text:
Q: Extracting files from merge module All I want is a command-line tool that can extract files from a merge module (.msm) onto disk.  Said differently, I want the same "administrative install" functionality that is possible for an MSI:
msiexec /a myProduct.msi TARGETDIR="C:\myInstallation" /qn
The above only works on an msi (near as I can tell).  So to get the same effect for a merge module, I'm trying msidb.exe and orca.exe  The documentation for orca states:

Many merge module options can be
  specified from the command line...
Extracting Files from a Merge Module
Orca supports three different methods
  for extracting files contained in a
  merge module. Orca can extract the
  individual CAB file, extract the files
  into a module tree and extract the
  files into a source image once it has
  been merged into a target database...
Extracting Files
To extract the individual files from a
  merge module, use the
... -x  ... option on the
  command line, where  is the
  desired path to the new directory
  tree.
The specified path is used as the root
  path for the extracted files. All
  files are extracted from the CAB file
  embedded in the module and placed in
  the specified path. The directory
  layout for the extracted files is
  based on the directory tree of the
  merge module.

It sounds like what I need.  But when I try it, orca simply opens up an editor (with info on the msm I specified) and then does nothing.  I've tried a variety of command lines, usually starting with this:
orca -x theDirectory theModule.msm
I use "theDirectory" as whatever empty folder I want.  Like I said - it didn't do anything.
Then I tried msidb, where a couple of attempts I've made look like this:
msidb -d theModule.msm -w {storage}
msidb -d theModule.msm -x MergeModule.CABinet
In the first case, I don't know what to put for {storage}.  In the second case, it turns out that the literal string "MergeModule.CABinet" is necessary (it is a reserved name).  However, the extracted cabinet does not preserve the file hierarchy or "normal" file names; so I can't use it for my purposes.
Can someone explain what I'm doing wrong with the command line options?  Is there any other tool that can do this?

A: I just had to do this by creating a blank msi and then use Orca to attempt to merge the module into my msi and then extract the files.

*

*Create a blank .msi. I used WiX 3.6 to create the .msi and below is the minimal source. I named it "blank.msi".
<?xml version="1.0" encoding="UTF-8"?>
<Wix xmlns="http://schemas.microsoft.com/wix/2006/wi">
    <Product Id="*" Name="blank" Language="1033" Version="1.0.0.0" Manufacturer="blank" UpgradeCode="298878d0-5e7b-4b2e-84f9-45bb66541b10">
        <Package InstallerVersion="200" Compressed="yes" InstallScope="perMachine" />

        <MediaTemplate />

        <Directory Id="TARGETDIR" Name="SourceDir">
            <Directory Id="ProgramFilesFolder"/>
        </Directory>

        <ComponentGroup Id="ProductComponents" Directory="ProgramFilesFolder" />

        <Feature Id="ProductFeature" Title="blank" Level="1">
            <ComponentGroupRef Id="ProductComponents" />
        </Feature>
     </Product>
</Wix>

*Use Orca to extract the files from the merge module.
orca -m "myModule.msm" -f ProductFeature -x .\xdir blank.msi

The files will be extracted to the directory specified by the -x parameter (in this case .\xdir).
Note that the value for the -f parameter "ProductFeature" matches the name of the feature specified in msi file above.

A: You can use the decompiler tool included with WiX (called Dark) to decompile the merge module and extract the files:
dark.exe myMergeModule.msm -x "path_to_extracted_files"

The files will get extraced to the path specified in the -x parameter.
Note: The files will get extracted using the names specified in the File table of the installation database, which may not actually be the file names used when the files actually get installed. If you need extract the files using the actual file names, see my other answer to this question: Extracting files from merge module

A: The DeploymentToolsFoundation class library in WiX, has an InstallPackage class with an ExtractFiles() method that should do just what you want, but fails for Merge Modules. This appears to be a bug.
The following PowerShell script, which uses DTF to access the CAB in the mergemodule, should do what you want. Apologies if the scripting is a bit wonky, I'm new to PowerShell.
[Reflection.Assembly]::LoadFrom("[InsertPath]\Microsoft.Deployment.WindowsInstaller.dll")

function ExtractMSM([string]$file, [string]$targetDir)
{
    write-host "Extracting files from merge module: "$file

    if(![IO.Directory]::Exists($targetDir)) { new-item -type directory -path $targetDir }

    $cabFile = join-path $targetDir "temp.cab"
    if([IO.File]::Exists($cabFile)) { remove-item $cabFile }

    $db = new-object Microsoft.Deployment.WindowsInstaller.DataBase($file, [Microsoft.Deployment.WindowsInstaller.DataBaseOpenMode]::ReadOnly)
    $view = $db.OpenView("SELECT `Name`,`Data` FROM _Streams WHERE `Name`= 'MergeModule.CABinet'")
    $view.Execute()
    $record = $view.Fetch()
    $record.GetStream(2, $cabFile)
    $view.Dispose()

    expand -F:* $cabFile $targetDir

    remove-item $cabFile

    $extractedFiles = get-childitem $targetDir
    $hashFiles = @{}
    foreach($extracted in $extractedFiles)
    {
        try
        {
            $longName = $db.ExecuteScalar("SELECT `FileName` FROM `File` WHERE `File`='{0}'", $extracted.Name)
        }
        catch
        {
            write-host "$($extracted.Name) is not in the MSM file"
        }

        if($longName)
        {
            $longName = $LongName.SubString($LongName.IndexOf("|") + 1)
            Write-host $longName

            #There are duplicates in the
            if($hashFiles.Contains($longName))
            {
                write-host "Removing duplicate of $longName"
                remove-item $extracted.FullName
            }
            else
            {
                write-host "Rename $($extracted.Name) to $longName"
                $hashFiles[$longName] = $extracted
                $targetFilePath = join-path $targetDir $longName
                if([IO.File]::Exists($targetFilePath)) {remove-item $targetFilePath}
                rename-item $extracted.FullName -NewName $longName
            }
        }
    }
    $db.Dispose()
}

A: I had a similar problem, but I went at it from a different direction.
I installed InstallSheild Express that came with an earlier version of Visual Studio, created a new project, but I only added the MSM file that I required.
After compiling and running my new install I was able to retrieve the files that the MSM file contained.

A: MSI2XML

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text:
openGlobalRights-openpage
Human rights evaluation—who is it really for?
The human rights community should embrace evaluation not for our donors, but for our beneficiaries. A contribution to the openGlobalRights debate on evaluation and human rights. Español
Claire Thomas
Although evaluations are often undertaken at the request of donors or as part of donor driven proposals, is that the only reason to conduct evaluations? As Emma Naughton and Kevin Kelpin point out, though quantifiable results may matter for donors, it is the assessment of the journey that matters equally if not more to those doing the work. And in the end, isn't that work really being done for the beneficiaries, and not the donors?
Beneficiaries (or more widely the communities affected by our work or their representatives) have a right to know what we tried to do on their behalf and whether we made a difference. If yes, what brought that about? And if no, (or not yet), why not? Should we have approached things differently? Beneficiaries clearly have less power than donors, which makes it feel like all the pressure for evaluation comes from donors—in the end project evaluations do not always involve and are not always shared with beneficiaries. But what happens when we have an entire evaluation and decision-making process that doesn't include the very people we are trying to help?
What happens when we have an entire evaluation and decision-making process that doesn't include the very people we are trying to help? A second important audience is made up of activists, staff, board members, members, volunteers, our peers and colleagues, and the wider human rights community. We also want to know if we made a real difference. We want to know which methods work, under which circumstances and why. We need this information to intervene effectively in the future and to know that all the risks have been worthwhile. Evaluations can feel risky to people working on human rights, because such processes question whether we have done the right things in the right ways. This can sometimes be demoralising to staff who have worked hard "at the coalface" and who may, at times, lose sight of the bigger picture.
In the worst-case scenario, evaluations can show that time and efforts have not made any difference (yet). But this knowledge of non-progress is just as important, and both processes and final results count in human rights work. Even though evaluation audiences may not always agree on what to measure, and although long-term social changes may not be achieved at the end of a specific project, small steps along the way can provide useful indications of progress.
Of course, donors and all those who provide support have a right to know what we did with the resources they provided. They also want to know if we have made a difference at all to the situation we were targeting. Almost all donors need evaluations to satisfy the needs of other audiences (beneficiaries, staff, etc.) and many will enter into an intelligent and constructive discussion about different evaluation methods that fit the programme and its constraints.
Although all three of these audiences are interested in what difference has been made, donors are more interested in concrete measurable results and proven successes. Within human rights organisations, for our own learning, we may be as interested in why things worked, or not, as in proving exactly how much they worked. We may also be more patient, being willing to work for ten years to see a real change emerge.
Flickr/Rainforest Action Network (Some rights reserved)
The human rights community "should embrace evaluation for our beneficiaries, on whose behalf we all work."
Beneficiaries' evaluation interests, on the other hand, vary greatly. Some are concerned only that their issue has been voiced and heard. Others want to know that everything that can be done is being done to try to resolve or react to ongoing human rights abuses affecting them. Great strides have been made in participatory evaluation methods, involving beneficiaries of programmes in gathering and analysing feedback about them. As previously noted in this debate, some human rights contexts are more difficult than some development contexts where these methods have mostly been applied. The individuals or groups of people on whose behalf human rights work takes place may be in incommunicado detention, or they may be at very great daily risk of physical attack or disappearance. Those working in governance to hold officials accountable for corruption face similar risks and threats. In addition, people working in gender issues gather views of women experiencing domestic violence or rape, which raises very similar challenges.
So if the human rights community is still resistant to evaluation solely for donors' benefit, we should embrace evaluation for our beneficiaries, on whose behalf we all work. Human rights work is not just done to meet an international norm, system or standard. Human rights are useful, ultimately, because they make peoples' lives a little better in myriad ways. We should be creative in finding ways to identify beneficiaries or those who could speak for them. We should also survey those in our intervention areas who did not benefit as well as those who did, making sure that we are not unknowingly leaving groups out or organising things in ways that some people feel unable to participate. We should evaluate so we can learn what works and why, not just to put ticks on a list.
Finally, we should also consider evaluating the unintended impact of our work. What changes occurred that we did not anticipate, or that we did not want, or that someone else did not want? If we really want to evaluate our work, these are the tough questions that everyone needs to be asking.
As much as all the audience needs may differ, Minority Rights Group's experience has been that if we lead the process, donors will accept our evaluations even if they are not the method they would have chosen. Although they may have specific requirements, it is rare for donors to specify any particular method. This means that organisations can add beneficiary participation and learning elements to an evaluation that is only required by the donor to validate results. Donors rarely cut or query evaluation costs, meaning that evaluation plans can be ambitious and work intensive. Beyond this, many donors (e.g., SIDA) will ask an organisation to designate focus areas for an evaluation, and design an evaluation methodology—they will just want to check that they are happy with it. And even donors with rules will vary those rules when it is clear that the nature of the work does not fit the kind of evaluation that that donor is used to seeing. We, the human rights organisations, need to pick up this baton and run with it: if we don't start leading the evaluation process, donors' upwards accountability demands will fill the vacuum. If that happens, everyone loses—we will be left with methods developed by and for others that won't improve our work, or help our beneficiaries.
Published in: openGlobalRights-openpage
When evaluating human rights progress, focus also on the journey
Written by: Kevin Kelpin All articles by: Kevin Kelpin
Written by: Emma Naughton All articles by: Emma Naughton
Human rights and results-based management: adopting from a different world
Written by: Vincent Ploton All articles by: Vincent Ploton
Can rights organizations use low-burden self-reflection for evaluation?
Written by: Brian Root All articles by: Brian Root
UNAIDS: Bold human rights targets need better monitoring
Written by: Meg Davis All articles by: Meg Davis
Finding balance: evaluating human rights work in complex environments
Written by: Tim Ludford All articles by: Tim Ludford
Written by: Clare Doube All articles by: Clare Doube
When protecting civilians in humanitarian crises, how do we measure success?
Written by: Helen Lindley All articles by: Helen Lindley
Making a case for change: the value of strategic plausibility in evaluation
Written by: Jeremy Smith All articles by: Jeremy Smith
How does professionalization impact international human rights organizations?
Written by: Carrie Oelberger All articles by: Carrie Oelberger
Firm yet flexible: keeping human rights organisations relevant
Written by: Lucia Nader All articles by: Lucia Nader
Internationalization is about more than just advocacy
Written by: Johanna Siméant All articles by: Johanna Siméant
Evaluation and Human Rights

