text:
\section{Introduction}

Lyman-alpha Emitters (LAE) are galaxies selected through strong Ly$\alpha$\ts\ts emission and are among the
most studied galaxy populations at high redshift. The use of narrow band filters over a wide area on
the sky has proven to be a very effective method to find galaxies up to $z\sim7$
\citep{iye2006,fontana2010,vanzella2011,rhoads2012,shibuya2012,schenker2012,ono2012}. The
possibility of finding LAEs from $z\sim1$  to $z\sim7$  shows that this type of galaxies can be
used to understand galaxy evolution over cosmic time.
It has been observed that the LAE fraction in UV selected galaxies increases with redshift up to
$z\sim6$ \citep{stark2010}, which is expected due to the decreasing dust content at higher
redshifts. Beyond $z\sim6$ it is expected that the LAE fraction decreases as the amount of neutral
Hydrogen (\ifmmode{{\rm H}{\rm \small I}}\else{H\ts {\scriptsize I}\ts}\fi) increases, due to the incomplete reionization of the Intergalactic Medium (IGM)
\citep{ota2008,stark2010,pentericci2011,ono2012,schenker2012}. This is consistent with the
comparatively low success rate of detection of Ly$\alpha$\ts\ts emission at $z\gtrsim 7$.

If Lyman-alpha photons from redshifts $z\geq7$ are absorbed by \ifmmode{{\rm H}{\rm \small I}}\else{H\ts {\scriptsize I}\ts}\fi\ts in the IGM
\citep{dayal2012}, it will be difficult to spectroscopically confirm the candidates at high redshift,
such as the candidate $z\sim12$ galaxy UDFj-39546284 discovered in the Hubble Space Telescope
(HST) Ultra Deep Field (UDF) \citep{bouwens2011a,ellis2013,brammer2013,capak2013}, and the
candidates found behind galaxy clusters at $z\sim9.6$ MACS1149-JD  and $\sim10.7$ MACS0647-JD\ts\ts
\citep{zheng2012,coe2013}.

Among the usual Interstellar medium (ISM) tracers at optical/UV wavelengths, the only line that has
been observed at $z>4$ in galaxies is Ly-alpha. The emission of Ly-alpha is complicated by its high
optical depth in the emission region and its escape through resonant scattering, by dust absorption,
and by the contribution from outflows.
Therefore direct constrains on the gas properties from the Ly-alpha line strength and shape are
difficult to derive. This motivates the exploration of alternative means to study the highest redshift
galaxies. Promising candidates include far-infrared fine structure emission lines, e.g., \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi
($^2$P$_{3/2}$ $\rightarrow$ $^2$P$_{1/2}$) at $157.74$ $\mu$m, which is not affected by the
increasingly neutral IGM at $z>7$ and can account for up to $1\%$ of the total infrared luminosity
in some galaxies, especially in those with low luminosity and metallicity
\citep{crawford1985,stacey1991,israel1996,madden1997}.

The \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line  traces photo-dissociation (a.k.a. photon-dominated) regions (PDRs), as well as diffuse
\ifmmode{{\rm H}{\rm \small I}}\else{H\ts {\scriptsize I}\ts}\fi\ts and \ifmmode{{\rm H}{\rm \small II}}\else{H\ts {\scriptsize II}\ts}\fi \ts  regions. In PDRs, the far-UV radiation produced by OB stars heats the surface
layers of molecular clouds, which cool preferentially  through \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission. It has been observed
that most of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission in IR-bright galaxies is coming from PDRs, and that the PDR gas mass
fraction can be up to $50\%$ in starbursts like M82 \citep{crawford1985}.

Modeling of FIR emission lines observed in starburst galaxies showed that at least 70\% of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi
emission is produced in PDRs \citep{carral1994,lord1996,colbert1999}. In the low-metallicity
system Haro 11, on the other hand, at least 50\% of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission arises from a more diffuse,
extended ionized medium \citep{cormier2012}. The different conditions in which the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission
is produced, and the direct or indirect relation of these conditions with the star formation process,
suggest that  \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission should be a good tracer of the global galactic star formation activity
\citep{delooze2011}, at least for galaxies with low $T_{\rm dust}$ or low
$\Sigma_{\rm IR}=L_{\rm IR}/\pi r^{2}_{\rm mid-IR}$ \citep{diaz-santos2013}. \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi is found to be
the strongest emission line, stronger than CO, and thus is the most promising tracer of the dense,
star forming regions in distant galaxies where \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi can be detected with ground-based telescopes
due to the redshift into observable atmospheric windows.

In the past years, the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi 158 $\mu$m emission line has been established as a promising
observable in high-redshift galaxies \citep{maiolino2005,
iono2006,maiolino2009,walter2009,hailey-dunsheath2010,stacey2010,ivison2010,wagg2010,
cox2011,debreuck2011,valtchanov2011,gallerani2012,venemans2012,wagg2012,walter2012a,carilli2013,wang2013,willott2013,riechers2013}.
Most of the high-z detections were for infrared-luminous starbursts, many of which also show signatures of AGN. See the review by \cite{carilli_walter2013} for more details.

With star formation rates of a few tens $\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi \rm{yr}^{-1}$, based on the Ly$\alpha$\ts\ts and UV continuum emission, LAEs are classified as ``normal''
star forming galaxies. Different studies claim that LAEs are young, dust free,
starbursting galaxies, supported by UV observations \citep{gawiser2006,finkelstein2007,lai2008}. Recent MIR detection
of LAEs at $z\sim2.5$ and $z<0.3$ show that a significant fraction of the star formation
in these galaxies is strongly obscured by dust \citep{oteo2012a,oteo2012b}. Thus, LAEs are promising targets for the
detection of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi at high redshift.

Previous attempts to detect \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi in a small sample of LAEs at $z\sim6.6$ were unsuccessful
 \citep{walter2012,kanekar2013,ouchi2013}.

Here we present the result of a search for \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi in three LAEs at $z>6.5$ and in
a lensed galaxy at $z\sim11$. In Sect. 2 we describe the target selection and
observations. The data is shown in Sect. 3 together with some implications
and analysis in Sect. 4. A summary of the paper is presented in Sect. 5.
Throughout this paper we use a $\Lambda$-Cold Dark Matter cosmology with
H$_{0}$ = 70 km s$^{-1}$ Mpc$^{-1}$, $\Omega_{\Lambda}=0.7$ and
$\Omega_{\rm m}=0.3$.

\section{Observations}
\subsection{Source Selection}
The three Lyman-$\alpha$ emitters targeted in this study were discovered in the Subaru Deep Field (SDF).
Two of the LAEs observed belong to the sample of LAEs at
$z\sim6.6$ discovered by \cite{taniguchi2005}.
The targets are the brightest LAEs (sources 3 and 4 in their catalog) and
have a narrow and bright Lyman-$\alpha$ emission line.
The third LAE (IOK-1) was discovered at $z\sim 7$ by \cite{iye2006}. It is one of the
brightest and most distant LAEs known to date.

The fourth target, MACS0647-JD, is a lensed Lyman-break galaxy (LBG)
discovered behind the galaxy cluster MACSJ0647.7+7015 at $z=0.591$
\citep{coe2013}. The galaxy was discovered as a J-Dropout galaxy lensed
into 3 magnified images  as part of The Cluster Lensing And Supernova
survey with Hubble (CLASH) \citep{postman2012}. The three images of
the galaxy MACS0647-JD1, MACS0647-JD2 and MACS0647-JD3, have a
magnification of $\sim$8,$\sim$7 and $\sim$2 respectively. The photometric
redshift of the galaxy is $10.7^{+0.6}_{-0.4}$ (95\% confidence limits).
This is one of the highest redshift galaxy candidates known to date.

\subsection{CARMA Observations}
Observations of the three $z\sim6.5-7$ LAEs were carried out using the Combined Array for Research in
Millimeter-wave Astronomy (CARMA) between 2008 July and 2010 July.
The array configurations used were the most compact, D and E, to minimize phase decoherence and maximize point source sensitivity.
The \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line has a rest frequency of 1900.54 GHz (157.74 $\mu$m). For
the redshifts of the targets, the line is shifted to the 1 mm band. The receivers
were tuned to a  frequency $\sim$150
\ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi bluer than the expected frequency from the redshift
determined by the peak of the Lyman-$\alpha$ line. This is for taking into account
the possible absorption by the IGM in the Lyman-$\alpha$ line.
The setups provide an instantaneous bandwidth of $\sim1.5$ GHz ($\sim 1800 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi$) with a
spectral resolution of 31.25 MHz ($\sim37-39$ \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi).

The observations were processed using MIRIAD \citep{sault1995}. The absolute
flux calibrators used  are 3C84, MWC349, 3C273 and Mars, the latter being
the most used. As passband calibrators the QSOs 3C273, 3C345
and 0854+201 were used. As gain calibrator the QSO 1310+323 was used.
The time on source for IOK-1 was 58.5 hours, for SDF J132415.7+273058\ts\ts was 15.9 hours and for SDF J132408.3+271543\ts\ts 4.6 hours.
The final cubes were made using natural weighting to maximize point
source sensitivity. The observations resulted in the following beamsizes: IOK-1:
$1.86" \times 1.33"$, PA$=-0.34^{\circ}$, SDF J132415.7+273058:
$1.92" \times 1.56"$, PA$=83.45^{\circ}$, SDF J132408.3+271543:
$2.54" \times 2.01"$, PA$=88.02^{\circ}$ (all targets: D and E configurations).
For D configuration the minimum baseline is 11 meters and the maximum is 150 meters.
For E configuration the minimum baseline is 8 meters and the maximum is 66 meters.
Table \ref{tab:table1} summarizes the sensitivities reached for the observations of the LAEs.

