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Plaoshnik – St. Clement church
The archaeological complex of "Plaošnik" in Ohrid is the most significant and sacred space for Macedonia and the whole Slavic world in historical, cultural and spiritual sense. It is situated on the higher hill of Ohrid, between Samuil's fortress and the picturesque area of the church St. John the Theologian of Caneo, on the coast of the Ohrid lake.
View other Archaeological sites in the Republic of Macedonia in a larger map
The chronological vertical life line spans from prehistoric times (end of Bronze age), over the antiquity and late antiquity period and Early Christianity, to the High Middle ages. The data indicate that towards the end of Bronze age and in Iron age at the area between Samuil's fortress and Plaošnik, the first settlement on Ohrid hill, existed. This is confirmed with the archaeological investigations (1996, 2007-2009) which unearthed numerous fragments of mat painted ceramics and Iron age tombs with rich offerings of ceramic, bronze and other objects, known in archaeology as "Macedonian Bronzes". Further on, the data also indicate that in antiquity, in the time of the large development of the aristocratic town of Lychnidos, (the old Ohrid) it was the location of the most significant antiquity temples, among which, also the temple of the god Dionysus.
In the late antiquity and Early Christianity (4 – 6 century), lychnidos was the Episcopal center of the Macedonian-Roman province of New Epirus, and Plaošnik was the place where monumental early Christian basilicas with rich architecture and with even richer mosaic floor areas were built on the ruins of the pagan temples. at the end of the 9 century the first Slavic archbishop St. Clement came to these areas, and he reconstructed an old three-foil church (built most probably at the beginning of 7 century) and he dedicated it to the holy doctor St. Panteleimon. Here and in the monastery complex that developed in the next centuries, St. Clement started with a strong educational and literary activity (Ohrid literacy School), the First Slavic University was started, and from there the Old Slavic literacy, art and culture had spread. Even during his lifetime, St. Clement expanded the church towards the west, and he built a modest grave in the pronaos where he was buried after his death in year 916.
The church of St. Clement was later reconstructed and painted with frescoes (13-14/15 century) on the same foundations and it functioned as such until the end of 15 century when it was demolished down to its foundations by the Ottomans, and Sultan Mehmed's Mosque was built on its place. This building functioned for some time and then it was deserted. In 1942/1943 the first archaeological excavations started here, when the remains of the old St. Clement's church dedicated to St. Panteleimon and the grave of the holy one were discovered. These discoveries were made by the head of the antiquity Office of Ohrid, Kiril Prličev, the son of the well known poet and romanticist from Ohrid Grigor Prličev, and the work was continued by his successor in the same office, also a man from Ohrid dimče Koco. In the period of 1964-1967 there were additional archeological excavations made and there was a conservation of the remains of the St. Clement's church made, while the ruined walls of the mosque were fortified in order to "physically protect the church".
On the occasion of the jubilee of "2000 years of Christianity in Ohrid and Macedonia", in the period between 1999 and 2002 at the area of the site i.e. at the area with the remains of St.Clement's church and the mosque, were performed revising and systematic archaeological investigations and onservation/restoration, upon which the Instauration of St. Clement's church "St. Panteleimon" commenced. The direct work on the reconstruction of St. Clement's temple started in March 2001, and in the summer of the same year, further systematic archeological research continued in order to provide appropriate conditions for the access to the St. Clement's church. The remains of the monumental five-nave early Christian basilica around St. Clement's church were discovered, placed in the central part of this big early Christian sacral facility. The work also continued in 2002 and there was a monumental baptistery discovered south from the apse of the basilica, with preserved mosaic floors and beautiful representations of the symbolic early Christian cosmogony (vegetal and zoomorphic representations, swastika crosses, etc), narthex with preserved parts of mosaic floors in many phases in the northern nave of the basilica; spacious atrium in the northern part with marble bases and pillars, auxiliary rooms and spacious yards in the eastern part of the complex etc.
St. Clement's church of St. Panteleimon was completely reconstructed by the end of July 2002, on the same foundations of St. Clement's time (9 century) and the additions (chapels, northern and southern porch and church bell (8-14/15 century) with the same construction materials and the same approach to work, as it was done in the old times of its former reconstructions. It is a three-foil church with a naos (central nave), narthex with a gallery, northern porch, southern open porch, dome above the altar area, dome above the central area and a church bell on the western part. In the interior, there is preserved fresco painting from the time of its reconstruction in 11-12, 13-14 century and the remains of older phases of floors that are today presented with floor glass areas. The old floor in the altar area and in the naos (central part) has been reconstructed in marble, based on the remains of the old original floor. There is a marble altar screen and carved gates, iconostasis and the grave of St. Clement. On the walls of the northern porch the discovered fragments of the frescoes of the old church are presented. St. Clement's temple has received its original shape with its whole historical magnitude and spiritual dimension that reminiscently brings back St. Clement's time to our modern times,to be reconstructed and last in the future with an eternal faith and respect to the immortal spirit of the holy one.
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In 2007-2009 were performed vast systematic archaeological investigations on the entire area of Plaošnik with the goal to discover all relevant data that would enable the implementation of another vast project at this area: the Instauration of the complex "St. Clement's University".
Koco D., Klimentoviot manastir "Sv. Pantelejmon" i raskopkata pri "Imaret" vo Ohrid, Godishen zbornik na Filozofskiot fakultet, 1, Skopje 1948, 129-180.
Grozdanov C, Kuzman P., Buntasheska-Paskali Т., Plaoshnik, Vozobnovenata crkva na Sv. Kliment i Pantelejmon, Ohrid 2003.
Bitrakova Grozdanova V., Linid vo ranohristijanskiot period i negovoto urbano jadro, Jubileen zbornik, 25 godini mitropolit Timotej, Ohrid 2007, 257-268.
Kuzman P., Plaosnik, Ohrid World Heritage Site, Cultural heritage protection office, Skopje 2009, 54-61.
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Ellice River (Inuktitut: Kuunnuaq) ist ein Fluss in der Kitikmeot-Region von Nunavut in Kanada.

Er hat seinen Ursprung etwa 25 km östlich des Beechey Lake. Von dort fließt er nordwärts zum Queen Maud Gulf. Dort mündet er in die Campbell Bay.

Das Gelände zwischen dem Ellice River und dem Sherman Inlet ist hauptsächlich ebenes Sumpfland. Moschusochsen und Barrenground-Karibu frequentieren das Gebiet.

Der Fluss wurde zu Ehren von Edward Ellice, Jr. benannt.

Fauna
Im Ellice River kommt der Seesaibling vor.
Große Ringelgans-Populationen brüten auf den Küsteninseln vor der Mündung des Ellice River.

Einzelnachweise

0Ellice River

redpajama_set_name: RedPajamaWikipedia


text:
Family & Education selected
Education & Family
Fine 'bad parents', says Ofsted boss
By Katherine Sellgren BBC News education reporter
https://www.bbc.co.uk/news/education-27884057
Image copyright PA
Head teachers in England should be given powers to fine parents who fail to support their children's education, the chief inspector of schools says.
Sir Michael Wilshaw told the Times parents who allow homework to be left, miss parents' evenings or fail to read with their children should be fined.
Currently parents receive a £60 penalty notice if their child plays truant.
But Education Secretary Michael Gove wants tougher penalties for those whose children are not "ready to learn".
In a speech earlier this month, Mr Gove pledged "stronger sanctions" - if the Conservatives won next year's general election - for parents who did not "play their full part in guaranteeing good behaviour".
'You're a poor parent'
Now in an interview with the Times newspaper, the Ofsted boss said parents who fail to do a good job in supporting their children's education should be penalised.
Image caption Experts advise reading with children from an early age
Speaking about his own experiences as a head teacher in London's inner-city schools, Sir Michael said: "I was absolutely clear with parents - if they weren't doing a good job I would tell them so.
"It's up to head teachers to say quite clearly, 'You're a poor parent.'
"If parents didn't come into school, didn't come to parents' evening, didn't read with their children, didn't ensure they did their homework, I would tell them they were bad parents.
"I think head teachers should have the power to fine them. It's sending the message that you are responsible for your children no matter how poor you are."
Inner-city schools
Sir Michael praised some schools in inner-city areas as among the best-performing, saying: "London is showing that all children can do well, including poor children, and what we need to do is replicate what's happening here elsewhere.
"There's too much variability and inconsistency across the country."
Sir Michael said it was striking that white British children were now doing worst of all.
He said the gap between white British children from poorer families and those from other ethnic groups needed to be closed for England to catch up with the world's leading nations.
"Immigrant communities are doing very well educationally and it should be recognised that they've added value to this country's performance."
Sir Michael said poverty was all too often used as an excuse for failure by white working-class families.
"It's not about income or poverty. Where families believe in education they do well. If they love their children they should support them in schools."
Head teachers
Image copyright ASCL
Image caption Malcolm Trobe says head teachers should be left to get on with the job
Sir Michael also said he agreed with the government's reforms to GCSE and A-level exams and called for the return of textbooks.
He backed Mr Gove's plans for changes, calling them "absolutely necessary", and urged heads to embrace their increased autonomy and "get on with it".
"Stop moaning, that's my message to head teachers."
Head teachers said they welcomed the autonomy that was being offered, but said all too often this was taken away.
Malcolm Trobe, deputy general secretary of the Association of School and College Leaders, said: "We're told head teachers have autonomy and then we're told what we should be doing.
"We're getting repeated messages from government and Ofsted telling us what we should be doing.
"Perhaps we should say to Sir Michael, if he believes in autonomy, then let us get on with the job."
As for confronting "bad" parents, Mr Trobe said engaging with parents was always the better option.
"It's very important that schools engage with their community and with the parent body and they are very aware of the need to do this.
"It's reasonable to challenge parents, but confrontation rarely leads to a positive outcome."
Michael Gove: Stronger sanctions for truants' parents
'Big rise' in fines for parents over holiday absences
Nurseries not preparing children for school - Ofsted
Class bears may lead to competitive parenting
Family & Education Sections

redpajama_set_name: RedPajamaCommonCrawl


text:
egghead-angular-karma-jasmine-testing
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redpajama_set_name: RedPajamaGithub


