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text:
Vespertijd is een werk van de Belgische kunstschilder Constant Permeke. Hij vervaardigde het doek in 1927. Het bevindt zich nu in de collectie van het Koninklijk Museum voor Schone Kunsten Antwerpen onder inventarisnummer 2779.

Context
Het was 1922 toen Constant Permeke zich terug voor korte tijd vestigde in Astene (streek van Sint-Martens-Latem) aan de Leie. Hij werd er getroffen door het harde plattelandsleven en de band tussen de boeren en hun land. Het is dan ook de eigen interpretatie van de kunstenaar en dat diepmenselijke meevoelen met de hard op het platteland werkende mens dat centraal staat in Permekes oeuvre. Het was tevens in Astene dat hij de moed vond om na een hele reeks marines opnieuw enkele monumentale werken te schilderen. Dit schilderij past in deze periode. Hij bereikte in 1927 volgens Nanny Schrijvers, medewerker aan het KMSKA, een grote virtuositeit, mede door het succes van zijn tentoonstellingen en zijn deelname aan de Biënnale van Venetië.

Piet Boyens, auteur van Sint-Martens-Latem: kunstenaarsdorp in Vlaanderen, zegt over Permekes stijl:"Permekes kunst staat naar de geest het dichtst bij het expressionisme: instinctieve gevoelsontladingen manifesteren zich in een onstuimige gebarentaal. Heel beslist wijst hij de controle af die de vrije expressie dreigt te verstikken. Zijn figuren zijn groot, monumentaal, boven iedere menselijke maat. Een driestheid, een levensdrift stuwt langs alle zijden naar buiten. Zijn kunst is kosmische vervoering, passie, de som van koortsige aandoeningen die niet kristalliseren tot een afgewogen structuur, maar vrij uitstromen over soms half voltooide doeken. De schilderkunst van Permeke drijft vooral op het instinct, de kunstenaar klampt zich niet halsstarrig vast aan een stijl die in bedachtzaamheid steeds verder wordt gezuiverd. Het expressionisme dringt zich onmiddellijk op, zonder verfijnde berekening, met macht en met arrogantie soms, in gedurfde vervormingen en in een beangstigend directe stijl. Permeke lijkt de vertolker van het sociale drama van boer, visser en arbeider. Maar in het stoere geweld en de primaire grootheid van zijn wezens heeft hij vooral zijn eigen ontketend instinct zichtbaar gemaakt en zijn elementaire verbondenheid met de aarde - de donkere zwarte aarde van Permeke - een monument gegeven."

Beschrijving
Vespertijd is een goed voorbeeld van Permekes artistieke visie. Het kenmerkt zich door de massieve figuren, weergegeven in grote geometrische vlakken en een overweldigende monumentaliteit. Het werk bestaat uit dragende vlakken die passen in een sterk geconstrueerd geheel dat een grote evenwichtigheid uitstraalt. Steeds wederkerend zijn de door elkaar en over elkaar heen getekende en onvoltooide motieven. In Vespertijd, maar ook in Permekes andere werken, wendt de kunstenaar trefzeker en op zeer expressieve wijze de deformatie en hypertrofie van onder meer handen en voeten aan. Het coloriet is grauw.

Ondanks dat de figuren breed zijn, lijken ze geen plaats in te nemen. Ze danken hun stabiliteit en onbeweeglijkheid aan de rok van de vrouw en de plaatsing van de voeten van de man. Ook de uitdrukking van de figuren draagt bij tot de onbeweeglijkheid. Ze spreken niet en terwijl de man achter de vrouw kijkt, staart zij voor zich uit.

Wat de figuratie betreft, opteerde Permeke voor een zeer hoekig en vlak weergegeven man en vrouw tijdens hun namiddagpauze. De vrouw maalt koffie terwijl haar man een pijp rookt. Ze nemen het hele doek in beslag, waardoor er nauwelijks nog plaats is om de omgeving te schilderen. Enkel de leuningen van de stoel waarop het paar gezeten is en een klein hondje op de voorgrond, dat de frontaal aankijkt, is zichtbaar. De figuren hebben daarentegen geen aandacht voor het publiek, enkel voor hun pauze. Het is namelijk het voorlaatste gebed van de dag, verplicht opgelegd door de katholieke kerk. De personages zijn uitgeput van het werk, in gedachten verzonken en niet in staat tot een gesprek.

Materiële aspecten

Afmetingen

 127 × 148,5 cm (Dagmaat)
 128 × 147 × 2 cm (Volledig)
 150,5 × 171,3 × 10,6 cm, 22,4 kg (Inclusief lijst)

Signaturen

 1927
 Plaats: recto, links onder
 Type: handschrift
 Datum: 1927
 Permeke
 Plaats: recto, midden onder
 Type: handschrift
 Lettertype: onderkast met beginkapitaal
 Auteur: Constant Permeke

Afkomst
Het werk was aanvankelijk in het bezit van W. Kleinberg. Daarna kwam het in handen van een onbekende eigenaar, van wie het KMSKA het (dankzij de bemiddeling van Galerie Georges Giroux) kon aankopen.

Referentielijst
Walther Vanbeselaere in Aanwinsten tijdens de ambtsperiode 1948-1972, in Jaarboek van het Koninklijk Museum voor Schone Kunsten, 1973, p. 68.

Schilderij in het Koninklijk Museum voor Schone Kunsten Antwerpen
Werk van Constant Permeke

redpajama_set_name: RedPajamaWikipedia


text:
Exclusive: Dr. Katrina McFerran Responds To Reaction Towards Her Study On Music And Mood
Posted by Metal Insider on October 26, 2011
Last week, many in the metal community had strong reactions towards Dr. Katrina McFerran's recent study. At first glance of the University Of Melbourne's posting, and other articles about the study, it appeared that Dr. McFerran was implying that youth at risk of depression are more likely to listen to heavy metal music. However, as many readers pointed out, there was more to the study than what the abstract had implied. With that in mind, we decided to let Dr. McFerran better explain what her study was actually trying to find. Dr. McFerran, a senior lecturer in music therapy and editor of the Australian Journal of Music Therapy, was kind enough to share the following:
Music is important, but it's not magic. It can't control your mind, although I think it can make a difference in your life. So why did so many people think that my study was saying 'Metal music CAUSES mental illness'? It totally doesn't. Music is not that powerful. And nor do all people who like metal music suffer from depression; although some do. In fact, studies bigger than mine show that the link between psychological distress and liking metal music is stronger than for any other type of music. Why is it so?
Well, it seems mind-blowingly obvious that if life feels intensely bad right now, there is little solace to be found in pop music. Metal music contains both emotion and power, sometimes wrapped up with some pretty awesome musical displays, so it isn't rocket science to understand why people might turn to it. In my study of Australian teenagers, most people expressed a preference for metal, rock and hip-hop when they were feeling angry – it matched their mood. But what was most interesting was that metal-heads were significantly more loyal to their style – across all moods – whereas others were more eclectic in listening to different sounds to match different emotional states. That's all good.
But what about the sub-group of young metal fans who were psychologically distressed and reported feeling WORSE after listening? That's why my study hit the press – because we need to get a better understanding of why some young people, who are already distressed, might find their music listening makes them feel worse. Most people declare that music makes them feel better – it fulfills emotional needs, fosters social connections and is personally satisfying (North and Hargreaves). It revives us, entertains us, diverts us, provides strong sensations, clarity, understanding and solace (Saarakallio).
As a music therapist that works with teenagers, my job is to make sure that young people are getting the most out of their music. In theory, making music has a stronger relationship to health than listening does, so I encourage that – playing is related to flow, stronger social connections and the release of chemicals in the brain that create trust and promote bonding. But nothing is simple. Take for example going to a live concert – there's so much action involved that it doesn't make sense to suggest that it is only a listening experience. Or dancing in your room? Anyway, it's complicated. And there is no doubt that listening can be good too, for all the reasons I quoted above.
So here's my question: What about that group of young people who describe feeling worse? Do they feel worse because they're connecting with complicated memories or feelings, but then feel better later because they've processed stuff (delayed gratification)? And if so, why did they still rate themselves as feeling worse when reflecting on that experience weeks later? Do people who are already feeling bad need to make themselves feel worse for some reason – we all like to wallow sometimes, but when you are struggling with depression, it's a constant fight to try to move out of that state, so you don't necessarily want to do something that makes recovery even tougher. What do you all think? Has music listening ever made you feel worse – and what conditions led to that? I'm obviously not saying that it's all about the music – it's about life being reflected in the music, emotions that are experienced in the world being heard in the music, and hope being found in the music when the world sucks. Life is complicated and music usually helps with that. But perhaps not always.
You can look at the following PDF to read Dr. McFerran's study for yourself.
Tags: Dr. Katrina McFerran, The University Of Melbourne
Categorised in: Guest Blog
A Majority Of Metal Fans Are At Risk Of Depression? That's What A New Academic Study Says
Effects of Listening to Heavy Metal Music on College Students
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redpajama_set_name: RedPajamaCommonCrawl


text:
\section{Introduction}
The origin of the structure in the Universe is due to the
primordial density perturbations that already existed when cosmological
scales started entering the horizon after the final reheating.

