text:
\section{Introduction\label{sec:intro}}
Young stars near the Sun are the targeting ground for direct imaging campaigns in search of hot massive planets.  Over the past two decades projects such as the Gemini NICI planet finding campaign, The Gemini Planet Imager Exoplanet Survey, the VLT/SPHERE survey for exoplanets, the Lyot Project Direct Imaging Survey of Substellar Companions, among others have examined the space around hundreds of young hot stars (\citealt{Chauvin2015}, \citealt{Vigan2020}, \citealt{Biller2013}, \citealt{Macintosh2008}, \citealt{Leconte2010}).  Interestingly the number of giant exoplanets --and even brown dwarfs -- at 10-100 AU separations from their host stars has been far fewer than hoped or predicted (\citealt{Nielsen2019}).

Even still there are now 37 systems listed on the NASA exoplanet archive\footnote{https://exoplanetarchive.ipac.caltech.edu/ As of April 23 2021 there are 4383 confirmed planets}  site as direct imaging discoveries of a planetary mass companion (using the 13M$_{Jup}$ definition) where the total mass of the system is larger than 0.1 $M_{\sun}$.  Among those 37 systems are the first multiple imaged exoplanet system  (HR8799bcde; \citealt{Marois2008,Marois2010}), systems with brown dwarf or extremely low mass star hosts (e.g. 2M1207b; \citealt{Chauvin04} and 2M0219b; \citealt{Artigau15}), and companions still accreting material (e.g. PDS70bc; \citealt{Muller2018}).  There is a large grey area in our understanding of how these systems formed given their largely model dependent masses and wide range of separations.  Competing pathways for the formation of these systems include the more traditional mechanisms of core accretion and disk instability for planets and cloud fragmentation for brown dwarfs.  The ability to differentiate between formation mechanism would aid in creating well defined classes of brown dwarfs versus exoplanets. While this is a well-trodden exercise (e.g. \citealt{Schlaufman2018}, \citealt{Brandt2014}, \citealt{Metchev08}, \citealt{Raghavan2010}, \citealt{Bowler2020b}) only tentative conclusions have been drawn on how to differentiate between a disk-formed object and a cloud fragmented object.

Meanwhile, numerous isolated low surface gravity brown dwarfs have been detected and confirmed to be members of 10 - 200 Myr moving groups like Tucana Horologium, $\beta$ Pictoris, and AB Doradus (e.g. \citealt{Gagne18, Gagne15}, \citealt{Best2017}, \citealt{Faherty13, Faherty16}, \citealt{Liu13}, \citealt{Zhang2021}, \citealt{Schneider2018}).  These sources are distinctly different from field brown dwarfs in their spectral morphology, colors, and absolute magnitudes (\citealt{Faherty16}, \citealt{Liu16}).  Studies of their photometric and spectral variability allude to complex atmospheres with strong weather related phenomena (e.g \citealt{Metchev2015}, \citealt{Vos2020}).  Given their young ages and low temperatures, many have masses that overlap with those of directly imaged planetary mass companions at just above and below 13 M$_{Jup}$ (see for example \citealt{Gagne17TWHya}).

In many ways the populations of giant exoplanets and isolated young brown dwarfs are identical. There are, at present, no defined spectral characteristics imprinted on a source that indicate which formation mechanism was responsible for its creation. Studies have shown that planetary mass companions and isolated planetary mass sources share spectral morphology as well as positions on color-magnitude diagrams (e.g. \citealt{Faherty16}, \citealt{Gagne15}, \citealt{Liu16}).  They have identical weather related phenomena (e.g. \citealt{Vos2019}, \citealt{Biller2018}, \citealt{Zhou2016}), temperatures, and gravities; therefore, it benefits both populations if they are studied in tandem.

In this paper we report the discovery of a new system containing a planetary mass companion.  Using the Backyard Worlds: Planet 9 citizen science project, we found that the young K0 star BD+60 1417 was co-moving with a late-type L dwarf with hallmark signatures of youth.  In section~\ref{sec:Discovery} we discuss the discovery of the system, in section~\ref{sec:newdata} we detail new data taken on both the primary and the secondary, and in section~\ref{sec:components} we provide a detailed discussion on each component. Section~\ref{sec:W1243spectra} discusses the spectrum of W1243 and section~\ref{sec:chancealign} evaluates the probability of chance alignment for the system. Section~\ref{sec:CMD} evaluates W1243 on color-magnitude diagrams, and section~\ref{sec:age} re-evaluates the age of the primary BD+60 1417. Section~\ref{sec:fundamentals} details how fundamental parameters were calculated for each component and section~\ref{sec:characteristics} places the BD+60 1417 system in context with other planetary mass companion systems.  Section~\ref{sec:discussion} is a discussion on potential formation mechanisms for this system.  Conclusions are presented in section~\ref{sec:conclusions}.

\begin{figure*}
\begin{center}
\includegraphics[width=0.8\linewidth]{Finder.pdf}
\caption{The finder chart for the BD+60 1417 and W1243+6001 system taken from the WiseView website (\citealt{Caselden18}).   To see the animated motion between available $WISE$ epochs visit the URL http://byw.tools/wiseview-v2 and use coordinates RA,DEC=190.88751026191, 60.01435471736.}
\label{fig:finder}
\end{center}
\end{figure*}

\section{Discovery\label{sec:Discovery}}
The Backyard Worlds: Planet 9 citizen science project (Backyard Worlds for short) has been operational since February 2017. The scientific goal of the project is to complete the census of the solar neighborhood (including the solar system, e.g. Planet 9) with objects that are detectable primarily at mid infrared wavelengths and that were missed by previous searches (see \citealt{Kuchner17}, \citealt{Debes19}, \citealt{Faherty2020}, \citealt{Bardalez2020}, \citealt{Meisner2020}, \citealt{Schneider2020}, \citealt{Kirkpatrick2021}, \citealt{Rothermich2021}, \citealt{Jalowiczor2021}). Backyard Worlds utilizes multiple epochs of NASA's Wide-field Infrared Survey Explorer ($WISE$) mission at both W1 ($\sim$3.4 $\mu$m) and W2 ($\sim$4.6$\mu$m) wavelengths. Project participants are asked to blink between four unWISE images (see \citealt{Meisner17b}) where the time-span between the first and last image is $\sim$ 4.5 years. Given this time baseline, objects of significant motion (e.g. $>$ 200\,mas\,yr$^{-1}$) are relatively easy to visually identify.

The BackyardWorlds.org\footnote{http://www.backyardworlds.org} website hosted by Zooniverse provides multiple avenues for reporting a proper motion candidate of scientific interest to the research team (see \citealt{Kuchner17} for details).  Since the program began a significant number of Backyard Worlds users have become heavily involved with the research aspect of the project and have earned the title ``super users".  These participants attend weekly calls with the science team, have increased contact via email and are much more engaged than a casual online subscriber to the project.  With the increased mentorship from the research team, the super users tend to take on more complex searches outside of the website itself and as such have well tuned eyes to detecting more obscure targets.  In fact one citizen scientist, Dan Caselden--also co-author on this work--, has developed a tool called WiseView (\citealt{Caselden18}) which allows users to flip through available $WISE$ images without the image subtraction used on the Zooniverse site.  WiseView has an array of functionality (changing the image stretch, zooming in and out, overlaying Gaia astrometry, etc.) which compliments the Zooniverse site but also greatly aids in complex searches.

For this discovery, citizen scientist J{\"o}rg Sch{\"u}mann was searching through subsets of images in WiseView and identified a faint comoving system. In this case, the secondary was both in the halo of the primary and along one of its diffraction spikes therefore it was easily missed by sophisticated catalog searches. Visual inspection was critical to the discovery of the secondary and it is an exemplary case of the power of the Backyard Worlds project.

J{\"o}rg used the Google form as well as the Backyard Worlds email distribution list to alert researchers to the discovery.  On 10 April 2018, the motion of W1243 was vetted by the research team and added to the high priority follow-up target list with a note that it was potentially co-moving with BD+60 1417. Figure~\ref{fig:finder} shows a screenshot from the WiseView website (\citealt{Caselden18}) which was used to identify and confirm the system.

\section{New Data\label{sec:newdata}}
To characterize this potential co-moving system, we followed up on both the primary and secondary with optical and infrared spectrographs (respectively).

\subsection{Optical Spectroscopy}
On the night of 10 January 2021 (UT) we observed the primary BD+60 1417 using the Kast optical spectrograph on the Shane 3m telescope at Lick observatory. Conditions were variable with some wind and cirrus clouds. The average seeing at the time of observations was $\sim$2$\arcsec$. We observed the system using the 2$\arcsec$ slit with one 60s exposure in the red channel (6300 - 9000 $\AA$).  The A0V telluric star 81 UMa was observed for absorption calibration and the flux standard Hiltner~600 was observed during the night for flux calibration \citep{hamuy1994}. We also obtained flat field and He, Hg-A, Ne, and Spare Ar lamps at the start of the night for pixel response and wavelength calibration. Data were reduced using the \texttt{kastredux} package\footnote{\url{https://github.com/aburgasser/kastredux}} using default settings.

\begin{figure*}
\begin{center}
\includegraphics[width=0.8\linewidth]{SpeX-New.pdf}
\caption{The SpeX Prism spectrum for W1243 normalized over the $J$ band with prominent features labeled.}
\label{fig:spectrasecondary}
\end{center}
\end{figure*}

\subsection{SpeX Prism Spectroscopy}
We observed the secondary W1243 on two separate nights using the SpeX spectrograph on NASA's IRTF telescope.  The first data were taken on the night of 04 January 2021 (UT) under good conditions with minimal cloud coverage and the second on 31 January 2021 (UT) under varying cloud conditions.  The data were taken in prism mode using the 0.8$\arcsec$ slit to achieve a resolving power of $\sim$100 - 500 over the 0.8 - 2.5$\mu$m coverage. We observed the object on two separate nights to get ample signal as the first spectrum was taken close to dusk and therefore we could not integrate for our desired amount of time.  On 04 January we obtained 8 AB nods using 180s exposures on the target and then acquired the A0 star HD 99966 for telluric correction using 0.1s exposures and 20 AB nods.  On 31 January we obtained 28 AB nods using 180s exposures on the target and then acquired the A0 star HD 116405 for telluric correction using 0.1s exposures and 20 AB nods.  All data were reduced using the \texttt{Spextool} package (\citealt{Cushing04}) with telluric correction and flux calibration of the A0 stars following the technique described in \citet{Vacca03}.

\begin{figure*}
\begin{center}
\includegraphics[width=0.8\linewidth]{IsolatedLComparison2.pdf}
\caption{The SpeX Prism spectra for W1243 as compared to data on the field age optical L7 standard DENIS 0205, and the $\sim$ 150 Myr AB Doradus L dwarfs 2M2244 and W0047.  Under the name of each object we list the 2MASS ($J$-$K_{s}$) color. Relevant spectral features are labeled.}
\label{fig:ComparisonPanel}
\end{center}
\end{figure*}

