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PowerKnowledge Physical Science is an online science resource specifically designed for learners in grades 3 to 6. Comprised of curriculum-correlated content, PowerKnowledge Physical Science promotes digital literacy and 21st-century learning skills while offering research, report, and homework help. If you do not find the answer to your question in our extensive help section, please contact us for further assistance.
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Compelling, authoritative Physical Science content from Rosen Publishing's PowerKids Press—a gold standard in nonfiction resources for over fifty years—is available online for the first time with PowerKnowledge Physical Science.
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All recommended Web sites and organizations are annotated and reviewed by Rosen Publishing Digital's team of editors, professionals experienced in creating content for grade 3 to 6 learners.
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Former Reds and Wallabies forward Mark Connors previews Round 10 of Super Rugby.
The Canes have been on the up of late and hit this game fresh after a bye week. The Blues on the other hand produced probably the most woeful display I've seen in years in round 8 against the Brumbies and should be primed to put in a better effort in this local derby. On recent form you couldn't tip the Blues and they are still struggling to find a settled No 10 to direct them, which is also a worry.
The Rebels have shown great spirit and determination in their recent close losses and will be glad to be back home for this clash. However, if the Force can again produce the smothering play that's given them their success this year they will be hard to stop with the confidence and momentum they have at present.
While they are still cruising and well up the leader board, the drop off in form is noticeable from the Chiefs which is a concern. The Crusaders have been flying under the radar of late and with 4 wins from their last 5 games will be brimming with confidence, especially after some more powerful displays over the last two weeks. I'm leaning the Chiefs way though, as they have had the Crusaders measure in recent years and this local derby should jolt them back into top form.
Back home after a difficult tour and some controversy, the Tahs need to freshen up for this must win clash.
The big Question remains? Will Izzy (Folau) play because it looks like they definitely need him to win.
The Bulls on the other hand will be ruing lost opportunities last week and will again be searching for the points. However their depth is being tested again with a few injury concerns.
The Sharks keep on winning and will need to do so again at home this week before their big "away" tour. Coach Jake White has them playing simple but winning rugby and they should account for an erratic Cheetahs side which is having regular lapses of discipline and with its defence.
The Stormers welcome back their captain De Villers after a bye week and with their recent improvement in form should be too good for the Lions. The Stormers superior defence and set piece will provide the basis for a home team win, but look for some fight from the Lions.


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SWINGING WITH OBAMA: Perlmutter Rewarded For Supporting Iran Deal?
"The Courses at Andrews Air Force Base carries an air of true timeless elegance. High-end amenities, exceptional facilities and an unforgettable golf experience are the standard at this military resort."
It appears that U.S. Rep. Ed Perlmutter's golf game Sunday with President Obama was his reward for praising the administration's troubling deal with Iran.
The Denver Post reported glowingly on the game, but failed to mention what prompted the leader of the free world to include Perlmutter and two other Democrats, when these outings are usually limited to the president's family and close friends.
However, the Washington Examiner and Jewish Political News and Update noted the connection between the golf game and the congressmen's public support for the deal to lift sanctions on Iran.
The invitation could be a thank you of sorts rather than a lobbying opportunity because all three House Democrats have offered praise for the deal over the past week.
Perlmutter told the Denver Post there was in fact no lobbying involved, but neglected to mention how he snagged the invitation in the first place.
As for shop-talk, Perlmutter said there was very little of it. Neither Iran nor problems at the U.S. Department of Veterans Affairs came up, he added.
"We just talked golf, family, sports and social media," he said. And while Perlmuter said expects to hear from the White House on those issues, "it wasn't part of yesterday."
The Post also has the photograph of the foursome posing between rounds at The Courses at Andrews Air Force Base resort, or as we like to call it, evidence.
Playing golf with Obama was the kiss of death for former U.S. Sen. Mark Udall. We don't expect it will aid in furthering Perlmutter's political game, either.

redpajama_set_name: RedPajamaCommonCrawl


• Net revenue totaled R$86.5 million in 4Q15, in line with 4Q14. In 2015 our consolidated net revenue reached R$331.2 million, growing 3.9% over the previous year.
• NOI reached R$83.7 million in 4Q15, a 0.4% increase compared to 4Q14. In 2015, the Company's NOI totaled R$315.3 million, a 3.8% increase over 2014.
• Adjusted EBITDA was R$60.2 million in 4Q15, a decrease over 4Q14. In 2015, Adjusted EBITDA increased by 2.6% in comparison with 2014, totaling R$232.6 million.
• Adjusted FFO totaled R$33.3 million in 4Q15 and R$142.6 million in the full-year of 2015.
• Occupancy in our mature portfolio closed 2015 at 96.8%.
• Considering 2015 full-year figures, same-store rents posted an increase of 7.0%. SSR continued to increase in 4Q15, at 5.8% compared to 4Q14, led by the combination of high leasing spreads in our mature malls and the ramp-up of our younger shopping centers.
• Late Payments index remained low at 3.67% in 4Q15.
• Same-store sales (SSS) decreased by 2.2% in 4Q15 compared to 4Q14, reflecting the adverse Brazilian economic scenario. Excluding electronics, SSS in the quarter declined by 0.8%. In the annual comparison, SSS closed 2015 up 0.4% from the previous year.
• Total sales at the Company's malls in 4Q15 totaled R$ 1.5 billion, decreasing 2.1% over 4Q14. The weak retail environment and unstable political scenario continued to pressure families' consumption, and, thus, tenants' sales in our malls. In 2015, our tenant's reported a 2.8% sales increase over 2014.
• On January 13th, the Company announced an agreement for the sale of our entire ownership on Boavista Shopping.
• The Company's Board of Directors will propose the payment of dividends related to the 2015 fiscal year, totaling R$34.8 million or R$0.455 per share.


