text:
\section{Introduction}

Gamma-ray bursts \citep[GRBs,][]{1973ApJ...182L..85K} are the most violent explosions in the Universe. They are characterized by a short flash of gamma-ray photons followed by a long lasting afterglow that can be observed at all wavelengths. They can be classified into two types based on the duration (and the hardness) of their $\gamma$-emission: short and long GRBs \citep[\hbox{$T_{90}$}\ $<$ 2 s (hard spectrum) and \hbox{$T_{90}$}\ $>$ 2 s (soft spectrum) respectively;][]{1993ApJ...413L.101K}. Currently, the most favored model to explain the origin of GRBs is a highly magnetized relativistic jet, but more prompt polarimetric observations are needed in order to confirm this \citep{2013Natur.504..119M,2015ApJ...813....1K}. The prompt emission likely originates from either internal shocks in the photosphere of the jet or magnetic dissipation in a magnetically dominated jet \citep[see][and references therein]{2011ApJ...726...90Z,2012ApJ...751...90Z}. The afterglow emission, however, is thought to originate from external shocks caused by the jet's interaction with the interstellar medium (ISM). Multiwavelength emission is expected to be produced by a forward shock moving into the ISM and a reverse shock moving into the expanding jet \citep{1993ApJ...405..278M, 1998ApJ...497L..17S,1999ApJ...519L..17S}. The reverse shock is supposed to be short lived, with most of the afterglow emission being generated by the forward shock.

The electrons accelerated at the shock fronts emit synchrotron radiation as they interact with the magnetic field behind the shock fronts. By modeling this emission we can determine the  physical parameters of the GRB ejecta and the structure of the ISM near the progenitor along the line of sight to Earth. The most popular way to extract the parameters is by using an analytical model for the expected shape of the afterglow light curves and spectrum \citep{1997ApJ...487L...1R,1998ApJ...497L..17S,1999ApJ...523..177W}. The emission is split into regions in time and wavelength, where the resulting light curve and spectrum can be approximated by power laws. The slopes of these segments along with the location of the spectral breaks are then used to determine the physical parameters. An alternative method is to model the emission using a numerical code that takes as input the physical parameters of interest \citep{2002ApJ...571..779P,  2006ApJ...647.1238J}. In  addition to requiring fewer approximations, the numerical models allow us to study a more complex structure for the ISM and the GRB ejecta and is therefore our method of choice for this study.

To properly determine the physical properties of the GRB ejecta a wide range of accurate multi-wavelength observations are needed with as good time coverage as possible. The millimetre/sub-millimetre range is of crucial importance in constraining the afterglow models as it is where the flux density of the emission peaks during the first few days after the GRB onset. In  this range the capabilities of the new ALMA observatory bring an important leap forward, thanks to its great improvement in resolution and sensitivity in comparison with previous observatories \citep{2012A&A...538A..44D}.

It is widely accepted that long GRBs are created by the explosive death of massive stars \citep{2003Natur.423..847H, 2006ARA&A..44..507W}, probably rapidly rotating Wolf-Rayets \citep[for a review see, e.g.,][]{2007ARA&A..45..177C}. However, it remains unclear what the specific mechanism in the core collapse process is that triggers the formation of a jet.  Given the short life periods of such massive stars and their luminosity, GRB afterglows can be used as powerful tracers of star-forming galaxies over a wide range of redshifts \citep[e.g.,][]{2009ApJ...705L.104K, 2012ApJ...744...95R, 2015A&A...581A.125K, 2015ApJ...808...73S, 2015A&A...581A.102V}. To date spectroscopically confirmed GRB redshifts range from $z$ = 0.0085 \citep[GRB\,980425A][]{1998IAUC.6896....3W,1998Natur.395..670G} to $z$ = 8.2 \citep[GRB\,090423A][]{2009Natur.461.1254T, 2009Natur.461.1258S}, and photometric redshifts have been proposed up to $z$ = 9.4 \citep[GRB\,090429B][]{2011ApJ...736....7C}.

Optical/NIR spectroscopy of GRB afterglows can also be used to study the intervening matter present along the line of sight at different distance scales, ranging from regions around the progenitor to distant intervening galaxies. Its strength resides in the extremely bright afterglow, making it possible to measure atomic/molecular transitions in the host galaxy and intervening systems \citep[e.g.][]{2014A&A...564A..38D}, even when the probed galaxies are not detected by deep direct imaging. It made possible to accurately probe absorption metalliticity out to $z$ $\geq$ 5 \citep[e.g.,][]{2014ApJ...785..150S, 2015A&A...580A.139H}.

In this paper we present observations of the afterglow and host galaxy of GRB\,110715A, aiming at understanding the physical processes involved in the explosion and the environment in which it occurred. Our data includes radio, submillimeter, near-infrared, optical, ultraviolet, and X-ray observations. In Section 2 we introduce the observations available for this event, in Section 3 we explain the results of these observations and discuss the implications, and in Section 4 we present our conclusions.

\section{Observations}

\begin{figure*}
\includegraphics[width=\textwidth]{figures/lc}
\caption{Afterglow light curve (Galactic extinction corrected) of the 17 bands observed. Upper limits are denoted by down-pointing triangles.}
\label{fig:obs}
\end{figure*}

\begin{table}
\caption{Broad band multiwavelength observations of GRB\,110715A. The full table is available in the online version.}
\centering
\begin{tabular}{cccc}
\hline\hline
$T$ - $T_{0}$ & Flux & AB & Band \\
days & Jy & mag & \\
\hline
0.00094 & (1.32 $\pm$ 0.33) $\times$ 10$^{-04}$ & 18.60$^{+0.24}_{-0.31}$ & XRT 2 keV \\
0.00096 & (1.52 $\pm$ 0.37) $\times$ 10$^{-04}$ & 18.44$^{+0.24}_{-0.31}$ & XRT 2 keV \\
0.00098 & (1.12 $\pm$ 0.27) $\times$ 10$^{-04}$ & 18.78$^{+0.24}_{-0.31}$ & XRT 2 keV \\
0.00100 & (1.01 $\pm$ 0.25) $\times$ 10$^{-04}$ & 18.89$^{+0.24}_{-0.31}$ & XRT 2 keV \\
0.00103 & (1.13 $\pm$ 0.26) $\times$ 10$^{-04}$ & 18.77$^{+0.23}_{-0.29}$ & XRT 2 keV \\
0.00114 & (1.19 $\pm$ 0.17) $\times$ 10$^{-04}$ & 18.71$^{+0.15}_{-0.17}$ & XRT 2 keV \\
0.00116 & (0.86 $\pm$ 0.13) $\times$ 10$^{-04}$ & 19.06$^{+0.16}_{-0.18}$ & XRT 2 keV \\
0.00119 & (1.16 $\pm$ 0.17) $\times$ 10$^{-04}$ & 18.74$^{+0.15}_{-0.18}$ & XRT 2 keV \\
... & ... & ... & ... \\
\hline
\end{tabular}
\label{tab:obs}
\end{table}

\subsection{Gamma-ray emission}

The \textit{Swift} \citep{2004ApJ...611.1005G} Burst Alert Telescope \citep[BAT,][]{2005SSRv..120..143B} triggered and located GRB\,110715A on 15 July 2011 at \hbox{$T_{0}$} = 13:13:50 UT \citep{2011GCN..12158...1S}. The gamma-ray light curve shows a double-peaked structure with a duration of \hbox{$T_{90}$} = 13.0 $\pm$ 4.0 s (90\% confidence level) in the observer frame. Therefore we classify GRB\,110715A as a long burst.

Analysis of the time-integrated spectrum from \textit{Konus-Wind} gave the best fit as a Band function with the following parameters: $\alpha_1$ = -1.23$^{+0.09}_{-0.08}$, $\alpha_2$ = -2.7$^{+0.2}_{-0.5}$, $E_p$ = 120$^{+12}_{-11}$ \citep{2011GCN..12166...1G}. GRB\,110715A was also detected by \textit{INTEGRAL}/SPI-ACS,  and \textit{Suzaku}/WAM  \citep[see more details in][]{2011GCN..12166...1G,2011GCN..12158...1S}.

\subsection{X-ray afterglow observations}

The X-Ray Telescope \citep[XRT;][]{2005SSRv..120..165B} onboard {\it Swift} began observing the field 90.9 seconds after the BAT trigger, localizing the X-ray afterglow at RA(J2000) = 15$h$ 50$m$ 44.00$s$, Dec.(J2000) = -46$^{\circ}$  14$\arcmin$ 07\farcs5 with an uncertainty of 1\farcs4 \citep[90\% confidence level;][]{2011GCN..12161...1E}.

The unabsorbed X-ray afterglow light curve used in this paper has been extracted from the Burst Analyzer \footnote{\url{http://www.swift.ac.uk/burst_analyser}} \citep{2007A&A...469..379E,2009MNRAS.397.1177E,2010A&A...519A.102E}, which uses the spectral slope to derive the flux densities at an energy of 2 keV and assumes a Hydrogen column density N(H) = 1.6$^{+0.5}_{-0.4}$ $\times$ 10$^{22}$ cm$^{-2}$. These observations are shown in Figure \ref{fig:obs} and tabulated in Table \ref{tab:obs}.

\subsection{UV/Optical/NIR afterglow observations}

\begin{table}
\caption{Effective wavelengths and extinction coefficients.}
\begin{tabular}{lcc}
\hline\hline
Band & $\lambda_{\rm eff}$ [$\mu$m] & A$_{\lambda}$ $^{(a)}$ \\
\hline
UVOT uvw2 & 0.193 & 4.099 \\
UVOT uvm2 & 0.225 & 4.582 \\
UVOT uvw1 & 0.260 & 3.623 \\
UVOT u & 0.351 & 2.587 \\
UVOT b & 0.441 & 2.021 \\
GROND g' & 0.459 & 2.018 \\
UVOT \textit{white} & 0.483 & 2.566 \\
UVOT v & 0.545 & 1.628 \\
GROND r' & 0.622 & 1.393 \\
GROND i' & 0.764 & 1.042 \\
FORS2 Ic & 0.786 & 0.949 \\
GROND z' & 0.899 & 0.775 \\
GROND J & 1.239 & 0.455 \\
GROND H & 1.646 & 0.291 \\
GROND K & 2.170 & 0.187 \\
\hline
\end{tabular}
\\[0.2cm]
\begin{scriptsize}
(a) $E(B-V)$~=~0.52 mag \citep{2011ApJ...737..103S}
\end{scriptsize}
\label{tab:extinction}
\end{table}

GRB\,110715A was followed up in UV/Optical/NIR wavelengths with \textit{Swift} (+UVOT) and the 2.2m MPG telescope (+GROND). Light curves are shown in Figure \ref{fig:obs} and tabulated in Table \ref{tab:obs} as well.

This burst had a very bright optical counterpart in spite of the high Galactic extinction caused by its location close to the Galactic plane \citep{2011GCN..12161...1E}. The GRB afterglow study was affected by the Galactic reddening, initially estimated to be $E(B-V)$ = 0.59 mag according to the dust maps of \citet{1998ApJ...500..525S}, and later $E(B-V)$ = 0.52 mag following \citet{2011ApJ...737..103S}. We adopted the latest value. Computed effective wavelengths and extinction for each band are presented in Table \ref{tab:extinction}.

