text:
\section{Introduction}

Nearly ten years after the discovery of the first Gamma-Ray Burst (GRB)
afterglow  in the optical/near-infrared \citep{Groot1997, vanParadijs1997},
the progress in the understanding of the GRB phenomenon is enormous
\citep[e.g.,][]{ZhangMeszaros2004, Piran2005}. From the observational point of
view nearly every individual afterglow has turned out to be specific in some
sense. The richness in afterglow properties observed so far is not much
surprising, however, given the fact that the afterglow phenomenon combines
internal properties of the underlying burster population with  properties of
the external circumburster medium. This in combination with redshift provides
a large parameter space for various flavors of GRB afterglows. However, in
spite of their individualities, as an ensemble afterglows trace the underlying
physical boundary conditions and the parameter space of the physical processes
involved. Revealing this parameter space is of fundamental interest since it
might much improve the understanding of the afterglow phenomenon. This has
already motivated several groups to perform a systematic analysis of
observational data from various afterglows \citep[e.g.,][]{Frontera2000,
PK2001a, PK2001b, PK2002, Yost2003, Frail2003a, Frail2004, Stratta2004,
Gendre2005, P2005a, P2005b}. The present work continues this kind of
investigations but concentrates on the optical/NIR bands.

While a fit of the observed broad-band spectral energy distribution (SED) of
an afterglow from the radio to the X-ray band is the best way in order to
extract the underlying physical parameters \citep[e.g.,][]{Frail2003b,
Yost2002, P2005b},  one might expect that the optical/NIR data alone are
completely explainable within the context of the underlying theoretical
model. In particular, in most cases it is the optical/NIR region where the
sampling and the quality  of the afterglow data is best.  It is clear that any
reliable theoretical model must be able to explain the observed richness in
the phenomenology of optical light curves of GRB afterglows. In this respect
it is worth summarizing and exploring the available data base on  afterglows
in the optical/NIR bands. This holds in particular with respect to the new era
in GRB research initiated by the launch and operation of the \emph{Swift}
satellite \citep{Gehrels2004}.

In the present paper we continue our systematic analysis of afterglow
parameters based on optical and near-infrared data (Zeh, Klose, \& Hartmann
2004, hereafter Paper I; Zeh, Klose, \& Hartmann 2005). Our study includes
$all$ afterglows in the pre-\emph{Swift} era with sufficient published
data. While in Paper I we analyzed the afterglow light curves with special
emphasis on an underlying supernova component, the goal of the present paper
is to explore the parameter space of the light curve parameters and of
physical quantities related to them. In Paper III \citep{KKZ}, we expand this
analysis to the spectral energy distribution of afterglows in the optical and
near-infrared bands in order to search for signatures of dust in GRB host
galaxies.

\section{Data analysis \label{data}}

We collected from the literature all available photometric data on GRB
afterglows observed by the end of 2004 and checked them for consistency. We
modeled the light curve of the optical transient (OT) following a GRB as a
composite of genuine afterglow light, supernova (SN) light, and constant light
from the underlying host galaxy. The afterglow is either modeled by a single
or a smoothly broken double power-law according to  \cite{Beuermann1999}.
Our fitting procedure is based on a $\chi^2$ minimization with a
Levenberg-Marquardt iteration. This minimization technique provides formal
uncertainties of the fitted parameters through the covariance matrix. For the
remainder of this paper, all uncertainties are 1$\sigma.$

We always fitted photometric magnitudes with a fitting equation as follows:
\begin{eqnarray}
m_{\rm OT}(t) &=& -2.5\,\log\{10^{-0.4\,m_c}
[(t/t_{\rm b})^{\alpha_1\,n} + (t/t_{\rm b})^{\alpha_2\,n}]^{-1/n} \nonumber \\
              &+& k\,10^{-0.4\,m_{\rm SN}(t/s)} + 10^{-0.4\,m_{\rm host}}\}\,.
\label{mag1}
\end{eqnarray}
The parameters in Equation~(\ref{mag1}) are the prebreak decay slope
$\alpha_1$, the postbreak decay slope $\alpha_2$, the break time $t_{\rm b}$,
the steepness of the break $n$, the brightness of the host galaxy $m_{\rm
host}$, the constant $m_c$ which corresponds to the magnitude of the fitted
light curve for the case $n=\infty$ at the break time $t_{\rm b}$ (it stands
for the intersection point of the prebreak and the postbreak slope,
without considering a smooth transition), as well as
the supernova parameters $k$ and $s$, which indicate the luminosity ratio and
the stretch factor normalized to SN 1998bw (cf. Paper I). If there is no break
in the light curve, then Equation~(\ref{mag1}) reduces to
\begin{eqnarray}
m_{\rm OT}(t) &=& -2.5\,\log\{10^{-0.4\,m_1}t^{\alpha} \nonumber \\
              &+& k\,10^{-0.4\,m_{\rm SN}(t/s)} + 10^{-0.4\,m_{\rm host}}\}\,,
\label{mag2}
\end{eqnarray}
where $m_1$ is the brightness of the afterglow at $t=1$ day after the
burst. Before the fitting process the data were corrected for Galactic
extinction using the maps of \cite{Schlegel1998}. For a more detailed
description of our procedure we refer to Paper I.

In the present paper, our input list contains 59 optical/NIR afterglows
observed in the pre-\emph{Swift} era which allowed us to perform a fit
(Table~\ref{tabres}).  Sixteen of these have a well-sampled light curve in at
least one photometric band (mostly the $R_C$ band). These light curves show a
well-detectable break and have sufficient data points before and after the
break time, so that the prebreak decay slope and the postbreak decay slope
according to Equation (\ref{mag1}) are well-defined. More precisely, our
selection criterium for the best-defined afterglow light curves is that the
$1\sigma$ error  is less than 0.2 for $\alpha_1$, less than 0.3 for
$\alpha_2$, and less than 1 day for $t_b$ (Table~\ref{tabres}).  We did not
use the accuracy of the fit ($\chi^2$ per degrees of freedom) as a selection
criterium, however.  We consider Equation (\ref{mag1}) as an empirical first
order approximation of an observed light curve and all deviations from the
corresponding fit as fine structure (\S~\ref{FineS}).  Light curves with no
break are by definition excluded from this sample of best-defined  afterglows,
because it cannot be ascertained with complete certainty if the slope is a
pre- or postbreak.  Whenever we did not  detect a break, the data quality was
usually insufficient to exclude the possibility of a jet break in the light
curve. In these cases there is either no early time data available, or the
break could have been missed because of a bright host galaxy or an underlying
SN component.

