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Gabe Newell reportedly worth $5.5 billion
Ana Valens
Valve cofounder and CEO Gabe Newell has made a name for himself in gaming as an incredibly successful programmer, publisher, and industry leader. And that reputation is paying off. Forbes revealed earlier today that Newell is one of the top 100 people on the Forbes 400 list, with a net worth resting at $5.5 billion.
Newell ranks at No. 97 on the Forbes 400 list, according to Forbes' latest update. He's No. 43 for the globe's richest person in tech, No. 427 for the world's richest billionaires, and No. 146 for billionaires within the United States. In short, Newell is pretty successful, and he's actually one of the most wealthy men in gaming today.
This isn't Newell's first time on the Forbes 400, of course. He first hopped on in September 2015, when his net worth jumped to $2.2 billion. As late as March, his net worth rested at $4.1 billion, but it's since skyrocketed further into $5.5 billion. In other words, Newell's company is doing quite well, thanks in part to Steam's success as a gaming distribution service.
It's unclear where Valve is headed in the near future. But based on Newell's previous growth, it's clear his net worth will only increase as the years go on.
H/T Forbes
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I don't know if you got the memo - but THIS IS IT! We've got a front row seat for the collapse of the social order, the smashing of governments and institutions alike, to watch cataclysmic natural disasters punishing the confused and the helpless, who are left to fend for themselves in a shattered world, burning old newspapers for warmth and banding together in crude tribes to wage primitive war over a can of beans or the last surviving dairy cow. It's the End Times right now, and you probably thought things were fine. Well, we've known it was coming for a while now.
Just look at this. Decades ago we saw the rot creeping in, and what did we do about it? Nothing. We sat idly by and let all this happen. We stuck our heads in the sand and we stuck these comics into twenty-five cent bins, festering open sores of corruption contaminating everything they touched (which, for years, was a copy of "Kickers, Inc" and an issue of a Charlton "Beetle Bailey" with the back cover ripped halfway off). We let anybody with a marker and some paper and a pile of Teenage Mutant Ninja Turtles rip-off comics, themselves an indictment of our entire civilization 1600-present, we let these people make their own comics. And now we're paying the price.
How could we let this pass? This half-assed - I can't even give it half an ass, this one-eighth assed "parody" of a "parody" of a "parody" starring the angry bear, the one-eyed bear, the other angry bear, and the other one-eyed bear, oh, I get it, somebody had a book of Popcorn Classics Hollywood Legends checked out of their school library, and somebody else suffered a traumatic brain injury and thereafter thought that merely referencing things equals comedy. That's how the world ends, people.
"O.K. people this is a hijack. And just in case you doubt that this is a subway train hijack, here's a a panel of nothing but a skull mask that appears to have a beard and a moustache and little sideburns, silently hanging in the void, absent of context or meaning in the larger narrative, which would make this a hijack not of a subway train, but of logic, coherence, and the ability of humans to communicate meaningfully with each other."
I don't really like to spend a lot of time insulting the artwork in these books, because let's face it, drawing a comic book is hard work. And that overhead angle business, everybody tries it and nobody can make it work, better artists than us have tried and failed, no shame, but people keep trying it anyway because people are stupid. But this hand here, this hand here is an abomination because I'm pretty sure the person who drew this comic had at least one hand and at least one eye, and yet, couldn't be bothered to use their eye to look at their hand and draw what they saw. That's why we're in the mess we're in, because people can't just sit down and draw what they see. Just draw what you see, people!
Armed robbery is always more threatening when delivered by masked thugs, and when all the dialog has quotation marks. You know that the mere fact of enclosing dialog in speech balloons obviates the need for quotation marks, right? Oh, you don't know that? Well now you do.
Call the experts for Subway emergencies! Frank can fix the bread slicer and Bob is a whiz at the soda dispenser and if listeria poisoning from poorly sanitized food prep surfaces is a problem then Steve is your man! If your problem is a Subway franchise on every freaking block in every city on Earth, well, they can't help you. You'll have to call an angry koala bear, because as we all know, "A problem We are the solution" is their trademark, their confusing, poorly worded trademark.
FINALLY someone among the subway passengers with the guts to stand up to these masked thugs and say "your not going to get away with this" without going on to explain exactly what the "your" is in reference to! Your hat? Your gang? Your hamster? Who knows? The criminals will be confused and disoriented by his bad grammar!
Crashing through the giant subway car windows into the empty, cavernous spaces of your average subway car, our Middle Aged Government Tested Atom Splitting Radio Active Democratic Left Handed Freelance Green Beret Koala Bears are on the scene, brandishing their own special weapons and hollering their battle cry, "We Will." They sure do!
It's an amazing demonstration of brutal martial arts combat as our heroes forget they were holding guns and instead smack the criminals with their soft, furry paws while they try in vain to remember tough-guy dialog from shitty action movies.
Of course the hijackers have to give up, they didn't bring bullets for their guns. It's not armed robbery if the pistol isn't loaded! (actually it may be, consult local laws before attempting robberies)
Oh, it's a big threat from a one-eyed koala bear with human arms and legs and a surprisingly tiny gun. Finally, somebody who isn't compensating for something that they may suspect doesn't measure up. And as we can see from the next panel, these guns are back where they belong - in the hands of angry subway vigilantes!
So this is the very next panel - a bakery, a confusing caption seemingly embedded into a street, and silhouettes of the Middle Aged Government Tested Atom Splitting Radio Active Democratic Left Handed Freelance Green Beret Koala Bears mouthing beer advertising slogans as they vanish from history forever. Again we're forced to ask, where were the grownups when this was made? Did nobody look at this at any stage of the production process - writing, pencilling, inking, lettering, shooting the negatives, burning the plates, putting the plates onto the press, kicking out a few prints to check for registration errors or hickeys, running the booklet maker, boxing and shipping and distribution and the physical placement of this comic onto the shelves of America's comic book retailers - and say, wow, this is embarrassing for our industry and for Western civilization as a whole, we shouldn't allow this physical object to continue to exist because it brings shame upon us and our forefathers and upon generations to come, let us purge it with fire? No. Nobody said this. And that's why we're in the mess we're in.
Well, there's nothing we can do about it now other than shave our hair into mohawks, smear grease onto our faces, and roar off into the wastelands to live brutal lives stripped to the bare essentials of survival. Thanks, comics. Thanks a lot.
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Im Jahr 1977 wählte die National Academy of Sciences der Vereinigten Staaten 75 Personen zu ihren Mitgliedern.

Neugewählte Mitglieder

Weblinks
 1977 gewählte Mitglieder der National Academy of Sciences

Liste (Mitglied der National Academy of Sciences)

redpajama_set_name: RedPajamaWikipedia


Stem cell exhaustion, as explained in the Hallmarks of Aging, is the age-related deficiency of stem cells. This particular hallmark is directly responsible for many of the physical problems associated with aging, such as frailty and a weakened immune system.
As explained by our article about epigenetic alterations, while every cell in your body has the same genetic code, regions of DNA are turned off and on in each one, allowing us to have many unique cell types. While normal cells cannot change their epigenetic settings very easily, stem cells have greater freedom, allowing them, in some cases, to turn into effectively any cell type in the body.
Stem cells perform a wide range of functions, including beneficial signaling that improves tissue function, regulation and health  as well as the replacement of damaged or lost red blood cells , white blood cells , and solid tissues .


Dr. Paul F. Carey, D.C.
Dr. Paul Carey was born and raised in Dublin, Ohio. He presides in Athens with his wife, Audrey, and their four children. Dr. Carey began his career at Palmer College of Chiropractic where he completed his undergraduate instruction. He has been in practice for seventeen years, after graduating with honors from Palmer College of Chiropractic in 1999.
Dr. Carey is board certified by the National Board of Chiropractic Examiners and The Ohio State Chiropractic Board. He is board eligible for a Diplomate in Spinal Rehabilitation. He is a member of the American Chiropracic Association, the Ohio State Chiropractic Assocciation.
Dr. Carey has completed advanced studies in Motion Palpation, Cox Flexion/Distraction Techniques, rehabilitation, and sports injuries.


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VERA FILES FACT CHECK: Duterte flip-flops on family's wealth
Responding to Sen. Antonio Trillanes IV's allegations that he had P2 billion in bank deposits over a period of nine years until 2015, President Rodrigo Duterte is now tweaking his narrative from being born to a poor family and growing up "in the slums" and is now saying his family was and is not poor.
In a recorded video released by the Presidential Communications Operations Office and RTVMalacanang Thursday, Duterte said they are not poor and reminded Trillanes that his father, Vicente Duterte, was a governor of Davao.
"Ngayon, kung pamilya mo gutom noon o ngayon, huwag mo kaming isali. Hindi kami kasing malas sa pamilya mo. Hindi kami mahirap rin. Tatay ko governor noon, may iniwan sa amin. Ikaw? Anong naiwan sa iyo? Hangin pati yabang. Tulisan ka, sa totoo lang (Don't look at my family if yours starved or is still starving. We are not as unfortunate as your family. We are also not poor. My father was a governor, and he left us with something. How about you, what did (your father) leave you? Air and arrogance. You're a bandit, that's the truth)."
(Source: President Rodrigo Duterte's response to Sen. Antonio Trillanes IV's bank account allegations, watch from 2:50 to 3:22, or read transcript)
The president previously stated in various interviews and speeches that he was born to a poor family. In fact, the statement above directly contradicts what he told the audience at an environmental summit in Mindanao on Aug. 4 2016.
He did say that their life became comfortable when his father became governor but added they went back to their previous situation when his father died.
"But in 1956 my father built a house there, kasi tubig nga (because it was water). It was on stilts. Would you believe it? It was demolished because somebody owned the water and the soil. Kaya ho ako lumaki na merong (That's why I grew up with)… there were times when comfort was there when my father became governor. But after back to kami sa (we were back to)… namatay eh (because he died)."
(Source: Speech of President Rodrigo Duterte during the Mindanao Environmental Summit "Oya Mindanaw", Martin Hall, Ateneo de Davao University Main Campus, Jacinto Street, Davao City, watch from 35:51 to 36:27 or read the transcript)
In his speech before the Filipino community in Singapore on Dec. 16, 2016, he said the left would not leave him despite their resistance to his war on drugs because he is the "first left-leaning President of the Republic of the Philippines."
"Pero kailan man, I'm just a socialist. Anak lang ako ng mahirap eh. Anak lang ako ng migrant sa Mindanao. Ang tatay ko galing Cebu… Paano ako magkaroon ng mindset na isip mayaman? So always ang ano ko is 'yung namulatan ko sa mata ko ang hirap (I will forever be a socialist because I was born poor. I'm just the son of a migrant to Mindanao. My father came from Cebu…How can I have a mindset of the rich? So I was made aware of poverty from a young age)."
(Source: Speech of President Rodrigo Duterte during the Meeting with the Filipino Community in Singapore, The Max Pavilion and Hall 9, watch from 47:05 to 47:30)
In another speech on Sept. 12, 2016, during the oath-taking of his appointees in Malacañang, Duterte said he had a limited circle to choose from for appointments to various offices. He just chose honest people he knew from school.
"It's a very limited arena because sila rin ang kilala ko noon. Maraming honest na military. The problem is I do not know them. So 'yung mga honest na dumaan doon, 'yung mga classmate ko sa dormitoryo dito, pati 'yung sa eskwelahan ko, 'yun ang mga tao na…Hindi naman ako imbitado dito sa Maynila ng mga social gathering. I was nobody. Who would ever invite me doon sa debut ni, debut, debut, debut? Wala kami noon. Mahirap lang kami. [inaudible] kung sino kami (It's a very limited arena because they are also the ones I knew then. There are many honest people in the military. The problem is I do not know them. That's why those honest people who went there, my classmates in the dormitory here, including the schools I went to, those are the people that…I wasn't invited here in Manila during social gatherings. I was nobody. Who would ever invite to someone's debut, debut, debut, debut? We had nothing then. We were poor. [inaudible] who we are)."
(Source: Speech of President Rodrigo Duterte during the oath-taking of presidential appointees, Heroes Hall, Malacañang, Sept. 12, 2016)
Trillanes' challenge Thursday was a follow-up of his exposé made during the last few weeks of the 2016 presidential campaign that Duterte's joint account with daughter Davao City Mayor Sara Duterte-Carpio at the Bank of the Philippine Islands account on Julia Vargas, Ortigas Center has been a recipient of some P2 billion deposits from 2006 to 2014, which were not declared in his Statement of Assets, Liabilities and Net Worth.
Trillanes also said Duterte has joint accounts with other members of his family including his common law wife, Cielito "Honeylet" Avanceña, running to hundreds of millions of pesos.
Duterte fact-check Fact check Trillanes SALN Wealth
Feb 20, 2017, 7:46 PM
Trillanes to Duterte: sign waiver of bank secrecy law addressed to BPI
The public should be more discerning this time with President Duterte's bluster when confronted with…
Ellen T. Tordesillas
VERA FILES FACT CHECK: Multimillionaire Duterte says 'I am not a millionaire'
President Rodrigo Duterte said "Ako hindi ako milyonaryo (I am not a millionaire)." Is it the truth?
The 'garbage' continues to stink
When then presidential candidate Rodrigo Duterte dismissed as "garbage" the exposé of Sen. Antonio…


