Kurt Cobain maintained that re-acquiring the Raincoats 1979 debut meant more to him than making his first million. Thirty years since the release of their sophomore album, Odyshape, in 2011 I got to interview The Raincoats about their legacy, working with Robert Wyatt and clear up about their involvement – or not -in Ten Things I Hate About You.
17 Seconds: You're just about to re-issue your sophomore album Odyshape. What are your thoughts and memories of the album thirty years on?
Gina: What I do remember is Robert Wyatt coming to the studio and playing drums along to our very oddly timed playing of 'And Then It's OK', which we had recorded drummerless, speeding up and slowing down as the mood took us. Robert slipped seamlessly into the plan, and played as if he knew exactly where it was going, where it had come from and tuning in totally to its intention. Amazingly he made it all sound so much more focused than it had been. We had played for a while with Ingrid Weiss, a drummer, who was a 17 year old girl. She was very musical. She played drums on Odyshape and came up with the origins of the music for Shouting Out Loud. Sadly it didn't work out with her for reasons I can't even remember. Ingrid now is in Daisy Kitty and Lewis (their Mum) playing a mean double bass, still fabulous, musical and beautiful as ever.
We were still rehearsing some of the time in the squat basement at the end of Monmouth Road, and then later in Vicky's squat in Brixton. I had no hot running water at the time, and was at Hornsey art school in Alexandra Palace. I remember turning up to a rehearsal one day, to say I was leaving the band to concentrate on my studies at art school, then burst into tears and decided to I take time out of school to concentrate on The Raincoats. I did go back and finish my degree after two years out, and I made super 8 films and videos for my graduation.
When we did Odyshape, as we didn't have a drummer in the band, everything seemed more vague and on the other hand more open to possibilities, so we asked different people to play drums according to what we thought was best for each particular song. Richard Dudanski had already played with us before Palmolive, so we asked him to contribute. We also asked Charles Hayward, whose rehearsal studio we had used for a while and who ended up playing with us after the release of Odyshape. He is a great and sensitive musician and contributed a lot to the sound we had at the time he played with us, between projects he had with This Heat.
It was very interesting to have other people come in and see how personal music really is.
17 Seconds: What does the album title mean? It comes from the song (track five on the album) but what was the concept behind the title?
Gina: The title was a pun on the odyssey of a body. The idea that a body could have an ideal shape and it if did, what happens when a body doesn't live up to that ideal. it was at a time, when (as probably now) there seemed to be a body fascism. It was important for women to be this shape or that shape. Thanks to people like Beth Ditto, and hopefully The Raincoats, things have been broken down a little. Hair can be crazy, messy, outfits can be baggy or tight, inside out or upside down, we can be fat or thin, creative, playful, stylish and beautiful without having to subscribe to some fashion mag ideal.
17 Seconds: You're going to be playing your debut album at All Tomorrow's Parties this December. How did this come about -and was this something that you had to think about, given that you have done this before?
Gina: It seems a thing that bands are doing nowadays, playing whole albums, songs in the order of the album. We have performed The Raincoatsat the Scala once before and it was fun. Shirley walked across the stage with the vinyl album for side two and turned it over and then we played all the songs from the second side onwards.
Ana: This ATP is curated by Jeff Mangum (Neutral Milk Hotel) and, apparently, he requested we play the first album. When we did this at the Scala, at the end we came back to do another set of songs. We'll also do this at the festival.
We've done ATP twice before and I really enjoyed the experience. Thanks Jeff for having us.
17 Seconds: Who will the live band be? And who are the fulltime members of the Raincoats in 2011?
for over a decade on violin and guitar and often we will play with Jean Marc Butty on drums, who has also played with us for many years. In the US we have sometimes had Vice Cooler playing drums with us, instead of JM Butty.
17 Seconds: It's been mentioned numerous times how much the Raincoats meant to Kurt Cobain. Do you feel that this opened up an awareness of the band to people or have you felt frustrated that it took his enthusing to make many people aware of what you had achieved as a band?
Gina: We didn't expect the kind of enthusiasm and praise that we have subsequently got for our work. We did it for ourselves to stretch ourselves, to make the best most creative music we could and then move on. That we are now revisiting that work is strange, but fun and exciting.
Ana: Having someone like Kurt Cobain and others of his generation praising our work definitely made a lot of people aware of it and therefore wanting to see those songs played live. We love playing live so, doing this is such a pleasure. We didn't feel frustrated at all. We weren't playing together anymore, so people were interested in other things, which is the natural way –new ideas, new challenges, new enthusiasms. But, in reality, some were actually interested without us knowing. This was a huge and rewarding surprise.
Gina: Ray is reported as saying that he likes people who take an album track and make it a hit, not those who take a hit and make it an album track. A joke I suppose, but I have never heard any reporting that he liked our version!! Perhaps you could ask him yourself!!
Ana: He made that comment when he had his eyes on Chrissie Hynde… she made the album track 'Stop your sobbing' a hit.
17 Seconds: As well as the Raincoats, what other projects have the members got on the go (musical, or otherwise)?
Gina: Too many to mention. Ana is doing a new solo album and making drawings. I am painting, knitting/felting, filming, editing, writing recording. The Raincoats documentary is coming on and most recently, managed to get an interview with John Lydon which is the last one I really wanted to get, apart from needing to rerecord the one with Beth Ditto as the tape screwed up.
Ana: Yes, I've got an album in a very advanced state, but that last leap is taking a while. Maybe I'll finish it during grim winter. Good time to work, isn't it? I've been also making paintings and lots of drawings, which I'll be showing together with Shirley's photographs and Gina's videos in an exhibition, which is part of Pop Montreal music and arts festival, where we'll also be playing in September 2011. We'll be doing a tour in the USA and Canada – New York, Washington, Chicago, Detroit, Toronto and finish in Montreal.
17 Seconds: Interviewing Viv Albertine last year, it's clear that there was a link between The Slits and The Raincoats. Which other bands (if any!) did The Raincoats feel a kinship with?
Gina: I think we felt a kind of kinship with many of the bands in and around Rough Trade, Swell Maps, Scritti Politti, Young Marble Giants. But we were very shy and didn't really commune with other bands too much. I was a huge fan of The Slits, because it was them that made it seem possible to pick up a guitar and make a noise, as a girl. People love to go on about how terrible they were, (because on the whole, boys (oh.. vast generalization, I'm sorry!) tend to sit in their bedrooms perfecting their guitar skills till they are ready to 'go public') but The Slits were just amazing, brilliant because they were totally in the spirit of punk, fresh, unschooled, and without the preconceptions and boundaries of many bands. They were so feisty, creative, emotional, boisterous and that was such a treat to witness.
Ana: We definitely felt part of something and Rough Trade bands were the ones we felt closest to, partly because we met there but also because we did gigs together. The reason for this was not because we were on the same label but because there was a lot of mutual respect based on the wonderful music they created, and because they were great people too.
We also felt a certain kinship with other female bands, probably because there weren't that many around and we were all fighting for a bigger female presence. There still aren't as many as there should be.
17 Seconds: At the end of the nineties, The Raincoats appeared in Ten Things I Hate About You. How did this come about and how was the experience?
Gina: The script writer I think was more 'indie' and 'radical' than the film turned out to be. We are not actually featured in anyway in the film, except for the namecheck. it would have been brilliant if they had used a Raincoats track on the soundtrack. Shucks!!! Maybe in the indie remake!!
Ana: There was no experience to speak of. The boy mentioned us to the girl so he would appear cool and when the film came out someone told us there was this mention.
17 Seconds: As well as Nirvana and Sonic Youth, who else do you see as being indebted to the Raincoats?
Gina: I have no idea!!!!
Ana: Lots of people say that, especially female bands, but I think they would have done it anyway. You don't only get inspiration from one thing or person.
But if we have inspired anyone to do anything, then that is one mission accomplished.
17 Seconds: You make reference in the sleevenotes to friends using their vinyl copies of Odyshape to make fruit bowls out of. This is just as joke, right…?
limb for some of my friends and they just didn't get it. I don't think Ana or I ever envisaged ourselves having a group, playing live or making records and when we got the opportunity we took the bull by the horns and stretched ourselves creatively as much as we could. Historically this has proved to be a good thing, but some of the time I felt quite vulnerable and was unsure that what we were doing was of any value. I am proud that we stuck to our guns and did not try to please others, just ourselves. There are obviously moments on all our records I think could be better or different, but they are a testament to where we were at the time.
Ana: My experience is different from Gina's. I think a lot of people, specially in other European countries, appreciated the quirkiness, guts, risk, variety and challenge of that album. We were in a different place as people and musicians and we let the new music reflect that. The first album is more punky but punk was all about challenge and thinking for yourself, about looking around and to yourself, about feeling free to find your own path, and Odyshape was as part of our path as the first album.
17 Seconds: As this is for a Scots-based blog, Is there ANY chance of Scottish dates any time in the future?
Gina: Invite us, (and if it makes sense financially!!) Ana and I will be there, bearing in mind our drummer comes from France and Anne from tippy top of Scotland!!
Ana: Anne wouldn't be that far then!
I remember one of the times we played in Scotland, it was Summer and we came back after the gig in a van, late, and soon after it got dark, it got light again. I'd never experience such a short night before the day broke.
One of my favourite eras of music is 1976-1982, the period that gave us punk and its even more interesting fall-outs. One of the key players in the scene was Viv Albertine. At the point of this interview, she had started recording again after a gap of many years. She had just released an EP, Flesh, which would be followed by an album, The Vermilion Border, and her autobiography Clothes, Clothes, Clothes, Music, Music, Music, Boys, Boys, Boys. Last year, I even got to meet her at the Edinburgh Book Festival, where she signed my copy of The Slits' debut album, Cut.
Who would have thought it? 17 Seconds is 10 years old this month. It's been a labour of love, but I've loved labouring over it. So, for what it's worth, I'm going to share some of the things that I've enjoyed doing most over the years.
Not that he doesn't go back occasionally. In fact, this year on November 5, Roy Harper will play his seventieth birthday concert at London's Royal Festival Hall. His profile has been helped along of late by endorsements from a younger generation of musicians, including Joanna Newsom and Fleet Foxes, amongst others. I ask him if he can hear his influence in the new generation of acts.
As well as his seventieth Birthday concert, he is re-issuing his back catalogue and is also set to release a new compilation, entitled Songs of Love and Loss, Volumes 1 & 2. Given the back catalogue that he has amassed, over the course of over forty years of recording, how did he go about selecting which songs made the cut?
'Ouch,' I say, somewhat involuntarily. I ask him about some of the musical collaborations he's been involved in over the years. Famously, Led Zeppelin III closes with the track 'Hats Off to (Roy) Harper.' Although he wasn't involved with the track, he did collaborate with the band members, and clearly has a lot of time for both Robert Plant and Jimmy Page on not just musical, but personal levels as well.
As well as collaborating with the Zeppelin boys, he also worked with Pink Floyd. I ask him about his contribution to Floyd's 1975 album, Wish You Were Here. Harper sang lead vocals on the track 'Have A Cigar.' He is, politely, rather guarded, about his work on this album, the only time during our conversation I sense some reluctance on his part.
'Roger [Waters, Floyd singer, songwriter and bassist] wrote a song he couldn't sing, basically,' he states. 'It was two semitones too high for either of them [Waters and Floyd guitarist David Gilmour] to sing. They were going to shelve it.' Harper however contributed his vocals to the track about the record exec who's purely out to make money, and it's gone on to be performed by Floyd's members since then. 'Roger's been singing it ever since -or trying to!' he chuckles. Of course, the reason why he was asked to perform on Wish You Were Here was that he was recording his own album, HQ, in the next door studio at Abbey Road. Known in the US and Canada under the title of the final, closing track 'When An Old Cricketer Leaves The Crease' which is probably the best known song in a very impressive catalogue. I ask him if he's comfortable with this being seen as his epitaph.
'There's plenty of songs that rival it, but it happens to ring a bell for people -and it's a bell I purposely rang.' It's a hugely affecting song, from its' deceptively simple melody, beautiful David Bedford arrangement and brass from the Grimethorpe Colliery band. 'Its' message is of someone looking back at these Islands, at this peculiar little corner of England. He adds: 'You say that there was some sort of perception that cricket was played by a certain class, but in your perfect Eleven [the number of players on a side in cricket] it's the blacksmith who traditionally gets the job as the fast bowler! He's the player who has to come in!' He is still a cricket fan -as well as being a lifelong supporter of Manchester City.
Earlier in the conversation he had spoken about his shared earlier influences in common with the Floyd and Zeppelin boys being Skiffle. But -and if you've heard his music you should know this – it's revealing that his early influences were the romantic poets, particularly Keats and Shelley. I tell him that his comment about 'iTunes and the dark satanic mills' reminded me of another poet who blew me away as a teenager: William Blake.
Not surprisingly, the man who wrote Songs of Innocence and Experience and 'Jerusalem' was a huge influence on Roy Harper. Partly, this is to do with Harper's well-documented distrust of organised religion. 'Blake's sensibilities told him other things, in an age when it was impossible not to be a Christian,' he states firmly. 'This was the age of reason, things were being discussed on a broader scale than ever before. I think of Blake as a hugely important figure. There's some kind of alternative ghost in the background – I love him because of that. You could see him struggling with that, and knowing that it was going to be discussed by people like me. He was a man worthy of being lauded in any age,' he says, decisively.