\subsection{PdBI Observations}
All MACS0647-JD\ts\ts observations were carried out in 2012 November as part of a DDT (Director's
Discretionary Time) program with the Plateau de Bure Interferometer (PdBI). The
target was observed with 4 WideX frequency setups (3.6 GHz bandwidth each), covering 80\%
of the photometric redshift range ($z=10.1-11.1$). Two of the three lensed images (JD1 and JD2) are within $18"$ of each other and
they were covered in a common 2 mm pointing.
The absolute flux calibrators used  are MWC349, 2200+420, 3C279 and 0716+714. As gain calibrator the QSO 0716+714 was used.
The total on source time for all tunings was 7.4 hours (6-antennas equivalent). The observations were processed  using GILDAS.
The beamsize of the observations is the following: MACS0647-JD\ts\ts: $2.10" \times 1.76"$, PA$=102.0^{\circ}$ (C configuration).
For C configuration the minimum baseline is 22 meters and the maximum is 184 meters.
Table \ref{tab:table2} summarizes the sensitivity reached for the observations of MACS0647-JD\ts\ts.

\section{Results}
\begin{deluxetable*}{ccccccccccc}
\tabletypesize{\scriptsize}
\tablecaption{Summary of Observations and Results for the LAEs\label{tab:table1}}
\tablehead{
\colhead{source} & \colhead{RA} & \colhead{DEC}  & \colhead{z\tablenotemark{a}} & \colhead{$\nu_{\rm obs}$\tablenotemark{b}} & \colhead{$\sigma_{\rm cont}$\tablenotemark{c}} & \colhead{$\sigma_{\rm line}$\tablenotemark{d}}  & \colhead{L$_{\rm [CII]}$\tablenotemark{e}} & \colhead{L$_{\rm IR, CMB}^{\rm N6946}$\tablenotemark{f}} & \colhead{SFR$_{\rm dust, CMB}$\tablenotemark{g}} & \colhead{SFR$_{\rm UV}$\tablenotemark{h}}\\
\colhead{}& \colhead{J2000.0}  & \colhead{J2000.0}&  \colhead{}   & \colhead{GHz} & \colhead{mJy\,b$^{-1}$}   &  \colhead{mJy\,b$^{-1}$} &  \colhead{10$^8$\,L$_{\odot}$}  &  \colhead{10$^{11}$\,L$_{\odot}$}& \colhead{M$_{\odot}$\,yr$^{-1}$} & \colhead{M$_{\odot}$\,yr$^{-1}$ }
}
\startdata
IOK--1& 13:23:59.80 & +27:24:56.0  & 6.965     & 238.881        & 0.19  & 1.17  & $<$2.05 & $<$6.34 &  $<$109.1 & $\sim$24  \\
SDF J132415.7 & 13:24:15.70 & +27:30:58.0  & 6.541     & 252.154        & 0.37  & 2.82  & $<$4.52 & $<$10.3 &  $<$177.2 & $\sim$34  \\
SDF J132408.3 & 13:24:08.30 & +27:15:43.0  & 6.554     & 251.594        & 0.75  & 5.67  & $<$10.56 & $<$21.0 &  $<$360.9 & $\sim$15
\enddata
\tablecomments{All luminosities upper limits are 3\,$\sigma$.}
\tablenotetext{a}{References: IOK--1:\cite{iye2006,ono2012} --SDF J132415.7+273058\ts\ts and SDF J132408.3+271543\ts\ts: \cite{taniguchi2005}}
\tablenotetext{b}{Observing Frequencies; tuned $\sim$125\,MHz blueward of the Ly--$\alpha$ redshifts for all targets.}
\tablenotetext{c}{1$\sigma$ continuum sensitivity at 158$\mu$m rest wavelength.}
\tablenotetext{d}{1$\sigma$ \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi\ line sensitivity over a channel width of 50 km\,s$^{-1}$.}
\tablenotetext{e}{3$\sigma$ \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi\ luminosity limit over a channel width of 50 km\,s$^{-1}$ assuming $L_{\rm line} = 1.04 \times 10^{-3} \, I_{\rm line} \, \nu_{\rm rest} (1+z)^{-1}\, D_{\rm L}^{2}$, where the line luminosity, $L_{\rm line}$, is measured in $L_\odot$; the velocity integrated flux, $I_{\rm line}$=$S_{\rm line}\, \Delta v$, in Jy\,\ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi; the rest frequency, $\nu_{\rm rest} = \nu_{\rm obs} (1+z)$, in GHz; and the luminosity distance, $D_{\rm L}$, in Mpc. (e.g. \cite{solomon1992}}
\tablenotetext{f}{3$\sigma$ limit based on the SED of NGC 6946 and including the effect of the CMB.}
\tablenotetext{g}{3$\sigma$ limit based on L$_{\rm IR}^{\rm N6946}$ including the effect of the CMB.}
\tablenotetext{h}{UV--based SFR from \cite{jiang2013}}
\end{deluxetable*}
\begin{center}
\begin{deluxetable}{lc}
\tabletypesize{\scriptsize}
\tablecaption{Summary of Observations and Results for MACS0647JD\label{tab:table2}}
\tablewidth{0pt}
\tablehead{
\colhead{Parameter} & \colhead{MACS0647-JD1, JD2}
}
\startdata
Coordinates (J2000) JD1          & 06:47:55.731,+70:14:35.76	\\
Coordinates (J2000) JD2          & 06:47:53.112,+70:14:22.94	\\
$\mu$ (JD1+JD2)						& $\sim15$									\\
Redshift  									& $10.7^{+0.6}_{-0.4}$				\\
UV SFR										& $\sim 1$ [M$_{\odot}$yr$^{-1}$]\\
$\nu$									    & 156.7-171.1 [GHz]					\\
$\sigma_{\rm cont}$ \tablenotemark{a}	    			& 0.17 mJy\,b$^{-1}$									\\
$\sigma_{\rm line}$ (Setup A)\tablenotemark{b}	& 3.31 mJy\,b$^{-1}$								\\
$\sigma_{\rm line}$ (Setup B)\tablenotemark{b}		& 4.12 mJy\,b$^{-1}$										\\
$\sigma_{\rm line}$ (Setup C)\tablenotemark{b}		& 3.19 mJy\,b$^{-1}$								\\
$\sigma_{\rm line}$ (Setup D)\tablenotemark{b}		& 6.42 mJy\,b$^{-1}$									\\
$L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}$ (Setup C)\tablenotemark{c}					& $<6.78\times10^{7}\times(\mu/15)^{-1}[\ifmmode{{\rm L}_{\odot}}\else{L$_{\odot}$\ts}\fi]$		\\
$L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}$ (Setup D)\tablenotemark{c}					& $<1.36\times10^{8}\times(\mu/15)^{-1}[\ifmmode{{\rm L}_{\odot}}\else{L$_{\odot}$\ts}\fi]$		\\
L$_{\rm IR}^{\rm N6946,}$\tablenotemark{d} (Corrected CMB)					& $<1.65\times10^{11}\times(\mu/15)^{-1}[\ifmmode{{\rm L}_{\odot}}\else{L$_{\odot}$\ts}\fi]$	\\
SFR ($L_{\rm IR}$) (Corrected CMB)\tablenotemark{e}					& $<28\times(\mu/15)^{-1}$ [M$_{\odot}$yr$^{-1}$]	\\
SFR ($L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}$) (Setup C)\tablenotemark{f}					& $<5\times(\mu/15)^{-1}$ [M$_{\odot}$yr$^{-1}$]	\\
SFR ($L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}$) (Setup D)\tablenotemark{f}					& $<9\times(\mu/15)^{-1}$ [M$_{\odot}$yr$^{-1}$]
\enddata
\tablecomments{All luminosities upper limits are 3\,$\sigma$.\\References: Coordinates,
magnification, redshift and UV-SFR from Coe et al. 2013.\\All the luminosities and SFR are corrected by  magnification.}
\tablenotetext{a}{1$\sigma$ continuum sensitivity at 158$\mu$m rest wavelength.}
\tablenotetext{b}{1$\sigma$ \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi\ line sensitivity over a channel width of 50\,km\,s$^{-1}$.}
\tablenotetext{c}{3$\sigma$ \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi\ luminosity limit over a channel width of 50\,km\,s$^{-1}$ as in Tab. \ref{tab:table1}. The two results correspond to the most sensitive and the least sensitive setups. }
\tablenotetext{d}{3$\sigma$ limit based on the SED of NGC 6946 and including the effect of the CMB.}
\tablenotetext{e}{3$\sigma$ limit based on L$_{\rm IR}^{\rm N6946}$ including the effect of the CMB.}
\tablenotetext{f}{Based on the De Looze et al., 2011 $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}-SFR$ relation.  The two results correspond to the most sensitive and the lest sensitive setups.}
\end{deluxetable}
\end{center}
\begin{figure}
\epsscale{1.2}
\plotone{IOK_1_50km_s.eps}
\plotone{SDF_1_50km_s.eps}
\plotone{SDF_A_50km_s.eps}
\caption{Spectra of the LAEs with a  velocity resolution of 50 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi. The relative velocities are with respect to the frequency expected
for the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line including absorption by the IGM (150 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi to the blue of $z_{\rm Ly\alpha}$). The redshifts of the target are z=6.965 for IOK-1, z=6.541 for SDF J132415.7+273058\ts\ts and z=6.554 for SDF J132408.3+271543\ts\ts. \label{fig:spectraLAEs}}
\end{figure}
\begin{figure*}
\epsscale{1.2}
\plotone{MACS0647JD_spec.eps}
\caption{Spectrum of MACS0647-JD\ts\ts. The spectrum shows the added fluxes measured on the positions of the two lensed images JD1 and JD2 (combined magnification $\mu\sim15$). The spectra of the two images were corrected by the primary beam pattern before combination.
The 4 setups are plotted in different colors, blue, red, green and orange the colors for the setups A, B, C and D respectively.
The error bars correspond to the quadrature of the errors of the individual measurement of the fluxes for JD1 and JD2 in each frequency channel.
For display purposes, the spectrum is sampled at a channel resolution of 200 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi, but the search of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line as well as the analysis was made with the
spectrum sampled to 50 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi.
   \label{fig:specLBG}}
\end{figure*}
\begin{figure*}
\epsscale{1.2}
\plotone{continuum_carma.eps}
\caption{Rest-frame 158 $\mu m$ continuum maps of the LAEs. Each contour level represents $1\sigma$ steps ($\pm1\sigma$ levels are not shown). Solid contours are positive signal
and dashed contour are negative signals. The $1\sigma$ levels are 0.75 $\rm{mJy}\ts\rm{beam}^{-1}$ for SDF J132408.3+271543\ts\ts, 0.37 $\rm{mJy}\ts\rm{beam}^{-1}$ for SDF J132415.7+273058\ts\ts and 0.19 $\rm{mJy}\ts\rm{beam}^{-1}$ for IOK-1.
The blue crosses represent the position of each LAE as given in Tab. \ref{tab:table1}. \label{fig:contCarma}}
\end{figure*}
\begin{figure}
\epsscale{1.2}
\plotone{cont_MACS0647JD.eps}
\caption{Continuum map of the field of MACS0647-JD\ts\ts.  Each contour level represents $1\sigma$ steps ($\pm1\sigma$ levels are not shown). Solid contours are positive signal
and dashed contour are negative signals. The $1\sigma$ level is 93 $\mu\rm{mJy}\ts\rm{beam}^{-1}$. The blue plus signs represent the positions of the
two lensed images MACS0647-JD1 and MACS0647-JD2 as given in Tab. \ref{tab:table2}.
\label{fig:contLBG}}
\end{figure}
\subsection{Line Emission}

