text:
\section{Introduction}

The onset of massive star formation episodes in galaxies drives their
observational properties in almost any wavelength range. The UV and optical
become dominated by the continuum of massive, hot and young stars, as well as by
the presence of nebular emission lines. After a few Myr of evolution, red
supergiant stars contribute to most of the near infrared emission. The heating
of interstellar dust particles by the powerful UV photons induces the thermal
re-emission of large amounts of energy in the { mid and far infrared} domain.
The injection of ionizing photons into the surrounding gas generates thermal
radio emission, which is replaced by non-thermal emission as the ionizing power
of the burst declines and the more massive stars begin to explode as supernovae.
 The direct relation between the strength of the star formation episode and the
intensity of the different observable parameters has allowed a number of star
formation rate calibrators to be defined, such as UV continuum, emission lines
intensity, far infrared or radio luminosities
\citep{Kennicutt98,Rosa02,Bell2003}. These calibrators have proven to be
invaluable for statistical studies of the star formation history of the
Universe.

Star-forming regions are also the source of  conspicuous X-ray emission,
generated by individual stars, by the injection of large amounts of
mechanical energy heating the interstellar medium, by supernova remnants, and by
binary systems transferring mass to a compact primary \citep{Cervino02,Persic02}. All of
these individual components are in principle  directly linked to the strength of
the star formation episode, so that the X-ray luminosity could also be used as
an estimator of star formation rates ({\em SFR}).

\begin{figure*}
\begin{center}
\includegraphics[width=8 cm,bb=5 39 786 521
dpi,clip=true]{8398fi1a.eps}
\hspace{1.0 cm}
\includegraphics[width=8 cm,bb=17 39 786 527
dpi,clip=true]{8398fi1b.eps}
\end{center}
\caption{Evolution of $L_{\rm{FIR}}$\ (left) and $L_{\rm{soft X}}$\ (right) for IB (dashed line, right
axis) and EB (solid line, left axis) models. IB models predictions are
shown normalized to $1$~M$_\odot$\ of gas transformed into stars, while for EB the
luminosities are scaled  to {\em SFR}\ $= 1$ M$_\odot$\ yr$^{-1}$. $L_{\rm{FIR}}$\ has been
plotted (from top to bottom) for {\em E(B-V)}\ $= 1.0$, $0.5$ and $0.1$. $L_{\rm{soft X}}$\ has been
computed (from top to bottom) for $\epsilon_{\rm{xeff}}$\ $= 0.1$, $0.05$ and $0.01$.  }
\label{lumin}
\end{figure*}

Several authors have in recent years discussed the feasibility of using the
X-ray luminosity as an {\em SFR}\ estimator. {\citet{Fabbiano02} already concluded
from the analysis of 234 S0/a-Irr galaxies observed with {\em Einstein}, that
the correlation they found between the X-ray and the FIR luminosities in Sc-Irr
galaxies was due to the young stellar populations in these objects.}
\citet{Ranalli03} proposed an empirical calibration of the soft ($0.5$--$2.0$
keV) and hard ($2$--$10$ keV) X-ray luminosities, based on their correlation
with the far infrared (FIR) and radio luminosities, and using the known
calibrations of these parameters as proxies. \citet{Grimm03} studied the
correlation between the number of high-mass X-ray binaries (HMXB) and the {\em SFR},
deriving different calibrations of the hard X-ray luminosity for low and high
star formation rates.  \citet{Persic04} obtained a calibration of the hard X-ray
luminosity as a {\em SFR}\ estimator by assuming that most of the emission in this
range is associated with HMXB, and scaling from the number of HMXB to the {\em SFR}\
of our Galaxy. \citet{Gilfanov2004} confirmed the {calibration} of the hard
X-ray luminosity associated with HMXB, using slightly different slopes at high
and low star formation rates.  In a recent paper, \citet{Persic07} found indeed
that the collective hard X-ray emission of young point sources correlates
linearly with the star formation rate derived from the far infrared luminosity.
\citet{Strickland04b} demonstrated that the luminosity of diffuse X-ray emission
in star-forming galaxies is directly proportional to the rate of mechanical
energy injection from the young, massive stars into the interstellar medium of
the host galaxies. A similar result was found by \citet{Grimes05} from the
analysis of  a sample of starburst galaxies of different types  (from dwarf
starbursts to ultraluminous infrared galaxies), which concluded that the
mechanism producing the diffuse X-ray emission in the different types of
starbursts was powered by the mechanical energy injected by stellar winds and
supernovae into the surrounding medium.  Recently \citet{Rosa07} confirmed the
reliability of the soft X-ray luminosity as an {\em SFR}\ estimator from the analysis
of a sample of star-forming galaxies in the {\em Chandra Deep Field South} at
redshifts $ z = 0.01 - 0.67$, using the UV continuum luminosity from {\em GALEX}
as a proxy.

While hard X-ray emission from star-forming regions may be dominated by binary
systems, diffuse soft X-ray emission is generated by reprocessed, mechanical
energy from stellar winds and supernovae explosions. This mechanical energy is
related to the strength of the burst of star-formation, and can be calculated
using evolutionary population synthesis models. In this paper, we analyze the
correlation between the soft X-ray and FIR luminosities in star-forming regions,
both predicted by evolutionary synthesis models. We study the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio as a
function of the {evolutionary state, the efficiency  of the conversion of
mechanical energy into soft X-ray luminosity, the star formation history
(instantaneous or extended), and the dust abundance,} and compare the computed
values with observations taken from the literature. { Our objective is to derive
a calibration of $L_{\rm{soft X}}$\ as a tracer of the star formation rate, based on the
predictions of evolutionary synthesis models, and to  test the validity of the
empirical calibration proposed by \citet{Ranalli03}.  }

In Sect.~2 we describe the evolutionary synthesis models that we use in the present study, in Sect.~3 we
present the observational data taken from the literature, and in Sect.~4 we
discuss the predictions and the comparison with the observational values.  {\
Throughout this work we have assumed $H_{\rm0} = 73$ km s$^{-1}$ Mpc$ ^{-1}$ to
convert fluxes into luminosities.}

\begin{figure*}
\begin{center}
\includegraphics[width=8cm,bb=20 39 713 527
dpi,clip=true]{8398fi2a.eps}
\hspace{1.0 cm}
\includegraphics[width=8cm,bb=20 39 713 527
dpi,clip=true]{8398fi2b.eps}
\end{center}
\caption{Evolution of the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio computed for $\epsilon_{\rm{xeff}}$\ $= 0.01, 0.1$ and {\em E(B-V)}\ $= 0.1,  1.0$. Left: predictions for IB models; right: predictions for EB models.  }
\label{ratio}
\end{figure*}

\section{Evolutionary synthesis models}

We have computed the predicted $L_{\rm{soft X}}$\ and $L_{\rm{FIR}}$\ values using the evolutionary
population synthesis models of \citet{Cervino02} (hereafter CMHK02 models\footnote{
Downloadable from {\rm http://www.laeff.inta.es/users/mcs/SED/}}), which are
based on the models of \citet{Arnault89}, \citet{MasHesse91} and
\citet{Cervino94}. These models compute the evolution of a cluster of massive
stars, formed at the same time (Instantaneous Bursts, IB), or {during an extended
period of time (typically several tens of Myr) at a constant rate (Extended
Bursts, EB)}, assuming different metallicities and Initial Mass Function (IMF)
slopes. { The CMHK02 models were developed to compute the evolution of a
starburst during the first 30~Myr, following the onset of the star formation
episode.} Once the structure {(number of stars of each spectral type and
luminosity class at a given evolutionary time)} of the stellar population is
derived, the models are used to compute a number of observable parameters, from X-ray to radio wavelengths.

In general, we assume a solar metallicity $Z_{\sun}$, and a Salpeter IMF ($\phi(m)\sim
m^{-2.35}$) with masses ranging between $2 \, M_{\sun}$ and $120 \, M_{\sun}$. {The output of the models are normalized to the star formation rate (mass of gas
transformed into stars per unit time, $M_{\sun}  yr^{-1}$) for EB cases, or star
formation strength (mass of gas transformed into stars at the onset of the
burst, in units of $M_{\sun}$) for IB scenarios. In both cases, the mass
normalization corresponds to the mass integrated between 2 $M_{\sun}$ and 120 $M_{\sun}$
assuming a Salpeter IMF. We emphasize that this normalization might differ
significantly if other mass limits are considered. For example, the ratio
between our mass normalization ($2-120 M_{\sun}$) and the one assumed by
\citet{Kennicutt98}  ($0.1-100 M_{\sun}$) is $M_2^{120}/M_{0.1}^{100} = 0.293$.
It is important to remark that this is the normalization implicitly assumed when
the {\em SFR}\ calibrations proposed by \citet{Kennicutt98} are used.}  Under our
assumptions, the soft X-ray ($0.4$ -- $2.4$~keV) and far infrared luminosities
were computed during the first 30~Myr after the onset of the massive starburst
episode.

One of the main sources of soft X-ray emission in a star-forming region is the
diffuse gas heated by mechanical energy from a starburst (massive
stellar winds or supernova explosions) into the surrounding medium. Its
contribution  is modeled by a Raymond-Smith thermal plasma with $kT=0.5$ keV,
which controls the fraction of the mechanical energy that heats the gas to X-ray temperatures, $\epsilon_{\rm{xeff}}$.  The models include the soft X-ray
radiation emitted during the adiabatic phase of the Supernova Remnant (SNR),
which is modeled by a composite Raymond-Smith plasma with $kT=0.23$, $0.76$ and
$1.29$ keV.  The total energy emitted by the SNR, during the adiabatic phase, has
been subtracted from the energy of each supernova explosion when computing the
injection of mechanical energy.  A more detailed description of our models is provided in \citet{Cervino02}.

The contribution of the stellar atmospheres to the soft X-ray emission was
neglected because it is expected to be two orders of magnitude lower than the
emission from the diffuse gas. The contribution of high-mass X-ray binaries to
the soft X-ray emission has in addition been neglected in this work.
\citet{MasHesse99a} discussed the properties of the HMXB population expected to
form during a massive star-formation burst. Binary systems become X-ray emitters
when the primary collapses into a black hole or neutron star, the atmosphere of
the secondary has started to expand, and the secondary is sufficiently close to
the collapsed primary for mass transfer to begin. Mass is accreted onto the
surface of the compact object and emits X-rays with a typical $L_{\rm{X}}$\ $\sim
10^{38}$ erg s$^{-1}$, peaking at energies between $5$ and $10$ keV \citep{Persic02}.
{The number of HMXB in a young starburst is dependent on many free parameters.
Following \citet{MasHesse99a}, we estimate that only a few HMXB should be active
after the first 5--6 Myr of evolution of starbursts that have transformed
approximately $10^6$ M$_\odot$ of gas into stars. This HMXB population should
contribute a few times  $10^{38}$ erg s$^{-1}$ to the total X-ray luminosity,
and a small fraction of this radiation to the soft X-ray emission.} In all
cases, the total contribution of HMXB, to the soft X-ray emission, remains
$15$\% for IB and $10$\% for EB. Only if one or a few of these HMXB develop into
an ultraluminous X-ray source (ULX), with $L_{\rm{X}}$\ $\sim 10^{40}$ erg s$^{-1}$
\citep{Miniutti06}, could the X-ray emission, from soft to hard X-rays, of the
entire galaxy, be dominated by the emission of HMXB, compared to that of the
diffuse gas.

