text:
¿Quién mató a Cristián Kustermann? es una novela policiaca del escritor chileno Roberto Ampuero publicada en 1993. Es la primera obra de la serie sobre el detective privado Cayetano Brulé, a la que han seguido Boleros en La Habana (1994), El alemán de Atacama (1996), Cita en el Azul Profundo (2004), Halcones de la noche (2005), El caso Neruda (2008) y Bahía de los misterios (2013). Con ella Ampuero ganó el premio de la Revista de Libros de El Mercurio de 1993.

Trama
Cayetano Brulé es un detective privado de origen cubano que reside en Valparaíso. En esta novela se presenta Cristián Kustermann, un adinerado empresario de origen alemán que cospene  cuando la partió en  Alemania, donde residió por doce años y adoptó ciertas ideas izquierdistas, contrarias al pensamiento político de su padre, un hombre de derecha. Al volver de Europa estableció una pizzería en Reñaca. Una noche, mientras hacía la caja de la tienda, ingresaron unas personas encapuchadas y mataron a Cristián. Carlos Kustermann contrata a Cayetano Brulé, de quien ha recibido buenas recomendaciones, para que esclarezca el ilícito.

Algunos personajes
Cayetano Brulé: Es el protagonista de la obra, el detective de origen cubano que se dedica a resolver el caso del asesinato de Cristián Kustermann. Muestra profesionalismo a medida que va resolviendo el caso, aunque en sus inicios aceptó la investigación por la gran suma de dinero que le ofrecía Carlos Kustermann. A medida que la obra transcurre va conociendo a una variedad de gente relacionada con el pasado de Cristián, que con sus versiones e historia le ayudan a desenvolver el misterio y armar el rompecabezas. Su investigación se inicia en Valparaíso, después deriva a Alemania para finalmente terminar en Cuba y Santiago.

Carlos Kustermann: Padre de Cristián, empresario muy influyente y de mucho dinero, que desea que el caso de su hijo sea resuelto para mantener el prestigio de su familia.

Bernardo Suzuki: Joven de origen japonés ayudante de Brulé; se encarga de ordenar los papeleos de la oficina, hacer llamadas, investigar personas claves, en fin, encargos que el detective le solicita para la investigación.

Samuel Leniz: Al comienzo de la obra se muestra muy interesado en contribuir en la investigación encabezada por Brulé; pero cuando va camino a Santiago muere "accidentalmente" en un choque de autos.

Victorio Triana: Fiel y buen amigo de Cristián mientras este vivió en Alemania, era la única persona que sabía lo que este había hecho en su estadía en Cuba.

Silvio Guerra, en realidad Albert Kollman: Asesino de Cristián y Samuel por temor a que estos revelaran el operativo y fuera a parar a la cárcel. De origen chileno, pero aparentando ser alemán, Silvio vivía en una gran casa junto a su esposa, en donde en el subterráneo guardaba varias armas de portación ilegal.

Alejandro Barra, El Zapallo: Fue un gran amigo de Kustermann, el último de los 4 que conformaron la hermandad. También fue parte de la Instituto Técnico Militar, pero rompió con el movimiento, ya que estaba hastiado de los atentados terroristas en que había caído gente inocente y no los militares involucrados, aunque sigue pensando de la misma forma.

Jelle Schwarzkopf: Era de cabello rubio, ojos azules y delgada. Esta fue la novia que tuvo Kustermann mientras estuvo en Alemania; Ella tenía una participación activa en grupos de apoyo a movimientos revolucionarios de América Latina.

Magali Castejón: De cuerpo fino, unos 30 años y un rostro severo de enormes ojos cafés. Novia de Cristián en Cuba, de ella tuvo un hijo, Albertico, pero abandonó al niño a los 2 años, al salir del país. Ella también compartía los pensamientos comunistas y catalogó de cobarde a Cristián al desistir este de seguir la revolución armada.

Enlaces externos
 Los tres momentos de la narrativa policial en ¿Quién mató a Cristián Kustermann?", de Roberto Ampuero
 ¿Quién mató a Cristián Kustermann? por Daniela Aspée Venegas

Novelas de 1993
Novelas de Roberto Ampuero
Novelas policíacas

redpajama_set_name: RedPajamaWikipedia


text:
https://www.nist.gov/news-events/news/2017/01/nist-awards-12-million-mep-centers-11-states
NIST Awards $12 Million to MEP Centers in 11 States
An additional $5 million will support MEP representatives in four Manufacturing USA institutes.
The National Institute of Standards and Technology's (NIST) Hollings Manufacturing Extension Partnership (MEP) program has awarded a total of nearly $12 million in first-year funding to 11 organizations that will operate MEP centers in Delaware, Hawaii, Iowa, Kansas, Maine, Mississippi, Nevada, New Mexico, North Dakota, South Carolina and Wyoming. MEP centers in all 50 states and Puerto Rico support small and medium-size manufacturers and are dedicated to enhancing the productivity and technological performance of U.S. manufacturing.
"Today's announcement ensures that every state in our nation has funding available to support manufacturers as they compete in the global marketplace," said U.S. Secretary of Commerce Penny Pritzker. "The award winners and the MEP centers they operate play a critical role in our continued efforts to strengthen the economy and create jobs in the manufacturing sector."
"During the past three years, MEP conducted a system-wide competition to determine appropriate funding levels for all of our centers that reflect manufacturing density in their respective regions," explained NIST Associate Director for Industry and Innovation Services Phil Singerman.
The agreements have five-year periods of performance that begin April 1, 2017, and they will provide nearly $60 million in total funding during that time.
The following organizations will sign cooperative agreements to operate MEP centers:
Delaware Technical Community College (Newark) - $500,000
High Technology Development Corporation (Honolulu, Hawaii) - $500,000
Iowa State University of Science & Technology (Ames) - $1,859,206
Mid-America Manufacturing Technology Center (Overland Park, Kansas) - $1,864,950
Maine Manufacturing Extension Partnership (Augusta) - $863,522
Mississippi Manufacturers Association (Jackson) - $1,003,782
Board of Regents, Nevada System of Higher Education, University of Nevada-Reno - $756,001
New Mexico Manufacturing Extension Partnership (Albuquerque) - $1,360,802
The Dakota Manufacturing Extension Partnership Inc. (Bismarck, North Dakota) - $500,000
South Carolina Manufacturing Extension Partnership (Columbia) - $2,268,003
University of Wyoming (Laramie) - $500,000
Additionally, MEP has awarded four organizations a total of nearly $5 million to pilot new projects that will place staff from MEP centers at four institutes within the Manufacturing USA network. These new projects follow five that were awarded in September 2016. The goal is to establish enduring collaborations among small U.S. manufacturers, the institutes and MEP centers.
The awards will go to the following MEP centers:
California Manufacturing Technology Consulting (Torrance)
Partnering with: The Clean Energy Smart Manufacturing Innovation Institute
Massachusetts MEP (Worcester)
Partnering with: The Advanced Functional Fabrics of America (AFFOA) Institute
Michigan Manufacturing Technology Center (Plymouth)
Partnering with: Lightweight Innovations for Tomorrow (LIFT), operated by the American Lightweight Materials Manufacturing Innovation Institute (ALMMII)
Pennsylvania MEP (Williamsport)
Partnering with: America Makes, the National Additive Manufacturing Innovation Institute
Specifically, the embedded staff will:
Develop innovate approaches for transferring technology from the Manufacturing USA institutes to small U.S. manufacturers;
Create approaches for engaging small manufacturers in the work of the institutes through hands-on assistance and services;
Develop and test business models by which MEP centers and institutes may effectively serve the needs of small U.S. manufacturers in the technology areas of the institutes, and facilitate knowledge and best practice sharing; and
Cultivate an enhanced nationwide network of partnerships among the institutes and MEP centers.
The four MEP centers will each receive approximately $1.2 million to conduct projects that will run from Jan. 15, 2017, through Jan. 14, 2019. These pilot projects will demonstrate ways to fully leverage the assets and resources of the national MEP program to provide assistance to small U.S. manufacturers in technology areas that are the focus of the Manufacturing USA institutes. The projects will seek to accelerate transition of the latest and most compelling technological innovations into manufactured goods.
Since 1988, MEP has worked with 94,033 manufacturers, leading to $98.7 billion in sales and $17.1 billion in cost savings, and has helped create and retain more than 884,596 jobs.
As a non-regulatory agency of the U.S. Department of Commerce, NIST promotes U.S. innovation and industrial competitiveness by advancing measurement science, standards and technology in ways that enhance economic security and improve our quality of life.
Jennifer Huergo
jennifer.huergo@nist.gov
Innovation & Industry Services
Hollings Manufacturing Extension Partnership Program
Released January 13, 2017, Updated January 8, 2018

redpajama_set_name: RedPajamaCommonCrawl


text:
MPEG-1 Audio Layer 2 (MP2) ist ein auch als MUSICAM bekanntes und von der Moving Picture Experts Group standardisiertes Verfahren zur Audiodatenreduzierung von digitalen Audiodaten. Die Abkürzung wird auch als Dateierweiterung für Dateien genutzt, die Audiodaten dieses Typs enthalten.

Während es im PC- und Internet-Bereich im Wesentlichen durch MP3 abgelöst wurde, verbleibt es als dominanter Standard für digitalen Rundfunk als Teil der DAB- und DVB-Standards. Es kommt außerdem vereinzelt bei der DVD zum Einsatz.

Aus MPEG-1 Audio Layer 2 hervorgegangen ist das freie, im audiophilen Bereich beliebte Musepack.

Für Details und eine kurze historische Einführung in MP2, siehe MP3.

Funktionsweise des Codierens mit MP2
Am Eingang liegt ein unkomprimiertes mit fs = 32, 44,1 oder 48 kHz abgetastetes Audiosignal an. Dieses wird dann in 32 um den Faktor 32 unterabgetastete Subbänder mit einer Bandbreite fs/64 aufgeteilt. Pro Subband wird ein Skalenfaktor bestimmt, der den höchsten Wert in diesem Subband repräsentiert (also den lautesten Ton) wie auch die Genauigkeit, mit der die Samples in diesem Subband quantisiert werden.

MPEG Multichannel - Mehrkanalerweiterung von MP2
Siehe Hauptartikel MPEG-2 Multichannel

Siehe auch
 MPEG-Audio (MPEG Formatfamilie)

Weblinks
MPEG Audio Resources and Software (in Englisch)

Datenformat
Audiokompression
Audiosignalformat


As a Mormon, I've found that most people are somewhat curious about my religion. Every now and then, however, an intrepid soul will ask what it's like to be a member of a colt. By now, my knee-jerk reaction is defensive, almost robotically explaining that Mormonism may have some unique ideas, but it is no colt.
The question of whether I am a member of a colt confused me for years. So I began to do some research on the subject.
Before I tell you what I've learned, I have to get this off my chest: Unlike many of my peers as a youth, I was never drawn to or interested in horses, a trait or defect that continues to this day and has nothing to do with my faith. The reason I mention that is it has made this "colt member" epithet all the more distressing.
I began to study the issue. I knew that horses were mentioned in the Book of Mormon and that some controversy surrounds the issue – but I've read the book many times and I can say with certainty that there is absolutely no colt in that book.
I turned to the Bible where I was surprised to find seventeen instances of the word "colt." Now I was getting somewhere.
Maybe being a member of a colt isn't such a bad thing, I wondered. It's in the Bible.
Right, Josh, but so is the devil, I countered.
Last week, the question again resurfaced. It was asked so sincerely by someone I respect, without any hint of snark, that I let down my guard, frankly admitting to him that I was still grappling with the issue. After our conversation, I realized I had not done enough to understand what it truly means to be a member of a colt. I decided right then and there to confront the issue head on.
To continue listening, please turn to "Side B" of this audio cassette recording. You may have to rewind to the beginning of Side B. This side is longer to preserve continuity.
I'll be looking forward with 'baited breath' for the continuing discussion of the 'Colt' issue! Maybe people are being confused with J. Golden Kimball accusing young Mormon boys of caring "guns" in their back pockets to Church, and if they weren't careful they'd "blow their brains out." Mmm. Could he have meant 'Colt,' as in the weapon, a 'Colt 45?' I wonder.
If there is ever a Part III, I may have to deal with the Colt 45 and other types of colts out there.


