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\section{Introduction}

It is now
believed that low-mass galaxies significantly
contribute the major fraction of the
ionization photons in the epoch
of reionization \citep[e.g.,][]{Atek2015,Bouwens2016}.
Observations of faint galaxies at high-redshift, though very difficult, are required, especially in the era of James Webb Space Telescope (JWST), to directly constrain the ionization
radiation, gas environment, galaxy growth, and metal enrichment of the surrounding intergalactic medium (IGM).

Extensive efforts have been conducted to study the intrinsic
ultra-violet (UV) continuum and the ionization of low-mass galaxies.
These studies aim to understand how ionization radiation escapes into the IGM \citep[e.g.,][]{Ramambason2020}.
 Before UV photons reach the IGM, how much radiation can escape
 from galaxies depends on:
(1) the intrinsic intensity and the slope of UV spectra; and
(2) the distribution of optically-thick neutral hydrogen (\ion{H}{1}) gas in the
interstellar and circumgalactic medium (CGM) \cite[e.g.,][]{Chisholm2018}.
It is therefore crucial to study
both UV continua and gas properties around
low-mass galaxies to quantify the \ion{H}{1} (Ly$\alpha$)
optical depth in the CGM for better understanding the
reionization process.

The
existence of the neutral gas in and around
low-mass star forming galaxies
has been suggested mainly through
observations of Ly$\alpha$ emission \citep[e.g.,][]{Stark2017,Gronke2017}.
Low-mass galaxies often have strong Ly$\alpha$ and other ionized nebular emission \citep[e.g.][]{Erb2010,Stark2014}.
The presence of optically-thick, \ion{H}{1} ``shell"  makes the Ly$\alpha$
emission
showing the double-peak structure \citep[e.g.,][]{Yang2017},
with the expanding outflow further suppressing blue peaks of Ly$\alpha$ emission \citep{Yang2014}.

Nevertheless,
 {only through emission, the nature of the interplay between the neutral gas and
 galaxy cannot be completely understood.}
Detailed gas properties, including the gas metallicity, geometry and density
need to be constrained.
The strong lensing, plus the deep integration of JWST and VLT/MUSE provide us with
an excellent opportunity to conduct direct and detailed observations of a low-mass
galaxy at $z=4$, through both emission and absorption. Here, we present a detailed analysis of a strongly magnified arclet
galaxy in the Abell2744 field, combined with optical, infrared and millimeter observations.
{ The system is lensed into three multiple images, and the arclet is composed of two of them
lying on both sides of the critical line, with three bright compact clumps (knots in the arc) mirrored on each side
\citep{Mahler2018,Bergamini2022}. We name this galaxy ``A2744-arc3".
It was also reported in \citet{Vanzella2022}.
Through spectral-energy-distribution (SED) fitting, they found that
these clumps are gravitationally-bound young massive star clusters  with bursty star formation.
}

\xj{In this paper, we probe detailed properties of the interstellar and circumgalactic medium (CGM) of A2744-arc3. With VLT/MUSE and JWST, we provide
detailed analysis of both nebular emission and absorption lines.
}
Copious emission lines, including the detection of
\ion{C}{4}~$\lambda\lambda1548,1550$, \ion{He}{2}~$\lambda1640$, \ion{O}{3}]~$\lambda\lambda1661,1666$, [\ion{Ne}{3}]~$\lambda3868$, [\ion{O}{2}]~$\lambda3727$, and Balmer series of Hydrogen,
allow us to quantify the low metallicity of the ionized medium.
Further, the high signal-to-noise (S/N) observations of absorption
enable us, for the first time, to
examine the detailed properties of the neutral gas reservoir surrounding a low-mass
galaxy at $z\approx4$. The excellent de-lensed spatial resolution down to $\approx100$ pc in rest-frame UV observations
 allow the examination of the spatial variations of the UV radiation. All these
information yield unparalleled understanding of low-mass, young galaxies at high-redshift
using A2744-arc3 as a textbook example.

This paper is organized as follows. In Section \ref{sec:data}, we describe the observations and data reduction, including JWST/NIRISS imaging and spectroscopy, HST imaging, VLT/MUSE and ALMA continuum observations; In Section \ref{sec:result}, we provide details of photometry, SED fitting, and the lensing reconstruction in source-plane. We also show the spatially resolved UV slope map. In Section \ref{sec:dla}, we present further analysis on the rest-frame UV and optical spectrum of A2744-arc3, including the analysis of both emission and absorption features. Discussions are conducted in Section \ref{sec:discussion}. We assume a flat cosmological model with $\rm{\Omega_{M} = 0.3, \Omega_{\Lambda} = 0.7}$ and $\rm{H_0 = 70\ km\ s^{-1}\ Mpc^{-1}}$.  The \texttt{Glafic} lensing model \citep{Oguri2010,Kawamata2016} is adopted.

\section{Data}\label{sec:data}
\subsection{JWST/NIRISS imaging \& grism observations}\label{sec:niriss data}
NIRISS observations of A2744 were taken by the
GLASS JWST Early Release Science Program \citep{Treu2022}, devoting about $2834.504\,\mathrm{s} \simeq 0.79\,\mathrm{hours}$ for F115W, F150W, and F200W direct imaging, respectively. \xxj{Especially the NIRISS/F200W data, spanning from 1.7$\mu{\rm m}$ to 2.2 $\mu{\rm m}$, allows us to better improve constraints on its stellar mass.} The data were reduced in the same way as shown in \citet{Wu2022}. Here we summarize the procedure as follows: the data were reduced using the standard JWST pipeline\footnote{\href{https://github.com/spacetelescope/jwst}{https://github.com/spacetelescope/jwst}} v1.6.2 with calibration reference files ``\texttt{jwst\_0944.pmap}'';
1/f noise (see \citealt{Schlawin20}) was modeled and removed using the code \texttt{tshirt/roeba}\footnote{\href{https://github.com/eas342/tshirt}{https://github.com/eas342/tshirt}}, and the ``snowball'' artifacts from cosmic rays \citep{Rigby22} were identified and masked; the world coordinate system of mosaicked images were registered using the Pan-STARRS1 catalog \citep{panstarrsdr1}; the pixel scale of final mosaicked images was resampled to 0.03\arcsec\ with \texttt{pixfrac}\,$=$\,0.8. We reduced NIRISS grism data using \textsc{Grizli} \footnote{\url{https://github.com/gbrammer/grizli/}}, and the 2D grism spectra were drizzled with a pixel scale 0.065\arcsec.

