Office of Public Affairs, 512-471-6504; David Springer, School of Social Work, 512-471-0512.


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text:
\section{Introduction}
\label{intro}
So far, more than 4000 planets (with more than 3000 transiting their stars) have been detected showing an incredible diversity in terms of masses, sizes and orbits. Moreover, thousands of Jupiter-size down to Earth-size planets are expected to be discovered in the next few years by Gaia \cite{Sozzetti2010,Perryman2014}, TESS \cite{Ricker2014}, CHEOPS \cite{Broeg2013} and the upcoming space surveys, such as  PLATO \cite{Rauer2016}, along with ground-based surveys, like WASP \cite{Pollacco2006}, NGTS \cite{Wheatley2013}, TRAPPIST \cite{Jehin2013}, HARPS \cite{Mayor2003} and ESPRESSO \cite{Pepe2010}, CARMENES\cite{Quirrenbach2016} and SPIRoU\cite{Artigau2016}.
The recent success of ground-based, space transit and radial velocity searches has ushered exoplanet research into an era of \emph{characterisation} studies
with the goal to investigate the nature, formation, and evolutionary history of the detected objects.\\
At first, these studies have been focused on understanding the internal structure of exoplanets. From the transit light-curve, the planet radius can be measured and from spectroscopic Doppler measurements, the planet mass is obtained. From the bulk density we have the first hints of the internal structure of the exoplanet and the gas/ice/rock ratios.
However, to have a reliable estimate of the density, an accurate knowledge of both radius (with a precision of up to 5$\%$) and planetary mass (up to 10$\%$) is necessary \cite{Wagner2011,Bean2011}.
Additionally, the absolute value of planetary radius and mass relies on the precise determination of the radius and mass of the exoplanet-host star. The derivation of these last two values is in turn strongly connected to the effective temperature ($T_{\rm eff}$), surface gravity ($\log g$), and the metallicity of the star. Thus, the planetary properties are critically dependent on their stellar host properties \cite{Torres2012,Sousa2015,Adibekyan2018}.

Furthermore, transiting planets provide us one of the best ways of characterising their atmospheres.
In-transit spectroscopy as well as secondary transit studies \cite{Brogi2012,Stevenson2014,Sing2016,Fu2017,Tsiaras2018,Zhang2018,Pinhas2019}
using space observatories, as Hubble and Spitzer, and some ground-based observatories,
have yielded the detection of some important molecules present in the planetary atmospheres for a limited number of targets,
or have identified the presence of clouds, probing the thermal structure and providing some constraints on the planet properties. However, the data available is still too sparse to provide a consistent interpretation and the achieved results point out the main limitations of the existing facilities:
very narrow wavelength coverage, observations usually not simultaneous for a wider spectral range with the introduction of systematic noise, insufficient time allocated to exoplanet science, and more in general
the lack of a dedicated space-based exoplanet spectroscopy mission.
Thus, our current knowledge of exoplanetary atmospheric and thermal characteristics is still very limited.

Ariel (\emph{Atmospheric Remote-sensing Infrared Exoplanet Large-survey}) has been selected as the next ESA-M4 science mission \cite{Tinetti2018} and it is expected to be launched in 2028.
During its 4-year mission, Ariel will observe the atmospheres of a statistically representative sample ($\sim$1000) of transiting gaseous (Jupiters, Saturns, Neptunes) and rocky (super-Earths and sub-Neptunes) planets
using transit spectroscopy in the 1.10-7.8$\mu$m spectral range and three narrow-bands photometry in the optical.
The wavelength range proposed covers all the expected major atmospheric gases from H$_{2}$O, CO$_{2}$, CH$_{4}$, NH$_{3}$, HCN, H$_{2}$S up to the more exotic metallic compounds, such as TiO, VO, and condensed species.\\
Ariel is designed as a dedicated survey mission for transit, eclipse and phase-curved spectroscopy,
 providing a homogeneous dataset, with a consistent pipeline and an well-defined target selection strategy, maximising the scientific yield.
 Focusing on transit, eclipse spectroscopy, the methods are based on the differential analysis of the star and planet spectra
 in and out of transit, allowing to measure planetary atmospheric signals of 10-100 ppm relative to the star.
Such small signals require an exact knowledge of the host star spectrum, at least at the same level of the planetary signal, to map any stellar intrinsic variation (i.e. due to magnetic activity and convective turbulence) in order to avoid misleading results with planetary features \cite{Robertson2015}.

Another important point is that information on the host star composition is critical to separate the signatures left on the planet by its formation, evolution and migration processes, from those due to the specific chemistry of the host star \cite{Turrini2018}.
Indeed, recent studies suggest that planetary O/H, C/H, C/O ratios and metallicity with respect to the stellar values
could provide stronger constraints on the planet formation region and their migration mechanisms
(see \cite{Madhusudhan2016} and references therein for a recent review),
but similar considerations apply to other elements (e.g., N, S, Ti, Al, \cite{Turrini2018}).

Finally, an increasing number of studies have pointed towards the existence of correlations between
the properties of the host stars and the characteristics and frequency of their planetary systems.
In this respect, the correlation between the stellar metallicity and the frequency of giant planets \cite{Santos2004,Valenti2005,Sousa2008},
the connection between radius vs metallicity \cite{Buchhave2014,Schlaufman2015},  eccentricity vs metallicity \cite{Adibekyan2013,Wilson2018},
the role of the abundances of other elements \cite{Adibekyan2012,Delgado2014,Delgado2017} in the host stars are only few examples of different results that take a clear shape as the new planet discoveries increase, shading light on many details still missing concerning planet formation and evolution.\\
Such works rely upon homogeneously and precisely derived stellar parameters.
Therefore, homogeneous derivation of stellar parameters using high-quality data is crucial for characterising
exoplanet-host stars \cite{Santos2013,Andreasen2017,Sousa2018}, and in turn, is fundamental to improve the accuracy of the planet properties.\\
It is important to underline how a well-defined target selection strategy and the definition of the input target list with a statistically significant dataset in the range of relevant stellar/planet parameters have a fundamental role for maximising the scientific yield and the achievement of scientific goals of Ariel. A meaningful choice of the targets requires an accurate study of the stellar properties that need to be derived in advance and continuously updated as the mission approaches launch and the target list evolves with the new exoplanet discoveries.\\
In this context, we have started a benchmarking analysis between three different spectroscopic techniques used
to determine stellar parameters for selected targets belonging to the Ariel Reference Sample \cite{Edwards2019}.
Our goal is to consolidate a method that will be applied to homogeneously determine the stellar parameters for the complete Ariel Reference Sample.
More generally, we refer also to the works of \cite{Lebzelter2012} and \cite{Smiljanic2014} where comparisons between the results from different spectroscopic techniques are discussed.

For a global approach to characterize the stars of Ariel Reference Sample see also \cite{Danielski2020}, where an overview on the methods used to determine stellar fundamental parameters, elemental abundances, activity indices, and stellar ages for the Ariel Reference Sample is given and in particular, results for the homogeneous estimation of elemental abundances of Al, Mg, Si, C, N, and the activity indices  S  and log(R' HK) are presented.

In the following sections we describe the star sample analysed, we give an overview of the methodology applied to derive the stellar parameters and then we present a comparative analysis of the results.

\section{Star Sample}
\label{sec:2}
On the bases of Ariel capabilities, a list of targets (Ariel Reference Sample) to be observed during the primary mission life
was prepared for the Phase A \cite{Zingales2018,Edwards2019}. The sample includes $\sim$1000 potential targets with stellar types FGKM (typically brighter than K\,=\,11 mag) and planetary parameters in a range of size between Jupiter down to Earth-like planets, temperature in the range between 500K-2500K and bulk density between 0.10-10.0g/cm$^{3}$.

We started our analysis cross-matching the Ariel Reference Sample with the stars available in the SWEET-Cat
(Stars With ExoplanETs Catalogue \footnote{\url{https://www.astro.up.pt/resources/sweet-cat/}})
 and we selected all the common targets with parameters source "flag=1", which
are the stars analysed homogeneously (see \cite{Santos2013}).
\begin{figure}
  \includegraphics[width=0.50\textwidth]{./Figure1.eps}
  \includegraphics[width=0.50\textwidth]{./Figure2.eps}

\caption{Top panel: Distribution of the star sample analyzed as a function of V mag listed in the SWEET-Cat catalog. Bottom panel: V mag vs S/N for our star sample.}
\label{fig:1}
\end{figure}
Thus, our starting sub-sample includes 155 FGK stars in a range of 5$<$V(mag)$<$16
with relative spectra having a signal-to-noise ratio (S/N) between $\sim$50 and $\sim$800 (see Fig.~\ref{fig:1}).
Stellar parameters for these 155 stars available in the SWEET-Cat, were considered our baseline for the comparison analysis.
An accurate description of the spectroscopic data used to derive SWEET-Cat stellar parameters is presented in \cite{Sousa2018} and \cite{Santos2013}.