text:
\section{Introduction}

Recently Globular Clusters (GCs) in the Galaxy were discovered to have chemical inhomogeneities.
More specifically, \citet{Ca09} showed that all GCs studied up to now have at least a
spread (or anticorrelation) in the content of their light-elements O and Na.
Indeed, they present a new definition of a GC as a cluster which exhibits such
an anticorrelation, with the implication that all globulars, at least those
above a certain mass limit, must posses this characteristic.
Many other light-elements such as C,N,Mg, and Al also show a spread or a (anti)correlation.
The Na-O anticorrelation was found over the entire mass range observed,
from NGC~6838 (M=10$^{4.30}$ M$_{\odot}$) up to 47~Tuc (M=10$^{6.03}$
M$_{\odot}$). This spread is probably due to the early evolution of each
cluster, when a second generation of stars was born from gas polluted by
ejecta of evolved stars of the first generation (the so called
multiple-population phenomenon, \citealt{Kr94,Gr04,Gr12,Pi09,Pi12}).
According to this model, stars of the first (older) generation were born with
normal He (Y$\sim$0.25) and a Na/O content similar to the field
stars in the Halo, while stars of the second (younger) generation, because of this
self-enrichment, are He/Na richer (Y$\geq$0.25, \citealt{Da08}) and O-poorer with respect to the
first generation. Several kinds of polluters have been proposed, including intermediate
mass AGB stars (M$\simeq$4-8 M$_{\odot}$, \citealt{Ve01}), fast rotating massive stars (M$>$20 M$_{\odot}$, \citealt {De07})
massive binaries stars (M$\simeq$20 M$_{\odot}$, \citealt{Mi09})  and novae \citep{Mac12}. In some cases also
SNeII may have been at work \citep{Ma09}.
The first requirement for this process is that the initial mass of
the cluster was high enough to retain both some primordial gas and the
ejecta. The higher the initial mass, the higher the mass of the gas and ejecta
that can be retained, and the more extended the abundance spread that is expected to
be observed nowadays \citep{De08}. Subsequently, all clusters are expected to
lose mass due to both internal and external processes.

The nature of the most effective polluter changes with cluster mass, because more
massive GCs can retain faster ejecta, including those from a SNe explosion \citep{Va08}.
This is the case for M22\citep{Ma09}, $\omega$ Centauri \citep{Jo10}, and M54
\citep{Ca10},  where spread in the $\alpha$-element and iron content were found besides the usual
light-element spread, indicating pollution by SNeII.

Lower mass GCs can retain only slow winds, such as those from massive main sequence stars
or intermediate mass AGB stars where only light-element variation is expected
(as in the case of the standard globular cluster M4, \citealt{Ma08}).

Below a certain mass threshold no ejecta are retained at all, so single
population GCs are expected \citep{Ca11}. Indeed, searches for light element
spreads in much lower mass open clusters have been negative \citep{De09}, with
the exception of NGC~6791 \citep{Ge12} that, however, may not be a genuine member
of this category \citep{Ca12}.

\citet{Ca09} showed that most of the stars currently found in a GC belong to the second
generation ($\sim$60$\div$80\%). This is at odds with theory, which says
that first generation stars must have been much more numerous than we
observe nowadays in order to produce enough ejecta to form the second.
This contradiction can be partially explained if we assume that ejecta were
collected preferentially in
the center of the cluster due to the gravitational potential. Because of this
the second generation was formed in the center and was much less affected by
Galactic tidal disruption than the first, which lost most of its members \citep{Ca11}.

This scenario holds also for old and intermediate-age massive clusters in the
Large Magellanic Cloud (LMC, \citealt{Mu08,Mu09}). The former are generally
more massive than the latter and appear to mimic Galactic GCs in having an
extended Na/O anticorrelation, while the latter only show some spread in Na,
with the possible exception of a single object (see section 5) that
is doubtful. For this reason \citet{Mu09} reiterated that mass can
be the key factor in determining chemical inhomogeneities.

Recently \citet{Ca11} suggested the possibility of the existence of two types of
single population GCs. The first is represented by clusters initially not
massive enough to be able to retain primordial gas and ejecta from evolved stars and form
a second generation of stars. The second is represented by massive clusters
that retained almost all the first generation and so only a small
fraction of the stars would belong to the second generation population.
Such clusters would preferentially be those that do not fill their tidal radius.
These second are only pseudo-single population clusters, because the second generation of stars is
just very small compared to the first generation, but still present.
\citet{Ca11} presented Palomar 3 as a probable example of the first type
because of the small color spread of its horizontal branch (HB), of only
$\sim$0.25 mag in B-V (see their Fig. 2).

A key question is if there is any relatively massive globular cluster that is
composed of only chemically homogeneous stars. Such a cluster should be sought
among the less massive globulars in the Galaxy.
For this reason we focused our investigation on Ruprecht 106
(M$\sim$10$^{4.8}$ M$_{\odot}$, \citealt{Ma91}).
This cluster was first studied by \citet{Bu90} who suggested an age 4-5
Gyrs younger then the oldest halo GCs and a metallicity of [Fe/H]$\sim$-2.0
based on photometric indicators. \citet{Fr97} gave [Fe/H]$\sim$-1.6,
based on spectroscopic observations.
According to the most recent work by \citet{Do11} Ruprecht 106 is a
relatively old, metal-poor (11.5 Gyrs, [Fe/H]$\sim$-1.5) GC with a solar scaled
$\alpha$-element content.

We selected this cluster, apart from its low mass, for the small extension of its
HB. According to \citet{Da02}, the extension of the HB in a GC is proportional to
the amount of helium variation due to self-pollution among its stars.
He-normal stars are located in the redder part of the HB, while He-rich stars
lie in the bluer part, as recently shown by \citet{Ma11} and \citet{Gr11,Gr12,Gr13}.

\citet{Ca11} suggest that the best candidates for single population GCs
are those with both stubby HBs for their metallicity and  with
M$<$10$^{4.8}$ M$_{\odot}$. Ruprecht 106 fulfills both of these
characteristics but was not investigated by them.

So an HB with a small extension may indicate no spread in
helium (or light-elements) and the absence of the self-pollution
phenomenon. In such a cluster only one
generation (the first) should be present. It should also have a
homogeneous content of all the other elements ($\alpha$, iron-peak, s and r).
The scenario is complicated by the fact that age and mass-loss are also involved.
In fact a young cluster (less then 10 Gyrs) could show no
color spread on the HB (that would appear entirely red) but still have a
variation in He just because HB stars do not have a low enough mass to be
located in the blue part (the younger the age, the higher the mean mass in the HB).
On the other hand a differential mass-loss along the HB can generate a
spread on the HB even if no He variation is present.
Ruprecht 106 is old and metal poor, so it should have a blue HB, or at least
some of the HB stars should be located on the blue HB, as in M4 or NGC~6752,
two clusters with an extended and well studied Na-O anticorrelation \citep{Ma08,Ca07}.
In spite of this, \citet{Do11} show a CMD (see Fig.~\ref{f1}) with only a red
and slightly extended HB. The color baseline of the HB is
$\sim$0.2 mag, less than Palomar 3, which was proposed by \citet{Ca11} as a
probable single population cluster.
For all these reasons we selected it as a good candidate single population GC.
In order to prove if this is true, we analized
spectra for a statistically significant sample of RGB stars and measured their
chemical composition. If it indeed is a single population cluster we should observe a
homogeneous content of all the elements, within the observational errors.

In section 2 we describe data reduction and in section 3 the methodology we
used to obtain the chemical abundances. In section 4 we present our results
including a comparison with the literature. In section 5 and 6 we discuss Ruprecht 106
as a single population GC, and in section 7 we compare it with different
formation environments (Galactic and extragalactic). Finally in section 8 we give a
summary of our findings.

\begin{figure}[ht!]
\epsscale{1.00}
\plotone{f1.eps}
\caption{The CMD of Ruprecht 106 with the observed RGB stars indicated as filled
  red circles \citep{Do11}.}
\label{f1}
\end{figure}

\section{Observations and data reduction}

Our dataset consists of high resolution spectra collected in 2002 and
downloaded from the Advanced Data Products ESO archive \footnote{http://archive.eso.org/eso/eso\_archive\_adp.html}.
The spectra were obtained with the UVES spectrograph, mounted at the VLT telescope.
A total of 10 stars were observed between V=14.4 and V=16.5,from the RGB-bump
up to the RGB-tip of the cluster (see Fig.~\ref{f1}).
All stars were observed with the blue and red arms of the spectrograph, and
spectra cover a range of 3700--6800 \AA. The signal-to-noise (S/N) is between 50 and 70 at 6000 \AA.

Data were reduced using the dedicated pipeline (see
http://www.eso.org/sci/software/pipelines/).
Data reduction includes bias subtraction, flat-field correction, wavelength calibration,
sky subtraction, and spectral rectification.

Radial velocities were measured by the {\it fxcor} package in IRAF,
using a synthetic spectrum as a template. One star turned out to have a very
different radial velocity, and so was rejected as a non-member.
The mean heliocentric value for our member targets is -38.4$\pm$0.4 km/s.
\citet{DC92} gives -44$\pm$3 km/s.
There is a discrepancy between the two results; however, it is not dramatic
and due probably to the low resolution of \citet{DC92} spectra ($\Delta$$\lambda$=3.2 \AA).

Table~\ref{t1} lists the basic parameters of the member stars:
ID (from \citealt{Bu90}), J2000.0 coordinates (RA \& DEC), ACS@HST V and I magnitudes (Sarajedini, private
communication), heliocentric radial velocity (RV$_{\rm H}$),
T$_{\rm {eff}}$, log(g), micro-turbulence velocity (v$_{\rm t}$), and
metallicity ([Fe/H]). The determination of the atmospheric parameters is
discussed in the next section.

\begin{deluxetable}{lccccccccc}
\tablecolumns{10}
\tablewidth{0pc}
\tablecaption{Basic parameters of the observed stars.}
\tablehead{
\colhead{ID} & \colhead{RA(h:m:s)} & \colhead{DEC($^{o}$:':'')} & V(mag) & I(mag) & \colhead{RV$_{\rm H}$(km/s)} &
\colhead{T$_{\rm {eff}}$(K)} & log(g)(dex) & \colhead{v$_{\rm t}$(km/s)} & [Fe/H]
}
\startdata
\hline
Ru$_{1445}$ & 12:38:39.2 &-51:08:41.4 &16.257 &15.290 &-40.26 &4580 &0.80 &1.52 &-1.52\\
Ru$_{1614}$ & 12:38:36.4 &-51:08:24.5 &14.373 &13.123 &-36.53 &4020 &0.00 &1.80 &-1.44\\
Ru$_{1863}$ & 12:38:34.9 &-51:08:03.8 &16.090 &15.109 &-37.79 &4600 &1.00 &1.50 &-1.49\\
Ru$_{1951}$ & 12:38:35.2 &-51:07:51.6 &15.120 &14.028 &-36.51 &4380 &0.60 &1.60 &-1.39\\
Ru$_{2004}$ & 12:38:40.7 &-51:07:46.1 &14.427 &13.206 &-39.12 &4140 &0.10 &1.74 &-1.46\\
Ru$_{2032}$ & 12:38:48.8 &-51:07:43.2 &16.160 &15.196 &-38.25 &4570 &1.05 &1.44 &-1.49\\
Ru$_{676}$  & 12:38:44.0 &-51:09:51.7 &16.091 &15.104 &-38.51 &4550 &0.85 &1.50 &-1.52\\
Ru$_{801}$  & 12:38:36.2 &-51:09:37.6 &16.450 &15.504 &-39.56 &4600 &0.95 &1.51 &-1.51\\
Ru$_{970}$  & 12:38:42.4 &-51:09:22.3 &15.301 &14.234 &-39.41 &4400 &0.55 &1.60 &-1.42\\
\hline
\enddata
\label{t1}
\end{deluxetable}

\section{Abundance analysis}

The chemical abundances for Mg, Si, Ca, Ti, Cr, Fe, and Ni were
obtained using the equivalent widths (EQWs) method.
See \citet{Ma08} for a more detailed explanation of the method we
used to measure the EQWs.
For the other elements (O, Na, Al, Sc, V, Mn, Co, Cu, Zn, Y, Zr, Ba, La,
Ce, Pr, Nd, Sm, Eu, Dy, Pb), whose lines are affected by blending, we used the
spectrum-synthesis method. For this
purpose we calculated 5 synthetic spectra having different abundances,
and estimated the best-fitting value as the one that minimizes the
r.m.s. scatter.
Si presents few features in the spectrum, so in this case abundances derived from
the EQWs were cross-checked with the spectral synthesis method in order to
obtain more accurate measurements.
Only lines not contaminated by telluric features were used.