Brick Lane sofa by Lema.
Square shapes and extra-softness, opposites that attract, for Brick Lane sofa with base flush with the floor designed by Christophe Pillet, perfect interpreter of the philosophy based on relax, typical of the design made in Lema that turns comfort and modularity, into its essential traits.
A balanced game of geometries and volumes that replicate for a new piece of furniture that cultivates the ambition to rise to a new classic, able to be introduced in any environment, whether private or contract. In addition to the neat shapes, this proposal is characterised by the flow of advanced technology, wisely hidden from the stitching, that allows reclining the backrest and bring forward the seat, ensuring utmost comfort. Careful tailoring works are combined to cutting-edge industrial processes, since always distinctive traits of Lema production.
Born in 1959, Pillet graduated from the Decorative Arts School in Nice in 1985, and gained a Masters at Domus Academy, Milano, in 1986. He worked with Martine Bedin in Milano for two years from 1986-1988. He then went on to collaborate with Philippe Starck, in Paris, from 1988 to 1993. Since May 1993, he has worked on his own. His first furniture was produced by XO in 1991 and he opened his own agency in 1993. Elected as Créateur de l'année 1994, he steps into different worlds with his work including Furniture Design, Architecture and Interior Architecture, for JC Decaux, Trussardi, Moët et Chandon, Lancôme, Ecart International, Shiseido, Bally, l'Oréal, JC Jitrois, Whirlpool and Veuve Clicquot.


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When an elevated highway is demolished to make way for a park, how does Art respond to such contrast? Find out how the Rose Kennedy Greenway park in Boston is serving as a bustling canvas for artists.
When an elevated highway that's long disrupted your city is finally destroyed, how do you turn its memory into something beautiful? The Rose Kennedy Greenway parks came as a breath of fresh air to residents of Boston in the 1990's, after the highway that once divided parts of the city was replaced by a tunnel system to make way for public space. A mile-and-a-half long oasis now lies where the highway once stood, between the towering glass and steel buildings of the city's Financial District. Not only is the green belt dotted with colourful plants that attract pollinators, but art has also been identified as an integral way to add life to the Greenway. But how do artists respond to such contrast, to such memory and restoration?
Without so much as a preamble, artist Sharah Hughes plunges us headlong into a hallucinatory world where caverns rise to frame a totally surreal landscape of waterfalls against the backdrop of a building facade. A crack seems to open up in the middle of the city, like a portal to another reality – perhaps it shows us a window into what existed here long before the elevated highway, perhaps in the time of the dinosaurs. Carving Out Fresh Options is a portal into a dream-like natural world. Its garish combination of colours claw at the monochrome fabric of the city.
Brooklyn-based Aakash Nihalani goes on to puzzle us even more with his cubes performing Balancing Acts. You might be forgiven for thinking for a moment that something's terribly amiss – did a space traveler from a two-dimensional cartoon planet just hijack your experience of the real world? Lending a false appearance of three-dimensionality, Nihalani's 2D figurines seem to be on the verge of collapse, prompting the human viewer to launch herself into an act of heroism and become intimately part of the work. With wry humour, Nihalani's Balancing Acts capture the tension between the orderly nature of the cubes and the imminent disorder that nature's force of gravity is about to subject them to. This "reflects the contrast of the Greenway against the surrounding urban landscape," says a write-up on the work.
Let the children remind us of the natural world even if we have forgotten it, a group of community organizations and artists seem to say. And so they do. Children of Boston were asked to sketch what they remember of the animals around Boston. They sketched sea turtles seen in the Boston aquarium, giant mythical sea serpents, whales far out in the sea, foxes glimpsed in the forest and squirrels in the park. To immortalize the natural world of the region, a host of artists then translated the children's sketches to create The Greenway Carousel. Unlike any other typical horseback carousel, it brings alive a host of lively animals figures crafted with taste.
Almost following suit is an elegant sculpture of a Giraffe at the Federal Reserve Bank of Boston that seems to longingly stride towards the Greenway from the hold of its concrete premises. Scrap metal seems to turn to muscle and sinew of the animal. It's as if the sculpture made by Madeleine Lord says that even a 10-foot-tall giraffe can seem tall in a district of skyscrapers when it has a vast horizontal vista to look at and not just planes in its face.
A spindly 'tunnel' made in wireframes by the duo of artists called Luftwerk is aptly called Transition and pays homage to the underground tunnel that made it possible to replace the elevated highway. It celebrates the new connection that this brave act of urban planning has restored between parts of the city that were previously divided by the highway. Like a vortex, the tunnel stretches a threshold moment so it can truly be experienced in time for the power of what this act has done for the city.
As if to compensate for all the nostalgia over nature, the Greenway then meets us with a host of neon advertising signs. At first, I'm appalled at the display of commercial ambitions. And then I read the fine print. The installation GLOW is meant as a way to appreciate the art of neon signs. Of course, neon signs have never been taken seriously in the pantheon of the art world, but they have, by every means, always served as a form of creative expression that was explored enthusiastically by family-run businesses. These signs might well be remembered by many Americans as being the much-loved landmarks that dotted the country's landscape from 1925 to 1970. The glowing sign of the Cycle Center promised to sell a sustainable means of travel in an increasingly automotive age for affordable prices. The locally produced State Line Potato Chips promised to deliver chips fresh, "the morning after they're made". At a time when commercial signs were becoming rather uniform and staid, the Flying Yankee restaurant paid ode to the Space Age with its creative rocket emblem.
Public art projects are so welcomed and encouraged in Greater Boston at large that the city might just serve as a precedent for public councils elsewhere in the world to take the integration of art into public life more seriously. What's the point of all this, you may ask? Simply to make you stop in your tracks and wonder, perhaps. Artist Hincman once installed a park bench at Jamaica Pond that looked every bit like your regular park bench except that it had two backs bending up to face each other. The uncommissioned "guerrilla" work was so witty and confusing that even the authorities opted in favour of having it remain there. Bumping into a work of art on your daily commute is simply an opportunity to allow yourself the joy of being perplexed.


