Here's another one to add to the glut of high grade, fast aperture, Micro Four Thirds, prime lens reviews: the Panasonic Leica Summilux 12mm F1.4 ASPH lens. At first, I decided not to review this lens mostly because I prefer to work with longer focal lengths. Also, the Panasonic 12mm F1.4 lens has been around since 2016 and there are already several reviews available. The lens has been sitting in my camera bag for a while now, as I went along shooting on the streets. I've used it for certain shots – out of curiosity or when I needed a wide angle lens. Eventually, I'd used it enough that it made sense to review it – if for nothing else, but the sake of completeness.
It isn't crucial to have wide apertures for very wide angle lenses since we generally want as much depth of field as possible. Even atn F1.4, it doesn't yield that much subject isolation via shallow depth of field on a Micro Four Thirds camera. The only real advantage I can think of is in very dark conditions, when the wide aperture will help keep the ISO numbers down. Having F1.4 gives you a lot of headroom to work with, compared to a typical F2.8 on standard zoom lenses such as Panasonic 12-35mm, or 12-60mm.
The Panasonic 12mm F1.4 lens and Lumix GH4 body were on loan from Panasonic Malaysia for review purposes only. Both the GH4 and the 12mm F1.4 lens have been returned to Panasonic at the time of writing. Neither myself nor Ming Thein are associated with Panasonic in any way, and this is an independent review. This is a user-experience based review and my approach and opinion in this article may be subjective.
Currently, the Panasonic Leica 12mm F1.4 lens is the only extra wide angle, large aperture prime lens available for Micro Four Thirds. The closest competition is the Olympus M.Zuiko 12mm F2 which lags behind by one full stop. This places the Panasonic 12mm F1.4 in a very unique position.
It is incredible how Panasonic has managed to control the size and weight (335g) of the lens. Hand-holding it on the Panasonic GH4 was comfortable and balanced. The lens construction consists of 15 elements in 12 groups, featuring 2 aspherical lenses, 1 ED lens and 2 UED lenses. The lens is weather-sealed against water splashes and dust, and the minimum focusing distance is 20cm, allowig magnification of 0.1x. The lens has dedicated aperture ring control but does not include image stabilization. For a full specification list, you can visit the official product page here.
I used the Panasonic 12mm F1.4 mainly on the Panasonic GH4 body, but some images in this review were also shot with the Olympus OM-D E-M1 Mark II. All images were post-processed with Capture One Pro. You may view the images at larger size in the online gallery here.
When I first used the Panasonic 12mm F1.4 lens, I wasn't consciously shooting for a review. Therefore, I usually shot with it stopped down to F4 or F5.6 in order to get everything in focus. I was pleased with the output from the lens but I did eventually shoot with it wide open at F1.4 to test the image quality. After all, if you are getting an F1.4 lens, you would expect to be able to use it at F1.4.
The Panasonic 12mm F1.4 is very sharp at the center of the frame, even when shooting wide open. At F1.4, the lens renders images with high level of detail and good contrast. I was repeatedly pleased by the output of the lens – both for shooting subjects up close (a few meters away from the lens) and far away.
However, sharpness is not even across the frame. Sharpness is gradually lost toward the edges. Consequently, at extreme corners of the lens, it is visibly very soft. In order to get even sharpness, you may need to stop down as far as F4 or further. Some may argue that when shooting at F1.4 (in low light conditions, or to achieve subject isolation), corner sharpness is not a priority. While I do agree to a certain extent, I had hoped that the corner performance was better, especially with the premium you pay for such a lens.
Barrel distortion is corrected automatically when shooting JPEG, and the lens profile is embedded in the RAW files and can be extracted for auto-correction (if your post-processing software allows for that). The lens and the software correction combination do a fantastic job at eliminating all traces of barrel distortion and leave only straight lines in their wake.
Chromatic aberration is an interesting topic to discuss with this lens. Obviously software correction is involved, but most of the time, the chromatic aberration is well controlled. In certain extremely complex scenes, the software correction may not successfully reduce purple fringing. For example, in very high-contrast images, the out of focus areas may exhibit severe purple fringing which are a pain to correct in post-processing.
There was this one particular image where the lens suffered purple haze at the center of the frame. I am not entirely sure why this or how this happened, but I haven't been able to replicate it since. I reshot that particular image 5 times, and the purple haze showed up in all 5 frames. I moved away from that spot and shot the same subject from a different angle and the purple haze was gone.
Panasonic GH4, F1.4, 1/3200, ISO200 – shooting at a different angle, the purple haze was gone.
Stopping down the lens to F4 or more eliminates flaws almost completely. In fact, compared to standard zoom lenses such as the Panasonic 12-35mm F2.8 lens, or the Olympus M.Zuiko 12-40mm F2.8, images from the Panasonic 12mm F1.4 have more contrast and punch in them, resulting in a livelier and more pleasing look. There is a "3-D pop" to how the lens renders images.
Flare is not a big issue with this lens, which was a surprise to me. Shooting the Panasonic 12mm F1.4 directly against strong source of light, the image appears clean of haze or ghosting. The few instances where flare occurs can be avoided by changing the angle of the shot slightly.
Autofocus is flawless on both the Panasonic and Olympus camera bodies. I managed to capture some quick action shots, which is important for me when dealing with fast moving subjects on the street. Much to my delight, I managed to capture some of my favourite shots from my recent street shooting sessions with this lens.
The Panasonic 12mm F1.4 allows close up shooting with a 20cm minimum focusing distance. The maximum magnification of 0.1x is nothing to write home about, but if used creatively you can get interesting results shooting close up with a wide angle.
The bokeh (out of focus quality) is excellent with this lens. Scrutinizing the images at various aperture openings (F1.4 to F5.6) the background blur roll-off is very smooth and soft to look at. When shooting very close to the subject, isolation can be easily achieved, and the background just melts beautifully into creaminess. The bokeh balls remain round even when the lens is stopped down.
Bokeh comparison, F1.4, F2, F2.8, F4 – To view individual full images (no crop), kindly visit the gallery here.
What started out as a lens I was reluctant to review, became one that I actually enjoyed using tremendously.
Besides being a sharp wide angle lens, there is a pleasing quality to the way this lens renders the images. There is good amount of contrast and pop, creating a 3-D look which I normally do not see from wide angle lenses. Bokeh quality is excellent and autofocus works flawlessly. Nonetheless, the Panasonic 12mm F1.4 is not without flaws – the corner softness and chromatic aberration can pose serious problems. The corner sharpness is so bad that you need to stop down to F4 for decent results. Purple fringing is noticeable in high contrast areas, and software correction cannot account for this very well.
Despite these flaws there is currently no other alternative to a wide angle F1.4 lens. There really is no benchmark to compare to. Perhaps, it is a huge challenge to create a 12mm lens with such a large aperture opening.
If you absolutely need wide angle coverage and a F1.4 aperture, then this Panasonic Leica 12mm F1.4 lens is the only option you have currently. If F1.4 is not a priority, and you can get away with F2 or F2.8, there are more budget friendly alternatives, such as Olympus M.Zuiko 12mm F2 or the vareity of standard zoom lenses that Panasonic and Olympus offer, many of which start at 12mm for the wide end of the focal range.
Hi Robin, thank you very much for a great review. Can you describe additionally your own subjective lens quality comparison (yes, about main flaws, sharpness, chromatic aberration) between Panasonic Leica 12mm f1.4 (this lens) and Panasonic Lumix G X Vario 12-35mm f/2.8 when is wide open, both at 2.8 aperture? Thank you in advance.
An alternative and probably cheaper lens is the PanaLeica 15 1.7 which produces excellent results overall.
15mm is barely wide enough. It cannot provide you with the same coverage as the 12mm. There is a huge difference in terms of field of view.
How does it compare to the voigkänder 12mm .95? I personally have the 35mm and while being soft at .95 (no free lunch) it is great at 1.4 and above. For the 12mm focal length, I prefer the Olympus one. Small light and sharp.
Hi, let's face it: I believe such an expensive lens with such purple fringing shouldn't really be sold.
It would help a lot if were kind enough to compare it with Olympus 12/2. How is it at f2 centre and edges? Is it worth paying for one stop and so on.
no more comparisons from me. Did it once, had to deal with bloodshed. People will only want to hear what they want to, no matter how fair and neutral I make the comparisons. No point to do anymore, and I sure have no time for such drama.
Not having those lenses one could at least say. If you don't mind the weight and size , if you need f1.4, if you need weather sealing whatever it means the go for Panasonic.
Great review. Not a lens that I'd have a use for, but interesting all the same.
Extra points for linking to the product specs instead of pasting them into the article.
Have you done a review on the Olympus 12mm?
Just my opinion, but mingthein.com does the most useful equipment reviews on the web. I'm much more interested in "What does this feel like?" and "How do the pictures look?" than in MTF charts and such.
I sold my copy because of the overall softness of the lens. I did a shootout been it and the Olympus 12-40 and the Olympus was clearly sharper. Disappointing that a Leica branded prime lost to a zoom, albeit a very good zoom. My findings were the same however regarding color and "pop" but I can make that happen in post. I can't make sharpness happen.
I don't find it to be sharper than the 12-40mm (center sharpness, corners the 12-40mm is clearly better even wide open), but I never did a side by side comparison. Did you use the Panasonic 12mm F1.4 on an Olympus body? Maybe the image was not optimized for Panasonic lenses, at least not as well as on a Panasonic camera.
Robin, I've found a lot of sample variance with the 12-40mm. The better ones are astoundingly sharp. Mine is like that, it puts many primes in shame, for example the 25mm f/1.8 couldn't keep up no matter the aperture. Some 12-40mm I've seen have been noticeably less sharp. So it's possible that sample variance can swing the comparison either way.
Having worked with Olympus, I have inside information on how the 12-40mm was designed and made. It was a marvel. Sample variation wise, it happens in all lenses, but then again, are we talking about people who use the 12-40mm on just Olympus bodies, or those who used it on Panasonic bodies complained that the lens being not as sharp?
At last I know what "3-D pop" means. The little seeds in the fruit bowl photo seem to be floating just slightly above the rest of the bowl's content. An illusion, certainly. But fascinating.
And, in a world awash in cat photos you've come up with one that really stands out. Possibly a Panasonic fancat. Can't think of any other way to explain that level of cooperation at such a close range.
One of my superpowers is the ability to attract stray cats and make them pose for me. Trust me, my friends who followed me shooting on the streets were all stunned by what I can do.
Jimi Hendrix had a hit with Purple Haze! But here it is a weird phenomenon. Maybe this is part of the Panasonic in-camera color processing and has nothing to do with the lens.
This was a one off thing, did not encounter it again after this one incident. But still troubling though!
It was soft in both RAW and JPEG, as I have inspected both with and without correction profiles. GH4 is not a new camera so I have full RAW support.
Hey…great review. I do agree that if you are paying that much for a lens you would expect it to be sharp in the corners wide open as well.
Btw…your article is about the Panasonic Leica 12mm f/1.4 ASPH but your link at the end of the article is for the Olympus M.Zuiko 17mm F1.2 PRO.
Thanks Don for the kind words and also spotting the mistake. It is fixed now!