All but one (GRB 980519) of the 16 afterglows  in our sample have a known
redshift, none of these bursts is classified as an X-ray flash\footnote{While
GRB 030429 is classified as an XRF in the observer frame \citep{Sakamoto2005},
it would be an X-ray rich GRB in the host frame with $E_{peak}=93^{+32}_{-21}$
keV.}. For the present study the afterglows of GRB 021004 and GRB 030329 were
excluded from our analysis because of their many rebrightening episodes (see
also \S~\ref{FineS}). In the case of the afterglow of GRB 030329, we performed
two additional fits that are also given in Table \ref{tabres}, the details are
in Appendix \ref{individual}. While these fits give very good results, they
are based on only a small part of the light curve and we thus do not include
their results in the selected sample for statistical study, with the exception
of Figure \ref{a1n}. The afterglow of GRB 000301C also shows a rebrightening
episode \citep[around 3.5 days after the burst;][]{GLS2000, Gaudi2001}, but as
the deviations are not that large and occur only during a certain period, the
light curve can still be fitted with a broken power-law, even though
$\chi^2_{\rm d.o.f.}$ becomes relatively large.

A special note is required for GRB 021211. The afterglow light curve  of this
burst fulfills the aforementioned criteria for the amount of the $1\sigma$
error bars of the fit parameters, nevertheless we have not included it  in our
subsample of well-defined light curves. According to our data, the light curve
shows a break 0.11$\pm$0.09  days after the burst with a steepening by
$\Delta\alpha = \alpha_2 - \alpha_1 = 0.26 \pm 0.11$.  This is in close
agreement with the amount of steepening expected for the passage of the
cooling break across the optical window \citep[for a Compton parameter less
than 1; e.g.,][]{PK2001a}. In addition, \cite{Nysewander05} report on evidence
for color changes  of the afterglow just  around this time. Given the fact
that  no optical data have been reported in the literature for the time period
between  1 and 10 days after the burst, we consider it as very likely that the
break in the light curve we have found does indeed signal the passage of the
cooling break \citep[as already suspected by][based on their finding of color
changes]{Nysewander05}, while the real jet break occurred between 1 and 10
days after the burst. Note that the light curve break around 0.11 days is not
identical to the break discussed by others concerning the very early light
curve, which has been attributed to the reverse shock \citep{Li03,Fox03,
Wei03, Holland04, KP03}. Given these findings, and  since we try to keep our
subsample as homogeneous as possible, we have not included this burst in the
following study.

The light curve parameters we have deduced from our data might be slightly
different to those obtained and used by other groups.  This is mainly due to
the fact that we use a different, and most likely larger data base. In
addition, there is still some bias in the selection of the data, in the
definition of what are outliers, which data should be used and which data
should not. While we do not claim that our data base is the best for every
individual GRB, most probably it is the most comprehensive set. The strength
of our approach is that we analyze all afterglow light curves using the same
numerical procedure. In this respect we are confident that the results we
obtain are statistically robust.

\section{Results}

The results of our light curve fitting of the individual afterglows are
summarized in Table~\ref{tabres}. Here, the second column indicates the sample
of the best-defined 16 afterglows. In some cases we could only derive upper or
lower limits for some parameters, because the light curve was poorly sampled
(see \S~\ref{individual}). In the following we discuss only the results
obtained for this sample of 16 afterglows.

The distributions of the deduced light curve parameters are shown in
Figures~\ref{a1Histo} to \ref{logtbz}. The mean of the prebreak decay slope is
$\alpha_1 = 1.05\pm 0.10$, with $\alpha_1$ ranging from $0.58\pm0.05$ (GRB
000301C) to $\alpha_1=1.76\pm0.05$ (GRB 011121), while $\alpha_2$ ranges from
$1.30\pm0.02$ (GRB 041006) to $3.03\pm0.27$ (GRB 030429) with the mean at
$2.12\pm0.14$. About half of the postbreak decay slopes have $\alpha_2<2.0$.
Both distributions overlap in the interval from about 1.3 to 1.7. The
distribution of $\alpha_2$ is almost constant, with a possible cutoff around
1.3 and no preference for any value.

Figure~\ref{DaHisto} displays the distribution of the difference of the decay
slopes before and after the break, $\Delta\alpha=\alpha_2-\alpha_1$.  The
distribution is asymmetric with its maximum around 0.8 and a longer tail
towards higher values. It is notably broader than the distribution of
$\alpha_1$ and $\alpha_2$. It also indicates the possibility that some
afterglows could have very shallow breaks with $\Delta\alpha< 0.3$ that could
easily be missed. The gap around $\Delta\alpha=1.7$ is probably due to
low-number statistics and we do not consider it to be significant. In this
respect we cannot confirm the potential evidence for a bimodality of the
distribution of $\Delta\alpha$ \citep{P2005a}, allthough we cannot
reject this possibility either.

In Figure~\ref{logtbz} we present the distribution of the observed break times
for the afterglows with the best-defined light curves, but translated into the
corresponding GRB host frame. This distribution is strongly asymmetric with a
clear peak in the host frame at lower values around 0.3 days. That most breaks
occur at relatively early times supports the view that in several cases
(Table~\ref{tabres}) light curve breaks might have been missed due to a lack
of early-time data. The afterglow with the earliest break in the host frame
was GRB 041006, while the afterglow of GRB 000301C had the latest break
time. On the other hand, late breaks might have been missed in several cases
too, because the afterglow was already too faint at the break time, and/or an
underlying SN component or a bright host galaxy simply made the discovery of
the break in the optical bands impossible. We conclude that these data
indicate, even though they do not prove, that in fact all afterglow light
curves have detectable breaks due to a collimated explosion, as long as they
are not hidden by rebrightening episodes as in GRB 030329
\citep[e.g.,][]{Lipkin2004}. It is clear that any model that explains the
observed light curve breaks must be able to reproduce this observed
distribution (Figure~\ref{logtbz}).