The spectra of the three $z\sim6.5-7$ LAEs are presented in Fig. \ref{fig:spectraLAEs} and the spectrum of MACS0647-JD\ts\ts is shown in Fig.\ref{fig:specLBG}.
No significant emission is detected at the redshifted line frequencies or close to them.
The observations were sampled to a channel resolution of 50 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi similar to
the expected FWHM of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission line  (see Sect. \ref{sec:widthline}).
We use our non-detections to put constrains on the luminosities of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi lines
for all targets. The results for the LAEs can be seen in the Table \ref{tab:table1}
and for the MACS0647-JD\ts\ts in Table \ref{tab:table2}. The upper limits were estimated assuming that the sources were unresolved. For MACS0647-JD\ts\ts the spectra of the two images were
corrected by the primary beam pattern before combination.
The \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi luminosities were estimated assuming that the velocity integrated flux
of the line is $I_{\rm line}$=$S_{\rm line}\, \Delta v$, with $S_{\rm line}$ being 3 times the r.m.s.
of the 50 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi channel and $\Delta v=50\ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi$ the range in velocity (details on Tab. \ref{tab:table1} notes).
Using  $3\sigma$ over a 50 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi channel to estimate the upper limit in the luminosities can result in a underestimation.
We point out that for a  more conservative estimation the luminosities should be multiplied by a factor 2. (i.e. $3\sigma$ over
200 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi channel). Assuming a channel width of 200 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi, our IOK-1 \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi limit is $\sim10\%$ deeper than the
previous PdBI limit \citep{walter2012}.

\subsection{Continuum Emission}
No continuum emission is detected in our observations of the three LAEs and
the $z\sim 11$ LBG. The sensitivity reached for the continuum observations is
given in the Tab. \ref{tab:table1} for the LAEs and a continuum map for the three LAEs
is shown in Fig. \ref{fig:contCarma}.
The results for the MACS0647-JD\ts\ts are given in Tab. \ref{tab:table2} and the continuum
map is shown in Fig. \ref{fig:contLBG}.
In Sect. \ref{sec:cmbeffects} we discuss how the CMB affects our continuum observations
and in Sect. \ref{sec:sed} we use our continuum measurements to constrain the nature of our targets.

\begin{figure}
\epsscale{1.2}
\plotone{SED_iok1.eps}
\plotone{SED_macs0647JD.eps}
\caption{{\it Top:} Spectral energy distribution of IOK-1. The photometric points correspond to those
measured by \cite{iye2006,ota2010,cai2011,ono2012}. The red triangle corresponds to the $3\sigma$ upper limit
given by the CARMA observations. The colored lines correspond to the SEDs of local galaxies shifted to the redshift
of IOK-1 and scaled to the observations in the UV band. The dashed lines correspond to the observed SED of the local galaxies after the effects
of the CMB on the observations are taken into account.
{\it Bottom:} Spectral energy distribution of MACS0647-JD.  The photometric points correspond to those presented by \cite{coe2013}.
The SED of the galaxies follow the same prescription as in the upper panel. The red triangle corresponds to the $3\sigma$ upper limit calculated as the quadrature of the errors of the individual fluxes of JD1 and JD2, in the same way as the errors presented by \cite{coe2013}. The $1\sigma$ photometric uncertainty of the observations is 0.093 mJy, and the error of the added fluxes is 0.13 mJy.
\label{fig:SEDs}}
\end{figure}

\section{Discussion}

\subsection{Width of the [CII] emission line.}
\label{sec:widthline}
Previous studies have presented the non-detection of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi \citep{walter2012,
ouchi2013} with a channel resolution of 200 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi, a choice motivated by the width
of the Ly$\alpha$\ts\ts emission line. We argue that recent observations
and models of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi in LAEs suggest that the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line could be
narrower that the previously assumed value.

\subsubsection{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi detection on a LAE z=4.7.}

In support of a the narrow emission line is the detection of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi
in a LAE at $z=4.7$ (Ly$\alpha$\ts\ts-1) with ALMA \citep{carilli2013}. The FWHM of the emission
line is 56 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi, which is one order of magnitude narrower than the width
of the Ly$\alpha$\ts\ts emission line of $\sim 1100$ \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi of the same source \citep{petitjean1996,ohyama2004}.
Despite of the LAE being at a separation of 2.3$''$ ($\sim 15$ kpc) to the quasar
BRI 1202-0725, there is no evidence for a significant influence of the quasar on the properties of the LAE from the
observations. \cite{carilli2013} tried to model the emission of the LAE taking into
account the radiation coming from the luminous nearby quasar. All the models
that reproduce the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi and Ly$\alpha$\ts\ts luminosities predict higher luminosities for
other UV lines that are not detected \citep{ohyama2004}.
Given this results, they conclude that the quasar is unlikely the source of heating
and ionization in the LAE.

Based on deep, spatially resolved optical spectroscopy of the LAE,
\cite{ohyama2004} argue that the LAE is likely the composition of a normal
star-forming galaxy and an extended nebula with violent kinematic status.
This nebula emission would produce a broadening of the Ly$\alpha$\ts\ts emission. This nebula
can be explained, at least in a qualitative way, as a superwind caused
by the supernovae explosion of  OB stars in the late phase of the evolution of a starburst.

In conclusion, this LAE is not intrinsically different from the general population of
LAE. The \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi detection in this LAE can thus be used as a reference for
\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi searches in other LAEs at high redshift.

\subsubsection{Himiko simulations.}
Simulations also suggest narrow \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission lines at high redshift for
LAEs. \cite{vallini2013} combine a high resolution cosmological simulation with a
sub-grid multi-phase model of the interstellar medium to simulate the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission
in a halo similar to the LAE Himiko at $z=6.6$. They find that 95\% of the
\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission is generated in the Cold Neutral Medium (CNM), mainly in
clumps of individual size $\leq 3$ kpc. They present a spectrum for the simulated
\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission, where the FWHM of the main peak is $\sim 50$ \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi, very similar
to the 56 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi of the LAE at z=4.7. This suggests that the width of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line is
to first order determined by the gravitational potential of the clumps. The \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission
produced in the CNM follows the gravitational potential of the clumps, resulting in narrow
emission lines associated with each clumps. An ensemble of emitting clumps
moving through the galaxy following the potential of the galaxy could combine and produce a broader line. Such behavior
is not observed in the simulations, where just a small number of clumps dominate the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission.

We conclude that the adopted width of $\sim 50$ \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi for the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line in LAEs agrees
with recent observations and simulations. Nevertheless, we do not discard the possibility of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi lines being
broader than our assumption, but that the occurrence of unusually narrow lines in this population appears
plausible.

\subsection{CMB effects.}
\label{sec:cmbeffects}
The Cosmic Microwave Background Radiation (CMB) emits as a black body with a temperature of
 \hbox{$T_\mathrm{CMB}^{\,z=0}$}$ =2.7$ K. The temperature of the CMB increases linearly with ($1+z$), becoming an
important factor to take into account for observations of objects at high redshift. \cite{dacunha2013}
showed the effect of the CMB on observations of high-redshift galaxies. Here we will follow the
prescription formulated by \cite{dacunha2013} to take into account the effects of the CMB in the
continuum observations of galaxies at high redshift in the mm and sub-mm. We will apply this
prescription to the SED of the local galaxies, as if they would be observed at a given redshift z.

The templates that we use are those presented by  \cite{silva1998} for the galaxies Arp 220, M82,
M51 and NGC 6946. For the galaxies assume cold dust with temperature \hbox{$T_\mathrm{dust}^{\,z=0}$}\ and an emissivity
index $\beta$. For Arp 220 we used $\hbox{$T_\mathrm{dust}^{\,z=0}$} =66.7$ K and $\beta=1.86$ \citep{rangwala2011}, for
M82 $\hbox{$T_\mathrm{dust}^{\,z=0}$} =48$ K and $\beta=1$ \citep{colbert1999}, for M51 $\hbox{$T_\mathrm{dust}^{\,z=0}$} =24.9$ K
and $\beta=2$ \citep{mentuchcooper2012} and for NGC 6946 we used $\hbox{$T_\mathrm{dust}^{\,z=0}$} =26$ K and
$\beta=1.5$ \citep{skibba2011}.
At a given redshift the CMB contributes to the dust heating such that the equilibrium temperature is:

\begin{equation}
\hbox{$T_\mathrm{dust}$}(z) = \Big( (\hbox{$T_\mathrm{dust}^{\,z=0}$})^{4+\beta} + (\hbox{$T_\mathrm{CMB}^{\,z=0}$})^{4+\beta} \big[(1+z)^{4+\beta} - 1 \big] \Big) ^{\frac{1}{4+\beta}}\,.
\label{tdustz}
\end{equation}
$\hbox{$T_\mathrm{dust}^{\,z=0}$}$ is a measurement of the mean dust temperature as determined by a modified
blackbody fit to an observed galaxy IR SED at $z = 0$, representing the total IR luminosity of the galaxy. As a representative fit, this is equally applicable to both optically thin galaxies and optically thick as in Arp 220. So long as the galaxy is transparent to the CMB radiation (true for even Arp 220), Eq. 1 holds.
The additional heating by the CMB affects the SEDs such that the peak of the emission is shifted to a shorter wavelength and
the total luminosity associated to the cold dust is higher by $[\hbox{$T_\mathrm{dust}$}(z)/\hbox{$T_\mathrm{dust}^{\,z=0}$}]^{(4+\beta)}$.
We need to modify the intrinsic SED of the galaxies to include this new $\hbox{$T_\mathrm{dust}$}(z)$. The flux density
depends on the black body radiation for the given temperature,

\begin{equation}
F_{\nu/(1+z)}\propto B_{\nu}(T_{dust}(z)),
\end{equation}

To include $\hbox{$T_\mathrm{dust}$}(z)$ we have to apply the following factor to convert the intrinsic SED flux density to the emission associated with the new temperature $F^{*}_{\nu/(1+z)}$.

