text:
\section{Introduction}
\label{sec:intro}

The galaxy \object{ESO 243-49} situated at $z=0.023$, is an almost edge-on, S0 or early-type spiral, located 0.3 Mpc from the central dominant galaxy in the cluster \object{Abell 2877} \citep{sant08}. \object{ESO 243-49} is one of the larger galaxies in the cluster \citep{huds01}.  Given its size and proximity to the host cluster centre, \object{ESO 243-49} is expected to have suffered dynamical effects, such as interactions or accretion of other bodies, though little evidence for such events were noted by  \cite{sant08} after analysing $R$-band data of this galaxy.

\object{ESO 243-49} is however fairly exceptional as it hosts the intermediate mass black hole (IMBH, $\sim$10$^{2-5}$ M$_{\odot}$) candidate \object{ESO 243-49 HLX-1} \citep{farr09}.  The observational evidence for the existence of IMBHs has until recently been weak, with few convincing examples, but they have been proposed to play a role in a number of astrophysical scenarios, including the formation of supermassive black holes through mergers and accretion \citep[e.g.][]{mada01}. Some IMBHs may avoid such mergers or may even be ejected during merger interactions \citep{merr04}. Studying these IMBHs and their environment should allow us to understand their origin, either as remnant primordial BHs \citep[][e.g.]{yoko97,duec04}, or from runaway stellar collisions \citep[e.g.][]{gier15,arca16}, or as the remnants of population III stars \citep[e.g.][]{rico16} for example and how they are fuelled \citep[from stellar winds, via Bondi accretion, or from Roche lobe overflow, e.g.][]{mill02,mill04}.

HLX-1 is situated just 8$\arcsec$ from the centre of \object{ESO 243-49}. HLX-1 was shown to be associated with the galaxy using optical spectroscopy of the optical counterpart \citep{sori10} which revealed an emission line consistent with the Balmer H$_\alpha$ line compatible with the distance of \object{ESO 243-49} \citep{wier10,sori13}. The physical process resulting in an  H$_\alpha$ emission line is unclear, where it could be from an accretion disc around the IMBH, created by material accreted from a companion star \citep{laso11} or the host star cluster or a photo-ionised/shock-ionised gas nebula close to HLX-1 \citep{wier10}. However, as \cite{sori13} stated, the  narrow  FWHM  of  the  line  observed from HLX-1 either requires an extremely face-on disk ($\leq$3$^\circ$) or, implies that the line does not originate from a Keplerian disc. They suggest that it may then come from a low density nebula around the IMBH.

The X-ray flux from HLX-1 has been shown to vary by a factor of $\sim$50 \citep[][and Fig.~\ref{fig:XrayLC}]{gode12}, quasi-periodically, initially with a period close to one year \citep{laso11}, but more recently, the period between outbursts has lengthened significantly, which may be due to the companion star becoming unbound from the IMBH \citep{gode14}. Whilst HLX-1 is faint, the X-ray emission is hard, typical of the X-ray emission seen in X-ray binaries in the low/hard state \citep{gode09a}. In the bright state, the emission is soft \citep{gode09a,serv11,yan15}, typical of the X-ray emission seen in X-ray binaries in the high/soft state.  Moreover, radio flares emitted during the transition from the low/hard to the high/soft state have also been observed \citep{webb12}, adding to the similarities between HLX-1's behaviour and that of X-ray binaries. The increase of flux in the case of HLX-1 was thought to be due to matter being tidally stripped from the companion as it passes at periastron, falling onto the IMBH \citep{laso11}, but this model has recently been questioned by various authors \citep[e.g.][]{king14,laso15}.

The mass of HLX-1 has been estimated to be $\sim$10$^4$ M$_\odot$ from modelling the X-ray spectrum with a variety of accretion disc models and from Eddington scaling \citep{gode12,serv11,davi11,webb12,stra14}.  The formation mechanism for HLX-1 is not clear from previous observations. \cite{webb10} proposed that HLX-1 could be an intermediate
mass black hole that was once at the centre of a dwarf galaxy, that had interacted with the host galaxy \object{ESO 243-49}, possibly like LEDA 87300 \citep{bald15,grah16}.  \cite{farr12} suggested that this merger may have been recent, possibly accounting for the presence of dusty lanes in the central regions of \object{ESO 243-49}. However, their study using {\em Swift} X-ray data and {\em HST} ultra-violet to infra-red photometry could not exclude that HLX-1 resides in an old stellar population, reminiscent of a globular cluster, one of the places IMBH are expected to form \citep[e.g.][]{mill04}.

To test the merger scenario, \cite{musa15} took {\em Australia Telescope Compact Array} (ATCA) H{\sc I} radio observations of ESO 243-49 and the surrounding neighbourhood, in order to search for signatures of a recent merger event.  No H{\sc I} emission was detected, indicating that any recent merger that may have taken place was not gas rich. The absence of gas may be due to the cluster environment depleting ESO 243-49's H{\sc I} gas reservoir.  They also identify another galaxy in the cluster \object{Abell 2877} undergoing a merger, where gas is being depleted due to the cluster.

\cite{mape12} investigated the minor merger scenario using N-body/smoothed particle hydrodynamics simulations and concluded that it was indeed possible.  However, to make realistic simulations of a merger between ESO 243-49 and another body that would give rise to the IMBH HLX-1, it is essential to know the mass of the supermassive black hole (SMBH) at the core of \object{ESO 243-49} and the mass of the galaxy.  The mass of SMBH can be estimated through the stellar velocity distribution of the central regions of the galaxy \citep[e.g.][]{gult09,grah13}. Alternatively, the mass can be estimated thanks to the correlation with the bulge luminosity. Such single parameter scaling relations, and indeed why we came to believe in massive BHs, are extensively reviewed in Graham (2016).   A third independent method for estimating the black hole mass is the {\em black hole fundamental plane} \citep[e.g.][]{merl03,koer06}. This plane best relates the radio emission for black holes in the low/hard state, the X-ray emission and the mass across more than eight orders of magnitude in black hole mass.

The stellar kinematics and population (i.e., age and metallicity), as well as the gas content are further parameters that can constrain realistic merger simulations. To make these constraints, we observed the galaxy \object{ESO 243-49} using the new integral field unit on the Very Large Telescope (VLT), {\em Multi Unit Spectroscopic Explorer} \citep[MUSE,][]{baco10}.  The data were taken in August 2014 during the Science Verification time for this new instrument. These data are the subject of the current paper, combined with {\em X-Shooter} data of \object{HLX-1} to make constraints on the nature of this source. We also re-analyse some archival data to estimate the mass of the central supermassive black hole in \object{ESO 243-49} using the different methods described above.

\section{Data reduction}

A brief overview of the observations used in this paper are given in Table~\ref{tab:obs}. The details of each data set are given in the following subsections.

\begin{figure*}
\includegraphics[width=18cm]{HLX1lc170317_new.eps}
\caption{Swift X-ray lightcurve of HLX-1 from 2008-2016. The four arrows show times when optical spectroscopy was taken and whether or not a significant detection of the H$_\alpha$ line was made.}
\label{fig:XrayLC}
\end{figure*}

\subsection{MUSE data}

Twelve 500s observations centred on \object{ESO 243-49} (RA = 01$^h$10$^m$27$\fs$746, dec= -46$^\circ$04$^\prime$27$\farcs$41, J2000) were taken with {\em MUSE} installed on UT4 of the VLT (PI: N. Webb). Four observations were taken on 2014 August 26, along with one blank sky image (taken after two target observations) and the remaining 8 were taken the following night, with a further two blank sky observations, one taken after the first pair of observations and a second after the third pair.  All the observations were made whilst HLX-1 was in the low/hard state, as determined from quasi-simultaneous {\em Swift} X-ray data (see Fig.~\ref{fig:XrayLC}). Bias, dark, flat and arc observations were taken each night and a field for the astrometric model was taken the 26th. Spectrophotometric standards were taken on the 27th August 2014.  {\em MUSE} was used in the wide field mode, which has a field of view of 1 $\times$ 1 arcmin$^2$ sampled at 0.2\arcsec. The spectral range covers 4750-9300 \AA, with a medium spectral resolution (average $\sim$3000). A maximum of 1\arcsec\ was recorded for the seeing. We used the {\em Recipe Flexible Execution Workbench} \citep[Reflex,][]{hook08} {\em MUSE} Workflow v1.0.1 \citep{weil14} to reduce the data. The data reduction was done in a similar way to \cite{baco15}. Bias, arcs and flat field master calibration solutions were created using the relevant exposures obtained each night. The bias and dark masters were subtracted from the ESO 243-49 observations, the blank sky observations and the sky flats. The observations were then divided by the master flats. An additional flat-field correction was made with the sky flats to correct for the difference between sky and calibration unit illumination. The wavelength calibration was done using the 15 Ne, Xe, HgCd arc observations made on each of the two observing nights. Further geometric and wavelength corrections were carried out using tables from the {\em MUSE} consortium, to calibrate in space and wavelength. The sky continuum and line correction was done by using the task {\em muse\_create\_sky} on observations of blank sky close to ESO 243-49 and taken between two observations of the galaxy and then subtracting these from the target observations. The astrometric fields and spectrophotometric standards were used to find the astrometric solution and calibrate the flux (respectively).  The data cube was produced from pixel-tables using a 3D drizzle interpolation process which included sigma-clipping to reject outliers such as cosmic rays. Using 5 bright, but non-saturated stars in the field, the offset between each observation was calculated using {\em iraf} and then all 12 data cubes were combined to make one single deep exposure.

\begin{table
\caption{Summary of the observations used in this paper}\label{tab:obs}
\centering
\begin{tabular}{lccc}
\hline \hline
Instrument & Data & Date & MJD  \\
\hline
MUSE/VLT & optical  & 26-27 Aug 2014 & 56895-6\\
 & spectroscopy &  & \\
X-Shooter & UV-IR & 3, 6, & 56538,41, \\
/VLT & spectroscopy & 29 Sep 2013 & 56564\\
WFC3/HST & H-band & 23 Sep 2010 & 55462\\
ATCA & 5.5+9 GHz& 13 Sep 2010& 55452\\
ACIS/Chandra & 0.5-10 keV & 6 Sep 2010 & 55445\\
XRT/Swift  & spectrum & 13-14 Sep 2010 & 55452-3\\
XRT/Swift  & lightcurve & Oct 2008 & 54763-\\
 &  & -Aug 2016 & 57628\\
\hline
\end{tabular}
\end{table}

