eSports has gained massive momentum in the past few years. Games like Overwatch and Fortnite lead the way for gamers to compete in an online competition. They also carry lifelong friendship and/or rivalry for a chance to gain achievements, prizes and more. You'd think that eSports would slow down. Oh no, it's just getting started. Almost every game besides the ones mentioned has an eSports league, and some are doing this at a national level. Renegade Rules #1 combines the thrill of eSports with the power of friendship sprinkled with some unapologetically relatable and queer characters to tell a story that's out of this world and charming to boot.
Ben Kahn and Rachel Silverstein grant readers with a brilliant, driven solid first issue that really stand out. It establishes so much of the primary dynamic in the issue, not leaving anything behind, but also not giving too much away. It forms the already in process friendship between the girls, gaming highlights and dating opportunities and crushes alike. They construct some of the personal challenges behind the scenes as well. Renegade Rule commands you at full attention once you open up the comic and that vibe lingers until you're done with the final page.
Something to note about Renegade Rule is how original and realistic it feels. When reading it for the first time, I thought about it a lot afterward. It felt all too familiar to me. Kahn and Silverstein nail every aspect of being a gamer in and out of the game. They also nail (most importantly) what a solid friendship looks and sounds like within their dialogue and direction.
With that said, one of the biggest things that drive this comic are the characters themselves. Kahn and Silverstein nail how beautifully each character is in their friendship but also how they shine individually as well. Each of them is a budding star within the comic with Amanda Cassidy as their leader. Jessie Nakamura. Tonya LaFleur, Sasha Zimmerman (my favorite with the best name) and Amanda share such exciting vibes between them with gaming to unite them. The queer vibe to characters feels so much a part of them. Kahn and Silverstein make this such a secondary but strong impression of who they are. It allows it to blend into the story so naturally and it left me completely shook how familiar it felt.
The thing that drew me into Renegade Rule from first glance was Sam Beck's art. Diving into the comic, it exceeded my expectations tenfold. Kahn and Silverstein excel in giving the voice, action, and personality to the characters. Beck doubled down on their excellence. She provides each of the characters their unique look, more personality, making them feel like your best friends instead of strangers. Your eyes are caught lingering on specific features between each of the characters.
Beck provides aesthetically pleasing online and offline looks. She also creates action-packed, out of this world backgrounds in the game and endearing and real down to earth settings off. Beck also does a phenomenal job with her colors as well. She brings pastel colors to lively sci-fi world, but pairs it up with muted neon colors within the real world setting.
There's something all too familiar with Renegade Rule that gamers and non-gamers alike can love equally. With dope likable characters, and storytelling that's incredibly down-to-earth, Renegade Rule is just scratching the surface of the marvel it can and will be. Renegade Rule is now available on Ben Kahn's Etsy. Don't hesitate to pick up Renegade Rule #1 today.
Looking for our favorite books this week? Head over to the NCBD section and find out. But if you want to support indie creators too have a look at the 5 comic Kickstarters you should be backing this week. And as always stay up to date on all comic news right here.


Author(s): Beijnum, J. van; Worp, H.B. van der; Algra, A.; Vandertop, W.P.; Berg, R. van den; Brouwer, P.A.; Sprenkel, J.W. van der; Kappelle, L.J.; Rinkel, G.J.; Klijn, C.J.
BACKGROUND AND PURPOSE: It is uncertain whether familial occurrence of brain arteriovenous malformations (BAVMs) represents coincidental aggregation or a shared familial risk factor. We aimed to compare the prevalence of BAVMs in first-degree relatives (FDRs) of patients with BAVM and the prevalence in the general population. METHODS: We sent a postal questionnaire to 682 patients diagnosed with a BAVM in 1 of 4 university hospitals to retrieve information about the occurrence of BAVMs among their FDRs. We calculated a prevalence ratio using the BAVM prevalence among FDRs and the prevalence from a Scottish population-based study (93 per 628 788 adults). A prevalence ratio of >/=9 with a lower limit of the 95% confidence interval of 3 was considered indicative of a shared familial risk factor. RESULTS: Informed consent was given by 460 (67%) patients, who had 2992 FDRs. We identified 3 patients with a FDR with a BAVM, yielding a prevalence ratio of 6.8 (95% CI, 2.2-21). CONCLUSIONS: The prevalence of BAVMs in FDRs of patients with a BAVM was increased but did not meet our prespecified criterion for a shared familial risk factor. In combination with the low absolute risk of a BAVM in FDRs, our results do not support screening of FDRs for BAVMs.


You are here: Home » Too Much Foam. Too Little Guinness: Accelerator Shakeout On The Horizon?
I have an ominous feeling of deja vu. But it may not be all bad. The "accelerator" business appears to be at a strategic inflection point. The indicators are increasingly pointing to the need for a rethink.
In 1849, thousands of aspiring gold miners arrived by ship at San Francisco. Very quickly, enterprising citizens in San Francisco set about selling premium priced shovels and mining pans to the fortune hunters, as they set off for the Sierra foothills. Even the crews jumped ship and headed for the hills, leaving their ships to rot into San Francisco Bay, until 150 years later the San Francisco Giants spectacular new AT&T Park was built on top of the old shipwrecks. Very few of those original "49'ers" hit pay dirt. Most lost their shirts.
Having been in the entrepreneurship business for many years in Silicon Valley, the current entrepreneurship industry environment feels more like the 49'ers bubble than did the 2001 Internet bubble. In that period, I was bemused by all the "dumb money," and the experience of breakfast at Buck's in Woodside, or Il Fornaio in downtown Palo Alto, both packed with VC's and wannabe entrepreneur's. The voices were muted to avoid being overheard, and the wine flowed freely. This time it is worse. There is no Il Fornaio. There is no money. It is more like an industrial ghetto out there. Erin Griffiths' PandoDaily December 3rd post (URL above) "We know accelerators are headed for a shakeout-but do they?," adds additional evidence to my earlier November 18th post on the depressing state of the app development industry and the dearth of Big Ideas. The new "49'er " is the Web entrepreneur.
This does not appear to be specific to any particular location or geography. It's happening in New York, Boulder, Austin, as well as here at home. It's everywhere. Investors' are openly bemoaning that there are too many accelerators cranking out too many mediocre ideas. It used to be that bad ideas died quick deaths in the Colosseum of competition. Erin's description of a typical company's "demo day" fiasco was painful to read, but so dead on the mark. I have seen it a hundred times. Some of the problem stems from the lack of meaningful accelerator performance metrics. Some of it stems from a lack of will to enforce "up or out" rules.
So seeing the writing on the wall, Y Combinator, most often ahead of the curve, is scaling back significantly without prompting from any source or market force.
There may be a silver lining in some hopeful signs. Communities that are focusing like a laser on their local economic environment, and working to enhance their core competencies, encouraging entrepreneurs in those niches, are winning. Those lost in the froth of trying to reinvent Silicon Valley are increasingly losing.
Too much foam. Too little Guinness.


If you are in the market for a Pre-Owned Boat or a Pontoon come in to South Austin Marine. We have a large selection of used marine craft in many brands and classes at both our locations. Our expert staff can point you in the right direction so stop by one of our two locations in South Austin, TX today!
Length Overall 42 ft. 0 in.


Unique animal jigsaw puzzles with colourful and vibrant illustrations that MOVE while you complete the puzzles!
4 levels of difficulty to match the skill level of your child, plus one hidden one!
Animated pictures are a new of experiencing a jigsaw puzzle, it's so much fun!
This excellent puzzle app inspires your child with a unique new way to complete jigsaw puzzles!
Once the puzzle is complete you can click on the animal picture to see it move for added delight!
Unlock the 12 animal puzzles one by one on each difficulty level. The puzzle pieces are ANIMATED as as you are placing them you see them moving, it's fun to try and 'pin them down' to the right place!
The difficulty levels range from 4, 9, 12 and 20 pieces. The puzzles really are quite challenging on the higher levels.
This is really a new way to complete jigsaws and uses iPad technology beautifully.
The illustrations are exquisitely crafted as I have found with all Kidoteca Apps so far! Well done developers!
The names of the animals are available in 10 different languages, both written and spoken. No reading required.
Toddler touch and watch app that is beautiful, creative and totally fun!


text:
package com.googlecode.pondskum.gui.swing.notifyer;

import java.awt.Dimension;
import java.awt.Graphics;
import java.awt.font.LineMetrics;

public final class LocationFinder {

    private static final int PADDING = 10;

    private LocationFinder() {
        //Utility
    }

    public static Dimension findRightCorner(final Graphics g, final String text, final Dimension parentSize) {
        FontedTextDimension textDimension = getTextDimensions(g, text);
        float x = Math.max(0, (parentSize.width - (textDimension.getWidth() + PADDING))); //leave a little space @ the border
        float y = Math.max(0, (parentSize.height + textDimension.getHeight()) / 2 - textDimension.getDescent());
        return new Dimension((int) x, (int) y);
    }

    public static Dimension findLeftCorner(final Graphics g, final String text, final Dimension parentSize) {
        FontedTextDimension textDimension = getTextDimensions(g, text);
        float x = PADDING;
        float y = Math.max(0, (parentSize.height + textDimension.getHeight()) / 2 - textDimension.getDescent());
        return new Dimension((int) x, (int) y);
    }

    public static Dimension findCentreLocation(final Graphics g, final String text, final Dimension parentSize) {
        FontedTextDimension textDimension = getTextDimensions(g, text);
        float x = Math.max(0, (parentSize.width - textDimension.getWidth()) / 2);
        float y = Math.max(0, (parentSize.height + textDimension.getHeight()) / 2 - textDimension.getDescent());
        return new Dimension((int) x, (int) y);
    }

    public static FontedTextDimension getTextDimensions(final Graphics g, final String text) {
        float width = (float) g.getFontMetrics().getStringBounds(text, g).getWidth();
        LineMetrics lm = g.getFontMetrics().getLineMetrics(text, g);
        float ascent = lm.getAscent();
        float descent = lm.getDescent();
        float height = ascent + descent;
        return new FontedTextDimensionBuilder().withHeight(height).withWidth(width).withAscent(ascent).withDescent(descent).build();
    }

}

redpajama_set_name: RedPajamaGithub


Please don't forget to check the lost and found at school this week. After this week, all sweatshirts will be donated to the Avon Middle School 1,000 Sweatshirts Campaign. Thank you!
When you clean out your closets, how many extra sweatshirts do you pull out that don't fit, or you just don't like anymore? Instead of having them lying around on your bedroom floors or throwing them out, please consider donating them to people in need.
We are a group of 7th grade students at Avon Middle School, and we are trying to collect 1,000 sweatshirts to donate to local charities and homeless shelters. Our idea is that many families in our community have "at least one" sweatshirt they no longer wear or need.
From now through February 7th, you can give or drop off sweatshirts to our committee members' houses. On Saturday, February 7th, please help us with our final push to reach our goal of 1,000 sweatshirts by dropping them off at Hartford Hospital's Helen & Harry Gray Cancer Center (80 Fisher Drive, Avon) from 10am-4pm.
All sweatshirts will be donated to the Hartford Boys and Girls Club, The Village for Families and Children, Gifts of Love, and local homeless shelters. They will give the sweatshirts to people who need help keeping warm the rest of the winter season. Our only requirement is that the sweatshirts are GENTLY USED and CLEAN. Please join us in helping to keep our community warm for the rest of the cold winter.