Concerning the FIR emission, a thermal equilibrium of dust is assumed, implying
that all the energy absorbed by dust, mostly originating from the UV continuum
of the  massive stars, is reemitted in the FIR range. { In this paper, $L_{\rm{FIR}}$\
refers to the total mid- and far-infrared luminosity integrated over the
wavelength range $1 -1000 ~\mu$m. We remark that this parametrization of $L_{\rm{FIR}}$\
implies a value of $L_{\rm{FIR}}$\ that is larger than that calculated using the FIR
parameter proposed by \citet{Helou88}, which is widely used in the literature.
\citet{Helou88} showed that the FIR luminosity computed from the {\em IRAS}
fluxes at $60$ and $100$ ~$\mu$m would intercept about 70\% (0.15 dex) of the
total FIR luminosity from 1 to 1000 $\mu$m, assuming that there is a single,
dominating component, at a temperature of 30 to 50 K.  The discrepancy would be
even larger in the presence of an additional warm dust component. This estimate
of $L_{\rm{FIR}}$\ is consistent with the range  ($8 -1000 ~\mu$m) considered by
\citet{Kennicutt98} for the calibration of $L_{\rm{FIR}}$\ as an {\em SFR}\ estimator, since
most of the FIR luminosity in starburst galaxies is emitted at wavelengths in
the range $10 -120 ~\mu$m. The models apply a Galactic extinction law
\citep{Cardelli89} to the synthetic spectral energy distributions, which is
parametrized by the colour excess {\em E(B-V)}. The energy absorbed due to extinction is
calculated using the models. It is assumed that all energy absorbed is reemitted
thermally by the dust, within the mid to far infrared domain, i.e., within the
$\sim$ $8-1000 ~\mu$m range. The models do not predict the shape of the FIR
emission, since we do not make any assumption about the expected dust
temperature. The presence of completely-obscured stars is not taken into
account. Furthermore, the models assume that a fraction $1-f$ of Lyman continuum
photons is directly absorbed by the dust, and does not contribute to the
ionization (see \citet{Mezger1974}). {\citet{Mezger1978} for the Galactic and
\citet{Degioia1992} for the Large Magellanic Cloud HII regions, derived $1-f$
values in the range $0.3-0.4$.} We have assumed $(1-f)=0.3$ in this work, as
proposed for starburst galaxies by \citet{Belfort1987}. }

The evolution of both $L_{\rm{FIR}}$\ and $L_{\rm{soft X}}$\ predicted by the models are shown in
Fig.~\ref{lumin}, while their ratio $L_{\rm{soft X}}/L_{\rm{FIR}}$\ is presented in Fig.~\ref{ratio}. For
IB models, the luminosities are shown scaled to $1$~M$_\odot$\ of gas transformed into
stars at the onset of the starburst.  In the case of EB models, the luminosities
are normalized to  {\em SFR}\ = $1 \, M_{\sun} \, yr^{-1}$. $L_{\rm{FIR}}$\ is presented in the
plot, computed for {\em E(B-V)}\ $= 0.1$, $0.5$ and $1.0$. It can be seen that FIR
emission saturates rapidly for {\em E(B-V)}\ values {above $0.5$.}  In the remainder of this work, we consider the value of $L_{\rm{FIR}}$\ calculated by assuming that {\em E(B-V)}\ $=
1.0$, which can be considered an upper limit to the expected FIR luminosity.
In the case of EB models, $L_{\rm{FIR}}$\ reaches an
asymptotic value after approximately $10 - 15$~Myr of evolution, when an equilibrium is
reached between the number of massive stars that die, and those forming
continuously. For coeval starbursts, $L_{\rm{FIR}}$\ declines rapidly after the
first $5$~Myr of evolution, when the most massive stars begin to end their
lifetimes and stop heating the interstellar dust.

\begin{figure}
\centering
\includegraphics[width=8cm,bb=20 39 713 527 dpi,clip=true]
  {8398fi3.eps}
\caption{{ Evolution of the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio as a function of metallicity and star
formation regime. {\em E(B-V)}$ =1.0$ and $\epsilon_{\rm{xeff}}$\ $=0.05$.}}
\label{ratio-met}
\end{figure}

$L_{\rm{soft X}}$\ is shown in Fig.~\ref{lumin} computed for $\epsilon_{\rm{xeff}}$\ values of $1$\%, $5$\%
and $10$\%. During the first few Myr, there is a rapid increase in $L_{\rm{soft X}}$\ because
both the luminosity and the stellar winds of the most massive stars, increase. After the first $3$~Myr of evolution, the most massive stars end
their lifetimes and explode as supernovae. The injection of mechanical energy
begins to be dominated by energy released by supernovae explosions, as the
importance of stellar winds rapidly diminishes. { During the first 35 Myr, this
remains the situation for IB models because, for a Salpeter IMF, the supernovae
rate declines slowly, while there exist stars of sufficient mass (of initial mass
above $8$~M$_\odot$) to produce supernovae \citep{Cervino94,Leitherer95}. In the
case of EB models, $L_{\rm{soft X}}$\ is expected to increase slowly after the first 5~Myr,
until an equilibrium is reached between the formation and destruction of stars
that end their lifes as supernovae, i.e., at around $40$~Myr at solar
metallicities, according to the evolutionary tracks considered.
\citet{Leitherer95} presented the evolution of both supernova rate and the
injection rate of mechanical energy for longer term evolution, up to ages of
300~Myr. Their Fig.~56 showed that the asymptotic rate of energy injection is
within 0.05 dex of the value predicted at 30~Myr}. Although the computation of
the soft X-ray luminosities in the CMHK02 models is simplistic, the
predictions are in good agreement with the results of \citet{Strickland99},
which were computed using hydrodynamical simulations of a young superbubble
driven by a cluster of massive stars.

\begin{figure}
\centering
\includegraphics[width=7cm,bb=50 34 705 521 dpi,clip=true]
  {8398fi4.eps}
\caption{$L_{\rm{soft X}}/L_{\rm{FIR}}$\ histograms for the samples of star-forming galaxies from
\citet{Ranalli03} (dashed line), \citet{Tullmann06b} (thick solid line) and
\citet{Rosa07} (thin solid line). { The bins have been computed with a slight
shift between each other for clarity.} }
\label{histo}
\end{figure}

Figure~\ref{ratio} shows the predictions for the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio evolution
with time.  It can be seen that $L_{\rm{soft X}}/L_{\rm{FIR}}$\ increases continuously with time after an
instantaneous burst, even after the first $5$~Myr, due to the fact that $L_{\rm{soft X}}$\
remains almost constant while $L_{\rm{FIR}}$\ decreases rapidly.  In extended burst
models, {the rate of increase of $L_{\rm{soft X}}/L_{\rm{FIR}}$\ with time,} after the first $5$~Myr, is smaller. As
discussed above,  we expect the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio to stabilize after about $40$ Myr
in EB models, when an equilibrium between formation and destruction of stars
susceptible to becoming supernovae, has been reached.  In both cases, there is a
rapid increase in the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio after the onset of the burst (one order of
magnitude in $3$~Myr in IB models), associated with the rapid increase in the
amount of mechanical energy injected during the first phase of the evolution of
the most massive stars.

{ In Fig.~\ref{ratio-met}, we plot the evolution of the $L_{\rm{soft X}}/L_{\rm{FIR}}$\
ratio as a function of metallicity ($Z = Z_\odot$ and  $Z = 0.4\times Z_\odot$)
and star formation history (instantaneous and extended bursts). Varying metallicity highlights two results: first, low-metallicity stars evolve more slowly and
have a longer lifetime, such that the evolution of $L_{\rm{FIR}}$\ is delayed with respect
to solar-metallicity stars. Second, the lower the metallicity, the less
efficient are the stellar winds, and therefore the lower is the amount of mechanical
energy released into the interstellar medium. As seen in Fig.~\ref{ratio-met}, the net
effect is a decrease in the value of $L_{\rm{soft X}}/L_{\rm{FIR}}$\, at intermediate ages by 0.2 dex, or by up to 0.5 dex within the first 4 Myr of evolution. At some ages, the trend is even reversed. For the time interval considered, however, the predicted values of $L_{\rm{soft X}}/L_{\rm{FIR}}$\ are similar for both values of metallicity.  }

\begin{figure}[ht]
\centering
\includegraphics[width=8cm, bb= 19 39 705 565
dpi,clip=true]{8398fi5.eps}
\caption{$L_{\rm{soft X}}/L_{\rm{FIR}}$\ histogram for the combined sample, over the evolution of
the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ computed for IB (dashed lines) and EB (solid lines) and $\epsilon_{\rm{xeff}}$\ $=
0.10$ (top) and $0.01$ (bottom). The horizontal line corresponds to the mean
ratio of the complete sample, $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ $= -3.92$.}
\label{sxf-histo}
\end{figure}

\section{Observational data sample}

We have compiled $L_{\rm{soft X}}$\ and $L_{\rm{FIR}}$\ data for 62 star-forming galaxies, of
different types and redshifts, to compare with our model predictions.

{The data compilation of \citet{Ranalli03} (hereafter RCS03) is for star-forming
galaxies, from the atlas of \citet{Ho97}, that have detectable X-ray emission in
ASCA and/or BeppoSAX observations. Only spiral and irregular galaxies from Sa to
later types were included in this sample, which was complemented by the authors
with data of six, well-known starburst galaxies observed in the southern
hemisphere.}

The sample compiled by \citet{Tullmann06b} (hereafter TUL06) is based on the nine
late-type starburst galaxies of \citet{Tullmann06a} ({\em XMM-Newton} data),
seven star-forming disk galaxies from \citet{Strickland04a} ({\em Chandra} data)
and seven additional late-type star-forming galaxies taken from the literature.
The contribution by obvious point-sources within the extraction regions was
removed from all objects in the original \citet{Tullmann06a} and
\citet{Strickland04a} compilations when possible.