\subsection{X-Shooter}

A total of twenty exposures was taken with the VLT instrument {\em X-Shooter} \citep{vern11} on the 3, 6 and 29 September 2013 (PI: N. Webb). These were centred on the intermediate mass black hole candidate \object{ESO 243-49 HLX-1} \citep[RA = 01$^h$10$^m$28$\fs$3, dec= -46$^\circ$04$^\prime$22$\farcs$3,][]{webb10}. Two observations were made on 3 September, 8 on 6 September and 10 more on the 29 September, whilst HLX-1 was in the low/hard state. The combined exposures totalled 16360s in the 5595-10240\AA\ (VIS) band, 12000s in the domain 10240-24800\AA\ (NIR) and 17400s in the domain 3000-5595\AA\ (UVB). The slit, of length 11$\arcsec$  was placed at the parallactic angle for all the observations. The slit width was set to 0.9$\arcsec$ for the VIS and NIR observations and 1.0$\arcsec$ for the UVB observations. The spectral resolution was 5100 for UVB, 8800 for VIS and 5300 for NIR for a source such as the galaxy filling the slit, but slightly better for a point like source with good seeing.  The seeing was between 0.8-0.9$\arcsec$ on 3 September, $\sim$0.7$\arcsec$ on 6 September and just over 1$\arcsec$ on 29 September.

The data were reduced with Gasgano and the X-Shooter pipeline \citep{modi10}. A master bias was created for each night of observations for the UVB and VIS observations and subsequently subtracted from the data. A master dark was created and subtracted from the NIR data.  The data were flatfielded and the orders were traced, the spectra were extracted and calibrated in wavelength and flux. The HLX-1 spectrum was derived from the combined spectrum and spectra of the galaxy ESO 243-49, from either side of HLX-1, were also determined.  The flux due to the galaxy at the position of HLX-1 was determined from the adjacent galaxy spectra and this subtracted from the HLX-1 spectrum, to correct for the diffuse galactic emission.

We also took advantage of the release of {\em X-shooter} science data products. The 2D spectra were downloaded from the ESO archive and then {\em iraf} tools, notably {\em apall} were used to extract the 1D spectra of HLX-1 and the galaxy. The galaxy spectrum, scaled to the value at the position of HLX-1, was subtracted from the HLX-1 spectrum as before.

\subsection{HST data}

An 806 s exposure in the $F160W$ ($H$-band) of the galaxy \object{ESO 243-49} was obtained with the {\em Wide Field Camera 3} onboard the {\em Hubble Space Telescope} ({\em HST}) on 23 September 2010, as described in \cite{farr12}.  The reduced images were analysed using the new tasks {\em Isofit} and {\em Cmodel} which comprise a new fitting formalism for isophotes to allow more accurate modelling of galaxies with non-elliptical shapes, such as disk galaxies viewed edge-on. These tasks are described in detail in \cite{ciam15}.  We extracted the 1-D major-axis surface brightness profile, $\mu(R_{\rm maj})$, which we further decomposed into its photometric constituents with the software $Profiler$, which solves for the best-fit parameters by minimising the RMS (root mean square) scatter $\Delta_{\rm rms} = \sqrt{\sum_{i=1,n} (\mu_{{\rm data},i} - \mu_{{\rm model},i})^2 /(n-\nu)}$, where $n$ is the number of data points, $\nu$ is the number of degrees of freedom and $\mu_{\rm model}$ is generated at each iteration and consists of the summed components convolved with the PSF \citep{ciam16}. The PSF was estimated by fitting a Moffat profile to 8 bright, unsaturated stars in the image, with the IRAF task $Imexamine$.

\subsection{ATCA data}

ESO 243-49 was observed with the Australia Telescope Compact Array (ATCA) on 13 September 2010 (PI: N. Webb), using the upgraded Compact Array Broadband Backend \cite[CABB,][]{wils11}. The data were taken using the CFB 1M-0.5k correlator configuration with 2 GHz bandwidth and 2048 channels, each with 1 MHz resolution. The observation was performed at the central frequencies of 5.5 GHz and 9 GHz simultaneously. The array was in the 750 m configuration (giving baselines up to 5 km when all 6 antennas are used).  The total on-source integration time was $\sim$11 h. The primary calibrator PKS 1934-638 was used for absolute flux and bandpass calibration, while the secondary calibrator 0048-427 was used for the phase and antenna gain calibration. For each observation, we observed 1934-638 for 10 min and the phase calibrator was observed every 15 min.

The data reduction and analysis was performed, as described in \cite{webb12}, with the Multichannel Image Reconstruction, Image Analysis and Display (MIRIAD) software \citep{saul95}.

\subsection{Chandra data}

10 ks of X-ray data were taken with the {\em AXAF CCD Imaging Spectrometer} (ACIS) onboard {\em Chandra} on 2010 September 6 (ObsID 13122, MJD 55445). These data were reduced in the standard way, as described in \cite{serv11}.  Thanks to the excellent spatial resolution (half energy width = 0.8$\arcsec$), emission from the central SMBH in ESO 243-49 situated at just 8$\arcsec$ from HLX-1 is resolved. We extracted the photons in a 5$\arcsec$ radius centred on ESO 243-49.  We examined four different background regions of the same size as the source extraction region, placed above and below the galaxy bulge and to the left and right of the galaxy, as shown in \cite{serv11}, their figure 5. The background in each of these four regions was found to be the same.

\subsection{Swift data}

{\em Swift} XRT Photon Counting data dating from 2008 to 2016 (PI: O. Godet) were processed using the tool XRTPIPELINEv0.12.6, as described in \cite{webb12}.  The lightcurve of these data can be seen in Fig.~\ref{fig:XrayLC}. We analysed the spectrum of 11 ks of {\em Swift} data taken on the 13-14th September 2010. To do this we
took the grade 0-12 events, giving slightly higher effective area at
higher energies than the grade 0 events.  The
ancillary response files were created using XRTMKARF v0.5.9 and
exposure maps generated by XRTEXPOMAP v0.2.7. We fitted the
spectrum using XSPEC v12.7.0 with the response file
swxpc0to12s6\_20010101v013.rmf \citep{gode09b}.

\section{Results}

\subsection{HLX-1}

To investigate the nature of the H$_\alpha$ emission line associated with HLX-1 we extracted the HLX-1 spectrum using regions with a radius of 3 pixels from the {\em MUSE} datacube. To correct for the diffuse emission from the galaxy, background spectra were extracted using similar sized regions around HLX-1, where no point-like sources were detected and the emission scaled to equal that at the position of HLX-1. This was then subtracted from the HLX-1 spectrum.  The spectrum corrected for the galaxy emission can be seen in Fig.~\ref{fig:HLX1spectraMUSE}. The blue nature of the spectrum, as noted in \cite{farr12} is immediately obvious. Estimating the (AB) V and the R band magnitude from the spectral continuum we find values of V=24.97$\pm$0.25 and R=24.76$\pm$0.25 (1 $\sigma$) and comparing these to previous values \citep[e.g.][]{webb14} we find that the magnitudes are comparable to the faintest detections that were made during the low/hard state.

We investigated the region around 6721 \AA\ (see insert of Fig.~\ref{fig:HLX1spectraMUSE}) where \cite{wier10} and \cite{sori13} detected an emission line with a flux $\sim$1-2 $\times$ 10$^{-17}$ erg cm$^{-2}$ s$^{-1}$. Such a line, if the flux had not varied since the previous detections using {\em FORS2} on the {\em VLT} (which were made during the high/soft state, see Fig.~\ref{fig:XrayLC}), should be detected with a signal to noise of 4.7 per spectral bin of 1.1\AA. No significant emission line was detected at this wavelength, although a fluctuation, resembling an emission line, with a signal to noise ratio (SNR) of $\sim$2 (signal to noise of the continuum $\sim$0.8, 1$\sigma$ detection) was noted (see inset of Fig.~\ref{fig:HLX1spectraMUSE}). This fluctuation is centred at 6720.3 \AA, and has a flux of $\sim$3 $\times$ 10$^{-18}$ erg s$^{-1}$ and a FWHM$\sim$12.5 \AA, similar to the value found by \cite{sori13}.  We take the flux value as the 1 $\sigma$ upper limit for the emission line, indicating that the line flux has varied by a factor of $>$6.

\begin{figure}
\includegraphics[width=9cm]{HLX1spectraMUSE.eps}
\caption{Smoothed (Gaussian boxcar=3) galaxy subtracted {\em MUSE} spectrum of HLX-1. Insert shows the region around the H$_\alpha$ line.}
\label{fig:HLX1spectraMUSE}
\end{figure}

We also searched for other emission lines that may also be observed from the region around an ultra-luminous X-ray source or an IMBH. We searched for H$_\beta$ (4861 \AA), [O {\sc III}] (4959 and 5007 \AA) as well as various H{\sc I} lines. However, we found no evidence for any of these lines, where  the 1 $\sigma$ upper limits on these lines are 1.2$\times$10$^{-18}$ erg cm$^{-2}$ s$^{-1}$ for H$_\beta$, 1.6$\times$10$^{-19}$ erg cm$^{-2}$ s$^{-1}$ for [O {\sc III}] (4959 \AA) and 4.7$\times$10$^{-19}$ erg cm$^{-2}$ s$^{-1}$ for the 5007~\AA\ line.

