text:
\section{Introduction}

Extremely metal-poor (EMP) stars are the shining witnesses of a primordial
Universe
corresponding to a redshift  higher than 10.
They belong to the second generation of stars, objects formed from the gas
enriched
only by the first generation of the stars, Pop\,III stars.
Direct observation at high redshift of the individual
massive Pop\,III stars is not feasible because they are too
faint for the current and next generation of telescopes.
There is one possible exception.
In the case of Pop\,III stars formed with masses of a few  hundred M$_\odot$
\citep{hirano14},
they could have ended their life with a pair-instability supernovae (PISN)
event.
According to \citet{bromm14}, this kind of event could be visible for the
James Webb Space Telescope (JWST) planned to be launched in 2019.
However, even in this event it is unlikely that the low-resolution spectra
that could be obtained from JWST would be able to provide a detailed chemical
inventory of PISN ejecta.
At the moment, EMP stars are  the only way to deduce the characteristics
of the Universe at the time they formed.
The TOPoS project \citep{topos1} has been designed to increase the number
and
chemical inventory of EMP turn-off stars. The TOPoS targets were selected
from the stars observed spectroscopically in the SDSS/SEGUE/BOSS survey
with the following colour cuts: $0.18 \le (g-z)_0 \le 0.70$ and $(u-g)_0
> 0.70$.
This allows the identification of  stars likely to be close to the main sequence
turn-off of halo stars.

\section{Observations and data reduction}

Target stars were observed using the ESO Ultraviolet and Visual Echelle Spectrograph
\citep[UVES,][]{dekker00} mounted at the Kueyen 8.2m telescope, the second
unit telescope
of the Very Large Telescope (VLT, Cerro Paranal, Chile). Observations of
five stars were collected in service
mode in the course of Large Programme 189.D-0165 (PI E. Caffau)
between April 2013 and March 2016. We adopted setting   Dic\,1 390+580  and
 therefore observed simultaneously with the blue and red UVES arms, centred
at 390\,nm and 580\,nm, and covering the spectral ranges 326-454\,nm and
476-684\,nm, respectively. The data were binned $2\times 2$ (spectral $\times$
spatial direction),
and a  1.4$^{\prime\prime}$ slit width was adopted. This resulted in a
resolving power of R$\simeq$30000 or larger when the image quality was better
than
1.4$^{\prime\prime}$. A different number of 3005\,s frames were taken for
six of the
target stars, namely 1, 5, 11, 5, 3, and 6 for stars SDSS\,J0140+2344,
SDSS\,J1034+0701, SDSS\,J1035+0641, SDSS\,J1247--0341,
SDSS\,J1442--0015, and SDSS\,J1507+0051, respectively. The
signal-to-noise ratios per pixel of individual  spectra  varied in the range
3-30 for the blue arm and  8-61 for
the red arm.

\begin{figure*}
\begin{center}
\resizebox{\hsize}{!}{\includegraphics[draft = false, clip=true]
{plot_cak.eps}}
\end{center}
\caption[]{Spectral ranges of the \ion{Ca}{ii}-H and -K lines  of the sample
stars.
}
\label{plot_HK}
\end{figure*}

\begin{figure*}
\begin{center}
\resizebox{\hsize}{!}{\includegraphics[draft = false, clip=true]
{cfe-topos4.ps}}
\end{center}
\caption[]{ Carbon abundances of the programme stars (filled red circles)

as a function of [Fe/H]. Other stars
published by our group are shown as open red circles.
Other stars from the literature
\citep{sivarani,Plez05,PCM05,frebel05,frebel06,thompson08,aoki08,behara,masseron10,masseron12,yong2013,Cohen13,Li2015}
are shown as blue squares.
The violet star is the upper limit on  SDSS\,J1029+1729 \citep{leostar,leostaraa}.
The horizontal dotted lines delimit the low-carbon band.
}
\label{plot_c}
\end{figure*}

\begin{table}
        \caption{ SDSS DR12 $^1$ photometry and exposure times for the programme
stars.}
\label{data}
\begin{center}
\renewcommand{\tabcolsep}{1pt}
\begin{tabular}{lccccccccr}
\hline \noalign{\smallskip}
 Star                   & $u$      & $g$      & $r$      & $i$     & $z$
     & T$_{exp}$ & N$_{\rm exp}$\\
                        &           &           &           &           &
          & s             & \\

\hline \noalign{\smallskip}

SDSS\,J014036.22+234458.0  & 16.78 & 15.82 & 15.35 & 15.12 & 15.03 & 3005
& 1 \\
SDSS\,J103402.71+070116.6  & 18.34 & 17.52 & 17.23 & 17.13 & 17.12 & 3005
& 5 \\
SDSS\,J103556.11+064143.9  & 19.53 & 18.65 & 18.37 & 18.31 & 18.26 & 3005
& 29 \\
SDSS\,J124719.46--034152.4 & 19.32 & 18.50 & 18.24 & 18.15 & 18.14 & 3005
& 5 \\
SDSS\,J134922.91+140736.9  & 17.44 & 16.65 & 16.33 & 16.24 & 16.19 & 3600
& 9  \\
SDSS\,J144256.37--001542.8 & 18.76 & 17.96 & 17.65 & 17.51 & 17.49 & 3005
& 3 \\
SDSS\,J150702.02+005152.6  & 19.75 & 18.77 & 18.57 & 18.48 & 18.41 & 3005
& 6 \\
\noalign{\smallskip}
\hline
\end{tabular}
$^1$In this work we used the SDSS DR12 photometry; the magnitudes of the

        latest release DR14, differ from these values by less that 0.015
mag.
\end{center}
\end{table}

Star SDSS\,J1035+0641 was also observed with setting Dic\,2 437+760
(programme ID: 096.D-0468 PI Sbordone), with the blue and red arms covering
the spectral ranges
373-499\,nm and 565-946\,nm, respectively. A total of 18\,$\times$3005\,sec
frames were acquired. The same slit width (1\farcs{4}) and on-chip
binning ($2\times 2$) were chosen. Signal-to-noise ratios per pixel of individual
spectra  varied in
the range 5-10 and 4-8 for the blue and red arms, respectively.

SDSS\,J1349+1407  was observed in service mode in the course
of programmes 090.D-0306 and 093.D-0136 (PI Sbordone) between March 2013
and
June 2014. The setting used in this case was  Dic2 437+760 with
a $1\times 1$ binning and a 1\farcs{0} slit, providing a resolving power
of R$\sim 48000$. A total of nine integrations
of 3600s each were acquired. The coadded spectrum attains a S/N $\sim 40$
per pixel at 400\,nm
and a S/N $\sim 60$ per pixel at 590\,nm.

The data were reduced by the ESO staff, and retrieved through the Phase\,3
spectral
data products query
form\footnote{\url{http://archive.eso.org/wdb/wdb/adp/phase3_spectral/form}}.

\section{Analysis}

The chemical analysis has been done with the code MyGIsFOS\ \citep{mygisfos}.
This code derives the chemical abundances by fitting a selected set of features.
The best fit profile is obtained by interpolating in a series of pre-calculated
synthetic spectra.
These synthetic spectra have been computed with {\tt turbospectrum} \citep{alvarez_plez,2012ascl.soft05004P}
and are based on a grid of 1D plane-parallel hydrostatic model atmospheres
previously computed with MARCS \citep{G2008}.
The procedure to derive the  atmospheric parameters and chemical composition
is described by \citet{topos1} and has
also been  used in the other papers of this series \citep{topos2,topos3}.
There were  two exceptions for which MyGIsFOS\ was not well adapted:    carbon
in all stars, and magnesium
in the star SDSS\,J1349+1407. Carbon  was derived by $\chi$-squared fitting
of the
G-band with a specifically computed grid of synthetic spectra with fixed
metallicity, $T\rm_{eff}$,\ and \ensuremath{\log g}\
and with varying C abundance. This technique is the same as that
used in our previous papers \citep{spite13,topos2}.
To take into account the known
granulation effects on the G-band \citep{Collet2007,behara,Gallagher2016,Gallagher2017},
we used the corrections provided by \citet{Gallagher2016}, assuming a metallicity
of --3.0.
The stellar parameters and abundances of C and Li are provided in Table\,\ref{param}.

Because
its [Mg/Fe] ratio is so extreme (Mg enhanced by more than 1\,dex over Fe),
one concern for  SDSS\,J1349+1407 was that its temperature
structure could be different
from
that of a normal solar-scaled and $\alpha$-enhanced model.
Magnesium
is one of the
main electron donors for solar-type stars, and its abundance may affect the
ionisation
structure of the atmosphere.
We verified that the high [Mg/H] does not affect the abundances derived with
models enhanced in Mg by
the canonical 0.4\,dex
by computing both the ATLAS\,9 and ATLAS\,12 models \citep{kurucz93,kurucz05,SBC04,sbordone05},
the latter with [Mg/Fe]=+1.4 to
derive
the abundances.
From this test we conclude that
the differences are negligible;  the largest difference reaches 0.05\,dex
for Mn.
At the very low metallicities relevant for the stars
analysed in this paper, Mg, Ca, and any metals cease to be important electron
donors;
as already discussed by \citet{nc04},
the main electron donor is, in fact, hydrogen.

\subsection{Individual stars and comparison with previous  analyses}

All  of our targets have already been analysed by our group
on the basis of X-Shooter spectra, and some have also been analysed  by other
groups.

\begin{itemize}
\item SDSS\,J0140+2344.
The stellar parameters and [Fe/H] we derive are in excellent agreement with
those determined
by \citet{topos1} from the analysis of an X-Shooter spectrum.
Our estimated upper limit of A(C) from the X-Shooter spectrum was too optimistic:
the carbon abundance we derive in this work is 0.3\,dex larger than the X-Shooter
upper limit.

The Mg and Si abundances
measured from the X-Shooter and UVES spectra are in excellent agreement.

The Ca abundance measurements are more problematic.
We detect two \ion{Ca}{i} lines, the resonance line at 422.67\,nm and the
subordinate line
at 442.54\,nm. The two lines are very discrepant, as is generally the case
in EMP stars, even when NLTE effects are taken into
account \citep[see][and references therein]{spite12}.
The  422.67\,nm resonance line provides $[{\rm Ca/H}]=-3.97$, in good agreement
with the X-Shooter
spectrum where  the only \ion{Ca}{i} line detected was in fact the 422.67\,nm
line,
                which implied $[{\rm Ca/H}]=-3.78$.
The subordinate line yields a Ca abundance that is over 1\,dex higher
($[{\rm Ca/H}])=-2.79$). In Table\,\ref{abbo2} we only provide  the value
from the subordinate line,
which, as discussed by \citet{spite12}, is more reliable.
The \ion{Ca}{ii} is derived from the K-line alone and it is a factor of three
lower  than
the value we had estimated from the X-Shooter spectrum; however, in that
case we relied only on the \ion{Ca}{ii} infrared triplet lines. The  abundance

from the K-line is also  strongly discrepant from
the \ion{Ca}{i} subordinate line.
\citet{yong2013} analysed a  Keck/HIRES spectrum of this star. They derived
$T\rm_{eff}$ = ${5703}$\,K from a combination  of spectrophotometry and
Balmer line analysis. This is in agreement, within the errors, with our
adopted $T\rm_{eff}$. The surface gravity was derived from isochrones and two
solutions were found, depending on whether the star is a main sequence
or a subgiant  star, this corresponds to \ensuremath{\log g} = ${3.36}$
or \ensuremath{\log g} = 4.68. In the two cases, they derive [Fe/H]=$-4.11$ or
[Fe/H]=$-4.02$ (with our adopted solar Fe abundance \citealt{abbosun}),
in excellent agreement with our result.
For Ca, they only measure the \ion{Ca}{i} 422.67\,nm resonance line
and derive [Ca/H]=$-3.82$ or [Ca/H]=$-3.88$, again in excellent
agreement with our results for the same line.

