text:
\section{Introduction}
The advent of multi-wavelength surveys in the past two decades has led to the consensus that the vast majority of super-massive black holes (SMBHs) in the local Universe are radiatively quiescent (e.g., \citealp{1997ApJ...487..568H,2005A&A...435..521N,zha09}), with bolometric luminosities only a small fraction of their Eddington limit ($\lesssim10^{-3}L_{\rm Edd}$).
Direct probes of these so-called low-luminosity active galactic nuclei (LLAGNs; see review by \citealp{2008ARA&A..46..475H}) prove to be challenging and often require high-resolution, high-sensitivity observations.
Nevertheless, studies of LLAGNs are crucial for our comprehensive understanding of the physics of SMBH accretion and feedback over cosmic time \citep{2012ARA&A..50..455F, 2013ARA&A..51..511K}.

Lying at the extreme faint end of the LLAGN family is the Galactic center black hole, Sgr A* \citep{2001ARA&A..39..309M}. At the radio band, in which it was first discovered, Sgr A* is a compact synchrotron source with an inverted spectrum extending into the millimeter wavelengths (e.g., \citealp{1998ApJ...499..731F}), and exhibits moderate flux variations on timescales from hours to years \citep{2003ANS...324..355Z,2004AJ....127.3399H,2011ApJ...729...44Y}.
The variability of Sgr A* is much stronger at higher frequencies \citep{2010RvMP...82.3121G}. In particular, X-ray flares have been detected on average once per day, with amplitudes reaching $\sim$100 times the quiescent level \citep{2013ApJ...774...42N}.
Despite this remarkable (and still not well understood) variability, Sgr A* is exceptionally underluminous, showing a bolometric luminosity only $\sim 10^{-8}L_{\rm Edd}$.
Nevertheless, Sgr A* occupies a key position in the development of theories for LLAGNs.
It is now widely thought that LLAGNs are powered by a radiatively inefficient, advection-dominated accretion flow (ADAF),
which is probably coupled with outflows in the form of jets and/or winds (see review by Yuan \& Narayan 2014).
This ADAF-jet paradigm gains support from radio interferometric surveys of nearby galactic nuclei, in which compact cores with high brightness temperatures, and sometimes with elongated components, are frequently detected and best interpreted as synchrotron radiation from the magnetized, relativistic jets (e.g., Nagar et al.~2000, 2005).
Ironically, the ADAF-jet paradigm is not without controversy with Sgr A* itself.
Despite its virtue of proximity, Sgr A* is persistently seen as a compact source (i.e., detailed morphology not detected)
under the currently best available resolution afforded by VLBI observations,
down to the vicinity of its presumed event horizon  (Bower et al.~2004; Shen et al.~2005; Doeleman et al.~2008), thus leaving serious doubt on the existence of the putative jet (but see Li et al.~2013).

The Andromeda galaxy (M\,31) hosts the second nearest SMBH, known as M\,31*, which has a dynamical mass of 1.4$^{+0.9}_{-0.3}\times10^8{\rm~M_{\sun}}$ inferred from stellar kinematics \citep{2005ApJ...631..280B}.
M\,31* has been detected only in the radio and X-rays to date. Crane et al.~(1992) first identified a compact 8.4 GHz source at the nucleus of M\,31 using the Very Large Array (VLA).
Its physical association with the putative SMBH was reinforced by a follow-up 8.4 GHz observation that found mild variability ($\sim 30-40~\mu$Jy; \citealp{1993ApJ...417L..61C}).
Due to its intrinsic dimness and contamination from neighboring X-ray sources, the X-ray counterpart of M\,31* was not firmly established until a much later time (Garcia et al.~2010).
The bolometric luminosity of M\,31* is estimated to be $\sim 10^{-8}L_{\rm Edd}$, making it only the second known LLAGN, after Sgr A*, to exhibit such a low state.
Interestingly, M\,31* has exhibited flaring X-ray emission since early 2006, with amplitudes similar to those seen in Sgr A* (Li et al.~2011).

The proximity of M\,31*, as well as its similarities with Sgr A*, holds promise for exploring the still poorly understood physics of SMBHs accreting at very sub-Eddington rates.
We have carried out a systematic observing campaign of M\,31*, using the Karl G. Jansky Very Large Array (JVLA\footnote{The official acronym for the Karl G. Jansky Very Large Array is VLA. Here and in the following we use the acronym ``JVLA" to avoid potential confusion with the observations taken in the pre-JVLA era.}) in multi-epoch and multi-frequency.
These observations of unprecedented sensitivity and resolution allow us to detect M\,31* at high frequencies, probe any extended component, constrain its instantaneous spectrum, and study its variability on various timescales.
We describe the observations and data reduction procedure in Section 2. The results are presented in Section 3, followed by a discussion in Section 4 and a summary in Section 5.
We adopt a distance of 780 kpc for M\,31* \citep{1998ApJ...503L.131S}.
Thus $1^{\prime\prime}$ corresponds to 3.8 pc, or $\sim$$2.8\times10^5 R_{\rm Sch}$ (the Schwarzschild radius for a black hole mass of 1.4$\times10^8{\rm~M_{\sun}}$).
Throughout this work, errors are quoted at the 1\,$\sigma$ confidence level, unless otherwise noted.

\section{Observations and Data Reduction} \label{sec:data}
\subsection{JVLA Observations} \label{subsec:JVLA}
We have observed M\,31* with JVLA at the C, X, Ku and K bands, in a total of 19 epochs between May 2011 and December 2012 (Project ID: 11A-178, SD0487, 11A-137 and 12B-002).
The array configurations included A, B and BnA, which are well suited for detecting a compact source.
The central frequencies were 5.0, 6.0 or 6.6 GHz for C-band, 8.5 or 10 GHz for X-band, 15 GHz for Ku-band and 20 GHz for K-band.
We note that these observations were carried out during several stages of commissioning of the new receiver systems, hence the different projects have different parameters (especially bandwidth and central frequency).
 In 17 of the 19 epochs, a dual-frequency was employed, including C-band and one of the other three higher-frequency bands, which allows us to measure an instantaneous spectral index. The remaining two epochs were taken with the C-band only.
In total, we obtained 19 C-band, 7 X-band, 2 Ku-band and 8 K-band observations, which together provide a good sampling of the potential variability in M\,31* on timescales ranging from hours to weeks and months.
Table \ref{tab:VLAresults} presents details of these observations (each assigned an ID), including observing date, central frequency, integration time, array configuration, bandwidth, beam size and RMS noise.

In all observations, the phase center was placed at the nucleus of M\,31, i.e., $[RA, DEC]$ (J2000) = [00$^{h}$42$^{m}$44\fs329, +41\arcdeg16\arcmin08\farcs42].
We used 3C48 as the flux density calibrator for the amplitude scale and instrumental bandpass, with the exception of Project 11A-137, in which 3C147 was used.
The Perley-Butler 2010 flux density scale was applied.
The on-target scans, 6-10 minutes each, were sandwiched between scans of the nearby gain calibrator J0038+4137.
Since the flux density of M\,31* is too weak to be self-calibrated, we relied on the cycle time being short enough to properly compensate for the temporal atmospheric phase fluctuations.

Each individual visibility data was flagged, calibrated, imaged and restored using the Common Astronomy Software Applications package\footnote{http://casa.nrao.edu} (CASA, version 4.3) in standard procedures.
We inspected all visibility data by eye, and manually flagged bad data (from RFI and instrumental effects).
The Stokes I images were then produced using the CLEAN task, with the Multi-frequency Synthesis mode, nterms=1 and natural weighting.
The flux densities of M\,31*, whenever detected, were measured by the IMFIT task, fitting an elliptical Gaussian to the Stokes I image.

To maximize the signal-to-noise ratio, we used the CONCAT task to combine the individual visibility data of same central frequency into a concatenated visibility data.
The CLEAN task was employed again to make Stokes I images at different bands.
Details of the concatenated images, including central frequency, total integration time, beam size, RMS level and the individual observations involved, are given in Table \ref{tab:concat}.

We note that Projects 11A-178 and SD0487 were taken in coordination with simultaneous {\it Chandra} observations. The relation between the radio and X-ray emission from M\,31* will be studied in a forthcoming paper.

\subsection{Historical VLA observations}
To extend our temporal baseline for variability study,
we revisit historical VLA observations of M\,31*, conducted by one of us (L.O.S.) during 2002--2005.
These ten observations, taken in the C-band (5 GHz) under A- or B-configuration, are summarized in Table \ref{tab:VLAresults} (IDs 37-46).
We reduced the data also using CASA, and following the standard ``old" VLA tutorial\footnote{https://casaguides.nrao.edu/index.php/Calibrating\_a\_VLA\_5\_GHz\_continuum\_survey}, to minimize systematics when compared to the JVLA data. The primary flux density calibrator was 3C48 and the gain calibrator was J0038+4137.
All Stokes I images were synthesized with natural weighting and fitted with the IMFIT task. We also used the CONCAT task to combine the ten observations to obtain a concatenated 5 GHz image.