text:
package ru.job4j;

/**
* Class Rotation.
*/
public class Rotate {
	/**
	* Rotate square array.
	* @param values square array.
	* @return rotated array.
	*/
	public int[][] rotateSquareArray(int[][] values) {
	    int[][] result = new int[values.length][values.length];
        int k = values.length - 1;
        for (int i = 0; i < values.length; i++) {
            for (int j = 0; j < values.length; j++) {
                result[j][k] = values[i][j];
            }
            k--;
        }
		return result;
	}
}

redpajama_set_name: RedPajamaGithub


Wise Chat Pro and BuddyPress groups integration.
BuddyPress is an amazing plugin that helps to build social networking websites based on WordPress. Among its many features like news feed, profiles, friends, groups there is a natural need for some kind of real-time communication service. Wise Chat Pro offers such facility. It integrates with BuddyPress groups. All group members gain access to the chat channel which is dedicated for each group exclusively. Additionally, it is possible to give administrators or mods Wise Chat Pro moderation permissions.
3. After the two settings are turned on pick one of your BuddyPress groups, log in as administrator of this group and go to "Manage" tab on the group's main page. You will see "Chat" tab in the group's secondary menu. Click on this tab, select "Enable Chat" option and save the changes.
4. From now Wise Chat Pro is enabled for this group. All members who have access to the group will gain access to Wise Chat Pro after clicking on "Chat" tab in the main menu of the group. Each group utilizes its own separate chat channel. In the following example we set a custom name for the tab. We named it "Chat Room" (see the previous step).
1. BuddyPress integration allows to give moderation rights to group's administrators or mods.


text:
<?php

namespace TwbsHelper\View\Helper;

/**
 * Abstract helper for group rendering
 */
abstract class AbstractGroup extends \TwbsHelper\View\Helper\AbstractHtmlElement
{
    protected static $groupClass;
    protected static $groupTag;
    protected static $helperName;

    /**
     * Render a group
     * @param array $aItems Array with the elements of the group
     * @param array $aOptionsAndAttributes Attributes for the group tag.
     * @param boolean $bEscape Escape the items.
     * @return string The group XHTML.
     */
    public function __invoke(array $aItems, array $aOptionsAndAttributes = [], bool $bEscape = true): string
    {
        return $this->htmlElement(
            static::$groupTag,
            $this->setClassesToAttributes($aOptionsAndAttributes, [static::$groupClass]),
            $this->renderGroupItems($aItems, $bEscape),
            $bEscape
        );
    }

    protected function renderGroupItems(array $aItems, bool $bEscape = true): string
    {
        $sContent = '';

        $oItemHelper = $this->getView()->plugin(static::$helperName);

        foreach ($aItems as $aItem) {
            $aArguments = \Laminas\Stdlib\ArrayUtils::isList($aItem) ?
                [$aItem[0], $aItem[1] ?? [], $aItem[2] ??  $bEscape]
                : [$aItem, [], $bEscape];

            $sContent .= ($sContent ? PHP_EOL : '') . $this->renderGroupItem(
                $oItemHelper,
                $aArguments
            );
        }
        return $sContent;
    }

    protected function renderGroupItem(
        \Laminas\View\Helper\HelperInterface $oItemHelper,
        array $aArguments
    ): string {
        return call_user_func_array([$oItemHelper, '__invoke'], $aArguments);
    }
}


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text:
\section{Introduction}
It is accepted that the density perturbations collapse and cool due to hydrogen molecules ($\mathrm{H_2}$) to form so called population III (popIII) stars (Bromm et al. 1999, 2002; Abel et al. 2000, 2002; Yoshida et al. 2008). PopIII is expected to form in halos with $\ge 10^6 M_\odot$ (Tegmark et al. 1997). If PopIII is massive star, it is expected to affect neighbor clouds via radiative feedbacks. Radiative feedbacks cause ionization and dissociation. Although ionization photon tends to be prevented from spreading out of halos because of large opacity of hydrogen atoms, dissociation photon tends to spread out of halos (Kitayama et al. 2004). Thus, some regions are expected not to be ionized but to be photodissociated. We consider the filamentary clouds in such a region.

Filamentary clouds are possible origin of stars. In general, non-spherical gas cloud tends to become sheet-like cloud, and sheet-like cloud tends to fragment into the filamentary clouds (Miyama et al. 1987). In numerical cosmological simulations of first star formation, filamentary structure is frequently seen (e.g., Abel et al. 1998; Bromm et al. 1999; Greif et al. 2006). Recently, many filamentary structures have been found through the $Herschel$ Gould Belt Survey (Andr\'e et al. 2010). A filamentary cloud is possible to fragment into many quasi-spherical clouds (Nagasawa 1987; Inutsuka $\&$ Miyama 1997). These spherical clouds are expected to become stars or other astronomical objects. We investigate how this process exceeds when first stars form.

There are previous works about fragmentation of the filamentary cloud (Uehara et al. 1996 ; Nakamura $\&$ Umemura 1999, 2001, 2002; Flower 2002; Omukai $\&$ Yoshii 2003). Among these, Nakamura $\&$ Umemura (1999, 2001, 2002) used one-dimensional hydrodynamical calculations and two-dimensional hydrodynamical calculations. The authors considered many cases with various initial density, temperature, line mass, and initial fraction of $\mathrm{H_2}$. It is found that fragment mass is $1-500M_\odot$ and has a bimodal distribution when initial $\mathrm{H_2}$ fraction is $10^{-3}$. However, the effect of the external radiation was not considered. Hence, these works is applicable only to first star formation. Among works mentioned above, Omukai $\&$ Yoshii (2003) considered the external dissociation radiation. Their work is applicable to formation of second-generation stars. They calculated the thermal evolution of the filamentary cloud under the isotropic external radiation with one-zone model assuming free-fall. They assumed that the filamentary cloud fragments when its density becomes $100$ times higher than the loitering point. Under this assumption, Omukai $\&$ Yoshii (2003) concluded that the effect of the external dissociation radiation decreases fragment mass.

In Bessho $\&$ Tsuribe (2012) (hereafter Paper I), we investigated collapse and fragmentation of a filamentary clouds under the isotropic external radiation using one-zone models. We assumed that the external radiation turns on when the filamentary cloud forms. By taking into accounts pressure effect explicitly, we found that the filamentary clouds with low initial density ($n_0 \le 10^2 \mathrm{cm^{-3}}$) suffer photodissociation and fragment into very massive clouds ($\sim 10^{4-5} M_\odot$). It was found that the effect of the external radiation increases fragment mass. The evolution of the filamentary clouds with high initial density ($n_0 > 10^2 \mathrm{cm^{-3}}$) or with sufficiently large line mass is not affected by the external radiation owing to self-shielding. In Paper I, at first, we assumed the uniform filamentary clouds with homologous collapse. However, in realistic situations, filamentary clouds are expected to collapse in run-away fashion. Hence, in Paper I, we also introduced "rarefied filament model" as an improved model which includes the effect of run-away collapse partly. In rarefied filament model, line mass of collapsing core decreases as rarefaction wave propagates from the cloud surface. As a result of the rarefied filament model, we found that the effect of the external radiation increases fragment mass. However, this result is apparently inconsistent with Omukai $\&$ Yoshii (2003).

The purpose of the present paper is to investigate whether or not fragment mass increases owing to the effect of the external radiation and to clarify the reason why our result is inconsistent with Omukai $\&$ Yoshii (2003). For this purpose, we extend our previous investigation using the one-dimensional model which includes the full characteristics of run-away collapse and have more realistic results. Furthermore, in this paper, we also consider the further evolution of each fragment.

We assume that the external radiation is isotropic. Intensity of the external dissociation radiation is set according to distribution of intensity of the dissociation radiation at redshift $z \sim 10$ (Dijkstra et al. 2008). The intensity which we consider is moderate ($\S 2.2$), and we consider the situation where the dissociation radiation originates from halos out of a halo including the filamentary cloud.

