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Trip Introduction
We organise tours in Kathmandu taking you around various historic, religious and cultural sites in and around the valley. During the tour, our experienced guide will take you to various important sites and explain you the significance of the places. We also take you to hill stations around Kathmandu valley from where you can enjoy great landscape views and mountains views. During a Kathmandu tour, you will see historically important places like Kathmandu durbar square, Patan Durbar Square, Bhaktapur Durbar Square, Swayambhunath (also known as Monkey Temple) and Pashupatinath temple. All of these places have their own significance. Kathmandu, Patan and Bhaktapur were three separate kingdoms in the past. Three different Malla kings ruled the Kathmandu, Patan and Bhaktapur separately. The sculpture and architecture, the durbar squares these three places have are mostly from the Malla regime
Kathmandu Durbar Square:
It is easy to be overwhelmed by the seemingly uncountable monuments in the Kathmandu Durbar Square. The house of the Living Goddess ( Kumari Ghar ), the ferocious Kal Bhairab, the red monkey god, and hundreds of erotic carvings are a few examples of the sights at the Square! The buildings here are the greatest achievements of the Malla dynasty, and they resulted from the great rivalry between the three palaces of Kathmandu, Patan, and Bhaktapur. The Valley was divided among the children of Yaksya Malla. For visitors today, and for the Nepalese, it was serendipitous that they, and later their off springs, began an artistic warfare trying to outdo each other in splendid constructions. Kings copied everything their neighbours built in an even grander style. A visitor who wanders around the Square will see a round temple in the pagoda architectural style, the temple of Goddess Taleju (legend has it that She played dice with King Jaya Prakash Malla), and an image of Shiva and Parbati sitting together among the many monuments.
The Square teems with colorful life. Vendors sell vegetables, curios, flutes, and other crafts around the Kastamandap rest house. This rest house is said to have been built with the wood of a single tree and is the source from which the Kathmandu Valley got its name. Nearby are great drums, which were beaten to announce royal decrees. All woodcarvings, statues, and architecture in this area are exceptionally fine, and Kathmandu Durbar Square is among the most important sights for travellers to see. The complex also houses the Tribhuvan Museum that carries the mementos of different Shah Kings.
Pashupatinath:
Pashupatinath is the holiest Hindu pilgrimage destination in Nepal. There are linga images of Shiva along with statues, shrines, and temples dedicated to other deities in the complex. A temple dedicated to Shiva existed at this site in AD 879. However, King Bhupatindra Malla built the present temple in 1697. A gold-plated roof, silver doors, and woodcarvings of the finest quality decorate the pagoda construction. Guheswari Temple, restored in AD 1653, represents the female "force". It is dedicated to Satidevi, Shiva's first wife, who gave up her life in the flames of her father's fire ritual.
A circuit of the Pashupati area takes visitors past a sixth-century statue of the Buddha, an eighth-century statue of Brahma the creator and numerous other temples. Some other places to visit are Rajrajeswari Temple, built in 1407, Kailas with lingas more than 1,400 years old, Gorakhnath temple, and the courtyard of Biswarup. There are rows of Shiva shrines and Hindu pilgrims from all over South Asia offer worship to Shiva, the Lord of Destruction.
The Bagmati River flows close by and the Arya Ghat cremation grounds are here. We strongly advise photographers not to take photos of cremations and of bereaved families. Sadhus, sages who follow the lifestyle of Shiva, may be seen covered in ashes and loincloths. They ask for money in case you want to take their photos. Those of Hindu faith only may enter the main Pashupatinath courtyard.
Swayambhunath:
The history of the Valley, according to the legends, begins with Swayambhu, or the "the self-existent". In times uncharted by history, Boddhisatwa Manjusri came across a beautiful lake during his travel. He saw a lotus that emitted brilliant light at the lake's center, so he cut a gorge in a southern hill and drained the waters to worship the lotus. Men settled on the bed of the lake and called it the Kathmandu Valley. From then on, the hilltop of the self-existent Lord has been a holy place.
Swayambhu's light was covered in time because few could bear its intensity. By the thirteenth century, after many layers were added to the original structure that enveloped the Lord's power, a dome-like shape had been acquired. The stupas central mast was damaged and replaced at that time. Peripheral sources of power were discovered on the hilltop as well and stupas, temples, and rest houses were built to honour them. Images of important deities, both Buddhist and Hindu, were also installed. Today, age-old statues and shrines dot the stupa complex.
Behind the hilltop is a temple dedicated to Manjusri or Saraswati – the goddess of learning.
Swayambhu is, perhaps, the best place to observe the religious harmony in Nepal. The stupa is among the most ancient in this part of the world, and its worshippers are diverse from Newar nuns, Tibetan monks, and Brahmin priests to lay Buddhists and Hindus. The largest image of the Sakyamuni Buddha in Nepal is in a monastery next to the stupa. Other monasteries here have huge prayer wheels; fine Buddhist paintings, and special butter lamps, which may be lit after presenting monetary offerings.
Swayambhu is a major landmark of the Valley and looks like a beacon below the Nagarjun hill. It provides an excellent view of the Kathmandu Valley. Devotees have climbed the steps on the eastern side for centuries. Statues of the Buddha, mini stupas, monasteries and monkeys make the climb to Swayambhu – which is fairly steep – worthwhile. But for someone who is pressed for time, the western road allows you to get off your transport almost at the base of the stupa.
Bouddhanath:
Bouddhanath is among the largest stupas in South Asia, and it has become the focal point of Tibetan Buddhism in Nepal. The white mound looms thirty-six meters overhead. The stupa is located on the ancient trade route to Tibet, and Tibetan merchants rested and offered prayers here for many centuries. When refugees entered Nepal from Tibet in the 1950s, many of them decided to live around Bouddhanath. They established many gompas, and the "Little Tibet" of Nepal was born. This "Little Tibet" is still the best place in the Valley to observe Tibetan lifestyle. Monks walk about in maroon robes. Tibetans walk with prayer wheels in their hands, and the rituals of prostration are presented to the Buddha as worshippers circumambulate the stupa on their hands and knees, bowing down to their lord.
Many people believe that Bouddhanath was constructed in the fifth century, but definite proof is lacking. The stupa is said to entomb the remains of a Kasyap sage who is venerable both to Buddhists and Hindus. One legend has it that a woman requested a Valley king for the donation of ground required to build a stupa. She said she needed land covered by one buffalo's skin and the King granted her wish. She cut a buffalo skin into thin strips and circled off a fairly large clearing. The king had no choice but to give her the land.
The Bouddha area is a visual feast. Colorful thangkas, Tibetan jewellery, hand-woven carpets, masks, and khukuri knives are sold in the surrounding stalls. Smaller stupas are located at the base. Gompa monasteries, curio shops, and restaurants surround Bouddhanath. Conveniently situated restaurants with rooftop patios provide good food and excellent views of Bouddhanath.
Machhendranath Temple:
The temple is situated at Machhendra Bahal near Indrachowk. This two storeyed temple was built by Yaksha Malla in 1500 AD. The chariot festival of white Mahchendranath (the god of mercy) is annually celebrated in Kathmandu Valley. The traditional music is always played in the evening at this temple, which is also open to westerners.
Thamel:
Thamel area has recently emerged as the most popular tourist area of Kathmandu. Thamel is a 15 to 20 minute walk from the center of Kathmandu. Thamel has clean narrow streets full of mushrooming lodges, hotels for budget travellers. Restaurants, bars and other tourists oriented shops can be seen bustling with activities.
Patan Durbar Square:
This whole square is a cluster of fine pagoda temples and stone statues; it is at the same time the business hub of the city. At every step one comes across a piece of art or an image of a deity, testifying to the consummate skill of Patan's anonymous artists. The ancient palace of the Malla kings and the stone baths associated with various legends and episodes of history are especially interesting to visitors. The stone temple of Lord Krishna and the Royal Bath (Tushahity) with its intricate stone and bronze carvings are two other masterpieces in the same vicinity.
Golden Temple:
This three-storey golden pagoda of Lokeshwar in Patan was built in the twelfth century A. D. by King Bhaskar Varma. Located in the courtyard of Kwabahal, this temple is in a class of its own. A golden image of Lord Buddha and a big prayer wheel can be seen on the pedestal of the upper part of the Car while intricate decorative patterns on its outer walls add charm to the mellow richness of the shrine.
Mahaboudha:
The temple of Mahaboudha is a masterpiece of terra cotta. Like the Krishna Mandir, it reveals an artistic tradition that evolved outside of Nepal and shows how native Nepalese craftsmen have been able to do justice to an unfamiliar art form. This temple was built by Abhaya Raj, a priest of Patan and is sometimes referred to as the temple of a million Buddha because every single brick bears a small image of Buddha. There is an astonishing total of nine thousand bricks. It was leveled to the ground in the great earthquake of 1933 but was rebuilt exactly to the original specifications, proving that the temple craft is still one of the living arts of Nepal.
Jagat Narayan:
The Jagat Narayan temple is a tall shikhara-style temple consecrated to Lord Vishnu. The temple is built of red bricks on the bank of the Bagmati at Sankhamul and enshrines many stone images. The fine metal statue of Garuda placed on a stone monolith is quite eye-catching and is accompanied by similarly placed images of Ganesh and Hanuman.
Krishna Temple:
The temple of Lord Krishna holds a commanding position in Patan's Palace complex. Though its style is not wholly native, it is one of the most perfect specimens of Nepalese temple craft. The three-storey stone temple continues to elicit high praise from lovers of art and beauty. It was built by King Siddhi Narasingha Malla in the sixteenth century A. D. Important scenes from the Mahabharata and Ramayana epics have been carved in bas-relief. The minute details of this work clearly show the high level that the art of stone carving attained in the sixteenth century.
Machhendranath:
The temple of Red Machhendranath is another center of attraction in Patan. The temple lies in the middle of a wide, spacious quadrangle just at the outer rim of the market place. A fine clay image of Red Machhendranath Avalokiteshwar is housed here for six months every year, after which it is taken round the city of Patan in a colourful chariot during the festival beginning in April-May and lasting sometimes for several months.
Bungmati & Khokana:
Bungmati and Khokana are listed in the UNESCO's list of world heritage sites as a medieval cultural town. The town is rich in culture and famous for its mustard oil and chilly.
Bhaktapur Durbar Square:
Bhaktapur Durbar Square is a conglomeration of pagoda and shikhara-style temples grouped around a fifty-five window palace of brick and wood. The square is one of the most charming architectural showpieces of the Valley as it highlights the ancient arts of Nepal. The golden effigies of kings perched on the top of stone monoliths, the guardian deities looking out from their sanctuaries, the woodcarvings in every place-struts, lintels, uprights, tympanums, gateways and windows-all seem to form a well-orchestrated symphony. The main items of interest in the Durbar Square are:
The Lion Gate:
Dating as far back as 1696 A.D., this gate is guarded on either side by two huge statues of lions. Alongside, there are two stone images of Bhairab (the dreadful aspect of Shiva) and Ugrachandi (the consort of Shiva in her fearful manifestation).
The Golden Gate:
The Golden Gate is said to be the most beautiful and richly moulded specimen of its kind in the entire world. The door is surmounted by a figure of the goddess Kali and Garuda (the mythical man-bird) and attended by two heavenly nymphs. It is also embellished with mythical creatures of marvellous intricacy. In the words of Percy Brown, an eminent English art critic and historian, the Golden Gate is the most lovely piece of art in the whole Kingdom: it is placed like a jewel, flashing innumerable facets in the handsome setting of its surroundings. The gate was erected by King Ranjit Malla and is the entrance of the main courtyard of the Palace of Fifty-five Windows.
The Palace of Fifty Five Windows:
This manificent palace was built during the reign of King Yakshya Malla in A.D. 1427 and was subsequently remodeled by King Bhupatindra Malla in the seventeenth century. Among the brick walls with their gracious setting and sculptural design, is a balcony with Fifty-five Windows, considered to be a unique masterpiece of woodcarving.
The Art Gallery:
The Art Gallery contains ancient paintings belonging to the Hindu and Buddhist traditions of various periods and descriptions. This gallery is open everyday except Tuesday.
The Statue of King Bhupatindra Malla:
This statue showing King Bhupatindra Malla in the act of worship is set on a column facing the palace. Of the square's many statues, this is considered to be the most magnificent.
Dattatraya Temple:
The temple of Dattatraya is as old as the Palace of Fifty-five Windows. Consecrated by King Yakshya Malla in 1427 A. D., this temple, according to popular belief, was built out of the trunk of a single tree. It was subsequently repaired and renovated by King Vishwa Malla in 1458 A. D. Just beside the temple is a monastery (Math) with exquisite carvings.
Nyatapola Temple:
This five-storey pagoda was built by King Bhupatindra Malla in 1702 A. D. It stands on five terraces on each of which squat a pair of figures: two famous wrestlers, two elephants, two lions, two griffins and Baghini and Singhini -the tiger and the lion goddesses. Each pair of figures is considered ten times stronger than the ones immediately below, while the lowest pair, the two strong men Jaya Malla and Phatta Malla, was reputedly ten times stronger than any other men. This is one of the tallest pagoda temples in Kathmandu Valley and is famous for its massive structure and subtle workmanship.
Bhairabnath Temple:
This is another pagoda style temple dedicated to Lord Bhairab, the dreadful aspect of Shiva. It stands a short distance away from the temple of Nyatapola and was originally constructed by King Jagat Jyoti Malla on a modest scale. It was later remodeled by King Bhupatindra Malla, a zealous lover of the arts, into what is now a three-storey temple.
Changu Narayan:
Narayan, or Vishnu, is the preserver of creation to Hindus. His temple near Changu village is often described as the most ancient temple in the Kathmandu Valley. A fifth century stone inscription, the oldest to be discovered in Nepal, is located in the temple compound and it tells of the victorious King Mandev. The temple now covers sixteen hundred years of Nepalese art history. The temple, built around the third century, is decorated by some of the best samples of stone, wood, and metal craft in the Valley. In the words of one tourist guide, "When you look upon Changu Narayan, you observe the complete cultural development of the Valley."
On the struts of the two-tiered Changu Narayan Temple, are the ten incarnations in which Narayan destroyed evildoers. A sixth-century stone statue shows the cosmic form of Vishnu, while another statue recalls his dwarf incarnation when he crushed the evil king Bali. Vishnu as Narasingha disemboweling a demon is particularly stunning. The western bronze doors sparkle in the evening sunlight, dragons decorate the bells, and handsome devas stare from the walls. Garuda, half man and half bird, is the steed of Vishnu, and his life-sized statue kneels before the temple. The favourite of many tourists is the statue of Vishnu sitting astride his steed.
Nagarkot:
Nagarkot, located 32 kilometers east of Kathmandu, is one of the most scenic spots in Bhaktapur district and is renowned for its spectacular sunrise view of the Himalaya when the weather is clear. Visitors often travel to Nagarkot from Kathmandu to spend the night so that they can be there for the breathtaking sunrise. Nagarkot has become famous as one of the best spots to view Mount Everest as well as other snow-topped peaks of the Himalayan range of eastern Nepal. It also offers an excellent view of the Indrawati river valley to the east. With an elevation of 2,195 meters, Nagarkot also offers a panoramic view of the Valley and is described by visitors as a place whose beauty endures year round.
Many visitors prefer to visit Nagarkot in the spring when surrounding valleys break out in a rich kaleidoscope of different coloured flowers. The flowers are beautiful against the serene backdrop of the snow-covered mountains. Ever popular among the tourists are the short treks and picnics, which Nagarkot offers. Treks from Nagarkot are unique and delightful. For anyone who wants to have an adventure without exerting much effort, a hike to Nagarkot's surrounding areas would be a good option. One can traverse short distances on trekking trails and come close to nature's wonders such as the outer of verdant forests, flower-covered meadows and unusual rock formations.
Dhulikhel, Panauti:
Both Panauti and Dhulikhel are traditionally Newar settlements. In Panauti, you can find traditional Newari culture, architecture and sculpture. Panauti is also features in the list of World Heritage Sites of UNESCO.
Dhulikhel is a Newar town similar to that of Nagarkot. You can see good landscapes and mountain views. You will stay overnight in Dhulikhel enjoying the sunset views and the great landscape.
Kathmandu Durbar Square, Swayambhunath and Pashupatinath
Patan Durbar Square, Bungmati/Khokana
Bhaktapur Durbar Square, Nagarkot
Dhulikhel, Panauti
Return to Kathmandu
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Title: Purothionin
Literature References: A low mol wt wheat protein composed of a1-, a2- and b-purothionins. Contains about 20% cystine, 10% arginine and 10% lysine. Isoln from unbleached patent flour: A. K. Balls, W. S. Hale, Cereal Chem. 17, 243 (1940); A. K. Balls et al., ibid. 19, 279 (1942). Inhibits the growth of bacteria and yeasts: L. S. Stuart, T. H. Harris, ibid. 288. Toxic effects in animals: E. J. Coulson et al., ibid. 301. Sepn and characterization of a- and b-purothionin: D. G. Redman, N. Fisher, J. Sci. Food Agric. 19, 651 (1968); C. C. Nimmo et al., ibid. 25, 607 (1974). Amino acid sequences of a1- and b-purothionin: S. Ohtani et al., Agric. Biol. Chem. 39, 2269 (1975); eidem, J. Biochem. 82, 753 (1977); of b-purothionin: A. S. Mak, B. L. Jones, Can. J. Chem. 54, 835 (1976); of a1 and a2-purothionin: B. L. Jones, A. S. Mak, Cereal Chem. 54, 511 (1977). Review: D. D. Kasarda et al., "Wheat Proteins" in Advances in Cereal Science and Technology vol. 1 (Am. Cereal Chem., St. Paul, 1976) pp 208-210.
Properties: Forms a cryst hydrochloride. Freely sol in water. Easily digested by proteolytic enzymes including cryst chymotrypsin, chymopapain, papain.
Derivative Type: a1-Purothionin
Additional Names: 5-L-Arginine-27-glycine-33-L-isoleucine-34-L-serine-42-glycine-purothionin A I (reduced); purothionin A II
Molecular Formula: C198H340N68O56S8
Molecular Weight: 4825.76
Percent Composition: C 49.28%, H 7.10%, N 19.74%, O 18.57%, S 5.32%
Additional Names: 5-L-Arginine-6-L-threonine-18-L-serine-26-L-serine-27-L-threonine-42-glycine-purothionin A I (reduced)
Derivative Type: b-Purothionin
Additional Names: Purothionin A I
Others monographs:
Ethyl Tartrate Glyceraldehyde 3-Phosphate Miglitol Ammonium Bisulfate
Renin Furfuryl Alcohol Tegaserod Ergoloid Mesylates
Adipsin Valacidin Reversine Barium Peroxide
5-Nitroquinaldic Acid Potassium Borohydride Uglow Black Silver Quinine
©2016 DrugLead US FDA&EMEA

