Comparing two Excel sheets for differences in values the Compare and Merge Workbooks feature is available in all versions of Excel Use Spreadsheet Compare to find differences between two Excel workbooks. Office for business Spreadsheet Compare Spreadsheet Compare of excel in excel there is option for file comparison. where . / article/compare-two-versions-of-a-workbook-by-using-spreadsheet-.
We show you two easy ways to compare your spreadsheets: manually side-by- side and how to compare two excel sheets side by side. Comparison of lists of data is something that we do all the time. This tutorial gives details that you can apply immediately to compare lists using Excel to. To compare two Excel worksheets for differences, just open a new .com/office- addins-blog//02/25/compare-two-excel-files-sheets/.
A method to resolve the challenge of the lack of an in-built compare documents feature in Microsoft Excel (or track changes in previous versions), as well as an. Compare 2 Excel Files using View side by side Mode [Quick Tip]. Often we have 2 Select sheet 1 in first window, sheet 2 in second window. If you have two similar Excel spreadsheets, or different versions of the same original spreadsheet, it can be useful to compare the Excel files.


We really enjoy your Buttermilk Pancake & Waffle Mix. It is truly delicious and it really IS "Quick & Easy." Whenever we decide to have breakfast for dinner it seems like only 15 minutes later, we're eating pancakes! It has certainly made my lack of meal planning less noticeable. We even drive to the fancy Kroger to pick it up – the one with the wine bar inside. (We think that's a little silly, too.) It's a bit pricey though. Do you know why that is? We don't really mind. We think delicious pancakes are worth it.
Anyway, your packaging has this interesting little green badge down in the lower right corner. See it down there?
It states that your yummy Buttermilk Pancake & Waffle Mix is "76% Organic." Not 100 percent or 50 percent or any other percent. 76 percent. Hmmm. That's rather… specific. Isn't it?
I'd be curious to find out how a claim like that ends up on the packaging. I have my theories and I'm betting it's probably those folks over in Marketing, am I right? They'll pimp anything and I know that because I used to be in Marketing. They probably sat around a conference table and all agreed that the public would most definitely appreciate the fact that you're TRYING to produce something that's organic even if it's not entirely organic. Like we would appreciate your effort and that's worth touting!
Now, I'm sure you will tell me that this is all part of some sort of really detailed USDA regulation that mandates specific labeling when it comes to organic foods and that's fair. Still, I guess it seems like you're trying a little too hard. Or, actually, maybe you're not trying hard enough? I mean, what's holding you back from figuring out that other 24 percent? You should shoot for the moon here.
Seems like you have some work to do on your end, Arrowhead Mills. Just think of the celebration you could have with the folks from Marketing when you reach 100 percent! Those people LOVE to party.
P.S. – Unrelated but of a topical nature, do you know why this thing below explodes every time I open the cap? Is it a design flaw? Seeing as you are in the same industry, can you look into it for me? Because, no matter what I do or how I shake or do not shake the bottle, as soon as I flip the cap, BLAMMO! Ketchup everywhere.
I do not like how this works.
Joanna • This entry was posted in Irritating and tagged arrowhead mills, dinner. Bookmark the permalink.


text:
North Korea fires another missile
THE Deputy Prime Minister has warned we could be vulnerable to North Korea's nuclear weapons, and hinted Australia would retaliate.
Liz Burke
@lizeburke
North Korea's ballistic rocket Hwasong-12 fired over Japan last month. Another missile has been launched following a similar trajectory. Picture: AFP Photo/KCNA via KNS
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DEPUTY Prime Minister Barnaby Joyce has warned North Korean missiles could potentially reach Australia after the rogue nation this morning launched its longest-ever missile flight.
The intermediate-range missile was launched from Pyongyang and flew over Japan just after 8am AEST.
The missile is believed to have taken a similar trajectory to a weapon fired over Japan last month, and flew about 3700km.
South Korea's military reported the weapon reached an altitude of about 770km and was in the air about 19 minutes, making its path both higher and further than the previous device launched.
The distance is far enough to reach the US Pacific territory of Guam, which North Korean leader Kim Jong-un only last month threatened to fire missiles at.
Prime Minister Malcolm Turnbull condemned the attack and emphasised Australia's alliance with the US and how both nations would come to the other's aid in terms of the attack, but refused to speculate about any "scenarios".
His deputy leader, however, was happy to speculate.
Addressing reporters, Mr Joyce suggested the range of missiles being tested could reach South Australia, AAP reports.
"If you have now set off a hydrogen bomb and you have the capacity to miniaturise is to vaporise and murder millions and millions of people, the world is not going to stand idly by," he said.
Mr Turnbull condemned North Korea's latest missile test, saying it was a sign the regime was frustrated by tough new United Nations sanctions.
Mr Turnbull told Sky News on Friday the test was a sign the sanctions were working.
"This is another dangerous, reckless, criminal act by the North Korean regime, threatening the stability of the region and the world," he said.
"We utterly condemn it ... what we do need to do is maintain the united global pressure on this rogue regime to bring it to its senses."
Mr Turnbull later told reporters a North Korean attack on the United States, as Kim Jong-un has previously threatened, would be like "signing a suicide note".
"Nobody wants to see a war on the Korean Peninsula," he said.
"If Kim Jong-un were to start a war, to attack the United States or one of its allies, he would be signing a suicide note.
"That would be the end for his government and thousands and thousands of people would die."
The White House confirmed US President Donald Trump had also been briefed on the launch, but was yet to comment.
The Pentagon confirmed the missile fired was an intermediate range ballistic missile (IRBM) and said it did not pose a threat to North America.
US defence secretary Jim Mattis called Friday's launch a reckless act by the North Koreans.
.@TurnbullMalcolm: It's another dangerous, reckless, criminal act by the North Korean regime and we condemn it MORE https://t.co/cFxxN5UZI4 pic.twitter.com/oJ1y09Vhb8
— Sky News Australia (@SkyNewsAust) September 14, 2017
Japan has previously vowed to shoot down any North Korean missile or rockets threatening to hit its territory, but instead responded to this morning's launch by warning residents to take cover and stay away from anything that could be debris from the weapon.
Japanese authorities today said the nation protested the latest launch in the strongest terms and would take appropriate and timely action at the United Nations and elsewhere.
Chief Cabinet Secretary Yoshihide Suga said Japan was staying in close contact with the United States and South Korea.
"Japan can never tolerate this repeated provocative action by North Korea," Mr Suga told reporters in Tokyo.
"We have strongly protested to the North, telling them the strong anger by the Japanese people and condemn with the strongest words possible."
A Japanese Self-Defence Force Patriot Advanced Capability-3 (PAC-3) missile launcher is seen at its position in the Defence Ministry headquarters in Tokyo. Japan did not attempt to shoot down the North Korean missile. Picture: Toshifumi Kitamura/AFP Photo
The August 29 launch was roundly condemned by Japanese Prime Minster Shinzo Abe, Mr Trump and allies.
Today's test also follows the rogue nation's largest test of a nuclear weapon on September 3, when North Korea claimed it successfully launched a hydrogen bomb.
Minutes before today's blast, the top commander of US nuclear forces said he "assumes" the September 3 test was in fact a hydrogen bomb, suggesting a heightened concern that the North had advanced to a new level of nuclear fire power.
Air Force General John E. Hyten, commander of Strategic Command, told reporters that while he was not in a position to confirm it, he assumed from the size of the underground explosion and other factors that it was a hydrogen bomb — which is a leap beyond the fission, or atomic, bombs North Korea has previously tested.
Moments after he made the remarks from the US, reports of today's launch emerged. Hyten made no mention of the launch.
North Korea claim it successfully tested a hydrogen bomb. Picture: KCNA/AP
The blast is believed to be in retaliation of sanctions against the rogue nation announced this week in response to its sixth nuclear test.
It comes just a day after North Korea threatened to sink Japan and reduce the United States to "ashes and darkness" for supporting a UN Security Council resolution imposing the new sanctions.
Pyongyang's Korea Asia-Pacific Peace Committee, which handles the North's external ties and propaganda, also called for the breakup of the Security Council, which it called "a tool of evil" made up of "money-bribed" countries that move at the order of the United States.
"The four islands of the archipelago should be sunken into the sea by the nuclear bomb of Juche. Japan is no longer needed to exist near us," the committee said in a statement.
North Korean leader Kim Jong-un has made repeated threats. Picture: AP Photo/Wong Maye-E
The North also targeted the US directly. "Let's reduce the US mainland into ashes and darkness. Let's vent our spite with mobilisation of all retaliation means which have been prepared till now," the statement said.
The threat also followed the release of satellite imagery taken just days after the September 3 nuclear test, showing the secretive state may be preparing for another blast.
Subsidence crater and scars
Possible crater and landslide scars
South Korean and US militaries are analysing details of the launch, and the South's presidential Blue House has called an urgent National Security meeting following the launch.
Seoul's military carried out a ballistic missile drill of its own on Friday in the East Sea, Korea's name for the Sea of Japan, the Yonhap news agency reported.
North Korea has raised tensions in the region with its rapid progress in weapons technology under leader Kim Jong-un, who is closely associated with the program and regularly pictured by state media overseeing launches and visiting facilities.
A damning new report has claimed to have exposed several instances of China overstepping its reach under a shady "anti-corruption" policy.
The world's best tennis players have been asked about the safety of China's Peng Shuai, with Ash Barty unable to answer one particular question.
More than 2000 animals will be killed after Covid-19 cases were linked to a pet shop, in a move that's upset animal rights activists.