\citet{aoki13} analysed  a Subaru spectrum of this star
and used  $T\rm_{eff}$ = ${6103}$\,K, which  was derived from the SDSS low-resolution
spectrum by the SEGUE Stellar Parameter Pipeline \citep[SSPP,][]{SSPP},
even though both $V-K$ and $g-r$ imply a temperature close to
that used by us. For the surface gravity they assumed
\ensuremath{\log g} = 4.0 and, like us, they derived [Fe/H]=$-3.67$ (on our adopted
solar abundance scale).  Considering their adopted higher effective
temperature, this metallicity is consistent  both with ours and with that
of \citet{yong2013}. For Ca they derive [Ca/H]=$-3.82$ from a single line.
Although it is not explicitly stated, it is highly probable that this
refers to the   \ion{Ca}{i} 422.67\,nm resonance line.

Finally, \citet{aguado16} analysed the SDSS spectrum and a  ISIS WHT spectrum
and derived
the stellar parameters ${6090\pm 200}$\,K/${4.7\pm 0.3}$/$-3.6\pm 0.2$.
Unsurprisingly, the $T\rm_{eff}$\ is close to the SSPP value and the derived metallicity
is consistent.

We conclude that the different analyses of this star are all consistent,
but we point
out the discrepancy of the Ca abundance derived from different lines. This
will have
to be revisited in the light of 3D NLTE computations in the future.

\smallskip
\item SDSS\,J1034+0701.
The  X-Shoooter spectrum is analysed in \citet{pfr17}.
The [Fe/H] from the UVES spectrum is about 0.4\, dex lower than the value
derived from the X-Shooter spectrum.
The Mg abundance is in  agreement within errors.
We did not derive the Ca abundance from the UVES spectrum, but the Ca abundance
from the X-Shooter spectrum, based on the \ion{Ca}{ii}  IR triplet, and the
X-Shooter based Fe abundance implies [Ca/Fe]=+0.33.

\smallskip
\item SDSS\,J1035+0641.
\citet{topos2} investigated an X-Shooter spectrum, but they could only derive
A(C) and an upper limit for the Fe abundance.
The A(C) derived from the UVES spectrum
is a factor of two higher than the value we derived from the X-Shooter spectrum,
which illustrates
the limit of measuring the G-band for a warm star like this at moderate resolution.
The non-detection of the 382.0425\,nm line  (equivalent width $< 0.4$ pm
at $1 \sigma$)
provides an upper limit of the Fe abundance [Fe/H]$< -5.2$, tighter than
the value
we derived from the X-Shooter spectrum.
A fit to the \ion{Ca}{ii} K line
provides an abundance that is consistent with that derived from the X-Shooter
spectrum.

We found a mistake in Table 7 of \citet{topos2} and in their Figure 10.
The upper limit on lithium, corresponding to an upper limit of 1.8\,pm,
is A(Li)$< 2.05$ and not 1.1, as incorrectly listed in Table 7. Our measured
equivalent
width of 1.3\,pm is consistent with that upper limit and corresponds to A(Li)=1.90.

\smallskip
\item  SDSS\,J1247--0341.
The metallicity determined by \citet{topos1} from the X-Shooter spectrum
is in good agreement with that derived from the UVES spectrum.
Also in this case the C abundance derived from
the UVES spectrum is larger by 0.6\,dex than the value we estimated
from the X-Shooter spectrum. The Mg abundances from X-Shooter and UVES spectra
are consistent
within 1$\sigma$. \citet{topos1} provided the Ca abundance from
two lines of the \ion{Ca}{ii} IR triplet, which we considered more reliable
than the \ion{Ca}{i} 422.67\,nm resonance line. That line implied [Ca/H]=$-3.96$,
which is consistent with the abundance provided here for the same line.
Also in this case we point out how different lines provide different abundances
for Ca; this is likely due to the inadequacy of the 1D LTE analysis of this
element
in these extremely metal-poor stars.
The Gaia data release 1 \citep{GaiaDR1} shows that this star
has a close-by companion at a distance of 0\farcs{01} and 0.5 mag
fainter in $G$. Certainly the light of this companion contaminates our
spectrum, but since we do not have any colour information at this time we
did not
attempt to correct our spectrum for the veiling.
We do not detect any sign of the spectrum of the companion star in our spectrum.

\smallskip
\item SDSS\,J1349+1407. \citet{sbordone12} announced it  as a Mg-rich star.
The quality of the spectrum available at that time was sufficient only for
giving abundances of a few elements.
The star was independently recovered as a Mg-rich star by
\citet{li14}, who analysed the SDSS\,DR9 spectra.
Their temperature for the star is higher by 230\,K and consequently their
metallicity is higher ([Fe/H]=--2.83).
In the UVES spectrum of SDSS\,J1349+1407
we identified six \ion{Mg}{i} lines in the blue spectrum (382.9, 383.2, 383.8,
405.7, 416.7, 470.2\,nm).
We fitted the line profiles and
we derived ${\rm A(Mg)}=5.30\pm 0.16$ and by removing the line  which is
in the wing of a Balmer line,
we derive ${\rm A(Mg)}=5.36\pm 0.11$.
The star is also enhanced in Na, with [Na/Fe]=+0.86.

\smallskip
\item SDSS\,J1442--0015.
We compared our spectrum with the X-Shooter spectrum of \citet{gto12}.
The metallicities from the analysis of the two spectra
are in good agreement within errors of less than $1 \sigma $. The Mg abundances
are in reasonable agreement with $1.5 \sigma$ errors.
The situation is slightly worse for the Ca abundance; the
abundances derived from the \ion{Ca}{i}
422.67\,nm resonance line from the two spectra are consistent to within
$1.8 \sigma$, i.e. 0.7\,dex. As usual, this is discrepant with the \ion{Ca}{ii}
IR
triplet lines, measured in the X-Shooter spectrum.
This example is a recommendation  not to  overinterpret the abundances
that rely on a single, weak line.

It is important to note that both here and in the study of \citet{gto12}

we adopted the effective temperature derived by fitting the wings of H$\alpha$,
which
is considerably lower than  the temperature implied by the $g-z$ colour (6161\,
K).

\smallskip
\item SDSS\,J1507+0051. The X-Shooter spectrum  was analysed by \citet{topos1}.
Both the metallicity and the Mg abundance of the  two analyses
are in agreement within less than $1 \sigma$. Instead, we have a strong discrepancy

for the abundances of Ca derived from \ion{Ca}{ii} lines.
In the UVES spectrum we detect the 370.6024\,nm line, while in the X-Shooter
spectrum, we relied on the IR triplet lines. This discrepancy needs to be
further investigated.
\end{itemize}

\begin{figure}
\begin{center}
\resizebox{\hsize}{!}{\includegraphics[draft = false, clip=true]
{pl_li_feh.eps}}
\end{center}
\caption[]{Lithium abundance in unevolved extremely metal-poor stars.
The different symbols refer to different carbon abundances.
The filled hexagons refer to carbon normal stars.
CEMP stars of the low- and high-carbon bands are shown as star symbols and
crossed squares, respectively.
Measurements and upper limits of the programme stars are shown in red.
Measurements and upper limits from our group's previous papers \citep{topos2,topos3}
are shown in blue.
Black symbols  are stars for which metallicity, lithium abundance,
and carbon abundance are taken from the literature
\citep{norris97,Lucatello03,
sivarani04,Ivans05,sivarani,frebel07,frebel08,thompson08,aoki08,
sbordone10,behara,leostaraa,
Carollo12,masseron12,aoki13,
Ito13,Carollo13,spite13,Roederer14,Aoki15,sdss_uves,Li2015,terese,topos3,
Placco16,Matsuno17}.
The two components of the binary system CS 22876-32 \citep{jonay08} are shown
as black crosses.
The green dashed line is the level of the {\em} Spite plateau
as determined by \citet{sbordone10}.
\label{plot_Li}
}
\end{figure}

\begin{figure}
\begin{center}
\resizebox{\hsize}{!}{\includegraphics[draft = false, clip=true]
{pl_teff_li.eps}}
\end{center}
\caption[]{ Lithium abundance in the unevolved extremely metal-poor stars
as a function of effective temperature. The meaning of the symbols
is the same as in Fig.\,\ref{plot_Li}. The high-carbon band CEMP stars have
not been included in this plot.
\label{plot_Li_teff}
}
\end{figure}

\begin{figure}
\begin{center}
\resizebox{\hsize}{!}{\includegraphics[draft = false, clip=true]
{plot_lim4.eps}}
\end{center}
\caption[]{ Lithium doublet in SDSS\,J1034+0701 (squares) and
SDSS\,J1247--0341 (triangles) compared to a 3D NLTE theoretical profile
($T\rm_{eff}$ = 6270\,K \ensuremath{\log g} = 4.0 [M/H]=--3.0, A(Li)=2.1). The observed spectra
have been smoothed with a Gaussian of
4 $\mathrm{km\, s^{-1}}$\ FWHM to increase the S/N.
\label{plot_lim4}
}
\end{figure}

\section{Results and discussion}

The main result of this investigation is the confirmation, based on
higher resolution spectra, of the very low metallicities that we derived
for these stars from the analysis of the X-Shooter spectra. Two stars have
[Fe/H] below $-4.3$,
three stars around $-4.0$, and two stars around $-3.5$. These numbers confirm
the high efficiency of the TOPoS strategy for target selection.
The five stars with [Fe/H]$\le -4.0$ discussed in this paper,
SDSS\,J1742+2531 ( [Fe/H]=$-4.80$, \citealt{topos2} ) and
SDSS\,J0929+0238 ([Fe/H]=$-4.97$, \citealt{topos3})
are the most iron-poor stars we found in the course of the TOPoS project
and they are all strongly C-enhanced. To date, among the stars with
[Fe/H]$\le -4.5$ the only `non C-enhanced star' found is  SDSS\,J1029+1729
\citep{leostar,leostaraa}.