To optimally extract 1D spectra of A2744-arc3, we first split the entire arclet into six segments, each with one clump. We extracted their 1D spectra using 5-th Chebyshev polynomials. We summed over five 1D spectra of the six segments to get the final spectra. One of them was excluded since it is severely contaminated by zero-th and first order images from other sources.

\subsection{Hubble Frontier Fields images}

The A2744 cluster was observed as part of the Hubble Space Telescope Frontier Fields program\footnote{\url{https://archive.stsci.edu/prepds/frontier/}} (HFF; ID: 13495, PI: J. Lotz)
between 2013 October 25 and 2014 July 1 for 164.5 orbits in total, in three filters with the Advanced Camera for Surveys (ACS; F435W,
F606W, F814W) and four with the Wide Field Camera 3
(WFC3; F105W, F125W, F140W and F160W).  The high-level science product released by Space Telescope
Science Institute (STScI) with a pixel size of 30 mas is used in this study.

\subsection{VLT/MUSE observation}

Multi Unit Spectroscopic Explorer (MUSE) observations toward A2744 were taken by the GTO Program 094.A-0115 (PI: Richard) between 2014 September and 2015 October, with a 2 arcmin$\times$2 arcmin designed mosaic of pointings centred at $\alpha$= 00h14m20.952s and $\delta$= -30$^\circ$23$^\prime$53.88$^{\prime\prime}$ \citep{Mahler2018}. Each pointing was observed for a total of 3.5, 4, 4 and 5h in addition to 2h at the cluster center. The publicly available data cube\footnote{\url{http://muse-vlt.eu/science/a2744/}}  is adopted in this work.

\subsection{ALMA continuum observations}

The millimeter continuum observations are obtained from the ALMA Lensing Cluster Survey (ALCS).
A2744 is observed by ALMA band 6 (Program 2018.1.00035.L, PI: Kohno; 2013.1.00999.S, PI: Bauer) which covers a frequency range with two tunings of $250.0-257.5$ GHz and $265.0-272.5$ GHz, corresponding to wavelengths of $\sim 1.15 $ mm \citep{Sun2022}.
The $1\sigma$ continuum sensitivity or say rms is 45\,$\mu$Jy\,beam$^{-1}$.
The data were reduced using the standard pipeline with the CASA \citep{McMullin2007} with natural weighting, and will be described in details in S. Fujimoto et al., in prep. This leads to a synthesized beam size (FWHM) of $\sim 1$\arcsec, corresponding to $\sim6.9$ kpc at $z\sim 4$.

\section{Result and Analysis}\label{sec:result}

\subsection{Photometry and SED fitting}\label{sec:photometry}

We use a box aperture along A2744-arc3 to carry out the photometry on seven broad-band HST observations (ACS/F435W, F606W, F814W and WFC3/F105W,  F125W, F140W, and F160W) and three JWST NIRISS observations (NIRISS/F115W, F150W, and F200W). For each band, the length and width of the box aperture are designed to match the 2$\sigma$ contours of the arc, where $\sigma$ is determined by the local sky background. A sersic modelling is performed to the nearest source in the north to exclude potential light contamination. Magnification and multi-image effects are corrected to determine the delensed flux. \xxj{The median magnification along the arc is about 45 according to the \texttt{Glafic} model. We repeat the photometry and SED analysis using \citet{Richard2021} model, as described in Appendix \ref{sec:lensing model systematics}, and yield consistent results.}

We perform SED modeling with the Bayesian code \texttt{BEAGLE} \citep{Chevallard2106}. We assume a constant star formation history, the dust extinction curve of the Small Magellanic Cloud with the optical depth in the V band varying in the range 0 -- 0.5, and the \cite{Chabrier2003} initial mass function (IMF) with an upper limit of 300${\rm M}_\odot$. The metallicity of the interstellar medium is kept the same as that of the stellar populations. A flat prior is applied for metallicity, $0.01<{ Z}/{\rm Z}_\odot<0.2$, and ionization parameter (the dimensionless ratio of the number density of H-ionizing photons to that of hydrogen) in log-space, $-3<\log{U}<-1$, for nebular emission \citep{Gutkin2016}.
\xxj{These
priors are chosen on the basis of detections of the UV emission lines (see Section \ref{sec:emission} for more details)}.
A JWST NIRISS/F150W view of A2744-arc3, the SED fitting results, and the NIRISS grism 2D and 1D spectra are shown in Figure \ref{fig:jwst}. It implies that A2744-arc3 is a young, low-mass galaxy with massive
star formation, \xxj{accompanied by blue UV slopes, strong nebular emission lines and a faint intrinsic UV luminosity}.  \xxj{The absence of a Balmer break in the NIRISS spectrum further confirms a
young stellar age.}
The continuum of ALMA band 6 at rest-frame 0.23\,mm shows no clear detection, which indicates a 3$\sigma$ upper limit of far-infrared luminosity surface density $<2.2\times 10^{11}{\rm L}_\odot/{\rm arcsec^2}$ assuming a dust temperature $T=35{\rm K}$ and dust emissivity spectral index $b=1.6$. This corresponds to an upper limit of star formation rate surface density $\approx 9\times 10^{-7} {\rm M}_\odot{\rm yr^{-1} pc^{-2}}$ \citep{Murphy2011}.
\xxj{and an upper limit of dust mass surface density $\approx 1.6 {\rm M}_\odot {\rm pc}^{-2}$ \citep{daCunha2013}.}

