text:
\section{Introduction}

In the standard model of cosmology, the formation of the large scale structure of the Universe (LSS) is driven by the competing action of dark matter and dark energy. During this process, baryons undergo gravitational collapse and condense to form the visible web of filaments and knots, separated by void regions, that we call the {\it{cosmic web}}. At high redshift, the amount of baryons measured from the Cosmic Microwave Background and Ly$\alpha$ forest, or derived from Big Bang nucleosynthesis is in good agreement with theoretical expectations. At low redshift, however, observational studies report systematically lower values, with around 30 percent of the baryons unaccounted for. The so called \textit{missing baryon problem} refers to this apparent lack of baryons as measured from observations \citep{Kirkman2003,Bregman2007,Nicastro2008,Pettini1999,Anderson2010,Shull2012,Nicastro2017}, which might be due to the fact that a large amount of gas lies in low-density, high-temperature regions that are hard to detect using current UV and X-ray instrumentation.

Baryons are, in fact, also missing in galaxies, where the baryonic fraction is much lower than the universal baryon-to-total-mass ratio \citep{Bregman2007,McGaugh2010}. The difference is more pronounced for smaller galaxies, suggesting that haloes with shallower potential wells are less efficient in terms of retaining baryons. Overall, these results seem to indicate that the ``missing baryons" could be somewhere in the circum-galactic space and possibly beyond the virial radius of the haloes
as well, as suggested by recent reports \citep[see e.g.,][]{Tumlinson2013,Bordoloi2014,Werk2014,Johnson2015,Johnson2017,Tumlinson2017}.

The baryons missing in galaxies and in the LSS are indeed part of the same problem. Theoretical models predict that a large fraction of them resides in filamentary structure conforming to the so-called warm-hot intergalactic medium (WHIM), composed of hot (T~$=10^5 - 10^7$~K) low-density gas ($n_b = 10^{-6} - 10^{-4} {\rm cm}^{-3}$). These baryons are initially shock-heated during the build-up of the large-scale structures. Subsequently, stellar feedback and galactic winds act as additional heating sources, regulating also the chemical abundances in the WHIM \citep{Cen1999,Cen2006,Dave2001}.

The gas in the WHIM can be detected through the radiation field it produces (i.e., emission lines), or through absorption lines in background sources. Due to its low density, current X-ray telescopes fail to detect most of the WHIM emission. Nevertheless, several reports show that
filamentary and intra-cluster structures can be mapped from the
tail of the WHIM X-ray intensity distribution \citep{Scharf2000,Markevitch2003,Kaastra2003,Eckert2015,Hattori2017,Connor2018,Tanimura2020}. These types of measurements are expected to be possible in forthcoming years, thanks to, e.g., the Athena space mission \citep[][]{ATHENA}.

The most common way to trace the WHIM is through absorption lines in UV/X-ray quasar spectra. Significant evidence of unaccounted baryons has been reported from O\,\textsc{vi} absorption lines measured with the Far Ultraviolet Spectroscopic Explorer (FUSE) and the Hubble Space Telescope (HST-COS) \citep{Savage1998,Tripp2000,Danforth2016}.
Measurements based on O\,\textsc{vii} and O\,\textsc{viii} absorption lines from Chandra and XMM-Newton have also been presented \citep{Fang2002,McKernan2003}. Several other lines have been used in similar analyses, including C\,\textsc{ii}, C\,\textsc{iv}, N\,\textsc{v}, Si\,\textsc{iii}, Si\,\textsc{iv}, and Ne\,\textsc{viii} \citep[see e.g.,][]{Cooksey2010,Nicastro2013,Danforth2016,Tejos2016,Burchett2019,Manuwal2019,Ahoranta2020,Chen2020}. The main disadvantage of absorption lines is that they can only provide information about the gas along the line of sight of the background quasar. Despite this limitation, the absorption-line approach has proven successful, as recently confirmed by \citet{Nicastro2018}  \citep[see also,][]{Nicastro2018_b}. Based on measurements of O\,\textsc{vii} absorption lines in the X-ray spectra of a blazar at $z=0.48$, the authors claim the detection of a significant fraction of the missing baryons in the WHIM.

An alternative way to investigate the gas in the WHIM is through the Sunyaev-Zel'dovich effect \citep[SZE,][]{Sunyaev1972,Mroczkowski2019}. Recent works have shown the potential of the SZE in terms of constraining the distribution and abundance of gas in the WHIM \citep{Hernandez2015,Hill2016,deGraaff2019,Tanimura2019,Lim2020,Chaves-Montero2021}. In this context, future instruments such as CMB-S4 \citep{Abazajian2016} are expected to be crucial to shed light onto the missing baryon problem.

From a theoretical perspective, hydrodynamical cosmological simulations have proven to be a useful and reliable tool to investigate the location and distribution of baryons in the cosmic web \citep{Cen1999,Dave2001,Cen2006,Shull2012,Roca2016,Suresh2017,GarragaEspinosa2021}. In fact, several analyses based on hydrodynamical simulations predict that the missing baryons are in the form of warm-hot diffuse gas located between galaxies in the circumgalactic medium (CGM) and beyond the virial radius in the intergalactic medium (IGM). Moreover, these simulations have shown that star formation regulates the production rate of metals, while processes such as supernova feedback, galactic winds, and active galactic nucleus (AGN) feedback are capable of expelling the enriched hot gas into the CGM and IGM \citep{Cen2006,Theuns2002,Oppenheimer2006,Cen2011,Tescari2011,Rahmati2016,Wijers2020}. In this intricate scenario, the impact of metals on the cooling properties of gas must also be considered.

In this work, we use the IllustrisTNG hydrodynamical cosmological simulation suite \citep{Pillepich2018b,Pillepich2018,Nelson2018_ColorBim,Nelson2018_Oxigen,Nelson2019,Marinacci2018,Naiman2018,Springel2018}
to investigate the evolution and distribution of ionized metals across cosmic time, between $z=0-6$. Our main goal is to provide a theoretical analysis to track the evolution of the different ionized metals in time. IllustrisTNG has proven capable of reproducing different observational features of galaxy formation and evolution, such as the evolution of the galaxy mass-metallicity relation, the galaxy color bimodality, and the cosmic star formation rate, among others. In particular, \citet{Nelson2018_Oxigen} use this simulation to investigate the spatial distribution and physical properties of O\,\textsc{vi}, O\,\textsc{vii}, and O\,\textsc{viii} in the CGM and IGM. Their results show that IllustrisTNG achieves a good level of agreement with observations of the column density distribution function for O\,\textsc{vi} at low redshift \citep{Danforth2008,Thom2008,Tripp2008,Danforth2016}.
\citet{Nelson2018_Oxigen} also explore the impact of AGN and stellar feedback on the physical state of the CGM. Their results suggest that these mechanisms are fundamental drivers of the properties of the CGM. In particular, the low-accretion AGN feedback is crucial to explaining the differences in the N$_{{\rm O}\,\textsc{vi}}$ columns between  star-forming and quiescent galaxies.

Our analysis focuses on a selected set of seven ions (C\,\textsc{ii}, C\,\textsc{iv}, Mg\,\textsc{ii}, N\,\textsc{v}, Ne\,\textsc{viii}, O\,\textsc{vi}, and Si\,\textsc{iv}), which are chosen because they are the ones more commonly detected in observations\footnote{In particular, absorption lines from C\,\textsc{ii}, C\,\textsc{iv}, O\,\textsc{vi}, Mg\,\textsc{ii}, and Si\,\textsc{iv} are commonly detected by quasar spectra.}. For this set of ions, we study their distribution in the cosmic web (filaments, knots and voids) along with their abundances in the different gas phases across cosmic time. Our procedure follows that of \citet{Haider2016} but it is applied to a more sophisticated hydrodynamical simulation.

The structure of the paper is the following. In \S~\ref{sec:SimuAndMetods} we provide a summary of the main properties of the IllustrisTNG simulations (\ref{sec:simu}), and the methodology adopted to identify the cosmic web (\ref{sec:definition_cosmicWeb}), and gas phases (\ref{sec:definition_ions}).
The results are presented in \S~\ref{sec:results}. Finally, the summary and conclusions are presented in \S~\ref{sec:conclusions}.

\section{Simulation \& Methods}\label{sec:SimuAndMetods}
\subsection{Simulation data}\label{sec:simu}

The main results of this paper are based on the IllustrisTNG\footnote{http://www.tng-project.org} project, whereas the previous Illustris simulation is used for comparison. IllustrisTNG is a suite of magneto-hydrodynamical cosmological simulations that model the formation and evolution of galaxies within the standard $\Lambda$-CDM paradigm \citep{Pillepich2018b,Pillepich2018,Nelson2018_ColorBim,Nelson2018_Oxigen,Nelson2019,Marinacci2018,Naiman2018,Springel2018}.
IllustrisTNG is performed with the moving-mesh {\sc arepo} code \citep{Springel2010}
and based on the sub-grid models implemented on the previous Illustris simulation \citep{Vogelsberger2014,Genel2014,Sijacki2015}.

The main improvements provided by IllustrisTNG as compared to its predecessor are the inclusion of magneto-hydrodynamics, an updated scheme for galactic winds, and a new kinetic black hole feedback model for the low accretion state \citep[see,][for further details]{Pillepich2018,Weinberger2017}.
IllustrisTNG includes sub-grid models that accounts for physical processes in galaxies such as star-formation,
metal-line gas cooling, stellar feedback from supernovae Type Ia, II and asymptotic giant branch stars (AGB),
and AGN feedback.
The model also follows the production and evolution of the following nine elements: H, He, C, N, O, Ne, Mg, Si, and Fe.
The model includes an update of the tabulated stellar yields
for the different stellar feedback channels \citep[see][for further  details]{Naiman2018,Pillepich2018}.
The sub-grid parameters of IllustrisTNG were calibrated to reproduce the cosmic star formation density, the galaxy stellar mass function at present, and the stellar-to-halo mass relation at $z=0$ \citep{Pillepich2018}.

The IllustrisTNG suite consists of simulations with three different box sizes publicly available on the website \citep{Nelson2019}. In this work, we use
two of the boxes: the ones with 75~$h^{-1}$~Mpc~(=~110.7~Mpc) and 205~$h^{-1}$~Mpc~(=~302.6~Mpc) side lengths (hereafter TNG100 and TNG300, respectively). Both boxes were run from $z=127$ up to $z=0$.
In TNG100, dark matter particles and gas cells are modeled initially through 1820$^3$ elements each, with masses of
$7.46\times10^{6}~{\rm M}_{\odot}$ and $1.39\times10^{6}~{\rm M}_{\odot}$, respectively.
The TNG300 run, conversely, follows dark matter and gas using 2500$^3$ elements each, with masses of
$5.88\times10^{7}~{\rm M}_{\odot}$ and $1.1\times10^{7}~{\rm M}_{\odot}$, respectively.
The gravitational softening lengths for dark matter and stars is of 1.0~$h^{-1}$~kpc for TNG300
and 0.5~$h^{-1}$~kpc for TNG100. The
IllustrisTNG suite was run using the  \cite{Planck2016} cosmology, defined by the following cosmological parameters:
$\Omega_{\rm m} = 0.3089$, $\Omega_{\rm b} = 0.0486$, $\Omega_{\Lambda}=0.6911$, ${\rm H}_{0} = 100~h~{\rm km~s^{-1}~Mpc^{-1}}$,
$h=0.6774$, spectral index $n_{s} = 0.9667$ and normalization $\sigma_{8} = 0.8159$.