\subsection{Carbon abundances}
It is interesting to note that all the C-enhanced stars that we have found
belong
indeed to the low-carbon band discussed by \citet{topos2}, as illustrated
in Fig.\,\ref{plot_c}.
These stars do not seem to be enhanced in $s$-process elements and we suggest
that they are indeed
CEMP-no stars.  This view is supported also by the
recent study of \citet{Hansen16} who analysed a sample of 27 metal-poor stars
and found that 20 of them
are CEMP,
3 of which are CEMP-no
stars  that  belong to the low-carbon
band.
We  suggest here that a useful classification of metal-poor stars
can be made using only their C abundance without any reference
to their abundance of n-capture elements.
This is related to the fact that, for unevolved stars, it is very difficult
to secure data quality high enough
to derive measurements or significant upper limits for the heavy elements.
Our proposed classification scheme is as follows:
\begin{itemize}
\item `carbon normal': for [Fe/H]$\ge -4$ [C/Fe]$< 1.0$,
for  [Fe/H]$< -4$ A(C)$<5.5$;
\item low-carbon band CEMP stars: stars that do not fulfil the carbon normal
criterion and have A(C)$\le 7.6$;
\item high-carbon band CEMP stars: stars that do not fulfil the carbon normal
criterion and have  A(C)$ > 7.6$.
\end{itemize}

This classification is qualitatively similar to that proposed by \citet{Yoon},
except that their Group II is partly included in our
low-carbon band and mostly in our carbon normal  stars, their
Group I is by and large coincident to our high-carbon band, except for the
stars with the lowest C abundances in their Group I, which we assign to the
low-carbon
band.

In \citet{topos2} we also used the working hypothesis that all the stars
on the high-carbon band
are binaries and the high carbon abundance is the consequence of mass-transfer
from a companion
during its AGB phase. This hypothesis, however, does not place any lower
limit to the [Fe/H]
of the high-carbon band stars. The fact that, observationally, we do not
find
any high-carbon band stars below [Fe/H]=--3.6 is intriguing. In Fig.\,\ref{plot_c}
we have 26 stars with a metallicity below --3.6, of which 25 are C-enhanced,
and none is a high-carbon
band star. It therefore seems unlikely to admit that this is just the result
of small number statistics.
The binary systems that can give rise to a high-carbon band star, in our
hypothesis, are severely constrained regarding the masses of the components.

In particular, the primary star should be larger than about $0.9 M_{\odot}$
to experience efficient third-dredge-up episodes during the AGB phase
\citep{stancliffe08, karakas10}, and consequently enrich its surface with
the carbon produced in the stellar interior.
The secondary should be less massive than about $0.8-0.85 M_{\odot}$, because
higher-mass stars would become white dwarfs
on a timescale shorter than $10-12$ billion years, which is the approximate
age of the Galactic halo. Finally, mass transfer
in binary systems with AGB donors is efficient in a limited range of orbital
periods between approximately $10^2$ and $10^5$ days \cite[e.g.][]{Izzard,
Abate}.

\citet{CL2008} computed the yields of AGB stars of extremely low  and zero
metallicity,
and they found that the [C/Fe] ratios of their yields increase
monotonically with decreasing [Fe/H] (as illustrated in their Figure 5).
The carbon abundance in the ejecta
of the AGB star varies within  a factor of four \relax  in the metallicity
range $-6.5\le$[Fe/H]$\le -3.0$
\citep{CL2008}.  Therefore, theoretically, there is no indication that
the nucleosynthetic yields of AGB stars  vary in metallicity in such
a way as to disfavour the formation of high-carbon band stars.
A recent review on the nucleosynthesis of AGB stars is given
by \citet{Karakas}.

\begin{figure*}
\begin{center}
\resizebox{\hsize}{!}{\includegraphics[draft = false, clip=true]
{plalpha_paper.eps}}
\end{center}
\caption[]{Ratio of $\alpha$ elements to iron
for the programme stars (red stars) compared to those measured
by our group in other extremely metal-poor dwarf stars \citep{bonifacio09,gto11,sdss_uves,gto12,topos1}.
Black squares are measurements from X-Shooter spectra, while black hexagons
are
measurements from UVES spectra. In the panel giving the [Ca/Fe] ratio, the
blue star symbols
are \ion{Ca}{ii} measures. We restricted the x-axis so as to exclude
SDSS\,J1035+0641; which only has an upper limit on iron and thus a lower
limit on [Ca/Fe] and is not informative.
}
\label{plot_alpha}
\end{figure*}

A possible explanation of the lack of high-carbon band stars at low [Fe/H]
is that at these
metallicities, such systems either do not form at all or are exceedingly
rare.
The existence of a rather sharp cut-off  suggests the existence of a physical
mechanism that prevents the formation of these systems.
Because the enriched material synthesised by the AGB star needs to be expelled
in the stellar wind
and accreted by a low-mass companion, the lack of high-carbon band stars
could indicate that at low [Fe/H]
binary mass-transfer processes become rarer or less efficient. Although the
binary-star fraction is not
well constrained at low metallicity, there is no evidence that it decreases
\cite[e.g.][]{gao14}.
The data on the binarity among stars with
[Fe/H]$<-3.6$ is scanty, yet the discovery of the binarity
of SDSS\,J0929+0238 \citep{topos3} suggests that it cannot
be much lower than among stars of higher metallicity.
It has been suggested that at low metallicity the ejection of the AGB envelope
becomes increasingly
inefficient \cite[][]{wood11}. If only a small mass is ejected by the primary,
the amount of
material accreted by the secondary may be insufficient to enhance the carbon
abundance up to
a typical high-carbon band value.

Another effect to take into account is that when a star accretes
material and becomes more massive, it evolves more quickly than a single
star of equal initial mass.
In the simulations of \cite{Abate} the synthetic population
of CEMP-$s$ stars has typically accreted a mass of approximately $0.1 M_{\odot}$.
Stars with
initial mass $0.8 M_{\odot}$ at low metallicity have a lifetime of approximately
the age of the Universe;
however, if they experienced binary mass-transfer they would become high-carbon
band CEMP-$s$
stars of mass $\approx 0.9 M_{\odot}$ and consequently their lifetimes would
be shorter than 12 Gyr.
Hence, they would not be visible any longer. Similarly, stars of initial
mass of $0.7M_{\odot}$
would reach masses of around $0.8 M_{\odot}$ and still be visible after 12
Gyr, but for a shorter
time than single stars of the same initial mass.
Also, the results of \cite{Moe} suggest that large initial mass ratios $q=M_{2,\mathrm{i}}/M_{1,\mathrm{i}}$
could be slightly more likely among low-mass binaries, hence increasing the
proportion of systems with initial
secondary mass $M_{2,\mathrm{i}}>0.8 M_{\odot}$.
The probability of observing a star at a given distance during its evolution
is
proportional to the time its  apparent luminosity is above our detection
threshold.  If a star is visible in its main sequence phase, it will also
be visible in the RGB phase, but not once it reaches the white dwarf stage,
unless it is very near to us.
A faster evolving star  reaches  the white dwarf stage more quickly
and  is thus less likely to be observed.
The decrease in lifetime of the high-carbon band population, due to their
increase in mass, naturally occurs at every metallicity,
but its consequences become more evident at [Fe/H]$\leq-3.5$ because fewer
stars are known in this range.

 The determination
of the binary fraction and the period distribution for different metallicity
bins
down to the lowest metallicities may provide a fundamental insight into the
properties of star formation at different metallicities.

\subsection{Lithium abundances}

In Fig. \ref{plot_Li} we show the Li abundances as a function of [Fe/H]
for our programme stars and  for stars taken from the literature.
We classify the stars in three groups: low-carbon band CEMP stars (star symbols);
high-carbon band CEMP stars (crossed squares); and carbon normal stars (filled
hexagons), which  includes all stars with [C/Fe]$< 1.0$ or for which
the C abundance has not been measured.
From this figure it appears that the Li abundances in the low-carbon band
CEMP stars have a behaviour
that is indistinguishable from that of the carbon normal stars.
On the other hand the high-carbon band CEMP stars are preferentially Li-depleted,
although there are a few measurements on the Spite plateau.
This is consistent with our hypothesis that the high-carbon
CEMP stars are the result of mass transfer from an AGB companion.
In most cases Li is depleted as a result of processing in the H-burning AGB
shell,
although in some cases it may also be produced through
the Cameron--Fowler mechanism \citep{CF71}.
Mass transfer from an AGB companion has been invoked
to explain the occurrence of Li-rich main sequence stars
in globular clusters \citep{koch11,monaco12}, although pollution
from  nearby RGB stars having undergone the Li-flash is
an alternative explanation \citep{Pasquini14}.
The point is that transfer from an AGB always results
in an enhancement of carbon, but  Li may be either depleted
or enhanced.

The stars SDSS\,J1034+0701 and  SDSS\,J1247--0341 both have
[Fe/H]\,$\sim -4.0 $. The measurements of the equivalent width
of the \ion{Li}{i} resonance doublet are very uncertain. In Fig. \ref{plot_lim4}
we show the observed spectra compared to a 3D NLTE synthetic spectrum.
We stress that this is not a fit; we just plot the synthetic spectrum to
provide guidance to the position and expected strength of the
 \ion{Li}{i} resonance doublet. Although
the measurement is uncertain, we believe that the detection of Li is robust.
Taken at face value, our measurements  place both stars
on the Spite plateau. All the other stars have either an upper limit
or a measurement that places them well below the Spite
plateau. While this behaviour, also referred to as `meltdown' of the Spite
plateau
(\citealt{sbordone10}, but see also \citealt{bonifacio07,aoki09}), is well
known,
these two stars on the Spite plateau appear exceptional.
In fact, recently \citet{Matsuno17} pointed out that
`no star in the literature
has comparable Li abundance to the Spite plateau below [Fe/H] of--3.5, except
for the primary of the
double-lined binary system CS\,22876--032.'
The two components of CS\,22876--032 are shown as $\times$ symbols in
Figs.\,\ref{plot_Li} and \ref{plot_Li_teff}.
While SDSS\,J1034+0701 and  SDSS\,J1247--0341 have
an effective temperature well above 6000\,K, as does
CS\,22876-032\,A \citep{jonay08},  the star SDSS\,J0140+2344 has an effective
temperature below 6000\,K;
it has roughly the same metallicity ([Fe/H]=--4.0) and,
like  CS\,22876-032\,B, it has a Li abundance well below the Spite plateau.
Therefore, our observations call into question the claim by
\citet{Matsuno17}, that Li abundances in the interval
$\rm -4.5 \le [Fe/H] \le -3.5$ are almost constant at a value
lower than the Spite plateau.
For stars with $T\rm_{eff}$ $> 6000$\,K,
there are some stars on the Spite plateau,
at least down to [Fe/H]=--4.0. On the
other hand, among the stars with $T\rm_{eff}$ $\le $6000\,K and
[Fe/H]$\le -3.5$, lithium is always below
the Spite plateau. This can be seen in Fig.\,\ref{plot_Li_teff},
where the only star at effective temperature below 6000\,K
on the Spite plateau is SDSS\,J0907+0246 ([Fe/H]=--3.44).
The current observations  suggest that
the $T\rm_{eff}$\ for which lithium destruction in the stellar
atmospheres becomes important, increases as metallicity decreases,
although it is unlikely that this is the only effect that drives Li destruction
since there are several
stars hotter than 6000\,K  that are found well below the Spite plateau.
\citet{BM97}  argued that for $T\rm_{eff}$ $\ge $5700\,K Li destruction
was negligible; however, their  sample had only three stars
with metallicity below --3.0. From Fig.\,\ref{plot_Li_teff} it is clear
that with increasing $T\rm_{eff}$\, there are fewer stars below the Spite plateau,
and, at any rate, the average Li abundance is higher.