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CONTRIBUTED PHOTO/VENTURA COUNTY FIRE DEPARTMENTA county helicopter rushed to the aid of Saturday's snakebite victim.
A woman in a Santa Monica Mountains hiking area Saturday became one of a handful of people who are bitten by snakes in Ventura County.
With the help of a helicopter, rescue crews evacuated her from the La Jolla Valley Trail area just north of the Pacific Coast Highway east of Mugu Rock. She was taken to a hospital after the incident that was reported just before 6 p.m., and information on her condition was not available.
Local fatalities from snakebites are rare, a paramedic said, but it's not something you want to take a risk with.
Snakebites usually increase in spring and summer as the reptiles come out of winter dormancy, said Joe Dullam, a firefighter and paramedic with the Ventura County Fire Department.
Dullam estimates that his department probably gets about a half dozen snakebite-related calls each year.
'It's important to remember that a snake is just as afraid of us as we are of them,' Dullam said, noting that anyone who encounters a snake should not make any quick movements. Instead, they should slowly walk away.
'A snake is normally not a threat unless you step on it,' Dullam said.
Anyone who is bitten should try to stay calm, he said.
'If you have a cellphone, call for help from where you're at,' he said.
Also, don't try to identify the snake, since hospitals are equipped to identify the venom from different snakes.
Dullam said he doesn't know of any snakebite-related fatalities during his time working for the county.
'Fortunately, fatalities are very rare,' he said.
Hikers should wear knee-high socks, high-top shoes or boots and long pants, experts say. They also should stick to open paths when possible, and avoid tall grass and heavy underbrush.
The snakebite victim wasn't the only person rescued from a hiking trail in the same area on Saturday.
Rescuers were sent Saturday evening to help an injured person on Overlook Trail. Crews were notified at 6:12 p.m. of the problem and planned to transport the patient from the scene. Crews on the scene said the patient had suffered a leg injury.


Hurricane-strength storms in the Mediterranean could hit the region with increasing power by the end of the 21st century, growing to robust Category 1 strength, according to a new study in the AGU journal Geophysical Research Letters.
Although Mediterranean tropical-like cyclones, known as "medicanes," are predicted to be less frequent in the future, they will develop a more robust hurricane-like structure and last longer, with higher winds and more rain, according to the new study. The new research predicts the change in storms will begin to emerge at the end of the century, from 2081 to 2100, with stronger storms appearing in the autumn.
Medicanes arise in the Mediterranean when an extratropical cyclone blunders into the sea basin and transforms to a more tropical cyclone-like storm, with symmetric structure and convective clouds circling a warm core and an eye-like center.
Extratropical cyclones are driven by temperature contrasts across the storm front and blow strongest in the tropopause, about 12 kilometers (8 miles) above Earth's surface. In contrast, tropical cyclones' strongest winds are at the surface, which can often be more damaging. Tropical cyclones are called hurricanes in the Atlantic and typhoons in the Pacific west of the International Dateline.
Currently, medicanes of tropical depression intensity or stronger occur a few times a year, but rarely reach the strength of a Category 1 hurricane. Tropical depressions have a maximum wind speed of 63 kilometers (39 miles) per hour.
"In their mature stage, medicanes are similar to hurricanes in the Caribbean," said Juan J. González-Alemán, a researcher at the University of Castilla-La Mancha in Toledo, Spain, and the lead author of the new study. "Even under an intermediate climate scenario, we will likely see a lower frequency of these storms, but when they occur, they will have a higher chance of reaching Category 1."
Other studies have predicted an increase in storm intensity in the Mediterranean with climate change, but the new study is the first to utilize a global coupled model, which combines atmospheric and ocean circulation models. Including ocean processes in the model is important for a realistic representation of medicanes, González said. The new model is more robust and addresses the precipitation intensity, tropicality and power dissipation indexes of future storms, according to González.
Tropicality is an indicator of how hurricane-like the storm's structure is, and power dissipation describes its potential for destruction. The new study predicts both tropicality and power dissipation will increase in magnitude in the coming century. The model could not discard the possibility that storms may reach Category 2 strength, although the main finding is for strong Category 1 storms, González said.
A tropical storm becomes a Category 1 hurricane when sustained winds exceed 119 kilometers (74 miles) per hour and a Category 2 at 154 kilometers (96 miles) per hour.
"The Mediterranean Sea is over-populated, so though smaller than Caribbean hurricanes, the impact on society from medicanes may be worse. They have a high chance of impacting people and societal interests," González said.


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\section*{Acknowledgements}
The authors acknowledge the financial support of the funding agencies:
Centre National de la Recherche Scientifique (CNRS), Commissariat \`a
l'\'ener\-gie atomique et aux \'energies alternatives (CEA),
Commission Europ\'eenne (FEDER fund and Marie Curie Program),
Institut Universitaire de France (IUF), LabEx UnivEarthS (ANR-10-LABX-0023 and ANR-18-IDEX-0001),
R\'egion \^Ile-de-France (DIM-ACAV), R\'egion
Alsace (contrat CPER), R\'egion Provence-Alpes-C\^ote d'Azur,
D\'e\-par\-tement du Var and Ville de La
Seyne-sur-Mer, France;
Bundesministerium f\"ur Bildung und Forschung
(BMBF), Germany;
Istituto Nazionale di Fisica Nucleare (INFN), Italy;
Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands;
Council of the President of the Russian Federation for young
scientists and leading scientific schools supporting grants, Russia;
Executive Unit for Financing Higher Education, Research, Development and Innovation (UEFISCDI), Romania;
Ministerio de Ciencia, Innovaci\'{o}n, Investigaci\'{o}n y
Universidades (MCIU): Programa Estatal de Generaci\'{o}n de
Conocimiento (refs. PGC2018-096663-B-C41, -A-C42, -B-C43, -B-C44)
(MCIU/FEDER), Generalitat Valenciana: Prometeo (PROMETEO/2020/019),
Grisol\'{i}a (refs. GRISOLIA /2018 /119, /2021 /192) and GenT
(refs. CIDEGENT/2018/034, /2019/043, /2020/049, /2021/023) programs, Junta de
Andaluc\'{i}a (ref. A-FQM-053-UGR18), La Caixa Foundation (ref. LCF /BQ /IN17 /11620019), EU: MSC program (ref. 101025085), Spain;
Ministry of Higher Education, Scientific Research and Innovation, Morocco, and the Arab Fund for Economic and Social Development, Kuwait.
We also acknowledge the technical support of Ifremer, AIM and Foselev Marine
for the sea operation and the CC-IN2P3 for the computing facilities.
\bibliographystyle{JHEP}

\section{The ANTARES neutrino telescope}
\label{sec:ANTARES}

The ANTARES detector is anchored at a depth of $\sim$ 2500~m on the Mediterranean seabed, 40~km offshore from Toulon \cite{ageron_antares_2011}. The ANTARES first detection line was deployed in 2006, and the apparatus reached its full configuration in 2008. Since then, the ANTARES detector has been taking data almost continuously.

