Bringing down the curtains on the controversy surrounding the infamous Darjeeling land scam, Army chief General Deepak Kapoor today ordered court martial proceedings against Lt Gen Avadesh Prakash, a military secretary and the senior-most three-star officer ever to face such an action.
Acting on an unprecedented "advice" from Defence Minister AK Antony, the Army chief issued the instructions for action against Lt Gen Prakash for his role in the issuance of a no-objection certificate to a private firm that falsely claimed to be establishing an affiliate of Ajmer-based Mayo College on the land adjacent to Sukhna cantonment in Darjeeling district of West Bengal.
Initially, General Kapoor had recommended administrative action against Lt Gen Prakash, who was to retire in two days, and had okayed disciplinary action against Lt Gen PK Rath, the then GoC of the 33 Corps at Darjeeling.
Separately, Lt Gen Ramesh Halgali and Maj Gen P Sen will face administrative action. Show-cause notices had been issued to them about two weeks ago. A court of inquiry ordered by the Eastern Army Commander, Lt Gen VK Singh, who is the Army chief-designate, had recommended "termination of service" for Lt Gen Prakash and administrative action against the other officers.
A court martial could even lead to imprisonment and being "cashiered" from service, which entails loss of rank, decorations and all post-retirement benefits, all depending on the severity of charges. However, Lt Gen Prakash would now get an opportunity to defend himself in the case.
Commenting on today's move, retired Army officers opined that General Kapoor knew that the unprecedented "advice" from Antony was like an order, which had to be complied with. "It was almost clear that the General was not to defy Antony. The Minister's clout within the Congress and his clean image was well known and a defiance would not have gone down well. Also, historically any defiance by the men in uniform has been viewed with suspicion by the elected representatives of Parliament," they said.
One such recent case was in 2008 when the then Navy Chief Admiral Sureesh Mehta had refused to implement the "insufficient" recommendations of the Sixth Pay Commission. He was asked to tow the line. The opposition parties and the media joined in telling how the Admiral was wrong while being totally in favour of "better pay and perks" for the forces.
Lastly, General Kapoor knew the implications even if he had opted to differ with Antony -- the Minister could have issued instructions himself, which could have caused even more embarrassment. "It was not a policy decision on national security that the Chief should stick to his own line and stand up to the Minister," said an officer.
One of the Army's senior-most generals will face a court martial for his alleged role in a land scam that runs into hundreds of crores.
The Chief had earlier refused to sack Prakash, despite the recommendation of an internal army inquiry. Instead, Kapoor gave Prakash 15 days to formally explain his role in the case.
Earlier this week, Defence Minister AK Antony advised the Army to order a court martial. That was seen as the government's way of expressing its dissatisfaction with what was seen as the Army Chief's inaction against Prakash. Sources say the government and former army chiefs were worried that the scam, and the lack of disciplinary action against Prakash, suggested that senior officers were being protected by the army.
Evidence will now be recorded against Prakash, who will later be cross-questioned as part of the court martial.
Lieutenant General Avadesh Prakash was indicted by an army inquiry of using his position to help a businessman in Siliguri in West Bengal.
The internal investigation found that Prakash influenced officers to permit a real estate developer to acquire 71 acres next to the Army's 33 Corps Headquarters in Siliguri in West Bengal. The Army, which had earlier told the government that this land could not be sold to any commercial developer for security reasons, okayed the transfer of the land to Agarwal.
The Army's inquiry said Prakash should be sacked for he "became a facilitator in promoting (his friend) Dilip Agarwal's business."
India has developed a new generation multi-sensor, multi-weapon defence system against enemy targets on board naval ships.
The state-of-the-art "Gun Fire Control System" (GFCS) developed by Bharat Electronics Limited will be installed on board the P-28 class of ships.
"The GFCS is a quick reaction, multi-sensor, multi-weapon, short/medium/long range defence system against air, surface or shore targets on board naval ships", a senior official of the Bangalore-based Navratna defence PSU told PTI.
The GFCS is designed to provide air, surface or shore defence with 76 MM and 30 MM guns. Its purpose is to locate a hostile target using a radar or video tracker, acting on early warning search radars and to track its approach with high accuracy, in order to obtain reliable target data.
The data is further processed and used to control the weapons by pointing it in an exact ballistic firing position for eventual destruction of the target. The GFCS continues to track the approaching target, simultaneously pointing the weapon on it, until it is completely destroyed.
The GFCS comprises five functional sub-systems: tracker, weapon control, sight control, combat management system and support systems, each of which can be used as an independent system.
The GFCS for the P-28 class of ships would be "handed over" to Defence Minister A K Antony at a ceremony here in the presence of BEL Chairman and Managing Director Ashwani Kumar Datt on February 2.
A state-of-the-art facility, dedicated to manufacture of Digital Flight Control Computer (DFCC) for the Light Combat Aircraft (Tejas) at BEL's Bangalore Complex will also come up.
DFCC is a multiple redundant (improving its reliability, one channel will take over if another fails) digital fly-by-wire flight control system of Tejas, which controls manoeuvering of the aircraft.
DFCC is a flight critical sub-system to be manufactured as per AS 9100 standards with stringent in-process and quality control processes, including environmental tests on each unit.
To meet this requirement, BEL has set up this integrated manufacturing facility for assembly, inspection and testing of DFCC, all under one roof.
The facility includes thermal cycling chamber, vibration machine, dehumidifying chambers for storing PCBs, high resolution inspection tools to identify process errors, automated test equipment for rigorous performance testing and engineering test station for testing the DFCC unit.
Antony will inagurate the DFCC.
It was a momentous occasion for 209 women, who created history by forming the first batch of women constables to join the ranks of the Indo-Tibetan Border Police (ITBP), on passing out from the Basic Training Center (BTC) here today.
Home Minister P Chidambaram reviewed the parade, which was commanded by Poonam Johari. Terming the Sino-Indian border as the most difficult, where these women constables would be deployed, he said the women personnel would be able to regulate and screen women during international trade between India and China at Nathu La and Sherathung, besides escorting female pilgrims on the Kailash Mansarovar Yatra.
Felicitating parents for taking a bold decision to let their daughters join a force entrusted with guarding one of the most challenging borders in the world, Chidambaram said these constables would always cherish this day even as it was written in golden letters in the history of the ITBP.
VVIP security duties, guarding vital installations, rescue and relief operations, including disaster management and psychological operations at border villages and during festivals, public meetings and agitations are other tasks they are expected to undertake.
ITBP Director General Vikram Srivastava said they would be further trained in counter-insurgency and jungle warfare and mountaineering and skiing as well. A Quick Reaction Team (QRT) and a Bomb Detection and Disposal Squad would also be formed in order to raise an independent women's battalion, he added.
The Home Minister also gave away awards for excellence during training.
The Taliban mounted their latest attack on Kabul on January 18 soon after British Foreign Secretary David Miliband affirmed that the London Conference on Afghanistan, which started on January 28, must show that there is a coherent international plan for the future of Afghanistan.
But the attack underlines that an agreement between the West and President Karzai is essential not only for the coherence of any plan that might emerge from the London conference, but more importantly, perhaps, for its implementation.
The Taliban assault highlighted yet again the inextricable intertwining of security and governance.
It was intended to tell the West and Karzai that a surge of 37,000 Nato troops won't achieve security in Afghanistan and that there will be no reconciliation with moderate or any other Taliban.
The Afghan National Army (ANA) restored order in Kabul. But paradoxes coexist. The ANA's success served as a reminder that the West has not trained enough Afghans to stabilise their country.
General Stanley McChrystal's advice, given to the Obama administration last summer, still needs to be followed: building up the Afghan security forces would be "the most important thing we do in the future." Only then will Karzai's government be able to establish a legal monopoly of force in Afghanistan.
Insecurity largely explains the weakness of political institutions and the rule of law in Afghanistan. Stable political institutions and a strong rule of law cannot be established in the middle of a war. As Transparency International pointed out in a recent report, instability and corruption reinforce each other.
But Karzai must realise that decent governance is necessary to deliver essential services to ordinary Afghans, and to enhance his legitimacy.
For their part his western allies will not enhance their legitimacy – or his – by publicly berating him for misgovernance.
The western criticism of Karzai can easily be construed as a slight to the proud Afghans: he has said that the poverty of Afghans should not become a means to insult and ridicule them.
In any case, Karzai can turn the tables on his western critics – as he did – by sharply denouncing the killing of civilians in recent Nato attacks.
And rumours that Nato soldiers had desecrated the Koran sparked a violent protest in the southern province of Helmand.
Denials by Nato could not hide the fact that such incidents only play into the hands of the Taliban.
Nato and Karzai must work together to strengthen the government in Kabul. For reconciliation with any 'moderate' Taliban, deemed vital by the West to win in Afghanistan, can only be achieved by a strong centre. Reconciliation will not be achieved either by a divided Nato or by Nato and Karzai blaming each other for Afghanistan's woes.
To some extent the onus for poor governance rests with the West. Omar Zakhilwal, the Afghan Finance Minister (favoured by the West), has said that western countries must share the blame for corruption in Afghanistan and that some in the West were using the issue to make domestic political mileage.
The allegation cannot be dismissed simply because it is made by an Afghan.
So first, Nato must provide security, which will include training more Afghans to assume full responsibility for their country's defence.
Success will only come when Karzai and his Nato backers agree that Afghans should have a government that is strong enough to protect them and provide them with essential services.
India's most senior army officer has declared that the country needs to prepare for a two-front war with China and Pakistan.
In what appear to be deliberately provocative remarks, India's most senior army officer has declared that the country needs to prepare for a two-front war with China and Pakistan.
Most of the Pakistani media dwelt only on that part of a lengthy statement at the end of last month by General Deepak Kapoor, the chief of the Indian army staff, and consequently it was scoffed at, even in political circles. But there is more to it than that.
To begin with, making contingency plans for all possibilities, however improbable, is bread and butter for all militaries in peacetime. But a two-front war is a nightmare scenario for any country, whatever its military strength. And the challenge of facing China's military forces by themselves should be sufficiently daunting for the Indians without adding the possibility of taking on Pakistan at the same time (indeed, Pakistan alone would be no walkover for the current Indian military).
It would seem, therefore, that Gen Kapoor is being unrealistic. But before attempting to understand the reasoning behind his assertion, let us examine what else he said.
In preparing for the two-front strategy, Gen Kapoor listed four requirements: first, continuing to develop a "Cold Start" strategy; second, countering "both military and non-military facets of asymmetric and sub-conventional warfare"; third, enhancing "strategic reach and out-of-area capabilities" and attaining "operational synergy" between the three services; and finally, achieving a "technological edge" over India's opponents.
While "strategic reach and out-of-area capabilities" and achieving a "technological edge" over China appear over-ambitious, it is a sorry military that is still seeking to synergise its tri-service operations. The second requirement is an obvious necessity of the times. It is the first point that needs to be understood from a military perspective.
Cold Start is a concept that the Indian military has been aspiring to for some years, to offset the advantage Pakistan enjoys of being able to assemble forces for war in a shorter period of time; an advantage offered to it by geography alone, because Pakistan lies linear to India, with little depth.
The Indian military is deployed in considerable depth, along both the Chinese border and the Pakistani one. In the event of a war with one of the two countries, some of the forces deployed against the other would have to be moved in support of those at war. Usually, this "assembly" of forces takes place before battle is joined. However, the concept of Cold Start envisages troops moving from peacetime quarters directly into battle.
In military parlance there is a concept referred to as "balance", which relates to the time-distance between forces; a force is said to be in a state of balance if it is capable of sustaining itself to achieve the assigned mission in a time period within which reserve forces can arrive, permitting the initial force to go further – whether in defence or attack.
In attempting a Cold Start there is an inherent risk to the maintenance of balance between the forces that have joined battle and those leaving barracks to reinforce them. There are too many imponderables, and the operation has to be impeccably planned. This delicate state of balance between his forces lay behind Napoleon's success at the battles of Ulm and Austerlitz in 1805, when he defeated far superior forces. But then, that was Napoleon and he was at the height of his military powers. His attempt to repeat the feat ended in defeat at Waterloo.
Peacetime military leaderships are usually not trained to take risks; in fact, they tilt towards being over-cautious, although there are exceptions. This applies to the Subcontinent as much as anywhere else. It would be a bold commander who was prepared to undertake military operations without being certain of timely reinforcement.
So the question arises, what provoked Gen Kapoor's remarks? After all, Pakistan is fighting a domestic war and making continuous overtures for peace with India. Relations between India and China have been steadily improving since the turn of the century; bilateral trade has almost tripled, and occasional hiccups such as the Chinese demands on India relating to the disputed territories of Himachal Pradesh are more tests of each other's tolerance than gestures of aggression; so why, and why now?
Almost certainly India is looking to the future, at a post-US withdrawal from Afghanistan scenario. Despite US efforts to build up Indian military capabilities as a counter-balance to growing Chinese strength, India remains conscious of its inability to meet China militarily or economically on equal terms.
With the imminent US departure from Afghanistan, China is going to be the undisputed regional power and, without considerably increased assistance from the US, India will never be able to catch up with it.
Simultaneously, the US is committed to assisting Pakistan in its war against terrorists, even after it withdraws from the region. Was Gen Kapoor trying to raise the bogey of such a possibility to receive enhanced aid from the US? Or was he merely talking to his domestic audience in an effort to reassure them?
And in any case, whatever his audience, were they listening? I suppose only time will tell.
Bollywood actress Gul Panag tweeted against Indian Army chief General Deepak Kapoor calling him 'spineless' and asked for a probe into why he recommended mild action against his top aide in a land scam in Sukhna cantonment in West Bengal.
'It is a first. Ministry of Defence had to step in as COAS (chief of army staff) continued his stand of trying to protect the said generals. Now WHY was he protecting them?... I would protect someone if 1. I had something to fear from disclosure 2. I am an accomplice 3. I am spineless. COAS is sadly all three,' Panag said in a series of postings on networking site Twitter Thursday.
Panag's father Lt. Gen. H.S. Panag retired as a top army commander.
In a first of its kind instance, Defence Minister A.K. Antony has 'advised' Kapoor to take disciplinary action against one of his top aides Lt. Gen. Avadesh Prakash which may even lead to the latter's court martial.
Earlier, a court of inquiry had indicted Prakash and Lt. Gen. P.K. Rath in the land scam. While the army chief recommended court martial of Rath, he merely sought an 'explanation' from Prakash.
'COAS (Chief of Army Staff) saving his buddy's neck as he is in all likelihood equally dirty,' the actress said in her tweet.
'I'd like to ask our government to enquire into 1. COAS 'reasons' for being 'soft' on said generals 2. Look into COAS assets,' she added Friday.
Panag is the daughter of Lt. Gen. H.S. Panag who retired as the chief of army's Central Command.
The top army commander was removed as the chief of the Northern Army Command in 2008 as soon as he convened inquiry into the irregularities in the purchase of tents made under the tenure of Kapoor.


