text:
\section{Introduction}
No experiment to date disagrees with quantum theory. However, it is often not appreciated that the theory has not been tested in all parts of the parameter space (as defined by the number of degrees of freedom in the system being tested).  The largest objects for which the theory has been tested have a mass of about $10^{5}$ amu, and the smallest objects for which classical mechanics is known to hold have a mass of about $10^{-6}$ grams [about $10^{18}$ amu]. This leaves a mesoscopic desert of some thirteen orders of magnitude over which we do not know whether the centre of mass motion of an object obeys quantum mechanics, or classical mechanics, or some new mechanics, to which the classical and quantum are approximations. Nor do we know for sure as to exactly where in this untested parameter space the quantum-classical transition takes place, and what the mechanism for this transition is \cite{Adler:09,Bassi:03,RMP:2012}.

[This is perhaps a suitable place to remark that while macroscopic quantum behaviour is indeed observed in superconductors, superfluids, and Bose-Einstein condensates, this by itself does not preclude the need to test quantum theory in the desert. The macroscopic quantum states in these systems are collective internal states akin to one-particle states, and what we are referring to above is the centre of mass motion of the object as a whole. One should also note that such macroscopic states put very weak bounds on collapse models such as Continuous Spontaneous Localization (CSL) and do not rule out these models \cite{Adler3:07}].

We could ask if we have any reason to suspect that quantum theory might break down in the desert. The quantum measurement problem which has been with us for nearly a century now, does give rise to the belief in a possible breakdown. It might well be that the problem will eventually go away in a suitable re-interpretation of the theory (many-worlds, consistent histories, ...) or in a suitable reformulation (Bohmian mechanics, ...). On the other hand, there remains open the possibility that the theory has to be modified to solve the measurement problem. It is precisely in the untested mesoscopic desert where the modified theories make experimental predictions different from quantum theory, making it all the more relevant that this regime be experimentally tested. If no departures from the standard theory are found, we can be sure that the answer to the foundational problems of quantum theory will lie in a re-interpretation \cite{RMP:2012}.

Mention must also be made of the curious status of the Born probability rule, a rule which has to be invoked in order to explain the random probabilistic outcomes of measurements. The status is curious because even though the Schr\"{o}dinger equation is perfectly deterministic, and the initial conditions unambiguously specified by prescribing the initial wave-function, the interaction of the quantum system with a classical apparatus produces unpredictable outcomes. The only meaningful way to remedy this unphysical situation is to introduce randomness in the initial conditions (Bohmian mechanics) or in the dynamics (collapse models) or to reinterpret measurements in such a way that collapse is only apparent, but not for real. Apart from the need to understand the Born rule, another shortcoming of the standard (Copenhagen) explanation is the vaguely defined classical apparatus - quantum theory has to depend on its own limit for properly understanding outcomes of experiments. This indeed is not satisfactory \cite{Bell,LandauLifshitz}.

In our opinion, the most significant incompleteness in our present understanding of quantum theory is the problem of time, even though this problem gets little attention in the literature. The time which describes evolution in quantum theory is part of a classical space-time whose geometry is produced by classical bodies, which in turn are a limiting case of quantum theory. Once again, the theory has to depend on its own limit for its formulation, and there ought to exist a more complete equivalent formulation which does not refer to classical time. As we briefly note in the next section, maybe when we have such a reformulation we will also understand how to solve the measurement problem \cite{Singh:2012}.

In summary, we may list the four frontiers along which we need to do better with quantum theory: (i) experimental tests of the theory in the yet unexplored part of the parameter space (ii) obtaining a time-independent reformulation of the theory (iii) finding a universally acceptable  resolution of the measurement problem (iv) understanding the origin of the Born probability rule in a deterministic theory.

Models for quantum theory without classical time have not received much attention, and are briefly discussed in the next section. Models which seek to modify quantum theory so as to solve the measurement problem, while taking classical time as given,  are themselves severely constrained on theoretical and experimental grounds. The modified theory should be stochastic nonlinear, and must include anti-Hermitean modifications to the Hamiltonian \cite{Pearle:76,Gisin:81,Gisin:84,Gisin:89,Gisin:95,Weinberg:11}. The most successful and well-studied  such phenomenological model is Continuous Spontaneous Localization (CSL) \cite{Pearle:89, Ghirardi2:90}. CSL bridges the microscopic quantum theory and macroscopic classical mechanics, acting as an underlying generalisation to which the former two are approximations, and a generalisation which solves the measurement problem (collapse is dynamical) and explains the Born rule (strictly speaking, the theory is constructed in such a way that the Born rule follows, and a fundamental explanation of the Born rule still alludes us).

Since CSL is a phenomenological theory, eventually one would like to look for a deeper explanation for the CSL mechanism, if it proves to be correct. Possible underlying physics could be that the stochastic field which drives the CSL effect is cosmological in origin [maybe having something to do with the cosmic microwave background] or it is a relic thermodynamic effect, as in Adler's theory of Trace Dynamics \cite{Adler:04,Adler:94,Adler-Millard:1996}. Alternatively, the origin of the CSL effect could lie in the universal interaction of gravitation. There are intrinsic quantum fluctuations in the gravitational field, because the objects which produce it are not exactly classical but possess an intrinsic uncertainty, and these fluctuations might feed back to decohere the quantum wave function and possible induce collapse. Such an idea forms the basis for investigating the possible role of gravity in collapse of the wave function., and a possible connection with CSL. Alternatively, maybe it is not the quantum fluctuations of gravity, but some other feature of gravity, not yet appreciated, which might account for collapse.

There is unfortunately no concrete theory to this effect as yet, although there have been a series of investigations. In the subsequent sections of the present modest review, we briefly survey some of the gravity related ideas that have been proposed in the context of quantum collapse. These include: a possible connection between the problem of time and problem of quantum measurement, decoherence models based on space-time uncertainty, the Scr\"{o}dinger-Newton equation and stochastic gravity, attempts to introduce gravity into collapse models such as CSL, ideas based on the black hole - elementary particle complementarity, and the possible role of a complex space-time metric. Earlier reviews of gravity based models include \cite{Diosi:05,Gao,Diosi:2013}.

\section{The problem of time in quantum theory}
The time that is used to describe evolution in quantum theory is classical time. It is a part of classical space-time on which there overlies a space-time geometry which is determined by classical matter fields, in accordance with the laws of general relativity. The Einstein hole argument implies that in order to give operational meaning to points on the space-time manifold, one needs to assign a metric at each space-time point. It evidently follows that classical matter fields are essential for this operational definition, and since such fields are a limiting case of quantum fields, we are forced to conclude that in the definition of the time that quantum theory employs, the theory depends on its own limit (Fig. 1).
\begin{figure} [ht]

  \centerline{\includegraphics{flowdiag.pdf}}
\caption{The circularity of time in quantum theory. From \cite{Singh:2012}}
\end{figure}%

A more complete formulation would be one where such dependence could be avoided, and we call such a formulation `quantum theory without classical time' \cite{Singh:2006}.  For brevity, we venture to name this as pure quantum theory. It is hoped that once such a pure formulation has been developed, standard quantum theory, with its classical time, will emerge as an approximation to the more general formulation.

Elsewhere we have suggested that pure quantum theory should be formulated by starting from a noncommutative generalisation of special relativity described by the line-element \cite{Lochan-Singh:2011}
\begin{equation}
ds^2 = Tr d\hat{s}^2 \equiv Tr [d\hat{t}^2 - d\hat{x}^2 - d\hat{y}^2 - d\hat{z}^2]
\end{equation}
Space-time coordinates and the matter degrees of freedom that reside on them acquire the status of matrices (equivalently operators). The statistical equilibrium thermodynamics of this noncommutative theory, in parallel with Trace Dynamics, is the sought for pure quantum theory \cite{Lochan:2012}. In the transition from here to a classical world, the role of gravity in causing collapse of the wave-function  is implicated. This is expected to come about because CSL type Brownian fluctuations around equilibrium cause collapse of the wave function describing the quantum space-time in pure quantum theory, as well as of the wave function describing the matter degrees of freedom.

A detailed discussion of this ongoing program can be found in \cite{Singh:2012}, and an overview in the context of collapse theories is given in \cite{RMP:2012}.

\section{Spacetime uncertainty and decoherence}
In the absence of a concrete formulation for pure quantum theory, it is useful to build heuristic models by asking how quantum fluctuations in space-time geometry can affect the propagation of the wave-function obeying the Schr\"{o}dinger equation. In order to make progress, one is compelled to start from some sort of description of space-time uncertainty, model it by a classical stochastic potential, and ask how the Schr\"{o}dinger propagation is affected by such a stochastic potential. Decoherence can be expected because of the stochasticity, and it maybe attributed to gravity. One of the earliest such studies was by Karolyhazy, as early as 1966 \cite{Karolyhazi:66} and then followed by Karolyhazy and collaborators in several papers \cite{Karolyhazi:86, Karolyhazy:74, Karolyhazy:90, Karolyhazy:95, Karolyhazy:1982, Frenkel:77, Frenkel:90, Frenkel:95, Frenkel:2002, Frenkel:97}. It was first shown that because of the intrinsic quantum nature of objects which produce gravity, there is a minimal length uncertainty $\Delta s$ in a geodesic of length $\Delta s$, which is given by the following universal relation:
\begin{equation}
\Delta s^3 \sim l_p^2 s
\end{equation}
where $l_p$ is Planck length.
One may imagine that Minkowski space-time has a perturbing stochastic gravitational field $\gamma({\bf x}, t)$ whose two point correlation is such that it is consistent with the above universal uncertainty. For a matter distribution described by the mass density operator $f({\bf x}, t)$ one then writes the stochastic Schr\"{o}dinger equation:
\begin{equation}
i\hbar\frac{\partial\psi({\bf x}, t)}{\partial t} = \left( H + \int d^3 x' f({\bf x'}) \gamma({\bf x'}, t) \right) \psi({\bf x},t)
\end{equation}