ANTARES is made of 12 detection lines of 450 m height, spaced by about 60--75 m and distributed on an octogonal grid. Each line holds 25 storeys vertically spaced by about 14 m. Each storey hosts 3 optical modules (OMs), made of high-pressure resistant glass transparent to 400--500 nm photons, and a local control module containing the electronics \cite{aguilar_performance_2010, aguilar_data_2007}. The 12$^\textnormal{th}$ line has 20 storeys equipped with OMs, and 5 storeys with acoustic devices for neutrino detection \cite{aguilar_amadeusacoustic_2011} and additional instruments to measure environmental parameters \cite{Aguilar_2006}.

The main component of the OM \cite{amram_antares_2002} is a 10" photomultiplier tube (PMT), oriented 45$^{\circ}$ downward in order to optimise the detection of light induced by relativistic upgoing charged particles, and to mitigate the effect of sedimentation and biofouling \cite{Amram_2003}. A $\mu$-metal cage is used in order to shield the electron trajectory inside the PMT from the effect of the Earth magnetic field.

Photons impinging in the sensitive area of a PMT generate a signal called \emph{``hit''} \cite{aguilar_performance_2010}, which carries information of the arrival time and collected charge. The information of all recorded hits in the detector is used to reconstruct the direction and energy of the event. Apart from the light induced by charged particles yielded by the neutrino interaction in the detector surroundings (the signal), other background light sources are present, the dominant ones being: atmospheric downgoing muons, bioluminescence activity and $^{40}$K decays \cite{Amram_2000}. The influence of the environmental background over the overall signal is reduced by applying dedicated trigger algorithms \cite{ageron_antares_2011}.

Depending on the interaction process, neutrino induced events fall into two main ca\-te\-go\-ries: \emph{track-like} and \emph{shower-like} events. Charged Current (CC) interactions of $\nu_\mu$ and CC interactions of $\nu_\tau$ with a subsequent muonic decay produce a long-range muon, the so-called \emph{track-like} event topology. All other neutrino interactions, both CC and Neutral Current (NC), produce a cascade of charged particles, and are classified as \emph{shower-like} events.

The ANTARES median angular resolution for muon \emph{tracks} ranges from $1^{\circ}$ for energies below 1 TeV, to better than $0.4^{\circ}$ for neutrino energies above 10 TeV \cite{ageron_antares_2011}.

\section{Analysis}
\label{sec:Analysis}

\begin{figure}[t]
	\centering
	\includegraphics[width=0.49\textwidth]{./Plots/PSFs_CR_1.png}
	\includegraphics[width=0.49\textwidth]{./Plots/SPSFs_CR_and_BG_1.png}\\
	\hspace*{0.01cm}
	\includegraphics[width=0.49\textwidth]{./Plots/PDF_beta_1.png}
	\includegraphics[width=0.49\textwidth]{./Plots/PDF_nhits_1.png}\\
	%
	\caption{Signal (blue) and background (red) PDFs used as inputs in the likelihood function (eq.~\ref{eq:likelihood}). On the top, the PDFs of the angular distance between the direction of the reconstructed track and the position of the Sun ($\Psi_\odot$) are plotted before (left) and after (right) normalising to the solid angle. The bottom plots show the PDFs of the $\beta$ (left) and $N_\text{hits}$ (right) parameters. The plots correspond to the baseline model with the final cuts applied ($\Lambda > -5.2$, $\beta<1^\circ$ and $\theta_\text{zenith} > 90^\circ$).}
	\label{fig:sig_bg_pdfs}
\end{figure}

The Sun is a moving source in the local sky coordinate system, therefore the signal of SA$\nu$s is expected to be found along the solar path (figure \ref{fig:Sun_path}). Discriminating variables, such as the reconstructed angular distance to the source, $\Psi_\odot$, the error estimate in the reconstructed angle, $\beta$, and the number of hits used for the track reconstruction, $N_\textnormal{hit}$, are used to identify the signal. The normalised distributions of these variables are used as probability density functions (PDFs) in an extended likelihood function, $\mathcal{L}(n_\text{sig})$, (eq.~\ref{eq:likelihood}).

\begin{equation}
	\small
	\mathcal{L}(n_\text{sig}) = e^{-(n_\text{sig} + n_\text{bkg})} \prod_i^{N} \left[n_\text{sig} \cdot \mathcal{S}(\Psi_{\odot,i}, \beta_i, N_{\text{hit},i}) + n_\text{bkg} \cdot \mathcal{B}(\Psi_{\odot,i}, \beta_i, N_{\text{hit},i}) \right].
	\label{eq:likelihood}
\end{equation}

The signal ($\mathcal{S}$) and background ($\mathcal{B}$) PDFs are shown in figure \ref{fig:sig_bg_pdfs}. They are built from simulated data \cite{albert_monte_2021} weighted with the SA$\nu$ flux \cite{edsjoe_neutrinos_2017} and scrambled data, respectively. To evaluate the signal significance, a large set of \emph{pseudo-experiments} (PE), or \emph{skymaps}, are generated injecting a number of signal events, $n_\text{sig}$, according to the signal PDF, over the total number of detected events in the data sample $N = n_\text{sig} + n_\text{bkg}$, where the $n_\text{bkg}$ represents the expected number of background events.

The excess of events in the solar path is searched for using the unbinned likelihood method \cite{neyman_outline_1937, albert_first_2017}. The likelihood maximisation process runs over the total number of reconstructed events within a Region of Interest (RoI) of $30^\circ$ around the Sun. Due to the small extension of the source, it is possible to constrain the search to this RoI, preserving a good number of reconstructed events without missing information and speeding up the maximisation process. The outcome of the maximisation is the number of signal events, $\hat{n}_\text{sig}$, which maximises the likelihood for each skymap.

The significance of an observation of a given number of signal events $\hat{n}_\text{sig}$ is evaluated through a test statistic, TS, defined as the ratio between the maximum and the background-only likelihoods:

\begin{equation}
\text{TS} = \log_{10}\left(\dfrac{\mathcal{L}(\hat{n}_\text{sig})}{\mathcal{L}(0)} \right).
\label{eq:TS}
\end{equation}

\begin{figure}[t]
	\centering
	\includegraphics[width=0.75\textwidth]{./Plots/Schematic_Sensitivity_calculation.pdf}
	%
	\caption{Schematic of the sensitivity calculation. The blue curve represents the TS distribution for zero number of injected signal (background-only hypothesis). The orange curve is the TS distribution for a number of signal events ($n_s$) injected on the skymaps (signal hypothesis), corresponding to the sensitivity. This curve has the 90\% of the distribution over the median TS of the background distribution. The upper limit is computed similarly, but instead of comparing with the TS of the median of the background distribution, the measured TS is used.}
	\label{fig:schematics}
\end{figure}

The sensitivity of the detector is defined as the 90\% CL median upper limit, which is computed by comparing the background TS distribution to the signal plus background TS distributions (see figure~\ref{fig:schematics}) \cite{neyman_outline_1937}. The measured upper limit is computed from the observed TS after unblinding the data.  If the observed TS is below the median of the TS background distribution, the upper limit is set equal to the sensitivity.

