text:
\section{Introduction}
Galaxy properties such as morphology, color, star--formation rate do vary with redshift, stellar mass and environment  (Kauffmann et al. 2004, Postman et al. 2005, Cucciati et al. 2006, Cooper et al. 2008).
In the local Universe,  large redshift surveys (SDSS) have shown that  the star--formation properties of galaxies are dependent on the local environment both in clusters and in low density environments, such as cluster outskirts and the field.
Red passive early--type galaxies (E+S0) are more frequently found in high density environments, while blue late--type, star--forming  galaxies tend to dominate in low density regions (Dressler 1980). The average star--formation rate (SFR) decreases with increasing density (SFR--density relation), suggesting a scenario where  galaxy interactions, and in general galaxy environment, play a major role in regulating star--formation.
AGN activity is also linked to the environment. In the local Universe luminous AGN are found preferentially in the field and  in underdense regions, where their hosts can preserve large amounts of gas to feed the black--hole (Kauffmann et al. 2004).
Using the SDSS data, Hwang et al. (2010) found no dependence of the fraction of LIRGs plus ULIRGs among infrared galaxies versus galaxy density at fixed stellar mass. Conversely, the star formation activity of LIRGs and ULIRGs are found to strongly depend on the morphology and the distance to the nearest neighbor galaxy, indicating that galaxy-galaxy interactions/merging play a critical role in triggering the star formation activity of local LIRGs and ULIRGs.
The morphology--density and color--density relations are observed at intermediate redshift and apparently are in place by $z\sim 1$ (Cassata et al. 2007, Capak et al. 2007, Tasca et al. 2009, Postman et al. 2005, Cucciati et al. 2006).
Recently,  Scoville et al. (2007b) found correlations between environment and stellar mass, SFR, SED type and morphology  for a large mass--selected sample over the redshift range $z=0.1\div1$ in the COSMOS survey (Scoville et al. 2007a).
Kovac et al. (2009) showed that  star--formation and color transformation rates of galaxies  are higher  in the group environment than outside groups by a factor of 2 to 4 since $z\sim 1$.
Elbaz et al. (2007) and Cooper et al. (2008) observed the reversal of the SFR--density relation at $z\sim 1$: the average SFR increases with increasing density.
An enhancement of the star--forming fraction at intermediate densities has also been reported for a $z\sim 0.8$ cluster  by Koyama et al. (2008). Tran et al. (2010) found an increasing fraction of IR luminous galaxies with increasing galaxy density in cluster at redshift $\sim$1.6.
Caputi et al. (2009) analyzed the close environment, on 1 Mpc scales, of luminous infrared galaxies (LIRGs, \LIR$=10^{11}\div 10^{12} $L$_{\odot}$) and ultra--luminous infrared galaxies (ULIRGs, \LIR$>10^{12} $L$_{\odot}$)  in zCOSMOS (Lilly et al. 2007),
finding that luminous infrared galaxies  between $z=0.6\div 1$ are more often found in overdense environments, while  ULIRGs prefer underdense environments.
Ideue et al. (2009) found an increasing fraction of [OII] emitters in the high density environments at $z\sim 1.2$ in the COSMOS field, based on narrow band imaging.

All these results suggest that  galaxy evolution and star--formation activity are dependent on the environment, and at z$\gtrsim1$ galaxies are caught in their active star--forming evolutionary phase in high density regions such as the center of groups.
This phase might precede the formation of red ellipticals observed in the cluster centers in the local Universe.
Both the SFR and the color--density relations exhibit strong stellar mass trends  (Kauffmann et al. 2004,  Balogh et al. 2004, Haines et al. 2007). Therefore, in order to isolate environment from mass--driven evolution (downsizing), it is crucial to study galaxy properties in bins of mass.

Galaxy interactions, fly--bys and minor mergers are among the mechanisms  expected to have an impact on evolution and star--formation activity of galaxies.
Ram pressure stripping by the intra--cluster medium (ICM) might also contribute to regulate star--formation processes in clusters (Kapferer et al. 2008a,b). However observations of intermediate redshift clusters tend to exclude ram pression stripping as a mechanism of star--formation quenching (Demarco et al.).
Disentangling the effect of the cosmological decline of the SFR from environmental effects is not straightforward   (Lilly et al. 1996, Madau et al. 1996, Le Floc'h et al. 2005, Hopkins et al. 2006, Caputi et al. 2007).
Large unbiased samples are needed to isolate the global evolution of the SFR and mass--driven effect (Bell et al. 2004) from environment--driven effects. Deep, large--area surveys, such as COSMOS (Scoville et al. 2007a), are useful to address this topic, as they can sample large volumes of Universe from moderate to high redshifts.
In particular, the COSMOS large area (2 square degrees in the sky, corresponding to physical scales of  $\sim 40$ Mpc at  $z=1$) allows probing,  from intermediate to high redshift, a wide range of stellar masses and galaxy densities, from the dense clusters and groups to the field.
This is usually not achieved with deep pencil beam surveys. However, for such large area a complete deep spectroscopic surey cannot be easily achieved.
For this reason the COSMOS collaboration acquired deep and accurate photometry in (so far) 34 bands from far--UV to mid--infrared, including imaging in 16 intermediate and narrow band filters from the Subaru Telescope (COSMOS--21, Taniguchi et al. 2007, Capak et al. 2009).
The survey has, on average, a photometric point every 200 \AA~  between the U and z bands (29 photometric bands in this wavelength range), simulating low resolution spectroscopy. Thus, highly reliable photometric redshifts are easily computed (Ilbert et al. 2009a, Salvato et al. 2009).  As demonstrated by Scoville et al. (2007b), at redshift below 1.2 the quality of the photometric redshifts is sufficient to achieve the accuracy needed for this work, i.e. tracing the evolution of galaxies, AGN and star--formation processes in the large scale structure.

In this paper we use the COSMOS dataset to characterizing the environment of bright star--forming galaxies , and studying their properties as a function of the environment.
The plan of the paper is as follows:  Sect. 2 presents the multiwavelength dataset. Sect. 3 presents the sample selection, while Sect. 4 presents the method for density computation. Sect. 5 presents the galaxy properties as a function of the environment, and Sect. 6 presents a summary of the results.
A standard cosmology ($\Omega_m = 0.3$ and $\Omega _{\lambda}=0.7$) with $H_0 = 70$ km s$^{-1}$ Mpc$^{-1}$ is used throughout. Magnitudes are given in the AB system.

\begin{figure}
\includegraphics[scale=.4]{zlir.eps}
\caption{$L_{IR}$ versus redshift  for the 24 \micron\ sample with S(24 \micron\  )$>80~\mu$Jy. Solid lines show the luminosity  and redshift selections.}\label{zlir}
\end{figure}

\section{Data}
The COSMOS field has deep multi--wavelength photometric coverage over an area of 2 square degrees from X--rays to the radio.
The photometric catalog includes data from 34 broad, intermediate and narrow bands from 1550 \AA\ to 8 \micron\ ,and it is complete down to $i^+ =26.2$ (5$\sigma$ for point a point source, Capak et al. 2009).
We use the  photometric redshifts drawn from the catalogs of  Ilbert et al. (2009a).
These have an accuracy as good as $\sigma_z/(1+z)=0.012$ up to $i^+=$24 and z$\leq 1.25$.  For fainter $i^+$ magnitudes the accuracy of photometric redshifts rapidly deteriorates  (Ilbert et al. 2009a).
This paper is limited to galaxies with $i^+<24$, i.e. the sample with the best photo--z accuracy available.
Ilbert et al. (2009a) photo--z were complemented by those computed by  Salvato et al. (2009) for the AGN detected in the XMM--Newton survey of COSMOS (Cappelluti et al. 2009, Brusa et al. 2007).
The latter account for AGN time--variability and use a library of composite template SEDs, including both AGN and galaxy contributions.
The precision of AGN photo--z is $\sigma_z/(1+z)=0.014$ for $i^+<24$ at any redshift.

The stellar masses were derived from K--band luminosity and mass--to--light ratio using the Arnouts et al. (2007) relation and Salpeter IMF  (Ilbert et al. 2009b). The measured mass--to--light ratios are consistent within 0.1 dex with the analytical relation of  Arnouts et al. (2007)  for stellar masses larger than $3\times 10^{10} $M$_{\odot}$ for both quiescent and star--forming galaxies (Ilbert et al. 2009b).

\subsection{MIPS 24 \micron\  data}
The full 2 deg$^2$ COSMOS field was observed by Spitzer/MIPS down to flux limits of 80 $\mu$Jy at 24 \micron\ (S--COSMOS,  Sanders et al. 2007).
The multiband catalog of the counterparts of the MIPS 24 \micron\ sources is described in Le Floc'h et al. (2009).
Here we briefly recall its main features.
The counterparts of the 24 \micron\  sources were first identified by cross--matching with the $K_s$--band COSMOS catalog (McCracken et al. 2010) using a matching radius of 2\arcsec.
The identification was based on the closest $K_s$--band source to the MIPS position, and using the IRAC 3.6 \micron\ as a prior in case of multiple possible  counterparts in the $K_s$--band.
About 90\% of the MIPS sources above 80 $\mu$Jy have been assigned a secure near--IR counterpart, and about 5.5$\%$ have less secure identifications. The final catalog consist of 39360 objects.
The $K_s$--band sources were merged with the photometric redshift catalog of Ilbert et al. (2009a) and Salvato et al. (2009) with a matching radius of 1\arcsec, in order to associate a photometric redshift to each 24 \micron\ source.
Here again the closest $i^+$--band source was chosen as the counterpart of the $K_s$--band source, yielding 90\% of optical identification for the full 24 \micron\ catalog down to $i^+ =26.5$ (see Le Floc'h et al. (2009) for a detailed discussion).
The MIPS 24 \micron\  sample used in this paper includes  AGN detected by XMM--Newton (about 1200 with \Lx$>10^{42} $ erg/s, Cappelluti et al. 2009, Brusa et al. 2007).

Overall, the photometric redshift accuracy for the 24 \micron\ sample is similar to that of the optical sample,  $\sigma_z/(1+z)=0.010$ for $i^+<24$ (Ilbert et al. 2009a). In particular the fraction of catastrophic outliers is $<1$\%  for sources with flux $S(24\micron)>80~\mu$Jy.