The mission of IRPE is to serve as a reliable and valid data resource and as an academic research consultant to the college and community. The primary goal is to provide timely and methodical research services and official data that can be used to prepare organizational reports, monitor programs, evaluate departmental progress, facilitate effective decision making, and assist in measuring overall institutional effectiveness. IRPE will aid faculty, staff, and related entities to meet common objectives in order to advance Northeast Lakeview College in its institutional goals. IRPE will support District IR to coordinate data preparation and submission for state and federal accountability directives.


text:
The Magic Cafe Forum Index » » Right or Wrong? » » Harmful exposure of Mentalists' props (23 Likes)
Go to page 1~2~3 [Next]
Posted: Dec 5, 2017 09:18 am
I am not a full-time professional, just a beginner, but I was dismayed to come across a dealer's website called Propdog Magic. Unlike most dealers' sites, which show the effect of the tricks on offer but not the secret, this site has videos for every prop it sells which explicitly show the workings of the prop, and even discuss patters and handling. It goes through a whole range of gaffed wallets, imp pads and other mentalists notepads showing the inner workings and secret moves. None of this is passworded - it's all open to anyone who stumbles across it. It's actually more damaging than an exposure show like the Masked Magician, because you are hearing the exposure from the seller of the effect himself, so there can be no doubt that it's genuine.
It is one thing for conjuring effects to be exposed like this - undesirable but ultimately maybe not the end of the world for a skilled magician. But for the basic tools of a mentalist act to be exposed like this risks sinking the whole art for good. Once a significant proportion of specs are alerted to the existence of p**k wallets, imp pads etc., the underpinning of a lot of professional mentalists' acts is undermined. All the effort we put into building up atmosphere and suggesting a supernatural or psychic element is rendered faintly ludicrous if the spec knows we already know what was written on the billet. It doesn't matter whether he knows precisely how we did it - the fact he knows it is possible at all, and knows to be suspicious of ordinary-looking items, undermines our whole performance. If he also knows to pull the string or look under the cover, that of course is the ultimate credibility-damaging outcome.
Anyone else share this sense of unease?
thomasP
A lot of gimmicks are exposed on youtube as soon as they are used for a TV show anyway.
If someone want to know it will.
We have to work more on the presentation, less on the effect.
How many laymen do you think are actively looking for this kind of stuff?
The truth is, if the audience is thinking about your pad or wallet, you're already sunk. It means they are not engaged in the performance, and you are not eliciting the belief required for good mentalism.
Mr. Woolery
I actually share the OP's sense of unease at this. I hate to tell others how to do business, but I'd be happier with the demos and secrets behind a password on dealer sites.
What about it is making you uneasy?
the Sponge
Here ya go, a two year old thread discussing the same thing:
https://www.themagiccafe.com/forums/view......&start=0
David Thiel
Western Canada...where all that oil is
Exposure of any stripe to ANYONE is the lowest form of bottom feeder betrayal of the art AND disrespect for secrets that are a huge part of what makes what we do a mystery. Period.
It is certainly true that if people go online to try to learn the nature of an effect that they already suspect they have been tricked. In a magic show that's perfectly reasonable. Magic is all about presenting 'tricks.' In a mentalism performance? Absolutely not. Part of mentalism's appeal is the tantalizing notion that what the audience is seeing just might be for real.
What we do is -- to one degree or another -- is based on keeping secrets...well...secret...of respecting the methods, concepts and ideas that allow us to present what we do to audiences.
And please...don't trot out that tiresome "you shouldn't be presenting mentalism as real" chestnut. Please...just don't.
As far as I am concerned -- if YOU have designed an effect that is unique and not based on anyone else's work -- and YOU decide to expose YOUR effect to the public? Go for it. But the fact is that those classically-pathetic-dried-up-bits-of-snot-dweebs who lack any sense of value within themselves have the mistaken notion that they can stop being CPDUBOSDs by exposing secrets designed by other people -- and performed by other people -- to the world.
That's theft.
That's betrayal.
Those who do it -- or companies that do -- are beneath contempt. Literally.
It is true that we live in a different age and that the vast majority of secrets can be purchased by anyone with the cash to do so. It's also true that many of the people doing the purchasing have the mistaken idea that, once they buy a prop/method/book, it's theirs to expose -- like they own it. Finally -- and depressingly -- it's also true that the secret can be bleated and blasted all over the world instantly by putting it on the internet.
Yup. It's all true -- but that doesn't make it right.
Whatever doesn't kill you makes you stronger. Except bears. Bears will kill you.
www.MindGemsBrainTrust.com
www.magicpendulums.com
www.MidnightMagicAndMentalism.com
Eternal Order
All shops expose, SW**is, everything...it's a massive shame..
Wouldn't take much that when you create an account you answer two questions, if you answer them right, can access the video or product, if you can't then you just get the text equivalent...
BRUTISHLY STARLIT
https://www.lybrary.com/brutishly-starlit-p-923169.html
http://www.lulu.com/spotlight/uncle90
Martin Pulman
Posted: Dec 5, 2017 03:26 pm
On Dec 5, 2017, WitchDocChris wrote:
Yes. How foolish of mentalists to spend all those decades trying to protect their secrets from open exposure.
On Dec 5, 2017, David Thiel wrote:
Thank goodness their are still some voices of reason around here.
Two Minnie's in The Hell's Half Acre, The Republic of Texas
On Dec 5, 2017, Martin Pulman wrote:
Mental-ist having nothing to fear but the mental magicians are doomed, doomed I say
GERMANY/ Hannover
It´s all about making money!
On Dec 5, 2017, KiKi wrote:
That's what the real mental-ist said (did) a 150 years ago
George Hunter
The "exposure" issue can be viewed in more than one way.
While I affirm the view that access to explanations should be password protected, I would like to affirm, and thank, the occasional magic shop that is willing to step out from behind the hype and tell us enough that we can judge whether the effect or prop fits our approach, competence, need and interest.
It is called "truth in advertising." It is not a new idea. Many demonstrators in the old brick and mortar shops showed or explained enough that a kid of any age could make an informed purchase decision.
The shift to internet shops has largely abandoned that kind of seller-buyer integrity. I have bought too many effects that, in the ads and endorsements, were simply misrepresented. You have too. Too often, the blatant misdirection begins in the selling phase.
If enough of us prioritized our shopping with vendors that told us enough, I'll bet we see change that would be good for the art, and its practitioners, and the shops.
Yepski
Still trying to figure out "CPDUBOSDs"
On Dec 5, 2017, RCP wrote:
Show business is about money forever.
Hang on a second.......so mentalism isn't real? :O
On Dec 5, 2017, Yepski wrote:
It means: "classically-pathetic-dried-up-bits-of-snot-dweebs."
Catchy, huh?
Ok, so if the store shows what they are selling, they're exposing and that's bad.
But if a store doesn't show everything about what they are selling, they're hiding things and false advertising, and that's bad.
So what do you people actually want? No stores?
The point is in the nuance. No one in this thread has called for the seller to show 'everything."
I simply reported my appreciation for sellers who explain enough for me to make an informed purchase decision.
If no one else appreciates that, and prefers to navigate purchase decisions informed only by the hype, some of the magic shops are glad to see you coming.


