text:
HomeFeaturesNewsSri Lanka: Commonwealth chair Rajapaksha party rejects Latimar House principles of the Commonwealth
Sri Lanka: Commonwealth chair Rajapaksha party rejects Latimar House principles of the Commonwealth
'Latimar House principles a necessity, beneficial to Lanka
UNP MP Wijeyadasa Rajapakshe yesterday claimed that some UPFA ministers didn't know what was good for the country as well as the government.
President's Counsel Rajapakshe said that he was dismayed by the UPFA's opposition to his motion seeking consensus on the removal of judges, of the Supreme Court and Court of Appeal, in accordance with the Latimar House Principles already adopted by several leading members of the Commonwealth.
Those vociferously opposed to Latimar House principles seemed to have forgotten now that Sri Lanka had taken over the Commonwealth leadership, the government couldn't shun them, the UNPer said.
Asked whether he was trying to cause political turmoil, Rajapakshe said that the government should have acted swiftly and decisively to introduce Latimar House principles on its own. Recollecting the circumstances under which the Chief Justice Dr. Shirani Bandaranayake was impeached, Rajapakshe said that the government could have earned the respect of the international community by introducing Latimar House principles.
Rajapakshe said: "My move was meant to prevent political interference in the judiciary. The removal of Dr. Bandaranayake under controversial circumstances underscored the necessity to take corrective measures. In the backdrop of Sri Lanka taking over the leadership of the Commonwealth there cannot be any ambiguity with regard to Latimar House principles."
The former President of the Bar Association of Sri Lanka (BASL) said that adoption of Latimar House principles would send a positive message to the United Nations Human Rights Council (UNHRC) ahead of its next session in March, 2014.
"The Principles provide an effective framework for the implementation of the Commonwealth's fundamental values of democracy, good governance, human rights and the rule of law", the MP said.
Rajapakshe said that the Latimar House Principles envisaged the appointment of a three-member panel consisting of three judges representing Superior Courts of the Commonwealth, other than the country where the move to impeach the CJ was made, to examine the allegations.
The UNPer said that in case allegations were brought against other judges or the President of Court of Appeal, a panel consisting of three sitting or retired judges of the Supreme Court would have to be appointed to go into the issue.
As the appointment of the panel was subject to consensus among the Speaker and Prime Minister representing the ruling party of any Commonwealth nation and the leader of the Opposition, the UPFA need not worry about political instability in the wake of Latimar House principles, he said.
Rajapakshe expressed the belief that the adoption of Latimar House principles would ease international pressure directed at the government over accountability issues.
Rajapakshe switched his allegiance to the UNP several years ago over differences with the SLFP leadership as regards good governance.
Recalling his efforts to arrange for Gen. Sarath Fonseka's release from Welikada, Rajapakshe said that the eventual freedom for one-time army commander eased international pressure, hence helped the government to improve its image. Adoption of Latimar House principles would be beneficial to the government struggling on the diplomatic front.
Rajapakshe said that he would press for reforms and take up the issue with the Commonwealth Secretariat
Shamindra Fernando
Tags: Commonwealth, Independence of judiciary, Sri Lanka
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Headed by neuroscientist Paul Fletcher, the team took 22 volunteers and had them play a cycling game. This is not exactly a large number of subjects, but let's skip that one.
What was the point of all this? Well, the majority of subjects associated the taste of the tea with the jerseys worn by the opposition. This is hardly surprising. So when they were asked to sit in a chair, they avoided the one that had a towel with that jersey design on it.
What does this have to do with real life? Not whole a lot that I can see. There was no control group to play the game without the juice drinks. There was no third group to receive some sort of virtual reward or punishment.
No, this was just the usual quick and dirty, shoddy methodology we have come to expect when anyone does "experiments in video game playing". Poorly thought out, and without proper controls. But of course, experiments conducted the right way likely wouldn't make the headlines. And that seems to be all that counts today.
Still, who knows? Dedicated players of "kill zombie" games, upon meeting one in the street – they're all over these days – would probably start reaching for a shotgun or chainsaw automatically.
Then again, maybe it's the zombies who are conducting these experiments. That would explain a lot.
Well, I remember reading an article by a fan of Rainbow Six games about "How you know you have been playing too much Rogue Spear (Rainbow Six 2)." Two of the amusing symptoms were that you begin to imagine how you would defend your office in case of a terrorist attack, and than you feel a desire to peek first before turning corners.
The funny part was that it was kinda true.
There was also a study that revealed that test subjects who were subjected to lots of First Person Shooter playing had better situational awareness and were better drivers. Not that the first-person shooters had anything to do with driving.
Does this have ANYTHING to do with the kind of silliness certain politicians, journalists, and ambulance chasers want this to mean? Not a bit.
I agree that "the tea vs juice" probably had more to do with the aversion than "the winning vs losing", which would mean that the video game itself was superfluous.
discusses a correlation between "Super Monkey Ball" and surgery.
Hey, I don't know about you but I go around all the time with a shotgun and chainsaw.


The News has two pairs of tickets to give away for the ECHO Players production of Dancing at Lughnasa this April.
The tickets are for the April 6 show. To enter, send your name, home town and phone number to editor@pqbnews.com by 12 noon on Tues., April 3. Or, drop your entry off at our office on Middleton Street in Parksville. On the entry, tell us in which Irish county the play takes place.
The News is also offering another pair of tickets to folks who visit us on Facebook. See our Facebook page for details this week.


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Our Santa Cruz Dowsers Group is now forming. It's wonderful to have such a large group in our town who are dedicated dowsers and diviners. We had our first field trip together to the "Mystery Spot" last weekend.
For those out of town, the Mystery Spot is described as a gravitational anomaly located in the redwood forests just outside of Santa Cruz, California. In the photo above, we are at the bottom of the hill all standing up straight, but at the top in the cabin there is a lot of leaning going on. When I was in the cabin, I realized I had visited the Mystery Spot decades ago with my father. I remember him tall, I was short, and together we were leaning in the little cabin.
All of us walked up the hill to the cabin together. It's so strange, but when you're in the 150 foot radius of this weird energy field, your body gets very heavy and it's hard to move. Once in the cabin, I tested to see what my pendulum would do it spun clockwise, then counterclockwise, and did this the whole time I was in the cabin.


text:
\section{Introduction} The values of the Hubble constant ($H_0$) inferred from  cosmic microwave
background (CMB) anisotropies ($ 67.5 \pm 0.6
\rm ~km\,s^{-1}Mpc^{-1}$~\cite{Ade:2015xua,Aghanim:2018eyx}) and
baryon acoustic oscillations
(BAO) measurements ($66.98 \pm 1.18 \rm ~km\,s^{-1}Mpc^{-1}$~\cite{Beutler:2011hx,Font-Ribera:2013wce,Delubac:2014aqe,Ross:2014qpa,Addison:2017fdm,alam2017})
are significantly smaller than the measurements from observations  of the
nearby Universe using the distance ladder ($74.03 \pm  1.42
\rm ~km\,s^{-1}Mpc^{-1}$~\cite{riess2016,riess2018,Riess:2019cxk}).  The
gravitational lensing time delay measurements in multiply imaged quasar
systems  which are independent of the cosmic distance ladder also gives a
higher value ($72.5^{+2.1}_{-2.3}\rm ~km\,s^{-1}Mpc^{-1}$~\cite{h0licow2017,h0licow2019}).
Recently, an independent calibration of distance ladder without using the cepheids but using the tip of the red giant branch gives a value of Hubble $ H_0 = 69.8 \pm 0.8 (\text{stat.}) \pm 1.7(\text{sys.})  $, which is in between the Planck and cepheid based distance ladder values~\cite{freedman2019}; see also Refs.~\cite{yuan2019,Freedman:2020dne}.
 This tension, calculated
using Gaussian error bars, between the Planck CMB and local Hubble
measurement  stands {at approximately $ 4\,\sigma$
  \cite{Riess:2019cxk,Aghanim:2018eyx}.}
  Increasingly, this
tension is being seen as a hint of physics beyond the  $\Lambda$CDM
cosmology~\cite{barreira,umilta2015,Lesgourgues:2015wza,Alam:2016wpf,DiValentino:2016hlg, Qing-Guo:2016ykt,Ko:2016uft,Karwal:2016vyq,Kumar:2016zpg,renk2017,DiValentino:2017zyq,DiValentino:2017iww,DiValentino:2017oaw,
	Bolejko:2017fos,DiValentino:2017rcr,Lancaster:2017ksf,Khosravi:2017hfi,Buen-Abad:2017gxg, DEramo:2018vss,Dutta:2018vmq,Banihashemi:2018has, belgacem2018,Pandey:2019plg,Agrawal:2019lmo,Agrawal:2019dlm, DiValentino:2019exe,
	Desmond:2019ygn, Pan:2019cot,
  Vattis:2019efj,Poulin:2018cxd,lin2019,Li:2019san,Alexander:2019rsc,lin2019b,DiValentino:2019ffd,Archidiacono:2019wdp,Knox:2019rjx}, rather than a
manifestation of possible systematics in the local distance
ladder~\cite{Shi:1997aa,efs2014,Aubourg:2014yra,Odderskov:2014hqa,Macaulay:2018fxi,Aylor:2018drw,Taubenberger:2019qna,Kenworthy:2019qwq,Rameez:2019wdt}.

The spectacular success of the standard models of cosmology and particle
physics in describing all cosmological and particle physics observables,
however, makes the task of explaining the Hubble tension from \emph{new
  physics} (NP) rather nontrivial.  Particularly in this context, if the
CMB data are to be reinterpreted with NP, the peaks and troughs of the power
spectra must match data at least as well as the $\Lambda$CDM
parametrization of the big bang cosmology.  {The locations of acoustic
  peaks~\cite{sz1970c,Peebles1970} in CMB  data approximately correspond to
  the extrema of the cosine function characterizing the photon temperature
  transfer function,} $\cos(kr_{\ast} + \phi)$, where $k$ denotes  the
comoving wave number, $r_{\ast}$ is the comoving sound horizon at
recombination, and $\phi$ {is the phase shift with contribution
  ($\phi>0$) from
free-streaming neutrinos in  $\Lambda$CDM cosmology
\cite{Bashinsky:2003tk}. The peak
  positions correspond to the } wave numbers $k_{\rm peak}$, which satisfy  $\kpr_{\ast} = m\pi-\phi$, where $m\ge 1$ is an integer. The corresponding observed CMB peak multipoles $ (\ell_{\rm peak}) $ are given by
\begin{equation}
\begin{split}
\ell_{\rm peak}\ \approx \ k_{\rm peak} D_{\rm A} \ = \ \left(  m\pi -\phi \right) \frac{D_{\rm A}}{r_{\ast}} \; , \qquad \text{where} \\
 D_{\rm A} = \int_0^{z_{\ast}} d \! z \frac{1}{H(z)} \; , \qquad \qquad  r_{\ast}=\int_{z_{\ast}}^{\infty} d \! z   \frac{c_s(z)}{H(z)} 	\; ,
\label{Eq:rs}
\end{split}
\end{equation}
{$c_s(z)$ is the speed of sound in the baryon-photon plasma, $ H(z) $ is the Hubble parameter, and
  $D_{\rm A}$ is the comoving angular diameter distance to the redshift of
  recombination $z_{\ast}$. Finding a solution to the Hubble tension requires
keeping $\ell_{\rm peak}$ fixed while increasing $H_0$.