\xj{In \citet{Vanzella2022}, SED analysis was performed on each mirrored clump using images from NIRISS/F115W, F150W, F200W, and HST/WFC3 F105W, F125W, F140W, F160W, along with the ground-based VLT/HAWKI Ks-band.
\xxj{Their derived star formation rate (SFR) is $1.47^{+0.85}_{
-0.25} /{\rm M}_\odot {\rm yr}^{-1}$, total stellar mass  of $1.6
^{+0.4}_{-1.3}\times 10^{8} {\rm M}_\odot$ (Table 1, 3c),
and age of $126^{+33}_{-108}$ Myr. Our derived properties are marginally consistent with theirs within $1\sigma$.} They found that these nucleated star-forming regions have optical/UV effective radii spanning 3--20 pc, bursty star formation activities ($\sim 10 {\rm Gyr}^{-1}$) and UV slopes of $\beta \simeq -1.9$, and  stellar mass surface densities  resembling those of local
globular clusters.
Our conclusion is consistent with theirs.
Note that the upper limit of IR-based SFR density is smaller than that obtained from UV
($\gtrsim 10^{-5} {\rm M}_\odot{\rm yr^{-1} pc^{-2}}$ for clumps in \citet{Vanzella2022}), and
this may be due to a low dust-obscured fraction of SFR in this low-mass galaxy
with negligible dust content.
}

\begin{figure*}
    \includegraphics[width=\textwidth]{Figure1.pdf}
    \caption{

    {\bf Top left}: JWST NIRISS F150W surface brightness image of A2744-arc3 with overlaid
    continuum contours of ALMA band 6. The contours levels are -2 (white dashed), 1 and 2$\sigma$ (white solid) with $1\sigma=44.5\mu$Jy/beam,
    showing no clear detection at a rest-frame wavelength of 0.23mm.  {\bf Top right}: Photometry and SED fitting for A2744-arc3, with derived physical parameters. Blue triangles denote the measurement and red circles the best-fit result. {\bf Bottom}: Optimally extracted 1D spectra (top panel) and joint 2D spectra covered by NIRISS three filters (F115W, F150W and F200W). In the top panel, shaded blue regions indicate flux uncertainties, and vertical red lines label common emission lines, among which \ion{Mg}{2} is not detected. The 2D spectra of the bottom panel are obtained by summing 2D spectra of the five segments as described in Section \ref{sec:niriss data}}
    \label{fig:jwst}
\end{figure*}

\subsection{Source Plane Reconstruction and Spatially-resolved UV Slope}\label{sec:reconstruction}

To explore the spatially-resolved UV slope variation, we construct UV slope $\beta$ maps in both
the image plane and source plane using HST and JWST broad-band images.  We recover the intrinsic source morphology by ray-tracing back the image-plane pixels on a regular source plane grid based on the corresponding deflection field \citep{Patricio2016}. \xj{More details about the selection of lensing models and the reconstruction are presented in Appendix \ref{sec:lensing model systematics}.}

The image-plane and reconstructed source-plane UV slope maps are shown in Figure \ref{fig:betamap}. The HST image plane $\beta$ map is constructed using \xj{PSF-matched} WFC3/F105W, F125W, F140W and F160W images which trace continua at 2125, 2513, 2805, 3091 \AA\ in the rest frame respectively. The JWST image plane $\beta$ map is constructed from \xj{PSF-matched} NIRISS/F115W and F150W, corresponding to rest-frame continua at 2315 and 3015 \AA. NIRISS/F200W is discarded to avoid potential [\ion{O}{2}] $\lambda\lambda 3729,3726$ and [\ion{O}{3}] $\lambda 4363$ emission. The $\beta$ map constructed from JWST images exhibits more fine structures and variations, thanks to its high spatial resolution. \xj{On both image- and source-plane $\beta$ maps, $\beta$
spans from -1.5 to -2.5. The bluest $\beta$ resides around the compact star clumps, reaching -2.5, caused by ionizing radiation from massive star formation. On the source plane, we confirm that $\beta$ varies on the physical scale of $<100$\,pc. }

\begin{figure*}[htbp]
    \centering
    \includegraphics[width=\textwidth]{betamap.pdf}
    \caption{

    The UV slope $\beta$ map in the image plane and source plane measured from HST and JWST broadband images. The HST UV slope maps are measured from WFC3/F105W, F125W, F140W and F160W images (2125-3091\,\AA\ in the rest frame), while the JWST UV slope maps are constructed only using NIRISS/F115W and F150W images (2315-3015\,\AA\ in the rest frame), to avoid emission lines captured by the NIRISS/F200W filter. The overlaid green contours in HST image/source plane denote the lensed/de-lensed WFC3/F160W surface brightness levels of 0.05,0.075,0.1 MJy sr$^{-1}$,

    and the contours in JWST image/source plane show NIRISS/F150W lensed/de-lensed surface brightness levels of 0.075,0.1,0.135 MJy sr$^{-1}$ respectively. The ellipses on the upper right corners correspond to the FWHM of image/source plane point spread function (PSF). Note that source-plane
    PSF varies among positions due to different magnification and distortion, and the shown one is with the largest
    FWHM determined by deflection fields at one of the three clumps. }
    \label{fig:betamap}
\end{figure*}

\section{Associated Damped Ly$\alpha$ System with Super-solar Metallicity}\label{sec:dla}

The optical spectrum of A2744-arc3, as shown in Figure \ref{fig:Fig1}(a), is extracted from the MUSE data cube by making a 2$\sigma$ deblended segmentation map on a 5 arcsec$\times$ 5 arcsec white-light image cutout around it. Abundant absorption and emission features are highlighted, including high-column density Ly$\alpha$ absorption line and the multiplicity of metal absorption lines (e.g., \ion{O}{1} $\lambda1302$, \ion{Si}{2} $\lambda 1304$, \ion{Si}{4} $\lambda\lambda 1393, 1402$), strong high-ionization emission lines such as \ion{C}{4} $\lambda\lambda1548,1550$, He\uppercase\expandafter{\romannumeral 2} $\lambda1640$ and \ion{O}{3}] $\lambda\lambda1661,1666$. We also detect a series of intervening \ion{Fe}{2} absorbers at $z=2.582$ along the sightline. The spectral properties of the arc are reported in Table \ref{tab}.