\subsection{Star-formation rates}
Chary \& Elbaz (2001) have shown that the mid--infrared flux is a good estimator for the total infrared luminosity (L$_{IR}$) emitted by a galaxy in the range $8 \div 1000$ \micron\ in the local universe.
Our sample is limited to $z < 1.2$, for which the mid--infrared and radio estimators provide consistent L$_{IR}$ values at least in the LIRG regime (Elbaz et al. 2002).
This assumption is based on infrared spectral energy distributions (SED) typical of luminous star--forming galaxies, whose bolometric output is dominated by star--formation. SFR of sources detected in X--rays may be overestimated due to the AGN contribution to their infrared SED.

Based on this assumption, we use the mid--infrared flux at 24 \micron\ and Chary \& Elbaz (2001) templates to compute the \LIR.
This method uses a library of 105 templates and the 24 \micron\  flux density to compute the mid--infrared rest--frame luminosity, and derive \LIR\ for each galaxy.
Figure \ref{zlir} shows the \LIR\ as a function of the redshift for the MIPS 24 \micron\ catalog down to 80 $\mu$Jy.
We convert $L_{IR}$ into the total star-formation rate ($SFR_{IR}$) by using the Kennicutt (1998) relation:
$SFR_{IR} = 1.72\times10^{-10} $L$_{IR}$[L$_{\odot}]$.
We neglect the UV contribution since this makes up a small fraction (about 10\%) of the bolometric luminosity for LIRGs at $z\sim 1$ (Burgarella et al. 2007). The SFR are derived assuming a Salpeter IMF, consistent with that used to derive stellar masses.

\begin{table*}
\begin{center}
\caption{Stellar mass completeness.\label{tbl-2}}
\begin{tabular}{crrrrrrrrrrr}
\tableline\tableline
Redshift &$0.3\div0.6$ & $0.6\div0.8$ & $0.8\div1$ &$ 1\div1.2$\\
\tableline
F$_{opt}(>10^{10}$M$_{\odot}$)      &      0.06 (94)                &       0.13  (87)                     &  0.34  (66)  &   0.57 (43)\\
F$_{opt}(>3\times10^{10} $M$_{\odot}$)     &    0.006  (99.4)           &     0.03  (97)                      & 0.22  (78)    &  0.41 (59)\\
F$_{IR}(>3\times10^{10} $M$_{\odot}$)    & 0.001 (99.9)&   0.01 (99)      &  0.06 (94)  &  0.25 (75)\\
\tableline
\end{tabular}
\tablecomments{Fraction of galaxies in the optical and 24 \micron\ samples with $i^+>24$ and stellar mass larger than $10^{10}$ and $3\times 10^{10} $M$_{\odot}$ from redshift $z=0.3$ to 1.2. The corresponding value of stellar mass completeness for $i^+<24$ is given in parenthesis for each bin.}
\end{center}
\end{table*}

\begin{figure}
\begin{center}
\includegraphics[scale=0.4]{frfaintgal_optmips.eps}
\caption{Upper panel: fraction of optically-selected galaxies with magnitude $i^+>24$ as a function of the stellar mass and redshift. Redshift is increasing from $z=0.4$ to 1.2, from left to right. Lower panel: fraction of 24 \micron selected galaxies with S(24\micron$)>80~\mu$Jy and  $i^+>24$ as a function of the stellar mass and redshift.}
\label{zlogm}
\end{center}
\end{figure}

\begin{figure}
\includegraphics[scale=.4]{istoz_wAGN.eps}
\caption{Open histogram: all sources with $i^+<$24, $M_{\ast}>10^{10.5} $M$_{\odot}$; filled histogram: LIRGs with the same selection; small panel: LIRGs detected in X--rays by XMM--Newton.  }\label{istoz}
\end{figure}

\section{Sample selection}
The following analysis is based on a mass--selected samples drawn from the MIPS 24 \micron\ and optical catalogues (Sanders et al. 2007, Le Floc'h et al. 2009, Ilbert et al. 2009a) in the $z=0.3\div 1.2$ redshift range.
In order to  assess the completeness of our samples in stellar mass, we compute the fraction of  optically and 24 \micron\ selected galaxies with apparent magnitude $i^+$ larger than a given value as a function of their stellar mass.
Figure \ref{zlogm}, upper panel, shows the fraction of optically selected galaxies with magnitude $i^+>24$ as a function of the stellar mass and redshift, in four redshift bins from $z=0.3$ to 1.2.
For M$^\ast>3\times 10^{10} $M$_{\odot}$ the fraction of  galaxies with  $i^+>24$ is $<0.01, 0.03, 0.22$ and 0.4 at  $z=0.3\div 0.6, 0.6\div 0.8$, $0.80\div 1$ and $1\div 1.2$, respectively (Table 1).
Therefore for  $i^+<24$ the stellar mass completeness at M$^\ast=3\times 10^{10} $M$_{\odot}$ is  99, 97, 78 and 60\%  in each of the previous redshift bins, respectively.
The 24 \micron\ detected galaxies are a subsample of the previous one, since they were selected to have an optical counterpart brighter than  $i^+=24$.
Figure \ref{zlogm}, lower panel, shows the same fraction as before for galaxies with S(24\micron\ )$>80~ \mu$Jy and magnitude $i^+>24$.
The fraction of such galaxies with M$^\ast>3\times 10^{10} $M$_{\odot}$ is $<0.001, <0.1, 0.06$ and 0.25 at $z=0.5, 0.7, 0.9$ and 1.1, respectively.
Thus, the completeness in stellar mass  is larger than $90\%$ up to $z=1$ and  75\% up to $z= 1.2$.

The cut in stellar mass adopted here implies that all star--forming galaxies in the sample are LIRGs or ULIRGs, given the relation between SFR and stellar mass at $z\sim 1$ (Elbaz et al. 2007).
We investigate the effects of environment on dusty, star--forming galaxies with $i^+\leq 24$, \LIR$> 10^{11} $L$_{\odot}$ and stellar mass M$^\ast>3\times 10^{10} $M$_{\odot}$ up to $z=1$.
In the redshift bin $z=1\div 1.2$ we will consider galaxies with \LIR$>2\times 10^{11} $L$_{\odot}$ (Figure \ref{zlir}).
This  selection implies  a SFR sensitivity SFR$>18 $M$_{\odot}$/yr and $35 $M$_{\odot}$/yr up to $z=1.2$.
The selected sources are LIRGs and ULIRGs. ULIRGs are a small fraction of the whole sample ($\sim 1.8\%$), therefore we will refer to the sample as LIRGs throughout the paper, keeping in mind that it includes also a small fraction of ULIRGs.
The properties of LIRGs will be compared to those of optically selected galaxies in the same range of stellar mass and magnitude (M$^\ast>3\times 10^{10} $M$_{\odot}$,  $i^+<24$).
By adopting this selection we focus on the high--mass end of the galaxy mass function (Ilbert et al. 2009b).
The final samples consist of  28455 optically selected galaxies  and 8234 LIRGs in the given redshift range.

The redshift distribution of the two samples is shown in Figure \ref{istoz}, where the X--ray detected AGN are also highlighted.
AGN  with L(2-10 keV)$>10^{42}$ erg/s among the 24 \micron\  detections down to 80 $\mu$Jy and $i^+<24$ represent a small fraction of the population: about 3\% in the redshift range  $z=0.3\div 1.2$  and 4\% at $z=0.8\div 1.2$.
For these the SFR might be overestimated due to the AGN contribution to the infrared SED.
We will show that the trends are not modified if they are excluded in the LIRG sample.
We do not attempt to account for the contamination by obscured, Compton--thick AGN at $z\sim 1$.
However, we notice that they can hardly outnumber X--ray detected AGN (Fiore et al. 2008, Martinez-Sansigre et al. 2007).  The fraction of highly obscured, not X--ray detected AGN at $z=0.7\div 1.2$ and with intrinsic luminosity $L(2-10 keV)=10^{43.5\div44}$ erg/s is $3.7\times 10^{5} $Mpc$^{-3}$, corresponding to ~67\% of that of X--ray selected AGN (Fiore et al. 2009).

\section{Projected densities}\label{dens}

We adopted the Nth nearest neighbor density estimate (Dressler 1980, Capak et al. 2007, Guzzo et al. 2007,  Postman et al. 2005, Smith et al. 2005).
Projected density measurements based on photometric redshifts are able to detect the structures and reconstruct the overdensities (Scoville et al. 2007b).
They have been successfully used to detect the large scale structure and nicely match the structures detected by X--ray and spectroscopic surveys.
Although limited by the photo--z precision (which implies a smoothing effect), the photometric redshifts trace the dependence of galaxy properties on environment in the LSS and can use large unbiased galaxy samples, a factor of $\sim 10$ larger samples than the largest spectroscopic surveys thus limiting the statistical scatter (Scoville et al. 2007b, Scoville et al. 2010).
In particular, Scoville et al. (2007b) showed that the correlations between galaxy properties, such as SFR, stellar mass, and environment are not smoothed out when using accurate photometric redshifts.
Conversely, spectroscopic surveys allow for precise distance measurements but are limited by the sampling rate which is usually low.

The projected density around each galaxy is derived from the distance to the Nth neighbor, {\emph r}, which defines a circular area whose surface density is  $\Sigma_N = \frac{N}{\pi r^2}$.
This density is then divided by the median of projected densities of each redshift slice across the whole COSMOS field, in order to obtain a relative density $\Sigma_N/\overline \Sigma$ in each redshift interval.
We compute projected densities for each galaxy with magnitude $i^+<24$ and stellar mass larger than 10$^{10} $M$_{\odot}$, outside masked areas contaminated by saturated stars (Ilbert et al. 2009a), using 50390 galaxies in total.
We use a cylinder with a depth of $\pm3\sigma_z$ centered on each galaxy.
The main difference with previous studies on the COSMOS field is that the accuracy of the photometric redshifts has now improved by roughly a factor of 3.
The density field of the COSMOS data is measured using the same selection described above.
At these stellar masses the completeness is 98, 88, 66 and 43\%  from $z=$0.3 to 1.2 (Figure \ref{zlogm}).
As discussed also in Scoville et al. (2007b), a higher stellar mass cut--off would be more conservative and yield larger completeness, but at the same time would limit the sample to only the most massive galaxies and under--represent lower mass galaxies, therefore limiting  the dynamic range. Therefore when computing densities we allow for a lower completeness. Conversely, when comparing LIRGs to optical galaxies we adopt a cut at $M^\ast>3\times 10^{10} $M$_{\odot}$ in order to have a higher completeness level (see Sect. 3).