A Vampire in a mirror!
Zigzag at 6 years old (January 2009). He weighs 4.8 Kg.
He died suddenly in early March, 2013, probably of a pancreatic problem.
Zoe and Zephyr. Zoe is a Miniature Fox Terrier and Zephyr is an Italian Greyhound.
Both dogs are now adults, altho Zephyr is not in this photo. Zoe is 4.5Kg and Zephyr is 5.5Kg.
Zephyr got cancer of the liver, and was put down in December, 2008, at the age of 11.
Italian Greyhounds from circa 150 CE.
Found near Civita Lavinia (Lanuvium) on a spur of the Alban Hills south of Rome, this endearing sculpture is in the Townley Collection of the British Museum. Another pair is in the Vatican Museum.


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Novum scire. A Future Scenario.
January 27, 2018 UncategorizedTakeo HARADA
Today, we proudly announce to release our institute's new scenario entitled "Novum scire". The Institute of International Strategy anf Information Analysis, Inc., IISIA, releases its strategic and risk scenario for both corporates and retail customers twice a year. This year's first issue, "Novum scire", or "Learn somthing new", includes particularly the following issues:
-The future of the global monetary system. The eternal war between "debt currency" versus "public money" ahead?
-The strategy of the Japanese Imperial House and its secret assets. The continuous and future role of gold.
-Cryptocurrency and Bloackchain: Be prepared for Bitcoin 2.0? The tokenized economy and beyond.
-Why "Pax Japonica" in the very near future? Sovereign crisis and its outcome for the global community.
Check it out with this URL and join us to anticipate the very near future.
The Next "X-Day".
January 6, 2018 UncategorizedTakeo HARADA
Since the North and South in the Korean Peninsula has resumed their "reconciliation process" recently, almost nobody in the world seems to believe any geopolitical incident will take place there. Instead, the situation would get better and better, while DPRK promised to dispatch its team even to the PyeongChang Winter Olympics in the forthcoming February, we firmly believe. Even US led by D. Trump agreed with ROK on suspension of their joint military excercise during the Winter Olympic Games.
However, one significant thing should be never forgot, when it comes to an issue of genuine "intelligence": Shodow men in the intelligence world always love to walk on the street where other ordinary people don't choose. Applying this principle to the current situation, we're now urged to reach the tentative conclusion that February ahead might include the next "X-Day".
Imagine what would take place one after another, when a severe terrorist attack with WMD would heavily damage the Olympic Games. The people in the South simply stick to "wishful thinking" that the North would never attack PyeongChang during the Winter Olympics, which should be, form their innocent viewpoint as usual, regarded as the festival of the whole Korean nation. But fot the North, the situation could be completely different. The Olympic Games could be the very best place where the North's self-proclaimed "nuclear force" would be showed up to the global community effectively.
For US, even a smaill incident of terrorism in PyeongChang would give her a very good reason to militarily attack DPRK, by arguing that would be the most effective "preemptive" attack to save the whole world. Of course, within 72 hours, US would completely succeed to win the battle of the "Korean Peninsula", which would give desireble impetus to D. Trump for the mid-term election.
Well, guys, stay alarmed. Particularly in East Asia including my country, Japan, accelerated procurment of foods and goods for your own safety is urgently needed. Keep in mind nobody helps you when a severe "nuclear" incident occurs in the neiborhood. In advance, I give you herewith a friednly advice.

redpajama_set_name: RedPajamaCommonCrawl


Ontario is increasing protections for renters with an easy-to-understand standard lease for new private residential leases, now in effect across the province.
Premier Kathleen Wynne was at Charles Hastings Co-Op Housing Inc. May 1 with Peter Milczyn, Minister of Housing and Han Dong, MPP for Trinity-Spadina, to explain how the government's new standard lease will help both tenants and landlords understand their rights and responsibilities and avoid disputes.
For new leases signed on or after April 30, most landlords are required to use the standard lease, which provides a template to gather basic information such as names and addresses, the total rent and when it is due, and any rules or terms about the rental unit or building. This includes tenancies in single and semi-detached houses, apartment buildings, rented condominiums and secondary units, such as basement apartments.
The standard lease reduces the use of illegal terms and potential misunderstandings caused by verbal tenancy agreements, which will make it easier for landlords to conduct their business and for tenants to understand their rights and responsibilities. It also has simple-to-understand general information on the rights and responsibilities of renting in Ontario.
If a landlord does not use the standard lease for tenancies that are entered into on or after April 30, 2018, renters can ask for one. If the landlord doesn't provide it within 21 days, the tenant can withhold one month's rent.
A guide to the standard lease is available in 23 languages including English and French. This will help ensure that more people understand their rights and what they are agreeing to when they sign a new lease.
The standard lease is part of Ontario's Fair Housing Plan, which includes 16 comprehensive measures to make housing more affordable for homebuyers and renters, while bringing stability to the real estate market and protecting the investment of homeowners. The Plan also includes an expansion of rent control protections for tenants in Ontario.
Expanded rent control means that as of April 20, 2017, approximately 1.3 million residential rental households are now protected from sudden, unexpected rent increases — including all private market rental units whether they are in apartment buildings, rented condominiums or homes. In 2018, those increases are capped at 1.8 per cent and future increases cannot exceed 2.5 per cent unless the landlord has approval from the Landlord and Tenant Board.
Strengthening tenant protections while ensuring predictability for landlords is part of the government's plan to support care, create opportunity and make life more affordable during this period of rapid economic change. The plan includes free prescription drugs for everyone under 25, and 65 or over, through the biggest expansion of medicare in a generation, free tuition for hundreds of thousands of students, a higher minimum wage and better working conditions, and free preschool child care from ages 2.5 to kindergarten.
The standard lease guide is available in 23 languages: Arabic, Simplified Chinese, Traditional Chinese, English, Farsi, French, German, Greek, Gujarati, Hindi, Italian, Korean, Polish, Portuguese, Punjabi, Romanian, Russian, Spanish, Tagalog, Tamil, Ukrainian, Urdu, and Vietnamese.
In the 2016 Census, 3.7 million people in Ontario — nearly 28 per cent of the province — reported a first language other than English or French.
The Fair Housing Plan also expanded rent control to all private rental units, including those built after 1991, strengthening protections for tenants against sudden, dramatic rent increases.
The standard lease does not apply to most social and supportive housing, co-operative housing, retirement and nursing homes, mobile home parks and land lease communities, and commercial properties.
Approximately 1.3 million private residential rental units are now covered by rent control thanks to the Fair Housing Plan. That means the approximately 1 in 5 people in Ontario who live in a private market rental unit are protected by rent control.


