text:
\section{Introduction}

Since the first definite detection of a planet around another main-sequence star, 51 Peg \citep{1995Natur.378..355M}
made with high-precision radial velocity measurements,
various detection techniques have been applied to find a diverse population of exoplanets. The transit method, which was first
used for HD~209458
\citep{2000ApJ...529L..45C}, later allowed for a boost of exoplanet discoveries after the successful launch of two dedicated satellite missions, CoRoT \citep{2007AIPC..895..201B} and Kepler
\citep{2010ApJ...713L..79K,2010Sci...327..977B}. These two methods indirectly discern the presence of a planet by the influence the planet has on its host star. The methods are most sensitive to small and moderate planet-star-separations around old main-sequence stars that are fairly inactive because of their age. The sensitivity diminishes fast for separations beyond 5 au because transits become less likely and the radial velocity amplitude declines with increasing orbital period.
In contrast, direct imaging allows discovering planets on wide orbits around nearby pre-main-sequence stars because such young planets
are still bright at infrared wavelengths as a result of the gravitational contraction during their still-ongoing formation process.

\begin{figure*}
  \centering
  \includegraphics[width=0.38\textwidth]{Keckbild4.eps}
  \includegraphics[width=0.4\textwidth]{CVSOFarb3.eps}
  \caption{Direct images of CVSO 30 c. \textit{Left:} Keck image of data by \cite{2012ApJ...755...42V}, re-reduced. We note that the companion is north-east and not a contaminant south-east, as
  given in \cite{2012ApJ...755...42V}. \textit{Right:} Our new VLT epoch, clearly showing the planetary companion, which has similar colour as its host star (Fig.~\ref{FigPhot}). This excludes
that it is a false positive for the inner planet candidate CVSO 30 b.}
  \label{FigImage}
\end{figure*}

The total number of imaged planet candidates has increased
to about 50-60 objects today. The first detections were made
in 2005, when the first four co-moving planetary candidates were found around the solar-like stars DH Tau \citep{2005ApJ...620..984I}, GQ Lup \citep{2005AandA...435L..13N}, and AB Pic \citep{2005AandA...438L..29C}, all with masses near the threshold of 13 M$_{\mathrm{Jup}}$ that
divides brown dwarfs from planets according to the current IAU working definition,
together with the planet candidate around the brown dwarf 2M1207 \citep{2005A&A...438L..25C}. A summary can be found in \citet{2012arXiv1201.3537N}, and the current status
is always available in several online encyclopaediae, such as the Extrasolar Planets Encyclopaedia at www.exoplanet.eu \citep{2011A&A...532A..79S}.
As in situ formation at $\sim$100 au to a few hundreds of au separation seems unlikely according to models, \citet{2006ApJ...637L.137B} argued that a third
body must exist that tossed these planets outward to their present distance from their young host stars. An alternative explanation might be a stellar encounter
\citep{2001Icar..150..151A}.

While early-type stars have less favourable planet-to-star contrast ratios, increasing evidence was found by millimeter-continuum measurements for larger
and more massive protoplanetary disks that are available for planet formation around these stars \citep{1997ApJ...490..792M,2013ApJ...771..129A}. These
conclusions were further strengthened when three of the most prominent planet candidates were found in 2008 and
2009 around the early F-type star
HR 8799 \citep{2008Sci...322.1348M}, which is the first system with multiple planets imaged around a star. The other two were around the A-type stars Fomalhaut \citep{2008Sci...322.1345K},
which is the first planet candidate discovered in the optical regime using the Hubble Space Telescope (HST), and $\beta$ Pic \citep{2009AandA...493L..21L,2010Sci...329...57L},
a planet within the large edge-on disk at only about twice the separation of Jupiter from the Sun. This had~previously been
predicted by \citet{2007A&A...466..389F}, for instance,
from the structural gaps in the disk.

Most of the direct-imaging surveys conducted so far have concentrated on AFGK stars. In 2012 a (proto-)planet candidate was discovered around the $\sim$2 Myr young
solar-like star LkCa 15 \citep{2012ApJ...745....5K}. This is a close ($\sim$11 AU) object found by single-dish interferometry, which is a technique that is also referred to as sparse aperture masking. Two companions of 4-5 M$_{\mathrm{Jup}}$ were recently
discovered around GJ 504 \citep{2013ApJ...774...11K}, which is a 160 Myr old solar-like star, and around HD 95086 \citep{2013ApJ...772L..15R}, an A-type star at about 10-17 Myr.
Additionally, first results from imaging surveys around
M dwarfs were published during the past two years, which increased our understanding of planetary systems around the most numerous stars in the Milky Way \citep{2013AandA...553L...5D,2015ApJS..216....7B}.

\begin{table}
\caption{Previously known CVSO 30 system data}
\label{TableCVSOsys}
\centering
\begin{scriptsize}
\begin{tabular}{lcc}
\hline
& \multicolumn{2}{c}{CVSO 30}\\
\hline\hline
Altern.~designations & \multicolumn{2}{c}{2MASS J05250755+0134243, PTF1 J052507.55+013424.3} \\
Location        & \multicolumn{2}{c}{25 Ori / Orion OB 1a [1,2]}\\
RA, Dec         & \multicolumn{2}{c}{05h 25m 07.57s, +01$^{\circ}$ 34$'$ 24.5$''$ [2]}\\
Spectral type   & \multicolumn{2}{c}{M3 (weak-line T-Tauri, WTTS) [2]}\\
Mass            & \multicolumn{2}{c}{0.34 / 0.44 M$_{\mathrm{\odot}}$ [2]}\\
Luminosity      & \multicolumn{2}{c}{0.25 L$_{\mathrm{\odot}}$ [2]}\\
Radius          & \multicolumn{2}{c}{1.39 R$_{\mathrm{\odot}}$ / 1.07 $\pm$ 0.10 R$_{\mathrm{\odot}}$ / [1.03 / 1.04 $\pm$ 0.01 R$_{\mathrm{\odot}}$] [2,3,4]}\\
Temperature     & \multicolumn{2}{c}{3470 K [2]}\\
Opt. extinction & \multicolumn{2}{c}{0.12 mag [2]}\\
\smallskip
Distance        & \multicolumn{2}{c}{[323$^{+233}_{-96}$, 322$^{+504}_{-122}$] pc / 357 $\pm$ 52 pc [2,5]}\\
Age             & \multicolumn{2}{c}{2.39$^{+3.41}_{-2.05}$ Myr [2,here]}\\
H$_{\alpha}$ equivalent width  & \multicolumn{2}{c}{-11.40 \AA \ [2]}\\
LiI equivalent width           & \multicolumn{2}{c}{0.40 \AA \ [2]}\\
v $\sin(i)_*$          & \multicolumn{2}{c}{80.6 $\pm$ 8.1 km s$^{-1}$ [3]}\\
Proper motion [E,N] & \multicolumn{2}{c}{[-0.1 $\pm$ 5.3, 0.9 $\pm$ 5.5] mas/yr [6]}\\
B, V, R photometry  & \multicolumn{2}{c}{[18.35, 16.26, 15.19] mag [7,2,3]}\\
J, H, K photometry  & \multicolumn{2}{c}{[12.232\,$\pm$\,0.028,\,11.559\,$\pm$\,0.026,\,11.357\,$\pm$\,0.021]\,mag [8]}\\
\hline
                    & \multicolumn{2}{c}{CVSO 30 b / PTFO 8-8695 b} \\
\hline\hline
(Projected) separation & \multicolumn{2}{c}{0.00838 $\pm$ 0.00072 au [3] } \\
Period (circular)      & \multicolumn{2}{c}{0.448413 $\pm$ 0.000040 d [3] } \\
Orbit.~inclination     & \multicolumn{2}{c}{61.8 $\pm$ 3.7 $^{\circ}$ [3] } \\
Orbit.~misalignment    & \multicolumn{2}{c}{69 $\pm$ 2 $^{\circ}$ / 73.1 $\pm$ 0.5 $^{\circ}$ [4] } \\
\hline
\end{tabular}
\begin{flushleft}
References: [1] \citet{2007ApJ...661.1119B}, [2] \citet{2005AJ....129..907B}, [3] \citet{2012ApJ...755...42V}, [4] \citet{2013ApJ...774...53B}, [5] \citet{2014MNRAS.444.1793D}
            [6] \citet{2013AJ....145...44Z}, \mbox{[7] \citet{2004AAS...205.4815Z}}, [8] \citet{2003tmc..book.....C,2006AJ....131.1163S}
\end{flushleft}
\end{scriptsize}
\end{table}

\begin{table}
\caption{CVSO 30 astrometry and photometry}
\label{TableCVSOAsPhot}
\centering
\begin{scriptsize}
\begin{tabular}{lcc}
\hline
                    & CVSO 30 b / & CVSO 30 c\\
                    & PTFO 8-8695 b \\
\hline\hline
                    & \multicolumn{2}{c}{Separation with respect
to~the host star [E,N]} \\
2010 September 25   & & [175.453,\,63.395] pixel \\
2012 December 3     & & [1.746 $\pm$ 0.006, \\
                    & & \ \ \ \ \ 0.621 $\pm$ 0.010] $''$ \\
\hline
(Projected) separation & 0.00838 $\pm$ 0.00072 au [1] & 662 $\pm$ 96 au \\
Period (circular)      & 0.448413 $\pm$ 0.000040 d [1] & $\sim$ 27250 years \\
Orbit.~inclination     & 61.8 $\pm$ 3.7 $^{\circ}$ [1] & \\
Orbit.~misalignment    & 69 $\pm$ 2 $^{\circ}$ / 73.1 $\pm$ 0.5 $^{\circ}$ [2] & \\
\hline
z$^{\prime}$ band (differential) & & > 6.8 mag \\
\hline
J band (differential)    & & 7.385 $\pm$ 0.045 mag \\
H band (differential)    & & 7.243 $\pm$ 0.014 mag \\
Ks band (differential)   & & 7.351 $\pm$ 0.022 mag \\
\hline
J band (differential)    & & 7.183 $\pm$ 0.035 mag \\
\hline
\end{tabular}
\begin{flushleft}
References: [1] \citet{2012ApJ...755...42V}, [2] \citet{2013ApJ...774...53B}
\end{flushleft}
\end{scriptsize}
\end{table}

In this article we describe for the first time the direct detection of a wide-separation (1.85$''$ or 662 au, see Fig.~\ref{FigImage}) directly imaged planet candidate around a star (\object{CVSO 30}) that also hosts a short-period transiting planet candidate; we refer to a more detailed discussion of this object in \citet{2012ApJ...755...42V}, \citet{2013ApJ...774...53B}, and \citet{2015ApJ...812...48Y}. A system that harbours two planets with such extreme orbits gives us for the first time the opportunity to study by observations
the possible outcome of planet-planet scattering theories, which have been used to explain the existence of close-in hot Jupiters in 1996 \citep{1996Sci...274..954R}.

