text:
\section{Introduction}

Observations of star-formation activity are critically important to
tackle open questions relating to galaxy formation and evolution. The
most direct view of cosmic star-formation history comes from observing
ultraviolet (UV) photons from the young massive stars. However, part
of this radiation is absorbed by dust, and the higher UV-energy
photons are absorbed by neutral hydrogen. Gas ionised by this
radiation eventually recombines, producing emission lines such as
Ly$\alpha$ and H$\alpha$, which have been used historically to
estimate the star-formation rate \citep[SFR, e.g., ][]{Sobral2019}.
Where the star-formation activity is shielded by gas and dust, the
ionising photons may get absorbed and re-radiated at far-infrared
(FIR) wavelengths by dust.
Therefore, the rest-frame FIR emission is used to trace dust-obscured
star formation in galaxies, and to derive total SFRs in combination
with tracers of unobscured emission \citep[e.g.][]{Kennicutt1998, Kennicutt2012}.

Different ways to estimate the SFR in galaxies have their own
limitations and biases. For example, the H$\alpha$ recombination line
is generated originally by the photo-ionising radiation from massive
stars ($\gtrsim 10$\,M$_\odot$), or AGN, and is therefore sensitive to
recent star formation, within $\sim$10\,Myr, and has modest
sensitivity to dust obscuration. The UV flux ($\sim 1600$\,\AA), on
the other hand, comes from young, massive stars but is also emitted by
older 10--100\,Myr stars \citep{Kennicutt2012}, and is very sensitive
to dust obscuration. The FIR emission produced by heated dust grains
comes from young star-forming regions but in lower luminosity sources,
it can also arise from dust heated by
older stellar populations.  Spatially-resolved observations of local
galaxies show that all of these SFR tracers are strongly correlated on
$\sim$\,kpc scales \citep[e.g.,][]{Boquien2016}.

Previous observations of high-redshift galaxies have shown that their
star-formation activity --- as traced by UV or H$\alpha$ emission ---
presents bright, clumpy star-forming complexes that could be up to
$\sim1000\times$ more massive than those seen in local galaxies
\citep[e.g., ][]{Genzel2006,Genzel2008, Schreiber2006, Schreiber2009,
  Schreiber2018, Shapiro2008, Swinbank2012a, Swinbank2012b}. However,
it may be that regions with fainter H$\alpha$ and UV emissions are
affected by significant dust obscuration.  Previous work has shown
that dust attenuation causes the SFR derived from different indicators to be inconsistent
\citep{Swinbank2004, Katsianis2017}, thus it is
essential to have a spatially resolved view of the ionised gas and the
dust content in order to characterise the total SFR (unobscured and
obscured), especially for high-redshift galaxies.

\begin{table*}
\centering
\caption{\label{tab:table1} ALMA observational set-up, ordered by the observation date.}
\small
\begin{tabular}{lccccccccc}
\hline
Source List   & Project ID     & Observation    & Flux       & Bandpass   & Phase      & P.W.V.  & Number of & Band ($\nu_{\rm obs}$ /GHz) & Time on \\
              &                & Date           & Calibrator & Calibrator & Calibrator & (mm) & antennas    &    & Target (min)\\
\hline
SHiZELS-8     & 2012.1.00402.S &  6 Nov.\ 2013  & Uranus     & J2148+0657 & J0215-0222 & 3.9  & 29 &  7 (344)     & 52 \\
              &                &  29 Nov.\ 2013 & Uranus     & J0334-4008 & J0215-0222 & 1.3  & 26 &      & 43 \\
              &                &  29 Nov.\ 2013 & J0423-013  & J0334-4008 & J0215-0222 & 1.0  & 26 &       & 43 \\
\hline
SHIZELS-7     & 2013.1.01188.S & 11 Aug.\ 2015 & Ceres       & J0006-0623 & J0208-0047 & 0.9 & 43  &  7 (344)     & 28 \\
SHiZELS-21    &                & 29 Aug.\ 2015 & J0334-401   & J0006-0623 & J0219+0120 & 1.5 & 37  &  6 (261)     & 30 \\
SHiZELS-2     &                & 29 Aug.\ 2015 & J0238+166   & J0224+0659 & J0219+0120 & 1.4 & 37  &  6 (261)     & 30 \\
\hline
SHIZELS-3      & 2015.1.00026.S & 28 Jul.\ 2016 & J1058+0133 & J1058+0133 & J0948+0022 & 0.6 & 37  &  6 (261)     & 26 \\
SHIZELS-9      &                & 16 Jul.\ 2016 & J0238+1636 & J0238+1636 & J0217+0144 & 0.4 & 38  &  7 (344)     & 43 \\
SHIZELS-10     &                & 26 Jul.\ 2016 & J0238+1636 & J0238+1636 & J0217+0144 & 0.4 & 38  &  7 (344)     & 43 \\
SHIZELS-11     &                & 26 Jul.\ 2016 & J0238+1636 & J0238+1636 & J0217+0144 & 0.6 & 45  &  7 (344)     & 43 \\
               &                & 10 Aug.\ 2016 & J0006-0623 & J0006-0623 & J0217+0144 & 0.2 & 42  &       & 43 \\
               &                & 10 Aug.\ 2016 & J0238+1636 & J0238+1636 & J0217+0144 & 0.2 & 39  &       & 43 \\
SHIZELS-14     &                &  2 Aug.\ 2016 & J1058+0133 & J1058+0133 & J0948+0022 & 0.7 & 39  &  6 (261)     & 26 \\
\hline
\end{tabular}
\end{table*}

The High-$z$ Emission Line Survey \citep[HiZELS,][]{Sobral2012,
  Sobral2013, Sobral2015, Geach2008} was designed to study `normal' star-forming
galaxies selected in narrow redshift slices at 0.4, 0.84, 1.47 and
2.23 via the identification of H$\alpha$ emission using near-infrared
(near-IR) narrow-band filter imaging in extragalactic survey fields including
the Subaru-{\it XMM} Deep Field / UKIDSS Ultra Deep Survey \citep[UDS, ][]{Lawrence2007} and the
Cosmological Evolution Survey \citep[COSMOS, ][]{Scoville2007} fields.
The HiZELS survey detects thousands of emission-line
objects, samples the `typical' galaxy population \citep{Oteo2015, Cochrane2018}, following the so-called
`main sequence' for star-forming galaxies at $z\simeq$ 1.47 and 2.23
\citep{Gillman2019}, and probing below the knee of the H$\alpha$
luminosity function ($<\,L^*_{\rm H\alpha}$) at these redshifts
\citep[$L^*_{\rm H\alpha} = 10^{42.6} \rm erg\,s^{-1}$ at $z \simeq 1.47$
and $L^*_{\rm H\alpha} = 10^{42.9} \rm erg\,s^{-1}$ at $z\simeq 2.23$, ][]{Swinbank2012a, Cochrane2017}.
Over thirty galaxies from HiZELS have also been
mapped in the follow-up near-IR using integral field unit (IFU) spectroscopy
(the `SHIZELS' sample) aided by adaptive optics (AO), with the
Spectrograph for INtegral Field Observations in the Near Infrared
(SINFONI) at the Very Large Telescope (VLT) or the Near-Infrared
Integral Field Spectrometer (NIFS) at Gemini-North
\citep{Swinbank2012a, Swinbank2012b, Molina2017, Gillman2019}. These
observations provide H$\alpha$ IFU imaging at $\sim$\,1\,kpc scales
for galaxies at $z \simeq $ 1.47 or 2.23.

In this work, we make use of the available AO-aided IFU data and the {\it
Hubble Space Telescope (HST)} F606W, F140W data, together with new
Atacama Large Millimeter/submillimeter Array (ALMA) observations
targeting the continuum emission at
submillimetre wavelengths at similar spatial resolution (synthesised beam of
$\sim0\farcs2-0\farcs3$ full width half maximum), to characterise the
spatial correlation between the the H$\alpha$/UV and dust emission of
high-redshift $z\simeq $ 1.47 and 2.23 galaxies (the `ALMA-SHiZELS' sample).
The combination of the AO-aided IFU H$\alpha$ data, {\it HST} data and the ALMA
observations provides a unique opportunity to characterise the spatial
correlation between the SFR tracers around the peak of cosmic star formation.
We describe our observations, data reduction and analysis in Section 2. In Section
3, we present the results and discussion, and summarise in Section
4. Throughout this work, we assume a $\Lambda$CDM cosmology with
${\rm H_0}$\,=\,70\,${\rm km s^{-1} Mpc^{-1}}$,
${\rm \Omega_M} = 0.3$, ${\rm \Omega_\Lambda} = 0.7$, where
$0\farcs15$ corresponds to a physical scale of $\sim$1.3\,kpc at
both $z\simeq 1.47$ and 2.23.

\section{Observations and data reduction, and analysis}

\subsection{ALMA observations}

Nine SHiZELS galaxies were observed with ALMA during
Cycle 2, 3, 4 (projects 2012.1.00402.S, 2013.1.01188.S and
2015.1.00026.S; P.I.: E.\ Ibar) in Bands 6 or 7,
depending on whether the galaxies were at $z=2.23$ or 1.47,
respectively, corresponding to rest-frame $\sim$\,355$\mu$m.  The
observations were designed to detect continuum emission using four
spectral windows (SPWs), each covering an effective bandwidth of
1.875\,GHz at a spectral resolution of 15.6\,MHz. Observations were
taken under relatively good weather conditions with precipitable water
vapour (P.W.V.) ranging from 0.2\,mm to 3.9\,mm, and using 29 to 45
antennas (the earlier the cycle, the smaller the number) with
the longest baselines spanning 1.0--1.5\,km.
The phase, bandpass and flux calibrators
for all observations used in this work are listed in
Table~\ref{tab:table1}.

Data reduction was carried out using the Common Astronomy Software
Applications ({\sc casa}) and using the ALMA pipeline up to the
production of calibrated $uv$ data products. Three imaging approaches
were performed using the task {\sc tclean}, exploring a Briggs
weighting ({\sc robust=0.5}), natural weighting, and $uv$ tapering
such that we created a synthesized beam of $\sim 1''$ (see
Figs~\ref{ALMAdet1}, \ref{ALMAdet2}).  In all cases, the signal is
interactively cleaned down to 2--3\,$\sigma$
(r.m.s.\,$\sim$\,25$\mu$Jy\,beam$^{-1}$) in regions with significant
emission at the source position. The astrometric accuracy of the ALMA
Band-7 image is around 1.5\,mas. Information about each target is
presented in Table~\ref{table2}.

Sources SHiZELS-7, SHiZELS-9, SHiZELS-11 and SHiZELS-14 were detected
by ALMA at a significance higher than 5$\sigma$ in at least one of the
three imaging approaches, while SHiZELS-21, SHiZELS-8, SHiZELS-10,
SHiZELS-2 and SHiZELS-3 remained undetected, regardless of the imaging
approach.