redpajama_set_name: RedPajamaCommonCrawl


text:
Haley Randall est une joueuse américaine de hockey sur gazon. Elle évolue au poste de milieu de terrain au Saints Field Hockey et avec l'équipe nationale américaine.

Biographie
 Naissance le 5 juillet 1998 à Virginia Beach.
 Élève à l'Université Duke.

Carrière
Elle a fait ses débuts en équipe première le 15 mai 2021 contre la Belgique à Anvers lors de la Ligue professionnelle 2020-2021 et elle arrête le 3 avril 2022 après son match de Ligue professionnelle 2021-2022 contre les Pays-Bas à Amsterdam.

Palmarès

Références

Joueuse américaine de hockey sur gazon
Naissance en juillet 1998
Naissance à Virginia Beach

redpajama_set_name: RedPajamaWikipedia


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Arsenal News Arsenal Rumours
Are Arsenal eyeing this winger to replace Alexis Sanchez?
By GoonerP - 12 March 2017, 23:59
Arsenal sent scouts to watch Wolverhampton Wanderers winger Helder Costa this weekend, amidst speculation linking Alexis Sanchez with a possible exit.
The Chilean has supposedly told his team-mates that he wishes to leave the club this summer, and his exit will leave the club with some seriously big shoes to fill.
Our club are unlikely to line up any signings before the end of the season due to the unknown uture of our boss, but whether Arsene Wenger remains in charge or not, our manager of next season will have a number of targets recommended to him from our scouting network.
One player who could potentially come in to take some of the slack off his exit is Helder Costa, who is currently the stand-out star for Wolves.
The 23 year-old joined the club on loan during last summer, before the club made the move permanent in January for a club-record £13 Million, and his agent, super-agent Jorge Mendes, is supposedly keen on earning him a move already, with a £20 Million fee being talked of.
Chelsea and Arsenal are said to have had scouts watching the Portugese star this weekend, while his side took on Rotherham in the Championship, although he did not put in the perfect display, including missing a penalty to put us ahead in the opening half, and found himself taken off just after an hours play.
The young star has racked up 10 goals for his side this season, but has failed to earn a regular role in any of his former sides, and could pose a risk signing at this point in his career.
Monaco chose to overlook trying to sign him permanently after using him on loan during the 2015-16 term, but after thoroughly impressing Wolves, the club moved to tie him down to a four-and-a-half year deal only half-way through his pre-agreed loan deal.
Wolves clearly felt they had to move fast to secure his signature, but is he ready for the top level? Should Arsenal make their move this summer? Could he prove a long-term replacement for Alexis?
Tags Arsenal Helder Costa Wolves
Arsenal gets harsh FA cup draw but very winnable
Budd says:
Mendes? Not going to happen if Wenger is still the manager.
ambitious teams replace their star man after departing with another star player or two, and we are talking about an unknown in a lower league who couldn't even play regularly in his previous clubs, to replace Alexis Sanchez.
the trend here could be well read, every year or 2, we sell players that could win us the league or more with some positive additions, we never build a team to win anything (FA cup not a major thing) coz we sell stars and remain with flops, it's a recurring trend and will never stop unless some old clueless someone is replaced
vinie2000 says:
WoW! not a surprise, is not it ? Our scouts are so GOOD , are not they? Helder Costa from Wolves for 20 millions to replace Alexis. what a wonderful world and for sure Mr Wenger will have look at him. Really? As i mentioned times after times. THE SCOUT TEAM SHOULD BE FIRED! the most incompetent scouts in the whole league. they spotted the likes of Sanogo, Park the korean wonder, the Japanese boy on loan in Germany who hardly touch a ball there, the Bolivian Messi ( Galindo ) , the next Neymar ( wellington ) just to mention few and Wenger approve the sings, really? what an ambitious team, aren't we? what about the likes of ABUMAYANG, LACAZETTE, Kante? that's ambition. If we have got 2 of those 3 players plus Mustaffi and Xhaka last summer spending 120 millions then we could not be in the position we are and behind the Manager all the way but we are not competing at all. Have your thoughts fellas, are we ambitious ?


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JASON ALDEAN SELLS OUT BOSTON'S FENWAY PARK IN 90 MINUTES
Kid Rock To Join Aldean on SIX STRING CIRCUS TOUR Stadium Stop Sept. 9
After previously smashing attendance records set by Paul McCartney and Dave Matthews Band at Boston's Fenway Park, this year's ACM "Entertainer of the Year" Jason Aldean will return to a sold out crowd at the home of the Red Sox on Sept. 9th. Serving as the first country artist to play at the iconic ballpark, fans snagged every ticket this morning within 90 minutes. The "Lights Come On" singer will co-headline the stop with multi-Platinum award-winner Kid Rock as part of his SIX STRING CIRCUS TOUR.
Aldean recently released his "muscular new single" (Rolling Stone) "Lights Come On" as the lead single from his upcoming seventh studio album, which immediately reached the No. One spot on Billboard's Country Digital Songs chart upon release. He will return to the road as his SIX STRING CIRCUS TOUR launches May 19th in Rogers, AR with continued support from Thomas Rhett and A Thousand Horses. For more information and for a full list of upcoming tour dates, visit www.jasonaldean.com.


This webinar will look at two districts that have pioneered the development of competency-based approaches and will examine how policies can support or hinder district level systems-change. Thomas Rooney, Superintendent, Lindsay Unified School District, California will discuss the district's motivation and approach to pursuing a district-wide competency-based system.
As school systems across the country recommit themselves to ensuring college and career readiness and success, they must rely on districts to translate federal and state policies into the local context.
The College & Career Readiness & Success (CCRS) Center recently released a brief titled How Career and Technical Education Can Help Students Be College and Career Ready: A Primer. This brief examines the role of career and technical education (CTE) in preparing students for both college and the workforce in a changing postsecondary landscape.
The importance of aligning college and career readiness initiatives—from the common core and career technical education standards, to funding streams like Title I and Perkins, as well as to school structural changes like expanded learning time and career academies—is a growing concern in the field. Dr.
Co-hosted with the Alliance for Excellent Education, this session focused on Linked Learning, a transformative approach for secondary education that integrates a college preparatory academiccore with career and technical education and work-based learning opportunities in small, career-themed pathways to increase student motivation, engagement and achievement.
Read more about Goals and Expectations for College and Career Readiness: What Should Students Know and Be Able to Do?