We used the Millennium Simulation mock catalogs (Kitzbichler \& White 2007) to compare the derived surface densities with the three dimensional (3D) volume densities for galaxies selected in the same way as for the COSMOS data.
We run the simulation here described using the same selection used for the observed data.
First, we compute the 3D volume densities by using the positional information available from the Millennium Simulation, and measure the density field around each galaxy in a sphere of radius equal to the distance of the 10th nearest neighbor.
In the simplest assumption, i.e. spherical symmetry, the 3D densities are related to the projected densities by
 $\rho= 10 \times 3 / 4  \pi r^3_{10}$,
where $r_{10}$ is the distance to the 10th nearest neighbor.
No redshift errors were included in the 3D density computation at this stage.
This density is  related to the projected density by the following relation: $\Sigma_{10} = \alpha \rho^{2/3} $ where $\alpha = 1.76$.
Figure \ref{app}  shows the correlation between the input and recovered densities.
The horizontal axis shows the projected 3D volume density in the Millennium simulation computed as described above. The vertical axis shows the $\Sigma_{10}$ measured in the Millennium simulation in the same way as for the COSMOS data as described at the beginning of this section.
This test indicates that projected densities on average overestimate the real densities by a factor of 2.2 but there is proportionality between the 2D and the 3D density estimates for the simulated data (Figure 4, black contours).
In order to estimate how the photo-z errors affect the 2D density computation
we  associate to each redshift in the mock catalog a random error drawn from a gaussian distribution  with $\sigma_z/(1+z)=0.012 $, equal to the error in the measured photometric redshift of COSMOS, and we measure the projected densities.
A gaussian error distribution is an approximation of the real error distribution.
However, it is reasonable, considering that catastrophic errors in the photo--z are not an issue both for the optically selected and the 24 \micron\ selected samples down to $i^+=24$, since they are of the order 1\% and will therefore only affect densities by that amount (Ilbert et al. 2009a).
The effect of the photometric redshift error is shown in Figure \ref{app} with red contours.
The errors in the photo--z increase the scatter in the correlation between 3D and projected densities. However projected densities are still proportional to 3D densities and environment can be characterized at least in the high density regime.
The scatter of the correlation is large at small densities but it decreases with increasing density. This can affect and smooth out possible existing trends by scattering galaxies between contiguous density bins.
At $\Sigma_{10}\sim 10$ the scatter is about 100\% of the density value, meaning that a galaxy residing in a region of density 10$/$Mpc$^2$ will be assigned to a density range $0\div 20/$Mpc$^2$ with a probability of 68.3\%. At $\Sigma_{100}>$100 the scatter is about 25\% of the density value. Therefore, for example, a galaxy residing in a region of 200/Mpc$^2$, has 68.3\% probability of being assigned to a density in the range $150\div 250/$Mpc$^2$. Around 50/Mpc$^2$ the scatter is $\sim 50$\%. This must be taken into account  when studying trends as a function of the environment, and the density bins must be chosen accordingly.
In particular, for the four density bins used in this paper (see section 5), the 1$\sigma$ error on the density estimate is 150\%, 68\%, 42\% and 32\% of the projected density value,  for each bin from the low density to the high density one, respectively.

\begin{figure}
\includegraphics[scale=.4,angle=0]{tredp_0312.v4.eps}
\caption{Isodensity contours of measured $\Sigma_{10}$ versus projected 3D galaxy density, from the Millennium Simulation (black contours).  Red contours: same relation where the error on photo--z is taken into account.}\label{app}
\end{figure}

\begin{figure*}[t]
\begin{center}
\includegraphics[scale=.5,angle=-90]{newdsfr3.eps}
\caption{ Upper panels: SFR versus density for the LIRG sample (black symbols) and  AGN (magenta symbols) in redshift bins. Red symbols represent the median values and standard errors in density bins, omitting AGN. Lower panels: SSFR versus density.  }\label{figdens1}
\end{center}
\end{figure*}

\section{Results}

\subsection{SFR and SSFR versus environment and redshift}

Figure \ref{figdens1}, upper panels,  shows the SFR of the LIRGs versus the projected density in four redshift bins from $z=$0.3 to 1.2.
The increase in the median SFR at $z=1\div 1.2$ is due to the luminosity cut adopted here (\LIR $>3\times 10^{11} $L$_{\odot}$).
The increase of the specific star--formation rate (SSFR) with redshift is expected given the evolution of the stellar mass--SSFR relation with redshift (Elbaz et al. 2007).

The SFR--density relation shows a large scatter and the median SFR is constant at all densities.
The median SFR per LIRGs does not vary with the environment.
In our analysis we do not find any excess of LIRGs in the high density environments up to $z=$1.
We notice that possible existing trends are likely to be erased in the low density regime (first two bins in projected densities), but the flat trend observed here is significant in the two highest density bins.
This said, we do not observe the reversal of the SFR--density relation  (i.e. average SFR increasing with density, Elbaz et al. 2007, Cooper et al. 2008) up to $z=1$.
At $z>1$ the median SFR is compatible with a flat dependence on density.
This difference may be due to the highest accuracy in the density measurements achieved by using spectroscopic redshifts.
However, the samples of Elbaz et al. (2007) and Cooper et al. (2008) are not mass--limited and spanned a broader range both in stellar mass and SFR, probing down to significantly lower SFR compared to our LIRG sample.
Therefore, such reversal by might be due to the contribution of galaxies with lower stellar mass and SFR.
Indeed, in the local Universe, the dependence of SFR on environment is weaker for massive galaxies (Kauffmann et al. 2004).
For massive LIRGs such reversal, if any, might occur at $z>1$.
Figure \ref{figdens1}, lower panels,  shows the SSFR versus density for each of the previous redshift bins.
Here again the SSFR is consistent with a constant trend at all densities.

\begin{figure*}[t]
\begin{center}
\includegraphics[angle=0,scale=0.8]{frlirg_lowz_v6.eps}
\caption{ Fraction of LIRGs to the optically selected galaxy population with M$_\ast>3\times 10^{10}$M$_{\odot}$ as a function of  galaxy density and redshift in two stellar mass bins: M$_\ast=3\times 10^{10}\div  10^{11}$M$_{\odot}$ (left panel), M$_\ast> 10^{11}$M$_{\odot}$ (right panel). Filled circles: X--ray detected AGN included, open circles : X--ray detected AGN excluded.}
\label{frlirglowz}
\end{center}
\end{figure*}

\subsection{LIRG fraction versus environment and redshift}

Figure \ref{frlirglowz} shows the logarithmic fraction of LIRGs among the whole population of galaxies with M$^\ast>3\times 10^{10} $M$_{\odot}$, as a function of the projected density  from redshift $z=0.3$ up to $z=1.2$, and in two stellar mass bins (M$^\ast=3\times 10^{10}-10^{11} $M$_{\odot}$  and M$^\ast>10^{11} $M$_{\odot}$).
For galaxies at $z>1$ the density bins are larger than at lower redshift in order to contain a sample large enough.
Filled circles represent the LIRG fraction among the whole optically selected population with M$^\ast>3\times 10^{10} $M$_{\odot}$.
Open circles represent the same fraction but where the contribution of X--ray detected AGN has been subtracted from the LIRG sample.
The error--bars on the measurements were computed propagating the poisson errors on the galaxy counts and using upper limits in the bins where we have only a few counts (Gehrels 1986).
The error--bars are large in the highest density bins, since these are in general less populated (hosting a few tens optical galaxies, and a few LIRGs).

We find that the LIRG fraction correlates with both redshift and environment.
{\emph i}) LIRGs show an overall increase of their fraction with increasing redshift.  Such rise is predicted by the evolution of the LIRG luminosity function(Le Floc'h et al. 2005, Caputi et al. 2007, Magnelli et al. 2009) and of the mass function by spectral type (Ilbert et al. 2009b).
{\emph {ii}})  We find that the LIRG fraction decreases in the high density environments.
At densities larger than about $80\div 100$ Mpc$^{-2}$ the LIRG fraction drops compared to the low density environment.
The decrease of the LIRG fraction with increasing density is observed up to $z\sim 1.2$, but the dependence flattens with increasing redshift.
The difference between  the 3rd and the 4th density bin decreases from the low redshift sample (2.0$\pm$0.2 factor at $z=0.3\div 0.6$) to the high redshift ones (1.6$\pm$0.16 and 1.3$\pm$0.1 factors at $z=0.7$ and 0.9, respectively), for stellar masses M$^\ast=3\times 10^{10}-10^{11} $M$_{\odot}$.
The first two density bins should not be considered since in this range the uncertainties in the density measurement probably erase possible existing trends.

Figure  \ref{frlirglowz}, right panel, the LIRG fraction is shown for galaxies with stellar masses larger than M$^\ast=10^{11} $M$_{\odot}$.
Again, the LIRG fraction decreases towards high densities, and the decrease appears to flatten with increasing redshift.
The ratio between the third and fourth density bin is 2.15$\pm$0.2 at $z=0.3\div 0.6$ and it decreases to $1.6\pm0.15$ and $1.3\pm0.1$ at $z=0.7$ and 0.9, respectively.
At $z>1$ the LIRG fraction is constant at all densities within the errors for both stellar mass bins.

We note that the dependence is observed also for the LIRG sample cleaned from contribution by the AGN detected by XMM--Newton survey.
Indeed, the two samples, with and without AGN,  follow the same trend within the errors (Figure \ref{frlirglowz}).
The environmental properties of AGN in the large--scale structure and the comparison with star--forming galaxies are beyond the aim of this paper, and they  will be addressed in a separate work.

The decreasing fraction observed here is not due to projection effects since: a) the size of the two highest density bins is larger than the average scatter of the relation shown in Figure 4; b) the errors on projected densities tend to smooth out trends by scattering galaxies between contiguous bins.
We explore the possibility that the decreasing fraction of LIRG in the high density environment might be produced by mass segregation, i.e.  the most massive galaxies are formed in the most massive halos at earlier times, and therefore, preferentially reside in high density environments.
As mentioned before, we studied the environmental dependence in two stellar mass bins in order to minimize such effect.
In Figure \ref{frmass} we plot the normalized distributions of stellar masses of LIRGs and of the optical sample in redshift bins and in two regimes, high and low projected density ($>$ and $< 90/$Mpc$^{2}$ respectively).  The red histograms show the LIRG fraction, with poisson errors taken into account. Such fraction is plotted in 0.5 dex wide bins of stellar mass in order to minimize the noise.
The mass distribution of LIRGs is not skewed towards lower masses compared to optically--selected galaxies. The Kolmogorov--Smirnov (KS) test shows that the distributions of LIRGs and optical galaxies derive from the same parent population with a probability larger than $98\%$ for all the bins except the last three ($z=1\div 1.2$ and $z=0.8\div 1$, high density), for which the KS test gives no significant result.
However, the LIRG fraction does not show any significant trend as a function of stellar mass in any environment in the stellar mass range studied here.
Therefore the decreasing fraction of LIRGs in high densities (Figure \ref{frlirglowz})  is not a mass related effect but it is due to the environment.