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Regional Transportation Project Awarded Federal Funds
December 9th, 2018 by WCBC Radio
West Virginia Governor Jim Justice today announced that West Virginia will receive $40 million through the U.S. Department of Transportation's Better Utilizing Investment to Leverage Development (BUILD) Grants. These grants are designated by the Federal Government for use by the West Virginia Department of Transportation on two major projects: a bypass around Berkeley Springs in Morgan County, and construction of approximately 10 miles of Corridor H, a four-lane expressway in Tucker County that is part of the Appalachian Development Highway System. Each project will receive $20 million.
"This is big-time grant money coming to us for the first time in four years," Gov. Justice said. "With this $40 million, the WV Department of Transportation can make real progress on these two projects, and keep the momentum going full-steam ahead on my initiative to improve West Virginia's aging transportation infrastructure."
"My office reached out to the White House and the U.S. Dept. of Transportation several months ago and asked why West Virginia had been overlooked for this funding the past several years. We then made a strong case for funding these projects, and I could not be happier with this announcement today. All West Virginians will benefit from these projects," Gov. Justice added.
Gov. Justice is scheduled to attend a press conference on Tuesday, December 11, in Washington, D.C. to accept the grant award.
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Harvard University uncovers DNA switch that controls genes for whole-body regeneration
Sarah Knapton
14 March 2019, 2:00 pm
A piece of non-coding DNA may hold the key to how humans could regenerate body parts
Humans may one day have the ability to regrow limbs after scientists at Harvard University uncovered the DNA switch that controls genes for whole-body regeneration.
Some animals can achieve extraordinary feats of repair, such as salamanders which grow back legs, or geckos which can shed their tails to escape predators and then form new ones in just two months.
Planarian worms, jellyfish, and sea anemones go even further, actually regenerating their entire bodies after being cut in half.
Now scientists have discovered that that in worms, a section of non-coding or 'junk' DNA controls the activation of a 'master control gene' called early growth response (EGR) which acts like a power switch, turning regeneration on or off.
"We were able to decrease the activity of this gene and we found that if you don't have EGR, nothing happens," said Dr Mansi Srivastava, Assistant Professor of Organismic and Evolutionary Biology at Harvard University.
Jellyfish have extraordinary powers of regeneration Credit: REX/Shutterstock
"The animals just can't regenerate. All those downstream genes won't turn on, so the other switches don't work, and the whole house goes dark, basically."
The studies were done in three-banded panther worms. Scientists found that during regeneration the tightly-packed DNA in their cells, starts to unfold, allowing new areas to activate.
But crucially humans also carry EGR, and produce it when cells are stressed and in need of repair, yet it does not seem to trigger large scale regeneration.
Scientists now think that it master gene is wired differently in humans to animals and are now trying to find a way to tweak its circuitry to reap its regenerative benefits.
Post doctoral student Andrew Gehrke of Harvard believes the answer lies in the area of non-coding DNA controlling the gene. Non-coding or junk DNA was once believed to do nothing, but in recent years scientists have realised is having a major impact.
"Only about two percent of the genome makes things like proteins," added Mr Gehrke said. "We wanted to know: What is the other 98 percent of the genome doing during whole-body regeneration?
"I think we've only just scratched the surface. We've looked at some of these switches, but there's a whole other aspect of how the genome is interacting on a larger scale, and all of that is important for turning genes on and off."
Marine animals, such as the moon jellyfish, are masters of regeneration and some have been found to clone themselves after death.
In 2016, a Japanese scientist reported that three months after the death of his pet jellyfish, a sea anemone-like polyp rose out of the degraded body, and then astonishingly aged backwards, reverting to a younger state.
In the 1990s, scientists in Italy discovered that the Turritopsis dohrnii jellyfish switches back and forth from being a baby to an adult, resulting in its nickname, the immortal jellyfish.
Dr Srivastava added: "The question is: If humans can turn on EGR, and not only turn it on, but do it when our cells are injured, why can't we regenerate?" added Dr Srivastava.
"It's a very natural question to look at the natural world and think, if a gecko can do this why can't I?
"The answer may be that if EGR is the power switch, we think the wiring is different. What EGR is talking to in human cells may be different than what it is talking to in the three-banded panther worm."
The research was published in the journal Science.
Sign up for your essential, twice-daily briefing from The Telegraph with our free Front Page newsletter.
US drops charges against Chinese-born MIT professor
The US Justice Department dismissed criminal charges on Thursday against a Chinese-born professor at the Massachusetts Institute of Technology (MIT) who had been accused of failing to disclose his ties with China.
Afghan NGO women 'threatened with shooting' for not wearing burqa
The Taliban's religious police have threatened to shoot women NGO workers in a northwestern province of Afghanistan if they do not wear the all-covering burqa, two staff members told AFP.
The cost of US sanctions for ordinary Zimbabweans
After violent elections in Zimbabwe 20 years ago, the United States and the European Union led mostly Western nations in imposing travel bans and freezing the assets of top officials. But their impact is much more far-reaching, hamstringing the efforts of ordinary people to rebuild their country.
With fish and turtles swimming around them, divers performed an underwater lion dance in a Malaysian aquarium on Friday, in a fresh take on the traditional Lunar New Year performance.
In Lima, infirm get Covid jabs at home as Peru's cases surge
As night falls over a dusty neighborhood in Lima, a team of health workers hustle from home to home to vaccinate the old and infirm as a third coronavirus wave sweeps over Peru, the world's hardest-hit country per capita.
China warns of 'no mercy' in corruption and monopoly crackdown
China has vowed to ramp up its regulatory crackdown and show "no mercy" against corruption as the ruling Communist Party gears up for a key meeting that could secure President Xi Jinping a third term.


A studio suite furnished to accommodate AirBnB guests... It's a compact space (370sqft) which was carefully planned out to allow a kitchenette, a bathroom, sufficient storage, a designated eating and lounge area aside from the queen size bed... The natural light in the space allows for a sense of spaciousness which really helps enlarge this otherwise small room.


Jim is trying to add records from the ORDER_DETAILS table to ORDER_DETAIL_HISTORY for orders placed before the current year. Which insert statement would accomplish his task?
When inserting from another table using a subquery, the VALUES clause should not be included. Options B and C are invalid syntaxes for the INSERT statement.
Which of the following statements will not implicitly begin a transaction?
None of the above; they all implicitly begin a transaction, if not started already.
If a transaction is not currently open, any INSERT, UPDATE, MERGE, DELETE, SELECT FOR UPDATE, or LOCK statement will implicitly begin a transaction.
Option A will error out because when using columns in set, a subquery must be used as in option C. Option D is wrong because AND is used instead of a comma to separate columns in the SET clause.
COMMIT, ROLLBACK, and any DDL statement end a transaction—DDL is automatically committed. INSERT, UPDATE, and DELETE statements require a commit or rollback.
Sara wants to update the SALARY column in the OLD_EMPLOYEES table with the value from the EMPLOYEES table for employees in department 90. Which SQL will accomplish the task?
Option A uses a correlated subquery to match the correct employee. Option B selects all the rows in the subquery and hence will generate an error. Option C is not valid syntax. Option D will update all the rows in the table since the UPDATE statement does not have a WHERE clause. The WHERE clause preset belongs to the subquery.


text:
Home NEWS Man defiles 3-yr-old daughter, attempts to sodomise sons
Man defiles 3-yr-old daughter, attempts to sodomise sons
FaithAdama February 06, 2018 NEWS,
A seven-year-old boy yesterday accused his father of sexually abusing his three-year-old sister and attempting to sodomize him and his five-year-old brother.
The boy said his father not only abused his sister five times but also attempted to sodomise him and his five-year-old brother, but they refused because the pain was too much.
In a detailed account of his ordeal he said: "My daddy slept with Favour from here (pointing at the private part of his sister.) He put her on the ground and then he did it. It was not once, it was five times. "He wanted to do my own from the back but I refused. He wanted to do Godspower too. When we refused, he started beating us."
Lagos state Commissioner of Police, Edgal Imohimi, said he ordered the arrest of Olusegun Adefemi after he got wind if how he defiled his daughter and attempted to sodomise his two sons. Parading the suspect, the CP said he was arrested at No. 6 Ipakan Street, Ijede, after an official of Lagos Neighbourhood Safety Corps (LNSC), Adekoya Sesan, reported the incident.
The police boss said Adefemi had unsupervised access to his kids as he was separated from his wife over alleged spousal abuse. Imohimi said: "He inflicted grievous injury in the private part of the child as a result of forceful penetration.
Two older siblings of the survivor were not as lucky as Olusegun Adefemi regularly abused them by beating them with cane each time they resisted him from penetrating them through their anus.
"The girl has been taken to Mirabel Medical Centre for examination and treatment while her siblings have been placed in temporary home. The suspect would be charged to court at the end of investigation." However, the suspect who denied the allegations and insisted that he was innocent, said he was shocked his kids could accuse him of wrongdoing.
He said, "I know I usually beat my kids when they do wrong. I do not think that is an offence because I would not want my children to grow up badly.
"Their mother left over a year ago and since then, I have been with them. I do bricklaying job sometimes, other times, I work as a conductor to provide our daily bread."
By FaithAdama at February 06, 2018


"It all started with the fact that our old friend turned to us and asked us to make him an apartment," says the architect. Julia Vishnepolskaya. - He bought it for himself, and he needed an unusual, bright interior for rest. Where after work you can escape from the hustle and bustle, relax, gain strength. He didn't limit us in anything and provided complete freedom, specifying only the main points: free planning, large bathroom with natural light. In general, everything. The rest - do what you want, your song. "
Andrey Kartsev: The apartment was a square, inscribed in a circle, with two short balconies. And when we started to design, all the time we were faced with a lack of something: there was not enough space, then there was no place to put the kitchen, you could not make the bathroom light, it turned out to be boring. We worked on various options until we came up with the central part - a kind of core - in the form of an egg. Around him, fanlikely arranged the premises, attached balconies and made a complete glazing instead of windows. So all at once there was a place. Directly from the entrance opens a wedge-shaped living room space with a home cinema, dining room and kitchen. Where there used to be a large balcony, a kitchen was equipped, and a bar counter was attached to the supporting column, which could not be removed, where the owner could have breakfast, drink tea or coffee. Further from the dining room through the office you can go into a spacious bedroom with a bathroom. From the bedroom there is also an exit to the living room, to the home cinema area. Thus, the rooms are interconnected - this is, you see, very convenient.
The cinema area deserves special attention, as it is located in the central part. The floor and ceiling here repeat the shape of an egg, but they are trimmed with different materials. There is a leather tile on the floor, and a round ceiling lamp imitating the yolk is decorated with aged gold. The shape of the egg is not only repeated in the plan, but also recreated in volume. In two places, the "oval" seems to be wedged into vertical planes, forming a concave oval niche and a wall in which there is a door leading to the master bedroom.
Вообще, яйцо по своей форме унandкально. Оно не andмеет радandуса - у каждой частand он свой. Чтобы повторandть его в andнтерьере, мы сделалand трехмерную модель and через каждые 40 см давалand строandтелям новые размеры. И нашлand спецandальную технологandю, которая позволяет создавать в пространстве любые сложные объемы.
Julia Vishnepolskaya: This apartment is heavily a game. For example, a closet-door between the office and the bedroom. And from the side of the bedroom, and from the side of the office, it looks like a regular built-in wardrobe. And no one guesses about his second function. If you press the button, a hidden door will open. In general, fun. And another customer's favorite toy is a curtain in a home theater. The bearing pylon in this zone could not be removed. At first we wanted to rock him, but then we realized that it was too much. And they decided to just drape a cloth that leaves because of it and moves in a circle. If one of the friends stays overnight, the curtain will completely hide the sofa group, forming a guest mini-room. In this case, you can go into the kitchen or leave the house without disturbing the guest. One or two people live in this apartment just fine. When she was done, she walked easily and pleased everyone. Pleased with the owner, the builders were proud of her. We were especially pleased.
Julia Vishnepolskaya: "This apartment was conceived from the very beginning as a place for rest and relaxation. The customer works a lot, so he dreamed of an interior that was radically different from those of standard office spaces where he spends most of his time. We came up with a little fabulous and cheerful for him a house with lots of fun stuff "