My husband accompanied our son to school. I stayed home to clean up the mess in the morning and arranged the shop for internet users. That's my morning routine every school days.
Before I do anything, I make sure that my Spotify music is on. I love music in different categories, depending on my mood. Because it is the morning, I browse for a guitar music on a prs 7 string. It might be weird for some people. This type of music makes me jump to start my work.


Next let's look how to delay our workflow actions. Or, go back and review our post on configuring Workflow Actions.
All the Actions above can fire instantly, or you can have them wait for a period of time before they fire. To setup a delay in the workflow action, click the "Add Time Trigger" button.
The next screen asks you to set the length of the delay in hours and days. Minutes is not available and even when you select hour, it can be anytime during that hour depending on what Saleforce is dealing with at that time. Don't expect the workflow to fire a 1PM sharp!
After that you create your Actions as you did in the Immediate Action section.
NOTE: One workflow rule can have multiple immediate actions and time delayed actions.
In the screen to the left you will need to specify which object you want to monitor (Leads, Opportunities, etc).
Workflow WILL NOT fire another workflow rule. You can not specify the order in which workflow fires. For example if workflow rule number one updates a field with the value "X," and workflow rule number two is monitoring the same field for a value of "X," the second workflow rule will not fire.


Appelgren Exclusive AR combines lightness with the unbelievable feel of an allround blade. This blade is highly recommended for allround players who value control when blocking but especially wish to incorporate variations of spin into their play. Donic's "exclusive" blade series at unbeatable value.
The specially selected ply combinations provide these competition blades with increased control and smooth playing characteristics. These blades are available in three speeds to suit different types of players.


There is nothing so beautiful as autumn in New England. Enjoy a relaxing ride through the country roads and byways awash with the color splashes of the season. A full-day of unforgettable scenic views and things to do awaits you.
Contact the tour office at +1 (617) 720-6342 to arrange hotel pick-up from selected properties.
Venture out of the city for a relaxing day in New Hampshire's gently rolling countryside for an exhibit of Mother Nature's handiwork. Foliage season in the Northeast is like none other as the sunny days and crisp nights cause the hardwood trees to change their color palate to blazing yellows, golds, reds and magentas. Add to the scenery, the quaint colonial homes, white church steeples, weathered roadside taverns and village greens for unforgettable memories to take back home.
Stretch your legs and warm your hands with a quick coffee and snack stop in the morning. Picture stops at the old-fashioned covered bridge and the state forest precede a wonderful buffet luncheon at the Woodbound Inn (included).
Continuing on the journey, the last stop of the day will be at Brookdale Farm for baked treats, apples and complimentary cider. Come along and don't forget your camera.
Mass Transportation Bldg, City Place, 8 Park Plaza, Boston, MA 02116.


text:
'Bachelor in Paradise' blues? Indiana native Jenna Cooper and Jordan Kimball may be splitting
Jenna Cooper's engagement was announced Tuesday on "Bachelor in Paradise." But now her fiance, Jordan Kimball, says they're breaking up.
'Bachelor in Paradise' blues? Indiana native Jenna Cooper and Jordan Kimball may be splitting Jenna Cooper's engagement was announced Tuesday on "Bachelor in Paradise." But now her fiance, Jordan Kimball, says they're breaking up. Check out this story on IndyStar.com: https://indy.st/2CPKtQ3
Dwight Adams, Indianapolis Star Published 5:49 p.m. ET Sept. 12, 2018 | Updated 10:34 a.m. ET Sept. 13, 2018
Jenna Cooper is an Indiana native and cast member on this season of "Bachelor in Paradise."(Photo: Provided by Jenna Cooper)
Talk about a summer romance… made for TV.
Tuesday night on "Bachelor in Paradise," Indiana native Jenna Cooper's engagement to Jordan Kimball was officially announced on national television.
But on Wednesday, she's facing a very-public breakup,USA TODAY reported.
The reason? The same cause that dooms many other relationships on-air or off.
Accusations of cheating.
Jenna Cooper: How this small-town Indiana native became a 'Bachelor' fan favorite
They were born in a small town: Meet 48 famous (or otherwise interesting) Hoosiers
Kimball had actually proposed to Cooper earlier this year in Mexico. But the announcement of the engagement had to wait until the season finale Tuesday.
Cooper told IndyStar last week that "Bachelor in Paradise" fans should prepare for a few happy endings during the show's two-part season finale airing Monday and Tuesday.
"Your love has made me feel alive again," Cooper told Kimball in the first hour of Tuesday's final episode. "And I can't wait to spend the rest of my life with you."
Cooper, 29, lives in Raleigh, North Carolina. But she was born in Indianapolis, and spent her formative years in a couple of small, Grant County towns.
Now, Kimball is saying his relationship with Cooper is over, after a report alleging that Cooper may have cheated on him and faked her relationship for monetary gain.
Reality Steve calls Cooper a fraud
Prior to Tuesday's show, Reality Steve published a report that included screenshots of a texting conversation Cooper allegedly had with another man.
"Me and Jordan aren't together for real. I don't even like him let alone love him. I'm better than him and once I'm able to I'll break it off for good and make up some story to make him look bad if it'll make you feel better. He means nothing to me and never has."
In a statement to People magazine on Wednesday, Cooper said the allegations are false.
"I am aware of the allegations being made against me and they are simply untrue. I am choosing to focus on my relationship right now. Thank you for respecting my privacy at this time."
Kimball 'cannot take a chance' with his heart
However, Kimball appears to have had enough of the drama.
He reportedly told Entertainment Weekly that while he doesn't know whether Cooper's alleged texts are true, he "cannot take a chance" with his heart and has decided to walk away.
"I'm removing myself from the relationship with intentions to take care of myself and find my happiness. I will not lash out, I will not try to convince people that she is a bad person. You will not see me pursue any kind of vengeance on her. I care about Jenna. Everyone saw me fall at first sight for her and I will never deny that. Just because this has happened does not mean that I will discount how I felt for her. I will not try to play it off that it doesn't hurt. I would be doing the love that I felt for her an injustice if I were to say that I didn't feel strongly about this."
Though Cooper has told him that the text messages are fake, Kimball says he does not want to remain "in limbo" by staying in the relationship. "I just can't wait and hold on to see if this is fake. I allowed myself to be played, but I will not allow myself to be fooled by this. If this turns out to be fake, then hey, it's a good thing that I didn't lash out at her," he says. "But I cannot take a chance with my heart."
To think, to feel, to fall. These emotions interact with experiences and people, when you find a person you think about them, you feel when they feel and sometimes you fall. When you're in love with even the experiences you've had with them it's something to respect. Being careless with someone that you give your heart to and reach milestones with isn't sensible no matter what the terms may be. I have not had an easy life and having struggles allows me to grab onto tough times and discard them from my path. I deal with unreasonable circumstances reasonably and have come to terms with a decision to remove myself from the relationship, it breaks my heart to think, feel and fall for this. It's dropped me. Fumbling emotions and being understanding is not easy. I'll be taking time to pursue my inner peace and she will always have me to talk to, if you've reached out to me, allow me time. Thank you to those that have.
A post shared by Jordan Kimball (@jordan__kimball) on Sep 12, 2018 at 11:25am PDT
Not a first for 'Bachelor' breakups
This isn't the first time an Indiana native has played a prominent role in a reality TV dating show — or an eventual, very-public breakup.
Remember Ben Higgins, the software salesman from Warsaw, Indiana?
"The Bachelor" star Ben Higgins and ex-fiancee Lauren Bushnell at the 66th men's Little 500, at Indiana University on April 16, 2016. (Photo: Jenna Watson/IndyStar)
In 2016, Higgins stole quite a few hearts on the 20th season of ABC's "The Bachelor."
But his televised romance with fiancée Lauren Bushnell also hit the skids in May 2017.
IndyStar reporter Justin Mack and digital producer Chris Sims contributed to this story. Call IndyStar digital producer Dwight Adams at 317-444-6532. Follow him on Twitter: @hdwightadams.
Other stories of interest:
What we know: NFL players kneeling in protest during the anthem has divided the nation
Wheelman: Reggie Miller has found a new hobby: Mountain biking for charity
Read or Share this story: https://indy.st/2CPKtQ3

redpajama_set_name: RedPajamaCommonCrawl


text:
\section{Introduction}

Gamma-ray Bursts (GRBs) are short, intense gamma-ray flashes that are by far the most violent explosions in the universe \citep{2006RPPh...69.2259M,2007ChJAA...7....1Z,2009ARA&A..47..567G,2015PhR...561....1K}. A lot of researches have shown that GRBs can be divided into two categories, the long Gamma-ray bursts (LGRB) with duration $\rm T_{90} > 2s$ and the short Gamma-ray bursts (SGRB) with $\rm T_{90} \leq 2s$ \citep{1993ApJ...413L.101K}. For different kinds of GRBs, their origins are also different. The progenitors of LGRBs are regarded as collapsed massive stars \citep{1993ApJ...405..273W}, while SGRBs are related to the coalescence of compact objects such as binary neutron stars or neutron star-black holes \citep{2007PhR...442..166N,2017PhRvL.119p1101A,2017ApJ...848L..14G,2017ApJ...848..115H}.