The fluctuating gravity causes distant parts of the wave-function to decohere,  and by considering the evolution of a spherical object of mass $m$ and size $R$ one obtains the following criteria for deciding whether the object is microscopic (quantum dominates over gravity) or macroscopic (gravity dominates over quantum, and the object is classical), and expressions for the critical separation length $a_c$ beyond which decoherence occurs:
\begin{eqnarray}
a_c\gg R &\rightarrow& \frac{\hbar^2}{G} \gg m^3 R \qquad: micro-region,\\
\nonumber\\
a_c \approx R &\rightarrow& \frac{\hbar^2}{G} \approx m^3 R \qquad: transition-region,\\
\nonumber\\
a_c\ll R &\rightarrow& \frac{\hbar^2}{G} \ll m^3 R \qquad: macro-region.
\end{eqnarray}
There arise two limiting cases: one for $R \gg a_c$ and another for $R \ll a_c$. For a micro-object of linear size $R\ll a_c$, the expression for the coherence length  reduces to that for an elementary particle of mass $m$ and the coherence length $a_c$ over which decoherence effects become relevant is given by
\begin{equation}
a_c \approx \frac{\hbar^2}{G}\; \frac{1}{m^3}  = \left(\frac{L}{l_p}\right)^{2} L; \qquad L= \frac{\hbar}{mc}.
\label{micro}
\end{equation}
For $R \gg a_c$, the critical length can be expressed as,
\begin{equation}
a_c \approx \left(\frac{\hbar^2}{G}\right)^{1/3}\; \frac{R^{2/3}}{m} =
\left(\frac{R}{l_p}\right)^{2/3} L.
\label{macro}
\end{equation}

In a different treatment, Di\'osi \cite{Diosi:87, Diosi:07, Diosi:89, Diosi:87a} considered a somewhat different starting point for understanding the intrinsic space-time uncertainty, by asking how much the uncertainty in a measured Newtonian gravitational field would be, if the intrinsic quantum uncertainty of the measuring probe is taken into account. It is shown that if a gravitational field ${\bf g}$ is probed over a volume $V$ for a time interval $T$, then the uncertainty $\delta\tilde{\bf g}$ in the averaged field $\tilde{\bf g}$ is given by
\begin{equation}
(\delta\tilde{{\bf g}})^2 \geq G \hbar/VT\; .
\label{dbound}
\end{equation}
Once again, this is modelled by a classical stochastic perturbing gravitational potential $\phi$ whose two-point correlation is consistent with the above uncertainty bound, and the impact of such a potential on the stochastic Schr\"{o}dinger equation is given by
\begin{equation}
i\hbar\dot{\psi}(t) = \left( H + \int \phi({\bf r}, t) f({\bf r}) d^3r \right) \psi(t)
\end{equation}

The conditions for decoherence and the micro-macro divide are the same as in the Karolyhazy model; however the actual expressions for decoherence length are different:
\begin{eqnarray}
a_{c}&\sim& (\hbar^2/Gm^3)^{1/4}R^{3/4}, \quad {\rm if} \quad Rm^3 \gg \hbar^2/G,\nonumber\\
&\sim& (\hbar^2/Gm^3)^{1/2}R^{1/2}, \quad {\rm if} \quad Rm^3 \ll \hbar^2/G\; .
\label{modelcoh}
\end{eqnarray}
The reasons for this difference were first studied by Di\'osi and Lukacs \cite{Diosi:87a}, and have also been recently studied in \cite{Bera:2014} and are reported by Bera et al. in the present volume.

These models based on modelling of space-time uncertainty can account for decoherence, but do not actually produce collapse to one of the many possible outcomes. This is because the modified Schr\"{o}dinger equation lacks an anti-Hermitean component. This lacking plagues essentially all treatments of collapse models: the anti-Hermitean component has to be put in by hand, for we know what outcome we desire. The fundamental origin for such a component remains to be understood.

\section{Schr\"odinger-Newton equation and stochastic gravity}
While on the one hand one takes into account the impact on the Schr\"{o}dinger equation of space-time uncertainty produced by other objects, one should also consider how the self-gravity of a quantum object influences its Schr\"{o}dinger evolution. This self-gravity itself has an inbuilt quantum uncertainty and even though we do not really know at present how to describe the self-gravity of a quantum object, we can attempt to model it.  One possible approach is the so-called Schr\"{o}dinger-Newton [SN] equation. It is proposed that that the self-gravitational potential $\Phi$ produced by a quantum source satisfies a semiclassical Poisson equation
\begin{equation}
\nabla^{2}\Phi = 4\pi G m |\psi|^2
\end{equation}
whose solution is fed into the potential dependent Schr\"{o}dinger equation
\begin{equation}
i\hbar\frac{\partial\psi}{\partial t} = - \frac{\hbar^2}{2m} \nabla^{2}\psi + m\Phi \psi
\end{equation}
so as to obtain the Schr\"{o}dinger-Newton equation \cite{Penrose:96, Penrose:98, Penrose:00, Diosi:84}
\begin{equation}
i\hbar \frac{\partial \psi({\bf r}, t)}{\partial t} =  - \frac{\hbar^2}{2m} \nabla^{2}\psi -
Gm^2 \int \frac{ |\psi ({\bf r'},t)|^2}{|{\bf r}-{\bf r'}|} d{\bf r'} \psi ({\bf r},t)
\end{equation}
This equation has been discussed extensively in the literature \cite{Bernstein:98,giulini2011gravitationally,Harrison:2003,Moroz:98,Ruffini:69,giulini:2012,giulini:2013,Hu:2014,Anastapoulos:2014, Bahrami:2014, Colin:2014}
and also in the present volume by Giulini. The equation is deterministic nonlinear, but not stochastic. This makes it different in character from the Karolyhazy and Di\'osi equation, where by virtue of the stochastic potential the models predict decoherence at the level of the master equation. The SN equation does not predict decoherence but is instead suggested as an equation whose stationary solutions are  ones to which the system will proceed upon decoherence / collapse, once a gravity-based decoherence / collapse mechanism can be incorporated in this system. What has been shown is that there is a gravitationally induced inhibition of dispersion of an expanding wave-packet, at the critical length $a_c \sim \hbar^2 / Gm^3$.

The reason decoherence is not observed is easy to see: one is only dealing with the mean potential in the semiclassical Poisson equation, whereas the Karolyhazy and Di\'osi models incorporate stochastic fluctuations by way of two point correlation of the stochastic potential, which is patterned after the space-time geodesic uncertainty.  One needs to bring in consideration of the stochastic fluctuations, apart from the mean, into the SN equation. One possible way to do this is to employ the theory of stochastic gravity \cite{Hu:2004}, which takes into account corrections to the semiclassical Einstein equations
\begin{equation}
R_{\mu\nu} -\frac{1}{2} g_{\mu\nu} R = \frac{8\pi G}{c^4} \langle\Psi| \hat{T}_{\mu\nu}|\Psi\rangle
\end{equation}
by considering the role of the two-point fluctuations of the energy-momentum tensor [going from semiclassical gravity to the Einstein-Langevin equation].

In order to take into account the effect of stress-tensor fluctuations on gravity, a classical stochastic perturbation is introduced in the metric:
\begin{equation}
g_{\mu\nu} \rightarrow g_{\mu\nu} + h_{\mu\nu}
\end{equation}
and a Gaussian stochastic tensor field $\xi_{\mu\nu}$ is defined though its two-point correlation as follows
\begin{equation}
\langle \xi_{\mu\nu}(x)\xi_{\alpha\beta}(y)\rangle_c = N_{\alpha\beta\mu\nu}
=\langle\{\hat{t}_{\alpha\beta}(x)\hat{t}_{\mu\nu}(y)\}\rangle
\end{equation}
where
\begin{equation}
\hat{t}_{\alpha\beta} = \hat{T}_{\alpha\beta} - \langle\hat{T}_{\alpha\beta}\rangle
\end{equation}
The Einstein-Langevin equation for the perturbed metric is given by
\begin{equation}
R_{\mu\nu} -\frac{1}{2} g_{\mu\nu} R = \frac{8\pi G}{c^4}
 \left( \langle\Psi| \hat{T}_{\mu\nu}|\Psi\rangle + 2\xi_{\mu\nu} \right)
\end{equation}
The Newtonian approximation to this equation is given by the modified Poisson equation
\begin{equation}
\nabla^{2}\Phi = \frac{4\pi G}{c^2} \left ( \langle \Psi | \hat{T}_{00}|\Psi\rangle+ \xi_{00}\right )
\end{equation}
It is hoped that since now the gravitational potential $\Phi$ is stochastic, its incorporation in the SN equation can induce decoherence. This is at present under investigation \cite{Mohan:2015}. A stochastic modification of the Schr\"{o}dinger equation has also been considered by \cite{Nimmrichter:2015}.

\section{Collapse models and gravity}
A collapse model modifies the Schr\"{o}dinger equation to include a stochastic element, which can dynamically explain the random outcomes of quantum measurements obeying the Born probability rule. The most successful example of a collapse model is [mass-proportional] CSL, described by the equation
\begin{eqnarray} \label{eq:csl-massa}
d\psi_t  =   \left[-\frac{i}{\hbar}Hdt
 + \frac{\sqrt{\gamma}}{m_{0}}\int d\mathbf{x} (M(\mathbf{x}) - \langle M(\mathbf{x}) \rangle_t)
dW_{t}(\mathbf{x}) \right. \nonumber \\
 -  \left. \frac{\gamma}{2m_{0}^{2}} \int d\mathbf{x}\, d\mathbf{y}\, g({\bf x} - {\bf y})
(M(\mathbf{x}) - \langle M(\mathbf{x}) \rangle_t) (M(\mathbf{y}) - \langle M(\mathbf{y}) \rangle_t)dt\right] \psi_t
\end{eqnarray}
$H$ is the standard quantum Hamiltonian of the system and the other two
terms induce the collapse of the wave function in space. The mass $m_0$ is a reference mass, which  is usually taken to be nucleon mass. The parameter $\gamma$ is a positive coupling
constant which sets the strength of the collapse process, while $M({\bf x})$ is
a smeared {\it mass density} operator:
\begin{equation}
M(\mathbf{x})
 =  {\sum}m_{j}\delta(\mathbf{x}-\mathbf{r_j}), \label{eq:dsfjdhz}\\
\end{equation}
The smearing function $g({\bf x})$ which encodes the noise correlation is taken equal to
\begin{equation} \label{eq:nnbnm}
g(\mathbf{x}) \; = \; \frac{1}{\left(\sqrt{2\pi}r_{c}\right)^{3}}\;
e^{-\mathbf{x}^{2}/2r_{C}^{2}},
\end{equation}
$r_c$ is the second new phenomenological constant of the model. $W_{t}\left(\mathbf{x}\right)$ is an
ensemble of independent Wiener processes, one for each point in space. Collapse models are discussed in detail in this volume by Bassi.