{ In both samples, the X-ray emission was corrected for Galactic neutral
Hydrogen absorption, but not for the intrinsic absorption of the galaxies. The
published far-infrared fluxes  were computed using the {\em IRAS} 60 and 100
$\mu$m flux following the procedure of \citet{Helou88}, corresponding to the energy emitted
within the range $40 - 120 ~\mu$m. \citet{Calzetti2000} found for local starburst galaxies that $F(1-1000)/F(40-120) = 1.75 \pm 0.25$. We have
therefore multiplied the FIR fluxes provided by RCS03 and
TUL06 by 1.75, in order to obtain a more realistic determination of
the total amount of energy being reemitted in the mid- and far- infrared range.
The luminosities were recomputed for all objects from the published  fluxes
by using the distances corrected to the Local Group reference frame as given in
the {\em Nasa Extragalactic Database} , assuming   $H_{\rm0} = 73$ km s$^{-1}$
Mpc$ ^{-1}$.

There is some overlap between the two samples. The $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio for M82 is
$-4.08$ in RCS03 (based on {\em BeppoSAX} data) and $-3.85$ for
TUL06 ({\em Chandra}).  For NGC~4631 $L_{\rm{soft X}}/L_{\rm{FIR}}$\ varies between $-3.96$
({\em ASCA}) and $-4.17$ ({\em XMM-Newton}), respectively. In these cases we
have taken the $L_{\rm{soft X}}$\ values provided by  TUL06 . }

To compare with star-forming galaxies outside the Local Universe, we consider
galaxies at redshifts $ z = 0.01 - 0.67$ studied by \citet{Rosa07} (hereafter
ROSA07). Both $L_{\rm{soft X}}$\ and $L_{\rm{FIR}}$\ data are available for these galaxies, which were
observed as part of the Chandra Deep Field South (CDFS) survey. The X-ray data
in this sample come from the catalog of \citet{Alexander03}, and were not
corrected for either Galactic or intrinsic absorption by neutral hydrogen.
Nevertheless, along the line of sight to the {\em CDFS} the expected Galactic
neutral hydrogen absorption in the soft X-rays band is only 4.2\% (0.02
dex) \citep{Alexander03}. { We exclude objects believed to harbour an obscured
AGN, or to be dominated by low-mass, X-ray binaries (LMXB). In total, we have
identified 18 objects with detectable soft X-ray, and far-infrared fluxes that
appear not to be contaminated by either an AGN or LMXB. }

ROSA07 derived the far infrared luminosities for these objects in the
full 8 -- 1000 $\mu$m band using Spitzer observations at 25 $\mu$m. They used the
empirical calibration of \citet{Takeuchi05} {based on the analysis of a
large sample of galaxies for which fluxes in the four {\em IRAS} bands at 12,
25, 60 and 100 $\mu$m were available.  The FIR luminosity computed in this way
should be consistent with the luminosities derived for the RCS03
 and TUL06 samples, extrapolated to the 1 -- 1000 $\mu$m range.
ROSA07 assumed   $H_{\rm0} = 70$ km s$^{-1}$ Mpc$ ^{-1}$ to convert
fluxes into luminosities. }

We note that the $L_{\rm{soft X}}$\ values are integrated over the $0.5 - 2.0$ keV band by
RCS03,   $0.2 - 2.0$ by ROSA07, and over the $0.3 -
2.0$ keV band by TUL06, while the model predictions were computed
for the $0.4 - 2.4$ keV band. We have verified that for the typical spectral
properties of the diffuse gas in these objects, the discrepancies associated with
the different bandwidths should be smaller than $9$\% ($0.04$ dex) in any case.

We have plotted in Fig.~\ref{histo} the histograms of the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ distribution
for each sample. It can be seen that while there is a significant overlap
between them, the star-forming galaxies compiled by RCS03 show the
smallest dispersion. The TUL06 galaxies show generally lower $L_{\rm{soft X}}/L_{\rm{FIR}}$\
values than the objects compiled by RCS03, while the sample of
ROSA07 presents the highest $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratios. The mean $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\
values derived for each sample are $-3.94$ (0.27) (RCS03), $-4.34$
(0.48) (TUL06), $-3.37$ (0.45) (ROSA07) and $-3.92$
(0.57)  for the whole compilation. Values within parentheses correspond to the
$\sigma$ dispersion of each sample. { We have looked for any possible
correlation between the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratios in the TUL06 galaxies and
their morphological type,  but there is no clear trend. Both Sc+Sd and SB galaxies in the sample cover a wide range of luminosities and $L_{\rm{soft X}}/L_{\rm{FIR}}$\
values and furthermore, they cover a similar range in luminosities than the
galaxies in the RCS03 sample. There is no obvious reason for the
differences between the two samples of local star-forming galaxies.  }

\section{Discussion}

Figure~\ref{ratio} indicates that our models predict a strong dependence of the $L_{\rm{soft X}}/L_{\rm{FIR}}$\
ratio on the star formation history (instantaneous or extended), and on the
evolutionary state of the star formation process. Moreover, the ratio is also
strongly dependent on the efficiency of the reprocessing of mechanical energy
and UV photons into soft X-ray and FIR emission, respectively. Therefore, we
would expect a significant scatter in the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ values observed in star-forming
galaxies. This is indeed what we find in Fig.~\ref{histo}, as discussed above.

\begin{figure*}
\begin{center}
\includegraphics[width=8 cm,bb=18 22 705 527
dpi,clip=true]{8398fi6a.eps}
\hspace{1.0 cm}
\includegraphics[width=8 cm,bb=18 22 705 527
dpi,clip=true]{8398fi6b.eps}
\end{center}
\caption{$L_{\rm{soft X}}$\ vs. $L_{\rm{FIR}}$\ for the RCS03 (squares),
TUL06 (triangles) and ROSA07 (circles) samples.
In the left panel  we have
overplotted the correlation lines corresponding to the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratios predicted
by IB models for different ages and $\epsilon_{\rm{xeff}}$\ values.  The right panel shows the
corresponding predictions for EB models.}
\label{mcorr}
\end{figure*}

\citet{MasHesse99b} showed that the star formation episodes taking place in
{ compact} starburst or HII galaxies are generally of short duration, and that
their properties can be better reproduced by evolutionary synthesis models
assuming (nearly) instantaneous bursts, than by long-lasting, extended-in-time, star-formation processes. The generally strong optical emission lines in these
galaxies constrain the evolutionary state of their massive star-formation
episodes to ages below $6$ Myr, { typically within $4-5$ Myr.} On the
other hand, star formation is expected to proceed during long periods of time in
the disks of late-type spiral galaxies, generally in the form of individual
bursts at different times.  The accumulation of individual starburst episodes
along the disks of these galaxies mimick a continuous star formation process
\citep{MasHesse99b}, so that extended star formation models might be a better
approximation to reproduce their spatially-integrated properties.

In Fig.~\ref{sxf-histo}, we have added to the predictions of the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ values
the histogram corresponding to the whole sample, as well as the average
observational $L_{\rm{soft X}}/L_{\rm{FIR}}$\ value. As discussed above, there is a degeneracy between
$\epsilon_{\rm{xeff}}$\ and the age of the star formation episode, so that it is not possible to
discriminate between both parameters without additional constraints on the
evolutionary state.  { Apart from a few irregular galaxies, for which an instantaneous
model would describe better the star-formation episodes they are hosting, most
of the galaxies in the sample are large spiral galaxies experiencing long-term
star formation. Figure 5 shows that the mean $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio can be reproduced by
relatively young EB models (after about 10 Myr of evolution) with moderate
efficiencies   $\epsilon_{\rm{xeff}}$\  of about $1$\%. Galaxies with higher  $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratios would
correspond to more evolved extended starbursts reaching the evolutionary
asymptotic  phase, with  $\epsilon_{\rm{xeff}}$\ in most cases below $10$\%.  On the other hand,
the galaxies with lower $L_{\rm{soft X}}/L_{\rm{FIR}}$\ values can only be reproduced by very young
models, after less than 10~Myr of evolution. The galaxies in the sample have been
selected in the various compilations for being {\em star-forming} or {\em
starburst} galaxies, i.e., galaxies experiencing a stronger than average episode
of star formation.  The integrated emission in the far infrared and soft X-ray
bands of some of these galaxies could be dominated  by a single but intense
burst of star formation. { While star formation proceeds in these objects for a
long time, these individual, intense bursts are not expected to last longer than
a few Myr.} Some of these starbursts could indeed be rather unevolved. We believe
that this is what we see in Fig.~\ref{sxf-histo}: some of the galaxies with low
$L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratios could be dominated by a single, intense and relatively unevolved
burst of star formation. A deeper study of the individual galaxies would be
required to confirm this hypothesis, but it is beyond the scope of this work.

\citet{Grimes05} computed the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratios for a sample of
ultraluminous infrared, starburst and dwarf starburst galaxies (the galaxies
classified as starburst are already included in the  TUL06
sample).  For their 7 dwarf starburst galaxies (2 are already included in the
sample by RCS03), they derived a mean  $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ of $-4.0$, close
to the average value found for our complete compilation. The $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio of
these galaxies (within the range $-3.58$ to $-4.29$) is properly reproduced by
IB models at approximately $4-5$ Myr, with $\epsilon_{\rm{xeff}}$\ within a realistic range  $1-5$\%
\citep{Strickland99,Summers01,Summers04}.  The mean $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ value of the 9
ultraluminous infrared galaxies (ULIRG) in their sample is $-4.5$, clearly below
our average.  This indicates that the star formation processes in this kind of
galaxy might be relatively unevolved and their emission dominated by a
single, intense episode of star formation. }

In Figure~\ref{mcorr}, we plot the observational $L_{\rm{soft X}}$\ vs. $L_{\rm{FIR}}$\ values
for the galaxies in the three samples. We include the predictions of
IB and EB models at different ages, and for $\epsilon_{\rm{xeff}}$\ values between $1$ and $10$\%.
{ These plots support the main points of our previous discussion: the observational $L_{\rm{soft X}}$\ vs.
$L_{\rm{FIR}}$\ correlation in star-forming galaxies can be well-reproduced by
evolutionary synthesis models, assuming realistic parameters: age below 6 Myr for
IB cases, and a spread of young to evolved bursts for EB models,  a high
efficiency in the reprocessing of UV photons into far infrared emission, and a
moderate ($1-10$\%)  efficiency in the heating of the diffuse interstellar
gas by the mechanical energy released by massive stellar winds. }