We see from
Eq.~\eqref{Eq:rs} that we can modify the late-time evolution of the Universe,
i.e., modify $H(z)$ for $z< z_{\ast}$, in such a way that $D_{\rm A}$ remains
unchanged but $H_0\equiv H(0)$ is pushed higher, to reconcile CMB/BAO or \emph{acoustic} $H_0$
with local $H_0$~\cite{barreira,DiValentino:2016hlg, Qing-Guo:2016ykt,Kumar:2016zpg,Bolejko:2017fos, renk2017,DiValentino:2017zyq,DiValentino:2017rcr,Khosravi:2017hfi,DiValentino:2017iww,Dutta:2018vmq,belgacem2018,Banihashemi:2018has,Agrawal:2019dlm,DiValentino:2019exe,Desmond:2019ygn,Pan:2019cot,Agrawal:2019lmo,Li:2019san,DiValentino:2019ffd}. Since in these solutions the early
expansion history of the  Universe ($H(z)$ for $z> z_{\ast}$) is unchanged, $r_{\ast}$ remains
unaltered. Therefore, $\ell_{\rm peak}$ remains unchanged from the observed
$\Lambda$CDM values.}    {A second class of proposals rely on altering
the cosmology before radiation domination, i.e., $H(z)$ for $z\gg z_{\ast}$. These
solutions } change $r_{\ast}$, while at the same time keeping $r_{\ast}/D_{\rm A}$
fixed~\cite{umilta2015,Lesgourgues:2015wza,Alam:2016wpf,Ko:2016uft, Karwal:2016vyq, DiValentino:2017oaw,
  Lancaster:2017ksf,Buen-Abad:2017gxg, DEramo:2018vss, Vattis:2019efj, Pandey:2019plg,Poulin:2018cxd,lin2019,Alexander:2019rsc,lin2019b,Archidiacono:2019wdp}.    {\emph{All of the solutions} that have been proposed
so far to alleviate the Hubble tension fall into the above two classes and, in particular, keep the acoustic scale at recombination $\theta_{\ast} = r_{\ast}/D_{\rm A}$
fixed} even after accommodating a larger Hubble constant.

\begin{figure*}
	\centering
	\includegraphics[width=0.85\linewidth]{lcTT-Hf3Gv2-6p}
	\caption{{CMB temperature (TT) power spectrum around first six acoustic peaks. The
			leftmost solid red line is the best-fit Planck \cite{Aghanim:2015xee} temperature power
			spectrum with a best-fit value of $H_0=67.9~{\rm
				kms^{-1}Mpc^{-1}}$. Introducing DNI, keeping all other cosmological parameters fixed,
			moves all peaks to the right/higher $\ell$ with larger shift for
			higher $\ell$ peaks (rightmost solid blue curves).

			However, DNI with higher $H_0$
			brings the peaks back to the
			original positions (dashed blue).  The amplitudes of DNI power
			spectra for each peak is adjusted so that the peak height
			is the same as the $\Lambda$CDM. Also shown as points with
			error bars is the binned
			Planck power spectrum.}}
	\label{fig:lcttee-hf}
\end{figure*}

\section{Undoing neutrino phase-shift}
In this paper, we propose a new class of solutions in which NP solves the Hubble tension by inducing changes in the phase shift $\phi$. These solutions are characterized by acoustic scales $\theta_{\ast}$ which are different from the acoustic scale in the $\Lambda$CDM model. To understand the nature of NP that can
accommodate a larger $H_0$, {let us consider a flat $\Lambda$CDM
cosmology, with the Hubble parameter given by $H(z)^2=H_0^2\left[\Omega_{\rm m}(1+z)^3
  + \Omega_{\rm r}(1+z)^4 + \left( 1- \Omega_{\rm m} - \Omega_{\rm r}\right) \right]$, where $\Omega_i$ are
 the ratios of physical energy densities $ (\rho_i) $ to the critical energy
density
today and $i=m,r$ for total nonrelativistic
matter and total radiation, respectively. To separate out the effect of changing $H_0$, let us keep the
physical energy densities of matter and radiation, $\Omega_{\rm m} H_0^2$ and $\Omega_{\rm r}
H_0^2$, fixed.  A change
$H_0^2\rightarrow H_0^2 + \delta (H_0^2)$ then
implies $H(z)^2\rightarrow H(z)^2+\delta(
H_0^2)$.\footnote{{We note that including a curvature term, $\Omega_{\rm K}(1+z)^2$,
  will result in a redshift-dependent change in the Hubble parameter and
  therefore cannot compensate for a constant shift in $H(z)^2$.}} This constant shift in $H(z)$ is only important at low redshifts and becomes unimportant at high redshifts,
when $H(z)$ is much larger, and thus has negligible effect on $r_{\ast}$. Therefore, we
see from Eq. \eqref{Eq:rs} that
increasing $H_0$ ($\delta (H_0^2)>0$) decreases $ D_{\rm A} $
($\delta D_{\rm A}<0$).}  If $\delta D_{\rm A}$ is
to be compensated mostly from the shift in $\phi$ so that $\ell_{\rm peak}$ remains unaltered, we get from
  Eq.~\eqref{Eq:rs}

\begin{equation}
\frac{\delta D_{\rm A}} {D_{\rm A}}  \ - \ \frac{\delta \phi_m} {m\pi -\phi}  \ = 0
\quad \Rightarrow \quad
\delta \phi_m   \ \approx \  {m\pi } \frac{\delta D_{\rm A}} {D_{\rm A}}  \; ,
\end{equation}
where we have explicitly used the notation $\delta \phi_m$ to refer to {the
fact that
the needed change in phase shift is different for different peaks. We have
also used the fact that $\phi \ll \pi$ in the approximate equality.}
Therefore, if NP needs to accommodate a larger $H_0$, it must induce a
\emph{negative} change in the phase shift that increases with $m$.

Incredibly, \emph{undoing} the phase shift from free-streaming neutrinos in
the standard $\Lambda$CDM cosmology \cite{Bashinsky:2003tk} produces
{almost exactly the required effect (see Fig. \ref{fig:lcttee-hf}).}  Neutrinos
with NP interactions
scatter  and do not free stream, effectively generating a
negative phase shift with respect to $ \Lambda $CDM. Even though there exists a plethora of studies of cosmological
impacts from
nonstandard neutrinos interaction~\cite{Bell:2005dr,Mangano:2006mp,Serra:2009uu,Cyr-Racine:2013jua,Archidiacono:2013dua,Wilkinson:2014ksa,Boehm:2014vja,Bertoni:2014mva,Escudero:2015yka,2015JCAP...07..014F,Lancaster:2017ksf,Oldengott:2017fhy,Kreisch:2019yzn,2019arXiv190407810F,DiValentino:2017oaw,Ghosh:2017jdy}, as well as studies of phase shift in the context of varying relativistic degrees of freedom ($ N_\text{eff} $) on the phase shift~\cite{Follin:2015hya,Baumann:2015rya,Pan:2016zla,Baumann:2017lmt,Baumann:2017gkg,Choi:2018gho,Baumann:2019tdh}, a detailed study of the impact of new neutrino
interactions
on
the scale-dependent acoustic phase shift while keeping $ N_\text{eff} $ fixed at the standard value of $ 3.046 $ has not been performed yet.

\section{DNI : Dark Neutrino Interactions} In this work, we present a simple proof-of-principle model, namely, Dark Neutrino
Interactions (DNI), where a
component of dark matter interacts with neutrinos stopping them from free streaming. {The DNI undo the
phase shift induced by the free streaming neutrinos in the standard model
and thus push $H_0$ to higher values and yet are} safe from all
cosmological and particle physics bounds.  The necessary feature of this
model is a two component dark matter.  Only a small  fraction, $f  $, of the total dark
  matter (DM) energy density $ (\Omega_{ \rm DM}) $ is contributed by the component $ ({\rm namely,}~ \chi) $ that interacts
with neutrinos, the rest being the standard non-interacting cold dark
matter (CDM).
\begin{equation}\label{eq:totdm}
\Omega_\chi \ = f \; \Omega_{ \rm DM} \;, \quad  \Omega_{ \rm CDM} = (1-f)  \; \Omega_{ \rm DM} \;.
\end{equation}
Note that having a small $f$ allows us to evade the
constraints typically obtained when all of the dark matter interacts with neutrinos~\cite{Mangano:2006mp, Serra:2009uu, Boehm:2014vja, Wilkinson:2014ksa, Bertoni:2014mva,Escudero:2015yka,Primulando:2017kxf}.
The primary ingredients for our model are therefore $(i)$ an interacting dark matter component, $\chi$; $(ii)$
a messenger, $\psi$ (triplet in flavor); and $(iii)$ an electroweak (EW) gauge invariant effective operator involving the Higgs scalar $ H $ and the lepton doublet $ l $. After $ H $ acquires a nonzero vacuum expectation value ($v$), the effective operator gives marginal  interactions among neutrinos, messengers, and dark matter,
\begin{equation}
\mathcal{L} \ \supset \   \frac{1}{\Lambda} \  \left( H^\dag l \right) \left( \psi \chi \right)  \qquad \Rightarrow \qquad
\     \ \frac{v}{\sqrt{2}\Lambda} \ \delta_{ij}  \ \nu_i \psi_j \chi \;,
\label{eq:interaction}
\end{equation}
where $ \Lambda $ is the scale of the effective operator  and  $i,j$ are flavor indices.  For a possible way to generate the interaction in Eq.~\eqref{eq:interaction} from a ultraviolet complete model using various symmetries see Ref.~\cite{Ghosh:2017jdy}.  By construction,  neutrinos remain massless and all three flavors interact with equal strength.

In this work, we focus on cases in which the mediators and dark matter
are nearly degenerate in mass. As shown in Ref.~\cite{Ghosh:2017jdy}, this allows the
scattering cross-section {($\sigma_{\chi\nu}$) between the dark
  matter and neutrinos to become independent of the neutrino temperature ($
  T_\nu $). The temperature independence of DNI enables neutrinos to
  decouple late, undoing the phase-shift from free streaming
  neutrinos for all the modes entering horizon until
  recombination.}  We can write the ``differential optical depth",
$\dot{\mu}\equiv {\rm d} \mu/{\rm d} \eta$, for neutrinos in the DNI model as
\begin{multline}\label{eq:mudot}
\dot{\mu} =   a n_{\chi} \sigma_{\chi\nu}   =   a \left( \frac{\rho_{\chi}}{m_{\chi}}\right)  \sigma_{\chi\nu}
=  a f u   \rho_\text{dm}
\left(\sigma_\text{th} \over 100\text{GeV}\right),
\end{multline}
where $ a $ is the scale factor; $ \eta $ is the conformal time; $ \sigma_\text{th} = 6.65 \times
10^{-25} ~\text{cm}^2$ is the Thomson cross-section; $n_{\chi},
\rho_{\chi}, m_{\chi}$ denote the number density, the energy density, and
the mass of $\chi$, respectively; and
\begin{multline}\label{eq:uzero}
u \equiv  \frac{\sigma_{\chi\nu} }{  \sigma_{\text{Th}} }\times\frac{100
\text{GeV}}{ m_{\chi}}
 \simeq \left(5.5 \text{TeV} \over \Lambda\right)^4\left(1 \text{MeV} \over m_\chi\right)^3.
\end{multline}

The perturbation equations for $\nu$ and $\chi$ in DNI are coupled together~\cite{Wilkinson:2014ksa} similar to the
perturbations of the baryon-photon system.