We then re-determined the stellar parameters of this sub-sample using two
different methods: FAMA (\emph{Fast Automatic MOOG Analysis}, \cite{Magrini2013}), based on the equivalent widths analysis
and FASMA (\emph{Fast Analysis of Spectra Made Automatically}, \cite{Tsantaki2018}), based on the spectral synthesis method.
For our work, we used the same archival spectra employed for the SWEET-Cat analysis.
The characteristics of each spectrograph and the number of stars considered in our analysis for each instrument are listed in Table~\ref{tab:1}.
\begin{table}
\caption{Spectrograph information: resolving power, spectral ranges and number of stars considered.}
\label{tab:1}
\begin{tabular}{llll}
\hline
\hline
Instrument & Resolving Power  & Spectral Range  & N \\
		 & ($\lambda / \Delta \lambda$) & ($\AA$)	&of Stars \\
\hline
ESPADONS & 80000 & 3700-10500 & 2 \\
FEROS & 48000 & 3600-9200 & 38 \\
FIES & 67000 & 3700-7300 & 7 \\
HARPS & 100000 & 3800-7000 & 39 \\
HARPSN & 115000 & 3830-6900 & 4 \\
NARVAL & 80000 & 3700-10500 & 2 \\
SARG & 57000-86000 & 5100-10100 & 5 \\
SOPHIE & 75000 & 3820-6920 & 15 \\
UVES & 110000 & 3000-6800 & 43 \\
\hline
\hline
\end{tabular}
\end{table}
Excluding stars for which FAMA and FASMA codes did not converge (spectra dominated by fringing, very low S/N, fast rotator targets, very cool stars), we obtained results for about 93\% of the sample.\\
Individual stellar parameters derived by FAMA and FASMA for each analysed star are provided as online material in the format listed in Table~\ref{tab:Summary}.

\section{Derivation of Stellar Parameters}

\subsection{SWEET-Cat}
\label{sec:2.1}
SWEET-Cat is a catalog of stellar parameters taken
in general from the literature for planet hosting stars listed within the Extrasolar Planets Encyclopaedia \footnote{\url{http://exoplanets.eu/}}.
This catalogue is continuously updated when new planets are announced and new stellar parameters derived.
In particular, for stars with spectra acquired with high resolution spectrographs (mainly HARPS, UVES, FEROS) and high signal-to-noise ratios (mostly S/N$>$100), the stellar parameters are obtained in a homogeneous way (flagging the targets with 1, as mentioned above). The method used to derive stellar parameters is described in, e.g., \cite{Santos2004} and \cite{Sousa2008}.
Briefly, local thermodynamic equilibrium (LTE) condition is assumed, a grid of Kurucz plane-parallel model
atmospheres (\cite{Kurucz1993}, ATLAS9), and the ARES code \cite{Sousa2007} for measuring line equivalent widths (EWs) are considered. Stellar parameters (effective temperature T$_{\rm eff}$, surface gravity log~g, microturbulence velocity V$_{\rm micro}$, and iron abundance [Fe/H]) are derived using the MOOG code (version 2002; \cite{Sneden1973}) and the line list by \cite{Sousa2008}. Excitation and ionization equilibria of the Fe I and Fe II weak lines were imposed to derive stellar parameters. The errors on the atmospheric parameters were derived as in \cite{Santos2004} and references therein.

The stellar masses listed in the SWEET-Cat catalog were derived with the  calibration  presented  in \cite{Torres2010}, using as input the spectroscopic parameters. According to \cite{Santos2013}, a correction was applied for the cases in which the calibration gives values between 0.7 and 1.3$M_\odot$.The errors for these mass values are computed as in  \cite{Santos2013} by means of a Monte Carlo analysis. For each case 10 000 random values of effective temperature, surface gravity, and stellar metallicity were drawn from a Gaussian distribution. From the resulting mass distribution, the central value for the mass and 1-sigma uncertainty were derived.
\begin{table*}[h]
\caption{Targets. Spectra source. Stellar Parameters (T$_{\rm eff}$, log~g and [Fe/H]) and errors obtained by FAMA and FASMA for each star of the analysed sample.}
\begin{center}

\begin{tabular}{ll|llllll|llllll}
\hline
\hline
  &  &  &  &  & FAMA &  &  &  &  &  & FASMA &\\
\hline
Star  & Spectra & T$_{\rm eff}$ & eT$_{\rm eff}$ & log~g & elog~g & [Fe/H] &
e[Fe/H]& T$_{\rm eff}$ & eT$_{\rm eff}$ & log~g & elog~g & [Fe/H] & e[Fe/H]\\
            &     & (K) & (K) & (dex) & (dex) & (dex) & (dex) & (K) & (K) & (dex) & (dex) & (dex) & (dex)\\

\hline
55Cnc & UVES & 5358 & 150 & 4.44 & 0.20 & 0.49 & 0.01 & 5295 & 20 & 4.455 & 0.03 & 0.359 & 0.01\\
CoRoT-10 & HARPS & 4908 & 150& 4.31 & 0.20 &0.26 & 0.01& 4972 & 10& 4.439 & 0.03& 0.262& 0.01\\
CoRoT-19 & HARPS & 6331& 150 & 4.07 & 0.20 & 0.15
&0.06 & 6313 & 40& 4.283  & 0.06 & 0.148 & 0.02 \\
\hline
\hline
\end{tabular}

\label{tab:Summary}
\end{center}
\end{table*}
\subsection{FAMA analysis}
\label{sec:2.2}
The aim of FAMA is to allow the computation of the atmospheric parameters and
abundances of a large number of stars using measurements of equivalent widths
(EWs) as automatic and as independent of any subjective approach as possible.
It is based on the simultaneous search for three equilibria: excitation
equilibrium, ionization balance, and the relationship between $\log n$(FeI) and EW/$\lambda$. FAMA also evaluates the statistical errors on individual element
abundances and errors due to the uncertainties in the stellar parameters. The
convergence criteria are not fixed a priori but are based on the quality of the
spectra. The code is described in \cite{Magrini2013}.
For our work, first, we have measured the EWs with DOOp (\emph{DAOSPEC Option Optimiser}, \cite{Cantat-Guadin2014}) an automatic tool developed within the Gaia-ESO survey. The code is based on DAOSPEC code \cite{Stetson2008} and uses Gaussian fit to measure EWs.
We adopted the line list of the Gaia-ESO survey \cite{Heiter2015}, which includes atomic parameters (log~g and damping coefficient) for
a large number of lines in the spectral range 4200-6800 \AA.
We adopted the MARCS model atmospheres (plane parallel and spherical) \cite{Gustafsson2008}.

\subsection{FASMA analysis}
\label{sec:2.3}
The analysis with FASMA is based on the spectral synthesis technique wrapped around the radiative transfer code, MOOG (version 2019; \cite{Sneden1973}).\\
FASMA creates synthetic spectra on-the-fly and delivers the best-fit parameters (effective temperature, surface gravity, iron abundance, and projected rotational velocity) after a non-linear least-squares fit (Levenberg-Marquardt algorithm). The line list is mainly comprised of iron lines initially obtained from VALD3 \cite{Ryabchikova2015}. The regions of the spectral synthesis are defined within small intervals around these iron lines ($\pm$2\AA). The atomic data are calibrated to match the spectra of the Sun and Arcturus but given the strongest constrains on the solar parameters, we gave higher weights to the Sun. The damping parameters are based on the ABO theory \cite{Barklem2000} when available, or in any other case, we use the Blackwell approximation. The model atmospheres are interpolated from the ATLAS grid \cite{Kurucz1993} in LTE. The minimization is a two step procedure where initially we obtain the best-fit values using fixed solar macro- and microturbulence. Then, we refine our results in a second step, with updated macro- and micro-turbulence based on empirical relations. Macroturbulence velocity is set by the calibration of \cite{Doyle2014} and microturbulence is set based on calibrations for either dwarfs \cite{Tsantaki2013} or giants \cite{Adibekyan2015}. The uncertainties are derived from the covariance matrix constructed by the nonlinear least-squares fit. The methodology is described in detail in \cite{Tsantaki2018,Tsantaki2020} where it is tested for both giant and dwarf samples, including stars with larger rotation.
\section{Comparison among the methods}
\label{sec:3}
\begin{figure*}
\includegraphics[width=0.5\textwidth]{./Figure3.eps}
 \includegraphics[width=0.5\textwidth]{./Figure4.eps}
 \includegraphics[width=0.5\textwidth]{./Figure5.eps}
 \includegraphics[width=0.5\textwidth]{./Figure6.eps}
 \includegraphics[width=0.5\textwidth]{./Figure7.eps}
 \includegraphics[width=0.5\textwidth]{./Figure8.eps}
\caption{Top panels: Difference between T$_{\rm eff}$ from SWEET-Cat and T$_{\rm eff}$ from FAMA (left)/FASMA (right) as a function of the T$_{\rm eff}$ SWEET-Cat. The colour scale indicates the value of log~g for SWEET-Cat. Red dashed line: average of the T$_{\rm eff}$ difference and 1$\sigma$ level.
Central panels: Difference between log~g from Sweet-Cat and log~g from FAMA (left)/FASMA (right) as a function of log~g from SWEET-Cat.The colour scale indicates the value of T$_{\rm eff}$ for SWEET-Cat.
Bottom panels: Difference between [Fe/H] derived using SWEET-Cat and FAMA (left)/FASMA (right)  as a function of [Fe/H] from SWEET-Cat. The colour scale represents T$_{\rm eff}$ from SWEET-Cat. Average errors are also indicated on the left of each plot.}
\label{fig:2}
\end{figure*}
We compare our results seeking possible outliers and trends among the parameters obtained by the three methods.
In this preliminary work, we explore the results of the three analysis, comparing with external benchmarks, as the surface gravities derived from light-curves in literature and from {\it Gaia} parallaxes and photometry, to identify the ranges of best performances.

