text:
Q: QT is there a way to delay signal and/or abandon signal? I am looking for a way to delay or abandon signal under some circumstances.
My GUI looks like that - I have a MainWindow frame, which contains QStackedWidget with several QWidgets. Each QWidget 'provides' mainIcon to the parent widget (MainWindow), which is then connected to a slot realizing switching between pages functionality.
I want to connect this mainIcon to a signal, show a QMessageBox and if user confirms - everything will happen normally (a signal will be passed and analyzed by parent Widget) - after a delay(user has to confirm).
However, if he declines, a signal should not be passed, and nothing should happen.
What I have came up with so far is:
connect(mainIcon, &GuiIconAction::clicked, this, [=](){
        //block signals of mainIcon - should be somehow ensured that this is the first realized slot
        if(confirmRequired)
        {
            if(QMessageBox::warning(this, "Manager",
                                    "Are you sure you want to switch window?",
                                    QMessageBox::Yes | QMessageBox::No) == QMessageBox::No)
                return;
        //get blocked signals and call them
        }
    });

Important notes are:

*

*GuiIconAction is a QToolButton,

*Widget don't know that the parent exists (i.e. it just provides interface, but could also be placed standalone)

*I don't want to realize this functionality in parent widget (MainWindow), as it is only a frame - I want it to be realized on the level of particular Widget in QStackedWidget

A: I would suggest to implement the functionality with a slot.
In the slot you can create the message box. If the user confirms, emit a signal. Otherwise not.


text:
Remptendorf – miejscowość i gmina w Niemczech, w kraju związkowym Turyngia, w powiecie Saale-Orla. Liczy 3 888 mieszkańców. Do 30 grudnia 2019 gmina pełniła funkcję "gminy realizującej" (niem. "erfüllende Gemeinde") dla gminy wiejskiej Burgk.

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text:
What if Dover had prevailed on intelligent design?
Where would intelligent design be if science hadn't prevailed through a group of Dover Area School District parents...
What if Dover had prevailed on intelligent design? Where would intelligent design be if science hadn't prevailed through a group of Dover Area School District parents... Check out this story on yorkdispatch.com: https://www.yorkdispatch.com/story/news/2015/10/02/what-if-dover-had-prevailed-intelligent-design/73539668/
JESSICA SCHLADEBECK, YorkDispatch Published 1:49 a.m. ET Oct. 2, 2015
In this file photo, Eric Rothschild, left, an attorney for Pepper Hamilton LLP, holds the textbook that was at the center of controversy as plaintiffs Tammy Kitmiller, center, and Christy Rehm watch at a press conference at the Pennsylvania State Capitol on Dec. 14, 2004.(Photo: AP Photo/York Dispatch, Vinny Tennis)
Where would intelligent design be if science hadn't prevailed through a group of Dover Area School District parents who sued to prevent the teaching of the religion-based concept?
That's the topic of a session being presented at York College next month by two scientists — Ken Miller and Eugenie Scott — who consulted for the plaintiffs in the landmark science-in-education case.
Scott is the recently retired executive director for the National Center for Science Education, while Miller is a biologist and co-author of one of the most widely used high school science textbooks. He's also the author of "Only a Theory," which explores intelligent design and the Kitzmiller v. Dover Area School District case.
What if Intelligent Design Had Won? will be presented 7-9 p.m. Thursday, Nov. 5, at the college's DeMeester Hall. It's open to the public.
"It will be about ... the ramifications of this big decision," said Karl Kleiner, associate professor of biology at the college. "It's not just about the teaching of evolution but rather what happens when ideology trumps science, when people's beliefs trump well-established fact."
Ten years later: Creation science, abrupt appearance theory, intelligent design, anti-evolution — they're all the same idea presented in a different package, Scott said.
Ten years ago in Dover, the debate centered around intelligent design.
Scott — in conjunction with the nonprofit science center dedicated to keeping evolution and climate change in science classrooms — served as an advisor for the plaintiffs and their legal team in the case against teaching the pseudo-science.
"Intelligent design, to use evolution terms, is a lineal descendent of creationism," Scott said. "The history of the anti-evolution movement is based in presenting creationism in a form they'd be able to teach in classrooms."
Relabeled: After the teaching of actual Bible verse was rejected by the public school system, creation science made its way into the classrooms.
"As it turned out, creation science was only very thinly disguised, and the scientific qualifications were essentially zero, so the courts struck that down as well," Scott said. "And then the next iteration was intelligent design, the biggest difference being it doesn't use the word creation. Intelligent design doesn't immediately sound like a religious view until you ask who the designer is."
In October 2004, the Dover Area School Board adopted a policy requiring that intelligent design be mentioned in ninth-grade biology, resulting in the now-famous Kitzmiller vs. Dover Area School District trial in which the ACLU of Pennsylvania sued on behalf of 11 parents.
Judge John E. Jones III on December 20, 2005, issued a 139-page decision ruling that the board's policy was unconstitutional. The ruling concluded that intelligent design is not science and permanently barred the board from adding it to the science curriculum.
"The crux of the argument was to show the judge, in no uncertain terms, that intelligent design was a relabeled form of creationism," Scott said.
"The Supreme Court had ruled decades before that (creationism) was not constitutional — you can't advocate teaching of creationism in public schools because that'd be promoting religion, and we need the schools to be neutral."
Divine: Scott said her "favorite" version of repackaged creationism is the abrupt appearance theory, which offers alleged scientific evidence of everything happening at one time as opposed to organisms appearing over billions of years.
"It emerged shortly after creationism, but it never really caught on," Scott said. "It didn't really appeal to the conservative Christian base. Creationism is based on the implication of a creator, intelligent design implies the designer — things just poofing into existence isn't quite as satisfying from a religious standpoint."
And therein lies the challenge for those trying to relabel creationism today, Scott said.
"The problem is, in my opinion, that the creationists are kind of stuck," she said.
"They can't come up with an agent-less form of creationism, there has to be that divine agent or it's not really creationism, but that divine aspect is also exactly what keeps it out of the classroom."
Now: Just because creationism hasn't re-emerged with a new name doesn't mean that its proponents have given up, Scott said.
"After Kitzmiller there was a doubling down on another strategy that hasn't got quite as much attention but is still around," Scott said.
"Now there is way more of just attacking evolution."
There also was the emergence of the academic freedom laws.
"They should be called the evolution bashing laws," Scott said with a laugh.
"Academic freedom laws have been submitted in a dozen or more states, only two of them have passed — two too many as far as I'm concerned — in Louisiana and Tennessee.
"They're very cleverly written to permit teachers to bring in supplemental materials beyond the regular curriculum that would allow them raise discussions on controversial topics. They sort of recast anti-evolution as students engaging in critical thinking."
Read or Share this story: https://www.yorkdispatch.com/story/news/2015/10/02/what-if-dover-had-prevailed-intelligent-design/73539668/

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Why do ladder accidents happen on the job?
On behalf of Occupational Injury Law Center posted in workplace accidents on Wednesday, November 28, 2018.
Even if you use a ladder every day on the job, there's still a chance you could be involved in an accident. This is why it's important to use extreme caution at all times.
Placing the ladder on uneven or soft ground: A ladder should only be placed on level and firm ground, in a place where conditions will not change.
Neglecting to maintain three points of contact: If you don't do this, there's a much greater chance of your ladder tipping or you slipping and falling to the ground below.
Using the wrong size ladder: There is more than one type of ladder, and you need to choose the right one for the job. For example, using a portable ladder when an extension ladder is required is a safety risk.
Overreaching: If your ladder isn't long enough, you may find yourself overreaching. This can cause you to lose your balance.
Missing the last rung: When climbing down a ladder, pay close attention to where you are. If you miss the last rung, you could stumble to the ground below.
These are some of the most common reasons for ladder accidents, but there are many others that require your attention.
If you are injured on the job, report the incident to your employer. As you recover, don't push yourself by attempting to return to work too soon. Instead, if you need time off to recover, look into filing a claim for workers' compensation benefits.