\subsubsection{UVOT imaging}

The \textit{Swift} Ultra-Violet/Optical Telescope \citep[UVOT;][]{2005SSRv..120...95R} began settled observations of the field of GRB\,110715A 100$s$ after the trigger \citep{2011AIPC.1358..373B}. The afterglow was detected in the $white$, $u$, $b$ and $v$ filters at RA(J2000) = 15h 50m 44.09s, Dec.(J2000) = -46$^{\circ}$  14$\arcmin$ 06\farcs5, with a $2\sigma$ uncertainty of about 0\farcs62. For this analysis, we have reduced both image and event mode data grouped with binning $\Delta t / t \sim 0.2$. Before the count rates were extracted from the event lists, the astrometry was refined following the  methodology in \citet{2009MNRAS.395..490O}. The photometry was then extracted from the event lists and image files based on the FTOOLs \textit{uvotevtlc} and \textit{uvotmaghist}, respectively, using a source aperture centered on the optical position and a background region located in a source-free zone. We used a 3" source aperture to avoid contamination from neighbouring stars and  applied aperture corrections to the photometry in order to be compatible with the UVOT calibration \citep{2011AIPC.1358..373B}. The analysis pipeline used software HEADAS 6.10 and UVOT calibration 20111031.

\subsubsection{GROND imaging}

We obtained follow-up observations of the optical/NIR afterglow of GRB\,110715A with the seven-channel imager GROND \citep[Gamma-ray burst optical/near-infrared detector;][]{2008PASP..120..405G} mounted on the 2.2m MPG@ESO telescope stationed in La Silla, Chile. The first observations were obtained 2.5 days after the trigger, after losing the first two nights due to weather. This first epoch suffers from very bad  seeing, 1\farcs5 -- 1\farcs9 depending on the band, but the optical/NIR afterglow was clearly detected \citep{2011GCN..12169...1U}.  Deeper follow-up  under  better conditions  in
three further  epochs reveals a faint nearby source which exhibits a stellar PSF. The presence of this source was carefully accounted for during the data analysis. The GROND optical and NIR image reduction and photometry were performed by calling on standard IRAF tasks \citep{1993ASPC...52..173T} using the custom GROND pipeline \citep{2008AIPC.1000..227Y}, similar to the procedure described in \cite{2008ApJ...685..376K}. Hereby, we used SExtractor \citep{1996A&AS..117..393B} for background modeling, and bright sources were masked out, which yields improved results in the case of this crowded field. A late epoch was obtained 38 days after the GRB which was supposed to be used for image subtraction purposes, but a positioning
error led to the afterglow position being covered only in the NIR frames.

Afterglow magnitudes in the optical were measured against comparison stars calibrated to the SDSS catalogue \citep{2011ApJS..193...29A}, obtained from observing an SDSS field at
similar airmass immediately after the fourth epoch, in photometric conditions. NIR magnitudes were measured against on-chip comparison stars taken from the 2MASS catalogue \citep{2006AJ....131.1163S}. The results of the photometry are displayed in Table \ref{tab:obs}.

\subsection{Submm afterglow observations}

\begin{figure}
\centering
\includegraphics[width=\columnwidth]{figures/alma}
\caption{ALMA image at 345 GHz. The beam size (0\farcs3 $\times$ 0\farcs1, P.A.=76 degrees) is showed in the lower left corner.}
\label{fig:alma}
\end{figure}

The Atacama pathfinder experiment telescope (APEX) observations began on July 16, 1.42 days after the burst and were performed in the 345 GHz band using the photometric mode of the Large Apex BOlometer CAmera \citep[LABOCA;][]{2009A&A...497..945S} under good weather conditions. Data reduction was done using the BoA (1), CRUSH and miniCRUSH \citep{2008SPIE.7020E..1SK} software packages. Using these observations we discovered a bright submm counterpart at 10.4 $\pm$ 2.4 mJy \citep{2011GCN..12168...1D}.

As a test of the target of opportunity programme, GRB\,110715A was also observed with the Atacama Large Millimeter Array (ALMA), yielding a detection with a flux density of 4.9 $\pm$  0.6 mJy at 345~GHz \citep{2012A&A...538A..44D}. The ALMA observations began on July 19 at 02:50 UT (3.57 days after the burst), and they were carried out making use of only 7 antennas during 25 mins on source. We present the data in Figure \ref{fig:alma}.

In spite of being obtained during a test observation, with almost an order of magnitude fewer antennas than are available with the full observatory, this was the deepest observation carried out to date at 345~GHz of a GRB afterglow \citep{2012A&A...538A..44D}. The ALMA observation also provides the most accurate coordinates available for this GRB. The centroid of the afterglow is located at RA(J2000) = 15$h$  50$m$  44.05$s$ and Dec.(J2000) = -46$^{\circ}$  14$\arcmin$ 06\farcs5 with a synthesized beam size of 0\farcs3 $\times$ 0\farcs1 at a position angle of 76 degrees, which provides an astrometric accuracy $\lesssim$ 0\farcs02. The differences between the optical and radio reference frames only limit this precision to be $\lesssim$ 0\farcs05 \citep[e.g.,][]{1986HiA.....7..103J}.

\subsection{Radio afterglow observations}

Following the detection of an afterglow at submm wavelengths with APEX \citep{2011GCN..12168...1D}, radio observations were obtained with the Australia Telescope Compact Array \citep[][ATCA]{2011MNRAS.416..832W} two and three days after the trigger. These observations resulted in further detections of the afterglow at $44$\,GHz \citep{2011GCN..12171...1H}. This GRB was monitored at 44, 18, 9, and 5 GHz for up to 75 days post-burst, where the flux remained at a sub-mJy level. The lower frequency observations were complicated by the presence of a second source within the field of view (MGPS\,J155058-461105). The data were reduced using standard procedures in MIRIAD \citep{1995ASPC...77..433S}. An additional late-time visit was performed on 12 Aug 2013 at 5.5\,GHz and 9\,GHz, to understand the possible contribution of the host galaxy, which was found to be negligible at both bands. The flux evolution of the afterglow at the four ATCA frequencies is also shown in Figure \ref{fig:obs} and tabulated in Table \ref{tab:obs}, together with the rest of the observing bands.

\subsection{Optical/nIR afterglow spectra}

\begin{table}
\caption{X-shooter observations log.}
\begin{tabular}{lllll}
\hline\hline
Mean T-\hbox{$T_{0}$} & Arm & Exp. time  & Slit width & Resolution $(a)$ \\
(hr)		&	&	(s)	&	(\arcsec)	& \\
\hline
12.60 & UVB & 618.02 & 1.0 & 4350 \\
12.60 & VIS & 612.04 & 0.9 & 7450 \\
12.60 & NIR & 600.00 & 0.9 $(b)$ & 5300 \\
\hline
\end{tabular}
\\[0.2cm]
\begin{scriptsize}
(a) Nominal values.
(b) K-band blocker was not used.
\end{scriptsize}
\label{tab:xshlog}
\end{table}

\begin{figure*}
\centering
\includegraphics[width=0.85\textwidth]{figures/XSspec}
\caption{X-shooter spectra. Upper panels are the finding chart (left) and an overview of the complete flux calibrated spectra, corrected for Galactic extinction (right). In the bottom plot, we show the normalised spectra, with 3 panels per arm, starting at top with UVB and followed by VIS and NIR. Each panel includes the 2D image and 1D signal and error spectrum. Telluric absorptions are indicated by black bands above the 1D spectrum, their thickness is a measure of the absorption strength.}
\label{fig:spec}
\end{figure*}

VLT/X-shooter \citep{2011A&A...536A.105V}, an optical/nIR intermediate resolution spectrograph mounted at the Very Large Telescope (VLT) Unit Telescope (UT) 2 in Paranal Observatory (Chile), was used to observe the GRB afterglow starting 12.7 hrs after the \textit{Swift} trigger. The seeing was 0\farcs9, but observations had to be interrupted due to wind constraints \citep{2011GCN..12164...1P}. The observing log is shown in Table \ref{tab:xshlog}. We processed the spectra using version 2.0.0 of the X-shooter data reduction pipeline \citep{2006SPIE.6269E..2KG, 2010SPIE.7737E..28M}. As the observations were stopped after one exposure, the standard nodding reduction could not be performed. We thus reduced the single frames of each arm with the following steps: We performed bias subtraction, cosmic ray detection and subtraction \citep{2001PASP..113.1420V}, and flat field division on the raw frames. From these processed frames the sky emission was subtracted using the \citet{2003PASP..115..688K} method and 1D spectra were extracted directly order by order from the sky-subtracted and flat-field divided frame using optimal extraction \citep{1986PASP...98..609H}. The resulting spectra were merged weighting them by the errors and the final merged spectra were then averaged in IDL. The spectra were flux calibrated using observations of the standard star LTT7987 taken the same night. The complete X-shooter spectrum is shown in Fig.~\ref{fig:spec}.

\subsection{Host galaxy imaging}

606 days after the burst, the field of GRB\,110715A was revisited using GROND searching for a possible host galaxy contribution. However, the data did not reveal any underlying source. We therefore derive only detection limits.

A deeper exposure was obtained on August 2013 with FORS2 at ESO's VLT 751 days after the burst. The observation consisted of $10\times240$ s in $I_C$-band, with a seeing of 0\farcs55, and data were reduced in a similar fashion as the GROND imaging. An object is detected close to the afterglow position at a magnitude of 26.40 $\pm$ 0.36 mag.

\begin{figure}
\centering
\includegraphics[width=\columnwidth]{figures/110715A_host.eps}
\caption{Observation of the host galaxy in the $I_C$-band from VLT/FORS2.}
\label{fig:host}
\end{figure}

\section{Results and discussion}

\subsection{The afterglow of GRB\,110715A in a global context}

\begin{figure*}
\centering
\includegraphics[width=\columnwidth]{figures/KP110715A_Obs.pdf}
\includegraphics[width=\columnwidth]{figures/KP110715A_zone.pdf}
\caption{The observed $R_C$-band afterglow of GRB\,110715A in comparison to a large sample of long GRB afterglows (left). After correction for the significant foreground extinction, it is seen to be one of the brightest afterglows ever observed. After correcting for rest-frame extinction and shifting to $z=1$ (right), the afterglow of GRB\,110715A is more common, although it remains among the more luminous detected to date at late times.}
\label{fig:complc}
\end{figure*}

\begin{figure}
\centering
\includegraphics[width=\columnwidth]{figures/Peak_mm_z.eps}
\caption{Top: mm/submm afterglow as compared with the sample of \citet{2012A&A...538A..44D}. Bottom: Radio afterglow of GRB\,110715A compared with the sample of \citet{2012ApJ...746..156C}}
\label{fig:mmrad}
\end{figure}

Using the UVOT and GROND data, and adding the early $R_C$ band observations from \cite{2011GCN..12174...1N}, we construct a composite light curve by shifting all data to the $R_C$ band (no evidence for chromatic evolution is found). This light curve extends over almost four decades in time. Comparing it to the sample of long GRB afterglow light curves taken from \citet{2006ApJ...641..993K, 2010ApJ...720.1513K, 2011ApJ...734...96K}, we find that (after correcting for the significant -- 1.6 magnitudes -- foreground extinction) the afterglow is  among the brightest ever detected (especially after $\sim0.3$ days, see Fig.~\ref{fig:complc} left panel), comparable to those of GRB\,991208 \citep{2001A&A...370..398C} and GRB\,060729 \citep{2011MNRAS.413..669C}, both at lower redshift (see section \ref{sec:spec}). It becomes fainter than 20th magnitude only after about 4.5 days. Using the GROND data, we find a best fit for the Spectral Energy
Distribution (SED) of the afterglow with $\beta=0.90 \pm 0.22$, and a small (essentially zero) $A_V=0.09 \pm 0.18$ using SMC dust. With these data and knowledge of the redshift, we use the method of \citet{2006ApJ...641..993K} to shift the afterglow, corrected for all extinction, to $z=1$. We find a magnitude shift of $dRc=+0.38^{+0.17}_{-0.32}$. At one day after the trigger (in the $z=1$ frame), it is $R_C=17.97^{+0.19}_{-0.33}$, and $R_C=13.90^{+0.23}_{-0.35}$ at 0.001 days. This places the afterglow into the tight  peak found by \citet{2010ApJ...720.1513K} (their figure 6), which is formed by afterglows which are likely forward-shock dominated at early times already. This does not mean that a reverse shock component is not present. According to \citet{2010ApJ...720.1513K}, the early afterglow can be classified as ``Limit + Slow Decay'' \citep[][their  table 5]{2010ApJ...720.1513K}. In this sense, except for the rebrightenings, the afterglow is seen to be typical.