 The IllustrisTNG suite presents excellent agreement with important observational constraints such as the galaxy color bimodality at low redshift \citep{Nelson2018_ColorBim},
the galaxy clustering at $z=0.1$ \citep{Springel2018}, the stellar mass content of galaxy clusters \citep{Pillepich2018b}, the black hole -- stellar mass relation \citep{Weinberger2018}, and the mass-metallicity evolution of galaxies \citep{Torrey2019}.

In the more specific context of this work, IllustrisTNG
has shown good agreement with several CGM and IGM properties reported from observations, which underpins the scientific relevance of our analysis. \citet{Nelson2018_Oxigen}, prove that the OVI content in the CGM and IGM is in good agreement with COS-Halos \citep[][]{Tumlinson2011}. Also, \citet{Truong2020} perform a complete analysis of the X-ray emission from diffuse, hot, metal-enriched gas with TNG50 and TNG100. Their results demonstrate that the IllustrisTNG suite is consistent with observed X-ray luminosity emitted by late- and early-type galaxies.
Other works such as \citet{Davies2020} and \citet{Terrazas2020} explore gas properties in the CGM, suggesting a strong correlation with the specific star formation rate of the galaxies.
\citet{Nelson2019} investigates the outflows and dynamics of gas, whereas \citet{Nelson2020,Nelson2021} focus on the cold gas in the CGM through MgII covering fractions in luminous red galaxies.
Finally, \citet{Torrey2019} prove that the IllustrisTNG suite includes a comprehensive feedback model that widely distributes the metal budget into different gas phases.
All these results make us confident that the IllustrisTNG simulation is suitable for the goal of the present work.

In the first part, we make use of the gravitationally bound dark matter haloes from each simulation. In the Illustris and IllustrisTNG simulations, haloes are identified using a friends-of-friends algorithm (FOF) that adopts a linking length of 0.2 times the mean inter-particle separation \citep{Davis1985}.
We characterize the mass of the dark matter haloes using M$_{\rm 500c}$, defined as the mass enclosed within a sphere of radius R$_{\rm 500c}$ (i.e., the radius at which the enclosed density equals 500 times the critical density). The total baryonic mass of each halo is also computed within a sphere of radius R$_{\rm 500c}$, referred to as M$_{\rm 500,baryon}$.

\subsection{Cosmic-web and gas-phase classifications}\label{sec:definition_cosmicWeb}

\begin{figure*}
\centering

 \large{$z=0$}
  \medskip

 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/Void_grid_dm_L75n1820TNG_99_abs1e-30_0_1.pdf}
 \caption*{Voids ($< 0.1 \rho_{\rm crit,0}$)}\label{fig:distr_voids}
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/Filament_grid_dm_L75n1820TNG_99_abs0_1_57.pdf}
 \caption*{Filaments ($0.1-57 \rho_{\rm crit,0}$)}\label{fig:distr_filaments}
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/Halo_grid_dm_L75n1820TNG_99_abs57_1e+30.pdf}
 \caption*{Haloes ($> 57 \rho_{\rm crit,0}$)}\label{fig:distr_haloes}
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/DMDens_255.pdf}
 \caption*{Dark matter density}\label{fig:distr_dens}
 \end{subfigure}

  \medskip
  \medskip

 \large{$z=2$}
  \medskip

 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/Void_grid_dm_L75n1820TNG_33_abs1e-30_0_1.pdf}
 \caption*{Voids ($< 0.1 \rho_{\rm crit,0}$)
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/Filament_grid_dm_L75n1820TNG_33_abs0_1_57.pdf}
 \caption*{Filaments ($0.1-57 \rho_{\rm crit,0}$)
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/Halo_grid_dm_L75n1820TNG_33_abs57_1e+30.pdf}
 \caption*{Haloes ($> 57 \rho_{\rm crit,0}$)
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/DMDens_255_snap33.pdf}
 \caption*{Dark matter density
 \end{subfigure}

  \medskip
  \medskip

 \large{$z=6$}
   \medskip

 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/Void_grid_dm_L75n1820TNG_13_abs1e-30_0_1.pdf}
 \caption*{Voids ($< 0.1 \rho_{\rm crit,0}$)}\label{fig:distr_voids}
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/Filament_grid_dm_L75n1820TNG_13_abs0_1_57.pdf}
 \caption*{Filaments ($0.1-57 \rho_{\rm crit,0}$)}\label{fig:distr_filaments}
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/Halo_grid_dm_L75n1820TNG_13_abs57_1e+30.pdf}
 \caption*{Haloes ($> 57 \rho_{\rm crit,0}$)}\label{fig:distr_haloes}
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \includegraphics[width=\textwidth]{./fig/DMDens_255_snap13.pdf}
 \caption*{Dark matter density}\label{fig:distr_dens}
 \end{subfigure}
\caption{Spatial distribution of the different cosmic-web regions (voids, filaments, and haloes/knots) for a slice of TNG100 at $z=0$, 2, and 6  (top, middle, and bottom panel, respectively). The cells corresponding to each region are drawn in white, otherwise they are in black. The haloes are highlighted with larger white points to make the figure more clear.
The rightmost panel shows the local comoving dark matter density to facilitate the comparison. }\label{fig:regions}
\end{figure*}

We use the comoving local dark matter density to identify different cosmic-web environments in the simulations, following the methodology of \citet{Haider2016}\footnote{Our method differs only slightly from that of \citet{Haider2016}. While they use the average dark matter densities in cells over a volume of (104 kpc)$^{3}$ each, we implement the local dark matter density available in the IllustrisTNG database, computed in spheres with $\sim 3-60 {\rm kpc}$ of diameter at $z=0$.}. In this work, the comoving local dark matter density ($\rho_{dm}$) of each gas cell is estimated as the standard cubic-spline SPH kernel over a radius enclosing 64$\pm$4 dark matter particles\footnote{SubfindDMDensity, on the IllustrisTNG database.}. Our criteria to define environments is the following:
\begin{itemize}
    \item \textit{Haloes} (or knots) are regions where $\rho_{dm}~>~57~\rho_{\rm crit,0}$. This threshold corresponds approximately with the local density of a dark matter halo at its virial radius\footnote{The virial radius, R$_{200}$, is defined as the radius enclosing a region with density equal to 200 times the critical density.}, assuming a Navarro-Frenk-White density profile \citep[][]{Navarro1997}.
    \item \textit{Filaments} are defined as regions with local dark matter density $\rho_{dm} = 0.1 - 57$~$\rho_{\rm crit,0}$. This definition encloses also the concept of \textit{sheets} (see Appendix~\ref{fig:Appendix_CosmicStructures} for further details).
    \item \textit{Voids} correspond to regions with $\rho_{dm}<0.1$~$\rho_{\rm crit,0}$.
\end{itemize}

 Figure~\ref{fig:regions} illustrates the criteria adopted to identify the cosmic web components in a slice of the TNG100 box at $z=0$, 2, and 6. Voids, filaments, and haloes are shown in white. The right panel shows the local dark matter density for the same slice.
 The efficiency of our method in terms of tracing cosmic web structures have been shown in several other previous analyses \citep{Sousbie2011,Cautun2013,Cautun2014}. Note that this approach yields a cosmic web classification in agreement with that derived from tidal fields, for redshifts $z \lesssim 4$, as shown in \citet{Martizzi2018}. As stated by the authors, the main difference between these two approaches is the smoothing scales adopted. While our method employs a density field smoothed by the local SPH kernel (i.e., spheres of radius $\sim 1 - 20$~kpc/$h$ at $z=0$), the method based on the deformation tensor uses larger smoothing scales, of typically 2--6~Mpc/$h$. As a consequence, the local dark matter density field method is more subject to small-scale fluctuations.
As shown in Figure 3 of \citet{Martizzi2018}, the structures that are more likely to be affected by the smoothing length variations are the voids. At redshift $z \gtrsim 4$, the local dark matter density is typically $\sim \Omega_{\rm m} \rho_{\rm crit} > 0.1 \rho_{\rm crit}$, which implies that most of the mass will be assigned to filaments and haloes, rather than voids. At redshift $z \lesssim 4$ the two methods present similar trends for the different cosmic web structures.
Finally, \citet{Libeskind2018} presents a further analysis of the variations in the mass fractions for each cosmic structure based on different classification methods. As stated in \citet{Martizzi2018}, the differences found between the local dark matter density and the tidal deformation tensor approach are not larger than the deviations presented in \citet{Libeskind2018} for a total of twelve different methods.

To investigate the different gas components, we follow the same classification introduced by \citet{Dave2001} and \citet{Haider2016}, based on the comoving gas density,
$\rho_{\rm gas}$, and temperature, T, of each gas cell. Four different gas phases are defined in the following way:
\begin{itemize}
\item \textit{Diffuse gas}, when $\rho_{\rm gas} < 1000 \rho_{\rm crit,0} \Omega_{\rm b}$ and $T<10^{5}$~K. This gas phase is mainly comprised of neutral gas located in the IGM.
\item \textit{Condensed gas}, when $\rho_{\rm gas} > 1000 \rho_{\rm crit,0} \Omega_{\rm b}$ and $T<10^{5}$~K.
It selects the gas in star-forming regions and located in the ISM.
\item \textit{Warm-hot intergalactic medium gas} (WHIM), when $10^{5}~{\rm K} < {\rm T} < 10^{7}$~K.
This gas phase region represents the circumgalactic medium and hot gas in low-density regions located mainly in the IGM.
\item \textit{Hot gas}, when ${\rm T} > 10^{7}$~K. This component is mainly composed of shock-heated gas near massive haloes.
\end{itemize}

As explained by \citet{Martizzi2018}, and \citet{Torrey2019}, IllustrisTNG displays an artificial curvature in the gas phase diagram in the low-density and low-temperature regime, due to a minor numerical heating associated with the expansion of gas in low-density environments. Following the aforementioned papers, we adopt a temperature correction to the gas with density $\rho < 10^{-6} {\rm cm}^3$, in order to ensure that it follows an adiabatic equation of state, ${\rm T }\propto \rho^{\gamma - 1}$. We note, nevertheless, that these corrections do not impact the results of this work in any significant way.

\subsection{Ion abundances}\label{sec:definition_ions}

To compute the fraction of each element in the ionization state of interest, we use the tables developed by \citet{Bird2015}\footnote{See also: \url{https://github.com/sbird/cloudy\_tables}}. The tables were created using {\sc cloudy} version 13.02 \citep{Ferland2013} and calculating both collisional and photo-ionization processes in ionization equilibrium, exposed to a uniform ultraviolet background \citep[UVB][]{Faucher2009}.
{\sc cloudy} was run in single-zone mode adopting constant density and temperature for each gas element. Thus, thermal structures on scales smaller than the gas cells are neglected.
{\sc cloudy} also adopts a frequency dependent self-shielding from UVB at high densities using the fitting function of \citet{Rahmati2013} and solar abundances from \citet{Grevesse2010}. No local radiation sources are considered for running the tables.

The tables computed by \citet{Bird2015} cover a density range of $-7.0 < \log_{10}(n_{\rm H} [{\rm cm}^{-3}]) < 4.0$ and temperatures $3.0 < \log_{10}({\rm T}[{\rm K}]) < 8.6$, assuming a metallicity of ${\rm Z}=0.1{\rm Z_{\odot}}$\footnote{As stated by \citet{Nelson2018_Oxigen} the dependence of metallicity on the fraction of the ionized metals is minor. For this reason and following the same criterion as \citet{Bird2015}, the tables were computed using 1/10 of the solar metallicity.}.
For a given redshift, the ionized fraction of a species in a gas cell is selected from the tabulated values according to its temperature and density. The total mass of a given ionized metal in each gas cell is computed as the ionized fraction selected multiplied by the gas cell mass.