Inflation can generate the primary source of the cosmological
perturbation, which is usually the vacuum fluctuation of a light scalar field.
In the original inflation model the primary perturbation of the light
field (i.e, the inflaton perturbation) is
converted into the curvature perturbation at the same time when the
perturbation leaves the horizon.\footnote{This mechanism
has been used for the PBH formation in Ref.~\cite{KKSY},
where the secondary inflation is considered for the creation of the
perturbation. This must be distinguished from the curvaton mechanism.}

However, later studies revealed that there are many other candidates
for the mechanism of generating the curvature perturbations after
inflation~\cite{Lyth:2002my, IRreheat, IPreheat, IPhaseTrans, Curvaton-paper,
pre-curv, Infcurvaton, Hybcurv, EKM, Pre-PBH}.
The idea of these alternatives is very simple:
~given that there are many scalar fields in the particle physics model,
there will be many fields displaced from their minima at the end of the
primordial inflation epoch, which leads to
 the multicomponent Universe after inflation where
any kind of isocurvature perturbations can be created.
Then the isocurvature perturbations
can source the creation of the curvature perturbations after inflation.

In this paper we consider an inflating curvaton~\cite{Infcurvaton,
infcurv-pre, Hybcurv, Furuuchi:2011wa, EKM} that
can lead to primordial black hole (PBH) formation.
Generation of the cosmic microwave background (CMB) perturbations is separated from the PBH formation,
since unification of these perturbations requires a highly
model-dependent argument that is not suitable for the purpose of this
paper.
Previously, such a unification scenario has been considered for the
running-mass model
or the Type-III hilltop inflation model~\cite{Kohri:2007gq,
Kohri:2007qn,pre-papers,
Erfani-pbh, Alabidi:2009bk, Alabidi:2012ex}.\footnote{Type-I hilltop
includes new inflation models in which the inflaton field rolls toward a larger value. Type-II hilltop includes supersymmetric hybrid inflation with a negative mass term in which the inflaton field rolls toward the origin.
Type-III hilltop includes running-mass models with a positive mass term in which the inflaton field rolls toward the origin.
One can find classifications of these hilltop models in
Ref.\cite{Kohri:2007gq}. }
PBH can also be produced from passive fluctuations~\cite{Lin:2012gs}.
(See also Ref.\cite{Linde:1212}.)
PBH in the curvaton model has been considered in Ref.\cite{PBH-curv-pre}
in connection with the so-called ``curvaton web''
concept~\cite{Curvaton-web}.

Our strategy is to separate PBH formation from the original inflation
scenario, so that PBH formation is liberated from the CMB conditions.
Note however that the seed perturbations are generated during primordial
inflation.

Although not mandatory, the secondary inflation may solve
cosmological problems of some specific models.
For instance:
\begin{enumerate}
\item The primordial inflation model may require e-foldings less than
      60 so that the model can explain the observed CMB.
      The short inflation could be needed to explain the spectral
      index and its running, or the inflation could be short because
      of the fast (rapid) rolling.
\item The model may predict unwanted relics after reheating. They must
      be diluted.
\item The model may not have an elementary dark matter (DM) candidate. Then
      the dark matter of the Universe must be explained by something
      other than the particles.
\end{enumerate}
The most optimistic scenario of the inflating curvaton is that all these
``problems'' are solved by the secondary curvaton inflation.

In the standard curvaton mechanism, the crucial assumption is that there
are two
components in the Universe, where one component
scales like matter ($\rho_\sigma \propto a^{-3}$)
while the other is the radiation ($\rho_r\propto a^{-4}$).
The inflating curvaton uses a slow-roll (or sometimes
fast-roll~\cite{Fast-roll}) field
instead of the oscillating
one, which is a natural generalization of the usual curvaton
mechanism.
We consider the slow- or fast-rolling curvaton (the inflating curvaton that
scales like $\rho_\sigma\propto a^{-3\epsilon_w}$) in the presence of
the radiation.
Then the curvature perturbation is expressed as~\cite{Lyth:2002my, Curvaton-paper}
\begin{equation}
\zeta=(1-f)\zeta_r+f\zeta_\sigma,
\end{equation}
where
\begin{eqnarray}
f&\equiv& \frac{\dot{\rho}_\sigma}{\dot{\rho}_r+\dot{\rho}_\sigma}
=\frac{3\epsilon_w \rho_\sigma}{3\epsilon_w \rho_\sigma+4\rho_r}
\nonumber\\
\zeta_r&\equiv& -H\frac{\delta \rho_r}{\dot{\rho}_r}
= \frac{\delta \rho_r}{4 \rho_r}
\nonumber\\
\zeta_\sigma&\equiv& -H\frac{\delta \rho_\sigma}{\dot{\rho}_\sigma}
=\frac{1}{3\epsilon_w }\frac{\delta \rho_\sigma}{\rho_\sigma}.
\end{eqnarray}
Here $\epsilon_w$ is defined as
\begin{equation}
\dot{\rho}_\sigma =-3\epsilon_w H \rho_\sigma.
\end{equation}

Unlike the usual curvaton mechanism, the constancy of
$\zeta_\sigma$ requires some debate in the practical calculation, since
there is no doubt that $\zeta_\sigma$ is time dependent when the
radiation density is comparable to the curvaton density.
However, after the beginning of the curvaton inflation,
the ratio of the radiation decreases rapidly, and $\epsilon_w$ will soon
behave like a constant.
In that sense the initial quantity of $\zeta_\sigma$ must be calculated
in the inflationary phase slightly after a few e-foldings, which however
must not be later than the significant evolution of the curvature
perturbation~\cite{Infcurvaton, EKM}.
In this paper $t=t_\mathrm{ini}$ is the time when the initial quantities
are defined.
Note that in the inflating curvaton model significant evolution occurs
when $\epsilon_w\ll 1$, while in the usual curvaton it occurs when
$\epsilon_w=1$.
The significant evolution is accompanied by the significant change of
the parameter $r_\sigma$, which will be defined later.
The curvature perturbation cannot evolve after $r_\sigma\simeq 1$.