\begin{figure*}
\gridline{\fig{full_spec2.pdf}{\textwidth}{(a)}}
\gridline{ \fig{fit_DLA.pdf}{\textwidth}{(b)}}
\gridline{ \fig{metal2.pdf}{.45\textwidth}{(c)}
        \fig{metalicity_compare.pdf}{.45\textwidth}{(d)}}
\caption{\textbf{(a)} Rest-frame UV spectrum of A2744-arc3 extracted from
 the VLT/MUSE 3D datacube, with the error spectrum shown in red.
 Nebular emission lines and absorption features associated with A2744-arc3 are labelled
 with dashed red and blue lines, respectively
 A series of absorption features from an intervening \ion{Fe}{2} absorber
 at $z=2.582$ are identified in orange.
 \textbf{(b)} Normalized spectrum zoomed into the DLA Ly$\alpha$ and Ly$\beta$ line profiles with the Voigt profile fits,
 with flux uncertainties indicated by gray shaded region. The red solid lines imply the best-fit result yielding
 $\log(N_\mathrm{HI }/{\rm cm}^{-2})=21.8\pm0.1$. Tentative residual in the trough is identified by the red shaded region. \textbf{(c)} Normalized spectrum zoomed into the metal absorption line profiles. The blue shaded regions are used to measure the equivalent width (EW) of the absorbers. A tentative velocity offset of -36 km~s$^{-1}$ relative to $z=3.980$ (blue dashed) is marked in green dashed lines. \textbf{(d)} The neutral gas metallicity derived from the \ion{O}{1} absorber in compared with metal abundances of DLAs (\citealt{Rafelski2012}; gray squares) and Lyman break galaxies (LBGs) (\citealt{Troncoso2014}; blue triangles) out to $z=5$.
 The gray dashed lines indicate the cosmic evolution of DLA metallicities in \cite{Rafelski2012}.
 The gray shaded region marks metallicities lower than solar values. The purple shadow ranging from $-1.39$ to $-0.94$ marks the \ion{H}{2} region [O/H] abundance of A2744-arc3 derived from mass-metallicity relations and [\ion{Ne}{3}]/[\ion{O}{2}] empirical metallicity calibrations, as described in Section \ref{sec:emission}.  \label{fig:Fig1}}
\end{figure*}

\begin{deluxetable*}{lcccccccccc}
\tabletypesize{\small}
\tablecaption{Physical Properties of the arc derived from the photometry, absorption and emission features.  In addition, column densities and abundances of neutral gas metallicity tracers are provided.\label{tab}}

\tablehead{\multicolumn{11}{c}{ Basic Physical Parameters}}
    \startdata
    R.A. (deg) & Dec (deg) & $z_{\rm spec}$\tablenotemark{a} & $\log M_*/M_\odot$ \tablenotemark{b} & Age (Myr) & SFR ($M_\odot$/yr) & $\log {\rm U}$ & $\mu_{\rm med}$\tablenotemark{c} & $\mu_1$\tablenotemark{c} & $\mu_2$\tablenotemark{c} & $\mu_3$\tablenotemark{c}\\

    3.589089 & -30.393844 & 3.980 & 7.59$^{+0.12}_{-0.10}$ & 23.95$^{+5.70}_{-8.44}$ & 1.80$^{+0.24}_{-0.21}$  & -1.34$^{+0.32}_{-0.26}$ & 45 & 142 & 46 & 30 \\
    \hline
    \hline
    \multicolumn{11}{c}{Absorption Features} \\
    \hline
      \multirow{2}{*}{Ion}& \multirow{2}{*}{$\lambda$ (\AA)}& & \multicolumn{3}{c}{CoG Method} & & \multicolumn{4}{c}{Voigt Profile Fitting} \\
     \cline{4-6}\cline{8-11}
         &   & & EW (\AA)\tablenotemark{d} & $\log$(N/cm$^{2}$)\tablenotemark{e} & [X/H]\tablenotemark{f} & & \multicolumn{2}{c}{$\log$(N/cm$^{2}$)\tablenotemark{g}} & \multicolumn{2}{c}{[X/H]\tablenotemark{h}}\\
     \hline
      \ion{H}{1}   &  1215.670 & & - & - & - & & \multicolumn{2}{c}{21.8$\pm0.1$\tablenotemark{1}} & \multicolumn{2}{c}{-}\\
      \ion{O}{1}   &  1302.168 & & 0.77$\pm$0.10 & 18.9$^{+0.2}_{-0.3}$ & 0.41$^{+0.20}_{-0.30}$ & &\multicolumn{2}{c}{18.7$\pm$0.4} & \multicolumn{2}{c}{0.21$\pm$0.40} \\
      \multirow{2}{*}{\ion{Si}{2}\tablenotemark{2}} & 1260.422 & &1.12$\pm$0.11 &- &  & & - &  \\
      & 1304.370 & & 0.47$\pm$0.10 & 17.8$_{-0.9}^{+0.4}$ &  \multirow{2}{*}{0.74$^{+0.36}_{-0.53}$} & & \multicolumn{2}{c}{18.0$^{+0.4}_{-0.6}$} & \multicolumn{2}{c}{\multirow{2}{*}{0.81$^{+0.36}_{-0.71}$}}\\
      \ion{Si}{4} & 1402.770 & & 0.67$\pm$ 0.11  & 17.7$\pm$0.3 & & & \multicolumn{2}{c}{17.5$^{+0.2}_{-1.6}$} \\
     \ion{C}{2}\tablenotemark{3} & 1334.532 & & 1.31$\pm$0.09 &- & -& & \multicolumn{2}{c}{-}&\multicolumn{2}{c}{-}\\
     \ion{Fe}{2}\tablenotemark{2}
     & 1608.451 & & 0.80$\pm$0.08 & 18.7$\pm 0.2$ & 1.40$\pm$0.20 & & \multicolumn{2}{c}{19.1$^{+0.2}_{-0.4}$} & \multicolumn{2}{c}{1.80$^{+0.20}_{-0.40}$} \\
     \ion{Al}{2} & 1670.787 & & 0.72$\pm$0.10 & 16.4$\pm$0.4 & 0.15$\pm$0.40 & & \multicolumn{2}{c}{16.4$^{+0.3}_{-1.3}$} & \multicolumn{2}{c}{0.15$^{+0.30}_{-1.30}$}\\
     \hline
     \hline
     \multicolumn{11}{c}{Emission Lines} \\
     \hline
     Ion & $\lambda$ (\AA) & & EW (\AA) & \multicolumn{3}{c}{FWHM (km s$^{-1}$)\tablenotemark{i}} & \multicolumn{4}{c}{Flux (10$^{-18}$ erg s$^{-1}$ cm$^{-2}$) } \\
     \hline
    \multirow{2}{*}{\ion{C}{4}} & 1548.187 & & \multirow{2}{*}{3.14$\pm$0.23} &  \multicolumn{3}{c}{118$\pm$9} &  \multicolumn{4}{c}{\multirow{2}{*}{7.8$\pm$0.6\tablenotemark{5}}}\\
     & 1550.772 & & & \multicolumn{3}{c}{$<$461\tablenotemark{4}} & \\
     \ion{He}{2} & 1640.420 & & 1.62$\pm$0.09 &  \multicolumn{3}{c}{143$\pm$8} & \multicolumn{4}{c}{3.8$\pm$0.2} \\
     \multirow{2}{*}{\ion{O}{3}]} & 1660.809 & & \multirow{2}{*}{6.25$\pm$0.27}  & \multicolumn{3}{c}{144$\pm$9} & \multicolumn{4}{c}{3.7$\pm$0.2} \\
     & 1666.150 & & &  \multicolumn{3}{c}{139$\pm$6} & \multicolumn{4}{c}{7.9$\pm$0.6}\\
     \hline
     [\ion{O}{2}]\tablenotemark{6} & 3727\tablenotemark{7} & & 80.2$\pm$12.9 & \multicolumn{3}{c}{-} & \multicolumn{4}{c}{56.0$\pm$6.4}  \\
     {}[\ion{Ne}{3}] & 3868.760 & & 105.6$\pm$16.7 & \multicolumn{3}{c}{-} & \multicolumn{4}{c}{66.1$\pm$7.3}  \\
    \enddata