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Jos̩ Serra РNet Worth 2022, Age, Height, Bio, Salary
See learn details about José Serra Net Worth, Age, Height, Bio, Salary. Also discover famous Politician José Serra's Birthday, Measurements, Physical Stats, Dating, Wiki and more.
José Serra was born in Brazil on March 19, 1942. Politician who served as Minister of Foreign Affairs of Brazil from 2016 to 2017. He received his Masters and Ph.D. in economics from Cornell University. He was exiled from Brazil when he was 22 for serving as president of the National Student Union which opposed the existing conservative regime.
His parents are Francesco Serra and Serafina Chirico. He married ballerina Mónica Allende in 1967. They have children Veronica and Luciano. he has not shared about he's parent's name. Our team currently working, we will update Family, Sibling, Spouse and Children's information. Right now, we don't have much information about Education Life.
he is one of the successful Politician. he has ranked on the list of those famous people who were born on March 19. he is one of the Richest Politician who was born in Sao Paulo. he also has a position among the list of Most popular Politician. José Serra is 1 of the famous people in our database with the age of 77 years old.
First Name Joy
Last Name Behar
Profession Politician
Birth Date March 19, 1942
Birthday March 19
Birth Place Sao Paulo
Shoe Size 11 (US), 9 (UK)
House José Serra has been known to live his own house.
Favorite Food Baguette
Favorite Color Turquoise
Favorite Place Pu'uhonua o Honaunau National Historical Park (Hawaii)
Favorite Sports Tennis
Favorite Books Hamlet
Favorite Movie Doctor Zhivago (1965)
Instagram José Serra on Instagram
Twitter José Serra on Twitter
Facebook José Serra on Facebook
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text:
\section{Introduction}

In 1998, two supernovae teams discovered that our Universe is undergoing an accelerated expansion \cite{ref:Riess98,ref:Perlmuter99}. From that time on, a flood of models have been presented to explain the accelerated expansion phase. For the reviews about the accelerated expansion and dark energy, please see
\cite{ref:DEReview1,ref:DEReview2,ref:DEReview3,ref:DEReview4,ref:DEReview5,ref:DEReview6,ref:DEReview7}.
A natural candidate to dark energy is the cosmological constant (CC) which was first introduced by Einstein to realize a static universe about a century ago. In the context of quantum field
theory (QFT), CC has relations with the vacuum or zero point energy
density of quantum fields, via
\begin{equation}
\rho_{\Lambda}=\frac{1}{2}\int^{\Lambda}_{0}\frac{4\pi k^2
dk}{(2\pi)^3}\sqrt{k^2+m^2}\approx\frac{\Lambda^4}{16\pi^2},
\end{equation}
where $\Lambda\gg m$ is a UV cut-off. To balance an assumed UV
cut-off $\Lambda$ and the observational smallness of CC, tremendous
fine tuning is required. This is the so-called cosmological constant
problem \cite{ref:DEReview1}. QFT in curved space-time leads to an infinite effective action or
vacuum expectation values (VEV) of the energy-momentum tensors of
the fields. A renormalization treatment can yield a scale-dependent
or running CC and a running Newton constant. Though, the absolute
values can not be calculated, the change with respect to the
renormalization scale can be calculated via renormalization group equations (RGEs) originating in QFT
\cite{ref:RGEsQFT} and quantum gravity \cite{ref:RGEsQG}. In the
cosmological context, it is reasonable to identify the
renormalization scale with some characteristic scales of cosmology.
The related investigation can be found in \cite{ref:PhDthesis},
where the renormalization scale $\mu$ was given by the Hubble scale
$H$, the inverse radius $R^{-1}$ of the cosmological event horizon
and the inverse radius $T^{-1}$ of the particle horizon.

Another interesting viewpoints about the relations between vacuum energy density and a cosmological scale come from the so-called holographic principle in cosmology. According to the holographic principle, the number of degrees of freedom in a bounded system should be finite and has relations with the area of its boundary. By applying the principle to cosmology, one can obtain
the upper bound of the entropy contained in the universe. For a
system with size $L$ and UV cut-off $\Lambda$ without decaying into
a black hole, it is required that the total energy in a region of
size $L$ should not exceed the mass of a black hole of the same
size, thus $L^3\rho_{\Lambda} \le L M^2_{pl}$. The largest $L$
allowed is the one saturating this inequality, thus $\rho_{\Lambda}
=3c^2 M^{2}_{pl} L^{-2}$, where $c$ is a numerical constant and
$M_{pl}$ is the reduced Planck Mass $M^{-2}_{pl}=8 \pi G$.
It just means a {\it duality} between UV cut-off and IR cut-off. The
UV cut-off is related to the vacuum energy, and IR cut-off is
related to the large scale of the universe, for example Hubble
horizon, event horizon or particle horizon as discussed by
\cite{ref:holo0,ref:holo1,ref:holo2}. Then in this context the so-called fine tuning problem is removed naturally.

In the paper \cite{ref:holo2}, the
author proposed a dark energy model, dubbed holographic dark energy (HDE), where the future event horizon
\begin{equation}
R_{eh}(a)=a\int^{\infty}_{t}\frac{dt^{'}}{a(t^{'})}=a\int^{\infty}_{a}\frac{da^{'}}{Ha^{'2}}\label{eq:EH}
\end{equation}
was taken as the IR cut-off $L$. This horizon is the boundary of the volume a
fixed observer may eventually observe. One is to formulate a theory
regarding a fixed observer within this horizon. As pointed out in
\cite{ref:holo2}, it can reveal the dynamic nature of the vacuum
energy and provide a solution to the {\it fine tuning} and {\it
cosmic coincidence} problem.

The concrete value of parameter $c$ is very important to determine the properties of HDE. For example in the epoch when the HDE becomes to dominate the energy density, i.e. $\Omega_{h}\sim 1$, if $c\ge 1$, $c=1$ and $c\le 1$ are respected, the HDE behaves like quintessence, cosmological constant and phantom respectively. One can clearly see that in the following Eq. (\ref{eq:DEEOS}) by setting $\Omega_{h}=1$. In the past years, the HDE model was confronted with cosmic observations. In Ref. \cite{ref:Kao2005}, the authors used the angular scale of the acoustic oscillation from the BOOMRANGE and WMAP data on CMB to constrain HDE model. Also the authors of Ref. \cite{ref:Gong2005} used the CMB shift parameter $R$ to constrain HDE model. For the recent result please see \cite{ref:holoZhang} where the best fit value of parameter $c=0.65^{+0.10}_{-0.08}$ in $1\sigma$ region was given. In that paper, about the CMB information only the CMB shift parameter $R$, acoustic scale $l_A$ and the redshift $z_\ast$ at the decoupling epoch of photons obtained from WMAP-7yr in $\Lambda$CDM model were employed. The main problem comes from the fact that the values of the CMB shift parameters used in the literature for example \cite{ref:holoZhang}, depend on the cosmological model, here the $\Lambda$CDM model. So, when one uses these derived data points to constrain other cosmological models, the so-called circular problem, i.e. dependence on cosmological models, would be committed. And the circular problem is what we try to avoid in the cosmological constraint issue. Therefore one should constrain the cosmological model in a consistent way by using cosmic observational data points which do not depend on any cosmological model. However to use full CMB data sets from WMAP7-yr to constrain the HDE model is still missing in the literature. In this paper to fill up the gap, we will use the full information from WMAP-7yr data sets in stead of CMB shift parameters. Furthermore, the CMB shift parameters contain information around the last scattering surface of background photons where the contribution from dark energy may not be neglected as CC case due to a nontrivial equation of state (EoS) of dark energy, for example early dark energy model \cite{ref:EDE}. In this situation, it is dangerous to use theses derived data points from $\Lambda$CDM model to constrain other cosmological model due to much departure from $\Lambda$CDM model. At late epoch when the dark energy dominates, the gravitational potentials decay and the late integrated Sachs-Wolfe (ISW) arises. It affects to the anisotropy power spectra of CMB at large scale (low $l$ parts). The ISW effect is sensitive to the properties of dark energy. Apparently, the late ISW effect is not expressed by the CMB shift parameters. So one can expect a tight constraint to cosmological model parameter space when the late ISW effect is included.

Base on these points mentioned above, in this paper we will not use the derived CMB shift parameters but the full information from WMAP-7yr data points to constrain the HDE model. The important is that there doesn't exist any circular problem. Due to the full information from WMAP-7yr is used, one can expect to obtain a tight constraint. At low redshift regions, the type Ia supernova (SN Ia) and baryon acoustic oscillations (BAO) are also included as geometric measures.

This paper is structured as follows. In section \ref{sec:bgpe}, we give a brief review of the HDE model where the radiation is included and the future event horizon adopted as an IR cut-off. The scalar perturbation evolution equations for a spatially flat FRW Universe will also be presented. In section \ref{sec:method}, the constraint methodology and results will be presented. We give a summary in section \ref{sec:summary}.