NBA Australia – Stop By Our Site Today To Locate Extra Info..
Purchasing an NBA jersey online in Australia for the first time can be a mine field for the new online shopper. The truth is, with a bit of knowledge, buying your next NBA jersey online from Australia is quick and easy, but there are some 'rules' that you should follow to ensure you are receiving the best bargain. Listed here are 3 top tips for purchasing nba store.
Check Around – The shopping window that has become the net gets better each day, and internet based stores are putting great effort on 'pretty on the eye' websites. This can be all good and well, but they are they offering you the greatest deal? You can answer this question through making sure you check around. This is no different to looking around at different shops or supermarkets, it's just online and way easier! When purchasing an NBA jersey online around australia don't automatically assume the official NBA website, or official team page are able to offer the best deal. There are lots of online retailers who sell NBA jerseys at different prices, so take advantage of the competition and seek the best offer.
b) what the expenses are – You could see that a particular retailer doesn't satisfy either or both so that you should start working on another retailer.
Look for a Returns Policy – Specifically when buying a product of apparel including nba store australia, there's nothing worse than receiving it only to have to return it as it is a bad size. Although returning a product may be straight forward, it is more the hassle (and extra wait) that is the problem. Although this ought to be a given, do ensure that a solid returns policy is within place, in particular what, if any costs (for instance, the postage cost that you should send the product back) you will need to bear.
A great way of avoiding the chance of this really is to look for the sizing chart for each NBA jersey you purchase. Most good internet retailers will incorporate a sizing chart for many different items and manufacturers. It is within their welfare to do this also, as they would like to avoid a returns process around you do!
So there you might have it. 3 top tips for buying an NBA jersey online within australia. I am just a massive NBA fan located in Australia, and have been buying NBA merchandise online for a long time, having had both negative and positive experiences in the process. However, one site has continuously stood out from the rest. Pro Sports Gear has been a store I actually have, of late, made many purchases from. In particular their freight costs to Australia are first rate, and this is just what tips the scales inside their favour over others.
Hopefully these 3 tips have helped you will make the next nba jerseys sydney easier, look for much more about our look for NBA and NFL merchandise here. Also, fabrics of each and every team are certainly not exactly the same which may be pytcff into three categories. For instance: the mesh fabric of Wizards, the mercerized cotton fabric of 76ers and the homemade mesh of Lakers. All of the names and numbers of players are embroidered, while different colors apply different fabrics for layering embroidery.
The jersey is not only the outfit for that basketball player, but in addition manifests a fashion, an attitude towards life and even the lifestyle which transmits unique charm among fans. In the usa, the NBA jersey culture is rich: The yellow on the Lakers and green on the Celtics are classic this year. Wearing NBA jerseys has been liked by street basketball players to win support from the audience using their dazzling skills.
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text:
\section{Introduction}
At the end of the last century,
the astronomical observation of
high redshift type Ia supernovae (SNeIa)
indicated that our universe is not only expanding,
but also accelerating,
which conflicts with our deepest intuition of gravity.
Current observations,
such as cosmic microwave background (CMB),
baryon acoustic oscillations (BAO)
and large scale structure (LSS),
converge on the fact of accelerating expansion.
In order to make reasonable sense of this acceleration,
an exotic component of the universe,
the mysterious dark energy (DE),
has been introduced.
Although many efforts have been made,
the identity and physical nature of DE
still seem to evade disclosure.
Besides seeing DE as a real content of our universe,
one possible way to address the problem
is to modify gravitation theory
such that the acceleration could be attributed to this modification
(for review, see, e.g., \cite{Capozziello2011}).

One of the extensively studied modified gravities is the $f(R)$ gravity,
in which one starts from the standard General relativity (GR),
and extends the standard Hilbert-Einstein action to
an arbitrary function of the Ricci scalar $R$\cite{Sotiriou2010,DeFelice2010,Nojiri2011}.
A further extension of $f(R)$ gravity proposed in \cite{Nojiri2004,Allemandi2005} and then studied in \cite{Bertolami2007,Harko2008,Harko2010,Bertolami2010} is to consider the nonminimal coupling
between matter and gravity,
i.e. the $f(R,\mathcal{L}_\text{m})$ gravity,
where $\mathcal{L}_\text{m}$ is the Lagrangian density of matter.
On the other hand,
one can also modify the gravitation theory
starting from the Teleparallel Equivalent of General Relativity (TEGR)
\cite{Einstein1928,Hayashi1979,aldrovandi2012teleparallel,Maluf2013}.
In the Lagrangian of TEGR,
the torsion scalar $T$ takes the place of the Ricci scalar $R$,
and hence in analogous to $f(R)$,
$f(T)$\cite{Bengochea2009,Linder2010,Cai2016}
and nonminimal coupling $f(T,\mathcal{L}_\text{m})$ gravities
\cite{Harko2014a,Feng2015}
have been studied.
Despite the equivalence between TEGR and GR,
$f(T)$ gravities are different from $f(R)$ gravities.
One of the important advantages of $f(T)$ gravities
is that the field equations are second order instead of fourth order.
It is also noticed that
non-trivial $f(T)$ gravities violate
the Lorentz invariance\cite{Li2011,Sotiriou2011,Bahamonde2015} and
particular choices of tetrad are important
to get viable models\cite{Tamanini2012}.

Concerning large scale evolution of the universe
and the linear perturbations of the background,
$f(T)$ gravities have been compared with the cosmological observation
data including CMB, BAO and SNeIa
\cite{Bengochea2009,Feng2015,Nunes2016}.
While the SNeIa data capture the late time accelerating behavior
(redshift $z<3$),
and the data of BAO and inhomogeneity of CMB
provide mostly the imprints of
the early development and linear perturbations of the background
before recombination ($z>1000\sim1500$),
most structures such as stars, galaxies and clusters of galaxies
are formed from the non-linear evolution of perturbations
during the post-recombination epoch,
which is usually referred as
the Dark Ages ($10<z<1000$).
However, a fully relativistic treat of this
non-linear perturbation is not currently available.
Thus it is usually handled by $N$-body simulation
(see e.g. \cite{Maccio2004,Aghanim2009,Baldi2010,Li2011a}),
which can be cumbersome and time-consuming,
and is not practical for one to use to study different gravitation models.
On the other hand,
there has been intermediate approximations to
the full-fledged theory before turning to simulation,
one of which is spherical collapse model
\cite{Gunn1972,Padmanabhan1993}.
In this simple semi-analytic model,
a spherical overdense region evolves with the expanding background universe,
and slows down and turns from expanding to collapsing.
As a simple but fundamental tool to describe
the growth of gravitationally bounded systems,
this model has been used in various studies of gravitation theories
in recent years
\cite{Mota2004,Maor2005,Nunes2006,Basilakos2009,Basilakos2010,Brax2010,Fernandes2012,Bellini2012,Li2014,Carames2014}.
The model has also been compared with the pseudo-Newtonian approach\cite{Abramo2007,Abramo2009}
and it is found that the two approximation schemes convey
identical equations for the density contrast.

After the turning around from expanding to collapsing,
the overdense region shall virialize and be prevented from
falling into a singularity.
For gravitationally bounded systems,
virialization is also a powerful approach
with a long history.
In fact,
the discrepancy between the virial mass $M_\text{vir}$
and the total baryonic mass $M_\text{b}$ of a cluster
contributed to the awareness of the existence of dark matter.
However, the virial theorem depends on the gravitation theory,
and hence the corresponding theorems in different modified gravities
have drawn a lot of attention lately
\cite{Bohmer2008,Sefiedgar2009,Capozziello2013,Milgrom2014,Santos2015,Javadinezhad2016}.
In the context of spherical collapse,
virialization provides a more realistic picture
of the collapsing structures,
and enable ones to calculate the main features of them
(collapse factor, virial density, virial mass, etc.),
which may be useful in further analytic investigation
or numerical simulation
(e.g. NFW profile\cite{Navarro1997} to describe the $N$-body simulation).

In this paper,
we look into the collapse of a spherically symmetric perturbation
for models in $f(T)$ gravities
with a classical top-hat profile,
including both minimal and nonminimal matter-gravity coupling cases.
Moreover, we consider the virialization of the collapse
after the turn-around point.
The paper is organized as follows:
in Section \ref{review},
we briefly review the bases and cosmologically tested models
of the $f(T)$ gravities,
including both minimal and nonminimal matter-gravity coupling cases.
In Sec.\ref{collapse} , we consider the spherical top-hat collapse
and evolution of perturbation in these models.
We study the virialization of the collapse in Sec.\ref{virial} .
Sec.\ref{conclusion} contains our conclusions and discussions.

We are going to use the Latin letters
$(a,b,c,\cdots=0,1,2,3)$
to denote the tangent space indices,
and Greek letters
$(\mu,\nu,\rho,\cdots=0,1,2,3)$
to denote the spacetime indices.
We assume the Lorentz metric of Minkowski spacetime
\begin{equation}
	\eta=\eta_{ab}\diff x^a\otimes\diff x^b
	\label{eta}
\end{equation}
has the form
$\eta_{ab}=\text{diag}(+1,-1,-1,-1)$.
And we use the unit
$c=1$
throughout the paper.

\section{From TEGR to $f(T)$ models}
\label{review}
\subsection{The field equations}
In the torsional formulations of gravity,
one uses tetrad fields $\{e_a,e^a\}$
as the fundamental dynamical variables.
The tetrad fields form an orthonormal base
of the tangent space $T_p\mathcal{M}$ at each point $p$
on the spacetime differentiable manifold $\mathcal{M}$.
The spacetime metric $g$
\begin{equation}
	g=g_{\mu\nu}\diff x^\mu\otimes\diff x^\nu
	\label{metricg}
\end{equation}
is related to the tangent space metric $\eta$ by
\begin{equation}
	\eta_{ab}=g(e_a,e_b)=g_{\mu\nu}e_a^{\:\mu}e_b^{\:\nu},
	\label{metrictrans}
\end{equation}
or conversely,
\begin{equation}
	g_{\mu\nu}=\eta_{ab}e^a_{\:\mu}e^b_{\:\nu}.
	\label{metrictrans1}
\end{equation}
And hence the determinant
\begin{equation}
	|e|\equiv\text{det}(e^a_{\:\mu})=\sqrt{-g}.
	\label{metricdet}
\end{equation}
One then can use the tetrad field to define
the curvatureless Weitzenb{\"o}ck connection\cite{Weitzenbock1923}
\begin{equation}
	\tilde{\Gamma}_{\nu\mu}^{\lambda}\equiv e_a^{\:\lambda}\partial_\mu e_{\:\nu}^a=-e_{\:\nu}^a\partial_\mu e_a^{\:\lambda}
	\label{connection}
\end{equation}
instead of the torsionless Levi-Civi{\'a} one.
The torsion and contorsion tensors are then given by
\begin{equation}
	T_{\:\:\mu\nu}^\lambda\equiv\tilde{\Gamma}_{\nu\mu}^\lambda-\tilde{\Gamma}_{\mu\nu}^\lambda=e_i^\lambda(\partial_\mu e_\nu^i-\partial_\nu e_\mu^i),
	\label{torsiontensor}
\end{equation}
and
\begin{equation}
	K^{\mu\nu}_{\quad\rho}\equiv-\frac12\left(T^{\mu\nu}_{\quad\rho}-T^{\nu\mu}_{\quad\rho}-T_{\rho}^{\:\mu\nu}\right),
	\label{contorsion}
\end{equation}
respectively.
Utilizing the tensor
\begin{equation}
	S_\rho^{\:\mu\nu}\equiv\frac12\left(K^{\mu\nu}_{\quad\rho}+\delta_\rho^\mu T^{\lambda\nu}_{\quad\lambda}-\delta_\rho^\nu T^{\lambda\mu}_{\quad\lambda}\right),
	\label{auxtensor}
\end{equation}
one can define the torsion scalar
\begin{equation}
	T\equiv T^\rho_{\:\mu\nu}S_\rho^{\:\mu\nu}.
	\label{torsionscalar}
\end{equation}
TEGR\cite{Hayashi1979,aldrovandi2012teleparallel,Maluf2013} uses this scalar $T$ as the gravitation Lagrangian density.
And the minimal matter-gravity coupling $f(T)$ gravity
extends it to an arbitrary function of $T$.
The nonminimal coupling $f(T)$ gravity\cite{Harko2014a}
further extends the matter Lagrangian term $\mathcal{L}_\text{m}$
into $(1+f_2(T))\mathcal{L}_\text{m}$.
To be unifiable, we write the action in the following form:
\begin{equation}
	S=-\frac1{16\pi G}\int|e|\left( 1+f_1(T) \right)T\diff^4x+\int|e|\left( 1+f_2(T) \right)\mathcal{L}_\text{m}\diff^4x.
	\label{actionnonmin}
\end{equation}
And the actions of TEGR and minimal coupling $f(T)$ gravity correspond to the
$f_1,f_2=0$ and $f_2=0$ cases of Eq.\eqref{actionnonmin}, respectively.
With the action principle applied on Eq.\eqref{actionnonmin}
with respect to the tetrad field,
the field equation is then given by
\begin{equation}
		\frac4{|e|}f\partial_\beta(|e|S_\sigma^{\:\:\alpha\beta}e_a^{\:\sigma})+4e_a^{\:\sigma}S_\sigma^{\:\:\alpha\beta}\partial_\beta f+4fS_\rho^{\:\:\alpha\sigma}T^\rho_{\:\:\sigma\beta}e_a^{\:\beta}+(1+f_1)Te_a^{\:\alpha}=-16\pi G(1+f_2)\mathcal{T}_\beta^{\:\alpha}e_a^{\:\beta},
	\label{eom}
\end{equation}
where $f\equiv1+f_1(T)+f_1'(T)T-16\pi Gf_2'(T)\mathcal{L}_\text{m}$, and $\mathcal{T}_\beta^{\:\alpha}$
is the energy-momentum tensor of matter given by
\begin{equation}
	\frac{\delta(|e|\mathcal{L}_\text{m})}{\delta e^a_{\:\alpha}}=-|e|\mathcal{T}_\beta^{\:\alpha}e_a^{\:\beta}.
	\label{emtensor}
\end{equation}
And it takes the usual form for perfect fluid
\begin{equation}
	\mathcal{T}_{\mu\nu}=pg_{\mu\nu}-(\rho+p)u_\mu u_\nu,
	\label{emtensor1}
\end{equation}
where $p$ and $\rho$ are the pressure and energy density of the matter, respectively,
and $u^\mu$ is the 4-velocity.