Figure~\ref{frmipsz} shows the fraction of LIRGs as a function of redshift, normalized to their values in our first redshift bin ($z=0.5$).  Empty triangles represent the whole sample, regardless of the environment. The LIRG fraction increases with redshift, reflecting the evolution of the whole infrared selected population. This increase is similar to the global increase observed in Figure~\ref{frlirglowz}.
We compare it with the expectations from the known evolution of the galaxy population: we use the mass functions of Ilbert et al. (2009b) to compute the expected number of galaxies with M$_{\ast} >  3\times 10^{10}$M$_{\odot}$ in our field as a function of  redshift, and the infrared luminosity function of Magnelli et al. (2009) for the number of LIRGs in the field.
Given the relation between SFR and stellar mass at $z\sim 1$ calibrated by Elbaz et al. (2007), we expect the average SFR of a M$^\ast=3\times 10^{10} $M$_{\odot}$  galaxy will be $20\pm 10 $M$_{\odot}$/yr.
With our LIRG selection, equivalent to $SFR > 18 $M$_{\odot}$/yr we expect that most LIRGs lie above our mass threshold, but not all of them, given the scatter of the relation.
Therefore we can compute from the luminosity and mass functions (LF and MF)  an upper limit to our observed relation. The solid curve in Figure~\ref{frmipsz} shows the expected upper limit variation for the LIRG fraction. We find a  similar behavior, with the LIRG fraction increasing with redshift, but at a lower rate than what the LF and MF would predict: between $z=0.5$ and $z=1$, we observe a 3 fold increase in the LIRG fraction, while the computed increase is 4 fold. This discrepancy is expected since the solid line is an upper limit.
We plot with open circles the evolution of the LIRG fraction in low density environment ($5 < \Sigma_{10} < 10$ Mpc$^{-2}$), and with solid circles that for high density environment ($\Sigma_{10} > 90$ Mpc$^{-2}$). We find that the LIRG fraction evolves faster (a factor of 2) in high density environments than in low density ones, at 2$\sigma$ confidence level.  However, given the large errors, the high density environment fractions are still consistent with the low density environment fractions within 3 $\sigma$.

\begin{figure}
\begin{center}
\includegraphics[scale=0.4]{histomasslirg.v2.eps}
\caption{Normalized distributions of the stellar mass for the optically selected sample (thick solid histogram) and for LIRGs (shaded histogram), in redshift bins. Left panels show the distributions for projected density $<90/$Mpc$^2$, right panels those for density $>90/$Mpc$^2$. Red histograms show the LIRG fraction to optically selected galaxies, and poisson errors.}
\label{frmass}
\end{center}
\end{figure}

\begin{figure}
\begin{center}
\includegraphics[scale=0.4]{frmipsz_massf_evol_v5.eps}
\caption{Evolution of the normalized LIRG fraction with redshift in 3 redshift bins up to $z=$1. Open triangles: all LIRGs, filled circles: LIRGs in high density environment ($\Sigma_{10}>90$), open circles: LIRGs in low density environment ($\Sigma_{10}=5\div 10$, slightly shifted for clarity), solid line: expected evolution from Magnelli et al. (2009) LF and Ilbert et al. (2009b) MF.  The fractions are normalized to the value at $z=0.3\div 0.6$.}
\label{frmipsz}
\end{center}
\end{figure}

\section{CONCLUSIONS}

We studied the properties of a sample of LIRGs detected at 24 \micron\ in the COSMOS survey and with stellar masses M$^\ast>3\times 10^{10} $M$_{\odot}$ and $z=0.3\div 1.2$, as a function of the environment, by using accurate photometric redshifts.
In order to disentangle environment from any other possible effect  (mainly mass segregation) we studied the properties of our infrared galaxy sample in two bins of stellar mass.
The environment was characterized by using the distance of the 10th nearest neighbor, and the derived projected galaxy density  around each galaxy in redshift slices.
Our results can be summarized as follows:
\begin{itemize}
\item The median SFR and SSFR per LIRG increase with redshift, in agreement with the expected evolution of the LIRG luminosity and mass functions (Le Floc'h et al. 2005, Caputi et al. 2007).
The median SFR and median SSFR are constant at all densities within the errors, in agreement with what found by Hwang et al. (2010) in local LIRGs.
We do not observe the reversal of the SFR density relation up to $z\sim 1$ for our mass--selected LIRG sample.
Such reversal, if any, might occur at $z>1$ for high--mass LIRGs.
This is not necessarily true for galaxies of smaller stellar mass.

\item We find that the fraction of massive LIRGs among optically selected galaxies with the same stellar mass, varies as a function of both redshift and environment.
The global LIRG fraction increases with increasing redshift, as expected from the cosmic evolution of the SFR density and of the infrared LF.
The LIRG fraction decreases with increasing environment density.  Such decrease flattens going from $z=0.4$ to $z\sim 1$ and the fraction is constant in all environments for $z>1$. These results imply that the evolution of the LIRG fraction among optically selected galaxies from $z=1$ to $z=0.4$ is roughly twice as fast in dense than in low density environments.

\item Finally, we find that a large fraction of LIRGs is present in the most dense environments by $z\sim 1$. These might be the progenitors of the  massive galaxies found today in the center of clusters, which therefore were not likely formed through dry mergers.
\end{itemize}

Using photometric redshift, with their inherent limitations, we have shown that LSS and environment has a role on star formation. Future works based on spectroscopic surveys will refine these results in the densest structures, and open the realm of low density where our estimator is limited.

\acknowledgments
This work is based on observations made with the \emph{Spitzer Space Observatory}, which is operated by the Jet Propulsion Laboratory (JPL) , California Institute of Technology  under NASA contract 1407.
Support for this work was provided by ANR "D--SIGALE" ANR--06--BLAN--0170 grant.
Support for this work was provided in part by NASA through contracts 1282612 and 1298231 issued by the JPL, and grants 1289085, 1310136.
We thank the anonymous referee for carefully reading and providing useful suggestions that improved the paper.

redpajama_set_name: RedPajamaArXiv


Can she ruin things for him and Jasmine?
During her first shift at Salt, Ebony listens as Colby opens up about how his stepdad took off with his mum and his sister several years ago. Pretending she doesn't already know this, Ebony plays sympathetic while also getting some intel on the status of Colby's casual relationship with Jasmine. Sure enough, it's not long before Jasmine gets suspicious over Colby and Ebony.
The next day, things get worse when Ebony "accidentally" lets slip to Jasmine that Colby confided to her about his sister. With her jealousy and insecurity sparked once more, Jasmine confronts Colby yet again and accuses him of flirting with Ebony. Colby is insulted by the accusation and Jasmine realises her mistake and tries to backtrack. She asks if they can meet up later and forget this conversation ever happened, but she's concerned the damage has already been done.
Later, Ebony apologises to Colby for "unintentionally" making things difficult with Jasmine. Colby promises that she doesn't have to worry about it and tells her that the pair of them are heading to Salt for a gig tonight. Jasmine gets dressed up for the occasion, trying to make up for her questioning earlier, but is rattled with Ebony turns up to crash the party.
Not wanting to look ungracious, Jasmine forces a smile and invites Ebony to join them – the more the merrier. Ebony happily accepts the invitation, glad to be driving a wedge between Colby and the woman he likes.
Meanwhile, after receiving a call from Ben revealing that Maggie has collapsed, a panicked Ziggy runs to Brody to give her a lift to the hospital. She arrives to find that Maggie has contracted pneumonia and is unable to fight the infection. Tori and the team endeavour to get the fever and infection under control as Ben blames himself for letting Maggie go back to work – no doubt she caught something while she was around the school kids.
Later, Tori has more bad news for the Astoni family. Maggie's cancer markers have gone up, which means the transplant with Ziggy was rejected, much to Ziggy's distress. Furthermore, the antibiotics haven't helped with Maggie's pneumonia. Tori explains that if there's no improvement in the next 48 hours, they'll have to put Maggie in an induced coma and on life support.
Elsewhere, Coco pushes Ryder further away.


Rocky Auto Electric and Diesel Repair Ltd A-T Driveline - Rocky Auto Electric & Diesel Repair ltd.
A-T Driveline offers driveline repair and manufacturing for automotive, heavy truck, off-road, and agricultural equipment. Our Rocky Mountain House location is equipped to offer in-house driveline manufacturing and repair using our full service lathe and balancer. We have the equipment, in-house expertise and capacity to offer our services to both our Rocky Mountain House customers, as well as, our customers in Drayton Valley and everywhere in-between.


Jack-o-Laterns used to require block underneath.
Then they could be placed w/o block underneath 'sticking' to side block and floating.
Now they are back to block underneath.
Why do they require a block underneath. Sea Lanterns don't. Glowstone doesn't. It was really nice not having to build top down to place.
If a block doesn't fall due to gravity (sand, gravel) it shouldn't require a block underneath it to place.


Quiz on Kingdoms, Immune System and Viruses the NEXT time we come to class.
Here are some videos that will help you with this unit of study.
Here are some videos that you can watch to help you review for Tuesday's test.
Make sure your notebook is in order. Check off sheet is below. ALL ITEMS MUSt BE AtTACHED IN THE PRONGS OF YOUR FOLDER.
Complete lab if you did not turn yours in during class today.
Finish lab to turn in if you did not finish it in class today.
Here's the Quizizz Link for tomorrow's Lab Safety and Tools Quiz. STUDY!!!!
Have parent/guardian to fill out Google Form with contact info. There is a link below.


text:
Q: Always append arguments to command in Powershell There's a few commands I need to run repetitively in Powershell, with some variable arguments in content and length, but some arguments must always be there. I don't want to forget those arguments, so is there a way to create a function that does this?
I have tried using things like Invoke-Expression, but when I use brackets in a command, Powershell thinks it's a type and tells me my cast is not valid. If I escape the argument list and provide an argument in the form Key=Value, PowerShell parses it into a System.Object[] and the command fails. I figured it might be better not to ask about how to fix that, but how to solve my root problem.
You can consider this a somewhat duplicate of How to always append an ampersand for certain commands? (MacOS / bash) but for PowerShell.