\section{Background and Perturbation Evolution Equations} \label{sec:bgpe}

Now, as is done in \cite{ref:holo2}, the event horizon $R_{eh}$
taken as the IR cut-off. Then, the HDE is written as
\begin{equation}
\rho_{h}=\frac{3c^2 M^2_{pl}}{R^2_{eh}},\label{eq:EHHDE}
\end{equation}
and the Friedmann equation in a spatially flat FRW Universe can be written as
\begin{equation}
H^2=H^2_0\left(\Omega_{r0}a^{-4}+\Omega_{b0}a^{-3}+\Omega_{c0}a^{-3}\right)+\Omega_{h}H^2,\label{eq:EHFE}
\end{equation}
where $\Omega_{i}=\frac{\rho_i}{3 M^2_{pl}H^2}$ are dimensionless energy densities for radiation, baryon, cold dark matter and HDE respectively. For convenience, the scale factor $a$ has been
normalized to $a_0=1$. Combining Eq. (\ref{eq:EHHDE}) and Eq.
(\ref{eq:EH}), one has
\begin{equation}
\int^{\infty}_{a}\frac{d\ln
a'}{Ha'}=\frac{c}{aH\sqrt{\Omega_{h}}},\label{eq:re}
\end{equation}
where the definition of dimensionless energy density parameter for HDE is used.
From Eq.(\ref{eq:EHFE}), one obtains
\begin{equation}
\frac{1}{Ha}=\frac{\sqrt{1-\Omega_{h}}}{a H_0
\sqrt{\left(\Omega_{r0}a^{-4}+\Omega_{b0}a^{-3}+\Omega_{c0}a^{-3}\right)}}.
\end{equation}
Inserting the above equation into Eq. (\ref{eq:re}), one has
\begin{equation}
\int^{\infty}_{x}\frac{\sqrt{1-\Omega_{h}}}{E(x')}dx'=\frac{c\sqrt{1-\Omega_{h}}}{E(x)\sqrt{\Omega_{h}}},\label{eq:difomehah}
\end{equation}
where $E(x)=\sqrt{\Omega_{r0}e^{-2x}+\Omega_{b0}e^{-x}+\Omega_{c0}e^{-x}}$ and $x=\ln a$. Taking derivative with respect to $x =\ln a$ from
both sides of the above equation, one has the differential equation
of $\Omega_{h}$
\begin{equation}
\Omega_{h}'=-2\Omega_{h}\left(1-\Omega_{h}\right)\left(\frac{E'(x)}{E(x)}-\frac{\sqrt{\Omega_{h}}}{c}\right),\label{eq:diffeq}
\end{equation}
where $'$ denotes the derivative with respect to $x =\ln a$. This
equation with initial condition $\Omega_{h0}=1-\Omega_{r0}-\Omega_{b0}-\Omega_{c0}$ describes the evolution of dimensionless energy density of
dark energy. Then the background evolution will be obtained by solving this differential equation and Friedmann equation. When the baryon and radiation components are omitted, one has $E'(x)/E(x)=-1/2$. Then the evolution equation for $\Omega_h$ \cite{ref:holo2}
\begin{equation}
\Omega_{h}'=\Omega_{h}\left(1-\Omega_{h}\right)\left(1+\frac{2}{c}\sqrt{\Omega_{h}}\right),
\end{equation}
is recovered. From the
conservation equation of the HDE
$\dot{\rho_{h}}+3H(\rho_{h}+p_{h})=0$, one has the equation of state (EoS) of holographic
dark energy
\begin{equation}
w_{h}=-1-\frac{1}{3}\frac{d \ln \rho_{h}}{d \ln a}
=-\frac{1}{3}-\frac{2\sqrt{\Omega_{h}}}{3c}\label{eq:DEEOS}
\end{equation}
where $w_{h}=p_{h}/\rho_{h}$.

In this paper, we take the HDE as a perfect fluid having EoS (\ref{eq:DEEOS}). Considering the perturbation in the synchronous gauge and the conservation of energy-momentum tensor $T^{\mu}_{\nu;\mu}=0$, one has the perturbation equations of density contrast and velocity divergence for the HDE
\begin{eqnarray}
\dot{\delta}_h=-(1+w_h)(\theta_d+\frac{\dot{h}}{2})-3\mathcal{H}(c^{2}_{s}-w_h)\delta_h\\
\dot{\theta}_h=-\mathcal{H}(1-3c^{2}_{s})\theta_h+\frac{c^{2}_{s}}{1+w_h}k^{2}\delta_h-k^{2}\sigma_h
\end{eqnarray}
following the notations of Ma and Bertschinger \cite{ref:MB}. For the gauge ready formalism about the perturbation theory, please see \cite{ref:Hwang}. For the HDE, we assume the shear perturbation $\sigma_h=0$.
In our calculations, the adiabatic initial conditions will be taken.

\section{Methodology and Constraint Results} \label{sec:method}

Before constraining the model parameter space, we study the effects of model parameter $c$ to the CMB power spectrum by setting different values of $c$ and fixing the other relevant cosmological model parameters. At fist, we modify the CAMB package \cite{ref:CAMB}, which is the code for calculating the CMB power spectrum and is publicly available, to include the HDE. The differential equation (\ref{eq:diffeq}) was solved by taking $\Omega_{h0}=1-\Omega_{m0}-\Omega_{r0}$ as initial condition. We borrow and fix the other relevant cosmological parameters values from WMAP7, the resultant CMB power spectra are shown in Fig. \ref{fig:cls} for different values of $c$, where $h=0.72$,  $\omega_c=0.112$, $\omega_b=0.0226$, $n_s=0.96$ are fixed.
\begin{widetext}
\begin{center}
\begin{figure}[htb]
\includegraphics[width=14cm]{cls.eps}
\caption{The CMB $C^{TT}_l$ power spectrum v.s. multiple moment $l$ and the corresponding ratio to $\Lambda$CDM model for different values of model parameter $c$, where $h=0.72$,  $\omega_c=0.112$, $\omega_b=0.0226$, $n_s=0.96$ are fixed. The main difference appears at low ($l<20$) multipole momentum parts which correspond to large scale.}\label{fig:cls}
\end{figure}
\end{center}
\end{widetext}

From Fig. \ref{fig:cls}, one can see that the main contribution to CMB power spectra from the HDE comes from the evolution of EoS and its domination at the late epoch through late ISW effect. At early epoch the contribution to CMB power spectra is small due to small energy density ratio of the HDE, that can be understood from the EoS of the HDE (\ref{eq:DEEOS}) which seems close to $-1/3$ before the last scattering surface. It means that a tight constraint would be obtained when CMB information from large scale is included. But unfortunately, the CMB data points are dominated by the so-called cosmic variance at large scale, i.e. low $l$ part.

We perform a global fitting to the model parameter space by using the Markov Chain Monte Carlo (MCMC) method. We modified publicly available {\bf cosmoMC} package \cite{ref:MCMC} to include the HDE in the CAMB \cite{ref:CAMB} code which is used to calculate the theoretical CMB power spectrum. The following $7$-dimensional parameter space  is adopted
\begin{equation}
P\equiv\{\omega_{b},\omega_c, \Theta_{S},\tau, c,n_{s},\log[10^{10}A_{s}]\}
\end{equation}
where $\omega_{b}=\Omega_{b}h^{2}$ and $\omega_{c}=\Omega_{c}h^{2}$ are the physical density of  baryon and cold dark matter respectively, $\Theta_{S}$ (multiplied by $100$) is the ration of the sound horizon and angular diameter distance, $\tau$ is the optical depth, $c$ is the newly added model parameter related to HDE, $n_{s}$ is scalar spectral index, $A_{s}$ is the amplitude of of the initial power spectrum. The pivot scale of the initial scalar power spectrum $k_{s0}=0.05\text{Mpc}^{-1}$ is used in this paper. The following priors to model parameters are adopted: $\omega_{b}\in[0.005,0.1]$, $\omega_{c}\in[0.01,0.99]$, $\Theta_{S}\in[0.5,10]$, $\tau\in[0.01,0.8]$, $c\in[0,1]$, $n_{s}\in[0.5,1.5]$, $\log[10^{10}A_{s}]\in[2.7, 4]$. Furthermore, the hard coded prior on the comic age $10\text{Gyr}<t_{0}<\text{20Gyr}$ is also imposed. Also, the physical baryon density $\omega_{b}=0.022\pm0.002$ \cite{ref:bbn} from big bang nucleosynthesis and new Hubble constant $H_{0}=74.2\pm3.6\text{kms}^{-1}\text{Mpc}^{-1}$ \cite{ref:hubble} are adopted.