Our detection of Li in SDSS\,J1035+0641 is to date the measurement of Li
in the most
iron-poor unevolved star. It poses a strong constraint on any theory that
aims
to explain the cosmological Li problem. Any theory involving stellar destruction
of Li must accommodate the fact that in SDSS\,J1035+0641 Li is measurable.

In other stars of comparable iron abundance, it is either completely
destroyed or, at least, more severely depleted.
Alternatively, if one tries to explain the Li abundance of this star
by a prompt enrichment in Li, one has to explain why such a prompt enrichment
has not taken place in the other stars with [Fe/H]$\le -5.0$.

\subsection{Abundances of other elements}

One of the main goals of the UVES observations was to increase the chemical
inventory
of the stars at very low metallicity.
The data presented in Table\,\ref{abbo2} fulfil this goal,
although the low metallicities of the stars imply that we have many
upper limits. We have two measurements
of Co that confirm that Co is enhanced over Fe in EMP stars, as already shown
by \citet{cayrel04} and \citet{bonifacio09}.  In the two cases where Sr is
measured,
it is enhanced over Fe; however, this is certainly a selection effect since
for a given
effective temperature, the higher  the abundance, the stronger  the line
and thus the
easier it is to detect it.

In Fig.\,\ref{plot_alpha} we provide the ratios of the measured $\alpha$
elements, Mg, Si, and Ca, to Fe.
In the upper panel, SDSS\,J1349+1407 clearly stands out as being extremely
enhanced in Mg, although its Ca abundance seems quite normal. There is another
star in our sample, SDSS\,J1050+2421 \citep{topos1},  that is highly enhanced
in Mg,
although not as much as SDSS\,J1349+1407.
We note that there is a discrepancy of about 1\,dex in the Ca abundance
of SDSS\,J1050+2421 derived from the \ion{Ca}{i} resonance line
or from the \ion{Ca}{ii} lines. This discrepancy
may be partly due to an incorrect gravity, since a
discrepancy of about 0.5\, dex is found between the iron abundances derived
from the \ion{Fe}{i}
and \ion{Fe}{ii} lines \citep{topos1}.
Based on
its proper motion, it has been pointed out that this star
is most probably a main sequence star with  a \ensuremath{\log g}\ $\sim$ 4.7, rather
than 4.0,
as was assumed in \citet{topos1} (M. Bessell, private communication).
The [\ion{Ca}{i}/\ion{Fe}{i}]
and the    [\ion{Ca}{ii}/\ion{Fe}{ii}] ratios differ by `only' about 0.6\,dex.

Thus, a change in gravity may alleviate the problem, but not solve it.
In Fig.\,\ref{plot_alpha} we plot the value
derived from the  \ion{Ca}{i} resonance line. Had we chosen the value derived
from \ion{Ca}{ii}, SDSS\,J1050+2421 would be highly enhanced in Ca as well.

The abundances of SDSS\,J1349+1407 resemble very closely those
of CS\,22949-037 \citep{depagne,norris02}; in fact, they have almost the
same [Mg/Ca]  ($\sim 1.2$).
Among the EMP stars, a [Mg/Ca]  almost as high is
found for HE\,1327-2326 (\citealt{frebel08} [Mg/Ca]=0.99) and an even higher
value is found
in SMSS\,J0313-6708  (\citealt{Keller14}) [Mg/Ca]=2.95).
Both CS\,22949-037 and HE\,1327-2326  are enhanced in Na: [Na/Fe]=+1.57 \citep{Andrievski}
and [Na/Fe]=+0.94 \citep{frebel08}.
Star  HE\,1012-1540,   analysed at high resolution by  the 0Z project
\citep{Cohen13}, also seems
to belong to this group ([Mg/Ca]=+0.83, [Na/Fe]=+1.02).
Quite intriguingly, a star with similar properties has been found
in the Hercules ultra faint dwarf galaxy \citep{Koch08}.
For Her-2, with [Mg/Ca]=+0.93 and [Na/Fe]=+0.78, \citet{Koch08}
argued that this may be understood in terms of enrichment from
very massive stars with masses of the order of 30 M\sun.

The other feature that stands out in Fig.\ref{plot_alpha}
is that we find additional stars with low $\alpha$-to-iron ratios,
for example SDSS\,J1442--0015 and SDSS\,J1247--0341.
This confirms our  earlier claim \citep{gto12}, based on X-Shooter
spectra, regarding the existence of a population of extremely metal-poor
$\alpha$-poor stars.
The presence of metal-poor stars with low  $\alpha$-to-iron ratios,
in some cases quite extreme \citep{Ivans03}, is also supported
by other investigations \citep{Cohen13,Susmitha16}. Recently
 \citet{hayes17} also recognised the presence of an $\alpha$-poor population
of stars belonging to the Galactic Halo,
albeit at a higher metallicity regime than the one considered in this paper.
The presence of these  $\alpha$-poor stars   has so-far
received little theoretical attention.
While \citet{Ivans03} has invoked a prompt enrichment by
type Ia supernovae, \citet{Cohen13} has suggested
that the diversity in nucleosynthesis products of
extremely metal-poor type II supernovae is greater than
that predicted by current models.
These stars could have formed in low-mass  dwarf galaxies and
subsequently accreted to the Milky Way Halo, carrying memory of
a different chemical evolution, as has been claimed
by \citet{hayes17}.

\section{Conclusions}

We have provided detailed abundances for a sample of seven EMP turn-off stars,
based on high-resolution spectra.
All the stars for which carbon could be measured are CEMP stars
and belong to the low-carbon band.
For the most iron-poor star,
SDSS\,J1035+0641, we are unable to detect any iron lines, but we
were able to place a stringent upper limit at [Fe/H]$\le -5.2$.
It is remarkable that we measure Li in this star, albeit
well below the Spite plateau. This is the first measurement of Li in
an unevolved star with [Fe/H]$\le -5$, and it places a strong constraint on any theory
to explain the cosmological Li problem.
Three of the programme stars have [Fe/H]$\sim -4.0$, and  lithium
has been measured in all three. Quite interestingly, the Li abundance of
the two warmer stars
places them squarely on the Spite plateau, while the cooler one lingers below.
This situation is reminiscent of what is observed in the binary system
CS\,22876-32 \citep{jonay08}. We have argued that this suggests that
the effective temperature at which Li depletion begins increases
with decreasing [Fe/H].

We confirmed that SDSS\,J1349+1407 is extremely enhanced in Mg but not
in Ca, and in fact its abundance pattern resembles that of CS\,22949-037
and
its Mg/Ca  is also similar to that of HE\,1327-2326.
This may suggest that there is a class of Mg-rich stars among EMP stars.

Our high-resolution observations have confirmed the existence of stars
with low $\alpha$-to-iron ratios, as pointed out by \citet{gto12}, based
on medium-resolution X-Shooter spectra.
The TOPoS project has been very successful in increasing the number of  stars
with detailed abundances at and below a [Fe/H] of --4.0, yet the numbers
are still
smaller than desirable for making robust statistical inferences.
Hopefully the Pristine survey \citep{Pristine1,Pristine2,Pristine3}
and its massive follow-up with WEAVE \citep{WEAVE} will soon boost the numbers,
and the LAMOST survey as well \citep{Li2015a,Li2015}.

\begin{table*}
\caption{Stellar parameters and abundances of C and Li}
\label{param}
\begin{center}
\begin{tabular}{lclrrcccll}
\hline \noalign{\smallskip}
 Star                   & $T\rm_{eff}$\ & \ensuremath{\log g}\ & $\xi$ & [Fe/H] & A(C) & A(C) & A(Ca) & A(Li) & EW(Li)\\
                        & K      & [C's]  & Km/s  &        &  1D  &  3D  & \ion{Ca}{ii}-K & & pm \\
\hline \noalign{\smallskip}
SDSS\,J0140+2344    & 5848   &  4.0   & 1.5   & \phantom{$<$}$-4.00\pm 0.14$ & 6.33 & 6.11 &      & \phantom{$<$}1.86 &\phantom{$<$}2.2 \\
SDSS\,J1034+0701    & 6224   &  4.0   & 1.5   & \phantom{$<$}$-4.01\pm 0.14$ & 6.28 & 5.96 &      & \phantom{$<$}2.24:&\phantom{$<$}2.8: \\
SDSS\,J1035+0641    & 6262   &  4.0   & 1.5   & $<-5.20$                     & 7.16 & 6.95 & 1.5  & \phantom{$<$}1.90  &\phantom{$<$}1.3\\
SDSS\,J1247--0341   & 6332   &  4.0   & 1.5   & \phantom{$<$}$-4.01\pm 0.32$ & 6.64 & 6.35 &      & \phantom{$<$}2.20:&\phantom{$<$}2.2:\\
SDSS\,J1349+1407    & 6112   &  4.0   & 1.5   & \phantom{$<$}$-3.60\pm 0.12$ & 7.00 & 6.82 &      & $< 0.9$ & $< 0.3$ \\
SDSS\,J1442--0015   & 5850   &  4.0   & 1.5   & \phantom{$<$}$-4.37\pm 0.16$ & 6.02 & 5.71 &      & $<1.58$ &$<1.2$   \\
SDSS\,J1507+0051    & 6555   &  4.0   & 1.5   & \phantom{$<$}$-3.41\pm 0.20$ &      &      & $<2.19$ &$<1.6$    \\
\noalign{\smallskip}
\hline
\end{tabular}
\end{center}
\end{table*}