\subsection{SWEET-Cat vs FAMA/FASMA: T$_{\rm eff}$}
Fig.~\ref{fig:2} (top panels) shows the difference in effective temperature (T$_{\rm eff}$) between SWEET-Cat and FAMA (left panel) or SWEET-Cat and FASMA (right panel) as a function of the SWEET-Cat T$_{\rm eff}$. The color scale represents log g for SWEET-Cat.

The bulk of the T$_{\rm eff}$ results for the SWEET-Cat and FAMA is in good agreement (within 1-$\sigma$), although there are some outliers: 28 stars show a difference in T$_{\rm eff}$ over 1$\sigma$ level but still within $\sim$417K (3$\sigma$ level). Among these outliers, we noticed that 7 stars present large vsini ($>$10km/s).
The T$_{\rm eff}$ spread seems more evident when considering stars with the lower and higher T$_{\rm eff}$ in the considered range. In addition, there is an offset between the
two methods, with the mean value (red dashed central line) for the difference of $\sim$70 K.\\
Focusing now on the FASMA analysis, also in this case, the bulk of the T$_{\rm eff}$ results for the SWEET-Cat and FASMA is in good agreement (within 1$\sigma$), although outliers are also present. For stars with the lower and higher T$_{\rm eff}$ in the range of interest, the dispersion between the two methods increases.
An offset between the two methods is present with a mean value (red dashed line) in the difference of $\sim$34K.
We note here that some of the outliers are not in common with the outliers found using the FAMA method.
\subsection{SWEET-Cat vs FAMA/FASMA: log g}
Fig.~\ref{fig:2} (central panels)  show respectively the comparison of log g derived using the FAMA (left panel) or FASMA (right panel) methods vs the results given in SWEET-Cat.
The colour scale represents T$_{\rm eff}$ for SWEET-Cat.
There are trends in both the FAMA and FASMA results: the differences between their log~g
and those of SWEET-cat are increasing with log~g. The differences are particularly
high for higher surface gravity (log~g $> $4.6\,dex). In the log~g range of $\sim4-4.6$\,dex, the trend is almost negligible.
In addition, FAMA, on average, gives lower gravities, of about $\sim-0.18$\,dex.\\
\subsection{SWEET-Cat vs FAMA/FASMA: [Fe/H]}
Fig.~\ref{fig:2} (bottom panels)  show respectively the comparison of [Fe/H] derived using the FAMA (left panels) method and FASMA (right panels) vs the results given in SWEET-Cat. The colour scale represents T$_{\rm eff}$ for SWEET-Cat.

Considering the typical errors on metallicity ($\sim$0.10 dex), the results are quite
satisfactory: there are almost no trend in the differences vs [Fe/H] and the
means are close to zero (slightly negative for FAMA).

This is one of the most important results of the analysis and we need to remark it.
Despite the differences in the derived stellar parameters, the three methods converge to very similar final metallicities [Fe/H].
\begin{figure*}[h]
\includegraphics[width=0.5\textwidth]{./Figure9.eps}
\includegraphics[width=0.5\textwidth]{./Figure10.eps}
\caption{Left panel: SWEET-Cat vs FAMA differences in log~g vs differences in [Fe/H], colour-coded by differences in T$_{\rm eff}$. Right panel: the same plot for the FASMA results. An offset of +0.05~dex is applied to FAMA metallicities, while an offset of -0.05~dex to the FASMA ones.   }
\label{fig:3}
\end{figure*}
The three methods rely, indeed, on different line lists, with different set of atomic data, which make them to converge on slightly different sets of T$_{\rm eff}$ and log~g values, which should satisfy the conditions of excitation equilibrium and ionization balance.  T$_{\rm eff}$ and log~g tend to vary along a local minimum, in which the value of [Fe/H] is usually more constant.

In Fig.~\ref{fig:3}, we show the differences in metallicity of the FAMA and FASMA results with respect to SWEET-Cat, as a function of the differences in the derived surface gravities. The symbol are colour-codes by the differences in the derived T$_{\rm eff}$, again, with respect to the SWEET-Cat ones.

Removing the systematic offsets (+0.05~dex from FAMA and -0.05~dex for FASMA with respect to the SWEET-Cat scale), the differences in [Fe/H] are negligible for variation in the surface gravity within $\pm$0.3~dex with respect to the SWEET-Cat ones. In the comparison between FAMA and SWEET-cat [Fe/H] even for differences in log~g$\sim$ -0.3~dex, the agreement in metallicity between the two methods is still good.
Larger differences in log~g$>$+0.3~dex, corresponds to higher [Fe/H] in SWEET-Cat than the ones obtained with the other methods.
This means that moving to higher effective temperatures the discrepancies between the methods increases also for the results in [Fe/H] and
the hottest temperature regime remains thus critical also to obtain reliable metallicities.\\
Concluding, the stars in the parameter space closer to the solar values
(T$_{\rm eff}$=$5000-6000$K, log~g=$4.2-4.6$ dex) are those for which the three methods are in better agreement.
Among the three parameters, the best accord is reached for [Fe/H] in the whole parameter space. The most critical parameter is, however, the surface gravity: external comparison (using {\it Gaia} data, asteroseismic data, isochrones) are needed to evaluate the results of the different methods.
A correct evaluation of all stellar parameters is indeed fundamental for a precise characterisation of the host star, including the determination of its age \cite{Bossini2020}.

\begin{figure*}
 \includegraphics[width=0.5\textwidth]{./Figure11.eps}
 \includegraphics[width=0.5\textwidth]{./Figure12.eps}
 \includegraphics[width=0.5\textwidth]{./Figure13.eps}
 \includegraphics[width=0.5\textwidth]{./Figure14.eps}

\caption{Left panels: Comparison between spectroscopic (Sweet-cat, FAMA and FASMA) and trigonometric log~g as a function of T$_{\rm eff}$ (top) and of trigonometric log~g (bottom). The corresponding T$_{\rm eff}$ for the trigonometric log~g, is derived from the {\it Gaia} measurements. Right panels: Comparison between spectroscopic (Sweet-cat, FAMA and FASMA) and log~g derived from the light-curves as a function of T$_{\rm eff}$ (top) and of light-curve log~g (bottom). Average errors are also indicate on a side of each plot. For the parameter differences we considered as error the larger value among the average errors from each method.}
\label{fig:4}
\end{figure*}

\section{Evaluation of the accuracy and precision of the stellar parameters}
\label{sec:4}
In this section, we discuss some indirect checks on the accuracy and precision of the stellar parameters.
We especially focus on the control of the stellar surface gravity, parameter that cannot be usually constrained well by spectroscopic methods (e.g. \cite{Mortier2013,Tsantaki2014}).  This fact has an impact on the calculation of other stellar parameters (T$_{\rm eff}$ and [Fe/H]) and subsequently on the derivation of the stellar chemical abundances.

\subsection{Comparison with surface gravity derived from trigonometric distances using {\it Gaia} {\sc dr2}}
\label{sec:4.1}
We compare the log~g derived using the three spectroscopic methods with the
trigonometric log~g based on {\it Gaia} {\sc dr2} photometry and parallax.
Photometric gravities have been obtained using the following equation
\begin{equation}
\log(g) = log(M/M_{\odot})+0.4\cdot M_{bol}+4\cdot \log(T_{\rm eff})-12.505
\end{equation}
where $M/M_{\odot}$ is the stellar mass (in solar mass units) provided by the Sweet-cat database. $M_{\rm bol}$ is the bolometric magnitude, obtained from the luminosity published in the {\it Gaia} {\sc dr2} catalog \cite{Gaia2018}
using the following relation M$_{\rm bol}$=4.75-2.5$\times\log$(L/L$_{\odot}$), and  T$_{\rm eff}$ is the {\it Gaia} photometric T$_{\rm eff}$.
Since the stars in our sample are nearby and thus the reddening is negligible, we can derive $M_{bol}$ from the {\it Gaia} luminosities and the distances obtained directly by inverting the parallaxes.
In Fig.~\ref{fig:4} (left top and bottom panels) we show the comparison (no outliers are removed in the plot).
Surface gravities from the SWEET-Cat appear to be slightly underestimated at low T$_{\rm eff}$, and highly overestimated at high T$_{\rm eff}$. The
same behaviour for FASMA at high T$_{\rm eff}$. No clear trend appears for the FAMA surfaces gravities vs T$_{\rm eff}$.
\begin{table*}[h]
\caption{Mean differences log~g$_{\it Gaia}$ - log~g$_{\rm spec}$  with standard deviation (1-$\sigma$) and median differences (in parenthesis) in three T$_{\rm eff}$ intervals. }
\begin{center}

\begin{tabular}{lllll}
\hline
\hline
Method  &   T$_{\rm eff} <$5000~K       & 5000~K$<$T$_{\rm eff} <$6000~K     & T$_{\rm eff} >$ 6000~K    &   Total T$_{\rm eff}$ range\\
\hline
SWEET-Cat & 0.132$\pm$0.068 (0.165)  &-0.042$\pm$0.017 (-0.032) & -0.381$\pm$0.037 (-0.393) & -0.115$\pm$0.023 (-0.083)\\
FAMA & 0.162$\pm$0.043 (0.160) &  0.059$\pm$0.020 (0.053) & 0.108$\pm$0.029 (0.126) & 0.088$\pm$0.016 (0.064) \\
FASMA &0.088$\pm$0.051 (0.037) &-0.086$\pm$0.011 (-0.084) & -0.280$\pm$0.014 (-0.289)  & -0.137$\pm$0.013 (-0.116) \\
\hline
\hline
\end{tabular}