\section{25 Ori group and the CVSO 30 system properties}

\begin{table*}
\caption{VLT/NACO, VLT/SINFONI, archival KeckII/NIRC2, and Calar Alto/2.2m/AstraLux observation log}
\label{TableLog}
\centering
\begin{footnotesize}
\begin{tabular}{llccccccccccc}
\hline\hline
Instrument         & JD-2455000      & Date of         & DIT        & NDIT    & \#        & Airmass & DIMM$^a$   & $\tau_{0}^b$ & Strehl & S/N \\
                   & $[\mathrm{days}]$ & observation   & [s]        &         & images    &         & Seeing     & [ms]         & [\%]   & (brightest pixel) \\
\hline
NACO J             & 1264.69416       & 03 Dec 2012     & 15         & 4      & 15        & 1.13    & 0.8        & 3.7          & 3.2    & 5.9  \\
NACO H             & 1264.70764       & 03 Dec 2012     & 15         & 4      & 15        & 1.12    & 0.6        & 4.6          & 11.2   & 24.6 \\
NACO Ks            & 1264.72079       & 03 Dec 2012     & 15         & 4      & 15        & 1.11    & 0.7        & 4.6          & 23.7   & 11.1 \\
NACO J             & 1266.72899       & 05 Dec 2012     & 30         & 2      & 15        & 1.12    & 1.3        & 2.8          & 2.0    & 6.6  \\
SINFONI H+K        & 1592.82609       & 27 Oct 2013     & 300        & 2      & 3         & 1.12    & 0.5        & 5.0          &        & $\lessapprox$15 \\
\hline
NIRC2 H            & \, 465.05374     & 25 Sep 2010     & 3          & 10     & 12        & 1.25    & 0.4        &              & 7.0    & 7.8  \\
\hline
AstraLux z$^{\prime}$ & 2260.6696     & 26 Aug 2015     & 0.02945    & 1      & 70000     & 1.73    & 1.1        &              & no AO  & non-detection   \\
\hline
\end{tabular}
\begin{flushleft}
\textbf{Remarks}: (a) Differential image motion monitor (DIMM) seeing average of all images (b) coherence time of atmospheric fluctuations.
\end{flushleft}
\end{footnotesize}
\end{table*}

\begin{table}
\caption{CVSO 30 deduced planetary properties}
\label{TableCVSOPlanets}
\centering
\begin{scriptsize}
\begin{tabular}{lcc}
\hline
                    & CVSO 30 b / & CVSO 30 c\\
                    & PTFO 8-8695 b \\
\hline\hline
\smallskip
Opt. extinction                     & & 0.19$^{+2.51}_{-0.19}$ mag\\
\smallskip
Luminosity (vs.~${\mathrm{\odot}}$) & & -3.78$^{+0.33}_{-0.13}$ dex\\
\smallskip
Eff.~temperature T$_{\mathrm{eff}}$ & & 1600$^{+120}_{-300}$ K\\
Surface gravity $\log{g}$           & & 3.6$^{+1.4}_{-0.6}$ dex\\
Radius                              & 1.91 $\pm$ 0.21 R$_{\mathrm{Jup}}$ [1] & \\
\smallskip
                                    & 1.64 / 1.68 $\pm$ 0.07 R$_{\mathrm{Jup}}$ [2] & 1.63$^{+0.87}_{-0.34}$ R$_{\mathrm{Jup}}$\\
\smallskip
Mass                                & $<$ 5.5 $\pm$ 1.4 M$_{\mathrm{Jup}}$ [1] & 4.3$^{+4.9}_{-3.7}$ M$_{\mathrm{Jup}}$ ($\log{g}$ \& Roche)\\
\smallskip
                                    & 3.0 $\pm$ 0.2 M$_{\mathrm{Jup}}$     [2] & 4.7$^{+5.5}_{-2.0}$ M$_{\mathrm{Jup}}$ (L, age) \\
\smallskip
                                    & 3.6 $\pm$ 0.3 M$_{\mathrm{Jup}}$     [2] & 4.7$^{+3.6}_{-2.0}$ M$_{\mathrm{Jup}}$ (L, T$_{\mathrm{eff}}$, age) \\
\smallskip
                                    &                                          & < 10 M$_{\mathrm{Jup}}$ (z$^{\prime}$ imaging limit) \\
\hline
\end{tabular}
\begin{flushleft}
References: [1] \citet{2012ApJ...755...42V}, [2] \citet{2013ApJ...774...53B}
\end{flushleft}
\end{scriptsize}
\end{table}

Despite their importance for the evolution of protoplanetary disks and the early phases in the planet formation process, sufficiently large samples of 10 Myr old stars have been difficult to identify, mainly because the parent molecular clouds dissipate after a few Myr
and no longer serve as markers of these populations (see \citet{2007prpl.conf..345B} and references therein).
The 25 Ori cluster \citep[25 Ori,][]{2007ApJ...661.1119B} contains $> 200$ PMS stars in the mass range $0.1 < M/M_{\odot} < 3$.
The Hipparcos OB and earlier A-type stars in 25 Ori are on the zero-age main sequence \citep[ZAMS,][]{2005AJ....129..856H}, implying a distance of $\sim$330 pc, with some of the A-type stars harbouring debris disks \citep{2006ApJ...652..472H}.
Isochrone fitting of the low-mass stars yields an age of 7-10 Myr \citep{2007prpl.conf..345B}. This is the most populous 10 Myr old sample within 500 pc,
which we consequently chose for a direct-imaging survey with ESO's VLT, the Very Large Telescope of the European Southern Observatory, to find young planetary and sub-stellar companions at or shortly after their formation. For this same reason, the 25 Ori cluster was also targeted in searches for transiting planets, like the Young Exoplanet Transit Initiative \citep[YETI,][]{2011AN....332..547N} and the Palomar Transient Factory \citep[PTF,][]{2012ApJ...755...42V}.

CVSO 30 (also 2MASS J05250755+0134243 and PTFO 8-8695) is a weak-line T Tauri star of spectral type M3 in 25 Ori at an average distance of 357$\,\pm\,$52 pc \citep{2014MNRAS.444.1793D}.
It was confirmed as a T Tauri member of the 25 Ori cluster by the CIDA Variability Survey of Orion (CVSO), with properties shown in Table~\ref{TableCVSOsys}.
As shown in Fig.~1 in \citet{2012ApJ...755...42V}, CVSO 30 is one of the youngest objects within 25 Ori, its position in the colour-magnitude diagram corresponds to 2.39$^{+3.41}_{-2.05}$~Myr (if compared to evolutionary models of \citet{2000A&A...358..593S}). The object is highly variable, rotates fast, and has a mass of 0.34 -- 0.44 M$_{\odot}$ (depending on the evolutionary model), and an effective temperature of $\sim$3470 K. The rotation period of CVSO 30, which is possibly synchronised with the CVSO 30 b orbital period, is still debated \citep{2012ApJ...755...42V,2015MNRAS.450.3991K}. \citet{2015PASJ...67...94K} concluded that the stellar spin period is shorter than 0.671 d.

In 2012 the PTF team \citep{2012ApJ...755...42V} reported a young transiting planet candidate around CVSO 30, named PTFO 8-8695 b, with a fast co-rotating or near co-rotating 0.448413 day orbit.
The very same object, henceforth CVSO 30 b for simplicity, was independently detected with smaller telescopes within the YETI
\citep{2013prpl.conf2K047N,2014CoSka..43..513E},
confirming the presence of the transit events by quasi-simultaneous observations.

Keck and Hobby-Eberly Telescope (HET) spectra \citep{2012ApJ...755...42V} set an upper limit to the mass of the transiting companion of 5.5 $\pm$ 1.4 M$_{\mathrm{Jup}}$ from
the radial velocity variation, which exhibits a phase offset that is likely caused by spots on the surface of the star. This RV limit was already corrected for the derived orbital inclination 61.8 $\pm$ 3.7 $^{\circ}$ of the system. With an orbital radius of only about twice the stellar radius and a planetary radius of 1.91 $\pm$ 0.21 R$_{\mathrm{Jup}}$, the object appears to be at or within its Roche-limiting orbit, raising the possibility of past or ongoing mass loss. A false positive by a blended eclipsing binary is unlikely because the only present contaminant in Keck near-IR images (see Fig.~\ref{FigImage}) with 6.96 mag of contrast to the star would have to be very blue to be bright enough in the optical to mimic a transit; it is unlikely to be a star in that case.

In 2013 \citet{2013ApJ...774...53B} fit the two separate light
curves observed in 2009 and 2010, which exhibited unusual differing shapes, simultaneously and
self-consistently with planetary masses of the companion of 3.0 -- 3.6 M$_{\mathrm{Jup}}$.
They assumed transits across an oblate, gravity-darkened stellar disk and precession of the planetary orbit ascending node. The fits show a high degree of spin-orbit misalignment of about 70$^{\circ}$, which leads
to the prediction that transits disappear for months at a time during the precession period of this system. The lower planet radius result of
$\sim$1.65 R$_{\mathrm{Jup}}$ is consistent with a young, hydrogen-dominated planet that results from hot-start formation mechanisms \citep{2013ApJ...774...53B}.

\begin{table}
\caption{Astrometric calibration of VLT/NACO}
\label{TableAstroCal}
\centering
\begin{footnotesize}
\begin{tabular}{llcc@{\,$\pm$\,}l}
\hline\hline
Object & JD - 2456000 & Pixel scale &  \multicolumn{2}{c}{PA$^a$ }\\
       & $[\mathrm{days}]$ & [mas/pixel] & \multicolumn{2}{c}{[$\deg$]} \\
\hline
47 Tuc & 264.62525 & 13.265 $\pm$ 0.041 & +0.60 & 0.31 \\
\hline
\end{tabular}
\begin{flushleft}
\textbf{Remarks}: All data from Ks-band images. (a) PA is measured from N over E to S.
\end{flushleft}
\end{footnotesize}
\end{table}

\section{Astrometric and photometric analysis}

\begin{figure*}
\centering
  \includegraphics[width=0.49\textwidth]{colorplot2.eps}
  \includegraphics[width=0.49\textwidth]{colorplot3.eps}
  \caption{CVSO 30, CVSO 30 c, and comparison objects, superimposed onto the colour data from \citet{2006MNRAS.367..454H}. CVSO 30 c clearly stands out in the lower left corner,
  approximately consistent with colours of giants, early-M and early-T dwarfs, and free-floating planetary mass objects \citep{2000Sci...290..103Z,2012ApJ...754...30P}, e.g. consistent with absolute magnitude and J-Ks colour of S Ori 64.
  Its unusual blue colour can most likely be attributed to the youth of these objects \citep{2008ApJ...689.1327S}, leading to
  L--T transition opacity drop at high brightnesses (see Fig.~\ref{FigColMag}). See Fig.~\ref{FigColMagAppend} for details.
  For CVSO 30 c we give the colours before (grey) and after (red) correcting for the NACO to the 2MASS filter set and we give the maximum possible systematic photometric offsets caused by the variability of the primary star that is used as reference (black).}
  \label{FigPhot}
\end{figure*}

After the discovery of the transiting planet candidate by \citet{2012ApJ...755...42V} and our independent detection of the transit signals with YETI, we included the system in our 25 Ori VLT/NACO direct-imaging survey with the intent to prove that the object labelled as a contaminant by \citet{2012ApJ...755...42V} is not able to produce the detected transiting signal and to confirm it as second planet. We performed our first high-resolution direct observations in December 2012 and obtained JHK-band photometry (Tables~\ref{TableCVSOAsPhot}\,and\,\ref{TableLog}
and Fig.~\ref{FigImage}).

During the course of their study of the transiting planet CVSO 30 b, the PTF team used Keck II/NIRC2 H-band images obtained in 2010 to identify contaminants capable of creating a false-positive signal mimicking a planet.
We re-reduced these data and found that they already contain the planetary companion CVSO 30 c that we report here. In Fig.~\ref{FigImage} we show the companion, erroneously given to lie south-east in \citet{2012ApJ...755...42V}; it is located north-east of the host star CVSO 30.

We astrometrically calibrated the VLT/NACO detector epoch using a sub-field of 47 Tuc (Table~\ref{TableAstroCal}) to determine pixel scale and detector orientation in order to find precise values for the separation of CVSO 30 c with respect to CVSO 30 in right ascension and declination. From this,
we find the object to be $\sim$1.85$''$ NE of CVSO 30 at a position angle of $\sim$70$^{\circ}$ from north towards east, corresponding
to a projected separation of 662 $\pm$ 96 au at the distance of the star.
No astrometric calibrator could be found in the night of the Keck observations (hence the position of the object is given in pixels in Table~\ref{TableCVSOAsPhot}), but we note that the
position is consistent with the VLT data. We used the nominal pixel scale of NIRC2 of 0.009942 $''$/pixel ($\pm$ 0.00005$''$) and assumed 0$^{\circ}$ detector orientation for the Keck epoch, which results in 1.744 arcsec right ascension and 0.630 arcsec declination separation in the relative position of CVSO 30 c with respect to its host star. The consistency was
expected for a companion because the proper motion of CVSO 30 is too small to distinguish a background source from a sub-stellar companion based on common proper motion (Table~\ref{TableCVSOsys}).