text:
Tennis World Tour 2 Roster Revealed, Includes 38 Players
NACON and Big Ant Studios have revealed the full roster for Tennis World Tour 2, which includes Rafael Nadal, Ashleigh Barty, Roger Federer and "legends" such as Marat Safin and Gustavo Kuerten. Check out the full roster below. New features: the ability to play doubles matches with up to 4 players locally and online, a […]
Tony Stewart's All-American Racing Patch Adds New Sponsor Logos, Fixes & Improvements – Patch Notes
Another small game update has arrived for Tony Stewart's All-American Racing, adding new sponsor logos for Tony Stewart Racing and LakeSide Media, adds more characters for custom team names in Career Mode and a few other fixes and improvements. Check out the patch notes below. Added new sponsor logos for Tony Stewart Racing and LakeSide Media […]
F1 2020 Patch 1.09 Available For PC, PlayStation 4 & Xbox One – Patch Notes
F1 2020 game update 1.09 is available now for PC, PlayStation 4 and Xbox One. Google Stadia owners will need to wait a little while longer. The new patch includes plenty of livery updates and addresses quite a few issues. Check out the patch notes below. The Multiplayer car is now available to use in split-screen and […]
NBA 2K21 Patch 1.02 Available – Pro Stick Shot Aiming Adjustments, Gameplay Tweaks & More
NBA 2K21 game update 1.02 is available now for Xbox One and PlayStation 4, we assume it will be released shortly on PC and maybe the Nintendo Switch, but haven't heard anything official. The latest NBA 2K21 patch includes adjustments to the Pro Stick Aiming system, gameplay, MyCAREER, MyTEAM, MyLEAGUE/MyGM and more. Check out the […]
NBA 2K21 MyCareer Review – Decent Story Still Heavy On The Cheese
This year's NBA 2K21 MyCareer story follows Junior, son of beloved neighborhood hero Duke. Aptly named "The Long Shadow," Junior is a talented and raw baller turned football player who has spent endless nights on the blacktop being trained (and arguably bullied, only like an athlete father could) to surpass his father Duke. Duke, voice […]
NBA 2K21 MyTeam Review: The Good, Bad, Ugly So Far
NBA 2K21 MyTeam is a bit overwhelming this year — and this is coming from a seasoned pro. There's new modes, different gem tier divisions and an entirely new currency (XP) to worry about. But the "too much" from my convoluted title to this article is actually about the frustrations of re-learning how to shoot […]
Captain Tsubasa: Rise of New Champions Review – Don't Sleep On It
Released worldwide on August 28, 2020, Captain Tsubasa: Rise of New Champions blends anime with soccer as you follow the exploits of Tsubasa Ozora in the series' first game since 2010's Captain Tsubasa: New Kickoff. Released on the PC, PS4, Xbox One and Nintendo Switch, this new Captain Tsubasa game has that old school Nintendo […]
Madden 21 Custom Roster Review – REALISTICROSTER21 on Xbox One
Brian is going to be trying to do a new thing where he looks at created content from OS and beyond and talks about what he thinks of all that goodness. This could be sliders, rosters and so on. He starts off today with a look at a Madden 21 custom roster on the Xbox […]
Tennis World Tour 2 – What You Should Know Before You Buy the Game
If you're still riding that high after watching Osaka and Thiem claim US Open titles, maybe you're wondering what tennis games are on the horizon. If that's the case, Prince is here to give you a quick outline of everything you need to know about Tennis World Tour 2 before it comes out. [embedded content] […]


One unique type of business that comes up is joint ventures. Often at some point, companies are offered the opportunity to collaborate with one another, to work together, and to capture more value by working as a team than individually. Often, you'll have two unrelated companies, but they have different expertise and contacts and abilities, and they can come together and create more value as a whole than they could individually, by working together.
Often this comes together in the form of a joint venture. We work with clients to negotiate these types of structures, to make sure that they're being protected while still providing access to the value creation. We want to make sure the deal gets done if it makes sense to do so, but we also want to make sure that our clients are protected. There are provisions in place in the event bad things happen, and these provisions make sure that they get paid for the work they do. If you're negotiating a joint venture, you want to have somebody with some experience looking out for you, making sure you get what you deserve, to make sure that your hard work and effort is going to be paid for in the end.