We note that IllustrisTNG adopts a two-phase model for star-forming gas cells \citep[][]{Springel2003}.
This assumption affects the abundance of the species in high-density and low-temperature regions.
To correct the effect of sub-grid physics, previous studies either place the star-forming cells to ${\rm T}=10^{3}~{\rm K}$ \citep[see e.g.,][]{Nelson2021}, or just simply neglect them from the analysis \citep[][]{DeFelippis2021}.
In our case, we have decided to keep the star-forming gas cell temperatures provided by the simulation, since they do not generate substantial changes in the results and conclusions of our analysis.

In this work, we study the following species:  C\,\textsc{ii}, C\,\textsc{iv}, Mg\,\textsc{ii}, N\,\textsc{v}, Ne\,\textsc{viii}, O\,\textsc{vi}, and Si\,\textsc{iv}. Each one of these metals maps different regions of the LSS of the Universe. Here we summarize the main properties reported in the literature for each case.
Mg\,\textsc{ii} in emission and absorption is typically detected in star-forming galaxies and planetary nebulae \citep{Rubin2010,Chen2017,Feltre2018}, and has shown to be a good tracer of star-forming regions and cold gas around galaxies \citep[typically at T$\sim10^4$~K, e.g.,][]{Bond2001,Steidel2002,Bouche2007,Weiner2009,Bouche2016,Chen2017}. In addition, different works have associate Mg\,\textsc{ii} absorption systems with galactic haloes \citep[see, e.g.,][]{Lanzetta1990}.  Mg\,\textsc{ii} has a ionization potential of $15.03~{\rm eV}$.
C\,\textsc{ii} is a good tracer of dense and low-temperature gas (n$_{\rm H} = 10^{2} - 10^{3}{\rm cm}^{-3}$, ${\rm T\sim 10^{4}} {\rm K}$ and ionization potential of $24.38~{\rm eV}$), associated with galactic haloes as well. It is also a star formation rate tracer and a major coolant for neutral atomic gas in the ISM \citep{Stacey1991,Wolfire2003,Stacey2010,Herrera-Camus2015}. C\,\textsc{iv} is a tracer of enriched gas in the IGM (with ${\rm n_{H} }\sim 10^{-1} {\rm cm^{-3}}$ and ionization potential of $64.49~{\rm eV}$). It is also mentioned as a good tracer of hot gas located in shock-heated regions and CGM \citep{DOdorico2010,Cooksey2010,
Danforth2016,Bouche2016,Chen2017}. Si\,\textsc{iv} in absorption is a strong doublet of Si and a good tracer of $\alpha$-elements and young metals. Si\,\textsc{iv} has a ionization potential of $45.14~{\rm eV}$, and is also typically present in high-density gas clouds \citep{Cooksey2011}.
Ne\,\textsc{viii} is mainly found in regions of gas at low densities and high temperatures  \citep[T~$\sim 10^5 - 10^6$~K, and n$_{H}\gtrsim10^{-4}~{\rm K}$, e.g.,][]{Meiring2013,Burchett2019}. Ne\,\textsc{viii} has a ionization potential of $239.09~{\rm eV}$.
N\,\textsc{v} has been shown to be a good tracer of the warm-hot CGM \citep[][]{Danforth2008}, and has a ionization potential of $97.89~{\rm eV}$.
O\,\textsc{vi} is a well-known tracer of warm hot gas in low-dense regions, typically located in galactic haloes and the CGM \citep[at T~$\gtrsim 2\times 10^4$~K, e.g.,][]{Werk2014,Roca-Fabrega2019}, with a ionization potential of $138.12~{\rm eV}$.
These features represent only a partial summary of each of the ionized metals studied in this work. We refer to the aforementioned references for further details.

\section{Results}\label{sec:results}

The results presented in this work address two main
aspects that are relevant to the missing baryons problem. First, we discuss the baryonic mass fraction (gas and stars) within dark matter haloes, as an extension of the results presented by \citet{Haider2016} for Illustris and \citet{Martizzi2018} for IllustrisTNG (Section~\ref{sec:baryons_haloes}).
The second part explores the distribution of ionized metals in the cosmic web (Section~\ref{sec:ions_cosmicWeb}) and in the density-temperature phase space (Section~\ref{sec:ions_phases}) across cosmic time.

\subsection{Baryon mass fraction in haloes}
\label{sec:baryons_haloes}

\begin{figure*}
\centering
\includegraphics[width=0.8\textwidth]{./fig/baryon_fraction_r500_99_vCel.pdf}
\caption{Baryon fraction as a function of the dark matter halo mass (M$_{500c}$). We compute the baryon and dark matter mass
within R$_{500c}$ at $z=0$ for Illustris (dashed lines), TNG100 (solid lines), and TNG300 (dotted lines).
We compare our results with observational data from \citet{McGaugh2010} (baryons: black squares, stars: grey triangles) and \citet{Gonzalez2013} (grey diamonds). The observational results from \citet{McGaugh2010} belongs to a set of galaxies (from dwarf to clusters) for which the baryonic and stellar fractions were computed according to the gas and stellar dynamics. As stated by \citet{McGaugh2010}, a significant gas fraction might be hidden in a state unable to be detected, suggesting that the reported fraction is incomplete. The observational data from \citet{Gonzalez2013} corresponds to the hot-gas from twelve galaxy clusters.}
\label{fig:baryonsInHalos}
\end{figure*}

The baryon mass fraction is computed as the total baryonic mass within the radius at which the density is equal to 500 times the critical density, M$_{\rm 500,baryons}$, normalized by the relative cosmological value, i.e., $[\Omega_{\rm b}/\Omega_{m}]{\rm M}_{\rm 500c}$.
Figure~\ref{fig:baryonsInHalos} presents the baryon mass fraction as a function of the halo mass at $z=0$, for haloes with M$_{\rm 500c} > 10^{9} {\rm M}_{\odot}$.
To analyse the impact of resolution and subgrid models, Figure~\ref{fig:baryonsInHalos} displays the results obtained for Illustris, TNG100, and TNG300.
We split the contribution from stars, hot gas (${\rm T}>10^{5}$K), and cold gas (${\rm T}<10^{5}$K) and compare them with the observational data from \citet{McGaugh2010} and \citet{Gonzalez2013}. Our results show that the baryonic mass fractions of TNG100 and TNG300 follow similar trends for almost the entire halo mass range under analysis, with differences mostly caused by resolution/volume effects.
Namely, TNG300 is able to reproduce the observations for massive clusters (${\rm M}_{500c} > 10^{13} {\rm M}_{\odot}$), reaching values between 0.75 to 1 for the baryon fraction (gas and stars) and 0.1 to 0.3 for the stellar fraction. The TNG100 box reproduces well the observations for clusters with masses above $10^{13} {\rm M}_{\odot}$ and up to  $2 \times 10^{14} {\rm M}_{\odot}$. The very massive end is not accessible in TNG100 due to its small size, which explains the artificial drop in the baryonic fraction shown for the largest clusters in Figure~\ref{fig:baryonsInHalos}. As shown also in \citet{Genel2014} and \citet{Haider2016}, the Illustris simulation is unable to reproduce the observed total baryon fraction in massive clusters above ${\rm M}_{500c} \simeq 10^{13} {\rm M}_{\odot}$.

For haloes with masses ${\rm M}_{500c} < 10^{13} {\rm M}_{\odot}$, the stellar mass fractions of TNG100 and TNG300 are in reasonable agreement with the observational constraints reported by \citet{McGaugh2010}. The missing baryon problem from observational data manifests itself in the vanishing
baryonic mass fraction below ${\rm M}_{500c} \simeq 10^{12} {\rm M}_{\odot}$. The simulated haloes from the three boxes display, conversely, a high baryon mass fraction for low-mass haloes, reaching six times the observed fraction in the TNG300 box and twenty times in the Illustris simulation at $\sim 5\times 10^{10}{\rm M}_{\odot}$, respectively. It is noteworthy, however, that observational estimates might be severely affected by uncertainties: current observations are not able to detect the different gas phases within haloes in the way we do in simulations. In fact, more recent measurements of the baryonic mass fraction for haloes with masses around $10^{12}{\rm M}_{\odot}$ from the COS-Halos survey claim a significantly higher value (45\%), suggesting as well that at least half of the previously reported missing baryons might be located in the CGM \citep{Werk2014}. The comparison presented in Figure~\ref{fig:baryonsInHalos} must therefore be taken with caution, since it is subject to uncertainties in the observational constraints that are not necessarily accounted for by the reported errors.

The general agreement between TNG100 and TNG300 in Figure~\ref{fig:baryonsInHalos} is expected since both simulation boxes use the same sub-grid model.
This is not the case for Illustris, which explains the differences with respect to the aforementioned IllustrisTNG boxes.
In particular, previous reports have identified
several caveats in the Illustris stellar and AGN feedback models \citep{Genel2014,Haider2016, Pillepich2018}. The consequences of these issues are actually noticeable in Figure~\ref{fig:baryonsInHalos}: the stellar feedback model in Illustris is not efficient in removing gas in dark matter haloes below $10^{12} {\rm M}_{\odot}$, while the radio-mode AGN feedback produces strong outflows mainly in haloes above 10$^{12.5}$~M$_{\odot}$.
These processes have been revised in the updated IllustrisTNG model, where AGN feedback is now described in terms of low and high accretion states that account for kinetic and thermal feedback.
For haloes with ${\rm M}_{500c} < 10^{12} {\rm M}_{\odot}$, supernova feedback prevents star formation and removes gas through an updated model for galactic winds.

We proceed now to address the redshift evolution
of the mass fractions. These results are shown for haloes in Illustris, TNG100, and TNG300 in
Figure~\ref{fig:halo_evolution}. The mass fraction is computed for dark matter, baryons (split also in gas and stars), and the full mass (baryons and dark matter), normalized by its respective total mass for each case. We find that dark matter mass in haloes increases with time for the three boxes, with values that range from $\sim 5-7$\% at $z=6$ to $\sim 40-55$\% at $z=0$ . The same behaviour is, as expected, found for the full mass fraction, since dark matter dominates the mass budget of haloes.

The baryon fraction in haloes shows a different behaviour in Illustris as compared to IllustrisTNG at $z < 2$. The difference lies in the gas fraction: while TNG100 and TNG300 show a monotonic increase as the redshift decreases, Illustris presents an artificial drop in the gas fraction. As stated by \citet{Haider2016}, the decrease in the gas fraction is connected with the time that the radio mode AGN feedback becomes overly efficient at expelling gas from the inner regions to the outskirts. As Figure~\ref{fig:halo_evolution} demonstrates, the updated AGN feedback model in IllustrisTNG alleviates this problem.

The results presented in this section demonstrate that IllustrisTNG provides better agreement with observations than Illustris, which is a consequence of the improved subgrid model of the former. In the next section, we will go a step further and investigate the large-scale distribution of ionized metals.