In this paper we are assuming that the effective curvaton potential is
always quadratic ($=\pm \frac{1}{2}m_\sigma^2\sigma^2$)
so that the ratio $\delta \sigma/\sigma$ behaves like a
constant after the horizon exit.
Thinking about the scale dependence of the perturbation,
``the initial $\delta \sigma/\sigma$ measured at the horizon exit''
depends on the corresponding scale if $\sigma$ is moving during the
primordial inflation,
and finally the distribution of $\delta \sigma/\sigma$ becomes scale dependent.
For the curvaton mechanism, a small $\sigma$ at the horizon exit
means a large perturbation $\propto \delta \sigma/\sigma$ on that
scale.\footnote{When we were finalizing
the manuscript we found a new paper~\cite{AxionPBH}, in which the
usual curvaton mechanism has been considered for a similar PBH
formation.
The secondary inflation is the crucial difference, since it expands the PBH
scale and usually makes PBH heavier than the usual curvaton scenario.}
If the effective curvaton mass is determined by the main component of
the Universe, one can expect a small mass during
the radiation-dominated epoch~\cite{Lyth-moroi}.
With these simple assumptions we examine the PBH formation in the
generalized curvaton mechanism.\footnote{For the scalar field $\phi$
with the bare mass $m_\phi$, the effective mass $m_{\mathrm{eff}}\sim \pm
H^2$ has been estimated~\cite{Hubble-mass} for the supergravity theory
in the regime $H^2\gg m_{\phi}^2$.
The possible flip of the sign has been used in supersymmetric cosmology,
for instance in Ref.\cite{AD-MSSM} for the Affleck-Dine baryogenesis.
Here the sign may depend on the main component of the energy
density (and of course on the effective interactions) at that moment. The
result is mostly due to the
F-term contribution from the K\"{a}hler potential, which gives
$m_\phi^2\sim |F|^2/M_p^2\sim H^2$. A similar
contribution ($\sim V/M_p^2$), may appear in the
nonsupersymmetric theory of the gravity~\cite{Hubble-mass}. }

\section{Scale-dependent perturbation for the Inflating curvaton}

To show an illustrative scenario
we consider a new inflation scenario or a Type-I hilltop inflation
\cite{Kohri:2007gq} for the inflating curvaton, in which
the curvaton potential satisfies
$\epsilon_\sigma \equiv \frac{1}{2}M_p^2 \left(\frac{V'}{V}\right)^2\ll
1$ during the curvaton inflation~\cite{Infcurvaton, Hilltop-curv}.

Consider the effective potential for the inflating curvaton,
\begin{equation}
V(\sigma)=V_0 + \frac{1}{2}m_\sigma(H)^2 \sigma^2,
\end{equation}
where $m_\sigma^2<0$ is possible.
Here the effective mass is determined by the main component of the Universe.
As is shown in Fig.\ref{fig:potential}, we are assuming
 $m_\sigma^2>0$ during the primordial inflation while
$m_\sigma^2 <0$ during the curvaton inflation.
Hereafter we use the index ``$1$'' for the primordial inflation and ``$2$'' for the
curvaton inflation, respectively.
\begin{figure}[t]
\centering
\includegraphics[width=1.0\columnwidth]{potential.eps}
 \caption{We are considering a scenario in which the curvaton potential
 is flipped during the primordial inflation
because of the Hubble-induced mass, while it is negative
 during the secondary (curvaton) inflation.
The density of the curvaton is subdominant during the primordial inflation.}
\label{fig:potential}
\end{figure}

In this paper we are assuming a quadratic potential for the curvaton
so that $\sigma$ and $\delta \sigma$ can share
the identical equation of motion.
At the same time the equation becomes a linear differential equation
and consequently the ratio $\delta \sigma/\sigma$ behaves like a constant.
We are avoiding any deviation from the quadratic assumption.

Let us see why the ratio can bahave like a constant when
the quadratic potential is assumed for the curvaton.
For the simplest example, consider the equations when $m_\sigma$ and $H$ are
 constants,
\begin{eqnarray}
\label{eqomo0}
\frac{d^2\sigma}{d t^2}+3H \frac{d\sigma}{d t}+ m^2_\sigma (H)\sigma
&=&0,
\end{eqnarray}
where the equation has the solution of the
form $\sigma \propto e^{-\alpha t}$, and the coefficient $\alpha$ is given
by
\begin{equation}
\alpha\equiv \frac{3}{2}H
\left[1\pm \sqrt{1-\left(\frac{2m_\sigma}{3H}\right)^2}\right].
\end{equation}
Defining $\beta\equiv \alpha/H$, we find
\begin{equation}
\label{typical-eq}
\sigma(t) \sim \sigma(0) e^{-\beta Ht}\equiv\sigma(0) e^{-\beta \Delta N},
\end{equation}
where $\Delta N\equiv Ht$ is the number of e-foldings spent after the horizon
exit.\footnote{Here we have omitted the subscripts, but
the evolution must be calculated for both inflationary stages.}
For the curvaton perturbation ($\sigma\equiv \bar{\sigma}+\delta
\sigma$), the equation of motion after the horizon exit
gives~\cite{Fast-roll}
$\delta \sigma_k(t) \sim \delta\sigma_k(0) e^{-\beta\Delta N}$.
We thus find $\delta \sigma_k(t)/\sigma(t) \simeq \delta
\sigma_k(0)/\sigma(0)$ because of the cancellation of the evolution factor.
Although the mass flips its sign during the evolution, one can take the
initial condition every time at the beginning of the epoch to find a similar
evolution factor.
Here the growing solution ($\beta<0$) is possible when the mass term has
the negative sign~\cite{Hilltop-curv}.
The equation of motion gives either a fast- or slow-rolling solution when
$|\eta_\sigma|<3/4$ (i.e, when $|m_\sigma|<\frac{3}{2}H$),
where the eta-parameter is defined by
$\eta_\sigma \equiv \frac{m_\sigma^2}{3H^2}$.
As a consequence of the cancellation, the ratio $\delta \sigma/\sigma$
behaves like a constant as far as
the evolution is given by the separable function. (See also Sec.\ref{mode-ind}.)

For the inflating curvaton model, the source of the
 curvature perturbation is $\delta \sigma$, which leaves the horizon during the
 primordial inflation and evolves thereafter until the curvaton
 mechanism starts to work.
At the horizon exit, the spectrum is given by
\begin{equation}
{\cal P}_{\delta \sigma_*}=\left(\frac{H_1}{2\pi}\right)^2,
\end{equation}
where $H_1$ is the Hubble parameter during the primordial inflation.

Since we have two inflation stages (primordial and curvaton), we also
need to consider the horizon exit during the
curvaton inflation.
Indeed, Ref.\cite{KKSY} used the perturbation that leaves the horizon during the
second inflation and explains the small-scale
perturbations.\footnote{Another scenario has been considered in
Refs.\cite{Kohri:2007gq, Alabidi:2009bk, Kohri:2007qn, Erfani-pbh,
Alabidi:2012ex}.
Given that the curvature perturbation at the scale is given by
\begin{equation}
{\cal P}_{\zeta_\varphi}\simeq\frac{{\cal P}_{\delta
 \varphi}}{2\epsilon_\varphi M_p^2},
\end{equation}
the significant scale dependence may appear either from $\epsilon_\varphi(k)$
(running potential) or from ${\cal P}_{\delta \varphi}(k)$.
Our paper complements the approach given in
Ref.\cite{Alabidi:2009bk} for the running $\epsilon_\varphi(k)$.}
We are considering the opposite scenario, in which the
perturbation that exits the horizon during the primordial inflation
seeds the curvaton mechanism.
The scale dependence of the perturbation is illustrated in
Fig.\ref{fig:peak}.
We are focusing on the specific case in which the amplitude of the
curvaton perturbation becomes strongly scale dependent due to the
Hubble-induced mass during the primordial inflation.
For that reason we are not avoiding the $\eta$-problem of the
curvaton potential.

In our scenario the seed perturbation (the curvaton perturbation)
created during primordial
inflation is highly scale dependent and it is converted into the
curvature perturbation during the curvaton inflation.
Our scenario complements the running-mass model or the Type-III hilltop
inflation model considered in Refs.~\cite{Kohri:2007gq, Kohri:2007qn,
Erfani-pbh,
Alabidi:2009bk, Alabidi:2012ex}.

\begin{figure}[t]
\centering
\includegraphics[width=1.0\columnwidth]{peak2.eps}
 \caption{The field perturbation has significant scale
 dependence.
The peak appears at $k^{-1}_\mathrm{PBH}$, which corresponds to the
 scale that touches the horizon at the beginning of the curvaton inflation.
In this picture the amplitude of the perturbation that leaves the horizon
  during the first inflation decreases during primordial inflation
 (${\cal T}_1 \ll 1$), while it increases during curvaton inflation
(${\cal T}_2 \ge 1$).
The perturbation entering into the horizon during the intermediate
 epoch causes oscillation around its average and decreases its amplitude.
In the third picture, the perturbation newly created during the curvaton
 inflation is not dominating the amplitude at $k_\mathrm{PBH}$.}
\label{fig:peak}
\end{figure}