In Paper I, we concentrated on the case where the external radiation turns on when the filamentary cloud forms ($n \ge 10\mathrm{cm^{-3}}$). To clarify the reason of the apparent difference of the conclusions between us and Omukai $\&$ Yoshii (2003), we also consider the case where the external radiation turns on at lower density ($n=0.1\mathrm{cm^{-3}}$) as in Omukai $\&$ Yoshii (2003).

In $\S 2$, we describe our model for the filamentary clouds. We present numerical results in $\S 3$. In $\S 4$, we investigate the reason for the difference between us and Omukai $\&$ Yoshii (2003). $\S 5$ is devoted to conclusions and discussion.

\section{Model for the filamentary clouds}
\subsection{Basic equations}
We assume the axisymmetric filamentary cloud. We do not consider dark matter for simplicity. This simplicity gives us a good approximation in the case with high initial density. In the case with low initial density, the effect of dark matter gravity is underestimated. Hydrodynamical equation of motion in Lagrangian form is given by
\begin{eqnarray}
\frac{Dv}{Dt}=-\frac{2Gl}{r}-2\pi r \frac{\partial P}{\partial l},
\end{eqnarray}
where $v$ is velocity in the cylindrical radial direction, $G$ is gravitational constant, $l$ is line mass within cylindrical radius $r$, and $P$ is pressure for ideal gas given by
\begin{eqnarray}
P=n k_B T,
\end{eqnarray}
with number density $n$, temperature $T$, and Boltsmann constant $k_B$.

We also solve energy equation given by
\begin{eqnarray}
\frac{du}{dt}=-P\frac{d\ }{dt}\frac{1}{\rho}-\frac{\Lambda_{\mathrm{net}}}{\rho}
\end{eqnarray}
where $\rho$ is density and $u$ is thermal energy per unit mass,
\begin{eqnarray}
u=\frac{1}{\gamma_{\mathrm{ad}}-1} \frac{k_B T}{\mu m_{\mathrm{H}}}
\end{eqnarray}
with adiabatic index $\gamma_{\mathrm{ad}}$, mean molecular weight $\mu$, and mass of a hydrogen atom $m_{\mathrm{H}}$. The symbol $\Lambda_{\mathrm{net}}$ in equation (3) is cooling rate per unit volume including lines of $\mathrm{H}$, lines of $\mathrm{H_2}$, lines of $\mathrm{HD}$, and chemical heating/cooling. Since continuum processes hardly change the evolution of the filamentary clouds (Paper I), we neglect them. As for lines, we estimate cooling rate from detailed balance of population of energy levels. The escape probability for emission by the transition between level $i$ and $j$ is given by
\begin{eqnarray}
\beta_{ij}=\frac{1-e^{-\tau_{ij}}}{\tau_{ij}},
\end{eqnarray}
with assuming the velocity profile $v_r (r) \propto r$ (Castor 1970). The cooling rate is multiplied by this escape probability. Optical depth, $\tau_{ij}$, is given by
\begin{eqnarray}
\tau_{ij}&=&\int^{R_{\mathrm{out}}}_r \kappa_{ij} (r^\prime) \ dr^\prime \nonumber \\
&=&\int^{R_{\mathrm{out}}}_r \frac{h \nu_{ij}}{8 \pi \Delta \nu_{ij}} (n_j B_{ji}-n_i B_{ij}) dr^\prime,
\end{eqnarray}
where $R_{\mathrm{out}}$ is radius of the outer boundary, $\kappa_{ij}$ is opacity for lines, $h \nu_{ij}$ is energy difference between levels $i$ and $j$, $n_i$ ($n_j$) is the level population at level $i$ ($j$), $B_{ij}$ and $B_{ji}$ are the Einstein $B$-coefficients, and $\Delta \nu_{ij}=\nu_{ij}/c \sqrt{2k_B T/\mu m_{\mathrm{H}}}$ is the thermal Doppler width of transition line $i \rightarrow j$.

We consider non-equilibrium chemical reactions by solving following equation for each fluid element :
\begin{eqnarray}
\frac{df_i}{dt}=\sum_{j,\ k} k_{ijk} f_j f_k n + \sum_j k_{ij} f_j ,
\end{eqnarray}
where $k_{ijk}$ and $k_{ij}$ are reaction rates for formation and destruction of speices $i$, and $f_i$ is fraction of species $i$. We consider fourteen species : $\mathrm{H}$, $\mathrm{H^+}$, $\mathrm{H^-}$, $\mathrm{H_2}$, $\mathrm{H_2^+}$, $\mathrm{He}$, $\mathrm{He^+}$, $\mathrm{He^{++}}$, $\mathrm{D}$, $\mathrm{D^+}$, $\mathrm{D^-}$, $\mathrm{HD}$, $\mathrm{HD^+}$, and $\mathrm{e^-}$. We consider 26 chemical reactions concerned with $\mathrm{H}$ and $\mathrm{He}$ taken from Nakamura $\&$ Umemura (2001), photodissociation of $\mathrm{H_2}$ (equation 10), and 18 chemical reactions concerned with $\mathrm{H}$ and $\mathrm{D}$ taken from Nakamura $\&$ Umemura (2002). We solve equation (7) with implicit integrator.

We solve equations (1)-(7) using 200 spatial meshes in cylindrical radial direction. As for initial interval of meshes, we set $\Delta r_{i+1} = 1.01 \Delta r_i$, where $\Delta r_i \equiv r_{i+1}-r_i$. Hence, spatial resolution is much better in the central region. The mesh size $\Delta r_i$ is checked to be shorter than $1/4$ of local Jeans length\footnote{The exact definition of Jeans length is given by
\begin{eqnarray}
\lambda_{\mathrm{J}}=\biggl(\frac{\pi}{G \mu m_{\mathrm{H}} n_c} \biggr)^{1/2} c_s.
\end{eqnarray}
} at all times (Truelove et al. 1997). We set outer boundary to be $10R_0$ as a sufficiently large value, where $R_0$ is the effective radius given by
\begin{eqnarray}
R_0=\sqrt{\frac{2fk_BT_0}{\pi G \mu^2 m_{\mathrm{H}}^2 n_0}},
\end{eqnarray}
with line mass parameter $f$ (equation 17), initial temperature $T_0$, and initial number density at the center $n_0$. As for the outer boundary condition, we assume that the external pressure is zero.

\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure1.eps}} \\
\end{tabular}
\caption{Error of density distribution of isothermal equilibrium filamentary cloud ($T=300\mathrm{K}$) for the numerical results with $100$ meshes and $200$ meshes. The symbol $\rho_{\mathrm{ana}}$ is analytic solution, and $\rho_{\mathrm{com}}$ is numerical results.}
\end{center}
\end{figure}

We solve equation (1) in the second-order-accurate finite-difference scheme with the artificial viscosity (Richtmyer $\&$ Morton 1967). We calculate in the same way as Thoul $\&$ Weinberg (1995), except for cylindrical geometry. To check accuracy of our code, first, we calculate the density distribution of isothermal equilibrium filamentary cloud ($T=300\mathrm{K}$) with 100 and 200 meshes, and fixed time step. Drag term $-2v(r)/dt$ is added to equation of motion and is eliminated after the step number reaches $125$ for case with $100$ meshes and $250$ for case with $200$ meshes. After $250$ steps ($100$ meshes) and $500$ steps ($200$ meshes), we have error of density distribution shown in figure 1. Error for case with $100$ meshes is $4$ times of error for case with $200$ meshes. Hence, our code is second-order-accurate in space.

Second, we check temporal accuracy of our code in time. We calculate collapse of pressure-less uniform filamentary cloud in free-fall state. Analytic solution is given by
\begin{eqnarray}
\int^{\sqrt{-\log F(t)}}_{0} e^{-x^2} dx = \sqrt{\pi G \rho(0)} t,
\end{eqnarray}
where $F(t)=r(t)/r(0)$, $\rho(0)$ is the initial density. Time step is set to be $\Delta t=10^{-4} t_{\mathrm{ff}}(t=0)$ and $2\Delta t$. Calculation is continued until the density becomes $100$ times of the initial density. In the case with $\Delta t$, $F$ at the end of calculation is $0.0913290$. In the case with $2\Delta t$, $F$ at the end of calculation is $0.09132307$. Analytic solution predicts $F=0.9132284$. Error with $2\Delta t$ is $4$ times larger than $\Delta t$. Hence, our code has second-order-accuracy in time.

\subsection{External radiation}
We assume that the external dissociation radiation is isotropic. Intensity of the external radiation is set according to Dijkstra et al. (2008). Dijkstra et al. (2008) calculated the probability distribution of mean intensity of the dissociation radiation at redshift $z \sim 10$ by estimating mean intensity of the dissociation photon from the surrounding halos to a single halo. In this paper, we use mean intensities whose probability is $0.4$ and $0.06$ as in Paper I. The external radiation is assumed to be thermal radiation of $120M_\odot$ star, and we determine surface temperature ($T_{\mathrm{sur}}=95719\mathrm{K}$) according to Schaerer (2002). We assume that the external radiation turns on when the filamentary clouds forms in $\S 3$. In $\S 4$, we change the density when the external radiation turns on.

We calculate the photodissociation reaction of $\mathrm{H_2}$,
\begin{eqnarray}
\mathrm{H_2} + \gamma \rightarrow \mathrm{H_2}^\ast \rightarrow 2 \mathrm{H},
\end{eqnarray}
(solomon process) where $\gamma$ is photon with $12.4 \mathrm{eV}$ and $\mathrm{H_2}^\ast$ is excited state of $\mathrm{H_2}$. The reaction rate is given by
\begin{eqnarray}
k_{\mathrm{2step}} = 1.4 \times 10^9 f_{\mathrm{sh}} J_{\mathrm{ext}} \ \mathrm{s^{-1}},
\end{eqnarray}
where $J_{\mathrm{ext}}$ is mean intensity of the external radiation at the surface of the filamentary cloud and $f_{\mathrm{sh}}$ is self-shielding function,
\begin{eqnarray}
f_{\mathrm{sh}}=\mathrm{min} \biggl[ 1,\ \biggl(\frac{N_{\mathrm{H_2}}}{10^{14} \mathrm{cm^{-2}}} \biggr)^{-3/4} \biggr],
\end{eqnarray}
where $N_{\mathrm{H_2}}$ is column density of $\mathrm{H_2}$ (Draine $\&$ Bertoldi 1996) estimated as
\begin{eqnarray}
N_{\mathrm{H_2}}(r)= \int^{R_{\mathrm{out}}}_{r} n_{\mathrm{H_2}} (r^\prime) dr^\prime.
\end{eqnarray}

\subsection{Fragmentation of the filamentary cloud}
There are two important timescales during the collapse of filamentary clouds. One is timescale for density evolution, $t_{\mathrm{dyn}} \equiv \rho_c/\dot{\rho_c}$, and the other is timescale for fragmentation, $t_{\mathrm{frag}} \equiv 5.17/\sqrt{2\pi \rho_c G}$ (Nagasawa 1987). The latter is the timescale during which the fastest growing mode of perturbation grows to non-linear. If the fastest growing mode has time enough to grow to non-linear before the fastest growing mode changes, the filamentary cloud is expected to fragment. Thus, we assume that the filamentary clouds fragment when $t_{\mathrm{dyn}}>t_{\mathrm{frag}}$. Once condition for fragmentation is satisfied, it has been satisfied after that.