Within the field of view (FoV) of SHiZELS-7 and SHiZELS-10, we
identify two serendipitous detections. We denote them as SHiZELS7-ID2
and SHiZELS10-ID2 and their properties are listed in Appendix~\ref{APC}.

\begin{table*}
  \centering
  \caption{\label{table2} Properties of the SHiZELS galaxies presented in this work. ID and
     z$_{\rm H\alpha}$ and $M_\star$ are extracted from previous AO-aided IFU observations
    presented in \citet{Gillman2019}. $S_{\rm 355\mu m}$ and $R_{\rm dust}$ are the observed continuum
    flux density and the deconvolved half-light radius at 355\,$\mu$m (rest-frame).  $\ddagger$ Possible AGN.}
  \resizebox{\textwidth}{!}{
  \begin{tabular}{lccccccccccc}
    \hline
    ID           & R.A.\ (J2000) & Dec. (J2000)  & $z_{\rm H\alpha}$ & $\log(L_{\rm H\alpha}/\rm erg\, s^{-1})$ & $S_{\rm 355\mu m}$ (mJy) & $\log(L_{\rm FIR}/{\rm L}_\odot)$  & $\log(M_*^{\rm MAGPHYS} /{\rm M}_\odot)$ & $\log(\rm SFR^{\rm MAGPHYS}/M_\odot \rm yr^{-1})$ & $A_v$  & $R^{\rm half-light}_{\rm dust}$ (kpc) & $R_{\rm dust}^{\rm uvfit}$ (kpc) \\
    \hline
    SHiZELS-7    & 02:17:00.34 & $-$05:01:50.6  & 1.455 & 42.1 & 0.15    $\pm$ 0.03  & 10.5 $\pm$ 0.4     & 10.4 $\pm$ 0.2 & 1.6$\pm$0.3 & 0.8$\pm$0.5  & 3.7 $\pm$ 0.3 & 4.3 $\pm$ 0.4 \\
    SHiZELS-9    & 02:17:12.99 & $-$04:54:40.7  & 1.462 & 42.4 & 0.51    $\pm$ 0.06  & 11.2 $\pm$ 0.4     & 10.6 $\pm$ 0.1 & 1.9$\pm$0.2 & 1.0$\pm$0.3  & 4.9 $\pm$ 0.3 & 4.8 $\pm$ 0.4 \\
SHiZELS-11$\ddagger$& 02:18:21.23 &$-$05:02:48.9& 1.492 & 42.3 & 1.34    $\pm$ 0.14  & 11.6 $\pm$ 0.4     & 11.5 $\pm$ 0.1 & 1.7$\pm$0.1 & 0.8$\pm$0.1  & 5.2 $\pm$ 0.4 & 4.3 $\pm$ 0.5 \\
    SHiZELS-14   & 10:00:51.58 & $+$02:33:34.1  & 2.242 & 42.9 & 2.31    $\pm$ 0.23  & 12.6 $\pm$ 0.3     & 11.1 $\pm$ 0.1 & 2.6$\pm$0.2 & 1.5$\pm$0.2  & 4.7 $\pm$ 0.3 & 4.1 $\pm$ 0.4 \\
    SHiZELS-10   & 02:17:39.02 & $-$04:44:41.4  & 1.447 & 41.9 & < 0.11 (5$\sigma$)  & <11.3 (5$\sigma$)  & 10.1 $\pm$ 0.1 & 2.0$\pm$0.2 & 1.4$\pm$0.2  &    --         &    --         \\
    SHiZELS-8    & 02:18:20.96 & $-$05:19:07.5  & 1.460 & 42.2 & < 0.12 (5$\sigma$)  & <11.2 (5$\sigma$)  & 10.3 $\pm$ 0.1 & 1.9$\pm$0.2 & 1.4$\pm$0.4  &    --         &    --         \\
    SHiZELS-2    & 02:19:25.50 & $-$04:54:39.6  & 2.223 & 42.3 & < 0.12 (5$\sigma$)  & <11.9 (5$\sigma$)  & 9.9  $\pm$ 0.2 & 1.4$\pm$0.3 & 0.3$\pm$0.3  &    --         &    --         \\
    SHIZELS-3    & 10:00:27.69 & $+$02:14:30.6  & 2.225 & 42.4 & < 0.10 (5$\sigma$)  & <11.8 (5$\sigma$)  & 9.0  $\pm$ 0.1 & 0.9$\pm$0.2 & 0.2$\pm$0.1  &    --         &    --         \\
    SHIZELS-21   & 02:16:45.82 & $-$05:02:45.0  & 2.237 & 42.6 & < 0.12 (5$\sigma$)  & <11.8 (5$\sigma$)  & 9.8  $\pm$ 0.1 & 1.6$\pm$0.2 & 1.2$\pm$0.3  &    --         &    --         \\
    \hline
  \end{tabular}}
\end{table*}

\begin{figure*}
\centering
\includegraphics[width=0.48\textwidth]{SHiZELS9-gb-ha-contour.eps}
\includegraphics[width=0.48\textwidth]{SHiZELS11-gb-ha-contour.eps}
\includegraphics[width=0.48\textwidth]{SHiZELS14-gb-ha-contour.eps}
\includegraphics[width=0.48\textwidth]{SHiZELS7-gb-ha-contour.eps}
\caption{The {\it HST} F606W (blue) and F140W (red) true-colour composite images, including ALMA
continuum contours (cyan) and H$\alpha$ contours (orange). Contour levels are shown at
2-, 3-, 4- and 5-$\sigma$, The ALMA synthesised beam is shown in the
lower left corner. The green dash lines show the direction of major kinematic axis \citep[$\rm PA_{vel}$, see the velocity map in][]{Gillman2019}.
The three different tracers of star formation are clearly
highlighting very different regions.}\label{colorimage}
\end{figure*}

\subsection{Global astrometry}
\label{astrometry-issue}

One of the main challenges when analysing multi-wavelength high-resolution
spatially-resolved observations is the global astrometric accuracy.
In particular, IFU observations with a small FoV (as obtained with
SINFONI, which has a FoV of about $3''\times 3''$) present a global
astrometric uncertainty which is larger than the resolution elements of
the observations, therefore they are difficult to anchor to other
observations at high-resolution. For this reason, we perform the
following astrometric corrections to analyse our data.

Firstly, we align the astrometry of the HiZELS narrow-band images by
the public {\it Gaia} DR2 catalogue.  The offset between the HiZELS
catalogue generated by SExtractor and the {\it Gaia} catalogue is
corrected to $\Delta {\rm R.A.} = 0\farcs004\pm 0\farcs13''$ and
$\Delta {\rm Dec.} = -0\farcs010 \pm 0\farcs10$.  We degrade the
resolution of the H$\alpha$ moment-0 SINFONI image down to $0\farcs7$
using a Gaussian kernel to get a similar resolution to the HiZELS
narrow-band images. Then we fit a Gaussian profile to this
low-resolution image in order to obtain the position of the peak,
identify the offset with respect to the narrow-band image, and use
this information to correct the astrometry of the IFU image.

As mentioned before, we have also used the available {\it HST} F606W and
F140W observations \footnote{{\it HST} proposal ID: 14719, P.I.:
  P.~Best}. The {\it HST} FoV is about $2'\times 2'$, which is too
small to apply a reliable astrometric correction using {\it Gaia}
DR2. Therefore, we correct the global astrometry of the {\it HST}
images using the HSC DR2 catalogue available in our fields
\citep{Aihara2019}. The 5$\sigma$ limiting magnitude within $2''$
diameter apertures of the HSC $i$-band catalogue is 26.7 AB mag, which is
similar to the {\it HST} images, and deep enough to have about
200 high-S/N sources for the alignment. The astrometric accuracy
of HSC DR2 catalogue derives from the {\it Gaia} DR2 catalogue
\citep{Aihara2019}. We match the {\it HST} and HSC catalogues for the
offsets of R.A., Dec., and correct the astrometry of the {\it HST}
image. After our astrometric correction, the catalogue match between
{\it HST} and HSC catalogues is consistent with an offset of zero, with
systematic errors of $\sim 0\farcs04$.

In Fig.~\ref{colorimage}, we show the true-colour image composite
from {\it HST} F606W (in blue) and F140W (in red) images, including
ALMA continuum contours in levels of $2\sigma$, $3\sigma$, $4\sigma$,
$5\sigma$ for the four ALMA-detected galaxies. The galaxy centres
revealed by {\it HST} more or less coincide with the ALMA imaging.
The observations reveal a complex state for the
interstellar medium in SHiZELS galaxies at $z\simeq$ 1.47 and 2.23.
We show multi-wavelength postage stamps of the {\it HST}, H$\alpha$
\citep{Gillman2019} and our ALMA images for each of the galaxies
presented in this work in Figs~\ref{ALMAdet1} and \ref{ALMAdet2}.

\begin{figure}
\centering
\includegraphics[width=0.47\textwidth]{Mdust-Mstar.eps}
\caption{The dust mass to stellar mass of our sample (red),
the local galaxies from the Dustpedia project \citep[green, ][]{Clark2018},
and the SMGs from the ALMA SCUBA-2 UDS survey \citep[purple, ][]{Dudzeviciute2020}.
The dust mass and the stellar mass of our sample and the comparison samples are derived
from the SED fitting results by MAGPHYS.
The red filled circles are the ALMA detected targets while the red open circles are the ALMA non-detected targets.
The target with the stellar mass above $10^{11}M_\odot$ is SHiZELS-14, which is a ULIRG.
}\label{duststellarratio}
\end{figure}

\begin{figure
\centering
\includegraphics[width=0.46\textwidth]{SFR-Ha-FIRerr.eps}
\caption{The total SFRs derived from the extinction-corrected
H$\alpha$ (Eq.~3), and FIR luminosities for $z\sim 2.23$ and
$z\sim 1.47$ samples, respectively. We show the ALMA detected
targets as filled red circles and the ALMA non-detected targets
as open red circles. We compare our findings with
previously observed SMGs at $z\sim$2 from \citet{Swinbank2004} and
\citet{Chen2020}.  A sample of 15-$\mu$m-selected galaxies (at
$z\sim1$) presented by \citet{Franceschini2003} are also shown.
The dotted lines show 0.5 dex above and below the solid line.}
\label{SFR_MASS}
\end{figure}

