text:
Q: How to estimate the contribution of an individual to a software project? I work on a software project and would like to estimate the percentage out of the total contribution that I have put in the development of the software. Is there some tool doing this? Such a tool can be useful for appraisals or negotiations, for example. After all, we work for money (yes, not only money, put the point remains). I think there is enough hand-waving for the most important things.
The estimation is very subjective (at least to me now) but I do not know of any tool that provides even a subjective estimate. I know of Sloccount that spells out the total effort using the lines of code but not on per-developer basis.
My idea of an ideal tool for this purpose would:

*

*measure the complexity of the code (more complex is more effort, but more effort is not necessarily more contribution)

*measure the decomposibility/flexibility of the software (more decomposable is better)

*how much library code is used -- using library code speeds up the development process, increases the associated risk and requires the developer to know from before or learn about the library.

*be intelligent enough to differentiate between "who wrote the code", "who copied the code" and "who indented the code".

It is difficult to differentiate between the complexity in the implementation and the intrinsic complexity of the problem. Perhaps a comparison can be made with an equivalent open source counterpart if there is, or for each submodule separately.
If there is no such tool, is there no merit in having such a tool? Or do you believe in "I do work, I do not measure"? It takes time after all. Perhaps the project manager should do this estimation continuously, say, weekly. Are there any standards? Yes, standardization is difficult because every project has different goals, but perhaps that should mean there should be multiple standards, not no standards at all. This looks similar to the how a company is valued in the market.
Update: after seeing a few initial answers: It does not make sense to imagine a tool that just outputs the percentages. Are there tools that can help humans (particularly managers) in making better decisions? Or what is the sufficient statistic for making better decisions? Are these statistics available?

A: I really doubt there is any reliable trustworthy way of measuring individual's contribution to the solution. Sometimes rewriting some complicated legacy code that results in less lines of code, less complicated solution (smaller cyclomatic complexity etc.) can be seen as a quite significant contribution, while in other cases deleting valuable code covering edge cases that results in the same statistics (less lines of code, smaller CC etc.) is definitely something bad. It all comes down to people, trust and cooperation, individualism in the team is almost always wrong and I would rather avoid it and especially not use it as a motivation factor.

A: This is a research topic on its own. There are several tools that have tried to define metrics like code ownership. There are other approaches which tackle other aspect of collaborative development, for instance the trustability we can have in the code.
There has been also several studies that tried to use the information from bug trackers. For instance, to identify the developer that is the more likely to introduce bugs. But it's hard to be objective (A brilliant developer that is assigned the most critical part of the system, will still be more likely to introduce critical bugs).
It's actually hard to monetize the development tasks. What is the cost of a bug? What is the gain of refactoring? That would be however one way to estimate the contribution of a developer.
The last cool tool I saw of this kind was the Game Plugin for Hudson continuous integration system. A score is assigned to each developer according their actions

*

*-10 if they break the build

*-1 for breaking a test

*+1 for fixing a test

*etc.

That's again a way to somehow assess the contribution of the developer.
All in all, I do feel like what you are asking for exist, but is still very immature.

A: I don't think you can get a tool to evaluate your share of the project. Measuring lines of source is all very well, but what of the quality of that source? You wouldn't want someone taking the credit for 200 lines of source if the job could have been easiy done in 20...
Also, thinking of my employer for a moment, a lot of people contribute to the project in ways other than code. Immediate examples I can think of would be Project Managers and Testers - both of whom are essential, both of whom rightly deserve some credit.
Martin

A: The only thing that I could imagine would be a voting system. I have absolutely no idea, if that would work in your team or anywhere - but I'm sure, that you will need humans for any realistic estimation of code quality.

A: In Stroustrup's Book on C++ I've read once "Don't try to solve social problems with technical means".
Thinking progmatically, the attitude and the ability of a programmer could be very quickly estimated by making a code-review together and having a talk on relevant topics.

Thinking as an IT-enthusiast and as a control-freak, this shouldn't be very hard, to implement a teachable machine-learning software, which uses version-cotrol, bug-database, etc and greates real-time performanced data for each contributor. E.g. R, KNIME or WEKA  could be used for this.


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SLX4 (also known as BTBD12 and FANCP) is a protein involved in DNA repair, where it has important roles in the final steps of homologous recombination. Mutations in the gene are associated with the disease Fanconi anemia.

The version of SLX4 present in humans and other mammals acts as a sort of scaffold upon which other proteins form several different multiprotein complexes.  The SLX1-SLX4 complex acts as a Holliday junction resolvase.  As such, the complex cleaves the links between two homologous chromosomes that form during homologous recombination. This allows the two linked chromosomes to resolve into two unconnected double-strand DNA molecules.  The SLX4 interacting protein interacts with SLX4 in the DNA repair process, specifically in interstrand crosslink repair. SLX4 also associates with RAD1, RAD10 and SAW1 in the single-strand annealing pathway of homologous recombination. The DNA repair function of SLX4 is involved in sensitivity to proton beam radiation.

Model organisms
Model organisms have been prominent in the study of SLX4 function. It was identified in 2001 during a screen for lethal mutations in yeast cells lacking a functional copy of the Sgs1 protein.  Based on that, SLX4 was grouped with several other proteins produced by SLX (synthetic lethal of unknown function) genes.

A conditional knockout mouse line, called Slx4tm1a(EUCOMM)Wtsi was generated as part of the International Knockout Mouse Consortium program, a high-throughput mutagenesis project to generate and distribute animal models of disease to interested scientists.

Male and female animals underwent a standardized phenotypic screen to determine the effects of deletion. Twenty four tests were carried out on mutant mice and ten significant abnormalities were observed. A viability at weaning study found less homozygous mutant animals were present than predicted by Mendelian ratio. Homozygous mutant animals of both sexes were sub-fertile and homozygous females had a reduced body weight, body length, heart weight, platelet count and lean mass. Homozygotes of both sex had abnormal eye sizes, narrow eye openings, skeletal defects (including scoliosis and fusion of vertebrae), and displayed an increase in DNA instability as shown by a micronucleus test. This and further analysis revealed the mouse phenotype to model the human genetic illness, Fanconi anemia. The association was confirmed when patients with the disease were found to have mutations in their SLX4 gene.

References

External links

DNA repair
Genes mutated in mice

redpajama_set_name: RedPajamaWikipedia


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>>> developers, designers, tech writers, tool builders, and so on.
>> people were welcoming these changes, often eagerly.
> remotely "HTML5" -- because it's so uber cool.
> Henri's one line was sufficient to disregard what I wrote.
W3C.  Both change proposals were carefully read.
> introduced as some form of justification.
therefore seeking to favor proposals that create the weakest objections.
proposal that creates the weakest objections.
>> well be treated as new information.
> didn't feel was worth addressing directly.
I did read your proposal, and specifically was looking for objections.
anything else with the simple addition of a link)."
do you have new evidence to present that substantiates this assertion?
where (it is asserted) this element can be applied in the real world.
fail, seek to favor proposals that create the weakest objections.
>>> co-chairs picked among the arguments, as justification.
Reply: Tab Atkins Jr.: "Re: Working Group Decision on ISSUE-91: Removing the aside Element"


text:
import styled from 'styled-components'

import Img from '@/Img'
import css, { theme } from '@/utils/css'

export const Wrapper = styled.div`
  ${css.flexColumn()};
  overflow: hidden;
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  margin-right: 30px;
`
export const InfoWrapper = styled.div`
  margin-top: 6px;
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  margin-right: 15px;
`

export const ListsWrapper = styled.div`
  width: 80%px;
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  overflow-y: scroll;
  overflow-x: hidden;
`
export const UserLabel = styled.div`
  ${css.flex('align-center')};
  margin-right: 8px;
  &:hover {
    cursor: pointer;
  }
`
export const UserAvatar = styled(Img)`
  ${css.circle(24)};
  margin-right: 8px;
`
export const UserNickname = styled.div`
  color: ${theme('thread.articleDigest')};
  margin-top: -2px;
  ${UserLabel}:hover & {
    color: ${theme('banner.title')};
  }
`
export const MessageLinker = styled.a`
  color: ${theme('thread.articleTitle')};
  margin-top: 5px;
  &:hover {
    text-decoration: underline;
    color: ${theme('thread.articleTitle')};
  }
`

export const Message = styled.div`
  ${css.flexColumn()};
  padding: 10px 15px;
  position: relative;
  &:hover {
    background: #113744;
  }
`
export const MessageDivider = styled.div`
  border-bottom: 1px solid;
  border-bottom-color: ${theme('banner.desc')};
  width: 100%;
  opacity: 0.3;
`
export const MessageHeader = styled.div`
  ${css.flex()};
`
export const MessageBody = styled.div``
export const TitleHeader = styled.div`
  ${css.flex('align-center')};
`
export const TypeLabel = styled.div`
  color: ${theme('thread.articleDigest')};
  background: ${theme('mailBox.headHightBg')};
  font-size: 0.85rem;
  margin-right: 3px;
`
export const SourceTitle = styled.div`
  color: ${theme('thread.articleTitle')};
  ${css.cutRest('350px')};
  font-size: 0.9rem;
  &:hover {
    cursor: pointer;
  }
`
export const SourcePreview = styled.div`
  ${css.flex()};
  color: ${theme('thread.articleDigest')};
  font-size: 0.8rem;
  margin-top: 3px;
  margin-left: 20px;
  &:hover {
    cursor: pointer;
  }
`
export const PreviewBody = styled.div`
  flex-grow: 1;
  font-style: italic;
  ${css.cutRest('400px')};
`
export const AtLabel = styled.span`
  margin-left: 3px;
  font-style: normal;
`
export const FloorNum = styled.span`
  color: ${theme('comment.floor')};
  margin-right: 2px;
`