We have analyzed the effect of some intrinsic properties of the sampled objects,
on the dispersion shown in the correlation plots. First, as noted above, the
measured $L_{\rm{soft X}}$\ values did not include the correction for intrinsic neutral
hydrogen absorption. \citet{Kunth98} measured the column density of neutral
hydrogen in the line of sight to $8$ compact starburst galaxies, by fitting
their $Lyman\,  \alpha$ profiles, finding values in the range  $log(n_H) \sim
19 - 21$ cm$^{-2}$. We have computed that for the typical spectral properties of
the hot diffuse gas this correction would be within $0.4$\% -- $50$\% (i.e.
$<0.18$ dex). { A second effect would be the contamination of
the soft X-ray emission by low mass X-ray binaries associated to the underlying,
older stellar population. ROSA07 estimated that the contribution by LMXB
in their sample of spiral star-forming galaxies was generally of few percent,
and concluded that the contamination should be negligible for galaxies with
{\em SFR}\ $ > 1 \, M_{\sun} \, yr^{-1}$. In the RCS03 sample only 7
objects have a value of {\em SFR}\ below  $1 \, M_{\sun} \, yr^{-1}$, but their average $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\
is $-3.7$ (in any case  within $-4.2$ to $-3.2$), i.e., with no deviation at all
from the total average $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio. Therefore, the contamination of $L_{\rm{soft X}}$\ by
LMXB does not seem to be important. Finally, TUL06 removed the
contamination by point sources before computing the integrated $L_{\rm{soft X}}$, so that the
contamination of this sample by LMXB should be negligible. An additional effect
is related to the relative strength of the starburst emission compared to the
galaxy as a whole. While the soft X-ray emission would be associated mostly with
the starburst regions, the far infrared luminosity can include a significant
contribution from the rest of the galaxy, so that the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratios obtained
from spatially-integrated measurements would be lower than the intrinsic value
produced by the starburst itself.  A detailed morphological analysis of the
galaxies in the sample is out of the scope of this paper, but we expect that at
least in some cases the observational $L_{\rm{soft X}}/L_{\rm{FIR}}$\ value might be contaminated by
emission not related to the star formation episode.}

Finally, $L_{\rm{FIR}}$\ has been computed assuming almost complete reprocessing of UV
stellar continuum photons ({\em E(B-V)}\ $= 1$), as discussed in Sect.~2. {Lower
values of the extinction, of the order of {\em E(B-V)}\ $= 0.1$, would raise the predicted $L_{\rm{soft X}}/L_{\rm{FIR}}$\
ratios by up to $0.15$ dex.} The effective extinction of these objects should be
in between both extreme values {of {\em E(B-V)}.} In conclusion, correcting the soft X-ray
luminosity from intrinsic photoelectric absorption and/or rejecting the far
infrared emission not associated with the starburst regions themselves, could
increase the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratios for some objects. On the other hand, smaller interstellar extinction values would increase the
predicted $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio by less than $40$\%.

We consider if it is possible to derive a calibration that would allow the $L_{\rm{soft X}}$\ luminosity to be used as a tracer of SFR. \citet{Strickland99} found from detailed hydrodynamical
simulations that superbubbles accelerated by the release of mechanical energy in
a starburst, would convert on average approximately $5$\% of the input mechanical energy
into soft X-ray emission. \citet{Summers01} analyzed Mrk~33, a dwarf
star-forming  galaxy, and concluded that it is dominated by an intense burst
$5$--$6$ Myr old, and that the rate of injection of mechanical energy from the
starburst is approximately $1.2\times10^{41}$ erg s$^{-1}$. The soft X-ray luminosity of the
central, extended diffuse gas derived by these authors is   $L_{\rm{soft
X}}\sim 2.2\times 10^{39}$ erg s$^{-1}$, corresponding to $\epsilon_{\rm{xeff}}$\ $\sim 0.018$.
Similarly, \citet{Summers04} estimated the mechanical energy injection rate from
the starburst in NGC~5253 to be $L_{\rm{mech}} = 3.6\times10^{40}$ erg s$^{-1}$. The
measured thermal X-ray emission associated with the starburst was $L_{\rm{soft X}}$\ $\sim
4\times10^{38}$ erg s$^{-1}$, yielding $\epsilon_{\rm{xeff}}$\ $\sim 0.01$.

{ We can therefore assume that  $\epsilon_{\rm{xeff}}$\ is constrained to be in the range
$1-5$\% for typical star-forming galaxies. Our evolutionary synthesis models
predict for  Instantaneous Bursts (of age between $3-6$ Myr) that $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ is approximately equal to $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ $\sim (-3.1, -4.0)$, with a central value
$log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ $\sim -3.5$. On the other hand, Extended Burst models predict
$log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ $\sim (-3.0, -3.4)$ after $30$ Myr of evolution, when the number of
supernova explosions begins to stabilize.  For less-evolved, extended episodes
(of approximately 10 Myr of continuous star formation) the predicted ratios would be
lower, within the range $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ $\sim (-3.5, -4.0)$.

These values are close to the average ratio $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ $\sim -3.92$ derived from
our total  sample of star-forming galaxies, supporting the use of the soft X-ray
emission  as a tracer of the star formation rate in starburst galaxies. Using
the $L_{\rm{soft X}}$\ values predicted by the models, as shown in Fig.~\ref{lumin}, we can
derive the calibration of the star formation rate (or strength) as a function of
$L_{\rm{soft X}}$. For this we have considered the points at which  $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ $= -3.5$ for IB
models, $log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ $= -3.1$ for EB cases in the asymptotic phase of evolution, and
$log(L_{\rm{soft X}}/L_{\rm{FIR}})$\ $= -3.7$ for extended, but non-evolved bursts, with ages of approximately 10~Myr,
according to the discussion above. The calibrations would therefore be:

\vspace{0.2cm}
\centerline  { {\em SFR}\  (M$_{\sun}$  yr$^{-1})  =  2\times 10^{-41}$  $L_{\rm{soft X}}$\ (erg s$^{-1}$)  (evolved EB)}
 \vspace{0.2cm}

\centerline  { {\em SFR}\  (M$_{\sun}$  yr$^{-1})  =  8\times 10^{-41}$  $L_{\rm{soft X}}$\ (erg s$^{-1}$)  (young EB) }
\vspace{0.2cm}

\noindent For comparison,  the semiempirical calibration derived by
\citet{Ranalli03}  is

\vspace{0.2cm}
\centerline  { {\em SFR}\  (M$_{\sun}$  yr$^{-1})  =  1.1\times 10^{-40}$  $L_{\rm{soft X}}$\ (erg s$^{-1}$) }
\vspace{0.2cm}

\noindent where we have  adapted the original calibration to the whole FIR
emission in the $1-1000 ~\mu$m band, to be consistent with  \citet{Kennicutt98}
(whose $L_{\rm{FIR}}$\ calibration is used as a proxy), and have scaled the original
\citet{Kennicutt98} mass normalization to the range $2-120 M_{\sun}$ to be
directly comparable with our results.

\noindent These calibrations should be applicable, within the range of validity
shown in Fig.~\ref{lumin}, for galaxies experiencing an extended episode of
star formation at a constant star formation rate. In the case of coeval, instantaneous
starbursts, the parameterization would be:

\vspace{0.2cm}
\centerline  { {\em SFS}\  (M$_{\sun}$)$  =  2\times 10^{-34}$  $L_{\rm{soft X}}$\ (erg s$^{-1}$) }
\vspace{0.2cm}

\noindent where the star formation strength ($SFS$) is the total mass
transformed into stars at the onset of the burst.

The semiempirical calibration proposed  by \citet{Ranalli03} is therefore in
good agreement with the calibration derived from synthesis models for relatively
unevolved star formation episodes, but it would tend to overestimate the star
formation rate for galaxies that have been forming massive stars over a long time, for example tens or hundreds of millions of years.

The models do not in principle predict any dependence of the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratios
on the strength (i.e. total luminosity) of the star formation episodes, as
proposed by some authors for the hard X-ray luminosity. Nevertheless, we want
to remark that our models do not study the detailed properties of the
medium surrounding the star-forming regions. The intensity of the star-formation episode could, for example, have a direct effect on the dust-grain properties of the interstellar medium. $\epsilon_{\rm{xeff}}$\ may, in addition, be a function of the burst intensity. Both effects could create a correlation between $L_{\rm{soft X}}/L_{\rm{FIR}}$\ and the star-formation burst intensity, although such a correlation is unclear in Fig.~\ref{mcorr}. }

\section{Conclusions}

 We have compared the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ values measured in a sample of  62 star-forming
galaxies with the predictions by our evolutionary synthesis models,  aiming to
analyze the validity of  semiempirical and theoretical calibrations of $L_{\rm{soft X}}$\ as a star
formation rate estimator. The main results can be summarized as follows:

   \begin{enumerate}

\item The $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratios are strongly dependent on the efficiency in the
conversion of the mechanical energy released by the young massive starburst into
soft X-ray luminosity, by interaction of the stellar winds and supernova ejecta
with the surrounding interstellar medium. From theoretical predictions and
observational data, we expect an $\epsilon_{\rm{xeff}}$\ value of few percent in starburst
galaxies.

\item $L_{\rm{soft X}}/L_{\rm{FIR}}$\ is also dependent on the evolutionary status of the star
formation episode. It increases rapidly with time during the first $5$ Myr of
evolution of a massive starburst, and shows a slower increase afterwards. After
a (nearly) instantaneous burst of star formation, $L_{\rm{soft X}}$\ decreases slower than
$L_{\rm{FIR}}$, as long as there remains a population of massive stars able to collapse
as supernovae (up to around 35~Myr).

\item When star formation proceeds at a nearly constant rate during
extended periods of time, the $L_{\rm{soft X}}/L_{\rm{FIR}}$\ ratio is expected to stabilize after around
$40$ Myr, when the number of massive stars that produce supernovae has
reached an equilibrium between death and birth of new stars.

{
\item The $L_{\rm{soft X}}/L_{\rm{FIR}}$\ values measured for the sample of star-forming galaxies are
consistent with the predictions by the models under realistic conditions:
relatively young and unevolved  star formation  episodes and $\epsilon_{\rm{xeff}}$\ values
within $1$--$10$\%.