A: Just write your own version of the command as a Function with mandatory parameters:
Function RunMyCommand {
    Param(
        [Parameter(Position=0,mandatory=$true)][string]$Argument1,
        [Parameter(Position=1,mandatory=$true)][int]$Argument2,
        [Parameter(Position=2,mandatory=$true)]$Argument3
    )
    # Amend this according to the syntax and string manipulation required for your command
    ThisIsMyCommand $Argument1 $Argument2 $Argument3
}

RunMyCommand -Argument1 ThisString -Argument2 ThisNumber -Argument3 ThisAnything

redpajama_set_name: RedPajamaStackExchange


text:
Martha W. McCartney is an American research historian and writer.

Biography
McCartney is a William and Mary graduate. She worked for thirteen years at the Virginia Research Center for Archaeology, researching and excavating archaeological sites in Virginia. Since 1986 she has worked as an independent historian. She is also a consultant for the Colonial Williamsburg Foundation and was project historian for the five-year Jamestown Archaeological Assessment conducted by the National Park Service.

Her books include James City County: Keystone of the Commonwealth (1997), The History of Green Spring Plantation (1998), The Free Black Community at Centerville (2000),  Jamestown: An American Legacy (2001), which won the 2004 National Park Service Excellence in Interpretive Media award in the Cultural Book Category, With Reverence for the Past: Gloucester County, Virginia (2001), Virginia Immigrants and Adventurers 1607–1635: A Biographical Dictionary (2007), Jordan's Point, Virginia: Archaeology in Perspective, Prehistoric to Modern Times (2011), and Mathews County, Virginia: Lost Landscapes, Untold Stories (2015).

McCartney has won historic preservation awards, including a National History Award from the Daughters of the American Revolution in 2001.

References

21st-century American historians
Writers from Virginia
Living people
Year of birth missing (living people)
Historians of the Thirteen Colonies
College of William & Mary alumni
American women historians
21st-century American women

redpajama_set_name: RedPajamaWikipedia


text:
49er Festival
Back to Yosemite Chamber
Historic Highway 120
Tuolumne County News
Yosemite Hwy 120 Rock Star
Kathy Brown
Taking You Back in History - Making the Grade
By Kathy Brown
Southern Tuolumne County Historical Society
Well known to "locals", and often awe-inspiring and a challenge to travelers, is "The Grade", the steep 1600 foot ascent connecting Moccasin at the bottom of Priest Hill to Priest Station and the rolling terrain beyond at the top. Priest Grade boasts two different roads - "Old" and "New" - on opposite sides of Grizzly Gulch.
The first track up the hill was a steep trail on the south side. In the 1850s, it was used by early miners and pack animals heading to the gold camps of Big Oak Flat and Garrote (now Groveland). The trail traversed the hill between the current Old Priest Grade and the Hetch Hetchy penstocks that are so visible to today's traveler on the approach to "The Grade" from the west. The miners trail was so rugged that a replacement – the Grizzly Gulch Wagon Road (now the Old Priest Grade) – was built in 1859. Even in 1900 freight wagons could take two days to haul a heavy load from Chinese Camp to Big Oak Flat. Surrounding communities began advocating for an easier and faster road.
The need for a less steep road increased after 1901 when the first loco-mobiles (steam-powered cars) could barely make it to the top and the first gas-driven automobiles were unable to "make the grade". With a can-do attitude and remarkable community spirit, local citizens banded together to build a new approach to the top without government assistance. In 1911 they surveyed a new route on the north side of the gulch. They donated labor, transport, and supplies and began construction, mostly by hand. They completed a rough 8 foot wide roadbed along most of the new route. Then the private project stopped due to problems in financing and gaining access from some landowners.
Watch for Part II of Making the Grade.
STCHS
Old Priest Grade
New Priest Grade
Big Oak Flat
Chinese Camp
Grizzly Gulch
Priest Station

redpajama_set_name: RedPajamaCommonCrawl


The complex is located in an elevated position in the foothills of Five Finger Mountain, some 7.5 km from Esentepe. The hotel's private beach is 1.5 km from the residences and a shuttle service is available. The harbour town of Girne (Kyrenia) is approximately 20 km away, while Ercan Airport is at 35 km. The residences form part of a golf and country club built on hills overlooking the Mediterranean Sea and offering a peaceful vacation for golf enthusiasts and guests who enjoy a relaxing location. Guests can benefit from the golf clubhouse facilities.


text:
Cleantech Lithium Share Price Today
Cleantech Lithium Share Price Chart
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Follow CTL
Cleantech Lithium Plc LSE:CTL London Ordinary Share JE00BPCP3Z37 ORD GBP0.01
0.50 0.92% 55.00 54.00 56.00 55.00 54.50 54.50 26,406 08:09:35
Alternative Energy 0.0 -1.2 0.0 - 58
CleanTech Lithium PLC Results of Fundraising
UK Regulatory (RNS & others)
Cleantech Lithium (LSE:CTL)
From Jul 2022 to Jan 2023
TIDMCTL
RNS Number : 6895D
CleanTech Lithium PLC
THIS ANNOUNCEMENT AND THE INFORMATION CONTAINED HEREIN IS RESTRICTED AND IS NOT FOR RELEASE, PUBLICATION OR DISTRIBUTION, IN WHOLE OR IN PART, DIRECTLY OR INDIRECTLY, IN, INTO OR FROM THE UNITED STATES, AUSTRALIA, CANADA, JAPAN, NEW ZEALAND, THE REPUBLIC OF SOUTH AFRICA OR ANY OTHER JURISDICTION IN WHICH SUCH RELEASE, PUBLICATION OR DISTRIBUTION WOULD BE UNLAWFUL.
THIS ANNOUNCEMENT CONTAINS INSIDE INFORMATION FOR THE PURPOSES OF REGULATION (EU) 596/2014 AS IT FORMS PART OF DOMESTIC LAW IN THE UNITED KINGDOM BY VIRTUE OF THE EU (WITHDRAWAL) ACT 2018 ("MAR").
("CleanTech" or the "Company")
Results of Fundraising
CleanTech Lithium PLC ("CTL", "CleanTech Lithium" or the "Company"), a company involved in the exploration and development of three lithium projects in Chile, is pleased to announce the successful completion of the Placing and Retail Offer (together the "Fundraising") announced on 20(th) October 2022 (the "Launch Announcement"), conditional inter alia on shareholder approval. The Fundraising raised gross proceeds of approximately GBP 12.3 million and was upsized due to investor demand.
Results of the Fundraising
A total of 25,531,915 Placing Shares will be issued to new and existing institutional investors pursuant to the Placing by Fox-Davies Capital Limited and Canaccord Genuity Limited (together the "Joint Bookrunners"), at the Issue Price. In addition, 568,343 Retail Offer Shares will be issued to retail shareholders who subscribed through the PrimaryBid platform at the Issue Price pursuant to the Retail Offer.
A total of 26,100,258 Fundraising Shares will therefore be issued pursuant to the Fundraising representing approximately 24.83 per cent. of the Company's enlarged ordinary share capital following Admission.
The Issue Price represents a 3.98 per cent. discount to the 10-day VWAP on 19 October 2022.
The Fundraising Shares will, when issued, be credited as fully paid and will rank pari passu in all respects with the existing Ordinary Shares of the Company, including the right to receive all dividends or other distributions made, paid or declared in respect of such shares after the date of issue of the Fundraising Shares.
General Meeting and Posting of Circular
The Fundraising is subject to shareholder approval at the General Meeting ("GM"), expected to be held on 14 November 2022. The Company expects to publish, on or about 24 October 2022, a shareholder circular to convene the General Meeting and a further announcement will be made in due course.
Admission and Trading
Application will be made to London Stock Exchange for the Fundraising Shares to be admitted to trading on AIM. It is currently expected that Admission will become effective, and trading of the Fundraising Shares will commence on AIM, at 8.00 a.m. on 16 November 2022.
Words and expressions defined in the Launch Announcement shall have the same meaning in this announcement.
Aldo Boitano, Chief Executive Officer of CleanTech Lithium Plc, commented:
"We are delighted at the outcome of the Placing which was oversubscribed and undertaken at a time of very difficult market conditions. We have secured some terrific new names on our share register and have also received excellent support from some of our current shareholders who have invested again in this round, some increasing their stake in the Company. We are very grateful for this support and believe this demonstrates the confidence of investors in our plans to deliver material growth for the Company over the coming years.
The new funds will enable the Company to progress our resource evaluation programmes on all three of our projects and will also allow us to undertake additional drilling activities at Llamara, should we have success on the exploration well. We are excited about the possibilities on that opportunity and should be reporting the results of the three drilling campaigns in Q1 2023 and Q2 2023, hopefully providing upgrades to our overall resource base, with more resource being categorised as Measured and Indicated. The new funds will also allow us to complete the important technical work being progressed on the EIA, Scoping and Hydrogeology Studies, and also on the Laguna Verde PFS when commenced in the near future.
Our Board is looking forward to the future with confidence and the new funds will provide the financial firepower to help us achieve our goals and deliver the increase in shareholder value we believe is possible."
For further information visit www.ctlithium.com or contact
the following:
Aldo Boitano                       Jersey office: +44 (0) 1534
Gordon Stein                       668 321
Chile office: +562-32239222
Or via Celicourt
Celicourt Communications           +44 (0) 20 8434 2754
Felicity Winkles/Philip Dennis     cleantech@celicourt.uk
Beaumont Cornish Limited
(Nominated Adviser)
Roland Cornish                    +44 (0) 207 628 3396
Fox-Davies Capital Limited
(Joint Broker & Bookrunner)        +44 20 3884 8450
Daniel Fox-Davies                  daniel@fox-davies.com
Canaccord Genuity Limited
(Joint Broker & Bookrunner)
James Asensio
Gordon Hamilton
Sam Lucas                          +44 (0) 207 523 4680
Expected Timetable of Principal Events
The times and dates set out below are subject to change, and may be adjusted by the Company in consultation with the Joint Bookrunners. The timetable below also assumes that the Resolutions are passed at the GM without adjournment. In the event of any significant changes from the below expected timetable, details of the new times and dates will be notified to Shareholders by an announcement on a Regulatory Information Service.
General Meeting                                           10.00 a.m. on 14
Expected time of announcement of results          Afternoon of 14 November
of the General Meeting
Admission effective and dealings in the           8.00 a.m. on 16 November
Fundraising Shares expected to commence
on AIM
Expected date for crediting of the Fundraising    8.00 a.m. on 16 November
Shares in uncertificated form to CREST stock
------------------------------------------------  -------------------------
CleanTech Lithium:
CleanTech Lithium (AIM:CTL) is an exploration and development company, advancing the next generation of sustainable lithium projects in Chile. The Company's mission is to produce material quantities of battery grade lithium with near zero carbon emissions and low environmental impact, offering the EU EV market a green lithium supply solution.
CleanTech Lithium has two prospective lithium projects in Chile - Laguna Verde and Francisco Basin projects located in the lithium triangle, the world's centre for battery grade lithium production. They are situated within basins entirely controlled by the Company, which affords significant potential development and operational advantages. The projects have direct access to excellent infrastructure and renewable power. The Company has also further applied for an additional 119 exploration licences at Llamara, as a low cost and commitment greenfield project to complement the existing more advanced projects.
CleanTech Lithium is committed to using renewable power for processing and reducing the environmental impact of its lithium production by utilising Direct Lithium Extraction (DLE). DLE is a transformative technology which only removes lithium from brine, with higher recoveries and purities. The method offers short development lead times, low upfront capex, with no extensive site construction and no evaporation pond development so there is no water depletion from the aquifer or harm to the local environment.
The distribution of this announcement and the offering of the Placing Shares in certain jurisdictions may be restricted by law. No action has been taken by the Company or the Joint Bookrunners that would permit an offering of such shares or possession or distribution of this announcement or any other offering or publicity material relating to such shares in any jurisdiction where action for that purpose is required. Persons into whose possession this announcement comes are required by the Company and the Joint Bookrunners to inform themselves about, and to observe, any such restrictions.
This announcement is not for release, publication or distribution, in whole or in part, directly or indirectly, in or into Australia, Canada, Japan or the Republic of South Africa or any jurisdiction into which the publication or distribution would be unlawful. This announcement is for information purposes only and does not constitute an offer to sell or issue or the solicitation of an offer to buy or acquire shares in the capital of the Company in Australia, Canada, Japan, New Zealand, the Republic of South Africa or any jurisdiction in which such offer or solicitation would be unlawful or require preparation of any prospectus or other offer documentation or would be unlawful prior to registration, exemption from registration or qualification under the securities laws of any such jurisdiction.
This announcement is not for publication or distribution, directly or indirectly, in or into the United States of America. This announcement is not an offer of securities for sale into the United States. The securities referred to herein have not been and will not be registered under the U.S. Securities Act of 1933, as amended, and may not be offered or sold in the United States, except pursuant to an applicable exemption from registration. No public offering of securities is being made in the United States.
Fox-Davies Capital Limited is authorised and regulated by the FCA in the United Kingdom and is acting as joint bookrunner exclusively for the Company and no one else in connection with the Placing and will not be responsible to anyone (including any Placees) other than the Company for providing the protections afforded to its clients or for providing advice in relation to the Placing or any other matters referred to in this announcement.
Canaccord Genuity Limited is authorised and regulated by the FCA in the United Kingdom and is acting as joint bookrunner exclusively for the Company and no one else in connection with the Placing and will not be responsible to anyone (including any Placees) other than the Company for providing the protections afforded to its clients or for providing advice in relation to the Placing or any other matters referred to in this announcement.
Beaumont Cornish Limited, which is authorised and regulated in the United Kingdom by the Financial Conduct Authority, is acting as nominated adviser to the Company in relation to the Placing and is not acting for any other persons in relation to the Placing. Beaumont Cornish Limited is acting exclusively for the Company and for no one else in relation to the matters described in this announcement and is not advising any other person and accordingly will not be responsible to anyone other than the Company for providing the protections afforded to clients of Beaumont Cornish Limited, or for providing advice in relation to the contents of this announcement or any matter referred to in it.
This information is provided by RNS, the news service of the London Stock Exchange. RNS is approved by the Financial Conduct Authority to act as a Primary Information Provider in the United Kingdom. Terms and conditions relating to the use and distribution of this information may apply. For further information, please contact rns@lseg.com or visit www.rns.com.
RNS may use your IP address to confirm compliance with the terms and conditions, to analyse how you engage with the information contained in this communication, and to share such analysis on an anonymised basis with others as part of our commercial services. For further information about how RNS and the London Stock Exchange use the personal data you provide us, please see our Privacy Policy.
ROIUAVVRUUURURA
October 21, 2022 02:00 ET (06:00 GMT)
1 Year Cleantech Lithium Chart
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Cleantech ..


