text:
Mit media lab jeffrey epstein
A spokesperson from the MIT Media Lab directed Business Insider to the open letter MIT's president wrote following the exposé, announcing an internal investigation. Gates' former chief scientific
2:07 The head of the the Massachusetts Institute of Technology's embattled Media Lab has resigned and the school has opened an investigation into "deeply disturbing" links between the lab and Two prominent researchers are quitting MIT's Media Lab over revelations that the famed technology research hub and its director took money from Jeffrey Epstein after he'd served time for sex MIT's media lab director resigns after report on his ties to Jeffrey Epstein. The director is standing down after admitting to taking over 1.5 million dollars from Epstein, for himself and the An investigation in The New Yorker published on Friday revealed that Epstein secured at least $7.5 million in donations to MIT's Media Lab, run by Ito. Internal emails discovered by The New Yorker But the review finds that three MIT vice presidents learned of Epstein's donations to the MIT Media Lab, and his status as a convicted sex offender, in 2013. In the absence of any MIT policy regarding controversial gifts, Epstein's subsequent gifts to the Institute were approved under an informal framework developed by the three administrators, R. Gregory Morgan , Jeffrey Newton , and Israel Ruiz . Signe Swenson, a former development associate and alumni coordinator at the MIT media lab, told CNN on Saturday that she repeatedly expressed concern about MIT's ties to Jeffrey Epstein, but the Joichi Ito, the director of the MIT Media Lab, resigned on Saturday, one day after an article in The New Yorker reported the lab hid its financial relationship with the disgraced financier Jeffrey Two prominent researchers are quitting MIT's Media Lab over revelations that the renowned technology research hub and its director took money from Jeffrey Epstein after he'd served time for sex MIT Media Lab director Joichi Ito has faced pressure to resign after revealing that he took research funding from financier and alleged sex trafficker Jeffrey Epstein. But today Nicholas A spokesperson from the MIT Media Lab directed Business Insider to the open letter MIT's president wrote following the exposé, announcing an internal investigation.
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Sep 07, 2019 · The M.I.T. Media Lab, which has been embroiled in a scandal over accepting donations from the financier and convicted sex offender Jeffrey Epstein, had a deeper fund-raising relationship with Aug 27, 2019 · A group of prominent academics have signed a letter in support of MIT Media Lab director Joi Ito, as MIT reckons with the revelation that it accepted around $800,000 in funds from Jeffrey Epstein Aug 27, 2019 · M any of us are reeling from the recent news that MIT's Media Lab, where I work as a researcher, took funding from Jeffrey Epstein, the late financier who faced federal sex-trafficking charges Sep 08, 2019 · Joi Ito resigned following new allegations that the MIT Media Lab tried to hide the extent of its financial ties to Jeffrey Epstein. The new allegations were brought to light in a New Yorker Sep 18, 2019 · The director of MIT's Media Lab, Joi Ito, resigned over Jeffrey Epstein's donations, which senior university officials knew about and approved. (Phillip Faraone/Getty Images ) By Nina Strohminger MIT's $16.4bn endowment is envied by many universities, as is its $472m tally of gifts and pledges last year, but both numbers pale beside Stanford's. Meanwhile, the Media Lab needs $80m to MIT had reportedly listed Epstein, who supposedly hung himself while behind bars, as a "disqualified donor" but was still taking handouts from him, The New Yorker reports. Ito admitted last week (CNN) — Joi Ito, the director of the Media Lab at MIT, resigned Saturday and the university is calling for an independent investigation following explosive allegations that he and at least one Director.
Sep 8, 2019 Media Lab on Saturday after a New Yorker article alleged the lab concealed its ties to disgraced financier Jeffrey Epstein. Kimberly White / Getty
Ito told investigators that he Googled Epstein after meeting him, and consulted with various The New Yorker reported that Jeffrey Epstein directed a $2 million donation from Bill Gates to the MIT Media Lab, and the two have other connections. Jan 10, 2020 · But the review finds that three MIT vice presidents learned of Epstein's donations to the MIT Media Lab, and his status as a convicted sex offender, in 2013. Sep 11, 2019 · Epstein was "disqualified" from the donor base of the MIT Media Lab — something of an East Coast answer to the cash-rich tech optimism of Stanford — so Ito and the lab's director of Sep 07, 2019 · MIT's media lab director resigns after report on his ties to Jeffrey Epstein The director is standing down after admitting to taking over 1.5 million dollars from Epstein, for himself and the media Aug 21, 2019 · Jeffrey Epstein AP. A director at Massachusetts Institute of Technology's prestigious Media Lab is resigning — because he's "ashamed" over the research center's link to Jeffrey Epstein Sep 11, 2019 · The Epstein situation forced MIT Media Lab to evolve the sort of institutional culture that could keep Epstein secret — which meant, in the New Yorker piece, dismissing and ignoring the concerns Aug 21, 2019 · A member of the Massachusetts Institute of Technology Media Lab plans to resign after the research center and its director accepted money from Jeffrey Epstein, the deceased sex trafficker, the Sep 05, 2019 · MIT Media Lab director Joichi Ito has faced pressure to resign after revealing that he took research funding from financier and alleged sex trafficker Jeffrey Epstein.
Sep 08, 2019 · Signe Swenson, a former development associate and alumni coordinator at the MIT media lab, told CNN on Saturday that she repeatedly expressed concern about MIT's ties to Jeffrey Epstein, but the
In the absence of any MIT policy regarding controversial gifts, Epstein's subsequent gifts to the Institute were approved under an informal framework developed by the three administrators, R. Gregory Morgan , Jeffrey Newton , and Israel Ruiz . Signe Swenson, a former development associate and alumni coordinator at the MIT media lab, told CNN on Saturday that she repeatedly expressed concern about MIT's ties to Jeffrey Epstein, but the Joichi Ito, the director of the MIT Media Lab, resigned on Saturday, one day after an article in The New Yorker reported the lab hid its financial relationship with the disgraced financier Jeffrey Two prominent researchers are quitting MIT's Media Lab over revelations that the renowned technology research hub and its director took money from Jeffrey Epstein after he'd served time for sex MIT Media Lab director Joichi Ito has faced pressure to resign after revealing that he took research funding from financier and alleged sex trafficker Jeffrey Epstein. But today Nicholas A spokesperson from the MIT Media Lab directed Business Insider to the open letter MIT's president wrote following the exposé, announcing an internal investigation. Gates' former chief scientific The MIT Media Lab is all over the news for all the wrong reasons. Instead of its cutting-edge ideas drawing attention, a seedy financial relationship with convicted sex offender Jeffrey Epstein is Published Sep. 07, 2019 12:45AM ET Scandal has been swirling around the MIT Media Lab because of its ties to Jeffrey Epstein, with the prestigious university apologizing for taking $800,000 from Aug 15, 2019 I met Epstein in 2013 at a conference through a trusted business friend and, in my fundraising efforts for MIT Media Lab, I invited him to the Lab Jan 10, 2020 But the review finds that three MIT vice presidents learned of Epstein's donations to the MIT Media Lab, and his status as a convicted sex Sep 7, 2019 Director of M.I.T.'s Media Lab Resigns After Taking Money From Jeffrey Epstein.
MIT A member of the Massachusetts Institute of Technology Media Lab plans to resign after the research center and its director accepted money from Jeffrey Epstein, Sep 7, 2019 MIT Media Lab director resigns after criticism over financial ties to Jeffrey Epstein. MIT's president said an article in The New Yorker "contains Aug 22, 2019 Update (September 9): The New Yorker reported on Friday (September 6) that Jeffrey Epstein made more contributions to the MIT Media Lab Sep 8, 2019 The head of the the Massachusetts Institute of Technology's embattled Media Lab has resigned and the school has opened an investigation Sep 7, 2019 MIT Media Lab head Joichi Ito resigns over Epstein donations the academic centre's financial ties to the late US financier Jeffrey Epstein. MIT Sep 6, 2019 Joi Ito should be fired from MIT's Media Lab after taking funding from felon Jeffrey Epstein.
Media Lab, which has been embroiled in a scandal over Jeffrey Epstein, had a deeper fund-raising relationship with Epstein than it Dec 22, 2020 The Media Lab said in an August 2019 statement that MIT had received around $800,000 in donations from Epstein over 20 years. Later, Ito Aug 22, 2019 Accused sex trafficker Jeffrey Epstein, who died in federal custody this month, allegedly took a predatory interest in teenage girls. But his Sep 7, 2019 Joi Ito, the director of the influential MIT Media Lab, submitted his women who survived the abuse of Jeffrey Epstein," the foundation tweeted. Sep 10, 2019 Joichi Ito has stepped down as director of the Massachusetts Institute of Technology's Media Lab after The New Yorker magazine claimed he Sep 8, 2019 This segment aired on September 8, 2019. Related: Director Of MIT Media Lab Resigns Over Financial Ties To Jeffrey Epstein · MIT's Media Lab Sep 7, 2019 The head of the MIT Media Lab resigned Saturday following fresh and financier Jeffrey Epstein, leaving the university and its acclaimed Aug 19, 2019 Joi Ito, head of the MIT Media Lab, apologized for taking investment money and donations from the now-deceased convicted sex offender. MIT A member of the Massachusetts Institute of Technology Media Lab plans to resign after the research center and its director accepted money from Jeffrey Epstein, Sep 7, 2019 MIT Media Lab director resigns after criticism over financial ties to Jeffrey Epstein. MIT's president said an article in The New Yorker "contains Aug 22, 2019 Update (September 9): The New Yorker reported on Friday (September 6) that Jeffrey Epstein made more contributions to the MIT Media Lab Sep 8, 2019 The head of the the Massachusetts Institute of Technology's embattled Media Lab has resigned and the school has opened an investigation Sep 7, 2019 MIT Media Lab head Joichi Ito resigns over Epstein donations the academic centre's financial ties to the late US financier Jeffrey Epstein.
Aug 22, 2019 · MIT Media Lab is in upheaval after the disclosure that its organization accepted financial support from now-deceased pedophile Jeffrey Epstein. Ethan Zuckerman announced Tuesday he was moving his work out of the MIT Media Lab by the end of May 2020. The revelation that MIT's Media Lab aggressively sought the financial support of the convicted sex offender Jeffrey Epstein, and tried to keep his donations secret, has left the once-prestigious Jan 10, 2020 · Afterward, a Media Lab staff member shared photos of the memorial with the note, "Feel free to post on social media—as long as Jeffrey Epstein does not appear in any of the photos!" Sep 05, 2019 · Jeffrey Epstein's Donations Create a Schism at M.I.T.'s Revered Media Lab The Media Lab, a prominent research center at M.I.T., was trying to move past questions about its ties to the financier Sep 11, 2019 · Development support staff are rarely in the limelight, even within their own organizations. But Signe Swenson has had a whirlwind of a week. The former development associate at the MIT Media Lab helped inform New Yorker reporter Ronan Farrow's exposé about the center's financial ties with the late Jeffrey Epstein, the financier and convicted sex offender. CAMBRIDGE, MA—Shortly after it became widespread public knowledge that the research institution had accepted contributions from the late convicted sex offender, the MIT Media Lab announced Monday that it had agreed to return all of Jeffrey Epstein's donated girls. "As soon as we learned that several high-level Lab officials had accepted underage girls on Mr. Epstein's behalf and then Nov 04, 2019 · Epstein reportedly made two donations to the MIT Media Lab that were worth $1.725 million, and this was after his 2008 conviction.
Sep 06, 2019 · Writer Anand Giridharadas went on Twitter to explain he was cutting ties with MIT's Media Lab after revelations its leader had taken more than $1.5 million from Jeffrey Epstein. Emails between officials at MIT obtained by The New Yorker indicated that Gates' $2 million gift to the Media Lab in October 2014 was "directed" by Epstein, whose name was nonetheless not Sep 16, 2019 · Epstein gave Mediated Matter Lab $125,000. Oxman said: "From Epstein's gifts to the Media Lab, my group received $125,000 with MIT's requirement that it be kept confidential so as to not enhance Aug 22, 2019 · Here are the core facts, as best as we can determine: Over the course of 20 years, MIT received approximately $800,000 via foundations controlled by Jeffrey Epstein. All of those gifts went either to the MIT Media Lab or to Professor Seth Lloyd. Aug 22, 2019 · MIT Media Lab is in upheaval after the disclosure that its organization accepted financial support from now-deceased pedophile Jeffrey Epstein. Ethan Zuckerman announced Tuesday he was moving his work out of the MIT Media Lab by the end of May 2020.
Gates asked Sep 8, 2019 Media Lab on Saturday after a New Yorker article alleged the lab concealed its ties to disgraced financier Jeffrey Epstein. Kimberly White / Getty Sep 7, 2019 Joichi Ito, the director of the Media Lab at MIT, admitted that he accepted a $525,000 donation from Epstein after he pleaded guilty in 2008 to Oct 4, 2019 Michael Bove was terminated last week, further roiling a center already in turmoil over ties to convicted sex offender Jeffrey Epstein. Sep 7, 2019 MIT Media Lab head Joichi Ito resigns over Epstein donations the academic centre's financial ties to the late US financier Jeffrey Epstein.
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FILE - This March 28, 2017 , Sep 10, 2019 lawyers to investigate the university's ties to businessman Jeffrey Epstein. The move follows the resignation of the head of the MIT Media Lab. Sep 7, 2019 Director of MIT's Media Lab steps down over Epstein ties photo, provided by the New York State Sex Offender Registry shows Jeffrey Epstein.
Signe Swenson, a former development associate and alumni coordinator at the MIT media lab, told CNN on Saturday that she repeatedly expressed concern about MIT's ties to Jeffrey Epstein, but the Joichi Ito, the director of the MIT Media Lab, resigned on Saturday, one day after an article in The New Yorker reported the lab hid its financial relationship with the disgraced financier Jeffrey Two prominent researchers are quitting MIT's Media Lab over revelations that the renowned technology research hub and its director took money from Jeffrey Epstein after he'd served time for sex MIT Media Lab director Joichi Ito has faced pressure to resign after revealing that he took research funding from financier and alleged sex trafficker Jeffrey Epstein. But today Nicholas A spokesperson from the MIT Media Lab directed Business Insider to the open letter MIT's president wrote following the exposé, announcing an internal investigation. Gates' former chief scientific The MIT Media Lab is all over the news for all the wrong reasons.
Signe Swenson, a former development associate and alumni coordinator at the MIT media lab, told CNN on Saturday that she repeatedly expressed concern about MIT's ties to Jeffrey Epstein, but the Joichi Ito, the director of the MIT Media Lab, resigned on Saturday, one day after an article in The New Yorker reported the lab hid its financial relationship with the disgraced financier Jeffrey Two prominent researchers are quitting MIT's Media Lab over revelations that the renowned technology research hub and its director took money from Jeffrey Epstein after he'd served time for sex MIT Media Lab director Joichi Ito has faced pressure to resign after revealing that he took research funding from financier and alleged sex trafficker Jeffrey Epstein. But today Nicholas A spokesperson from the MIT Media Lab directed Business Insider to the open letter MIT's president wrote following the exposé, announcing an internal investigation. Gates' former chief scientific The MIT Media Lab is all over the news for all the wrong reasons. Instead of its cutting-edge ideas drawing attention, a seedy financial relationship with convicted sex offender Jeffrey Epstein is Published Sep. 07, 2019 12:45AM ET Scandal has been swirling around the MIT Media Lab because of its ties to Jeffrey Epstein, with the prestigious university apologizing for taking $800,000 from Aug 15, 2019 I met Epstein in 2013 at a conference through a trusted business friend and, in my fundraising efforts for MIT Media Lab, I invited him to the Lab Jan 10, 2020 But the review finds that three MIT vice presidents learned of Epstein's donations to the MIT Media Lab, and his status as a convicted sex Sep 7, 2019 Director of M.I.T.'s Media Lab Resigns After Taking Money From Jeffrey Epstein. Sep 11, 2019 Why MIT Media Lab thought it was doing right by secretly accepting Jeffrey Epstein's money. Sometimes very smart people have a very bad idea. Jan 16, 2020 The revelation that MIT's Media Lab aggressively sought the financial support of the convicted sex offender Jeffrey Epstein, and tried to keep his Nov 21, 2019 Leon Black's Art Collecting Company Paid Millions of Dollars to Jeffrey Epstein: Report · Nancy Duvergne Smith, "Deploy or Die—Media Lab Sep 7, 2019 The M.I.T.