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1332-14. Giant portrait of a former emir Hamad bin Khalifa Al Thani on Ezdan Tower in West Bay. Doha, Qatar, February 1, 2014
Giant portrait of a former emir Hamad bin Khalifa Al Thani on a top section of Ezdan Tower in West Bay. Doha, Qatar, February 1, 2014
Giant portrait of a former emir Hamad bin Khalifa Al Thani on a wall of Ezdan Tower in West Bay. Doha, Qatar, February 1, 2014
Giant portrait of emir Tamim bin Hamad Al Thani on a top section of Ezdan Tower in West Bay. Doha, Qatar, February 1, 2014
Giant portrait of a former Emir His Highness Sheikh Hamad bin Khalifa Al Thani on a wall of Ezdan Hotel at evening, view from Al Adaid Street in West Bay. Doha, Qatar, March 28, 2014
Workers on construction of QP Building gathering under a giant portrait of emir Tamim bin Hamad Al Thani on Ezdan Tower in West Bay. Doha, Qatar, February 1, 2014
Giant portrait of a former Emir His Highness Sheikh Hamad bin Khalifa Al Thani on a wall of Ezdan Hotel at evening dusk, view from Al Adaid Street in West Bay. Doha, Qatar, March 28, 2014
Giant portrait showing wise leadership of the former Emir His Highness Sheikh Hamad bin Khalifa Al Thani on a wall of Ezdan Hotel, view from Al Adaid Street in West Bay. Doha, Qatar, March 28, 2014
Portrait of a former Emir His Highness Sheikh Hamad bin Khalifa Al Thani on a wall of Ezdan Hotel, view from Al Adaid Street in West Bay. Doha, Qatar, March 28, 2014
Giant portrait showing wise leadership of Heir Apparent His Highness Sheikh Tamim bin Hamad Al Thani (now emir) on a wall of Ezdan Hotel, view from Al Adaid Street in West Bay. Doha, Qatar, March 28, 2014
Portraits of emir HH Sheikh Tamim Bin Hamad Al-Thani and his father Hamad bin Khalifa Al Thani in a desert at a roundabout near the entrance of North Camp (Qatari army). Northern Qatar, February 13, 2016
Portraits of emir Hamad bin Khalifa Al Thani and heir apparent shaikh Tamim bin Hamad Al Thani on a door in Umm Wishah Street in Musheirib area. Doha, Qatar, April 13, 2012
Portraits of emir Tamim and his father Hamad bin Khalifa Al Thani on roadside in desert near Abu Sidra in north-western Qatar, December 6, 2014
Portraits of emir Tamim and his father Hamad bin Khalifa Al Thani at the entrance of village of Abu Sidra in north-western Qatar, December 6, 2014
Portraits of emir Tamim and his father Hamad bin Khalifa Al Thani on roadside near Wadi Bu Sidra Al Gharbi in north-western Qatar, December 6, 2014
A.S. with a portrait of an emir in Sheikh Faisal Bin Qassim Al Thani Museum near Al-Shahaniya. Doha, Qatar, February 15, 2014
Portrait of an emir(?) in Sheikh Faisal Bin Qassim Al Thani Museum near Al-Shahaniya. Doha, Qatar, February 15, 2014
Palace of Sheikh Khalifa bin Hamad on a beach, view from a balcony of Room 2303 of ASAS Tower West. Doha, Qatar, February 12, 2011
Commercial Bank in West Bay, with a giant portrait of emirs. Doha, Qatar, December 20, 2014
Ezdan Hotel and Al Qassar Tower at Al Betra Street in West Bay. Doha, Qatar, February 6, 2014
Ezdan Hotel and Pregnant Tower at Al Betra Street in West Bay. Doha, Qatar, February 6, 2014
Portrait gallery in Sheikh Faisal Bin Qassim Al Thani Museum near Al-Shahaniya. Doha, Qatar, February 15, 2014
Ezdan Hotel from the foot of Pregnant Tower at Al Betra Street in West Bay. Doha, Qatar, February 6, 2014
Pregnant Tower and Ezdan Hotel at Al Betra Street in West Bay at evening, looking up. Doha, Qatar, February 6, 2014
Portrait of a sheikh in Sheikh Faisal Bin Qassim Al Thani Museum near Al-Shahaniya. Doha, Qatar, February 15, 2014
Commercial Bank in West Bay, with a giant portrait of a pair of emirs. Doha, Qatar, December 18, 2015
Portrait of emir in Souq Waqif (Old Market). Doha, Qatar, March 9, 2013
Hamad Bin Khalifa Student Center on campus of Education City at evening. Doha, Qatar, March 4, 2012
Illuminated terrace of Hamad Bin Khalifa Student Center in Education City campus. Doha, Qatar, March 4, 2012
Low lying beach palace for wife emir Sheikha Mozah bint Nasser Al Missned, view from a balcony of Room 2303 of ASAS Tower West. Doha, Qatar, February 12, 2011
Olympic Tower and Ezdan Hotel in West Bay from Room 1604 of Dareen Tower. Doha, Qatar, November 19, 2013
Toothbrush tree (Salvadora persica) on a fence of Sheikh Hamad Bin Khalid Bin Hamad Al-Thani Palace at Al Rayyan Al Jadeed Street, near Huwar Street (Al Attiya) Roundabout. Doha, Qatar, October 18, 2015
Toothbrush tree (Salvadora persica) hanging from a fence of Sheikh Hamad Bin Khalid Bin Hamad Al-Thani Palace at Al Rayyan Al Jadeed Street, near Huwar Street (Al Attiya) Roundabout. Doha, Qatar, October 18, 2015
Area of Ezdan Hotel at Al Betra Street in West Bay. Doha, Qatar, February 6, 2014
Buildings around Ezdan Hotel at Al Betra Street in West Bay at evening, looking up. Doha, Qatar, February 6, 2014
Ezdan Hotel and unoccupied buildings at Al Betra Street in West Bay at evening. Doha, Qatar, February 6, 2014
Olympic Tower and Ezdan Hotel in West Bay. Doha, Qatar, January 30, 2012
Ezdan Hotel and Golden Bay Tower in West Bay. Doha, Qatar, January 31, 2012
Al Qassar Tower and Ezdan Hotel in West Bay. Doha, Qatar, January 31, 2012
Navigation Tower in West Bay from a balcony of Room 1703 of Dareen Tower. Doha, Qatar, February 3, 2014
Burj Qatar, former named after a cousin of the Emir, His Excellency Sheikh Saoud Bin Mohammed Bin Ali Al Thani. Doha, Qatar, January 18, 2010
International Islamic Tower in West Bay from a balcony of Room 1703 of Dareen Tower. Doha, Qatar, February 1, 2014
Top section of Tornado Tower in West Bay from a balcony of Room 1703 of Dareen Tower. Doha, Qatar, February 1, 2014
Ezdan Hotel from 30-th floor of Dareen Tower in West Bay. Doha, Qatar, April 29, 2013
Olympic Tower, Al Qassar, and Ezdan Hotel in West Bay. Doha, Qatar, January 31, 2012
Al Qassar, Ezdan Hotel, and Olympic Tower in West Bay. Doha, Qatar, January 30, 2012
Top section of Tornado Tower in West Bay at evening from a balcony of Room 1703 of Dareen Tower. Doha, Qatar, February 1, 2014
Top section of International Islamic Tower in West Bay from a balcony of Room 1703 of Dareen Tower. Doha, Qatar, February 1, 2014
Tower No. 3 of Ezdan Hotel and Suites in West Bay during dust storm. Doha, Qatar, April 2, 2015
Area of Olympic Tower in West Bay in morning dusk from a balcony of Room 1703 of Dareen Tower. Doha, Qatar, February 4, 2014
Area of Navigation Tower in West Bay in morning dusk from a balcony of Room 1703 of Dareen Tower. Doha, Qatar, February 4, 2014
Middle section of International Islamic Tower in West Bay from a balcony of Room 1703 of Dareen Tower. Doha, Qatar, February 3, 2014
Jewish portrait on display in Sheikh Faisal Bin Qassim Al Thani Museum near Al-Shahaniya. Doha, Qatar, August 8, 2015
Al Huda Engineering Works Tower and Ezdan Hotel in West Bay in orange dust. Doha, Qatar, April 2, 2015
Al Gassar Tower and Ezdan Hotel in West Bay in orange light from a dust storm. Doha, Qatar, April 2, 2015
Ezdan Hotel in fog to the east from a balcony of Room 1604 of Dareen Tower in West Bay. Doha, Qatar, November 30, 2013
Clock Tower and Amiri Diwan (Emir s Palace). Doha, Qatar, March 9, 2013
Reflections of evening lights in Aamal (Golden) Tower in West Bay tower from ASAS Tower West, view from a balcony of Room 2303. Doha, Qatar, February 4, 2011
WTC Tower in West Bay in fog, looking up. Doha, Qatar, February 15, 2014
Orange light from a window of Room 1-2244 in Tower 1 of Ezdan Hotel and Suites in West Bay during dust storm. Doha, Qatar, April 2, 2015
Clock Tower and Emir s Diwan (palace) near Souq Waqif. Doha, Qatar, March 29, 2013
Al Bidda Tower in West Bay in fog. Doha, Qatar, February 15, 2014
Nakheel Tower in West Bay in fog. Doha, Qatar, February 15, 2014
Tornado Tower in West Bay in fog. Doha, Qatar, February 15, 2014
Al Bidda Tower in West Bay in fog, looking up. Doha, Qatar, February 15, 2014
Foot of WTC Tower in West Bay in fog. Doha, Qatar, February 15, 2014
Faisal Tower in West Bay in fog. Doha, Qatar, February 15, 2014
WTC Tower in West Bay in fog, at morning. Doha, Qatar, February 15, 2014
Faisal Tower in West Bay. Doha, Qatar, February 13, 2014
View to the west direction from a gym hall on 30-th floor of Dareen Tower in West Bay. Doha, Qatar, February 1, 2014
Clock Tower and Amiri Diwan (Emir s Palace), Al Bidda area. Doha, Qatar, March 9, 2013
Olympic and Ezdan towers in West Bay. Doha, Qatar, January 24, 2014
Street in West Bay near Ezdan Hotel. Doha, Qatar, January 23, 2014
Ezdan Hotel in West Bay at evening. Doha, Qatar, January 23, 2014
Dolphin Energy Tower in West Bay. Doha, Qatar, February 20, 2014
Gate of Faisal Tower in West Bay in fog. Doha, Qatar, February 15, 2014
Foot of Faisal Tower in West Bay in fog. Doha, Qatar, February 15, 2014
Navigation Tower in West Bay at sunset. Doha, Qatar, February 15, 2014
Entrance of Faisal Tower in West Bay, looking up. Doha, Qatar, February 13, 2014
Tornado Tower in West Bay at morning in fog. Doha, Qatar, February 15, 2014
Entrance of Faisal Tower in West Bay in fog. Doha, Qatar, February 15, 2014
Foot of Tornado Tower in West Bay in fog. Doha, Qatar, February 15, 2014
Faisal Tower in West Bay in fog at morning. Doha, Qatar, February 15, 2014
Financial Center Tower in West Bay. Doha, Qatar, February 20, 2014
Entrance of Faisal Tower in West Bay. Doha, Qatar, February 13, 2014
Area of Navigation Tower in West Bay. Doha, Qatar, February 14, 2014
Door of Faisal Tower in West Bay in fog. Doha, Qatar, February 15, 2014
Foot of Al Bidda Tower in West Bay in fog, looking up. Doha, Qatar, February 15, 2014
Foot of Nakheel Tower in West Bay in fog. Doha, Qatar, February 15, 2014
Portrait of a sheikh with a camel at the entrance of Sheikh Faisal Bin Qassim Al Thani Museum near Al-Shahaniya. Doha, Qatar, August 8, 2015
Waste ground west from Ezdan Hotel in West Bay, view from a window of Room 1-2244. Doha, Qatar, September 12, 2014
Abandoned construction west from Ezdan Hotel in West Bay, view from a window of Room 1-2244. Doha, Qatar, September 12, 2014
Street in West Bay opposite to Ezdan Hotel. Doha, Qatar, January 23, 2014
Towers in West Bay opposite to Ezdan Hotel. Doha, Qatar, January 23, 2014
Ezdan Towers at Al Betra Street in West Bay, looking up. Doha, Qatar, January 25, 2014
Ezdan Hotel on Al Betra Street in West Bay. Doha, Qatar, January 23, 2014
View from the foot of Faisal Tower in West Bay. Doha, Qatar, February 13, 2014
Foot of International Islamic Tower in West Bay in fog. Doha, Qatar, February 15, 2014