\section{Results} \label{sec:result}
\subsection{Morphology} \label{subsec:morphology}
Figure \ref{fig:combinedimage}a-d display the concatenated JVLA images in the four bands, enclosing the central $4\arcsec\times4\arcsec$ ($\sim$15.2 pc$\times$15.2 pc) region of M\,31.
These images have RMS noise of 1.9, 2.0, 2.0 and 2.0 $\mu$Jy at 6, 10, 15 and 20 GHz, respectively,
and corresponding beam size of $0\farcs58\times0\farcs50$, $0\farcs25\times0\farcs23$, $0\farcs17\times0\farcs16$ and $0\farcs25\times0\farcs24$.
M\,31* is detected as a compact source at its putative position at all four frequencies, in particular, at 10, 15 and 20 GHz for the first time.
On the other hand, M\,31* was not detected in either of the two observations at 8.5 GHz, nor in their concatenated image (hence not shown here).

A closer look at the 6 GHz image (Figure \ref{fig:combinedimage}a) indicates substructures on a scale of $\lesssim 1^{\prime\prime}$, immediately around an otherwise point-like source. Two small ``plumes'' seem to protrude toward the north and the south, reminiscent of a bipolar outflow or jets from the central black hole. Complicating this picture, another ``plume" reaching out to the west is also hinted.
We further show in Figure \ref{fig:combinedimage}e the concatenated C-band image including the 11 A-array JVLA observations only.
The above substructures persist in this image of higher resolution (beam size of $0\farcs51\times0\farcs42$).
This remains true in further tests in which a subset of data is taken out from the concatenated image.
A similar morphology appears in the 15 GHz image, but the source is virtually unresolved in the 10 and 20 GHz images.
Finally, the concatenated image of the historical VLA observations (Figure \ref{fig:combinedimage}f) shows a markedly different morphology of M\,31*, but this is likely affected by the poorer resolution and sensitivity in this image.
We caution that the ``plumes" are only detected at a $\sim$3\,$\sigma$ level. The reality and physical meaning of these substructures will be further discussed in Section \ref{sec:discussion}.

\subsection{Variability}
We have measured the flux density (or upper limit, in the case of non-detection) of M\,31* in a uniform fashion for both the JVLA and historical VLA images.
The peak flux density, Gaussian size and integrated flux density are listed for each image (ID) in Table \ref{tab:VLAresults}.
Figure \ref{fig:curve} presents the light curves of M\,31* derived from the 19 JVLA epochs, with different color-coded symbols representing different bands.
To facilitate the comparison among the slightly different C-band central frequencies, we have converted the 5.0 or 6.6 GHz flux density into a 6.0 GHz flux density, assuming a spectral index of $\alpha = -0.45$ ($S_\nu \propto \nu^\alpha$; sec Section \ref{subsec:spec}).
From the C-band light curve (red circles), which covers all epochs, we identify two significant variations: the peak flux density reached a maximum of $48.6\pm8.0$ $\mu$Jy/beam on Jun 05, 2011, having increased by $\sim$71\% ($\sim$2\,$\sigma$ significance) in about eight days;
On December 22, 2012, the peak flux density increased by $\sim$44\% ($\sim$3\,$\sigma$ significance) within just six hours.
Otherwise the C-band light curve appears flat, exhibiting a modest rms fluctuation of $\sim15$\% about its mean ($28.3\pm1.9$ $\mu$Jy/beam).
The light curves at the other bands are much more sparse and show no significant variability, either.
The mean peak flux densities of M\,31* are $20.2\pm2.0$, $16.6\pm2.0$ and $15.0\pm2.0$ $\mu$Jy/beam, derived from the concatenated images at 10, 15 and 20 GHz, respectively.

 More quantitatively, we calculate for each band the variability index \citep{2011ApJ...740...66P},
\begin{equation}
VI = \frac{1}{N}\sum_i\left|\frac{S_i-\bar{S}}{\bar{\sigma}}\right|,
\end{equation}
where $S_i$ the flux density at the $i$th epoch, $\bar{S}$ the mean flux density, and $\bar{\sigma}$ the mean error over $N$ epochs.
A source is considered variable in the case of $VI$ $>$ 1.0, i.e., its flux density varies more than the mean measurement error.
We find that in the C-band $VI \approx 1.1$, whereas $VI < 1.0$ in the other bands.
This reinforces our conclusion that during 2011-2012, M\,31* shows marginal variability at 6 GHz, but is consistent with no significant variability at higher frequencies, due partially to the limited coverage.

A comparison with the historical VLA observations allows to probe the long-term variability in M\,31*.
We measure a mean peak flux density of $60.0\pm10.0$ $\mu$Jy/beam at 5 GHz between 2002-2005, which is consistent with that reported in Garcia et al.~(2010).
Compared to the mean value of $28.3\pm1.9$ $\mu$Jy/beam at 6 GHz between 2011-2012, this indicates a $\sim$50\%  ($\sim$3\,$\sigma$ significance) decrease over about a decade.
We note that the 5 GHz flux density of our calibrator, 3C48, exhibits no significant variability (to within 0.2\%) in the mean time.
A long-term decrease is also evident at a higher frequency: Crane et al. (1992, 1993) measured 8.4 GHz flux densities of $28 \pm 5$ and $39 \pm 5$ $\mu$Jy, while our observations set a 3\,$\sigma$ upper limit of 22 $\mu$Jy at 8.5 GHz.

\subsection{Spectral Index} \label{subsec:spec}
In 9 of the 17 dual-frequency epochs, M\,31* is detected (i.e., $>$ 3\,$\sigma$) in both frequencies.
We derive a quasi-instananeous spectral index for each of these 9 epochs and find values ranging from $-1.09\pm0.16$ to $-0.31\pm0.28$ (see lower panel of Figure \ref{fig:curve}).
We also obtain a time-averaged spectral index over the longest possible frequency range (Figure \ref{fig:SED}), based on the peak flux densities at 5, 6.0, 6.6, 10, 15 and 20 GHz from the concatenated images.
This leads to $\alpha = -0.45\pm0.08$ (if instead the integrated flux densities were adopted, the resultant spectral index is $\alpha = -0.44\pm0.10$), which is consistent with synchrotron radiation.
The upper limit at 8.5 GHz is compatible with this average spectrum.
Notably, the average spectrum predicts a flux density of 12.5 $\mu$Jy at 30 GHz and 11.0 $\mu$Jy at 40 GHz, inviting future JVLA observations at these higher frequencies.

\section{Discussion} \label{sec:discussion}
Our JVLA observations reveal unprecedented details about the radio emission from M\,31*. This provides important clues to its otherwise underluminous radiation, and in turn sheds light to the nature of LLAGNs in general, as addressed below.

\subsection{Temporal behavior: LLAGN in context}

The 19 C-band observations taken during 2011-2012 provide insights on the variability in M\,31* arising from a physical scale of $\lesssim10^5 R_{\rm Sch}$.
In particular, the rms fluctuation is found to be only modest ($\sim$15\%) on weekly to monthly timescales. This is comparable to that in Sgr A* ($\sim17$\% at 5 GHz; Zhao et al.~1989).
It is often considered that interstellar scintillation contributes substantially to the observed variability in Sgr A* at low frequencies ($\lesssim$ 5 GHz; e.g., \citealp{2006ApJ...641..302M}). Since M\,31* has a much lower line-of-sight column density ($\lesssim 10^{21}{\rm~cm^{-2}}$; Li et al.~2009), the 15\% fluctuation can be considered intrinsic, which might be due to a stochastic accretion rate or plasma instability in the course of jet propagation.
It remains to be explored whether such fluctuations are typical of LLAGNs.
Significant variations are also caught on short timescales (Section 3.2). In particular, the $\sim$40\% increase in the 6 GHz flux density, which occurred within 6 hrs on December 22, 2012, places a strong constraint on the size of the emitting region, $\lesssim16$ $R_{\rm Sch}$. The amplitude and physical scale of this event are similar to some of the radio flares in Sgr A*.
We point out, however, the 15 GHz flux density measured at the same epochs showed no significant variability (Figure \ref{fig:curve}).

The comparison between the JVLA and historical VLA measurements further reveals that M\,31* has decreased its mean flux density by about 50\% over about a decade (Section 3.2; Figure 3).
On such timescales, M\,31* might have experienced a substantial adjustment in its accretion rate, leading to a subsequent change in the jet power.
Interestingly, the mean X-ray flux of M\,31* had shown an opposite trend in the past decade.
M\,31* was essentially undetected in any {\it Chandra} observation taken before 2006 (with a mean X-ray luminosity $\lesssim 10^{36}{\rm~erg~s^{-1}}$), but alleviated its X-ray emission by a factor of $\sim$5 on average, apparently after an outburst on January 6, 2006 (Li et al.~2011).
We note that such a trend has not been found in the X-ray emission from Sgr A*, although the two most underluminous LLAGNs both currently exhibit flaring X-ray emission.
A long-term decrease in the radio flux of Sgr A* has not been reported, either.
Unfortunately, there was no useful VLA observation of M\,31* between March 2005 and April 2011, i.e., the period during which the mean radio flux presumably experienced a substantial (and perhaps abrupt) drop.
Whether there is a causal relation between the increase in X-rays and decrease in radio remains an intriguing possibility to investigate. We defer such a study, to be assisted with standard ADAF-jet models (Yuan et al. 2009), to a future work.