text:
Emancipation Day and Juneteenth celebrations aren't new to Georgia
By Ronda Racha Penrice
Atlanta — and Georgia — has a long, storied history with 'Freedom Day'
Until recently, Juneteenth was not a celebration or historic event familiar to most Americans. Widely celebrated as "Freedom Day" in black communities throughout Texas for decades, Juneteenth commemorates the June 19, 1865 date enslaved African Americans in Galveston learned that President Lincoln had freed them through the Emancipation Proclamation — more than two and a half years after it was first announced January 1, 1863. Over time, the celebration, also known as Jubilee Day, gained momentum, especially as black Texans spread out to other parts of the country.
That momentum is one of the main reasons President Trump's initial decision to resume his re-election campaign rallies in Tulsa, Oklahoma — the site of one of the worst massacres of African Americans in US history — on Juneteenth angered so many. As highlighted by the HBO series, "Watchmen," filmed in the Atlanta metro area and starring Oscar-winner Regina King, white mobs attacked black Tulsans May 31 and June 1, 1921 in the Greenwood District, known as "Black Wall Street" for its distinction as the nation's then wealthiest black community. The attack devastated the area, resulting in the deaths of around 30 black people, with more than 800 gaining hospital admission.
ExploreJuneteenth events and observances in metro Atlanta
After a series of high-profile critics, who questioned the location in light of the massive protests taking place throughout the nation in the wake of George Floyd's death after being knee-ed in the neck by then-Minneapolis police officer Derek Chauvin, Trump moved the rally to the next day, June 20.
Since that development, Juneteenth news has been nonstop. Locally, the Atlanta Hawks made Juneteenth a paid holiday for its employees. Virginia, with help from music producer/artist Pharrell Williams, and New York state both announced that Juneteenth would become a state holiday. In the late 1800s and early 1900s, however, Juneteenth was one of many Emancipation Day celebrations in various parts of the Midwest and, of course, the South, including Atlanta and Georgia overall.
"African Americans held Emancipation Day celebrations really on January 1, because that was the day in which the Emancipation Proclamation went into effect," shares Savannah native Dr. Karen Cook-Bell, who serves as associate professor of history at Bowie State University, a public HBCU in Maryland. This was true of Savannah and surrounding areas, notes Cook-Bell, who authored the 2018 book, "Claiming Freedom: Race, Kinship, and Land in Nineteenth-Century Georgia" and has done extensive slavery and Civil War-era research in the area.
ExploreUS Senate approves bill to make Juneteenth a federal holiday
Georgia State University professor Wendy Venet, who specializes in 19th century U.S. history, teaching courses about the Civil War and Reconstruction, chimes in via email that "annual occasions often took place in local churches or sometimes on one of the black college campuses. Ceremonies included reading of the Proclamation by a prominent member of the community, speeches and music."
"Sometimes these occasions began with a parade," she continues. "Often the festivities focused on a message of racial advancement, especially when the celebrations took place at black colleges and universities. Sometimes they were occasions for getting a message out, such as news about the lynching of three black men in south Georgia during the last week of December 1889, [which was a focal point for the Emancipation Day Celebration held January 1, 1890]."
ExploreWhy Juneteenth has taken on greater meaning
In other communities like Galveston, Emancipation Day celebrations took place annually on or around the day African Americans in those areas learned of the Emancipation Proclamation. For Thomaston, a predominantly white town still over an hour's drive south of Atlanta in Upson County, May 29, 1865 is that day. And, until this year, Thomaston, according to multigenerational native Rev. James McGill, who wrote "The First One Hundred Years of Upson County Negro History," published in 2017, that milestone had been celebrated each year around Memorial Day since 1866. It's widely considered the longest-running consecutive celebration of its kind.
William A. Guilford, a businessman and early black state legislator born in 1844, says Rev. McGill was key in organizing that very first 1866 Emancipation Celebration. "William Guilford," says Rev. McGill, "wrote there were five speakers," including James Milton Smith, who later served as Georgia's 48th governor from 1872-1877. The next day, May 30, white Thomaston resident, James W. Greene, wrote "The freed people had a brilliant celebration on yesterday" in a letter.
Explore5 things to know about Juneteenth
Over time, the Emancipation Celebration grew. In 1921, according to Rev. McGill's book, "It was estimated that from 3,000 to 5,000 Negroes were present." Early 20th century photographs of Emancipation Celebration confirm a sizable crowd. "The Central of Georgia Railway," Rev. McGill claims at one point in the book, "ran four special coaches for colored people for this occasion, three from Macon and one from Atlanta."
Civil rights icons Ralph Abernathy and Hosea Williams are just two of the many historic speakers who have participated in the celebration since its inception, says Lankston Johnson, who led the effort for eight years from the late 2000s into the mid-2010s. Floats, marching bands, vendors and more dot the parade route extending from the predominantly black downtown area, where the parade historically started, to Lincoln Park, another predominantly black area.
At 67, Rev. McGill can't recall missing one Emancipation Celebration. Neither can 38-year-old Markeevius Smith, who attended both Morris Brown and Georgia State University. At 41 years of age, Johnson only recalls missing one when he was a student at Georgia Southern. It's a tradition they pass down to their children just as their parents, grandparents, great-grandparents and beyond passed it down.
Today, Thomaston is extremely rare. "Nationally, Juneteenth celebrations have replaced Emancipation Day celebrations as popular events," notes Venet. "The Atlanta History Center holds annual celebrations over two days that include storytelling, crafts, and costumed interpreters acting as Civil War soldiers in the U.S. Colored Troops."
Some historians credit the 1968 Poor People's Campaign for giving Juneteenth a boost through its Solidarity Day event held on Wednesday, June 19, which attracted over 50,000 people in Washington, D.C. Both Ralph Abernathy and Coretta Scott King spoke that day.
ExploreNew book explores origins of Juneteenth
"Juneteenth has really had a revival of sorts really since the 1980s to '90s," observes Cook-Bell. That revival, she says, can be attributed to "the momentum of the post-Civil Rights period when African Americans were claiming the gains they had made since the Civil Rights Movement, politically, economically and even socially."
"Texas became the first state to recognize Juneteenth as an official state holiday in 1980, and other states followed suit in terms of recognizing it either as a state holiday or as a special ceremonial holiday… Today 47 out of 50 states recognize Juneteenth as a state holiday or either as a ceremonial holiday."
And Georgia is one of them. According to JuneteenthAtl.com, website to Atlanta's own Juneteenth celebration, "In 2011, Georgia became the thirty-seventh state to recognize Juneteenth at its state capitol with the passage of S.R. 164." State senator Lester Jackson from Savannah, along with Atlanta-area state senators Donzella James and Valencia Seay co-sponsored the legislation.
The following year, Bob Johnson, who came to Atlanta back in 1988, created Juneteenth Atlanta which today, he boasts, is "one of the largest Juneteenth events in the country."
"Last year, we actually held the event at The Home Depot Backyard at Mercedes-Benz Stadium," he explains. "We also did a three-mile black history parade as part of our events that span over three days instead of one."
Ronda Racha Penrice
Credit: Uncredited
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text:
\section{INTRODUCTION}

Images of SAO 206462 \citep{stolker16} and HD 142527 \citep{marino15} have revealed azimuthally-localized dark features in their outer disks. Both studies interpret the features as shadows cast by an optically thick, non-coplanar inner disk. Such an inner disk may be indicative of the existence of planets or large dynamical changes in the disk's history. Modeling of the disk structures can provide a predictive tool for where low mass companions may be hiding. Sequential follow-up observations can then detect these worlds, as was the case with the young gas giant $\beta$ Pic b, which due to its inclined orbit is driving a similar gravitational warp in the inner disk that was seen before the planet \citep{apai15}.

Another disk that exhibits azimuthally-localized dark features is associated with HD 100453A (A9V, luminosity L $\sim$ 9 L$_{\astrosun}$, mass M $\sim$ 1.7 M$_{\astrosun}$ \citep{dominik03}, d = $103 \pm 3$ pc \citep{gaia16}) which has an M4 companion at a separation of $1\farcs06 \pm 0\farcs02$ \citep{chen06}.  Total intensity (TI) imaging at Y-K2 bands, obtained by \citet{wagner15} with the extreme AO imager Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE), revealed two spiral arms, dark features, and the outer extent of the large radial gap inferred from the IR spectral energy distribution (SED) \citep{khalafinejad16,maaskant13}.

We present Gemini Planet Imager (GPI) polarized intensity (PI) imagery \citep{macintosh14} of HD 100453. This dataset, the SPHERE data, and the infrared SED are modeled using the 3D Monte Carlo radiative transfer code HOCHUNK3D \citep{whitney13}. This code allows for two, independent and radially separated two-layer disks which need not be coplanar, and the use of multiple grain opacity models. Model images are compared to image data, while simultaneously fitting the SED, to find the cause of the dark features and investigate how structural changes within the disk affect their shape and locations.

\section{OBSERVATIONS AND DATA REDUCTION}

\subsection{GPI Observations and Data Reduction}

HD 100453 was observed with GPI on 2015 April 10-11th UT using polarimetric differential imaging mode in J-, Y-, and K1-bands. GPI's "direct" mode utilizes polarization to suppress stellar light, but not a coronagraphic mask, thereby sacrificing contrast in favor of a tighter inner working angle. We used the shortest exposure time (1.49 seconds) to minimize saturation and co-added 10 frames to increase the signal-to-noise ratio. The half-wave plate angle was rotated from 0 to 67.5$\degr$ with 22.5$\degr$ steps to obtain linear polarization. This sequence was repeated 41, 35, and 36 times, resulting in total exposure time of 41, 35, and 36 minutes for Y-, J-, and K1-bands, respectively. The averaged airmass values were 1.21 and 1.19 in the $J$- and $K1$-bands, respectively.