A variety of correlations between observable GRB properties have been proposed in the literatures, and they can be classified into prompt correlations, afterglow correlations and prompt-afterglow correlations based on the episode in which the observables are measured \citep{2017NewAR..77...23D,2018PASP..130e1001D}. Among the prompt correlations, the so-called ``Amati relation'' \citep{2002AA...390...81A} has been widely discussed. It describes a relation between the isotropic-equivalent energy ($E_{\rm iso}$) and the rest-frame peak energy ($E_{\rm peak}$) of the $\gamma$-ray spectrum. Another commonly cited relation is the ``Yonetoku relation'' \citep{2003MNRAS.345..743W,2004ApJ...609..935Y}, which demonstrates the connection between $E_{\rm peak}$ and the isotropic–equivalent luminosity ($L_{\rm iso}$). The interpretation of these relations are still under debate \citep{2006ApJ...645L.113C,2006MNRAS.372.1699G}, and it is noteworthy that though the Amati relation and Yonetoku relation exist in both LGRBs and SGRBs, the best-fit parameters of the two relations are very likey to be different for the two GRB categories \citep{2012ApJ...750...88Z}. Since LGRBs and SGRBs are thought to have different origins but may share similar jet launching and radiation mechanisms, the correlations may help to discriminate among different models.

The prompt correlations related to the intrinsic energy/luminosity can serve as distance indicators, hence can help to study the luminosity function and redshift distribution of GRBs \citep{2002AA...390...81A,2003A&A...407L...1A,2004ApJ...612L.101D,2004ApJ...609..935Y,2005ApJ...633..611L,2014ApJ...789...65Y,2018ApJ...852....1Z,2018AdAst2018E...1D,2019gbcc.book.....D}. However the large dispersion, which is about an order of magnitude for both Amati relation and  Yonetoku relation brings extra uncertainties on such studies, hence finding new correlations as redshift/distance indicators is more important and challenging.

Inspired by the $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ relation for long GRBs found by \citet{2006MNRAS.370..185F}, here we manage to find a universal correlation for both LGRBs and SGRBs using the prompt emission properties $E_{\rm iso}$, $L_{\rm iso}$, $E_{\rm peak}$ and $T_{0.45}$. This paper is arranged as follows. In Section \ref{data}, we describe the selection of GRB samples; in Section \ref{correlations} we analyze the reliability of some potential correlations, and report the discovery of a universal correlation; in Section \ref{application}, the application of the universal correlation on the study of SGRB's luminosity function and formation rate is presented; finally, we give conclusions and discussion in Section \ref{SD}.

\section{Sample Selections}\label{data}

In order to reduce the uncertainties in the correlation study, we require a careful selection on the GRBs samples. For the purpose of this work, we only include samples with the following information:
\begin{enumerate}
    \item the redshit z.
    \item the peak flux P and the peak fluence F.
    \item the peak energy $E_{\rm peak}^{\rm obs}$ in the observer's frame. And we take $E_{\rm peak} \equiv (1+z)E_{\rm peak}^{\rm obs}$ as the cosmological rest-frame $\nu f_\nu$ spectrum peak energy (in brief, the rest-frame peak energy).
    \item low-energy power-law index $\alpha$ and high-energy power-law index $\beta$ of Band fuction \citep{1993ApJ...413..281B}.
    \item $T_{0.45}^{\rm obs}$, and we take $T_{0.45} \equiv T_{0.45}^{\rm obs}/(1+z)$.
\end{enumerate}

One uncertainty for calculating a burst's intrinsic energy/luminosity comes from the assumed spectrum in the integration, so the 4th criterion above is to ensure we use a unified spectral form to evaluate $E_{\rm iso}$ and $L_{\rm iso}$, and the most energetic part of the emission is within the observed frequency band. As a consequence, all of our samples are reported to be best fitted with the Band function:
\begin{equation}
  \mathop N\nolimits_{{\rm{band}}}  = \left\{ {\begin{array}{*{20}{c}}
  {A{{\left( {E/100} \right)}^\alpha }\exp \left( { - E\left( {2 + \alpha } \right)/{E_{{\rm{peak}}}}} \right)}&{{\rm{if\ }}E < {E_{\rm{b}}}}\\
  {A{{\left\{ {\left( {\alpha  - \beta } \right){E_{{\rm{peak}}}}/\left[ {100\left( {2 + \alpha } \right)} \right]} \right\}}^{\left( {\alpha  - \beta } \right)}}\exp \left( {\beta  - \alpha } \right){{\left( {E/100} \right)}^\beta }}&{{\rm{if\ }}E \ge {E_{\rm{b}}}}
\end{array}} \right.
\end{equation}
where ${E_{\rm{b}}} = ({\alpha  - \beta }){E_{{\rm{peak}}}}/( {2 + \alpha })$. Finally, after applying all the selection criteria, our sample includes 49 LGRBs and 19 SGRBs. In Table \ref{tab:1} we list the information of the 49 LGRBs, and the information of the selected SGRBs are listed in Table \ref{tab:2}. In our following analysis we also include the 20 LGRB samples in \citet{2006MNRAS.370..185F}.

In order to eliminate the influence of different observational energy bands on the calculating results, we make K-correction \citep{2001AJ....121.2879B} in the calculation of bursts' isotropic-equivalent luminosity/energy:
\begin{equation}\label{liso}
L_{\rm iso} = 4\pi D_{\rm L}^2(z)PK
\end{equation}
\begin{equation}
d_{\rm L}(z)=\frac{c}{H_0}\int_{0}^{z}\frac{dz}{\sqrt{1-\Omega_{\rm m}+\Omega_{\rm m}(1+z)^3 }}
\end{equation}
\begin{equation}
K=\frac{\int_{1KeV}^{10^4KeV}Ef(E)dE}{\int_{E_{\rm
 min}(1+z)}^{E_{\rm max}(1+z)}Ef(E)dE}
\end{equation}
where $P$ is the peak flux observed between a certain energy range $(E_{\rm min},E_{\rm max})$ in the unit of $\rm erg/cm^2/s$ (For $E_{\rm iso}$, $P$ is replaced by the Fluence $F$ in Eq.(\ref{liso})). We assume a flat $\Lambda$ cold dark matter universe with $\Omega_{\rm m}=0.27$ and $H_0=70\ \rm{km\ s^{-1}Mpc^{-1}}$ in the calculation.

\section{Study on The Correlations}\label{correlations}
\subsection{The $E_{\rm iso}-E_{\rm peak}$ and $L_{\rm iso}-E_{\rm peak}$ Correlations}

In previous studies, a plenty of works about LGRB's prompt correlations were carried out. For SGRBs, however, such studies are much less due to the number of SGRBs with konwn redshifts are very small. Nevertheless, several studies have shown that for SGRBs they may follow a different $E_{\rm iso}-E_{\rm peak}$ relation with respect to LGRBs, while the $L_{\rm iso}-E_{\rm peak}$ relation may be similar to that of  LGRBs \citep{2012ApJ...755...55Z,2013MNRAS.430..163Q,2012ApJ...755...55Z,2014ApJ...789...65Y,2014PASJ...66...42T}. In the following we will test these correlations with our samples (49 LGRBs and 19 SGRBs together with 20 LGRBs in Firmani et al. (2006)).

Here we constructed a likelihood function \citep{ 2006ApJ...653.1049W,2007ApJ...665.1489K} to fit the data. It can be defined as:
\begin{equation}\label{the_L}
\L(a_{j},b|x_{j},y)=\prod_{i}\frac{1}{\sqrt{2\pi(\sigma_{yi}^2+\sum_{j}(a_{j}\sigma_{xji})^2)}}exp({-\frac{1}{2}\frac{(y_{i}-b-\sum_{j}a_{i}x_{ji})^2}{\sigma_{yi}^2+\sum_{j}(a_{j}\sigma_{xji})^2}})
\end{equation}
where $y_i$ and $x_{ji}$ are the $E_{\rm peak}$ and $E_{\rm iso}$(or $L_{\rm iso}$) of GRB samples, $\sigma_{yi}$ and $\sigma_{xji}$ are their measurement errors. As shown by \citet{2002ApJ...574..740T} and \citet{2006ApJ...653.1049W}, the above likelihood function can be expressed as:
\begin{equation}\label{the_log(L)}
\log[L(a_{j},b|x_{j},y)]=- \sum_{i}\frac{(y_i-b-\sum_{j}a_{j}x_{ji})^2}{\sigma_{yi}^2+\sum_{j}(a_{j}\sigma_{xji})^2}+constant=-\chi^2+constant
\end{equation}
where $\chi^2$ is merit function \citep{1992nrca.book.....P,2003MNRAS.345.1057M,2006A&A...456..439K}. We determine the values of the parameters and their confidence intervals by performing Bayesian estimation based on the likelihood constructed above, we set uniform priors for all parameters. The results are presented in Fig.\ref{fig:fit1}. Obviously, the SGRB samples show systematically bias against the best-fit curve (see Section \ref{corrlation} for more details), thus it is inadequate to fit both LGRB and SGRB samples with a single relation on $E_{\rm iso}-E_{\rm peak}$ or $L_{\rm iso}-E_{\rm peak}$ plane.

\begin{figure}[ht!]
	\figurenum{1}\label{fig:fit1}
	\centering
	\includegraphics[angle=0,scale=0.4]{fig1a.png}
	\includegraphics[angle=0,scale=0.4]{fig1b.png}
	\caption{The $E_{\rm iso}-E_{\rm peak}$ and $L_{\rm iso}-E_{\rm peak}$ for LGRBs and SGRBs, the blue hollow points is the data for LGRBs in table 1, the red solid points is the data for LGRBs in \citet{2006MNRAS.370..185F} , the green solid points is the data for SGRBs in table 2. The solid line is the best-fit line for LGRBs and SGRBs. The Spearman's rank correlation coefficients are P= 0.71 and P= 0.46 for left and right, respectively.}
	\hfill
\end{figure}

\subsection{Discovery of a Universal Three-Parameter Correlation}\label{corrlation}

\citet{2006MNRAS.370..185F} found a correlation between $L_{\rm iso}$, $E_{\rm peak}$ and $T_{0.45}$ of LGRBs. Inspired by their work, and benefit from the accumulating number of SGRBs with know redshifts these years, we may be able to clarify whether both the SGRBs and LGRBs have the same three-parameter correlation. In the following we discuss both $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ and $E_{\rm iso}-E_{\rm peak}-T_{0.45}$ relations.