In Figure \ref{fig:mmrad}, we compare the radio and submm emission of GRB\,110715A to the samples of \citet{2012A&A...538A..44D} and \citet{2012ApJ...746..156C}: in submm, the afterglow peak brightness is among the brightest observed, with similar luminosity as GRB\,030329, GRB\,100621A or GRB\,100418A, but still an order of magnitude less luminous than the highest luminosity events (GRB\,980329, GRB\,090313, GRB\,080129 or GRB\,050904). The situation in radio is similar, with GRB\,110715A being amongst the brightest events.

At early times the physical size of the GRB afterglow emission region will be small, and thus there is the possibility of interstellar scintillation (ISS) modulating the observed flux of the afterglow, as has been seen previous in GRBs such as GRB\,970508 \citep{1997Natur.389..261F}. GRB\,970508 was seen to have large (40-50\%) fractional modulations in flux at 1.4 and 8.6~GHz for up to two months post burst, after which the intrinsic source size became large enough to break the conditions under which ISS is possible.

According to \citet{1998MNRAS.294..307W} the transition frequency at the location of GRB\,110715A is $\sim$ 40~GHz, indicating that, when present, scintillation should be strong (m$_d$ $>$ 1) below this frequency, and weak (m$_d$ $<$ 1) at higher frequencies. The temporal resolution of our observations during the first two weeks after the GRB is low so we are unable to measure scintillation. However, differences between the modelled and observed flux densities seen at $\lesssim$ 40~GHz in the first 2 weeks post burst are consistent with scintillation.

\subsection{Spectral absorption lines of the optical afterglow}
\label{sec:spec}

\begin{figure*}
\centering \includegraphics[width=0.8\textwidth]{figures/lsp.eps}
\caption{Line strength diagram of the afterglow spectrum of GRB\,110715A, following the prescription of \citet{2012A&A...548A..11D}.}
\label{lsp}
\end{figure*}

We detect eight absorption features in the complete X-shooter spectrum that we identify as caused by \hbox{{\rm Fe}{\sc \,ii}}, \hbox{{\rm Mg}{\sc \,ii}}, \hbox{{\rm Mg}{\sc \,i}}, \hbox{{\rm Ca}{\sc \,ii}}, and \hbox{{\rm Ca}{\sc \,i}}\ at a common redshift of 0.8225 $\pm$ 0.0001. For recent Planck cosmological parameters \citep[$\Omega_{\rm   M}$ = 0.315, $\Omega_\Lambda$ = 0.685, $H_0$ = 67.3 \hbox{km~s$^{-1}$}\ Mpc$^{-1}$;][]{2014A&A...571A..16P}, this redshift corresponds to a luminosity distance of 5357.86 Mpc.

We have measured the equivalent widths of these lines and limits for several others using the self-developed code used in \citet{2009ApJS..185..526F} and \citet{2012A&A...548A..11D}. The results are shown in table \ref{table:ew}, as well as the composite afterglow spectrum by \citet{2011ApJ...727...73C} for comparison purposes. Using the prescriptions given by \citet{2012A&A...548A..11D}, we find that the neutral element population is higher than average. Detection of \hbox{{\rm Ca}{\sc \,i}}$\lambda 4227$, a line rarely observed in GRB afterglows \citep{2012A&A...548A..11D}, also supports the low ionisation hypothesis of the material in the line of sight to GRB\,110715A.

Following the prescription of \citet{2012A&A...548A..11D}, we obtain a line strength parameter for GRB\,110715A of LSP = -0.83 $\pm$ 0.47, implying that this event is in the percentile 13.4 of line strengths, and indicating a lower than average column density of material in the line of sight (86.6\% of GRBs have stronger lines). This often indicates a small host galaxy \citep{2012A&A...548A..11D}. This is consistent with the fact that there are no velocity components in the absorption features faster than 30 \hbox{km~s$^{-1}$}.

\begin{table}

\caption{Features in the X-shooter spectra.}
\label{table:ew}
\begin{tabular}{lccc}
\hline\hline
Feature & $\lambda_{obs}$ [\AA] & $EW$ [\AA] & $EWc$ [\AA] $(a)$ \\
\hline
\hbox{{\rm Al}{\sc \,ii}}$\lambda$1671 & $\sim$3045 & $<$ 7.82 & 1.04 $\pm$ 0.02 \\
\hbox{{\rm Al}{\sc \,iii}}$\lambda$1855 & $\sim$3380 & $<$ 1.92 & 0.89 $\pm$ 0.02 \\
\hbox{{\rm Al}{\sc \,iii}}$\lambda$1863 & $\sim$3395 & $<$ 2.32 & 0.68 $\pm$ 0.02 \\
\hbox{{\rm Zn}{\sc \,ii}}$\lambda$2026+\hbox{{\rm Cr}{\sc \,ii}}$\lambda$2026 & $\sim$3692 & $<$ 1.97 & 0.60 $\pm$ 0.02 \\
\hbox{{\rm Cr}{\sc \,ii}}$\lambda$2062+\hbox{{\rm Zn}{\sc \,ii}}$\lambda$2063 & $\sim$3758 & $<$ 1.30 & 0.53 $\pm$ 0.02 \\
\hbox{{\rm Fe}{\sc \,ii}}$\lambda$2261 & $\sim$4120 & $<$ 1.81 & 0.38 $\pm$ 0.02 \\
\hbox{{\rm Fe}{\sc \,ii}}$\lambda$2344 & $\sim$4272 & $<$ 1.68 & 1.74 $\pm$ 0.02 \\
\hbox{{\rm Fe}{\sc \,ii}}$\lambda$2374 & $\sim$4327 & $<$ 1.63 & 1.00 $\pm$ 0.02 \\
\hbox{{\rm Fe}{\sc \,ii}}$\lambda$2383 & $\sim$4342 & $<$ 1.60 & 1.65 $\pm$ 0.02 \\
\hbox{{\rm Fe}{\sc \,ii}}$\lambda$2587 & 4714.04 & 1.07 $\pm$ 0.47 & 1.33 $\pm$ 0.02 \\
\hbox{{\rm Fe}{\sc \,ii}}$\lambda$2600 & 4737.32 & 2.47 $\pm$ 0.73 & 1.85 $\pm$ 0.03 \\
\hbox{{\rm Mg}{\sc \,ii}}$\lambda$2796 & 5096.44 & 1.99 $\pm$ 0.34 & 1.71 $\pm$ 0.02 \\
\hbox{{\rm Mg}{\sc \,ii}}$\lambda$2803 & 5109.09 & 1.50 $\pm$ 0.31 & 1.47 $\pm$ 0.02 \\
\hbox{{\rm Mg}{\sc \,i}}$\lambda$2853 & 5198.29 & 1.50 $\pm$ 0.40 & 0.78 $\pm$ 0.01 \\
\hbox{{\rm Ca}{\sc \,ii}}$\lambda$3935& 7171.01 & 0.72 $\pm$ 0.07 & 0.76 $\pm$ 0.02 \\
\hbox{{\rm Ca}{\sc \,ii}}$\lambda$3970 & 7234.51 & 0.74 $\pm$ 0.07 & 0.66 $\pm$ 0.02 \\
\hbox{{\rm Ca}{\sc \,i}}$\lambda$4228 & 7705.26 & 0.37 $\pm$ 0.06 & 0.11 $\pm$ 0.02 \\
\hline
\end{tabular}
\\[0.2cm]
\begin{scriptsize}
(a) Equivalents widths measured on the composite GRB afterglow spectrum \citep{2011ApJ...727...73C}.
\end{scriptsize}
\end{table}

\subsection{The host galaxy}

We computed the distance between the afterglow and the host galaxy core. The centroid is offset by 0.21 $\pm$ 0.03 \arcsec\ with respect to the ALMA position, which at the redshift of GRB\,110715A corresponds to 1.56 $\pm$ 0.19 kpc. This is comparable to the typical offset of 1.2 kpc seen for long GRBs \citep{2002AJ....123.1111B,2012A&A...548A..11D}. The host absolute magnitude (AB) would be $M$ = -18.2 mag at a restframe wavelength of 4200 \AA, which is similar to the Johnson $B$-band (without needing to make assumptions on the host galaxy spectral index).

The luminosity of the host galaxy is low, even relative to other GRB hosts \citep[which tend to occur in lower-mass and lower-luminosity galaxies than average at $z \lesssim 1.5$; e.g.][]{2016ApJ...817....7P}, although it is by no means extreme or exceptional. For example, relative to the UV luminosity distribution of nine galaxies at roughly similar redshift ($0.5<z<1.1$) in the TOUGH sample \citep{2015ApJ...808...73S}, this host galaxy is less luminous than six or more, depending on the unknown $k$-correction across the Balmer break which is not known for the TOUGH sample. We also compared this magnitude to synthetic $B$-band magnitudes of galaxies from the larger, multi-colour SHOALS sample \citep[][and work in prep.]{2016ApJ...817....8P}. The host of GRB\,110715A is about 0.6 mag less luminous than the median $B$ magnitude of $0.5<z<1.1$ galaxies in this sample, and is more luminous than only five out of these 21 galaxies. Compared to a more local galaxy population, it is slightly more luminous than the LMC ($M_B \sim -17.5$) but of course much less luminous than nearby spirals such as the Milky Way or M31 ($M_B \sim -20.5$ to $-21$). This faint host galaxy is consistent with the faint and unresolved absorption features seen in the afterglow spectrum. Considering also its very low ionisation environment, all evidence suggest that the sight-line towards GRB\,110715A is probing an small dwarf host galaxy, maybe in its initial star-forming episode due to the low background ionising radiation, which keeps an unusual abundance of \hbox{{\rm Ca}{\sc \,i}}.