The distribution of the shape parameter $n$ (Equation~\ref{mag1}) is more
difficult to quantify. While for about half of the afterglows the data allowed
us to determine $n$ during the fitting procedure, in the other cases $n$ did
not converge during the fit ($n\rightarrow\infty$), because the sampling of
the data is not good enough. It is worth noting that whenever we were able to
determine $n$, we obtained a relatively soft break ($n\approx1-2$) and in each
case the prebreak decay slope $\alpha_1$ was very shallow. In the
other cases we had to fix $n$ at a relatively large value in order to obtain
an acceptable fit, and we chose $n=10$. Choosing $n\approx1-2$ made the fit
worse. Whether this indicates a possible bimodal distribution of the parameter
$n$ is an open question. The distribution of the shape parameter $n$ is the
biggest unknown, so far, including its theoretical interpretation.

\section{Discussion}

\subsection{Wind versus ISM models \label{profile}}

Figure~\ref{a1a2} shows the correlation between the parameters $\alpha_1$ and
$\alpha_2$ in comparison with eight standard afterglow models that cover the
cases (1) $\nu < \nu_c$, (2) $\nu_c < \nu, Y<1$, (3) $\nu_c < \nu, Y>1,
2<p<3$,  (4) $\nu_c < \nu, Y>1, p>3$  for the ISM and for the wind model,
where $\nu$ is the observed frequency and  $Y$ is the Compton parameter
\citep[][their eqs. 21, 22 and 29]{PK2001a}.  Those models with $\nu < \nu_c$
and $Y<1$  require $p<2$ in order to explain an observed $\alpha_2<2$.  In
particular, there is a group of five bursts (GRBs 990123, 991216, 010222,
030328, 041006) that cluster around $\alpha_2=1.5$. Within the
corresponding 1$\sigma$ error bars $\alpha_2>2$ is basically ruled out and so
is $p>2$. Such shallow postbreak decay slopes cannot be explained by a flat
electron distribution either \citep {Dai2001, B2001, Wu2004}.

Based on the underlying theoretical models, which predict $p=\alpha_2$,
then we find that the parameter space of $p$ is rather broad, ranging from
about 1.5 to 3. While the results obtained for $p$ for the individual
afterglows differ among various authors, all studies agree that within the
current theoretical framework no evidence for a universality of $p$ is found
\citep[e.g.,][;Paper III]{PK2001a, PK2001b, PK2002, Preece2002, Yost2003,
P2005b}. This is contrary to what one might expect from theoretical models of
highly relativistic shocks \citep{Achterberg2001, Kirk2000}, and contrary to
what one might prefer on theoretical grounds \citep{FW2001}.

If one allows for $p<2$ then an inspection of Figure~\ref{a1a2} shows that a
wind model with $\nu < \nu_c$ is preferred for GRBs 980519, 990123, 991216,
000926, 020124, 020405, 030328, and 041006, even though GRBs 990123, 991216
and 000926 lie fairly off the models because of their relatively small
$\alpha_2$ or large $\alpha_1$. On the other hand, an ISM model with $\nu <
\nu_c$ is preferred for GRB 990510 and GRB 011211. GRB 020813 is either an ISM
case with $\nu < \nu_c$ or an ISM/wind case with $\nu > \nu_c$, in the
following, we will assume this to be an ISM case. Two afterglows (GRB 010222
and GRB 011121) could be an ISM or a wind case with $\nu > \nu_c$. In the case
of GRB 011121, the error bars are so large that $\nu < \nu_c$ cannot be fully
excluded.  Finally, the afterglows of GRBs 000301C, 030226, and 030429 are
outliers because of their relatively large $\alpha_2$. It is noteworthy that
all afterglows with soft breaks in the light
curve ($n\approx1-2$) belong to the group of bursts that are less compatible
with a wind profile, and all these afterglows have $\alpha_1<1$.

It is difficult to quantify whether the outliers really represent a different
population or whether in these cases the light curves are simply ill-defined.
For example,  the afterglow of GRB 000301C was affected by a strong
rebrightening episode that has been modeled by a gravitational microlensing
event \citep{GLS2000}. As these authors note, the removal of this event
leads to $\alpha_1\approx1.1$, which would shift GRB 000301C toward the
theoretical prediction of the ISM model with $\nu < \nu_c$. In the case of GRB
030226 there is evidence that the afterglow light curve showed fluctuations.
In combination with the relatively sparse set of postbreak data it is well
possible that the late-time observations stopped when the afterglow underwent
a fluctuation, so that finally  the deduced postbreak decay slope is too
large. On the other hand, early-time spectra of this afterglow reveal features
that can be best understood as due to a stellar wind profile
\citep{Klose2004}. In the case of 030429, \cite{Jakobssonz030429} find that
the light curve undergoes a significant rebrightening around 1.7 days after
the burst. They suggest to exclude the data around the rebrightening from the
fit and fix $\alpha_2=1.7$ (deduced from the SED and the $\alpha - \beta$
relations). In this case the light curve would be compatible with an ISM/wind
model and $\nu>\nu_c$, although it is unclear how large the error in
$\alpha_2$ would be.

If we neglect GRBs 000301C, 030226, and 030429, then Figure \ref{a1a2} shows
that the group of optical afterglows that is compatible with a wind model is
notably larger than the group of afterglows that prefers an ISM model.  While
basically all studies in the literature  agree that afterglows seem to
separate into a group that can be best described by a wind model and a group
that can be best described by an ISM model, our data show that the wind
scenario is statistically preferred. In fact, within their 1$\sigma$ error
bars nearly all $(\alpha_1, \alpha_2)$ pairs are compatible with a wind
profile while for the ISM model  such a statement is clearly ruled out.

\subsection{The jet opening angles \label{theta}}

Figure~\ref{thetaHisto} displays the distribution of the jet half-opening
angle, $\theta_{\rm jet}$, for our sample of 16 bursts (GRB 980519 is not
included as no redshift of this burst is known) as derived from the observed
break time, assuming the uniform jet model \citep{Rhoads1999}. We calculated
$\theta_{\rm jet}$ following \cite{Sari1999} for an ISM medium (GRBs 990510,
000301C, 011211, 020813, 030226, 030429) and \cite{Bloom2003} for a wind-like
medium (GRBs 990123, 991216, 000926, 010222, 011121, 020124, 020405, 030328,
041006), according to the results obtained for the density profile of the
individual afterglows (\S~\ref{profile}). For the isotropic equivalent energy
$E_{\rm iso}$, the radiation efficiency and the redshift we adopted the values
given by \cite{Friedman2005}. In the case of an ISM model we used the
circumburster density as given in \cite{Friedman2005}, while for the wind
model we assumed a mass-loss rate to wind speed ratio of $A_* =1$
\citep[cf.][]{Chevalier2000}. The distribution of $\theta_{\rm jet}$ that we
have found is strongly asymmetric with a peak between 2 and 5 degrees, has a
lower cutoff around 2 degrees and rapidly falls towards larger angles, in
agreement with what has been found in previous studies \citep{Frail2001,
PK2001b, PK2002, Bloom2003}.