\section{Details on the components\label{sec:components}}
\subsection{Primary}
BD+60 1417 is a well known nearby star (e.g. \citealt{Tycho}).  Given the notable X-ray detection in \citet{Rosat} and the Li I absorption for this source it was an attractive target for numerous nearby young star studies (e.g., \citealt{Wichmann2003}).  \citet{Wichmann2003} estimate an age for the star of 50 - 150 Myr based on its X-ray flux compared to equivalent Pleiades sources. Due to its relatively young age, nearby distance ($\sim$45\,pc) and K0 spectral type (solar type-esque), BD+60 1417 was a target of choice for the Gemini deep planet survey (\citealt{Lafreniere2007}), the Palomar/Keck adaptive optics survey of young solar analogs (\citealt{Metchev2009}) as well as other planet finding programs (e.g. \citealt{Heinze2010}).  There was an object of interest imaged around BD+60 1417 by \citet{Lafreniere2007} and \citet{Heinze2010} but it was ruled out as a background object due to a mismatched proper motion.  As such BD+60 1417 remained a young K0 star with no directly imaged exoplanet discovered to date and became a statistical null-detection point for analysis papers looking at the frequency of giant planets (e.g. \citealt{Nielsen2010}, \citealt{Vigan2017}, \citealt{Meshkat2017}).

\begin{figure}[!ht]
\begin{center}
$\begin{array}{cc}

\includegraphics[width=3.1in]{Comparison2.pdf}&\\
\includegraphics[width=3.1in]{OtherYoungL2.pdf} \\
\includegraphics[width=3.1in]{HR8799Comparison.pdf} \\
\end{array}$
\end{center}
\caption{ The SpeX prism spectrum of W1243 normalized band by band and compared to various isolated young L dwarfs and planetary mass companions.  Top: Compared to DENIS 0205, 2M2244, and W0047.  Middle: Compared to 2M1207b, PSO318, W1147, and W1119. Bottom: Compared to the HR8799bcde planets. Error bars are shown for the HR8799 companions given their significance against the data. }
\label{fig:spectra-bands}
\end{figure}

\subsection{Secondary\label{sec:secondary}}
CWISER  J124332.12+600126.2 (W1243) is detected in both the 2MASS Survey Point Source Reject (using a reliability limit $>$ 20\%) and CatWISE2020 reject tables (\citealt{Cutri03}, \citealt{Catwise2020}). For 2MASS there was a reported $K_{s}$ photometric point while $J$ and $H$ bands were limits only.  W1243 falls in a part of the sky observed by Pan-STARRS although only a detection in $y$ band is reported. Despite being in the CatWISE2020 reject table, W1243 is well detected at both W1 and W2 bands.  Looking at the flags, it is noted as being near a diffraction spike and near the halo of a bright star in  both W1 and W2 bands.  Proper motion component values for W1243 are listed in the CatWISE2020 reject table.  While the primary has been looked over by numerous surveys for a close-in companion with a comparable or lower temperature to W1243, no survey looked far enough from the primary to detect this object.

\section{Analysis of the NIR spectrum of W1243\label{sec:W1243spectra}}
The SpeX prism spectrum of W1243 is shown in Figure~\ref{fig:spectrasecondary} normalized over the peak of the $J$ band with pertinent atomic and molecular features labeled. The source shows strong H$_{2}$O and CO absorption as well as FeH, and KI features.  The distribution of flux across the normalized spectrum visually indicates a very red late-type L dwarf.  We used the 2MASS filter profiles overlaid on the SpeX spectrum to compute synthetic magnitudes for this source in $J$ and $H$.  We calibrated using the synthetic ($J$- $H$) and ($J$-$K_{s}$) colors along with the 2MASS $K_{s}$ detection and list the photometry in Table~\ref{tab:param}. We find the ($J$-$K_{s}$) color of 2.72 makes W1243 one of the reddest known brown dwarfs characterized to date (see e.g. \citealt{Marocco2014} and \citealt{Liu13} for details on ULAS J222711-004547 and PSO 318 the two record holders for reddest isolated brown dwarfs).

Figure ~\ref{fig:ComparisonPanel} shows W1243 compared to three late-type L dwarfs normalized over the peak of the $J$ band.  We compare W1243 to the $\sim$150 Myr AB Doradus moving group objects WISEP J004701.06+680352.1 (W0047, \citealt{Gizis2015}) and 2MASS J22443167+2043433 (2M2244, \citealt{Faherty16}, \citealt{Vos2018}) as well as the field source and optical L7 standard DENIS-P J0205.4-1159 (DENIS 0205, \citealt{Kirkpatrick99}).  Under each object name we also denote the 2MASS ($J$-$K$) color.  The spectrum of W1243 is substantially redder than DENIS 0205.  It most closely resembles W0047 in its spectral morphology although it also appears slightly redder than this source.

W0047 was evaluated by \citet{Gizis2015} to be an infrared L7 with signatures of a low surface gravity. \citet{Faherty16} evaluated a sample of over 150 low surface gravity M and L dwarfs and determined that both W0047 and 2M2244 should be considered L6 - L8$\gamma$ prototypes where the $\gamma$ designation indicates a very low surface gravity (see \citealt{Kirkpatrick2005}, \citealt{Cruz09}, \citealt{Gagne15}).

Evaluating the exact spectral subtype of a red L dwarf against the array of known objects can be difficult given the significant color difference across the spectrum.  As recommended by \citet{Cruz18} we also performed a band by band normalization across $J$, $H$, and $K_{s}$ so we could compare to other field, young and planetary mass objects -- the latter of which only have spectra taken band by band.

The top panel of Figure~\ref{fig:spectra-bands} shows the band by band normalization of W1243 as compared to DENIS 0205, 2M2244, and W0047.  With the color term minimized, it is far easier to compare the spectral morphology.  Most notably, compared to the field source DENIS 0205, W1243 has a much sharper $H$ band peak which is a hallmark signature of low surface gravity L dwarfs (e.g. \citealt{Allers13}).  The $K$ band of W1243 is also enhanced compared to DENIS 0205, a feature seen in other low gravity L dwarfs and attributed to a change in collision induced $H_{2}$ absorption (e.g. \citealt{Saumon2012}).  The depth of the NaI and KI alkali lines in the $J$ band is also a low surface gravity diagnostic.  \citet{Allers13} and \citet{Martin17} evaluated the equivalent width values from medium resolution SpeX or NIRSPEC (respectively) data to determine trends between gravity and alkali depths.  In general, younger sources show narrow, shallow lines  compared to older field objects.  The low resolution SpeX prism data hint that the KI lines are shallower for W1243 than DENIS 0205 and far more similar to W0047 or 2M2244.

We also investigated the recommended indices from \citet{Allers13} to evaluate the gravity class for W1243.  That work was calibrated on sources warmer than W1243 (L5 or earlier) therefore only the $H$- band continuum index can be reliably used.  Using that we find this source would be classified as a  L6$\gamma$ consistent with our analysis.

Based on these spectral comparisons we determine that W1243 should be considered a very low surface gravity late-type L dwarf and we assign a spectral type of L6 - L8$\gamma$ mimicking the conclusions for both W0047 and 2M2244 which are members of the $\sim$150 Myr AB Doradus moving group.

We expanded our analysis to include other L6 - L8$\gamma$ objects which are in younger moving groups.  In the middle panel of Figure~\ref{fig:spectra-bands} we do a band by band comparison of W1243 to the candidate $\sim$10 Myr TW Hya association L dwarfs WISEA J114724.10-204021.3 (W1147; \citealt{Schneider2016}) and WISEA J111932.43-113747.7 (\citealt{Kellogg2016}) as well as the $\sim$24 Myr $\beta$ Pictoris moving group member PSO J318.5338-22.8603 (PSO 318; \citealt{Liu13}).  The spectra for W1147 and W1119 were obtained from FIRE Echelle (from \citealt{Faherty16}) and are  higher resolution than the prism data (R$\sim$3000-5000 compared to R$\sim$100-500 for prism). Moreover, they are stitched together order by order which might introduce shape anomalies across a band (e.g. W1147 K band). In this comparison we find that W1243 shows similarities to all three of the young sources with W1147 showing more of a triangular H band and W1119 and PSO 318 showing sharper $J$ band peaks.  However it is well known that even low surface gravity L dwarfs in the same association with the same estimated temperatures can show a range in their spectral features (e.g., 2M0355, CD35 -2722B from AB Doradus moving group \citealt{Allers13}).  Consequently we can not conclude whether W1243 is better matched by an AB Doradus moving group age of 149$^{+51}_{-19}$ {Myr} or a TW Hya or $\beta$ Pictoris younger age of 10$\pm$3, $<$24$\pm$3 Myr respectively (\citealt{Bell2015}).  Based on these comparisons we can confirm that W1243 rivals the low surface gravity features of even the youngest late-type L dwarfs confirmed in moving groups and we estimate an age of $\lesssim$ 150 Myr for our source.

Given the discovery that W1243 was co-moving with a young K0 star, we also wanted to compare this source to known planetary mass companions. The bottom spectrum in the middle panel of Figure~\ref{fig:spectra-bands} shows the planetary mass companion 2MASSWJ 1207334-393254b (2M1207b; \citealt{Chauvin2004}) using the Sinfoni spectrum from \citet{Patience2010}. 2M1207b is classified as an L7 and is co-moving with an M8 dwarf in the $\sim$10 Myr TW Hya association. Compared to W1243, we find that 2M1207b has a sharper shape to the $H$ band but similar CO absorption in $K$ band.

In the bottom panel of Figure~\ref{fig:spectra-bands} we show a band by band comparison to the HR8799 planets (HR8799 bcde; \citealt{Marois2008,Marois2010}). We have pieced together the spectra of each source from Keck, Sphere, and/or GPI data, much of which was taken over multiple observing runs and extracted using different methods (\citealt{Barman2011,Barman2015}, \citealt{Greenbaum2018}, \citealt{Zurlo2016}). The HR8799 planets do not have confident spectral subtypes assigned but are classified as L type objects co-moving with an A5 star thought to be 40$\pm$5 Myr.    Compared to the HR8799 planets we find similarities and differences to each object depending on the band we examine.  The $J$ band data for both HR8799d and e match within uncertainties showing similar depths in $H_{2}$O absorption. The shape of the $H$ band for HR8799c matches that of W1243 as well.  HR8799b appears to have a much sharper triangular H-band shape than W1243 (also much sharper than any of its planetary siblings) and the data for HR8799e in both GPI and SPHERE hint at a similar sharp shape in that object.  The morphology of the $K$ band for each planet shows differing structure and we find the strongest similarities to HR8799c which appears to match most closely.

From this comparison we can conclude that W1243 resembles both the isolated young L dwarfs as well as the young planetary mass companions with no obvious spectral differences that would differentiate it as having formed with one mechanism or another.

\section{Evaluating the probability of Companionship for the System\label{sec:chancealign}}
BD+60 1417 has a well measured parallax (22.2437 $\pm$ 0.0135 mas) and proper motion ([$\mu_{\alpha}$, $\mu_{\delta}$] = [-126.401$\pm$0.013, -64.141$\pm$0.015]\,mas\,yr$^{-1}$) in Gaia's eDR3 catalog (\citealt{eDR32020}). W1243 has proper motion components reported in the CatWISE2020 catalog ([$\mu_{\alpha}$,$\mu_{\delta}$] = [-133$\pm$8,-55$\pm$8]\,mas\,yr$^{-1}$; \citealt{Catwise2020}).  We estimate a photometric distance to W1243 using the $K_{s}$ band young L dwarf relation and a conservative ten percent uncertainty based on the parallax sample of late-type L dwarfs (44$\pm$4\,pc; \citealt{Faherty16}). We find that the $\mu_{\alpha}$ proper motion component and distance match well within 1$\sigma$ and the $\mu_{\delta}$ component matches just beyond 1$\sigma$.  We evaluated the probability of chance alignment in two ways.