redpajama_set_name: RedPajamaGithub


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Is vehicle size a big deal when it comes to safety?
Monday, August 6, 2012 7:02:52 AM
Marcus Pickett
You may have heard that bigger vehicles are better when it comes to your safety during an auto accident. Crash tests and safety studies suggest that may be the case in many circumstances. However, that doesn't necessarily mean that your small car is a death trap. There are several interwoven factors that affect your safety -- and you auto insurance premiums.
The type of accident
All cars can get in accidents, no matter their size. SUVs are just as likely as subcompacts to hit patches of ice and run into other vehicles. The type of accident (single-vehicle, rollover or multivehicle) can make all the difference.
Actually, according to the Insurance Institute for Highway Safety (IIHS), larger vehicles like SUVs and pickup trucks may be more likely to get into rollover accidents because of their higher centers of gravity. In fact, because of the greater frequency of rollovers, pickups had overall higher death rates than smaller cars did in 2008 (87 passenger deaths per million registered passengers vs. 65 for cars).
But when it comes to multicar accidents, the size of your vehicle can play a huge role in determining fatality risk. In general, occupant deaths in multicar crashes are higher for small cars than they are for SUVs and pickups, according to IIHS. Small cars had the highest death rate in 2008 for multivehicle crashes (35 deaths per million registered passengers vs. 31 for pickups and 16 for SUVS). In other words, if a big car and a small car get in a serious accident, you'll want to be in the bigger one.
Across all accident types, SUVs fared the best at keeping their passengers alive. They had the lowest death rates for multivehicle, single-vehicle and rollover accidents, according to IIHS. Vehicle design may explain some of this discrepancy. SUVs are frequently designed with more advanced safety features, as they tend to be marketed as family vehicles.
Safety in size
Within each category analyzed by IIHS (cars, pickups and SUVs), there are different sizes, such as subcompact vs. sedan. When size (not accident type) is the only factor, size does seem to mean safety. The largest vehicles in the car category had half the death rate of the smallest, according to IIHS numbers. And, when it came to SUVs and pickups, the death rate decreased as size increased.
Can small be safe?
What if you're concerned about both your safety and fuel efficiency? Fortunately, improvements in technology are making small cars safer. According to a June 2011 news release from Allstate, 20 of the 29 small vehicles tested by IIHS for the 2011 and 2012 model years earned a "Top Safety Pick" designation.
To get this designation from IIHS, vehicles must perform well in crash tests that measure performance in front, side and rear collisions, as well as rollover accidents. According to Allstate, fuel-efficient models that got top marks included the 2011 Hyundai Elantra, the 2012 Ford Focus and the 2012 Honda Civic.
However, Edmunds.com cautions drivers that many crash test ratings reflect only how well a car performs when it collides with others in its class. So a small car with an impressive safety rating still would not be any match for a huge SUV.
Auto insurance implications
There is no direct connection between vehicle size and auto insurance premiums. Insurers take a multitude of factors into account, including your driving record, your age, your gender and the value of your car. However, safer cars can be less expensive to insure, with insurance companies offering discounts for auto safety features, from air bags to antilock brakes.
4 little driving failures with potentially big consequences
Linda Melone
Drivers in the U.S. fail to use their turn signals over 2 billion times each day, resulting in as many as 2 million crashes a year, according to a report from the Society of Automotive … Read More
Event data recorders: Is your car spying on you?
Chris Kissell
Today's cars are bursting with technological bells and whistles designed to improve your driving experience. But one high-tech feature has caused some controversy.
Event data … Read More
7 options for negotiating a price for a new car
Kathryn Hawkins
When you're shopping for a new car, it's easy to get caught up in the excitement and agree to a price that's higher than you should be paying. In fact, haggling … Read More
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redpajama_set_name: RedPajamaCommonCrawl


text:
\section*{REFERENCES}
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\defRoberto Trasarti--Battistoni{Roberto Trasarti--Battistoni}
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\begin{document}

\title{A global descriptor of spatial pattern interaction in the
galaxy distribution }

\author{
Martin Kerscher\altaffilmark{1,7},
Mar{\'\i} a Jes\'us Pons--Border{\'\i} a\altaffilmark{2},
Jens Schmalzing\altaffilmark{1,3},
Roberto Trasarti--Battistoni\altaffilmark{1,4},
Thomas Buchert\altaffilmark{1},
Vicent J. Mart{\'\i} nez\altaffilmark{5},
and Riccardo Valdarnini\altaffilmark{6} }
\altaffiltext{1}{Ludwig--Maximilians--Universit\"at, Theresienstra{\ss}e 37,
80333 M\"unchen, Germany}
\altaffiltext{2}{Departamento de F\'{\i}sica Te\'orica, Universidad
Aut\'onoma de Madrid, 28049 Cantoblanco, Madrid, Spain }
\altaffiltext{3}{Max--Planck--Institut f\"ur Astrophysik,
Karl--Schwarzschild--Stra{\ss}e 1, 85740 Garching, Germany}
\altaffiltext{4}{Sezione di Astrofisica \& Cosmologia, Dipartimento di
Fisica, Univerist\`a di Milano, via Celoria 16, 20133 Milano, Italy}
\altaffiltext{5}{Departament d'Astronomia i Astrof\'{\i}sica, Universitat de
Val\`encia, 46100 Burjassot, Val\`encia, Spain}
\altaffiltext{6}{SISSA, Via Beirut 2-4, 34014 Trieste, Italy}
\altaffiltext{7}{email kerscher@stat.physik.uni-muenchen.de}

\begin{abstract}
We present  the function $J$ as a   morphological descriptor for point
patterns formed by the distribution of galaxies in the Universe.  This
function  was recently introduced in  the field of spatial statistics,
and is  based  on  the  nearest  neighbor  distribution and   the void
probability  function.  The  $J$   descriptor  allows to   distinguish
clustered (i.e.\ correlated) from ``regular'' (i.e.\ anti--correlated)
point distributions.  We  outline  the theoretical foundations  of the
method, perform tests with a Mat\'ern  cluster process as an idealised
model of  galaxy clustering, and apply the  descriptor to galaxies and
loose    groups in  the    Perseus--Pisces Survey.   A comparison with
mock--samples extracted from a mixed dark matter simulation shows that
the $J$  descriptor can be profitably  used to constrain (in this case
reject) viable models of cosmic structure formation.
\end{abstract}

\keywords{methods: statistical; galaxies: clusters: general;
large--scale structure of universe}

\section{Introduction}

Three--dimensional  patterns formed by   the spatial  distribution  of
galaxies in the Universe have already been described and quantified by
various    methods:      correlation     functions,  counts--in--cells
{}\cite{peebles:principles},        the      void probability function
{}\cite{white:hierarchy},    the  genus  {}\cite{melott:review},   the
multifractal spectrum  {}\cite{martinez:clustering},     skewness  and
kurtosis  {}\cite{gaztanaga:bias},      and      Minkowski functionals
({}\pcite{mecke:robust},  {}\pcite{schmalzing:beyond}).  Some of these
descriptors are complementary and suggest a physical interpretation of
cosmic patterns   by  emphasising different  spatial  features  of the
galaxy distribution.

The treatment of the galaxy distribution as a realization of a spatial
point process promises   useful insights  through the  application  of
methods from   the  field  of   spatial statistics.    The forthcoming
three--dimensional galaxy   catalogues with more  than half  a million
redshifts additionally motivate  the  development of new   statistical
techniques.

In this article  we want to reinforce a  morphological measure for the
study of the distribution of galaxies, the $J(r)$--function, which has
recently  been  introduced into the    field of spatial statistics  by
{}\scite{vanlieshout:j}   and is  related   to   the nearest--neighbor
distribution  $G(r)$  and the  spherical  contact distribution $F(r)$.
Indeed,  the   $J(r)$--function  is equal   to   the first conditional
correlation       function              (\pcite{stratonovich:topicsI},
{}\pcite{white:hierarchy}), and was  used  by {}\scite{sharp:holes} to
test a  hierarchical ansatz for $n$--point  correlation functions.  We
will  focus on different features of  the $J(r)$--function showing its
discriminative power as a measure of the strength of clustering.

Our  article is organised  as  follows: In Sect.~\ref{sect:nearest} we
present the  distribution functions $F$ and  $G$ and show  how the $J$
function is constructed. A Mat\'ern cluster process is considered as a
simple example of a clustering point distribution.
In  Sect.~\ref{sect:galaxies} we study the  clustering properties of a
galaxy   sample and  of   galaxies   in   groups extracted  from   the
Perseus--Pisces redshift survey (PPS).
We   compare   the observed   galaxy   distribution with  mock samples
extracted  from  a    Mixed  Dark     Matter  (MDM)  simulation     in
Sect.~\ref{sect:nbody}.
We summarise and conclude in Sect.~\ref{sect:outlook}.

\section{The $J$ function}
\label{sect:nearest}

In the theory of spatial point processes the distribution of a point's
distance to its nearest neighbor is a common tool for the analysis of
point patterns {}\cite{stoyan:stochgeom}.   We  consider  the redshift
space coordinates $\{{\mathbf{x}}_{i}\}_{i=1}^{N}\in{{\rm I\kern-0.16em{}R}}^{3}$ of $N$ galaxies
inside  a region $D\subseteq{{\rm I\kern-0.16em{}R}}^3$  as  a realization  of the point
process  describing  the  spatial  distribution   of galaxies  in  the
Universe.

The nearest neighbor distribution $G(r)$ is the distribution function
of the distance $r$  of a point of   the process to the  nearest other
point of the process.
Similarly,  the  spherical  contact    distribution $F(r)$     is  the
distribution function of  the distance  $r$  of an  arbitrary point in
${{\rm I\kern-0.16em{}R}}^{3}$ to the nearest point of the process.
$F(r)$  is equal to  the  volume fraction  occupied by the  set of all
points in $D$ which  are closer than  $r$ to  a point of  the process.
Hence, $F(r)$ coincides with the volume density of the first Minkowski
functional   ({}\pcite{mecke:robust} and {}\pcite{kerscher:abell}) and
is related     to  the void   probability function     $P_{0}(r)$  via
$F(r)=1-P_{0}(r)$.