\begin{table*}
\caption{Abundances relative to hydrogen [X/H] with solar abundances from \citet{lodders09}
for all elements except Fe and C whose solar abundances are from \citet{abbosun}.}
\label{abbo2}
\begin{center}
\begin{tabular}{llllllllll}
\hline
\noalign{\smallskip}
El          & Sun  &  J0140+2344     & J1034+0701     & J1035+0641                   & J1247--0341     & J1349+1407      & J1442--0015     & J1507+0051      \\
\hline \noalign{\smallskip}
\ion{C}{i}  & 8.50 &  $-2.17$        & $-2.22$        &  \phantom{$<$}$-1.33$        & $-1.86$        & $-1.50$         & $-2.48$        &                 \\
\ion{Na}{i} & 6.30 &  $-4.22$        &                &                              &                & $-2.74\pm 0.12$ &                &                 \\
\ion{Mg}{i} & 7.54 &  $-3.37\pm 0.02$& $-3.28\pm 0.10$&                              & $-3.77\pm 0.23$& $-2.18\pm 0.11$ & $-4.19\pm 0.05$& $-3.30\pm 0.13$ \\
\ion{Al}{i} & 6.47 &  $-4.29$        & $-4.27$        &                              & $<-4.23$       & $-3.97$         & $<-4.68$       & $<-4.03$       \\
\ion{Si}{i} & 7.52 &  $-3.91$        & $-4.12$        &                              & $-4.27$        &                 & $-4.53$        & $-3.67$         \\
\ion{Ca}{i} & 6.33 &  $-2.79$        & $-4.17$        &                              &                & $-3.42\pm 0.16$ & $-4.48$       & $-3.35$         \\
\ion{Ca}{ii}& 6.33 &  $-3.66$        &                &  \phantom{$<$}$-4.83$        & $-4.07$        &                 &                & $-3.05$         \\
\ion{Sc}{ii}& 3.10 &                 & $-3.38$        &                              &                & $-3.54$         &                &                 \\
\ion{Ti}{i} & 4.90 &                 &                &                              &                &                 & $-2.33$        & $-3.04\pm 0.12$ \\
\ion{Ti}{ii}& 4.90 &  $-3.75\pm 0.14$& $-3.84\pm 0.04$&                              &                & $-3.22\pm 015$  & $-2.44$        &                 \\
\ion{Cr}{i} & 5.64 &  $-4.17\pm 0.12$&                &                              &                & $-3.73$         &                &                 \\
\ion{Mn}{i} & 5.64 &                 &                &                              &                & $-3.87\pm 0.03$ &                &                 \\
\ion{Fe}{i} & 7.52 &  $-4.00\pm 0.14$& $-4.01\pm 0.14$&  $<-5.20$                    & $-4.01\pm 0.32$& $-3.60\pm 0.12$ & $-4.37\pm 0.16$& $-3.41\pm 0.20$ \\
\ion{Fe}{ii}& 7.52 &                 &                &                              &                & $-3.58\pm 0.16$ &                & $-3.56$         \\
\ion{Co}{i} & 4.92 &  $-3.13\pm 0.34$&                &                              &                & $-2.87$         &                &                 \\
\ion{Ni}{i} & 6.23 &  $-3.86\pm 0.12$& $-3.99$        &                              &                & $-3.43$         &                &                 \\
\ion{Sr}{ii}& 2.92 &  $-3.43\pm 0.06$&                &                              &                &                 &                & $-3.16\pm 0.02$ \\
\noalign{\smallskip}
\hline
\end{tabular}
\end{center}
\end{table*}

\begin{acknowledgements}
We are grateful to our referee Mike Bessell for his very thorough and useful
 report of our paper.
The project is supported by fondation MERAC.
N.C., H.G.L., and A.J.G. were supported by Sonderforschungsbereich SFB 881
``The Milky Way System'' (subproject A4) of the German Research
Foundation (DFG).
R.S.K. acknowledges support from the European Research Council via the Advanced
Grant
``STARLIGHT: Formation of the First Stars'' (project number 339177).
C.A. acknowledges funding from the Alexander von Humboldt Foundation
\end{acknowledgements}

\bibliographystyle{aa}

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text:
DISIM Teaching Information Engineering TUNING
Equation of Mathematical Physics / Equazioni della fisica matematica
Integrated course
Modules:
The course profile, written following the Tuning international methodology, is available here.
MAT/05,MAT
Bachelor Degree in Mathematics: 6 Ects (b)+3 Ects (c)
Module Partial differential equations: 1° semester
Module Modelli Matematici: 1° semester
Compulsory 3rd year Bachelor Degree in Mathematics curriculum Generale
Corrado Lattanzio
Maurizio Serva
Module Partial differential equations: EQUATIONS OF MATHEMATICAL PHYSICS Students will know basic of properties (existence, uniqueness, etc.) and techniques (characteristics, separation of variables, Fourier methods, Green's functions, similarity solutions, etc.) to solve basic PDEs (conservation laws, heat, Laplace, wave equations).
Module Modelli Matematici: This course aims to enable the students to understand basic Quantum Mechanics and to handle the Schrödinger Equation.
Module Partial differential equations
Integral curves and surfaces of vector fields. First order partial differential equations. Linear and quasi linear partial differential equations (PDEs) of first order. Method of characteristics. The initial value problem: existence and uniqueness. Development of shocks.
The Cauchy-Kovalevsky theorem. Linear partial differential operators and their characteristic curves and surfaces. Methods for finding characteristic curves and surfaces. The initial value problem for linear first order equations in two independent variables. Holmgren's uniqueness theorem. Canonical form of first order equations. Classification and canonical forms of second order equations in two independent variables. Second order equations in two or more independent variables. The principle of superposition.
The divergence theorem and the Green's identities. Equations of Mathematical Physics.
LAPLACE'S EQUATION AND HARMONIC FUNCTIONS Elementary harmonic functions. Separation of variables. Inversion with respect to circles and spheres. Boundary value problems associated with Laplace's equation. Representation theorem. Mean value property. Maximum principle. Harnack's inequality and Liouville's theorem. Well-posedness of the Dirichlet problem. Solution of the Dirichlet problem for the unit disc. Fourier series and Poisson's integral. Analytic functions of a complex variable and Laplace's equation in two dimensions. The Neumann problem.
GREEN'S FUNCTIONS. Solution to the Dirichlet problem for a ball in three dimensions. Further properties of harmonic functions. The Dirichlet problem in unbounded domains. Method of electrostatic images.
THE WAVE EQUATION. Cauchy problem. Energy method and uniqueness. Domain of dependence and range of influence. Conservation of energy. One-dimensional wave equation. D'Alembert formula. Characteristic parallelogram. Non homogeneous equation and Duhamel's method. Multi-dimensional wave equation. Well posed problems. Fundamental solution (n=3) and strong Huygens' principle. Kirchhoff formula. Method of descent. Poisson?s formula (n=2). Wave propagation in regions with boundaries. Uniqueness of solution of the initial-boundary value problem. Separation of variables. Reflection of waves.
THE HEAT EQUATION. Heat conduction in a finite rod. Maximum principle and applications. Solution of the initial-boundary value problem for the one dimensional heat equation. Method of separation of variables. The initial value problem for the one dimensional heat equation. Fundamental solution. Non homogeneous case and Duhamel's method. Heat conduction in more than one space dimension.
Module Modelli Matematici
The behavior of quantum systems and a little of hystory.
Postulates, principles and mathematical tools of Quantum Mechanics.
Position and momentum: the Heisenberg's uncertainty principle.
The dynamics: the Shrödinger equation.
The Shrödinger equation in one dimension.
The Shrödinger equation for the harmonic oscillator.
have advanced knowledge of classical theory for first and second order PDEs of Mathematical Physics;
have basic notions of fluid mechanics from an engineering point of view;
be able to understand when an elementary problem from Mathematical Physics is well posed;
be able to solve classical problems coming from Mathematical Physics such as initial, boundary, initial-boundary value problems;
be able to learn autonomously additional results for PDEs of Mathematical Physics.
• have acquired the basic notions of Quantum Mechanics, • be able to handle the Shrödinger Equation in simple cases, • be able of reading and understanding more advanced topics in Quantum Mechanics, • have acquired a deeper comprehension of the physical world, • be able to face novel problems with a similar mathematical modeling.
Module Partial differential equations: The student must know the basic notions of mathematical analysis, including Fourier series and ordinary differential equations and the basic notions of continuum mechanics.
Module Modelli Matematici: Classical Mechanics, Elementary Probability Theory, Linear Algebra.
Module Partial differential equations: Lectures and exercise sessions.
Module Modelli Matematici: Lectures and exercises.
Module Partial differential equations: Written and oral.
Module Modelli Matematici: Written and, if necessary, oral examination.
S. Salsa, G. Verzini, Equazioni a derivate parziali: complementi ed esercizi. Springer-Verlag Italia. 2005. In Italian, ISBN 10 88-470-0260-5
E. C. Zachmanoglou and Dale W. Thoe, lntroduction to Partial Differential Equations with Applications. Dover Publications, Inc.. 1986. ISBN 0-486-65251-3
L.C. Evans, Partial Differential Equations. American Mathematical Society. 2010. Second edition, ISBN-13: 978-0821849743
S. Salsa, Partial Differential Equations in Actions: from Modelling to Theory. Springer-Verlag Italia. 2008. ISBN 978-88-470-0751-2
W. A. Strauss, Partial Differential Equations, Student Solutions Manual: An Introduction. John Wiley & Sons, LTD. 2008. Second edition, ISBN-13: 978-0470260715
W. A. Strauss, Partial Differential Equations: an introduction. John Wiley & Sons, LTD. 2007. Second edition, ISBN-13 978-0470-05456-7
Lev D. Landau e Evgenij M. Lifšits, , Fisica Teorica 3 - Meccanica quantistica Teoria non relativistica. Editori Riuniti, University Press. 2010.
P. A. M. Dirac, I princ??pi della Meccanica Quantistica. Bollati Boringhieri. 1990.
K. Konishi e G. Paffuti, Meccanica Quantistica: nuova introduzione. Pisa University Press. 2005. http://people.disim.univaq.it/?serva/teaching/teaching.html
http://people.disim.univaq.it/~serva/teaching/teaching.html
http://people.disim.univaq.it/~serva/teaching/teaching.html (Module Modelli Matematici)
Teaching material:
Click here to access the teaching material available on this site (last update: 27/12/2019).
Teaching material available on the external website http://people.disim.univaq.it/~serva/teaching/teaching.html. Teaching material available on the external website http://people.disim.univaq.it/~serva/teaching/teaching.html. (Module Modelli Matematici)
Course information last updated on: 08 ottobre 2018, 15:02

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text:
Q: How can pass a props to a variable? I'm trying "hydrate" props from elements to child components that will render. The problem is that I can't figure out how I can do it with my configuration.
I have seen this answer, I tried to adapt it, but so far I'm getting errors (see bottom).
For a bit of background, I'm developing a Rails based application that uses React for the front end. So I don't use React router or such, it just "displays" the datas.
Here is how I set everything up:
front.js (where everything gets rendered)
import React from 'react';
import ReactDOM from 'react-dom';
import extractActionName from './lib/extractActionName';
import {elementForActionName} from './lib/elementForActionName';
import 'jquery';
import 'popper.js';
import 'bootstrap';

let actionName = extractActionName();
let value = "value";

let renderElement = function (Element, id) {
    ReactDOM.render(
        <Element value={value} />,
        document.getElementById(id)
    );
};

renderElement(elementForActionName[actionName], actionName);

lib/elementForActionName.js
import React from 'react';
import Homeindex from '../home/home';
import Contact from '../home/contact';

// This files create an associative array with id React will be
// looking for as a key and the component as value

export const elementForActionName = {
    'index': <Homeindex />,
    'contact': <Contact/>,
};

lib/extractActionName.js
export default function extractActionName() {
  // The body contains classes such as "home index", so
  // I return the "action name" of my controller (home) to
  // front.js so I will render the good component

  return document.body.className.split(' ').pop();
}

home/home.js
import React from 'react';
import Header from '../layout/header';
import Footer from '../layout/footer';

export default class homeIndex extends React.Component {
  render() {
    return(

Hello this will be the content of the landing page hello

    )
  }
}

My problem is that I'd like to make an Ajax call in my "front.js" file, then transmit the received data (here, "value"). The error I'm getting is the following:

Uncaught Error: Element type is invalid: expected a string (for
  built-in components) or a class/function (for composite components)
  but got: object.