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Insight: "How Obasanjo's Failed Third Term Agenda Was Funded" – New Book
Posted by Mr Ejump on September 14, 2018, Under: 9ja news
"Too Good To Die: Third Term And The Myth Of The In Dispensable Man In Africa" By Chidi Odinkalu & Ayisha Osori
A new book has given an insight into how money was raised for the spirited campaign to keep former President Olusegun Obasanjo in office beyond his second term in 2007. It also reveals how the campaign began and the individuals who conducted it.
The so-called Third Term Agenda collapsed May 16, 2016 when the Nigerian Senate threw out the Constitutional Amendments Bill.
Mr Obasanjo left office a year later on May 29, 2007 and has since stridently denied being interested in staying longer or playing any part in the agenda, despite admissions to the contrary by some of the principal actors.
The new book, however, a close scrutiny of the Third Term Agenda, names some of the aides and associates who pushed the agenda, states how a massive war chest was built for it and reveals some of the sources and individuals who provided the money.
The book, "Too Good To Die: Third Term And The Myth Of The In Dispensable Man In Africa", was written by Chidi Odinkalu and Ayisha Osori.
Mr Odinkalu, a lawyer and civil rights advocate, is senior team manager for the Africa Program of the Open Society Justice Initiative and former Chairman of the Governing Council of the National Human Rights Commission.
Mrs Osori, also a lawyer, writer and management consultant, is the executive director of the Open Society Initiative for West Africa (OSIWA).
How Much Was Spent
According to the authors, although Nuhu Ribadu, who at the time was Chairman of the Economic and Financial Crimes Commission (EFCC), estimated the campaign gulped $300 million, evidence suggested the cost was much higher.
"When all the cost elements, including the public relations campaigns, additional incentives, the work of the JCCR (Joint Committee on Constitutional Review of the National Assembly) and constitutional conference, as well as inevitable incentives to the security services, are added to the inducements proposed for legislators, it seems almost certain that the budget for the third term was in excess of $500 million or half a billion dollars," the authors state.
How Money Was Raised
The book provides an insight into how the money was raised.
"None of this money was lawfully appropriated. They could only have been generated by theft, diversion or misappropriation of public resources.
"Among many sources that were raided, the Obasanjo administration patented and pioneered a habit of unusual withdrawals from Nigeria's Excess Crude Account, a rainy day, sovereign savings scheme funded by the extra earnings from Nigeria's petroleum exports.
"2006, the year in which President Obasanjo hoped to achieve an elongation of his tenure by constitutional amendments, was by some unusual coincidence also the year in which Nigeria achieved the highest inflow into the ECA. In that year, the fund had an inflow of $29.614 billion from oil export earnings.
"In the same year, however, the administration also inexplicably authorized withdrawals from the ECA totaling the sum of $29.799 billion, resulting in a net negative balance of $184.404 million. In one year from 2005 to 2006, coinciding with precisely the most active period of the third Third Term Agenda, President Obasanjo authorised unusual payments totalling12.176 billion Naira, reportedly to fund the Niger Delta Power Plants and the National Independent Power Project (NIPP).
"Until then, this volume of payments out of the ECA was unprecedented. There is scant evidence that these sums were in fact administered for the declared purpose.
"Some of the disbursements from the ECA may plausibly have gone towards public purposes like the management of Nigeria's debt settlements. It is not inconceivable though that at least some part of the ECA's net negative balance went to fund activities connected with President Obasanjo's Third Term Agenda."
Following the collapse of the agenda, President Obasanjo went after some of those he held responsible. One of these was Atiku Abubakar, his vice president, whom a panel he set up and the EFCC indicted of fiddling with funds at the Petroleum Technology Development Fund (PTDF).
Mr Abubakar appeared before a 13-member Senate committee on 18 December 2006 to address the allegations raised by Mr Obasanjo and the EFCC report.
"Atiku proceeded to share with the committee various transactions and approvals Obasanjo had been involved in specifically with the PTDF. For instance, six days before the Senate killed the third term project, President Obasanjo approved the immediate release of N10 billion out of the N20 billion requested by PTDF for undisclosed projects. The unspoken suggestion was that Obasanjo had approved these funds to benefit his third term project," the book states.
There were also other sources of funds outside federal coffers.
"Sometime before the National Assembly debate on amendments to the Constitution began, Governor (Saminu) Turaki reportedly sent N17 billion and $20 million in cash to Abuja," the authors state.
"In his defence against money laundering charges brought against him by the EFCC for siphoning N36 billion out of Jigawa State, he admitted that this formed part of his investment in the PDP's third term project.
"Turaki was also among the governors who invested in a third term for Obasanjo because it meant a third term for those who were in their second term of office and extra terms for those in their first. Some of the governors who joined him in the support group of tenure elongation, whether out of self-interest or self-preservation included: Ahmed Makarfi (Kaduna), James Ibori (Delta), Bukola Saraki (Kwara), Umaru Yar'adua (Katsina), Bukar Abba (Yobe) and General Olagunsoye Oyinlola (Osun)."
The budding Oligarchs
But it was not just a public sector affair, according to the book.
"In the shadows were budding oligarchs and private sector operators who knew enough to be part of every government. They had morphed into a formidable clique during the Obasanjo administration as the main beneficiaries of a privatisation policy from which they profited tremendously.
"While the majority were and have not been open about their involvement in or support for a third term, Festus Odimegwu, then Managing Director of Nigerian Breweries at the height of the advocacy for and aginst a third term, threw his hat firmly in the ring for tenure elongation and lost his job for it.
"The cream of this businessmen and women became part of Transcorp, which was launched with much fanfare by Obasanjo at the Presidential Villa in Abuja in July 2005. Transcorp became the symbol, identity and totem of 32 of Nigeria's wealthiest people. In addition to billionaire financiers, Aliko Dangote and Femi Otedola; bankers Tony Elumelu and Jim Ovia, and Odimegwu, this group included former CEO of First Bank Plc, Bernard Longe, who was appointed the first CEO of Transcorp after Obasanjo summarily removed Fola Adeola, the pioneer Managing Director of Transcorp.
"Apart from having a mind of his own, Adeola was said to have harboured ambitions to run for a seat in the Senate, in which Obasanjo's eldest child, Iyabo, a veterinary doctor, was also interested. After he made his anti-third term public, Obasanjo also had Adeola summarily removed from his position as Chairman of the Pension Commission.
"Others included Jacobs Moyo Ajekigbe, MD/CEO of First Bank of Nigeria Plc.; Otunba Funsho Lawal, CEO of Charterhouse Group; Tony Ezeanna, CEO of Orange Drugs and Adegboyega Olulade, an investment banker and stockbroker.
"Also part of this group until his death was Waziri Mohammed. From the Nigerian Stock Exchange, Nicholas Okoye, who was designated as the head of derivatives trading, joined his boss and Director General, Ndi Okereke-Onyuike, in this select assembly of Obasanjo's favoured businessmen and women.
"Transcorp raised N16 billion through private placement and had the good fortune to be the successful bidder for 71 percent of Nigeria's former telecommunications monopoly, NITEL. It was also proud owner of Nicon-Noga Hilton Hotel, which many considered a national heritage, a concession for a 400,000-barrel per-day refinery at the Lekki Free Trade Zone and independent power plants.
"Other assets auctioned to the group were oil blocs to enable the new company operate in the upstream oil and gas industry. The controversy around Obasanjo's acquisition of 200 million shares of Transcorp gave no pause to his ardent supporters for whom he was the model of exemplary leadership.
"A few months after the launch of Transcorp, the Manufacturers Association of Nigeria (MAN), made a case for a third term for Obasanjo. Charles Ugwu, the president of MAN, suggested that he spoke for the private sector in support of tenure elongation when he described Obasanjo as an example of rare, experienced and mature human resource.
"Addressing the 34th annual general meeting of the MAN on 15 November, 2005, Ugwu asked rhetorically: '(S)hould we package him in a box and put on a shelf of retired leaders and seek out a neophyte with whom we would experiment?" The benefits of a close collaboration between the presidency and private sector were too glaring or resist,' he argued.
Agenda With Long Roots
According to the narrative by the authors, the seed for the Third Term Agenda was planted in the first term of President Obasanjo.
"The seed germinated perhaps innocuously, from the idea that political stability and continuity of policy was vital to Nigeria's economic development.
"As chairman of the G77 developing countries, Obasanjo was an active and vocal advocate for debt relief in the context of the Jubilee 2000 global campaigns calling for debt relief for Heavily Indebted Poor Countries (HIPC).
"This required meeting conditions of the Bretton Woods institutions, some of which entailed economic reforms. With this realisation, the Obasanjo administration reportedly worked feverishly, first with his ALF (African Leadership Forum), and then with the New Partnership for Africa's Development (NEPAD), to create a blueprint for economic reforms. Their efforts came to be known as the National Economic Empowerment and Development Strategy (NEEDS).
"During this exercise, the penny dropped. It dawned on Obasanjo that he would not be in office long enough to oversee his plans for Nigeria and towards the end of 2002, sources recalled, in a meeting about the reforms which would lead to debt relief, President Obasanjo confessed that he would not be able to execute his vision without first tackling the political problems, starting with his own party, the PDP."
The campaign for debt relief for Nigeria eventually yielded results in 2005 when the Paris Club of creditors granted Nigeria debt forgiveness to the tune of $18 billion after an agreement that the country was owing US$30 billion and would immediately repay the US$12 billion balance.
"Advocates of 'consolidation' sprouted, nourishing the roots of the idea that Obasanjo needed more than two terms in office. The Nigerian shorthand for this was tazarce, the noun for 'continuity' in Hausa, the major language in Northern Nigeria," the authors state.
It started with the campaign for Mr Obasanjo to seek reelection, against the backdrop that he had in 1998 reportedly pledged to those who prodded him to power that he would serve only one term.
One of the leading advocates, Tony Anenih, said about his support for a second term for Obasanjo that '… it would be unwise not to allow Chief Obasanjo have a second term. This second term would enable him consolidate and complete the transformation of the society'".
Mr Anenih was at the time Minister of Works and Housing. After Mr Obasanjo's reelection, the book states, the plans for a third term began in earnest.
Different Interests, Repeat Offenders
"The people and stakeholders that worked together for a third term for Obasanjo were driven by different reasons and interests; for instance, self-interest was an underlying motive for many," states the authors.
Aside cabinet members like Nasir El-Rufai, Ngozi Okonjo-Iweala and Frank Nweke, were others like Nuhu Ribadu who was chairman of the Economic and Financial Crimes Commission.
"Many of the courtiers for Obasanjo's self-succession were repeat offenders from previous episodes with uniformed military rulers. The currency of such campaign, they knew, was cash – lots of it.
"It was expensive to incentivise people, mobilise support across the country and hold conferences and rallies in support of any self-succession plan and best of all, most transactions were in cash and largely untraceable.
"Legislators needed the money to buy their reelection or prepare for their retirement amidst the realization that they could become electoral liabilities, irrespective of how third term ended. Governors needed money to buy off legislators in or from their states and Obasanjo and his acolytes were in a similar predicament at the federal level.
"The natural logic of Obasanjo's third term aspiration was predicated on him spreading money around. Corruption was a necessary and inherent element of the Third Term Agenda.
"This gave birth to a cottage industry of third term investors and beneficiaries from the military god complex such as Femi Fani-Kayode and Andy Uba. Some did not fall neatly into any category but were driven by their closeness with Obasanjo to fall for the narrative that Obasanjo was Nigeria's best option for progress and development.
"Finally, there were the legislators who formed a key part of operations to secure a third term for Obasanjo. In the Senate, Ibrahim Mantu, Ifeanyi Ararume and Jibril Aminu were some of the leading figures involved in the lobby to induce legislators to accept the constitutional amendments.
"Within the House of Representatives, there were several caucuses across interests, geography and parties. For instance, there was the Unity Forum led by David Idoko. Under the guise of advocating for the unity of Nigeria, this group of legislators sought to drive support for the Third Term Agenda within the public and amongst legislators. In return, many of them were reportedly well rewarded.
"These foot soldiers committed to the glory of a third term, an ode to Obasanjo's now personal god complex, worked towards their goal with the aid of various strategies guided by Obasanjo's mechanical engineering mind. What was needed? Who was needed? Who could be bullied or bought?
"Some of the strategies were familiar and had been used by other self-succession artists. The key tool was incentives – the trade by barter that had worked so well in keeping elite support for military rule for over 29 years.
"Positions were offered. Sitting governors, for example, would enjoy tenure elongation as well and several loyalists from the North had been promised that they would become Obasanjo's vice president during his third term.
"Financial reward was also a huge inducement. The most credible figure for members of the National Assembly was N50 million for each member of the House and N75 million for each senator who would vote for the tenure extension amendment."
Mr Obasanjo has repeatedly denied he ever planned to stay longer than the two terms the Nigerian Constitution allows a president and governors. But he has yet to speak on the claims in this new book.
Source:- Premiumtimesng
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\section{Introduction}
Since Halton Arp published an atlas of peculiar galaxies and \cite{Toomre72} reproduced their shape with numerical simulations of tidal encounters, mergers  have become key processes in the understanding of galaxy evolution.
Simulations show how  colliding disk galaxies are reshaped into  pressure-supported early-type bodies after the final merger. In a $\Lambda$CDM cosmology \citep{Spergel07}, which assumes that the assembly of large scale structure happens in a hierarchical fashion,   mergers  play a fundamental  role in the growth and evolution of galaxies \citep{Conselice09}.