The covariant derivative (related to the Levi-Civit{\'a} connection) of Eq.\eqref{eom} gives
\begin{equation}
	\nabla^\nu\mathcal{T}_{\mu\nu}=-\frac{f_2'(T)\nabla^\nu T}{1+f_2(T)}(\mathcal{T}_{\mu\nu}+g_{\mu\nu}\mathcal{L}_\text{m}).
	\label{covder}
\end{equation}
This suggests that the energy-momentum tensor is no longer conservative.
However,
contracting Eq.\eqref{covder} with $u^\mu$, we have
\begin{equation}
	\begin{split}
		u^\mu\nabla^\nu\mathcal{T}_{\mu\nu}=&\frac{f_2'(T)\nabla^\nu T}{1+f_2(T)}(\rho-\mathcal{L}_\text{m})\\
		=&-u^\mu\nabla_\mu\rho-(\rho+p)\nabla_\mu u^\mu.
	\end{split}
	\label{mattere}
\end{equation}
If we take the matter Lagrangian density to be
$\mathcal{L}_\text{m}=\rho$\cite{Gron2007,Bertolami2008,Minazzoli2012,Harko2014},
then in cosmological cases,
as discussed in Ref.\cite{Feng2015},
Eq.\eqref{mattere} will return to the usual form of conservation law of matter in
Friedmann-Lema{\^i}tre-Robertson-Walker (FLRW) metric.

\subsection{Observationally tested models}
Consider a flat FLRW universe with metric in Cartesian coordinates
\begin{equation}
	g_{\mu\nu}=\text{diag}(1,-a^2(t),-a^2(t),-a^2(t)),
	\label{FRWmetric}
\end{equation}
with scale factor $a(t)$.
It is found\cite{Tamanini2012} that for this form of metric,
the diagonal vierbein $e^a_{\:\mu}=\text{diag}(1,a(t),a(t),a(t))$
is a viable choice for $f(T)$ gravities.
And then the torsion scalar $T=-6H^2$,
where $H=\dot{a}/a$ is the Hubble parameter,
and the overdot denotes derivative with respect to time.
The 00 entry of Eq.\eqref{eom} then reads
\begin{equation}
	12fH^2-6\left( 1+f_2 \right)H^2=16\pi G\left( 1+f_2 \right)\rho.
	\label{coseom}
\end{equation}
When $f_1,f_2=0$, i.e. $f=1$,
Eq.\eqref{coseom} gives the usual Friedmann's equation in GR or TEGR,
and when $f_2=0$, Eq.\eqref{coseom} gives the field equation of minimal coupling $f(T)$ gravities.

For another equation to determine the system,
one can either use the rest components of Eq.\eqref{eom} or
the evolution of matter.
Here we take the latter scheme.
From Eq.\eqref{mattere},
if we take $\mathcal{L}_\text{m}=\rho$
and assume the matter is dust-like $p\ll\rho$,
we can have the familiar evolution of matter $\rho=\rho_0 (a_0/a)^{3}$,
where $\rho_0$ and $a_0$ are the energy density of matter and
scale factor at present time, respectively.
Usually $a_0$ is set to be 1.

In Ref.\cite{Feng2015},
we have constructed two concrete models of
nonminimal coupling $f(T)$ gravities
for cosmological fitting.
For completeness,
here we consider one additional model
of minimal coupling $f(T)$ gravity.
They are listed as follows:
\begin{itemize}
	\item Model I: $f_1=\frac{12BH_0^4}{T^2}$, $f_2=0$;
	\item Model II: $f_1=H_0(-T)^{-\frac12}$, $f_2=\frac{-2AH_0^2}{\Omega_\text{m0}T}$;
	\item Model III: $f_1=\frac{12BH_0^4}{T^2}$,  $f_2=\frac{-2AH_0^2}{\Omega_\text{m0}T}$,
\end{itemize}
where $A,B$ are the parameters of the models,
$H_0$ is the Hubble parameter at present time and
$\Omega_\text{m0}=\frac{8\pi G\rho_0}{3H_0^2}$ is the matter density parameter.
Model I represents the case of minimal coupling $f(T)$ gravity,
while Model II and III are the models of nonminimal coupling $f(T)$ gravity
constructed and fitted in Ref.\cite{Feng2015}.
Then Eq.\eqref{coseom} can be unifiably written as
\begin{equation}
	\left( \frac{\dot a}a \right)^2=\Omega_\text{m0}H_0^2a^{-3}+\frac{\left( B+Aa^{-3} \right)H_0^4}{\left( \frac{\dot a}a \right)^2}.
	\label{flatunieom}
\end{equation}
Denoting $E=H/H_0$, we have
\begin{equation}
	E^2=\Omega_\text{m0}a^{-3}+Aa^{-3}E^{-2}+BE^{-2}
	\label{unieom}
\end{equation}
with $1=\Omega_\text{m0}+A+B$.
Model I, II, III correspond to the cases
$A=0$, $B=0$ and $A,B\ne0$, respectively.

We use the data set of SNeIa, BAO and CMB,
the same as Ref.\cite{Feng2015},
to find the best-fit values of parameters for Model I,
and retain the fitting results of Model II and III,
listed in Table \ref{bestfit}.

\begin{table}[htbp]
  \centering
  \caption{Best-fit parameters for the models}
    \begin{tabular}{cccc}
    \hline
    \hline
          & \multicolumn{3}{c}{models} \\
\cline{2-4}    parameters & Model I & Model II & Model III \\
    \hline
    $\Omega_\text{m0}$   & $0.274\pm0.008$ & $0.367\pm0.011$ & $0.302\pm0.011$ \\
    $H_0$    & $73.73\pm0.79$ & $60.97\pm0.44$ & $68.54\pm1.27$ \\
    $A$   &   -    &   $0.633\pm0.011$    & $0.188\pm0.048$ \\
    $\chi_\text{min}^2/\text{d.o.f.}$     & 707.455/739 & 729.429/739 & 683.846/739 \\
    \hline
    \hline
    \end{tabular
  \label{bestfit
\end{table

\section{Spherical top-hat collapse}
\label{collapse}
The classical spherical top-hat collapsing formalism
considers a spherical region with uniformly perturbed energy density
immersed in the homogeneous universe.
The initial magnitude of the perturbation is
denoted as $\delta_\text{i}$,
and it occurs at the redshift $z_\text{i}$,
where the subscript "i" hereinafter indicates
the initial evaluation of the quantities at this very moment.
The initial radius of the overdense region
and the density of the universe are denoted as
$R_\text{i}$ and $\rho_\text{i}$, respectively.
Thus the initial density of the overdense region is $\rho_\text{i}(1+\delta_\text{i})$
and the scale factor at that time is $a_\text{i}=1/(1+z_\text{i})$.

This region then detaches from the rest of the universe
and evolves on its own like a non-spatial-flat universe
\cite{Gunn1972,Padmanabhan1993,Mota2004,Abramo2009}.
For this reason,
we need the equation of a spatial curved universe
besides the flat background evolution.
For a universe with spatial curvature $k$,
the torsional formalism gives the torsion scalar\cite{Tamanini2012}
\begin{equation}
	T=-6H^2+\frac{6k}{a^2}.
	\label{kT}
\end{equation}
And the 00 entry of Eq.\eqref{eom} is
\begin{equation}
	\left( 2f-1-f_1 \right)\left( 6H^2-\frac{6k}{a^2} \right)=16\pi G\left( 1+f_2 \right)\rho.
	\label{curvcoseom}
\end{equation}
When $k=0$, Eq.\eqref{coseom} is recovered.
For the three models listed above,
Eq.\eqref{curvcoseom} is then
\begin{equation}
	\left( \frac{\dot a}a \right)^2-\frac{k}{a^2}=\Omega_\text{m0}H_0^2a^{-3}+\frac{\left( B+Aa^{-3} \right)H_0^4}{\left( \frac{\dot a}a \right)^2-\frac{k}{a^2}}.
	\label{unieom0}
\end{equation}
Denoting $H_\text{i}=H(a_\text{i})$,
$\tilde k=\frac{k}{a_\text{i}^2H_\text{i}^2}$,
$\Omega_\text{mi}=\frac{8\pi G\rho_0}{3H_\text{i}^2a_\text{i}^3}$,
$\tilde A=A\frac{H_0^4}{a_\text{i}^{3}H_\text{i}^{4}}$ and
$\tilde B=B\frac{H_0^4}{H_\text{i}^{4}}$, we have
\begin{equation}
	\left(\frac{\dot a}{H_\text{i}a_\text{i}}\right)^2-\tilde k=\Omega_\text{mi}\frac{a_\text{i}}{a}+\frac{\tilde A\left( \frac{a}{a_\text{i}} \right)+\tilde B\left( \frac{a}{a_\text{i}} \right)^4}{\left(\frac{\dot a}{H_\text{i}a_\text{i}}\right)^2-\tilde k}.
	\label{unieom1}
\end{equation}
This is the equation governing the scale factor $a$
in a spatial curved universe.
Therefore the equation for the radius $R$ of the overdense region is in the similar form,
\begin{equation}
	\left(\frac{\dot R}{h_\text{i}R_\text{i}}\right)^2-\tilde k=\Omega_\text{mi}\left( 1+\delta_\text{i} \right)\frac{R_\text{i}}{R}+\frac{\tilde A\left( \frac{R}{R_\text{i}} \right)+\tilde B\left( \frac{R}{R_\text{i}} \right)^4}{\left(\frac{\dot R}{h_\text{i}R_\text{i}}\right)^2-\tilde k},
	\label{reom}
\end{equation}
with
\begin{equation}
	1-\tilde k=\Omega_\text{mi}\left( 1+\delta_\text{i} \right)+\frac{\tilde A+\tilde B}{1-\tilde k},
	\label{rnorm}
\end{equation}
where $h=\dot R/R$ is the expansion rate of the region
and initially $h_\text{i}=H_\text{i}$.