The data were reduced using the standard polarized data reduction recipe available in GPI pipeline \citep{maire10, perrin14} v. 1.3, with notable customizations. First, microphonics noise was minimized by eye through tuning parameters in the ``destripe science image" primitive. Second, the ``subtract mean stellar polarization" primitive was added to the standard polarization recipe to remove instrumental polarization (estimated in the region $1<$ r $< 10$ pixels, which shows no significant disk emission). Finally, a custom pipeline fix was implemented to allow image alignment in unblocked mode. GPI image alignment typically relies on well-calibrated satellite spots injected by the GPI apodizers which are not present in unblocked mode, so a Gaussian stellar centroid was used instead. Though this alignment method is imperfect due to stellar saturation, it worked well in this case. The resulting images were transformed to ``radial" Stokes parameters (Schmid et al. 2006). Images used here represent the Q$_R$ component, which holds all linear polarized flux oriented either parallel (negative) or perpendicular (positive) to the line connecting that pixel to the central star. Positive flux in these images therefore represents singly-scattered photons from the circumstellar disk.

HIP~56071 was observed as a flux standard, with the same procedures, except without closing the AO loop, thereby avoiding saturation. This allowed us to derive conversion factors between ADU sec$^{-1}$ pixel$^{-1}$ and mJy asec$^{-2}$. Since the K1-band magnitude in HIP~56071 was unavailable, we translated the 2MASS K$_{\rm s}$-band magnitude into this band by relating the stellar flux to the Vega flux assuming box passbands in two bands (the GPI K1-band with 1.9-2.19 $\mu$m and the 2MASS K$_{\rm s}$-band with 1.989-2.316~$\mu$m) and blackbody radiation with a T$_{\rm eff}$ of 9200~K for HIP~56071 (A1V) and 9700~K for Vega (A0V). The color correction of K$_{\rm s \ 2MASS} - $K1$_{\rm GPI}$ was $-$0.002; thus, we derived HIP~56071's K1$_{\rm GPI}$ magnitude is 7.860. We derived conversion factors of 1~ADU sec$^{-1}$ pixel$^{-1}$ are 0.846 and 0.853 mJy asec$^{-2}$ in the J and K1-bands, respectively. Note that Y-band flux was not converted to mJy asec$^{-2}$ due to no literature value for the Y-band.

We find the projected separation between the image center and the companion to be $1\farcs05$, in agreement with \citet{chen06}. The region within $\sim$4 pixels (corresponding to $\sim$0$\farcs$06) from the central star is saturated.  We conservatively estimate the features outside 6-7 pixels from the center to be real while the area interior to this radius is washed out by speckle residuals. We detect the outer disk and spirals, as in \citet{wagner15}. The total PI within $0 \farcs 1 < r < 1 \farcs 0$ (the inner radius corresponds to 7 pixels) is 13~mJy and 22~mJy for J- and K1-bands, respectively.

\subsection{Archival Total Intensity Imagery and Assembly of the IR SED}
\citet{wagner15} also observed HD 100453 with VLT/SPHERE on 2015 April 10. The observations were carried out in IRDIFS extended mode\footnote{Very Large Telescope SPHERE User Manual} \citep{gpimanual} using IRDIS to take dual-band TI images in K1- and K2-bands and simultaneously using the IFS to obtain low-resolution spectra from Y- to H-bands. Data reduction is described in \citet{wagner15}. Photometry used in constructing HD 100453's SED includes all sources mentioned in \citet{khalafinejad16} as well as \textit{Herschel} PACS data at 70, 100, and 160 $\mu$m \citep{pascual16}, and 2MASS at J-, H-, and Ks-bands \citep{cutrie03}.

\section{RESULTS}

\subsection{SPHERE and GPI Imagery}
A radial gap can clearly be seen from $9 \pm 2$ au, to $18 \pm 2$ au in the GPI imagery (Figure~\ref{fig:r^2 SPHERE and GPI}). Inside 9 au the GPI image is saturated, making the inner edge of the gap inaccessible in the image. The outer radius agrees with the \citet{wagner15} estimate of $\sim$19 au using $d = 103 \pm 3$ pc \citep{gaia16}, and the \citet{khalafinejad16} estimate of $20 \pm 2$ au from SED modeling. We measure a pericenter offset upper limit of $1 \pm 1$ pixels (0$\farcs014 \pm 0\farcs014$) (Figure~\ref{fig:r^2 SPHERE and GPI}).

The outer disk is brightest on the southern side in both PI and TI imagery implying this is the near side of the disk. However, the northern spiral arm is brighter in PI images while the southern arm is brighter in TI images, indicating possible differences in grain properties. Additionally there is a dropoff in the spiral arm intensity at longer wavelengths in SPHERE TI images which suggests they made of smaller grains than the outer disk. After absolute flux calibration of the TI images using archival 2MASS photometry \citep{cutrie03} we measure the total TI flux between $0 \farcs 1 < r < 1 \farcs 0$ is 49 mJy and 70 mJy in J- and H-bands respectively. Using this and the 2MASS flux we calculate a fractional luminosity for the outer disk \(\frac{fdisk}{ftotal}\) of $0.018 \pm 0.001$ for J-band and $0.025 \pm 0.002$ for H-band which may suggest that the outer disk is reddish and therefore comprised of large, compact grains \citep{mulders13}.  By contrast we calculate a fractional luminosity for the spiral arms of $0.0040 \pm 0.001$ for J-band and $0.0045 \pm 0.001$ for H-band which, though slightly red, is more blue than the rest of the outer disk indicating they may be comprised of smaller grains \citep{mulders13}.

Two distinct azimuthally-localized dark features are seen at the same position angle (PA) in both TI and PI images, and are therefore not artifacts of PI imagery. They also have a similar outer disk to feature contrast in all available bands (Figure~\ref{fig:r^2 SPHERE and GPI}).

\subsection{Determining the Likely Cause of the Dark Features}

We discuss three possible physical scenarios for the origin of the dark features: a physical gap due the dynamical clearing of a large body, grain growth and settling, or shadows cast from an inner disk component.

The SPHERE Y-band PSF for HD 100453A has a FWHM of ~5 pixels (~3.8 au). This suggests the dark features are resolved and have an azimuthal extent of $14 \pm 2$ pixels ($10 \pm 1.5$ au) based on the FWHM of the eastern feature in this image. If the dark feature is due to the clearing of a single body's Hill sphere \citep{hamiltonandburns92}, it would correspond to an M-type star with a mass of at least 0.4 M$_{\astrosun}$. The M-type companion, HD 100453B, is visible in SPHERE, GPI, and Chandra \citep{collins09} imagery. An M-type star with a mass of 0.4 M$_{\astrosun}$ therefore would certainly be visible in the location of the dark features if it existed. Thus, we reject the hypothesis of local clearing to explain the dark features.

Grain growth and settling has been suggested as a source of dark regions at NIR wavelengths \citep{dullemondanddominik04a, dullemondanddominik04b, birnstiel12}, and should also produce bright rings in the sub-mm. This would require resolution of at least $0\farcs03$, which is reachable by interferometric telescopes such as ALMA. The differential rotation of the disk would cause the dark features to deform over time however, which suggests that grain growth and settling is not the cause of the features.

An inner disk would cast two shadows which have a large radial extent and have similar outer disk to shadow contrast over the wavelength range in which it is optically thick \citep{stolker16}, similar to what is seen in the GPI and SPHERE images. We will show that shadows cast by an inner disk with a suitable inclination is fully capable of producing such dark features. In the following sections we present a model that is capable of generating the dark features as well as reproducing the observed SED.

\subsection{Development of Preliminary Model}

\subsubsection{Literature Values for Outer Disk Inclination}

\citet{dong16} adopted $i\sim$ 5$\degr$, where $i$ is the outer disk inclination from face on with respect to the observer, to reproduce the spiral arm morphology in hydrostatic modeling of the HD 100453 system. If we accept the \citet{dong16} assumption of a completely coplanar disk, we can also assume the equatorial plane of the star is coplanar because, according to \citet{greaves14}, most stars rotate in the same plane as their disks. Using the 5$\degr$ inclination for the outer disk and a $v \, sin \, i$ of $48 \pm 2$ km s\textsuperscript{-1} for HD 100453A \citep{guimaraes06} we find the equatorial velocity of HD 100453A would be $\sim$550 km s\textsuperscript{-1}, which is $150$ km s\textsuperscript{-1} above the break-up velocity of the star \citep{slettebak66}. Because HD 100453A is still intact, a 5$\degr$ inclination for the star is non-physical which implies, by extension, that the inclination of the outer disk also cannot be $5\degr$. Moreover in GPI images we can clearly see the major and minor axes of the disk which would not be possible given a nearly face on disk as in TW Hydrae \citep{andrews16}. If the spiral arms are close to face on as \citet{dong16} suggest, they are not coplanar with the outer disk.