Considering the relations have the form of $L_{\rm iso} \propto E_{\rm peak}^{p1} T_{0.45}^{p2}$ ($E_{\rm iso} \propto E_{\rm peak}^{p1} T_{0.45}^{p2}$), and using the statistics defined by Eq.(\ref{the_log(L)}), we derive the best-fit correlation:
\begin{equation}\label{the_relation}
L_{\rm iso} \propto E_{\rm peak}^{1.94 \pm 0.06} T_{0.45}^{0.37 \pm 0.11}
\end{equation}
\begin{equation}
E_{\rm iso} \propto E_{\rm peak}^{1.68 \pm 0.09} T_{0.45}^{1.09 \pm 0.13}
\end{equation}
Where the errors are reported in 1 $\sigma$ confidence level. The results are shown in Fig.\ref{fig:fit2} together with their $3\sigma$ intervals.

\begin{figure}[ht!]
	\figurenum{2}\label{fig:fit2}
	\centering
	\includegraphics[angle=0,scale=0.4]{fig2a.png}
	\includegraphics[angle=0,scale=0.4]{fig2b.png}
	\caption{The three-parameter relations for LGRBs and SGRBs, the blue hollow points is the data for LGRBs in table 1, the red solid points is the data for LGRBs in \citet{2006MNRAS.370..185F}, the green solid points is the data for SGRBs in table 2. The solid line is the best fit line. The dotted lines represent  the 3$\sigma$ confidence bands. The Spearman's rank correlation coefficients are P= 0.81 and P= 0.78 for left and right, respectively.}
	\hfill
\end{figure}

We quantitatively discuss the reliability of the relations above (i.e., $E_{\rm iso}-E_{\rm peak}$, $L_{\rm iso}-E_{\rm peak}$, $E_{\rm iso}-E_{\rm peak}-T_{0.45}$ and $L_{\rm iso}-E_{\rm peak}-T_{0.45}$) in two aspects. First, by using the Anderson-Darling test, we find that the residuals of the data points with respect to the best-fit line can be fitted with a Gaussian function. The residuals of each fit are plotted in Fig.\ref{fig:res}, and we fit the LGRB samples (blue) and SGRB samples (red) separately with Gaussian function. We find that in the $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ and $E_{\rm iso}-E_{\rm peak}-T_{0.45}$ fits, the mean values of the residuals of the two GRB categories are consistent with zero within the error range, and their standard deviation ($\sigma$) of LGRB and SGRB also consist with each other, indicating that in this two correlations the dispersions of LGRB and SGRB  are nearly the same. We further perform Student's t test on the residuals, the null hypothesis is that the mean values of the residuals of LGRBs and SGRBs are equal. We find that, given the significant level $a = 0.01$, only the residuals in the $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ fit pass the test, with $P=0.07$, while in other correlations, $P=0.009, 2\times 10^{-6}$ and $1.5\times10^{-11}$ for  $E_{\rm iso}-E_{\rm peak}-T_{0.45}$, $E_{\rm iso}-E_{\rm peak}$ and $L_{\rm iso}-E_{\rm peak}$ respectively. Second, the robustness of a relation can be reflected by the correlation coefficient, here we use the Spearman's rank correlation coefficient. For the correlations $L_{\rm iso}-E_{\rm peak}-T_{0.45}$, $E_{\rm iso}-E_{\rm peak}-T_{0.45}$, $L_{\rm iso}-E_{\rm peak}$ and $E_{\rm iso}-E_{\rm peak}$, the correlation coeffiicients are 0.81, 0.78, 0.71 and 0.47 respectively, which indicates that the $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ relation is tighter than any of other relations.
\begin{figure}[ht!]
	\figurenum{3}\label{fig:res}
	\centering
	\includegraphics[angle=0,scale=0.8]{fig3a.pdf}
	\includegraphics[angle=0,scale=0.8]{fig3b.pdf}
	\includegraphics[angle=0,scale=0.8]{fig3c.pdf}
	\includegraphics[angle=0,scale=0.8]{fig3d.pdf}
	\caption{Left: The graph at the top shows that scatter with gaussian distribution of LGRB and SGRB for $L_{\rm iso}-E_{\rm peak}$ relationship. The red part is the SGRBs' scatter with $\mu=-0.42$, $\sigma=0.21$, the blue part is the LGRBs' scatter with $\mu=0.01$, $\sigma=0.22$. The graph below shows that scatter of LGRB and SGRB for $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ relationship. The red part is the SGRBs' scatter with $\mu=0.06$, $\sigma=0.37$, the blue part is the LGRBs' scatter with $\mu=-0.12$, $\sigma=0.38$. Right: The graph at the top shows that scatter with gaussian distribution of LGRB and SGRB for $E_{\rm iso}-E_{\rm peak}$ relationship. The red part is the SGRBs' scatter with $\mu=-0.34$, $\sigma=0.30$, the blue part is the LGRBs' scatter with $\mu=0.08$, $\sigma=0.31$. The graph below shows that scatter of LGRB and SGRB for $E_{\rm iso}-E_{\rm peak}-T_{0.45}$ relationship. The red part is the SGRBs' scatter with $\mu=0.23$, $\sigma=0.46$, the blue part is the LGRBs' scatter with $\mu=-0.10$, $\sigma=0.47$.}
	\hfill
\end{figure}

Based on the analysis above, we conclude that LGRBs and SGRBs could follow a universal $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ correlation as shown in Eq.(\ref{the_relation}). We also compare this relation with the Yonetoku relation which using only SGRB samples and find that this relation is also slightly tighter than SGRB's Yonetoku relation, therefore the  $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ correlation can serve as a potential redshift indicator for SGRBs.

\section{Application on the Study of Luminosity Function and Formation Rate of SGRBs}\label{application}
\subsection{A New Redshift Indicator}

The $E_{\rm iso}-E_{\rm peak}$ and $L_{\rm iso}-E_{\rm peak}$ correlations were widely used to estimate the redshifts of GRBs \citep{2002AA...390...81A,2004ApJ...612L.101D,2004ApJ...609..935Y,2005ApJ...633..611L,2011MNRAS.418.2202D,2012int..workE.116A,2014ApJ...789...65Y,2018ApJ...852....1Z}. In order to apply the  $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ correlation to the estimation of the redshift of GRBs, we first need to discuss the accuracy of the redshift calculated from this correlation. In Fig.\ref{fig:redshift}, we present the pseudo-redshifts $z^*$ calculated by the $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ correlation versus the true observed redshift $z$ of our SGRB samples. By calculating the relative errors between pseudo-redshifts of SGRBs and observed redshifts, we find that the $68\%$ of our pseudo redshifts (i.e. 13 out of 19 sources) are within the $30\%$ of the real values. Then we perform the Kolmogorov–Smirnov test between them and find the chance probabilities of this is 0.74, which indicates that our estimated pseudo redshifts are reasonable. Then this encourages us to take a further step of using it in the study of Luminosity Function and Formation Rate of SGRBs.

\begin{figure}[ht!]
	\figurenum{4}\label{fig:redshift}
	\centering
	\includegraphics[angle=0,scale=0.9]{fig4.pdf}
	\caption{Comparison of real and pseudo-redshifts of 19 short GRBs. Y-axis is pseudo-redshifts, X-axis is real redshifts.}
	\hfill
\end{figure}

\subsection{Constraining the Luminosity Function and Formation Rate of SGRBs}

We use the $L_{\rm iso}-E_{\rm peak}-T_{0.45}$ correlation to determine redshifts of SGRBs.  Our samples are collected from the \textit{Swift} GRB catalog with known $T_{0.45}$, peak flux and $E_{\rm peak}$ (or Bayes $E_{\rm peak}$ \footnote{\url{http://butler.lab.asu.edu/Swift/bat_spec_table.html}}) but lack of redshift detection. There are 75 bursts satisfy this criterion. Together with the 19 short burst samples with known redshifts, we use a total number of 94 bursts to study the luminosity function of SGRBs.

The observed GRB distributions suffer from selection effects, which are dominated by the Malmquist bias caused by the limited sensitivity of instruments. We use Lynden-Bell's $c^-$ method, which has been widely used in the previous studies, to eliminate this effect \citep{1971MNRAS.155...95L,1992ApJ...399..345E,1993ApJ...402L..33P,1999ApJ...518...32M,2002ApJ...574..554L,2004ApJ...609..935Y,2014ApJ...789...65Y,2012MNRAS.423.2627W,2013ApJ...774..157D,2015ApJS..218...13Y,2015ApJ...800...31D,2016A&A...587A..40P, 2017ApJ...850..161T,2018ApJ...852....1Z}, The distribution of SGRB can be written as $\Psi(L,z)=\psi(L)\rho(z)$ \citep{1992ApJ...399..345E}, where $\psi(L)$ is the luminosity function and $\rho(z)$ is the formation rate of SGRBs. However in general the luminosity and redshift is not independent \citep{2002ApJ...574..554L}, the luminosity function $\psi(L)$ could still evolve with redshift z, and this degeneracy can be eliminated by adjusting the luminosity L with a factor $g(z)$, so that $\Psi(L,z)=\rho(z)\psi(L/g(z))/g(z)$, where $g(z)$ means the luminosity evolution, and the value $L_0=L/g(z)$ corresponds to the luminosity after removing the luminosity evolution effect. By making such substitution, the $\psi(L/g(z))$ is independent of redshift and represents the local luminosity distribution.

$g(z)$ is often taken as $g(z)=(1+z)^k$ in the literatures \citep{2002ApJ...574..554L,2014ApJ...789...65Y,2015ApJS..218...13Y}. Following \citet{1992ApJ...399..345E}, we use the non-parametric test method of $\tau$ statistical to derive the value of $k$. We get $k=4.78^{+0.17}_{-0.18}$ (the error is reported in 1$\sigma$ confidence level). For comparison, \citet{2014ApJ...789...65Y} gave $k=3.3^{+1.7}_{-3.7}$ using Swift samples, \citet{2018MNRAS.477.4275P} gave $k=4.269^{+0.134}_{-0.134}$ and \citet{2018ApJ...852....1Z} gave $k=4.47^{+0.47}_{-0.47}$ for Fermi samples.