As the evolution continues,
the region may stop expanding and start collapsing due to the overdensity.
At the turn-around point,
if it ever occurs,
the radius of the region reaches its maximum $R_\text{max}$
and $\dot R=0$.
Denoting $\beta\equiv R_\text{max}/R_\text{i}$,
we can rewrite Eq.\eqref{reom} at the turn-around point as
\begin{equation}
	\tilde B\beta^5+\tilde A\beta^2-\tilde k^2\beta-\tilde k\Omega_\text{mi}(1+\delta_\text{i})=0.
	\label{quintic}
\end{equation}
It is a quintic equation of $\beta$.
The region will turn from expanding to collapsing
if only Eq.\eqref{quintic} has real positive root(s).
According to the Passare-Tsikh solution\cite{Passare2004}
of the principal quintic
\begin{equation}
	m x^5+n x^2+x+1=0,
	\label{pquintic}
\end{equation}
Eq.\eqref{quintic} has real positive root(s) if and only if (See Appendix \ref{appendix})
\begin{equation}
	3125|m|^2-256|m|+108|n|^5-27|n|^4+625|m||n|-2250|n|^2|m|<0
	\label{condition}
\end{equation}
where
\begin{equation}
	m=-\frac{\tilde B\Omega_\text{mi}^4(1+\delta_\text{i})^4}{\tilde k^6},\quad n=-\frac{\tilde A\Omega_\text{mi}(1+\delta_\text{i})}{\tilde k^3}.
	\label{mn}
\end{equation}
For Model I ($A=0$),
the quadratic term of Eq.\eqref{pquintic} vanishes,
while the discriminant \eqref{condition} is still valid
and reduces to
$3125|m|-256<0$, namely
\begin{equation}
	\frac{\left( 1+z_\text{i} \right)^{12}\left( 1+\delta_\text{i} \right)^{3}}{H_\text{i}^{12}\tilde k^6}<\frac{256}{3125 BG^4H_0^{12}\Omega_\text{m0}^4}.
	\label{disI}
\end{equation}
For Model II ($B=0$),
the quintic term of Eq.\eqref{pquintic} vanishes
and the equation reduces to a quadratic one.
And Eq.\eqref{condition} gives the same inequality
as the discriminant of the quadratic:
$4|n|-1<0$, namely
\begin{equation}
	-\frac{\left( 1+z_\text i \right)^3\left( 1+\delta_\text i \right)}{H_\text i^2\tilde k^3}<\frac1{4A\Omega_\text{m0}H_0^2}.
	\label{disII}
\end{equation}
For Model III ($A,B\ne0$),
similar inequality can be obtained,
which is omitted here for its lengthiness.
In Eqs.\eqref{disI}, \eqref{disII} and the corresponding inequality for Model III,
$H_\text{i}$ and $\tilde k$ depend on $z_\text{i}$ and $\delta_\text{i}$
according to Eqs.\eqref{unieom} and \eqref{rnorm}, respectively.
And thus for given $A$ and $B$,
these inequalities give constraints on the time ($z_\text{i}$)
and magnitude ($\delta_\text{i}$)
of the initial perturbation.
For the three models listed above,
we have plotted these constraints in Fig.\ref{tacon},
where the models have taken the best-fit parameters listed in Table \ref{bestfit}.
Any pairs of $\left( z_\text{i},\delta_\text{i} \right)$ above
the illustrated lines can guarantee real positive root(s)
of Eq.\eqref{quintic},
namely make sure that the overdense region will
eventually collapse and form structure.
The result is not surprising in that
a perturbation that either is too weak (low $\delta_\text{i}$)
or occurs too late (low $z_\text{i}$,
and such that the matter of the universe is too thin)
will not be able to provide a self-gravity strong enough
to slow down the expanding and turn the region into collapsing.
Compared to the minimal coupling Model I,
the constraint for Model II is more stringent,
while the one for Model III is slightly looser.

\begin{figure}[!htp]
	\centering
	\includegraphics[width=0.9\textwidth]{ta.eps}
	\caption{The constraints of $z_\text{i}$ and $\delta_\text{i}$
for Model I(dashed), II(dashdot) and III(solid),
where the models have taken the best-fit parameters
listed in Table \ref{bestfit}.
The shaded area is forbidden for
not being able to turn the region
from expanding to collapsing.}
	\label{tacon}
\end{figure}

Note that
if $\tilde A=\tilde B=0$ in Eq.\eqref{quintic},
$\beta=-\Omega_\text{i}(1+\delta_\text{i})/\tilde k>0$
is automatically the physical root we need.
That is,
for Einstein-de Sitter universe in GR or TEGR,
as shown in many standard cosmology textbooks,
these constraints for $\delta_\text{i}$ and $z_\text{i}$ do not exists
and collapse will always happen eventually due to
the lack of persistent driving source of the expansion.

For a given model and initial perturbation,
Eq.\eqref{reom} determines the evolution of the radius of the overdense region,
which can be carried out numerically.
The evolution of $R/R_\text{i}$ of all three models are plotted in Fig.\ref{revol},
where we have set $z_\text{i}=1200$, $\delta_\text{i}=0.003$,
and taken the best-fit parameters from Table \ref{bestfit}. The variation of $\delta_\text{i}$ will also alter the evolution of $R/R_\text{i}$, which is illustrated in Fig.\ref{m3di} for Model III.
\begin{figure}
	\centering
	\includegraphics[width=0.9\linewidth]{revol.eps}
	\caption{The evolution of $R/R_\text{i}$ of all three models,
where $z_\text{i}=1200$, $\delta_\text{i}=0.003$,
and the models have taken
the best-fit parameters from Table \ref{bestfit}.}
	\label{revol}
\end{figure}

\begin{figure}
	\centering
	\includegraphics[width=0.9\linewidth]{m3di.eps}
	\caption{The evolution of $R/R_\text{i}$ for different $\delta_\text{i}$ in model III,
where $z_\text{i}=1200$,
and the models have taken
the best-fit parameters from Table \ref{bestfit}.}
	\label{m3di}
\end{figure}

We have also calculated the evolutions of the expansion rate $h=\dot R/R$ of the region,
and plotted them in Fig.\ref{hevol}.
The markers in Figs.\ref{revol}-\ref{hevol}
correspond to the turn-around points of the models,
the evaluations of which are listed in Table \ref{betaalpha}.
One can see that
compared to the minimal coupling model (Model I),
the collapsing processes are slower
in the nonminimal coupling models (Model II and III),
thus the turn-arounds
happen at lower redshift $z_\text{ta}$
and consequently larger $\beta=R_\text{max}/R_\text{i}$ are reached.
In the case of Model II where effective dark energy
is entirely attributed to the nonminimal torsion-matter coupling,
the collapsing is the slowest among the three,
and largest $\beta$ is reached at latest time $z_\text{ta}$.

\begin{figure}[!htp]
	\centering
	\includegraphics[width=0.9\linewidth]{hevol.eps}
	\caption{The evolution of $h=\dot R/R$ of all three models,
where $z_\text{i}=1200$, $\delta_\text{i}=0.003$,
and the models have taken
the best-fit parameters from Table \ref{bestfit}.}
	\label{hevol}
\end{figure}

Moreover, it is also worth considering
the evolution of the density contrast between
the collapsing region and the background universe.
Denoting the density of the universe as
$\rho_\text{u}=\rho_\text{i}(a_\text{i}/a)^3$ and
that of the collapsing region as
$\rho_\text{c}=\rho_\text{i}(1+\delta_\text{i})(R_\text{i}/R)^3$,
one then can define the density contrast $\Delta$ by
$\rho_\text{c}=\rho_\text{u}\Delta$.
Utilizing the evolutions of $R$ from Eq.\eqref{reom} and
$a$ from Eq.\eqref{flatunieom},
we have carried out the evolution of $\Delta$,
and illustrated in Fig.\ref{devol}.
\begin{figure}[!htp]
	\centering
	\includegraphics[width=0.9\linewidth]{devol.eps}
	\caption{The evolution of $\Delta=\rho_\text{c}/\rho_\text{u}$ of all three models,
where $z_\text{i}=1200$, $\delta_\text{i}=0.003$,
and the models have taken
the best-fit parameters from Table \ref{bestfit}.}
	\label{devol}
\end{figure}

\section{Virialization of the collapse}
\label{virial}
In Fig.\ref{devol},
one can see that after the turn-around point,
the region governed by Eq.\eqref{reom}
will soon collapse into a singularity,
which, however,
is not the actual fate for all the collapsing structures.
As the clustering continues,
the kinetic energy of the matter
will be no longer negligible,
which will eventually take the system to an equilibrium
and stop the collapsing.
This highly non-linear process is simplified
and described by the virialization of a self-gravity system.

The relativistic virial theorem starts from the
Boltzmann's equation for collisionless particles
(see, e.g., \cite{Jackson1970,Debbasch2009}):
\begin{equation}
	u^\mu\partial_\mu F_\text{B}+\frac{\diff p^\mu}{\diff\tau}\frac{\partial F_\text{B}}{\partial p^\mu}=0,
	\label{boltzmann}
\end{equation}
where $u^\mu$ is the 4-velocity, $p^\mu$ is the 4-momentum,
$\diff p^\mu/\diff\tau$ is the 4-force,
and $F_\text{B}$ is the Boltzmann distribution function
on the 6-dimensional phase space $\{\vec{x},\vec{p}\}$.
Assume that $F_\text{B}$ vanishes sufficiently rapidly
as the velocities tend to infinity,
Eq.\eqref{boltzmann} will lead to the virial theorem
(see, e.g., \cite{Gunn1972,Bohmer2008,Javadinezhad2016}):
\begin{equation}
	2\mathcal{E}_\text{K}+\int\vec{f}\cdot\vec{x}\diff V=0,
	\label{virialth}
\end{equation}
where $\mathcal{E}_\text{K}$ is the kinetic energy of the system
and $\vec{f}$ is the force that the system imposes on
the local volume element $\diff V$ located at $\vec{x}$.
The integral is taken over the whole system.

Usually, the force $\vec f$ or the 4-force $\diff p^\mu/\diff\tau$
should be obtained from the geodesic equation,
or the non-geodesic equation for the nonminimal coupling cases
(see, e.g. \cite{Harko2014,Harko2014a,Feng2015}),
but that requires full knowledge of the spherical symmetric solution
to the field equation of the modified gravity,
which we do not currently have.
On the other hand,
the Newtonian-like gravity force and potential
are connected to the cosmology.
In GR, this argument is originated by Milne\cite{MILNE1934},
and presented in many standard cosmology textbooks.

Consider a comoving test particle located at $r=r_\text{i}a/a_\text{i}=r_0a$,
where $r_0=r_\text{i}/a_\text{i}$ is its comoving position,
then Eq.\eqref{flatunieom} can be written in terms of $r$ as
\begin{equation}
	\begin{split}
		\left( \frac{\dot r}r \right)^2=&\frac{8\pi G}3\frac{\rho_0r_\text{i}^3}{a_\text{i}^3r^3}+\frac{AH_0^4r_\text{i}^3}{a_\text{i}^3r^3}\left( \frac r{\dot r} \right)^2+BH_0^4\left( \frac r{\dot r} \right)^2\\
		=&\frac{8\pi G\rho_\text{i}}3\left( \frac{r_\text{i}}{r} \right)^3+\left[\tilde A\left( \frac{r_\text{i}}r \right)^3+\tilde B\right]h_\text{i}^4\left( \frac r{\dot r} \right)^2,
	\end{split}
	\label{comove}
\end{equation}
which is the equation of motion of the test particle.
Denoting the mass inside a spherical region of radius $r$ as $m=4\pi r_\text{i}^3\rho_\text{i}/3$,
we have
\begin{equation}
	\frac{\left( \dot r \right)^2}2=\frac{Gm}{2r}+\frac12\sqrt{\left( \frac{Gm}r \right)^2+h_\text{i}^4\left( \tilde Ar_\text{i}^3r+\tilde Br^4 \right)}.
	\label{comove1}
\end{equation}
In classic analogy, $\dot r$ is the velocity of the particle,
and the left hand side of Eq.\eqref{comove1}, $(\dot r)/2$,
is the kinetic energy density of it.
We then can identify the right hand side of Eq.\eqref{comove1} as the gravitational potential per unit mass at $r$
\begin{equation}
	V(r)=-\frac{Gm}{2r}-\frac12\sqrt{\left( \frac{Gm}r \right)^2+h_\text{i}^4\left( \tilde Ar_\text{i}^3r+\tilde Br^4 \right)},
	\label{potentialr}
\end{equation}
where $m=4\pi r_\text{i}^3\rho_\text{i}/3=4\pi r^3\rho/3$.
When $\tilde A=\tilde B=0$, it is obviously the Newtonian potential.