redpajama_set_name: RedPajamaCommonCrawl


я добавил иконок. под названием ad1. ad2. и тд.
как или через какую команду можно ( изменить/добавить игроку на сервере ) иконку которую я добавил ??
Ps. ЧТобы это иконка оставалась на всегда ???
а что в pvpgn- есть команда /icon ???
если да то возможно сделать чтобы только админы могли давать икоки остальным ?
Шевели мозгами, тебе надо переписать код (поставить условие что игрок является админом или как ты хочешь).
или если есть тут тема про иконки дайте ссылку плз.
Добавил новую настройку "master_commandgroups" в icons.conf, в ней можно перечислить группы, которые смогут управлять иконками. Ранее это было разрешено всем админам и операторам.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\conf\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\man\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\files\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\compat\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\common\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\win32\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\tinycdb\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bntrackd\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\client\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bniutils\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bnpass\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bnetd\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\d2cs\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\d2dbs\CMakeFiles\". Устройство не готово.
1>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\test\CMakeFiles\". Устройство не готово.
2>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
2>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\tinycdb\Release\". Устройство не готово.
3>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
3>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\win32\Release\". Устройство не готово.
4>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
4>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\common\Release\". Устройство не готово.
6>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
6>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
6>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bniutils\Release\". Устройство не готово.
5>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
5>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\compat\Release\". Устройство не готово.
7>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
7>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
7>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\test\Release\". Устройство не готово.
8>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
8>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
8>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
8>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/win32/win32.vcxproj' does not exist.
8>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\d2cs\Release\". Устройство не готово.
9>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
9>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
9>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
9>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/win32/win32.vcxproj' does not exist.
9>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\d2dbs\Release\". Устройство не готово.
10>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
10>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
10>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
11>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
11>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
11>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
10>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bnpass\Release\". Устройство не готово.
11>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bntrackd\Release\". Устройство не готово.
12>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
12>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
12>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
13>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
13>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
13>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
12>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\client\Release\". Устройство не готово.
13>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bnpass\Release\". Устройство не готово.
14>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
14>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
14>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
15>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
15>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
15>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
15>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bniutils\Release\". Устройство не готово.
14>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bniutils\Release\". Устройство не готово.
17>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
17>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
17>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
17>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\client\Release\". Устройство не готово.
16>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
16>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
16>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
16>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bniutils\Release\". Устройство не готово.
18>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
18>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
18>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
18>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/tinycdb/tinycdb.vcxproj' does not exist.
18>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/win32/win32.vcxproj' does not exist.
18>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bnetd\Release\". Устройство не готово.
19>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
19>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
19>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
19>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\client\Release\". Устройство не готово.
20>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
20>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
20>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
20>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/tinycdb/tinycdb.vcxproj' does not exist.
20>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\tinycdb\Release\". Устройство не готово.
21>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
21>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
21>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
21>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\client\Release\". Устройство не готово.
22>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
22>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
22>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\test\Release\". Устройство не готово.
23>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
23>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
23>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
23>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(301,6): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\src\bniutils\Release\". Устройство не готово.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/ZERO_CHECK.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/test/bigint.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/client/bnbot.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/tinycdb/bncdb.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/client/bnchat.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/bnetd/bnetd.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/test/bnetsrp3_test.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/client/bnftp.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/bniutils/bni2tga.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/bniutils/bnibuild.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/bniutils/bniextract.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/bniutils/bnilist.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/bnpass/bnpass.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/client/bnstat.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/bntrackd/bntrackd.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/common/common.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/compat/compat.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/d2cs/d2cs.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/d2dbs/d2dbs.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/bnpass/sha1hash.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/bniutils/tgainfo.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/tinycdb/tinycdb.vcxproj' does not exist.
24>C:\Windows\Microsoft.NET\Framework\v4.0.30319\Microsoft.Common.Targets(1200,9): warning : The referenced project 'E:/Ghost ++/pvpgn/build/src/win32/win32.vcxproj' does not exist.
24>C:\Program Files\MSBuild\Microsoft.Cpp\v4.0\Microsoft.CppBuild.targets(806,5): error MSB3191: Не удается создать каталог "E:\Ghost ++\pvpgn\build\CMakeFiles\". Устройство не готово.
Если построение делается через Magic Builder, то не использовать в пути пробелы, и возможно символ "+".
harpywa почему хотел скомпилировать новый сервер.
а где можно исходники взять?


text:
Walpole Express Hockey
Sullivan Commits To Gustavus
By @ExpressJrMens, 12/15/20, 4:45PM EST
Walpole, MA - The Walpole Express are proud to announce the commitment of Justin Sullivan to Gustavus Adolphus College. Gustavus is located in St. Peter, MN and competes in the MIAC. Justin is the 4th player off the Express roster to commit to a college this season.
Sullivan spoke about why he made the decision to commit to Gustavus, saying, "Academics have always come before hockey for me. So, when I was presented with the opportunity to go to such a prestigious academic school like Gustavus it really seemed like a no brainer."
"As an athlete I know how much the coaches at Gustavus care about their players, and how hard they work to develop each player into the best that they can be," added Sullivan.
Express Coach Cody Campbell had great things to say about the recently committed Sullivan, "Justin has been a offensive threat for us all year long. He has also taken major steps in his play without the puck that has made him effective even if he isn't producing points. We are thrilled for Justin as he has absolutely earned the opportunity he has to be a student athlete at Gustavus."
"Playing for Coach Campbell and the Express has helped me reach my goal of playing college hockey in many different ways. He has given me the opportunity and the confidence to play to the best of my ability every time I touch the ice. Without his help I'm not sure where I would be as a player," Sullivan said about the reigning Eastern Hockey League Coach of the Year.
Please join the entire Express organization in congratulating Justin Sullivan on his NCAA College Commitment.
Tag(s): EHL
This website is powered by SportsEngine's Sports Relationship Management (SRM) software, but is owned by and subject to the Walpole Express Hockey privacy policy. ©2020 SportsEngine, Inc.


Come to the RPL for a Halloween story, craft, and candy hunt!
There will NO Preschool Storytime this Monday, October 29. Instead, we are having a special HALLOWEEN STORYTIME on Wednesday, October 31!
Join Storytime Lady Sianna on Halloween at 4pm for a story, craft project, and candy hunt. Costumes are highly encouraged!
Our preschool storytime program is designed for kids age 0-7, but all are welcome!
THE RPL HAS PROGRAMS FOR ALL AGES!
Residents are welcome to attend.
Must have great written communication skills.
The ideal candidate would be available to fill in to take minutes for other board meetings as needed.
The Budget Committee meets quarterly and also almost weekly in the fall on Wednesday nights at the town office at 6:30pm.
The Town of Rollinsford is seeking a qualified individual to complete bookkeeping and administrative tasks on a temporary to permanent basis. This is a part-time position, 20 hours per week, located in Rollinsford, NH.
Please send resume and cover letter to: Rollinsford Select Board, PO Box 309, Rollinsford NH 03869 or email selectboard@rollinsford.nh.us.
Rollinsford resident Stephen H. Roberts has been chosen by the Association of Rollinsford Culture and History (ARCH) as the 2018 recipient of the ARCH Heritage Award, which is presented annually to a person who has made significant contributions to the preservation of the history, heritage and culture of Rollinsford and the lower Salmon Falls region. The award will be presented at the organization's annual dinner and auction gala on Saturday, November 17 at Spring Hill in South Berwick, ME.
Roberts is a partner in the law firm of Hoefle Phoenix Gormley and Roberts in Portsmouth, and is a retired district court judge. In addition to his efforts on behalf of ARCH and the Wentworth House, Roberts also currently serves as president of the Board of Trustees of the Portsmouth Athenaeum,which maintains a library of over 40,000 volumes and an archive of manuscripts, photographs, objects, and ephemera relating to local history.
Budget workshop on Monday, October 29, 2018 at 6:00pm. The Select Board meeting will start at 6:30pm.
Budget Workshop on Saturday, November 3, 2018 at 9:00am.
The above meetings will be at the town hall.
Wednesday, October 24, 2018 at 6:30pm at the Town Office.
Tuesday, October 23, 2018 at 6:00pm at the District office on Front Street.
On Saturday, October 27, the Rollinsford Police Department will be participating in the DEA Take Back Drug Campaign. The PD will be open from 10 am to 2 pm so residents can drop off unwanted, outdated, medications, pills, etc., no questions asked.
If you are unable to make it to the pd that day, you can make arrangements for pickup or drop off at the pd that is convenient to you by calling our dispatch center at 742-2724 or by emailing Chief Bob Ducharme.
Lets keep these items out of the hands of people who should not have them.
The Supervisors of the Checklist will be holding the last session before the Nov 6th General Election.
This is an opportunity to register to vote or to change party affiliation prior to the election.
This meeting will take place at 7:00pm in the meeting room of town hall.