I'm lacking experience with React, how can I resolve this problem?
Thank you in advance.

A: You are currently returning the instance of a component:
export const elementForActionName = {
    'index': <Homeindex />, <--- here
    'contact': <Contact/>,
};

And then attempting to instantiate it again:
let renderElement = function (Element, id) {
    ReactDOM.render(
        <Element value={value} />,  // <--- here
        document.getElementById(id)
    );
};

Instead, just use the component class:
export const elementForActionName = {
    'index': Homeindex,
    'contact': Contact,
};

redpajama_set_name: RedPajamaStackExchange


text:
Star Trek TV series to begin filming in Toronto this fall, CBS confirms
Wednesday May 04th 2016
Heads up, Trekkies — filming for the new Star Trek television series is slated for Toronto, where local fans hope it will live long and prosper.
The news about the new television series was confirmed by CBS Television Studios on Twitter. The show will begin filming in the city sometime this fall.
"We don't have [any] other details to share at this point," Kristen Hall, CBS Television Studios' vice-president of communications, told CBC News via email.
Last November, CBS said the series would make its debut in January 2017.
"The brand-new Star Trek will introduce new characters seeking imaginative new worlds and new civilizations, while exploring the dramatic contemporary themes that have been a signature of the franchise since its inception in 1966," CBS said last fall in a release.
"The new series will be produced by CBS Television Studios in association with Kurtzman's Secret Hideout."
The original Star Trek television series debuted on Sept. 8, 1966, and led to the creation of 12 feature films and five successful series on television, CBS Television Studios said last November.
Source: CBC


text:
India and Japan have shared a rich past with various fruitful business relationships; and in the coming future, the trend doesn't seem to slow down any time soon. Our Japan Business Desk aims to be an active stakeholder between the two countries, opening gateways of opportunities for Japanese investment and businesses coming to India and vice versa.
Why India?
India and Japan have complemented each other productively on the global stage, with both the countries sharing a high regard of mutual business interests. Japan has carved a niche of its own as one of India's prime business allies. Japanese Industrial Townships (JITs) have been established dedicated hubs across several states and various key Indian cities.
3rd largest FDI partner
Japan is currently India's 3rd largest investor in terms of FDI, with investments to the tune of 30.27 billion USD from April 2000 – March 2019
14th largest import partner
Japanese imports to India were worth 12.77 billion USD in 2018-19, making it India's 14th largest import partner
Over 1,400 companies
As of date, over 1,400 Japanese companies (ranging from SMEs to major corporations) have set up operations in India
Over 5,000 business establishments
As of date, over 5,000 Japanese business establishments have been set up in India
JITs have tax incentives and exemptions
Tax incentives, exemptions in utility charges for 5-10 years, single window clearances and quality infrastructure are some of the benefits provided to investors in the JITs
India Entry Strategy
In order to gain an understanding of the local market and develop a medium or long-term presence, a Japanese company can partner with an Indian company to form a joint venture
Wholly owned subsidiaries are preferred as the mode of incorporation in cases such as setting up a manufacturing capability, or aiming to establish long-term market presence
To study the local market or to stay in India for a short-term duration for certain projects or activities, incorporation of liaison offices, branch offices and project offices are preferred as the mode of entry
Factors Affecting India Entry
While evaluating the Indian market for business expansion and to better prepare for undertaking operations in the Indian market, below are a few important aspects that should be considered
Indian tax scenario
An evolving tax scenario which aims to strike the right balance between direct taxes and indirect taxes can be seen as a challenge for market entrants
Ease of doing business ranking
After climbing to rank 63, India has steadily improved in the EODB rankings and now plans to improve further with focus on 6 major areas
Evolving market and consumer dynamics
Modernization and a rising urban population has heavily influenced consumer dynamics, as India continues its push to become a global business hub
A suitable base of operations
A strong push towards business-conducive public policy and development of relevant ecosystems has primed the country for foreign entrants in its market
What Can Coinmen Do To Help
As a multi-disciplinary firm, Coinmen helps companies by helping them incorporate, operate and expand in the Indian landscape. Via our specialties in financial and business advisory, we undertake a holistic approach to bridge cultural and business gaps for continual growth. Our range of services is highlighted below.
Download our firm profile for complete details on what we do to help Japanese companies do business in India.


text:
A Face in the Crowd
While many of us can't even remember what the business world was like in the pre-Internet era, the transfer of so much of our personal and professional information into a virtual online world is really still in its infancy compared to the other forms of communication that have existed for centuries.
Why is this important? Because we're still assessing the ramifications of this tech-dominated culture, and how each new advance will impact individuals and organizations. For those of us dedicated to securing the data that exists in a constant state of flux, staying ahead of this curve is one of the challenges we take most seriously.
Recently, CNN reported that Google was hard at work on a facial recognition feature, which would be achieved by storing pictures of millions of faces in a photographic encyclopedia database. That means you could take a picture of someone, including a stranger on the street, and then upload that photo and receive relevant information about that person, including his or her name, email address and phone number. The feature could be introduced as a new app or as an update to an existing tool, such as Google's image search engine.
In theory, a person would have to approve the use of their likeness in this type of venture. But individuals and companies who do not pay attention to online security, or hire a specialist to create a safe environment for them, may have already had their security compromised by more than one website. We all thought Google Maps with those Street Views were a great idea, until some enterprising criminals used the app to case empty houses.
How would Google acquire the photos? Their web bots have already crawled across trillions of Web pages to deliver results to search engine queries, including Facebook pages, Flickr and other photo-sharing sites.
One implementation of facial recognition software is already in existence – it's called Recognize Me and it was made available as an iPhone app to plug a potential security hole. If your phone is stolen, its front-facing camera can scan the identify of the person holding it, and will not open if that face does not match the owner's.
As to the larger facial recognition feature, a Google representative has responded to the CNN story, saying it was "unlikely" they will create such a database, and that doing so was "crossing the creepy line." The network is standing by its reporting.
Stay tuned – this one could get interesting.


Robert of Mayflower's talks on self-unfoldment and living a spiritual life.
Unedited talks, up to two hours long, given by Robert are available for purchase.
with the name of the talk requested. The talk(s) will be emailed to you.
Deep insights into one of Blavatsky's last works on developing intuitive understanding of one's own self-initiation, in light of stillness, universal love, opening the chakras with virtue, and transforming death into the three immortal bodies of the buddha. Wisdom and compassion as two wings to the heart of enlightenment.
Includes insights into theosophy (the wisdom of God), meditation, and Rudolf Steiner's use of mantra. Secrets of space, time and self, and Tibetan buddhist emptiness practice. Empowerment through meditation and prayer.


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CS ROSETTA is a protocol which generates 3D models of proteins, using only the 13CA, 13CB, 13C', 15N, 1HA and 1HN NMR chemical shifts as input. Based on these parameters, CS ROSETTA uses a SPARTA-based selection procedure to select a set of fragments from a fragment-library (where the chemical shifts and the 3D structure of the fragments are known). The fragments are assembled using the ROSETTA protocol. The generated models are rescored based on the difference between the back-calculated chemical shifts of the generated models and the input chemical shifts. For more information see our online web portal manual and tutorial and/or consult the CS-Rosetta home page at: http://spin.niddk.nih.gov/bax/software/CSROSETTA/index.html.
Give your run a name Required!
TALOS file to submit Required!
Number of models to generate A value is required. Invalid format. The entered value is less than the minimum required. The entered value is greater than the maximum allowed.
"The eNMR platform for structural biology."
J. Struct. Funct. Genomics, 11, 1-8 (2010).
"The eNMR and WeNMR projects (European FP7 e-Infrastructure grants, contract no. 213010 and 261572), supported by the national GRID Initiatives of Belgium, Italy, Germany, the Netherlands (via the Dutch BiG Grid project), Portugal, UK, South Africa and the Latin America GRID infrastructure via the Gisela+ project is acknowledged for the use of web portals, computing and storage facilities."


text:
Breaking News Politics
Nigeria Overtakes India In World's Extreme Poverty Ranking
Fearless Reports Reply 26 June A+ A-
https://www.fearlessreports.com/2018/06/nigeria-overtakes-india-in-worlds.html
File picture
Nigeria has overtaken India as the country with the largest number of people living in extreme poverty, a new report by the World Poverty Clock has said.
According to the report, extreme poverty in Nigeria is growing by six people every minute, the highest number in the world.
India on the other hand, is witnessing a decline in its level of extreme poverty.
At the end of May (2018), the survey showed that Nigeria had an estimated 87 million people in extreme poverty, compared to India's 73 million.
The report further stated that in Africa, D.R Congo may soon overtake India as number two, while Africa may be home to additional 3.2 million people living in extreme poverty by the end of 2018.
With the report, the United Nations' Sustainable Development Goal (SDG) to end extreme poverty by 2030 may be unattainable even as Africa faces major population Increase.
-Channel TV
Breaking News, Politics


Cayenne pepper is a finely grounded powder arranged from the seeds and pods of different sorts of chile. It is a hot chilli pepper used to flavour dishes. The fruits are for the most part dried and ground.
Cayenne pepper powder can be utilised to make spicy beverages, chutney, sauce or can even be utilised for pickling.
Powdered cayenne pepper is added to suppers for a health and spicy taste.
It can be added to eggs, pasta, veggies and nuts.
Can be utilised as a spice, as a topping at thetable, generally seafood, for example, clams, smoked salmon and trout, sardines, singed mussels,crawfish, scallops, crab and lobster.
It is great with cooked, roasted, grilled, stewed or fried meats.
It adds piquancy taste to casseroles, stews, particularly cheese, grill and shellfish sauces.
Cayenne pepper can be utilised as a part of the making of cheese biscuits and straws, pickles, ketchup, chutneys, marinades, and smoked foods.
Cayenne can ease resentful stomach, sore throats, ulcers, spasmodic and bothering coughs, anddiarrhoea.
Cayenne pepper could successfully keep the arrangement of the fungal pathogens.
Cayenne pepper is a well-known stomach digestive aid. It stimulates the stomach related tract.
Cayenne pepper may help hypersensitivities.
Cayenne empowers the creation of saliva, a critical key to excellent digestion and keeping up ideal oral wellbeing.
Cayenne is a brilliant additive and has been utilised generally to keep foodcontamination from bacteria.
It is trusted that birds are the main distributors of Cayenne Pepper. They cannot taste the warmth and eat the berries with the seeds intact. When these seeds go through the bird'sdigestion they are kept in another place with enough fertiliserrich with nitrogen to get started.
The seeds are up to 12cm long and 2.5cm in diameter. Cayenne is produced using the matured fruit, differing from red to yellow. The powder is red-brown or red in shading. A few cayennes incorporate the ground seeds and are hotter than those which prohibit them.