\begin{equation}
F^{*}_{\nu/(1+z)}=F^{\rm int}_{\nu/(1+z)}\times \frac{B_{\nu}(\hbox{$T_\mathrm{dust}$}(z))}{B_{\nu}(\hbox{$T_\mathrm{dust}^{\,z=0}$})}.
\end{equation}

This factor will only apply to the part of the SED that correspond to the emission of the cold dust. To accomplish this, we scale a modified black body (MBB) to the peak of the FIR emission of the SED at $\hbox{$T_\mathrm{dust}^{\,z=0}$}$, and then use this MBB emission to estimate the ratio ($R_\nu$) of emission associated with the cold dust at a given frequency,

\begin{equation}
R_{\nu}	=	\frac{K\nu^{\beta}B_{\nu}(\hbox{$T_\mathrm{dust}^{\,z=0}$})}{F^{\rm int}_{\nu}},
\end{equation}
where $K$ is just the scaling factor. The flux density associated to the new temperature of the cold dust will be:

\begin{equation}
F^{*}_{\nu/(1+z)}=M_{\nu}\times F^{\rm int}_{\nu/(1+z)}
\end{equation}

with

\begin{equation}
M_{\nu}=\left[\left(1-R_{\nu}	\right)+R_{\nu}	\times \frac{B_{\nu}(\hbox{$T_\mathrm{dust}$}(z))}{B_{\nu}(\hbox{$T_\mathrm{dust}^{\,z=0}$})}\right].
\end{equation}

Finally, following \cite{dacunha2013}, we have to take into account the effect of the CMB as an observing background. For this we have to multiply the flux associated
with $\hbox{$T_\mathrm{dust}$}(z)$ by $C_{\nu}$,

\begin{equation}
C_{\nu}=\left[1-\frac{B_{\nu}(\hbox{$T_\mathrm{CMB}$}(z))}{B_{\nu}(\hbox{$T_\mathrm{dust}$}(z))}\right],
\end{equation}

resulting in the flux observed of the galaxies as:

\begin{equation}
F^{\rm obs}_{\nu/(1+z)}=C_{\nu}\times M_{\nu}\times F^{\rm int}_{\nu/(1+z)},
\end{equation}

with $C_{\nu}\times M_{\nu}$ representing the effect of the CMB in the observations at a given frequency.
The same corrections are derived when an optically thick emission is assumed, as in the case of Arp 220.

As we can see in Fig. \ref{fig:SEDs}, the effect of the CMB decreases the observable flux density at 2 mm by up to a factor of $5\times$ (in the case of M51) for the galaxy at $z\sim 11$, when
the temperature of the CMB is higher, as expected. Also, the effect is higher for galaxies with a lower temperature of the cold dust.
Galaxies with temperature of order of 25-30 K are more affected than those with temperature of 40-50 K.
The CMB effects will be important for estimations of the flux densities of these type of galaxies in the continuum and for
the correct interpretation of the observations.

The CMB effects on the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line observations are similar to those on the continuum.
The flux of an emission line observed against the CMB
is:

\begin{equation}
\label{eq:lineflux_aCMB}
\frac{S^{\rm obs}_{\nu/(1+z)}}{S^{\rm int}_{\nu/(1+z)}}=\left[1-\frac{B_{\nu}(\hbox{$T_\mathrm{CMB}$}(z))}{B_{\nu}(T_{\rm exc})}\right],
\end{equation}

with $T_{\rm exc}$ being the excitation temperature of the transition.
For the case of local thermal equilibrium (LTE), when collisions dominate the excitation of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line, the excitation temperature of the transition
is equal to the kinetic temperature of the gas ($T_{\rm kin}$). The kinetic temperature varies for the
different \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission regions. Gas temperatures within PDRs are typically  $T\sim100-500$ K \citep{stacey2010},
for the CNM  $T\approx 250$ K, for the WNM $T\approx 5000$ K and for the ionized medium $T\approx 8000$ K\citep{vallini2013}.
Since the CMB temperature at $z=6.5-11$ is much lower than the gas temperature of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emitting region, it will not contribute significantly to the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi excitation, but must be taken into account as the background against which the line flux is measured. In most of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission regions, the temperatures
are so high that the observed flux of the line against the CMB is similar to the intrinsic flux ($S^{\rm obs}_{\nu/(1+z)}/S^{\rm int}_{\nu/(1+z)}\approx 1$). For the extreme case where all the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission is being produced in PDRs with temperature of 100 K in a galaxy at $z=11$, the
observed flux (using Eq. \ref{eq:lineflux_aCMB}) would be 90\% of the intrinsic flux.
We found this case very unlikely, since in low redshift galaxies the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission produced in PDRs is 50-70\% of the total \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi luminosity and the gas temperatures associated to the PDRs are higher \citep{crawford1985,carral1994,lord1996,colbert1999}.
We conclude that the CMB effects on the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line observations are negligible for our observations.

\subsection{Spectral energy distribution of the galaxies.}
\label{sec:sed}
Using the upper limits on the continuum, we compare the targets with
the spectral energy distribution templates of local galaxies (SEDs). For the LAEs, the SEDs
of the local galaxies are scaled to the flux of a near-IR filter that is not contaminated
by the Ly$\alpha$\ts\ts emission line. For MACS0647-JD\ts\ts, the filter used for the scaling is the one next
to the Lyman Break. The photometry of  IOK-1 and MACS0647-JD\ts\ts together with the SED
of  local galaxies are shown in Fig. \ref{fig:SEDs}.
For SDF J132415.7+273058\ts\ts and SDF J132408.3+271543\ts\ts (not shown) the situation is very similar: the sources have a similar redshift,
the continuum upper limits are comparable and the CMB effects are of the same order.
Our upper limit for IOK-1 is
comparable to the upper limit found by \cite{walter2012} using PdBI observations.

Using the SED of NGC 6946 as a template, we estimate
the IR luminosity given the upper limit flux densities, similar to the approach shown by
\cite{walter2012}. We scale the SED of NGC 6946 to the 3 sigma upper limits of
the mm observations and integrate from 8 $\mu\rm m$ to 1 mm (rest frame) to
compute the IR luminosity.

The IR luminosity corresponding to this intrinsic SED and the SFR
associated \citep{kennicutt1998} are given in Tab. \ref{tab:table1} for the LAEs and
in Table \ref{tab:table2} for MACS0647-JD\ts\ts.
We note that estimating the IR luminosity using NGC 6946
without taking into account the CMB result in a significant underestimation  of the luminosity upper limits.
The IR luminosity limit corrected by the CMB  of
the LAEs at $z\sim 6.6$ is 35\% higher than without correcting by the CMB. For
IOK-1 at $z\sim7$, the IR luminosity limit is a 50\% higher than the estimation without
correcting by the CMB. For MACS0647-JD\ts\ts at $z\sim10.7$, the IR luminosity limit corrected
for the CMB is $\sim 3.5$ times the IR luminosity limit not corrected by the CMB.
For galaxies with cold dust temperature of $\sim 25$ K, the effect of the
CMB on the observations is very important at high redshift, and it will significantly limit the
feasibility of detecting not extremely starbursting galaxies in the IR continuum, it will not greatly affect the detectability of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission.

\subsection{Ratio $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$}
Figure \ref{fig:CIIFIR} presents our upper limits to $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ and $L_{\rm FIR}$ together
with detections of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi in other galaxies. The arrows represent the region of possible values for
$L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ and $L_{\rm FIR}$ (integrated from $42.5 \mu{\rm m}$ to $122.5 \mu{\rm m}$ rest frame). If we used UV-based SFR estimates to infer $L_{\rm FIR}$,
our data points would move across the diagonal arrows towards the region where local galaxies are,
putting our $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ upper limits close to the average value found
for the local galaxies.
The ratio $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ is a measure of how efficient the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission is
in cooling the gas.
The values presented for our targets, $\log(L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR})\sim-2.9$, do not necessarily imply
that \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi is not efficient in cooling the gas in these galaxies, it is most likely a consequence of the galaxies having
much lower FIR luminosities than our conservative upper limits.
Different processes can affect the ratio $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$.
In galaxies with low extinction and low metallicity, like in Haro 11, about 50\% of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission arises from the diffuse ionized
medium \citep{cormier2012}. Variations on the fraction of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission associated with the ionized medium will also affect the ratio $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$.
In some galaxies, the internal dust extinction can affect the ratio $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$. In Arp 220, the dust is optically thick at 158 $\mu$m and
can absorb part of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission, decreasing the ratio $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ \citep{rangwala2011}.