To our knowledge, long-term radio variability has been reported for few LLAGNs, due partially to the lack of extensive monitoring observations.
One exception is M\,81*, an archetype LLAGN with a black hole mass of $7\times10^7{\rm~M_{\sun}}$ and a bolometric Eddington ratio of $\sim10^{-5}$ \citep{2003AJ....125.1226D}.
\cite{2011A&A...533A.111M} reported a long-term radio (5.0 and 8.4 GHz) flare in M\,81* from 1997 to 2001, which climbed to a peak more than twice the quiescent level. This suggests that decade-long monitoring observations be crucial to obtaining a clear picture of the variability in LLAGNs.

\subsection{Spectrum and morphology: insights on the putative jet}
We have derived an average spectral index of $\alpha\approx-0.45\pm0.08$ over the available frequency range of 5-20 GHz (Figure \ref{fig:SED}).
While none of our 19 epochs covers more than two frequencies, this average slope is expected to represent the true slope, in view of the very modest variability among these epochs. Indeed, the six epochs with a C/K combination show an instantaneous spectral index ranging between $-0.31\pm0.28$ to $-0.72\pm0.26$.

This relatively steep spectrum is to be contrasted with that of Sgr A*,
which is observed to be $\alpha \approx 0.2-0.3$ over a similar frequency range \citep{1998ApJ...499..731F}.
In the case of M\,81*, in which substructures are clearly resolved,
\cite{2004ApJ...615..173B} measured~$\alpha \ga0$ near the core and $\alpha\approx-0.7$ in the apparently one-sided jet at $\sim1$ milli-arcsec ($\sim 3\times10^3$ times the Schwarzschild radius of M\,81*) away from the core.
These are understood in the standard jet models (e.g., \citealp{2000A&A...362..113F, 2010LNP...794..143M}), which predict a negative gradient in the spectral index along the jet path as the result of decreasing synchrotron opacity.
In this regard, the spectral index of M\,31* ($\sim$-0.45) suggests that the observed radio emission over 5-20 GHz is dominated by the optically-thin part of the jet.
We note that the physical scale corresponding to the synthesized beam of our JVLA images, is $\sim (2-7)\times10^{4}R_{\rm Sch}$. This places an upper limit in the distance of the emitting region from the black hole. The short-timescale variability might take place much closer to the black hole (Section 4.1).

It is natural to look for a trace of the putative jet on larger scales.
In this regard, the three ``plumes" seen primarily in the concatenated JVLA C-band image (Figure 1a and e) deserve some remarks.
These faint ($\sim$3\,$\sigma$) features are the only hint for an extended component around an otherwise unresolved core.
Their combined morphology, however, is not easily compatible with a canonical bipolar jet/outflow.
On the other hand, the vicinity of M\,31* on a scale of few arcsecs is known to be devoid of cold gas and young, massive stars (Li et al.~2009).
Therefore, it is also unlikely that these ``plumes" arise from circumnuclear free-free emission.
We speculate, on the basis of their combined morphology, the ``plumes" might be tracing the synchrotron radiation from a hot wind launched from the inner part of the accretion flow of M\,31*. Such a wind/outflow is a generic prediction by the theories and numerical simulations of hot accretion flows in LLAGNs (Blandford \& Begelman 1999; Yuan, Bu \& Wu 2012; Narayan et al. 2012; Yuan et al. 2015).
These theoretical works have gained increasing observational support, from LLAGNs (e.g., Wang et al. 2013; Tombesi et al. 2014) to the hard state of black hole X-ray binaries (Homan et al. 2016).
The predicted winds have a wide opening angle as compared to the highly collimated jet, as they
originate from the corona region of the hot accretion flow, where frequent magnetic reconnection should occur and can efficiently accelerate electrons (Yuan et al. 2009b).
Therefore, relativistic electrons should be present in the winds and emit radio emission via synchrotron radiation.
Recently, we detected the radio counterpart of the central SMBH in M\,32 (named M\,32*), a dwarf elliptical companion of M\,31, using deep JVLA C-band observations (Yang et al.~2015). M\,32* has a 6 GHz flux density similar to that of M\,31*, and also shows a pc-scale, extended morphology marginally resolved by the synthesized beam.
This source could be another case of synchrotron radiation from the wind of a LLAGN.
A more meaningful test of our speculation awaits further work.

\section{Summary}
Thanks to the unprecedented sensitivity afforded by our JVLA observations, we have significantly advanced our knowledge about the radio properties of M\,31*, one of the nearest and most underluminous SMBHs. Our main results include:

\begin{enumerate}

\item Detection of M\,31* at 10, 15 and 20 GHz for the first time;

\item Constraints on the short- and long-term variability in M\,31*. In particular, a curious decrease of the mean flux density, by $\sim$50\%, is found between the JVLA and historical VLA observations separated by nearly a decade, which might be associated with an observed increase in the mean X-ray flux of M\,31*;

\item Measurement of the spectral index covering 5-20 GHz. The relatively steep spectrum ($\alpha \approx -0.45$) is best interpreted as dominated by the optically-thin part of a putative jet, which is located at no more than a few thousand Schwarzschild radii from the black hole. However, no clear evidence is provided in our images for an extended component tracing this putative jet.

\end{enumerate}

These findings clearly invite further high-resolution interferometric observations, as well as dedicated numerical models, to deepen our understanding of the formation and evolution of jets and outflows from M\,31*.

\begin{acknowledgements}
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.
This work is supported by the National Natural Science Foundation of China under grants 11473010, 11573051 and 11633006.
We thank Mike Garcia for the effort in preparing Project SD0487.
Z.L. acknowledges support from the Recruitment Program of Global Youth Experts.
F.Y. acknowledges support from the Key Research Program of Frontier Sciences of CAS
(No. QYZDJ-SSW-SYS008) and the Ministry of Science and Technology
of China (No. 2016YFA0400704).
\end{acknowledgements}

\begin{figure*}\centering
\epsscale{1}
\plotone{fig1.eps}
\caption{The concatenated images of M\,31* in different bands. (a) 6 GHz; (b) 10 GHz; (c) 15 GHz; (d) 20 GHz;
(e) 6 GHz, from only the A-array observations; (f) 5 GHz, from the historical VLA observations taken during 2002-2005.
Contour levels are at [-2, 3, 5, 10] $\times$ RMS in (a), (b) and (e), and at [-2, 3, 5] $\times$ RMS in (c), (d) and (f).
Positive and negative levels are denoted by solid and dash contours, respectively.
In each panel, the magenta cross marks the putative position of M\,31*, $[RA, DEC]$(J2000) = [00$^{h}$42$^{m}$44\fs325, +41\arcdeg16\arcmin08\farcs43]),
and the ellipse at the lower left corner represents the synthesized beam.
The major axis of the M\,31 disk is indicated by a solid line (position angle of $38 \degr$) in (e).
}
\label{fig:combinedimage}
\end{figure*}

\begin{figure*}\centering
\epsscale{1}
\plotone{fig2.eps}
\caption{{\it Upper panel}: Light curves of M\,31* during the 2011-2012 observing campaign.
Filled circles represent central frequency at 6.0 GHz, while open circles denote 5.0 and 6.6 GHz measurements converted into 6.0 GHz, assuming a spectral index of $-0.45$.
Arrows represent 3-sigma upper limit in the case of non-detections.
The dash lines and corresponding shaded regions show the mean peak flux densities and errors from the concatenated images.
{\it Lower panel}: the instantaneous spectral index derived for the epochs in which M\,31* is detected in dual frequencies.}
\label{fig:curve}
\end{figure*}

\begin{figure*}\centering
\epsscale{1}
\includegraphics[width=0.8\textwidth,angle=0]{fig3.eps}
\vskip3.5cm
\caption{The radio spectral energy distribution of M\,31*.
The color-coded filled symbols denote the mean peak flux densities, as measured from the concatenated JVLA images (red for C band, green for X band, gray for Ku band and blue for K band).
The solid line and the shaded region denote the best-fit power-law and its uncertainty, fitted to the filled symbols only.
For comparison, the 3\,$\sigma$ upper limit at 8.5 GHz is marked by an arrow, along with open symbols showing historical VLA measurements at 5 GHz (this work) and 8.5 GHz (Crane et al.~1992, 1993).
}
\label{fig:SED}
\end{figure*}