This dish used to be my go-to, only-thing-I-was-confident-enough-to-serve-to-others dish. Not sure what happened, but I don't think I'd made it in a few years. It's still just as good, sweet, and fruity as before. It's also easy – not much hands-on time.
Start off by combining a can of pineapple chunks with a bunch of brown sugar, and stirring until the sugar is dissolved in the pineapple juice.
Mmm, sugar! Hah, did you know both my parents are dentists?
Place your chicken breasts in an 8X8″ baking dish. Cut off any particularly massive/offensive chunks of fat, but otherwise leave the breasts whole. Pour the pineapple/brown sugar mixture over the chicken.
This will be delicious so soon!
Throw it in the oven for 55 minutes, get some rice cooking as well, and take a quick nap. Or make a side? I marinated some asparagus in soy sauce with garlic for a few hours earlier that day, and just cooked that on a flat pan towards the end of the 55 minute, but feel free to do something fancier.
Once the chicken is done cooking, carefully (not because this is important or easy to mess up, just because you don't want to burn yourself) pour off the pineapple juice into a pot. It's ok if a few chunks of pineapple go into the pot, but try to keep them mostly in the dish with the chicken. Throw some foil over the chicken and pineapple to keep it warm, and put it aside for a minute. Put the pineapple juice pot on the stove, and heat over medium high heat, stirring frequently and using cornstarch to thicken to a consistency you like. I aim for duck sauce-esque.
If you're not too familiar with cornstarch, don't pour the powder straight from the box into anything you're trying to thicken – it'll just clump up. Instead, put a tablespoon or so (really, don't bother measuring, it's not that important) in a cup and mix in a small amount of cold water – just enough to be able to wet all the cornstarch. Stir that up, and then spoon into the liquid you're thickening and it'll do the job.
Serve the chicken and pineapple over rice, and top with the pineapple sauce you just made. Yum!
So many food groups, it must be good for you!
Preheat oven to 350 degrees. Combine brown sugar and pineapple in medium bowl and stir to dissolve sugar.
Cut any excessive fat chunks off chicken and then place the breasts in an 8X8″ baking dish. Pour the pineapple mixture over the chicken and bake 50-55 minutes or until lightly golden.
Remove chicken from oven and pour pineapple juice into pot. Tent chicken with foil and set aside. Heat juice over medium high heat on the stove and thicken with cornstarch.
Serve chicken over rice, and top with pineapple sauce.
This entry was posted in Dinner and tagged Brown Sugar, Chicken, Pineapple. Bookmark the permalink.
Quick and easy is the best way to do dinner. I tend to be starving by about 4:30, so…complex dinners are really weekend only.
I remember when you mad this chicken for me. It was delicious.
Oooh yeah, that did happen once! And chicken and broccoli once at Tufts, and that enchilada lasagna on Mothers' Day… At this rate it'll only be 2 1/2 years until the next time I cook for you!
At Easter dinner at my friend Megan's house, her dad made Asparagus in the oven with Mandarin Oranges (in syrup). It might be too much fruitiness to go with this chicken, but it was sooo good!
Ooh, yeah, I might not put that with this meal, but I'd definitely try it in general!


Marinade chicken breasts in the Garlic Mango Dressing a few hours (just enough to coat) in a zip lock bag. Discard marinade when done.
Slice chicken breasts open without cutting all the way through to create a pocket where you can stuff the goat's cheese.
Bake in 425°F oven until done, about 40 minutes.
While chicken is cooking, sauté asparagus in frying pan with olive oil. Can season with fresh sliced garlic cloves, salt and pepper. (BBQ asparagus is also good).
SPINACH SALAD – on the side, mix spinach, almonds (green onions – optional) and oranges segments into a bowl. Toss with Garlic Mango Salad Dressing before serving.


Police want to speak to this man after a woman was allegedly sexually harassed and assaulted during a prolonged period while using the Tube in west London earlier this month.
The 30-year-old victim had boarded a Victoria Line service heading towards central London on April 11 at 4.45pm when a man, believed to be in his late 20s, approached the woman and sat opposite her.
During their journey, he repeatedly made eye contact with the victim whilst touching himself inappropriately.
She got off at Green Park to change onto the Jubilee Line, but the suspect followed the victim, standing behind her on the escalator and touching her inappropriately.
He continued to follow her onto the Jubilee Line tube, where he again sat opposite his victim, this time exposing himself to her.
The incident comes shortly after exclusive figures show sexual offences have nearly doubled on some Tube lines.
British Transport Police (BTP) have now released the photo of a man they wish to speak to in connection with this incident. They also want to speak to a person who may have come to the aid of victim while she was in Green Park.
Investigating officer Detective Constable Andrew Parkinson said: "The man responsible was committed to harassing his victim and it is essential he is identified.
"I am keen to speak to the man in the CCTV image as I believe he may hold vital information to this investigation.
"We understand that a member of the public may have come to the aid of the victim on the escalator at Green Park.
Anyone with any information can contact BTP on 0800 40 50 or text 61016 quoting reference 300 of 27/04/2016. Alternatively, information can be passed anonymously through Crimestoppers on 0800 555111.
Earlier in April BTP said a man sitting at a platform at Green Park was punched in the thigh with such force he was left with a puncture wound on his leg.


UMCP currently registered student in good judicial standing.
Have at least a 3.5 cumulative GPA.
Demonstrates campus and community involvement.
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Brief statement of your involvement in the campus community.
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Brief statement of any work experience you have.
An unofficial transcript in the envelope containing your application.
An essay (no more than 250 words).
Electronic submission is available here.


Join Larry, Moe, and Curly, those comedy icons, as they search for a secret treasure. Stay one step ahead of their dastardly landlord, Mr. G. Reedy while hunting for clues in a variety of levels.
Relive the hilarious antics of the The Three Stooges, inspired by classic in-game shorts and movies.
Challenge time frenzy mode or search for clues at your own pace in relaxed mode!
Hundreds of hand-illustrated objects to find!
Unlockable secret levels and high score tracking!
A humorous original concept in casual gaming's most popular genre!


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See where the collarbones meet the sternum? That's it for the shoulder girdle's connection to the ribcage.
The thing about the shoulder exercises gathered on this page is that they all work, in the sense that a good cookbook works if you actually open it and cook.
And these are the general guidelines to help you cook with your shoulders.
• Look closely at a skeleton. Notice that the shoulders and arms make a delicate "girdle" that drapes over the upper rib cage – a girdle so expressly designed for mobility that it's attached to the ribcage, bone-to-bone, in only one place: where the collarbones meet the sternum.
Incorporate that image into your mental body map, and remember, despite what it sometimes feels like, your shoulder blades are not nailed in place. It's in their nature to glide.
• Whenever you can, roll your upper arm bones out – your palms will rotate forward. Notice how doing that firms your shoulder blades and presses their outer edges gently toward your spine.
Then bend your elbows, pull the backs of your elbows gently down, and draw your inner shoulder blades down your back.
This outward rotation of the upper arms, and downward action of the inner shoulder blades is present in almost every yoga pose. Make it part of your body's habit pattern, and it will be that much more accessible when you practice.
• In shoulder stand, make sure that you can press down on your outer shoulders.
The gap between the top blankets will help you press down with your shoulders.
If you can't, and instead you feel weight on your neck, try this shoulder stand setup from Donald Moyer.
Even if you're just not sure, give it a try. If you suddenly find a new clarity and strength in your shoulders, you'll be glad you did.
This setup, by the way, isn't necessarily your new shoulder stand prop forever.
The goal is to work the outer shoulders so well, and become so strong and open, that you can work on a flat surface.
But you won't move toward that goal if you can't work your outer shoulders in the first place.
That would be like trying to bake without turning on the oven.
I've always been told that tucking the baby finger inside is not a good idea, although I can't pretend to tell you exactly why. I do know what you're talking about with the wrists feeling more even and less strain in the fingers when you tuck it in.
For me it's less the baby fingers than the ring fingers. Every time I do a headstand I have to take my wedding ring off, or the pain in my fingers will take me out of the pose.
Intuition says that for both of us, the solution is in working the hands less and the forearms more. Even when I'm stretching my fingers away from my hands, I'm still trying to keep my hands relaxed. Over time it's been getting better. My fingers used to get wet with sweat and go white in headstand – quite disturbing really.
Next post: Five-Minute Yoga Challenge: hang your head to free your neck.


text:
Hoverboards Will Be Banned From Metrolink Commuter Trains In The New Year
By Danny Jensen
Published Dec 29, 2015 11:00 PM
"Hoverboards" (Photo by Christopher Furlong/Getty Images)
Beginning in the new year, Metrolink will ban hoverboards from all commuter trains.
Days after the new California law that says where you can and can't ride the electronically motorized skateboards goes into effect, Metrolink will prohibit passengers from bringing the boards onto all of their trains starting Jan. 4, reports City News Service. Citing safety concerns over the popular self-balancing, two-wheeled boards, Metrolink spokeswoman Sherita Coffelt says that they wanted to take proactive steps to ban the devices, even though there have been no reported injuries involving them on Metrolink trains or at its 55 stations.
"This is a proactive step we've taken to ensure the safety of our passengers," Coffelt tells City News Service. "There have been concerns voiced about these devices catching fire and blowing up, and until there are more studies done, we're not going to allow them on the trains."
There have been reports of hoverboards—a far cry from what Marty McFly rode in Back to the Future II—bursting into flames in at least 10 states, including California. Safety concerns have also been raised over riding the boards in pedestrian areas, and they're illegal in New York City.
Metrolink says that if someone tries to get on a Metrolink train with one of the boards, they'll be asked to exit the train, but the boards won't be seized. "They may not be able to ride," Coffelt says. "We'll try to work with them and give them the option of returning to take another train."