For a homogeneous Poisson process we have
\begin{equation}
\label{eq:vpf}
F_{\rm P}(r)=1-\exp\left(-\frac{4\pi}{3}{r^3}n\right)=G_{\rm P}(r) ,
\end{equation}
where $n$ is the number density.
Boundary--corrected   estimators  for   both  the    nearest  neighbor
distribution and  the   spherical contact  distribution  used  in  our
studies are   provided   by    minus  (reduced   sample)    estimators
({}\pcite{stoyan:stochgeom},          also       detailed           in
{}\pcite{kerscher:fluctuations}).

In a recent paper, {}\scite{vanlieshout:j} have suggested to use the
quotient
\begin{equation}
J(r) = \frac{1-G(r)}{1-F(r)}
\end{equation}
for characterising a point process; in that  way the surroundings of a
point belonging to the process and  the neighborhood of a random point
are compared.  They consider several point  process models and provide
limits     and       exact   results   on         $J(r)$   (see   also
Section~\ref{sect:matern}).

If  the process under consideration  is  clustered, an arbitrary point
usually lies farther away from a point of the process than in the case
of    a  Poisson  process.    Hence,   clustering   is   indicated  by
$F(r)<F_{\rm P}(r)$.  Consistently, $G(r)>G_{\rm P}(r)$,  since  clustered
points tend  to lie closer to their  nearest  neighbors than randomly
distributed points.  So, for a clustered point distribution, $J(r)<1$.

In case of  anti--correlated, ``regular'' structures  the situation is
the opposite: on average a point of a  regular process is farther away
from the nearest other point of the process, so $G(r)<G_{\rm P}(r)$, and
a  random point is  closer to  a  point of  the process,  resulting in
$F(r)>F_{\rm P}(r)$.    Therefore, regular structures   are indicated by
$J(r)>1$.

For a homogeneous Poisson process we obtain $J_{\rm P}(r)=1$, separating
regular from clustering structures.

\subsection{The Mat\'ern cluster process}
\label{sect:matern}

\begin{figure}
\begin{center}
\epsfxsize=8cm
\begin{minipage}{\epsfxsize}\epsffile{fig1.eps}\end{minipage}
\end{center}
\caption{
\label{fig:matern}
Sketch  of a two--dimensional  Mat\'ern  cluster process  with cluster
radius $R=1.5\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$ and mean number of clusters $\mu=5$.}
\end{figure}

Before attempting to  apply $J(r)$ to galaxy  samples, we want to test
it  on a model with  non--trivial yet analytically tractable behaviour
of $J(r)$.

In   order    to   describe     the      clustering    of    galaxies,
{}\scite{neyman:statistical} suggested a class of point processes that
was   subsequently named after   them.  We concentrate   on a subclass
called Mat\'ern cluster   processes.   They are constructed   by first
distributing   uniformly  $M$ cluster  centres.    Around each cluster
centre, which is itself not  included in the final point distribution,
$m$ galaxies are placed randomly within a  sphere of radius $R$, where
$m$ is a   Poisson distributed random variable with   mean  $\mu$.  In
Figure~\ref{fig:matern} we show a sketch of such a process.  Note that
overlapping clusters are allowed.

For  a Mat\'ern cluster  process, {}\scite{vanlieshout:j}  proved that
$J(r)$ is monotonically  decreasing from  1   at $r=0$ and attains   a
constant value for $r>2R$, where $R$ is the radius of a cluster.  This
constant  value  can  be   interpreted  as a   relic   of  the uniform
distribution of the cluster centres.
In three dimensions
\begin{equation} \label{eq:j_matern_1}
J_{\rm M}(r) = \left\{
\begin{array}{ll}
\frac{1}{{\rm Vol}(B_R)} \int_{B_R}{\rm e}^{-\mu V({\mathbf{x}},r,R)}{\rm d}^3x
& \mbox{for}~0{\leq}r{\leq}2R, \\
\exp(-\mu)  &\mbox{for}~r>2R,
\end{array} \right.
\end{equation}
where
\begin{equation}
V({\mathbf{x}},r,R) = \frac{{\rm Vol}(B_r({\mathbf{x}})\cap B_R)}{{\rm Vol}(B_R)}
\end{equation}
denotes the  ratio of the volume  of the intersection of  two balls to
the volume of a single ball.   Here $B_r({\mathbf{x}})$ is a ball of radius $r$
centred  at the  point ${\mathbf{x}}$,  while  $B_R$ is  a ball  of radius  $R$
centred at  the origin.   This quantity can  be calculated  from basic
geometric considerations, both  in two {}\cite{stoyan:fractals} and in
three dimensions, where the result is
\begin{equation}
V(x,r,R) = \left\{
\begin{array}{ll}
c_3x^3+c_1x+c_0+c_{-1}x^{-1}
& \mbox{for}~0{\leq}r{<}R~\mbox{and}~R-r{<}x{<}R, \\
& \mbox{or}~R{\leq}r{\leq}2R~\mbox{and}~r-R{<}x{<}r, \\
r^{3}/R^{3}
& \mbox{for}~0{\leq}r{<}R~\mbox{and}~0{\leq}x{\leq}R{-}r, \\
1
& \mbox{for}~R{\leq}r{\leq}2R~\mbox{and}~0{\leq}x{\leq}r{-}R.
\end{array} \right.
\end{equation}
with $x=|{\mathbf{x}}|$ and
\begin{equation}
\begin{array}{llll}
c_{3}  = \frac{1}{16 R^{3}}, &
c_{1}  = -\frac{3}{8} \big(\frac{r^{2}}{R^{3}} + \frac{1}{R}\big), &
c_{0}  = \frac{1}{2}  \big(\frac{r^{3}}{R^{3}} + 1\big), &
c_{-1} = \frac{3}{16} \big(\frac{2 r^2}{R} - \frac{r^4}{R^3} -  R\big) ,
\end{array}
\end{equation}

\begin{figure}
\begin{center}
\epsfxsize=8cm
\begin{minipage}{\epsfxsize}\epsffile{fig2.eps}\end{minipage}
\end{center}
\caption{
\label{fig:Jmatern}
In this panel we show $J_{\rm M}$ for Mat\'ern cluster processes with fixed
cluster radius $R=1.5\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$  and varying mean  number  of galaxies per
cluster  $\mu=1,3,10,30$  (bending   down successively).   The   areas
indicate 1--$\sigma$ fluctuations of 50 realizations.}
\end{figure}
In  Figure~\ref{fig:Jmatern} we show\footnote{Throughout this article,
distances  are  given in \ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi,  where $h$  denotes  the value  of the
Hubble  parameter   measured   in   units of  $100\frac{\ifmmode{{\rm km}/{\rm s}}\else{${\rm km}/{\rm s}$}\fi}{\ifmmode{{\rm Mpc}}\else{Mpc}\fi}$.}
$J_{\rm M}(r)$ for  $R=1.5\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$   and  several   values  of   $\mu$;  this
represents typical situations  of galaxy clustering.  Obviously $J(r)$
discriminates between the  varying richness  classes of the   Mat\'ern
cluster processes.

\section{Galaxy samples}
\label{sect:galaxies}

In this section  we want to go one  step further by applying $J(r)$ to
catalogues of  galaxies and groups of  galaxies, and compare them with
a Mat\'ern cluster process.

\subsection{Description of the PPS galaxy and group samples}
\label{sect:pps}

The     PPS   database   was      compiled   in   the   last    decade
({}\pcite{giovanelli:redshift}, {}\pcite{wegner:survey}).  The    full
redshift survey is magnitude--limited down   to a Zwicky magnitude  of
$m_{\rm Z}\leq15.7$ {}\cite{zwicky:catalogue},  and at least  95\% complete
to  $m_{\rm Z}\leq15.5$   (see  Figure~1 in  {}\pcite{iovino:galaxy}).   We
extract a  volume--limited  subsample  with  $M_{\rm Z}\leq-19$ and  radius
$79\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$,   confined  to        $-1^h.50\le\alpha\le+3^h.00$      and
$0^{\rm o}\le\delta\le40^{\rm o}$, i.e.\ a solid angle of $0.76{\rm sr}$.
Redshifts are corrected for the motion of the Sun relative to the rest
frame    of   the    Cosmic  Microwave   Background     (CMB)   as  in
{}\scite{peebles:principles},  and  we also correct  Zwicky magnitudes
for interstellar extinction as in {}\scite{burstein:HI}.
The final volume--limited sample PPS79 contains 817 galaxies.

To find  groups,  we   use the  redshift   space  friends--of--friends
algorithm of {}\scite{huchra:groups},  suitably adap\-ted to our case.
It  is a truncated percolation algorithm  with two independent linking
parameters  $D$ and  $V$.   Briefly, two  galaxies are  ``friends'' if
their transverse    and   radial    separations $r_{ij}^{\perp}$   and
$r_{ij}^{\parallel}$   satisfy       $r_{ij}^{\perp}     \leq  D$  and
$r_{ij}^{\parallel}     \leq V/H_0$,   respectively.  Friendship    is
transitive, and a set of {\em three} or more friends is called a loose
group of galaxies.

Usually, loose   groups are identified in  magnitude--limited samples.
Here,  we  consider    only   volume--limited   samples.    Values  of
$D=0.52\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$  and $V=600~\ifmmode{{\rm km}/{\rm s}}\else{${\rm km}/{\rm s}$}\fi$  give  very good  agreement of  global
properties (e.g.\ the total fraction  of galaxies in groups, the ratio
of groups to galaxies, or the  median velocity dispersion) between our
volume--limited group catalogue  and the  magnitude--limited catalogue
constructed by {}\scite{trasarti:loose}.

The final sample contains 230 galaxies  in 48 loose groups.  A typical
group    has 5  observed   members,    a  ``virial   mass''   of  some
$10^{13}M_\odot$, and an observed luminosity of some $10^{10}L_\odot$.
Both its  radius and its  inter--member pairwise separation are around
$0.5\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$, and  the  line--of--sight velocity  dispersion amounts  to
roughly $200~\ifmmode{{\rm km}/{\rm s}}\else{${\rm km}/{\rm s}$}\fi$,   so  the groups   appear  thin  and elongated  in
redshift space.