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{./fig/Fraction_In_halos.pdf
\caption{Evolution of the mass fraction within dark matter haloes for TNG100 (solid lines), TNG300 (dotted lines) and Illustris-1 (dashed lines).
We show the mass fraction of dark matter (black lines), baryons (green lines), and the contribution from gas (cyan lines) and stars (yellow lines).
Each of these fractions is computed by normalizing by its respective total mass in each simulated volume.}
\label{fig:halo_evolution}
\end{figure}

\subsection{Ionized metals in the Cosmic Web}
\label{sec:ions_cosmicWeb}

\begin{figure*}
\centering
\includegraphics[width=0.47\textwidth]{./fig/Mass_metal_distribution33_NormRhoMean.pdf}
\includegraphics[width=0.47\textwidth]{./fig/Mass_metal_distribution99_NormRhoMean.pdf}
\caption{Mass distribution as a function of the local dark matter density, normalized by the mean density for TNG100 (solid lines), and TNG300 (dotted lines) at $z=0$ and 2.
The dashed vertical lines indicate the boundaries between the voids, filaments and haloes.}
\label{fig:mass_distribution}
 \end{figure*}

\begin{figure*}
\centering
\includegraphics[width=0.47\textwidth]{./fig/mass_metalION_distributionNorm33_wNormRhoMean_Corr.pdf}
\includegraphics[width=0.45\textwidth]{./fig/mass_metalION_distributionNorm99_wNormRhoMean_Corr.pdf}
\caption{Fraction of ions, as a function of the local dark matter density at $z=2$ (\textit{left panel}) and $z=0$ (\textit{right panel}),
for TNG100. The fraction of ions is computed as the mass at a fixed local dark matter density, normalized by the total mass of each ion.
The local dark matter density is also normalized by the mean dark matter of the simulated box.
Vertical black dotted lines represent the criterion adopted to identify the haloes, filaments and voids. The double peak of C\,\textsc{iv} and N\,\textsc{v} at $z=2$, and of Si\,\textsc{iv} at $z=0$ must be interpreted with caution, since these peaks are produced by star-forming gas affected by the sub-grid physics of the simulation (see Section~\ref{sec:definition_ions}).}
\label{fig:ions_distribution}
 \end{figure*}

We begin by analyzing the performance of the method adopted to trace the cosmic web (described in Section~\ref{sec:definition_cosmicWeb}). Figure~\ref{fig:mass_distribution} shows the distribution of the mass fraction of baryons, stars, metals\footnote{The mass fraction of metals (which in turn represents a portion of the baryons) is computed by selecting all the metal elements heavier than He.}, and dark matter at $z=0$ and 2
in TNG100 and TNG300, as a function of the comoving local dark matter density normalized by its mean density (i.e., $\rho_{dm}/\bar{\rho}_{dm}$, where $\bar{\rho}_{dm} = \Omega_{dm}$ $\rho_\textrm{\small crit,0}$). Dotted vertical lines indicate the criterion to define voids ($\rho_{dm} < 0.1$~$\rho_\textrm{\small crit,0}$), filaments ($\rho_{dm}$ = 0.1 - 57~$\rho_\textrm{\small crit,0}$), and haloes ($\rho_{dm} > 57$~$\rho_\textrm{\small crit,0}$).

From the comparison of the two panels of Figure~\ref{fig:mass_distribution}, we find that metals slightly move from high-density to low-density regions as the redshift decreases. This is probably a consequence of the outflows and chemical enrichment produced by the stellar and AGN feedback processes, which tend to transport enriched gas from haloes to voids and filaments.
Conversely, dark matter is unaffected by baryonic processes on large scales. It continues assembling and condensing in filaments and haloes, as Figure~\ref{fig:mass_distribution} demonstrates. Good agreement is again found between the distributions obtained with TNG100 and TNG300, confirming that resolution does not affect the results and main conclusions of this work in any significant way.
For simplicity, the analysis of the ionized metals is presented in what follows only for the higher-resolution TNG100 box, since similar trends are obtained for the TNG300 box.
Finally, the cosmic evolution of the total baryonic budget in IllustrisTNG is discussed in detail in \citet{Martizzi2018,Martizzi2020} and is out of the scope of this work. We review some of the main features in Appendix~\ref{fig:Appendix_CosmicStructures}.

Figure~\ref{fig:ions_distribution} displays the distribution of our set of ionized metals as a function of the local dark matter density normalized by its mean density, $\rho_{dm}/\bar{\rho}_{dm}$, at $z=0$ and 2 for TNG100. The fraction of ions is computed as the mass of each ion normalized by its total mass at a fixed local dark matter density. Again, dotted vertical lines represent the criterion to define voids, filaments and haloes. Our results show that C\,\textsc{ii}, Mg\,\textsc{ii} and Si\,\textsc{iv} are significantly more abundant in haloes than in filaments and voids, both at $z=2$ and 0. At $z=2$ these three ions concentrate in haloes with local dark matter densities around $\rho_{dm}/\bar{\rho}_{dm} \sim 10^4 - 10^5$. At $z=0$, the distribution remains in the same range for Mg\,\textsc{ii} and C\,\textsc{ii} but splits into two peaks at low and very high densities for Si\,\textsc{iv}. O\,\textsc{vi}, C\,\textsc{iv}, Ne\,\textsc{viii}, and N\,\textsc{v} tend to move from haloes and filaments at $z=2$ to voids and filaments at $z=0$ (towards lower-density regions in general). These ions display a peak in their fractions for local dark matter densities of $\rho_{dm}/\bar{\rho}_{dm} \sim 10 - 10^2$ at $z=0$.  Figure~\ref{fig:ions_distribution} also shows a bimodal distribution for C\,\textsc{iv} and N\,\textsc{v} at $z=2$, reflecting the presence of collisionally ionized gas in dense regions. The same result is found for Si\,\textsc{iv} at $z=0$. These features, however, must be interpreted with caution, since they are produced by ionized metals in star-forming gas cells (see Section~\ref{sec:definition_ions}). In order to investigate the impact of the sub-grid model on the mass distributions, we have replaced
the tabulated temperature of the star-forming cells by a fixed value of 10$^3$~K \citep[based on other recent analyses,][]{Nelson2021}. We have checked that imposing this value effectively removes the double peak in C\,\textsc{iv}, N\,\textsc{v}, and Si\,\textsc{iv}, while maintaining the overall shape of the mass distributions displayed in Figure~\ref{fig:ions_distribution}.

\begin{figure*}
\centering
\includegraphics[width=0.95\textwidth]{./fig/evo_IONsHaloFilamentsVoids_Norm0.pdf}
\caption{Fraction of the ionized metals as a function of redshift, split in voids, filaments and haloes for TNG100.
It is computed as the total mass of each ionized metal at a given redshift
normalized by its total mass budget at $z=0$, (i.e., $f_{\rm ion} = M_{X, z} / M_{X,z=0}$).
}
\label{fig:ions_VoidsFilamentsHaloes}
\end{figure*}

To investigate in more detail the evolution of each ion, Figure~\ref{fig:ions_VoidsFilamentsHaloes} shows the mass fraction for each ionized metal in voids, filaments, and haloes normalized by the total mass of each ion at $z=0$ (i.e., f$_{\rm ion} = M_{X, z} / M_{X,z=0}$) for the redshifts $z=0-6$. Using f$_{\rm ion}$ allows us to trace the evolution of the mass budget with redshift in an effective way since the abundance of metals increases with time.
At first glance, our results show that most of the mass budget for all the ionized metals under analysis is either in filaments or haloes throughout the entire redshift range considered. However, each one presents different properties and evolution across cosmic time. We now proceed to analyse the contribution of the ions to the mass budget in each cosmic web region. In voids, the highest contribution belongs to O\,\textsc{vi} and Ne\,\textsc{viii}, but
N\,\textsc{v} and C\,\textsc{iv} are also present. All of these ions increase their mass fractions towards lower redshift. C\,\textsc{ii}, Mg\,\textsc{ii}, and Si\,\textsc{iv} are not found in this cosmic web environment.

For filaments, O\,\textsc{vi}, N\,\textsc{v}, and Ne\,\textsc{viii} show a similar and significant increase of their mass fractions as redshift decrease, of a factor $\sim$60 from $z=6$ to $z=0$. We note that most of the mass budget for Ne\,\textsc{viii} and O\,\textsc{vi} is located in this region of the cosmic web. Their large abundance in filaments has been reported by previous observational and numerical studies, showing that O\,\textsc{vi} is an excellent tracer of filamentary diffuse and warm gas between clusters \citep[see e.g.,][]{Nicastro2017,Nicastro2018,Tepper-Garcia2011,Tejos2016,Marra2020,Strawn2020}. This characteristic makes O\,\textsc{vi} arguably one of the best ``footprints" of missing baryons together with O\,\textsc{vii} and O\,\textsc{viii}. The evolution of the mass fractions for O\,\textsc{vi}, N\,\textsc{v}, and Ne\,\textsc{viii}
is determined by the chemical enrichment of the gas due to stellar evolution and feedback, together with virial shock-heating increasing its temperature \citep[see e.g.,][]{Tepper-Garcia2011,Faerman2017}. It is also noteworthy that the mass fractions of C\,\textsc{iv} and Si\,\textsc{iv} in filaments are roughly flat, showing almost no redshift dependence.
Finally, the contribution of C\,\textsc{ii} and Mg\,\textsc{ii} is only visible, although tiny ($<1\%$), at low redshift, around $z\sim0-2$.

Figure~\ref{fig:ions_VoidsFilamentsHaloes} shows that haloes contain all ionized metals over the entire redshift range, albeit in different proportions.  Interestingly, two different behaviours are observed for the set of ions investigated. While all metals begin increasing their fractions at high redshift, Si\,\textsc{iv}, C\,\textsc{iv}, N\,\textsc{v}, and O\,\textsc{vi}, seems to reach their peak abundances around $z\sim2$, which roughly coincides with the peak of the cosmic star formation rate. At lower redshifts, the evolution of these ions either stalls or their abundances actually drop. Conversely, the fractions of C\,\textsc{ii} and Mg\,\textsc{ii} continue rising towards lower redshift and only seem to reach a plateau, if anything, at $z=0$. At face value, these results indicate that Si\,\textsc{iv}, C\,\textsc{iv}, N\,\textsc{v}, and O\,\textsc{vi} in haloes are strongly affected by stellar and AGN feedback mechanisms, together with gas recycling and radiative cooling. While the total mass budget of each metal increases with time, the ionization species are influenced by gas cooling, and star formation in dense regions. The contribution of all these effects together may explain the cosmic evolution of the mass fractions for Si\,\textsc{iv}, C\,\textsc{iv}, N\,\textsc{v}, and O\,\textsc{vi} in haloes.