text:
Jason Jaspers (* 8. April 1981 in Thunder Bay, Ontario) ist ein deutsch-kanadischer Eishockeyspieler und -trainer, der zuletzt bei den Grizzlys Wolfsburg aus der Deutschen Eishockey Liga unter Vertrag stand.

Seit der Saison 2020/21 trainiert er den dänischen Erstligisten Esbjerg Energy.

Karriere
Jaspers wechselte 1998 von den Thunder Bay Kings zu den Sudbury Wolves, ein Team aus der kanadischen Profijuniorenliga Ontario Hockey League. Für die Wolves spielte er bis 2001, in seiner letzten Spielzeit in der OHL schaffte er den Sprung ins OHL-Second-All-Star-Team und gewann zudem OHL-Plus/Minus Award. Beim NHL Entry Draft 1999 war Jaspers in der dritten Runde an Position 71 von den Phoenix Coyotes gezogen worden, für die er in der folgenden Saison seine ersten drei NHL-Einsätze absolvierte. Die meiste Zeit spielte er allerdings bei den Springfield Falcons, dem damaligen Farmteam der Coyotes in der American Hockey League. An dieser Tatsache änderte sich auch in den folgenden Jahren nichts, da es Jaspers nicht gelang, einen Stammplatz im NHL-Kader zu erhalten. 2004 stand er aus diesem Grund das bislang letzten Mal in der höchsten nordamerikanischen Profiliga auf dem Eis.

Aufgrund mangelnder Perspektive in Nordamerika plante Jaspers bereits zu dieser Zeit, seine Karriere in Deutschland fortzusetzen, ein Transfer nach Nürnberg scheiterte jedoch, sodass er weiter in der AHL spielte. Nach der Saison 2005/06 wechselte Jaspers dann von den Falcons für zunächst ein Jahr zu den Adler Mannheim, mit denen er 2007 die deutsche Meisterschaft gewann. Sein Vertrag in Mannheim wurde bis 2009 verlängert.

Zur Saison 2009/10 wechselte Jason Jaspers zu den Kölner Haien, wo er zunächst einen Ein-Jahres-Vertrag unterschrieb, welcher jedoch anschließend um zwei weitere Spielzeiten verlängert wurde. Im April 2012 wechselte er zu den Nürnberg Ice Tigers. Im Juni 2015 wechselt er zur neuen Saison zu den Iserlohn Roosters. Nach einer starken Saison in Iserlohn verlängerte er seinen Vertrag bei den Roosters um ein Jahr und wurde nach dem Abgang von Mike York zum Mannschaftskapitän ernannt.

Nach drei Jahren in Iserlohn nahm er an der Saisonvorbereitung bei den Eisbären Berlin teil und erhielt im September 2018 einen Einjahresvertrag. Am 10. Oktober 2018 wechselte er zu den Grizzlys Wolfsburg.

Erfolge und Auszeichnungen

 2000 OHL Second All-Star Team
 2001 Bronzemedaille bei der U20-Junioren-Weltmeisterschaft
 2007 Deutscher Meister mit den Adler Mannheim

Karrierestatistik

Weblinks

Einzelnachweise

Eishockeyspieler (Sudbury Wolves)
Eishockeyspieler (Utah Grizzlies, AHL)
Eishockeyspieler (Springfield Falcons)
Eishockeyspieler (Phoenix Coyotes)
Eishockeyspieler (Adler Mannheim)
Eishockeyspieler (Kölner Haie)
Eishockeyspieler (Nürnberg Ice Tigers)
Eishockeyspieler (Iserlohn Roosters)
Eishockeyspieler (Eisbären Berlin)
Eishockeyspieler (Grizzlys Wolfsburg)
Eishockeytrainer (Dänemark)
Person (Esbjerg Energy)
Deutscher Meister (Eishockey)
Deutscher
Kanadier
Geboren 1981
Mann

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Should You � Exercise 💪when You Are Sick 🤒?


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Nike Reveals Tokyo Olympics Collection
Those of us who haven't been living under a rock-hard rock for the past few days may have noticed this thing called The Olympic Games, or The Olympics for short. It's been everywhere: on the TV, on every news site, at bars, brought up in friendly small talk; it seems as though there's just no getting around it. So if you can't beat them, why not join them? And while this definitely may require a change of attitude on our part, it's a given for Nike and other sportswear brands who thrive on the popularity and screentime of such events.
Gettyimages / Bennett Raglin / Getty Images Entertainment
That being said, it should come as no surprise that Nike has sponsored pretty much every athlete on god's green Earth and that they've made their 2021 Tokyo Olympics collection available for the public at large. One of the most notable items on their Tokyo Olympics catalog would be the incredibly wide array of colorful and futuristic sneakers they've released. Whether they're outrageously pink (in a good way), asymmetrically colored, futuristic and oddly shaped, or just plain glitchy, the new Nike sneakers have got to be some of the most creative and remarkable pieces of footwear we've seen in quite a while now.
The Nike Tokyo Olympics fashion show was held in order to showcase these outlandish pieces of fashion. The event was attended by such A-List stars as Drake and Rosalia, the former being a vocal advocate of the brand's signature style. And these are just two of the many instantly recognizable names in attendance. Nike has been garnering an ever-growing list of notable personalities whom they sponsor, which makes their actual fashion events quite the spectacle when all those A-Listers actually show up. The Tokyo Olympics runway was definitely one of those notable fashion moments that we'll be talking about in the near future.
Healthy Snacks for Study Dates
With exam season around the corner, group study sessions and all-nighters are inevitable. However, powering through these sessions and staying motivated can take a lot of effort. Spicing up the study sessions with creative and energizing snacks can help you, and your group members stay focused for prolonged periods and turn them into the ultimate study date with the right foods. The key to keeping yourself from getting tired is to consume healthy foods. And healthy foods do not necessarily have

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text:
\section{Introduction}
\label{sec:intro}

Strongly gravitationally lensed quasars with image separations $\gtrsim 10"$ are exceptionally rare. Such large image splittings
require a lensing mass corresponding to a galaxy cluster, and a fortuitous close line-of-sight alignment of such a mass distribution and a background
quasar. In fact, only two such systems have previously been discovered, \QSOLone \, (Inada et al.\ 2003) with a maximum image separation of $14\farcs 6$ and \QSOLtwo \, (Inada et al.\ 2006)
with a maximum image separation of $22\farcs 5$. Such systems provide unique information on the abundances and internal structure of galaxy clusters, yielding stringent tests of the
current $\Lambda$CDM paradigm, both through their observed abundances (e.g., Hennawi et al.\ 2007), the relative fractions of different image multiplicities (e.g., Oguri \& Keeton 2004), and from detailed models
of the cluster mass distribution based on the available constraints (e.g., Sharon et al.\ 2005; Oguri 2010; Oguri et al.\ 2012),
including measured time delays between the quasar images (Fohlmeister et al.\ 2008, 2012). Being effectively point sources, the positions of multiply lensed quasar images provide mass modelling constraints which are free from the ambiguities which sometimes plague the identification of multiple images of strongly lensed galaxies, particularly the fainter de-magnified images located closest to the mass center.

