text:
CCPD: Car slams into Flour Bluff apartment building
By: Site Administrator
An apartment building is damaged after a car smashed into it.
The crash happened around 1:45 pm Sunday afternoon at an apartment building near Waldron Road and the Knickerbocker Street intersection.
According to police, the driver of the car was backing out of a parking lot and thought he had the vehicle in reverse. But unfortunately, he didn't and instead drove into an apartment building.
Police say no one was living inside the apartment at this time. Police issued a ticket to the driver.
Crash investigators also said the driver and his passenger were not injured, only shaken up because of the crash.


text:
How the Arts were Won
By How the Arts were Won
The intersection of politics, culture, and the arts. Hosted by executive Matt Joseph Misetich (Pipeline Media Group) and writer / multi-multi-hyphenate Michelle Daniel.
Ep5 - The Art of 'Art and Life:' A Conversation with Author Nicole Tersigni
How the Arts were Won • By How the Arts were Won • Oct 02, 2022
Ep6 - The Art of NaNoWriMo
Did you know writing 3,000 words a day is harder than it seems? November is National Novel Writing Month (aka NaNoWriMo), which is a rad if you have the time and the motivation and a story idea. This episode features a bonus opening musical number for FREE, so you're welcome.
The Coffee Table Book has evolved. We have proof. Author of 'Men to Avoid in Art and Life' and 'Friends to Keep in Art and Life,' writer and generally humorous Twitterer Nicole Tersigni reveals the origins of her already-popular and soon-to-be-iconic-one-day-if-we-had-to-bet book series.
Ep4 - The Art of Conferences
What a snoozefest topic … but wait! It isn't! Not really anyway! A short but in-depth chat about the current state and future of conferences in the arts. With a metaverse twist and special mystery guest, self-proclaimed "conference junkie" J***** B*******.
Ep3 - The Art of Sport: A Conversation with Jack Baric (GameChange)
There are many parallels between artists and athletes, and--lucky you--we touch upon some of them here for a small but fervent dose of inspiration. Guest: documentary filmmaker and co-founder of the new sports empowerment company GameChange, Jack Baric.
Ep2 - The Art of Open Discourse: On Theater-Going, Acting, and Nepotism
A two-hander with comments on the state of streaming and movies, actors playing roles they "shouldn't" be playing, and biblical levels of nepotism.
Ep1 - The Art of Ambitious Comedy (Part 2)
The second part of Episode 1, where we fall deep in the weeds on the culture of comedy ... Guests: stand-up comics / writers / newly minted playwrights Bret Raybould and Cristian Duran, writers of "Race: The Movie: The Play."
How to be funny in an unfunny world, featuring a special apology to Kellogg's. Guests: stand-up comics / writers / newly minted playwrights Bret Raybould and Cristian Duran, writers of "Race: The Movie: The Play." Swear to God, that's the title.
Ep0 - The Art of First Episodes
Why art is politics, the ennui of Columbus (Indiana), breakfast tacos, a quick word on cancel culture, [redacted content], and a preview of things to come.

redpajama_set_name: RedPajamaCommonCrawl


On behalf of Garton & Harris posted in Power of Attorney on Monday, September 4, 2017.
At times, adult children are asked by their parents to undertake things for which they're unprepared. No one likes to think about the death of his or her parents. But being named power of attorney in British Columbia is a role for which many children are unprepared and one which merits much forethought.
The Baby Boomer generation continues to age, and with that, their children are often called upon to look after things like finances. This is likely when the power of attorney talks happen. Acting as power of attorney isn't always a cut and dry job, and should something go wrong, there can be dire consequences, and litigation could ensue.
Many things can come into play in a power of attorney situation. If dealing with blended families, the division of a parent's estate may involve children and step children. That means the child(ren) named power of attorney will have to work even more diligently to avoid any conflicts of interest.
Abusing the duties of power of attorney is a serious problem and allegation. But after a parent or grandparent has died, the power of attorney is often accused of acting inappropriately by some family members. They may be less than happy with what they have been left.
A power of attorney is often asked to make decisions on behalf of an elderly or incapacitated relative, and those decisions can have a bearing on his or her inheritance and the inheritance of others. For instance, if grandpa's will states one granddaughter is to get his house while her sister gets cash, the will could come into question, and one benefactor could come out with more than another. That could cause strife even though grandpa's wishes were carried out as stated in his will.
People who have been asked to become a power of attorney are well advised to discuss the role with a British Columbia lawyer experienced in wills and estates law. It is better to have questions regarding the legalities of the position answered prior to agreeing to take on the task. Being prepared for the role is better than taking it on without any information.


A missionary's life – like mine – is well-documented. For over thirty years we sent out three or four newsletters annually.
This week I have been perusing some of those letters, writing a history of camping ministry in Bolivia for the 50th anniversary celebration coming up in July.
And at the same time I started gleaning through the brown paper bag of old cards and letters that I wrote to my parents, a bag I picked up in Dallas some years ago. My mom had kept all my letters since I left for college. That was a lot of stuff!
It was interesting to compare the letters, the public ones with the private ones.
The details in the letters to my mom must have bored her at times. I was wordy and repetitive and petty. But I did enjoy reading about my growing children and remembering the minutiae of the small and mostly-happy life that was mine.
I might think How could they have forgotten God's rescuing them out of slavery? Parting the Red Sea? Feeding them miraculously in the desert? How could they forget how he guided them so clearly with fire and cloud?
But then, of course, this week I've been reminded of how forgetful I am.
Our public newsletters report what God did. Buildings completed. Programs fulfilled. Lives changed. Stories we have forgotten.
And my private letters remind me he also did amazing things for little ol' me.
One of those letters told the story of my struggle to readjust to life in Bolivia after a vacation at the Florida beach. I compared the two places, and everything about Bolivia felt like a wilderness.
Those words – 'God led you' . . . 'in the wilderness' . . . 'to humble and test you' – changed me. I saw there was a God-led purpose for me in Bolivia: to test me to see if I would obey him.
I also saw the faith and hope in there.
I remember: I did pass that test. God helped me get out of that crater of complaining.
And he's helped me many times since.
Truly.: God is merciful and forgiving.
I've got lots of letters to prove it.
We understand! And I so appreciate your 'voicing' what I have been thinking lately. Yes, His mercy is amazing! Why do I compare events, or my life vs. "hers" (place name here). God is working in the other one so I can give grace rather than be consimed by envy, discontent, and such. Thank you, Sarah!
Consumed, not consimed….. small keyboard…..
Thank you again Sarah for this wonderful reminder.
God forgive us for not thanking Him enough for all He's done for us.. and is doing for us.. and will do for us! Gifted writing, my friend.
amen sister….i remember our missionary days in the Philippines and can attest to what you're writing. Thanks for the reminder…and isn't that what we just need from time to time in our faith journey? Reminding ourselves of God's faithfulness. Love it sister.


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You are here: Home1 / Featured2 / The Future of the Experimental Music Festival
The Future of the Experimental Music Festival
Dr Paul Rekret, who teaches political theory in the School of Communications and Social Sciences at the University, has recently had an article published on the politics of experimental music for Frieze: https://frieze.com/article/future-experimental-music-festival
In the article, entitled, The Future of the Experimental Music Festival, Dr Rekret takes this year's Wysing Polyphonic music festival as the starting point. He states that a recurring theme of the event, which is held annually on the rural grounds of Wysing Arts Centre in Cambridgeshire, was the intersection of electronic and analogue sound.
Dr Rekret also highlights the Festival's extra-musical aspects, saying, "For the first time in the festival's decade-long existence, Wysing held panel discussions as part of the day-long event. This echoes a wider tendency in recent years for festivals of experimental music to replicate formulas commonly found on the global art circuit, where curated panels, workshops, installations and exhibitions now often appear alongside music programmes assembled under the banner of some nebulous theme."
He concludes, "Music's place in everyday life has shifted in recent years, however, as live venues and nightclubs have been displaced by other modes of music consumption: as an endlessly streamed personal soundscape or as background noise in cafes and bars."
Dr Rekret is also the author of Derrida and Foucault: Philosophy, Politics, Polemics and Down With Childhood: Pop Music and the Crisis of Innocence. In addition to Frieze, his work has appeared in the New Inquiry and the Quietus, among others.
October 21, 2019 /by Alastair Wells
Tags: Art History & Visual Culture (MA), Art History & Visual Culture BA (Hons), Communications BA (Hons), Creative Industries: Visual Arts Management & Curating (MA), Dr. Paul Rekret
https://www.richmond.ac.uk/wp-content/uploads/2014/11/rekret.jpg 2063 2521 Alastair Wells https://www.richmond.ac.uk/wp-content/uploads/2020/10/union-stripes-bound-website.svg Alastair Wells2019-10-21 09:37:352021-04-22 12:15:43The Future of the Experimental Music Festival
Paul Rekret's essay "Affect & Politics: A Critical Assessment" published in new book on Politics and Emotion
Film Screening and Discussion of 'Positive Women, Heartache, Hope and Living with HIV', with Anne Lotter FRAI, co-hosted by IVAC and SPG
Professor of Politics at Richmond analyses leading philosopher's legacy in influential publication
Leading British photographer to hold lecture at Kensington campus
'Socialism: No Man is an Island' talk given by Dr Rafal Soborski in Madrid
Dr Rafal Soborski makes presentation at Political Studies Association workshop
Professor of Politics at Richmond analyses leading philosopher's legacy in... Leading British photographer to hold lecture at Kensington campus