After removing the effect of luminosity evolution through $L_0=L/(1+z)^{4.78}$, the cumulative luminosity function can be obtained by the following method \citep{1971MNRAS.155...95L,1992ApJ...399..345E}. For each point $(L_i, z_i)$, we define the set $J_i$ as
\begin{equation}
J_i=\lbrace{j}\mid{L_j}\geq {L_i},{z_j}\leq {z^{max}_{i}}\rbrace
\end{equation}
where $L_i$ is the luminosity of $i$th SGRB, the parameter $z^{max}_{i}$ is the maximum redshift at which the SGRBs with the luminosity $L_i$ can be detected. The number of SGRBs contained in this region is $n_i$. Then we use the following equation to calculate the cumulative luminosity function \citep{1971MNRAS.155...95L}
\begin{equation}
\psi(L_{0i})=\prod_{j<i}(1+\frac{1}{N_j})
\end{equation}
where $j < i$ means that the $j$th SGRB has a larger luminosity than $i$th sGRB. The results are shown in the left panel of Fig.\ref{fig:distribution}, which can be fitted with a broken power-law as
\begin{eqnarray}\label{lcmf}
\psi(L_0) \propto \left\{
\begin{array}{cc}
L_0^{-0.63 \pm 0.07} \qquad L_0 \le L_0^b \\
L_0^{-1.96 \pm 0.28} \qquad L_0 > L_0^b
\end{array} \right.
\end{eqnarray}
where $L_0^b = 6.95_{-0.76}^{+0.84}\times10^{50} \rm{erg/s}$ is the break luminosity. This result is roughly in agreement with previous works \citep{2014ApJ...789...65Y, 2018ApJ...852....1Z}. For the formation rate of sGRBs, we define $J^{\prime}_i$  as
\begin{equation}
J_i^{\prime}=\lbrace{j}\mid{L_j}> {L_i^{lim}},{z_j}< {z_{i}}\rbrace
\end{equation}
Where $z_i$ is the redshift of $i$th SGRB, the parameter $L^{min}_i$ is the minimum luminosity which can be detected at redshift $z_i$. The number of SGRBs contained in this region is $m_i$. Then we can obtain the cumulative redshift distribution as \citep{1971MNRAS.155...95L}:
\begin{equation}
\phi(z_i)=\prod_{j<i}(1+\frac{1}{M_j})
\end{equation}
where $j<i$ means that the $j$th SGRB has a less redshift than $i$th SGRB. The results are shown in the middle panel of Fig.\ref{fig:distribution}. Then the probability density function (PDF) of redshift distribution can be calculated by:
\begin{equation}
\rho(z)=\frac{d\phi(z)}{dz}(1+z)(\frac{dV(z)}{dz})^{-1}
\end{equation}
\begin{equation}
\frac{dV(z)}{dz}=4\pi \left ( \frac{c}{H_0} \right )^3 \left [ \int_{0}^{z}\frac{dz}{\sqrt{1-\Omega_{\rm m}+\Omega_{\rm m}(1+z)^3}}\right ]^2 \times \frac{1}{\sqrt{1-\Omega_{\rm m}+\Omega_{\rm m}(1+z)^3}}
\end{equation}

The results are shown in the right panel of Fig.\ref{fig:distribution}. Again, the formation rate of SGRBs can be fitted by:
\begin{eqnarray}\label{zpdf}
\rho(z) \propto \left\{
\begin{array}{cc}
(1+z)^{-4.39 \pm 0.55} \qquad z \le 1.5 \\
(1+z)^{-5.51 \pm 0.32} \qquad z > 1.5
\end{array} \right.
\end{eqnarray}

Meanwhile, we can derive the formation rate of sGRBs in the local universe, $\rho(0)=15.5 \pm 5.8\ \rm{Gpc^{-3}yr^{-1}}$, which is roughly consistent with the results of \citet{2015ApJ...815..102F} that the local event rate is $10 \rm{ Gpc^{-3}yr^{-1}}$ and $\rho(0)=7.53 \rm{Gpc^{-3}yr^{-1}}$  in \citet{2018ApJ...852....1Z}.

At last, we perform the Monte Carlo simulation to test whether our results can recover the sGRB distributions. We simulate a set of points $(L_0, z)$ which follow the equations Eq.(\ref{lcmf}) and Eq.(\ref{zpdf}), and then calculate the luminosity $L$ using the relation $L=L_0(1+z)^{4.78}$, thus we obtain a set of points $(L, z)$. We simulate $10^{5}$ points and divide them into 100 groups. For each group, we select one sGRBs from them and get 100 pseudo sGRBs to compare with the observed data. Finally, we perform the same analysis as above to obtain the luminosity function and formation rate of sGRBs. In Fig.\ref{fig:mctest} we present our results, where the blue lines are the simulated data for the cumulative luminosity function and cumulative redshift distribution, the red lines and green lines are the observed data and the mean of the simulated data, respectively. We also perform the Kolmogorov–Smirnov test between observed data and the mean distribution of simulated data, the chance probabilities are 0.62 and 0.83 respectively, which indicates that the cumulative luminosity function and formation rate are reliable.

\begin{figure}[ht!]
	\figurenum{5}\label{fig:distribution}
	\centering
	\includegraphics[angle=0,scale=0.26]{fig5a.png}
	\includegraphics[angle=0,scale=0.26]{fig5b.png}
	\includegraphics[angle=0,scale=0.26]{fig5c.png}
	\caption{Left: cumulative luminosity function of SGRBs. The dotted lines are the $95\%$ confidence bands (Moreira et al. 2010); middle: cumulative redshift distribution of SGRBs; right: the PDF of the redshift distribution derived from the cumulative distribution, with its first bin normalized to unity.}
	\hfill
\end{figure}

\begin{figure}[ht!]
	\figurenum{6}\label{fig:mctest}
	\centering
	\includegraphics[angle=0,scale=0.4]{fig6a.png}
	\includegraphics[angle=0,scale=0.4]{fig6b.png}
	\caption{Comparison of simulated data (blue) and observed data (red). Left is the cumulative luminosity function. Right is the cumulative redshift distribution. The green lines are the mean of simulated data.}
	\hfill
\end{figure}

\section{Summary and Discussion}\label{SD}

Gamma-ray bursts are the most powerful explosions in the universe, although great progress have been achieved in recent years, their nature is still unclear. Meanwhile since their huge luminosity/energy, GRBs can be detected to large redshift and thus can serve as a valuable cosmological tool.

A variety of correlations among intrinsic properties have been proposed in these years, on one hand these correlations can help to reveal the nature of GRBs, and on the other hand some correlations may be used as a redshift indicator, such as the so-called "Amati relation" \citep{2002AA...390...81A} and "Yonetoku relation" \citep{2014ApJ...789...65Y}. However none of these correlations is valid for both long GRBs and short GRBs. In this paper, we study the correlations among gamma-ray burst prompt emission properties and find a universal correlation which is suitable for both long and short GRBs, i.e. $L_{iso}\propto {E^{1.94}_{peak}}T^{0.37}_{0.45}$ This universal correlation may have important implications for GRB physics, implying that the long and short GRBs may share similar radiation processes. The parameters of the relation obtained in our study is different from that in \citet{2006MNRAS.370..185F}. The reason may not only be the different sample (more long GRBs and the inclusion of short GRBs) we used in our study, but could also be the degeneracy between parameters in the three-parameter fitting. The degeneracy could be studied by examine the joint posterior distributions obtained via MCMC/nested sampling approaches, and we leave it for future study.

Some other three-parameter correlations have also been found for GRBs, for example, \citet{2005ApJ...633..611L} found that there is a tight correlation between the isotropic gamma-ray energy, the peak energy of the gamma-ray spectra, and the break time of the optical afterglow light curves. For GRBs with X-ray plateau phase, the three-parameter correlations also have been reported to exist between the end time of the plateau phase, the corresponding X-ray luminosity and the peak luminosity or isotropic energy in the prompt emission phase \citep{2014PASJ...66...42T,2016ApJ...825L..20D,2017ApJ...848...88D, 2019ApJS..245....1T}. In these relations we need to know the information of the afterglow emission, such as the break time of the afterglow light curves, the duration and  luminosity of the X-ray plateau phase. Nonetheless, the universal correlation found in this paper only involves properties of GRB prompt emission and does not require any information of afterglow phase.

This universal correlation can be used as a redshift indicator. Here we use this relation to calculate the pseudo redshifts of short GRBs, and then use the Lynden-Bell's $c^-$ method to study the luminosity function and formation rate of SGRBs. We find that the luminosity function can be expressed as $\psi(L_0)\propto{L_0^{-0.63\pm{0.07}}}$ for dim SGRBs and $\psi(L_0)\propto{L_0^{-1.96\pm{0.28}}}$ for bright SGRBs, with the break luminosity $L^b_0=6.95_{-0.76}^{+0.84}\times{10^{50}} \rm{erg/s}$. For the formation rate of sGRBs, we give the result that $\rho(z)\propto(1+z)^{-4.39\pm{0.55}}$ for $z<1.5$ and $\rho(z)\propto(1+z)^{-5.51\pm{0.32}}$ for $z>1.5$, and also we have obtained the local SGRB rate as $\rho(0)=15.5 \pm 5.8\ \rm{Gpc^{-3}yr^{-1}}$, these results are roughly consistent with \citet{2018ApJ...852....1Z}. If we take the typical beaming factor as $f_b^{-1}=30$ \citep{2015ApJ...815..102F}, then the actual total local event rate of SGRBs is about $450 \rm{Gpc^{-3}yr^{-1}}$, which is also consistent with the results inferred from the gravitational wave detections \citep{2019PhRvX...9c1040A}.

\acknowledgments

We thank the anonymous referee for valuable comments. We thank Jinyi Shangguan for helpful discussions. This work was supported by NSFC (No. 11933010), by the Chinese Academy of Sciences via the Strategic Priority Research Program (No. XDB23040000), Key Research Program of Frontier Sciences (No. QYZDJ-SSW-SYS024).