\subsection{Correlations \label{correlations}}

Using the derived jet half-opening angles (\S~\ref{theta}) we find that the
distribution of the beaming corrected energy release in the gamma-ray band
ranges from $E_{\rm cor}=10^{49.9}$ erg (GRB 041006) to $E_{\rm
cor}=10^{51.4}$ erg (GRB 990123). In combination with the corresponding peak
energies, $E_{\rm peak}$, in the gamma-ray band \citep{Friedman2005}, in
Figure~\ref{EcorEpeak} we plot the correlation between $E_{\rm cor}$ and
$E_{\rm peak}$ in the GRB host frame, as it was  first reported by
\cite{Ghirlanda2004}. Considering  bursts \#9 and \#12 as outliers and
excluding them from the fit, we find $E_{\rm peak}\simeq 748\, (E_{\rm
51,cor})^\eta$, with $\eta = 0.79 \pm 0.09$.  This is  in qualitative
agreement with Ghirlanda et al. (2004) as well as \cite{Dai04}. On the other
hand,  there are differences, in particular concerning the existence of the
two outliers. They can be understood, however, since the fit includes
assumptions about the gas density in the GRB environment, which enters  the
calculation of the jet opening angle. We made use of the values provided by
\cite{Friedman2005} and these are higher by a factor of 10/3 compared to the
values used by Ghirlanda et al. (2004).  In addition, in several cases the
gamma-ray data given in \cite{Friedman2005} are notably different from those
used by Ghirlanda et al. (2004). Additionally, we also considered a wind-like
circumburst medium for some cases to calculate the jet half-opening angle,
while Ghirlanda et al. (2004) only regard an ISM-like circumburst medium.  It
is therefore not surprising that we do not exactly reproduce their results
(for a discussion, see also Friedman \& Bloom 2005). For instance, if we
reduce the assumed circumburster gas density  for bursts \#9 and \#12 from 10
to 1 cm$^{-3}$, then the corresponding data points do not fall out of the
sample anymore. A fit then provides $\eta = 0.78 \pm 0.09$.  While our data
base is too small in order to investigate the role of  outliers in the
Ghirlanda relation, we note that also the relation between the isotropic
equivalent energy release in the gamma-ray band and the intrinsic peak energy
\citep{Amati2002} is not very tight. In a recent study on BATSE GRBs,
\cite{Nak05} find that about 25\% of all bursts do substantially deviate from
this empirical relation \citep[see also][]{BP2005}.

In addition to the Ghirlanda relation, we have searched for linear
correlations between all individual afterglow parameters and between the burst
parameters in the gamma-ray band and the corresponding afterglow
parameters. Table~\ref{tabcor} lists the corresponding correlation
coefficients derived from weighted linear fits. The Ghirlanda relation
(here including the two outliers discussed above) is between $\log(E_{\rm
cor})$ and $\log(E_{\rm peak})$. Relatively tight correlations between
$\theta_{\rm jet}$ and $t_b/(1+z)$ and between $\theta_{\rm jet}$ and $\log
E_{\rm cor}$ are expected, as $\theta_{\rm jet}$ derives from $t_b/(1+z)$ and
$\log E_{\rm cor}$ derives from $\theta_{\rm jet}$. Note that the correlations
for the wind model are much tighter than for the ISM model, giving further
significance to the statistical conclusion that most circumburst environments
are wind-blown (\S~\ref{profile}). Next to the Ghirlanda relation and the
others just discussed, there are more correlations that seem significant
according to the absolute correlation coefficient, but visual inspection does
not support this conclusion. This holds also for the potential correlation
between  $\theta_{\rm jet}$ and $\alpha_1$ which has been reported for X-ray
data \citep{Liang2004}. Still, it is interesting to note that $\alpha_2$ seems
more or less correlated with all other parameters, including the redshift. On
the other hand, $\theta_{\rm jet}$, $\log E_{\rm cor}$ and $\log E_{\rm peak}$
are completely uncorrelated with the redshift. We conclude that no
evolutionary effect in the initial  explosion parameters is evident over a
wide range of redshifts.

Of special interest is the  parameter $n$,
which indicates the smoothness of the break (Equation~\ref{mag1}).  Even
though we could only determine $n$ for a few afterglows, it looks suspicious
that each time we had to fix $n$ to a relatively high value in order to get an
acceptable fit, the prebreak decay slope is $\alpha_1>1$. To test if this
could be due to a numerical problem we reconsidered the afterglow light curve
of GRB 030329 and fitted it only between 0.28 and 1 days, which includes the
time around the supposed jet break \citepeg{Uemura2003} but excludes the
cooling break \citep{Sato2003} and the rebrightening episodes
\citep[e.g.,][]{Lipkin2004}. For this time period the data density is high
enough in order to deduce a value for $n$ even if the break is very
sharp. Indeed, in this case we find  $\alpha_1=1.17\pm0.01, t_b=0.68\pm0.02$ days,
$\alpha_2=2.21\pm0.07$ and $n=7.54\pm1.47$. Adding this to our sample of afterglows
with a deduced parameter $n$ (Table~\ref{tabres}), a weak trend between $n$
and $\alpha_1$ becomes apparent (Fig.~\ref{a1n}). It indicates that a shallow
prebreak decline leads to  a smooth break or, seen the other way around, a
smooth break (a "rollover") implies a shallow prebreak decay slope. As we only
have very few values of $n$, we do not regard this as strong statistical
evidence for a correlation, since an  observational bias cannot be
excluded. Afterglows with a shallow decay are bright for a longer period of
time, which makes them easier to follow. Therefore, the data density around
the break  time is usually  higher compared to most afterglows with a steep
decline. A high data density around the break time is essential to determine
a value for $n$, however.  Nevertheless, it is worth to check if this trend is
confirmed in the \emph{Swift}-era.

Unfortunately, most bursts in our sample are at high redshift, so that no
supernova data are available. Consequently, no statistically founded
conclusions can be drawn on a potential correlation between afterglow
parameters and the corresponding supernova parameters (Paper I).

