text:
\section{Introduction}

The ISS has recently completed its construction activities and is now moving
into its period of utilization, providing space payloads with a long-term,
stable platform\footnote{http://www.nasa.gov/mission\_pages/station/research/benefits}. Its large solar arrays and Ku-band antennas provide the ISS
with power and data capabilities which are capable of supporting multiple
payloads. The result is that scientific payloads can be attached to the ISS
without needing their own power supply or data downlink capability, and with
reduced requirements on the attitude control system, thus significantly
reducing the cost and time required to fly an experiment in space. Also, since
payloads are launched to the station on independently scheduled rockets, they
do not need to fund their own dedicated rocket, further reducing the cost of
the mission.

One such payload is the Optical Testbed and Integration on ISS Experiment
(OpTIIX), a mission to demonstrate the capability of robotically assembling a
1.5 m diffraction limited optical telescope in space. The key long-term goal of
this technology is to enable the robotic assembly of a future 10 m+ size
telescope capable of characterizing extrasolar terrestrial planets and
searching them for signs of life.
OpTIIX also has a number of potential science applications, including monitoring of outer
solar system planetary atmospheres, stellar population studies of nearby
star-forming regions, and fast followup of astrophysical transient
events. OpTIIX has completed a Preliminary Design Review and is now
seeking funding for the construction phase, with a possible operation
start in 2017.

Another potential payload, now in the conceptual study phase to address an
upcoming NASA Mission of Opportunity, is ISS-Lobster, a wide-field imaging
X-ray telescope. Based on glancing incidence focusing of 0.3-5 keV X-rays,
ISS-Lobster is intended to provide a simultaneous wide field of view, high
spatial resolution, and high sensitivity, to advance the field of time-domain
X-ray astronomy. Its scientific goals include the study of tidal disruptions of
stars by supermassive black holes, the observation of supernova shock
breakouts, gamma-ray bursts, and the long-term variability of active galactic
nuclei.

Both OpTIIX and ISS-Lobster are planned for mounting on platforms which will be
in nearly continuous communication with ground-based alert networks through the ISS
data link, allowing the fast pointing of the telescopes in response to an
astronomical transient. This suggests the possibility of their use in an
extremely important scientific scenario around the middle of this decade, the
electromagnetic follow-up of ground-based gravitational wave detections.
Gravitational waves are produced by the interaction of extremely dense and
massive objects including black holes (BH) and neutron stars (NS). Mergers of
these compact objects also produce electromagnetic radiation: NS-NS and/or
NS-BH mergers are likely to be the source of short Gamma-Ray Bursts, a very
bright transient source of gamma, optical and X-ray signals, and also the
source of a predicted long-lived optical afterglow known as a kilonova. The
observation of BH and NS mergers is likely later this decade with the
availability of a network of gravitational wave detectors; the coincident
observation of a compact object merger event in the electromagnetic bands would
provide a rich complement to the science of the merger, and crucially, would
also help to verify the event itself.

In this article we give an overview of the OpTIIX and ISS-Lobster designs. We
then describe the network of planned gravitational wave detectors, and then
discuss the possibilities for electromagnetic follow-up observations with the
ISS telescopes.

\section{ISS telescopes}

\subsection{OpTIIX}

The OpTIIX (Optical Testbed and Integration on ISS Experiment) instrument \citep{2}
consists of six modules that will be launched separately and assembled
robotically on the ISS, including six deformable primary mirror segments. An
overview of the experiment is as follows. The modules as shown in figure \ref{fig:1} are: the
Telescope Core Module, including the avionics, star trackers to determine the
telescope position, the wavefront sensing and control unit used to focus the
telescope, and the imaging camera; the Gimbal Module to provide three
degree of
freedom pointing; the Secondary Tower Module which contains the secondary and
tertiary mirrors and coarse steering mirror; and three Mirror Segment Modules,
each of which contain two primary mirror segments and their actuators, along
with laser metrology components.

\begin{figure}
	\includegraphics[width=\columnwidth]{1-optiix}
	\caption{Exploded view of OpTIIX}
	\label{fig:1}
\end{figure}

The modules will be assembled on the ISS with the use of the Special Purpose
Dexterous Manipulator (SPDM), the ISS robot arm. All of the telescope
components handled by SPDM will contain the necessary interfaces and attachment
mechanisms. The SPDM has an articulating body, an assortment of tools, cameras
and sensors, and a pair of seven-jointed arms to allow efficient assembly of
OpTIIX. The ISS location of OpTIIX has not yet been determined.

The assembled telescope can be described as follows. The primary mirror,
comprised of six hexagonal segments of 50 cm diameter, has the shape of a conic
asphere, and has a diameter of 1.45 m. The primary shape is adjusted by means
of six rigid-body actuators, and 90 shape actuators, attached to each mirror
segment backing structure. The actuators provide primary figure control, as
well as high precision alignment of the segments to the telescope. Laser
metrology, enabled with a frequency stabilized laser source \citep{3,4} and beam
launchers on the primary and fiducials on the secondary, provides the
measurement of the distance and alignment between the primary and secondary \citep{5}.
The telescope is focused with image-based wavefront sensing and control
algorithms. The focus process proceeds in three stages: Shack-Hartmann sensing
for the segments initial alignment, dispersed fringe sensing for segment
co-phasing, and phase-retrieval sensing for the final wavefront adjustment to
achieve diffraction-limited performance. An imaging camera is used to obtain
the diffraction-limited images, and will include a filter wheel with eight
positions, including three wide-band and three narrow-band optical filters. The
final OpTIIX performance specifications are: diffraction limited performance
with a Strehl ratio of 80\% at 600 nm, signal-to-noise (SNR) of 5 for a star of AB
magnitude 22 or fainter in a total exposure time of 20 min, and field of view
of $\sim$3 arc min square.

Jitter noise on the ISS from anthropogenic sources as well as the expression of
ISS structural modes is attenuated with the use of a pointing platform which
also serves to position the telescope at a given sky location. This is a key
technical challenge for OpTIIX since the full telescope performance corresponds
to a sub arc sec pointing requirement. The current pointing control design
includes three loops: star trackers and gyro input to the gimbal, coarse steering mirror control
using data from the gyro, and tertiary mirror control using feedback from the
fine guidance sensor. Trade studies are ongoing.

Once assembled and operational, OpTIIX will be tasked with the acquisition of
at least 50 color images of diffraction-limited astronomical targets for
education and public outreach (EPO) use. A set of science observations will
also be undertaken, to the extent that time permits.

\subsection{ISS-Lobster}

ISS-Lobster is a wide-field X-ray telescope now under study at Goddard
Space Flight Center, planned to be situated on the ISS Express
Logistics Carrier.  It consists of two instruments, the soft
  X-ray (0.3-5 keV) Wide Field Imager (WFI), and the hard X-ray
  (10-1000 keV) Gamma-ray Transient Monitor (GTM).  It simultaneously
provides wide field of view (FOV), high position resolution, and high
sensitivity. These characteristics enable the search for transient
X-ray events.

\begin{figure}
\begin{center}
	\subfigure[Lobster focusing optic]{
	\includegraphics[width=0.8\columnwidth]{2a-raypath}
	\label{fig:2a}}
	\subfigure[ISS-Lobster instrument on 3-axis gimbal]{
	\includegraphics[width=0.8\columnwidth]{2b-pointing_platform}
	\label{fig:2b}}
	\caption{ISS-Lobster elements}
\end{center}
\end{figure}

Figure \ref{fig:2a} shows the principle of operation, which is similar to that employed
(in the optical band) by the namesake crustacean \citep{6}. The WFI X-ray optic consists of
an array of square-packed channels, molded into a spherical shape. The long
axes of the channels intersect a distance R along the axis of symmetry. X-rays
undergoing odd numbers of grazing reflection are brought to a focus a distance
R/2 along the symmetry axis. This gives rise to a cruciform point-spread
function consisting of a cross-shaped pattern (caused by X-ray reflections an
odd number of times in one plane and an even number of times in the other) with
a central focus, and a uniform background (caused by an even number of
reflections in both planes). The ratio of the components is about 25\% in the
focus, 50\% in the cross-arms, and 25\% diffuse background.

ISS-Lobster WFI will consist of a microchannel plate array with 75 cm radius of
curvature, with an area of 40 cm $\times$ 40 cm. The focal plane detector will be a CCD
camera, with image resolution of about 250 $\mu$m (FWHM), and energy
resolution better than 100 eV. These parameters give rise to a wide field X-ray
telescope with FOV of 30$^\circ$ x 30$^\circ$, an angular resolution
of 8 arcmin FWHM and 1 arcmin localization accuracy,
and a sensitivity of 1.3$\times$10$^{-11}$ erg/(cm$^2$\,sec) in 2000 sec for an energy range
of 0.3 to 5 keV. The focusing capability gives ISS-Lobster over a factor of 30
more sensitivity than previous wide-field X-ray telescopes -- e.g. the BAT
detector on {\it Swift} \citep{7} and the GSC detector on MAXI \citep{8}.