\begin{landscape}
\begin{deluxetable}{cccccccccccc}
\tabletypesize{\scriptsize}
\tablecaption{Observation Log and M\,31* Measurements in Individual Images}
\tablewidth{0pt}
\tablehead{
\colhead{}&
\colhead{}&
\colhead{}&
\colhead{}&
\colhead{}&
\colhead{}&
\colhead{}&
\colhead{}&
\colhead{}&
 \multicolumn{3}{c}{IMFIT Gaussian}\\
\cline{10-12}
\colhead{ID}&
\colhead{Project}&
\colhead{Date}&
\colhead{$\nu$}&
\colhead{Time}&
\colhead{Config.}&
\colhead{Bandwidth}&
\colhead{Beam size}&
\colhead{RMS}&
\colhead{$I_{{\rm peak}}$}&
\colhead{Image component size}&
\colhead{$S_{{\rm int}}$}\\
\colhead{}&
\colhead{}&
\colhead{}&
\colhead{(GHz)}&
\colhead{(hr)}&
\colhead{}&
\colhead{(MHz)}&
\colhead{($\arcsec\times\arcsec, \degr$)}&
\colhead{($\mu$Jy/beam)}&
\colhead{($\mu$Jy/beam)}&
\colhead{($\arcsec\times\arcsec, \degr$)}&
\colhead{($\mu$Jy)}\\
\colhead{(1)}&
\colhead{(2)}&
\colhead{(3)}&
\colhead{(4)}&
\colhead{(5)}&
\colhead{(6)}&
\colhead{(7)}&
\colhead{(8)}&
\colhead{(9)}&
\colhead{(10)}&
\colhead{(11)}&
\colhead{(12)}\\
}
\startdata
1&11A-178& 2011 May 27& 5.0& 2.5& BnA& 256& $1.52\times0.67$, -68&6.0&$34.9$&$1.58\times0.78$, 113&$42.1\pm5.5$\\
2&11A-178& 2011 May 27& 8.5&  2.5& BnA& 256& $0.91\times0.42$, -66& 11.0&$< 33.0$ & - & -\\
3&11A-178& 2011 May 28& 5.0&  2.5& BnA& 256& $1.52\times0.62$, -68&7.0 &$30.8$&$1.66\times0.91$, 129&$49.0\pm9.6$\\
4&11A-178& 2011 May 28& 8.5&2.5  & BnA& 256& $0.95\times0.38$, -65&8.0 &$< 24.0$&-&-\\
5&11A-178& 2011 Jun 05&  5.0& 2.5 & BnA& 256& $0.71\times0.50$, -87&8.0 &$52.8$&$0.79\times0.53$, 96&$62.2\pm7.9$\\
6&11A-178& 2011 Jun 05&  8.5& 2.5 & BnA& 256& $0.45\times0.30$, 89&10.0 &$< 30.0$&-&-\\
7&11A-178& 2011 Jul 01&   5.0&2.5  & A& 256& $0.50\times0.45$, -74&7.0 &$37.9$&$0.50\times0.45$, -74&$37.9\pm7.0$\\
8&11A-178& 2011 Jul 01&   8.5& 2.5 & A& 256& $0.30\times0.27$, -73&8.0 &$< 24.0$&-&-\\
9&11A-178& 2011 Jul 27&   5.0& 2.5 & A& 256& $0.59\times0.44$, -78& 6.5&$32.0$&$0.59\times0.44$, -78&$32.0\pm6.5$\\
10&11A-178& 2011 Jul 27&   8.5& 2.5 & A& 256& $0.38\times0.27$, -71& 7.5&$< 23.0$&-&-\\
11&11A-178& 2011 Aug 27& 5.0& 2.5 & A& 256& $0.46\times0.41$, -6& 11.0&$< 33.0$&-&-\\
12&11A-178& 2011 Aug 27& 8.5& 2.5 & A& 256& $0.28\times0.24$, 12& 9.0&$< 27.0$&-&-\\
13&SD0487&  2011 Sep 02&   5.0& 6 & A& 256& $0.45\times0.43$, -4&5.0 &$33.0$&$0.62\times0.46$, 113&$48.6\pm5.7$\\
14&11A-137& 2011 Sep 04&   6.6& 1 & A& 2048& $0.36\times0.33$, -73&4.5 &$24.4$&$0.36\times0.33$, -73&$24.4\pm4.5$\\
15&11A-137& 2011 Sep 04&   20& 4.5 & A& 2048& $0.12\times0.11$, -5&4.5&$18.1$&$0.12\times0.11$, -5&$18.1\pm4.5$\\
16&11A-137& 2011 Sep 06&   6.6& 1 & A& 2048& $0.37\times0.33$, -64&11.0 &$< 33.0$&-&-\\
17&11A-137& 2011 Sep 06&   20& 4.5 & A& 2048& $0.11\times0,10$, -10&4.5 &$24.9$&$0.11\times0.10$, -10&$24.9\pm4.5$\\
18&SD0487&  2011 Sep 07&   5.0& 6 & A& 256& $0.57\times0.44$, -40&6.0 &$19.4$&$0.75\times0.66$, 159&$38.2\pm6.6$\\
19&SD0487&  2012 Jun 01&   6.6& 1.5 & B& 2048& $1.20\times1.08$, -86&6.0 &$35.2$&$1.20\times1.08$, -86&$35.2\pm6.0$\\
20&SD0487&  2012 Jun 01&   20& 4.5 &  B& 2048& $0.35\times0.35$, 12&3.0 &$21.6$&$0.42\times0.33$, 94&$24.2\pm1.2$\\
21&SD0487&  2012 Jun 06&   6.6& 1.5 & B& 2048& 1.35$\times$1.11, 53& 7.0&$32.4$&$1.59\times1.44$, 97&$49.0\pm11.0$\\
22&SD0487&  2012 Jun 06&   20& 4.5 &  B& 2048& 0.40$\times$0.35, 38& 3.0&$15.3$&$0.40\times0.35$, 38&$15.3\pm3.0$\\
23&SD0487&  2012 Jun 12&   6.6& 1.5 & B& 2048& 1.22$\times$1.18, 80& 8.0&$24.0$&$2.42\times1.46$, 168&$58.7\pm5.2$\\
24&SD0487&  2012 Jun 12&   20& 4.5 &  B& 2048& 0.39$\times$0.35, -26&3.5 &$15.8$&$0.39\times0.35$, -26&$15.8\pm7.0$\\
25&SD0487&  2012 Jul 01&   6.6& 1.5 & B& 2048& 1.23$\times$1.05, -89&4.5 &$24.8$&$1.50\times0.98$, 55&$28.3\pm4.7$\\
26&SD0487&  2012 Jul 01&   20& 4.5 &  B& 2048& 0.35$\times$0.34, -54& 4.5&$16.0$&$0.50\times0.31$, 24&$20.4\pm4.5$\\
27&SD0487&  2012 Aug 14&   6.6&1.5 & B& 2048& 1.24$\times$1.10, 76& 4.5&$30.3$&$1.24\times1.10$, 176&$30.3\pm4.5$\\
28&SD0487&  2012 Aug 14&   20& 4.5 &  B& 2048& 0.37$\times$0.35, -76&7.0 &$< 21.0$&-&-\\
29&SD0487&  2012 Oct 29&   6.6& 1.5 & A& 2048& 0.39$\times$0.33, -80& 5.0&$23.3$&$0.60\times0.48$, 29&$52.6\pm5.7$\\
30&SD0487&  2012 Oct 29&   20& 4.5 &  A& 2048& 0.16$\times$0.13, -22& 4.5&$17.0$&$0.19\times0.15$, 158&$22.4\pm4.6$\\
31&12B-002&  2012 Dec 22&   6.0& 0.9 &  A& 4000& 0.36$\times$0.36, 31&3.0 &$29.1$&$0.45\times0.32$, 100&$31.1\pm3.4$\\
32&12B-002&  2012 Dec 22&   15.0& 2.7 &  A& 6000& 0.16$\times$0.14, 35& 2.0&$17.5$&$0.19\times0.16$, 26&$23.2\pm2.8$\\
33&12B-002&  2012 Dec 22&   6.0& 0.9 & A& 4000& 0.45$\times$0.36, 80&3.0 &$41.9$&$0.53\times0.48$, 102&$65.9\pm5.1$\\
34&12B-002&  2012 Dec 22&   15.0& 2.7 &  A& 6000& 0.18$\times$0.17, 73&2.0 &$15.4$&$0.18\times0.18$, 96&$16.9\pm1.7$\\
35&12B-002&  2012 Dec 30&   6.0& 0.9 &  A& 4000& 0.39$\times$0.36, -74&3.0 &$27.3$&$0.39\times0.36$, -74&$27.3\pm3.7$\\
36&12B-002&  2012 Dec 30&   10.0& 2.7 &  A&4000 & 0.25$\times$0.23, -20&2.0 &$21.0$&$0.25\times0.25$, 11&$22.7\pm2.2$\\
\hline
\hline
37&AJ0289&2002 Jul 05&5&8&B&100&$1.52\times1.46$, 83&7.0&$25.8$&$1.52\times1.46$, 83&$25.8\pm7.0$\\
38&AJ0289&2002 Jul 06&5&8&B&100&$1.52\times1.46$, 85&7.0&$32.8$&$1.52\times1.46$, 85&$32.8\pm7.0$\\
39&AJ0289&2002 Jul 29&5&8&B&100&$1.53\times1.48$, -88&7.0&$48.7$&$1.53\times1.48$, -88&$48.7\pm7.0$\\
40&AJ0289&2002 Aug 12&5&2&B&100&$1.69\times1.43$, -80&12.0&$37.8$&$1.69\times1.43$, -80&$37.8\pm12.0$\\
41&TLS17&2002 Aug 14&5&1&B&100&$1.53\times1.40$, -53&15.0&$66.7$&$1.53\times1.40$, -53&$66.7\pm15.0$\\
42&AS0819&2004 Oct 27/28&	5&6.3&A&		100&$0.66\times0.44$, -71&18.0&$65.0$&$0.72\times0.31$, 51&$65.0\pm18.0$\\
43&S6314& 2004 Dec 06/07&   5& 12  &A&     100&   $0.64\times0.51$, 68  &8.0&$54.4$&$0.64\times0.51$, 68& $54.4\pm8.0$\\
44&S6314& 2004 Dec 27/28&   5& 12 &A&     100&   $0.56\times0.44$, -88  &9.0&$54.0$&$0.56\times0.44$, -88&$54.0\pm9.0$\\
45&S6314& 2005 Jan 28/29&   5& 12  &AB&   100&   $1.27\times0.67$, 80&9.0&$65.0$&$1.27\times0.67$, 80&$65.0\pm9.0$\\
46&S6314& 2005 Feb 21/22&   5& 12  &B&     100&   $1.83\times1.41$, -79 &8.0&$67.9$&$1.83\times1.41$, -79&$67.9\pm8.0$\\
\enddata
\vspace{-0.6cm}
\tablecomments{(1) Image ID; (2) Project ID; (3) Date of observation; (4) The central frequency; (5) Total integration time; (6) Array and configuration; (7) Total bandwidth; (8) Synthesized beam FWHM of major and minor axes, and position angle of the major axis; (9) Image RMS level; (10) Peak flux density of M\,31*; (11) major axis, minor axis and position angle of the fitted elliptical Gaussian; (12) integrated flux density.}
\label{tab:VLAresults}
\end{deluxetable}
\end{landscape}