\subsection{Modeling of the afterglow evolution}
\label{sec:agm}

\subsubsection{Model and fitting description}

\begin{table}
\caption{The lower and upper boundaries of the priors on parameters used in the analysis.}
\label{tab:priors}
\begin{tabular}{llll}
\hline\hline
Parameter & Distribution & Lower & Upper \\
\hline
$E_{iso}$ [$10^{53}$ erg] & log-uniform & 0.01 & 10000 \\
$\Gamma_0$ & log-uniform & 10 & 2000 \\
$\theta_0$ [deg] & log-uniform & 0.1 & 90 \\
$p$ & uniform & 1.1 & 4.0 \\
$\epsilon_i$ & log-uniform & 0.0001 & 0.5 \\
$\epsilon_e$ & log-uniform & 0.0001 & 0.5 \\
$\epsilon_B$ & log-uniform & 0.0001 & 0.5 \\
$A_*$ [$5.015 \cdot 10^{11}$ cm$^{-3}$] & log-uniform & 0.00001 & 100 \\
$n_0$ [cm$^{-3}$] & log-uniform & 0.0001 & 1000 \\
$t_{sh}$ [min] & log-uniform & 0.00001 & 200 \\
$r_{sh}$ & uniform & 1 & 50 \\
$t_1^{(a)}$ [days] & log-uniform & 0.0001 & 200 \\
$E_1/E_0^{(b)}$ & uniform & 0 & 50 \\
$A_{V, host}$ [mag] & uniform & 0 & 1.0 \\
$E(B-V)$ [mag] & Gaussian$^{(c)}$ &  & \\
\hline
\end{tabular}
\\[0.2cm]
\begin{scriptsize}
(a) $t_1$ is the time in the observer's frame at which the energy injection catches up with the forward shock. \\
(b) $E_1$ is the energy of the injection and $E_0$ is the initial energy release. \\
(c) $\mu$ = 0.56, $\sigma$ = 0.04
\end{scriptsize}
\end{table}

The afterglow emission was modeled with the numerical code of \citet{2006ApJ...647.1238J}. This software has been used successfully to model several different afterglows, including GRB\,060121 \citep{2006ApJ...648L..83D}, GRB\,050408 \citep{2007A&A...462L..57D}, GRB\,060526 \citep{2010A&A...523A..70T}, and GRB\,050525A \citep{2012MNRAS.427..288R}. This model assumes the emission originates in a forward shock only, with a top-hat jet configuration. The algorithm simulates that a slab of matter with mass $M_0$ is ejected with a Lorentz factor of $\Gamma_0$ into a cone with a half-opening angle of $\theta_0$. The slab starts accumulating matter and slows down in the process. Energy injections ($E_i$) at a time $t_i$ are modelled as slabs of matter moving at lower speeds than the forward shock ($\Gamma_i < \Gamma_0$) and catching up to it at later times. At the time of collision, the energy and momentum of the forward shock of the injected slab is instantaneously added to the already moving mass. The emission from any reverse shock formed in the collision is ignored. To calculate the emission, we assume that a fixed fraction of the energy of the forward shock is contained in the magnetic field and electron distribution of the forward shock. For the magnetic field, this fraction is denoted with $\epsilon_B$. In \citet{2006ApJ...647.1238J}, the fraction of energy contained in the electrons was denoted with $\epsilon_e$. This is now  changed, to allow for the slope of the electron power-law distribution, $p$, to be less than 2. We used the formalism of \citet{2001ApJ...554..667P} and denote with $\epsilon_i$ the fraction of energy contained in the electrons with the lowest energy in the distribution. The highest energy in the distribution is then limited such that the total energy of the electron distribution never exceeds a fraction $\epsilon_e$ of the forward shock energy.

To explain the data, we need a model that includes a temporary increase in flux around 0.3 days after the onset of the GRB that is observed in the light curves shown in Figure~\ref{fig:obs}. We chose three different types of models that we expect have this behaviour: a model with a constant density interstellar medium ($n_0$) and a single energy injection (CM), a model with a wind density external medium ($\rho = A_* r^{-2}$) and a single energy injection (WM), and a model with a wind termination shock (with fractional change in density at the shock front denoted by $r_{sh}$) but no energy injection (TS).

The best fit model parameters are found using Bayesian inference using the MultiNest tool \citep{2009MNRAS.398.1601F}. MultiNest is well suited for exploring the parameter space of the non-linear afterglow model and finds parameter correlation as well as all modes in the parameter space fitting the data similarly well. In addition to the afterglow model parameters, we also determine the host dust extinction in the fit, which we assume follows an SMC-like extinction curve. It is also possible to let the Galactic dust extinction vary as a nuisance parameter. This is of special interest in our case due to the large and uncertain value along the GRB line of sight through our Galaxy.

One of the main benefits of a Bayesian analysis is the introduction of prior distributions on parameters. For this analysis we have unfortunately very little prior knowledge on their values. We therefore opted for flat priors on all parameters, but Galactic reddening, and made sure the parameter limits were large enough so that the posterior is not affected by these limits unless they are physical (see Table~\ref{tab:priors}). Examples of such physical boundaries are the requirements that the extinction of the host be positive ($A_{V, host} > 0$) and the fractional change in density at the shock front should not decrease ($r_{sh} > 1$). We also constrain the fraction of energy in the electrons ($\epsilon_e$) and magnetic field ($\epsilon_B$) such that the fraction of energy contained in the rest of the jet, $\epsilon = 1 - \epsilon_e - \epsilon_B$, is larger than both $\epsilon_e$ and $\epsilon_B$.  This is to make sure the jet's energy is not dominated by that of the electrons and the magnetic field. The constraint is not hard and $\epsilon$ is usually somewhere in between $\epsilon_e$ and $\epsilon_B$ if both are large like in this analysis. There is also the hard prior that $\epsilon_e > 1.1 \epsilon_i$ so the energy in the total electron distribution is always at least 10 percent greater than that contained in the electrons with the lowest value. This constraint is actually reached in all of our models, resulting in a strong correlation between $\epsilon_e$ and $\epsilon_i$ (see Fig.~\ref{fig:marginal2d}).

Due to several reasons, such as the high Galactic reddening, the wavelength range on which \hbox{{\rm H}{\sc \,i}}\ absorption is located, and the difficulties to compute the effective wavelength of the UVOT \textit{white} filter due to its band width, we performed different fits in order to identify and quantify the sources of systematic uncertainties. We excluded the upper limits from the UV filters of UVOT as well as observations using its $u$-band filter because of the uncertainty on the Galactic dust extinction (none of  the models are able to accurately reproduce those data points, either when included in the fit or not). Below we discuss the best fit results that were obtained, and refer the interested reader to the material contained in the Appendix \ref{app:view} and online material for the result details of the complete set of Bayesian fits.

\subsubsection{The best fit}

\begin{figure*}
\centering
\includegraphics[width=\textwidth]{figures/lc06.jpg}
\caption{Best fits to the GRB\,110715A light curves. Fluxes are independently scaled for each band for clarity. The full set of plots for each subset is available in the online version.}
\label{fig:lc}
\end{figure*}

\begin{figure*}
\centering
\includegraphics[width=\textwidth]{figures/sed06.jpg}
\caption{Best fits to the SED for GRB\,110715A observed at several epochs. The full set of plots for each data subset is available in the online version.}
\label{fig:sed}
\end{figure*}

\begin{figure*}
\centering
\includegraphics[width=\textwidth]{figures/marginal1d_06.jpg}
\caption{Posterior distributions of the three models for the best fit data subset. In all marginal plots, CM is represented in green, TS in red, and WM in blue. The full set of plots for each set is available in the online version.}
\label{fig:marginal1d}
\end{figure*}

\begin{figure*}
\centering
\includegraphics[width=\textwidth]{figures/marginal2d_TS_06.jpg}
\caption{Parameter correlations for the best fit model. The full set of plots for each data subset is available in the online version.}
\label{fig:marginal2d}
\end{figure*}

\begin{table*}
\caption{The Bayesian evidence and the parameter posterior mean as reported by MultiNest for the three different models of the best fit data-set. The full table for each data subset is available in the online version.}
\label{tab:pars}
\begin{tabular}{l|ccc}
Parameter & CM & TS & WM \\
\hline\hline
Evidence & --1015.83 & --995.70 & --1129.24 \\
$\chi^2_r$ & 5.73 & 5.50 & 7.30 \\
$\chi^2_{r, x}$ $^{(a)}$ & 2.47 & 2.15 & 2.76 \\
$\chi^2_{r, o}$ $^{(b)}$ & 13.00 & 11.34 & 17.48 \\
$\chi^2_{r, r}$ $^{(c)}$ & 26.79 & 32.54 & 36.38 \\
$E_{\rm iso}$ [erg] & $53.63^{+0.66}_{-0.62} \times 10^{51}$ & $55.10^{+0.92}_{-0.82} \times 10^{51}$ & $0.38^{+0.60}_{-0.26} \times 10^{55}$ \\
$E_0$ [erg] & $3.63^{+0.14}_{-0.12} \times 10^{50}$ & $5.36^{+0.18}_{-0.17} \times 10^{50}$ & $3.64^{+0.15}_{-0.14} \times 10^{49}$ \\
$\Gamma_0$ & $1799^{+82}_{-110}$ & $1510^{+180}_{-200}$ & $184^{+35}_{-12}$ \\
$\theta_0$ [deg] & $9.44^{+0.22}_{-0.20}$ & $11.32 \pm 0.12$ & $0.35^{+0.27}_{-0.13}$ \\
$p$ & $1.8334^{+0.0038}_{-0.0036}$ & $1.8148 \pm 0.0041$ & $1.8124^{+0.0037}_{-0.0039}$ \\
$\epsilon_e$ & $9.32^{+0.57}_{-0.41} \times 10^{-2}$ & $(11.64 \pm 0.40) \times 10^{-2}$ & $(8.53 \pm 0.26) \times 10^{-2}$ \\
$\epsilon_i$ & $(8.31 \pm 0.31) \times 10^{-2}$ & $(10.44 \pm 0.32) \times 10^{-2}$ & $(7.62 \pm 0.19) \times 10^{-2}$ \\
$\epsilon_B$ & $(2.72 \pm 0.28) \times 10^{-1}$ & $(1.59 \pm 0.16) \times 10^{-1}$ &  $(4.44 \pm 0.47) \times 10^{-2}$ \\
$A_*$ [$5.015 \cdot 10^{11}$ cm$^{-3}$] &  & $0.01747^{+0.00078}_{-0.00074}$ & $0.571^{+0.023}_{-0.022}$ \\
$n_0$ [cm$^{-3}$] & $1.05^{+0.12}_{-0.10}$ &  &  \\
$t_{sh}$ [min] &  & $3.13^{+0.13}_{-0.12} \times 10^{1}$ &  \\
$r_{sh}$ &   & $8.33^{+0.56}_{-0.54}$ &  \\
$t_1$ [days] & $5.03^{+0.42}_{-0.44} \times 10^{1}$ &   & $(6.79 \pm 0.91) \times 10^{-4}$ \\
$E_1/E_0$ & $1.34^{+0.59}_{-0.35}$ &   & $49.01^{+0.43}_{-0.61}$ \\
$E_{\rm total}$ [erg] & $1.72^{+0.42}_{-0.24} \times 10^{51}$ & $10.72^{+0.36}_{-0.34} \times 10^{50}$ & $3.62^{+0.14}_{-0.12} \times 10^{51}$ \\
$A_{V, host}$ [mag] & $0.0048^{+0.0031}_{-0.0021}$ & $0.0102^{+0.0063}_{-0.0046}$ & $0.0099^{+0.0064}_{-0.0042}$ \\
$E(B-V)$ [mag] & $0.5249 \pm 0.0030$ & $0.5277^{+0.0037}_{-0.0044}$ & $0.5749^{+0.0035}_{-0.0043}$ \\
\hline
\end{tabular}
\\[0.2cm]
\begin{scriptsize}
(a) $\chi^2$ computed only with the X-ray data.\\
(b) $\chi^2$ computed only with the UV, optical and nIR data.\\
(c) $\chi^2$ computed only with the submm and mm data.\\
\end{scriptsize}
\end{table*}

\begin{figure}
\centering
\includegraphics[width=\columnwidth]{figures/photonIndex04.png}
\caption{Best fit of the evolution of the photon index to that found from XRT data analysis. The full set of plots for each subset is available in the online version.}
\label{fig:photon}
\end{figure}

We found the best fit models to be those in which we excluded the UV bands, we set MW extinction as a nuisance parameter, and the UVOT \textit{white} band was shifted to V (see Table~\ref{tab:goodness} for a detailed statistical analysis of the results for the complete grid of fits). This table suggests the TS fit as the most plausible model that describes the afterglow. However, none of them is either a statistically good fit or can fully explain the temporary flux increase at $\sim$0.3~days. We can also observe that there are no statistical arguments to reject most of the fits when compared with the best. Fit results are shown overlaid on the data in Figures \ref{fig:lc} (light curves) and \ref{fig:sed} (spectral energy distributions).