We estimate fragment mass by integrating region with the density higher than 10$\%$ of central density $n_c$,
\begin{eqnarray}
M_{\mathrm{frag}}=\lambda_{\mathrm{frag}} \int^{r(n=0.1n_c)}_{0} 2\pi r^\prime \rho dr^\prime,
\end{eqnarray}
where
\begin{eqnarray}
\lambda_{\mathrm{frag}}=2\pi \frac{c_s}{0.288 \sqrt{4 \pi G \mu m_{\mathrm{H}} n_c}}
\end{eqnarray}
is the wave length of the fastest growing mode for equilibrium filamentary clouds (Nagasawa 1987) and $c_s$ is sound speed. Since $\lambda_{\mathrm{frag}} \propto \rho^{-1/2}$, fragment mass is smaller when the filamentary cloud reaches higher density before fragmentation. Since interval of integration in equation (14) is approximately Jeans length, Jeans mass at fragmentation is close to fragment mass (see $\S 3.3$).

\subsection{Parameters and initial conditions}
In this paper, we treat three physical quantities as parameters. First is initial density $n_0$, second is normalized mean intensity of the external radiation,
\begin{eqnarray}
J_{21} \equiv \frac{J_{h\nu=13.6\mathrm{eV},\mathrm{ext}}}{10^{-21} \mathrm{erg\ cm^{-2} s^{-1} Hz^{-1} sr^{-1}}},
\end{eqnarray}
and third is line mass parameter\footnote{If a filamentary cloud forms as a result of fragmentation of the fastest growing mode in a sheet-like cloud, the typical value of $f$ is $2$ (Miyama et al. 1987).},
\begin{eqnarray}
f \equiv \frac{\pi G \mu^2 m_{\mathrm{H}}^2 n_0}{2k_B T_0} R_0^2.
\end{eqnarray}
Line mass parameter is important in the view point of dynamical evolution. Initial density $n_0$ is important for thermal evolution. With respect to photodissociation, mean intensity $J_{21}$ and initial density $n_0$ are important.

We consider cases with $\log_{10} n_0=1$, $1.5$, $2$, $2.5$, $3$, $3.5$, $4$, $4.5$, $5$, $5.5$, and $6$ for $n_0$ and $f=1.5$, $2$, $2.5$, $3$, $3.5$, $4$, $5.5$, and $6$ for $f$. For $J_{21}$, we consider $J_{21}=0$, $1$, $6.5$, and $10$. According to Dijkstra et al. (2008), the case with $J_{21}=1$ represents the weak external radiation case, $J_{21}=6.5$ is mean intensity with the highest probability ($0.4$), and $J_{21}=10$ represents the strong radiation case whose probability is $0.06$.

We assume initial density distribution as
\begin{eqnarray}
n(r)=n_0 \biggl( 1+ \frac{r^2}{R_0^2} \biggr)^{-2}
\end{eqnarray}
with $R_0$ given in equation (8). With $f=1$, equation (18) represents equilibrium density distribution for the isothermal filamentary cloud (Ostriker 1964). In this paper, we concentrate on collapsing filamentary cloud with $f>1$. Initial velocity distribution is assumed to be
\begin{eqnarray}
v(r)=- \frac{c_s}{R_0+ \sqrt{R_0^2+r^2}} r.
\end{eqnarray}
Equation (19) indicates that infall velocity is proportion to radius at $r \rightarrow 0$ and is constant ($\sim -c_s$) at $r \rightarrow \infty$. Although the actual initial velocity may be different from equation (19) depending on the detail of dynamical evolution of the filamentary cloud formation, results in this paper will not change qualitatively unless initial velocity is much faster than a few times of equation (19).

As initial temperature, we adopt $T_0=300\mathrm{K}$, assuming that the filamentary cloud forms after the cloud undergoes $\mathrm{H_2}$ cooling. We also adopt $f_{\mathrm{H_2}}=10^{-4}$ and $f_{\mathrm{e}}=10^{-4}$. As for the value of $f_{\mathrm{H_2}}$, we refer the result in Paper I. Fraction of electron is set in order not to change $f_{\mathrm{H_2}}$ artificially via $\mathrm{H^-}$ channel. Initial fraction of proton is set to be $f_{\mathrm{p}}=10^{-4}$ for charge conservation. We assume $[\mathrm{H}]/[\mathrm{D}]=4 \times 10^{-5}$, which is consistent with observations of the deuterium Ly$\alpha$ feature (e.g., O'Meara et al. 2001). Initial fraction of the others is set to be zero.

\section{Results of one-dimensional hydrodynamical calculations}
\subsection{Cases without the external radiation}
To investigate the effect of the external radiation, at first, we show the results of the cases without the external radiation.

\subsubsection{Low density filamentary cloud with small line mass}
\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure2.eps}} \\
\end{tabular}
\caption{Evolution of the temperature (a), $f_{\mathrm{H_2}}$ and $f_{\mathrm{HD}} \times 10^4$ (b), the heating and cooling rate (c), and $t_{\mathrm{dyn}}$ and $t_{\mathrm{frag}}$ (d), respectively, as a function of the central density for the case with $(f,n_0,J_{21})=(1.5,10 \mathrm{cm^{-3}},0)$. In the diagram (c), "adiabatic" denotes the adiabatic heating, "$\mathrm{H_2}$" does the $\mathrm{H_2}$ line cooling, "$\mathrm{HD}$" does the $\mathrm{HD}$ line cooling, and "chemical" does the chemical heating or cooling.}
\end{center}
\end{figure}

First, we show the results for the case with low initial density and small line mass, $(f,n_0,J_{21})=(1.5,10\mathrm{cm^{-3}},0)$ (figure 2). In the early stage of collapse, $\mathrm{H_2}$ cooling dominates adiabatic heating a little, and temperature decreases. After the density reaches $n \sim 10^3 \mathrm{cm^{-3}}$, adiabatic heating dominates $\mathrm{H_2}$ cooling. In $n > n_{\mathrm{crit}} \sim 10^4 \mathrm{cm^{-3}}$, $\mathrm{H_2}$ cooling rate is proportional to $n$, while it is proportional to $n^2$ in $n < n_{\mathrm{crit}}$. Hence, since cooling time becomes constant in $n > n_{\mathrm{crit}}$, dynamical time becomes constant and longer than fragmentation time. When $n$ reaches $\sim 2 \times 10^5 \mathrm{cm^{-3}}$, condition for fragmentation is satisfied with $M_{\mathrm{frag}} \sim 1220 M_\odot$. To ensure that fragmentation occurs, we continue to calculate the evolution until free-fall time has past after the condition for fragmentation is first satisfied. Once condition for fragmentation is satisfied, it has been satisfied.

\subsubsection{Low density filamentary cloud with large line mass}
\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure3.eps}} \\
\end{tabular}
\caption{Same as figure 2, but $(f,n_0,J_{21})=(6,10\mathrm{cm^{-3}},0)$.}
\end{center}
\end{figure}

Next, we show the result for the case with low initial density and large line mass, $(f,n_0,J_{21})=(6,10\mathrm{cm^{-3}},0)$ (figure 3). Owing to larger line mass, the filamentary cloud collapses to higher density than figure 2. Collapse continues up to high density ($n \sim 10^6 \mathrm{cm^{-3}}$), and the filamentary cloud fragments. Fragment mass is $\sim 490 M_\odot$. Until fragmentation, adiabatic heating and $\mathrm{H_2}$ cooling balance, and temperature is approximately constant ($T \sim 350 \mathrm{K}$).

\subsubsection{High density filamentary cloud with small line mass}
\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure4.eps}} \\
\end{tabular}
\caption{Same as figure 2, but $(f,n_0,J_{21})=(1.5,10^6\mathrm{cm^{-3}},0)$.}
\end{center}
\end{figure}

As the final example, we show the result for the case with high initial density and small line mass, $(f,n_0,J_{21})=(1.5,10^6\mathrm{cm^{-3}},0)$ (figure 4). In the early stage of collapse, Adiabatic heating dominates $\mathrm{H_2}$ cooling and temperature increases. During collapse, $\mathrm{H_2}$ cooling rate increases and approximately balances with adiabatic heating rate at $n \sim 3 \times 10^6 \mathrm{cm^{-3}}$. After temperature decreases a little, fragmentation condition is satisfied at $n \sim 10^7 \mathrm{cm^{-3}}$ since collapse is suppressed owing to high temperature. Fragment mass is $\sim 370 M_\odot$.

In summary, in the cases without the external radiation, the filamentary cloud undergoes approximately isothermal states and fragments. This feature comes from the fact that $\mathrm{H_2}$ cooling and adiabatic heating compete each other. The results in this subsection are similar to previous works (Nakamura $\&$ Umemura 2001, 2002). For the parameter set same as figure 2, in Paper I, fragment mass was $23 M_\odot$ in the uniform model and $3500 M_\odot$ in rarefied filament model. Fragment mass $1220 M_\odot$ in the one-dimensional model is close to the results of the rarefied filament model. This result indicates that the effect of run-away collapse is important to estimate fragment mass.

\subsection{Cases with the external radiation}
In this subsection, using the same parameters as figure 2, 3, and 4, we investigate how the external radiation changes the thermal evolution and fragment mass of the filamentary cloud.

\subsubsection{Low density filamentary cloud with small line mass and strong radiation}
\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure5.eps}} \\
\end{tabular}
\caption{Same as figure 2, but $(f,n_0,J_{21})=(1.5,10\mathrm{cm^{-3}},10)$.}
\end{center}
\end{figure}

First, we show the result for the case with low initial density, small line mass, and strong external radiation, $(f,n_0,J_{21})=(1.5,10\mathrm{cm^{-3}},10)$ (figure 5), where the external radiation is added to the case of figure 2. This case would be affected by the external radiation because of low density. Most of $\mathrm{H_2}$ are photodissociated in the early stage of collapse, and temperature increases adiabatically. The filamentary cloud fragments into very massive fragments ($\sim 2.4 \times 10^5 M_\odot$) at $n \sim 30 \mathrm{cm^{-3}}$. This result demonstrates that in the case with low initial density and small line mass the external radiation increases fragment mass and changes the thermal evolution.