And the force per unit mass acting on the volume element at $r$ is
\begin{equation}
	\begin{split}
		f(r)=&-\frac{\diff V(r)}{\diff r}\\
		=&-\frac{Gm}{2r^2}+\frac{-2\frac{G^2m^2}{r^3}+h_\text{i}^4\left( 4\tilde Br^3+\tilde Ar_\text{i}^3 \right)}{4\sqrt{\frac{G^2m^2}{r^2}+h_\text{i}^4\left( \tilde Br^4+\tilde Ar_\text{i}^3r \right)}}.
	\end{split}
	\label{forcer}
\end{equation}
Hence the virial theorem is
\begin{equation}
	\begin{split}
		2\mathcal{E}_\text{K}=&-\int_0^Rf(r)r4\pi r^2\rho\diff r\\
		=&-\frac{9M}{20R}\frac{h_\text{i}^4R^3\left( 2\tilde BR^3+\tilde AR_\text{i}^3 \right)}{\sqrt{G^2M^2+h_\text{i}^4R^3\left( \tilde BR^3+\tilde AR_\text{i}^3 \right)}}\\
		&+\frac{3GM^2}{10R}+\frac{3M}{10R}\sqrt{G^2M^2+h_\text{i}^4R^3\left( \tilde AR_\text{i}^3+\tilde BR^3 \right)}.
	\end{split}
	\label{virialend}
\end{equation}

From Eq.\eqref{potentialr},
if a spherical system has a radius $R$ and mass $M=4\pi R^3\rho/3$,
the total potential energy of it is
\begin{equation}
	\begin{split}
		V_\text{tot}(R)=&\int_0^RV(r)4\pi r^2\rho\diff r\\
		=&-\frac{3GM^2}{10R}-\frac{3M}{10R}\sqrt{G^2M^2+h_\text{i}^4R^3\left( \tilde AR_\text{i}^3+\tilde BR^3 \right)},
	\end{split}
	\label{potentialtot}
\end{equation}
where $R_\text{i}^3=R^3\rho/\rho_\text{i}$.

Although usually the energy conservation is considered violated
in the nonminimal coupling cases due to
the extra force and non-geodesic movement
(see Eq.\eqref{covder} or, e.g., \cite{Harko2014,Harko2014a,Feng2015}),
here the energy conservation is still hold in form during the collapse,
since we have put the effect of the extra force into
the gravitation potential.
And hence, we have
\begin{equation}
	\mathcal{E}_\text{K,vir}+V_\text{tot}(R_\text{vir})=V_\text{tot}(R_\text{max}),
	\label{conservation}
\end{equation}
where $R_\text{vir}$ is the radius of the collapsing region
when it reaches virialization.

Denote $\alpha=R_\text{vir}/R_\text{i}$,
Eq.\eqref{conservation} gives
\begin{equation}
	\begin{split}
		&\frac{\Omega_\text{mi}(1+\delta_\text{i})}{2\beta}+\frac1{\beta}\sqrt{\frac{\Omega_\text{mi}^2(1+\delta_\text{i})^2}{4}+\beta^3(\tilde A+\tilde B\beta^3)}\\
		=&\frac{\Omega_\text{mi}(1+\delta_\text{i})}{4\alpha}+\frac1{2\alpha}\sqrt{\frac{\Omega_\text{mi}^2(1+\delta_\text{i})^2}{4}+\alpha^3(\tilde A+\tilde B\alpha^3)}\\
		&+\frac{3\alpha^2(2\tilde B\alpha^2+\tilde A)}{4\sqrt{\frac{\Omega_\text{mi}^2(1+\delta_\text{i})^2}4+\alpha^3(\tilde A+\tilde B\alpha^3)}},
	\end{split}
	\label{alpha}
\end{equation}
where $\beta=R_\text{max}/R_\text{i}$.
Using the numerical evaluation of $\beta$ from Eq.\eqref{quintic}
and $\alpha$ from Eq.\eqref{alpha},
one can obtain the collapse factor $\lambda=R_\text{vir}/R_\text{max}=\alpha/\beta$.
Furthermore, one can in turn calculate the redshifts and density contrasts
at turn-around $(z_\text{ta},\:\Delta_\text{ta})$
and virialization $(z_\text{vir},\:\Delta_\text{vir})$
from the evolutions plotted in Figs.\ref{revol} and \ref{devol}.
The evaluations at the turn-around and virialization for the models with
$z_\text{i}=1200$, $\delta_\text{i}=0.003$
are listed in Table \ref{betaalpha}.
The corresponding results for Einstein de Sitter universe
are also listed for comparison.
One can see that the results for the minimal coupling model (Model I)
are relatively closer to the E-dS model,
while the nonminimal coupling models (Model II and III)
virialize slower.
The virialization for Model II even happens in the future
$(z_\text{vir}<0)$ for the given setting.

\begin{table}[htbp]
  \centering
  \caption{Turn-around and virialization of the models}
    \begin{tabular}{ccccc}
    \hline
    \hline
          & \multicolumn{4}{c}{models} \\
\cline{2-5}    & Model I & Model II & Model III & E-dS\\
    \hline
    $z_\text{ta}$   & $0.994$ & $0.578$ & $0.816$ & $1.031$\\
    $R_\text{max}/R_\text{i}$    & $335.864$ & $377.229$ & $351.814$ & $334.333$\\
    $\Delta_\text{ta}$   &  $ 5.781$    &  $ 8.242 $   & $6.666$ & $5.551$\\
    \hline
    $z_\text{vir}$   & $0.258$ & $-0.189$ & $0.110$ & $0.363$\\
    $R_\text{vir}/R_\text{i}$    & $167.245$ & $176.837$ & $171.118$ & $167.167$\\
    $\Delta_\text{vir}$   &  $186.470$    &  $ 589.284 $   & $253.331$ & $146.841$\\
    \hline
    $\lambda$& $0.498$ & $0.469$ & $0.486$ & $0.5$\\
    \hline
    \hline
    \end{tabular
  \label{betaalpha
\end{table

\section{Conclusion and discussion}
\label{conclusion}
Most structures in our universe
such as stars, galaxies and clusters of galaxies
are formed from the nonlinear evolution of perturbations during the post-recombination epoch. Ideally, we should hope to investigate the problem by combining $f(T)$ models of large-scale structure formation with hydrodynamic codes which follow the dynamical and thermal histories of the diffuse intergalactic gas. A fully relativistic treat of this non-linear perturbation is not currently available. The intrinsically non-linear nature of the processes is usually handled by N-body simulation, which can be cumbersome and time-consuming, and is not practical for one to use to study different gravitation models. However, the spherical top-hat profile is the simplest analytic model which can be used to study the non-linear growth of spherically symmetric density perturbation and structure formation in $f(T)$ gravities. Though density perturbation will not be spherically symmetric in most of the realistic cases, the spherical top-hat profile can give significant enlightenment for the true picture of physics. Anyhow, the top-hat profile is a useful means for the non-linear evolution of perturbation. In this paper, we have studied the non-linear growth of perturbation in $f(T)$ gravities, including both minimal and nonminimal coupling cases. And then we looked into the virialization of the collapsing region after the turn-around point. Our main results are as follows:

\begin{enumerate}[(i)]
	\item The numerical calculation of redshift $z_{\text{ta}}$ at the turn-around point indicates incontestably that galaxies and other large-structure features must have formed relatively late in the history of the universe in three $f(T)$ models. If we take appropriate initial conditions $\delta_\text{i}$ at $z=z_\text{i}$, the value of $z_{\text{ta}}$ will not conflict with the late time formation of the structures(see Fig.\ref{m3di}). As a matter of fact, the population of galaxies and quasars have evolved dramatically over the redshift range $0<z<6$.

\item The perturbations were still in the linear regime at $z\sim 1000$, but as they entered upon the later phase of the post-recombination era, their evolution became non-linear. In Ref.\cite{Feng2015}, we have given the relation between $a(t)$ and $t$ at the post-recombination era for the $f(T)$ cosmological models (see Eqs. (45)-(47) in Ref.\cite{Feng2015}). Thereby, we can use the linear evolution equation of density perturbation and get the result of $\delta(z_{\text{ta}})$ which is far more smaller than that of top-hat profile. By the time the perturbed sphere had stopped expanding, its density in the three models is already 5.781, 8.242 and 6.666 times greater than that of the background density. These pictures are consistent with the primitive spherical top-hat collapse (E-dS model).

\item The existence of turn-around point is the crux of matter in the non-linear collapse of density perturbations. The perturbation can always reaches maximum radius for the primitive top-hat model. There are constraints of initial value $\delta_\text{i}$ at $z_\text{i}$ in three $f(T)$ models (see Fig.\ref{tacon}), which reinforce our intuition that in an accelerating expanding universe, a magnitude of perturbation  $\delta_\text{i}$ that is too weak will not be able to turn the overdense region from expanding to collapsing. In Ref. \cite{Feng2015}, we have given $z_{\text{crit}}=0.3298$ and 0.6694 for Model II and Model III, respectively. Here, $z_{\text{crit}}$ is defined as the critical values of the redshift through which the universe changes to the acceleration phase from the deceleration one. Therefore, we have a reasonable explanation for our numerical results. We find that compared to Model III, the collapsing processes are slower since $z_{\text{crit}}$ is smaller in Model II (see Fig.\ref{revol}). Furthermore, the turn-around happens at lower redshift $z_{\text{ta}}$ and consequently larger $R_{\text{max}}/R_\text{i}$ is reached.

\item Outwardly, the subsequent collapse occurs very rapidly (see Fig. \ref{revol}) after the redshift of $z_{\text{ta}}$ and the spherical perturbed region collapses ultimately to a black hole. In reality, however, it is much more likely to form some sort of bound object. If the density becomes high enough, we cannot neglect the internal pressure in the overdense region. As the gas cloud collapses, its temperature increases until pressure gradients becomes sufficient to balance the attractive force of gravitation. The ultimate result is a system which satisfies the virial theorem. By the numerical calculation, we have obtained the density contrast between the collapsing region and the background universe by the time the region is virialized (see Table 2). Since the critical value $z_{\text{crit}}$ of Model II is smaller than that of Model III, we have a good reason to expound the slower virialized process for Model II.

\item  The numerical results show that nonminimal coupling models collapse slower than the minimal coupling model, which may be an indication for alleviating the small scale problems
    \cite{Moore1994,Boylan-Kolchin2012}.

\item The virialization for Model II happens in the future ($z_{\text{vir}}=-0.189$) for the given setting $z_\text{i}=1200$ and $\delta_\text{i}=0.003$. This is not strange because the spherical top-hat collapse is a highly idealised picture. The better approximation is to assume that the collapsing regions are ellipsoidal with three unequal principal axes. In this model, the ellipsoid collapses to a 'pancake' which is the collapsing result of the non-linear regime in the more general case.
  \end{enumerate}

To sum up, the spherical top-hat collapse is a qualitative analysis which successfully expounds the aspects of non-linear evolution in $f(T)$ gravities. But this is a highly idealised description, so we do not really expect that it is quantitatively consistent with the process of formation of bound structures in the expanding universe. For example, the observation of CMB requires $\Delta T/T\sim 10^{-5}$, which is corresponding to $\delta\rho/\rho\sim 10^{-5}$ at $z=1200$. In other words, the spherical top-hat collapse is only a toy model. For comparison with the observation, we should study further the pancake model and N-body simulations in $f(T)$ gravities. We will look into these issues in the future works.

redpajama_set_name: RedPajamaArXiv


Good medium-deep red. High-toned aromas of raspberry, mocha and nutty oak, with a suggestion of berry liqueur. Sweet, lush and broad, with enticing flavors of dried cherry, raspberry and milk chocolate. Finishes with ripe tannins. Interestingly, this struck me as a bit fatter and lower in acidity than the 2004 release."