To get the distribution of parameters, we calculate the total likelihood $\mathcal{L} \propto e^{-\chi^{2}/2}$, where $\chi^{2}$ is given as
\begin{equation}
\chi^{2}=\chi^{2}_{CMB}+\chi^{2}_{BAO}+\chi^{2}_{SN}.
\end{equation}
The $557$ Union2 data \cite{ref:Union2} with systematic errors and BAO \cite{ref:BAO} are used to constrain the background evolution, for the detailed description please see Refs. \cite{ref:Xu}. SN Ia is used as standard candle. And BAO is used as standard ruler. At the last scattering of CMB radiation, the acoustic oscillation in the baryon-photon fluid was frozen and imprinted their signature on the matter distribution. The characterized scale of BAO in the observed galaxy power spectrum is determined by the comoving sound horizon at drag epoch $z_d$ which is shortly after photon decoupling and defined as the redshift at which the drag optical depth $\tau_d$ equals one. To calculate $r_{s}(z_{d})$, one needs to know the redshift $z_d$ at the drag epoch and its corresponding sound horizon. The baryon drag epoch redshift $z_d$ can be obtained from its definition and be calculated numerically \cite{ref:Hamann}
\begin{eqnarray}
\tau(\eta_d)&\equiv& \int_{\eta}^{\eta_0}d\eta'\dot{\tau}_d\nonumber\\
&=&\int_0^{z_d}dz\frac{d\eta}{da}\frac{x_e(z)\sigma_T}{R}=1
\end{eqnarray}
where $R=3\rho_{b}/4\rho_{\gamma}$, $\sigma_T$ is the Thomson cross-section and $x_e(z)$ is the fraction of free electrons. Then the sound horizon is
\begin{equation}
r_{s}(z_{d})=\int_{0}^{\eta(z_{d})}d\eta c_{s}(1+z).
\end{equation}
where $c_s=1/\sqrt{3(1+R)}$ is the sound speed. Also, to obtain unbiased parameter and error estimates, we use the substitution \cite{ref:Hamann}
\begin{equation}
d_z\rightarrow d_z\frac{\hat{r}_s(\tilde{z}_d)}{\hat{r}_s(z_d)}r_s(z_d),
\end{equation}
where $d_z=r_s(\tilde{z}_d)/D_V(z)$, $\hat{r}_s$ is evaluated for the fiducial cosmology of Ref. \cite{ref:BAO}, and $\tilde{z}_d$ is redshift of drag epoch obtained by using the fitting formula \cite{ref:EH} for the fiducial cosmology. Here $D_V(z)=[(1+z)^2D^2_Acz/H(z)]^{1/3}$ is the 'volume distance' with the angular diameter distance $D_A$. In this paper, for BAO information, the SDSS data points from \cite{ref:BAO} and the WiggleZ data points \cite{ref:wiggles} are used. For CMB data set, the temperature power spectrum from WMAP $7$-year data \cite{ref:wmap7} are employed as dynamic constraint.

After running $8$ independent chains and checking the convergence to stop sampling when the worst e-values [the variance(mean)/mean(variance) of 1/2 chains] $R-1$ is of the order $0.01$, the global fitting results are summarized in Table \ref{tab:results} and Figure \ref{fig:contour}. We find that the values of $c$ in $1,2,3\sigma$ regions are $c= 0.696_{-  0.0737-   0.132-  0.190}^{+   0.0736+   0.159+  0.264}$, which are compatible with the result obtained in \cite{ref:holoZhang}. And the error bars are slightly smaller than that in \cite{ref:holoZhang}. This result shows that the values of $c$ are less than $1$ at $3\sigma$ level. Correspondingly, we plot the CMB power spectrum for the mean values estimated from MCMC analysis in Figure \ref{fig:mean}, where the observational data points of $7$-year WMAP with uncertainties are also included. As comparisons, the CMB temperature power spectrum for $\Lambda$CDM with same cosmic observational data sets combination and results from \cite{ref:wmap7} are also shown. One can see that the CMB power spectrum for the HDE is well inside the error bars of the binned measurements from WMAP $7$-year results and matches to $\Lambda$CDM model very well. This strongly implies that current cosmic observational data combinations of SN Union2, BAO and WMAP $7$-year can not almost discriminate the HDE  from $\Lambda$CDM model. In this sense, the HDE is a competitive model of dark energy.

\begingroup
\begin{table}
\begin{center}
\begin{tabular}{ccc}
\hline\hline Prameters&Mean with errors & Best fit \\ \hline
$\Omega_b h^2$ & $    0.0226_{-    0.000546-    0.00107}^{+    0.000536+    0.00108}$ & $0.0226$\\
$\Omega_{DM} h^2$ & $    0.110_{-    0.00414-    0.00838}^{+    0.00422+    0.00866}$ & $0.112$\\
$\theta$ & $    1.0396_{-    0.00263-    0.00520}^{+    0.00268+    0.00513}$ & $1.0400$\\
$\tau$ & $    0.0892_{-    0.00719-    0.0226}^{+    0.00635+    0.0251}$ & $0.0865$\\
$c$ & $    0.696_{-    0.0737-    0.132}^{+    0.0736+    0.159}$ & $0.643$\\
$n_s$ & $    0.971_{-    0.0134-    0.0255}^{+    0.0135+    0.0262}$ & $0.971$\\
$\log[10^{10} A_s]$ & $    3.0802_{-    0.0337-    0.0646}^{+    0.0340+    0.0704}$ & $3.0805$\\
$\Omega_h$ & $    0.727_{-    0.0171-    0.0349}^{+    0.0172+    0.0323}$ & $0.733$\\
$Age/Gyr$ & $   13.878_{-    0.113-    0.216}^{+    0.110+    0.221}$ & $13.839$\\
$\Omega_m$ & $    0.273_{-    0.0172-    0.0323}^{+    0.0171+    0.0349}$ & $0.267$\\
$z_{re}$ & $   10.623_{-    1.161-    2.229}^{+    1.189+    2.352}$ & $10.468$\\
$H_0$ & $   69.916_{-    1.844-    3.585}^{+    1.867+    3.635}$ & $71.0657$\\
\hline\hline
\end{tabular}
\caption{The mean values of model parameters with $1\sigma$ and $2\sigma$ errors, where WMAP $7$-year, SN Union2 and BAO data sets are used.}\label{tab:results}
\end{center}
\end{table}
\endgroup

\begin{widetext}
\begin{center}
\begin{figure}[htb]
\includegraphics[width=17cm]{cont.eps}
\caption{The 1D marginalized distribution on individual parameters and 2D contours  with $68\%$ C.L. and $95\%$ C.L. by using CMB+BAO+SN data points. The shade regions show the mean likelihood of the samples.}\label{fig:contour}
\end{figure}
\end{center}
\end{widetext}
\begin{widetext}
\begin{center}
\begin{figure}[htb]
\includegraphics[width=17cm]{mean.eps}
\caption{The CMB $C^{TT}_l$ power spectrum v.s. multiple moment $l$, where the grey dots with error
bars denote the observed data with their corresponding uncertainties from WMAP $7$-year results, the green solid line is for HDE with mean values as shown in Table \ref{tab:results}, the red dotted line is for $\Lambda$CDM model with mean values taken from \cite{ref:wmap7} with WMAP+BAO+$H_0$ constraint results.}\label{fig:mean}
\end{figure}
\end{center}
\end{widetext}

We can show the evolutions of dimensionless energy density of the HDE and the EoS of the HDE with respect to redshift $z$ in Fig. \ref{fig:omhwh}, one can solve the differential equation (\ref{eq:difomehah}) by setting the initial conditions $\Omega_{h0}$ and model parameters $\Omega_{m0}=\Omega_{b0}+\Omega_{c0}$ and $c$ to their central values as listed in Table \ref{tab:results}, here $\Omega_{r0}$ is derived from the temperature of CMB background $T_0=2.726 K$.
\begin{widetext}
\begin{center}
\begin{figure}[htb]
\includegraphics[width=8cm]{omegah.eps}
\includegraphics[width=8cm]{wh.eps}
\caption{The evolutions of dimensionless energy density of the HDE (left panel) and EoS of the HDE (right panel) with respect to redshift $z$, where the central values of model parameters are taken as listed in Table \ref{tab:results}.}\label{fig:omhwh}
\end{figure}
\end{center}
\end{widetext}
From the Fig. \ref{fig:omhwh}, one can read off that the HDE is phantom like at late time and quintessence like at early epoch.

