text:
package org.wso2.carbon.event.statistics.internal.jmx;

import org.wso2.carbon.event.statistics.EventStatisticsObserver;
import org.wso2.carbon.event.statistics.internal.data.CollectionDTO;
import org.wso2.carbon.event.statistics.internal.data.StatsDTO;

import java.util.ArrayList;
import java.util.HashMap;
import java.util.List;
import java.util.Map;
import java.util.concurrent.ConcurrentHashMap;

public class JMXObserver implements EventStatisticsObserver {

    private ConcurrentHashMap<String, List<String>> registeredMbeanIds = new ConcurrentHashMap<String, List<String>>();
    private ConcurrentHashMap<String, Map<String, StatisticsView>> data;

    public JMXObserver() {
        data = new ConcurrentHashMap<String, Map<String, StatisticsView>>();
    }

    public void destroy() {
        for (Map.Entry<String, List<String>> entry : registeredMbeanIds.entrySet()) {
            for (String value : entry.getValue()) {
                MBeanRegistrar.getInstance().unRegisterMBean(entry.getKey(), value);
            }
        }
    }

    @Override
    public void updateStatistics(CollectionDTO collectionDTO) {
        String id = collectionDTO.getStatsDTO().getName();
        updateView(collectionDTO.getStatsDTO(), id);//tenant

        if (collectionDTO.getChildCollectionDTOs() != null) {
            for (CollectionDTO collectionDTO1 : collectionDTO.getChildCollectionDTOs()) {
                String id1 = id + "." + collectionDTO1.getStatsDTO().getName();
                updateView(collectionDTO1.getStatsDTO(), id1);  //category

                if (collectionDTO1.getChildCollectionDTOs() != null) {
                    for (CollectionDTO collectionDTO2 : collectionDTO1.getChildCollectionDTOs()) {
                        String id2 = id1 + "." + collectionDTO2.getStatsDTO().getName();
                        updateView(collectionDTO2.getStatsDTO(), id2);   //deployment

                        if (collectionDTO2.getChildCollectionDTOs() != null) {
                            for (CollectionDTO collectionDTO3 : collectionDTO2.getChildCollectionDTOs()) {
                                String id3 = id2 + "." + collectionDTO3.getStatsDTO().getName();
                                updateView(collectionDTO3.getStatsDTO(), id3);   //element

                            }
                        }
                    }
                }
            }
        }
    }

    private void updateView(StatsDTO statsDTO, String id) {
        Map<String, StatisticsView> map = data.get(statsDTO.getType());
        if (map == null) {
            data.putIfAbsent(statsDTO.getType(), new HashMap<String, StatisticsView>());
            map = data.get(statsDTO.getType());
        }

        StatisticsView view;
        if (!map.containsKey(id)) {
            view = new StatisticsView();
            MBeanRegistrar.getInstance().registerMBean(view,
                                                       statsDTO.getType(),
                                                       id);
            // store this information to unregister the MBeans later
            List<String> ids = registeredMbeanIds.get(statsDTO.getType());
            if (ids == null) {
                registeredMbeanIds.putIfAbsent(statsDTO.getType(),
                                               new ArrayList<String>());
                ids = registeredMbeanIds.get(statsDTO.getType());
            }
            ids.add(id);
            map.put(id, view);
        } else {
            view = map.get(id);
        }

        updateView(view, statsDTO);
    }

    private void updateView(StatisticsView view, StatsDTO statsDTO) {
        view.setRequestCount(view.getRequestCount() + (statsDTO.getRequestTotalCount() - view.getRequestTotalCount()));
        view.setResponseCount(view.getResponseCount() + (statsDTO.getResponseTotalCount() - view.getResponseTotalCount()));

        view.setRequestTotalCount(statsDTO.getRequestTotalCount());
        view.setRequestAvgCountPerSec(statsDTO.getRequestAvgCountPerSec());
        view.setRequestMaxCountPerSec(statsDTO.getRequestMaxCountPerSec());
        view.setRequestLastUpdatedTime(statsDTO.getRequestLastUpdatedTime());

        view.setRequestLastSecCount(statsDTO.getRequestLastSecCount());
        view.setRequestLastMinCount(statsDTO.getRequestLastMinCount());
        view.setRequestLast15MinCount(statsDTO.getRequestLast15MinCount());
        view.setRequestLastHourCount(statsDTO.getRequestLastHourCount());
        view.setRequestLast6HourCount(statsDTO.getRequestLast6HourCount());
        view.setRequestLastDayCount(statsDTO.getRequestLastDayCount());

        view.setResponseTotalCount(statsDTO.getResponseTotalCount());
        view.setResponseAvgCountPerSec(statsDTO.getResponseAvgCountPerSec());
        view.setResponseMaxCountPerSec(statsDTO.getResponseMaxCountPerSec());
        view.setResponseLastUpdatedTime(statsDTO.getResponseLastUpdatedTime());

        view.setResponseLastSecCount(statsDTO.getResponseLastSecCount());
        view.setResponseLastMinCount(statsDTO.getResponseLastMinCount());
        view.setResponseLast15MinCount(statsDTO.getResponseLast15MinCount());
        view.setResponseLastHourCount(statsDTO.getResponseLastHourCount());
        view.setResponseLast6HourCount(statsDTO.getResponseLast6HourCount());
        view.setResponseLastDayCount(statsDTO.getResponseLastDayCount());

    }

}

redpajama_set_name: RedPajamaGithub


text:
Zlata Tkacz (ur. 16 maja 1928 w Lozovej, zm. 1 stycznia 2006 w Kiszyniowie) – mołdawska kompozytorka i pedagog.

Życiorys
Jej rodzice Moise Berehman i Fania Kofman pochodzili z bogatych żydowskich rodzin. Ojciec ukończył Konserwatorium i uczył gry na skrzypcach. Zlata urodziła się w Lozowej, gdzie jej babcia prowadziła firmę. Gdy miała 3 lata rodzina przeprowadziła się do Kiszyniowa. Po wybuchu wojny niemiecko-sowieckiej rodzina została ewakuowana, ale Zlata zgubiła się podczas podróży. Wsiadła sama na statek w Machaczkale i dotarła do Krasnowodzka. Początkowo mieszkała w rodzinie znajomej ze statku, ale widząc problemy z wyżywieniem postanowiła zamieszkać w domu dziecka. Wyjechała do Namanganu w Uzbekistanie. Dzięki kierowniczce domu dziecka odnalazła matkę, która w 1943 roku przyjechała i pracowała jako nauczycielka. W międzyczasie dotarł do Namanganu również ojciec, zwolniony z wojska z powodów zdrowotnych. W sierpniu 1944 roku rodzina wróciła do Kiszyniowa.

Po ukończeniu szkoły podstawowej Zlata rozpoczęła studia na uniwersytecie w Kiszyniowie. Studiowała fizykę i matematykę, ale wkrótce przerwała studia i zaczęła naukę na Wydziale Muzykologii Konserwatorium w Kiszyniowie. W 1949 roku wyszła za mąż za Jefrima Tcaci, a w 1952 roku skończyła studia. W latach 1952–1962 uczyła w szkole muzycznej w Kiszyniowie. Cały czas komponowała, a w 1957 roku rozpoczęła naukę w klasie kompozycji Leonida Gurowa. Po zakończeniu nauki pozostała w Konserwatorium i pracowała jako wykładowca do końca życia. W 1986 roku otrzymała tytuł została profesora nadzwyczajnego, a w 1993 profesora kompozycji. W 1962 roku została członkiem Związku Kompozytorów Mołdawii.

Odznaczenia
 1974 Honorowa Artystka Mołdawskiej SRR
 1982 Nagroda Państwowa Mołdawii
 1998 Kawaler Orderu Gloria Muncii

Twórczość (wybór)
Zlata Tcaci skomponowała około 800 utworów. Są wśród nich: sonaty, kwartety smyczkowe, muzyka wokalna, utwory chóralne i instrumentalne, kantaty, opery, balet, miniatury instrumentalne, piosenki dla dzieci oraz muzyka filmowa. Skomponowała między innymi:

Balet
 1979: Andries balet do utworu Emiliana Bucova

Opery
 1981: Floricica-floricea opera libretto Victor Ciudin
 1983: Capra cu trei iezi opera libretto Grigorij Wijeru
 1985: Un pas în nemurire opera libretto Emilian Bukov
 1987: Unchiul meu din Paris opera na podstawie utworu Aureliu Busuioca
 1988: Micul prinț opera na podstawie utworu Antoine de Saint-Exupéry

Utwory wokalne
 1981: Plai de cint, plai de dor na chór
 1981: Povestea codrului na chór dziecięcy
 1991: Numele sau sfint cykl wokalny do tekstu Owsieja Driza
 1993: Iad-Va-shem na głos, perkusję i orkiestrę kameralną
 1983: Eu muzica as scrie na głos i fortepian do wiersza Robierta Rożdiestwienskiego
 1992: Idise oisiis (1992) na chór do wiersza Ichiła Szrajbmana
 1995: Vajs gadol, vajs kados na baryton i orkiestrę do wiersza Mojsze Lemstera
 1998: Doina la fluer, Ciocirlia na chór mieszany a capella do utworu Vasile Romanciuca
 2001: De profundis do wiersza Miroslavy Metleaevaej

Utwory instrumentalne
 1982: Quatuor à cordes n° 1
 1982: 2 suite din balet Andrieș na orkiestrę symfoniczną
 1989: Dublu concert pentru flaute na orkiestrę symfoniczną
 1995: 5 peșrevuri de Dmitrie Cantemir na kwartet smyczkowy
 1993: Aureliu Busuioc na orkiestrę kameralną
 1995: Perpetuum mobile na skrzypce
 2020: Concerto na fortepian i orkiestrę symfoniczną

Upamiętnienie
Od 2010 roku przez Żydowskie Centrum Kultury KEDEM, Filharmonię Narodową, American Jewish Joint Distribution Committee w Mołdawii, pod patronatem Ministerstwa Edukacji, Kultury i Badań Naukowych jest organizowany Międzynarodowy Konkurs Młodych Wykonawców Zlata Tcaci.