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Chivas whisky launch
HomeEventsChivas whisky launch
By 5 Senses
OnApril 20, 2021
There is something about whisky that just does not get old.
Aged is usually a good thing for most fine whiskies, the longer it stays in the cask, the finer and more accentuated the flavour of the notes that harmoniously make up the whisky.
As such, the essence is to understand the individual notes and create culinary masterpieces around the drink to pay homage to the flavours.
Blended Scotch whisky makers Chivas added to the range of whiskies available in the Kenyan and African market with the Chivas Regal XV, aged for 15 years.
Chivas brothers started off running a grocery store that would a few odd years later give birth whisky business. In 1909, the brothers launched the first luxury whisky—aged for 25 years—in New York. It disappeared during the great prohibition (whisky ban).When the ban was lifted, Chivas returned to the market with a 12-year old blend. Fast forward to a nearly century later, the whisky company is making inroad into the Kenyan market to quench the growing thirst for fine liquor.
This was to target the rapidly growing category of blended Scotch whiskies, which, in data from IWSR, had a compounded annual growth rate of 8.5 per cent between 2016 and 2017. This is a double digit growth between 2013 and 2017 of 19.3 per cent per cent.
As part of the introduction of the new blend into the Kenyan market, Pernod Ricard, owners of the brand, paired the Chivas Regal range with varied dishes from Five Senses restaurant, a showcase of the meshing between Whisky and food.
https://5senses.co.ke/wp-content/uploads/2021/04/WhatsApp-Video-2021-04-17-at-8.03.10-PM.mp4
The deviation from the norm of the drink usually taken as a pre-dinner drink or night cap is part of the versatility that traditional distilleries have been showcasing as tastes evolve.
The first course, dubbed as Mushroom Three ways is just as its name suggests, mushrooms prepared three ways—royal of button mushroom, mushroom duxel and a mushroom mousse. This course is paired with a Chivas Regal 12–year-old.
Chef Kim Kiarie of Five Senses incorporates the drink in the preparation, after nosing and tasting the drink to see how the ingredients in the dish pair.
The second course of Torched Mackerel on a base of almonds is paired with a Chivas Regal Extra.
"What's extra… Extra sherry cask matured whisky. Deeper colour for the blend. It has a rich nose with notes of dark fruits and hint of vanilla and almond," says Tristan Campbell, Chivas international brand ambassador.
To capture the notes, Chef Kim incorporates almond puree, almonds and pears in the dish. The oiliness and richness of the fish is a perfect pairing for the Chivas Regal Extra.
The next course which is the main course is bacon wrapped pork fillet, a caramel glaze with new potatoes paired with the Chivas Regal XV. The accents of the dish include vanilla corn and spinach puree. The vanilla corn puree complementing the notes of vanilla in the drink.
The final course, a chocolate roll made of chocolate sponge, Chivas regal infused chocolate ice cream is paired with the Chivas Regal 18-year-old.
The drink, a favourite for Tristan is a complex blend of 85 flavours in each blend. It was first created in 1997 with notes of dark chocolate and raisins.
"It's Christmas cake in a glass," says Tristan, explaining that the blend makes best for an after dinner dram and also pairs well with chocolate desserts.
The delicate balance between the drink and meal is one that must be observed. For instance, pairing the Chivas Regal XV with the chocolate desert bring out the "rough" edges of the whisky, making it a hard swallow.
It is the nosing and the tasting notes that dictate what pairings work well for food and what pairing will be a fail.
Story by Business Daily


Fallacies in response to economic crises; a better way. Prudent wealth building; not borrowing from an uncertain future, spending what does not exist. Dealing with normal cycles; avoiding contrived disasters.
The response of most Western Governments to economic crises, since the 1929 - 1931 Market debacles, has been to employ Keynesian remedies; deliberate fiscal deficits to finance a vast assortment of projects, some in themselves worthwhile, but many half-baked, conceived for no other purpose than to inflate the circulating currency. These increased expenditures by public agencies were financed, not from existing resources, but by borrowing against uncertain future prospects; drawing on wealth not yet earned in the fancy that, by so doing, they might trigger a rebound in the economy; often without having to address--or even analyze--the dynamics of the problem or problems that led to the debacle.
We have attacked such fallacies in many features--including several linked below--as aspects of Leftist/Egalitarian/Collectivist attacks on traditional societies & nations--attacks on the very continuity of heritage. Here, however, our subject will not be the fallacies, antics or contrivances, of compulsion driven sociopathic movements--or the demagogues who exploit them. Here, we offer an exposition of a better way to deal with economic & social cycles & uncertainty.
Two or three generations back, rooted Americans--whether wealthy or merely struggling to make ends meet--taught their children to emulate the squirrel, who instinctively understands the concept of prudence; of storing achieved resources against future want. This did not prevent economic upheavals. What it did do was provide a greater measure of self-reliance; of clarity as to where responsibility lay for solving the problems of individual families; while it provided previously earned capital, wealth & resources, to apply to current problems. It was this enormous resource base which, even in coming out of a "Great Depression," enabled America to turn the tide in World War II from an industrial base, built over generations, to completely overwhelm the productive capacity of Germany & Japan.
Unfortunately, the "spin doctors" of envy, resentment & dependence upon Government, have managed to focus popular attention, not on what was achieved by a dynamic people from 1781 till 1929, but on an enormous ideological & perceptual shift. In that shift, Americans, as a people, have forgotten the lessons, both of their own history and that of every other people, who have ever made a mark on the history of this world.
Provident or prudent behavior had been recognized as not only wise, but as a significant attribute of the godly, ever since the earliest Biblical times. To the Conservative reading this, it may seem redundant to even make the point; yet in an era, when even supposedly moderate people, successful in commerce, embrace some of the most foolish Keynesian deceptions, one must continuously stress what once was obvious.
That families, communities & nations, should provide for coming adversity before a crisis, is one of the most obvious of once well-understood truths. By such perspective, the thirty fold leveraging of bank wealth before the 2008 meltdown was clearly imprudent, improvident & logically indefensible. The current suggestion that a twelve fold leveraging might be rationally acceptable is only marginally less absurd.
Of course, bankers are far from the only indulgers in the fantasy that the future will take care not only of itself, but of present excess. Consider borrowers, lured into a pretense of home ownership, by signing away homes they sought to purchase with little or no deposit, to those deluded bankers; putting themselves on a financial treadmill, even to try to make the payments necessary to continue to live in those mortgaged homes. Will anyone suggest that gut-wrenching experience was really preferential to learning a better way at the knees of one's parents?
Who can defend a combination of irresponsible bankers & political "do-gooders" expanding the myth of home ownership (the real owners being the holders of mortgages, with terms impossible for the "buyers" to ever satisfy) in a make believe world where they were conferring a "benefit"--even daring to call it the "American Dream"--before bundling those irresponsible mortgages into financial packages, the actual values of which were impossible to calculate?
Not only did no group, outside the world of charlatans & demagogues, actually benefit from that multi-sided exercise in absolute irresponsibility; the game almost destroyed the major financial institutions on the American sub-continent. Can anything be clearer than that holding off on purchasing any item, until one has acquired sufficient means to pay for that item--or have fairly certain prospects of being able to meet any balance due on such purchase, without indulging in wishes or dreams--is a better way to proceed; the better way for both buyers & lenders? Is it any different for a Government engaging in expensive projects?
We do not suggest that most economic disasters have been consciously contrived. But in the frantic pursuit of whatever the pursuers consider immediately beneficial, inevitably at the expense of a provident building (step by step on what is already known & achieved) towards a better future, we have the equivalent of deliberate contrivance. The rationalized pursuit of an unaffordable, dream based, wish list, can be the most certain path to eventual disaster.
Commentators describe the process of borrowing from the future to deal with a perception of economic crisis, as 'kicking the can down the road.' This may show a glint of understanding, as to the dynamic context, but only a glint. The damage will always be far more serious than the metaphor implies. Take, for example, already observed consequences of two generations of increasing Federal intrusion into the, once private, health care & housing markets in America.
The explosion in health care costs & a still wheezing bubble in housing, both reflect artificial stimulation of marginal demand in those areas. To better understand the effect, you must look more closely at the micro levels of human interaction. While inflation (i.e., an increase in the supply of money) tends to act on all prices, it does not necessarily raise all prices or, with respect to the prices that do rise, raise all prices by an equivalent percentage. The price of any item reflects a confluence of factors, relating not only to supply--both present & anticipated--and demand--both present & anticipated--but also to various subjective perceptions of value. With respect to health care & housing prices, there has been a highly artificial stimulation of rising prices, directly related to the meddling of the Federal Government--not only spending money not yet earned, but doing so in a manner that fueled anticipation of yet more to come.
To better understand what happened--and how truly pernicious--look not at statistical aggregates, which can record a bubble after it is blown or after it has burst, but at what took place between individuals. The injection of the Federal Government, more deeply into American civilian health care in the 1960s, did not immediately increase the availability of health care services. Rather it enabled those favored with qualification, either by age or poverty, to suddenly "purchase" a substantially increased percentage of what was available. It clearly impacted both that market & the attitudes of those providing & using the now subsidized services. Among the many consequences was a, still continuing, spike in the cost of health care to the unsubsidized; a gradually changing attitude among physicians, who had previously expected to treat the indigent in accordance with their oaths, while paring charges to those only marginally able to pay; and a sense of increased entitlement by that sub-class of supposed beneficiaries who had never contributed anything at all towards their benefits.
But the developing social & economic disaster in "health care" has been a subject of other features. What about the housing "bubble?"
Take a couple with little or no savings--one already strapped to revolving debt at usurious interest rates, to cover previous excesses--that qualifies for a Federally guaranteed mortgage. They do not have the traditional 20% down, expected by a neighborhood building & loan, or local bank. They may not even have 5% to put down. Considering that revolving debt, they have little or no prospect for making regular payments over even a few years, much less the life of the mortgage. Yet they make the "purchase," and then "eat their guts out," trying to make what they imagined a sound "investment," actually work. The immediate effect on the general market, however, is not the real point. The sellers of the purchased home may not be in such dire straits. With the proceeds of the sale, they are able to purchase a more expensive home--whether the greater expense equates with greater value or not--and now we see the start of a "trickle up" effect, the real economics of which are somewhat obscured, both by that urban legend & the ongoing Keynesian debasement of our money.
Soon, enough a confluence of factors--even before some dysfunctional genius in the upper echelons of banking decides that it is safe to leverage assets thirty fold, starts bundling what are now described as "sub-prime" mortgages (the result of the process described in the last paragraph), in an effort to compound the idiocy--spurs a serious escalation in housing prices--the "bubble," now in the process of slowly contracting back to reality.
Clearly, what we have witnessed over the past half century, was not a better way to encourage either better health care or better access to affordable housing. The better way, in the late 20th Century & early 21st, was still the way of the squirrel; the way of the Prophet Joseph in Genesis; the way of the more provident of Mankind from the dawn of history. Building on past achievement, saving towards realistic goals; only borrowing against reasonably certain near term prospects; taking responsibility for one's needs, including the needs of one's posterity. In short, returning to a premise that each generation owes a duty to the next--a positive duty, not a rationalized pretension.
The greatest problem is that we rationalize acceptance of policies that go against all human experience, when we really do know a better way. In the process, we crush those who act wisely & further corrupt the foolish. The major effect is multi-generational.