CVSO 30 is in general currently not suitable for a common proper motion analysis because the errors in proper motion exceed the proper motion values (Table~\ref{TableCVSOsys}).
As orbital motion around the host star might be detectable, we performed a dedicated orbit estimation for the wide companion.
The analysis shows that even after two to three years of epoch difference, no significant orbital motion is expected for the wide companion (Fig.~\ref{FigOrbit}).

Using the Two Micron All Sky Survey (2MASS) \citep{2003tmc..book.....C,2006AJ....131.1163S}
photometry for the primary and our NACO images for differential brightness measurements, we find CVSO 30 c to exhibit an unusually blue H-Ks colour, while its J-H colour indicates the companion candidate to be redder than the primary. This implies that the companion is too red to be an eclipsing background binary mimicking the transiting signal of CVSO 30 as a false-positive signal, which is further indication for the planetary nature of CVSO 30 b.

The differential photometry (Table~\ref{TableCVSOAsPhot}) of CVSO 30 c was achieved using psf fitting with the \textit{Starfinder} package of IDL \citep{2000SPIE.4007..879D} using the primary star
CVSO 30 as psf reference. First the noise of the final jittered image was computed, taking the photon noise, the gain, RON, and the number of combined images into account, and then it was transferred to the starfinder routine for psf fitting. This resulted in the values given in Table \ref{TableCVSOAsPhot}. The values were checked with aperture photometry.

\begin{table}
\caption{Photometric rejection significance, spectroscopic reduced $\chi^2$ results, and corresponding formal significance without systematics for different comparison objects.}
\label{TableChi}
\centering
\begin{scriptsize}
\begin{tabular}{ccccccc}
\hline
Object & SpT & \multicolumn{2}{c}{Photometry} & add. & \multicolumn{2}{c}{Spectroscopy}                  \\
       &     & J-H           & H-Ks           & ref. & H-band                  & K-band                  \\
       &     & [$\sigma$]    & [$\sigma$]     &      & [$\sigma$\,/\,$\chi^2_r$] & [$\sigma$\,/\,$\chi^2_r$] \\
\hline\hline
HD 237903 & K7V        & 3.4 & 0.5 & [1]       & >6\,/\,2.66 &  >6\,/\,1.60 \\
Gl 846    & M0V        & 2.8 & 1.8 & [1]       & >6\,/\,2.38 & 5.4\,/\,1.51 \\
Gl 229    & M1V        & 0.6 & 0.3 & [1]       & >6\,/\,2.37 & 5.3\,/\,1.50 \\
Gl 806    & M2V        & 4.5 & 2.5 & [1]       & >6\,/\,2.73 & 4.3\,/\,1.40 \\
Gl 388    & M3V        & 3.7 & 2.8 & [2],[1]   & >6\,/\,2.57 & 3.7\,/\,1.33 \\
Gl 213    & M4V        & 5.5 & 2.6 & [2],[1]   & >6\,/\,2.80 & 2.5\,/\,1.21 \\
Gl 51     & M5V        & 3.8 & 3.5 & [2],[1]   & >6\,/\,2.47 & 2.6\,/\,1.21 \\
Gl 406    & M6V        & 3.4 & 4.6 & [2],[1]   & >6\,/\,2.50 & 2.5\,/\,1.20 \\
Gl 644C   & M7V        & 4.1 & 5.1 & [2],[1]   & >6\,/\,2.87 & 2.2\,/\,1.17 \\
Gl 752B   & M8V        & 2.6 & 6.4 & [2],[1]   & >6\,/\,2.76 & 2.3\,/\,1.18 \\
LHS 2065  & M9V        & 1.7 & 7.5 & [1]       & >6\,/\,2.45 & 2.2\,/\,1.17 \\
LHS 2924  & L0         & 1.4 & 6.5 & [2],[1]   & >6\,/\,2.77 & 2.1\,/\,1.16 \\
2MUCD 20581 & L1       & 2.2 & 7.5 & [2]       & >6\,/\,3.96 & 3.7\,/\,1.33 \\
Kelu-1AB  & L2+L3.5    & 2.2 & 9.8 & [2]       & >6\,/\,3.68 & 3.6\,/\,1.32 \\
2MUCD 11291 & L3       & 1.8 & >10 & [2]       & >6\,/\,3.66 & 3.8\,/\,1.34 \\
2MUCD 12128 & L4.5     & 5.5 & >12 & [2]       & >6\,/\,3.09 & 3.4\,/\,1.29 \\
2MUCD 11296 & L5.5     & 1.3 & >10 & [2]       & >6\,/\,4.60 & 5.5\,/\,1.52 \\
2MUCD 11314 & L6       & 2.0 & 8.4 & [2]       & >6\,/\,3.64 &  >6\,/\,1.66 \\
2MUCD 10721 & L7.5     & 5.8 & >11 & [2]       & >6\,/\,3.49 & 3.4\,/\,1.29 \\
2MUCD 10158 & L8.5     & 2.5 & 9.8 & [2]       & >6\,/\,4.87 & 5.0\,/\,1.47 \\
SDSS 1520+354 & T0     & 1.0 & 5.4 & [3]       & >6\,/\,4.63 &  >6\,/\,2.15 \\
SDSS 0909+652 & T1.5   & 0.3 & 0.4 & [4]       & >6\,/\,8.04 &  >6\,/\,3.64 \\
SDSS 1254-012 & T2     & 0.8 & 2.0 & [2]       & >6\,/\,7.97 &  >6\,/\,2.90 \\
2MASS 055-140 & T4     & 9.4 & 0.1 & [2]       & >6\,/\,16.2 &  >6\,/\,19.1 \\
\hline
HD 204585 & M4.5III    & 0.4 & 0.8 & [1]       & >6\,/\,1.86 &  >6\,/\,1.88 \\
HD 175865 & M5III      & 0.1 & 0.5 & [1]       & >6\,/\,1.91 &  >6\,/\,1.78 \\
BK Vir    & M7III      & 0.4 & 0.9 & [1]       & >6\,/\,2.47 &  >6\,/\,1.72 \\
HY Aqr    & M8-9III    & 0.6 & 8.5 & [1]       & >6\,/\,5.78 &  >6\,/\,1.61 \\
Galaxies  & various    & 4.2 & 3.0 & [5],[6]   & >6\,/\,2.28 &  >6\,/\,1.61 \\
Quasars   & ---        & 4.4 & 3.9 & [5]       & ---         & ---          \\
White Dwarfs & various & 6.4 & 3.9 & [5]       & ---         & ---          \\
\hline
CVSO 30   & M3         & 2.7 & 1.7 &           & >6\,/\,3.31 & 6.0\,/\,1.57 \\
PZ Tel B  & M7         & 2.1 & 1.4 & [7]       & >6\,/\,3.29 & 3.0\,/\,1.25 \\
CT Cha b  & M9         & 0.4 & 1.3 & [8],[9]   & >6\,/\,2.27 & 1.8\,/\,1.13 \\
2M0441 Bb & L1         & 0.5 & 2.4 & [10]      & >6\,/\,3.13 & 1.9\,/\,1.13 \\
1RXS 1609 b   & L4     & 1.1 & 3.0 & [11]      & >6\,/\,2.70 & 2.3\,/\,1.18 \\
$\beta$ Pic b & L4     & 1.0 & 3.5 & [12]      & >6\,/\,2.06 & ---          \\
2M1207 b      & L7     & 3.5 & 4.4 & [13]      & >6\,/\,2.66 & 2.5\,/\,1.20 \\
S Ori 64      & L/T    & 0.9 & 0.7 & [14]      & ---         & ---          \\
DP (Fig.~\ref{FigSpec2}) & --- & --- & --- & [15] & 2.2\,/\,1.16 & 2.0\,/\,1.14 \\
\hline
\end{tabular}
\begin{flushleft}
References: [1] \citet{2009ApJS..185..289R}, [2] \citet{2005ApJ...623.1115C}, [3] \citet{2010ApJ...710.1142B}, [4] \citet{2006AJ....131.2722C}, [5] \citet{2006MNRAS.367..454H}, [6] \citet{2001MNRAS.326..745M}, [7] \citet{2014A&A...566A..85S}, [8] \citet{2009AIPC.1094..852S}, [9] \citet{2008AandA...491..311S}, [10] \citet{2015ApJ...811L..30B},
[11] \citet{2008ApJ...689L.153L}, [12] \citet{2015ApJ...798L...3C}, [13] \citet{2010A&A...517A..76P},
[14] \citet{2012ApJ...754...30P}, from VISTA to 2MASS magnitudes
using colour equations from http://casu.ast.cam.ac.uk/surveys-projects/vista/technical/photometric-properties,
[15] \citet{2008ApJ...675L.105H}
\end{flushleft}
\end{scriptsize}
\end{table}

As given in \citet{2012ApJ...755...42V}, our psf reference CVSO 30 varies by 0.17 mag (min to max) in the R band, consistent with our estimates within YETI.
The present steep wavelength dependence of the variability amplitudes is best described by hot star-spots \citep{2015MNRAS.450.3991K}, therefore we can extrapolate from measurements of the very similar T Tauri GQ Lup \citep{2007A&A...468.1039B}. According to this, 0.17 mag in R correspond to about 0.1 mag and 0.055 mag variability in J and Ks band, respectively. As the hot spots change the bands simultaneously,
this gives rise to a maximum systematic offset of 0.045 mag in J-Ks colour. We give an estimate of this variability as black error bars for a possible additional systematic offset of CVSO 30 c in Fig.~\ref{FigPhot}.

The colours of CVSO 30 and CVSO 30 c are very similar (Table \ref{TableCVSOAsPhot}\,and\,Fig.~\ref{FigPhot}). We currently lack a spectrum of CVSO 30 c in J band, therefore we used the M3V star Gl 388 \citep{2005ApJ...623.1115C,2009ApJS..185..289R} and the L3/L4 brown dwarf 2MASS J11463449+2230527 \citep{2005ApJ...623.1115C} to derive a preliminary filter correction between 2MASS and NACO for CVSO 30 and CVSO 30 c. The colours of CVSO 30 are well known from 2MASS (Table \ref{TableCVSOsys}), the differential brightnesses to CVSO 30 c vary from NACO to 2MASS by 28 mmag in J, -21 mmag in H, and -38 mmag in Ks. Thus CVSO 30 c is 49 mmag redder in J-H and 17 mmag redder in H-Ks in 2MASS (red in Fig.~\ref{FigPhot}) than in the NACO results (grey in Fig.~\ref{FigPhot}).

In Fig.~\ref{FigPhot} and Table \ref{TableChi} we compare CVSO 30 c to the colours of several possible sources. We find that background stars of spectral types OBAFGK are too blue in J-H, late-M dwarfs are too blue in J-H and too red in H-K, while foreground L- and late T-dwarfs are either too red in H-K or too blue in J-H. In addition, background galaxies, quasars, and H/He white dwarfs are also inconsistent with the values of CVSO 30 c. Only late-type giants, early-M and early-T dwarfs, and planetary mass free-floating objects such as are found in the $\sigma$ Orionis star cluster have comparable colours \citep{2000Sci...290..103Z,2012ApJ...754...30P}.