\cite{diaz-santos2013} present the results of a survey of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi in luminous infrared galaxies (LIRGs)
observed with the PACS instrument on board the \textit{Herschel Space Observatory}. They found a tight correlation
between the ratio $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ and the far-IR $S_{\nu}(63\mu m)/S_{\nu}(158\mu m)$ continuum color, independently
of their $L_{\rm IR}$. They found that the ratio decreases as the average temperature of dust increases, suggesting that the main observable linked to the variation of  $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ is the average dust temperature.
For the galaxies with dust temperatures $\sim20 K$ the average ratio is $\log(L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR})\sim 10^{-2}$, suggesting that for galaxies like NGC 6946 with a dust temperature of $\approx26$ K, the ratio $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ should be on the same order of magnitude.
\cite{diaz-santos2013} also found a correlation between $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ and luminosity surface
density of the mid-IR emitting region ($\Sigma_{\rm IR}=L_{\rm IR}/\pi r^{2}_{\rm mid-IR}$). LIRGs with
lower $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ ratios are warmer and more compact. We can use this relation to find a rough estimation for $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ of our targets.
As $r_{\rm mid-IR}$ we use the size found in the UV observations of the targets. The half-light radius of IOK-1 is $\approx0.62$ kpc \citep{cai2011}.
The full width at half maximum size of SDF J132415.7+273058\ts\ts and SDF J132408.3+271543\ts\ts  are $\approx 4.0$ and 3.2 kpc respectively \citep{taniguchi2005}. For MACS0647-JD\ts\ts  the delensed
half-light radius is $\lesssim 0.1$ kpc \citep{coe2013}. Using our $L_{\rm IR}$ upper limits as an approach to $L_{\rm IR}$ we can estimate $\Sigma_{\rm IR}$. For IOK-1 the estimated ratio is $\log(L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR})\sim-2.9$,  for SDF J132415.7+273058\ts\ts is $\log(L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR})\sim-2.5$ and for SDF J132408.3+271543\ts\ts is $\log(L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR})\sim-2.6$. For the LAEs the average of $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ is similar to the average value for the local galaxies (Fig. \ref{fig:CIIFIR}).
For MACS0647-JD\ts\ts the estimated ratio is $\log(L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR})\sim-3.2$.

\begin{figure}
\epsscale{1.2}
\plotone{CII_FIR.eps}
\caption{Ratio of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi luminosity to the FIR luminosity vs the FIR luminosity (integrated from $42.5 \mu{\rm m}$ to $122.5 \mu{\rm m}$ rest frame) for galaxies at different redshifts.
The green symbols correspond to the upper limits of the LAEs presented here. The blue hexagon corresponds to the upper limit of MACS0647-JD\ts\ts using the
most sensitive setup. The FIR luminosities for the galaxies are upper limits estimated from the observations including the CMB effects. The black diamond corresponds to the upper limit for Himiko with ALMA observations \citep{ouchi2013}.
The horizontal dashed line is the average value for $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}/L_{\rm FIR}$ on the local galaxies.
\citep{malhotra2001,negishi2001,luhman2003,iono2006,maiolino2009,walter2009,stacey2010,
ivison2010,wagg2010,cox2011,debreuck2011,swinbank2012,venemans2012,walter2012a,wang2013,riechers2013,ouchi2013}
\label{fig:CIIFIR}}
\end{figure}

\subsection{SFR-$L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}$ Relation}
In Fig. \ref{fig:CIISFR} we present our $L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}$ upper limits with the UV-SFR estimated for the targets together with upper
limits detections for published LAEs \citep{carilli2013,kanekar2013,ouchi2013}. The black solid lines corresponds to the relation
found by \cite{delooze2011}, with the gray area corresponding to $2\sigma$ scatter in the relation. Our upper limits
for the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi luminosity fall within the scatter of the SFR-$L_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}$, with the exception of SDF J132408.3+271543\ts\ts, where the upper limit falls above the
relation due to the moderate depth of its observations. The detection of the LAE at z=4.7 (Ly$\alpha$\ts\ts-1) agree very well with the relation found by \cite{delooze2011} using the UV-SFR estimated by
\cite{ohyama2004}. The upper limits for the lensed LAE at $z=6.56$ HCM 6A and Himiko suggest that LAEs at $z>6$
could fall below the relation found at low redshift. More observations are needed to clarify if there is an intrinsic difference between
the LAEs at $z\sim4.5$ with the higher redshift population.
The high magnification of MACS0647-JD\ts\ts allows us to explore an UV-SFR one order of magnitude lower than the ones of the LAEs, showing the advantage
of observing lensed galaxies to cover the intrinsically faint population at high redshift.

\begin{figure}
\epsscale{1.2}
\plotone{CII_SFR.eps}
\caption{Relation of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi luminosity with the UV-derived star formation rate of galaxies. The black solid lines correspond to the relation
found by \cite{delooze2011}, with the gray area corresponding to $2\sigma$ of the scatter in the relation. The black dots with error bars
correspond to the data used to find the relation of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi - SFR. The green circle, square and pentagon correspond to the LAEs with the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi upper limits presented in this paper
assuming the star formation rate estimated from the UV fluxes. The blue hexagon corresponds to the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi upper limit of MACS0647-JD\ts\ts with based in the most sensitive setup and the star formation rate estimated from the UV fluxes. The red star corresponds to the LAE detected with ALMA at $z\sim4.7$ \citep{carilli2013}. The black triangle corresponds to the upper limit of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission found for HCM-6A by \cite{kanekar2013}.  The black diamond corresponds to the upper limit of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission found for Himiko by \cite{ouchi2013}. \label{fig:CIISFR}}
\end{figure}

\subsection{IOK-1 Models}
\label{sec:iok1_simulations}
Using the same procedure presented in \cite{vallini2013} for the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission of Himiko, we estimate the emission of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi for IOK-1 at $z\sim7$.
 For this simulation, the star formation rate was set to 20 $\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi yr^{-1}$ and a stellar population age of 10 Myr. The metallicity was set to solar to have
 a conservative estimation of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission. The simulation does not include the emission from PDRs and should be seen as a lower limit. In Fig. \ref{fig:specCIIZ1}, we show the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission produced by the three modeled phases, cold neutral medium (CNM), warm neutral medium (WNM) and the ionized medium. Most of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission comes from the CNM ($\sim50\%$), the rest
 is coming from the WNM ($\sim20\%$) and from the ionized medium ($\sim30\%$). For comparison, in Himiko,  95\% of the emission is produced in the CNM and the rest in the WNM. No emission from the ionized medium was modeled in the simulation of Himiko \citep{vallini2013}. We can also see in the emission that the FWHM of the main peak is $\sim 50$ km\ts s$^{-1}$, just as expected.

In Fig.  \ref{fig:contour_iok1}, we present the integrated flux of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi for a different combination of metallicities and stellar population ages. This shows a strong dependency on the metallicity, which is expected, since it is treated linearly with the abundance of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi in the gas.
The second main feature of this results is the dependency with the stellar population age. Here we assumed a continuum star formation rate of 20 $\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi yr^{-1}$, for the older stellar populations there is a higher amount of heating photons coming from the UV part of the spectrum. This is a result of using a continuum star formation mode, for a given SFR, older populations have more time generating young UV emitting stars. These extra heating photons avoid the cooling of the gas, which decrease the amount of gas in the cold neutral medium, where most of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission is produced.

\begin{figure}
\epsscale{1.2}
\plotone{specCII_Z1.eps}
\caption{Simulated \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi spectrum of a galaxy similar to IOK-1 at $z\sim7$. The parameters set for this simulation
 were a SFR of $20$M$_{\odot}$yr$^{-1}$, and stellar population age of 10 Myr and a solar metallicity. The blue spectrum corresponds
 to the emission produced in the cold neutral medium, the orange spectrum corresponds to the emission produced in the warm neutral medium and
 the green spectrum corresponds to the emission produced in the ionized medium. The main peak (at $\sim 80 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi$)  of the cold neutral medium has a FWHM of $\sim50$ \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi. For more details on the simulations of \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission in high redshift galaxies see \cite{vallini2013}.
 \label{fig:specCIIZ1}}
\end{figure}

\begin{figure}
\epsscale{1.2}
\plotone{contour_IOK1.eps}
\caption{Contour plot of the integrated \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi flux of IOK-1 in ${\rm mJy} \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi$ for different simulation conditions. As comparison, our upper limit for integrated flux of IOK-1 is 175 ${\rm mJy} \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi$. The two independent parameters are the stellar population
age and the metallicity of the gas. The flux is integrated over the whole area of the cube and in a channel
resolution of 500 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi around the peak of the emission. The integrated flux is a conservative upper limit for the different parameters.
We can see from the contour plot that the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission is very sensitive to the metallicity of the galaxy, and in a less significant way to the age of the stellar population.
The different ages correspond to a different amount of heating photons coming from the young stars, which is critical for the cooling of the gas.
\label{fig:contour_iok1}}
\end{figure}

\subsection{Spectral Resolution}

For a Gaussian emission line, with a FWHM of 50 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi observed at a channel resolution of 200 km\ts s$^{-1}$, emission lines will be significantly diluted.  In the best case scenario of the
line falling completely in one channel, we will recover 38\% of the peak flux density of the line. This suggests to carry out observations a sufficiently high
spectral resolution. E.g. with a line of FWHM of 50 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi and a channel resolution of 10 km\ts s$^{-1}$, we expect to recover
97\% of the peak flux density of the line.

\subsection{Atomic Mass Estimation}
We use Equation 1 from \citep{hailey-dunsheath2010} to give rough upper limits to the atomic mass associated with PDRs in our targets (Assuming all \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi would arise from PDRs). As approach to the PDRs conditions we use the result of \cite{vallini2013} for the temperature and density in the CNM of Himiko,
$n=5\times10^{4} $ cm$^{-3}$ and T=250 K. Using our upper limits for \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi we obtain the following upper limits to the atomic mass:
For IOK-1 $M_{\ifmmode{{\rm H}{\rm \small I}}\else{H\ts {\scriptsize I}\ts}\fi}\lesssim 2\times10^{8}\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi$, for SDF J132415.7+273058\ts\ts $M_{\ifmmode{{\rm H}{\rm \small I}}\else{H\ts {\scriptsize I}\ts}\fi}\lesssim 4\times10^{8}\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi$, for SDF J132408.3+271543\ts\ts $M_{\ifmmode{{\rm H}{\rm \small I}}\else{H\ts {\scriptsize I}\ts}\fi}\lesssim 1\times10^{9}\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi$ and
for MACS0647-JD\ts\ts $M_{\ifmmode{{\rm H}{\rm \small I}}\else{H\ts {\scriptsize I}\ts}\fi}\lesssim 6\times10^{7}\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi$.
Assuming that the mass of atomic gas is similar to the mass of molecular gas, we can compare our upper limits with the measurements of similar galaxies at lower redshift.

