We have asked both Tom and Digigurl some questions about what's happening with Yellow, and they both replied. Here is a combined report on their answers. Because of technical hassles we had to do the interviews by email. The interview is on this page.
New Object yard for Yellow Digigurl is currently building a new object yard for Yellow. There will be a number of categories that will be linked to a hub teleport located in the bottom right hand corner of the screen. Categories include: indoor furnishings, outdoor building pieces, and miscellaneous. Each part of the yard will be spaced 200 meters apart to attempt to avoid lag. Digigurl states that the yard should be up and running soon.
Ozman has been accepted as a Teacher's Aide in AWSchool. His hours there will be Tuesday and Wednesday 10-12pm VRT. He may be found there at other times as well.
AWSchool is setting up a new university too. The AWNewsletter and the AWSchool websites will provide further details. Be sure to take note of when the AWSchool workshops and classes are on; they are run by specialists and can provide you with an immense amount of help in your building.
Cut the salmon into 1" chunks and place in the bowl of a food processor. Pulse rapidly several times until the salmon is finely chopped.
Add breadcrumbs, mustard, shallot and cayenne and pulse until blended.
Form the salmon mixture into 6 patties. Lightly oil and season just before cooking.
Pan sear or broil for about 3 minutes on each side until golden.
After three consecutive blizzards, the intrepid Old Winter Mountain Fire and Rescue team has managed to get the roads open to Upper and Lower Kringle Village. Be sure to visit the Sleepy Bear Play house where you can dance and listen to the ever popular PK toons. You can take a walk thru upper Kringle village. Catch a sled ride at the reindeer barn that will take you through the snow sculptures to lower Kringle valley were you can ride the Skylift and dare to try the giant bear scoot slide. Play games at the snow carnival. Visit the Kringle Factory, and even say hi to Santa. And be sure to give the Blizzard Ball game a try. There's lots fun to be had and sights to see.
This month, in Builds of the Month, we feature the Winter Wonderland Village. This was a very fun contest with lots of great builders who created some wonderful sights to see. We also bring you Old Winter Mountain, and the Snow Carnival by Apooka and Ozman. This was a build that was long in the making, but we are sure you will find it well worth it.
In Building Tips, we introduce some new features that AW has put into the latest versions of the program (AW 5.1).
Fuzzy's tale continues with some interesting twists and turns, and this month we feature two episodes. Little Nellie's Garden brings more interesting plant facts and pictures, with free plant graphics for you to use.
Dora stood there not saying a word, her face turning a bright scarlet. Her bottom lip began to quiver. Fuzzy braced himself for what he was sure would be a fierce temper. "You!" Dora nearly shouted. Before either of them could think or say another word. Shakey and Nora walked up, and to Fuzzy's relief Dora seemed to relax or was it retreat, he mused.
"Did you tell him?" Nora asked Dora in a firm motherly tone. "Well?"
"No, I did not." Dora mumbled.
"Well do you not think it is about time you did? We are waiting," said Nora. Nora began tapping her foot as to put a measure of pressure on the point.
"Hold on" said Fuzzy, "Look , now I'm not sure what is going on ,but let us not ruin a great night with bad feelings, What do ya say we all go have a sit down, and I for one could use something to eat, how about you Shakey ?" Said Fuzzy, with a wink and a plea in his eye.
"Sounds good to me, I am about half starved." said Shakey, "Come on Nora, Joe makes the most amazing salmon burgers". He smiled and gave her a hug then quickly directed her toward the food tent. She giggled as they walked and cooed "You do know what I like".
Fuzzy turn to Dora, "Come on Dora you will really enjoy them, honest." She squinted her eyes stared at him for second then turned and huffed off toward the food tent. Fuzzy was in such a great mood he did not care what drama maybe waiting at that moment, he just wanted a great night to last.
Two Eskimos sitting in a kayak were chilly, but when they lit a fire in the craft, it sank, proving once again that you can't have your kayak and heat it, too.
A woman has twins and gives them up for adoption. One of them goes to a family in Egypt and is named "Ahmal." The other goes to a family in Spain; they name him "Juan." Years later, Juan sends a picture of himself to his birth mother. Upon receiving the picture, she tells her husband that she wishes she also had a picture of Ahmal. Her husband responds, "They're twins! If you've seen Juan, you've seen Ahmal."
These friars were behind on their belfry payments, so they opened up a small florist shop to raise funds. Since everyone liked to buy flowers from the men of God, a rival florist across town thought the competition was unfair. He asked the good fathers to close down, but they would not. He went back and begged the friars to close. They ignored him. So, the rival florist hired Hugh MacTaggart, the roughest and most vicious thug in town to "persuade" them to close. Hugh beat up the friars and trashed their store, saying he'd be back if they didn't close up shop. Terrified, they did so, by proving that Hugh, and only Hugh, can prevent florist friars.
Mahatma Gandhi, as you know, walked barefoot most of the time, which produced an impressive set of calluses on his feet. He also ate very little, which made him rather frail and with his odd diet, he suffered from bad breath. This made him ....what? (Oh, man, this is so bad, it's good) A super callused fragile mystic hexed by halitosis.
And finally, there was a guy who sent ten different puns to friends, with the hope that at least one of the puns would make them laugh. Unfortunately, no pun in ten did.


Kip Moore made a special teenager's wish come true when he invited her to his show before she attends 2018 ACM Awards in Las Vegas.
In partnership with Make-A-Wish, Moore reached out to 15-year-old Sydney and asked her to be his guest at his upcoming concert for ACM Party for a Cause: Stoney's Tailgate Party on April 13.
"Because of my 'Last Shot' video and the power it's had, we teamed up with Make-A-Wish and we wanted to do something special for Sydney so I'm going to invite her to my show in Vegas during ACM week," Moore explains in the video above before he picks up the phone. "Have her come backstage, have her come hangout with me and my friends. Hopefully she's into it."
Of course, Sydney is in for it. The country superstar FaceTimes her to ask, and she can barely hold back her excitement, responding eagerly when Moore asks if she'd like to get the VIP treatment.
"Yes, sir! I'm so excited," she responds.
Sydney is from south Texas, and Make-a-Wish is sending her to the ACM Awards on April 15. She's a big music fan and hasn't been deterred by a critical illness she's been battling since birth. Her wish to attend the awards show will include Moore's set at Stoney's.
The 2018 ACM Awards air live on CBS at 8PM ET on April 15.


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text:
New York City Flexes Again, Extending Cap on Uber and Lyft
Author: Aarian MarshallAarian Marshall
In many ways, New York stands apart from other American cities. It's got yellow cabs and Broadway and these goofy things called boroughs. It has a sprawling subway system. Another way the city differs: New York regulates ride hailing more thoroughly. The city licenses Uber and Lyft vehicles, and collects information on where they drive. (In places like Los Angeles, Boston, and Austin, the state, not the city, regulates.) That's turned New York into the country's premier ride-hail regulation lab—often to the ride-hail companies' chagrin.
Aarian Marshall covers autonomous vehicles, transportation policy, and urban planning for WIRED.
New York is again flexing its control. On Thursday, Mayor Bill de Blasio announced the city would seek to maintain its almost year-old freeze on "for-hire vehicle" registrations, a category that includes black cars, livery cabs, limos, and vehicles hailed by app. About 80,000 of those vehicles—two-thirds of them—are operated by drivers working for ride-hail companies like Uber, Lyft, Via, and Juno. (There are 13,500 traditional taxicabs in the city.) De Blasio also said New York would force the ride-hail companies to cut down on how much time their drivers spend "cruising"—that is, waiting for their next rides, or driving to their next passengers.
Officials in New York and elsewhere say the ride-hail business model depends on crowding the streets with as many drivers as possible, keeping both wait times and driver wages low. That's not fair to workers, and it's not fair to the other New Yorkers who get stuck in traffic, de Blasio said Thursday.
Other cities have observed similar phenomena. A recent study blames ride hailing for the bulk of congestion increases in San Francisco between 2010 and 2016, though the study didn't account for other factors such as the growth of home delivery services.
According to a report released this week by New York's Taxi and Limousine Commission, 29 percent of all Manhattan traffic is now for-hire vehicles, and those cars spend 41 percent of their time empty (and not making their drivers money) as they pick up or wait for fares. (The report assumes that cars spend a lot of this downtime double-parked or circling the block, which would also affect traffic.) New York would like to force the companies to reduce such "cruising" to 31 percent by August 2020.
As for how New York would practically limit cruising—that's to be determined. The city is slated to post a more specific proposal next week. Both of these new ride-hail regulations will be subject to public hearings, and then a vote by the nine-member Taxi and Limousine Commission.
In a statement, Uber spokesperson Harry Hartfield said extending the cap would "create another medallion system," a reference to New York's 80-year-old system requiring a taxi owner to purchase a special license to operate in the city. The company suggests that the owners of licensed for-hire vehicles might sell or lease those licenses, and that prospective Uber drivers might have to rent more expensive licensed cars instead of using their own. In other words: Uber says the city is re-creating the system that ride-hail so successfully "disrupted"—and that the city allowed it to disrupt.
In fact, Uber sued the city in February over the ride-hail vehicle cap, arguing it unfairly affects riders in the outer boroughs. A state judge will hear the latest on that case on July 15.
At Lyft, a spokesperson said in a statement that congestion pricing would be a better solution to New York's traffic issues. The New York State legislature passed a first-in-the-country congestion charge plan for the busiest parts of Manhattan in March. But it's not yet clear how the new road charge might apply to ride-hail vehicles. Via, which operates a fleet of minivans, called the cap on for-hire vehicles "counterproductive," but the company said it supports rules to cut down on cruising.
In the past year, New York has implemented other rules that affect Uber and Lyft. It added a $2.75 surcharge to any ride-hail trip that begins, passes through, or ends below Manhattan's 96th Street, the most congested part of the city. (Taxis got an extra $2.50 fee.) The city also passed a law requiring ride-hail companies pay drivers a minimum wage of at least $17.22 per hour, which has netted them an estimated $172 million extra in pay since that rule went into effect in February. Lyft and another local ride-hail company, Juno, argued the city's rationale for its wage floor was biased towards Uber, and sued. A judge dismissed that case last month.
There's a reason ride-hail companies are so prickly about the rules in New York. It's one of their most important global markets. Uber's public S-1 filing shows New York is one of its top five markets globally, which are together responsible for nearly a quarter of all its bookings. As some guy once said: "If I can make it there, I'll make it anywhere." Ride-hail companies hope that goes for their business model, too.
Zoom Through Seattle's Nearly Completed SR-99 Tunnel
Now that Bertha's done digging, the new underground highway is nearly ready for human travelers. Fly through the project from a drone's perspective.
#ride sharing
#Uber
#Lyft
#New York City

redpajama_set_name: RedPajamaCommonCrawl


The kingdom gained popularity owing to its recipe for layered rice which was served to the kings and mass alike on festivities- A dish that is now known as Biryani.
The recipe was lost forever when King Cyrus laid siege to Behrouz.
Mouth watering Minced chicken kebabs cooked into soft delicious meatballs served with Minty dip.
Disclaimer - behrouz biryani is neither offering any rewards nor responsible for any queries/issues related to the rewards being offered by cash2kart. Therefore, for any rewards related issues/queries, kindly cash2kart's Customer Support team. No queries in this regard will be entertained by behrouz biryani.