\subsection{$J(r)$ for the  galaxy samples}
\label{sect:pps_groups}

\begin{figure}
\begin{center}
\epsfxsize=8cm
\begin{minipage}{\epsfxsize}\epsffile{fig3.eps}\end{minipage}
\end{center}
\caption{
\label{fig:J_PPS_GAL}
$J(r)$ for  all galaxies in the  PPS79 sample (solid line)  and for 50
realizations  of a  Poisson process  with  the same  number of  points
(dashed area).  The dashed area indicates 1--$\sigma$ fluctuations.}
\end{figure}
We calculated $J(r)$   for all galaxies from   the PPS79  sample;  the
results  are  shown in Figure~\ref{fig:J_PPS_GAL}.   With $J(r)$ lying
outside the area  occupied by realizations  of a Poisson process,  one
can  clearly see   that galaxies  are   strongly clustered  -- not   a
particularly surprising result.    In Sect.~\ref{sect:PPS-simulation},
somewhat  more   interesting  comparisons   with  galaxy mock--samples
extracted from $N$--body simulations are performed.

\begin{figure}
\begin{center}
\epsfxsize=8cm
\begin{minipage}{\epsfxsize}\epsffile{fig4.eps}\end{minipage}
\end{center}
\caption{
\label{fig:J_PPS_GR}
$J(r)$  for the galaxies in  groups in the  PPS79 sample (solid line),
for a Mat\'ern  cluster process with  $\mu=5$ and $R=1.5\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$ (dashed
line), for the average of 50 samples extracted  from all galaxies with
the same number density as the galaxies in groups (light shaded area),
and for the average  and fluctuations of  50 realizations of a Poisson
process (dark shaded area).}
\end{figure}
Figure~\ref{fig:J_PPS_GR}      displays  the   results   for   grouped
galaxies. Since  each   group contains  at  least  three  members, the
nearest neighbour  of a grouped  galaxy is  certainly found within the
largest link length used in the friends--of--friends procedure.  Hence
we observe $G(r)=1$ and subsequently  $J(r)=0$ for $r>5.6\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$ in the
grouped galaxy sample.
$J(r)$ is in general {\em  not} invariant under  changes of the number
density {}\cite{vanlieshout:j}.   To compare  the $J(r)$  for  grouped
galaxies with the $J(r)$   for all galaxies,  we subsample  the denser
PPS79.  $J(r)$   is  calculated from  50   subsamples of 230  galaxies
randomly selected from the whole PPS79  sample. With $J(r)$ we measure
the strength   of  clustering, which  is  emphasised when  we consider
galaxies  in groups only,  and is less  pronounced when we look at the
whole sample with field galaxies included.
Similarly the  value of  $J(r)$ for the  sub--sampled PPS79  is higher
than  $J(r)$  for  the   whole  PPS79,  because  Random  sub--sampling
(thinning) tends to increase $J(r)$ towards the Poisson value.

The  centers  of loose  groups  show  a strong  correlation themselves
{}\cite{trasarti:clustering}, therefore a Mat\'ern cluster process can
only serve   as  a rough approximation   to  the true  distribution of
galaxies  in groups.  Despite  this,  a Mat\'ern cluster process  with
$\mu=5$  galaxies   per  group   (cluster)  and  a  group    radius of
$R=1.5\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$ shows a $J(r)$ comparable to the $J(r)$ obtained from the
galaxies in groups, where  in the mean  4.8 galaxies reside in a group
(see Fig.~\ref{fig:Jmatern}).
We see a low, almost constant value of $J(r)$  for $r>2.5\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$.  This
suggests that we are indeed looking  at highly clustered galaxies with
small contamination by ``field'' galaxies.

The $J_M(r)$  of a Mat\'ern  cluster process  gets constant  for radii
twice      as     large   as   the       cluster   radius.    Already,
{}\scite{vanlieshout:j} express their hope  to deduce a cluster  scale
$R$ in a point distribution  from $J(2R)\approx{\rm const}$.  However,
this must be    taken with extreme caution.     As can  be seen   from
Fig.~\ref{fig:Jmatern} we may be  fooled by a  factor of three by  the
fluctuations in the estimated $J(r)$.    The uncertainty becomes  even
worse when we  consider certain Cox--processes, where $J(r)$ decreases
strictly     monotonically     towards      a       constant     value
{}\cite{vanlieshout:j}, and in principle  no scale can be deduced from
the  comparison  with the   oversimplified  Mat\'ern cluster  process.
Either we have to   restrict ourselves to qualitative  statements,  or
come up with more refined and realistic models.

\section{Comparison with  N--body simulations}
\label{sect:nbody}

The  preceding section  showed that  the qualitative  features  of the
galaxy distribution are well  described by the $J$--function.  In this
section we  explicate that  the $J$--function is  also suitable  for a
quantitative  comparison,  and  allows  us to  constrain  cosmological
models.

\subsection{N--body simulations and mock--catalogues}
\label{sect:simulation}

We extract 64    mock--PPS  catalogues from a    cosmological  N--body
simulation of a Mixed Dark Matter (MDM) model.

We consider  a   MDM model with  one   species  of  massive neutrinos,
dimensionless  Hubble   parameter $h  =  0.5$  and  density parameters
$\Omega_c = 0.8$,  $\Omega_h  = 0.2$ for  cold  and hot  dark  matter,
respectively.  The analytical   expressions for the MDM  power spectra
$P(k)$  was taken from  {}\scite{ma:linear}.   The initial $P(k)$  was
normalised to the   COBE 4-yr  data {}\cite{bunn:fouryear}, giving   a
corresponding   value  of $\sigma_8 =  0.82$    for the  r.m.s.\  mass
fluctuation in an $8\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$ sphere.

The simulation was  run from an initial  expansion factor $a_i=1$ down
to $a_f=4.5$ using a P$^3$M code  with $100^3$ particles of mass $1.49
\cdot 10^{13} M_\odot$, on a cubic grid of $256^3$ cells, with a force
softening radius  $0.32\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$,  in  a box   of  side $300\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$.   The
integration was performed in comoving coordinates using $a(t)$ as time
variable for a total of 225 steps.

We identify ``galaxies'' in our   simulation with a method similar  to
the one discussed by {}\scite{little:cosmic}:

First, we associate with each particle a number $n_i$ of galaxy--scale
peaks   calculated     from  the   initial   density   contrast  field
$\delta({\mathbf{x}})$.    In    the   peak--background  split    approximation
(\pcite{bardeen:gauss},                      {}\pcite{white:clusters},
{}\pcite{park:biasing})   $n_i$ is the  number   of galaxy peaks  with
height $\delta_s({\mathbf{x}}_i) \geq \nu_{th} \sigma_s$, where $\delta_s({\mathbf{x}})$
denotes  the  field    smoothed   with a   Gaussian    kernel of width
$R_s=0.55\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$, and $\sigma_s^2$ gives the smoothed field's variance.
The  field is  subject   to the constraint  that   it takes the  value
$\nu_b\sigma_b$      when   smoothed  on  a       scale $R_b>R_s$ (see
{}\pcite{park:biasing}   for more details).  Choosing $\nu_{th}=0.05$,
at $a=4.5$  the  particle  two--point correlation  function,  weighted
according   to $n_i$, matches     in slope and  amplitude the   galaxy
two--point correlation function.    For  the adopted   parameters, the
total number of peaks in the box is $\sum n_i \simeq 690,000$.

Then,  we select the  $i$--th particle as a  galaxy if $An_i>p$, where
$p\in (0,1)$ is a uniformly distributed  random variable, and $A$ is a
constant of proportionality.   The  latter is  set by the  requirement
that the mean  number density of ``galaxies'' in  the box matches  the
mean   density of $M\leq  -19+5   \log(h)$ galaxies  expected from the
Schechter  luminosity function   with  $\alpha=-1.15$, $M_*=-19.3  + 5
\log(h)$,  $\phi_*=0.02  \,  h^{3}$Mpc$^{-3}$   appropriate   for  PPS
(\pcite{trasarti:loose};       {}\pcite{marzke:luminosity}).      This
Monte--Carlo procedure makes the  implicit assumption that the  higher
the peak, the more luminous the associated galaxy.

The mock--PPS  catalogues were built as follows.   The simulation cube
was  divided into $64$  sub--cubes of  side length  $75\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$.  Within
each  sub--cube  we  fit   a  PPS--like  wedge  of  radius  $79\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$.
Redshift--space coordinates $\alpha$,  $\delta$, $cz$ were assigned to
all the  ``galaxies'' of  the sub--cubes.  Finally,  we kept  only the
``galaxies'' within  the redshift--space--boundaries of  the mock--PPS
catalogues.