text:
Miss N.C. prepares for Miss America finals
David Anderson, Staff Writer
Jan 11, 2013 at 12:01 AM Jan 11, 2013 at 10:21 PM
Top 15 will compete for 2013 crown live on ABC tonight
LAS VEGAS � Arlie Honeycutt, like the rest of North Carolina, will be waiting with baited breath tonight as the names of the top 15 contestants in the 2013 Miss America pageant will be announced on live television.
Those 15 women will go on to compete � also on live television � for the Miss America crown. They will be chosen from among 53 contestants representing all the U.S. states, the District of Columbia and U.S. territories.
�It will all be right there,� said Honeycutt, 20, who is representing The Tar Heel State as Miss North Carolina 2012.
The Garner native and current ECU junior is the former Miss Kinston-Lenoir County 2012. She spoke to The Free Press by telephone Friday following a whirlwind week of preliminary competitions, interviews and seeing some of the Las Vegas sights.
�I�ve been kind of star studded by the former Miss America, the judges, the star personalities,� Honeycutt said. �It�s just a really, really cool experience.�
Honeycutt was the 75th Miss N.C. when she was crowned last June, and she is the first representative of Kinston and Lenoir County to win the state title and compete for the national title since Constance Ann Dorn of Kinston was crowned in 1972, according to the Miss N.C. website.
�It�s been awesome, the support team from Kinston,� she said. �I�ve been really excited to get to see so many people.�
Honeycutt�s parents, Beth and Scott, and her 15-year-old brother Jackson are with her in Las Vegas, as well as extended family, a number of supporters from the Miss North Carolina and Miss Kinston-Lenoir County organizations, even winners of local Kinston and Lenoir County pageants, such as Teigha Beth Bailey, the current Kinston-Lenoir County�s Outstanding Teen.
�I have a nice group of family, my extended family is here, and so that�s been really great,� she said.
Honeycutt and her fellow contestants have taken part in swimsuit, evening gown, talent and on-stage interview competitions. The judges will tabulate the scores for each contestant, and the top 15 scorers will be announced tonight live.
Honeycutt�s talent is singing � she is majoring in vocal performance at ECU.
�Go Pirates!� she exclaimed.
Although she and her fellow contestants are under protection �24/7� by �an awesome� security team, they have been able to get out to see various hotels, casinos and other attractions in Las Vegas.
�We�re really grateful to represent our towns, our states; and to be here it�s just icing on the cake,� she said.
David Anderson can be reached at 252-559-1077 or David.Anderson@Kinston.com. Follow him on Twitter at DavidFreePress.
WANT TO WATCH?
The 2013 Miss America pageant will air live on ABC � WCTI-12 locally � at 9 p.m. today