\subsection{Fine structure in the light curves \label{FineS}}

In principle, Equation (\ref{mag1}) represents a first order approximation of
an observed afterglow light curve. We consider any residuals that remain after
subtraction of the  fit from the observational data as the fine structure in
the light curve. Since the detection of fine structure in optical afterglows
depends  strongly on the sampling density of the light curve and the quality
of the data,  an observational bias cannot be excluded, which makes it
difficult to compare  the fine structure among the individual afterglows. On
the other hand, it is well-known that some afterglows show basically little or
no evidence for fine structure when sampled very densely with the same
telescope \citep[the best example being GRB 020813;][]{LaursenStanek2003},
while others show a  substantial amount of fine structure \citep[e.g., GRB
030329;][their figure 4]{Lipkin2004}. In order to investigate the occurrence
of fine structure in more detail, we have shifted all residuals to a common
evolutionary phase of an afterglow. We favor the idea that this can be done by
normalizing the time $t$ that has elapsed sind the GRB trigger to the break
time $t_b$ of the corresponding afterglow (Table~\ref{tabres}).  While
Figure~\ref{GS1} displays the individual light curves and corresponding
residuals that remain after subtraction of the fitted curves from the
observational data of the 16 afterglows in our sample, Figure~\ref{residuals}
displays all residuals in a single plot as a function of $t/t_b$.  We have
included here only those data with less or equal 0.05 mag individual
photometric error. The ratio $t/t_b$ is independent of redshift and allows us
to draw some general conclusions about the occurrence of fine structure in
afterglow light curves.

First at all, again  we find no evolutionary effect in the data. The  width of
the magnitude distribution of the fine structure of all 16 afterglows in the
prebreak evolutionary era spanning one decade in time ($0.1 \le t/t_b \le 1$),
is identical to the width of the  magnitude distribution in the postbreak era
spanning one decade in time ($1 \le t/t_b \le 10$), namely $\pm$ 0.1
magnitudes. The handful of data points around $t/t_b=0.2$ that reach beyond
$\pm$0.2 magnitudes mainly belong to GRB 011211 \citep[cf.][]{HollandAJ2002,
JakobssonNA2004} and is statistically not significant. This picture does not
change if we allow for larger individual photometric errors but then the
statistical significance of this finding becomes less strong. We conclude
that, on average, a patchy surface structure of afterglow shock fronts
\citep{Meszaros1998, Nakar2003} is not present in the photometry at times
later than $t/t_b>0.1$, with the probable exception of GRB 011211. In
addition, we find that the amplitude of the fine structure of all 16
afterglows as a group ($\pm$0.1 mag) is smaller by a factor of 4 compared to
the fine structure (or fluctuations) seen in the  optical afterglows of GRB
021004 \citep[e.g.,][]{deUga05} and GRB 030329 \citep{Lipkin2004}, which are
plotted in comparison\footnote{Note that our broken power law fits find late
breaks for both these afterglows (Table~\ref{tabres}), so most of the data is
at $t/t_b<1$.}. In other words, the latter two optical afterglows are indeed
very different from all other afterglows we have investigated, as the
deviations persist even after the break.

On the other hand, the residuals of the early afterglows of GRB 021004 and GRB
030329 are very similar. We find via $\chi^2$ minimization that a shift  of
the GRB 021004 light curve in $t/t_b$ by a factor of about  2.7 superposes the
early light curve evolution of both bursts (the $\chi^2$ minimum we find is
not sharp, shifts between 2.4 and 3.0 are acceptable). This is astounding, as
the bursts happened at two very different cosmological epochs. A deeper
analysis of this result will be pursued in a future publication (Kann et
al. 2005, in preparation).

\section{Summary}

Based on a systematic analysis of the optical and NIR data of \emph{all} GRB
afterglows with sufficient published data in the pre-\emph{Swift} era we have
explored the parameter space of the afterglow light curves and of physical
quantities related to them. From the 59 afterglows investigated
(Table~\ref{tabres}) we constructed a sample of 16 bursts with the
best-defined light curves useful for our purposes. Thereby we excluded the
afterglows of GRB 021004 and GRB 030329 because of their many re-brightening
episodes which made it difficult to fit them.

Using the sample of the 16 afterglows with the best defined light curves, we
find that in the optical bands, the average afterglow light curve is
characterized by a prebreak decay slope $\alpha_1 = 1.0\pm 0.1$ and a
postbreak decay slope  $\alpha_2 = 2.1\pm 0.1$. The distribution of both
parameters is rather broad but possible cutoffs are apparent in the available
data set. In particular, there is no evidence for a universality of $\alpha_2$
as it has been  predicted in some afterglow models. The distribution of the
break time in the host frame rises sharply towards smaller values, with the
most likely value at $t_b/(1+z)= 0.3\pm 0.2$ days.

We have then used the deduced light curve parameters to extract information
about the nature of the GRB environment using standard afterglow models
\citep{PK2001a}. We find that in most if not all cases the data are in
agreement with a wind model. A general preference of an ISM model is ruled
out. In addition, we find that the distribution of  the power-law index $p$ of
the electron distribution function  is rather broad ranging from about 1.5 to
3, supporting the view of a non-universality of $p$, in agreement with other
studies \citep[e.g.,][Paper III]{PK2001a, PK2001b, PK2002, Preece2002,
Yost2003, P2005b}.  Furthermore, we have searched in our data set for potential
correlations between the various light curve parameters and those that
characterize the corresponding burst in the gamma-ray band. With the exception
of the Ghirlanda relation between the beaming corrected energy release in the
gamma-ray band and peak energy in the GRB host frame (Ghirlanda et al. 2004),
no other tight correlation has been found. An intriguing correlation may exist
between the pre-break decay slope $\alpha_1$ and the smoothness parameter of
the break $n$, but more data is needed to verify this.

Finally we have analyzed in which manner the data indicate to a  general fine
structure that is superimposed a light curve decay according to the empirical
Beuermann double power-law. When normalized to the  corresponding break time
$t_b$ of a burst we find no evidence in the data that there is more structure
in the light curves  at times $0.1 < t/t_b < 1$ than at times $1 < t/t_b <
10$.  On the other hand, we find that the afterglows of GRB 021004 and
GRB 030329 are very different from all 16 afterglows in our sample. While the
latter vary  on average by only 0.1 magnitudes around the fitted light curve,
the former vary by 0.4 magnitudes. Moreover, the fine structure of
the light curves of GRB 021004 and GRB 030329 are initially very similar.