Behavior management is similar to behavior modification. . In behavior modification the focus is on changing behavior, while in behavior management the focus is on maintaining order. Behavior management skills are of particular importance to teachers in the educational system. Behavior management include all of the actions and conscious inactions to enhance the probability people, individually and in groups, choose behaviors which are personally fulfilling, productive, and socially acceptable.


SoR typically has a new tutorial every few weeks. Keep updated with an RSS feed!
What is an RSS feed? Its a way of knowing when your favorite websites have new updated content. Instead of visiting 20 of them to check for something new, instead all you need to do is check your single feed server.


Through the 4 week Yin yoga course we invoke and embody the creative and transformational energies of the Hindu Tantric Goddesses into our yoga practice and our lives. Each class is uniquely created with the different Goddess archetypes, using variations in sequence, asana, pranayama and meditations, with evocative and enchanting music.
Dates: 10 week course, Monday Evenings (Commencing Monday 29 April until Monday 1 July 2019).


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ALLL Regulations / CECL Model / FASB seeks comments on proposed CECL updates on accrued interest, recoveries, prepayments
The Financial Accounting Standards Board has proposed updating its guidance for accounting for credit losses using the current expected credit loss model, or CECL, and asked for comments on the potential changes.
In an exposure draft issued Nov. 19, the FASB said that stakeholders had helped it identify areas that require clarification and correction in ASU No. 2016-13, Financial Instruments—Credit Losses (Topic 326) Measurement of Credit Losses on Financial Instruments, as well as in the two other ASUs it issued over the last several years that are related to financial instruments (ASU 2016-01: Financial Instruments—Overall and ASU 2017-12, Derivatives and Hedging).
Several of the proposed CECL changes arose from recent meetings of the Transition Resource Group, including a Nov. 1 meeting that covered disclosing lines-of-credit that are converted to term loans and determining the contractual term of a financial asset with extension or renewal options.
Amendments in its proposed CECL update would apply to all reporting entities. Some entities may have already adopted the new methodology by the time these latest proposals are finalized, the FASB acknowledged, saying it will need to set an effective date and transition requirements for the proposed amendments for those entities. For all others, however, effective dates and transition requirements of CECL would remain unchanged. The board said it would accept comments on the proposals through Dec. 19.
Here are some of the changes proposed, as outlined in the exposure draft issued:
Accrued interest: The first area relates to accrued interest and was a topic at the June 11 transition resource group meeting. There were concerns about current guidance related to some unintended implementation costs because of the requirement that writeoffs of assets measured at amortized cost be deducted from the allowance for credit losses when the financial assets are deemed uncollectible.
Because accrued interest is included in the definition of amortized cost basis, an entity would have to write off accrued interest amounts through the allowance, so the board proposed several options. Among them:
• Measuring the allowance for credit losses on accrued interest receivables balances separately from other components of the amortized cost basis of associated financial assets and net investments in leases and
• Allowing an accounting policy election not to measure an allowance for credit losses on accrued interest if the entity reverses or writes off uncollectible accrued interest amounts in a timely manner.
Recoveries: FASB proposes clarifying that an entity should include recoveries when estimating the allowance for credit losses, and its draft explains how to account for an amount expected to be collected greater than the amortized cost basis. Recoverable amounts included in the valuation account should not exceed the aggregate of amounts previously written off and expected to be written off.
Reinsurance recoveries: The proposal clarifies the FASB's intent to include all reinsurance recoverables – even those measured on a net present value basis – within the scope of the guidance, regardless of the measurement basis of the recoverables.
Projections of interest-rate environments for variable-rate instruments: The proposal would remove the prohibition on using projections of future interest-rate environments when using a discounted cash flow method to measure expected credit losses on variable-rate financial instruments. The proposed amendments instead clarify that the same projections or expectations of future interest-rate environments should be used in both estimating expected cash flows and in determining the effective interest rate used to discount those expected cash flows.
Prepayments' role in determining effective interest rate: An entity would be allowed, under the proposed amendment, to make an accounting policy election to adjust the effective interest rate used to discount expected future cash flows for expected prepayments. However, effective interest rates used to discount expected cash flows shouldn't be adjusted for subsequent changes in expected prepayments if the financial asset is restructured in a troubled debt restructuring.
When to consider selling costs on probable foreclosures: The proposal is intended to clarify that an entity must consider estimated costs to sell if it intends to sell rather than operate the collateral when foreclosure is deemed probable.
Vintage disclosures—Line-of-credit arrangements converted to term loans: The proposed amendments would require disclosing the amortized cost basis of line-of-credit arrangements that are converted to term loans by origination year when an additional credit decision was made by the entity after the original credit decision. An entity isn't required to disclose by origination year the amounts of line-of-credit arrangements that are converted to term loans if no additional credit decision was made by the lender or if they were converted to term loans because of a troubled debt restructuring. Instead, an entity should disclose these line-of-credit arrangements in a separate column within the vintage disclosure, according to the FASB's exposure draft.
Contractual extensions and renewals: The proposal is intended to clarify that an entity should (with some exceptions) consider extension or renewal options in determining the contractual term of a financial asset if they are included in the original or modified contract at the reporting date and are not unconditionally cancellable by the entity.
As previously discussed at its Nov. 7 meeting, the FASB will issue a separate exposure draft on codification improvements to the CECL standard that will include its proposed amendments to vintage disclosures of gross writeoffs and gross recoveries. The board at that meeting agreed to clarify that "gross writeoffs and gross recoveries should be presented by vintage year and class of financing receivable within the credit quality information vintage disclosure" offered by entities, according to meeting minutes. However, board members wanted to provide more time for feedback that would have been improbable had they included it in the current exposure draft.
The latest proposed changes to CECL also don't include any mention of a potential extension of the CECL effective date – something that 45 larger banks have requested through their public policy and advocacy group, The Bank Policy Institute, in an Oct. 17 letter to the Financial Stability Oversight Council. The banks asked the FSOC, a panel of regulators, to evaluate "systemic and economic risks posed by CECL" and to engage with the FASB and regulators to seek a delay.


trazer31 has contributed to 1 posts out of 468613 total posts (0.00%) in 3,270 days (0.00 posts per day).
Hi. I'm King Trazer. I need help with installing Halo Custom Edition on my computer. I'm running Windows vista.
It tells me that It cannot find language specific something.
Does anybody know what I can do? It tells me that I should restart to try and resolve the error but I've restarted 14 times and it still does it.
Time: Sat April 20, 2019 1:21 AM 313 ms.