\item A calibration of $L_{\rm{soft X}}$\ as a star formation rate estimator, based on the
predictions of evolutionary synthesis models, has been derived. The calibration
proposed by  \citet{Ranalli03} is consistent with the predictions for
relatively unevolved, time-extended bursts of star formation.
}
\end{enumerate}

\begin{acknowledgements}

JMMH and HO are partially funded by Spanish MEC grants AYA2004-08260-C03-03 and
ESP2005-07714-C03-03. OH is funded by Spanish FPI grant BES-2006-13489. MCS
acknowledges funding by Spanish MEC grant AYA2004-02703, and by Spanish {\em
Ram\'on y Cajal} fellowship El 01/08/2007.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


text:
Haitian migrants thought Biden would welcome them. Now deported to Haiti, they have one mission: Leave again.
Fegenson Elie on Sept. 27 at the boardinghouse where he and his family are staying in Port-au-Prince, Haiti. (Ralph Tedy Erol for The Washington Post)
By Widlore Mérancourt
Anthony Faiola
Arelis R. Hernández
October 1, 2021 at 4:18 p.m. EDT
PORT-AU-PRINCE, Haiti — As Haitians living in Brazil, Fegenson Elie and his family were struggling when he received a phone call from his sister-in-law. She had recently joined thousands of migrants — including many families with children — who had successfully crossed the U.S. border.
Month by month, the Biden administration had been allowing an increasing number of Haitians to enter the country, which allowed them to make asylum claims, and expelling far fewer on pandemic-era public health grounds. Elie's sister-in-law, taking advantage of the easing policy, was establishing a new life in Florida with her husband and child — and beckoning the Elies to follow.
"She told me people with children won't have a problem, because it had been easy for them," said Elie, 33.
He emptied the family's life savings and joined the surge of Haitians migrating from the South American nations where many settled years ago. But after a dangerous odyssey to Texas — and as pressure mounted on the Biden administration over a burgeoning migrant camp near the border — Elie and his family were apprehended by U.S. agents and summarily deported to a country they had not seen in years.
"Biden called us," Elie said. Then, "Biden betrayed us."
Deportees land in Port-au-Prince: 'Nobody told us we were going back to Haiti'
Now bankrupt and desperate, the Elies are far worse off than when they started — scrambling to find a way out of their homeland, an unstable and dangerous country they had previously escaped and never wanted to return to.
On a recent afternoon, Elie stood at the gates to the Port-au-Prince airport, his 3-year- old son clinging to him, his wife nervously holding their 1-year old daughter. They wore their only possessions — the clothes they had landed in two days earlier after being forced onto a U.S. deportation flight.
Elie begged the guards to let them into the airport. Their bags, which held their IDs as well as their children's Brazilian birth certificates, had been missing since their flight here. He needed to find them to have any hope of leaving again.
The sooner they can leave, he said, the better. The sound of gunfire outside their cheap boardinghouse makes their children cry. In a nation with the world's highest per-capita kidnapping rate, rumors are rife that the deportees have bales of cash.
The airport guard shook his head: No entry.
"This country is hell," Elie said back in the small, dingy room at the boardinghouse where the family has been staying. "We need to leave."
The Biden administration continues to send thousands of Haitians back to the hemisphere's poorest country to break up a surge in migration that some say it might unwittingly have fueled.
Interviews with nearly three dozen Haitian migrants in Haiti, Texas and Mexico indicated that virtually all expected to be granted entry to the United States. Rumors and incomplete information about asylum and relief, spurred at least in part by the administration's inconsistent application of border policies, reached them through messaging apps, social media and phone calls.
Haiti buries a president, but its long-term crises live on
The Biden administration has used Title 42 — a public health policy embraced by the Trump administration during the coronavirus pandemic — to summarily expel the Haitians before they can file asylum claims. The expulsions are happening without systematic coronavirus testing; six deportees have tested positive for the coronavirus in Haiti, according to the International Organization for Migration.
But the deportations come after months in which the policy was unevenly applied. From January to August, as the number of migrants crossing the border climbed, the percentage ejected under Title 42 fell from 82 percent to 45 percent. For Haitians, the drop was steeper: 55 percent to 8 percent.
By July, a majority of migrants were being processed under Title 8, which allows them to request asylum. Although migrants processed under Title 8 may also face expedited deportation, most families with children were being released into the United States.
The numbers suggest the improving success rate for entering the United States might have encouraged more migration. During the first seven months of the Biden administration, from February through August, 92 percent of Haitian migrants — or 24,707 people — were processed in ways that granted them access to asylum claims. That compares with 44 percent — or 1,641 people — during the last seven months of the Trump administration, when the majority were rapidly expelled under Title 42.
The treatment of Haitians in recent months has been roughly on par with that of migrants from other, more distant countries, such as Brazil. But it contrasts sharply with, say, Mexican migrants — a far larger percentage of whom have been immediately expelled by the Biden administration.
The Department of Homeland Security did not respond to a request for an explanation. Analysts attribute the disparity at least in part to the relative ease in returning Mexicans back to their home country.
The Biden administration's decision to grant temporary protection to undocumented Haitians living in the United States might also have encouraged migration. The policy was announced in May and finalized in August. Eligibility was limited to migrants who had arrived in the country by July 29.
"I think when there is a confusing policy landscape at the border," said Jessica Bolter, associate policy analyst for the Migration Policy Institute, "when there are instances of people getting through despite the messaging coming out of the administration, and then those people pass on word through their social networks, then it can certainly create a draw for more migration at the border."
What happens next in Haiti?
A White House official disputed claims that the administration's policies were unclear or had encouraged migration.
"We've been clear from even before President Biden took office that migrants should not irregularly try to enter the United States, and those attempting to enter will be subject to border restrictions," the official said in a statement to The Washington Post, commenting on the condition of anonymity under protocols set by the White House. "Currently, the administration continues to enforce Title 42 and expel people with this authority when possible, and those who cannot be expelled are placed into immigration proceedings. There are a number of operational capacity constraints in place that determine whether an individual is able to be expelled or not."
Most of the Haitians massing at the U.S.-Mexico border had fled to South America after the 2010 earthquake, which killed more than 220,000 people. Many had settled in Chile or Brazil, countries where they say they faced obstacles to legalization, rising discrimination and a severe job-market downturn due to the pandemic.
It is clear that not all migrants who tried to enter the United States were successful. But interviews with Haitian migrants suggested that the number who succeeded was great enough to inspire an exodus.
"Why did this happen to us?" asked Marinise Cédieu Sinaus, 38, deported to Haiti this week with her husband and 3-year-old son. "Lots of people were getting into the U.S. without any problem whatsoever." Her son, she said, had barely eaten during their five-day detention in Texas and required hospitalization in Haiti.
"My husband has a sister in the U.S. who would have received us," she said. "I did not decide to come to Haiti. I do not have a house here. I don't have anything here. I want to go back to Chile where I worked at a supermarket."
Elen Pierre, 28, lived in Brazil and later Chile with his partner and daughter before getting stranded in Mexico while trying to come to the United States.
"You learn from the one who came before you, and they pass it on to the next person," he said. "It could be a brother, a cousin or a friend. They tell you what to expect, what to avoid and where the police are on the journey. When they make it through, they tell you who will help and what to say. You expect to make it, too."
"We were expecting the United States to accept us with open arms," Pierre said. "That's what we were told."
Deportations have left thousands stranded in a country shattered by violence and rocked by political instability after an unsolved presidential assassination. An earthquake in August killed more than 2,200 people and left tens of thousands homeless.
In Haiti, a brutal reckoning over an all too familiar task: Rebuilding
The converging crises have sparked a fresh wave of Haitian migration. Hundreds have departed by boat in recent weeks, only to be intercepted and turned back by U.S., Bahamian and other authorities. On Thursday, four U.N. agencies called on governments to refrain from expelling Haitian migrants "without proper assessment of their individual protection needs."
"Our fear is that the [new deportees] will put themselves at high risk and try leave the same way they did the first time, using irregular routes, because right now it's very difficult to get a visa for Chile or Brazil, and other countries are also restricting their policies for Haitians," said Giuseppe Loprete, Haiti mission chief for the International Organization for Migration.
Many of the deportees remain determined to leave.
Elie, a former rice farmer in the northern city of Gonaïves, fled to Brazil in 2013 after bandits seized his crops. In Brazil, he worked construction and met his Haitian wife, Bencia Revangil, 27, also a migrant. By last year, as the pandemic caused Brazil's economy to buckle, they had saved $1,200 and considered heading to the United States.
But they waited, Elie said, because "Donald Trump was in power."
Then his wife's sister told them in April that she and her husband and child had managed to cross into Texas, been processed by immigration officials and been allowed to travel on to Florida. The Elies borrowed money from Revangil's father and set off a couple of weeks later, enduring a grueling trip by bus and foot through jungles and over rushing rivers, paying guides and smugglers the lion's share of their savings. Along the trails, they were robbed of $300 and passed the bodies of dead migrants.
"But the worst thing done to us was in the U.S.," he said.
"They did not treat us like human beings," he said. "We spent five days in prison without taking a bath, without brushing our teeth. We were there looking for asylum, because we are Haitian. The deported us, illegally I would say. We were not given a chance."
Elie and his wife say they were chained in front of their children for the deportation flight and not told where they were going. Revangil said she fainted on the plane, suspecting they were returning to Haiti.
Their bags lost with their documents, clothes and electronics, they borrowed a phone and called Revangil's father, who lives outside the capital and called a friend to aid them. He found them a room in a boardinghouse in the Carrefour Feuilles neighborhood, where violent gangs are staging incursions. There's no bed; the family sleeps at night on the room's concrete floor.
The day after they arrived, an evangelical preacher was shot dead in front of a nearby church as kidnappers took his wife.
The family eventually returned to the airport and finally persuaded guards to let them in.
Elie found their bags. But their children's Brazilian birth certificates — their best hope, they believed, for leaving the country by plane — were missing.
Nevertheless, Elie said, they would find a way to get out, even if it meant risking treacherous seas.
"We have nothing now, but we will try again to get back to the U.S.," he said. "I prefer to die on the way than stay here."
Faiola reported from Miami. Hernández reported from Ciudad Acuña, Mexico.
U.S. preparing to nearly double deportations to Haiti as some returnees decry being shackled
A Haitian prosecutor sought charges against the prime minister in the president's assassination. He was fired.
A lament for Haiti: 'It is as if we are cursed'

redpajama_set_name: RedPajamaCommonCrawl


Narendra lives in the woods without electricity and running water.
Nicholas definitely has the ability to be the boss.
Colin was kind to everybody.
Eddie is a lot like Tyler.
I don't think Shamim is a bad boy.
How long were you and Alex friends?
Keith held onto the rope.
Daniele missed the last train and had to take a taxi home.
Louiqa showed me a picture.
Why would somebody hit Valerie?
Lar didn't come, did he?
I asked around about Craig.
I'm well aware of Win's shortcomings.
Francis started working for us when he was only thirteen.
Ozan wanted to impress her friends.
Shawn likes the extreme cold of Alaska.
I have to help Space clean his room.
I wish Roderick were on our team.
Sri wanted to hang out with Maureen.
I think Mehrdad has a little crush on you.
Pontus spoke very quietly, but loud enough to be heard.
Olof will never pay me what he owes me.
I don't want Leung to take over.
Roxana wondered what had made Clem so unhappy.
Lin wondered if Siping liked him as much as he liked her.