Discussion in 'iOS 10' started by bernardkost, Jul 21, 2016.
What needs to be done to get this feature working on pb2? Option is on in maps settings.
Bluetooth is on. Works just fine. For some reason the feature won't activate. Are there any other settings other than that in the maps that need to be enabled?
I don't think anyone is exactly sure how Apple determines that a bluetooth device is "your car". It may be by device name or device address. That would rely on Apple knowing that your particular device is a car device. I've submitted an enhancement request suggesting a method to allow a user to go into bluetooth settings and identify a bluetooth device as "My Car". That way it will work with any device including 3rd party dongles.
g.fowler, DrewDaHilp1 and Kelowna77 like this.
willmtaylor and cmeisenzahl like this.
Mine worked on the first beta but since then it's stopped working on beta 2 and 3. Everything is turned on.
This has been my experience too, very strange.
I have same problem too, I was working before on iOS 9 (with map and traffic) and I was getting parked location (on beta1) in addition to the traffic map and then it stopped working all of the sudden and it haven't worked yet, but the thing is I wasn't using car bluetooth and it was a usb bluetooth connected to my car usb port and aux, and that usb bluetooth had some random name.
So I don't know what changed and how to turn it back.
Everything also for me is enabled and it doesn't want to work!!!
Thank you for doing this. I use a third party Bluetooth device in my car and it would really enhance my Proactive experience if you could tell iOS which device is your vehicle. I encourage everyone else to make this a feature request as well!!!
CopyChief and darrencp22 like this.
Same here, I have a 2007 Yaris and changed the original radio for a 3rd-party bluetooth device... So far I have no idea how my iPhone can do to tell this is the bluetooth device of my car.
Just think in 2021 you will need to buy an Car for it to work.
willmtaylor and The Merg like this.
Today, I drove an hour and a half away from home today and used Maps for navigation. I noticed that my car was listed on the map as "Parked Car" even though I didn't get a notification. So maybe they changed the implementation to no longer notify you; although it could just be a bug. Something to check for those of you who were experiencing what I was.
Bluetooth has little to nothing to do with the functionality. 'Maps' just checks if you stopped driving and tries to remember the location, that's it.
You are wrong, bluetooth is the main thing in this, if you don't have any bluetooth connection, you can drive anywhere you want with the map, but it won't tell you where you park.
Bluetooth here is the trigger for the map to when it connect to it, know that you are with your car, and not getting ride with someone else or anything else, and then when it disconnect, get the gps info and save the location.
That's how this feature work.
that's correct - it states this fact when you turn the feature on. it would be annoying to know where the buss is parked.
I agree. There should be a way to mark third-party devices as "My car" so this feature will work in more cars. It works perfectly with my wife's car, which is newer and has a built-in system. However, with my car, which has a third-party bluetooth receiver hooked up to the AUX port, it doesn't work.
Incidentally, you can trigger it manually (if you want) when you get out of your car. Just tell Siri, "Remember where I parked my car."
Kelowna77 and HopefulHumanist like this.
Well that's still in beta, cause back when I had the beta 1, it was working with third party bluetooth and was ok and after that beta 1 didn't work anymore.
edit: Fixed mine so others may want to try I deleted and repaired the car stereo. Now working. Still glitchy. First said my car was 50 ft then when I got in the car said it was 100 ft away.


Water loss from, or water ingress into a wide variety of structures is a common problem….
… and one that Ram Services Limited have been using structural leak sealing techniques to deal with for over 30 years.
We have developed techniques for a wide variety of leak sealing requirements. These use a variety and combination of caulking compounds and injected cementitious, epoxy, polyurethane and acrylic resin grouts.
Leak sealing work is often carried out in a confined space working environment, and utilises a variety of conventional and specialist plant.
Other measures are available to effectively deal with leaks through mechanical expansion joints of car parks and bridges, through joints in water retaining structures subject to large movements and in large diameter pipe joints.


text:
\section{Introduction}

The current cosmological paradigm postulates that large galaxies formed
from the hierarchical aggregation of smaller ones \citep[e.g.,][]{wr78}.
Within this context, a galaxy such as the Milky Way (MW) is expected to
have an assembly path where infall, mergers, and interactions
contribute, with their different relative importance influenced by the
local environment. Cosmological simulations are the most suitable tool
to describe this complex history of formation, and to confront the
adopted cosmological scenario and baryonic sub-grid models with
observations. Sophisticated numerical codes have been developed over the
past few years, and they are continuously being updated to improve their
representation of different physical processes \citep[e.g.,
][]{sprin2005,stin2006,scan09, schaye2011, guedes2011,brook2012}. In
particular, the treatment of chemical evolution within cosmological
codes provides a powerful tool for exploring galaxy formation, and to
confront models and observations \citep[e.g.,][]{mosc2001, lia2002,
gove2007}. In this regard, stellar haloes, such as those of the MW and
M31, are valuable laboratories for confronting expectations from
cosmological models, since most of their stars are quite old, and were
born in the first epochs of galaxy formation. Their chemical abundance
patterns, preserved basically unchanged over their long lifetimes,
provide a fossil record of the physical characteristics of the
interstellar medium at the time and place of their birth \citep[e.g.,
][]{freeman}. We also acknowledge the need to better develop the sets of
questions to be posed to models, so that their full utility for
exploration of the expected behaviour of actual galaxies can be
realized. In this paper, we make a first effort in this direction.

Recent observations provide evidence that the MW halo system comprises
at least two overlapping stellar components, an inner-halo population
and an outer-halo population, with different metallicities, kinematics,
and spatial density profiles \citep[see, e.g., ][]{caro2007,caro2010,
dejong2010,jofre2011,beers2012,kin2012,an2013,hat2013,kaf2013}. These
findings suggest a dual history of halo formation, with contributions
from stars accreted from lower-mass sub-galactic systems and those formed
\insitu. Important additional information on the nature of the halo of
the MW has begun to emerge from consideration of the chemical abundances
of the light and heavy elements. For example, \citet{caro2012} have
shown that clear differences exist between the frequencies of the
so-called carbon-enhanced metal-poor (CEMP) stars that they
kinematically associate with the inner- and outer-halo populations. They
also present evidence for the existence of a correlation between the
frequency of CEMP stars and distance from the Galactic plane, a result
which is difficult to understand in the absence of (at least) a dual
halo. \citet{roederer2009} has argued that kinematically separated
members of the inner- and outer-halo population exhibit a mean [Mg/Fe]
ratio for the outer halo that is lower than that of the inner halo, by
about 0.1 dex. He also demonstrated that the star-to-star scatter in
[Ni/Fe] and [Ba/Fe] for stars associated with the inner halo is
consistently smaller than that of the outer halo. The existence of
different stellar populations located within the inner-halo region of
the MW has recently emerged from studies of the $\alpha$-elements
\citep[e.g., ][]{nissen2010, sheffield2012}. Clearly separable
correlations have been shown to exist between [$\alpha$/Fe] and [Fe/H]
(`high-$\alpha$' and `low-$\alpha$' sequences), as well as with
kinematics. Most recently, \citet{schuster2012} have extended these
differences to include ages.

State-of-the-art observations are also providing information on the
stellar haloes of nearby galaxies. The nature of the stellar halo of M31
has only recently become feasible to explore in detail, due to
large-scale surveys enabled by modern detectors as well as deep Hubble
Space Telescope observations\citep[e.g.,][]{saraje2012,williams2012}.
Sarajedini et al. presented evidence that the M31 spheroid possesses a
bimodal metallicity distribution, similar in many ways to that suggested
by \citet{caro2007, caro2010} to apply to the MW. In addition, M32 has
been reported to exhibit different spheroid populations, with the outer
one being $~ 1.3$ Gyr older and $\sim 0.2 $ dex more metal poor than its
inner halo \citep{brown2007}.

From a theoretical point of view, cosmological simulations of galaxy
formation within the concordance $\Lambda$-CDM model have also made
progress in the description of the formation history of stellar haloes.
\citet{zolo2009} showed a dual history of formation for stellar haloes,
with contributions from both accreted sub-galactic systems and \insitu star
formation, the latter principally located in the central regions of the
haloes. More recently, similar findings have been reported by
\citet{font2011}, \citet{mcc2012} and \citet{tissera2012},
through the analysis of stellar haloes in simulated galaxies using a
variety of numerical codes and sub-grid physics models. Considering
the different approaches used for the baryonic sub-grid models among
these cosmological codes, it is noteworthy that they all agree on
suggesting a dual formation history for the stellar haloes, in the sense
that they are formed by the combination of stars born \insitu and in
accreted sub-galactic systems. This simple way of describing a complex
assembly process, which depends strongly on the galaxy evolutionary
path, has been successful at illustrating the global picture. To move
forward, in this work we aim at studying in more detail the origin of
each different stellar populations that form the diffuse haloes in a
$\Lambda$-CDM scenario.

The results discussed in this paper are related to those reported by
\citet[hereafter, Paper I]{tissera2012} who analysed the chemical
properties of galaxies formed in eight MW mass-size systems of the
Aquarius Project, with different assembly paths within the $\Lambda$-CDM
scenario \citet{scan09}. Paper I shows that, although the central
regions of these simulated galaxies and their stellar haloes are
dominated by very old stars, their chemical properties differ as a
consequence of their individual formation histories. The former were
dominated by \insitu star formation, the latter were assembled mainly
from small accreted sub-galactic systems. Although the mass scales and time
scales involved resulted in different chemical patterns at $z=0$, these
simulations successfully reproduced the global chemo-dynamical trends
observed in the MW.

Following Paper I, we adopt binding energy criteria defined to
dynamically separate two stellar halo populations without any
assumptions on the chemical abundances or kinematics of the stars.
Hereafter, to clarify the description of our results, the most
gravitationally bound stars, dynamically associated with the so-called
inner haloes, will be referred to as inner-halo populations (IHPs), while
the less bound stars, associated with the so-called outer haloes, will
be referred to as outer-halo populations (OHPs). Note that, as the
separation of these stellar components is performed on the basis of
their binding energy content, the IHPs and OHPs can be spatially
superposed. We thus also distinguish these spatial differences by
referring to the inner-halo regions (IHRs) and outer-halo regions
(OHRs); the relative dominance of the different stellar populations
found within these regions naturally differs from one simulated galaxy
to the next, depending on its formation history. The IHR and OHR
  are defined by the spatial distributions of the IHPs and OHPs. The
  crossing radius between the density distributions of these two
  populations  is $\sim 20$ kpc
  (Tissera et al., in preparation).