As shown by Refsdal (1964), the relative time delays of multiple quasar images visible around the lensing mass center can provide an estimate of the Hubble parameter $H_0$. However,
as $H_0$ is presently increasingly well constrained by a host of methods, including gravitational lensing time delays from galaxy-scale lenses, the main interest of quasar time delays are
related to their ability to provide unique detailed constraints on the slope of the projected matter density distribution over the range of radii where the quasar images are found (e.g., Refsdal 2004).

In this paper, we present the discovery of a third lensing system
where a quasar is being multiply lensed by a galaxy cluster, but with
a higher image multiplicity than the previously known such
systems. The discussion in subsequent sections of this paper describes
the evidence for the lensing interpretation of this system and the
identification of an increasing number of components in the lensing
system, through analysis of progressively deeper photometric and
spectroscopic data, coupled with parametric modelling of the lens.

In \S~\ref{sec:ima1} we describe the initial identification of \QSO \,
as a likely gravitational lens system in the course of a larger survey
for strong cluster lenses.  The spectroscopic confirmation of the
three brightest lensed images of the quasar is outlined in
\S~\ref{sec:ABCspec}, and \S~\ref{sec:DEF} details the evidence for
three additional fainter quasar images from deeper imaging of the
field, coupled with further spectroscopic observations. In
\S~\ref{sec:phot} we report photometry of the quasar images, some
showing significant brightness changes over a time span of one
year. In \S~\ref{sec:cluster} we provide a summary of the observed
properties of the lensing cluster, and in \S~\ref{sec:model} we
develop a parametric model of the lens system, which is used to
predict time delays. Our main results are summarized in
\S~\ref{sec:discuss}.  Unless otherwise noted, throughout this work we
assume an $\Omega_m = 0.3$, $\Omega_{\Lambda} = 0.7$, $H_0 = 70$ km
s$^{-1}$ cosmology.

\section{Lens candidate selection and initial imaging}
\label{sec:ima1}

We have undertaken a search for cluster lenses, the Sloan Giant Arcs Survey (SGAS; Hennawi et al.\ 2008; Bayliss et al.\ 2011; Gladders et al.\ in prep.\ 2012), based on public data from the Sloan Digital Sky Survey (SDSS; York et al.\ 2000).
Potential lines of sight for lensing by clusters are identified by running an automated cluster finding algorithm on the SDSS imaging data. This is followed by visual inspection,
by multiple persons in our collaboration, of color images of these lines of sight, generated from the SDSS data. New lens candidates are flagged and given a grade according to the likelihood of
being a true lens, and a final grade is calculated for each lens candidate. The list of lens candidates is then checked against public data bases such as the NASA/IPAC Extragalactic Database,
and remaining candidates after removal of known lenses are targeted for deeper follow-up imaging. In September 2011, we targeted such lens candidates selected from the SDSS Data Release 8 (Aihara et al.\ 2011)
using the MOsaic CAmera (MOSCA) at the 2.56m Nordic Optical Telescope (NOT). MOSCA is a $2\times 2$ mosaic of four $2048 \times 2048$ Loral-Lesser thinned CCDs with excellent blue sensitivity
(Quantum Efficiency $> 90\%$ across the SDSS $g$-band), mounted at the Cassegrain focus of the telescope. MOSCA is normally used in $2\times 2$ binned mode, yielding a pixel scale
of $0.217\arcsec {\rm pixel}^{-1}$ and a total field of view of $7\farcm 7 \times 7\farcm 7$.

\begin{deluxetable*}{lccc}
\tabletypesize{\footnotesize}
\tablecaption{ Log of NOT/MOSCA imaging observations\label{tab:MOSCAlog}}
\tablehead{
\colhead{Epoch } & \colhead{Filter}    & \colhead{Exposure time}  & \colhead{FWHM}
}
\startdata
\hline \\
{\bf 2011 Sep.\ 24.93 UT} & $g$ & $2\times 300$s & $0\farcs 87$ \\
{\bf 2011 Sep.\ 24.94 UT} & $r$ & $2\times 150$s & $0\farcs 81$ \\
{\bf 2011 Sep.\ 24.95 UT} & $i$ & $2\times 150$s & $0\farcs 74$ \\
\hline \\
{\bf 2012 Sep.\ 13.97 UT} & $u$ & $3\times 600$s & $0\farcs 81$ \\
{\bf 2012 Sep.\ 12.96 UT} & $g$ & $3\times 600$s & $0\farcs 70$ \\
{\bf 2012 Sep.\ 13.04 UT} & $r$ & $3\times 300$s & $0\farcs 68$ \\
{\bf 2012 Sep.\ 12.95 UT} & $i$ & $3\times 300$s & $0\farcs 61$ \\
\hline \\
{\bf 2012 Sep.\ 15.98 UT} & $g$ & $3\times 600$s & $0\farcs 68$ \\
\end{deluxetable*}

\QSO \, was imaged using MOSCA in September 2011 (see Table~\ref{tab:MOSCAlog} for details)
with our nominal survey exposure time of $2\times 300$s in the $g$-band. Based on a visual inspection of the raw data, it was noted as a probable lens,
and subject to immediate follow-up with $2\times 150$s exposures in each of the SDSS $r$- and $i$-bands. In addition to the apparent blue arc south of the cluster core,
three blue stellar images (labelled ``A'',''B'', and ''C'' in Figure~\ref{fig:Firstepoch}) located at similar cluster-centric radii as the arc,
were considered as candidate multiple images of a gravitationally lensed quasar.
In addition, three red galaxies,
labelled ``G1-G3'' in Figure~\ref{fig:Firstepoch}, were seen in the cluster core.
Publicly available photometric redshift estimates from SDSS (see Table~\ref{tab:astrom}) indicated that all three galaxies are consistent with being located in a cluster at $z\sim 0.50$.

The stellar source (labelled ``WD'' in Figure~\ref{fig:Firstepoch}) of magnitude $g=21.09$, similar in apparent brightness to A and B, seen superposed on the giant arc, was also noted as a candidate quasar image.
Although this image has a significantly redder color ($g-i = 1.33$) than A and B, it might be considerably reddened by extinction in galaxies (the galaxy corresponding to the arc being one potential
such candidate) along its line of sight, and it was kept as a target for future spectroscopic follow-up.

\begin{figure*}
\begin{center}
\includegraphics[angle=0,scale=.60]{Firstepoch.pdf}
\end{center}
\caption[NOT/ALFOSC spectra of the three brightest quasar images.]
{NOT/MOSCA $gri$ color composite image of \QSO \, from our initial epoch of photometry (see Table~\ref{tab:MOSCAlog}).}
\label{fig:Firstepoch}
\end{figure*}

\begin{deluxetable*}{lcccccccc}
\tabletypesize{\footnotesize}
\tablecaption{ SDSS DR8 astrometry, photometry, and photometric redshift estimates for the three brightest quasar images and three brightest galaxies in \QSO \label{tab:astrom}}
\tablehead{
\colhead{Object} & \colhead{RA}    & \colhead{Dec}  & \colhead{u} & \colhead{g} & \colhead{r} & \colhead{i} & \colhead{z} &  \colhead{Photometric} \\
      & \colhead{(h m s)} & \colhead{(d m s)}  & \colhead{SDSS} &  \colhead{SDSS} & \colhead{SDSS} & \colhead{SDSS} & \colhead{SDSS} &  \colhead{redshift}
}
\startdata
\hline \\
A            & 22:22:09.04 & +27:45:37.9 & 24.55$\pm$0.93 & 21.10$\pm$0.03 & 20.67$\pm$0.04 & 20.87$\pm$0.07 & 21.00$\pm$0.27 & \nodata \\
B            & 22:22:08.80 & +27:45:40.0 & 22.07$\pm$0.19 & 21.43$\pm$0.04 & 21.03$\pm$0.05 & 21.27$\pm$0.10 & 21.08$\pm$0.29 & \nodata \\
C            & 22:22:07.90 & +27:45:37.8 & 24.50$\pm$0.93 & 21.51$\pm$0.05 & 21.14$\pm$0.05 & 21.28$\pm$0.10 & 22.14$\pm$0.63 & \nodata \\
G1            & 22:22:08.57 & +27:45:35.6 & 25.42$\pm$2.41 & 20.92$\pm$0.08 & 19.00$\pm$0.03 & 18.05$\pm$0.02 & 17.65$\pm$0.05 & 0.485$\pm$0.015 \\
G2            & 22:22:08.70 & +27:45:33.0 & 24.33$\pm$1.01 & 22.13$\pm$0.08 & 20.86$\pm$0.05 & 19.88$\pm$0.04 & 19.33$\pm$0.07 & 0.528$\pm$0.157 \\
G3            & 22:22:08.62 & +27:45:29.9 & 24.39$\pm$2.32 & 22.28$\pm$0.20 & 20.43$\pm$0.07 & 19.48$\pm$0.05 & 19.13$\pm$0.16 & 0.509$\pm$0.031 \\
\tablecomments{Epoch: 2009 October 18.19 UT}
\end{deluxetable*}

\section{Follow-up observations and results}
\label{sec:results}

\subsection{Spectroscopic confirmation of the three brightest quasar images}
\label{sec:ABCspec}

The spectroscopic observations described in this paper were obtained using the Andalucia Faint Object Spectrograph and Camera (ALFOSC) at the NOT. We used grism \# 4, covering a wavelength range
$3800 {\rm {\AA}} - 9000 {\rm {\AA}}$ with a resolution of about $R=350$ and dispersion 3.0 {\AA} pixel$^{-1}$. The ALFOSC pixels were binned by a factor of two in the dispersion direction
but kept unbinned at the native pixel scale of 0\farcs 188 pixel$^{-1}$ in the spatial direction. The slit width was 1\farcs 3. Redwards of $\sim 7000$ {\AA} strong fringing is present in the spectra, effectively
restricting the upper limit of the spectral range to this value unless special care is taken during the observations to suppress the effects of fringing. An order-sorter filter was used to suppress
second-order contamination in the spectra.