The WFI module will be deployed on a pointing platform to remove the ISS
jitter, and to allow fast positioning (Figure \ref{fig:2b}) This will require a control
system consisting of a three-axis gimbal and star tracker. Initial studies have
shown that pointing at the level of 1 arcmin is achievable.

The WFI FOV of $\sim$2\% of the sky will enable the detection of gamma-ray
bursts ($\gtrsim$0.3/day), supernova shock breakouts ($\sim$1-2/yr), and tidal disruptions of
stars by supermassive black holes ($\gtrsim$14/yr). Many other sources will be available
for study, including active galactic nuclei, stellar flares, and neutron star
bursts.

ISS-Lobster GTM consists of a single Sodium Iodide (NaI)
  scintillation detector identical to those comprising the {\it
    Fermi}-GBM.  It will provide high time resolution data on transient
  sources over an energy range of 10-1000 keV.  While it will provide no source
  localization within its FOV, the simultaneous gamma-ray trigger with
  a GW event will confirm the astrophysical origin of the GW source, and allow for
  the possible verification of sub-threshold GW triggers.

\section{LIGO and the ground-based gravitational-wave network}

Gravitational radiation arises in regions of strong and dynamical gravitational
fields from astronomical sources, including very dense and
massive objects such as black holes and neutron stars. Its character describes
the nature of gravity in the extreme, testing the predictions of Einstein's
theory of gravity and providing information about its sources unobtainable
through other means. In contrast to the electromagnetic waves of conventional
astronomy, which arise from the incoherent superposition of emission from the
acceleration of individual electric charges, gravitational waves result from
coherent, bulk motions of matter. Also, because gravitational waves interact
only weakly with matter they are able to penetrate the very densely
concentrated matter that produces them. The direct detection and study of
gravitational waves has the potential to revolutionize our understanding of the
universe.

A gravitational wave produces a differential strain (ratio of change in
distance to distance between two points) in space-time along orthogonal
directions, and can be observed through the relative timing of the passage of
light waves along these directions. Because gravity is a very weak force, the
strain expected at the earth from the gravitational waves of the most likely
astrophysical sources is very small, of order 10$^{-21}$.

A number of detectors around the world have been built, or are being
constructed, to search for gravitational waves. The general design is shown in
figure \ref{fig:3}, and is based on the principle of laser interferometry \citep{9}. A frequency
stabilized laser injects light into an interferometer beam splitter, where the
light is split and directed downstream through a light storage arm to test mass
end mirrors, and then reflected back and recombined at the beamsplitter. The
interferometer is operated so that destructive interference of the recombined
light occurs; the photodiode monitoring the output light of the interferometer
is then highly sensitive to any differential motion of the mirrors which
disturbs the exact cancellation of the light. A very high level of displacement
sensitivity, of order 10$^{-18}$ m rms, is achieved through careful attention to the
frequency and amplitude stability of the laser light, the losses of the
interferometer optics, the seismic isolation system which decouples the
interferometer from motions of the earth, and the suspension system which
stabilizes and positions the optics. Kilometer scale detectors are required to
enable sufficient strain sensitivity for gravitational wave detection.

\begin{figure}
\begin{center}
	\includegraphics[width=\columnwidth]{3-interferometer}
	\caption{Gravitational wave interferometric detector schematic}
	\label{fig:3}
\end{center}
\end{figure}

Gravitational wave signals anticipated by these ground-based detectors include:
continuous waves from non-axisymmetric pulsars, stochastic backgrounds of
sources from the early universe, burst signals from a non-axisymmetric
supernova explosion or other unmodeled event, and signals from the inspiral and
merger of a compact binary system with a black hole and/or neutron star. The
most promising of these sources for the first detection is the NS-NS or NS-BH
merger, which becomes likely with a detector strain sensitivity of 10$^{-22}$ rms,
integrated over the  detector frequency range of 10 Hz to 2000 Hz.

The gravitational wave network of detectors includes the Laser Interferometer
Gravitational Wave Observatory (LIGO) \citep{10}, with 4 km detectors in Hanford,
Washington (Figure \ref{fig:4a}) and Livingston, Louisiana; the 3 km Virgo \citep{11} observatory
in Pisa, Italy; the 600 m GEO \citep{12} interferometer in Germany; the 3 km KAGRA \citep{13}
detector under construction in Japan; and a 4 km detector recently approved for
construction in India \citep{14}. LIGO and Virgo completed in 2010 a one year period of
observation, and both projects are undergoing an upgrade to their
detectors\footnote{Advanced Virgo documentation and notes https://wwwcascina.virgo.infn.it/advirgo/docs.html} \citep{15}. Full sensitivity for these detectors is expected for LIGO and
Virgo around 2018, for KAGRA around 2020, and for the India detector in 2022.
At full sensitivity LIGO will have a detection range for a NS-NS binary merger
of 200 Mpc, and for a NS-BH merger of 400 Mpc. The detection rate for these
sources is uncertain to a factor of 10 in both directions, but the highest
probability is 40/yr and 30/yr, respectively \citep{17}.

\begin{figure}
	\begin{center}
	\subfigure[Aerial view of LIGO site at Hanford, WA]{
	\includegraphics[width=0.9\columnwidth]{4a-hanford}
	\label{fig:4a}}
	\subfigure[World network of GW detectors]{
	\includegraphics[width=\columnwidth]{4b-network}
	\label{fig:4b}}
	\caption{Current and future ground-based interferometric GW detectors}
\end{center}
\end{figure}

As more detectors become operational in the network the result will be a higher
detection sensitivity, as well as a better sky location of sources: for three
detectors, the sky error box for the binary NS merger will be $\sim$100 deg$^2$ at a
network SNR of 10, but with four and five detectors the error becomes 20 deg$^2$
and 5 deg$^2$, respectively \citep{18}. For the time frame of the deployment of the ISS
telescopes, 2016--2017, the gravitational wave network will consist of the three
detectors from LIGO and Virgo.

\section{Electromagnetic Follow-up of Gravitational Wave Detections with OpTIIX and ISS-Lobster}

\subsection{Electromagnetic counterpart science}

The detection of electromagnetic counterparts to gravitational wave signals
from these NS-NS and NS-BH mergers with OpTIIX and/or ISS-Lobster will
powerfully enhance the science of the compact merger event. In brief, the
detection of an EM counterpart will:
\begin{itemize}
	\item{Locate the galaxy of the source progenitor. The position resolution
			of OpTIIX and ISS-Lobster is at the level of 1 arcsec and 1 arcmin,
			respectively, both easily high enough to locate the progenitor
			galaxy for an event within the LIGO detection range of 400 Mpc.}
	\item{Determine the source redshift. With the galaxy location determined,
			ground based spectroscopic telescopes can follow-up the detection
			and determine the host redshift. When combined with the source
			distance that can be extracted from the gravitational waveform,
			this could lead to a more precise local determination of H$_0$, the
			Hubble constant \citep{19}.}
	\item{Deliver information on source beaming,
			and examine the afterglow energetics to probe the progenitor and
			its gas environment.}
	\item{Test predictions of General Relativity,
			including the speed and polarizations of gravitational waves.}
	\item{Lift degeneracies associated with the binary source parameters \citep{20}.
			Extraction of key binary source information such as luminosity
			distance and inclination is limited by the poor sky localization of
			the Gravitational Wave (GW) network. The precise sky localization enabled by the EM
			counterpart signal will assist in the analysis of the gravitational
			waveform, allowing significantly higher precision in the extraction
			of source parameters.}
	\item{Raise the confidence level of a GW
			detection. The coincident measurement of an EM signal with a GW
			detection, both spatially and temporally, will greatly aid in
			reducing false detections. This can allow the lowering of the GW
			detection threshold, extending the range of the measurement.}
	\item{Determine the engine of the short Gamma-Ray Burst (sGRB). The sGRB,
			extensively studied by the NASA mission {\it Swift} \citep{21}, is believed to be
			due to a compact object merger. Analysis of a gravitational wave
			signal coincident with an EM signal from an sGRB will definitively
			determine whether the event is due to an NS-NS or NS-BH merger.}
\end{itemize}