Cadillac has come a long way since hitting bottom in the '80s and '90s, and the revival of its '60s-vintage Art & Science design language—which hearkens back to better times for the brand—is in full swing.
Sharp body creases and rakish lines likely sculpted to incite imagery of wind tunnel testing give the updated 2018 Cadillac XTS a more distinctive appearance and better tie the car to the rest of the company's lineup. The look can be polarizing, though. Not everyone likes its edginess, and many prefer the more sedate aesthetics of vehicles from Audi, BMW and Mercedes-Benz. The question is: does the substance below this Cadillac's skin meet the standards of luxury car shoppers who are also looking at alternatives from Germany's big three?
The 2018 XTS has freshened styling with the same edgy look as other Cadillacs, but its design is less refined than more recent introductions to the lineup.
Cadillac certainly seems to understand that today's luxury customer isn't interested in boring cars, and the XTS V-Sport toes the line on that count thanks to a 410-horsepower V6 offering gutsy acceleration. The car handles well, too.
But it's difficult to understand why the XTS still exists, because Cadillac has clearly moved on to better things. Side by side, the XTS looks, feels, and drives in far less refined manner than the weirdly invisible CT6, and the company is already reassigning "XT" naming conventions to its growing lineup of crossover SUVs.
Clearly, a customer for this kind of car remains, and so Cadillac has spruced the XTS up even as the car's twilight approaches.
Dash, door panels, seats and carpet are all top quality, as they should be in a Cadillac.
Spacious and attractive, the XTS Platinum trim employs only top quality materials, as it should for a price that starts at $66,690 before adding the V-Sport treatment (my test car opened at $73,490).
The V-Sport's 22-way power adjustable front seats, which are comfortable to begin with, included heating, cooling and several massage settings. The back seat, as one would expect from a larger Cadillac, is cavernous.
What detracted most from comfort were the V-Sport's 20-inch wheels and low-profile tires, which transmitted the jolts from New York City's myriad potholes directly to the driver and passengers in spite of the car's adaptive suspension. No amount of seat cushioning and suspension wizardry can overcome inadequate sidewall height.
The XTS has an 18 cubic-foot trunk, one that's laid out well for fitting suitcases and other bulky items. But—and this is a big but—because of the car's fastback profile, the trunk opening is very small, which makes it difficult to fit some of the bulky items the trunk would otherwise be large enough to accommodate. Also, because of its depth from front to back, you might have to climb halfway into the trunk to reach smaller items that have made their way forward while you were driving.
Cadillac has finally done away with its haptic feedback non-buttons, in all models but the 2018 XTS.
I can't say anything about the controls on this car without expressing how much I hate Cadillac's haptic feedback non-buttons.
There's no doubt that the dash looks super clean without a bunch of knobs and buttons cluttering up its space-age aesthetic. But as of right now, this method of controlling electronic devices isn't a good one. There's too much unpredictability. As in, is this button going to work when I press it? Half the time, the answer is no.
Fortunately, Cadillac has solved this problem in the much better CT6 by hiding the buttons beneath a smooth veneer. There's a solid click when you depress the button beneath the panel's glasslike surface—confirmation that what you're trying to do is going to work.
One could certainly argue that fickle, blood pressure-boosting touch panel controls—always so prone to hiccups—are a serious driver-distracting safety hazard. For instance, I lost an undue amount of focus from the road when I went to un-mute the stereo and it didn't do anything for a while until it boosted the volume to full blast and wouldn't go back down.
Fortunately for Cadillac, the relevant authorities have deemed the XTS safe on the structural end of things. The Insurance Institute for Highway Safety (IIHS) gave it top marks in most of its crash tests (the XTS hasn't been assessed for small overlap frontal impact safety). Additionally, the federal government awarded the car with a 5-star overall rating.
The 2018 Cadillac XTS may be a bit behind the curve in other respects, but in V-Sport guise it lacks nothing in the performance department.
This car runs like a scalded monkey, thanks to a 410-horsepower, 3.6-liter twin-turbocharged V6.
Unlike the performance-tuned Cadillac ATS-V and CTS-V, which give away their muscular mechanicals with sculpted-in body bulges and more aggressive stances, the only thing to let you know there's anything that sets this XTS apart from the others sitting in the country club parking lot is its subdued V-Sport badging.
That makes this car a sleeper.
From every stoplight I departed, I was the undisputed king in this car, which is probably why my in-town fuel economy was a dismal 10.3 mpg, according to the car's mileage computer. Overall, when I drove the car like a semi-sane human being on a mix of highway and city roads, it returned a respectable 17.5 mpg, coming close to matching the EPA's rating of 18 mpg in combined driving.
Naturally, there's a Sport mode. And when you shift the transmission lever into its manual mode, the tachometer in the center of the instrumentation glows white so that you know it's go time. The transmission's paddle shifters work well, although this low-revving turbocharged V6 wants you to shift sooner than you might think.
A standard Magnetic Ride Control adaptive suspension made for responsive handling, and the XTS's four-wheel Brembo performance brakes added plenty of driving confidence.
The Cadillac XTS has had a good run, but it's time to cancel it in favor of more modern and capable models like the CT6.
The XTS is in a funny place within Cadillac's current lineup. Something of a holdover from days gone by, it doesn't really fit into a Cadillac stable that's seen significant modernization and improvement over the past decade.
In terms of its size, it's very similar to the CT6, Cadillac's fantastic new flagship sedan. Comparatively speaking, though, the XTS is a dated artifact of days gone by, making it difficult to imagine why anyone would select this car over the sleeker (although more expensive) CT6.
In terms of its price, it overlaps with the impressive Cadillac CTS, which drives dynamic rings around the XTS even if it cannot match the car for rear seat room and trunk space.
I don't understand why the XTS still exists, let alone why the car is updated for 2018. Cadillac is, in theory, a prestige brand. But I live in New York City, where the who's who haven't driven Cadillacs since Jimmy Carter was president.
Presumably, in other parts of the country, things are different. Here in NYC though, there's nothing this car can do that a comparable Audi A6, BMW 5 Series, or Mercedes-Benz E-Class can't. Those cars also carry more weight, prestige-wise.
Let's say you're in it for the luxury and don't care what other people think. Well, the Korean car companies are making some really nice luxury sedans for a lot less money.
If you're a Cadillac loyalist, you can buy a similarly equipped CT6—a car that's a lot nicer than the XTS and is available with technology that will drive the car for you on the interstate—for about the same price.
It's not that the XTS is a bad car. It's not. In fact, it's actually quite nice, and the V-Sport version is a blast to drive. But there isn't a compelling reason to get one when both Cadillac and the competition have better cars available.
Clearly perhaps to everyone but Cadillac, the time has come for the XTS to go gentle into that good night.


text:
WhatsApp Officially Launches New, 8-Person Group Video Chat Option
After it was previewed by Facebook CEO Mark Zuckerberg late last week, WhatsApp has now officially announced the launch of its new, 8-person, encrypted video chat option, which doubles the capacity of WhatsApp group video calls. As explained by WhatsApp: "The COVID-19 pandemic has meant that many of us are isolated from friends and family, and as a result, we've seen that people are turning to voice and video calling on WhatsApp more than ever before. Group calling has been particularly useful and our users have asked to connect with more people at once. Starting today, we're doubling the number of participants you can have on a WhatsApp video or voice call […]
Andrew Hutchinson News Aggregation #digitalmarketing, Social Media Today
Pinterest Joins 'Stand for Small' Coalition to Assist SMBs, Provides New Resource Hub
With Pinterest searches for "support small business" increasing by over 350% during the COVID-19 lockdowns, and small businesses playing a key role in the broader Pinterest eco-sphere, the platform is looking to provide more assistance for SMBs impacted by the pandemic. This week, Pinterest has announced that it's joining the 'Stand for Small' collective, while it's also put together a new collection of resources to help businesses optimize their Pin presence. As explained by Pinterest: "Small businesses today are among the hardest hit by the effects of COVID-19, as they have less of a cushion to withstand such a dramatic slowdown. That's why we're proud to join the #StandForSmall coalition along […]
Facebook's Holding a Virtual a Graduation Event for the Class of 2020, Hosted by Oprah Winfrey
Among the various impacts of the COVID-19 shutdowns, one of more significant aspects that can get overlooked is the amount of social and development time that youngsters are losing out on by being at home, and away from schools, sports and other connective events. Teenagers, in particular, are at a crucial stage of their lives, where they're learning more about who they are, what they're interested in, and where they stand in the broader social scale. The more they miss out on this, the bigger the impact becomes, so it's important, where possible, that we look to facilitate ways for younger people to connect with friends and maintain those links, […]
Facebook's Holding a Virtual Graduation Event for the Class of 2020, Hosted by Oprah Winfrey
YouTube Expands Fact Check Panels to US Users as It Works to Counter COVID-19 Misinformation
After recently ramping up its efforts to remove videos that include 'medically unsubstantiated' claims about COVID-19 from its platform, YouTube has now announced another element in its push to reduce the distribution of coronavirus conspiracy theories, with the expansion of its fact-check pop-up alerts on searches that are prone to misinformation. As you can see in this example, the new 'independent fact check' alerts will appear on searches related to topics that have seen significant misinformation, or have been debated by official review sources. YouTube partners with various fact-checking organizations to review such claims, and the alerts aim to help reduce the spread of misinformation by providing alternate links to authoritative […]
Instagram Publishes New Guide to Help Businesses Make Best Use of the Platform Amid COVID-19
Instagram has published a new COVID-19 playbook for businesses, which outlines a range of ways in which brands and marketers can make best use of the platform's various tools to help maintain connection with their audiences, and maximize performance, during the global pandemic. The guide includes both specific tips on what you should be looking to use Instagram's functions for, as well as 'how to' overviews for each element. The first section of the guide looks specifically at how brands can 'take action during COVID-19' by utilizing the available tools, including notes on Instagram Live, IGTV and Stories. These are some good pointers and considerations – and while Instagram only touches on […]
Instagram Adds Live Donations Feature for Fundraising via Instagram Live
Instagram continues to explore new ways to help people and businesses impacted by COVID-19. Today, Instagram has launched a new fundraising option within Instagram Live, which will enable users to raise funds during a Instagram Live stream – like a small-scale telethon via the app. As explained by Instagram: "Many people are facing challenges at this time, and we want to do our part to support nonprofits and communities who need it the most. Now, you can easily create a fundraiser on Live with 100% of the money raised going directly to the nonprofit of your choice." As you can see in the above screenshots, to create your own Instagram […]
Content Mapping 101: The Template You Need to Personalize Your Marketing
What is a Content Map? A content map is a plan to deliver the right content, to the right people, at the right time. Content mapping takes into account the characteristics of the person who will be consuming the content and their lifecycle stage. Marketers hear it all the time: The content you create needs to be personalized. It needs to be aligned with the wants and needs of your customers (and prospective customers). It needs to resonate with them. It needs to feel like it was created just for them. On its surface, this sounds like great advice. Personalization, giving people content that they're actually interested in … it […]
edevaney@hubspot.com Erik Devaney News Aggregation #digitalmarketing, HubSpot
How working from home has thrown a wrench in campaign targeting [Video]
The ability to work from home is helping businesses stay in operation as the world continues to find ways to overcome COVID-19. For some businesses, this is a mixed blessing as their now decentralized staff has to make sense of data that may not be as reliable due to the unexpected shift in work environments. "One thing we've noticed a lot in B2B, almost more than B2C, is analytics data being terrible right now, because all of a sudden your B2B companies who are 10, 20, 30,000 employees are at home, logging into your corporate website and all your IP filters are gone," said Brad Geddes of AdAlysis during our […]
Did you know that 92% of U.S. organic visits are produced by Google?
Google reigns over organic search, we knew that. According to Merkle, in Q3 2019, Google produced 92% of total U.S. organic search visits (95% on mobile). With a dominant presence, it comes as no surprise that Google continues to move the needle in SEO. The search titan is driving innovation, and they aren't slowing down any time soon – BERT, anyone? This SEO trend is one of many trends you'll uncover in MarTech Today's Enterprise SEO Tools for Content Marketing, Search Intelligence, UX and More. Our free, downloadable guide looks at the trends SEOs and vendors are adapting to. It also features 20 in-depth SEO platform company profiles and the software they […]
Lauren Donovan News Aggregation #digitalmarketing, Search Engine Land