Stephen Stanek, MD, President, and the leadership of The Toledo Surgical Society are pleased with your interest in our Society. The Society, founded in 1970 is dedicated to the advancement of the science of surgery and to the education of surgeons, residents, and students.
The Society holds five regular meetings per academic year beginning in the fall. Continuing Medical Education (CME, CEU, etc.). Category 1 credits are available for each meeting. The Society has a long standing tradition of sponsoring an annual Resident Research Forum and a Medical Student Scholarship. Click to view our current and past winners: Residents / Medical Students.
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text:
\section{Introduction} \label{sec:introduction}
Gamma-Ray Bursts (GRBs) are the most luminous astrophysical phenomena currently observed in the Universe. They appear with a rate of the order of few per day, at random locations in the sky \cite{band,kouveliotou,meegan}. The released energy amounts up to $\sim$ 10$^{54}$ erg \cite{max_e_grbs,max_e_grbs_erratum} in a time lasting from a fraction of a second to several thousands of seconds. Since their serendipitous discovery in the late 1960s \cite{firstGRB}, gamma-ray satellites have been detecting the so-called GRB \emph{prompt}
radiation, a non-thermal high-energy emission characterized by a gamma-ray energy flux peaking at few hundreds keV in the observer frame and that occasionally extends in a long tail up to the GeV band \cite{GRBreview}. When broadband data are available, a typical GRB spectrum, $dN/dE$, can be fitted between $\sim$~10 keV and 10$^4$ keV by two smoothly connected power laws, also known as the Band function \cite{band}, with typical low and high-energy spectral slopes $\alpha\sim-1.0$ and $\beta\sim-2.5$, respectively.

The origin of the emission mechanism powering GRBs has been object of active debates since the early days of their discovery. The commonly accepted picture is the so-called \emph{fireball model} \cite{piran1999}, where a mildly-relativistic outflow is launched by the compact central engine, most likely a newly formed black hole \cite{GRBreview}. Substantial efforts have been made to model the jet outflow dynamics and the subsequent radiative processes, giving rise to a variety of scenarios, such as internal shocks \cite{is1,is2}, dissipative photospheres \cite{ph_model} and magnetic reconnection phenomena occurring above the photosphere \cite{mag_rec_1,mag_rec_2,mag_rec_3,mag_rec_4}.

Internal shock models are particularly suited for the description of the prompt emission: the powerful and collimated jet produced in the explosion converts a fraction of its kinetic energy into internal energy through shocks occurring among non-uniform shells characterized by different Lorentz factor values \cite{bustamante_nature}, at a typical distance of $10^{13}$~cm from the central engine \cite{guetta2004}. Part of the energy that gets dissipated at the shocks is expected to be converted into non-thermal particles, through the acceleration of hadrons and leptons, that hence radiate via synchrotron and Inverse Compton (IC). In spite of its ability to explain most of the high-energy properties of the prompt emission phase, including time variability and energetics, some of the observed GRB spectra appear in conflict with this scenario. Indeed, the synchrotron model predicts GRB spectra with $\alpha \sim -1.5$, while the fitted values are often significantly harder. E.g. long GRBs (LGRBs), characterized by a gamma-ray duration longer than 2 seconds, show on average $\alpha \sim -1.0$ \cite{alpha_long_1,alpha_long_2,alpha_long_3,alpha_long_4,alpha_long_5}. Some GRBs are even showing spectra beyond the so-called \emph{synchrotron line-of-death} (i.e. $\alpha \geq -2/3$) \cite{preece}, especially short GRBs (SGRBs) with observed gamma-ray duration shorter than 2 seconds \cite{alpha_short_1,alpha_short_2}.

The inconsistencies between the synchrotron model and the observations have revived photospheric models, where the emission takes place closer to the photosphere of the jet. Actually, the photospheric emission is a natural consequence of the fireball model, the fireball being an optically thick expanding plasma made of particles and photons \cite{piran1999}. Photospheric emission from highly relativistic outflows was early considered as an explanation for the prompt emission of GRBs \cite{ph1,ph3}. However, these models did not have a significant impact for many years, as the observed GRB spectra appeared to be non-thermal since their very first observations. In photospheric models, the emission is expected to be constituted by a freely expanding radiation-dominated outflow with a thermal spectrum (Planck-like) peaked at $\sim$1 MeV in the observer frame. Thus, to explain the observed non-thermal emission, the photospheric component was proposed either to be reprocessed into a non-thermal emission arising from optically thin regions (e.g. \cite{meszaros}) or to be the result of projection effects. In the former case, several mechanisms have been suggested to operate below the photosphere, e.g. kinetic energy dissipation due to shocks \cite{rees,lazzati,ryde}, collisional processes \cite{belobodorov,vurm}, or magnetic energy dissipation due to field line reconnection \cite{ph2,spruit,giannios,zhang_yan}. In the geometrical interpretation, in turn, the observed emission would result in a superposition of spectra generated by photons emitted from a vast range of radii and angles which are detected simultaneously, rendering the inferred photosphere location angle dependent \cite{ph_angle_dep,peer}. Overall, it appears clear that radiation produced at this stage is an unavoidable component in GRB emission.

The first clear observation of a narrow thermal component in a GRB spectrum occurred in 2009, within the bright long GRB 090902B, detected by the Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) instruments on-board the \textit{Fermi} observatory \cite{grb090902b}. A time-resolved spectral analysis of such burst revealed an initial peaked component, with a spectral shape resembling the Planck function, interpreted as a clear sign of photospheric origin, followed by a later broadening of the spectrum described by a Band function with $\alpha=-0.6$ \cite{ryde}. This would suggest that the photospheric emission lasts during the whole burst duration, with the contribution of an additional component making the spectrum non-thermal. This picture has been corroborated by the discovery of other GRBs with a non-thermal spectrum overlapping the thermal one, e.g. GRB 100724B \cite{grb100724b} and GRB 110721A \cite{grb110721a}.
Given the complexity of the emission observed from the prompt phase of GRBs, both in terms of spectral and temporal features, it is likely that different radiative stages occur. A key issue that still remains to be addresses is to which extent photospheric emission has to be complemented by additional processes and how to identify these different spectral components from observations.

In the present work, we investigate the so-called \textit{inelastic collisional model} \cite{belobodorov}, where a baryonic jet gets significantly heated as it propagates away from the central engine because of inelastic $pn$ collisions among a proton component and a slower neutron one, taking place in the sub-photospheric region of the jet. These collisions, besides being responsible for energy dissipation, are also expected to originate neutrinos in the multi-GeV energy range \cite{derishev,bahcall,meszaros_multiGeV_nu,asano,bartos,murase}. On the other hand, internal shock models predict the existence of TeV-PeV neutrinos as a result of $p\gamma$ interactions among shock accelerated protons and the radiation field located in the optically thin region of the jet \cite{waxman1997,rachen1998,piran1999,guetta2004,murase2006,zhang2013}.
Hence, if neutrinos were revealed in coincidence with a GRB, they would allow to discriminate among the leptonic and hadronic nature of radiation; additionally, the measurement of their characteristic energy could be the key to identify the origin of the GRB prompt radiation (e.g. internal shocks vs photospheric emission). Thus, it is crucial to investigate neutrino emissions in a broad energy range.
To date, temporal and spatial associations among GRBs and neutrinos have only been searched for in the high-energy domain, mostly because the operating large volume neutrino telescopes IceCube \cite{icecube} and ANTARES \cite{antares} are designed to be mainly sensitive to TeV-PeV neutrinos. So far, these searches have not found any $\gamma-\nu$ association (refer to \cite{antares_first_grb_analysis,bright_grb_antares,my_analysis} for ANTARES analyses and \cite{icecube_analysis,icecube_grb2016} for the IceCube ones).
Thus, after about fifty years from the discovery of GRBs, the lack of $\gamma-\nu$ associations still prevents us from undoubtedly establishing the mechanism responsible for the GRB prompt emission.

Low-energy neutrinos produced in collisionally heated GRBs, i.e. those explained by the inelastic collisional photospheric model, might contribute to solve the puzzle. Some investigations in this direction have lead to the theoretical calculations of detection prospects of such neutrinos with IceCube \cite{icecube}, the South Pole neutrino observatory, and its low-energy extension, namely DeepCore \cite{deepcore}, sensitive to neutrinos with energies as low as $\rm E_{\nu}\sim$10 GeV. From a sample of bursts observed by BATSE \cite{meegan}, predictions estimated a non-negligible chance for detecting 10-100 GeV neutrinos in 5-10 years by using combined IceCube and DeepCore data \cite{bartos}. Other authors \cite{murase} showed that few neutrino-induced events can be detected by analyzing $\sim$1000-2000 GRBs stacked in a decade. Motivated by this, a first all-flavor search for transient emission of 1-100 GeV neutrinos was carried out using three years of data collected by the IceCube-DeepCore detectors. No significant emission was found in this sample, and upper limits on the expected volumetric rate of the transient neutrino sources were obtained, by assuming neutrino spectra consistent with the sub-photospheric emission \cite{icecube_analysis_lowE,icecube_analysis_lowE_ICRC}. However, it is worth noting that this analysis is time-dependent and it only refers to individual GRBs characterized by a duration up to approximately 600~s, a mean neutrino energy of 100~GeV, and a bolometric energy of 10$^{52}$~erg. Recently, an extension of this analysis has been presented \cite{icecube_analysis_lowE_ICRC}.

We investigate here for the first time about the possibility to reveal multi-GeV neutrinos from collisionally heated GRBs with the new generation neutrino telescope, KM3NeT \cite{km3net_loi}, currently under construction at two sites in the depth of the Mediterranean Sea. This detector will be sensitive to neutrinos down to few GeV energies thanks to the denser and compact array named KM3NeT/ORCA. We consider both individual and stacked searches on LGRBs and SGRBs, additionally exploring different bulk Lorentz factor values, ranging from low-luminous GRBs (i.e. those with $\Gamma \sim 100$) to high-luminous ones ($\Gamma \sim 600$).

The paper is structured as it follows. In Sec.~\ref{sec:model} we present the inelastic collisional model, detailing the gamma-ray production expected within such framework, as well as the spectral properties of the predicted neutrino fluxes. In Sec.~\ref{sec:neutrino_detectors} we describe the effective areas of neutrino detectors able to investigate the model predictions, both the currently operative ones and those under construction, focusing on the low-energy extensions for which we derived analytical parametrizations. In Sec.~\ref{sec:performances}, we discuss the neutrino signal and background characteristics, focusing on those parameters that are crucial for clearly assessing GRB-neutrino detections.
Afterwards, in Sec.~\ref{sec:prospects_neutrino_detections}, we derive detector sensitivities with respect to both individual and stacking GRB-neutrino searches, the latter spanning over a GRB sample expected to be collected by the operative gamma-ray satellites in about five years. Finally, we discuss our results in Sec.~\ref{sec:conclusion}.

\section{Gamma-ray and neutrino production in the GRB inelastic collisional model} \label{sec:model}
The basic assumptions of the inelastic collisional model considered in this work \cite{derishev,review2008,belobodorov} are: (i) the presence of a dense, hot and neutron-rich central engine \cite{derishev,belobodorov2003}; (ii) a non-magnetized baryonic jet (see \cite{vurm} for an extension of the model including also a magnetized jet). These two requirements are not far from being realized since GRB jets are possibly produced by hydrodynamic processes taking place in the accretion disk around a black hole or a neutron star, and the dissociation of nuclei by gamma-ray photons in the inner regions of the disk could produce free neutrons \cite{GRBreview}. Initially, neutrons and protons accelerate as a single fluid because of frequent nuclear collisions, while at a later expansion stage the jet evolves into the two-fluid or \textit{compound state}: a slower neutron component with Lorentz factor $\Gamma_n$ is embedded in a faster proton flow with $\Gamma>\Gamma_n$. This compound flow develops when the timescale for $pn$ collisions becomes longer than the jet expansion time, at radius $R_n$ \cite{derishev,bahcall,meszaros_multiGeV_nu,belobodorov2003}. The jet becomes transparent to radiation at the photosphere ($R_{\rm ph}\sim(10-20)R_n$), where the thermal emission is effective, as modified by the sub-photospheric collisional process. Such a heating mechanism, that is realized in the region of the jet between $R_n$ and $R_{\rm ph}$, injects energy into electron-positron pairs via two branches occurring at comparable heating rates: (i) electrons are heated by Coulomb collisions with protons and consequently radiate; (ii) inelastic $pn$ collisions. As a result, nuclear and Coulomb collisions in GRB jets create a hot $e^{\pm}$ plasma, that radiates its energy producing an escaping radiation with a well-defined spectrum. In the following, we will focus on inelastic nuclear collisions, as this channel is responsible for neutrino production within the photosphere.