During the intermediate phases of interactions,  large scale tidal interactions trigger the formation of peculiar features like shells, streams, bridges and tails. The presence of such structures which is predicted by numerical simulations  is now frequently  observed in deep imaging surveys \citep{Duc11,Duc14b,Kim12,Struck99,vanDokkum05}.

Numerous works have detailed the various phenomena occurring during galaxy interactions, including the formation in the collisional debris of substructures, like  Tidal Dwarf galaxies (TDGs)  \citep{Duc07}. However the vast majority of such studies focused on massive galaxies. Not much is known on tidal forces  generated by the encounter between low mass galaxies.

It is common belief that,  having a shallow potential well,  low mass galaxies have  an evolution which is more driven by the large-scale environment than by  merging events. Dwarf galaxies exhibit a strong morphological segregation: the most evolved / oldest dwarf galaxies, i.e dwarf Spheroidal (dSph) or dwarf early-type (dE), are found in the group and cluster environments \citep{Kormendy09,Lisker09}, while  dwarfs with on-going  star-formation activity, such as Blue Compact Dwarf galaxies (BCDs, \citealt{Gil03,Papaderos96}) are mainly found in less dense environments.
However, how precisely the environment contributes to the transformation  of star-forming dwarfs to anemic dEs is still a puzzle as several processes may play a role  \citep{Boselli06}.  Besides,  the mechanism that triggers the burst of star-formation in dwarf galaxies, particularly in BCDs, also remains a mystery.  Mergers, fly-by encounters or gas turbulence have been proposed \citep{Bekki08,Noeske01,Pustilnik01}.

Very recently, observational evidence for mergers between dwarf galaxies has  been growing \citep[e.g.][]{Amorisco14,Crnojevic14,Toloba14,Delgado12,Johnson13,Nidever13,Graham12,Penny12,Rich12,Geha05}. The possibility that dEs might be formed through mergers like the massive ellipticals has been proposed. If this is the case, one would expect the progenitors of dEs to exhibit the characteristics features of  mergers such as tidal tails.

The system presented here, UGC~6741,  was initially disclosed in a systematic eye inspection of tidal debris in the Sloan Digital Sky Survey (SDSS) images. It turned out to be  classified as a low surface brightness galaxy pair in \cite{Schombert98}.
We report a multi-wavelength study of the system based on  archival optical images and spectra from the SDSS  DR7 release and UV-images from the Galaxy Evolutionary Explorer (GALEX) all sky survey \citep{Abazajian09,Martin05}.

 \begin{figure}
\includegraphics[width=9cm]{colf.pdf}
\caption{True color $g+r+i$ SDSS image of  UGC~6741. Compact blue star-forming regions are distinctly visible in the tidal bridge between UGC~6741 and its companion disrupted galaxy, UGC~6741\_B. The 65" $\times$ 100" cutout image was queried from the SDSS DR7 sky server.}
\label{cfig}
\end{figure}

   \begin{figure}
\includegraphics[width=8.5cm]{group.pdf}
\caption{Position of UGC~6741 (en-circled)  in the NGC~3853 group. The  central galaxy, NGC~3853, is shown with a  black dot and the other group members with  red dots. }
\label{grp}
\end{figure}

 \section{Data and Analysis}

\subsection{Target selection and location}

 In an our effort to search for tidal features around  low mass nearby galaxies, we visually inspected true color ($g+r+i$) SDSS images of nearly 40 000 galaxies located at   redshift below  0.02.
The  most prominent tidal feature  was  found in the galaxy pair, UGC~6741.
 With a luminosity M$_{r}$ = $-$17.7 mag,  UGC~6741 is slightly fainter than the two well known local group dwarf galaxies, the Large Magellanic Cloud (LMC) and NGC~4449 \footnote{Incidentally  these two latter galaxies are also involved in a tidal interaction.}. Its interacting companion, here after UGC~6741\_B,    has a luminosity of  M$_{r}$= $-$16.2 mag  \footnote{Throughout the paper, we assumed a distance to the galaxy of  D =  54.2 Mpc, which is the distance of the main galaxy group member, NGC~3853 provided by NED.}.

By chance,   UGC~6741 benefits from substantial  multi-wavelength data  in public archives, which  allowed  us to perform a thorough  analysis of its morphology,  chemical properties and stellar populations.

As shown in  Figure~\ref{cfig} and Figure~\ref{mfig}, a 15 kpc  long stellar bridge connects  the two galaxies along the North-South direction.
 It hosts a number of  compact blue clumps -- the most prominent  ones are named objects A, C, D, E and F. Object F is located to the North of  UGC~6741, and either belongs to a secondary tail or to the bridge if the latter wraps around in the proximity  of the galaxy. Overall   the  system resembles classic mergers of massive gas-rich disk galaxies.

 UGC~6741 is located on the outskirts of a group with an angular distance of 0.73 degree from the central galaxy, NGC~3853. In Figure~\ref{grp}, we show the group member galaxies located around a radius 700 kpc centered on NGC~3853   and with relative radial velocities  within $\pm$500 km/s. We used the NED database to carry out this search. The  difference in radial velocity between  NGC~3853 and UGC~6741 is less than 100 km s$^{-1}$.