The time of the wind termination shock for the best TS model agrees very well with the time of the flux increase in the light curve. The density increases by a factor of 8.3 at that time, more than 2 times the expected density increase for strong shocks. Despite this, the effect on the light curves is not strong enough to explain the data. Due to the spectral parameters required in the fit, the wind termination shock causes a flux decrease rather than an increase as the cooling break is just below the optical band. The slow decay in the early X-ray light curve in the model is caused by the injection break being above the X-ray frequency. This requires there to be a spectral evolution in the X-ray light curve that is not observed. In both cases the preferred location of the energy injection is at a different point than expected. For the best fit of the CM model it is much later and serves only to explain the latest radio points while for the WM model it happens very early to explain the shallower decay between 0.01 and 1 days. The best model also has a hard time explaining the rapid decline in the light curve observed by the GROND instrument. The earliest points are under-predicted while the later points are over-predicted. This is again something that all the models fail to reproduce. The CM model does a slightly better job, but the WM model is worst. The models have a similarly hard time at explaining the late time X-ray light curve as they don't decay rapidly enough.

Figure \ref{fig:marginal1d} compares the evolution of the photon index of our best fit models to that found from XRT data analysis. The CM and TS models do a reasonable job of explaining the X-ray spectral evolution with the exception of the first time bin where the models are harder than observed. The WM model agrees with the first time bin but is then too soft for the next two bins.

Finally, the best model is unable to explain the early and late radio and submm data. The model has a hard time explaining the rapid rise of the 44~GHz data simultaneously with the decay of the 345~GHz data and the rather flat light curve at 5.5~GHz. The self-absorption break, $\nu_a$, needs to pass through the 44~GHz band at around 2 days to explain the rapid increase and it should have already passed the 345~GHz band at 1 day and the 5.5~GHz band at 2 days. It is impossible for the model to meet these criteria. In addition, the 44~GHz light curve starts decaying at around 10 days with a slope that is incompatible with post jet-break evolution and at the same time the 18~GHz band is compatible with being nearly constant. The CM model has similar issues as the TS model although it does slightly better at late times because the injection lifts the radio light curve to match the last points. There is, however, no other indication for the energy injection and it is unlikely to be the correct physical interpretation. The WM model does the best job with the submm and radio data, but is still far from explaining the details of the observed afterglow.

Table~\ref{tab:pars} shows the best fit model posterior median for the parameter values and their associated 68\% statistical errors. Figure~\ref{fig:marginal1d} shows a plot comparing the resulting distributions of the models for the best data subset. The parameter values that give the smallest $\chi^2$ are usually located near the peak of the posterior distributions, and their distributions are mostly symmetric, with notable exceptions in the WM model where long tails can be seen for $E_{\rm iso}$, $\Gamma_0$, and $\theta_0$. The inferred values are mostly typical for a GRB afterglow with a few exceptions. The half opening angle $\theta_0$ in the WM model is unreasonably low and requires an extreme confinement of the outflow. It is also the worst performer of the 3 models and we therefore consider it an unreasonable model. The value of the electron power-law index $p$ is on the lower side and lower than expected from shock-acceleration theory \citep{2001MNRAS.328..393A}. It is, however, well within the range of values deduced from observations of relativistic shocks \citep{2006MNRAS.371.1441S}. The fraction of energy contained in the magnetic field and the electron distribution, $\epsilon_B$, and $\epsilon_e$, respectively is rather large. $\epsilon_i$ is also larger than usual and constrained mostly by the equipartition requirements for the electron energy distribution rather than the position of the injection peak in the synchrotron spectrum. These large values cause the afterglow to be in the fast-cooling regime for the entire duration of the afterglow and the assumption of no radiative losses is likely invalid.

Our values for the host extinction are compatible with the value being very small as found earlier using GROND data only. The statistical error is significantly smaller because we use  the entire data-set, but the exact value is model dependent. As already discussed, the Galactic line of sight extinction is important in the GRB direction. The expected uncertainty could be large too, so similarly to the host galaxy, the Galactic $E(B-V)$ was left in some fits as a free parameter. Resulting Galactic and host galaxy solutions show a clear anti-correlation, limiting our constraints of the inferred host galaxy A$_{V, host}$. In Figure~\ref{fig:marginal2d} we include the two dimensional marginal plots for the $E(B-V)$ of the Galactic extinction with the rest of the parameters when it is included in the fit. As shown in Appendix~\ref{app:view}, the galactic $E(B-V)$ value is model dependent, and results are somewhat bimodal, sometimes consistent with the dust maps of \citet{1998ApJ...500..525S}, and sometimes with \citet{2011ApJ...737..103S}, the latter being the more favoured. The figures also show that the upper value found for the $E(B-V)$ parameter in this analysis is basically bound by the host extinction going to 0.

We also discuss in Appendix \ref{app:view} the hypothesis that the reverse shock (RS) contribution has to be taken into account \cite[e.g.,][]{2006A&A...454L.119J, 2013ApJ...776..119L}, as well as the possibility that a double jet model \citep[e.g.][]{2005MNRAS.360..305S, 2008Natur.455..183R, 2011A&A...526A.113F, 2014MNRAS.444.3151V} is necessary to explain this afterglow. The conclusion is that, in spite of them possibly being present, none of the options can improve the fit starting at 0.5 days after the trigger, so other considerations must be taken into account to improve the fits we performed.

\section{Conclusions}

We present an extensive follow-up of the afterglow of GRB\,110715A in 17 bands ranging from a few seconds up to 74 days after the trigger. The line of sight is affected by strong foreground Galactic extinction, which complicated the follow-up and the analysis of the data.

GRB\,110715A had a very bright afterglow at all wavelengths, although its intrinsic luminosity is not exceptional.

Optical/nIR spectroscopy obtained with X-shooter shows weak absorption features at a redshift of $z$ = 0.8224 with no resolved velocity components ($\lesssim$ 30 \hbox{km~s$^{-1}$}). Absorption line ratios indicate a low ionization environment, confirmed by the rare detection of \hbox{{\rm Ca}{\sc \,i}}.

Deep late imaging reveals a faint host galaxy with an absolute magnitude of M$_B$ = -18.2. This is consistent with the weak absorption features detected in the spectrum.

We attempted to model the broadband data with a fireball model based on the prescription of \citet{2006ApJ...647.1238J}. The best model implies a forward shock evolving through a wind environment with a termination shock. In spite of describing roughly the behavior of the afterglow, none of the models is able to get a statistically acceptable fit. This shows the need for better broadband sampling and more complex models to accurately describe the physics of GRB afterglows. There are several works that explore other possibilities, such as magneto-hydrodynamic simulations \citep{2012ApJ...749...44V}, which was satisfactorily used, e.g., in \citet{2014MNRAS.438..752G,2015ApJ...799....3R,2015ApJ...806...15Z}, or central engine activities \citep{2014ApJ...787...66Z}. These and other effects might be considered together in future works to get a more accurate view of the GRB afterglow physics.

Radio and sub-mm, along with X-ray observations, have been proven to be the most constraining bands for the afterglow modeling. We were limited by sensitivity for a long time in the crucial wavelength range of sub-mm, but now that ALMA is available, we have a good chance of getting high-quality data for a larger number of GRBs. This new, current and future facilities will allow us to probe the emission mechanisms in greater detail than previously possible, and will be determinant in the evolution of the GRB afterglow models.

\section*{Acknowledgements}

In memory of Javier Gorosabel: an exceptional supervisor, a brilliant scientist, and an even better human being.
RSR is grateful to SEPE for financial support while finishing this work and his PhD thesis.
RSR, SRO, AJCT, YDH, SJ, and JCT acknowledge financial support of the Spanish Government projects AYA 2009-14000-C03-01 and AYA 2012-39727-C03-01.
Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.
AdUP and CT acknowledge support from Ram\'{o}n y Cajal fellowships and from the Spanish research project AYA 2014-58381.
JJ acknowledges financial contribution from the grant PRIN MIUR 2012 201278X4FL 002 "The Intergalactic Medium as a probe of the growth of cosmic structures".
DAK acknowledges financial support by MPE Garching and TLS Tautenburg.
Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1).
PS and TK acknowledges support through the Sofja Kovalevskaja Award to P. Schady from the Alexander von Humboldt Foundation of Germany.
AU is grateful for travel funding support through the Max-Planck Inst. for Extraterrestrial Physics.
SK and ANG acknowledge support by DFG grant Kl 766/16-1.
ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.
This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester.

\bibliographystyle{mnras}

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Nearly 120,000 children and their parents flocked to the Marunouchi Kids Jamboree, an annual three-day educational event for elementary and junior high school students in the Tokyo Metropolitan area during a recent school break.
Aramco Asia-Japan (AAJ) took part this year in the event, co-organizing a user-experience-based workshop under the theme of "Do You Know a Coral Reef? Why Is It Important?" for the students while teaming up with its corporate social responsibility partner of eight years, the Okinawa Coral Reef Conservation Consortium (OCRCC).
The goal of the workshop was to raise interest in kids from the nation's capital for protection of the marine ecosystem in the southern utmost prefecture of Okinawa — a popular tourist destination for its beautiful ocean and beaches.
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The interactive and entertaining programs prompted the audience to better understand the importance of coral reefs in Okinawa and their priceless value in making the island one of the world's most diversified marine spots.
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Through engaging activities such as card games, handicrafts, and ad-lib performances, the workshop provided a firsthand experience to children in Tokyo to learn more about the reef building corals and the importance of protecting the marine environment. Photos and videos of the beautiful underwater world around the Okinawa prefecture enabled the students to literally dive into biodiversity and the symbiotic relationship with the coral reef ecosystem.
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The Marunouchi Kids Jamboree, a public cultural event, is jointly sponsored by the country's leading daily newspaper, Yomiuri, and the Tokyo International Forum with the goal of encouraging urban kids to develop their curiosity in science, engineering, music, and art.
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The vessel loops were removed after the anastomosis was found to be hemostatic.
Flow in the right internal carotid was confirmed with Doppler.
Thrombin and gelfoam was placed temporarily around the anastomosis.


For demolition in Bateau Bay, choose the demolition contractor providing service in the suburb.
Check for a contractor offering the most competitive rates.
The contractor must have licensed and insured workmen.
Make sure that they use appropriate safety measures while the work is in progress.
If you require demolition in Bateau Bay, you can rely on us as we are one of the best demolition contractors in the area. We at Complete Demolition are renowned for our punctual and efficient demolition service within the suburb. We handle every residential and commercial demolition project with equal amounts of dedication and ensure that the service is completed within the deadlines. With our wide range of services and latest machinery we are capable of providing guaranteed customer satisfaction at highly cost effective rates.
With this extensive range of services we cover every aspect of demolition. There is never any break during the process as we have an unrestricted demolition license enabling us to carry out industrial level demolition as well.
At Complete Demolition, we have over 20 year of experience in the demolition field. Our main focus is on providing a completely environment-friendly service; and we take special care that all the materials removed from the site are either recycled through our recycling depot or sent on to an EPA approved recycling yard. We have handled numerous projects of demolition in Bateau bay, maintaining an impeccable track record. Our company also has a large number of repeat customers who request our services for different projects. They know that the work will be completed within the shortest possible time and in the most expert manner. If you are looking for any residential, commercial or industrial demolition in Bateau Bay, just give us a call on 0424 541 452. You can also choose to email us via the online Email Us Form and our expert will get in touch with in the shortest possible time.


text:
Q: Magento database tables - where is EAN stored I am working on a Magento project and to complete an import to ebay process I may need to do a bulk update on EAN numbers.
I am reviewing the database and the tables - and I haven't found or see any indication as to where this "EAN" field is stored.
I can see it present on individual products under "general" in the edit panel on the magento site

A: Read about EAV.
get eans with product ids
SELECT entity_id, value FROM catalog_product_entity_varchar
WHERE attribute_id IN ( SELECT attribute_id FROM eav_attribute WHERE attribute_code = 'ean');

write ean to magento
INSERT INTO catalog_product_entity_varchar
(value, entity_id, entity_type_id, attribute_id, store_id)
VALUES ('".$value."', ".$productId.", 4, ".$attributeId.", ".$storeId.")
ON DUPLICATE KEY UPDATE value = '".$value."'

where $attributeId is the id of "ean" attribute from table eav_attribute

A: As it is present under "General" tab when viewing individual products, it means that EAN is a product attribute.
Values are stored in catalog_product_entity_* tables, based on the backend type of the EAN product attribute. In case you don't know the type, you will need to check the contents of eav_attribute table for the EAN record.
A good article that explains Magento's database structure can be found here: https://fishpig.co.uk/magento/tutorials/eav-database-structure/

A: I dont think Magento comes with EAN code out of the box. You have to create an attribute for that.

redpajama_set_name: RedPajamaStackExchange


text:
Q: How can I update the other select2 selectbox value based on the value of a select2 selectbox? I tried it like this but it didn't work. How can I do that?