\begin{table*}
	\centering
	\scriptsize
	\caption{Gas phase metallicities derived from previous AO-aided IFU observations
	(following \citet{Curti2017}),
	gas to dust ratio (see \S~\ref{metalicity}),
	total ISM mass estimated following \citet{Scoville2016},
	the dust mass from gas-to-dust ratio  ($\log (M_{\rm dust}^{\rm GDR}$) and SED fitting  ($\log (M_{\rm dust}^{\rm SED}$)
	for the ALMA-SHiZELS galaxies presented in this work. $\ddagger$ Possible AGN. For the ALMA detected galaxy, the MAGPHYS fitting includes the new ALMA flux. }
	\label{tab3}
	\begin{tabular}{lcccccccccccc}
		\hline
		ID         & [N\,{\sc ii}]/H$\alpha$ & 12+log(O/H)   & $\delta_{\rm GDR}$ & $\log(M_{\rm ISM}/{\rm M}_\odot)$  & $\log (M_{\rm dust}^{\rm GDR}/{\rm M}_{\odot})$& $\log (M_{\rm dust}^{\rm SED}/{\rm M}_{\odot})$ & $\log(M_{\rm dust}^{\rm MAGPHYS}/{\rm M}_{\odot})$ & $\log(M_{\rm dust}^{\rm MAGPHYS}/M_*)$ \\
		\hline
		SHiZELS-7  &   0.43   $\pm$  0.05 & 8.79 $\pm$ 0.11  & 69 $\pm$ 24        &  9.65 $\pm$ 0.05             &7.8  $\pm$ 0.2     &7.5$\pm$ 0.2     & 7.4$\pm$0.2  & -3.2 $\pm$ 0.3\\
		SHiZELS-9  &   0.27   $\pm$  0.03 & 8.64 $\pm$ 0.11  & 97 $\pm$ 30        & 10.17 $\pm$ 0.04             &8.2  $\pm$ 0.1     &8.1$\pm$ 0.2     & 7.9$\pm$0.1  & -2.9 $\pm$ 0.2 \\
SHiZELS-11$\ddagger$ & 0.60   $\pm$  0.10 & 8.87 $\pm$ 0.12  & 57 $\pm$ 21        & 10.59 $\pm$ 0.06             &8.8  $\pm$ 0.2     &8.5$\pm$ 0.2     & 8.6$\pm$0.1  & -2.3 $\pm$ 0.3 \\
		SHiZELS-14 &   0.60   $\pm$ 0.05  & 8.87 $\pm$ 0.11  & 57 $\pm$ 21        & 11.19 $\pm$ 0.06             &9.4  $\pm$ 0.2     &8.8$\pm$ 0.1    & 9.0$\pm$0.1  & -2.1 $\pm$ 0.2 \\
		SHiZELS-10 &   0.13   $\pm$  0.04 & 8.47 $\pm$ 0.17  & 143 $\pm$ 37       &  $<9.50$                     &$<$7.3             &$<$7.4             & 8.0$\pm$0.5      & -2.1 $\pm$ 0.5  \\
		SHiZELS-8  &   $<$0.1             &$<$8.42           & $>$264             &   --                         &--                 &$<$7.4             & 8.0$\pm$0.5      & -2.3 $\pm$ 0.5  \\
		SHiZELS-2  &   0.12   $\pm$  0.01 & 8.45 $\pm$ 0.11  & 150 $\pm$ 38       &  $<9.92$                     &$<$7.7             &$<$7.6             & 7.3$\pm$0.6      & -2.5 $\pm$ 0.6  \\
		SHiZELS-3  &   0.03   $\pm$  0.01 & 8.13 $\pm$ 0.29  & 310 $\pm$ 52       &  $<9.84$                     &$<$7.3             &$<$7.5             & 6.3$\pm$0.6      & -2.7 $\pm$ 0.6  \\
		SHiZELS-21 &   0.23   $\pm$  0.04 & 8.60 $\pm$ 0.16  & 106 $\pm$ 32       &  $<9.92$                     &$<$7.9             &$<$7.6             & 7.6$\pm$0.5      & -2.1 $\pm$ 0.5  \\
		\hline
	\end{tabular}
\end{table*}

\subsection{MAGPHYS fitting with ALMA flux}
SEDs of the SHiZELS sample were previously fitted using MAGPHYS \citep{2008MNRAS.388.1595D} in \citet{Gillman2019}.
The ALMA detected fluxes of the ALMA-SHiZELS galaxies can help to constrain the FIR properties.
Therefore, we re-fit the SEDs of the four ALMA detected galaxies including the FIR flux we obtained in this work,
and list the main results in Table \ref{table2} and \ref{tab3}. For the ALMA non-detected
galaxies, we list the dust mass given by MAGPHYS from fitting the optical-to-NIR SEDs.
The stellar mass and dust mass show reasonable consistencies from the different approach.

We show the dust-to-stellar mass ratio ($\log_{10}(M_{\rm dust}/M_*)$) in Fig. \ref{duststellarratio}
and compare our results with the local galaxies from Dustpedia \citep{Clark2018, Casasola2020}.
The only ULIRG in our sample, SHiZELS-14, has a larger $\log_{10}(M_{\rm dust}/M_*) = -2.1\pm 0.2$
than the local galaxies, while this value is consistent with the typical value of $\log_{10}(M_{\rm dust}/M_*)$
in SMGs at redshift about 2 \citep{Calura2017}. The rest targets of our sample all have
consistent or 1$\sigma$ higher $\log_{10}(M_{\rm dust}/M_*)$) values as the local galaxies,
even for the targets with no ALMA detection.

\subsection{Global SFRs from H$\alpha$ and FIR emission}\label{Sect3.1}

To estimate the FIR luminosity (and SFR$_{\rm FIR}$) using the ALMA
observations (rest-frame continuum at $\sim$355\,$\mu$m), we assume a
FIR SED template based on previous stacking analyses for HiZELS
galaxies at $z \sim 1.47$ \citep{Ibar2013} and 2.23
\citep{Thomson2017}. Thanks to the rich multi-wavelength coverage, the
stellar masses of the HiZELS galaxies can be estimated reasonably well
\citep[see ][]{Sobral2014, Gillman2019}.  For the purpose of this
work, for the $z\sim1.47$ targets, we adopt the stacked SEDs derived
by \citet{Ibar2013} in the stellar mass bins of
$9.9<\log(M_* /M_\odot)<10.3$ and $10.3<\log(M_* /M_\odot)<11.8$.
For galaxies at $z\sim2.23$, we consider the FIR template
presented in \citet{Thomson2017}.

We fit each FIR template SED following the modified-blackbody
fitting method described by \citet{Beelen2006}, assuming a fixed
power-law index for the dust emissivity, $\beta = 1.8$.
The fitting results show a dust temperature of about 25 $\pm$ 1 K
for $z \simeq 1.47$ targets and 32 $\pm$ 2 K for the $z \simeq 2.23$ targets,
similar to previous measurements of luminous IR galaxies at high redshift \citep{Hwang2010, Oteo2017, Liang2019}.
To estimate FIR luminosities, we normalise the assumed SED to the observed ALMA flux densities.
We derive dust masses following the method presented in \citet{Beelen2006},
finding values in the range of $10^{7.1} - 10^{8.9}$\,M$_\odot$.
From Table \ref{tab3} we can see that the dust masses derived from SED fitting and the
MAGPHYS are consistent.
For the galaxies with no ALMA detection, we use global upper limits using
$5\times$ the r.m.s.\ of the tapered image.

Uncertainties for the FIR properties come from the SED fitting, FIR
flux measured from ALMA results, and template assumption.  We expect
dust-temperature uncertainties for galaxy templates for
$M_* > 10^{10}$\,M$_\odot$ galaxies of about 5\,K \citep[see the
Fig. 5 in ][]{Ibar2013}, which leads to a systematic uncertainty in
$\log(L_{\rm FIR}/$L$_\odot)$ of about 0.3\,dex.  We run a Monte-Carlo
simulation to sample the dust temperature, assuming a Gaussian
distribution centred at $T_{\rm dust}$ from the FIR SED templates, and
a scatter $\sigma_{T_{\rm dust}} = 5$\,K. We also sample the ALMA flux
density (or flux density limit) from a Gaussian distribution centred
at the measured flux density with the observed scatter. Then we derive
$L_{\rm FIR}$ and $M_{\rm dust}$, and their r.m.s.\ scatter, such that
the scatter of $L_{\rm FIR}$ includes the uncertainty in
$T_{\rm dust}$ and ALMA flux density. Since we only have one detected FIR
band for most sources, we cannot sensibly adopt a more complex model
to understand the FIR properties.

The obscured SFR, as derived from the observed FIR emission, can be
estimated by \citet{Kennicutt2012}:
\begin{equation}
    \log {\rm SFR}_{\rm FIR}({M_{\odot}\,\rm yr^{-1}}) = \log L_{\rm FIR (8-1000\mu m)} ({\rm erg\,s^{-1}}) -  43.47,
\end{equation}
assuming a Chabrier initial mass function \citep[IMF; ][]{Chabrier2003}.

\begin{figure}
\centering
\includegraphics[width=0.47\textwidth]{mass-metallicity.eps}
\caption{The stellar mass versus [N\,{\sc ii}]/H$\alpha$ for our
  ALMA-SHiZELS galaxies. The ALMA-detected targets are shown in red
  while the non-detected targets are coloured blue. Since the
  metallicity could be derived from the [N\,{\sc ii}]/H$\alpha$ ratio \citep{Curti2017},
  we show the metallicity on the right-hand axis. We also show the
  mass-metallicity results at redshift $\sim$2 from
  \citet{2006ApJ...644..813E} in blue dots. Only the more massive
  galaxies with high metallicities are detected in continuum by
  ALMA.}\label{metamass}
\end{figure}

\begin{figure*}
\centering
\includegraphics[width=0.47\textwidth]{S7-uv-real.eps}
\includegraphics[width=0.47\textwidth]{S9-uv-real.eps}
\includegraphics[width=0.47\textwidth]{S11-uv-real.eps}
\includegraphics[width=0.47\textwidth]{S14-uv-real.eps}
\caption{The $uv$-real visibility diagrams of the ALMA detected targets.
The black dots and blue error bar are obtained from the ALMA data while the red
lines are the fitting results by disk model in the CASA task {\sc uvmodelfit}.
}\label{uv-profile}
\end{figure*}

On the other hand, to correct the flux observed from the narrow-band
H$\alpha$ imaging for dust extinction, we assume a parametrisation of
the H$\alpha$ extinction as a function of stellar mass following
\citet{Garn2010}:
\begin{equation}
    A_{\rm H\alpha}(M_*) = -0.09 X^{3} + 0.11 X^{2} + 0.77 X + 0.91,
\end{equation}
where $X = \log_{10}( M_* / 10^{10} {\rm M}_\odot)$.
This correlation between H$\alpha$ extinction and stellar mass
has also been confirmed by \citet{Sobral2012}, \citet{Koyama2019} and \citet{Qin2019}.
Using the stellar masses presented by in Table \ref{table2}, we derive the
extinction-corrected H$\alpha$ luminosity ($L^{\rm corr}_{\rm H\alpha}$) to obtain the SFR:
\begin{equation}
    \log {\rm SFR}_{\rm H\alpha}({{\rm M}_{\odot}\,\rm yr^{-1}}) = \log L^{\rm corr}_{\rm H\alpha} ({\rm erg\,s^{-1}}) -  41.27,
\end{equation}
assuming the same Chabrier IMF.