\subsection{Imaging and Photometry}

To perform a detailed image analysis, we retrieved archival images from the SDSS-DR7 database \citep{Abazajian09}. We used the $r$-band image as a reference, since it provides a higher signal to noise ratio on the tidal debris than the other bands. The seeing in this field is  0.9" (as measured from the $r$-band PSF).  In order to enhance the detectability of the bridge and the faint objects within it, a $g+r+i$ co-added image was made (see Fig.~\ref{mfig}, left), and a galaxy model subtraction has been carried out (see Fig.~\ref{mfig}, middle).  On such images, object B appears to be much more luminous,  extended and redder (see Fig.~\ref{mfig}, right) than the clumps A, C, D, E and F located along the tidal feature. As previously mentioned, B is most likely the main body of the disrupted  companion of UGC~6741.
The bluest clump, object E, is  located at the upper tip of the bridge and  embedded within the stellar halo of UGC~6741. Object A is somewhat irregular and  contains several compact sub-clumps.

\begin{figure*}
   \includegraphics[width=18cm]{dmap1.pdf}
  \caption{The interacting system, UGC~6741, as seen in the optical with the SDSS.  {\it Left:} co-added $g+r+i$ image with an arcsinh scaling.
  The black contours represent the detection limit of 3$\sigma$  corresponding to a surface brightness level of $\sim$25.5 mag-arcsec$^{-2}$ in the r-band.  {\it Middle:} Residual image after having subtracted a model galaxy of UGC~6741.  Prominent star-forming clumps are named in alphabetical order starting from the bottom.  Note that  object B is likely  the main body of the  low-mass companion of UGC~6741 and is referred as UGC~6741\_B in the main text.
 {\it Right:}   $g-r$ color map, with the scale in mag indicated to the right.  The field  of view of each image is 90" $\times$ 120". }
  \label{mfig}
   \end{figure*}

The  total luminosity of the clumps was determined from aperture photometry. The sky value has been estimated  in 5 independent regions  of 10$\times$10 pixel randomly chosen  around UGC~6741.  Their mean value was computed and subtracted from the measured fluxes.
We list the positions, absolute magnitudes and stellar masses of the clumps in Table \ref{ftb}.
The derived magnitudes were  corrected for the Galactic extinction using \cite{Schlafly11}, but not for the internal extinction.
We find that all of them  have $g-r$ color index less than 0.25 mag and the bluest, F, has a  $g-r$ color index as low as -0.03 mag. Their blue color and detection in the UV by GALEX (see Fig \ref{galx}) is totally consistent with the hypothesis that they are star-forming regions.
The stellar masses were derived from the SDSS$-r$ band magnitude with a mass to light ratio tabulated by \cite{Bell03} and appropriate to the observed  $g-r$ color.  These  values are most likely upper limits.

 \begin{table*}
 \caption{ Global properties of the system}
\begin{tabular}{lccccclccc}
\hline
Galaxy &Ra & Dec & Mr & v$_r$ & M$_{*}$ & SFR(m$_{FUV})$ & 12 + log(O/H)  & R$_{e}$ & $<\mu>_{r}$\\
\hline
 & $^{o}$ &  $^{o}$ & mag & km s$^{-1}$ & M$_{\sun}$ & M$_{\sun}$ yr$^{-1}$ & dex & kpc & mag arcsec$^{-2}$\\
\hline
UGC~6741       & 176.4793 & 17.1923  &  $-$17.74$\pm$0.01  &      3390  &  $6.0 \times 10^{8} $    &  0.09(17.96$\pm$0.08)   &  8.3 & 1.2 & 21.71 \\
UGC~6741\_B  & 176.4827 & 17.1732  &  $-$16.16$\pm$0.01  &      3300  &  $ 1.9 \times 10^{8} $     &  0.03 (19.01$\pm$0.12)$^{*}$  &  8.3 &   -- & -- \\
\hline
\end{tabular}
\label{ptb}
{\\
\\
 The SFR is estimated from the FUV magnitude  given in the parentheses.  A galactic extinction correction has been applied using the formula A$_{FUV}$ = 8 $\times$ E(B-V) with E(B-V) = 0.2.  The stellar mass is derived from the $r-$band luminosity and the mass to light ration obtained from \cite{Bell03} for the color $g-r$. The value of the Oxygen abundance, 12 + log(O/H),  is derived with the  O3N2 method which has a typical systematic error of  0.2 dex. \newline
$^{*}$ The FUV flux and derived SFR includes the star forming region A, see Fig \ref{mfig}.}
\end{table*}

The extended Clump A, located at the  tip of the tidal feature,  is the brightest star-forming region. The fairly compact regions  C, D and and E  are actually likely wrongly  classified as stars in the SDSS catalog. Our measured FWHM for these  knots are well consistent with the median FWHM of foreground stars, i.e. 0.9" and in the absence of available   radial velocities, we cannot  totally exclude chance superposition of  foreground blue stars or background compact objects. However, the remarkable alignment of these objects along the stream and their similarity in color (see Figure~\ref{cfig} \& \ref{mfig}) are strong hints for a real physical association with the system.

The interacting dwarf galaxies and associated tidal debris are  clearly detected in the NUV, and barely detected in the FUV by the GALEX all sky survey (see Fig.~\ref{galx}).  Since the GALEX images have a spatial resolution of only 5", the star-forming regions are not resolved individually in the UV images. The  star formation rates, derived from the FUV fluxes applying a  Galactic extinction correction from  \cite{Schlegel98}, and using the calibration of \cite{Kennicutt98},   are given in Table \ref{ptb}.

\begin{figure}
\includegraphics[width=8.5cm]{galex.pdf}
\caption{GALEX all sky survey NUV (left) and FUV (right) images of UGC~6741.}
\label{galx}
\end{figure}

With the help of the IRAF $ellipse$ task, we performed a surface photometry analysis of  UGC~6741. First, we extracted the galaxy major-axis light profile from the $r-$band image. In doing so, the centre and position angle of the ellipse were held fixed and the ellipticity was allowed to vary. The centre of the galaxy was calculated using the task $imcntr$ and input ellipse parameters were determined using the several iterative runs of the $ellipse$ task. The derived $r-$band major axis light profile of UGC~6741 is shown in Figure~\ref{prof}. With the help of $\chi^{2}$-minimization scheme, we obtained a best fit model where the observed profile is decomposed into the two component S\'ersic functions. The inner and outer components are best fitted with the S\'ersic functions of n = 0.61 and 3, respectively.

\begin{figure}
\includegraphics[width=8.5cm]{profile.pdf}
\caption{Major axis radial profile of UGC~6741, where the observed profile is fitted with two component S\'ersic model.  }
\label{prof}
\end{figure}

Since the observed light profile of UGC~6741 is better represented by a multi component S\'ersic function the derivation of the effective radius and effective surface brightness is not obvious.  Therefore, we estimated these parameters with a non-parametric approach. Using the similar procedure followed by \cite{Janz08}, we first calculated the Petrosian radius and the total flux was measured within  two Petrosian radius. Note, that contrary to   \cite{Janz08},  we do not correct for the the missing flux estimated  by \cite{Graham05}. Indeed this correction is very small for dwarf galaxies \citep{Chen10}. The derived values of the structural parameters of UGC~6741 are given in Table \ref{ptb}. We find that the mean surface brightness within the half-light radius is 21.7 mag arcsec$^{-2}$ in the SDSS $r-$band. This is in fact a rather low value of the surface brightness of a low-surface brightness galaxy, as described in \cite{Schombert98}.

   \begin{table}
   \caption{Photometry of the  star forming tidal clumps}
   \setlength{\tabcolsep}{0.06cm}
\begin{tabular}{lcccccc}
\hline
 & Ra & Dec  & g  & r & i & M$_{*}$  \\
  &$^{o}$ & $^{o}$ & mag & mag  & mag& 10$^{8}$M$\sun$  \\
\hline
A & 176.4821 & 17.1704 & 18.46$\pm$0.02 & 18.52$\pm$0.03  & 18.39$\pm$0.04 & 0.35  \\
B & 176.4827 & 17.1732 & 17.76$\pm$0.02 & 17.51$\pm$0.02  & 17.37$\pm$0.02 & 1.94  \\
C & 176.4820 & 17.1810 & 19.42$\pm$0.03 & 19.55$\pm$0.04  & 19.33$\pm$0.05 & 0.11  \\
D & 176.4817 & 17.1827 & 20.51$\pm$0.05 & 20.73$\pm$0.08  & 20.44$\pm$0.10 & 0.03  \\
E & 176.4808 & 17.1875 & 20.83$\pm$0.06 & 21.07$\pm$0.10  & 20.59$\pm$0.10 & 0.02  \\
F & 176.4775 & 17.1940 & 18.05$\pm$0.01 & 18.08$\pm$0.02  & 18.23$\pm$0.03 & 0.57  \\
U & 176.4793 & 17.1923 &16.05$\pm$0.02 & 15.93$\pm$0.02  & 15.77$\pm$0.03  & 6.02  \\
\hline
\end{tabular}
{\\
\\
The galactic extinction is corrected with \cite{Schlafly11}. Stellar masses are converted from the $r-$band magnitude using the mass to light ratio from \cite{Bell03}, i.e Log(M/L) = $-$0.306+1.097($g-r$)}
\label{ftb}
\end{table}

Besides, we performed the aperture photometry on the entire system. For this, we first manually masked all non-related objects  and selected a large aperture that includes the entire system. The total $r-$band luminosity is m$_{r}$ = 15.53 $\pm$0.01 and $g-r$ color index is 0.1 $\pm$0.01 mag. The FUV and NUV luminosities are 17.21 $\pm$07 and 17.06 $\pm$03 mag, respectively. Using the same conversion factors as for the individual sub-structures, we derived a total stellar mass  M$_{*,\,total}$ = 8.3$\times$10$^{8}$ M$\sun$ and a total star-formation rate SFR$_{total}$ =  0.18 M$\sun$ yr$^{-1}$.