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text:
Exposure to aluminium may have impact on male fertility
by Keele University
New research from scientists in the UK and France suggests that human exposure to aluminium may be a significant factor in falling sperm counts and reduced male fertility.
Fluorescence microscopy using an aluminium-specific stain confirmed the presence of aluminium in semen and showed aluminium inside individual sperm.
And the team of scientists, at the universities of Lyon and Saint-Etienne in France and Keele in the UK, found that the higher the aluminium, the lower sperm count.
The research, led by Professor Christopher Exley, a leading authority on human exposure to aluminium at Keele, and Professor Michele Cottier, a specialist in cytology and histology at Saint-Etienne, measured the aluminium content of semen from 62 donors at a French clinic.
Professor Exley said: "There has been a significant decline in male fertility, including sperm count, throughout the developed world over the past several decades and previous research has linked this to environmental factors such as endocrine disruptors.
"Human exposure to aluminium has increased significantly over the same time period and our observation of significant contamination of male semen by aluminium must implicate aluminium as a potential contributor to these changes in reproductive fertility."
The mean aluminium content for all 62 donors was found to be very high at 339 ppb with the aluminium content of semen from several donors being in excess of 500 ppb. A statistically significant inverse relationship was found between the aluminium content of semen and the sperm count. Higher aluminium resulted in a lower sperm count.
Aluminium and its likely contribution to Alzheimer's disease
More information: J.P. Klein, M. Mold, L. Mery, M. Cottier, C. Exley, "Aluminium content of human semen: implications for semen quality," Reproductive Toxicology, DOI: 10.1016/j.reprotox.2014.10.001
Journal information: Reproductive Toxicology
Provided by Keele University
Citation: Exposure to aluminium may have impact on male fertility (2014, October 22) retrieved 16 January 2021 from https://medicalxpress.com/news/2014-10-exposure-aluminium-impact-male-fertility.html
Action is needed now to lower the content of aluminium in infant formulas
Humans experiencing increased exposure to aluminium and it's predicted to get worse
Elevated brain aluminium and early onset Alzheimer's disease in worker exposed to aluminium
Does aluminium cause Alzheimer's and breast cancer?
High strength cellular aluminium foam for the automotive industry


text:
\section{INTRODUCTION}

Several decades ago, \citet{BahcallSpitzer1969} postulated
that the absorption lines observed in the spectra of
distant QSOs are due to the extended gaseous halos of
intervening galaxies.  Since that time, astronomers have
identified the galaxies associated with the observed absorption \citep[e.g.,][]{Yanny1990,BergeronBoisse1991,Steidel1995} and
have used QSO spectroscopy of various rest-frame ultraviolet transitions to
constrain the
nature of baryonic processes in the outer regions of galaxies,
e.g., feedback, accretion, and cooling \citep{Mo1996,MB2004,Tobias2006}.
These transitions include Ly$\alpha$\ and \ion{Mg}{2} lines that probe cooler,
photoionized gas \citep{Wolfe1995,Bergeron1986}, and \ion{C}{4} and \ion{O}{6}
doublets that trace warmer, more diffuse material
\citep{Chen2001,Tripp2008}.
However, while the apparent brightness of QSOs
enables high
signal-to-noise, high spectral resolution datasets,
they severely outshine the galaxies projected nearby and therefore limit
follow-up analysis, especially at small impact parameters.
Furthermore, QSOs
are too rare in the sky
to probe numerous individual galaxies with
multiple sightlines.  Therefore,
constraints on the
covering fraction ($C_f$) and spatial distribution of halo gas
must be statistical \citep[e.g.,][]{Chen2001,CT2008}.

The \ion{Mg}{2} $\lambda \lambda 2796, 2803$ doublet in particular has been studied extensively, as it is easily accessible at optical wavelengths at redshifts $0.3 \lesssim z \lesssim 2.3$ and traces cool gas \citep[with temperature $\rm T \sim 10^4~K$;][]{BergeronStasinska1986} in a broad range of neutral hydrogen column densities \citep[$N($\ion{H}{1}$) = 10^{18} - 10^{22}~\rm cm^{-2}$;][]{Churchill2000,Rao2006}.  In spite of this, the physical origins of the gas giving rise to \ion{Mg}{2} absorption remain obscure.
Several studies \citep[e.g.,][]{MB2004} suggest an infall origin for this gas; for example, \citet{TC2008} present an infall model with which they reproduce the observed frequency distribution function for \ion{Mg}{2} systems as well as their clustering properties \citep{Bouche2006,Gauthier2009}.
Other studies \citep{Bond2001,Schaye2001,Bouche2006,Bouche2007,MenardChelouche2009}
suggest instead that these systems arise in gas which has been blown out of star-forming galaxies via superwinds.
In support of this latter scenario, a recent study
by \citet{Weiner2009} of \ion{Mg}{2} kinematics in coadded DEEP2 spectra of a sample of star-forming galaxies at $z \sim 1.4$  reveals frequent, perhaps even ubiquitous, outflows of cool gas.
\citet{Tremonti2007} also detect very high velocity outflows in $z \sim 0.6$ post-starburst galaxies traced by \ion{Mg}{2} absorption.  Such winds may redistribute \ion{Mg}{2} absorbing gas, possibly to a galaxy's halo, although the distances to which the winds extend remain uncertain.
In one of the only studies addressing this issue, \citet{Martin2006} observes cool outflowing gas
several kiloparsecs from the nuclei of a sample of $z \sim 0.1$ ultraluminous infrared galaxies.

In principle, galaxy spectra can also probe the halo gas of foreground galaxies along the sightline \citep[e.g.,][]{Adelberger2005,Barger2008}.  This novel technique offers several advantages over QSO-galaxy pair studies (D. Koo et al. 2009, in preparation).  The projected number density of galaxies on the sky is much greater than that of QSOs; therefore the use of galaxies can vastly increase the number of potential background probes for a given galaxy halo.  Moreover, many galaxies are extended sources which provide the opportunity to study gas along multiple lines of sight through a given foreground halo, including their own \citep[e.g.,][]{Phillips1993,Heckman2000}.  Integral Field Unit (IFU) spectrographs may then be used to study the morphology of halo absorption and the spatial distribution of outflowing gas.

Close transverse pairs of galaxies may be identified in large spectroscopic or photometric surveys so that a targeted search for foreground \ion{Mg}{2} absorption in the background galaxy spectra can be performed.
This technique has been used at $z > 1.5$ to study absorbing gas traced by transitions such as \ion{C}{4} near Lyman Break Galaxies
 by \citet{Adelberger2005}; but it has not yet been used at lower redshifts where higher resolution imaging and spectroscopy can be obtained for each galaxy.

In the process of carrying out a spectroscopic survey to measure outflow properties in galaxies at $0.3 < z < 1.4$, we identified a close transverse pair of galaxies in which the spectroscopy of the more distant object ($z = 0.6942$)
allows the detection (in absorption) of gas in the environs of a foreground
galaxy (at $z = 0.4729$ and at impact parameter $\rho = 16.5~ h_{70}^{-1} $~kpc).
This foreground absorber shows signs of recent merger activity, has a stellar
continuum consistent with that of a post-starburst galaxy, and is host
to a low-luminosity AGN.
Here we analyze the spectrum of the background galaxy to examine halo gas in the foreground system.
We discuss our observations of the galaxy pair and data reduction in \S\ref{sec.thepair}.  Analysis of the luminous components of the galaxies and the foreground halo absorption is given in \S\ref{sec.analysis}.  The possible origins of the observed cool halo gas are discussed in \S\ref{sec.discussion}, and we conclude in \S\ref{sec.conclusions}.
We adopt a $\rm \Lambda CDM$ cosmology with $h_{70} = H_0 / 70~\rm km~s^{-1}~Mpc^{-1} $, $\rm \Omega_M = 0.3$, and $\rm \Omega_{\Lambda} = 0.7$.  Where it is not explicitly written, we assume $h_{70} = 1$.  Magnitudes quoted are in the AB system.

\section{THE GALAXY PAIR}\label{sec.thepair}

Our targeted galaxy pair is located in the GOODS-N field \citep[Great Observatories Origins Survey;][]{Giavalisco2004} and has been imaged by the HST Advanced Camera for Surveys in 4 optical bands (F435W, F606W, F775W and F850LP, or $B_{435}$, $V_{606}$, $i_{775}$ and $z_{850}$).  Galaxy properties derived in previous studies and references are given in Table~\ref{tab.photinfo}.

We obtained spectroscopy of both galaxies using the Low Resolution Imaging Spectrometer (LRIS) on Keck 1 \citep{Cohen1994} on 2008 May 30-31 UT.  We used the $\rm 600~ l~mm^{-1}$ grism blazed at 4000~\AA~on the blue side and the $\rm 600~ l~mm^{-1}$ grating blazed at 7500~\AA~on the red side with the D560 dichroic.  This setup affords a FWHM resolution ranging between $400~\rm km~s^{-1}$  and $180~\rm km~s^{-1}$ and wavelength coverage between $\sim 3200$~\AA~ and $\sim 7600-8000$~\AA.  Two sets of spectra were obtained.  We first used a slitmask to place a $0.9\arcsec$ slitlet across the center of the background galaxy oriented NE and collected $6 \times \sim 1800\rm~ sec$ exposures with FWHM $\sim 0.6\arcsec$ seeing.  We also placed a $1\arcsec$-wide longslit across both galaxies and obtained $2 \times 1000\rm~ sec$ exposures with $\sim 1\arcsec$ seeing (see Figure~\ref{fig.im}).