\clearpage

\begin{landscape}
\begin{deluxetable}{cccccccccc}
\tabletypesize{\scriptsize}
\tablecaption{Mean Flux Densities of M\,31*}
\tablewidth{0pt}
\tablehead{
\colhead{}&
\colhead{}&
\colhead{}&
\colhead{}&
\colhead{}&
\colhead{}&
 \multicolumn{3}{c}{IMFIT Gaussian}\\
 \cline{8-10}
 Reference image &ID&Config.&$\nu$&Time&Beam size&$RMS$&$I_{\rm peak}$&Image component size&$S_{\rm int}$\\
&&&(GHz)&(hr)&($\arcsec\times\arcsec$, $\degr$)&$(\mu$Jy/beam)&$(\mu$Jy/beam)&($\arcsec\times\arcsec$, $\degr$)&($\mu$Jy)\\
(1)&(2)&(3)&(4)&(5)&(6)&(7)&(8)&(9)&(10)\\
}
\startdata
\multirow{4}{*}{Fig. 1(a)}&1, 3, 5, 7, 9, 11, 13, &\multirow{4}{*}{A, B, BnA}&\multirow{4}{*}{6.0}&\multirow{4}{*}{40.7}&\multirow{4}{*}{$0.58\times0.50$, -78}&\multirow{4}{*}{1.9}&\multirow{4}{*}{$28.3$}&\multirow{4}{*}{$0.64\times0.57$, 125}&\multirow{4}{*}{$35.5\pm4.4$}\\
&14, 16, 18, 19, 21, \\
&23, 25, 27, 29, 31,\\
 &33, 35&&&&&\\

Fig. 1(b)&36								&A&10&2.7&$0.25\times0.23$, -14&2.0&$20.2$&$0.26\times0.26$, 39&$23.9\pm3.5$\\
Fig. 1(c)&32, 34							&A&15&5.4&$0.17\times0.16$, 46&2.0&$16.6$&$0.18\times0.17$, 19&$20.7\pm2.1$\\
\multirow{2}{*}{Fig. 1(d)}&15, 17, 20, 22,&\multirow{2}{*}{A, B}&\multirow{2}{*}{20}&\multirow{2}{*}{27}&\multirow{2}{*}{$0.25\times0.24$, -3}&\multirow{2}{*}{2.0}&\multirow{2}{*}{$15.0$}&\multirow{2}{*}{$0.27\times0.22$, 9}&\multirow{2}{*}{$17.0\pm3.4$}\\
&24, 26, 28, 30&\\
\multirow{2}{*}{Fig. 1(e)}&7, 9, 11, 13, 14, 16,&\multirow{2}{*}{A}&\multirow{2}{*}{6.0}&\multirow{2}{*}{22.2}&\multirow{2}{*}{$0.41\times0.38$, -81}&\multirow{2}{*}{1.2}&\multirow{2}{*}{$28.7$}&\multirow{2}{*}{$0.51\times0.42$, 114}&\multirow{2}{*}{$39.7\pm3.2$}\\
&18, 29, 31, 33, 35&&&&\\
Fig. 1(f)&37-46							&A, B&5&81.3&$0.88\times0.66$, 80&10.0&$60.0$&$0.79\times0.65$, 87&$62.0\pm7.6$\\
\enddata
\vspace{-0.6cm}
\tablecomments{(1) Concatenated image in Figure \ref{fig:combinedimage}; (2) ID as in Table 1; (3) Configuration; (4) Central frequency; (5) Total integration time; (6) Synthesized beam size, including major and minor axis, and position angle of the major axis; (7) Image RMS noise; (8) Peak flux densities of M\,31*; (9) Major and minor axes, and position angle of the fitted elliptical Gaussian; (10) Integrated flux density.}
\label{tab:concat}
\end{deluxetable}
\end{landscape}