If no signal is observed, a limit on the neutrino flux is computed from the limit on the number of signal events, $n_\text{sig}^{90\% \text{CL}}$, according to the following expression:

\begin{equation}
\dfrac{d \Phi^\text{90\%\ CL}_{\nu_\mu} (E)}{dE} =
\dfrac{n^\text{90\%\ CL}_\text{sig}}{\bar{n}^\text{theor}_\text{sig}}
\dfrac{d \Phi^\text{theor}_{\nu_\mu} (E)}{dE}=
C_{90} \cdot
\dfrac{d \Phi^\text{theor}_{\nu_\mu} (E)}{dE}
.
\label{eq:flux_sensi}
\end{equation}

The first term in equation \ref{eq:flux_sensi} corresponds to the flux upper limit. The second and third terms represent the theoretical flux model multiplied by a scale factor, $C_{90}$,  defined as the ratio between $n_\text{sig}^{90\% \text{CL}}$ and the expected number of signal events $\bar{n}^\text{theor}_\text{sig}$ detected. The expected number of signal events $\bar{n}^\text{theor}_\text{sig}$ is computed in the following way:

\begin{equation}
\bar{n}^\text{theor}_\text{sig} =
T \displaystyle\int{
\sum_{l\in \nu_\mu, \bar{\nu}_\mu}{
\left( \dfrac{d \Phi^\text{theor}_{l} (E)}{dE} A^\text{eff}_{l} (E) \right) dE}},
\label{eq:nsig_expected}
\end{equation}

\noindent where $T$ is the livetime of data taking, $A^\text{eff}$ is the ANTARES effective area for this analysis (see figure \ref{fig:Aeff}), and ${d \Phi^\text{theor}_{l} (E)}/{dE}$ is the theoretical flux model.

\begin{figure}[t]
	\centering
	\includegraphics[width=0.65\textwidth]{./Plots/ANTARES_Effective_Area_Sun.pdf}
	%
	\caption{ANTARES effective area for $\nu_\mu$, $\bar{\nu}_\mu$ and the sum of the two, arriving from the Sun direction, for the final cuts that optimise the sensitivity ($\Lambda>-5.2$, $\beta<1^{\circ}$ and $\theta_{\text{zenith}} > 90^{\circ}$).}
	\label{fig:Aeff}
\end{figure}

Given the excellent angular resolution of ANTARES for track-like events, and the small angular size of the Sun seen from Earth ($\theta_\odot  \sim 0.5^{\circ}$), most of the sensitivity to SA$\nu$ comes from the $\nu_\mu$ CC channel. In order to avoid any bias, the event selection follows a \emph{blind} policy based on \emph{pseudo-experiments} before performing the analysis on data described in section \ref{sec:Analysis}.

As mentioned in section \ref{sec:data_set}, in the baseline scenario the \emph{H3a} CR model and the \emph{Ser+Stein} solar density profile are considered. Normal mass ordering and neutrino oscillation parameters from best-fits values are assumed \cite{edsjoe_neutrinos_2017, Esteban_2017}. Finally, the analysis is optimised for $\nu_\mu$ CC interactions arriving at the detector. Table~\ref{tab:SAv_sensitiv} shows the sensitivities and $C_{90}$ scale factors achieved for the final cuts, and the three source shapes considered.

The total data sample, after cuts, consists of $7 071$ tracks, with a livetime of 3022 days. The contribution to the data sample estimated from the MC is:  $\nu_\mu \text{ CC} \simeq 84.7\%$, atm. $\mu \simeq 14.8\%$ and $\nu$ NC + $\nu_e$ CC $\simeq 0.5\%$.

\newcolumntype{P}[1]{>{\centering\arraybackslash}p{#1}}
\newcolumntype{M}[1]{>{\centering\arraybackslash}m{#1}}
\begin{table}[h]
    \centering
	\begin{tabular}{c|c|c||c|c|c|c|c|P{1cm}}
	$\Lambda$ & $\beta$ [deg] & $\theta_\text{zenith}$ [deg] & $n^{\text{Point}}_{_{90}}$ & $n^{\text{Ring}}_{_{90}}$ & $n^{\text{Disk}}_{_{90}}$ & $\bar{n}_\text{sig}^{\text{theor}}$ & $C_{90} = \dfrac{n^{\text{Point}}_{_{90}}}{\bar{n}_\text{sig}^{\text{theor}}}$ & Total events \\
	\hline \hline
	 $-5.2$ & $1.0$ & $ 90$ & $2.70$ & $3.45$ & $2.80$ & $0.37$ & $7.4$ & $7071$\\
	\end{tabular}
	\caption{Sensitivity ($n_{_{90}}$), expected signal from model ($\bar{n}_\text{sig}^{\text{theor}}$), scaling factor $C_{90}$ and total number of events for the final cuts. Period from 2008 to 2018 (3022 days of livetime). The percentage of expected signal falling inside the RoI is about $99.6\%$.}
    \label{tab:SAv_sensitiv}
\end{table}

\section{Results and conclusions}
\label{sec:Results}

In the baseline scenario, the expected number of signal events is $\bar{n}_\text{sig}^\text{theor} = 0.37$ within the RoI, for the 3022 days of livetime. The expected number of background events is $n_\text{bkg}^\text{MC} = 470$. The number of detected events in the data sample contained in the RoI is 461. No excess of SA$\nu$ signal over the expected background is observed in the 11 years of analysed data.