Although we are looking at a large volume with a  depth 79\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi\ and a
solid  angle of $0.76{\rm sr}$,  we observe large fluctuations of 25\%
in         the     number     of      points     per      mock--sample
(Fig.~\ref{fig:counts_histogram}).     This  is  consistent  with  the
large--scale   fluctuations  of  the  clustering   properties  of IRAS
galaxies, as found by {}\scite{kerscher:fluctuations} out to scales of
200\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi, and  expresses cosmic  variance  in agreement  with expected
sample--to--sample variations  {}\cite{buchert:two-point}.  As we will
see, this slightly complicates the analysis.
\begin{figure}
\begin{center}
\epsfxsize=8cm
\begin{minipage}{\epsfxsize}\epsffile{fig5.eps}\end{minipage}
\end{center}
\caption{
\label{fig:counts_histogram}
This   histogram displays the number  of  points per mock--sample; the
solid lines give the values in redshift--space, while the dashed lines
corresponds to selection in real--space.}
\end{figure}

\subsection{$J(r)$ for the mock--samples}
\label{sect:J-mock}

\begin{figure}
\begin{center}
\epsfxsize=8cm
\begin{minipage}{\epsfxsize}\epsffile{fig6.eps}\end{minipage}
\end{center}
\caption{
\label{fig:red-all-simul}
The mean $J(r)$ and  the 1$\sigma$  range  for the mock--samples  with
$\Delta=30$ (solid line, dark shaded), with $\Delta=100$ (dotted line,
medium shaded), and for  all mock--samples (dashed line, light shaded,
the 1$\sigma$ range is plotted symmetrically).}
\end{figure}
At first we investigate the mock--samples selected in redshift--space.
If  we  use  all  the   64  mock--samples  we  are  dominated  by  the
fluctuations  between samples  with  a different  number density  (see
Fig.~\ref{fig:red-all-simul}).   Therefore, we  restrict  ourselves to
mock--samples with approximately  the same number of points  as in the
observed  galaxy  sample: $N_{\rm  gal}-\Delta  \le  N_{\rm mock}  \le
N_{\rm gal}+\Delta$, with $N_{\rm gal}=817$.  For $\Delta=30$ only six
samples  enter, whereas  for  $\Delta=100$ we  already have  seventeen
mock--samples  to analyse.  The  mean value  of $J(r)$  hardly changes
between samples with different  $\Delta$.  Obviously, samples with low
density  tend  to  be  centred  on voids,  and  high--density  samples
typically include large, Coma--like clusters. So large fluctuations in
the  number  density lead  to  large  fluctuations  in the  clustering
properties  measured  by  $J(r)$   but  cancel  in  the  mean.   These
fluctuations      decrease     for      smaller      $\Delta$     (see
Fig.~\ref{fig:red-all-simul}; this was confirmed by inspecting samples
with $\Delta=50$ and $\Delta=200$).
In  order  to look  at  structures comparable  to  the  PPS sample  we
consider  mock--samples  with  a  similar  number density  as  in  the
observed galaxy  sample, and do  not subsample the  mock--samples with
high number density.

\begin{figure}
\begin{center}
\epsfxsize=8cm
\begin{minipage}{\epsfxsize}\epsffile{fig7.eps}\end{minipage}
\end{center}
\caption{
\label{fig:real-red-data}
This plot shows  the average value of $J(r)$  and  1$\sigma$ range for
the mock--samples with $\Delta=100$  in real--space (solid lines), and
for the mock--samples in redshift--space (dotted lines).}
\end{figure}
In Fig.~\ref{fig:real-red-data}  the results  of the  mock--samples in
real-- and  redshift--space are compared.  The  mock--samples selected
in   redshift--space  show a   weaker  clustering  than  mock--samples
selected in real--space on small  scales out to  at least $2\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$, as
can be deduced from  the higher  $J(r)$.   This can be traced  back to
redshift space distortions.
The peculiar motions act  by erasing small scale clustering; therefore
the J value of redshift-space samples is larger (less clustering) than
that of  real-space samples. This  effect changes at a  given distance
(2\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi). The same  effect  was found by {}\scite{martinez:galaxy}  in
volume--limited subsamples,   extracted  from CfA-I, by  means  of the
two--point correlation function.

\subsection{Comparison of the PPS galaxies with the mock--samples}
\label{sect:PPS-simulation}

\begin{figure}
\begin{center}
\epsfxsize=8cm
\begin{minipage}{\epsfxsize}\epsffile{fig8.eps}\end{minipage}
\end{center}
\caption{
\label{fig:redshift-data}
$J(r)$ is   shown for the PPS79   galaxy sample (solid   line) and the
1$\sigma$ range   for   the   mock--samples   with   $\Delta=100$   in
redshift--space (dashed area).}
\end{figure}
In Fig.~\ref{fig:redshift-data}   the results of  the mock--samples in
redshift--space  are compared with the  results of the observed galaxy
distribution  in  the   PPS.    The mock--samples show    insufficient
clustering on small scales out to at least $3\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi$, as can be deduced
from the higher $J(r)$.   This is  probably  due to the high  velocity
dispersion in  MDM models  {}\cite{jing:largescale}.  In  real--space,
which  is {\em  not}  directly  comparable   with  the  PPS data,  the
mock--samples reproduce the clustering on small  scales out to 1\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi,
but  again show   not  enough  clustering,   even though they   become
marginally consistent with the  observed galaxy distribution on larger
scales.
We have  to conclude that this  MDM simulation is  unable to reproduce
the observed strong clustering of galaxies on small scales.  Of course
this result depends on our method of galaxy identification. A different
biasing prescription might change this.
On large  scales a  definitive answer is  not possible, since  for $r$
larger than  6\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi\ an estimation  of $J(r)$ becomes  unreliable; the
empirical $G(r)$ and $F(r)$ approach unity, and the quotient $J(r)$ is
ill--defined.

\section{Conclusion and Outlook}
\label{sect:outlook}

We  have highlighted promising properties  of the global morphological
descriptor $J(r)$.  It  connects the distribution functions $F(r)$ and
$G(r)$ and, hence,  incorporates all orders of correlation  functions.
$J(r)$ measures   the strength of  clustering  in a point  process and
distinguishes between correlated  and  anti--correlated patterns.
The  example of  a  Mat\'ern cluster  process  illustrates that $J(r)$
sensitively depends on the richness of the clusters or groups.

Since $J(r)$ is built  from  cumulated distribution functions, we  do
not   encounter spurious  results   due   to  binning.  This   becomes
particularly important on small scales.

The application  of the $J$-function  to galaxies in a  volume limited
sample and to a sample of  galaxies in loose groups clearly showed the
stronger clustering  of galaxies  in groups.  In  a comparison  with a
Mat\'ern cluster we found  that internal properties, like the richness
of  loose  groups,  are  satisfactorily modelled.   However,  for  the
large--scale  distribution of galaxies,  the Mat\'ern  cluster process
clearly is an over--simplification.

We used   the $J$-function for  a  comparison  of the  observed galaxy
distribution with  galaxy  mock--samples.  Although  the mock--samples
extracted from   a MDM--simulation cover  a large  volume, we detected
large  fluctuations of the  order of 25\%  in the number of points per
sample.  On small scales, out to 1\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi, the clustering in real--space
is   as strong as    in the  observed galaxy   distribution,   but the
comparable redshift--space mock--samples show too weak clustering.  On
larger  scales   from  2--6\ifmmode{h^{-1}{\rm Mpc}}\else{$h^{-1}$Mpc}\fi\   both real--   and  redshift--space
mock--samples show too weak clustering.  Hence, this MDM simulation is
not able  to reproduce the  observed strong clustering of the galaxies
on small scales.

The function $J(r)$  has  proved to achieve comparable  discriminative
power as the Minkowski functionals {}\cite{kerscher:fluctuations}, and
is  most suitable for  addressing  the  question of ``regularity''  on
large--scales  as demonstrated in  an analysis of  the distribution of
superclusters {}\cite{kerscher:regular}.
In  this article we have  shown that the   $J(r)$ function is a useful
tool for quantifying the clustering of galaxies on small scales and is
capable of constraining cosmological models of structure formation.

\section*{Acknowledgements}

It is a pleasure to thank Adrian Baddeley, Bryan Scott, Claus Beisbart
and  Herbert Wagner for   useful discussions  and comments.   We thank
Simon D.M.~White  for pointing  out the  relation to   the conditional
correlation function.   This  work was partially   supported by the EC
network of the program Human Capital and Mobility No.\ CHRX-CT93-0129,
the  Acci\'on     Integrada  Hispano--Alemana HA-188A    (MEC),    the
Sonderforschungsbereich SFB     375   f\"ur   Astroteilchenphysik  der
Deutschen Forschungsgemeinschaft, and the Spanish DGES (project number
PB96-0797).

\providecommand{\bysame}{\leavevmode\hbox to3em{\hrulefill}\thinspace}

redpajama_set_name: RedPajamaArXiv


I am currently an undergraduate student at the University of New Hampshire at the Peter T. Paul College of Business and Economics with a declared major in Finance and a minor in Sales. Ultimately, I am seeking to grow into the Sales industry, using the information and experience I have gained over the years to propel me to success. The UNH Sales Program has offered me an extensive amount of opportunity through avenues, such as the Professional Sales Group, the UNH Sales Club, and the Sales Minor.
I have always possessed a great interest in the field of business and use my skills and talents from past experiences to continue to grow and succeed each and every day. Currently seeking full-time opportunities after graduation in May 2019 in sales specific roles.
Please reach out to me with any questions you may have!
Developed relationships with healthcare professionals in order to provide a comprehensive solution.
Resulting in over 3,000 calls made during the Summer, placement margins as high as 44%, and a copious amount of experience talking to C-Level Executives.
High-end home improvement company that provides essential home improvements to residential properties.
Various and important skills acquired, such as sales, marketing, budgeting, accounting, and management.
Various skills in multiple fields, such as painting, carpentry, landscape, and hardscape learned to deliver a successful job outcome.
Branch Manager: experience provided skills in the fields of marketing, sales, and management while managing a branch comprised of 6 towns and cities in Southern New Hampshire.
Provided over 100 students an advanced sales acumen and education of the critical pillars in the sales cycle while organizing meetings with various Program sponsors and professionals.
Participate in multiple internal and intercollegiate Sales Competitions (ICSC, Orlando), dissect the sales process, and extend sales acumen through each opportunity the Group offers.
Alpha Kappa Psi fosters both personal and professional growth of its members.
Held positions in various committees while being an active, leading veteran for new members.
Managed a committee of 12 individuals who were responsible for generating leads, prospecting companies, and closing partnerships between the company and the fraternity.
Countless skills learned throughout many years, such as leadership, organization, first aid, soft skills, and many more.
The srazzetti site is maintained by Scott Razzetti using the myPages at UNH.