\subsection{Inelastic nuclear collisions}
The region between $R_{n}$ and $R_{\rm ph}$ is characterized by inelastic nuclear collisions between protons and neutrons, significantly affecting the jet dynamics (sub-photospheric collisional heating), namely
\begin{equation}
\left\{\begin{matrix}
p+n\rightarrow p+p+\pi^{-} & \\
p+n\rightarrow n+n+\pi^+ & \\
\end{matrix}\right.,
\end{equation}
as well as
\begin{equation}
\left\{\begin{matrix}
p+p\rightarrow p+n+\pi^{+} & \\
p+p\rightarrow p+p+\pi^0 & \\
n+n\rightarrow p+n+\pi^{-}
\end{matrix}\right..
\end{equation}
The rate of $pn$ collisions per unit volume is given by \cite{belobodorov}:
\begin{equation}
\dot{\rm N}=n n_n \Gamma_{\rm rel} \sigma c,
\end{equation} where $\sigma=3\times 10^{-26}~\rm cm^2$ \cite{GRBreview} is the nuclear cross section, $n$ and $n_n$ are respectively the proton and neutron number densities, $c$ is the speed of light in vacuum, and $\Gamma_{\rm rel}$ is the relative Lorentz factor of the neutron and proton component of the jet, i.e.
\begin{equation}
\label{eq:rel_lorentz_factor}
\Gamma_{\rm rel}=\frac{1}{2}\left(\frac{\Gamma}{\Gamma_{ n}}+\frac{\Gamma_{n}}{\Gamma}\right)\simeq \frac{\Gamma}{2\Gamma_{n}},
\end{equation}
with $\Gamma \gg \Gamma_n$.
Each collision between protons and neutrons dissipates a fraction of kinetic energy, and quasi-thermal nucleons are produced with $ \rm E_{N,\rm c}^{\rm th}\simeq k_p \Gamma_{\rm rel} m_p c^2$ in the comoving frame of the interacting flow\footnote{Neutrons that survive these collisions travel to larger distances before decaying, possibly affecting the afterglow radiation from GRBs
\cite{belobodorov_afterglow}.}.
Here $\rm k_p \approx 0.5$ is the nucleon inelasticity (i.e. the ratio between the inelastic and the total interaction cross section) \cite{murase}, and $\rm m_p$ the proton mass. A comparable amount of energy converts to mildly relativistic pions. Charged pions immediately decay into muons (in 26 ns), in turn unstable towards the production of electron/positron pairs:
\begin{equation}
\label{eq:charged_pion_decay}
\pi^{\pm} \rightarrow \mu^{\pm} + \nu_{\mu}/\bar{\nu}_{\mu} \rightarrow e^{\pm} + \nu_e / \bar{\nu}_e.
\end{equation}
In addition, from the neutral pion decay, high-energy gamma rays are produced, that quickly convert to $e^{\pm}$:
\begin{equation}
\pi^0 \rightarrow \gamma+\gamma \rightarrow e^{\pm}.
\end{equation}
Such $e^{\pm}$ pairs, together with the ones produced by the aforementioned Coulomb collisions, can either up-scatter the thermal photons produced at the jet launch site to higher energies (via IC) and/or radiate via synchrotron emission, modifying the radiation spectrum and thus introducing a non-thermal component. The photon spectrum emitted by a collisionally heated jet was first derived by \cite{belobodorov}, through accurate  Monte Carlo simulations of the radiative transfer in the expanding jet. The resulting GRB spectra were shown to peak at $\sim$1 MeV
and to extend at higher energies with a photon index $\beta \sim -2.5$, well reproducing the prompt observations \cite{preece,band}.

\subsection{Neutrino production at the source}
\label{sec:neutrinoproduction}
From hadronic collisions in the sub-photospheric region of GRB jets, neutrinos are also produced (see Eq.~\eqref{eq:charged_pion_decay}). Charged pions on average carry 2/3 of the energy transferred by the protons in hadronic nuclear $pn$ collisions. By considering that neutrinos take $\sim 3/4$ of $\pi^{\pm}$ energy,
we can evaluate the average fraction of pion energy that is given to neutrinos, $f_{\nu}$, as:
\begin{equation}
\label{eq:fract_en_neutrinos}
f_{\nu} \sim \frac{2}{3} \cdot \frac{3}{4}=\frac{1}{2}.
\end{equation}
Neutrinos therefore carry away a significant fraction of the energy $ \rm E_{\rm k,diss,s}$ dissipated in inelastic nuclear collisions, where the subscript $s$ refers to the source rest frame, which is related to the comoving one through the Lorentz boost $ \rm E_{\rm s}=\Gamma E_{\rm c}$. The corresponding energy of the neutrino burst (which does not suffer any adiabatic cooling) is
\begin{equation}
{\rm E_{\nu, \rm s}}=f_{\nu} \rm E_{\rm k,diss,s}\simeq \frac{1}{2}E_{\rm k,diss,s}.
\end{equation}
Therefore, the energy channeled into radiation produced by the GRB jet is the remaining
\begin{equation}
\label{eq:egamma}
{\rm E_{\gamma,\rm s}}=f_{\rm ad}(1-f_{\nu}){\rm E_{\rm k,diss,s}}\simeq \frac{f_{\rm ad}}{2}\rm E_{\rm k,diss,s},
\end{equation}where $f_{\rm ad}<1$ describes the reduction in radiation energy due to adiabatic cooling in the expanding opaque jet below the photosphere.\\
Hence, the ratio among the neutrino and the radiation burst energies (or their isotropic equivalents) is given by
\begin{equation}
\label{eq:w}
w=\frac{\rm E_{\nu, \rm s}}{\rm E_{\gamma, \rm s}}=\frac{\rm E_{\nu, \rm s}^{\rm iso}}{\rm E_{\gamma, \rm s}^{\rm iso}}=\frac{1}{f_{\rm ad}}.
\end{equation}
Assuming that half of the energy is dissipated in the adiabatic expansion (i.e. $f_{\rm ad}=0.5$), we expect
\begin{equation}
\label{eq:enu}
\rm E_{\nu, \rm s}=2E_{\gamma, \rm s} \rightarrow E_{\nu, \rm s}^{\rm iso}=2E_{\gamma, \rm s}^{\rm iso}.
\end{equation}
By defining the ratio $\xi_{\rm N}$ among the energy dissipated in inelastic nuclear collisions and the gamma-ray energy produced in the GRB jet as
\begin{equation}
\label{eq:xi}
\xi_{\rm N} = \frac{E_{\rm k,diss,s}^{\rm iso}}{E_{\gamma,\rm s}^{\rm iso}},
\end{equation}
the benchmark scenario with $f_{\rm ad}=0.5$ would imply $\xi_{\rm N}=4$ (see Eq.~\eqref{eq:egamma}). \\
In the present work, we consider only muon neutrino (and the corresponding anti-neutrino) emissions, since their interactions in charged current with nucleons inside large volume neutrino telescopes are well identified, resulting in long muon tracks.
By considering the energy carried by $\nu_{\mu}$ and $\bar{\nu}_\mu$ only, Eq.~\eqref{eq:enu} can be written as:
\begin{equation}
\label{eq:nu_energy}
\rm E_{\nu_{\mu}+\bar{\nu}_{\mu},\rm s}^{\rm iso} \sim \frac{2}{3}E_{\gamma, \rm s}^{\rm iso}.
\end{equation}
Thus, the energy going in muon neutrinos is estimated to be $\sim$67\% of the gamma-ray energy. Such a linear scaling implies that the absolute gamma-ray energy and the model parameter $\xi_{\rm N}$ in Eq.~\eqref{eq:xi} are crucial, as they influence the neutrino spectral normalization \cite{murase}.

The energy of the emitted neutrinos is a function of the Lorentz factor of the jet, $\Gamma$, and of the relative Lorentz factor of the proton and neutron components (given in Eq.~\eqref{eq:rel_lorentz_factor}), through \cite{belobodorov,asano,bartos,murase}:
\begin{equation}
\label{eq:peak_energy}
\rm E_{\nu} \approx 0.1 \Gamma~\Gamma_{\rm rel}~\mathrm{m_p c}^2 \rightarrow E_{\nu} \simeq 100~\rm GeV \left(\frac{\Gamma}{500}\right) \left(\frac{\Gamma_{\rm rel}}{2}\right).
\end{equation}
This relation implies an average expected neutrino energy of $\rm E_{\nu}\sim$~10-100 GeV for Lorentz factors $\Gamma \sim 100-1000$. Therefore, measuring the neutrino energy would provide a direct handle on the Lorentz factor of the jet, which is a key in resolving GRB dynamics.\\The neutrino spectra arising from sub-photospheric collisionally heated model are quasi-thermal, hence their shape is bell-like. The exact details of neutrino spectra have been obtained with detailed Monte Carlo simulations including cooling processes of secondary mesons and leptons (hadronic losses, radiative cooling and adiabatic expansion) by \cite{murase}. The resulting spectra are further discussed in Sec.~\ref{sec:prospects_neutrino_detections}.

\section{Current and future low-energy neutrino detectors} \label{sec:neutrino_detectors}
The search for multi-GeV neutrinos from GRBs with Cherenkov telescopes needs a compact arrays of 3D photomultiplier sensors, in order to detect the Cherenkov light induced by the propagation of the relativistic particles produced in neutrino interactions.

The IceCube observatory, operating at the South Pole, is complemented by DeepCore \cite{deepcore}, an array characterized by a higher concentration of digital optical modules (DOMs), optimized for the detection of neutrinos with energies down to 10 GeV. DeepCore is constituted by 15 strings located in a radius of 125 m at a depth from $\sim$2100 m to $\sim$2450 m in the ice. Eigth strings are very close to the bottom center of IceCube, with a DOM-to-DOM vertical spacing varying between 7 and 17~m. The DeepCore detector is operational since about 10 years. A low-energy in-fill extension to IceCube has also been proposed, named PINGU \cite{pingu}, that will be characterized by an effective mass of about 6~Mton for neutrino energies above few GeV. So far, no public effective area is available for PINGU, thus it will not be considered in the following estimations.

Currently, another low-energy neutrino detector is under construction in the Northern hemisphere, off the Mediterranean France coast at about 2450 m depth, namely the KM3NeT/ORCA neutrino telescope. Its optical modules are being arranged in the dense configuration required for detecting events with energies as low as few GeV. This range is three orders of magnitude lower that the typical energy scale probed by the high-energy detector KM3NeT/ARCA (currently under construction offshore Sicily, in Italy), designed for neutrino astroparticle physics studies \cite{km3net_loi}. At the time of writing, KM3NeT/ORCA is taking data with 10 strings, with an average horizontal spacing between strings of about 20~m and a vertical spacing between DOMs of about 9~m
\cite{km3net_loi,km3net_design,last_km3net_orca}. Once completed, KM3NeT/ORCA will consist of 115 strings, arranged in a circular footprint with a radius of about 115 m.