The firm represented a national insurance company against a personal injury plaintiff who pursued his own third party bad faith claim against the company as well as first party breach of contract and bad faith claims assigned to him by the insured. The case arose from a tragic car accident. A mine employee who left work allegedly fell asleep after working a double shift, crossed the center line and collided with the accident victim. The mine employee died in the accident, and the plaintiff victim suffered other catastrophic injuries allegedly rendering him unable to work again. He filed suit and subsequently added the mine that employed the tortfeasor as a defendant. He claimed his injuries arose from their negligent supervision of the tortfeasor. The insurer for the mine denied the claim and did not provide a defense, relying upon a total auto exclusion in their CGL policy. Ultimately, the insured assigned its rights against the insurer to the plaintiff and filed suit directly against the insurer. The case ended in a voluntary settlement.


Indian Ocean hotels are seeing larger but fewer deals. In the Middle East, stagnant oil prices are prompting more outbound capital investment.
ABU DHABI, United Arab Emirates—The Middle East and Indian Ocean are seeing healthy investment numbers overall, but a closer look at investment in the region reveals most of the money is finding its way to one or two large deals, according to speakers at the recent Gulf & Indian Ocean Hotel Investors' Summit.
"In the Indian Ocean, we've seen $300 million worth of transactions in 2017, an increase of 65% over the previous year, but that is mostly down to the purchase of one resort in The Maldives," said Nihat Ercan, managing director of investment sales, Asia, at JLL Hotels & Hospitality Group.
That impressive deal was the $200 million sale, to an undisclosed owner, of the Cheval Blanc Randheli, Ercan said. The price per key was approximately $5 million for that property, which has an average daily rate of approximately $1,700.
"Over the last six years, 34% of transactions (across the Indian Ocean) have been institutional in nature. This bodes well for liquidity," Ercan said.
Ercan added The Maldives has become especially investor-friendly, but that is not necessarily the situation across the region.
Ercan's colleague Marko Vucinic, SVP, Middle East & Africa, at JLL Hotels, said there is money moving in the Middle East, as well, but much of it is headed for other regions, including Europe. Vucinic noted 95% of Middle Eastern capital was outbound, and overall there was an 11.6% decrease in volume of all sales, domestic and international.
Investment within the Gulf region tended to be domestic over the last few years, Vucinic said.
"The bulk of deals outside off the Middle East (in 2017) have been with local partners, which was not the case so much in the past," he said.
Vucinic pointed to two key deals that are emblematic of the new status quo: the €56 million ($69 million) sale of the 361-room Westin Warsaw in January 2017 by Qatari firm Al Sraiya Holding Group and Abu-Dhabi-based Twenty14 Holdings' €85 million ($117 million) purchase of the 214-room Waldorf Astoria Edinburgh.
One stumbling block in the region, he added, is the ongoing boycott of Qatar and Qatari investment, which started in June amid Gulf Cooperation Council countries accusing Qatar of supporting terrorism.
Robin Rossmann, managing director of STR, parent company of Hotel News Now, said there is projected to be 105,616 hotel rooms across the Middle East by 2020.
Rossmann pointed to several factors in the region: supply ramping up in Saudi Arabia, whether demand growth can match supply in Dubai and whether investor sentiment will improve.
Performance in the area remains tied to the price of oil, he said.
"(Gross operating profit per available room) is closely aligned with the oil price, which continues to fall," he said.
Overall, yields are declining in the Indian Ocean, Ercan said. "Cash-on-cash returns are tightening, with stabilized yields in the order of 8% to 9%," he said.
Supply moratoriums have been impactful recently in Mauritius and The Seychelles, Ercan said.
"The Seychelles offers freehold land, but has a moratorium in supply. Mauritius ended its (two-year) moratorium late last year, which obviously has limited supply," he said, adding that Mauritius is expanding its airport.
Sri Lanka, Ercan said, is putting into place legislation to support foreign investment.
infrastructure problems in Sri Lanka and the perception of it being a budget destination.
Vucinic said for Dubai and the United Arab Emirates, midscale properties will continue to be a target for investment.
"Between 2014 and 2017, we've seen a twofold increase in upscale properties but a five-time increase in midscale properties," he said.


text:
Remembrance Day in Brixton's Windrush Square
West Indian Association of Service Personnel (WASP) parade in Windrush Square last year
Brixton's Windrush Square will host an inaugural Remembrance Day Heroes Parade on Sunday (12 November). Lambeth council leader Lib Peck, mayor Marcia Cameron, Baroness Howells and veterans and serving personnel are due to take part. A wreath-laying ceremony will take place from 1 to 2pm at the African Caribbean war memorial with a choir and a bugle call to begin a two-minute silence.
The ceremony will be hosted by Jak Beula, who designed the memorial and worked tirelessly to see its find its place in Windrush Square, and Nairobi Thompson, the grandniece of First World War hero Walter Tull.
Earlier, Stockwell memorial gardens will be the scene for a remembrance service and wreath laying ceremony. After a two-minute silence at 11am, a short service will be conducted by the Rev Erica Wooff of the Stockwell parish of St Andrew and St Michael.
There will also be ceremonies at the Albert Carr Gardens War Memorial, on the corner of the High Road and Streatham Common Northside, SW16 (10.30am); a service and wreath laying at Kennington Park War Memorial, after a parade starting at 10.35 am from the junction of Braganza Street/Doddington Grove to arrive at the Kennington memorial at 11am; the SOE Agents Monument, Lambeth Palace Road, SE1 (between Lambeth Palace and the Thames) at 10.40am; and Vincennes War Memorial, Hamilton Road, SE27 at 3pm.
Windrush Square
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text:
Ecological overlap and horizontal gene transfer in Staphylococcus aureus and Staphylococcus epidermidis
Guillaume Méric, Maria Miragaia, Mark de Been, Koji Yahara, Ben Pascoe, Leonardos Mageiros, Jane Mikhail, Llinos G Harris, Thomas S Wilkinson, Joana Rolo, Sarah Lamble, James E Bray, Keith A Jolley, William P Hanage, Rory Bowden, Martin C J Maiden, Dietrich Mack, Hermínia de Lencastre, Edward J Feil, Jukka Corander & 1 others Samuel K Sheppard
Department of Biology & Biochemistry
Centre for Networks and Collective Behaviour
Centre for Mathematical Biology
EPSRC Centre for Doctoral Training in Statistical Applied Mathematics (SAMBa)
Milner Centre for Evolution
The opportunistic pathogens Staphylococcus aureus and Staphylococcus epidermidis represent major causes of severe nosocomial infection, and are associated with high levels of mortality and morbidity worldwide. These species are both common commensals on the human skin and in the nasal pharynx, but are genetically distinct, differing at 24% average nucleotide divergence in 1,478 core genes. To better understand the genome dynamics of these ecologically similar staphylococcal species, we carried out a comparative analysis of 324 S. aureus and S. epidermidis genomes, including 83 novel S. epidermidis sequences. A reference pan-genome approach and whole genome multilocus-sequence typing revealed that around half of the genome was shared between the species. Based on a BratNextGen analysis, homologous recombination was found to have impacted on 40% of the core genes in S. epidermidis, but on only 24% of the core genes in S. aureus. Homologous recombination between the species is rare, with a maximum of nine gene alleles shared between any two S. epidermidis and S. aureus isolates. In contrast, there was considerable interspecies admixture of mobile elements, in particular genes associated with the SaPIn1 pathogenicity island, metal detoxification, and the methicillin-resistance island SCCmec. Our data and analysis provide a context for considering the nature of recombinational boundaries between S. aureus and S. epidermidis and, the selective forces that influence realized recombination between these species.
Genome biology and evolution
https://doi.org/10.1093/gbe/evv066
Staphylococcus epidermidis
gene transfer
Staphylococcus aureus
recombination
commensal
pathogenicity islands
Genomic Islands
pathogenicity
Multilocus Sequence Typing
Ecological and Environmental Processes
Evolution, Molecular
Gene Transfer, Horizontal
Genes, Fungal
Genome, Fungal
Méric, G., Miragaia, M., de Been, M., Yahara, K., Pascoe, B., Mageiros, L., ... Sheppard, S. K. (2015). Ecological overlap and horizontal gene transfer in Staphylococcus aureus and Staphylococcus epidermidis. Genome biology and evolution, 7(5), 1313-1328. https://doi.org/10.1093/gbe/evv066, https://doi.org/10.1093/gbe/evv066
Ecological overlap and horizontal gene transfer in Staphylococcus aureus and Staphylococcus epidermidis. / Méric, Guillaume; Miragaia, Maria; de Been, Mark; Yahara, Koji; Pascoe, Ben; Mageiros, Leonardos; Mikhail, Jane; Harris, Llinos G; Wilkinson, Thomas S; Rolo, Joana; Lamble, Sarah; Bray, James E; Jolley, Keith A; Hanage, William P; Bowden, Rory; Maiden, Martin C J; Mack, Dietrich; de Lencastre, Hermínia; Feil, Edward J; Corander, Jukka; Sheppard, Samuel K.
In: Genome biology and evolution, Vol. 7, No. 5, 05.2015, p. 1313-1328.
Méric, G, Miragaia, M, de Been, M, Yahara, K, Pascoe, B, Mageiros, L, Mikhail, J, Harris, LG, Wilkinson, TS, Rolo, J, Lamble, S, Bray, JE, Jolley, KA, Hanage, WP, Bowden, R, Maiden, MCJ, Mack, D, de Lencastre, H, Feil, EJ, Corander, J & Sheppard, SK 2015, 'Ecological overlap and horizontal gene transfer in Staphylococcus aureus and Staphylococcus epidermidis', Genome biology and evolution, vol. 7, no. 5, pp. 1313-1328. https://doi.org/10.1093/gbe/evv066, https://doi.org/10.1093/gbe/evv066
Méric G, Miragaia M, de Been M, Yahara K, Pascoe B, Mageiros L et al. Ecological overlap and horizontal gene transfer in Staphylococcus aureus and Staphylococcus epidermidis. Genome biology and evolution. 2015 May;7(5):1313-1328. https://doi.org/10.1093/gbe/evv066, https://doi.org/10.1093/gbe/evv066
Méric, Guillaume ; Miragaia, Maria ; de Been, Mark ; Yahara, Koji ; Pascoe, Ben ; Mageiros, Leonardos ; Mikhail, Jane ; Harris, Llinos G ; Wilkinson, Thomas S ; Rolo, Joana ; Lamble, Sarah ; Bray, James E ; Jolley, Keith A ; Hanage, William P ; Bowden, Rory ; Maiden, Martin C J ; Mack, Dietrich ; de Lencastre, Hermínia ; Feil, Edward J ; Corander, Jukka ; Sheppard, Samuel K. / Ecological overlap and horizontal gene transfer in Staphylococcus aureus and Staphylococcus epidermidis. In: Genome biology and evolution. 2015 ; Vol. 7, No. 5. pp. 1313-1328.
@article{7d17cc89ee5b4473b61c679258df5602,
title = "Ecological overlap and horizontal gene transfer in Staphylococcus aureus and Staphylococcus epidermidis",
abstract = "The opportunistic pathogens Staphylococcus aureus and Staphylococcus epidermidis represent major causes of severe nosocomial infection, and are associated with high levels of mortality and morbidity worldwide. These species are both common commensals on the human skin and in the nasal pharynx, but are genetically distinct, differing at 24{\%} average nucleotide divergence in 1,478 core genes. To better understand the genome dynamics of these ecologically similar staphylococcal species, we carried out a comparative analysis of 324 S. aureus and S. epidermidis genomes, including 83 novel S. epidermidis sequences. A reference pan-genome approach and whole genome multilocus-sequence typing revealed that around half of the genome was shared between the species. Based on a BratNextGen analysis, homologous recombination was found to have impacted on 40{\%} of the core genes in S. epidermidis, but on only 24{\%} of the core genes in S. aureus. Homologous recombination between the species is rare, with a maximum of nine gene alleles shared between any two S. epidermidis and S. aureus isolates. In contrast, there was considerable interspecies admixture of mobile elements, in particular genes associated with the SaPIn1 pathogenicity island, metal detoxification, and the methicillin-resistance island SCCmec. Our data and analysis provide a context for considering the nature of recombinational boundaries between S. aureus and S. epidermidis and, the selective forces that influence realized recombination between these species.",
keywords = "Ecological and Environmental Processes, Evolution, Molecular, Gene Transfer, Horizontal, Genes, Fungal, Genetic Variation, Genome, Fungal, Homologous Recombination, Staphylococcus aureus, Staphylococcus epidermidis",
author = "Guillaume M{\'e}ric and Maria Miragaia and {de Been}, Mark and Koji Yahara and Ben Pascoe and Leonardos Mageiros and Jane Mikhail and Harris, {Llinos G} and Wilkinson, {Thomas S} and Joana Rolo and Sarah Lamble and Bray, {James E} and Jolley, {Keith A} and Hanage, {William P} and Rory Bowden and Maiden, {Martin C J} and Dietrich Mack and {de Lencastre}, Herm{\'i}nia and Feil, {Edward J} and Jukka Corander and Sheppard, {Samuel K}",
note = "{\circledC} The Author(s) 2015. Published by Oxford University Press on behalf of the Society for Molecular Biology and Evolution.",
doi = "10.1093/gbe/evv066",
journal = "Genome biology and evolution",
T1 - Ecological overlap and horizontal gene transfer in Staphylococcus aureus and Staphylococcus epidermidis
AU - Méric, Guillaume
AU - Miragaia, Maria
AU - de Been, Mark
AU - Yahara, Koji
AU - Pascoe, Ben
AU - Mageiros, Leonardos
AU - Mikhail, Jane
AU - Harris, Llinos G
AU - Wilkinson, Thomas S
AU - Rolo, Joana
AU - Lamble, Sarah
AU - Bray, James E
AU - Jolley, Keith A
AU - Hanage, William P
AU - Bowden, Rory
AU - Maiden, Martin C J
AU - Mack, Dietrich
AU - de Lencastre, Hermínia
AU - Feil, Edward J
AU - Corander, Jukka
AU - Sheppard, Samuel K
N1 - © The Author(s) 2015. Published by Oxford University Press on behalf of the Society for Molecular Biology and Evolution.
N2 - The opportunistic pathogens Staphylococcus aureus and Staphylococcus epidermidis represent major causes of severe nosocomial infection, and are associated with high levels of mortality and morbidity worldwide. These species are both common commensals on the human skin and in the nasal pharynx, but are genetically distinct, differing at 24% average nucleotide divergence in 1,478 core genes. To better understand the genome dynamics of these ecologically similar staphylococcal species, we carried out a comparative analysis of 324 S. aureus and S. epidermidis genomes, including 83 novel S. epidermidis sequences. A reference pan-genome approach and whole genome multilocus-sequence typing revealed that around half of the genome was shared between the species. Based on a BratNextGen analysis, homologous recombination was found to have impacted on 40% of the core genes in S. epidermidis, but on only 24% of the core genes in S. aureus. Homologous recombination between the species is rare, with a maximum of nine gene alleles shared between any two S. epidermidis and S. aureus isolates. In contrast, there was considerable interspecies admixture of mobile elements, in particular genes associated with the SaPIn1 pathogenicity island, metal detoxification, and the methicillin-resistance island SCCmec. Our data and analysis provide a context for considering the nature of recombinational boundaries between S. aureus and S. epidermidis and, the selective forces that influence realized recombination between these species.
AB - The opportunistic pathogens Staphylococcus aureus and Staphylococcus epidermidis represent major causes of severe nosocomial infection, and are associated with high levels of mortality and morbidity worldwide. These species are both common commensals on the human skin and in the nasal pharynx, but are genetically distinct, differing at 24% average nucleotide divergence in 1,478 core genes. To better understand the genome dynamics of these ecologically similar staphylococcal species, we carried out a comparative analysis of 324 S. aureus and S. epidermidis genomes, including 83 novel S. epidermidis sequences. A reference pan-genome approach and whole genome multilocus-sequence typing revealed that around half of the genome was shared between the species. Based on a BratNextGen analysis, homologous recombination was found to have impacted on 40% of the core genes in S. epidermidis, but on only 24% of the core genes in S. aureus. Homologous recombination between the species is rare, with a maximum of nine gene alleles shared between any two S. epidermidis and S. aureus isolates. In contrast, there was considerable interspecies admixture of mobile elements, in particular genes associated with the SaPIn1 pathogenicity island, metal detoxification, and the methicillin-resistance island SCCmec. Our data and analysis provide a context for considering the nature of recombinational boundaries between S. aureus and S. epidermidis and, the selective forces that influence realized recombination between these species.
KW - Ecological and Environmental Processes
KW - Evolution, Molecular
KW - Gene Transfer, Horizontal
KW - Genes, Fungal
KW - Genetic Variation
KW - Genome, Fungal
KW - Homologous Recombination
KW - Staphylococcus aureus
KW - Staphylococcus epidermidis
UR - http://dx.doi.org/10.1093/gbe/evv066
U2 - 10.1093/gbe/evv066
DO - 10.1093/gbe/evv066
JO - Genome biology and evolution
JF - Genome biology and evolution
10.1093/gbe/evv066
10.1093/gbe/evv066Licence: CC BY
http://dx.doi.org/10.1093/gbe/evv066Licence: CC BY
http://dx.doi.org/10.1093/gbe/evv066