It would be significant progress if the origin of the CSL mechanism was shown to lie in some universal phenomenon such as gravity. This would imply a gravitational origin for the two new fundamental constants. However, to date such an understanding has not been achieved. In order to incorporate gravity into collapse models Di\'osi \cite{Diosi:89} proposed to replace the CSL noise correlation by the Di\'osi white noise correlation of his model discussed above, and a CSL-like collapse equation
\begin{eqnarray} \label{eq:csl-massa2}
d\psi_t  =   \left[-\frac{i}{\hbar}Hdt
 + \int d\mathbf{x} (M(\mathbf{x}) - \langle M(\mathbf{x}) \rangle_t)
dW_{t}(\mathbf{x}) \right. \nonumber \\
 -  \left.  \int d\mathbf{x}\, d\mathbf{y}\, g({\bf x} - {\bf y})
(M(\mathbf{x}) - \langle M(\mathbf{x}) \rangle_t) (M(\mathbf{y}) - \langle M(\mathbf{y}) \rangle_t)dt\right] \psi_t
\end{eqnarray}
The noise correlation is now of gravitational origin, and is given by
\begin{equation}
g({\bf x} - {\bf y}) = \frac{G}{\hbar} \frac{1}{|{\bf x} - {\bf y}|}
\end{equation}
The corresponding master equation has divergences; to regularise these a cut-off was proposed, at the natural choice of a nucleon scale \cite{Diosi:89}. Unfortunately a cut-off at this scale produces excessive stochastic heating inconsistent with observations. It was then proposed to raise this cut-off to the much higher value $r_c$ which is the new length scale in the CSL model \cite{Ghirardi3:90}. This solves the heating problem but it is difficult to physically justify the inclusion of $r_c$ in the Di\'osi collapse model, one of whose motivations was to achieve a parameter free description of collapse. In an interesting recent discussion \cite{Bahrami:2014a} Bahrami et al. compare the Di\'osi  model with CSL in some detail, and also consider the possibility   of avoiding overheating by introducing dissipation in the dynamics, instead of by going to a high cut-off.

\section{The black-hole elementary particle complementarity}
Considering that black holes and a large class of elementary particles are both fundamental entities characterized  by mass, charge and intrinsic angular momentum, it is suggestive, almost cliched, to consider a possible correspondence between the two.  While the task of searching for such a correspondence is made difficult by the fact that black holes are classical whereas elementary particles are quantum [and an $\hbar$ of course enters in the description of a quantised spin] here we discuss some ongoing work on developing such a correspondence. This work also opens up a possible way in which one might understand involvement of gravity in collapse of the wave-function.

We begin by returning to Eqn. (\ref{macro}), which is Karolyhazy's expression for the coherence length of an extended object. It can be shown that this relation continues to hold for a micro-object as well, and hence it can be treated as a general relation. It can be written in the following useful form
\begin{equation}
\frac{a_c}{R} \approx \left(\frac{L}{R_S}\right)^{2/3}\; \left(\frac{R_S}{R}\right)^{1/3}
\label{ratio}
\end{equation}
where $R_S\sim Gm/c^2$ is of the order of the Schwarzschild radius of the object. If we specialise to the case $R=R_S$ we would be dealing only with black holes [assuming they can be described classically] and this relation becomes
\begin{equation}
\frac{a_c}{R} = \left(\frac{L}{R_S}\right)^{2/3}
\end{equation}

In the macroscopic limit  $a_c\ll R$ the Schwarzschild radius  exceeds the Compton wavelength, and this also implies that $m\gg m_{pl}$, $R_S\gg l_p$ and $L\ll l_p$. The macroscopic black hole limit is obtained for large masses such that Schwarzschild radius is much larger than Planck length, and Compton wavelength is much less than Planck length. Conversely the quantum microscopic limit
$a_c\gg R$ is obtained if  Compton wavelength exceeds Schwarzschild radius, i.e.   $m\ll m_{pl}$, $R_S\ll l_p$ and $L\gg l_p$. The quantum limit is obtained for small masses such that Schwarzschild radius is much less than Planck length, and Compton wavelength is much larger than Planck length: the concept of black hole is not defined in this limit, and we are dealing with a quantum object characterized by its Compton wavelength. It is reassuring that Karolyhazy's analysis for the role of gravity in decoherence produces expected results for the quantum-classical transition from classical black holes to quantum objects.

The macroscopic limit is described accurately by general relativity, accompanied by classical equations of motion for the particle. The
microscopic limit is described by the Dirac equation  for a relativistic particle of mass $m$. (For now, it is easier to consider the relativistic case, as opposed to the non-relativistic Schr\"{o}dinger equation).  In both these cases [general relativity and the Dirac equation] the mass $m$ acts as a source term. One could enquire as to how the particle `decides' whether it should obey Einstein equations or the Dirac equation? There is no
information either in Einstein equations or in the Dirac equation which would provide an answer to this question, because neither of the equations involve Planck mass. It is only through experience that we know that micro-objects should be described by the Dirac equation and macro-objects [such as an astrophysical rotating black hole] should be described by the Kerr solution of
Einstein equations. And according to the argument presented above, for gravity induced quantum-classical transition,  the behaviour of an object is quantum or classical, depending on whether or not the associated Compton wavelength exceeds the Schwarzschild radius.  It would be significant if there was a system of equations describing the dynamics of a mass $m$, irrespective of whether or not this mass satisfies $m\ll m_{pl}$ or $m\gg m_{pl}$, and to which system the Einstein equations and the Dirac equation were approximations. Such a system of equations would significantly help in understanding the transition region $m\sim m_{pl}$ as well as provide a more fundamental understanding of gravity induced quantum collapse.

In order to make some progress towards describing Einstein equations and Dirac equations as part of a common structure, we first look for a common language for describing gravity and the Dirac field. Gravity described via the metric and the Dirac field described by spinors look very different. On the other hand, it is promising to consider Einstein gravity in the tetrad formalism; in particular through the spin coefficients which are employed for writing the Riemann tensor in the Newman-Penrose formalism, via the so-called Ricci identities. The Dirac equation too can be written for a curved space in the Newman-Penrose formalism, and then the set of four Dirac equations look strikingly similar to the Riemann tensor equations [the Ricci identities] written in terms of spin coefficients in the N-P language
\cite{Chandra:43}.

The N-P formalism is a tetrad formalism in which the basis vectors are  null vectors $\bf l, n, m, \overline{m}$ where ${\bf l}$ and ${\bf n}$ are real, and ${\bf m}$ and ${\bf \overline{m}}$ are complex conjugates of each other.  These basis vectors are regarded  as directional derivatives and are denoted by the symbols
\begin{equation}
D={\bf l}, \quad \Delta={\bf n}, \quad \delta = {\bf m}, \quad \delta^{*} = \overline{\bf m}
\end{equation}
Ricci rotation coefficients (i.e. spin coefficients) arise in the definition of the covariant derivatives of these four null vectors. There are twelve such spin coefficients, conventionally denoted by the  standard symbols
\begin{equation}
 \kappa, \sigma, \lambda, \nu, \rho, \mu, \tau, \pi, \epsilon, \gamma, \alpha, \beta
 \end{equation}

The ten independent components of the Weyl tensor are expressed by five complex Weyl scalars, denoted as
\begin{equation}
 \Psi_0, \Psi_1, \Psi_2, \Psi_3, \Psi_4
 \end{equation}
 The ten components of the Ricci tensor are defined in terms of four real scalars and three complex scalars
 \begin{equation}
 \Phi_{00}, \Phi_{22}, \Phi_{02}, \Phi_{20}, \Phi_{11}, \Phi_{01}, \Phi_{10}, \Lambda, \Phi_{12}, \Phi_{21}
 \label{Ricci}
 \end{equation}
 The Riemann tensor can be expressed in terms of Weyl scalars and Ricci scalars, and directional derivatives of the spin coefficients. There are eighteen complex equations to this effect, known as Ricci identities. A typical Ricci identity has the form
\begin{equation}
D\rho - \delta^{*}\kappa = (\rho^2+\sigma\sigma^{*}) + \rho( \epsilon + \epsilon^{*})
 -\kappa^{*}\tau -\kappa (3\alpha +\beta^{*}-\pi) + \Phi_{00}
 \end{equation}
The Ricci components are determined from the Einstein equations, and the eighteen complex Ricci identities obey sixteen real constraints known as eliminant conditions, since there are only twenty independent Riemann components \cite{Chandra:43}.

The four Dirac equations for the four spinor components $F_1, F_2, G_1, G_2$ can also be written in the N-P language, and a typical equation has the form
\begin{equation}
(D+\epsilon - \rho) F_1 + (\delta^{*} + \pi - \alpha) F_2 = i\mu_{*} G_{1}
\label{D1}
\end{equation}
where $\mu_* = mc / \sqrt{2}\hbar$. The Dirac equation has a striking similarity with the Ricci identity, with both having a pair of derivatives of spin-coefficients / Dirac spinors.  This similarity can be converted into an actual correspondence, and the four Dirac equations can be recovered as special cases of the Ricci identities, provided eight of the spin coefficients are set to zero
\begin{equation}
\rho=\mu=\tau=\pi=\epsilon=\gamma=\alpha=\beta=0
\label{vanishspin}
\end{equation}
and the following fundamental identification is {\it assumed} between the four Dirac spinors and the remaining four non-zero spin-coefficients:
\begin{equation}
F_1 =\frac{1}{\sqrt{l_p}}\; \lambda, \quad F_2=-\frac{1}{\sqrt{l_p}}\;\sigma, \quad G_1=\frac{1}{\sqrt{l_p}}\;\kappa^{*}, \quad G_2=\frac{1}{\sqrt{l_p}}\;\nu^{*}
\label{match}
\end{equation}
The Dirac equations follow provided one assumes relations between the Riemann components and the Dirac mass, a typical example being
\begin{equation}
\Phi_{20}  + \Phi_{01} = (i\mu_* + \nu)\kappa^*
\label{EDNT1}
\end{equation}
Unfortunately however, the sixteen constraints [the eliminant conditions alluded to above] on the Ricci
identities lead to undesirable constraints on the Dirac equation, and this particular approach to the Einstein-Dirac correspondence has to be abandoned.

One then looks for possible circumstances when there are no constraints on the thirty-six real Ricci identities. This can happen when the Riemann tensor has thirty-six independent components, instead of twenty. Indeed there is such a situation possible, and that is when the space-time admits torsion, and hence a Riemann-Cartan geometry, torsion being the anti-symmetric part of the connection:
\begin{equation}
\Gamma_{\mu\nu}^{\ \ \lambda} = \left\{ _{\mu\nu}^{\ \ \lambda} \right\} - K_{\mu\nu}^{\ \ \lambda}
\end{equation}
Here $\left\{ _{\mu\nu}^{\ \ \lambda} \right\}$ is the Christoffel symbol of the second kind, and  $K_{\mu\nu}^{\ \ \lambda}$ is the contortion tensor which describes the presence of torsion.
Now the Ricci tensor is no longer necessarily symmetric, and there are six additional components in the Ricci tensor, described by  the three complex quantities ($\Phi_0, \Phi_1$ and $\Phi_2$).  The Weyl tensor has ten additional components, described by the real quantities ($\Theta_{00}, \Theta_{11}, \Theta_{22}, \chi$) and the complex quantities ($\Theta_{01}, \Theta_{02}, \Theta_{12}$). For definition of these notations the reader is referred to \cite{Jogia}. Thus the Riemann tensor now has exactly thirty-six components, for which there are thirty-six real Ricci identities. There are no eliminant conditions.