Przypisy

Urodzeni w 1928
Zmarli w 2006
Mołdawscy kompozytorzy

redpajama_set_name: RedPajamaWikipedia


text:
How to Use A Waterproof Camera?
1 Comment / By Devansh Pathak / July 23, 2020 July 1, 2021
Today I will tell you how to use a waterproof camera to get best images and videos. Waterproof cameras are essential equipment for a great traveler who loves to memorize the most important moments during a stay. The performance of the camera varies, however, depending on the brand. But it also largely depends on how it turns out to be used.
1. Capture Your Highlights with A Waterproof Device
When you are passionate about underwater photography, you have to find a waterproof camera. This revolutionary equipment allows you to take snapshots or record HD videos underwater or in the sea.
The most advanced models can even withstand dust (dustproof), extreme temperatures (freezeproof). Some have been specially designed to cope with shocks (shockproof).
2. Make Sure Your Device Meets Quality Standards
If your device meets IEC ‒ 60529 IP68 or IP58, it means that it is practically resistant to dust and water. So, you can take it with you to the pool or the beach without being afraid to spoil it.
But it will be even more convenient and robust if it corresponds to the MIL-STD 810F (US Military Standard) law. This feature gives it optimal protection against the most severe shocks. However, remember that this tightness has its limitations. It may indeed depend on the depth and duration of the presence in the water.
3. Avoid Using Your Camera Beyond an Hour
It is interesting to know that submersible models cannot continue to operate for more than an hour. Some products exceed this limit, but not many have this somewhat unique ability. After undergoing several tests, the device was certified waterproof. This waterproof feature does not mean that it will be forever because it risks being damaged at a certain level.
It's pretty much the same story for shockproof models. Before being marketed, they threw these devices on a plywood board 5 cm thick to know their impact resistance after a fall.
4. Use It to Take Pictures Out of The Ordinary
Since this device has nothing to do with classical models, it allows you to capture unusual scenes usually at risk.
Photographing sharks in action or taking pictures of you climbing during snowy weather or in the rain is quite possible. This famous device remains the champion in this field, whether for a professional or a photography lover. It remains easier to use.
5. Observe the Immersion Time Indicated on The Package Leaflet
A digital camera can take photos in HD underwater. But do not believe that there is no limit. To avoid damage due to improper handling, read the user manual carefully.
So, you'll know when to get out of the water before it's too late. For this, you must respect the immersion time that the device can take.
You may also like to read: Best Waterproof Cameras: Buying Guide, Rating and Reviews
The Most Popular Brands
Currently, photography is evolving with technological advancement. On land, in the air, underwater, and whatever the climatic conditions, nothing prevents amateurs and professionals of photography. The most popular brands in this field have understood this well and try to bring extraordinary innovations to their products to satisfy each user.
When we talk about technological innovations, the Japanese always find themselves in the first choices regarding sales. In the field of lenses and precision digital, Olympus is probably the preferred brand. When it was founded in 1919, the company first specialized in thermometers and medical microscopes.
It was from the 30s that the brand focused on the manufacture and marketing of cameras. And to this day, Olympus continues to satisfy its buyers with revolutionary products in image quality. Like the tough series, which offers dedicated devices for extreme sportspeople and adventurers. These models know no limits, whether in harsh mountain conditions, in nature, or under the ocean.
Olympus Tough TG 5
Check the Latest Price on Amazon
Stoga
Stoga is especially famous for its computer accessories such as wireless or wired game controllers and smartphone holders for your car trips. Also, for its smartwatches that are taking up more space in our daily lives due to their practicality.
Stoga is also a camera specialist. In recent years, it has found its place among the major brands in the field by offering its consumers classic models and a series of revolutionary prototypes in terms of shooting. For the latter, you can count on the CGT series. They are equipped with LCD screens and sensors initially designed to guard against all contingencies.
Stoga Waterproof Camera
If you are looking for a camera, you will most likely come across a model of the Easypix brand on price comparators. Indeed, the brand focuses on designing this device to bring satisfaction to both young and old.
In this sense, the manufacturer offers its customers several varieties of cameras and for all budgets. As for the category of waterproof cameras, the design is a feature that the company has put forward. With their double screens, lovers of selfies will be able to find their pleasure in all conditions. Also, users will have the opportunity to retouch their snapshots directly on the material using the filters and modes offered.
Easypix Splash W1024
Fujifilm has been present in the field of camera lenses for 88 years now. The Japanese brand has become one of the first consumer choices in cameras because of its technological innovations.
Fujifilm FinePix XP130
In this sector, the brand also offers a series of models designed to face the extreme conditions of nature. We are talking about watertight devices here. You will find the FinePix or XP series equipped with sensors at more than 16 million pixels. And with their Wi-Fi connections, you can directly transfer your shots to your smartphone or computer without the need for cables. They are particularly resistant to water and frost but also shockproof.
Before embarking on the design of cameras for the general public, the company first specialized in sunglasses with polarizing lenses. But Polaroid distinguished itself with the manufacture of the first instant print devices in the 40s.
With its years of experience in the field, Polaroid is still a sought-after brand nowadays. Meanwhile, the models of waterproof cameras of the brand offer an attractive efficiency because they can take your shots at 3 m depth underwater. They are waterproof and have an image quality of 16 megapixels.
Polaroid Underwater Camera
Best Camera For Video Vlogger and Youtubers in 2020
Cameras / July 9, 2020 March 28, 2021
Buying Guide: Best Canon Bridge Camera of The Year
Cameras / July 20, 2020 June 23, 2021

redpajama_set_name: RedPajamaCommonCrawl


Tasting Notes: Tsugu has a delicate and elegant floral aroma with a soft and mouthfeel. Splendidly balanced flavor, and a clean, dry, medium-long finish. This sake is Asahi Brewery's greatest achievement, and represents the culmination of all of their history, technique, research and technology.Only 2500 bottles are produced each year.
Profile: Established in 1830 with the motto of "quality first". Brewing sake is making rice. Not only do they focus on obtaining high quality sake rice, they dedicate time and effort in their labs to increase said rice's quality. Their efforts do not stop there however - in order to help sustain the environment, they implement the ISO14000 system of environmental sustainability, and also participate in various activities to preserve their natural surroundings. Additionally, they hold tea ceremonies, concerts, and cultural events for the local community. The goal is to make a fun, sustainable, and ultimately enjoyable environment with sake.


text:
Q: power shell script to get data from each subfolders I have a folder inside this folder I have around 20 sub folders, each sub folder having .wav files and I have a power shell script using this script I am able to get data from a single folder, but I want to get data from all sub folders in one go when I click on main folder. Below is my power shell script. Please help me to modify my script.
# Show an Open Folder Dialog and return the directory selected by the user.
function Read-FolderBrowserDialog([string]$Message, [string]$InitialDirectory, [switch]$NoNewFolderButton)
{
    $browseForFolderOptions = 0
    if ($NoNewFolderButton) { $browseForFolderOptions += 512 }

    $app = New-Object -ComObject Shell.Application
    $folder = $app.BrowseForFolder(0, $Message, $browseForFolderOptions, $InitialDirectory)
    if ($folder) { $selectedDirectory = $folder.Self.Path } else { $selectedDirectory = '' }
    [System.Runtime.Interopservices.Marshal]::ReleaseComObject($app) > $null
    return $selectedDirectory
}
$folder= Read-FolderBrowserDialog
$com = (New-Object -ComObject Shell.Application).NameSpace($folder)
for($i = 0; $i -lt 64; $i++) {
                $name = $com.GetDetailsOf($com.Items, $i)
                if ($name -eq 'Length') { $lengthattribute = $i}
}
$com.Items() |
ForEach-Object {
[PSCustomObject]@{
Name = $_.Name
Path = $_.Path
Size = $com.GetDetailsOf($_, 1)
DateCreated = $com.GetDetailsOf($_, 4)
Length = $com.GetDetailsOf($_, $lengthattribute)
}
} |
Export-csv report.csv -notypeinformation

A: It is not quite a PowerShell way anymore to use Com-objects for folder operations and I generally don't like mixing UI controls with scripts, unless those are controllers.
Once you know the $folder as the parent, I would filter sub-directories and then foreach subdir I would recursively measure the files within, enrich the original object and select the relevant Properties. Something like:
$folder | Get-ChildItem -Directory | ForEach-Object {
    $files = ($_ | Get-ChildItem -Recurse | Measure-Object -Sum Length);
    $_ |
    Add-Member -NotePropertyName FileCount -NotePropertyValue $files.Count -PassThru |
    Add-Member -NotePropertyName Length -NotePropertyValue $files.Sum -PassThru
} |
Select Name,FileCount,Length,LastWriteTime

So you will get a result like:
Name           FileCount   Length LastWriteTime
----           ---------   ------ -------------
subfolder_A          499   679695 2/02/2017 12:23:21 PM
subfolder_B           35    21033 12/01/2017 1:36:53 PM
subfolder_C           18    10777 12/01/2017 1:38:28 PM
...

A: Your question has already been answered. But still if you want to try by your approach, then you can use the Type method of $com.Items() Marshal object. One way will be to check if an item is of type File Folder. If yes, then you can use -Recurse parameter along with Get-ChildItem cmdlet to list all subfolders and files in your folders. Your code will look something like this
# Show an Open Folder Dialog and return the directory selected by the user.
function Read-FolderBrowserDialog([string]$Message, [string]$InitialDirectory, [switch]$NoNewFolderButton)
{
    $browseForFolderOptions = 0
    if ($NoNewFolderButton) { $browseForFolderOptions += 512 }

    $app = New-Object -ComObject Shell.Application
    $folder = $app.BrowseForFolder(0, $Message, $browseForFolderOptions, $InitialDirectory)
    if ($folder) { $selectedDirectory = $folder.Self.Path } else { $selectedDirectory = '' }
    [System.Runtime.Interopservices.Marshal]::ReleaseComObject($app) > $null
    return $selectedDirectory
}
$folder= Read-FolderBrowserDialog
$com = (New-Object -ComObject Shell.Application).NameSpace($folder)
for($i = 0; $i -lt 64; $i++) {
                $name = $com.GetDetailsOf($com.Items, $i)
                if ($name -eq 'Length') { $lengthattribute = $i}
}
$com.Items() | ForEach-Object {
    if ($_.Type -ne "File Folder")
    {
        [PSCustomObject]@{
        Name = $_.Name
        Size = $com.GetDetailsOf($_, 1)
        DateCreated = $com.GetDetailsOf($_, 4)
        Length = $com.GetDetailsOf($_, $lengthattribute)}
    }
} | Export-csv report.csv  -Encoding ascii -NoTypeInformation

$com.Items() | ForEach-Object {
    If ($_.Type -eq "File Folder")
    {
        Get-ChildItem -path $Folder -Recurse | ForEach-Object {
        [PSCustomObject]@{
        Name = $_.Name
        Size = $_.Length/1KB
        DateCreated = $_.CreationTime }
        }
    }
}  | Export-csv report.csv -Encoding ascii -NoTypeInformation -Append -Force

I have used -append and -force parameters to output everything in one CSV.
The above script will list you files in subfolders of a folder as well as in the subfolders of subfolders. Also, it will list out the folders in you root directory. I think this is what you were looking for. You can anyway add more conditions depending upon your requirement, that's why instead of continuing in a single Foreach-Object, I have split the Foreach-Object into the number of conditions (2 in this case, one for folders and another for files within subfolders). You can tweak around this script depending upon your requirements.

