VANCOUVER, March 2, 2017 /CNW/ - Hannan Metals Limited ("Hannan" or the "Company") (TSX.V: HAN) is pleased to provide an exploration update and an outline of upcoming work programs for the Company's zinc projects in Ireland. Following Hannan's recent listing on the TSX Venture Exchange ("TSXV"), and the closing of a C$1.5 million financing, the Company is well positioned to commence exploration.
The Company's flagship project, Kilbricken, is drilled over more than 1.5 kilometres of strike length with better drill intersections including DH46: 20.5m @ 7.5% Zn, 9.9% Pb, 74.6g/t Ag; and DH06: 21.3m @ 11.0% Zn, 4.8% Pb, 94.4g/t Ag. The Kilbricken area provides excellent potential for new discoveries, as it lies upon a 40-kilometre long structural trend 100% owned by Hannan, that includes the Milltown prospect, where drilling results included DH19: 13.3m @ 10.5% Zn, 5.8% Pb.
Mr Hudson, CEO and Chairman states, "Although Hannan only listed on the TSXV last month, we have hit the ground running with our first diamond drill program planned to commence during April. Hannan owns one of the few high-grade, zinc-rich, massive sulphide discoveries made over the last decade, with the advantage of being in Ireland, one of the world's premier exploration and mining zinc terrains. Our challenge is now to expand on the very strong start we have been afforded and we look forward to building a sustainable business in Ireland by defining a large and long-life asset at Kilbricken. The Hannan team has been busy compiling and interpreting the tens of millions of dollars of proprietary data we purchased with the project, placing us in an excellent position to identify new drill targets to extend the known mineralized zone."
Diamond drilling from April 2017 at Kilbricken, with permitting for that program now underway. The early part of the program (3 holes for 1,500m) will focus on extracting metallurgical samples and expanding the footprint of the known mineralization beyond the current 1,500 metres strike length (Figure 1). The second stage of the drill program (10 holes for 5,000m) will test semi-regional targets within 1 to 2 kilometres from the Kilbricken project. The third stage will focus on testing regional structural targets that may host additional mineralized bodies.
Delivery of an initial resource and accompanying NI43-101 report for the Kilbricken project by independent resource evaluation geologists. This work is ongoing and planned for completion during Q2 2017.
A gap analysis of prior mineralogical and metallurgical test work and plan for future metallurgical studies. Dr Kurt Forrester will lead this study and has been appointed as Process Development Advisor. Dr Forrester is a Chartered Chemical Engineer (CEng MIChemE) and Chartered Professional Metallurgist (MAusIMM CP (Metallurgy)).
Other field based activities including soil sampling, paleo-dating and field mapping.
Later in 2017, the Company plans to collect additional 2D seismic data, commencing with a 25 kilometre regional line across the Company's 32,223 hectare prospecting licences followed by infill 2D seismic lines along the Kilbricken structural trend.
Since acquiring the project in September 2016, Hannan has focussed on advancing the technical understanding of the Kilbricken project to develop a rigorous geological model to guide future exploration. The Company has engaged a specialist group of geological experts in rift tectonics, structural geology of Irish Zn-Pb deposits and local geology of the project area to re-interpret the structural controls on mineralization at Kilbricken, and the regional structures that controlled development of the Clare rift basin and subsequent Zn-Pb mineralization. In addition, 28-line kilometres of 2D seismic and four square kilometres of 3D seismic data have been re-processed; three airborne magnetic data surveys have been "de-cultured" and had spectral depth filtering applied; gravity data has been reprocessed; and >30,000 soil samples have been re-levelled and combined with geophysical data to define drill targets.
Hannan has also commenced a formal technical collaboration with iCRAG at the University College Dublin, an EU and industry funded research centre with experts in Irish mineral deposits.
A NI 43-101 Technical Report for the Clare Project, dated December 23, 2016, is available on the Company's profile on SEDAR at www.sedar.com or directly from the Company's website. The Technical Report was authored by Dr. John Colthurst, PGeo, EurGeol, who is an independent "qualified person" as defined by National Instrument 43-101.
Certain information set forth in this news release contains "forward-looking statements" and "forward- looking information" under applicable securities laws. Except for statements of historical fact, certain information contained herein constitutes forward-looking statements, which include the Company's expectations regarding future performance based on current results, expected cash costs based on the Company's current internal expectations, estimates, projections, assumptions and beliefs, which may prove to be incorrect. These statements are not guarantees of future performance and undue reliance should not be placed on them. Such forward-looking statements necessarily involve known and unknown risks and uncertainties, which may cause the Company's actual performance and financial results in future periods to differ materially from any projects of future performance or results expressed or implied by such forward-looking statement. These risks and uncertainties include, but are not limited to, timing of permitting, commencement and successful completion of planned drill programs, timing of delivery of an initial resource calculation, liabilities inherent in mine development and production, geological risks, the financial markets generally, and the ability of the Company to raise additional capital to fund future operations. There can be no assurance that forward-looking statements will prove to be accurate, and actual results and future events could differ materially from those anticipated in such statements. The Company undertakes no obligation to update forward-looking statements if circumstances or management's estimates or opinions should change except as required by applicable securities laws. The reader is cautioned not to place undue reliance on forward-looking statements.


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redpajama_set_name: RedPajamaCommonCrawl