We examined the Gaia Catalog of Nearby Stars (GCNS; \citealt{GCNS}) -- which contains 331312 stars within 100pc -- and found there were 1602 objects with proper motion components that matched W1243 within 2$\sigma$ or 0.48\% of the catalog.  We then restricted that match to only sources that matched the photometric distance of W1243 within 20\% and were left with 159 objects or 0.05\% of the catalog.  Looking at the distribution of matches we found only one of those 159 objects -- BD+60 1417 at a 37$\arcsec$ physical separation-- was within 1 degree of W1243.  The next closest object was 1.5 degrees from our target making a co-moving kinematic match unreasonable.  \citet{GCNS} states that they are complete down to M9 dwarfs at 92\% confidence therefore this should be a robust examination of the spatial and kinematic distribution of nearby stars that might have matched W1243.

For a fully quantitative approach, we used a modified version of the BANYAN {$\Sigma$} code (\citealt{Gagne18}) called \texttt{common\_pm\_banyan} to evaluate co-evality.  This code -- described in \citet{BanyanComover} -- uses the sky position, proper motion, parallax and heliocentric radial velocity of a host star (with their respective measurement errors), and compares it to the observables of a potential companion (with their respective measurement errors) in order to determine a probability that the two stars are co-moving and thus gravitationally bound. When all kinematic observables are provided, a single spatial-kinematic model is built, consisting of a single 6-dimensional multivariate Gaussian in Galactic coordinates (XYZ) and space velocities (UVW). The observables of the potential companion are then compared to this model and the field-stars model of \citet{Gagne18} --a 10-component multivariate Gaussian model appropriate only within a few hundreds of parsecs of the Sun-- with Bayes' theorem by marginalizing over any missing kinematic observables of the companion star with the analytical integral solutions also detailed in \citet{Gagne18}. After inputting all values for both BD+60 1417 and W1243, the \texttt{common\_pm\_banyan} code yielded a 0\% probability of chance alignment for the system confirming all other approaches to determine its co-moving nature. Given our high level of confidence in the co-moving nature of this system we refer to the secondary as BD+60 1417B from here-on.

\begin{figure}[!ht]
\begin{center}$
\begin{array}{cc}

\includegraphics[width=3.1in]{BEST-CMD3.pdf}&\\
\includegraphics[width=3.1in]{BEST-CMD1.pdf} \\
\includegraphics[width=3.1in]{BEST-CMD2.pdf} \\
\end{array}$
\end{center}
\caption{ The color-magnitude diagrams for field sources, low gravity brown dwarfs and directly imaged planetary mass companions color coded by spectral subtype. Top: M$_{J}$ (2MASS) vs. (J-W2) Middle: M$_{J}$ (MKO) vs. (J-K) (MKO) Bottom: M$_{H}$ (MKO) vs. (H-L) (MKO).  In the absence of L band photometry for brown dwarfs we used the relation in \citealt{Faherty16} to convert $WISE$ $W1$ photometry to L (MKO).}
\label{fig:CMD-Young}
\end{figure}

\begin{figure*}
\begin{center}
\includegraphics[width=0.8\linewidth]{Kast-Spectrum.eps}
\caption{The Kast optical spectrum of BD+60 1417 obtained for this work. In the inset we show the H$\alpha$ and Li features.  The flux is normalized over the peak of the full range.  Overplotted is a K0 star from the Sloan Digital Sky Survey in red.}
\label{fig:spectraprimary}
\end{center}
\end{figure*}

\section{BD+60 1417B on Color-Magnitude diagrams\label{sec:CMD}}
Using the parallax of the primary we can evaluate the position of BD+60 1417B on color-magnitude diagrams (CMDs) and compare/contrast it to other young L dwarfs and planetary mass companions.  The near- and mid-infrared CMDs have proven powerful diagnostic tools for deciphering the physical characteristics of young brown dwarfs (e.g. \citealt{Faherty16} and \citealt{Liu16}).  Recent studies have shown that low surface gravity brown dwarfs have redder near- to mid-infrared colors and fainter absolute magnitudes when compared to the sequence of field sources.  Young, warm, planetary mass companions share this observed feature, affirming that the two populations should be studied in tandem.

Figure~\ref{fig:CMD-Young} shows three relevant panels of CMDs across near to mid infrared bands that are inclusive of the majority of planetary mass companions and isolated brown dwarfs with a parallax and relevant photometric measurements.  The (J-W2) CMD is inclusive of brown dwarfs only but allows us to put BD+60 1417B in context against all field and low gravity brown dwarfs.  Direct imaging studies of companions primarily observe with MKO $JHKL$ bands, so we also show the MKO (J-K) and MKO (H-L) CMDs. The majority of field and low gravity brown dwarfs have near infrared MKO band magnitudes but lack $L$ band photometry.  As such, in the (H-L) plot, we converted the W1 magnitude for field and low gravity brown dwarfs into L band magnitudes using the polynomial relation from \citet{Faherty16}.  Moreover, for BD+60 1417B we obtained synthetic MKO $J$ and $K$ photometry from the SpeX spectrum. The parallax sample was drawn from recent compilations by \citet{Best2020}, \citet{Kirkpatrick2021}, and \citet{Smart2019}. In each panel objects are color-coded by their spectral subtype, low surface gravity dwarfs (designated as $\gamma$ or VL-G only -- see \citealt{Faherty16}) are plotted as filled squares and planetary mass companions are plotted as filled five-point stars.  We collected planetary mass companion photometry from the compilation of \citet{Best2020}, as well as the NASA Exoplanet Archive\footnote{https://exoplanetarchive.ipac.caltech.edu/}.

As can be seen in each plot, the low gravity brown dwarfs differentiate themselves as redder and simultaneously fainter than field objects of the same subclass.  As spectral subtypes increase across the L dwarfs, the low gravity objects deviate significantly from the field sample.  BD+60 1417B shares a similar position on the (J-W2) and (J-K) (MKO) CMDs as W0047 and PSO318.  As stated above, both sources are confirmed members of nearby moving groups with ages of $\sim$150 Myr and $\sim$24 Myr respectively.  Both sources have been noted as having particularly cloudy atmospheres with weather related variability (e.g. \citealt{Vos2018, Vos2019}, \citealt{Lew2016}).  BD+60 1417B also shares a spatial locus on the MKO (J-K) and (H-L) diagrams with planetary mass companions such as VHS1256B and 2M1207b.  VHS1256B was a recent target in a spectral monitoring campaign and was found to have strong near-infrared variability in HST/WFC3/G141 light curves (\citealt{Bowler2020}). \citet{Zhou2020} found the spectral variability of VHS1256B was consistent with predictions from partly cloudy models, suggesting that heterogeneous clouds are the dominant source of the observed modulations. The extreme positions of young, late-type objects on color-magnitude diagrams may be a strong signature of a particularly cloudy, active atmosphere (e.g. \citealt{Barman2011}, \citealt{Faherty12, Faherty16}, \citealt{Bowler2013}).  From the position of BD+60 1417B on each color-magnitude diagram we can conclude it is an excellent candidate for spectral and photometric variability studies.

\section{The Age of BD+60 1417\label{sec:age}}
As stated above, BD+60 1417 was categorized as a young star by \citet{Wichmann2003} and given an age range of 50 - 150 Myr.  In this section we revisit the parameters of the primary and re-evaluate the age using new indicators of youth from recent observations.

\subsection{Age Indications from Li I absorption}
We obtained optical spectral data on the primary BD+60 1417 to investigate relevant molecular features.  Figure ~\ref{fig:spectraprimary} shows the 6000 - 9000\AA~spectrum with an inset of the wavelength regime for H$\alpha$ and Li I.  For comparison, we have overplotted the K0 star SDSS J012703.04+383611.1 that was spectroscopically characterized with the Sloan Digital Sky Survey.  There looks to be a slight slope in our Kast spectrum compared to the SDSS data, potentially due to imperfections in the reduction. However we find comparable features confirming the K0 spectral subtype. In \citet{Wichmann2003}, the authors reported a Li I measurement corrected for Fe I of 96 m\AA.  We can not confirm that value with our data given our resolution of $\sim$6000\AA~means the feature is too contaminated by Fe I.   Using the measured value of Li I absorption from \citet{Wichmann2003} we can compare to values for other young stars near the Sun.  Similar to the conclusions of \citet{Wichmann2003} we find that BD+60 1417 is consistent with values for the Pleiades indicating that this source is likely of a similar age range ($\sim$110 - 125 Myr).

\subsection{Age Indications from Gyrochronology}
BD+60 1417 was observed by NASA's Transiting Exoplanet Survey Satellite (TESS; \citealt{TESS}) telescope in sectors 15, 21, and 22 in both 30 minute and 2 minute cadences. From the full frame images we generated light curves for each sector using simple aperture photometry and background subtraction. We present these light curves in Figure~\ref{fig:lightcurves_ls}, along with the results of running each through a Lomb-Scargle periodogram (\citealt{lomb_1976}, \citealt{scargle_1982}). The periodogram shows a strong peak at around 7.5 days in both sector 15 and 21, and at the half harmonic of 3.7 days in sector 21 and 22. The morphology of the light curve changes between sectors; in sector 15 the shape is a simple sinuosoid, while in sectors 21 and 22 it is a double dip pattern. Between sectors 21 and 22 the shape of the double dip changes between cycles. Likely we are seeing the evolution of sunspots across the surface of the star.  Averaging across sectors we report a rotation period of 7.50 $\pm$ 0.86 days.