For later use, we define the evolution of the perturbations as
\begin{equation}
{\cal P}^{1/2}_{\delta \sigma}(t_\mathrm{ini})
\simeq \frac{H_I}{2\pi}\times {\cal T}_1 {\cal T}_{\mathrm{int}} {\cal T}_2,
\end{equation}
where $t_\mathrm{ini}$ denotes the time when the inflating curvaton
starts to work.
Here the $k$-dependent functions $ {\cal T}_1$, ${\cal T}_\mathrm{int}$ and $
{\cal T}_2$ denote the translation functions during primordial
inflation (${\cal T}_1\sim e^{-\beta_1 \Delta N_1}\ll 1$ for $\beta_1>0$),
intermediate evolution (${\cal T}_\mathrm{int}\simeq 1$ for
$\beta_\mathrm{int}\sim 0$)
and the second inflation (${\cal T}_2\sim e^{-\beta_2  \Delta N_2}> 1$
for $\beta_2<0$).
Here $\Delta N_1$ and $\Delta N_2$ are the number of e-foldings elapsed
during each inflation stage, defined for the perturbation
on that scale ($k=k_{\mathrm{PBH}}$).
$\Delta N_1$ is defined after the perturbation leaves the horizon,
and $\Delta N_2$ is defined before the inflating curvaton starts to work at
$t=t_\mathrm{ini}$.
${\cal T}_2$ is usually negligible for the inflating curvaton.

Here the inhomogeneity ($\delta \sigma$)
entering into the horizon can never be
kept frozen even if the potential is flat.
Oscillation around the average (not around the true vacuum)
starts just after the horizon entry and
the amplitude is decreasing in the expanding Universe.
If the oscillation is sinusoidal, the evolution of the amplitude can be
approximated as $\propto a^{-3/2}$, which causes a significant reduction
of the amplitude, as is illustrated in the second picture of Fig.\ref{fig:peak}.
We thus find a peak on the scale that touches the horizon at the
beginning of the curvaton inflation.
We are using this scale for the PBH formation.

For the PBH formation, we consider the spectrum of the source
perturbation ($\delta \sigma/\sigma$), focusing on the scale corresponding to the peak.
The scale of the PBH satisfies
\begin{eqnarray}
\ln\left(\frac{k_\mathrm{PBH}}{a_0 H_0}\right)&\sim&62-\Delta N_1- N_2
-\frac{1}{2}\ln\left(\frac{10^{14}\mathrm{GeV}}{H_1}\right)\nonumber\\
&&-\frac{1}{12}\ln\left(\frac{3H_1^2M_p^2}{\rho_{R1}}\right)\nonumber\\
&&-\frac{1}{12}\ln\left(\frac{3H_2^2M_p^2}{\rho_{R2}}\right).
\end{eqnarray}
Here $H_i$ is the Hubble parameter during
inflation, and $\rho_{Ri}$ is the energy density at the reheating
after each inflation stage.
The reheating after the first inflation could be avoided, but for
simplicity we are assuming the reheating.

Since the perturbation ($k=k_\mathrm{PBH}$)
does not enter the horizon before the curvaton
      inflation, there is a bound for $\Delta N_1$,\footnote{The number
      of e-foldings during inflation is usually given by
      $N=\ln\frac{a(t_e)H(t_e)}{a(t){H(t)}}\simeq
\ln\frac{a(t_e)}{a(t)}$. In the above calculation the factor $1/6$
appears because $H$ varies.}
\begin{eqnarray}
\label{mindeln}
\Delta N_1 &\ge&\frac{1}{6}\ln\left(\frac{3H_1^2 M_p^2}{\rho_{R1}}\right)
+\frac{1}{4} \ln\left(\frac{\rho_{R1}}{3H_2^2 M_p^2}\right)\nonumber\\
&\simeq&9 +
 \frac{2}{3}\ln\left(\frac{M_1}{10^{15}\mathrm{GeV}}\right)
-\ln\left(\frac{M_2}{10^{10}\mathrm{GeV}}\right)\nonumber\\
&&
+\frac{1}{3} \ln\left(\frac{T_{R1}}{10^{12}\mathrm{GeV}}\right),
\end{eqnarray}
where the scales are defined by $M_1^4 \equiv 3H_1^2M_p^2$ and
$M_2\equiv 3H_2^2M_p^2$.

Although the evolution of $\delta \sigma$ is highly nontrivial,
our final result does not depend explicitly on the evolution after the
horizon exit, as far as the curvaton potential is quadratic.
That is because the ratio $\delta \sigma/\sigma$ behaves like a constant
after the horizon exit and thus the quantity evaluated just
at the horizon exit is what we need for the PBH formation.
Therefore, we find the perturbation using $\delta \sigma/\sigma$, which
is  evaluated at the horizon exit~\cite{Infcurvaton, EKM},
\begin{eqnarray}
\zeta&\simeq& r_\sigma \frac{2R}{3\epsilon_w}
\frac{\delta \sigma}{\sigma}\nonumber\\
&\simeq&\frac{r_\sigma A}{3\eta_2}\frac{\delta \sigma}{\sigma},
\end{eqnarray}
where the equation of motion is approximated  by
$AH\dot{\sigma}\simeq -\partial V/\partial \sigma$ with the coefficient
$A=\beta$ for the fast-rolling and
$A=3$ for the slow-rolling.
Here $\eta_2$ denotes the value of $\eta_\sigma$ during the curvaton inflation.
The fraction
\begin{eqnarray}
r_\sigma&\equiv& \frac{3\epsilon_w \rho_\sigma}{3\epsilon_w
 \rho_\sigma+4\rho_R}\nonumber\\
&\simeq& \frac{3\epsilon_w}{3\epsilon_w +4 e^{-4N_2}}
\end{eqnarray}
is defined at the end of curvaton inflation and
throughout this paper we expect $r_\sigma\sim 1$ for simplicity.
In the above calculation we have used the ratio defined by $R\equiv \frac{m_\sigma^2\sigma^2}{2V_0}$
($m_\sigma^2<0$ is assumed during the curvaton inflation)
and the obvious relations
\begin{eqnarray}
\dot{\rho}_\sigma&\equiv&-3\epsilon_w H_2 \rho_\sigma \nonumber\\
\dot{\rho}_\sigma&\simeq& \frac{\partial V}{\partial \sigma}\dot{\sigma}.
\end{eqnarray}

The PBH is formed when the perturbation with the significant density
contrast ($\delta \rho/\rho\ge 0.1$) enters the horizon.
In our case the PBH formation occurs when the perturbation of the scale
$\sim k_\mathrm{PBH}$ becomes accessible within the horizon.
The typical mass of the PBH is given by~\cite{Green:1999xm, Alabidi:2012ex}
\begin{equation}
\frac{k_\mathrm{PBH}}{0.00974\mathrm{Mpc}^{-1}}\simeq
\left(\frac{g_*}{g_{*eq}}\right)^{-\frac{1}{12}}
\left(\frac{M_\mathrm{PBH}}{6.67\times 10^{50}\mathrm{g}}\right)^{-\frac{1}{2}},
\end{equation}
which gives
\begin{eqnarray}
M_\mathrm{PBH}
&\simeq & 10^{46}\mathrm{g} \left(\frac{g_*}{100}\right)^{-\frac{1}{6}}
\left(\frac{k_\mathrm{PBH}}{1 \mathrm{Mpc}^{-1}}\right)^{-2},
\end{eqnarray}
where $g_*$ is the degrees of freedom in the radiation.
Let us see more details of the scenario.