*

*Do not show category option unless Type is selected

*1 time selection for both selectboxes (without removing multiple)

$("#clct, #cyc").select2({
    //maximumSelectionLength: 1,
});

// Select step by step for homepage
$('#clct').on('change', function() {
  var selected = $(this).val();
  $("#cyc option").each(function(item){
    console.log(selected) ;
    var element =  $(this) ;
    console.log(element.data("tag")) ;
    if (element.data("tag") != selected){
      element.hide() ;
    }else{
      element.show();
    }
  }) ;

  $("#cyc").val($("#cyc option:visible:first").val());

});
<link href="https://cdnjs.cloudflare.com/ajax/libs/select2/4.0.3/css/select2.min.css" rel="stylesheet"/>
<script src="https://cdnjs.cloudflare.com/ajax/libs/jquery/3.3.1/jquery.min.js"></script>
<script src="https://cdnjs.cloudflare.com/ajax/libs/select2/4.0.3/js/select2.min.js"></script>
<select name="bt" id="clct" class="clct input--style-1" data-placeholder="All Types" multiple>
<option value="1">TypeA</option>
      <option value="2">TypeB</option>
      <option value="3">TypeC</option>
      <option value="4">TypeD</option>
</select>

<select name="yc" id="cyc" data-placeholder="Please select type" multiple>
    <option  value="1" data-tag="1">CategoryA</option>
    <option  value="2" data-tag="1">CategoryB</option>
    <option  value="3" data-tag="1">CategoryC</option>
    <option  value="4" data-tag="1">CategoryD</option>
    <option  value="5" data-tag="1">CategoryE</option>
    <option  value="0" data-tag="2">CategoryF</option>
    <option  value="0" data-tag="3">CategoryG</option>
    <option  value="0" data-tag="4">CategoryH</option>
</select>

A:

var clct = $("#clct").select2({
    maximumSelectionLength: 1
});
var cyc = $("#cyc").select2({
    maximumSelectionLength: 1
});

var selectClone = cyc.clone();
cyc.find("option").remove();

$('#clct').on('change', function() {
var arr=$(this).val();
cyc.find("option").remove();

  if (arr.indexOf("1")>-1){
    let opts = selectClone.find('option[data-tag="1"]').clone();
    cyc.append(opts);
  }
  if (arr.indexOf("2")>-1){
    let opts = selectClone.find('option[data-tag="2"]').clone();
    cyc.append(opts);
  }
  if (arr.indexOf("3")>-1){
    let opts = selectClone.find('option[data-tag="3"]').clone();
    cyc.append(opts);
  }

});
<link href="https://cdnjs.cloudflare.com/ajax/libs/select2/4.0.3/css/select2.min.css" rel="stylesheet"/>
<script src="https://cdnjs.cloudflare.com/ajax/libs/jquery/3.3.1/jquery.min.js"></script>
<script src="https://cdnjs.cloudflare.com/ajax/libs/select2/4.0.3/js/select2.min.js"></script>
<select name="bt" id="clct" class="clct input--style-1" data-placeholder="All Types" multiple>
<option value="1">TypeA</option>
      <option value="2">TypeB</option>
      <option value="3">TypeC</option>
      <option value="4">TypeD</option>
</select>

<select name="yc" id="cyc" data-placeholder="Please select type" multiple>
    <option  value="1" data-tag="1">CategoryA</option>
    <option  value="2" data-tag="1">CategoryB</option>
    <option  value="3" data-tag="1">CategoryC</option>
    <option  value="4" data-tag="1">CategoryD</option>
    <option  value="5" data-tag="1">CategoryE</option>
    <option  value="0" data-tag="2">CategoryF</option>
    <option  value="0" data-tag="3">CategoryG</option>
    <option  value="0" data-tag="4">CategoryH</option>
</select>


text:
Mets overcome Matt Harvey's terrible start, beat Marlins 8-6 | Rapid reaction
Updated: Jan. 16, 2019, 9:15 p.m. | Published: Jul. 04, 2016, 11:50 p.m.
MLB: Miami Marlins at New York Mets
New York Mets starting pitcher Matt Harvey (33) pitches against the Miami Marlins during the first inning at Citi Field. (Andy Marlin | USA TODAY Sports)
NEW YORK -- The only thing that dazzled for Mets' right-handed starter Matt Harvey on Monday were his all-white cleats. Everything else was a mess.
But his team bailed him out.
New York orchestrated an 8-6 comeback win over the Miami Marlins at Citi Field on the July 4 holiday, pushing its win streak to five games.
Down 6-0 before their turn to hit in the fourth, the Mets scored in every inning the rest of the game, capped by a two-out, two-run double to right-center in the bottom of the eighth by center fielder Yoenis Cespedes scoring catcher Travis d'Arnaud and second baseman Neil Walker. Jeurys Familia notched his 29th save of the season a few minutes later.
Indeed, aside from Harvey, the Mets were great on Monday. d'Arnaud hit his first home run of the year and finished 3-for-4 with two RBI. Right fielder Curtis Granderson socked his 15th. And in the sixth and seventh innings the Mets plated four runs total, tying the game after Harvey dug such a deep hole. Cespedes finished 3-for-5 with two runs driven in and scored a run.
By almost all measures the Mets are ahead of where they were this time last season, one that ended in a World Series appearance. They should feel good. They just have to figure out Harvey.
HARVEY'S NO GOOD, PRETTY BAD DAY
The big righty threw in the mid to upper 90s all day and struck out four of the 21 Marlins he faced, but of the 17 others who strolled to the plate, 11 collected hits. And perhaps the worst moment of the day wasn't on a pitch at all, but when Harvey tried to throw home after fielding a ground ball in the fourth inning with the bases loaded. He skipped the ball by catcher Travis d'Arnaud, allowing a run to score.
After Monday Harvey's now made 17 starts this season and in six of them he's allowed four or more earned runs. That already matches his 2015 total (29 starts).
When Harvey finally exited the field Monday it was to a loud round of boos from the Citi Field crowd. Statistically it was his second-worse start of the season, the only worse one a six-run, 2.2 inning outing on May 19 against the Nationals.
Final line Monday: 3.2 IP, 11 hits, 5 ER, 4 SO, 0 BB (75 pitches, 50 strikes)
HUGE PLAY
In the top of the eighth inning the Marlins had runners on first and second with no outs when Miami third baseman Martin Prado tried to bunt them into scoring position. It back-fired, though, as first baseman James Loney was able to toss the bunted ball to third for a force out on Ichiro Suzuki and then Prado, who got out of the box slowly, was thrown out at first for a double play. The Mets escaped the inning unscathed.
7TH INNING
Walker walked and Cespedes doubled to lead off the inning. Walker came around to score on a Loney ground out, and Cespedes came in two batters later when Wilmer Flores flew to center, tying the game at six apiece.
NOTES TO KNOW
d'Arnaud homer to right-center in the fourth inning to cut the lead 6-1.
Granderson's fifth inning solo shot to right field cut the lead to 6-2.
Justin Dunn
What will the Mets' lineup look like when Jose Reyes returns?
The Mets and Marlins play Tuesday night (7:10 p.m.) at Citi Field before the series finale on Wednesday (1:10 p.m.). Probably starters:
LHP Wei-Yin Chen (4-3, 5.11) vs. LHP Steven Matz (7-3, 3.40)
LHP Justin Nicolino (2-4, 5.43) vs. Jacob deGrom (4-4, 2.62)


In4All programs bring educators and business professionals together to create learning experiences that impact students at critical times in their K-12 education. All of our programs are informed by research, tied to educational standards, and measured through formal evaluation to ensure we are making a difference for students who have been historically underserved in Oregon.
The STEM Connect 4/5 program partners a sponsoring business with a local elementary school to deliver hands-on learning experiences in the classroom that increase interest in STEM-related fields.
Launched this year, the middle school program partners a business and middle school on a project that is jointly defined by the business volunteers, teachers and students.
Our high school program has provided hundreds of students work-based learning opportunities in real-world settings. And we are looking to expand those opportunities in the years ahead.
In4All programs impacted 4,000 elementary and middle school students in the 2017-2018 school year and we are poised to exceed that number this year. Read our impact report to learn more.


Car Accident Attorney | Should I Take Car Accident Pictures?
Car Accident Attorney | Many of us experience an accident, but do we really know what do to, how to get help, or what our rights are?
An car accident attorney will agree your smart phone may come in handy. Your photos may be used to prove you weren't at fault for the accident, and could ultimately determine how much you could get in a claim settlement.
Your photos won't tell the whole story of the accident, and there's other evidence that can help during a car accident investigation. You'll also want to gather insurance and contact information for everyone involved in the accident. (Taking photos of insurance cards can help.) And you'll want to talk to anyone who witnessed the car accident, record what they saw, and gather their contact information as well.
By Clekis Law|2017-01-25T10:09:20+00:00January 25th, 2017|Auto Accident Attorney|Comments Off on Car Accident Attorney | Should I Take Car Accident Pictures?


A couple of weeks ago we had a triumphant performance of Handel's Messiah – one of the greatest works of music ever written, and a great joy to hear it under our roof. And then, hot on its heels came another amazing achievement directed by Rachel Moon as the Drama Group presented Macbeth – one of the greatest plays ever written. It's probably Shakespeare's most famous and best known play, combining fact and fiction in a blend which raises questions about the supernatural, about witchcraft, about ambition, loyalty, honour, evil and betrayal. I must say I was very proud of our Drama Group that first weekend in July, and I'm sure you too were spellbound by the strong characterisations, the enthusiasm and authenticity of the acting and were filled with admiration for the energy and success of the whole venture.
Derek Parr as Macbeth and Chris Moon as Banquo, Colin Guthrie as Malcolm and Michael Appleby as Macduff, were worthy of a London stage. I shall never forget his chilling portrayal of Macduff on hearing that his family had been murdered. Our resident witches, Joan Yates, Rachel Moon and Jayne Buckland were terrifyingly realistic, and Alison Reeve as Lady Macbeth was utterly convincing as were the boozy, lecherous porter, Ivan Moody and Michael Dixon's regal Duncan and Vic Harrington's Thane of Ross. The attack on Banquo scene was a wonderful cameo for Maria Giles as Fleance and Colin Gibbens and Joy Heywood as murderous rogues, while David Bird and Sue Gooch and Cristyn Williams had gentler roles as doctor and servants. It was a performance to celebrate, remember and look back on with a great deal of satisfaction.