A comparison between these two SFR estimates is shown in Fig.~\ref{SFR_MASS}.

Previous studies of the SFR from FIR and H$\alpha$ show that SMGs at $z\sim 2$
have much larger SFR$_{\rm FIR}$ than SFR$_{\rm H\alpha}^{\rm corr}$ \citep{Swinbank2004, Chen2020}.

Due to the sensitive H$\alpha$ selection of our HiZELS parent sample,
our sample comprises more typical `main sequence' galaxies, and is not
limited to the most dusty starbursts. Only one of the ALMA-SHiZELS galaxies
has FIR-derived SFR above 100 M$_\odot \,\rm yr^{-1}$. It is therefore not surprising
that the SFRs derived from H$\alpha$ and FIR emission are more similar
for our sample than for literature SMGs.

\subsection{The role of stellar mass and gas-phase metallicity}\label{metalicity}

We consider the gas-phase oxygen abundance as a proxy for metallicity,
and estimate it from the [N\,{\sc ii}]/H$\alpha$ emission line ratio
\citep{Pettini2004, Curti2017} from the near-IR IFU spectroscopy (see
Table~\ref{tab3}). The SHiZELS population has mainly Solar to
sub-Solar values (\citealt{Swinbank2012b,Molina2017}).  We show the
mass-metallicity relation of our ALMA-HiZELS sample in
Fig.~\ref{metamass} and identify the ALMA-detected and non-detected
targets.  We show the mass-metallicity relation at redshift $\sim 2$ from
\citet{2006ApJ...644..813E} as a comparison. In our observations, we
find that the lower the metal content or stellar mass, the weaker the
ALMA continuum emission. Indeed, all of the ALMA-detected galaxies
have [N\,{\sc ii}]/H$\alpha \gtrapprox 0.2$ or $M_*>10^{10.5}{\rm M}_\odot$, corresponding to
12+log(O/H)\,$>8.5$. The typical [N\,{\sc ii}]/H$\alpha$ emission line
ratio for galaxies at $z\sim2$ ranges from 0.03 to 0.3
\citep{Strom2017}, thus our ALMA-detected sample is indeed biased
towards massive and high-metallicity galaxies. As expected,
dust continuum is more easily detected for a
galaxy with higher stellar mass or metallicity.

The ALMA detected targets have stellar mass values about one order of magnitude
higher than the ALMA non-detected targets. Since the SFR of the ALMA-SHiZELS
sample is in the range of 10 to 100  M$_\odot$\,yr$^{-1}$ \citep[within one order of magnitude;][]{Gillman2019},
the ALMA detected targets in this work mainly have low specific SFR
compared to the rest of the SHiZELS sample.

Using the metallicity measurements, we can also derive the gas-to-dust
mass ratio ($\delta_{\rm GDR}$) following \citet{Magdis2012}:
$\log\delta_{\rm GDR} = (10.54\pm1.0) - (0.99\pm0.12)\times
[12+\log(\rm O/H)]$.
We estimate ISM mass using the ALMA-derived 355\,$\mu$m flux,
following \citet{Scoville2016} (Eq 16).
Our derived dust masses are presented in Table \ref{tab3}.
As shown there, these estimates are in good agreement with
the values derived from SED fitting.

\subsection{Dust radius of the ALMA detected targets}
To estimate the dust radius, we fit the $uv$-real visibility of the
ALMA detected targets by {\sc casa} task {\sc uvmodelfit}, and show the results
in Fig. \ref{uv-profile}. We chose the $disc$ model in {\sc uvmodelfit} to fit
the $uv$ profile.
The circularised radius $R^{\rm uvfit}_{\rm dust} = \sqrt{R_{\rm maj}\, R_{\rm min}}$ of our targets are shown in Table \ref{table2}.
Since the FIR morphology is not regular, and thus the disk fitting results
may not represent the flux distribution, we also measure the half-light radius ($R^{\rm half-light}_{\rm dust}$)
of the ALMA images from the surface brightness distribution in the image plane
and show the results in Table \ref{table2}. The FIR surface brightness
profiles in real plane are also fitted by S\'ersic function and can be found in Section \ref{dustsurfacebrightness}.
The different approaches adopted for the measurements of the dust radii all show that the radii are 4-5 $\pm$ 0.5 kpc,
larger than the typical size of the high-redshift SMGs \citep{Ikarashi2015, Simpson2015, Fujimoto2017}.
Dust emission from the four ALMA-detected galaxies is found to extend up to $\sim 2''$ ($\sim16$\,kpc, Fig. \ref{dust-profile}).

\section{Results and discussion}

\subsection{Individual galaxy properties}

Figs~\ref{colorimage} and \ref{ALMAdet1} and \ref{ALMAdet2} show the
{\it HST}, SINFONI and ALMA images of our SHiZELS sample.  For the
galaxies at redshift about 1.47 and 2.23, the {\it HST} F606W filter
corresponds to rest-frame 2400\,\AA\ and 1800\,\AA, therefore these
images are tracing mainly the detectable UV emission, i.e.\ the star
formation that is not obscured by the dust. On the other hand, the
observed {\it HST} F140W image reveals the rest-frame $r-$ or $g-$band
morphology (free of strong line emission), which is more sensitive to stellar mass.  Thus
Figs~\ref{colorimage}, \ref{ALMAdet1} and \ref{ALMAdet2} show proxies
for the stars (F140W), UV-traced star formation (F606W), H$\alpha$-traced star
formation (SINFONI), and dust mass distributions (ALMA).
In this section, we describe properties of our
ALMA-detected targets individually\footnote{Most of our targets have
two versions of the H$\alpha$ maps \citep{Swinbank2012a, Gillman2019}.
The main difference in the H$\alpha$ morphology is
caused by the different S/N criteria to create the H$\alpha$
maps. \citet{Gillman2019} built H$\alpha$ maps with high S/N spectra
while the results in \citet{Swinbank2012a} use all the available
spectra, which would then trace more extended H$\alpha$ emission.}.

We caution that morphological information derived from the rest-frame
UV/optical can be potentially very misleading in sources with substantial
dust extinction and on-going star formation and in particular it is
difficult to trace the true stellar mass \citep[see ][]{Lang2019}.

\begin{itemize}
\item {\bf SHiZELS-7}: The H$\alpha$ kinematics reveal the presence of
  an extended disc-like rotating structure. Two H$\alpha$ star-forming
  clumps, separated by 4\,kpc, are identified by \citet{Swinbank2012a},
  although the fainter clump is not seen in \citet{Gillman2019}
  because of the different S/N criteria. The FIR continuum is spread
  over a diffuse structure. The two H$\alpha$ clumps are not likely to
  be affected by significant dust obscuration, so there might be no
  massive dust and gas clouds associated with the H$\alpha$ features.
  The {\it HST} F140W and F606W images show that the least obscured regions in this galaxy
  show a compact stellar core and a extended UV morphology.

\item {\bf SHiZELS-9}: shows an extended rotation-dominated structure
  in H$\alpha$ with three bright clumps \citep[separated by $\sim$ 3\,kpc,][]{Swinbank2012a}. The FIR continuum shows a
  V-like structure in the central 3\,kpc, linking a bright stellar
  core with a fainter one. A third stellar core shows both UV and FIR
  emission.

\item {\bf SHiZELS-11}: This source was classified as a disk galaxy
  with a compact H$\alpha$ structure \citep{Swinbank2012a};
  although a newer analysis shows a marginally extended morphology
  \citep{Gillman2019}. SHiZELS-11 has an active galactic nucleus (AGN)
  identified in the X-rays by {\it XMM-Newton} and in the radio by the
  Very Large Array \citep[VLA ---][]{2006MNRAS.372..741S,
    2008ApJS..179..124U}.
SHiZELS-11 is also detected by {\it Chandra} in X-UDS survey \citep{Kocevski2018}, with X-ray luminosity is $ L_{X} = 10^{43.3} $ erg $\rm s^{-1}$.
The velocity dispersion of H$\alpha$ is about 90\,km\,s$^{-1}$
  \citep{Gillman2019}, much less than the typical velocity dispersion
  of type-I AGN, implying that the AGN in SHiZELS-11 must be
  obscured. Rotation is not clear from the H$\alpha$ dynamics, and the
  position of the maximum velocity dispersion is offset from the
  brightest H$\alpha$ pixel \citep{Gillman2019}. The {\it HST} F140W
  image shows a smaller source to the south, which may suggest a close
  merger or dust lane. The source has an apparently high metallicity
  and a steep metallicity gradient \citep{Swinbank2012a}, which might
  be due to contamination from an AGN. Both UV and FIR are bright in
  the galaxy centre, while the rest-frame optical is mainly coming from
  a clumpy structure surrounding the centre. The ALMA continuum shows compact and extended
  emission, which does not overlap with the H$\alpha$.

\item {\bf SHiZELS-14}: This galaxy has been identified as a merger
  with three H$\alpha$ clumps separated by $\sim$ 5\,kpc
  \citep{Swinbank2012b}. The H$\alpha$ morphology in
  \citet{Gillman2019} is less clumpy, but still extends to a half-light
  radius of about 7\,kpc (Sersic model fitting results). The H$\alpha$
  kinematics show a velocity-dispersion-dominated system. The galaxy
  has the highest metallicity in the SHiZELS sample of
  \citet{Swinbank2012a}. The full extent of the H$\alpha$ emission is
  not traced by the rest-frame UV imaging. The ALMA continuum emission
  shows one dominant compact component at the centre, and more
  extended emission following a similar orientation as the F140W
  morphology. The FIR emission spreads up to $2''$,
  i.e.\ $\sim$16\,kpc at $z=2.23$. This target is comprehensively studied
  by Cochrane et al. (in preparation), including new Jansky VLA data.