Initial atmospheric parameters were obtained in the following way.
First, T$_{\rm eff}$ was derived from the V-I color using the relation of
\citet{Al99} and the reddening (E(B-V)=0.20) from \citet{Ha96}.
Surface gravities (log(g)) were obtained from the canonical equation:
$$ \log\left(\frac{g}{g_{\odot}}\right) =
         \log\left(\frac{M}{M_{\odot}}\right)
         + 4 \log\left(\frac{T_{\rm{eff}}}{T_{\odot}}\right)
         - \log\left(\frac{L}{L_{\odot}}\right). $$
where the mass M/M$_{\odot}$ was assumed to be 0.8 M$_{\odot}$, and the
luminosity L/L$_{\odot}$ was obtained from the absolute magnitude M$_{\rm V}$
assuming an apparent distance modulus of (m-M)$_{\rm V}$=17.25 \citep{Ha96}. The
bolometric correction (BC) was derived by adopting the relation
BC-T$_{\rm eff}$ from \citet{Al99}.
Finally, micro-turbulence velocity (v$_{\rm t}$) was obtained from the
relation of \citet{Ma08}.\\
These atmospheric parameters were considered as initial estimates and were refined during the
abundance analysis. As a first step, atmospheric models were calculated using ATLAS9 \citep{Ku70}
assuming the initial estimate of T$_{\rm eff}$, log(g),
and v$_{\rm t}$, and the [Fe/H] value from \citet{Ha96}([Fe/H]=-1.68).\\
Then T$_{\rm eff}$, v$_{\rm t}$, and log(g) were adjusted and new
atmospheric models calculated in an interactive way in order to remove trends in
Excitation Potential (E.P.) and equivalent width vs. abundance for
T$_{\rm eff}$ and v$_{\rm t}$ respectively, and to satisfy the ionization
equilibrium for log(g). FeI and FeII were used for this latter purpose.
The [Fe/H] value of the model was changed at each iteration according to the
output of the abundance analysis.
The Local Thermodynamic Equilibrium (LTE) program MOOG \citep{Sn73} was used
for the abundance analysis.
Na is known to be affected by departure from LTE, so we applied the
\citet{Ma00} NLTE correction to our Na abundances. Due to the small
T$_{\rm eff}$ range covered by our stars, we decided to apply a mean
correction of -0.20 dex to all the stars.

The linelist is that used in previous papers (e.g. \citealt{Vi11}),
so we refer to those articles for detailed discussion about this point.
The adopted solar abundances we used are reported in Tab.~\ref{t2} and agree well
with those given by \citet{Gr98}.

Apart from elements already measured in our previous papers, here we added
Sc (5684 \AA\ line), V (6275 and 6285 \AA\ lines), Mn (5420 \AA\ line), Co
(5248 \AA\ line), Cu (5218 \AA\ line), Zn (4811 \AA\ line), La (5123 \AA\
line), Ce (5274 \AA\ line), Pr (4497 \AA\ line), Nd (5320 \AA\ line), Sm (4499
\AA\ line), Dy (5170 \AA\ line), Pb (4058 \AA\ line).
We could measure Al only for the star Ru$_{1614}$. For the other targets we
give upper limits. Element abundances are reported in Tab.~\ref{t2} and
Fig.~\ref{f2}.

A detailed internal error analysis was performed by varying T$_{\rm eff}$, log(g), [Fe/H], and
v$_{\rm t}$ and redetermining abundances of star \#Ru$_{1951}$, assumed to represent
the entire sample. Parameters were varied by $\Delta$T$_{\rm eff}$=+30 K,
$\Delta$log(g)=+0.09, $\Delta$[Fe/H]=+0.05 dex, and $\Delta$v$_{\rm t}$=+0.03
km/s. This estimation of the internal errors for atmospheric parameters was
performed as in \citet{Ma08}.
Results are shown in Tab.~\ref{t3}, including the error due to the noise
of the spectra. This error was obtained for elements whose abundance was
obtained by EQWs, as the average value of the errors of the mean given by
MOOG, and for elements whose abundance was obtained by spectrum-synthesis, as
the error given by the fitting procedure. $\sigma_{\rm tot}$ is the
squared sum of the single errors, while $\sigma_{\rm obs}$ is the mean
observed dispersion. The agreement between the two values is
well within 3$\sigma$ for all elements, indicating that there is no evidence for chemical
inhomogeneity for the 9 giants studied in Ruprecht 106. This is our principle finding.
Only for Ce we have a 3$\sigma$ difference, while for Sm $\sigma_{\rm tot}$ differs from
$\sigma_{\rm obs}$ by 6$\sigma$ and is larger. This suggests some
overestimation of the internal error.

\begin{deluxetable}{lccccccccccc}
\tablecolumns{13}
\tablewidth{0pc}
\tablecaption{Columns 2-10: abundances of the observed stars. Column 11: mean abundance for the cluster.
Column 12: abundances adopted for the Sun in this paper.
Abundances for the Sun are indicated as log$\epsilon$(El.)}
\tablehead{
El. & \colhead{Ru$_{1445}$}& \colhead{Ru$_{1614}$}& \colhead{Ru$_{1863}$}&
\colhead{Ru$_{1951}$}& \colhead{Ru$_{2004}$}& \colhead{Ru$_{2032}$}&
\colhead{Ru$_{676}$}& \colhead{Ru$_{801}$}& \colhead{Ru$_{970}$}& Cluster & Sun
}
\startdata
\hline
${\rm [O/Fe]}$  &  -0.15 &  +0.02 &  -0.13 &  -0.06 &  -0.03 &  +0.00 &  -0.10 &  -0.05 &  -0.14 & -0.07$\pm$0.02& 8.83\\
${\rm [Na/Fe]}$ &  -0.41 &  -0.45 &  -0.44 &  -0.56 &  -0.50 &  -0.46 &  -0.43 &  -0.51 &  -0.44 & -0.46$\pm$0.02&  -  \\
${\rm [Na/Fe]_{NLTE}}$ &  -0.61 &  -0.65 &  -0.64 &  -0.76 &  -0.70 &  -0.66 &  -0.63 &  -0.71 &  -0.64 & -0.66$\pm$0.02& 6.32\\
${\rm [Mg/Fe]}$ &  -0.07 &  -0.03 &  -0.04 &  +0.03 &  -0.05 &  -0.02 &  +0.00 &  +0.04 &  -0.03 & -0.02$\pm$0.01& 7.56\\
${\rm [Al/Fe]}$ &$<$-0.31&  -0.43 &$<$-0.54&$<$-0.24&$<$-0.47&$<$-0.54&$<$-0.01&$<$+0.08&$<$-0.41& -0.43$\pm$0.10& 6.43\\
${\rm [Si/Fe]}$ &  +0.09 &  +0.03 &  -0.02 &  -0.02 &  -0.06 &  +0.03 &  -0.03 &  +0.04 &  -0.08 & +0.00$\pm$0.02& 7.61\\
${\rm [Ca/Fe]}$ &  +0.06 &  -0.10 &  +0.02 &  +0.00 &  -0.03 &  +0.00 &  +0.03 &  -0.01 &  +0.04 & +0.00$\pm$0.02& 6.39\\
${\rm [Sc/Fe]}$ &  -0.45 &  -0.29 &  -0.41 &  -0.33 &  -0.28 &  -0.34 &  -0.40 &  -0.36 &  -0.47 & -0.37$\pm$0.03& 3.12\\
${\rm [Ti/Fe]}$ &  -0.07 &  -0.06 &  -0.07 &  -0.02 &  -0.02 &  -0.05 &  -0.08 &  -0.16 &  -0.03 & -0.06$\pm$0.01& 4.94\\
${\rm [V/Fe]}$  &  -0.44 &  -0.60 &  -0.54 &  -0.58 &  -0.51 &    -   &    -   &    -   &  -0.53 & -0.53$\pm$0.02& 4.00\\
${\rm [Cr/Fe]}$ &  -0.16 &  -0.14 &  -0.18 &  -0.08 &  -0.11 &  -0.17 &  -0.14 &  -0.17 &  -0.12 & -0.14$\pm$0.01& 5.63\\
${\rm [Mn/Fe]}$ &  -0.34 &  -0.38 &  -0.33 &  -0.33 &  -0.28 &  -0.38 &  -0.40 &  -0.42 &  -0.30 & -0.35$\pm$0.02& 5.37\\
${\rm [Fe/H]}$  &  -1.52 &  -1.44 &  -1.49 &  -1.39 &  -1.46 &  -1.49 &  -1.52 &  -1.51 &  -1.42 & -1.47$\pm$0.02& 7.50\\
${\rm [Co/Fe]}$ &  -0.15 &  -0.08 &  -0.11 &  -0.30 &  -0.12 &    -   &  -0.05 &    -   &    -   & -0.14$\pm$0.04& 4.93\\
${\rm [Ni/Fe]}$ &  -0.29 &  -0.25 &  -0.26 &  -0.28 &  -0.24 &  -0.34 &  -0.31 &  -0.37 &  -0.27 & -0.29$\pm$0.01& 6.26\\
${\rm [Cu/Fe]}$ &  -0.71 &  -0.88 &  -0.76 &  -0.86 &  -0.80 &    -   &    -   &  -0.72 &  -0.74 & -0.78$\pm$0.03& 4.19\\
${\rm [Zn/Fe]}$ &  -0.04 &  -0.02 &  -0.30 &  -0.13 &  -0.20 &  -0.30 &  -0.30 &  -0.31 &  -0.22 & -0.20$\pm$0.04& 4.61\\
${\rm [Y/Fe]}$  &  -0.79 &  -0.67 &  -0.74 &  -0.65 &  -0.63 &  -0.75 &  -0.80 &  -0.80 &  -0.69 & -0.72$\pm$0.02& 2.25\\
${\rm [Zr/Fe]}$ &  -0.18 &  -0.27 &  -0.15 &  -0.26 &  -0.22 &  -0.16 &  -0.12 &  -0.09 &  -0.09 & -0.19$\pm$0.02& 2.56\\
${\rm [Ba/Fe]}$ &  -0.53 &  -0.42 &  -0.46 &  -0.46 &  -0.41 &  -0.42 &  -0.55 &  -0.45 &  -0.47 & -0.46$\pm$0.02& 2.34\\
${\rm [La/Fe]}$ &  -0.33 &  -0.25 &  -0.26 &  -0.26 &  -0.25 &  -0.23 &  -0.31 &  -0.27 &  -0.31 & -0.27$\pm$0.01& 1.26\\
${\rm [Ce/Fe]}$ &  -0.54 &  -0.60 &  -0.54 &  -0.59 &  -0.64 &  -0.59 &  -0.56 &  -0.50 &  -0.65 & -0.58$\pm$0.02& 1.53\\
${\rm [Pr/Fe]}$ &    -   &  -0.15 &  -0.18 &  -0.23 &  -0.13 &    -   &    -   &    -   &    -   & -0.17$\pm$0.02& 0.71\\
${\rm [Nd/Fe]}$ &  -0.42 &  -0.39 &  -0.40 &  -0.38 &  -0.43 &  -0.43 &  -0.42 &  -0.35 &  -0.37 & -0.40$\pm$0.01& 1.59\\
${\rm [Sm/Fe]}$ &    -   &  -0.11 &    -   &  -0.08 &  -0.04 &  -0.02 &    -   &    -   &  -0.12 & -0.07$\pm$0.02& 0.96\\
${\rm [Eu/Fe]}$ &  -0.23 &  -0.13 &  -0.20 &  -0.18 &  -0.07 &  -0.16 &  -0.28 &  -0.16 &  -0.26 & -0.19$\pm$0.02& 0.52\\
${\rm [Dy/Fe]}$ &    -   &  -0.60 &    -   &  -0.37 &  -0.36 &    -   &  -0.18 &  -0.28 &  -0.19 & -0.33$\pm$0.06& 1.10\\
${\rm [Pb/Fe]}$ &  -0.20 &  -0.21 &  -0.34 &  -0.40 &  -0.25 &  -0.27 &  -0.30 &  -0.12 &  -0.19 & -0.25$\pm$0.03& 1.98\\
\hline
\enddata
\label{t2}
\end{deluxetable}

\begin{figure}
\epsscale{1.00}
\plotone{f2B.eps}
\caption{Element abundance for the single stars (red crosses) and for the
cluster mean (black filled circles). See text for more details.}
\label{f2}
\end{figure}

\section{Results and comparison with literature}

In the following sections, we will discuss in detail our results.
In addition, we will compare them with the literature,
and specifically with \citet{Bu90}, \citet{Sa97}, \citet{DC92}, \citet{Fr97}, \citet{Br97},
\citet{Do11}. The first two give a photometric metallicity, while the
third and the fourth give a spectroscopic metallicity using low-resolution
spectra. \citet{DC92} use the Ca triplet method, while \citet{Fr97}
use a global-fitting of the 4780$\div$5300 \AA\ region including all
the spectral lines. The fifth gives a metallicity based on high-resolution
spectra including [Fe/H] and [O/Fe]. \citet{Bu90} and \citet{Do11}
also discuss the age of the cluster.