\clearpage

\acknowledgments

redpajama_set_name: RedPajamaArXiv


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Washington, D.C., Sept. 06, 2017 (GLOBE NEWSWIRE) -- Give an Hour™ a national nonprofit 501 (c)(3), founded in September 2005, announces that it is opening its network to provide immediate and long term mental health support for those affected by Hurricane Harvey. Give an Hour will extend these services to those affected by Hurricane Irma should the need arise.
As the flood waters begin to recede in Hurricane Harvey's wake, Give an Hour is partnering with the American Red Cross to bring mental health and emotional support services to those affected. While some people will be in immediate need of intensive mental health treatment, many more people will be in need of someone who can provide emotional support and assistance. As our nation closely watches the approach of Hurricane Irma, Give an Hour stands ready to help those affected by this massive storm as well.
"Give an Hour is proud to partner with the American Red Cross to provide this essential mental health support and we are grateful to our network of 7000 generous mental health professionals – many of whom are already stepping up during this time of need", said Dr. Barbara Van Dahlen, Founder and President of Give an Hour. "Some Give an Hour providers may join efforts on the ground – others in our vast network will offer phone support to the thousands who need their compassion, expertise and assistance. We all have gifts to give to those who are hurting." Since 2005, Give an Hour has provided free and confidential mental health care to those who serve, our veterans, and their families – providing over 224,000 hours of free care valued at nearly $23M. Give an Hour has since expanded efforts to address the mental health needs of other populations.
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text:
Why Are People Often Reluctant to See a Psychiatrist?
People living with mental illness may be eager to seek relief for their condition yet decide to avoid visiting a psychiatrist. Of course, psychiatry is not the only field that deals with the treatment of mental health conditions but it is the institution that specifically exists to diagnose, prescribe treatment for, and treat conditions that psychiatry itself delineates.
The general public, however, does not tend to view psychiatrists in the same way as physicians who deal primarily with physical issues and illnesses, even though all psychiatrists are themselves medically qualified doctors (this separates them from psychologists and psychotherapists). Indeed, there appears to be a widespread aversion toward seeing a psychiatrist.
In this piece, I would like to outline some of the main reasons why people avoid psychiatrists. This piece is not intended to remark on these reasons in a highly critical way – I bring them up only to highlight that there are various barriers to mental health treatment; the outcomes of avoiding psychiatry may be beneficial or misguided, depending on the context and the individual's circumstances. I hope that the following is a balanced and measured discussion on public attitudes toward psychiatry.
Stigma Toward Psychiatrists and Psychiatric Medication
To begin with, many people feel an aversion towards psychiatrists because of the stigma attached to the profession. Many believe psychiatrists are evil, manipulative, and coercive, impressions that – I argue – are influenced by portrayals of psychiatrists in mass media. This isn't to say that some psychiatrists or the profession of psychiatry aren't flawed, only that a strong fear towards psychiatrists may come down to certain misconceptions and prejudices. The cruel and inhumane mental health treatments of the past may also feed into people's fear of psychiatrists.
Negative attitudes toward psychiatric medication are also pervasive. Many people, including those with severe mental illness, might be reluctant to see a psychiatrist because they don't want to be prescribed psychotropic medication. People may believe that taking such medication is a 'quick fix' (implying that non-medicated recovery is more admirable), even though the process of finding the right medication and dosage – as well as recovery through the use of medication – can be a long process. It is also common to view taking medication as a sign of laziness or weakness, or to view medication (antidepressants in particular) as 'happy pills', which provide a fake or forced kind of happiness.
Concerns About Psychiatric Medication
Here I should reiterate the point made about stigma towards psychiatrists: there may be valid criticisms of psychiatric medication and concerns related to it (such as efficacy, unpleasant side effects, emotional blunting, dependence, withdrawal symptoms, and overprescription), but feelings of aversion toward psychiatric medication can at the same time be influenced by stigma. Thus, in some instances, avoidance of psychiatric treatment can be more based on fear than a careful appraisal of the treatment and its efficacy.
The Way People View Psychiatry Compared to Psychotherapy
In many people's minds, the cultural implications of visiting a psychiatrist and seeing a therapist are vastly different. There is, undeniably, a stigma attached to help-seeking in general, which includes seeking out a therapist, as this can be seen as a failure of self-reliance, an impression that disproportionately puts men off seeking mental health treatment.
Yet such stigma may be especially pronounced in the case of seeking help from a psychiatrist. This could partly come down to the negative attitudes toward psychiatric medication already touched upon – engaging in talk therapy might be viewed in a more favourable light if the person in therapy is seen as putting more effort into their recovery and confronting their issues, rather than supposedly avoiding those issues through medication. This is in spite of the fact that many patients who take psychiatric medication also attend therapy sessions, and they might find that the relief and stability from medication benefit their therapy sessions (indeed, some research underscores that therapy plus medication is better for the treatment of certain conditions than just medication alone).
Another potential reason for this difference in judgement toward psychiatry and therapy is that the former could be perceived as reserved for the most severely ill and dysfunctional, whereas the latter is seen as being acceptable, not just for those with more mild mental health issues but also for healthy, typical people who might want to work on their personal problems and relationships. So, out of fear of being perceived by others as 'crazy' or 'mad', people may avoid psychiatry.
Also, those who do have symptoms of severe mental illness could worry that visiting a psychiatrist will result in a loss of autonomy via involuntary admission (this is when you are admitted to a psychiatric hospital against your will, based on the belief that you are at serious risk of causing harm to yourself or others). This worry could be unfounded or founded. In the latter case, many people intent on taking their life will be reluctant to get help from a psychiatrist because they don't want to be involuntarily admitted and therefore be unable to go through with the act. Moreover, they could perceive a psychiatrist as the type of person most likely to – or most able to – involuntarily admit them to a psychiatric facility.
Other people have reservations about whether they want to potentially receive a psychiatric diagnosis (as these labels carry potential benefits and downsides). For some people experiencing mental distress, a diagnostic label can be illuminating and beneficial, whereas for others it can magnify feelings of shame, isolation, and hopelessness.
Critical and Anti-Psychiatry Perspectives
Critical psychiatry refers to constructive criticism of diagnostic classification and the use of psychiatric medication. It is distinct from anti-psychiatry, a movement that calls for the abolition of psychiatry and advocates for more talking-based therapies, although some psychiatrists, such as Jonathan N. Stea, believe the distinction between the two is nebulous, similar to the distinction between being vaccine-hesitant and anti-vaccine.
It's hard to say how much of people's aversion toward psychiatrists boils down to critical or anti-psychiatry perspectives, but many patients who have received psychiatric treatment and had negative experiences will adopt such perspectives and hence avoid seeking help from a psychiatrist in the future. Additionally, people who have never sought treatment from a psychiatrist may hold critical and anti-psychiatry beliefs and so naturally avoid that option should mental illness ever strike.
This is not to say that critical psychiatry or anti-psychiatry is counterproductive in terms of mental health recovery, only to highlight that scepticism and ideology can be a further reason why people are often reluctant to see a psychiatrist.
The Cost of Seeing a Psychiatrist
On the practical side of things, the cost of visiting a psychiatrist can be off-putting to many people. Someone may have no personal or ideological aversion toward psychiatry – they want the perspective, diagnosis, and prescription from a psychiatrist – but they are unable to – or don't want to – pay the cost. The average psychiatrist's fee is between $100 and $300 per appointment, and around $500 for an initial consultation. After several or continual appointments with a psychiatrist, treatment for mental health can turn out to be quite expensive. And based on the uncertainty of whether people will initially get the right diagnosis (misdiagnosis is common) or find the correct medication and dosage, people may decide that, financially, seeing a psychiatrist isn't worth it.
Financial concerns, however, really only apply to visiting a psychiatrist with a private practice. If you live in a country with universal healthcare, or if your health insurance plan covers psychiatric treatment, then there may be fewer financial disincentives. Practically speaking, though, seeking help from a psychiatrist though universal healthcare can be more challenging than if seeking assistance from a private psychiatrist, due to issues like waiting lists and overstretched services, leading to limited appointments.
The reasons for avoiding psychiatrists are manifold. If you are someone who is in psychological distress – or someone close to you is – and psychiatry is an option being considered, it's important to carefully think about what might be behind hesitancy about going down that route. Being as informed as possible about psychiatry will ensure that any decision made is based on evidence and what your needs are in that moment.
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anti-psychiatry, critical psychiatry, psychiatric medication, psychiatrist, psychiatry, psychotherapy, stigma, therapy
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text:
Synaptec Raises £2.9M in Funding
Published on May 16, 2019 By FinSMEs
Synaptec, a Glasgow, UK-based energy tech company, raised £2.9m in funding.
Backers included:
– the Foresight Williams Technology EIS Fund, which invested £2m,
– the newly created Foresight Scottish Growth Fund, which invested £100k, and
– existing shareholders, including The Scottish Investment Bank, the investment arm of Scottish Enterprise, Equity Gap and the University of Strathclyde, which invested £800k.
The funding will be used to scale-up production, grow international sales and exploit future data analytics opportunities.
Founded in 2015 as a spinout from the University of Strathclyde and led by Philip Orr, Managing Director, Synaptec has developed innovative technology that can reduce downtime and allow monitoring of the complex electric power grid, using existing optical fibre networks.
The technology measures voltage, current, temperature, and vibration over long distances, at multiple locations, without power supplies, and using only a single standard optical fiber.
The system has already seen demand for its systems from international customers.
The innovations developed by the company are based on work Orr and his co-founders conducted at the University of Strathclyde's Institute for Energy and Environment.
Tagged with: Equity Gap, Foresight Scottish Growth Fund, Foresight Williams Technology EIS Fund, Scottish Investment Bank, Synaptec, University of Strathclyde
Previous storyDNA Script Secures $38.5M in Series B Funding
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By FinSMEs	Published on October 3, 2014
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Planning / Sep. 05, 2018
Off-Price Retailer Familia Deploys Merchandise Planning Solution from TXT Retail, an Aptos Company
Leading Russian retailer known for its 'treasure hunt' experience optimizes planning and buying decisions across categories
ATLANTA — Sept. 5, 2018 — TXT Retail, an Aptos Company, today announced that Familia, a leading Russian off-price retailer, has successfully rolled out the TXT Retail Merchandise Planning solution across its product categories and more than 200 stores.
The TXT Retail solution is now supporting Familia in all aspects of strategic product and store planning to set up financial targets for the company.
The Merchandise Planning solution is in use by multiple teams and departments, including analysts, buyers, the product team and the finance department.
The technology initiative is a joint delivery with system integrator KORUS Consulting, TXT Retail's partner in Russia.
Familia sells a wide range of apparel, footwear, accessories, household goods and other merchandise from global brands, with up to an 85 percent discount.
During the next project phase, Familia is focusing on in-season planning and the ability to deal with supply and demand variability faster and with greater efficiency.
"Familia is the only retailer in Russia operating in the off-price format and has a successful business model that is much appreciated by consumers, and also extremely complex to manage with constant change," said Noel Goggin, Aptos CEO and culture leader.
"We are proud to deliver a successful implementation in a business area that is so strategic to Familia, while also continuing to expand Aptos' presence in Russia. Together with our local partner KORUS Consulting, Aptos is prepared to meet the growing demand from tier-1 retailers in Russia for advanced planning applications that support their merchandise lifecycle and business transformation," Goggin said.
About KORUS Consulting:
KORUS Consulting is a Russian system integrator that offers services in the creation, optimization, and automation of business processes. Founded in 2000, now KORUS Consulting has developed a unique expertise in retail optimization, successfully working with the dozens of fashion, grocery, DIY and specialty retail chains. Learn more: www.korusconsulting.com


2015 was a year that I didn't expect to be elk hunting, as I'd drawn a great early archery elk just two years prior. I was able to kill a 370" 7x7 on the fourth day of that hunt. As most hunters know, it isn't easy to get drawn for two early season elk tags in three years but that's exactly what happened. I drew a tag in a unit that most would consider less than optimal but having grown up and hunted in the unit my whole life I felt I could still kill a good bull.
Trail cameras were placed starting in June and checked throughout the summer. Unfortunately we weren't seeing anything real big and we're getting discouraged as the beginning of September approached. I ended up guiding a deer hunter the week leading up to the hunt so my plans of scouting hard that week were shot. As opening day came I had no idea where I was even going to start. I decided I would go help my dad on his hunt in another unit for the first three days and come up with a game plan when I got back.
Upon returning to my unit the following week I was able to chase a few bulls and pass on some small ones but could never find what I was looking for. The temperatures were in the mid 80's and the bulls weren't talking so that wasn't helping either. After a hard weeks hunt and only seeing one bull over 300" I was about to throw in the towel. I went into town to get some lunch when my friend called me saying he was watching a bull in the 340-350" range and it was in an area no one would ever expect. I skipped the lunch idea and headed straight out there. We located the bull and knew it was going to be tough because he had 30 cows and 5 satellite bulls following him around.
Tough was an understatement when it came to getting close to this bull. He was in wide open country and with all the elk around him it felt more like spot and stalk archery antelope hunting. Over the next four days we couldn't get closer than 100 yards from him without getting busted by a cow. Finally on the fifth day and third before the last day of the hunt he made his fatal mistake. I glassed the herd up from about a mile away near a pond. I got over to them as fast as I could and thankfully they hadn't moved far. The bulls were screaming and I had an idea of where they were headed so I got in front of them and waited. They were moving down a fence line that they didn't want to cross and I had set up just 30 yards from the fence. Eventually I had cows moving by me at 20 yards. Cows in front of me, behind me, all over the place. Just when I thought they would smell me the bull let out a bugle just on the other side of the juniper tree I was hiding in. Next thing I knew he stepped out at 15 yards and I put an arrow in him, which at the time I thought was too low to kill him. He ran out to 30 yards and I put another one in him that I knew finished him off because he fell over within sight. Just like that all the frustration and negativity about the hunt was forgotten and my bull was down. He was even nice enough to die in a spot we could get the truck to and load him up. We taped him at 343" with 19" and 20" firsts and seconds. He was a great bull to finish off a tough hunt.
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We're 32 days into the record-breaking US government shutdown, and while most economists agree it will weigh on US economic growth, the chorus of warnings about doomsday scenarios is getting louder.
Bank of America Merrill Lynch reiterated its concern about the economic cost of the shutdown. It "definitely becomes a significant shock if it lasts for months rather than weeks," Ethan Harris, the head of global economics research, told the Financial Times. "There is a sensitivity in the markets to signs of dysfunction in Washington."
The White House even increased its internal estimate of the hit to gross domestic product. A White House official confirmed to Business Insider that the Trump administration's model estimated that the shutdown would shave off 0.13 percentage points from GDP for every week of the shutdown - higher than the 0.08 percentage points originally assumed.
JPMorgan CEO Jamie Dimon said that the shutdown was a serious problem for the US economy and cited research that found US GDP growth could go to zero if the shutdown continued.
Credit Suisse economists estimated that the shutdown would come to an end relatively soon and shave off 0.6 points to 0.8 points from first quarter GDP. But if the closure were to go for longer than another week or two the economic impact could be seriously damaging. "If the shutdown persists though, a substantially larger drag is possible," the Credit Suisse economists wrote. "An outright contraction in the first quarter, and downgrades to the entire 2019 outlook are not out of the question."
Moody's economist Adam Ozimek told Business Insider that while contraction isn't likely, "you also can't rule it out." Ozimek also decried the unforced error caused by the shutdown. "The fact that we are even discussing the possibility of a wholly government created contraction in GDP is enough to really make you scratch your head," he said.