The data were reduced using the XIDL LowRedux\footnote{http://www.ucolick.org/$\sim$xavier/LowRedux/} data reduction pipeline.  The pipeline includes bias subtraction and flat-fielding, slit finding,
wavelength calibration, object identification, sky subtraction, cosmic ray rejection, and flux calibration.  Vacuum and heliocentric corrections were applied.  Because the separation between the galaxies is only 2.8\arcsec, we used a spatially narrow Gaussian centered on the foreground object to weight the extracted spectrum (with $\rm FWHM \sim 0.54\arcsec$ and $0.75\arcsec$ for the blue and red sides, respectively).  This limits contamination of the foreground spectrum by emission from the background object to $< 2\%$.  Using a wider extraction window ($\rm FWHM \sim 1.8\arcsec$) does slightly change the equivalent widths (EWs) of absorption lines (e.g., H9, \ion{Ca}{2}) measured for the foreground galaxy, but it does not affect the results of our stellar population modeling (discussed in \S\ref{sec.fg}).

We derive redshifts for the two galaxies using IDL code adapted for use in the DEEP2 survey \citep[S. Faber et al. 2009, in preparation;][]{Coil2004} from the publicly available programs developed for the SDSS.\footnote{$\rm http://spectro.princeton.edu/idlspec2d\_install.html$}  In brief, this code calculates the minimum $\chi^2$ value
as a function of the lag between an observed spectrum and a linear combination of three templates.  One template is an artificial emission line spectrum with lines broadened for consistency with an instrumental resolution of $\rm FWHM \sim 235~\rm km~s^{-1}$, one is the coadded spectrum of thousands of absorption-line dominated galaxies \citep{Eisenstein2003}, and one is an A star spectrum.  The spectral region which includes interstellar UV absorption lines was not used to constrain the fits.  Each galaxy redshift has also been confirmed by eye.  We find that the redshifts of the background and foreground galaxies are $z=0.694248 \pm 0.000001$ and $z=0.47285 \pm 0.00002$, respectively.  The errors are the formal $1\sigma$ uncertainties in the fitted values.  These redshifts are within $\lesssim 92~\rm km~s^{-1}$ of the redshifts obtained in the Team Keck Treasury Redshift Survey \citep[TKRS;][]{Wirth2004} for these objects.  We define the systemic velocity of each galaxy to be at the corresponding fitted redshift.

Figures~\ref{fig.im} and~\ref{fig.fullspec} show HST imaging of the galaxy pair and our  LRIS spectrum of the background galaxy, respectively.  UV absorption lines in the rest-frame of the background object are marked in red and are offset to negative velocity from systemic, indicating the presence of an outflow.
Emission due to \ion{Mg}{2}, as well as emission near the \ion{Fe}{2} absorption lines, is also evident.
The same lines in absorption are marked at the systemic velocity of the foreground galaxy in blue; these marks coincide with strong absorption in the spectrum, and are presumably due to gas associated with
the $z=0.4729$ foreground galaxy.

We measured EWs of absorption and emission features after normalizing the spectra to the continuum level.  This level was determined via a linear fit to the continuum around each feature of interest.  We selected different continuum regions for each transition with widths between 8 \AA\ and 72 \AA.
We used a feature-finding code described in \citet{Cooksey2008} to identify and measure the boxcar EW in both emission and absorption lines with $\rm EW / \sigma_{EW} \ge 3$
(Table~\ref{tab.ew}).
The foreground galaxy halo/disk absorption has rest equivalent width $W_r (2796) = 3.93 \pm 0.08$ \AA \ and is classified as an ``ultrastrong" \ion{Mg}{2} absorber \citep{Nestor2007}.  $W_r (2796)$ values this large are rare in surveys of \ion{Mg}{2} absorption in QSO
sightlines; e.g., absorbers with $W_r (2796) > 3.5$ \AA \ make up only 3\% of the population of all absorbers with $W_r(2796) > 1$ \AA \ \citep{Prochter2006}.  Although the number of known galaxy-QSO absorber pairs with impact parameters less than $ 20~\rm kpc$ is quite small \citep[$\sim 30$ from][]  {Bouche2007,Kacprzak2007,Churchill2005intermediatez,Steidel1995}, only two of these have $W_r (2796) > 3.5$ \AA.  (We are not including the  galaxy-absorber pairs from the sample of \citet{Nestor2007} here, as they lack spectroscopic confirmation of the redshifts of the associated galaxies.)  This system also exhibits $W_r (3935) \sim 1$ \AA \ and is classified as a ``strong" ($W_r (3935) > 0.5$ \AA) \ion{Ca}{2} absorber  \citep{Wild2006}.  The $W_r (3935)$ of this halo/disk gas is among the largest measured for the absorbers in the \citet{Wild2006} study.

We find no evidence of emission (e.g., [\ion{O}{2}] $\lambda \lambda 3727, 3729$) due to another galaxy at the redshift of the foreground absorber in either the slitmask or the longslit spectrum.  Furthermore, the other objects identified in the HST image are significantly fainter and lie at larger impact parameters than the previously identified foreground galaxy.  We conclude that the foreground absorption is associated with this galaxy located at $\rho = 16.5~ h_{70}^{-1} \rm~kpc$ from the center of the background galaxy, where the center is determined from quantitative morphological analysis of the $i_{775}$-band image by J. Lotz (2008, private communication), using the method described in \citet{Lotz2004,Lotz2006}.

\begin{figure*}[ht]
\begin{center}
\includegraphics[width=6in]{f1_both.eps}
\caption{{\it (Left)} Color image of the galaxy pair in the HST/ACS
$B_{435}$, $V_{606}$ and $i_{775}$ bands.  TKRS4389 is to the southeast in the image and marked with a ``B"; TKRS4259 is to the northwest and marked with an ``F".  These galaxies are offset by an impact parameter of 2.8\arcsec; i.e., $16.5~h_{70}^{-1}~ \rm kpc$ at the foreground redshift.  {\it (Right)}
Same images as on the left, convolved with a $\rm FWHM = 0.8\arcsec$ Gaussian to simulate the effects of seeing.  The orientations of the slitlet used to obtain the $2.9$ hour spectrum (position angle $\sim 45^{\circ}$ East of North) and the longslit used to obtain the 33 minute spectrum (position angle $\sim 110^{\circ}$ East of North) are shown in white solid and dashed lines, respectively.  The position of the slitlet through B was obtained from the TKRS astrometry.  The position of the longslit was inferred by assuming the position angle given in the LRIS image header, convolving the HST $V_{606}$-band image with the seeing disk, and adjusting the slit position on the convolved image until the spatial profile best matched the profiles actually observed in the LRIS longslit between 5500 and 7100 \AA.
\label{fig.im}}
\end{center}
\end{figure*}

\begin{figure*}[ht]
\begin{center}
\includegraphics[width=3.in,angle=90]{f2.eps}
\caption{Keck/LRIS spectrum (unsmoothed) obtained with our slitlet observations (with orientation shown with the solid lines in Figure~\ref{fig.im}) of the background galaxy. This galaxy exhibits \ion{Mg}{2}, \ion{Mg}{1} and \ion{Fe}{2} absorption offset by $\sim \rm -300~ km~s^{-1}$ from systemic velocity (shown in red), indicating an outflow of cool gas.  \ion{Fe}{2} fine-structure transitions at the systemic velocity of the background galaxy are marked above the spectrum with short vertical red lines.  The green line at  flux levels $\approx 0.1\sci{-17} \rm erg~s^{-1}~cm^{-2}~\AA^{-1}$ shows the $1\sigma$ error in each pixel.
Strong \ion{Mg}{2}, \ion{Mg}{1} and \ion{Fe}{2} absorption features from the foreground
galaxy are shown in blue.
\label{fig.fullspec}}
\end{center}
\end{figure*}

\section{ANALYSIS OF THE GALAXIES}\label{sec.analysis}

\subsection{TKRS4389 (Background Galaxy)}\label{sec.bg}
The background galaxy is one of the brightest galaxies in the $B_{435}$-band
in the TKRS \citep{Wirth2004} at its redshift
and is among the bluest objects in the ``blue cloud" in the galaxy
color-magnitude diagram (CMD), as shown in the left panel of Figure~\ref{fig.cmd}.
We derive a star formation rate (SFR) of $\sim 80\rm~M_{\odot}~yr^{-1}$ using
the luminosity of the H$\beta$ line measured in \citet{Weiner2007} and
assuming a \citet{CharlotFall2000} dust attenuation curve with effective V-band optical depth $\tau_V \sim 1.5$
as derived from the stellar population modeling discussed below.  We assume case B recombination to
calculate an H$\alpha$ luminosity and apply the calibration of \citet{Kennicutt1998} to convert this to SFR.
\citet{KK2004} measure an oxygen abundance of $\rm 12 + log(O/H) = 8.76 \pm 0.15$, close to
the solar abundance value of 8.72.
Our LRIS spectrum reveals a weak [\ion{Ne}{5}] $\lambda 3426$ emission line, which indicates the
object is host to an AGN \citep[e.g.,][]{Ho2008}.  AGN activity may therefore affect the SFR estimate and the estimate of the oxygen abundance.  Because the [\ion{Ne}{5}] emission is weak, a Gaussian fit to the line profile results in a rest-frame dispersion of $125 \pm 40~\rm km~s^{-1}$; this value is within $\sim 0.8\sigma$ of the instrumental velocity dispersion at this wavelength.  (All other velocity dispersions reported are calculated by performing a nonlinear least-squares fit of a Gaussian to the appropriate emission line and its surrounding continuum and subtracting the instrumental velocity dispersion from the fitted Gaussian $\sigma$ in quadrature.  Continuum regions were chosen to extend at least 7 \AA \ from line center.)  We also observe strong \ion{Mg}{2} emission
that results in a P-Cygni line-profile (Figure~\ref{fig.fullspec}), as well as
a series of emission features near the \ion{Fe}{2}
resonance lines which we identify as fine-structure transitions from excited states of \ion{Fe}{2}.  To our knowledge, this is the first reported case of
\emph{narrow} fine-structure \ion{Fe}{2} emission from any extragalactic object.
These emission features may be related to AGN activity, but perhaps could be attributed to
some other physical mechanism.  Their origin will be discussed in a future work.

To estimate the contribution of the AGN to the continuum emission,
we used \citet{BC2003} stellar population synthesis models to generate a grid
of synthetic starburst galaxy spectra.  All models include an old stellar population, specifically a 7 Gyr-old single-burst stellar population (SSP7) with solar metallicity, and
the stellar population of an 100 Myr-old ongoing burst with constant star formation rate.
These particular choices of old and bursting stellar populations are motivated by \citet{Yan2006}, who use them to identify post-starburst galaxies via stellar population modeling.

To each of these spectra, we add
a featureless power-law continuum with a variable normalization to model
the AGN contribution to the galaxy continuum.  We also allow for a variable amount of dust attenuation, parametrized by $\tau_V$.  (Details of the fitting are discussed in \S\ref{sec.fg} and K. Rubin et al. 2009, in preparation.)
The spectrum is fit well by models with a range in $\tau_V \sim 1.5 - 1.7$ that combine
a strong starburst
with a power-law component that
contributes less than 30\% of the emission at 4200 \AA \ in the rest frame.
We conclude that the continuum emission is consistent with a galaxy spectrum that is dominated by intense star formation, rather than
AGN activity.