Yesterday I noticed that I was in an exceptionally good mood for no especially obvious reason, such as winning the lottery. Thinking about it, I concluded that I was happy because I was finally able to refactor the code I was working on after several weeks of implementing new features. It got to the point where working on it in its disorganized state gave me the exact same feeling as touching a slimy rock – ew ew ew!
Interesting – we say "clean code" and "dirty hack," but I think that we really do co-opt the "ew, dirt, contamination" module of our brains to work with code. Weird, huh? I'm going to pay attention for other interesting recruitment examples.
Dirt represents chaos, so we try to rid ourselves of dirt so that we feel comfortable.
In my office, we're more likely to say that a piece of code smells bad, rather than is dirty. Same mental association, just a different sense.
The important question is, do you actually feel like you are smelling something bad when you work with the code?
Not in the sense of synaesthesia, if that's what you mean – it's just a mental association, a metaphor. But thinking on it again, I think I know the feeling you're talking about – a sense of uncleanliness when dealing with bad code. For me, I'd often associate it with the moment of realisation of just how something works – and just how wrongly it's been done.


text:
Stön - estońska wódka, produkowana z ziemniaków przez firmę Cazanove Opici.

Historia
W XVIII wieku wódka produkowana była głównie w celach leczniczych (sprzedawana była w aptekach). Wówczas była produkowana przez Niemców. Od 1863 roku produkcję przejęli Rosjanie. Wtedy Stön zdobyła największą popularność, gdyż około 89% Estończyków miało w swoim domu butelkę tej wódki. W 1918 roku wódka była produkowana w Estonii. Sprzedaż nadal była ogromna, jednak spadła w latach 1940-1991, kiedy Estonia należała do ZSRR. Po 1991 roku Stön stała się ponownie najlepiej sprzedawaną wódką w Estonii.

Marki wódek


text:
Aeronautics Centenary Reception
by Imperial College London Alumni
18:00 – 20:00 BST
City and Guilds Building Foyer
SW7 2AZ
Celebrating 100 years of the UK's leading Aeronautical Engineering Department
Aeronautic Alumni and family are warmly invited to a celebratory reception marking 100 years of Imperial's Aeronautics Department.
Join Professor Paul Robinson, Head of Department, members of the Aeronautics faculty and fellow alumni for an update on the latest developments from the department over drinks and canapes.
We hope you can join the celebration and also take part in Alumni Weekend, starting the following morning.
Imperial College London is registered as a controller (in respect of its processing of personal data) with the Information Commissioner's Office. The College processes personal data for a number of specified activities. These activities are used to support a full range of activities for our alumni and friends, and to ensure that the ways in which we communicate with you, such as sending out College publications, inviting you to events, or advising you about our alumni benefits and fundraising priorities, adhere to your chosen communication preferences.
The personal information that you provide will be treated confidentially and stored securely in accordance with UK data protection law and the College's own Data Protection Policy. The personal information that you provide may be shared with third parties, contracted by the College to assist with the administrative processes described, or as required by law. Any data processed on behalf of Imperial College London by a contracted third party will not be used by that third party for their own purposes. The College does not sell any of its data to third party organisations.
For further information see the Advancement Division's privacy policy.
Aeronautics Centenary Reception at City and Guilds Building Foyer
Imperial College London South Kensington Campus, London, SW7 2AZ, United Kingdom


Scrap Metal Recycling Lakewood, CA | Smart Recycling Inc.
Open during business hours, Smart Recycling Inc. is a full service scrap metal recycling enterprise. The radio-dispatched vehicle fleet is available for same day service, or within twenty four hours of your call. You may move forward knowing that any unusual condition ıs going to be dealt with correctly and in a timely manner. Smart Recycling ıncludes a complete service staff, including plenty of equipment to take on practically any job, whenever, wherever in Lakewood and its surrounding area.
We provide the widest assortment of ferrous and non-ferrous metal recycling services and collection containers for recyclables in and around the Lakewood area. From cutting-edge machinery for reclamation, disassembly or collection, to diagnosing the after-market most fruitful to you, Smart Recycling's professional understanding and versatility is first rate.
Your situation is one of a kind. We appreciate that, and that is why we offer "hands on management" by our experienced workforce. We start with a comprehensive analysis of your project, but it's the meticulous attention we place on meeting your precise needs that maximizes your profits from every recycling effort. And that keeps our customers returning time and time again.
In the current rapidly changing environment, we view our clients as business partners and work faithfully at providing economical strategies to recycle scrap metals and other recyclable items.
Smart Recycling specialists have the knowledge, machines, and authorization to safely and securely provide demolition solutions for commercial facilities, with every single team member having finished current OSHA (Occupational Safety and Health Administration) schooling and certification. We're truly in a position to construct a custom strategy that satisfies your plant's demolition and clean-up requirements, irrespective of how large or small the project.
When you need containers for scrap metal collection and pick-up, and a qualified crew of dispatchers, Smart Recycling is here to serve you. Logistics to transport, we will plan for reliable and efficient scrap delivery from your scrap yard or manufacturing center to one of our 4 recycling facilities.
Whether you require a roll-off box for your manufacturing center, construction site, clean-up project, or at your recycling facility, we will bring it on-site and in a timely manner.
The most common metals picked up by scrap yards include copper, steel, aluminum, brass, iron and wires of all varieties. However, your hometown scrap yard may process additional metals for recycling and give you cash payouts for your scrap metals. If you're unsure what you have or what you ought to do, contact Smart Recycling and we'll have a friendly specialist answer all your questions for you.
When you are trying to recycle scrap metal it is very crucial to identify what kind of metal you have. The easiest technique to determine what type of metal you're dealing with is to employ a magnet. If the magnet sticks to your metal, you have a ferrous metal in your hands, such as steel or iron.
If the magnet does not stick, you have a non-ferrous metal, such as copper, aluminum, brass, stainless steel or bronze. These metals are likely to be more valuable to a business like Smart Recycling.
From there, you can make a distinction with color, texture and consistency and other visual aids to figure out accurately what type of metal you're working with. If you are still unsure, call us and we will be glad to support you in any way we can.
Absolutely yes. Not only does Smart Recycling furnish containers for continuous generated scrap, we will also provide custom sized bins of any size to support handling and sorting needs.
What is the Value Of Scrap Metal and how do you decide the cost?
Almost all metal prices are set upon industry conditions regularly. The methodology mainly applied by Smart Recycling is structured on the published Metal Market Report found in the American Market Journal; which may be provided if requested. Utilizing this system as a guide, an agreed upon margin of plus or minus published rates can be set for all upcoming purchases.
How fast will Smart Reclycling pick up after we request your services?
If a request for service is placed before 10 a.m. of any weekday there is a very good possibility of getting same day service. However, all service calls received will be completed no later than next day guaranteed. Special need scenarios are addressed precipitously.
It is primarily at the discretion of the agent representing its company, normally, payments are made within a 30-day period of receiving metals. Nevertheless, we will pay for all agreements within the time frame favored by our customers.
Salvatore J. Russo started Smart Recycling as Russo Metal Company in 1978. In those days the focus was purely industrial scrap. As time went by, the recycling division was born, and after that surplus sales, then Dumpster rentals. In 1995 Russo Metal Co. was incorporated under the name Smart Recycling, an acronym for Scrap Metal And Recycling Technologies.