\subsubsection{Low density filamentary cloud with large line mass and strong radiation}
\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure6.eps}} \\
\end{tabular}
\caption{Same as figure 2, but $(f,n_0,J_{21})=(6,10\mathrm{cm^{-3}},10)$.}
\end{center}
\end{figure}

Next, we show the result for the case with low initial density, large line mass, and strong external radiation, $(f,n_0,J_{21})=(6,10\mathrm{cm^{-3}},10)$ (figure 6), where the external radiation is added to the case of figure 3. This case is also excepted to be affected by the external radiation because of low density. However, the filamentary cloud may collapse up to higher density than figure 5 because of large line mass. In figure 6, it is seen that most of $\mathrm{H_2}$ is photodissociated in the early stage of collapse and temperature increases adiabatically as in figure 5. However, since the filamentary cloud is more massive than in figure 5, stronger gravity and large inertia help collapse. Fragmentation does not occur during early adiabatic phase, and collapse continues until the density becomes higher than in figure 5. At $n \sim 10^2 \mathrm{cm^{-3}}$, $\mathrm{H_2}$ starts to form and shields itself from the external radiation. The filamentary cloud starts to cool owing to $\mathrm{H_2}$ cooling. After $n \sim 10^3 \mathrm{cm^{-3}}$, Since $\mathrm{H_2}$ cooling balances with adiabatic heating, temperature becomes nearly constant ($T \sim 400 \mathrm{K}$). The filamentary cloud fragments into clouds with $\sim 590 M_\odot$ at $n \sim 10^6 \mathrm{cm^{-3}}$. Fragment mass and density at fragmentation are similar to the case without the external radiation (figure 3). In the case with large line mass ($f=6$), it is found that fragment mass is hardly affected by the external radiation although the evolution of temperature is affected by the external radiation in the early stage of collapse.

\subsubsection{High density filamentary cloud with small line mass and strong radiation}
\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure7.eps}} \\
\end{tabular}
\caption{Same as figure 2, but $(f,n_0,J_{21})=(1.5,10^6\mathrm{cm^{-3}},10)$.}
\end{center}
\end{figure}

Finally, we show the result for the case with high initial density, small line mass, and strong external radiation, $(f,n_0,J_{21})=(1.5,10^6\mathrm{cm^{-3}},10)$ (figure 7), where the external radiation is added to the case of figure 4. This case may not be affected by the external radiation because of high density. Since initial density is high enough to shield the filamentary cloud from the external radiation, $\mathrm{H_2}$ near the center of cloud is not photodissociated. The evolution of temperature at the center is hardly affected by the external radiation and is similar to figure 4. The filamentary cloud fragments into clouds with $\sim 400 M_\odot$ at $n \sim 10^7 \mathrm{cm^{-3}}$. It is found that the effect of the external radiation is not important in the case with high initial density ($n_0=10^6 \mathrm{cm^{-3}}$).

In summary, in the case with low initial density ($n_0<10^2\mathrm{cm^{-3}}$), the filamentary cloud suffers photodissociation in the early stage of collapse. In such case, temperature increases adiabatically. The filamentary cloud with small line mass ($f=1.5$) fragments during adiabatic phase. On the other hand, the filamentary cloud with large line mass ($f=6$) does not fragment during adiabatic phase and collapses with shielding itself from the external radiation. In this case, fragment mass is hardly affected by the external radiation. In the case with high initial density ($n_0=10^6 \mathrm{cm^{-3}}$), the thermal evolution of the filamentary cloud is hardly affected by the external dissociation radiation.

One-zone model predicts fragment mass different from $2.4 \times 10^5 M_\odot$ which one-dimensional model predicts. For example, for the parameter set same as figure 5, in Paper I, the uniform model predicted $1.5 \times 10^5 M_\odot$ and rarefied model predicted $2.7 \times 10^4 M_\odot$. Difference between one-zone models and one-dimensional model originates from difference of dynamical equation (virial equation in one-zone model and hydrodynamical equation of motion in one-dimensional model). In one-dimensional model, collapse is run-away collapse, and fragmentation condition is satisfied at lower density since free-fall time balances with sound crossing time in the central dense region. Hence, in one-dimensional model, fragment mass becomes larger than in one-zone model.

\subsection{Property of the filamentary cloud at fragmentation}
In this subsection, we show the profile of physical quantities (density, temperature, in-fall velocity, and ratio of pressure gradient to gravitational force) at fragmentation. We focus on density profile and investigate whether or not the universal profile at fragmentation exists. Moreover, we compare fragment mass (equation 14) with Jeans mass estimated with the central density and temperature.

\subsubsection{Case without the external radiation}
\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure8a.eps}} &
\resizebox{80mm}{!}{\includegraphics{figure8b.eps}} \\
\resizebox{80mm}{!}{\includegraphics{figure8c.eps}} &
\resizebox{80mm}{!}{\includegraphics{figure8d.eps}} \\
\end{tabular}
\caption{Profile of density (a), temperature (b), in-fall velocity profile (c), and ratio of pressure gradient to gravity (d) at fragmentation of the filamentary cloud with $(f,n_0,J_{21})=(1.5,10\mathrm{cm^{-3}},0)$.}
\end{center}
\end{figure}

We show the profiles of density, temperature, infall velocity, and ratio of pressure gradient to gravitational force at fragmentation in the case with $(f,n_0,J_{21})=(1.5,10\mathrm{cm^{-3}},0)$ (figure 8). In diagram (a) in figure 8, it is seen that dense central region within Jeans length ($\lambda_J \sim 2.3 \times 10^{18} \mathrm{cm}$) has uniform density, and the density profile in the outer envelope is proportional to $r^{-4}$. This density profile is similar to that of equilibrium solution for the isothermal filamentary cloud (Ostriker 1967). However, between $r=10^{19}\mathrm{cm}$ and $r=10^{20}\mathrm{cm}$, slope of the density profile is sallower than $r^{-4}$. Temperature is highest outside $r_{\mathrm{cool}} \sim 2 \times 10^{18} \mathrm{cm}$ where $t_{\mathrm{cool}}=t_{\mathrm{ff}}$, and pressure gradient force is stronger than gravity force outside $r_{\mathrm{cool}}$. Hence, matter is pushed outward. Velocity profile is in proportion to radius in the central dense region and is constant larger than sound speed in the outer envelope. Ratio of pressure gradient to gravity is nearly $1$ ($\sim 1.01$) inside $r_{\mathrm{cool}}$. In diagram (b), drop of temperature at the surface is seen. Since we assume that the external pressure is zero, adiabatic cooling occurs at several meshes of the surface. Moreover, these meshes are pushed by inner meshes with higher pressure and fall more slowly than inner meshes. However, these effects do not affect the central region. Fragment mass is $1220M_\odot$ which is close to Jeans mass ($1140M_\odot$) estimated with central density and temperature. Since $t_{\mathrm{dyn}}$ is about 6 times of $t_{\mathrm{ff}}$ at the center when the filamentary cloud fragments, pressure gradient force is important to calculate the further evolution of fragments. Further evolution of each fragment is shown in $\S 4$.

\subsubsection{Case with the external radiation}
\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure9a.eps}} &
\resizebox{80mm}{!}{\includegraphics{figure9b.eps}} \\
\resizebox{80mm}{!}{\includegraphics{figure9c.eps}} &
\resizebox{80mm}{!}{\includegraphics{figure9d.eps}} \\
\end{tabular}
\caption{Same as figure 8, but $(f,n_0,J_{21})=(1.5,10\mathrm{cm^{-3}},10)$.}
\end{center}
\end{figure}

We show profiles of the same quantities as figure 8 for the case with $(f,n_0,J_{21})=(1.5,10\mathrm{cm^{-3}},10)$ in figure 9. In figure 9, it is seen that except for temperature, profiles of physical quantities are similar to figure 8. Most of $\mathrm{H_2}$ is photodissociated, and the filamentary cloud loses the ability to cool. Hence, temperature is higher in the central dense region than in the outer envelope. Ratio of pressure gradient to gravity is larger than $1$ ($\sim 1.2$). Fragment mass is $2.4 \times 10^5 M_\odot$ which is close to Jeans mass ($3.0 \times 10^5 M_\odot$) estimated with central density and temperature. In the case with the external radiation, since $t_{\mathrm{dyn}}$ is about 5 times of $t_{\mathrm{ff}}$ at the center when the filamentary cloud fragments, pressure gradient force is important to calculate the further evolution of fragments (see $\S 4$). In figure 10, the density profiles in figure 8 and 9 are simultaneously plotted, and each profile is found to be similar to each other. The profiles at $r/\lambda_J<0.5$ are similar to the profile of isothermal filamentary cloud in equilibrium state.

\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure10.eps}} \\
\end{tabular}
\caption{Normalized density profile for figure 8 (solid line) and figure 9 (dashed line). The initial density profile in the case with $f=1$ is also shown (dotted line). The symbol $n_c$ is central density and $\lambda_J$ is Jeans length at the center.}
\end{center}
\end{figure}

\subsection{Fragment mass}
\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure11a.eps}} &
\resizebox{80mm}{!}{\includegraphics{figure11b.eps}} \\
\resizebox{80mm}{!}{\includegraphics{figure11c.eps}} &
\resizebox{80mm}{!}{\includegraphics{figure11d.eps}} \\
\end{tabular}
\caption{The contours map for the fragment mass for the case with (a) $J_{21}=0$, (b) $J_{21}=1$, (c) $J_{21}=6.5$, and (d) $J_{21}=10$. Solid lines in each diagrams represent constant fragment mass. The number near each solid line is mass of fragment in units of $M_\odot$.}
\end{center}
\end{figure}

We show how much the external dissociation radiation changes fragment mass. Figure 11 shows the fragment mass for all the parameters in $n_0 - f$ plane using contours. Results for the cases with $J_{21}=0$, $1$, $6.5$, and $10$ are presented in different diagrams. In the case with the external radiation, it is seen that the filamentary clouds fragment into very massive clouds ($> 10^5 M_\odot$) in the cases with low initial density ($n_0 \le 10^2 \mathrm{cm^{-3}}$). Since very massive fragments are not seen in the case without the external radiation, this can be regarded as a result of the effect of the dissociation photon. This feature is similar to the result of the one-zone models in Paper I. Thus, formation of very massive fragments under the external radiation with moderate intensity can be regarded as the robust result, provided that the external radiation turns on when the filamentary cloud forms.