The spin coefficients now have an additional term due to torsion, which is denoted by $\gamma_{1}^{nlm}$. Thus, the spin coefficients can now be written as $\gamma_{lmn} = \gamma_{lmn}^{\circ} + K_{nlm} $, where the first term corresponds to the torsion free part and the second term corresponds to the torsion component of the spin coefficients. We further use the following notation to represent the spin-coefficients (see \cite{Jogia} for details):
\begin{equation}
\kappa = \kappa^{\circ} +\kappa_1, \qquad \rho = \rho^{\circ} + \rho_1
\end{equation}
etc.

A few remarks on the fundamental significance of torsion are in order. In special relativity, the symmetry group of the Minkowski space-time is the Poincar\'e group, which includes both Lorentz transformations and translations.  In quantum theory, elementary particles are irreducible, unitary representations of the Poincar\'e group (not the Lorentz group), and these are labelled by mass as well as spin.  On the other hand, in general relativity, which describes a curved space-time, the structure group acting on the tangent space is the Lorentz group, ${\it not}$ the Poincar\'e group. Translations are not included. By introducing torsion and relating it to intrinsic angular momentum, translations are included, and the structure group of the space-time becomes the Poincar\'e group, and is no longer the Lorentz group [Riemann-Cartan geometry]. Curvature is related to Lorentz transformations in the same way that torsion is related to translations \cite{Hehl, Trautmann}. Thus, since both the Dirac equation and Einstein gravity with torsion have the Poincar\'e group as their symmetry group, it seems that correspondence between Einstein equations and Dirac equations might be more easily established if torsion is included. Of course we have to respect the fact that to date there is no observational evidence for torsion in the astrophysical world, and in empty space outside of matter, torsion vanishes. This can be achieved in the construction we now describe.

One first writes down the eighteen complex Ricci identities, now with torsion included in the spin-coefficients \cite{Jogia}. A typical example is
\begin{eqnarray}
D\rho - \delta^{*}\kappa = &\ \rho (\rho + \epsilon + \epsilon^{*}) + \sigma \sigma^{*} - \tau \kappa^{*} - \kappa (3\alpha + \beta^{*} - \pi) + \Phi_{00} \nonumber  \\
&- \rho(\rho_1 - \epsilon_1 + \epsilon_{1}^{*} ) - \sigma \sigma_1^{*} + \tau \kappa_1^{*} + \kappa(\alpha_1 + \beta_{1}^{*} - \pi_1 ) + i\Theta_{00}
\end{eqnarray}
We consider two limits. In the first limit, the torsion part of the spin-coefficients is set to zero. In this limit the Ricci identities reduce to the ones discussed previously, and if the source for the Ricci tensor is taken as the energy-momentum tensor, one recovers Einstein gravity. In the other limit, we set the torsion free part of the spin-coefficients to zero, and retain only the torsion part. We now assume that eight of these torsion dominated spin-coefficients are zero, precisely as in (\ref{vanishspin}) above, and the remaining four non-vanishing spin-coefficients are proportional to the Dirac spinors, as in (\ref{match}).  The Dirac equations then follow from the Ricci identities provided the Riemann tensor obeys the following conditions:
\begin{equation}
\Phi_{20} + i\Theta_{20} + \Phi_{01} + i\Theta_{01} - \Psi_1 - \Phi_0  = i\mu_*\kappa^*
\label{dir1}
\end{equation}
\begin{equation}
\Phi_{21} + i\Theta_{21} + \Phi_2 - \Psi_3 + \Phi_{02} + i\Theta_{02}  = i\mu_* \nu^*
\label{dir2}
\end{equation}
\begin{equation}
i\Theta_{12} - \Phi_{12} + i\Theta_{00} - \Phi_{00} + \Phi_{2}^* -\Psi_{3}^* = i\mu_* \sigma
\label{dir3}
\end{equation}
\begin{equation}
i\Theta_{10} - \Phi_{10} - \Phi_{0}^* - \Psi_{1}^* + i\Theta_{22} - \Phi_{22} = i\mu_* \lambda
\label{dir4}
\end{equation}
Thus we have the torsion-dominated limit, which are the Dirac equations, and we have the gravity dominated limit, which are the Einstein equations. In the former case, gravity is absent (Minkowski space-time) and the material behaviour is quantum. In the latter case matter behaviour is classical, and gravity dominates. Thus there must be a more general underlying theory in which the torsion-free and the torsion part of the spin-connection are both present, and to which general relativity and quantum theory are both approximations. We conjecture that GR is the $m\gg m_{pl}$ approximation, and Dirac theory is the $m\ll m_{pl}$ approximation, and the more general underlying theory, which is valid for $m\sim m_{pl}$ has the schematic structure
\begin{equation}
\frac{c^3}{G} G_{\mu\nu} - \frac{i\hbar}{l^2} [Riem]^{torsion}_{\mu\nu} = \frac{mc}{l^2} f_{\mu\nu}
\label{genee}
\end{equation}
Although the dynamics of this theory remains to be understood, some general remarks could be made. The length scale $l$ should be determined by the solution of the field equations.
In the first term on the left, $G_{\mu\nu}$ is the Einstein tensor. If this term dominates over the second term, the right hand side  reduces to the symmetric stress-energy tensor. The function
$f_{\mu\nu}$ then defines an inverse length scale $1/l$, in which case the right hand side
reduces to a mass density times speed of light. It can be inferred that when the second term on the left is negligible, the length scale $l$ is  the Schwarzschild radius.

The second term on the left side is the new idea: the Dirac field could be identified with a complex torsion in a Riemann-Cartan spacetime. If this term dominates over the first term on the left hand side, then by the quantities $[Riem]^{torsion}_{\mu\nu}$ we mean the physics in the left hand side of the four equations (\ref{dir1}) to (\ref{dir4}) above. Now the quantities $f_{\mu\nu}$ on the right hand should be linearly proportional to the corresponding spin coefficients, so that the Dirac equations maybe recovered. If the spin coefficient is of the order $1/l$, then the scale $l$ is found to be of the order of Compton wavelength $L$,  as expected. If the first term dominates we have $R_S\gg L$ and $m\gg m_{pl}$ and if the second term dominates the inequalities are reversed \cite{Sharma2014,Sharma2014a}.

When $m\sim m_{pl}$ we expect the two terms on the left side to be comparable, and this is the key point of our argument: to propose the Dirac equations as consequence of a modified Einstein gravity, with the modification being caused by inclusion of a complex torsion on a Riemann-Cartan space-time, via the Newman-Penrose equations. We can think of the first term, which contains gravity, as introducing self-gravity into the formalism, which is the modification we seek. Since the non-relativistic limit of the Dirac equation is the Schr\"odinger equation, if we could construct the non-relativistic limit of the gravity-Dirac equation (\ref{genee}) we expect to obtain a non-linear Schr\"odinger equation which incorporates the effect of self-gravity, and which could help understand role of  gravity in collapse of the wave-function.  This work is under progress.

\section{Complex space-time metric, and other ideas}
CSL sets out to construct a model for dynamical collapse based on a stochastic non-linear modification of the Schr\"odinger equation. The structure of the CSL model is uniquely determined by imposing two requirements, whose eventual origin would have to be explained by a more fundamental theory underlying CSL. These requirements are:  preservation of the norm of the state-vector, and no faster than light signalling. An anti-Hermitean linear term is added for obtaining wave-vector reduction, and a supplementary quadratic term is enforced by the requirement of norm preservation. Stochastic noise is introduced to achieve random outcomes of measurements. In order to avoid conflict with experiments \cite{Pearle:94} the noise is assumed to be mass-proportional, and couples to the local mass density operator. This is the preferred form of the CSL model, described in Eqn. (\ref{eq:csl-massa}) above.
To complete the specification of the model, the form of the noise correlation must be prescribed.

How does one introduce gravity into the CSL model? One idea, as we saw above, is due to Di\'osi, where the noise correlation of the collapse model is assumed to be the same as in the decoherence model based on gravity. However, this cannot really be called a fundamental approach, because the stochastic part of the Schr\"odinger equation has already been introduced, without ascribing any connection with gravity. In fact, as Adler points out \cite{Adler:2014}, and as we also noted above, real valued metric fluctuations lead to unitary evolution, and can at best induce decoherence, but not collapse of the wave-function.

An interesting way to relate gravity to actual collapse is to propose that the classical gravitational metric has, apart from the conventional real space-time metric $\overline{g}_{\mu\nu}$, a complex fluctuating term $\phi_{\mu\nu}$, so that \cite{Adler:2014}
\begin{equation}
g_{\mu\nu} = \overline{g}_{\mu\nu} + \phi_{\mu\nu}
\end{equation}
and a noise correlation is prescribed for the fluctuating part. From the standard definition of the energy-momentum tensor in terms of variation of the metric, it can be shown that the imaginary part of $\phi_{00}$ gives rise to a real noise coupling in the CSL equation of the type (\ref{eq:csl-massa}), thus providing a gravitational origin for the CSL noise. It should be noted that the fluctuation term is of an entirely classical nature, and in fact it is assumed that gravity itself does not have to be quantised. Although complex valued classical metrics have been considered earlier in the literature, and in some sense could be considered more natural than real metrics, it remains to understand why the complex part should be stochastic.

The issue of whether or not gravity should be quantised deserves some more discussion perhaps. If by `quantisation' is meant the application of the rules of quantum field theory to a classical theory of gravity, then the answer is likely to be no. There are various conceptual reasons to believe this, including the one that rules of quantisation are written down assuming a classical space-time background, and it does not appear logically sound to apply those rules to the very background whose pre-existence was assumed for writing down those rules. What then is the status of gravity? Can it be classical, and be described by say semiclassical Einstein equations: a quantum matter source for a classical gravity? Maybe. But then it has been argued that when fluctuations in the quantum energy-momentum tensor operator become significant, the semiclassical description will break down, and will have to be replaced at least by an Einstein-Langevin equation, with the metric acquiring a stochastic component.  To counter such arguments, Dyson has noted that objections against coupling quantum matter to classical gravity apply only to the semiclassical Einstein equations model, and further that the Bohr-Rosenfeld type argument in favour of quantising the electromagnetic field does not apply in the case of gravity \cite{Dyson:2012}. Still, we do not believe that a universe made of only quantum matter fields can coexist
with a classical space-time manifold: the quantum theory requires a classical time to describe evolution, and classical time is produced by classical bodies: there is no self-consistent demonstration that quantum matter can produce a classical space-time background in which the quantum fields evolve. Perhaps a universe made of only quantum fields requires the space-time to be noncommutative, which in itself is a `nonclassical' feature, which might act as an effective  source of stochasticity and gravity induced collapse.