To understand their history of assembly, we classify the stars in the
IHPs and OHPs into three sub-populations according to their sites of
formation:

 (1) {\it debris} stars are formed in separate sub-galactic systems
  located outside the virial radius of the main progenitor
   galaxies\footnote{We define the main galaxy as the most massive
     galaxy within the virial radius at $z=0$, and its main progenitor as the most
   massive sub-galactic system from where it formed, as a function of
   redshift.} at the time they were born, and were later accreted onto
   the main galaxy (i.e. stars from dry mergers
as well as the existing populations from wet mergers),

 (2) {\it disc-heated} stars are formed in the disc structure of the
 main progenitor galaxies, then heated up
by some violent event, and

(3) {\it endo-debris} stars are those formed
in gas-rich sub-galactic systems  located within the virial radius of the
  main progenitor galaxies at their time of formation (i.e. wet mergers).

 In  Paper I, disc-heated and
endo-debris stars were classified as the \insitu component.  In
  this paper, we
distinguish them as separate sub-populations because, at least in our simulations, they exhibit
different properties which might help link observations with
galaxy formation models.  We note that
  endo-debris stars could be taken either as part of  the \insitu population, because they
  formed within the virial radius of the main progenitor galaxy, or as
  part of the
  debris population, because they were born from gas associated with
a sub-galactic system. Although we analyse the three sub-populations
separately, when required and to be consistent with Paper I, we adopt the
former interpretation.
Note that we have cleaned our haloes from
bound substructures that could be isolated in density phase. These
substructures will be considered in a separate paper.

This paper is organized as follows. In Section 2, we describe the
simulations and the main aspects of our chemical-enrichment model. This
section also explains the criteria adopted to separate different stellar
components. In Section 3, we study the chemical and kinematic properties
of the different stellar sub-populations contributing to the IHPs, In
Section 4, we discuss the nature of the OHPs. We summarize our findings
in Section 5.

\section{The simulated Milky Way-like systems}

We analyse a suite of six high-resolution simulations of MW galaxy-sized
systems of the original sample from the Aquarius Project,  which include the physics of baryons as described by
\citet{scan09}. We first
selected six out of the eight cases discussed by \citet{scan09}, because two
haloes experienced important mergers in the recent past, unlike in the
MW. The six selected haloes (A, B, C, D, G and H) have surviving discs
of different bulge-to-total mass ratios \citep[see][ and Paper
I]{scan11}.

The target haloes were selected from a cosmological volume consistent
with a $\Lambda$-CDM cosmogony, with parameters $\Omega_{\rm m}=0.25,
\Omega_{\Lambda}=0.75, \sigma_{8}=0.9, n_{s}=1$ and $H_0 = 100 \ h \ { \rm km s^{-1}
Mpc^{-1}}$, and $h =0.73$  \citep[see][]{sprin2008} for further details on
the generation of the initial conditions). The simulations were run with
a version of {\small GADGET-3} \citep{sprin2005}, which includes a
multiphase medium, SN energy feedback, and chemical evolution, as
described in \citet{scan05, scan06}. Maximum gravitational softenings in
the range $\epsilon_{G} =0.5 - 1$ kpc $h^{-1}$ were adopted. Virialized
structures are identified by requiring the mean overdensity to reach
$\approx 200$ times the cosmological critical density. The simulated
haloes have $\approx 1$ million total particles within the virial
radius, and a virial mass in the range $\approx 5 - 11 \times 10^{11}
{\rm M_\odot} h^{-1}$ at $z=0$. Dark matter particles carry masses on
the order of $\approx 10^{6}{\rm M_\odot }h^{-1}$, while, initially, gas
particles possess a total mass of $\approx 2 \times 10^{5}{\rm M_\odot}
h^{-1}$. Their characteristic parameters are summarized in table 1 and
table 2 of \citet[see also Scannapieco et al. 2009]{tissera2010}.

\subsection{The numerical code}

The version of {\small GADGET-3} used to run these simulations includes
a multiphase model for the gas component, metal-dependent cooling, star
formation, and SN feedback, as described in \citet{scan05} and
\citet{scan06}. These multiphase and SN-feedback models have been
used to successfully reproduce the star-formation activity of galaxies
during quiescent and starburst phases, and are able to drive violent
mass-loaded galactic winds with a strength reflecting the depth of the
potential well \citep{scan06, dero10}. This physically-motivated thermal
SN-feedback scheme does not include any ad hoc mass-scale-dependent
parameters, and has no requirement to switch off cooling or provide a
dynamical ``kick'' to other particles. As a consequence, it is
particularly well-suited for the study of galaxy formation in a
cosmological context.

Our chemical evolution model includes the enrichment by Type~II and
Type~Ia Supernovae (SNII and SNIa, respectively). A Salpeter Initial
Mass Function is assumed, with lower and upper mass cut-offs of 0.1
${\rm M_{\odot}}$ and 40 ${\rm M_{\odot}}$, respectively. We follow 12
different chemical isotopes: H, $^4$He, $^{12}$C, $^{16}$O, $^{24}$Mg,
$^{28}$Si, $^{56}$Fe, $^{14}$N, $^{20}$Ne, $^{32}$S, $^{40}$Ca, and
$^{62}$Zn. Initially, baryons are in the form of gas with primordial
abundance, X$_{\rm H}=0.76$ and Y$_{\rm He}=0.24$.

SNII are considered to originate from stars more massive than 8 ${\rm
M_{\odot}}$. Their nucleosynthesis products are adopted from the
metal-dependent yields of \citet{WW95}. The lifetimes of SNII are
estimated according to the metal-and-mass-dependent lifetime-fitting
formulae of \citet{rait1996}. For SNIa, we adopt the W7 model of
\citet{thie1993}, which assumes that SNIa events originate from CO white
dwarf systems in which mass is transferred from the secondary to the
primary star until the Chandrasekhar mass is exceeded, and an explosion
is triggered. For simplicity, we assume that the lifetime of the
progenitor systems are selected at random over the range $[0.7, 1.1]$
Gyr. To calculate the number of SNIa, we adopt an observationally
motivated relative ratio of SNII to SNIa rates, as explained by
\citet{mosc2001}.

The ejection of chemical elements is grafted onto the SN-feedback model,
so that chemical elements are distributed within the cold and hot gas
phases surrounding a given star particle. The fraction of elements going
into each phase is regulated by a free parameter, $\epsilon_{\rm c}$,
which also determines the amount of SN energy received by each phase.
While the injection of energy follows two different paths, depending on
the thermodynamical properties of the gas, chemical elements are
injected simultaneously with the occurrence of the SN event. All of
these simulations were run with $\epsilon_{\rm c}=0.5$.

\begin{table*}
 \begin{center}
\caption{ Median Abundances of  IHPs and OHPs. First column shows
the encoding name of the simulations. The percentage of stellar
mass, median [Fe/H] and median [O/Fe] for stars identified as
disc-heated, endo-debris and debris sub-populations.  }
\label{tab1}
\begin{tabular}{|l|ccccccccccccccc}\hline

{Systems}   & \multicolumn{9}{c}{ IHPs} & \multicolumn{6}{c}{ OHPs}\\
               & \multicolumn{3}{c}{ Disc-heated}& \multicolumn{3}{c}{   Endo-debris} &\multicolumn{3}{c}{ Debris} & \multicolumn{3}{c}{Endo-debris} &\multicolumn{3}{c}{ Debris}\\
               & \% &   [Fe/H]&[O/Fe] &  \% &   [Fe/H]&[O/Fe] & \% &   [Fe/H]&[O/Fe] & \% &   [Fe/H]&[O/Fe]& \% &   [Fe/H]&[O/Fe]\\\hline
Aq-A-5&	31  &  -1.11  &  0.18 &   41 &-1.26  & -0.10   &   25 &-1.45&0.35 & 20 &  -1.94& 0.02& 80 & -1.42 &   0.18  \\
Aq-B-5& 3  & - &- &  29 &  -1.34 &    0.01  &   67 & -1.22   & 0.15 & 12 &    -1.31&  0.02 &88&-1.67&     0.19\\
Aq-C-5& 24 &  -0.78 & -0.05  &32 &-1.37 &   0.01 &   44 &-1.20 &  0.31 &  21 &     -1.90&  0.05 &79&-1.29&     0.12\\
Aq-D-5&	26& -0.90  & -0.06  &  30 & -1.28 &  -0.09 &  43&-1.02 &  0.16 & 24  &     -1.75&   0.02&76 &-1.32&     0.15\\
Aq-G-5 & 35 &-0.90 &  0.00 &  23 & -1.21   & 0.07  &41   &-1.00 &   0.07& 5&  -1.57&  0.02 & 93&-1.81&   0.18\\
Aq-H-5 & 18 & -0.80 &   0.02  & 35 &-0.74 &   -0.14 &45  &-0.86&0.16& 29&     -1.16&   0.02&   71 &-1.17&     0.10 \\
\end{tabular}
   \end{center}
\end{table*}

\subsection{The simulated Aquarius galaxies}

In order to analyse the chemical properties of the stars, and to relate
them to the assembly history of the final galaxy, Paper I defined
different dynamical components by using the binding energy ($E$) and
angular momentum content along the rotational axis, $J_{z}$. Discs are
defined by those particles with $J_{z}/J_{z, \rm max(E)} > 0.65$ , where
$J_{z, \rm max(E)}$ is the maximum $J_z$ over all particles of a given
binding energy $E$. The rest
of the stellar particles are taken as part of the spheroidal component.
Taking into account their binding energies, stellar particles are
classified as belonging to the central spheroid (`bulge') or the inner
and outer haloes, so that more energetic particles end up in the halo
systems while the less energetic particles define the central spheroids.
Although the classification of stars belonging to the inner and outer
haloes is made on the assumption of a certain binding energy (as
explained in Paper I), variations of this limit only weakly affect our
results, if these variations are sensible.
By applying this methodology, the dynamical decomposition of the stellar populations of the main
  progenitor galaxies into discs, central spheroids, IHPs and OHPs
  was performed from $z\approx 4$ to $z =0$ for all of the Aquarius simulated systems.
 We also cleaned the stellar
haloes of substructure, as defined by the SUBFIND algorithm, so that the
analysed stellar haloes correspond to the diffuse components in density
space.