The {\em X-shooter} data were also taken during the low hard state. We examined the HLX-1 spectrum corrected for the galaxy emission. No emission lines around 6721 \AA\ were found (both the gasgano reduced and the ESO reduced spectra were analysed). If the flux was the same as that observed during the high state, we would expect to detect the line with signal to noise of $\sim$3 per spectral bin of 0.3 \AA.  However, if the flux in the line was similar to the upper limit identified from the {\em MUSE} data, then a signal to noise of $\sim$0.9 per spectral bin of 0.3\AA\ would be expected, insufficient to detect the line.  The flux level in the continuum for HLX-1 in the low hard state is expected to be negligible (signal to noise of 0.05-1.0 per pixel in the UV and VIS wavelength ranges using the {\em X-Shooter} exposure time calculator), making it difficult to place upper limits on other possible emission lines. None of the lines investigated in the {\em MUSE} data, nor O {\sc II} (3726 and 3729 \AA), or the Bowen blend (4686 \AA) nor the Paschen and Brackett lines, were detected.

\subsection{The galaxy ESO 243-49}

\subsubsection{The mass of the central supermassive black hole}
\label{sec:MassSMBH}

Figure~\ref{fig:decompositionESO243} displays, from top to bottom: the modelled {\it HST} major-axis light profile, the residual profile ($\Delta\mu$), the isophote ellipticity ($\epsilon$) profile (also Fig.~\ref{fig:decompositionESO243}) and finally the $B_4$ harmonic amplitude (the measure of the isophote's boxiness or discyness) profile.  In addition to the bulge and edge-on disc components, the light profile displays the characteristic signature of a bar. We determined a major-axis bulge S\'ersic index \citep{grah05} of $n = 1.44 \pm 0.08$, and half-light (effective) radius of $R_{\rm e} = 1.84 \pm 0.11\arcsec$.  The (black hole mass)--(host spheroid S\'ersic index) scaling relation of \cite{savo16} yields a SMBH mass estimate of $1.4 \times 10^7 M_{\odot}$, with a $1\sigma$ interval of $(0.7 - 3.0) \times 10^7 M_{\odot}$.

\begin{figure}
 \centering
\includegraphics[width=9cm]{Decomposition_new_ciambur.ps}
\caption{$H$-band major-axis surface brightness profile of ESO~243-49. The red circles are the data extracted from the $HST$ image, while the black curve represents the best-fitting model, which in turn is built up of a spheroid/bulge (red dashed line), a bar (yellow dot-dashed line) and an edge-on disc (blue dotted line). The inset numbers are the S\'ersic parameters of the bulge. The residual profile is shown in the next panel below, followed by the ellipticity and $B_4$ amplitude (discyness) profiles.}
\label{fig:decompositionESO243}
\end{figure}

To compute the total magnitude of each component, we mapped the major-axis profile onto the `equivalent-axis', which circularises each isophote such that its enclosed area is conserved ($R_{\rm eq} = R_{\rm maj} \sqrt{1-\epsilon(R_{\rm maj})}$, where $\epsilon$ is the isophote ellipticity). We determined the $H-$band bulge apparent magnitude to be $m_H = 12.72\pm0.10$ [Vega] mag, and a bulge-to-total flux ratio of $0.25\pm0.06$, making this a barred S0 or S0/a galaxy. The mass of the central SMBH in ESO~243-49 was estimated using the (black hole mass)--(host spheroid luminosity) relation \citep{savo15} to be $2.3 \times 10^7 M_{\odot}$. Taking into account the scatter on the relation places the mass in the ($1\sigma$) range of $(0.5 - 11) \times 10^{7} M_{\odot}$. As this scaling relation is calibrated for 3.6 $\mu$m, we assumed a $(H - 3.6 \mu m)$ colour of $0.55\pm0.18$ \citep{savo15}.

We extracted the {\em MUSE} spectra from within the effective radius determined from the HST data and determine its velocity dispersion using the Penalized PiXel-Fitting software \citep[pPXF][]{capp16,capp04}. The PSF was determined to be less than 1$\arcsec$, much smaller than R$_e$, therefore we did not correct our measurement for the PSF. To determine the central velocity dispersion, we used the full MILES stellar library \citep{sanc06,falc11} and the same method as described in Section~\ref{sec:kinematics}. This gives a central velocity dispersion of 224$\pm$1 km s$^{-1}$, which is fairly high, but may be due to the bar discerned in this galaxy \citep[e.g.][]{hart14}. Using the relationship for a barred S\'ersic galaxy given in \cite{grah13} we determine a black hole mass of 10.6 $\times$ 10$^7$ M$_\odot$. Taking into account the RMS scatter on the relation gives a mass range of 4.8 -- 23 $\times$ 10$^7$ M$_\odot$.

The X-ray photons extracted from the region surrounding the SMBH in ESO 243-49  in the {\em Chandra} data, are soft. Fitting a typical galaxy spectrum to these photons (mekal in $xspec$), as described in \cite{serv11}, we determine an unabsorbed luminosity in the 0.2-10 keV domain of $\sim$6 $\times$ 10$^{39}$ erg s$^{-1}$, assuming a source
distance of 95 Mpc \citep[using the WMAP cosmology,][]{benn13}. The ATCA data reveal a 5 GHz flux of 180$\pm$15 $\mu$Jy/beam (1 $\sigma$ error). To estimate the mass of the black hole using the X-ray and radio fluxes/luminosities, we used the sample presented by \cite{merl03}, which includes black holes in all states and the correlation presented from the analysis of this sample by \cite{koer06}. The energy bands used in \cite{koer06} are better suited to the ESO 243-49 SMBH,  as the X-ray emission is soft and shows very few counts in the 2.0-10.0 keV band used by \cite{merl03}, leading to large uncertainties in the X-ray luminosity.  We determine a mass of 2.9 $\times$ 10$^8$ M$_\odot$. Taking into account the errors on the radio and X-ray fluxes, as well as on the relationship gives a mass range of  0.029 -- 290 $\times$ 10$^8$ M$_\odot$.  However, \cite{serv11} state that the X-ray emission appears to be extended and therefore it may not come from the central SMBH, but from diffuse gas around the central black hole, in which case this mass estimate is not reliable.

Although the radio and X-ray data are taken a week apart, analysing the {\em Swift} data taken on the same day as the radio data, we do not see any strong evolution of the flux from the SMBH. We prefer, however, to use the luminosity estimated from the {\em Chandra} data, as this is more accurate thanks to a better spatial resolution than {\em Swift}.

\subsubsection{Stellar and gas kinematics}
\label{sec:kinematics}

\begin{figure*}
 \centering
\includegraphics[width=6cm]{eso24349_kin_new.eps}
\includegraphics[width=6cm]{eso24349_kin_h3h4_new.eps}
\includegraphics[width=6cm]{eso24349_pop.eps}
\caption{Top left: Stellar velocity in ESO 243-49 as determined from the {\em MUSE} data. Bottom left: Stellar velocity dispersion in ESO 243-49. Top middle: Skewness of ESO 243-49. Bottom middle: Kurtosis of ESO 243-49. Top right: Age. Bottom right: Metallicity in ESO 243-49. Each figure is centred on ESO 243-49 and the distance in arcsec is the offset from the galaxy centre in right ascension and declination.  The X marks the position of HLX-1.}
\label{fig:ESO243}
\end{figure*}

We also investigated the kinematics of the galaxy \object{ESO 243-49}. To do this we binned the combined data cube in the spatial directions to create pixels (spaxels) with a signal to noise of 50. We chose a signal to noise of 50 as it allows  robust extraction of the kinematics and stellar populations while keeping a reasonable spatial sampling \citep[e.g.][]{capp11}. We used the adaptive spatial binning software developed by \cite{capp03}, based on Voronoi tessellation. We estimated the original SNR of each spectrum by taking the ratio of the signal and the square root of the variance produced by the {\em MUSE} pipeline. We took the median of that ratio between 5500 \AA\ and 6000 \AA\ which is representative of the wavelength range used for extracting the stellar kinematics and population properties. The adaptive spatial binning delivered more than 62\% of the bins with a SNR equal to or greater than 50. The central 3\arcsec\ were not binned as the signal to noise was above 50 for each pixel, with a scatter of 6 and a minimum signal to noise of 40.

We used the full MILES stellar library that covers the wavelength range 3525 - 7500 \AA\ with a constant spectral resolution of 2.50 \AA\ FWHM, similar to but lower than the {\em MUSE} spectral resolution. Since the difference in spectral resolution between the {\em MUSE} data and the MILES stellar library, i.e., 0.2 \AA\ FWHM at 5000 \AA\ ($\sigma$ = 5 km s$^{-1}$), is significantly lower than ESO 243-49 velocity dispersion ($\sigma >$ 50 km s$^{-1}$), we did not convolve the stellar library to the same spectral resolution as the observed spectra. We derived the first four order moments of the line of sight velocity distribution (LOSVD), namely stellar velocity (V), velocity dispersion ($\sigma$), skewness of the stellar distribution ($h_3$) and kurtosis of the stellar distribution ($h_4$), for each spaxel of the {\em MUSE} cube, in the following manner. We set up pPXF to use additive polynomials of the 8th order and the default value of penalisation (0.4). We restricted the fitted wavelength range to 4600 - 6800 \AA\ as it contains strong absorption lines (H$_\beta$, Fe, etc.) as well as to avoid spectral regions highly contaminated by sky lines residuals ($\lambda >$ 7000 \AA). We masked five bright sky emission lines at 5577 \AA; 5889 \AA; 6157 \AA; 6300 \AA, and 6363 \AA, as well as the potential H$_\alpha$ and N {\sc II} gas emission lines.  We first fitted the stacked spectrum of the central 2\arcsec with the full MILES stellar library, and then used the best fit (resulting from a combination of $\sim$30 original MILES templates) as the stellar template to fit each spatially binned spaxel of the {\em MUSE} data.