Since it is my first message, please let me introduce myself. I am a medical doctor who recently crashes his hdd (probably after using an "optimising" tool under windows 7). I love (and hate) computers since 30 years (you know: commodore 64, Amiga, i386, windows 3.10, etc...).
Internal WD7500BPVT "scorpio" SATA disk had a boot error either, probably after intempestive reboots.
Creating a Windows 7 DVD after having downloaded the official iso from microsoft also failed.
I bought a USB2-SATA interface and connected it to a Sony Vaio VPCEB3L1E (sic!). Windows considered my disk unreadable and suggested I format it (which I did not!).
At that time, I discover TESTDISK.
A was please to see 3 partitions PQSERVICE, SYSTEM RESERVED, and ACER, the one I woud like to restore.
Then I heard about DDRESCUE. I therefore installed ubuntu on another partition of the above cited VAIO and started to use the soft in order to make an image. The problem was that the transfer rate was about 10 to 30 Kb (not Mb) per second, so that my 750 Gb would not have been backed up even after a year of work.
Ok, I guess that's enough for a first post.
My question is: "should I try to change the number of bytes per sector"?
4096 Bytes sectors are a little bit difficult to handle.
It's a new standard and should improve memory management, because it would decrease the amount of sectors to manage.
Otherwise it can bypass the 2 TB limit of Intel-MBR and increase it up to 16 TB, because one sector is 8 times as big.
But there is a certain problems about Intel MBR and 4096 Bytes sectors.
Problems are booting and some other related stuff.
If you'd like to boot, the BIOS simulates the sector size as 512 Bytes.
In this case you're limited to 2 TB again.
For example as an external USB device sector size is not changed and will cause a message that's 4096.
So there is nothing to do.
Determining your sector size you can use the TestDisk log.
At your Disk selection the sector size is available.
Manufacturer often offer an advanced format tool for 4096 Bytes sector size disks.
Some things about partitions found by TestDisk.
TestDisk using Quick Search always is setting up the first partition as bootable.
You can watch it that your first partition has a star at the left side.
Star always means bootable activ, P is primary only and L for logical partitions.
A logical partition requires a container which is the extended partition to manage all local partitions.
It also a bypasses that an Intel-MBR disk can contain more than 4 primary partitions.
TestDisk recognizes the structur of your logical disk and is setting up the extended partition automatically.
Logically partitions requires some small additional space.
Otherwise a logical partition wouldn't fit.
TestDisk after Quick Search displays your first partition as activ and bootable.
It's a partition created from your computer manufacturer and has another partition type as PQService.
It's intended that windows doesn't recognize it and will use it.
Your second partition "System Reserved" is a normal NTFS partition used by Win7, but without driveletter, so you can't change anything either.
It's intended for using bootrec and encryption bitlocker.
This is your boot partition and should be set to * star as active partition, where you boot from.
Acer is your normal OS-partition and is only P for primary, because you boot from your system reserved partition.
A disk always can contain one active partition.
To get an overview about your current partition table you can use TestDisk and the menu Analyse.
<Analyse displays your current partition table just as it is.
Thank you for your quick and detailled answer.
For sure, I'll get more info about 4096 sectors.
Is there a way to correct the drive (bad sectors), without spending months.
Could a reformating followed by a chkdsk be useful, prior to using an undelete program able to found files on a reformated drive (which soft do you recommand?).
I didn' try to change the sector size, since it is probably correct (I checked that my Acer computer proposed NTFS 4096 as a standard format for HDD...).
I Tried again to do an image with ddrescue, but it should take months... even with the newest options from version 1.16.
Do you I would be able to recover most files by myself in a reasonable amount of time or I should give and send the HDD to a recovery company?
How did you try to improve boot sectors?
Because, now all partitions are listed as invalid boot.
-Not to change anything to your disk.
- You mentioned, testdisk doesn't list all directories?
Please let me know, what's lacking?
TestDisk is only used by arrow and page up and down keys.
To enter a folder, you can use the right arrow key.
Normally, testdisk copy speed should be ok.
It should keep your directories and file names.
-What kind of win7 version do you use?
To get full support of 4 k sector size, you shoul use win7 servicepack 1.
In case it should be also possible to create a disk containing win7 and servicepack 1.
It's only intended to exclude problems related to bad sectors.
In your case, there should be only a necessity to send your disk to a labor, if your disk has a physically or electronically defect.
Another datarecovery software would be, if you're not satisfy with PhotoRec, scavenger or restorer ultomate to test the trial first.
But only if there is a necessity to, and you can't fix your problems using TestDisk.


text:
Q: Query related to my encryption so i have a login system and i have used some security measures to make it secure.
Firstly i salt my passwords:
$salt = openssl_random_pseudo_bytes(1024);
file_put_contents("salt.txt", $salt);

Next i hash it using the whirlpool algorithm:
function myhash($password){
    $salt = file_get_contents("private/salt.txt");
    $password = hash_hmac('whirlpool',$password,$salt);
    return $password;
}

This is an example of the password that would get returned and stored in the Database:
56a8cf545750eec78cb58582829636b1e0378cf0fff4982305a7171f06593fb92735d3576f0ad7ba8aec40c914abc38424885cb7ac2672b1d8da36e3b95c80ce

Now my question:
If a hacker was able to recover that long string above, would they be able to somehow reverse/decrypt it to return them the actual password. Let me know what you guys think/know, is it impossible?
This is not a thread for people to suggest other things to me, please keep answers strictly related to the single question.

A: One area of attack seems to be that two same passwords result in the same string, because you use the same salt for everyone.
So without decrypting anything, they can already tell who has the same password. That probably indicates weak passwords, and they can start brute-forcing there.

A: Short answer "NO". whirlpool is fairly strong hashing algorithm (not encryption algorithm as encryption assumes ability to decrypt in some way). Salt (AKA shared key) just makes is even stronger. But having the same salt for everyone does not make it much weaker but makes it possible to find out who has the same password (without knowing the password itself).
Better use of salt is that it is randomly generated before use in hash function (and it does not need to be 1024 bytes - 8 bytes is more than enough for salt) and then prepended to resulting hash. This way function which will check the password knows which salt must be used and what hash is expected.
Whirlpool algorithm has no known weaknesses and uses 512 bit. Therefore it is regarded as secure. However I personally have two negative views on it:

*

*It underwent two modifications from its inception in 2000

*It is less used than other algorithms (namely SHA512).

So my personal view is that nothing wrong with your code and it is quite secure. But you may be better off switching to SHA512.
Only way to recover password from that long string is brute force for VERY LONG TIME (if password is strong of course) or may be using some technology from NSA :)