We use the notations and  perturbation variables in conformal Newtonian
gauge as defined in  Ref.~\cite{Ma:1995ey}, where
$ \delta_i $, $ \theta_i $ stand for over-density and divergence of fluid
velocity respectively for $ i $-th species.
The total DM transfer functions are just the weighted sum of the
corresponding perturbation variables of the two dark
matter components,
\begin{align}
\delta_{\rm DM} &= f\delta_{\chi} + (1-f)\delta_{\rm CDM}\;,\nonumber\\
\theta_{\rm DM} &= f\theta_{\chi} + (1-f)\theta_{\rm CDM}\;.\label{Eq:f}
\end{align}
In the limit, $f\rightarrow 0$, we recover the standard $\Lambda$CDM
cosmology. In addition, for $f\ll 1$, the total dark matter transfer functions are
negligibly different from the CDM transfer functions and the modifications
to the dark matter power spectrum are of order $f^2$. Thus, the \emph{only}
difference from the $\Lambda$CDM cosmology, when  $f\ll 1$, comes from
modification of the free streaming of neutrinos. This regime is exactly what we
are interested in.

The evolution equations of CDM are unchanged, while the equations of
interacting component of DM, $ \chi $, get additional terms due to interactions. The neutrino Boltzmann equations are also modified, picking up extra
interaction terms,
\begin{align}
\dot{\delta}_{\chi} &= -\theta_\chi + 3\dot{\phi}\;,\\
\dot{\theta}_\chi &= - {\dot{a}\over a}\theta_\chi + k^2\psi - \left(4\rho_\nu \over 3 \rho_\chi\right)\dot{\mu}(\theta_\chi-\theta_\nu)\;,\\
\dot{\delta}_\nu &= -{4 \over 3}\theta_\nu + 4\dot{\phi}\;,\\
\dot{\theta}_\nu &=k^2\left({1 \over 4}\delta_\nu - \sigma_\nu\right) + k^2\psi + \dot{\mu}(\theta_\chi-\theta_\nu)\;,\\
\dot{F}_{\nu l} &= {k \over (2l+1)}\left[lF_{\nu ~l-1}-(l+1)F_{\nu ~l+1}\right] - \dot{\mu} F_{\nu l}\;,
\end{align}
 where $ k $ is the comoving wave number; the dots represent derivatives with respect to the conformal time; $ \phi $ and $
 \psi $ are the Newtonian potentials and $ F_{\nu l} $, with $l \ge 2 $, is the $ l $-th multipole moment of neutrino distribution function.
The initial conditions are also modified as the initial anisotropic stress is zero for tightly coupled neutrinos.

\begin{figure}[t]
	\centering
	\includegraphics[width=\linewidth]{mfpHv7z}
	\caption{Comparison of \emph{optical depth} of neutrinos in DNI $ (fu = 0.034) $ with models of neutrino self-interaction~\cite{Oldengott:2017fhy} and~\cite{2019arXiv190407810F} having different temperature dependences.
          The top axis shows the modes $ \ell_H $ which enter horizon at redshift $ z $.	}
	\label{fig:mfpcomp}
\end{figure}

{We plot the ratio of interaction rate to Hubble rate, $\dot{\mu}/(aH)$, in
Fig. \ref{fig:mfpcomp} for the current upper limits $ (fu=0.034) $ for our model derived in this work. For comparison, we also show cases with  neutrino self-interaction
models~\cite{Oldengott:2017fhy,2019arXiv190407810F} where crosssections vary as $T_\nu^2$ and  $T_\nu^{-2}$.
We see from Fig. \ref{fig:mfpcomp} that with the current upper bounds (fixed $ N_\text{eff} $) on neutrino
interactions, we can significantly modify the free streaming of neutrinos for all scales which enter horizon before recombination \emph{only in the
temperature independent case}.}

\section{Impact on Hubble tension} We have implemented the DNI cosmology in the publicly available code Cosmic Linear Anisotropy Solving
System ({CLASS})~\cite{2011JCAP...07..034B}.

 In DNI cosmology,  the modes which enter horizon earlier
(higher $\ell$) get a larger phase shift (with respect to $\Lambda$CDM cosmology) compared to the modes which enter later as shown in Fig. \ref{fig:lcttee-hf} where we use $ f=10^{-3}, u =34 $.
This is because  the relative contribution of neutrinos (proportional to $ \rho_\nu /( \rho_r + \rho_m) $, where $ \rho_\nu $ is the neutrino energy density) to the metric perturbations
decreases with time as matter starts to dominate the energy density of the
Universe. This is almost exactly the $\ell$ dependence that we need to
alleviate the Hubble tension (Eq.~\eqref{Eq:rs}).
\begin{figure}[h]
	\centering
	\includegraphics[width=\linewidth]{lcTT-ps-3Gv7}
	\caption{Shift of the position of peaks of CMB TT $
          (\Delta\ell_{TT}) $and EE $ (\Delta\ell_{EE}) $  spectrum in
          $\Lambda$CDM and DNI cosmologies $ (f = 10^{-3}, u=34) $ with respect to bestfit $ \Lambda $CDM model with $ H_0 = 67.9 ~\rm km/s/Mpc$.}
	\label{fig:lctt-ps-3}
\end{figure}
{We show this explicitly in Fig. \ref{fig:lctt-ps-3} where we plot
(negative of) the shift in peak positions for the CMB temperature and $E$-mode
polarization angular power spectra $ (\ell(\ell+1)C_\ell /(2\pi)) $ as we
change the Hubble constant in $\Lambda$CDM cosmology from the best fit
value while keeping other parameters ($\Omega_m H_0^2$, etc.) constant.
For reference, we show the maximum effect we can get in the curve labelled ``No
$\nu$-freestreaming"  with
$\dot{\mu}/(aH) \ggg 1$.  We
see that the shift in $\ell_{\rm peak}$ for DNI cosmology, with the current upper
bound in temperature independent interactions, is approximately of the same
size (but in the opposite direction) as $\Lambda$CDM cosmology with $H_0=70 {\rm km/s/Mpc}$.
The scalings in $ \ell $ are also similar in both the cases. The small residual peak shifts at high multipoles are  within the errorbars.
Therefore,
we expect that the Hubble tension should reduce considerably in a DNI
cosmology. We verify this in the DNI curves with $H_0=70 {\rm km/s/Mpc}$, in
which the peak shifts are negligible compared to the best fit Planck
$\Lambda$CDM cosmology.  }

	\begin{figure*}[t]
		\centering
		\begin{subfigure}{0.32\linewidth}
		\centering
		\includegraphics[width=\linewidth]{h0lnu0cf-in5}

		\label{fig:h0fu0}
	\end{subfigure}
	\begin{subfigure}{0.32\linewidth}
		\centering

		\includegraphics[width=\linewidth]{cf1d-H3d-fv2}

		\label{fig:h0fu2}
	\end{subfigure}
	\begin{subfigure}{0.32\linewidth}
		\centering
		\includegraphics[height = 5.4 cm ,width=\linewidth]{H-tenv3}

		\label{fig:H-ten}
	\end{subfigure}
	\caption{The left panel shows $1\sigma,2\sigma,~\text{and}~3\sigma$ constraints in DNI and $H_0$
		for different data set combinations. The light and dark grey band shows $ 1\sigma $ and $ 2\sigma $ band for SH0ES~\cite{Riess:2019cxk} measurement respectively. The central panel shows the
		MCMC samples in the $f-fu$ plane. The right most panel shows
		calculation of Hubble tension (values given in the legend) taking into account
		non-Gaussianity of PDFs. The $ 2\sigma $ upper-limit from P15 is $ fu <0.034 $.}
	\label{fig:mcmc}
\end{figure*}

We perform a Markov-Chain Monte Carlo (MCMC) analysis of the DNI  model
using publicly available code \textsc{Monte Python}~\cite{Audren:2012wb}. In addition to the $ \Lambda $CDM parameters, we varied $ \omega_\chi = \Omega_{\chi} h^2$ and $ u $, where $h\equiv H_0/(100 ~{\rm kms^{-1}Mpc^{-1}})$ is the reduced Hubble constant. The fraction $ f $ was extracted as a derived parameter,  $ f = {\omega_\chi \over \omega_{\rm CDM} + \omega_{\chi}} $, where $ \omega_{ \rm CDM} = \Omega_{ \rm CDM} h^2 $. For all the parameters in the MCMC analysis
we satisfy the Gelman-Rubin convergence criterion $ R - 1 < 0.1 $.

For $ \omega_\chi $ and $ u $ we have used flat priors with no hard prior upper boundaries. The lower
	prior boundary was set to 0 for physicality.
We use the following cosmological data
sets:
Planck CMB 2015 Low-$ \ell $ TEB, High $ \ell $ TT EE TE - Plik lite and CMB lensing T+P~\cite{Aghanim:2015xee} (named `P15')
and  full shape of Galaxy power spectrum measured
by WiggleZ Dark Energy Survey~\cite{PhysRevD.86.103518}. We have checked that in DNI cosmology the difference when using lite vs full likelihood is insignificant. WiggleZ data are sensitive to the modification of matter power spectrum due to the small fraction of interacting dark matter and the strongly interacting neutrinos.
	The WiggleZ power spectrum goes upto $ k=0.5~  h \ \text{Mpc}^{-1} $. We have used
        different $ k $-cutoff of the full dataset for three separate
        analyses and label them W1, W2, W3 for cutoff  $k_\text{max} = 0.12h, 0.2h,
        0.3  h \ \text{Mpc}^{-1}$ respectively.
        We used \textsc{CLASS} Halofit module
        \cite{Smith:2002dz} to incorporate non-linear modifications in the
        power spectrum, since the WiggleZ power spectrum (specifically W2 \& W3) goes
        	upto the k modes where these effects are important. Although the Halofit is tested tool for $ \Lambda $CDM cosmology, since DNI introduce very small changes in the matter power spectrum by construction, the use of Halofit is justified in this case.

We note that for the BAO data, it will be incorrect to use just the BAO scale
(or $\theta_{\ast}$)
extracted from the power spectrum (e.g., Ref.~\cite{alam2017}) assuming
$\Lambda$CDM cosmology, available as BAO likelihood modules in public MCMC codes, to constrain any new physics which
modifies the phase shift $\phi$ of the acoustic oscillations and allows
$\theta_{\ast}$ to vary from the $\Lambda$CDM value. This is the case for us and
also for any model with non-standard $N_{\rm
  eff}$, since any new free streaming relativistic species contributes to $\phi$ in a scale dependent manner.

The marginalized constraints from our MCMC analysis, with two extra parameters ($f$,$u$)  are shown in  Fig. \ref{fig:mcmc}.  The local measurement
from Ref.~\cite{Riess:2019cxk} of $ H_0 = 74.03 \pm  1.42
~\text{km} ~\text{s}^{-1} ~\text{Mpc}^{-1} $ is shown in gray horizontal
bands. There is a clear degeneracy between the
neutrino stopping power ($\propto fu$)  and $H_0$ which reduces the Hubble tension.
We see from the MCMC samples plotted in Fig. \ref{fig:mcmc} (centre) that
stronger neutrino interaction favours higher $ H_0 $. The 2D contours
  clearly indicates that data prefer small $ f ~(\lesssim 10^{-2}) $  and,
  as discussed above, for small $ f $ the results (limits) become
  independent of the value of $ f $ (Eq. \ref{Eq:f}). These are general features of DNI which are present in all the datasets we have analysed.