The galaxy is clearly rotating with speeds up to $\sim$200 km s$^{-1}$ (see Fig.~\ref{fig:ESO243}, top left). We discern a disc and an inner thin disc in Fig.~\ref{fig:Vcut} as shown in \cite{come16}. There is also evidence for the presence of a slower (than the disk) spheroid component, see Fig.~\ref{fig:ESO243} (top middle) in which an anti-correlation of the skewness parameter can be seen with respect to the velocity field in Fig.~\ref{fig:ESO243}, \citep[top left, e.g.][]{bend94,kraj08}. The correlation of the skewness parameter with the velocity field along the major axis around 3-5\arcsec\ is likely to be associated with the inner-disk, as evidenced from modelling the H-band photometric data of the bulge of ESO 243-49, see Section~\ref{sec:MassSMBH}. We extracted optical spectra of the extremities of this disc, from the {\em MUSE} data. Strong H$_\alpha$ and [N {\sc II}] (6583 \AA) emission lines are detected in this region. We used the Doppler shift of these lines to determine the rotation rate of the gas in the disc. The H$_\alpha$ line and the [N {\sc II}] are centred at wavelengths of 6717.4$\pm$0.5 \AA\ and 6738.4$\pm$0.5 \AA\ on the left side of the disc respectively and at 6703.7$\pm$0.5 \AA\ and 6725.3$\pm$0.5 \AA\ on the right side of the disc respectively. This indicates maximal speeds of 300 km s$^{-1}$. We find that the radius of the inner disc is 3.9$\arcsec$ or 1.8 kpc.

Using the spectrum extracted from the central pixel of the galaxy we determine the wavelength of the  H$_\alpha$ and [N {\sc II}] (6583 \AA) emission lines, as well as the Na D (5892.5 \AA), Mg {\sc I} (5175.4 \AA) and Ca (5269.0 \AA) absorption lines due to the galaxy. We detect these lines at 6710.6 \AA, 6731.0\AA, 6025.5\AA, 5290.7\AA\ and 5387.3\AA\ respectively which gives a redshift of the galaxy of $z=0.0225\pm0.0001$. Searching for any perturbation to the galaxy that could be caused by a merger event, we examine the stellar velocity distribution, the stellar velocity dispersion, the stellar skewness and kurtosis of ESO 243-49 as well as the stellar age and metallicity distributions (see Figs.~\ref{fig:ESO243} and \ref{fig:Vcut}). All of the distributions are smooth, with no region showing different behaviour from the rest of the galaxy. The rotation of the galaxy is homogeneous as is the velocity dispersion. The exception is the more rapidly rotating disc in the centre of the galaxy seen in the skewness distribution (i.e., central anti-correlation seen in the skewness (h3) and stellar velocity (V) maps). The stellar velocity dispersion peaks in the central regions of the galaxy (following the high velocity gradient in this region) and falls off more slowly to the exterior where the velocity gradient is low, as would be expected for a non-perturbed galaxy (see also Fig.~ \ref{fig:Vcut}). A similar result has also been seen by \cite{come16}.

\begin{figure}
\includegraphics[width=9cm]{eso24349_kin_cut_new.eps}
\caption{Top: The stellar velocities (km s$^{-1}$) as a function of the distance from the centre of ESO 243-49.  Bottom: The stellar velocity dispersion (km s$^{-1}$) as a function of the distance from the centre of ESO 243-49.  Orange points are along the major axis and blue points are offset at 3\arcsec.}
\label{fig:Vcut}
\end{figure}

We also examine the age and metallicity of the stellar population of \object{ESO 243-49} (see again Fig.~\ref{fig:ESO243}), using the MIUSCAT library \citep{vazd12}. We used a subset of 120 models from the MIUSCAT library covering an age range of 0.5 to 14.1 Gyr, and a metallicity range of -0.71 to +0.22 dex, therefore all included in the "SAFE" range of the library \citep[see][for more details]{vazd12}. These models were computed using a unimodal IMF with a slope of 1.3 and based on Padova isochrones \citep{gira00}. We used the same pPXF settings as for the kinematics analysis except that we used only multiplicative polynomials of the 12th order. The age and metallicity values are mass-weighted and obtained from a regularisation approach as in \cite{guer16}. Some spatial bins gave very young ages but the spectra showed relatively strong sky residuals which biased the fits so these bins were not deemed reliable and were masked in the plots. These masked bins are located in the outskirts of the galaxy.  This analysis reveals that the central disc is old ($\sim$12-13 Gyr) and metal-rich \citep[see Fig.~\ref{fig:ESO243}, top and bottom right and consistent with the independent analysis of][see their figure 5]{come16}.  There is nothing peculiar in other regions of the galaxy nor at the position of \object{HLX-1}.

\subsubsection{Other objects in the ESO 243-49 field of view}
\label{sec:background_sources}

To better understand the dynamics in \object{ESO 243-49}, we extracted the {\em MUSE} spectra of the brighter globular clusters, identified using the HST observations. However, due to their faint nature, no useful spectral information could be obtained.

Examining the spectra of other sources in and around \object{ESO 243-49} reveals some interesting objects. Firstly, the {\em blue patch} noted in \cite{wier10} and \cite{sori13} located at 01$^h$10$^m$27$\fs$99 -46$^\circ$04$^\prime$23$\farcs$55 and with extent of $\sim$11 pixels ($\sim$2$\farcs$2) shows a very strong emission line at 6763.3\AA\ (wavelength in air), with an equivalent width of -125 \AA, likely to be H$_\alpha$ at a redshift of $z=0.0306\pm0.0001$.  A second line at 5010.0 \AA\ with an equivalent width of -350 \AA\ is then H$_\beta$ and we also identify O{\sc III} (5007\AA) at 5160.0 \AA\ and two other significant lines at 5576.5 \AA\ and 6088.87 \AA.  The extent, spectral features and redshift of this source implies that it is a background galaxy.  Four other background objects are also identified thanks to their H$_\alpha$ and H$_\beta$ lines, but at much greater redshifts. The positions and redshifts of these sources can be seen in Table~\ref{tab:bkg_objects}.

\begin{table
\caption{Background objects in the field of view of ESO 243-49}\label{tab:bkg_objects}
\centering
\begin{tabular}{ccc}
\hline \hline
RA & dec. & z  \\
\hline
01$^h$10$^m$27$\fs$99 & -46$^\circ$04$^\prime$23$\farcs$55 & 0.0306$\pm$0.0001\\
01$^h$10$^m$27$\fs$07 & -46$^\circ$04$^\prime$32$\farcs$55 & 1.280$\pm$0.004 \\
01$^h$10$^m$28$\fs$55 & -46$^\circ$03$^\prime$56$\farcs$15 & 1.13$\pm$0.01 \\
01$^h$10$^m$29$\fs$74 & -46$^\circ$04$^\prime$47$\farcs$95 & 1.140$\pm$0.002 \\
01$^h$10$^m$27$\fs$76 & -46$^\circ$04$^\prime$52$\farcs$35 & 1.240$\pm$0.003 \\
\hline
\end{tabular}
\end{table}

\section{Discussion}

The non-detection of the H$_\alpha$ line in the vicinity of HLX-1 in the {\em MUSE} and the {\em X-Shooter} data indicates that the  H$_\alpha$ line flux has diminished by more than a factor 6 since HLX-1 was observed in the high/soft state.  The line flux would not be expected to vary by at least a factor 6 over a year if the emission were to emanate from a nebula, as the size of such a nebula is expected to be much larger than the distance travelled by the electromagnetic radiation from the central X-ray source over one year. The variability of the H$_\alpha$ line also implies that the emission is not related to star formation, as no such variations on this timescale are expected. The variability suggests that the H$_\alpha$ emission comes from close to the black hole, either from the disc or possibly from a corona, thus confirming the distance of $\sim$95 Mpc and re-enforcing its association with the galaxy \object{ESO 243-49}.  Further, the fact that no [O {\sc III}] (5007 \AA) is detected in the {\em MUSE} or the {\em X-Shooter} spectra, nor He II (4686 \AA) in the {\em X-Shooter} spectrum, counts against a ULX bubble \citep{sori13}.

Confirming the distance to \object{HLX-1} also corroborates that \object{HLX-1} shows sub-Eddington outbursts \citep[e.g.][]{gode14}. \cite{laso15,laso11} state that if HLX-1 is indeed at 95 Mpc and shows sub-Eddington outbursts, then the outbursts can not be driven by the thermal–viscous disc instability. The outbursts are then likely to be triggered as material from a companion star in a highly eccentric orbit, impacts the inner regions of the accretion disc around the IMBH, as the star passes at periastron \citep{webb14}. In this case the mass-transfer propagation cannot be viscous but must be mediated by waves, as proposed in \cite{webb14,laso11}. We have demonstrated that such a binary could form and remain bound for a number of orbits \citep{gode14}. \cite{gode14} demonstrated, however, that such a system would then slowly become unbound, due to tidal effects and increasing mass transfer. This indeed appears to be occurring, if the outbursts we observe are due to the passage at periastron of the companion star. We have observed four full orbits that last approximately one year and since then, the subsequent orbits have been 13.5 months, 15 months and $>$26 months (see Fig.~\ref{fig:XrayLC}). The alternative to this scenario, as suggested by \cite{king14}, proposes that the variability seen is due to the precessing of relativistic jets. However, this is ruled out by the fact that if the increase in luminosity is due to the jet precessing into our line of sight, we would expect the X-ray emission to become harder due to the Doppler boosting, but instead we observe softer emission \citep{gode09a,serv11}. Further, as the H$_\alpha$ emission can not be due to star formation, as noted above, then the H$_\alpha$ may be produced by photo-ionisation by the X-ray source or collisional ionisation by an outflow.  The H$_\alpha$ emission should be nearly isotropic for any situation where it is powered by photonisation or a low speed shock.  The relatively narrow line suggests that this is the case for HLX-1.  As a result, if it is powered by photoionisation, it should be a tracer of the luminosity of the source averaged over $4\pi$, and if it is powered by a shock, it should be constant in luminosity.  The fact that the H$_\alpha$ emission is detected from this source near its peak, despite the low column density local to the source, suggests that there is not a strong beaming of the X-ray flux \citep[see also][]{farr11}.  The fact that the luminosity varies, such that it is found to be a factor of at least 6 fainter when the X-ray luminosity is low than near the X-ray peak, indicates that the emission is not from collisional ionisation in a large shock.  Therefore, the totality of the evidence from the H$\alpha$ emission indicates that the X-ray source is not strongly beamed.  These constraints apply generically to beaming models, and not only to the particular model of \cite{king14}.

