text:
\section{Introduction}

Intermediate mass black holes may represent the link between the
stellar mass black holes seen in the Milky Way (which are probably all
less massive than 20$M_\odot$) and the supermassive black holes
thought to exist in the centers of galaxies (which are mostly more
massive than $10^6 M_\odot$, but see e.g. Greene \& Ho 2004 for a
sample of AGN whose black hole masses are likely to be a few hundred
thousand solar masses and Fillipenko \& Ho 2003 for the discussion of
an especially low mass AGN).  It is possible that the AGN have grown
from $\sim 100-1000 M_\odot$ formed from core collapses of Population
III stars (see e.g. Fryer, Woosley \& Heger 2001).  On the other hand,
another natural place to produce these intermediate mass black holes
is in the centers of globular clusters (Miller \& Hamilton 2002) or
young dense star clusters (Portegies Zwart \& McMillan 2002; Portegies
Zwart et al. 2004; G\"urkan, Freitag \& Rasio 2004).

Several methods have been considered for proving the existence of
these intermediate mass black holes, but to date, there is no
conclusive evidence for the existence of a black hole in the
$10^2$-$10^4$ $M_\odot$ range.  Attempts have been made to associate
some or all of the ultraluminous X-ray sources with intermediate mass
black holes on various bases - X-ray spectra showing cool discs yet
high luminosities compared to what would be expected from a stellar
mass black hole (e.g. Miller et al. 2003), quasi-periodic oscillations
similar to those observed from stellar mass black holes, except at a
frequency an order of magnitude lower (Strohmayer \& Mushotzky 2003),
and the association of one of the brightest ULXs (in fact the same one
showing the low frequency QPO) with a young dense star cluster which
is a plausible birth location for this source (Portegies Zwart et
al. 2004) and a plausible scenario for the evolution of an X-ray
binary with such a black hole has been laid out as well.

Some work has suggested that gravitational radiation recoil should
lead to the ejection, rather than merger of unequal mass black holes
(e.g. Redmount \& Rees 1989; Favata, Hughes \& Holz 2004; Merritt et
al. 2004; Madau \& Quataert 2004), which would suggest that build-up
of black holes through mergers in the centers of globular clusters
should be ineffective.  The most recent work (Favata et al. 2004)
suggests that the recoil kicks should be of order 10-100 km/sec; since
several of the Milky Way's globular clusters have escape velocities
from their cores as large as 50-100 km/sec (Gnedin et al. 2002), it is
plausible that some clusters can grow black holes through mergers,
although the fraction of such clusters might be rather small (see
e.g. Merritt et al. 2004).  Newtonian dynamical interactions may also
eject black holes by releasing gravitational potential energy when
binaries are hardened (Portegies Zwart \& McMillan 2000).  However,
these calculations are usually simplified, and neglect factors such as
the possible effects of gas, which can be quite important, for
example, in the mergers of supermassive black holes in galaxies
(e.g. Escala et al. 2004).  Given that whether globular clusters can
grow intermediate mass black holes is an important theoretical
question, attempts to search for observational signatures of such
objects are well motivated.

Attempts to identify signatures of the influence of a black hole on
stellar orbits have a rather spotty record.  Claims have been made for
intermediate mass black holes in the globular cluster G1 in M~31 and
in M~15 in our own Galaxy (Gebhardt, Rich \& Ho 2002; van der Marel et
al. 2002; Gerssen et al. 2002), but the statistical significance of
these detections is less than $3\sigma$, and more sophisticated
treatments of stellar dynamics found that the mass concentration
observed at the center of M~15 could be explained by a concentration
of heavy stellar remnants (i.e. neutron stars and white dwarfs -
Baumgardt et al. 2003; Gerssen et al. 2003).  In fact, it has been
argued that many globular clusters may simply not have enough stars to
probe the gravitational potential well enough ever to conclusively
prove the existence of a black hole (Drukier \& Bailyn 2003),
motivating other search techniques.

Long ago it was suggested that black holes in the center of globular
clusters should accrete gas, and perhaps produce observable X-ray
emission (Bahcall \& Ostriker 1975).  Their original suggestion that
IMBHs should dominate the X-ray emission has been proven false by the
detection of orbital periods and Type I X-ray bursts (see Liu, van
Paradijs \& van den Heuvel and references within); however, the basic
idea that an accreting black hole should be detectable from its X-ray
emission has been re-stimulated by the capability of the {\it Chandra
X-ray Observatory} to resolve out sensitively the X-ray emission from
the very center of globular clusters.  Searches have been made for
X-ray emission from the accretion onto possible central black holes,
but with only upper limits found (Grindlay et al. 2001; Ho, Terashima
\& Makishima 2003).  Unfortunately, these upper limits are not
currently particularly constraining of theoretical models, and they
already approach closely the limits of current X-ray instrumentation.

Recent advances in our understanding of accretion and its relation
with relativistic jet formation indicate that the most sensitive
waveband for detecting low luminosity intermediate mass black holes
is, in fact, the radio.  As the luminosity of accretion onto a black
hole decreases, the ratio of radio to X-ray power increases (Gallo,
Fender \& Pooley 2003); the ratio of radio to X-ray power also
increases with increasing black hole mass (Falcke \& Biermann 1996,
1999; Merloni, Heinz \& Di Matteo 2003; Falcke, K\"oerding \& Markoff
2004).  Furthermore, as accretion theory is now suggesting that the
Bondi-Hoyle (1944) rate overestimates the actual accretion rate by 2-3
orders of magnitude (e.g. Perna et al. 2003), the X-ray luminosities
from accretion of the interstellar medium by intermediate mass black
holes in globular clusters are likely to be well below detection
limits of currently existing X-ray observatories, but given the
prediction of Miller \& Hamilton (2002) that the black holes should be
about 0.1\% of the total cluster mass the radio luminosities of the
brightest cluster central black holes may be detectable with existing
instrumentation (Maccarone 2004).  The idea of constraining the masses
of black holes based on combined measurements of their X-ray and radio
emission has also been put forth by Merloni (2004) in the context of
high redshift AGN, where dynamical measurements are also not likely to
be possible for quite some time.  In this paper, we present the upper
limits on the radio luminosity of the nucleus of Omega Centauri from
an Australian Telescope Compact Array (ATCA) observation, and
reconsider the implications of past upper limits on radio emission
from VLA searches for pulsars, and consider the implications of these
results for the possible masses of central black holes.  We also apply
the same methodology in order to discuss the possibility that an
source found by the NRAO VLA Sky Survey (NVSS) may be an intermediate
mass black hole near the center of the of the Ursa Minor dwarf
spheroidal galaxy.

\section{Predicted luminosities}
The method for predicting the radio and X-ray luminosities of an
accreting black hole in a globular cluster was set forth in Maccarone
(2004).  There it was shown that radio emission provides a much more
sensitive means of detecting low luminosity, intermediate (or higher)
mass black holes, as have been speculated to exist in globular
clusters.  Here we briefly review the assumptions and summarize the
results:

\begin{itemize}
\item Black hole mass of 1/1000 of the globular cluster's stellar mass (Miller\& Hamilton 2002)
\item Gas density of 0.15 H cm$^{-3}$, approximately the value estimated from pulsar dispersion measures in M~15 and 47~Tuc, and expected from stellar mass loss (Freire et al. 2001).
\item Accretion at 0.1-1\% of the Bondi rate, due to disk winds
(e.g. Blandford \& Begelman 1999) and/or convection (e.g. Quataert \&
Gruzinov 2000), calculated from numerical simulations of low
luminosity flows (e.g. Hawley, Balbus \& Stone 2001; Igumenshchev,
Narayan \& Abramowicz 2003), and constrained by observations of low
luminosity AGN in elliptical galaxies and the lack of observations of
isolated neutron stars accreting from the interstellar medium (Perna
et al. 2003 and references within).  The low end of this range is in good agreement with the constraints on the accretion rate in Sagittarius A* derived from millimeter polarization measurements (see e.g. Bower et al. 2003).
\item A radiative efficiency in the X-rays of:
\begin{equation}
\eta=(0.1)\times\left(1+\frac{A^2}{2 L_{tot}}-A\sqrt{\frac{A^2}{4 L_{tot}^2}+\frac{1}{L_{tot}}}\right),
\end{equation}
with $A$ a constant to be fitted from observations (and being larger
when the jet's kinetic power is a larger fraction of the total
accretion power), and $L_{tot}$ the radiative plus kinetic luminosity
of the system in Eddington units, as used by Fender, Gallo \& Jonker
(2003) to explain the $L_X-L_R$ correlation obsered by Gallo, Fender
\& Pooley (2003), with the idea being that enough kinetic power is
pumped into a jet to make the accretion flow radiatively inefficient
(see also, e.g. Malzac, Merloni \& Fabian 2004).  Whether the
radiative inefficiency is due to mass and energy loss into a jet or
also partially due to advection into the black hole (e.g. Ichimaru
1977; Narayan \& Yi 1994) is not clearly established by these
relations, and does not affect the results presented here.  We have
set $A=6\times10^{-3}$ for these calculations, which is based on a
conservative estimate of the jet power.  This relation is used to
convert a calcuated accretion rate (from the assumed fraction of the
Bondi-Hoyle rate) into a calculated X-ray luminosity.
\item The fundamental plane relationship among X-ray luminosity, radio luminosity and  black hole mass of Merloni et al. (2003), parameterized for convenient applications to Galactic globular clusters:
\begin{equation}
F_{5 GHz} = 10 \left(\frac{L_x}{3\times10^{31} {\rm ergs/sec}}\right)^{0.6}
\left(\frac{M_{BH}}{100 M_\odot}\right)^{0.78} \left(\frac{d}{10 {\rm kpc}}\right)^{-2} {\rm {\mu}Jy}.
\label{merloni}
\end{equation}
We note that the relation found by Falcke et al. (2004), which
considered only flat spectrum, low luminosity radio sources like those
we expect to see in the centers of dwarf galaxies or globular
clusters, is consistent with this relation within the uncertainties.
\end{itemize}
We then take the numerical data for the globular cluster's masses and
distances from the Harris catalogue (Harris 1996), compute the X-ray
luminosity under the assumptions given above for the gas density,
fraction of the Bondi-Hoyle accretion rate, and radiative efficiency,
and convert the X-ray luminosity into the radio luminosity using the
fundamental plane relation.  The typical flux values predicted are
less than 40 $\mu$Janskys, even with the accretion rate set to
$10^{-2}$ of the Bondi rate, with the exception of that for Omega Cen,
where the cluster is quite large and reasonably close (see the
tabulation of results in Maccarone 2004).

\section{Observational Data}

Omega Cen was observed with ATCA simultaneously at 4.8 and 8.6 GHz
over 12hr on 2004 May 8. The array was in the '6C' configuration, with
baselines up to 6km. Data reduction was performed with the MIRIAD
software package (Sault, Teuben \& Wright 1995). Flux and bandpass
calibration was performed on PKS 1934-638, and the phase calibrator
was 1315-46 (SUMSS J131829-462034). No source was detected (limits
given below).

We also consider the upper limits on the flux from a central black
hole in M~15 based on the deep VLA observations of Kulkarni et
al. (1990) and Johnston et al. (1991).  These observations were made
at 1.4 GHz and reached a noise level of 43 $\mu$Jy.  Finally, we also
consider the NVSS detection of a 7.1 mJy radio source within the
$1\sigma$ error box of the center of the Ursa Minor dwarf spheroidal
galaxy.