text:
Mercedes-Benz E-Class Powers Up for 2019
May 23, 2018 • by AF Staff
The Mercedes-Benz E450 (with optional 4Matic) replaces the E400 sedan for 2019 in four body styles, including sedan, coupe, cabriolet, and wagon.
Photo courtesy of Mercedes-Benz USA.
Mercedes-Benz is upgrading its V-6-powered E-Class lineup for the 2019 model year by boosting engine power, a new navigation logic that increases safety, and interior upgrades, the company has announced.
For 2019, the E450 and E450 4Matic all-wheel drive models will replace the existing E400 and E4Matic sedans. Mercedes-Benz will again offer four body styles, including sedan, coupe, cabriolet, and wagon.
The 2019 E450 will be equipped with a more powerful 3.0-liter biturbo V-6 that generates 362 horsepower (a 33-hp boost) and 369 pound-feet of torque (15 lb.-ft. more) than the outgoing model. The E300 and E300 4Matic sedans will return equipped with a 2.0-liter turbo inline four-cylinder that makes 241 hp and 273 lb.-ft. of torque.
The 2019 E-Class lineup will recieve safety and driver-assisting features that were added to the S-Class that was redesigned in 2017. It will add a feature known as route-based speed adaptation that uses a substantially broader scope of map and navigation data to more safety navigate different driving roads and situations, according to the company.
Interior upgrades include a three-spoke Nappa leather steering wheel, two additional trim options with matching center consoles, and 19-inch AMG wheels available with Night Package and Rear Safety Package.
The new models will go in sale this fall. Mercedes-Benz will announce pricing closer to launch.
Related Photos: Mercedes-Benz 2018 S450 Sedan
Read more about Mercedes-Benz Mercedes-Benz E-Class Luxury Sedans 2019-MY Midsize Sedans
Volkswagen Discontinues Golf Alltrack, SportWagen
Volkswagen of America will cease production of its Golf-based SportWagen and Alltrack European-style wagons by the end of this year to focus on sport utility vehicles, the automaker has announced.
Subaru Prices 2020 Outback, Legacy
Subaru's 2020 Legacy midsize sedan and 2020 Outback crossover will see price increases of $200 and $300 respectively as they enter new generations, the automaker has announced. Subaru has also announced pricing for its new optional driver distraction technology.
Ongoing Strong Economy to Bolster 2020-MY Fleet Orders
The majority of fleets report new-vehicle acquisitions will continue to be elevated due to strong business growth, comparable to MY-2019, with most forecasting an increase or continuation of similar order volume in MY-2020.
Mazda's 2019 Mazda3
Mazda has brought back its 2019 Mazda3 sedan and hatchback — we will review this model separately — with a smart update that improves handling and interior quality.
FCA Offers 2020-MY Fleet Incentives
Fiat Chrysler Automobiles has announced fleet incentives for 18 nameplates in its 2020 lineup of Ram, Dodge, Chrysler, Jeep, Fiat, and Alfa Romeo vehicles.
Cadillac's 2019 XT4
Cadillac's SUV onslaught continues with the 2019 XT4, which follows the XT5 and precedes the 2020 XT6.
Buick Adds Tech to 2020 Enclave
Buick's flagship Enclave seven-passenger SUV is adding technology and a back massage feature for 2020 as part of a midcycle update that will also bring the new Sport Touring trim grade.
Toyota Slates New SUV for Alabama Plant
Toyota will build a yet-to-be-announced SUV at an Alabama assembly plant that it's sharing with Mazda, the automaker has announced.
Volkswagen Ends Beetle Production
Volkswagen is ending production of its Beetle, and will send the final vehicle to a museum in Puebla, Mexico, near the factory that produced the iconic car. Several companies, including Best Buy, have used the Beetle as a branded fleet vehicle.
Audi Announces 2020 Fleet Incentives
Audi of America has set its corporate incentives for nine of its vehicles, including three of its luxury SUVs, the Volkswagen division has announced.


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Crunch crunch crunch. We're walking on an old lava field, from one of the last lava flows in Maui's history, possibly 500 years old. It sounds like walking on tortilla chips.
walking on the old lava flow, jagged rocks, and bottom right: goat pellets.
So I just had a tremendous wake up call this week.
I love this quotation from French writer, Andre Gide.
Came across it recently, and it speaks to me.
My posts will be less frequent, maybe only a couple of times this month or next month.
After listening to Jon Morrow's webinar on launching a blog, I realized I am doing something wrong. Ouch. It was the same webinar I had listened to in January or December. Ouch. Same message. Ouch. I'm not willing to pay the hefty price to take his intensive training, but will do my best to apply his message.
I will be focusing on making a Facebook page for this site, revamping some older posts, doing better descriptions, doing more guest blogging, refining my newsletter, redoing my Etsy store, redoing Pinterest (they have a nasty copyright violation policy which affects everyone), and doing some deep inner work. Plus I never got around to accepting four Liebster Blog awards from April and I want to do that (This also requires answering some questions).
If you'd like to stay connected and know when the next real post will be up, sign up for the newsletter (upper right corner if you're on a desktop or below). People who sign up will get first notice of when a new post goes live. To tempt you, some posts I'm working on: a journey to a secret spot on Maui, the rest of the infamous Road to Hana Trip series, and other tales of life and madness on Maui.
I only send the newsletter out once every two weeks, or maybe twice a month. For a sample of what it looks like, here's the latest issue. I won't spam you! I personally hate spam and excessive emails.
A to Z Challenge - Exploring the cultural icons of Hawaii, and debunking them! Grass shacks! Bah! Grass skirts! Bah! Coconut bras! Bah! 26 posts in 26 days from A to Z.
If you sign up for the newsletter, I'll also tell you when and where I'm guest posting.
You can also send me feedback by commenting below or email me direct at maui jungalow (at) gmail (dot) com. Take out all the spaces and punctuation so it looks right!
On twitter, I can easily be reached at @mauijungalow.
If you've loved any of my posts and would like me to guest blog, please contact me or comment below.
Big Beach on Maui's South Shore has some of the most intriguing waves I've ever seen. I'm not a wave expert, oceanographer, or a surfer, but the wave patterns here are kind of strange.
Tail end of a T-shaped wave.
A brown speckled egg from one of the Rhode Island Reds.
I found this post in my drafts, from a year ago! A very short post today, because I feel pretty darn eggs-hausted from the new chickens who arrived last week.
I have been googling chickens, asking random people about chickens, and learning to understand chicken sounds.
There are three of the little terrors, and now I understand why chicken eggs are $6 or $7 a dozen on Maui.
They are all females and I was told that chickens can't have PMS, but you could have fooled me.
They are sometimes quiet, but more often than not, loud, especially when I'm trying to work. They were always kept in a cage, and I am trying to teach them to free range. It has been a bit feather-raising for all of us, but some progress is being made.
This informal calendar will be updated as time permits. Events are subject to change, so please check the linked websites for updates. I tend to focus on free or low-cost events.
but I wanted a picture!
8/2 – First Friday in Wailuku, Town Party.


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AlexCockburn--Emanuel's exit
""""By the time Obama hired him, Emanuel already had a proven record of toadyism to corporate America and the neocon lobby. Emanuel was a relict of all that was sleazy in the Clinton White House. Among the body blows that have brought the Democrats to their present ebb, the passage of NAFTA in 1993, with consequent destruction of the American industrial economy, must count as among the most lethal. Key to that passage was Emanuel, who directed the Clinton White House operation to get the treaty passed by any means necessary.
Following his departure from the White House in 1998, Emanuel headed to a well upholstered post in a Chicago banking firm before he won election to Dan Rostenkowski's old Chicago seat. By 2005 he headed the Democratic National Campaign Committee. As such, he decided which candidates for the House should get money and other support from the national party. As Andrew Cockburn and later John Walsh described on this site at that time, Emanuel did his best to recruit candidates, preferably rich ones, guaranteed to eschew vocal opposition to the Iraq war, which Emanuel, a veteran of the Israeli army strongly favored. """"
After the midterm election John Walsh totted up the scorecard achieved by the man hailed as the Democrats' can-do guy, as efficiently ruthless as the Great Satan himself, Karl Rove.
Emanuel had chosen chose 22 key races, open or Republican seats, where Democrats might win. "By any reasonable criteria," Walsh wrote, " all the candidates chosen by Emanuel, save perhaps for one, were pro-war as Emanuel himself. In two cases Rahm had to put in considerable dollars and effort in the primaries to drive out antiwar candidates. He drove out Cegelis in Illinois's 6th CD, at the cost of one million dollars, in favor of Tammy ("Stay the course") Duckworth who lost in the general election. In California's 11th CD primary, Emanuel backed the prowar Steven Filson who lost to the antiwar candidate, Jerry McNerney, who went on to win in the general election."""""
Amazingly, many corporate "Democrats" seem to consider RE , at least as neo-con-ish as a Lieberman, an authentic liberal--then, many think the same of General Hillary, hardly any different than a McCaint on most foreign policy issues.
CharleyCarp said...
See, this is why I get so irritated with 'progressives' who go on at length about how the Dems ran on ending the war in 2006, and didn't do it. I'm no fan of RE, not by a long shot. But it's important to understand just how thin (ie too thin to see) the mandate to end the war really was.
I agree, Mr Carp. Obama sounded progressive only until he secured the nomination. Once he'd disposed of Hillary, he then turned fairly centrist---and started to hire Clintonites, such as RE...and Hillary herself (as well as G-sachs people, the bailout, etc).
I suspect that was all part of some backroom deal with Hillary's people (given how ready and willing she was to concede at the convention in 2008).
I also find it a bit odd that RE, a former Israeli soldier, could attain such a powerful position in the US govt.


The image of Warrior Cat Deaths Coloring Pages is really great cat coloring pages for your kids. You are enable to download without charge by clicking the DOWNLOAD button under the photograph. It will be connected to a new window. Do right click on the photo, then pick save picture as… After that you are allowed to revise the file name and the folder where you want to keep the file. Then click the save button.
Check out these photographs corresponding to Warrior Cat Deaths Coloring Pages, hope it is useful..


Teter claimed its fourth Little 500 women's title on Friday.
Ski went to the lead early in the race, opening up a bit of a gap by Lap 20. In the next few laps, they broke away from most of the field with Delta Gamma and Teter. Those three teams had a lap lead on the rest of the field 80 laps in.
A little more than midway through the race, Ski's lead was as many as 20 seconds over Delta Gamma. But DG was able to gradually cut down on the difference, and Ski had the white jersey on its tail, every exchange making the difference.
Alpha Chi Omega made a play to get back into the top four with eight laps remaining, but Ski had a nice exchange a couple laps later to get back a healthy lead. They had a four-second advantage with four laps remaining.
With three laps left, Ski exchanged to put Delta Gamma and Teter back out front. But after an early explosion by Ski with 99 laps in, Teter and Delta Gamma went out front in the final one.
Teter then exploded for the win at 1:23:47. Delta Gamma was second and Ski finished third.