As explained in Sec.~\ref{sec:intro}, HLX-1's behaviour shows many similarities with black hole X-ray binaries. Indeed black hole X-ray binaries often show the H$_\alpha$ line luminosity dropping as the X-ray and optical emission drops \citep{fend09}. \cite{hyne02} also showed that the  H$_\alpha$ emission was correlated with the continuum emission in V 404 Cyg and \cite{jin12} and \cite{pane06} showed a correlation between the H$_\alpha$ emission and the X-ray luminosity in active galactic nucleii (AGN). Further, \cite{dewa08} showed the same correlation for AGN with lower mass black holes, approaching the mass of the black hole in HLX-1, supporting the idea that we could expect to observe less H$_\alpha$ flux in the low/hard state than was observed in the high/soft state.

Alternatively, the variability may not be linked to the X-ray state, but the phase at which we observed HLX-1, in a similar way to that observed in the black hole binary XTE J1118+480 \citep{torr04}.  If we suppose that HLX-1 goes into outburst as the companion star reaches periastron \citep{laso11}, which we can call phase 0, and that the time between outbursts is the time taken for the companion to orbit the black hole, the spectroscopy presented by \cite{sori13} was taken shortly after this time (roughly at phase 0) and that presented in \cite{wier10} was taken almost three months after phase 0 (roughly at phase 0.25). The {\em X-Shooter} data were taken between one month and one week before outburst, i.e. around phase 0.95 given the roughly year long orbit. The {\em MUSE} data were taken 4 months before outburst (where that orbit had a 15 month duration), i.e. around phase 0.75. The data taken at different points in the orbit may then lead to the variability observed.

The four mass measurements of the central SMBH in ESO 243-49 are very similar. The estimate using the black hole fundamental plane has larger error bars than the other estimates. It should also be noted that the X-ray emission appears to come from hot diffuse gas \citep{serv11} and not from an accretion disc. Further, there is no evidence for a low luminosity AGN in the optical spectra. The X-ray emission may then be due to star formation in the central region, which may also account for the radio emission. Therefore the mass estimate using this method should be used with caution and at best as an upper limit. We therefore take only the mass estimates from the two other methods which give a 1$\sigma$ range of  0.5-23 $\times$ 10$^7$ M$_\odot$  for the mass of the central SMBH in ESO 243-49.

The rapidly spinning disc discerned in the {\em MUSE} data, compared to the slower bulge is compatible with mergers in the history of the galaxy, e.g. \cite{arno14}.  \cite{mape15} found using Smoothed Particle Hydrodynamic simulations, that the fingerprints of minor mergers of dwarf galaxies with elliptical galaxies is the formation of a gas ring in the S0 galaxy. This ring may be related to the orbit of the satellite galaxy, and its lifetime should depend on the merger properties.  The high gas velocity observed from the inner disc may be related to the bar discerned in Sect.~\ref{sec:MassSMBH}, which could be oriented towards the observer (boxy bulge, but not peanut) and would then explain the high gas velocity. Indeed the isophotal fitting supports this interpretation.

Whilst the current {\em MUSE} data is insufficient to examine the region around HLX-1 and determine whether this object is associated with ESO 243-49 due to a minor merger, as first proposed in \cite{webb10}, or whether it was born in situ, the rapidly rotating central disc in ESO 243-49 is compatible with the idea that such mergers may have taken place during the history of the galaxy.  Given the close proximity of ESO 243-49 to the most massive central galaxy in the cluster, a number of close satellites and minor mergers are to be expected, as noted in Sec.~\ref{sec:intro}.   If there has been a dry minor merger in the past, it should have taken place more than a dynamical time ago, i.e.  t $>$ 300 Myr as we no longer see any evidence of such an event \citep{barn92,duc13}. However, with regards to a minor-merger that gave rise to HLX-1, it is less clear. Maybe the minor-merger is still ongoing, with the orbit of the dwarf galaxy being highly eccentric so that the timeframe for the dwarf galaxy to encounter the host galaxy again would be long. Without additional radial velocity for the system, it is difficult to assess the status of the merger and only with future data and detailed computer modelling will it be possible to estimate the time of the latest minor-merger.

\begin{acknowledgements}
Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 60.A-9328 and 091.D-0823. We thank the referee for constructive and pertinent suggestions that helped to improve this paper.  NW, MC, OG, DB, AG, AD, and MM acknowledge the Centre National d'Etudes Spatiales (CNES) for their support.
\end{acknowledgements}

   \bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


"MOIL must make significant contribution to Make in India by developing technology to meet manganese requirement of batteries to be used in Electric Vehicles etc," Singh was quoted as saying.
NEW DELHI: Bullish on future prospects for the electric vehicles in the country, Steel Minster Birender Singh today asked state-owned MOIL to make significant contribution to the Centre's 'Make in India' programme by developing technology to meet manganese requirement for batteries to be used in electric vehicles.
In view of growing future prospects for the electric vehicles in the country, the minister said the PSU needs to take measures to remain a leader in the market.
Chairing the mid-year review meeting of MOIL, the minister also asked the PSU to plan for building capacities in tungsten mining and production for strengthening manufacturing capabilities for defence production in India, the Ministry of Steel said in a statement.
He further said, the miner should strategically plan for forward integration to leverage its leadership position of manganese ore production in India. The company can also think of acquiring or taking majority stake in ferro-alloy production facilities, in addition to expansion efforts.
There is huge potential for e-rickshaws, e-tempos and e- cars in India, he told the PSU and said MOIL must be prepared for harnessing. In fact, the company should innovate to find new uses of manganese ore, apart from steel making, dry cell batteries and paints, he added.
Further, he advised MOIL that R&D efforts should aim for development of new technologies rather than updating or buying technologies from others and there is a need to work on utilising every grade of ore gainfully including the lowest quality ore.
The minister assured that his ministry will support every R&D initiative aimed at self-sufficiency and indigenisation. Mineral exploration activities need to be speeded up for strengthening the resource base in India.
MOIL can also examine the feasibility of using alternate modes of ore transportation, which could be environment friendly and cost effective. For closure of mines, sand requirement can be met by innovative means like collaboration with local farmers, he said.
In view of increase in requirement for manganese for steel production capacities up to 300 million tonnes and insufficient availability of the ore in India, MOIL must also explore the possibility of acquiring or taking stake in manganese ore assets abroad, the minister said.
Steel Secretary Aruna Sharma, senior officials from the Ministry of Steel and top management of MOIL were among those who attended the meeting.


August 12, 2014, news broke that Robin Williams, the star of Popeye and many more movies had died, apparently by his own hand. My thoughts quickly returned once more to Popeye Village Malta and this earlier review of our visit.
Hubby and I had a fun day out at Popeye Village, which can be found near Mellieha on the Island of Malta. The fact that we were two adults, approaching middle age made not one difference to the visit experience.
However, if you visit as a family or with a group of children the experience will be even better. Since our visit, Popeye or Sweethaven Village has grown in size and added many more attractions.
We stayed at the resort Bugibba on the Mediterranean Island of Malta. Sandy beaches are in short supply on this lovely Island and Bugibba has only rocks near the water's edge where holiday makers gather like basking seals.
Mellieha is only a short bus journey west of Buggiba and has a pleasant village, a magnificent church, some hotels and a beautiful sandy beach; this meant that we visited a couple of times during our two-week vacation.
We actually came upon Popeye Village almost by chance.
Being too hot for the beach at Mellieha one day we opted for a stroll. Not far from the beach we saw a dirt track between fields which had Popeye Village signposted. The sign stated the distance and as it did not sound far away, intrigued, off we went.
As we strolled in the hot afternoon sun there were huge gourds at the side of the road. It was September and the crops were rolling in. About halfway along this track we could see back to Mellieha and forward to the coast in the south of the island, where Popeye village is located. This part of the island is so slender that you can see the water in both the north and the south of the island at once; well you can if you look at the right time and you are in the right place.
One thing we learned when we visited Malta is that the island's tourism is ingenious and inventive. Anything that could be even remotely turned into a tourist attraction is! This made for some unusual and fascinating attractions.
Popeye Village was actually the set of the 80's Robin Williams film Popeye.
Ever the opportunists the Maltese had turned this set into an attraction for tourists. These days it is more like a small theme park though.
When we visited the entrance fee was reasonable, so in we went.
The setting was certainly perfect. Popeye Village is set on the coast of Malta where the beach is a soft sand and the waters turquoise blue. There was a tourist shop with the usual gifts such as Popeye tea-towels and numerous items displaying Popeye Village or Malta.
Hubby and I stuck our heads through wooden cut-outs of Popeye and Olive. When I find the old photos, if I ever do, I will scan them and add to this review.
These days the programme of events includes boat trips, mini golf, beach sun bathing, wine tasting, a silversmith demonstration, fun park, cinema screenings and more. There are special school package deals for organised visits. Popeye Village also hosts various corporate events.
The characters and events at Popeye Village will vary according to the time of year.
But I have fond memories of our visit to a less commercialised Popeye Village.
Even if you just briefly visit, like we did, and sunbathe, have a dip in the Mediterranean, stroll around Popeye village and saunter back to Mellieha it is a great day out.


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Sumptuous fine Italian leather, traditional details and elegant design combine to create the luxurious Charisma sofa collection. With deep scroll arms, high padded back and button detailing, the collection boasts a range of sofas and chairs to elevate your home with style. Finished with dark wood accents and turned wood feet for a polished look, the Charisma collection is available to order online in a choice of high-quality leather finishes, with the full vibrant range of shades available to view and order in store. Manufactured using a hardwood frame, which is expertly carved by master craftsmen, for the ultimate in durability and support. A handy storage stool completes the range, helping you to create a streamlined and seamless feel in your home.