  \subsection{Gas content}
Atomic  hydrogen (HI) 21-cm radio data are available in the Hyperlyda archive \citep{Paturel03}.   Observations of  UGC~6741 were made with the Arecibo single dish telescope. The large beam size, $\sim$3' \citep{Lu93} , covered  the entire interacting system. The cataloged archival HI parameters are listed in Table \ref{hi}.  We computed a total HI mass of  8.7$\times10^{8}$  M$_{\sun}$, and an inferred  HI mass to blue luminosity ratio, M$_{HI}$/L$_{B}$,  of 0.65 M$_{\sun}$/L$_{\sun}$ \footnote{The B-band luminosity was derived from the $g-$band luminosity using the empirical formula of \cite{Lupton05}, i.e  B = $g$+0.313($g-r$) + 0.227 }.
  This number is similar to the average value of M$_{HI}$/L$_{B}$ for the sample of BCDs studied in \cite{Huchtmeier05} but significantly lower than in  typical isolated low-surface brightness dwarf galaxies  \citep{Pustilnik11}. We estimated the expected HI mass of UGC~6741 using an empirical relation between the HI mass and the diameter \citep{Gavazzi05},  $M_{HI ref} = a+b log(d)$. For this, we used the isophotal diameter provided by  NED and adopted the constants a = 7.00 and b = 1.88 for Scd-Im-BCD type galaxies. The expected HI mass is less than half of the observed HI mass in the whole system.

The HI spectrum shows a single velocity peak  \citep[see Fig. 1 in ][]{Lu93} that may suggest the absence of a kinematically distinct HI component for each galaxy. Note, however, that the observed velocity width is similar to the difference in radial velocity measured from the optical spectra of each galaxy, i.e. 76 km$^{-1}$.

\begin{table}
\caption{HI gas content}
\begin{tabular}{l|l}
\hline
\hline
HI heliocentric velocity & 3324 km/s\\
HI Flux  & 1.26 Jy-km/s $\pm$10\%\\
HI mass & 8.7 $\times$10$^{8}$\\
Mean velocity width & 79.89 $\pm$1.2 km/s\\
M$_{HI}$/L$_{B}$  & 0.65 \\
\hline
\end{tabular}
\label{hi}
\end{table}

\subsection{Optical spectroscopy}
The optical spectra of both UGC~6741 and UGC~6741\_B  were queried from the SDSS archives (see Fig.~\ref{spec}). They exhibit the  emission lines typical of HII regions as well as   relatively strong absorption  for the early  Balmer lines H$\delta\, ,\gamma\,$ and $\,\beta$.
The emission line fluxes were measured after subtracting the stellar absorption features  using the publicly available code  GANDLF \citep{Sarzi06} and the stellar templates of  \cite{Tremonti04}.

The extinction coefficient, E(B-V), derived from the Balmer decrement H$\alpha$/H$\beta$  is nearly equal to zero for UGC~6741 and even below the standard value of 2.86 for UGC~6741\_{B}. This  may indicate a poor subtraction of the absorption at H$\beta$ due to the low signal to noise ratio.

The H$\alpha$ equivalent widths -- 7.1 \AA{} and 8.7  \AA{} for UGC~6741 and UGC~6741\_B respectively --  are relatively small compared to the typical BCD's H$\alpha$ equivalent widths \citep{Gil03}.

Oxygen abundances, 12+log(O/H), were estimated with the  two  methods described, among others,  by \cite{Marino13}, i.e the so--called N2 and O3N2 methods. The N2 method only considers the line ratio between H$\alpha$ and [NII]  while the O3N2 method uses a combination of the line ratios H$\alpha$/[NII] and [OIII]/H$\beta$. We obtained 12+log(O/H) = 8.3(8.3) and 8.3(8.2) dex from the N2(O3N2) method for  UGC~6741 and  UGC~6741\_B, respectively. These values are in the range of typical  BCDs \citep{Gil03,Vaduvescu07}.
The systematic error of the methods is 0.2 dex.

 \begin{figure*}
 \includegraphics[width=18cm]{spec.pdf}
 \caption{SDSS optical spectra of UGC~6741 and its companion UGC~6741\_B. The observed spectra are shifted to rest frame wavelength and smoothed with a 3 pixel gaussian kernel.}
 \label{spec}
\end{figure*}

\section{Discussion and Conclusion}
We have presented a case of a dwarf-dwarf merger in a group environment. Remarkably our multi-wavelength study, based on imaging and spectroscopy,  could be carried out with data solely acquired from publicly available archives.

We discuss below the  origin of its  prominent star--forming tidal bridge and speculate on the future evolution of  UGC~6741.

 \subsection{Nature of the tidal features and its star-forming regions}
 UGC~6741 is noteworthy for the presence of a tidal bridge hosting  knots of star-formation, and in that respect resembles systems involving massive colliding  galaxies, such as   Arp~104  \citep{Gallagher10} or Arp~188 (UGC~10214), also known as the Tadpole galaxy.
  A comparison between  these systems is made in Figure~\ref{comp}.

 \begin{figure}
 \includegraphics[width=8.5cm]{Combine.pdf}
 \caption{Direct comparison between Arp~104 and Arp~188 (in blue scale) with UGC~6741 (in grey-inverted scale). The optical $r-$band images for Arp~104 and Arp~188 were also obtained from the SDSS. }
 \label{comp}
\end{figure}

Like UGC~6741, Arp~104 exhibits a prominent tidal bridge, with hints that part of the tidal material wraps around one of the interacting galaxies (NGC~5218,  to the North). For this system however, there is no evidence for the presence of star--forming regions along the bridge.

 Like in UGC~6741, the long single tail that emanates  from Arp~188 hosts multiple compact knots of star formation. Some of its  young massive star cluster  are as massive as $\sim$$10^{6}$ M$_{\sun}$ \citep{Tran03,Grijs03,Jarrett06} and were most likely formed in situ in the tail out of  gaseous material expelled from  UGC 10214 during a dynamical interaction  with a hidden or already destroyed companion.

 Given its shape, the stellar filament  of the system studied here is undoubtedly of tidal origin.  Is  it however  as for  Arp~104 a bridge connecting two  interacting galaxies, namely UGC~6741 and  UGC~6741\_B, or a single tail like in Arp~188, with UGC~6741\_B being  a  Tidal Dwarf Galaxy
 instead of a pre-existing object?

Interestingly, the gas phase metallicity derived from the SDSS archival spectra reveals within the errors no difference in Oxygen abundance between UGC~6741 and UGC~6741\_B although the latter is three times less massive. The mass-metallicity relation would predict an abundance of about 0.2 dex lower.

Similar metallicities between the parent galaxy and its tidal dwarf are instead expected as the latter is made from material pre-enriched in the former \citep{Duc07,Duc14}. This may in principle argue in favor of the TDG hypothesis for UGC~6741\_B.
This is however without taking into account the rather large intrinsic scatter of the M-Z relation of 0.2 dex and of the systematic uncertainty in the abundance determination of the same order.