The only molecular gas masses measured in high redshift UV-selected star-forming galaxies come from the detection of CO transition lines in lensed LBGs.
The measured values are, $\sim 4\times10^{8}\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi$, $\sim 9\times10^{8}\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi$ and $\sim 1\times10^{9}\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi$ for  MS 1512--cB58 ($z=2.73$), the cosmic eye ($z=3.07$)
and MS1358--arc ($z=4.9$) respectively \citep{coppin2007, riechers2010, livermore2012}. Our upper limits for the LAEs are similar to the values estimated for the observed LBGs. For MACS0647-JD\ts\ts our upper
limit for the molecular mass is at least $8\times$ lower than in the observed LBGs.

Using the UV-SFR relation we can estimate the gas depletion timescales for our targets, assuming $\tau_{\rm dep}=M_{\rm gas}/{\rm SFR_{\rm UV}}$. We estimate upper limits for the depletion time of
$\lesssim 8 \rm Myr$, $\lesssim 11 \rm Myr$ and $\lesssim 66 \rm Myr$ for IOK-1, SDF J132415.7+273058\ts\ts and SDF J132408.3+271543\ts\ts respectively. For MACS0647-JD\ts\ts the depletion time is $\lesssim 60 \rm Myr$. The estimated depletion times
for the observed lower redshift lensed LBGs are within the range of $\sim7-24$ Myr, similar to our upper limits. The depletion times for the LAEs are consistent with the ages estimated for the young population of LAEs
at $z\sim4.5$ of $<15$ Myr found by \cite{finkelstein2009} and to the simulated LAEs at $\sim3.1$ with ages $<100$ Myr \citep{shimizu2011}. The depletion times of the LBGs are consistent with the
LBG-phase predicted duration of $20-60$ Myr \citep{gonzalez2012}.

\cite{saintonge2013} presented molecular gas masses and depletion timescales for a sample of lensed star forming galaxies at $z=1.4-3.1$. The range of measured molecular gas masses is $5.6\times10^{9}-4\times10^{11}\ifmmode{{\rm M}_{\odot}}\else{M$_{\odot}$\ts}\fi$ and of depletion timescales is $127-1089$ Myr.
The longer depletion timescales measured for the lower-z sources could indicate that they experience less `extreme' bursts of star formation in comparison to our $z>6.5$ sample. Although, assuming a higher molecular-to-atomic gas ratio (of at least 5) would put our upper limits within the values measured by \cite{saintonge2013}.

\section{Summary and Outlook.}

We have presented a search for \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission in three LAEs
at $z\sim 7$ and in a LBG at $z\sim11$ using CARMA and the PdBI.
We summarize our results and conclusions as follows:

\begin{enumerate}
\item We have not detected \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission line any of our targets.
Given the recent observational results and simulations of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission in high redshift LAE, we adopt
 a line width of 50 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi for the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission. We put constrains on the luminosity of the line for the targets.
 For the LAEs the $3\sigma$ L$_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}$ upper limit are $<2.05$, $<4.52$ and $<10.56\times10^{8}\ifmmode{{\rm L}_{\odot}}\else{L$_{\odot}$\ts}\fi$ for
 IOK-1, SDF J132415.7+273058\ts\ts and SDF J132408.3+271543\ts\ts respectively. Our \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi upper limits are consistent with the relation of SFR-L$_{\ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi}$ found by \cite{delooze2011}.
 The $3\sigma$ upper limit in the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi luminosity of MACS0647-JD\ts\ts is  $<5.27\times10^{7}\times(\mu/15)^{-1}\ifmmode{{\rm L}_{\odot}}\else{L$_{\odot}$\ts}\fi$ (Assuming that the redshift of the galaxy is within the most sensitive setup).

\item No detection of the FIR continuum is found at a wavelength of 158 $\mu \rm m$ rest frame for any of the 4 targets.
Assuming a spectral energy distribution template for the local galaxy NGC 6946 as a template for the high redshift galaxies observed here,
we present conservatives upper limits for the FIR luminosity.  We find $<2.33$, $3.79$ and $7.72\times10^{11}\ifmmode{{\rm L}_{\odot}}\else{L$_{\odot}$\ts}\fi$ as upper limits
for IOK-1, SDF J132415.7+273058\ts\ts and SDF J132408.3+271543\ts\ts respectively, these values account for the effect of the CMB on the observations.
For MACS0647-JD, the upper limit in the FIR luminosity is $<6.1\times10^{10}\times(\mu/15)^{-1}\ifmmode{{\rm L}_{\odot}}\else{L$_{\odot}$\ts}\fi$, after correcting for the CMB and the lensing magnification.

\item We present the results of simulations supporting the brightest component of the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi line having a width of the order of $50$ \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$\ts}\fi. Here we want to emphasize the necessity of resolving such emission lines in future ALMA observations, to not loose signal-to-noise ratio, by selecting a channel resolution that is too low.

\item The effect of the CMB must to be taken into account in attempts to detect the FIR continuum in galaxies at high redshift.
The heating of cold dust by CMB photons can shift the peak of the FIR continuum to values up to a $\sim400$ microns for
galaxies with temperature of $\sim25$ K and redshift of $z\sim11$.
We emphasize that not including the effects of the CMB on the observations results in an underestimation of the FIR luminosities for the targets.
The CMB corrected FIR luminosity limits are 35\% higher than those without CMB correction at $z\sim6.6$, 50\% higher at $z\sim7$, and 350\% higher
at $z\sim11$ for a T$=26$ K.

\item Simulations are already showing us that the task of detecting \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi in high redshift galaxies is going to be difficult even with ALMA, as confirmed
by the recent sensitive non-detection of Himiko by \cite{ouchi2013}.
Accordingly to our IOK-1 simulations, a key parameter for the \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi emission in LAEs is the metallicity, as we discussed in Sect. \ref{sec:iok1_simulations}.
If these simulations were applicable to all high redshift LAEs, we should first try to detect \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi in the LAEs with the highest metallicity.
Estimating the metallicity of LAEs at high redshift is not an easy task, however, \cite{cowie2011} found that for the sample of LAEs discovered by the Galaxy
Evolution Explorer (GALEX) grism in the redshift range of $z=0.195-0.44$, there is an anti-correlation of the equivalent width of the H$\alpha$ emission line with metallicity. Higher EW(H$\alpha$) sources all have lower metallicities, bluer colors, smaller sizes, and less extinction. \cite{cowie2011} also found a broad general trend that for higher EW(H$\alpha$), the EW($\rm{ly}\alpha$) is also higher. If we assume that these relations are valid for the LAEs at high redshift, and that the goal is to observe the LAE with the highest metallicity possible, it may be best to target the brightest LAE in the UV but with the lowest Ly$\alpha$\ts\ts equivalent width. Lyman-break galaxies with Ly$\alpha$\ts\ts detection may thus be ideal targets for \ifmmode{{\rm [C}{\rm \small II}]}\else{[C\ts {\scriptsize II}]\ts}\fi searches at high redshift.
\end{enumerate}

We thank the referee for his/her useful comments and suggestions which significantly improved the quality of this paper. We thank Brent Groves for the discussion on the effects of the CMB.
Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities.
Based on observations with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).
LI and JG obtained partial support from CATA, Conicyt Basal program. LI and JG acknowledge support from FONDAP ``Centro de Astrof\'isica" 15010003. LI thanks the collaboration of the CLASH team.

redpajama_set_name: RedPajamaArXiv


Our people are ERP and ecommerce operations experts. But where some people write memos to capture what they learn, we write software.
Etail is a purpose-built platform and a process designed to execute what we've learned about solving complex ecommerce problems at scale.
Every ecommerce business is different. Each faces its own unique opportunities and challenges. We designed the Etail platform to be almost infinitely configurable to meet those challenges. And we offer years of experience and expertise in EDI, ecommerce, logistics and operations management.
We help merchants and brands streamline their operations, connect with customers, and deliver on their service-level commitments.
It all starts with the platform. The Etail Sales and Supply Chain Management (SSCM) platform was specifically built for the needs of fast-growing ecommerce businesses and brands which sell across multiple marketplaces and utilize multiple fulfillment methods.
Outsourcing ecommerce helps ramp up quickly, avoid hidden costs and minimize risks – all while increasing revenue and margins. Outsourced ecommerce managed services from Etail leverages the best-in-class Etail platform plus the knowledge that grew many of our clients to become Top 100 sellers.
Etail isn't just a platform, it's a system. We provide responsive customer support and a proven blueprint to drive growth. We work with only a handful of clients at a time so you get the one-on-one attention you deserve.
*Many Etail customers prefer not to be identified because they consider Etail to be their competitive edge.
From a 10×10 garage to a 30,000 square foot distribution center, how one home improvement retailer leveraged a strategic partnership to become a top Amazon seller.
From selling a handful of SKUs on Amazon to over 14,000 SKUs on three additional channels, how one western wear retailer leveraged ecommerce business intelligence to increase sales by 450%.
How a liquidation retailer streamlined operations, added multiple new channels, cut order fulfillment time from 4 days to 4 hours, and increased sales 3X.


text:
Q: Por qué se reacomodan los controles al mover algún elemento? En mi vista de diseño los controles los tengo de la manera que aparecen en la imagen, pero cuando ejecuto mi aplicación se muestra todo bien ordenado, y cada vez que intento mover algún elemento siempre regresa a la posición que se muestra en la imagen:

El código correspondiente es:
class IncomeFragment : Fragment() {

    lateinit var ingresosDao: IngresosDao
    var spinner: Spinner? = null
    var button: Button? = null

    override fun onCreateView(
        inflater: LayoutInflater, container: ViewGroup?,
        savedInstanceState: Bundle?
    ): View? {
        // Inflate the layout for this fragment
        val view = inflater.inflate(R.layout.fragment_income, container, false)
        ingresosDao = AppDatabase.getInstance(requireContext()).ingresosDao()
        button = view.findViewById(R.id.btnAgregar) as Button
        spinner = view.findViewById(R.id.spMes) as Spinner
        val adapter: ArrayAdapter<CharSequence> = ArrayAdapter.createFromResource(requireContext(),R.array.Meses, android.R.layout.simple_spinner_item)
        spinner!!.adapter = adapter
        button!!.setOnClickListener{
            val Mes = spMes.selectedItem.toString()
            val Monto = txtMonto.text.toString().toFloat()
            val TipoIngreso = txtTipoIngreso.text.toString()

            if (TipoIngreso.isEmpty()){
                Toast.makeText(requireContext(), "Complete El Campo Anterior", Toast.LENGTH_SHORT).show()
            }
            else{
                val intent = Intent()
                intent.putExtra("id", 0)
                intent.putExtra("mes", Mes)
                intent.putExtra("monto", Monto)
                intent.putExtra("tipoIngreso", TipoIngreso)
                activity!!.setResult(Activity.RESULT_OK, intent)
                txtMonto.setText("")
                txtTipoIngreso.setText("")
                Toast.makeText(requireContext(),"Correcto", Toast.LENGTH_SHORT).show()
            }
        }
        return  view
    }
}

A: El problema se debe a que seguramente estas usando ConstraintLayout y en este caso las vistas contenidas dentro de este tipo de layout deben tener restricciones ("Constraints"),

si estas no se definen, el resultado es que cuando cargues tu aplicaciòn las vistas dentro del layout se veran amontonados, similar a lo que sucediò en esta pregunta:
Error para mostrar una Activity, elementos amontonados posición 0,0
Es importante revises la documentaciòn:
Como crear una Interfaz de Usuario responsiva usando ConstraintLayout

Para definir la posición de una vista en ConstraintLayout, debes
agregar al menos una restricción horizontal y una vertical. Cada
restricción representa una conexión o alineación con otra vista, el
diseño de nivel superior o una guía invisible. Cada restricción define
la posición de la vista a lo largo del eje vertical u horizontal, por
lo que cada vista debe tener un mínimo de una restricción para cada
eje, aunque a menudo se necesitan más.
Cuando sueltas una vista en el editor de diseño, esta permanece donde
la dejas, incluso si no tiene restricciones. Sin embargo, esto solo
sirve para facilitar la edición. Si una vista no tiene restricciones
cuando ejecutas su diseño en un dispositivo, se abre en la posición
[0,0] (la esquina superior izquierda).
En la figura 1, el diseño se ve bien en el editor, pero no hay
restricción vertical en la vista C. Cuando este diseño se abre en un
dispositivo, la vista C se alinea horizontalmente con los bordes
izquierdo y derecho de la vista A, pero aparece en la parte superior
de la pantalla porque no tiene restricción vertical.

Figura 1.

Figura 2.

redpajama_set_name: RedPajamaStackExchange


text:
Share this Story: Florida city forced to pay hackers $600,000 in cryptocurrency to get its computer systems back
Florida city forced to pay hackers $600,000 in cryptocurrency to get its computer systems back
With Riviera Beach's records held hostage, its city council voted unanimously to pay 65 bitcoin to the hackers
Rachel Siegel
Jun 20, 2019 • June 20, 2019 • 2 minute read • Join the conversation
The saga began when a municipal employee opened a corrupted email. Photo by Getty Images
A saga that began with a municipal employee opening a corrupted email has forced a small Florida city to take the extraordinary step of agreeing to pay nearly $600,000 to the hackers who paralyzed their computer systems.
With Riviera Beach's records held hostage, its city council voted unanimously to pay 65 bitcoin to the hackers — a tab that will be picked up by the city's insurance carrier. For the past three weeks, city employees have not been able to access their emails, emergency dispatchers couldn't log calls into computers, and workers and vendors had to be paid with paper checks. Even cops had to dig through closets at the police headquarters to find paper traffic citations, The Palm Beach Post reported.
Florida city forced to pay hackers $600,000 in cryptocurrency to get its computer systems back Back to video
Though city spokeswoman Rose Anne Brown told the Associated Press there is no guarantee the city's records will be returned after the hackers collect, outside security consultants said paying the ransom was the best course of action. The culprits insisted that the ransom be paid in Bitcoin, a cryptocurrency that is difficult trace.
British hacker jailed for blackmailing $1.2 million from porn site users
Toronto-born Canadian is mystery man behind ISIL's high-profile cyber attacks
U.S. charges 22-year-old Canadian Karim Baratov and two Russian spies with massive Yahoo data breach
Before the city council approved the ransom payment, it decided to spend nearly $1 million on new computers, hardware and other system upgrades.
"We are relying on their (the consultants') advice," Brown told AP. The city did not immediately respond to a request for comment Thursday morning.
The waterfront suburb of West Palm Beach joins a growing list of ransomware victims, which include governments and businesses alike. In May, Baltimore said it would not pay hackers $76,000 after its systems were attacked. The city is still trying to recover, and this week, Gov. Larry Hogan, a Republican, appointed Maryland's first statewide chief information security officer to help guard against cyber threats.
Two Iranians were indicted by the U.S. government last year for launching more than 200 ransomware attacks, including those that hit the cities of Atlanta and Newark. Those hackers collected more than $6 million in ransom and caused $30 million in damage to computer systems.
The FBI did not immediately respond to a request for comment. But the agency told the AP that 1,493 ransomware attacks were reported in 2018. Victims, including individuals, paid $3.6 million to hackers — an average of $2,400 per hit.

redpajama_set_name: RedPajamaCommonCrawl


text:
Q: Command Button Visibitly based on Application.Username I am looking at creating an administration button on my user-form.
Now i want it to look up against the application.Username to determine whether the button is visible or not.
My current code is:
Private Sub AdminBtn()

If Application.Username = "Peter.Mogford" Then
AdminCmd.Visible = False
Else
AdminCmd.Visible = True
End If

End Sub

I have put myself in to test it and asked for the visibility to be false but for some reason it is still showing.
I'm not sure whether it has something to do with me writing the code in the user-form instead of a module or something like that.
Please can someone offer a bit of advise.
Thanks in advance

A: The good practice here in case you only need to update the visibility once the form is shown would be using a Form constructor.
Use it like this:
Public Class Form1

Public Sub New()
    InitializeComponent()
    If Application.Username = "Peter.Mogford" Then
    AdminCmd.Visible = False
    Else
    AdminCmd.Visible = True
    End If
End Sub

End Class

When writing a custom form constructor, it is important to call the InitializeComponent() function, which does the controls initialization, before you call any of them.


text:
Bastwick History, Family Crest & Coats of Arms
The name Bastwick first arose amongst the Anglo-Saxon tribes of Britain. It is derived from their having lived in Cheshire, where they derived their name from the township of Bostock, in the parish of Davenham.
Early Origins of the Bastwick family
The surname Bastwick was first found in Cheshire at Bostock, a township, in the parish of Davenham, union and hundred of Northwich. "This place gave name to a family descended from Osmerus, lord of Bostock in the reign of William the Conqueror: the heiress of the elder branch brought the manor in the latter part of the 15th century to the Savages." [1]
"John Bostock, Abbot of St. Alban's, a learned divine and poet in the time of Henry VI., was born [at Wheathampstead, Hertfordshire], and was commonly called John of Wheathampstead." [1]
Important Dates for the Bastwick family
This web page shows only a small excerpt of our Bastwick research. Another 85 words (6 lines of text) covering the years 1593, 1654, 1614, 1623, 1773 and 1846 are included under the topic Early Bastwick History in all our PDF Extended History products and printed products wherever possible.
Bastwick Spelling Variations
One relatively recent invention that did much to standardize English spelling was the printing press. However, before its invention even the most literate people recorded their names according to sound rather than spelling. The spelling variations under which the name Bastwick has appeared include Bostock, Bowstock, Boast, Bostake, Bostick and many more.
Early Notables of the Bastwick family (pre 1700)
Distinguished members of the family include John Bastwick (1593-1654), an English Puritan physician and controversial writer, born at Writtle, in Essex. "He was entered of Emmanuel College, Cambridge, on 19 May 1614, but remained there only a very short time. Leaving the university without a degree, he went 'on his travels,' and served for a...
Another 55 words (4 lines of text) are included under the topic Early Bastwick Notables in all our PDF Extended History products and printed products wherever possible.
Migration of the Bastwick family
At this time, the shores of the New World beckoned many English families that felt that the social climate in England was oppressive and lacked opportunity for change. Thousands left England at great expense in ships that were overcrowded and full of disease. A great portion of these settlers never survived the journey and even a greater number arrived sick, starving, and without a penny. The survivors, however, were often greeted with greater opportunity than they could have experienced back home. These English settlers made significant contributions to those colonies that would eventually become the United States and Canada. An examination of early immigration records and passenger ship lists revealed that people bearing the name Bastwick arrived in North America very early: Francis Boast and his wife and five children settled in Nova Scotia in 1774; Henry Bostock settled in Maryland in 1779; Henry Bostock settled in Barbados in 1635.
^ Lewis, Samuel, A Topographical Dictionary of England. Institute of Historical Research, 1848, Print.
Bastwick (English)