The 1-D probability distribution functions (PDF)
shown in inset of Fig.~\ref{fig:mcmc} (left) are
highly non-Gaussian. To quantify the tension between non-Gaussian PDFs, we
define a quantity $d=(H_1-H_2)/\sqrt{\sigma_1(t)^2+\sigma_2(t)^2}$, where
  $H_1,H_2$ are two $ H_0 $ measurements and
  $\sigma_1(t),\sigma_2(t)$ are the corresponding `$t$-$\sigma$' upper or lower
  limits.

  For a Gaussian PDF
  $\sigma(t)=t\sigma_G$, where $\sigma_G$ is the Gaussian $1$-$\sigma$
  error. We use Gaussian errorbar for the local $H_0$ measurement and plot
  the quantity $d$ in Fig. \ref{fig:mcmc} (right). The tension is then given by
  the value of $t$ where $d=1$. Our definition is equivalent to the
  usual definition of tension in the Gaussian case. We see that for
  $\Lambda$CDM the tension is at $3.8\sigma$,

  which reduces to $\lesssim 3\sigma$ in
  DNI cosmology.
The small secondary peak for the `P15 + W1' dataset within the $ 3 $$ \sigma $ region results in a jump in $ d $ and reduction in tension to $ 2.1 $$ \sigma $. We note that the effect of neutrino interactions on the matter power spectrum is not just a phase shift in BAO. The matter power spectrum is also enhanced because the perturbations in neutrinos do not decay away completely on horizon entry in DNI cosmology and contribute to metric perturbations. Both the phase shift in the CMB and the modifications of the matter power spectrum help in reducing the tension to $ 2.1\sigma $.

  \setlength{\tabcolsep}{0.4em}
  \renewcommand{\arraystretch}{1.3}
  \begin{table*}
  	\centering

  	\begin{tabular}{l c|c c|c}

  		&\multicolumn{2}{c}{P15+W1+SH0ES} & \multicolumn{2}{c}{P15+W1}\\
  		\hline
  		&$ \Lambda $CDM &  DNI  & $ \Lambda $CDM &  DNI  \\

  		$H_0~(\rm km/s/Mpc)$(bf) & $68.89_{-0.59}^{+0.58}$~$ (68.86) $&$70.25_{-0.61}^{+0.63}$~$ (70.37) $&$68.01_{-0.6}^{+0.58}$~$ (68.08) $&$69.39_{-0.68}^{+0.69}$~$ (69.31) $\\

  		$ fu $ (bf) & $ 0 $ &$0.02321_{-0.012}^{+0.0065}(0.01874)$&$ 0 $& $0.01744_{-0.011}^{+0.0062}(0.01567)$\\

  		$100~\omega_{b }$ & $2.243_{-0.015}^{+0.015}$ & $2.251_{-0.015}^{+0.015}$& $2.226_{-0.016}^{+0.015}$& $2.238_{-0.015}^{+0.015}$\\

  		$\omega_{\rm DM }$ & $0.1176_{-0.0013}^{+0.0013}$ &$0.1181_{-0.0013}^{+0.0013}$&$0.1194_{-0.0013}^{+0.0013}$& $0.1195_{-0.0013}^{+0.0013}$\\

  		$ln10^{10}A_{s }$ & $3.07_{-0.025}^{+0.024}$ & $3.005_{-0.026}^{+0.025}$ & $3.052_{-0.025}^{+0.017}$ & $2.998_{-0.027}^{+0.021}$\\

  		$n_{s }$ & $0.9709_{-0.0046}^{+0.0045}$ & $0.9492_{-0.0048}^{+0.0047}$ & $0.966_{-0.0045}^{+0.0043}$ & $0.9467_{-0.0051}^{+0.0044}$\\

  		$ \sigma_8 $ &$0.8283_{-0.009}^{+0.0088}$ & $0.831_{-0.0092}^{+0.0091}$ &$0.826_{-0.0087}^{+0.0072}$ &$0.8308_{-0.0087}^{+0.0076}$ \\

  		\rule[-2ex]{0pt}{6ex}
  		\makecell[l]{$ 100\theta_{\ast} $\\bf} &\makecell{$ 1.04201_{-0.00030}^{+0.00030}$ \\ $1.04205 $} & \makecell{$ 1.04643_{-0.00078}^{+0.00094}(+14.7\sigma)$ \\ $1.04614(+0.4\%) $} &\makecell{$ 1.04183_{-0.00029}^{+0.00031}$ \\ $1.04188 $} & \makecell{$1.04573_{-0.00087}^{+0.00125}(+13\sigma)$ \\ $1.04587 (+0.4\%)$}\\

  		$ r_{\ast} $(Mpc),bf &$ 145.07 $ & $ 144.93 ~(-0.1\%) $ &$ 144.81 $ &$ 144.52 ~(-0.2\%)$ \\

  		$ D_{\rm A} $(Mpc),bf &$ 12.78 $ & $ 12.71 ~(-0.5\%)$&$ 12.75 $ & $ 12.68 ~(-0.6\%)$\\

  		$ \Delta\chi^2 $ & $ 0 $ & $ -9.08 $ & $ 0  $ & $ -2.42 $
  	\end{tabular}
  	\caption{Parameter table for different data-set combinations with
  		fixed  $f=10^{-3}$ for DNI. Best-fit values are indicated by `bf'. We also show the baryon density ($ \omega_b \equiv\Omega_b h^2 $),  total dark matter density ($ \omega_{\rm DM} \equiv\Omega_{ \rm DM} h^2 $) and the magnitude of matter power spectrum on $ 8h^{-1}~{\rm Mpc}$ scale $ (\sigma_8) $.}
  	\label{tbl:chisq}
  \end{table*}

In Table \ref{tbl:chisq} we present results of a MCMC analysis of DNI cosmology for fixed $ f = 10^{-3} $, only varying $ u $ along with the $ \Lambda $CDM parameters\footnote{We varied the energy density of total DM $ \omega_{\rm DM} $ and set the CDM energy density $ \omega_{\rm CDM} = (1-f) \times \omega_{\rm DM} $ and interacting DM energy density $ \omega_\chi  = f \times \omega_{\rm DM}$.}, where we also include the local measurement of $ H_0 $ (SH0ES collaboration~\cite{Riess:2019cxk}). With respect to $ \Lambda $CDM, $ \chi^2 $ reduces by $ 9 $ in DNI with one extra parameter $ u $. The bestfit value of the Hubble constant turns out to be $ H_0 = 70.4 $.  Note that, as argued before, this increase in $ H_0 $ is associated with a decrease in $ D_A $ which in turn gets compensated mostly from a change in $ \phi $. Therefore, the bestfit for DNI cosmology is characterized by a $ \theta_{\ast} $ which is approximately $ 15\sigma $ away from that of $ \Lambda $CDM. There is however a small change in $ r_{\ast} $ which roughly compensates approximately $ 20\% $ change in $ D_A $.
Interestingly, DNI cosmology is a slightly better fit to the `P15 + W1'
datasets than the $ \Lambda $CDM cosmology and $ H_0 $ tension is reduced
to $ 2.9 \sigma $. Since $ f \ll 1$, the modification of neutrino
	free streaming alone results in a higher $ H_0 $ and the better fit
        of the data.  In particular, the modification of the dark matter
        power spectrum due to the effect of radiation pressure of
	neutrinos on dark matter is not important for $f\ll 1$.

\begin{figure*}[t!]
	\begin{subfigure}{0.43\linewidth}
		\centering
		\includegraphics[width=0.9\linewidth]{f1d-fixed}
	\end{subfigure}
    \begin{subfigure}{0.43\linewidth}
    	\centering
    	\includegraphics[width=\linewidth]{fu-dect_f}
    \end{subfigure}
	\caption{Left: 1-D posterior for $ fu $ for fixed $ f $ DNI
            cosmology (see Table.~\ref{tbl:chisq}). The dashed vertical
            lines marks the $ 3\,\sigma $ upper and lower limit for the
            corresponding dataset. Right: The $ x\,\sigma $ lower limit
            on $ fu $ plotted against $ x $.
          It can be seen from both the plot that $ fu = 0 $ is excluded at
          more than $ 3\,\sigma $ when we include SH0ES data.}
	\label{fig:fu-post}
\end{figure*}

We show the posterior distribution of $ fu $ for fixed $ f ~(=
  10^{-3})$ DNI cosmology  (see Table.~\ref{tbl:chisq}) in
  Fig. \ref{fig:fu-post} (left). DNI cosmology prefers non-zero dark  neutrino
  interactions at $\gtrsim 3\sigma$ in order to reconcile the local Hubble
  measurements with the CMB and high redshift $ (0.2 \lesssim z \lesssim 0.8) $ large scale structure data.
  The dashed lines show the $ 3\sigma $ upper and lower limits of $ fu $. Even without the SH0ES
  data a non-zero interaction is preferred, however, a zero interaction is
  not ruled out as the posterior extends to the $fu=0$ boundary. When we
  include SH0ES data,  the $fu=0$ point is outside the $3\sigma$ lower
  limit. This can be also be seen  in the right panel of
  Fig.~\ref{fig:fu-post} where we plot the $x\sigma$ lower limit vs
  $x$. This curve flattens out when the PDF starts falling sharply for the
  without-SH0ES case as we hit the boundary.   Thus
  we  conclude that non-zero interactions are demanded for reconciliation of
  SH0ES data with Planck and WiggleZ.
 For clarity we also show the posterior distributions of all the parameters in Fig.~\ref{fig:u1e-1p2-vs-u1e-1p3triangle} in Appendix~\ref{sec:app1}. The shift in $ \theta_\ast $ and $ H_0 $ is clearly visible in the figure. The other parameters having significant shift are $ n_\text{s} $ and $ A_\text{s} $.

  We see in Table.~\ref{tbl:chisq} that the bestfit $ fu\approx 2 \times 10^{-2} $ requires $ u \approx 20$. For $ m_\chi\lesssim1~\text{MeV} $ we find the scale of the effective operator to be $ \Lambda \gtrsim 2.5~\text{TeV} $ from Eq. \eqref{eq:uzero} . For this high a $ \Lambda $ we do not expect any significant constraint from particle physics.

\begin{figure}[h!]
	\centering
	\includegraphics[width=0.9\linewidth]{prism-matPSv3}

	\caption{Absolute change in CMB B-modes [primordial (red),
			lensing (black) and combined (pink)] from $ \Lambda $CDM due to
			DNI is shown in the top panel. 	The solid (dotted) lines
			represent enhancement (suppression) of power. The blue dashed
			line shows sensitivity of PRISM~\cite{Andre:2013nfa}. The
			bottom panel shows the fractional change in matter power
			spectrum w.r.t $ \Lambda $CDM cosmology.
	}
	\label{fig:prismbb}
\end{figure}

The gravity of new neutrino
interactions
modifies the $B$-mode CMB power spectrum \cite{Ghosh:2017jdy} and matter power spectrum as shown in Fig.~\ref{fig:prismbb} .
We compare in Fig.~\ref{fig:prismbb} (top) the modification of $ B $-modes for tensor to scalar ratio $ r=0.06 $~\cite{Ade:2015fwj,Ade:2015xua,Ade:2018gkx} with the sensitivity of the proposed experiment Polarized Radiation Imaging
	and Spectroscopy Mission (PRISM)~\cite{Andre:2013nfa}. This effect, in principle, can be detected if $ r $ is close to the current upper limit~\cite{Ade:2015fwj,Ade:2015xua,Ade:2018gkx} with a future PRISM like experiment~\cite{Andre:2013nfa,core,pico,cmbs4,Hazumi2019}.
	In DNI cosmology, the perturbations in neutrinos do not decay away and influence the matter perturbations gravitationally. This results in the enhancement of the matter power spectrum as shown in Fig~\ref{fig:prismbb} (bottom). Of course, there are shifts in the BAO peaks which are analogous to the shifts in the CMB acoustic peaks, as discussed before. The effects in the matter power spectrum are much stronger compared to the CMB B mode. The future Large Scale Structure surveys~\cite{Aghamousa:2016zmz,Amendola:2016saw,Ivezic:2008fe,2011arXiv1110.3193L} will greatly improve the accuracy of matter power spectrum measurements achieving approximately $ 1\% $ accuracy~\cite{2011arXiv1110.3193L} and will therefore be able probe the DNI cosmology.