We briefly mention three other ideas where gravity has been invoked to explain decoherence or collapse of the wave-function. Pearle and Squires \cite{Pearle:96a} proposed to relate the CSL noise to fluctuations in the Newtonian potential or the curvature scalar.  The theory of Primary State Diffusion due to Percival \cite{Percival:95, Percival:2005}, proposes non-differentiable fluctuations in space-time on the Planck scale to introduce stochastic terms into the evolution equation for a quantum state. The theory bears resemblance to the work of Karolyhazy described earlier. Ellis, Mohanty and Nanopoulos \cite{Ellis:84} discussed how interaction of a microscopic system with space-time wormholes can induce a non-unitary modification in the Hamiltonian evolution.

Another theoretical testing ground for CSL and gravity induced collapse is the very early universe, where these models have been applied to understand the origin of quantum to classical transition of inflationary density perturbations. While theoretical understanding is still in early stages, many investigations have been carried out, and this promises to be a useful line of research where it might be possible to put constraints on gravity induced collapse from observations of the cosmic microwave background \cite{Das:2014,Das:2013,Martin:2012,Leon:2015,Unanue:08,Castagnino:2014}. Constraints on CSL from the bounds of $\mu-$ and $y-$ distortions of the CMB have been studied in \cite{Lochan:2012a}.

It has also been suggested that a modification in quantum theory of the CSL type (or gravity induced modification) can help resolve the black hole information loss paradox \cite{Okon:2014}. Thus it seems that time is ripe to consider applications of collapse models in diverse theoretical, astrophysical and cosmological situations, apart from solving the measurement problem or understanding the quantum-classical transition in laboratory systems. Doing so will on the one hand constrain collapse models, and on the other hand might even assist in solving long-standing theoretical puzzles.

\section{Possible experimental tests}
The most direct experimental tests of departure from quantum theory in the mesoscopic regime are being carried out through molecular interferometry, and optomechanics \cite{Kleckner1999,Marshall:03,RMP:2012,Aspelmeyer:2011,nimmrichter2011testing,Hornberger2011review}. These tests look for a possible breakdown of the quantum superposition principle. No breakdown has been observed to date. Even if a breakdown were to be discovered, it will signal that quantum theory is approximate, but the source of the departure cannot be pinned down to gravity. It is curious that we do not have a gravity specific test, even at the gedanken level, using which we can say that if a violation is discovered, it is necessarily due to gravity. One reason for this is that predictions of gravity induced decoherence / collapse are not sufficiently accurate quantitatively - for instance the quantitative predictions of the Karolyhazy model and the Di\'osi model differ substantially. Theoretical studios have to improve considerably in their precision and reliability, before a gravity specific test can be proposed.  In the same vein, bounds on CSL models coming from laboratory and astrophysical data are also bounds on gravity models \cite{RMP:2012}.

Another promising avenue, apart from interferometry and optomechanics, is a laboratory test for anomalous random walk of a quantum object induced by CSL or by gravity. It is known that the CSL effect induces a tiny stochastic heating of the collapsed particle, leading to a very small energy-momentum violation, too small to contradict any of the known data. However, the momentum violation induces an anomalous random walk which can be in principle be detected at low temperatures and extremely low pressures. Such an experiment has been proposed, but not yet planned or executed. The CSL induced random walk competes with two other standard effects, these latter two being thermal Brownian motion of the particle under consideration, coming from its interaction with ambient radiation (scattering, absorption and emission). The second  standard effect is collision with molecules of the ambient gas (normal Brownian motion). Both these effects can be reduced sufficiently by going to pressures of about
a pico Torr (achievable) and a temperature of 100 Kelvin or lower. It also turns out that the anomalous effect  is easier to detect via the rotational displacement of a disc, as opposed to the translational displacement of a sphere, by levitating the disc, its ideal linear size being about $10^{-5}$ cm  \cite{Bera2015, Collett:2003}.
Gravity induced collapse / decoherence also predicts such a random walk, though the effect is typically a few orders of magnitude smaller than in the case of CSL \cite{Bera2015, Collett:2003}.
Another promising approach which has recently gained prominence is investigation of spectral line broadening due to stochastic heating \cite{Bassi:2014a,Bassi:2014b}. While the focus has been on CSL, it would be worthwhile looking into gravity induced effects as well.
It seems particularly relevant and important to look for an experimental effect which could discriminate between a gravity induced collapse and a non-gravitational CSL mechanism.

\section{Concluding Remarks}
There are indeed very many ideas which have been tried to investigate if decoherence and collapse of the wave-function can be caused by a gravitational effect. Maybe finding a formulation of quantum theory which does not refer to classical time will throw light on the nature and origin of the quantum-classical transition. The models of Karolyhazy, Di\'osi and Percival, though built on heuristic principles, give very suggestive results. Similarly, including stress tensor fluctuations in the Schr\"{o}dinger-Newton equation indicates gravity induced decoherence. The idea of a complex metric with a stochastic imaginary part is also very attractive, as a neat source for the CSL noise. The black hole - elementary particle complementarity suggests that a gravity theory with torsion bridges general relativity and relativistic quantum mechanics contained in the Dirac equation, and the underlying theory incorporates quantum effects as well as self-gravity. None of the models proposed thus far provide a fundamental explanation for the Born probability rule, nor definitively conclude whether or not special relativity needs to be modified when gravity and quantum mechanics are combined. It is difficult at this stage of our understanding to say whether gravity should be `quantised' in the sense of there being a description of gravity which necessarily has quantum fluctuations as opposed to classical stochastic fluctuations. Nevertheless, diverse investigations of this nature, where the gravity-quantum interface is studied to address unresolved issues in quantum theory, have fascinating conceptual facets, and should be pursued vigorously. These should be accompanied by experimental efforts to ascertain the domain of validity of quantum theory.

\vskip 1 in

{\it ``...I would like to suggest that it is possible that quantum mechanics fails at large distances and for large objects. Now, mind you, I do not say that quantum mechanics does fail at large distances, I only say that it is not inconsistent with what we know. If this failure is connected with gravity, we might speculatively expect this to happen such that $GM^2/\hbar c=1$, or $M$ near $10^{-5}$ gm....If there was some mechanism by which phase evolution had a little bit of smearing in it, so it was not absolutely precise, then our amplitudes would become probabilities for very complex objects. But surely, if the phases did have this built in smearing, there might be some consequences to be associated with this smearing. If one such consequence were to be the existence of gravitateion itself, then there would be no quantum theory of gravitation, which would be a terrifying idea..."}

\bigskip

\rightline{- Feynman (1961)}

\newpage

\noindent {\bf Acknowledgements:} I would like to thank the organisers of DICE2014 for giving me an opportunity to speak at the conference. It is a pleasure to thank my collaborators Angelo Bassi, Shreya Banerjee, Sayantani Bera, Suratna Das, Sandro Donadi, Kinjalk Lochan, Satyabrata Sahu,  Seema Satin, Anushrut Sharma, and Hendrik Ulbricht for interaction and discussions. This work is supported by a grant from the John Templeton Foundation ({\#39530}).

\section*{References}

redpajama_set_name: RedPajamaArXiv


USATF Certified (VA13030RT) loop course through River Club community on roads, paved trails and a small section of grass.
The Mile course is an out and back course in River Club community on roads, using the last 1/2 mile of the 5km course.
I-95 to exit 126. Rt 1 South to left on Rt 17 (Mills Drive). Left on Benchmark Road. Take Benchmark Road to Tidewater Trail (Rt 2) and continue straight at the light into the parking lot of River Club Church.


vTiger and SuiteCRM are both open source CRM solutions and are being widely used in the industry. Both of them are the offshoots of the SugarCRM CE and have added quite a lot of functionality since. They both are loved equally by the business owners and are actively developed and supported by the developers of the software and the community alike. The post digs deep into various factors while deciding vtiger vs suitecrm for your business implementation.
While the main motto of vTiger is Grow Sales, Improve Marketing ROI, and Deliver Great Customer Service, SuiteCRM intends to build a software to be used as an alternative to Microsoft Dynamics, SalesForce and SugarCRM Professional. In this post, we will have a look at various aspects and features of both and how they fair with regards to each other.
Both vtiger and suitecrm have moved quite far from original implementation of SugarCRM CE. They are quite comparable as and when it comes to features and you wont be disappointed with one or the other. While the normal features like Account, Leads, Contacts, Campaigns, Opportunities, calls, quotes, documents, notes, products are common in both the product, vTiger moves more towards Purchase order, sales order and some other ERP side features. SuiteCRM on the other hand keeps focused on workflow and other important CRM functions.
The UI of both the CRMs re not that very much 2017ish but its improving as they develop. In a nutshell, one must research a bit on the organisation workflow and then decide on which one tom implement in your organisation. This can go a long way in impacting your organisation's productivity.
Both the vtiger and SuiteCRM come with fully featured free versions. Both of them require that you host the free version on your own servers only.
Paid versions are priced differently, while the vtiger's business model is reliant on the Saas hosting of the platform and the support it offers along with, the SuiteCRM earns by offering various levels of paid support and other features. vtiger's pricing starts from 10USD per user per month. SuiteCRM pricing varies on the level of support you are looking for.
While the free version of both SuiteCRM and vtiger require that you use the forum and community support may you get stuck with some problem, the paid versions have genuine support levels built into them. The developer community is very well developed for both the platforms and there is no dearth of plugins and extensions for both the systems.
Both the SuiteCRM and vtiger are very well integrated with various business apps and tools like Google Apps, Microsoft Office, outlook, Calendar and Task tools. You can find various integrations as plugins and extensions built by the developers.
In the modern day, its very important that the CRM data be available across mobile and on the field where your team is actually working. Both SuiteCRM and vtiger have a lot of apps available on apple and google play store to complement both your free and paid versions. These apps take your data mobile and you can work and perform quite a few actions on the go itself.
NextRedmine Installation Guide: How to install Redmine on Shared/Dedicated Host?
This is really interesting comparison.Nicely explained.