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This page is the brochure for your selected program. You can view the provided information for this program on this page and click on the available buttons for additional options.
IES Abroad Nice Direct Enrollment – SKEMA Business School (Outgoing Program)
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Locations: Nice, France
Program Terms: Academic Year, Fall, Spring
Homepage: Click to visit
Program Sponsor: IES
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Fact Sheet:
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Language(s) of Instruction:
English, Other (non-English)
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Program Description:
Nice Direct Enrollment - SKEMA Business School
Conveniently located between Cannes and Monaco, Nice is well-known for its breathtaking waterfront and idyllic lifestyle on the French Riviera. But did you know that Nice is also close to Sophia Antipolis, Europe's well-known science park that houses more than 1,300 international companies in information and communications technology, biotechnology, and research? This park is also known as the French Silicon Valley.
This is your opportunity to live and learn alongside students from France and around the world by directly enrolling at SKEMA Business School. SKEMA's state-of-the-art business campus is located in the heart of Sophia Antipolis, where you will directly enroll in English-taught Business courses. SKEMA, which has AACSB and EQUIS accreditation, is consistently ranked as one of the best European business schools by the Financial Times.
Visit www.IESabroad.org for complete program details.
Why Nice?
As the fifth largest city in France, Nice is the capital of the French Riviera and an international metropolis, with more than 160 different nationalities living and working in the region. Because Nice is a European and Mediterranean hub to the world (its international airport is just 5 km from the city center), the city is host to a large number of international businesses and schools, a center for innovation, and a celebrity hotspot.
We strive to make sure you feel safe, cared for, and at home while you're away from home. Whether it's the orientation program that makes you feel prepared, your housing that is well-located and comfortable, the cultural events that make it easy and fun to meet other international and local students, or the field trips and walking tours that take you to places tourists don't usually see—we're all about our student service. Learn more about the day-to-day studying abroad on this program. From field trips to housing, it's all on IES Abroad's website.
IES Abroad firmly believes that financial limitations should not prevent a qualified student from participating in an IES Abroad program. That's why we commit $5 million in study abroad scholarships and aid, all offered through one quick and easy application. Check out all of our scholarship options at www.IESabroad.org/aid.
Aid Application Deadlines:
Summer – April 1
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Spring/Calendar Year – November 1
The IES Abroad Difference
We can say that our academic standards are completely unmatched, our partnerships with more than 500 global universities and colleges speak to the quality of our programs, and our health and safety practices have set the standards for the entire field of study abroad. And all of that would be true…. But what really sets us apart is our commitment to you. As a not-for-profit study abroad and internship provider, you are our bottom line. Your success is our success. And in today's world, that's a pretty extraordinary thing.
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About IES Abroad
Founded in 1950, IES Abroad is a not-for-profit academic consortium of more than 260 top-tier American colleges and universities, with more than 240 additional partner universities worldwide. IES Abroad provides premier study abroad and internship programs around the world through IES Abroad, IES Internships, IES Abroad Customized & Faculty-Led Programs, and The Study Abroad Foundation. With more than 400 study abroad programs in 85 locations worldwide, the organization creates authentic global education opportunities for thousands of students annually. IES Abroad has nearly 140,000 alumni who have benefited from studying in IES Abroad programs since its inception. Discover more about what we offer with all of our programs.
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One common mistake when we configure a server is forgot run backups, No enough time and other excuses can convince you that make a backup of a new server is not a priority, but sometimes a hipervisor fails and recover data from your virtual machine is hard or impossible. Trust me i saw a lot of unrecoverable databases in development environments unrecoverable after a power outage or hardware fail.
This tutorial will covered a basic backup for a database server with a small number of small – medium size databases.
1 step create a mysql backup user.
*trick in my case I mounted a nfs share in this directory.
# if backup set specific modifications are required.
# - ZRM plugin parameters.
# see mysql-zrm(1) and/or Administration manual at Zmanda Network.
# about the backup set.
# This parameter is optional and has no defaults.
# This parameter is optional and default value is full backup.
# This parameter is optional and default value is "raw".
# Values can be "regular" or "quick".
# compression algorithm should be used, it must be set in "compress-plugin"
# parameter. Default: There is no data compression.
# This specifies the program to be used for compression. The "compression"
# value is not specified then gzip(1) is used for compression.
# This parameter should be set to 1 if backups should be encrypted.
# backup data encryption. "decrypt-option" parameter should also be specified.
# program specified as "encrypt-plugin" parameter for decryption.
# should be specified. If none of the them are specified, "all-databases"
# "all-databases" is set 1.
# should not be specified if all tables in the databases in "databases"
# to should be specified in "database" parameter.
# MySQL database user used for backup and recovery of the backup set.
# MySQL database user password.
# my.cnf configuration file or no password is used.
# Fully qualified domain name of the MySQL server.
# required only if MySQL server allows SSL connections.
# This can be set to specify that mysqldump should dump stored routines also.
# use as default. This parameter is optional.
# If not specified utf8 is used as the default character set.
# Directory where MySQL commands can be found. The parameter is optional.
# Directory where MySQL binary logs can be found. The parameter is optional.
# default value is 0 (less verbose).
# Values can be "always", "never" or "only-on-error"
# "html-report-directory" parameter is specified.
# If this parameter is not specified, "backup-status-info" report is generated.
# See mysql-zrm-reporter(1) for details of backup reports.
# Multiple report names should be separated by ",".
# administrator/user to browse HTML reports and can get to the RSS feeds.
# must be provided if "webserver-url" is specified.
# the backup to their environment.
# COPY plugin: Only one copy-plugin must be configured for a backup set.
# the machine running ZRM for MySQL with sockets.
# passed to "pre-backup-plugin" before a backup run for the backup set.
# "pre-backup-plugin" parameter must be specified.
# passed to "post-backup-plugin" after a backup run for the backup set.
# "post-backup-plugin" parameter must be specified.
# start time for a backup run.
# specifies the file containing the passphrase.
# to specify the location of mysql client binaries on the remote host.
# to be opened on the remote host.


text:
Os Parças é um longa-metragem de comédia, com produção da Formata e distribuição da Downtown e direção de Halder Gomes. Os parças, como sugere o título do filme, será interpretado pelo próprio Tom Cavalcante, Bruno de Luca, o comediante Tirullipa e o youtuber Whindersson Nunes. O longa foi rodado entre os meses de maio e junho de 2017. O primeiro trailer do filme foi divulgado no dia 15 de outubro no canal do youtuber, Whindersson.

Enredo
Fugindo de problemas, um locutor de loja de varejo, dois trambiqueiros e um técnico de informática atrapalhado são obrigados a participar de um golpe. Eles são chantageados por Mário, um vigarista que se aproveita da boa-fé alheia para ganhar dinheiro. O desafio é nada mais nada menos do que montar uma firma de casamento para produzir a festa da filha do maior contrabandista da Rua 25 de Março, o temido Vacário. Juntos eles vão enfrentar muitos desafios na produção da festa e terão que fazer de tudo para não levantar a desconfiança de Vacário.

Elenco
Tom Cavalcante como Toinho / Helga
Whindersson Nunes como Ray Van
Tirullipa como Pilôra
Bruno de Luca como Romeu
Paloma Bernardi como Cintia Maria Barolo
André Bankoff como Marcelo Paranhos
Taumaturgo Ferreira como Vacário Barolo
Oscar Magrini como Mário
Carolina Chalita como Samantha
Carol Garcia como Ritinha
Pedro Moutinho como Policial Fabio Júnior
Milhem Cortaz como Sargento Pena
Marcos Oliveira como Seu Juvêncio
Carlos Alberto de Nóbrega Como Toninho La Paz
Ricardo Macchi como Borges
Romeu Evaristo como Mulumba
Fábio Goulart como Peçanha
LC Galetto como Soares
Neymar como Ele mesmo
Wesley Safadão como Ele mesmo

Recepção
Atraiu um milhão de espectadores aos cinemas, sendo o 4° filme mais assistido no Brasil em 2017, depois de Liga da Justiça (3°), Extraordinário (2°) e O Último Jedi (1°). Ganhou nota 5,3/10 no IMDb, 3,1/5 no AdoroCinema.

Ligações externas

Filmes do Brasil de 2017
Filmes de comédia do Brasil
Filmes em língua portuguesa
Filmes distribuídos pela Paris Filmes


The upstream HTTP proxy of InterScan Web Security Virtual Appliance 6.5 (IWSVA) fails to connect to IWSVA.
This article discusses scenarios and workarounds to alleviate the connection failure.
Trend Micro recommends that the workaround for each scenario is implemented in advance if you use an upstream HTTP proxy.
The upstream HTTP proxy often reuses the same TCP client port for a new connection despite the relevant TCP session being still left in IWSVA. This leads to the upstream HTTP proxy failing to connect to IWSVA.
When the upstream HTTP proxy uses the same TCP client port as the TIME_WAIT state session left in IWSVA and sends TCP SYN to IWSVA, IWSVA regards it as the response for the TIME_WAIT state session and replies TCP ACK (not TCP SYN/ACK). The upstream HTTP proxy gets the ACK reply and sends TCP RCT to IWSVA because the reply is invalid.
However, IWSVA disregards the TCP RCT response according to RFC 1337 by default without closing the TIME_WAIT state session. Therefore, the upstream HTTP proxy continues to reuse the same TCP client port for a new connection until it gives up as TCP 3-way handshake failure.
The following makes IWSVA accept TCP RST for the TIME_WAIT session and immediately close the session. As a reference, to increase "IP addresses/TCP ports for TCP client" in the upstream HTTP proxy also resolves the issue.
The load balancer located between the upstream HTTP proxy and IWSVA might change the information of the TCP segments. When this happens, IWSVA's firewall might discard the TCP segments by default when it classifies them as invalid. This leads to the upstream HTTP proxy failing to connect to IWSVA.
Add an IWSVA firewall rule so that any TCP segments from the upstream HTTP proxy are accepted.
Example: For the upstream HTTP proxy "192.0.2.1"