Italian rough-haired Segugio are an ancient Italian hunting dog breed. They date back probably to the time of Phoenix traders from ancient Egypt. They are present, in fact, in several Egyptians drawings at the time of the Pharaohs. Since their introduction in Italy they became very popular and still are today.
Italian rough-haired Segugio are strongly built, mesomorphic dogs. Their trunk has a perfect symmetry and harmony on the whole. They have medium built muscles and well developed bones, but a thin aspect. Their body does not present any fat under skin.
Italian rough-haired Segugio are very extrovert dogs - lively and playful. They are agile and fast, which makes them one of the best hunting dog in the world. They are gifted with an exceptional sense of smell and find traces of game during hunting very easily. They have very sweet eyes and a pleasant ringing voice. They love helping their master in the hunt and like walking, running, and exploring around in the woods, never getting apart their master. They are a very affectionate and obedient breed.


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The Simple Reality About Free Outdoors Golf That Nobody Is Telling You
9.	Adrian Peterson. The Minnesota Vikings chosen Adrian "All Day" Peterson within the 2007 NFL Draft. Peterson went on to set an NFL file for many rushing yards in a recreation and win NFL Offensive Rookie of the 12 months. Peterson continued to excel with the Vikings and the Brett Favre led offense.
For an umpire, calling them as seen issues more than being favored. Every name makes a friend and an enemy. The integrity of the game is more necessary. As the great arbiter of our nationwide pastime, the umpire stands between the unprincipled lords of Camelot who crave to win at all costs and the simple peasants who care extra about getting it right, letting the chips of victory fall the place they might. Most acutely aware of this dilemma, Mark Twain, when given the prospect to umpire a recreation in 1887, chose instead to ponder the sport from the centerfield bleachers. The very considered calling balls and strikes from behind the plate triggered him to build a field of dynamite to brandish at any and all fans who might disagree with one among his calls. Good deterrent, Mr. Clemens!
But each seem to be very all the way down to earth.
5.	Ben Roethlisberger. Large Ben has spent his entire career with the Pittsburgh Steelers, leading them in two Tremendous Bowl victories-turning into the youngest Tremendous Bowl successful quarterback at only 23. Roethlisberger and the Pittsburgh Steelers have dominated a lot of the last decade, although Ben has had his share of accidents and controversy to associate with his success.
Nicely, this one is fairly obvious. Andrew Bynum has struggled after coming back from a mid-season knee damage and Dwight Howard was unstoppable vs. the Cavs. The thing Bynum ought to offer that Cleveland did not is enough athleticism and dimension to make Howard shoot over him. If Howard is not dunking the ball, he's a mean offensive participant. If the rotation of Gasol, Bynum and Mbenga and stay in front of Howard and make him shoot excessive, he won't be almost as effective. Howard is the Defensive Player of the Yr and he's a beast on the boards. L.A. will have their fingers full with this match up.
•	Aggressive firms' earnings reports
I played at the Junior National Championship twice once I was sixteen and 17. The primary time I ever went was among the finest occasions of my life. I got there a few days early and went to the conference center where we have been going to play and received to walk round. I used to be amazed at what number of courts there were and the way massive the building was. When the primary game was about to start I was so excited, I had never felt like this before any other volleyball game in my life. Before the primary sport they choose a player to sing the Nationwide Anthem which was actually cool getting to listen to a regular individual similar to everybody there singing. When the primary recreation begins everybody is very excited and aggressive because I believe when enjoying in a tournament the primary game defines how you will play for the rest of the event. Once I was 16 we opened up by enjoying towards the number one group within the match.
Youth basketball fundamentals are the cornerstone of basketball expertise as youth become better gamers. There are three major key issues that it is advisable understand with reference to constructing basketball skill. These three things vary from psychological, to physical, and revolve round discipline. If a participant doesn't adhere to these three key steps we will explore, they won't move ahead in their quest to get better on the craft of basketball.
Its attraction is that it's a world sport. Mark Cuban has change into famous as an NBA owner who was all the time loud, brash, and never overly concerned with what others considered him, including NBA Commissioner, David Stern. The 4 ending holes make up one of the toughest home stretches in the entire PGA Tour.
Posted in: Golf
The Birth of Players Football Game Free
The Death of Players Football Game Free


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The Rise of The Metaverse. What Should The Gambling Industry Expect?
Written by Chris James
Where would we be without technology? It has changed the way we work, play, communicate, and more, while its influence has also transformed entire sectors, including the wonderful world of iGaming.
However, perhaps one of the most fascinating things about the tech world is how it never seems to sit still. Fresh innovations seem to emerge year after year, and, at present, all eyes are on a major development that is on its way. Yes, the metaverse is on its way, and it has the potential to completely revolutionize the game in iGaming and beyond.
Based on a collection of assumptions and hypotheses, the team at Uplatform analyzed the latest trends and technological innovations to formulate a possible metaverse scenario for gaming.
When we talk about the metaverse, what exactly do we mean? It is a rather complex idea, but that has not stopped people from trying to define what it is or will be. Earlier this month, a report by Global Industry Analysts examined the area and provided its own description of the concept.
The organisation outlined how the metaverse is regarded as the internet's future, with it revolving around an ecosystem involving mobile networks, social media, virtual and augmented reality, and other elements. Global Industry Analysts also stated that the worldwide metaverse market could reach $758.6 billion by 2026.
Interest in the concept is undoubtedly high and IZEA Worldwide recently examined how the issue is impacting social media influencers. It found that 70 percent believe the metaverse will replace social media, while it added that one of the top activities for those looking to get involved in the area is gambling. So, with that in mind, what could the future of iGaming look like as the metaverse develops?
Metaverse in iGaming
We cannot predict the future with certainty, but it is undoubtedly fun to speculate. For instance, how great would it be to wear a headset and experience an authentic casino experience modelled on renowned locations like Macao or Las Vegas? Even if you're sitting in your living room, the metaverse may be able to transport you away to the heart of the action.
Maria, Head of Marketing in Uplatform, shared her thoughts about how land-based casinos could expand their presence with Metaverse.
"I believe that casinos are set to benefit hugely from the exciting new immersive nature of the metaverse. It's expected to be a futuristic step beyond the experience towards what you might call super-real casino gaming. For a long time, the pinnacle of immersion was live dealer games, where players could sit in the comfort of their home and interact with other players and a dealer at a poker or blackjack table.
However, virtual reality technology has given new life to the idea of immersive gambling. VR and Metaverse gaming go beyond just social interaction with a dealer over chat communication by providing players with the sights, sounds, and atmosphere of a real casino. I'm expecting, that many of the casino games we know and love will remain the same in the Metaverse. Blackjack will still be blackjack, and roulette will still be roulette. These games might have additional features, and most of them will probably function on a Metaverse token or crypto payment system, but the fundamental games will remain the same."
A metaverse online casino could be designed to closely mirror gaming floors in integrated resorts in cities like Las Vegas and Macau or it could be completely different, perhaps with various them options like underwater, space, or the Wild West.
On a similar note, this technology could have a massive bearing on the future of live casino experiences. These games have risen to prominence in recent years, but the metaverse could impact them in many ways. For example, it could introduce a new format of navigation, while it could even change deposits and betting.
The main difference between online casino gaming and metaverse casino gaming is that you will be much more physically involved in the metaverse. Donning your VR or AR headset is all that's needed to enter the virtual world, and from there, you'll be able to walk around and go wherever you want.
Imagine walking into an expensive-looking virtual casino, where a friendly host greets you and directs you to your favourite table. You take a seat, chat with the other players, and start playing for real money! Metaverse casino gaming is set to take live casino gameplay to a fascinating new level!
In addition, just imagine being able to watch the latest big sporting events in the metaverse. The technology could let you experience the best seats in the stadium or venue from the comfort of your own home. It could very well take betting to a whole new level, as you might be able to swipe through a wide array of options on side menus as the action unfolds in front of you.
The Metaverse has really sparked a fire under the seats of the gambling industry, though, and many providers are hard at work creating virtual and decentralized casinos. The concept of metaverse casino gaming represents a significant step into the future, something many of us have only ever dreamed of or seen in movies. Launching the endlessly popular online casino gaming industry in a virtually accessible world will mark the start of a new era of gamification. More elaborate and futuristic games and gambling opportunities will become the new norm.
A new era of VR
While all of that might be pure speculation, it is clear that augmented and virtual reality could have a big part to play in the metaverse. The latter has already had an impact in the iGaming world to some extent, as some organisations have taken the time to craft VR experiences in recent years.
For example, leading developer Evolution outlines how its Gonzo's Treasure Hunt title offers the option to play in a virtual reality mode. However, the metaverse could really signal a new dawn for the technology, as it could become a crucial part of how we access iGaming and other experiences going forward.
Another element that could have an influence on iGaming's future in the metaverse is the NFT. The concept of non-fungible tokens has become a real talking point in recent months and Bloomberg recently reported on estimates that suggest the market was worth around $40 billion in 2021. Finally, socialisation might also be a big part of iGaming in the metaverse, as it could change the way that players and dealers communicate. Wouldn't it be fun to meet up with friends in a virtual casino and explore a range of games together? It is an interesting possibility that could well become a reality.
A new reality
So much of our speculation about the metaverse and iGaming might have sounded like science fiction a few years ago. However, with recent events like the pandemic highlighting how technology can bring people together and create fresh experiences, it suddenly feels closer than ever before.
Many organisations are already investigating what the metaverse could mean for them and how they could play a role in it, so an exciting future undoubtedly awaits. It will be fascinating to see how this all develops and we are keen to find out if some of our own predictions come to fruition.
Based in entire virtual worlds, like something out of a sci-fi movie, metaverse casinos look set to be the next big thing for the gambling industry, and they're already here and ready to be explored.
Published on: 11th April 2022
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Tamera Foster has had her fair share of Rihanna comparisons since joining the X Factor, and her love of leather leggings isn't the only thing earning her the likeness.
Her flawless complexion and incredible ability to rock a bold lip colour are really reminding us of the Bajan beauty, but we're not the only ones. Former X Factor champ, James Arthur, recently described Nicole Scherzinger's contestant as 'a better looking Rihanna'.
So you can hardly blame us for making a beeline for Tamera's make-up chair when the X Factor's chief make-up artist, Julia Carta, took us behind the scenes.
Julia talks us through the easy-to-master look below. Enjoy!