\subsection{Iron-peak and $\alpha$ elements}

We found a mean [Fe/H] value for the cluster of:

\begin{center}
{\rm [Fe/H]=-1.47$\pm$0.02 dex}
\end{center}

All the other Fe-peak elements (Sc,V,Cr,Mn,Co,\\ Ni,Cu, and Zn) are underabundant
with respect to Fe, with a range for [El/Fe] between -0.14 dex (Cr and Co) and -0.78 dex (Cu).
The chemical abundances for the $\alpha$ elements O, Mg, Si, Ca, and Ti listed
in Table \ref{t2} are solar scaled or slightly underabundant.
If we use Mg, Si, Ca, and Ti to estimate a mean $\alpha$-element value (O will
be treated separately) we obtain:

\begin{center}
{\rm [$\alpha$/Fe]=-0.02$\pm$0.01 dex}
\end{center}

We conclude that the cluster is solar-scaled as far as $\alpha$-elements are
concerned, in agreement with \citet{Br97}, and at odds with all the other Galactic
GCs of low metallicity. However this behavior is common among
extragalactic objects. We will further discuss $\alpha$ and iron-peak
elements in section 7.

Our results permit us also to explain the disagreement of metallicities
in the literature. Many authors (\citealt{Bu90}, [Fe/H]$\sim$-2; \citealt{Sa97},
[Fe/H]=-1.90; \citealt{DC92}, [Fe/H]=-1.69; \citealt{Fr97}, [Fe/H]=-1.9)
who obtained a metallicity based on photometry (slope and/or color of the RGB) or low-resolution
spectroscopy (Ca triplet or comparison with low-resolution synthetic spectra)
implicitly assumed a typical halo alpha-enhancement, as in all other Galactic GCs.
This fact led them to underestimate the cluster metallicity because
Ruprecht 106 simply is not $\alpha$-enhanced, so, for a given metallicity
([Fe/H]) the RGB-slope is larger or low resolution spectra are apparently
more metal-poor (e.g. the EQW of the Ca triplet is smaller) with respect to
any other GC with similar iron content. \citet{Br97} ([Fe/H]=-1.45) instead obtained a
more reliable result because they measured directly Fe lines. Their value is
in excellent agreement with our.

\subsection{Neutron-capture elements}

We measured neutron-capture elements from Y to Pb. They
are produced through the capture of a neutron by a iron-peak seed nucleus.
Once captured, the neutron decays into a proton, and a new nucleus with higher atomic
number is formed.
The capture can is considered slow if the timescale for the neutron capture is large
compared to the timescale of the nuclear decay. In this case we have the
s-process. In the case that the neutron capture is rapid compared with the
timescale of the decay, we have the r-process.
The distribution of neutron-capture elements is different in the two cases,
and a study of their relative abundance gives
information on the relative importance of the two processes on the
contamination of the gas the cluster was formed from.
Because the s-process happens in low-mass AGB stars (1.5-3 M$_{\odot}$,
\citealt{Bu01}), intermediate mass AGB stars (4-8 M$_{\odot}$,
\citealt{Ka07}), and possibly also in massive stars (M$>$20 M$_{\odot}$,
\citealt{Pi08}), while the r-process most
probably occurs in SNeII explosions, abundances of neutron-capture
elements tell us how these kind of stars contributed to the formation of the
cluster.
For this purpose in Fig.~\ref{f3} we plotted the abundance of Ba, La, Pr, Nd,
Sm, Eu, Dy, and Pb. On our data we superposed the two abundance curves
of the pure s (dashed black line) and r (continuous black line) process taken from \citet{Sn08}. Ba and
Pb were used to set the
zero-point of the pure s and pure r process curves (see below), while La, Pr, Nd, Sm, Eu,
and Dy are those elements more sensitive to the s and r processes.
The Ce abundance does not
follow any curve in Fig.~\ref{f3}, probably because
of some non-negligible systematic error in our abundance estimation for this
element, so we decided not to use it in our investigation.
The two curves were shifted in the y direction in order to match the Ba and Pb
abundances that are the same for the two processes. Abundances of the other
elements are in between the two curves and the best fitting line (the blue
continuous line) indicates  that r-process contributed 66\% and s-process
34\% to the cluster abundances. This result is confirmed by the mean
log$\epsilon$(La/Eu) of the cluster, that is:

\begin{center}
{\rm log$\epsilon$(La/Eu)=0.65$\pm$0.02}
\end{center}

According to \citet[Fig. 4]{Ro09}, this corresponds to a contribution of 71\%
from the r-process. We can summarize these results by estimating that r-process contributed
a 68.5$\pm$2.5\% and s-process a 31.5$\pm$2.5\% to the contamination
of the primordial gas the cluster was formed from.

\begin{deluxetable}{lccccccc}
\tablecolumns{8}
\tablewidth{0pc}
\tablecaption{Estimated errors on abundances due to errors on atmospheric
parameters and to spectral noise compared with the observed errors.}
\tablehead{
ID & \colhead{$\Delta$T$_{\rm eff}$=30 K}  & \colhead{$\Delta$log(g)=0.09} &
\colhead{$\Delta$v$_{\rm t}$=0.03 km/s}  & \colhead{$\Delta$[Fe/H]=0.05} & S/N
& \colhead{$\sigma_{\rm tot}$} & \colhead{$\sigma_{\rm obs}$}
}
\startdata
\hline
$\Delta$([O/Fe])  & 0.03 & 0.06 & 0.03 & 0.02 & 0.02 & 0.08 & 0.06$\pm$0.02\\
$\Delta$([Na/Fe]) & 0.01 & 0.01 & 0.00 & 0.01 & 0.05 & 0.05 & 0.05$\pm$0.01\\
$\Delta$([Mg/Fe]) & 0.02 & 0.01 & 0.00 & 0.01 & 0.05 & 0.06 & 0.04$\pm$0.01\\
$\Delta$([Al/Fe]) & 0.01 & 0.00 & 0.01 & 0.01 & 0.05 & 0.08 & -            \\
$\Delta$([Si/Fe]) & 0.03 & 0.01 & 0.01 & 0.01 & 0.05 & 0.06 & 0.05$\pm$0.01\\
$\Delta$([Ca/Fe]) & 0.00 & 0.00 & 0.00 & 0.00 & 0.04 & 0.04 & 0.05$\pm$0.01\\
$\Delta$([Sc/Fe]) & 0.04 & 0.05 & 0.02 & 0.01 & 0.01 & 0.07 & 0.07$\pm$0.02\\
$\Delta$([Ti/Fe]) & 0.02 & 0.00 & 0.00 & 0.01 & 0.03 & 0.04 & 0.04$\pm$0.01\\
$\Delta$([V/Fe])  & 0.02 & 0.01 & 0.00 & 0.01 & 0.08 & 0.08 & 0.06$\pm$0.02\\
$\Delta$([Cr/Fe]) & 0.02 & 0.00 & 0.00 & 0.00 & 0.03 & 0.04 & 0.03$\pm$0.01\\
$\Delta$([Mn/Fe]) & 0.01 & 0.01 & 0.01 & 0.00 & 0.04 & 0.04 & 0.05$\pm$0.01\\
$\Delta$([Fe/H])  & 0.04 & 0.01 & 0.01 & 0.01 & 0.01 & 0.05 & 0.05$\pm$0.01\\
$\Delta$([Co/Fe]) & 0.01 & 0.00 & 0.00 & 0.01 & 0.08 & 0.08 & 0.09$\pm$0.03\\
$\Delta$([Ni/Fe]) & 0.00 & 0.00 & 0.00 & 0.00 & 0.02 & 0.02 & 0.04$\pm$0.01\\
$\Delta$([Cu/Fe]) & 0.01 & 0.00 & 0.00 & 0.01 & 0.05 & 0.05 & 0.07$\pm$0.02\\
$\Delta$([Zn/Fe]) & 0.06 & 0.02 & 0.01 & 0.01 & 0.08 & 0.10 & 0.11$\pm$0.03\\
$\Delta$([Y/Fe])  & 0.04 & 0.04 & 0.02 & 0.00 & 0.08 & 0.10 & 0.07$\pm$0.02\\
$\Delta$([Zr/Fe]) & 0.05 & 0.04 & 0.02 & 0.02 & 0.04 & 0.08 & 0.07$\pm$0.02\\
$\Delta$([Ba/Fe]) & 0.02 & 0.05 & 0.02 & 0.03 & 0.01 & 0.07 & 0.05$\pm$0.01\\
$\Delta$([La/Fe]) & 0.04 & 0.03 & 0.02 & 0.00 & 0.02 & 0.06 & 0.04$\pm$0.01\\
$\Delta$([Ce/Fe]) & 0.05 & 0.04 & 0.01 & 0.01 & 0.04 & 0.08 & 0.05$\pm$0.01\\
$\Delta$([Pr/Fe]) & 0.02 & 0.04 & 0.01 & 0.00 & 0.05 & 0.07 & 0.04$\pm$0.02\\
$\Delta$([Nd/Fe]) & 0.02 & 0.03 & 0.01 & 0.00 & 0.02 & 0.04 & 0.03$\pm$0.01\\
$\Delta$([Sm/Fe]) & 0.02 & 0.05 & 0.03 & 0.02 & 0.07 & 0.10 & 0.04$\pm$0.01\\
$\Delta$([Eu/Fe]) & 0.04 & 0.05 & 0.03 & 0.02 & 0.02 & 0.08 & 0.07$\pm$0.02\\
$\Delta$([Dy/Fe]) & 0.01 & 0.07 & 0.02 & 0.01 & 0.02 & 0.08 & 0.15$\pm$0.04\\
$\Delta$([Pb/Fe]) & 0.04 & 0.01 & 0.01 & 0.02 & 0.03 & 0.06 & 0.09$\pm$0.02\\
\hline
\enddata
\label{t3}
\end{deluxetable}

\begin{figure}
\epsscale{1.00}
\plotone{f3.eps}
\caption{Abundance pattern of heavy neutron-capture elements.
Red points represent single stars, while black points the mean abundance for
the cluster. Continuous and dashed lines are pure r and s process patterns
respectively. Continuous blue line is the best fit to our data.}
\label{f3}
\end{figure}

\section{Ruprecht 106 as the first single population GC}

As mentioned in the Introduction, other
GCs have been proposed as single population objects, like Palomar 3 \citep{Ca11},
due to the small extension of its red HB. \citet{Ko09} studied
spectroscopically four bright RGB stars in this cluster, but due to the low
S/N and the small statistics they could not prove the presence or absence of
a spread in light elements, and so they could not confirm or
reject the \citet{Ca11} hypothesis.
The main aim of this paper is to verify if Ruprecht 106 might be the first
bonafide example of a single population old Galactic GC.
For this purpose we report in Fig.~\ref{f4} the Na-O abundances of our 9 stars
(black points with errorbars). In this figure, for comparison, we report also
data for the GCs studied in \citet[filled cyan squares]{Ca09}, NGC~1851 \citep[filled blue
circles]{Vi10}, NGC~2808 \citep[filled black squares]{Ca06}, M4 \citep[open magenta
circles]{Vi11}, M22 \citep[open red squares]{Ma09}, old (filled green
circles) and intermediate-age (other open green symbols) clusters in the LMC studied by
\citet{Mu08,Mu09}, and the Sagittarius cluster Terzan 7 \citep[open black stars]{Sb07}.
Open red stars represent the two targets in Ruprecht 106 studied by \citet{Br97}. These stars are
\#Ru$_{\rm 1614}$ and \#Ru$_{\rm 2004}$ and the authors find
[O/Fe]=-0.05,+0.08 and [Na/Fe]=-0.47,-0.44 respectively. Their Na abundance is based
on the 8190 \AA\ doublet so, according to \citet{Ma00}, a NLTE correction of
$\sim$-0.2 dex looks appropriate. The agreement with our results is good.