\label{tab:diff:logg}
\end{center}
\end{table*}
In Table~\ref{tab:diff:logg} we divide the sample in three temperature regimes: T$_{\rm eff}<$5000 K, 5000 K$<$T$_{\rm eff} <$6000 K, and finally T$_{\rm eff}>$ 6000 K.
We compute the mean differences between the log~g from {\it Gaia} and the spectroscopic log~g from the three methods, and their standard deviation (1-$\sigma$).
In the coolest regime, all methods tend to underestimate the surface gravities, with differences consistent with each other within the error.
The spectral synthesis method FASMA provides gravities, on average, in better agreement with  the trigonometric ones.
In the intermediate regime, with 5000 K$<$T$_{\rm eff}<$6000 K, the three methods show the better agreement with the  log~g from {\it Gaia}: FAMA slightly underestimates the trigonometric gravities, while SWEET-Cat and FASMA slightly  overestimate them.
The most challenging regime is the hottest one, with T$_{\rm eff} >$ 6000 K.
In this temperature range, there is no agreement between the spectroscopic methods and the trigonometric one (FASMA and SWEET-Cat overestimate the trigonometric log~g, while FAMA slightly underestimates it).
In the last column, we report the mean differences for the whole sample: slightly negative differences for SWEET-cat and FASMA, and positive for FAMA. However, it is clear that global mean differences mask the most critical regimes, for the hottest and coolest stars of the sample.

\subsection{Comparison with log~g derived from the light-curves}
\label{sec:4.2}
\begin{figure}
\includegraphics[width=0.50\textwidth]{./Figure15.eps}
\caption{Trigonometric surface gravity vs surface gravity derived with the other methods, including spectroscopic methods and light-curve method.}
\label{fig:5}
\end{figure}
We compare the trigonometric and spectroscopic gravities with those derived from the light-curves in literature, and available in the SWEET-Cat database.
In Fig.~\ref{fig:4} (right top and bottom panels)  we show the difference between the log~g derived from the light-curves (literature values for 48 targets were found) and the respective spectroscopic log~g listed in the SWEET-Cat (green filled squares) and obtained through FASMA (red filled triangles) and FAMA (blue filled circles) as a function of T$_{\rm eff}$ and of the light-curves log~g.
First, we notice the good agreement between the trigonometric and light-curve surface gravities,
despite the two methodologies are quite different, and this is an encouraging result (see also Fig.~\ref{fig:5}).
Concerning the other methods, similar considerations as in the previous section can be obtained:
FAMA shows a bit higher dispersion and a positive offset, but almost no trend. FASMA displays the lower dispersion, but tends to
overestimate log~g at high T$_{\rm eff}$. SWEET-cat seems to overestimate log~g at high T$_{\rm eff}$, and underestimate at low T$_{\rm eff}$.
Clearly the hottest region is the most critical one, both because hot stars have less absorption lines useful to constrain the photospheric parameters and because stellar rotation might become important, making more difficult to measure absorption lines which can be blended.
Moreover, in the low-temperature regime, the presence of molecular bands can blend and hide the atomic lines.

\subsection{Comparison with isochrones }
\label{sec:4.3}

 Another important check is based on the comparison with theoretical isochrones, computed in
T$_{\rm eff}$ vs log~g plane, for a set of ages, keeping the metallicity constant at [M/H]=0.058
\footnote{Most of our targets have indeed close-to-Solar metallicity, with a mean [Fe/H] of the sample +0.11$\pm$0.18~dex ([Fe/H] from Sweet-cat values)}.
Fig.~\ref{fig:6} shows the Kiel diagrams (log~g vs T$_{\rm eff}$) for the values of log~g and T$_{\rm eff}$ listed in the Sweet-Cat, obtained by FAMA and by FASMA, and derived through {\it Gaia} photometry and parallax, respectively.
The PARSEC isochrones \cite{Bressan2012} in a range of ages are over-plotted:
the outermost tracks correspond to log(age/yr)$=8.95$ (bottom track) and $10.15$ (upper track)
with [M/H]$=0.058$, $Z=0.0198$, $Y=0.273$.
\begin{figure*}
 \includegraphics[width=0.5\textwidth]{./Figure16.eps}
 \includegraphics[width=0.5\textwidth]{./Figure17.eps}
 \includegraphics[width=0.5\textwidth]{./Figure18.eps}
 \includegraphics[width=0.5\textwidth]{./Figure19.eps}

\caption{Kiel diagram (log~g vs T$_{\rm eff}$) using values listed in SWEET-Cat, obtained by FAMA, FASMA and derived by {\it Gaia}. The outermost tracks correspond to log(age/yr)$=8.95$ (bottom track) and $10.15$ (upper track) with [M/H]$=0.058$, $Z=0.0198$, $Y=0.273$.}
\label{fig:6}
\end{figure*}

Fig.~\ref{fig:6} (left top panel) points out how the SWEET-Cat gravities are not matching the isochrones path and appear to be overestimated at the highest temperatures and underestimated at the lowest temperatures.
In Fig.~\ref{fig:6} (right top panel) we present the same plot for the results obtained with FAMA: T$_{\rm eff}$ and log~g follow the expected trend, however there is an offset towards lower gravities.
In Fig.~\ref{fig:6} (left bottom panel) we show the results of FASMA. The dispersion is lower, however, at high temperature there is still an overestimation of log~g.
Finally, in Fig.~\ref{fig:6} (right bottom panel) the {\it Gaia} parameters are displayed, pointing out the best match with PARSEC isochrones.

\section{Conclusions}
\label{sec:5}
In our first test, we have compared the analysis of a sample of $\sim$150 spectra (high S/N and high spectral resolution).
In the parameters space close to Solar values the agreement among the three methods is good (T$_{\rm eff}$= $5000-6000$ K, log~g $=4.2-4.6$\,dex).
However, at low and high temperatures some methods tend to under/overestimate the surface gravity log~g.
 This might have important effects on the derived stellar abundances.
External comparisons (using trigonometric log~g, log~g from light-curves and from isochrones) confirm the trends.
Corrections to these trends were already available (see, e.g, \cite{Mortier2014,Delgado2017}).
We plan in the next tests to apply them,
using both corrections from asteroseismology and light-curves to provide more realistic gravites.
In this context we refer also to the wider discussion present in literature on the disagreement
between spectroscopic and evolutionary or photometric log~g values (e.g. see \cite{Torres2012,Sozzetti2007}).

However, it is important to notice that, despite the differences in the derived photometric parameters,
especially in log~g, the three spectroscopic methods agree very well on the final metallicity, except in the hottest temperature regime.
Due to high quality of the {\it Gaia} photometry and parallax for the Ariel targets, a viable and welcome possibility is to adopt the surface gravity
homogeneously derived from {\it Gaia} to compute chemical abundances.

\begin{acknowledgements}
We like to thank the anonymous referees for the fruitful comments on our paper.\\
AB, MT, LM, MvS, GC acknowledge  the funding from MIUR Premiale 2016: MITIC.\\
E.D.M., V.A. and S.G.S. acknowledge the support from Funda\c{c}\~ao para a Ci\^encia e a Tecnologia (FCT) through national funds and from FEDER through COMPETE2020 by the following grants: UID/FIS/04434/2019, UIDB/04434/2020\\ and UIDP/04434/2020;
PTDC/FIS-AST/32113/2017 \\and POCI-01-0145-FEDER-032113;\\ PTDC/FIS-AST/28953/2017
\\and POCI-01-0145-FEDER-028953.\\
https://www.overleaf.com/project/5ee29f0469a39e00013326b1.\\
E.D.M., V.A., S.G.S. also acknowledge the support from FCT through Investigador FCT contracts\\
IF/00849/2015/CP1273/CT0003,\\ IF/00650/2015/CP1273/CT0001,\\ IF/00028/2014/CP1215/CT0002.
\end{acknowledgements}