text:
Egyptian TV Swayed Public Against Morse, in Favor of Sisi
Egyptian TV Swayed Public Against Morse, in Favor of Sisi by Eoin Treacy
This article by Matt Bradley for the Wall Street Journal may be of interest to subscribers. Here is a section:
Mr. Sisi, who as army chief removed Mr. Morsi from office last July and then oversaw a crackdown on his supporters from behind the scenes, is on his way to being elevated to the presidency after a new election this week, the second held since the 2011 overthrow of longtime ruler Hosni Mubarak. Preliminary results published by state media after polls closed Wednesday showed Mr. Sisi with over 90% of the vote.
Given their huge power to shape public opinion, Egypt's news media seem sure to play a decisive role in the success or failure of Mr. Sisi's presidency, as well.
His luster may already be wearing off. In a move that revealed deep official disappointment with low turnout in the election Monday and Tuesday, electoral authorities extended the polls to Wednesday.
Pro-Sisi television presenters, including OnTV's hosts, reacted with rage to the low turnout, accusing the public of being lazy, selfish and even treasonous.
"I'm willing to cut my veins for the country—right now, on air—for people to go down and vote," said Amr Adeeb, a presenter on the Al Youm channel.
In the nearly yearlong military crackdown on Morsi supporters that followed his July 3, 2013, overthrow by Mr. Sisi, as many as 30,000 Egyptians have been arrested and more than 1,000 killed by security forces in street violence, according to human-rights groups.
Mr Modi's victory can be viewed as a massive step forward for the prospects of India standards of governance improving. Indonesia's upcoming presidential election has equal potential to cause an upset but the result will likely be much closer. Very often democracy goes hand in hand with improving standards of governance because populations generally vote for what will improve their individual standards of living. However democracy represents only part of the challenge of fostering a vibrant middle class. Property rights, respect for minority shareholders, an improving regulatory structure, infrastructure and education are all also important ingredients.
The election of Mr Morsi following the Arab Spring was democratic but it is questionable whether the other ingredients for growth would have been met under his administration. Mr. Sisi is likely to ensure public unrest is held in check through whatever means are necessary and will be eager to encourage investment to help alleviate the high youth unemployment that was one of the primary fuels for the Arab Spring. However, investors are probably going to want to see how his administration is going to deal with these challenges and particularly how they will differ from the last military administration.
The Egyptian Pound stabilised following its steep devaluation in the first half of 2013 but its renewed weakness over the last month suggests the new government will be constrained in how much it can do with the budget and is likely to continue to be heavily reliant on foreign investment.
The stock market posted a large key day reversal today suggesting supply dominance in the region of the March peak. At least a process of mean reversion appears to be underway.
Elsewhere in the Middle East, the Saudi Arabian Index is closing in on the psychological 10,000 level and while somewhat overextended relative to the 200-day MA in the short term, a sustained move below 9000 would be required to question medium-term uptrend consistency.
The Dubai Index has bounced back from last week's low and will need to hold above 4500 if the medium-term uptrend is to be given the benefit of the doubt.
The Qatar Index surged higher over the last week and some consolidation of recent gains appears likely. A break in the progression of higher reaction lows, currently near 12,700 would be required to check the consistency of the overall uptrend. (Also see Comment of the Day on October 18th 2013).
The UK listed, US Dollar denominated Qatar Investment Trust continues to trade at a discount to NAV of 10.89%. While the pace of the trust's advance has picked up, a break in the progression of higher reaction lows would be required to question medium-term potential for additional upside.
The US listed Market Vectors Gulf States ETF completed a first step above the base in December and continues to extend its uptrend. A sustained move below last week's low near $31.80 would be required to check the advance.


Your Riviera Holiday captured in a dress this season is the Tropez Ruffle Midi. An exclusive scarf print features in symmetrical placement to flatter. A subtly shaped neckline is enhanced with tapered ruffles over the bust and across the shoulders while a mock central tie adds sopistication. Fuly lined throughout.


It's a re-post by GLORI Foundation — the English original can be found through this link.
With cities across the globe growing rapidly, the future looks set to be urban with an estimated 66 percent of the population to be living in urban areas by 2050 up from 54 percent today. The number of megacities housing over 10 million people has tripled since 1990 to 31 with the United Nations forecasting this will rise to 41 by 2030. While cities can drive development and reduce poverty, rapid urban growth can also create a new set of problems if the right infrastructure is not in place or policies don't ensure the benefits of city life are equally shared.
In the first poll of its kind, the Thomson Reuters Foundation asked experts in women's issues which of the world's megacities are safe for women – and which need to do more to ensure women are not at risk of sexual violence and harassment and harmful cultural practices and have access to healthcare, finance and education.


text:
Vlinderc
=====

** TODO: Add description **

redpajama_set_name: RedPajamaGithub


Stress & depression – the greatest challenges facing us today.
Stress and depression are becoming a significant health issue in Australia. There is a great deal of isolation, not only within the community, but even within the family. Originally the family was the strongest foundation in society, but with so many family breakdowns occurring, we are becoming vulnerable to greater stress and depression.
In many cases stress and depression go undiagnosed and it can take years until there is a significant illness or emotional problems (Such as anger, panic attacks, prolonged crying spells, rashes, allergies, breathing difficulties etc) that will be the first hint that something is wrong.
How can you help someone with stress or depression?
The first step is self empowerment. A significant factor in stress and depression is addressing how we breathe. There are many clinical studies that show that specific breathing techniques will affect the chemicals in the brain and lead to a feeling of calm and peace.
Depression and stress are not one dimensional, they are a multi faceted problem. It is important to still the mind and its incessant thoughts. The next step after breathing is meditation. Meditation is an essential skill which we have taught at the College with great success. I would encourage everyone to attend our practical meditation course which focuses on giving participants the skills and techniques to achieve a stress free life. I promise, that if the techniques taught in the course are followed, this can be so.
Depression and stress can also be caused by the dynamics in a relationship.
Counselling and supportive guidance can help the person to understand and express themselves effectively. I often see couples or individuals whose problems are to do with communication. In this instance, it is important to teach the skills and techniques of effective and clear communication, so that we are able to communicate with honesty and openness. There is a need for greater emotional intimacy in relationships.
Specific healing technques are used. i.e. Ajna Tibetan Healing is extremely effective in balancing the body and enabling the person being healed to transcend the emotional and mental aspect of the illness they are facing. By working with the body on a physical level, we can make significant changes in the way the person is responding to their stress, depression or other illnesses, such as trauma, abuse, separation, grief, migraines, allergies, chronic fatigue, addictions etc.
Grandmaster Dr Issam is available for counselling & healing consultations (including couples counselling) on Monday,Tuesday and Friday. To book in a counselling or healing session, please contact 0402 944 303.


Oral history interviewing is a documentary technique that preserves the cultural heritage of people from all economic and social classes by recording individuals' reminiscences about events that impacted their lives. The sound recordings and their transcriptions produce a rich body of primary resource material that can be a useful tool for historians, genealogists, and other researchers. Below you will find information on the nature and scope, process, availability and digitization status of the Forest History Society's oral history collection.
The Society's Oral History Interview Collection includes more than 250 oral history interviews (OHIs) conducted with individuals involved with the management and use of forests and their related resources. The sound recordings are in various analog formats, including reel-to-reel recordings, stenorette tape recordings, and cassette recordings. Most interviews have at least rough transcriptions in typescript format. Electronic transcriptions for more recently conducted interviews are available for research in the Society's library, and some are accessible from links in our Annotated Guide to the FHS Oral History Collection.
Subjects discussed in our oral history interviews broadly pertain to the history of human interaction with the forested environment. Many people interviewed by the Society in the 1940s and 1950s were veterans of the forest products industry whose first-hand accounts of momentous events document critical policy changes that occurred within the industry in the late-nineteenth and early-twentieth centuries. As the boundaries of the field of forest history broadened in the 1960s, 1970s, and 1980s to include the associated fields of conservation and environmental history, the Society's OHI mission expanded to include projects that recorded the reminiscences of forestry educators and researchers, conservationists, and employees of American government agencies charged with managing natural resources. Several interviews conducted over the last couple of decades relate the contentious political atmosphere experienced by women who held relatively high positions of leadership within the United States Forest Service (USFS) or describe the challenges endured by heads of the USFS and the United States Environmental Protection Agency (EPA).
The oral history technique employed by the Society is essentially the same as that generally accepted and practiced by other oral history programs in the United States. The subject field and respondent are carefully selected and researched prior to the interview. The interviewer then meets the interviewee and establishes a plan for conducting the interview during several sittings. Hours of tape-recorded question-and-answer sessions follow. The tapes are transcribed to a rough typescript that is edited for accuracy by all parties to the interview. Some interviews have been footnoted, illustrated, and indexed before being copied and bound. Interviews are copyrighted with the Library of Congress.
All interviews are available for research in the Society's library, and copies of many can be found in other libraries' collections. Copies of interview transcriptions are available for purchase. The Society's Annotated Guide to the FHS Oral History Collection provides summary information about each interview; some descriptions include links to online transcriptions. The interviews are also searchable via the Oral History section of the FHS Research Portal, which provides brief descriptions of oral history interviews conducted by FHS and others.
To requests copies or other information pertaining to the collection, contact FHS library staff.
No part of an interview may be used or reproduced in any manner without written permission, except in the case of brief quotations.
The Society, with Philadelphia's George Blood, L.P., has completed a test project to digitize a small sample of recordings from its Oral History Interview Collection, including an mp3 of paper industry leader Reuben B. Robertson in 1959 recounting some of his impressions of Dr. Carl Alwin Schenck, founder of America's first forestry school at George Vanderbilt's Biltmore Estate in Asheville, North Carolina. This interview with Robertson is included in the Early Forestry Education in North Carolina Oral History Collection.