The 90\% CL upper limit obtained after analysing the unblinded data is $n_\text{sig, up-lim}^\text{90\% CL} = 3.15$, corresponding to a flux scale factor of $C_\text{90, up-lim}= 8.6$. The value of this scale factor indicates the possibility of excluding at 90\% CL the tested model. A value smaller than one will directly constrain the model. In this study the flux that can be constrained is 8.6 times larger than the one of the baseline model. Figure \ref{fig:cos_psi} shows the distribution of the events within the RoI of $30^\circ$ around the Sun, for the expected signal (blue histogram) and background (green line), alongside the observed data (black dots). The signal is magnified by a factor 8.6 for comparison. Table \ref{tab:sensi} shows the sensitivities and upper limits for the three Sun shapes considered, as well as the corresponding \emph{p-values}. Figure \ref{fig:ant_upp_lim} presents the sensitivity (dotted red line) and the 90\% CL upper limit (solid red line) on the SA$\nu$ flux for the ANTARES detector over 11 years of data taking. The theoretical flux model (solid blue line) and latest upper limit results obtained by the IceCube collaboration (solid black line) \cite{IC_solarnu_2021} are shown for comparison.

\begin{figure}[h]
	\centering
	\includegraphics[width=0.7\textwidth]{./Plots/Distance_from_source_cos_log_sim_masbin4.pdf}
	\caption{Event distribution as a function of the reconstructed angular separation $\Psi_\odot$ around the Sun. The expected signal, in blue, is scaled up by a factor 8.6. The expected background (green line) is shown with a $2\sigma$ band along the data (black dots).}
	\label{fig:cos_psi}
\end{figure}

\begin{table}[h]
    \centering
    \begin{tabular}{l||lccc}

        Model & Sun Shape & $n^\text{90\% CL}_\text{sig, sens}$ & $n^\text{90\% CL}_\text{sig, up-lim}$  & \textit{p-val} \\
        \midrule\midrule
        \multirow{3}*{\textit{H3a-Ser+Stein} \cite{Gaisser_2012, serenelli_new_2009}} & Point-like & 2.70 & 3.15 & 0.41 \\% & 0.22 $\sigma$\\
        & Filled disk & 2.80 & 3.25 & 0.43 \\% & 0.19 $\sigma$ \\
        & Ring-shaped & 3.45 & 3.45 & 0.50 \\%& 0.0 $\sigma$\\

    \end{tabular}
    %
    \caption{Sensitivities and 90\% CL upper limits for the baseline Solar Atmospheric neutrino model, and for three different Sun shapes considered. The last column shows the \textit{p-values} corresponding to the quoted upper limits.}
    \label{tab:sensi}
\end{table}
The \emph{GST4} cosmic ray model and the \emph{Ser+GS98} solar density profile, which are already included within the \texttt{solar\_crnu} package available in WimpSim, have been tested in combination with the models used in the baseline scenario (see figure \ref{fig:SAV_flux_vs_honda}), and the results are within a 2\% difference with respect to the values shown in table \ref{tab:sensi}.

\begin{figure}[h]
	\centering
	\includegraphics[width=0.8\textwidth]{./Plots/Solar_Flux_limits_comparative_with_bands.pdf}
	%
	\caption{ANTARES upper limit (solid red) and sensitivity (dashed red) for 11 years of data, assuming the Sun as a point-like source for the baseline model \textit{H3a-Ser+Stein} (solid blue line). For comparison, the current 6 years IceCube upper limit \cite{IC_solarnu_2021} is also shown (solid black line). The ANTARES limit and sensitivity lines expand in the energy range which contains 90\% of the expected number of events.}
	\label{fig:ant_upp_lim}
\end{figure}

After analysing 11 years of ANTARES data, corresponding to 3022 days of total livetime, with an unbinned likelihood method, using three different sun shapes, no signal evidence of SA$\nu$s is observed. As a result, assuming the  {\it GST4} cosmic ray model, a 90\% CL upper limit on the flux of 7$\times$$10^{-11}$ TeV$^{-1}$cm$^{-2}$s$^{-1}$ at $1$ TeV is established. Comparing our result with that of the IceCube telescope (which has a much larger instrumented volume than ANTARES) it is evident that the detection of the SA$\nu$s signal relies not only on the detector size, but also on its angular precision (to significantly decrease the number of Earth atmospheric neutrinos entering in the $\Psi_\odot$ window) and energy estimation of the neutrino candidates (due to the different $\nu_\mu$ energy fluxes for SA$\nu$ and Earth neutrinos, figure~\ref{fig:SAV_flux_vs_honda}). In this context, the advent of the new neutrino telescope in the Mediterranean Sea (the KM3NeT detector \cite{adrianmartinez_letter_2016}) that will improve both the mentioned requirements would represent a significant progress toward the important observation of SA$\nu$s.
\section{Introduction}
\label{sec:Introduction}
In addition to the electromagnetic radiation, the Sun is also a source of neutrinos.\footnote{Hereafter, the word \emph{neutrino} refers to both, $\nu$ and $\bar{\nu}$ unless otherwise specified.}
An intense flux of neutrinos is generated by nuclear fusion reactions in the Sun core at MeV energies \cite{Antonelli2013, Bahcall1989, Haxton2013}. At higher energies (GeV to TeV), an additional flux of neutrinos is expected from the Sun direction, coming from the decay products of the Cosmic Rays (CRs) interacting in the Sun. The flux of these neutrinos, so-called Solar Atmospheric Neutrinos (SA$\nu$s), would then reach the Earth \cite{Moskalenko_1993,masip_high_2018} after being modulated by oscillation phenomena. SA$\nu$s represent an unavoidable source of background for Dark Matter (DM) indirect searches \cite{adrianmartinez_limits_2016, AdrianMartinez2016, Ng2017, argueelles_solar_2017, navas_dark_2019}, even though the sensitivity of current experiments has not yet been able to determine the intensity of their flux. The detection of SA$\nu$s would allow for the characterisation of this potential background. In addition, it also can shed light on understanding of the primary CR composition, the solar density or even the parameters of neutrino oscillation \cite{edsjoe_neutrinos_2017}.

Even though the production mechanism of SA$\nu$s is similar to the one of the terrestrial atmospheric neutrinos, the flux of SA$\nu$s is expected to be slightly harder. Indeed, since  the solar atmosphere is less dense than the Earth's atmosphere, the secondary particles pro\-du\-ced by the CR interaction are more likely to decay than to interact in the solar medium. Considering that at sufficiently large depth in the solar medium almost every secondary CR would have decayed, the overall neutrino production occurs on the solar surface. The flux ratio at production site is approximately $\{ \nu_e \}: \{ \nu_\mu \}: \{ \nu_\tau \} = 1:2:0$. However, the final neutrino flux at Earth, after oscillations, has a flavour ratio of $1:1:1$ \cite{edsjoe_neutrinos_2017}. Since the solar density and composition play a crucial role in the final neutrino flux, several models have been proposed in the literature \cite{serenelli_new_2009, Hettlage_2000,Grevesse_1998, Seckel1991}.