A: Actually this whole thing could be done way easier if you just take the childitem of a path and then check for the childitem of that path. So just do this and enjoy the bright side of life.
$folder = Get-Childitem 'C:\'

Get-Childitem $folder

If you want to work with the Output just put Get-Childitem $folder into another variable, like this.
$folder2 = Get-Childitem $folder

I hope i was able to help you out on this buddy ;).

redpajama_set_name: RedPajamaStackExchange


*Depending on the marble available at time of production, coloring and shade may vary from picture shown.
The original Christus statue by Sculptor Albert Bertel Thorvaldsen (1770-1844) was made of plaster in 1823 and was used to create the 11-foot marble version in 1839 that stands today in the Church of Our Lady in Copenhagen, Denmark.
Thorvaldsen spent 40 years in Rome. There he made a sepulchral monument for Pope Pius VII in St. Peter's Cathedral and numerous statues in the style of antiquity. While in Rome he also worked on another one of his masterpieces, "Christ and the 12 Apostles" which made him internationally known as the greatest sculptor of neo-classicism.
He returned to Copenhagen where he started and completed his greatest work, the Christus. After Thorvaldsen's death in 1844, the Christus was erected in the Copenhagen Cathedral. This marvelous work of inspired art has now been painstakingly created in exact detail as the original.
** This item can ship internationally via International Priority. Recipient is responsible for all customs, duties, and taxes.
Wonderful color! No quality concerns or aesthetic imperfections. I highly recommend this piece for any collection.
I ordered a 19" "Marble Christus Statue". I got a plaster statue that's not cleaned very well and still has mold marks on it. It's not worth the money I paid for it. I'm VERY disappointed. I expect more from Deseret Book.
This is such a marvelous, beautifully done art piece of the Saviour.
It warms my heart when I view it and think of him.
I am just giving 3 stars because the statue is NOT made by marble, as advertised, and this is not fair. You can feel the strong resin smell right out of the box. You can even see traces of pressing molding process. So, maybe this is a little bit pricey for not being real marble. But the statue is marvelous. A perfect decoration to remind us (and our guests!) about the Savior.
Very Pleased with the Christus Statue. It looks better than the picture of it online.
I just had a birthday, and my husband (a nonmember) gave me the 12 inch Christus. It is beautiful, and was a real surprise. He is stunning, and I feel such a sense of peace when you look at him. I really pleased with this statue. And, it lets me know that he knows how important my chuch is to me. Makes a wonderful gift.
Firstly, you wouldn't want to get the statue any smaller than the 12". The 12" is nice but still small.
I am very happy with my purchase. For me, this item brings the spirit every time I look at it. It helps me make better choices in my home.
You won't regret this purchase.
Throughout the past 4 years I have purchased 7 of the 19 in versions of the the marble Christus. I have two in my own home and have given away 5. Every time I have presented this beautiful work of art the recipient has cried and commented on how much it meant to them. It really does have a beauty beyond price and a meaning beyond words. Even after having it in my home for so long, I still find myself just sitting and gazing at it.
I purchased the 9" version at the City Creek Center location while I was visiting the Salt Lake area last week. It is now the center piece on the mantle above the fire place. Having the opportunity to see The Christus at The Visitor's Center at Temple Square the day I purchased this makes it even that much more special to my family. I sat looking at the full size statue for probably half an hour, and can say this is a fairly good recreation of that. I also bought two of the 3" versions which are equally remarkable for their size.
I was very happy when my copy arrived. I love it!
We have had our Christus for a number of years but has stood in our Bishops office until we had our own home. Well, the other day our Great Grandson age 4 came round for the day with his parents who are not members of the Church and we have a lovely contempory painting of the Salt Lake Temple in the same room. Our Grandson looked at the Christus and then pointed to the painting and said to his Granny, 'Does that man live in that house'. What a wonderful moment that was!.
A wonderful spirit envelops your home.
Our son's beloved wife passed away suddenly, leaving him with a tiny four month old baby. My Husband and I moved in with him to help care for the baby. I brought my Christus Statue as I felt we needed it and for the peace it brings.
One morning the baby was restless and seemed to be missing her Mother so I took her over to the Statue which was bathed in the early morning light. The baby literally jumped in my arms and threw her little arms around it like she knew him.
The spirit was very strong and I knew she was enveloped in our Savior's love. I told her that her mother was with Jesus now and she seemed to know and was a much calmer child. What a blessing this has been to our family. The statue now sits on my organ under the picture "O Jerusalem" and I feel a special feeling whenever I play hymns of Jesus.
Unfortunately, the workmanship is very poor.
I'm sad to say that the Christus statue we received is not of very good workmanship. It is very yellowish cream colored, not white and the detail work extremely lacking. Extra material from the molding process hangs off the fingers, and the hands barely represent the real statue. We can actually see a seam where it appears the head may have broken off and then been "repaired"--needless to say, I'm very dissappointed.
Today our family still enjoys this beautiful art piece in our home. "Christ" is the foundation of our Church and family. that is why the family portrait is directly above the statue. Our grandchildren especially like to stand at look without touching this reminder to be kinder, gentler and happier. Joy is the goal.
Best reminder of Christ and the His Atonement.
I ordered this statue as a gift for my husband. It makes a beautiful addition to our home and is the centerpiece to our sitting room. Highly recommend!!
It is wonderful to have this on display. It reminds me of the D.C. temple.
This truely captures the feeling you want in your home, it's amazing!


David Mills has an MA (New York University). He is the author of the small press bestseller "TheDream Detective" and the 2012 prize finalist "the Sudden Country." His poems have appeared in Ploughshares, Jubilat, Fence and Brooklyn Rail. He received a New York Foundation for the Arts fellowship.


At the core of employee engagement are relationships built on trust and a positive work environment that keeps an organization's employees happy, healthy, and engaged. Whether it's uncompetitive pay, lacking development opportunities, unavailable managers, or unappealing benefits, there are many reasons today's workers cite for being disengaged with their work.
Automation is currently transforming the world of HR and payroll, as a function and as a service. Thankfully, the emergence of the cloud and Software as a Service (SaaS) applications have made it possible for providers to tackle the complexity of global policies and practices. With automation comes an opportunity to think about the employee experience and address outdated systems that may be preventing an organization from achieving its talent strategies and goals.
An excellent step in improving employee engagement is to integrate HR and global payroll data systems. By combining this critical information, multinational organizations are equipped to centrally manage and analyze employee-related data to create significant efficiencies and improvements for both functions.
When choosing payroll and HR technology, it is often limited budgets, existing internal processes, and the bottom line that drive decisions. As a result, many organizations are still faced with using outdated and disparate systems that were implemented when integration wasn't an option. Global payroll data is an example of information that can offer a vast amount of insight for executives to reference when making business decisions. But if that data is not incorporated or accessible within other HR systems, the data becomes less relevant.
By comparison, with an integrated approach to HR and payroll systems, an organization can conduct a meaningful analysis of payroll data that—when combined with other relevant employee data (e.g., benefits, tenure, performance, development)—has the potential to provide executives and HR leaders with all the figures that impact employee engagement. Integration puts required information in one location so that an organization can assess competitive pay in the market, determine the financial requirements to employ staff around the globe, and develop robust HR programs to make meaningful decisions around how to engage employees best.
Organizations that run their multinational payroll on a single, unified platform will reap the benefits of an engaged workforce. A system that is easy for everyone from top executives to system administrators to frontline employees to use not only streamlines operations, it also demonstrates a commitment to understanding and improving the employee experience, and to putting yourself in their shoes.
"Picture yourself as a new hire, a fledgling manager, or an employee who just gave birth to her first child. What are your interactions with the company like? Can you get the information you need quickly? Are the company's communications effective? Is the required paperwork onerous and redundant? Are the processes convenient? All of these routine touchpoints contribute to employee experience," according to the article "Creating an Optimal Employee Experience" from the Society for Human Resource Management (SHRM).
HR leaders and other executives may be afraid to ask for feedback about employee touchpoints with existing systems, for fear of facing unrealistic requests. That may occur, but if you don't ask for employee input about how processes and procedures impact their experience, you risk the repercussions of not removing barriers. It's better to seek feedback, learn what needs to change, and be transparent about what is and isn't possible. When it comes to engagement, seeking input about ease of use is a meaningful way to reinforce relationships built on trust and a work environment that supports employees.
For administrative users who access payroll and HR systems as part of their daily work, systems must be standardized, synchronized, and available in real time. Many international payroll providers aggregate data from multiple sources. These systems and their data are not always compatible and can at best cause confusion and at worst create unreliable information and inaccurate analysis.
Issues with global payroll and HR data not only inhibit productivity for system users, but also thwart productive use of the information for strategic purposes. To positively impact critical drivers of employee engagement (respectful treatment, compensation, and benefits, according to SHRM's 2016 Employee Job Satisfaction and Engagement survey), an organization must have access to a comprehensive set of all data related to employees. A payroll platform that offers full integration with a variety of human capital management (HCM) providers enables leaders to make informed decisions regarding these relevant payroll and HR metrics, and overall engagement.
As multinational businesses continue to expand their reach into new territories, they often encounter unforeseen challenges with different payroll and HR regulations and requirements. Powered by integrated and automated systems, HR and payroll leaders have an opportunity to serve as advisors to the business by delivering strategic value that will enable an organization to engage employees around the world.


This is truly a must see located right in the heart of Breaux Bridge. Originally it was built as a single family home. Currently it is a duplex that has been completely renovated. There are so many possibilities for its use; it could be a home with a separate office, or a home with a mother-in-law suite attached, or one side can even be used as an office as long as the other side is rented out as a residence. It can also be easily converted back to one family dwelling by adding a doorway back between the units. The original door is still in the house. The beautiful original hard wood flooring is throughout both units except for the bathrooms. All bathrooms have been completely redone with new tubs, sinks, tub surround and ceramic tile flooring.