\newpage

\bibliographystyle{spmpsci}

redpajama_set_name: RedPajamaArXiv


text:
← The Starry Night
Meet The Fetals →
Finer Diner
Posted on August 20, 2012 by Val
54 Twenty
Hollywood (Los Angeles), California
The newly-refurbished 54 Twenty in Hollywood
It's a sweltering mid-morning in Hollywood; a man in a plaid short-sleeved shirt and a pair of jeans with frayed knees walks into a small diner that looks as though it has been pristinely preserved since the 1960s. As he makes himself comfortable in one of the red plush swivel chairs along the long faux-wood Formica counter top, he picks up a freshly printed paper menu and makes his selection from what at first glance appears to be a traditional diner menu. He requests the French toast and a cup of coffee, places his menu on the counter and quickly receives a sucker punch square against his jaw, his head awash in a myriad of stars – he has just been indoctrinated in a new traditionalism, the next wave of diner culture as imagined by Chef Kyle Schutte.
The decadent stuffed French toast
Chef Schutte has been plying his interpretation of molecular gastronomy since arriving in the Los Angeles area by way of Charlotte and Atlanta in 2010. While in residence in Marina del Rey's Vū Restaurant, he was named by Angeleno Magazine as one of L.A.'s top young chefs to watch in 2011, although he admits that his experimental style was misunderstood in an area where the locals were complacent with chains such as Cheesecake Factory and Killer Shrimp – the texture and intense flavor of his sous vide eggs and other non-traditional takes on familiar items left them slightly confused. As Executive Chef at 54 twenty, Schutte applies those techniques to diner fare, turning that genre of cuisine on its ear. His heavy use of sous vide is borne partially out of the quality and flavor it imparts to the food and out of space considerations; since the every inch of space is open and exposed, storage considerations and appliances are at a minimum (several small freezers and refrigerators were installed around the cooking area with 54 Twenty depleting its inventory almost daily). Bread is the only staple that is not made in-house – everything else is handmade, right down to the ketchup. There is a small oven on the premises, but because resources don't allow it to be turned down for some time, Chef Schutte resorted to "sous viding" garlic for two hours in olive oil to compensate; when the result was tested he vowed never going back to roasting traditionally again.
The corned duck Ruben is an onslaught of flavor
The restaurant is attached to the Dixie Hollywood hotel, formerly a Days Inn; it spent the first half century or so of its life as Angel's Diner. By the time owner Deepa Patel hired young gun Schutte as Executive Chef, the space was looking a bit long in the tooth, a shadow of its former self. Schutte gutted the room, tearing out booths and replacing them with a long, plush banquette wall bench and tables and demolishing the lowered ceiling to its original height to open the room up. For Schutte, working in the open environment is conducive to the personal style of customer service he had been known for even at Vū where it was not uncommon to see him working the room, talking to the patrons about the food and even bussing tables. 54 Twenty has been dubbed a "guestaurant", and although the first inclination would be to assume the moniker referred to it being part of the hotel, Schutte explains that the industry term essentially describes a dining experience that is part dinner party, part intimate restaurant. For the time being the menu offers all-day brunch dining (through 9 PM); by request of patrons who arrive at the evening looking for dinner items, a tasting menu is planned for late in the fall that will feature 5 to 9 courses. 54 Twenty has not yet been granted a liquor license, but encourages diners to bring their own bottle.
Ketchup tomatoes crown the short rib burger
The coffee beats the pants off the garden variety cuppa joe available at your neighborhood greasy spoon; their caffeinated staple is from local roasters Handsome Coffee Roasters. If you're leaning towards the "br" side of brunch, Chef Schutte takes the familiar and re-engineers it into a unique breakfast experience; the steak and eggs features Paso Prime top sirloin cap coulotte sous vide in chimichurri with triple-cooked fries tossed in ketchup spice and sous vide-baked eggs; the off-menu bacon and eggs includes a 6-oz slab of Niman Ranch ham sous vide in maple syrup. The French toast is recognizable in name only – the massive wedge of bread is stuffed with cinnamon cream cheese and is positioned over a scrape of strawberry and thyme jam; a small container of syrup is placed on the side with an intoxicating blend of maple syrup infused with vanilla bean and star anise. To describe the dish gives the impression of a dentist's nightmare, but the sweetness is cut by the flavors of the other ingredients; texture-wise, the softened cream cheese plays off the spongy quality of the bread and is complemented by the condiments.
A three egg omelet with Lamb Chopper sheep milk cheese, cheddar and arugula
The outstanding dish that raises a defiant finger to local delis, diners and drive-ins is the incomparable duck Reuben. Chef Schutte starts with free range duck from Mary's (Pittman Family Farms) which is brined and then sous vide in the brine, after which the outside flesh is then seared. The top layer of the sandwich is populated with a pickled red cabbage that packs an explosion of equal parts sweet and sour – after finishing the sandwich it seems unfathomable to consume it without the slaw. A layer of gruyere cheese is added and the rye is then grilled and served with house-made potato chips. 54 Twenty has a slicer that shaves the potatoes razor-thin, but when the hardware becomes uncooperative they are sliced by hand; salt is added sparingly towards the end of the cooking process and the wispy chips are tossed with pastrami spice, resulting in a light-as-air potato wafer that dissolves on the tongue.
Unique touches accentuate traditional fare; the BLT is dubbed the "B³LT" as it features bacon three ways, including the bread being grilled in bacon fat; the short rib burger is capped with ketchup tomatoes (quartered Romas which are skinned before pickling with ketchup flavors) that keep the bun from turning into a soggy mess. 54 Twenty is changing the way we think of a slice of Americana that is going by the wayside, revitalizing and taking the cuisine to the next plateau; think of it as Guy Fieri with a pedigree.
5420 Hollywood Boulevard
GPS Coordinates: 34° 6'5.71″N 118°18'28.90″W
GALLERY: See images from Val's visit to 54 Twenty in Hollywood, California
NOTE: This cost for this meal was provided by the restaurant. The content provided in this article was not influenced whatsoever by the organizer of the event.
This entry was posted in Southern California and tagged 54 Twenty, Angeleno Magazine, Angel's Diner, Atlanta, BLT, CA, California, Charlotte, cheese, chef, chips, Days Inn, Deepa Patel, Diner, Dixie Hollywood, duck, executive chef, French toast, frittata, guestaurant, Handsome Coffee, Hollywood, ketchup, Kyle Schutte, L.A., LA, Lamb Chopper, Los Angeles, Marina Del Rey, Niman Ranch, Paso Prime, red cabbage, Restaurant, Reuben, short rib burger, sous vide, Vū. Bookmark the permalink.


The next Workation Camp that the DNX team will organize will be located in the famous kitesurfing destination Jericoacoara in Brazil. If you've been part of the Digital Nomad Tribe for a while you are familiar with DNX and you have probably already heard of the legendary DNX camps that Marcus and Feli are putting out there. So even if you are not into kitesurfing, this destination might still be interesting to you as there are plenty of other features involved.
The DNX team invites a special guest who you can talk to. They will organize a trip to the Tatajuba Lagoon.
The residence is a villa with a lounge, balcony, garden and barbecue. Cleaning is included.
In this Workation Camp, you can do sport activities such as Windsurf, wave surf, Kitesurfing sand-boarding and horseback riding. They also provide dance classes, yoga and zumba. You can join six kitesurfing trips (45€ including transportation; lessons and gear extra).
11 digital nomads will join this Workation Camp in Brazil.
In the price is included accommodation, workspace, breakfast, cleaning and the trip to Tatajuba Lagoon.


text:
Milita negli ZZ Top fin dagli esordi. È l'unico dei tre membri a non portare una lunga barba (paradossalmente il suo cognome "Beard" significa proprio "barba" in inglese) ma solo un paio di baffi.

Con 50 milioni di album venduti (di cui 25 milioni negli Stati Uniti), 8 successi nella Top 40 delle classifiche statunitensi, 6 prime posizioni nella Mainstream Rock Songs e 3 MTV Video Music Awards conquistati, il 15 marzo 2004 è stato inserito, insieme agli ZZ Top, nel Rock and Roll Hall of Fame.

Strumentazione
 batterie Tama
 piatti Paiste
 bacchette Pro-Mark
 trigger Ddrum

Note

Voci correlate
 ZZ Top

Altri progetti

Collegamenti esterni

Batteristi blues rock
Batteristi hard rock
Batteristi southern rock
Batteristi boogie rock
Batteristi country rock

redpajama_set_name: RedPajamaWikipedia


Allan Curran Architects are a small firm based primarily in Donegal but with offices – and clients – in Enniskillen also. I've worked with them for over 10 years now and this latest iteration of their website puts a strong emphasis on the photography of their projects. They're just beautiful.
Five minutes spent clicking through their portfolio is enough to leave you with home envy – their focus on making the most of the surrounding natural environment, and blending their buildings into it, marks them out as an exceptional local firm.


Welcome to Midway Dental Laboratory website, we are always ready for your needs of low price and high quality customized abutment made in China and China customized abutment.
our lab offers three customized implant abutments, Custom Implant Abutments are available in Titanium, Zirconia with Titanium Base and All-Zirconia to fit your patients' individual needs. Titanium abutments are commonly used in all regions of the mouth due to their strength. Zirconia abutments provide the best possible esthetics and are commonly used in the anterior with all-ceramic or zirconia restorations.
When you prescribe our customized Abutments, a natural-looking emergence is designed using 3-D CAD technology and then fabricated using precision 5-axis milling. This precise interface optimizes soft tissue contours and crown esthetics and also ensures excellent gingival health.