In the ISS telescope observational scenarios described next, we will consider
first the known optical and X-ray afterglow signatures which follow the prompt
gamma-ray signal of the sGRB. The sGRB afterglows decay
with a several hour timescale, and are excellent candidates for follow-up
detection within an ISS orbital period of 90 minutes. The engine for the
extremely high energy sGRB has been established with a reasonable degree of
confidence as an NS-NS or NS-BH merger by examining the stellar populations
associated with observed sGRBs \citep{22}; this implies a known gravitational
wave signal associated with this source. We can estimate the rate of a GW/X-ray
or GW/optical coincidence for the sGRB as follows. The observed sGRB rate
\citep{23,32} is $\sim$10/(Gpc$^3$\,yr) (which includes beaming of the prompt
gamma-ray into a nominal 15 deg cone); within the advanced LIGO range of 200
Mpc for a randomly oriented NS-NS merger, this gives an afterglow coincidence
rate of 0.3/yr, assuming the afterglow has the same beaming as the prompt
signal. However two factors enhance this rate. First, the amplitude of a
gravitational wave is peaked along the GRB axis by a factor of 1.5. Second, the
requirements of a time coincidence between the GW and prompt gamma-ray, and a
spatial coincidence between the GW and the X-ray or optical afterglow source
locations, can lower the GW network threshold by a factor of 1.5 while keeping
the same false positive rate\footnote{The sensitivity improvement from
	requiring an EM coincidence depends on both the gravitational-wave
	background rejection factor, and the empirical shape of the background
	about the threshold of interest. The factor of 1.5 used in this calculation
	is consistent with a factor of 10$^7$ GW background rejection from the
	requirement of a prompt short gamma-ray coincidence within 5 sec and X-ray
	afterglow within 100 deg$^2$, and a GW background distributed approximately
	exponentially with rate $\sim$ 100$^{-\mathrm{SNR}}$ about SNR=10 (e.g. the
	two-detector NS/NS background in \cite{34}, figure 3. The X-ray transient
	rate within 100 deg$^2$ was estimated from \cite{35}, which looked for
	transients visible for 7.5 hours or less at a flux limit of
	$\sim$10$^{-12}$ erg/s/cm$^2$. 32 potential candidates were found in a
	survey coverage of 76,000 deg$^2$ day, giving a rate of $\sim$10$^{-4}$
	transients per deg$^2$. This may be extrapolated to 10$^{-3}$ per 100
	deg$^2$ at 10$^{-11}$ erg/s/cm$^2$ as a rough estimate for the Lobster
	transient rate.}. Together these two factors will extend the gravitational
wave detection range by 2.3, leading to a coincidence rate of 4/yr. For the
NS-BH merger engine, the advanced LIGO range is 400 Mpc, and similar reasoning
gives an EM/GW coincidence rate of 30/yr.  These rates need to be adjusted for
the efficiency of the X-ray and optical afterglow detection by the ISS
telescopes, discussed below.

We also consider the signature for a so-called kilonova \citep{25}, a predicted (but not
yet observed) optical afterglow from a NS-NS merger, powered by heating from
the radioactive decay of heavy elements created in the merger ejecta. A
significant advantage in the detectability of the kilonova coincidence with a
gravitational wave is that its optical emission is believed to be isotropic, so
that its rate is not limited by the possibility of beaming away from the
earth \citep{26}. Since all NS-NS mergers are expected to result in a kilonova, we use a
NS-NS merger rate of 1,000/(Gpc$^3$\,yr) \citep{17} and a sky-average range of 200 Mpc for
randomly oriented NS-NS mergers to predict a GW-EM rate of 40/yr. (For the
kilonova there is no preferred orientation, and the optical afterglow is
expected to occur amidst a significant  background level, and thus the GW range
enhancements discussed above do not apply. Also, the difference in kilonova and
sGRB rates of a factor of 100 can be reconciled through the beaming associated
with the sGRB emission.) Finally, kilonova emission still occurs in low-density
environments where sGRB optical afterglows become very weak.

\subsection{ISS telescope pointing}

In the event of a gravitational wave candidate signal from an NS-NS or NS-BH
merger, an alert can be issued to the astronomical community within 5
minutes \citep{27}. The alert will contain the sky localization error box associated
with the event, and will be immediately available to the ISS telescopes through
the continuous ISS data link. Both OpTIIX and ISS-Lobster will be mounted on
pointing platforms that can slew to a given sky position, with a time lag
dependent on the ISS position. The maximum delay for ISS-Lobster to access the
LIGO-generated sky position will be slightly less than 1/2 the period of the
ISS orbit, or 40 min, with an average delay equal to half the maximum, or 20
min. OpTIIX is expected to be able to schedule follow-up observations within
the next orbit, which makes it an excellent complement to a related
ground-based optical telescope follow-up effort \citep{28,29}; a further advantage of
the OpTIIX ISS deployment is the increased angular resolution possible above
the atmosphere.

In order to maximize the likelihood of detecting the
  electromagnetic counterpart to a GW trigger, ISS-Lobster will begin
  pointed observation as soon as a GTM short duration trigger occurs
  by tiling the $2\pi$ steradian GTM FOV with the WFI in 25 short ($\sim$1
  min) pointings starting from the zenith direction, until a source is either
  detected or the GW position is uploaded.

The main impediment to full sky viewing on the ISS are the solar panels, whose
position varies on a daily and seasonal basis, and the Sun; after accounting
for these factors, the average viewing efficiency
of ISS-Lobster and OpTIIX are expected to be about 80\%. To avoid excessive
repointings from the large number of false positives associated with LIGO
sub-threshold triggers, a coincidence with the sGRB prompt gamma-ray signal,
obtained with the ISS-Lobster NaI detector, will be required before either
telescope is slewed to the LIGO sky position.

\begin{figure}
	\includegraphics[width=\columnwidth]{5-skymap-withfov}
	\caption{ISS-Lobster FOV (dotted line) and NS-NS location error box \citep{36} where contours indicate 1, 2 and 3$\sigma$ confidence. The star indicates the true source location.}
	\label{fig:5}
\end{figure}

An important issue for the telescopes is locating the source within the 100
deg$^2$ gravitational wave error box. ISS-Lobster has a significant advantage
here, as its large 30$^\circ$ $\times$ 30$^\circ$ field of view allows it to encompass
the gravitational wave sky error box from a NS-NS merger with a network SNR of
10, as shown in figure \ref{fig:5}, and localize the source to 1 arcmin. The large FOV
for ISS-Lobster is optimal for the early phase of operation of the
gravitational wave detector network ($\sim$2017), with three detectors and a sky
localization error box of 100 deg$^2$. In contrast, covering the full error box by
tiling observations with OpTIIX would require an excessively large and
impractical number of pointings, since its FOV is only 3 arcmin. Instead, the
detection of the optical afterglow of an sGRB could be enabled by first
localizing the source position with ISS-Lobster to 1 arcmin, so that it can be
contained within the OpTIIX field of view. In this case the OpTIIX detection
rate is limited by ISS-Lobster.

\begin{figure}
	\subfigure[{\it Swift} sGRB X-ray afterglows scaled to GW
          horizon (400 Mpc). The vertical lines represent the fastest
          response times for the follow-up scenarios.  At least 80\%
          of the afterglows will be detectable by ISS-Lobster.]{
	\includegraphics[width=\columnwidth]{6a-xrt_lc_at_400mpc_comb2}
	\label{fig:6a}}
	\subfigure[sGRB optical afterglows with OpTIIX threshold]{
	\includegraphics[width=\columnwidth]{6b-optical_lc_at_400mpc_comb2}
	\label{fig:6b}}
	\caption{{\it Swift} known-sGRB afterglow light-curves with flux re-scaled to 400 Mpc}
	\label{fig:6}
\end{figure}

If ISS-Lobster is not available, another possible solution, for sources within
100 Mpc, is to restrict OpTIIX pointings to galaxies within the LIGO range,
since the location of a compact merger (as seen as an sGRB) appears to track
the total mass of galaxies. For this purpose a galaxy catalog was assembled
from publically available information, known as the GW Galaxy Catalog (GWGC) \citep{30}.
This catalog (60\% complete at present), contains $\sim$50,000 galaxies out to a
distance of 100 Mpc, with roughly one galaxy per square degree of sky, or 100
hosts for a typical sky position error of 100 deg$^2$. By using a weighting with
the galaxy luminosity (a proxy for total mass), the potential number of hosts
can be further reduced to $\sim$40, which captures 90\% of the total catalog luminosity, and
can finally be reduced to 10, by requiring the capture of 50\% of the total
luminosity, resulting in (0.6 $\times$ 0.5) or 30\% total probability of detection. This is a
number of pointings (1 or 2 per orbit) that could be realistically accomplished
by OpTIIX within the day-long decay time of an optical afterglow. An upgrade to
GWGC to increase its listings, optimize its performance and increase its range
is ongoing\footnote{J. Kanner, private communication}.

\subsection{ISS-Lobster follow-ups}

At least 80\% of sGRBs produce an X-ray afterglow, as detected
by {\it Swift} within the first few hundred seconds.  The
efficiency of detecting an X-ray afterglow with ISS-Lobster is
indicated in figure \ref{fig:6a}, where the flux from 43 sGRBs (17
with measured redshift, and 26 with no redshift) is plotted versus
time, with the redshift used to scale the source flux to a distance of
400 Mpc (those GRBs with no measured redshift are considered to be
located at a median redshift of 0.7.)  The vertical lines
  indicate the minimum times to begin WFI observation after a GTM sGRB
  trigger and subsequent tiling, or follow-up observations of GW
  trigger position.  Roughly 80\% of the afterglows will be detectable
  with the WFI. Including the ISS viewing efficiency (80\%), a
  conservative X-ray/GW coincidence rate is 1-2 sGRB/yr (at 440 Mpc;
  NS-NS) and 12 sGRB/yr (at 900 Mpc; NS-BH). These rates are also
  based on the assumption that the GW detector network is operating
  at full sensitivity (200 Mpc for LIGO, 100 Mpc for Virgo) and 80\%
  duty cycle.