     \tablenotetext{a}{Redshift determined by \ion{O}{1} absorption.}
     \tablenotetext{b}{Physical parameters are derived from \texttt{BEAGLE} SED fitting.}
     \tablenotetext{c}{Magnification from the \texttt{Glafic} model. $\mu_{\rm med}$ is the median value along the arc based on the JWST/NIRISS F115W $2\sigma$ profile. $\mu_{1}$, $\mu_2$ and $\mu_3$ is the median magnification of the three mirrored clump pairs from inside (closest to the axis of symmetry/critical curve) to outside respectively.}
     \tablenotetext{d}{Rest-frame equivalent width of the absorbers. The uncertainties are estimated by varying the continuum level by 10\%, combined with the flux uncertainties.}
     \tablenotetext{e}{Column densities are derived assuming $b$=10km s$^{-1}$. Uncertainties are estimated by varying the doppler parameters $b$ from 5-15km s$^{-1}$, combined with the uncertainties from EW measurements.}
    \tablenotetext{f}{[X/H] = $\log$(X/H) - $\log$(X/H)$_\odot$. Solar (photosphere) abundances from the compilation by \cite{Asplund2009}.}
    \tablenotetext{g}{Column densities are determined by two-component Voigt profile fits to the absorption features simultaneously, assuming $b=10$km s$^{-1}$. We also perform  Voigt profile fits using  $b$=5 and 15km s$^{-1}$, and the uncertainties presented here include systematics induced by different $b$ values.}
    \tablenotetext{h}{Metallicities are calculated by summing over column densities of the two Voigt profiles.}
    \tablenotetext{i}{FWHMs are measured in the rest-frame relative to $z=3.980$, using Gaussian fits and eliminating the effect of MUSE line spread function (LSF) \citep{Bacon2017}.}
    \tablenotetext{1}{The uncertainty is determined by varying the continuum level by 10\% and the doppler parameter $b$ from 50 to 200km/s.}
    \tablenotetext{2}{The \ion{Si}{2} $\lambda$1260 and \ion{Fe}{2} $\lambda$1608 absorption might be blended with other lines.}
    \tablenotetext{3}{The \ion{C}{2} $\lambda$1334  absorption is saturated. }
    \tablenotetext{4}{The \ion{C}{4} $\lambda$1550 emission line is likely interfered by noise.}
    \tablenotetext{5}{There might be potential \ion{C}{4} absorption from neutral gas blended with its emission.}
    \tablenotetext{6}{Measured from the coadd of JWST/NIRISS slitless spectra as described in Section \ref{sec:niriss data}. We do not provide FWHMs due to blending effect in grism data and the low resolving power of NIRISS (R$\approx$150). Flux is measured by fitting single Gaussian profiles to each emission line.}
    \tablenotetext{7}{The doublet of [\ion{O}{2}]  at 3726.032 and 3728.815\AA\  cannot be distinguished.}

\end{deluxetable*}

\subsection{Metal-enriched \ion{H}{1} gas with high column density}

\sw{In Figures \ref{fig:Fig1}(b) and \ref{fig:Fig1}(c), we display the DLA \ion{H}{1} and its associated metal absorption-line profiles, respectively. The metal lines exhibit tentative P-Cygni features. We use the Voigt profile to fit
absorption lines.} The Ly$\alpha$ and Ly$\beta$ absorption associated with the galaxy at $z=3.98$, depicted in Figure \ref{fig:Fig1}(b), indicates a \ion{H}{1} column density of $N_{\rm{HI}}=10^{21.8\pm0.1}$cm$^{-2}$, i.e.\ an extremely strong damped Ly$\alpha$ systems \citep[ESDLA, $N_{\rm{HI}}>5\times 10^{21} {\rm cm}^{-2}$;][]{not14}.
The measurement is performed using \texttt{VoigtFit} \citep{VoigtFit}, varying the continuum level by 10\% and the doppler parameters in the range 50-200 km s$^{-1}$.  Tentative detection of residual Ly$\alpha$ emission in the absorption trough might imply partial DLA coverage. \xxj{Nevertheless,
the possibilities of contamination from
foreground sources or imperfect sky subtraction cannot be excluded.}
The source-reconstruction in Figure \ref{fig:betamap} illustrates that the ESDLA extends over at least sub-kpc scales.