It is clear that more afterglows with well-sampled optical light curves are
needed in order to get better insight onto the parameter space of the physical
processes involved.  Even in the \emph{Swift} era this might not be an easy
task since most afterglows are simply very faint some days after the
burst. The observational challenge therefore remains the availability of
observing time on large optical telescopes in order to determine the light
curve parameters as well as possible.

\acknowledgments A.Z. and S.K. acknowledge financial support by DFG grant Kl
766/11-1. D.A.K. and S.K. acknowledge financial support by DFG grant Kl
766/13-2. We wish to thank S. Covino, J. Gorosabel, T. Kawabata,  B. C. Lee,
K. Lindsay, E. Maiorano, N. Masetti, R. Sato, P. M. Vreeswijk, and K. Wiersema
for contributing unpublished or otherwise unavailable data to the database,
and S. Cortes for reducing additional data. D.A.K. wishes to thank N. Masetti
and D. Malesani for enlightening discussions. We wish to thank S.  Barthelmy,
NASA, for the upkeep of the GCN Circulars and J. Greiner, Garching, for the
"GRB Big Table". We thank the anonymous referee for very constructive
remarks.

redpajama_set_name: RedPajamaArXiv


text:
Review: Zadie Smith's brilliance is on display in 'Feel Free'
(AFP/Getty Images)
By Walton Muyumba
Upon opening "Feel Free," Zadie Smith's new essay collection, you'll be surprised to learn that she doubts her literary talent, her critical acumen. I suppose that many literary writers are skeptical or anxious about their chosen profession. I know I am: though some invisible force compels us to create, we writers sometimes feel ourselves fraudulent intellectually, not knowing enough about anything to represent human experience or critique the arts successfully. Smith ought not be one of those writers though. Since 2000, Smith — London born and bred, now a New Yorker — has published six substantial, exceptional works of fiction (including the 2012 novel "NW," a tour de force formally and stylistically) and an excellent work of nonfiction, "Changing My Mind: Occasional Essays" (2009).
Across her eighth book's five parts — "In the World," "In the Audience," "In the Gallery," "On the Bookshelf," "Feel Free" — Smith has distributed a slew of essays, reviews (including a folio of "Harper's" columns) and lectures written from 2009-17. Over the course of 435 pages, she covers Brexit and the waning British state; climate change; David Fincher, Facebook and internet 2.0; Billie Holiday; Joni Mitchell; Key & Peele; Schopenhauer, Charlie Kaufman and stop-motion animation; black beauty, black sorrow, oil painting and a horror movie about white liberals; the vagaries of lower-middle-class British life in the 1980s and '90s; literary fiction and the discontinuous self; Justin Bieber, Jay-Z and joy.
Smith's continuous stream of productivity, her topical range, the accolades laureling her books, her prodigious artistic abilities, should be evidence enough to assuage her fears about credibility. And yet, as Smith explains in the new collection's foreword, her anxiety arises from believing she has "no real qualifications" to write as she does. "Not a philosopher or sociologist, not a real professor of literature or film, not a political scientist, professional music critic or trained journalist," Smith thinks that her essays rest shakily on evidence that is "almost always intimate. I feel this — do you? I'm struck by this thought — are you?" She worries that her writing has "not a leg to stand on" because it's born from "affective experience" and not argument. "All [the essays] have is their freedom. And the reader is likewise unusually free, because I have absolutely nothing over her, no authority."
Zadie Smith a reading her debut novel "White Teeth" at Skylight Books in 2000
(Ken Hively/Los Angeles Times )
Smith, of course, has authority: It often arises from her sentence-level precision, the refined elucidation of her insights, the exuberance and humor that sustains readers' attention. It's there when she parses Hanif Kureishi's "The Buddha of Suburbia" and J.G. Ballard's "Crash"; it's there in the hyper-intelligent micro reviews from "Harper's." Taking up Edward St. Aubyn's novel, "At Last" (2012), for example, Smith describes how the author draws from "the wit of Wilde, the lightness of Wodehouse and the waspishness of Waugh" as he fashions his meticulous personal style:
"Oh, the semicolons, the discipline! Those commas so perfectly placed, so rhythmic, creating sentences loaded and blessed, almost o'erbrimmed, and yet sturdy, never in danger of collapse. It's like fingering a beautiful swatch of brocade. This refusal to submit to the puritan brevity of the American sentences (or, worse, the artificial naivety of an English sentence intended to sound as if it has been translated from the French) — it's almost enough to make you feel patriotic.
These sentences aren't merely decorative. They're important because they enable the comedy: when you create this many compartments in each line, you have space for at least two jokes and one sly dig."
Effectively a pastiche of St Aubyn's style, Smith's close reading illustrates and explicates simultaneously. She's also performing what I'll call her "affective" critical practice. Smith seems to define that mode while appraising the intellectual prowess on display in Geoff Dyer's "Otherwise Known as the Human Condition: Selected Essays and Reviews." When she writes that each of Dyer's essays "is an attempt to respond in kind, to be equal to the artwork, in some way to meld with it, like a love object," Smith could be describing her own approach. Pastiche melds the critic to the love object and creates intimate, meaning-driven analysis.
When writing about singers and rappers, Smith's pieces seem shaped by the sonic motions of musical voices. In "Some Notes on Attunement," Smith responds pastiche as in kind to Joni Mitchell and her 1971 album, "Blue." Like a literary approximation of Mitchell's wandering notes, Smith wanders through Wordsworth, Kierkegaard, Abraham and Isaac, connoisseurship, novel reading (and writing) and the Talking Heads to get to Mitchell.
Considering Mitchell's own artistic and personal transformations, Smith points out that "these days, Mitchell thinks of herself more as a painter than a singer. She is so allergic to the expectations of her audience that she would rather be a perfectly nice painter than a singer touched by the sublime." Mitchell's life demonstrates the "inconsistency of identity, of personality."
Attuning to Mitchell, Smith realizes that while she herself is both "the girl who hated Joni and the woman who loves her," they're divorced from each other. Recognizing her own discontinuities allows Smith to notice "the transformation of [her] listening," shifting away from hating Mitchell to a space where "Blue" triggers "uncontrollable tears. An emotional overcoming, disconcertingly distant from happiness, more like joy — if joy is the recognition of an almost intolerable beauty. It's not a very civilized emotion." In transformation, in the gap between separated selves, Smith finds freedom, the portal to joy.
Zadie Smith's essay collection "Feel Free"
(Penguin Press )
But there is dis-ease in this transition too. Our separation from our various selves, Smith writes, is an everyday sensation, "yet it proves a tricky sort of problem for those people who hope to make art. For though we know and recognize discontinuity in our own lives, when it comes to art we are deeply committed to the idea of continuity. I find myself to be radically discontinuous with myself — but how does one re-create this principle in fiction?" This professional literary problem is enmeshed with Smith's apprehension about her intellectual authority.
In "Some Notes," when Smith worries that she cannot develop a connoisseur's command of, say, Mitchell's or David Byrne's music, or some other subject, her anxiety stems from a belief that she doesn't have the time it takes to generate command. Like many of us just entering the long middle section of our lives, Smith's time is taken up by work (writing and teaching writing), parenting two young children, and partnering an equally ambitious and prolific writer, her husband, Nick Laird. Life, in other words, strips time away from taking in or occludes altogether the newness and sublimity that strong artwork can provide.
One way to read "'Crazy They Call Me': On Looking at Jerry Dantzic's Photos of Billie Holiday" is as an attempt to solve this riddle. Fashioning her introduction to the photos in "Jerry Dantzic: Billie Holiday at Sugar Hill" as a fictional memoir in Holiday's voice, Smith makes the singer the beloved and tries equaling the wonder of her persona in Dantzic's images. Smith merges her style partly with an imagined Holiday and partly with the sound of the singer's memoir, "Lady Sings the Blues" (isn't Holiday's collaboration with her amanuensis, William Duffy, a form of melding?).
((AP Photo/FILE )
The voice Smith hears emanating from the pictures glides across various points of view to tell her story. Though she was born Eleanora Fagan and performed as Billie Holiday, the witty figure who emerges is angular and shifting: "though many aren't hip to this yet — not only is there no more Eleanora, there isn't any Billie either. There is only Lady Day." It's ventriloquism as loving, musical homage.
Like singers, writers create secondary or tertiary selves, using "them to slip from every bind and definition, but … can also prove callous with the lives of others and in their dash for freedom knock their loved ones out of the way." As Smith argues late in "The Bathroom," a funny, gorgeous, mournful essay about what their arrival in the British lower middle class cost her parents, family life "is always an event of some violence." How then does the writer balance desired freedoms, minimize family as an event of violence, and access joy? Smith has built a career as a novelist dancing among these poles, dancing between (as the title of one her essay names it) optimism and despair.
Smith's most recent novel, "Swing Time" (2016) is an attempt to wrestle with her doubts about fiction's capabilities. To great effect, Smith achieves a formally unified literary novel while simultaneously illustrating a unnamed narrator recognizing her discontinuous selves. It's a novel about dance that ends with a major character, Tracy, herself a lapsed professional dancer, joyously whirling dervish-like with her children. While Smith may not be able to assuage her doubts about her authority, she can "dance" with and around them. In fact, those dancing with doubt seems central to her "affective" critical process.
(Getty Images )
There's so much at play in "Feel Free" that a reader might feel anxious about how to gain purchase on all of Smith's ideas. "Getting In and Out," "Mark Bradford's 'Niagara,'" "A Bird in a Few Words: Narrative Mysteries in the Paintings of Lynette Yaidom-Boakye," present Smith's most forceful writing yet about film, visual art and blackness. "The Bathroom," "Love in the Gardens," "The Shadow of Ideas" and "Joy" demonstrate Smith's mastery of creative nonfiction and the essay form. However, as she points out in "The Tattered Ruins of the Map," when confronted with the "rapidly revolving ideas," the constellated materials, objects and digital images that make up Sarah Sze's "Centrifuge," "it is hard to know which element to separate from the rest. Yet if you are to write about something you must choose."
Here, I've chosen the bits of this tremendous, enthralling book that might explain how Smith, in spite of her doubts about it, demonstrates authority. My hunch about this book is this: While paying attention to Smith's doubts might get you into these essays, getting out may require some improvised dance moves.
That means, I think, rejecting linear movement through the work. This may not seem a proper way to address this work, but, as Smith writes in "Dance Lessons for Writers," "between propriety and joy choose joy." In any case, she's suggesting that we follow her lead. Early in "Feel Free" Smith describes her writing as the intersection of language, the world, the self: "The first is never wholly mine; the second I can only ever know in a partial sense; the third is a malleable and improvised response to the previous two." It's this improvised Smith whom we're dancing with throughout these pages.
Muyumba, associate professor of English at Indiana University-Bloomington, is the author of "The Shadow and the Act: Black Intellectual Practice, Jazz Improvisation, and Philosophical Pragmatism."
"Feel Free: Essays"
Penguin Press: 464 pp, $28
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redpajama_set_name: RedPajamaCommonCrawl