\clearpage

\begin{deluxetable*}{lrrrrrrrrl}
\tablecaption{The 49 Long GRB samples\label{tab:1}}
\tablewidth{700pt}
\tabletypesize{\scriptsize}
\tablehead{
\colhead{Name} & \colhead{$z$} & \colhead{$E_{\rm peak}$} &
\colhead{$T_{\rm 0.45}$} & \colhead{$\alpha$} & \colhead{$\beta$} &
\colhead{$L_{\rm iso}$} & \colhead{$E_{\rm iso}$}  & \colhead{Detection Band} & \colhead{Ref.} \\
\colhead{} & \colhead{} & \colhead{(KeV)} &
\colhead{(s)} & \colhead{} & \colhead{} &
\colhead{($10^{52}$erg/s)} & \colhead{($10^{52}$erg/s)} & \colhead{(KeV)} & \colhead{}
}
\startdata
50401	&	2.9	&	$	464.10	\pm	26	$	&	$	5.18	\pm	0.212	$	&	-0.83	&	-2.37	&	$	20.90	\pm	0.1	$	&	$	35.00	\pm	7	$	&	$	20-2000	$	&	2	\\
050416A	&	0.6535	&	$	26.01	\pm	2	$	&	$	0.63	\pm	0.043	$	&	-1	&	-3.4	&	$	0.10	\pm	0.99	$	&	$	25.10	\pm	0.01	$	&	$	15-150	$	&	1	\\
50603	&	2.821	&	$	1333.53	\pm	28	$	&	$	1.6	\pm	0.08	$	&	-0.79	&	-2.15	&	$	225.00	\pm	0.14	$	&	$	60.00	\pm	4	$	&	$	20-3000	$	&	3	\\
60124	&	2.296	&	$	816.62	\pm	88	$	&	$	2.38	\pm	0.129	$	&	-1.29	&	-2.25	&	$	13.70	\pm	0.74	$	&	$	41.00	\pm	6	$	&	$	20-2000	$	&	4	\\
61007	&	1.261	&	$	1125.98	\pm	48	$	&	$	16.8	\pm	0.122	$	&	-0.53	&	-2.61	&	$	17.80	\pm	0.31	$	&	$	86.00	\pm	9	$	&	$	20-10000	$	&	5	\\
061222A	&	2.088	&	$	1090.06	\pm	54	$	&	$	8.97	\pm	0.159	$	&	-1	&	-2.32	&	$	14.80	\pm	0.4	$	&	$	20.80	\pm	0.602	$	&	$	20-10000	$	&	1	\\
071010B	&	0.947	&	$	101.24	\pm	10	$	&	$	4.68	\pm	0.075	$	&	-1.25	&	-2.65	&	$	0.65	\pm	2.17	$	&	$	1.70	\pm	0.9	$	&	$	20-1000	$	&	6	\\
080319B	&	0.937	&	$	1307.48	\pm	22	$	&	$	20.3	\pm	0.058	$	&	-0.86	&	-3.59	&	$	10.50	\pm	0.1	$	&	$	114.00	\pm	9	$	&	$	20-7000	$	&	1	\\
080319C	&	1.95	&	$	905.65	\pm	0.06	$	&	$	5.04	\pm	0.152	$	&	-1.01	&	-1.87	&	$	9.46	\pm	2.28	$	&	$	14.10	\pm	2.8	$	&	$	20-4000	$	&	7	\\
80605	&	1.6398	&	$	784.02	\pm	40	$	&	$	4.75	\pm	0.079	$	&	-0.87	&	-2.58	&	$	33.30	\pm	0.69	$	&	$	24.00	\pm	2	$	&	$	20-2000	$	&	8	\\
80607	&	3.036	&	$	1404.53	\pm	27	$	&	$	7.52	\pm	0.094	$	&	-0.76	&	-2.57	&	$	221.00	\pm	0.44	$	&	$	188.00	\pm	10	$	&	$	20-4000	$	&	9	\\
80721	&	2.602	&	$	1790.19	\pm	62	$	&	$	4.51	\pm	0.195	$	&	-0.96	&	-2.42	&	$	111.00	\pm	0.18	$	&	$	126.00	\pm	22	$	&	$	20-7000	$	&	1	\\
80810	&	3.35	&	$	2523.00	\pm	263	$	&	$	31.35	\pm	2.914	$	&	-1.2	&	-2.5	&	$	239.00	\pm	0.14	$	&	$	45.00	\pm	5	$	&	$	15-1000	$	&	11	\\
80913	&	6.7	&	$	931.70	\pm	39	$	&	$	2.16	\pm	0.139	$	&	-0.82	&	-2.5	&	$	12.40	\pm	0.18	$	&	$	8.60	\pm	2.5	$	&	$	15-150	$	&	12,13	\\
81028	&	3.038	&	$	240.91	\pm	6	$	&	$	78.12	\pm	2.09	$	&	0.36	&	-2.25	&	$	4.91	\pm	0.45	$	&	$	17.00	\pm	2	$	&	$	8-35000	$	&	10	\\
81121	&	2.512	&	$	726.63	\pm	43.8	$	&	$	5.51	\pm	0.26	$	&	-0.21	&	-1.86	&	$	13.80	\pm	0.22	$	&	$	26.00	\pm	5	$	&	$	8-35000	$	&	10	\\
81222	&	2.77	&	$	629.59	\pm	8	$	&	$	4.2	\pm	0.053	$	&	-0.9	&	-2.33	&	$	10.10	\pm	0.03	$	&	$	30.00	\pm	3	$	&	$	8-35000	$	&	1	\\
90424	&	0.544	&	$	250.13	\pm	2	$	&	$	1.98	\pm	0.03	$	&	-1.02	&	-3.26	&	$	1.14	\pm	0.02	$	&	$	4.60	\pm	0.9	$	&	$	8-35000	$	&	1	\\
90516	&	4.109	&	$	262.60	\pm	11.4	$	&	$	36.96	\pm	2.259	$	&	-1.03	&	-2.1	&	$	8.70	\pm	0.33	$	&	$	88.50	\pm	19.2	$	&	$	8-1000	$	&	14	\\
90618	&	0.54	&	$	482.33	\pm	14	$	&	$	23.04	\pm	0.706	$	&	-0.91	&	-2.42	&	$	1.87	\pm	0.08	$	&	$	25.40	\pm	0.6	$	&	$	8-35000	$	&	10	\\
90809	&	2.737	&	$	722.74	\pm	11	$	&	$	3.43	\pm	0.456	$	&	-0.47	&	-2.16	&	$	34.00	\pm	0.28	$	&	$	4.20	\pm	1.2	$	&	$	8-35000	$	&	10	\\
90927	&	1.37	&	$	141.42	\pm	1.81	$	&	$	0.84	\pm	0.09	$	&	-0.68	&	-2.12	&	$	0.37	\pm	0.23	$	&	$	0.70	\pm	0.312	$	&	$	8-35000	$	&	10	\\
91020	&	1.71	&	$	506.77	\pm	25	$	&	$	6	\pm	0.166	$	&	-1.2	&	-2.29	&	$	3.44	\pm	0.04	$	&	$	12.20	\pm	2.4	$	&	$	8-35000	$	&	1	\\
91127	&	0.49	&	$	88.91	\pm	1.81	$	&	$	1.54	\pm	0.063	$	&	-0.68	&	-2.12	&	$	0.77	\pm	0.19	$	&	$	1.63	\pm	0.02	$	&	$	8-35000	$	&	10	\\
100615A	&	1.398	&	$	205.58	\pm	8	$	&	$	9.43	\pm	0.222	$	&	-1.24	&	-2.27	&	$	1.06	\pm	0.03	$	&	$	4.22	\pm	1.21	$	&	$	8-1000	$	&	15	\\
100621A	&	0.542	&	$	146.49	\pm	15	$	&	$	19.43	\pm	0.327	$	&	-1.7	&	-2.45	&	$	0.32	\pm	0.25	$	&	$	4.37	\pm	0.5	$	&	$	20-2000	$	&	1	\\
100728A	&	1.567	&	$	1001.13	\pm	25	$	&	$	57.35	\pm	0.185	$	&	-0.47	&	-2.5	&	$	6.45	\pm	1.08	$	&	$	63.74	\pm	12.2	$	&	$	20-10000	$	&	16	\\
100816A	&	0.8049	&	$	246.73	\pm	4.7	$	&	$	0.84	\pm	0.016	$	&	-0.31	&	-2.77	&	$	0.74	\pm	0.12	$	&	$	0.73	\pm	0.02	$	&	$	10-1000	$	&	17,18	\\
100906A	&	1.727	&	$	490.86	\pm	40	$	&	$	11.07	\pm	0.123	$	&	-1.1	&	-2.2	&	$	6.90	\pm	0.77	$	&	$	28.90	\pm	0.3	$	&	$	20-2000	$	&	19	\\
101213A	&	0.414	&	$	437.91	\pm	40	$	&	$	20.16	\pm	0.69	$	&	-1.1	&	-2.35	&	$	0.06	\pm	0.43	$	&	$	3.01	\pm	0.64	$	&	$	10-1000	$	&	20	\\
101219B	&	0.55	&	$	108.50	\pm	8	$	&	$	8.36	\pm	0.736	$	&	-0.33	&	-2.12	&	$	0.04	\pm	0.38	$	&	$	0.59	\pm	0.04	$	&	$	10-1000	$	&	21	\\
110422A	&	1.77	&	$	681.42	\pm	34	$	&	$	9.24	\pm	0.09	$	&	-0.53	&	-2.65	&	$	0.29	\pm	0.36	$	&	$	43.10	\pm	0.13	$	&	$	20-2000	$	&	22	\\
110503A	&	1.613	&	$	572.25	\pm	19	$	&	$	2.1	\pm	0.056	$	&	-0.98	&	-2.7	&	$	18.90	\pm	0.19	$	&	$	10.49	\pm	11.4	$	&	$	20-5000	$	&	1	\\
110715A	&	0.82	&	$	218.40	\pm	11	$	&	$	1.45	\pm	0.025	$	&	-1.23	&	-2.7	&	$	1.19	\pm	0.39	$	&	$	2.93	\pm	0.12	$	&	$	20-10000	$	&	23	\\
110731A	&	2.83	&	$	1164.32	\pm	13	$	&	$	3.36	\pm	0.071	$	&	-0.8	&	-2.98	&	$	30.60	\pm	0.07	$	&	$	118.05	\pm	9.12	$	&	$	10-1000	$	&	24	\\
110801A	&	1.858	&	$	400.12	\pm	50	$	&	$	54.56	\pm	1.731	$	&	-1.7	&	-2.5	&	$	0.44	\pm	0.84	$	&	$	15.84	\pm	1.32	$	&	$	15-350	$	&	25	\\
111228A	&	0.714	&	$	58.28	\pm	3	$	&	$	9	\pm	0.307	$	&	-1.9	&	-2.7	&	$	0.67	\pm	0.25	$	&	$	4.41	\pm	0.202	$	&	$	10-1000	$	&	26	\\
120119A	&	1.728	&	$	516.14	\pm	8	$	&	$	13.6	\pm	0.198	$	&	-0.98	&	-2.36	&	$	5.98	\pm	0.14	$	&	$	20.79	\pm	1.98	$	&	$	10-1000	$	&	27	\\
120326A	&	1.798	&	$	129.97	\pm	3.67	$	&	$	4.68	\pm	0.114	$	&	-0.98	&	-2.53	&	$	0.59	\pm	0.1	$	&	$	3.11	\pm	0.617	$	&	$	10-1000 	$	&	28	\\
120712A	&	4.1745	&	$	641.64	\pm	26	$	&	$	4.68	\pm	0.146	$	&	-0.6	&	-1.8	&	$	13.50	\pm	0.08	$	&	$	8.35	\pm	1.49	$	&	$	10-1000	$	&	29	\\
120922A	&	3.1	&	$	154.57	\pm	3.5	$	&	$	43.93	\pm	1.488	$	&	-1.6	&	-2.3	&	$	3.02	\pm	0.27	$	&	$	19.79	\pm	5.89	$	&	$	10-1000	$	&	30	\\
121128A	&	2.2	&	$	199.04	\pm	4.6	$	&	$	4.75	\pm	0.198	$	&	-0.8	&	-2.41	&	$	1.53	\pm	0.19	$	&	$	9.24	\pm	1.11	$	&	$	10-1000	$	&	31	\\
130215A	&	0.597	&	$	247.54	\pm	63	$	&	$	19.5	\pm	1.148	$	&	-1	&	-1.6	&	$	0.22	\pm	0.18	$	&	$	3.14	\pm	0.88	$	&	$	10-1000	$	&	32	\\
130408A	&	3.758	&	$	1294.18	\pm	40	$	&	$	1.26	\pm	0.092	$	&	-0.7	&	-2.3	&	$	61.20	\pm	0.59	$	&	$	7.41	\pm	1.41	$	&	$	20-10000	$	&	33	\\
130427A	&	0.3399	&	$	1112.12	\pm	5	$	&	$	7.64	\pm	0.382	$	&	-0.789	&	-3.06	&	$	19.00	\pm	0.001	$	&	$	46.18	\pm	8.26	$	&	$	8-1000	$	&	34	\\
130505A	&	2.27	&	$	1975.08	\pm	49	$	&	$	6.23	\pm	0.623	$	&	-0.31	&	-2.26	&	$	398.00	\pm	0.17	$	&	$	1012.60	\pm	253.9	$	&	$	20-1200	$	&	35	\\
130831A	&	0.4791	&	$	99.10	\pm	4	$	&	$	4.07	\pm	0.094	$	&	-1.51	&	-2.8	&	$	0.34	\pm	0.39	$	&	$	1.49	\pm	0.0578	$	&	$	20-10000	$	&	36	\\
130907A	&	1.238	&	$	872.82	\pm	16	$	&	$	40.31	\pm	0.139	$	&	-0.65	&	-2.22	&	$	18.20	\pm	0.08	$	&	$	122.31	\pm	10.92	$	&	$	20-10000	$	&	37	\\
131030A	&	1.295	&	$	406.22	\pm	10	$	&	$	7.35	\pm	0.118	$	&	-0.71	&	-2.95	&	$	10.80	\pm	0.11	$	&	$	24.72	\pm	3.19	$	&	$	20-10000	$	&	38	\\
\enddata
\tablecomments{
References. (1) \citet{2012MNRAS.421.1256N}; (2) \citet{2005GCN..3179....1G}; (3) \citet{2005GCN..3518....1G}; (4) \citet{2006GCN..4599....1G}; (5) \citet{2006GCN..5722....1G}; (6) \citet{2007GCN..6879....1G}; (7) \citet{2008GCN..7487....1G}; (8) \citet{2008GCN..7854....1G}; (9) \citet{2008GCN..7862....1G}; (10) Nava et al. (2011); (11) \citet{2008GCN..8101....1S}; (12) \citet{2008GCN..8256....1P}; (13) \citet{2009ApJ...693.1610G}; (14) \citet{2009GCN..9415....1M}; (15) \citet{2010GCN.10851....1F}; (16) \citet{2010GCN.11021....1G}; (17) \citet{2010GCN.11124....1F}; (18) \citet{2010GCN.11124....1F}; (19) \citet{2010GCN.11251....1G}; (20) \citet{2010GCN.11454....1G}; (21) \citet{2010GCN.11477....1V}; (22) \citet{2011GCN.11971....1G}; (23) \citet{2011GCN.12166....1G}; (24) \citet{2011GCN.12223....1G}; (25) \citet{2011GCN.12276....1S}; (26) \citet{2011GCN.12744....1B}; (27) \citet{2012GCN.12874....1G}; (28) \citet{2012GCN.13145....1C}; (29) \citet{2012GCN.13469....1G}; (30) \citet{2012GCN.13809....1Y}; (31) \citet{2012GCN.14012....1M}; (32) \citet{2013GCN.14219....1Y}; (33) \citet{2013GCN.14368....1G} ; (34) \citet{2013GCN.14473....1V}; (35) \citet{2013GCN.14575....1G}; (36) \citet{2013GCN.15145....1G}; (37) \citet{2013GCN.15203....1G};  (38)  \citet{2013GCN.15413....1G}.
}
\end{deluxetable*}