redpajama_set_name: RedPajamaStackExchange


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My boyfriend gets really bad heartburn and he took this brand and he said it helps a lot. He takes one in the morning and one at night. It works really well for him. It the only brand he will use.
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News Criminal: Obama Vows Veto on House Punishment of Sanctuary Cities
Criminal: Obama Vows Veto on House Punishment of Sanctuary Cities
The Republican-led House of Representatives passed a bill on Thursday that would punish sanctuary cities and Barack Obama has threatened a veto should it end up on his desk.
WASHINGTON—The Republican-controlled House Thursday passed legislation that would withhold federal law-enforcement grants from cities that shelter illegal immigrants from federal authorities, part of a campaign to punish what are known as sanctuary cities.
The bill, passed 241-179, is the GOP's answer to the shooting this month of Kathryn Steinle, 32 years old, on a San Francisco pier, allegedly by an illegal immigrant who had been convicted of seven felonies and previously deported to Mexico.
The Associated Press provided the lame excuse from the Obama administration that the bill would "lead to mistrust between local communities and law enforcement agencies" and, therefore, he would veto the bill.
Jim Steinle, Kathryn Steinle's father, testified before a Senate committee last Tuesday and told them, "Due to disjointed law and basic incompetence on many levels, the U.S. has suffered a self-inflicted wound by the hand of a person who never should have been on the streets of this country."
Leo Hohmann reported:
Rep. Steve King, R-Iowa, said President Obama relaxed the rules on ICE detainers, making it optional instead of mandatory for cities to comply. This opened the door for the ACLU to file lawsuits on behalf of illegal aliens, he said.
An ICE detainer is a written request that a local jail or other law enforcement agency detain an individual for an additional 48 hours (excluding weekends and holidays) after his or her release date in order to provide ICE agents extra time to decide whether to take the individual into federal custody for removal purposes.
"ICE detainers are not mandatory as a matter of law. So this is not initiated by ICE, they're reacting to the threat of litigation by the ACLU, and by changing the word 'shall' in these detainer orders," King said. "I think we've clearly heard today the effect of that, and we've heard it from expert testimony and from very painful experience."
The painful experience was that of Jim Steinle, father Kate Steinle, 32, who died at the hands of an illegal alien July 1 who had a string of prior arrests. "This will make you cry too, and it happens every day. This story happens every day in the U.S.," King said.
King also said that in 2011 along, 48,000 crimes were committed by illegal aliens against US citizens and that 30,000 were arrested and released in 2014.
The author of the bill, Rep. Duncan D. Hunter (R-CA) said, "The American people have the right to not give their tax dollars to municipalities and states that do not follow federal law. The fact that San Francisco and L.A. and other cities disagree with the politics of federal enforcement does not give them a free pass to subvert the law."
While Democrats have charged that the measure is "anti-immigrant," they fail to distinguish between those who come into our country legally and those that don't. Rep. Mike Coffman (R-CO), whose represents a district that is made up of twenty percent Hispanic, says the bill is neither "anti-immigrant" nor "anti-Hispanic." Rather it should be seen as "pro-law enforcement."
While Republicans view the passing of the bill as a victory, Democrats claim that it is pandering to people who agree with the statements of Donald Trump concerning illegal aliens. While one does not know the motives of Republicans in the matter, it seems to have been a push to actually attempt to move in the right direction of dealing with the issue of illegal aliens and sanctuary cities, not to be confused with the Bible's cities of refuge.
This isn't the only bill that is attempting to deal with the issue of sanctuary cities.
On Saturday, Suzanne Hamner reported on another bill in the Senate to deal with the issue.
"Sen. Jeff Sessions (R-AL) and Sen. Ron Johnson (R-WI) joined forces to initiate the 'Protecting American Lives Act' or S. 1842 that would end sanctuary cities and 'severely punish any illegal aliens who illegally re-enter the United States after previous deportation,' she wrote. "It sounds great; however, it would require catching the sneaky snakes as they cross the Obama 'welcome mat' on the open southern border."
And that is the issue, isn't it? After all, this administration orchestrated the illegal alien invasion in 2014 of tens of thousands of illegals and sought to bring more into the country by airplane at taxpayer expense. This year the administration has brought tens of thousands of Muslims from Syria into the US without proper vetting and colonizing them in US cities. All of this and then the administration continues to release thousands of convicted illegal alien criminals back onto American streets.
He doesn't follow immigration laws. In fact, Barack Obama doesn't follow the law at all. Again, it's not incompetence, it's purposeful.
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WINDHOEK, 24 SEP (NAMPA) – The Namibian Standard Institution (NSI)'s Chief Executive Officer Riundja Ali Kaakunga says people are becoming more sensitive to what they consume.
Speaking in the capital on Tuesday at the official opening of a two-day seminar on the ISO 22000 standard developed by the International Organisation for Standardisation (ISO), Kaakunga said food safety has become a global issue and producers are required to deliver safe products in order to avoid loss of lives and to minimise production costs.
The ISO 22000 international standard specifies the requirements for a food safety management system.
"In order to achieve the delivery of safe food products, ISO has develop a standard called the ISO 22000 FSMS (Food Safety Management System), and that is why you are all here today," he said while addressing the seminar.
He called on the participants to, during the seminar, get to grips with the benefits of implementing a food safety management system according to the ISO 22000 standard and equip themselves with the necessary skills.
Kaakunga indicated that this is the third seminar on ISO 22000 to be held in Namibia.
The first awareness raising seminar in this regard was held in Windhoek on 15 and 16 March 2010, while the second seminar took place in Walvis Bay from 19 to 23 August this year.
The main objective of the workshop is to support the dissemination of information on the ISO 22000 standard and help organisations operating in the food chain to understand the benefits of implementing a food safety management system according to the standard, as well as informing them about modern techniques in food safety management.
About 50 representatives of various sectors of the food industry such as restaurants, franchises, hotels, breweries, dairies, and the City of Windhoek, among others, are attending the seminar.


text:
Home / News / First red squirrel documented in Nome
First red squirrel documented in Nome
Diana Haecker
When young Jack James looked out the window of his home at Anvil Mountain on June 7, he saw a red squirrel.
It's quite remarkable that Jack recognized it as such, as the species doesn't exactly live here, on Nome's tundra.
"Mom, there is a squirrel on the deck," he said to his mother Donna James. She took her phone, snapped a few photos and the family marveled at the unusual sight of the squirrel. "It just sat there," Donna James said. But after it left the deck, it remained elusive and hasn't been seen anymore.
The photographs documenting the squirrel, and identifying it without a shadow of a doubt as a red squirrel, give it the distinction as "the first documented occurrence of a red squirrel on the Seward Peninsula and the westernmost record in North America," according to Link Olson, Curator of Mammals at the University of Alaska Museum in Fairbanks.
Photos of the squirrel made it to his desk and he confirmed that the animal is indeed a red squirrel.
Anecdotal reports exist of red squirrels in Council and of one red squirrel that was seen hiding in the rocks of the Nome seawall years back. But James' photos put the squirrel literally on the map of documented sightings and proof that it was here.
Olson said red squirrels are mostly associated with subsisting on spruce cones and depending on trees. But they also eat fungi, bird eggs, baby birds and even baby snowshoe hares, Olson said. Asked if the squirrel just got lost or if their range is extending, Olson said that ranges are dynamic and change and that animals are also experimenting with finding new territory. "They do disperse farther than we think," he said. Asked if this occurrence of a new species can be linked to climate change as warming encourages vigorous shrub growth and the tree line to march west and northward, he said, "I would not jump to the conclusion that this has anything to do with climate change."


text:
\section{Introduction}
The general astrometric principle of Gaia is similar to that of
Hipparcos. It scans the sky with a pre-defined scanning law measuring
the relative positions of objects. However, the two missions are
fundamentally different in various ways, one of the most relevant
being that Gaia goes much deeper, namely to about $G$\,=\,20
rather than $H_p$\,=\,12.4 as with Hipparcos.  Thus whereas
Hipparcos had an input catalogue, Gaia performs real-time onboard
detection. Consequently, we generally have very little prior
information about the targets which Gaia observes.