\sw{We measure the gas-phase metallicity from the accurate indicator \ion{O}{1}. Because \ion{O}{1} and \ion{H}{1} have similar ionization potentials and are coupled by resonant charge exchange reactions, we then have [\ion{O}{1}/\ion{H}{1}] $\approx$ [O/H]. Considering the \ion{O}{1} $\lambda$ 1302 line may be saturated, we estimate the metallicity from both the Voigt profile fitting and curves of growth (CoG) analysis. By varying the Doppler parameter $b$ between 5--15 km s$^{-1}$, we obtain the metallicity [O/H] varying from $-0.11$ to 0.61. We list both the Voigt fitting results ($b = 10$ km s$^{-1}$) and the estimates from the curves of growth of metallicity in Table \ref{tab}.} {\xj More details about the Voigt fitting results are presented in Appendix \ref{sec:VoigtFit}.} The estimates from \ion{O}{1} and other metal lines such as \ion{Si}{2}
all yield a super-solar metallicity, with [O/H]=0.41$^{+0.20}_{-0.30}$\ and [Si/H]=0.74$^{+0.36}_{-0.53}$\ (\ion{Si}{2} + \ion{Si}{4}) respectively, corresponding to 2.57$^{+1.50}_{-1.28}$ ${\rm Z}_\odot$ and 5.50$^{+7.09}_{-3.87}$ ${\rm Z}_\odot$.
This metallicity, as highlighted in Figure \ref{fig:Fig1}(d), is much higher than the prediction of the cosmic metallicity evolution of DLAs ([X/H]~$\approx-1.5$ at $z=3.98$, \citealt{Rafelski2012}), and the metal abundances of typical
star-forming galaxies at $z= 3-5$,
measured using nebular emission lines originated from
their \ion{H}{2} regions  (e.g, [X/H]~$\approx -0.5$ in \citealt{Troncoso2014}). \sw{However, we are cautious to conclude the high metallicity given the low resolution spectra (R $=$ 2000-3000) and the non-detection of weak lines such as \ion{Ni}{2} and \ion{Zn}{2}. We need high resolution spectra to confirm our measurements.}

\sw{Additionally, we also obtain super-solar metallicity from the \ion{Fe}{2} absorption lines. Since \ion{Fe}{2} can be depleted onto the dust, the high abundance of \ion{Fe}{2} indicates not much dust in both the absorbing gas and the galaxy, consistent with the ALMA millimeter continuum non-detection. }

\subsection{Strong narrow nebular emission -- an indication of metal-poor \ion{H}{2} region}\label{sec:emission}

\xj{A2744-arc3 exhibits significant high-ionization nebular emission in both optical and infrared spectra, e.g., \ion{C}{4} $\lambda 1548, 1550$, \ion{He}{2} $\lambda 1640$, \ion{O}{3}] $\lambda 1661,1666$ and [\ion{Ne}{3}] $\lambda 3638$
(see Figure \ref{fig:jwst}, \ref{fig:Fig1}(a) and Table \ref{tab}), which
have been detected in nearby dwarf galaxies and $z\approx1-2$ metal-poor or strong LyC emitting galaxies
\citep[e.g.,][]{Erb2010,Schaerer2022_C4}, but not typically detected in
Lyman break galaxies (LBGs)
\citep[e.g.,][]{Reddy2008}.
These strong narrow nebular emission lines, especially \ion{He}{2} $\lambda 1640$, are believed to be tightly linked to low-metallicity galaxies with a possible contribution from Pop III-like stars \citep{Schaerer2003,Patricio2016}.
}

The line ratio between [\ion{O}{2}] and [\ion{Ne}{3}], two of the principal coolants in \ion{H}{2} regions, serves as a metallicity indicator for star-forming galaxies. In A2744-arc3, we obtain $\log$([\ion{Ne}{3}]/[\ion{O}{2}])$=0.07^{+0.06}_{-0.07}$, i.e.\ 12+$\log{( {\rm O/H})}=7.75\pm 0.05$, based on the empirical metallicity calibrations in \cite{Bian2018}, corresponding to [O/H] = $-0.94\pm0.05$ or ${ Z}/{\rm Z}_\odot=0.12\pm 0.01$\footnote{\xxj
Possible systematics are discussed in Appendx \ref{sec:Ne3O2_ratio}, e.g., line blending and the scatters of the calibration relation. More observations are expected to
confirm its metal abundance.}}. The mass-metallicity relation (MZR) in \cite{Sanders2021} predicts 12+$\log$(O/H)=7.7$\pm$0.1 for a $M_*\approx 10^{7.6\pm0.1} {\rm M}_\odot$ galaxy
at $z\approx3.3$; \cite{Ma2016} predicts 12+$\log {\rm (O/H)}=7.27\pm0.04$ at $z=3.98$. These values, including our SED fitting result,
are well consistent with models of \ion{He}{2} emitters, which favour
sub-solar metallicities ($\sim0.1~{\rm Z}_\odot$) and young stellar ages ($10^{7}-10^{8}$ years; \citealt{Saxena2020}).
The line ratio of \ion{O}{3}] $\lambda$1666/\ion{He}{2} $\lambda$1640  is $2.08\pm0.19$,
inconsistent with any photoionization models powered by AGN or shocks which expect more flux in
\ion{He}{2} $\lambda$1640 than in \ion{O}{3}] $\lambda$1666 ($\log$(\ion{O}{3}] $\lambda$1666/\ion{He}{2} $\lambda$1640) $\approx -3$ to $-0.5$) \citep{Allen2008,Feltre2016,Mainali2017,Senchyna2017}.
This disjoint favours the explanation that the
nebular emission in A2744-arc3 should primarily be powered by photoionization due to massive stars \citep{Gutkin2016}.

\bigskip

\section{Discussion}\label{sec:discussion}

\subsection{A2744-arc3 has properties similar to those local analogues}\label{sec:analogue}

SL2S J0217 \citep{James2014} and SBS 0335-052 \citep{Brammer2012,Berg2018,Erb2019} at lower redshifts share
similar features to A2744-arc3. Strong nebular emission lines such as \ion{C}{4} $\lambda\lambda 1548,1550$, \ion{He}{2} $\lambda 1640$ and \ion{O}{3}] $\lambda\lambda 1661,1666$ are notable in their UV spectrum, suggesting a very high ionizing field from the low-metallicity starbursting region and young stellar populations.
SBS 0335-052 is a nearby blue compact dwarf galaxy ($z=0.0009$) which shows a damped Ly$\alpha$ profile of $\log{N_{\rm{HI}}/{\rm cm^{-2}}}=21.70\pm0.05$, while SL2S J0217, a low-mass ($M<10^9\ {\rm M}_\odot$), low-metallicity (${ Z}<1/20\ {\rm Z}_\odot$) galaxy at $z=1.8$
magnified by a foreground massive galaxy, may be characterized by a superposition of strong Ly$\alpha$ emission and
damped absorption. SL2S J0217 also shows a blue UV slope of $\beta=-1.7\pm0.2$ over rest-frame 2100-2800 \AA,
and an ionization parameter of $\log{ U}\approx -1.5$.