\end{itemize}

\begin{figure*}
\centering
\includegraphics[width=0.98\textwidth]{LIR-Reff-1.eps}
\caption{Comparison between different surveys, local and high-$z$,
with previous spatially resolved FIR observations.
We show our ALMA-HiZELS galaxies (red dots), the galaxy sample from
KINGFISH \citep[green filled circles][]{Kennicutt2011},
GOALS \citep[green cross filled circles][]{Armus2009, Chu2017},
DANCING-ALMA with S/N of $L_{\rm FIR}$ higher than 5 \citep[cross filled blue circles][]{Fujimoto2017}
and the recent ALMA observation results of the SCUBA-2 bright galaxies \citep[purple diamonds]{Gullberg2019}.
The figure shows that our ALMA-SHiZELS are fainter than
observations of typical sub-millimetre bright galaxies at similar redshifts, and also present larger sizes.
The sizes of the SHiZELS galaxies compare better with those of low-redshift star-forming galaxies from KINGFISH and GOALS.
}
\label{LIR_RE}
\end{figure*}

\begin{figure*}
\centering
\includegraphics[width=0.47\textwidth]{HiZELS-Re-Swinbank-deconv.eps}
\includegraphics[width=0.47\textwidth]{HiZELS-Re-F140W-deconv.eps}
\caption{
 {\bf Left panel: }Comparison of the half-light radii measured in the ALMA
  continuum imaging with respect to those measured in H$\alpha$
  \citep{Swinbank2012b, Molina2017}. We also overplot the {\it
    Herschel} 350-$\mu$m and narrow-band H$\alpha$ radii (obtained
  after convolving both to the same resolution) from the
  KINGFISH \citep{Kennicutt2011} and {\it Spitzer} Infrared Nearby
  Galaxies Survey
  (SINGS) projects \citep{Kennicutt2003, Dale2005, Dale2007}. Our
  high-redshift galaxy sample shows a broadly similar behaviour as is seen in
  these local galaxies, except SHiZELS-11 which shows a significantly
  larger radius in the FIR than in H$\alpha$. We also show the recent
  ALMA-resolved SMG sample at $z\sim2$ \citep{Chen2020} and one
  starburst galaxy (GOODSN-18574) at $z=$\,1.25 \citep{Nelson2019}.
{\bf Right panel:} The stellar mass size as derived from the {\it HST}
F140W image compared to the FIR size as derived from the ALMA observations.
We show the H$\alpha$ selected main sequence star-forming galaxies at redshift about 2.2-2.5
by \citet{Tadaki2017}, the star-forming galaxies presented
by \citet{Rujopakarn2016}, the z$\sim$2 SMGs from \citet{Lang2019},
and the massive star-forming galaxy sample at z$\sim$2 from \citet{Tadaki2020}.
The dot line shows the one-to-one relation.
Our targets are roughly the largest galaxies in both rest-frame optical band and FIR radius,
and may evolve into massive disk galaxies.
}
\label{HiZELS-Re}
\end{figure*}

\subsection{Spatially resolved properties}
\subsubsection{The dust emission from $z=1.47$ \& 2.23 galaxies}

Previous sub-millimetre studies of high-redshift galaxies at high spatial
resolution have revealed that clumps at $\sim$1\,kpc scales do not
particularly dominate the total flux emission, as is often seen in UV
or H$\alpha$ imaging \citep{Hodge2019}. For example, \citet{Hodge2016} used ALMA to
observe a sample of $z\sim2.5$ submillimeter galaxies (SMGs) at $0\farcs16$ resolution and
found that the observed 870$\mu$m continuum morphologies are
predominantly smooth and disc-like with typical radii of
$\sim 1.8$\,kpc. \citet{Gullberg2019} also shows that dust emission size from SMGs is
about $\sim 1.5$\,kpc at $z \sim$\,1--4, with a larger sample.

Although these previous studies have revealed the internal properties
of the brightest SMGs, our focus is on the normal star forming galaxy population
\citep[i.e. galaxies selected by H$\alpha$ flux, with many having $\lesssim L_{\rm H\alpha}^*$][]{Swinbank2012a} at high redshift.
We find that our sample shows sub-millimetre continuum emission which is $\sim2\times$ more extended than
that seen in SMGs at $z\sim3$.
In the local universe, it is well known that ULIRGs present compact star-formation cores,
which may eventually lead to a compact stellar core. The large FIR radius of our ALMA-HiZELS
observations reveal the existence of a high-redshift galaxy population with extended
star-formation activity at $z=1.47$ or 2.23, possibly sustained in thick rotating disc-like
structures.

In Fig.~\ref{LIR_RE} we compare our results to previous spatially resolved FIR studies.
For the galaxies at $z=0$ and $L_{\rm FIR}<10^{11}L_\odot$,
the Key Insights on Nearby Galaxies: a Far Infrared Survey with {\it Herschel}
project \citep[KINGFISH;][]{Kennicutt2011} surveys have found a typical radius
of about $\sim$4 kpc with predominately disc-like morphologies \citep{Mosenkov2019}.
For isolated LIRGs taken from the Great Observatories
All-sky LIRG Survey \citep[GOALS, ][]{Armus2009, Chu2017} we also find relatively large FIR sizes, similar to those from KINGFISH.
To have enough spatial resolution, we measure the GOALS galaxy FIR size based on the
{\it Herschel} PACS 160$\mu$m image. The difference between the FIR radius in 160$\mu$m and 350$\mu$m
is about 1.5 times or less \citep{Mosenkov2019}, which will not affect our results.
Some of the LIRGs in GOALS sample are galaxy pairs or merging galaxies. To avoid the contamination
from the neighbours, we only make use of the isolated galaxy sample here.

On the other hand, Demonstrating a New Census of Infrared Galaxies with ALMA \citep[DANCING-ALMA, ][]{Fujimoto2017}
project presents $\sim$1000 galaxies ($0<z<6$ mainly ULIRGs) resolved
by ALMA at 1\,mm and finds a positive correlation between the radius
and $L_{\rm FIR}$ (in Fig.~\ref{LIR_RE} we only chose $1<z<3$, $S/N>10$ galaxies).
The recent work by \citet{Gullberg2019} shows compact FIR emission for $\sim$ 150 SMGs,
when the IR luminosity of the galaxy exceeds $10^{12}L_\odot$.

Our ALMA-SHiZELS sample is different from the previous luminous high redshift
dusty populations as we are targeting a much fainter population. As shown in Fig. \ref{LIR_RE}
and Tab. \ref{table2}, our sample has typically lower IR luminosity, larger dust size
than the high-redshift SMGs, which suggests that our survey are targeting the high-redshift
star-forming galaxy population, rather than the high-redshift starburst galaxies.

The extension of the dust emission ($R_{\rm dust}$) could be roughly estimated
from a theoretical point of view, assuming $L_{\rm FIR} = 4\pi R_{\rm
  eff}^2\sigma T_{\rm mbb}^{4.32}$, where $\sigma$ is the
Stefan-Boltzmann constant, and the dust temperature ($T_{\rm mbb}$)
and $L_{\rm FIR}$ are
derived from SED templates (see \S~\ref{Sect3.1}; \citealt{Ma2015,
  Yan2016, Dudzeviciute2020}). This effective radius can be considered as the lower size
limit of the galaxy FIR emitters, hence the difference with respect to
the half-light radius could be understood as the spatial occupation of
dust structures below the resolution elements. Using this equation, we derive effective
radii for our SHiZELS galaxies of 0.3--1.1\,kpc, much smaller than the
observed half-light radii of about 4.5 kpc, implying typical dust filling factors from
5 to 10 for our sample. \citet{Hodge2019} have found that at 500\,pc
resolution they can see tentative evidence of the spiral and bar structures of SMGs ($z=1.5-4.9$)
at $\sim$250\,$\mu$m (rest-frame). Subject to surface brightness limitations,
higher resolution ALMA imaging might reveal similarly complex structures in our galaxies.

\subsubsection{Spatial correlation between dust and ionised gas}

The observed morphologies of dust and H$\alpha$ emissions are well known
to be correlated (at kpc scales) for samples of local star-forming galaxies,
such as the KINGFISH project \citep{Kennicutt2011}. In the left panel of
Fig. \ref{HiZELS-Re} we show that if we compare the half-light radii measured by
ALMA with respect to the H$\alpha$ emission, we see good agreement for
sources SHiZELS-7, -9 and -14, suggesting spatial coexistence (at $\sim$ kpc scales)
of the dust and the ionised gas. In contrast, the source presenting an AGN,
SHiZELS-11, shows a significantly larger FIR radius than that seen in H$\alpha$.

We compare our results to the recent high resolution ALMA and H$\alpha$ observations of
a sample of $z\sim 2$ SMGs \citep{Chen2020} and one starburst galaxy \citep{Nelson2019}
in the left-hand panel of Fig.~\ref{HiZELS-Re}. We find that our sample has a similar H$\alpha$ radius
to previously observed SMGs, suggesting extended star formation for these high-redshift
galaxies. Despite this agreement, the dust emission from SMGs is typically more compact than
our galaxies \citep{Gullberg2019}.
The starburst galaxy in \citet{Nelson2019} has a dust radius higher than the SMGs, but
still lower than our sample.

Although the SHiZELS sample shows a larger dust radius than the SMGs and starburst galaxy,
most of the high-redshift galaxies in Fig. \ref{HiZELS-Re} have similar H$\alpha$ radius of about 4 kpc.
So the SMGs appear also to have an extended star formation region, as well as a compact dusty
core in the galaxy center (e.g., Fig. \ref{LIR_RE}). SMGs may obscure H$\alpha$ emission especially
in the center kpc region, so the H$\alpha$ distribution in the SMG center might be more flatter, leading to a larger
H$\alpha$ half-light radius. Since H$\alpha$ in SMGs can be bright and extended \citep{Swinbank2004, Swinbank2006},
while the dust morphology is compact \citep{Rujopakarn2019, Chen2020}, the large dust radii we observe in ALMA-SHiZELS
sample may caused by the low SFR ($L_{\rm H\alpha} < L^*_{\rm H\alpha}$) of the SHiZELS sample,
rather than with the H$\alpha$-selection method.

The strong dust extinction in SMGs may also affect the H$\alpha$ emission
such that the SFR derived from H$\alpha$ is lower than the SFR$_{\rm FIR}$ (Fig. \ref{SFR_MASS}),
even though both SFR indicators may only reflect one aspect of the star formation
and may still lower than the intrinsic SFR in galaxies.

The SHiZELS sample was selected on H$\alpha$, down to a flux limit that traces below the knee of the luminosity function,
and therefore the bulk of the sample will be less dusty than submm selected galaxies.
Our results show that the SHiZELS galaxies have very similar
dust and H$\alpha$ radii as the star-forming galaxies from KINGFISH at low redshift (Fig. \ref{LIR_RE} and \ref{HiZELS-Re}).
In the low-redshift universe, most of the star-forming galaxies are found to be spiral galaxies with low star-formation
efficiency over an extended large disk \citep[e.g., ][]{Leroy2008, Cheng2018},
while ULIRGs usually have a more violent compact nuclear starburst in the galaxy center \citep{Solomon1997, Downes1998}.
The similarity between the bulk of the ALMA-SHiZELS sample and the KINGFISH sample in Fig. \ref{LIR_RE}
and \ref{HiZELS-Re} is in line with the two samples tracing more similar modes of main sequence star formation,
compared with the extreme starburst modes witnessed in SMGs.