\section{Comparison of Observations with predictions}

\subsection{Omega Cen}

The ATCA data showed no sources within 10 arcseconds of the center of
Omega Cen.  In naturally weighted maps, the rms noise was 57 $\mu$Jy
at 8.6 GHz, and 38 $\mu$Jy at 4.8 GHz.  We assumed a flat (i.e. $f_\nu
\sim$ const) spectrum (as is likely for a low luminosity accreting
black hole) in order to combine the data sets and reduce the noise.
After doing so, the noise level becomes 32 $\mu$Jy, giving a 3$\sigma$
upper limit of just under 100 $\mu$Jy.  For what seems to be the most
likely set of parameters - a gas density which is the same as that in
M~15 and 47~Tuc, an accretion rate of 0.1\% of the Bondi rate, and a
black hole mass of 0.1\% of the cluster's stellar mass - the
prediction of Maccarone (2004), using the methodology outlined
in section 2, was that the radio flux should be about 0.15 mJy.  That
no detection is made while the predicted level value is 4.5$\sigma$
should not as yet be taken as evidence against the hypothesis that
IMBHs can form in globular clusters.  There are several factors of
$\sim$ a few that could be contributing scatter in the theoretical
predictions - most notably the gas density and temperature, but also
the scatter in the fundamental plane relations of MHDM and FKM, and
possible scatter in the black hole mass-globular cluster mass
relation.  We can say with reasonable confidence that there cannot be
both a black hole with a mass of 1/1000 of the cluster mass {\it and}
accretion at $\sim10^{-2}$ of the Bondi rate (considered to be the
likely upper limit of the accretion rate in the work of Perna et
al. 2003), as the predicted level of radio emission in that case would
be more than 20 times the observed level.  Still, in order to make a
strong statement about whether Omega Cen contains an IMBH, we would
need either a detection, or an upper limit about 10 times lower than
the current upper limit.  Since Omega Cen is far south of the
declinations which can be reached with the VLA, this does not seem
likely unless and until the Square Kilometer Array is built in the
Southern Hemisphere.

\subsection{M~15}
Given that Omega Cen is by far the best candidate in the Southern
Hemisphere for detecting an intermediate mass black hole in a globular
cluster, and that it seems unlikely that it will provide useful limits
without new instrumentation, we turn our attention to the Northern
Hemisphere.  Since M~15 had been claimed to show evidence for a
$\sim2000$ $M_\odot$ black hole, and has been the subject of deep
radio observations to search for pulsars, we consider it as well.  The
3$\sigma$ upper limit on the flux from the center of M~15 is 130
$\mu$Jy (Johnston et al. 1991).  Since the nearest ``bright'' source,
AC 211, is about 2.2 arcseconds away, and the data was taken in VLA A
configuration, with 1.4 arcsecond resolution, confusion is not likely
to be a major problem here, as can be verified from looking at the
image of M~15 presented in Johnston et al. (1991).  Furthermore, M~15
is a core collapse globular cluster, so its central position is quite
well defined.  We again assume that the putative IMBH should have a
flat spectrum, and that hence its radio flux should be below about 130
$\mu$Jy at 5 GHz as well as at 1.4 GHz.  This flux level is already
well above that predicted in Maccarone (2004), even for accretion at
$10^{-2}$ of the Bondi rate.  On the other hand, the predicted radio
luminosity in the model of Maccarone (2004) scales roughly as
$M^{3.2}$, and since the claims exist for a black hole much larger
than 1/1000 of the cluster mass (i.e. a 2500 $M_\odot$ black hole has
been claimed, while 1/1000 the cluster mass is only about 440
$M_\odot$), we can come close to making a useful prediction about the
black hole mass with these data.  These data rule out a black hole
more massive than about 600 $M_\odot$, provided that the systematic
factors discussed above are small.

Since the gas density is well measured in M~15 from pulsars, one
source of uncertainty can be eliminated.  Given that a large fraction
of the scatter in the MHDM relation probably comes from the inclusion
of some steep spectrum radio sources (which any BH accreting from the
ISM of a globular cluster is very unlikely to be), and that the more
restrictive sample of FKM shows somewhat less scatter despite imposing
a theoretical mass-X-ray-radio relation rather than fitting to the
data, it seems likely that even this scatter is not too large.  We are
cautious about interpreting the current upper limits as evidence
against a $\sim2000$ $M_\odot$ black hole in M~15, but we note that
this upper limit, unlike the upper limit on the radio luminosity of
Omega Cen, can easily be reduced by looking at higher frequency (where
the VLA is more sensitive), for longer integrations.  A factor of 5
improvement of the upper limit could be obtained in a quite reasonable
4 hour integration, or in a few years with a much shorter integration
from the Expanded VLA (EVLA).  The project to expand the MERLIN array
should also result in the capability to reach similar flux limits.

\subsection{Ursa Minor dwarf}
The Ursa Minor dwarf spheroidal galaxy is one of the closest dwarf
galaxies to the Earth, at a distance of about 66 kpc.  It is one of
the largest of the Milky Way's dwarf spheroidal galaxies in terms of
mass, with an estimated mass of $2.3\times10^{7} M_\odot$ (see Mateo
1998 and references within for the properties of the Milky Way's dwarf
galaxies, including all the data on dwarf spheroidal galaxies' masses
and distances used in this paper).  The NVSS survey (Condon et
al. 1998) indicates the presence of a 7.1 mJy source 20 arcseconds
from the center of the Ursa Minor dwarf.  While this may seem rather
far from the galaxy's center, we note that this is only 0.02 core
radii for this galaxy, and only 1 $\sigma$ from the measured central
position of the galaxy, using the method of Webbink (1985) to estimate
the uncertainties.  We note that this is an inherent uncertainty in
the galaxy's center when measured from stellar light due to the finite
number of bright stars.

Recent work has suggested that the dwarf spheroidal galaxies might
actually have black holes substantially larger than 1/1000 of their
total mass, if they are the remnants of Population III stars and they
began accreting rapidly soon after forming, and contributed to
re-ionizing the universe (Ricotti \& Ostriker 2004).  Given this
suggestion, we have repeated the calculations of Maccarone (2004), for
black holes of 0.1\%, 1\% and 10\% of the galaxy's mass.  We retain
the assumption made for globular clusters that the gas density should
be about 0.15 H cm$^{-3}$.  This is likely to be an overestimate, as
the dwarf spheroidal galaxies are less dense than globular clusters
and their gas should be more spread out, but we note that at the
present, the constraints on gas densities of dwarf spheroidal galaxies
are rather poor (see e.g. Gallagher et al. 2003).  As we find that for
a fraction of the Bondi rate of $10^{-2}$ the radio flux levels are
all substantially higher than could possibly be allowed by the
observations, we make calculations for only $10^{-3}$ of the Bondi
rate.  We find that the three predicted radio fluxes are 1.7 mJy, 510
mJy, and 97 Jy, respectively.  The predicted X-ray luminosities are
$7\times10^{34}$ ergs/sec, $5\times10^{37}$ ergs/sec, and
$1.5\times10^{40}$ ergs/sec.  We note that {\it Einstein} observed the
Ursa Minor dwarf for about 5.5 kiloseconds, and detected no sources
with positions coincident with the NVSS source.  The upper limit of
those observations was $\sim$$10^{35}$ ergs/sec, if at the distance of
the Ursa Minor galaxy (Markert \& Donahue 1985; see also ROSAT upper
limits at a similar flux level from Zang \& Meurs 2001).  These data
are thus all in accord with a black hole of about 40000 $M_\odot$; if
the gas density is $\sim30$ times lower than in the globular clusters,
then a black hole mass about 4-5 times as large can be accomodated.

\subsubsection{The other dwarf spheroidal galaxies}
To determine the false source probability, we have also looked at the
NVSS catalog around the center of the Ursa Minor galaxy with a search
radius of 20 arcminutes.  In this region, 20 sources are found,
leaving a spurious source probability of about 5\% under the
assumption that any source within 1 arcminute of the center of the
galaxy (the 3$\sigma$ error circle) would be a candidate central IMBH.
We argue that there are few hidden trials here by noting that we would
not expect to detect most of the other Milky Way dwarf spheroidals;
scaling the flux from the Ursa Minor dwarf galaxy, the only other
dwarf spheroidal galaxies massive enough and near enough and far
enough North to be detected in the NVSS are those in Draco,
Sagittarius, Sextans and Fornax, and none of these are detected.  The
other four Milky Way dwarf spheroidal galaxies are those in Sculptor
and Carina (which are too far south to have been observed by the VLA);
and Leo I and Leo II, which are at distances of 205 and 250 kpc,
respectively, and have masses of about half the mass and the same mass
of the Ursa Minor, respectively, leading to fluxes expected to be
about 100 times and about 15 times lower than Ursa Minor's, assuming
that $L$$\propto$$M^{3.2}$, as explained above.

Draco's flux would be expected to be a factor of about 2 lower than
that of the Ursa Minor dwarf because of its greater distance (82 vs 66
kpc), while the Sextans galaxy is further than Draco (86 kpc) and less
massive (by about 20\%), their expected fluxes are thus pushed into
the region where the NVSS suffers from serious incompleteness effects.
The expected flux of Sagittarius would be quite hard to determine; if
the mass is assumed just to be the mass in M~54, the globular
cluster-like object thought to be the core of the Sagittarius dwarf
galaxy, then the calculation of Maccarone (2004) is valid and the
expected flux should be only a few microJanskys.  If, on the other
hand, one scales from the mass of the dwarf, then the fact that this
galaxy is in the process of being tidally destroyed makes estimating
its mass quite difficult.  Furthermore, the gas in the Sagittarius
galaxy is likely to have been stripped during its ongoing encounter
with the Milky Way.  The Fornax dwarf is more problematic; assuming
that galaxy mass and distance are the only important parameters, this
galaxy should actually have a brighter radio source than does Ursa
Minor by a factor of about 3 (it is about 3 times as massive and about
twice as far away).  No detection was made in the NVSS within about 2
arcminutes of the galaxy's center, but a factor of 3 in flux is well
within the uncertainties of our calculations.  Furthermore, we note
that the hidden trial problem is less severe than 3 (to account for
the reasonable chance of detecting a radio source in the centers of
Ursa Minor, Draco \& Fornax) times 5\% (the probability of detecting a
source by chance in the 3$\sigma$ error circle of the Ursa Minor
galaxy); the Ursa Minor galaxy has an error radius for its center
about ten times larger than those of Fornax and Draco, the two other
best candidates (largely because it has a much lower core stellar
density, so a small number of bright stars can affect its
center-of-light location much more); the false detection probabilities
in those galaxies are close to zero, so searching the other two
galaxies adds almost nothing to the probability of finding a source by
chance. We thus believe that the central IMBH hypothesis is more
likely than the background AGN hypothesis, but only marginally so, and
that the best way to make this identification more secure is by
localizing it well enoough to identify a unique optical counterpart to
the radio source, and then to take a spectrum of that object.

\section{Conclusions}

At present, we have shown merely that stricter observational upper
limits can be placed on the maximum mass of a possible accreting black
hole in globular clusters through measurements made in the radio than
through measurements made in the X-rays.  Under the assumptions which
most strictly constrain the presence of intermediate mass black holes
without violating other observational constraints, we can rule out the
presence of a black hole in Omega Cen larger than about 20 $M_\odot$ -
that is we can rule out the presence of an intermediate mass black
hole.  Under more realistic assumptions, though, we cannot rule out a
black hole of a few hundred solar masses.