\section{CVSO 30 c spectroscopic analysis}

\begin{figure}
  \centering
  \includegraphics[width=0.16\textwidth]{bigcubefull.eps}
  \includegraphics[width=0.16\textwidth]{rotcubefull.eps}
  \includegraphics[width=0.16\textwidth]{sdcubefull.eps}
  \caption{Median in wavelength direction of the reduced VLT/SINFONI integral field cubes. \textit{Left:} Cube after reduction. \textit{Centre:} Cube after removing the primary halo, assumed to be centred at the separation of 1.85$``$, as measured in the VLT/NACO images. North is about 70$^{\circ}$ from the right-hand side towards the bottom of the plots. \textit{Right:} Cube after removing
the primary halo, spectral deconvolution, and polynomial flattening of the resulting background, used for the extraction of the final spectrum.}
  \label{FigCubes}
\end{figure}

\begin{figure*}
  \centering
22  \includegraphics[width=0.68\textwidth]{CVSO30c_FinalChiplot_1600K_logg3.6_Metallicity0.3_Extinction0.19mag.eps}
  \caption{Spectrum of CVSO 30 c as extracted from the spectral deconvolution-corrected cube in the right panel of Fig.~\ref{FigCubes}. \textit{Top:} The spectrum in resolution 700 (black) is
  shown after binning of the original extracted spectrum in resolution 1500 (green). The best-fitting Drift-Phoenix model of \cite{2008ApJ...675L.105H} is shown in red, fitting both the
  individually normalised H and K spectra. This type of normalisation was necessary because the redder colour of the models, in comparison to the unusually blue nature of CVSO 30 c, would steer
  the best-fitting model to higher temperatures, which would
prevent fitting the individual features in H and K band. The best-fitting model (red) corresponds to 1600 K, surface gravity log g 3.6 dex,
  metallicity [M/H] 0.3 dex, and 0.19 mag of visual extinction. \textit{Bottom:} Absolute value of the difference between spectrum and model from the top panel (black) versus noise floor at the
  corresponding position (green).
  }
  \label{FigSpec2}
\end{figure*}

\begin{figure}
  \centering
  \includegraphics[width=0.35\textwidth]{CVSO30c_FinalCountourplot1.eps}
  \includegraphics[width=0.35\textwidth]{CVSO30c_FinalCountourplot2.eps}
  \includegraphics[width=0.35\textwidth]{CVSO30c_FinalCountourplot3.eps}
  \caption{1 $\sigma$ contour plots of the $\chi^2$ Drift-Phoenix model fit to the spectrum shown in Fig.~\ref{FigSpec2}. Contour plot in extinction vs.~effective temperature (top), surface gravity log g vs.~effective temperature (centre) and metallicity [M/H] vs.~effective temperature (bottom). The fit shows a best fit at 1600 K, low extinction of 0.19 mag, higher values becoming
increasingly less likely, and a best fit at log g 3.6. While all surface gravities seem to be almost of equal probability, a high surface gravity foreground brown dwarf can be excluded from the shape of the H band in Fig.~\ref{FigSpec}. Although the young planetary models differ in photometric colours, this could be because of a not yet fully understood change in the cloud properties at the L-T transition that is indicated by the change in brightness of the L-T transition with age of the system, which we show in Fig.~\ref{FigColMag}.}
  \label{FigContSpec}
\end{figure}

A common proper motion analysis is not feasible because of the low proper motion of the host star (Table~\ref{TableCVSOsys}), therefore we carried out spectroscopic follow-up observations at the end of 2013, using the ESO VLT integral field unit SINFONI. The observations were made in H+K band with 100 mas/spaxel scale (FoV: 3 arcsec x 3 arcsec). The instrument provides information in the two spatial directions of the sky in addition to the simultaneous H- and K-band spectra. An unfortunate timing of the observations led to a parallactic angle at which a spike,
probably of the telescope secondary mounting, was superimposed onto the well-separated spectrum of the companion candidate CVSO 30 c.

After correcting, the resulting spectrum can be compared to model atmospheres to determine its basic properties and to other sub-stellar companions to assess its youth and the reliability of the models at this low age, surface gravity, and temperature regime.

In an attempt to optimally subtract the spike of the host star, we performed several standard and customised reduction steps. After dark subtraction, flat-fielding, wavelength calibration, and
cube reconstruction, we found that the spike was superimposed onto the companion in every one of the three individual exposures, but at slightly different orientation angles
(Fig.~\ref{FigCubes}, left panel). As a first step, we used the NACO astrometry to determine the central position of the primary, which is itself outside the observed field of view of the integral field observations. The orientation of the SINFONI observations was intentionally chosen to leave the connection line of primary and companion exactly in x direction. The primary is
about 1.85 arcsec exactly to the left of CVSO 30 c in the data because the x direction offers a twice as good sampling regarding the number of pixels for the separation.
We were thus able to subtract the radial symmetric halo of the host star from the data cube (Fig.~\ref{FigCubes}, central panel) using the nominal spatial scale.
This is necessary because the halo of the primary star is determined by the AO performance at the different wavelength.
At this stage, we extracted a first spectrum by subtracting an average spectrum of the spike, left and right of the companion psf from the superposition of companion and spike.
We find the results in Fig.~\ref{FigSpecAppend} before (red spectrum) and after (blue spectrum) spike subtraction, which also removes the still-present OH lines.
The horizontal spike in Fig.~\ref{FigCubes} appears too narrow to the right. This is a projection effect because the rotation of the spike within the three median-combined cubes
leads to less overlap on the right-hand side of the cube than on the left-hand side. For this reason, the continuum in Fig.~\ref{FigSpecAppend} is not trustworthy because the flux of the spike
below the companion candidate is not the average of the spike flux to the left and right of the object.

We tried several methods to remove the spike and decided to follow the spectral deconvolution technique \citep{2002ApJ...578..543S,2007MNRAS.378.1229T}.
This method is able to distinguish both the wavelength-dependent airy rings and speckles and the spike from the light of the wavelength-independent companion position by using the long wavelength coverage of the observed data cube.
As given in \citet{2007MNRAS.378.1229T} for the same instrument, the bifurcation radius for SINFONI H+K is for $\epsilon$=1.1 r=246 mas, and for $\epsilon$=1.2 r=268 mas, which means that parts of the
data without contamination of the companion could be found at the much higher separation of about 1.85 arcsec.
The reduction was then completed by applying a polynomial background correction around CVSO 30 c because the previous reduction steps left a low spatial frequency remnant around it (Fig.~\ref{FigCubes}, right panel). Finally, the optimal extraction algorithm \citep{1986PASP...98..609H} was performed around the companion and subtracted by the corresponding background flux from the close, well-corrected vicinity, and the telluric atmosphere correction using HD 61957, a B3V spectroscopic standard observed in the same night.

\begin{figure*}
  \centering

  \includegraphics[width=\textwidth]{Hbandplot4.eps}
  \caption{
  H-band spectrum of CVSO 30 c (lower left) compared to several known planetary candidates

  and background objects (subplots A, D, E).
  The triangular shape of the H band (A), with red linear fits guiding the eye, indicates that it is not a background galaxy, but a sub-stellar companion. Beta Pic b has approximately
  the same luminosity and temperature \citep{2015ApJ...798L...3C} but a different surface gravity, hence about twice the mass of CVSO 30 c. As shown (C), the Drift-Phoenix models indicate that the H band becomes less steep with temperature. This means that CVSO 30 c is even slightly lower in temperature than $\beta$ Pic b.
  In the upper left panel another candidate is shown, detected at 4.3'' from the A1 star HD 35367, which is about 0.5 mag brighter in the K band than CVSO 30 c, but is obviously located in the background.
  In addition, the H band (D) and K band (E) of CT Cha b and 2M 0441 Bb, the best-fitting comparison objects, are given in K band. These two and CVSO 30 c are given in (D, E) with identical offsets in H band and K band. Additionally, the best-fitting giants and a sample of late-type dwarfs is shown for comparison.
  References and individual reduced $\chi^2_r$ comparison values are given in Table \ref{TableChi}. Low-resolution spectra of free-floating planetary candidates are not shown, but can be found in \citet{2001ApJ...558L.117M}.
  }
  \label{FigSpec}
\end{figure*}

We first compare the spectrum of CVSO 30 c to spectra derived from Drift-Phoenix atmosphere simulations. These are dedicated radiative transfer models that take the strong continuum altering influence of dust cloud formation in the detectable parts of planetary atmospheres into account \citep{2008ApJ...675L.105H}. From a $\chi^2$
comparison of the H- and K-band spectra to the model grid, we find an effective temperature of about 1800 - 1900 K, while the individual fit of the H- and  K-band spectrum give a lower T$_{eff}$ of about 1600 K. In addition, the slope of the blue part of the triangular H band is too steep in the atmosphere models of about 1800 K and does not fit the continuum well. The higher T$_{eff}$ is only needed to fit the unusually blue H-Ks colour of the object, as already discussed in the previous photometry section and visible in Fig.~\ref{FigPhot}, since the models do yet not include a good description of the dust opacity drop at the L-T transition. We thus decided to fit the H and K band simultaneously, but normalising them individually, to cope with the unusual colours, while using all the present information for the fit. In this way, we find a best-fitting T$_{\mathrm{eff}}$=~1600$^{+120}_{-300}$ K, an extinction A$_V$=~0.19$^{+2.51}_{-0.19}$ mag, a surface gravity $\log{g}$\,[cm/s$^2$]=~3.6$^{+1.4}_{-0.6}$ dex, and a metallicity log[(M/H)/(M/H)$_{\odot}$]=~0.3$_{-0.9}$ dex at the upper supersolar edge of the grid.
The 1 $\sigma$ fitting contours are shown in Fig.~\ref{FigContSpec},
where they delineate the full regime for the error bars, and the best fit itself is shown in Fig.~\ref{FigSpec2}.

In Fig.~\ref{FigSpec} we compare the spectrum of CVSO 30 c to the triangular shaped H-band spectrum of the $\beta$ Pic b planet
that was obtained with the Gemini Planet Imager \citep[GPI,][]{2015ApJ...798L...3C}.
We also compare this to other planetary mass objects. $\beta$ Pic b is particularly suited as comparison object because it is young (10--20 Myr) and has about the same luminosity and effective temperature (1600--1700 K) while being of higher mass (10--12 M$_{\mathrm{Jup}}$).
We show linear fits to the blue and red part of the H band and the triangular shape of the chosen Drift-Phoenix models. In contrast to M5~--~L5 companions,
for which the H$_2$O index in \citet{2007ApJ...657..511A} shows an increase in water absorption, the absorption becomes shallower for later spectral types. This means that even though the formal $\chi^2$ fit finds a best temperature of 1600 K for CVSO 30 c, the temperature is likely to be lower than for $\beta$ Pic b, exhibiting a steeper H-band spectrum.
The object's spectrum is not consistent with a giant of any spectral type. The best-fitting giants with consistent photometry (Fig.~\ref{FigPhot}\,and\,Table \ref{TableChi}) are shown as comparison in Fig.~\ref{FigSpec} and would be at a distance of about 200 Mpc. To improve the fit in the K band, the spectral type would have to be later than M7III, while the H band does not fit for these objects.
Finally, CVSO 30 c, which is comparable but younger, must have a lower surface gravity than $\beta$ Pic b, which is determined to have a 1$\sigma$ upper limit of $\log{g}$\,[cm/s$^2$]=~4.3 dex according to the linear prior orbit fit in \citet{2014AandA...567L...9B}.
This corrects the surface gravity of CVSO 30 c to $\log{g}$\,[cm/s$^2$]=~3.6$^{+0.7}_{-0.6}$ dex.