Today's baleen whales (Mysticetes) support their massive bodies by filtering huge volumes of small prey from seawater using comb-like baleen in their mouths much like a sieve.
But new evidence based on careful analysis of a 34-million-year-old whale skull from Antarctica–the second-oldest "baleen" whale ever found–suggests that early whales actually didn't have baleen at all. Their mouths were equipped instead with well-developed gums and teeth, which they apparently used to bite large prey.
Like modern whales, Llanocetus had distinctive grooves on the roof of its mouth, the researchers explain, which usually contain blood vessels that supply the baleen. In Llanocetus, however, those grooves cluster around tooth sockets, where baleen would have been useless and at risk of being crushed.
The findings suggest that large gums in whales like Llanocetus gradually became more complex over evolutionary time and, ultimately, gave rise to baleen. That transition probably happened only after the teeth had already been lost and whales had switched from biting to sucking in small prey–as many whales and dolphins now do. Marx and Fordyce suggest that baleen most likely arose as a way to keep such small prey inside the mouth more effectively.
Soft tissues, including baleen, normally rot away, making it difficult to study their evolution. As a result, researchers must rely on indicators preserved on the bones, such as tell-tale grooves or lumps indicating the position of a muscle, or holes for the passage of particular blood vessels and nerves.
In the new study, Fordyce and Marx found that the broad rostrum of Llanocetus had sharp, widely spaced teeth with marked tooth wear suggesting that they were used to bite and shear prey. As in living Mysticetes, the palate bears many grooves, which have commonly been interpreted as evidence for baleen. However, the researchers showed that those grooves instead converged on the bony tooth sockets, suggesting a peri-dental blood supply to well-developed gums, rather than racks of baleen.
The findings show that the evolution of filter feeding wasn't as straightforward as previously thought, the researchers say. They'd now like to sort out when filter feeding and baleen first evolved.


The first danish Danish National Championship in SUP was finally a reality after tree weeks of following cancelations because of hopeless weather conditions. Normally it always very windy in the Northern Part of Jylland, accually the wind have shaped the landscape and trees grow sideways - BUT - as soon as this event was announced Mother Nature decided otherwise, and the wind turned arround and stayed there for several weeks!
But as they say in Denmark - the third time is where the luck set in - and finally the conditions were right.
Here is a photo essay from this great event and I'm sure that this is an event which we will hear much more about in the future.
Try it out, SUP is a very fast growing water sport for everyone and next year is already being planned as I'm writhing this post.


text:
Kacey Musgraves Welcomes A Baby Deer To Her Home
Train Derailment This Morning in Richmond County: The Richmond County Sheriff's Office says 9 CSX railroad cars derailed this morning in the area near 11th and Walton Way, all on CSX property. …
Nancy Brooks // Country Writer, Beasley Media Group July 22nd, 2020
Kacey Musgraves has, like many of us, had a rough 2020. For Kacey not only the virus and her tour getting canceled, but she recently divorced her husband of a couple years, Ruston Kelly.
Musgraves did have something very pleasant happen to her in the last few days as she shared a special visitor to her Nashville area home.
She posted to Instagram a few photos and a video of her touching a baby deer, "Still not over this and never will be. It made this year hurt a little less for just a few. It kept visiting me. Such a beautiful memory. (the last pic is mama coming back to get her baby. I watched the reunion from the window.)"
Kacey Musgraves (L) and Shane McAnally, winners of the Best Country Song award for 'Space Cowboy, pose in the press room during the 61st Annual GRAMMY Awards at Staples Center on February 10, 2019 in Los Angeles, California.
Katy Perry, Dolly Parton, and Kacey Musgraves perform onstage during the 61st Annual GRAMMY Awards at Staples Center on February 10, 2019 in Los Angeles, California.
Kacey Musgraves attends the 91st Annual Academy Awards at Hollywood and Highland on February 24, 2019 in Hollywood, California.
2019 iHeartRadio Music Awards – Show
LOS ANGELES, CALIFORNIA - MARCH 14: (EDITORIAL USE ONLY. NO COMMERCIAL USE) Kacey Musgraves performs onstage at the 2019 iHeartRadio Music Awards which broadcasted live on FOX at Microsoft Theater on March 14, 2019 in Los Angeles, California. (Photo by Kevin Winter/Getty Images for iHeartMedia)
Kacey Musgraves performs onstage for Loretta Lynn: An All-Star Birthday Celebration Concert at Bridgestone Arena on April 1, 2019 in Nashville, Tennessee.
Female Artist of the Year winner Kacey Musgraves poses in the press room during the 54th Academy Of Country Music Awards at MGM Grand Garden Arena on April 07, 2019 in Las Vegas, Nevada.
Kacey Musgraves performs at the 2019 Governors Ball Festival at Randall's Island on June 01, 2019 in New York City.
Kacey Musgraves performs at Red Rocks Amphitheatre on June 26, 2019 in Morrison, Colorado.
Kacey Musgraves and Ruston Kelly attend the Country Music Hall of Fame and Museum opening of new exhibition, Kacey Musgraves: All of the Colors, at Country Music Hall of Fame and Museum on July 01, 2019 in Nashville, Tennessee.
Kacey Musgraves discusses her new exhibit: "Kacey Musgraves: All Of The Colors" at Country Music Hall of Fame and Museum on July 06, 2019 in Nashville, Tennessee.
Kacey Musgraves performs as she opens for George Strait during the first of his "Strait to Vegas" shows at T-Mobile Arena on April 22, 2016 in Las Vegas, Nevada.
Kicks99

redpajama_set_name: RedPajamaCommonCrawl


I have lost a front tooth in an accident.In the treatment another tooth has been removed(its a milky tooth)It lead to have a bridge for over five teeth.Now i would like to have implants for the both lost teeth.
Remove the bridge, get implants in missing area . While the implants are healing a temporary acrylic bridge with good aesthetics can be given ,once the implants heal all individual crowns ie on implants as well as on adjacent teeth can be given.


Saturday we were in MindLab session four, renewing our knowledge on Constructivist and Constructionism theory of learning using Scratch and Makey Makey. It seemed to be meaningful and relevant considering integration of educational technology. Monday we had to go back to school teaching and following the regular choirs of school life. Finally had to go to the departmental meeting where 'professional development' was one of the agenda. We were told to introduce Algebraic Equation Solving by 'rigid' rule of 'change of side and change of sign'. I heard one or two feeble voices of discomfort, otherwise we were all silent 'followers'.
I like 'MindLab'- a forum we are allowed to be 'free' and 'democratic'. We can share our anxieties, hope and frustration. It is interesting how I co-construct knowledge and strategy with a few teachers who I barely know, but they make me happy.


text:
Home : Casey Benito
Casey Benito
cbenito@calpoly.edu
Casey Benito is a California based designer and educator. He is a graduate of the Southern California Institute of Architecture where he received his master's in architecture. Casey also holds a bachelor's degree from the University of Hawaii and an associate's degree in photography. He has a variety of professional experience including working at Michael Maltzan Architecture, an award-winning, international architecture firm based in Los Angeles. Casey has traveled extensively throughout East Asia, and, in 2007, lived in Kyoto, Japan, where he studied Japanese arts and craft.
Master of Architecture, Southern California Institute of Architecture, Los Angeles, CA, 2012
Bachelor of Arts, University of Hawaii at Manoa, Honolulu, HI, 2006
Midori-Kai, Urasenke College of Chadou, Kyoto, Japan, 2006
Associate in Applied Science, Colorado Mountain College, Glenwood Springs, CO, 1999
Lecturer, Cal Poly, San Luis Obispo, CA, 2017-Present
Lecturer, Woodbury University, Burbank, CA, 2013
Teaching Assistant, Southern California Institute of Architecture, Los Angeles, CA, 2010-2011
Teaching Assistant, University of Hawaii at Manoa, Honolulu, HI, 2006
Principal, Casey Benito Design Build, San Luis Obispo, CA, 2014-Present
Technician, Cal Poly, San Luis Obispo, CA, 2015-2017
Designer, Michael Maltzan Architecture, Los Angeles, CA, 2012-2014
Designer, Yeh + Jerrard, Los Angeles, CA, 2007-2009
Selected Projects:
191 Chorro Street, San Luis Obispo, CA (Design/Build) 2017
3906 Sunset Drive, Los Angeles, CA (Design/Build) 2015
3530 Cazador Street, Los Angeles, CA, 2015
1646 Waterloo Street, Los Angeles, CA, 2015
607 Avenue 54, Los Angeles, CA, 2014
335 Mavis Drive, Los Angeles, CA, 2014
Created 01.16.17


SHENZHEN, China, June 14, 2018 /PRNewswire/ -- Ping An Fin+Tech Accelerator hosted its Opening Ceremony at Futian, Shenzhen on June 14th, 2018. The program is a collaboration between Ping An Group and SparkLabs Group under Futian District government's full support. The accelerator is dedicated to providing innovative transformation of modern finance by nurturing global advanced technologies. Jie He, Shenzhen Futian Deputy District Governor, Ericson Chan, CEO of Ping An Technology, Jonathan Larsen, CEO of Ping An Global Voyager Fund and other Ping An delegates, William Chu, Co-Founder and Managing Director of SparkLabs FinTech and other corporate partners will attend this Opening Ceremony. Ten selected companies stood out from over 120 applicants from around the world and they have started the 3-month "Acceleration Adventure".
The accelerator is eager to place its footprint on the global stage, the selected companies come from China, United States, United Kingdom, Singapore, Nigeria, India and Pakistan. They will leverage blockchain, big data, AI and other cutting edge technologies to provide "Finance + Technology" solutions with multiple scenarios.
The ten selected companies, renowned advisors and mentors, industry leaders, experts and scholars in various fields from around the world were formally announced and introduced. They included Jessica Tan, Deputy Group CEO, Group COO and CIO of Ping An Group, Ericson Chan, CEO of Ping An Technology, Jonathan Larsen, CEO of Ping An Global Voyager Fund and other industry thought leaders such as on the advisor group; Ricky Ou, Chief Product Officer of Ping An Technology, Jay McCarthy, Managing Partner of Pacific Advisers, Emmanuel Pitsilis, former Senior Partner of McKinsey and 60 additional global corporate executives that are part of the mentor group.
Ericson Chan, CEO of Ping An Technology states, "Ping An Group continuously drives Finance + Technology dual innovation strategy. Technology is penetrating the core of traditional finance industry, and the Ping An Accelerator is keen to develop a technology hub that integrates innovation, capital, talent and thought leadership to discover, acquire and monetize technological assets. In the past decade, Ping An expanded rapidly into the FinTech, healthcare, AI and other verticals. Ping An Technology is the technology incubator of Ping An Group and capable of deploying Ping An Cloud ecosystem resource to global enterprises. Meanwhile, Ping An Fin+Tech Accelerator will become a key component of this ecosystem, empowering and optimizing solutions for the entire tech industry.
The 3-month program will equip and empower the selected companies with education and resources to optimize their product, technology and business model at scale. The program includes extensive corporate partnership of Ping An Group's network, professional global mentors, workshops, Ping An Cloud service which provides invaluable support to the participating companies during their product development and a large Demo Day at the end of the program to help them drive market localization and secure next round of funding.
Ping An endeavors to become a world-leading technology-powered personal financial services group upholding the belief of "technology-powered financial services for a better life" and pursuing "finance + technology" and explore "finance + ecosystem". Peter Ma, President of Ping An Group stated, "…the era of intelligent technology is coming, technology is the key to success for the future. Ping An Group is transforming from a capital-driven company to a technology-driven company."
Ping An has invested over 50 billion in FinTech, healthcare, artificial intelligence industries in the past decade; developed over 200 projects in the following areas: financial service, transportation, accommodation and government service with AI capability. With the support of Ping An Group and Ping An Cloud ecosystem, Ping An Fin+Tech Accelerator will focus on finding and partnering with advanced FinTech companies from around the globe to drive the finance revolution and industry transformation.