It's funny, Jon says Babis instead of Bäbis (swedish for baby). This is a joke only my swedish readers will get because most people don't know how to pronounce "ä" differently from "a". Anywaaaay, I recieved my new "babis" as it is so popular to call your electronical devices. I have bought a new laptop. Or my company has.
Speaking of that, I really need to get that website up asap. I am attending a pre-event next week for an event in April. Need to get a lot of things sorted before that. It's a business to business event called Kent 2020 and I will use it to do my market research and promote my business hopefully.
I had the worst day ever yesterday. Well not EVER maybe, but it wasn't good put it that way. For some reason I couldn't see anything positively. I went to body pump even though I did not feel like it at all, but after that it actually felt so much better. I didn't feel like going btw because I didn't feel like socializing. As if you socialize a lot during a class. But that might explain how little I wanted to. Unbelievable though how physical workout can change your mental state. I was happy when Jon got home though and I could vent, complain and hug a bit.


text:
Benicei és micsinyei Beniczky Gáspár, Benyiczky (Nagyrákó?, 1674. november 1. előtti napokban – Nagyrákó?, 1734. június 21. előtt röviddel.) II. Rákóczi Ferenc magántitkára.

Családja
Kiterjedt felvidéki köznemesi család evangélikus ágának sarja, Beniczky Farkas és felsőszúdi Duló Krisztina fia. Fivérei közül Márton nevű bátyja hadbiztos, Mátyás nevű öccse pedig hadi pénztáros volt a kuruc hadseregben. Legifjabb testvére, Farkas, a fejedelem apródjaként szolgált. Unokatestvérei közül Beniczky Gábor kuruc alezredes, Gerhard György pedig szenátor volt.

Élete
Pályafutását gróf Erdődy Sándor Vas vármegyei főispán szolgálatában kezdte (1704–1705), majd csatlakozott Rákóczihoz. 1707–1712 között a fejedelem bizalmas belső embere, "privatus secretariusa", azaz magántitkára volt. 1710. március 7-étől a fejedelmi magánbirtokok igazgatására létrehozott Udvari Gazdasági Tanács titkári teendőit is ellátta. 1707–1710 között napról napra a fejedelem oldalánál volt, elkísérte őt a tanácsülésekbe és a táborokba, s 1707. május 24-étől (az ónodi gyűléstől) 1710. február 28-áig részletes naplóban örökítette meg II. Rákóczi Ferenc napjait.

1711 elején ő is Lengyelországba ment, az év őszén Rákóczi kíséretében Danckába költözött. 1712 tavaszán diplomáciai megbízatást kapott: Rákóczi érdekeit kellett volna képviselnie az utóbb elnapolt lengyel országgyűlésben. Miután Rákóczi 1712 őszén Franciaországba hajózott, Beniczky Danckában maradt a Vay Ádám irányítása alatt álló udvar tagjaként. A fejedelmi levéltárat rendezgette, majd miután rokonai és pártfogói (Pálffy Miklós nádor, Csáky Zsigmond és korábbi ura, Erdődy Sándor) révén kegyelmet nyert III. Károly királytól, 1721–1722 körül hazatért.

Lengyelországban nehéz anyagi körülmények között élt, s Mányoki Ádámtól is kölcsönt kapott, amelyet hazatérése után, még az 1730-as évek elején sem tudott rendezni.

Munkája
Említett naplóját Thaly Kálmán adta ki magyarázó előszóval a hidaskürthi Nagy István gyűjteményében levő eredeti kéziratból a Rákóczi Tár első kötetében. (Pest, 1866. 1–232.)

Modern kiadása: II. Rákóczi Ferenc ezertizenkét napja. Beniczky Gáspár fejedelmi titkár diáriuma 1707. május 24. – 1710. február 28. S. a. r., az előszót és a jegyzeteket írta Bánkúti Imre. Nap Kiadó, Budapest, 2005 (Rákóczi források)

Jegyzetek

Források

Magyar történelmi személyek
A Rákóczi-szabadságharc fontosabb alakjai


text:
The South Australian Museum unveils refurbished Australian Polar Collections gallery
The South Australian Museum has unveiled a new look on level three, with the Mawson Gallery being transformed into the Australian Polar Collections gallery.
This much-loved gallery now features improved displays and digital features and showcases the very best of the Museum's Antarctic collections highlighting expeditions, biodiversity and the myriad achievements of Sir Douglas Mawson's life. It also for the first time introduces Sir Hubert Wilkins and John Riddoch Rymill and their collections to the public.
Mr Mark Pharaoh, Senior Collections Manager of Australian Polar Collections at the South Australian, says the redevelopment is a showcase for contemporary and historical Antarctic research.
"It is a magnificent opportunity for the Museum to tell the exciting story of Antarctic exploration," said Mr Pharaoh.
"Many of us are familiar with Sir Douglas Mawson, the man responsible for the legacy of scientific knowledge of the Antarctic region since the 1910s and Chair of the South Australian Museum Board from 1951-1958. Visitor favourites in the gallery include Mawson's sled, letters and balaclava, as seen on the first Australian $100 note.
"We are less familiar with Sir Hubert Wilkins, who carried out the first aerial exploration of Antarctica in the 1920s, and John Riddoch Rymill, who won several medals for his survey work in the Antarctic during the 1930s.
"Then there are the contemporary Antarctic researchers, including the Museum's very own Associate Professor Mark Stevens, as well as me, whose current day work is also represented in the updated gallery.
"With these new additions, the transformation of the Mawson Gallery into the Australian Polar Collections Gallery will create a new chapter for sharing the history of South Australian exploration in the Antarctic," said Mr Pharaoh.
Funding to renew the gallery was generously donated by the Mawson Collection Trust, which is made up of descendants of the late Sir Douglas Mawson, and through a public appeal.
Sir Douglas Mawson's grandson Alun Thomas said it was an honor to help promote and encourage scientific research and education.
"It's great to be able to work on this redevelopment, help preserve the history of my grandfather and continue to share his story with Australia," he said.
The gallery is now open to the public, just in time for the school holidays.