For this reason, Gaia is equipped with multiband CCD photometry in
order to characterize its targets.  As described elsewhere
in these proceedings, this consists of 4--6 broad band filters in the
Astrometric instrument, and around 12 medium band filters in the
Spectroscopic instrument.

The main scientific goal of Gaia is to study the composition, origin
and evolution of our Galaxy. Its main contribution to this topic is
establishing very accurate stellar distances and 2D (or 3D) space motions,
enabling us to study the 3D spatial structure and 3D kinematic phase
space of different types of stars in the Galaxy. However, such
information is of limited use if it cannot be associated with the
intrinsic physical properties of these stars, in particular their
abundances, masses and ages (or evolutionary state).  Hence Gaia is
not ``just'' about producing a catalogue of highly accurate
astrometry and multiband photometry on hundreds of millions of stars.
An integral part of the mission and data processing is to add
essential scientific value to these by providing fundamental physical
information on the targets.  The challenge is
to design a classification system -- and develop appropriate
algorithms -- which can take the heterogeneous Gaia data and extract
reliable estimations of the classes of objects and their
physical parameters.  This article gives a brief outline of the goals,
requirements and issues facing this work.

\section{Overall requirements and\\available data}

The main objectives of the classification are as follows
\vspace*{-2ex}
\begin{description}
\item[Discrete Source Classification]Determination of whether an object is a star, galaxy, quasar or asteroid
etc. This could also include the use of morphological information.
\item[Estimation of Astrophysical Parameters (APs)]For those objects identified as stars, determine their intrinsic
physical properties. The relevant (and obtainable) ones are effective
temperature, ${\rm T}_{\rm eff}$, surface gravity, $\log g$, metallicity, [Fe/H], and
line-of-sight interstellar extinction, A$_{\rm V}$. Although this last one is
of course not intrinsic to the star, we would ideally determine it on
a star-by-star basis, so we can consider it as such.
Other APs of interest (and which could be determined for bright stars
with the spectroscopy from the RVS instrument) include: alpha-process
elements, [$\alpha$/Fe], CNO abundance anomalies, the microturbulence
velocity, rotational velocity  and activity.
\item[Identification of unresolved binaries]Most stars are in multiple systems. Some of these can be recognised
from the astrometry, and a few will be visual binaries, but most will
go undetected in this way. Nonetheless, with favourable brightness
ratios, a binary could be detected from the shape of its composite
spectral energy distribution. This is important for determining the
stellar mass function (as opposed to the system mass function) and for
investigating the evolution of stellar clusters.
\item[Identification of new types of objects]The history of astronomical discovery shows that new instruments,
surveys and data analysis techniques lead to new, unexpected
discoveries.  Thus with Gaia we must be open to the prospect of
detecting new types of objects (summarized by the cliche ``expect the
unexpected''.) This includes new types of variable stars, rare stars
(e.g.\ brief phases of stellar evolution), abnormal abundance patterns
or multiple systems. Those supervised classification methods which are
commonly used for determining stellar parameters from spectra are
generally forced to classify new types of objects into pre-existing
classes. New objects would therefore go undetected (and samples of
known types of objects would be contaminated). Thus special attention,
including the use of unsupervised methods, is required to deal with
this.
\end{description}

These classification tasks must rely mostly on the photometric data,
as only these extend to the magnitude limit of Gaia's onboard
detection and thus astrometry. But recall that the photometry is
obtained in two separate instruments, BBP and MBP.  Only the former is
obtained at the same spatial resolution as the astrometric data. Thus
in sufficiently crowded fields we will only have BBP data, that is
between 4 and 6 broad photometric bands.\footnote{We may still have
the MBP data -- if it is deemed worth transmitting to the ground --
but only then of composite objects. This might be
useable.} For bright stars, say brighter than $V=15$, we will also have
reasonable quality RVS spectra, which will add considerable
information, in particular on detailed abundances, peculiarities,
rapid rotation and so forth. Finally, the parallaxes will of course
also be valuable, as discussed in the next section.

\section{Stellar astrophysical parameter estimation}

The most fundamental properties of a star are its mass, age and
chemical composition.  Of course, age is not directly observable and
masses can only be determined directly (i.e.\ dynamically) in select
binary systems.  Thus we must rely on indirect atmospheric indicators
which can be obtained from the spectral energy distribution (SED).
In particular, we are interested in the effective temperature, ${\rm T}_{\rm eff}$,
surface gravity, $\log g$\ and the iron-peak metallicity, [Fe/H].  Combined
with the parallax and interstellar extinction, the luminosity, radius
and mass can be determined.

\begin{table*}[t]
\begin{center}
\begin{minipage}{12cm}
\begin{tabular}{llll}
\hline
\multicolumn{4}{l}{{\it non-astrometric parametrizer:}} \\
nSED, (RVS)	& $\Rightarrow$	& ${\rm T}_{\rm eff}$, $\log g$, [Fe/H], & \\
	& 	&  {\bf A}($\lambda)$, BC, [$\alpha$/Fe] ?	& atmospheric model 	\\
\\
\multicolumn{4}{l}{{\it additional use of astrometry gives:}} \\
SED, BC, $\pi$, {\bf A}($\lambda)$\	& $\Rightarrow$	& L	& $2.5\log L - f(\rm{SED,BC})$\\
&&& \hspace*{1em}$= A - 5\log{\pi}$ \\
L, ${\rm T}_{\rm eff}$\	& $\Rightarrow$	& R	& $L = 4 \pi R^2 \sigma T_{\rm eff}^4$ \\
$\log g$, R	& $\Rightarrow$	& M	& $g=GM/R^2$	\\
\\
SED, RVS, {\bf v}(t), {\bf r}(t)	& $\Rightarrow$	& detect unresolved binaries	& orbital model \\
SED(t), RVS(t)	 		& $\Rightarrow$	& detect variables		& variability model \\
\hline
\end{tabular}
\caption[]{Stellar parameters derivable from the Gaia data.
SED=spectral energy distribution (ca.\ 15 photometric measures in medium
and broad band filters); nSED=normalized SED (absolute flux
information removed); RVS=radial velocity spectrum; BC=bolometric
correction; $\pi$=parallax; {\bf A}($\lambda)$=interstellar extinction
function; {\bf v}(t) \& {\bf r}(t)=point source velocity and position as a
function of time (from c.\ 85 observations over five years).}
\label{parameters}
\end{minipage}
\end{center}
\end{table*}