\begin{figure*}[ht!]
\epsscale{2.00}
\plotone{f4.eps}
\caption{[Na/Fe] vs. [O/Fe] in GCs. Filled cyan squares: GCs from
\citet{Ca09}. Filled blue circles: NGC~1851. Filled black squares:
NGC~2808. Filled red squares: M22. Filled magenta circles: M4. Filled green
circles: Old LMC clusters. Open green symbols: intermediate-age LMC clusters.
Open black stars: Terzan 7. Filled black circles: Ruprecht 106 (this paper). Open red
stars: Ruprecht 106 by \citet{Br97}. See text for more details.}
\label{f4}
\end{figure*}

Ruprecht 106 stars define a clump at [O/Fe]=-0.07 dex and [Na/Fe]=-0.66 dex
that has no intrinsic dispersion. This is confirmed by
Tab.~\ref{t3}, where the theoretical spread ($\sigma_{\rm tot}$)  matches very
well within the errors with the observed spread ($\sigma_{\rm obs}$) both for
O and Na. This is true also for the other elements.
This confirms our initial hypothesis that  Ruprecht 106 is the first
example of a single population GC, although it is possible that nature has
conspired against us and we simply did not detect a true spread. See below
for further discussion of this point. Recall that the Na-O
anticorrelation has been used to define a GC \citep{Ca09}, so its
absence in Ruprecht 106 is of particular importance.

However Fig.~\ref{f4} has several other interesting implications.
First of all Ruprecht 106 occupies a totally unique position in this diagram
(see Section 7 for further discussion).
In addition, among Galactic GCs at least two distinct Na-O anticorrelations appear, that are
plotted as red lines. One is O-richer (continuous line) and represented by the
trend of the stars in M4 and M22, while the other is O-poorer (dashed line) and
represented by the trend of the stars in NGC~1851 and NGC2808. This fact can be
explained by the $\alpha$-enhancement a cluster was formed with and remembering
that O is an $\alpha$ element too.
If first generation stars in a cluster were born relatively O-poor (with
respect to the continuous line of Fig.~\ref{f4}), second generation stars
will also share the same chemical behavior.

As an example, NGC~1851 and M4 have a difference
in their $\alpha$-enhancement of 0.07 dex (as defined by the mean abundance of
Si and Ca), while the difference between their O content is $\sim$0.1 dex
among the entire Na-O anticorrelation. So the O content of second generation
stars does not depend only on the internal chemical evolution of the clusters,
but also on the primordial O abundance of the progenitor cloud.

Old LMC clusters also follow the general Galactic trend, but this is not the case for
intermediate-age LMC clusters and Terzan 7 which do not show an appreciable spread in O. On the other
hand three of them show a possible spread in Na (NGC~1651: open green circles,
NGC~1978: green crosses, NGC~2173: open green stars). NGC~1978 also shows a
hint of a Na-O anticorrelation. Only two clusters (NGC~1783: open green squares) and Terzan 7 have a
small dispersion in Na, possibly compatible with zero, but still larger then
Ruprecht 106, but all of these samples are relatively small.

In Fig.~\ref{f4} the region presumably inhabited by first generation stars in Galactic
and LMC globular cluster is indicated by a large black circle.
Even if Ruprecht 106 does not fit at all with any known Milky Way or LMC cluster,
we can still state that these stars still correspond to the first generation.
This is because this first generation is characterized by the fact that
[O/Fe]=[$\alpha$/Fe] within 0.1 dex (where $\alpha$ is defined as
the mean abundance of Si and Ca). Second generations stars
have [O/Fe]$<$[$\alpha$/Fe]. As an example, in M4 stars of the first generation ([$\alpha$/Fe]=+0.42)
have [O/Fe]=+0.42 dex, while stars of the second have [O/Fe]=+0.25 (the
difference with respect the $\alpha$-enhancement is -0.17 dex).
This behavior is expected because the first generation was
born from fresh material, enhanced in all $\alpha$-elements,
including O. Instead the second generation was born from O-depleted material,
which however had other $\alpha$-elements untouched.
For Ruprecht 106 we found that the O content is only slightly lower than other
$\alpha$-elements (0.07 dex), so we can say that the observed stars correspond to the first
generation.
With this information we can answer the following question: what is the
probability that we have missed a second generation if present? \citet{Ca09}
found that $\sim$30-40\% of stars now remaining in a GC belong to the first generation. We observed
9 stars and all belong to it. So the probability that we have
missed the second population is:

\begin{center}
{\rm P$\sim$0.35$^{9}$=0.00008=0.008\%}
\end{center}

This probability is low enough to confidently state that we did not miss any
cluster sub-population. This would be true (however not in as clear a way)
also if our stars had belonged to the second generation, for which we would
obtain P=2\%. However, we recognize that our sample is still small,
especially compared to the samples generally used to define the Na-O
anticorrelation often with $>$100 stars. Spectra of additional stars in Ruprecht
106 would be most welcome.

Another relevant piece of evidence comes from the HB.
It has a dispersion in color of $\sim$0.2 mag (see Fig.~\ref{f1}).
According to \citet{Ca11} a dispersion of 0.3 mag or lower is an indication
that no multiple populations are present in a cluster. So this fact further
reinforces our main result.

The last possibility could be that Rup 106 represents one of those
first generation-mainly clusters, where a second generation is present but not dominant
\citep{Ca11}. However in this case we should still see a HB extended to the
blue because second generation HB stars populate a hotter and bluer HB part
than first generation stars as discussed in the introduction. In Rup 106 this
would correspond to HB stars with (V-I)$<$0.5 (see Fig.~\ref{f1}), where no
stars at all are present.
On the other hand the chances that Rup 106 is such an object are decreased by
the fact that first generation-mainly clusters are assumed to not have filled
their tidal radius and thus did not lose many first generation stars. However,
odds with this, Rup 106 is known to be a tidally-filling cluster \citep{Ba11}.
In conclusion, the evidence strongly points to Rup 106 asa first generation
only cluster.

Considering the above factors, we conclude that it is very likely that
Ruprecht 106 is the first confirmed example of a single population, globular cluster.

What about other possible candidates?
One is Palomar 3. \citet{Ca11} suggested it as a single
population cluster based on its HB, that has a color spread of 0.25 mag (see
their Fig. 2). For Ruprecht 106 instead we found a value $\leq$0.20 mag (see Fig.~\ref{f1}).
On the spectroscopic side, \citet{Ko09} found that the observed Na spread in
Palomar 3 slightly exceeds that expected from theoretical errors and is not accompanied
by a spread in O. This is not surprising because Palomar 3 stars are
located in a region of the Na-O anticorrelation where little or no O variation
is expected.
In our opinion, these results together suggest that
Palomar 3 has a small but real spread in light elements, and it is therefore
probably not an example of a single population GC. In addition only 4 stars
have been observed at high resolution.
On the other hand, NGC~1783 and Terzan 7 have a dispersion in Na of 0.10
and 0.12 dex respectively, larger then Ruprecht 106, but that could be due to
larger internal errors. So they could be single population GCs.
In any case for these three clusters further investigation is required to
reveal their nature. Obviously, it is of interest to observe other possible
candidate single-population GCs.

We finally note that these candidates are extragalactic or, in the case of
Palomar 3, probably have an extragalactic origin \citep{Ca11}. This is true
also for Ruprecht 106 (see next section). A possible reason could be that all
low mass single population Galactic GC were destroyed due to the tidal
interaction with the Milky Way, or simply they did not form at all.
However, most low mass GCs have not been adequately investigated yet.

\begin{figure}[ht!]
\epsscale{1.10}
\plotone{f5b.eps}
\caption{Upper pannel: V vs. U-R CMD of the cluster zoomed on the RGB.
Lower pannel: V vs. B-R CMD of the cluster zoomed on the RGB.}
\label{f5b}
\end{figure}

\begin{figure}[ht!]
\epsscale{1.00}
\plotone{f5.eps}
\caption{Na-O anticorrelation. Filled cyan triangles:
Draco, Sextans, and Ursa Minor dwarf galaxies. Filled blue squares:
Sagittarius dwarf galaxy. Filled green circles: LMC. Open black
circles: GCs from \citet{Ca09}. Filled black circle: Ruprecht 106.
See text for more details.}
\label{f5}
\end{figure}

\section{Additional photometric evidence}

It now well known that the U filter is able to disentagle multiple populations along
the RGB of Globular Clusters \citep{Ma08,Sb11} due to its sensitivity to
chemical inhomogeneities.
For this purpose we extracted photometric material for
Ruprecht 106 from the ESO public archive
\footnote{http://archive.eso.org/eso/eso\_ archive\_ main.html}.
It consists of a series of images in UBVRI taken with the SUperb Seeing Imager (SUSI2) at
La Silla Observatory on the night of July 21, 2002.
The detector has a scale of 0.08 arcsec/pixel, allowing to cover
5.5$\times$5.4 arcmin on the sky.

This data-set has the widest optical wavelength coverage for Ruprecht 106 available, and it is
ideal to study the detailed shape of the Red Giant Branch. The night was
photometric according to the weather report from ESO La Silla, with an average
seeing of 0.8 arcsec in the V pass-bands. Exposures range from 30 to 900 in U,
B, V, and R. The cluster was also observed in I, but the images show
significant fringing, which made it impossible to extract good
photometry. Only the north-east portion of the cluster was surveyed.
After pre-reduction (bias and flat-field corrections) images have been reduced
using the DAOPHOT/ALLSTAR routines. SUSI2 has two detectors, which have been
separated and reduced individually. The two extracted catalogs have then
been merged.
To tie the instrumental photometry to the standard system we used  the average
zero-points and color terms reported in the website of the instrument.
\footnote{http://www.eso.org/sci/facilities/lasilla/}.

In Fig.~\ref{f5b} we present a zoom on the RGB region in 2 different
color combinations: V vs. U-R in the upper panel, and V vs. B-R in the lower,
to maximize the color range of the stars. The V vs. B-R combination was
included as a reference only, because colors other than U are not as sensitive to
chemical inhomogeneities.
We use the metallicity derived in this paper to fit the star distribution
with theoretical isochrones (red lines) from the Padova database \citep{Mar08}.
We find that the best-fitting parameters are an age of 12 Gyrs, a reddening E(B-V) =0.19,
and an apparent distance modulus (m-M)$_{\rm V}$= 17.20 mag.  Both reddening and
distance modulus are in good agreement with the literature value.

Color-coded in blue is the region where bona-fine
RGB stars are located. Lacking any quantitative membership, these have been
selected as the RGB stars lying within the cluster core region (core radius=1.0 arcmin, \citealt{Ha96}).
Photometric errors, in magnitude and color, are also indicated with
error-bars color-coded in black.
To investigate a possible intrinsic photometric spread in the RGB, we compared
its observed color scatter with the natural width expected from considering the
photometric errors only. These are calculated as

\begin{center}
$\sigma_{B-R}=2\times \sqrt(\sigma_B^2 + \sigma_R^2)$
$\sigma_{U-R}=2\times \sqrt(\sigma_U^2 + \sigma_R^2)$
\end{center}

depending on the CMD. As for the observed color scatter at a given V, we simply
consider the difference in color  $\Delta (B-R)$, and $\Delta (U-R)$ between
the two most separated stars in the RGB at about the same V. This is because
the RGB is not very rich, and therefore any other statistical calculation
would be not robust.
The results for 4 different V magnitudes are reported directly
in the figure as $\sigma$/$\Delta$ with their errors.
Apart from the value at V = 17, where no RGB stars are located, the
ratios are compatible with 1 within the errors, indicating that the RGB is not
wider than the amount expected from photometric errors only.
We therefore conclude that this photometric dataset supports
the spectroscopic result that no significant spread exists among
Ruprecht 106 RGB stars.