\section{AstraLux lucky imaging follow-up observations}

\begin{figure}
  \centering
  \includegraphics[width=0.30\textwidth]{pic.eps}
  \caption{AstraLux z$^{\prime}$ band image of CVSO 30, taken on Aug 27, 2015. The dotted circle indicates an angular separation of 1.8 arcsec to CVSO 30 (see Fig.~\ref{AstraLuxLimit}). No other
objects are detected except for the star, which is located in the centre of the AstraLux image.
  }
  \label{AstraLux}
\end{figure}

\begin{figure}
  \centering
  \includegraphics[width=0.35\textwidth]{limit.eps}
  \caption{S/N=\,5 detection limit of our AstraLux observation of CVSO 30 (Fig.~\ref{AstraLux}). The reached magnitude difference that is dependent on the angular separation to the star is shown. The horizontal dashed lines indicate the expected magnitude differences of sub-stellar companions of the star at an age of 3 Myr. Beyond about 1.8 arcsec (or $\sim$640 au of projected separation), all companions with masses down to 10 M$_{\mathrm{Jup}}$ can be excluded around CVSO 30.
  }
  \label{AstraLuxLimit}
\end{figure}

We performed a follow-up of CVSO 30 with 2000\,s of AstraLux integration in z$^{\prime}$. The individual AstraLux images were combined using our own pipeline for the reduction of lucky imaging data. The fully reduced AstraLux image is shown in Fig.~\ref{AstraLux}. z$^{\prime}$ photometry of CVSO 30 was not measured so far, but can be derived from its magnitudes in other photometric bands using the colour transformation equations\footnote{$r - R = 0.77 \cdot (V - R) - 0.37$ and $r - z^{\prime} = 1.584 \cdot (R - I) - 0.386$} from \citet{2006A&A...460..339J}. The V- and R-band photometry of CVSO 30, as given by \citet{2005AJ....129..907B} and \citet{2012ApJ...755...42V} (V = 16.26 $\pm$ 0.19 mag, and R = 15.19 $\pm$ 0.085 mag), and the I-band photometry of the star, listed in the 2005 DENIS database (I = 13.695 $\pm$ 0.030 mag), yield z$^{\prime}$ = 13.66 mag.

The (S/N= 5) detection limit reached in the AstraLux observation is given in Fig.~\ref{AstraLuxLimit}. At an angular separation of about 1.8 arcsec from CVSO 30 (or $\sim$640 au of projected separation), companions that are $\Delta$z$^{\prime}$= 6.8 mag fainter than the star are still detectable at S/N = 5. The reached detection limit at this angular separation is z$^{\prime}$= 20.5 mag, which is just a tenth of magnitude above the limiting magnitude in the background-noise-limited region around the star at angular separations larger than 2 arcsec. This results in a limiting absolute magnitude of M$_{\mathrm{z}^{\prime}}$= 12.7 mag, allowing the detection of sub-stellar companions of the star with masses down to 10 M$_{\mathrm{Jup}}$ according to the evolutionary models
of \citet{2015A&A...577A..42B}.

Furthermore, the AstraLux observations also exclude all young (3 Myr) stellar objects (mass higher than 75 M$_{\mathrm{Jup}}$) that are unrelated to CVSO 30, which are located in the AstraLux field of view at distances closer than about 3410 pc. All young M dwarfs with an age of 3 Myr and masses above 15 M$_{\mathrm{Jup}}$ (T$_{\mathrm{eff}}$ > 2400 K) can be ruled out up to 530 pc. All old stellar objects (mass higher than 75 M$_{\mathrm{Jup}}$) with an age of 5 Gyr can be excluded when they are located closer than about 130 pc.

The AstraLux upper limit results in z$^{\prime}$\,-\,Ks\,$\gtrsim$ 1.75 mag, which corresponds to excluding $\gtrsim$ 0.2 M$_{\odot}$ or $\gtrsim$ 3300 K \citep{2015A&A...577A..42B} as possible sources or about earlier than M4.5V in spectal type \citep{1995ApJS..101..117K}. Because any object later than $\sim$\,M2V\,/\,M3V can be excluded by $\gtrsim$ 4 $\sigma$ from JHKs photometry (Table \ref{TableChi}), no M dwarf can be a false positive of the new companion candidate CVSO 30 c.

\section{Mass determination and conclusions}

With the object brightness determined from the direct near-IR imaging and the information provided by the spectroscopic analysis, we can directly estimate the basic parameters of CVSO 30 c.
To determine the luminosity, we considered the extinction law by \citet{1985ApJ...288..618R}, a bolometric correction of B.C.$_K$= 3.3$^{+0.0}_{-0.7}$ mag for spectral type L5-T4 \citep{2004AJ....127.3516G}, and a distance of 357$\,\pm\,$52 pc to the 25 Orionis cluster.
From the 2MASS brightness of the primary and the differential brightness measured in our VLT NACO data (Table~\ref{TableCVSOAsPhot}) and the extinction value towards the companion derived from spectroscopy, we find $\log{L_{bol}/L_{\odot}}= -3.78^{+0.33}_{-0.13}$~dex. From the luminosity and effective temperature, we calculate the radius to be R=~1.63$^{+0.87}_{-0.34}$ R$_{\mathrm{Jup}}$. In combination with the derived surface gravity, this would correspond to a mass of M=~4.3
M$_{\mathrm{Jup}}$, dominated in its errors by high distance and surface gravity uncertainties.
While the latter value and the photometry (Fig.~\ref{FigPhot}) would be consistent with a high surface gravity, thus old foreground T-type brown dwarf, but inconsistent with an L-type brown dwarf, the available spectroscopy excludes an old T-type brown dwarf (Fig.~\ref{FigSpec}\, and \,Table \ref{TableChi}).
While the photometry is also consistent with early-M dwarfs, the K-band spectroscopy and z$^{\prime}$ upper limit show the opposite behaviour, being only consistent with late-M dwarfs, excluding all types with
high significance. Similarly, the remaining H-band spectroscopy excludes all comparison objects.
Only the best-fitting Drift-Phoenix model (Fig.~\ref{FigSpec2}) shows
low deviation in H band, consistent with the fact that the only available very young directly imaged planet candidates exhibit higher temperatures, thus a steeper H band (Fig.~\ref{FigSpec}).

Although recent observations by \citet{2015ApJ...812...48Y} cast doubts on the existence of the inner transiting planet candidate CVSO 30 b or PTFO 8-8695 b, we assume its existence throughout the remaining discussion because all five hypotheses have difficulties
in reproducing the observations presented in \citet{2015ApJ...812...48Y}, including for example~different types of starspots. The inner planet hypothesis gives another constraint, namely that the system has to be stable with both its planets. As described in \citet{2012ApJ...755...42V}, CVSO 30 b is very close to its Roche radius, the radius of stability.
Assuming the values for mass of CVSO 30 b, its radius and orbital period (Tables~\ref{TableCVSOAsPhot} and \ref{TableCVSOPlanets}), we find from the Roche limit an upper limit for the mass of CVSO 30 of $\leq$ 0.92 M$_{\odot}$ for a stable inner system comprised of CVSO 30 A and b.
This mass limit for CVSO 30 is fulfilled
at 1 Myr for masses of CVSO 30 c of $\leq$ 6.9 M$_{\mathrm{Jup}}$ at $\leq$ 760 pc up to 5.8 Myr with masses of CVSO 30 c of $\leq$ 9.2 M$_{\mathrm{Jup}}$ at $\leq$ 455 pc, according to BT-Settl evolutionary models \citep{2014IAUS..299..271A,2015A&A...577A..42B}. Higher ages are not consistent with the age estimate of the primary, but even at 20 Myr we find a mass of CVSO 30 c of $\leq$ 12.1 M$_{\mathrm{Jup}}$ at $\leq$ 340 pc. With the Roche stability criterion for CVSO 30 b, the previous calculations result in a mass estimate of M=~4.3$^{+4.9}_{-3.7}$ M$_{\mathrm{J up}}$ for CVSO 30 c.

For the approximate age of CVSO 30, 2--3 Myr BT-Settl evolutionary models \citep{2014IAUS..299..271A,2015A&A...577A..42B} predict an apparent brightness of m$_K\sim$ 18.5 mag (assuming the distance to 25 Ori), effective temperature $\sim$1575 K, mass 4\,--\,5 M$_{\mathrm{Jup}}$, and $\log{L_{bol}/L_{\odot}}\sim$~-3.8 dex. These expected values are very close to the best-fit atmospheric model spectra fits above, and even the derived visual extinction of about 0.19 mag is very close to the value of the primary $\sim$0.12 mag \citep{2005AJ....129..907B}.

Of course, these evolutionary models can also be used to determine the resulting mass from the luminosity and age of the companion candidate and system, respectively. To put CVSO 30 c into context, we show the models and several of the currently known directly imaged planet candidates in Fig.~\ref{FigEvol}. The new companion is one of the youngest and lowest mass companions, and we find a mass of
4.7$^{+5.5}_{-2.0}$ M$_{\mathrm{Jup}}$ because the luminosity is not very precise as a result of the rather scarce knowledge of the distance of the system.
However, if we take temperature additionally into account, we find a more precise mass determination of 4.7$^{+3.6}_{-2.0}$ M$_{\mathrm{Jup}}$, which places CVSO 30 c well within the planetary regime and would mean that it is very close in mass to the probable inner companion of the system CVSO 30 b with about 2.8 -- 6.9 M$_{\mathrm{Jup}}$ \citep{2012ApJ...755...42V,2013ApJ...774...53B}.

\begin{figure}
  \centering
  \includegraphics[width=0.5\textwidth]{evolutionplot.eps}
  \caption{Evolution of young stars, brown dwarfs, and planets with BT-Settl evolutionary tracks \citep{2014IAUS..299..271A,2015A&A...577A..42B}. Shown are a few of the planet candidates known so far in comparison to the new sub-stellar companion candidate CVSO 30 c (see Table~\ref{TableRefEvol}).}
  \label{FigEvol}
\end{figure}

\begin{figure}
  \centering
  \includegraphics[angle=90,width=0.5\textwidth]{CVSO30_Ks_2.eps}
  \caption{Dynamic range per pixel achieved in our VLT / NACO Ks-band observations, given as 3 $\sigma$ contrast to the primary star. The companion would have been detectable until 0.48 arc seconds or 171 au separation. A depth of 20.2 mag was reached at maximum, corresponding to 2.8 M$_{\mathrm{Jup}}$.}
  \label{FigDynRan}
\end{figure}

In Fig.~\ref{FigDynRan} we show the depth reached per pixel in the Ks-band epoch of 20.2 mag, corresponding to 2.8 M$_{\mathrm{Jup}}$ at the age of CVSO 30, using the same models as above. Brown dwarfs could be found from 30 au outwards, planets from 79 au outwards, and CVSO 30 c could have been found from 171 au outwards.

The core-accretion model
\citep{1969Icar...10..109S,1973ApJ...183.1051G,1996Icar..124...62P},
one of the much debated planet formation scenarios, is unlikely to form an object in situ at
$\geq$662 au because the timescale would be prohibitively long at such separations.
In principle, the object could also have formed in a star-like fashion by turbulent core fragmentation as in the case of a binary star system, since the opacity limit for fragmentation is a few Jupiter masses \citep{2009MNRAS.392..590B}, but the large separation and high mass ratio argue against this hypothesis.

The even more obvious possibility would be planet-planet scattering
because an inner planet candidate CVSO 30 b of comparable mass is present that could have been scattered inward at the very same scattering event.
Several authors simulated such events and found mostly highly eccentric orbits for the outer scattered planets of up to 100s or 1000s of au \citep{2009MNRAS.392..413S,2011ApJ...742...72N}, which is similar to the minimum separation of our outer planet candidate of 662 au.
The closest match to CVSO 30 bc of a model simulation was presented by \citet{2011ApJ...742...72N} with an object at $\sim$300 au, which has an inner hot planet with
which it was scattered. Scattering or gravitational interaction might not be that uncommon as $72\%\pm16\%$
of hot Jupiters are part of multi-planet and/or multi-star systems \citep{2015ApJ...800..138N}.

The luminosity of CVSO 30 c is only consistent with hot-start models that usually represent the objects formed by gravitational disk-instability, not with cold-start models that are attributed to
core-accretion-formed planets \citep{2007ApJ...655..541M}. However, as stated in \citet{2012ApJ...745..174S}, first-principle calculations cannot yet specify the initial (post-formation) entropies of objects with certainty in the different formation scenarios, hence CVSO 30 c could have formed through a gravitational disk-instability or core accretion and might have been scattered with CVSO 30 b afterwards.