We put BD+60 1417 on a color-period plot in Figure~\ref{fig:color_period}. To provide context we include rotation periods from the gyrochronology benchmark clusters the Pleiades (\citealt{rebull_2016_pleiades}) and Praesepe (\citealt{douglas2017}) at $\sim$120 Myr and 650 Myr respectively. For its color BD+60 1417 is rotating faster than the majority of Praesepe objects, and slightly slower than the majority of Pleiades objects.  We also report an average amplitude variation across the three sectors of 2.23\%. While variation for a single star can depend on various factors such as inclination and activity cycle, this is consistent with the amplitude variation of a $\sim$100 Myr object (e.g. \citealt{morris_2020}). Conservatively, we find that a rotation period analysis indicates an age range of 100-650 Myr for BD+60 1417.

\begin{figure}[ht!]
\begin{center}
\includegraphics[width=0.5\linewidth]{Gyro.png}
\caption{The TESS light curve in sectors 15, 21, and 22 as well as the power spectrum of the Lomb Scargle periodogram for these data.}
\label{fig:lightcurves_ls}
\end{center}
\end{figure}

\begin{figure}[ht!]
\begin{center}
\includegraphics[width=0.8\linewidth]{bd+60_1417_color_period.png}
\caption{The color-period plot for BD+60 1417 (five point star) in context with the 650 Myr Praesepe (purple filled circles) and 120 Myr Pleiades (blue filled circles) clusters. }
\label{fig:color_period}
\end{center}
\end{figure}

\subsection{Age Indications from Color-Color and Color-Magnitude Diagrams}
Pulling together all of the catalog detections of BD+60 1417 we can look at where it stands on color-color and color-magnitude diagrams in order to re-assess the extent of its youth.  Using the Gaia parallax and photometry we can compare BD+60 1417 to the 150pc sample of young stars from \citet{GagneFaherty2018}.  The top panel of Figure~\ref{fig:CMDandCC} shows the empirical isochrones from \citet{GagneFaherty2018} for objects across the color-magnitude diagram at ages of 10-15 Myr, 23 Myr, 45 Myr, 110 Myr, and 600 Myr with a zoom-in on the position of BD+60 1417 as an inset.  As one goes from younger to older ages for the main sequence, the isochrones shift to fainter absolute magnitudes.  BD+60 1417 is situated at a CMD position where the 45 Myr, 110 Myr, and 600 Myr isochrones are difficult to distinguish.  We can conclude that it does not share properties with 23Myr
sources and the inset shows that it is most consistent with the 110 Myr sequence.

\begin{figure}[!ht]
\begin{center}$
\begin{array}{cc}

\includegraphics[width=0.6\linewidth]{BEST-CMD-Gaia.pdf}\\
\includegraphics[width=0.6\linewidth]{bd_60_1417_uv.png}\\
\end{array}$
\end{center}
\caption{ {\bf Top:} The Gaia color-magnitude diagram for both the field sample and the 150pc sample of young stars discussed in \citet{GagneFaherty2018}. We have zoomed in on the position of BD+60 1417 as an inset to show the closest isochrone. {\bf Bottom:} GALEX to Gaia (NUV-G) color vs Gaia (G-$G_{RP}$) for both the field sample and the 150pc sample of 10-150 Myr young stars from \citet{GagneFaherty2018}.  The position of BD+60 1417 is marked by a red five-point star.}
\label{fig:CMDandCC}
\end{figure}

Combining the ultraviolet flux detected from BD+60 1417 from the Galaxy Evolution Explorer (GALEX) survey we can use the (NUV-G) color as a proxy for enhanced magnetic activity which has also been shown to scale with younger ages (e.g. \citealt{Gagne2020}, \citealt{GagneVolans}).  The bottom panel of Figure~\ref{fig:CMDandCC} shows the field sequence as black unfilled circles and the young sample (10 - 150 Myr group members) as purple upward facing triangles.  BD+60 1417 falls just outside the tighter field sequence.  At this temperature (or (G-G$_{RP}$) color) the NUV is not very diagnostic of youth however it is safe to say that the position of BD+60 1417 is consistent with a 10-150 Myr source.

Similarly, we can compare the X-ray luminosity for our source as calculated using the ROSAT detection (\citealt{Rosat}) to the sample of young stars near the Sun.   With a log (L$_{x}$)$\sim$ 29 (erg s$^{-1}$) BD+60 1417 is consistent with a star of age $\sim$150 Myr or younger (see for example \citealt{Kastner2003}, \citealt{Malo2014}, \citealt{Gagne2020}).

Putting all these primary star diagnostics together with our assesment of the secondary, we decide to maintain the 50 - 150 Myr age range given by \citet{Wichmann2003} as our re-analysis is consistent with this value.

\begin{figure*}
\begin{center}
\includegraphics[width=1.0\linewidth]{BEST-FINAL-BE.pdf}
\caption{Mass ratio versus separation for a collection of companions from stellar to planetary.  We have color coded the exoplanet detections (as defined by the exoplanet archive) by the detection method of the source.}
\label{fig:Mass-Sep}
\end{center}
\end{figure*}

\section{Fundamental Parameters\label{sec:fundamentals}}
In order to evaluate the physical characteristics of the BD+60 1417 system, we needed to obtain fundamental parameters of each component, such as mass, luminosity, radius, etc.

For the primary, we examined the range of values cited for BD+60 1417 in the literature (T$_{eff}$ for instance is listed as 5142 K in \citealt{Starhorse2018}, 4981 K in \citealt{GaiaDR2}, 5198 K in \citealt{Miller2015}, and 4993$\pm$124 K in \citealt{TIC2018}).  There is clear variety in values listed.  For the analysis that follows we chose to use the fundamental parameters listed in the TESS Input Catalog (TIC; \citealt{TIC2018}) because they present mass, radius, log(g), L$_{bol}$ uniformly with uncertainties while other catalogs limit to just a few parameters.   We note that the TIC does not necessarily take into account the youth of this source and therefore the uncertainties and the values such as the radius may be underestimated.  Given that we wanted to understand the mass ratio of the system in context with other wide co-movers, we choose to use the mass published in  \citet{Metchev2009} which did take into account the youth of the source.  All parameters for BD+60 1417 can be found in Table~\ref{tab:param}.

We used the $v\sin(i)$, radius, and rotation rate for BD+60 1417 to infer its viewing inclination.  Assuming rigid body rotation, the $\sin(i)$ distribution can be calculated by:
\begin{equation}
    \sin(i) = \frac{P v\sin(i)}{2 \pi R}
\end{equation}
where $P$ is the rotation period, and $R$ is the stellar radius. We use Monte Carlo analysis to determine the $\sin (i)$ and inclination distributions, using Gaussian distributions for $v \sin (i)$, period and radius. Monte Carlo analysis is especially well-suited to this computation as it can take into account a variety of distributions for $v\sin(i)$, $P$ and $R$ \citep[e.g.][]{Vos2017, Vos2020}, although we assume Gaussian distributions in our case.   \citet{Wichmann2003} report the $v\sin (i)$ of BD+60 1417 as $11$\,km\,s$^{-1}$, citing an approximate error for their entire sample of 10\%. However, measuring low $v \sin (i)$ values is particularly difficult due to the weak rotational broadening of the spectral lines for slow rotators. When values for $\sin (i)$ fell above 1, we set these values to 1 as discarding them would bias our results towards lower inclinations \citep{Vos2017}.
Since $11$\,km\,s$^{-1}$ is one of the lowest $v \sin (i)$ values reported in the Wichmann study, we assume larger error bars of $3$\,km\,s$^{-1}$. Using the parameters listed in Table~\ref{tab:param}, we find that the  majority of the $\sin (i)$ distribution ($\sim96\%$) falls above 1, with a median $\sin(i)=2$. This results in an inclination distribution with a sharp peak at $90^{\circ}$, or equator-on. A doubling of the radius or a halving of the rotation period would bring the median value to 1. Although we observe a period harmonic at half our reported rotation period, we consider it unlikely to be the true period due to the repeating double-peaked pattern observed  in Figure~\ref{fig:lightcurves_ls}. We consider it more likely that the radius is inflated due to its youth (e.g., \citealt{Somers2015, Somers2017}). Either way, the measured rotation rate and $v\sin(i)$ values and estimated radius suggest that  BD+60 1417 is inclined close to equator-on.

As shown in Figure~\ref{fig:lightcurves_ls}, the light curve of BD+60 1417 shows some starspot evolution but is otherwise a clean rotation curve.  We find no signature of a transiting world over the TESS cadences even though we are staring at the star across the equator.

For the secondary, to determine all fundamental parameters we followed the prescription of \citet{Filippazzo15}. We used the Gaia eDR3 parallax of BD+60 1417 combined with all available photometric and spectroscopic information on BD+60 1417B to produce a distance calibrated spectral energy distribution.  By integrating over the SED, we directly calculated the bolometric luminosity. Using the evolutionary models of \citet{Saumon08} paired with the 50 - 150 Myr age range cited above, we obtained a radius range and semi-empirically obtained estimates for the $T_{\rm eff}$, mass, and log(g).  All fundamental parameters are listed in Table~\ref{tab:param}.

\section{Characteristics of the BD+60 1417 System\label{sec:characteristics}}
Figure~\ref{fig:Mass-Sep} shows the separation versus mass ratio of a wide variety of companion systems.  For stellar binaries, we drew from the literature compilations in \citet{Faherty10} appended with recent discoveries of 50pc co-moving companions in \citet{ElBadry2021}.  For brown dwarf companions we used the recent compilation by \citet{Faherty2020} appended with a thorough literature search performed for this work of MLT companions in systems with total mass $>$ 100 M$_{Jup}$ (for example adding recent discoveries by \citealt{Zhang2021B} and Schneider et al. 2021) and for planetary companions we used the NASA exoplanet archive database.

From the bottom left corner of Figure~\ref{fig:Mass-Sep} to the top right corner we are sampling objects that form via traditional planetary processes (e.g. core accretion) to objects that form via traditional stellar processes (e.g. cloud fragmentation).  As we pass from the lower left to the upper right, we may sample a mix of those formation processes or a clear delineation between differing populations (e.g. \citealt{Kratter2010}).  We also must note that there are observing biases on this plot given that transiting planets and radial velocity planets have limitations to the maximum separation they can be detected given the long baseline required to find more distant planets.

We have color coded Figure~\ref{fig:Mass-Sep} by exoplanet detection method as the question at hand is whether BD+60 1417B should be considered a young companion formed via binary star processes or a young planet formed via accretion or similar processes.  Directly imaged companions occupy a sparsely sampled region of Figure~\ref{fig:Mass-Sep} which is detached from the locus of stellar binaries (grey overdensity at upper right) and exoplanet companions (lower left).  The BD+60 1417 system sits squarely between the two loci in a very similar position to the Ross 458, HIP 78530, HN Peg, and HD 106906 systems.  It has the largest separation known for its mass ratio\footnote{The estimated mass ratio for BD+60 1417 is just smaller than that of the recently published COCONUTS-2b source by \citet{Zhang2021B}}, making it a boundary setting object on Figure~\ref{fig:Mass-Sep}.

Assuming the mass of the primary is $\sim$1.0 M$_{\sun}$ (from \citealt{Metchev2009}), the secondary is 15 M$_{Jup}$, and the physical separation is 1662 AU x 1.26 (for orbital inclination angle correction; see \citealt{Fischer1992}), we find a binding energy of $\sim$1.204 x 10$^{41}$ erg.  In our analysis of main sequence star co-moving systems, brown dwarf and exoplanet companions we find this source in the lowest 4\% in terms of binding energy. We also find it joins just a handful of companion objects (GU Pscb, USco 1621b, USco 1556b, Ross 458c, FU Taub, COCONUTS-2b, 2MASSJ21265040-8140293b, WD0806b, and Ross 19B) with estimated masses $<$ 20 M$_{Jup}$ and a separation $>$ 1000 AU\footnote{The separation is evaluated as 1.26x the projected separation to account for inclination angle}.  Among those systems and with the exception of WD0806 which has evolved off the main sequence, BD+60 1417 has nearly twice the primary mass of any other.

\section{Discussion\label{sec:discussion}}
Determining the formation mechanism for planetary mass objects (companion or isolated) remains difficult. It is very likely that as we move down in mass, there are contributions to the mass function from competing mechanisms that can create identical looking objects.  BD+60 1417B is an object with photometric and spectral characteristics perfectly in line with isolated and companion $<$ 20 M$_{Jup}$ objects.  It does not differentiate itself from closer planets in any of its fundamental parameters.  In fact, it resembles those sources so well it should be considered an important laboratory for investigating weather related atmospheric phenomenon relevant to giant planet analyses.