Can you imagine what our society will look like at the end of the decade? How will we shop, socialise and consume services?
How as businesses will we authenticate customers, manage our services and protect critical data from a growing array of increasingly sophisticated and determined adversaries?
Of course, we don't have all the answers at Trend Micro but we've taken a big step in the right direction with our 2020 web-series.
With 2020 we're trying to get everyone from policy-makers and IT bosses to school kids, to start thinking about the future, how technology will influence our lives at the end of this decade and the implications for data security and privacy.
So often in the information security industry we restrict ourselves by operating to 12 month prediction cycles, but as we all know, advances in technology and online threats move at a much faster rate.
IT professionals in particular need to think further into the future to better fortify their systems against attack and avoid wasted investments in outdated technology.
We hope this nine video series will help get the ball rolling.
Based on an ICSPA report "Project 2020 Scenarios for the future of cybercrime", the web series is set in the fictitious European country of South Sylvania.
A technologically advanced nation where every citizen maintains multiple online profiles, with a secure centralized hub known as The Switch managing authentication as they move between each.
The majority of citizens in this future world wear contact lenses or glasses through which they consume personalized digital content, including advertising and marketing, all served up by a burgeoning Content Service Provider industry.
Episode one, launched today, introduces us to South Sylvania on the eve of its first all-digital election. We meet Kinuko, a twenty-something software engineer and digital native; Prime Minister Carrington, Yanek, a career cyber criminal; and Adam, a hacktivist.
Trend Micro invested a great deal of time, effort and thought into creating this online video series. The future of our society is intrinsically linked to advances in technology and the ways people find to subvert it, so we hope 2020 will get as many folk as possible thinking about what may happen as we approach the end of the first decade of the 21st Century.


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text:
\section{Introduction}
\label{sec:intro}

Gamma--ray bursts (GRBs) are transient emission episodes of radiation
detected at high energies.  The first emission phase, detected at hard
X--rays and $\gamma$--rays, lasts for $\sim$~0.01 ms--100 s (prompt
phase).  Then, the bulk of emitted radiation shifts to lower energies
and becomes observable at longer wavelengths, from X--rays to radio,
with typical duration of $\sim$~days--months (afterglow phase).  The
observed duration of the prompt phase is characterised by the $T_{90}$
parameter, i.e. the time interval during which the central 90\% of the
counts are recorded by the detector.  The distribution of $T_{90}$ of
GRBs observed by the Burst And Transient Source Experiment (BATSE) on
board the Compton Gamma Ray Observatory ({\it GCRO}) has been found to
be bimodal with a separation at $\sim$~2 s in the observer frame
\citep{1993-Kouvelioutou-shortVsLong}.  According to this finding,
GRBs are classified either as {\it short} gamma--ray burst (SGRB) if
$T_{90} <$~2, or as {\it long} ones (LGRB) if $T_{90} >$~2 s (but see
\citealt{2013-Bromberg-ShortVsLongCollapsars}).  Besides, the prompt
phase of SGRBs is characterised by harder spectra
\citep{1993-Kouvelioutou-shortVsLong} and smaller spectral lags
between different energy bands \citep{2000-Norris-SpecLag} with
respect to the prompt phase of LGRBs.

For bursts with reliable redshift estimates, it has been shown that
SGRBs are systematically less energetic than LGRBs, with total X and
$\gamma$--ray emitted energies smaller by a factor $\sim$~10--100
\citep{2009-Ghirlanda-ShortVsLong}.  Also, the afterglows of SGRBs,
when detected, are correspondingly dimmer than those of LGRBs, but
similar in other respects \citep{2008-Gehrels-PromptAfterglow,
  2013-Margutti-PromptAfterglowConn, 2014-DAvanzo-SBAT8}.  Finally,
several nearby ($z<0.5$) long GRBs have been associated with
explosions of core--collapse supernovae
\citep{2012-Hjorth-GRB-SN-Connection}, while there is no similar
evidence for short bursts \citep{2013-Berger-SGRB}.  These findings
suggest that short and long GRBs might originate from different
progenitors (\citealt{2006-Meszaros-GRB, 2013-Berger-SGRB}).

Observationally, the most important difference between short and long
GRBs is their $T_{90}$ duration.  A first attempt to compare the
spectral properties of short and long GRBs detected by {\it
  CGRO}/BATSE showed that (i) the difference in hardness could be due
to a harder low energy spectral index of short GRBs rather than a
harder peak energy and (ii) that the spectra of SGRBs and the first
1--2 s of LGRBs appear similar \citep{2004-Ghirlanda-SpectraSGRB}.
These results suggested that the engine might be similar in the two
classes, but the activity would last longer in the case of LGRBs
\citep{2010ApJ...725..225G}.  Also, \citet{2002-Nakar-TempoPropSGRB}
found that the ratio of the shortest pulse duration to the total burst
duration for both short and the first 1--2 s of long GRBs were
comparable.

With the advent of the Gamma Burst Monitor (GBM) on board {\it Fermi},
it became possible to compare the spectral properties of large samples
of short and long GRBs and to compare them with those detected by {\it
  CGRO}/BATSE.  \citet{2011-Nava-GBMBatseComparison} showed that long
and short GRBs occupy different regions in the observer frame hardness
(defined by the peak of the $\nu F_\nu$ spectrum) versus fluence, with
SGRBs having smaller fluences than long events. This also suggested
that the possible selection of fluence limited samples for the
comparison of SGRBs and LGRBs could introduce biases.

The availability of redshift estimates for long GRBs allowed one to
estimate their rest frame (intrinsic) spectral properties, and to
highlight a few correlations among them (see
\citealt{2006-GhirlandaRev-GRBCorrCosmo} for a review).
\citet{2002-Amati-rel} found that the rest frame $\nu L_{\nu}$ peak
energy ($E_{\rm p}$) is correlated with the total energy emitted in
the 1 keV--10 MeV energy range (under the hypothesis of isotropic
emission, $E_{\rm iso}$), with a slope of $\sim$~0.5.
\citet{2004-Yonetoku-EpLiso} found a correlation between $E_{\rm p}$
and the isotropic peak luminosity evaluated at the flux peak over an
interval of 1 s ($L_{\rm p,iso}$), with a slope of $\sim$~0.4.  The
latter correlation is valid also when considering the time resolved
spectral quantities $E_{\rm p}(t)$ and $L_{\rm iso} (t)$ of a single
burst, i.e. the evolutionary tracks of GRB spectra in the $E_{\rm
  p}$--$L_{\rm iso}$ plane align with the Yonetoku relation
\citep{2009-Firmani-TimeResolvedCorrel,
  2010-Ghirlanda-TimeResolvedFermi, 2012-Frontera-TimeResolvCorr}.

With the fast slewing {\it Swift} satellite \citep{2004-Gehrels-Swift}
it became possible to localize the X--ray afterglows of short GRBs,
and estimate their redshifts by means of the associated host galaxies
\citep{2005-Gehrels-ShortAfterglow}.  The comparison of intrinsic
spectral properties of short and long GRBs have shown that short GRBs
are consistent with the Yonetoku relation, but are significant
outliers of the Amati relation \citep{2006-Amati-rel-update,
  2008-Amati-rel-5SGRB, 2009-Ghirlanda-ShortVsLong,
  2014-DAvanzo-SBAT8}.  However, by analyzing a sample of 7 short
GRBs, \citet{2012-ZhangRevisitingLongShortClassif} suggest that short
GRBs might follow a parallel Amati relation at lower values of $E_{\rm
  iso}$.  Moreover, the SGRBs follow the same three parameter
correlation ($E_{\rm X,iso}$--$E_{\rm \gamma,iso}$--$E_{\rm p}$) valid
for long GRBs \citep{2012-Bernardini-UnivScalingRel3Param,
  2013-Margutti-PromptAfterglowConn}.  The isotropic luminosities are
similar in both short and long GRBs, but the former are less energetic
than the latter by a factor similar to the ratio of their durations.
When considering the time averaged spectra, short GRBs have harder
low--energy spectral index, but this difference vanishes when
comparing the SGRBs with only the first 1--2 s of long GRBs
\citep{2009-Ghirlanda-ShortVsLong}.

Also the time resolved spectroscopy has shown that the observed peak
energy tracks the flux evolution in both short and long GRBs
\citep{2010ApJ...725..225G, 2011-Ghirlanda-ShortVsLong}, suggesting a
common physical mechanism linking these quantities.  The existence of
a time resolved correlation between $E_{\rm p}(t)$ and $L_{\rm
  iso}(t)$ was also shown to hold in short GRBs
\citep{2011-Ghirlanda-ShortVsLong}.  This is the most compelling
evidence that the $E_{\rm p}(t)$--$L_{\rm iso}(t)$ correlation holding
in long and short GRBs (with similar slope and normalization) hints to
a common origin which could be related to the emission mechanism
\citep{2011-Ghirlanda-ShortVsLong} and that the corresponding Yonetoku
correlation (holding between time integrated properties) cannot be
subject to strong selection effects.  An interesting hypothesis
discussed in \citet{2009-Ghirlanda-ShortVsLong,
  2011-Ghirlanda-ShortVsLong, 2013ApJ...770...32G} is that both short
and long GRBs may share a common emission process, and that the
observed differences may be ascribed to the different engine lifetime
of their progenitors.