Student focused. Depending on thier level and examination board we will work through the specifications together. We can also focus on any topics that students find difficult. We will work with online videos, create own revision resources and go through past papers. But ultimately I will work with the student to discover how they learn best.
I currently teach Biblical Hebrew in 2 high schools up to GCSE level to the full classes, and also give private or group tutoring for the GCSE too.
Specialist in Chinese, Japanese, korean , Thai, spanish, swedish Deep tissue and sport massages with more than 4 years of experience in Birmingham and manchester. Rite now availability is for Manchester only. Female only massage, 10£ an hour with money back guarantee if customer is not satisfied and first visit is no charge! Highly professional and 100%satisfaction is guaranteed.
Hola! My name is Laura and I am a native Spanish speaker from Madrid. I have a passion for the Spanish language and enjoy helping others to learn it. I have 4 experience of teaching a wide range of different age groups of all levels for more than three years. I offer Skype lessons and will customize the lessons to both your level and your specific needs.
My approach depends on the level of the student.
Religions Studies exam preparation courses for GCSE to A-Level in Manchester and North West.
I'm fun, relaxed and respond to your individual needs. It will feel like being taught by a friend. Natural, easy.
My teaching method is based on books that i have used for my exams and notes are provided. There will also be practice given during lessons.
Having a good foundation is very important therefore i will start from thw basic and take note of the standards of each student.
Fully qualified and experienced chemistry and science teacher who is currently teaching in the UK.
My teaching method involves questioning and formatively assessing a student using a range of methods in order to find out that student's weak topics and skills. This gives me an idea about what we need to work on and improve.
Health and social care student with 10 years of experiance in care can offer you help with level 2 and 3.
I teach one topic at a time i can do 1 to 1 or teach a few together.
The way I teach is based on the student's need, since every person is different, but I like to use different material to not get bored, and learning in different ways, especially the Speaking.
Computer Science student offers a basic programming lessons up to university level in The University of Manchester.
My teaching method is first giving the problem and then the solution, explainig things most simple way with associations from life.
Masters student offering academic English tutoring up to grade 12 level. I will assist with essay writing skills and understanding the English language.
My teaching method starts with understanding the level each student is at in order to adequately supplement the skills one has in a given subject.
Politcs and international relations student offering German, English and Hungarian classes with teaching experience.
I believe in the power of conversations and switching your free time activities to the language you want to learn.
Eager Hospitality Business Management student, that enjoys the english language and wants to teach.
My teaching method, is to start off ''fun''. I try to make the other person happy. I'm willing for other people to interrupt me, if they have a question, or if I'm going too fast. I talk positively and fluently.
Passionate physics tutor and current Masters in engineering student giving GCSE physics lessons in Manchester!
My methodology is to relate theory to practical everyday life experiences. Physics can sometimes be hard to get your head around, especially for younger ages. It is easier to understand how to apply the knowledge and theories if they can relate it to everyday life and understand why it's needed or what it's used for.
I like to have fun when coaching football as when the player is enjoying himself is more likely to improve. If the activity is engaging and stimulating then much more can be taken away from it in my opinion. There will be a lot of time with the ball at feet and sessions will be well planned to make the best of the time available.
A-level student currently studying Maths based in Bolton tutoring up until high school level Maths.
My teaching method is aiming to listen to the student and approaching my teaching ways specific to the student as everyone learns differently.
My teaching method is to get students interested into the topic, learn it with them and look at ways to improve their understanding.
Having been taught multiple teaching styles to myself, I can test and adapt my teaching style to suit the student to make is as easy as possible to understand.
Manchester-based pofessional actor/playwright in Manchester offering advice on all things theatre.
To engage and excite younger pupils into finding confidence with text and finding comfort on stage, harbouring natural instincts and talent.
Hi, love to tell you all I know to add to your knowledge.
I am University graduate for Computer Science and I have knowledge of the subject area and I am able to transfer it to you.
Learning a new language can be really repetitive and boring. if you choose to learn with me I will introduce fun, creative and exciting methods for learning English. Learning any new language should be with an aim for creativity and excitement, as you're more likely to remember what you've learnt AND want to learn again.
Giving lessons to primary school any maths subject and extremely cheap price.
My teaching method is by starting with the basics or whatever you don't know and then building it up. If they do not understand I will go over it until they get it. I am committed to getting it right.
Software engineer offering in depth knowledge in programming languages with industrial practical examples to individual or group.
My teaching Methodolgy is always starts from scratch.. So no prerequisite. Only interest is a prerequisite.. Also I believe more hands on will make you understand the topics very clearly... So in my class I will give more hands on each topic and every quarter one project will be given as assignment.. On completion one end to end project will be given as assignment.


Defence Minister John Faulkner has joined his New Zealand counterpart Dr Wayne Mapp at a Gallipoli ceremony honouring fallen ANZAC and Turkish soldiers.
Senator Faulkner took the opportunity to visit Turkish battlefields and war memorials after attending a NATO Defence ministers meeting in Istanbul.
He and Dr Mapp laid wreaths at Lone Pine, the Turkish National Memorial, Chunuk Bair and ANZAC Cove.
"The sacrifice at Gallipoli is deeply felt by Australians almost 100 years after the 1915 campaign, and is a fundamental part of our cultural identity," Senator Faulkner said on Sunday.


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László Kövér turned down Orbán's offer to be head of state
Jan 1, 2022 Gergely Gulyás, Katalin Novák, László Kövér
Chancellor Gergely Gulyás gave a long interview to atv.hu in which he spoke about Fidesz's nomination of Katalin Novák to become the next head of state.
According to Gulyás, Novák was chosen because "out of several possible candidates, László Kövér (pictured) did not want it, and knowing this, we agreed that nominating Katalin Novák was the best choice."
The minister confirmed in the interview that Viktor Orbán first offered the job to founding Fidesz member and current House Speaker László Kövér, but "he clearly indicated that now, as before, he was not interested in taking the seat as the head of state."
The interview with atv's Ildikó Csuhaj also includes this brief exchange:
Csuhaj: Do you consider [opposition prime ministerial candidate] Péter Márki-Zay a dangerous character?
Gulyás: To the opposition or the government?
Csuhaj: Either one.
Gulyás: Yes, to one of them. To one of them, very much.
[HVG]
Prosecutor General's Office not saying much about Völner corruption case
What Hungary's leading politicians posted to Facebook on the last day of the year