First, we need to check
that $\zeta$ at the PBH scale is dominated by the curvaton.
Since the creation of $\delta \sigma$ is also possible  in the secondary
inflation epoch, we need to compare it with the one generated during the
primordial inflation.\footnote{The spectrum of $\delta
\sigma$, which is (newly) created during curvaton inflation, must not
dominate the perturbation on the PBH scale,
since otherwise the curvaton mechanism is irrelevant for the PBH formation.}
We thus need the following condition at the beginning of the secondary
inflation:
\begin{equation}
\frac{H_2}{2\pi}<\frac{H_1}{2\pi} e^{-\beta_1 \Delta N_1},
\end{equation}
which gives a rather trivial condition,
\begin{equation}
\frac{M_2}{M_1}<e^{-\frac{\beta_1}{2} \Delta N_1}.
\end{equation}

Second, since the PBH formation requires significant density
contrast, we need
\begin{eqnarray}
\label{PBHsecond}
{\cal P}^{1/2}_{\zeta_\sigma}
&\simeq&\frac{r_\sigma A}{3\eta_{2}}\frac{H_1}{2\pi
\sigma_{k_\mathrm{PBH}}} \sim 0.1,
\end{eqnarray}
where $\sigma_{k_\mathrm{PBH}}$ denotes the value of $\sigma$ when the perturbation
      ($k=k_\mathrm{PBH}$) leaves the horizon.
Then we find
\begin{eqnarray}
\sigma_{k_\mathrm{PBH}} &\sim& \left(\frac{r_\sigma A}{3\eta_{2}}\right)
 \frac{H_1}{2\pi}\nonumber\\
&\sim& 10^{11}\mathrm{GeV}\left(\frac{r_\sigma A}{3\eta_{2}}\right)
\left(\frac{M_1}{10^{15}\mathrm{GeV}}\right)^2.
\end{eqnarray}

Third,
 $\zeta$ at the CMB scale must not be dominated by the curvaton.
The consistency at the CMB scale requires
\begin{eqnarray}
\label{PBHthird}
{\cal P}^{1/2}_{\zeta_\sigma}
&\simeq&\frac{r_\sigma A}{3\eta_2}\frac{H_1}{2\pi
			      \sigma_{k_\mathrm{CMB}}} <10^{-5}.
\end{eqnarray}

Therefore, from Eqs.(\ref{PBHsecond}) and (\ref{PBHthird}), we find
\begin{eqnarray}
\frac{\sigma_{k_\mathrm{PBH}}}{\sigma_{k_\mathrm{CMB}}}&\simeq&
e^{-\beta_1(N_1-\Delta N_1)}\nonumber\\
&<&10^{-4}.
\end{eqnarray}
This condition suggests that $\sigma$ moves significantly during the
primordial inflation stage.
We thus find
\begin{equation}
N_1-\Delta N_1 >9.2 \times \frac{1}{\beta_1}.
\end{equation}
Here the scale can be given by
\begin{eqnarray}
\left(\frac{k_\mathrm{CMB}}{k_\mathrm{PBH}}\right)&\simeq& e^{N_1 -\Delta N_1},
\end{eqnarray}
where $k_\mathrm{CMB}\le 1 \mathrm{Mpc}^{-1}$.
Note that the steep potential allows significant running of the perturbation
that leads to a small $k_{PBH}$ (heavy PBH).\footnote{Note however
that Eq.(\ref{PBHthird}) gives only the upper bound for the
perturbation. The bound gives the heaviest PBH.}

According to Carr {\it et al.} in Ref~\cite{Carr:2009jm}, only PBHs with
$10^{21} {\rm g} < M_{\rm PBH} < 10^{28} {\rm g}$ and $10^{35} {\rm g}
< M_{\rm PBH} < 10^{36} {\rm g}$ can be allowed to become dark
matter.\footnote{CMB observations might have already excluded the
latter parameter space. In addition, quite recently it was reported
that successful star formation could exclude PBH dark matter with
$10^{16} {\rm g} < M_{\rm PBH} < 10^{26} {\rm g}$~\cite{Capela:2012jz}.}
By observing $\mu$-distortion due to the dissipation of a large density
fluctuation at a small scale after the decoupling of the
double-Compton scattering, we will be able to check the amplitude of
the small-scale fluctuation by PIXIE~\cite{Chluba:2012we}.

As an illuminating example, consider $M_1\sim 10^{15}$GeV, $M_2\sim
 10^{10}$GeV and $T_{Ri}/M_i\sim10^{-3}$.
These give a typical set of the supersymmetric grand unified theory
 (SUSY-GUT) model.
Then we find that $N_1-\Delta N_1\simeq 10$ and
$N_2\sim 30$ (maximum curvaton inflation) gives
 $M_\mathrm{PBH}\simeq 10^{38}$g, or
$N_2 \sim 5$ (minimum curvaton inflation) gives
 $M_\mathrm{PBH}\simeq 10^{14}$g.
For $k_\mathrm{PBH}\sim 10^{5}\mathrm{Mpc}^{-1}$, we find
$N_1-\Delta N_1 \simeq 11.5$ and $\beta_1> 0.8$, which allows
$M_\mathrm{PBH}\sim 10^{36}\mathrm{g}$.

In the original argument of the inflating curvaton model,
there was a prediction for the running spectral index
($n'$)~\cite{Infcurvaton}.
(Note that this ``running'' is not for the PBH perturbation.
We are arguing here about the possible relation between the PBH mass and
the running spectral index of the CMB.)
A similar argument can be applied for the PBH model, which
suggests that a large $N_2$ (i.e, small $N_1$) gives both a large
$M_\mathrm{PBH}$ and an enhanced running of the CMB spectrum.

To be more precise about the relation between the CMB spectrum and
the PBH mass, let us assume that the primordial chaotic inflation is
driven by the
potential $\propto \phi^\alpha$ and that it generates CMB through the
conventional curvaton mechanism.
In that specific model we find the spectral index $n(k)-1\simeq -2\epsilon_1
=-\alpha/2N_1(k)\simeq -0.037\pm0.014$ with the running $n'\simeq
-\alpha/2N_1^2 \simeq -(0.037\pm0.014)/N_1$.
For the quadratic potential ($\alpha=2$), one will find $N_1
\sim 30$ from the spectral index, which cannot be realized without the
secondary inflation.
The running of the spectral index is enhanced because of the small
$N_1$, which could be distinguished from other predictions.
Note that in that model the second inflation is mandatory and the condition
$N_1+N_2\simeq 60-\ln(10^{-5}M_p/H_1)$ gives
the PBH mass  $M_\mathrm{PBH}\le 10^{38}\mathrm{g}$.
Here Eq.(\ref{mindeln}), which bounds $\Delta N_1$ from below,
is given by the scale of the inflating curvaton and thus it
can be related to the theory beyond
the standard model.
For instance, the gravity-mediated SUSY breaking may
predict the scale of the inflating curvaton at $\sim 10^{10}$GeV
and the inflating curvaton can dilute unwanted cosmological
relics of the model such as the gravitino or light moduli.

For the fast-roll inflation~\cite{Fast-roll}, the number of e-foldings is
usually expected to be smaller than 60 ($N_1<60$). In that sense the
secondary inflation is mandatory for the scenario.
Also, the inflating curvaton could have a very interesting application
to the rapid-roll inflation~\cite{Kofman:2007tr}.
Using the inflating curvaton, one can increase the inflation scale of
this model to such an extent that gravity waves could be generated without
worrying about curvature perturbation.
Anyway, the curvaton-like mechanism is inevitable if
the primordial inflation may not generate the required CMB spectrum.
If the primordial inflation is short, the mechanism must be accompanied
by the secondary inflation stage, which can be used either for CMB
or for short-scale perturbations.
In that sense the inflating curvaton is quite important for these models
that do not have enough e-foldings by themselves.

There are other types of observations by which we can check the large
running. If ${\cal P}_{\zeta}$ is larger than $\gtrsim 10^{-6}$ at small
scales, ultra-compact mini halos (UCMHs) can be produced, which may be checked
by observing future lensing events or gamma rays due to dark matter
annihilation~\cite{Josan:2010vn, Bringmann:2011ut}.
The observation may help distinguish the running-mass  or
the Type-III hilltop inflation model from
the inflating curvaton model, since in the running-mass inflation model
the perturbation on the CMB scale is fixed by the usual
CMB observation and therefore its tail could be observed at smaller
scales, while there is no such bound in the inflating curvaton model.

\subsection{Model dependence}
\label{mode-ind}
Basically, the evolution of the perturbation  before the curvaton mechanism
is highly mode dependent.
In order to avoid the model dependence,
we considered the ratio $\delta \sigma/\sigma$, for which the
model-dependent evolution cancels when the quadratic assumption is valid.
Any deviation from the quadratic assumption can lead to a highly
mode-dependent result, which does not meet the purpose of this paper.