\citet{wagner15} measured an outer disk inclination of $i\sim$ 34$\degr$ from face on through fitting an ellipse to the peak intensity along the center of outer disk and assuming circular geometry. However, because the outer disk has finite thickness, this method will overestimate the outer disk's inclination. We will review this inclination in Section 3.3.3.

\subsubsection{Initial Modeling Parameters}

In order to reduce the degeneracies in our model, literature values, SPHERE and GPI imagery, and the SED (Figure~\ref{fig:SED}) are used in combination to determine initial modeling parameters. For the star we used a PHOENIX stellar atmosphere model \citep{brott05} with T = 7400 K (appropriate for an A9 star) and a distance of 103 pc \citep{gaia16}. HOCHUNK3D uses the \citet{lucy99} method for calculating temperature in our model. Box filters were created in Y-K2 to allow for direct comparison of the model to data.

Through SED fitting \citet{khalafinejad16} suggested that the the inner disk extends from 0.25 to 1.7 au. Confirmation of the inner edge radius is provided by H-band interferometry with VLTI/PIONIER \citep{lazareff16} who find an upper limit of 0.27 au. The inner disk extends to at least $0.9 \pm 0.1$ au from the N-band half light radius of VLTI/MIDI \citep{menu15}, updated using $d = 103 \pm 3$ pc \citep{gaia16}. The long wavelength slope obtained from the 1.2 mm SIMBA point\citep{meeus02b}, the reddish color of the outer disk (Section 3.1), and the lack of a strong silicate peak in the SED \citep{meeus02a}, imply that the inner and outer disks are comprised of large, compact dust grains \citep{mulders13}.

To match these dust properties we used Model 2 from \citet{wood02} for the settled disk grain opacities. This contains a mixture of amorphous carbon and astronomical silicates, a radial power-law exponent (a) of 3.5 for both grain compositions, no exponential cutoff to the grain size distribution, a a maximum particle size $\leq$ 1 mm, and a minimum particle size of 0.01 $\mu m$. For the less-settled grain opacities we used Model 1 from \citet{wood02}.  Similarly this contains a mixture of amorphous carbon and astronomical silicates, a power law size distribution with a = 3.5 and 3.0, respectively, plus an exponential cutoff with a turnover at 50 $\mu$m, a maximum particle size $\leq$ 1 mm, and a minimum particle size of 0.01 $\mu m$.

\subsubsection{Inclination of the Outer Disk}

Because reproducing the spiral arms is not necessary for studying the cause of the dark features, they are not included in our models. We calculated models with $5\degr \leq i \leq 45\degr$ in 5$\degr$ increments and compared the resulting model images to observed images and find a best fit of $25 \pm 10\degr$. From this model we also find a PA for the outer disk's major axis of $140 \pm 10\degr$ east of north.

\subsection{Adopted Model Parameters}

After initial modeling of the outer disk, we constructed a more complete disk model to fit the SED (Figure~\ref{fig:SED}). We find that our model closely matches the observed SED including the NIR region, which was ignored by \citet{benisty17}, to be discussed later. It consists of an inner disk ($\sim0.13 - 1 \pm 0.5$ au) which reproduces the IR excess of the SED and is in agreement with VLTI/MIDI measurements of $0.9 \pm 0.1$ au. This is followed by a depleted region to 18 au, and finally an outer disk ($18-39$ au). The inner disk has a vertical inner-edge thickness of 0.11 $\pm$ 0.05 au as defined by $z = Cr^b$ where z is the density scale height (thickness) of the disk, C is a constant, r is the radial distance from the star, and b is the flaring exponent \citep{whitney03a}. To match mid-far IR emission we find b = 1.28 $\pm$ 0.02 which falls within the canonical values of 1.25 - 1.3 for irradiated disks \citep{chiang97, hartmann98}. Changes in the settled disk have little effect on the SED and were not changed appreciably in our modeling. Our final parameters for the settled disk were z = 0.0004 au and b = 1.25. Both the vertical density and the surface density profile are as described in \citep{whitney13} for a disk in hydrostatic equilibrium. In particular for the less settled disk and settled disks we chose density exponents $\alpha = 2.30$ and $\alpha = 2.25$ respectively.

\subsection{Difference in Inclination for Inner Disk}

\subsubsection{Definition of $\Delta i$}
In this section we test the validity of a difference in inclination between the inner and outer disk as the cause of the dark features. We define this difference in inclination as $\Delta i = i - \beta$ where $i$ is the inclination of the outer disk from face on and $\beta$ is the inclination of the inner disk from face on. While we define $i$ as positive, $\beta$ can be positive or negative depending on the inner disk's direction of tilt (Figure~\ref{fig:Schematic of Disks}).

\subsubsection{Azimuthal Separation of Dark Features and Comparison to Model}
Model images were produced with the adopted $i = 25\degr$ while $\Delta i$ is varied in 10$\degr$ increments from 0$\degr$ to 70$\degr$ (Figure~\ref{fig:Delta i model and sed}). These are convolved with the PSF of SPHERE J-band images and therefore produce clearer shadows than longer wavelength bands. No azimuthally-localized dark features were observed in model images with $\Delta i = 0\degr$ despite a good fit to the SED, excluding a coplanar disk system. At $\Delta i = 20\degr$ the inner disk shadows the northern section of the image and predicts too much flux between 1-10$\mu$m because of its nearly face-on orientation with respect to the observer (Figure~\ref{fig:Delta i model and sed}). Moving to $\Delta  i =  70\degr$ the shadows narrow and predicts too little flux between 1-10$\mu$m because the inner disk is nearly edge-on to the observer. We find $\Delta i = 45 \pm 10\degr$ matches the general appearance of the imagery, to be quantified below.

Azimuthal intensity profiles of the GPI images and model imagery were generated for the outer disk (Figure~\ref{fig:Separation of Dark Features}) and measure an azimuthal separation of $140 \pm 10\degr$ for the dark features which are in the same locations in each band. The additional local minimum in intensity profile plots is due to polarization effects along the minor axis of the outer disk. We find that as $\Delta  i$ is increased, the shadow separation also increases and produces a best fit to the dark features at $\Delta  i = 45 \pm 10\degr$ which corresponds to $\beta = -20 \pm 10\degr$. This deduced inner disk inclination angle is significantly different from the one found in \citet{lazareff16}, $\beta = -48\degr$, using H-band interferometry with VLTI/PIONIER. The main source of uncertainty in our measurement comes from azimuthal extent of the shadowed region. To match the dark features' azimuthal location we rotate the inner disk by -40$\degr$ with respect to the outer disk which places the major axis of the inner disk at $100 \pm 10\degr$ east of north. This differs from the PA for the major axis found in \citet{lazareff16}, 81$\degr$, and will be discussed later.

A recent study by \citet{benisty17} also proposed a misaligned inner disk as the cause of the outer disk shadowing in HD 100453. In their paper they generate a model to test this hypothesis using measurements from \citet{lazareff16}. In order to test the validity of their model we generated our own using their value for the outer disk inclination, $i = 38\degr$, and their quoted $\Delta i$ of  $72\degr$. This model however does not produce shadows in the same locations as in the data (Figure~\ref{fig:Benisty}), similar to what was found earlier in this section.

In our modeling we find that the inclination of the outer disk had little effect on the separation of the shadows on it's own unless the near side of the outer disk is reversed. We also find that the separation of the shadows is less than $180\degr$ on the side of the outer disk which corresponds to the near side of the inner disk. Essentially the inner disk major axis divides the outer disk into two semicircles. The $180\degr$ constraint implies that the centers of the shadows cannot exist in separate semicircles and this strongly constrains the orientation of the inner disk. In Figure~\ref{fig:Benisty} we see that the quoted orientation of the inner disk major axis places the shadows in separate semicircles in the GPI image which cannot occur if the inner disk is the source of the shadows. In addition the gap has a visibly more elliptical structure in the \citet{benisty17} model than in the data which is likely due to the thickness of the outer disk as discussed in Section 3.4 as well as the larger inclination of the outer disk. It is important to note that this $\Delta i$ corresponds to $\beta = -34\degr$ instead of the inner disk inclination proposed separately in \citet{benisty17} of $\beta = -48\degr$. Additionally in our modeling we find that the NIR region of the SED is fairly sensitive to the inclination of the inner disk (Figure~\ref{fig:Delta i model and sed}). Because \citet{benisty17} did not fit the NIR excess of the SED, the \citet{benisty17} model is not as tightly constrained as our simultaneous image and SED fitting. We found the inclination of the inner disk proposed \citet{benisty17} did not produce a good match to the 1-10 micron SED nor the constraints on the shadows that that we found (Figure~\ref{fig:bensitytrace}). Differences in the inner disk orientation which produce shadows along an axis other than the major axis may be possible, though we did not observe this in our modeling.

\subsection{Effects of Inner Disk Thickness and Outer Disk Flaring on Shadows}

To examine how inner disk thickness affects the morphology of the shadows, we generated model images at inner-edge inner disk thicknesses from 0.07 - 0.14 au in increments of 0.014 au without fitting the SED. We find that as the thickness increases, the width of the shadows increases with no change in the location of the shadows. (Figure~\ref{fig:Thickness vs Width}). The differences in width become small at smaller thicknesses however, suggesting that shadows can act as an upper constraint of inner disk thickness.