One other additional caveat is that that accreted gas might have some
angular momentum and hence might form an accretion disk.  In this
case, gas might pile up at some outer radius, and then undergo
outbursts, much like the soft X-ray transients in the Milky Way.  In
this case, the assumption we have made that the instantaneous
accretion rate equals the time averaged accretion rate would be
violated, and substantially lower X-ray and radio luminosities might
be expected most of the time than those we have predicted.  However,
the interstellar gas would have to cool down and condense in order to
form an accretion disk.  This seems to be plausible in galaxies such
as the Milky Way, where there may exist a thin disk as a remnant from
a past strong accretion episode (Nayakshin 2003), but seems less
likely in a globular cluster where it is thought that any IMBHs would
have grown through mergers rather than accretion.

Upper limits which would truly constrain the theoretical suggestions
of Miller \& Hamilton (2002) are likely to come only with the Square
Kilometer Array, or possibly from extremely deep observations made by
the High Sensitivity Array or the Very Large Array.  In Maccarone
(2004), the 15 best candidates for detecting an intermediate mass
black hole through its radio emission; 13 of these are in the Southern
Hemisphere, including the 6 best candidates.  If the detection of
intermediate mass black holes in globular clusters is considered a key
science goal of SKA, then this provides a strong justification for
locating the array south of the equator.

One of the key causes for systematic uncertainty in these measurements
is the uncertainty in the gas density in any globular cluster or gas
poor galaxy which does not contain a large number of pulsars.  While
it is comforting to note that the two globular clusters which contain
large number of pulsars have gas densities in close agreement with the
predictions of stellar mass loss (Freire et al. 2001), passages
through the plane of the Galaxy can strip the clusters of most or all
of their gas, so this will not necessarily be the case in all stellar
systems.  In the ROSAT era, X-ray images were obtained of two of the
Milky Way's dwarf spheroidal galaxies in order to find background
quasars, primarily in order to establish an extragalactic reference
frame for astrometric studies of these galaxies, but it was also noted
that these objects might be useful as probes of the interstellar
medium in the dwarf galaxies, in much the same way that high redshift
quasars are used to study the Lyman $\alpha$ forest (Tinney, Da Costa
\& Zinnecker 1997), but it seems that this technique as not yet
produced any detections of gas.  If this technique can be taken better
advantage of, then it should be possible to convert upper limits on
radio emission from the cores of the dwarf galaxies directly into mass
upper limits in the same way as we have done for the globular
clusters; at the present time, it would be premature to do so, given
the greater uncertainties in the dwarf galaxies' gas densities.  It
should be noted that one dwarf galaxy, that in Scultptor (i.e. the
closest one) does have a substantial gas content (Bouchard, Carignan
\& Maschenko 2003), with a central density at least $10^{-3}$
cm$^{-2}$ in neutral gas, and higher concentrations off center, as the
gas distribution is asymmetric.  The suggestion above that the gas
density might be about 1/30 of that in the globular clusters is thus
in reasonable agreement with the data for the one galaxy with the best
observational constraints.

We have found suggestive evidence for an intermediate mass black hole
in the Ursa Minor dwarf spheroidal galaxy.  This should be followed up
first in X-rays, to determine whether its ``radio mass,'' to use the
terminology of Merloni et al. (2003) is of order $10^4 M_\odot$ before
a strong claim of a detection is made, and an optical counterpart
should be searched for as well.  Since the gas density is probably a
lower in this galaxy than in a typical globular cluster, the true mass
may be higher than suggested by the observed radio luminosity in the
context of our calculation, and hence closer to the $10^{6} M_\odot$
suggested by Riccotti \& Ostriker (2004).  If an X-ray source in the
$10^{33}-10^{35}$ ergs/sec range is found, the case for an
intermediate mass black hole would be strengthened dramatically, and
X-ray luminosities in the lower end of that range would be most likely
to indicate the highest mass black holes.

\section{Acknowledgments}
We thank Dave Meier for pointing out that SKA could be especially
useful for future work in this area.  We also are grateful to the
referee Heino Falcke for useful suggestions which have helped improve
the clarity and content of this paper, and to Eva Grebel for brief but
useful discussions of the gas content of dwarf spheroidal galaxies.

redpajama_set_name: RedPajamaArXiv


text:
Prominent ear, otapostasis or bat ear is an abnormally protruding human ear. It may be unilateral or bilateral. The concha is large with poorly developed antihelix and scapha. It is the result of malformation of cartilage during primitive ear development in intrauterine life. The deformity can be corrected anytime after six years of age. The surgery is preferably done at the earliest possible age in order to avoid psychological distress. Correction by otoplasty involves changing the shape of the ear cartilage so that the ear is brought closer to the side of the head. The skin is not removed, but the shape of the cartilage is altered. The surgery does not affect hearing. It is done for cosmetic purposes only. The complications of the surgery, though rare, are keloid formation, hematoma formation, infection and asymmetry between the ears.

See also
 Cauliflower ear
 Incisionless Fritsch otoplasty

References

Ear

redpajama_set_name: RedPajamaWikipedia


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LibriVox Audio Books
Subjects: Fiction, Historical Fiction
Collections: Literature, Sociology, Education, History, Uncle Tom's Cabin; by Harriet Beecher Stowe, Audio Books Collection
Uncle Tom's Cabin; or, Life Among the Lowly is a novel by American author Harriet Beecher Stowe which treats slavery as a central theme. Stowe was a Connecticut-born teacher at the Hartford Female Academy and an active abolitionist. The novel is believed to have had a profound effect on the North's view of slavery. First published on March 20, 1852, the story focuses on the tale of Uncle Tom, a long-suffering black slave, the central character around whose life the other characters—both fellow slaves and slave owners—revolve. The novel depicts the harsh reality of slavery while also showing that Christian love and faith can overcome even something as evil as enslavement of fellow human beings. (Summary from wikipedia) Note From the Reader: The listener is about to enter a world rich with diverse characters. In order to differentiate between the characters, the reader has given each, his/her own voice. As an adult male reader, however, the reader's representation of women and children will, necessarily be less than adequate. He asks for your indulgence....
White Company, The
Subjects: Fiction, Historical Fiction, Adventure
Collections: Military Science, Literature, Naval Science, Education, History, White Company, The, Audio Books Collection
Set during the Hundred Years' War with France, The White Company tells the story of a young Saxon man who is learning what it is to be a knight. Raised by Cistercian Monks and rejected by a violent elder brother, Alleyn Edricson takes service with one of the foremost knights in the country. When Alleyn falls in love with the knight's daughter, he must prove himself to be a courageous and honourable knight before he can win her hand. Alleyn and his friends set forth with the other men-at-arms to join Prince Edward in Bordeaux, from where they will take part in the Prince's campaign into Spain. It is in Spain that Alleyn and others must prove themselves to be very valiant and hardy cavaliers. (Summary by Clive Catterall)...
Historical Fiction, Adventure, War stories
Rasselas, Prince of Abyssinia
Subjects: Fiction, Adventure, Historical Fiction
Collections: Literature, Language, Law, Sociology, Education, History, Philosophy, Rasselas, Prince of Abyssinia, Audio Books Collection
In this enchanting fable (subtitled The Choice of Life), Rasselas and his retinue burrow their way out of the totalitarian paradise of the Happy Valley in search of that triad of eighteenth-century aspiration - life, liberty and happiness. According to that quirky authority, James Boswell, Johnson penned his only work of prose fiction in a handful of days to cover the cost of his mother's funeral. The stylistic elegance of the book and its wide-ranging philosophical concerns give no hint of haste or superficiality. Among other still burning issues Johnson's characters pursue questions of education, colonialism, the nature of the soul and even climate alteration. Johnson's profoundest concern, however, is with the alternating attractions of solitude and social participation, seen not only as the ultimate life-choice but as the arena in which are played out the deepest fears of the individual: Of the uncertainties of our present state, the most dreadful and alarming is the uncertain continuance of Reason." (Summary by Martin Geeson)...
Adventure, Historical Fiction, Literature, Romance, Travel
Fabiola or The Church of the Catacombs
Cardinal Nicholas Patrick Wiseman
Subjects: Fiction, Historical Fiction, Religion
Collections: Literature, Sociology, Religion, Education, Finance, Criminology, History, Fabiola or The Church of the Catacombs, Audio Books Collection
This historical novel is set in Rome in the early 4th century AD, during the time of the cruel persecution of Christians under the Emperor Diocletian The heroine of the book is Fabiola, a young pagan beauty from a noble Roman family. Fabiola seems to have everything, including a superior education in the philosophers, yet under the surface, she is not content with her life. One day, in a fit of rage, she attacks and wounds her slave girl Syra, who is a secret Christian. The proud, spoiled Roman girl is humbled by Syra's humility, maturity and devotion to her in this situation, and a slow transformation begins. Woven into this fictitious story are a number of martyrdom accounts of real-life Christian saints, including Saint Agnes, Saint Tarcisius and Saint Sebastian. Cardinal Wiseman wrote Fabiola in part as an answer to the vigorously anti-Catholic book Hypatia by Charles Kingsley. The novel was mainly aimed at the embattled Catholic minority in England, who had recently emerged from a half-illegal status. (Summary adapted from Wikipedia)...
Historical Fiction, Religion
Ben-Hur: A Tale of the Christ
Lew Wallace
Collections: Military Science, Literature, Sociology, Naval Science, Education, History, Ophthalmology, Ben-Hur: A Tale of the Christ, Audio Books Collection
Ben-Hur is a story of two very different heroes. Judah Ben-Hur, a prince of Jerusalem, is involved in an accident to the Roman procurator which is taken to be intentional. He is seized and sent to the fleet as a galley-slave, while his family is imprisoned and the family goods confiscated. When Ben-Hur saves the fleet captain from drowning after his ship is sunk in a fight with pirates, that officer adopts him as son and heir. With Roman training, Ben-Hur distinguishes himself in the arena and the palistrae and appears to be on the way to high military command.With the help of a faithful family retainer and a generous Arab sheik, Ben-Hur is enabled to take part in a widely touted chariot race, where one of the other charioteers is the boyhood friend who connived to punish him for the accident and split his estate. That rival is crippled, financially and bodily, in a no-holds-barred race (memorable from the 1959 movie with Charlton Heston).Ben-Hur turns his attention to the prophesied King of the Jews, when through the sheik he meets Balthasar, one of the Three Wise Men, and hears of the child born years ago. Will Ben-Hur be the gene...
Historical Fiction, Adventure
Yankee Girl at Fort Sumter, A
Alice Turner Curtis
Subjects: Fiction, Children, Historical Fiction
Collections: Political Sociology, Military Science, Literature, Sociology, Naval Science, Education, Political Science, History, Yankee Girl at Fort Sumter, A, Audio Books Collection
Sylvia Fulton is a ten-years-old girl from Boston who stayed in Charleston, South Carolina, before the opening of the civil war. She loves her new home, and her dear friends. However, political tensions are rising, and things start to change. Through these changes, Silvia gets to know the world better: from Estrella, her maid, she starts to understand what it is to be a slave, from her unjust teacher she learns that not all beautiful people are perfect, and from the messages she carries to Fort Sumter she learns what is the meaning of danger. However, this is a lovely book, written mostly for children.(Summary by Stav Nisser)...
Children, Historical Fiction, Teen/Young adult, War stories
Prime Minister, The
Subjects: Fiction, Historical Fiction, Politics
Collections: Political Sociology, Finance Management, Literature, Sociology, Government, Education, Political Science, History, Prime Minister, The, Audio Books Collection
The Prime Minister is the fifth in Trollope's series of six Palliser novels. With Phineas' difficulties resolved, Trollope introduces new characters. A respectable young girl forsakes the man her family had always intended her to marry when she falls in love with a man of foreign extraction and an unknown family. He has a gentleman's education and manners, but his family background and financial means are mysterious. Is he really a gentleman? Meanwhile, Plantagenet Palliser becomes Prime Minister of a shaky coalition government, and Glencora and Madame Goessler are busy with the ensuing social obligations. (Summary by Karen Merline)...
Historical Fiction, Politics, Romance

redpajama_set_name: RedPajamaCommonCrawl


Since January 2014, Fresno County has issued over 2,800 well drilling permits with few restrictions despite the adverse impacts of these new wells on rural residents in our fourth year of severe drought. With thousands of dry household wells in the San Joaquin Valley, our counties need to do a better job monitoring well drilling and addressing the negative impacts of virtually unrestricted groundwater pumping. At the Board of Supervisors meeting, Kristin Dobbin of the Community Water Center, Leticia Corona of Leadership Counsel for Justice and Accountability, and Austin Hall of the Fresno Regional Partnership attended to testify in support of applying for state funding to develop an interim groundwater ordinance.
By voting to include funding for the development of a groundwater ordinance, the Board of Supervisors took a huge step forward towards protecting our most vulnerable residents and setting the County on the path towards sustainable groundwater management, as mandated by the new Sustainable Groundwater Management Act. Once the funding application is approved, our next step will be to work with Fresno County to ensure the interim groundwater ordinance adequately protects our valuable groundwater resources and prioritizes the human right to water.