In our calculation the ratio $\delta
\sigma/\sigma$ evolves like a constant before the beginning of the
curvaton mechanism.
Our observation is very simple: since $\sigma$ and $\delta\sigma$
 are sharing the same equation of motion (when the potential is
 quadratic and the perturbation is beyond the horizon), and the equation
 is a linear differential equation, their ratio
behaves like a constant.
The typical evolution is shown in Eq.(\ref{typical-eq}) for constant
$m_\sigma$ and $H$, which gives the identical evolution factor $\sim
e^{-\beta \Delta N}$ for both $\delta \sigma_k$ and $\sigma$.
The evolution is thus cancelled in the ratio.

\subsection{Non-Gaussianity}
There have been many papers suggesting that the local-type
non-Gaussianity could prevent PBH formation~\cite{PBH-ng} when
$f_{NL}<-0.5$.
This bound could be crucial for the oscillation curvaton,
since in that model one may find $f_{NL}\simeq -1$ when $r_\sigma\simeq 1$.
On the other hand, the exact non-Gaussianity in the inflating curvaton
scenario has been calculated in Ref.\cite{EKM},
\begin{eqnarray}
\label{NG-eq}
f_{NL}&=&
\frac{1}{r_\sigma}
\frac{5\epsilon_w}{4R}\left(\frac{gg''}{g^{'2}}-1\right)\nonumber\\
&&-5\epsilon_w+\frac{10}{3}
+\left(\frac{5}{2}\epsilon_w-\frac{10}{3}\right)r_\sigma\nonumber\\
&&+\frac{5}{2}\epsilon_w\left(\frac{1}{r_\sigma}-\frac{1}{R}\right),
\end{eqnarray}
where the ratio is defined as
$R\equiv \pm\frac{1}{2}m_\sigma^2\sigma^2/V_0$.
Note that $R$ is negative for the hilltop potential.
With the quadratic assumption we have
\begin{eqnarray}
g'&=&\frac{d g}{d \sigma_*}=\frac{g}{\sigma_*}\nonumber\\
g''&=& \frac{-g+g'\sigma_*}{\sigma_*^2}=0.
\end{eqnarray}
Here the non-Gaussianity is evaluated for the PBH scale perturbation of
the inflating curvaton.

Unlike the oscillating curvaton, $r_\sigma \simeq 1$ in the inflating
 curvaton does not lead to $f_{NL}\sim -1$.
For $r_\sigma\simeq 1$ there are cancellations in Eq.(\ref{NG-eq}),
which finally gives $f_{NL}>0$ for $R<0$.
For  $r_\sigma <1$ there is no cancellation but Eq.(\ref{NG-eq}) gives
$f_{NL}>0$.

We thus find that the sign of the non-Gaussianity parameter is plausibly
positive in our model.
The problem of the oscillating curvaton is avoided in the inflating
curvaton.

\section{Conclusion and discussion}
In this paper we have shown that the PBH formation with the typical mass
range $10^{14}\mathrm{g}\le M_\mathrm{PBH}\le 10^{38}\mathrm{g}$ is
possible if the curvaton potential is flipped due to the Hubble-induced
mass.

We have been avoiding a highly model-dependent argument, but the result
suggests that the inflating curvaton can generate the PBH that could
be the dark matter, and/or the PBH with the interesting scale
that could be observable in future
observations~\cite{Alabidi:2009bk, Alabidi:2012ex}.

The secondary inflation stage, which has been considered in this paper,
sometimes plays an important role in specific cosmological models.
Although it depends on the inflationary model, the spectral
 index can be tuned by changing $N_1$, which usually leads to an enhanced running
 of the spectral index.
In other cases one may expect fast-(rapid-) rolling inflaton
for the primordial inflation, which requires additional expansion.
In both cases the secondary inflation is mandatory for the scenario.

The inflating curvaton can also dilute unwanted
 cosmological relics that are produced after primordial
 inflation~\cite{second-inf}.
In the most optimistic case, the inflating curvaton solves the above problems
 and at the same time it explains the dark matter of the Universe.

Neither artificial interaction nor fine-tuning of the potential has been
 assumed for the mechanism.

Our result also suggests that the Universe's
 many isocurvature components
may naturally lead to significant short-length perturbations.
Even if they will not source PBH formation, they might leave an observable
signal in the small-scale perturbations.

In addition, at small scales the second-order induced gravitational-wave
signal can be larger than the first order in these types
of running models~\cite{Alabidi:2012ex}.
In Ref.\cite{Alabidi:2012ex}, Alabidi {\it et al.} studied this effect
and showed that one could discriminate models by observing gravitational
waves in the future project BBO/DECIGO.
Those observations at small scales may complement CMB observations
at large scales, or UCMHs and $\mu$-distortion at small scales
to reveal the physics related to the PBH formation.

\section{Acknowledgment}
T.M. and K.K. thank Anupam Mazumdar for valuable discussions in the
early stage of this work.
This work was started when T.M. was visiting Lancaster University.
C.M.L. thanks Kazuyuki Furuuchi for useful discussions.
K.K. is partly supported by the Grant-in-Aid for the Ministry of
Education, Culture, Sports, Science and Technology, Government of
Japan Nos. 21111006, 22244030, 23540327.