The diagram (a) of figure 11 is similar to figure 6 of Nakamura $\&$ Umemura (2001). In the range of $2-100M_\odot$, the contours are dense. This is because the filamentary cloud becomes isothermal once $\mathrm{H_2}$ cooling becomes effective owing to three body reaction, and continues to collapse to high density ($\sim 10^{13} \mathrm{cm^{-3}}$). In such a case, fragment mass is small ($\sim 2-10 M_\odot$). This feature is seen in Nakamura $\&$ Umemura (2001).

Nakamura $\&$ Umemura (2002) concluded that there are some parameter sets where $\mathrm{HD}$ is main coolant. However, in our results, $\mathrm{HD}$ is found not to be important. Deuterated hydrogen molecules $\mathrm{HD}$ mainly forms from $\mathrm{H_2}$\footnote{Main chemical reaction of formation of $\mathrm{HD}$ is given by
\begin{eqnarray}
\mathrm{H_2} + \mathrm{D^+} \rightarrow \mathrm{HD} + \mathrm{H^+}.
\end{eqnarray}
}. Since initial $\mathrm{H_2}$ fraction in this paper is assumed to be small ($10^{-4}$), even in the case without the external radiation, sufficient amount of $\mathrm{HD}$ to cool does not form. This result is consistent with Nakamura $\&$ Umemura (2002). In the case with the external radiation, since $\mathrm{H_2}$ is photodissociated, $\mathrm{HD}$ is less important.

\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure12a.eps}} &
\resizebox{80mm}{!}{\includegraphics{figure12b.eps}} \\
\resizebox{80mm}{!}{\includegraphics{figure12c.eps}}
\end{tabular}
\caption{The ratio of the fragment mass with the external radiation ((a) $J_{21}=1$, (b) $J_{21}=6.5$, and (c) $J_{21}=10$) to that without the external radiation ($J_{21}=0$). The number near each solid line is the ratio of fragment mass.}
\end{center}
\end{figure}

We show the effect of the external radiation on fragment mass quantitatively. Figure 12 shows the similar contours but about the ratio of the fragment mass between the cases with and without the external radiation. In addition to figure 11, figure 12 clearly shows that the filamentary clouds with low initial density ($n_0 \le 10^2 \mathrm{cm^{-3}}$) and moderate $f$ ($<4.5$) fragment into more massive fragments than the case without the external radiation. This feature agrees with the results of the rarefied filament model in Paper I.

It is seen that fragment mass for the case with high initial density ($n_0 > 10^2 \mathrm{cm^{-3}}$) does not increase owing to the external dissociation radiation. This is because the initial density is high enough for the filamentary cloud to shield itself from the external dissociation radiation. In this case, the evolution is similar to the case without the external radiation.

\subsection{Self-shielding function of Wolcott-Green et al. (2011)}
Wolcott-Green et al. (2011) have recently suggested self-shielding function indicated by three-dimensional radiative transfer. In this subsection, we investigate dependence of fragment mass on the self-shielding function quantitatively. The new self-shielding function is given by,
\begin{eqnarray}
f_{\mathrm{sh,WG}}=\frac{0.965}{(1+x/b_5)^{1.1}}+\frac{0.035}{(1+x)^{0.5}} \exp [-8.5 \times 10^{-4} (1+x)^{0.5}],
\end{eqnarray}
where
\begin{eqnarray}
x \equiv \frac{N_{\mathrm{H_2}}}{5 \times 10^{14} \mathrm{cm^{-2}}},
\end{eqnarray}
and
\begin{eqnarray}
b_5 \equiv \frac{b}{10^5 \mathrm{cm/s}} = \frac{1}{10^5 \mathrm{cm/s}} \sqrt{\frac{2k_B T}{\mu m_{\mathrm{H}}}}.
\end{eqnarray}
Since $f_{\mathrm{sh,WG}}$ is $1-10$ times larger than original $f_{\mathrm{sh}}$ (equation 12). Hence, Wolcott-Green et al. (2011) suggested that the effect of photodissociation is actually stronger than the result with $f_{\mathrm{sh}}$. Thus, the results which we have ever considered are expected to be modified quantitatively.

\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure13.eps}} \\
\end{tabular}
\caption{The ratio of the fragment mass with $f_{\mathrm{sh,GW}}$ to that with $f_{\mathrm{sh}}$ in the case with $J_{21}=10$. The number near each solid line is the ratio of fragment mass.}
\end{center}
\end{figure}

To see the difference between shielding function, we calculate fragment mass using $f_{\mathrm{sh,WG}}$ in the case with $J_{21}=10$. Figure 13 shows the ratio of fragment mass between the cases with $f_{\mathrm{sh,GW}}$ and with $f_{\mathrm{sh}}$. When we use $f_{\mathrm{sh,GW}}$, fragment mass increases comparing with the case with $f_{\mathrm{sh}}$ especially for the cases with $n_0=10-10^3 \mathrm{cm^{-3}}$ and $f \ge 2$. This feature is consistent with the relation, $f_{\mathrm{sh,GW}} \ge f_{\mathrm{sh}}$.

\section{Criterion for increase of fragment mass}
Omukai $\&$ Yoshii (2003) calculated the evolution of the filamentary cloud under the external dissociation radiation assuming free-fall. The authors assumed that fragmentation occurs at density 100 times higher than the loitering point and concluded that the effect of the external dissociation radiation decreases fragment mass. This conclusion apparently disagrees with our results in $\S 3$. In this section, we consider whether or not the external radiation increases fragment mass when the filamentary cloud reaches the loitering point. Initial density of the filamentary cloud is assumed to be very low ($n_0=0.1 \mathrm{cm^{-3}}$). As the timing when the external radiation turns on, we consider various cases. The investigation in this section provides systematic study which includes the situation of Omukai $\&$ Yoshii (2003).

\subsection{Whether the filament reaches the loitering point}
Suppose a filamentary cloud with $n_0=0.1 \mathrm{cm^{-3}}$ and the external radiation turns on when density reaches $n_{\mathrm{UV}}$. We consider the cases with $n_{\mathrm{UV}}=0.1\mathrm{cm^{-3}}$, $1\mathrm{cm^{-3}}$, and $10\mathrm{cm^{-3}}$. We also assume $T_0=300\mathrm{K}$ and $f_{\mathrm{H_2}}=0$ at $n_0$. As for the evolution of the filamentary cloud, we solve one-dimensional hydrodynamics as in $\S 3$.

We calculate the evolution of the filamentary cloud with various values of $f$. In order for the filamentary cloud not to fragment during adiabatic phase in the case with $J_{21}=10$, it is found that $f$ is required to be larger than $30$, $25$, $10$, and $5$ for various values of $n_{\mathrm{UV}}$ ; $n_{\mathrm{UV}}=0.1\mathrm{cm^{-3}}$, $1 \mathrm{cm^{-3}}$, $10\mathrm{cm^{-3}}$, and $\infty$, respectively. Hence, we investigate how massive fragments are in the case with $f=30$, $25$, $10$, and $5$. Does fragment mass increase when the filamentary cloud reaches the loitering point?

\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure14.eps}} \\
\end{tabular}
\caption{Thermal evolution of the filamentary cloud with $f=30$, $n_0=0.1\mathrm{cm^{-3}}$, $J_{21}=10$, and various $n_{\mathrm{UV}}$ where the external radiation turns on ; $n_{\mathrm{UV}}=0.1\mathrm{cm^{-3}}$ (thick solid line) $n_{\mathrm{UV}}=1\mathrm{cm^{-3}}$ (thick long-dashed line), $n_{\mathrm{UV}}=10\mathrm{cm^{-3}}$ (thick short-dashed line), $n_{\mathrm{UV}}=\infty$ (thick dash-dotted line). Thin lines shows the thermal evolution of fragments. Dotted lines indicate the constant Jeans masses.}
\end{center}
\end{figure}

First, we show the case with $f=30$ where the filamentary cloud reaches the loitering point for any $n_{\mathrm{UV}}$. Figure 14 shows the thermal evolution of the filamentary cloud with $f=30$, $n_0=0.1\mathrm{cm^{-3}}$, $J_{21}=10$, and various $n_{\mathrm{UV}}$. Thin lines indicate thermal evolution of each fragment (see $\S 4.2$). Fragment mass is largest ($550M_\odot$) in the case with $n_{\mathrm{UV}}=\infty$. Fragment mass is smaller in the case with lower $n_{\mathrm{UV}}$. As a result, the external radiation decreases fragment mass. All filamentary clouds fragments at the density which is roughly $1000$ times higher than loitering point, which is qualitatively consistent with Omukai $\&$ Yoshii (2003).

\begin{figure}
\begin{center}
\begin{tabular}{cc}
\resizebox{80mm}{!}{\includegraphics{figure15.eps}} \\
\end{tabular}
\caption{Same as figure 14, but $f=5$.}
\end{center}
\end{figure}

Next, we investigate whether or not the external radiation decreases fragment mass when the filamentary cloud does not reach the loitering point. Figure 15 shows the same figure as figure 14 except for the value of $f$ : $f=5$. It is found that the filamentary cloud which does not reach the loitering point fragments into more massive clouds than the case with $n_{\mathrm{UV}}=\infty$. This feature agrees with our result of $\S 3$. Also in the cases with $f=25$ and $10$, the filamentary cloud fragments into more massive clouds than the case without the external radiation ($n_{\mathrm{UV}}=\infty$) when it does not reaches loitering point ($n_{\mathrm{UV}} \le 0.1 \mathrm{cm^{-3}}$ for $f=25$ and $n_{\mathrm{UV}} \le 1 \mathrm{cm^{-3}}$ for $f=10$). Whether or not the external radiation increases fragment mass is determined by whether or not line mass is small enough for the filamentary cloud not to reach the loitering point.

It is explained as follows that fragment mass decreases under the external radiation : after the external radiation turns on, the filamentary cloud suffers photodissociation. The outer region loses more amount of $\mathrm{H_2}$ than the dense central region. Since temperature of the outer region becomes higher than the dense central region, pressure gradient becomes sallower at the region between the dense central region and the outer region. Then, such a region sticks to the dense central region owing to gravity, and line mass of the central dense region increases. As a result, the filamentary cloud collapses up to higher density ($n \sim 10^{6-7} \mathrm{cm^{-3}}$) owing to larger line mass and fragments into less massive clouds than the case without the external radiation.

\subsection{Sub-fragmentation}
It is found that the external radiation increases fragment mass when the filamentary cloud fragments before the loitering point. However, each fragment may occur sub-fragmentation and mass of final outcome may be as small as fragment mass in the case without the external radiation. To clarify mass of final outcome, we investigate the further evolution of each fragment.