Yet, the comparison of short and long GRBs in search for possible
similarities or differences should account for their possible
different redshift distributions.  While several LGRBs have their
redshift measured, the population of short bursts still suffers from a
lack of redshift measures. However, recent collection of small, well
defined, samples of SGRBs with measured redshifts
\citep[e.g.][]{2014-DAvanzo-SBAT8} allowed us to compare the energetic
properties of short and long events in their rest frame.

The aim of this work is to further explore the similarities between
short and long GRBs by comparing their intrinsic (i.e. rest frame)
spectral properties estimated on the same rest frame time scales.  The
average $T_{90} / (1+z)$ duration of the short GRBs with reliable
(spectroscopic) redshifts and without X--ray extended emission in the
\citet{2014-DAvanzo-SBAT8} sample is 0.3 s (10 bursts).  This will be
our reference time scale to perform spectral analysis of the first
part of long GRBs, and compare the results with those of short GRBs.

Throughout the paper, we assume a $\Lambda$CDM cosmology with H$_0$ =
71 km s$^{-1}$ Mpc$^{-1}$, $\Omega_{\rm m}$ = 0.27, $\Omega_\Lambda$ =
0.73.

\section{The sample}
\label{sec-sample}

Since we aim to study the prompt emission spectral properties and
energetic/luminosity of GRBs, we need a broad energy coverage in order
to determine where the peak energy is. While {\it Swift}/BAT has a
limited energy range (15--150keV) which is not suited for GRB prompt
emission spectral characterization, the GBM instrument on board {\it
  Fermi} covers almost 2 orders of magnitude in energy with the NaI
detectors (8keV--1MeV) and can extend this energy range to a few tens
of MeV with the inclusion of the data of the BGO detectors.  Hence we
selected all GRBs observed by {\it Fermi}/GBM up to December 2013 with
a redshift estimate.  This amounts to 64 long and 7 short GRBs.

Among the long ones we discarded:
2 GRBs with missing response matrix files;
2 GRBs observed with a non--standard Low Level Threshold\footnote{\href{http://fermi.gsfc.nasa.gov/ssc/data/access/gbm/llt\_settings.html}{http://fermi.gsfc.nasa.gov/ssc/data/access/gbm/llt\_settings.html}};
3 GRBs whose first part was missed by the GBM;
12 GRBs for which we could not constrain either the low energy
spectral index or the peak energy (\S\ref{sec-data_an}).  The final
LGRB sample comprises 45 long bursts.

{\it Fermi}/GBM observed 7 short GRBs with known redshift.  To this
sample we added the SGRB flux limited sample of 12 sources with
redshift discussed in \citet[][hereafter D14
  sample]{2014-DAvanzo-SBAT8}, but discarded: GRB 080905A since its
redshift is likely not accurate, GRB 090426 and GRB 100816A since
their classification as short GRB is debated.  Four GRBs in the D14
sample were also in the GBM sample: for these bursts we considered the
results reported in D14.  The final SGRB sample comprises 3 GRB
observed with {\it Fermi}/GBM and 9 from D14.

The short GRB sample, although relatively small, stems from a flux
limited sample of short GRB with a redshift completeness of $\sim$70\%
\citep{2014-DAvanzo-SBAT8}.  We dropped three burst from this sample,
hence the redshift completeness drops to $\sim$~60\%, but we added
three more bursts detected by {\it Fermi}/GBM.  The distributions of
low--energy spectral index in both our short sample and the
corresponding one\footnote{Bursts with $T_{90} < 2$ s and a either a
  Band or cutoff power law best fitting model in the
  \citet{2014-Gruber-GBMCat-4yr} catalog: 70 GRB.} in the
\citet{2014-Gruber-GBMCat-4yr} catalog are actually indistinguishable
(K--S test probability: 0.47).  Since the spectral index is a redshift
independent property we assume that our short GRB sample is a
reasonably good representation of the parent distribution of short
GRBs observable with currently available detectors.

The total (LGRB+SGRB) comprises 57 bursts (Tab.\ref{tab1}).
Fig. \ref{fig-z} shows the redshift distribution for both the SGRB and
LGRB samples (references for redshift estimates are given in
Tab.\ref{tab1}).

\begin{figure}
  \includegraphics[width=.45\textwidth]{z}
  \caption{Redshift distribution for both the SGRB (12) and LGRB (45)
    bursts (references for redshift estimates are given in
    Tab.\ref{tab1}).}
  \label{fig-z}
\end{figure}

\section{Data analysis}
\label{sec-data_an}

Our spectral analysis aims at estimating the intrinsic peak energy
($E_{\rm p}$), isotropic equivalent luminosity ($L_{\rm iso}$) and
emitted energy ($E_{\rm iso}$) for the GRBs in our sample.  For the 3
short GRBs observed by {\it Fermi}/GBM we performed a spectral
analysis on the entire duration of the burst ({\em short} analysis).
For the remaining 9 SGRB we considered the spectral properties
relative to the time integrated emission reported in the D14 paper
({\it short D14}).  For the 45 long GRBs we perform two different
spectral analysis: one for the first 0.3 s in the rest frame
(corresponding to $0.3 \times (1+z)$ s in the observer frame, {\em
  first} analysis) and one for the whole duration of the burst ({\em
  whole} analysis).  All $E_{\rm iso}$ and $L_{\rm iso}$ quantities
are evaluated in the (rest frame) energy range 1 keV--10 MeV.

All data analysis has been carried according to the
procedure outlined below.

\subsection{Detectors, energy selection and background fitting}

For each GRB we selected the most illuminated NaI detector(s), and the
corresponding BGO one.  The BGO detector is always included, even if
there is no significant detection above background.  The energy
selection is in the range 8--800 keV for NaI detectors, and 200
keV--35 MeV for BGO ones.  Systematic residuals at $\sim$~33 keV of
the NaI
detectors\footnote{\href{http://fermi.gsfc.nasa.gov/ssc/data/analysis/GBM\_caveats.html}{http://fermi.gsfc.nasa.gov/ssc/data/analysis/GBM\_caveats.html}}
are neglected.

For each channel of all detectors we perform a polynomial fit (up to
the third order) to the observed background count rate in the CSPEC
files,\footnote{Time binned count spectra with time resolution of
  1.024 s from the burst trigger time $T_0$ to $T_0$+600 s, and time
  resolution of 4.096 s for a few thousands seconds before and after
  the burst.} on a time interval before and after the burst longer
than the burst duration (typically $\gtrsim$~100 s).  The length of
the background time intervals is progressively increased until the
uncertainties on the expected background counts during the burst
becomes smaller than their intrinsic statistical fluctuations.  This
approach provides an objective way to select the background time
intervals.  We also checked that the background fit provide an
adequate fit for all energy channels by means of $\chi^2$
goodness--of--fit test.  For long bursts, we used exactly the same
background model for both the {\it first} and {\it whole} analysis.

The detectors used and the background time selections for each burst
are shown in Tab. \ref{tab1}.

\subsection{Time selection}

For the GRB spectral analysis we used the TTE data files\footnote{The
  list of all recorded counts with time and channel tags (Time Tagged
  Events).  Data are available from $\sim T_0 - 25$ s to $\sim T_0 +
  300$ s.} to select the counts in the appropriate time intervals:
either the first 0.3 seconds (rest frame) for the {\em first}
analysis, or the whole burst duration for both the {\em short} and
{\em whole} analysis.

For the {\it short} and {\it whole} analysis of GRBs present in both
our sample and the \citet{2014-Gruber-GBMCat-4yr} catalog we consider
their time selection.  This choice allows us to compare our results
with those of \citet{2014-Gruber-GBMCat-4yr}, as discussed in
\S\ref{cmp-g14}.  For the other bursts the time selection was
performed by a visual inspection of the count rate light curves.

For the {\em first} analysis we searched for the first occurrence of a
0.3 s long (rest frame) time bin in which the counts in all NaI
detectors were significantly (at 3$\sigma$ level) above the expected
background.  The search has been performed with a 0.2 s resolution
starting at 10 s before the trigger time.

The time selections for each burst are shown in Tab. \ref{tab2}.

\subsection{Spectral fitting}
\label{sec-specfit}

The GRB spectral models used for spectral analysis are a modified
version\footnote{The \texttt{XSPEC} implementation of this spectral
  model is available
  \href{http://www.giorgiocalderone.url.ph/xspec\_ggrb.tar.gz}{http://www.giorgiocalderone.url.ph/xspec\_ggrb.tar.gz}.}
of either the cutoff power law or the Band model \citep{1993-Band}, in
which the free parameters are:
\begin{itemize}
\item \texttt{log\_Ep}: the logarithm of the $\nu F_{\nu}$ peak energy
  in keV;
\item \texttt{alpha}: the photon spectral index for energies smaller
  than the peak energy;
\item \texttt{beta} (only for the Band model): the photon spectral
  index for energies greater than the peak energy;
\item \texttt{log\_F}: the logarithm of the integrated flux in the
  rest frame energy range 1 keV--10 MeV.
\end{itemize}
The spectral indices are bounded to be \texttt{alpha} $>-2$ and $-6 <
$ \texttt{beta} $ <-1.7$.  For the {\em whole} spectral analysis we
also included detectors effective area correction as free parameters,
bounded in the range 0.5--2.  Whenever the resulting area corrections
are not constrained we set all calibration factors to one.  The
\texttt{log\_F} parameter is used to estimate the intrinsic isotropic
luminosity $L_{\rm iso} = 4 \pi D_{\rm L}^2 \times F$, without the
need to propagate the uncertainties on the other parameters.  Finally,
isotropic emitted energy is estimated as $E_{\rm iso} = L_{\rm iso}
\Delta T_{\rm rest}$, where $\Delta T_{\rm rest} \times (1+z)$ is the
spectrum integration time.