text:
Manager, Software Engineering - Assessment (USA Remote)
Company: Turnitin
100% REMOTE POSITION (MUST BE U.S. BASED)
When you join Turnitin, you'll be welcomed into a company that is a recognized innovator in the global education space. For more than 20 years, Turnitin has partnered with educational institutions to promote honesty, consistency, and fairness across all subject areas and assessment types. Over 16,000 academic institutions, publishers, and corporations use our services: Gradescope by Turnitin, iThenticate, Turnitin Feedback Studio, Turnitin Originality, Turnitin Similarity, ExamSoft, and ProctorExam.
Turnitin has offices in Australia, India, Indonesia, Japan, Korea, Mexico, the Netherlands, the Philippines, Ukraine, the United Kingdom, and the United States. Our diverse community of colleagues are all unified by a shared desire to make a difference in education. Come join us, and let's make change together.
Turnitin is seeking a Manager of -Software Engineering to lead -a high performing front-end/back-end team and drive development, coding and programming projects and changes for Turnitin, ensuring that all code produced and delivered by the team meets the brief/pitch and is to the highest quality standards.
This position will be managing a team of 6+ engineers who will be working on products such as Turnitin's Assessment Platform and a variety of core micro-frontend and related micro-services that will be shared across our entire product line, collaborates cross-functionally with people from Product, UX/Research, DevOps and other engineering/worktrack teams in order to deliver solutions that support our strategic company goals, using innovative technologies that maximize our productivity and help our company grow.
What You'll be Doing: -
Provide -hands on leadership of the team, setting goals and driving performance.
Collaborate -with Peers and team to define, develop and implement best practices and procedures.
Partner -with QA testing, UX, PMO, Engineering Leaders and product management to ensure on-time delivery of high quality features and to ensure resources are applied appropriately and cross-departmental issues are addressed.
Provide technical leadership and architectural oversight as necessary. Be practical enough to strike a balance between doing things 'perfectly' and doing things 'well enough to ship'.
Analyze -and utilize -quality metrics across development projects
Take -passionate ownership of the software your team builds, and the way that they build it. - Take pride in both the quality of the code we produce and on our commitment to improving our processes along the way.
Promote -a healthy culture, shaping and evangelizing engineering standards and best practices to improve team productivity. -
Providing and environment of openness and transparency while sharing your opinions and speaking up when you think we could be doing something better than we're doing it now - tactfully and empathetically to communicate continuous improvement opportunities in a way that brings people along instead of distancing them
Mentor, coach -and develop the careers of a talented group of engineers
Provide -development opportunities for the team to broaden and enhance their skill sets, working with the team to ensure they have Individual development plans to stretch and grow their skills
Identify -opportunities for improvement by challenging the status quo and defining alternative and creative solutions
Stay -up-to-date with new tools and development strategies while -bringing recommendations for change and innovation to leadership and own team.
Ensure -the team has great communication across the organization and are up to date with the vision and mission of the company.
Be a proactive team player and communicator - both to your teammates and our collaborators from other engineering teams, product, customer support, sales, you get the picture. - Our work impacts a lot of people, and there are a lot of stakeholders who need to maintain context alongside us as progress / decisions are made.
Take -part in projects as requested.
3+ years hiring, managing and mentoring quality/software engineering staff
Experience building and architecting highly scalable front-end/back-end serverless applications (Angular, Java, AWS)
Strong knowledge of software methodologies, tools and processes
Experience working and collaborating with teams across multiple time zones and geographies.
Experience working collaboratively with cross-functional Agile teams.
Excellent organizational communication and leadership skills. -
Excellent analytical and problem-solving skills.
Proactive working style with the ability to adapt to change.
Our Mission is to ensure the integrity of global education and meaningfully improve learning outcomes. -
Our Values underpin everything we do.
Customer Centric - We realize our mission to ensure integrity and improve learning outcomes by -putting educators and learners at the center of everything we do.
Passion for Learning - We seek out teammates that are constantly learning and growing and build a workplace which enables them to do so.
Integrity - We believe integrity is the heartbeat of Turnitin. It shapes our products, the way we treat each other, and how we work with our customers and vendors.
Action & Ownership - We have a bias toward action and empower teammates to make decisions.
One Team - We strive to break down silos, collaborate effectively, and celebrate each other's successes.
Global Mindset - We respect local cultures and embrace diversity. We think globally and act locally to maximize our impact on education.
Seeing Beyond the Job Ad
At Turnitin, we recognize it's unrealistic for candidates to fulfill 100% of the criteria in a job ad. - We encourage you to apply if you meet the majority of the requirements because we know that skills evolve over time. If you're willing to learn and evolve alongside us, join our team! - -
Turnitin, LLC is committed to the policy that all persons have equal access to its programs, facilities and employment. We strongly encourage applications from people of color, persons with disabilities, women, and the LGBTQ+ community, regardless of age, gender, religion, marital or veterans status.
Keywords: Turnitin, San Diego , Manager, Software Engineering - Assessment (USA Remote), IT / Software / Systems , San Diego, California
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text:
Marketing Apps
Why Vionic?
Deal Maker
Jeff Donahue
Mr. Donahue has a comprehensive finance and strategy background in start-up and privately-held companies in North America and Europe. He also has extensive international finance experience with Fortune-100 companies and privately held companies in Asia-Pacific, Europe, Russia and the CIS, Africa, Latin America and North America.
Prior to joining Ostendo Technologies in Carlsbad, CA, as CFO in October 2011, Mr. Donahue was CFO of EMN8, Inc. in San Diego, a 2010 Red Herring North America 100 and Global 100 company whose investors include Allegis Capital, Global Retail Partners, Sid R. Bass Associates, Sequoia Capital and Steamboat Ventures. EMN8 designs, manufactures, sells and services self-service ordering and payment hardware and software for the retail and hospitality industries. Previously, he was acting CFO of SKY MobileMedia, Inc. in San Diego, a wireless applications software platform company funded by Enterprise Partners and Sid R. Bass Associates, and CFO of Accordent Technologies, Inc. in Hermosa Beach, a venture-backed enterprise media management solutions company acquired by Polycom.
Mr. Donahue also was CFO of Castify Networks S.A. in Sophia Antipolis, France, a content net-working and delivery software company funded by Swiss, Italian and UK venture capital firms acquired by Omneon. Prior to Castify, he was co-founder and Senior Vice President – Finance of AduroNet Ltd. in London, a pan-European IP-VPN company funded by US and European venture capital firms and institutional investors.
Mr. Donahue also was Vice President – Corporate Development for Global TeleSystems Group in London (pre- and post-IPO), and CFO of the Russian Telecommunications Development Corpor-ation in Moscow. Prior to entering the technology and telecommunications sector, Dr. Donahue spent 3 years with W.R. Grace & Co. in Florida and Hong Kong and 14 years with Union Carbide Corporation in various overseas locations, New York and Connecticut.
Mr. Donahue has completed over $250 million of funding for early and late stage start-up companies since 2000, including venture capital financing, equipment lease financing, working capital financing and bridge financing. He also completed over $300 million of institutional and sovereign financing for emerging growth companies and over $2 billion in various types of debt and equity financing for public multinational companies. His financing transactions include an IPO in Sri Lanka, project financing in China, Islamic funding across Asia-Pacific, bridge financing in India, fixed asset, institutional equity and working capital financing in Russia, and export financing in Africa. He also has an extensive global mergers, acquisitions and divestitures background. He has served on the Board of Directors of public companies in Australia, India, New Zealand and Sri Lanka.
Mr. Donahue holds Ph.D. and M.Sc. degrees in Economics from Florida State University and a B.A. in business from the University of South Florida. He also attended the Executive Program (SEP) at Stanford University's Graduate School of Business. He is a member of the International Advisory Board of the School of International Relations and Pacific Studies (IR/PS) at the University of California, San Diego. He and his wife, Gail, are founding members of the IR/PS 21st Century China Program, a leading research and educational center dedicated to the study of contemporary China and emphasizing interactive as well as scholarly engagement with China.
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Our main program that we offer, EAP, is an innovative approach to professional counseling using horses to help address and resolve emotional, behavioral, relational and spiritual issues. A holistic healing therapy between a child and a horse through measured success with a licensed Mental Health Therapist, teamed with a EAGALA Certified Equine Specialist.
Research and studies demonstrate that this approach provides an atmosphere whereby a child is actively engaged in posing questions, investigating, experimenting, being curious, solving problems, assuming responsibility, being creative, and constructing meaning. This offers the child insight on how to find their own best solutions.
The EAGALA model EAP has effectively been employed in the treatment of numerous behavioral and emotional disorders that are traditionally resistant to intervention and change including conduct disorder, oppositional-defiant disorder, personality disorders and eating disorders.
Cross Roads is involved with Fostering Great Ideas, a non-profit charity that focuses on impacting foster children's lives by pairing up adult volunteers mentoring these children in the hopes of creating a better experience while in foster care. We are committed to empowering these foster children with the tools that are needed to guide them when important decisions arise at the cross roads in their lives.
Our Rodeo team consists of the transition from beginner to intermediate riders and on to advanced. The rodeo team members practice technique, timed events, such as barrels, poles etc. and then give back to the beginners by volunteering their time teaching, in order for the beginners to advance their horsemanship skills.
A great program that we offer every Tuesday night down at the Ranch. Wonderful fellowship with each other with a variety 0f backgrounds intertwined. Our wonderful volunteers from the local churches bring Inspiration and the Word to these teens, as well as local music artists delivering beautiful sounds, encouragement and praise. A big hit with these teens is the delicious meals that are provided by our generous and charitable volunteers.
Our summer work program acts as a regular summer job for foster care teens close to aging out of the foster care system. They are at the ranch early in the morning, working a real job to teach values like leadership, communication, respect and responsibility.
The youth participates in the program by working at the ranch for 6 weeks and are paid for their time, helping them to transition into adulthood in many ways. The program has been extremely beneficial to all youth involved.
The ranch has successfully administered this program in conjunction with Urban League to both boys and girls in the foster care for the past 4 years.
Providing children with professional, hands on instruction in horsemanship skills, safety and care.
Beginning in June of 2016, we will be offering a week long camp dedicated to children, ages 6-18. This program comprises a wide variety of goals and activities. All campers will learn about horses, the basic fundamentals and care regime. The difference between English & Western styles and each category of competition. Learning how to ride barrels, posting and jumping. How to become savvy and have basic survival skills in the woods by obtaining a sense of direction through hiking, marking and compass reading. Activities include but not limited to swimming, kayaking, slip and slide, fishing and crafts.


text:
\section{Introduction}
The recent cosmic acceleration has emerged as an intriguing phenomenon in cosmology. It was first observed during supernova observations in late nineties \cite{RiessPerlmutter}. Subsequent cosmological  observations like type Ia supernova data \cite{suzuki,betoul}, galaxy cluster measurement \cite{allensw} etc have confirmed the accelerated expansion of the universe. The discovery of this phenomenon has propelled the research in cosmology towards a new direction, particularly the basic understanding about the contents of the universe has been  changed radically.  The spectacular development in cosmological observations in the last two decades have imposed tighter constraints on various cosmological models, but the genesis of the cosmic acceleration is still far from being resolved.

\par Various possibilities are explored in order to find an explanation of the late time cosmic acceleration. One way is to introduce an exotic component in the matter sector. This exotic component, dubbed as {\it dark energy}, with a  characteristic negative pressure, leads to the repulsive nature of gravity at cosmological scale. The most popular model of dark energy is the cosmological constant $\Lambda$, which is based upon the assumption that the constant vacuum energy density serves as the candidate of dark energy. The appearance of $\Lambda$ in cosmological models is not new and thus a less radical change in the cosmological models. Though strongly supported by observations, the $\Lambda$CDM (cosmological constant $\Lambda$ with pressureless cold dark mattre) model suffers from various inconsistencies, mainly the fine tuning problem. An elaborate discussion on the merits and problems of the  $\Lambda$CDM model and various related issues have been discussed by Padmanabhan\cite{padmanabhan}. Dark energy candidates that evolve with time  provide efficient alternatives, but have the disadvantage of not properly motivated from other branches of physics.  There  are some excellent reviews on different dark energy models\cite{sahnicopeland}. The other way to look for a plausible reason behind the cosmic acceleration is to find a suitable modification of the General Relativity (GR) such as $f(R)$ gravity models \cite{CappozilloCarroll}, scalar-tensor theories \cite{scalten} and different higher dimensional gravity theories \cite{dvalideffayet}. The most common problem of such models is that they can hardly match GR in the context of local astronomy.

\par The recent trend in the modelling of cosmic evolution is to build up the model from observational data. This reverse way of finding viable a cosmological model is called {\it reconstruction}. Pioneering work in this direction was by Starobinsky \cite{starore}, where the scalar field potential, used as the dark energy, has been reconstructed by using the density perturbation data. The data of distance measurement of supernova has been utilized in the context of reconstruction by Huterer and Turner \cite{huterner} and by Saini et al. \cite{sainiray}. Parametrization of quintessence scalar field and potential from effective equation of state of dark energy has been discussed by Guo, Ohat and Zhang \cite{guohta}. Construction of non-canonical kinematic terms has been discussed by Li, Guo and Zhang \cite{liguo}. There are two types of practice in reconstruction. The first one is parametric reconstruction which is based upon the assumption of a parametric form of cosmological quantities  like the dark energy equation of state ($w_{DE}$), dark energy density ($\rho_{DE}$), the quintessence the potential etc \cite{cpl,gph} and an estimation of the parameters from the available data. The other one is a non-parametric reconstruction which is an attempt to estimate the evolution of $w_{DE}$ directly from observational data without an assumption of any parametric form \cite{nonpara}.

\par The normal practice in cosmology is to write down Einstein equations, $G_{\mu\nu}=-8\pi G T_{\mu\nu}$ for a spatially homogeneous and isotropic model with the right hand side taking care of the matter sector. The present work has a completely different approach. We assume a spatially flat homogeneous and isotropic metric and define the usual kinematical quantites like the Hubble paramater $H$, the deceleration parameter $q$ and the jerk parameter $j$, which are respectively the first order, second order and third order time derivatives of the scale factor $a$. The derivatives are all fractional derivatives and furthermore $q$ and $j$ are dimensionless. We have observational results of the evolution of $q$, in the sense that the parameter is negative at the present epoch and had been positive in a recent past, the epoch of transition from the decelerated to the accelerated expansion is also known. The natural choice of the kinematical quantity of interest is thus the evolution of $q$, which is the jerk parameter $j$. We now assume a constant jerk and find the evolution of the other kinematical quantities from the definition of jerk. The values of the various kinematical quantities and the model parameters, which come out as the constant of integration and the value of $j$, are then estimated from known observational data sets.

\par The reconstruction technique normally involves finding out the equation state parameter $w_{DE}$ given by $w_{DE}=\frac{p_{DE}}{\rho_{DE}}$, the ratio of the contribution to the pressure and density sectors from the dark energy. The approach is indeed physical, as it directly talks about the nature of the dark energy sector. Although much less used, the kinematical approach has the virtue of not having any apriori prejudice regarding the dark energy. Pioneering work in the kinematic modelling of cosmic acceleration was by Riess {\it et al.} \cite{riess} where a linear parametrization of the deceleration parameter has been adopted to estimate the redshift at which the transition from decelerated to accelerated expansion phase occurred. Different parametrization of deceleration parameter have been discussed by Shapiro and Turner \cite{shapiroturner}, Gong and Wang \cite{gongwang}, Xu and Liu \cite{xuliu} and Elgaroy and Multamaki \cite{elgaroymultamaki}. Recently kinematic method to investigate the cosmic acceleration has been discussed by Barboza and Carvalho \cite{barbozacarvalho}.