 \citet{Kirkpatrick2021} recently analyzed the mass function of the 20pc sample of brown dwarfs into the Y dwarf regime and discovered that the current sample implies that the cutoff of star formation is lower than 10 M$_{Jup}$ with some hint from moving group members that it might be lower than 5 M$_{Jup}$.  Based on these cut-off values, even the lower mass limit for BD+60 1417B would argue for its formation mechanism still aligned with that of higher mass isolated brown dwarfs. However, the BD+60 1417 system occupies a unique and sparsely populated region in Figure~\ref{fig:Mass-Sep} and BD+601417B has a mass above the 5 M$_{Jup}$ cut-off. The dearth of brown dwarf companions close-in to their host stars is a well known phenomenon and has been dubbed ``the brown dwarf desert".  Studies such as \citet{Raghavan2010}, \citet{Metchev2009}, \citet{Brandt2014} conducted detailed investigations on the companion frequency for low mass secondaries.  \citet{Metchev08} concluded that the companion mass function follows the same universal form over the entire range between 0 - 1590 AU in orbital semi-major axis and $\sim$0.01–20 $M_{\sun}$ in companion mass therefore the brown dwarf desert is a logical extension of the field mass function.  \citet{Brandt2014} concluded that many of the directly imaged exoplanets known formed by fragmentation in a cloud or disk, and represent the low-mass tail of the brown dwarfs. It is completely logical that BD+601417B formed as a binary system with BD+60 1417 and is simply a rare, planetary-mass product of the lowest mass limit of star formation.

Even still, there remains the possibility that BD+60 1417B formed closer in through core accretion or disk instability and was dynamically disturbed to its current position.  Recent investigations of the planetary mass companion HD 106906b (estimated mass$\sim$11$\pm$2 M$_{Jup}$ at 738 AU) suggested that a stellar fly-by may have disturbed the companion to its current position and orbit given that the planet is not coplanar with the surrounding disk (\citealt{DeRosa2019}).  Other works have shown the significant influence that stellar fly-bys may have on young forming planetary systems (e.g. \citealt{Malmberg2011}, \citealt{Picogna2014}) and the potential for disturbing or even ejecting a companion.  While there is currently no evidence for a dynamic disturbance to this system, the possibility can not be ruled out.

 \citet{Bowler2020b} used eccentricity values for low mass companions to determine that when subdivided by companion mass and mass ratio, the underlying distributions for
giant planets and brown dwarfs show significant differences. The large separation of this system and consequent significant period to complete an orbit precludes any eccentricity measurement to place it in context.  However, another avenue of investigation could be using the inclination angle for BD+60 1417B and compare that to BD+60 1417.  As stated in section~\ref{sec:fundamentals}, BD+60 1417 appears to be viewed equator on.  A measurement of the rotation rate and vsini for BD+60 1417B would allow us to calculate the viewing angle (e.g. \citealt{Vos2017}) and compare it to that of the primary.

Yet another avenue that might help disentangle the formation mechanism for this companion is a comparison of the bulk composition of the secondary with the primary.  The spectral inversion technique can successfully recover gas abundances and atmosphere properties of brown dwarfs (e.g. \citealt{Burningham2017, Burningham2021}, \citealt{Line2017}) including C/O, Mg/Si, etc. Previous studies of giant planetary mass companions (e.g. \citealt{Konopacky2013}) have used the C/O ratio comparison between components to speculate on a formation route.  Recent work by \citet{Gonzales2020} used the spectral inversion technique to confirm two brown dwarfs as common origin based on similar composition measurements including a measurement of C/O for both components.  The BD+60 1417 system is an excellent candidate for a spectral inversion approach to determine if chemical composition could help differentiate the formation mechanism.  While that is outside of the scope of this work, the data collected here-in can and should be used by retrieval codes such as BREWSTER (\citealt{Burningham2017}, \citealt{Burningham2021}) which uses complex cloud approaches to examine the detailed atmospheric chemistry of a given source.

\section{Conclusions\label{sec:conclusions}}
In this work we have discussed the discovery of a young L dwarf companion to a nearby young K0 primary through the Backyard Worlds: Planet 9 citizen science project.  Using SpeX prism follow-up spectroscopy, we classify BD+60 1417B as an L6-L8$\gamma$ and find it to be one of the reddest known L dwarfs in the near infrared.  We find its spectral morphology is similar to other 10 - 150 Myr L dwarfs such as W0047, PSO 318, and W2244, and --similar to those sources-- its shape suggests that it is a cloudy object with the potential to demonstrate cloud-driven variability. The position on near- and mid-infrared color-magnitude diagrams -- using the parallax of the primary -- places BD+60 1417B as redder and fainter than the field sample, another hallmark characteristic of $<$150 Myr L dwarfs.  BD+60 1417B shares spectral and photometric properties with both isolated low gravity objects and young giant planets orbiting higher mass stars (e.g. HR8799bcde).  Using the parallax and spectral data we compute a spectral energy distribution and find log($L_{\rm bol}$/$L_{\odot}$)=-4.33$\pm$0.09, T$_{eff}$=1303$\pm$74 K, and Mass=15$\pm$5M$_{Jup}$ for BD+60 1417B.

The angular and physical separation of this system are 37$\arcsec$ and 1662 AU respectively.  We investigated the mass ratio vs. separation for the BD+60 1417 system and found it occupied a unique and sparsely populated region of the diagram between two loci of binary stars and planet companions.  It belongs to a sub-population of only 9 objects with an estimated mass $<$20 M$_{Jup}$ that orbit their host star at more than 1000AU. Among that small list it has a primary mass almost twice that of any other main sequence system (the exception being WD0806 which has a white dwarf host star with a progenitor mass of $\sim$2M$_{sun}$). We can not conclude a formation mechanism from any of the parameters presented in this paper (core accertion, disk instability, cloud fragmentation) but we are optimistic that future retrieval or viewing angle comparisons with the primary will shed light on how this system formed.  BD+60 1417B is an exciting target for future missions such as JWST which will open the mid-infrared spectral window on studying the clouds and composition of the source.

\begin{acknowledgments}
The Backyard Worlds: Planet 9 team would like to thank the many Zooniverse volunteers who have participated in this project, from providing feedback during the beta review stage to classifying flipbooks to contributing to the discussions on TALK. We would also like to thank the Zooniverse web development team for their work creating and maintaining the Zooniverse platform and the Project Builder tools. This research was supported by NASA Astrophysics Data Analysis Program grant NNH17AE75I as well as NASA grant 2017-ADAP17-0067, and National Science Foundation Grant No.'s 2007068, 2009136, and 2009177. F.M.~also acknowledges support from grant 80NSSC20K0452 under the NASA Astrophysics Data Analysis Program.  E.G. and J.F. acknowledge support from the Heising-Simons Foundation. This research has made use of: the Washington Double Star Catalog maintained at the U.S. Naval Observatory; the SIMBAD database and VizieR catalog access tool, operated at the Centre de Donnees astronomiques de Strasbourg, France (\citealt{Ochsenbein00}); data products from the Two Micron All Sky Survey (2MASS; \citealt{Skrutskie06}), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC)/California Institute of Technology (Caltech), funded by the National Aeronautics and Space Administration (NASA) and the National Science Foundation; data products from the Wide-field Infrared Survey Explorer ($WISE$; and \citealt{Wright10}), which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory (JPL)/Caltech, funded by NASA.  This work has made use of data from the European Space Agency(ESA) mission Gaia, processed by the Gaia Data Processing and Analysis Consortium. Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.
\end{acknowledgments}