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Titans Complete Interviews with Bears Assistant General Manager Ian Cunningham and Cardinals Vice President/Player Personnel Quentin Harris for the Team's General Manager Position
NASHVILLE – The Titans on Saturday interviewed Bears Assistant General Manager Ian Cunningham and Cardinals Vice President/Player Personnel Quentin Harris for the team's General Manager position.
Cunningham, who just completed his first season with the Bears, has 14 years of NFL front office experience.
Cunningham previously served as Director of Player Personnel for the Philadelphia Eagles, a position he was promoted to at the beginning of the 2021 season. Prior to his promotion, Cunningham worked as the Assistant Director of Player Personnel (2019-20) and oversaw the college scouting department from 2017-18 as the Director of College Scouting with the Eagles.
Cunningham's NFL front office career began in 2008 when he was hired in Baltimore as a Player Personnel Assistant. After five seasons as an assistant, he worked as a Southeast Area Scout for the Ravens for two seasons (2013-14) before taking on additional responsibility as the Southeast/Southwest Area Scout from 2015-16.
Cunningham, who played at the University of Virginia, was an offensive lineman who signed with the Kansas City Chiefs in 2008 as an undrafted free agent.
Harris, meanwhile, just completed his 15th season in Arizona's scouting department and second as Vice President, Player Personnel after being promoted last February. Prior to his promotion, Harris spent two years (2019-20) as Director, Player Personnel after working as the team's Director, Pro Scouting for six seasons (2013-18).
According to the Cardinals media guide, worked alongside former Cardinals GM Steve Keim, managing both the college and pro personnel departments. His duties include evaluating the top college prospects nationally as well as the organization and implementation of the draft process. Harris oversees the pro personnel department which includes player acquisition, evaluation and assisting with player contract negotiations.
Harris, who played free safety for four seasons with the Cardinals (2002-05), began his scouting career after finishing his NFL playing career with the Denver Broncos in 2007. He joined the Cardinals in 2008 as a pro scout and was elevated to Assistant Pro Personnel Director in 2010.
On Friday, the Titans interviewed with Browns Assistant General Manager/VP of Player Personnel Glenn Cook and 49ers Director of Player Personnel Ran Carthon.
On Thursday, the Titans interviewed in-house candidates Ryan Cowden and Monti Ossenfort.
Back on December 6, Titans controlling owner Amy Adams Strunk made the decision to part ways with general manager Jon Robinson, who was hired prior to the 2016 season.
Strunk is leading the process of finding his replacement, and the plan is to interview a large number of candidates, including personnel evaluators across the NFL.
Strunk said a committee including herself, Kenneth S. Adams, IV from the ownership group, President and CEO Burke Nihill, Senior VP/Business Affairs and Chief Legal Officer Adolpho Birch III and Senior VP/General Counsel & Chief of Staff Dan Werly will be involved in the interviews.
"We want someone who is an exceptional talent evaluator, exceptional at roster building, and someone who is an excellent decision-maker," Strunk said in recent interview. "I also want someone who is a collaborator, someone who is able to find and build consensus to get to the best answers for the team, someone who is open to innovation and evaluating talent beyond the traditional avenues. Just really a talented person in all areas. But more than anything I want someone that can collaborate – that is super important to me, being able to find this person who can collaborate so we're all working together, rowing the same direction.
"I am excited about the process, and I am excited about finding the right person. I think this is going to be a great reset for us going forward, a chance to bring in new ideas, a new way of doing things."


My love language is Portuguese.
I know, I know. There are 5 love languages and everyone has a primary one. But honestly, I need different things at different times. It hasn't rung completely true for me. So my love language probably seems like jibberish—unrecognizable and illegible the majority of the time. Kindness and patience always work. When in doubt, use those tools.
"Put each other first" is easier said than done.
Donny and I are pretty good about taking a few trips here and there. We go to Notre Dame games, take kid-free vacations. But on the daily, putting each other first seems almost laughable. How do you put each other first when you're both trying to get ready for work and there's a naked 3 year old face down throwing a tantrum while you're feeding the baby a bottle and listening to the 6 year old whine about how soggy her cereal is? We put each other first by helping each other survive. We make time and space for each other away from the daily routine because within it there isn't much to spare.
Communication is so important in marriage, and you hear it all the time. But the weird part is that you have to communicate things you thought were just understood. See #4.
Assumptions are the devil's work.
Learning to live with someone who grew up differently than you did is hard! It's easy to just assume that on Sundays you'll go to church and your husband will mop the floors, or that Tater Tot Casserole will be part of the dinner rotation (say what!?). Those are really small, minor, non-deal-breaking examples but even the little stuff builds up over time. Say what you want or need before it makes you angry. Never assume your spouse can read your mind.
When it's hardest to love, love harder.
This one goes for pretty much all things in life. Usually when things get hard its because you're growing. Either you or your spouse is growing personally or professionally or you're all going through the natural growing pains of life, like buying a house or adding a child. Regardless, when you feel like you don't have an ounce of energy/affection/kindness/support to give, give it anyway. You will be rewarded ten-fold.
Treat each other the way you want to be treated, not the way you feel they deserve to be treated.
Forgiveness is not about the past.
Apologies are about the past. However, forgiveness is about the future. Forgiveness is a promise to trust your partner to do things right the next time. That you won't hold it over their head. That you believe they will do better, and that they don't have to prove it. That took me a while to learn.
Keep arguments about today. Drop the always, nevers, evers and ….ests.
Nothing makes you want to run straight through a wall faster than hearing, "You always forget to empty the pant pockets before you do laundry," when you mostly always remember, but had just got done cleaning poop out of the bathtub before starting this particular cycle. Amirite?
Say, "Hey, you must have forgot to empty the pant pockets today." And boom, no Megan-sized hole through the wall.
Filter the advice you are given.
There is so much advice that comes from so many different people and places. Don't let advice turn into expectations that turn into disappointment if they're not properly communicated. Talk about advice you're given with your spouse, and decide what works for you.
On to the next 8!
Damn, you learned all that in just 8 years? I want to copy off you on my next text!


Whether they are sending snaps or tweets, teens spend hours on social media. While you might only think of the negative effects that social media can have on teens, there are several positive effects as well. Look at the different ways that social media can affect teens and their relationships with peers.
Social media isn't all bad for teens. In many ways, social media can be a great outlet for students to stay connected with one another and share their feelings when they are having a hard day. Their online friends can also be a great support system for them when they are going through a tough time. While it might sound amazing, it also has negative effects on teens' health. Not only can it affect their mental health but bullying become much easier hiding behind a keyboard. While the bully is faceless, the words are just as hurtful and have the same effect. Before going all out on social media, it is important to explore both the beneficial and the ugly of your favorite sites like Instagram, Facebook, Snapchat, Twitter, etc.
There is a reason most kids on school campuses today can be found with their nose in their smartphone. They are checking their feeds, messaging their friends or just laughing at a funny snap. Whether you are shy or outgoing, Snapchat and Instagram might be your favorite go to places to keep connected with friends both near and far. And it isn't just about staying connected, social media has a lot of different benefits for teens.
When you think of social media, cyberbullying might be the first thing that pops into your head. However, surprisingly research shows that social media can actually help to strengthen friendships for teens. A study by Common Sense Media showed that 52 percent of teens thought that their friendships were improved by social media and 30 percent said it improves their confidence. This makes sense since social media gives you easy access to your friends. Not only can you talk to one friend, but you can have a group chat or just virtually hang out.
Sometimes this world is lonely. Maybe you are fighting with your bestie or just having a hard time connecting with people in school, social media can help isolated or lonely teens. According to PyschCentral, lonely teens turn to social media like Facebook and Snapchat to connect with friends. A study also showed that social media can help to curb loneliness overtime and improve mental, emotional and social well-being in some teens. Additionally, those that are more introverted might not be as cautious on social media and relate to their peers more.
When you are having a bad day, sometimes a virtual hug is the next best thing to the real deal. Not only that but with a few simple clicks of the keys you can share your bad day with your friends. This can help them to understand and relate to you about problems maybe they didn't even know existed. According to a study by Pew Research Center, 7 out of 10 teens feel that they get support from friends over social media when they are having a tough day. This happens more among girls at 73 percent than among boys at 63 percent.
Writing is writing. While social media writing is informal writing, these sites do get kids writing, which is important to communication development. And some teens get creative with their writing by creating poetry, memes, etc. that they share with their friends through sites like Instagram and Snapchat. Writing and communication don't just encompass academic writing. Texts and tweets help teens to find their inner voice, according to Edutopia.
Gone are the days when you would send a friend in France a letter through snail mail. The emergence of social media lets you connect with teens all over the world in a few clicks. Not only does social media allow you to connect with kids across states but you can gain friends from another country. And Google Translate can ensure that you can semi-understand one another.
Social media like Pinterest and Instagram can open the door to creative outlets for teens. For example, a 16-year-old art student might share her art to gain feedback or they might create a digital piece. An aspiring writer might share her words through unique tweets. The opportunities for teens on social media to express their creativity is endless, and it will be viewed by all their friends.
It isn't all just lollipops and rainbows in the social media world. When a teen logs on to their account, there are some very serious negative side effects that they could be exposed to. Not only are cyberbullies more aggressive but social media can affect your mental and emotional health. Learn some pitfalls of your favorite social media sites.
While the statistics aren't conclusive, many studies show that there is a correlation between the increase in suicidal thoughts and depression in teens and social media. One study points out how depression is on the rise and one of the main changes between teens now and teens 10 years ago is social media and cell phones. Many researchers hypothesize that social media connections don't allow teens to make the deep connections that only face-to-face transactions can stimulate. Additionally, anxiety and stress can be exacerbated by social media. One wrong tweet and millions of cyberbullies can attack.
One of the greatest forms of social media abuse for teens is cyberbullying. Statistics show that nearly half of young people have been on the receiving end of online bullies. Instagram was a big culprit with a whopping 42 percent bully rate. Facebook came in a close second at 37 percent with Snapchat trailed at 31 percent. With nearly three-quarters of kids worrying about being bullied, this is a real problem on social media. In addition to bullying, social media also increase the instances of peer pressure for kids to do what is cool or trending.
With kids spending so much time online on social media sites, it isn't surprising that teens are becoming addicted. Teens have a need to answer that message or complete their streaks for the day. And not doing so can be nearly the end of the world. With teens spending as much as 9 hours a day on social media, it is easy to see how addiction to social connections can happen.
Social media exposes teens and tweens to unrealistic standards from not only ads but their friends. With beauty filters that can make your eyes bigger and your skin clearer along with the right angles, any teen can be a supermodel. But this isn't real life. Teens that see this on social media can start to have unrealistic expectations for themselves that can lead to self-esteem issues with an unhealthy ideal body image. The personas that they create that are different from their real selves can also lead to anxiety and self-esteem issues.
Many professionals point out that social media communication has replaced face-to-face interaction and changed grammar and syntax through shortened versions and acronyms. The lack of communication can hinder a teen's ability to read body language and engage in a meaningful conversation away from a screen. It can also hinder their ability to form meaningful relationships in adulthood as well.
Not only can social media open the door for predators, but it can create a false sense of security for some teens. Since they only have people on their friends' list, they might share more information than they would share on a chat room. But the problem is that many of their "friends" they don't truly know. For example, the average teen Facebook user has 300 friends that can see and share their information. With only 60 percent keeping their page private, teens can be found by child predators and lured by human traffickers.
Social media is a powerful tool to connect teens with friends and family. Not only can they find the support they need but make friends around the world. However, social media can affect teens self-esteem and mental health because of the unrealistic expectations found online. After learning the pros and cons, make your own decision about whether Facebook is good or bad for you.