\par As already mentioned, the jerk parameter had hardly been used until very recently. However, its importance in building a cosmological model had been emphasized long back in terms of a ``state-finder'' parameter\cite{varun1}. The indication of importance of jerk as a future tool for the reconstruction of cosmological models was also indicated by Alam, Sahni, Saini and Starobinsky\cite{varun2}. The reason for its being overlooked as the starting point of reconstruction was perhaps the unavailability of clean data. Reconstruction of dark energy model using deceleration parameter ($q$) and jerk ($j$) as model parameters was discussed by Rapetti {\it et al.} \cite{rapetti} where the present values of the kinematical parameters have been constrained using observational data. Parametrization of time evolving jerk parameter models  have been discussed recently by Zhai {\it et al.} \cite{zhai} and by Mukherjee and Banerjee \cite{mukban}.

\par If the agent driving the present acceleration is the cosmological constant, then certainly the dark matter sector follows its own conservation equation. However, if the dark energy is an evolving one, there is always a possibility that the two dark sectors interact with each other, one may grow at the expense of the other. Naturally there is a lot of work in the literature where the interacting dark energy model has been discussed. Cosmological evolution of interacting phantom dark energy has been discussed by Guo, Cai and Zhang \cite{guocai}. Guo, Ohta and Tsujikawa have emphasised on the observational constraints on the coupling between different dark components of the universe \cite{guohtatsu}. The last two investigations assume that the interaction is proportional to the total energy density. An interacting dark energy model has recently been  given by Pan, Bhattacharaya and Chakraborty \cite{panbhatta} where again the interaction term is assumed to be proportional to the total energy density. Holographic dark energy models with Hubble scale as the infra red cut off require the interaction between dark energy and dark matter to yield the recent accelerated expansion with a history of a decelerated expansion in the past. Interacting holographic dark energy model has been discussed by Zimdahl and Pavon \cite{zimdahlpavon}. For a {\it graceful entry} of the universe from a decelerated to an accelerated phase in Brans-Dicke theory, the interaction of the Brans-Dicke scalar field and the quintessence scalar field had been discussed by Das and Banerjee \cite{sudipta}. An attempt towards a covariant Lagrangian formulation of the interaction has been made by Faraoni, Dent and Saridakis\cite{faraoni}. Reconstruction of the interaction rate in holographic dark energy model has been discussed by Sen and Pavon \cite{senpavon} where the reconstruction has been done with a prior assumption about the dark energy equation of state. Reconstruction of interaction rate in holographic dark energy from parametrizations of deceleration parameter has been discussed by Mukherjee \cite{amholography}. Recently non-parametric reconstruction of dark energy interaction using Gaussian process has been discussed by Yang, Guo and Cai \cite{yangguocai} where the signature of dark energy interaction has been obtained for a deviation of dark energy equation of state parameter from the value -1.

\par The present work is an attempt to reconstruct the possible interaction of various matter components from the data sets in a kinematical approach. The starting point is a constant jerk parameter. The result is that any deviation from the $\Lambda$CDM model indicates a possibility of an interaction amongst various matter sectors. The best fit values, however, are tantalizingly close to the $\Lambda$CDM scenario. Another important result is that the allowance of any interaction is more stringent at recent times, but slightly more relaxed in the past.

\par It should also be mentioned at the outset that the entire work depends upon the dogma that a $\Lambda$CDM model should be included as a possibility in an endeavour leading to the reconstruction of the dark energy, at least as a limit.

\par In the following section (section II), the reconstruction of the model has been discussed. The results of the statistical analysis have been presented in section III. A discussion of the results and some concluding remarks have been included in section IV.

\section{Reconstruction of the model for a constant jerk parameter}
The mathematical framework of cosmology begins with the assumption of a homogeneous and isotropic universe, where the distance element is defined as
\be
ds^2=-dt^2+a^2(t)\Big[\frac{dr^2}{1-kr^2}+r^2d\Omega^2\Big].
\ee
Here $k$, which can have values $0$ or $\pm1$, conveys the information regarding the nature of spatial curvature. The time dependent quantity in the coefficient of the spatial part of the metric, $a(t)$, is called the scale factor. It takes care of the time evolution of the spatial separation of two space-time point. Here further calculations have been continued assuming the spatial flatness of the universe, i.e. $k=0$.
\par The fractional rate of expansion of the linear size of the universe, dubbed as the Hubble parameter, is defined as
\be
H(t)=\frac{\dot{a}}{a},
\label{hubbleparameter}
\ee
where the overhead dot denotes a derivative with respect to the cosmic time $t$. To understand the nature of the expansion, higher order time derivatives of the scale factor are to be invoked. The measure of cosmic acceleration is presented in a dimensionless way by the deceleration parameter $q$, defined as
\be
q(t)=-\frac{\ddot{a}/a}{\dot{a}^2/a^2}=-1-\frac{\dot{H}}{H^2}.
\label{decelerationparameter}
\ee
If the value of the deceleration parameter is negative, then the expansion is accelerated.
\par The cosmic `jerk parameter', which is the dimensionless representation of the third order time derivative of the scale factor, is defined as
\be
j(t)=-\frac{1}{aH^3}\Bigg(\frac{d^3a}{dt^3}\Bigg).
\label{jerkparameter}
\ee

\par It is convenient to convert the time derivatives to the derivatives with respect to the redshift $z$ (where $1+z=a_0/a$, $a_0$ being the present value of $a$) for studying the dynamics of the universe as $z$ is a dimensionless quantity. From the equation (\ref{jerkparameter}), the expression for the jerk parameter will be
\be
j(z)=-1+(1+z)\frac{(h^2)'}{h^2}-\frac{1}{2}(1+z)^2\frac{(h^2)''}{h^2},
\label{jerkequation}
\ee
where $h(z)=\frac{H(z)}{H_0}$, ($H_0$ being the present value of the Hubble parameter) and a prime denotes the derivative with respect to $z$. In the present work, the reconstruction is done with the assumption that $j$ is a slowly varying quantity, and will be considered a constant in the subsequent discussion. The solution of the differential equation (\ref{jerkequation}) yields the expression of $h^2(z)$ as
\be
h^2(z)=A(1+z)^{\frac{3+\sqrt{9-8(1+j)}}{2}}+B(1+z)^{\frac{3-\sqrt{9-8(1+j)}}{2}},
\label{h2zABj}
\ee
where $A$ and $B$ are the constant dimensionless coefficients. Now the relation between $A$ and $B$ is obtained from the boundary condition $h(z=0)=1$ as $A+B=1$. Finally $h^2(z)$ is written as a function of redshift $z$ and two parameters $j$ and $A$ as
\be
h^2(z)=A(1+z)^{\frac{3+\sqrt{9-8(1+j)}}{2}}+(1-A)(1+z)^{\frac{3-\sqrt{9-8(1+j)}}{2}}.
\label{h2zAj}
\ee
Therefore this is effectively a two parameter model where $j$ and $A$ are the model parameters. The value of $j$ obtained from the statistical analysis of the reconstructed model using different observational data would indicate the consistency or deviation of this model from the $\Lambda$CDM and it exactly mimics the $\Lambda$CDM for $j=-1$. The deceleration parameter (defined in equation (\ref{decelerationparameter})) can also be expressed for the present model in terms of the model parameters and the redshift as,

\be
q(z)=-1+\frac{A\Bigg(\frac{3+\sqrt{9-8(1+j)}}{4}\Bigg)(1+z)^{\frac{3+\sqrt{9-8(1+j)}}{2}}}{h^2(z)}
+\frac{(1-A)\Bigg(\frac{3-\sqrt{9-8(1+j)}}{4}\Bigg)(1+z)^{\frac{3-\sqrt{9-8(1+j)}}{2}}}{h^2(z)}.
\ee

\par One component of the matter content of the universe, whether it interacts with the dark energy sector or not, is generally believed to be a cold dark matter with an equation of state $p=0$. If we stick to this presupposition, and attempt to recover a non-interacting pressureless fluid at least as a limit from equation (\ref{h2zAj}) for some value of $j$, we find that the second term of the right hand side of equation (\ref{h2zAj}) can yield a highest power of $(1+z)$ as $3/2$ and can not serve the purpose. The only possibility that remains is $j=-1$ which yield the standard $(1+z)^3$ behaviour in the first term. So we identify the first term to represent the contribution from the cold dark matter, which, in the non-interacting limit, yield a $(1+z)^3$ behaviour as in the standard dust model. The rest of the work will depend on this identification. One should note that this is not the only plausible choice. It may well be possible to find a corresponding pressure to each of the contribution to the matter sector so that both the component conserve by themselves. One can easily calculate the equation of state parameter $w$ (given by $w=\frac{pressure}{density}$) for both the contribution. A straightforward calculation for a constant $w$ will yield

\be
9w(w+1)+2(1+j)=0,
\label{weqe}
\ee

It is easy to see that $j=-1$ again gives two solutions of equation (\ref{weqe}) $w=0$ and $w=-1$ leading to a $\Lambda$CDM behaviour where $w=0$ corresponds to the cold dark matter and $w=-1$ corresponds to the cosmological constant. However, this will not lead to any interaction. One should also note that starting from the definition of the jerk parameter (equation (\ref{jerkparameter})), with the assumption that $j$ is a constant, one actually recovers one of the Einstein's equations for the system, where the nature of the matter sector depends on the value of the parameter. Thus the parameter $A$ is equivalent to the matter density parameter $\Omega_{m0}$ because for $j=-1$, the power of $(1+z)$ in the first term on the right hand side of equation (\ref{h2zAj}) is 3 and the second term is a constant, equivalent to the constant vacuum energy density. If the power of $(1+z)$ in the first term is different from  3, the dark matter is not separately conserved. This invokes the possibility of interaction between the dark matter and the dark energy.