In this context, it would also be important to clarify the nature of the unusually blue H-Ks colour of CVSO 30 c. It is consistent with colours of free-floating planets (Fig.~\ref{FigPhot}) and might
be caused by its youth, allowing the companion to be very bright, still already being at the L-T transition, which would be consistent with simulations of cluster brown dwarfs at very young ages and
their colours in \citet{2008ApJ...689.1327S} (Fig.~\ref{FigColMag}). This would imply a temperature at the lower end of the 1$\sigma$ errors found for CVSO 30 c, $\leq$ 1400 K, which is consistent with the less steep H band in comparison to $\beta$ Pic b of about 1600--1700K \citep{2015ApJ...798L...3C}, however, as shown in Fig.~\ref{FigSpec}.
For old brown dwarfs the L-T transition occurs at T$_{eff}$ 1200--1400 K, when methane absorption bands start to be ubiquitously seen. However, in the $\sim$30 Myr old planet candidates around HR 8799 no strong methane is found, while the spectrum of the $\sim$90 Myr old object around GU Psc shows strong methane absorption \citep{2014ApJ...787....5N} all at temperatures of about 1000--1100 K. Thus the L-T transition might be gravity dependent \citep{2012ApJ...754..135M}.
Binarity of CVSO 30 c cannot be excluded either, which would also explain the unusual blue H-Ks colour.

Since we cannot confirm that CVSO 30 c is co-moving with its host star from our proper motion analysis, we cannot exclude the possibility that CVSO 30 c is a free-floating young planet belonging to the 25 Ori cluster, which is not gravitationally bound to CVSO 30. However, such a coincidence is highly improbable. \citet{2000Sci...290..103Z} searched 847 arcmin$^2$ of the $\sigma$ Orionis star cluster for free-floating planets and found only six candidates in the survey with similar colours as CVSO 30 c. This means that the probability to find a free-floating planet by chance within a radius of 1.85'' around the transiting planet host star CVSO 30 is about 2$\cdot$10$^{-5}$.

With a mass ratio of planet candidate to star q= 0.0115 $\pm$ 0.0015, CVSO 30 c (and CVSO 30 b) is among the imaged planets with the lowest mass ratio
\citep[see e.g.][]{2014MNRAS.445.3694D}.

\begin{figure}
  \centering
  \includegraphics[width=0.5\textwidth]{SMplot.eps}
  \caption{Colour-magnitude diagram of a simulated cluster brown dwarf population from \citet{2008ApJ...689.1327S}. Each sequence corresponds to a different age as given in the legend.
  Superimposed we show the positions of several planet candidates and CVSO 30 c. Its unusual blue colour can most likely be attributed to its youth; it is about 2.4 Myr old. The younger the objects, the brighter they are because of not-yet-occurred contraction. Hence they reach the L- and T-dwarf regime at higher brightnesses. If this extrapolation is correct, CVSO 30 c is at the L-T transition, which is roughly consistent with its low effective temperature results. See the discussion and Table~\ref{TableRefColMag} and Fig.~\ref{FigColMagAppend} for details.
  }
  \label{FigColMag}
\end{figure}

In summary, CVSO 30 b and c for the first time allow a comprehensive study of both a transiting and a directly imaged
planet candidate within the same system, hence at the same age and even similar masses, using RV, transit photometry, direct imaging, and spectroscopy.
Within a few years, the GAIA satellite mission
\citep{2005ASPC..338....3P}
will provide the distance to the system to a precision of about 10 pc, which will additionally restrict the
mass of CVSO 30 c.
Simulations of a possible scattering event will profit from the current (end) conditions found for the system. Considering that the inner planet is very close to the Roche stability limit and the outer planet is far away from its host star, the future evolution and stability of the system is also very interesting for dedicated modelling.
To investigate how often
these scattering events occur, inner planets need also be searched for around other stars with directly imaged wide planets.

\begin{acknowledgements}
We thank the ESO and CAHA staff for support, especially during service-mode observations. Moreover, we would like to thank Jeff Chilcote and David Lafreni\`ere for kindly providing electronic versions of comparison spectra from their publications and the anonymous referee, the editor
and our language editor
for helpful comments that improved this manuscript.

TOBS and JHMMS acknowledge support by the DFG Graduiertenkolleg 1351 ``Extrasolar Planets and their Host Stars``.
RN and SR would like to thank the DFG for support in the Priority Programme SPP 1385 on the
"First Ten Million Years of the Solar system" in project NE 515/33-1.
SR is currently a Research Fellow at ESA/ESTEC.

This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the VizieR catalog access tool and the Simbad database, both operated at the Observatoire Strasbourg.
This research has made use of NASA's Astrophysics Data System.

\end{acknowledgements}

\listofobjects

redpajama_set_name: RedPajamaArXiv


text:
Papal Visit
Same-sex marriage signed into law by Ministers
May referendum 'reaffirmed the importance of marriage and family for our society', Fitzgerald says
Tue, Nov 10, 2015, 18:22
Patsy McGarry
Minister for Justice and Equality Frances Fitzgerald signed the commencement order for the Marriage Act 2015 which will enable same-sex couples to marry in Ireland. Tánaiste Joan Burton signed an accompanying regulation under the Civil Registration Act 2004 at Dublin Castle. Photograph: Dara Mac Dónaill/The Irish Times
The Minister for Justice and Equality Frances Fitzgerald signed the commencement order for the Marriage Act 2015 at Dublin Castle on Tuesday evening. It will bring provisions of the Marriage Act 2015 into effect from Monday next November 16th. From then a marriage can take place between two persons of the same sex.
Tánaiste Joan Burton signed an accompanying regulation under the Civil Registration Act 2002.
The signing by both Ministers order gives effect to the referendum of May 22nd last which approved marriage being available to same-sex couples. Such couples, including those already in civil partnerships, will be able to give notice of their intention to marry from Monday next.
My advice to all #MarRef campaigners right now.... pic.twitter.com/ASvbkJTUvq
— Aodhán Ó Ríordáin TD (@AodhanORiordain) November 10, 2015
Tanaiste says that first marriages of same-sex couples will take place from next week! #MarRef #YesEquality #YestoLove
— Colm O'Gorman (@Colmogorman) November 10, 2015
As of round about NOW all Irish people can marry who they love regardless of their gender. Hurray for us! #MarRef
— Conor Pope (@conor_pope) November 10, 2015
At the Dublin Castle ceremony Ms Fitzgerald said "the Irish people blazed a trail on May 22nd 2015 when they became the first sovereign people to choose marriage equality by popular vote. They determined that Ireland should be characterised by solidarity and inclusiveness. They have reaffirmed the importance of marriage and family for our society."
Signing the order she added "it is a real pleasure to sign this order in the company of some of the couples who will be able to marry in the coming weeks and months. The Marriage Act has profound symbolic importance, but will also have a real and tangible impact on their family life."
The Dublin Castle ceremony brings to an end a successful campaign by the Yes Equality coalition of the Irish Council for Civil Liberties (ICCL), GLEN (Gay and Lesbian Equality Network) and Marriage Equality, Mark Kelly, ICCL executive, director said.
"The ICCL is profoundly grateful to Ailbhe Smyth of Marriage Equality and Kieran Rose of GLEN for their decades of dedicated advocacy in favour of full equality for same sex couples. The campaign stood on the shoulders of giants," he said. "We should also like to express our appreciation for the sheer hard graft of Gráinne Healy and Brian Sheehan, especially during the last intensive weeks of the campaign, during which they served as co-directors of campaign operations," he said.
"A small army of volunteers at headquarters and across the country truly brought the campaign alive and it is thanks to them - and everyone who voted yes in May 2015 - that marriage equality will become the law of the land on November 16th," he said.
Ailbhe Smith
Brian Sheehan
Frances Fitzgerald
Grainne Healy
Joan Burton Tanaiste
Kieran Rose
Irish Council For Civil Liberties
Miriam Lord: Pink ladies squeeze last mileage out of The Gays
Róisín Meets: Yes Equality activist Gráinne Healy
How the Yes was won: the inside story of the marriage referendum
Same sex marriage vote thwarted by DUP veto
Criminal Court
Kerryman bled to death after blood vessel sliced with butcher's knife, court hears
Week beginning Saturday, July 13th, 2019
Week beginning Saturday, June 22nd, 2019

redpajama_set_name: RedPajamaCommonCrawl


Creating a schedule that works for you both can be difficult, but it's worth it!
If you want to create a parenting plan that work for both parents, and doesn't favor one over the other, you're going to have to agree to work together. This means that you and your spouse need to lay aside your differences in the name of creating something that is good for your kids, and works well for BOTH of you. You may be justifiably angry at your spouse, but this is not the time to get back at them. This is about working together for the betterment of your kids' lives.
You can't have everything your own way. If you are going to work together with your spouse to craft a schedule that honors both of your individual needs, you have to be willing to compromise. Some aspects of the schedule will be convenient for you, and some won't. But the same goes for your spouse. Both of you have to be willing to be flexible and work around each other's commitments.
Sit down and create a list of your commitments.
Sit down, apart from your spouse, and write down all of the commitments you have in the average month. This includes your work schedule, your standing social engagements (weekly bowling perhaps, or Thursday night drinks with coworkers?), and regular appointments you have to keep (maybe your weekly therapy appointment, or a monthly meeting with a medical specialist). Now categorize your commitments into "fixed" and "flexible" – in other words, things that you can't change, and things that you could reschedule or skip if you had to.
You and your spouse need to sit down and compare your calendars. Do they have something on a Wednesday after work that they simply can't get out of, while you have a social engagement that you could afford to miss? Their situation trumps yours. Do you have a fixed work schedule, while they have more flexibility with their hours? Then your situation trumps theirs. Compare your commitments, and try to work out what days are best for you to have the kids, and what days work best for them.
Write up a tentative schedule that honors both of your schedules.
Now that you both know what's flexible and what isn't, you need to set to work creating a schedule that honors both of your commitments. If you both have fixed commitments at the same time, discuss options like taking turns to keep the kids on that night, or getting a scheduled babysitter for that evening and splitting the cost. There are lots of ways to work around a hectic schedule, but only if you're both willing to compromise.
Do you need help creating your parenting time schedule?
When parenting time was known as visitation, the idea was that the parent with greater physical custody had greater say in decisions regarding the rights of the child. However, this is no longer true in Michigan Family Courts. If you feel sidelined by your child's other parent during your parenting time, then it's time to discuss your situation with one of the skilled family law attorneys at The Kronzek Firm. We are available 24/7 at 866 766 5245 to help you work through your challenges.


March 29, 2018, 12:11 p.m.
NewsWhip, the social media monitoring company, crunched some numbers on how publishers' Facebook pages have been faring since then and offered some tips for not being the next Little Things, Cooking Panda, or Opposing Views. The full report can be found here.
Over half of the stories with top engagement in the past two months include hard news/current events/breaking news: "Surprisingly, the top stories since the algorithm change have had a good deal of breaking news at the top of the chart. In fact, since the Facebook algorithm change, 56 of the top 100 most engaging articles as of March 15th have been hard news/current event stories." NewsWhip also noted that 53 of the top 100 stories were from general news publishers.
Misinformation isn't gone: A fake story about how the "'disastrous' flu shot is causing a deadly flu outbreak" was the 26th most engaging story since the algorithm change, with almost 850,000 engagements on Facebook.
Niche, viral publishers are still figuring things out, though Little Things was the first one to go. Some organizations are using e-commerce as a buffer: NewsWhip says PopSugar will start hawking beauty products and High Snobiety has a goal to make e-commerce 30 percent of its revenue.
NBC News has bested Fox News as the most engaged publisher on Facebook for the first time since January 2017, signaling that "the major sites with network abilities and scale in breaking news events are likely to continue to perform well on social media," NewsWhip says. Reporters from hyperpartisan sources are still outpacing non-hyperpartisan reporters.
Schmidt, Christine. "Two months post-News Feed tweak: real news is not drowning, comments are growing, and videos are still winning, NewsWhip says." Nieman Journalism Lab. Nieman Foundation for Journalism at Harvard, 29 Mar. 2018. Web. 25 Apr. 2019.
Schmidt, Christine. "Two months post-News Feed tweak: real news is not drowning, comments are growing, and videos are still winning, NewsWhip says." Nieman Journalism Lab. Last modified March 29, 2018. Accessed April 25, 2019. https://www.niemanlab.org/2018/03/two-months-post-news-feed-tweak-real-news-is-not-drowning-comments-are-growing-and-videos-are-still-winning-newswhip-says/.