Because of its high surface brightness and strong continuum
blueward of observed wavelength $\rm \lambda_{obs} \sim 5000$ \AA,
this galaxy is an excellent and rare candidate for
probing gas in foreground halos.  At the same time, its spectrum
may be used to probe cool gas (via low-ionization absorption) associated with its own ISM and halo but foreground
to its bright star-forming regions.  As noted previously (see \S\ref{sec.thepair}),
the spectrum of TKRS4389 exhibits evidence for a substantial outflow of cool gas.
A quantitative analysis of the outflow properties (e.g., velocity, $C_f$,
limits on the outflow column density, and mass outflow rate) of a large sample of galaxies including this one will be
undertaken by K. Rubin et al. (2009, in preparation).

\begin{figure}[ht]
\begin{center}
\includegraphics[width=1.8in,angle=90]{f3.eps}
\caption{$U-B$ vs.\ $M_B$ for TKRS galaxies with $0.60 < z < 0.80$ (left-hand panel) and $0.37 < z < 0.57$ (right-hand panel).  Background (TKRS4389) and foreground (TKRS4259) galaxies are marked with a large circle and square, respectively.  The solid line divides the ``red sequence" from the ``blue cloud" as given in \protect \citet{Willmer2006}.  The foreground galaxy lies in the so-called ``green valley" and may evolve to the bright end of the red sequence \protect \citep[e.g.,][]{Faber2007}. \label{fig.cmd}}
\end{center}
\end{figure}

\begin{figure}
\includegraphics[width=2.in,angle=90]{f4.eps}
\caption{Spectrum of the foreground galaxy smoothed over 7 pixels (black)
and the smoothed post-starburst model spectrum which yields the best fit (with $A = 4$
and $t_{burst} = 1.0\rm~Gyr$; red).  The smoothed error values in the data are shown with the dotted line.
Emission lines and the central regions of Balmer absorption lines
in the galaxy spectrum were masked out prior
to fitting (masked regions are shown in green), as the model
spectra do not include line emission from AGN or \ion{H}{2} regions.   Bad pixels are also masked out.  Models with 600\,Myr $\leq t_{burst} \leq$ 1.4\,Gyr successfully reproduce the strong Balmer, \ion{Ca}{2} K and G band absorption in the data.  \label{fig.specmodel}}
\end{figure}

\begin{figure}[ht]
\begin{center}
\includegraphics[width=4.in,angle=90]{f5.eps}
\caption{UV absorption lines due to the foreground halo in the spectrum of the background galaxy at a distance of $16.5~ h_{70}^{-1}$ kpc.  The systemic velocity is marked with vertical dotted lines.  The dashed line marks the continuum level.  The rest EW of \ion{Mg}{2} $\lambda 2796$ absorption due to the foreground halo is $3.93 \pm 0.08$ \AA.  We note that these absorption profiles are asymmetric about the deepest part of each line.  The \ion{Mg}{2} lines are heavily saturated (see \S\ref{sec.psb_scenario}) and have depths of $\sim 20$\% of the continuum level.  This is indicative of a $C_f$ for \ion{Mg}{2} absorbing clouds of $\gtrsim 0.8$.  \label{fig.fgspecstamps}}
\end{center}
\end{figure}

\subsection{TKRS4259 (Foreground Galaxy)}\label{sec.fg}
The proximity of this galaxy pair allows us to analyze the halo properties
of the foreground galaxy at an impact parameter of $16.5~ h_{70}^{-1}$ kpc.  To
understand these properties in context, we
first present an analysis of the luminous components of the foreground galaxy.

TKRS4259 is a massive ($\rm \log M_*/M_{\odot} = 11.15 \pm 0.08$, where $\rm M_*$ is the stellar mass; \citealt{Bundy2005}), relatively luminous galaxy, located in the ``green valley" between the red sequence and the blue cloud in the $U-B$ vs.\ $M_B$ CMD \citep[Figure~\ref{fig.cmd};][]{Willmer2006}.
Although a Gini/M20 analysis (J. Lotz, 2008, private communication)
indicates TKRS4259  is an early-type galaxy, it shows signs of a
disturbed morphology or dust lane in
all of the HST/ACS bands
(i.e., a low surface brightness tidal feature; Figure~\ref{fig.im}).
Both its location in the CMD and its morphology indicate the galaxy
may be transitioning from a previously star-forming galaxy to a fully quenched object.
TKRS galaxies of similar $M_B$ and redshift have approximately solar
oxygen abundance or greater \citep{KK2004}.

The [\ion{O}{2}], $\rm H\beta$, and [\ion{O}{3}] emission-line luminosities
for this galaxy were measured by \citet{Weiner2007} and are included in Table~\ref{tab.photinfo}.
We also detect narrow [\ion{Ne}{5}] $\lambda 3426$ emission with rest-frame velocity dispersion $143 \pm 55\rm~km~s^{-1}$
(see Table~\ref{tab.ew}), indicating this galaxy hosts an AGN.
Before calculating a SFR based on the $\rm H\beta$ or [\ion{O}{2}] luminosities, we investigate the possible AGN contribution to this lower ionization line emission.  The line luminosity ratio [\ion{O}{3}]$\rm /H\beta \sim 2.3$; the galaxy falls just below the [\ion{O}{3}]$\rm /H\beta = 3.0$ ratio dividing LINERs (at lower values) and Seyferts (at higher values) in the system of spectral classification described in, e.g., \citet{BPT1981},  \citet{VeilleuxOsterbrock1987} and \citet{Veilleux1995}.
Unfortunately, we do not have spectral coverage of [\ion{N}{2}] and $\rm H\alpha$ and
cannot strictly classify this galaxy as a LINER.
However, because [\ion{N}{2}]/H$\alpha$ is correlated with
metallicity in star-forming galaxies, and because there is a tight relation
between mass and metallicity in these objects \cite[e.g.,][]{Tremonti2004},
we may use $\rm M_*$ as a proxy for [\ion{N}{2}]/H$\alpha$.  This is demonstrated in Figure 2 of \citet{Weiner2007},
which shows a correlation between absolute $H$-band magnitude and both [\ion{N}{2}]/H$\alpha$ and [\ion{O}{3}]/H$\beta$
in blue cloud galaxies.
Our foreground galaxy lies
far from the locus of star-forming galaxies in [\ion{O}{3}]/H$\beta$ - $\rm M_*$ space, with a $\rm M_* \gtrsim 20$ times higher than in
galaxies with similar [\ion{O}{3}]/H$\beta$ ratios in the TKRS.
It also satisfies the AGN criterion of R. Yan et al. (2009, in preparation), who find that $U-B$ color
can serve as a proxy for [\ion{N}{2}]/H$\alpha$ as well.
We conclude that LINER or AGN activity dominates the observed line emission.
In addition, \citet{Ptak2007} measure an X-ray luminosity of
$\rm log~L_X = 40.83~(erg~s^{-1})$ for this object.  This luminosity is low enough to be produced by star formation; however, based on our analysis of the optical spectrum, we attribute the X-ray emission to weak AGN activity.

\subsubsection{Ongoing Starburst Scenario}
We cannot, however, rule out ongoing star formation based on this analysis alone.
The upper limit on the SFR assuming all $\rm H\beta$ emission is due to star formation (and assuming the largest $\tau_V$ from the range derived from stellar population modeling, $\tau_V = 1.8$, as discussed below),
is $\rm 11~M_{\odot}~yr^{-1}$.  We measure a velocity dispersion of $158 \pm 32~\rm km~s^{-1}$ for this line, and note that a line of this width may arise from an AGN, as narrow emission from AGN has been shown to have approximately the same velocity dispersion as the bulges of the AGN host galaxies \citep{GreeneHo2005}.
In order to further constrain the rates of current and recent star formation, we
generate synthetic starburst spectra as described in \S\ref{sec.bg}.
As above, all models include a 7.0 Gyr-old single-burst stellar population (SSP7) of mass $\rm M_{SSP7}$ with solar metallicity ($Z_{\odot} = 0.02$) and  an 100 Myr-old burst with constant SFR which generates a mass in stars $\rm M_{burst}$.  We generate a similar set of models with supersolar metallicity ($Z = 2.5 Z_{\odot}$). The strength of the burst is parametrized by $A$, where $A = \rm M_{burst} / M_{SSP7}$ \citep[e.g.,][]{Kauffmann2003}.  We create models with $ 10^{-5} < A < 4$ and compare them to the LRIS spectrum of the foreground galaxy at 5620 \AA \ $< \lambda_{obs} <$ 7550 \AA \ (see Figure~\ref{fig.specmodel}).  We do not fit the portion of the spectrum blueward of this range, as it falls on the opposite side of the D560 dichroic, and because it lacks spectral features useful for distinguishing star formation histories.  The portion redward of this range is quite noisy and is subject to atmospheric absorption.

For each model, we find the best-fit value of $\tau_{V}$, with an attenuation curve parametrized in \citet{CharlotFall2000}, by performing a $\chi^2$ minimization.
The models do not include nebular or AGN line emission, so emission lines in the data are masked out prior to fitting.  We find that both solar and super-solar metallicity model spectra
cannot simultaneously match the strengths of the Balmer absorption and the \ion{Ca}{2} K and G band absorption in the data.
The addition of a featureless power-law (QSO) component \citep[$F_{\lambda} = \lambda^{\alpha_{\lambda}}$ with $\alpha_{\lambda} = -1.6$;][]{VandenBerk2001} does not improve the fits significantly.
These results suggest that there is no ongoing star formation in this galaxy.  A strictly passively evolving model is ruled out by the spectrum as well.