The long awaited sequel to Adventures Aboard Rick's Place will be released September 30, 2010!
So get ready to join Rick as he sets sail once again and experiences the highs and lows of the roller coaster cruising life visiting Mexico's Sea of Cortez and Riviera Coast then across the Pacific to the remote islands of French Polynesia.
This humorous travel-adventure novel is based on the authors true adventures and gives a realistic look at the crazy cruising lifestyle.
Did you enjoy reading Rick's Place?
Then enter it as a suggested read to Jimmy Buffett's new book club!
Go to the Jimmy Buffett's Margaritaville Book Club link to the left and submit it for consideration!
You'll need the following information for the form -- the Amazon Link at the bottom should be copied and pasted into the form.
Rick's Place is a story of a solo sailor and is based on the author's adventures, both real and imagined.
Follow Rick through his carefree youth and later as a series of events leave him jobless and wondering just what to do with his life. Then live vicariously through this charming landlubber turned sailor as he lives everybody's dream of escaping the rat race and sailing off into the sunset.
The road to paradise is a bit rocky as Rick faces fear and loneliness when he encounters storms, a stowaway cat and unrequited love along the way. There is also a lot of fun as Rick meets an odd assortment of new friends and quirky characters during his journeys.
The story culminates in a life changing event that once again leaves Rick wondering what to do with his life and you'll find yourself rooting for this resilient young man.
This humorous account will leave you longing to visit the beautiful South Pacific Isles Rick sails to, as well as giving you a realistic look at the adventurous cruising lifestyle experienced by those traveling the Coconut Milk Run.


text:
Capricorn History, Mythology And Predictions
Color: Brown, Black
Day: Saturday
Ruler: Saturn
Greatest Overall Compatibility: Cancer, Taurus
Lucky Numbers: 4,8,13,22
Date range: December 22 - January 19
THE HISTORY OF CAPRICORN
THE MYTH OF CAPRICORN
THE RELATION BETWEEN THE CAPRICORN MYTH AND THE CAPRICORN ZODIAC SIGN
Everything about Capricorn History and Myth
The indication of Capricorn isn't the same thing as the star grouping Capricornus. They don't harmonise, and the entirety of the stars from the heavenly body Capricornus is now in the indication of Aquarius. The movement of Capricorn takes the 10th 30 levels of the zodiacal circle and starts with the primary day of winter. This is a cardinal sign, which means it denotes the start of the period and the change it carries with it. The heavenly body Capricornus characterised the colder time of year solstice in the Early Bronze Age, for the Sun was in it when winter started until 130 BC.
The name of this heavenly body is Latin for "horned goat" or "goat horn", and it is portrayed as an ocean goat, a legendary animal that is half goat, half fish, focusing on its tail with the most splendid star in the heavenly body in it. The actual bottom emblematically addresses the past, our obligations, and what we are hauling from quite a while ago. The star grouping is the littlest of every single zodiacal heavenly body. It is set in the sky called "Ocean" that comprises many water-related heavenly bodies like Pisces and Eridanus.
Capricornus was recorded by the second-century stargazer Ptolomy, yet before this posting, it was one of the heavenly bodies most established known to men, notwithstanding its faintness. It was addressed as half of a goat and a fish since the Middle Bronze Age, with the verified initial portrayals dated around the 21st century BC. In Babylonian star indexes, it was recorded as "The Goat-Fish" before 1000 BC.
Intriguingly, the planet Neptune was found in the heavenly body Capricornus, close to Deneb Algedi, the most splendid star in the goat's tail, on September 23, 1846. The connection between Capricorn and Pisces is by all accounts excellent, particularly when you consider the imagery of the animals and every one of the narratives in regards to Capricorn and Capricornus.
The legend of Capricorn is associated with Pan, the lord of the wild, shepherds and rushes, nature of mountain wilds, and local music. He had goat legs and the instrument he played, the panpipes, recounting an uncommon romantic tale of a lady who dreaded her subject, fleeing from his commendations. One of the narratives of Pan talks about a social occasion of divine beings that Typhon, the colossal monster, hindered. Out of dread, the entirety of the heavenly beings changed shape, while Pan bounced into the Nile waterway, transforming his legs into a tail of the fish, and his middle to a goat, confounding the beast and alarming it away with his appearance.
The powerful story taken cover behind Capricorn is where Zeus was helped by a goat that designed the terrifying horn called "pinkos" on his primary goal to crush the Titans. The horn was found in the ocean, and this clarifies the fishtail that was given to the goat, while the horn probably was a shell that made a sound to drive every one of the Titans to dissipate, froze. At the point when Titans were at last crushed by the Olympians and shipped off the underworld, every day as the night fell, there was a feeling of dread that the Titans would ascend not too far off.
"Frenzy" is derived from the name of god Pan, or really from pinkos, the instrument with a sound that made the Titans disperse away. Every form of the fantasy associated with the indication of Capricorn and its comparing star grouping is, for the most part, about dread. This is dread that makes individuals change shape and profess to be what they are not. This is dread that gets everybody around an individual, driving them to exact torment.
We can see a lady fleeing from the commendations of a man, yet additionally a lady who fears a man with a peculiar appearance that frightens her in a dull spot. At the same time, she is separated from everyone else. We can perceive the force of dread that makes significantly more dread, as Pan transforms into a beast himself, to frighten Typhon. What's more, we can see a wide range of issues with the lower half of one's body. The dread in these accounts never blurs, and it is there in any event, when the fight is finished, in anticipation of the foe to return.
Capricorn is an indication that addresses time and duty, and its delegates are conventional and frequently intense naturally. These people have an internal condition of freedom that empowers huge advancement both in their own and expert lives. They are bosses of restraint and can lead the way, make solid and reasonable plans, and oversee numerous individuals who work for them whenever. They will gain from their errors and get to the top, dependent on their experience and mastery.
In addition to the fact that they focus on the material world, yet they can utilise the most out of it. Shockingly, this component additionally makes them hardened and, some of the time, too difficult to even think about moving from one viewpoint or point in a relationship. They struggle tolerating contrasts of others that are excessively far from their character, and out of dread may attempt to force their conventional qualities forcefully.
Saturn is the decision planet of Capricorn, and this planet addresses limitations. Its impact makes these individuals reasonable and capable, yet also calm, removed, and unforgiving, inclined to the sensation of blame and going to the past. They need to figure out how to pardon to make their own life lighter and more sure.
Capricorn – A goat with the tail of a fish is made to confront fear and make alarm. Continuously prepared to change into something that frightens those nasty things away, Capricorn discusses every normal chain response of dread, where something startling prompts numerous others, ascending as cautious components that compound the situation. Drenched in their mystery, they face the world similarly as they are – adequately courageous to never flee, however continually scared of their internal beasts.
Capricorn Horoscope: Daily
Love Don't let yourself be stressed out by people who only want to take advantage of you. Be aware and stay away. MONEY You should thoroughly evaluate all
Capricorn Horoscope: Weekly
LOVE You might feel a new sincere enthusiasm when it comes to your romantic relationship. If there has been some detachment in your interactions, then you
Capricorn Horoscope: Monthly
Love Venus and Mars are linked to love life and are at a complicated angle. Unreasonable demands and harsh criticism could jeopardize the continuity of the
Capricorn Horoscope: yearly
Capricorn Compatibility with other Signs
Capricorn And Aries
Capricorn And Taurus
Capricorn And Gemini
Capricorn And Cancer
Capricorn And Leo
Capricorn And Virgo
Capricorn And Libra
Capricorn And Scorpio
Capricorn And Sagittarius
Capricorn And Capricorn
Capricorn And Aquarius
Capricorn And Pisces
Capricorn sign
Everything about Capricorn History and Myth THE HISTORY OF CAPRICORN The indication of Capricorn isn't the same
Capricorn man
CAPRICORN MAN IN LOVE Capricorn men will start behaving strangely when they fall in love. He
Capricorn woman
CAPRICORN WOMAN IN LOVE At the point when a Capricorn woman falls head over heels, she
Capricorn horoscope
Capricorn history
Capricorn symbol
Capricorn daily horoscope
Capricorn weekly horoscope
Capricorn monthly horoscope
2021 Capricorn horoscope