Most work on stellar parametrization has relied on relatively high resolution
spectra from which ${\rm T}_{\rm eff}$, $\log g$\ and [Fe/H]\ have been determined. Gaia
is rather different in that it observes at lower spectral resolution
but measures absolute fluxes as well as parallaxes.
Table~\ref{parameters} shows how stellar parameters can in principle
be derived from these data.  The distance measurement accuracy for
V\,=\,15 is 1\% at 1\,kpc and 5\% at 5\,kpc. At V\,=\,18 these are
about 4\% and 20\% respectively. (These improve by a factor of two or
more for late-type or very reddened stars.) Thus some 20 million stars
will have their distances determined to better than 1\% and have high
precision SEDs. If ${\rm T}_{\rm eff}$\ can be established to 1\% then the radii of
many of these stars is determinable to within 2\%. If $\log g$\ can be measured to
0.2~dex, then provided R (radius) can be established to within 10\%, a mass
determination to within 50\% is possible without calibration from
binary systems. Although poor for an individual star, it becomes
statistically meaningful for a large sample of similar stars, which is
where Gaia's strength lies. Better individual masses will be possible
from calibration using the tens of thousands of visual binaries
observed by Gaia for which masses should be obtained to within 10\%
(and many thousands within 1\%). Individual ages (possibly with large
uncertainties) can be quantified from evolutionary models.

A proper treatment of interstellar extinction is very important.
Without accurate line-of-sight extinction measurements, the accurate
parallaxes and apparent magnitude measurements cannot be converted
into absolute magnitudes and thus intrinsic luminosities and radii.
For example, to determine the radius to 2\%, the extinction must be
measured to within 0.03 mags.

When trying to determine several astrometric parameters from a dataset
there exists the problem of parameter degeneracy, i.e.\ two different
astrophysical parameters manifesting themselves in the same way in the
SED in certain parts of the astrophysical parameter space. An example
is ${\rm T}_{\rm eff}$\ and extinction in late-type stars, where lowering ${\rm T}_{\rm eff}$\ has
a similar effect on the SED (at low resolution) as increasing the
extinction.\footnote{The radial velocity spectrum will help for the brighter
stars as this reddening-free information provides an independent
measure of the stellar parameters.} Clearly, for degenerate cases, a
parametrization algorithm is required which can give a range of
possible parameters, and not just a single set.

Most stellar systems consist of more than one component. Undetected
binaries bias the parameter determinations when the brightness ratio
is small (e.g.\ a higher luminosity for a given ${\rm T}_{\rm eff}$\ leads to an
erroneous [Fe/H]\ determination).  Many long period and/or distant
binaries will go undetected with the astrometry.  In these cases,
parametrization techniques are required which can identify binary
stars from their composite SEDs and ideally parametrize both
components.

\section{The approach to classification and regression}

Classification and parameter estimation is the problem of assigning
object classes or APs and generally involves determining some kind of
mapping from the data space to the parameter space
(Fig.~\ref{mapping}).\footnote{The {\it data space} refers to the data
acquired from Gaia, such as fluxes in different filters or the RVS
spectrum. The {\it parameter space} refers to those properties of the
sources we wish to determine, such as ${\rm T}_{\rm eff}$\ or extinction, but could
also refer to discrete classes (e.g.\ star, galaxy, quasar).}  A
frequently used approach is the {\it supervised} or pattern matching
approach, in which pre-classified data ({\it templates}) are used to
infer the desired mapping. This mapping is then applied to new data to
establish their classes or APs. Perhaps the most familiar such
technique is the minimum distance method (MDM), shown schematically in
Fig.~\ref{mdm}. This is a {\it local} template matching method, in
which only the properties of the local neighbours in the data space
influence the APs of the new object.  Here, we make a local fit of the
mapping function, or even just assign the APs of the nearest template
to the new object.

\begin{figure}[ht]
\begin{center}
\epsfxsize=0.45\textwidth \epsfbox{bailer-jones_b_f1.eps}
\end{center}
\caption{Classification or parametrization is the process of
determining the mapping from a data domain to a class or astrophysical
parameter (AP) domain. The opposite mapping is equivalent to the
simulation of the data, e.g.\ the emergent stellar spectral energy
distribution (SED).}
\label{mapping}
\end{figure}

\begin{figure}[t]
\begin{center}
\epsfxsize=0.35\textwidth \epsfbox{bailer-jones_b_f2a.eps}
\epsfxsize=0.40\textwidth \epsfbox{bailer-jones_b_f2b.eps}
\end{center}
\caption{Schematic illustration of the generic minimum distance method
(MDM). Top: a two-dimensional data space populated with pre-classified
templates.  Assigning parameters to a new object involves
looking at the APs of the nearest neighbours (with the data dimensions
suitably scaled).  APs are assigned either by interpolating in the
data space (i.e.\ solving the function APs\,=\,f\,(data) locally at the
new object -- in the simplest case this is just an average of one or
more neighbours) or in the parameter space (i.e.\ minimising the function
D\,=\,g\,(APs), shown for one AP in the bottom panel).}
\label{mdm}
\end{figure}