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Ravens cornerback Tray Walker mourned, remembered at funeral in Miami
By Jeff Zrebiec
| MIAMI
Mourners started stepping out of a hot Florida afternoon and into the 93rd Street Community Baptist Church just after noon Saturday. For the next hour, they kept filing in, intent on honoring late Ravens cornerback Tray Walker.
Mourners started stepping out of the hot Florida afternoon and into the 93rd Street Community Baptist Church just after noon Saturday. For the next hour, they steadily filed in, intent on honoring late Ravens cornerback Tray Walker.
Friends and family members wore shirts with his picture and number on them. High school and college administrators came with stories about a fun yet rebellious boy who grew into a dedicated and driven NFL prospect. His NFL head coach marveled about the competitive spirit of a rookie who twice challenged potential Hall of Fame wide receiver Steve Smith Sr. in one-on-one drills early in training camp.
"The first thing I noticed was the smile, that big Tray Walker smile," Ravens coach John Harbaugh told those in attendance. "That smile can light up a room. Tray Walker, we love you, we're going to miss you."
Walker died on March 18, a day after his motorbike collided with an SUV in a north Miami neighborhood near where he grew up. Hundreds gathered Saturday at the Baptist church to pay their respects. Walker, a fourth-round draft pick in 2015, was 23 and just months removed from playing eight games in his rookie season with the Ravens.
The crowd included Minnesota Vikings quarterback Teddy Bridgewater, Walker's former teammate at Miami Northwestern Senior High School; DeMaurice Smith, the executive director of the NFL Players Association; and approximately 45 Ravens players, coaches and team officials, many of whom arrived from Baltimore in a plane chartered by team owner Steve Bisciotti.
[More from sports] Assistant coach Steve Johns adds special touch for Mids »
About 10 minutes before the ceremony began, Harbaugh and general manager Ozzie Newsome walked shoulder to shoulder down the middle aisle of the church, followed by a line of Ravens that included Smith, Kamar Aiken, Breshad Perriman, Buck Allen, Timmy Jernigan, Crockett Gilmore, Matt Elam and defensive coordinator Dean Pees. Perriman wore a T-shirt with Walker's picture on it.
"It was a tough day," Ravens reserve safety and special teams captain Anthony Levine said after the ceremony. "We're mourning our brother and we're going to miss him, but we know that he's gone up to a better place."
The approximately 90-minute service celebrated Walker's journey from an often in-trouble young boy, to a lightly recruited high school player, to a raw NFL prospect who had vowed to return to Baltimore this summer and win a starting cornerback job.
Walker overcame a tough childhood and just one scholarship offer before garnering the attention of the NFL.
"His NFL career had just begun," Bridgewater said outside the church. "He had tremendous upside, size, everything that you look for in a defensive back. But it was an outlet. Like everyone said in there, football was an outlet for us. So when he was out there on that field, football was a vacation for him. That's how it is for a lot of us down here. So he was just scratching the surface and getting his feet wet in the NFL, and I was just excited for him, knew that he would have a tremendous career."
[More from sports] Annapolis boats find success at Block Island Race Week »
Mourners entered the church to Dorothy Norwood's "Victory is Mine" and later joined in singing Marvin Sapp's "I made it through," celebrating Walker's improbable rise to the NFL.
"My heart is filled with pride and joy," said Dionne Pollock, Walker's godmother. "Don't cry for him. He lived his life. He beat the odds. He graduated from high school. He was going to make a difference in somebody's life with his diploma."
Speakers were asked to keep their message between two and three minutes, but Pollock spoke far longer, joking that her watch was broken. She spoke of the pride she felt when Walker left his college diploma on her bed, and how he ended every conversation by saying or writing, "I love you."
Harbaugh recalled how Walker stayed late for one mandatory rookie event to hang around at-risk Baltimore kids, and how the cornerback told him in their first meeting that his primary motivation was to help out his mother.
Dr. Sheri Mitchell, a pediatrician in Houston who worked with Walker and other Texas Southern athletes, remembered Walker's promise to help her convert written medical files into electronic ones. Four days after the draft, Walker was supposed to meet with Mitchell and complete the task. He didn't show, not that Mitchell minded. She knew that he was on to bigger things.
[More from sports] Twin gymnasts drive their own careers to U.S. Classic »
"I told him, 'I don't care that you were drafted in the fourth round. You better have a note from John Harbaugh [if you don't come],'" Mitchell said. "Greatest pleasure I've ever had in firing someone."
There were plenty of poignant moments. Raymond Sands, the former vice principal at Miami Edison Senior High School, where Walker went before transferring to Miami Northwestern, often had to discipline Walker. After he was drafted, Walker sent Sands a text message that said, "It was because of you."
"You talk about humbleness and humility," Sands said. "I'll never forget that."
Walker's young niece, Tearria Wells, read a tribute that ended with her saying, "We have to keep telling ourselves that we will meet again."
Rev. John White II told the gatherers that "you have my permission to cry" because "a life full of promise and potential, not just on the field but off the field, is no more."
[More from sports] Wellner named defensive coordinator at Notre Dame »
"Farewell Tray, you made the team," White said.
White later announced that another member of the family, Walker's uncle, had died Saturday. One family member, overcome with grief, was helped out of the church following the announcement.
At around 3 p.m. Saturday, Walker's casket, decorated with his name and number, was loaded onto a chariot in front of the 93rd Street Community Baptist Church. On top of the chariot was Walker's helmet from his time at Miami Northwestern, Texas Southern and the Ravens.
The entombment was held later at Caballero Rivero Dade North cemetery. About 1,100 miles away, flags flew half staff at the Ravens' facility in Owings Mills.
jeff.zrebiec@baltsun.com
twitter.com/jeffzrebiecsun
Tray Walker
Teddy Bridgewater
Steve Smith Sr.
National Football League Players Association


The state Department of Education released the 2018 Minnesota graduation rates. More Minnesota seniors than ever before graduated in 2018 with 55,869, it is 83.2% of the graduating class overall, making it the state's highest rate on record. Education Commissioner Mary Catheryn Ricker says the credit for the historic numbers goes to the teachers, coaches, and administrators on a local level that work daily to keep students engaged in learning.
Minnesota DNR Commissioner Sara Strommen is touring the state highlighting budget items. She made her way to the Nicollet Conservation Club to discuss projects that will impact southern Minnesota. Among the projects includes funding for buildings, water/wastewater systems, water access sites, trails and bridges. There are also proposed fee increases. She adds that another big project involves combating Chronic Wasting Disease.
The CityArt Walking Sculpture Tour will welcome 26 new sculptures to the City Centers of Mankato and North Mankato on Saturday, May 11 for its ninth public art installation. The exhibit will feature stunning works of art created by artists from across North America, including many pieces by Minnesota sculptors. Artists and volunteers will begin installing the sculptures at 6:00 a.m. that morning.


Effect: Fanfare: Banish an enemy follower with 3 defense or less. Then draw a card.
A judge who descended from the heavens. He unleashes retribution on the lost souls who pray to be purged of sin, and then he guides them to the light of mercy.
With his staff of salvation, the judge opens a path into the light for those who endure his retribution. His blessings illuminate the sky, and the sinful weep before his forgiveness.


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\begin{document}

\baselineskip=16pt
\begin{titlepage}
\begin{center}

\vspace{0.5cm}

\large {\bf Constraints on scalar-tensor theories of gravity from observations}
\vspace*{5mm} \normalsize

{\bf Seokcheon Lee$^{\,1,2}$}

\smallskip
\medskip

$^1${\it Institute of Physics, Academia Sinica, \\
Taipei, Taiwan 11529, R.O.C.}

$^2${\it Leung Center for Cosmology and Particle Astrophysics, National Taiwan University, \\ Taipei, Taiwan 10617, R.O.C.}

\smallskip
\end{center}

\vskip0.6in

\centerline{\large\bf Abstract}
In spite of their original discrepancy, both dark energy and modified theory of gravity can be parameterized by the effective equation of state (EOS) $\omega$ for the expansion history of the Universe. A useful model independent approach to the EOS of them can be given by so-called Chevallier-Polarski-Linder (CPL) parametrization where two parameters of it ($\omega_{0}$ and $\omega_{a}$) can be constrained by the geometrical observations which suffer from degeneracies between models. The linear growth of large scale structure is usually used to remove these degeneracies. This growth can be described by the growth index parameter $\gamma$ and it can be parameterized by $\gamma_{0} + \gamma_{a} (1 - a)$ in general. We use the scalar-tensor theories of gravity (STG) and show that the discernment between models is possible only when $\gamma_a$ is not negligible. We show that the linear density perturbation of the matter component as a function of redshift severely constrains the viable subclasses of STG in terms of $\omega$ and $\gamma$. From this method, we can rule out or prove the viable STG in future observations. When we use $Z(\phi) =1$, $F$ shows the convex shape of evolution in a viable STG model. The viable STG models with $Z(\phi) = 1$ are not distinguishable from dark energy models when we strongly limit the solar system constraint.

\vspace*{2mm}

\end{titlepage}

\section{Introduction}
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The late-time acceleration of the cosmic expansion invokes the mysterious dark energy or the modification of the gravity theory beyond Einstein's general relativity. Although there exist a number of dark energy and modified gravity models, both can be described by the effective equation of state (EOS) $\omega$ when one considers the expansion history of the Universe. Chevallier-Polarski-Linder (CPL) parametrization $\omega = \omega_0 + \omega_a (1 - a)$ is one of the suitable candidates to describe the general $\omega$ \cite{0009008,0208512}.

However, models of different physical origins with the same background expansion history can not be separated with $\omega$. Thus, the growth of large scale structure is used as a complementary probe to segregate models \cite{0503644,0507184,0612452,07042421,07090307,08012431,08021068,08033292}.

The growth index parameter (GIP) $\gamma$ defined by $\fr{d \ln \delta_{\m}(a)}{d \ln a} \equiv \Oma^{\gamma}$ is often used to discriminate different models using the linear matter perturbations \cite{Peebles1,Peebles2,Lahav}. Although $\gamma$ is time dependent by its definition even for the simple dark energy models \cite{09051522,09061643,09072108}, the constant value of it can be well matched with some dark energy and modified gravity models \cite{0507263,0608681,0701317,07101092,08024122,08081316}. However, it can be generalized as a time dependent $\gamma(a)$ \cite{9804015,07101510,08032236,09052470,09053444,09084379}.

Behavior of $\gamma$ in the so-called Dvali-Gabadadze-Porrati (DGP) braneworld model \cite{0005016,0010186,0105068} has been widely investigated \cite{08033292,0701317,08024122,09051735,09053444,0401515}. $\gamma$ for a modification of gravitational action with a general function of the scalar curvature instead of the standard Einstein-Hilbert term, named f(R) gravity \cite{Buchdahl} has been also studied \cite{08032236,08093374,09035296,09082669}. In general, $\gamma$ has a scale dependence in this model. Also when one considers the scalar-tensor theories of gravity (STG) \cite{Bergmann,Nordtvedt,Wagoner}, one can obtain the specific $\gamma$ for the certain STG model \cite{07101510,0001066,08024196}.

There is a useful approximate solution for the growth factor within general relativity \cite{0507263} \be \delta_{\m}(a) = a e^{\int_{0}^{a} (da'/a') [\Omega_{\m}(a')^{\gamma} - 1]} \, , \label{Linderg} \ee where $\Oma$ is the matter density contrast, $\delta_{\m} = \delta \rho_{\m} / \rho_{\m}$ is the linear density perturbation of the matter, and $\gamma = 0.55 + 0.05 [ 1 + \omega(z=1)]$ for $\omega > -1$. However, the accuracy of this solution is misinformed. As either $\omega_{0}$ or $\omega_{a}$ increases, the accuracy of the approximate solution given in Eq. (\ref{Linderg}) is decreased. For example, the error of approximate solution is about $1.2 \%$ when one consider ($\oo, \oa$) $=$ ($-0.78, 0.32$). If $\oa$ increases to $0.4$, then the error becomes $2.0 \%$ for the same value of $\oo$.