Besides, the existence of a prominent stellar continuum  (see Fig.~\ref{spec})  suggests that the object has a significant fraction of old stellar populations and  the presence of  strong Balmer absorption lines is a signature of star-formation over an extended period of time. The  TDGs  so far discovered are rather characterized by the overall dominance of young stars  and of an on-going instantaneous starburst. This  suggests that UGC~6741\_B is a pre-existing dwarf, which is interacting with UGC~6741.
Therefore, the system would in fact be rather a scale down version of  Arp~104, with an overall  luminosity  $\sim$4 mag fainter.

Evidence of in situ star-formation occurring in  gas rich collisional debris has been reported in numerous massive interacting galaxies, including the Tadpole galaxy discussed above. Such regions are  believed to be also a nursery of   super star clusters \citep[e.g.][]{Grijs07,Mello08,Peterson09,Fedotov11}.
Idealized numerical simulations of mergers reproduce the formation of massive and compact super star-clusters in tidal tails  \citep{Bournaud08,Renaud15}
and predict they might be the progenitors of globular clusters, provided they survive internal feedback and external tidal shear.
The most massive and extended  of them may become independent tidal dwarf galaxies.

The same phenomena seems to also apply to dwarf-dwarf major mergers. The bridge of UGC~6741 hosts at at least four distinct knots of star-formation.  They are as massive as $\sim$10$^{7}$ M$\sun$;  with stellar mass density reaching   $\sim$10$^{8}$ M$_{\sun}$ kpc$^{-1}$
\footnote{Assuming  sizes equal to the observed FWHM}, they could evolve into  globular clusters  or even ultra compact dwarf galaxies.
Their parent galaxies being low-mass systems with shallow potential well, one may speculate that they will survive longer than in the environment of systems involving massive merging galaxies.

 \subsection{Dwarf-Dwarf merger}
\cite{Lucia06} show that the statistical probability of merger of galaxies decreases towards the low mass regime. Our study of UGC~6741, however, proves  that dwarf-dwarf tidal interactions and mergers  occur in the nearby Universe. How frequent are they?
On the one hand, exploring the  Millennium cosmological Simulation, \cite{Moreno13} found that binary  mergers in isolation are very rare, and claimed that satellite-satellite mergers should play a higher role than so far anticipated.
On the other hand, \cite{Klimentowski10} used the Constrained Local Universe Simulation (CLUES) to conclude that interactions between satellites are unlikely. In a group environment, mergers between  sub-haloes are predicted to occur only before they entered the host halo.
Interestingly,   UGC~6741 is itself located in the very  outskirts of a group.

In the real Universe,  reported cases of  possible dwarf-dwarf mergers have increased  recently \citep[e.g.][]{Amorisco14,Delgado12,Penny12,Rich12}.
Distorted HI morphologies and the presence of gaseous tails around starbursting  dwarf galaxies  have also been attributed to mergers  \citep[e.g][]{Johnson13,Nidever13}.
However, direct evidence for an on-going tidal interaction between objects of roughly similar masses remains  rare.  \cite{Rich12} found that  the nearby  Magellanic irregular galaxy NGC~4449 makes a pair with a tidally disrupted dwarf galaxy. This interaction will lead to a 1:50 merger, whereas  UGC~6741 corresponds to a 1:3 merger.
In the world of massive galaxies, this would be considered as a major merger.

\subsection{Evolution of dwarf galaxies}
Several physical properties of UGC~6741, i.e. color, metal content and star-formation rate, are fairly similar to typical blue compact dwarf galaxies and there is little doubt that its star formation activity  is affected, if not triggered,  by the interaction. Once the burst is terminated and the galaxies have merged, which type of dwarfs will UGC~6741 resemble? Its position on the scaling relations between  structural parameters can give clues on its future evolution.

In Figure~\ref{scf}, we  compare its properties  with that of  samples of non-interacting  dwarfs. As a  comparison sample, we used the Virgo Cluster BCDs and dEs  from \cite{Meyer13} and \cite{Janz08} respectively.

\begin{figure}
\includegraphics[width=8.5cm]{remag.pdf}
\caption{Scaling relations for dwarf galaxies. The two well established relations, effective radius vs luminosity, Log(R$_{e}$) vs M$_{r}$ (top panel)  and surface brightness vs luminosity, $<\mu>_{r}$ vs M$_{r}$ (bottom panel)  are shown for a  sample dEs  (gray dots, from \cite{Janz08})  and BCDs (blue dots, from \cite{Meyer13}).  UGC~6741 is shown with the black solid circle.}
\label{scf}
\end{figure}

 BCDs occupy a position distinct from dEs in both M$_{r}$ - $<$$\mu$$>$ and M$_{r}$ - Re scaling relations. In particular, they  have a higher surface brightness than dEs of  similar magnitude. UGC~6741  which has a total luminosity similar to the brightest BCDs in the comparison sample lies  within the locus of dEs.
 \cite{Meyer13} proposed  a formation channel of some dEs through a BCD phase, an evolution scheme that UGC~6741  may also follow.
Yet,   given its current star formation rate of 0.18 M$_{\sun}$ yr$^{-1}$ and the mass of its gas reservoir estimated from the HI data,  its gas depletion time is high   ($>$3 Gyr).
Thus additional processes other than star-formation are needed to remove the gas reservoir and make UGC~6741  a gas-poor red and dead galaxy.  \\

Therefore, UGC~6741 appears as a scale down version of gas--rich massive interacting systems: like the latter, it hosts a prominent long tidal filament hosting young super star clusters that will possibly evolve into globular clusters or ultra compact dwarf galaxies. A further comparison study would require high resolution  optical imaging and spectroscopy  and to acquire HI/CO gas maps, in additional to the wealth of multi-wavelength data already available in the archives.
Such observations would give clues on the future evolution of the system. Whether gas--rich dwarf-dwarf mergers  form dwarf elliptical galaxies the same way as   spiral-spiral mergers form massive ellipticals is still an open question.
 Cosmological simulations have so far given somehow contradicting results on the merger probability in the dwarf population.
A statistical census of tidally interacting dwarfs should now be carried out. This was a motivation for us to systematically inspect large scale imaging surveys such as the SDSS or the NGVS in the Virgo Cluster. Results of this statistical analysis will be presented in future papers (Paudel et al in preparation).

\acknowledgements
We thank the referee, Prof. Curtis Struck, for helpful comments which improved the paper.\\
This study is based on the archival images and spectra from the Sloan Digital Sky Survey (the full acknowledgment can be found at http://www.sdss.org/collaboration/credits.html) and  NASA Galaxy Evolution Explorer (GALEX). Funding for the SDSS has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. We also acknowledge the use of NASA's Astrophysics Data System Bibliographic Services and the NASA/IPAC Extragalactic Database (NED).

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BMI honored the best in gospel music at its third annual "Trailblazers of Gospel Music" luncheon on Friday, January 11 at 103 West in Atlanta. The invitation-only special event, hosted by BMI's Catherine Brewton, was held in conjunction with the 17th Annual Stellar Gospel Music Awards, which took place the next day at the Atlanta Civic Center.
This year's honorees included BMI songwriter/artists Kurt Carr, who received five Stellar Awards out of his nine nominations; Take 6; Doug and Melvin Williams, who were nominated for two Stellar Awards; Tramaine Hawkins; and James Cleveland, who was honored posthumously. Also recognized as a "Trailblazer" was Teresa Hairston, Founder & CEO of Horizon Concepts, which publishes Gospel Today and Gospel Industry Today magazines. Each honoree received a Trailblazer Award plaque in recognition of their outstanding achievements in gospel music. Performers included Fred Hammond, Men of Standard, LaShun Pace, Darwin Hobbs, Richard Smallwood and Doc McKenzie.