The primary goal of low-energy neutrino detectors is to unveil the intrinsic properties of neutrinos, as the mass hierarchy, by investigating neutrino oscillation studies in the atmospheric sector. Still, the low energy domain offers interesting possibilities for exploring astrophysical science cases, e.g. the collisional heating mechanism powering the GRB prompt emission presented above. Hence we proceed by investigating the KM3NeT/ORCA and DeepCore performances in the context of multi-GeV GRB analyses. The following part of the current section presents an analytical parametrization of the detector effective areas, while the next section details about expected background rate in each detector.

\begin{figure}[t!]
    \centering
    \includegraphics[width=\columnwidth]{fit_aeff_deepcore.pdf}
    \caption{DeepCore effective area at trigger level for neutrino energies between $\sim$10 GeV and 100 GeV. Black points represent published values from the IceCube Collaboration \cite{deepcore}, while the red solid line shows the best fit obtained with Eq.~\eqref{eq:fit_deepcore}.}
    \label{fig:fit_deepcore}
\end{figure}
\begin{figure}[t!]
    \centering
    \includegraphics[width=0.95\columnwidth]{fit_aeff_orca_deepcore_comparison.pdf}
    \caption{KM3NeT/ORCA effective area at trigger level for neutrino energies between $\sim$10 GeV and 100 GeV (orange line) as compared to the DeepCore effective area (red line). The orange solid line, extending up to $\sim$20 GeV, shows the computation resulting from Eq.~\eqref{eq:veff}, namely starting from the detector effective volume $\rm V_{eff}(E)$ \cite{new_veff_orca}. In turn, the orange dashed line $\rm E_{\nu_{\mu}}>20~GeV$ represents its extrapolation, by adopting the same energy dependence as in DeepCore.}
    \label{fig:aeff_orca}
\end{figure}

\subsection{Detector effective areas}
The present study is performed by considering instrument response functions of each detector at trigger level: in particular, effective areas for $\nu_{\mu}+\bar{\nu}_{\mu}$ events in IceCube-DeepCore and KM3NeT/ORCA-KM3NeT/ARCA are taken by \cite{deepcore} and \cite{km3net_loi}, respectively, accordingly with the actual detector configurations. Note that the KM3NeT/ORCA effective area at trigger level is not directly available from literature, but it can be obtained by knowing its effective volume $\rm V_{eff}$ towards muon neutrino events, which has been published for the complete detector configuration up to energies of $\sim 20$~GeV \cite{km3net_loi}. By defining the muon neutrino charged current cross section $\sigma_{\nu_{\mu}^{\rm CC}}(\rm E)$, the medium density $\rho$ (i.e. the water density at KM3NeT/ORCA site), and the Avogadro constant $\rm N_A$, we derived the KM3NeT/ORCA effective area as
\begin{equation}
\label{eq:veff}
\rm A_{\rm eff}(E)=\sigma_{\nu_{\mu}^{\rm CC}}(E) \rho N_A V_{\rm eff}(E) \, .
\end{equation}
Since our GRB-$\nu$ flux evaluation requires values up to $\sim$1 TeV, we further extrapolate the KM3NeT/ORCA effective area behaviour at higher energies than available, by using the same energy dependence as in DeepCore\footnote{This assumption can be considered valid as both detectors are characterized by a dense configuration of optical modules.}.
A best fit procedure to the DeepCore effective area results into:
\begin{equation}
\label{eq:fit_deepcore}
    \rm A_{eff}^{\rm DeepCore}(E_{\nu_{\mu}})=15\left(\frac{E_{\nu_{\mu}}}{100~\rm GeV}\right)^{1.6}~cm^2,
\end{equation}
as shown in Fig.~\ref{fig:fit_deepcore}. Hence, we expect the KM3NeT/ORCA effective area at trigger level to correspond in the energy range $10-100$~GeV to (see Fig.~\ref{fig:aeff_orca})
\begin{equation}
\label{eq:fit_orca}
    \rm A_{eff}^{\rm ORCA}(E_{\nu_{\mu}})=12\left(\frac{E_{\nu_{\mu}}}{100~\rm GeV}\right)^{1.6}~cm^2.
\end{equation}
These parametrizations show that DeepCore and KM3NeT/ORCA are expected to have comparable performances. Note that performances at trigger level are the highest possibly achievable by experiments, later reduced by the efficiency of the event selection at analysis level. However, since none of the detectors under investigation has yet implemented analysis tailored at identifying low-energy neutrinos from cataloged GRBs, we will conservatively adopt the trigger level performances in the following, in the forms of Eqs.~\eqref{eq:fit_deepcore} and \eqref{eq:fit_orca}. Note also that triggering strategy are subject to change: e.g., recently, a new approach has been developed for KM3NeT/ORCA \cite{new_veff_orca,last_km3net_orca}, which is expected to increase the trigger efficiency in the few GeV neutrino energy range with respect to the case here considered.

\section{Signal and background estimation for GRB-neutrino detections} \label{sec:performances}
Quantitative estimations concerning detection prospects of low-energy neutrinos emerging from collisionally heated GRBs with current (DeepCore and IceCube) and under construction (KM3NeT/ORCA and KM3NeT/ARCA) neutrino telescopes are here presented.  As at multi-GeV energies the atmospheric background is severely limiting the identification of cosmic signals, in this search we will consider only upward going neutrinos. Indeed, Earth-filtered events allow to reduce significantly the atmospheric muon background. Additionally, we will consider only events due to $\nu_{\mu}$ charged current (CC) interactions: the muon originated in such interactions indeed results into a long track that allows to define with good accuracy the direction of the incoming neutrino. In turn, a worse directional reconstruction is expected for shower-like events, e.g. those originated by $\nu_e$ and $\nu_{\tau}$ CC interaction channels, as well as by all flavor neutral current (NC) interactions. The addition of this event topology in the present work would require to extend the search cone around each source (particularly for large values of $\Gamma$, see Sec.~\ref{sec:prospects_neutrino_detections}), implying a higher background level affecting the analysis, while at the same time allowing to probe the entirety of the neutrino flux reaching Earth. The exact balance among these two effects deserves a detailed investigation, that we defer to a future work because instrumental performances at such low energies are currently not available for all neutrino telescopes under exam.

For the purposes of this analysis, synthetic GRB characteristics are considered: in particular, as we aim at evaluating the neutrino flux expected on Earth from a GRB population powered by the collisional heating mechanism, we define a source sample reflecting the observed properties of the population.
Therefore, by collecting satellite's published data, we built distributions of several quantities, as the time interval over which a burst emits from 5\% of its total measured gamma-ray emission to 95\% (also known as $T_{90}$), and the gamma-ray fluence $F_\gamma$, that are key parameters for the background and signal estimation, respectively. Under the hypotheses of the inelastic collisional model (explained in Sec.~\ref{sec:model}), the neutrino signal would be produced in spatial and temporal coincidence with the prompt phase of GRBs. For this reason we conservatively define a temporal search window around each burst as wide as $T_{90} \pm 0.3T_{90}$

The neutrino spectra produced in collisionally heated GRBs are taken from \cite{murase} under the following assumptions: i) the neutrino and electromagnetic emission is released at the photosphere (i.e. at $R_{\rm ph}$), where the optical depth for the $pn$ reactions is close to unity; ii) the relative Lorentz factor between the proton and the neutron component is $\Gamma_{\rm rel}=3$ ($\Gamma\simeq6\Gamma_{n}$, see Eq.~\eqref{eq:rel_lorentz_factor});
iii) the fraction of gamma-ray energy dissipated in nuclear collision is $\xi_{\rm N}=4$. Note that $\Gamma_{\rm rel}$ influences the characteristic energy of emitted neutrinos, which scales as $\Gamma_{\rm rel}/2$ (Eq.~\eqref{eq:peak_energy}), namely a faster proton flow inside the jet would imply a higher value for the peak of neutrino spectra. In particular, with respect to the reference case with $\Gamma_{\rm rel}=3$, a proton flow with $\Gamma \simeq 20 \Gamma_{n}$ gives typical neutrino energy higher by a factor $\sim3$ once the jet Lorentz factor $\Gamma$ is fixed. In turn, $\xi_{\rm N}$, in Eq.~\eqref{eq:xi}, influences the neutrino fluence normalization, since it is related to the ratio among neutrino and gamma-ray energies, as demonstrated in Sec.~\ref{sec:neutrinoproduction}. The inelastic collisional model predicts at most $\xi_{\rm N} \approx 20$ \cite{murase}, which corresponds to $f_{\rm ad}\sim 0.1$ (see Eq.~\eqref{eq:egamma} and Eq.~\eqref{eq:xi}). In such a case, the neutrino fluence normalization would rise by a factor 5 with respect to the benchmark case here considered, thus increasing the expected GRB-emissivity rate of neutrinos. While the spectral details of emission, and hence the expected number of events in neutrino telescopes, might depend on the specific values of the model parameters assumed, the results of the neutrino sensitivity computation presented in the following are quite stable against reasonable variations of these parameters, i.e. $4\leq\xi_{\rm N}\leq20$ and $3\leq\Gamma_{\rm rel}\leq10$. In fact, the sensitivity is rather dominated by the large variety of the GRB population in terms of temporal and spectral properties (namely $T_{90}$ and $F_\gamma$, that affect respectively the number of background and signal events).