We can further compare our (U-R) vs. V CMD with that for M4 \citep[(U-B) vs
U, Fig. 11]{Ma08}. M4 has a very broad RGB with a spread of $\sim$0.2
mag. in color. At odds with this, the Rup 106 RGB spread is only 0.1
mag. Because M4 has one of the lowest Na-O spreads among GCs
\citep{Ca09}, we conclude that this photometry further supports our
spectroscopic result.

\section{Comparison with Galactic and extragalactic environments}

The position of Ruprecht 106 stars in Fig.~\ref{f4} is extraordinary. They do not fit
any Na-O trend defined by Galactic GC.
This is an indication that Ruprecht 106 has an extragalactic origin.
In order to investigate this point more deeply, we compare our results with
Galactic and extragalactic environments.
For this purpose, we plotted in Fig.~\ref{f5} data for Galactic GCs
\citep[open black circles]{Ca09} to trace the Na-O trend for the Galactic
Halo. In addition we added data for the LMC field and cluster stars \citep[green filled
circles]{Jo06,Po08,Mu08,Mu09}, Sagittarius dwarf galaxy field and cluster
stars \citep[filled blue squares]{Sb07}, the Draco, Sextans, and Ursa
Minor dwarf galaxy field stars \cite[filled cyan triangles]{Sh01}.
The continuous red line indicates the mean trend for a Galactic GCs. The main result
is that, while the area occupied by the Galactic stars is common also to
the extragalactic objects, there is a region occupied only by extragalactic
stars, indicated by the shaded region, that are more Na-poor with respect to the
Galactic Halo.
Ruprecht 106 (the filled black circle) lies at the opposite extreme of this
area, and because of this it can be considered with high confidence an extragalactic
object.

Additional support for an extragalactic origin comes from Fig.~\ref{f6}. Here we plot the [$\alpha$/Fe]
vs. [Fe/H] relation for extragalactic stars defined as in Fig.~\ref{f5} and
galactic field stars (red crosses) from the following sources:
\citet{Fu00,Ca04,Re03,Ba05,Re06}. In this plot we added also LMC stars from
\citet{Mo05}.
[$\alpha$/Fe] was defined as the mean abundance of Mg, Si, Ca, and Ti except
for \citet{Po08,Ba05,Mo05} for which we used Mg, Ca, and Ti. For \citet{Mu09}
we were forced to use the only $\alpha$-element available (besides O), i.e. Mg.
In any case, stars from \citet{Mu09} follow the general trend of the LMC.
First of all, in Fig.~\ref{f6} we identified a double trend of [$\alpha$/Fe]
vs. [Fe/H] for the Galaxy, where stars define a first continuous path from
[Fe/H]$\sim$-3.5 dex up to  [Fe/H]$\sim$-0.2 dex, indicated by the upper black
dashed line. The second continuous path goes from [Fe/H]$\sim$-1.2 up to
[Fe/H]$\sim$+0.2 and is indicated by the lower black dashed line.
Between the two trends there is an almost empty region indicated by the blue
shaded area. This result is not new and was recently noticed by \citet{Ad11}.
These authors found two distinct [$\alpha$/Fe] vs. [Fe/H] trends among
Galactic stars, with an almost empty region between them (see their Fig. 1),
exactly as in our case.
Apart from that, we can see that extragalactic stars have the same mean
$\alpha$-enhancement as the Milky Way up to [Fe/H]$\sim$-1.5. More metal rich
extragalactic stars instead tend to have a much lower $\alpha$ content than
Galactic stars of the same metallicity.
The black shaded area indicates the region populated only by
extragalactic objects.
Again Ruprecht 106 (the filled black circle) lies in this area well removed
from any Galactic star.

Finally in Fig.~\ref{f7} we compare the Ni and Cu content of Rup 106 with
Galactic and extragalactic stars. Literature sources are those discussed above.
Solar-scaled abundances are shown as continuous black lines for reference.
As far as Ni is concerned, Galactic stars follow a solar-scaled trend with a
large spread for [Fe/H]$<$-2. On the other hand, extragalactic objects are
solar scaled below [Fe/H]=-1.5. Then they start to deviate, reaching
[Ni/Fe]$\sim$-0.5 for solar metallicity. Rup 106 is located at the metallicity
where the deviation starts, but below the Galactic trend and fully compatible
with extragalactic targets.

As for Cu, Galactic stars follow a solar scaled trend down to
[Fe/H]$\sim$-0.9. Below that metallicity they drop to
[Cu/Fe]$\sim$-0.4. Extragalactic targets are more Cu poor on average with
$<$[Cu/Fe]$>$$\sim$-0.6 regardless of the iron content. Although the number of
Galactic stars at the metallicity of Ruprecht 106 is very small, our
cluster is again located below the Galactic trend and fully compatible with
extragalactic targets, once again pointing to an extragalactic origin.

It is of course very difficult to say where Ruprecht 106
comes from. It was suggested initially to be part of the  Sagittarius dwarf
galaxy \citep{Be03}, but \citet{La10} discarded this hypothesis because it does not belong
to any possible stream of this system, so we regard its exact origin as an
open question, but an extragalactic formation is strongly favoured by our data.

\begin{figure}[ht!]
\epsscale{1.00}
\plotone{f6.eps}
\caption{[$\alpha$/Fe] vs. [Fe/H]. Filled cyan triangles:
Draco, Sextans, and Ursa Minor dwarf galaxies. Filled blue squares:
Sagittarius dwarf galaxy. Filled green circles: LMC. Red
crosses: Milky Way. Filled black circle: Ruprecht 106.
See text for more details.}
\label{f6}
\end{figure}

\begin{figure}[ht!]
\epsscale{1.00}
\plotone{f7.eps}
\caption{[Ni/Fe] vs. [Fe/H] and [Cu/Fe] vs. [Fe/H]. Filled cyan triangles:
Draco, Sextans, and Ursa Minor dwarf galaxies. Filled blue squares:
Sagittarius dwarf galaxy. Filled green circles: LMC. Red
crosses: Milky Way. Filled black circle: Ruprecht 106.
See text for more details.}
\label{f7}
\end{figure}

\section{Summary and conclusions}

In this paper we present detailed chemical abundances of red giants in the globular
cluster Ruprecht 106. We studied 29 elements from C to Pb, including light,
$\alpha$, iron-peak, and neutron-capture. Our main aim was to investigate if
Ruprecht 106 is a single population GC.
All GCs studied up to now show some spread in their chemical abundances. There are a
few examples where no spread was found, but those results are doubtful due to the
small sample of stars observed and to the lack of an accurate error analysis.
We analyzed 9 member stars and performed an accurate error abundance analysis.
We found that the observed spread in all elements, in particular Na and O, is
totally within the measurement errors.
We calculated also a negligible probability of having missed stars with an intrinsic
difference in their chemical content with respect to our targets given the
nominal ratio of first to second generation stars.
This is also confirmed by the small color spread of the HB.
No intrinsic abundance spread is present in this GC in any element. Although our sample
is still relatively small and more observations would be of great
interest, our evidence strongly suggests that Ruprecht 106 is the first
genuine old, massive GC with only a single population.

In addition, we could establish the following:

\begin{itemize}
 \item Ruprecht 106 has [Fe/H]$\sim$-1.5 and [$\alpha$/Fe]$\sim$0.0.
 This solves the disagreement in the literature between metallicity measurements based on
 photometry or low resolution spectroscopy and those based on high resolution
 spectroscopy.
 \item Its neutron-capture element abundances point toward a contamination
 of the gas the cluster was formed from by both the s and r processes. The
 contamination fraction is $\sim$30\% and 70\% respectively.
 \item NGC~1783, Terzan 7, and Palomar 3 are candidate single population
 GCs. Available data are uncertain and new more accurate studies are
 required to confirm their nature.
 \item Na/O, $\alpha$, and iron-peak abundances clearly point toward an
 extragalactic origin of the cluster. No progenitor galaxy or stream have been
 clearly identified yet.

\end{itemize}

Ruprecht 106 has a present day mass of M=10$^{4.83}$ M$_{\odot}$. This is not its
initial mass because it lost a fraction of its stars due to internal precesses
and to interaction with the Milky Way. A determination of the initial mass
would require the knowledge of its orbit and a detailed dynamical
simulation. This is beyond the scope of this paper. In any case we can fix
M=10$^{4.83}$ M$_{\odot}$ as a lower limit for the initial mass threshold
below which no ejecta are retained by the gravitational potential of a cluster
and no second generation of stars is formed. Note that NGC~6838, one of the
\citet{Ca09} sample clusters, has a present day mass of M=10$^{4.30}$
M$_{\odot}$, much less than that of Ruprecht 106, but shows a real Na-O
spread. We hypothesize that NGC~6838 was originally more massive than Ruprecht
106, but subsequently lost more mass.

\acknowledgments
S.V. and D.G.gratefully acknowledge support from the Chilean
Centro de Excelencia en Astrof\'\i sica
y Tecnolog\'\i as Afines (CATA) grant PFB-06/2007.
The authors gratefully acknowledge also Ata Sarajedini who kindly provided
the ACS@HST photometry.
S.V. gratefully acknowledges the support provided by FONDECYT N. 1130721

redpajama_set_name: RedPajamaArXiv


text:
Australian supermarket chain Ritchies celebrates 150 years
Mike Wheeler July 28, 2020, 8:00 am July 28, 2020
This year, Australian supermarket chain, Ritchies, celebrates its 150th birthday.
"When Thomas Ritchie established the first Ritchies grocery store in Frankston in 1870, I don't think he could have anticipated the business growing into one of the longest running in Australia," says Fred Harrison, CEO of Ritchies Supermarkets.
Thomas Ritchie opened a general store in Frankston Victoria in 1870, with one legacy being the company's ability to give back to the communities where the stores are located. So far, Ritchies Community Benefit card has given away almost $50 million dollars over the last 25 Years to local charities.
Ritchies grew from a small local grocery store to a large group with 78 supermarkets and liquor Stores. Today, Ritchies is still a family-owned business and has a turnover in excess of $1.1 billion.
150 eyarsRitchies


Service with integrity and professionalism. That is my promise to you. I have been a Realtor for 32 years and am a lifelong Morro Bay resident. I am a past Multiple Listing Chairperson and President of our Scenic Coast Association of Realtors, along with having been a State Director for the California Association of Realtors. I was chosen REALTOR OF THE YEAR by my peers. I have attained a Senior Real Estate Specialist designation as I enjoy working with Seniors as well as the first time home buyer. I am involved in and support many community activities including the Morro Bay Yacht Club, Friends of the Morro Bay Police Dept, K-9 unit, Best Friends Animal Sanctuary, Morro Bay Pups (board member/Treasurer), and advocate for the homeless through EBAC and many other programs with children and seniors. I currently am a member of the Measure Q Oversight Committee for the City of Morro Bay. I would love to be your Realtor. Please take advantage of the years of experience I can share with you. I'm available on my cell phone at (805)235-1924 or email: Elainegnmb@aol.com. I have an extensive knowledge of the area serving clients from Paso Robles to Santa Maria.