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After all the drama and trauma of her recent past, Lori is taking only easy assignments — her life needs to coast for a bit. Naturally, that's not going to work too well (why would we read about that? Also, why would Broadribb be nice to her now?) — she'd kidnapped by the Miami Mob and we readers have to be braced for all sorts of nasty things to happen to her. And while it is nasty — no one is prepared for what happens to her.
They want her to do a job for them. If she succeeds, they offer to wipe the slate clean. If she fails (or refuses), she, Dakota and JT are dead. Honestly, there's a pretty good chance they'll die no matter what, but there's a chance with the former. All she has to do is retrieve the "numbers man" for the family, currently under FBI protection before he testifies against the family in a couple of days. It's pretty cool to see how good Lori does at this until things go horribly, horribly wrong (not much of a spoiler, really — the book isn't going be too suspenseful if she has an easy time of it).
Meanwhile, JT and Dakota run to safety — which goes only slightly worse than Lori's assignment. JT isn't anywhere near as healthy as he should be to handle this kind of thing — but he doesn't have much of a choice. It's his little girl, what else can he do? It's great to see JT in action like this. But at some point, at the rate things are going for her, Dakota's going to end up catatonic or like the little girl in Logan. My money's on the latter.
So we've got the Mob on one hand, the FBI on the other, and a distinct lack of options for this family — it's all about survival. The longer you're alive the more opportunities will present themselves to extricate yourself from this Catch-22. As much as Lori (and JT and Dakota) is tough and resilient, it's her ability to improvise, to think quickly and to pounce on the chances that life gives her that makes her an action hero to pay attention to.
A female bounty hunter with skills and the kind of grit you want to see in an action hero, Lori is a great character. The physical toll on her in this novel is up there with the psychological toll previous adventures have taken on her — not that she gets out of this one emotionally/mentally unscathed (nor did she get out of the previous adventures without a physical injury or 8). She's smart, determined and prepared to dish it out as well as take it.
I walked away from book 2, Deep Blue Trouble with a pretty strong idea about what book 3 was going to be about. I was wrong, but I'm pretty confident that I know what book 4 will be about (at least initially). I'm very glad to be wrong, actually — because this was a lot of fun, and sets things up to be a more satisfying version of the story I imagined Broadribb would be telling. I'm eager to find out how wrong I am about book 4 (because I will be).
I've spent about a month working on this post in fits and starts, because I'm having a hard time saying something about this book that I didn't say about the other two. Broadribb started off strong — a veteran from the get-go, and the other two have been of the same quality. Consistency is great when you're a reader — but it's hard to write about. So I give up — I'm not going to have anything insightful to say or any dazzling or penetrating analysis to offer. I'll keep it basic — Deep Dirty Truth is a good, fast-paced, white-knuckle ride written by someone who knows what she's doing. Go read it.
Hmm… I see people really enjoying the series!
I think I remember something like that happening in book 1 – but it didn't hurt the experience for me as it did for you. Ilbut I can see where something like that could put me off a series.
If you have the time, you might want to give Broadribb/Lori another shot.


Columbia Entertainment Company presents �Fat Pig� March 11 to 14 at 1800 Nelwood Drive. A Stage II Production, recommended for age 18 and older. Performance times are 7:30 p.m. Thursday through Saturday and 2 p.m. Sunday. Tickets are $10 for general admission, $9 for students with ID, $8 for seniors and children. For more information, visit www.cectheatre.org.
University of Missouri Department of Theatre: �Brighton Beach Memoirs,� a coming-of-age comedy by Neil Simon, and directed by James Miller, will be Thursday through Saturday at Rhynsburger Theatre. Performance times are 8 p.m. Thursdays through Saturdays and 2 p.m. Sundays. Tickets are $12 general public, $10 faculty and staff, $8 for students and seniors.
University Concert Series: Moscow State Radio Symphony Orchestra 7 p.m. Thursday at Jesse Auditorium on the University of Missouri campus; $17, $24, $32. Also St. Louis Symphony Orchestra 7 p.m. March 9; $17, $27, $37. 882-3781. www.concertseries.org.
Fayette Area Community Theatre: �Doubt, A Parable� by John Patrick Shanley 2 p.m. today in the Assembly Hall underneath Linn Memorial Church on Central Methodist University campus. Adults $5, seniors $4, students $2. (660)248-2826.
University of Missouri Department of Theatre presents a free �Evening of Improv� with Emily Wilson, star of �The Second City Mainstage,� 4 p.m. Thursday at Jesse Wrench Auditorium.
Stephens College Playhouse Theatre Company �Playhouse Creatures� 7:30 p.m. Wednesday through Saturday at Warehouse Theatre, 104 Willis Ave. $8 general public, $6 students and seniors. 876-7199.
Independent Actors Theatre: �Dead Man�s Cell Phone� by Sara Ruhl, March 11 to 13. Learn more at www.iatheatre.org.
PACE Youth Theater: �The Sound of Music� April 15 to 18 at the Missouri Theatre Center for the Arts, 203 S. Ninth St. www.kidsintheact.org, 443-0541.
TRYPS Children�s Theater: �Disney�s Aladdin Jr.� May 14 to 17 at Launer Auditorium at Columbia College. www.tryps.missouri.org. Call Jill Womack at 449-4536 or e-mail tryps@me.com.
Deja Vu Comedy Club presents Kenny Kane and Drake Witham 9:30 p.m. Thursday, 8 and 10:15 p.m. Friday and Saturday. $7 Thursday and $8 Friday and Saturday. www.dejavucomedy.com.
5th Wall Productions seeks directors or those interested in being involved behind the scenes for the 2010 season. Directorial positions are paid by stipend. Interested applicants should send a current theatrical r�sum� to Artistic Director Amanda Altier at artisticdirector@5thwallproductions.org. The deadline is Wednesday.
Arrow Rock Lyceum Theatre 2010 season includes �The Producers,� �Anything Goes,� �Red, White and Tuna,� �My Fair Lady,� �The Man Who Came To Dinner,� �And Then There Were None,� �Pump Boys and Dinettes� and �Nuncrackers.� The season kicks off June 2. www.lyceumtheatre.org.
Maplewood Barn Community Theatre will hold auditions for its 37th season beginning with �Arsenic and Old Lace� from 1 to 4 p.m. March 13 and 14 in Room 110 of Lee Hills Hall, at Eighth and Elm. Roles are available for 11 men in their early to mid-20s through late 50s and three women, one early to mid-20s and two mid- to late 60s. The classic comedy revolves around Mortimer Brewster, a marriage-hating drama critic who must deal with his crazy, homicidal family and local police in Brooklyn as he debates whether to go through with his recent promise to marry the woman he loves. Performances are in May. See the 2010 season at www.maplewoodbarn.com.


text:
Der Trauben-Gamander (Teucrium botrys), auch Feld-Gamander genannt, ist ein Angehöriger der Lippenblütler (Lamiaceae).

Beschreibung
Die einjährige, selten auch zweijährige krautige Pflanze erreicht eine Wuchshöhe von 10 bis 30 cm. Sie hat einen unangenehmen Geruch. Der Stängel ist aufsteigend, drüsig zottig behaart und unten meist mit bogig aufsteigenden Ästen versehen. Die Blätter sind langgestielt, 1,5 bis 2,5 cm lang, die unteren einfach, die oberen meist doppelt fiederspaltig mit lanzettlich-linealischen Lappen.

Die Blüten stehen zu 2 bis 4 (bis 6) in den Achseln der Laubblätter, sind 10 bis 15 Millimeter lang und besitzen 3 bis 7 Millimeter lange Stiele. Die Krone ist trübrosa, sehr selten auch weiß gefärbt. Die Staubblätter und Griffel ragen weit hervor und sind herabgebogen. Der Kelch ist etwas aufgeblasen, besitzt eine große, nach hinten gerichtete Aussackung und ist dicht drüsig-flaumig behaart. Die beiden unteren Kelchzähne sind kleiner als die 3 oberen. Die Unterlippe der Blütenkrone ist schwach behaart und hat einen großen, konkaven, mit dunkelpurpurnen Strichen und Flecken versehenen Mittellappen. Die vorderen Seitenlappen sind ausgebreitet, die hinteren sind klein, spitz und aufgerichtet. Die Staubblätter und der Griffel sind weit vorragend und herabgebogen. Die Nüsschen sind fast kugelig, 1,5 bis 2 mm lang, grubig-rau und besitzen eine von einer tiefen Furche umzogene Anheftungsfläche.

Die Art blüht von Juli bis Oktober.

Die Chromosomenzahl beträgt 2n = 10, seltener 32.

Ökologie
Die Blüten zeigen die Eigentümlichkeit, dass sich die Blütenstiele oft nach rechts drehen, so dass die Unterlippe nach links oder selbst nach oben zu liegen kommt. Diese schwach angedeutete, so genannte Resupination, tritt bei einigen mediterranen Arten regelmäßig auf.

Die Blüten werden durch Bienen der Gattungen Anthidium und Sphecodes bestäubt. Auch Selbstbestäubung soll vorkommen.

Verbreitung und Standortansprüche
Der Trauben-Gamander wächst in Äckern, Weinbergen, Lesesteinhaufen, Kiesgruben, Steinbrüchen, auf Geröllhalden, an Bahndämmen und an Ruderalstellen. Er kommt besonders auf kalkhaltigen, humus- und feinerdearmen Böden vor, gelegentlich ist er auch auf kalkarmem Gestein zu finden. Er ist in Mitteleuropa eine Charakterart des Teucrio-Melicetum aus dem Verband Seslerio-Festucion pallentis. Er steigt im Schweizer Jura bis 1020 Meter, im Allgäu bis 1300 Meter, im Kanton Wallis bis 1440 Meter und in Tirol bis 1500 Meter Meereshöhe auf.

Teucrium botrys kommt vom westlichen Mittelmeergebiet mit Algerien und Marokko bis Mittel- und Osteuropa vor. Er dringt östlich bis Polen, die Ukraine und den nördlichen Balkan vor.  Er ist ein submediterran-subatlantisches Florenelement. In Österreich und der Schweiz findet man ihn allgemein zerstreut vor. Gebietsweise ist er auch gefährdet.