text:
Q: Precise Membership Test in Python The in operator tests for equivalence using comparison, but Python's comparison isn't precise in the sense that True == 1 and 0 == False, yielding -
>>> True in [ 1 ]
True
>>> False in [ 0 ]
True
>>> 1 in [ True ]
True
>>> 0 in [ False ]
True

whereas I need a precise comparison (similar to === in other languages) that would yield False in all of the above examples. I could of course iterate over the list:
res = False
for member in mylist:
    if subject == member and type( subject ) == type( member ):
        res = True
        break

This is obviously much less efficient then using the builtin in operator, even if I pack it as a list comprehension. Is there some native alternative to in such as a list method or some way to tweak in's behavior to get the required result?
The in operator is used in my case for testing the uniqueness of all list members, so a native uniqueness test would do as well.
Important note: The list may contain mutable values, so using set isn't an option.
Python version is 3.4, would be great for the solution to work on 2.7 too.
EDIT TO ALL THOSE WHO SUGGEST USING IS:

*

*I look for a non-iterating, native alternative to a in b.

*The is operator is not relevant for this case. For example, in the following situation in works just fine but is won't:
>>> [1,2] in [[1,2]]
True

Please, do read the question before answering it...

A: in doesn't test for equivalence at all. It checks if an item is in a container. Example:
>>> 5 in [1,2,3,4,5]
True
>>> 6 in [1,2,3,4,5]
False
>>> True in {True, False}
True
>>> "k" in ("b","c")
True

What you are looking for is is.
>>> True == 1
True
>>> True is 1
False
>>> False == 0
True
>>> False is 0
False

EDIT
After reading your edit, I don't think there is something built in in python libraries that suits your needs. What you want is basically to differentiate between int and bool (True, False). But python itself treats True and False as integers. This is because bool is a subclass of int. Which is why True == 1 and  False==0 evaluates to true. You can even do:
>>> isinstance ( True, int)
True

I cannot think of anything better than your own solution, However, if your list is certain to contain any item not more than once you can use list.index()
try:
    index_val = mylist.index(subject)
except ValueError:
    index_val = None

if (index_val!=None):
    return type(subject) == type(member)

Since index is built-in, it might be a little faster, though rather inelegant.

A: You're looking for the is operator:
if any(x is True for x in l):
    ...

is, however, isn't exactly === from other languages. is checks identity, not just equality without type coercion. Since CPython uses string and integer interning, two objects that are equal may not be the same object:
In [19]: a = '12'

In [20]: b = '123'

In [21]: a += '3'

In [22]: a is b
Out[22]: False

In [23]: a == b
Out[23]: True

In [27]: 100001 is 100000 + 1
Out[27]: False

In [28]: 100001 == 100000 + 1
Out[28]: True

In Python 3, None, True, and False are essentially singletons, so using is for discerning True from 1 will work perfectly fine. In Python 2, however, this is possible:
In [29]: True = 1

In [31]: True is 1
Out[31]: True

Equality can be overridden __eq__ method, so you can define an object that is equal to any other object:
In [1]: %paste
    class Test(object):
        def __eq__(self, other):
            return True

## -- End pasted text --

In [2]: x = Test()

In [3]: x == None
Out[3]: True

In [4]: x == True
Out[4]: True

In [5]: x == False
Out[5]: True

In this case, how would === work? There is no general solution, so Python has no built-in method of lists that does what you want.

A: Python in operator is precise and the behavior you're complaining of is perfectly expected, since bool is a subclass of int.
Below is the excerpt of the official Python documentation describing the boolean type:

Booleans
These represent the truth values False and True. The two objects representing   the values False and True are the only Boolean objects. The Boolean type is a   subtype of plain integers, and Boolean values behave like the values 0 and 1, respectively, in almost all contexts, the exception being that when converted to a string, the strings "False" or "True" are returned, respectively.

You can also have a look at PEP 285.

redpajama_set_name: RedPajamaStackExchange


Toga Sports are delighted to announce we have now become part of the hugely successful 'Serious Sport Group'.
Serious Football, the partner brand to Toga Sports and host of our online club shop model are delighted to be announced as the preferred kit supplier to the Walking Football Association.
Toga Sports, in association with the Serious Sport Group, are delighted to launch their brand-new website and Club Shop Platform.
We are delighted to announce the rebrand and redesign of the hugely successful Toga Sports website.
We are delighted to announce that our partner brand Serious Football have been confirmed as the kit supplier to the Goals Soccer Centres, who are the largest and best provider of small sided football in the UK.


text:
Sandbox is een album van de Amerikaanse indierockband Guided by Voices. Het album werd gezien als een kwalitatieve stap terug ten opzichte van Guided by Voices' vorige album.

Tracklist

Bezetting
 Robert Pollard, zang en gitaar
 Jim Pollard, gitaar
 Mitch Mitchell, basgitaar
 Kevin Fennell, drums en percussie

Referentie

Muziekalbum uit 1987
Muziekalbum van Guided by Voices

redpajama_set_name: RedPajamaWikipedia


text:
Suspect killed in Canal St. shootout was member of Houston-area gang
Police in Texas say that Reginald Romero Bursey was a member of gang that operated in the Houston area
Author: WWL Staff
Published: 1:28 PM CST February 18, 2019
Updated: 5:16 PM CST February 18, 2019
NEW ORLEANS — The man killed in a shootout with New Orleans and State Police that wounded five innocent bystanders was a member of a Houston-area gang known as 59 Piru Street gang, according to police in Texas and sources.
Reginald Romero Bursey, 32, did not have much of a record in the New Orleans area, but was considered 'armed and dangerous' and was wanted for two counts of aggravated robbery in Columbus, Texas for an incident on Sept. 8.
Bursey was apparently also a person of interest in two recent armed robberies in New Orleans before being confronted by police Sunday night.
WWLTV
In the Columbus, Texas crime, the Columbus Police Department said two victims had been bound and robbed of property at gunpoint by Bursey.
According to NOPD Superintendent Shaun Ferguson, detectives identified a man who was located near Canal and Elk Street as a person of interest in two recent armed robberies.
The detectives called for uniformed officers, who confronted the suspect, who then opened fire. Officers returned fire. Bursey was eventually chased to Tulane Avenue where State Police shot and killed him.
Sunday on Canal Street
One of the people shot in an exchange of gunfire between officers and Bursey remained in critical condition Monday, according to the NOPD.
RELATED: 7 dead in violent weekend across New Orleans metro area
RELATED: New Orleans shootout: 5 wounded, suspect dead; Here's what we know
Of the other five gunshot wound victims, three have been released from the hospital and two others remain in the hospital after undergoing surgery.
None of the victims had injuries that were considered life-threatening. The NOPD said Sunday night that it hadn't been determined if the victims were shot by bullets fired by the suspect or police or a combination of both.
The conditions of the five innocent bystanders were released by police Monday afternoon.
- 17-year-old black female sustained a gunshot wound to the left leg and underwent surgery. Still in the hospital.
- 34-year-old black male sustained a gunshot wound to the left arm, and upper abdomen. He was still hospitalized and listed as critical but stable.
- 37-year-old Hispanic male suffered a gunshot wound to the left shoulder. Released from the hospital.
- 33-year-old black male suffered a gunshot wound to the right elbow. Released from the hospital.
- 32-year-old black male suffered a gunshot wound to the right hip. Still hospitalized.
According to an incident report, the shooting started when an undercover NOPD detective identified Bursey at the corner of Canal Street and Elk Place and called for a uniformed officer for backup.
When they responded, Bursey allegedly open fired at the officer who could not shoot back and called for more officers on the scene. When they arrived, the shootout ensued that injured the bystanders.
Bursey then ran off, police said. He was chased down and was found hiding in bushes outside Tulane Medical Center. NOPD and LSP officers told Bursey to come out of the bushes and he fired again. That's when police said they returned fire, hitting him. EMS arrived and took him to the hospital, where he died from his wounds.