We use one-zone model for each fragment. We assume that each fragment is spherical and has $M_{\mathrm{frag}}$ (see equation 14), chemical composition same as at the center of the filamentary cloud, radius $r_{0.1}$ where $n (r_{0.1})=0.1 n_c$. Infall velocity at fragmentation is proportional to radius, and we use infall velocity at $r_{0.1}$ as infall velocity of each fragment. The density of fragment is estimated from the mass and radius as
\begin{eqnarray}
\rho_{\mathrm{frag}}=\frac{M_{\mathrm{frag}}}{\frac{4\pi}{3} r_{0.1}^3}.
\end{eqnarray}
This density, $\rho_{\mathrm{frag}}$, is different from the density of the filamentary cloud before fragmentation and corresponds to the one at the end of fragmentation. Temperature and fraction of each fragment is approximated by the value when the filamentary cloud fragments. According to the result in $\S 3.3$, in the view point of dynamical evolution, we should consider the effect of pressure gradient force. Hence, we treat pressure effect explicitly using the virial equation for uniform sphere. The virial equation is given by
\begin{eqnarray}
\frac{dv}{dt}=\frac{10}{3}\frac{k_B T}{\mu m_{\mathrm{H}}} \frac{1}{R} -\frac{GM}{R^2},
\end{eqnarray}
where $R$ is radius and $M$ is mass of the cloud (see Appendix 1). Radiative transfer is treated by the same method as in Omukai (2001) except for we use $f_{\mathrm{sh,GW}}$ instead of $f_{\mathrm{sh}}$. The same routine as $\S 3$ is used for chemical reactions.

In figure 15, it is found that if each fragment occurs sub-fragmentation at the loitering point ($n \sim 10^3 \mathrm{cm^{-3}}$), mass of final outcome is $\sim 10^4 M_\odot$. This is larger than fragment mass in the case without the external radiation. Hence, even if sub-fragmentation occurs, mass of final outcome increases owing to the external radiation when the filamentary cloud fragments before the loitering point. This tendency is found in the other cases with $f=25$ and $10$.

When the filamentary cloud reaches the loitering point, temperature of each fragment increases adiabatically after fragmentation ($n \sim 10^{6-7} \mathrm{cm^{-3}}$). This is because gravity dominates pressure gradient after fragmentation and dynamical time becomes shorter than cooling time.

\section{Conclusions and discussions}
In this paper, collapse and fragmentation of primordial filamentary cloud was investigated using one-dimensional hydrodynamical calculations with the effect of the external dissociation radiation. Especially, the effect of run-away collapse to fragment mass is considered by comparing with previous results with one-zone models. Results are summarized as follows :
\begin{itemize}
\item Comparing with the uniform model in Paper I, one-dimensional filament model predicts lower fragmentation density and larger fragment mass. This is because fragmentation occurs only in the central region with low virial temperature in one-dimensional model.
\item Comparing with the rarefied filament model in Paper I, one-dimensional filament model predicts similar fragment mass. This explains that the discrepancy between the uniform filament model and one-dimensional filament model mainly comes from the run-away collapse which is partly induced by the pressure effect.
\item As long as the external radiation is assumed to turn on when the filamentary clouds form, low initial density ($n_0 \le 10^2 \mathrm{cm^{-3}}$) filamentary clouds with moderate line mass are expected to fragment into very massive clumps ($\sim 10^5 M_\odot$) as a result of photodissociation of molecular hydrogen. This result which is originally indicated in Paper I is confirmed in this paper using one-dimensional hydrodynamical calculations.
\item The external dissociation radiation increases fragment mass when the filamentary cloud fragments during adiabatic phase after the external radiation turns on. On the other hand, when the filamentary cloud with sufficient line mass reaches the loitering point, the dissociation radiation decreases fragment mass, which is consistent with Omukai $\&$ Yoshii (2003).
\end{itemize}

As seen in figure 15, the thermal evolution of a filamentary cloud and a spherical cloud is different after each cloud reaches loitering point. The thermal evolution of the filamentary cloud is isothermal, and temperature of spherical cloud increases. This is explained as follows : since the central region of the filamentary cloud is approximately dynamical equilibrium ($\S 3.3$), we have
\begin{eqnarray}
\frac{1}{\rho} \frac{P}{r} &\sim& \frac{Gl}{r} \nonumber \\
T &\sim& \mu m_{\mathrm{H}} Gl \propto const.
\end{eqnarray}
As for spherical cloud, the central region is not dynamical equilibrium. Hence, we investigate relation between $T$ and $n$ from balance between adiabatic heating and $\mathrm{H_2}$ cooling. Adiabatic heating rate is
\begin{eqnarray}
-P \frac{d\ }{dt} \frac{1}{\rho} \sim P \frac{1}{t_{\mathrm{ff}}\rho} \propto T n^{1/2}
\end{eqnarray}
where we assume that spherical cloud collapses in free-fall timescale. When density is larger than the critical density of $\mathrm{H_2}$, $\Lambda_{\mathrm{H_2}} \propto n T^\alpha$ ($\alpha \sim 3.8$ at $T \sim 300 \mathrm{K}$ and $\alpha \sim 4.8$ at $T \sim 1000 \mathrm{K}$), and we have
\begin{eqnarray}
\frac{\Lambda_{\mathrm{H_2}}}{\rho} &\propto& \frac{n T^\alpha}{n} \propto T^\alpha.
\end{eqnarray}
From equations (29) and (30), we have $T \propto \rho^{1/2(\alpha-1)}$. Temperature depends on density as,
\begin{eqnarray}
T \propto \left\{ \begin{array}{ll}
n^{1/2(\alpha-1)} & \mathrm{sphere} \\
const. & \mathrm{filament}. \\
\end{array} \right.
\end{eqnarray}

In this paper, we consider the filamentary cloud with variety of line mass. Hence, we estimate $f$ for the filamentary clouds in cosmological simulation. As an example, we refer with figure 2 of Greif et al. (2008). In this figure, the filamentary cloud with density $n \sim 10^{-2} \mathrm{cm^{-3}}$ and radius $\sim 7 \mathrm{kpc}$ is shown. Line mass of this filamentary cloud is $\sim 7.8 \times 10^{18} \mathrm{g/cm}$. When temperature is $300\mathrm{K}$, the critical line mass is $l_{\mathrm{crit}} \sim 3.5 \times 10^{17} \mathrm{g/cm}$. Hence, $f \sim 22$ and according to our results in $\S 4$, fragment mass may increase if the external radiation turns on at $n \le 1 \mathrm{cm^{-3}}$.

For simplicity, the model and numerical calculations in this paper are one-dimensional for the filamentary cloud and one-zone for each fragment. In order to discuss fragmentation, we assume the condition for fragmentation ($\S 2.3$) and assume that each fragment is spherical. During further collapse, spherical clouds are possible to be the filamentary cloud again or may become disk-like if it rotates. Although we discussed a possible sub-fragmentation at the loitering point for each clumps in $\S 4.2$, the final fate of the cloud is still open question. Furthermore, if the filamentary cloud with large line mass is not axisymmetric, it may become sheet-like cloud. Such a cloud may collapse and fragment into many filamentary clouds. In this paper, the external radiation is assumed to be uniform, and the intensity does not depend on time. These problems require three-dimensional calculations. As for three-dimensional simulation with the external radiation, Susa (2007) investigated collapse of spherical cloud under the single light source. However, further investigations with three-dimensional simulation which statistically investigate fragment mass of the filamentary cloud under the external radiation will be desirable. Despite simplicity, one-dimensional hydrodynamical calculations in this paper are useful in the view point of extracting physical processes which are important in formation of the astronomical objects. These one-dimensional calculations and the realistic three-dimensional calculations may be complementary.

\bigskip

We thank Fumio Takahara for fruitful discussion and continuous encouragement. We also acknowledge the referee for improving the manuscript.

redpajama_set_name: RedPajamaArXiv


text:
Interview: What Vigil's core team is up to at its new Crytek home
Crytek has long had plans to open a U.S. branch, but the opportunity to do that never really presented itself in such an appealing way as it did when Vigil's talent was up for grabs.
Crysis developer Crytek has long had plans to open a U.S. branch, but the opportunity to do that never really presented itself in an appealing way. That is, until Vigil Games' talent was up for grabs in Austin. Vigil Games was one THQ studio that was up for auction following the publisher's collapse, but despite building a fanbase with the Darksiders franchise, no one tried to buy the Austin studio. So along came Frankfurt, Germany-based Crytek, which just so happened to be looking to get its foot in the door in the U.S. market. Crytek saw an opening, and expanded its footprint using Vigil's core talent as a foundation. "Crytek U.S. was always the plan for us," Crytek CEO Cevat Yerli told us in a phone interview. "It's a very significant expansion of our development culture and a big step for our CryEngine business." Crytek USA is made up of 35 game developers -- some from Vigil's core team (but not the whole studio) and a number of Austin-based developers who were looking for new jobs. Leading Crytek USA is David Adams, former general manager and co-owner of Vigil, a studio whose fate will ultimately be decided during THQ's upcoming bankruptcy case. Crytek became a significant player in the aftermath of THQ's bankruptcy and asset sell-off. The studio bought the Homefront first-person shooter property (Crytek's Nottingham, UK studio has 140 developers who had been working on Homefront 2 for THQ) for $500,000 in order to ensure work on the game would continue. The founding of Crytek in Austin will mean more game and CryEngine development in the U.S., and access to more development talent. "We weren't just looking at Vigil's team [for recruitment], but the whole Austin development community," said Yerli. "Austin is a very small, connected community of game developers." With the expansion into the U.S. still fresh, Yerli could only talk broadly about near- and long-term goals for Crytek USA. But it sounds like the new branch will play a significant role in the company's future. "It would be pretty much safe to say that this team will be working on online games," he said, adding that the new team at Crytek USA will focus on "online games and kick-ass triple-A productions. It is going to be quite a significant investment for Crytek over the next five years." Yerli also made clear that Crytek was not intending to purchase THQ's Darksiders IP. For Crytek, the Austin game development community and the 35 game developers with jobs, things seemed to work out okay, despite the manic nature of the branch's founding. "Austin was high on the list. It was pretty much highest on the list," said Yerli. "... We saw this as an opportunity. These guys are jobless, we can save their jobs at the same time, we can move Crytek forward in the U.S., and make steps that are in line with our strategies."