\section{Conclusions} In this work we have proposed a qualitatively new framework that ameliorates the Hubble tension by primarily using
the phase
shift in the acoustic oscillations of the primordial plasma.
Amazingly, this framework undoes the neutrino induced phase-shift of $ \Lambda $CDM, generates the
shift in the acoustic peaks of CMB with the required scale dependence
and pushes the \emph{acoustic}  $H_0$ higher
towards
 the locally measured value of $H_0$. We note that the BAOs are the imprints of the same acoustic oscillations of the primordial plasma in the matter power spectrum~\cite{sz1970c,Eisenstein:1997ik} and, therefore, any phase shift or the lack of it would be carried over to the BAOs also.

  Using the Planck CMB and WiggleZ (W1) datasets along with SH0ES, we find that new interactions of neutrinos are preferred and no interaction $ (fu=0) $ is disfavoured  at $ \gtrsim 3 \sigma $ (Fig.~5).
  We therefore might have found evidence of new interactions
of neutrinos in the Hubble tension. \emph{Our modified version of \textsc{CLASS} used in this paper is made publicly available at}
\href{https://github.com/subhajitghosh-phy/CLASS_DNI}{https://github.com/subhajitghosh-phy/CLASS\_DNI}.

\begin{acknowledgments}
	This work was supported by Science and Engineering Research Board (SERB),
Government of India Grant No. ECR/2015/000078 and No. ECR/2015/000196. This work was also
supported by Max-Planck-Gesellschaft funded Max Planck partner group
between Tata Institute of Fundamental Research, Mumbai and
Max-Planck-Institut f\"ur Astrophysik, Garching.
The PDF plots and MCMC analysis were done using
public python package \textsc{GetDist}
\cite{Lewis:2002ah}. This work used computational facility
of Department of Theoretical Physics, Tata Institute of Fundamental Research. We thank Basudeb Dasgupta for useful comments. We acknowledge support of the Department of Atomic Energy, Government of India, under Project No. 12-R\&D-TFR-5.02-0200.
\end{acknowledgments}

redpajama_set_name: RedPajamaArXiv


Joyce Murray, David Murray, Freda Chandler, Monisha George and Nigesh Karattu Madathil.
The Eneabba Mingenew Health Service emergency department were gifted an AccuVein infrared vein finder last month to assist clinicians in inserting cannula tubes into patient's veins.
The $10,000 donation was made by the Dongara Denison Lions Club after the nursing team demonstrated the benefits the machine would have on community members if the emergency department were to acquire a machine.
Jeffrey Calver, the WA Country Health Service Regional Director (Midwest) said that the AccuVein machine was especially helpful for finding veins in dehydrated patients, the elderly and children.
"Haemoglobin in the blood is attracted to infrared light which is why the AccuVein machine is helpful to clinicians in finding appropriate veins to place a cannula tube into, especially in dehydrated patients, the elderly and children, where unassisted cannulation may be difficult," Mr Calver said.
The new piece of medical equipment isn't the only donation the health service has received from the Dongara Denison Lions Club. The community group has also donated a shower trolley for the aged care home and along with the Dongara Local Charities, co-donated an i-Stat blood analyser machine to provide clinicians with faster lab results.
"The AccuVein machine is a great piece of innovative equipment and a welcome addition to the Emergency Department. The Eneabba Mingenew Health Service is very fortunate to have such a generous community," said Mr Calver.


text:
4af3f79f-cdae-4af8-985c-6c5e9adb74a7
Foster announces £1m export deal for Deli Lites
Photography: Michael Cooper
Pictured with the Minister making the announcement are Jackie Reid, Deli Lites, and Joe Barrett, Applegreen.
The contract with Applegreen, a leading supplier of convenience foods to forecourt operators in the Republic of Ireland, will see Deli Lites supply Applegreen with an extensive range of gourmet sandwiches and tortilla wraps on a daily basis.
The Minister said: "This very significant contract establishes Deli Lites as a major supplier of gourmet food solutions to Applegreen for its network of more than 70 forecourts throughout the Republic of Ireland. It positions the company for further growth not only with Applegreen, but also many others, in a marketplace which continues to offer substantial business opportunities for Northern Ireland suppliers.
"The clear message from the success of Deli Lites is that Northern Ireland companies can compete and win in export markets. They simply need to invest resources on developing close working relationships with customers and by being flexible as well as responsive to their specific requirements."
Jackie Reid, who formed the business with husband Brian in 1999, said: "The contract is a tremendous endorsement of our products and the customer focus which underpins our business approach. Over the past year, our business has grown by 40 per cent, assisted by a commitment to grow sales substantially in the Republic.
"We've been building a relationship with Applegreen over the past year, which has enabled us to understand fully their food retailing operation, their commitment to provide consumers with premium quality products and their specific requirements especially in terms of healthy eating. Our products, for instance, are free from hydrogenated fats and use only free-range eggs.
"The new business is also benefiting other Northern Ireland companies because of our commitment to source as many ingredients as possible from local suppliers. In addition to support for our current expansion, Invest NI has provided assistance towards new product development, export marketing and staff development as well as expert lead generation advice in our target market," she added.
Adrian Grimes, Head of Food at Applegreen, said: "We are proud to serve over 400,000 customers a week in our forecourts. It's extremely important to us to provide tasty and high quality sandwiches and other delicious sweet treats to our travelling and commuting consumers.
"The response to our teaming up with Deli Lites has been overwhelmingly positive. Since January 2012 Deli Lites has been providing us with a range of excellent food products which have delighted our discerning customers. It's refreshing to work with people that have such passion and take such pride in turning out high quality affordable food. We look forward to working with Deli Lites into the future to develop new and even more delicious ways of making our customers happy."
Adrian Grimes / Applegreen / Deli Lites / Jackie Reid / Joe Barrett / Republic of Ireland / Warrenpoint

redpajama_set_name: RedPajamaCommonCrawl


A new year, a new beginning, a new chance to do it better, to apply the lessons we've had the opportunity to learn in previous months and years.
Recently, an idea was shared with me about similar experiences and places: Why compare? Why not appreciate each as they are. And so as 2017 begins and 2016 is placed in the archives to reflect upon and remember for the joy it brought as well as the challenges it presented, why not see 2016 as the stepping stone to making 2017 even better than imagined?
What lessons were presented to you to learn, or revealed to you that you needed to improve upon in the past year? The quote above is a gentle reminder that living well is a skill. It is something we learn how to do based on observing the proper models, practicing what we have learned and coming to fully understand why we are doing what we practice. Tomorrow's first episode of the podcast in 2017 will dive deeply into a very particular and important skill to learn for an improved quality of living. But whether 2016 was a year for the record books for the goodness it brought or the frustration, why not reflect upon it as a map guiding you to where you can go successfully so long as you choose the improvements that need a bit of tuning up?
The goodness that you seek begins by tending to yourself. As I shared on Afternoon Live this past Friday (view the video here), what is it that you most want, but that because of a fear standing in the way, you haven't taken that leap yet? Why not take the leap? Why not take that important risk? This is your life. This is your one and only life, and it is finite. While simply putting out into the universe what you desire will not guarantee it will materialize, it is far more likely to eventually become a reality at some point once you do.
A concept was recently introduced to me via a book I was given by my father called the Adjacent Possible. In other words "Each new combination opens up the possibility of other new combinations". And to reframe for what we're talking about today, each time you open new possibilities in your life, sharing with the world your truth, you open yourself up to new possibilities that were originally closed to you. In other words you are enabling what you seek to become more possible each time you take a step toward it.
Take a look at either image above. Both reveal clouds and glimmers of blue sky. Focus on the beautiful aesthetic that is cultivated as both are present. Unexpectedly there is a revelation, an awareness made known, that we must experience both struggle and celebration in order to move forward successfully. While we will want to focus on the items to celebrate (in this case the sun which I was moved to dance giddily about on the coast as it had unexpectedly shown itself yesterday morning during our walk), we do not want to forget to apply the lessons the clouds provide enabling us to move forward and become more skilled living our lives well.
So let's make 2017 a year where we make the life we desire more capable of unfolding. Let's begin to make the small changes, one at a time. Let's change our minds to work for us, rather than against us. Let's adopt behaviors that enrich us rather than break us down. Let's be hopeful and take action, rather than worrisome and passive.
We cannot be guaranteed anything, but we can put the odds in our favor.
~Why Not . . . Prep for a Wonderful 2013?
Loved this Shannon. All the best in 2017!
Thank you Colleen! 🙂 Thank you for stopping by and may 2017 be a most amazing year.
Happy New Year, Shannon! Watched your "Afternoon Live" appearance and appreciated the idea of taking on fewer, more specific goals. Years aren't meant to be compared, one to the other, because we'll never have "the best" year at that rate! They're meant to be lived, learned from, and enjoyed as much as possible.
Your advice is so practical – do things that enrich us. Indeed a good start to 2017. All the best!
Deanne, All the best to you as well!
Happy New Year Shannon! I so appreciate all that you do!
The Simply Luxurious Life was one of my favorite discoveries of 2016. I look forward to all you have to share in the coming year. Wishing you a simply chic 2017!
Watched Afternoon Live – Thank you for sharing yourself with us. Appreciated very much the practical thoughts of not overloading oneself with too many goals, and taking one big risk. Also read your blog and was very encouraged by your quotes and am going into this new year with a much more positive outlook. Thank you .
I love the concept of Adjacent Possible. Looking back, I can see several small steps I took, which, together, led in very unexpected directions.