There are both theoretical and phenomenological motivations for STG. The former is related to the existence a ubiquitous fundamental scalar coupled to gravity in theories which unify gravity with other interactions \cite{Fradkin,Callan,Lovelace,Green,Polchinski}. Also the dynamical equivalence between f(R) theories and a particular class of STG has been shown in the case of metric formalism \cite{Teyssandier,Magnano,9307034,0307338,09100434} as well as in the Palatini formalism \cite{0308111,0604028}. The later have several aspects. First, ``the lithium problem'' in the standard big bang nucleosynthesis (BBN) might be solved in STG due to the slower expansion than in general relativity before BBN, but faster during BBN \cite{0511693,0601299,08111845}. The weak lensing (WL) shear power spectrum in STG predicts the different one compared to in GR because they cause the different growth history of the matter \cite{0503644,0403654,0412120}. Integrated Sachs-Wolfe (ISW) effect probes modified gravities on cosmological scales through the matter potential relation \cite{9906066,08032238,SLAIP,09092045}. The crossing phantom $\omega < -1$ also can be naturally obtained in STG \cite{0504582,0606287,0610092}.

There have been a number of reconstructions of specific STG models which is consistent with known observational constraints \cite{0011115,0107386,0508542,0612569,07053586,08031106,10031686,10061246,10112915}. However, we need to reconstruct theory without any specific theory {\it a priori}. Thus, we use both background and growth history parameters ($\omega, \gamma$) to find the viable subclasses of STG.

We briefly review the basic background evolution equations of STG model in the next section. In Sec. 3, we also review the linear perturbation equations of the model. We derive the reconstruction equations for model functions $F(\phi)$ and $U(\phi)$ as a function of scale factor $a$ and check the viability of specific models in terms of parameters $\omega$ and $\gamma$ in Sec. 4. We conclude in Sec. 5. We also show the accuracy of the approximate solution in Eq. (\ref{Linderg}) for the general values of ($\oo, \oa$) and find the initial values of $\phi'$ and $U$ in the appendix.

\section{Scalar-Tensor Theories of Gravity}
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STG are described in the Jordan frame (JF) by the action \cite{Bergmann,Nordtvedt,Wagoner}
\be S = \fr{1}{16 \pi G_{\ast}} \int d^4 x \sqrt{-g} \Biggl[ F(\phi) R - Z(\phi) \nabla^{\mu} \phi \nabla_{\mu} \phi - 2 U(\phi) \Biggr] + S_{\m}(g_{\mu\nu}, \psi_{\m}) \, , \label{SST} \ee
where $G_{\ast}$ denotes the bare gravitational coupling constant which differs from the measured one, $F(\phi)$ and $Z(\phi)$ are dimensionless, and $U(\phi)$ is the potential of the scalar field $\phi$. $F(\phi)$ needs to be positive to ensure that the gravity is attractive. In the matter action $S_{\m}(g_{\mu\nu},\psi_{\m})$, the matter fields $\psi_{\m}$ is universally coupled to the metric $g_{\mu\nu}$ and all experimental data including Hubble parameter $H$ and redshift $z$ will thus have their usual interpretation in this JF \cite{0009034}.

The evolution equations in the flat Friedmann-Lemaitre-Robertson-Walker (FLRW) metric are given by
\ba && 3 F H^2  = 8 \pi G_{\ast} (\rho_{\m} + \rho_{\rad}) + \fr{1}{2} Z \dot{\phi}^2 - 3 H \dot{F} + U \, , \label{G00} \\ && 2 F \dot{H} = - 8 \pi G_{\ast} (\rho_{\m} + \fr{4}{3} \rho_{\rad}) - Z \dot{\phi}^2 - \ddot{F} + H \dot{F} \, , \label{Gii} \\ && Z \Bigl( \ddot{\phi} + 3 H \dot{\phi} \Bigr) = \fr{1}{2} F_{,\, \phi} R - \fr{1}{2} Z_{,\, \phi} \dot{\phi}^2 - U_{,\, \phi} \, , \label{phieq} \\ && \dot{\rho}_{i} + 3 H ( 1 + \omega_{i}) \rho_{i} = 0 \hspace{0.2in} {\rm with} \hspace{0.2in}  (\omega_{\m} =0 \, \rm{and} \, \omega_{\rad} = 1/3) \, , \label{rhoi} \ea where dots denote the differentiation with respect to (w.r.t) the (JF) cosmic time $t$, $F_{,\phi} = \fr{d F}{d \phi}$, and $R = 6(2H^2 + \dot{H})$ is the Ricci scalar. We limit our consideration after the matter dominated epoch and ignore the radiation component. The effective gravitational constant $G_{\eff}$ between two test masses measured in laboratory Cavendish-type experiments is given by \cite{0001066,Damour} \be G_{\eff} = \fr{G_{\ast}}{F} \Biggl(\fr{2 Z(\phi) F + 4F_{,\, \phi}^2}{2 Z(\phi) F + 3F_{,\,\phi}^2} \Biggr) \, . \label{Geff} \ee This is different from the Newton's gravitational constant $G_{N} = G_{\ast} / F$ as the inverse factor of the curvature scalar $R$. In Eq. (\ref{Geff}), $G_{\ast}/F$ comes from the exchange of a graviton between the two masses, whereas $(G_{\ast}/F) [F_{, \phi}^2/(2 Z F + 3 F_{, \phi}^2)]$ is due to the exchange of a scalar particle between them. When we use the familiar expression for Brans-Dicke (BD) representation, $F = \phi$ and $Z = \omega_{BD}/ \phi$, Eq. (\ref{Geff}) becomes $G_{\eff}^{BD} = G_{\ast} \phi^{-1} (2 \omega_{BD} + 4)/(2 \omega_{BD} + 3) = G_{\ast} \phi^{-1} (1 + \fr{4}{3} \beta^2) $ by using the conversion relation $\beta = \sqrt{\fr{3}{4 (2 \omega_{BD} + 3)}}$ between STG coupling constant and BD parameter \cite{07042421}. We can recover $G_{\eff} = G_{\ast}$ in $\beta \rightarrow 0$ ({\it i.e.} $\omega_{BD} \rightarrow \infty$) limit. $G_{\eff}$ is experimentally bounded
$G_{\eff}(z=0) - G_{N}(z=0) = 0.02 \%$ and  $\Bigl| \dot{G}_{\eff} / G_{eff} \Bigr| < 6 \times 10^{-12} yr^{-1} $ \cite{solar1,solar2,Cassini}. One can always reduce $Z(\phi)$ and $F(\phi)$ to one unknown function by a redefinition of the scalar field and thus we will consider $Z(\phi) = 1$ case. However, this parametrization $Z(\phi) = 1$ can sometimes be singular \cite{0009034}.

There are several features we need to emphasize. First, the positive energy does not imply that $\dot{\phi}^2 > 0$ due to the mixture of tensor and scalar degrees of freedom in the JF. As the same reason, the second derivative of $U$ does not give the precise value of its squared mass. Secondly, the evolution of the scalar field is determined by the effective potential $U_{\eff}(\phi) = U(\phi) - \fr{1}{2} F(\phi) R$ as shown in Eq. (\ref{phieq}). If we consider a light scalar field weakly coupled to matter ($F \sim {\cal O}(1)$ and $F_{,\, \phi} \sim 0$), then at early epoch $U_{\rm{eff}}$ is dominated by $F(\phi) R$-term. Thus, the scalar field is dynamically driven to General Relativity corresponding value ($\phi = 0$) and deviate from it at late epoch when $U_{\eff}$ is approximated by $U(\phi)$.

In order to study the cosmological dynamics of the system, it is convenient to rewrite the evolution Eqs. (\ref{G00})-(\ref{rhoi}) by using the new variable, $n = \ln a$ and normalize the $H^2$ and $H'$ by the present value of $F$ \ba && 3 F_{0} H^2  = 8 \pi G_{\ast} \rho_{\m} + \fr{1}{2} H^2 \phi^{'2} - 3 H^2 F' + 3 H^2 (F_0 - F) + U  \, , \label{G00n} \\ && 2 F_0 H H' = - 8 \pi G_{\ast} \rho_{\m} - H^2 \phi^{'2} - H^2 F'' + (H^2 - HH') F' + 2 HH' (F_0 - F) \, , \label{Giin} \\ && \phi'' + \Biggl( 3 + \fr{H'}{H} \Biggr) \phi' = 3 \Biggl( 2 + \fr{H'}{H} \Biggr) \fr{F'}{\phi'} - \fr{1}{H^2} \fr{U'}{\phi'} \, , \label{phieqn} \\ && \rho_{\m}^{'} + 3 \rho_{\m} = 0 \, , \label{rhoin} \ea where primes denote the differentiation w.r.t $n$, $F_{0}$ means $F(n=0)$ and we only consider the matter component which is relevant to the late-time universe. We will use the above background equations (\ref{G00n}) - (\ref{rhoin}) in followings.