We note that these rates assume that the X-ray afterglow is beamed to the same
degree as the prompt signal, however the evidence for this is weak at best, as
evidence for beaming (an achromatic break in the X-ray light curve) is seen in
only two or three of the 43 sGRB afterglows \citep{32}. If the afterglow is more
isotropic than the prompt signal, as some models assume \citep{33,37}, the X-ray/GW
coincidence rates will go up accordingly (in this case we may modify the prompt
coincidence requirement with the GTM.

\subsection{OpTIIX follow-ups}

About 30\% of all sGRBs have optical afterglows. The optical afterglow to an
sGRB within the LIGO detection range will appear bright (16--18 mag) at times
less than 5 hours after the gravitational wave alert, and then dim
significantly over the course of a day. Thus OpTIIX will be able to observe the
decay of the light curve by repeated exposure to the source over multiple ISS
orbits. Figure \ref{fig:6b} shows the flux from 13 sGRBs (8 with measured redshift, and 5
with no redshift) plotted versus time, with the redshift used to scale the
source flux to a distance of 400 Mpc (those GRBs with no measured redshift are
considered to be located at a median redshift of 0.7.) The vertical dotted line
is set at the average time required for a source to come in view by OpTIIX, and
the horizontal line shows the sensitivity. All the afterglows are bright enough
to be detected. Assuming OpTIIX is pointed to the source location by first
imaging the X-ray afterglow to 1 arcmin with ISS-Lobster, the sGRB optical/GW
coincidence rate is 1/yr for the afterglow of the NS-NS merger engine, and 4/yr
for the NS-BH merger. Again, these rates will increase if the afterglow beaming
is more isotropic than the prompt gamma-ray.

The isotropic kilonova optical afterglow has a longer timescale than that of
the sGRB. It is predicted to peak around 1 day after the NS-NS merger with a
magnitude between 19 and 22, and decay over the following 3 days. Again
assuming that the source is first localized by the (beamed) X-ray afterglow
with ISS-Lobster, the OpTIIX detection rate for the kilonova optical/GW
coincidence is $\sim$2/yr. In contrast, if the source is within 100 Mpc, the galaxy
map can be used to guide the OpTIIX search for the kilonova signal with about
10 pointings, yielding a rate of about 1/yr given the 30\% detection
probability achievable with the galaxy catalog mentioned above. This may be an
important followup source in the time period before LIGO reaches its full
sensitivity. Finally, addressing the difficult problem of distinguishing a
kilonova from background transient events including supernovae and variable
stars will require an accurate measure of the candidate signal time variance,
measured over successive ISS orbits. The ISS deployment of OpTIIX will mean
that atmospheric fluctuations will not be present in the measurement of source
variability (a key challenge for ground-based optical telescopes).

\section{Conclusions}

The ISS platform offers a unique and inexpensive opportunity for
electromagnetic follow-up studies of gravitational wave sources. These
follow-up studies will offer a wealth of complementary science including
determining the source location and redshift, removing degeneracies in the GW
analysis, and raising the signal-to-noise of the event. The technology
demonstrator OpTIIX, a 1.5 m diffraction limited optical telescope, is
scheduled for ISS operation in 2016. ISS-Lobster, a time-domain X-ray
observatory, is in the conceptual design phase for a proposal to a Mission of
Opportunity, which could be operational in 2017. These schedules coincide well
with the planned operation of the LIGO and Virgo gravitational wave detectors.

Both OpTIIX and ISS-Lobster will be mounted on pointing platforms in continuous
communication with ground-based gravitational wave alerts, allowing the fast
acquisition of the source sky location. The source location within the large GW
sky error box ($\sim$100 deg$^2$) expected in the initial operating phase of the GW
network can be imaged within the FOV of ISS-Lobster to 1 arcmin, allowing a
follow-up by OpTIIX and localization to 1 arcsec. Use of a galaxy catalog can
also independently guide the pointing of OpTIIX if the source is within 100
Mpc.

With the assumptions that 1) a short GRB is powered by either an NS-NS or an
NS-BH merger, 2) the X-ray and optical afterglows of an sGRB are beamed into
the same opening angle as the prompt gamma-ray, and 3) a kilonova is the
correct description of the long-term optical afterglow of a NS-NS merger, the
coincident rates for EM/GW signals are: X-ray signal from sGRB with NS-NS
(NS-BH) merger engine, 2/yr (12/yr); optical signal from sGRB with NS-NS
(NS-BH) merger engine, 1/yr (4/yr); optical signal from NS-NS kilonova using
galaxy catalog to guide pointing, 1/yr; optical signal from NS-NS kilonova
using ISS-Lobster to localize source, 2/yr. These rates encourage the planned
use of these ISS telescopes for electromagnetic follow-up to gravitational wave
detections, an exciting emerging astronomical field which is certain to contain
sources and surprises beyond those described here.

redpajama_set_name: RedPajamaArXiv


A mind map is a diagram used to represent words, ideas, tasks, or other items linked to and arranged around a central key word or idea. Mind maps are used to generate, visualize, structure, and classify ideas, and as an aid in study, organization, problem solving, decision making, and writing.
Click the figure below to see the Index of Mind Maps.
Machu Picchu and Yale: Peru drops six charges in suit.
The Republic of Peru has withdrawn six of the 17 charges filed against Yale in its 2008 lawsuit demanding the return of ancient Inca artifacts removed from Machu Picchu by Yale professor Hiram Bingham III between 1911 and 1915 and now housed at Yale's Peabody Museum.
Machu Picchu and Yale Controversy: Peru drops six charges in suit.


text:
Canadian TV, Computing and Home Theatre Forums > Canadian Internet, Phone, TV and Wireless Service Providers > Internet Television: Streaming Services including Netflix and Apple TV > Disney Ditches Netflix Ads
1 Post By ExDilbert
post #1 of 10 (permalink) Old 2019-10-04, 11:55 PM Thread Starter
Location: Swift Current SK
Disney Ditches Netflix Ads
https://www.theverge.com/2019/10/4/2...-fire-tv-apple
Last edited by 57; 2019-10-05 at 02:52 PM. Reason: Title
Smokin Joe is online now
post #2 of 10 (permalink) Old 2019-10-05, 01:46 PM
ExDilbert
Location: 43° N, 81.2° W
/sarcasm on/ Banning advertising for their main streaming competitor. That's very competitive of them. It's so nice to see fair and open competition in the marketplace. /sarcasm off/
ExDilbert is online now
bev fan
Netflix doesn't advertise Disney on their platform so it is just fair for Disney to do the same especially that they will become streaming competitors.
bev fan is online now
Netflix is user supported and does not sell advertising so that argument is a fallacy. It's like Disney not accepting General Motors ads and saying it's because GM does not advertise Disney on their vehicles. I'm sure a lot of people will be fooled by Disney's argument though. After all, it must be right because Disney wouldn't lie would they? See here for more insight on Disney's strategy.
No, it is more like GM advertising Chrysler vehicles which means that Disney would be shooting itself in the foot if they were to continue advertising Netflix and at the same time trying to get their own streaming service going.
Netflix makes money on advertising almost in every movie or a show.
Except that GM and Chrysler don't sell advertising, they sell vehicles. Maybe a better example would be for Disney owned companies to refuse to sell advertising to any company that sells products that compete with Disney. That would include all other theme parks, movie studios, TV companies, all actors, directors and producers that don't work for Disney, etc. It's not usually done because it would start an advertising boycott war (similar to a trade war,) kill revenue and create chaos in the industry.
Disney has effectively declared war on Netflix. It may be considered to be anti-competitive and be deemed illegal in some countries. Disney now has such size and reach that it could easily come under anti-competition rules if it decides to use that power to hurt competitors. Actions like refusing to sell advertising to competitors could also violate FCC regulations since it regulates public broadcasting. That may not happen with the current FCC administration since it's clearly in the pocket of big business but that could easily change in a few years.
Cite a few examples and prove that it benefits Netflix, not the studio that creates the show.
emmy1500 likes this.
NeilN
Location: North York
Don't know what's with the tortured analogies but I'll take "may be considered to be anti-competitive and be deemed illegal in some countries" seriously when CBS is forced to show ads for NBC programming or ESPN is forced to show ads for Fox Sports.
NeilN is online now
I see celebrities on talk shows promoting their shows airing on different networks quite often. It's not like the networks come right out and ban them. I've also seen ads for Global or CTV on the other network. Within certain legal, moral and ethical guidelines, advertising is generally available for anyone who wants to pay. Banning competitors' advertising to gain an advantage is generally not done, at least not as blatantly as the recent Disney action.
...tortured analogies...
Look into the EU's anti-competition laws some time. American companies are being slapped with multi-billion dollar fines for trying to do what they get away with in the US. Also check out United States v. Microsoft Corporation, 253 F.3d 34 some time. Using market position to hurt competitors is also illegal in the US, though not often used since. That is probably due to the difficulty and expense of prosecuting a large, powerful company such as Microsoft.
I repeat my skepticism. Guests promoting their ABC TV shows on The Tonight Show is not the same thing as ABC buying commercials on NBC. Also, I suggest you read United States v. Microsoft Corporation, 253 F.3d 34 yourself as it seems you've missed the whole basis of the lawsuit - abuse of monopoly power. Arguing that Disney has a monopoly on TV entertainment is going to get quickly tossed if that's the basis of your antitrust suit (same with the EU suits). Now, if you can provide examples of one non-monopoly service being forced to show advertising for a rival service then you may have a case.
post #10 of 10 (permalink) Old 2019-10-07, 08:25 PM
Exid0r
Premium Supporter
It's really just a drop in their ad budget bucket for Netflix, to be cut off by Disney.
Netflix spent $1.8 billion on advertising last year, including $99.2 million on U.S. TV ads, with some 13% [$12.9 million] going to Disney-owned entertainment networks.
This is the original WSJ article (much more detailed than The Verge article summary in an earlier post):
Disney Bans Netflix Ads as Streaming's Marketing Wars Intensify
Comcast's NBCUniversal has targeted to spend roughly $100 million on ads outside of its own properties to launch Peacock.
NBCUniversal is expected to spend at least double that amount on its own properties, including airing a heavy amount of promotions for Peacock on its coverage of the 2020 Olympics,
AT&T's WarnerMedia is planning to spend roughly $300 million on advertising over the next year to push HBO Max.
Hulu, which is now majority-owned by Disney, has spent heavily on promotions. It shelled out $574 million in 2010 amid a major push, and even as a more mature company last year spent $161.2 million.
Meanwhile [as of Oct. 3, 2019], Amazon Fire TV has no deal in place to carry Disney+.
Amazon Clashes With Disney Over Terms for Offering Apps in Fire TV
Though Disney+ won't have ads, the discussions with Amazon to carry it on Fire TV gave the tech giant an opportunity to revisit advertising terms for various other Disney apps. Disney won't want to have the service's distribution curtailed at the launch, and Amazon won't want to miss out on offering a service that will include classic Disney movies, a lineup of Star Wars and Marvel content, the full catalog of "The Simpsons" and more.
Exid0r is offline