Alzheimer's & Peanut Butter: Is There Really a Connection?
Imagine peanut butter helping you or a loved one determine your risk for Alzheimer's. It may seem far-fetched at first mention, however researchers at The University of Florida believe there could be a significant connection between the sense of smell and Alzheimer's. The Mayo Clinic helped identify that one of the first indicators of cognitive decline, even before noticeable memory loss, is a failing sense of smell – and so the Alzheimer's peanut butter test was created.
The Sniff Test: Can Smelling Peanut Butter Detect Alzheimer's?
In the experiment, the researchers gathered 90 participants who ranged from having confirmed early stage Alzheimer's and other forms of dementia, as well as a control group with no cognitive or neurological problems. The participants then took part in a "smell test." They were each asked to smell a spoonful of peanut butter from a short distance.
The results found that those with a confirmed early stage Alzheimer's diagnosis had trouble smelling the peanut butter. Even further, that group had more difficulty when it came to smelling with the left nostril versus the right nostril, something unique to the disease.
Does the Sniff Test Actually Pass the Sniff Test with Experts?
It isn't time to start self-diagnosing Alzheimer's peanut butter links just yet. Other scientists have research that refutes these findings. Some question the validity of the study itself. The sample size was relatively small, with less than 100 people participating.
Additionally, researchers at the University of Florida noted that a variety of non-Alzheimer's-related traumas can affect olfactory abilities. For instance, someone having difficulty smelling may have had a severe sinus infection at some point in their life, inhibiting their ability to complete the test accurately. So, while Alzheimer's and sense of smell are related, there isn't always a direct cause-and-effect relationship.
While the link between Alzheimer's, smell, and the peanut butter test is being developed in a meaningful way, there are more conclusive signs that could indicate a cognitive decline. Memory loss, especially with recently learned information is one sign, as is a decrease in judgement.
Other signs include difficulty completing familiar tasks or an inability to retrace steps and find missing objects. Problems defining time or place, understanding visual images, and suddenly stumbling with words while speaking are also indicators.
Finally, friends and family should take notice of a senior's withdrawal from social activities and a change in personality — another Alzheimer's related abnormality. A comprehensive list can be found at Alzehimhers.org along with a helpful chart that outlines the important differences between normal age related changes (for instance, forgetting which word to use) and dementia-related cognitive decline (difficulty having a conversation).
The research going into the discovery of early indicators of cognitive decline can ultimately help with the research into cures. Additionally, knowing the warning signs can mean earlier diagnosis by a doctor and subsequently a head start on treatment from facilities that offer Alzheimer's and dementia support like Griswold Home Care. Memory care for the patient will be important in the early stages of the disease as it helps them retain meaningful activity and interpersonal connections.
What do you think of the Alzheimer's peanut butter test? Do you think it may hold some validity, or have you heard of other research being done to more easily diagnose this disease. We'd love to hear from you in the comments below.


text:
Tag Archives: robbers
10 reasons why you should sell your diamonds IMMEDIATELY
All across the country, many people can be found who own diamonds. Some women wear them on the forth finger of their left hand to indicate that you shouldn't ask them out; others sport large versions of the stones, hanging from their ears, as an alternative to "spacers"; certain gentlemen, who recite lyrical words for a living into microphones, have diamonds embedded into miniature avatars of themselves that hang from gilded chains around their necks. Then there are the people that have diamonds hidden in their attics, in tiny treasure chests, saving them in the event of a complete economic breakdown where we must resort back to a pre-civilized barter system. Of all the multitude of the diamond hoarding human classifications, there is one thing that unites them: they all should sell their diamonds ASAP.
1 – Walking around with valuable pieces of glittering, sparkling glass fragments on your body is a surefire way to draw the attention of criminals looking to make an easy score. Just look at what happened to Batman's parents. Ditch those pricey pieces post haste, before you become the prime target for a malicious mugging/horrendous hugging.
2 – In the same way that you become the pièce d' résistance for professional bandits, you make yourself ready bait for bothersome relatives and deadbeat friends. They won't rob you in quite the exact aggressive manner as the aforementioned gem-snatchers, but they will bombard you with nonstop requests for monetary assistance. The ugly, glittering truth is that they are not even to blame; by wearing diamonds you turn yourself into a walking billboard for ostentatious luxury and arrogant opulence.
3 – You work hard every day at your job. You put in extra hours, you follow up with all business leads that may benefit the company – you even attend the damnable Holiday Party every year with a warm (however forced and obsequious) grin on your face. Think you're due for a raise, right? NOPE. Not with that huge rock on your finger/ear/nose. You look like you have too much money already. Sorry, you can email HR though – who'll promptly delete your complaint, for all the same gem encrusted reasons.
4 – Diamonds are very hard, and in some cases, very sharp. Now, what do you think happens when you lose weight? Your digits shrink and your rings become loose. The harmless activities of every day life can cause your ring to droop down, and when you go to close your hand around a plump orange or send a hilarious (in your mind) tweet – OW! Your backwards set diamond has just stabbed ye, and it's off to the E.R. for an afternoon of agony.
5 – Let's paint a similar scenario: you've dropped some pounds and all your clothes are now hanging on you. You casually attempt to hail a cab and – whoosh – your ring goes flying off your slender finger and into the night. Oops. You are not even aware of this until later, when you realize you've just lost an item that cost thousands upon thousands of greenbacks.
6 – You may be grinning to yourself at this point, thinking "Ha! I never lose weight – in fact, I've been steadily gaining girth for years!" Well, touché. Oh, you may want to consider this though; those who have amassed extra poundage and have rings that are now permanently stuck on their fingers are at a great risk of losing circulation entirely and, ultimately, needing to have their finger amputated. Won't be so funny anymore, when you're walking around giving people 'High Fours.'
7 – Diamonds are forever. That is, until you can't find them anymore. If you happen to fall into the grouping of people who squirrel away your diamonds in remote corners of your cellar, attic or furnace, there may come a day when you are ready to remove said stones and: WAH? They're missing! From actual squirrels (and other pesky varmints) that just love to burrow into tight places and pilfer shiny things to similarly rodential children and grabby roof shingle repairmen, there's a whole host of creatures/people who can get to your gems before you do. Sell those rocks before they get their grubby little mitts on them first.
8 – For every old diamond that doesn't get sold, a "new" diamond must be excavated from the ground to meet diamond consumer demand. This endless stream of terrestrial destruction has anything but a positive impact on the environment; in fact, it wreaks havoc on certain sensitive ecosystems, which can ultimately lead to the decimation of endangered species and worldwide environmental devastation. So, essentially, every time you don't sell your old diamonds, the air we breathe becomes poisonous and a baby seal dies.
9 – Owning a diamond engagement ring leads to divorce. Statistics show that out of all divorced couples, over 80% of them had a diamond engagement ring exchanged (well, this documentation refers to 'married coules,' but all divorced couples were married at one time, so whatever). The numbers don't lie. Sell your diamond engagement ring right now, or the chances are highly in favor that you will get divorced. Already divorced? Well, there you have it then. Best to sell any residual diamonds before they can do any more damage.
10 – Finally, we have the most substantial (and serious) reason. While diamond demand has not waned dramatically in the U.S., international diamond prices have seen a significant downward spiral. This is no passing trend; it's just the way things are. Take a gander at what some of these news sources have to say on the matter: Forbes, Time, MarketWatch. The smartest economic decision you can make in this very moment is to sell your diamonds now, before things get exponentially worse. The good news here is that at Diamond Lighthouse we can help you recover the absolute highest value for your diamond jewelry (typically any piece that features a diamond 1 carat and higher). Our unrivaled open bidding platform will get you the best price for your diamond, every single time. Find out more, right…NOW!
November 17, 2015 Expertisebeggers, broken engagement, carat, cash for diamond, diamond, diamond appraisal, diamond engagement ring, diamond jewelry, diamond lighthouse, diamond news, diamond upgrade, diamond worth, diamonds, engagement ring, french bulldog, gemstones, how to sell diamond, how to sell my diamond, Liza Minelli, moving on, relationships, rick ross, rings, robbers, secondhand diamond dealer, sell diamond, sell diamond advice, sell diamond rings, sell jewelry, sell my diamond, sell my jewelry, sell my ring, sell your diamond, selling diamonds, selling your diamond ring, separation, Wedding Ring, what to do with rejected engagement ringjoediamondlighthouse
Recent (and Insane) Jewelry & Cash Heists
This has been quite a year in the world of high stakes jewelry heists. All over the globe, from right here in NYC's Diamond District to the luxury boutiques of London to Thai airports to Mom 'n Pop Shops in the Midwest, jewel thieves have been striking with reckless abandon. The caliber of gem pilferers have ranged from highly successful and calculating posses, like the infamous Pink Panthers, to renegade solo stealers, like a particular femme fatale who has been on quite the tear as of late – and is currently wanted in several US states.
What has lead to this dramatic increase in dangerous, violent and unfortunately lucrative jewel crimes? Are these new age criminals utilizing technology to figure out the security patterns of jewelry stores with deadly precision, and seeing this as a way to make 'easy money?' Have international economic woes contributed to people seeking innovative and coincidentally illegal methods for obtaining cash? Is it somehow Trump's fault?? Not ruling out any of these options, it really is hard to say with any certain degree of accuracy what is the true root cause. One thing is for sure; many of these elite larcenies have been hair-raising, to say the least. Here we take a look at some of the more jaw-dropping-ly fascinating tales of jewel and dough poaching that have occurred over the last few years.
Diamonds of Anarchy
London's Brent Cross Mall, 2012. A fairly standard autumn morning in homogenized British shopping. Then…half a dozen masked (helmeted) motorcycle men (presumably from Hades) rode INTO a jewelry store on the second floor of the shopping complex and proceeded to wreak havoc. They smashed the jewelry containers with bats and axes and grabbed whatever they could carry in their avaricious mitts. Riding two to a bike, the loot snatchers jumped back on their partners' backs and blazed out of there to freedom. After all was said and stolen, 3.1 million dollars in Rolex and Cartier watches, along with sundry loose diamonds and gems (and even a few sale items) were gone forever. All the police were able to turn up in the ensuing investigation were the motorcycles themselves, which had been stolen and were left abandoned in a golf course not far from the mall. The motorcycle gang, or "club" as Jax Teller would say, remain at large to this day.
Couldn't Belieb their Own Eyes
In May of 2013, a truly pop-tastic heist occurred. Technically, no jewelry was stolen, but the amount of plundered cash (half a mil) is enough to raise an eyebrow or two. More importantly, is the venue where this caper went down: FNB Stadium in Johannesburg, South Africa. Thousands of adoring fans were rocking out to arguably one of the greatest musical talents of our time – heck, of EVER. That's right; the Bieb. While the concert raged on, and many a tween girl wept with hormonally confused ecstasy, a cadre of supplemental security guards (hired just for this epic event) were chainsawing or exploding or god-only-knows-what-ing a two foot concrete floor which gave way to where all the cash from the night's revelry was stored. The thieves then high tailed it out of there before the final, haunting refrain of "If I Was Your Boyfriend" was even sung.
Cannes Not Believe this Happened
When one thinks of the city of Cannes, nestled on the coast of the French Riviera, images of film festival opulence and extravagant vacations come to mind. A lone dude in a "baseball cap and scarf" toting a handgun who is somehow able to steal 136 million dollars in gems, watches and baguettes from the extra fancy Carlton International Hotel is probably not what you would picture. However, that is precisely what went down in 2013 at the famed location. The reason all these valuables were just hanging around the hotel was because Lev Avnerovich Leviev, an Israelite with billions of shekels to his name, had them on display there, in a "private salon." Too bad the paltry guards assigned to watch said watches and jewels were not trained to deal with an actual robbery (also, they had no guns themselves). So, the solitary fellow strolled over with his pistol, politely asked for the goods and said "au revoir." Ironic twist: this hotel is where Hitchcock's 1955 hit "To Catch a Thief" was filmed.
…This thief has not been caught.
Putting Seniors to Work
This past May, London's premier jewelry district, Hatton Garden (a name befitting a location out of "Great Expectations") felt a little bit of a squeeze. One of the area's "safest" safety deposit vaults was expertly invaded and drained of 300 million dollars worth of jewels and pounds. Aside from the staggeringly high amount of quid that was snatched, what makes this case so intriguing is the age of the robbers. The youngest man, out of the nine suspects, was 48, and the most senior was 76. They tunneled their way into the vault, carving out a perfectly cylindrical hole just wide enough to fit presumably the thinnest member of the elder gang. Ultimately, all nine of the thieves were apprehended, which confirms the theory that older people may have the wisdom to pull off a heist of this magnitude, but probably aren't that particularly great at running away from the police.
One Bold Babe
The Eastern Seaboard has very recently fallen prey to one daring and dazzling dame. The unidentified woman has hit three states thus far: South Carolina, Georgia and Florida (appears this larcenous lady has an affinity for beachy locales). In all of the accounts, she has allegedly overpowered all the workers, zip-tied 'em up and made off with thousands of dollars in jewels. The FBI has stepped in and vows to take immediate action (but if anything can be learned from watching the 'X-Files,' it's that the FBI is not always adept at getting to the truth…even if it really is out there). Surveillance footage of the woman depicts a tough and attractive individual (possibly similar to Gina Gershon's character in the film "Bound"), but the police sketch of her makes her look like Carmen San Diego.
via CNN.com
Each day it seems at least one jewelry store is hit, somewhere on this vast planet of ours. No one can say what exactly motivates these enterprising thieves (aside from the obvious: money), or if they will slow down any time soon. All we can do is hope that no one is injured in any way in these robberies, that the victims are fully insured…and that the stories continue to be this juicy.
September 21, 2015 ExpertiseCartier, diamond watches, diamonds, famous thieves, female robber, Femme Fatale, gemstones, heists, how to sell my diamond, international crime, international criminals, jewel thieves, jewelry, jewelry heists, jewels, Justin Bieber, London robbery, money, motorcycle gang, pink panthers, robberies, robbers, Rolex, sell my diamond, sell my diamond jewelry, selling diamonds, stealing diamonds, thievesdiamondadmin
Pink Panthers: Diamond Thieves
Watching cartoons as children made us all fantasize about "what-ifs." What if we could actually make cartoons real? What if we could have our favorite heroes' powers? What if our favorite characters walked among us? From G.I. Joe to Marvel's Avengers to Snow White and the Seven Dwarves, we dreamed of making our cartoon world a reality.
When a group of diamond thieves from various Balkan countries were dubbed the "Pink Panthers," they probably weren't necessarily sharing the same dream. They probably weren't watching cartoons and dreaming of becoming jewel thieves, but they did succeed in making their exploits worthy of Hollywood. Some of their heists being so well orchestrated many believe they are similar to the big screen productions like The Avengers or Transformers. Video footage of the heists awes audiences when their signature car, an Audi, crashes into a jewelry store and two gun men armed with revolvers and crowbars leap out of the crash and start robbing all the diamonds they can get their hands on as helpless bystanders flee for their lives. It's a scene from a movie made reality.
Continue reading Pink Panthers: Diamond Thieves →
May 8, 2015 Expertisecash for ring, diamond heists, diamond jewelry, diamond news, diamond ring, diamond thieves, diamond value, diamond worth, diamonds, how to sell diamond, how to sell jewelry, how to sell my diamond, panthers, pink panthers, robberies, robbers, secondhand diamond dealer, sell diamond advice, sell jewelry, sell my diamond, sell your diamond, selling your diamond, selling your diamond ring, stealing diamondsdiamondadmin
Stolen Diamonds: Reclaimed!
All good things must come to an end. That includes the dizzyingly euphoric and fancy free period when a purloined gemstone comes into one's possession. Due to inscriptions and intaglios of authenticity etched directly on to the facets of super valuable diamonds, it's a lot harder than one would think to "move" them. Unlike stolen cash or even gold (which can easily be melted down), diamonds are highly traceable, and often result in reclamation by the rightful owners (unless of course the thieves in question are smart enough to employ a corrupt diamond cutter, who can expertly remove any signatures of ownership without significantly diminishing the carat weight …just saying). Of the millions and millions of dollars worth of stolen diamonds that have disappeared over time, many have been recovered and the perpetrators of the crimes punished accordingly. Here are some of our favorite tales of thievery…and retribution.
Continue reading Stolen Diamonds: Reclaimed! →
August 22, 2014 Celebritycash for diamond, diamond crimes, diamond news, heists, pawn shop, reclaimed diamonds, robbers, sell my diamond, sell your diamond, selling your diamond, stealing diamonds, stolen diamonds, thievesjoediamondlighthouse