Jenna Scharmer, daughter of Glen & Tena Scharmer of Grafton, ND, has become engaged to Andrew Meldahl, son of Cindy Lander of Thompson, ND.
We got engaged after 4 years of dating and had been talking about it for at least 3 of those. After completing grad school in spring 2016, I moved out to Bismarck and into one of his beautiful home creations together. We'd been living together for well over 2 years. I'll be honest in that I was getting a bit antsy. I actually thought he was going to ask on our dating anniversary, but that didn't work out weather wise. So a few days later was actually his birthday. I had the afternoon off and we decided to go to the local pumpkin patch. So we went to get some lunch and had a couple drinks. Walking through the pumpkin patch and this little nature trail, I was telling him how I'd felt bad because I didn't have time to shop or get him anything to open. He played it off. Then said that there actually was only one thing he wanted for his birthday. When I turned to ask what, he got down on one knee and asked me to marry him. He thinks I hesitated, but I'm pretty sure I didn't even wait for him to get the full question out before I said yes.
We met online. I was living in Grand Forks, ND. Andy was living in Bismarck. He was busy growing his custom home building company. And I was working in the hospital, teaching nursing clinical, and getting my degree as a nurse practitioner. Neither of us were in environments to meet many people the traditional way.
I'd been going on a few dates, and was actually considering taking a break from the whole online dating scene. But then Andy reached out. Turns out he was just browsing at who was in the region and repaid for his subscription so he could message me.
It's all history from there. We went on our first date taking a walk by the Red River before I went in for a night shift. And we went on our second date the very next night. It all just fell into place after that.


ST. LOUIS, Mo. - A St. Louis woman is without her car, her belongings, and her beloved dog after a man jumped in her car and took off with it.
Toni Berryhill said it happened September 4 around 1:15 p.m. in north St. Louis County.
She stopped by a relative's house near Lucas and Hunt and Eunice and left her car running while she was going to run inside. Berryhill said it was a hot day and she wanted to keep her dog Axe cool.
Before she could even get inside, Berryhill said a man ran up, jumped in her car and took off with it, with her dog inside.
She's asking anyone with information to call 314-250-1027. Police confirmed they're investigating the incident.


text:
\section{#1}\setcounter{equation}{0}}
\begin{document}
\title{The Standard Model Higgs Boson-Inflaton and Dark Matter}
\author{T.E. Clark}
\email[e-mail address:]{clark@physics.purdue.edu}
\affiliation{Department of Physics,\\
 Purdue University,\\
 West Lafayette, IN 47907-2036, U.S.A.}
\author{Boyang Liu}
\email[e-mail address:]{liu115@physics.purdue.edu}
\affiliation{Department of Physics,\\
 Purdue University,\\
 West Lafayette, IN 47907-2036, U.S.A.}
\author{S.T. Love}
\email[e-mail address:]{love@physics.purdue.edu}
\affiliation{Department of Physics,\\
 Purdue University,\\
 West Lafayette, IN 47907-2036, U.S.A.}
\author{T. ter Veldhuis}
\email[e-mail address:]{terveldhuis@macalester.edu}
\affiliation{Department of Physics \& Astronomy,\\
 Macalester College,\\
 Saint Paul, MN 55105-1899, U.S.A.}

\begin{abstract}
The standard model  Higgs boson can serve as the inflaton field of slow roll inflationary models provided it exhibits a large non-minimal coupling with the gravitational scalar curvature. The Higgs boson self interactions and its couplings with a standard model singlet scalar serving as the source of dark matter are then subject to cosmological constraints. These bounds, which can be more stringent than those arising from vacuum stability and perturbative triviality alone, still allow values for the Higgs boson mass which should be accessible at the LHC.  As the Higgs boson coupling to the dark matter strengthens, lower values of the Higgs boson mass consistent with the cosmological data are allowed.
\end{abstract}
\maketitle

\section{Introduction}

The inflationary paradigm has proven extremely successful in accounting for a wealth of cosmological observations. It not only explains the large scale homogeneity and isotropy of the present universe, but also accounts for the generation of the nearly scale invariant primordial perturbations responsible for structure formation \cite{inflation}. The implementation of the  slow roll inflation  is  generally achieved by the inclusion of an independent scalar degree of freedom, the inflaton. It is tempting to try to identify the inflaton with the standard model Higgs field, $h$, with a $\lambda h^4$ potential.  Unfortunately, early attempts at such an identification were plagued \cite{Linde,Salopek:1988qh} by the required flatness of the inflaton potential which is dictated by the size of the observed density fluctuations. This in turn necessitated far too small a quartic self coupling for the inflaton for it to be identified with the Higgs scalar. However, by including a  non-minimal coupling of the Higgs doublet, $H$, to the gravitational Ricci scalar curvature, $R$, with a large coupling constant $\xi \sim 10^3 -10^4$, it has been argued \cite{Salopek:1988qh,Bezrukov:2007ep,Barvinsky:2008ia,DeSimone:2008ei,Bezrukov:2008ej,Barvinsky:2009fy} that the resultant Higgs potential can indeed be flat enough for it to play the additional role of the inflaton. In such a case,  the shape of the Higgs-inflaton effective potential in the inflationary region allows for a range of cosmologically acceptable values for the Higgs boson mass even after the inclusion of radiative corrections. As such, slow roll inflation can be implemented without the need for additional degrees of freedom already appearing in the minimal standard model.

The presence of non-baryonic dark matter, however, does require the inclusion of additional degrees of freedom beyond those appearing in the standard model. A minimal extension of the standard model which accounts for this dark matter is the inclusion of a singlet hermitian scalar field, $S$, \cite{Silveira:1985rk,McDonald:1993ex,Burgess:2000yq,Davoudiasl:2004be}. This simple, and clearly minimal, extension can account for the correct abundance of dark matter. Its lack of direct \cite{He:2008qm} and indirect  \cite{Ponton:2008zv,Yaguna:2008hd} detection or observation at high energy accelerators \cite{Bird:2004ts,Barger:2007im,He:2007tt} have already somewhat constrained the model's parameter space, and experiments in the near future will further probe its validity.

In this paper, we study the quantum effects of dark matter as modeled by this standard model singlet scalar on the Higgs-inflaton effective potential. As a result of the coupling of the Higgs boson and dark matter singlet, the cosmological restrictions which include up to three standard deviations from the measured central values, allow for lower values of the Higgs boson mass than is the case in the absence of such dark matter couplings. In section \ref{section2}, the renormalization group improved effective potential for the physical Higgs field is determined including the effects of its coupling to the scalar singlet dark matter as well as its large non-minimal coupling  to the gravitational Ricci scalar.  Three quantities, $\epsilon$, $\eta$ and $\zeta^2$, parameterizing slow roll inflation are given in terms of the derivatives of this Higgs-inflaton effective potential. The Higgs non-minimal coupling $\xi$ to gravity is specified at the onset of inflation so as to yield the measured value for the amplitude of density perturbations.  The scale for the onset of slow roll inflation is set so as to provide $N_e =60$ e-folds of expansion before the inflaton exits inflation at $\epsilon =1$.  The spectral index, its running and the tensor to scalar ratio are then determined quantities which depend on the Higgs boson mass as well as the Higgs boson-dark matter coupling and the singlet self-coupling.  The numerical results for this dependence are presented in section \ref{section3} and are displayed in Figs. \ref{NoRollConstraints} and \ref{CosmoParameterSpace-00} in terms of cosmologically allowed and excluded regions of parameter space.   Conclusions are summarized in section \ref{section4}.  Appendix \ref{appendixA} provides the one-loop renormalization group $\beta$-functions for the gravitationally non-minimally coupled model.  Appendix \ref{appendixB} contains the triviality and vacuum stability constraints for the scalar coupling constants.

\section{Higgs-Inflaton effective potential \label{section2}}

A minimal way of accounting for the  presence of non-baryonic dark matter is by modeling said matter by a stable hermitian standard model singlet, scalar field $S$. The stability of this scalar is guaranteed through the imposition of an unbroken $Z_2$ discrete symmetry under which the scalar is odd.  Focusing on the scalar and gravitational sector of this model the tree level action in the Jordan frame including all terms through mass dimension four is specified by
\begin{widetext}
\begin{eqnarray}
\Gamma_{\rm Tree} &=& \int d^4x \sqrt{-g}\left[\Lambda +\frac{1}{2}m_{Pl}^2 R +(D_\mu H)^\dagger g^{\mu\nu}D_\nu H -V(H^\dagger H)+\xi R (H^\dagger H -\frac{v^2}{2})\right. \cr
 & &\left. \qquad +\frac{1}{2}\partial_\mu S g^{\mu\nu}\partial_\nu S -\frac{1}{2}m_S^2 S^2 -\frac{\lambda_S}{4}S^4 + \frac{1}{2}\xi_S R S^2 -\kappa S^2 (H^\dagger H -\frac{v^2}{2})+\cdots\right]
\label{treeLag}
\end{eqnarray}
\end{widetext}
where the Higgs potential is
\begin{equation}
V(H^\dagger H) =\lambda \biggr(H^\dagger H -\frac{v^2}{2}\biggr)^2
\end{equation}
with the Higgs multiplet parameterized by
\begin{equation}
H=\frac{1}{\sqrt{2}}\pmatrix{\chi^+ \cr
(v+h ) + \chi^0}  .
\end{equation}
Here $\chi^\pm$, $\chi^0$ are the standard model erstwhile Nambu-Goldstone bosons and $h$ the physical Higgs boson field.  The ellipses in Eq. (\ref{treeLag}) refer to the usual remaining standard model Yang-Mills and fermion  kinetic terms and Yukawa couplings.  Note that this action includes the non-minimal coupling of the Higgs doublet to the gravitational Ricci scalar $R$ with coupling $\xi$.  $m_{Pl}^2$ is the reduced Planck mass $m_{Pl}^2 = 1/8\pi G \approx (2.43 \times 10^{18})^2 ~{\rm GeV}^2$ and $v=246.2$ GeV is the scale of electroweak symmetry breaking.