\begin{deluxetable*}{lrrrrrl}
\tablecaption{The 19 Short GRB samples\label{tab:2}}
\tablewidth{700pt}
\tabletypesize{\scriptsize}
\tablehead{
\colhead{Name} & \colhead{$z$} &
\colhead{$E_{\rm peak}$} & \colhead{$T_{\rm 0.45}$} &
\colhead{$L_{\rm iso}$} & \colhead{$E_{\rm iso}$} & \colhead{Ref.} \\
\colhead{} & \colhead{} & \colhead{(KeV)} & \colhead{(s)} &
\colhead{($10^{52}$erg/s)} & \colhead{($10^{52}$erg/s)} & \colhead{}
}
\startdata
050509B	&	0.225	&	$	102	\pm	10	$	&	$	0.02	\pm	0.04	$	&	$	0.01	\pm	0.09	$	&	$	0.00024	\pm	0.00044	$	&	14	\\
051221A	&	0.546	&	$	621	\pm	114	$	&	$	0.16	\pm	0.008	$	&	$	2.77	\pm	0.29	$	&	$	0.3	\pm	0.04	$	&	1,2	\\
060502B	&	0.287	&	$	193	\pm	19	$	&	$	0.04	\pm	0.007	$	&	$	0.089	\pm	0.05	$	&	$	0.003	\pm	0.005	$	&	1	\\
61201	&	0.111	&	$	969	\pm	508	$	&	$	0.22	\pm	0.014	$	&	$	0.3445	\pm	0.4	$	&	$	3	\pm	4	$	&	1	\\
61217	&	0.827	&	$	216	\pm	22	$	&	$	0.1	\pm	0.008	$	&	$	1.498	\pm	2.2	$	&	$	0.03	\pm	0.04	$	&	1	\\
070429B	&	0.902	&	$	813	\pm	81	$	&	$	0.08	\pm	0.011	$	&	$	1.873	\pm	1.6	$	&	$	0.07	\pm	0.11	$	&	1	\\
070714B	&	0.92	&	$	2150	\pm	1113	$	&	$	1.4	\pm	0.132	$	&	$	6.56	\pm	1.36	$	&	$	0.83	\pm	0.1	$	&	4	\\
070724A	&	0.457	&	$	119	\pm	12	$	&	$	0.11	\pm	0.011	$	&	$	0.087	\pm	0.005	$	&	$	0.00245	\pm	0.00175	$	&	13	\\
70809	&	0.473	&	$	91	\pm	9	$	&	$	0.26	\pm	0.018	$	&	$	0.042	\pm	0.001	$	&	$	0.00131	\pm	0.00103	$	&	1	\\
90510	&	0.903	&	$	8370	\pm	760	$	&	$	0.12	\pm	0.013	$	&	$	104	\pm	24	$	&	$	3.75	\pm	0.25	$	&	5	\\
090426A	&	2.609	&	$	320	\pm	54	$	&	$	0.32	\pm	0.025	$	&	$	1.46	\pm	0.38	$	&	$	1.1	\pm	0.38	$	&	1	\\
100117A	&	0.915	&	$	551	\pm	135	$	&	$	0.14	\pm	1.693	$	&	$	1.89	\pm	0.21	$	&	$	0.09	\pm	0.01	$	&	5	\\
100206A	&	0.407	&	$	638.98	\pm	131.21	$	&	$	0.06	\pm	0.009	$	&	$	1	\pm	1.15	$	&	$	0.0763	\pm	0.03	$	&	5	\\
100625A	&	0.452	&	$	1018	\pm	166	$	&	$	0.14	\pm	0.007	$	&	$	1.4	\pm	0.06	$	&	$	0.399	\pm	0.06	$	&	11	\\
101219A	&	0.718	&	$	842	\pm	170	$	&	$	0.24	\pm	0.011	$	&	$	1.56	\pm	0.24	$	&	$	0.49	\pm	0.23	$	&	6	\\
130603B	&	0.356	&	$	891.66	\pm	135.6	$	&	$	0.04	\pm	0.007	$	&	$	3.04	\pm	0.44	$	&	$	1.476	\pm	0.44	$	&	9	\\
61006	&	0.4377	&	$	966	\pm	322	$	&	$	0.24	\pm	0.01	$	&	$	2.06	\pm	0.15	$	&	$	0.983	\pm	0.15	$	&	3	\\
71227	&	0.381	&	$	1000	\pm	31	$	&	$	0.5	\pm	0.034	$	&	$	0.443	\pm	0.139	$	&	$	0.1	\pm	0.01	$	&	12	\\
101224A	&	0.72	&	$	393.88	\pm	161	$	&	$	0.12	\pm	0.013	$	&	$	0.824	\pm	0.125	$	&	$		--		$	&	10	\\
\enddata
\tablecomments{
Reference: (1)\citet{2007ApJ...671..656B} and references therein; (2)\citet{2005GCN..4394....1G}; (3)\citet{2006GCN..5710....1G}; (4)\citet{2007GCN..6638....1O}; (5)\citet{2013MNRAS.431.1398T}; (6)\citet{2010GCN.11470....1G}; (7)\citet{2016GCN.19843....1S}; (8)\citet{2016GCN.19570....1H}; (9)\citet{2013GCN.14771....1G}; (10) \citet{2010GCN.11489....1M}; (11)\citet{2010GCN.10912....1B}; (12)\citet{2007GCN..7155....1G}; (13)\citet{2007GCNR...74....2Z}; (14)\citet{2005GCN..3385....1B}.
(15)\citet{2019arXiv190205489W}  (16)\citet{2018ApJ...852....1Z} (17)\citet{2013MNRAS.430..163Q}.
}
\end{deluxetable*}
\clearpage