As shown in Paper I, the different dynamical components receive
contributions from stars formed both {\it in situ} and in
sub-galactic systems that were later accreted into the potential well of the
progenitor systems.   As defined in the Introduction,  the \insitu
component is split into two categories: the disc-heated and endo-debris
sub-populations.
The latter are formed in  gas-rich sub-systems which could
  survive farther into the dark matter haloes and
continued their star formation activity. New
stars formed in this environment would be more chemically enriched by
SNIa than older ones, particularly if these sub-galactic systems had bursty
star formation histories.
The fractions of each stellar  sub-population (debris, endo-debris
  and disc-heated) associated with each dynamical
component (IHP or OHP) is different, and varies from system-to-system, depending on
their history of assembly.

Paper I also demonstrated that the OHPs are mainly formed from debris
stars, along with a small fraction of \insitu stars. In order to
understand the origin of these stars, we followed each of them back in
time, and identified the first sub-galactic system that hosted them. We
found that most of the stars that were originally classified as \insitu
stars were in fact formed {\it in between} available snapshots of the
simulations, which complicated their detection. From seeking the
original gas particles in which they formed, it is clear that most of
them were part of small sub-galactic systems. A negligible fraction of
the stars (and their progenitor gas particles) could not be related to
any system, but all of them are old, with formation redshift $z > 5$. At
such high redshifts, our simulations do not possess sufficient
resolution to reliably follow the evolution of the smallest
clumps, so we include them within the endo-debris populations.
Thus, we will hereafter consider that the OHPs are built up mainly by
debris stars from accreted sub-galactic systems,  with  a small
fraction  corresponding to endo-debris stars.

A similar analysis was carried out for the \insitu stars in the IHPs. We
found that these stars included endo-debris sub-populations as well as
disc-heated stars. The latter are stars formed in the disc components,
but that were heated sufficiently to become part of inner haloes by $z
\sim 0 $, contributing from $\sim 3 \%$ to $\sim 30 \%$ of the IHPs.
Disc-heated stars are defined by checking if  they were
  formed from cold gas which was part of  the disc component of the
  main progenitor galaxy at the time they were born.
To do that we traced each star particle back in time, and examined to
which dynamical component it belonged at that time. This was possible because we
defined disc and halo components at every available snapshot of the
simulations, as discussed above.
These fractions are in agreement with the recently reported $\sim 20\%$
of disc-heated stellar fraction estimated for the MW halo by
\citet{sheffield2012}. Endo-debris stars contribute $\approx 30 \%$
of the IHPs, on average, and include a small fraction of stars which
could not be identified as belonging to any sub-galactic system (neither
could their gaseous progenitors). We also checked for possible
contamination of the IHPs from very extended thick-disc populations, by
relaxing the condition for particles to be classified as part of the
disc components at $z=0$, assuming $J_{z}/J_{z, \rm max(E) } > 0.5$. No
significant differences were found.

In the following sections we analyse the chemical and dynamical
properties of the IHPs and OHPs, as populated by contributions from the
three different sub-populations: debris stars, disc-heated stars, and
endo-debris stars. Table \ref{tab1} summarizes the percentage of stars
in each sub-populations and their median abundances. We emphasize that, at any given time (owing to their
extended orbits), stars that are members of the IHPs and OHPs can occupy
the same spatial regions (both the IHR and the OHR), with different
relative fractions at different distances from the centre.  We perform
an analysis and further discuss this important point, and its consequences,
in Tissera et al. (in preparation).

\section{The diffuse IHPs}

As discussed above, our simulated IHPs are complex structures, with
contributions from disc-heated stars, as well as from the debris and
endo-debris stellar sub-populations. The debris sub-population is the
primary contributor, with an average of $\sim 45 \%$ across the six
simulated haloes, while the endo-debris and disc-heated sub-populations
each contribute $\sim 25 \%$ to  $\sim 30 \%$ , on average.

To better visualize the global differences between the IHPs in our
simulated galaxies, Fig. ~\ref{toomregeneral} (left panel) shows the
Toomre diagram defined by the median velocities, with each of the
contributing sub-populations marked.   Following \citet{mcc2012},
 the velocity coordinates $U, V$, and $W$ are estimated in the
  rest frame of fiducial Solar Neighbourhoods defined for  the stellar disc
  component of the simulated galaxies.
 The rest frames are defined by estimating
  the mean velocity components for stars in the stellar discs at
  $\approx 8$ kpc.  Velocities are normalized to the median rotation
  velocity of the disc, V$_{\rm LSR}$, in the fiducial Solar Neighbourhoods,
in order to consider the
  differences in mass between the simulated galaxies. Hence, the limit
  between retrograde and prograde motions is set at $-1$.
 As can be seen from inspection of this figure, the
debris and endo-debris sub-populations exhibit, on average, little
evidence for strong rotation. Typically, disc-heated stars exhibit
different kinematics; most are more rotationally supported than the
stars in the other two sub-populations.  However, there exist an
important subset of disc-heated stars
which cannot be distinguished from debris or endo-debris stars. In fact,
there is a clear age dependence on the behaviour of the disc-heated
stars -- old disc-heated stars ($> 10$ Gyr; open circles) do not show
significant rotational velocities, while  younger stars ($< 10$ Gyr; filled circles)
exhibit clear signals of rotation. Note that, in these
simulations, young disc-heated stars are nevertheless older than $\sim
8$ Gyr \footnote{It is worth mentioning that the simulated discs at $z
  =0$ are
  dominated by young stars as shown by \citet{tissera2012}. However,
  discs contributed with heated stars to the IHPs  mainly
  at $z > 1$. For this reason, the disc-heated stars found
  in the IHPs are older than $\sim 8 $ Gyrs.}. In the case of Aq-A-5, a fraction of old disc-heated stars
actually exhibit retrograde rotation, illustrating the complexity and
diversity of halo assembly in a hierarchical clustering scenario.

Due to the time delay between the corresponding evolution of the
progenitor stars of  SNII and SNIa, the $\alpha$-element-to-iron ratios provide
information about the star-formation history of the systems. Fig.
~\ref{toomregeneral} (middle panel) shows the median [O/Fe] vs. [Fe/H]
for the IHPs, segregated into the different stellar sub-populations. On
average, debris stars are $\alpha$-enriched relative to iron.
However, we also find a number of stars with low [$\alpha$/Fe] ratios,
varying from $7\%$ to $35\%$, evidencing contributions from SNIa. The
fraction of such stars correlates with the mass of the accreted
sub-galactic systems, so that the larger fractions are found in  IHPs
that formed from more massive systems. The endo-debris and disc-heated
sub-populations have a larger fraction of low (or even sub-solar)
[$\alpha$/Fe] ratios. The stellar sub-populations also occupy different
locations in the  [O/Fe] vs [Fe/H] plane. Debris stars are metal poor, and have the
smallest contribution from low-[$\alpha$/Fe] stars. Endo-debris stars
have lower mean [$\alpha$/Fe] ratios. The disc-heated stars tend to
exhibit, on average, both higher metallicities and lower [$\alpha$/Fe]
ratios compared to the other sub-populations. As expected, this is
particularly true for the younger disc-heated stars.

We found that, on average, $55\%$ of the $\alpha$-enriched stars in IHPs
belong to the debris sub-components, while disc-heated stars and
endo-debris stars contribute, individually, on the order of $20-25\%$ of
the total mass fraction of $\alpha$-enriched stars, on average.
Observationally, there is evidence for the existence of halo stars with
low $\alpha$-enrichment \citep{nissen2010, sheffield2012}, although
their frequency is not yet clearly determined. The endo-debris
sub-populations in the IHPs could be associated with the low-$\alpha$ and
low [FeH] stars classified as the accreted stars by
\citet{sheffield2012}.  In the middle panel of
  Fig. ~\ref{toomregeneral}, we show the observations of  \citet{sheffield2012}
  superposed with the median values estimated for the three
  sub-populations in our  simulated IHPs\footnote{The differences in the estimators used for observations and simulations
 could explain in part the narrow range of metallicities covered by the
simulated data compared to the observations in this figure. The lack of very high metallicity stars in
the simulations could be also related to the action of very efficient mass-loaded simulated galactic winds
 or to  a different evolutionary
path for the MW compared to those of our simulated systems. It is beyond the scope of this paper to carry out a detailed comparison with the MW.}.
Observations of the [$\alpha$/Fe] abundance ratios for large, unbiased
samples of MW halo stars will provide very important constraints on
galaxy formation models. According to our present models, such
measurements would be a probe of the complex mixture of stellar
sub-populations in the inner haloes of large spiral galaxies such as the
MW and M31. Testable predictions of various formation and evolution
scenarios could then be made from which models can be revised and
improved.