\subsubsection{Post-starburst Scenario}\label{sec.psb_scenario}
We also wish to investigate alternative star formation histories.  One possible star formation history that suggests itself, based on the location of the galaxy in the CMD as well as its morphology, is one in which the galaxy evolved passively for several billion years and then experienced a burst of star formation, which has since ceased \citep[``post-starburst"; e.g., ][]{DresslerGunn1983}.  We again generate a suite of solar metallicity models, all with a SSP which formed 7 Gyr ago.  A burst with constant SFR lasting 100 Myr is added to each model at a time $t_{burst}$, where $t_{burst}$ varies between 1.8 Gyr ago and 200 Myr ago.  As described below, this span in burst age encompasses the range in ages for models which provide a good fit to the data.  Models have values $0.03 < A =\rm M_{burst}/M_{SSP7} < 4$.  We allow for the addition of a QSO power-law continuum component as described above.  We find the best-fit values of $\tau_V$ and the fraction of light contributed by the power-law component by minimizing $\chi^2$ for each model in our grid.
We perform a visual inspection of the fit of each model, and find that
models with intermediate $t_{burst}$ values and larger values of $A$ are most successful at fitting the deep Balmer absorption and \ion{Ca}{2} K and G band absorption strengths in the data.
The best-fit model has
a high value of $A$ ($A = 4$; larger values give similar results) and a 1 Gyr-old burst; this model is shown in Figure~\ref{fig.specmodel}.
The best-fit value of $\tau_V \sim 0.6$, and the fraction of the total light contributed by the power-law component at 4200 \AA \ in the rest-frame is $\sim 15\%$.  Models with $t_{burst} > \rm 1.4~Gyr$, with $t_{burst} = \rm 1.4~Gyr$ and $A < 4$, or with $t_{burst} < \rm 600~Myr$ cannot simultaneously match the Balmer, \ion{Ca}{2} K and G band absorption strengths and thus yield unacceptable fits.
Models with $600~\mathrm{Myr} \leq t_{burst} \leq 1.4~\mathrm{Gyr}$ yield acceptable fits if $A$ is large enough at older ages, with a range in fitted $\tau_V$ values between 0 and 1.8.
We conclude that a starburst occurred in the galaxy between 1.4\,Gyr and 600\,Myr ago.
The results are similar for $Z = 2.5 Z_{\odot}$ models.
\\

In summary, we find that the foreground galaxy is host to a low luminosity AGN and has a stellar continuum consistent with that of a post-starburst galaxy.  It has an asymmetric morphology and is located in the ``green valley" in the CMD.  We note that the morphology of this object in the $ V_{606}$ band is in general consistent with that of simulated merger remnants $\gtrsim 0.5~\rm Gyr$ after the final coalescence \citep{Lotz2008}.  These results can be explained by a scenario in which the galaxy recently experienced a merger which triggered a starburst.  The starburst then ceased, perhaps because the cool gas supply was exhausted or expelled.
In this case, the galaxy will migrate to the red sequence.
\\

Analyzing our spectrum of the background galaxy
(TKRS4389) which lies at an impact parameter of $16.5~h_{70}^{-1}~\rm kpc$,
we identify strong \ion{Fe}{2}, \ion{Mg}{2}, \ion{Mg}{1} and \ion{Ca}{2} absorption from gas associated with
the foreground galaxy.  A subset of these features is shown
in Figure~\ref{fig.fgspecstamps} with velocities relative to the systemic velocity of TKRS4259.
The spectrum shown was obtained with the slitlet marked with the solid lines in
Figure~\ref{fig.im}; however, the spectrum taken with the longslit (marked with dashed lines
in Figure~\ref{fig.im}) exhibits foreground absorption line profiles with similar depths and
shapes as those shown.
The measured \ion{Mg}{2}~$\lambda 2796$ EW is extreme:
$W_r (2796) = 3.93 \pm 0.08$ \AA.
The oscillator strengths of the lines in the \ion{Mg}{2} doublet have a ratio 2:1, and as
the optical depth of the lines increases and they saturate, the EW ratio of the doublet decreases from 2:1 to
1:1.  The EW ratio of the \ion{Mg}{2} lines in our system is $\sim 1.1$, indicating a high degree of saturation.
In the case of heavily saturated lines, the $W_r (2796)$ value is indicative of extreme kinematics, i.e.,  a
large velocity width of $\Delta v \gtrsim 400~\rm km~s^{-1}$ \citep{Ellison2006}.
At such a low impact parameter, it is possible that our line of sight
is probing gas in the outer disk of the galaxy.
However, even if the galaxy were edge-on (it is not), the predicted differential
rotation of a disk at this impact parameter would be of the order a few tens of $\rm km~s^{-1}$.
We conclude that the gas dynamics are dominated by non-rotational motions
and that the majority of gas is extraplanar, i.e., tracing material in the
halo of TKRS4259.

Because the \ion{Mg}{2} lines are strongly saturated, the depth of the lines depends
only on the fraction of the background light source that is covered by absorbing gas ($C_f$) and the
instrument resolution.  The deepest parts of the line profiles from the spectra taken with slits at \emph{both} orientations
reach $\sim 20$\% of the continuum level,
which places a lower limit $C_f \gtrsim 0.8$.  The relatively low spectral resolution smears
the profiles, and the deepest parts of the lines may in fact appear at much lower normalized flux levels when observed at higher resolution.
This constraint on $C_f$ is particularly striking given the large beam size provided by the background galaxy:
the distance between the
two brightest knots in this galaxy is $\sim 4~ h_{70}^{-1}$ kpc at $z = 0.4729$.  This may suggest
that the absorbing gas complex almost completely covers the background source and has a large
velocity dispersion at all the locations probed.  This is consistent with previous results from
\citet{Rauch2002}, who report velocity coherence in \ion{Mg}{2} absorbing clouds on $\sim 0.4~h_{70}^{-1}$ kpc scales.
We leave detailed modeling of the effect of such a large
beam size on the observed absorption to a future work (although see \citealt{Frank2007} for an analysis of the effects of GRB vs.\ QSO beam size on \ion{Mg}{2} absorption system studies).

\section{DISCUSSION}\label{sec.discussion}

Here we examine several possible scenarios for the origin of the \ion{Mg}{2} gas in the foreground galaxy halo.

\subsection{Multiphase Cooling of the Halo / Cold Inflow}\label{sec.multiphase}
In the galaxy formation scenario proposed by \citet{MB2004} and \citet{Mo1996}, $\sim 10^4\rm~K$ clouds condense out of the hot gas in galaxy halos as it cools.  The velocity dispersion of these clouds is approximately that of the galaxy halo; we may therefore estimate the expected velocity dispersion in \ion{Mg}{2}-absorbing clouds given a halo mass for the galaxy.  Using the relation between halo mass and stellar mass derived in \citet{ConroyWechsler2009} via the ``abundance matching" technique, we estimate that the halo mass ($\rm M_h$) of the foreground galaxy is $\rm \log M_h/M_{\odot} \sim 12.9$ for $H_0 = 70~\rm km~s^{-1}~Mpc^{-1}$.  Using the relations between $\rm M_h$ and halo virial velocity given in \citet{MB2004} and assuming a
singular isothermal sphere for the halo density profile,
we find that the expected FWHM of the line-of-sight velocity distribution for cool clouds in a halo this massive is
$\sim 490\rm~km~s^{-1}$.
This dispersion could easily produce a $W_r (2796) > 3$ \AA \ \citep{Ellison2006}, consistent with the measured $W_r (2796)$ for this galaxy.

The thermal stability analysis of the hot gas surrounding galaxies performed by \citet{Binney2009} suggests that in the case of an isolated halo more massive than that of the Milky Way \citep[$\rm M_h = 10^{12}~ M_{\odot}$;][]{Klypin2002}, a smoothly stratified hot gaseous corona is stable to thermal perturbations and thus will not condense into cool clouds.  However, this study does not account for the effects of gas inflow from the IGM; nor does the assumption of a smooth hot gaseous halo likely apply in this case, given that our host galaxy is a merger remnant.  The three-dimensional cosmological simulations of \citet{Keres2009} show that even in halos well above the ``transition" mass ($\rm M_h \sim 2-3 \times 10^{11}~M_{\odot}$), in which hot, virialized atmospheres develop via shock-heating during gas accretion, cold filaments of gas from the intergalactic medium (IGM) can penetrate deep into the hot halo.  At high redshifts ($z \gtrsim 2$), these cold flows reach the central galaxy and fuel star formation.  At $z \sim 1$, in the case of a $\rm 9 \times 10^{12}~M_{\odot}$ halo, the filaments penetrate to only half the virial radius, but can fragment into dense, cold clouds via shocks, cooling instabilities, or other mechanisms.  As these clouds are
virialized within the halo, they will acquire a large velocity dispersion and produce a large $W_r(2796)$, as discussed above.

However, we do not consider cold inflow from the IGM to be the most likely origin of the cool halo gas we observe.  First, our detection of $\sim 3.9$ \AA \ \ion{Mg}{2} $\lambda 2796$ halo absorption and $\sim 1$ \AA \ \ion{Ca}{2} K halo absorption in this system (as noted in \S\ref{sec.thepair}; see also Figure~\ref{fig.fgspecstamps} and Table~\ref{tab.ew}) may indicate that the absorbing gas is enriched with metals and dust.  We cannot measure the metallicity or dust content of this system directly, as we lack the necessary spectral coverage.  However,
strong \ion{Mg}{2} absorption systems in the redshift range $0.4 < z < 2.2$ have been shown to significantly redden background QSOs \citep{Menard2008}; furthermore, the degree of reddening increases with $W_r(2796)$.  \citet{Menard2008} find that for absorbers with $W_r(2796) \sim 3.9$ \AA \ at $z=0.4729$, the mean rest-frame $E(B-V) \sim 0.05$ (see their Equation 18).  They also find that absorbers with $W_r(2796) > 1$ \AA \ have an average dust-to-metals ratio close to those measured in the Milky Way ISM.
Similar results for the mean dust-to-metals ratio of strong \ion{Ca}{2} absorbers have been reported by \citet{Wild2006},
who additionally show that dust content increases with larger $W_r (3935)$ \citep[see also][]{WildHewett2005}.
As noted above, the \ion{Ca}{2} absorption we observe has an $W_r (3935)$ value as large as the strongest absorbers in these \ion{Ca}{2} studies.  These findings suggest that there may be a substantial amount of dust in this system.
Second, we do not resolve individual gas clouds because of our low spectral resolution ($\rm \sim 290~km~s^{-1}$); however, we note that the absorption line profiles in Figure~\ref{fig.fgspecstamps} exhibit asymmetry.  \citet{Prochaska1997} find that cool gas clouds distributed such that the gas density is proportional to the total matter density in an isothermal spherical halo tend to produce a symmetric velocity profile, although this depends on the number of absorbing clouds in the halo and the particular sightline observed.
Both the likely high dust content of the absorption system and the line profile asymmetry suggest an alternate origin for the observed cool gas.

\subsection{Ejection of ISM into the Halo}
We next consider whether the observed halo gas could have plausibly originated in the ISM of the host galaxy or progenitor galaxies which was ejected during a previous starburst, merger or luminous AGN phase.
If this phase occurred $\sim 1$ Gyr ago (as is likely; see \S\ref{sec.psb_scenario}), cool outflows would have had to reach speeds of only $\sim 16~h_{70}^{-1} / \rm cos(\theta)~km~s^{-1}$
to reach a projected distance of $16.5~ h_{70}^{-1}$ kpc today, where $\theta$ is the angle between the plane of the sky and the path taken by the gas.  Cool outflows commonly reach speeds in excess of $\sim 100\rm~km~s^{-1}$ in starburst galaxies \citep{Weiner2009,Martin2005,Rupke2005b}
and have even been observed in post-starburst galaxies at intermediate redshifts \citep{Tremonti2007,Sato2009}.
Cool gas which has been tidally stripped from the progenitor galaxies of this merger remnant may also give rise to enriched halo absorption with large $W_r (2796)$, provided that the velocity spread in the stripped clouds is large enough \citep{Wang1993}.  The Magellanic Stream, for instance, has a velocity dispersion of $\rm \sim 15-20~km~s^{-1}$ \citep{Bruns2005}, and so could not produce the observed $W_r (2796)$ in the absence of other clouds.
Additionally, anisotropic ejection of gas clouds or tidal streams could easily produce asymmetric absorption line profiles.  We conclude that cool ISM which was driven or stripped out of the galactic star-forming regions during a past starburst, merger or AGN phase is a plausible origin for this gas.  If in reality the gas originated in a cold inflow or halo condensation as discussed in \S\ref{sec.multiphase}, our finding that the galaxy experienced a starburst $\sim 1$ Gyr ago is simply a coincidence, and is not necessarily related to the observed absorbing gas.  We note that it is unlikely that there is ongoing expulsion of ISM, as there is little current star formation activity in the galaxy, and the observed AGN activity
is weak.
Therefore, in this scenario, once the cool gas was ejected or stripped, it is likely to have remained cold for approximately 1 Gyr, i.e., since the starburst activity.  The analysis of \citet{Binney2009} suggests that ejected \emph{hot} gas could not have cooled through condensation, although again, the assumptions made in that analysis may not apply in this case.