Model images were also generated at flaring exponents (Section 3.4) of 1.00, 1.20, and 1.40 (Figure~\ref{fig:Flaring}) in order to examine the effect of outer disk structure on shadow morphology, also without fitting the SED. We find that the width of the shadows' inner edge decreases with increasing b, while the outer edge remains largely unaffected. In addition we observe that the flaring of the disk causes the outer disk to appear thicker on the far side as seen in Figure~\ref{fig:Flaring} where the SW side is the near side of the outer disk. This effect is most prevalent in the rightmost panel where the SW side of the disk is approximately half the thickness of the NE side. In the case of HD 100453, the SW side of the outer disk is narrower in GPI images (Figure~\ref{fig:r^2 SPHERE and GPI}) indicating that this is the near side. The ratio of thicknesses between the near and far side of the disk, coupled with the inclination of the outer disk, could allow us to quantitatively describe the degree of flaring of the outer disk. When taken in conjunction with the inner disk thickness, this should allow us to strongly constrain the disk's physical structure.

\subsection{Using Shadows to Determine Near Side of Inner and Outer Disk}

Due to thickness of the outer disk, we find that any $\Delta i \neq \vert90\degr\vert$ will offset the apparent location of the shadows on the outer disk in the direction of the tilt of the inner disk (Figure ~\ref{fig:Disk Cross-section}). The shadows are cast along the major axis of the inner disk and create a shadow, which is not coplanar with the outer disk, on the inner edge of the outer disk. The shadow will therefore be shifted by an amount which depends both on the thickness of the outer disk and the value of $\Delta i$. This suggests the separation of shadows must be less than 180$\degr$ on the side of the outer disk which corresponds to the near side of the inner disk as seen in Figure~\ref{fig:Disk Cross-section}. Examination of the shadow location therefore allows for a simple, effective method of determining the near side of the inner disk. In the case of HD 100453 it is clear that the northern side of the inner disk is the near side because the shadow separation is less than $180\degr$ on that side. In contrast, it is much more difficult to discern the near side of the outer disk via examination of the shadows as this depends on both the tilt of the outer disk and $\Delta i$. In this case, because we know $\Delta i = 45\degr$, the inclination of the outer disk is $\vert25\degr\vert$ from Section 3.3.3, and from the NIR portion of the SED we are not looking along the edge of the inner disk, the SW side of the disk must be the near side.

\section{DISCUSSION}

\subsection{Dropoff in Spiral Arm Intensity with Wavelength}

We observed a dropoff in spiral arm intensity at longer wavelengths in SPHERE TI imagery, most prevalent in K1 (Figure~\ref{fig:r^2 SPHERE and GPI}), which suggests they are made up of small, compact grains. Though there is a low gas to dust ratio in the disk of HD 100453 \citep{kama16} there is also no detection of a small dust grain dominated tail by HST ACS \citep{collins09}. The lack of a tail, as seen in HD 141569 \citep{konishi16} and young debris disks, suggests the gas to dust is not low enough for radiation pressure to dominate. If gravitational interactions with the M-type companion are the source of the spiral arms, the small grains, which are more tightly coupled to the gas than the large grains, would be pulled more easily with the gas and may lie in a slightly different plane than the rest of the disk. This could explain why the arms are bluer than the rest of the outer disk and according to \citep{dong16} appear to be almost face on. When coupled with the difference in optical depth between the arms and the ring of the outer disk, this suggests that there is a gradient in the particle size distribution of the disk.

\subsection{Rejection of a Coplanar Disk System}

A coplanar inner and outer disk cannot reproduce the shadows seen in the SPHERE and GPI data. From the shadow separation and comparison of model images to data we find a misaligned inner disk with $\Delta i = 45 \pm 10\degr$ and a rotation of the inner disk major axis of -40 $\pm 10\degr$ with respect to the outer disk or 100$ \pm 10\degr$ East of North. This disagrees however with \citet{lazareff16} who find a major axis PA for the inner edge of the inner disk of 81$\pm 1\degr$ East of North. This measurement was found using simplified ellipse and ring models of the inner disk based on VLTI/PIONIER H-band data taken from 2012 December 19 to 2013 February 20.

\subsection{Investigation into Shadow Location Over Time}

At this time there has been no observed change in the shadow pattern over the $\sim11.5$ months spanned by the SPHERE data taken by \citet{wagner15} and \citet{benisty17}. There is the possibility however, of a 19$\degr$ change in major axis position angle between the \citet{lazareff16} measurement and the \citet{wagner15} measurement which spans $\sim25-27$ months. If this is a change in the major axis it could be due to precession of the inner disk, orbital motion of material in the inner disk, or the discrepancy could be a warp between the shadowing structure and the inner region of the inner disk.

Though the cause of the misalignment between the inner and outer disk is unknown, it has been shown in $\beta$ Pic \citep{lagrange10} that a planet can warp the inner disk. If a planet did cause the misalignment of the inner disk in HD 100453 as suggested above, it would likely cause precession of the inner disk, and by extension the shadows. However, this precession would occur on a timescale on the order of $10^3$ times the orbital timescale expected from Newtonian dynamics \citep{rawiraswattana16}. This suggests we should not observe a change in the location of the shadows due to precession for timescales less than a decade. A change of $19 \pm 10\degr$ in $\sim25-27$ months ($\sim16\degr yr^-1$) is too large to be accounted for with precession and is therefore not the cause of the discrepancy.

The orbital radius of an object with this orbital motion would be $\sim10$ au. This is much larger than the proposed outer radius of the inner disk and just outside the region excluded by speckle residuals in GPI data. The large radius and lack of any disk detection in GPI data suggest this is also likely not the cause of the discrepancy between major axis PAs.

This leaves us with a warp between the inner region of the inner disk (traced by VLTI/PIONIER) and a shadowing region further out. Though this cannot be ruled out using existing GPI or SPHERE data, N-band measurements using VLTI/MATISSE would allow for the angular resolution necessary to detect any difference in the inner and outer portions of the inner disk.

\subsection{Frequency of Transitional Disks with Misaligned Inner Disks}

To date, three of the fourteen, $\sim21\%$, transitional disks of with published images have exhibited these shadows which suggests they are not uncommon. The origin of the shadows however, is still under debate. Suggested causes include: stellar magnetic activity \citep{pffeiferanddong04}, perturbation by the binary companion \citep{martin14}, an unseen planet on an inclined orbit \citep{mouillet97}, etc. However magnetic field strengths in Herbig stars like HD 100453A are small, $\sim$100G \citep{hubrig15} compared to the magnetic fields required for disk misalignment $\sim 10^3$G \citep{pffeiferanddong04}. A close binary system can cause a misaligned inner disk however \citet{collins09} did not observe a strong X-ray source at the location of HD 100453A which would be indicative of another M-type companion, and brighter stars would be visible in the SED. Alternatively a wide binary system, where the companion lies outside of circumstellar disk (as in the case of HD 100453), can also cause misaligned disks. However, this causes large outer disk eccentricity at higher misinclinations \citep{martin14} which is not seen here. The possibility of an unseen planet however, makes HD 100453 a promising candidate for future planet searches \citep{gratiaandfabrycky16}. To date however, there have been no radial velocity measurements taken for the star with the intent of planet detection. In addition this system resembles $\beta$~Pic in having a two belt architecture and a misaligned inner disk, indicating that similar structure in young debris disks is likely inherited from the transitional disk phase.

\section{Conclusions}

We have carried out GPI PI imaging of HD 100453 in Y-, J-, and K1-bands, and have examined the circumstellar disk using this data, the SED, and archival SPHERE TI imagery. With the help of the Monte Carlo Radiative tranfer code HOCHUNK3D, we have generated models which allowed us to probe the inner and outer disk morphology and make several testable predictions about the structure of the disk. Our conclusions are:

\begin{itemize}

\item The circumstellar disk of HD 100453 contains an inner disk which SED fitting suggests extends from 0.13 - 1 au, followed by a large radial gap (1 - 18 au), and an outer disk (18 - 39 au).

\item The outer disk is red in TI imagery, with \(\frac{fdisk}{ftotal}\) = $0.018 \pm 0.002$ in J-band and \(\frac{fdisk}{ftotal}\) = $0.025 \pm 0.002$ in H-band. This is similar in disk color to HR 4796, HD 169142, and 142527 \citep{schneider09,fukagawa10}, and is inconsistent with ISM-like grains at the disk surface. It's low gas to dust ratio \citep{kama16} point to HD 100453 evolving into a young debris disk.

\item Both TI and PI images exhibit azimuthally-localized dark features at similar PAs. The size of the features is sufficiently large that any single body clearing them would be detected as a bright source \citep{janson12}. Given the sharpness and narrow size of the features and their consistent appearance in PI and TI light we also exclude inhomogeneities in grain properties. We therefore suggest that they are shadows cast by an optically thick, misaligned inner disk.