The spectral model is folded with the detector response matrix, summed
with the background counts expected in the same time interval, and
compared to the observed counts by means of the Cash statistic
\citep{1979-Cash-Cstat} with Castor normalization (C--STAT).  The
model fitting is performed with \texttt{xspec} ver. 12.8.1g
\citep{1996-Arnaud-xspec} by minimizing the C--STAT value.  We always
used the detector maximum energy resolution, i.e. we did not rebin the
channels.

The choice of the spectral model (cutoff power law or Band) is
performed according to the following criterion: for each burst we
started with the Band model with both spectral indices free to vary in
the minimization process.  If the \texttt{beta} parameter uncertainty
is larger than a nominal threshold of 0.5, but still significantly
lower than the \texttt{alpha} parameter, we fixed \texttt{beta} to its
typical value, namely --2.3 \citep{1993-Band,
  2002-Ghirlanda-TimeResolvSpecBrightGRB}, and repeat the fit.  If
\texttt{beta} hits the lower limit (--6) we use the cutoff power law
model instead of the Band model.  If \texttt{beta} is $>-2$ and
\texttt{alpha}$>$\texttt{beta} we consider the resulting $E_{\rm p}$
and $L_{\rm iso}$ as lower limits.  The true location of the $\nu
F{\nu}$ peak likely lies on the extrapolation of the spectrum actually
constrained by the data.  By assuming \texttt{alpha}=--1 \citep[the
  typical value for this parameter, ][]{2011-Nava-438FermiGRB}, this
extrapolation lies on a line of slope 1 in the $E_{\rm p}$--$L_{\rm
  iso}$ plane.

In 12 cases we could not detect a curvature in the spectrum,
i.e. we could not constrain either the \texttt{alpha} or the
\texttt{log\_Ep} parameters.  These bursts were discarded from our
sample (\S\ref{sec-sample}).

The parameter uncertainties (quoted at 1$\sigma$) for the {\em whole}
analysis are estimated with the usual $\Delta \chi^2$ method
\citep{1976-Avni-DeltaChisqUncert, 1976-Cash-DeltaChisqUncert}.  For
the {\em short} and {\em first} analysis we adopted a different
approach since the counts in the high--energy channels of the
detectors are often very low.  In these cases we start by performing a
fit in the usual way, and use the best fit parameter estimates to
simulate several data sets for each detector (using the
\texttt{fakeit} command).  Then we run the fitting process on the mock
data sets, and consider the distribution of the resulting best fit
parameters.  The final uncertainties are estimated as the central
interval containing 68.3\% of the best fit values.  The simulation
iterates until the lower and upper limits of the confidence interval
change by less than 5\%.  Typically 400--600 simulations are required
to satisfy the convergence criterion.  This Monte Carlo method is
described in detail in \citet[][their Sect. 15.6.1]{2007-nr-3rd}.

In \S\ref{cmp-g14} we compare the results of our {\it whole} analysis
to those of \citet{2014-Gruber-GBMCat-4yr}, for the bursts present in
both samples, and show that the two methods produce very similar
results.  However, our method ensures a homogeneous approach in all
our spectral analysis: we established an objective criterion to select
the background time intervals, and used exactly the same background
model in both the {\em first} and {\em whole} analysis.  The use of
logarithmic quantities in our spectral model results in simpler and
more symmetric parameter uncertainties, with respect to their linear
counterparts \citep[e.g.][]{2007-Cabrera-SpAnalysisSwift-wZ}.  Also,
the use of the integrated flux as model parameter, instead of the flux
at a given energy, allows us to directly evaluate the uncertainties on
$L_{\rm iso}$, avoiding the necessity to estimate the parameter
covariance matrix for error propagation.  Finally, the use of Monte
Carlo simulations in the {\em short} and {\em first} analysis provide
reliable parameter uncertainties even in the low count regime, when
the assumption that the C--STAT value is drawn from a $\chi^2$
distribution is not reliable.

\subsection{Results}

The results of spectral analysis, as well as the spectral quantities
reported in D14 for the short GRB sample, are shown in
Tab. \ref{tab2}.  The relevant quantities for the {\em short}, {\em
  first} and {\em whole} sub samples are shown in
Fig. \ref{fig-histo}.  The lower limits for $E_{\rm p}$ and $E_{\rm
  iso}$ (2 in the {\it short}, 4 in the {\em first} and 3 in the {\em
  whole} analysis, respectively) are not accounted for in the
histograms.
\begin{figure*}
  \includegraphics[width=.48\textwidth]{h_alpha}
  \includegraphics[width=.48\textwidth]{h_ep}\\
  \includegraphics[width=.48\textwidth]{h_eiso}
  \includegraphics[width=.48\textwidth]{h_liso}
  \caption{Histograms of relevant results of the spectral analysis.
    Upper panels: the low energy spectral index \texttt{alpha} (left);
    intrinsic $\nu L_{\nu}$ peak energy $E_{\rm p}$ (right).  Lower
    panels: isotropic equivalent, emitted energy $E_{\rm iso}$ (left)
    and luminosity $L_{\rm iso}$ (right), integrated in the 1 keV--10
    MeV energy range (rest frame).  The lower limits for $E_{\rm p}$
    and $E_{\rm iso}$ and the analysis on precursors are not accounted
    for in the histograms.}
  \label{fig-histo}
\end{figure*}

Fig. \ref{fig-ratio} (left panel) shows the ratio of {\em first} to
{\em whole} peak energy vs. the same ratio of $E_{\rm iso}$.  The blue
dashed lines are the median values of both ratios.  The right panel
shows the $E_{\rm iso, whole} / E_{\rm iso, first}$ ratio vs.  $\Delta
T_{\rm whole} / \Delta T_{\rm first}$.  The blue dashed line is the
1:1 line.  The numbers beside the symbols are the GRB identifiers
shown in Table \ref{tab1} and \ref{tab2}.
\begin{figure*}
  \includegraphics[width=.48\textwidth]{ratio}
  \includegraphics[width=.48\textwidth]{ratio_eiso_t}
  \caption{Left panel: ratio of {\em whole} to {\em first} peak energy
    vs. the same ratio for $E_{\rm iso}$.  The blue dashed lines are
    the median values of both ratios.  Right panel: the $E_{\rm iso,
      whole} / E_{\rm iso, first}$ ratio vs.  $\Delta T_{\rm whole} /
    \Delta T_{\rm first}$.  The blue dashed line is the 1:1 line.  The
    numbers beside the symbols are the GRB identifiers shown in Table
    \ref{tab1} and \ref{tab2}.}
  \label{fig-ratio}
\end{figure*}

Finally, in Fig. \ref{fig-corr1} and \ref{fig-corr2} we show the
location of all bursts in the $E_{\rm p}$--$E_{\rm iso}$ and $E_{\rm
  p}$--$L_{\rm iso}$ planes respectively.  The lower limits are shown
with arrows of slope 1, as discussed in \S\ref{sec-specfit}.

\subsection{Notes on individual bursts}
\label{sec-notes}
\begin{itemize}
\item GRB 091024 \citep{2011-Gruber-091024,
  2014-Nappo-Afterglow091024}: the GBM data are separated in two burst
  intervals, hence this GRB appear twice in Tab. \ref{tab1} (ID 23).
  The first interval is actually a precursor and it is analysed
  according to the {\em first} prescription.  The second interval
  comprises a second precursor and the main event.  The {\em first}
  analysis at the beginning of the main event did not provide reliable
  constraints on the peak energy, hence we consider only the {\em
    whole} analysis.

\item GRB 110213: for this burst the {\em first} analysis did not
  provide reliable constraints on the peak energy because the signal
  is significantly background dominated, hence we consider only the
  {\em whole} analysis.

\item GRB 120711A and GRB 120716A show a precursor in their light
  curve.  For these bursts we analysed the precursor spectra according
  to the {\em first} analysis.

\item GRB 130427A: the GBM data are unreliable after $\sim$~4 seconds
  from the trigger since the large amount of recorded events, due to
  the exceptional brightness of this burst, saturated the available
  bandwidth \citep{2014-Preece-GBM130427}.  Hence we consider only the
  {\em first} analysis for this burst.
\end{itemize}

By taking into account these notes the final subsamples comprises:
\begin{eqnarray}
  \nonumber
  Short: \ {\rm 12\ bursts,\ with\ 2\ lower\ limits}\\
  \nonumber
  First: \ {\rm 43\ bursts,\ with\ 4\ lower\ limits}\\
  \nonumber
  Whole: \ {\rm 44\ bursts,\ with\ 3\ lower\ limits}
\end{eqnarray}

\subsection{$E_{\rm p}$--$E_{\rm iso}$ and $E_{\rm p}$--$L_{\rm iso}$ correlations}

We use the results of the spectral analysis to test the
spectral--energy correlations in the $E_{\rm p}$--$E_{\rm iso}$ and
$E_{\rm p}$--$L_{\rm iso}$ planes.  The former is the Amati relation,
while the second is only similar to the Yonetoku relation, since we
use the $L_{\rm iso}$ values estimated on the time averaged spectra,
rather than the peak isotropic luminosity $L_{\rm p,iso}$
\citep{2004-Yonetoku-EpLiso}.