text:
Franz Joseph, Prince of Hohenzollern-Emden
Franz Joseph Maria Ludwig Anton Thassilo Prinz von Hohenzollern-Emden[1][2][3] (English: Prince Francis Joseph of Hohenzollern-Emden; 30 August 1891 – 3 April 1964) was a member of the Roman Catholic branch of the House of Hohenzollern. He was born as Prince Franz Joseph of Hohenzollern and adopted the surname Prinz von Hohenzollern-Emden in 1933.
Prince Franz Joseph
(1891-08-30)30 August 1891
Heiligendamm, Grand Duchy of Mecklenburg-Schwerin
3 April 1964(1964-04-03) (aged 72)
Tübingen, Baden-Württemberg, Germany
Princess Maria Alix of Saxony
Prince Karl Anton
Prince Meinrad Leopold
Princess Maria Margarethe
Prince Emanuel Joseph
Franz Joseph Maria Ludwig Anton Thassilo
Hohenzollern-Sigmaringen
William, Prince of Hohenzollern
Princess Maria Teresa of Bourbon-Two Sicilies
Early lifeEdit
Franz Joseph was born in Heiligendamm in the Grand Duchy of Mecklenburg-Schwerin,[2][3] the second son of Wilhelm, Prince of Hohenzollern and Princess Maria Teresa of Bourbon-Two Sicilies. He had a twin brother, Frederick, Prince of Hohenzollern, who was born a few minutes before he was.
Military serviceEdit
During World War I Franz Joseph served in Germany's Kaiserliche Marine (Imperial Navy) as the second torpedo officer on the light cruiser SMS Emden at the Battle of Cocos.[4] The SMS Emden had an extraordinary record capturing British ships, and as a result all those who served on her, including Franz Joseph, were given the right to add the ship's name to the end of their surnames.[5][6] Since Germany had converted titles of nobility into family names in 1919, he became Franz Joseph Prinz von Hohenzollern-Emden.[2][3]
In 1925 Franz Joseph wrote a book recording his naval service, Emden: Meine Erlebnisse auf S.M Schiff Emden (Leipzig: Eckstein, 1925), translated into English and published as Emden: My Experiences in S.M.S. Emden (reprinted as Emden: The Last Cruise of the Chivalrous Raider, 1914, Brighton: Lyon, 1989, ISBN 0-904256-45-6).
Franz Joseph also had the rank of Konteradmiral in the Romanian Naval Forces.[7]
Nazi Party membershipEdit
In 1933 Franz Joseph became a member of the SS (member number 276 691).[8] On 1 April 1936, he became as full member of the Nazi party with membership number 3765580.[9] As a leading Roman Catholic nobleman and a near relative of the Habsburg, Bourbon, and Saxon dynasties, Franz Joseph did much to lend respectability to the Nazi party.[10][11][12]
From 1939 to 1944 Franz Joseph commanded a marine flak battery at the Cuxhaven naval base.[13] In June 1944 he was released from active service. In November 1944 he was expelled from the SS together with other upper class Nazis whose devotion was becoming suspect in the face of Germany's, by then, near-certain defeat.[14] In a letter to Heinrich Himmler dated 3 January 1945, Franz Joseph proclaimed his continued devotion to the Nazi cause and unsuccessfully begged to be readmitted to the SS.[14]
Marriage and familyEdit
On 25 May 1921, Franz Joseph married Princess Maria Alix of Saxony, a daughter of Friedrich August III of Saxony and Archduchess Luise, Princess of Tuscany.[2][3] His twin brother was married to Maria Alix's sister, Princess Margarete Karola of Saxony.
Franz Joseph and Maria Alix had four children:[2][3]
Karl Anton Friedrich Wilhelm Ludwig Maria Georg Manuel Rupprecht Heinrich Benedikt Tassilo Prinz von Hohenzollern-Emden; born on 28 January 1922 in Munich, Bavaria, Germany; died on 3 November 1993 in Hechingen, Baden-Württemberg, Germany; married in Rome, Italy on 15 August 1951 to Alexandra Afif (16 November 1919 - 26 June 1996)[2][3]
Meinrad Leopold Maria Friedrich Christian Ferdinand Albert Prinz von Hohenzollern-Emden; born on 17 January 1925 in Sigmaringen, Baden-Württemberg, Germany; died on 9 September 2009 in Murnau Hechendorf, Germany; married (civil) in Frankfurt, Germany on 25 August 1971 and (religious) in Sigmaringen on 11 September 1971 to Edina Freijn von Kap-Herr (born 23 August 1938[2][3]
Maria Margarethe Anna Viktoria Luise Josephine Mathilde Theresia vom Kinde Jesu Prinzessin von Hohenzollern-Emden; born on 2 January 1928 in Sigmaringen, Baden-Württemberg, Germany; died on 4 August 2006 in Hechingen, Baden-Württemberg, Germany; married (civil) in Hechingen 18 December 1965 and (religious) at Burg Hohenzollern, Hechingen on 18 December 1965 to Duke Carl Gregor of Mecklenburg, second son of George, Duke of Mecklenburg head of the House of House of Mecklenburg-Strelitz[2][3]
Emanuel Joseph Maria Wilhelm Ferdinand Burkhard Prinz von Hohenzollern-Emden; born in Munich, Bavaria, Germany on 23 February 1929; died in Hechingen, Baden-Württemberg, Germany on 8 February 1999; married (civil and religious) at Burg Hohenzollern on 25 May 1968 to Katharina Feodora Adelheid Sabine Sophie Felicitas Sieglinde, Princess of Saxe-Weimar-Eisenach (born 30 November 1943) a granddaughter of William Ernest, the last Grand Duke of Saxe-Weimar-Eisenach; divorced in 1985[2][3]
Franz Joseph lived with his family at Villa Eugenia in Hechingen.[15]
Franz Joseph died on 3 April 1964 at Tübingen, Baden-Württemberg.[2][3] He and his wife are buried in the Erlöserkirche in Sigmaringen.[16]
AncestryEdit
Ancestors of Franz Joseph, Prince of Hohenzollern-Emden
8. Karl Anton, Prince of Hohenzollern
4. Leopold, Prince of Hohenzollern
9. Princess Josephine of Baden
2. William, Prince of Hohenzollern
10. Ferdinand II of Portugal
5. Infanta Antónia of Portugal
11. Maria II of Portugal
1. Franz Joseph, Prince of Hohenzollern-Emden
12. Ferdinand II of the Two Sicilies
6. Prince Louis, Count of Trani
13. Archduchess Maria Theresa of Austria
3. Princess Maria Teresa of Bourbon-Two Sicilies
14. Duke Maximilian Joseph in Bavaria
7. Duchess Mathilde Ludovika in Bavaria
15. Princess Ludovika of Bavaria
^ Prinz von Hohenzollern-Emden, Franz Joseph (1914). Emden: the Last Cruise of the Chivalrous Raider-1914. Brighton, England: Lyon Publishing. pp. i. ISBN 0-904256-45-6.
^ a b c d e f g h i j Darryl Lundy (10 May 2003). "Franz Joseph Prinz von Hohenzollern-Sigmaringen". thePeerage.com. Retrieved 2008-12-28.
^ a b c d e f g h i j Paul Theroff. "HOHENZOLLERN". Paul Theroff's Royal Genealogy Site. Archived from the original on 2009-04-28. Retrieved 2008-12-28.
^ Ray Riling Arms Books review of EMDEN - THE LAST CRUISE OF THE CHIVALROUS RAIDER, 1914. Retrieved on 2008-10-26.
^ Revell 1/350 SMS Emden, previewed by Kyle Bodily Archived 2009-01-20 at the Wayback Machine Retrieved on 2008-10-26
^ "Junk-Emden". Time Magazine. 1929-05-06. Retrieved 2008-10-25.
^ Stammbaum der Hohenzollern
^ Höhne, Heinz Zollin; Barry, Richard (2001), The Order of the Death's Head: the Story of Hitler's SS, p. 129, ISBN 0-14-139012-3
^ Petropoulos, Jonathan (2006), Royals and the Reich, Oxford: Oxford University Press, p. 383, ISBN 0-19-533927-4
^ Burleigh, Michael; Wipperman, Wolfgang (November 29, 1991). The Racial State: Germany, 1933-1945. New York: Cambridge University Press. p. 274. ISBN 978-0-521-39114-6.
^ Mayer, Arno J. (March 17, 1990). Why Did the Heavens Not Darken?. New York: Pantheon. p. 139. ISBN 978-0-679-72899-3. Perhaps most controversial work of Marxist historian Arno J. Mayer, but the fact that he has been professor at Wesleyan University (1952-1953), Brandeis University (1954-1958) and Harvard University (1958-1961), before settling at Princeton in 1961 (where he is now Dayton-Stockton Professor of History, Emeritus), and the fact that publisher Pantheon is a division of Random House (one of the world's largest publishers) give credence to his scholarship if not his conclusions. None of the criticism of Why Did the Heavens Not Darken? challenged his statement that the Nazi nobility, among who he specifically cites Hohenzollern-Emden, gave valuable support and prestige to the Nazi movement.
^ Thomas, W Hugh (March 22, 2002). The strange death of Heinrich Himmler: a forensic investigation. New York: St. Martin's Press. p. 32. ISBN 0-312-28923-5.
^ Lohmann, Walter; Hildebrand, Hans H. (1956). Die deutsche Kriegsmarine 1939 - 1945. 3. Bad Nauheim, Hessen, Germany: Podzun-Verlag. |access-date= requires |url= (help)
^ a b Petropoulos, 425.
^ Genealogisches Handbuch des Adels, Fürstliche Häuser VIII (1968): 75.
^ Hohenzollern-Sigmaringen
Works by or about Franz Joseph, Prince of Hohenzollern-Emden at Internet Archive
Retrieved from "https://en.wikipedia.org/w/index.php?title=Franz_Joseph,_Prince_of_Hohenzollern-Emden&oldid=906454224"


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The Frank J. Tyler House is a historic house at 240 Linden Street in Waltham, Massachusetts.