\par To investigate the nature of interaction for the present model, the total conservation equation which is a direct consequence of contracted Bianchi identity, can be divided into two parts as the followings,
\be
\dot{\rho}_m+3H\rho_m=\eta,
\label{mattcon}
\ee
and
\be
\dot{\rho}_{DE}+3H(1+w_{DE})\rho_{DE}=-\eta.
\ee
The over head dots represent the differentiation with respect to cosmic time, $\rho_m$ and $\rho_{DE}$ are the matter density and dark energy density respectively, $w_{DE}$ is the dark energy equation of state parameter. As the dark energy and dark matter interact with themselves, they are not conserved individually. The growth rate of one component, namely $\eta$, is the decay rate of the other. In the present work, the possibility of interaction has been studied. For a dimensionless representation, $\eta$ has been scaled by ($3H_0^3/8\pi G$) and written as
\be
Q=\frac{8\pi G}{3H_0^3}\eta.
\label{Qz}
\ee
For the $\Lambda$CDM model, the value of $Q$ is zero. In the present work, observational constraints on the late time evolution of $Q(z)$ has been obtained. As in the expression of the Hubble parameter (equation (\ref{h2zAj})), the first term of the right hand side, i.e. $A(1+z)^{\frac{3+\sqrt{9-8(1+j)}}{2}}$, is considered to be the matter density scaled by the present critical density, from equation (\ref{mattcon}), the interaction term $Q$ can be expressed in terms of the parameters and redshift, as
\be
Q(z)=A\Bigg(\frac{3-\sqrt{9-8(1+j)}}{2}\Bigg)(1+z)^{\frac{3+\sqrt{9-8(1+j)}}{2}}h(z).
\label{intQ}
\ee

It is important to note that the second  term on the right hand side of equation (\ref{h2zAj}) is considered to be the contribution from the dark energy density. Thus the expression of the dark energy equation of state parameter ($w_{DE}=p_{DE}/\rho_{DE}$) looks like,

\be
w_{DE}(z)=-\Bigg(\frac{3+\sqrt{9-8(1+j)}}{6}\Bigg)-\Big(\frac{A}{1-A}\Big)
\Bigg(\frac{3-\sqrt{9-8(1+j)}}{6}\Bigg)(1+z)^{\sqrt{9-8(1+j)}}.
\ee

\section{Results of statistical analysis}

\begin{figure}[htb]
\begin{center}
\includegraphics[angle=0, width=0.28\textwidth]{SNeNHBAO1_constjerk.eps}
\includegraphics[angle=0, width=0.28\textwidth]{SNeNHBAO2_constjerk.eps}
\includegraphics[angle=0, width=0.28\textwidth]{SNeNHBAO3_constjerk.eps}
\end{center}
\caption{{\small Confidence contours on the 2D parameter space of the reconstructed model. The 1$\sigma$, 2$\sigma$ and 3$\sigma$ confidence regions have been presented from inner to outer area and the central black dots represent the corresponding best fit point. The left panel shows the confidence contours obtained for the statistical analysis using OHD+SNe data, the middle panel is  obtained SNe+BAO and the right panel is for OHD+SNe+BAO.}}
\label{contourplot1}
\end{figure}

\begin{figure}[htb]
\begin{center}
\includegraphics[angle=0, width=0.35\textwidth]{SNeNHBAOLikelihoodA_constjerk.eps}
\includegraphics[angle=0, width=0.35\textwidth]{SNeNHBAOLikelihoodj_constjerk.eps}
\end{center}
\caption{{\small Plots of marginalized likelihood functions of the reconstructed model. The dotted curves represents the likelihood obtained for OHD+SNe, dashed curves represents the likelihood for SNe+BAO and the solid curves represents the likelihood for OHD+SNe+BAO.}}
\label{likelihoodplot1}
\end{figure}

Now the remaining task is to estimate the parameter values from observational data sets. In the present work, three different data sets have been adopted. These are (i) the observational Hubble parameter data (OHD), (ii) the distance modulus data of type Ia supernova (SNe) and (iii) baryon acoustic oscillation data (BAO).

\par For the first set of data, measurement of Hubble parameter at different redshift by using differential age  of galaxies as an estimator \cite{simonohd}, measurement from red-enveloped galaxies \cite{sternohd}, measurement of expansion rate of the universe by Moresco et al \cite{morescoohd}, Measurement of expansion history from WiggleZ Dark Energy Survey as discussed by Blake et al. \cite{blakeOHD}, the measurement of Hubble parameter from Sloan Digital Sky Survey (SDSS) data by Zhang et al \cite{zhangohd} have been adopted in the present analysis. The recent measurement of Hubble parameterat z=2.34 by Delubac et al \cite{delubacohd} has also been incorporated in the present analysis. The present value of Hubble parameter $H_0$, estimated from the combined analysis with Planck+WP+highL+BAO \cite{planck}, has also been adopted in the present analysis.

\par  The supernova distance modulus data (SNe) of joint lightcurve analysis (jla) has been adopted in this work \cite{betoul} for the second category. The binned data of jla has been used along with the covariance matrix of the binning.

\par Finally, baryon acoustic oscillation (BAO) measurements at three different redshifts (6dF Galaxy Surve at redshift z=0.106 \cite{beutlerbao}, the Baryon Oscillation Spectroscopic Survey at redshift z=0.32 (BOSS LOWZ) and at redshift z=0.57 (BOSS CMASS) \cite{andersonbao}) along with the measurement of acoustic scale and comoving sound horizon at photon decoupling and drag epoch from CMB \cite{planck,wangwangCMB} have been adopted.

\par The $\chi^2$ minimization technique which is equivalent to the maximum likelihood analysis, has been adopted to find the best fit values of the model parameters. The results have been obtained for different combinations of the data sets. The $\chi^2$ is defined as
\be
\chi^2=\sum_i\frac{[\epsilon_{obs}(z_i)-\epsilon_{th}(z_i.\{\theta\})]^2}{\sigma_i},
\ee
where $\epsilon_{obs}$ is the value of the observable measured at redshift $z_i$, $\epsilon_{th}$ from of the observable quantity as a function of the set of model parameters $\{\theta\}$ and $\sigma_i$ is the uncertainty associated to the measurement at $z_i$. The combined analysis has been carried out by adding the $\chi^2$ of the individual data sets taken into account for that particular combination. The combined $\chi^2$ is defined as,
\be
\chi^2_{combined}=\sum_d\chi^2_d,
\ee
where $d$ represents the individual data set.
\par The kinematic model discussed in the present work contains two parameters ($A$, $j$) where the parameter $A$ is coming as an integration constant and the $j$ is the constant jerk parameter. As mentioned earlier, it is imperative to note that the parameter $A$ is equivalent to matter density parameter. The value of jerk parameter $j$, estimated from observational data, would indicate the deviation, if any, of the present model from $\Lambda$CDM, for $j=-1$, the present model mimics the $\Lambda$CDM.

\par The expression of the Hubble parameter  obtained for the present model (equation (\ref{h2zAj})) shows that the matter sector has two components. The first one, with constant coefficient $A$, is the dark matter density and the other one is the dark energy density. As the  energy density of relativistic particles, mainly the photon and neutrino, have an effective contribution to the dynamics of the of the universe at very high redshift, an additional energy density term, evolving as $(1+z)^4$ for radiation, has been taken into account while using the  angular diameter distance measurement in the analysis with BAO data. The present value of the energy density of relativistic particles scaled  by the present critical density is taken to be $\Omega_{r0}=9.2\times10^{-5}$ with the adopted fiducial value of current CMB temperature $T_0=2.7255$K. The adopted fiducial value of $T_0$ is based on the measurement of current CMB temperature $T_0=2.7255\pm0.0006$K \cite{fixsenT0}. As the prime endeavour of the present work is to reconstruct the late time dynamics of the universe, the radiation energy density is not taken in account as it has a negligible contribution at late time, i.e., in equation (\ref{h2zAj}).

\begin{table}[h!]
\begin{center}
\resizebox{0.6\textwidth}{!}{
\begin{tabular}{ c |c |c c }
\hline
 \hline
  Data & $\chi^2_{min}/d.o.f.$  & $A$ & $j$ \\
 \hline
  OHD+SNe & 47.30/54 & 0.305$\pm$0.023 & -0.861$\pm$0.127\\

  SNe+BAO & 33.95/28 & 0.297$\pm$0.024 & -1.014$\pm$0.045\\

  OHD+SNe+BAO & 48.28/54 & 0.286$\pm$0.015 & -1.027$\pm$0.037\\
 \hline
\hline
\end{tabular}
}
\end{center}
\caption{{\small  Results of statistical analysis with different combinations of the data sets. The value of $\chi^2_{min}/d.o.f.$ and the best fit values of the parameters along with the  associated 1$\sigma$ uncertainties are presented.}}
\label{tableAj}
\end{table}

\begin{figure}[htb]
\begin{center}
\includegraphics[angle=0, width=0.35\textwidth]{q.eps}
\includegraphics[angle=0, width=0.35\textwidth]{weffz.eps}
\end{center}
\caption{{\small The plots of the deceleration parameter ($q(z)$) (left panel) and the effective equation of state parameter ($w_{eff}(z)$) (right panel) for the reconstructed model. The corresponding 1$\sigma$ and 2$\sigma$ confidence regions and the best fit curves obtained in the analysis combining OHD, SNe and BAO data sets, are presented.}}
\label{qzweffz}
\end{figure}

\begin{figure*}[ht]
\begin{center}
\includegraphics[angle=0, width=0.30\textwidth]{wDEz1.eps}
\includegraphics[angle=0, width=0.30\textwidth]{wDEz2.eps}
\includegraphics[angle=0, width=0.30\textwidth]{wDEz3.eps}
\end{center}
\caption{{\small The plots of the dark energy equation of state parameter ($w_{DE}(z)$), obtained from the analysis with different combination of the data sets are presented. The corresponding 1$\sigma$ and 2$\sigma$ confidence regions and the best fit curves are shown.}}
\label{wDEz}
\end{figure*}

\begin{figure*}[htb]
\begin{center}
\includegraphics[angle=0, width=0.30\textwidth]{Qz1.eps}
\includegraphics[angle=0, width=0.30\textwidth]{Qz2.eps}
\includegraphics[angle=0, width=0.30\textwidth]{Qz3.eps}
\end{center}
\caption{{\small The plots of interaction term $Q(z)$, obtained from the analysis with different combination of the data sets are presented.  The corresponding 1$\sigma$ and 2$\sigma$ confidence regions and the best fit curves are shown. The Q=0 straight line represents the $\Lambda$CDM model.}}
\label{Qz}
\end{figure*}

\par Figure \ref{contourplot1} shows the confidence contours on the two dimensional (2D) parameter space of the model for different combinations of the data sets and figure \ref{likelihoodplot1} presents the plots of marginalized likelihoods as functions of the model parameters. The likelihoods are well fitted to Gaussian distributions. Table \ref{tableAj} shows the results of the statistical analysis for different combinations of the data sets. The reduced $\chi^2$ (i.e. $\chi^2/d.o.f.$) values are also presented to have an estimation of the goodness of fitting. Both figure \ref{contourplot1} and table \ref{tableAj} clearly show that the best fit value of $j$ is very close to $-1$, indicating clearly that the model with a constant jerk parameter is tantalizingly close to $\Lambda$CDM model.