The observed neutrino fluence produced in collisionally heated GRBs from a source at redshift $z$ is
\begin{equation}
\label{eq:nu_fluence_obs}
F_{\nu} \propto \frac{1+z}{4\pi d_L^2(z)} \int \rm dE \left({\rm E} \frac{\rm dN}{\rm dE}\right)_{\nu,\rm s} \, ,
\end{equation}
where $d_L(z)$ is the luminosity distance of the source and the factor $\frac{1+z}{4\pi d_L^2(z)}$ takes into account the cosmological distance of the source and the dilution of the neutrino energy flux from the source to Earth.
It is also worth noting that, as sub-photospheric gamma rays constitute the prompt emission, the neutrino fluence is proportional to the observed gamma-ray fluence through Eq.~\eqref{eq:nu_energy}, namely $F_\nu \sim F_{\gamma}$.
To define the GRB of the sample of our simulation, we extracted for each source the spectral parameters $F_{\gamma}$ and $T_{90}$ in accordance with \textit{Fermi}-GBM distributions\footnote{\textit{Fermi}-GBM catalogue: \url{https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html}.}. The extracted values are only accepted if their ratio falls into the observed distribution of $F_{\gamma}/T_{90}$.
Such a selection was performed in order to ensure that the simulated GRB sample only contains physical sources, i.e. bursts with values of the ratio $F_{\gamma}/T_{90}$ compatible with observed GRBs, given that this parameter is a key in the determination of the isotropic gamma-ray luminosity in the observer frame, $L_{\gamma,\mathrm{iso}}=4 \pi d_{L}^2(z)\frac{F_{\gamma}}{T_{90}}$. Note however that fixing the value of $F_{\gamma}/T_{90}$ actually implies that each GRB of the sample is degenerate in $L_{\gamma,\rm iso}$ and $z$ (through the luminosity distance), since different combinations of these quantities might yield the same value of $F_{\gamma}/T_{90}$.
\begin{table*}
\begin{ruledtabular}
\begin{tabular}{lcccccccc}
 &\multicolumn{2}{c}{$\Gamma=100$}
&&
 \multicolumn{2}{c}{$\Gamma=300$}
&&
\multicolumn{2}{c}{$\Gamma=600$} \\\cline{2-3}\cline{5-6}\cline{8-9}
Detector & $\rm E^{*}_{\nu_{\mu},\rm max}$ [GeV] & $\theta^{*}$ [deg] && $\rm E^{*}_{\nu_{\mu},\rm max}$  [GeV] & $\theta^{*}$ [deg] && $\rm E^{*}_{\nu_{\mu},\rm max}$ [GeV] & $\theta^{*}$ [deg]     \\
\hline
KM3NeT/ORCA & 27 & 26 && 73 & 13 && 121 & 9\\
KM3NeT/ARCA & - & - && 129 & 9 && 227 & 6\\
DeepCore & 27 & 26 && 78 & 13 && 165 & 8\\
IceCube & - & - && 156 & 8 && 258 & 5\\
\end{tabular}
\caption{Energy values $\rm E^{*}_{\nu_{\mu},\rm max}$, in GeV, at which each detector is expected to observe the highest number of $\nu_{\mu}+\bar{\nu}_{\mu}$ induced events, and corresponding plane angle values $\theta^{*}$, in degrees, adopted to search for such events around GRBs, corresponding to a solid angle $\Omega=2\pi(1-\cos(\theta^{*}/2))$.}
\label{tab:bkg_angles}
\end{ruledtabular}
\end{table*}
This method was applied to SGRBs and LGRBs, separately, as to correctly characterize the two different populations.
To obtain the muon neutrino spectrum characteristic of each GRB of the sample, we considered as reference model the neutrino production simulation presented in \cite{murase}. This refers to a high-luminous GRB with bolometric (i.e. E$_1=1$~keV and E$_2=10$~MeV) isotropic gamma-ray energy $E_{\gamma,\rm iso}=10^{53.5}$ erg at $z=0.1$, resulting in a gamma-ray bolometric fluence $F_{\gamma}^* \sim 10^{-2}$ erg cm$^{-2}$.
Since the fluence values assigned to each GRB of the synthetic sample are extracted from the \textit{Fermi}-GBM catalog, that provides measurements from $e_1=10$~keV to $e_2=1000$~keV, we need to first estimate the corresponding gamma-ray fluence in the bolometric range $F_{\gamma,\rm bol}$. This correction is also known as $k$-correction \cite{bloom}:
\begin{equation}
  k = \frac{F_{\gamma,\rm bol}}{F_\gamma} = \frac{F_{\gamma}\rm\left [ \frac{E_1}{1+z}, \frac{E_2}{1+z} \right ]}{F_{\gamma}\left [e_1,e_2 \right ]},
\end{equation}
Given the linear scaling among neutrino and gamma-ray fluences predicted by the collisionally heating GRB model, we can rescale the neutrino fluence predictions from \cite{murase} by a factor $\sim F_{\gamma,\rm bol}/F^*_\gamma$.
This factor could be obtained directly from gamma-ray spectra specifically for each GRB. However, since the shape of the gamma-ray spectrum does not enter additionally into our computations, and since most of GRB spectra can be described by the same functional form (the Band function discussed in Sec.~\ref{sec:introduction}), we decided to include a median correction in our analysis. In order to do so, we collected all the $k$-corrections calculated based on the GRB sample observed by \textit{Fermi}-GBM during the first ten years of its operation and with known redshift ($\sim$4.5\% out of the total sample) \cite{k_corrections} and computed the median value of such a distribution. Then, each time a value of gamma-ray fluence was extracted in a synthetic GRB of the sample, this was $k$-corrected with the median of such distribution, i.e. $\bar{k}=1.13$ (see Fig.~\ref{fig:k_corr}):
\begin{equation}
    F_{\gamma,\rm bol}=\bar{k} \cdot F_{\gamma} = 1.13 \cdot F_{\gamma}.
\end{equation}
\begin{figure}[t!]
    \centering
    \includegraphics[width=\columnwidth]{distribution_k_corr_FermiGBM.pdf}
    \caption{$k$-correction values calculated on the GRB sample collected by \textit{Fermi}-GBM during the first ten years of detector operation, including both LGRBs and SGRBs \cite{k_corrections}. The red and blue dashed lines show the mean and the median of the $k$-correction values, respectively.}
    \label{fig:k_corr}
\end{figure}
In principle, different $k$-corrections should be applied to the two samples of LGRBs and SGRBs, because these manifestly show different spectral slopes of the emitted prompt radiation. However, the \textit{Fermi}-GBM sample from which the $k$-correction is extracted \cite{k_corrections} is quite limited: it contains only sources with known redshift (amouting to 13 SGRBs and 122 LGRBs). As a result, the sample of SGRBs for which the $k$-correction has been evaluated is not statistically relevant to derive a physically motivated $k$-correction different than that of LGRBs. Hence, we will adopt the median value for both populations. \\
In the data sample of up-going events collected by a neutrino telescope, the background is mainly constituted by atmospheric neutrinos \cite{gaisser}. The Honda model is adopted as a reference for the atmospheric neutrino flux \cite{honda}. The number of events expected in coincidence with the burst depends on: i) its duration, namely the temporal window defined by $T_{90}$; ii) the search angular window around the GRB position, i.e. the solid angle $\Omega=2\pi(1-\cos(\theta/2))$, where $\theta$ is the aperture of the search cone. The aperture of the search cone should be carefully chosen as to maximize the detection prospects of a signal against the background. Given a model, determined by a specific value of $\Gamma$, we adopted the same aperture cone angle for all the simulated GRBs, the angle changing with the value of $\Gamma$. We conservatively set it to $\theta^{*}=3\theta_{\nu \mu}(\rm E^{*}_{\nu_{\mu},\rm max})$, where $\theta_{\nu \mu}(\rm E_{\nu})=0.7^{\circ}/(\rm E_{\nu}[\rm TeV])^{0.7}$\cite{review2000} is the kinematic angle between the incoming neutrino and the emerging muon directions, while $\rm E^{*}_{\nu_{\mu},\rm max}$ is the energy at which each neutrino telescope would observe the maximum number of neutrinos expected according to the model (which depends on $\Gamma$). To obtain this value, we convolved the energy-dependent effective area $\rm A_{eff}(E_{\nu_{\mu}})$ of the detectors with the expected differential energy fluence $\rm \frac{dN(E_{\nu_{\mu}})}{dE_{\nu_{\mu}} dS}$ predicted by the model, obtaining the so-called \emph{parent function}, and then we multiplied it by the width of each energy bin $\Delta E_{\nu_{\mu}}$, as follows:
\begin{equation}
    \rm N_{\nu_{\mu}}(E_{\nu_{\mu}})= A_{eff} (E_{\nu_{\mu}}) \left(\frac{dN(E_{\nu_{\mu}})}{dE_{\nu_{\mu}} dS}\right) \Delta E_{\nu_{\mu}}.
\end{equation}
Then, for each distribution $\rm N_{\nu_{\mu}}(E_{\nu_{\mu}})$ we looked for the energy $\rm E^{*}_{\nu_{\mu},\rm max}$ corresponding to the maximum number of expected events for each $\Gamma$ and each detector.
The values so determined are given in Tab.~\ref{tab:bkg_angles}, together with the corresponding opening angle of the angular window.
For the low-energy neutrino telescopes, namely KM3NeT/ORCA and DeepCore, the solid angle opened around each GRB changes from $\Omega\simeq0.2~\rm sr$ to $\Omega\simeq0.02~\rm sr$ for Lorentz factor values from $\Gamma=100$ to $\Gamma=600$, respectively. Indeed, according to the model, the greater the value of $\Gamma$ and the higher the mean energy of the emitted neutrinos (see Eq.~\eqref{eq:peak_energy}), hence the higher the energy peak of the detectable neutrino sample.
For values of $\Gamma\geq300$, where the energy peak in the neutrino spectrum is expected beyond 100 GeV, joint analyses that include both low and high-energy neutrino detectors (namely KM3NeT/ARCA and IceCube) are possible.
In the search performed with high-energy neutrino telescopes, the solid angle where background evaluation is performed is rather within the range $\Omega\simeq0.02~\rm sr$ and $\Omega\simeq0.01~\rm sr$.
In the combined investigations, different angular windows are set for the different detectors in order to optimize the search, as given in Tab.~\ref{tab:bkg_angles}. For further details on the choice of the aperture cone we defer the reading to Appendix \ref{appA}.
In the following, we will evaluate the perspectives of a search over a sample comprehensive of neutrino interactions in low (DeepCore and KM3NeT/ORCA) and high (IceCube and KM3NeT/ARCA) energy specialized detectors.

\begin{figure*}[t]
\subfigure[\label{fig:neutrino_spectra}]{\includegraphics[width=\columnwidth]{models.pdf}}
\subfigure[\label{fig:neutrino_ns}]{\includegraphics[width=\columnwidth]{ns_number.pdf}}
    \caption{(a) The $\nu_{\mu}+\bar{\nu}_{\mu}$ energy fluence for a GRB with observed gamma-ray fluence $F_{\gamma}\sim2\times10^{-3}$ erg cm$^{-2}$ for $\Gamma$=100 (cyan), $\Gamma$=300 (orange) and $\Gamma$=600 (green). (b) Number of signal events per GeV expected in KM3NeT/ORCA (solid lines) and DeepCore (dotted lines) for the neutrino energy fluences shown in (a).

    These results are all given at trigger level.}
    \label{fig:fig_model}
\end{figure*}
\begin{table*}[t]
\centering
\begin{tabular}{lccc}
\hline
\hline
 &\multicolumn{3}{c}{$n_s$}
 \\\cline{2-4}
Detector & $\Gamma=100$ & $\Gamma=300$ & $\Gamma=600$ \\
\hline
KM3NeT/ORCA & 4$\times$10$^{-2}$ & 7$\times$10$^{-2}$ & 1$\times$10$^{-1}$\\
KM3NeT/ORCA+KM3NeT/ARCA & - & 9$\times$10$^{-2}$ & 2$\times$10$^{-1}$\\
DeepCore & 5$\times$10$^{-2}$ & 9$\times$10$^{-2}$ & 1$\times$10$^{-1}$ \\
DeepCore+IceCube & - & 3$\times$10$^{-1}$ & 8$\times$10$^{-1}$\\
\hline
\hline
\end{tabular}
\caption{Number of events from $\nu_{\mu}+\bar{\nu}_{\mu}$ interactions expected from a GRB with gamma-ray fluence $F_{\gamma}\sim 2\times 10^{-3}$~erg~cm$^{-2}$ in low-energy detectors (KM3NeT/ORCA and DeepCore) alone, or in a combined search with high-energy detectors (KM3NeT/ARCA and IceCube, respectively). These results are all given at trigger level.}
\label{tab:number_events}
\end{table*}

\section{Prospects for neutrino detections}
\label{sec:prospects_neutrino_detections}
We here estimate whether it would be promising to look for GRB low-energy neutrino emissions with existing and under construction telescopes. Two possibilities are explored in the following: i) the search for neutrinos from individual GRBs is discussed in Sec.~\ref{sec:prospects_1grb}, with reference to an extremely bright GRB, that would represent the most optimistic scenario for individual detection of low-energy neutrinos; ii) the quasi-diffuse neutrino search from a population of GRBs with a stacking technique implemented over approximately 5 years of data acquisition is presented in Sec.~\ref{sec:stacking_prospects}.