However, such local approaches quickly run into the well-known `curse
of dimensionality'.  As the dimensionality, $p$, of the data space
increases, the density of the templates decreases (for a fixed number
of templates).  For example, with MDM we may assign APs by averaging
the APs of those nearest neighbours selected such that they fill a
fraction $x$ of the entire data space around the new object. To do this
in $p$ dimensions, and if the templates were uniformly spaced, we
would have to include neighbours out to a fractional distance of order
$d = x^{(1/p)}$ in each data dimension.  With $x=0.01$ and $p=2$ this
gives $d=0.1$, i.e.\ templates out to 10\% of the full range of each
data dimension are included. But if we increase the number of data
dimensions (i.e.\ if we have more filters or more spectral bins),
to, say $p=10$, then we see that $d=0.63$. That is, the ``nearest''
neighbours now extend to 63\% of the entire range of each data
dimension. Such distant neighbours are likely to be completely
unrelated to the new object. The result is that we get a very large
bias in our AP estimation using local methods.  The only way to avoid
this is if we increase the number of templates exponentially with $p$,
but this quickly becomes inhibitive. If we simply shrink our
neighbourhood volume we may not have any neighbours at all, or, if we have
only one or two neighbours then we will get a large variance in the AP
estimate.\footnote{For more on the curse of dimensionality and the
bias--variance trade-off, see, for example, Hastie et al.\ 2001.}

A more sensible way of overcoming this problem is to either use
structured regression or a global regression approach.  In the former
we compensate for the lack of data at a local scale by making
assumptions about the shape or properties of the mapping function.
With global regression we also do this, but we furthermore use all of
the available data to form a single regression over the entire data.
Examples of this include neural networks and support vector machines.

\begin{figure}[t]
\begin{center}
\epsfxsize=0.35\textwidth \epsfbox{bailer-jones_b_f3a.eps}
\epsfxsize=0.35\textwidth \epsfbox{bailer-jones_b_f3b.eps}
\end{center}
\caption{Schematic diagram of the functional relationship between a
one-dimensional data and a one-dimensional AP space showing
degeneracies. We see degeneracies, i.e.\ several AP solutions for a
single given data measurement (shown by the horizontal line).  The
dashed lines show the noise level, so that any of the four templates
in the top diagram consistent with this (shown with vertical lines)
are consistent with this measurement.  We cannot choose between them.
If we had a lower density template grid, we would even miss entire
parts of the AP space as solutions.}
\label{degeneracy}
\end{figure}

There are, however, additional issues.  Classification and AP
estimation is the process of mapping from the data space to the AP or
class space.  By contrast, simulation of source SEDs is the opposite
mapping, i.e.\ from the AP space to the data space.  The fomer mapping
which we are interested in determining is therefore an inverse
mapping.  This is generally non-unique. In other words, whereas a
given set of APs provides a unique SED, two sets of APs could produce
the same SED. This is compounded by the effects of noise. The larger
the photometric noise on a SED or set of flux measurements, the greater
the number of different possible sets of APs this could correspond to.

This is illustrated schematically in Fig.~\ref{degeneracy}. In the
top panel we see that there are four templates (those lying within
the noise bounds) which give rise to data consistent with the new
observation. Confronted with this degeneracy we must decide what to
do. Do we quote all results? Do we average the APs?  There are in fact
whole ranges of the AP which are consistent with the data, so an
unweighted average will be biased by the distribution of the nearest
templates.  Moreover, at large AP, there is actually another solution
which we have completely failed to recognise due to the low density of
templates in that region.  The problem is worse with a lower density
template grid (bottom panel), or, equivalently, lower noise
data. Clearly, a local method which just assigns the APs using the
nearest neighbours will give biased results.

But even with a global regression we have problems, as the function we
are trying to approximate may not be single valued, so the regression
could go very wrong where we have these degeneracies.  (Think of
rotating the top panel of Fig.~\ref{degeneracy} by 90$^{\circ}$ and
trying to fit a single-valued function through the templates.)

We may assess this by training a global model (in this case a neural
network) on simulated Gaia photometric data and then examining the
mapping it has learned. This is shown in Figs.~\ref{pred_teff}
and~\ref{pred_feh}. Projections of the true relationship
between the filter fluxes and the APs are shown as stars. Projections
of the mapping learned by the network are shown as triangles. Of course, the
network is learning the mapping in the inverse sense from the way it
is plotted (that is, given the fluxes in all filters, it predicts the
APs). Both plots are derived from the same network which had 15 inputs
(one per filter) and 3 inputs (one per AP). The training data grid
consisted of many thousands of spectra over a wide range of ${\rm T}_{\rm eff}$,
$\log g$\ and [Fe/H]\ combinations for stars of $G=15$ with simulated
end-of-mission photometry.

\begin{figure*}[t]
\begin{center}
\psfig{width=0.65\textwidth, angle=90, figure=bailer-jones_b_f4.ps}
\end{center}
\caption{Each panel shows show the photon counts in
a filter varies as a function of log\,${\rm T}_{\rm eff}$\ for stars with
$\log g$\,=\,4.0 and [Fe/H]\,=\,0.0 and zero extinction. The filter system
is the 1X BBP+MBP system, with each filter named according to the
first two digit of its central wavelength in nm. The trailing `B'
denotes a broad band (BBP) filter. The photon counts are normalized,
that is their sum across all filters for a star is the same for all stars.
The
stars show the simulated data (stellar spectra passed through
the Gaia instrument model) and the triangles the neural network
predictions.}
\label{pred_teff}
\end{figure*}

\begin{figure*}[t]
\begin{center}
\psfig{width=0.65\textwidth, angle=90, figure=bailer-jones_b_f5.ps}
\end{center}
\caption{Same as Fig.~\ref{pred_teff}, but now showing photon counts as a function of [Fe/H]\ for fixed ${\rm T}_{\rm eff}$\,=\,6000.}
\label{pred_feh}
\end{figure*}

Examining Fig.~\ref{pred_teff} we see that the network has done very
well in determining the ${\rm T}_{\rm eff}$\ mapping. It manages to reproduce most
of the small scale feature of the mappings. Only at the lowest
temperatures does it have problems. This is due at least in part to
the difficulty most regression models have at the boundaries of data
sets, which arises because the regression is essentially only constrained on
one side. In many of these one-dimensional cuts, the data to AP mapping
is not single valued. The fact that the neural network
can nonetheless produce the correct mapping shows that in this 15
dimensional data space the stellar data must lie on a lower
dimensional manifold which does not show any serious degeneracies (for
[Fe/H]\ and $\log g$\ fixed).  Fig.~\ref{pred_feh} shows the mapping as
a function of metallicity keeping ${\rm T}_{\rm eff}$\ and $\log g$\ fixed. We straight
away see that even though the true mapping is simpler, the neural
network has more problems reproducing it.  The reason for this can be seen when
we compare the vertical (photon count) scale of the two plots: the
variance in counts across the full range of [Fe/H]\ is much smaller than
the count variance across the full range of ${\rm T}_{\rm eff}$. Putting it another
way, [Fe/H]\ is a `weak' AP compared to ${\rm T}_{\rm eff}$, in that varying [Fe/H]\ by
X percent of its full range has a much smaller effect on the data
(SED) than does varying ${\rm T}_{\rm eff}$\ by the same amount. The effects of
[Fe/H]\ are subtler and therefore harder to extract from the dominant
effect of ${\rm T}_{\rm eff}$. This is compounded further by noise (which is small
here) and the effects of the other parameters.\footnote{$\log g$\ varies
in this data set, so the network had to try and learn its mapping
too. Adding additional parameters, in particular interstellar
extinction (which is a `strong' parameter), make this harder still.}