The best thing to do is to not rush to any decisions, even though your emotions may tell you to run away as fast as you can. With the help of a good Utah marriage and relationship counselor, you can deal with the fear and anxiety caused by a cheating spouse and be proactive about where your relationship should go next.
It's normal for both partners in a marriage or long-term relationship to suffer from things like grief, guilt, panic, and depression when an affair takes place. Without professional guidance, these symptoms can spiral into larger mental health issues that impact you both emotionally and physically. They can obviously also impact other family members like children, in-laws, and mutual friends.
What Should You do If You Catch Your Significant Other Cheating?
If you know that your spouse has cheated, or you suspect an affair has taken place, you may not know where to turn for help. A professional marriage therapist near Salt Lake City can guide you through the conversation with the added support of an unbiased third party. We know that this is a very sensitive and upsetting event, and our extensive experience can help create a dialogue to work through the feelings and needs of each party in the relationship.
Whether it was you or your spouse who cheated, an adulterous relationship (or history of several) can push your marriage's foundation to its limits. Some couples decide to split and go separate ways, calling it quits for good. Others care for each other too much to give up on what they have worked so hard to have, and know that it's not worth giving up just yet. But without professional guidance, it may be difficult to know where to draw the line or how to rebuild trust that has been lost.
Any trouble during a marriage — especially adultery or an affair — can be hard to work through if you're not sure where to turn for help. A good marriage counselor or family therapist can show you ways to look at the situation and come to reconciliation, so that the marriage can recover and you can learn to trust one another again.
The Dell Center for Therapy has helped numerous couples in the Park City, Salt Lake and the surrounding Utah City areas deal with infidelity and affairs in a private, respectable manner. Our Utah marriage counselor works with couples to emotionally sort through their feelings and look at underlying issues that may not have yet been addressed. Infidelity counseling can help.
A marriage counselor can help you or your partner work through the effects of what an affair can do to your relationship. Whether you decide to reconcile, separate, or just put things on hold for a while, it can be extremely difficult to know how you're supposed to be feeling. Processing your emotions and concerns can help you to work through infidelity or cheating in a mindful way, so that you don't make hasty decisions that you wind up regretting.
Our Utah based counselors can meet you in our Park City practice, at a convenient location in Salt Lake City, or even over the internet. When it comes to real life struggles like an affair or infidelity, we understand what a sensitive subject it can be to discuss. Through guided conversations and mindful techniques, we can show couples how to take a step back and process everything that has gone on before, during, and after an affair. When you want to save your relationship or before you decide to end your marriage for good, the best thing that you and your spouse or partner can do is to seek out the help of a good relationship counselor.


Growing up I didn't know how to swim and never even bothered learning until 2 years ago. The fact is I was afraid. After almost drowning in a river as a kid when I was 6 I was scarred.
Fast forward 18 years later and at 24 I still wasn't comfortable in the water. Things were getting serious because I was slightly overweight. I had tried running but HATED it, and my feet and knees would hurt afterwards.
So I decided to try swimming.
After all, it is easy on the bones and joints and you don't get hurt swimming.
Although I lived in an apartment that had a pool I almost never went because I was embarrassed I couldn't swim. My boyfriend offered to teach me but I didn't want to learn how to swim in front of other college students.
He mentioned taking swimming lessons but I thought that would be almost as embarrassing. What kind of adult takes swimming lessons? They are meant for little kids!
After a couple of months of slowly gaining weight I decided I needed to do something about it and saw that a near by city (Sierra Madre, California -US) offered some group swimming lesson for all ages and so I decided to take the plunge and enroll.
On my first day of the group lessons I was still very nervous. I didn't feel quite like myself because I also bought a onesy and didn't want to wear a bikini in front of potentially tons of kids and adults!
I arrived a little early and my stomach shrank as I saw the other people in the class arrive – they were all little kids with not one being older than 10. Needless to say I was ashamed.
It was hard for me to focus because I was so nervous and thinking about how I was a grown adult learning how to swim in a group full of kids. The instructor, Damien, however was really nice and encouraging to me. I think he could tell I felt.
However, towards the end of my class another person comes in, apologizing she was late, and guess what! She was actually just 2 years younger. Her name was Susan and we quickly became fast friends over the next 8 weeks and learned how to swim together.
As I learned how to swim through class I quickly began to really enjoy swimming. What used to be a childhood fear quickly became a wonderful form of exercise and passion.
Doctors told me my bones and joints were looking healthy, and my shin splints went away, but I never needed to go back! I was swimming laps 3-4 times a week – often with Susan because we lived so close together.
I quickly lost some weight and slimmed down from the constant exercise and I noticed a big improvement not only in my physical health, but also was a LOT happier. This was the first time I had consistently been physically active and now I understand the benefits of it.
And guess what. I haven't stopped.
Now, I continue to swim about 2 times a week as my primary form of exercise, and also enjoy playing in the pool with my kids. Fortunately, I live in California so the pool never gets too cold to swim and it's a great way to cool off in the hot summer.
Honestly, I can't imagine my life without swimming. I know there are a ton of other adults out there who can't swim – whether you are older or younger. It's hard to take the plunge (literally) and learn how to swim, but honestly it's so worth it.
Thanks Laurie! Laurie is a proud mother of 2 and home owner with a pool. Her two favorite hobbies include hiking and swimming. She created a blog to help others learn about pool care and maintenance. You can find it here.


While the deal on the home has been closed on, and is officially sold, you still have a few more things to do. Here are some things you can do to save money post-sale. Keep copies of all paperwork that was accumulated throughout the sale. You'll want these papers for taxes in April. This is because to file them properly, you'll need documentation for the expenses and proceeds of the sale. And after you file your return, you'll want to keep the paperwork in case you're audited. See: 9 Tax-Related Tips About Selling Your Home.
Be sure to change your mail! We took a while to change ours, and even after we changed it, it still took a while before everything came to our house. At the very least, contact the new owner and let them know that they may still get some of your mail, and set a date and time each week to come pick it up. This is important, because you'll miss out on a lot of bills and miss payments. I missed three speeding tickets and had to pay double for each of them! It is not the new owners' responsibility to get your mail to you.


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Eve Net Worth, Early Life, Music Career, Acting Career, Personal Life And More
Eve is a rapper, songwriter, and actress. She became a household name after releasing her first debut album in 1999. Her album was a massive success, and she became the third female hip-hop artist to reach the #1spot on the album charts of the "Billboard" 200. She has received many awards like the Grammy Award for Best Rap/Sung Collaboration in 2002 for her song, "Let Me Blow Ya Mind," that she collaborated with Gwen Stefani.
Eve has an estimated net worth of $10 million dollars. She is a popular actress, singer, and songwriter and her net worth come from her career in the entertainment industry. Eve has appeared in many popular films such as "XXX" (2002) and "Barbershop" (2002), and also was a part of the UPN sitcom "Eve". She also has a successful fashion line, Fetish, and has acquired her net worth through her business ventures as well.
Eve was born Eve Jihan Jeffers on November 10, 1978, in Philadelphia, Pennsylvania. Her mother was a supervisor and worked at a publishing company. Her father is a chemical plant supervisor. Her mother and father Jerry split up when Eve was just 12. Her mother got married to Ron Wilch and Eve has a half-brother named Farrow. After she graduated she moved to New York and worked as a stripper.
Read more: Erica Hill Net Worth, Bio, Age, Husband, Kids, Career, Salary & More
Music Career
When Eve was 18, she auditioned for Dr. Dre and signed with Aftermath Entertainment. She signed with Interscope's Ruff Ryders label and released her first single, "What You'll Want. The song reached #1 on the "Billboard" 200 and Hot Rap Songs charts. The album certified Double Platinum and sold 2 million copies. She released other successful albums that include:
"Scorpion" (2001)
"Eve-Olution" (2002)
"Lip Lock" (2013)
"Let Me Blow Ya Mind"
"Gangsta Lovin'."
Eve collaborated with many artists and her two major collaborations include Gwen Stefani, "Let Me Blow Ya Mind" and "Rich Girl". Her song "Gangsta Lovin'," featured Alicia Keys, and the song reached #2 on the "Billboard" Hot 100 chart. She performed on many tracks that were sung by popular artists like:
The Roots' "You Got Me
Missy Elliott's "Hot Boyz"
"4 My People
Mary J. Blige's "Not Today
Kelly Rowland's "Like This."
Read more: Ted Cruz Net Worth, Early Life, Legal Career, Political Career, Relationships And More
Film and Television Career
Eve released her film debut in 2002's "XXX. The movie grossed over $277.4 million at the box office. She continued to do many other popular films that include:
"Barbershop" (2002)
"The Woodsman" (2004)
"Barbershop 2: Back in Business" (2004)
"The Cookout" (2004)
Whip It" (2009)
"Bounty Killer" (2013)
"Barbershop: The Next Cut" (2016)
Glee" (2009)
Eve was in a relationship with British entrepreneur Maximillion Cooper in 2010. She got married to him on June 14, 2014. The businessman has four children from his previous marriage. Eve is a stepmother to four of his children Lotus, Jagger, Mini, and Cash. Eve was accused of DUI after she crashed her car into a median in Hollywood.
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Year 3 visited Nell Bank to experience what life was like in the Stone Age.
This week we have been learning all about Chinese New Year! This year is the year of the pig. We talked about where China is and why people celebrate Chinese New Year. The children have really enjoyed tasting noodles, dressing up in traditional Chinese clothes, doing a lion dance and our Chinese restaurant role play. What a busy week!
Year 3 enjoying a ribbon dancing workshop for Chinese New Year.
We have been learning about people who help us and we have been visited by a firefighter and police officers. We have been talking about keeping ourselves safe, always doing the right thing and listening to adults.


text:
April 13 2018, 12:01am, The Times
Times Newspapers Ltd
The Queen has made the following appointments on the advice of the Rt Hon David Gauke MP, the lord chancellor, and the Rt Hon the Lord Burnett of Maldon, the lord chief justice of England and Wales:
● Shefali Talukdar to be a district judge. The lord chief justice has deployed her to the Northern Circuit, based at Manchester County and Family Court with effect from April 30, 2018.
● James Nicholas Glassbrook to be a district judge. The lord chief justice has deployed him to the Midland Circuit, based at Northampton Combined Court with effect from May 8, 2018.
● Louise McCabe to be a district judge. The lord chief justice has deployed her to the Midland Circuit, based at Coventry Combined Court with effect…


text:
#region License
// CommandLineOptionFactoryTests.cs
// Copyright (c) 2013, Simon Williams
// All rights reserved.
//
// Redistribution and use in source and binary forms, with or without modification, are permitted provide
// d that the following conditions are met:
//
// Redistributions of source code must retain the above copyright notice, this list of conditions and the
// following disclaimer.
//
// Redistributions in binary form must reproduce the above copyright notice, this list of conditions and
// the following disclaimer in the documentation and/or other materials provided with the distribution.
//
// THIS SOFTWARE IS PROVIDED BY THE COPYRIGHT HOLDERS AND CONTRIBUTORS "AS IS" AND ANY EXPRESS OR IMPLIED
// WARRANTIES, INCLUDING, BUT NOT LIMITED TO, THE IMPLIED WARRANTIES OF MERCHANTABILITY AND FITNESS FOR A
// PARTICULAR PURPOSE ARE DISCLAIMED. IN NO EVENT SHALL THE COPYRIGHT HOLDER OR CONTRIBUTORS BE LIABLE FOR
// ANY DIRECT, INDIRECT, INCIDENTAL, SPECIAL, EXEMPLARY, OR CONSEQUENTIAL DAMAGES (INCLUDING, BUT NOT LIMITED
// TO, PROCUREMENT OF SUBSTITUTE GOODS OR SERVICES; LOSS OF USE, DATA, OR PROFITS; OR BUSINESS INTERRUPTION)
// HOWEVER CAUSED AND ON ANY THEORY OF LIABILITY, WHETHER IN CONTRACT, STRICT LIABILITY, OR TORT (INCLUDING
// NEGLIGENCE OR OTHERWISE) ARISING IN ANY WAY OUT OF THE USE OF THIS SOFTWARE, EVEN IF ADVISED OF THE
// POSSIBILITY OF SUCH DAMAGE.
#endregion

using Fclp.Internals;
using Fclp.Internals.Parsing;
using Fclp.Internals.Parsing.OptionParsers;
using Moq;
using NUnit.Framework;

namespace FluentCommandLineParser.Tests.Internals
{
	/// <summary>
	/// Contains unit tests for the <see cref="CommandLineOptionFactory"/> class.
	/// </summary>
	[TestFixture]
	public class CommandLineOptionFactoryTests
	{
		[Test]
		public void Ensure_Can_Be_Constructed()
		{
			new CommandLineOptionFactory();
		}