H$\alpha$ clumpy features are commonly found in high-redshift galaxies \citep{Genzel2006, Swinbank2012b}.
However, our ALMA continuum images do not show clear counterparts of the H$\alpha$ clumps,
at least at $\sim$\,kpc scales (Fig. \ref{colorimage}).
It may be that the observed clumps are not tracing true star-forming clumps,
but less dusty regions of the galaxy, from which the H$\alpha$ can escape \citep{Swinbank2004}.

\subsubsection{A comparison between the {\it HST} and ALMA morphologies}

The {\it HST} F140W images of our sample which trace the rest-frame optical emission
(Fig. \ref{ALMAdet1} and \ref{ALMAdet2}), reveal that only SHiZELS-9 has an apparently dual stellar core (the two cores have similar fluxes),
which may be evidence of a major merger, or caused by a dust lane. SHiZELS-11 and -14 may both be undergoing or recently have undergone a minor merger event.

Spatial offsets between the rest-frame optical and FIR observations
have been found in low and high-redshift (U)LIRGs \citep{Charmandaris2004,  Hodge2016}.
In Fig.~\ref{colorimage} we see the spatial offsets and the overlap between the F140W and ALMA emission.
For SHiZELS-9, the two major (rest-frame) $V$-band cores present dust emission, while additional FIR
emission comes from a region connecting to the third $V$-band core.
The $V$-band flux distribution does not always follow the H$\alpha$ or the dust morphology in our sample.
A detailed study of spatially resolved dust extinction maps
and the IRX-$\beta$ relation \citep[the FIR and UV luminosity ratio versus the UV SED slope, ][]{1999ApJ...521...64M}
of our high-redshift star forming galaxies will be presented in a forthcoming paper.

The rest-frame UV images also show complex morphologies. Compared to the detected FIR emission from SHiZELS galaxies,
the UV morphologies are extended and clumpy. For the ALMA non-detected galaxies, SHiZELS-10, -2, 3, and -21,
the rest-frame UV and optical band images show compact cores at their centres (Fig. \ref{ALMAdet2}),
evidencing compact UV star formation cores or regions of lower obscuration which is also found in the low-redshift low mass galaxies \citep{Cheng2020}.
We see that $z\simeq 2.23$ galaxies display more compact rest-frame UV morphologies than the $z\simeq 1.47$ sample, which is
consistent with previous studies \citep{Paulino2017}.

We show the half-light radii of the F140W emission in the right panel of Fig.~\ref{HiZELS-Re}.
The F140W radii (adopted from \citet{Gillman2019}) have typical effective radii of $\sim$\,4.5\,kpc,
consistent with the typical size of the full HiZELS sample \citep{Stott2013}.
Using the stellar masses for our targets to predict half-light radius based on the mass-size relation \citep{Suess2019},
we find that the size revealed by the F140W imaging are consistent with the predicted radius within 1$\sigma$.
We also present the galaxy sample from \citet{Rujopakarn2016} composed of star-forming galaxies at redshift $\sim 2$,
observed by ALMA (870\,$\mu$m, 1.3\,mm) and VLA (5\,cm) at 0\farcs4, the H$\alpha$ selected main sequence star-forming galaxies from \citet{Tadaki2017},
the SMGs at redshift 2 observed by ALMA 870 $\mu$m from \citet{Lang2019}
, and the recent ALMA 870$\mu$m observation results of the massive star-forming galaxies at redshift 2 \citep{Tadaki2020}.
in the right panel of Fig.~\ref{HiZELS-Re}. \citet{Tadaki2017}'s sample of proposed elliptical progenitor galaxies has systematically
smaller FIR size similar to other SMGs, suggesting the future formation of compact red cores. Our targets are roughly the largest galaxies in both rest-frame optical band and FIR radius.
The large FIR radius indicate the stellar mass is assembling at a larger radius, thus our targets would evolve into massive disk galaxies.

\section{Conclusion}

We present high-resolution ($0\farcs25$) ALMA continuum observations
(rest-frame $\sim355\mu$m) of nine star-forming galaxies at redshift 1.47
and 2.23, taken from the HiZELS survey. These galaxies have been observed with previous
AO-aided IFU H$\alpha$ spectroscopy and {\it HST} at similar resolution,
facilitating a spatial exploration of the star formation at high-redshift
at kpc scale resolution. Our sample comprises a population of star-forming
galaxies at redshift 1.47 and 2.23, which are mainly `main sequence'
galaxies, and have H$\alpha$ luminosities close to or below $L_{\rm H\alpha}^*$ at their redshift.

We detect four out of nine galaxies with ALMA. Their morphologies present extended faint structures,
out to 16\,kpc in diameter, much larger than the typical FIR size of sub-millimetre galaxies at high redshift.
Our ALMA observations also reveal two serendipitous detections within the ALMA primary beams.
Both of these are detected in previous optical and NIR surveys, located at different redshifts.
For the ALMA non-detected galaxies, we find they mainly have either lower stellar masses ($M_*<10^{10.5}{\rm M_\odot}$)
and lower [N\,{\sc ii}]/H$\alpha$\,$<0.25$ ratios, corresponding to 12+log(O/H)\,$<$\,8.5.

The SFR derived from FIR and dust corrected H$\alpha$ are consistent with each
other within 1$\sigma$. However, the spatially resolved FIR and H$\alpha$ morphologies do not
show a similar distribution, implying a complex distribution of the ISM state in these galaxies.
At least at $\sim$kpc scales, the H$\alpha$ emission do not show a clear spatial correlation
with respect to the FIR emission. We find that the brightest
H$\alpha$ clumps, previously identified via AO-aided IFU spectroscopy,
are not significantly spatially correlated with the dust continuum emission which traces the bulk of the ISM, which appears smooth.

Our sample of SHiZELS galaxies have a typical rest-frame FIR size twice larger than the SMGs at high-redshift,
while the H$\alpha$ emission size of our sample and SMGs are similar. The similarity between the
extent of the dust continuum emission, and IR luminosities of our sample and the local star-forming disky galaxies
is in line with our sample being drawn from the `normal' star-forming galaxy population at z=1.5-2.2.
The dust continuum emission in these systems is dominated by a cool extended component,
while in more active galaxies such as SMGs, compact nuclear starbursts dominate the dust emission \citep{Gullberg2019}.

\section*{Acknowledgements}
This paper benefited from a number of thoughtful comments made by the anonymous referee.
C.C.\ appreciates useful comments from Dr.\ Wenda Zhang.
This work is supported by the National Key R\&D Program of China grant 2017YFA0402704.
C.C. is supported by the National Natural Science Foundation of China (NSFC), No. 11803044, 11673028, and
J.H. is supported by the NSFC, No. 11933003. E.I.\ acknowledges partial support from FONDECYT
through grant N$^\circ$\,1171710. SG acknowledges the support of the Science and Technology Facilities Council through grant ST/N50404X/1 and ST/L00075X/1.
IRS acknowledges support from STFC (ST/T000244/1).
PNB is grateful for support from STFC through grant ST/R000972/1.
This work is sponsored in part by the Chinese Academy of Sciences (CAS), through a
grant to the CAS South America Center for Astronomy (CASSACA) in
Santiago, Chile.
This work was supported by the National Science Foundation of China (11721303, 11991052) and the National Key R\&D Program of China (2016YFA0400702).
A.E. acknowledges partial support from the Center of Excellence in Astrophysics and Associated Technologies (AFB-170002) and FONDECYT Regular Grant 1181663.
This paper makes use of the following
ALMA data: ADS/JAO.ALMA\#2012.1.00402.S, ADS/JAO.ALMA\#2013.1.01188.S,
ADS/JAO.ALMA\#2015.1.00026.S. ALMA is a partnership of ESO
(representing its member states), NSF (USA) and NINS (Japan), together
with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of
Korea), in cooperation with the Republic of Chile. The Joint ALMA
Observatory is operated by ESO, AUI/NRAO and NAOJ. A work based on
observations collected at the European Organisation for Astronomical
Research in the Southern Hemisphere under ESO programmes 082.B-0300(A)
and 092.A-0090(A). This research is based on observations made with
the NASA/ESA Hubble Space Telescope obtained from the Space Telescope
Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5--26555. These observations are associated with program 14719.

{\it Data availability:} The data underlying this article
are available in http://almascience.nrao.edu/aq/ and
https://archive.stsci.edu/index.html, and can be accessed
with ALMA project ID: 2012.1.00402.S; 2013.1.01188.S;
2015.1.00026.S and HST proposal ID: 14719

redpajama_set_name: RedPajamaArXiv


Butter is molded by hand with wooden palet in bricks or in "custom made" portions for the great chefs with the salt content, shape and weight they want, depending on their desires.
Bordier butter can be found in the best creameries, throughout France and in a few other countries.
Son of a cheese maturer, Jean-Yves Bordier defines himself as a cheese chooser and refiner. He selects his cheeses for the quality of the artisans who made them. Our team, in our maturing cellars, brings those cheeses to optimum stage of savouring. Maturing is a fundamental step during cheese production, a whole role!


All employees are set up within the Employees menu in the same manner.
At employee level, the employee's pay frequency must be selected at the time of setting up the employee record - from this BrightPay will recognise which frequency of pay is required for the employer.
In addition to the pay frequency, the employee's rate of pay to be applied to their payslip is also to be entered at this setup stage.
Whilst the rate of pay for the first payslip is applied from the employee payment record, this is of course available to amend as required, before the payslip is finalised.
Once the first payslip is finalised, the pay from the previous payslip is copied forward. Therefore subsequent payslips do not take the rate of pay from the employee payment record, it is taken from the previous payslip instead.