A video demonstrating the asymmetrical tonic neck reflex (ATNR).
The asymmetrical tonic neck reflex (ATNR) is a primitive reflex found in newborn humans, but normally vanishes around six months of age.
When the face is turned to one side, the arm and leg on the side to which the face is turned extend and the arm and leg on the opposite side bend.
It is also known as the "fencing reflex" because of the characteristic position of the infant's arms and head, which resembles that of a classically trained fencer.


text:
stack: stack_template.c
	gcc stack_template.c -o stack

deque: deque_template.c
	gcc deque_template.c -o deque
clean:
	rm -f *~ *.o stack deque

redpajama_set_name: RedPajamaGithub


Cztery roku opóźniony w 1825 dwa jej stare siostry umierał -, gdy Charlotte był dziewięć, Maria starzejący się jedenaście i Elizabeth, starzeliśmy się dziesięć.
Focus groups are few and much between, and expecting to get even one a month is reaching high. They will indicate upon the top if ought to available. Not having become a proactive to help shop.
Các video sẽ tạo cho bé không khí vừa chơi vừa học, với mục đích mục đích giúp các bé nhận biết các loài động vật tốt hơn.
We supply beautiful and original quality cheap Stone Island polo shirts at the best price, with a large variety of fashionable styles cheap Stone Island to choose from.Fashion Stone Island Jackets cheap for sale!Buy cheap Stone Island from our store.
Charakter Jane Eyre wiele podobieństwa życie autor. Charlotte Bronte żyjący w ponurym moorland blisko Haworth, jej ojciec był pastorem i rodzina żył na skromnej pensi.


text:
https://planktonchronicles.org/wp-content/uploads/2015/12/backloop.webm
DIVE INTO THE HEART OF BIODIVERSITY AND EVOLUTION
Through hundreds of photographs, Plankton transports readers into the currents, where jeweled chains hang next to phosphorescent chandeliers, spidery claws jut out from sinuous bodies, and gelatinous barrels protect microscopic hearts. The creatures' vibrant colors pop out against the black pages, allowing readers to examine every eye and follow every tentacle. Jellyfish, tadpoles, and bacteria all find a place in the book, representing the broad scope of organisms dependent on drifting currents.Christian Sardet's enlightening text explains the biological underpinnings of each species while connecting them to the larger living world. He begins with plankton's origins and history, then dives into each group, covering ctenophores and cnidarians, crustaceans and mollusks, worms and tadpoles. He also demonstrates the indisputable impact of plankton in our lives.
Also available in French German Japanese and Chinese.
«Plankton: Wonders of the Drifting World» was awarded «Best Underwater World Publication» by the World Festival of Underwater Images (Marseille 2014)
QR codes inserted in the chapters of the book provide access to «Plankton Chronicles» videos for total immersion.
Plankton: Wonders of the Drifting World
University of Chicago Press (May 2015)
550 photos, 224 pages,
Hardcover, list price: $ 45
Ebook: $ 27
«Filled with more than five hundred close-ups of jewel-like diatoms and gelatinous comb jellies, each accompanied by a condensed history and biography, the book is a long overdue introduction to the oceans' ninety-eight percent.»
«It's the catalog of a mission that has revealed just how diverse and gorgeous the lowly plankton can be, and how indispensable they are to life on Earth.»
«Striking close-up photos and micrographs take center stage . . . revealing the dazzling diversity of these tiny creatures—from microscopic unicellular organisms to complex crustaceans.»
«In this beautiful book, marine scientist Christian Sardet shows that tiny plankton, not enormous blue whales, are the real stars of the ocean.»
«An extraordinary new book highlights the remarkable diversity of plankton.»
«Beautiful and informative, and written for a broad audience, Plankton: Wonders of the Drifting World should be on everyone's gift list this year.»
Photo: Dennis Allen
Christian Sardet
Christian Sardet obtained a biochemical engineering degree from l'INSA (Lyon, France) and a PhD from the University of California, Berkeley. He is a founder of the Laboratory of Cell Biology at the Marine Station of Villefranche-sur-Mer, IMEV, Centre National de la Recherche Scientifique (CNRS) and Sorbonne Université.
Presently emeritus research director at the CNRS, Christian Sardet is the author of numerous scientific publications on the cell and molecular biology of fertilization and development of embryos, and more recently on plankton. He is the recipient of the Grand Prix des Sciences de la Mer from the French Academy of Sciences. Creator of award-winning documentaries, animated films and DVDs, Christian received the European Award for Communication in Life Sciences from the European Molecular Biology Organization (EMBO).
Christian Sardet was a co-founder and one of the scientific coordinators of the Tara Oceans expedition, devoted to a global study of plankton in all the oceans of the world.
The « Plankton Chronicles » project was made to accompany the expedition. Initiated with CNRS Images (Véronique Kleiner, Catherine Balladur) the project continues today with Noé Sardet and Sharif Mirshak (Parafilms).
© 2016 Crónicas del Plancton – Todos los derechos reservados
Web por TONTON
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text:
OKC Media
According to these videos, Emily Sutton had fun at Single in the City
10:49 AM EST on February 25, 2013
That's a pic of local broadcasting legend (kidding) Brent Skarky talking to Emily Sutton at Saturday night's "Single in the City" auction. Why would Brent Skarky be allowed in the same room as Emily, much less granted time to have a conversation with her on a stage??? Well, the people at Oklahoma Magazine picked Brent to emcee the auction. That's right, they went with the Skarkster. Apparently their first choice, Driver from the Sports Animal, called in sick at the last second.
Anyway, I didn't make this year's auction, but an Ogle Mole in attendance provided me with some grainy, poorly lit videos of Emily on the auction block. I think you can say she had a good time. Here are the videos.
In the first clip, Emily talked about why she got into weather. She also told some storm chasing stories:
Emily decided to sing in the the second video. This isn't surprising. Emily does seems like the type of girl who will randomly burst into song at any moment.
The third clip was the best. Emily was being auctioned and decided to show off some of her favorite dance moves. She'd fit in great at a bachelor or bachelorette party:
Wow, Emily's even adorable when dancing like a drunk girl at a club. She could make the Elaine look charming and sweet.
Anyway, the real story in all of this is that Emily Sutton was auctioned for only $700 dollars. That's the steal of the century. Wouldn't it have been an awesome thing to split with five or six of your buddies?
"Hey, what are all you all doing tonight?"
"Going on a date with Emily Sutton!"
"Awesome. Where are you going?"
"Not sure, we're just going to try to get her drunk!"
Okay, so maybe it would have been awkward, but at least the money would have gone to a good cause.
KFOR,


Looking for a winter Wahoo? Visit our mobile unit on Route 100 in Dover.
Open Fridays 11-midnight, Saturday 12- Midnight, Sunday 12-8.
464-0110 to call ahead, or order online!
Tired of Lines? Go onLINE & Order.
Skip The Line-Grab & Go!


text:
Q: After installing Ubuntu I no longer have the option to start Windows 7 Professional I have just installed Ubuntu for the first time. I followed the steps for partitioning and root directories as recommended. However, when I partitioned the /dev/sda1 was green and the disk did not recognize Windows 7. After installation, the Ubuntu was orange. When I reboot I am not given a choice of operating system: instead it goes straight to Ubuntu. How do I change this so I can access Windows 7 again?

A: You can try using Boot-Repair: Boot-Repair instructions

A: Presuming that you installed Ubuntu 13.04, here is what you can try.  Boot from the Ubuntu 13.04 LiveCD.  Open Gparted by typing it in the Dash.  When it loads you should see all the partitions that are on the hard drive. Linux partitions will be EXT4 and the windows partitions will probably be NTFS.
Look at the list of partitions and see which one is the Linux partition, and look at the Mount Points of the partitions. You should see one with a / under Mount Point with a file system of EXT4, and look to see the name of it. In my case as per the images below of terminal, and Gparted its called /dev/sda1 (yours may be different).  Open Terminal, just press Ctrl+Alt+T on your keyboard to open Terminal. When it opens, run the command(s) below:
sudo mount /dev/sdXY /mnt

(Change the XY to match the name of your Linux partition).
sudo grub-install --root-directory=/mnt/ /dev/sdXY

Once done close terminal and any other open windows, and reboot.  Make sure that you remove the LiveCD.
Once rebooted, open Terminal and type:
sudo update-grub

When you it displays Done, reboot and you should be able to boot into windows again.

A: I presume you have deleted your windows 7 loader from your MBR, Boot repair should help solving the issue.
Try this post
http://ubuntuforums.org/showthread.php?p=10871917#post10871917

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This entry was posted on Thursday, March 29th, 2018 at 12:07 am	and is filed under Ben NanoNote, English, Fiasco.OC, Free Software, L4, MIPS, NanoNote, operating systems. You can follow any responses to this entry through the RSS 2.0 feed. Both comments and pings are currently closed.


@Joe. Thanks. I'll look forward to your order :) Most of what you need is online here.
That is fantastic! Congratulations on your milestone!
looking forward to it, are you guys going to make the source code downloadable ?
@Isaiah. Thanks. Yes, we're planning to have an associated web site.
Skimming the blog post (linked from Spring)...read the title of the post as "Book: The Worst Ever" as a comment by a user.... surely I am not the only one to make that mistake?
Haven't read the book to confirm nor deny...but may want to edit the title?


Everyone knows how important email is. You probably check yours several times a day for new updates.
messages posted since July 14, 2010 12:17 PM.
If you're in Winnipeg, I encourage you to come to our monthly meetup. It's a great little gathering of local creative/tech people.
Now, I signed up for email notifications because I'm just not going to check the site (which I never visit) every time I want to know if something new has been posted. In fact, the less I have to visit the site, the better.
The Winnipeg Film Group is proud to announce an open call to our second annual 90 SECOND QUICKIE film contest. The 90 Second Quickie was created in 2009 by the Winnipeg Film Group to encourage the creation of new, micro films. Blown away by the shorts in our first year we are doing it again – this time bigger, brighter and bolder!


This is a day of volunteering which is held in Mid and East Antrim in March.
Mid and East Antrim mayor Cllr Paul Reid said: "Be a Saint Day is an annual day of volunteering which encourages employers to release their employees for a day to get involved in practical tasks.
"Mid and East Antrim Borough Council has wholeheartedly supported the initiative for the last number of years.
"We have had a great number of hardworking volunteers out in our green spaces across the borough, and I would personally like to thank them for their time and effort.
Volunteers from Invest NI, Norbev, JP Corry, Belfast Harbour, P&O Ferries and Danske Bank all came out to help with practical tasks including essential tree maintenance at Diamond Jubilee Wood and Ecos Nature Park, and spring planting at The People's Park.


How far do you have to get from a big city before vacation mode sets in? If the city is Atlanta, and the destination is Lake Oconee, the answer would be 75 miles. The Ritz-Carlton Reynolds, Lake Oconee sits on 30 of the 374 miles of shoreline along this eastern Georgia lake, known for its golf courses and lakeside houses; the Ritz-Carlton is one of the few places to stay as a non-resident. Atlanta may be the closest big city, but it's a popular place for people all over the Southeast to visit — by car or quick flight into the Atlanta airport.
Where does the pool end and the lake begin? The endless view from the Ritz-Carlton's swimming pool seems to merge into Lake Oconee below.
Not large but definitely swanky, the Ritz-Carlton property includes a beach area along with the pool and other amenities.
Private porches off guest rooms offer a view of the lake and grounds.
The Ritz attracts a lot of families — with its man-made sandy beach and myriad activities for all ages — but we think it's an ideal place to grab a girlfriend or two and relax … there's enough to do, but not too much to do, so you'll have plenty of time for visiting.
Suggested itinerary: Make a stop on the way there in charming Madison, a small town about a half-hour away from Lake Oconee. Stroll the historic town square and make sure to browse Madison Markets, a renovated cotton warehouse full of antiques, art, plant creations and other finds. There are quaint places to eat lunch, such as Town 220 or Madison Produce Company.
Specialty cocktails at Georgia's include fruits from local farms and herbs from the on-site garden.
The fried-green tomato appetizer includes poached lobster and fresh herbs as a garnish.
Dining al fresco at Georgia's is a year-round event, thanks to the area's mild winters.
The centrally located fire pit is a place to relax at night with s'mores or an adult beverage.
Check in or stash your bags at the Ritz and start enjoying the peaceful setting at the pool (heated year-round), a scenic infinity pool that seems to blend in with the lake beyond. Waiters regularly make the rounds to serve you, and sometimes they may stop by with a smoothie or other complimentary treat. The nearby beach area is good for dipping your toes in the lake, but more adventurous souls can take a YOLO board, kayak or canoe out as part of the resort fee, or rent something faster like jet skis.
A Starbucks on the property is a convenient place for an easy breakfast or afternoon pick-me-up, but don't get too full, since the restaurants have a lot of temptations on the menu. Georgia's specializes in regional cuisine, with specials that incorporate items from local farms. The view is swanky, too … overlooking the grounds and lake. Save room for a s'more, since the Ritz is well-known for its nightly campfire and a well-stocked s'more bar.
The lodge-like décor of the Ritz-Carlton's lobby includes a vaulted ceiling and ample seating.
Walking trails along Lake Oconee often meander along golf courses.
Carefully maintained gardens and pots are a hallmark of this resort.
Gaby's by the Lake is a casual destination for lunch or dinner.
After a good night's sleep, get a tee time for golf or go hiking along one of the lakeside trails as a morning activity. Afternoon might be good for a spa treatment at the on-site spa — a bit of a splurge (facials start at $155), but they — and you — are worth it. Arrive at the spa early to enjoy the quiet lounge or to take a soak in the whirlpool.
Make sure to have lunch or brunch at Gaby's by the Lake, the resort's casual restaurant overlooking the pool and lake. Feeling like you want to imbibe? The restaurant's Georgia John mixes Firefly tea vodka, peach liquor and lemonade.
Large groups can rent a cottage at Lake Oconee or through the Ritz-Carlton.
Nearby town Madison, Georgia is known for its antebellum mansions and shopping, such as the sprawling antiques mall, Madison Markets.
Lunch spots in Madison often have brick walls and decorative ceilings as an architectural clue to their historic past.
Rooms include signature robes, Frette linens and porches to enjoy a good book, so nobody will judge if you want to just relax in the room. Check the website for current promotions; the resort's "Reconnect" package starts at $429 per night and includes breakfast and $75 resort credit.
For more ideas for you next adventure, check out the SB Travel suggestions!