On August 21-22, 2012, a series of ALFOSC spectra were obtained in the area of \QSO : Three 1200s spectra were obtained with the rotation angle set to provide simultaneous coverage of
the A and B images. In addition, two single spectra of 1000s exposure time were obtained to simultaneously cover image C and galaxy G1 and image B and image C, respectively.
Finally, the blue giant arc and the stellar source superposed on it (labelled ``WD'' in Figure~\ref{fig:Firstepoch}) were observed for a total exposure time $3\times 1000$s.
The spectra were wavelength calibrated using He$+$Ne arc lamps and flux calibrated based on observations of the spectrophotometric standard star BD$+$33~2642.
As shown in Figure~\ref{fig:Johanfig} the three images A,B, and C all have identical spectra modulo noise, containing typical spectral features of a quasar (e.g., Vanden Berk et al.\ 2001) with a set of
prominent emission lines, redshifted to $z=2.82$. This demonstrates that the lensing interpretation is correct for these three quasar images.
\begin{figure}
\plotone{Lens.pdf}
\caption[NOT/ALFOSC spectra of the three brightest quasar images.]
{NOT/ALFOSC spectra of the three brightest quasar images A-C. The most prominent quasar emission lines, redshifted to $z=2.82$, are indicated in the figure.}
\label{fig:Johanfig}
\end{figure}

Despite having a significantly redder color, the stellar source superposed on the giant arc was also
targeted for ALFOSC spectroscopy as a potential additional image of the quasar. Although a significant continuum was detected, emission lines were completely absent at the wavelengths
of the prominent quasar emission lines in the A,B, and C component spectra. A more careful analysis of the spectrum reveals the typical signatures of a DZ white dwarf (e.g., Koester et al.\ 2011).

\subsection{Identification of the D, E and F images}
\label{sec:DEF}

Having confirmed the three images A-C as gravitationally lensed images
of the same quasar, two alternative image configurations may be
considered: \QSO \, is either a naked cusp lens with three quasar
images, similar to \QSOLtwo \, (Oguri et al.\ 2008) or a five-image
system similar to \QSOLone \, (Inada et al.\ 2008). Being able to
distinguish between the two cases is important, not only for the
understanding of the \QSO \, lens system itself, but also in the
context of using the statistics of cluster-lensed quasars as a
cosmological tool. Naked cusps, i.e., lensing configurations where the source lies on a
tangential caustic that extends outside a radial caustic, are extremely
rare among galaxy-scale lenses, the only known candidate among $~\sim
100$ such lens systems being APM~08279$+$5255 (Lewis et
al.\ 2002). However, due to their shallower central matter density
slopes, naked-cusp lenses are expected to be much more common for
clusters than for galaxies.  Oguri \& Keeton (2004) predicted that
$30-60\% $ of all cluster lenses will be of this type, the fraction
depending on the central slope and triaxiality of clusters.

To further investigate the lensing system configuration of \QSO \, we
searched our initial MOSCA imaging for potential stellar sources with
blue colors consistent with the quasar. A blue source, labelled ``D''
in Figure~\ref{fig:Firstepoch}, was identified just south of, and
partially superposed on, galaxy G2. The source was apparently stellar,
but the modest exposure time and overlap with G2 made this conclusion
somewhat uncertain.  A set of deeper $ugri$ images in better seeing
was obtained at the NOT in September 2012 (see
Table~\ref{tab:MOSCAlog}). These images revealed image D to have a
clearly stellar point-spread-function (PSF), motivating further
spectroscopic follow-up of this image. On 2012 September 16-17 UT, a
series of $8 \times 2400$s integrations were made using ALFOSC, using
the same setup as for the earlier observations described in
\S~\ref{sec:ABCspec}.  The telescope pointing was dithered along the
slit between exposures to improve fringe suppression at the red end of
the spectrum. The spectra were flux calibrated based on observations
of the spectrophotometric standard star BD$+$33~2642.

The slit orientation is illustrated in Figure~\ref{fig:Slitpos},
providing simultaneous spectroscopic coverage of images B and D,
galaxies G2 and G3, and the giant arc.  Inspection of the reduced 2D
spectrum (see Figure~\ref{fig:2Dspec}) reveals the strong spectral
line in the quasar B image around 4640~{\AA}, corresponding to
Lyman-alpha at the redshift of the quasar.  A Lyman-alpha line is also
clearly evident at this wavelength in the spectrum of the D image,
confirming its identification as a gravitationally lensed image of the
quasar.  More surprisingly, a Lyman-alpha line at the same redshift is
also seen superposed on the spectrum of galaxy G3, providing clear
indication of a fifth (E) quasar image spatially coincident with this
galaxy. The extracted 1D spectra of image D and E in a $\sim
1200${\AA} wide region surrounding the Lyman-alpha line of the quasar
are plotted in Figure~\ref{fig:DEFspecs}: A clear peak is seen at the
location of the Lyman-alpha line in both the D and E image
spectra. Redward of this line, there is some visible discrepancy in
the slopes of the two spectra. This discrepancy is caused by the
spatial superposition of image E and the red galaxy G3, the latter
having a continuum which is rising towards longer wavelengths.

Figure~\ref{fig:gisub} shows a scaled subtraction of the second epoch
$i$-band image from the $g$-band image (see
Table~\ref{tab:MOSCAlog}). The PSF of the $i$-band image was matched
to that of the $g$-band image by convolving it with an elliptical
gaussian kernel. The $i$-band image was then scaled so that the
subtraction optimally removes the light of galaxies G1-G3. Any
remaining flux, shown in the negative in Figure~\ref{fig:gisub}, is
bluer than galaxies G1-G3, and should be considered candidate images
of the quasar.

In Figure~\ref{fig:gisub}, image D is obvious. A comparison of this
residual image to the residual quasar images A-C shows that it has a
PSF consistent with a point source, as expected. Additionally there is
excess blue flux at the spectroscopically indicated position of image
E; this flux is obviously extended however. Figure~\ref{fig:uzoom},
which shows the $u$-band image with contours from the $g$-$i$
subtraction overlayed, shows the reason for this; the excess blue
light is a combination of light from the core of galaxy G3, and offset
from this, excess blue light attributable to image E.

Finally, in Figure~\ref{fig:gisub} there is also an additional blue
excess source, near galaxy G1, which we label F in
Figures~\ref{fig:gisub} and ~\ref{fig:uzoom}. This source is
consistent with being a point source. One of the slit placements from
the initial spectroscopic observations includes this possible quasar
image, and Figure~\ref{fig:DEFspecs} includes a spectrum extracted
at that location. The extracted spectrum suggests the presence of
Ly$\alpha$ emission; taken together, the imaging and spectroscopic
data suggest that this source is a sixth image of the quasar.

\begin{figure}
\includegraphics[angle=0,scale=.40]{Slitpos_annotated2.pdf}
\caption[.]  {Position of the slit for spectroscopic observations of
  \QSO \, using ALFOSC in September 2012. The field of view and
  orientation is the same as for Figure~\ref{fig:Firstepoch}. The
  background image is a 1h $g$-band MOSCA image combining all
  exposures obtained in this passband in September 2012 (see
  Table~\ref{tab:MOSCAlog}).}
\label{fig:Slitpos}
\end{figure}

\begin{figure}
\includegraphics[angle=0,scale=.35]{2Dspec.pdf}
\caption[.]  {Reduced 2D spectrum with slit orientation as shown in
  Figure~\ref{fig:Slitpos}. The brightest spectrum near the bottom is
  the B image of the quasar. The locations of other sources along the
  slit are indicated along the left margin.  The D and E images (the
  latter superposed on the spectrum of galaxy G3) display clear
  Lyman-alpha emission lines at the same redshift as the B image. The
  image has been gaussian smoothed on a scale of FWHM$=12${\AA} in the
  spectral direction and FWHM$=0.4\arcsec$ in the spatial direction.}
\label{fig:2Dspec}
\end{figure}

\begin{figure}
\includegraphics[angle=0,scale=.35]{DEFG2specs.pdf}
\caption[.]  {Spectra of the D, E, and F images and galaxy G2, showing
  the spectral region surrounding the Lyman-alpha emission line. The
  wavelength of Lyman-alpha at the $z=2.82$ redshift of the quasar is
  indicated by the vertical dotted line. To dampen small-scale noise
  the spectra have been smoothed with a Gaussian filter of
  FWHM$=18${\AA}.  }
\label{fig:DEFspecs}
\end{figure}

\begin{figure}
\plotone{newfig5.pdf}
\caption[.]  {Residuals after subtracting the second-epoch stacked
  $i$-band image from the $g$-band image. Prior to the subtraction,
  the $i$-band image was PSF-matched by convolution with an elliptical
  gaussian kernel and then scaled to match the $g$-band flux of
  galaxies G1-G3. The field of view and orientation is the same as for
  Figure~\ref{fig:Firstepoch}. To indicate the locations of the
  galaxies we also show intensity contours from the $i$-band
  image. Objects with excess blue light in the cluster core are
  candidate quasar images. Images A-E are clearly confirmed by
  spectroscopy and readily visible in this image subtraction; a
  possible sixth quasar image (F) is also indicated.}
\label{fig:gisub}
\end{figure}

\begin{figure}
\plotone{newfig6.pdf}
\caption[.]  {A zoomed view - 4$\times$ finer than
  Figure~\ref{fig:gisub} - of the $u$-band image. Red contours, as
  in Figure~\ref{fig:gisub}, show the second epoch $i$-band
  image. Blue contours show the residual $g$-$i$ shown in greyscale in
  Figure~\ref{fig:gisub}. Note that at the position of image E, the
  residual blue light is extended, and that it partially coincides
  with an excess of $u$-band light that is most prominent at the
  center of galaxy G3. The peak of the excess blue light in $g$-$i$ is
  offset from the center of G3; we interpreted this light as the sum
  of an image of the quasar (E) and a blue core in galaxy G3.}
\label{fig:uzoom}
\end{figure}

\subsection{Photometry of Quasar Images}
\label{sec:phot}

To achieve the most accurate photometry of images of the quasar, we
have constructed a model of the lensing cluster core using GALFIT
(Peng et al.\ 2010). The input PSF for each of the models discussed
below was in all cases constructed by fitting bright, isolated and
unsaturated stars using a multi-component Moffat profile using
GALFIT. Typically 3 Moffat components were used; we have explored the
effects of PSF reference star selection and find that it introduces an
uncertainty of less than 0.01 magnitudes for the brighter quasar
images, with no significant biases.