Students in grades 9-12 are invited.
Bill Stanley will be preaching, Harvest will be leading worship and we will gathering with students to pray for the next generation, call students to Jesus and invite students to follow God's call on their lives!
For more information contact Tim Price, 618-667-6241.
An all-new College Track has been added to Fire-Up this year. College students (18-23) will attend worship times and most meal times, but will mainly have a separate schedule including small groups, community times and mission projects.


text:
HBO Max / News / TV News
'The Last of Us' Renewed For Season 2 By HBO
Christian Hubbard Posted On January 27, 2023
With just two episodes released over the last few weeks, HBO's The Last of Us adaptation is one of the biggest hits of 2023 so far. Now, as first revealed by the program's social media platforms, HBO is already giving […]
Hulu / News
Meryl Streep Joins 'Only Murders In The Building' For Season 3
Season two of Hulu's Only Murders In The Building was an even bigger hit than season one was and earned the cast and crew a bevy of nominations and rave reviews since its release. Now, it appears the series is […]
News / The CW / TV News
'The Flash': First Look At The Return Of Stephen Amell On Set
Jacob Campbell Posted On January 11, 2023
Now that it is officially confirmed Stephen Amell's Oliver Queen will return for the final season of The Flash, fans are anxiously waiting for his on-screen reunion with Grant Gustin's Barry Allen. Thankfully, new images from the set of filming have […]
News / Paramount+ / TV News
Live-Action 'Dungeons & Dragons' Series In The Works At Paramount+
With the Chris Pine-starring Dungeons & Dragons: Honor Among Thieves film right around the corner, it appears Paramount remains firmly in the DnD franchise for future live-action projects. According to a new report by Deadline, a live-action series based on the […]
Anime / News / TV News
'Zom 100: Bucket List Of The Dead' Anime Announced
Jacob Campbell Posted On January 7, 2023
It has been confirmed another hit manga series will soon have its own anime. The Zom 100: Bucket List of the Dead anime has been officially announced and is set to premiere this July. Written by Haro Aso and illustrated […]
Movie News / Netflix / News
Noah Baumbach's New Film To Star Adam Sandler & Brad Pitt
Jacob Campbell Posted On December 31, 2022
Noah Baumbach's White Noise hit Netflix this week, and it seems his next picture for the streamer already has stars in mind. According to the New York Post, Adam Sandler and Brad Pitt are set to star. Details on the upcoming project […]
'Toilet-Bound Hanako-Kun' Anime Announces New Project
In unexpected news, it was officially announced that a new Toilet-bound Hanako-kun anime project is in the works. The announcement was shared on the series' Twitter account, along with a teaser trailer and key visual. Created by Aisalro in 2014, the manga is […]
'Blue Exorcist' Announces New TV Anime Project In The Works
Fans were in for a welcome surprise during Jump Festa 2023 as it was announced that a new Blue Exorcist anime project is in production. The project will come in the form of a third season that will pick up where the Blue […]
Anime Adaptation of Akira Toriyama's 'Sand Land' In Development
It appears that a new anime based on Dragon Ball creator Akira Toriyama's series Sand Land is in development. The project has been officially announced and is scheduled to release in 2023. Created by Toriyama in 2000, the series was published by […]
Anime / Movie News / News / TV News
'Spy x Family' Season 2 & Movie Special Trailer Released
During Jump Festa 2023, it was confirmed that not only is season 2 of Spy x Family in the works, but an original movie is also being developed. Now a special trailer for both releases has been revealed, confirming they will premiere […]
'The Last of Us' Episode 3 Review: "A Touching Love Story"


The landscape surrounding the Great Rivers is a blend of rolling hills falling away from the bluffs and, closer to the rivers themselves, large areas of flat floodplain.
Some of the floodplain is devoted to farming, some to industry and some to conservation. The Columbia Bottom Conservation Area is one such.
It's found close to the Missouri/Mississippi Confluence, on the south bank of the lower of the two rivers, the Missouri.
Not wholly conserved land in the sense that part of it is farmed, but following guidelines that preserve most of the natural vegetation and wetland.
It's traversed by a single paved road and a number of gravel tracks that converge at their end close to the Confluence. Most visitors end up there, either to take in the view, or, more commonly, to find a spot for fishing.
I, on the other hand, prefer to remain in the open for it is one the few local places where you can get a full sense of a big sky over a large expanse of flat land.
Perhaps because I grew up in a hilly and forested part of England, there is something very appealing to me about standing in an open area that stretches away in all directions. I love the sense of solitude, of being a small part of something much bigger.
As you might expect, I've devoted a lot of camera time to this scene over the years. There is always something striking to see even though the land has become comfortingly familiar.
Many years ago, when I first moved to Missouri, I felt little affinity for the land. I was consumed by homesickness for my native England. It took time, yes, but now I feel precisely the same fondness for these landscapes as I used to feel for the downs of Surrey.
In some senses more. I'm grateful for that.


text:
Qatar Tourism issues call to enlist in its Tour Guide Training Programme
Qatar Tourism issues call to enlist in its Tour Guide Training Program
The 14-day course provides comprehensive information about Qatar's history, environment and culture, and is required to obtain an official tour guide license
Qatar Tourism is offering its Tour Guide Training Programme to give practicing tour guides and eligible residents the opportunity to enhance their skills in the tourism sector. Developed by Qatar Tourism in collaboration with stakeholders, the programme aims to raise standards and regulate tourism service providers through providing official tour guide licenses to those who complete the required work. The initiative is part of Qatar Tourism's efforts to achieve Service Excellence in the sector and provide an unforgettable experience to the visitors, especially as borders reopen and Qatar prepares to host mega sporting events.
Dates of the upcoming training sessions will be announced in the coming months. Interested parties can register through the Qatar Tourism website or in person at the Ministry of Commerce and Industry office in Lusail, Al-Jassra Tower, first floor counter 44. The course will be conducted in English and the exam fee is QAR1,200 while the Tour Guide license fee is QAR1,000.
Berthold Trenkel from Qatar Tourism said: "As the main point of contact for visitors, tour guides need to be able to tell stories, giving visitors information and insights into the country's history, culture and heritage, that will help deliver an unparalleled experience. As part of our Tourism Sector Strategy, we are working closely with all tourism-facing entities to implement Service Excellence at every touch point of the visitor's journey. With Qatar's FIFA World Cup 2022 around the corner, we need more guides to cater to the huge number of visitors who will be arriving in the country."
The Tour Guide Training Programme uses the Tour Guide Manual that was developed by Qatar Tourism in partnership with stakeholders including Qatar Museums, Msheireb Museums, the Ministry of Municipality and Environment, Souq Waqif, Qatar Foundation, Qatar TV, and Sheikh Abdulla bin Zaid Al Mahmoud Islamic and Cultural Center (Al Fanar). While enabling tour guides to deliver insightful information about Qatar's society and ecosystem, the manual also contains a section on tour group management, highlighting the skills tour guides need to provide an ideal visitor experience.
Since the beginning of the programme in 2017, more than 100 tour guides have been trained, helping position Qatar as an ideal tourism spot.
Website: www.visitqatar.qa


South Branch Estates is a residential neighborhood in Wilmington, North Carolina. This community features a variety of mostly custom homes. Floor plans can range from as small as 1,500 square feet to over 3,500. Located off of Middle Sound Loop Road, this community is in the Ogden area of Wilmington, which has several popular attractions and anticipates many new options in the near future. Click on the listings below to see pictures, features, amenities, school information, and more. Interested in viewing a home or have questions? Please don't hesitate to contact us. We can help you with this community or any other in the Greater Wilmington real estate market.


RISE is for grades 7th through 12th. At RISE, we encourage teens to grow in their relationships with Christ by knowing Him through worship and His word. We also empower this generation to be the church of today and not wait until they are older to get involved. We run a church service led by empowered teens to reach others for Christ.
Join us at 6:30 p.m. for supper, service is from at 7:00 p.m. - 8:15 p.m.
1. We take the kids on several outings per semester, Please fill out the permission form here.
2. Click here to see what's happening next at Rise.
3. Click Here to be a part of our parent Facebook Group and get all the latest updates!


text:
02.10.2015China to supply two MRI scanners to Belarus Society
China will supply two permanent-magnet magnetic resonance imaging (MRI) scanners to Belarus. The decision is contained in an agreement between the governments of Belarus and China concluded through an exchange of letters on 14 May 2015. The information was published on the national legal Internet portal 2 October, BelTA has learned.
02.10.2015Belarus' lower house of parliament ratifies China-Belarus friendship and cooperation treaty
Members of the House of Representatives ratified the treaty on friendship and cooperation between China and Belarus on 2 October, BelTA has learned.
01.10.2015Belarusian Amkodor, Sinomach Heavy Industry to make excavation machines
The Belarusian mechanical engineering company Amkodor and the Chinese company Sinomach Heavy Industry intend to set up a joint venture to make excavation machines, representatives of the Belarusian company told BelTA.
01.10.2015Air China opens representative office in Belarus
Air China is going to open a representative office in Belarus, BelTA learned from the website of the National Airport Minsk.
01.10.2015Lukashenko: Belarusian-Chinese dialogue is vigorously developing
On behalf of the Belarusian people and himself President Alexander Lukashenko has sent greetings to China President Xi Jinping and the friendly people of China on the occasion of the 66th anniversary of the founding of the People's Republic of China, BelTA learned from the press service of the Belarusian leader.
29.09.2015Snopkov: Belarus takes active part in Silk Road Economic Belt initiative
Belarus takes an active part in the implementation of the initiative to build the Silk Road Economic Belt, Deputy Head of the Belarus President Administration Nikolai Snopkov said at the event timed to the 66th anniversary of the founding of the People's Republic of China on 29 September, BelTA has learned.
28.09.2015Five companies to become residents of Great Stone park soon
Five companies will become residents of the Chinese-Belarusian Industrial Park Great Stone in the near future, head of the park's administration Andrei Gal told reporters on 28 September, BelTA has learned.
27.09.2015Association of Chinese companies set up in Belarus
The association of Chinese companies has been set up in Belarus. Its presentation was held in Minsk on 27 September, BelTA has learned.
22.09.2015BelTA, China's Renmin Ribao sign memorandum of cooperation
The Belarusian news agency BelTA and China's Renmin Ribao (People's Daily) concluded a memorandum of cooperation in Beijing on 22 September, BelTA informs. The document was signed by First Deputy Director General of the Belarusian news agency BelTA Oksana Kirilchik and Renmin Ribao President Yang Zhenwu.
21.09.2015Wang Jiarui: The Silk Road project should meet the interests of its member states
The development of the new Silk Road project should take into account the interests of all the participating states, said Wang Jiarui, the Vice Chairman of the National Committee of the Chinese People's Political Consultative Conference and the Minister of the International Department of the Central Committee of the Communist Party of China, at the opening ceremony of the Media Cooperation Forum One Belt, One Road on 21 September, BelTA informs.