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Run a search by name for anyone in Pecatonica, Illinois & get free white pages information instantly. Pecatonica, Illinois white page directory listings include full name, phone number and address.


text:
In The Footsteps of Wim Wenders — Berlin Like You've Never Seen Before
Travel Accounts
Berlin,Cinema,Travel,Wim_Wenders
Before moving here some 10 years ago, I used to think of Berlin as the city of angels Cassiel and Damiel, the characters of Wim Wenders' cult movie The Wings of Desire. In these 10 years, I have changed a lot — you know, life happens; while Berlin still projects the same two colors — The black and white of a timeless masterpiece.
The Wings of Desire [Der Himmel Über Berlin] was released in 1987, only two years before the fall of the Berlin Wall. Now in its fully restored version, with its slow scenes and poetic dialogues, the movie tells the story of a city that does not exist anymore.
But, if you carefully observe its frames, you may get a glimpse of Wim Wenders' treasure map — A map that will take you back to that timeless Berlin.
Let's discover it together.
As of October 2018, the C/O Berlin proposes a selection of 240 Polaroids for the temporary exhibition entitled: Wim Wenders. Instant Stories — check it out
International Congress Center and the Funkturm
Already in the first scenes of The Wings of Desire, you stumble upon two architectural pearls — The International Congress Center (ICC) and the Funkturm.
The Nord Messe / ICC station, with its beautiful red columns and round lamps, is the starting point of your adventure.
"Why am I me, and why not you?"
Designed by architects Ralf Schüler and Ursulina Schüler-Witteis, the ICC, with its 320 meters of lengths and 40 of height, is one of the largest convention centers in the world. Located in the rich neighborhood of Charlottenburg, the ICC hosts conferences, fairs, theatrical productions and concerts since 1979.
In addition to the film by Wim Wenders, the ICC is the protagonist of the musical The Apple, in which it appears as a futuristic concert hall.
The structure of the ICC, futuristic indeed, is definitely worth a visit.
Beyond the ICC, an old West Berlin radio tower rises majestically — it is the Berliner Funkturm or lange Lulatsch, the lanky lad. Built between 1924 and 1926 as an homage to the Eiffel Tower, it was initially designed by architect Heinrich Straumer as an antenna for radio transmissions but was then integrated with a restaurant as well as an observation point at a height of 125 meters.
Zoologischer Garten and the Maison de France
From the Nord Messe / ICC station, the U-Bahn line U2 takes you to Zoologischer Garten, the famous subway station of Christiane F. – Wir Kinder vom Bahnhof Zoo.
From there, you walk to Kurfürstendamm, the chic shopping boulevard of Berlin, also known as Ku'damm, to reach another gem that appears in one of the scenes of The Wings of Desire.
"Why am I here, and why not there?"
Sitting on a convertible car, Cassiel tells Damiel the story of a Soviet jet that crashed into the Spandau Lake twenty years before. Damiel stops him when he notices a couple dancing on the sidewalk. At this point, Damiel admits of being tired of his angelic timelessness and yearns for simple humanity.
In the background of the scene, you can spot the Maison de France, the Institute of French culture in Berlin. Art, theater, cinema, music, the cultural program offered by the Institute is rich and diverse.
Even just a short visit to the Maison de France hall is worth the walk.
Potsdamer Platz and the Staatsbibliothek
After enjoying Kurfürstendamm dining options and exclusive shops, you hop on the U2 train to Potsdamer Platz, one of the most characteristic city centers of Berlin.
Potsdamer Platz today has regained the magic charm of its past, with the renowned Sony Center, an imposing space that hosts blockbuster cinemas, shops, hotels, and restaurants.
If you have time to spare, the nearby Museum für Film und Fernsehen, the German film and television museum, is worth a visit.
Wim Wenders' Potsdamer Platz is an entirely different entity, an alien space lost in time — Still divided by the Wall, that Potsdamer Platz resembles a vast desert rather than the busy crossroads of a Capital.
In that desert, we get to know Homer, an old gentleman roaming around in search of the glorious Café Josty, once the meeting place of the flamboyant artists who used to live in the city, like the Brothers Grimm or Heinrich Heine.
"When did the time begin and when does space end?"
Within walking distance of Potsdamer Platz, you discover one of the most fascinating buildings depicted in The Wings of Desire — The Staatsbibliothek, Stabi for short, the National Library of Berlin.
There, Damiel and Cassiel hover over the desks and the stairs to listen to the thoughts of the people reading and consulting books, revealing to us the breathtaking details of the building design — Spectacular! I totally recommend a visit.
Just a few steps away from the library, the fine music lovers will recognize Hans Scharoun's Berliner Philharmonie — A concert hall with a perfect sound and home of the Berliner Philharmoniker, one of the most prestigious orchestras in the world.
The Victory Column
From the Berliner Philharmonie, take the public bus 200. At a price of a standard ticket, this bus line takes you to virtually any tourist attraction in Berlin Mitte. It is an excellent alternative to expensive tourist buses.
You get off at the Nord-Botschaften / Adenauer-Stiftung stop. There, Golden Elsa is waiting for you.
The Siegessäule, the Victory Column, is one of the major symbols of the city, together with the Fernsehturm (TV tower) and the Brandenburg Gate.
About 70 meters high, the Siegessäule was designed in 1864 by Heinrich Strack and erected in 1873 to celebrate the victory of the Prussians in the Prussian-Danish war. Initially placed in front of the Reichstag (the German Parliament — go visit its marvelous glass dome!), it was repositioned at the end of the 30's by the urbanists of the Nazi regime in the Straße des 17. Juni — The heart of the Tiergarten.
"I now know what no angel knows"
In one of the most representative scenes of The Wings of Desire, Damiel stands on the top of the Victory Column and looks at Berlin in all its magnificence.
Climb up the spiral stairs to the observation point of the statue. There and for a split second, with the wind hissing through the protection iron bars, you will feel like an angel flying over Berlin to catch the thoughts of its people.
Now you Know what the angels know
Berlin, I have realized it over the years, is a generous city that knows how to give it all, but never forgets. And in winter, during those gray days, so long that no reflections can be seen on the Fernsehturm, Berlin takes everything back.
It is this taking and giving, this pumping, gentle like a heartbeat, that makes Berlin alive. That makes my city eternal.
All photos in this post were taken by Sebastiano Lora
The cover photo and all quotes are from the movie The Wings of Desire
Do You Really Want To End It All? Be a Famous Writer First
Uncreative Writing — The Copy and Paste Literature of The Stealing Writer
"The Best Years of My Life" — Discover Galileo Galilei's Padua


The Artigiano Collection – Subway Ceramic Wall Tiles By Daltile. Inspired by the homes of southern Europe, Artigiano brings artisan appeal into any room. Its glossy, hand-painted appearance and irregular edges add to its rich, old-world look. Offered in seven earthy, neutral colors and two linear sizes, this resurgent design adds subtle charm to wall designs.
Artigiano - Florentine Gates Subway Ceramic Wall Tile 3" x 6"
Artigiano - Tremiti Sand Subway Ceramic Wall Tile 3" x 6"
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Artigiano - Tremiti Sand Subway Ceramic Wall Tile 3" x 12"
Artigiano - Florentine Gates 6" Side Ceramic Bullnose 3" x 6"
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Artigiano - Milan Arena 6" Side Ceramic Bullnose 3" x 6"
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Artigiano - Venice Statue 6" Side Ceramic Bullnose 3" x 6"


How difficult and what is the process to animate a pie chart in 3D? I suspect you have to build the pie with it's various sections/colors and use an animated alpha channel mapped to the geometry in (I suspect) the transparency setting. Am I on the right track? Anyone know of examples or tuts available with the set up?
"Animated" is a big range of possibilities. What exactly is the pie doing?
FWIW, flying wedges in is the EASIEST.
Good point. I thought the animated alpha would suggest what I was looking for (not really necessary for a flying wedge).
Example, A pie chart in perspective depicting three different percentages, 40%, 35% and 25%. The 40% wedge will be the base pie and is already visible. I want the 35% wedge to draw on followed by the 25% slice. Simple enough with mattes in 2D but to maintain the pie's thickness while the slices animate is where I'm unsure.
"Draw on". So, you want it to unfold?
Bryphii77 showed me how to do this: sadly my blog lapsed, 'cuz I did a whole article about it.
Basically, it's possible to make a gradient w.map that spans each part, one end of a wedge is 100%, the other zero.
Using dpkit's ROTATE (???? maybe MOVE) node, you can make each wedge unfold over time.
I've done animated alpha maps in the past, and it's a PITA.
Thanks I'll look into dpkit - sounds simple enough. Wouldn't happen to have that article somewhere else would you?
BTW, I like your tag line. Here's another (similar). "If you want peace - be peaceful."
"In order for evil to flourish, all that is required is for good men to do nothing." --Edward Burke.
I learned a lot from this tutorial, including how to use expressions. I think it is from LW forum poster Meatycheesyboy(?).


text:
Q: Collapse Tableview Sections in UITableview Can any one give me some advice or point me to any samples for how to achieve a collapsible UITableview sections effect in UITableView like accordian panel in web application?
Thanks

A: Apple provides some sample code in his documentation for making a section collapse:
Table View Animations and Gestures


text:
U.S. claims for unemployment aid hit lowest level since '69
The Labor Department says claims for jobless aid fell by 5,000 last week to 192,000, lowest since September 1969
U.S. claims for unemployment aid hit lowest level since '69 The Labor Department says claims for jobless aid fell by 5,000 last week to 192,000, lowest since September 1969 Check out this story on detroitnews.com: https://www.detroitnews.com/story/business/2019/04/18/unemployment-benefits/39361561/
Paul Wiseman, Associated Press Published 9:23 a.m. ET April 18, 2019 | Updated 9:33 a.m. ET April 18, 2019
The U.S. Capitol dome in Washington. The number of people applying for unemployment aid fell last week to its lowest level in nearly five decades, solid evidence that the job market is healthy and layoffs scarce. (Photo: Manuel Balce Ceneta / AP)
The number of Americans filing for unemployment benefits dropped to the lowest level in nearly half a century.
The Labor Department says claims for jobless aid fell by 5,000 last week to 192,000, lowest since September 1969. The four-week average, which is less volatile, dropped by 6,000 to 201,250, lowest since November 1969.
More: Michigan unemployment rate unchanged at 4% in March
Weekly claims have been at historically low levels – below 300,000 – for more than four years.
Unemployment claims are a proxy for layoffs. The low levels show that most American workers enjoy job security. The employment rate is 3.8%, the lowest in almost 50 years.
Read or Share this story: https://www.detroitnews.com/story/business/2019/04/18/unemployment-benefits/39361561/
Tesla cuts Model 3 price after tax credits shrink
FCA, GM warn their futures are at stake ahead of UAW talks
Senators want probe of faulty Ford transmissions
Forever 21 reportedly in financial trouble
First tenants to move into The Corner at former Tiger Stadium site


Service: Sunday Morning (48), Sunday Evening (43), Midweek Meeting (8), Hot Potato (3), Special event (1), Good Friday (1), Candlelit Carol Service (1).
Preached by Tim Gill on December 30, 2018 (Sunday Evening).
Preached by Lloyd Pritchard on December 30, 2018 (Sunday Morning).
Hebrews 2:5-18 (Part of the series).
Preached by Tim Gill on December 23, 2018 (Sunday Morning).
1 Thessalonians 5:12-28 (Part of the Thessalonians series).
Preached by Lloyd Pritchard on December 16, 2018 (Sunday Morning).
Preached by Tim Gill on December 2, 2018 (Sunday Evening).
1 Thessalonians 4:13-5:11 (Part of the Thessalonians series).
Preached by Lloyd Pritchard on December 2, 2018 (Sunday Morning).
Micah 6:1-16 (Part of the Micah series).
Preached by Tim Gill on November 25, 2018 (Sunday Evening).
1 Thessalonians 4:1-12 (Part of the Thessalonians series).
Preached by Lloyd Pritchard on November 25, 2018 (Sunday Morning).


text:
Тракторы Holt — это семейство тракторов, созданных компанией Holt Manufacturing Company, названной в честь Бенджамина Холта.