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text:
Money Jungle è un album jazz del pianista e compositore Duke Ellington con il batterista Max Roach ed il bassista Charles Mingus, realizzato per la nota etichetta discografica jazz Blue Note nel 1963.

Origine e storia

Nel 1962 Duke Ellington aveva intrapreso diversi progetti solisti senza la sua abituale orchestra: prima un album in coppia con Coleman Hawkins in agosto, poi un album in collaborazione con John Coltrane il 26 settembre, entrambi per la giovane etichetta Impulse! Records. Nello stesso periodo si ritrovò a collaborare con due musicisti facenti parte del contemporaneo cosiddetto "jazz d'avanguardia", il bassista e compositore Charles Mingus e il batterista Max Roach (già protagonista anni prima della scena bebop), con i quali aveva lavorato a stretto contatto nei primi anni cinquanta, per la loro etichetta comune Debut Records.

La sessione di registrazione venne fissata dalla United Artists per il sessantatreesimo compleanno del pianista, nel contesto di un'operazione di rinnovamento attraverso una collaborazione con "una nuova generazione di modernisti" (Mingus e Roach), "per dimostrare la compatibilità tra i musicisti più disparati". Le sessioni per l'album furono anche la prima registrazione in trio di Mingus dopo le sue sedute di registrazione per la Jubilee Records con Hampton Hawes e Dannie Richmond. Nel 1974, Mingus in un'intervista rilasciata alla rivista Downbeat raccontò: «Ho ricevuto una telefonata dalla casa discografica e poi abbiamo incontrato il "duca" nel suo ufficio per discutere di quello che voleva fare esattamente».

Nonostante le circostanze avverse che si verificarono durante la sessione in studio (Mingus litigò aspramente con Max Roach, si rifiutò di continuare a suonare, e fu convinto a non andarsene solo dalle lusinghe di Ellington); i musicisti si amalgamarono bene suonando insieme man a mano che la sessione procedeva.

Mingus riferì in seguito di essere rimasto estremamente irritato per tutto il tempo dell'intera sessione con Ellington e Roach, non solo a causa della lite con Roach, ma anche a causa di suoi problemi professionali connessi alla sua prossima esibizione in concerto alla Town Hall. Ad un certo momento, ripose il contrabbasso nella custodia e stava per lasciare lo studio, ma "The Duke" lo convinse a restare. Ellington stesso riportò in seguito questo dialogo:
 Mingus: «Amico, non posso suonare con questo batterista!»
 Ellington: «Perché, cosa sta succedendo?»
 Mingus: «Duke, ti ho sempre ammirato, e stimo quello che hai fatto musicalmente, ma dovrai trovarti un altro bassista.»

Il disco

Musica

Ellington scrisse appositamente per questo incontro con Mingus e Roach alcuni pezzi nuovi, anche se nessuno dei quattro titoli: Money Jungle, Les fleurs Africaines, Very Special, e Wig Wise, può dirsi tipicamente nello stile Ellingtoniano. Inoltre vennero rielaborati alcuni classici di Ellington come Solitude e Caravan.

L'apertura dell'album è affidata alla title track Money Jungle, "un brano blues a metà strada tra il post-bop e il jazz d'avanguardia" contenente diversi "passaggi sperimentali". La ballata Fleurette Africaine (intitolata nell'LP originale Les Fleurs Africaine), è un pezzo di stampo "impressionista", scritta in onore di quei fiori che fioriscono solo nel pieno della giungla africana.

Segue il vivace, blues ottimista intitolato Very Special, il cui tema è suonato solo per breve tempo, per poi culminare nelle improvvisazioni di Ellington al piano. Warm Valley è una ballata indelebilmente legata alla figura di Johnny Hodges.

Dopo il brano riempitivo Wig Wise, si arriva al classico Ellingtoniano Caravan, riletto con vigore e forza percussiva inusitata. L'album si conclude con un assolo di Ellington in Solitude, l'altro suo classico. Il pianista introduce il tema e dopo i tre all'unisono iniziano ad improvvisarci sopra.

Diverse edizioni
La Blue Note Records rieditò Money Jungle in CD in due differenti versioni. La prima volta nel 1987 (Blue Note CDP 7 46 398 2) con l'aggiunta dei brani inediti A Little Max (Parfait) (2 versioni), Switch Blade, Rem Blues, Backward Country Boy Blues e una versione alternativa di Solitude; ma con alterato l'ordine originale dei brani su disco. La seconda volta nel 2002 (Blue Note 38 227), in un'edizione più corretta filologicamente, con l'aggiunta di altre quattro ulteriori alternate takes (Rem Blues, Money Jungle, Switch Blade e Solitude), poste alla fine della scaletta dei brani dell'LP originale.

Tracce LP 1963 (United Artists Records UAJ 14017)

Lato 1
 Money Jungle — 5:20
 Le Fleurs Africaines (African Flower) — 3:36
 Very Special — 4:26
 Warm Valley — 3:32
Lato 2
 Wig Wise — 3:20
 Caravan — 4:12(Musica di Juan Tizol; testo di Irving Mills).
 Solitude — 5:33(Musica di Duke Ellington; testo di Eddie DeLange e Irving Mills).

Tracce CD 1987 (Blue Note CDP 7 46398 2)

 Very Special — 4:27
 A Little Max (Parfait) — 2:58
 A Little Max (Parfait) [alternate take] — 3:56
 Fleurette Africaine (African Flower) — 3:37
 REM Blues — 4:17
 Wig Wise — 3:19
 Switch Blade — 5:25
 Caravan — 4:14
 Money Jungle — 5:30
 Solitude [alternate take] — 4:44
 Solitude — 5:34
 Warm Valley — 3:34
 Backward Country Boy Blues — 6:19

Tracce CD 2002 (Blue Note 38 227)

 Money Jungle –5:27
 Fleurette Africaine –3:33
 Very Special –4:23
 Warm Valley –3:31
 Wig Wise –3:17
 Caravan –4:11
 Solitude –5:31

Bonus tracks
 Switch Blade –5:21
 A Little Max (Parfait) –2:57
 Rem Blues –4:15
 Backward Country Boy Blues –6:30
 Solitude –4:42
 Switch Blade –5:11
 A Little Max (Parfait) –2:57
 Rem Blues –5:44

 Tutte le tracce sono composizioni di Ellington, eccetto nº 6: composta da Ellington, Mills & Tizol, e nº 7: composta da DeLange, Ellington & Mills. Le tracce 12-15 sono alternate takes, inserite nell'edizione ampliata dell'album.

Crediti
 Duke Ellington — pianoforte
 Charles Mingus — contrabbasso
 Max Roach — batteria

Note

Collegamenti esterni

redpajama_set_name: RedPajamaWikipedia


text:
La stagione 1958-59 dei Cincinnati Royals fu l'11ª nella NBA per la franchigia.

I Cincinnati Royals arrivarono quarti nella Western Division con un record di 19-53, non qualificandosi per i play-off.

Roster

Staff tecnico
Allenatori: Bobby Wanzer (3-15) (fino al 1º dicembre), Tom Marshall (16-38)

Note

Collegamenti esterni

Stagione 1958-1959 delle squadre di pallacanestro
1958-1959