Molly Malone's is an Irish pub located in the Chartron district of Bordeaux. Committed to a convivial way of life we don't forget our Irish roots.
The pub spirit continues with events that bring us in close proximity to our customers. Rugby, football and live music are an habituel part of enjoying time spent at Mollys.


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text:
A Fully-Dramatized Audio Production From Folger Theatre
Part of Folger Shakespeare Library Presents
Read by Full Cast Dramatization
Unabridged Audio Download
Unabridged Compact Disk
PRICE MAY VARY BY RETAILER
The Folger Shakespeare Library, home to the world's largest Shakespeare collection, brings Julius Caesar to life with this new full-length, full-cast dramatic recording of its definitive Folger Edition.
Shakespeare may have written Julius Caesar as the first of his plays to be performed at the Globe, in 1599. For it, he turned to a key event in Roman history: Caesar's death at the hands of friends and fellow politicians. Renaissance writers disagreed over the assassination, seeing Brutus, a leading conspirator, as either hero or villain. Shakespeare's play keeps this debate alive.
This new unabridged audio recording of the well-respected edition of Shakespeare's classic—expertly produced by the Folger Theatre—is perfect for students, teachers, and the everyday listener.
William Shakespeare was born in April 1564 in the town of Stratford-upon-Avon, on England's Avon River. When he was eighteen, he married Anne Hathaway. The couple had three children—an older daughter Susanna and twins, Judith and Hamnet. Hamnet, Shakespeare's only son, died in childhood. The bulk of Shakespeare's working life was spent in the theater world of London, where he established himself professionally by the early 1590s. He enjoyed success not only as a playwright and poet, but also as an actor and shareholder in an acting company. Although some think that sometime between 1610 and 1613 Shakespeare retired from the theater and returned home to Stratford, where he died in 1616, others believe that he may have continued to work in London until close to his death.
About The Reader
Full Cast Dramatization
The Folger Shakespeare Library is a world-renowned research center on Shakespeare and on the early modern age in the West. Its conservation lab is a leading innovator in the preservation of rare materials. Its well-known public programs include plays, concerts, literary readings, family activities, and exhibitions, as well as numerous programs for students and teachers. The Folger also publishes the illustrated, completely re-edited Folger Editions of Shakespeare's plays, award-winning exhibition catalogs, and the journal Shakespeare Quarterly. The Folger opened in 1932 as a gift to the American nation from Henry Clay Folger and his wife Emily Jordan Folger. It is administered by a Board of Governors under the auspices of Amherst College, Henry Folger's alma mater.
Publisher: Simon & Schuster Audio (February 24, 2015)
Runtime: 2 hours and 20 minutes
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text:
El centén fue una moneda española de 100 escudos de oro emitida en 1609 bajo el reinado de Felipe III, también fue acuñada bajo los reinados de Felipe IV y Carlos II, tiene un peso de 359 gramos de oro. Durante el reinado de Isabel II se llamó centén a la moneda de 100 reales.