\subsection{Detection prospects from an individual extreme GRB} \label{sec:prospects_1grb}
For the purposes of exploring the maximum discovery potential of the collisional heating mechanism in terms of individual neutrino emissions, we here consider the case of a very fluentic GRB, namely with $F_{\gamma}\sim 2\times 10^{-3}$ erg cm$^{-2}$. This value is comparable to that of the highest fluence GRB present in the \textit{Fermi}-GBM catalogue, i.e. GRB130427A. The expected differential neutrino fluence depends on the value of Lorentz factor, particularly because of the maximum energy (see Eq.~\eqref{eq:peak_energy}): in Figure \ref{fig:neutrino_spectra} we show this dependence for different values of $\Gamma$, i.e. $\Gamma=100$, $\Gamma=300$ and $\Gamma=600$. For comparison with predictions from the internal shock model, refer to Fig.~1 of \cite{bright_grb_antares}, where the neutrino fluence expectations for GRB130427A are shown.

In order to compute the expected number of signal events in each detector, we proceeded by evaluating the parent function for each of them, as shown in Fig.~\ref{fig:neutrino_ns} for DeepCore and KM3NeT/ORCA. By integrating it over the energy, we derived the results given in Tab.~\ref{tab:number_events} concerning the number of muon tracks induced by neutrino interactions.
Though the GRB considered in this example is characterized by a high fluence (comparable to the highest fluence ever observed among all GRBs in the \textit{Fermi}-GBM catalogue), the number of signal events observable in each neutrino telescope is quite limited ($n_{\rm s}<1$), even when the events measured with low-energy detectors are integrated with those collected by high-energy ones. Nonetheless, we suggest to implement a combined search among low and high-energy neutrino detectors, i.e. KM3NeT/ORCA+KM3NeT/ARCA and DeepCore+IceCube, in order to increase the expected signal event rate. Only in the case with $\Gamma=100$ the high-energy detectors can not provide a significant contribution, given that the expected signal is entirely below 100~GeV. According to our calculations, in order to measure $n_{\rm s}\geq1$ from a single GRB in at least one of the considered detectors, this source should be characterized by an extreme fluence, as $F_{\gamma}\geq 10^{-2}$ erg cm$^{-2}$. So far, no such kind of GRBs has ever been observed, but we cannot exclude in the future a serendipitous occurrence of a nearby and very energetic explosion.

\subsection{Stacking detection prospects} \label{sec:stacking_prospects}
The signal detection rate can be greatly increased when summing up the contribution of many GRBs. However, the same holds for the background, such that stacking techniques are necessary in order to obtain a significant detection level. In fact, selecting events restricted in an angular cone around sources allows the signal to stand out with respect to the background. In our case, since the cone aperture around each GRB is not optimized individually, a source ordering in cumulative detection significance $\sigma_{\rm tot}$ is required when sources are summed up. Thanks to the stacking procedure, the cumulative significance results higher since Poissonian fluctuations of the cumulative background are smaller than the sum of background fluctuations expected from a single source. Additionally, our stacking techniques profit of the transient nature of the sources under investigation. We here present a study on expected performances of current and under construction neutrino detectors after $\sim$5 years of stacking analysis in a half-sky search for tracks (namely only upgoing muon neutrinos).

We started by building two synthetic populations of GRBs detectable by current gamma-ray satellites in 5 years of operation, one for long and one for short GRBs, each reproducing the observed rate per year in the half of the sky equal to N$_{\rm SGRB}=75$ yr$^{-1}$ and N$_{\rm LGRB}=175$ yr$^{-1}$ \footnote{Such values were obtained from the Gamma-Ray Bursts Interplanetary Network (IPNGRB) database \url{https://heasarc.gsfc.nasa.gov/w3browse/all/ipngrb.html}.}. Each GRB of the sample is described by values of $F_{\gamma}$ and $T_{90}$, randomly extracted from \textit{Fermi}-GBM observed distributions and selected as explained in Sec.~\ref{sec:performances}. For each extracted source, we estimated the expected neutrino fluence for three different values of Lorentz factor, i.e. $\Gamma= [100,300,600]$. The average source in the sample is way less fluentic than the one considered in the previous section, being characterized by a median value of $F_\gamma \sim 8 \times 10^{-6}$~erg~cm$^{-2}$ for LGRBs and $F_\gamma \sim 6 \times 10^{-7}$~erg~cm$^{-2}$ for SGRBs. The linear scaling among gamma-ray and neutrino fluence predicted by the inelastic collisional model implies a peak value in the neutrino spectrum at the level of $2\times 10^{-3}$~GeV~cm$^{-2}$ and $1\times 10^{-4}$~GeV~cm$^{-2}$ respectively, to be compared with what shown in Fig.~\ref{fig:neutrino_spectra} for an extremely fluentic GRB. The stacking approach appears therefore to be a necessary condition to test the model.

The expected background occurring inside the detector in coincidence with the signal from each GRB is estimated in a temporal window as wide as $T_{90}\pm 0.3T_{90}$, and in an angular window defined by values reported in Tab.~\ref{tab:bkg_angles}. Once the GRB sample was populated by $\rm N$ objects, we proceeded in the following way: (i) we selected the GRB with the highest level of significance, defined as $\sigma=n_{\rm s}/\sqrt{n_{\rm b}}$; (ii) starting from such a GRB, we added one by one the others, choosing each time the GRB that provides the maximum increase of the total level of significance $\sigma_{\rm tot}$, defined as:
\begin{equation}
\sigma_{\rm tot} (\mathrm{N})=\frac{n_{\rm s,tot}}{\sqrt{n_{\rm b,tot}}}=\frac{\sum_{i=1}^{\mathrm{N}} n_{\rm s,i}}{\sqrt{ \sum_{i=1}^{\mathrm{N}} n_{\rm b,i}}} \, .
\end{equation}
We repeated the full procedure 1000 times, obtaining the median value of significance after stacking 875 LGRBs or 375 SGRBs (acquired in $\sim$5 years of half-sky gamma-ray observations), with an uncertainty band calculated through percentiles at one and two standard deviations.

By requiring $\sigma_{\rm tot}>3$ and $n_{\rm s,tot}\geq$1 as minimum conditions to define a detection, we conclude that: \\
(i) a detection of subphotospheric neutrinos is possible if LGRBs are included in the search, since SGRBs alone would not provide signal enough to satisfy the requirements above, in spite of the lower background level expected with respect to LGRBs; \\
(ii) the model with $\Gamma=100$ is characterized by a median value of $\sigma_{\rm tot}$ lower than unity; \\
(iii) higher values of $\Gamma$ result into a higher probability of detecting multi-GeV neutrinos in 5 years of observation with KM3NeT/ORCA and DeepCore; \\
(iv) such a possibility is increased if high-energy detectors are integrated in the search.

The results obtained with $\Gamma=300$ for all detectors are shown in Fig.~\ref{fig:results_stacking}. Though a higher statistical significance can in principle be obtained by assuming $\Gamma=600$ (lower amount of background  entering the search, mostly because of the smaller angular search window selected, see Tab.~\ref{tab:bkg_angles}), we here present only the results for $\Gamma=300$, since this value is expected to more realistically describe the entire population of GRBs (see e.g. \cite{bulk_lorentz_factor}). With such a value, we obtain that there is a good chance to significantly detect multi-GeV neutrinos by stacking $\sim$900 LGRBs under the hypothesis that their prompt gamma-ray emission is explained by the collisional heating model. As visible, the overall detection significance is characterized by an extended uncertainty band, which is mostly due to the high range of values allowed for the intrinsic properties of the GRB population, namely $T_{90}$ and $F_\gamma$. While reflecting the observed distributions, the spread in GRB luminosity can lead to quite different sample realizations, which might impact the analysis results into a non significant outcome. The situation improves when combining low and high-energy detectors, as shown by the case with $\Gamma=300$ in Figs.~\ref{fig:e} and \ref{fig:f}, such that a sensitivity above $3\sigma$ is generally expected to be achieved after analyzing few hundreds of GRBs.\\
Note that the stacking procedure here implemented, once applied within the framework of the classical internal shock scenario of the fireball model, provides results in terms of expected signal neutrinos and analysis significance compatible to the limits set by the IceCube and ANTARES collaborations with respect to such a model \cite{icecube_analysis,my_analysis}. Though minor differences arise because of the adoption of trigger level effective areas and full efficiency for neutrino detectors in this work, the comparison highlights the validity of the methods here developed and the consequent conclusions.
In view of the promising results here obtained, we strongly encourage to perform optimized stacking analyses for testing the inelastic collisional model, and either confirm its occurrence or constrain the amount of GRBs possibly powered by this mechanism. \\
Note that the quasi-diffuse signal flux expected to arise as a result of the collisionally heating mechanism in the 875 LGRBs of our sample would result at the level of $\sim 2 \times 10^{-9}$~GeV~cm$^{-2}$~s$^{-1}$~sr$^{-1}$ at $\rm E_\nu \sim 100$~GeV. This value is much smaller than the atmospheric neutrino background flux at the same energy, which is rather of the order of $\sim 5 \times 10^{-4}$~GeV~cm$^{-2}$~s$^{-1}$~sr$^{-1}$. These numbers highlight the challenging task of pure diffuse searches in revealing the presence of a tiny signal, like that from the GRB population, on top of the huge atmospheric background. In turn, as Fig.~\ref{fig:results_stacking} demonstrates, the stacking approach provides a more promising perspective than the pure diffuse analysis.
In particular, the IceCube and DeepCore detectors could already have collected enough data to constrain the model here investigated and eventually confirm our finding, with the analysis technique here presented. This result encourages dedicated stacking analyses, optimized for energies lower than 1 TeV, which have not been implemented yet relatively to the GRB population at such low energies.

\section{Summary and Conclusions}
\label{sec:conclusion}
In this work, we considered GRB jets consisting of protons and neutrons, where a fraction of the outflow kinetic energy is converted to thermal energy and radiation via inelastic nuclear collisions occurring in the photosphere. This hypothesis significantly deviates from the classical model explaining the GRB observed radiation through particles accelerated at internal shock in the optically thin region of the jet. In the photospheric scenario, a thermal spectrum is released near the photosphere and this is then modified by a dissipation mechanism related to the above mentioned $pn$ collisions. Such collisionally heated GRBs could produce multi-GeV neutrinos, namely neutrinos with energies much lower than those produced in photo-hadronic mechanisms so far investigated in the context of astrophysical neutrino data analyses. Hence we tested the possibility to detect low-energy neutrinos, on top of the expected atmospheric background, with current and under construction neutrino telescopes. As a result of our investigation, we found that these detectors are able to explore the occurrence of inelastic collisions in GRB jets by means of a stacking analysis of upgoing tracks with data collected in coincidence with $\sim$900 LGRBs.
As previous experimental studies conducted with neutrino data indicate, it is likely that such a number of LGRBs will actually be selected for analyses after more or less 10 years of data taking \cite{antares_first_grb_analysis,my_analysis,icecube_grb2016,icecube_analysis}. We remark that the search for upgoing events requires detectors in different hemispheres to probe the entire population of GRBs, as to guarantee full sky coverage.\\
According to our results, short GRBs alone do not provide enough signal. Concerning individual GRBs, we conclude that only nearby and very energetic GRBs (rare events) can produce at least one signal event in the available detectors. The key role of neutrinos in assessing the origin of the prompt radiation emerging from GRBs demonstrates the importance of dedicated searches in the multi-GeV domain, that we encourage to start,
by combining data collected both by low and high-energy detectors (DeepCore+IceCube and KM3NeT/ORCA+KM3NeT/ARCA). A detection of such a neutrino emission would allow to establish the baryonic nature of GRB jets, although within the context of a model that does not directly involve particle acceleration. In fact, so far, the lack of a correlation among gamma-ray signals from GRBs and neutrinos did not allow to distinguish among the possible leptonic or hadronic nature of radiation from GRB jets. Furthermore, the detection of multi-GeV neutrinos in coincidence with GRBs would provide information on the occurrence of photospheric dissipation, as well as the on the jet composition.