In addition, Green Pea galaxies at $z<1$
with extremely high degree of ionization
in \ion{H}{2} regions often present a blend of strong emission and
underlying absorption \citep{McKinney2019}, with column densities
ranging from $\log{N_{\rm HI}/{\rm cm^{-2}}}=19-21$, well above the LyC thick limit \citep[e.g.,][]{Steidel2018}. The presence of the DLA in the spectra of A2744-arc3 at $z=4$
further
suggests that low-mass, low-metallicity galaxies, even at high redshift of $z\gtrsim4$,
may commonly possess abundant neutral hydrogen gas,
and the ultimate Ly$\alpha$ and ionizing photon escape may strongly depend on geometrical effects.

\bigskip

\subsection{The metal-enriched neutral gas reservoir around young, low-mass and metal-poor Galaxies}

\sw{\xj{As discussed above, A2744-arc3 is a low-mass ($M_*\approx10^{7.6}\ {\rm M}_\odot$) galaxy with low-metallicity (${ Z} \approx 0.1\ {\rm Z}_\odot$) \ion{H}{2} regions},
estimated from the nebular emission lines. In contrast, metal absorbers associated with the DLA
shows that the HI gas around the galaxy may have the super-solar metallicity.}
Super-solar metallicity of the neutral gas around a low-Z, high-U and low-mass galaxy is also
reported in \cite{Berg2018}. The metal-enriched gas can be generated by a high efficiency in
the gas cooling and enriched by the recycled inflow from the star formation \citep[e.g.,][]{Frye2019}.
Due to the metal-enrichment process is rapid, the metal-enriched environment may be
further enhanced by the continuous star formation in the high-redshift Universe.

We propose a simple schematic model to explain the \sw{metallicity variances in the ISM/CGM and star-forming region at $z\approx4$}, as shown in Figure \ref{fig:diagram}. Massive stars produce a hard radiation field, forming a highly ionized \ion{H}{2} region.
As mentioned above, the compact star-forming regions could be surrounded by  \ion{H}{1} clouds with varying column densities \citep{Erb2019}.
DLA can be observed when the sightline is completely blocked by high column density neutral clouds,
while
residual Ly$\alpha$ emission in the absorption trough can be detected in partially obscured cases. These outskirt environments
could be metal-polluted by the efficient feedback from massive stars
due to the high-velocity stellar wind.
The metal-enriched gaseous environment could result in the presence of
metal absorbers detected in Figure \ref{fig:Fig1}(c),
sometimes with the detectable P-Cygni profiles \citep{Erb2012}. This scenario explains the tentative detection of Ly$\alpha$ emission shown in Figure \ref{fig:Fig1}(b) and asymmetry profiles of metal
absorbers shown in Figure \ref{fig:Fig1}(c).

\begin{figure*}[htbp]
    \centering
    \includegraphics[width=\textwidth]{diagram_resize.pdf}
    \caption{The schematic toy model of A2744-arc3 as a low-mass, low-metallicty galaxy with high metallicity neutral gas reservoir. The blue stellar clumps inside mark the compact and bursty star-forming regions in A2744-arc3, on scales of sub-kpc.  Their hard ionization field forms hot, thin and highly-ionized \ion{H}{2} regions around them, where strong narrow nebular emission lines are produced. The gas outer layer denotes the neutral gas reservoir with varying column densities in the CGM. Its geometry determines the shape of Ly$\alpha$ emission/absorption we observed. When sightlines are blocked by high-column density gas, damped Ly$\alpha$ absorption is observed; in partially obscured case, Ly$\alpha$ emission with underlying absorption is observed. Three arrows mark possible gas cycles within the galaxy. Feedback from central star-formation, such as stellar winds, could metal-enrich the neutral gas, leading to strong metal absorbers with P-Cygni profiles. The recycled neutral gas
    can further efficiently fuel the next-generation star formation.

    }
    \label{fig:diagram}
\end{figure*}

\subsection{Implications of the spatially resolved UV slope map}
\xj{The ultraviolet (UV) continuum slope $\beta$ ($f_\lambda \propto \lambda^{\beta}$) is a prominent metric for properties of high-redshift galaxies. Both simulations and observations suggest that,
bluer galaxies observed at $z = 3--4$ have $\beta = -2$,
while values as blue as $\beta = -3$ can in principle be produced by
a young (age $\lesssim10^8$ years), low-metallicity (${ Z}\lesssim10^{-3}{\rm Z}_\odot$) stellar population \citep[e.g.,][]{Schaerer2003,Jiang2020,Topping2022}. \citet{Bouwens2010} predicted that the bluest $\beta$ for low metallicity ($0.02 - 0.2\ {\rm Z}_\odot$) starbursts is about $-2.7$,
consistent with $\beta$ around the three clumps in Figure \ref{fig:betamap}. This further indicate the low-metallicity nature of these early star clusters.
Aside from the blue radiation from young stars, recombination continuum radiation from the ionized gas can make the UV spectrum redder. When metallicity is greater than 0.02~${\rm Z}_\odot$, the UV slope generated by the recombination continuum become greater (redder) than $-2.5$.  With a high spatial resolution, we are  able to separate the relatively red nebular continuum emission from the ionized gas from the massive star continuum \citep[e.g.,][]{Bouwens2009} which may be consistent with what we have observed
here in A2744-arc3 with JWST.
}

\subsection{Implication of such a Low-mass, but dominating population of galaxies during  Reionization}

The UV luminosity of A2744-arc3 is $M_{\rm UV}=-17.8\pm 0.1$, corresponding to 0.049 $L_{\rm{UV}}^*$ galaxies
in the faint-end of the galaxy luminosity function \citep[$M^*=-20.88\pm0.08$,][]{Bouwens2015}.
Through the spatially-resolved emission and absorption lines,
A2744-arc3 at $z=4$ provides us with a text-book example, allowing
an unparalleled view of low-mass galaxies at the epoch of Reionizaiton (EoR).