		[Test]
		public void Ensure_CreateCommandLineOption_Returns_Expected_Object()
		{
			var factory = new CommandLineOptionFactory();

			const string expectedShortName = "my short name";
			const string expectedLongName = "my long name";

			var mockParserFactory = new Mock<ICommandLineOptionParserFactory>();
			mockParserFactory.Setup(x => x.CreateParser<string>()).Returns(Mock.Of<ICommandLineOptionParser<string>>);
			factory.ParserFactory = mockParserFactory.Object;

			var actual = factory.CreateOption<string>(expectedShortName, expectedLongName);

			Assert.IsInstanceOf<CommandLineOption<string>>(actual, "Factory returned unexpected object");
			Assert.AreEqual(expectedShortName, actual.ShortName, "Factory returned Option with unexpected ShortName");
			Assert.AreEqual(expectedShortName, actual.ShortName, "Factory returned Option with unexpected LongName");
		}
	}
}

redpajama_set_name: RedPajamaGithub


Thousands of Palestinians on Thursday marked the 61st anniversary of the Naqba, the "catastrophe" that sparked an exodus of hundreds of thousands of refugees after Israel was created in 1948.
Holding Palestinian flags and photos of Arab villages razed by Israeli forces six decades ago, demonstrators marched in the centre of Ramallah in the Israeli-occupied West Bank.
"The right of return is sacred", "No peace without the right of return", proclaimed banners held by the marchers.
The ceremonies took place a day early, because this year the May 15 anniversary of the Naqba falls on a Friday, a day off in the mostly Muslim Palestinian territories.
The demonstration was headed by political figures and religious leaders and began at the tomb of legendary Palestinian leader Yasser Arafat at the headquarters of the Palestinian Authority, today run by his successor, President Mahmoud Abbas.
In the northern West Bank town of Nablus, about 2 000 people participated in a march, holding Palestinian flags tied with black ribbons as a sign of mourning.
In Aqabet Jaber refugee camp, in the oasis town of Jericho, participants unveiled a statue featuring a six-metre metallic key, symbolising the refugees' attachment to the houses from which they fled or were forced out in 1948.
About 700 000 people were exiled in this way in 1948, with the United Nations estimating that today they and their decendants number 4,6-million.
In the Gaza Strip, its Hamas rulers prevented the Palestine Liberation Organisation (PLO) from holding a ceremony to mark Naqba in the tiny territory that today is home to one million refugees.
Witnesses said Hamas police were deployed in force in the centre of Gaza City, preventing any public gathering. No comment was immediately available from the Islamists.
The commemoration committee is part of the PLO which is headed by Palestinian president Abbas.
Hamas is not a member of the PLO, which the international community considers the sole legitimate representative of the Palestinian people.
The Islamists and rival secular Fatah have been at loggerheads ever since June 2007, when Hamas forced pro-Abbas forces out of Gaza, splitting the Palestinian territories into two entities.
Since then, Abbas's writ has been reduced to the occupied West Bank, while Hamas has ruled the Gaza Strip.
"In these days ... [the longing for peace] takes on a particular poignancy as you recall the events of May 1948 and the years of conflict, as yet unresolved, that followed from those events," he said at Aida refugee camp outside Bethlehem.


text:
SepOct, 1900Nov
October 5th, 1900 Chinese Zodiac, Moon Sign and Birth Chart
An observer located in New York City on Friday October 5, 1900, would see:
The moon, being 92% full, rising at 03:38 pm and setting at 03:35 am. The previous full moon was on Sep 09, 1900 while the next full moon would come on Oct 08, 1900.
Your place in the Universe on October 05, 1900
Zodiac sign: Rat
You may not believe in horoscopes but you may like this free video based on October 05, 1900
Mercury rising at 07:24 am and setting at 06:08 pm with a 89% of surface illuminated. Mercury would be orbiting the Sun at a distance of 0.47 astronomical units (AU) and would be found at a distance of 1.33 astronomical units (AU) from Earth. Given the planet elongation, the observer would see Mercury at an angle of 16° 12' 42.6" with the Sun. The brightness would be -0.27 this day, as measured by the planet magnitude.
Mars would look like 90% full, orbiting the Sun at a distance of 1.57 AU and be at 1.66 AU from Earth. The planet would be seen rising at 12:18 am and setting at 02:49 pm. The angular separation of the Sun and the planet, with Earth as the reference point, would be -67° 14' 24.5". The brightness of Mars, that is its magnitude, would be 1.14.
Jupiter's distance from the Sun would be 5.30 AU and 5.82 AU from Planet Earth. Jupiter rising and setting times would be 10:38 am and 08:08 pm respectively. Jupiter would appear with a 99% illuminated fraction of its surface and a magnitude (brightness of the star) of -1.76. Its angular separation between the Sun would be 54° 21' 49.0".
Saturn would rise at 12:18 pm and set at 09:34 pm, appearing 99% full. The angular separation of Saturn from the Sun, as seen by the observer, would be 76° 00' 48.0", its magnitude 0.52. Saturn would orbit the Sun at a distance of 10.07 astronomical units (AU) and would be located at a distance of 10.26 astronomical units (AU) from Earth.
Uranus would appear 99 full, its brightness being 5.68. It would be seen rising at 10:49 am and setting at 08:12 pm. Uranus would be 19.04 AU far from the Sun and 19.58 AU far from Planet Earth (average distance). The observer, looking up into the sky, would see Uranus with a 56° 11' 37.3" angle of separation from the Sun.
Neptune rising at 09:29 pm, and setting at 12:22 pm, its magnitude (the degree of brightness of a star) being 7.86. The difference between the celestial longitude of the Sun and that of Neptune would be -103° 44' 05.0". At 29.88 AU distance from the Sun and at 29.62 AU from Earth, 99 % of Neptune would be illuminated by the Sun.
Pluto would be seen as 99% full and would have an elongation of -114° 56' 06.6". It would orbit the Sun at an average distance of 46.86 astronomical units (AU) and be located at an average distance of 46.43 astronomical units (AU) from Earth. The observer would see Pluto rising at 09:17 pm and setting at 11:00 am, its magnitude (brightness of the star) being 15.72.
Virgo 13:48:14.50 -12:01:31.1
Leo 10:00:48.59 11:50:09.1
Cancer 8:34:07.97 19:56:04.9
See what else happened on October 5th, 1900