\begin{figure*}[h!]
\subfigure[\label{fig:a}]{\includegraphics[width=\columnwidth]{stacking_estimation_300_long_orca.pdf}}
\subfigure[\label{fig:b}]{\includegraphics[width=\columnwidth]{stacking_estimation_300_long_deepcore.pdf}}
\subfigure[\label{fig:c}]{\includegraphics[width=\columnwidth]{stacking_estimation_300_long_arca.pdf}}
\subfigure[\label{fig:d}]{\includegraphics[width=\columnwidth]{stacking_estimation_300_long_icecube.pdf}}
\subfigure[\label{fig:e}]{\includegraphics[width=\columnwidth]{stacking_estimation_300_long_orca_arca.pdf}}
\subfigure[\label{fig:f}]{\includegraphics[width=\columnwidth]{stacking_estimation_300_long_deepcore_icecube.pdf}}
\caption{Level of significance $n_{\rm s,tot}/\sqrt{n_{\rm b,tot}}$ (left y-axis) achieved by stacking 875 LGRBs (equivalent to $\sim$ 5 years of half-sky search) with $\Gamma=300$, under the assumption that the gamma-ray prompt emission is originated by $pn$ collisions at sub-photospheric radii (inelastic collisional model). The level of signal and background in each detector (indicated in the right y-axis for the median result) are estimated at trigger level. Results are shown for the following neutrino detectors: (a) KM3NeT/ORCA, (b) DeepCore, (c) KM3NeT/ARCA, (d) IceCube, (e) KM3NeT/ORCA+KM3NeT/ARCA, (f) DeepCore+IceCube. The shaded red and grey regions indicate the uncertainty bands at one and two standard deviations, respectively, obtained with percentiles. The horizontal dashed black lines highlight the levels of significance $n_{\rm s,tot}/\sqrt{n_{\rm b,tot}}$=3 and $n_{\rm s,tot}/\sqrt{n_{\rm b,tot}}$=5.}
\label{fig:results_stacking}
\end{figure*}

\section*{Acknowledgmements}
We thank the anonymous referee for the helpful comments, and constructive remarks on this manuscript. The authors acknowledge the support from the Amaldi Research Center funded by the MIUR program "Dipartimento di Eccellenza" (CUP:B81I18001170001), the Sapienza School for Advanced Studies (SSAS) and the support of the Sapienza Grant No. RM120172AEF49A82.
We gratefully acknowledge Kohta Murase for the useful discussions and the material provided, which has allowed the model investigation. We also thank Dafne Guetta for the fruitful conversations on the topics treated in the present paper.

\clearpage

redpajama_set_name: RedPajamaArXiv


text:
By Simon Batt / Coding Concepts Articles for Kids / October 2021 Issue
Image by K?rlis Dambr?ns on Flickr
As the world moves from 4G to 5G, people are enjoying faster download speeds on their mobile phones. The thing is, what is a "G," anyway? Why did it take so long to add another G to 4G and make it 5G? And how long will it be until we can add another one and get 6G?
As it turns out, the "G" doesn't really mean a whole lot in technological terms. It does in the way that 5G is faster than 4G, but a "G" isn't a direct representation of computing power. It's not the same as, say, the gigabytes in RAM or the gigahertz in a processor; both of which are direct measurements of how capable the hardware is.
In fact, all the "G" stands for is — ready for this? — "Generation." Yes, it's that simple. 4G is the "fourth generation" of mobile data technology, and 5G is the "fifth generation." Whenever cellular data technology advances a huge step, we christen it the next generation of technology. When this happens next, we'll get 6G.
But hold on a minute. We have 4G, and we're moving onto 5G. But if 4G is the "fourth generation," that means there were three other generations before it, right?
You don't need to look too hard to find 3G. The world used to use it as the primary way to go online with their phones, but when 4G arrived, 3G began looking really slow. Now 5G is out, and 3G is looking very, very slow — but it's still around for people to use.
Before then, however, were the other generations. 0G is a term used for the very start of mobile phones, and it's labelled "Generation 0" because it doesn't use cellular data at all. Instead, these chunky phones used radiotelephone technology to call other people. These came into the scene around 1945, and lasted until the 1980s when 1G came in.
1G brought about the cellular technology that mobile phones use these days. These connect to data towers placed around the countries, and the range of each data tower is a "cell." That's why it's a "cellular network" and why we had "cellphones." 1G was pretty slow, clocking in at 2.4 kbps. It also used an "analog" data signal to send information.
2G was a lot faster at 64 kbps, but it was still slow to modern standards. 2G rolled out in 1991, and used a digital data signal instead of analog. The digital format resulted in less errors and allowed calls to be digitally encrypted, so it was a lot better than 1G.
So there you have it. A 5G connection isn't just five Gs slapped together; in fact, it's the fifth version of the technology that helps connect us together. As such, who knows what 6G will look like? Guess we'll have to wait and find out!


In this project, I will show you how to make ANY printer in your house AirPrint Compatible. AirPrint is the service that allows all of the i-Devices to print to an actual printer without having to put the file on Google docs and print it from there. So Lets get to it!
Be Sure that you are an administrator on your computer. Go to Control Panel > User Accounts and Family Safety > User accounts, and on the right hand side, you will see a box with your account information. Make sure that it says Administrator under your name.
Make your printer Shared. Go to Devices and Printers, and Right Click on the printer you want to make AirPrint Compatible, and click Printer Properties. Then Click the 'Printer Properties' Option That will bring up a window, and you want to click the tab on the top that says sharing. Check both checkboxes, and click apply.
Now go to My Computer > C Program Files (x86), and create a new folder there called AirPrint with the same capitalization as I wrote it.
You will see a little bit of flashing on the screen, and there will be a firewall window coming up. You want to click Allow Access.
Now go onto your iPad. Go to Photos > Export (The Box with an arrow)>Print, and you should see your printer there!
Thewbot was created based on the A.L.I.C.E. Artificial Intelligence Framework and has been expanding ever since its incarnation in 2012. Thewbot is still not complete, though. It is always learning. Please correct the bot if it says something back to you that does not make a lot of sense. I try to do my best, but I can never predict just what A person will say to the robot. So challenge the robot– ask it tough questions! The robot can only get better here on out.


text:
Home MGM+ Originals
NOTABLE CURRENT SERIES
An epic romantic adventure series based on the life of famous American outlaw Billy the Kid — from his humble Irish roots, to his early days as a cowboy and gunslinger in the American frontier, to his pivotal role in the Lincoln County War and beyond.
Genre: Adventure / Romance
No. of Seasons: 1
Status: Renewed for a Second season; premiere TBA
Canadian Broadcast: Paramount+ Canada
Britannia is the epic story of the Roman invasion of Britain in 43AD that forces rival kingdoms to join forces.
Genre: Historical Fantasy drama
Status: Third season premiered November 19, 2021
Canadian Broadcast: CBC Gem
Set in the 1850s, the series follows Captain Charles Boone (Adrien Brody) who relocates his family to their ancestral Maine home. Charles has to soon confront his family's sordid history and fight to end the darkness that has plagued them for generations.
Genre: Horror drama
Canadian Broadcast: CTV Sci-Fi Channel
Based on the novel Six Days of the Condor by James Grady, Condor follows CIA analyst Joe Turner (Max Irons) who stumbles onto a plan that threatens the lives of millions.
Status: Renewed for a Third season; premiere TBA
Canadian Broadcast: Super Channel Fuse
After 10 years in exile, Livia Drusilla, the golden girl of the prominent Claudii family, returns determined to regain everything that was stolen from her. Domina follows Livia's journey from a naïve young girl to Rome's most powerful Empress.
Genre: Historical drama
Canadian Broadcast: Crave
FROM unravels the mystery of a nightmarish town that traps all those who enter. As the unwilling residents search for a way out, they must also survive the threats of the forest including the terrifying creatures that come out at night.
Genre: Sci-Fi / Horror
Status: Renewed for a Second season; premieres April 23, 2023
Godfather of Harlem tells the "true story of infamous crime boss Bumpy Johnson, who in the early 1960s returned from ten years in prison to find the neighborhood he once ruled in shambles.
Genre: Crime drama
Canadian Broadcast: Disney+ Canada
Frustrated with military command and their handling of the war in North Africa, David Stirling and Jock Lewes formulate a plan to parachute men into the desert to attack enemy forces from behind the front line.
Canadian Broadcast: Amazon Prime Video Canada
In this multifaceted re-imagining of the timeless classic by H.G. Wells, a catastrophic attack on Earth by intelligent extraterrestrial life forces the remainder of humanity to struggle for survival.
Genre: Sci-Fi drama
Status: Third season premiered September 14, 2022
NOTABLE ENDED SERIES


Made with five varieties of early season tree ripened pears. No concentrates, just 100% Fresh juice, love and passion.
Eighty years ago Erroll Chamberlain created Chamberlain Orchards. Four generations later, great grandson Damian uses the original trees to produce this semi dry Perry on the original orchard.
We only produce 45 cartons of this magnificent Perry each year.


The qualities of water create an ideal therapy environment to treat many conditions. The characteristics of water create an environment where you are weightless which reduces stress on the joints and allows for balance training without the fear of falling. Patients can start rehabilitation earlier than with standard therapy because movement in water does not cause stress to the injured site. Aquatic therapy relaxes tight muscles, increases blood flow, and makes therapy less painful.
Aquatic Physical Therapy is covered by most insurance companies with a written prescription from your physician. Simply ask your doctor if Aquatic Physical Therapy is right for you or call us for a free consultation.


The Whetman® SCENT FIRST® Collection is characterized by its delightfully spicy fragrance, compact free flowering habit, silver-blue foliage, and lengthy blooming periods. Ideal for compact containers.
Eternity 'Wp05 Pp22': Highly fragrant semi double blooms, rose pink in color with a darker eye, carried on sturdy stems. Repeat blooming.


Having Spoken about defilement coming from within, rather than outside someone, Jesus again retreats from the crowds and then encounters a Gentile woman who might be considered to be defiled herself. The disciples want rid of her (a Gentile and a woman!), and Jesus playfully challenges her with a commonplace insult (Gentiles were called 'dogs' by Jews). Her response is clever, and while it acknowledges the primacy of the Messiah's mission to Israel, it also hints at the future opening up of the kingdom to all believers. Jesus concurs, and her daughter is healed.
or Box Office PO Box84 Lymington SO41 3ZA with a cheque to Music at Beaulieu and a s.a.e.
The Benefice Office is now fully installed in the Vicar's vestry in the Abbey Church. The phone number is still 01590 612242 and the answer-phone will be cleared every day. In an emergency please ring one of the church wardens.
Our church magazine, parish news or whatever name it is known by is thoroughly good value at 50p. A lot of people, churchgoers and non churchgoers, like to read it from cover to cover but some people I know say "O I never get one" or "I never read it." If you are one of these then try it. I guarantee there will be something of interest, however small and 50p really isn't much. I would be sad to see it go.
Weddings: We pray for Philip Graham Woodhead and Tessandre Elaine Matwychuk, married on Saturday 16th August in the Abbey Church.
The prophet Isaiah calls God's people to bear witness that the Lord is the only God and to proclaim as witnesses all that the Lord has done for them.
Through the apostles chosen by Jesus and sent to bear witness to his resurrection, God continues to work miracles of healing and deliverance and more people come to believe in Jesus, the Son of God, as they witness these signs and wonders.
Jesus teaches the disciples that although they will be with him in heaven, while they are his apostles in the world they must follow his example and be humble servants of others, not seeking power and glory for themselves.
As we are in an Interregnum, there will be no Daily Offices in any of the churches in the Benefice. Normal Sunday services in all the churches and Wednesday Holy Communion Services in the Abbey Church will continue as usual.
Please note the new e mail address at the top of the page.