redpajama_set_name: RedPajamaCommonCrawl


text:
Q: If $\frac{a(m^n-1)}{n(m-1)}+1$ divides $m^n-1$, then $(n,m,a)=(2,5,1),(2,9,3),(2,13,1)$? Let $n,m,a$ be integers such that $n\gt 1, m\geq5$ and $a>0$.
Then, is the following true?

If $\frac{a(m^n-1)}{n(m-1)}+1$ divides $m^n-1$, then $(n,m,a)=(2,5,1),(2,9,3),(2,13,1)$.

With the help of computer, the answer is non-divisible in many cases. But I cannot prove it. Do you have any idea?

A: You've already got that $n=2$ or $3$, and that for $n=2$, $m\in\{5,9,13\}$.
For $n=3$, $$\frac{m^3-1}{\frac{a(m^3-1)}{3(m-1)}+1}=k\implies (3m-3-ak)(m^2+m+1)=3k$$
where $k$ is a positive integer.
So, writing $s=3m-3-ak$ where $s$ is a positive integer to have
$$s=3m-3-a\cdot\frac{s(m^2+m+1)}{3}\implies asm^2+(as-9)m+as+3s+9=0$$
Considering the discriminant, we get
$$\small (as-9)^2-4as(as+3s+9)\ge 0\implies 27\ge as(as+18+4s)\ge as(as+22)\implies a=s=1$$
Then, the solutions of $m^2-8m+13=0$ are not integers.

redpajama_set_name: RedPajamaStackExchange


text:
India pitches for H-1B visa holders, says movement of people deepened ties
Jaishankar said the two countries have agreed to take steps to promote better understanding and awareness around among each other's stakeholders who are connected at multiple levels.
World's most powerful passports in 2019
External Affairs Minister S Jaishankar on Wednesday, December 18, pitched strongly for H-1B visa holders and reiterated the significant contribution made by the movement of persons in a fair and non-discriminatory manner to the deepening of bilateral ties between India and the United States.
Jaishankar addressed a joint news conference in Washington with the US Secretary of State Mike Pompeo.Twitter
Addressing a joint news conference in Washington, Jaishankar said that people-to-people ties have been one of the defining elements of our friendship. The US Secretary of State Mike Pompeo was also present with Defence Minister Rajnath Singh and US Secretary of Defense Mark Esper.
"We take great pride in the achievements of Indians and Indian-Americans in the United States and their contribution to American society, economy and polity," he said.
"Trade and services, including the movement of persons in a fair and non-discriminate discriminatory manner has contributed significantly to the deepening of ties," Jaishankar said.
India, US on a fair, reciprocal trade deal
Looking forward to working with the US side to nurture and sustain these ties, Jaishankar said the two countries have agreed to take steps to promote better understanding and awareness around among each other's stakeholders who are connected at multiple levels.
"We've arrived at a common intent to facilitate regular exchanges between our parliamentarians and also to provide short-term internship opportunities for aspiring entrepreneurs to through dedicated programmes," he said.
He also praised Secretary Pompeo for reiterating the US governments support to the Chhabahar project, which he said will immensely benefit Afghanistan. Referring to the ongoing negotiations on the subject of trade, he exuded confidence that they will find a balanced outcome that satisfies both sides. "India and the United States have excellent cooperation in science and technology and we have concluded and brought into effect a new agreement that facilitates science and technology cooperation," he said.
"We have also today reached an agreement on water resources between our ministry and the US geological survey for collaboration and quality assessment of the management of water," the minister said.
Mike Pompeo said that the United States and India are working on a fair and reciprocal trade deal.
"Over the last 24 months, US crude and LNG exports to India have increased by more than USD 6 billion. That is great for the United States and it is great for India as well. I am especially proud of how we are pursuing a common vision for the region with allies and partners," he said.


Aloe vera has been used for a host of purposes for at least 5,000 years. The ancient Egyptians called it the `Plant of Immortality`. Lets see how many of you can tell about the various magical properties of Aloe Vera.
Really it`s a magical plant. I was having several skin problems. But all have been cure once I started using the Aloe Vera gel of that plant. It really worked like wonder.
Drinking aloe vera juice can be a natural and easy weight loss solution. It increases your metabolic rate and reduces lipid levels which in turn can help you lose weight. Aloe vera juice also contains natural antioxidants that inhibit the spread of free radicals in your body.
Can aloevera help reducing hairfall? If yes, then please tell me how?
I am extremely overweight. Please tell me how to drink aloe vera juice?
Many Aloe vera juices of different brands are available in the market.


Short Inca Trail with GreenTracks.
A One-Day Hike with overnight in Hotel at Machu Picchu.
This hike gives one a taste of the Inca Trail without days of hiking and camping. We begin the hike from the train stop at Kilometer 104 and follow the trail for six hours to the spectacular view of Machu Picchu from Inti Punku, the Gate of the Sun. From here we descend into the world famous "Lost City." After a restful night in a hotel, we return to Machu Picchu at dawn to see the ruins in perfect morning light. In the afternoon, we return to Cusco by train.
2 days / 1 night No camping, 1 night hotel.
Departs every day, all the year except February.
you can depart any day.
- One night hotel accommodation.
- Inca Trail permit fee. $85 per person. Fee subject to change.
- Round trip train ticket to/from Ollantaytambo or Poroy as needed.
for our different Inca Trail Hikes.
We take the train from Cusco or Ollantaytambo, following the Urubamba river to Km.104 of the railroad, where we alight and cross a footbridge to begin our hike at the Inca site of Chachabamba. After a brief visit to this lovely ruin with its water channels and fountains, we start the four-hour ascent that will take us past spectacular overlooks above the great valley, then below a lovely waterfall near the delightful site of Wiñay Wayna (Forever Young). We ascend through this largest and most exquisite of the Inca Trail sites, passing its chain of ritual baths and elegantly curved terracing, and then joining the main Inca trail.
We follow it across a steep mountainside and up narrow stairways through lush, humid cloud-forest of giant ferns and broad-leaf vegetation. Suddenly we cross the stone threshold of Intipunku (Sun Gate) and encounter an unforgettable sweep of natural beauty and human artistry – a backdrop of twisting gorge and forested peaks framing the magical city of Machu Picchu.