With respect to the mean rotational velocities, the $\alpha$-enriched
stars followed the same mean trends of their corresponding
sub-populations -- those belonging to the debris or endo-debris
sub-populations exhibit little or no net rotation with respect to the
galactic centre in the range $ [-15,15]$ km s$^{-1}$, while those
classified as disc-heated stars tend to exhibit clear prograde rotation
($\sim 50$ km s$^{-1}$), particularly the younger stars. The
$\alpha$-rich stars tend to be $1-2$ Gyr older than $\alpha$-poor stars.
A portion of the latter coming from the disc components can be up to 1
Gyr younger.

\begin{figure*}
\hspace*{-0.2cm}\resizebox{5.5cm}{!}{\includegraphics{toomre_general1halo.ps}}
\hspace*{-0.2cm}\resizebox{5.5cm}{!}{\includegraphics{ofesheffield.ps}}
\hspace*{-0.2cm}\resizebox{5.5cm}{!}{\includegraphics{ofevtan_halo.ps}}
\caption{ Median rotation velocities for stars in the simulations assigned to the IHPs,
displayed as the Toomre diagram (left
panel), [O/Fe] versus [Fe/H] (middle panel), and [O/Fe] versus rotation
velocity for the averaged stellar sub-populations for each of the six
simulated haloes, encoded according to: debris stars (diamonds),
endo-debris stars (triangles), old disc-heated stars ($> 10$ Gyr; open
circles) and young disc-heated stars ($8-10$ Gyr; filled circles).
The vertical dashed lines in the left and right
panels denote the limit between prograde and retrograde rotation with
respect to the corresponding galactic disc in each simulation.  The
horizontal dashed lines in the middle and right panels indicate the
solar abundance ratio for [O/Fe]. Note that only five symbols are
included for the disc-heated stars since Aq-B-5 has a negligible
contribution of this sub-population.
 In the middle panel, we show the
observations from \citet{sheffield2012} for a sample of individual
stars in the Solar Neigbourhood (violet points and errorbars). Note
that for the observed sample, each point represents the properties
of individual stars while
for the simulated data, median estimations over the sub-populations
are included.
 }
\label{toomregeneral}
\end{figure*}

\begin{figure*}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{Ebinagehalo_Aq-A-5.ps}}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{Ebinagehalo_Aq-B-5.ps}}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{Ebinagehalo_Aq-C-5.ps}}\\
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{Ebinagehalo_Aq-D-5.ps}}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{Ebinagehalo_Aq-G-5.ps}}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{Ebinagehalo_Aq-H-5.ps}}
\caption{Age versus binding energy for the IHPs associated with each of
our simulated haloes. Stars
are coloured according to their assigned sub-population:
debris stars (black), endo-debris stars (magenta) and disc-heated stars (green).
For the sake of clarity, we only show $\sim 30\%$ of the total sample. }
\label{ages}
\end{figure*}

Fig. ~\ref{ages} shows the ages of the IHPs, as a function of
binding energy, for the three different stellar sub-components. The
debris stars are the oldest, and they span the entire range of total
energies. These stars are among the first ones to be formed; as a
consequence, they are primarily low metallicity and $\alpha$-enriched
relative to iron (as can be appreciated from inspection of
Fig.~\ref{toomregeneral}). The endo-debris stars tend to be slightly
younger, and relatively more gravitationally bound. They formed in
gas-rich satellites accreted at $z > 3$; $50\%$ of them were formed
in sub-galactic systems with dynamical masses smaller than $10^{8.5} $
M$_\odot$.  On average, these stars have a larger fraction of low
$\alpha$-enrichment when compared to the debris sub-populations. As
mentioned before, there are two distinctive regions occupied by
disc-heated stars -- the most tightly bound stars tend to be older and
$\alpha$-enriched, while the younger disc-heated stars extend to higher
energies and are more $\alpha$-poor.

Our IHPs comprise primarily very old stars, with more than $50\%$ older
than 10 Gyrs (a lookback time comparable to redshift $z \approx 2$),
while, on average, only $\sim 5\%$ of them are younger than $\sim 7.5$
Gyrs ($z \approx 1$). Most of the latter stars are disc heated. As
mentioned above, the oldest stars tend to dominate at higher energies,
thus the proportion of old and young stars might be expected to vary
with galactocentric distance. Observations of stellar populations in
galactic haloes at higher redshifts should help to constrain their
assembly \citep{trujillo2012}.

\subsection{[Fe/H] profiles of the diffuse IHPs}

The different chemical abundances and binding energy distributions of
the stellar sub-populations can imprint differences onto their
metallicity distribution profiles, which, in turn,  provides information
on the relative contributions of each of the sub-populations.
Previous works have examined the metallicity profiles of their simulated
stellar spheroids as a whole (i.e., central spheroids, inner and outer
stellar haloes; Font et al. 2011), or looked at the difference between
the inner and the outer stellar haloes \citep{tissera2012}, and reported
that these simulations, within the concordance $\Lambda$CDM scenario,
are able to reproduce metallicity trends similar to those reported by
observers for the MW and M31 (see Introduction for a discussion on this
point).

Fig. ~\ref{gradhaloes} shows the [Fe/H] profiles of the disc-heated,
endo-debris, and debris stars, as well as the total
profiles. The abundance profiles represent the median [Fe/H] estimated  in equal-size radial
intervals (displayed medians have been estimated with at
least 100 stellar particles). The total metallicity
profile is clearly a combination of the contributions from each of the
sub-populations, the relative importance of which varies from
galaxy-to-galaxy. The resulting metallicity profiles depend on both the
level of enrichment of the different stellar sub-populations, and their
final spatial density distributions. The latter has been included in the
corresponding insets of Fig. ~\ref{gradhaloes}. Hence, although each of
these sub-populations may exhibit weak gradients individually, when they
are combined, the outcome could be a steeper profile. In fact, in some
cases, there exists a sharp transition between the region dominated by
the \insitu sub-populations (i.e., disc-heated plus endo-debris stars)
and that dominated by the debris sub-population. In such cases, fitting a
simple linear relation might provide spurious results. Consequently, we
prefer to understand the characteristics of the metallicity profiles by
analysing the spatial and binding energy distribution of each stellar
sub-population. This allows us to assess the role played by each
sub-population in shaping the final abundance profiles of the IHPs. The
eventual aim is to make use of such profiles (or quantities derived from
them) as tools for describing the assembly histories of individual
galaxies.

From inspection of Fig.~\ref{gradhaloes}, there are three IHRs that
exhibit steeper variations of [Fe/H] with distance than the rest. In
these cases, the \insitu sub-components (disc-heated stars and/or
endo-debris stars) are more centrally concentrated with respect to the
debris sub-populations. In the cases with flat [Fe/H] profiles, the
three stellar sub-populations are better mixed. This can be seen from
the inset of Fig. ~\ref{gradhaloes}, where we display the spatial
distributions of the three different stellar sub-populations in the six
analysed haloes. It is clear that Aq-A-5, Aq-C-5, and Aq-G-5 have their
\insitu stars more concentrated toward lower energies (see Fig.
~\ref{ages}) and the central regions with respect to the debris stars.
Since the disc-heated stars and, in some cases, the endo-debris stars,
have higher metallicities in the central regions than debris stars, the
abundance profiles are steeper. It can be also seen that the debris
stars dominate at larger distances.

According to our simulations, a steep [Fe/H] profile is the result of
poorly mixed sub-populations, with significant contributions from either
disc-heated stars, endo-debris stars, or both, in the central regions.

\begin{figure*}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{sigma_feh_newhaloAq-A-5.ps}}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{sigma_feh_newhaloAq-B-5.ps}}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{sigma_feh_newhaloAq-C-5.ps}}\\
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{sigma_feh_newhaloAq-D-5.ps}}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{sigma_feh_newhaloAq-G-5.ps}}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{sigma_feh_newhaloAq-H-5.ps}}
\caption{Abundance profiles for stellar
sub-populations assigned to the IHPs of our six simulated haloes
(black lines). The so-called \insitu component, made up of disc-heated stars  (green lines)
and endo-debris stars (magenta lines),
tends to be located in the central regions and to be dominated by low
binding energy particles. The debris stars (violet  dashed lines)  are more uniformly distributed with
distance, and as a consequence, dominate at larger radii. The total
abundance profiles are shown in black lines. The inset shows the
spatial distribution of the three sub-populations.
 }
\label{gradhaloes}
\end{figure*}

\section{The diffuse OHPs}

The OHPs in our simulated halo systems comprise stars older than $\sim
11$ Gyr, which are very metal poor and $\alpha$-enriched relative to
iron. They formed from the accretion of satellite systems, so that most
of the stars belong to the debris sub-population. There is a small
fraction of stars that originated from an endo-debris sub-population
(which were in part classified as \insitu in Paper I; see see Section
2.2).

Regarding the kinematics, we find that most of the OHPs
exhibit low net global rotation with respect to their corresponding galactic
centres, with mean values in the range $<V_\phi > \sim 20-25 $ km
s$^{-1}$. One of the six OHPs (Aq-G-5) has a mean $<V_\phi > \sim 7 $ km
s$^{-1}$, and another (Aq-C-5) exhibits a retrograde net rotation
$<V_\phi > \sim -33 $ km s$^{-1}$. At least in our simulations, the
stars are very well-mixed dynamically, so no significant differences in
the Toomre diagram could be found between the debris stars and the
endo-debris stars, or between the low- and high-[$\alpha$/Fe]
sub-populations (left panel of Fig. ~\ref{toomrehaloex}).

The middle panel of Fig. ~\ref{toomrehaloex} shows the [O/Fe] versus
[Fe/H] plane for the debris and endo-debris sub-populations. It is very
clear that the endo-debris sub-populations exhibit a larger contribution
from low-[$\alpha$/Fe] stars, on average. However, there is no trend
with rotational velocity, as can be seen from the right panel of Fig.
~\ref{toomrehaloex}. The existence (or absence) of such stars might be
tested with observations; their frequency could provide strong
constraints on galaxy-formation models and on how the star-formation
activity proceeded in small systems at high redshift. Note that
most of the stars in the OHPs are located outside the Solar Neighbourhood; less
than $\approx 10\%$ can be found within this region (Tissera et al. in
preparation), thus caution should be taken when compared to available
observational surveys.

\begin{figure*}
\hspace*{-0.2cm}\resizebox{5.5cm}{!}{\includegraphics{toomre_generalhaloexhalo.ps}}
\hspace*{-0.2cm}\resizebox{5.5cm}{!}{\includegraphics{ofehfeh_haloex.ps}}
\hspace*{-0.2cm}\resizebox{5.5cm}{!}{\includegraphics{ofevtan_haloex.ps}}
\caption{Median rotation velocities for stars in the simulations assigned to the OHPs,
displayed as the Toomre diagram (left
panel), [O/Fe] versus [Fe/H] (middle panel), and [O/Fe] versus rotation
velocity for the averaged stellar sub-populations for each of the six
simulated haloes, encoded according to: debris stars (diamonds) and
endo-debris stars (triangles).
We also included the estimates for the high [$\alpha$/Fe]
stars (red circles) and low [$\alpha$/Fe] stars (magenta circles).
The
vertical dashed lines in the left and right panels denote the limit
between prograde and retrograde rotation with respect to the
corresponding galactic disc in each simulation. The horizontal dashed
lines in the middle and right panels indicate the solar abundance ratio
for [O/Fe].}
\label{toomrehaloex}
\end{figure*}

\subsection{[Fe/H] and [O/Fe] Profiles of the OHPs}

Previous works have reported the existence of a `gradient' in the
metallicity of stars in the simulated halo systems by considering the
difference between the so-called IHRs and OHRs. In Paper I, we measured
the difference between the median [Fe/H] of the IHRs and OHRs, finding
that simulations were capable of reproducing values similar to those
estimated in the the MW \citep{zolo2009,font2011,mcc2012, tissera2012}.
However, if the analysis is restricted only to the OHRs, one might
expect little or no metallicity gradients, at least if the stars from
the accreted sub-galactic systems were well-mixed. In Paper I, we found that
the median [Fe/H] ([O/Fe]) of our OHPs are correlated (anti-correlated)
with the fractions of stars coming from massive satellites, indicating
that some memory of the history of formation may still remain in this
component. Below we check on this possibility, assuming that their
formation histories are consistent with those predicted by a
hierarchical clustering scenario.