text:
Best Cruise Tips
How to Prevent Motion Sickness
Tips to Save Money on a Cruise
What to Bring on a Cruise
Best Things to do & Visit in Miami
Allcruisehotels > Blogs > Ports of Call > Best Things to do near Cruise Port of Miami
Best Things to do near Cruise Port of Miami
Miami is one of the most visited places in the United States and the world.
From its inviting climate to the beautiful sights, port, and packed streets, there isn't a dull moment in Miami.
It is the perfect place for a cruise, especially since there isn't a time of the year when you cannot take a cruise from Miami to the Bahamas or Caribbean.
Be sure to arrive a couple days early and stay a few nights in one of Miami's best hotels near the port, some offer a free shuttle to the cruise terminal.
In addition to the cruise, there is a myriad of adventurous experiences that you can enjoy before and after your voyage.
Below are some of the top places to visit and things to do in Miami.
Miami Cruise Port Hotels
Best Places to Stay in Miami
Fun Things to do in Miami
What are the Best Places to Visit in Miami ?
Miami is the premier tourist destination in Southern Florida. Home to the world's largest cruise port it attracts millions of people, many are looking for some exciting things to see and do while spending a few days in the city before or after a cruise vacation.
We have listed the best places to visit and some top activities in Miami Florida. So, if you're planning your next trip, these are some attractions not to be missed.
1. Enjoy Prime Entertainment at the Jungle Island
Jungle Island
Jungle Island is one of the prime entertainment and tourist destinations in the city of Miami. The place was formerly known as the Parrot Jungle. This contemporary theme park has been in existence for more than eight decades and comprises of more than 300 vibrant birds, rare twin orangutans and the only trained Cassowary in the world.
The Island is also known for its rick tropical landscape. At the Jungle Island, visitors get to enjoy viewing the animals, playing paintball, airsoft, and nerf games. See tickets.
2. Bond with Nature at the Miami Zoo
Miami Zoo
Miami Zoo is the oldest and the largest zoological garden in Florida. It is also the only sub-tropical zoo in the continental United States. Miami Zoo is home to a wide range of animals from different parts of the world, including Asia, Australia, and Africa.
The animals feature a mix of species, which is rare for zoos in the United States. The lush and tropical open-air landscape makes it suitable for the different species of animals. It also makes it a safe place for endangered wildlife.
Book your general admission ticket to Zoo Miami in advance and don't wait in line.
3. Enjoy the Fun and Serenity at Miami Beach
Miami Beach is a coastal resort that is located in Miami-Dane County, Florida. It is located on barrier islands between Natural and Manmade Island, a place which is made up of a wide range of sunbaked beaches.
The beaches are located in an environment that is packed with beautiful hotels with the best scenery. Nightlife at the beach is also quite active, primarily because the climate is suitable for outdoor activities. The beaches to the south are more active while the north beaches are quieter and calmer.
4. It is Never a Dull Moment at South Beach & Ocean Drive
Ocean Drive South Beach
Ocean Drive is one of the major thoroughfares in South Beach Miami. It is closely located near Miami Beach on the Atlantic coast of Florida and is known for its Art Deco-style hotels, restaurants, and bars. Tourists are attracted to these sights because they are commonly featured in movies and the media. The most famous building in the area is the Colony Hotel, which was built in 1939. The hotel holds the record of the most decorated art deco place in the United States.
A popular thing to do is taking a food‐filled walking tour of South Beach and taste cuisines of different Latin American countries.
5. Experience Architectural Genius in Art Deco District
The Art Deco District is also known as the Miami Beach Architectural District. The place is a historic district in the US, well known as the home district of Gianni Versace, an internationally-recognized Italian designer. The district is made up of about 960 historic buildings. All the buildings feature the Art Deco design, and they are all within a mile.
Some of the buildings host the best restaurants and hotels to visit. Tourists enjoy walking through the place and taking photos, as well as making visits to the Deco Museum in the district. To learn more you can take a 2 hour guided Art Deco Walking Tour.
6. Enjoy an Exceptional Shopping Experience at Bayside Marketplace
The Bayside Marketplace is a two-story open-air shopping center that is located in downtown Miami, Florida. The Greater Miami Convention & Visitor's Bureau recognizes the marketplace as the most visited attraction in Miami.
The marketplace differs significantly from regular shopping malls, especially because it offers an entertainment experience with live music every day. It also hosts the best restaurants, bars, family activities, and open-container places. Bayside marketplace consists of 140 inline spaces and more than 50 carts and kiosks scattered in different places in and around the center.
From Bayside Marketplace you can also take a city sightseeing cruise through Biscayne Bay to see the Port of Miami and Millionaire's Row.
7. Explore Cuban Culture at Little Havana
Little Havana is home to Cuban exiles and immigrants from central and south America. This is the reason why it was named after the capital city in Cuba. It is recognized as the center of social, cultural, and political activity in Miami and is also known for festivals like the Three Kings Parade and the Calle Ocho Festival.
The home for Cuban exiles also features some amazing landmarks like the Latin Walk of fame and the SW 8th Street. Street life, restaurants, and music characterize Little Havana.
When looking for a tour, the most popular one is a guided walking tour in Little Havana which includes samples of the local cuisine.
8. Experience Extraordinary Views at Miami Seaquarium
Miami Seaquarium
This is a 38-acre tropical paradise characterized by its spectacular view of the skyline. The Miami Seaquarium is also known as the place where dolphins walk on water, and extraordinary whales fly through the air. It is home to some of the most amazing sea lions that both parents and kids of all ages enjoy seeing.
The marine-life entertainment park features eight different species of marine animal shows hosted at different times of the day. At the Miami Seaquarium, there is a Dolphin Habor, where visitors can enjoy hands-on experience with the mammals.
9. Brickell City Centre & The Shops at Mary Brickell Village
This is a shopping and multiuse project in Miami, Florida that costs more than a billion dollars to construct. The Brickell City Centre & The Shops at Mary Brickell Village is set to span up to five blocks, and it will be anchored by a 107, 000 square-foot fifth avenue in Miami.
The village and city center spans a bit over 9 acres with amenities like a department store, restaurants, shops of all kinds, hotels, office towers and condominiums.
10. Relax and Learn at the Vizcaya Museum and Gardens
Vizcaya Museum and Gardens
The Vizcaya Museum and Gardens was formerly known as the Villa Vizcaya. James Deering, a famous businessman formerly owned the property. It is currently owned by the Miami Wade Country and is open to the public. The museum and gardens consists of 50 acres where the villa and gardens, as well as the remaining of the native forest, lies.
The garden section is made up of Italian Renaissance gardens with a native woodland landscape and a historic village outbuilding compound. The landmark is constructed in an open-air courtyard and has undergone a series of reconstructions.
11. Airboat Ride in Everglades National Park
This is an American National Park that hosts twenty percent of the original Everglades in Florida. It is the largest tropical wilderness in the United States and of any kind in the East of the Mississippi River.
After Death Valley and Yellowstone, it is the third-largest national park in the contiguous US. The national treasure is home to some incredible geographic features, a network of wetlands and forests. The national park covers slightly more than 1.5 acres throughout Dade, Monroe, and Collier counties in Florida.
You can easily take a guided tour from Miami to Everglades National Park, which includes an airboat ride and often a nature walk.
12. Explore Bayfront Park
Bayfront Park is a 32-acre public, urban park in Downtown Miami, Florida, on Biscayne Port. Inside the park is a bronze statue of Christopher Columbus that was sculpted by Count Vittorio, one of the handpicked guards of Mussolini.
The national attraction is also the assassination site of Aton Cermak, who was the Mayor of Chicago at the time. The incident occurred while the president was shaking hands with former President Franklin D. Roosevelt. The park was constructed in the mid-1920s and went through reconstruction in 1980.
13. Get Educated at the Miami Children's Museum
The Miami Children's Museum was founded in 1983 and was initially known as the Miami Youth Museum. However, in 2003, the place was transformed to the Miami Children's Museum. The museum is located on Watson Island and consists of 14 permanent galleries, pre-school classrooms, and a parents and teachers resource center.
The Children's Museum also hosts a 200-seat auditorium, as well as a subway restaurant. The exhibits, programs, and classes at the museum are offered in a wide range of languages. Materials in arts, culture, community, and communication are also available at the Miami Children's Museums.
14. Experience the Beauty of Wynwood Walls
Wynwood walls was established in 2009 by Tom Goldman, a legendary place maker and visionary. The landmark was established as an outdoor museum of International Street Art and is the best venue in the world for viewing a wide variety of works by top street artists. It features an open green space with murals.
The Wynwood Walls is currently a phenomenon that has spurred the creation of several murals in the Wynwood District. Adjacent to the Wynwood walls is the Wynwood doors, which have 176 feet of roll-up storefront gardens. Tour the street art in Miami's Wynwood neighborhood by golf cart, a pedal-powered vehicle or classic car.
15. The Fontainebleau Miami Beach hotel
The Fontainebleau Miami Beach hotel is also known as Fontainebleau hotel. The hotel is located at Collins Avenue and is owned by the Fontainebleau Resorts. The beach hotel was designed by Morris Lapidus and was officially opened in 1954.
Fontainebleau Miami was ranked by the American Institute of Architects in the top-ten list of America's Favorite Architecture. Parts of the pool are featured in films, television shows, and music videos. The hotel includes accommodation spaces, restaurants, and nightclubs. It was renovated for two years and re-opened in 2008.
What are the Best Things to do before or after a Cruise ?
Miami ranks at the top of the world's most visited destinations.
If you and your family are looking for the top things to do in Miami during your trip, check out our list of some of best activities you can take.
16. Take the Big Bus Miami Open Top Hop-On-Off Tour
By taking the bus tour, you can explore some of the most popular sites in Miami. The tour will take you through some of the top attractions in Wynwood, Coconut Grove, Little Havana, and South Beach.
It allows you to enjoy the flexibility of exploring the city at a pace that you can control. The big bus tour features live on-board commentary and also allows you to enjoy the unparalleled views from an open-top double-decker style bus.
You can also opt to take a double-decker bus night tour which takes you through South Beach and downtown Miami and see the city lit up at night.
17. Enjoy Miami Combo Tour; City Sightseeing, Biscayne Bay Cruise & Everglades Airboat Ride
Through the Miami Combo tour, you can enjoy an escape to the Florida Everglades by bus and boat. The combo tour is a guided, full-day city sightseeing adventure that features an exciting package, including a coach tour around Downtown Miami and its environs.
The tour also features a cruise on the Biscayne Port and its clear waters. During the combo tour, you also get to enjoy the Miami Skyline and the beach, the abundant wildlife in Florida, including alligators and turtles.
18. Take a Private Exclusive Classic Car Tour of Miami
This tour will have you explore the streets of Miami in a classic convertible car. It is a half-day tour with a private chauffeur who will pick you up and drop you off at select hotels in the Miami Beach area.
The tour covers the area around the Art Deco district of South Beach. You also get to cruise the port and explore the design district, Downtown Miami, Bayside, Coral Gables, and Wynwood. Onboard, you get bottled water, a live documentary, and photo stops.
19. Learn the History of Miami with the Duck Tours in South Beach
The Miami Duck tour is hosted both on a boat and a car and is a unique land and sea cruiser. The 90-minute tour will take you through famous attractions in Miami. For example, you can take a splashdown into the Biscayne Bay and Port, as you learn about the history of Miami Beach.
The guides for this tour have a background in acting and comedy. Therefore, you can expect an entertaining experience. The departure point and return point of the tour are at James Avenue 1661.
20. Explore Miami Landmarks with the Miami City Tour Shopping and Bay Cruise
This tour includes a round trip from Miami Beach or Downtown, and it features narration by a professional guide with knowledge of the history of the area. The guides are also very entertaining. The trip involves a 90-minute cruise at the Biscayne Bay and a free lunch.
During the tour, you get to travel on a comfortable coach and go through some landmarks like The Magic City. You also get to explore the beauty of beachside neighborhoods such as Coconut Grove and Coral Gables. Read more.
21. Get a Taste of South Beach Food Tour
On this small-group tour, you get to experience the diverse and unique culture of Miami through its cuisine. The food tour is led by enthusiastic and entertaining local foodie guides with a vast knowledge of the diverse cuisines. On tour, you get to sample American, Cuban, French, Mediterranean, and Peruvian dishes, among others.
The foods are made by some of the most popular restaurants in the South Beach area. You also get to learn about the history, architecture, and culture of the city while enjoying the food.
22. Try the Seaplane Tour of Miami
On seaplane tours, you get to enjoy the beauty of Miami through aerial views. The tour glides over the best coastal hotspots like Key Biscayne, Coconut Grove, Star Island, and South Beach. Your guide here will be the pilot, who is equipped with incredible know-how of the history and details of the sites.
You also get to experience breathtaking views of the mansions and the signature Art Deco style of the city from the sky. The takeoff and landing area is on the waters of Key Biscayne.
(Latest update June 30th 2020)
Please contact us if any information is incorrect or not up-to-date.
Disclosure: This page contains affiliate links, and at no additional cost to you, we earn a small commission if you click through and make a reservation.
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027: KYLE THIERMANN - Pro Surfer, Podcaster, Filmmaker.
Kyle Thiermann is a professional surfer, podcaster, and filmmaker from California. He creates gonzo-style mini-documentaries about current issues happening all over the world. Tune in to his podcast for conversations with fascinating people he meets along the way.
Kyle rips small waves and charges big waves, and he wants to keep getting better. He shares some insights into how he got so good and how he plans to improve.
026: NAM BALDWIN - Flow, Flow State, "the Zone"
We discuss what Flow is, why some surfers get into 'the zone' more often and more easily than others. How do we train, warm-up and think in a way that elicits more flow. How to turn a bad surf into a great surf.
025: CLAYTON NIENABER - Surf Coach, Shaper, shredder.
Clayton shares some of his back-stories into how he became a world-class surfer, surf coach, and surfboard shaper. Clayton has a unique take on advanced surfing, he breaks it down very clearly, simplifying what to most surfers seems magical. We clarify the proper surf stance - squat or lunge? Or Squnge? We talk in depth about Kelly Slater, and even break down one of his waves on a very detailed level. This podcast will give you an in-depth look at the worlds best surfers Kelly Slater - his approach, his technique and some never heard before quotes. 35 mins into the interview we break down a vid of Kelly surfing, so make sure you watch the vid posted below.
The link between health and performance is undeniable, so it makes perfect sense to optimise health in order to optimise surfing performance and enjoyment. Health begins in the gut, and in this episode, we discuss gut health and some simple strategies to optimise yours. For more info check out Kale via the links below.
Kale Brock is an Award-nominated writer, producer and speaker. With a background in TV journalism, Kale has a passion for creative storytelling with a special interest in health & wellbeing. His long-awaited documentary, The Gut Movie, investigates the human microbiome in a scientific, quirky & fun journey in which he travels to Namibia to live with The San tribe. Kale's books, The Gut Healing Protocol and The Art Of Probiotic Nutrition, have generated international acclaim.
023: BUD FREITAS - Surf Coach & Shredder.
Gee Cormack is the founder and head surf coach at Chix Surf School in Sydney Australia. Gee coaches and speaks about surfing on a much deeper level than just technique and wave selection. She helps her clients discover why they surf, and what they want to achieve with their surfing. Helping surfers to find their own rhythm by developing and combining self-awareness with ocean-awareness.
Ben has been the Head forecaster at Coastalwatch for ten years. In this episode, he explains how waves are made, what he looks for when making surf predictions, dispels some common misbeliefs about reading synoptic charts, describes some of the nuances of swells and most importantly educates us on how to find the best waves. We also talk about how secondary and tertiary swells affect the primary swell and your local break. If you have never looked at a synoptic chart, isobar map, satellite image etc, then this episode may be a little confusing (unless you are in front of google & can look up the referenced images). Below are some links to some introductory tutorials that will get you up to speed pretty quickly. Most of the references are based on Australian, and Indonesian surf.
Michael talks about how your mind affects your surfing, as well as surfing's effect on our minds.
Mindfulness, flow state, being present, living in the now, awareness, in the zone, in the pocket, focus on 'now', meditation, mind-set, surfing philosophy. It's all in here, and it's all relative to surfing.