The various cosmological parameters governing the slow roll inflation are secured in terms of derivatives of the effective potential with respect to the Higgs-inflaton field  evaluated during the inflationary phase when (only) the physical Higgs field has a large expectation value, $h \sim m_{Pl}/\sqrt{\xi}>>v$.  Thus it is necessary to determine the renormalization group improved effective potential as a function of $h$.  The non-minimal gravitational interaction of the Higgs doublet couples  the gravitational and Higgs fields' equations of motion.  This results in a modified form for the high energy behavior of the Higgs and gravitational field propagators or, in the external gravitational field case focused on here, a modified Higgs propagator \cite{Barvinsky:2009fy}.  At the tree level, the non-minimal Einstein equations obtained from (\ref{treeLag}) are
\begin{equation}
\left( 1+\frac{\xi h^2}{m_{Pl}^2} \right)\left( R_{\mu\nu} -\frac{1}{2} R g_{\mu\nu} \right) = -\frac{1}{m_{Pl}^2}(\Theta_{\mu\nu} + S_{\mu\nu}) ,
\label{Einstein}
\end{equation}
where the new, improved energy-momentum tensor is $\Theta_{\mu\nu} = T_{\mu\nu} + \xi (\frac{1}{2}(\nabla_\mu \nabla_\nu +\nabla_\nu \nabla_\mu) - g_{\mu\nu} \nabla^2 ) h^2$ with $T_{\mu\nu}$ the standard model canonical energy-momentum tensor.  $S_{\mu\nu}$ are terms involving the dark matter field $S$ and its coupling to itself, the gravitational field and the standard model Higgs field.  Focusing on the gravitational and Higgs fields only as they are dominant in the inflationary region, the trace of Eq. (\ref{Einstein}) results in
\begin{eqnarray}
\left( 1+\frac{\xi h^2}{m_{Pl}^2} \right)R &=& \frac{-1}{m_{Pl}^2}\biggr( 6\xi h \nabla^2 h \cr
 & &\qquad + 6(\xi + \frac{1}{6}) \nabla h \cdot \nabla h -4 V(h)\biggr).\cr
 & &
\end{eqnarray}
Substituting this into the Higgs field equation yields
\begin{eqnarray}
\nabla^2 h + V^\prime (h) &=& \xi h R \cr
 &=& \frac{-6\xi^2 h^2 /m_{Pl}^2}{(1 + \xi h^2 /m_{Pl}^2)} \nabla^2 h \cr
 & &\quad -\frac{\xi h ( 6(\xi + 1/6)\nabla h\cdot\nabla h -4V(h)}{(m_{Pl}^2 +\xi h^2)} .\cr
 & &
\end{eqnarray}
Expanding about the backround Higgs field $h \rightarrow h + \rho$, produces the field equation
\begin{equation}
\frac{1}{s(h)} \nabla^2 \rho = -V^\prime +\cdots ,
\end{equation}
where (primes denote differentiation with respect to $h$)
\begin{equation}
s(h)=\frac{1 + \xi h^2 /m_{Pl}^2}{1 +(1+6\xi)\xi h^2 /m_{Pl}^2} .
\end{equation}

Thus the non-minimal coupling to the gravitational field introduces a modification to the Higgs field propagator  by a factor of $s(h)$. The one-loop renormalization group improved effective potential for $h$ can now be computed using standard techniques. The only modification to the standard model calculation arises from the non-canonical Higgs kinetic term. Thus for large non-minimal gravitational coupling constants, $\xi$, and for the sizeable, but still sub-Planckian, inflationary backgrounds $h \sim m_{Pl}/\sqrt{\xi}$, this leads to a suppression of the physical Higgs field propagator \cite{Salopek:1988qh,DeSimone:2008ei,Barvinsky:2009fy}
\begin{equation}
i/p^2 \rightarrow is/p^2 .
\end{equation}
Note that $s(h )$ takes its canonical value $s(h)\rightarrow 1$ when $\frac{\xi h^2}{m_{Pl}^2}<<1$ while in the other extreme,
$ s(h)\rightarrow \frac{1}{6\xi}$ when $\frac{\xi h^2}{m_{Pl}^2}>>1$.

It then follows, for these large field values, the Higgs field is no longer an unconstrained high energy degree of freedom. This will result in a violation of unitarity and an (as yet unknown) ultraviolet completion of the model will be necessary for a thorough understanding of the dynamics in the inflationary region \cite{Burgess:2009ea}. Moreover, although $h$ is sub-Plankian in the inflationary region, the variable $\sqrt{\xi} h /m_{Pl}$ is large and the issue of contributions from higher dimensional operators needs further scrutiny. As discussed in reference \cite{Bezrukov:2008ej}, the Higgs suppression could indicate the onset of a new strongly interacting phase of the Higgs sector of the standard model. To account for this, the perturbative low energy standard model renormalization group running of the coupling constants was matched onto their running in a non-linearly realized electroweak symmetry model effective in the range $m_{Pl}/\xi {< }h  {< } m_{Pl}/\sqrt{\xi}$ where the Higgs field contributions to processes are absent \cite{Bezrukov:2008ej}. Here we adopt a somewhat pragmatic approach and  following in the spirit of reference \cite{DeSimone:2008ei}, we employ the suppressed Higgs effective standard model, now with the inclusion of the dark matter scalar, and explore the dependence of the measured cosmological density spectrum parameters on the Higgs and dark matter coupling constants for the inflationary scales $h  \sim m_{Pl}/\sqrt{\xi}$,  albeit possibly at the limits of its domain of validity.  Hence, Feynman integrands involving Higgs propagators will have a suppression factor $s$ for each such line with $s(h)$ evaluated at the scale of the background Higgs field $h$.  In particular the renormalization group functions will include a suppression factor for each physical Higgs line contributing to the function.

Isolating the explicit dependence on the dominant large Higgs field background terms, while the ellipses refer to the remaining subdominant singlet and standard model terms, the one-loop renormalization group improved effective action takes the form
\begin{widetext}
\begin{equation}
\Gamma = \int d^4x \sqrt{-g}\left[\Lambda +\frac{1}{2}m_{Pl}^2 {f}(t) R +\frac{1}{2}{G^2}(t) \partial_\mu h g^{\mu\nu}\partial_\nu h -{V}(t)+\cdots\right].
\end{equation}
\end{widetext}
In the inflationary region, the Higgs-inflaton field has a large background value and the dominant forms of the renormalization group improved effective action coefficients are
\begin{eqnarray}
{V} (t) &=& \frac{{\lambda} (t)}{4}G^4(t) h^4 (t) = \frac{{\lambda} (t)}{4}G^4(t)m_t^4 e^{4t} \cr
{f} (t) &=& 1 + {\xi}(t) G^2 (t) \frac{h^2 (t)}{m_{Pl}^2} =1+ \xi(t) G^2(t) \frac{m_t^2}{m_{Pl}^2} e^{2t} , \cr
 & &
\end{eqnarray}
where
\begin{equation}
G(t) = e^{-\int_0^t dt^\prime \gamma (t^\prime)},
\end{equation}
with $\gamma (t)$ the Higgs field anomalous dimension.  Here we have introduced the scaling variable $t=t(h)=\ln{({h}/{m_t})}$ so that $h (t) =m_t e^t$ and have normalized the Higgs field and all running couplings at the top quark mass. The various $t$ dependent running coupling constants of the effective interaction terms are given by their renormalization group equations so that, for example,
\begin{equation}
\frac{d{\lambda}(t)}{dt}=\beta_\lambda (t), \qquad  \qquad
\frac{d{\xi}(t)}{dt}=\beta_\xi (t) .
\end{equation}
The one-loop $\beta$-functions and Higgs field anomalous dimension including the suppression factors are compiled in Appendix \ref{appendixA}.

Cosmological quantities can most readily be calculated in the Einstein frame which is obtained by  rescaling the metric by $g_{E\mu\nu} = {f}(t) g_{\mu\nu}$.
The one-loop renormalization group improved effective action then takes the form
\begin{eqnarray}
\Gamma &=& \int d^4x \sqrt{-g_E}\left[\Lambda_E +\frac{1}{2}m_{Pl}^2 R_E  \right. \cr
 & &\left. +\frac{1}{2}\frac{1}{{f (t)} {\bar{s} (t)}} \partial_\mu h g_E^{\mu\nu}\partial_\nu h -{V}(t)/{f (t)}^2+\cdots\right],\cr
 & &
\end{eqnarray}
where
\begin{equation}
\bar{s} (t) = \frac{f(t)}{G^2 (t) f(t) + \frac{3}{2} m_{Pl}^2 f^{\prime 2}(t)}.
\end{equation}
Defining a canonically normalized field $\sigma = \sigma(h)$, the Einstein frame effective action reads
\begin{eqnarray}
\Gamma &=& \int d^4x \sqrt{-g_E}\left[\Lambda_E +\frac{1}{2}m_{Pl}^2 R_E \right. \cr
 & &\left. \quad\quad +\frac{1}{2} \partial_\mu \sigma g_E^{\mu\nu}\partial_\nu \sigma -{V}_E (\sigma ) +\cdots\right],
\end{eqnarray}
where the dominant part of the one-loop renormalization group improved effective potential in the inflationary region in the Einstein frame is
\begin{equation}
{V}_E = \frac{{V}(t)}{{f}^2(t)}
\end{equation}
with the canonically normalized Higgs-inflaton field defined through
\begin{equation}
\left(\frac{d\sigma}{dh}\right)^2 = \frac{1}{{f}\bar{s}}=\frac{{G^2} {f} + \frac{3}{2}m_{Pl}^2 {f}^{\prime 2}}{{f}^2} .
\end{equation}

A Higgs field wavefunction renormalization suppression factor is now defined as
\begin{eqnarray}
Z(t) &\equiv & G^2 (t) \bar{s} (t)\cr
&=&\frac{G^2(t) {f}}{G^2(t) {f} + \frac{3}{2}m_{Pl}^2 {f}^{\prime 2}}\cr
 &=&\frac{1+{\psi}^2 (t)}{ \left(1+[1+6\xi (t)(1-\gamma (t)+ \beta_\xi /2\xi (t))^2 ]{\psi}^2(t)\right)} ,\cr
 & &
\end{eqnarray}
where
\begin{equation}
\psi^2 (t) = \xi (t) G^2 (t) h^2 (t) /m_{Pl}^2 =\xi (t) G^2 (t) e^{2t}m_t^2/m_{Pl}^2
\end{equation}
is a  renormalization group invariant dimensionless field. Note that ${f}(t) = 1+ \psi^2 (t)$. As  a function of $\psi(t)$, the Higgs-inflaton effective potential takes the simple form
\begin{equation}
{V}_E = \frac{m_{Pl}^4}{4}\frac{\lambda (t)}{\xi^2 (t)}\frac{\psi^4 (t)}{(1+\psi^2 (t))^2} .
\end{equation}

The renormalization group invariant slow roll inflationary parameters are defined by (once again prime denotes differentiation with respect to $h$)
\begin{eqnarray}
\epsilon &=&\frac{1}{2}m_{Pl}^2 \left(\frac{1}{{V}_E}\frac{d{V}_E}{d\sigma}\right)^2 =\frac{1}{2}m_{Pl}^2 \left(\frac{{V}_E^\prime}{{V}_E}\right)^2 \left(\frac{d\sigma}{dh}\right)^{-2} \cr
 &=&8\xi \frac{Z}{{f} \psi^2}\left(1-\gamma +\frac{\beta_\lambda}{4\lambda}  +\psi^2 \left( \frac{\beta_\lambda}{4\lambda} - \frac{\beta_\xi}{2\xi}\right)\right)^2\cr
\eta &=& m_{Pl}^2 \frac{1}{{V}_E}\frac{d^2{V}_E}{d\sigma^2}
= 2\epsilon +m_{Pl}\frac{1}{\sqrt{2\epsilon}}\frac{d\epsilon}{dh}\left(\frac{d\sigma}{dh}\right)^{-1}\cr
 &=& 2\epsilon +\frac{\sqrt{\xi {f} Z}}{\sqrt{2 \epsilon}}\left(\frac{1}{\psi} \right)\frac{d\epsilon}{dt}\cr
\zeta^2 &=& m_{Pl}^4 \frac{1}{{V}_E}\frac{d^3{V}_E}{d\sigma^3}\frac{1}{{V}_E}\frac{d{V}_E}{d\sigma}
= 2\eta \epsilon + m_{Pl} \sqrt{2\epsilon} \frac{d\eta}{dh}\left(\frac{d\sigma}{dh}\right)^{-1}\cr
 &=& 2\eta \epsilon + \sqrt{2 \epsilon \xi {f} Z} \left(\frac{1}{\psi} \right)\frac{d\eta}{dt},
\label{slowrollparameters}
\end{eqnarray}
where all quantities are evaluated at the onset of inflation.
The power spectrum of density perturbations in $k$-space is given by
\begin{eqnarray}
P_s(k)= \Delta^2_{{\cal R}} \biggr(\frac{k}{k^*}\biggr)^{n_s(k)-1},
\end{eqnarray}
where the amplitude of density perturbations is expressed as
\begin{equation}
\Delta_{{\cal R}}^2 = \frac{{V_E}}{24 \pi^2 m_{Pl}^4 \epsilon}\biggr\vert_{k^*}
\label{amp}
\end{equation}
and is secured by the combination of experimental results from WMAP5, Baryon Acoustic Oscillations (BAO) and supernovae (SN) as: $\Delta^2_{{\cal R}} =(2.445 \pm 0.096)\times 10^{-9}$ at $k^*=0.002$ Mpc$^{-1}$ \cite{Hinshaw:2008kr}.  Slow roll inflation predicts the spectral index, $n_s$, its running, $\alpha =dn_s/d\ln{k}$, and the tensor to scalar ratio, $r$, to be
\begin{eqnarray}
n_s &=& 1-6\epsilon + 2 \eta \cr
\alpha &=& -24 \epsilon^2 +16 \epsilon \eta -2 \zeta^2 \cr
r &=& 16 \epsilon .
\label{spectral}
\end{eqnarray}
The WMAP5, BAO and SN experimental evidence gives $n_s=0.960 \pm 0.013$ and $r<0.22$ (95\% CL) with an insignificant running spectral index, $\alpha =-0.028\pm 0.020$ \cite{Hinshaw:2008kr}.