Chelsea boot in bright transparent pvc with elastic band on ankle sides and cut &sewn inner sock with pattern "Green Tropical Flowers". Made in Italy. Size run: 35-41.
previous: Chelsea boot in bright transparent pvc with elastic band on ankle sides and cut &Sewn lining with pattern "Coffee colour Maculato"


text:
Verstappen leads Red Bull one-two in second Belgian GP practice
By Luke SmithAug 26, 2016, 9:32 AM EDT
Max Verstappen headed up a Red Bull one-two in the second Formula 1 practice session for the Belgian Grand Prix on Friday afternoon at Spa-Francorchamps.
After seeing Nico Rosberg and Lewis Hamilton lead for Mercedes in FP1, Red Bull bounced back in the second session with Verstappen setting a fastest lap of 1:48.085.
Verstappen finished three-tenths of a second clear of teammate Daniel Ricciardo at the top of the timesheets, giving the army of Dutch fans that had made the trip to Spa plenty to smile about.
Mercedes opted to alter its usual FP2 running plan by getting both Rosberg and Hamilton to focus on their long-run pace ahead of Sunday's race instead of chasing optimum lap time.
Rosberg finished the session sixth-fastest as the leading W07 Hybrid driver, with Hamilton down in P13. The Briton also has a 30-place grid penalty hanging over him for the race.
Nico Hulkenberg continued Force India's impressive start to the weekend by finishing third-fastest for Force India, with teammate Sergio Perez following half a second behind in P5. Ferrari's Sebastian Vettel split the pair in fourth, while Kimi Raikkonen was seventh in the second SF16-H.
Haas drivers Romain Grosjean and Esteban Gutierrez both finished inside the top 10 in FP2, ending up P8 and P10 respectively at the checkered flag. Jenson Button was ninth for McLaren.
The session was without major incident bar one short Virtual Safety Car period following a stoppage for Renault's Jolyon Palmer. Palmer was able to get his car back going again while sat in the run-off area and returned to the pits.
The on-track action at Spa resumes on Saturday with FP3, live on the NBC Sports app and on desktop from 5am ET.


Last weekend, my wife and I were hiking in the Stehekin Valley, some 51 miles up lake from Chelan. I turned a corner in the trail and I heard big sounds from the brush about 75 feet from where I stood. And there I saw my first black bear chewing up a ripe blueberry bush! I was downwind from this bear, so he couldn't smell my presence. I started yelling at the bear to leave (I knew that announcing my presence would suggest that he find another place to dine). But instead of ambling off, he stood up on his hind legs, leaned against a tree and turned and looked directly at me! He was huge! My heart started pounding and we slowly walked backwards as he dropped down to the ground. We retreated about 500 yards away while we made a racket, singing and banging our steel water bottles, hoping that he would mosey on down the hill. There was no way to get past him, as he was about 25 feet away from the trail. We had no other way to go. So we waited, making as much noise as we could! We wondered if he was going to come towards us or leave.
When I saw the bear stand up and look at me, my body said run (the fight or flight response)! But I had read that running makes you look like prey, which could ignite the bears prey instinct. So we slowly walked backwards, looking toward the bear. Diane wanted to be silent ("Hoping that the bear thinks you aren't there any more!"), but the books say to make a racket. The noise kindles the bear's flight response. Walking backwards slowly and making noise are all strategies that are counter to what our bodies wanted us to do!
The bear and I have something in common other than loving blueberries! (At least I don't eat the branches and leaves too). We both have sympathetic nervous systems that awaken the flight or fight response when confronted by a potential threat. After about 15 minutes we slowly walked forward, making noise, and thankfully, Mr. or Ms. Bear decided to eat blueberry bushes somewhere else. Phew!
The moral of the story—There are many situations in life where it makes good sense to override the wisdom of your body and use the knowledge and insight of your head. Fortunately, in modern life, a bear rarely confronts us. More commonly, an angry spouse, a difficult co-worker, an irritated customer, a demanding supervisor, an impolite driver, or a grumpy neighbor challenges us.
Your body is wired to react. But your brain can also employ good judgment, by using past experience, learned strategies, knowledge, and wisdom. All of those facets of our mind help us to pick a better path.
They help us do the right thing. They help us choose wisely.
Yes, it is important to listen to your intuition (that will be another post) and your emotional response. But, when facing a modern challenge or potential conflict, use your head.
Lets hear about your wildlife encounters in the rugged Northwest!
I was driving up a logging road on Green Mountain one time about 15 years ago, when a grizzly cub jumped out of the bushes and ran side by side with my car for about 100 feet or so before jumping back into the bushes. He gave me the impression that he thought we were playing - race you to the switchback! It was one of the most amazing moments of my life, but in addition to the awe of the moment, I also vividly remember thinking, "if the cub is right here, where's his mom!?" I knew that she couldn't be far, and THAT was a scary thought!


← Lily, The Lucky Dog!
In the spirit of the Olympics (and Michael Phelps' amazing performance) and the release of the Hitchhiking Ghosts photo yesterday, here's Michael Phelps and Julianne Moore in an Annie Leibovitz 'sDisney Dream Portrait from 2008. Having Phelps as a merman to Moore's Ariel is a nice touch!
This entry was posted in Uncategorized and tagged Annie Leibovitz, Julianne Moore, Michael Phelps, Olympic, Olympic Games, The LIttle Mermaid. Bookmark the permalink.


The various factors of fuels, weather, topography and risk are combined to assess the daily fire potential on an area. Fire danger is usually expressed in numeric or adjective terms. Most of us are familiar with the adjective terms low, moderate, high, very high and extreme. The fire danger rating of an area is a tool to help with the day to day "fire business" decisions. The above maps are simply that, tools. They are tools that can be used to start the process of informed decision making and awareness. Refer to the Fire Danger Color Guide for a description of the colors.
Yesterday's fire danger is the actual observed data, Todays fire danger is a Forecast and like all forecast is on a prediction based on evidence and science. The KBDI represents the condition of the top 8 inches of soil, The Burn Ban map is for reference purposes only. Please check with the local authorities to determine official status of Burn Bans. This information is gathered in part from the NWCG, Texas A&M Forest Service and NOAA.
This information will assist you in finding more specific and geographical information. This page includes many helpful Fire Weather Forecast links for South Texas and the surrounding counties.
The hourly weather graph is a graphical depiction of forecast trends such as temperature, humidity, wind speed and direction, over time. The hourly weather graph is an excellent indicator of not only changes in the weather but an approximate TIME and quality of the changes.
With the cooperation of your neighborhood, or Homeowner's Association, a San Antonio Fire Department member can conduct a fuel assessment of your neighborhood. The information will identify the level of threat your neighborhood faces should a wildfire occur nearby, as well as identify resources available to firefighters. A completed report will help firefighters better protect the residents and their property and may highlight actions the homeowners can take to better prepare their property from a wildfire.


text:
Brighton Beach: Bouncing Back after Hurricane Sandy
As soon as there's a touch of warmth in the air, the kids start asking when we'll be able to go to the beach. So this past Saturday we took advantage of the nice weather and hopped the D train to the Q train to see how our beloved Brighton Beach was doing was doing after Hurricane Sandy.
All in all, we were relieved! We walked the very wide, 2.5-mile-long boardwalk from Brighton Beach at the eastern-most end, past the still-shuttered New York Aquarium, to Coney Island on the western edge. The boardwalk itself survived Hurricane Sandy in good form but sand was piled high around the benches that line the beach side of the boardwalk, and many big drifts of sand still remain across the promenade.
Like many children we observed, Halina, age 7, loved these ad-hoc sandboxes. We hadn't brought any beach toys but she made do by plowing the sand with her hands and rolling around in it to fully absorb its warmth. Many people were out walking the boards, and surf anglers dotted the water's edge. It was wonderful to see so much activity when other beaches are still struggling.
We recently visited Point Pleasant, NJ, another of our favorite beaches that we wrote about in October, just prior to Hurricane Sandy. The damage to the boardwalk and much of the shoreline heading south through Mantoloking was still severe, bordering on apocalyptic in some places. A few restaurants and businesses on surviving (or repaired) sections of the boardwalk were open, including the aquarium, but boardwalk pedestrians and beach wanderers were few and far between. The pre-season crowds you typically see by that time of year still hadn't returned.
Rebuilding Beach Facilities
Though it fared comparatively well, Brighton Beach did not escape totally unharmed, however. Several of the large restroom buildings and shower facilities were damaged and have been permanently closed. Three new restroom buildings are going up along the boardwalk—at New Brighton Street, Brighton 2nd Street, and at West 2nd Street—so big stretches of the beach are currently cordoned off with chain-link fencing. Construction work has been underway practically around the clock, with the goal of having the new facilities open in time for Memorial Day, when beaches open for the season.
The New York Aquarium, which sustained serious damage throughout its campus, is also slated to open partially by Memorial Day.
Unrelated (we believe) to Hurricane Sandy, Surf Avenue—which runs inland along the beach route—is also undergoing a renaissance. Construction was underway at many of the charming, if time-worn, buildings up and down the avenue. It is worth walking this route too, taking mental notes of area because it is destined to change dramatically over the coming years.
Fortunately, Deno's famed and fabled Wonder Wheel and all the other legendary rides at Coney Island were up and running full swing. Owing to massive summertime crowds, we'd never ventured close to that part of the boardwalk but now is the perfect time to go, before the crowds set in.
From the vantage of the Wonder Wheel, the views out to Sandy Hook, NJ, in the south, and Manhattan to the north are amazing. Truly, where else in the world can you take in both vistas simultaneously? Luna Park has obviously received extensive renovations as many of the rides are pristine and new. The famous Cyclone roller coaster was also zooming around its hairpin turns, steep inclines, and deep plunges—but we didn't venture on it. Riley was completely disinterested and while Halina was dying to go, at 4 feet she was too short to ride even with an adult. (Riders need to be 54 inches.)
The D, F, N and Q trains all terminate at the Coney Island-Stillwell Avenue stop, which might be one of the most beautiful stations in New York City. It also has restrooms, which is hardly standard throughout the system. We got off the Q at Brighton Beach to begin our walk there.
Restrooms are open (and new) at Luna Park, Coney Island, and at Asser Levy Park along Surf Avenue at West 5th Street.
Food and beverage options abound, from the trio of Russian restaurants at Brighton Beach to Nathan's Famous hotdogs sold at concessions throughout the area.
What is your Brighton Beach memoir?
Cleaner Cars Help Kids Breathe Better Outdoors
I want kids to get out in nature so they can enjoy all its benefits. Not so they will suffer extra lung damage.


2015-07-01 Mendelssohn: Songs without Words Opus 30 No. 4.
2015-06-01 Mendelssohn: Songs without Words Opus 30 No. 3.
2015-05-01 Mendelssohn: Songs without Words Opus 30 No. 2.
2015-04-01 Mendelssohn: Songs without Words Opus 19 No. 6 - Venetian Gondola Song.
2015-03-01 Mendelssohn: Songs without Words Opus 19 No. 5.
2015-02-01 Mendelssohn: Songs without Words Opus 19 No. 4.
2015-01-01 Mendelssohn: Songs without Words Opus 19 No. 3.