Fig. ~\ref{gradhaloex} shows the median [Fe/H] and [O/Fe] profiles for
the OHPs in our six simulated halo systems. For [Fe/H], there is
considerable variation in both the level of enrichment and the predicted
slopes with galactocentric distance. We also note that, although this
component has been defined to be smooth, the abundance distributions
might still reveal their complex assembly histories as shown by $Jz$
-$E$ in Paper I \citep[see also][]{helmi2001}. This is particularly
clear from the [$\alpha$/Fe] profiles plotted in the lower panel of
Fig.~\ref{gradhaloex}, where the contributions from the sub-populations
with different levels of $\alpha$-enrichment as a function of
galactocentric radius can be seen.

For the [Fe/H] profiles, a linear regression was fit between $\sim 20$
kpc and $\sim 130$ kpc, in order to avoid the central and very outer
parts of the distributions, which might be affected by the IHPs and the
boundaries of the systems, respectively. Fig. ~\ref{corre} shows the
slope and zero points, as a function of the fraction of stars formed in
more massive sub-galactic systems (M $ > 5 \times 10^9$ M$_\odot$). As
expected from the results already discussed in Paper I, the zero point
shows a trend indicating higher metallicities in OHPs formed from larger
contributions of debris stars acquired from relative more-massive
systems. Although the slopes vary from mild to flat, there is a trend
with $F_{\rm massive}$ such that steeper negative slopes are found in
diffuse OHPs formed with significant contributions from relatively
higher-mass systems. Massive sub-galactic systems would tend to survive
farther into the potential wells, carrying relatively more metal-rich
stars and gas available for star formation toward the central regions.
The OHPs received a significant contributions of debris from relatively
lower-mass satellites will tend to be better-mixed, and exhibit more
homogeneous chemical distributions.

In order to better understand the differences in the abundance
gradients, we also analysed the ages, spatial distributions, and binding
energy distributions of the simulated OHPs. We found that the oldest
stars are less metal-enriched, as expected, and they span a larger range
of total energy and radial distances. Relatively higher-metallicity
stars tend to be more gravitationally bound, and are more centrally
concentrated. The outer portions of the OHPs are dominated by
high-energy stars, which are also the oldest and the lowest metallicity.
To illustrate this, Fig. ~\ref{binding} shows the distribution of
binding energies for stars in the simulated OHPs, segregated according
to [Fe/H]. The two haloes with the flattest metallicity profiles are
those that have similar total energy distributions for stars of
different [Fe/H] abundances. Those with the steeper slopes possess
relatively higher-metallicity stars predominantly at low total energies.
As discussed previously, relatively more-massive satellites contribute
higher-metallicity stars.  Thus, the existence of a gradient in the OHPs is a
  consequence of the properties of the accreted satellites, and how
  they were disrupted within the potential well of the systems. This
  might explain why analytical models grafted onto the purely dynamical
  versions of the Aquarius systems obtained flatter slopes
  \citep{cooper2010, gomez2012}. A comprehensive discussion on the
  metallicity gradients of both IHPs and OHPs is considered in Tissera et al. (in preparation),
  together with  comparisions with recent observations. Accordingly, our results indicate that the
observed metallicity gradient in the diffuse OHR of a galaxy such as the
MW can provide clues about the mass distributions of the satellites that
contributed to its formation.

\begin{figure}
\hspace*{-0.2cm}\resizebox{6.5cm}{!}{\includegraphics{sigma_Feh_v_Mediashaloex.ps}}
\hspace*{-0.2cm}\resizebox{6.5cm}{!}{\includegraphics{sigma_OFe_v_Mediashaloex.ps}}
\caption{Median abundance profiles of [Fe/H] (upper panel) and [O/Fe] (lower panel) for stars
in the diffuse OHPs of our six simulated galaxies: Aq-A-5 (black), Aq-B-5 (red), Aq-C-5 (magenta),
Aq-D-5 (cyan), Aq-G-5 (green), and Aq-H-5 (violet). See text for
discussion.  }
\label{gradhaloex}
\end{figure}

\begin{figure}
\resizebox{6cm}{!}{\includegraphics{fehgrad_revised.ps}}
\resizebox{6cm}{!}{\includegraphics{fehcero_revised.ps}}
\caption{Slopes (upper panel) and zero points (lower panel) of  linear
regressions fit to the [Fe/H] profiles versus the fraction of
stars in the diffuse OHPs formed in satellites more massive than
$5 \times 10^9M_\odot $h$^{-1}$.  See Fig.~ref{gradhaloex} for colour
coding of the simulated galaxies.}
\label{corre}
\end{figure}

\begin{figure*}
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{HIST_binding_com_haloex_Aq-A-5.ps}}
\resizebox{4.5cm}{!}{\includegraphics{HIST_binding_com_haloex_Aq-B-5.ps}}
\resizebox{4.5cm}{!}{\includegraphics{HIST_binding_com_haloex_Aq-C-5.ps}} \\
\hspace*{-0.2cm}\resizebox{4.5cm}{!}{\includegraphics{HIST_binding_com_haloex_Aq-D-5.ps}}
\resizebox{4.5cm}{!}{\includegraphics{HIST_binding_com_haloex_Aq-G-5.ps}}
\resizebox{4.5cm}{!}{\includegraphics{HIST_binding_com_haloex_Aq-H-5.ps}}
\caption{Distribution of binding energy, $E$, for stars in the diffuse OHPs,  divided according to
their [Fe/H] abundances: [Fe/H]$> -1$ (black lines), $-1.5<$ [Fe/H]$<-1$
(magenta lines) and [Fe/H]$<-1.5$ (green lines).
Aq-A-5 and A-D-5 have steeper metallicity gradients than Aq-C-5 and A-G-5. }
\label{binding}
\end{figure*}

\section{Conclusions}

We have analysed a suite of six MW mass-sized systems, simulated within
$\Lambda$CDM using a version of {\small P-GADGET3} that includes a
prescription for self-consistent SN feedback. This scheme allows us to
follow the chemo-dynamical evolution of baryons as they are assembled
into galaxies. Our simulated diffuse stellar haloes can be described as
assembled from three  stellar sub-populations: debris, endo-debris and
disc-heated stars.
Debris stars
 formed in separate sub-galactic systems located outside the virial radius of
the main progenitor galaxies at their time of formation. These
sub-galactic systems were later accreted by the main progenitor galaxies, donating stars primary to the OHPs, but as well as to
IHPs. The Endo-debris sub-populations formed in gas-rich sub-galactic systems
within the virial radius of the main progenitor galaxies. These
systems were disrupted
farther in the potential well,   contributing stars primarily to the
IHPs, and to a lesser degree, to the OHPs. Disc-heated  stars can
represent a significant percentage of the IHPs.
 These
sub-populations are distinguished from one another as they exhibit, on
average, stars of different chemical abundances, ages, kinematics, and
binding energies. The relative fractions of debris stars and endo-debris
stars provides clues to the mass distribution (and relative number) of
the sub-galactic systems that contribute to form the stellar haloes. These
results have clear implications for observational studies that attempt
to identify different populations in the MW and other galaxies
\citep[e.g.][]{caro2010, caro2012,sheffield2012}.

Summary of the main results:

The simulated IHPs possess three clear stellar sub-populations -- the
debris stars, the endo-debris stars, and the disc-heated stars. Debris
stars are $\alpha$-enhanced relative to iron, low metallicity, and
on average, show no clear signals for rotation. Endo-debris stars exhibit lower
$\alpha$-enhancement than debris ones, on average. Endo-debris stars could
be associated with the stars observed and classified by \citet{sheffield2012}
as accreted stars. In our simulations endo-debris stars exhibit  larger
velocity dispersions, on average,  than the disc-heated stars. Disc-heated stars are
less $\alpha$-enhanced and more metal-rich compared to the endo-debris
stars, with characteristics that depend on their ages. Disc-heated stars
with ages greater then $\sim 10$ Gyr  are dominated by their dispersion,
while those with ages in the range $\sim 8-10$ Gyr have a larger
  rotational velocity component, and exhibit solar to sub-solar [$\alpha$/Fe] ratios. Although
it is feasible, on average, to distinguish these different components by
comparing their chemical abundances and kinematic properties, there
exists considerable overlap between these sub-populations.

The simulated IHPs exhibit metallicity gradients, the strength of which
are determined by the relative fractions of the three sub-populations
that contributed to their formation. While the endo-debris and
disc-heated stars dominate in the central parts of IHRs (within $\approx
20$ kpc), the debris stars dominate in the outer parts of the IHRs.
Hence, the relative contributions of the different sub-populations can
conspire to produce steeper metallicity gradients than those exhibit by
each sub-populations separately.

The simulated OHPs are primarily comprised of debris stars that formed
in accreted sub-galactic systems. The relatively less-massive systems are
easily disrupted, while the relatively more-massive ones are able to
survive farther into the global potential well of the system before
being disrupted. As a consequence, although stars of the OHPs are
generally of very low metallicity, the relatively more metal-rich ones
tend to be more centrally concentrated. Some of the OHPs show
  signals of weak prograte rotation ($\approx 15\%$  V$_{\rm LSR}$).The relative distribution of
debris stars from these different accreted sub-galactic systems can result
in a genuine metallicity gradient within the OHRs, which although weak,
can be used to constrain the assembly history of the OHPs. The
[$\alpha$/Fe] ratios exhibit a heterogeneous distribution from simulated
galaxy-to-galaxy, reflecting the mixture of contributions from accreted
galactic systems with different star-formation histories. A future
comparison between the frequency of low-[$\alpha$/Fe] stars in the
haloes can provide clues on the history of formation and the masses of
the accreted systems, as well as on the validity of current
chemical-enrichment schemes.