\section{Summary and Discussion} \label{sec:summary}

In this paper, we perform a global fitting to the HDE model by using MCMC method with the combination of the full information from CMB, BAO and  SN Ia data points. We analyze the effect of model parameter $c$ to the CMB power spectra by taking its different values. We find out that $c$ mainly contributes to CMB power spectra at large scale where the so-called cosmic variance is dominated. However, we still obtain a relative tight constrain to model parameter space where the values of $c$ with $1,2,3\sigma$ regions are achieved: $c= 0.696_{-  0.0737-   0.132-  0.190}^{+   0.0736+   0.159+  0.264}$. So at $3\sigma$ level, $c$ is a number less than $1$. As a comparison to the previous results obtained in \cite{ref:holoZhang}, a slightly tight constraint is achieved in this paper. More important is that a consistent constraint is carried out instead of using the derived CMB shift parameters. Based on this result, one can conclude that at least $3\sigma$ level the future Universe will be dominated by phantom like dark energy. Then the positive energy condition is not respected, however this condition must be satisfied to derive the holographic bound. So the current cosmic observational data points disfavor the HDE model based on our analysis.

Based on the holographic principle,  other HDE models were proposed in the literature where different IR cut-offs were adopted. For example, the Hubble horizon as IR cut-off was discussed when the model parameter $c$ is constant \cite{ref:holo1,ref:holo2} or time variable \cite{ref:XuJCAP}. In Ref. \cite{ref:Gao}, the authors took the Ricci scalar as the IR cut-off and named it Ricci dark energy, the corresponding cosmic observational constraint to this model could be found in Ref. \cite{ref:WangXu}. Interestingly, Cai, {\it et. al.} found out that the holographic Ricci dark energy had relations with the causal connection scale $R^{-2}_{CC} = \text{Max}(\dot{H} + 2H^2,-\dot{H} )$ for a spatially flat Universe \cite{ref:CAI}. Based on the idea that gravity as an entropic force \cite{ref:Verlinde},  a similar DE density was given in \cite{ref:EFS} where a linear combination of $H^2$ and $\dot{H}$ was also presented, see also \cite{ref:Hcom1,ref:Hcom2}. And a generalized HDE model $\rho_{R}=3c^2M^{2}_{pl}Rf(H^2/R)$ and $\rho_{h}=3c^2M^{2}_{pl}H^2g(R/H^2)$ were presented in Ref. \cite{ref:XuGHDE}. To the best of our knowledge, the full information from CMB has not been used to test these models yet. One can apply the method and data sets presented in this paper to these models directly.

\acknowledgements{The author thanks an anonymous referee for helpful improvement of this paper and Dr. Chan-Gyung Park for helping to plot the figures for CMB power spectra. L. Xu's work is supported by the Fundamental Research Funds for the Central Universities (DUT10LK31) and (DUT11LK39).}

redpajama_set_name: RedPajamaArXiv


If you're a particularly county proud smoker, then I believe I've just found the tobacco for you my friend!
Swizzels Matlow have been registering some old skool sweets as Trade Marks. I'm instantly pining for a double lolly!
'Snowfall' has been registered by Twentieth Century Fox Film Corporation – ALWAYS gets my attention. I've done some googling, and it looks like a series on FX written and directed by the director of Boyz in the Hood (after which I insisted picking up our house phone and answering 'who dis' every time it rang) – Pilot is already shot apparently, so coming soon!
'Tis the season and all of that! This company has a trade mark for Jingle Bells for Christmas Decorations and what not. Pretty neat.
Calling all gamers. This is a big release coming in 2016 to Europe on PS4 – It's called something else over in the east, but it's going to be called 'Nights of Azure' in Europe, that's official now!
I just thought this was a great play on executioner for an insect repellant!
I've just got something in my eye….
Sooooo, yesterday Irish Trade Mark Agents FR Kelly filed an application for 'Phantom' in the classes for radio and television broadcasting.
Could Phantom FM be returning is some shape or form now that the original has re-branded as TXFM?
The Irish registration for Phantom was renewed in 2014, but Wireless Media Limited, who initially registered it in 2004 was dissolved in 2012.
So who now owns the Irish registration, who is applying for the Europe Wide Trade Mark, and more importantly, why??
*I had originally stated that FR Kelly registered this Irish Trade Mark initially, however on further inspect that doesn't appear to be the case. Without sight of the whole file, I can't be certain, but it looks as though the Irish Trade Mark may have been registered by Wireless Media limited themselves on the initial application in 2004, and the address for service was changed to FR Kelly's offices in 2011. Apologies for any confusion, it wasn't my intention to mislead.
It's been a week or so since I trawled the European Trade Mark filings to see who has been filing what (I've been busy, ok?!) – Quite a few marks with noting so there is.
I didn't know what a 'subtweet' was until I Googled it (you mention someone without using their handle, FYI), but Twitter seem to want to take ownership of it anyway!
HBO (I just discovered that it stands for 'Home Box Office, who knew) have registered 'Winter is Coming' for T-Shirts and Hats and what not. If you're a Game of Thrones fan, apparently that will mean something to you!
Dublin's new logo has been filed for Europe Wide Protection, and on the same day it was revealed as well. How very efficient.
It's official 'Hangry' is here to stay, particularly if these new meat based snacks take hold!
Could it be? New music from Des'ree? According to Wikipedia she's retired and hasn't released any new music since 2003, but she's registered her name as a Trade Mark for music and recording.
Watch out Transformers, the Go-Bots are coming for you! Apparently, this brand is being re-launched! I don't really remember them, but I assume they were a poor mans transformers, were they?
The company behind Beanie Babies, have filed an application for Teenie Beanie Boos (apparently they came with McDonald's Happy Meals last year, I must have missed them).
And Body and Soul have applied to a Trade Mark for, well, Body and Soul.
I can't find anything about this on Google, so I'm assuming it's an as yet unannounced Huawei tablet/laptop/chromebook type device. Remember where you saw it first.
I'm not sure if this is the pizza or the drink, but either way, consider me interested.
Speaking of Facebook, it is going to warn you if your account has been hacked by a government, which was nice.


text:
Q: Why is subversion using system-name as username when running as system user? This has got me the whole day digging for answers. The bottom line is that when I run svn as system user it seems to use the system-name to authenticate against the SVN server regardless of what credentials are passed. Following is the long explanation that made arrive at that conclusion.
When running from a Windows 7 Professional, if I run svn from the console under any normal user, the application works as expected: if credentials have been cached in %AppData%/Roaming/Subversion it will use them, if not it will prompt for username and password unless I use the options --username and --password. If I enter credentials using the options then the commit works with no problem. All good so far.
But when I try to run svn as the system user (nt authority\system) in the same computer, it behaves differently. To begin with, %AppData%/Roaming/Subversion points to C:\Windows\System32\config\systemprofile\AppData\Roaming\Subversion, and I make sure there is no auth folder there, so no credentials cached. Then I run svn without any parameters and it doesn't prompt for username/password, instead it executes the action and receives an error from subversion:
svn: E175013: Commit failed (details follow):
svn: E175013: MKACTIVITY of '/svn/Development/!svn/act/f20db493-48f1-9c43-a957-541584be555e': 403 Forbidden (http://<ip-address>)

If I run it indicating --username and --password, it gets the same error. But then I check the error logs from subversion and find this:
[Fri Aug 08 17:32:18 2014] [error] [client <client IP>] Access denied: '<clienthostname>$' MKACTIVITY Development:
[Fri Aug 08 17:32:18 2014] [error] [client <client IP>] Access denied: '<clienthostname>$' DELETE Development:

Where <clienthostname> is the hostname of the computer where I'm trying to commit from (note the '$' at the end of the subversion log, that's not part of the hostname but it does appear in the log as part of the username).
So that's the question: why is svn behaving differently when running as system user? Why does it use the hostname as username when authenticating against the SVN server? And why do other users work correctly?
Note: I believe my problem is different from the following questions in stackoverflow:

*

*Subversion ignoring "--password" and "--username" options: I don't get any prompts to enter username and password, regardless of whether I indicate the options --username and --password or I don't

*SVN Error when commiting Access denied: 'foobar' MKACTIVITY MYREPO: I saw this question and I tried double checking the case of all the items in the URL, no luck.

*svn: MKACTIVITY 403 Forbidden: I have checked that no credentials are cached in %AppData%/Roaming/Subversion

For those who are wondering why I'm trying to run svn as system user, the answer is that I am trying to make a commit from TeamCity, which means it is the Build Agent the one executing the svn command. The Build Agent is a Windows Service and runs as system user, and the svn command fails in the way explained above.

A: *

*Use the "--no-auth-cache" in your svn commands and you won't see this issues. You might however run into other set of issues.