Galveston County Commissioners have urged TxDOT to finish Grand Parkway traffic and revenue study.
Galveston County officials are calling for the Texas Department of Transportation to look at the traffic and revenue study for Segment B of the Grand Parkway.
Segment B would run from Hwy. 288 to I-45 through Brazoria and Galveston counties and through League City.
"The better transportation access we have in Brazoria County will benefit Pearland and the whole county," said Matt Buchanan, president of the Pearland Economic Development Corp.
The discussion over Grand Parkway Segment B is starting up again as the deadline for the county to decide who has primacy for the project passed in January, said Galveston County Commissioner Ken Clark, who requested the county's resolution. The governing body with primacy over the project would design, construct and operate the toll road.
Clark said he does not believe the county will be held to the original deadline because TxDOT has not completed the traffic and revenue study.
Segment B is expected to be completed before Segment C, which would connect Segment B to the rest of the existing Grand Parkway. However, this could change, TxDOT Public Information Officer Danny Perez said.
On one hand, the county and TxDOT need the population to support the project being built, which Segment B can already provide, Perez said.
"The growth is going to come, but it's a matter of prioritizing money now or later," he said.
On the other hand, it might not be as useful to build a toll segment that does not connect to the majority of the toll road, Perez said. This might make a difference in whether or not Galveston County asks for primacy, Clark said.
"TxDOT is generating some excess funds from the Grand Parkway system, and they can probably absorb lower ridership longer than the Galveston County taxpayers can," Clark said.
While Segment B would run roughly 10 miles south of Pearland, the city would benefit from the addition, Buchanan said.
"On the economic side, you will get even more growth, and a lot of that growth will be primarily residential," Buchanan said.
The Grand Parkway will lead to long-term residential growth, followed by industrial and commercial growth for the area as well, Buchanan said.
"It's quite a bit south of Pearland, but it will give our residents in the northern part of county much greater access to other areas in our region," Buchanan said.
Developers are the only supporters of these segments. We need to densify metropolitan areas, not perpetuate suburban sprawl.


text:
BuddyTV Holiday Trivia Challenge
HOW TO WIN FRIENDS AND INFLUENCE MONSTERS
GISHWHES
"Season 7, Time for a Wedding!"
Missing Misha?
SPN inspired book
The Mentalists Recap
I love when the writers get all cheeky and poke fun at industry conventions! I wonder what else they'll decide is supposed to be included in season 7.
We start with "Then" and with so much focus on Becky, I'm guessing she's the one who will marry Sam. Yeah, despite my attempts to remain unspoiled, I knew Sam was the one getting married. :(
We're in Las Vegas, with Dean talking up a hot waitress. He's actually pretty relaxed and into the flirtation, which is nice to see. But this opening talk confuses the heck out of me. Since when do they have a sacred annual pilgrimage to Vegas? It took me a long time to get into the flow of the story after that.
Dean's main problem, coaxed out of him by the waitress (stripper?), is actually pretty great. His brother is batshit nuts, but the shit's not hitting the fan. He's all reasonable and stuff, though he's worried about Sam being out camping by himself. She says "we all need to face ourselves sometime," not referring to Sam, and when we get to the end of the episode, that idea is revisited. Nice circle there. But I'll come back to that.
So Sam texts Dean to come down the street, and wear his Fed suit. Hey, I recognize this church! It was the one where Sam defeated Samhain in "It's the Great Pumpkin, Sam Winchester." Pretty sure it was also the entry to the tombs in "Houses of the Holy," too. You know you're obsessed when you recognize repurposed locations. :)
So Dean comes in packing, but Sam assures him he doesn't need the pistol. Dean asks what their pretext is (I love when they use the lingo, though I'm not sure we've heard this one since "Tall Tales"). What are they hunting, a siren?
No. Sam's in love, and he's getting married.
Enter the creepy bride, with the thickest veil this side of the Boar's Head (<---Harry Potter reference). Dean's reaction, to both Sam's announcement and to his bride, is priceless. I LOVE when Jensen gets to do comedy! Beautiful black-and-white wedding cake that explodes into the title shot. That was AWESOME. Dean's still trying to figure this out. Sam's explanation? "We met, we ate..." Ah-HA. She had to do something to him, right? A spell or potion, maybe? But despite Sam being a bit mild and oddly unquestioning, he seems fine. Very natural with Becky, who of course is thrilled beyond belief. She doesn't care about the average life span of his hookups—eyes wide open—and is even paying for the wedding. "Really?! SuperFan99?!"
Sam and Becky leave for her home in Delaware. Dean calls Bobby but has to leave a message, as Bobby's got his hands full with a nest in Oregon. I love that Bobby's presence is so strong, even when he's not on screen.
Sam and Becky pull into a restaurant parking lot. Sam says they just ate, and for a moment I think Becky must be a monster of some sort who needs lots of calories, but no, it all becomes clear when she walks in to the site of her high school reunion, with the requisite mean girl handling the planning. Becky shows off Sam, then introduces him to her friend Guy, who has an interesting reaction to Sam. I assumed on first watch that he was part of Becky's plan, and he is, but his surprise is not just that it worked, as we later find out.
"Guy's a really good friend. We met in the erotic horror section at the Novel Hovel..."
Guy's an event planner, and reunion season is very busy for him, but Becky runs after him to get some silver-clad glass bottle and makes reference to him being Wiccan. Dean drives up as they drive away. He doesn't follow, but goes inside and pulls out Dad's journal, presumably to do research (though I'd think he has that thing memorized by now) or take notes (maybe it's his own journal now). He's immediately distracted by a newspaper story about some guy's good fortune and immediate tragedy.
Sam's sitting at a lovely dinner (rotisserie chicken from the grocery store) and Becky comes out in sexy lingerie. Anyone else reminded of "Wishful Thinking" at this point? Or, like, for the full 11 minutes up to this point? But Sam gets vision-like headaches and comes painfully to reality, with no clue how he got there, and I can't help wondering why I thought he seemed so normal. Now he's really Sam, for a few crucial seconds. Becky gives him the potion, and he's back to being in "love" with her. Poor Sam.
Cut to a guy hitting balls on a baseball field, and another guy using mojo of some sort (his hand movements remind me of Castiel, but I'm thinking more like demon or witch). Baseball to the face, requisite blood splatter, ewwwww.
Dean, being supportive, brings Sam a waffle iron. Sam's a little standoffish but displays no animosity. He's just...I don't know, kind of empty? Dean brings up the job in town. Baseball guy just got called up to the majors. Becky says their first thought was crossroads demon, but there's the 10-year time frame. Dean's totally flummoxed that Sam and Becky are working the case together. He's pissed at Becky, but even when Sam says "that's my wife you're talking about," there's no heat. He's talking the talk, but there's no real emotion behind it.
Dean says people who get their dreams come true bite it pretty quick. Sam says maybe what's bothering Dean is that Sam doesn't need him anymore. Ouch. Dean leaves, and tells Bobby he doesn't want another hunter, but since Bobby's all the way across the country (sorry, Dean, he's not close to his magic South Dakota wormhole), he's going to hook Dean up with someone local.
Sam catches Becky writing in her journal (swirly "Sam loves Becky" crap) and sniffing the presumably scented ink. When he licks his thumb and rubs the ink off her nose, there is nothing romantic about it. Except to her. He's found another dream-achiever...and Becky's journal. But despite her hilarious panic, he thinks it's beautiful and hugs the book. He's so adorable!
Dean goes back to the restaurant to meet the hunter, but the burly guy he approaches first isn't who he's looking for. It's the scrawny guy in the corner (DJ Qualls!), who says, "I thought you'd be taller." Bobby told him Dean would be all surly and premenstrual working with him, but he's cool with it. So do you think he'll go the way of Tamara, a hunter never seen again, or Rufus, recurring until he dies?
Dean (in a sweater vest?!) and his new partner cross paths with Sam and Becky at the CEO's office. Dean plays hard-hitting journalist very well, while Garth cuts right to the chase and hits the guy with "nefarious means" questions about black magic and hoodoo. Between the two of them, they get that the guy didn't want the job. But his bitchy wife obviously did want it. Dean tries to get the story from her, but she blows them off.
"Why do people keep thinking I'm threatening them?"
"Because it sounded exactly like a threat, dude."
Sam's trying to work the case while Becky tweets about going on a romantic getaway. The elixir wears off again, but it leaked in Becky's purse, and she can't stop Sam from reverting.
Dean saves the CEO's wife, whose story makes it sound like a demon deal. But the timeline is whack. Garth shows his hunter chops and lays out the plan. They'll stow the wife with his cousin, a tri-racial paraplegic sniper, while they go after the demon.
Becky makes a desperation call to Guy, Sam is in pain and asks Becky what's going on, and when he says he's calling Dean, she knocks him out with a waffle iron.
Sam wakes up tied to a bed in a nice cabin.
Tied. To a bed.
Okay, I'm back. Sam's fully himself, and what a friggin' relief! Becky tests him for concussion symptoms, says he's pantsless because they're very constricting, but don't worry, she didn't do anything weird. Guy calls her back on her computer, and she wants the elixir. She says the stuff is wearing off faster and faster and whines that they haven't even consummated their marriage. Guy says to meet him in an hour, and Sam heard everything. He's pissed, while Becky is full of justification. Sam knows right away that Guy is the one killing everyone, and says Becky is on his list. Crazy woman. She refuses to untie him, stuffs a rag in his mouth, and calls "love you too!" as she runs off for more love potion.
I know she's pathetic and doing something awful here, but I really like Becky!
But it turns out Sam was right. Guy wants payment now, and reveals his red eyes. Reunions give him tons of clients, and he admits (kind of) that he's responsible for the deaths. He says he wasn't thrilled to see her new hubby was Sam Freakin' Winchester, but he'll give her a special deal. Twenty-five years—unprecedented—with Sam for her soul and her promise not to tell the Winchesters any of it.
The timeline gets a little murky for me from this point. She wants a drink, but Guy hands over the potion, then she goes back to the house and talks to Sam, then she's drinking at the end of the reunion. I think the editing could have been tidied up a little.
Dean and Garth go to Becky's apartment and find enough clues to send them to the lake house (Loon Lake, nice pun :) ). Becky is there lamenting that her plan to show off Sam—he's tall and nice, and they'd think she was happy—isn't going according to plan. She does a short rundown of her life and fondles the bottle of elixir. Sam tells her she's better than this, she says she's not so sure, and now we're back at the restaurant after the reunion. She tells Guy she's in.
Wow. I can't believe we still have 20 minutes to go. This episode was actually shorter than normal, but seemed to go on for a long time.
Becky gets close enough to the demon to seal the deal, but instead drops a lighter on a devil's trap made from blueberry vodka. Sam, Dean, and Garth show up, so apparently they made it to the lake house. Guy asks for Dean's autograph, Dean pulls out the demon-killing knife. Guy claims to be an innovator instead of a cheater, using an "intern" to arrange accidents and collect early on the souls. Intern flings all three hunters across the room. He's pretty powerful. Fights ensue, Garth gets knocked out, Sam and Dean are getting throttled, season 1 style. Becky saves Sam with a knife through the intern's torso (that knife isn't that long!) and Sam tosses it to Dean, who turns it on Guy.
Guy says "oh crap" and Dean thinks it's because of him, but then Crowley appears. Oh, crap. But Crowley isn't too happy with Guy's stupidity. The "intern" ratted him out. Crowley's pissed at the damage to their credibility.
"There's a reason we don't call our chits in early. Consumer confidence. This isn't Wall Street, this is Hell! We have a little something called integrity."
Crowley makes a deal to cancel all Guy's deals (15 of them) and take Guy from Dean. Sam's suspicious, and Crowley points out that demons have left Sam and Dean alone while they're dealing with the Leviathans.
"You met that dick, yeah? Smuggest tub of goo since Mussolini. I hate the bastards. Squash them all. Please. I'll stay clear."
His "done. and done." when he cancels the deals reminds me of Ash. *sniff*
Man, I love Crowley.
Sam, with absolutely no sympathy for Becky, gets an annulment and says she'll probably never see him again. But he does take pity and tells her she's not a loser, to just do her thing, whatever that is, and the right guy will find her. Then Garth gets all crushy on her, but Dean squashes that pretty quick.
We have the goodbye scene, when Dean tells Garth he doesn't suck. "Thank you, man. That's the nicest thing anyone's ever said to me." I like Garth. I hope we see him again.
Sam says he does need Dean watching his back, but Dean admits Sam's a grown up and doesn't need him any more.
"It's still a Denver scramble up here, I just know my way around the plate now."
Sam says it's about time Dean gets to just look out for himself, but Dean doesn't look too thrilled about that. This is where we're supposed to reflect back on the waitress (stripper?) saying he needed to face himself. Come on, Dean, you can do it. You're a helluva guy, you know.
Final verdict: This wasn't my favorite episode, but I really liked the tone and the characters, and I have a feeling this will be one of my favorites to rewatch. It's always nice to have a light episode among all the heavy, dark ones.
Labels: crossroads demons, Crowley, Episode Review, Jared Padalecki, jensen ackles, Mark Sheppard, Season 7, wishful thinking
kp said...
I liked the 'lighter' tone as well. These guys need a normal day more than anyone. (and normal for them STILL includes violent deaths and crossroads demons!) It was ...I mean...Dean and a WAFFLE IRON? LOL
I also loved the return of Becky. I kind of hate that they made her SUCH a lunatic. It would have been better if she'd grown up except for being unable to resist the temptation of having her fantasy (Sam) become real. Class reunions can make you crazy.
The lunaticness bothered me less than the "loser" part. Like Crowley saying he was sure she had a nice personality. There was a little too much of that edge, though, I agree.
good point. I almost want to say they aren't so much giving a noogie to their geeky little sister 'the fandom' as say treating her like 'Carrie'. lol
LOL Good analogy!
Kp, love the analogy! Lol
And great write-up, Nat.