\section{Perturbations}
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In this section, we review the matter density perturbations of STG in the longitudinal gauge w.r.t the JF \cite{0009034,Mukhanov} \be ds^2 = -(1 + 2 \Phi) dt^2 + a^2(1 - 2 \Psi) d \vec{x}^2 \, . \label{LG} \ee Also the energy momentum tensor components of the matter are given by \be T_{0}^{0} = - (\rho_{\m} + \delta \rho_{\m}) \, , \hspace{0.2in} T_{i}^{0} = - \rho_{\m} v_{i} \label{Tm} \ee where $\rho_{m} \, (\delta \rho_{m})$ is the energy density (contrast) of the pressureless matter and $v_{i}$ is its velocity. The gauge invariant quantity is defined as $\delta_{\m} \equiv \fr{\delta \rho_{\m}}{\rho_{\m}} + 3 H v$. The perturbed part of the energy momentum conservation in the Fourier space gives \ba \delta_{\m}' &=& -\fr{k^2}{a^2} \fr{v}{H} + 3 (\Psi + Hv)' \, , \label{dotdelta} \\ v' &=& \fr{\Phi}{H} \, , \label{dotv} \ea where $k$ is a comoving wavenumber.
On the other hand, the first order perturbed Einstein equations give
\ba 3 F' \Phi' + \Biggl( 2 \lambda^{-2} F - Z \phi'^2 + 3 F' \Biggr) \Phi &=& - \Biggl[\fr{8 \pi G_{\ast} \rho_{\m}}{H^2} \delta_{\m} + \Biggl( \lambda^{-2} - 6 - 3 \fr{F'^2}{F^2} \Biggr) \delta F + \fr{\delta U}{H^2} \nonumber \\ && + 3 \fr{F'}{F} \delta F' + Z \phi' \delta \phi' + 3 Z \phi' \delta \phi + \fr{1}{2} \delta Z \phi'^2 \Biggr] \, , \label{dG00} \\ 2 F ( \Psi' + \Phi ) + F' \Phi &=& 8 \pi G_{\ast} \rho_{\m} \fr{v}{H} + Z \phi' \delta \phi + \delta F' - \delta F \, , \label{dG0i} \\ \Psi - \Phi &=& \fr{\delta F}{F} \, ,\label{dGij} \ea where $\lambda^2 = \fr{a^2H^2}{k^2}$. Also the perturbed part of the scalar field equation gives
\ba && \delta \phi'' + \Bigl(3 + \fr{H'}{H} + \fr{Z_{,\phi}}{Z} \phi' \Bigr) \delta \phi' + \Biggl[\lambda^{-2} -3(2 + \fr{H'}{H}) \Bigl( \fr{F_{,\phi}}{Z} \Bigr)_{,\phi} + \fr{1}{H^2} \Bigl( \fr{U_{,\phi}}{Z} \Bigr)_{,\phi} + \Bigl( \fr{Z_{,\phi}}{Z} \Bigr)_{,\phi} \fr{\phi'^2}{2} \Biggr] \delta \phi \nonumber \\ && = \Biggl[\lambda^{-2}(\Phi - 2\Psi) - 3 \Bigl( \Psi'' + (4 + \fr{H'}{H}) \Psi' + \Phi' \Bigr) \Biggr] \fr{F_{,\phi}}{Z} + ( 3\Psi' + \Phi' ) \phi' - 2 \fr{\Phi}{Z} \fr{U_{,\phi}}{H^2} \, . \label{deltaphieq} \ea
From the equations (\ref{dotdelta}) and (\ref{dotv}), we obtain \be \delta_{\m}'' + \Bigl( 2 + \fr{H'}{H} \Bigr) \delta_{\m}' + \lambda^{-2} \Phi = 3 (\Psi + H v)'' + \Bigl( 6 + 3 \fr{H'}{H} \Bigr) (\Psi + H v)' \, . \label{ddotdelta} \ee
We neglect time derivative terms w.r.t spatial derivative terms of corresponding perturbed variables ({\it i.e.} subhorizon limit). This simplification holds at scales $k \ga aH \la 10^{-3} h/$Mpc. In this limit we can write the approximate equations for (\ref{dG00}) and (\ref{deltaphieq}) \ba \lambda^{-2} \Phi &\simeq& - \fr{1}{2F} \Biggl[\fr{8 \pi G_{\ast} \rho_{\m}}{H^2} \delta_{\m} + \lambda^{-2} \delta F \Biggr] \, , \label{dG00app} \\ \delta \phi &\simeq& (\Phi - 2 \Psi) \fr{F_{,\phi}}{Z} \simeq - \fr{F F_{,\phi}}{Z F + 2 F_{\, ,\phi}^2} \Phi \, , \label{deltaphiapp} \ea where we use Eq. (\ref{dGij}) in the second equality of Eq. (\ref{deltaphiapp}). From the above two equations, we have the Poisson's equation \be \fr{k^2}{a^2} \Phi \simeq - 4 \pi G_{\eff} \rho_{\m} \delta_{\m} \, , \label{Poisson} \ee where $G_{\eff}$ is given in (\ref{Geff}). Combining equations (\ref{ddotdelta}) and (\ref{Poisson}) gives \be \delta_{\m}'' + \Bigl( 2 + \fr{H'}{H} \Bigr) \delta_{\m}' - \fr{4 \pi G_{\eff} \rho_{\m}}{H^2} \delta_{\m} \simeq 0 \, . \label{ddotdelta2} \ee We can find the anisotropic parameter $\eta$ defined by $\eta = (\Phi - \Psi)/\Psi$ \cite{07042421} from the equations (\ref{dGij}) and (\ref{deltaphiapp}) \be \eta \simeq - \fr{F_{,\phi}^2}{Z F + 3 F_{,\phi}^2} \, . \label{eta} \ee

\section{Constraints of $F(\phi)$ and $U(\phi)$}
\setcounter{equation}{0}

From the observational viewpoint, it is quite useful to use a parametrization of both the expansion history and the growth factor of the matter perturbation in terms of the EOS $\omega(n)$ and the GIP $\gamma(n)$. Chevallier-Polarski-Linder (CPL) parameterization $\omega = \omega_{0} + \omega_{a} (1 - e^{n})$ uses its present value ($\omega_{0}$) and variation ($\omega_{a}$) and it might be suitable for future observations \cite{0009008,0208512}. The growth factor can be given by $\delta_{\m}(n) = e^{n} g(n)$ where $g(n)$ is given in Eq. (\ref{Linderg}) with $\gamma = 0.55 + 0.05 (1 + \omde (z=1))$\cite{0507263,9804015}. Although this functional form is accurate at certain level, there are several drawbacks in it. We explain the details about these problems in the appendix.

Eq. (\ref{ddotdelta2}) can be rewritten if we use the definition of the GIP $\gamma$ by using $f = \fr{d \ln \delta_{\m}(n)}{d n} \equiv \Omn^{\gamma}$ \cite{Peebles1,Peebles2,Lahav} \ba && \Omn^{2 \gamma} + \Biggl( \gamma' \ln \Omn + \gamma \fr{\Omn'}{\Omn} + 2 + \fr{H'}{H} \Biggr) \Omn^{\gamma} -\fr{3}{2} \fr{F_{0}}{F} \Biggl[ \fr{2F + 4 (F'/\phi')^2}{2F + 3 (F'/\phi')^2} \Biggr] \Omn \nonumber \\ && \simeq  \Omn^{2 \gamma} + \Biggl( \gamma' \ln \Omn + \gamma \fr{\Omn'}{\Omn} + 2 + \fr{H'}{H} \Biggr) \Omn^{\gamma} -\fr{3}{2} \fr{F_{0}}{F} \Omn = 0 \, , \label{geq} \ea where we use the assumption $|F(n)| \gg |F_{, \, \phi}(n)^2|$ in the approximation. Thus, $F(n)$ is given by \ba \fr{F(n)}{F_{0}} &=& \fr{3}{2} \fr{\Omn}{P(n)} \,\,\,\, , {\rm where} \nonumber \\ P(n) &=& \Omn^{\gamma} \Biggl( \Omn^{\gamma} + \gamma' \ln \Omn + \gamma \fr{\Omn'}{\Omn} + 2 + \fr{H'}{H} \Biggr) \label{FoF0} \\ &=& \Omn^{\gamma} \Biggl( \Omn^{\gamma} + \gamma' \ln \Omn - \gamma \Bigl[ 3 + 2 \fr{H'}{H} \Bigr] + 2 + \fr{H'}{H} \Biggr) \, , \nonumber \ea where we use the relation $\Omn' = - (3 +2 H'/ H) \Omn$ in the second equality of $P(n)$. When we adopt CPL $\omega$, then $H^2$ and $H'/H$ are given by
\ba \fr{H^2}{H_0^2} &=& \Omo e^{-3n} + (1 - \Omo) e^{-3(1 + \oo + \oa) n} e^{-3 \oa (1 - e^{n})} \, , \label{H2oH0} \\
\fr{H'}{H} &=& -\fr{3}{2} \Biggl[ 1 + \omega \fr{(1 - \Omo) e^{-3(\oo + \oa)n} e^{-3 \oa (1 - e^{n})}}{\Omo + (1 - \Omo) e^{-3(\oo + \oa)n} e^{-3 \oa (1 - e^{n})}} \Biggr] \, . \label{HpoH} \ea
$F_{0} \simeq 1$ in order to satisfy $G_{\eff}(0) \simeq G_{N}$. After we obtain the functional form of $F(n)$, we can also derive the that of the potential $U(n)$ by using Eqs. (\ref{G00n}) and (\ref{Giin}) \be \fr{U(n)}{F_{0} H_{0}^2} = \fr{1}{2} \fr{H^2}{H_{0}^2} \Biggl( \fr{F''}{F_0} + \Bigl[ 5 + \fr{H'}{H} \Bigr] \fr{F'}{F_0} + 2 \Bigl[ 3 + \fr{H'}{H} \Bigr] \fr{F}{F_0} - 3 \Omn \Biggr) \, . \label{U} \ee The effective equation of state $\omega$ is obtained from the same equations \be \omega = \fr{\phi'^2 + 2 F'' +  2 (2 + H'/H) F' + 4 (F - F_{0}) H'/H + 6 (F - F_{0}) - 2U/H^{2}}{\phi'^2 - 6F' - 6(F - F_{0}) + 2U/H^{2}} \, , \label{omde} \ee where the evolution equation of scalar field $\phi'$ is given from Eq. (\ref{Giin}) \be \phi' = \sqrt{-F'' + \Bigl(1 - \fr{H'}{H} \Bigr) F' - 2\fr{H'}{H} F - 3 F_{0} \Omega_{\rm{m}}} \, . \label{phiprime} \ee Thus, the EOS obtained from Eq. (\ref{omde}) should be same as that of CPL. As long as $F_{0} \simeq 1$ is satisfied, the above constraint is well matched. We obtain the useful recursion relations for the differentiation of $F$ from Eq. (\ref{FoF0}) \ba \fr{F'}{F_0} &=& - \Biggl( 3 + 2 \fr{H'}{H} + \fr{P'}{P} \Biggr) \fr{F}{F_{0}} \, , \label{FpoF0} \\ \fr{F''}{F_0} &=& \Biggl( \Bigl[3 + 2 \fr{H'}{H} + \fr{P'}{P} \Bigr]^2 - 2 \Bigl[ \fr{H'}{H} \Bigr]' - \Bigl[ \fr{P'}{P} \Bigr]' \Biggr) \fr{F}{F_0} \, . \label{FppoF0} \ea

Now we probe the viabilities of some specific models which can mimic some well known dark energy and modified gravity models. We assume that $\gamma = \gamma_0 + \gamma_a (1 - a)$ and $\Omo = 0.3$ in the following analysis. One can always find the constant value of $\gamma$ ({\it i.e.} $\gamma_a = 0$) from Eq. (\ref{FoF0}) by using $F(0)/F_0 = 1$.