My target point was met, so I sold my puts. I've switched to longs. I think in the short-term this market will become bullish . Overall, I'm still bearish .
Comment: Wow, that's my first post from my phone. What a crappy picture!
Trade closed manually: Strong start but failure to hold, so I'm out.
can i ask. what's your target?
@yogamarc, I'm actually trying to figure that out now... I'm currently guessing around 2500 on SPX (+/-10).
@yogamarc, will do. I am disappointed with the rebound. Pretty weak. I normally would sell at this point but I'm going to gamble here and wait it out a little bit.


text:
Despite thunderstorms, high school sports are now underway
StarNews Sports Department
The first day of high school football practice started with a bang, as usual. It was the boom that caught everyone off guard.
Rain, thunder and a little lightning scrambled a few plans, but there were still players in helmets and coaches barking out orders across Southeastern North Carolina on Thursday morning and into the evening.
The StarNews will be checking in with schools from across the area over the next week to see how things are going. Be sure to check back at StarNewsVarsity.com for plenty of photos and updates between now and opening night on Aug. 23.
Hoggard
The summer left the Vikings' practice field lush and green for the opening day. Another night – and morning – precipitation meant that sections of it were already a muddy mess 30 minutes into the first practice.
Yet the 100-plus players on the field were moving quick and feeling great, even if the instruction had to be original at times.
Braswell related to his offensive linemen that pass blocking was like playing man-to-man defense on the basketball court, "and that your quarterback is the hoop."
"The one thing I do think," he said during the ensuing break, "maybe the guys would have taken the field with a lot of enthusiasm either way, but I think this cool break … kids are kids. It felt a little like playing football in the rain."
Braswell, in his 17th season at Hoggard, said he couldn't ever remember rain on the first practice day.
"I woke up with the thunder about 1:30 (a.m.) and thought, 'No! No way!' But then I thought, it's OK. It's 1:30, it'll be out of here. And then of course it wasn't."
The Buccaneers trotted onto the practice field Thursday morning as drizzle increased into a light rain. They ran drills on the front lawn of the school, where the turf seems to drain much better than it does in the stadium or adjacent practice field.
In a pre-practice huddle, Laney head coach Greg Ditz weeded out a couple of players who still needed physical forms on file. He stressed the schedule and what he expected early on from his roster.
Ditz said he had over 170 players during summer workouts. He was not sure about the exact number for Thursday, adding players are still signing up.
"The numbers are definitely up from a couple of years ago," Ditz said. "So we're excited about that."
As the rain and the workouts increased in intensity, Ditz wore a towel around his neck as he corrected miscues and instructed receivers on short passing routes.
Head coach Kevin Motsinger called off his first official session, as the turf at the 13th and Ann streets practice facility had taken on too much water.
The staff moved the players inside Jap Davis Field House to work on film study, white boards, walk-throughs, fundaments, alignments and assignments.
"A lot of it's little stuff," Motsinger said "But it's very important stuff. The little things make the big things. So today's kind of a little-thing day and a mental day."
Between now and the run-up to the first preseason games, "We've got to really improve the mental understanding. You've got to know what we're asking you to do.
"Today, that's what we're spending all our time on."
"I don't like people wasting my time so I don't waste the kids' time," Motsinger said. "So we wanted to maximize this time that we're allotted."
New Hanover has the fewest number of bodies in camp in the Motsinger era, at 118. He said he started his first year at the school with 175 players.
Garry Bishop's North Brunswick squad took the field early Thursday evening, and most of the first practice was spent on fine-tuning the team's new up-tempo spread offense.
"We'll be calling stuff from the line, so that's why we did that," Bishop said about a no-huddle drill the Scorpions spent about 10 minutes on.
The coaching staff was already in midseason form with their one-liners. During the drill, one of the linemen who was tiring let out a "God." An assistant responded back, "I heard 'God.' Yeah he's watching."
During a JV drill, the team had a hard time getting quiet in the huddle, and another assistant barked at the kids, "Backline, you aren't worried about what you're having for dinner."
About 70 kids were at the first practice, and Bishop said he expected to have between 85-95 when everyone showed up.
With only about 50 total kids coming to summer workouts, Ashley coach Tom Eanes knows his kids are going to have to be prepared to play on both sides of the ball this year.
That's why the Screaming Eagles did both offensive and defensive drills during their first day of practice.
"We just don't have a lot of numbers," said Eanes, who is beginning his third year with the program. "For whatever reason, they aren't here and that's the way it is."
Eanes has seen a big difference in how the first day of practice runs since he began coaching. With new rules in place, kids are working out with the staff all summer long.
"Nowadays with football the way it is, it's kind of just a continuation of the whole summer, so I don't think (the first practice) is much of anything new like it used to be in the old days," Eanes said.
- From staff reports

redpajama_set_name: RedPajamaCommonCrawl


Twitter Novels are one use of Twitter that many of us would never consider – but there's a growing number of Twitter Novelists exploring the medium. Today Brandon J. Mendelson, author of The Falcon Can Hear The Falconer (a Twitter Novel) gives some tips for writing Twitter Novels.
A word of caution: As far as English language Twitter novels go, this is new territory. Based on early results, as compiled by ReadWriteWeb, there have not been any success stories. RWW never spelled out what would be defined as a success, but I took their comments to assume no Twitter novelists have crossed into the mainstream or made money. It may be only a matter of time before this changes.
What I'm presenting here are suggestions on how to write and operate your new Twitter novel based on my experience writing "The Falcon Can Hear The Falconer". I hope what I'm proposing will provide a blueprint for interested writers to create successful Twitter novels.
Twitter is instantaneous. Serializing a manuscript may be easy, but trying to contract and make logical sense of it in 140 character bursts is not. By doing this, you limit the flexibility that Twitter grants in presenting your fiction. Start fresh.
Although there's no need for a manuscript, you should know where the story is going. I found writing a scene for a play to be more helpful than translating a manuscript for Twitter. The formatting for a scene provides more freedom to work within the spaces you've created and allow the story to grow organically. Don't hesitate to explore.
What's great about a Twitter novel is that your content is no longer static. Depending on how committed you are, you could have events happen in real time using services like Tweetlater.
If a character is mugged at 6am, you could post a police announcement on the Twitter novel looking for the perpetrator. What are the characters listening to on the radio? Is someone calling them that's important to the story? Use Twitpic to show a photo of one of your friends or an actor to show the reader who is calling or what the mugger looks like.
The post doesn't have to be from your outline, it could be something within the environment that adds to the story.
More than five Twitter posts on any given day can be dangerous. You'll induce reader fatigue, and new readers will get lost quickly.
Simply put: Each tweet should move the story forward in some way. If it doesn't, cut it.
Finally, you may have readers follow you after the novel has started. I recommend setting up a simple website that contains the story's updates from where it began. Include this link on your Twitter page. Occasionally remind readers on days that you do not update that they can catch up at this website.
The format is still new, but it won't be long until we start to read about successful Twitter novelists getting publishing deals. Why? A large following equates to a large potential customer base. If you can show you have a customer base, you are better positioned to land a book deal.
Best of luck to you on your literary journey.


text:
Lee disappointed by India rift
New Allan Border Medallist Brett Lee admitted here on Wednesday he was disappointed by the continuing ill will between Australia and India.
After a summer of simmering tension stretching back to the contentious second Test at the Sydney Cricket Ground (SCG), relationships between the sides are again strained after a controversial tri-series one-day clash in Sydney on Sunday. Teenage Indian paceman Ishant Sharma was fined after a verbal clash with Andrew Symonds during the game, with the Indians making an official complaint about the "provocative" behaviour of the Australians.
On Tuesday, Australian opener Matthew Hayden called Harbhajan Singh an "obnoxious weed" on radio. Lee, who has a close affinity with India and has a small part in an upcoming Bollywood film, said he hoped the teams could put the controversies behind them and concentrate on their cricket when the tri-series finals start on Sunday.
"It's a bit of a shame a few things have happened on the cricket field, people know where the line in the sand is and if you cross that line well you know you will get dealt with," Lee said. "The thing we have to acknowledge too is that once you do walk onto the cricket field and go over that line it doesn't matter whose made friendships, it's very important we go out there and play the hardest, toughest, fairest cricket we possibly can," he added.
Lee was still basking in the glow of winning his first Allan Border Medal, awarded to Australia's best player for the previous 12 months, on Tuesday evening. Having cooled his heels on the fringes of the Australian team earlier in his career, Lee is thriving on the added responsibility of leading the attack in the absence of retired champions Glenn McGrath and Shane Warne. He said past frustrations only made him more determined to succeed in Test cricket.
"It made me very hungry and it made me appreciate the chance to wear the baggy green cap once it was taken away, and to never become complacent," he said. "To appreciate the good times you've got to go through the bad I think. "Everyone's been through it, people have had time on the sidelines. Players have had times where they've missed out through injury, I think it comes down to how much you want it," he added.
More on:Andrew Symonds, Australia, Brett Lee, Harbhajan Singh, India, Ishant Sharma, Matthew Hayden
This entry was posted on Thursday, February 28th, 2008 and is filed under General, Cricket.
Tagged with: Andrew Symonds, Australia, Brett Lee, Harbhajan Singh, India, Ishant Sharma, Matthew Hayden
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Lorgat says Tests must stay No. 1
Bangalore's match in Jaipur to go ahead as scheduled
Sizzling Jayasuriya pounds Chennai


The Handbook of Optical Constants of Solids gathers data from different papers to list the kappa values along with the wavelengths; consistency is not maintained. I show you the graph found in the handbook along with the excel plots of the absorption coefficients that my arrays are based on so the user can quickly see if the calculated value makes sense.
The Silicon, Gallium Arsenide, and Indium Phosphide kappa values come from a linear interpolation of data found in Handbook of Optical Constants of Solids that is found here. However, Geranium is pulled straight from the Handbook of Optical Constants of Solids and is why there are several "jumps" in the excel plot as different reported research doesn't match up. For this reason the "Warning" display is provided to inform you when you have fallen into this questionable range. The Excel graph below shows the inconsistencies of Geranium while the other graph shows the general flow of the constants.
Handbook of Optical Constants of Solids, edited by Edward D. Palik, (1985), Academic Press, NY.
Maintained by ECEn IMMERSE Web Team.
Copyright © 1994-2009. Brigham Young University. All Rights Reserved.


Synopsis Drama Caught in between an ethnic war, Bee struggles between love and death.
Synopsis Drama Debt collector Bruce has unusual collection methods, including torture by rock music.
Synopsis Drama Six Days (Kathy Chow) has been in prison since she was 18.


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To increase viewers traffic, and to raise audience satisfaction levels, try these top 5 takeaways.
You must be asking yourself, "How do I make a video fun to watch?" This is how: Offer audiences rich content and personalized messages. In addition, it should be easily manipulated like in a video or computer game. And allow people to interact with your video. They should be asking themselves, what would I do?.
Think of yourself as a reporter, and find a specific topic you would like to talk about on your channel. It's like shopping in the supermarket, you are a customer looking for a product. You may read it's ingredients and information about it on the box and then make a descision on whether to buy it or pass on it. Simlarly, decide on what your story is about and then add the necessary ingredients. In other words, the content of the video should be very entertaining and interesting to watch. Try a topic that can be interesting to both males & females, adults or children. Research the insights of the current story & then carefully shaped the details. Simultaneously outline the differnt messages to add to your story or idea.
I doubt you are interested in promoting your video more than you are in promoting yourself. That means you will need to prepare yourself before you begin. Usually standing in front of a mirror gives you a good idea about how your expressions & gestures will look on camera. Acting is a talent, but having said that, experience is what makes you a good actor. Are you prepared? If you are not fully prepared and confident in yourself, don't press that record button.
Adding a nice introduction in the beginning of your video is a good idea. It should not be longer than 15 seconds. Nowadays there are many editing software packages under $70 that would do the trick. I've used cyberlink "Power Director" software for some of my videos, and with the press of a button, the software edits and adds effects for you. All you need to do next is to upload your video to the internet. For better quality, it is best is to compress your video to 720p pixels HDTV High Definition video mode, which is 1280 x 720. Remember, don't make your compression too high, as it will slow down the viewing.
When you upload your video and post it on YouTube, Vimeo or other website, the best thing to do is to let others know about it. And the best way to do that is through social media sites, such as Facebook and Twitter. Search engines pay specific attention to social media accounts in realtime searches, and if your video is entertaining, you will start noticing an increase in traffic over the next few days or few months. Good luck, and mostly, have fun !!!