redpajama_set_name: RedPajamaArXiv


text:
More than a library
After the genocide of 1994, Rotarians led a successful campaign to build Rwanda's first public library. A bastion against ignorance and tyranny, it has become a gathering place where a culture of reading, the arts, and democracy thrives.
by Jina Moore Photography by Andrew Esiebo
Twenty-year-old Noella Umutoniwase and her friends have been hanging out at the library for as long as they can remember. They come to study in its quiet spaces, chill at its rooftop cafe, or chat with friends in the garden. In fact, if you ask her whether she remembers Kigali before there was a library, Umutoniwase scrunches up her face in disbelief. "Before there was a library?" she asks, as if evoking the dawn of time.
For her, it might as well be. The brainchild of Rotarians in Rwanda, the Kigali Public Library was born, at least as an idea, not long after Umutoniwase herself. Back then, the Rotarians who proposed it must have seemed crazy. Only six years before, more than 800,000 people had been killed in an event known today as the 1994 Genocide Against the Tutsi. Farms and businesses were destroyed, basic infrastructure was broken, Rwandans were traumatized. A public library must have seemed like a strange priority.
In the stacks, a patron reads a book titled Transforming Rwanda, one of the library's 19,000 volumes and 30,000 digital titles.
But the members of the Rotary Club of Kigali-Virunga, Rwanda's first English-speaking club, thought the idea made sense. One of them was Beth Payne, an economic, commercial, and consular officer at the U.S. Embassy in Rwanda and a fan of libraries; she had put herself through law school partly by working at one. But it was more than a personal affection: "I had always believed that a free library is one of the cornerstones of America's democracy," she says. When the Rotary Club of Kigali-Virunga was chartered, in 2000, Rwanda was focused on its future — on ensuring peace and reconciliation, stability and security, and economic growth — and Payne believed it was the perfect time to think about how literacy and access to information could support those goals.
Payne taught a class about the internet to Rwandan businesspeople. "I watched how they responded to this wealth of knowledge and information all of a sudden becoming available to them," she says. "So I suggested to our club that one of the ways to support stability and growth, even if it's not as direct as other ways, is by having a place where people can come and get information and knowledge. And that captured people's imaginations — although, I'll be honest, I was thinking of something a lot smaller."
Thinking small, however, wasn't something that the country's newest Rotary club wanted to do. Most of its members were Rwandans whose families had fled the country in 1959, in another episode of violence that many consider Rwanda's first genocide. They had grown up on stories of Rwanda and dreams of return, and now that they had arrived, they had ambitious ideas and limitless energy.
Gerald Mpyisi, the charter president of the Rotary Club of Kigali-Virunga and a key figure in the library's founding, was one of those people. He had grown up in Zimbabwe, gone to college in Uganda, and worked in Kenya, where he had loved the McMillan Library — Nairobi's oldest — a neoclassical edifice filled with literary treasures. He drew on the inspiration he had felt while wandering its stacks to galvanize his fellow club members. "Those of us who had lived outside knew the importance of libraries," Mpyisi says. "I said, 'Guys, let's think big. There's no public library in this country. Does anyone here know a country without a library?'"
"You cannot learn when you're in trouble. Psychologically, you just can't. A library needs peace."
Building a library was a daunting undertaking. But the club was new, energetic, and ambitious, and the members felt buoyed by the scale of the project. "Everyone was in unison; everyone thought it was a great idea, even though we didn't have the means. But if you don't dream big, nothing becomes a reality," says Cally Alles, a member of the Rotary Club of Colombo, Sri Lanka, who lived in Rwanda for more than two decades and is now that country's honorary consul in Sri Lanka. As a member of the French-speaking Rotary Club of Kigali, Alles helped start the English-speaking Kigali-Virunga club to channel the energy of the country's earliest returnees, many of whom had grown up in Anglophone countries. The club received a $2,000 Matching Grant from The Rotary Foundation for a computer and other items and decided to raise the construction funds itself, tapping support from then-U.S. Ambassador George McDade Staples, himself a member of the Kigali-Virunga club, and the country's president, Paul Kagame, who was the guest of honor at the club's first fundraiser in November 2000. In one night, the club brought in $250,000 in cash and pledges, about 20 percent of the project's total budget, Mpyisi says. "That boosted our morale," he says.
Rotarians carried the message abroad, and soon they and their friends were donating hundreds of books to the future library. The club began hosting monthly used book sales of duplicate or unneeded volumes, putting the proceeds toward the costs of construction. At the time, books in Rwanda were difficult to find, and prices were far beyond the reach of ordinary citizens, so the club's sales became hugely popular. Virtually all the books on offer would find homes, but some were more sought after than others. "This was when Americans were all getting rid of their encyclopedias," Payne recalls. "Imagine, in Rwanda back then, seeing a whole set of encyclopedias, and you could buy it for $5. People ate those encyclopedia sets up."
At one early book sale, President Kagame and his family showed up unannounced. His children picked out several books — and, Mpyisi remembers with a laugh, their father insisted on a receipt.
In fact, Kagame was a key figure in the library's evolution. In his personal capacity, he was among its first donors. Later, when the global economic crisis stalled the club's fundraising and slowed the library's construction, the president stepped in to help keep things moving, according to Paul Masterjerb, a member of the Kigali-Virunga club and the current chair of its library committee. In 2009, Masterjerb says, Kagame donated $500,000 personally and asked the country's ministers of finance, infrastructure, education, and culture to make a plan and allocate funds to finish building the structure.
In 2012, the library opened its doors. It is managed as a public-private partnership between the Ministry of Education and Innovation Group, a local company that offers online and offline creative platforms to communities. The partnership is overseen by a board that includes representatives from the offices of the president and the prime minister, as well as the Imbuto Foundation, a private foundation of first lady Jeannette Kagame that promotes literacy and other programs. The Rotary Club of Kigali-Virunga also has a seat on the board, held by the club's library committee chair. Masterjerb says this form of partnership ironed out some early wrinkles in the library's day-to-day functioning. Now, he says, it's "perfect."
A display inside the Kigali Public Library acknowledges the building as "a project of Rotary, dedicated to the Rwandan public."
Kigali Rotaractors use the library as a gathering space: (front row, from left) Paul Joseph, Jeremiah Thoronka, Gladys Keza, and Samuel Oluwapelumi; (back row) Abdel Essay, Hussinatu Bah, Abubakarr Barrie, and Foday Kargbo.
Nabu, a New York-based organization that champions literacy worldwide, has an office at the library, where it sponsors writing workshops and other events.
A boy inspects the robot he built at the library's robotic workshop.
Known as the "interactive zone," the library's ground floor has a large, colorful children's room, an internet cafe, and a self-guided language and culture lab called the Korea Corner.
"We all felt most comfortable at the library because it's a public place suitable for equal discussion between equal parties."
The Kigali Public Library has taken its place as a major institution in the now-bustling capital. On any given afternoon, the reading tables in the "study zone" are full of people in deep concentration, many of them secondary school or university students.
"The library came at the right time," says Jenipher Ingabire, the Kigali-Virunga club's current president. "We didn't have places you could sit down and read. During summer holidays, when my three children are at home, I take them to the library. We borrow books; sometimes we sit there and read together. For adults, I see it as an opportunity, as a good place for us as Rwandans. As a club, we are really proud to have built that place, for having come up with an idea that not everybody would have thought of at the time as a priority."
There are also older patrons for whom the library is part of a daily routine. Aime Byimana, 62, is one of them. He wants to start his own firm, and nearly every day for the past year, he has spent a few hours reading textbooks about information systems, corporate management, and business strategy. He finds the library, free and open to all, a hopeful and exciting place — and a reminder of how far Rwanda has come. "You cannot learn when you're in trouble. Psychologically, you just can't," he says. "A library needs peace."
Byimana doesn't have the money for the membership fee of 12,000 Rwandan francs, or about $13, that is required to check books out of the library. But many patrons say they prefer to leave the books on the shelves — and hold on to an excuse to get out of the house and come to the library, where they can peruse the more than 19,000 volumes that are housed on three floors (the library also has 30,000 digital titles in its collection). Byimana spends his days upstairs in the study zone; that floor also holds a collection of French books and a corner that's home to the Institut Français. The ground floor, or "interactive zone," has a large, colorful children's room, an internet cafe, and the Korea Corner, a kind of self-guided language and culture lab. The basement is the "collaboration zone," with a large conference room and smaller meeting rooms.
That is where Joseph Kalisa, current president of the Rotaract Club of KIE, coordinated the team that planned a national trauma symposium in February 2019 that brought together mental health practitioners, social workers, and community leaders. The symposium, the first of its kind in Rwanda, was one of the events held in 2019 to commemorate the 25th anniversary of the genocide, and Kalisa says the library was a key force in making the symposium possible. "The planning team chose the Kigali Public Library for its neutrality," he says. "We were 15 or 20 people from different organizations and NGOs, and we felt it was important to work from a neutral space where no one would be seen to be taking the lead. We all felt most comfortable at the library because it's a public place suitable for equal discussion between equal parties."
A thriving culture of arts and literature has also blossomed here. Huza Press, the first independent publisher in Rwanda, got its start in a library conference room in 2015. For several years, Huza Press offered a literary prize to encourage Rwandans to write their own stories and to identify emerging talent. Last year, on the library's rooftop exhibition and events space, the publisher launched RadioBook Rwanda, a three-part audiovisual chapbook series of new fables written in the tradition of Rwanda's old tales, the kind that Huza founder Louise Umutoni grew up listening to her parents read at bedtime. "The library is a space that's been created as a celebration of books, as a celebration of storytelling, as a celebration of literature," says Umutoni, who grew up in Uganda. "We've worked hard to reinforce that and to use the space that celebrates what we do as a publisher."
"The regimes that were here knew that the best way to rule over people was to keep them ignorant. If you have a library accessible to everyone, it's much harder."
Solange Impanoyimana feels the same loyalty, born of the same appreciation. She's a co-founder of Generation Rise, a local nongovernmental organization that uses literature as the foundation of a leadership curriculum that teaches girls in secondary school self-expression, confidence, and creativity through discussions, debates, and journaling about books. "The library promotes the culture of reading and helps people understand that reading is important, especially in the lives of young people," Impanoyimana says. "When young people have access to books, they are exposed to different opinions, different stories, different places. They train their minds to imagine new things or to be creative, not to find themselves locked in one place. The more they read, the more they can believe in different possibilities, not just what they have seen in their families."
Creating "a culture of reading" is precisely what Paul Masterjerb and his fellow Rotarians had in mind nearly 20 years ago. Though the young generation that fills the library's corridors today doesn't think in these terms, its elders believe that literacy is one of the most powerful tools to help fight the divisions that led to so much tragedy in the past. "The Rotarians thought that we need to boost a reading culture in our society so that the people can know more about what has been written historically in the world, and then they won't be pulled so much toward committing genocide," Masterjerb says.
Mpyisi, who chaired the club's library committee for six years, says that preventing another genocide was "at the core of our thinking" from the start. "You know, it was easy for simple-minded people to be influenced by bad government. The reason why people were so quick to kill their own people was because the majority of the people in the country were illiterate. For them, any word that comes from the government at any level, that is the gospel truth," he says. "The regimes that were here knew that the best way to rule over people was to keep them ignorant. If you have a library accessible to everyone, it's much harder to keep people ignorant."
For Nancy Wanny Mpadu, a 24-year-old medical student at the University of Rwanda, the tranquility that the library nurtures and protects for those who spend time there is like sunlight or oxygen — part of the invisible fabric of everyday Rwanda. She was born after the genocide, and heavy words like "reconciliation" and "stability" don't weigh on her the way they do on the generation before her. For Mpadu, another value stands out: equality. When she first walked past the library a year or so ago, she didn't know what it was or how it worked. "They told me the place is free for anyone to use," she says. "And I feel good seeing so many people here. I even see my senior colleagues here, senior doctors. It's a place any person, big or small, can come and mix with anyone else — a place that's equal for everybody."
• Jina Moore, formerly the East Africa bureau chief for the New York Times, has been reporting from Africa for 15 years.
• This story originally appeared in the February 2020 issue of The Rotarian magazine.
Rwanda's not-so-distant horror
A symbol of Rwanda's reconciliation, the library is an oasis of tranquility inside and out.
Peacebuilding and conflict prevention is one of Rotary's six areas of focus, as is basic education and literacy. Learn more at rotary.org/our-causes. Find out more about the Kigali Public Library at kplonline.org.
Rotarian Action Groups provide assistance and support to Rotary clubs and districts as they plan and implement community development and humanitarian service projects. For help with peace projects, go to rotarianactiongroupforpeace.org; for literacy projects, go to litrag.org.