\subsection{Ionized metals in density-temperature phase space}
\label{sec:ions_phases}

\begin{figure*}
\centering
\includegraphics[width=1.\textwidth]{./fig/plotTvsBaryonHistogram-IONS-FINAL.pdf}
\caption{Gas density--temperature diagram at redshifts $z=0, 0.1, 1$, and 2 (from top left to bottom right, respectively) for the TNG100 simulation.
The colour map represents the mass fraction of gas, while the contours indicate the regions enclosing 80 per-cent the mass of the ionized metals Mg\,\textsc{ii}, Ne\,\textsc{viii}, N\,\textsc{v}, O\,\textsc{vi}, Si\,\textsc{iv}, C\,\textsc{ii} and C\,\textsc{iv}.
Black dashed lines demarcate the gas phases adopted in this work (hot, WHIM, diffuse, and condensed). }
\label{fig:T_rho_ions}
\end{figure*}

\begin{figure*}
\centering
\begin{subfigure}{0.24\linewidth}
 \caption{\centering Voids+Filaments+Haloes}
  \includegraphics[width=\textwidth]{./fig/L75n1820TNG_PhaseDistrib_ALL_CHECK.pdf}
 \end{subfigure}
\begin{subfigure}{0.24\linewidth}
 \caption{\centering Voids}
 \includegraphics[width=\textwidth]{./fig/L75n1820TNG_PhaseDistrib_VOIDS.pdf}
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \caption{\centering Filaments}
 \includegraphics[width=\textwidth]{./fig/L75n1820TNG_PhaseDistrib_FILAMENTS.pdf}
 \end{subfigure}
 \begin{subfigure}{0.24\linewidth}
 \caption{\centering Haloes}
 \includegraphics[width=\textwidth]{./fig/L75n1820TNG_PhaseDistrib_HALOS.pdf}
 \end{subfigure}
\caption{Cosmic evolution of the mass fraction for the ionized metals normalized by the mass of each ion at $z=0$ (f$_{\rm ion}$ = M$_{\rm ionized\,metal,z}$/M$_{\rm ionized\,metal,z=0}$) split by gas phase in diffuse (green), WHIM (red), condensed gas (blue) and hot gas (yellow). We also divide the sample according the cosmic-web definition. From left to right: all the sample (voids+filaments+haloes), voids, filaments, and haloes.
Faint lines are used for condensed gas in voids to indicate that the fractions are computed with less than $10^4$ gas cells (see Section~\ref{sec:ions_phases} for further details). The results correspond to the TNG100 box.}
\label{fig:gasPhase_evol_ions}
\end{figure*}

We proceed now to investigate the distribution of ionized metals in the different gas phases. Figure~\ref{fig:T_rho_ions} shows the mass fraction of gas of the total baryonic mass in the density--temperature diagram for TNG100 at $z=0$, 0.1, 1, and 2. Vertical and horizontal lines demarcate the different gas-phase regions adopted.
We start by analysing the evolution of the diffuse phase, typically associated with the intergalactic low-dense and low-temperature gas. Our results indicate that this gas phase comprises 75.3 percent of the gas at $z=2$, a fraction that decreases significantly, to 37.3 per cent, at $z=0$. In addition, the comparison of the different panels shows that a large amount of diffuse cold gas increases its temperature with time, moving to the WHIM and hot phases. This is a consequence of the different feedback mechanisms and galactic outflows heating and ionizing the gas that reaches the ICM and IGM.

Both the WHIM and hot-gas phases display an increase in the mass fraction with time. The WHIM phase makes up 17.8 per cent of the total gas at $z=2$, reaching 46.6 per cent at $z=0$. On the other hand, only 0.2 per cent of the gas is located in the hot phase at $z=2$, while this fraction raises to 6.8 per cent at $z=0$. The mass fractions for the different gas phases from $z=6$ to $z=0$ are listed in Table~\ref{table:mass_fraction}. We note that a comparison with previous works is difficult since the definitions of gas phases vary in the literature - the definition chosen for this work follows the one adopted in \citet{Haider2016}. Regardless of the definitions employed, our results are qualitatively in good agreement with previous findings  \citep[e.g.,][]{Rahmati2013,Oppenheimer2016}.

\begin{table*}
\caption{Mass fraction of baryons in the different gas phases at $z=0, 0.1, 1, 2, 3, 4, 5,$ and 6 for TNG100.}
\label{table:mass_fraction}
\centering
\begin{tabular}{lcccccccc}
\hline
            &  $z=0$ & $z=0.1$  & $z=1$ & $z=2$ & $z=3$ & $z=4$ & $z=5$ & $z=6$ \\
\hline
Condensed & 0.041 &  0.042  &  0.051 & 0.047 & 0.036 & 0.025 & 0.013 & 0.007 \\
Diffuse   & 0.373 & 0.387   &  0.564 & 0.753 & 0.863 & 0.923 & 0.961 & 0.977 \\
WHIM      & 0.466 & 0.463   &  0.335 & 0.178 & 0.091 & 0.047 & 0.024 & 0.014 \\
Hot       & 0.068 & 0.058   & 0.015  & 0.002 & 0.001 & 3.45$\times$10$^{-5}$ & 3.12$\times$10$^{-6}$ & 4.08$\times$10$^{-8}$\\
\hline
\end{tabular}
\end{table*}

The contours in Figure~\ref{fig:T_rho_ions} represent the regions enclosing 80 per cent of the total mass for each ionized metal. Particularly interesting in the context of the missing baryons problem is the evolution of Ne\,\textsc{viii}, O\,\textsc{vi}, and N\,\textsc{v}, which remain excellent tracers of the WHIM and diffuse gas throughout the redshift range considered. A fraction of these ions residing in diffuse gas at high redshift is in fact progressively pushed towards the WHIM gas phase by shock-heating and feedback processes that tend to increase gas temperature (this is particularly evident for Ne\,\textsc{viii}).
Also, a significant fraction of C\,\textsc{iv} is located in the diffuse and WHIM gas phases. As expected, Si\,\textsc{iv}, Mg\,\textsc{ii}, and C\,\textsc{ii} are, on the other hand, good tracers of the condensed gas up to high redshift.

Finally, Figure~\ref{fig:gasPhase_evol_ions} provides a complete summary of the main results presented in this paper regarding the cosmic evolution of ionized metals. The figure displays the mass fraction  normalized by the total mass of each ion at $z=0$ (f$_{\rm ion}$, defined as in Figure~\ref{fig:ions_VoidsFilamentsHaloes}) in condensed, diffuse, WHIM, and hot gas as a function of redshift and cosmic
web environment. In the remainder of this section, we will describe the main features found.

For condensed gas, our results show that the abundance of C\,\textsc{iv},  Ne\,\textsc{viii}, N\,\textsc{v},  O\,\textsc{vi}, and  Si\,\textsc{iv}, typically increases from early on, peaking at $z\sim2$. The trends found for these ionized metals resemble the evolution of the cosmic star formation rate, and it can be explained as a direct consequence of the chemical enrichment from different feedback mechanisms together with gas cooling and metal recycling in dense regions \citep[][]{Pillepich2018}.
On the other hand, C\,\textsc{ii} and Mg\,\textsc{ii} continue growing in mass up to $z=0$ (see Figure~\ref{fig:gasPhase_evol_ions}--a).

When the cosmic web environments are taken into account, we find that the mass fractions at $z=0$ in the condensed gas phase in haloes are 0.99 for C\,\textsc{ii} and Mg\,\textsc{ii}, while a value of 0.75 is measured for Si\,\textsc{iv} (Figure~\ref{fig:gasPhase_evol_ions}--d). Our results indicate that these metals are mostly in high-density and low-temperature regions. The mass fractions for the remaining ions in the condensed gas phase are distributed in haloes and filaments.
As an example, C\,\textsc{iv} in condensed gas phase has a mass fraction of $\sim 0.1$ in haloes and $\sim0.005$ in filaments at $z=0$.

The connection between haloes and the condensed phase is easily understood, since both criteria map the densest and lowest-temperature regions of the Universe. These findings are in line with previous works. As an example, Mg\,\textsc{ii} has shown to be abundant in galactic haloes of luminous and massive galaxies, thus tracing the gas in transition between the IGM and the ISM. These are condensed and low-temperature gas regions, suggesting that  Mg\,\textsc{ii} is indeed a good tracer of star formation, galactic outflows, and accreted gas \citep[see e.g.,][]{Steidel2002,Zibetti2007,Weiner2009,Rubin2010,Martin2012,Rubin2012,Dutta2020,Anand2021}. It is also noteworthy that results obtained for the condensed phase should be treated with caution since numerical codes do not resolve properly the high-density low-temperature gas, due to a transition in sub-grid scaling for cooling and mass flow \citep[see][]{Chen2017,Vogelsberger2014}. Finally, we note that all the ionized metals in condensed gas in voids are modelled with less than $10^{4}$ cells over the entire TNG100 volume, resulting in a stochastic behavior for the trends. To indicate this caveat, we use blue faint lines for condensed gas in Figure~\ref{fig:gasPhase_evol_ions}--b.

A significant amount of C\,\textsc{iv}, N\,\textsc{v}, O\,\textsc{vi}, and Si\,\textsc{iv} is measured in a diffuse gas phase (f$_{\rm ion}$=0.48, 0.32, 0.23, 0.17 at $z=0$, respectively).
In particular, the mass fractions of N\,\textsc{v} and  O\,\textsc{vi} increase as redshift decreases.
Conversely, Mg\,\textsc{ii} and Si\,\textsc{iv} present a significant drop in their diffuse-gas mass fractions around $z\sim2$, followed by a subsequent increase (a factor of $\sim 10^{2}$ of difference for the mass fractions between these redshifts).
This might indicate that a fraction of the latter in diffuse gas is accreted to high-density regions, shifting to the cold phase at $z\sim2$ and progressively moving to low-dense regions due to stellar winds after the star formation peak. C\,\textsc{ii} shows a nearly constant mass fraction of the order of $\sim 10^{-5}$ for diffuse gas between $z=6$ and $z=2$, increasing towards low redshifts and reaching a fraction of $\sim 0.007$ at $z=0$ (Figure~\ref{fig:gasPhase_evol_ions}-a).

As for the WHIM phase, the mass fractions of C\,\textsc{iv}, Ne\,\textsc{viii}, N\,\textsc{v}, and O\,\textsc{vi} at $z=0$ are 0.41, 0.91, 0.68, and 0.77, respectively (Figure~\ref{fig:gasPhase_evol_ions}-a). If we also consider the cosmic web environment, we find that for C\,\textsc{iv} the mass fraction at $z=0$ is $\sim 0.22$ in haloes and $\sim0.19$ in filaments.
Most of Ne\,\textsc{viii} in WHIM phase is in filaments (f$_{\rm ion}=0.66$ at $z=0$), while the fraction in haloes is $\sim 0.12$  and in voids $\sim 0.13$. Similar mass fractions are also found for  N\,\textsc{v}, O\,\textsc{vi}.
Again, our results confirm that these ions are unique tracers of warm and low-density gas, where most of the missing baryons at low redshift are expected to be stored. On the other hand, the mass fractions of C\,\textsc{ii}, Mg\,\textsc{ii}, and Si\,\textsc{iv} in the WHIM phase are lower than those of the other ions considered. These latter ions present a subtle increase with redshift with a maximum fraction at around $z\sim2-3$ and a turn-down from $z\sim 2$ to $z=0$.

Finally, none of the ionized metals under analysis keep a large mass reservoir in the hot phase. Namely,  Ne\,\textsc{viii} has a mass fraction of $4\times10^{-4}$ at $z\sim 0$, while for
O\,\textsc{vi} the measured fraction is $\sim 2.4\times10^{-6}$. The mass fractions are lower for C\,\textsc{iv} and N\,\textsc{v}, and no contribution is found for C\,\textsc{ii}, Mg\,\textsc{ii}, and Si\,\textsc{iv}. Overall, the mass budget in the hot gas phase increases towards low redshift.