Think getting a loan for an investment property will be as easy as your home mortgage? Think again.
Lenders are far more strict in their underwriting of investment properties and require more money down. Why? Simple: Borrowers will always default on their investment property loan before they default on their home mortgage.
With higher risk comes higher pricing, lower LTVs (loan-to-value ratios), and generally more runaround.
Here's what new real estate investors need to know about how investment loans differ from homeowner mortgages.
Plan on having to put down at least 20% of the purchase price if you're buying an investment property.
There are exceptions, of course (most notably for house hacking, which we'll delve into later on). By and large, however, plan on putting down 20-40% of the purchase price.
The good news is that you won't have to worry about mortgage insurance—but that's really the only good news.
Some conventional loan programs for investment properties allow for 80% LTV, although you should know going in that it's a best-case scenario. You can also explore real estate crowdfunding websites, which tend to be more expensive than conventional loans, but may be more flexible.
Depending on the lender and loan program, you might also find that pricing goes down alongside LTV. In other words, if you're willing to put down more money, you may secure a lower interest rate and lower fees.
As a final note, plan on needing at least three months' payments as a liquid cash reserve.
It will be higher. The end.
Alright, there's a little more to know. Plan on both the interest rate being higher and the upfront lender fees being higher.
On paper, conventional lenders often quote that their investment property loans are only 0.25-0.5% more expensive than their homeowner loans. In my experience, it never turns out that way. Expect to add 1-3 percentage points more than an owner-occupied loan rate. That means that if a lender charges 4% interest for homeowner loans, you'll likely pay 5-7% interest for investment loans.
And don't forget points. Lenders charge up-front fees for mortgage loans, and one "point" is equal to one percent of the total loan amount. These obviously add up quickly.
It just gets more expensive from there, as you get away from conventional lenders and toward community banks or crowdfunding websites.
Credit matters, of course, although not as decisively as in homeowner lending.
If your credit score isn't perfect, you'll still have options; they'll just cost you more. A score below 740 will spell higher interest rates, higher lender fees, and lower LTVs. The lower your credit score, the more you can expect to cough up at the table and in ongoing payments.
For borrowers with mediocre credit, conventional loans may not be an option.
Still, investment property financing is often based more on the collateral (the property) than you as a borrower. Remember, lenders know that investors are far more likely to default than homeowners, so they've already built some extra caution into the loan programs in the form of lower LTVs.
Your options start dwindling, the more mortgages you have on your credit report.
Once you have four mortgages on your credit, many conventional lenders won't touch you anymore. There is a program, however, introduced by Fannie Mae in 2009 to help spur investment that allows 5-10 mortgages to be on a borrower's credit.
The program requires six months' payments held as a liquid reserve at the time of settlement. It requires at least 25% down for single-family homes and 30% down for 2-4 unit properties. But with any late mortgage payments within the last year or any bankruptcies or foreclosures on your record, you're persona non-grata.
There's also a hard limit of a 720+ credit score for borrowers who already have six or more mortgages.
Own More Than 10 Properties?
Small community banks are an option because many keep their loans within their own portfolio. These are a good starting place for investors.
Commercial lenders sometimes lend "blanket" loans, secured against multiple properties. But if you go this route, be sure to ask what happens if you want to sell only one of the properties in the blanket or umbrella loan.
Seller financing is always an option if you can convince the seller to take on the headache (and risk). However, most sellers aren't interested in becoming your bank.
Hard money lenders are great for flips but usually terrible for long-term rentals. They're simply too expensive.
Look into crowdfunding websites—new ones pop up all the time and are often unafraid of lending to investors with multiple properties.
And, of course, you can great creative. Perhaps you can get a HELOC on your primary residence? Or maybe your friends and family want to invest money toward your next rental?
If all this borrowing talk is starting to get tedious, why not skip investment loans altogether?
You can borrow an owner-occupied mortgage for buildings with up to four units, with cheap interest rates and low (3-5%) down payments. You can even use FHA or VA financing to do it!
The idea is you move into one of the units, with your rents from neighboring units enough to cover your mortgage. In other words, you live for free. Pretty sweet deal, eh?
After living there for a year, you can go out and do it all over again, with another four-unit building!
You also score some great hands-on experience managing rental units. If you're looking for a little inspiration, read this case study of how one newbie house hacked a duplex.
No matter your real estate investing niche, more cash gives you more options. That means stockpiling cash should become a priority for you.
The less income that you can live on, the better. Some investors even live on half their income and save and invest the rest!
Between down payments, closing costs, cash reserves, renovation budgets and more, investors always need cash and lots of it. As you buy rental properties, set aside all the profits toward your next property.
Through house hacking, you can get away with buying your first property or two with minimum cash. But that will quickly change, so make cash planning a part of your real estate investing strategy.
Here's a prefab plan for how to make the most of your initial savings, and remember to secure your financing before you actually need it for a deal!
Have any questions or concerns about financing your first few deals? What about financing deals after conventional lenders won't touch you anymore?
Fire away. The BiggerPockets community has your back!
I did have one question though. In the section on house hacking a small multi family, you recommend getting an owner-occupied mortgage for the first property, but only living there for a year, and then doing the same with the second property. Doesn't this violate some clause in the mortgage when it is no longer owner occupied? If it does violate the mortgage, the bank could foreclose on you, right? In reality, they probably wouldn't care, as long as you keep making payments on time, but, if interest rates go up significantly, they might be motivated to to get rid of lower interest rate mortgages so they could loan the money out at higher rates. Or, is it perfectly OK with the banks, FannieMae for example, if you no longer owner occupy a property that was financed as owner-occupied?
The loan paperwork includes an "intent to occupy" clause, in which you are signing that you intend to occupy the property as your primary residence. But that doesn't mean you need to occupy it forever. One year is considered the rule of thumb, for the minimum time required to meet that intent to occupy.
It may be worth noting that while you can get a second conventional loan, after moving out, usually you can't get a new FHA loan unless you've paid off the prior FHA loan.
Can I convert my original FHA loan to a conventional loan, then take out a new FHA loan on another property after I have occupied for 1 year?
In essence, is there anyway I can take hold of 3.5% more than once?
@JORDAN COUGHENOUR, absolutely! It's not a one and done deal.
Wow! That's taking candy from a baby! So that's usually the process? Converting my loan to conventional, and then moving out of that property into a new 1 year owner occupied property at 3.5% down again? How many times can you do this?
Yes, you can refinance your FHA to conventional, then get another FHA loan on a new property with up to 4 units.
As mentioned in the article, once you reach 3-4 mortgages on your credit report it becomes much harder to get another conventional loan however. But there are other options available.
Hello Cindy and Brian. I was wondering about this too. I was able to get owner occupied conventional financing on 2 properties (four years apart) but it wasn't easy. I'm trying for a third right now but have been told it'll be nearly impossible. Underwriters want extensive detail on why I'm applying for an owner occupied loan every 1-4 years. I read columns on BP all the time advising people to house hack every year for lower financing but talking from experience, it's not as cut and dry. Do these regulations vary based on state? If anyone out there is able to get owner occupied loans every year, I'd love some advice!
It can definitely be tricky. Keep in mind the article is about what's allowed generally for conventional loans, but as you said, in practice it can be tricky. Lenders have the option to turn down your loan even if it meets their guidelines.
Still, you should be able to find a conventional lender who will lend on a third property if you're legitimately moving into it. They may request a higher down payment, or they may be willing to cross-collateralize your existing home(s).
Excellent article! Great tip about coming in with three months payments reserved in the bank. This would definitely be helpful if it takes longer than anticipated to find renters for the property. Nothing is better than making sure you are protected should any unexpected expenses arise!
Thanks Robert! I agree, that's actually one of the most common mistakes new landlords make – being undercapitalized and then surprised when expenses pop up.
Brian, good advice. Started 15 years ago buying a home for our college daughter as a second home. Later we sold it to her and her new husband and 1031 into 3 single family homes all in a row. 2 on 1 and a single. Was great until last administration war on oil and gas and coal which Farmington NM is dependent on. One house has been vacant for 6 months another For 8. Tried selling but nothing for 4 months so I'm back making more improvements hoping to better value as well as attract renters. Had been in remodeling business for 38 years but now retired and lack of Rental income is hurting. We saved enough buy another investment in Durango where we live and rent that 1 bed for what we can't get for 1800sf house. Am trying to just gut it out but life is stressful to say the least. Do you have any magical advise?
Hi Tony, I'm sorry to hear that about your properties in New Mexico. That's a terrible feeling.
Local realtors may be able to give you some tips on what exactly it will take to sell (price, improvements, marketing gimmicks, whatever).
You could always try leasing gimmicks, such as offering a month's free rent. The free month could be the 12th month of the lease, and contingent on the renters paying the first 11 months' rent on time.
But there's no easy answer, when there simply isn't much demand for housing in an area. I'm sorry again to hear it. There's always the chance that the current administration's pro-fossil fuels stance will revitalize jobs in that town, but you have no control over that of course.
Thanks Brian. Did the realtor thing already and they don't know what else to suggest. My current direction is to do what I know which is improving the properties and wait it out. If and when we decide to sell at least I've added value. (One would think). When all is rented we do have a great cash flow which for retirees that is the key.
Great information in this post Brian! One thing I would add is to contact several lenders and shop around for lower rates, lower loan origination fees, or lower down payment requirements depending on your situation calls for. A good lender can be a great asset to your team.
Very good advice Walker! Always worth shopping around. Lender pricing and programs can vary quite a bit.
What about a person who is a professional with a career and a good income, buys a primary residence with a conventional loan, moves in, then moves into an apartment and rents the place out? If they keep repeating the process can they have more favorable financing options?
Hi Kris, that will work the first couple times probably, but as you get a few mortgages on your credit it becomes harder and harder to be approved for conventional financing. As mentioned in the article, at a certain point you have to start looking elsewhere for funding. But you can definitely get started in real estate investing using conventional loans.
Thank you for your article. Good points.
I have a question on non-recourse loans for investment property purchase. I assume the lending bank will always want collateral, thus they would have the tittle of the property in their name. Is there a certain down payment amount or range for which the bank would be ok with the purchased property being collateral versus having to acquire by using a personal guarantee?
To answer your question, I've never known a bank to not require a personal guarantee.
Lima One appears to do non-recourse loans. Of course, the rates are high. I'm considering it as a way to mitigate risk. They will do a 30 year loan as low as $50k.
Thanks Brad, and you're absolutely right, investors should have both good financing set up and sufficient cash BEFORE they make an offer. Otherwise investors are setting themselves up for a mad scramble to put together funds for settlement.
TY Brian another great overview! Always appreciate your insight.
One option is to sign a lease-option agreement with responsible renters who want to buy their first home. It wouldn't solve your immediate cash needs, but you could come to some arrangement with them regarding repairs, where they are partially (or perhaps even fully) responsible for repair costs.
Great breakdown of the different options out there, thank you for sharing Brian! As a newbie who's still researching the best option for getting started, this was really helpful!
Glad to hear it was helpful Sara! Please don't hesitate to PM me any time with questions, I'm extremely responsive.
Super helpful! Thanks a bunch Brian. I'm currently in the education phase of investing. My wife and I have only just recently even been considering investments as a means of passive income. We haven't yet taken the plunge on our first property, so I'm doing as much research as my brain can handle to quell the (normal, I'm sure) fear in taking the first steps.
I gather that eventually we're just going to have to jump, maybe land flat on our face, but get up and go for the next one.
Glad to hear it was helpful Logan! And while it's a bit scary to buy any asset that valuable, the nice thing about rentals is it's easy to forecast their returns.
Don't hesitate to reach out if I can help in any way!
Great article Brian, especially for newbies like me 🙂 Thank you!


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