\item An outer disk inclination of $5\degr$ \citep{dong16} from face on is not supported by the data. In contrast we measure an inclination of $25 \pm 10\degr$, in broad agreement with the 34$\degr$ inclination reported in \citet{wagner15}.

\item The degree of misalignment between the inner and outer disk can be determined using the separation of the shadows. We find this separation is best reproduced with a $\Delta i = 45 \pm 10\degr$ which also gives us the best fit to the NIR region of the SED.

\item Examination of the shadows can constrain the thickness of the inner disk. As the inner disk thickness increases the width of the shadows it causes also increases.

\item There is a difference in the color of the spiral arms and the rest of the outer disk. This suggests that they are likely made of small grains which couple to gas more easily and are separated from the outer disk through interaction with the M-type companion.

\item There is  a discrepancy of $\sim19\degr$ between the major axis PA for the inner disk found by \citet{lazareff16} and the one found in our study. Because of the long timescale required for precession and the lack of a visible blob at 10 au, we suggest that the cause of this discrepancy is a warp between the inner portion of the inner disk and an outer shadowing portion.

\end{itemize}

We have shown that shadow morphology and location constrains both the thickness and orientation of the inner disk as well as the flaring of the outer disk. This offers an independent means of measuring structure in transitional disks. In addition the possibility of differences between the inner and outer edges of the inner disk is intriguing and should be investigated further. Predictions of the shadowing model will be tested for this and other Herbig Ae/Be stars with VLTI/MATISSE and other interferometric instruments in the future.

\acknowledgements{Based in part on data obtained at the Gemini Observatory via the time exchange program between Gemini and the Subaru Telescope (GS-2015A-C-1). The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnolog\'{i}a e Innovaci\'{o}n Productiva (Argentina), and Minist\'{e}rio da Ci\^{e}ncia, Tecnologia e Inova\c{c}\~{a}o (Brazil). MT is partly supported by JSPS KAKENHI 2680016. CAG is supported under NASA Origins of Solar Systems Funding via NNG16PX39P. Y.H. is supported by Jet Propulsion Laboratory, California Institute of Technology under a contract from NASA. MS is supported by NASA Exoplanet Research Program NNX16AJ75G. J.K. acknowledges support from Philip Leverhulme Prize (PLP-2013-110, PI: Stefan Kraus). S.K. acknowledges support from an ERC Starting Grant (Grant Agreement No. 639889). We also thank the referee for their comments and suggestions which added clarity to this paper.}

redpajama_set_name: RedPajamaArXiv


Aims The purpose of this short article is to examine the safety and efficacy data of dapagliflozin, saxagliptin, and their combination in the administration of patients with type 2 diabetes. monotherapy. Summary 471-05-6 manufacture Dapagliflozin/saxagliptin combination is normally well tolerated 471-05-6 manufacture and is an efficient tool in assisting individuals with diabetes improve glycemic control. solid course="kwd-title" Keywords: SGLT2 inhibitor, DPP4 inhibitor, single-tablet mixture, diabetes mellitus Intro By 2015, 415 million people all over the world possess type 2 diabetes (DM2), which is likely to boost to 600 million by 2040.1 Tight glycemic control can hold off or avoid the development of macrovascular2,3 and 471-05-6 manufacture microvascular complications.4,5 Like a progressive disease, individuals often require multiple antihyperglycemic agents for adequate control.6 However, lots of the diabetes medicines are 471-05-6 manufacture connected with undesirable unwanted effects. Insulin and secretagogues can raise the risk for hypoglycemia and trigger putting on CXCR6 weight.7 As much as 85% of individuals with DM2 already are overweight,9 and weight-loss is an integral objective in the management of diabetes since it will certainly reduce insulin resistance and comorbid conditions such as for example hypertension and dyslipidemia.7 Thiazolidinediones can result in fluid retention aswell as putting on weight, and could be unsafe for sufferers with preexisting center failing.8 Metformin make use of may be tied to gastrointestinal unwanted effects or renal insufficiency.10 Provided the potential risks for complications with intensified glycemic control4,11 and the various side-effect profiles of varied antihyperglycemic agents, an individualized approach should be used.12,13 Although metformin continues to be first-line together with way of living adjustment, add-on therapy is still left up to individual preference and doctor common sense.12,13 Within their placement statement for administration of hyperglycemia in DM2, the American Diabetes Association (ADA) as well as the Western european Association for the analysis of Diabetes (EASD) recommend initiation of mixture therapy if hemoglobin A1c (HbA1c) is 9.0% to attain target quicker.6 The Canadian Diabetes Association also recommends initiating combination therapy when HbA1c is 8.5%.12 Similarly, the 2015 American Association of Clinical Endocrinologists/American University of Endocrinology (AACE/ACE) In depth Diabetes Administration Algorithm recommends the initiation of mixture therapy if HbA1c is 7.5% at diagnosis or if an individual does not meet glycemic focuses on after three months of monotherapy.14 This recognizes the higher problems in achieving glycemic control if added therapy is delayed,12 as extended hyperglycemia can lead to glucotoxicity, increasing progressive -cell function reduction.15 Whenever combination therapy is necessary, drugs using different mechanisms of action are suggested.12 The most recent suggestions from AACE/ACE and ADA/EASD cite more impressive range evidence helping the addition of a dipepti-dyl peptidase-4 (DPP4) inhibitor and/or a sodium-glucose cotransporter type 2 (SGLT2) inhibitor.6,14 Although SGLT2 inhibitors can increase insulin awareness, endogenous glucose creation is increased through increased glucagon.16 Conversely, DPP4 inhibitors can also increase insulin awareness but suppresses glucagon, producing their pairing mechanistically complementary.17 Single-pill mix of dapagliflozin 10 mg/saxagliptin 5 mg continues to be developed to capitalize upon this benefit.18 Single-tablet combination (STC) supplements have been found in many chronic illnesses such as for example cardiovascular illnesses, AIDS, and diabetes.19 By simplifying medication regimen, combination pills have already been proven to improve adherence and standard of living.20,21 Dapagliflozin/saxagliptin was the initial SGLT2 inhibitor and DPP4 inhibitor mixture tablet approved in European countries.22 By Feb 2017, this medication in addition has been approved for make use of with the U.S. Meals and Medication Administration (FDA) as an adjunct to way of living adjustment for the administration of DM2.23 This content will review the data for efficiency and protection of dapagliflozin and saxagliptin as person and add-on therapy. The five existing stage III studies because of their combined make use of and their function in the administration of DM2 are talked about later. Strategies A non-systematic search was performed on Ovid, PubMed, and Google Scholar utilizing a mix of keywords, including SGLT2 inhibitor, DPP4 inhibitor, dapagliflozin, saxagliptin, and diabetes. Relevant content were selected predicated on name and abstract review. Ongoing scientific trials were determined from www.clinicaltrials.gov for dapagliflozin and saxagliptin, with a particular curiosity for combined make use of in diabetes. For completeness, sources had been also mined from essential review content and meta-analyses. Saxagliptin System of actions DPP4 is certainly a course of membrane-bound endopeptidases in.


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The Worthing Street Velodrome returns to Beach House Grounds tomorrow, buildingon the success of the inaugural 2015 event.
It features a dedicated schools' day on the Friday, free public drop-in tuition and have-a-go sessions on Saturday followed by amateur and pro-level competitive races on Sunday.
In addition to the track action, there will be a range of cycling related trade stands, an international pop-up food arena from the Proto Group, further edible treats from other local providers alongside a live acoustic music stage hosted by Northbrook College and Shoreham Allstars.
On Saturday, the acoustic stage will remain open until 9pm, with food and drink continuing to be provided until the last note of the evening's entertainment rings out.
The music stage is a new addition and will feature Northbrook current and graduating students, together with the stars of S'koolFest and the Shoreham Allstars.
Sunday will begin with a Peloton along the Prom starting at 9.30am from the seafront shelter at the foot of George V Avenue, organised by Worthing resident Jeremy Strutt.
See www.WorthingStreetVelodrome.co.uk for a full list of the events each day.