\startlongtable
\begin{deluxetable*}{cccccc}
\tablecaption{Measured Parameters\label{tab:param}}
\tablehead{
\colhead{Parameter} & \colhead{BD+60 1417} & \colhead{BD+60 1417B} & \colhead{System} & \colhead{Units} & \colhead{Reference}}
\colnumbers
\startdata
{\bf ASTROMETRY}\\
\hline
\hline
$\alpha$ &  190.88751026191\tablenotemark{a}& 190.8838648 &$\cdots$ & deg &1,5\\
$\delta$ &  +60.01435471736\tablenotemark{a}& 60.0239567  &$\cdots$ & deg &  1,5\\
$\varpi$ & 22.2437\,$\pm$\,0.0135 &$\cdots$    &$\cdots$ & mas &1\\
Distance       & 44.957$\pm$0.027\tablenotemark{b} & 44$\pm$4\tablenotemark{c} &  & pc & 2\\
$\mu_{\alpha}$ & -126.401\,$\pm$\,0.013 & -133\,$\pm$\,8 & $\cdots$ & mas\,yr$^{-1}$ & 1,52\\
$\mu_{\delta}$ & -64.141\,$\pm$\,0.015  & -55\,$\pm$\,8 & $\cdots$ & mas\,yr$^{-1}$ & 1,5\\
\hline
\hline
{\bf ROTATION}\\
\hline
\hline
Prot     & 7.50$\pm$0.86 &$\cdots$&$\cdots$& days & 2\\
vsini &$11\pm3$&$\cdots$&$\cdots$&km\,s$^{-1}$&8\\
inc angle  & {$\sim90^{\circ}$} &$\cdots$&$\cdots$& deg & 2\\
\hline
\hline
{\bf PHOTOMETRY}\\
\hline
\hline
$G_{BP}$ & 9.652961$\pm$0.003343 & $\cdots$ & $\cdots$ & mag &  1\\
$G$     & 9.183514$\pm$0.002805 & $\cdots$ & $\cdots$ & mag &  1\\
$G_{RP}$ & 8.551546$\pm$0.003985 & $\cdots$ & $\cdots$ & mag &  1\\
Pan-STARRS $y$ & $\cdots$ & 20.481$\pm$0.178& $\cdots$ & mag &  1\\
2MASS $J$ & 7.823$\pm$0.020  & $>$17.452 & $\cdots$ &  mag & 3\\
2MASS $H$ & 7.358$\pm$0.016  & $>$16.745 & $\cdots$ &  mag & 3\\
2MASS $K_s$ & 7.288$\pm$0.024 & 15.645$\pm$0.216 & $\cdots$ &  mag & 3\\
2MASS $J$\tablenotemark{d} & $\cdots$  & 18.37$\pm$0.22 & $\cdots$ &  mag & 2\\
2MASS $H$\tablenotemark{d} & $\cdots$  & 16.66$\pm$0.22 & $\cdots$ &  mag & 2\\
MKO $J$\tablenotemark{e} & $\cdots$  &18.53 $\pm$ 0.20 &$\cdots$  &  mag & 2\\
MKO $H$\tablenotemark{e} & $\cdots$  &17.02 $\pm$ 0.20 &$\cdots$  &  mag & 2\\
MKO $K$\tablenotemark{e} & $\cdots$  &15.83 $\pm$ 0.20 &$\cdots$  &  mag & 2\\
$W1$&  7.230$\pm$0.030 & 14.461$\pm$0.014 & $\cdots$ & mag &4,5\\
$W2$&  7.285$\pm$0.019 & 13.967$\pm$0.013 & $\cdots$ & mag &4,5\\
$W3$&  7.248$\pm$0.017 & $\cdots$         & $\cdots$ & mag & 4\\
$W4$&  7.145$\pm$0.080 & $\cdots$         & $\cdots$ & mag & 4\\
ROSAT HR1 & -0.25 $\pm$ 0.23 & $\cdots$ & $\cdots$ & & 6\\
ROSAT HR2 &  0.23 $\pm$ 0.38 & $\cdots$ & $\cdots$ & & 6\\
ROSAT Count & 4.13e-02 $\pm$ 1.17e-02 & $\cdots$ & $\cdots$ & ct s$^{-1}$ & 6\\
GALEX NUV & 16.29 $\pm$ 0.022 & $\cdots$ & $\cdots$ & mag  & 7\\
GALEX FUV & 21.286 $\pm$ 0.371 & $\cdots$ & $\cdots$ & mag  &7\\
\hline
\hline
{\bf SPECTROSCOPY}\\
\hline
\hline
Spectral Type (OpT) & K0 & $\cdots$ & $\cdots$ &$\cdots$ &2\\
Spectral Type (IR) & $\cdots$ & L8$\gamma$ & $\cdots$ &$\cdots$ & 2\\
\hline
\hline
{\bf FUNDAMENTALS}\\
\hline
\hline
Age & 50 - 150 & $\le$150 & 50 - 150 & Myr & 8, 2\\
log($L_{\rm bol}$/$L_{\odot}$) & 0.35595$\pm$0.01021 & -4.33$\pm$0.09 & $\cdots$ & &9, 2\\
$T_{\rm eff}$ &  4993$\pm$124&  1303$\pm$74 & $\cdots$  & K &9, 2\\
Radius        &  0.797$\pm$0.051& 1.31 $\pm$ 0.06 & & $R_{\rm sun}$, $R_{\rm Jup}$ & 9, 2\\
Mass          &  1.0&  15$\pm$5 &  & $M_{\rm sun}$,  ~$M_{\rm Jup}$ & 10, 2\\
$\log{g}$     &  4.5539 & 4.3$\pm$0.17 & $\cdots$  & cm s$^{-2}$ & 9,2\\
\hline
\hline
{\bf KINEMATICS}\\
\hline
\hline
U     & -13.798$\pm$0.076 &$\cdots$&$\cdots$& km\,s$^{-1}$ & 2\\
V     & -28.681$\pm$0.108 &$\cdots$&$\cdots$& km\,s$^{-1}$ & 2\\
W     & -1.923$\pm$0.203 &$\cdots$&$\cdots$& km\,s$^{-1}$ & 2\\
X     & -13.923$\pm$0.010 &$\cdots$& $\cdots$ &pc & 2\\
Y     & 20.073$\pm$0.014 &$\cdots$&$\cdots$& pc & 2\\
Z     & 37.741$\pm$0.023 &$\cdots$&$\cdots$& pc & 2\\
RV & -10.15$\pm$0.24 &  $\cdots$ &  $\cdots$ & km\,s$^{-1}$ & 1\\
\hline
\hline
{\bf SYSTEM}\\
\hline
\hline
Separation&$\cdots$ & $\cdots$& 37 & $\arcsec$ & 2\\
Separation& $\cdots$ & $\cdots$& 1662 & AU & 2\\
Binding Energy & $\cdots$ & $\cdots$&1.204 & 10$^{41}$ erg  & 2\\
\enddata
\tablenotetext{a}{epoch J2016.0, ICRS}
\tablenotetext{b}{Calculated using D = 1/$\pi$, which is good approximation for parallax known to $\pi$/$\sigma_{\pi}$ = 0.75\% accuracy}
\tablenotetext{c}{Calculated using the spectrophotometric relation for young L dwarfs in \citet{Faherty16}}
\tablenotetext{d}{Synthetic 2MASS photometry from SpeX spectrum.}
\tablenotetext{e}{Synthetic MKO photometry from SpeX spectrum.}

\tablecomments{References: (1) \citet{eDR32020}, (2) This paper, (3) \citet{Cutri03}, (4) \citet{Wright10}, (5) \citet{Catwise2020}, (6) \citet{Rosat}, (7) \citet{Galex2020}, (8) \citet{Wichmann2003}, (9) \citet{TIC2018}, (10) \citet{Metchev2009} }
\end{deluxetable*}

\vspace{5mm}
\facilities{\emph{Gaia}, NASA IRTF, LICK Shane, \emph{WISE}, \emph{2MASS}}

\software{Aladin, BANYAN~$\Sigma$ (\citealt{Gagne18}), Lightkurve, SEDkit, WISEview}

redpajama_set_name: RedPajamaArXiv


When it comes to dealing with contraception, the primary accountability tends to fall on the girl; and that is very true in monogamous and married relationships the place condoms are given up, as there isn't any longer a perceived need to guard oneself from sexually transmitted infections. Sign up for a free Medical Information Right this moment account to customise your medical and health news experiences. Well being Minister Greg Hunt publicizes a $3 million funding boost for providers to assist the 1 million Australians presently suffering from an eating dysfunction.
EMPLOYEES at an NHS organisation have fashioned a gaggle aimed toward making it simpler for participants to talk about psychological well being at work. Go to for medical information and well being news headlines posted throughout the day, day-after-day. Paul praised the chief order as one thing that will assist reform the well being care system.
Mr. Trump has long talked about his desire to make health insurance plans accessible across state strains. We discovered a minimum of 8 totally different sites with barely totally different information names – Health Information 6, News Health 9, New 7 Health, and so forth.
It is important to plan the matters from the within out, which means one core article (i.e. the first topic of the week, month or quarter) and secondary articles which either help the first subject, or in a roundabout way provide supplementary recommendation.
The order could additionally allow employers in the same line of work to hitch together to supply health care to workers, no matter their state. You'll be able to subscribe to some of these digital newsletters that characteristic well being information.


text:
Pannekeet is een buurtschap in de gemeente Dijk en Waard in de Nederlandse provincie Noord-Holland.

Pannekeet ligt in het noorden van de gemeente Dijk en Waard, tussen Zuid-Scharwoude, Kanaal Alkmaar (Omval)-Kolhorn, en De Noord in. De plaatsnaam komt al in 1840 voor in de huidige spelling. De naam verwijst naar het oorspronkelijke kleine gebouw waaruit de buurt is ontstaan. Het is onduidelijk of de plaatsnaam verwijst naar het pannendak van het gebouwtje of naar de familienaam, die veel voorkomt in dit deel van West-Friesland.

Van de uitgegroeide en uitgestrekte plaats is weinig meer te zien, een groot deel van het gebied is industrieterrein geworden. Aan het westelijk deel daarvan is de huidige bewoning van Pannekeet nog wel te vinden.

Buurtschap in Noord-Holland
Geografie van Dijk en Waard

redpajama_set_name: RedPajamaWikipedia


text:
Q: Remove the Dots for Spaces in VS2019 I know this has been asked many times on here as I have read so many posts on how to fix this issue... the problem is that CTRL+R CTRL+W (or CTRL+E CTRL+S) doesn't fix it; neither does the menu option to toggle 'View White Space' (Edit > Advanced).  None of the solutions that I can find have fixed this problem.
These dots only appear in the front of a line, and only seem to span across the first two tab/indentation indicators.
I can't figure out how to remove these dots!!  Please help.

redpajama_set_name: RedPajamaStackExchange


How much space free is required to run Rollback RX Free?
I understand this might be a difficult question because it all depend on user behavior regarding usage of it's system.
I have a notebook with a partitioned SSD, I tried to keep the OS part as small as possible but just leave enough space to run RX normally.
Currently the notebook has 65GB reserved for windows and the only applications installed are: Office 2016 and Chrome.
The notebook is used for Browsing and Office only and it has 38,5 GB free space left. The RAM is 8GB.
I was wondering if the OS space could be shrinked about 15GB more without compromising the behavior of RX negatively.
I have 3 snapshot's set on the machine and will making a 4th (final!) snapshot.
I will from time to time go back to the 3th snapshot, update the notebook (windows update) and create a new 4th snapshot (deleting the older 4th snapshot).
The operating system is Windows 10 professional pro 64bit.
Each snapshot can be given a short description, could it be made possible to give bigger/larger descriptions.
A few lines in stead of one. (multi-line input field).
Each time the user reverts back to an earlier, give the user a head-sup about the applications that will be undone/removed.
Some applications require an online re-activation, an uninstall is needed to properly deactivate some applications.
The free version of rollback triggers itself on "setup.exe" to create a new snapshot.
I had constant crashes with this. I eventually resolved it (for now) but it is still very annoying to have it constantly having to pop-up.
It still might interfere especially when doing a clean reinstall meaning you are going through several "setup.exe".
Some application setups spawn different "setup.exe" meaning rollback is constantly popping up.
Could there be an option to temporarily postpone the triggering on "setup.exe" (if it can not be removed).
For example have an option to postpone triggering for 20 minutes.
- It avoids troubling/annoying the user.
Another option could be to have the user optionally disable this behavior.
Would you please consider to pass this on to the support/development team.
Thank you for your response. RollBack Rx itself doesn't take up much disc space at all, as it only uses up to 20mb or 7% of your hard drive space. Once you start creating snapshots and install new software or Windows updates on your PC, then that's when it will start to take up more hard disc space. If you need more information on how Rollback calculates and uses disk space, feel free to send me an email: shainal.reman@horizondatasys.com, and I can help you with that. In terms of your request mentioned on the post, I will pass it on to our development team and hopefully they will make those changes in a future build release.


text:
Whip-Poor-Will, I
By L. Lamar Wilson Reprinted with permission from University of Georgia Press
Play dead, like you, all day, then rise at night
& sing—my throat Gabriel's genuflected cry. O
Let the souls slain at night rise first, reclaim
This desolate terrain. O let this land's redeemed
Say No more & drive these maniacal white ghosts
More mad. So many black & luminous smiles,
Our seek a found invisibility. Like you, I work
Now while it is night, when no white man can
Without my never-ready back. Unfurl
My ancient tongues & fill the holes in their
Sacked hearts with this terrifying refrain:
This world's all mine. All mine. All mine. All
Mine. All mine. All mine. You've lied to your
Selves. You've occupied my home too long. Get out.
EASTERN WHIP-POOR-WILL
Habitat and Range: Ground and low horizontal branches in mixed pine-deciduous and deciduous woods. Eastern United States, as far west as Nebraska and Kansas, north to Canada, and south to Florida. Migrates from Florida and the tropics in spring and arrives in the Southern Appalachians in late March and early April.
Description and Notes: The whip-poor-will is also known as a "night jar"; a group of whip-poor-wills may be known as "a seek" or "an invisibility." The mottled gray and brown plumage of this chesty little bright-eyed and short-billed bird gives it exceptional camouflage in the leaf litter of its woodland habitat, where it nests on the ground and sleeps during the day. At dusk and on moonlit nights, it declares its presence (and its name) with its sharp, insistent call: "whip-poor-will, whip-poor-will, whip-poor-will." Whip-poor-wills sing more with moonlight. (A 1981 study in Georgia correlates decelerating and accelerating call frequency with the diminishing and then increasing light of a lunar eclipse.) What's more, whip-poor-wills sync their egg-laying with the lunar cycle. By timing the eggs to hatch a week and a half or so before the full moon, the parents have the best light in which to forage moths, beetles, and other insects for their new young. Because of its nocturnal habits and haunting call, the whip-poor-will in folk and native lore is a harbinger of human loneliness and death. As populations are now declining steeply, however, the bird's association with omen or lament reads differently. If nothing else, its presence will continue in literature and music; whip-poor-wills appear in stories by Washington Irving, William Faulkner, and James Thurber, poems by Stephen Vincent Benét and Robert Frost, and songs by Hank Williams and Elton John.
A Literary Field Guide to
Southern Appalachia
University of Georgia Press