\section{Areas currently under\\investigation}

The task of designing the classification system for Gaia, and for
developing, testing and implementing the required algorithms, is the
task of the Gaia Classification Working Group.\footnote{also called
ICAP, for {\it Identification, Classification and Astrophysical
Parametrization}, for the slightly pedantic reason that
`classification' strictly only refers to placing objects into discrete
boxes.} A number of different tasks have been completed or have made
some progress. These can be found in detail on the working group web
site.\footnote{Currently http://www.mpia.de/GAIA/ although it can
always be found via the main Gaia website at ESA-ESTEC.} Here I just
provide a brief summary of the main tasks and provide the reference of
the relevant working group document (things like ICAP-CBJ-013). These
can be obtained from the ICAP web site or from Livelink.
\begin{itemize}
\item{Design and implementation of the overall classification system.
ICAP-CBJ-002/Bailer-Jones (2002), ICAP-CBJ-007, ICAP-CBJ-011.}
\item{A `blind testing' procedure to assess the performance of various
photometric systems and classification algorithms for performing
discrete classification and for estimating stellar
parameters. ICAP-AB-003 (collation of results), ICAP-PW-001 (detailed
analysis of MDM and neural network results for AP estimation),
ICAP-CH-001 (analysis of various statistical algorithms for discrete
classification and outlier detection).}
\item{Minimum distance and perturbation methods. ICAP-VM-001.}
\item{Identification and parametrization of unresolved binaries. ICAP-PW-003.}
\item{Design of the Gaia photometric systems by direct optimization using
evolutionary algorithms. ICAP-CBJ-013/Bailer-Jones (2004),
GAIA-CBJ-016.}
\item{The effect of CNO and $\alpha$ elements on the Gaia photometry.
ICAP-GT-002.}
\item{Stellar parameter uncertainty estimates using bootstrapping neural
networks. ICAP-PW-004.}
\item{Classification of QSOs and determination of their intrinsic parameters,
including photometric redshift. Claeskens et al.\ (these
proceedings).}
\end{itemize}
Several articles in the present proceedings describe some of these and
other classification issues in more detail. In particular see the
contributions by Bailer-Jones, Carrasco et al., Claeskens et al.,
Girard \& Soubiran, Maiz-Apellaniz, Malyuto, Picaud et al.,
Recio-Blanco et al., Willemsen et al. and Zwitter et al.

\section{Issues and future work}

Work on the classification system for Gaia is still in its early
days. Given the heterogeneity of the Gaia data, plus the enormous
range of objects and APs which it must deal with, classifying the Gaia
data is not a simple task of applying some black box classifier to the
entire data set. Some of the key issues which need to be addressed
are as follows.
\begin{enumerate}
\item{A proper handling of AP degeneracies.  If degeneracies cannot be
avoided in the photometric system (and they almost certainly cannot
be), then we must at least identify where they occur. Because we know
the forward mapping (data $\rightarrow$ APs) from stellar models, we
can in principle determine this. This information could be
used to perform a partition of the data space such that each partition
is handled by a separate regression model, free of degeneracies.}
\item{Coping with `weak' APs. Methods exist for boosting the sensitivity of
a regression model to weak APs, e.g.\ increasing their contribution in
the error minimization used to train the model (this is already used
in our neural network models). However, other approaches need to be
considered, such as iterative or hierarchical approaches in which
first the strong APs are determined and then the weaker ones given our
knowledge of the strong APs.}
\item{Dealing with systematic and correlated errors.
This is related to the issue of `strong' and `weak' APs.}
\item{Training and regularization of models. While global models have
some advantages over local ones, they are sensitive to the
distribution (across APs) of the training data. This can introduce
biases in the sense that it implicitly sets a prior probability on the
APs of new objects.}
\item{Combining heterogeneous data. For sufficiently bright objects we have
available two sets of photometric data (at different spatial
resolutions), spectroscopic data and a parallax. It needs to be
carefully considered how, from an algorithmic perspective, these data
should best be combined to yield a self-consistent set of APs for a
object. On the other hand, discrepancies could be important as they
could indicate peculiar objects. Not all objects can be treated the
same way. For example, the quality of the RVS data will vary
enormously, and the good estimates of the data uncertainties which we
can get from our instrument models should also be utilized.}
\item{Calibration. So far we have trained models and assessed performance
mostly using synthetic data, as this is the only source of data at the
required resolution and wavelength coverage (for simulating the Gaia
photometry) covering the required wide range of APs.  Determining
physical parameters is the ultimate goal, so at some level stellar
models and synthetic spectra must be used. But there will be
limitations if we rely only on synthetic data for training models. One
idea is to use a limited set of actual Gaia data of well-known stars
to calibrate the classification models, for example by adjusting the
training data. If insufficient well-known stars (with well determined APs)
exist in Gaia's catalogue, additional ground-based observations
will be necessary to better characterize them in a homogeneous way. Such
observing programs could and should start before the Gaia mission.}
\item{So far no attention has been paid to using morphological information, for
example to perform star/galaxy discrimination. This will be partly the
role of the onboard detection algorithms.}
\item{A number of issues have not yet been addressed, although work is
starting on them. These include: galaxy classification; asteroid
classification; classification of special types of stars (i.e.\ those
for which we do not have reliable synthetic spectra); dealing with
anomalous extinction. Finally, some kind of unsupervised
classification, or internal classification scheme, should be
investigated. Such approaches are independent of any physical models
or pre-defined classification scheme and allow us to look for natural
groupings within the data. This type of exploratory data analysis is
an important complement for discovering new types of objects.}
\end{enumerate}

redpajama_set_name: RedPajamaArXiv


likely to happen. The nice selection of local attractions, and so much to do will beyond doubt have you coming back persistently.
Gigantea Campground is to be found in the Central Sierra Nevada.
There's absolutely no way to run out of fun stuff to do near Gigantea Campground; scores of people enjoy coming here to get away.
of hard backcountry hiking on the Red Mountain Trail is time well expended. The 8-mile-from-start-to-finish Deep Creek Trail has a variation in height of 1,608 feet; it is a charming great outdoors hiking trail.
Outdoors recreation in the vicinity of Visalia-Porterville, California, the metro area neareast to Gigantea Campground. Find info on campgrounds, marinas, hiking trails, ski resorts, lakes, beaches, parks, whitewater, golf courses and more.