Race Information: Penguin in the Park 5K Run/Walk is coming soon this spring! After his namesake, the Penguin, John Bingham, inspires us all to get out there and be active. Penguin in the Park is the largest 5K in the Decatur area. This race embraces the Penguin in all of us — a race for the speedy, and those who want to take their time and enjoy the course! This year will once again include the 300 meter "Penguin Dash" for the younger penguins that will take place before the start of the 5K at 8:30 am. This is a great opportunity to include youth in a sport and activity that is life long. Make Penguin in the Park a family activity this year. Penguin in the Park participants will receive a short sleeve t-shirt and goody bag along with a finisher ribbon/medal. Starting at 9:00am, the 5K race takes place in Fairview Park on a rolling bike path; afterwards, we move to the post-race party inside to Millikin's Griswold Gym for awards, and warm food.


I was searching for a Property and found this listing (MLS® #20191200). Please send me more information regarding 19 Elizabeth Street, Kerhonkson, NY, 12446. Thank you!
I'd like to request a showing of 19 Elizabeth Street, Kerhonkson, NY, 12446 (MLS® #20191200). Thank you!


This determination is the Goods and Services Tax: Waiver of Adjustment Note Requirement Determination 2017 - for Decreasing Adjustments from Intangible Supplies from Offshore.
This determination replaces determination A New Tax System (Goods and Services Tax) Act 1999 - Waiver of Requirement to hold an Adjustment Note for a Decreasing Adjustment Determination - F2006B11575 (previous determination), registered on 14 November 2006. The previous determination is repealed from 1 April 2017.
but for this determination, the adjustment would not be attributable to that tax period because of paragraph 29-20(3)(c) of the GST Act.
This determination is substantially the same as the previous determination that it replaces. An entity that satisfied the requirements of the previous determination will satisfy the requirements of this determination.
The requirement for an adjustment note under subsection 29-20(3) of the GST Act does not apply where the decreasing adjustment arises from an adjustment event that relates to an intangible supply from offshore that is a taxable supply under section 84-5 of the GST Act.
Expressions in this determination have the same meaning as in the GST Act.


text:
Q: Advantage of STL resize() The resize() function makes vector contain the required number of elements. If we require less elements than vector already contain, the last ones will be deleted. If we ask vector to grow, it will enlarge its size and fill the newly created elements with zeroes.
 vector<int> v(20);
 for(int i = 0; i < 20; i++) {
     v[i] = i+1;
    }
  v.resize(25);

 for(int i = 20; i < 25; i++) {
     v[i] = i*2;
   }

But if we use push_back() after resize(), it will add elements AFTER the newly allocated size, but not INTO it. In the example above the size of the resulting vector is 25, while if we use push_back() in a second loop, it would be 30.
 vector<int> v(20);
 for(int i = 0; i < 20; i++) {
     v[i] = i+1;
  }
 v.resize(25);
  for(int i = 20; i < 25; i++) {
  v.push_back(i*2);   // Writes to elements with indices [25..30), not [20..25) ! <
 }

Then where is the advantage of resize() function ? Doesn't it creates a confusion for indexing and accessing elements from the vector ?

A: It sounds as though you should be using vector::reserve.
vector::resize is used to initialize the newly created space with a given value (or just the default.) The second parameter to the function is the initialization value to use.

A: Remember the alternative - reserve. resize is used when you want to act on the vector using the [] operator -- hence you need a "empty" table of elements. resize is not intended to be used with push_back. Use reserve if you want to prepare the array for push_back.
Resize is mainly usefull if the array has  meaningful "empty" constructor, when you can create an array of empty elements, and only change the ones that are meaningful.

A: The resize() method changes the vector's size, which is not the same as the vector's capacity.
It is very important to understand the distinction between these two values:

*

*The size is the number of actual elements that the vector contains.

*The capacity is the maximum number of elements that the vector could contain without reallocating a larger chunk of memory.