To summarize, we have shown that each ionized metal displays complex features, localizing its mass budget in different proportions across different gas phases and cosmic web environments. These findings are in agreement with previously reported numerical and observational measurements. Of particular importance in the context of the missing baryon problem at low redshift are our results for O\,\textsc{vi}, N\,\textsc{v}, and Ne\,\textsc{viii} as tracers of the WHIM and diffuse gas in filaments \citep[see e.g.,][]{Cen2006,Werner2008,Tepper-Garcia2011,Rahmati2013,Werk2014,Nelson2018_Oxigen,Roca-Fabrega2019}. In this context, \citet{Tepper-Garcia2011} investigated the physical properties of O\,\textsc{vi} absorbers at low redshift in the OWLS simulation. Their results suggest that the bulk of O\,\textsc{vi} mass is in gas with overdensities of $\rho/\langle \rho \rangle = 10^{0.5} - 10^{2.5}$, and temperatures in the range ${\rm T}=10^{4}-10^{6}{\rm K}$. Hence, detectable O\,\textsc{vi} absorbers are good tracers of shock-heated over-enriched gas. Also \citet{Marra2020} investigated the enriched gas in the CGM around galaxies from the EAGLE simulation, finding that ions such as O\,\textsc{vi} and Ne\,\textsc{viii} constitute a large fraction of gas with ${\rm T}\sim 10^{5.5}-10^{7}$~K in massive systems. \citet{Burchett2019} studied the CGM of 29 galaxies with masses M$_{*} \sim 10^{9}-10^{11} {\rm M}_{\odot}$ at $0.49<z<1.44$. Their results suggest that Ne\,\textsc{viii} in CGM gas encompasses $\sim 6-20$\% of the total baryonic mass. Also \citet{Tejos2016} studied the gas in filaments connecting massive galaxy cluster pairs, showing that warm-hot gas ($10^5-10^6$~K) is enhanced within filaments.

In conclusion, the fact that O\,\textsc{vi}, N\,\textsc{v}, and Ne\,\textsc{viii} are located in filaments in the WHIM and diffuse gas phases, together with the fact that a significant baryonic mass budget is in these phases at $z=0$  ($>70\%$), adds up to the growing evidence that these ionized metals are good tracers of the missing baryons.

\section{Summary and conclusions}\label{sec:conclusions}

Understanding the evolution and distribution of metals on large scales provides information about the processes that regulate star formation and gas dynamics within and around galaxies. Moreover, studying these distributions allow us to map the baryons on large scales and thus shed light on the so-called missing baryon problem discussed at low redshift.
Current state-of-the-art hydrodynamical cosmological simulations have improved the way they model and reproduce different observational tracers, providing an exceptional tool to track the evolution of baryons across cosmic time \citep[see e.g.,][]{Cen1999,Cen2006,Cen2011,Tepper-Garcia2011,Oppenheimer2012,Oppenheimer2016,Nelson2018_Oxigen,Martizzi2018,Roca-Fabrega2019,Marra2020,Martizzi2020,Strawn2020}. Despite this success, even the most accurate simulations producing self-consistent outflows also need calibration of their sub-grid models. This, in turn, impacts the hydrodynamics of the gas and distribution of metals. Different works have indeed confirmed the impact that sub-grid models have on the temperature distribution of the gas and its ionization state \citep[see e.g.,][]{Cen2011,Roncarelli2012,Oppenheimer2016}. Hence, caution must be exercised when comparing observational results with those obtained from hydrodynamical simulations.

    In this work, we investigate the large-scale distribution of ionized metals in the IllustrisTNG simulation across cosmic time, from $z=6$ to $z=0$. To this end, we use two different simulation boxes with the highest resolution available for each size in the IllustrisTNG suite: TNG100-1, with side length 75~$h^{-1}$~Mpc and  TNG300-1, spanning 205~$h^{-1}$~Mpc. The IllustrisTNG suite represents a revised version of the Illustris simulation, which among other features, reproduces the cosmic star formation rate, the galaxy stellar mass function, and includes updated prescriptions for the chemical yields -- all fundamental elements for this work.

With the aim of providing a revised vision of the missing baryon problem, we map the redshift evolution of seven ionized metals, C\,\textsc{ii}, C\,\textsc{iv}, N\,\textsc{v}, Ne\,\textsc{viii}, Mg\,\textsc{ii}, O\,\textsc{vi}, and Si\,\textsc{iv}, in the cosmic web (haloes, filaments, and voids), and in the different gas phases (WHIM, hot, diffuse, and condensed gas). The selected set of ionized metals is chosen because they are commonly detected in observations. Moreover, they are excellent tracers of the baryonic content on large scales, mapping the cosmic web and the different gas phases.
Our main results can be summarized as follows:
\begin{itemize}
    \item We find that the mass fraction of baryons in WHIM and hot-gas phases (with ${\rm T}>10^5$K) increases significantly as the redshift decreases. Namely, the WHIM phase represents 17.8 per cent of the gas at $z=2$, reaching 46.6  per cent at $z=0$. These trends are a consequence of galactic outflows heating and shifting the gas from high-density to low-density regions in the ICM and IGM (Figure~\ref{fig:T_rho_ions}).
    \item We show that each ionized metal maps different parts of the density-temperature diagram and cosmic-web environments. Furthermore, their total masses and distributions evolve with redshift as a consequence of chemical enrichment due to star formation, and AGN and stellar feedback processes together with strong kinetic outflows expelling enriched gas to the outer parts of the galaxy in the IGM.
    \item We find that most of the mass budget for C\,\textsc{ii} and Mg\,\textsc{ii} is in haloes in the condensed gas phase (at $z=0$ it represents 99 per cent of the mass fraction of each of these ions). Our findings suggest that C\,\textsc{ii} and Mg\,\textsc{ii} are excellent tracers of star-forming regions and the gas in transition between the IGM and the ISM (Figure~\ref{fig:ions_VoidsFilamentsHaloes}).
  \item
 Our findings show that C\,\textsc{iv} and Si\,\textsc{iv} present similar evolution in their mass fractions.
 For instance, the mass budget in condensed gas in haloes resembles the cosmic star formation rate evolution, with a maximum around $z\sim2$ (Figure~\ref{fig:gasPhase_evol_ions}-d). This is explained by chemical enrichment from stellar feedback combined with gas cooling in dense star-forming regions.
 At $z=0$, the mass fraction for C\,\textsc{iv} and Si\,\textsc{iv} in condensed gas inside haloes is $\sim 0.10$ and $\sim0.73$, respectively. The diffuse and WHIM-phase components of these ions show similar trends.
 \item For O\,\textsc{vi}, N\,\textsc{v}, and Ne\,\textsc{viii} most of the mass budget is in the WHIM phase in filaments. The mass fractions in these regions increase as redshift decrease. In particular, for Ne\,\textsc{viii}, we find a mass fraction of $\sim 0.91$ in the WHIM at $z=0$. When analysing different cosmic web environments separated, the mass fraction measured in filaments is $\sim0.66$, while values of $\sim0.12$ and
$\sim 0.13$ are obtained in haloes and voids, respectively.
Similar results are found for N\,\textsc{v} and O\,\textsc{vi} (Figure~\ref{fig:gasPhase_evol_ions}). These findings suggest that Ne\,\textsc{viii}, N\,\textsc{v}, and O\,\textsc{vi} are the best tracers of the low-density and warm/hot gas.
\end{itemize}

Our results confirm that most baryons at low redshift are in low-density regions and in the form of warm/hot gas. Among the different ionized metals considered, Ne\,\textsc{viii},  N\,\textsc{v}, and O\,\textsc{vi} in filamentary structure emerge as the best tracers of this baryonic component. We expect that the predictions reported in this work can contribute to the quest of unveiling the long-standing mystery of the missing baryons in the local Universe. In this context, our results will hopefully serve as an additional guide for upcoming surveys aimed at scanning the cosmic web through X-ray absorption spectroscopy with instruments such as the Athena Observatory.

\section*{Acknowledgements}
We thank the anonymous referee for her/his careful reading and constructive comments which helped improve the paper. MCA acknowledges Dylan Nelson, and Annalisa Pillepich for useful comments. MCA acknowledges financial support from the Austrian National Science Foundation through FWF stand-alone grant P31154-N27. ADMD thanks FAPESP for financial support. AMD also thanks Fondecyt for financial support through the Fondecyt Regular 2021 grant 1210612.
SB was supported by NSF grant AST-1817256. FM acknowledges support through the Program "Rita Levi Montalcini" of the Italian MUR. The computations in this paper were run on the FASRC Odyssey cluster supported by the FAS Division of Science Research Computing Group at Harvard University.

\section*{Data availability}
The data underlying this article will be shared on reasonable request to the corresponding authors.