The 7 Steps to Better Writing workshop was developed by writers who have extensive experience working with government, private sector, and nonprofit clients.
We brainstormed about our thought process when we write for clients. Then we distilled that process into 7 Steps.
Tackle your workplace writing like a pro! Our workshop explains a simple system you can apply again and again, to anything from emails and blogs to technical reports.


We are very excited to announce the first three Featured schools for our College ID Camp. At our C3 College Clinics players participate in 3 session. Players are trained by 3 different colleges each session. (9 Total) Come be a part of a rich history of players recruited via C3 Soccer Camps events.
This event is open to players from any club.


text:
Q: How to add condition to EmberJS Input Helper How can I build a this input <input class="{{unless isEditing "hidden"}}" /> with the input helper of Ember.js?

A: You can use parenthesis to have another helper within a helper
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redpajama_set_name: RedPajamaStackExchange


text:
M74 overnight road closures set to cause disruption for Glasgow drivers
Local diversions will be in place.
Magdalene Dalziel
(Image: Media Scotland)
Drivers are being warned of a series of overnight closures on the M74 near Mount Vernon this month.
Scotland Transerv will be resurfacing the 1.6m northbound route between Junction 3 and 3A from Monday, November 11 - Monday, November 18.
The upgrades are part of a £500,000 Transport Scotland project and motorists are advised to prepare for extra time to journeys as a result.
Urgent appeal to reunite heartbroken Glasgow woman with lost engagement ring
Adam Sarwar, Scotland TranServ's project design lead on the scheme, said: "We have been working in liaison with local authorities, emergency services and key stakeholders to carefully schedule this programme of work to minimise impact on commuters and businesses using this busy route every day.
"In addition, it is important that we avoid impacting late night Christmas shopping traffic and deliver this scheme before the weather deteriorates. We would like to take this opportunity to thank drivers in advance for their patience while we complete the project and deliver long-term benefits to the road surface of the M74 northbound through this stretch of carriageway."
Scotland TranServ will deliver this resurfacing programme under the following programme of overnight closures:
• 8pm on Monday 11 until 6am on Tuesday November 12
• 8pm on Tuesday 12 until 6am on Wednesday November 13
• 8pm on Wednesday 13 until 6am on Thursday November 14
• 8pm on Thursday 14 until 6am on Friday November 15
• 8pm on Friday 15 until 6am on Saturday November 16
• 8pm on Saturday 16 until 6am on Sunday November 17
• 8pm on Sunday 17 until 6am on Monday November 18
Drivers are advised to allow some additional time for their journeys, with local diversions in place.
Special arrangements will be made for emergency service vehicles, however no additional arrangements will be made for windfarm traffic during this time.
This investment into the M74 is one of a number of such programmes being carried out by Scotland TranServ across South West Scotland, supporting the economic growth and development of the area.
Alan Murray, Scotland TranServ's Principal Road Design Engineer added: "This project has been scheduled to be delivered with maximum efficiency and minimal disruption. Across South West Scotland, we're working on behalf of Transport Scotland to prioritise such road maintenance issues and deliver our programme of work as quickly and safely as possible."


HOUSTON — President Donald Trump late Tuesday ordered flags lowered to half-staff through Saturday night in memory of former first lady Barbara Bush, who died earlier Tuesday at the age of 92.
And the White House Historical Association announced Tuesday that members of the public who wish to sign the official condolence book for Bush can do so beginning at 9 a.m. Wednesday.
The condolence book will be at the White House Visitor Center, steps from the White House, at 1450 Pennsylvania Ave. NW in Washington. The center is open daily from 7:30 a.m. to 4 p.m. and is free to the public, according to the historical association.
Members of the public also can pay their respects Friday as Bush's body lies in repose at St. Martin's Episcopal Church in Houston. An invitation-only funeral will be Saturday at Second Baptist Church.
A website for the former first lady suggests donations to the Barbara Bush Foundation for Family Literacy.
Bush was married to former President George H.W. Bush for 73 years. The mother of six children — including President George W. Bush — grandmother to 17 and great-grandmother to seven, the former first lady spearheaded family literacy programs during her time in office and beyond.
"Mrs. Bush played an especially important role in the White House in that she reactivated the Committee for the Preservation of the White House and helped establish the White House Endowment Trust," White House Historical Association President Stewart McLaurin said in a statement, thanking Bush for her work that continues to provide financial assistance for conservation projects in the state rooms of the White House and other collections.
Bush was known as a matriarch to a political dynasty, and for her quick wit and strong personal views.
Speaking to Wellesley College's Class of 1990, an appearance that drew criticism from students who questioned her credentials to address female graduates entering the workforce, she addressed the audience with her signature good humor.
"Somewhere out in this audience may even be someone who will one day follow my footsteps and preside over the White House as the president's spouse. I wish him well," she said.


Večeras s početkom u 19 sati, kandidati HDZ-a s liste za IX. izbornu jedinicu predstavit će se u Maslenici (središnji trg kraj zgrade Općine Jasenice, ulica Petra Zoranića 61).
Bit će to središnji predizborni skup za grad Obrovac i općine Jasenice, Gračac i Starigrad.
Skupu će nazočiti i predsjednik Hrvatske demokratske zajednice Andrej Plenković.
Načelnik općine i predsjednik Općinskog odbora HDZ-a općine Jasenice, Martin Baričević, poziva sve članove stranke, kao i sve ostale građane, da dođu na predizborni skup.
"Velika je čast i meni kao kandidatu, i svim ostalim Jeseničanima, što budući premijer dolazi u Jasenice poslati poruku pobjede. Pripremamo impresivan skup i svi su pozvani." – istaknuo je za portal Kalelarga info Baričević.
Shopping for a new or used auto can be quite a tough process if you do not know what you really are doing. By educating yourself about car purchasing prior to go to the dealership, you can make things much easier for your self. The following advice may help your following buying journey be more satisfying.
Usually take a mechanic alongside when looking for a brand new automobile. Automobile merchants are well known for offering lemons and you may not want to be their next target. If you can not get a mechanic to check out cars together with you, at least make certain you have him review your last selection before you purchase it.
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Prior to signing any contract spend some time to study each and every line, for example the small print. When there is nearly anything detailed that you just do not understand, do not indicator up until you receive an response that you comprehend. Unsavory salesmen can use a legal contract to put in a lot of costs that have been not mentioned.
When you retain the preceding advice in your mind the very next time that you go purchasing a automobile, you will certainly be very likely to get a good package. Investing in a vehicle lacks as a headaches. Simply use the tips using this post and you may have the vehicle you would like in a great value.


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Q: Initializer for conditional binding must have Optional type, not 'String'? Unable to read FCM notification Userdata, I am trying this-
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text:
El mètode alemany és un dels molts esquemes tradicionals d'excavar túnels amb tècniques poc mecanitzades (de fet, gairebé cada país tenia el seu mètode particular). Com tots els mètodes tradicionals, consisteix a excavar el túnel mitjançant galeries independents (unes més avançades que d'altres) que formen en el seu conjunt l'àrea total d'excavació. Cada galeria s'apuntala convenientment per sostenir el terreny provisionalment, de manera que el sosteniment arriba en tot moment fins al front d'excavació. D'aquesta manera, els assentaments en superfície són mínims. Segons aquest mètode, les primeres galeries a ser excavades són les de les cantonades inferiors. Les següents se situen immediatament a sobre de les primeres per facilitar la connexió de sosteniments. Seguidament, s'excava la futura clau del túnel, i després s'acaba d'excavar tota la part superior, clavant els sosteniments des de les galeries ja excavades. Amb tota la volta ja revestida, només resta la part central inferior del túnel, que s'excava en l'última fase mentre es canvien els sosteniments provisionals pels revestiments definitius, normalment una capa de formigó armat d'entre 80 i 100 cm de gruix.

Aquest és un dels pocs mètodes tradicionals (juntament amb el belga i el de Sant Gotthard) que ha sobreviscut al pas dels anys, ja que encara s'usa (tot i que molt poques vegades).