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text:
port knew how the case would be, before he recommended him to the office of missionary; and that Mr. Sergeant, after fourteen years study, had never been able to preach in it, nor even to pray in it except by a form, and had often expressed the opinion, previous to his death, that his successor ought not to trouble himself, in learning the language. He then requests, that the Speaker would communicate his letter to the Assembiy, and prays that honourable body, if they proposed to take any order on the case, first to give him opportunity to meet his accuser face to face.
I have no means of ascertaining whether the preceding letter was, or was not, read to the Legislature. If not; it was because the Honourable Speaker, who was a personal friend of Mr. Edwards, found it to be wholly unnecessary. And it can scarcely be necessary to inform the reader, that the attack, made thus directly upon Mr. Edwards, and indirectly upon all his associates in the mission, not only failed altogether of its intended effect; but, by leading to a developement of the mercenary scheme, devised to divert, to the purposes of private emolument, the consecrated charities of the Province and of individuals, recoiled with increased violence upon its authors.
Thus far the individuals, opposed to the Stockbridge missionaries, had met with little success, to encourage their efforts. They had looked for help to various sources : to the Indians and to the people of Stockbridge, to the Commissioners and to the Provincial Legislature, to Mr. Hollis and to the Society in London: and in every instance, so far as the result was known, they had looked in vain. The Housatonnucks had refused all intercourse with them. From disgust at their management, a part of the Mohawks had actually retired, and the rest were threatening to retire, to their own country. The people of Stockbridge had, to a man, umited against them. The Commissioners were equally unanimous, in sustaining the individuals, whose overthrow they had attempted. And now, before the Provincial legislature, they had made their great and united effort, and had failed. In the mean time, Mr. Edwards was even more firmly established, as the Indian Missionary, and Mr. Woodbridge as the school-master of the Housatonnucks ; Mr. Hawley had not been compelled to resign his place to the son of the resident trustee; the female school had not as yet been secured to his wife, and obviously could not now be, unless secured to her in London; and the stewardship of the three schools was not likely to be conferred on himself. Such was the state of things in the spring of 1753. It looked as though the great struggle was over; and that the party, which had thitherto acted on the offensive, would thenceforward be quiet, from a conviction, that every hostile movement must issue in defeat. The result justified this conelusion.
To Mr. Edwards, and his associates in the mission, as well as to their friends, this result must have been in a high degree satisfactory. On his arrival in Stockbridge, he found this controversy waging, and soon discovered that it was a controversy between the friends and enemies of the mission; between those who aimed at the real welfare of the Indians, and those who endeavoured to use them as instruments of their own private emolument; that one party relied on wealth, and office, and influence, to carry its measures; and the other, on personal integrity, a conscientious discharge of duty, and the protection of God. For a time he avoided taking any part in
and his own temporal comfort, and the welfare of his family, seemed to require, that he should persevere in the same course. But his conscience forbade it. He must either sit quietly by, and see the charities of the Province, of the Society in London, and of Mr. Hollis, diverted from their appointed course, to fill the coffers of private avarice; or he must unite with those who were exerting their whole influence to prevent it. In such a state of things, he could not deliberate; and, through the divine blessing, he and his associates were now permitted to see, that they had not toiled and suffered in vain.
it;
CHAPTER XXVIII.
Letter to his eldest Son.— Return of greater part of the Mohawks.
-Letter to Commissioners.-Mission of Mr. Hawley to Onohquauga.—Remainder of Mohawks directed to return.-Freedom of the Will.—Letter to Mr. Erskine.—Proposal of Society in London.—Letter to Mr. Gillespie.- Design and Character of the Freedom of the Will.-Letters from Mr. Hollis.-Surrender of Mohawk School to Mr. Edwards.-Entire Defeat of Enemies of Mission.—Return of remaining Mohawks.
Early in the ensuing spring, the eldest son of Mr. Edwards, then a lad of fourteen, went to New-York, and thence to New-Jersey; and on his way, was much exposed to the sinall-pox. On his return to New-York, he was seized with a violent fever. His father hearing this, and not knowing whether it was an ordinary fever, or the small-pox, addressed to him the following letter; which, like all his letters to his children, indicates that his chief anxiety was for their salvation.
"To Master Timothy Edwards, at New-York.
Stockbridge, April, 1753. "MY DEAR CHILD,
" Before you will receive this letter, the matter will doubtless be determined, as to your having the small-pox. You will either be sick with that distemper, or will be past danger of having it, from any infection taken in your voyage. But whether you are sick, or well, like to die, or like to live, I hope you are earnestly seeking your salvation.
I am sure there is a great deal of reason it should be so, considering the warnings you have had in word and in providence. That which you met with, in your passage from New York to Newark, which was the occasion of your fever, was indeed a remarkable warning, a dispensation full of instruction, and a very loud call of God to you, to make haste, and not to delay in the great business of religion. If you now have that distemper, which you have been threatened with, you are separated from your earthly friends, as none of them can come to see you ; and if you
should die of it, you have already taken a final and everlasting leave of them while you are yet alive, so as not to have the comfort of their presence and immediate care, and never to see them again in the land of the living. And if you have escaped that distemper,
it is by a remarkable providence that you are preserved. And your having been so exposed to it, must certainly be a loud call of God, not to trust in earthly friends, or any thing here below. Young persons are very apt to trust in parents and friends, when they think of being on a death bed. But this providence remarkably teaches you the need of a better Friend, and a better Parent, than earthly parents are; one who is every where present, and all-sufficient, that cannot be kept off by infectious distempers, who is able to save from death, or to make happy in death, to save from eternal misery, and to bestow eternal life. It is indeed comfortable, when one is in great pain, and languishing under sore sickness, to have the presence, and kind care, of near and dear earthly friends ; but this is a very small thing, in comparison of what it is; to have the presence of an heavenly Father, and a compassionate and almighty Redeemer. In God's favour is life, and his loving kindness is better than life. Whether you are in sickness or health, you infinitely need this. But you must know, however great need you stand in of it, you do not deserve it: neither is God the more obliged to bestow it upon you, for your standing in need of it, your earnest desiring of it,
, your crying to him constantly for it from fear of misery, and taking much pains. Till you have savingly believed in Christ, all your desires, and pains, and prayers lay God under no obligation; and, if they were ten thousand times as great as they are, you must still know, that you would be in the hands of a sovereign God, who hath mercy on whom he will have mercy. Indeed, God often hears the poor miserable cries of sinful vile creatures, who have no manner of true regard to Him in their hearts; for he is a God of infinite mercy, and he delights to show mercy for his Son's sake, who is worthy, though you are unworthy, who came to save the sinful and the miserable, yea, some of the chief of sinners. Therefore, there is your only hope; and in him must be your resuge, who invites you to come to him, and says, " Him that cometh to me, I will in no wise cast out." Whatever your circumstances are, it is your duty not to despair, but to hope in infinite mercy, through a Redeemer. For God makes it your duty to pray to him for mercy; which would not be your duty, if it was allowable for you to despair. We are expressly commanded to call upon God, in the day of trouble, and when we are afflicted, then to pray. But, if I hear that you have escaped, either that you have not been sick, or are restored,—though I shall rejoice, and have great cause of thankfulness, yet I shall be concerned for you. If your escape should be followed with carelessness and security, and forgetting the remarkable warning you have had, and God's great merey in your deliverance, it would in some respects be more awful than sore sickness. It would be very provoking to God, and would probably issue in an increasing hardness of heart; and, it may be, divine vengeance may soon overtake you. I have known various in
stances of persons being remarkably warned, in Providence, by being brought into very dangerous circumstances, and escaping, and afterwards death has soon followed in another way. I earnestly desire, that God would make you wise to salvation, and that he would be merciful and gracious to you in every respect, according as he knows your circumstances require. And this is the daily prayer of " Your affectionate and tender father,
" JONATHAN EDWARDS. "P. S. Your mother and all the family send their love to you, as being tenderly concerned for you."
At length the event, so long predicted by Mr. Edwards, actually took place. The Mohawks, who had manifested exemplary patience, under the vexations and embarrassments, to which they had been subjected by the whites, were at last wearied out; and, in the month of April, the greater part of them relinquished their lands and settlements at Stockbridge, and returned finally to their own country After a brief allusion to this fact, in a letter to the Commissioners, Mr. Edwards communicated to them a variety of interesting intelligence relative to the Iroquois, and to the mission proposed to be established among them.
" To the Commissioners in Boston.
" Stockbridge, April 12, 1753. - GENTLEMEN,
" The last Tuesday, about two thirds of the Mohawks, young and old, went away from Stockbridge, and are never likely to return again. They have long inanifested a great uneasiness, at the management of affairs here, and at the conduct of those persons, on whom their affairs have almost wholly fallen; and have shown themselves very much grieved, that others, who used to be concerned, have been excluded. They have, once and again, represented the grounds of their uneasiness, to the provincial agent, but without redress. They have been dissatisfied with his answers, and there has appeared in them a growing dislike of the family, who have lately left their own house, and taken up
their constant abode among them, in the female boarding-school.
"The Correspondents, in New-York and New-Jersey, of the So- . ciety in Scotland, for propagating Christian Knowledge, have determined, if Providence favours, to settle a mission anong Six Nations. To that end, they have chosen Mr. Gordon, a pious young gentleman, who has lately been a Tutor at New-Jersey College, to come to Stockbridge, and remain here with Mr. Hawley, to learn the Mohawk language with him, in order to his being


During the first telephone call, we can give you more information about the cost of an intake interview and the total cost of your stay in Spain. The costs in Spain are inclusive of therapy, full or half board, flight, car rental and / or return to the airport in Alicante. Optional is that you will arrange the transport yourself. Also included are two post treatment conversations by telephone or Skype of about 15 minutes each. Supplementary post-treatment sessions in the Netherlands are optional and can be discussed. Based on your wishes and possibilities, we will send you a quotation.


A number of changes to the Food Safety Modernization Act (FSMA) implementation timeline were announced Wednesday. First, the U.S. Food and Drug Administration plans to publish revised language for the proposed rule on preventive controls for animal food in early summer 2014, alongside the revised produce safety and preventive controls for human food rules. FDA also plans to extend the comment period for other elements of FSMA. The new deadline for the intentional adulteration and accompanying draft qualitative risk assessment will be June 30, a 90-day extension from the March 31 deadline originally set by the court. The announcement comes a week after FDA held its third and final public meeting on the rule in Anaheim, CA. Because the agency will release a revised version of the animal food rule, the March 31 deadline for comments on preventive controls for animal food will remain despite calls for an extension from the grain and feed industry. Richard Sellers, the American Feed Industry Association's senior vice president of legislative and regulatory affairs, said that his organization is "disappointed" that FDA is not giving the industry more time to review the rule "provided the agency themselves was given an extension by the courts." Last on the list of Wednesday's updates, FDA is also extending the comment period on the draft methodological approach to identifying high-risk foods an additional 45 days until May 22. "The Agency is committed to providing adequate time to comment on proposed rules while recognizing the need to meet court-ordered deadlines for final rules," reads an FDA statement. FDA will officially announce the extensions in the Federal Register and will issue constituent updates to inform stakeholders.