Cool gas clouds ejected or stripped from the ISM and moving through a hot medium may be subject to the Kelvin-Helmholtz instability.  \citet{Vietri1997} showed that such disturbances on the surface of a cloud cannot completely disrupt the cloud unless its cooling time is longer than its sound crossing time.
Following \citet{MB2004}, we assume an isothermal halo with temperature $\rm T_h = 3.3 \times 10^6 K$ and with gas density profile $\rho_g = f_b  V_{max}^2 / 4 \pi G R^2$, where $f_b = 0.17$ is the cosmic baryon fraction \citep{Spergel2003}, and $V_{max}$ is the maximum rotation velocity of the halo (equal to the virial velocity in this case; see \citealt{MB2004} for details).  We assume that the cool clouds are at $\rm T = 10^4 K$ and that they immediately come into pressure equilibrium with
the surrounding hot gas as soon as they enter the halo.  The sound crossing time for a cloud is given by the ratio of the cloud radius to the cloud sound speed ($\sim 12~\rm km~ s^{-1}$).  To calculate the cooling time of the cloud, we use Equation 33 from \citet{MB2004}.  We find that the sound crossing time exceeds the cooling time by at least one order of magnitude for clouds with masses $5 \times 10^4 - 5 \times 10^6 \rm M_{\odot}$ out to the halo virial radius ($\sim 390$ kpc).  We expect that these clouds will be stable against the Kelvin-Helmholtz instability.  We also note that the clouds at the upper end of this mass range are evaporated by conduction on timescales of $\gtrsim 2$ Gyr, where the evaporation timescale is given by Equation 35 in \citet{MB2004}.  If we assume that the hot gas profile does not change substantially with time, we can conclude that cold clouds driven into the halo from the ISM during a starburst or merger occurring $\sim 1$ Gyr ago should remain cold today, and indeed for at least 1 Gyr more.

Outflow during the past starburst, merger or luminous AGN event may have been powered by a variety of mechanisms.  The galaxy evolution model advocated by \citet[][and references therein]{Hopkins2008} suggests that in a gas rich major merger gas is driven to the center of the galaxies once they have coalesced, fueling powerful starburst activity and black hole growth and igniting a luminous QSO.
Feedback from supernovae explosions is well known to drive outflows in starburst galaxies \citep[e.g.,][]{Heckman1990,Rupke2005b} and could have contributed all of the power needed to accelerate the cool ISM to velocities of $\gtrsim 100{\rm \; km\;s^{-1}}$.
Simulations of major mergers \citep{Cox2004,Cox2006a} show that they can generate a shock-heated gas wind, possibly forcing cool gas into the halo.  In addition, gas from the ISM that was tidally stripped during a merger event may have been left behind at large impact parameters.  Finally,
a luminous AGN could have contributed to driving cool gas into the galactic halo and to the quenching of star formation.  In the \citet{Hopkins2008} scenario, the phase in which the remaining ISM material is blown away and the QSO is revealed is expected to occur within a few hundred Myr of the merger itself.  The phase in which the QSO has faded and the merger remnant reddens and exhibits a post-starburst stellar continuum occurs  $\sim 800~\rm Myr$ after the merger.  Our results on the star formation history, colors, and morphology of this galaxy fit well into this scenario.
However, we note that we have the strongest evidence that the galaxy is post-starburst; the occurrence of a quasar phase is purely speculative.

We also consider whether clouds ejected from the ISM would have a large spread in velocities of $\gtrsim 400~\rm km~ s^{-1}$ 1 Gyr after the starburst event has ceased.  To determine this, we construct a toy model of the behavior of the outflowing gas inside the halo potential.  To start, we follow \citet{Murray2005} and assume that the velocity ($V(r)$) of the outflowing gas as a function of distance from the starburst region ($r$) is given by $ V(r) = 2 \sigma_h \sqrt{(\frac{L}{L_M} -1) \ln \frac{r}{R_0} + V(R_0)^2}$, where $\sigma_h$ is the halo velocity dispersion, $L_M$ is the lower limit on the starburst luminosity needed to expel a large fraction of the galaxy's gas when it is optically thick, and $R_0$ is the initial radius of the outflow.  This equation applies until the terminal velocity is reached, $V_{term } = 3 \sigma_h$.  For $L/L_M = 2$, $R_0 = 1$ kpc and $V(R_0) = 10~\rm km~ s^{-1}$, the gas is driven to radii of $\sim 60$ kpc during a 100 Myr-long starburst.  The results are insensitive to the choice of $V(R_0)$ as long as $V(R_0) \ll \sigma_h$; however, $L/L_M$ and $R_0$ must have values such that the gas does not fall back onto the galaxy in 1 Gyr.  If $R_0 = 1$ kpc, values of $L/L_M \geq 1.4$ are viable; if $R_0$ is doubled, slightly lower values of $L/L_M \gtrsim 1.3$ yield cloud distances and velocities high enough so that they remain in the halo for the necessary amount of time.

We then assume that the starburst ends abruptly, and that the clouds from the wind are now subject only to the gravitational potential of the halo, and neglect the effect of drag forces from the surrounding hot halo gas.
By integrating the equations of motion for clouds with distances $ \lesssim 60$ kpc and with initial velocities given by the above equation for $V(r)$, we calculate the final positions and velocities after 1 Gyr.  A bipolar geometry for the outflow with an opening angle of $60^{\circ}$ is assumed, consistent with measurements of the opening angle of the outflow cones traced by H$\alpha$ and CO emission in M82 \citep[e.g.,][]{Heckman1990,Walter2002}, such that our line of sight intersects both outflow cones and is parallel to the axis passing through the centers of the cones.  We calculate the line-of-sight velocities for the clouds that are at a projected distance of $\sim 16.5~ h_{70}^{-1}$ kpc after 1 and 2 Gyr.  The velocity spread is well above $400~\rm km~ s^{-1}$ at both time increments.  While this model is quite rudimentary, it indicates that clouds driven out of a galaxy 1 Gyr ago may have the large velocity dispersion that is observed, and that they will maintain this large dispersion for at least another 1 Gyr.

From all of the evidence discussed above, we conclude that the absorption system is most likely gaseous fragments of the ISM from the merger remnant we observe.  This gas may have been ejected by
a wind driven by a starburst, merger, or AGN, or tidally stripped from the progenitor galaxies.  If indeed these clouds originated in the ISM, this is one of the first measurements of the radial extent of such outflows or tidally stripped gas in the distant Universe and suggests that it reaches far beyond the stellar disk.
Because the clouds we observe are likely dusty (see \S\ref{sec.multiphase}), this mechanism may be responsible for distributing the diffuse dust detected in galaxy halos to projected separations much larger than the scales of galactic disks \citep{Menard2009}.

\subsection{The Relationship Between $M_h$ and $W_r (2796)$}
A complementary method which has recently been used to study the host galaxies of \ion{Mg}{2} absorption systems measures the clustering strength of a large sample of absorbers with respect to that of luminous red galaxies (LRGs), to determine the mean halo masses in which absorbers of varying strengths are found.
These studies have shown that there is a weak anticorrelation between $W_r(2796)$ and the bias of \ion{Mg}{2} systems at $z \sim 0.5$.
This has been interpreted as an anticorrelation with mean absorber halo mass, significant at the 1$\sigma$ level; i.e., absorbers with 1.0 \AA \ $ < W_r (2796)   \le  $ 1.5 \AA \ have mean halo mass  $\mathrm{M_h} \sim 10^{13.2}~ h_{70}^{-1} ~\mathrm{M_{\odot}}$, while $W_r (2796) \ge \rm 1.5 \AA$ absorbers have mean halo mass $\mathrm{M_h} \sim 10^{12.2}~ h_{70}^{-1}~ \mathrm{M_{\odot}}$ (\citealp{Gauthier2009}; see also \citealp{Bouche2006} and \citealp{Lundgren2009}).
The number of $ W_r (2796) \sim 4$ \AA \ absorbers in these studies is relatively small;
however,
the $\rm log~M_h/M_{\odot} \sim 12.9$ we infer for our foreground absorber, while higher than the mean halo mass of strong absorbers quoted above, is well within the uncertainties in the estimates of the mean halo masses for \emph{both} weak and strong absorbers \citep[see Figure 7c,][]{Gauthier2009}.

One explanation proposed by \citet{Bouche2006,Bouche2007} for the origin of strong \ion{Mg}{2} absorbers suggests that cool gas is driven into galaxy halos via starburst-driven winds.   These authors propose that winds are more likely to remove gas from galactic disks in shallower potential wells, and therefore expect strong absorbers to be preferentially found in lower-mass halos.  \citet{Gauthier2009} show, however, that the clustering of strong absorbers is \emph{unbiased} with respect to dark matter halos and thus strong absorption does not occur preferentially at low masses.  Furthermore, the present study provides one example of strong \ion{Mg}{2} absorption which is most likely due to past outflow or merger activity in a high mass ($\rm \log M_h/M_{\odot} = 12.9$) halo.  Our result implies that while galactic winds may be an important source of cool halo gas, they should not necessarily be the dominant contributor in only low mass halos, and indeed \emph{must} not occur preferentially in lower mass halos if they are to fully explain the bias results of \citet{Gauthier2009}.

An alternative picture is inspired by
simulations of, e.g., \citet{DekelBirnboim2006} and \citet{Birnboim2007}, which provide evidence for the ``transition" halo mass,
above which cold gas is shock heated as it is accreted onto a halo as discussed in \S\ref{sec.multiphase}.
 \citet{TC2008} find that an anticorrelation between $\rm M_h$ and $W_r(2796)$, as well as the observed frequency distribution of \ion{Mg}{2} absorbers, can be reproduced in a halo occupation model which includes such a transition mass, so that the most massive halos are mostly too hot to produce large $W_r (2796)$ while lower mass halos contain more cool gas and can give rise to high $W_r (2796)$ systems.
 As shown in \citet{Keres2009}, cold flows can partially penetrate through the hot gas in massive halos at $z \lesssim 1$ and form cold clouds, which may even then fuel further star formation.  While our galaxy is unusual in that it is post-starburst, the existence of an \emph{enriched} $W_r(2796) = 3.93 \pm 0.08$ \AA \ system in a halo with a mass well above the ``transition mass" is consistent with this picture, and if the observed gas originated in an outflow, implies that (1) the effects of star formation on halo gas are observed well into the mass regime in which hot gas accretion dominates the total gas accretion, or (2) there is a spread in transition mass for different galaxy halos.