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


Daytona Beach, FL (October 15, 2013) – Hyatt Hotels Corporation (NYSE: H) and Avista Hotels and Resorts today announce the opening of Hyatt Place Daytona Beach-Oceanfront, the world's first oceanfront Hyatt Place.
The Hyatt Place Daytona Beach-Oceanfront is directly on the beach in beautiful Daytona Beach Shores. The hotel is conveniently located only 10 minutes from Interstate-95. It also features easy access to the Daytona International Speedway, Daytona Beach Pier and Boardwalk, Daytona Lagoon Waterpark, Jackie Robinson Ballpark, The Halifax Historical Museum and the Ocean Walk Shoppes and Movies.
Hyatt Place Daytona Beach-Oceanfront is under the leadership of General Manager Don Terzieff and Director of Sales Andrew Wright. In his role, Terzieff is directly responsible for managing the day-to-day operations of the hotel, including overseeing the hotel's associates and ensuring guests encounter the purposeful service for which Hyatt Place is known. Wright is responsible for providing sales service and support to travelers and meeting planners frequenting the Daytona Beach area.
Launched in 2006, Hyatt Place brings to the upscale select service hotel category the authentic hospitality for which Hyatt is known. Inspired by multitasking travelers' 24/7 lifestyle, Hyatt Place combines stylish design and practical amenities with forward-thinking technology and purposeful service. Spacious guestrooms feature multiple areas to work and relax, and include the Cozy Corner; plush Hyatt Grand Bed; and ergonomic work center. Every guestroom is also equipped with a state-of-the-art media center that allows electronic devices to plug directly into the 42-inch, high-definition television, giving guests instant access to the technological amenities they're accustomed to accessing at home or in the office. Hyatt Place hotels also feature complimentary Wi-Fi access, a [email protected] fitness center, a coffee and wine bar serving specialty coffees and premium wine and beer, and a Grab 'n Go case stocked with freshly made sandwiches and salads. The 24/7 Gallery Menu offers made-to-order breakfast, lunch and dinner entrées around the clock, in addition to the a.m. Kitchen SkilletTM, a complimentary hot breakfast served daily. Specially trained Hosts are on hand to offer assistance with everything from directions to check-in to a freshly made meal.
Hyatt Place, a brand of Hyatt Hotels Corporation, offers more than 170 locations in the United States, Costa Rica and India. For Hyatt Place information or to make a reservation, call 1-888-HYATT-HP (888-492-8847) or visit www.HyattPlace.com.
Launched in 1983, Avista Hotels and Resorts is based in Orlando, Florida and has developed over 65 hotels. Avista Hotels & Resorts is proud to add the Hyatt Place Daytona Beach-Oceanfront hotel to its collection.
Orlando, Florida March 15, 2013 – The 160-room Fairfield Inn & Suites by Marriott in Orlando, Florida is scheduled to open this March with its smart, inventive public space and guest room design, and its bright and inviting décor. Located at 8214 Universal Boulevard, the Fairfield Inn & Suites Orlando International Drive/Convention Center will operate as a Marriott franchise, owned and managed by Avista Hotels XI, LLC. This is the first Fairfield Inn & Suites in Orlando to feature the brand's new design and décor, which enhance the guest experience through flexible features, and a warm and welcoming environment.
Located a mile from Universal Orlando and 12 miles from Orlando International Airport, the hotel offers guests convenient access to the Orlando Convention Center, SeaWorld Orlando, Discovery Cove, Aquatic and the Disney Theme Parks. Rates begin at $99 per night.
From the moment they arrive, Fairfield Inn & Suites Orlando International Drive/Convention Center's modern, bright new design features welcome guests, including an updated exterior with a signature tower, a curved porte-cochere and an inviting glass entrance that ushers them into the hotel. Once inside, guests experience the hotel's open public space featuring natural light and views throughout the lobby to connect the indoors with the outdoors. Consistent with the Fairfield brand's heritage of great service and a warm welcome, guests are greeted by associates who can easily move from behind the angled front desk to interact and answer questions.
In the hotel lobby area, guests can choose to be productive, relax or enjoy breakfast or a snack in a modern and flexible environment featuring a vibrant, natural color palette of greens, blues and oranges. The spacious lobby gives guests ample connectivity options, as well as a "connect and print" area that offers both standing and seated Internet stations. Guests can also unwind in the lobby's inviting living area ― whose focal points include a natural stone hearth, organic-shaped sofa and lounge chair, and unique local features — or they can grab a drink or snack item from the 24/7 Corner Market.
The breakfast area's signature farm table provides a central gathering place where guests can watch television, meet up with colleagues or get work done. In the morning, guests can enjoy a complimentary breakfast, choosing from delicious breakfast sandwiches, make-your-own waffles and other healthy items, such as fruit, yogurt, and whole grain cereals and breads.
The Fairfield Inn & Suites Orlando International Drive/Convention Center's signature "smart" room décor warmly welcomes guests into a comfortable, productive and restful environment. Flexible and functional, the guest room includes a well-designed work area, an ergonomic chair, task lighting and electrical outlets where guests need them. A curved, mobile desk enables guests to create their own work space, while also optimizing their television viewing.
Inspired by nature, the hotel's thoughtfully designed rooms and suites place the living and working area near the window to allow for more natural light and views. Building on this natural design, the room décor features organic patterns and fresh colors, blending wood tones with bright pops of color. The new design also places the sleeping area toward the middle of the room, helping to give guests a better night's sleep on plush mattresses, as well as easier access to the bathroom and wardrobe. The bright, spacious living area also offers a comfortable couch, refrigerator, coffeemaker and microwave, and the bath area continues the room's bright, spacious, contemporary feel with showers available in all standard king rooms and suites.
The six-story hotel features three types of one-bedroom suites. The Executive King Suite with kitchenettes and separate bedroom, the Executive Kitchen Suite with full kitchen and the Family Fun Suite with king-size bed, bunk beds and kitchenette.
Additional hotel amenities include an outdoor swimming pool with a whirlpool spa, an exercise room, valet laundry service, complimentary Wi-Fi, as well as fax and copy services. The hotel also offers 3,000 square feet of space to accommodate functions of up to 150 people.
Fairfield Inn & Suites by Marriott is designed for today's traveler who is looking to be productive on the road, whether for business or leisure. In addition to complimentary Wi-Fi and breakfast, Fairfield Inn & Suites offers thoughtfully designed rooms and suites that provide separate living, working and sleeping areas. With more than 675 properties throughout the United States, Canada and Mexico, Fairfield Inn & Suites hotels participate in the award-winning Marriott Rewards® frequent travel program that allows members to earn hotel points or airline miles for every dollar spent during each stay. For more information or reservations, contact the Fairfield Inn & Suites Orlando International Drive/Convention Center hotel directly at 407-581-9001, call the Fairfield Inn & Suites toll-free number at 800-228-2800, visit www.fairfieldinn.com or become a fan at www.facebook.com/fairfieldinnandsuites.
Orlando, FL -- (February 15, 2008) --- Avista Hotels& Resorts announces the opening of its new 196-room Radisson, Lake Buena Vista Orlando Hotel on Valentine's Day, February 14th, 2008 at 12799 Apopka Vineland Road in Orlando, Florida. This Radisson property is located 1/4 mile from the entrance to Walt Disney World. Resort and minutes from Universal Studios, Sea World, Wet n Wild and the Orange County Convention Center.
This new Radisson is a great example of our commitment to deliver the highest quality product and service for today's travelers. Said Nancy Johnson. Executive Vice President and brand leader of Radisson hotels & Resorts. "With innovative offerings like Radisson's express yourself online check-in and the custom Sleep Number. Bed by Select Comfort, guests can stay their own way."
"This new Radisson is a wonderful opportunity for us at Avista Hotels and Resorts, Not only to expand the Avista portfolio and the Radisson brand but also to provide an innovative, full service hotel that will secure a successful place in this ever competitive niche market" said Atif Nabi General Manager of the Radisson Lake Buena Vista Hotel.


6 Bedroom Detached House For Sale in Chorley for Asking Price £350,000.
Six bedroom extended family home is well worth taking time out to view, situated in a quiet Cul-de-Sac in the ever popular Pear Tree Avenue area within a short distance of the local Yarrow Valley Park, starting with the ground floor accommodation this fantastic home has a welcoming hallway with Wc/Cloaks fitted with a modern two piece suite, superb size open lounge dining room with French doors leading onto the rear garden, kitchen dining room with separate utility room and from this room access to the double integral garage, first floor there are five double bedrooms with ensuite and walk in wardrobe to the master, great size study and separate family bathroom. Externally there are well maintained gardens to the front and the rear with driveway for ample off road parking and direct access to the double garage. Early viewing is strongly advised on this highly desirable, well maintained spacious family home.
welcoming entrance hall with cosy seating and stairs leading to the first floor.
Fitted with a modern two piece suite with low level Wc, wash basin, tiled flooring and Upvc double glazed window.
Fantastic size room with Upvc double glazed bay fronted window, living flame gas fire and Upvc French doors opening onto the rear garden.
Fitted with a range of wall and base units with integrated double oven and hob, one and a quarter bowl sink and drainer with mixer tap, tiled flooring and to compliment, built in pantry cupboard and two Upvc double glazed windows over looking the rear garden.
Sink and drainer, plumbing for appliances, Upvc double glazed door and window to the rear garden and access to the double garage.
Loft access with pull down ladder.
Master bedroom with fitted wardrobes, Upvc double glazed window, access to ensuite and walk in wardrobe ( which has loft access).
Large ensuite bathroom fitted with a three piece suite with panel bath, low level Wc, pedestal wash hand basin and Upvc double glazed window.
Double bedroom with Upvc double glazed window.
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Fitted wardrobe and over head storage and Upvc double glazed window.
Great size room which could be used as a sixth bedroom with Upvc double glazed window.
Fitted with a three piece suite with panel bath with over head shower, low level Wc, wash basin, Upvc double glazed window and built in storage.
Driveway to the front with access to the double garage, well maintained front and rear gardens with paved patio to the rear and gate access to both sides.


text:
By Jay Davis | on December 30, 2021
Funeral services for William "Willie" Hepper, 89, of Mobridge, were held on Wednesday, Dec. 22, 2021, at Kesling Funeral Home Chapel in Mobridge.
Burial was in Greenwood Cemetery under the direction of Kesling Funeral Home of Mobridge.
William Raymond "Willie" Hepper was born on Nov. 28, 1932, in Sioux County, North Dakota, to Rose (Mattis) and Rudolph Hepper. He joined his brothers Calvin, Edward, and Adolph, and his sister, Emma. They were later joined by Rudy, Norman, Stanley, Alvin, Harold and Ronnie.
Willie graduated from McLaughlin High School in 1950 and worked on the family farm until volunteering for Army service in 1954, where he served in Japan. After his discharge in 1956, he worked in Kalispell, Montana, as a lineman before moving back to Selfridge, North Dakota.
Willie married Cecilia "Sis" Imberi on Sept. 29, 1956, and they settled in McLaughlin where they co-owned the Corner Bar with his brother-in-law, Tony Schneider, and sister, Norma.
In 1963, Willie and family moved to Mobridge where they ran the Gay Time Bar on South Main Street.
In 1972, Willie sold the Gay Time and was able to follow his life's passion of farming and ranching full time. For the next 36 years, he and Sis ran their operation from a place on the southeast side of Mobridge, operating from land on the east and west side of the river.
In 2008, they moved to town and Willie began the slow process of retirement.
Willie's civic activities included work on the Mobridge Rodeo board and being a hard-working member of the Moose Club.
Willie is survived by his wife, Cecilia; children, Kenny, Kelly, Larry (Kendra), Kim (Leonard) Linde, and Jim; grandchildren, Karolina, Alexandra (Justin) Rapetti, Travis, Laurel Linde, Clayton, Jacob, Hudson, Sabrina (Daniel) Dehart, and Troy; and great-grandchildren, Calvin and Julia.
He was preceded in death by his parents; daughter, Lauri; and brothers, Eddie, Ronnie, Calvin, Adolph and Alvin.
More From Obituaries Go To The Obituaries Section
Cheryl Ahl passes Jan. 11 in Huron
Donald Pfaff passes in Washington
'Doc' Salem was Mobridge veterinarian

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There are three species of bluebirds in the US, Western, Eastern and Mountain bluebirds. Mountain bluebirds are found at higher elevations in the West, Western Bluebirds are found to the west of the Great Plains and Eastern Bluebirds on the Great Plains. Bluebirds have bright colours and a cheerful song and are great favorites with lovers of wild birds. Populations of bluebirds drastically decreased all through the last century, being ejected from their favorite nesting sites by predatory birds.
Several organisations of bird watchers have instituted different means to promote the nesting and breeding of bluebirds. In Missouri in the 1950's the inhabitants made a National Bluebird Trail with more than 6000 bluebird boxes. Formed in 1978 The North American Bluebird Society furthers the revival of bluebirds. To help bluebirds you can establish up a Bluebird Trail by erecting a succession of bluebird houses The perfect bluebird house has been specified by the Bluebird Society and you could make your own or purchase a ready made bluebird house.
The best place for a Bluebird Trail is a country area with thin ground cover and dotted trees or bushes. There ought to be perch sites such as fences, wires and trees to allow the bluebirds to perch while hunting for food. By 2005 sightings of bluebirds in southern states have shown that they have come back to to this area. This has shown that bluebirds have benefited from the establishment of Bluebird Trails. Locations suitable for a Bluebird Trail are out-of-the-way locations of parks and golf courses or cemeteries as long as pesticides have not been applied. You should keep away from thickly forested areas with lots of of undergrowth. Bluebird houses ought to be located 150 yards away from each other and be between four and six feet high.
You can invite bluebirds to your backyard by placing mealworms (available to buy online) or water soaked raisins on platform garden bird feeders. Heated birdbaths will be a big attraction for them during the winter months.


Such the spirits co-exist with us whether in heaven, in hell or in earth.Anywhere, it is for sure that our loved ones will not harm us as we love each other.That will help ensure that the game you intend to purchase will run correctly without any problems.
In general, if you have a little scare of the séance ceremony, why don't you try Psychic Medium Chat?
That can be attributed to its exceptional features which draw more and more new players each day.
These include the Big Picture Mode and In-Home Streaming.
Below, we discuss some of the key features of Steam: Aside from games which run across nearly all genres out there, Steam is filled with titles which you can run from your device without any problem.