One of products on the basis of which the balanced food allowances are under construction is kefir. The reasons of it are not accidental. The demand of kefir is caused, in addition to its fine nutritiousness, also unusual medical qualities. Extraordinary useful properties of kefir root in the process of formation of kefir of milk.
The technology of kefiric production is concluded in milk souring by introduction of special microorganisms – yeast and lactic bacteria. Process of transformation of milk into kefir approximately such is. Milk proteins are split by bacteria to the lactic acid which is easier acquired by organism and serving as nutrient for barmy fungi. Barmy fermentation leads to formation of alcohol and release of carbon dioxide, in easy degree of irritating stomach wall that involves strengthening of gastric sokoobrazovaniye and increases intensity of secretion of digestive enzymes. Working jointly, barmy fungi and lactic bacteria destroy large molecules of milk protein. Therefore in comparison with whole milk kefirs are acquired several times quicker.


text:
Corporate Funders
Sport + Prevention Center
District Advocacy Toolkit 2019
Impact Grant Program
Nov 22 2018 December 19, 2018
RALIANCE joins the line-up on the Comedy Cellar Podcast November 22, 2018
Blog, Podcasts
Listen to RALIANCE's Kristen Houser, journalist Dahlia Lithwick, and comedian Mateo Lane discuss important topics on November 22, 2018's edition of The Comedy Cellar Podcast.
Nov 19 2018 November 15, 2018
Uber and NSVRC release new taxonomy to tackle sexual violence
Blog, Workplace
In Uber's new policy blog, "Counting it is the first step towards ending it," Uber's Chief Legal Officer Tony West and Kristen Houser, Chief Public Affairs Officer at RALIANCE and our partner organization the National Sexual Violence Resource Center, unveil a new taxonomy developed in partnership with the Urban Institute to help categorize incidents of sexual misconduct and sexual assault reported on the Uber platform.
Around the world, from corporate boardrooms to government offices, data drives decision-making.
So when it comes to sexual harassment, misconduct and assault, which is significantly underreported and thus lacks widely available data – particularly for acts that may not be considered criminal such as inappropriate comments – having very clear data is critical to pursuing sustainable solutions that will help end sexual violence in one generation. The new taxonomy categorizes reports of sexually violent experiences based on very specific, easy to understand language based on human behavior. Using and categorizing this more precise language will ultimately increase the availability of data and drive appropriate courses of prevention activity, ultimately informing how best to support users of the Uber platform.
As Tony and Kristen write:
These challenges create a landscape in which the limited information that is reported out provides only an incomplete and fragmented understanding of the true scope and scale of sexual violence. The value of a carefully-developed taxonomy for reported incidents of sexual harassment, sexual misconduct, or sexual assault is that it can increase consistency and help us to identify trends, thereby informing the development of more effective response and prevention efforts.
This new taxonomy is a step towards Uber's goal of creating transparency reports for sexual violence that are shareable and useful to support and advance similar efforts in other businesses and industries. RALIANCE applauds this effort and we see this as the latest step in our mission to end sexual violence in one generation.
You're invited! Please join us on November 28 for a Twitter Chat about supporting incarcerated survivors
For the #MeToo movement to survive, it's important for all voices to be heard. Groups such as incarcerated survivors, asylum seekers and members of the disabilities and transgender communities are a part of the #MeToo movement. Yet, many of their stories and experiences have yet to be amplified in the national conversation about how to prevent and end sexual harassment, misconduct and abuse in our society.
Join RALIANCE and partners at the New York State Coalition Against Sexual Assault and the South Carolina Coalition Against Domestic Violence and Sexual Assault on Wednesday, November 28 at 3pm ET for #PREAChat, an important Twitter Chat about meeting the needs of incarcerated survivors.
Send your RSVP and questions to [email protected]. We look forward to chatting with you soon!
Preventing Sexual Violence in Sport: Panel at APHA Annual Meeting
Blog, Sport
Sport Panelist at APHA. Left to Right: David Lee, Jennifer Yore, Katie Hanna, and Jeff Milroy
At the 2018 American Public Health Association Annual Meeting in San Diego on Monday, RALIANCE's David Lee presented at a great panel session titled "Preventing sexual violence in sport." Along with three colleagues, they shared the opportunities for sport to be part of the solution in ending sexual violence. Each of us shared examples of comprehensive prevention efforts that involve engaging athlete, coaches and administrators in advancing sexual violence prevention within sport and how sport can take leadership in prevention efforts for the broader society.
I started the session describing the work of RALIANCE in its Sport + Prevention Center.and the report How sport can end sexual violence in one generation. In the presentation I share how our research showed that sport can promote accountability, social cohesion and self control, all of which are protective factors for sexual violence prevention. Jeffrey J. Milroy, DrPH, MPH, of the University of North Carolina Greensboro followed with his presentation on "Translating evidence into sexual violence prevention for collegiate student-athletes."
Jennifer Yore, MPH, of Center on Gender Equity and Health (GEH), University of California, San Diego, describe the researcher think tank hosted by the GEH and RALIANCE "Sport as an incubator and accelerator for sexual violence prevention. " which resulting the RALIANCE report Recommendations for Next Steps In Research and Evaluation. The final presentation by Katie Hanna, MEd, U.S. Center for SafeSport, "Putting Athlete Well-being First: How the U.S. Center for SafeSport is working to champion respect and prevent abuse in sports." Described sexual violence prevention efforts in the 50 National Governing Boards of the US Olympic movement.
This panel presentation was important to demonstrate how public health concepts of prevention can support making changes in sport in order to prevent sexual violence.
Oct 31 2018 December 19, 2018
RALIANCE impact grantee Our VOICE featured on PreventConnect podcast on prevention work in bars and breweries
Learn more about RALIANCE impact grantee Our VOICE in Asheville, NC working to change the local culture around alcohol and sexual violence on this latest episode from PreventConnect's Podcast series: Partnering with bars to prevent sexual violence across North Carolina.
PreventConnect RALIANCE Podcast Series: Marketing Consent in Missoula, MT
Hear Brenna Merrill of Make Your Move Missoula chat about the consent campaign supported by funding from a RALIANCE impact grant on the lateste episode from PreventConnect on the RALIANCE Podcast Series: Marketing Consent in Missoula, MT.
Oct 24 2018 October 24, 2018
It's Not "A Very Scary Time for Young Men"
Blog, Culture
Changing the culture of sexual violence starts with men acknowledging that our words and actions have been part of the problem
Kicking off Give A Buck – Because change can't wait!
Today, we are launching a new social media and crowd-funding campaign called Give A Buck! We know sexual violence is a serious and widespread problem. And – change can't wait.
Sexual violence has dominated headlines for years – sexual harassment and assault on campuses, in churches, in Hollywood, in newsrooms, in the military… it happens everywhere. It's time to act now – all of us working together to end sexual violence in one generation.
We have the opportunity now to build broad support for programs that prevent sexual harassment, misconduct, and assault in our communities. #TimesUp and #MeToo have made wonderful advances for victims' services. Our #GiveABuck social media campaign builds awareness and supports prevention.
Are you ready to tell the world you Give A Buck about ending sexual harassment, misconduct, and assault?
Go to our Give A Buck site and sign up to be a participant, take the pledge, or to learn more today!
A year after #MeToo, taking the pulse of sexual violence prevention
Blog, Media
"What a difference a year makes," or so goes the old adage.
It's been one full year since the New York Times broke the story about Harvey Weinstein's decades of sexual harassment abuses. One year later, The Cut published "Our Year of Reckoning: An Exhaustive Timeline," detailing the day-to-day developments over the past 365 days related to how the world has sought long-overdue accountability for decades of sexual harassment, misconduct, and abuse. The Silence Breakers made room for so many more to come forward and continue driving social change. We're finally seeing a true public reckoning with the societal attitudes, behaviors, and beliefs that must change for sexual violence to be eradicated once and for all.
Another old adage: "What gets measured, gets done." That's why over the last three years, since our founding, RALIANCE has been tracking and benchmarking what's been unfolding related to our shared mission to end sexual violence in one generation. Last year's report foreshadowed just how powerful social media and other forms of activism could be, helping survivors of sexual violence find their agency and their voice. When we released that report in late September 2017, we had no idea how powerful the collective voice would be for the thousands who said #MeToo in the following days and weeks.
As RALIANCE is poised to release our 2018 report, we continue our focus on several key themes:
Accountability: For the first time, many who used their positions of power to cause harm faced actual repercussions. This also forced many of us to think beyond criminal justice solutions and engage corporations and institutions to lean into their values to examine accountability as part of healthy workplace cultures.
Prevention is possible: #MeToo has brought basic principles of prevention into living rooms and lunch rooms, into our homes, workplaces, and streets. We can build a culture that promotes equity, consent, and safety for all.
Leaders are needed: To end sexual violence, we need more people to come forward in their own communities to show courage. We must continue to be bold in 2018 and beyond. And we must continue to invest resources and commit to change to build safer, healthier environments.
Be on the lookout for our annual report, "Ending Sexual Violence in One Generation: A Progress Report for the United States 2018," publishing soon!
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Aziz Ansari is back – are we ready for redemption?
Accepting Nominations for the Linda Saltzman New Investigator Award
RALIANCE celebrates 3rd anniversary
RALIANCEFollow
RALIANCE@RALIANCEOrg·
Do you know of an outstanding investigator working in the field of sexual violence or related issues? Nominate them for the Linda Saltzman New Investigator Award: https://t.co/PvSglqBYVH
Our criminal justice system often automatically disbelieves people who say they've been raped. https://t.co/vsl4qc0KJA
Today's your LAST CHANCE to register for the @ItsOnUs National Student Leadership Summit: https://t.co/q41sIHQkPw
RALIANCE was created with seed-funding from the National Football League.
We are pleased to help drive real change, support innovative programs and make significant & lasting headway in combatting sexual violence. We all have a role to play.
- Roger Goodell, NFL Commissioner
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