\subsection{Comparison with Dark Energy models}
First, we investigate the models which mimic the cosmological constant ($\oo, \oa$) = ($-1.0, 0$) in the background evolution. We can further specify the models by considering the different growth history ({\it i.e.} different value of $\gamma$). When $\gamma_{a} = 0$, $\gamma_{0} \simeq 0.56$ is found to get $F(0) = 1$. However, this gives $(F_{\, , \phi}/\sqrt{F}) |_{0} = -0.2$ which violates the solar system test. The parameter set ($\gamma_{0}, \gamma_{a}$) = ($0.56, -0.012$) gives $F(0) = 1.017$ and $(F_{\, , \phi}/\sqrt{F}) |_{0} = -0.019$ and passes the solar system test. But $\phi'$ becomes imaginary at $n < -0.6$ ({\it i.e.} $z \ga 0.8$) in this case. This is quite similar to the result in Ref. \cite{0009034} where $F(n)/F_0$ is defined as $e^{-2n} f(n)$ with $f(n)$ is a general function of $n$. Thus, we may need to consider general $Z(\phi)$ in order to avoid this singular behavior of $\phi'$ \cite{SLeefu}. Even though the above case ($0.56, -0.012$) might be cured by introducing the nontrivial $Z(\phi)$, it is difficult to be distinguished from the cosmological constant ($\Lambda$) model because the values of both $\omega$ and $\gamma$ are quite similar to those of $\Lambda$ model. Thus, it is worth to check the case when $\gamma$ is quite different from that of $\Lambda$ model. We try with ($\gamma_{0}, \gamma_{a}$) $\simeq$ ($0.6, 0.126$) which gives the quite interesting evolutions of physical quantities. Even though the potential $U(n)$ is negative at present, it is fine because the second derivative of $U(\phi)$ does not give the precise value of its squared mass in JF. We show the evolutions of physical quantities in Fig. \ref{fig1}. As shown in the first column at the first row, $\omega$ obtained from Eq. (\ref{omde}) is exactly same as that of CPL with $\oo = -1.0$ and $\oa = 0$. Thus, if one investigate only the geometrical tests, then this STG theory can not be distinguished from $\Lambda$ model. However, $F(n)/F_0$ can reach to $1.5$ around $n \sim -0.4 - -0.3$ ({\it i.e.} $z \sim 0.3 - 0.4$), which can give some significant effects on ISW or WL. The growth index $f$ obtained from general $\gamma$ (dotted line) is also consistent with the exact solution (solid one). The dashed line in $f$ deviating from the exact solution is the one obtained when one use the constant $\gamma = \gamma_0 = 0.6$. The only problem in this model is that it violates the solar system limit by $F_{\, , \phi} / \sqrt{F} |_{0} \simeq -0.7$. If one release this limit which might be plausible in cosmological scale, then we may have a very interesting STG model which mimics exactly $\Lambda$ model for the background evolution but shows the totally different behavior for the growth history. When we consider $\gamma_0 < 0.56$, the value of $\phi'$ becomes imaginary at the present. Thus, STG with simple form of $Z(\phi) = 1$ may not be consistent with small value of $\gamma_0$ ({\it i.e.} negative $\gamma_a$). The shape of $F(n)/F_0$ is determined by the sign of $\gamma_a$. If $\gamma_a$ is positive (negative), then $F(n)/F_0$ shows the convex (concave) shape with the minimum (maximum) as $1$. Thus, the value of $F(n)$ is bigger than $F_0$ in the past for the viable STG.

\begin{figure}
\centering
\vspace{1.5cm}
\begin{tabular}{ccc}
\epsfig{file=Fig1a.eps,width=0.3\linewidth,clip=} &
\epsfig{file=Fig1b.eps,width=0.3\linewidth,clip=} &
\epsfig{file=Fig1c.eps,width=0.31\linewidth,clip=} \\
\epsfig{file=Fig1d.eps,width=0.3\linewidth,clip=} &
\epsfig{file=Fig1e.eps,width=0.29\linewidth,clip=} &
\epsfig{file=Fig1f.eps,width=0.3\linewidth,clip=} \\
\end{tabular}
\vspace{-0.5cm}
\caption{ a) In the first row, we show the evolutions of $\omega$, $F/F_0$, and $F_{\, , \phi} / \sqrt{F}$ (from left to right) when ($-1.0, 0$) and ($0.6, 0.126$) for ($\oo, \oa$) and ($\gamma_0, \gamma_a$), respectively.  b) The evolutions of $\phi$, $U$, and $f$ for the same values of $\omega$ and $\gamma$ (from left to right) in the second row.} \label{fig1}
\end{figure}

Second, we probe the models which show the similar background evolutions as the some coupled quintessence models ($\oo, \oa$) = ($-1.0, 1.0$). In these models, $\omega = 0$ during the tracking region and it approaches to $-1$ at present \cite{9904120,0601333}. Again we find $\gamma_{0} \simeq 0.56$ for $\gamma_{a} = 0$ to get $F(0) = 1$. However, these values of STG model can not pass the solar system test because $(F_{\, , \phi}/\sqrt{F}) |_{0} = -0.17$. STG with other set of parameters ($\gamma_{0}, \gamma_{a}$) $\simeq$ ($0.562, 0.006$) gives $F(0) = 1.00$ and $(F_{\, , \phi}/\sqrt{F}) |_{0} = -0.02$. Also $\phi'$ well behaves in this case. Thus, this model satisfy all known observational constraints. We show the evolutions of physical quantities of this in Fig. \ref{fig2}. Again $\omega$ obtained from Eq. (\ref{omde}) is exactly same as CPL $\omega$ with $\oo = -1.0$ and $\oa = 1.0$. $F(n)$ decreases during the evolution which is opposite to the previous case even though $\gamma_a > 0$. However, this is only possible when $\gamma \simeq 0$. The growth index $f$ obtained from general $\gamma$ (dotted line) is also consistent with the exact solution (solid line). Again $f$ with constant value of $\gamma_0 = 0.562$ is deviated from the exact one. For ($\gamma_{0}, \gamma_{a}$) $\simeq$ ($0.6, 0.126$),  $F(n)/F_0$ increases to $1.1$ around $n \sim -0.4$ ({\it i.e.} $z \sim 0.4$). This case also violates the solar system limit by $F_{\, , \phi} / \sqrt{F} |_{0} \simeq -0.45$.

\begin{figure}
\centering
\vspace{1.5cm}
\begin{tabular}{ccc}
\epsfig{file=Fig2a.eps,width=0.3\linewidth,clip=} &
\epsfig{file=Fig2b.eps,width=0.3\linewidth,clip=} &
\epsfig{file=Fig2c.eps,width=0.31\linewidth,clip=} \\
\epsfig{file=Fig2d.eps,width=0.3\linewidth,clip=} &
\epsfig{file=Fig2e.eps,width=0.29\linewidth,clip=} &
\epsfig{file=Fig2f.eps,width=0.3\linewidth,clip=} \\
\end{tabular}
\vspace{-0.5cm}
\caption{ a) In the first row, we show the evolutions of $\omega$, $F/F_0$, and $F_{\, , \phi} / \sqrt{F}$ (from left to right) when ($-1.0, 1.0$) and ($0.562, 0.006$) for ($\oo, \oa$) and ($\gamma_0, \gamma_a$), respectively.  b) The evolutions of $\phi$, $U$, and $f$ for the same values of $\omega$ and $\gamma$ (from left to right) in the second row.} \label{fig2}
\end{figure}

In Table \ref{table1}, we show the behaviors of physical quantities for various models with some parameter sets. There have been various quintessence models \cite{0604602} but we just investigate the inverse power-law potentials ($\phi^{\alpha}$) \cite{Ratra,9809272} with $\alpha = 1$ which is well approximated by $\oo = -0.74$ and $\oa = 0.07$. STG for the same values of $\oo$ and $\oa$ with $\gamma_0 = 0.57$ is hardly distinguished from the $\phi^{-1}$ quintessence model because $f$ of both models are quite similar to each other. $F(n)/F_0$ reaches to the maximum value $1.015$ and then approaches to $1$ at early time. No known observation can distinguish this from $\phi^{-1}$ quintessence model. If ($\gamma_0, \gamma_a$) are ($0.6, 0.08$) for the same $\omega$, then the maximum value of $F(n)/F_0$ is $1.15$ which can give some effects on ISW and WL. Also the time varying growth index parameter can be distinguished from the constant one. We also investigate the model inspired by the supergravity (SUGRA) \cite{0208156}. The background evolution of SUGRA can be parameterized by ($\oo, \oa$) $=$ ($-0.92, -0.08$). Again, only STG with $\gamma_0 = 0.6$ with $\gamma_a = 0.11$ can give some significant deviations from SUGRA for the growth history. We also check the phantom crossing models in this table. Phantom crossing I means the model with $\omega > -1$ in the past becomes $\omega < -1$ at present. Phantom crossing II indicates the other model where $\omega < -1$ in the past and $\omega > -1$ at present. The results do not change much for these cases. From this table, we find that only STG models with the high values of $\gamma_0$ can be distinguished from the other models. However, all of high values of $\gamma_0$ STG models violate the solar system test.