\section{CONCLUDING REMARKS}\label{sec.conclusions}
Using multiwavelength analysis of the luminous components of a galaxy at $z = 0.4729$ in concert with spectroscopy of a bright, close transverse background galaxy at $z = 0.6942$, we demonstrate that the cool gas traced by \ion{Mg}{2} absorption in the foreground galaxy halo at impact parameter $16.5~h_{70}^{-1}$ kpc most likely originated in the ISM of the host galaxy or its progenitors.  This galaxy has little ongoing star formation and exhibits only weak AGN activity; however, it experienced a starburst $\sim 1$ Gyr ago, which may have been triggered by a merger event.  The cool halo gas could have easily been driven or stripped away from the star-forming regions during this past violent phase, and could have survived in the hot halo since that time.  Our rudimentary toy model for the motions of clouds driven into the halo by a past starburst suggests that these clouds would have a large velocity dispersion $ \gtrsim 400~\rm km~s^{-1}$ today, consistent with our observations.

We emphasize that the
analysis of the luminous components of this
galaxy achieves an unprecedented level of detail in the context of studies of distant
absorption-selected
galaxies with $W_r (2796) \gtrsim 2$ \AA.  Such detail is possible because of the rich dataset available in GOODS, including
the galaxy redshifts from TKRS \citep{Wirth2004} and our LRIS spectroscopy.
We were able to identify the post-starburst and age-date it using this dataset; previous works could
not necessarily find such a galaxy, and thus present a less complete view of the host galaxies of strong absorbers.
\citet{Bouche2007} searched for $\rm H\alpha$ emission near $W_r (2796) > 2$ \AA \
absorbers at $z \sim 1$ to investigate a starburst origin for \ion{Mg}{2} absorption;
this method cannot be used to identify host galaxies without $\rm H\alpha$ emission,
such as post-starbursts with weak AGN activity.  \citet{Nestor2007} investigated
environments of $\rm 3~\AA < W_r(2796) < 6~\AA$ absorbers by imaging the corresponding
QSO fields; however, they lacked spectroscopic confirmation of galaxy-absorber associations
and have not constrained the star formation history of absorber hosts.

Our study only begins to demonstrate the power of using background galaxies to probe foreground halo gas.
Several large spectroscopic surveys have recently concluded or are nearing completion that can be used to identify pairs suitable for a targeted search for foreground \ion{Mg}{2} absorption.  Spectroscopic followup with an instrument such as LRIS requires that the background source be bright and blue so that a continuum signal-to-noise ratio of $\sim 15-20$ at $\sim 4200$ \AA \ can be acquired in a reasonable exposure time (i.e., $ B < 22$ in less than 4 hours).  This $\rm S/N$ is needed to achieve a $5\sigma$ EW detection limit of 0.5 \AA \ for a \ion{Mg}{2} absorber at $z \sim 0.5$.
There are $\sim 40$ galaxy pairs with redshifts measured as part of the DEEP2 survey of the Extended Groth Strip (EGS) with angular separations $< 15\arcsec$ \citep{Davis2003} which meet these requirements.
Surveys such as COMBO-17 \citep{Wolf2004} and zCOSMOS \citep{Lilly2007} will provide pair candidates in numbers on the same order as DEEP2, as will the forthcoming VIMOS VLT Surveys \citep{LeFevre2005}.  The PRIMUS survey\footnote{http://cmb.as.arizona.edu/$\sim$eisenste/primus/Home.html} \citep{Cool2008} will take galaxy spectra over 10 square degrees and should enable selection of over 1500 galaxy pairs.
The Pan-STARRS survey\footnote{http://pan-starrs.ifa.hawaii.edu/public/home.html}, which will image 1200 square degrees in 4 filters to $g < 27$, will provide an unprecedented number of photometric redshifts.  Using the average sampling rate and the average redshift success rate of the EGS portion of the DEEP2 survey \citep{Willmer2006} to scale the number of pair candidates to that expected from a photometric survey, and additionally scaling by the 2400-fold increase in sky coverage with Pan-STARRS, we expect that $> 150,000$
galaxy pairs will be available for spectroscopic followup.

The use of galaxies as background probes is complementary to analysis of GRB sightlines, which have a negligible beam size but similarly allow for close analysis of the absorber host \citep{Pollack2009}.  In good seeing conditions and with extended background galaxies, one may probe multiple sightlines through a given foreground halo.
Size scales smaller than $\sim 4$ kpc at $z = 0.5$ are not currently accessible because of seeing limitations.  However, with adaptive optics and IFUs on 10m-class telescopes and beyond, spatially extended background galaxies will enable study of the morphology and kinematics of halo absorption in concert with detailed analysis of the luminous components of absorber hosts.

\acknowledgements
The authors are grateful for support for this project from NSF grants AST-0808133 and AST-0507483.
J.X.P. acknowledges funding though an NSF CAREER grant (AST-0548180).

The authors wish to thank C. Tremonti for freely providing her stellar population modeling code, K. Cooksey for providing her absorption feature-finding code and for a careful reading of the manuscript, and S. Patel for providing IDL code to produce color images.  We thank James Bullock, Hsiao-Wen Chen, Sara Ellison, Jenny Graves, Bill Mathews, Crystal Martin, Brice M{\'e}nard, David Rosario, Jeremy Tinker, Chris Thom and Luke Winstrom for interesting and helpful discussions during the analysis of these results.

The authors wish to recognize and acknowledge the very significant
cultural role and reverence that the summit of Mauna Kea has always
had within the indigenous Hawaiian community.  We are most fortunate
to have the opportunity to conduct observations from this mountain.

{\it Facilities:} \facility{Keck:I (LRIS)}, \facility{HST (ACS)}.

redpajama_set_name: RedPajamaArXiv


Last week we began to talk about the book, "Autopsy of a Deceased Church." We talked about the most pervasive trait of churches that die: They live in the past. Today we're going to talk about a second widespread trait of dying churches: They focus on their own comfort first.
That shouldn't surprise us. Is not our culture obsessed with ease and comfort? When you watch a car commercial, don't they always focus in on the exquisite detailing of the Italian leather upholstery and the exotic wood trim and the heated seats? How many billions of dollars do we spend annually on clothes, medicines, furniture, appliances, and everything else that makes us feel comfortable? Why wouldn't we expect people to bring the same attitude into the Church? Why would people not want their opinions, their styles, and so on to run the day in the Church?
But that's not what the gospel calls us to. Jesus preached a message of self-denial, not comfort.
We heard from Mark 8. Now, I think it's certain that Peter wanted God's Kingdom to come. He just didn't want it to come in the way Jesus was talking about. Jesus spoke of his own death. Peter wanted Jesus to put their enemies to death. He wanted a worldly and politically powerful Kingdom of God, not an other-worldly and politically powerless Kingdom of God.
Jesus said, "If you want to follow me, deny yourself." Say no to your desires, your will, your comfort. "If you try to cling to things, you will lose them anyway." Nothing in this world will last. It's not worth clinging to the things of this world. We should cling to Jesus and do his will.
"Is anything worth more than your soul? Is anything worth more than your eternal life?" Let me turn that question around: "Is your comfort worth more than your neighbor's soul?" That's the real issue. Many churches are not reaching their neighbors with the life-giving message of the gospel for the sake of their own comfort.
First, dying churches want the comfort of people just like themselves. Sometimes that means they cease to look like the communities that they are located in. This is more obvious in urban areas, where changes tend to happen more rapidly, but it can also happen in other places.
My mother grew up in a neighborhood in Pittsburgh that was predominantly white when she was born and predominantly non-white by the time she graduated from high school. She attended a Methodist Church. As the community changed, the church did not. Members moved away, but kept driving back to the church. Years after she moved away, the church was still 100% white, but almost none of the members lived in the neighborhood. Eventually, it closed. It died. No one took seriously the idea of stepping out of their comfort zones to welcome the people that lived in the community.
Why not? Because dying churches are comfortable in their fortress. I mean church building. You know what I mean.
Walls keep people in and they keep people out. The people outside the church walls feel uncomfortable in them, and the people in the walls are uncomfortable outside of them. They may say, "Everyone is welcome in here!" But do they really mean it?
I don't get many chances to be an outsider in a church. When you're the pastor, you have an "inside track." But from time to time, I get to visit churches as an outsider to see what happens. My experience, by and large, has been that I was unwelcome.
When Sharon and I were both in college, we attended several different churches together. One was the United Methodist Church where her father was appointed after she started college, so we had an inside track there. But the other United Methodist Church we went to a few times was in the town where she attended school. I don't remember how many times we went to that church, but I remember we had the same experience every time: No one spoke to us. No one. One time we couldn't find a bulletin, and no one helped us. We just wandered around till we stumbled on one.
I've had similar experiences in other places. We went once to a UMC in Vienna, VA while we were visiting family. No one spoke to us, except the pastor. After all, that's the pastor's job. Once we went with Sharon's folks to a UMC in Myrtle Beach while on vacation. No one spoke to us, but the ladies in the pew behind us made it very clear in loud whispers that they didn't appreciate us sitting in their seats. When Sharon tried to take the kids to the nursery, she couldn't find it. And no one offered to help.
Strangely, the one experience we had of a friendly church was a Church of the Nazarene in the town where Sharon went to college. They were so friendly we walked out with a CD from their choir and had to turn down two invitations to lunch.
search committee" at work, and the chairperson came to the conclusion: "Okay, so let me get this straight: We want a pastor who will challenge us and lead us in new directions by keeping everything exactly the same, right?" There it is: Dying churches want to keep the same programs, the same worship, yet somehow still attract new people, but only if the new people are just like the people already there.
A good example of this, which I've heard of several times, is that a church will decide to start a contemporary worship service. But they won't move the worship service they already have. Or the Sunday School. So they end up starting a new worship service to attract new people at 8 AM. Because, of course, the people sleeping in instead of going to worship at 10:30 will be willing to go at 8, right? Sure.
The third way this comfort-driven focus can be seen is that dying churches are comfort-driven with their money.
Often the church staff becomes the largest expense. And the staff are primarily expected to minister to the congregation, not to the community. By the way, United Methodist pastors are appointed to serve congregations and communities.
When budget cuts are made, the first things to go are typically the outward-oriented ministries. The things that the members enjoy are not cut.
Let me close with a thought from Paul in Philippians. He says, "Real contentment can only be found in Jesus. Without him, we can never be content. With him, we can be content no matter our circumstances." Paul was content to sit in a jail cell if it would further the cause of Christ. By contrast, some Christians, apparently, are unwilling to sit in a different pew to further the cause of Christ.
The gospel is not about our comfort. It is about being a part of a great work of God. And I do believe we are quite capable of embracing that. Deep down, we really do long to be a part of something great, something that changes the world. But, if we take our focus off of our great mission for too long, then we fall back onto our default position: We want to be comfortable. But we'll talk more about that in a couple weeks.