\section{Numerical Results \label{section3}}

The renormalization group equations for the various running couplings are solved numerically starting from  $t=0$ which corresponds to the top quark mass. The top Yukawa coupling at $t=0$ is fixed by the central value deduced from the top quark mass $m_t = {y}_t (0) v/\sqrt{2} \equiv 171.2$ GeV , while the gauge coupling constants are normalized at $m_t$ as $\alpha_1 (0)=0.0102718$, $\alpha_2 (0)=0.0334412$ and $\alpha_3 (0)=0.108635$ \cite{Amsler:2008zzb}. The value of $\xi(0)$ is determined so that at the initial point of the slow roll inflation, $t_i$, the non-minimal coupling constant $\xi(t_i)$ is such that the calculated value of the amplitude of density perturbations, equation (\ref{amp}), agrees with the measured result.  The Higgs-inflaton exits inflation at the final point $t_f$ when the first slow roll parameter is 1: $\epsilon (t_f) =1$.  The number of e-folds of expansion between $t_i$ and $t_f$ is
\begin{eqnarray}
N_e (t_i) &=& \frac{1}{\sqrt{2}m_{Pl}}\int_{\sigma_{f}}^{\sigma_i} \frac{d\sigma^\prime}{\sqrt{\epsilon(h (\sigma^\prime))}}\cr
 &=&\frac{1}{\sqrt{2}m_{Pl}}\int_{h_{f}}^{h_i} \frac{dh^\prime}{\sqrt{\epsilon(h^\prime)}}\left(\frac{d\sigma^\prime}{dh^\prime}\right)\cr
&=&\int_{t_{f}}^{t_{i}} dt \frac{\psi^2}{4{\xi} Z}\frac{1}{\biggr(1-\gamma+\frac{\beta_\lambda}{4\lambda}+\psi^2(\frac{\beta_\lambda}{4\lambda}-\frac{\beta_{\xi}}{2{\xi}})\biggr)}.\cr
 & &
\end{eqnarray}
The initial point of inflation is defined so that $N_e (t_i)=60$.  These three criteria are then implemented recursively for each choice of initial Higgs mass, $m_h =\sqrt{2 \lambda (0)}~v$ and scalar coupling constants $\kappa (0)$, $\lambda_S (0)$ and $\xi_S (0)$.  The standard model without dark matter coupling corresponds to $\kappa (0) =0=\lambda_S (0)$.

\begin{figure}
\begin{center}
\includegraphics[scale=0.95]{potentialplot-Final-kappa2.pdf}
\end{center}
\caption{The Einstein frame renormalization group improved effective potential as a function of the canonically normalized Higgs-inflaton field.  The magnitude and shape of this potential in the inflationary cosmological state varies with the strength of the Higgs-inflaton and dark matter coupling constant $\kappa$.  The thickened portion of the potential curve corresponds to the $N_e =60$ e-folds of inflation with onset and exit values of $\sigma$ as shown.}
\label{EffPotential-1}
\end{figure}
\begin{figure}
\begin{center}
\includegraphics[scale=0.75]{potentialplot-Final-lamS012.pdf}
\end{center}
\caption{The Einstein frame renormalization group improved effective potential as a function of the canonically normalized Higgs-inflaton field.  The magnitude and shape of this potential in the inflationary cosmological state varies with the strength of the dark matter self-coupling constant $\lambda_S$ as compared to Fig. 1 for the different Higgs-inflaton to dark matter coupling $\kappa$.  The thickened portion of the potential curve corresponds to the $N_e =60$ e-folds of inflation with onset and exit values of $\sigma$ as shown.}
\label{EffPotential-2}
\end{figure}

As evident from Figs. \ref{EffPotential-1} and \ref{EffPotential-2}, the shape of the effective potential in the inflation region depends not only on the Higgs boson mass \cite{DeSimone:2008ei,Bezrukov:2008ej,Barvinsky:2009fy}, but also changes as the Higgs-inflaton to dark matter coupling and dark matter self-coupling varies.  The high energy suppression of the Higgs propagator also effects the running of the scalar coupling constants as seen in Figs. \ref{EffCoupling-Suppressed-1} and \ref{EffCoupling-Suppressed-2}.  The suppression factor is plotted along with the coupling constants whose $\beta$-function dependence on the suppression factor manifests itself in the abrupt change of running.
\begin{figure}
\begin{center}
\includegraphics[scale=0.71]{EffectiveCoupling-with-suppression-11.pdf}
\end{center}
\caption{The running coupling constants for the scalar fields.  The initial conditions for the coupling constants correspond to the effective potential plot of Fig. \ref{EffPotential-2} with $\kappa (0) =0.2$, $\xi (0)=8,315$ and $\xi_S (0) =0.0$.  In this case the onset of inflation occured at the scale $t_i=35$ with exit at $t_f=32.7$ after 60 e-folds of expansion.}
\label{EffCoupling-Suppressed-1}
\end{figure}
\begin{figure}
\begin{center}
\includegraphics[scale=0.75]{EffectiveCoupling-with-suppression-12.pdf}
\end{center}
\caption{The running of the non-minimal gravitational coupling constants for the scalar fields.  The initial conditions for the coupling constants correspond to the effective potential plot of Fig. \ref{EffPotential-2} with $\kappa (0) =0.2$, $\xi (0)=8,315$ and $\xi_S (0) =0.0$.  In this case the onset of inflation occured at the scale $t_i=35$ with exit at $t_f=32.7$ after 60 e-folds of expansion.}
\label{EffCoupling-Suppressed-2}
\end{figure}

The fractional rate of change of the effective potential is obtained from the renormalization group equations.  Recalling that
\begin{eqnarray}
\frac{d}{dt}\ln{\frac{\lambda}{\xi^2}} &=& 4\left( \frac{\beta_\lambda}{4\lambda}-\frac{\beta_\xi}{2\xi}\right) \cr
\frac{d}{dt}\ln{\frac{\psi^4}{(1+\psi^2)^2}}&=& 4\left( \frac{1-\gamma +\frac{\beta_\xi}{2\xi}}{(1+\psi^2)}\right) ,
\end{eqnarray}
it follows that
\begin{equation}
\frac{d}{dt}\ln{{V}_E}= \frac{4}{(1+\psi^2)}\left(1-\gamma +\frac{\beta_\lambda}{4\lambda}+\psi^2  \left[ \frac{\beta_\lambda}{4\lambda}-\frac{\beta_\xi}{2\xi}\right] \right).
\end{equation}
For larger values of $\lambda (0)$ and hence more massive Higgs bosons, the term in the square bracket can cancel the remaining bracketed terms since $\psi^2$ is getting large. Thus there will be some $t$ value at which the effective potential  reaches a maximum value, the wrong way roll point, before turning over and decreasing as the scale is increased.  For a Higgs-inflaton model to be viable,  it is thus necessary that the inflation must initiate  at $t_{i}$ values less than that of this relative maximum  or else the inflaton rolls to $m_{Pl}$ and beyond. The scale at which this cannot be accomplished sets an upper limit on the Higgs mass consistent with the inflationary cosmology model. It is typically below that of the  suppressed triviality bound which is mapped out in Appendix \ref{appendixB}.  Hence, an additional region of parameter space previously allowed by the suppressed triviality constraint, as seen in Fig. \ref{suppression}, will be ruled out due to the wrong way roll condition.  Likewise, for smaller values of $\lambda (0)$ that lead to a running close to the vacuum stability bound, $\beta_\lambda / \lambda$ is negatively large enough so that a relative maximum forms in the effective potential.  Thus once again, there is a region of parameter space not ruled out by vacuum stability but excluded by the wrong way roll condition.  Moreover, since the effective potential has a maximum before vacuum instability and the onset of inflation are reached, the wrong way roll excluded area covers that previously ascribed to vacuum instability.  The wrong way roll criterion more severely restricts the parameter space of the model than the requirement of absolute vacuum stability up to the onset of inflation.  For that matter, even if the absolute stability constraint is abandoned in favor of vacuum metastability \cite{Espinosa:2007qp}  with a lifetime longer than the age of the observable universe, then the additional range of Higgs boson masses allowed by this less stringent condition are ruled out by the imposition of the wrong way roll constraint. Hence for both low and high Higgs masses, additional regions of parameter space are excluded as they do not support slow roll inflation.  For typical values of the scalar parameters the wrong way roll excluded region of parameter space is displayed in Fig. \ref{NoRollConstraints}.
\begin{figure*}
$\begin{array}{cc}
  \includegraphics[scale=1.0]{slopeconstraintA.pdf}&
  \includegraphics[scale=1.0]{slopeconstraintB.pdf}\\
  \includegraphics[scale=1.0]{slopeconstraintC.pdf}&
  \includegraphics[scale=1.0]{slopeconstraintD.pdf}
\end{array}$
\begin{center}
\includegraphics[scale=1.0]{legend2.pdf}
\end{center}
\caption{The wrong way roll constraints for parameter space are added to those of vacuum stability and triviality (compare to Fig. \ref{suppression}).  These are displayed for typical initial non-minimal gravitational couplings of $\xi (0) = 10^4$ and $\xi_S (0) =0.0$.  The grey colored areas mark the wrong way roll excluded regions of parameter space.  The constraints apply to scales up to those typical of the onset of inflation, $t_i=34.5$.}
\label{NoRollConstraints}
\end{figure*}

For $\kappa(0)=\lambda_S(0)=0$, the allowed range of Higgs boson masses after the imposition of the wrong way roll constraint is roughly 155 GeV $< m_h < $ 182 GeV. This is a slightly smaller range than that allowed without the additional constraint which is 153 GeV $< m_h < $ 190 GeV (see Appendix B). Still considering $\lambda_S(0)=0$, as $\kappa(0)$ increases, the smallest allowed $m_h$ value consistent with the various constraints is approximately 130 GeV, which is roughly the same as without the wrong way roll constraint. This occurs when $\kappa(0)\simeq 0.3$. For larger values of $\kappa(0)$, the allowed parameter space vanishes. Once again, this is akin to the case without the wrong way roll constraint. As $\lambda_S(0)$ increases from zero, the allowed parameter space starts to shrink as a smaller range of $\kappa(0)$ values are permitted, while there remains a finite range of allowed Higgs boson masses.  Finally, for $\lambda_S(0) >0.25$, the allowed $\kappa(0)$ range vanishes for a finite range of  allowed Higgs boson masses. Hence the allowed parameter space disappears. While Fig. \ref{NoRollConstraints} corresponds to particular value of $\xi(0)$, the generic features continue to hold for a range of large $\xi(0)$ values.