Referències

Túnels

redpajama_set_name: RedPajamaWikipedia


text:
Home NEWS Science News Health
Novel PET radiotracer reduces number of false-positive cancer findings after COVID-19 vaccination
Reston, VA—A novel imaging agent, 68Ga-FAPI, can reduce the number of false-positive PET/CT findings among cancer patients recently vaccinated for COVID-19. New research published ahead of print in The Journal of Nuclear Medicine shows that 68Ga-FAPI imaging offers superior lesion detection without vaccine-related tracer uptake in locoregional lymph nodes that is common with 18F-FDG imaging. This can help to prevent costly follow-up and false management decisions for cancer patients.
Credit: Image created by Tristan T. Demmert et al., Department of Nuclear Medicine, University Hospital Essen.
One side effect of the COVID-19 vaccine is that 18F–FDG (the most commonly used PET imaging agent) is taken up by immune cells responding to the mRNA inflammatory stimulus caused by the vaccine. This is known as a reactive uptake and does not always indicate that a tumor is present.
"This observation is concerning as vulnerable groups, such as oncologic patients, undergo both regular COVID-19 booster shots and medical imaging," said Tristan T. Demmert, researcher in the Department of Nuclear Medicine at Essen University Hospital in Essen, Germany. "False positive findings on 18F-FDG PET due to reactive uptake may trigger false management decisions."
To find a way to avoid these false positives, researchers compared two radiotracers, 68Ga-FAPI and 18F-FDG. Using a large prospective imaging registry, researchers investigated 11 oncologic patients who had received a COVID-19 vaccination within six weeks, had 68Ga-FAPI and 18F-FDG imaging on the same day, and had documentation of tracer uptake in locoregional lymph nodes. Visual readings of the images were performed by two nuclear medicine physicians.
Significant lymph node uptake adjacent to the injection site was noted in 11/11 patients with 18F-FDG PET/CT versus 0/11 with 68Ga-FAPI PET/CT. In addition, 18F-FDG detected 73 percent of tumor lesions, while 68Ga-FAPI detected 94 percent of all tumor lesions.
"In patients with suspected tumors in the axillary region, a costly follow-up was often recommended to avoid incorrect patient treatment. According to our results, this could have been prevented by using 68Ga-FAPI, which would have allowed higher tumor detection at the same time," noted Demmert. "Considering that further booster vaccinations are expected, 68Ga-FAPI could show its potential in avoiding vaccine-related misinterpretations on PET/CT while providing equivalent tumor detection."
This study was made available online in November 2022.
The authors of "Novel 68Ga-FAPI PET/CT offers oncologic staging without COVID-19 vaccine-related pitfalls" include Tristan T. Demmert, Ines Maric, Katharina Lueckerath, Ken Herrmann, and Wolfgang P. Fendler, Department of Nuclear Medicine, West German Cancer Center, University of Duisburg-Essen, Essen, Germany, and German Cancer Consortium (DKTK), Partner Site University Hospital Essen, and Germany Cancer Research Center (DKFZ), Essen, Germany; Kelsey L. Pomykala, Institute for AI in Medicine (IKIM), University Medicine, Essen, Germany; Jens Siveke, German Cancer Consortium (DKTK), Partner Site University Hospital Essen, and Germany Cancer Research Center (DKFZ), Essen, Germany, and Bridge Institute of Experimental Tumor Therapy, West German Cancer Center, University Hospital Essen, University of Duisburg-Essen, Essen, Germany; Benedikt M. Schaarschmidt, Department of Diagnostic and Interventional Radiology and Neuroradiology, University Hospital Essen, University of Duisburg-Essen, Essen, Germany; and Rainer Hamacher, German Cancer Consortium (DKTK), Partner Site University Hospital Essen, and Germany Cancer Research Center (DKFZ), Essen, Germany, and Department of Medical Oncology, West German Cancer Center, University Hospital Essen, Essen, Germany.
Visit the JNM website for the latest research, and follow our new Twitter and Facebook pages @JournalofNucMed or follow us on LinkedIn.
Please visit the SNMMI Media Center for more information about molecular imaging and precision imaging. To schedule an interview with the researchers, please contact Rebecca Maxey at (703) 652-6772 or [email protected].
About JNM and the Society of Nuclear Medicine and Molecular Imaging
The Journal of Nuclear Medicine (JNM) is the world's leading nuclear medicine, molecular imaging and theranostics journal, accessed 15 million times each year by practitioners around the globe, providing them with the information they need to advance this rapidly expanding field. Current and past issues of The Journal of Nuclear Medicine can be found online at http://jnm.snmjournals.org.
JNM is published by the Society of Nuclear Medicine and Molecular Imaging (SNMMI), an international scientific and medical organization dedicated to advancing nuclear medicine and molecular imaging—precision medicine that allows diagnosis and treatment to be tailored to individual patients in order to achieve the best possible outcomes. For more information, visit www.snmmi.org.
Journal of Nuclear Medicine
10.2967/jnumed.122.264872
Novel 68Ga-FAPI PET/CT offers oncologic staging without COVID-19 vaccine-related pitfalls
COI Statement
Katharina Lueckerath reports fees from SOFIE Bioscience (consultant) and Enlaza Therapeutics (consultant). Rainer Hamacher is supported by Clinician Scientist Program of the University Medicine Essen Clinician Scientist Academy (UMEA) sponsored by faculty of medicine and Deutsche Forschungsgemeinschaft (DFG) and has received travel grants from Lilly, Novartis and PharmaMar as well as fees from Lilly and PharmaMar. Jens T. Siveke received honoraria as consultant or for continuing medical education presentations from AstraZeneca, Bayer, Bristol-Myers Squibb, Eisbach Bio, Immunocore, Novartis, Roche/Genentech, Servier; his institution receives research funding from Bristol-Myers Squibb, Celgene, Eisbach Bio, Roche/Genentech; he holds ownership and serves on the Board of Directors of Pharma15, all outside the submitted work. Benedikt M. Schaarschmidt received a research grant from PharmaCept for an undergoing investigator-initiated study not related to this paper. Ken Herrmann reports personal fees from Bayer, personal fees and other from Sofie Biosciences, personal fees from SIRTEX, non-financial support from ABX, personal fees from Adacap, personal fees from Curium, personal fees from Endocyte, grants and personal fees from BTG, personal fees from IPSEN, personal fees from Siemens Healthineers, personal fees from GE Healthcare, personal fees from Amgen, personal fees from Novartis, personal fees from ymabs, personal fees from Aktis Oncology, personal fees from Theragnostics, personal fees from Pharma15, outside the submitted work. Wolfgang P. Fendler reports fees from SOFIE Bioscience (research funding), Janssen (consultant, speakers bureau), Calyx (consultant), Bayer (consultant, speakers bureau, research funding), Parexel (image review) and AAA (speakers bureau) outside of the submitted work. All disclosure were outside of the submitted work.
Study shows FDA-approved TB regimen may not work against the deadliest form of TB due to multidrug-resistant strains


Today we constructed the tea cabinet, which will fit on the left of the microhood and is a narrow cabinet which I plan to use to store canisters of various teas. We realized the cabinet needed to be installed prior to installing the remove-able back of the above microhood shelf so we can install a cleat on the tea cabinet to hold the back in position.
Much careful measuring ensued, but we still cut the back of the tea cabinet incorrectly on the first try. We subtracted the width of the cabinet sides twice, grr, leading to the cabinet back being cut one inch too narrow. The second time we were dead on, though. The cabinet went together pretty quickly. We discovered veneer edging on some past project, and put it too good use here covering the exposed plywood edges. The veneer is a huge timesaver, it is covered with a heat sensitive adhesive, you use an ordinary household iron to attach the veneer, let it set, then trim the veneer to fit. Amazing! What takes longer is covering it all with several coats of polyurethane --very tedious.
The cabinet is made from red oak plywood, as white oak plywood, so popular 25 years ago, was nowhere to be found. It won't match the existing cabinets exactly, but we hope with the addition of some red oak molding here and there, it will look planned. Probably not, but it will be the cabinetry equivalent of plaid, my favorite color, so it will work for me.
With luck and perseverance, we should be able to hang the cabinet and put in the back wall tomorrow.
The new microwave, BTW, works great, heating things much faster than the old one, and more quietly, too. The fan feature of the vent is quiet, but I haven't given it a real workout yet -- I foresee some sauteed garlic and onions on the menu soon.
Nice work! That looks great, and I love those tea tins.
The green color on the back of the wine glass shelf--is that paint? I love that color; our bedroom is the same shade.
It looks like you and Dan did a marvelous job on your project! I also did not know that you collect tins. because I collect tins too.
p.s. We may need to get together and maybe get one for Mommy and Daddy if at all feesable. Or if we all get-together and buy Mommy a new stove.
Meg: the green is paint, I believe it is called Fox Hollow or something equally descriptive. I love that color too, it is in our living room and in parts of the kitchen. How great that your bedroom is that color! One of the things I hated about apartment living was the endless array of landlord beige walls.
Jean: I love those vintage metal canisters! I use a lot of them in the pantry for flour, sugar, rice, etc. They work great and look good.
Mom: We debated for hours about whether to paint the back of the mug cabinet green or taupe. We finally picked taupe, and until we finish painting all the rooms in the house, there is no going back! I'll post a photo of the whole wall with the photos of the tea cabinet. xoxo.


sexual assault are particularly sensitive.
The trauma they've undergone is both physical and intensely emotional.
While medical care and evidence collection are essential, the right temperament and training are two additional, imperative factors required to ensure these patients aren't subjected to further anguish.
Sexual assault nurse examiners go through extensive instruction on how to best support victims that come through the emergency department doors, including being fully aware of each patient's mindset.
They require time, encouragement, and support to be able to share their story with the nurse.
SANE training employs trauma-informed care. Nurses put themselves in the shoes of the patient and try to understand what the patient may have experienced.
To attain SANE certification in the state of Illinois, emergency room nurses must take a 40-hour didactic course through the Illinois Attorney General. This is followed by a rotation of clinical requirements that include caring for patients and survivors of sexual assault.
Online training takes place before in-person classes are attended. SANE training is conducted by the SANE coordinator, who travels around the state to teach the courses. Three days are spent in the classroom, focusing on the anatomy and physiology of male and female genitalia and reproductive systems. Proper techniques for evidence collection are covered as well.
Staff are instructed to be aware of red-flag indictors of human trafficking. Human trafficking isn't limited to big cities, and Riverside emergency staff are primed to know what to look for. SANE nurses also screen for domestic violence, neglect, and abuse.
If you or someone close to you has been sexually assaulted, it is critical to pursue medical care. Go to the emergency department immediately. One can also call the emergency department to speak to a sexual assault nurse at Riverside by dialing 815-935-7500.
Patient trust is a priority in treating sexual assault victims. "The number-one thing is that you make sure patients can trust you and they know you believe them," explains Booker.
Unfortunately, when survivors have to recount the story to multiple people many times over, the process can re-victimize them. This is called "secondary victimization." In order to prevent further trauma, nurses try to limit the number of encounters patients must have with both the police and providers.
As uncomfortable as it may be for victims, a full examination and evidence collection are crucial components of the emergency visit. Proper evidence collection will aid any legal pursuits.
SANE works closely with the Kankakee County Center Against Sexual Assault (KCCASA), a team of advocates and representatives in the community. Counselors are available 24/7, responding to emergency room reports of sexual assault victims. They follow up with the patient, providing medical legal services and advice.
Kankakee Iroquois Human Trafficking Task Force is another entity that collaborates with emergency personnel. This task force works to combat human trafficking within the community. In conjunction with KCCASA and SANE, new laws and community efforts are being implemented to take care of sexual assault survivors in the area.


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Energy Central News
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Businesses rank PPL Electric Utilities best in the East in study conducted by J.D. Power
Dec 3, 2021Dec 3, 2021 3:46 pm GMT
ENP Newswire
ALLENTOWN - Business customers of PPL Electric Utilities have rated the utility first in electric business customer satisfaction among its peers in the East large-size segment, according to a study conducted by consumer insights, data and analytics company J.D. Power.
The results were recently released in the J.D. Power 2021 Electric Utility Business Customer Satisfaction Study.
Currently in its 23rd year, the study measures satisfaction among the business customers of 87 U.S. electric utilities, each of which serves more than 40,000 business customers. PPL Electric Utilities serves more than 200,000 business customers across its 29-county service territory in eastern Pennsylvania.
'The satisfaction of our customers, whether business or residential, is one of our top priorities,' said PPL Electric Utilities President Steph Raymond. 'I'm proud to see our customer-first mindset and the continued hard work of our team reflected in this ranking. Providing the safe, reliable and affordable electric service that our customers need to power their daily lives is essential to building, and keeping, their trust.'
PPL Electric Utilities scored highest among its peers in five of six study factors: power quality and reliability, billing and payment, price, communications, and customer contact. Additionally, the study showed that PPL Electric Utilities excelled in outage management, scoring highest among large utilities for providing accurate information about outages and promptly restoring customer power after an outage has occurred.
Overall, PPL Electric Utilities now boasts a total of 29 J.D. Power Awards, which includes 17 in the J.D. Power Electric Utility Residential Customer Satisfaction Study.
PPL Electric Utilities provides electric delivery service to more than 1.4 million homes and businesses in Pennsylvania and ranks among the best utility companies in the country for customer service and reliability. PPL Electric Utilities is a major employer in the communities it serves. It is a subsidiary of PPL Corporation (NYSE: PPL).
Russ Hryvnak
Email: rhryvnak@pplweb.com
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