redpajama_set_name: RedPajamaCommonCrawl


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text:
Lancashire bolstered by 100 extra police officers
Thursday, 29 October, 2020
New statistics show that nearly 6,000 extra officers have been recruited in the first year of the Government's major police recruitment drive, with 100 more in Lancashire alone.
This confirms that the Government is on track to deliver 20,000 extra officers by 2023, and is ahead of schedule to have the first 6,000 in place by March 2021.
These new officers will be crucial in the fight against coronavirus, as well as helping to drive down crime and to make our streets safer.
Andrew Snowden has welcomed the announcement that Lancashire has been bolstered by an additional 100 officers since the Government launched its major police recruitment drive one year ago.
The addition of these new officers brings the total number of police across Lancashire up to 3,088, meaning there are now more frontline officers on our streets to keep the public safe.
Since the launch of the Government's recruitment campaign one year ago, a total of 5,824 extra officers have joined police forces across England and Wales.
These statistics confirm that the Government remains fully on track to meet its manifesto commitment of recruiting 20,000 extra officers by 2023, and is ahead of schedule to have the first 6,000 in place by March 2021.
The new statistics also show that the police workforce is now more diverse than ever before, with 10.7 per cent of new recruits identifying as Black, Asian and Minority Ethnic, and with 9,842 of all officers now being from these groups.
This recruitment drive is at the centre of the Government's commitment to back the police with more resources, powers and support to keep the public and their communities safe.
Alongside the recruitment campaign, the Government is also boosting police pay by 2.5 per cent this year, equivalent to a constable receiving an extra £1,100, providing officers with an increase above inflation for the second year running, the largest pay rise in a decade.
The Government is also enshrining a new police covenant into law, which will offer enhanced support and protection for frontline officers, and is bringing forward legislation to double the maximum sentence for those convicted of assaults on frontline staff including police officers, firefighters and paramedics.
Other steps to support our frontline officers include a £1.1 billion funding boost for police forces this year – the biggest increase in a decade, funding to provide over 8,000 more officers with Taser devices, and personalised new stop and search powers so that officers can effectively target repeat offenders.
Commenting, Andrew Snowden said:
"Getting more police officers onto our streets is one of the people's priorities, and so I am delighted that in just over one year, this Conservative Government has already delivered an extra 100 officers across Lancashire.
"Every one of these officers will make an enormous difference in helping to cut crime and keep people safe – and I know that many more will follow as this Government continues to deliver on its promise to recruit 20,000 more over the next three years.
"By backing our police with the funding, powers and resources they need, we are keeping the public and our communities safe, so that people everywhere can live their lives free from the fear of crime."
Home Secretary Priti Patel said:
"Getting more police officers on our streets is a priority for the British people – therefore a priority for me.
"Just one year since we began recruiting, I am delighted that there are nearly 6,000 of the 20,000 additional officers on our streets cutting crime and making your communities safer.
"As we've seen from the frontline response to coronavirus, the work of each and every police officer helps to save lives and I would like to extend my gratitude to them, and to the new recruits, for joining the police and being a part of this heroic national effort."
Andrew Snowden
Andrew is the Conservative choice for Lancashire's Police and Crime Commissioners candidate for the May 2021 election. He also represents the Hoghton with Wheelton Division on Lancashire County Council.


We seek European folk dancing and shadow puppet enthusiasts to join us in making spectacle to celebrate the glories of the longest day of the year! Come make giant shadow puppets, dance and perform with us on June 18th. Details below. Thanks to the gracious support of the Toronto Arts Council.
On June 14 and 15, come to Amos Waites Park from 6-7:30pm to learn the basics of Balfolk dancing. With a live band and our wonderful dance teacher Emilyn, you'll be able to learn some of the dances before the big celebration on the 18th. No partner or dance experience needed - these are folk dances and meant to be danced by everyone.
On June 16 and 17, we invite you to join us in the park from 6-7:30pm for workshops in shadow puppetry. We will experiment with making shadow puppets from paper cuts as well as found materials. We also encourage participants in these workshops essions to join us on the performance day for a small role in our final show!
Thanks to the Toronto Arts Council and Arts in the Parks for their support of this event.


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Find out what a Domain Manager is really along with what functions Domain Managers usually have.
Since a site requires both hosting space and a domain, it's vital to be able to effortlessly manage not only the former, but also the latter. Even if the web hosting service is fast and stable, registering a new domain name and linking it to a particular website may be a torture and may involve plenty of time and effort. In fact, that's the situation with the great majority of hosting platforms out there – you'll have at least two accounts, one hosting account and one billing account, and registering a domain name and taking it online will involve logging in and out of the two accounts. It'd be far more convenient if you could carry out all these things from one and the same place and focus on your website, not on various administrative tasks.
If you order a shared website hosting plan from our company, you'll get access to a feature-laden Domain Manager, which is part of our all-inclusive Hepsia Control Panel. You will be able to register a brand-new domain name and then to host it or park it, to activate Whois Privacy Protection or to edit its WHOIS information with only several clicks. Using quick-access buttons, you will also be able to set up a subdomain, an email or a database, to keep an eye on traffic statistics, to access the website files or to request a brand new SSL certificate. All functions are conveniently grouped and are available in one place, which will save you plenty of time, so you'll never have to sign out of the Domain Manager tool. You will not experience any difficulties, as we've included how-to articles and video lessons to demonstrate the full capacity of our domain management tool.
The Hepsia Control Panel, which is included with each semi-dedicated server package that we offer, is an all-in-one tool, which will give you absolute authority over your semi-dedicated account and which includes our fully featured Domain Manager. It permits you to manage everything connected with the domain names in your account – both the registered and the hosted ones. The most essential functions are all here – you can register or renew a domain name, enable Whois Privacy Protection for it, park and redirect it or change its WHOIS info. The Domain Manager, however, is much more than just a list of your domains, plus a few ordinary functions. It's an avant-garde tool, inside which you will discover fast-access buttons, using which you can easily set up a database or an email address, access the website files pertaining to a certain domain name or view exhaustive traffic statistics and access logs. The Domain Manager is intuitive (albeit powerful), so it can be used by individuals with little or no experience.


text:
package com.mscharhag.errorhandling.article;

import com.mscharhag.errorhandling.ErrorResponse;
import org.springframework.http.HttpStatus;
import org.springframework.http.ResponseEntity;
import org.springframework.web.bind.annotation.ControllerAdvice;
import org.springframework.web.bind.annotation.ExceptionHandler;

@ControllerAdvice
public class ArticleExceptionHandler {

    @ExceptionHandler(ArticleNotFoundException.class)

    public ResponseEntity<ErrorResponse> onArticleNotFoundException(ArticleNotFoundException e) {
        String message = String.format("No article with id %s found", e.getArticleId());
        return ResponseEntity
                .status(HttpStatus.NOT_FOUND)
                .body(new ErrorResponse("ARTICLE_NOT_FOUND", message));
    }
}


text:
TREES PLANTED TILL 18th
July 1,54,324
Home / Letter from President | Photo Gallery | Contact Us
Features / Knowledgebase
How to Plant a Tree
Start your own Nursery
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Sumant Dhamija
Suneela Khosla
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Website is currently under construction
and some portions are being updated.
Please visit later to find more updates.
Letter from the President - Planting a million trees in Delhi !
Welcome to TreeDelhi.org!
TreeDelhi has come about directly in consequence of the high and almost intolerable levels of air pollution in Delhi and the knowledge that growing more trees, part of wider initiative, will give the people of Delhi a cleaner and healthier environment. It would also help combat Climate Change. (Click here for a description of Global Warming/CC , PDF Document) Our target is 30,000 trees in the first year (2013-14) , 70,000 trees in year2 and then 100,000 trees each following year so that, taking account of fatalities, we ought to achieve our target by around 2027-28.
Why Trees?
Planting trees is always a good idea. There is a saying that the best time to plant trees was 20 years ago. The second best time is now! Trees give us countless benefits. Apart from beautifying the surroundings they give shade, reduce temperatures and noise levels, improve soil quality, absorb carbon and pollutants. The increase in rainfall as a consequence of more trees is vitally required to replenish our diminishing ground water reserves. The list of benefits goes on
Why plant trees in Delhi?
Although parts of Delhi appear to have sufficient foliage, we are seriously short of trees commensurate to the population (over 16 million) and high pollution levels caused by cars, two wheelers, and three wheelers (each polluting as much as 50 cars!) and the enormous amount of dangerous chemical pollutants spread in our atmosphere due to air traffic which is increasing by the day! These include (bad)Ozone, Toluene, and Xylene with significant and immediate impacts on our internal organs and general health. One only has to look at the Delhi Delhi Pollution Control Board's website www. dpcc.delhigovt.nic.in and note that we have already exceeded acceptable limits. Air quality is also measured privately by Mr Samir Khosla, in one of the leafiest parts of Delhi- Pushpanjali Farms- gives a worrying picture.
If all the adults of Delhi's population (16 m) were persuaded to plant a tree each, we would have met our target with ease but this is not practical. Our objective therefore is to persuade and encourage institutions and people (specially thought leaders) to plant/care for trees. Our target is to plant at least a million trees– as soon as possible and certainly by the end of 2020. 'The govt and tree planting' describes the role of govt. for the environment of Delhi and its many services including providing free seeds/saplings for the citizens of Delhi. A list of such nurseries and other distribution points is given. There is also a list of commercial nurseries. TreeDelhi plans to have its own nurseries later this year in Delhi, Gurgaon and Panipat.
As part of our program, an attempt is being made to create eco-consciousness in schools and other institutions. See under Cutting the Carbon. For this we have partnered with 'Clean India', part of the 'Development Alternatives' started by Mr Ashok Khosla in 1996 which we hope will excite and enthuse students/others to plant/care for trees. Part of their presentation 'Cutting the Carbon' can be seen here. Schools and others may contact Ranjeeta Ghosh (+919560961433) or email at rghosh@devalt.org for further information/action and on how to measure your Carbon Footprint.
The trees to plant / The Neem Tree
There is a section on 'How to plant a Tree' with suggestions and tips. Fruit trees may be preferred and constitute most of the planting in homes; for others we like indigenous trees – Peepal, Philkhan, Semal, Jhinjeri, Kachnar, Sheesham etc but particularly- Neem. The latter is hardy, requires little water to grow and has a great CO2 absorption capacity producing equally large quantities of oxygen. It acts as a natural air filter by absorbing dust particles and because of its large leaf area it accumulates higher quantities of lead. A study by the National Engineering Research Institute in 1996 concluded that Neem was the most suitable species for checking urban pollution. You can read more of qualities of the 'Neem Tree' growing which can enable, for some entities, the accumulation of Carbon Credits.
On this page, we have created a counter for the number of trees planted. We will give credit to persons/institutions under Tree Planters to all those who let us know when and where they have planted a tree(s). Please do send photos of beautiful trees in Delhi/your planting(s), the best of which, chosen by our panel every month, will be on the website under Best Photos.
Finally should you wish to donate for the cause, you can click here.
Happy Planting!
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