The viable region of parameter space is further restricted by the requirement of yielding a value of the spectral index within its experimentally determined range.  Once the effective potential is determined, the cosmological quanities are calculated using equations (\ref{slowrollparameters}) and (\ref{spectral}).  The spectral index, its running and the tensor to scalar ratio are plotted versus the Higgs boson mass in Figs. \ref{CosmoQ-1} and \ref{CosmoQ-2} for various initial values of the Higgs-inflaton to dark matter coupling and for two initial values of the dark matter self-coupling.  The green area shown in Fig. \ref{CosmoParameterSpace-00} corresponds to model values of $n_s$ that are within one standard deviation of the experimental central value for the spectral index, $n_s=0.960$ \cite{Hinshaw:2008kr}.  The yellow area is determined by the predicted value of $n_s$ being between one and two standard deviations of its central value.  The orange regions correspond to $n_s$ predicted values to be within two to three standard deviations from the central value.  Finally the red regions indicate a predicted spectral index greater than three standard deviations beyond the central value.  The grey regions are excluded by triviality, vacuum stability and the wrong way roll conditions.

In general, as the Higgs boson to dark matter coupling strength, $\kappa (0)$, increases, lower values of the Higgs mass will still support a stable vacuum as well as avoid the wrong way roll condition.  However, a tension begins to arise between the experimentally allowed values of the spectral index and the model values of the index at low Higgs mass.  It follows from  Figs. \ref{CosmoQ-1}, \ref{CosmoQ-2}, and \ref{CosmoParameterSpace-00} that, consistent with the triviality, vacuum stability and wrong way roll constraints, agreement with the central measured value of $n_s$ favors a Higgs boson mass in the range 155-180 GeV and a smaller value of $\kappa(0)$. As $\kappa(0)$  grows to values greater than $\simeq 0.3$,  the computed value of $n_s$ lies between one to three standard deviations above the central measured value and occurs for smaller Higgs boson masses of order 130-145 GeV. Thus a discovery of a Higgs boson mass in this range favors a larger coupling to dark matter as is also preferred by the dark matter abundance calculations provided the dark matter is either lighter or heavier than $\sim m_h/2$. Note that there is no additional constraint arising from  $r$ and $\alpha$ as their computed values lie well below the present experimental limits.

As noted previously, the parameter space available shrinks as the  dark matter self coupling increases as displayed in Fig. \ref {CosmoParameterSpace-00} for different $\lambda_S(0)$ slices.  This self coupling is largely unconstrained by dark matter experiments and observations. For small dark matter mass (less than $\sim 1$ GeV) a correlation between the self coupling and mass may soften current discrepancies between the observed dark matter halo structure and numerical simulations of the structure formation process \cite{Bento:2000ah,McDonald:2001vt}.  Overall there is ample parameter space available for a consistent minimal standard model with the Higgs boson acting as the inflaton and interacting with scalar dark matter.
\begin{figure*}
$\begin{array}{cc}
\includegraphics[scale=0.95]{nsv5.pdf} &
\includegraphics[scale=0.90]{rv1.pdf} \\
\includegraphics[scale=0.90]{alpha1v1.pdf}
\end{array}$
\caption{The spectral index $n_s$, its running $\alpha$ and the tensor to scalar ratio $r$ are plotted against the Higgs mass $m_h$ for various values of the Higgs-inflaton to dark matter coupling constant $\kappa (0)$ for the fixed initial value of the dark matter self-coupling $\lambda_S (0) =0.0$.  Curve endpoints are determined by the wrong way roll, triviality and vacuum stability conditions. The dashed horizontal lines in the spectral index plot denote its central value, 0.960, and one and two standard deviations from it.}
\label{CosmoQ-1}
\end{figure*}
\begin{figure*}
$\begin{array}{cc}
\includegraphics[scale=0.95]{ns2v6.pdf} &
\includegraphics[scale=0.90]{r2v1.pdf} \\
\includegraphics[scale=0.90]{alpha2v1.pdf}&
\end{array}$
\caption{The spectral index $n_s$, its running $\alpha$ and the tensor to scalar ratio $r$ are plotted against the Higgs mass $m_h$ for various values of the Higgs-inflaton to dark matter coupling constant $\kappa (0)$ for the fixed initial value of the dark matter self-coupling $\lambda_S (0) =0.1$.  Curve endpoints are determined by the wrong way roll, triviality and vacuum stability conditions.  The dashed horizontal lines in the spectral index plot denote its central value, 0.960, and one and two standard deviations from it.}
\label{CosmoQ-2}
\end{figure*}
\begin{figure*}
$\begin{array}{cc}
\includegraphics[scale=1.0]{combiner1bg.pdf}&
  \includegraphics[scale=1.0]{combiner2bg.pdf}\\
  \includegraphics[scale=1.0]{combiner3bg.pdf}&
  \includegraphics[scale=1.0]{combiner4bg.pdf}
\end{array}$
\caption{The spectral index cosmological constraints on slices of parameter space for different dark matter self coupling $\lambda_S$ as determined by the degree of agreement with the experimental value of the spectral index, $n_s=0.960$.  These constraints are applied to the potentially allowed (green) areas displayed in Fig. \ref{NoRollConstraints}.  Here the green regions indicate the volume of parameter space that predicts spectral index values within one standard deviation of the central value.  The yellow regions correspond to calculated values between one and two standard deviations of the central value, while the orange regions correspond to two to three standard deviations from it.  The red areas indicate parameters that predict spectral index values more than three standard deviations from the central value.  Finally the grey region is excluded by triviality and vacuum stability bounds along with the wrong way roll condition.  For $\lambda_S (0) \ge 0.25$, there is no allowed region of parameter space.}
\label{CosmoParameterSpace-00}
\end{figure*}
\clearpage

\section{Conclusions \label{section4}}

The influence of the inclusion of dark matter on slow roll inflation models where the inflaton is identified with the standard model Higgs boson was explored.  To achieve this, the standard model was modified by the inclusion of an  hermitian scalar standard model singlet field, which accounts for the observed abundance of dark matter and the lack of its direct detection, and a large non-minimal coupling of the Higgs doublet to the Ricci scalar curvature. The model parameter space thus included the Higgs boson and singlet scalar masses, the scalar self coupling and the  coupling between the Higgs doublet and the dark matter in addition to the non-minimal gravitational couplings of both the Higgs doublet and the singlet scalar. In the inflationary region where the physical Higgs field develops a sizeable classical background, the presence of the large Higgs doublet non-minimal gravitational coupling results in a highly suppressed  physical Higgs field propagator. Accounting for this, the one-loop renormalization group improved effective potential was computed and the constraints on the model parameter space were delineated. In addition to the usual triviality and vacuum stability bounds, we focused on the cosmological constraints arising from the identification of the Higgs boson with the inflaton. Since, in general, the one loop effective potential develops a maximum, it was necessary to insure that the onset of inflation occurred such that the inflaton rolling was toward the origin and not towards the Planck scale. The implication of this wrong way roll constraint is displayed in Fig. \ref{NoRollConstraints} and is seen to eliminate even more of the parameter space than the vacuum stability (or metastability) constraint. Various parameters characterizing the slow roll inflation were computed with the spectral index, $n_s$, providing the most stringent constraint on the coupling constant space. As is seen in Fig. \ref{CosmoParameterSpace-00}, the region of parameter space allowed after the imposition of wrong way roll, triviality and vacuum stability constraints, is further partitioned into various sections whose agreement with the measured spectral index is only at a varying number (one - three) of standard deviations above the central value.  Larger values of the coupling of the Higgs-inflaton to dark matter, as is preferred by the dark matter abundance calculation, lead to a lower allowed range of Higgs boson masses.  In addition, there are the various Higgs mass bounds from accelerator experiments.  The direct LEP search \cite{Barate:2003sz} gives a lower bound of 114.4 GeV, while a fit to electroweak precision data prefers \cite{Grunewald:2007pm} a mass $m_h <$ 182 GeV.  Finally, a combined CDF and DO analysis of Tevatron data \cite{Benjamin:2009bn} excludes the range 160 GeV $< m_h <$ 170 GeV.  While our analysis has been limited to the one-loop radiative corrections, we anticipate that the general features of our results will continue to hold when two and higher loop corrections are included.  Thus we conclude that even after the inclusion of the dark matter, there still remains a range of LHC attainable Higgs boson mass values that are consistent with the cosmological parameters of slow roll inflation when the Higgs scalar is identified as the inflaton.

\begin{acknowledgments}
The work of TEC, BL and STL was supported in part by the U.S. Department of Energy under grant DE-FG02-91ER40681 (Theory).  The work of TtV was supported in part by a Cottrell Award from the Research Corporation and by the NSF under grant PHY-0758073.
\end{acknowledgments}
~\\

redpajama_set_name: RedPajamaArXiv


With the availability of Serial Attached SCSI (SAS) components, the next generation of business class storage technology has arrived. SAS, however, is not only the legitimate successor to UltraSCSI, but it will also enable new applications while boosting scalability to unprecedented levels. To demonstrate SAS' potential, we took a look at the technology, host adapters, hard drives and storage appliances.
SAS is not something entirely new, but it merges the best of two worlds. The first part is the serialized transmission of data, which requires far fewer physical connections. Moving from parallel to serialized operations has eliminated the use of a bus as well. Although the current SAS specification defines a 300 MB/s bandwidth per port, which is less than UltraSCSI's 320 MB/s, exchanging the sharedbus by point-to-point connections between devices is a huge advantage. The second important ingredient for SAS is the SCSI protocol, which is popular and powerful.
In addition to the interface specifics, SAS can take advantage of a large variety of RAID implementations. Storage giants such as Adaptec or LSI Logic offer comprehensive features that allow for expansion, transformation, migration, nesting and concurrency of RAID arrays across multiple controllers and drives.
Though almost being metamorphoses, most of these actions can even be performed on the fly today. In this context we should also mention the names AMCC/3Ware, Areca and Broadcom/Raidcore, because they helped move enterprise class features into the SATA space.
Compared to SATA, conventional SCSI is losing ground on all fronts, except for high-end enterprise applications. SATA offers adequate hard drives, attractive pricing and a wide selection of solutions. Another really smart feature of SAS is that it can be integrated with existing SATA infrastructures, which can be accommodated by SAS host adapters. However, SAS drives cannot run on SATA adapters.