Overview
Built in 1894, this -story wood-frame house is one of Waltham's finest Queen Anne Victorians. It is particularly distinguished by its elaborate three-story tower, which has a conical roof and bands of decorative shingles. The main entry is framed on the left by the tower, and on the right by a polygonal bay that rises a full two stories, and is capped by a squared-off projecting gable. The gable tympanum is filled by a three-bay window and clad in decorative cut shingles. The main entry is sheltered by a porch supported by paired Tuscan columns. The paneled door is flanked by sidelight windows and topped by a transom window.

Despite its location in a fashionable neighborhood of the city and the relatively high quality of its construction, the house was used as a rental property, passing through a large number of nonresident owners until 1907. Frank J. Tyler, who subdivided his property and built it on speculation, was a Boston-based manufacturer of agricultural machinery.

The house was listed on the National Register of Historic Places in 1989, where it is listed at 238 Linden Street.

See also
National Register of Historic Places listings in Waltham, Massachusetts

References

Houses in Waltham, Massachusetts
Houses on the National Register of Historic Places in Waltham, Massachusetts
Queen Anne architecture in Massachusetts
Houses completed in 1894


Pakistanis are taking their fight against US poodle Pervez Musharaff to the internet in the face of mounting attacks on press freedom and free assembly. This is new media taken to a level infinitely higher than the mad drive to raise Page Ranks or shore up Google Adsense earnings.
Musharaff's muzzling of the press and the consequent ban on rallies have compelled Pakistani's to be more creative and more daring, and the internet has become a virtual campaign center where protests are announced and vital news are spread for all the world to see.
The most popular Facebook protest group for Pakistan is "We Oppose Emergency in Pakistan", which had 11,471 members as of Sunday.
One of its members announces a candlelight vigil in Lahore, giving just a few hours' notice.
"This is the time when we the future of the country can act. It is our future that is in jeopardy and it's our country that needs our support," says the Facebook user.
The group has links to protest blogs, pictures of rallies and a mass petition (http://www.gopetition.com/online/15064.html) with nearly 16,000 signatures calling for the restoration of the constitution.
Users can also click on videos showing the final transmission by Geo, the country's leading news channel, and a recording made in hiding by Khan before his arrest.
Another Facebooker posts a link from the group to his own petition to free Khan, who was detained by police on Wednesday while trying to ignite a student protest movement against Musharraf — although it has yet to be signed.
Pakistanis have also turned to blogs as a political tool, with one (http://emergencypk.blogspot.com/) being the major premier alert service for demonstrations.
Others circulate mobile phone text messages—perhaps one of the most effective means of dissent with more than 70 million cell phones nationwide, said Adnan Rehmat, who heads Internews Pakistan, a Washington-based media watchdog group.
The protest yesterday at LUMS will go down as the dawn of a new era in this country's history. It will, God Willing, mark the end of the debilitating cynicism and social apathy that has afflicted the people of this country and led to the crossroads we find ourselves at today. Even in the darkness that engulfs us, our voices are being heard, people are joining the movement. Even as we speak, civil society is organizing. Students from Punjab University, LSE, BNU, Quaid-e-Azam University, UET, GIKI, Bahria and others are all standing up in protest. The students have awoken. The rest of civil society is on its way, even as the political parties awake.
Attempting to fill the void created by the suppression of the press is the blog Pakistan Blackout which provided updates on protests led by lawyers, including a link to a video address by the Chief Justice of the Supreme Court. FAST Rising reports on a very recent protest vigil.
Published by Academics for Freedom is an essay on how to help and how to understand the Pakistani situation.


"I am human. One of billions but unique." This simple book is full of "I am" statements that establish the brown-skinned boy character as being important. His statements of all he can do also promote empathy and finding his way in the world. The book is simple enough for a toddler to enjoy but good for an older child to ponder as well.


Home › Age 6-9 › Muffy Turns One: The Mini Tour – COVER REVEAL!
Muffy Turns One: The Mini Tour – COVER REVEAL!
Today I get to kick off blog tour celebrating the one year birthday of a great story about a little dog and her great adventure. Since I am the first stop on this mini tour, I get to reveal the cover!
Synopsis (from the publisher) – Muffy is a happy and curious Goldendoodle puppy who lives on a farm. One day she chases a silly grasshopper and gets lost. She finds herself alone and hungry, on the point of collapse, but luck is on her side and she is adopted by a wonderful family, the Gabriels, who have a very orderly and devoted pack of dogs. Muffy becomes part of her new family, and is accepted by Radar and Oliver and the gang, but she still pines for her sister, Riff, and misses the farm. One of her new friends, Wise Dog, introduces her to a very unusual Dog Catcher who has a special talent.
Muffy's courageous journey is full of laughter and adventure as she tries to unite her two families.
The cover is in the same style as the other illustrations in the book. The whimsical illustration style adds depth to the story. I found Robitalle's story-telling to be thoughtful and entertaining. The story is so much more than a lost puppy story. There are shades of lessons on the struggles of growing up, what family truly is and also diversity. It is a rich and well crafted book that packs a lot in the 65 pages of text!
Visit the Hologram Library Website by clicking HERE!
Muffy sounds sweet. Plus one of my best friends is a goldendoodle puppy! His name is Sonny, but I call him Sunny. Wait. What?
That's a wonderful cover. Looking forward to seeing more of the illustrations!


If you are going to add a contract heal and toe, see the add heal and toe instructions.
Turn the cuff right side out. Press stocking.
At this point you can add a decorative cuff or finish the stocking.
Stocking Pattern for top Cuff This will add a 4.5 inch top cuff to your stocking.
Stocking Pattern contrast pointed heal and toe.
Stocking Pattern small elf toe.
Stocking Pattern large elf toe.


text:
Home » Alternatives » 10+ Amazing Whatsapp Alternatives and Competitors for 2023
10+ Amazing Whatsapp Alternatives and Competitors for 2023
One of the most popular apps used on today's date is WhatsApp. The cross-messaging platform has over a billion users, and the numbers have just looked up.
WhatsApp somehow has become an integral part of our lives in such a way that without WhatsApp, life has started seeming difficult.
Headquarters: Menlo Park, California, United States
Launched in 2009, WhatsApp was an immediate success. The downloads were rising exponentially as more and more people started using the app.
It rose so high that now, almost every person with a smartphone has WhatsApp. Downloading WhatsApp now is sort of a ritual and not a choice.
WhatsApp has many features like text messaging, group messaging, video calling, and audio calling options. One can send all media types with WhatsApp, like audio, videos, and documents. It comes in with an integrated camera option to capture images and record videos to send them in real time.
However, after its merger with Facebook, WhatsApp's privacy has recently been questioned quite often, leading some users to shift to other platforms.
Pros– audio and video-calling features, live location sharing
Cons– no virtual assistant, takes up a lot of storage
Best Whatsapp Alternatives You can Use for Privacy and Safety:
Google Messages
Bridgefy
What is the best alternative to WhatsApp?
What are some free alternatives to WhatsApp?
Which app is the most attractive alternative to Whatsapp?
Do we need an account to use Whatsapp?
Alternatives are needed with various issues cropping up lately and crippling WhatsApp's image! We are here to help. Here are some of the best WhatsApp alternatives one could have asked for!
Headquarters: Mountain View, California, United States
Relatively new to the competition, Signal is a rock-solid W alternative. Founded by Signal Foundation (responsible for providing WhatsApp and Facebook with encryption), Signal is one of the most secure and simplest alternatives to WhatsApp.
It is so particular about its security concerns that every file sent or received, every conversation, and every backup is encrypted and secured in Signal.
The best part is that Signal provides all these features without compromising on their features.
One can do video and audio calls, send files and perform every other important activity that WhatsApp can, making it one of WhatsApp's biggest competitors.
Pros– fully open-sourced, supports audio chat.
Cons– requires a lot of personal information before starting, not widely known.
Headquarters: Dubai, United Arab Emirates
Arguably, WhatsApp's biggest nemesis to date, Telegram, is an open-source cross-messaging platform.
Telegram packs in all the essential features that WhatsApp has. However, certain factors give Telegram an easy, competitive edge over WhatsApp.
With Telegram, one can create groups with up to 10000 people onboard and send files up to 1.5 GB in size.
Moreover, there is a feature of self-destructing texts and end-to-end encryption. With minute security compromises as compared to the features, Telegram is one of the best WhatsApp alternatives.
Pros– one of the most secure apps of its kind, personal servers
Cons– does not support voice chats, has unnecessary ads
Headquarters: San Francisco, California, United States
A platform initially designed for gamers to connect with their fans and streams, Discord has now become one of the best WhatsApp alternatives.
One can use Discord's personal messages center to chat and send audio, media, and even documents, for say.
Users can even make calls via audio or video medium and share screens to enjoy the content. With integrations from Spotify, Twitch, Steam, Reddit, and many more, Discord has covered the user in all aspects, making it a great WhatsApp alternative.
Pros– fun and interactive servers, the convenience of creating personal servers
Cons– chat rooms are extremely crowded sometimes.
Headquarters: Luxembourg, Europe
Another great but underrated alternative to WhatsApp is Viber. With its feature set, Viber deserves to have a huge user base.
Offering every feature that WhatsApp has to offer, except for the part of payments, Viber goes one step ahead to pack in a multi-device support feature, which WhatsApp lacks.
Viber also offers a premium feature Viber Out, that allows users to make international calls at nominal rates, even to non-Viber users. Packing in a great package, Viber is a seriously good alternative to WhatsApp.
Pros– easy method of use, minimalist interface
Cons– lacks a lot of useful features and needs regular updates.
Headquarters: Pfaffikon, Zurich, Switzerland
Swiss-based platform Threema is another great alternative to WhatsApp. With security being Threema's main objective, it offers encryption for almost every process that a user executes.
It also offers encryption for backups and does not collect any metadata. With Threema, one can access unique features like fingerprint or password-protected conversations. If security is a major concern, then for those users, Threema is the best alternative to WhatsApp.
Pros– secure encryption protocols, easy to use
Cons– interface can be optimized in a better way
Headquarters: Luxembourg
Founded in 2003 by Microsoft, Skype is a great alternative to WhatsApp. At one point in time, Skype was used only for video calling purposes.
However, after all the updates, Skype can now work as a full-fledged cross-messaging tool as well. Group calls and chats are Skype's biggest USP.
That also leads to Skype being a very popular tool when it concerns businesses.
Pros– one of the best for professional use, smooth video calling features
Cons– camera malfunctions sometimes, needs optimizations
Headquarters: Berlin, Germany
Founded and headquartered in Switzerland, Wire came into existence when some Skype employees quit Skype to start their own platform. The wire is reputed to be one of the safest social platforms.
It can perform almost every action that WhatsApp does. Moreover, Skype also has features like end-to-end encryption and multiple account support, which WhatsApp lacks.
Pros– reliable privacy protocols, easy to use
Cons– lacks some basic features; updates are required.
Headquarters: Herzliya, Tel Aviv, Israel
Until now, we have discussed alternatives with the same professional approach as WhatsApp. However, Spike is different. With Spike, professionalism is retained but in a more interactive and fun way.
Spike looks more like a chat than an email service. Spike's biggest advantage is that it looks way more attractive than any other WhatsApp on this list and its free package almost completes the work. All these make Spike a pretty good alternative to WhatsApp.
Pros– very convenient for business purposes, clean interface
Cons– has some optimization issues
A very good alternative to WhatsApp, Google Messages' biggest priority is the users and their privacy. A very simple-to-use interface, Google Messages, is the easiest to use.
It offers end-to-end encryption and also features like exchanging messages with one another, sharing files, and audio notes. However, what it lacks are the calling features.
Pros– safety protocols are reliable, perfect for professional use
Cons– could be made more user-friendly
Headquarters: California, United States
Bridgefy is a very interesting application to use. Bridgefy eliminates the biggest factor that WhatsApp is barred from; Internet Connectivity. Bridgefy allows one to text based on Bluetooth and wi-fi connectivity up to a certain range.
One can send messages to a friend and broadcast them to the entire group. It can even share media files over the broadcast and mesh network. It is one of the best WhatsApp alternatives in the offline mode though, which makes it stand out.
Pros– easy file sharing, has almost all the basic features
Cons– interface can be made more user-friendly
Based on their feature sets, Telegram, Viber, and Signal are the closest when it comes to battling WhatsApp out.
Telegram Messenger is clearly the best free-to-use alternative to WhatsApp.
Spike and Viber Messenger are the most attractive alternatives to WhatsApp of all the above-mentioned applications.
No. One needs a phone number to use WhatsApp. However, adding a google account is needed for WhatsApp.
A Beginners Guide For WhatsApp Marketing for Small Businesses
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Research and related welfare information from the Heritage Foundation, a conservative policy think tank.
Located at the University of Chicago. Includes information on the official measures of, populations in, and myths of, poverty.
MDRC is a nonprofit, nonpartisan social policy research organization. We are dedicated to learning what works to improve the well-being of low-income people.
Walk a Mile brings together policymakers and people receiving public assistance to walk a mile in each other's shoes.
Background information and links on the Temporary Assistance for Needy Families (TANF) program and U.S. federal welfare policy generally.