The cluster core model was constructed initially using a stack of the
second epoch $g$, $r$ and $i$ images. Sources were placed initially at
locations of obvious galaxies, and at the six quasar image positions
discussed above.  Quasar images are PSF components, and all galaxies
are S\'{e}rsic profile components. We continued adding components to
the model iteratively at the locations of any significant residuals
revealed by the modeling process, until a final complete model
incorporating all significant sources was achieved. This model was then
translated to individual epoch and filter images by transforming the
image coordinates to match the image to be analyzed, fixing those
coordinates, and then refitting the model component magnitudes, sizes
and shapes to the image to be analyzed.

The modeling process described above reveals that the images of the
quasar include a contribution from the underlying host galaxy, as is
seen in the two other quasars strongly lensed by galaxy clusters
(Inada et al. 2005; Oguri et al. 2012). The data show that the host
galaxy is blue - unlike the red hosts seen in the other two
quasar-cluster lenses - and is most clearly seen in the brightest (and
thus most likely the most magnified) image A. Figure 8 shows residuals
from a GALFIT model for image A in which only a PSF component is used,
and a second model consisting of a PSF component plus a single
S\'{e}rsic component; this second model is a much better fit.

\begin{figure}
\plottwo{fig8a.pdf}{fig8b.pdf}
\caption[.]  {Left Panel: The residuals in a 40$\times$40 pixel region
  from the $g$-band image resulting from a single PSF GALFIT model
  centered on image A. Right Panel: the same region fit by a
  PSF+S\'{e}rsic profile. Note that the PSF-only fit clearly indicates
  the presence of an underlying host galaxy component, and that it is
  oriented tangentially to the cluster center, as expected, and that
  this component is well fit by a single S\'{e}rsic profile.
 }
\label{fig:hostgal}
\end{figure}

In the $g$-band, including the host galaxy makes the fitted quasar
0.086 magnitudes fainter. In our judgement, none of the other images
of the quasar allow for clear modeling of the host galaxy component -
image B is bright enough, but complicated by a second galaxy less than
two arcseconds to the north, and images C-F are insufficiently
magnified. Thus, for images B-D, we proceed by measuring the quasar
brightness using a simple PSF-only fit in GALFIT, and then correct
each measured magnitude fainter by the host galaxy contribution as
measured from image A. Though the quasar and host magnifications are
not expected to be identical across the images, and the quasar/host
ratio will not be completely fixed due to temporal variation of the
quasar (see below), this simple procedure nevertheless avoids
systematic noise that would be introduced by attempting to model the
host galaxy independently in multiple images. For reference, in
addition to the $g$-band above, the correction for the host galaxy in
$r$ and $i$ is measured to be 0.084 and 0.071 magnitudes,
respectively. Within the uncertainties, this correction is the same
across bands - i.e., the host galaxy has a color comparable to the
quasar. For the $u$-band the image is of insufficient depth to model
the host galaxy directly, we adopt the same correction as the
$g$-band. The resulting photometry for images A-D, across four bands
and two epochs, is reported in Table 3. Uncertainties are calculated
by using the full GALFIT model to generate realisations of each
measured frame with appropriate noise, which are then refit. The
measured scatter in the photometry of quasar images, combined in
quadrature with the estimated calibration uncertainty, is
reported. For the brighter images, systematics due to uncertain
treatment of the host galaxy are likely dominant, and not addressable
with these limited data.

Images E and F must be treated with further care. The photometry of
image E is complicated by the blue core of galaxy G3, and image F is
simply very faint, and near the core of the brightest cluster galaxy,
G1. Particularly at redder wavelengths, this makes its measurement
highly uncertain. Furthermore, tests using the full GALFIT model, in which we
re-measured noisy realisations of the full model, also show
potentially strong biases - up to factors of 3 - in the photometry of
image F. To attempt best possible photometry for these we proceeded as
follows.

First, note that if the colors of the various quasar images are the
same, then the relative photometry of residual images in the $g$-$i$
subtraction in Figure~\ref{fig:gisub} can be used to measure the fainter
images. Matched colors are not guaranteed, due both to intrinsic
variability (e.g., Schmidt et al. 2012) coupled with time delays, as
well as variations induced by differential magnification between the
quasar and underlying host galaxy, and possible extinction of
individual images due to intervening galaxies in the complex cluster
core. However, we can validate the likely variability in color between
the images by considering the three brightest and most isolated images
(A-C); these show that the typical scatter about a fixed color is 0.05
in $g$-$i$ and 0.03 in $g$-$r$. This uncertainty is much less than the
systemic biases noted above in attempts at direct measurement, and so
the fixed color assumption is sufficient given these data.

Thus for image F, we use difference images to measure the differential
flux of image F relative to images A-C. Assuming that F has the same
color as these images, the flux of image F is then given simply by the
mean flux of images A-C times the flux ratio in the difference
image. All magnitudes are measured using PSF fitting photometry, for
consistency. The difference image $g$-$i$ provides the best
measurement of the residual fluxes, and is the basis of the
measurements reported in Table 3. As before, we estimate uncertainties
by using the fitted GALFIT model to generate and refit noisy
realisations of the measured image. In the case of image F, the final
reported uncertainty is the scatter in the magnitude offset in the
residual image, combined in quadrature with the color scatter between
the brighter images.

For image E we must further account for the residual flux from the
core of galaxy G3. We proceed as for image F, but additionally use
GALFIT to model a best-fitting S\'{e}rsic profile fixed at the center
of G3 concurrent with the PSF component for image E.

Finally, we note that each frame is directly calibrated to the SDSS
using many hundreds of objects; calibration uncertainties are 0.01
magnitudes at worst.

\begin{deluxetable*}{lcccccc}
\tabletypesize{\footnotesize}
\tablecaption{ Photometry of QSO images \label{tab:QSOphotom}}
\tablehead{
\colhead{Data Frame} & \multicolumn{6}{c}{Quasar Image}\\
\colhead{} & \colhead{A}& \colhead{B}& \colhead{C}& \colhead{D}& \colhead{E}& \colhead{F}
}
\startdata
\hline \\
$g$-band 1st epoch   &   21.03$\pm$0.01 & 21.52$\pm$0.01 & 22.13$\pm$0.01 & 23.48$\pm$0.04 & 24.32$\pm$0.09 & 25.21$\pm$0.24 \\
$g$-band 2nd epoch   &   21.15$\pm$0.01 & 21.57$\pm$0.01 & 22.22$\pm$0.01 & 23.74$\pm$0.03 & 24.22$\pm$0.08  & 24.81$\pm$0.07 \\ \hline
$r$-band 1st epoch   &   20.66$\pm$0.01 & 21.13$\pm$0.01 & 21.69$\pm$0.01 & 23.13$\pm$0.11 & 23.92$\pm$0.09 & 24.81$\pm$0.24 \\
$r$-band 2nd epoch   &   20.80$\pm$0.01 & 21.16$\pm$0.01 & 21.79$\pm$0.01 & 23.46$\pm$0.08 & 23.82$\pm$0.08 & 24.41$\pm$0.07 \\ \hline
$i$-band 1st epoch   &   20.82$\pm$0.01 & 21.20$\pm$0.01 & 21.81$\pm$0.01 & 23.46$\pm$0.12 & 24.04$\pm$0.09 & 24.92$\pm$0.24 \\
$i$-band 2nd epoch   &   20.95$\pm$0.01 & 21.31$\pm$0.01 & 21.90$\pm$0.01 & 23.78$\pm$0.08 & 23.96$\pm$ 0.08 & 24.55$\pm$0.07 \\ \hline
$u$-band 2nd epoch   &   22.85$\pm$0.08 & 23.29$\pm$0.09 & 24.18$\pm$0.17 & $>$24.58 &  $>$24.58 & $>$24.58 \\
\tablenotetext{}{Uncertainties are quoted at the 1-$\sigma$
  level. Images D,E,F are not detected in the $u$-band; the 1-$\sigma$
  detection limit in our data is 24.58 mag. When comparing this photometry to the SDSS photometry reported in Table 2, a correction for the quasar host galaxy
  should be applied to the SDSS photometry, as detailed in the main text.}
\end{deluxetable*}

\subsection{Lensing cluster}
\label{sec:cluster}

The maximum separation of the quasar images is $15\farcs 1$ (between quasar images A and C)
clearly indicative of a cluster-sized lensing mass. The SDSS photometric redshift estimates
of galaxies G1-G3 (see Table~\ref{tab:astrom}) are consistent with all three galaxies being located in a cluster at
$z \sim 0.5$. As part of the observations described in \S~\ref{sec:ABCspec} and \S~\ref{sec:DEF} above, all three galaxies were targeted
spectroscopically. Redshift estimates were obtained through cross-correlation with the elliptical galaxy template of Kinney et al.\ (1996),
yielding the redshift estimates listed in Table~\ref{tab:galaxies}. The redshifts are consistent within the measured uncertainties, and
all three galaxies G1-G3 clearly belong to the same cluster at a redshift consistent with the SDSS photometric redshift estimates.
To further investigate the properties of the lensing cluster, we applied the SExtractor software (Bertin \& Arnouts 1996) for galaxy photometry
to the stacked second-epoch MOSCA $gri$ images. Prior to obtaining the photometric measurements, the stacked $r$- and $i$-band images
were smoothed to match the resolution of the $g$-band image. Object detection was initially performed on the stacked $g$-band image,
and SExtractor was subsequently run in dual-image mode on the stacked images in the other passbands, using the $g$-band image
as a reference for object detection. The observed magnitudes were subsequently converted to AB magnitudes in the SDSS system using
objects in the MOSCA field with catalogued SDSS photometry. Total magnitudes were determined using the SExtractor \texttt{MAG\_AUTO} parameter,
and colors were determined from aperture magnitudes (\texttt{MAG\_APER}) within a $2\arcsec$ diameter aperture.
A $g$-$i$ vs.\ $i$ color-magnitude diagram of non-stellar objects, selected based on their location in a magnitude - $\mu_{\rm max}$ diagram
(where $\mu_{\rm max}$ is the central surface brightness of objects), is shown in Figure~\ref{fig:cmag}.
A red sequence is evident at $g$-$i \sim 2.5$, similar to the $g$-$i$ colors of the three galaxies G1-G3 (see Table~\ref{tab:galaxies}).
Figure~\ref{fig:lightcont} shows a smoothed map of the light distribution of red sequence galaxies over the observed MOSCA field.
A strong peak in the luminosity distribution is located at the position of galaxies G1-G3.