Like last year, immunotherapy continues to be a hot topic at the AACR Annual Meeting 2017. Now that a plethora of clinical trials have established positive responses from immunotherapies—immune checkpoint inhibitors, in particular—in patients with a variety of cancer types, one of the logical next questions is, are the responses durable?
According to data presented on Monday, April 3, from a number of clinical trials across an array of cancer types, the answer appears to be "Yes." For many patients whose cancers responded to treatment with an immune checkpoint inhibitor, particularly those that target the immune checkpoint proteins PD1 and PDL1, the responses appeared to have lasted for several years.
In a phase I clinical trial, CA209-003, patients with heavily pretreated, advanced non-small cell lung cancer (NSCLC) were randomly assigned to three different dose levels of the anti-PD1 immunotherapeutic nivolumab (Opdivo). Prior analysis of data from this trial showed that nivolumab had promising clinical activity in this patient population.
Data presented on Monday showed that after following 129 patients in this phase I trial for a minimum of about 58 months, overall survival rates in patients with squamous and non-squamous NSCLC were 16 percent and 15 percent, respectively. According to the National Cancer Institute's SEER data, the five-year survival rate for patients with advanced lung and bronchus cancer is 4.3 percent, and for those with advanced NSCLC, it is 4.9 percent.
"This is the first report of the long-term survival rate in patients with metastatic NSCLC treated with an immune checkpoint inhibitor. Our study results show that for a small subset of patients, immunotherapy can work for a very long time," said the study's lead author Julie Brahmer, MD, associate professor of oncology at the Bloomberg~Kimmel Institute for Cancer Immunotherapy at Johns Hopkins.
David Gobin, a retired police officer who entered this clinical trial in late 2010 after multiple rounds of prior treatment of his advanced lung cancer, including two surgeries, radiation, and chemotherapies, continues to benefit from nivolumab.
Data from a phase I clinical trial showed that metastatic triple-negative breast cancer (TNBC) patients who experienced positive responses to the anti-PDL1 immune checkpoint inhibitor atezolizumab (Tecentriq) had a significantly longer overall survival compared with those who did not respond.
This study involves the largest cohort of patients with metastatic breast cancer treated with immunotherapy to be presented to date, and it is the first study to report data on survival for this subgroup, according to the study's lead author Peter Schmid, MD, PhD, director of the St. Bartholomew's Breast Centre at St. Bartholomew's Hospital and Barts Cancer Institute in London.
While both one- and two-year overall survival rates for responders were 100 percent, for nonresponders, the rates were 33 percent and 11 percent, respectively. "Another noteworthy finding is that metastatic TNBC patients treated with atezolizumab had a prolonged median duration of response of 21 months, which is substantially longer than what has been seen with any other treatment to date for this patient population," Schmid said.
Results from the phase III clinical trial CheckMate 067 showed that patients with advanced melanoma who received a combination of nivolumab and the anti-CTLA4 immune checkpoint inhibitor ipilimumab (Yervoy) had improved overall survival compared with those who received ipilimumab alone.
After a minimum follow-up of 28 months, median overall survival had not been reached for patients in the combination arm and those who received nivolumab only (because most of them were still alive at the time of data evaluation), but for those in the ipilimumab arm, the median overall survival was 20 months.
Data from a phase II clinical trial, JAVELIN Merkel 200, presented by Howard L. Kaufman, MD, a surgical oncologist at Rutgers Cancer Institute of New Jersey in New Brunswick, New Jersey, showed that patients with advanced Merkel cell carcinoma, an aggressive type of skin cancer, who responded to the anti-PDL1 immunotherapeutic avelumab (Bavencio), had durable responses.
After a median of 16.4 months of follow-up, 29 of the 88 enrolled patients had positive responses to avelumab, for an overall response rate of 33 percent. This included 10 patients with a complete response. The researchers estimate that 74 percent of patients will have a response that lasts one year or longer.
While the latest data from these clinical trials attest to the durability of immune checkpoint inhibitor responses, it is important to note that only a fraction of patients in these clinical trials responded to these therapies: The objective response rate (patients who had complete responses plus those who had partial responses) in patients with advanced NSCLC who received 3mg/kg nivolumab was 32 percent, while it was 31.8 percent for patients with advanced Merkel cell carcinoma treated with avelumab, and 10 percent for patients with metastatic TNBC treated with atezolizumab.
Further, even though the objective response rate for patients with metastatic melanoma who received the ipilimumab-nivolumab combination was 61 percent, as Larkin noted, the combination resulted in increased rates of adverse events.
The challenge of immune checkpoint inhibitors working only for a fraction of patients is one of the areas highlighted as needing more research by AACR President-Elect Elizabeth Jaffee, MD, in a post to forecast immunotherapy advances in 2017. She also emphasized that we still need to address the fact that some patients experience serious side effects, and some develop resistance to treatment, but she predicts we will make progress in these areas this year, along with identifying mechanisms to deliver immune checkpoint inhibitors in a more targeted way to circumvent the toxic side effects.


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What is Chris O'Donnell's Golf Handicap?
He is not only a talented actor.
Chris O'Donnell's Golf Handicap is around 5.
More about Chris O'Donnell's Golf Handicap
Chris O'Donnell was born on 26th June 1970. Chris is a famous actor and former model.
O'Donnell is a solid golfer who has been playing at the Pebble Beach AT&T Pro-AM for years.
His brother John O'Donnell is founder of the golf clothing brand Johnnie-O.
Last updated: 10-Dec-2021
How many Majors has Martin Kaymer won?
Who has won the most US PGA Championships?
How Many Majors Has Hideki Matsuyama Won?
Who was the 2021 US Ryder Cup Captain?
How many British Opens did Peter Thomson win?


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Evremar de Therouannes foi um clérigo francês medieval que exerceu temporariamente a função de Patriarca Latino de Jerusalém de 1102 a 1105. Foi também arcebispo de Cesareia, a partir de 1108.

Biografia
Após a expulsão de Dagoberto de Pisa do cargo de Patriarca de Jerusalém, em 1102, Evremar foi escolhido como substituto deste. Em 1105, porém, Dagoberto dirigiu-se a Itália, e insistiu junto do papa Pascoal II para a sua reintegração. Pascoal acabou por ceder, e Dagoberto foi renomeado patriarca. Contudo, este acabou por morrer em 1107, quando se preparava para regressar à Palestina. Apesar disto, o papa não reintegrou Evremar de imediato, pois este, como patriarca, fora bastante inactivo. Assim, o caso foi entregue a Gibelino de Sabran, nomeado núncio papal. Quando Gibelino chegou a Jerusalém, em 1108, depôs o patriarca e acabou por substituí-lo ele próprio. Evremar recebeu, como compensação, o arcebispado de Cesareia.

Patriarcas latinos de Jerusalém
Arcebispos de Cesareia

redpajama_set_name: RedPajamaWikipedia


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fou un piragüista hongarès que va competir durant les dècades de 1960 i 1970.

El 1968 va prendre part en els Jocs Olímpics d'Estiu de Ciutat de Mèxic, on va disputar dues proves del programa de piragüisme. Junt a Csaba Giczy guanyà la medalla de plata en la prova del K-2 1.000 metres, mentre que junt a Csaba Giczi, Imre Szöllősi i István Csizmadia guanyà la medalla de bronze en el K-4 1.000 metres.

En el seu palmarès també destaquen dues medalles d'or, una de plata i una de bronze al Campionat del Món en aigües tranquil·les i una d'or i dues de bronze al Campionat d'Europa.

Referències

Piragüistes hongaresos
Medallistes hongaresos als Jocs Olímpics d'estiu de 1968
Esportistes de Budapest
Morts a Budapest


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Ornex es una comuna francesa del departamento de Ain, en la región de Auvernia-Ródano-Alpes. Pertenece a la comunidad de comunas del Pays de Gex.

Geografía
Forma parte de la aglomeración urbana de Ginebra-Annemasse.

Demografía

Referencias

Enlaces externos
 INSEE
 Ayuntamiento

Localidades de Ain


Is there a basis for Human Rights?
God's existence and His revelation are necessary conditions for meaningful human rights. Christianity gives a firm foundation for human rights. Not only that, but Christianity has "the strongest possible resource for practicing sacrificial service, generosity, and peace-making. At the very heart of [Christianity's] view of reality [is] a man who died for his enemies, praying for their forgiveness. Reflection on this could only lead to a radically different way of dealing with those who [are] different from them. It [means] they [could] not act in violence and oppression toward their opponents." Of course, that doesn't mean that the ideal is always followed.
There have been Christians that have done very wicked things. There have also been many wicked things that have been done by atheists. That, however, does not mean that all atheists are bad or even that atheism is wrong. As we will see below though, atheists do not finally have any basis for morality or human rights.
Scripture, on the other hand, clearly condemns injustice. Scripture shows us that God loves justice and, conversely, hates injustice; He has compassion for those who suffer injustice—everywhere around the world; He judges and condemns those who perpetrate injustice; and He seeks active rescue for victims of injustice. Much of secular society, however, does not have a reason to condemn injustice.
2. "The American church needs to face the inevitable and prepare for the next stage of her history—we are looking at a nonwhite majority, multiethnic American Christianity in the immediate future" (p.The Next Evangelicalism, 12).
We remember that Jesus Himself was criticized by religious leaders because of the type of people that He hung out with and helped (cf. Matt. 9:9-13; 11:19; 21:31-32; Mk. 2:15-17; Lk. 3:12-14; 5:29-32; 7:36-50; 15; 19:1-10). So, we're not like the hypocritical religious leaders. Instead, we're like our Leader, the One who reaches out to heal our brokenness.
The Crash of the American Church?
Research shows that the "evangelical church" lost around 10 percent of her people in the last decade. There are many factors that are involved that have resulted in this decline. Further, most churches that are growing are just taking people from other churches, not converting people. The Great Evangelical Recession explores the factors involved in the decline of the church and offers suggestions for the future. I found the book helpful and thought-provoking.
As Christians have different beliefs regarding certain doctrines, Muslims have different beliefs as well. Christianity has many expressions, liberal and fundamental and various particular denominations. In this post (and in part two), we will explore the Islamic understanding of jihad and contrast it with Christianity. Our first observation is to realize the multifaceted nature of our exploration.
As we have briefly seen, not all Muslims are the same and not all Muslims understand jihad in the same way. So, some Muslims emphasize the more peaceful passages (e.g. surah 5:32; 2:256; Allah is also repeatedly said to be "most gracious, most merciful") and that the Qur'an seems to teach to not begin the fight (2:190; 22:39). However, others believe that those who have not confessed Allah and his prophet have already essentially made war with Muslims and should be subjugated. Some Muslims are strict adherents to Islam and some are secular. Muslims are not homogeneous. (For example, we see two very different narrative accounts in Nabeel Qureshi's, Seeking Allah, Finding Jesus and Mosab Hassan Yousef's, Son of Hamas). In fact, "not all Muslims believe that the Qurʾān is the literal and inerrant word of God, nor do all of them believe that Islam requires strict conformity to all the religious and moral precepts in the Qurʾān." We could group Muslims into three broad groups: secular Muslims, traditional Muslims, and fundamentalist Muslims.


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