Protecting your personal data and your general personal rights in collecting, processing and using your personal data is important to us. Accordingly, we are committed to complying with the data protection laws in place. We have briefly summarized for you what we do to protect your data and what using our online offering will entail for you.
The term "personal data" refers to information that is expressly collected and used in order to determine your identity. This includes your name, your postal mail or e-mail address, for example. We store personal data in addition to the access data only if you have provided them to us of your own free will, for example when you contact us to identify an appropriate partner for your needs. Other data are collected automatically by our IT systems when you visit the website. These data are primarily technical data such as the browser and operating system you are using or when you accessed the page. These data are collected automatically as soon as you enter our website.
In order to enable us to comply with our contractual obligations, we will sometimes forward your data to selected partner companies, who will then process these personal data on our behalf. These services include, to cite some examples, construction services for stands. Data will not be forwarded to third parties in any other way unless you have expressly agreed to this being done, or unless statutory provisions place us under obligation to forward them to public authorities.
Some of the websites operated by TEM will contain links to other websites or will otherwise tie in with them. While we use appropriate care in reviewing these direct links, TEM is not responsible for the content of the websites to which we have set a link. Exclusively the provider of the website to which a link was set will be held liable for illegal, erroneous or incomplete content as well as for damages resulting from the use of such information. Moreover, TEM is not responsible for the content of websites providing links to our pages.
TEM reserves the right to modify the present data protection guidelines at any time, subject to the requirements under data protection law.


text:
import dialogTests from './dialog.spec';
import formattersTests from './formatters.spec';
import localizationTests from './localization.spec';
import currentProjectTests from './projectId.spec';
import targetTests from './target.spec';

describe('Utils', () => {
  dialogTests();
  formattersTests();
  localizationTests();
  currentProjectTests();
  targetTests();
});

redpajama_set_name: RedPajamaGithub


Last Minute Healthy Holiday Tips!
It's here. Between the holiday parties and busier schedules, this time of year can be very challenging when it comes to nutrition and exercise. The average weight gain for healthy weight individuals is about 1-2 pounds and approximately 5 pounds for those who are overweight. Research shows that these pounds are stubborn and tend to stay on, especially if you don't seem to notice them. So what can you do to help avoid weight gain and minimize the bloat when constantly surrounded by sweets, rich foods and alcohol? Focus on balance and the little things that you can do each day!
Eat Regular, Balanced Meals Everyday (and don't forget the Protein & Fiber!). Eating regularly (about every 3-4 hours) is key for controlling your appetite, making healthy food choices and portion control. The last thing we need when we show up to a holiday party is to feel overly hungry. Protein and fiber are so important because they help balance blood sugars and increase satiety. Start the day off right with a balanced breakfast such as scrambles eggs with a side of berries, and a lunch or dinner of a salmon bowl loaded with veggies, and quinoa. Keep snacks handy such as nuts, string cheese, fruits, veggies, whole grain crackers and hummus.
Highlight Fruits & Veggies Everyday: Packed with fiber, potassium and water, fruits and vegetables will help fill you up without filling you out, as well as, decrease water retention from all of those high sodium foods. Consider buying veggie trays and/or fruit trays for your very own refrigerator so you can easily just grab and go. Keep them front and center so that you see them first and foremost.
Hydrate and Step it Up! Every single day- stay active! Step it up by avoiding escalators or elevators, aim for 10,000 steps. You can burn 100 calories in just a short 20 minute brisk walk. Find the furthest spot in the grocery store parking lot. It only takes 100 calories a day to lose 10 pounds in a year. Drink up (water that is!). Staying properly hydrated throughout the day is something proactive you can do each day to keep your metabolism burning efficiently, helps with energy levels and appetite control.
http://cherrycreeknutrition.com/wp-content/uploads/2017/12/bigstock-209478583.jpg 600 900 ccnutrition http://cherrycreeknutrition.com/2015/wp-content/uploads/2015/01/final-logo1.png ccnutrition2017-12-21 15:45:022018-01-26 15:12:58Last Minute Healthy Holiday Tips!


text:
Aleksandra Nina
Vladimir M. Čadež
Maša D. Lakić́ević
Milan R. Radovanović
Aleksandra B. Kolarski
Luka Č Popović
VARIATIONS IN IONOSPHERIC D-REGION RECOMBINATION PROPERTIES DURING INCREASE OF ITS X-RAY HEATING INDUCED BY SOLAR X-RAY FLARE
In this paper we present an analysis of parameters describing the effective recombination processes in the upper ionospheric D-region in the period of its additional heating by the X-radiation emitted during a solar X-ray flare. We present a procedure for calculation of the effective recombination coefficient and electron loss rate in the period when the X-radiation flux detected by the GOES satellite in the wavelength domain between 0.1 and 0.8 nm increases. The developed procedure is based on observational data obtained in the low ionospheric monitoring by the very low/low frequency (VLF/LF) radio waves and it is related to the considered area and time period. The obtained expressions are applied to data for the VLF signal emitted in Germany and recorded in Serbia during the solar X-ray flare detected by the GOES-14 satellite on May 5, 2010.
effective recombination coefficient, electron loss rate, ionospheric D-region, solar X-ray flares
DOI REFERENCE: https://doi.org/10.2298/TSCI190501313N
Singh, A.K., et al., Solar Flare Induced D-region Ionospheric Perturbations Evaluated from VLF Measurements. Astrophysics and Space Science, 350 (2014), pp. 1:1-9
Srećković, V.A., et al., The Effects of Solar Activity: Electrons in the Terrestrial Lower Ionosphere. Journal of the Geographical Institute "Jovan Cvijic" SASA, 67(2017), 3, pp. 221-233
Todorović Drakul, M., et al., Behaviour of Electron Content in the Ionospheric D-region During Solar X-ray Flares. Serbian Astronomical Journal, 193 (2016), pp. 11-18
Nina, A., et al., Diagnostics of Plasma in the Ionospheric D-region: Detection and Study of Different Ionospheric Disturbance Types. European Physical Journal D, 71 (2017), 7, pp. 189: 1-12
Nina, A., et al., Analysis of the Relationship Between the Solar X-ray Radiation Intensity and the D-region Electron Density Using Satellite and Ground-based Radio Data. Solar Physics, 293 (2018), pp. 64: 1-19
Uigman, V., et al., D-region Electron Density Evaluated from VLF Amplitude Time Delay During X-ray Solar Flares. Journal of Atmospheric and Solar-Terrestrial Physics, 69 (2007), pp. 775-792
Nina, A., Čadež, V.M., Electron Production by Solar Ly-α Line Radiation in the Ionospheric D-region. Advances in Space Research, 54 (2014), 7, pp. 1276-1284
Bajčetić, J., et al., Ionospheric D-region Temperature Relaxation and its Influences on Radio Signal Propagation after Solar X-flares Occurrence. Thermal Science, 19 (2015), Suppl.2, pp. S299-S309
Thomson, N.R. et al., Large Solar Flares and their Ionospheric D Region Enhancements. Journal of Geophysical Research (Space Physics), 110 (2015), pp. A06306: 1-10
Ferguson, J.A., Computer Programs for Assessment of Long-Wavelength Radio Communications, Version 2.0, Space and Naval Warfare Systems Center, San Diego, USA, 1998
Woods, T.N., et al., et al., New Solar Extreme-ultraviolet Irradiance Observations, The Astrophysical Journal, 739 (2011), 2, pp. 59: 1-13
Cohen, M.B., et al., Sensitive Broadband ELF/VLF Radio Reception With the AWESOME Instrument. IEEE Transactions on Geoscience and Remote Sensing, 48:3-17, January 2010.
Radovanović. M, Investigation of Solar Influence on the Terrestrial Processes: Activities in Serbia. Journal of the Geographical Institute "Jovan Cvijic" SASA, 68 (2018), 1, pp. 149 - 155
Wait, J.R., Spies, K.P., Characteristics of the Earth-ionosphere Waveguide for VLF Radio Waves, NBS Technical Note, CO, USA, 1964
Thomson, N.R, Experimental Daytime VLF Ionospheric Parameters. Journal of Atmospheric and Terrestrial Physics, 55 (1993), pp. 173-184
Grubor, D.P., et al., Classification of X-ray Solar Flares Regarding their Effects on the Lower Ionosphere Electron Density Profile. Annales Geophysicae, 26 (2008), pp. 1731-1740
Kumar, S., et al., Perturbations to the Lower Ionosphere by Tropical Cyclone Evan in the South Pacific Region. Journal of Geophysical Research: Space Physics, 122 (2017), pp. 8720-8732
Nina,A., et al., Altitude Distribution of Electron Concentration in Ionospheric D-region in Presence of Time-varying Solar Radiation Flux. Nuclear Instruments and Methods in Physics Research B, 279 (2012), pp. 110-113
Kolarski, A., Davorka Grubor, D., Sensing the Earth's Low Ionosphere During Solar Flares Using VLF Signals and GOES Solar X-ray Data. Advances in Space Research, 53 (2014), 11, pp. 1595 - 1602
McEwan M., Phillips, F., Chemistry of the Atmosphere, Mir, Moscow, Russia, 1978
Blaunstein N., Christodoulou, C., Radio Propagation and Adaptive Antennas for Wireless Communication Links: Terrestrial, Atmospheric and Ionospheric, John Wiley and Sons, Inc., Hoboken, New Jersey, 2006
Deshpande S.D., Mitra, A.P., Ionospheric Effects of Solar Flares - III. the Quantitative Relationship of Flare X-rays to SID's. Journal of Atmospheric and Terrestrial Physics, 34 (1972), 2, pp. 243 - 253
Hayes, L.A., et al., Pulsations in the Earth's Lower Ionosphere Synchronized with Solar Flare Emission. Journal of Geophysical Research: Space Physics, 122 (2017), 10, pp. 9841-9847
Mitra, A.P., Ionospheric Effects of Solar Flares, Mir, Moscow, Russia, 1974
Sato, T., The Response of the Lower Ionosphere to the Great Solar Flare of August 7, 1972. Journal of Geomagnetism and Geoelectricity, 27 (1975), 5, pp. 383-407
Osepian, A., et al., D-region Electron Density and Effective Recombination Coefficients During Twilight - Experimental Data and Modelling During Solar Proton Events. Annales Geophysicae, 27:3713-3724, October 2009.
Basak, T., Chakrabarti, S.K., Effective Recombination Coefficient and Solar Zenith Angle Effects on Low-latitude D-region Ionosphere Evaluated from VLF Signal Amplitude and its Time Delay During X-ray Solar Flares. Astrophysics and Space Science, 348 (2013), 2, pp. 315-326
Rowe, J.N., Model Studies of the Lower Ionosphere, Sci. Rep.No. 406, Pennsylvania State Univ., Univ. Park, USA, 1972, 1972.
Aikin, A.C., et al., Some Results of Rocket Experiments in the Quiet D Region. Journal of Geophysical Research, 69 (1964), pp. 4621-4628
Bourdeau, R.E., et al., The Lower Ionosphere at Solar Minimum, Greenbelt, Md.: NASA, Goddard Space Flight Center. 1965.