\begin{deluxetable*}{lcccc}
\tabletypesize{\footnotesize}
\tablecaption{ Photometry and redshift measurements for galaxies in the cluster core.\label{tab:galaxies}}
\tablehead{
\colhead{Galaxy} & \colhead{i} &  \colhead{g$-$i} & \colhead{r$-$i} & \colhead{Redshift} \\
      & \colhead{ } & \colhead{($2\farcs 0$ aperture)  } & \colhead{($2\farcs 0$ aperture) } &  \colhead{ }
}
\startdata
\hline \\
G1         & 18.74 & 2.71 & 0.97 & $0.493 \pm 0.013$ \\
G2         & 18.97 & 2.53 & 0.96 & $0.496 \pm 0.012$ \\
G3         & 19.37 & 2.45 & 0.93 & $0.489 \pm 0.013$ \\
\end{deluxetable*}

\begin{figure}
\includegraphics[angle=0,scale=.35]{cmag_sdssj2222p2745_new.pdf}
\caption[.]
{Color-magnitude diagram of 3033 non-stellar objects detected in the MOSCA field containing \QSO . The galaxies G1-3 are indicated by green dots. Other galaxies with $g$-$i$ colors within $\pm 0.35$ magnitudes from the red sequence formed by early-type galaxies in the lensing cluster are indicated by red dots.  }
\label{fig:cmag}
\end{figure}

\begin{figure}
\plotone{colcont3.pdf}
\caption[color contour plot.]
{A contour plot showing a smoothed map of the light distribution of the red sequence galaxies indicated by the red and green colors in
Figure~\ref{fig:cmag}. The background figure is a $gri$ composite based on the second-epoch MOSCA images. The coordinates are relative to the position of galaxy G1, which closely coincides with the cluster lens (see \S~\ref{sec:model}). A strong peak in the light distribution is seen at this location.}
\label{fig:lightcont}
\end{figure}

\subsection{Giant arc}
\label{sec:arc}

The identification of \QSO \, as a candidate gravitational lens system was partially due to recognition of the giant arc just
south of the cluster center. The extent of the arc in our deepest stacked $g$-band image (see Figure~\ref{fig:Slitpos}) is $10\arcsec$.
Our SExtractor photometry (see \S~\ref{sec:cluster}) of the arc yields $g=21.57$, and $u$-$g = 0.87$, $g$-$r = 0.21$, $g$-$i = 0.41$,
where the colors are measured in $2\arcsec$ diameter apertures centered on the brightest central portion of the arc.
We note that the quoted magnitude of the arc can be considered a lower limit on its brightness, given the very extended mophology of the arc.
Although SEXtractor attempts to treat the arc and the WD as separate objects, a more careful modeling of the shape of the arc (including PSF modeling and removal of the superposed white dwarf point source)
would be required to obtain an accurate total magnitude.
The spectrum of the arc shows a single emission line at $\lambda_{obs} = \sim 4015${\AA}, which we interpret as Lyman-alpha at $z=2.30$.
The alternative interpretation of [O II] (3727 {\AA}) at $z=0.077$ would put the arc in front of the cluster, which is obviously inconsistent
with the lensed morphology of the arc. The lens model presented in the following section does not predict a counter-image of the arc.

\section{Lens model}
\label{sec:model}

We compute a parametric lens model using the publicly available software \texttt{Lenstool} (Jullo et al. 2007), through Markov Chain Monte Carlo minimization in the image plane. The lens is modeled with several components: a cluster halo, BCG, and cluster galaxies.
All the components are represented by a pseudo-isothermal elliptical mass distributions (PIEMD\footnote{This profile is formally the same as dual Pseudo Isothermal Elliptical Mass Distribution (dPIE, see El{\'{\i}}asd{\'o}ttir et al. 2007).}; Limosin et al. 2005, El{\'{\i}}asd{\'o}ttir et al. 2007), parametrized by its position $x$, $y$; a fiducial velocity dispersion $\sigma$; a core radius $r_{core}$; a scale radius $r_s$; ellipticity $e=(a^2-b^2)/(a^2+b^2)$, where $a$ and $b$ are the semi major and semi minor axes, respectively; and a position angle $\theta$. All the parameters of the cluster halo distribution are allowed to vary within priors, except for $r_s$, which is not constrained by the lensed images.

Cluster members are selected based on their $g$-$i$ color in a color-magnitude diagram, with respect to the cluster red-sequence (see Figure~\ref{fig:cmag}, and their position, ellipticity and position angle are fixed at their observed values, as measured with SExtractor. The parameters $\sigma$ and $r_s$ are determined through scaling relations (see Limousin et al.\ 2005 for a description of the scaling relations).
Three galaxies, G1, G2 and G3, are in close proximity to three lensed images of the quasar, and thus affect their positions more directly than other cluster members. To account for the intrinsic scatter in the scaling relations, we allow some of the parameters of these three galaxies to be modeled separately from the rest of the cluster galaxies.

As constraints, we use the redshift and positions of the images of the quasar and of the lensed galaxy at $z=2.30$.
We have a total of 12 free parameters: 6 free parameters for the cluster halo, and 2 free parameters for each of the galaxies, and 14 constraints. The best fit parameters are listed in Table~\ref{t.parameters}. The uncertainties were estimated through the MCMC sampling of the parameter space. For parameters that were not well-constrained, we list the priors that were set in the minimization.
To account for systematics due to misidentification of the sixth image, we also compute a model assuming only five images. The two families of models are similar, although we note that G1 is poorly constrained in the model without image F.

The image-plane RMS scatter of the quasar images is 0.14'' in the 5-image model and 0.18'' in the 6-image model; the RMS of the blue arc is somewhat larger (0.26'',0.38'', respectively), due to the difficulty of measuring its positional constraints, and the larger weight given to the quasar images in the modeling process.

Both models successfully predict the locations of all the observed
images (either five or six, depending on the model constraints), and
do not predict additional images, with the exception of demagnified
central images that cannot be detected in our data: the model with six
images predicts a demagnified seventh image close to the center of
galaxy G2. This is expected in this strong lensing configuration. Our
imaging data do not reveal any hint of this seventh image, though a
positive identification might be possible with the superior spatial
resolution of {\it HST}. A careful re-examination of the spectroscopic
data for G2 shown in Figure~\ref{fig:2Dspec} and plotted in
Figure~\ref{fig:DEFspecs} may indicate a weak signature of the
Lyman-alpha line from the seventh image (G), but this feature is
almost at the level of the noise, and more sensitive spectroscopy with
8-10m class telescopes will be required for a definite detection.

Table \ref{t.mag} lists the model-predicted magnifications and time
delays for the two model families. Uncertainties are computed from a
suite of models, drawn from the MCMC chain, that represent the
1-$\sigma$ uncertainty in the parameter space. All time delays are
given relative to image A.  The best-fit models predict short time
delays of order of 100 days between the close pair (A-B), and between
the central images (D-E-F). Image C precedes A and B by 1400 days, and
D-E-F follow A and B by $700-1000$ days.  In the 6-image model, 66\%
of the models, as well as the best-fit model, predict the order of the
images to be C-B-A-F-E-D. All the models predict that image C is the
first one to occur, followed by B-A (in 93\% of the models) or A-B
(7\%); followed by F-E-D (72\%) F-D-E (16\%) or D-F-E (12\%).  In the
5-image model, 62\% of the models, as well as the best-fit model,
predict C-B-A-E-D; here too, all the models predict that C is the
first image to occur, followed by B-A (77\%) or A-B (23\%), and then
E-D (81\%) or D-E (19\%).

\begin{figure}
\includegraphics[angle=0,scale=.425]{sdss2222_model.pdf}
\caption[.]
{Caustics, critical lines, and image positions from the best-fit model, superposed on a $gri$ color image of the \QSO \, lens system. The critical curves for a source
at the quasar redshift ($z=2.82$) are indicated in red. The caustic curves in the source plane are shown as yellow lines,
and the predicted source locations of the quasar and arc with respect to these curves are indicated by green crosses. The observed locations of the six quasar images A-F are indicated by blue circles.
}
\label{fig:Model}
\end{figure}

\begin{deluxetable*}{lccccccc}
 \tablecolumns{8}
\tablecaption{Best-fit lens model parameters  \label{t.parameters}}
\tablehead{\colhead{Halo }   &
            \colhead{RA}     &
            \colhead{Dec}    &
            \colhead{$e$}    &
            \colhead{$\theta$}       &
            \colhead{$r_{\rm core}$} &
            \colhead{$r_{\rm cut}$}  &
            \colhead{$\sigma_0$}\\
            \colhead{(PIEMD)}   &
            \colhead{($\arcsec$)}     &
            \colhead{($\arcsec$)}     &
            \colhead{}    &
            \colhead{(deg)}       &
            \colhead{(kpc)} &
            \colhead{(kpc)}  &
            \colhead{(km s$^{-1}$)}  }
\startdata
\cutinhead{Model 1: constraints from 5 QSO images. RMS$_{\rm QSO}$=0.14''}
Cluster  & $-0.14 ^{+0.50}_{-1.03}$        & $1.18 ^{+1.90}_{-0.81}$         & $0.66 ^{+0.25}_{-0.14}$    & $ 97 ^{+  5}_{-  4}$    & $ 26 ^{+ 15}_{- 42}$   & [2000] & $580 ^{+ 64}_{-163}$  \\
G1       & [0.0]      & [0.0]       & [0.26] & [3.8]         & $0.77 ^{+0.77}_{-0.23}$ & [47]     & $155 ^{+ 55}_{-168}$  \\
G2    & [-0.596] &[-5.220] & [0.21]  &[75.5]       & 0.13 [0.0 0.3] & [24]     & $212 ^{+ 40}_{- 44}$ \\
G3    & [-1.762] &[-2.308] &[0.41] &[-18.3]       &0.19 [0.0 0.3]  &[20]     & $279 ^{+ 76}_{- 21}$ \\
L* galaxy  & \nodata & \nodata & \nodata & \nodata &  [0.15]  &     [20]&  [100]  \\
\cutinhead{Model 2: constraints from 6 QSO images.  RMS$_{\rm QSO}$=0.18''}
Cluster  & $-0.16 ^{+0.58}_{-0.71}$        & $2.10 ^{+2.58}_{-0.90}$         & $0.75 ^{+0.13}_{-0.05}$    & $ 96 ^{+  4}_{-  3}$    & $ 37 ^{+ 13}_{- 40}$   & [2000] & $578 ^{+ 50}_{-114}$  \\
G1       & [0.0]      & [0.0]       & [0.26] & [3.8]         & $0.05 ^{+0.04}_{-0.93}$ & [47]     & $303 ^{+ 34}_{- 46}$  \\
G2    & [-0.596] &[-5.220] & [0.21]  &[75.5]       & 0.15 [0.0 0.3] & [24]     & $226 ^{+ 29}_{- 36}$ \\
G3    & [-1.762] &[-2.308] &[0.41] &[-18.3]       &0.15 [0.0 0.3]  &[20]     & $235 ^{+ 46}_{- 33}$ \\
L* galaxy  & \nodata & \nodata & \nodata & \nodata &  [0.15]  &     [20]&  [100]  \\
\enddata
 \tablecomments{All coordinates are measured in arcseconds relative to the center of G1, at [RA, Dec]=[335.53573, 27.75986]. The ellipticity is expressed as $e=(a^2-b^2)/(a^2+b^2)$. $\theta$ is measured north of West. Error bars correspond to 1 $\sigma$ confidence level as inferred from the MCMC optimization. Values in square brackets are for parameters that are not optimized. Errors in square brackets represent the lower and upper limits that were set as prior in the optimization process, for parameters that were not well-constrained by the data.
The location and the ellipticity of the matter clumps associated with the  cluster galaxies were kept fixed according to their light distribution.}
\end{deluxetable*}