Low-mass, metal-poor galaxies with hard ionizing radiation show much promise to dominate the ionizing photon budget during EoR \citep{Wise2014}, with a predicted escape fraction of $\sim 20\%$ \citep{Duffy2014}.
Similar to lower-redshift analogs \citep[e.g.,][]{James2014,Berg2018,Erb2019}, A2744-arc3 at $z=4$
has shown the prevalence of a neutral gas reservoir.
Given these observations,
we argue that, when modelling the escape of ionizing radiation into the intergalactic medium during EoR, the neutral gas reservoir surrounding galaxies themselves (see Figure \ref{fig:diagram}) should be seriously considered.
Our identification of the metal-enriched, neutral-gaseous clouds might support the picture that only a small fraction of ionizing radiation of low-mass galaxies escape through the circumgalactic channels with low column density of neutral gas.
With more observations of such galaxies, the statistics of the spatial variations of ionization, metallicity, HI covering fraction can be
better constrained.
In particular, the distribution of the optically thick HI clouds could
affect the photon escape by geometrical effects. Then, these HI clouds could
regulate the star formation and ionization fields through feedback.
On the one hand, the outflow from stellar winds could metal enrich the clouds, and then, the
clouds could further power the star formation through the recycled inflow \citep[e.g,][]{Frye2019}.
In the future, with telescopes such as the Large Ultraviolet Optical Infrared Surveyor (LUVOIR; \citealt{Roberge2018}), we will be able to better constrain the spatial distribution of optically-thick HI absorbers at
$z=2-5$, and improve our understanding towards the UV photon escape of low-mass galaxies in the high-redshift Universe.

\section{Conclusion}
In this letter, we presented a detailed analysis on a strongly magnified arclet, A2744-arc3, in the Abell 2744 field with the combination of  JWST/NIRISS (both imaging and grism spectroscopy), HST/WFC3, HST/ACS, VLT/MUSE and ALMA observations. The photometry and SED fitting imply that A2744-arc3 has a young age of $ 24^{+6}_{-8}$ Myr, high-ionization of $\log{ U}$ of $-1.3\pm0.3$, low-mass of $\approx 10^{7.6\pm0.1} {\rm M}_\odot$, and the low-metallicity \ion{H}{2} regions of 12+$\log{\rm (O/H)}\approx7.75$, corresponding to 0.12 ${\rm Z}_\odot$) at $z=3.98$.

The reconstructed source-plane images based on JWST observations provide
the resolved UV slope at the spatial resolution of $\approx$100 pc.
Three compact clumps show blue UV slopes, ranging approximately from $-1.5$ to $-2.5$, consistent with  \cite{Vanzella2022}, implying
young massive star clusters with bursty star formation activities.

Through absorption studies, we have identified an associated extremely strong DLA system, with $\log N_{\rm HI} = 21.8\pm0.1$.
Multiple metal absorbers indicate that this DLA may be super-solar metallicity,
with [O/H]=0.41$^{+0.20}_{-0.30}$,
higher than typical DLAs and LBGs at similar redshifts, indicative of strong metal-enrichment from low-mass galaxies. Additionally, the tentative P-Cygni profiles of the metal lines strengthen evidences for the young stellar feedback. \sw{To confirm our conclusion, we need higher resolution spectra with further larger wavelength coverage to measure the absorbing gas-phase metallicity.} A2744-arc3 also shows strong narrow nebular emission lines of \ion{C}{4} $\lambda\lambda 1548, 1550$, \ion{He}{2} $\lambda 1640$ and \ion{O}{3}] $\lambda\lambda 1661,1666$, indicative of a metal-poor \ion{H}{2} region with a hard ionization field.

Combing the lower-redshift analogs SL2S J0217 at $z=1.8$ and SBS 0335-052 at $z=0.0009$, our observations of A2744-arc3 at $z=4$ suggest that neutral gas reservoir may be prevalent around low-mass galaxies.
In our schematic model (Figure \ref{fig:diagram}),
massive star formation reside within a metal poor \ion{H}{2} region. The galaxy is surrounded by a large reservoir of neutral gas with a metallicity that could reach solar metallicity.
The
ionizing photons
could only escape through low column density channels.
A2744-arc3 at $z=4$ provide us an excellent picture in understanding
 faint-end galaxies that may have played a vital role during the EoR.

\section*{Acknowledgments}

Xiaojing Lin and Zheng Cai thank Eros Vanzella, Lilan Yang, Dandan Xu and Shiwu Zhang for very helpful discussions.  X.L. thanks Zechang Sun for the useful tool \texttt{SpecViewer} \citep{ZechangSun2021}.
Zheng Cai, X.L., Y.W., Z.L., M.L.,\& S.Z. are supported by the National Key R\&D Program of China (grant no.\ 2018YFA0404503), the National Science Foundation of China (grant no.\ 12073014), and the science research grants from the China Manned Space Project with No. CMS-CSST2021-A05.
F.S.\ acknowledges support from the NRAO Student Observing Support (SOS) award SOSPA7-022.
F.S.\ and E.E.\ acknowledge funding from JWST/NIRCam contract to the University of Arizona, NAS5-02105. J.X.P. acknowledges partial support from NSF AST-2107991. D.E. acknowledges support from the Beatriz Galindo senior fellowship (BG20/00224) from the Spanish Ministry of Science and Innovation, projects PID2020-114414GB-100 and PID2020-113689GB-I00 financed by MCIN/AEI/10.13039/501100011033, project P20\_00334  financed by the Junta de Andaluc\'{i}a, and project A-FQM-510-UGR20 of the FEDER/Junta de Andaluc\'{i}a-Consejer\'{i}a de Transformaci\'{o}n Econ\'{o}mica, Industria, Conocimiento y Universidades.

This work is based on observations made with the VLT/MUSE, ALMA, NASA/ESA Hubble Space Telescope and  NASA/ESA/CSA James Webb Space Telescope. MUSE observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO program 094.A-0115. HST and JWST data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST and NAS 5–26555 for HST. The JWST observations are associated with program ERS-1324. The HST observations are associated with the Hubble Space Telescope Frontier Fields program. The authors acknowledge the GLASS team for developing their observing program with a zero-exclusive-access period. The following ALMA data is also adopted: ADS/JAO.ALMA\#2018.1.00035.L and \#2013.1.00999.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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.