In this paper, a search for SA$\nu$s using 11 years of ANTARES data (2008--2018) is presented.  The outline of the paper is the following: in section \ref{sec:ANTARES}, the ANTARES detector, the event topologies and the main background sources present in a neutrino telescope are des\-cribed. The ANTARES simulation and reconstruction chain, as well as the event selection and the different models tested in the analysis, are presented in section \ref{sec:data_set}. Section \ref{sec:Analysis} describes the strategy used to search for an excess of SA$\nu$s over the background. Finally, the results and conclusions of the analysis are presented and discussed in section \ref{sec:Results}.

\section{Simulation, reconstruction and event selection}
\label{sec:data_set}

\begin{figure}[t]
	\centering
	\includegraphics[width=0.7\textwidth]{./Plots/sav_fluxes_vs_honda_flux.pdf}
	\caption{Muon neutrino energy fluxes, from the four different models tested in this work (see details in the text), after neutrino propagation, at the Earth position (color lines). Normal ordering and neutrino oscillation parameters from the world best-fit values are assumed. The Honda flux for Earth atmospheric muon neutrinos is shown for comparison (black dashed line) \cite{Honda_2007}. Fluxes are integrated over the solar solid angle $\Omega_\odot \simeq 6.8 \times 10^{-5}$ sr.}
	\label{fig:SAV_flux_vs_honda}
\end{figure}

The full neutrino detection process with the ANTARES detector is simulated. First, particles and their properties (energy, charge, angular information) are generated (GENHEN \cite{bonis_genhen_2014} for neutrinos, CORSIKA \cite{heck_corsika_1998} and MUPAGE \cite{carminati_atmospheric_2008} for cosmic rays and atmospheric muons). Then, particles are propagated and tracked through the detector, and Cherenkov photons are simulated and propagated to the optical modules. Finally, the data acquisition system is simulated. The environmental conditions, bioluminescence processes and sea current changes to which an undersea neutrino telescope is exposed, may affect the trigger and data acquisition system. In order to reproduce the detector response under these conditions as accurately as possible, a Monte Carlo \emph{run-by-run} strategy \cite{albert_monte_2021} is followed, in which the atmospheric muons and neutrino interactions are simulated according to the corresponding detector state.

Once the trigger algorithms have filtered the interesting events, the energy and direction are reconstructed from the positions and times of photomultiplier hits. The quality of the track reconstruction is given by the parameter $\Lambda$, which is a maximum likelihood estimator obtained with a multi-line reconstruction fit of hits passing a pre-defined threshold condition \cite{adrianmartinez_search_2012}. The algorithm provides also a parameter related to the uncertainty on the recontructed direction, $\beta$. The energy reconstruction follows two main strategies \cite{Schnabel_2013}. The first one uses the total muon energy loss per amount of matter traversed as an energy estimator. The other main estimator uses an artificial neural network to derive the dependece between a set of observables and the energy estimate.

A set of selection cuts is applied on the reconstruction parameters \cite{AdrianMartinez2013, Adrian_Martinez_2014} in order to obtain a sample of well reconstructed neutrino events and reject as much background of atmos\-pheric muons and noise as possible. The atmospheric muon background is heavily reduced by selecting upward-going events ($\theta_\text{zenith} > 90^\circ$). Surviving events mis-reconstructed as upgoing are removed by using cuts on the parameters related to the quality of the reconstruction algorithm, $\Lambda$, and of the uncertainty on the reconstructed direction, $\beta$.

In this analysis, the CR models \emph{Hillas-Gaisser 3-generation model (H3a)} \cite{Gaisser_2012} and the \emph{Gaisser-Stanev-Tilav 4-generation model (GST4)} \cite{Gaisser_2013} have been tested as signal components, as well as the \emph{Ser+Stein} \cite{serenelli_new_2009} and the \emph{Grevesse \& Sauval} (referred to as \emph{Ser+GS98}) for the solar density profiles \cite{Grevesse_1998}. These models are included within the \emph{WimpSim 5.0} simulation package \cite{edsjoe_wimpsim_2019, blennow_neutrinos_2008}. Neutrino oscillation parameters from world best-fit values \cite{Esteban_2017} and normal mass ordering are assumed.
In addition, the spatial distribution of the incoming neutrinos are simulated following three different shapes for the Sun: {\it a)} point-like, i.e., SA$\nu$s are emitted from a single point in the sky coincident with the Sun centre; {\it b)} filled disk shape, with neutrinos produced uniformly from a disk of $0.27^\circ$ radius; {\it c)} ring-shaped, in which the outcoming neutrinos are yielded close to the Sun surface and orthogonally with respect to the direction to the Sun centre (inner radius of $0.26^\circ$ and outer radius of $0.27^\circ$).

The reference case selected for this analysis uses the \emph{H3a} CR model with the \emph{Ser+Stein} solar density profile, and considers the Sun as a \emph{point source}({\it baseline} case). The signal consists of $\nu_\mu$ CC simulated events, weighted with the SA$\nu$ energy spectra. Figure \ref{fig:SAV_flux_vs_honda} shows the signal spectra corresponding to the four tested models, alongside the Earth atmospheric neutrino flux according to \textit{Honda} \cite{Honda_2007}. The Honda flux dominates for neutrino energies below $\sim 40$ GeV, while the SA$\nu$ flux prevails for $E_\nu \gtrsim  40$ GeV. The difference between the solar solid angle (for the signal) and the \emph{all-sky} solid angle (for the background) reduces the conventional atmospheric neutrino rate at the detector by a factor $\Omega_\odot / 4\pi \simeq 5.4 \times 10^{-6}$.