We estimate the Spearman rank correlation coefficients and the
associated chance probability for the {\em short}, {\em first} and
{\em whole} results.  Also, we estimate the best fit correlations by
applying the unweighted bisector method
\citep{1990-Isobe-LinearRegression}.  Lower limits and precursor data
are not considered in this analysis.  The histograms of the residuals
from the best fit line, once projected on a scale perpendicular to the
line itself, are fitted with a Gaussian function in order to estimate
the scatter ($\sigma_{\rm sc}$) from the best fit.  Results are shown
in Tab.\ref{tab-corr}.

In Fig. \ref{fig-corr1} we show the best fit correlations
(solid lines) on the $E_{\rm p}$--$E_{\rm iso}$ plane for the {\it
  short} (purple), {\it first} (blue) and {\it whole} (red) results,
as well as the histograms of residuals (inset plots).  For comparison
we also plot the corresponding relations from the total sample of
\citet{2012-Nava-Amati} (black dashed line) and from both the short
and long GRB sample of \citet{2012-ZhangRevisitingLongShortClassif}
(double dot--dashed lines).  In Fig. \ref{fig-corr2} we
show the corresponding results in the $E_{\rm p}$--$L_{\rm iso}$
plane.  For comparison we show the $E_{\rm p}$--$L_{\rm p,iso}$
relations from the total sample of \citet{2012-Nava-Amati} (black
dashed line) and from the combined short and long GRB sample of
\citet{2012-ZhangRevisitingLongShortClassif} (double dot--dashed
lines).

\begin{table*}
  \begin{center}
    \caption{Results of the statistical analysis of the $E_{\rm
        p}$--$E_{\rm iso}$ and $E_{\rm p}$--$L_{\rm iso}$ correlations
      for the {\em short}, {\em first} and {\em whole} results. $A$,
      $B$ and $\gamma$ are the correlation parameters, while
      $\rho_{\rm s} $ and P$_{\rm chance}$ are the Spearman's rank
      correlation coefficient and the associated chance probability.
      Results from precursors data are not considered.}
    \label{tab-corr}
    \begin{tabular}{ccccccccc}
    \hline
    \hline
    {\bf Correlation} &
    {\bf Results}     &
    {\bf No. GRBs}    &
    {\bf $A$}         &
    {\bf $B$}         &
    {\bf $\gamma$}    &
    {\bf $\sigma_{\rm sc}$} &
    {\bf $\rho_{\rm s}$}     &
    {\bf P$_{\rm chance}$}\\
    \hline
    \multirow{3}{*}{$\log \frac{E_{\rm p}}{\rm keV} = \gamma(\log \frac{E_{\rm iso}}{\rm erg} - A) + B$}
    &   {\em short}   & 10 & 51.45 & 2.99 & 0.59 $\pm$ 0.07 & 0.15 & 0.71 & 0.02              \\
    &   {\em first}   & 39 & 51.62 & 2.92 & 0.65 $\pm$ 0.07 & 0.29 & 0.50 & $1\times 10^{-3}$ \\
    &   {\em whole}   & 41 & 53.21 & 2.73 & 0.57 $\pm$ 0.06 & 0.25 & 0.73 & $5\times 10^{-8}$ \\
    \hline
    \multirow{3}{*}{$\log \frac{E_{\rm p}}{\rm keV} = \gamma(\log \frac{L_{\rm iso}}{\rm erg\ s^{-1}} - A) + B$}
    &   {\em short}   & 10 & 52.28 & 2.99 & 0.63 $\pm$ 0.11 & 0.30 & 0.50 & 0.14             \\
    &   {\em first}   & 39 & 52.15 & 2.92 & 0.65 $\pm$ 0.07 & 0.29 & 0.50 & $1\times 10^{-3}$ \\
    &   {\em whole}   & 41 & 51.92 & 2.73 & 0.58 $\pm$ 0.07 & 0.29 & 0.7  & $4\times 10^{-7}$ \\
    \hline
  \end{tabular}
  \end{center}
\end{table*}
\begin{figure*}
  \includegraphics[width=\textwidth]{scatter}
  \caption{Rest frame $E_{\rm p}$--$E_{\rm iso}$ plane for all GRBs
    considered in this work.  The {\it short}, {\it first} and {\it
      whole} analysis results are shown with purple, blue and red
    symbols respectively, while the best fit correlations are shown
    with solid lines of the corresponding colors.  The numerical
    values of the slope and the scatter of the correlations are shown
    near the edges of the plots.  The inset plots show the histogram
    of the residuals from the best fit correlations.  The {\it first}
    analysis on precursors data are shown with green symbols.  The
    shaded areas are the 2$\sigma_{\rm sc}$ of the correlations of the
    {\it first} (orange) and {\it whole} (cyan) results.  Also shown
    are the $E_{\rm p}$--$E_{\rm iso}$ relations from the total sample
    of \citet{2012-Nava-Amati} (black dashed line) and from both the
    short and long GRB sample of
    \citet{2012-ZhangRevisitingLongShortClassif} (double dot--dashed
    lines) for comparison.}
  \label{fig-corr1}
\end{figure*}
\begin{figure*}
  \includegraphics[width=\textwidth]{scatter_yone}\\
  \caption{Rest frame $E_{\rm p}$--$L_{\rm iso}$ plane for all GRBs
    considered in this work with the same colors and symbols used in
    Fig. \ref{fig-corr1}.  Also shown are the $E_{\rm p}$--$L_{\rm
      p,iso}$ relations from the total sample of
    \citet{2012-Nava-Amati} (black dashed line) and from the combined
    short and long GRB sample of
    \citet{2012-ZhangRevisitingLongShortClassif} (double dot--dashed
    lines).}
  \label{fig-corr2}
\end{figure*}

\section{Discussion and conclusions}

We performed the spectral analysis of a sample long GRBs observed by
{\it Fermi}/GBM with a redshift estimate, using time integration equal
to 0.3 s rest frame ({\em first} analysis) and to the whole burst
duration ({\em whole} analysis).  Besides, we considered a sample of
short GRBs ({\em short} analysis), both by performing spectral
analysis of {\it Fermi}/GBM data and by reporting data from
\citet[][D14 sample]{2014-DAvanzo-SBAT8}. Our aim is to compare the
results of the {\em first} analysis to those of the {\em short} and
{\em whole} analysis.  The comparison of the relevant quantities are
shown in Fig. \ref{fig-histo}. Tab. \ref{tab-KS} shows the probability
that the distributions of the quantities shown in Fig. \ref{fig-histo}
are drawn from the same parent population.

The distributions of both $E_{\rm p}$ and $L_{\rm iso}$ are similar
for the the {\em short}, {\em first} and {\em whole} results.  The
distributions of low energy spectral index (\texttt{alpha}) for the
{\em short} and {\em first} results are very similar, but the
distribution for the {\it whole} results is significantly different
(K--S test probabilities $5.3 \times 10^{-5}$ and $\mathbf{8.9 \times
  10^{-4}}$, when compared to {\em first} and {\em short} results
respectively), with the latter showing lower values of \texttt{alpha}.
Also, the distribution of $E_{\rm iso}$ of the {\em whole} results is
significantly different from the {\em first} and {\em short} results
(K--S test probability: $4.1 \times 10^{-13}$ and $\mathbf{2.1 \times
  10^{-6}}$, when compared to {\em first} and {\em short} results
respectively), with the {\em whole} results lying a factor of a few
tens above the others.
\begin{table*}
  \begin{center}
    \caption{Results of Kolmogorov--Smirnov tests: column 2 and 3 show
      the probability that the distributions of the quantity shown in
      column 1 for the {\em short}, {\em first} and {\em whole}
      results are drawn from the same parent population.}
    \label{tab-KS}
    \begin{tabular}{cccc}
      \hline
      \hline
      {\bf Quantity}                          &
      {\bf {\em Short} vs. {\em First}}       &
      {\bf {\em Whole} vs. {\em First}}       &
      {\bf {\em Whole} vs. {\em Short}}       \\
      \hline
      alpha               & 0.83 & $5.3 \times 10^{-5}$   &  $8.9 \times 10^{-4}$\\
      log $E_{\rm p}$      & 0.71 & 0.11                  &   0.10\\
      log $E_{\rm iso}$    & 0.43 & $4.1 \times 10^{-13}$  &  $2.1 \times 10^{-6}$ \\
      log $L_{\rm iso}$    & 0.54 & 0.19                  &   0.29 \\
      \hline\hline
    \end{tabular}
  \end{center}
\end{table*}

The peak energy $E_{\rm p}$ of long GRBs, going from the first 0.3 s
(rest frame) to the whole burst duration, evolves either to lower or
higher energies, hence we do not find strong evidence for
hard--to--soft evolution of the peak energy.  The logarithmic median
value of the {\it whole} to {\it first} $E_{\rm p}$ ratio is
$\sim$~0.7 (Fig. \ref{fig-ratio}, left panel).  The total emitted
energy $E_{\rm iso}$ increases by a factor 5--10$^3$, with a
logarithmic median of $\sim$~35.  It is not clear what drives the
evolution of $E_{\rm p}$ towards either lower or higher energies,
since the $E_{\rm p, whole} / E_{\rm p, first}$ ratio does not show a
clear correlation with any other quantity.  The main driver for the
$E_{\rm iso}$ evolution is the total burst duration $\Delta T_{\rm
  whole,rest}$, i.e. longer burst likely evolve towards higher $E_{\rm
  iso}$ (Fig. \ref{fig-ratio}, right panel).