Supported modes are -bs and -t, with any additional flags desired. It is advised to use -bs mode since error reporting with -t mode is not possible.
Create a new SendmailTransport with $buf for I/O.
Get the sendmail command which will be invoked.
Recipient/sender data will be retrieved from the Message API.
The return value is the number of recipients who were accepted for delivery. NOTE: If using 'sendmail -t' you will not be aware of any failures until they bounce (i.e. send() will always return 100% success).
Set the command to invoke.
If using -t mode you are strongly advised to include -oi or -i in the flags. For example: /usr/sbin/sendmail -oi -t Swift will append a -f flag if one is not present.
The recommended mode is "-bs" since it is interactive and failure notifications are hence possible.
Start the standalone SMTP session if running in -bs mode.


Injured Bears QB Jay Cutler's absence raises lots of questions.
Aaron Rodgers got a big assist from the Packers' defense.
We've got complete coverage of the Bears' NFC title game loss.
What's your opinion of the Packers-Bears NFC Championship Game?
Many teams created buzz, but who has done the best work in free agency? We hand out grades.
Mailbag: We explain why expanded playoffs are on hold and discuss overtime rules and extra points.
Will the NFL eat humble pie when revenues and TV ratings are at an all-time high?
The draft is about fit. Here are the perfect destinations for some of this year's top prospects.
Marcus Mariota still doesn't trump Jameis Winston, but he makes a lot of sense for Tennessee at No. 2.
Stan Kroenke is a reclusive sports mogul, but he's making noise with his efforts to move the Rams to L.A.
Jameis Winston is expected to be the No. 1 pick of the draft. It would look bad if he wasn't there.
NFL retirees want their peers who are battling depression to know they aren't alone in the struggle.
Play Podcast Ross Tucker recaps all the games from Week 17, takes an early look at the playoff matchups and discusses the coaching firings as they happened during the recording.
Play Podcast ESPN.com bloggers Kevin Seifert and Mike Sando revisit the impact of the "Fail Mary" and how it served as a catalyst for Russell Wilson's chances to win rookie of the year.
Play Podcast ESPN.com bloggers Kevin Seifert and Mike Sando look at the weak quarterback class of 2013 and which teams will be looking to make a change at that position.
AccuScore has powered more than 10,000 simulations for every NFL game for ESPN.com, each simulated one play at a time and minimum of 10,000 times. View all projections.
NFC: Atl. | Det. | G.B. | N.O. | NYG | S.F.
AFC: Balt. | Cin. | Den. | Hou. | N.E. | Pitt.


text:
Efficiency & Environment, Finance & Markets, Top Stories
EU approves state aid for Drax biomass unit
The EU Commission has approved the UK support for the conversion of one unit of the Drax power station from coal to biomass. The Commission said the plans complied with […]
Jacqueline Echevarria
Drax power station at night. Image: Thinkstock
The EU Commission has approved the UK support for the conversion of one unit of the Drax power station from coal to biomass.
The Commission said the plans complied with EU state aid rules as the project will support the region's environmental and energy targets without distorting competition in the Single Market.
Drax's unit will have a capacity of 645MW running exclusively on wood pellets. It is due to use around 2.4 million tonnes of them per year.
The UK Government, which notified the EU of its plans last year, intends to support the project with a premium paid on top of the market price of the electricity generated.
The project will receive the support until 2027 will generate around 3.6TWh of electricity per year according to UK estimates.
The Commission opened an investigation to check the aid would not lead to overcompensation and undue distortions of competition in the biomass market.
It concluded the project's contribution to increasing the share of renewable energy produced in the UK outweighs any potential distortions of competition that could be triggered by the government support.
biomass coal Drax EU


text:
Has Colts Linebacker Shaquille Leonard's Expected Return Shifted to a Later Date?
By Luke Schultheis Aug 9, 2022, 9:00am EDT
Share All sharing options for: Has Colts Linebacker Shaquille Leonard's Expected Return Shifted to a Later Date?
Photo by Zach Bolinger/Icon Sportswire via Getty Images
While there's never been a set in stone return date, Indianapolis Colts' team officials initially expected 4x NFL All-Pro linebacker Shaquille Leonard, coming off offseason back surgery, to be ready for their regular season opener on September 11th against the Houston Texans:
Update from the Colts on star LB Darius Leonard: No second surgery on his ankle, but he has been having back issues that require surgery. Operation is today. He'll miss some camp time but the team's expectation is he's ready for the regular season.
— Zak Keefer (@zkeefer) June 7, 2022
However, it now appears that maybe that (overly optimistic?) expected return to the field has slightly shifted to a potential later date during the first half of training camp:
Colts All-pro LB Shaquille (Darius) Leonard watched practice in street clothes as he recovers from June back surgery.
I'm told there is no set return timetable but per source they do expect him back at "some point" this year. 17-game season. They'll need him but won't rush him.
— Cameron Wolfe (@CameronWolfe) August 9, 2022
Maybe I'm reading too much between the lines, but "at some point" doesn't seem nearly as encouraging that Leonard will be ready for the opener, right?
Don't get me wrong, it's not time to panic yet—as this situation remains entirely fluid, and it's still quite possible that Leonard can return early on this season, if not necessarily even for the opener per se. The Colts may be able to 'buy some time' until Week 3 against the Kansas City Chiefs at home on September 25th (playing the Texans and Jacksonville Jaguars during the first two weeks of the season, but at Jacksonville is never easy for the franchise).
Back surgeries are always tricky, and this isn't something to rush for one of the Colts cornerstone defensive players who plays an incredibly physically demanding position—with nearly constant contact on each play. The Colts defense needs Leonard healthy and at full strength to truly ascend into an elite defensive unit—as the squad's undisputed top playmaker and arguably best player.
However, it does raise the question of whether his expected return is starting to at least slightly shift to a later date with the regular season opener just a little over a month away.


Gone are the days of the Unicorn Frappuccino, that was so 2017! We are now well into a new year and with that comes new trends and Starbucks is looking to cash in on the millennials obsession with their establishment.
In a culture where Instagram and Snapchat reign supreme Starbucks has learned to harness the power of social media to build buzz around their latest and greatest creations. I imagine somewhere up in Seattle there's a room at the Starbucks headquarters filled with magical creatures sprinkling fairy dust over empty cups while they sit back and wait to see what appears.
Okay, I am sure there is more to it than that but one look at the specialty drinks they come up with and you can understand why I would think that. I know that their marketing department is sitting back and salivating over the free advertising they're going to be getting as our social media feeds are filled with pictures of warm beaches and Crystal Ball Frappucinos.
Let's take a closer look at what this drink actually entails.


Item: 11-2690 - Type: Cross Stitch Patterns.
"Seasons Greetings, Merry Christmas". Model stitched on 30 count Parchment Linen with Weeks Dye Works thread (DMC alternates listed), DMC floss, Mill Hill Seed Beads, and Just Another Button Company buttons. Stitch count is 97H x 58W.


text:
Pick the best hand(s) from a list of poker hands.

See [wikipedia](https://en.wikipedia.org/wiki/List_of_poker_hands) for an
overview of poker hands.

Your function will receive an array of strings. Each string represents
a hand composed of 5 cards separated by spaces. A card is represented
by a number and its suit.

You are to return an array containing either the best hand or, in case
of a tie, the best hands. Each hand should be a string in the same
format as given to you initially as input.

## Coding the solution

Look for a stub file having the name poker.go
and place your solution code in that file.

## Running the tests

To run the tests run the command `go test` from within the exercise directory.

If the test suite contains benchmarks, you can run these with the `--bench` and `--benchmem`
flags:

    go test -v --bench . --benchmem

Keep in mind that each reviewer will run benchmarks on a different machine, with
different specs, so the results from these benchmark tests may vary.

## Further information

For more detailed information about the Go track, including how to get help if
you're having trouble, please visit the exercism.io [Go language page](http://exercism.io/languages/go/resources).

## Source

Inspired by the training course from Udacity. [https://www.udacity.com/course/viewer#!/c-cs212/](https://www.udacity.com/course/viewer#!/c-cs212/)

## Submitting Incomplete Solutions
It's possible to submit an incomplete solution so you can see how others have completed the exercise.

redpajama_set_name: RedPajamaGithub


text:
Чемпіонат Європи з легкої атлетики в приміщенні 1992 відбувся 28 лютого–1 березня в  Генуї.

Це був перший чемпіонат в історії, який тривав три дні. На попередніх першостях розклад змагань був дводенним.

Також на чемпіонаті вперше в історії були розіграні нагороди у багатоборстві серед чоловіків та жінок.

Призери

Чоловіки

Жінки

Див. також

 Чемпіонат України з легкої атлетики в приміщенні 1992

Медальний залік

Джерела

 Офіційна сторінка змагань на вебсайті Європейської легкоатлетичної асоціації

1992
Європа
Легка атлетика
Легка атлетика
Легка атлетика
Легка атлетика
Європа

redpajama_set_name: RedPajamaWikipedia


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text:
Russian deputies demand for new Georgian wine embargo; Abashidze is skeptical
22.07.2016 (Hvino News). Russia's State Duma has recommended the government to ban import of wine and mineral water from Georgia.
Ian Zelinsky of Duma's foreign relations committee talked about need to 'take measures' against Georgia and other countries (Montenegro, Lichtenstein, Norway, Albania and Ukraine) for joining the European Union's economic sanctions against Russia. The EU decided recently to extend its sanctions until June 23, 2017, and onn July 20 Georgia and five other countries followed suit. On 23 June 2014, the Council of the European Union adopted Decision 2014/386/CFSP concerning restrictions on goods originating in Crimea or Sevastopol in response to the illegal annexation of Crimea and Sevastopol and Georgia joined this decision in the same year. The sanctions ban import of goods from Crimea, prohibits investing in the island and bans tourism services there.
Mr. Zelinsky, who represents the far-right Liberal Democratic Party, said Russia can easily do without Georgian wine and mineral water. "We have to develop Crimea, where unlike Georgian wine, we can produce wine without any chemical impurities," he said.
Russia has previously embargoed Georgian wine in 2006. The embargo lasted until May 2013 and was removed after the direct negotiations between Moscow and Tbilisi were opened under the current government. In 2014, Kremlin embargoed import of onions, carrots, peppers, melons and watermelons from Georgia as a response to the EU sanctions.
According to Russian MP, this will be an official respond to Tbilisi, which has joined policy of anti-Russian sanctions due to crisis in Ukraine and annexation of Crimea.
Georgia's special envoy on relations with Russia Zurab Abashidze has no expectations that Russia will impose an embargo on Georgian wine and mineral water ."I'm not expecting that to happen. It's not a decision yet, just an initiative proposed by one of the members of Russian parliament, - said Mr. Abashidze.
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Recognizes undergraduate students who, since the beginning of their junior year (last six quarters or four semesters), have distinguished themselves through excellence of scholarship and campus leadership. The aim is to single out those who have brought distinction to industrial engineering at their institution.
The nominees should be graduating seniors during the academic year in which they are nominated and must be members of the Institute of Industrial & Systems Engineers.
Each IISE university chapter is encouraged to nominate up to two members for this award.
No more than one first place, one second place, and one third place award will be given each year.
Complete and return the nomination form.
This award is judged by the CIEADH committee.