We also know it can be risky trying a salon for the first time. After all, who knows how good the staff really are, right? Visiting us is totally risk free. In fact, we are so confident you will leave looking and feeling a million dollars we personally GUARANTEE IT!
If in the unlikely event you are not delighted with the results of your service, we will not only redo it free, if needed we will also credit your account with a complimentary service.
WARNING: You must hurry, we can only give 20 of our best selling Package over the WHOLE YEAR and once they're gone….they're GONE until the next year!
Please note: Vouchers are downloadable through clickable link to voucher on screen or within your Email Confirmation, sent after payment made.
You can only click to download on the vouchers link(s) ONCE. Please make sure you can save the voucher or print it before clicking on the link. If multiple quantities are bought, for example, 2 x £10 voucher you can click the download link TWICE.
Alternatively you can click on the link whilst in the salon to show your voucher to a member of staff. If you have clicked on the voucher link and not saved, please tell a member of staff quoting your order number, so we can check against our system.


Stunning almost NEW home boasting 3,000 SF of living space with 4 bedrooms & 3.1 baths on a corner lot with 3-car garage. This classic craftsman design will wow you from the moment you enter- wide plank, classic grey solid oak hardwood floors throughout the home with chef's kitchen featuring custom white cabinetry, quartz countertops and stainless steel appliances including wine fridge. An oversized master suite includes a large walk-in closet with custom shelving and a spa-like bath with dual vanity, free standing tub and large walk in shower. 2 additional bedrooms offer a Jack & Jill bath and a 4th bedroom with private bath. This home is beautiful and will not last long!


text:
Q: Kernel and image of Linear Map between different bases of domain I have a basis B of $\mathbb{R^3}$ $\\{(1,2,3),(1,3,4),(1,3,5)\\}$
I have this matrix of a linear map F from basis B to canonical basis C of $\mathbb{R^3}$
$$
    \begin{pmatrix}
    6 & 9 & 12 \\
    2 & 3 & 5 \\
    0 & 0 & 0 \\
    \end{pmatrix}
$$
I calculated the same matrix from C to C
$$
    \begin{pmatrix}
    -3 & 0 & 3 \\
    -2 & -1 & 2 \\
    0 & 0 & 0 \\
    \end{pmatrix}
$$
I have to calculate kernel and image of F.
Calculating them from the second matrix I obtained:
$\text{Ker(F)}= \{x(1,0,1)\} $ and $\text{Im(F)}= \{x(-3,-2,0)+y(0,-1,0)\} $
My question is: can I calculate them directly from the first matrix?

A: Yes. The kernel are those vectors $v$ whose coordinates $x$; $y$, and $z$ with respect to the basis $B$ are such that$$\begin{bmatrix}6&9&12\\2&3&5\\0&0&0\end{bmatrix}.\begin{bmatrix}x\\y\\z\end{bmatrix}=\begin{bmatrix}0\\0\\0\end{bmatrix}.$$This is equivalent to$$\left\{\begin{array}{l}6x+9y+12z=0\\2x+3y+5z=0\\0=0.\end{array}\right.$$That is, the kernel is$$\left\{-\frac{3y}2\begin{bmatrix}1\\2\\3\end{bmatrix}+y\begin{bmatrix}1\\3\\4\end{bmatrix}\,\middle|\,y\in\mathbb R\right\}.$$
The image of $F$ is$$\left\langle\begin{bmatrix}6\\2\\0\end{bmatrix},\begin{bmatrix}9\\3\\0\end{bmatrix},\begin{bmatrix}12\\5\\0\end{bmatrix}\right\rangle.$$

redpajama_set_name: RedPajamaStackExchange


text:
Юрий Александрович Головашенко (28 ноября 1910, Кременчуг — 15 октября 1976, Ленинград) — русский советский театровед, доктор искусствоведения (1970).

Биография
Родился в 1910 году в городе Кременчуг Полтавской губернии Российской империи.

В 1937 году окончил театроведчекий факультет ГИТИСа, в 1940—1942 годах — аспирант там, в 1947 году защитил кандидатскую диссертацию.

Награжден медалью «За доблестный труд в Великой Отечественной войне 1941—1945 гг.».

С 1949 года — старший научный сотрудник и преподаватель в Ленинградском государственном институте театра, музыки и кинематографии.

В 1972 году присвоена научая степень доктора искусствоведения за книгу «Режиссерское искусство Таирова».

С июля 1974 по сентябрь 1976 года — старший научный сотрудник в Отделе новой русской литературы в ИРЛИ АН СССР.

Умер в октябре 1976 года в Ленинграде.

Труды
С 1938 года выступал как театральный критик и театровед. Автор ряда монографий и свыше 200 статей по истории театра.

Библиография
Отдельные издания:
 Героика гражданской войны в советской драматургии / Ю. А. Головашенко. — Л.: Советский писатель, 1957. — 357 с.
 Классика на цене: критические очерки / Ю. А. Головашенко. — М.: Искусство, 1964. — 300 с.
 Режиссерское искусство Таирова / Ю. А. Головашенко. — М.: Искусство, 1970. — 352 с.
 Многообразие реализма: сборник статей / Ю. А. Головашенко. — Л.: Искусство, 1973. — 285 с.
Публикации в периодике:
 Образ героя в драме и театре // сб.: Театральный альманах. — М., 1946. — с. 3 — 14
 Проблема героической драмы // Театр, № 2, 1958
 Проблема типического конфликта // Звезда, № 10, 1960
 Образ, В. И. Ленина на сцене // Звезда, № 1, 1960
 О многообразии реализма // Литература и искусство, № 19, 1944
 О специфике видов искусства // Литература и искусство, № 4, 1961
 Черты советского балета // Советская музыка, № 8, 1960
 Проблемы сценического истолкования «Горя от ума» // сб.: А. С. Грибоедов: Тв-во. Биография. Традиции. — Л.: ИРЛИ, 1977

Источники
 Головашенко Юрий Александрович // Театральная энциклопедия. Том 2 / Глав. ред. П. А. Марков — М.: Советская энциклопедия, 1963
 Головашенко Юрий Александрович // Энциклопедический словарь «Литераторы Санкт-Петербурга. XX век», 2015
Выпускники театроведческого факультета ГИТИСа
Театроведы СССР
Доктора искусствоведения
Сотрудники Пушкинского Дома


As discussed by our colleagues many states prohibit general business corporations from employing or contracting with physicians to provide medical services. This prohibition, known as the corporate practice of medicine prohibition, has existed as a public policy for nearly a century. The justification for this doctrine has always been to address concerns about business corporations and profit-maximizing interests interfering with the medical judgment of physicians in the treatment of patients. Depending on the state, the corporate practice of medicine prohibition may be found in statutes, regulations, board of medicine guidance, attorney general opinions, or case law.
Notably, the IRS had issued a similar ruling in 1996, which had allowed medical practices to join a health insurance company's consolidated tax group. However, the IRS later revoked that ruling after discovering that the ownership arrangements involved did not comply with the applicable state law. Interestingly, in the recent Ruling the IRS required a representation that "applicable law does not prohibit the beneficial ownership of stock" in the PCs by the subsidiary. Accordingly, although the Ruling is favorable from a tax perspective to management companies entering into friendly physician arrangements, parties to these transactions must still carefully structure such arrangements to comply with applicable state corporate practice of medicine restrictions. In addition, management companies should be aware that private letter rulings are limited to the specific question and fact pattern involved and may not be relied upon or cited by other taxpayers as precedent.