text:
Food Stamp Increase 2023: What You Need to Know
By Aswini V Jan 19, 2023
Food Stamp Increase 2023: The Supplemental Nutrition Assistance Program (SNAP), also known as food stamps, is a vital safety net program that helps millions of Americans access nutritious food. In 2023, there is a proposal to increase the food stamp benefit amount for families and individuals who are struggling to make ends meet. This increase is aimed at helping those who have been impacted by the economic downturn caused by the COVID-19 pandemic. In this article, we will discuss the proposed food stamp increase, who will be eligible for the increased benefits, and how to apply for food stamps in 2023.
The Proposed Food Stamp Increase 2023
The proposed food stamp increase in 2023 is a part of the Biden Administration's efforts to provide relief to families and individuals who have been affected by the economic downturn caused by the COVID-19 pandemic. The proposed increase would raise the monthly benefit amount for SNAP recipients by 15%. This would be a significant boost for many families and individuals who are struggling to afford basic necessities, including food.
The proposed increase is also aimed at addressing the issue of food insecurity, which has been exacerbated by the pandemic. Food insecurity refers to the lack of access to enough nutritious food for an active and healthy life. According to the USDA, food insecurity rates have increased dramatically since the pandemic began. In 2020, an estimated 35 million Americans experienced food insecurity, a 70% increase from 2019. The proposed food stamp increase would help to mitigate this issue by providing additional assistance to those who need it most.
Eligibility for the Increased Benefits
To be eligible for the increased food stamp benefits in 2023, individuals and families must meet certain income and resource requirements. These requirements vary depending on the state in which the individual or family lives. However, generally, households with incomes at or below 130% of the federal poverty level are eligible for SNAP. Additionally, households with children, the elderly, and the disabled may have higher income and resource limits.
It's important to note that eligibility for SNAP is based on the household's gross income, which includes all income before taxes and deductions. This includes wages, salaries, self-employment income, and rental income, among others. Additionally, the household's resources, such as cash, checking and savings accounts, stocks, and bonds, must also be considered when determining eligibility.
How to Apply for Food Stamps in 2023
Applying for food stamps in 2023 is a relatively simple process, and there are several ways to do it. The most common way is to apply online through the SNAP website. The online application process is easy to navigate and can be completed in a relatively short amount of time. However, if you prefer, you can also apply for food stamps by mail or in person at your local SNAP office.
When applying for food stamps, you will need to provide certain information such as your household income, resources, and expenses. You will also need to provide proof of your identity, such as a driver's license, passport, or birth certificate. Additionally, you will need to provide proof of your income, such as pay stubs, bank statements, or tax returns.
The proposed food stamp increase in 2023 would provide much-needed assistance. To millions of Americans who are struggling to make ends meet. The increase would raise the monthly benefit amount for SNAP recipients by 15%, providing a significant boost for many families. And individuals who are struggling to afford basic necessities, including food. The proposed increase is also aimed at addressing the issue of food insecurity, which has been exacerbated by the pandemic. Eligibility for the increased benefits will depend on the individual.
Vidant HR Phone Number: Contacting Human Resources
Henry County Schools Payroll Dates: Keep Track of Your Earnings


text:
Q: IOS Social framework and image post I am experimenting with the Social Framework.
I was wondering if there is any possible way to attach the last photo taken and currently saved in the camera roll using this implementation from my app:
 - (IBAction)shareByActivity:(id)sender {
    NSArray *activityItems;

    if (self.sharingImage != nil) {
        activityItems = @[self.sharingImage, self.sharingText, self.addURL];
    } else {
        activityItems = @[self.sharingText, self.addURL];
    }

    UIActivityViewController *activityController =
    [[UIActivityViewController alloc] initWithActivityItems:activityItems
                                      applicationActivities:nil];

    [self presentViewController:activityController
                       animated:YES completion:nil];
}

If so how do I modify the shareImage name in this specific portion of my -(void)viewDidLoad ?
self.sharingImage = [UIImage imageNamed:@"notSureWhatToPutHere"];

Everything works well, the social panel opens and has all the needed service. My only request is to find out how to call the latest image from the camera roll.
I am not sure if I need the image real name or if there is any other way to achieve what i would like: a post with a picture attached (most recent picture in camera roll).
Any help is appreciated.

A: You can pretty painlessly get the last image in the camera roll using the asset library framework. Give this a try:
#import <AssetsLibrary/AssetsLibrary.h>

Then to get the image:
ALAssetsLibrary *cameraRoll = [[ALAssetsLibrary alloc] init];
[cameraRoll enumerateGroupsWithTypes:ALAssetsGroupSavedPhotos usingBlock:^(ALAssetsGroup *images, BOOL *stop) {
    [images setAssetsFilter:[ALAssetsFilter allPhotos]];
    [images enumerateAssetsAtIndexes:[NSIndexSet indexSetWithIndex:[images numberOfAssets] - 1] options:0 usingBlock:^(ALAsset *result, NSUInteger index, BOOL *stop){
        if (result) {
            ALAssetRepresentation *rep = [result defaultRepresentation];
            self.sharingImage = [UIImage imageWithCGImage:[rep fullScreenImage]];
        }
    }];

}
                        failureBlock: ^(NSError *error) {
                            NSLog(@"An error occured: %@",error);
                        }];

A: Thanks for the great help NSPostWhenIdle!
I was able to resolve the issue of getting "newest photos" from camera roll by moving my ALAssettsLibrary chuck of code away from viewDidLoad and created a refreshAlbum
 - (void) refreshAlbum
{
ALAssetsLibrary *cameraRoll = [[ALAssetsLibrary alloc] init];
[cameraRoll enumerateGroupsWithTypes:ALAssetsGroupSavedPhotos usingBlock:^(ALAssetsGroup *images, BOOL *stop) {
    [images setAssetsFilter:[ALAssetsFilter allPhotos]];
    [images enumerateAssetsAtIndexes:[NSIndexSet indexSetWithIndex:[images numberOfAssets] - 1] options:0 usingBlock:^(ALAsset *result, NSUInteger index, BOOL *stop)
     {
         if (result) {

             ALAssetRepresentation *rep = [result defaultRepresentation];
             self.sharingImage = [UIImage imageWithCGImage:[rep fullScreenImage]];
         }
     }];
}
                        failureBlock: ^(NSError *error) {
                            NSLog(@"An error occured: %@",error);
                        }];
}

Then I am calling the newly created refreshAlbum from the same button that enable the shareByActivity
- (IBAction)refreshButton:(id)sender {
    [self refreshAlbum];
}

This work particularly well as my app does not have any picture to share as it starts up.
The first time that imageShare become available is after activating the shareByActivity button that now carries the refreshButton function as well!
Thanks again, this really work.

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