Die ökologischen Zeigerwerte nach Landolt et al. 2010 sind in der Schweiz: Feuchtezahl F = 1+w+ (sehr trocken aber stark wechselnd), Lichtzahl L = 4 (hell), Reaktionszahl R = 4 (neutral bis basisch), Temperaturzahl T = 4+ (warm-kollin), Nährstoffzahl N = 2 (nährstoffarm), Kontinentalitätszahl K = 4 (subkontinental).

Der Trauben-Gamander kommt in Deutschland in den südlichen Kalkgebieten zerstreut bis verbreitet vor (unter anderem Oberrhein- und Neckargebiet, Pfalz). Darüber hinaus ist er selten oder nur verschleppt aufzufinden.

Nutzung
Der Trauben-Gamander wurde nur gelegentlich als Arzneipflanze kultiviert.

Literatur
 Gustav Hegi: Illustrierte Flora von Mitteleuropa. Verlag Paul Parey, Berlin und Hamburg 1975, ISBN 3-489-78021-3
 Christian August Friedrich Garcke: Illustrierte Flora. Verlag Paul Parey 1972, ISBN 3-489-68034-0
 Wolfgang Adler, Karl Oswald, Raimund Fischer: Exkursionsflora von Österreich. Hrsg.: Manfred A. Fischer. Ulmer, Stuttgart/Wien 1994, ISBN 3-8001-3461-6.
 August Binz, Christian Heitz: Schul- und Exkursionsflora für die Schweiz. Schwabe & Co. AG, Basel 1986, ISBN 3-7965-0832-4
 Erich Oberdorfer: Pflanzensoziologische Exkursionsflora. Ulmer Verlag, Stuttgart 1990, ISBN 3-8001-3454-3

Einzelnachweise

Weblinks

 Thomas Meyer: Gamander Datenblatt mit Bestimmungsschlüssel und Fotos bei Flora-de: Flora von Deutschland (alter Name der Webseite: Blumen in Schwaben)

Gamander


text:
The Sovetsky District court of Nizhny Novgorod will examine Andronovs' case on the 13th of September
At the preliminary hearing of the case judge Tatiana Kuzina examined a number of technical questions necessary for the case preparation for the new examination on the merits.
As you may remember, the ground for the the appeal for compensation for non-pecuniary damage that was made to minor Dmitry Andronov was his unlawful detention.
On the 9 of March 2007 the Nizhny Novgorod regional court ruled to free Mr. Andronov from detention, but the detention facility administration refused to do so alluding to the end of workday. Mr. Andronov was released only after a day.
You may also remember that the applicant and his relatives are represented in court by the lawyers of the Committee Against Torture. Besides, the Committee specialists are holding a public investigation on the Andronovs' claim that states that the boy was cruelly tortured by the policemen and prosecution officers of the city Pavlovo.
In the course of the preliminary hearing the federal judge Kuzina decided to recognize the detention facility 52/1 that had been considered a third party as a co-defendant in this case.
The representative of the guardianship authorities that was present at the hearing supported the position of the Committee specialists actively, and welcomed the decision, pointing out, that the rights of minor Andronov in the situation examined had surely been violated by the detention facility.
In the course of hearing the court asked the representative of the detention facility whether the fact that a person freed by the court decision was kept in prison because the work day of the detention facility officials was over, corresponded to the international law. The representative of the detention facility admitted that that was a violation of the international law.
The judge also touched upon the details of Mr. Andronov's release that took place on the 10 of March 2007. It was proved, that the court decision to release Mr. Andronov was brought to the detention facility on the 9 of March by a court official, but it was not accepted. Meanwhile, the next morning Mr. Andronov was released by the order of vice-prosecutor of the region, Tkachev. This situation caused the federal judge to ask quite an expected question: why did the administration of the detention facility execute the decisions of the prosecutor's office immediately but ignore the court decisions? This is one more question to answer at the case hearing that will take place on the 13 of September.


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text:
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    <title>Tonga</title>

CAAMBILIZYO CA MULAWO WA MASI OONSE WA LWAANGULUKO LWA MUNTU MATALIKO

Mbuli mbokunga kulemeka muntu oonse ncizyalilwa ca lwaanguluko lwa mikwasyi yoonse kuba matalikilo akuliiba, kukwabililwa amulawo alimwi aluumuno munyika:

Kakuli kutalemeka alimwi akutyola milawo ya lwaanguluko lwa muntu kuleta micito yabujayi mibyaabi kulanyemya akutakkazyika kabotu bantu alimwi kwazungaanya nyika kuti ijane nzila yakwaangulula bantu kuti kabaliiba kukanana zyobayanda alimwi akutobela zyobasyoma alimwi akwaanguluka kwakutayoowa kwakaambilizyigwa kuba nenzila mpati veelede kuyumya muntu.

Kakuli ncintu cipati, kuti muntu tasungilizyi kulomba lugwasyo kuba nenzila ilikke yamamanino, ulakonzya kucita zyintu zyimbi zyibyaabi zyakulikwabilila kudyaamininwa, kuti buumi bwa muntu weelede kukwabililwa amulawo.

Kakuli ncintu cipati kusumpula lumvwano akati kamasi, kakuli bantu bamasi aali mu mbunga ya United Nations mu milawo ya malembo amumbunga eeyi akasyomenzya lusyomo mu milawo ya lwaanguluko lwa muntu, kubulemu alimwi abuvubi bwamuntu alimwi alwanguluko lweelene ku basankwa abakaintu alimwi akuba amakanze akusumpula bukkale bwabuumi bwabo mukuliiba kunji.

Kakuli masi aali ma memba ambunga eeyi akasyomezya kuya kuzwidilila, mukubelekela antoomwe ambunga ya United Nationes, kusumpula akucita kulemeka mulawo wa lwaanguluko lwa muntu alimwi akulekela bantu kuliiba, kakuli kumvwa kwa lwaanguluko oolu alimwi akuliiba nkupati mukubona kuti kusyomezya ooku kwabeleka.

Lino aboobo, Muswaangano Mupati (Generl Assembly) waambili zya zyeezyi: Eeci cizumino ca kwaambilizya lwaanguluko lwa muntu kuba nenzila ngubauba yabantu boonse alimwi amasi oonse kujana, kumasimpilo kuti muntu oonse alimwi azyibeela zya buleya, kuyeeya cisyomezyo eeci lyoonse mu myoyo, ciya kusola mbocikonzya kuyiisya alimwi akusumpula kulemeka lwaanguluko alimwi akuliiba alimwi kwiinda munzila isumpukide, masi alimwi akubantu bamumasi aali mubweendelezi bwa bantu bambi.

CIZUMINANO CA MULAWO UJATIKIZYA MASI OONSE CAKULESYA BUTUNDULUZI BWA MUNTU

Kapango 1

Bantu boonse balazyalwa kabaangulukide alimwi kabeelene alimwi akwaanguluka kucita zyobayanda. Balazyalwa amaanu akuyeeya, aakusala alimwi beelede kulanga bambi mbuli banabokwabo.

Kapango 2

Mukuya ambele, kunyina kusalaula kweelede kucitwa akaambo katwaambo twacisi, bweendelezi bwa milawo antela bulemekwa cisi nkwazwa muntu, cibe cisi cakalilela kale, citaninga kulilela nokuba kuba amweele wakutaindilizya.

Muntu oonse ulaangulukide ku zyintu zyoonse zyili mucizuminano, kakunyina kusalaula mbuli kwakusiyana cikanda, musyobo, buzyale, cikombelo, makani a twaambo twacisi antela kwiimpana kwakuyeeya, busicisi antela bukkale, buvubi, nkokazyalilwa antela kwiimpana kumbi.

Kapango 3

Muntu oonse ulaangulukide kubukkale bwabuumi, lwaanguluko alimwi akukwabililwa.

Kapango 4

Kunyina weelede kuba muzike antela cibelesyo, buzike alimwi amakwebo aabuzike zyeelede kukasyigwa munzila zyoonse.

Kapango 5

Kunyina weelede kupezyegwa, kutalanganyizyigwa mbuli muntu antela kubelesyegwa mbuli cibbalo antela kupegwa cisubulo.

Kapango 6

Muntu oonse ulaangulukide kulemekwa koonse nkwabede kuba muntu kubusyu bwa mulawo.

Kapango 7

Bantu boonse baleelene kubusyu bwa mulawo alimwi balizumizyidwe kakunyina kusalaula kubukwabilizi bwa mulawo bweelene. Boonse balaangulukide kukwabililwa kweelene kumicito yakusalaula mukutyola cizuminano eeci alimwi akumicito ya kubisya zyintu zyikonzya kuleta kusalaula.

Kapango 8

Muntu oonse ulaangulukide kwiimininwa ambunga ya bantu basalwa mucisi kubona kaambo kakwe nkasinkilwa kulwaanguluko lwakucita ncayanda ncazumizyilwe amulawo.

Kapango 9

Kunyina muntu weelede kwaangwa, kuyobolwa muntolongo kakunyina mulandu antela kutija kuya kukkala kucisi cimbi.

Kapango 10

Muntu oonse ulaangulukide kakunyina kwaandana kubetekwa ambunga yasalwa inyina nkoilikumbtizya alimi isitikene kulanga kukwabililwa ku lwaanguluko ndwajisi alimwi ayimwi milandu njakonzya kupegwa.