redpajama_set_name: RedPajamaCommonCrawl


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Takanori Nishikawa to perform Kamen Rider Zero One Opening Theme Song
Takanori Nishikawa, originally known as T.M. Revolution, is confirmed to perform the opening song for Kamen Rider Zero One!
Takanori Nishikawa will also be collaborating with J of Luna Sea.
J of the band Luna Sea, composer of the show's theme song.
The song is entitled "「REAL×EYEZ」".
Takanori Nishikawa aka T.M. Revolution is best known for performing various theme songs for anime series such as Rurouni Kenshin, Gundam Seed/Seed Destiny, and Thunderbolt Fantasy.
Kamen Rider Zero-One premieres Sept. 1, 2019.
https://natalie.mu/music/news/344013
Categories: Kamen Rider , Kamen Rider Zero-One , TM Revolution
Good choice of singers Toei, made me impressed
If nothing else, at least the theme song should be awesome af
I feel that Gundam rhythm on zero one, cannot wait fo the song preview.


Interviews with Richard Godwin, Gilbert King, Conor McCreery, Laura McDermott, and Will Viharo. Visual Art by Andrés Pruna and Terry Wright. Fiction by William Auten, M.H. Burkett, Paul Colby, T.C. Jones, Gary Porter, K.J. Hannah Greenberg, and Tony Press. Nonfiction by Anna Laird Barto, Sarah Pearsall, and Jeffrey Weinstock. Poetry by Chris Abbate, Sean Ball, Jonathan Duckworth, Roberta Feins, Ariel Francisco, Peter Grieco, Allison Joseph, Joseph Mills, Barbra Nightingale, and Pad Wadsworth. Welcome Betty-Jo Buro and Thomas Logan.


This is SHA Scotland's contemporary motion to the 2012 Scottish Labour Party conference.
This conference notes that the Alcohol (Minimum Pricing) Bill is currently being considered by the Scottish Parliament. The Bill seeks to introduce a price at which a unit of alcohol cannot be sold below with the aim of reducing alcohol consumption and related harms.
Conference recognises that Scotland has one of the fastest growing rates of chronic liver disease and cirrhosis in the world. There are more than 42,000 hospital discharges due to alcohol related illness and injury and mortality as a direct result of alcohol has more than doubled since the early 1990s. Alcohol is a contributory factor in 1 in 20 deaths in Scotland. 49% of Scottish prisoners (including 76% of young offenders) and two-thirds of those accused of homicide said they were drunk at the time of their offence. Alcohol misuse costs Scotland an estimated £3.56bn per annum. Scottish consumption of alcohol is now 23% higher than in England.
Conference accepts that there are legitimate concerns about the legislation. The measure can be viewed as unfairly penalising the majority of moderate drinkers and disproportionately affecting low income groups who tend to pay less for a unit of alcohol. There is also a concern that if alcohol prices increase, problem drinkers with a low income may use spending from elsewhere in their budget to maintain their consumption levels to the detriment of families. The legislation may also be incompatible with EU law. However, we have to accept the evidence of the relationship between price and consumption.
Conference recognises that taxation could achieve the same benefits, with the added advantage that revenue would go to the state rather than the retailers. However, excise duty is a reserved power and there are no indications that the UK Government is prepared to act. A compensatory levy, similar to the recent 'Tesco Tax', could cover this point.
Conference believes that for Scottish Labour the impact on reducing health inequalities by reducing the harm caused by alcohol is a key issue. People living in our poorer communities carry a disproportionate share of alcohol-related health and social harm. Alcohol mortality rates are six times higher in the most deprived areas. Our primary concern should therefore be to introduce alcohol policies which are in the public health interest and will be effective in reducing the high levels of alcohol harm in Scotland.
Conference recognises that minimum unit pricing is widely supported by the medical and public health community and also by the police, children's charities and a wide section of civil society. While we recognise concerns over the effectiveness of the measure there is an overwhelming need to take action.
Conference therefore believes that we should be prepared to consider supporting the Alcohol Minimum Pricing Bill as one measure in a more comprehensive plan to reduce alcohol harm, subject to a detailed evaluation process including fully assessing adverse effects particularly on poorer communities, families, and individuals; extension of the compensatory levy, and a corresponding sunset clause.