\begin{center}
    \begin{table}
    \begin{tabular}{ | c | c | c | c | c | c | c | c |  }
    \hline
      $\rm{Models}$ & $\oo$  & $\oa$ & $\gamma_0$ & $\gamma_a$& $F(n)/F_0$ & $F_{\, , \phi}/\sqrt{F} |_0$ & $\phi'$ \\ \hline
      $ $ & $$  & $$ & $0.56$ & $-0.018$& $\bigcup$ \rm{min} $0.986$ & $0.018$ & \rm{fine}  \\ \cline{4-8}
      $V(\phi) \propto \phi^{-1}$ & $-0.74$  & $0.07$ & $0.57$ & $0$& $\bigcap$ \rm{max} $1.015$ & $-0.09$ & \rm{fine}  \\ \cline{4-8}
      $ $ & $ $  & $ $ & $0.6$ & $0.08$& $\bigcap$ \rm{max} $1.150$ & $-0.48$ & \rm{fine}  \\ \hline
      $ $ & $$  & $$ & $0.56$ & $-0.016 $& $\nearrow$ \rm{max} $1.01$ & $0.00$ & $z < 1.3$  \\ \cline{4-8}
      $\rm{SUGRA}$ & $-0.92$  & $-0.08$ & $0.563$ & $0$& $\bigcap$ \rm{max} $1.02$ & $-0.18$ & \rm{fine}  \\ \cline{4-8}
      $ $ & $ $  & $ $ & $0.6 $ & $0.11 $& $\bigcap$ \rm{max} $1.14$ & $-0.70$ & \rm{fine}  \\ \hline
      Phantom & $$  & $$ & $0.53$ & $-0.09 $& $\bigcup$ \rm{min} $0.93$ & $\rm{none}$ & imaginary  \\ \cline{4-8}
      Crossing & $-1.1$  & $0.3$ & $0.557$ & $0$& $\bigcap$ \rm{max} $1.01$ & $-0.24$ & \rm{fine}  \\ \cline{4-8}
      I & $ $  & $ $ & $0.6$ & $0.143$& $\bigcap$ \rm{max} $1.15$ & $-0.68$ & \rm{fine}  \\ \hline
      Phantom & $$  & $$ & $0.55$ & $-0.049 $& $\bigcup$ \rm{min} $0.97$ & none & imaginary  \\ \cline{4-8}
      Crossing & $-0.8$  & $-0.3$ & $0.568$ & $0$& $\bigcap$ \rm{max} $1.03$ & $-0.18$ & $z < 3$  \\ \cline{4-8}
      II & $ $  & $ $ & $0.6$ & $0.09 $& $\bigcap$ \rm{max} $1.13$ & $-0.69$ & $z < 7$  \\ \hline
    \end{tabular}
    \caption{Physical quantities for various models. $\bigcup$ ($\bigcap$) means the concave (convex) shape of $F(n)/F_0$. Also $\nearrow$ indicates the monotonic increase of $F/F_0$ as $n$ increases. $\phi'$ becomes imaginary after the maximum $z$ for certain parameter set. }
    \label{table1}
    \end{table}
\end{center}

\subsection{Comparison with DGP model}

DGP model \cite{0005016,0010186,0105068} is one of the well studied modified gravity models. The background evolution of this model can be parameterized by ($\oo, \oa$) $=$ ($-0.78, -0.32$) with $\gamma_0 = 11/16$ \cite{0507263}. In Ref. \cite{08024122}, $\gamma_0 = 4/7$ at high $z$. We show the evolutions of physical quantities of STG with ($\gamma_0,\gamma_a$) $=$ ($11/16, 0.32$) in Fig. \ref{fig3}. Again except the solar system constraints, this model shows the interesting and different behaviors compared to DGP model ($\gamma_a = 0$) for the growth history. $F_{\, , \phi}/F |_0$ becomes very big negative value and this is due to the fact that $\phi'$ approaches to $0$ at present which is used in $F_{\, , \phi} = F' / \phi'$. Usually, $f$ is smaller than $1$ in general DE and MG models. However, we can produce $f > 1$ for $\gamma_0 < 0.5$ with non-vanishing $\gamma_a$ models even though $\phi'$ is imaginary. If observations do confirm this fact ($f > 1$), then this kind STG might be a useful candidates to explain it.

\begin{figure}
\centering
\vspace{1.5cm}
\begin{tabular}{ccc}
\epsfig{file=Fig3a.eps,width=0.3\linewidth,clip=} &
\epsfig{file=Fig3b.eps,width=0.3\linewidth,clip=} &
\epsfig{file=Fig3c.eps,width=0.31\linewidth,clip=} \\
\epsfig{file=Fig3d.eps,width=0.3\linewidth,clip=} &
\epsfig{file=Fig3e.eps,width=0.29\linewidth,clip=} &
\epsfig{file=Fig3f.eps,width=0.3\linewidth,clip=} \\
\end{tabular}
\vspace{-0.5cm}
\caption{ a) In the first row, we show the evolutions of $\omega$, $F/F_0$, and $F_{\, , \phi} / \sqrt{F}$ (from left to right) for STG model with ($\gamma_0, \gamma_a$) $=$ ($11/16, 0.32$).  b) The evolutions of $\phi$, $U$, and $f$ for the same values of $\omega$ and $\gamma$ (from left to right) in the second row.} \label{fig3}
\end{figure}

We show the current observational limits on $f$ and $\gamma$ in Table \ref{table2}. $\gamma$ value is obtained from $f^{\rm{obs}}$ when we assume $\Lambda$ model. The current observations may be consistent with $\Lambda$ model except the Lyman-$\alpha$ forest result \cite{0407377}. However, there exist huge errors in observations and it might be too early to extract any physical properties for specific models.

\begin{center}
    \begin{table}
    \begin{tabular}{ | c | c | c | c | c | c | }
    \hline
      $z_{\ast}$ & $n_{\ast}$  & $\Omo$ & $f^{\rm{obs}}$ & $\gamma^{\rm{obs}}$ & Ref \\ \hline
      $0.15$ & $-0.14$ & $0.3$  & $0.51 \pm 0.11$ & $0.72^{+ 0.26}_{- 0.21}$ & 2dFGRS \cite{0112161,0212375} \\ \hline
      $0.32$ & $-0.28$ & $0.26 $  & $0.654_{-0.132}^{+0.185}$ & $0.52^{+0.28}_{-0.31}$ & SDSS R$= 10-50 h^{-1}$ Mpc \cite{10032185} \\ \cline{4-6}
      $ $ &  & $\pm 0.02$ & $0.641_{-0.134}^{+0.191}$ & $0.55^{+0.29}_{-0.32}$ & R$= 2-50 h^{-1}$ Mpc  \\ \hline
      $0.35$ & $-0.3$ & $0.3$  & $0.70 \pm 0.18$ & $0.54^{+ 0.45}_{- 0.34}$ & SDSS \cite{0608632} \\ \hline
      $0.55$ & $-0.44$ & $0.3$ & $0.75 \pm 0.18$ & $0.59^{+ 0.60}_{- 0.44}$ & 2dF-SDSS \cite{0612400} \\ \hline
      $1.4$ & $-0.88$ & $0.3$  & $0.90 \pm 0.24$ & $0.68^{+ 2.0}_{- 1.5}$ &  2dF-SDSS \cite{0612401} \\ \hline
      $3.0$ & $-1.39$ & $0.3$  & $1.46 \pm 0.29$ & $-10.6^{+ 6.2}_{- 5.1}$ & Ly-$\alpha$ (SDSS) \cite{0407377} \\ \hline
    \end{tabular}
    \caption{$z_{\ast}$ is the corresponding redshift for each observation. $\gamma^{\rm{obs}}$ is the derived quantities from the observational value of $f^{\rm{obs}}$ when we assume $\Lambda$ model ($\omega = -1$). }
    \label{table2}
    \end{table}
\end{center}

\section{Conclusions}
\setcounter{equation}{0}

Scalar-tensor gravities theories can produce many possible background evolutions which mimic dark energy models and other modified gravity models. We need to consider the growth of the linear matter perturbation to distinguish between models. However, STG models are strongly limited by the solar system constraint when we normalize the kinetic energy term $Z(\phi) = 1$. The main reason for this is that $\phi'$ becomes singular with this normalization. Thus, we may need to investigate the STG models with general $Z(\phi)$ in order to distinguish STG model with others.

When we allow the time variation of the growth index parameter $\gamma$, usually the negative value of $\gamma_{a}$ models have the singular problem of $\phi'$. Some models with the positive $\gamma_{a}$ have the interesting features like large enough $F/F_0$ values at early epoch while mimic the dark energy models background evolution. However, these cases violate the solar system test and again this might be able to be cured when we consider STG models. If $\gamma_a$ is positive (negative), then $F(n)/F_0$ shows the convex (concave) shape with the minimum (maximum) as $1$. Thus, the value of $F(n)$ is bigger than $F_0$ in the past for the viable STG. There can be exception for this case, when $\gamma_a \simeq 0$ but positive.

The main conclusion is that the viable STG models with $Z(\phi) = 1$ are not distinguishable from dark energy models or other modified gravity models when we strongly limit the solar system constraint.

redpajama_set_name: RedPajamaArXiv


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Car manufacturer and the largest passenger car exporter Hyundai Motor India Ltd is all set to launch its much awaited Global SUV-CRETA tomorrow, riding high on the news of more than 10,000 pre-bookings.
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Rocky & Amanda had an amazing East Indian wedding which took place in Winnipeg but if that wasn't enough they decided to invite their close friends and family to Mexico for another ceremony and another week of partying. It was such a great privilege to witness and document all the love between these two families and the tight group of brothers and sisters they call friends. There wasn't a moment wasted… if there was a chance to dance they danced… or a moment to grab the mic and sing… they sang! This wedding was almost 2 weeks of festivities What a fun and memorable time together. I hope you guys enjoy some of these moments put together from the Winnipeg wedding. Also a special thanks to Curtis from Moore Photography for helping out on this wedding. You're awesome buddy.