text:
More Alameda Turmoil
As the special election for a schools parcel tax neared, supporters and opponents exchanged charges of illegality.
by Michele Ellson
Whatever the outcome of this week's special election in Alameda, the battle over Measure A, the school parcel tax, has been another example of increasing tumult on the island. The opposing sides of the campaign have publicly attacked each other, repeatedly. And, most recently, they've filed complaints with the state's campaign watchdog accusing each other of improprieties. Each has denied wrongdoing.
Michael Robles-Wong, chairman of the Alameda Save Our Schools (SOS) campaign, the pro-parcel tax group, filed a complaint with the state's Fair Political Practices Commission late last month, alleging that the Committee Against Measure A illegally issued robocalls that failed to identify to voters who paid for the calls.
The Committee Against Measure A, meanwhile, announced that Leland Traiman, one of the leaders of that campaign, had filed an FPPC complaint against two pro-A campaign leaders; the campaign's political consultants; Alameda schools Superintendent Kirsten Vital; and Gray Harris, the teacher who appears in one of the ads. Traiman claimed the district subsidized Save Our Schools' campaign efforts by providing classroom space and a teacher for a campaign mailer in violation of state law. Representatives with the Committee Against Measure A, however, didn't provide a copy of the complaint when a reporter requested it.
Measure A would replace the school district's existing and soon-to-sunset taxes and increase the amount collected from $7 million to $12 million annually. It requires a two-thirds vote to pass. The outcome may be close because a similar school district measure last June fell just short of the two-thirds requirement, garnering 65.62 percent of the vote. Measure A, however, was crafted with extensive community input, including business owners who declined to endorse last year's Measure E. Proponents argued in this year's campaign that Alameda schools will have to endure devastating cuts without the tax measure, while opponents said it was unfair because it gave discounts to some large property owners, such as Alameda Towne Center and the Oakland Raiders.
A spokesperson for the pro-Measure A group called Traiman's claims that the school district subsidized the campaign "baseless" and said the campaign has complied with the law. Vital also denied that the district provided the pro-A campaign either free space or a teacher. She said the campaign requested, paid for, and received a permit to shoot their photos after school hours.
A copy of a permit supplied by the school district shows that the campaign paid a charge of $12.25 to access a room at Otis Elementary School for a photo shoot between 4 p.m. and 5:30 p.m. on December 9, 2010. The district also supplied a copy of a second permit for another photo shoot at Alameda High School on the afternoon of December 10.
"The photos were not taken during the school day and no public funds were used to create the campaign flyer," Vital said. "SOS, or any other community organization, may apply for use of district facilities pursuant to the Civic Center Act and board policy."
When asked whether Measure A's opponents violated the law with the robocalls, Traiman said that mistakes made by volunteer campaign activists are "understandable," but said no state laws were broken by the Committee Against Measure A because the calls came from out of state. "Robocalls originating in California are prohibited," Traiman noted. "If they originate from outside the state, they are not. California regulators have no jurisdiction over calls which originate from out of state or else those calls would also be prohibited."
He said he paid for the calls independent of the campaign, supplying a reporter with a copy of a to-be-filed disclosure form that listed the calls as an independent expenditure. A recent call received by a reporter at her home included a message saying it had been paid for by Traiman, whereas earlier anti-A calls the reporter received at home did not say who paid for them.
State law prohibits campaigns from making mass phone calls without disclosing who paid for or authorized the calls. Robles-Wong's complaint alleges that Traiman, who is identified in the complaint as the secretary of the Committee Against Measure A, told participants in a February 22 public forum that he paid for the calls, "but that he had not included identifying information because he was being charged by the word and including the identifying information would have been too expensive."
According to the web site of Winning Calls, the Colorado-based firm that was used to make the calls, the company requires campaigns that use its services to sign a disclaimer saying they are conducting their campaign legally. An FPPC spokesperson said that while the department can't comment on a specific situation, as a general rule committees are prohibited from contracting with any phone bank vendor that doesn't disclose the information required by state law.
Violations of campaign finance laws carry penalties of up to $5,000 each, the FPPC spokesperson said. The state law that prohibits school districts from supplying funds, services, supplies or equipment to urge support or defeat of a ballot measure carries a fine of up to $1,000 and possible jail time for violators.
Committee Against Measure A spokesman David Howard filed a similar complaint against the school district in 2010, alleging it illegally used public funds to pay for mailers supporting the Measure E parcel tax campaign. The FPPC closed the case without charges, saying that while some of the language used in the mailer was "inflammatory," it didn't "fall squarely within the parameters of a prohibited mailing."
News Measure A Michael Robles-Wong Alameda Save Our Schools Fair Political Practices Commission Committee Against Measure A Leland Traiman Kirsten Vital Gray Harris Measure A Alameda Towne Center Oakland Raiders Otis Elementary School Alameda High School Winning Calls David Howard


Thumbsticks, as you can guess by their name, are designed to be held with the thumb hooked over the V of the handle and the handle should be at shoulder height or lower on the user. It can also been leant on with the elbow in the V with the V at chest height instead. This stick is bought in at 138cm approximately in height and finished with a metal ferrule. We can make it shorter for you before we send it out if you like, just add the crop service to your order and specify the height required (to the bottom of the V). This thumbstick is made from one single piece of chestnut wood and is very strong because of this. We supply various different models and our handmade selection is always worth a look.


Mamaison Residence Sulekova is one of the most popular places of accomodation in Bratislava. This is an apartment hotel with high level of luxury and very satisfied guests. The only minus might be the location which is a little walk from the Main Square of Bratislava, but the plus is that you have a beautiful view to the Castle from the hotel.


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Home/News/USA/Youth dance team injured in Waukesha Christmas parade chaos
Youth dance team injured in Waukesha Christmas parade chaos
Members of a youth dance team were reportedly among the victims injured when a crazed driver plowed through a Christmas parade in Wisconsin on Sunday night.
A witness who spoke to Fox 6 Now reporter Sam Kraemer estimated that up to 20 young girls with the Waukesha Xtreme Dance Team were struck by the red SUV at the annual celebration in the small city of Waukesha.
Corey Montiho, a School District of Waukesha board member, told the Milwaukee Journal Sentinel that his daughter was on a dance team that was struck by the driver.
"There were pom-poms and shoes and spilled hot chocolate everywhere," Montiho said.
The report didn't specify if Montiho was referring to the Waukesha Xtreme Dance Team — or potentially a separate youth squad.
"I had to go from one crumpled body to the other to find my daughter. My wife and two daughters were almost hit," the father told the newspaper.
"My family is safe but many are not. I held one little girl's head in my hand, she was seizing and she was bleeding out of her ears. I held her mother as she collapsed," he said.
In a Facebook post, the dance school addressed the parade mayhem.
A woman who lives on Main Street says she saw the SUV barrel through a dance team of girls between 9 and 15 years old.
She says the immediate reaction was silence, followed by screaming, running, checking on those injured. @fox6now
— Sam Kraemer (@SamKraemerTV) November 22, 2021
"Thank you for everyone who has reached out checking on the safety of Xtreme Dance Team members and their families," the school wrote.
"At this time, we ask that the media and those reaching out, give us and our families time and privacy to process the tragic events of this evening."
Police said during a press conference just hours after the carnage unfolded that at least 12 children were wounded in the chaos. At least 11 adults were also among the victims.
Multiple fatalities were also reported, but police did not immediately provide further information.
A person of interest was in custody and police have not ruled out terrorism as a motive, according to Police Chief Daniel Thompson.
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New Clutches by Peach Couture. Peach Couture is a registered trademark.
The perfect evening piece with a touch of glimmer and sparkles, is just the choice for you. This glitter box clutch has no sequins or crystals, but this glamour rectangle is all about the shine, courtesy of its colored, glitter fabric exterior. This shimmer hard case purse is finished with a silver snap closure. Inside, this mini handbag is a lined compartment with plenty of space to keep your small essentials - like lipstick, keys, tissues, and ID. Carry this evening purse as a clutch, or attach chain strap converting to shoulder bag. This flashy accessory is great for proms, cocktail party or wedding reception.
Actual colors may vary slightly from the color on your screen due to monitor color restrictions. If you have any questions,please email us freely,we will do our best to satisfy you.


Innovation can be viewed as the application of better solutions that meet new requirements, unarticulated needs, or existing market needs. This is accomplished through more effective products, processes, services, technologies, or ideas that are readily available to markets, governments and society. The term innovation can be defined as something original and more effective and, as a consequence, new, that "breaks into" the market or society.
Norman Ryder (1965) sheds light on the sociology of the discord between generations by suggesting that society "persists despite the mortality of its individual members, through processes of demographic metabolism and particularly the annual infusion of birth cohorts". He argues that generations may sometimes be a "threat to stability" but at the same time they represent "the opportunity for societal transformation". Ryder attempts to understand the dynamics at play between generations.
In kinship terminology, it is a structural term designating the parent-child relationship. It is also known as biogenesis, reproduction, or procreation in the biological sciences. The term is also often used synonymously with cohort in social science; under this formulation the term means "people within a delineated population who experience the same significant events within a given period of time". Generation in this sense of birth cohort, also known as a "social generation", is widely used in popular culture, and has been the basis for societal analysis. Serious analysis of generations began in the nineteenth century, emerging from an increasing awareness of the possibility of permanent social change and the idea of youthful rebellion against the established social order. Some analysts believe that a generation is one of the fundamental social categories in a society, while others view its importance as being overshadowed by other factors such as class, gender, race, education, and so on.
Social generations are cohorts of people who were born in the same date range and share similar cultural experiences. The idea of a social generation, in the sense that it is used today, gained currency in the 19th century. Prior to that the concept "generation" had generally referred to family relationships, not broader social groupings. In 1863, French lexicographer Emile Littré had defined a generation as, "all men living more or less at the same time".
For the purposes of this list, "Western world" can be taken to mean North America, Europe, South America, and Oceania. However, it should also be noted that many variations may exist within the regions, both geographically and culturally, which mean that the list is broadly indicative, but necessarily very general. For details see the individual articles.
The word generate comes from the Latin generāre, meaning "to beget". The word generation as a cohort in social science signifies the entire body of individuals born and living at about the same time, most of whom are approximately the same age and have similar ideas, problems, and attitudes (e.g., Beat Generation and Lost Generation).
The concept of a generation has a long history and can be found in ancient literature. However, there are also psychological and sociological dimensions in the sense of belonging and identity that can define a generation.


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A Kapellbrücke é uma ponte de madeira em Lucerna, Suíça. A Kapellbrücke (ponte da capela) foi erigida em 1365. Na ponta sul da ponte fica a Wasserturm (torre da água). Bem alto, nas traves de madeira encontram-se 112 pinturas datadas do início do século XVII e restauradas no princípio do século XX.
Da Kapellbrücke pode-se avistar a igreja de São Léger e São Maurício.

Um incêndio destruiu parte da ponte em 18 de Agosto de 1993. Foi reconstruida e reabriu em 14 de Abril de 1994.

Pontes cobertas da Suíça
Pontes pedonais da Suíça
Lucerna

redpajama_set_name: RedPajamaWikipedia


The Lemon Drop Top in Pink is a simple style shirt with a gathered feature across the bust line. An easy top to pair with jeans or shorts. Made from 100% linen sourced from deadstock fabric (unused fabrics from other designers), making it breathable and hard wearing.


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I am Trying to upload geojson file into laravel. But in the validation it is not working.

redpajama_set_name: RedPajamaStackExchange


Vancouver, February 12, 2013 – The BC Chamber welcomed the Throne Speech delivered by the Lieutenant Governor today as a measured series of commitments that look to balance the constraints placed on government revenue with the need to focus on certain key areas.
"We are particularly pleased to see that even with an election imminent the government has resisted the temptation to make grand promises and has focused on fiscal prudence and a measured approach that looks to long terms sustainability," said John Winter, President & CEO of the BC Chamber of Commerce.
The Throne Speech outlined several new commitments that reflect issues of concern to the business community. These measures include a renewed commitment to ensuring BC is the most friendly small business jurisdiction in Canada, a new structure to focus on the Asia Pacific and a focus on debt reduction and balanced budgets.


First Bank is located solely within the state of Kansas, County of Harvey, USA. Our trade area includes Harvey County and under certain circumstances neighboring counties including Sedgwick, Reno, Butler, McPherson and Marion. Applications outside our trade area will not be accepted.
Personal installment loans are available to qualified applicants for a variety of purposes, including: vehicle, boat, mobile home, vacation, home improvement, debt consolidation or other personal use. With a First Bank loan you're on your way to achieving your dreams!
First Bank is Harvey County's leading mortgage lender. Our expert real estate lending staff will assist you with first and second mortgage loans, lines of credit, bridge loans or construction loans.