Гражданское применение
В промежутке между 1908 и 1913, 27 из 100 первых гусеничных тракторов Holt использовались во время работ над Лос-Анджелесским Акведуком, что послужило хорошим испытанием для этих машин.

Военное применение
Тракторы Holt применялись во время Первой мировой войны войсками Антанты в качестве артиллерийских тягачей, в том числе для 9,2-дюймовой гаубицы и 8-дюймовой гаубицы Mk V. Около 2000 тракторов Holt 75, 698 тракторов Holt 120 и 63 трактора Holt 60 использовались военными во время войны.

Так же трактор стал основой для многих первых танков, таких как французские Сен-Шамон, Шнейдер и немецкий A7V.

Технические характеристики
Как минимум 3 различных модели использовались военными: Holt 75, Holt 120 и, в меньшей степени, Holt 60.

Производство Holt 75 началось в 1913 году. Его бензиновый двигатель обеспечивал максимальную скорость чуть более 24 км/ч. В Британии компанией Ruston & Hornsby из Линкольна были произведены 442 экземпляра Holt 75, в дополнении к тем что производились в США. Производство Holt 75 продолжилось и после окончания войны, вплоть до 1924 года.

Holt 75 имел 120 лошадиных сил, обладал рулём румпельного типа, расположенным спереди. Вес составлял более 8 тонн. Трактор был разработан в связи с запросом военных на тяжёлый артиллерийский тягач. Прототип был изготовлен в 1914, а производство началось в 1915 году.

Holt 60, ограниченно применявшийся во время войны, был представлен в 1911 году.

Примечания

Литература
 Holt Tractors Photo Archive: An Album of Steam and Early Gas Tractors,

Ссылки

 Holt tractor models

Артиллерийские тягачи
Гусеничные тракторы

redpajama_set_name: RedPajamaWikipedia


text:
Home News You don't have to be a sports fan to become a...
You don't have to be a sports fan to become a fan of these athletes
By Juanice Gray, jgray@natchitochestimes.com
Did you know you do not have to be a sports fan to become a fan of the person that is the athlete? That is the lesson I'll learned as I met the La. Sports Hall of Fame inductees Thursday afternoon. As I heard their stories of their lives and their passions for education, passions for living life, passions for their teammates and players, I learned that although I do not follow their sport as a fan, I will now follow them as a fan of them as a person.
Being inducted into the Hall of Fame is the first rodeo cowboy, who at 92 had to be called in from his tractor in the field where he was cutting hay to be given the news. That is the caliber of person we're dealing with here. I also heard from an educator who said his greatest accomplishment would be the Education Hall of Fame because there is where he had the opportunity to touch more lives.
Then there is the mom who encourages her young daughter to participate in a variety of things from individual sports to team sports and the arts from piano to dance to not make her a better athlete, but to make her a better person.
How about the All-American football player who got misty eyed because he felt his whole team should've been inducted. He and one other player from his team were named All-Americans, but in his mind he and the other guy did not make the team, they were simply a part of it.
The eight athletes, writers and sportscasters being inducted were chosen from among 145 nominees.
Marie Gagnard with emcee Doug Ireland
Marie Gagnard-world class tennis judge
Gagnard got into tennis because one summer she and her sister were bored. Her mother wrote to The Town Talk and found out about a tennis camp. Emcee Doug Ireland, SIC at Northwestern State University, asked Gagnard if she ever was intimidated while calling a tennis match. "I taught public elementary school P.E., I did a stint in the army, not much intimidates me," she quipped. She likened dealing with schoolchildren and professional athletes saying, "They had similar issues."
Philip Timothy – sports and outdoors writer
Philip Timothy
Timothy has done everything in journalism from graphic design to team sports to outdoor sports. He said is first love is prep football but when he was "volun-told" at the Advertiser to write about the outdoors, his immediate reply was "yes. Who wouldn't love to get paid to hunt and fish?" Timothy had an integral part in establishing the Hall of Fame Museum. He was in a serious car crash that had him immobile for three months. During that time he began talking and planning. "I nudged it along. It became a part of my therapy," he said.
Dave Nitz – 45 years as sportscaster for LSU
Dave Nitz
Nitz said never say never in sports. After all his years, one would think he had seen it all, but at a game in Nebraska a play at home plate was a new experience. He said the play was called a "balk on the catcher" and the run counted. Nitz said he began looking through the rule book and learned a balk is "…delivers a pitch during a squeeze play or a steal of home, if the catcher or some other player steps on or in front of home plate without possession of the ball, or touches the batter or his bat. The ball is dead, the batter is awarded first base, the pitcher is charged with a balk, and the run scores."
"I've never seen it before or after," Nitz said. He said he doesn't know how his trademark phrase, "You gotta love it" got its start. "I just must have said it once and it stuck."
Teaberry Porter – rodeo cowboy
Teaberry Porter
At 92, he is the oldest athlete ever inducted into the La. SHOF. He said he went to LSU for a quarter and "got smart and quit." "I'm proud of being a cowboy," Porter said. "I've never been drunk, never drank a beer…I drove a school bus for 30 years and had a 450 John Deere run over me and lost my arm. I've had a life and have lived to see a cowboy in a sports hall of fame." Porter should be familiar, his face was on all the tags on Wrangler jeans for years. Ireland asked Porter what he thought of that publicity. "I'm proud of it and proud of what I got!" Porter said of being a lifelong cowboy, "I hope I leave more here than I take away."
Roger Cador – coach
Roger Cador
When Roger Cador walked in as coach of Southern, the baseball equipment would all fit in a shopping cart. "I called Baker, who I played with at the Braves and he said meet me in Atlanta. My wife and I drove there and when we came back it was with a U-Haul full of equipment. Sometimes you just have to ask for help. Don't be afraid to ask," he said. When he started, he had a $3,000 recruiting budget. When he left the program, there was still a $3,000 budget, but the program had vastly expanded. He said his philosophy is first, tell a true story and second, make good choices.
Max Fugler – football
Max Fugler
"My teammates are on that wall (of the museum)," he said as he became misty eyed. "To be associated with them, that is an honor. We were not a team, we were friends taking care of one another." Fugler was on the Ferriday team that won 54 consecutive games. Of 11 players, nine received college scholarships and two, including Fugler, were named All-Americans. He recalled one pro gam when he faced off with Heisman Trophy winner Texas A&M halfback John David Crow. "I tackled him and in one play he gained 14 yards – 10 of them were in my chest!" he laughed.
Danielle Scott – 5 time Olympian – volleyball
Danielle Scott
"The Hall of Fame is never something you work for, but it's great to be recognized for your work," she said. An athlete in volleyball, track and field and basketball, she said she landed in volleyball because of her respect for the teamwork atmosphere. "You can be powerful, yet graceful," she said. "In my first Olympics in '96, it was about getting into something bigger than you. When you are there and you're dressed in red, white and blue, it's about representing your team and your country." She credits her longevity in the sport to playing a variety of sports. "I never burned out because I love it."
Les Miles – coach
Les Miles
"When the guy on the field is willing to give everything he has for you at the risk of injury, I'm in their debt," he said. Miles has had an extensive career that included coaching at LSU but has also expanded into acting. He was treated to a party at home June 5, which also happened to be his wedding anniversary, with hundreds of family, friends, players and former players. "My wife said we'd be serving hamburgers and hot dogs. Always the planner I said, 'We made enough money to provide a decent meal!' " he laughed. "The men I coached really touched me last night." Ireland asked if he ever decided to stop coaching. "I never got out of coaching," Miles said. "It was very politely said that once you're on the other side of those doors, they'll be locked."
Matt Dunigan – football
Matt Dunnigan
"I learned to do the right thing, and sometimes the right thing isn't the easy thing. That is what football means to me," he said. He related how his football career began. "I was in the seventh grade and the ball went over my head. I picked it up and slung it back. The coach made me quarterback."
Charles Smith – basketball coach
"The teaching profession has changed since 1971, the kids have changed and the parents have really changed," he said. "I went about coaching like I did teaching trigonometry and calculus. On day one, students said it was too hard. On day two, I had to have figured out a way for them to get it and to help them learn. He said he will never forget being told once that "…the high school level is where you develop young men." He said that is one of the reasons he never moved to the college level, although he was approached to do so.
LaCapitol has been a sponsor of the Hall of Fame for 14 years. At left is Mary Ann Nowlin.
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AC Sparta Praha was one of 18 clubs from the Czech Republic that had teams playing during Gothia Innebandy Cup 2019. They participated with one team in Boys 16.
In addition to AC Sparta Praha, 27 other teams from 4 different countries played in Boys 16. They were divided into 5 different groups, whereof AC Sparta Praha could be found in Group 5 together with Carlshamns IBK Ci85, IBK Lund, Sandö IBK, Ajer IBK and Hovshaga AIF.
AC Sparta Praha continued to Playoff A after reaching 1:st place in Group 5. In the playoff they made it to 1/4 Final, but lost it against Panthers Praha with 3-4. In the Final, FBC Liberec won over FBC Aspen and became the winner of Playoff A in Boys 16.
AC Sparta Praha comes from Praha which lies approximately 870 km from Göteborg, where Gothia Innebandy Cup takes place. The area around Praha does also provide 17 additional clubs participating during Gothia Innebandy Cup 2019 (Among others: FBC Přerov, SK Florbal Benešov, FBC Liberec, FBC Dobruška, Prague Tigers, TJ Znojmo LAUFEN CZ, FBC Ceska Lipa, Z.F.K. AQM Petrovice, Tigers Jizni Mesto and 1. MVIL Ostrava).


text:
Q: Angular Material Dropdown with Router ( UI - Router ) when user clicks on the person it calls a form (form.html) using ui-router logic defined in app.js. I have 2 type of drop-down boxes, (1) using select tag and (2) using md-select tag. Pages works fine until i click on 2nd dropdown, which doesn't open the dropdown option window instead it freezes the page. I added code here in plunker however page routing doesn't work in plunker but you can reference the code.
index.html

form.html

 Normal DropDown

    <select ng-model="selectedName" ng-options="x for x in names">
    </select>

I have three elements in my list, you should be able to pick whichever you like

 Material DropDown

    <md-select onclick='console.log("clicked")' ng-model="selectedFilter" placeholder="Select a filter">                             <md-select-label>{{ selectedFilter.name }}</md-select-label>
        <md-option ng-value="opt" ng-repeat="opt in filters">{{ opt.name }}</md-option>
    </md-select>

app.js
var myApp = angular.module('myApp', [ 'ngAnimate', 'ngAria', 'ui.bootstrap', 'ngMaterial', 'ngMessages', 'ui.router' ]);

//routing
angular.module('myApp').config(function ($stateProvider){

    $stateProvider
        .state('form', {
        url:"/form",
            views:  {
                "listColumn": {

                  },
                "formColumn": {
                      templateUrl: "/form.html"
                  }
            }
        })
});

//dropdown
myApp.controller('myCtrl', function($scope) {
    //log
    console.log($scope.names);
    $scope.names = ["Emil", "Tobias", "Linus"];

    $scope.filters = [
            {
                value: 'mine',
                name: 'Assigned to me'
            },
            {
                value: 'undefined',
                name: 'Unassigned'
            },
            {
                value: 'all',
                name: 'All Tickets'
            },
            {
                value: 'new',
                name: 'New Tickets'
            }
        ];

    //log
    console.log($scope.filters);
    console.log($scope.selectedFilter);
});

http://plnkr.co/edit/SB7MUM44Ly01aWyL5M28?p=preview
View upon clicking person icon

Note: Dropdown for md-select doesn't load.
Thanks in advance

A: Changed .css and .js version to have the same and it fixed it.
angular-material.js ( v 1.0.6 )
angular-material.css ( v 1.0.6 )
Links:
<link rel="stylesheet" href="https://rawgit.com/angular/bower-material/master/angular-material.css">
-->


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