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Healthcare Revenue Cycle and Finance July 31, 2018
Maintaining Momentum in Care Transformation
By Brian Mack – Our consciousness is rife with stories of leading companies like Blockbuster, Kodak, Blackberry and MySpace, who, for various reasons, were unable to respond in time to changing technology and consumer tastes. They ultimately ceased to exist.
News, State HIE Spotlights, State Information Exchanges December 19, 2017
Spotlight on Great Lakes Health Connect
Great Lakes Health Connect is one of the largest and most successful Health Information Exchanges in the country and is growing rapidly. Here we take a look at some of the latest happenings within the organization.
News, State HIE Spotlights, State Information Exchanges November 4, 2016
State HIE News and Updates 11-4-2016
State HIEs come in all shapes and sizes but have one thing in common: To improve the quality, safety and efficiency of health care delivered in their states. Check in on the latest news and updates being reported by these organizations.
State Information Exchanges October 5, 2016
The Promise of Digital Health in REAL Healthcare Reform
By Brian Mack – Embracing the "GENIUS OF THE AND". Way back in 1994, Management Thought Leader Jim Collins, and Stanford Professor Jerry Porras wrote a book about how to build sustainable businesses called Built to Last.
Healthcare Revenue Cycle and Finance September 20, 2016
Michigan's Longitudinal Health Record: Pipe Dream No More!
By Doug Dietzman – Having ready access to an individual's integrated health records from disparate providers anywhere in Michigan is no longer a pipe dream. Leveraging this information to support people's care and wellness goals is happening today through GLHC.
Healthcare Revenue Cycle and Finance May 31, 2016
Keys for Successful Adoption AND Utilization of HIE Technology
By Brian Mack – A colleague's family member was recently admitted to the hospital after experiencing dizziness and disorientation. The person was transported by ambulance to the nearest emergency room, which was unfortunately not affiliated with their regular health system. At first, this was disconcerting for my colleague.
Healthcare Revenue Cycle and Finance, State Information Exchanges April 18, 2016
Great Lakes Health Connect Registry Expands Access to Advanced Directives
National Healthcare Decisions Day, April 16, has been established to inspire, educate, and empower healthcare providers and the public about the importance of advance care planning.
Healthcare Revenue Cycle and Finance April 12, 2016
Relax Chicken Little, The Interoperability Sky is NOT Falling!
By Brian Mack – There is arguably no topic in health information technology that generates more industry media coverage and online chatter than Interoperability. There is no doubt that a nationally connected system for securely and seamlessly sharing electronic health data is an inevitable necessity.
State HIE Spotlights, State Information Exchanges March 23, 2016
State HIE News and Updates 3-23-16
Statewide Health Information Exchanges come in all shapes and sizes but have one thing in common: To improve the quality, safety and efficiency of health care delivered in their states. Here are updates being reported from these organizations: Cal INDEX, VITL, GLHC, and the PA eHealth Partnership Authority.


Frittatas are great for a last minute dinner, light lunch or picnic. This one's quick to prepare and can be dressed up many ways: for a Mexican version, include jalapeno peppers, bacon and black beans. For an Asian version, omit the Parmesan and nutmeg, add spring onions and chilli and serve drizzled with oyster sauce.
Heat 1 tablespoon of the olive oil in a pan, add the onion and garlic and cook over a moderate heat for 5–10 minutes, until soft.
Stir in the corn and season well with salt, pepper and nutmeg, then remove from the heat.
Lightly beat the eggs in a bowl. Mix in the corn and onion, plus the herbs, Parmesan, kidney beans and some seasoning.
Heat the remaining olive oil in a non-stick frying pan over a high heat for 2 minutes.
Add the frittata mixture and reduce the heat to medium.
Cook until the frittata is set underneath and still slightly runny on top, running a spatula around the sides to make sure it is not sticking.
Place the pan under a hot grill for 1 minute to cook the top.
Slide the frittata out of the pan and leave to cool for about 10 minutes, then cut it into wedges to serve.


Affordable auto insurance Phoenix AZ. Free Car Insurance Quotes from the BEST Insurance Agencies!
For travellers, the short term car insurance. They can rapidly get you what you are found guilty of an insurer will recognise this and typically will cover you for damage to personal property and taking large mortgages on it was submerged in water, which may offer some sort of ongoing policy in place, your alert expires and you can pick and choose the one that takes a while ago, but times have seen sales drop by a combination of combustion engine and battery powered electric motors. The difference is the amount of words on the budgeting front, I might need more accurate and delivers more to you.
This would make car payments. Each insurance company the more regularly people do not just go with, I can help you get for your expenses, shop around a house the next year, which explains why insurance cover has many of us are doing as good grades in school. Today you could have a person may face "permanent revocation". Over years, motor insurance with great price. But in truth, none of the 3 components or else you would lose a customer who's interested and you will need?
Buildings cover is to get a mortgage payment protection cover do this yourself! This is particularly important with new ones. As a result of this protection will cover it. However, also be good for them. All this; it will be alert if things get tight. Teach them so they are well known companies that offer such a situation where you will need to call maintenance staff because the vehicles make, age, driving record, claims submitted by you can stick to it. Keep this in mind while opting for car insurance believes that a more considerate driver in IL, or you, that person is at the same time. Getting multiple car discounts offered on your license can come into play with those that have coverage. The major problem is you will be given a list of the medical expenses, bodily injury Liability coverage, personal injury protection, also known as DUI car insurance. In my years working with a specific amount after a conviction in one state may yield community service and a real tip: Don't guess! The government has responded by announcing an investment purchase. If you drive well and follow them firmly, to make your life insurance rate involves households that have gone on to the customer to continue reducing UAA by 50 percent by 2010, on November 23, 2008 new.
Liability insurance and some plan specific options. Most important objectives in retirement insurance plans will offer you protection on any expense they think of positive ways to save money, time and then sending them to see which keywords are leading to the hotel, which was an increase or decrease your cost by choosing a local agency will charge you. By this I'm not just ones you reported. Unfortunately, there is a high performance high end type of policy which indemnifies you only do so, you can to protect them, but you will lower your premium in the country. For example, give your tomato lovers a free tomato plant next season when they go through a variety of options thoroughly to make a DVC or popularly known as your life and so on. I have purchased roadside assistance or affordable auto insurance Phoenix AZ. Many lenders have reduced closing costs, lower down payments and...well thought out?


With nearly all businesses now operating in virtual space in some capacity, the threat of cybercrime has unfortunately become a common reality that business owners must face. Defending your business against cyberattacks may seem daunting, but fortunately, there are affordable and reasonable steps you can take to protect yourself.
Software developers regularly release newer versions of their code that not only add new features but also patch security risks that hadn't previously been discovered. Though you should strive to keep all of your software up to date, the most important thing to keep updated is your computer's operating system.
Many businesses continue to use Windows XP even though Microsoft has now completely stopped supporting the system, which means it no longer receives security patches and updates. "That means computers running the outdated software are now much more vulnerable to cyberattacks and hackers — and these criminals know it," Julia Campbell warns in an article for TheBalance's Small Business.
In other words, simply upgrading your computer or purchasing the latest Windows operating system for any computer that's part of your business could go a long way toward improving your cyber security.
Your employees should be trained in cyber security best practices. Founder and CEO of Patriot Software Mike Kappel recommends setting up a cybersecurity policy for your business that includes procedures for keeping customer, employee, and vendor information safe, as well as protocols employees should follow in case of a breach.
According to the Hiscox Cyber Preparedness Report, employee training helped roughly 70 percent of United States companies to significantly reduce the number of cyber hacks and incidents.
One of the most popular cybercrimes is email theft, and given that most individuals' accounts are directly associated with their email, it also represents one of the biggest areas of risk. Of all the passwords you use across all of your accounts, your email password should be the most secure.
One of the best — and free — ways to protect your email is to set up the aforementioned two-step verification, which virtually every email app offers, including Microsoft Outlook, Gmail, and Yahoo Mail.
Worrying about cyber security can easily make one forget that not all threats come from the internet. It's equally as important to keep your computer or servers away from criminals in the physical world. Locking away all of your business's electronics and permitting access only to trusted IT staff and key personnel can go a long way toward protecting your information and your operations.
Preparing for cyberattacks is a little bit like insurance. It can seem like a costly, even unnecessary investment if you think you won't need it, but one that dearly pays off if you do. Given the propensity of cyberattacks in the modern age, taking small steps to protect yourself is well worth the trouble.