text:
Home » Lifestyle » Is Chinese Food Bad For You?
Is Chinese Food Bad For You?
Health organizations recommend limiting sodium and trans fat, which brings up the question: Is Chinese food bad for you? The answer depends on what you order. Soy sauce, shrimp chips, and other Chinese specialties are high in sodium, but you can still enjoy them every now and then. Better yet, choose healthy options like steamed fish, Buddha's delight, or stir-fries.
There's no such thing as "good" or "bad" foods, points out the Academy of Nutrition and Dietetics. An occasional serving of egg rolls or fried rice is unlikely to affect your health — or your waistline. But it's one thing to enjoy these foods once or twice a year, and another thing to include them in your daily menu. Like with most things, moderation is the key.
Chinese food is more or less healthy, depending on the cooking method and ingredients used. Egg rolls, for example, boast a whopping 223 calories, 24 grams of carbs, and over 10 grams of fat per piece, according to MyFoodData. Wonton soup, by comparison, has roughly 70 calories, 12 grams of carbs, and less than 1 gram of fat per cup (via MyFoodData). Choosing one over the other comes down to your health goals.
Chinese food can be high in sodium, sugar, and trans fats
General Tso's chicken and other Chinese dishes are often loaded with sodium, sugar, and trans fats. Some specialties also contain monosodium glutamate (MSG), a potentially harmful food additive (via the Mayo Clinic). Any of these ingredients can harm your health when consumed in excess.
High-sodium diets, for example, may increase your risk of stroke, heart failure, kidney stones, and stomach cancer, warns the American Heart Association (AHA). Excess sodium also raises blood pressure, which may lead to cardiovascular problems in the long run. AHA recommends no more than 1,500 milligrams per day for optimal heart health. A single tablespoon of soy sauce provides 880 milligrams of sodium — that's more than half the maximum daily salt intake (per MyFoodData).
Chinese chefs also use a lot of sugar as a spice. Sweet and sour chicken, for instance, contains about 39 grams of carbs, including 19 grams of sugar, per serving (5.8 ounces), according to MyFoodData. On top of that, many foods are fried or cooked with large amounts of oil and high-fat sauces.
Traditional Chinese food looks nothing like American-Chinese food
Chinese people tend to focus more on food texture, flavor, and aroma, and less on its nutritional value, notes EthnoMed. The same source reports that traditional Chinese foods are rarely deep-fried. However, most Chinese restaurants in the U.S. serve spring rolls, crab puffs, ginger beef, and other deep-fried dishes to meet the demand for western food.
Many so-called "Chinese" dishes, such as General Tso's chicken, were created with the American consumer in mind. They also contain a lot more soy sauce and other ingredients compared with traditional Chinese food. Some dishes, like chop suey, egg foo young, deep-fried chicken wings, and anything with broccoli, are not authentic Chinese foods, says The Huffington Post.
Despite these differences, you can still find healthy food options in American-Chinese restaurants. Steamed rice or vegetables, wonton soup, Kung Pao chicken, and egg foo young are all a good choice. If you are on a diet or trying to eat healthier, ask for extra veggies and skip the noodles. Choose brown rice instead of white rice and cut back on soy sauce. Look for stir-fried, steamed, or braised dishes and limit deep-fried foods.
So, is Chinese food bad for you? Yes and no. Egg rolls, deep-fried beef, and other high-sodium or high-fat foods can skyrocket your cholesterol levels and blood pressure. However, they're unlikely to affect your health if you enjoy them in moderation. What matters most is your overall diet. Remember that you can always use healthy ingredients to recreate your favorite Chinese dishes at home.
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text:
ABŪ ḤAYYĀN TAWḤĪDĪ
ABŪ ḤAYYĀN TAWḤĪDĪ, ʿALĪ B. MOḤAMMAD B. AL-ʿABBĀS, an outstanding man of letters and essayist of the Buyid period. He was born between 310/922 and 320/932, probably in Shiraz, though his birthplace is also given as Nīšāpūr, Wāseṭ, or even Baghdad. He is said to have received the name Tawḥīdī because his father was a seller in Baghdad of a type of date known as tawḥīd; but it is possible (cf. Soyūṭī, Lobb al-lobāb) that Tawḥīdī is derived from the name ahl al-tawḥīd wa'l-ʿadl adopted by the Moʿtazela and so would refer to his philosophical views. He spent his youth in Baghdad, where he studied law with the Shafeʿite scholar Abū Ḥāmed Marvarrūḏī and Hadith with Abū Bakr Šāšī, Abū Saʿīd Sīrāfī, and others. His studies must have included philology and literature, and at least a smattering of Sufism.
On the completion of his studies he made a living as a professional scribe and moved to various cities. He was in Mecca in 353/964 (al-Emtāʿ, Cairo, 1939-44, II, p. 79) and at Ray in 358/968 (Yāqūt, Odabāʾ II, p. 292). On the latter occasion he was scribe to Ṣāḥeb b. ʿAbbād (q.v.), vizier to the Buyid prince Moʾayyed-al-dawla; but he also had connections with Ebn al-ʿAmīd (d. 360/970), vizier of Rokn-al-dawla, the father of Moʾayyed-al-dawla. Abū Ḥayyān himself tells us (Moqābasāt, Cairo, 1929, p. 156) that in 361/971 he was in Baghdad listening to Yaḥyā b. ʿAdī's lectures on philosophy. Before long, however, he was back in Ray in the employment of Ebn al-ʿAmīd's son and successor, Abu'l-Fatḥ b. al-ʿAmīd, who fell into disfavor and was executed (shortly after the death of Rokn-al-dawla) in 366/976. Almost immediately Abū Ḥayyān returned to the post of secretary to Ṣāḥeb, and retained this post until the end of 370/980, when he moved to Baghdad and was recommended by friends to the vizier Ebn Saʿdān. He continued to serve Ebn Saʿdān until the latter's dismissal and execution in 375/985. While working for Ebn Saʿdān, he was also a member of the distinguished literary and philosophical circle or salon of Abū Solaymān Manṭeqī Seǰestānī (d. about 375/985). He was probably also in touch with Abū Solaymān during earlier periods of residence in Baghdad. It is chiefly through the writings of Abū Ḥayyān that we know about this circle. After the death of Ebn Saʿdān he seems to have had no regular appointment, though he wrote a book (al-Moḥāżarāt wa'l-monāẓarāt) for Abu'l-Qāsem Modleǰī, vizier in Shiraz of Ṣamṣām-al-dawla. The poverty and lack of recognition from which he suffered for twenty years embittered him to such an extent that toward the end of his life he burnt his own books as a gesture of despair and defiance. He was certainly alive in 400/1009 and may have continued to live in Shiraz until 414/1023, by which time he would have been a centenarian.
Abū Ḥayyān aimed at playing a part in the literary life of his age comparable to that played by Jāḥeẓ two centuries earlier. The first main influence which carried him toward the fulfillment of his aim was the brilliant intellectual life surrounding the viziers Ebn al-ʿAmīd (Abu'l-Fażl) and his pupil and protégé, Ṣāḥeb b. ʿAbbād. Both viziers were themselves litterateurs of merit, and by their patronage attracted distinguished writers and thinkers. Abū Ḥayyān came to feel that the Ṣāḥeb was requiring him to perform tasks beneath his dignity, and his conduct led to dismissal. He took his revenge in a book called Maṯāleb (or Ḏamm) al-wazīrayn, "The vices of the two viziers" (ed. E. Kaylānī, Damascus, 1961). He had already made an anthology of adab, al-Baṣāʾer wa'l-ḏaḵāʾer, in ten volumes (ed. E. Kaylānī, Damascus, 1964-66). The second main influence on him was Abū Solaymān, who was himself in contact with Ṣāḥeb. However, where the latter had a leaning towards Muʿtazilite views, Abū Solaymān belonged to the Neoplatonic tradition of Fārābī and the Christian Yaḥyā b. ʿAdī; and in philosophy Abū Ḥayyān followed Abū Solaymān closely. The charges of extreme heresy made against him by some medieval Muslim writers do not seem to be justified. Abū Solaymān's salon was literary, rather than strictly philosophical, and discussed all sorts of intellectual questions. On the premature death of ʿAżod-al-dawla in 372/983, the circle decided that each member should make some appropriate statement; in this they were deliberately imitating certain Greek philosophers who expressed opinions on the death of Alexander the Great. Many of the discussions of Abū Solaymān's salon have been recorded by Abū Ḥayyān in his distinctive prose, firstly in al-Moqābasāt ("Adaptations") and secondly in al-Emtāʿ wa'l-moʾānasa ("Pleasure and conviviality"). Both books have survived and have been printed. Several other minor works have also survived.
Yāqūt, Odabāʾ, pp. 380-407 (with many quotations in other articles; see indices).
Ebn Ḵallekān, in article on Ebn al-ʿAmīd, tr. de Slane, III, p. 264.
Sobkī, Ṭabaqāt, Cairo, 1906, IV, p. 2. Brockelmann, GAL I, p. 283; S. I, pp. 435-36.
F. E. Peters, Allah's Commonwealth, New York, 1973, pp. 529-35.
EI2 I, pp. 126-27.
(W. M. Watt)
Vol. I, Fasc. 3, pp. 317-318
Cite this entry:
W. M. Watt, "ABŪ ḤAYYĀN TAWḤĪDĪ," Encyclopædia Iranica, I/3, pp. 317-318; an updated version is available online at http://www.iranicaonline.org/articles/abu-hayyan-tawhidi-ali-b (accessed on 30 January 2014).
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DALI Lighting Awards 2021 - Judges
DALI Lighting Awards 2021: Our judging panel
Jeff Shaw Associate Director, Lighting, Arup
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Matt Waring Tad Trylski Scott Wade
Chen Zhongli Karen van Creveld Markus Helle
Jeff Shaw Mark Lien
CHEN ZHONGLI
Currently the chief electrical engineer of Shanghai Architectural Design and Research Institute Co., Ltd., Chen Zhongli also holds social positions: IEC/TC-64 expert committee, expert of the Ministry of Housing and Urban-Rural Development Engineering Technical Expert Committee, vice chairman of the Intelligent Engineering Design Branch of the China Survey and Design Association, and the Electrical Branch of the Architectural Society of China Vice chairman, chairman of Shanghai Intelligent Building Construction Association, and many other positions. At the same time, he has edited and participated in the compilation of nearly 30 national norms and standards. Participated in design projects: Shanghai Jin Mao Tower, Shanghai Citigroup Tower, Shanghai Science and Technology Museum, Shanghai International Financial Center, Shanghai World Expo China Pavilion and other hundreds of project design consulting work.
MARKUS HELLE
Markus Helle is Editor-in-Chief of the magazine HIGHLIGHT, a special magazine for lighting, targeting the German speaking lighting designers, luminaire trade, manufacturers and specifiers. He has a university degree in Economics and Journalism and has been publishing on lighting and luminaires since 1992. Since 1998 he is developing the magazine HIGHLIGHT into one of the leading communication platforms for the lighting industry, with special issues, books, website and job portal. HIGHLIGHT is today reporting on trends for luminaires, technical aspects as well as on trends in the industry and the economic development.
MARK LIEN
Mark has designed lighting systems for a wide range of applications including residential, retail, healthcare and both conventional and nuclear power plants. He has provided lighting education while working, presenting and teaching across four continents. He serves on ASHRAE, ANSI, IEEE, ISO and IES committees. Mark is a columnist for LD&A magazine and he hosts a podcast on lighting trends and technologies. Mark is currently on several executive committees advising various organizations. Mark ran the educational centers for both Cooper and Hubbell Lighting and was the Director of Government & Industry Relations for OSRAM SYLVANIA before joining the Illuminating Engineering Society.
JEFF SHAW
Jeff has 25 years' experience as a lighting designer, and is the part of the leadership team of Arup's UK lighting design studio. He has led the lighting design on a wide range of projects, including the Tate Modern (twice) and the 'Bird's Nest' Stadium for the Beijing 2008 Olympics, and is currently the lighting lead for the design of HS2 Euston Station. Jeff plays an active role in the lighting industry, promoting lighting education and authoring guidance. He served as the President of the Society of Light and Lighting (SLL) in 2016.
TAD TRYLSKI
Lighting designer Tad Trylski is an active member of the IALD and former chair of the LIRC (IALD's industry liaison group). Formerly design director at design studio, Light Bureau, Tad now runs his own independent lighting design practice, and is a lecturer on the Masters course in Light and Lighting at London's Bartlett School. A self-confessed lighting control geek, he's very familiar with the deployment of DALI-based technologies.
KAREN VAN CREVELD
Karen van Creveld is an independent lighting designer with more than 25 years' experience. Throughout her career she has been responsible for a diverse range of both interior and exterior architectural lighting designs. She was born in South Africa and began her career as a sculptor, before immigrating to the UK and specializing in architectural lighting design. She achieved her MSc with Distinction in lighting from the Bartlett School of Architecture in 1996 and has recently returned to academic study to undertake her PhD in lighting at UCL.
SCOTT WADE
Scott Wade has been Technical & Certification Manager for the DALI Alliance (DiiA), and previously the DALI working group, since August 2013. As a leading international authority on DALI lighting control and related specifications, he has been invited to speak at numerous events around the globe. On behalf of DiiA, Scott developed and implemented the DALI-2 certification program, which was subsequently extended to include the D4i specifications. Since 2005, he has been an industry expert member of the IEC 62386 standardisation team, and is one of two convenors of the IEC working group TC 34/WG 11.
MATT WARING
Matt Waring is the editor of arc, the international architectural lighting design magazine which covers all aspects of lighting design, including retail lighting. An NCTJ qualified journalist, Matt leads the creative output for the publication, while also managing the day-to-day activity across its website and various social media accounts. Matt's role also sees him support [d]arc media's events, the [d]arc awards, and [d]arc room exhibition.