redpajama_set_name: RedPajamaArXiv


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Kingsgate: News
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King County Library System Releases its Best Books of 2018
King County Library System (KCLS), one of the busiest library systems in the country, released its selections for the Best Books of 2018. The annual list includes KCLS' top 25 titles each under four categories: adult fiction, adult nonfiction, teens and children's.
View More about King County Library System Releases its Best Books of 2018
KCLS Foundation awarded $80,000 Boeing Grant for KCLS to Expand STEAM Education
The King County Library System Foundation (KCLSF) has been awarded an $80,000 grant from the Boeing Company to help the King County Library System (KCLS) expand STEAM education, with the aim of increasing access to technology and 21st-century workplace skills for thousands of low-income and underserved families. The Boeing grant will enable KCLS to broaden…
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KCLS, Nation's Leader in Digital Downloads, Launches New Podcast for Readers
KCLS just launched a podcast called "The Desk Set," co-hosted by KCLS librarians Emily Calkins and Britta Barrett. The podcast features author interviews, book reviews, literary conversations, and encourages listeners to expand their reading horizons.
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King County Library System Squares Off Against New York Public Libraries at Sixth Annual Sorting Smackdown
MEDIA ALERT November 2, 2018 What: The New York Public Library (NYPL) and Brooklyn Public Library (BPL) will join forces to take on the King County Library System (KCLS) in the sixth annual Book Sorting Competition at 10 am PST Friday, November 9. KCLS, which has a 3-2 lead over the New Yorkers, will be…
View More about King County Library System Squares Off Against New York Public Libraries at Sixth Annual Sorting Smackdown
King County Library System's New eCard is Now Available
ISSAQUAH, WA-August 10, 2018 – A new online access opportunity for King County Library patrons is now available. The King County Library System is unveiling a new eCard for residents in the KCLS service area who may not yet have a library card and would like online access to KCLS resources. With the new…
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text:
Q: Migrating from Windows 7 to Ubuntu 14.1 64 bit Couple of questions before we as a company migrate:
Our server is Windows 2008 std. Will it support Ubuntu clients?
Data backed-up from Windows client can it be restored on Ubuntu
We connect to remote Servers thru Remote Desktop.. will Remmina work?
Normal usage software like Adobe/VLC/Teamviewer work on Ubuntu?
Thanks & Regards
Sanjiv

A: Some advice for doing windows stuff on ubuntu: try installing wine, it does the job. download here or you can search for it on the ubuntu software center.

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Serbia's Minister for Kosovo says U.N. Secretary-General Ban Ki-moon was wrong when he said the prolonged deadlock over the future of Serbia's breakaway province could create instability in the region.
Slobodan Samardzic told Serbia's Tanjug news agency that Kosovo independence would actually cause instability because it would send a signal to separatist movements everywhere to pursue similar goals.
On Monday, in a report to Security Council members, Mr. Ban said delaying a decision on the future status of Kosovo could lead to events on the ground that would put U.N. achievements in the area at risk.
The Security Council has not been unified on the future status of Kosovo.
The province's ethnic Albanian majority wants independence from Serbia. Belgrade has offered broad autonomy to the province with many elements of statehood, but insists on retaining sovereignty over the territory.
Samardzic said the U.N. secretary-general should pay more attention to international law and less to what he called the separatist aspirations of militant members of ethnic minorities.
Russia has backed Serbia and has threatened to veto any resolution on Kosovo independence. The United States and many European countries have indicated readiness to recognize independence.
Kosovo has been under U.N. administration since 1999, when NATO airstrikes halted Belgrade's deadly crackdown on ethnic Albanian separatists.


After the site's owners couldn't convince the school board to throw its support behind their project, the Doraville Downtown Development Authority voted unanimously Tuesday night to award incentives worth 35 percent of the site's annual property tax bill for the next 30 years.
For eight years since the GM plant closed, the site has been dormant. Developers said they couldn't wait any longer to get started on the project. Already, businesses that could have brought 1,200 jobs to the site have passed on the opportunity because of uncertainty and delays, Schmit said.
"This is such an important project. We don't want it to go by the wayside," said Doraville Mayor Donna Pittman.
But Tom Hart, a former city councilman, said the tax incentives are a handout that will take money from the school system, DeKalb County's government and the city government.
The site's property owners have formed an organization called a community improvement district, which will be used to spend money generated from the tax breaks specifically for public infrastructure.


text:
029| Interview with Jordana Arkin (Part Two)
On this episode of the podcast I conclude my conversation with What's New, Scooby-Doo? writer, Jordana Arkin.
028| Interview with Jordana Arkin (Part One)
We're back with another great conversation on the podcast, this time featuring What's New, Scooby-Doo? writer, Jordana Arkin. Jordana had a hand in writing two episodes for the series (in its second and third seasons, respectively) and shares her experiences of getting involved with the show, writing for the gang,...
027| Interview with Aaron Lopresti
On this episode of the podcast I continue my exploration of the Future Quest universe with amazing series artist, Aaron Lopresti, discussing his work on the highly entertaining Herculoids segments for the DC/Hanna-Barbera books.
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'All Fear the Freak' Isolated Episode Commentary with Victor Cook
It's another installment of APNSD! Extra featuring returning guest commentator and friend of the show, Victor Cook. Victor was a Supervising Director and episode director for Scooby-Doo: Mystery Incorporated and was kind enough to give of his time to provide an isolated audio commentary for the season one SDMI finale...
APNSD! Presents A Scooby-Dooniversary 2: Podcasters Unleashed!!
The original Scooby-Dooniversary commentators are once again unleashed on the podcast to celebrate, as promised, the 15th anniversary of the theatrical release for Scooby-Doo 2: Monsters Unleashed! Join Billy Seguire (Scooby Dos or Scooby Don'ts), nic robes (What's With You? Scooby-Doo), and myself as we discuss...


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text:
Q: How to fixed PermGen memory issue I got the following error in browser when log into the system

java.lang.RuntimeException: javax.servlet.ServletException:
  java.lang.OutOfMemoryError: PermGen space
    com.opensymphony.sitemesh.webapp.decorator.BaseWebAppDecorator.render(BaseWebAppDecorator.java:39)
    com.opensymphony.sitemesh.webapp.SiteMeshFilter.doFilter(SiteMeshFilter.java:84)

A: java.lang.OutOfMemoryError

Thrown when the Java Virtual Machine cannot allocate an object because
  it is out of memory, and no more memory could be made available by the
  garbage collector. OutOfMemoryError objects may be constructed by the
  virtual machine as if suppression were disabled and/or the stack trace
  was not writable.

Increase the heap size of your JVM
It is possible to increase heap size allocated by the JVM by using command line options Here we have 3 options
-Xms<size>        set initial Java heap size
-Xmx<size>        set maximum Java heap size
-Xss<size>        set java thread stack size

Common causes of OutofMemory in PermGen is ClassLoader. Whenever a class is loaded into JVM, all its meta data, along with Classloader, is kept on PermGen area and they will be garbage collected when the Classloader which loaded them is ready for garbage collection. In Case Classloader has a memory leak than all classes loaded by it will remain in memory and cause permGen outofmemory once you repeat it a couple of times.
Now there are two ways to solve this:
1. Find the cause of Memory Leak or if there is any memory leak.
2. Increase size of PermGen Space by using JVM param -XX:MaxPermSize and -XX:PermSize.

A: Either optimize your program or increase java heap size with run time parameters.(-Xxx)

A: java.lang.OutOfMemoryError: PermGen space
Two step solution.
Step One : Alter your application launch configuration and add (or increase if present) the -XX:MaxPermSize parameter . This is a temporary step as if this is a live system most probably the extra memory will also get filled at some time in the future.But this will fix the error for now.
Step two : Release unnecessary resources. Make sure all database connections are closed. Load and unload classes judiciously.restructure you program to work with small amounts of data at a time. Analyse and Fix memory leaks

A: It is important to know, whether the PermGenError occurs after every depolyment, or after few ones.
If it is the first case, just increase the memory size for your PermGen.
If it is the second, you have some dead cows in your code. In this case, increasing memory size will only postpone the error, as your memory is still growing in size after every deployment. You have to profile your app like for example with jvisualvm (here is nice tutorial) and find some dead cows. It is important to understand, that PermGenError is not about the classes itself, but about classLoaders (Classloader leaks: the dreaded "java.lang.OutOfMemoryError: PermGen space" exception).
In my case (Glssfish server), the problem was the Log4j2 libs added to the web app. I had to add them also to the server  libs (domain-dir/lib), so that according to the Glassfish Class Loaders Hierarchy they where loaded by the Common classLoader.


text:
Dwayne Johnson makes amends for shoplifting at 7-Eleven in the past
Writer: Heidi Hsia
The Rock used to shoplift from this store
1 Dec - Dwayne Johnson recently atoned for his sin of "shoplifting chocolates" by buying all the chocolates from a 7-Eleven convenience store in Hawaii.
The actor recently posted a video of him visiting the same store he frequented as a teen in his hometown, saying, "I finally exorcised this damn chocolate demon that's been gnawing at me for decades. We were evicted from Hawaii in '87 and after all these years - I finally got back home to right this wrong."
Johnson shared that as a poor kid, he used to steal a king-sized Snickers bar every day from 7-Eleven for almost a year on his way to the gym as his pre-daily workout snack.
This is Dwayne Johnson at 15. Yes. We are not joking.
"The same clerk was there every day and always just turned her head and never busted me. I've exorcised a few big demons over the years (I still have a few left;) so I know this one seems VERY SILLY, but every time I come back home to Hawaii and drive by 7-Eleven... I always knew I needed to go in and clean out every Snickers bar they had - the right way," he added.
The "Black Adam" star, who bought all the Snickers that were on the shelf, also left the bags in the store, telling the cashier to just give the Snickers to anybody who looked like they were going to steal it so that they won't have to do what he did in the past.
At the same time, he also paid for the items bought for other customers who were lucky enough to be in the store at the same time.
"We can't change the past and some of the dumb stuff we may have done, but every once in a while, we can add a little redeeming grace note to that situation - and maybe put a big smile on some strangers' faces," he said.
I'll take that and that and that
This time, he pays for the Snickers
... and made their day
Cinema Online, 01 December 2022
Related Movies:
Black Adam (20 Oct 2022)
Jumanji: The Next Level (05 Dec 2019)
Jungle Cruise (29 Jul 2021)
Fast & Furious: Hobbs & Shaw (01 Aug 2019)
Fast And Furious 8 (13 Apr 2017)
Dailymotion article page COSG
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