text:
Burning Steel Wool Looks Amazing Up Close Through a Macro Lens
By NY - NewsRoom on October 8, 2016
How does the camera quality of Apple's latest flagship smartphone compare to Leica's high-end digital rangefinders? Respected Japanese street photographer Shin Noguchi decided to find out by shooting the same scenes and then comparing them side-by-side.
Tragic news from Mexico this week. Gifted Canadian artist and photographer Barbara McClatchie Andrews, 74, was found dead on the side of the road last Friday. Her suspected assailant is now in custody.
Being an Army Photographer means multitasking in the most stressful and dangerous of circumstances: swapping between camera and rifle while taking fire. In this video, British Army Photographer Rupert Frere gives us a POV glimpse at what this is actually like in real life.
Say it with me folks: Holy Bokeh Batman! Back in 2014, photographer Matt Granger got his hands on the Canon 50mm f/1.0—a legend of a lens that's accurately been described as, "wholly impractical and yet highly desirable"—and took it for a spin. See what this bokeh monster can do.
A New York-based photographer and Instagram star was killed yesterday after apparently trying to subway surf by climbing onto a train car in Brooklyn.
Here's a video that's going viral on the Web right now: Korean YouTuber MichealHrd shared this short video showing the power of a 200x camera zoom. You can zoom in on an airplane cruising by overhead and read the name of the airline on the side.
The folks at crowdsourced camera gear statistics website Explorecams have released a new infographic that reveals the most commonly used camera and lens combinations used to capture over 11.5 million photos they've analyzed online.
There is something eerily unsettling about old hospitals, even more so when a portion of that old hospital is abandoned and once housed psychiatric patients.
In his collection entitled "Library of Dust", fine art photographer David Maisel gives us a glimpse into the Oregon State Hospital, formally known as the Oregon State Insane Asylum.
I love toys… camera equipment toys, that is. And thanks to my never-ending photographic ADD, I have owned a lot of different cameras. I have a pretty good understanding of most of the different camera makes and models that are on the market today. I've shot most of them to some degree, and I have been able to really dial in what works best for me as a professional wedding photographer.
Sony has just announced its latest Cyber-shot RX camera, and this one's a doozy. The new Sony RX100 V boasts the world's fastest AF speed, the world's fastest continuous shooting, and the world's most AF points for a compact camera.
Sony just introduced its new a6500 camera, the company's flagship APS-C mirrorless camera with the world's fastest AF speed and highest number of AF points among cameras of its category.
Google announced its new in-house Pixel smartphone this week, boasting that it has "the best smartphone camera ever." DxOMark agreed, giving the phone's camera a record-breaking score of 89. If you'd like a taste of the camera's quality, there are now sample photos showing how it performs in the real world.
The Tessina is a vintage Swiss camera that was created by an Austraian chemical engineer named Rudolph Steineck and introduced in 1957 in Switzerland. What's neat about the camera was that one of the accessories was a special wrist bracket that allowed you to wear the camera on your wrist like a watch.
It isn't often that your hobby and your career collide but recently that is just what happened to me. Photography is my hobby. Fraud and Security management is my profession. So when I learned that cameras were used to launch one of the largest cyber attacks in history, I was intrigued.
The Slow Mo Guys have captured some amazing things for their YouTube channel—including this amazing footage of glass shattering at 340,000fps—but their latest creation might be our favorite yet. Click play to see a firecracker explode underwater at a mind-bending 120,000fps.
Here's a simple tip that'll come in particularly handy for the smartphone photographers out there: you can use an old phone's LCD screen as a cheap, portable polarizing filter.
The Duke and Duchess of Cambridge, Prince William and Kate, were ever so kind to drop into Kelowna as part of their royal tour of British Columbia and the Yukon this week. Here's a behind-the-scenes look at what it was like to photograph their visit.
Here's a helpful 12-minute video by landscape photographer and vlogger Thomas Heaton about lens filters. With the emergence of digital photography and powerful editing software, the benefits of some filters can be recreated digitally while others cannot.
The talented Felix Hernandez is back with another beautiful scene captured using tiny objects. This time, he's taken a scale model of a microbus and placed it into a snowy scene in the middle of nowhere… of course "nowhere" is actually his home studio.
If you look at the product page of any "exotic" piece of camera equipment on Amazon, there's a good chance that you'll come across some humorous fake reviews left by photographers looking to poke fun at the product's features. Last September, we shared some funny reviews left for the Sigma 200-500mm, which looks more like a bazooka than a lens. Another one is the Hasselblad H4D-50, a medium format DSLR that costs $19,000… as an open box demo. You can probably guess what the reviews poke fun at.


The Fayette County School Corporation receives teacher applications on a year-round basis. This procedure is not necessarily indicative of specific vacancies, but rather serves to activate individual applications for consideration as vacancies occur. To apply, click on Applications below. .
Please contact Mike Cerqua or Cristal Howe with any questions at 825-2178.


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Better herbicide tolerance technologies are on the way
December 19, 2018 Crops
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country guide response to covid-19 See Details
Better technologies are coming, but we'll need patience and shrewd management until they arrive
By Ralph Pearce
CG Production Editor
Growers in the U.S. are dealing with the spread of Palmer amaranth, which overcame glyphosate as far back as 2010. Photo: File
Count off the many challenges facing a farmer in any growing season and outside of weather conditions, the biggest impediment has to be weed management, particularly as it relates to herbicide tolerance. In spite of the importance of varietal or hybrid selection and fertility, and the potential for yield losses from insect pests and diseases, weed management remains the most perennial of issues for growers.
By contrast, diseases require the right pathogen, the right host and the right environment to flourish, and insect outbreaks also require "the right conditions." But weeds are an every-year occurrence, made that much more daunting by the increasing reality of herbicide tolerance.
Recognize the threat of these invasive weeds
The U.S. 'No. 1 weed problem' heads north
Soybeans, dicamba and you
At the 2018 London Farm Show, Charlie Zila, a research scientist with Corteva Agriscience, agriculture division of DowDuPont, made a presentation in which he highlighted some of the company's technology targets for the years to come. Among some of the directions available to breeders, he mentioned the ongoing need to combat herbicide-tolerant weed species, including Canada fleabane, common waterhemp and Palmer amaranth.
Understanding that there is very little that can be done in a quick three- or five-year window in research and breeding, Zila combines a short- and a longer-term view on the subject of weed management in his assessment. From a short-term perspective, he talks about maximizing performance by using existing varieties and hybrids, and by enhancing them with a more robust portfolio of biotech options. In the longer term, he turns his eyes to current efforts in research and breeding to bring new technologies and perhaps different modes of action to the fight.
"In the past, it was basically Roundup Ready that was the main tool in the toolbox," says Zila, who's based at Corteva's Windfall, Indiana research centre. "But now we have Roundup Ready 2 Xtend in the market, and with the merger with Dow Agroscience, we have access to Enlist technology. There are some growers who are still interested in using LibertyLink and then, of course, there are still conventional chemistries that work for some."
In the past five years, growers in the U.S. Midwest and Corn Belt have had to adjust their tank-mix blends and reliance on biotech traits in the face of increasing resistance. In some regions of Illinois, Iowa and Missouri, biotypes of common waterhemp are now resistant to Group 2 (ALS inhibitors), Group 14 (PPO inhibitors), Group 9 (glyphosate), Group 5 (triazines) and Group 27 (HPPD inhibitors) herbicides. There are also documented cases of Group 4 (2,4-D) resistance in waterhemp found in Nebraska and Missouri.
The problem isn't going to go away on its own.
The other smaller measure that can be employed is to take advantage of some of the native traits that researchers have available in a non-biotech or conventional breeding approach. A specific example of this can be found in variations for tolerance to some common pre-emerge chemistries.
"There was a trap during the past two decades where you didn't put down a pre-plant and then relied on Roundup PowerMax over the top — clearly that won't work anymore," adds Zila. "When we look at PPO chemistries, which are common pre-plant options in the U.S., we know that some products are a little more tolerant than others. Exploiting some of that information is something else we can use as plant breeders."
Trying to overcome Canada fleabane via breeding is the target of many researchers and breeders.
photo: File
What it all comes down to — again, in the short-term — is relying on diversity: varying the environment by not using the same chemistries, the same biotech events or even the same varieties or hybrids for any length of time. It's one reason why, with the advent of the LibertyLink system, weed scientists advocated rotation of Roundup Ready varieties and hybrids with those containing the LibertyLink trait. The purpose wasn't solely to boost yields, it was to keep weed species "confused," thereby reducing their ability to select for resistance.
Now with the launch of both Roundup Xtend and Enlist technologies, growers have additional tools in the toolbox to combat herbicide resistance, at least in the immediate future. From there, Zila sees more opportunities using up-and-coming technologies to create resilient varieties and hybrids with an even greater capacity to avoid selection for resistance.
Just as rotating chemistries and technologies can help diversify that approach, Zila says using conventional breeding techniques, transgenic means and, further into the future, perhaps genetic editing will produce even more solutions.
Although CRISPR (Clustered Regularly Interspaced Short Palindromic Repeats) technology or RNAi (ribonucleic acid interruption) are strong possibilities too, these technologies are still in their early stages.
Corn or soybeans?
Asked if these methods favour corn more than soybeans, Zila sees no great difference. It's the combination of conventional breeding, traditional biotech traits and then using other options at their disposal that will define their success, he says, not whether the developments are geared more to corn than soybeans.
The same is true with weed species. Although there are weed species that are specific to different regions, it's not as though researchers and plant breeders can afford to focus only on those species or those regions. Palmer amaranth may be the weed that is spreading the fastest northward, but for Zila, giant ragweed can be added to his list of problem weeds for corn growers in the U.S. Corn Belt.
"Just to say they are the problems today doesn't mean those same few are going to be only the problems we'll have five years from now — there may be species out there that we don't know about," he says.
It's not a question of "if" there's going to be a problem, but "when." The lesson learned from Roundup Ready technology during the last 20 years is that breeders and researchers want to make sure the new portfolio of traits — be it Xtend or Enlist or Liberty or something completely revolutionary — has durability.
"We don't want resistance in the weeds and we don't want to be looking for even more modes of action five years from now," cautions Zila. He notes that as the Enlist trait becomes more widely available — with glyphosate + glufosinate + 2,4-D-tolerance, there'll be more opportunities for greater diversity in herbicide modes of action. "There's still some breeding work to do with that system but in the next few years, Enlist will be a larger player than it is right now, and having three solid modes of action in one soybean is going to be a pretty exciting thing."
Ralph Pearce
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Hilde Müller, senior partner of MC-Bauchemie, passed away on 9 November 2017, a few days before her 95th birthday.
Together with her husband Heinrich W. Müller, she founded MC-Bauchemie and actively contributed to the creation of a modern, international company from these early beginnings. While in the early years Heinrich W. Müller was responsible for sales development, Hilde Müller managed the company's finance and accounting department. Even when her sons Claus-Michael and Bertram joined the Executive Board, she remained dedicated to MC with her unfailing modesty and discretion. Consistently prepared to relegate her personal concerns to the back of her mind, she was both balanced and positive in her influence. She thus played a decisive role in the successful establishment and expansion of our company.
With her winning personality, natural authority and social responsibility, she served as a paradigm for us all.
At an intimate family ceremony, Hilde Müller was laid to rest this weekend.