text:
EyeFAQ Roundup January 2021
Posted on January 06, 2021 by Glaucoma Research Foundation
The EyeFAQ series of videos are presented by Glaucoma Research Foundation to answer frequently asked questions about glaucoma.
Leading ophthalmologists answer questions from patients about traumatic glaucoma, natural childbirth and glaucoma, how vision loss is defined and measured, and why it's important to have so many glaucoma examinations.
This January 2021 EyeFAQ Roundup features recent videos from Andrew Iwach, MD from the Glaucoma Center of San Francisco, Davinder Grover, MD, MPH from the Glaucoma Associates of Texas, and Ranya G. Habash, MD from the Bascom Palmer Eye Institute.
Q: Can a Traumatic Head Injury Cause Glaucoma?
Ranya G. Habash, MD Head injuries can cause glaucoma because there's a traumatic component. That trauma, especially if you have direct eye trauma can cause things like inflammation and damage to the structures of the eye that drain the [fluids to maintain the] pressure appropriately. Just imagine if the drain in your sink gets clogged or something is covering it, or something breaks, then it can't filter the water as well. This is the same kind of thing that happens in the eye too. The structures in there that are supposed to keep the pressure regulated can't act the same way that they need to because sometimes there's scar tissue or damage to those filtering structures.
Sometimes we see it in athletes, for instance, who get hit in the eye or a basketball injury to the eye. We see it in people who've had bar fights and got hit in the eye, airbag injuries, for instance. Anything that has basically direct impact onto the eye can potentially cause that.
Q: How is Vision Loss Defined and Measured?
Andrew G. Iwach, MD Defining vision, what is it? There actually are different characteristics to how we see. For example, most people will hear, "20/20." Well, that refers to how sharply you can see print, or let's say a road sign where you're driving, but there are other aspects of vision.
For example, the side vision. And why is it important to know that? Well, unfortunately, with glaucoma, it's often the side vision that gets affected first. That's where you lose it. In fact, the challenge with glaucoma is that you can lose a lot of side vision and not know about it.
Typically, we walk around with both eyes open, and hopefully, both of your eyes are healthy. And one eye can lose a lot of side vision, this peripheral vision, and you don't know it. And this is why we call sometimes glaucoma "the thief of vision," because you're doing everything right, and you don't realize that, unfortunately, it's taking away your vision without you even knowing it.
So those are two common aspects. There are other aspects. For example, your ability to see color or how you see contrast. So there are different ways we measure the quality of vision, but for glaucoma patients, the two most common measurements that we make are the visual acuity — the sharpness with which you see, and we measure the side vision.
Q: How Accurate are Visual Field Tests? Why is it important to have multiple glaucoma exams?
Davinder Grover, MD, MPH A glaucoma patient understands the way we monitor glaucoma with pressures and imaging and then visual fields. And visual fields are an essential component of glaucoma monitoring. But anybody that's ever taken a visual field test, myself included, can realize how frustrating that can be sometimes and [how] annoying they can be. They're not fun, and they're sometimes miserable and anxiety provoking, right? Because you're trying to get every one, especially if you're like me, type A personality, you want to get all the ones and you don't like the idea of missing something. But some days are good, some days are bad. Some days you're a little sleep deprived, some days you're a little distracted, some days you're thinking about what you want to do right after this exam and it's hard to maintain focus.
So I tell my patients, I don't ever get too excited or too worried about one visual field change because if you look back at all the studies we've done on visual fields, when you see a subtle change in a visual field, 80% of the time when you repeat it, it goes back to its baseline. So I know it can be worrisome when you're taking a visual field and you want to do your best and you want to get the best result. Sometimes we just aren't having a good day and sometimes the visual field is not the most reliable or sometimes it shows a little change. But don't get too worried or excited unless you repeat it and it confirms that change. But it's a subjective test and again, there's a human subjective component. So there's always some variability. There's always some background noise. And what we're looking at is for a trend over time.
The other thing to remember is that when you have a visual field defect from glaucoma, that's actually when you've lost a significant amount of your nerve tissue. So we want to be careful with that and if you have already lost enough nerve tissue where you have a visual field defect, we've got to be very careful with you. You can lose a lot of nerve tissue and have glaucoma damage without having a visual field change. So don't be falsely reassured because you have a normal visual field that everything is fine, you can lose a significant amount of nerve tissue and not actually have an impact on your visual field.
So visual field, as well as electronic imaging of the optic nerve tissue and pressure checks, as well as all of the things that are such important vital signs for monitoring glaucoma. Visual fields are one of the more annoying ones because it's really not fun to take them, but they are an important thing. Again, do your best not to let every click make you feel that every one [click] matters and if you miss one, it's done. Because that test is very smart. It knows what you should see. It knows what you may not be seeing, and it'll go back and test things. And again, your doctor will look at the [visual] field [test results] and if there's a change, repeat the [visual] field [test] before making any significant change in your treatment plan.
Q: Pregnancy and Glaucoma Treatment
Ranya G. Habash, MD It is possible for a pregnant lady to have glaucoma and also to have a natural delivery. Even if you've had glaucoma surgery, it really shouldn't impact the pregnancy per se. One of the things maybe that we would look out for is if you had a really long delivery and there was a lot of Valsalva or a lot of pushing, for instance, you just want to have your glaucoma filtering surgery checked afterwards just to make sure that it's still functioning properly. But we have plenty of patients with this type of situation and it really shouldn't affect a normal birth.
Last reviewed on January 06, 2021
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text:
Powerband CEO To Voluntarily Hold Shares For 12 Months
"I want people to know I am invested in PowerBand for the long run" – CEO, Kelly Jennings
VANCOUVER, BC / ACCESSWIRE / January 29, 2020 / The CEO and largest shareholder of PowerBand Solutions Inc. (TSXV:PBX)(OTCQB:PWWBF)(Frankfurt:1ZVA) ("PowerBand", "PBX" or the "Company"), has announced he will be entering into a voluntary escrow agreement with Computershare and that he will not sell his shares in the Company for at least 12 months, until January 29, 2021. This commitment is in addition to any escrow imposed by the TSX Venture Exchange.
The voluntary move by CEO Kelly Jennings comes as PowerBand continues to advance plans to put its transformational, cloud-based transaction platform into the hands of thousands of dealerships and consumers across North America.
"I want people to know I am invested in PowerBand for the long run as we revolutionize how cars and trucks are bought, sold, leased and auctioned," said Jennings, who founded the company 9 years ago.
"PowerBand intends to make buying, selling and leasing a car as easy as ordering an Uber on your smart phone or buying a product from Amazon," Jennings said. "This is a transformational solution, removing unnecessary middlemen, to benefit consumers, dealers, rental and commercial fleets, OEM's and funders."
Jennings has more than 27 years of automotive dealership ownership and management experience, and has won numerous awards from major OEM's for industry-leading business performance and customer satisfaction. Jennings holds 41,865,283 shares of PowerBand, representing approximately 37 per cent of the Company's outstanding shares.
About PowerBand Solutions Inc.
PowerBand Solutions Inc. is a technology provider listed on the TSX Venture Exchange. The Company's cloud-based platform is revolutionizing how we buy, sell, lease, and auction vehicles. With the recent receipt of its exporter license and its acquisition of MUSA Auto Finance, the Company is now well positioned to become a leader in the USD$10 billion cross-border used vehicle export market, the USD$100 billion used vehicle auction market, and the USD$120 billion vehicle leasing market in the U.S. and Canada.
Richard Goldman, VP Corporate Development
rgoldman@powerbandsolutions.com
This news release contains forward-looking statements relating to the Company and other statements that are not historical facts. Forward-looking statements are often identified by terms such as "will", "may", "should", "anticipate", "expects" and similar expressions. All statements other than statements of historical fact, included in this release, including, without limitation, statements regarding future plans and objectives of the Company, are forward looking statements that involve risks and uncertainties. There can be no assurance that such statements will prove to be accurate and actual results and future events could differ materially from those anticipated in such statements.
The reader is cautioned that assumptions used in the preparation of any forward-looking information may prove to be incorrect. Events or circumstances may cause actual results to differ materially from those predicted, as a result of numerous known and unknown risks, uncertainties, and other factors, many of which are beyond the control of the Company. As a result, we cannot guarantee that any forward-looking statement will materialize and the reader is cautioned not to place undue reliance on any forward-looking information. Such information, although considered reasonable by management at the time of preparation, may prove to be incorrect and actual results may differ materially from those anticipated.
Forward-looking statements contained in this news release are expressly qualified by this cautionary statement. The forward-looking statements contained in this news release are made as at the date of this news release, and the Company does not undertake any obligation to update publicly or to revise any of the included forward-looking statements, whether as a result of new information, future events or otherwise, except as expressly required by Canadian securities law.
Neither the TSXV nor its Regulation Services Provider (as that term is defined in the policies of the TSXV) accepts responsibility for the adequacy or accuracy of this news release.
This press release does not constitute an offer to sell or a solicitation of an offer to buy any of the securities in the United States. The securities have not been and will not be registered under the United States Securities Act of 1933, as amended (the "U.S. Securities Act") or any state securities laws and may not be offered or sold within the United States unless registered under the U.S. Securities Act and applicable state securities laws, unless an exemption from such registration is available.
SOURCE: PowerBand Solutions Inc.
https://www.accesswire.com/574473/Powerband-CEO-To-Voluntarily-Hold-Shares-For-12-Months


Turntable Demonstration: Witness our Roundhouse turntable rotated by a single person — with a rail car or locomotive on top!
"Fair of the First Mile" is a fresh new spring break outing that you don't want to miss! This fun-filled outdoor festival for guests of all ages highlights the railroad's historical entwinement with horses and police as well as the present and future of these enduring connections.
• Legend has it that in 1830, America's first steam locomotive, the Tom Thumb, raced against a horse-drawn rail car to demonstrate the power of steam locomotives. At the "Fair of the First Mile" children will have the chance to reenact this legendary race using stick ponies and wearable steam engine costumes, and to learn about the broader story of American transportation in the process!
• The B&O Railroad established the first railroad police unit in 1847. During "Fair of the First Mile, children will enjoy guided activities themed around locomotives, horses and police officers as well as a 10:30am story time each day featuring Kersten Hamilton's "Police Officers on Patrol".
• The very first mile of commercial railroad track was by the B&O Railroad in 1832. Families attending the "Fair of the First Mile" will have the opportunity to climb aboard the Mile One Express and travel along this most historic stretch of railroad.
• The B&O Railroad's Centenary Fair of the Iron Horse brought millions of families and railroad lovers to Baltimore in 1927 to celebrate the first 100 years of American railroading. At the "Fair of the First Mile", families can experience the essence of that momentous affair as they join us in celebration of the past and future of the proud B&O railroading tradition.
• Along America's first mile of commercial railroad track are the aptly-named First Mile Stables: a state-of-the-art equestrian facility currently under construction for Baltimore City's Mounted Police Unit. Families in attendance of the "Fair of the First Mile" will be able to travel via train to see the site that will be the new home of the oldest continuously operated mounted police division in the United States.
• Families will meet the award-winning Baltimore City Mounted Police horse Dino, known as 'Big D' and other members of the unit on Friday, April 19 from 11am - 1pm. 'Big D' was awarded the Klinger Award in October 2018 for best demonstrating the values of honor and service as embodied by Klinger, a special horse who touched the lives of many in his life of service with the 3rd U.S. Infantry Regiment (The Old Guard) Caisson Platoon.
• Families will learn why it is important to build a new home for 'Big D' and his fellow equine officers in the Baltimore City Mounted Police Unit and will have the opportunity to give support to the building campaign.
• September 2019 is the expected date by which visitors may board the Mile One Express train ride and enjoy an educational visit to the First Mile Stables: new home of the Baltimore City Mounted Police unit.
• The museum is looking ahead to the 2027 bicentennial of the B&O Railroad - an affair that will celebrate the past, present and future of the birthplace of American railroading.