This typical Italian dish is really easy to make. The filling is open to different versions and innovation, but the traditional one is the following: you can stuff the artichokes with ham, salami, egg, Parmesan or Pecorino Romano, slices of bread melted in milk.
Tubettini with Piattoni beans means a particular type of green beans with a flat shape. You should prepare it with fresh tomatoes or tomatoes puree and a "soffritto" of onions (white for a sweeter flavour or red to gain more consistency).
Pizza Chiena is a southern Italian pie with a variety of cheese, cold cuts, and eggs in a bread crust. Traditionally made on Good Friday to be eaten on Easter Sunday or to be taken on the traditional Easter Monday picnic, the pizza can be made using cubes of meat and cheese instead of slices.


text:
TMCP 58: Self-Promotion Without Promoting Self [Terry Whalin]
Do you ever struggle to promote your business or brand? Maybe you find it hard to strike a balance between featuring your content or products while keeping your life anchored in God.
Terry Whalin is certainly no stranger to marketing. As someone who has over 195k followers on Twitter and the author and editor of over sixty books, Terry understands the importance of promoting material. But in doing so, he strikes a balance between humility and content promotion that many find it hard to maintain.
If you are a small business owner, this podcast is a MUST LISTEN!
W. Terry Whalin understands both sides of the editorial desk–as an editor and a writer. He worked as a magazine editor and his magazine work has appeared in more than 50 publications. A former literary agent, Terry is an Acquisitions Editor at Morgan James Publishing. He has written more than 60 books through traditional publishers in a wide range of topics from children's books to biographies to co-authored books. Several of Terry's books have sold over 100,000 copies. Terry's newest book, JUMPSTART YOUR PUBLISHING DREAMS, INSIDER SECRETS TO SKYROCKET YOUR SUCCESS is packed with insight. Also Terry has an innovative online training course to help authors effectively connect with literary agents and editors called Write A Book Proposal. Terry is a popular speaker and teacher at numerous writers' conferences and an active member of the American Society of Journalists and Authors.
Terry's Personal Website
Terry's Book on Billy Graham
Support this podcast: https://anchor.fm/the-monday-christian/support


Approximately 5.7 million Americans have bipolar disorder, a brain disorder also known as manic-depressive illness.
Approximately 5.7 million Americans have bipolar disorder, a brain disorder also known as manic-depressive illness. The Bipolar Disorder Answer Book is an authoritative reference for people with Bipolar Disorder and their loved ones, providing sound advice and immediate answers to their most pressing questions. Written by an experienced psychiatrist, The Bipolar Disorder Answer Book covers such topics as: -What are the symptoms and different types of Bipolar Disorder? -Can other illnesses cause Bipolar Disorder? -What therapies, medications and relapse-prevention strategies can help with Bipolar Disorder? -How does Bipolar Disorder differ in children and adults? -What special issues are there for women with Bipolar Disorder? -How can family and friends respond in a psychiatric emergency? The Bipolar Disorder Answer Book offers up clear, confident counsel in an easy-to-read Q&A format that explains confusing medical lingo and guides readers through the world of Bipolar Disorder.
Charles Atkins, MD, is a board-certified psychiatrist working in Waterbury, Connecticut. He's on the clinical faculty at Yale University, where he trained. He has published over a hundred articles and columns, as well as psychological thrillers, including one with a hero who has bipolar disorder. His website is www.charlesatkins.com.
Bipolar disorder, which until the 1980s was called manic-depression, is a diagnostic term used to describe patterns of abnormal and severe mood swings, ranging from disabling depression to mania. For the sake of clarity, we're using the term "mood" to describe a sustained or prevailing emotional state. The term "bipolar" refers to extreme moods, from depressed on one pole to manic on the other.
There are four variants of bipolar disorder included in the current psychiatric diagnostic manual (the DSM-IV-TR), a book medical professionals use to diagnose patients.
These will be described in detail, along with their variants, in Chapter 2.
In the real world, what we find is that while these diagnoses are useful and provide a common language with which behavioral health professionals (psychiatrists, psychologists, social workers, counselors, therapists, and others) can communicate, the reality is that bipolar disorder represents a complex spectrum. Each person with bipolar disorder will have an array of symptoms unique to them and to their changing lives, circumstances, and moods. The range is vast, from people who will have multiple mood swings in a year to some who may go for years or even decades with the disorder lying dormant.
There is no one face to bipolar disorder, and because we're discussing moods—something everyone has—we'll need to define where normal ends and a disordered state begins.
Mood disorders, also referred to as affective disorders, include the full range of depressive disorders (major depression, dysthymia, etc.) as well as the bipolar spectrum (bipolar I, bipolar II, cyclothymia, bipolar disorder NOS, and some would also include schizoaffective disorder). All of these are discussed and defined in Chapter 2. In practical terms, mood disorders are where sustained emotional states (days, weeks, months, or years as opposed to minutes and hours) are so extreme that they are out of proportion to the situation and cause impairment in major areas of a person's life (work, relationships, health).
When does a mood state become a disorder?
This is a fundamental question: when does a mood cross some imaginary line from normal to abnormal? Probably the best way to approach this is to look at disruptions and overall functioning in the individual's life. If someone gets by with four hours of sleep a night, has tons of energy, is extremely productive, feels rested, is getting on well with family, friends, and co-workers, does this make them hypomanic, or are they just energetic and happy? In this example you could argue that we're in the realm of normal, because there's no disruption being caused by the good mood and revved up personality; it's just the person's natural way of being.
In order for a mood state to cross the line into a disorder there must be—in addition to various symptoms and durations of symptoms that we will outline for each of the mood states (mania, mixed and depressed)—a significant disruption in overall functioning, at work, home, or in other settings.
Additionally, as is seen in depressed and mixed states, the presence of significant to severe and disabling emotional distress is what pushes a case of the everyday blues and occasional irritability that we all get into something that is a disorder.
Bipolar disorder, like many medical conditions, is treatable, although there is no known cure. People do recover, however, and by learning to manage their symptoms can have lives that are highly productive, rich, and meaningful.
How long has bipolar disorder been around?
The first recorded mention of mental illness of any sort dates back to Egyptian hieroglyphs. The ancient Greeks conceptualized various moods through the balance of four humors or biles (black, green, yellow, and red), which included melancholia or black bile to describe a depressed state. Mentions of a connection between depressed and manic states can be found in Roman writings of the second century.
The modern conceptualization of bipolar disorder/manic-depression is credited to the psychiatrist Emil Kraepelin (1856–1926), who coined the term "manic-depressive insanity." His careful descriptions of the natural course of the illness (before medications were around) still read true and laid much of the groundwork for current diagnostic thinking.
How many people have bipolar disorder?
According to the National Institute of Mental Health (NIMH), 2.6 percent of Americans age eighteen or older (5.7 million Americans) have bipolar spectrum disorder. Other sources place the incidence between 1 and 1.6 percent.
The broad discrepancy in reporting has a lot to do with how different researchers have looked at the disorder. Some include just bipolar I, while others include bipolar II, cyclothymia, and bipolar disorder NOS (not otherwise specified).
Has there been a rise in the disorder in the last few years?
The answer is both yes and no. The number of people with bipolar I—people who get both depressed and manic or mixed episodes— has remained relatively stable. But as the concept of a bipolar spectrum has expanded to include people who never become fully manic (bipolar II and cyclothymia—see Chapter 2), the actual number of individuals with bipolar diagnoses has increased.
A manic episode is a sustained period of abnormally elevated mood. This can range from a glowing sense of euphoria to a pressured and agitated state, in which people feel as though they could jump out of their skin. When someone is manic he has seemingly boundless energy, and in the early phases may be quite productive. His speech becomes too rapid and the normal give-and-take of conversation is lost—you can't get a word in edgewise. The person with mania may become easily distracted and will describe his thoughts as having a racing quality. When listening to a person who is manic, the ideas that fly from his mouth seem to blossom one on top of the other (flight of ideas). Elaborate—and sometimes unrealistic and grandiose—plans are laid out. These take many forms, such as get-rich-quick schemes or religious revelations that he, and he alone, has discovered. If you attempt to reason with a person who is manic, he may become agitated, condescending, and openly hostile.


Today's 'Freedom Fighters' Tomorrow's Terrorists?
The 3,000-year-old cemetery on the Mount of Olives in Israel is one of the oldest Jewish burial sites. Yet it suffers from rampant desecration of graves and violence against visitors by.... guess who?
Nothing is more worrisome than a risk-averse intelligence community. So what will it take to persuade the U.S. intelligence community that Tehran's nuclear intentions are NOT peaceful?
So Where Are The Apologies Now?


text:
Vingt Jours sans guerre (, ) est un film soviétique réalisé par Alexeï Guerman, sorti en 1977.

Synopsis
Le journaliste de guerre soviétique Lopatine prend le congé et va à Tachkent où il rencontre les gens blessés par la guerre et trouve son amour.

Fiche technique

 Titre français : Vingt Jours sans guerre
 Titre original : ,
 Réalisation : Alexeï Guerman
 Scénario : Constantin Simonov d'après son roman Из записок Лопатина publié en 1965.
 Photographie : Valeri Fedossov
 Pays de production :
 Langue de tournage : russe
 Format : Noir et blanc - Mono - 35 mm
 Genre : Film dramatique, film de guerre
 Durée : 101 minutes
 Dates de sortie :
 Union soviétique :
 Grèce :
 France :

Distribution
 Yuri Nikulin : major Vassili Lopatine
 Lioudmila Gourtchenko : Nina
 Alexeï Petrenko : Youri Stroganov, pilote
 Angelina Stepanova : Zinaïda Antonovna, directeur du théâtre
 Yekaterina Vasilyeva : Roubtsova, la femme de Roubtsov
 Nikolaï Grinko : Viatcheslav (voix : Innokenti Smoktounovski)
 Lyusyena Ovchinnikova : Ksenia, ex-femme de Lopatine
 Mikhaïl Kononov : Pacha Roubtsov, correspondant de guerre
 Liya Akhedzhakova : femme à la montre
 Rachide Sadykov : secrétaire du comité central
 Constantin Simonov : narrateur

Notes et références

Liens externes

 Critique du film

Film soviétique sorti en 1977
Film soviétique en noir et blanc
Film dramatique soviétique
Film sur le front est de la Seconde Guerre mondiale
Film de Lenfilm
Film se déroulant dans les années 1940
Adaptation d'un roman russe au cinéma
Film réalisé par Alexeï Guerman

redpajama_set_name: RedPajamaWikipedia


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