The signal has been simulated using the Monte Carlo (MC) sample corresponding to 11 years of ANTARES data weighted with the SA$\nu$s flux models. For the background, 11 years of ANTARES data (2008--2018) scrambled in right ascension (RA) were used. This process, which circumvents the systematics from the MC simulation of the background, consists in replacing the real measured RA angle with a random number between $0$ and $2\pi$.

\begin{figure}[t]
	\centering
	\includegraphics[width=0.75\textwidth]{./Plots/Sun_Path_2008.pdf}
	\caption{Solar path for the 2008--2018 period as seen from the ANTARES site. The red (yellow) dashed line shows the solar path on January (July) $1^\text{st}$, as a reference.}
	\label{fig:Sun_path}
\end{figure}

redpajama_set_name: RedPajamaArXiv


text:
James W. Covert
Chairman of the House Committee on Patents
Chairman of the House Committee on Agriculture
from New York's 1st district
March 4, 1889 – March 3, 1895
Perry Belmont
Richard C. McCormick
Henry B. Metcalfe
New York State Senate (1st District)
(1842-09-02)September 2, 1842
Oyster Bay, New York
May 16, 1910(1910-05-16) (aged 67)
James Way Covert (September 2, 1842 – May 16, 1910) was a United States Representative from New York.
Born at Oyster Bay, he attended the public schools and received an academic education in Locust Valley. He studied law, was admitted to the bar in 1863, and commenced practice in Flushing. He was district school commissioner from 1867 to 1870, assistant prosecuting attorney of Queens County, and Surrogate of Queens County from 1870 to 1874.
Covert was elected as a Democrat to the 45th and 46th United States Congresses, holding office from March 4, 1877 to March 3, 1881. He was Chairman of the House Committee on Agriculture (46th Congress). He was a member of the New York State Senate (1st D.) in 1882 and 1883.
He was elected to the 51st, 52nd and 53rd United States Congresses, holding office from March 4, 1889 to March 3, 1895. He was Chairman of the House Committee on Patents (53rd Congress). Covert moved to Brooklyn in 1896 and resumed the practice of law. He died in Brooklyn in 1910; interment was in Mount Olivet Cemetery in Maspeth.
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Henry B. Metcalfe Member of the U.S. House of Representatives
from New York's 1st congressional district
Perry Belmont Member of the U.S. House of Representatives
John Birdsall New York State Senate
James Otis
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142 What About K-6 and 7-12?
What About K-6 and 7-12?
����������� Q. For a generation, we've had the grade school, middle school and high school concept in most public-school districts. But people aren't happy with what happens in the middle. They say it's a black hole, academically. Successful private schools usually don't have middle schools. Perhaps we should copy them. Should we get rid of middle schools and go back to the "grammar school" and "secondary school" structure?
����������� Possibly. That might be a productive change, although there is evidence on both sides of the coin on whether it would pay off.
����������� The "junior high" concept was intended to cushion young adolescents from the sometimes inappropriate pressures of being around older adolescents. But unfortunately, especially on the high end and low end of the achievement scale, the middle school concept seems to be counter-productive. It appears to have contributed to an epidemic of dropping out in the lower-income areas, and concerns in higher-income areas that it's just a "holding pen" until stronger students can get into high-school honors classes.
����������� Most private schools offer an elementary track, usually K-8 but increasingly K-6, and/or a secondary track, which is usually Grades 9-12, but increasingly, Grades 7-12. It is thought that making one fewer transition to a new school, new peers, new teachers, new curriculum and new expectations is better than the grade school / middle school / high school model.
����������� Those who support the middle-school concept counter that good teaching and a good school environment mean a lot more than what grades are clustered together in the same building.
����������� However, secondary educators who focus on at-risk kids, and those at the upper levels of the� academic ladder, appreciate a chance to work with students two years earlier in their schooling careers. They can begin grooming seventh-graders for challenging college-prep high school work, and mentor the stronger students so that they can achieve even more.
����������� They say the vast majority of inner-city students have the same problem: they can't read very well. With a� hyperfocus on reading and writing instruction, those same students can be brought up to speed and prepared for high school by the same education staff who then are responsible for preparing them for college.
����������� That's especially a good idea for dropout prevention, educators in inner-city campuses say, since reading disability is the No. 1 correlate of dropping out. Simply giving kids hope that they can handle college-level work might be all the help they need.
����������� For example, consider University Park Campus School in Worcester, Mass. It's a Grades 7-12 public school that has had extraordinary success with kids from working-class families. It demands that they take honors-level curriculum, and over the past several years, every single one of its graduates so far to college. Ninety-five percent of those graduates are the first ones in their families to achieve post-secondary education status.


African-American legacies, and the legacies of all of the many different people and cultures of the African diaspora, need to be identified, documented and shared much more widely than they presently are. Legacies offer lessons that are important for everyone-- today and for our future generations. These are the land, properties and true-life stories that represent past and present resilience, creativity and perseverance.
The Clemmons Family Farm represents a unique legacy for many reasons. Most importantly, it is one of the very few African-American-owned farms remaining in Vermont and New England. A large and beautiful property, the Farm has 148 acres of prime farm land, forests, woodlands and wetlands full of wildlife, and six historic buildings dating back to the late 1700's-early 1800's. The Farm's legacy also includes the remarkable stories of the owners, Dr. Jack and Lydia Clemmons- now in their 90's- and their families' resilience and achievements over 150 years of African-American history. Their oral histories and storytelling share fascinating chapters in the lives of their families, beginning with slavery in the 1800's in the rural south, segregation and Jim Crow, the Great Migration to the mid-west and California, World War II, and eventually life on a farm in a small rural town in Vermont. Jack and Lydia were among the first African-Americans on staff and faculty at the University of Vermont medical center and hospital. They have been vibrant and beloved members of their local and extended communities ever since moving to Vermont in 1962.
Holding on to farms and property is an important legacy for all people, and especially for African-Americans and other populations who have lost so much of their lands through social and economic injustices. There are 1 billion acres of farmland in the United States. During this century, African-American land ownership in the United States has dwindled from 41 million acres of land to less than 4 million acres of land. In Vermont, among nearly 7000 farms only about 19 are African-American-owned, and of the 1.2 million acres of farm land in the state, only 740 acres are African-American-owned.
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Partly cloudy this morning with thunderstorms becoming likely this afternoon. A few storms may be severe. High 71F. Winds SSE at 10 to 15 mph. Chance of rain 90%..
Showers and thunderstorms likely. Low 62F. Winds SSE at 10 to 15 mph. Chance of rain 100%. Locally heavy rainfall possible.
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