redpajama_set_name: RedPajamaCommonCrawl


text:
The First 5G Phone Might Be a OnePlus
By Holly Brockwell on at
The race to 5G is speeding up, and OnePlus want to cross the finish line first.
Qualcomm, one of the major driving forces behind 5G, have announced at a conference in Hong Kong that they're expecting at least two 5G flagship phones next year, one of which will be in the first half of the year. Shortly afterwards, OnePlus CEO Carl Pei joined them on stage and announced that OnePlus will be one of the manufacturers with a 5G phone coming out in 2019, and they expect to be either one of the first, if not THE first.
We already knew OnePlus had something planned for January, and the rumour mill is now churning at turbo speed speculating that it could be the OnePlus 5G (as we're calling it).
The Chinese company has a significant advantage over bigger, more traditional tech companies when it comes to adopting new tech early. Their audience is hardcore phone fans who want the newest and best of everything, which is presumably why we haven't seen any lower-spec phones like the OnePlus X recently.
It seems OnePlus has rightly surmised that its audience of early adopters will want to be the first to get 5G, and with some major capital behind it from strong sales (for a challenger brand) and recent high-street deals, the company is one of the best placed to take the gamble.
That's not to say Pei and co always give the fans what they ask for – they famously ignored protests about including a notch on their phones, and more recently they've come under fire by the fanbase for removing the 3.5mm headphone jack on the upcoming OnePlus 6T.
January seems early to expect a fully-fledged 5G phone, especially when the 6T will only have been released a few months before, but it's theoretically possible. Whatever the mystery announcement is, hopefully it'll be something to cheer up our grey British January – i.e. not another all-black phone and dear god, please not another backpack. [Engadget]
carl pei
Holly Brockwell


text:
msodradek:
Still from chapter 8 of Roberto Rossellini's Francesco, giullare di Dio (Francis, God's Jester, 1950)
Franciscan Grotesquerie
… [Francis of Assisi]'s public appearances … are always impressive, graphic, and indeed scenic. The anecdotes which relate them are very numerous, and among them there are some which strike later taste as almost grotesque or even farcical; as when we are told that, celebrating Christmas in the stable at Greccio, with ox and ass and praesepium, both in singing and preaching he pronounced the word Bethlehem in imitation of a bleating lamb; or that after an illness in the course of which he had taken some choicer food, upon his return to Assisi he ordered one of the brothers to lead him through the town on a rope, as though he were a criminal, shouting: Behold the glutton who crammed his belly full of chicken behind your backs! But in their time and place such scenes did not produce a farcical effect. Their arrestingness, exaggeration, vividness did not appear shocking, but as a graphic, exemplary revelation of a saintly life, directly illuminating, comprehensible to all, and inspiring all to examine themselves in comparison and to share in the experience. …
The saint's manner of life and expression was taken over by the Order and produced a very peculiar atmosphere. In both the good and bad sense, it became extremely popular. The excess of drastic vigor of expression made of the friars the creators, and soon too the subject, of dramatic, witty, and frequently coarse and obscene anecdotes. The coarser realism of the later Middle Ages is often linked to the activity and appearances of the Franciscans. Their influence in this direction can be traced down to the Renaissance. …
—Erich Auerbach, Mimesis: The Representation of Reality in Western Literature (1946), ch. 7 "Adam and Eve", tr. Willard R. Trask, Princeton University Press, 2003, pp. 168-170.
I have seen that "peculiar atmosphere" in the contemporary church: both the "exemplary revelation of the saintly life" and the "farce". What a fine blade fits between the two: the difference between being wise as serpents and innocent as doves. I don't think I could say what it is, but there seems to be a lot riding on it. Maybe it simply is gratitude in both the observer and the "performer".
October 4, 2012 January 29, 2017 / Seth Wieck	/ Leave a comment


text:
IEBC new and old guard wrangle over President-elect polls victory
IEBC vice chairperson Juliana Cherera. PHOTO | NMG
The announcement of William Ruto as the President-Elect on Monday split the electoral body, with all the four commissioners appointed a year ago questioning the credibility of the results Independent Electoral and Boundaries Commission (IEBC) chairman Wafula Chebukati declared.
The four, led IEBC vice-chairperson Juliana Cherera, disowned the results at a news conference Monday evening, saying some aspects of the electoral process were opaque.
Others were Francis Wanderi, Irene Masit and Justus Nyang'aya.
They were appointed in September last year to replace commissioners Consolata Nkatha, Margaret Mwachanya, Paul Kurgat and Roselyn Akombe, who resigned after the 2017 polls -- marred by the nullification of the presidential election outcome by the Supreme Court.
Abdi Yakub Guliye and Boya Molu who have been with the electoral body since January 2017, however, stuck with Mr Chebukati as he announced the results at Bomas of Kenya in Nairobi.
The four dissenting commissioners said the exercise of verification was all right until the last phase when the process turned opaque and that they did not wish to be part of it.
Ruto to start receiving security briefings after election victory
They declined to answer questions from journalists, saying they would issue a comprehensive statement later.
The claims by the four commissioners might be used as one of the grounds in a presidential election petition, in case Azimio la Umoja or any other Kenyan challenges the results at the Supreme Court.
A petition should be filed within seven days from the day the results are announced and determined within 14 days.
Mr Chebukati disclosed that a number of IEBC officials were under arrest for unknown reasons and one official is reported missing. The returning officer for Nairobi's Embakasi East Constituency Daniel Musyoka has been missing since he announced the results on August 11.
He also claimed that IEBC officials had been harassed, intimidated and injured during the process.
"I stand here despite intimidation and harassments. I took an oath of office to serve this country and I have done my duty in accordance to the Constitution and the laws of the land," said Mr Chebukati.
If a petition is filed at the Supreme Court, it would be the third time the apex would be asked to arbitrate a presidential election dispute since it was created under the 2010 Constitution.


text:
Comparative study QFR vs iFR
Dr Masahiro Watarai and colleagues from Cardiovascular Center, Ogikubo hospital in Tokyo, under the supervision of Dr Yasuhiro Ishii published a paper in the Intern J of Cardiovascular Imaging on the applicability of the QFR for rapid evaluation evaluation of intermediate coronary stenosis and the comparison with iFR. This was a prospective study in which 150 coronary lesions were enrolled, including 50 lesions for on-site QFR. The mean QFR and IFR were 0.81 and 0.89, respectively. In ROC analysis, the AuC of QFR for predicting iFR<0.89 was 0.91. Applying the cut-off values of 0.80 for QFR and 0.89 for iFR, the sensitivity, specificity, positive and negative predictive values were 85%, 83%, 72% and 91, respectively in all subjects, and 82%, 82%, 78% and 85%, respectively in the on-site analysed vessels. They concluded that the QFR has a diagnostic performance comparable to that of iFR.
For further read: doi.org/10.1007/s10554-019-01656-z.
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text:
You are here: Parliament home page > Parliamentary business > Business Papers > Public Bills before Parliament > Bill home page
Session 2010-12
fixed-term parliaments Bill
These notes relate to the Lords Amendments to the Fixed-term Parliaments Bill,
as brought from the House of Lords on 24 May 2011.
1. These Explanatory Notes relate to the Lords amendments to the Fixed-term Parliaments Bill, as brought from the House of Lords on 24 May 2011. The Notes have been prepared by the Cabinet Office in order to assist the reader of the Bill and the Lords amendments, and to help inform debate on the Lords amendments. They do not form part of the Bill and have not been endorsed by Parliament.
2. These Notes, like the Lords amendments themselves, refer to HL Bill 40, the Bill as first printed for the Lords.
3. These Notes need to be read in conjunction with the Lords amendments and the text of the Bill. They are not, and are not meant to be, a comprehensive description of the effect of the Lords amendments.
4. Lords Amendments 5, 7 and 8 were tabled in the name of the Minister. Lords Amendments 3, 4 and 6 were supported by the Government. Lords Amendments 1, 2 and 9 were opposed by the Government.
5. In the following Commentary, an asterisk appears in the heading of each of the paragraphs dealing with non-Government amendments.
Bill 195-EN
COMMENT A RY ON LORDS AMENDMENTS
* Lords Amendment s 1, 2 and 9
6. Lords Amendments 1 and 2 would provide that the polling day for a subsequent parliamentary general election (that is, elections after the next parliamentary general election under the Bill) is only to be fixed under the Bill if each House of Parliament resolves that that polling day should be so fixed. Lords Amendment 9 would provide that clauses 2, 3 and 4(3) are to have effect only until the first meeting of the new Parliament after the next general election. The amendment would provide that these provisions may be brought back into force for that or any subsequent Parliament if each House passes a resolution at any point in that Parliament to that effect. Amendment 9 would therefore provide in particular that the amendments and repeals in the Schedule would take effect or not have effect for each subsequent Parliament depending on whether or not each House has passed a resolution that clauses 2, 3 and 4(3) are to be brought back into force.
* Lords Amendments 3 and 4
7. Lords Amendments 3 and 4 would amend the power at clause 1(5) which would otherwise allow the Prime Minister to vary the date of a scheduled general election, by affirmative order, by up to two months earlier or later. The amendments would remove the words "earlier or" in the two places where they appear, meaning that the order making power could only be used to defer an election by up to two months, and not bring it forward by up to two months.
Lords Amendment 5
8. Lords Amendment 5 would provide that, where the Prime Minister lays before Parliament a draft of an order under clause 1(5) to change the date of poll for a parliamentary general election, he or she must at the same time lay a statement before both Houses setting out his or her reasons for proposing the change in the polling day.
* Lords Amendment 6
9. This amendment would omit clause 2 and substitute a new version of that clause. Like the version of clause 2 which would be omitted, the amendment would provide two triggers for an early parliamentary general election. The first would be where the House of Commons has passed a motion that there be an early parliamentary general election with the support of at least two thirds of all MPs. The second would be where the House of Commons has passed a motion of no confidence in the Government and no Government has secured the confidence of the House of Commons within 14 days. In contrast to the version of the clause which would be omitted, the amendment would set out the precise form of motions for an early parliamentary general election, of no confidence and of confidence for the purposes of the Bill. The version of the clause which would be omitted contains provisions by which an early general election is only triggered if the Speaker of the House of Commons has certified that the conditions for those triggers have been met. The amendment does not contain these provisions. The amendment would mean therefore that there would be no role for the Speaker under the Bill.
Lords A mendments 7 and 8
10. Lords Amendments 7 and 8 would provide that the general elections for the Scottish Parliament and the National Assembly for Wales which are scheduled to take place on 7 May 2015 will instead take place on 5 May 2016. The amendment s would provide that subsequent ordinary general elections for each institution would be scheduled to be held on the first Thursday in May in the fourth calendar year after the May 2016 general elections. The amendments would provide that the provisions under the Scotland Act 1998 and the Government of Wales Act 2006 relating to varying the date of ordinary general elections and the effect on the date of ordinary general elections of extraordinary general elections would apply to the deferred polls.
11. These amendments would implement the agreement reached earlier this year between the UK Government and, respectively, the Scottish Parliament and the National Assembly for Wales to ensure that the general elections for each institution and the UK Parliament do not coincide on 7 May 2015.
FINANCIAL EFFECTS OF THE LORDS AMENDMENTS
12. The Lords amendments would not affect the assessment of the financial effects concerning the Bill; that the Bill will have no substantial effect on public expenditure.
©Parliamentary copyright
Prepared 25th May 2011