Moscow, October 13, Interfax - The Synod of the Constantinople Patriarchate has reinstated the primate of the Kiev Patriarchate, Filaret Denisenko, as an hierarch but does not see him as the patriarch, according to a Phanar hierarch.
Archbishop Job (Getcha), who represents the Ecumenical Patriarchate in the World Council of Churches, said in his correspondence with Russian Orthodox Church protodeacon Andrey Kurayev that Phanar deemed Filaret to be "the former Metropolitan of Kiev."
Archbishop Job said in response to the protodeacon's question about the Church rank of Denisenko in the eyes of the Ecumenical Patriarchate, "To my knowledge, he is the former Metropolitan of Kiev."
This means that the Ecumenical Patriarchate has acknowledged the legitimately of Filaret but views him as a former Metropolitan of Kiev.
"Filaret said yesterday that he 'was, is, and will be patriarch', but this is just a self-presentation. His conduct already buried Phanar's autocephaly project in 2008. The old man is walking down the same road," Kurayev said in his blog.


text:
Stocks making the biggest moves midday: Twitter, Tilray, Penn National and more
Published Thu, Oct 7 202112:31 PM EDT Updated Thu, Oct 7 20214:10 PM EDT
FCX
Twitter CEO and Co Founder, Jack Dorsey addresses students at the Indian Institute of Technology (IIT), on November 12, 2018 in New Delhi, India.
Amal KS | Hindustan Times | Getty Images
Check out the companies making headlines in midday trading.
Freeport-McMoRan — The mining company's shares were more than 8% higher and were the biggest gainers in the S&P 500. The stock's jump comes amid a broad market rally Thursday and a pop in copper prices.
Penn National Gaming — Shares of the casino and sports betting company jumped almost 5% after Canadian regulators approved its acquisition of sports media company TheScore. The deal is expected to close on Oct. 19, the companies said.
Levi Strauss & Co — Shares of the denim maker jumped 8.4% after the company's blowout earnings report. Levi's posted earnings of 48 cents per share during its fiscal third quarter, compared to 37 cents expected by Refinitiv. Revenue also topped analysts' expectations as consumer demand picked up during the back-to-school season and shoppers looked to stock up on the latest denim trends.
Lamb Weston — The frozen potato company saw shares sink more than 6% after it reported its quarterly results. Lamb Weston recorded a loss of 20 cents per share, which is greater than the 38 cents per share loss estimated by analysts, according to Refinitiv. The company also missed on revenue estimates.
Tilray — Tilray shares jumped over 1% after the Canadian cannabis producer's quarterly earnings of 8 cents per share matched Wall Street expectations, according to Refinitiv. Revenue gained 43% from a year prior.
Helen of Troy — The maker of houseware and health care products added nearly 6% after reporting quarterly adjusted earnings of $2.65 per share, beating estimates. Revenue also came in above analysts' forecasts.
Twitter — The social media company's shares added 4.3% after it announced plans late Wednesday to sell its MoPub mobile advertising network to mobile game developer AppLovin for $1.05 billion in cash. Twitter bought MoPub for a reported $350 million in September 2013.
Meredith Corp., IAC/InterActiveCorp — Meredith gained more than 6% following news that IAC's Dotdash will acquire the company's digital and magazine businesses for $42.18 per share in an all-cash transaction. The combined company will be called Dotdash Meredith and include popular brands like People and Better Homes & Gardens. Shares of IAC added 7%.
Healthcare Trust of America — Shares of Healthcare Trust jumped 2.9% after Bloomberg reported that activist investor Elliott Management is pushing for a strategic review that could result in a sale of the real estate investment trust.
Rocket Lab USA — Shares of the space company gained 10% after announcing on Wednesday it won a NASA contract to launch an Advanced Composite Solar Sail System, which will launch as part of a rideshare mission scheduled for lift-off in mid-2022.
Pinduoduo, Baidu, JD.com — U.S.-listed Chinese stocks moved higher after President Joe Biden and President Xi Jinping announced they would hold their first summit, virtually, before the end of 2021. Pinduoduo and JD.com rose more than 6% while Baidu added roughly 4%.
— CNBC's Hannah Miao, Jesse Pound and Yun Li contributed reporting
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text:
Q: Is there a method like onrotate() or something with a similar functionality in Android? I call a method based on a boolean value. I try setting that value in onRetainNonConfigurationInstance() to handle screen rotation but somehow it does not call the function correctly. What is the best method to call that will allow me to this:
public void methodName() //ideally something like onRotate()
{
  if (booleanValue == true)
  {
    booleanValue2 = false;
    method1();
   }
   else
  {
    booleanValue2 = true;
    method2();
   }
}

here

A: Maybe you're looking for this: http://developer.android.com/reference/android/view/OrientationListener.html
onOrientationChanged(int)

Called when the orientation of the device has changed. orientation
  parameter is in degrees, ranging from 0 to 359. orientation is 0
  degrees when the device is oriented in its natural position, 90
  degrees when its left side is at the top, 180 degrees when it is
  upside down, and 270 degrees when its right side is to the top.
  ORIENTATION_UNKNOWN is returned when the device is close to flat and
  the orientation cannot be determined.

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Nexcopy SD Duplicator solutions are manufactured to be feature rich and durable for industrial and heavy use applications. Our extensive line of SD Duplicators include models for any type of application. Nexcopy manufactures models ranging from 16 target to 60 target systems and support SD, SDHC, SDXC and UHS.
The Nexcopy systems are ultra-fast SD copiers designed for one thing – copy fast! The standalone systems copy from a physical master to all connected cards. The system can be set for synchronous or asynchronous duplication modes. With 32CRC verification we insure every copy is the same as the master, therefore you will get the most accurate copies available.
The standalone SD duplicators are binary copiers. They copy the boot code, all partition tables, file system, folders and files.
Nexcopy offers the standalone systems in 16 socket and 32 socket configurations.


text:
Le Mausolée d'Ali ebn-e Sahl est un mausolée historique à Ispahan, en Iran. Le mystique Abolhassan Ali ebn-e Sahl Azhar Esfahani vécut dans l'ère de Al-Mutadid, le calife abbasside. Il eut un Khanqah et une école à nord de le cimetière Toghtchi. Il mourut en 894 à Ispahan et fut inhumé dans son Khanghah. Le mausolée d'Ali ebn-e Sahl devint un lieu de réunion des mystiques et derviches. Actuellement, le mausolée appartient aux derviches Khaksaries. Le mausolée possède un grand jardin. La plus grosse partie du jardin est en la possession de l'Organisation des Aides Sociales.

Description
Au milieu de la construction cruciforme se trouve la tombe d'Ali ebn-e Sahl. La pierre tombale est carrée, elle a une longueur de 2 mètres et une hauteur de 120 centimètres. Elle fut décorée avec des carreaux jaunes, blancs, bleus et noirs.

Articles connexes
 Liste des constructions historiques de la province d'Ispahan

Notes et références

Ali ebn-e Sahl
Ispahan
Monument en Iran
Architecture au IXe siècle

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text:
Schumer requests Mulvaney, Bolton to testify in Senate's impeachment trial
Democrats have requested for present and former Trump administration officials including John Bolton, former National Security advisor, to testify in the Senate's forthcoming impeachment trial. Photo by Kevin Dietsch/UPI | License Photo
Dec. 16 (UPI) -- Senate minority leader Chuck Schumer said Democrats want to hear from four administration officials during the Senate's forthcoming impeachment trial of President Donald Trump.
In a letter to Senate majority leader Mitch McConnell, R-Ky., Schumer said the Democrats want White House Chief of Staff Mick Mulvaney, former Nation Security adviser John Bolton, Senior White House Chief of Staff Advisor Robert Blair and National Security Associate Director Michael Duffy to be subpoenaed to testify before the Senate.
He said the Democrats would be open to hearing from additional witnesses with knowledge concerning the delay of security funds to Ukraine in exchange for the country investigating Trump's political rival former Vice President Joe Biden and his son Hunter Biden.
"Senate Democrats believe strongly, and I trust Senate Republicans agree, that this trial must be one that is fair, that considers all of the relevant facts and that exercises the Senate's 'sole Power of Impeachment' under the Constitution with integrity and dignity," said Schumer, D-N.Y. "This trial must be one that not only hears all of the evidence and adjudicates the case fairly; it must also pass the fairness test with the American people."
RELATED 5 staffers to Democrat lawmaker Jeff Van Drew resign
He also proposed for pre-trial housekeeping to begin Jan. 6, for chief justice and senators to be sworn-in Jan. 7 and for House mangers to make their presentations Jan. 9, which would be followed by the presentation by the president's counsel.
Senators would have eight hours to question each side followed by a period of six hours equally divided between the House managers and the president's lawyers for final arguments that would be followed by a 24-hour period for senators to deliberate before voting on the articles of impeachment, Schumer proposed.
Democrats also proposed for the Senate to subpoena documents regarding the delay in the dispersal of funds to Ukraine. He said the electronic communications, memoranda and records have already been collected by the White House counsel "so production in response to the Senate subpoenas should be neither burdensome nor time-consuming."
RELATED House Democrats rebuke Senate GOPs for quick impeachment trial goal
"We believe this proposal ... will allow for a trial in which all of the facts can be considered fully and fairly, and in which final votes can be taken within a reasonable period of time, without any unnecessary delay," Schumer said. "Conducting the trial according to this plan will also allow the public to have confidence in the process and will demonstrate that the Senate can put aside partisan concerns and fulfill its constitutional duty."
The letter comes as the Democrat-controlled House is expected to vote later this week on two articles of impeachment charging Trump with abuse of power and obstruction of Congress.
McConnell has said that he will take his "cues" concerning the trial from the president's lawyers and hopes the trial will be short.
RELATED Trump, Democrats agree to U.S.-Mexico-Canada trade deal
Mick Mulvaney


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Cooperation with Indian pharmaceutical company Cipla Limited was discussed at National Academy of Sciences of Belarus
Vladimir Gusakov, Chairman of the Presidium of the National Academy of Sciences of Belarus, and Dr. Lalit Chokani, Honorary Consul of the Republic of Belarus in India, held talks at the National Academy of Sciences of Belarus. They discussed issues of expanding cooperation and promising mechanisms for interaction between the NAS of Belarus and the Indian pharmaceutical company Cipla Limited, arranging a scientific and technological center for the production of solid dosage forms using innovative technologies at the state enterprise Academpharm of the NAS of Belarus.
The Indian side has already invested $ 1 million in this project. Arranging such a medication production involves the development of new technological methods: micronizing, dry granulation, production of multilayer tablets, etc. It is planned to produce new medicines on a full cycle: from a scientific concept to manufacturing.
Currently, the sides agreed to localize in the Republic of Belarus the production of effective and safe medicines for the treatment of socially significant diseases: HIV infection, hepatitis B and hepatitis C, as well as Alzheimer's disease and arterial pulmonary hypertension. The General Designer of the center actively works on an architectural project. Work is underway to obtain the entire list of technical conditions for the project. The Protocol of instructions of the President of the Republic of Belarus Alexander Lukashenko, given on 11 – 13 September 2017 following the visit of the state delegation of the Republic of Belarus to the Republic of India, provides for transferring technology of medication production with the participation of Cipla Limited experts and setting up the production of medicines on the full technological cycle at the Academpharm by 31 December 2020. It is planned that a delegation of the Indian pharmaceutical company Cipla Limited headed by the Chairman of the Board Dr. Yusuf Khwaja Hamid, an honorary member of the National Academy of Sciences of Belarus, will visit Minsk in July 2019 to discuss the further progress of this project.
Cooperation between Cipla Limited and Academpharm on arranging contract manufacturing of socially important medicines started in 2016. In August 2018, a ceremonial opening of a landscape complex for a scientific and technological center at the Republican Manufacturing Unitary Enterprise "Academpharm" of the NAS of Belarus took place.
#international cooperation
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