As discussed in \S\ref{sec-sample} the short GRB sample, although
relatively small when compared to the long sample, is a reasonably
good representation of the parent distribution of short GRBs
observable with currently available detectors.  Moreover, the short
GRB sample is large enough to provide evidence for significant
different distributions of \texttt{alpha} and $E_{\rm iso}$ when
compared to the {\it whole} sample.  Hence the K--S tests to compare
the spectral properties of the {\it short} and {\it first} samples are
reliable, and the corresponding distributions are actually
indistinguishable, i.e. we are unable to distinguish a short GRB from
the first 0.3 seconds of a long one with currently available
detectors.  Clearly, as new redshift estimates for SGRB become
available, our results may need to be reconsidered.

The plot of the $E_{\rm p}$--$E_{\rm iso}$ plane is shown in
Fig. \ref{fig-corr1}.  There is a clear correlation between $E_{\rm
  p}$ and $E_{\rm iso}$ for the {\em whole} results, with a chance
probability of obtaining a higher value of the Spearman's rank
correlation of $\sim 10^{-7}$ (Tab. \ref{tab-corr}).  In the $E_{\rm
  p}$--$E_{\rm iso}$ plane this is the well known Amati relation
\citep{2002-Amati-rel}.  The correlation slope and scatter
(0.57$\pm$0.06 and 0.25) are very similar to the ones found in
\citet{2012-Nava-Amati} for their total sample (0.55$\pm$0.02, 0.23),
and in \citet{2012-ZhangRevisitingLongShortClassif} for their long GRB
sample (0.51$\pm$0.03). For the {\em first} results we found a new
$E_{\rm p}$--$E_{\rm iso}$ relation with a probability $\sim 10^{-3}$
of being spurious.  The best fit {\em whole} relation lies at 3--4
$\sigma_{\rm sc}$ away from the {\em first} relation, hence the {\em
  first} and {\em whole} populations are well separated in the $E_{\rm
  p}$--$E_{\rm iso}$ plane.  The {\em short} GRBs alone do not provide
a strong statistical evidence for the existence of such a correlation
($P_{\rm chance} = 0.02$).  However, all {\em short} results lie
within 2$\sigma_{\rm sc}$ from the best fit relation for the {\em
  first} results.  Moreover, the best fit {\em short} correlation, if
it actually exists, lies very close to the {\em first} one, and
significantly away from the {\em whole} one.  Therefore, the {\em
  short} and {\em first} results are actually indistinguishable in the
$E_{\rm p}$--$E_{\rm iso}$ plane.  The lower limits for $E_{\rm p}$
and $E_{\rm iso}$ were not considered in the correlation analysis.
However, the true values of $E_{\rm p}$ and $E_{\rm iso}$ of the {\em
  short} and {\em first} population are not supposed to lie closer to
the {\em whole} correlation than their lower limits, as shown by the
arrows in Fig. \ref{fig-corr1}.  Hence our conclusions
can not be hampered by the presence of lower limits.  GRB precursors,
when present, also lie in the {\em short}--{\em first} region.

In the $E_{\rm p}$--$L_{\rm iso}$ (Fig. \ref{fig-corr2}) similar
considerations apply: there is a strong correlation for the {\em
  whole} results, a marginally significant correlation for the {\em
  first} results\footnote{The correlation analysis for the {\em first}
  results are the same in both the $E_{\rm p}$--$E_{\rm iso}$ and
  $E_{\rm p}$--$L_{\rm iso}$ planes, since the rest frame time
  interval is the same for all GRBs: 0.3 seconds.}, and a weak
correlation for the {\em short} results.  However, in the $E_{\rm
  p}$--$L_{\rm iso}$ plane all correlations overlap and are very
similar.  Note that these correlations are not equivalent to the
Yonetoku relation, since we used the $L_{\rm iso}$ values estimated on
the time averaged spectra, rather than the peak isotropic luminosity
$L_{\rm p,iso}$ \citep{2004-Yonetoku-EpLiso}.  Hence, we do not expect
to find the same results found in literature.  In particular we expect
our results to lie at lower $L_{\rm iso}$ since the peak luminosity is
by definition the highest luminosity for each burst.  Indeed the
Yonetoku relation found in \citet{2012-Nava-Amati} for their total
sample, and by \citet{2012-ZhangRevisitingLongShortClassif} for their
combined short and long sample, lie on the right of our best fit
correlation.  Nevertheless, our analysis shows that the $E_{\rm
  p}$--$L_{\rm iso}$ relation turns out to be very similar for the
{\em first} and {\em short} results (under the assumption that the
latter actually exists).  Hence, these correlations are possibly the
manifestation of the same physical process acting in all GRBs, and
even in small temporal intervals within a single GRB.

It has been debated if the Ep-Eiso and Ep-Liso correlation are
affected by selection effects
\citep{2005-Preece-TestingGRBRelationships,
  2005-Nakar-OutliersOf-EpEisoRelation,
  2007-Butler-CompleteCatalogSwift-SpectraDuration,
  2009-Butler-GeneralizedTestSelectionEffects-Correlations,
  2011-Shahmoradi-ImpactOfDetectorThreshold,
  2012-Kocevski-OriginOfHighEnergyCorrelations}. The possible
existence of similar correlation within individual GRBs, i.e. between
the peak energy and the luminosity as a function of time in a single
GRB \citep{2009-Firmani-TimeResolvedCorrel,
  2010-Ghirlanda-TimeResolvedFermi, 2011-Ghirlanda-ShortVsLong,
  2011-Ghirlanda-SpectralEvolutionFermiSGRB,
  2012-Frontera-TimeResolvCorr} seems to point to a physical origin of
these correlations. Similarly the use of a flux limited complete
sample of long GRBs seems to support the idea that instrumental
selection effects are not shaping these correlations
\citep{2012-Nava-Amati, 2012-Ghirlanda-EpLisoSelectionEffects}.  Hence
these correlations are likely the manifestation of fundamental GRB
properties.  Since our correlations for the {\it whole} analysis
(Tab. \ref{tab-corr}) are very similar to those found in literature we
do not expect our long sample to be strongly biased by selection
effects.  As a consequence, also the {\it first} correlation is not
biased, since the sample is the same.  The {\it short} analysis, on
the other hand, has been performed on a flux limited short GRB sample
with a redshift completeness of $\sim$~60\%, hence we do not expect
the selection effects (beyond the limiting flux threshold) to play a
dominant role.

The 0.3 s (rest frame) time scale chosen for the {\it first} analysis
has a clear interpretation: it is the representative duration of the
short GRBs in the D14 catalog.  Since the main driver for the $E_{\rm
  iso}$ evolution is the integration time (Fig. \ref{fig-ratio}, right
panel), a longer timescale would result in higher values of $E_{\rm
  iso,first}$.  Hence, in order to obtain significantly higher (or
lower) values of $E_{\rm iso}$, we should overcome the intrinsic
scatter of the correlations, namely 0.25--0.3 dex (a factor $\sim$~2,
i.e. $\Delta T_{\rm first} \lesssim$~0.15 s or $\Delta T_{\rm first}
\gtrsim$~0.6 s).

In summary, we found that the intrinsic spectral properties (peak
energy and luminosity) of both the short GRBs and the first 0.3 s
(rest frame) of long ones are actually indistinguishable.  Hence if
the central engine of a long GRB would stop working after $\sim$~0.3
s, we would have no means to distinguish it from a genuine short GRB.
Clearly, short and long GRBs remains two distinct phenomena, each one
with its own duration.  In particular short GRBs lasts longer or
shorter than 0.3 s.  Likewise, we do not expect the short--like phase
at the beginning of long GRBs to always lasts 0.3 s.  Our findings are
in agreement with those in \citet{2009-Ghirlanda-ShortVsLong}, which
found no differences in the (observed) spectral properties of short
GRBs and the first 1--2 s of long GRBs.  We extended this work by
comparing the intrinsic (rest frame) properties rather than the
observed ones.

Moreover, we found that the spectral quantities in the first 0.3 s of
long GRBs define new $E_{\rm p}$--$E_{\rm iso}$ and $E_{\rm
  p}$--$L_{\rm iso}$ correlations.  These correlations are possibly
the manifestation of an underlying physical process common to all
GRBs, despite the possibly different progenitors of short and long
GRBs, and the great variety of energetics and spectral properties
involved.

\bigskip

\noindent
{\bf ACKNOWLEDGMENTS}

\noindent

We gratefully acknowledge the Referee for the useful comments and
suggestions which greatly improved the paper.  The research activity
of A. Melandri, M.G. Bernardini and P. D'Avanzo is supported by ASI
grant INAF I/004/11/1.  G. Calderone was supported by PRIN INAF 2011
(1.05.01.09.15).

\bibliographystyle{mn2e}

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