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When deciding whether it is time to repair or replace your roof, it is important you have a certified professional you can trust that will help you explore your options. Cross Construction Co. Roofing & General Contractors has served the New York area since 2002. We always offer free estimates and a thorough consultation so that together we can determine if a roof replacement is a viable option for your business or home. We operate with the highest ethical standards and will always give you an honest and realistic estimate for our work. With Cross Construction Co. Roofing & General Contractors you should only expect the highest quality materials and installation procedures.
We have built our reputation on service excellence, so when its time to evaluate your roofing, we are New York's roof replacement professionals you can count on. One of the things to consider when evaluating repair or replacement is future costs. When only part of your roof has a problem, but the roofing crew is there with all the equipment, scaffolding in place and permits, would it be feasible to go ahead and have the entire roof done now, rather than have all this set back up again in the future? The best way to decide is to look at the average lifespan of your roof, serviceable years left, frequency of malfunctions and current condition. Whenever a major repair is necessary, since estimates are free it is never a bad idea to price out the cost of a roof replacement as well.
Should you decide to take the plunge into new roof territory, rest assured there are some market advantages. First is peace of mind. With a new roof you won't have to worry about leaks, blowoffs or other repair necessities for some time. Then you have energy efficiency. When your roof begins to have visible problems, one of the other issues you may be suffering that is unseen is loss of energy. With a new roof, energy efficiency is restored and that makes a noticeable difference in your energy costs. Lastly, and arguably the most important advantage, is increased comfort. Whether for your home or business, roof disrepair causes inconvenience and discomfort. A new roof from Cross Construction Co. Roofing & General Contractors will alleviate all that.


text:
A History Of British Airways Advertising – Part 9
A look at British Airways' advertising over the past 50 years as BA seeks to recover from the financial crisis, delves into the past to relaunch its brand identity and tells passengers not to fly.
London Air Travel » British Airways » British Airways Advertising & Branding » A History Of British Airways Advertising – Part 9
British Airways "Taxi" Advertisement, 2012 (Image Credit: Bartle Bogle Hegarty for British Airways)
Welcome to the ninth part of our series on the most influential and noteworthy BA advertising of the past 50 years.
We turn towards the end of the first decade of the century. BA seeks to recover from the global financial crisis, delves into the past to relaunch its brand identity and tells passengers not to fly.
Kitesurfer
"Don't Fly"
The Happy Lemon, Happy Jumper & Relaxed Trainer
The collapse of Lehman Brothers in September 2008 had a huge impact on BA.
The airline's financial lifeblood, long-haul premium traffic, fell away sharply.
BA swung from a profit of £922m in 2008 to a loss of £401m in 2009. There were even questions as to whether the airline would survive in its current form.
Here is a very softly spoken advertising campaign BA ran 12 months after the collapse of Lehman Brothers.
It featured 9 films in total gently encouraging both business and leisure passengers to fly and pursue new opportunities around the world such as Mumbai Fashion week and the migration of wildebeest across the Serengeti.
The campaign was noteworthy in that apart from a reference to BA's route network at the end of the voiceover, it does not make any specific reference to any relative benefits of flying BA, nor does it feature any visuals of BA aircraft or cabins.
In September 2011, BA relaunched its brand by reintroducing the slogan "To Fly. To Serve."
This had been a long part of BA's heritage. It features on its Coat Of Arms.
This advert "aviators" focuses the role of BA and its predecessor airlines in aviation history right from the very first flight on 25 August 1919. It is notable for its focus on the "hardware" of aviation rather than the softer aspects you usually see in advertising.
This was an online advert featuring Boeing 747 Captain Claire Bunton demonstrating her passion for being in the air kitesurfing on the coast of East Preston, West Sussex.
What do you when you are the official airline of Team GB and Paralympics GB, the Olympic Games and Paralympic Games are taking place in your home city, where to its residents your whole raison d'être (in the good times at least) is to fly them elsewhere?
Well, tell your passengers not to fly. That's what BA did ahead of the 2012 Olympic Games and Paralympic Games.
In a series of print adverts and a TV advertising campaign, BA simply told people not to fly, stay at home, and support the home team.
"Don't Fly. Support Team GB" (Image Credit: Bartle Bogle Hegarty for British Airways)
In the TV advert a British Airways Boeing 777 aircraft is being prepared for take-off at Heathrow. Instead of taxing to the runway, it makes its way to the Olympic Park in Stratford, passing a number of London landmarks (Trafalgar Square, The Palace of Westminster, The Shard) on the way.
The advert features many touches that show attention to detail, such as the seat belt sign being activated as the aircraft passes a speed bump on the road.
The clever move behind this campaign is that it is easy for people to be cynical about brands supporting major events and appearing to simplify piggyback on the achievements of others. This avoids that. Though of course by the time the campaign was run those who had already decided to leave London during the games had already made plans.
These were three spots from 2012 highlighting the specific benefits of short-haul flying, namely complimentary drinks, a checked luggage allowance, and free seat selection 24 hours before departure.
Just one of these is now offered.
Author LondonAirTravelPosted on 24 April 2020 22 February 2022 Categories British Airways, British Airways Advertising & Branding
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According to our database1, Colleen Richey authored at least 24 papers between 2003 and 2018.
Voices Obscured in Complex Environmental Settings (VOiCES) Corpus.
Robust Speaker Recognition from Distant Speech under Real Reverberant Environments Using Speaker Embeddings.
Toward human-assisted lexical unit discovery without text resources.
The SRI Speech-Based Collaborative Learning Corpus.
Privacy-Preserving Speech Analytics for Automatic Assessment of Student Collaboration.
Classification of lexical stress using spectral and prosodic features for computer-assisted language learning systems.
Morphological Modeling for Machine Translation of English-Iraqi Arabic Spoken Dialogs.
The SRI AVEC-2014 Evaluation System.
Lexical stress classification for language learning using spectral and segmental features.
Emotion detection in speech using deep networks.
Articulatory trajectories for large-vocabulary speech recognition.
Identifying Agreement/Disagreement in Conversational Speech: A Cross-Lingual Study.
Using Prosodic and Spectral Features in Detecting Depression in Elderly Males.
Automatic identification of speaker role and agreement/disagreement in broadcast conversation.
Acoustic data sharing for Afghan and Persian languages.
Detection of Agreement and Disagreement in Broadcast Conversations.
Improving Language Recognition with Multilingual Phone Recognition and Speaker Adaptation Transforms.
Recent advances in SRI'S IraqCommTM Iraqi Arabic-English speech-to-speech translation system.
Effects of vocal effort and speaking style on text-independent speaker verification.
Iraqcomm: a next generation translation system.
Speech Recognition Engineering Issues in Speech to Speech Translation System Design for Low Resource Languages and Domains.
Limited-Domain Speech-to-Speech Translation between English and Pashto.
Development of phrase translation systems for handheld computers: from concept to field.


Bill O'Brien confirmed that the starting quarterback job is indeed Tom Savage's.
For as much time as Houston Texan fans have had to spend watching semi-infuriating quarterback competitions during the Bill O'Brien Era, the 2017 preseason is probably the one time that those fans would have welcomed a true competition. With Tom Savage and his two career starts named the incumbent by O'Brien, and with future franchise QB Deshaun Watson waiting in the wings, most fans would rather just cut to the chase and start the Watson era now.
During training camp and the preseason, Savage has been fine. Nothing spectacular, just fine. Meanwhile, Watson has been inconsistent with flashes of spectacular. In preseason games, Savage has had a high completion percentage on largely dink and dunk type stuff, while Watson has made a few "WOW" plays each game, including two rushing touchdowns that made him look like an alien compared to Texans quarterbacks of years gone by.
So barring a medical issue or just a complete collapse in this Saturday's game in New Orleans, it will be Savage leading this team onto the field on September 10. The early schedule will be tough sledding for a guy with two career starts — home for the Jaguars (not a bad defense), a Thursday night game in Cincinnati (against whom Savage generated 12 points last season AT HOME), and a Sunday in New England.
The bottom line? Watson better stay warmed up and ready, as there's a good chance his services will be required at some point before October.


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Post award to your blog.
Thanks the blogger who presented this award to you and link back to their blog.
Nominate 11 bloggers who you believe deserve some recognition and have less than 200 followers.
Note: I'm not making any nominations, since I haven't followed any new blogs since my last Liebster Award.
If you had the opportunity, would you go see a musical based on an anime or manga?
YES! Sailor Moon, Naruto, and Haikyuu!!
Mac. Transitioned over to Mac after my Dell died in 2007 and have loved it since. Only have had to put my MacBook in the shop once due to me *giggles* crashing the hard drive. It didn't cost me a penny.
What Internet browser do you usually use?
At work: Firefox & Chrome. At home: Safari & Firefox.
iOS, Android, Windows Phone, other, or none?
iOS. Since iPod Touch(2008), which still works. Finally got an iPhone 4 in 2010 and upgraded last year to iPhone 5S. I typically change phones every 3-4 years or till the hardware doesn't work anymore.
Do you (or have you ever) played an instrument?
I played piano when I was younger, but never really went back to it.
Have you ever traveled outside of your country?
Multiple times. Canada, Germany, England, France, Austria, Italy, Slovenia, Belgium, and Japan (this December).
Can I choose more than 1? 20s for tap dance, 70s for rock music, and 80s for my childhood TV shows.
What's the weirdest anime or manga you've ever watched or read?
Hmm… That's a tough one. The only one that comes to mind is Terra Formars because I find cockroaches creepy and the enemies are humanoid roaches. *shivers* Ironically it's also one of my favorite seinen series.
Currently obsessed with all the stories available through Sparkler Monthly. *psst* If you love strong female characters, then you should check them out and become a member.
I'm a bookworm who wishes to have 1 room in my future house dedicated to my library.
I think I went overboard on the number of conventions I'm attending this year (7 in total).
Have I mentioned I LOVE to dance?! 😀 I dance while cleaning house, while sitting in my desk chair, and even while cooking. On occasion has gotten comical when I get caught.
I love food especially German, Mexican, and Italian cuisine.
A pet-peeve of mine is people sending texts all in acronyms. I have to sit there and decipher some of the ones I don't recognize.
Favorite characters I adore… Wait for it… Grimmjow Jaegerjaques, Kakashi Hatake, and Sousuke Yamazaki.
I'm a late adopter to social media networks. MySpace: 3 years after "everyone" was on it in 2006. Facebook: 2 years after it went public. Twitter: Late 2011. Pinterest: last week.
I'm bilingual in English and German. Can partially get by in Spanish, Italian, and Slovenian.
Hmm… What else? Oh! I was almost a July 4th baby. I was born at 21:21 July 3rd.
Whoa! I just realized that 21 is a frequent number in my personal information: full name = 21 characters long, born at 21:21, numeral birthdate – 7 x 3 = 21. Now I wonder what the numerology charts say about that.
Well, that ended up being really personal. Hope y'all enjoyed it!
The 21 thing is pretty interesting!
I'd definitely go see a Sailor Moon musical, and the Naruto cast made me drop my jaw in how closely the cast looks like the manga. Props to the casting directors and makeup/costume staff. Would also love to see the upcoming Kodocha play just for Mitsuishi.
Oh! I totally forgot about Kodocha. I'd see that, too.


Waren House Hotel is easily found from the A1 by following the signs to Bamburgh (signposted B1342). Whilst the mapping doesn't indicate it very clearly, the hotel is a few hundred yards from Budle Bay (it's at the bottom of the drive) - a tidal bay famous for its wading sea bird population.
Just a short distance away is the village of Bamburgh which is dominated by a magnificent castle which sits atop a rocky outcrop.


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