If you do not use the no-auth-cache it tries to figure out default username and password anyways

*

*A better way would be to create a .subversion folder and store the authentication in that folder. So for the system account, you can specify a differrent userid and password for the login.

redpajama_set_name: RedPajamaStackExchange


text:
Highways remain busy in the southeast
The Saskatchewan Ministry of Highways and Infrastructure has released its latest Traffic Volume Map, and it shows that the highways in southeast Saskatchewan continue to have a lot of traffic.
The data was recorded but it takes some time to compile and release, as it includes daily traffic numbers for hundreds of locations on highways throughout the province. It also shows how busy many highways are at city limits.
The busiest highway in the Estevan area is Highway 39 east of the city, with 5,900 vehicles a day at the area where the double lanes begin. That number drops down to 5,420 vehicles per day east of the junction of Highway 39 and the Shand Access Road, and then 4,850 vehicles per day prior to the junction of Highways 39 and 18.
It marked the first time a daily traffic tally has been taken for the double lane portion of Highway 39, since that project was completed in November 2017.
Further along, there were 1,410 vehicles per day near the Roche Percee access road, and 980 per day at the Canada-U.S. border.
Highway 39 west of the city limits is at 2,730 vehicles, and 3,490 vehicles per day west of the junction of the truck bypass.
The traffic doesn't dissipate a lot moving further from Estevan, as it consistently hovers around the 2,800 mark, and was at 2,790 vehicles per day around Midale.
As for the truck bypass itself, its busiest point is 2,310 vehicles per day east of the junction with Highway 47. The lowest point is 1,270 vehicles per day near the west junction with Highway 39. There were 1,690 per day at the east junction.
Highway 47 north of the city limits is at 2,650 vehicles per day, and 2,740 per day north of the truck bypass, which makes it the busiest spot for Highway 47 in the province.
Moving closer to Stoughton, it was at 1,960 per day at the junction of Highways 361 and 47, and at 1,450 south of Stoughton.
As for the area south of the city, Highway 47 sits at 1,250 vehicles at the south city limits, and 160 per day at the Canada-U.S. border crossing.
Highway 18 just west of Estevan had 1,910 vehicles and 1,180 a day west of the Boundary Dam Power Station access road. It dropped to 570 per day near Torquay and 470 per day west of Oungre.
Highway 18 east of Estevan and Highway 13 from Stoughton to the Manitoba border continue to have lots of traffic, too. Highway 18 had 2,380 vehicles per day near Oxbow, making it one of the busiest portions of Highway 18 in the province. In fact, the highway hovered between 2,380 vehicles and 1,990 vehicles each day from Bienfait to Oxbow, and remained above 1,400 vehicles heading into Carnduff.
Highway 13 peaked in the southeast from Stoughton to Carlyle, with 1,470 to 2,710 vehicles each day, and 1,500 to 2,100 per day from Carlyle to Redvers.
Highway 9 from Alameda to Moose Mountain provincial Park continues to see lots of activity as well, with anywhere from 1,750 per day at Alameda to 2,490 per day north of Carlyle. And Highway 361 near Lampman has 1,040 per day on the east town limits and 1,120 per day on the west town limits.
Dustin Pratt Memorial Fund supports St. Joseph's Hospital Foundation
Candidates share platforms at forum
Dustin Pratt Memorial Fund supports St. Joseph's Hospital ...
Popular Regional News
The Wheeler family loved playing The Feud
Carievale 4-H Beef Club remains busy
Seeing Estevan with a horse and carriage tandem
Meeting will look at the future of ECS
Year in Review 2019: What occurred in the Estevan area from September-December


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text:
Tears open trial of Kenyan leader
Charles Bremner
Wednesday September 18 2013, 1.01am, The Times
Uhuru Kenyatta, President of Kenya, is to stand trial next month
NOOR KHAMIS/REUTERS
A Kenyan woman described at the International Criminal Court (ICC) yesterday how a mob of machete-wielding youths locked her in a church along with many neighbours and set it alight, killing at least 28 people.
The woman, identified only as witness P-0536, was the first to appear at the trial in the Hague of William Ruto, Kenya's Deputy President, on charges of orchestrating violence after elections in 2007.
The burning of the Kenyan Assemblies of God church in the Rift Valley village of Kiambaa was one of the worst incidents in the blood-letting that killed more than 1,100. "I was carrying my small child with me," said the survivor, who wept as she spoke. "I threw my child out of the window."
The prosecutors at


Solar water heating, stage notice SWH, is water turned hot by solar moving picture acquired from sunlight for public publication, industrial or residential doings. Solar water heating systems are comprised of a water storage tank, heat transfer formless (HTF), and solar thermal collectors.
Solar hot water devices are accessible in two versions: responsive (pumped) or passive (compact). The solar collector, fitted regarding a wall facing the sun or a roof, warms occurring the liquid that is later circulated through an swift SWH or propelled by convection in a passive system. Collectors are composed of an insulated crate when a glass cover to the fore a black painted, solar metal absorber that is flat and fastened to the copper pipes, or several metal tubes enclosed by a unventilated vacuum (evacuated) cylinder of glass. Heat is stored in an cushioned water storage tank subsequent to an inlet and outlet attached to and out of the squirrel. Passive or alert household solar water heaters comprise of a auxiliary simulation-source (electricity or gas) activated approaching sunless days to guarantee a steady hot water supply behind tank water plummets under a sure temperature, typically of fifty five Celsius.
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Whereas the money of inactive solar hot water devices is cheap and effortless, non-passive appliances are much more useful at heating and retaining hot water. Non passive water heating systems are more costly and more complicated to repair in.
The tank is situated in a box related to a glass cover and insulated walls. The glass summit permits sun heat obtain to the storage tank, and the insulated sides decrease heat wastage from the water storage tank put taking place to to the vibes. The box additionally accommodates a mirror moreover surface that gives by now happening glow notice to the tank.
A two-dimensional exploit surrounding a network of piping, gone a grand glass summit that faces the sun.
As vacuity closes taking place heat wastage, water lines in an evacuated tube solar magpie are enclosed by 2 concentric tubes of heat-resistant glass that create a vacuum to recognize and retain glowing feeling within the solar collector pipes.
Flat plate solar collectors are typically more useful than evacuated tube collectors in sunny spells. Nevertheless, the cartoon agree of two-dimensional plate collectors subside shortly upon cloudy days similar in the midst of the go along bearing in mind of evacuated tube solar collectors that falls less hurriedly.
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text:
Apple's Budget iPhone Will Feature A Plastic Exterior Shell With Possible Metal Innards, According To Report
By Paul Morris | January 15th, 2013
The continuing reports and speculation surrounding the possibility of Apple releasing a budget iPhone suggests that even a denial from Phil Schiller can't seem to derail the iPhone rumor train. It has been widely speculated in the last few days that Apple intends to appeal to emerging markets and territories like Latin America with the release of a budget iPhone during 2013, with the latest reports suggesting that the company could save money on a phone of this nature by manufacturing it with a plastic outer shell and only including metal parts where necessary.
The latest in the wild speculation comes courtesy from the hit-and-miss rumor site DigiTimes. In an effort to cut costs and allow them to offer the device to their intended market at the intended price, it is being suggested that Apple intends to regress in terms of design and move back to a plastic type exterior shell that we originally saw with the iPhone 3G and iPhone 3G. At the time, the design of the 3G and 3GS the design was envied by other manufacturers, but as time has progressed and engineering and design principles developed it's unlikely that any premium iPhone user would be interested in a model with that design.
The same report is also suggesting that Apple is intending to use internal metal components within the budget iPhone and potentially make a feature out of the internals through a special design that would be saved purely for the budget iPhone. If Apple is intending to design and manufacture a budget iPhone to appeal to markets who are unable to justify the cost of a standard iPhone then it is widely speculated that we will see the device hitting shelves before the end of 2013. It remains to be seen whether or not the sixth-generation iPhone will land in October of this year or fall back to June for a Worldwide Developer Conference announcement in San Francisco.
The talk of a budget iPhone was initially laughed off when first discussed, but The Wall Street Journal and Bloomberg have both added fuel to the fire recently by publishing their belief that a secondary and cheaper iPhone is definitely on Apple's agenda. Everything we think we know about Apple and their desire to produce the best quality hardware would indicate that they won't ever do 'budget' hardware, but as the fire begins to grow, so does the potential for this to come to fruition.


Tarnya, 20, appeared on ABC's current affairs program Four Corners on July 4 2016. The program asked a simple question: Are we preparing our children and young people for the workplace of the future? Watch our video to get another take on Tarnya's story.