\par Figure \ref{qzweffz} presents the plots of deceleration parameter $q(z)$ (left panel) and the effective or total equation of state $w_{eff}(z)$ (right panel) where $w_{eff}=p_{DE}/(\rho_m+\rho_{DE})$. The deceleration parameter plot clearly shows that the reconstructed model successfully generates the recent cosmic acceleration along with the decelerated expansion phase that prevailed in the past. The redshift of transition from decelerated to accelerated expansion phase obtained for the present model is 0.6 to 0.8 which is consistent with the result of recent analysis by Farooq and Ratra \cite{farooqratra}. Figure \ref{wDEz} presents the plots of dark energy equation of state parameter $w_{DE}$, obtained from the analysis with different combinations of the data sets. The best fit curves remain very close to the corresponding $\Lambda$CDM value $w_{DE}=-1$ and the deviation increases at high redshift. The best fit curve obtained in the analysis combining OHD, SNe and BAO data sets shows a slight inclination towards the non-phantom nature of dark energy. But the phantom nature ($w_{DE}<-1$) is also well within the 1$\sigma$ confidence region (figure \ref{wDEz}). The interaction between the dark matter and dark energy that crosses the phantom barrier of $w_{DE}=-1$ has been discussed by Guo {\it et al.} \cite{guopiao1,guopiao2}. It is clear from the plots the the nature of the best fit curve is sensitive to the combination of  the data sets taken into account.   The plots also show that the $w_{DE}(z)$ is constrained better at low redshift and the uncertainty increases at high redshift. It deserves mention in this context that the value of jerk parameter ($j$) and the the evolution of dark energy equation of state parameter ($w_{DE}$), obtained in the analysis with different combinations of the data sets,indicate that the reconstructed model is at close proximity of $\Lambda$CDM.

\begin{table}[h!]
\begin{center}
\resizebox{0.35\textwidth}{!}{
\begin{tabular}{ c |c  }
\hline
 \hline
  Data  & $Q(z=0)$ \\
 \hline
  OHD+SNe  & $0.0292\pm0.0293$\\

  SNe+BAO &  $-0.0026\pm0.0087$\\

  OHD+SNe+BAO &  $-0.0051\pm0.0067$\\
 \hline
\hline
\end{tabular}
}
\end{center}
\caption{{\small The present value of the interaction term i.e. $Q(z=0)$ obtained for different combinations of the data sets. The corresponding best fit values and the associated 1$\sigma$ uncertainties are presented.}}
\label{tableQ0}
\end{table}

\par Figure \ref{Qz} shows the evolution of  the interaction term $Q(z)$, defined in equation (\ref{intQ}). For the present model, any deviation from $\Lambda$CDM indicates a possibility of interaction between dark energy and dark matter. For non interacting models, the interaction term $Q(z)$ is zero. The plots of $Q(z)$ of the present model obtained from the analysis with different combination of the data sets show that the evolution of  $Q(z)$ is also sensitive to the choice of data sets. However, for all combinations of the data sets taken in the present work show the possibility of interaction between dark energy and dark matter is very low at present epoch. But the possibility of interaction is high at high redshift. The $\Lambda$CDM always remains within the 1$\sigma$ confidence region. The result obtained from the combination of SNe, OHD  shows a higher preference towards the interaction at high redshift (left panel of figure \ref{Qz}). But the addition of BAO data brings best fit curve closer to $\Lambda$CDM. It is also easy to note that the present analysis allows both positive and negative value for the interaction term $Q(z)$. Table \ref{tableQ0} presents the present values of the interaction term obtained from the analysis with different combination of the data sets. The result obtained from the analysis combining SNe, OHD and BAO data shows that the best fit curve of $Q(z)$ has an inclination towards negative value. But the possibility of a positive $Q(z)$ is also well within the 1$\sigma$ confidence region. The requirement of a positive $Q(z)$ in the context of thermodynamics has been discussed by Pavon and Wang \cite{pavonwang}.

\section{Discussion}
The present work is an attempt to search for the possibility of interaction between the dark matter and the so-called dark energy with a kinematic approach. The other crucial factor is that we start from the dimensionless jerk parameter $j$ which is a third order derivative of the scale factor $a$. This choice is of a natural interest, as the evolution of $q$, the second order time derivative of $a$ is an observational quantity now. We start from the geometrical definition of jerk, and do not use even Einstein equations to start with. We reiterate the word of caution, the conclusion that any deviation of the jerk parameter from $-1$ indicates an interaction between dark matter and dark energy sectors is actually based on the particular choice of identification of the matter density term in equation (\ref{h2zAj}).

\par The result obtained clearly shows that the best fit value of $j$ (chosen as a constant parameter) is very close to $-1$, which is consistent with a $\Lambda$CDM model. The interaction term $Q$, in a dimensionless representation, is very close to zero at the present era. This is completely consistent as $\Lambda$, being a constant, does not exchange energy with dark matter. Table \ref{tableQ0} shows the best fit values of $Q$ at $z=0$ for various combinations of data sets. It is easily seen that the values are two orders of magnitude smaller than $\Omega_{m0}$ and $\Omega_{DE0}$, which are approximately $0.3$ and $0.7$ respectively. All these quantities are expressed in a dimensionless way. So this comparison is possible.

\par As already mentioned, investigations regarding a reconstruction of interaction are not too many. But the very recent work by Yang, Guo and Cai\cite{yangguocai} is a rigorous and elaborate one. The method adopted is the Gaussian processes. Although the work is model dependent, as the equation of state parameter is not specified, it can be applied to a large variety of dark energy models. The $w$CDM model is particularly emphasized. The basic result is the same as that of the present work, the interaction appears to be negligible and consistent with the $\Lambda$CDM model at $z=0$.

\par An intriguing feature in both the present work and that in ref \cite{yangguocai}, is that although the best fit value still hovers around being negligible, it is allowed to have a non-trivial value for higher $z$ even in the 1$\sigma$ confidence region. So the interaction, if any, took place in the earlier epoch. The physics of this is not yet quite understood.

\par Another interesting result in the present work is the fact that $Q$, if it has a sizable value, it can be both positive or negative, so the pumping of energy is possible both ways. Intuitively it might appear that the dark energy should grow at the expense of dark matter ($Q<0$). However, the thermodynamic considerations demand that the flow of energy should be the other way round, from dark energy to dark matter\cite{pavonwang}.

\par It  has already been mentioned that the reconstructed model mimics the $\Lambda$CDM for the value of cosmological jerk parameter $j=-1$ and prevent the possibility of interaction between dark energy and dark matter. Any observational measurement which is based on the fiducial assumption of a $\Lambda$CDM cosmology, might affects the results of statistical analysis by making the parameter values highly biased towards the corresponding $\Lambda$CDM values and leading to far too optimistic error bars. Hence such kind of data, like the CMB distance prior measurement, has not been introduced directly in the likelihood analysis. The correlations of distance modulus measurement of type Ia supernova have been taken into account as it might  have its signature on the results. The error bars of dark energy equation of state parameter ($w_{DE}$) are found to be quite consistent with the results of Planck 2015 \cite{planck2015}.

\par The recent works on the reconstruction of jerk show that definitely a $\Lambda$CDM is favoured\cite{zhai, mukban}, where $j$ was allowed to be a function of $z$. Now a reconstruction of interaction through a constant $j$ also indicates towards a similar result.

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Foo Fighters Radio Is Coming To Triple M
This is call for all the Foo Fighter fans across the land! To celebrate the band's eighth number one album in Australia they will be taking over the airwaves every Friday night on Triple M from 19th March through to 23rd April.
Dave Grohl, Taylor Hawkins, Nate Mendel, Chris Shiflett, Pat Smear and Rami Jafee will Breakout and play their favourite songs and share stories from their time on the road touring like only the Foos can.
Head of Triple M Music, Mickey Maher, said: "No band fits hand in Triple M's glove more than the Foo Fighters. To have the band host these one-off, personally curated shows, exclusive to listeners across our network, is very exciting. Obviously COVID is limiting their chance to grace our shores but with their eighth number one album in Australia we are thrilled they want to do something like this to celebrate with their Aussie fans. Who are we to turn them down!"
Each week a different member of the Foo Fighters will take over Triple M with their own radio show and music fans will learn who from the band digs the music of Jane's Addiction, Van Halen, Queen, The Rolling Stones, AC/DC, Phil Collins, Alice Cooper and Jack White to name a few.
The Generator will kick over every Friday night from 19 March for Foo Fighters Radio after the footy across Triple M's enviable 49 stations across the country. Check local guides for exact times.
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text:
package org.springframework.beans.propertyeditors;

import junit.framework.TestCase;

import java.beans.PropertyEditor;

/**
 * Unit tests for the {@link CharArrayPropertyEditor} class.
 *
 * @author Rick Evans
 */
public final class CharArrayPropertyEditorTests extends TestCase {

	public void testSunnyDaySetAsText() throws Exception {
		final String text = "Hideous towns make me throw... up";

		PropertyEditor charEditor = new CharArrayPropertyEditor();
		charEditor.setAsText(text);

		Object value = charEditor.getValue();
		assertNotNull(value);
		assertTrue(value instanceof char[]);
		char[] chars = (char[]) value;
		for (int i = 0; i < text.length(); ++i) {
			assertEquals("char[] differs at index '" + i + "'", text.charAt(i), chars[i]);
		}
		assertEquals(text, charEditor.getAsText());
	}

	public void testGetAsTextReturnsEmptyStringIfValueIsNull() throws Exception {
		PropertyEditor charEditor = new CharArrayPropertyEditor();
		assertEquals("", charEditor.getAsText());

		charEditor.setAsText(null);
		assertEquals("", charEditor.getAsText());
	}

}


Xian, the capital of Shaanxi province is famous for the terracotta warriors, its city walls, and the large wild goose pagoda. It is not only the birthplace of Chinese Nationality, but also the important human birthplace and one of the prehistoric culture centers in Asia. Xi'an is located in the guanzhong Basin of the middle section of Yellow River Valley in the center area of mainland China. Tourism has been an important component of the local economy, and the Xi'an region is one of China's most popular tourist destinations.
Asia travel ideas brings this exotic city to you and provide information on culture, history and places of attraction. Idea travel also provides information on vacation rentals.
Over a period of more than 2000 years, Xi'an was the capital for eleven dynasties. Along with Rome and Constantinople, this city was a world leader in culture and trade and played a vital role in bridging the gap between east and west. This city contains very beautifuk places which are major tourist attraction like Famen Temple which contains Buddha's fingers. Xi'an is an important industrial and manufacturing center. The city has set up a number of fairly large wholesale markets and trade centers. Among those there are 33 wholesale markets of every type of meat, non-staple food, vegetables, general merchandise, clothing, hardware and chemical industry products, etc.
Some historical sites of this city are Mausoleum of Qin Shi Huang and his Terracotta Army, the tombs of the Zhou Dynasty kings located in the city, Xi'an also contains some 800 royal mausoleums and tombs from the Han Dynasty.