\begin{deluxetable*}{lccccccc}
 \tablecolumns{8}
\tablecaption{Model-predicted magnifications and time delays\label{t.mag}}
\tablehead{\colhead{Image }   &
            \colhead{Magnification (1)}     &
            \colhead{Time delay (1) [days]}    &
            \colhead{Magnification (2)}     &
            \colhead{Time delay (2) [days]}    &
}
\startdata
A  & $5.7 ^{+14.5}_{-3.1}$ & $  0 $ &$4.7 ^{+3.4}_{-1.6}$ &$  0$  \\
B  & $5.6 ^{+12.8}_{-2.2}$ & $-87 ^{+187}_{-296}$ &$5.4 ^{+4.6}_{-1.6}$ &$-112 ^{+158}_{-225}$  \\
C  & $2.5 ^{+3.6}_{-0.6}$ & $-1399 ^{+850}_{-776}$ &$2.4 ^{+1.1}_{-0.3}$ &$-1368 ^{+456}_{-344}$  \\
D  & $0.6 ^{+0.7}_{-0.2}$ & $960 ^{+365}_{-254}$ &$0.7 ^{+0.3}_{-0.2}$ &$931 ^{+237}_{-233}$  \\
E  & $0.7 ^{+0.9}_{-0.3}$ & $851 ^{+448}_{-278}$ &$0.6 ^{+0.3}_{-0.2}$ &$806 ^{+370}_{-224}$  \\
F  & \nodata & \nodata &$0.5 ^{+0.5}_{-0.2}$ &$723 ^{+223}_{-161}$  \\
\enddata
 \tablecomments{Model (1): constraints from 5 QSO images.   Model (2): constraints from 6 QSO images. Time delay is given in days, relative to image A.}
\end{deluxetable*}

\section{Summary and discussion}
\label{sec:discuss}

\subsection{Previous observations and predictions of high image multiplicities}
\label{sec:multiplicity}

We have identified \QSO \, as a gravitational lens system producing six observed images of the same quasar. This is the third known
cluster-scale lens and the only such lens producing more than five observed images. The only previously known six-image AGN lens
is B1359$+$154 (Rusin et al.\ 2001), where a radio source at $z_s = 3.235$ is being lensed by a compact group of three galaxies at $z_l \sim 1$.
However, the quasar image separations we observe in \QSO \, are an order of magnitude larger than in B1359$+$154, and the lensed images are
$\sim 3$ magnitudes brighter at optical wavelengths, making six images detectable in ground-based imaging of \QSO .
The B1359$+$154 lensed image configuration is similar to what we find in \QSO , with the three fainter images located in close proximity to the
three galaxies situated within the Einstein radius of the lens system, and three brighter images located further away from these galaxies.
However, the lens model of B1359$+$154 presented by Rusin et al.\ (2001) does not allow a significant dark matter halo associated with the
galaxy group in addition to the three halos corresponding to the three individual galaxies. In contrast, in our model the cluster halo
component is the dominant contributor to the observed image splitting of \QSO .

Since cluster-scale quasar lenses and image multiplicities $>5$ are both rare, we would expect a lensing system such as
\QSO \, to be extremely rare. There are no appropriate quantitative predictions for the
occurrence of this type of lens systems available in the literature. Evans \& Witt (2001) calculate the incidence of sextuplet
and octuplet image systems (with demagnified seventh and ninth images, respectively)
and estimate that these constitute $\sim 1\%$ of the population of quasars multiply imaged by galaxy-scale lenses.
This is consistent with the single known sextuplet case of B1359$+$154 among the $\sim 100$ known galaxy-scale quasar lenses.
For the larger image separations produced by cluster lenses, published
studies of the probabilities of different lensing multiplicities (Oguri \& Keeton 2004; Li et al.\ 2007; Minor \& Kaplinghat 2008)
only include double, quadruple (with demagnified third and fifth images, respectively) and naked cusp configurations.
Li et al.\ (2007) state that they do not expect a significant fraction of sources to have image numbers exceeding 5.

\subsection{Comparing the lens and source redshifts to predictions}
\label{sec:redshifts}

Both the quasar source redshift and cluster lens redshift of \QSO \, are comparable to the two other cluster quasar lenses and in good
agreement with theoretical expectations: The observed lens redshift in \QSO \, is $z=0.49$, which is similar, but slightly lower than
the cluster lenses in \QSOLone \, ($z=0.68$) and \QSOLtwo \, ($z=0.58$). This redshift is very close to the peak (at $z \simeq 0.5$) of the predicted lens redshift distribution for photometrically selected wide-separation quasars in the SDSS (Li et al.\ 2007).
The observed quasar source redshift in \QSO \, is $z=2.82$, slightly higher than the sources in \QSOLone \, ($z=1.73$)
and \QSOLtwo \, ($z=2.20$). These three redshifts are all near the peak (around $z=2$) of the predicted source redshift distribution for
photometrically selected wide-separation quasars in the SDSS (Li et al.\ 2007).

\subsection{Prospects for time delay measurements}
\label{sec:delta_t}

The photometry reported in \S~\ref{sec:phot} shows significant variability in the quasar, demonstrating the feasibility of making time
delay measurements in \QSO \, from monitoring campaigns using ground-based 2-4m class telescopes. We have recently initiated a monitoring
program for \QSO \,
at the NOT for this purpose. The predicted time delays from our lens model (see \S~\ref{sec:model}) indicate that three independent
time delays $\Delta t_{AB}$ ($\equiv \Delta t_{B} - \Delta t_{A}$), $\Delta t_{ED}$ and $\Delta t_{FE}$ in the system are all of order 100 days.
This suggests that several time delay measurements could, in the best case, be obtained from a single season of monitoring.
The predicted time delays between image C and the close pair (A-B) and between (A-B) and the central images (D-E-F)
are of order 1400 days and 700-1000 days, respectively. These values are similar to the two longest predicted time delays for \QSOLone , of 1218 and 1674 days, respectively (Oguri 2010) and the measured longest time delay in \QSOLtwo \, of $\Delta t_{AB} = (744 \pm 10)$~days (Fohlmeister et al.\ 2012).

\subsection{Future work}
\label{sec:future}

Morphological, photometric and spectroscopic evidence presented in this paper strongly suggest the presence of a sixth
(F) image of the quasar located closest to the lensing mass center. The odd number theorem of strong gravitational lensing theory
will then require the presence of a seventh (G) image, for which our model predicts a location close to the center of cluster galaxy G2.
In the case of galaxy-scale lenses, the faintest image of a multiply lensed quasar is typically highly demagnified and hence unobservable
in the vast majority of cases. However, the shallower central slopes of the mass density profiles of clusters
increases the chance of observing the final odd image, as exemplified by the identification of the demagnified fifth central
image in \QSOLone \, using {\it HST} imaging (Inada et al.\ 2005, 2008).

While the data presented in this paper do not provide conclusive evidence for the presence of the seventh image,
there is a hint of Lyman-alpha emission from this image in the spectrum of G2. If this feature is indeed emission from the quasar,
a firm confirmation would be possible through spectroscopic observations with 8-10m class telescopes.

While time delay measurements would provide important additional modelling constraints on the \QSO \, lens system, follow-up
HST imaging will also be crucial to improve the modeling constraints from the observed locations of the quasar images and hopefully
provide morphological and photometric confirmation of the predicted seventh (G) image close to the center of galaxy G2. Further constraints
on the lens system could also come from spatially resolved, multiply imaged structures within the giant arc and from the identification of additional fainter,
multiply imaged, galaxies as revealed by the HST observations of \QSOLone \, (Sharon et al.\ 2005) and \QSOLtwo \, (Oguri et al.\ 2012).

\subsection{Broader significance of this discovery}
\label{sec:significance}

The significance of the discovery of \QSO \, is twofold: Firstly, the presence of six quasar images (and potential future confirmation
of a seventh image), spread over a range of clustercentric radii, with good prospects for future time delay measurements,
coupled with the presence of an additional lensed source producing a bright giant arc, can provide unique detailed measurements of the
matter distribution in the core of a cluster. Such measurements provide a stringent test of the scenario of structure formation, including the
properties of dark matter in cluster cores.

Secondly, adding our new discovery of \QSO \, to the previous detections of
\QSOLone \, and \QSOLtwo \, makes a significant contribution towards establishing quasars strongly lensed by galaxy clusters
as a cosmological tool. The probability of such rare lenses depends very sensitively on cosmological parameters, in particular
the normalization of the matter power spectrum $\sigma_8$ and the matter density $\Omega_M$ (e.g., Li et al.\ 2007).
Even though no directly applicable predictions can be found in the literature, the occurrence of lens systems with image separations
and image multiplicities as high or higher than \QSO \, must necessarily be exceptionally rare, and this could conceivably be the
the only such system, provided that the current $\Lambda$CDM paradigm is correct.

\input{bib.tex}
\acknowledgments

HD acknowledges support from the Research Council of Norway. MDG
thanks the Research Corporation for support of this work through a
Cottrell Scholars award. KS acknowledges support from the University
of Michigan's President's Postdoctoral Fellowship. JPUF acknowledges
support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre
is funded by the DNRF.  We thank the NOT staff, in particular our
support astronomer Stefan Geier, for excellent support, including
accommodating a last-minute instrument change which allowed the
spectroscopic confirmation of the D image and discovery of the E image
of the quasar.