In this paper, we have studied the IHPs and OHPs as separate
sub-populations in relation to their assembly histories in a
cosmological context. The properties of the combined IHPs and OHPs will
be discussed in a forthcoming paper, which considers comparisons of the
nature of the observed stellar populations in the MW, M31, and and other
nearby galaxies with predictions from the simulations.

\section*{Acknowledgments}

We thank Simon D.M. White for useful comments and suggestions.
This work was partially funded by L'Oreal-Unesco-Conicet Award for
Women in Science, PICT Max Planck 245 (2006) of the Ministry of Science
and Technology (Argentina), and the Cosmocomp and Lacegal Networks of
FP7 Programme of the European Community.  TCB acknowledges partial
funding from grants PHY 02-16783 and PHY 08-22648:  Physics Frontier
Center / Joint Institute for Nuclear Astrophysics (JINA), awarded by the
U.S. National Science Foundation.

redpajama_set_name: RedPajamaArXiv


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text:
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redpajama_set_name: RedPajamaGithub


text:
ELECTRONIC PRESS KIT SERVICE MYPPK POWER PRESS KITS LAUNCHES PRIVATE SCREENING ROOM FEATURE
Electronic-Press-Kit-Service-myPPK----Power-Press-Kits--Launches-Private-Screening-Room-Feature.pdf
Electronic press kit service, myPPK™ – Power Press Kits™ (www.powerpresskits.com) recently developed and installed a new private Screening Room feature that allows users to set their electronic press kits to private, password-only viewing.
Since the release of Power Press Kits (PPK) in 2007, the service has quickly grown to become the online promotional tool and website of choice for startups, stars and legends on six continents™ including GRAMMY® winners and nominees, multi-platinum-selling artists, record labels, American Idol finalists, world-champion athletes, models, colleges, top management agencies, international businesses and many more.
"We are extremely excited about our new Screening Room feature," said Ron Schock, President of Impact Artist Promotions, LLC which developed and operates the PPK service. "For the vast majority of our current users, PPKs are an international, online promotional service utilized for promoting their skills and services to the global media and public. However, we know there are many users across the globe that have greater needs.
"They may have all of the websites and social-networking sites that they need, yet they don't have the ability to professionally and privately share files and information over the internet, free from the public eye. Our new Screening Room feature provides them the technology to do that very thing."
Penny Foster, a songwriter / artist from London, UK commented, "As a songwriter I find the new screening room feature is perfect for sending a mixture of finished productions and demos to selected producers, managers labels and publishers along with all of the information they need, when pitching songs or putting yourself forward for projects."
According to Schock, others to utilize the new feature include a record label from Los Angeles advancing a band assembled by a multi-platinum-selling producer which includes a guitarist who played in a multi-platinum-selling (20M) mega band, another rock band from Los Angeles comprised of the sons of a GRAMMY-nominated multi-platinum-selling R&B legend, a former American Idol finalist from Nashville, a Christian worship band from Pennsylvania, an author from Florida and others requesting anonymity.
Additional information on Power Press Kits and the new Screening Room feature can be found at www.powerpresskits.com.


text:
Candy Rules!
A Sherman Oaks sweet shop makes mouths water for kids of all ages.
Linda Grasso •
On a typical summer day, Rocket Fizz Soda & Candy Shop is jammed with children. No surprise. What's more eyebrow-raising is the number of big kids in the old-fashioned-style store. "I'd say 65% of our customers are adults," co-owner Dustin Ellis says. Although there's an extensive selection of international candy (ever seen green tea-flavored Japanese Kit Kats?) as well as unusual stuff like acai pomegranate mints, the most popular items are the "nostalgic" sweets. Dustin explains, "Rocket Fizz is a trip down memory lane, whether you were born in the 50s or 70s."
Floors are concrete, displays are wooden carts and walls are covered with retro, whimsical tin signs and cardboard posters. Candy is organized by country. Ever savored a Crunchie? That's a best-selling bar in the UK section. "Try this!" quips Dustin's partner Rusty Hadjilou as he grabs something off the Japanese table. "It's a cross between a Starburst and gum. The taste lasts and lasts!" Indeed the grapefruit-flavored hard candy has a remarkably pungent, citrus flavor that does seem to go on and on.
The duo opened the Sherman Oaks store in December (Dustin also owns one in Woodland Hills), and despite the closing of nearby Borders, sales have been steady. "People like to walk in this area, which is a plus." Rusty, a former cartoon producer, and Dustin, a business school graduate, happen to be first cousins. "We complement each other and truly enjoy being here," Rusty explains.
The owners love a challenge. Rusty says, "A kid will say 'gimme something really sour. I can handle it!' So I go crazy coming up with stuff. I'm like, 'Have you tried Toxic Waste Bubblegum?' That's a seriously sour gum where the sour lasts for several minutes." Other times they've got to satisfy a connoisseur. "I might offer someone like that Dutch licorice—it's incredible!" So here's a challenge: What would you suggest for a girl who doesn't like sweets? Rusty pauses before quickly darting around the store, "Ever tried Manner Wafers? They're these really light wafers filled with chocolate hazelnut and vanilla crème. What about apple licorice?"
The owners also relish making custom gift baskets. Rusty says, "We can do any theme. For example, we've done a cat lover basket with items like Kiddle Piddle soda and a Don't Let the Cat Out tin sign. A slam-dunk is to fill a basket with items from the era of their childhood. I just did one for the '70s with Pop Rocks, Astro Pops and Laffy Taffy."
Rocket Fizz Soda Pop & Candy Shop
14613 Ventura Blvd., Sherman Oaks | 818-981-9009 | rocketfizz.com
It's Raining Men!
Three Places to Eat Foie Gras in the San Fernando Valley


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text:
Уильям Ралф Беннетт (1930—2008) — американский физик.

В 1952—1957 гг. работал в Колумбийском университете, в 1957—1959 — в Йельском, в 1959—1962 — в Bell Labs. С 1962 — профессор Йельского университета.

Исследования по физике газовых лазеров и атомной физике. В 1960 г. совместно с А. Джаваном и Д.Эрриотом (Хэрриотом) построил первый газовый лазер на смеси гелия и неона. В 1962 г. с П. Киндлманом — лазер с магнитострикционной настройкой. В 1962 г. получил для гелий-неоновой системы выражение для величины среднего усиления при оптимальных условиях.

В 1959 г. указал процессы в разряде в чистом неоне, которые можно использовать для получения усиления, и в 1962 г. впервые наблюдал оптическое усиление в разряде в чистом неоне. Предложил лазер на смеси неон — кислород (с Джаваном) и на смеси аргон — кислород (с К. Пателом). В 1962 г. разработал метод отрицательной обратной связи для долговременной стабилизации частоты лазера (метод Беннетта).

В 1962 г. постулировал существование провалов в кривой усиления на частотах генерации и обнаружил (1963) их совместно с Джаваном и У.Лэмбом. В 1964 г. разработал метод стабилизации частоты лазера, основанный на зависимости частоты генерации от амплитуды поля. В том же году предложил механизм образования инверсной заселенности в ионном аргоновом лазере и независимо от У. Бриджеса и др. получил импульсную лазерную генерацию в ионизированном аргоне.

Примечания

Литература

Выпускники Колумбийского университета
Преподаватели Йельского университета
Лауреаты премии Морриса Либманна
Стипендиаты Гуггенхайма

redpajama_set_name: RedPajamaWikipedia


text:
A bioengineered nisin derivative to control biofilms of Staphylococcus pseudintermedius
Microbiology - Journal Articles
dc.contributor.author Field, Des
dc.contributor.author Gaudin, Noemie
dc.contributor.author Lyons, Francy
dc.contributor.author O'Connor, Paula M.
dc.contributor.author Cotter, Paul D.
dc.contributor.author Hill, Colin
dc.contributor.author Ross, R. Paul
dc.identifier.citation Field D, Gaudin N, Lyons F, O'Connor PM, Cotter PD, Hill C, et al. (2015) A Bioengineered Nisin Derivative to Control Biofilms of Staphylococcus pseudintermedius. PLoS ONE 10(3): e0119684. doi:10.1371/journal.pone.0119684
dc.identifier.volume 10 en
dc.identifier.issued 3 en
dc.identifier.doi 10.1371/journal.pone.0119684
dc.description.abstract Antibiotic resistance and the shortage of novel antimicrobials are among the biggest challenges facing society. One of the major factors contributing to resistance is the use of frontline clinical antibiotics in veterinary practice. In order to properly manage dwindling antibiotic resources, we must identify antimicrobials that are specifically targeted to veterinary applications. Nisin is a member of the lantibiotic family of antimicrobial peptides that exhibit potent antibacterial activity against many gram-positive bacteria, including human and animal pathogens such as Staphylococcus, Bacillus, Listeria, and Clostridium. Although not currently used in human medicine, nisin is already employed commercially as an anti-mastitis product in the veterinary field. Recently we have used bioengineering strategies to enhance the activity of nisin against several high profile targets, including multi-drug resistant clinical pathogens such as methicillin-resistant Staphylococcus aureus (MRSA) and vancomycin-resistant enterococci (VRE) and also against staphylococci and streptococci associated with bovine mastitis. However, newly emerging pathogens such as methicillin resistant Staphylococcus pseudintermedius (MRSP) pose a significant threat in terms of veterinary health and as a reservoir for antibiotic resistance determinants. In this study we created a nisin derivative with enhanced antimicrobial activity against S. pseudintermedius. In addition, the novel nisin derivative exhibits an enhanced ability to impair biofilm formation and to reduce the density of established biofilms. The activities of this peptide represent a significant improvement over that of the wild-type nisin peptide and merit further investigation with a view to their use to treat S. pseudintermedius infections. en
dc.description.sponsorship Science Foundation Ireland (Investigator Award 10/IN. 1/B3027); Society for Applied Microbiology, United Kingdom (Students into Work Grant) en
dc.publisher Public Library of Science en
dc.rights © 2015 Field et al. This is an open access article distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited en
dc.rights.uri http://creativecommons.org/licenses/by/4.0/ en
dc.subject Antimicrobial cationic peptides en
dc.subject In vitro activities en
dc.subject Methicillin-resistant en
dc.subject Enhanced activity en
dc.subject Aureus biofilms en
dc.subject Lantibiotics en
dc.subject Combination en
dc.subject Cows en
dc.subject Biosynthesis en
dc.subject Bacteriocins en
dc.title A bioengineered nisin derivative to control biofilms of Staphylococcus pseudintermedius en
dc.internal.authorcontactother Colin Hill, School of Microbiology, University College Cork, Cork, Ireland. +353-21-490-3000 Email: c.hill@ucc.ie en
dc.contributor.funder Science Foundation Ireland
dc.contributor.funder Irish Government
dc.contributor.funder Society for Applied Microbiology, United Kingdom
dc.identifier.journaltitle PLOS ONE en
dc.internal.IRISemailaddress c.hill@ucc.ie en
dc.identifier.articleid e0119684
Name: DF_BioengineeredP ...
APC Microbiome Institute- Journal Articles [614]
Microbiology - Journal Articles [437]
Except where otherwise noted, this item's license is described as © 2015 Field et al. This is an open access article distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited


text:
Liquid Assets: Impact Investing in the Water Sector
By Marta Maretich
Water is a hot issue in investing circles these days. Once considered a free natural resource, water is increasingly a focus for finance and speculation; hardly surprising in a world where water stress is a reality, global demand for water is on the increase and investment in water-related infrastructure is urgently needed, according to sector-watchers such as the World Bank-sponsored 2030 Water Resources Group.
There are a number of well-known "tailwinds" pushing this trend. Population growth, uneven distribution of resources, increasing urbanization and new government regulations are some of the factors influencing the rise in demand for water. Pollution, deforestation and climate change are taking a toll on supply, with many dry regions, like California and Australia, experiencing the longest droughts in their history.
Large international development organizations like the UN, the WEC and the WHO have been vocal about the need for more water investment and cross-national cooperation and now key players, like China and the US, are waking up to the urgent need to invest in infrastructure and water security. Collecting water data will be part of this. Earlier this month the US launched a climate data collection initiative to "stimulate innovation and private-sector entrepreneurship in support of national climate-change preparedness." The results will certainly influence future government spending on water-related issues, and probably increase it. In drought-hit states, like California, the spending has already begun and the trend toward more state investment activity is likely to continue, spurring overall market growth in the water sector.
Doing good and preventing harm
All these factors are coming together to produce what some commentators have called a "blue gold rush"; a sharp rise in interest in water investing among mainstream investors that clearly holds opportunities for impact investors, too. The reasons for this are obvious: Clean, plentiful water is necessary to all forms of life on the planet. Animals, plants, ecosystems and habitats all require adequate water to thrive. Human societies need water, too, for health, agriculture, industry and economic development. Investing in water is clearly a way to create a whole range of positive impacts.
There's another compelling reason for impact investors to get involved now: Preventing harm. Water sector investment is undergoing a boom and, if the right safeguards aren't applied, social and environmental concerns could fall by the wayside. Water that serves people has to come from somewhere, for example, and irresponsible extraction or dam building can lead to destruction of habitats and communities. Polluted water; such as agricultural runoff, which is often full of nitrates; can devastate whole ecosystems and destroy species. Competition for water can mean the poor and marginalized are denied fair access. Water grabs, linked to land grabs, are becoming more common in places where resources are scarce. Pricing is an issue in a sector where many analysts agree that consumers have not been paying enough for the water they consume; a situation that is set to change as water becomes more market-oriented.
Addressing the risks of privatization
As business becomes more involved in the supply and management of water, there's concern about negative consequences of treating water as a commodity. Water hoarding and monopolizing, and the exploitation of water rights, could all be harmful to human communities, to the environment and even to world peace.
There are certainly wrong; as well as bizarre; ways to invest in water. And some business leaders have shown a distinct lack of understanding of the complex issues surrounding water. Yet there are moves in many parts of the business community to manage the risks of privatization. Ceres, a US nonprofit that encourages sustainability, works with businesses to identify and address negative water impacts across their operations. The CPD, a UK charity, works with investors and companies to uncover risk and catalyze corporate water stewardship. It holds the largest collection of self-reported climate change, forestry and water risk data in the world.
Water activist Maude Barlow takes a different tack. Starting from the premise that water is a human right, she recommends limits to its commoditization and calls for businesses and governments to adopt a new "water ethic":
"Water must never be bought, hoarded, sold or traded as a commodity on the open market," she writes, "and governments must maintain the water commons for the public good, not private gain. While private businesses have a role in helping find solutions to our water crisis, they shouldn't be allowed to determine access to this basic public service. The public good trumps the corporate drive to make profits when it comes to water."
Building robust impact portfolios with water
Whatever one's stance on the commercialization of water, it's clear that the water sector is now at a turning point and this means impact investors have a golden opportunity to shape its future. What's more, water investments may be the ideal basis for building robust, profitable impact portfolios. In the words of Steve Falci, head of strategy development: sustainable investments, for Kleinwort Benson Investors, "Water is probably the biggest win-win of all the sectors in terms of delivering reliable financial returns and positive impact."
In a recent white paper, Integrating Publicly Traded Water and Agribusiness Equities Into Impact Investor Portfolios, impact advocate Jed Emerson and Falci explore the potential of including water sector investments in impact portfolios. Water, the paper argues, has much to offer impact in financial terms. First, it's a huge sector that boasts a wide range of investment opportunities in companies that provide the operations, equipment, chemicals, and services that make water available for municipal, industrial, and agricultural markets worldwide. These include:
-Water waste and water utilities: Companies managing infrastructure and delivery of water and or treating wastewater or reuse and safe remediation back into the environment
-Water infrastructure: Companies providing pipes, filters, pumps, seals, valves, water purification and desalination equipment, design engineering and construction services
-Water technology: Companies providing filtration, disinfection, test and measurement products and metering.
Next, not only does the water sector offer a vast array of different companies to invest in, it also offers a complete spectrum of different types of investments to choose from.
Without straying from the water sector, investors can elect to place their money in seed stage businesses, mid-sized growth businesses or large, established corporations. They can combine investments from different asset classes, each carrying a different level of risk and reward, and choose defensive and cyclical holdings to create a solid portfolio that gives reliable returns. For an explanation of how this works, see Matt Sheldon's article on how he constructs Calvert's successful Global Water Fund.
Including publicly traded equities
Most importantly, Falci and Emerson stress, impact investors can expand their horizons by including investments in publicly traded companies in their portfolios. As Falci explained, "Impact's success so far has been in channeling private capital to small businesses that lacked access to other sources of finance. Many impact investors have focused entirely on investing in private markets, but publicly traded equities, chosen carefully, can help strengthen and balance an impact investment portfolio without sacrificing the commitment to positive impacts or small businesses."
Falci and Emerson aren't alone in advocating impact's expansion into publicly traded equities. Others, including Michael Van Patten of Markets With Mission, have made similar suggestions. However using this method with water equities may work particularly well, according to Falci, because few water sector companies engage in activities considered negative or even controversial.
And what about managing negative social or environmental impacts of capitalizing on water? The authors suggest using SRI and ESG screening, both well established in mainstream business, to provide assurance. "Public equity managers increasingly have the tools to assess areas such as companies; carbon footprints, water usage and Base of the Pyramid activities," they write. Undesirable consequences may be addressed through "engagement with company management; an element of investor strategy that has been a central part of most sustainable/responsible investing approaches for years."
Whether one agrees with this "total portfolio management" approach or not, what's interesting is the way it brings together several strands of the larger social and sustainable investing movements. Emerson and Falci are both social investing veterans with track records that predate the "invention" of impact. Their approach calls for the judicious application of various systems for ensuring positive outcomes and avoiding negative ones; including established systems like SRI and ESG and newer ones, like ISIS; to evaluate a variety of impact investments across a diverse impact portfolio. The water sector, with its great size and diversity, as well as its benign reputation, offers the perfect opportunity to experiment with this sophisticated approach to investing for impact.
The issues surrounding water; its use and abuse, its scarcity, its relative availability, its cost to consumers; are set to be high on the global agenda for the foreseeable future. With the situation becoming more critical, governments, international development agencies and businesses are all stepping up efforts to find solutions. This will create a buoyant marketplace for water-related investing in coming years. Impact investing, with its pragmatic approach to profit and its commitment to delivering social and environmental benefit, has a unique opportunity to engage with this market and influence its development for the better.
Read the white paper on water investing by Jed Emerson and Steve Falci
10 Things You Should Know About Water Infographic from Circle of Blue
To find live impact deals in the water sector, logon to Maximpact.
Image Credit: 123rf stock photography
Impact investing in water Jed Emerson Maude Barlow Publicly traded companies in impact portfilios Steve Falci Sustainable invsesting in water
Cities Show Strong Climate Leadership in Paris
Funding Water and Sanitation Business at the Bottom of the Pyramid
Making Safe: Seven Strategies for Managing Risk in Impact Investing
From Net Zero to Net Positive in Water and Energy Sectors: The Time is Now
Impact Investing 2.0 and the Rise of Multilingual Leadership Teams: An Interview with Jed Emerson
2 thoughts on "Liquid Assets: Impact Investing in the Water Sector"
Courtney Smith says:
I am interested in reading your white paper on water investing by Jed Emerson and Steve Falci, however the link on the website to access it is broken. Is it possible to have this white paper emailed to me?
maximpact says:
Thank you for letting us know that links needed updating. We have updated all the links in the post that had changed, including the white paper.
Enjoy Reading.
Maximpact Team


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