Last week I described five of my favorite things about freelancing. It's not all puppies and rainbows, though, so today I'm sharing some thoughts on one of the biggest challenges to the freelance life: the instability.
Pursue intense short term gigs. Last summer, I worked full time for one client for 12 weeks while they were looking for a permanent person. This worked out great for them (no need to make a desperate hire) and for me (12 weeks of steady work is enough to sock away some money for leaner times). I've even had some success responding to job postings with an offer of acting as a "stand-in" while the company keeps looking for a full time hire.
Cultivate regular clients. Doing one-off projects is great in that it exposes me to a lot of companies, methodologies, and topics. But I always make time for the client who asks me to write a questionnaire almost every week. Having that small but reliable weekly income is a relief for me, and they like knowing that I know their processes and preferences.
Use the slow times well. I used to spend lean months either gallivanting around spending all the money I had made the month before, or panicking that the leanness would never end. Now I try to relax, be confident that another project will come in soon, and be grateful that I have a little down time. I also use slow weeks to prospect like crazy, reaching out to my network and sometimes even cold calling. And finally, I work on other things that don't get much attention when I'm on deadlines for clients: writing academic papers, catching up on industry news, and, recently, developing an online "Questionnaire Design Boot Camp" course for Skillshare.


Spiritual Clearings and Spiritual Surgery — Stand in the Light - Healer, Reiki, Spiritual Coach.
To become your healthiest, happiest self, it is important to make sure you are free of unwanted energies, entities and past life issues. Any of these can throw road blocks in your path to success and make you operate at a lower level, or worse!
When sage simply doesn't make a dent and you've gotten a Feng Shui or general spirit clearing and the problems still persist, it's time to call the doctor; The Entity Doctor! Specializing in removing dark entities and repairing past life soul damage, The Entity Doctor can give a fresh start to people, homes and property, businesses, and even unborn babies. Because this is energy work, The Entity Doctor is able to help anywhere in the world.
One of the best in the business at detecting, removing and repairing things that most practitioners are not aware of or prefer not to deal with because let's face it, these things are SCARY! The Entity Doctor will gently and lovingly remove these unwanted parasites and send them off to continue with their journey so you can be free to pursue your path unencumbered.
After a clearing, a Reiki session can help you return to normal much faster and easier.


After having been named during the Operación Puerto investigation and suspended by his team, Scarponi admitted to the Italian Olympic Committee that he had been involved with Fuentes.
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text:
Negative Energy Cosmology and the Cosmological Constant
@article{Prokopec2011NegativeEC,
title={Negative Energy Cosmology and the Cosmological Constant},
author={Tomislav Prokopec},
journal={arXiv: Cosmology and Nongalactic Astrophysics},
T. Prokopec
arXiv: Cosmology and Nongalactic Astrophysics
It is well known that string theories naturally compactify on anti-de Sitter spaces, and yet cosmological observations show no evidence of a negative cosmological constant in the early Universe's evolution. In this letter we present two simple nonlocal modifications of the standard Friedmann cosmology that can lead to observationally viable cosmologies with an initial (negative) cosmological constant. The nonlocal operators we include are toy models for the quantum cosmological backreaction. In…
Figures from this paper
Stochastic dark energy from inflationary quantum fluctuations
D. Glavan, T. Prokopec, A. Starobinsky
We study the quantum backreaction from inflationary fluctuations of a very light, non-minimally coupled spectator scalar and show that it is a viable candidate for dark energy. The problem is solved…
A unifying theory of dark energy and dark matter: Negative masses and matter creation within a modified ΛCDM framework
J. Farnes
Dark energy and dark matter constitute 95% of the observable Universe. Yet the physical nature of these two phenomena remains a mystery. Einstein suggested a long-forgotten solution: gravitationally…
A stable flat universe with variable cosmological constant in f(R, T) gravity
N. Ahmed, S. Alamri
Research in Astronomy and Astrophysics
In this paper, a general FRW cosmological model has been constructed in f(R,T) gravity reconstruction with variable cosmological constant. A number of solutions to the field equations has been…
A Proposal for a Unifying Theory of Dark Energy and Dark Matter
A cyclic universe with varying cosmological constant in f(R, T) gravity
Canadian Journal of Physics
A new kind of evolution for cyclic models in which the Hubble parameter oscillates and remains positive has been explored in a specific f(R, T) gravity reconstruction. A singularity-free cyclic…
De Sitter universe in nonlocal gravity
E. Elizalde, E. Pozdeeva, S. Vernov
A nonlocal gravity model, which does not assume the existence of a new dimensional parameter in the action and includes a function $f(\Box^{-1} R)$, with $\Box$ the d'Alembertian operator, is…
Transition from decelerating to accelerating universe with quadratic equation of state in f(R,T) gravity
N. Ahmed, M. Fekry, A. A. Shaker
NRIAG Journal of Astronomy and Geophysics
ABSTRACT In this paper, we have constructed a flat Friedmann-Robertson-Walker (FRW) cosmological model in gravity. The solution of Friedmann equations has been obtained assuming the quadratic…
Spontaneous Symmetry Breaking in the Early Universe with a Negative Temperature and a Broken Lorentz Symmetry
R. El-Nabulsi
In this paper we show that, in the early universe, higher order curvature corrections induce spontaneous symmetry breaking with negative temperature and broken Lorentz symmetry when the gravitational…
Cosmology with scalar–Euler form coupling
Adolfo Toloza, J. Zanelli
A coupling between the spacetime geometry and a scalar field involving the Euler 4-form can have important consequences in General Relativity. The coupling is a four-dimensional version of the…
A soliton and a black hole are in Gauss-Bonnet gravity: Who wins?
A. Wong, R. Mann
We study here the phase-transitional evolution between the Eguchi-Hanson soliton, the orbifolded Schwarzschild Anti de-Sitter black hole, and orbifolded thermal Anti de-Sitter space in Gauss-Bonnet…
A Solution to the cosmological constant problem
We argue that, when coupled to Einstein's theory of gravity, the Yukawa theory may solve the cosmological constant problem in the following sense: The radiative corrections of fermions generate an…
Phenomenological model for the early universe
N. Tsamis, R. Woodard
We consider the description of cosmological dynamics from the onset of inflation by a perfect fluid whose parameters must be consistent with the strength of the enhanced quantum loop effects that can…
Primordial density perturbations and reheating from gravity
We consider the presence and evolution of primordial density perturbations in a cosmological model based on a simple ansatz which captures--by providing a set of effective gravitational field…
Generating the curvature perturbation without an inflaton
D. Lyth, D. Wands
We present a mechanism for the origin of the large-scale curvature perturbation in our Universe by the late decay of a massive scalar field, the curvaton. The curvaton is light during a period of…
A simplified quantum gravitational model of inflation
Inflationary quantum gravity simplifies drastically in the leading logarithm approximation. We show that the only counterterm which contributes in this limit is the 1-loop renormalization of the…
Towards inflation in string theory
S. Kachru, R. Kallosh, Andrei Linde, J. Maldacena, L. McAllister, S. Trivedi
We investigate the embedding of brane inflation into stable compactifications of string theory. At first sight a warped compactification geometry seems to produce a naturally flat inflaton potential,…
Adiabatic CMB perturbations in pre - big bang string cosmology
K. Enqvist, M. Sloth
Abstract We consider the pre-Big-Bang scenario with a massive axion field which starts to dominate energy density when oscillating in an instanton-induced potential and subsequently reheats the…
De Sitter vacua in string theory
S. Kachru, R. Kallosh, Andrei Linde, S. Trivedi
We outline the construction of metastable de Sitter vacua of type IIB string theory. Our starting point is highly warped IIB compactifications with nontrivial NS and RR three-form fluxes. By…
Nonlocal cosmology.
S. Deser, R. Woodard
Physics, Medicine
Nonlocally modified models of gravity, inspired by quantum loop corrections, are explored, as a mechanism for explaining current cosmic acceleration, and their solar system effects are safely negligible, and they may even prove useful to the black hole information problem.
The Inflationary Universe
A. Guth


Terrascapes was formed in May 2003 by Giles Granger. Giles started the company having completed his HND in Landscape Construction and it is still owned and run by him to this day.
We work on projects from small private gardens, to multi-million-pound new build projects in the housing sector.
We can offer all aspects of landscape construction along with foundation work and drainage. We work closely with our private clients and housing developers to ensure that we achieve the high standard that they require.


text:
February 9, 2008 by Cheryl Spelts
Rock Star: Season Three
Got some lovely news yesterday! Rock Star III is still a very real possibility! In an interview with thedeadbolt.com, Mark Burnett said…
"Yes, it's funny… you look at these online studies and one of the most requested shows to come back, from anything I've done, is Rock Star. And yes, I'm in discussions with various bands. But there is one flaw as a business in that you have to find a suitable rock band that actually wants to find a new lead singer. So you've got a barrier to entry, but yes, we are in discussions and people do want to see that series again."
He's looking for a band? He's in discussions? Such GREAT news!
Mr. Burnett, this is a direct plea to you! Please listen to those who are telling you they want the show back! And don't worry if you can't get a band – we WANT you to find a band, but if you can't find one that's no reason to discard the show… Just do like we did with All-Stars and let the public decide. We had a lot of fun, and had a GREAT ending with All-Stars, and I firmly believe you don't need a band for this show. And if you feel you need the star power, invite Tommy Lee and Tim Farriss back to join Dave Navarro as judges, and give them a say in the decision, but make the "prize" for the winner, a record contract and solo tour with the House Band. It could work…
And to anyone who loved the show as much as me, this is a direct plea to YOU! More letters! More letters! More letters! If Mark Burnett is considering it, let's give him even more reasons to go for it!
Join our Big Letter Writing Campaign at RBL! It's clear that the public is being heard, so I've decided to split my letters between CBS and Mark Burnett Productions. In the past it seemed smarter to concentrate on CBS, but since Mark Burnett is the one talking about the show right now, and he has serious clout, I wanted to throw half my letters directly to his company.
Ghen Maynard
CBS Paramount Network Television Entertainment Group
Conrad Riggs
Mark Burnett Productions
640 North Sepulveda Boulevard
Just do it. Just write a letter or two. When your favorite show comes back it'll feel really good to know you were a part of the reason it's on!
CategoriesTelevision TagsRock Star: INXS, Rock Star: Supernova
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One Reply to "Rock Star: Season Three"
Velvet Revolver?
Rock Star: Led Zeppelin? Rock Star: House Band? RBL Rock Star: All-Stars Backstage at Rock Star: Supernova
Canon EF 50mm f/1.2 L USM Lens
My favorite basic lens! #ad


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