\end{document}

redpajama_set_name: RedPajamaArXiv


text:
Home > About Us > Our People > Susan Mairs
Susan Mairs
Susan qualified as a solicitor in 1998 and has specialised in all areas of insolvency since then. She was a partner at an established practice which she left to set up Clarke Mairs LLP in October 2007.
Susan predominantly acts for Insolvency Practitioners who have already received appointments as office holders. She largely acts for them in contentious matters, assisting them in recovering assets, setting aside antecedent transactions and pursuing claims against directors such as misfeasance and wrongful trading. She also particularly enjoys the investigatory work which is often required into the affairs of either an individual or a company prior to it being placed into an insolvent estate.
She also acts for companies and individuals who find themselves in financial difficulties in advising them on rescue measures.
Susan is a member of the Insolvency Lawyers Association and the Association of Business Recovery Professionals (R3).
sm@clarkemairs.com


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Lately, I am more careful with my actions I let Geoff see. I used to not mind him watching whenever I put my makeup on. It was just this one morning 3 weeks ago that I realized that he was actually observing and now knowledgeable with how he uses MY makeup.
He used his face as his canvass!
This entry was posted in Cute, Geoff, Personal, Random Thoughts and tagged 52 week challenge, 52 week project, baby on makeup on June 19, 2014 by meeyeow.
Summer this year is really scorching, so the rain was really welcome. Quite obvious with how the baby smiled.
This entry was posted in Cute, Geoff, Personal, Random Thoughts and tagged 52 week challenge, 52 week project, fun in the rain, summer rain on June 4, 2014 by meeyeow.
My brother invited us to his company's family day one weekend of May. Ironic as it sounds, it was our little family who went, sans the employee who was supposed to be there. Be as it may, we enjoyed the day but, resolved to going to amusement parks when Geoff is a bit older.
Here is the only picture that we managed to get during the event because the baby was active the whole time.
Borlogs after mangulit the whole day!
This entry was posted in Cute, Event, Personal, Random Thoughts and tagged 52 week challenge, 52 week project, baby, sleeping baby boy, Star City on June 2, 2014 by meeyeow.
I am thankful that Geoff is healthy and has a big appetite most of the time. Though I am guilty that he eats junk food, we still make sure that what we buy outside or cook at home will compensate the unhealthy stuff. Anyway, here is Geoff's "very magana" picture when we ate at Savory last payday.
This entry was posted in Cute, Food, Geoff, Personal, Proud Achievements and tagged 52 week challenge, 52 week project, big appetite, hungry baby, nomnom, savory on May 22, 2014 by meeyeow.
Woke up to this giggly baby boy one morning. Geoff looks so big here. Where's my little baby boy? Ambilis talaga ng oras. Don't grow up so fast my love!
This entry was posted in Cute, Geoff, Personal, Proud Achievements and tagged 52 week challenge, 52 week project, cute baby on May 9, 2014 by meeyeow.
It's quite funny because eversince Geoff saw the ipod, he would use it as an imaginary phone. During this week, I figured it's high time for me to experiment how he would react if I let him use the earphones as well.
I guess, this photo shows that he enjoyed it and that the experience was rather new, but enjoyable.
This entry was posted in Cute, Geoff, Personal, Proud Achievements and tagged 52 week challenge, 52 week project, baby on ipod on May 9, 2014 by meeyeow.
This entry was posted in Cute, Geoff, Proud Achievements and tagged 52 week challenge, 52 week project, baby boy, cute baby on May 8, 2014 by meeyeow.
And no, this is not a trip "trip" but merely what the baby enjoys most when it gets extremely hot at home.
Magbabad – Like a boss!
This entry was posted in Cute, Geoff, Personal, Random Thoughts and tagged 52 week challenge, 52 week project, kidie pool, summer, trip lang on April 22, 2014 by meeyeow.
At 2 years and 1 month, we always encourage Geoff to do things that he should be able to do. He has chores this early, and some of them includes putting his dirty clothes in his hamper and fetching his own sippy cup from the fridge whenever he needs to drink.
Anyway, this is his photo as he is getting down from the chair. He wanted to read his books and one of his favorite things to do is to ask us get one book at a time (this is very tiring, I tell you), so I suggested that he tries doing it on his own.
on his way down. great job, baby!
This entry was posted in Cute, Geoff, Personal, Proud Achievements and tagged 52 week challenge, 52 week project, milestones on April 15, 2014 by meeyeow.
There was this one day last last week when, despite of the terrible summer heat, it rained. This baby, despite of my constant yelling reminder not to go out, insisted to go because he wanted to take a bath in the rain. Too bad the it wasn't raining very hard that time for him to be drenched.
This entry was posted in Cute, Geoff, Personal, Proud Achievements and tagged 52 week challenge, 52 week project, baby expression on April 2, 2014 by meeyeow.


Tatiana Kouchnareva (B.C KO T). Box Car Willie - ripe fruit. 2014-09-09.
Indet., regular leaf plants. Medium sized red fruits are round and oblate, 6-10 oz. Very good rich old-fashioned flavor.
80 days, indet., regular leaf plant with high yield of 6-12 oz red fruit with very good flavor.
Bred by Joe Bratka's father. Joe found the seeds for this tomato and several others (Red Barn, Mule Team, and Great Divide) in a toolshed, could not get the seeds to germinate, and sent them to Carolyn Male, who succeeded in germinating the seed and shared this variety with other gardeners and SSE members in the mid-1990s.
First offered in the Seed Savers 1994 Yearbook by Carolyn Male of Latham, New Jersey (NY MA C), who got the seeds from Joe Bratka of New Jersey.
Could be named after Lecil Travis Martin, an American country music singer.
Klaus-Peter Schurz (GERM SC K). Box Car Willie - leaf. May 2011.
Klaus-Peter Schurz (GERM SC K). Box Car Willie - flower. June 5, 2011.
Tatiana Kouchnareva (B.C KO T). Box Car Willie (1) - ripe fruit. 2014-09-09.
Tatiana Kouchnareva (B.C KO T). Box Car Willie (1) - sliced fruit. 2014-09-09.
Tatiana's TOMATObase Seeds - new, sold out for 2015 . .
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Tomato Growers Supply 12 .
Description Indet., regular leaf plants. Medium sized red fruits are round and oblate, 6-10 oz. Very good rich old-fashioned flavor.
History * Bred by Joe Bratka's father. Joe found t … * Bred by Joe Bratka's father. Joe found the seeds for this tomato and several others (Red Barn, Mule Team, and Great Divide) in a toolshed, could not get the seeds to germinate, and sent them to Carolyn Male, who succeeded in germinating the seed and shared this variety with other gardeners and SSE members in the mid-1990s.
Could be named after Lecil Travis Martin, an American country music singer. Martin], an American country music singer.
This page was last modified on 15 February 2017, at 17:47.


text:
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Republican consultant Anthony Pedicini is the latest target of a negative mailer in the vitriolic House District 58 primary.
Tom Lee files bill to protect seniors
State Sen. Tom Lee's office announced he had again filed legislation to add financial protections for residents of continuing care retirement
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Published on June 29, 2017 in 2017 by Staff Reports
Americans for Prosperity wants Sen. Marco Rubio to lead the charge to pass pro-growth tax reform. The organization launched its third ad as part of a grassroots campaign urging members of Congress to "un-rig the economy by seizing the opportunity to enact pro-growth tax reform. The digital ad is part of a summer-long effort by Americans for Prosperity to push for broad, pro-growth tax reform. "Congress has a once in a generation opportunity to fix our broken tax code. Americans…
Florida calls for $27 billion in hurricane recovery funding
In the wake of Hurricanes Harvey, Irma and Maria, U.S. Senators Marco Rubio and Bill Nelson, along with 26 U.S.
Interior Secretary heading to South Florida
U.S. Interior Secretary Ryan Zinke will be in South Florida this week reviewing damage from Hurricane Irma and getting a
State prepares for influx from Puerto Rico
From schools to shelters, Florida is readying for an influx of people struggling for food, water and power in hurricane-damaged
AFP-FL releases digital ad calling on Senate to 'end corporate welfare'
Published on April 13, 2017 in Statewide by Staff Reports
Americans for Prosperity-Florida is continuing its efforts to try to put an end to economic incentives in Florida. The organization launched a 60-second digital ad campaign Thursday, urging Floridians to "contact (their) legislator and tell them the game's over: end this corporate welfare." The release comes one day after the Florida Senate approved its 2017-18 budget, which included money for Enterprise Florida and economic incentive programs. The House budget does not include funding for Enterprise Florida, and the House earlier…
Enterprise Florida gives raises, ditches bonuses
Raises will be provided to 16 upper-level and mid-level employees of Enterprise Florida, as the state's business-recruitment agency does away
Enterprise Florida could give employee pay raises
Pay raises may be in store for some employees at the state's business-recruitment agency as bonuses have been withheld this
Deadlines likely pushed back for ballot proposals
Following the disruption of Hurricane Irma, a panel on Monday recommended that the Florida Constitution Revision Commission give residents more
AFP-FL launches direct mail campaign to support lawmakers who backed bill to kill Enterprise Florida
Published on March 20, 2017 in Statewide by Staff Reports
Keep an eye on your mailboxes, Florida: Americans for Prosperity-Florida is out with a new mailer. The statewide organization launched a direct mail campaign Monday in districts of state lawmakers who supported a proposal (HB 7005) Enterprise Florida and other economic incentive programs. The mailer, according to the organization, is meant to "educate citizens in the districts of legislators that voted to eliminate corporate welfare." "Corporate welfare is the result of government, at any level, picking winners and losers by…
House sets schedule for September committees
Major policy committees will be first up when the House starts holding committee meetings in September to prepare for the
Americans for Prosperity-Florida is hitting the road to energize activists about tax reform. The grassroots organization is scheduled to hold
Dan Raulerson resigning from Florida House in August
Dan Raulerson is resigning from the Florida House. The Tampa Bay Times reported Tuesday that the Plant City Republican has
AFP-FL encourages Legislature to continue to support bill to eliminate Enterprise Florida
Published on March 7, 2017 in Statewide by Staff Reports
Americans for Prosperity-Florida applauded Gov. Rick Scott for his passion for job creation, but once again called on the Legislature to approve legislation that would eliminate economic incentive programs. "There is no question that Governor Scott and the Florida legislature have helped Florida endure the recent recession, and through their effective leadership the state of our state is strong," said Chris Hudson, the state director for AFP-FL, in a statement. "But make no mistake, the positive strides and gains we've…
Siemens, Chromalloy joint project to bring 350 new Hillsborough jobs
Two global engineering companies, Siemens and Chromalloy Gas Turbine Corporation, have chosen Hillsborough County for the headquarters of a new joint
Broward nursing home expands lawsuit against state
A Broward County nursing home has expanded a lawsuit challenging moves by Gov. Rick Scott's administration that effectively shut down
Dismantling Enterprise Florida is a top priority for AFP-FL
Published on March 6, 2017 in 2017/Top Headlines by Drew Wilson
The Florida branch of the conservative group Americans for Prosperity announced its 2017 legislative priorities Friday; dismantling Enterprise Florida is on the top of the list. "In 2015 the Governor boldly stated that 'taxpayers are better investors than government.' We completely agree. That's why we're calling on both chambers to put politics aside and work towards dismantling the failed quasi-state agency, Enterprise Florida," said AFP-FL Director Chris Hudson. "Government shouldn't be in the business of picking winners and losers. Let's…


The TCO Labels are today tucked to more than 240 million Display units, representing more than half of the global market for display units. It was initiated by the white collar workers trade union central, TCO, and is regarded as one of the most important Swedish IT innovations during the 1990's.
UsersAwards software certification is a direct follow-up of the successful TCO initiative. It is the most research intensive activity of the Users' IT quality network. The quality criteria that underpin the certification are based on a long-term research effort and by an ongoing dialogue between researchers, service providers, and user panels throughout universities, industry and users networks.
Service providers that register a particular service for certification has to go through two hearings with certification staff and get their service scrutinized at three independent sites of use through a standardized interview and questionnaire procedure.
While winning the User's IT Prize gives publicity, the Users' certification gives a thorough quality documentation of how satisfied users actually use the certified service. For service providers who want to retain their customers, and thereby gain new ones, this kind of "open source" documentation of users' satisfaction is hard to beat.
Create or support initiatives in which user organisations such as trade unions, professional associations, consumer organisations work together with research organisations in order to label software products or services on grounds of publicly declared measurements open for scientific scrutiny and media inspection.


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