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Journeys End Vineyards' objective is to develop a strong, lasting and profitable relationship with many partners on a global basis, and consequently it seeks expressions of interest from parties who would like to develop export markets in their countries. Journeys End Vineyards wishes to develop realistic growth expectations and work with people who understand how to handle and care for wine. We would like to hear from export partners who are as passionate as we are about wine.
The name "Journeys End" and its assosciation with vineyards has its inception in a little known poem by C.P. Cavafy, simply titled "Ithaka." In this short but powerful work, Cavafy captures the essence of the Journey which life is, in all of its joys and dissappointments - or more exactly, the journey which we make of it. For as Cavafy so correctly points out - all of life's potentials begin within the human heart and their final culmination - the Journeys End - should be a time of celebration and reflection and never despair.
There are many similarites in the 'life' of a vineyard. Each year is a new journey with new expectations and hopes, new learning experiences and challenges. The journey from vine to bottle is a long and often anxious one, the ending of which marks the beginning of a new cycle, a new season. And just as each bottle in itself marks the end of another year, each Journeys End label also reflects a different aspect of that journey - from the careful preparation of new cuttings to the relief felt in picking the last bunch of the harvest and finally, the ecstatic escape to Maslin Beach. We hope that Cavafy's poem "Ithaka" offers you a similar inspiration as it did to us, and you find yourself returning to it often over a bottle of wine.
Arriving there is where you're destined for.
But don't hurry the journey at all.
Without her you wouldn't have set out.
And if you find her poor, Ithaka won't have fooled you.
you'll have understood by then what all these Ithakas mean.


text:
Alejandro César Alonso (Buenos Aires, Argentina, 3 de marzo de 1982), es un exfutbolista argentino. Jugaba de volante y su último equipo fue el AS Saint-Étienne de la Ligue 1 de Francia.

Selección nacional

Ha sido internacional con la Selección de fútbol de Argentina Sub-23.

Clubes

Palmarés

Campeonatos nacionales

Referencias

Enlaces externos

Futbolistas de la Ciudad de Buenos Aires
Futbolistas de las inferiores del Club Atlético Huracán
Futbolistas del Club Atlético Huracán
Futbolistas del Football Club des Girondins de Bordeaux
Futbolistas de la Association Sportive de Monaco Football Club
Futbolistas de la Association Sportive de Saint-Étienne

redpajama_set_name: RedPajamaWikipedia


Home → Latest Hud News → When should I target getting information to my accountant to begin the audit?
When should I target getting information to my accountant to begin the audit?
Get all audit work papers "audit ready" for your accountant by the first week of February as the Financial Statements need to be filed with REAC by March 31 or March 30 if in a leap year.


text:
PURC orders GWCL to reduce water tariffs by 10%
The order for the 10,08 reduction takes effect from September 16, 2018, a statement from PURC said.
The Public Utilities Regulatory Commission (PURC) has ordered the Ghana Water Company Limited (GWCL) to reduce tariff on the prevailing rates for all of its customers by 10.08%.
READ ALSO: Menzgold 'temporarily' halts gold vault business after SEC pressureMenzgold 'temporarily' halts gold vault business after SEC pressure
The GWCL has also been ordered to pay a total of GHS14,640,084.48 to all its customers for breaching Section 11 of the PURC Act 1997, (Act 538).
The statement, which was signed by the Executive Secretary of the PURC, Mami Dufie Ofori, indicated that monitoring exercises revealed that the GWCL refused to comply with regulatory directives concerning the Teshie Desalination plant.
The PURC said following the GWCL's agreement with Befesa to build, own, operate and transfer water purchase agreement, the Commission has since December 2015 included the contracted cost of the plant in its major tariff reviews.
The Commission holds that this was in breach of its acts and has therefore ordered a refund to customers.
"Between January and July 2018, the Commission undertook a number of measures aimed at giving GWCL a hearing and clarifying the tariff implications associated with GWCL's operational decisions in respect of the desalination plant. The Commission subsequently issued an enforcement notification which the company failed to comply with," sections of the PURC statement read.
READ ALSO: Collapsed Banks;
It said the reduction "represents the component of costs related to the desalination plant approved as part of the July 2018 water tariff decision."
The statement added that the GWCL will refund "an amount totalling GHS14,640,084.48 only to all its customers. The amount represents five months' tariff income unfairly over-recovered by GWCL between March 15, 2018, and September 15, 2018."


From August 11-20, 2014, you can download two free ebooks by KS Augustin.
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Quinten Tamlan was once the scourge of the Republic. Then he disappeared….
It's been seven long years for Quinten Tamlan. Scarred and bitter, he has lost direction and the spark of idealism that once fired his resolve. But when he is forced to take on a new crewmember, he is once more pulled back into a past that refuses to let go.
Quinten believes he has his own problems. He believes he is alone and forgotten. He is wrong. Quite wrong.
Another novel, and the first in the Perdition series, this book would appeal to fans of space opera, evil empires, redemption. This one isn't SFR but does have romantic elements.


text:
Intracom signs Romanian deal worth 11.8 mln euros
December 15, 2009 15.12.2009 • 08:00
Intracom Telecom has signed an 11.8-million-euro deal with Romania's Administration and Interior Ministry, it said yesterday. Intracom said its Romanian subsidiary, Intrarom, signed the agreement which will «provide an integrated system to maintain and distribute information for border control, national security and law enforcement both on a national and European Union level.» The project is scheduled for completion in 10 months, the Greek company said in a statement. Intracom Telecom, controlled by Russia's JSC Sitronics, has subsidiaries in 16 countries, including Bulgaria, Cyprus and Saudi Arabia. The company is 49 percent-owned by Intracom Holdings, whose shares are listed on the Athens bourse.
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