Kapango 11

Oonse wapegwa mulandu ulaangulukide kwiitwa kuti ucisalalakusikila akaianwe amulandu mu nkuta mbuli bwaamba mulawo libetekwa alimwi ulizumizyilwe kujmana bamwiimiminina libetekwa mulandu wakwe.

Kunyina ukonzya kujanwa mulandu kuti kakuli cintu comwe cicaala citakonzyi kupa kuti ube mulandu, kwiinda mu milawo ya cisi antela ijatikizya masi oonse, ciindi mulandu ooyu niwakacitika. Lyalo kunyina cisubulo cipati ceelede kupegwa kunze aacisubulo ceendelana amulawo ciindi mulandu niwakacitwa.

Kapango 12

Kunyina muntu weelede kunyonganyizyigwa kutayelede kuzyintu zyakwe, mukwasyi, munzi antela magwalo, antela kumutalika akaambo kabulemu bwakwe. Oonse ulaangulukide kukwabililwa amulawo kukunyonganyizyigwa antela kutalikwa ooku.

Kapango 13

Oonse muntu ulaangulukide kweenda mbwayanda alimwi akukkala kufumbwa mucisi.

Oonse muntu ulaangulukide kuzwa kufumbwa mucisi, kusanganizya acisi cokwabo, alimwi akupiluka kucisi cokwabo.

Kapango 14

Oonse muntu ulaangulukide kulomba kukkala akuliiba mucisi cimbi mwaatijila kuyuba kwaangwa antela kupezyegwa musi mwazwa.

Kukwabililwa kulwaanguluko oolu kulakozya kutyolwa kubantu batija kubetekwa milandu isalala kabotu itali mbuli ya makani atwaambo twacisi antela itayendelani anzila alimwi amilawo ya mbunga ya manyika oonse (United Nations).

Kapango 15

Oonse muntu ulaangulukide kuba munacisi wacisi ncayanda kukkala.

Kunyina uyedele kukasyigwa kucinca busicisi antela kukasyigwa kutacinca.

Kapango 16

Basankwa abakaintu bakakomena, kakunyina kubakasya akaambo kacikanda cabo, cisi ncobazwa antela cikombelo, balangulukide kukwata kufumbwa ngobayanda alimwi akubamba mukwasyi. Balangulukide kuba alwaanguluko lweelene lwa bakwetene ciindi nobacikwetene alimwi anobalekana.

Kukwatana kuya kulembezyegwa abaabo basikuyandana bobile kakunyina kuyoowa.

Mukwasyi ncilenga cabuleya kukkala antoomwe alimwi mukwasyi weelede kukwabililwa ku buleya alimwi akucisi.

Kapango 17

Oonse muntu ulaangulukide kuba alubono alikke antela kubeleka aatomwe abamwi.

Kunyina weelede kunyonganizyigwa antela kunyangwa lubono lwakwe.

Kapango 18

Muntu oonse ulaangulukide kuliyeeyela, kulisalila cikombelo ncayanda; lwaanguluko oolu lulajatikizya alusyomo ndwajisi alikke antela mu mbunga ya bana maleya nokuba kuliiba alikke, kutobela buyiisya cikombelo antela walo kuyyiisya, alimwi akukomba.

Kapango 19

Muntu oonse ulaangulukide kwaamba zyili kumoyo; kwaanguluka ooku kulajatikizya akubuzya, kulaigwa alimwi akupa mizeezo kwiinda mumapepa antela mulisikapepele kakunyina munyinza.

Kapango 20

Muntu oonse ulaangulukide kuba mukabunga antela kubungana kwaluumuno.

Kunyina weelede kusungilizyigwa kuba mukabunga nkatayandi.

Kapango 21

Muntu oonse ulaangulukide kutola lubazu mubweendelezi bwa mfulumende mucisi cokwabo antela kwiinda kumuntu usalwa biya abana maleya antela lwakwe mukamwini.

Muntu oonse ulaangulukide kupegwa lugwasyo lweelene alugwasyigwa bana maleya mucisi.

Kuyanda kwabantu kweelede kuba ciiminizyo ca mfulumende; kuyanda ooku kweelede kutondezyegwa kwainda ciindi alimwi akusala kwamasimpe kweelede kucitwa abana maleya bamucisi bazumizyigwa amulawo kusala alimwi akuzumizyigwa kusala ngwayanda kakunyina kunyonganyizyigwa.

Kapango 22

Muntu oonse, muna maleya, ulaangulukide kuyobwedwa mali ngakoswedwa ku mali ngavwola ku nkampani yakabambwa mucisi antela kwiinda mukumvwana acisi cimbi kweelene amulawo wacisi. Alimwi ulaangulukide kulyeezyela buvubi, kuba abukkale alimwi akucita zyilengwa zyacisi zyitakonzyi kumusala akaambo ka ciimo cakwe alimwi alwaanguluko lwa kusumpula bukkale bwakwe.

Kapango 23

Muntu oonse ulaangulukide kujana mulimo, kulisalila mulimo ngwayanda, kububotu bujanwa amulimo ooyo alimwi akukwabililwa kupenzi lyakubula milimo.

Oonse, kakunyina kusalaula, ulakwabililwa kuvwozyegwa mali ayelene amulimo ngwabeleka.

Oonse ubeleka ulaangulukide kupegwa mali abikkilwa atala antela bbonasi alimwi akukwabililwa buumi bwakwe alimwi abwamukwasyi wakwe azyintu zyimbi zyeelede kukwabililwa.

Muntu oonse ulaangulukide kunjila antela kutalika mbunga ilwanina akukwabilila babelesi.

Kapango 24

Muntu oonse ulaangulukide kupumuna akulyookezya kubeleka, kusanganizya kupegwa mawoolo ayelede ciindi cakubeleka alimwi akubbadelwa mali waunka kukupumuna kwa mazuba manji.

Kapango 25

Muntu oonse ulaangulukide ku buumi abukkale bubotu antoomwe amukwasyi wakwe, mbuli kuli cakulya, zyakusama, ng'anda yakukkala alimwi amicelo yakusilikwa azyintu zyimbi ziyandika kumuntu, alimwi akukwabililwa buumi bwakwe wani kubeleka, kukwabililwa kumalwazi, bulema, kufwidwa, kucembaala alimwi azyimbi zyikonzya kusinkila muntu kubuumi zyatakonzyi kucita akaambo kakubula nzila yakuzyicita.

Bamatumbu alimwi abana balaangulukide kulugwasyo luyandika. Bana boonse, abe wamung'anda antela wamusyokwe, beelede kulangwa kabotu alimwi akukwabililwa kweelene.

Kapango 26

Muntu oonse ulaangulukide kuyiya, lwiiyo lweelede kupegwa biyo kakunyina kubbadela, kapati muma giledi akutalisya masyoonto alimwi aakati-kati. Kunjila cikolo kumagiledi akutalisya weelede kuba mulawo natayandi nayanda mwana. Lwiiyo lwa milimo ya maanza alimwi aiyandika kuba haanzyibwene wa mulimo umwi lweelede kuti lyoonse kaluliko alimwi lwiiyo lwa mabbuku mapati alwalo lweelede kupegwa kuli baabo bajisi maanu.

Lwiiyo lweelede kuba lwakusumpula bukkale bwa muntu alimwi akuyumya lwaanguluko alimwi akusala ciyanda muntu. Lupa bantu kumvwisisya, kuba sicamba alimwi akusumpula lumvwanoakati kamasi, kakunyina kusalaula cikanda, cikombelo alimwi akuyumya milimo ya mbunga ya masi oonse munyika ya United Nations kutontozya luumuno munyika.

Bazyali balaangulukile kusala lwiiyo ndobayanda antela ndobayeeyela kuba lubotu kubana babo.

Kapango 27

Oonse muntu ulaangulukide kakunyina kukasyigwa kutola lubazu mubuumi bukkala bana maleya, kuyiya zyilenwa zyacisi alimwi akwaabana busongo.

Oonse muntu ulaangulukide kukwabililwa ku zyintu zyayanda mbuli zya kulyaanzila, nyimbo azyisobano zyalilembela mukamwini.

Kapango 28

Oonse muntu ulizumizyilwe Kuba mumakamu alimwi amunkamu zyijatikizya masi manji oomo mujanwa lwaanguluko lwakazuminanwa akwaambilizyigwa amilawo ya mbunga eeyi.

Kapango 29

Muntu oonse ujisi mulimo kubuleya ooko nkwaangulukide kuliiba akusumpula buntu bwakwe.

Mukubelesya lwaanguluko anguzu zyapedwe, muntu oonse ulaangulukide kulikkalila kwakutaindilizya ku lwaanguluko ndwapedwe amulawo kutegwa awalo kalemeka lwaanguluko lwa bantu bambi alimwi abulemu buyandika kumuntu alimwi akuliiba kwa bana maleya.

Lwaanguluko alimwi akuliiba takweelede kwiindilizyigwa ku mizeezo yakabambwa ambunga ya masi oonse aamunyika ya United Nations.

Kapango 30

Kunyina cili mucizuminano eeci ceelede kwendelezyegwa amasi aambi, mbunga ya bantu antela muntu biyo, kuba anguzu zyakucita zyilengwa zyimbi zyikonzya kutyola milawo ya lwaanguluko lupedwe ku bantu lwapandulwa kale.

redpajama_set_name: RedPajamaGithub