Centenes segovianos

Los centenes segovianos fueron una serie de monedas de oro españolas que equivalían a cien escudos. Se hicieron dos series, una en 1609 y otra en 1633, ambas con solo siete piezas cada una. Están consideradas las monedas de oro más grandes de la historia y actualmente un ejemplar de 1609 es considerado la moneda más cara del mundo. Una de estas monedas pertenece al Museo Arqueológico Nacional de España en Madrid, con el inventario número 108085.

Se cree que debido al exagerado valor de la moneda en su época, solamente se utilizaba como símbolo de reconocimiento u ostentación pública y para engrandecer o premiar a algunos personajes de la nobleza castellana en tiempos de Felipe III.

Centén segoviano de 1609

Características
 Origen: España, acuñada en 1609, en los talleres del Real Ingenio de Segovia, edificio construido sobre un antiguo molino situado sobre el río Eresma, que en 1586 comenzó la acuñación de moneda.
 Valor: 100 escudos.
 Técnica: Acuñación.
 Material: oro.
 Diámetro: 7,15 centímetros.
 Peso: 339,35 gramos.

Conservación
Se conserva actualmente una pieza. Pertenece a la colección de monedas de oro españolas llamada «Caballero de las Yndias», que se compone de 2200 monedas que se acuñaron en España y sus antiguas colonias y que fueron adquiridas por un numismático vasco (que vivió en Cuba) a lo largo de su vida.

El 22 de octubre de 2009, fue adquirida en una subasta promovida por la firma Áureo&Calicó, llevada a cabo en el Hotel Arts de Barcelona, (España), por un comprador suizo por un precio final de 800.000 euros.

Centén segoviano de 1633

Características
 Origen: España, acuñada en 1633, en los talleres del Real Ingenio de Segovia, edificio construido sobre un antiguo molino situado sobre el río Eresma, que en 1586 comenzó la acuñación de moneda.
 Valor: 100 escudos.
 Técnica: Acuñación.
 Material: oro.
 Diámetro: 7,15 centímetros.
 Peso: 339,35 gramos.

Exposiciones
La moneda ha participado en varias exposiciones desde que pertenece a las colecciones del Museo Arqueológico Nacional de España:
 De Gabinete a Museo. Tres Siglos de Historia; Madrid (m): Museo Arqueológico Nacional, 1993, [Suermondt-Ludwig Museum]
 Tesoros del Gabinete Numismático. Las 100 mejores piezas del monetario del Museo Arqueológico Nacional; Madrid (m): Museo Arqueológico Nacional, 1999, [Suermondt-Ludwig Museum]
 El oro y la plata de las Indias en la época de los Austrias; Madrid (m) (Área Metropolitana de Madrid (comarca), Madrid (provincia): 1999, [Se prestó la reproducción.]

Véase también
 Numismática

Referencias

Enlaces externos
 Página Web de la Fábrica nacional de Moneda y Timbre española.

Monedas de España
Monedas de oro
Monedas fuera de curso
Real Ingenio de Segovia

redpajama_set_name: RedPajamaWikipedia


The last time we weight pulled we attended the K9 Fanciers/AABC UKC pull. As I blogged about prior, UKC altered their rules to limit how much a dog can actually pull. For a dog like Ryker, who pulled this past weekend, which is an incredibly hard thing to do. Limiting a dog that has been conditioned and trained to continue to pull well above the 20pt rule – which is only 35x his body weight on the surface we pulled (wheels). Ryker has pulled well above the 20pt pull with UKC on wheels and has taken many Most Weight Pulled (MWP) and Most Weight Pulled Percentage (MWPP) placements in the regular and Grand classes (when they were offered – they have since been discontinued).
We have not pulled competitively since the weight pull rule change, that is, until last weekend. We had a chance to get out and pull with the NWDA (National Working Dog Association) for the first time. Their rules are very similar to the APA (American Pulling Alliance) in that there is one foul and then the dog is done (versus the UKC where you have two fouls), but you are only able to pass two weight increases before you must pull again (APA is unlimited passes). It really was, in my honest opinion, the best of both the UKC and the APA pulling rules.
The same camaraderie that used to be present at the UKC pulls was there in spades. It was nice to see some familiar faces, but even more to see a lot of the newer weight pullers who had been training at Currey's Family Pet Care and were incredibly new to the competition aspect. Those of us who are 'old hats' at this have a lot to look forward to with our new 'competition' this coming season and I, for one, can't wait to attend another NWDA pull. Thank you, NWDA for giving me and other weight pullers another place to work our dogs!
This entry was posted in Dog Sports, Weight Pull and tagged apa, dog sports, nwda, ryker, ukc, weight pull on January 25, 2012 by ShadowWolf.


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You can get creative with the design and have fun with it yourself. Designing advertising t shirts does not necessarily need to be done by your innovative people. Any printing business can deal with you to produce a distinct style. Constantly remember though to make the shirt representative of who you are as a brand. You are most passionate about your business. So make certain you are clear on the message you wish to go out on your custom t shirt printing.
Establishing promotional t shirts can lead to your producing a revenue on the products, or just getting the word out to the public. boxingdirectory In any case, when completion user has the garment in their hands, they cannot forget you. Whenever they see or place on the shirt, they are advised of you, and isn't that exactly what advertising and promo is everything about? This develops a long-term impression on your customized t shirt printing, so make sure it's a good one!
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