A vector's capacity is always larger or equal to its size. A vector's capacity never shrinks, even when you reduce its size, with one exception: when you use swap() to exchange the contents with another vector. And as others have mentioned, you can increase a vector's capacity by calling reserve().
I think that using the correct terminology for size and capacity makes it easier to understand the C++ vector class and to speak clearly about its behavior.

A: resize() function changes the actual content of the vector by inserting or erasing elements from the vector. It does not only change its storage capacity. To direct a change only in storage capacity, use vector::reserve instead. Have a look at the vector visualization in the link, notice where v.back is pointing to.

A: I don't really understand the confusion. The advantage of resize is that it resizes your vector. Having to do a loop of push_backs is both tedious and may require more than one "actual" resize.
If you want to "resize" your vector without changing its accessible indexes then use std::vector<T>::reserve. That will change the size of the internal allocated array without actually "adding" anything.


Buy Benzodiazepines online.Benzodiazepines (BZD, BDZ, BZs), sometimes called "benzos", are a class of psychoactive drugs whose core chemical structure is the fusion of a benzene ring and a diazepine ring. The first such drug, chlordiazepoxide (Librium), was discovered accidentally by Leo Sternbach in 1955, and made available in 1960 by Hoffmann–La Roche, which, since 1963, has also marketed the benzodiazepine diazepam (Valium).In 1977 benzodiazepines were globally the most prescribed medications. They are in the family of drugs commonly known as minor tranquilizers.
Benzodiazepines are generally viewed as safe and effective for short-term use, although cognitive impairment and paradoxical effects such as aggression or behavioral disinhibition occasionally occur. A minority of people can have paradoxical reactions such as worsened agitation or panic.Benzodiazepines are also associated with increased risk of suicide.Long-term use is controversial because of concerns about decreasing effectiveness, physical dependence, withdrawal, and an increased risk of dementia.Stopping benzodiazepines often leads to improved physical and mental health. The elderly are at an increased risk of both short- and long-term adverse effects, and as a result, all benzodiazepines are listed in the Beers List of inappropriate medications for older adults. There is controversy concerning the safety of benzodiazepines in pregnancy. While they are not major teratogens, uncertainty remains as to whether they cause cleft palate in a small number of babies and whether neurobehavioural effects occur as a result of prenatal exposure; they are known to cause withdrawal symptoms in the newborn.


text:
4.13: The Rate of Collisions between Unlike Gas Molecules
[ "article:topic", "showtoc:no", "license:ccbysa", "authorname:pellgen" ]
https://chem.libretexts.org/@app/auth/3/login?returnto=https%3A%2F%2Fchem.libretexts.org%2FBookshelves%2FPhysical_and_Theoretical_Chemistry_Textbook_Maps%2FBook%253A_Thermodynamics_and_Chemical_Equilibrium_(Ellgen)%2F04%253A_The_Distribution_of_Gas_Velocities%2F4.13%253A_The_Rate_of_Collisions_between_Unlike_Gas_Molecules
Physical & Theoretical Chemistry
Book: Thermodynamics and Chemical Equilibrium (Ellgen)
4: The Distribution of Gas Velocities
Contributed by Paul Ellgen
Retired Teach (Chemistry) at Oklahoma School of Science Mathematics
We define the collision frequencycollision frequency, \({\widetilde{\nu }}_{12}\), as the number of collision per unit time between a single molecule of type 1 and any of the molecules of type 2 present in the same container. We find \({\widetilde{\nu }}_{12}=N_2\pi {\sigma }^2_{12}\left\langle v_{12}\right\rangle\). If there are \(N_1\) molecules of type 1 present in a unit volume of the gas, the total number of collisions between type 1 molecules and type 2 molecules is \(N_1\) times greater. For clarity, let us refer to the total number of such collisions, per unit volume and per unit time, as the collision rate, \({\rho }_{12}\). We have
\[{\rho }_{12}=N_1{\widetilde{\nu }}_{12}=N_1N_2\pi {\sigma }^2_{12}\left\langle v_{12}\right\rangle =N_1N_2{\sigma }^2_{12}{\left(\frac{8\pi kT}{\mu }\right)}^{1/2}\]
4.12: The Frequency of Collisions between Unlike Gas Molecules
4.14: Collisions between like Gas Molecules
Paul Ellgen
Show Page TOC
no on page
© Copyright 2022 Chemistry LibreTexts


There's nothing quite like watching athletics live - fun and excitement for all ages. Check out our events calendar for upcoming events and links to event website and tickets.
If you cannot get to the event itself, why not watch on TV? BBC TV currently cover major championships, British Athletics Indoor and Outdoor events, plus IAAF Diamond League highlights. Diamond League and IAAF world series events are usually shown live on Eurosport. Athletics is also often broadcast live on BBC Radio 5 Live.
Run England is the official England Athletics recreational running project which aims to get the whole nation running. Jogscotland is Scotland's national recreational running network.


When I was in college, my parents and little brother came to visit me in my dorm room when I was setting up my bed in my dorm room. Cushy mattress topper, high thread count sheets, fluffy comforter, just the right pillows. Little brother asked why I had all that stuff. My mom explained that I had to build my little nest. Even on a skimpy first job salary, pillows and sheets were a priority for me. You see, I have always been a master of comfort, a queen of comfy if you will, plotting out blankets and pillow arrangements and scheming about how to get things just so to maximize snugness. I still remember my first restorative yoga workshop — bolsters and blankets, total immersion in finding new ways to be comfortable, to find deeper rest. I was smitten.
Similarly, I remember the very first time that I learned how to properly set up the side lying position in massage school. I was the demo body for the class, happily bolstered by my teacher, bundled in sheets, fully supported. It was bliss. Don't get me wrong — I love a good prone/supine massage, pillow under the ankles when face down and under the knees when facing up to put some slack in the hamstrings and lower back, totally supported by the table. But there's something about side lying that feels so luxuriously cozy. I'd say it was just me and my deep appreciation for being properly bolstered, but I've heard far too many people extol the virtues of this position to be so naive.
Just look at this lady from the Body Support Systems website — velour tracksuit and proper bolstering. How psyched is she? She looks pretty cozy to me.
In my massage practice, I use side lying position for prenatal massage. Not only does this position offer maximum safety and comfort, minimizing strain on uterine ligaments and the body as a whole, it is also a fabulous position to massage the lower back and hips, both of which are taxed and oft-complained-about during pregnancy. There are a number of reasons why side lying position is great for pregnant clients, but what speaks to me the loudest (and in a real, human voice to boot!) are the women who have struggled to get comfortable during pregnancy, tossing and turning at night, pillows not quite right, who have told me that being bolstered for massage is the most comfortable they have been in months. Can't beat that!
This position can obviously be used for anyone — pregnant or not — who wants to try it out. Please let me know before your session if you'd like to give it a whirl so I can make sure to get set up for you. And, even though I use the fancy pants massage cushions shown above, I will happily discuss how to replicate supported side lying position with regular pillows so that you, too, can be a queen or king of comfy in your own home.
I agree sideline is extremely comfortable with the body cushions. Do you use the cushions for prone prenatal massage, too? Is this an issue in New York?
Hi Becky! I use the cushions for prone prenatal massage in the early weeks of pregnancy for women who love lying on their bellies and want to squeeze in as many opportunities to do so as they can. I have heard of massage therapists in New York who bolster in prone throughout pregnancy, but I am on board with the reasoning laid out by Carol Osborne Sheets in the article linked to in my post, and I follow those guidelines.
Thank you for your response. I'm familiar with Carol's training, I've been certified. I do not follow her recommendations. I learned prone pre natal in massage school (pre Carol Osborne Sheets making a name for herself) and I still practice prone today as long as the client is comfortable with it. I absolutely disagree with a few of her points on the link (but thank you for sharing it). Our liability insurance covers with both methods: prone and sideline. If it was a risk to mother or baby they would drop the coverage in a heart beat. I was hoping to have some conversations on the benefits to prone vs. sideline. Keep up the good work. Love your blog and articles.
I should have said that, in addition to people I know of who bolster throughout pregnancy, there are definitely spas that have the tables with the belly hole for prone positioning. It's definitely done, just not by me. To be clear, when clients have asked about prone positioning later in pregnancy, I explain that I use side lying (and why), but I always, always, always am honest about the fact that there are people who do it differently. Maybe not the level of discussion you were looking for, but you've inspired me to do some more thinking/reading refreshment, and I would love to hear more if there's more you want to say on this topic (or if you have counter-to-what-I've-learned resources to recommend). Thanks for reading and engaging!
Prone is an interesting discussion. I don't tend to use it much after the first trimester, but it depends on what you are doing with the client, types of techniques and how long you use it for so I don't consider it is absolutely contra indicated. I discuss it in more detail also in my book Pregnancy and Childbirth. I am a big fan of side lying but also in third trimester forward leaning as this way gives much better positioning for deeper access to sacrum and helps with baby's position too!
I don't consider it absolutely contraindicated either. Thanks for sharing, and for sharing your info — I'm always interested in hearing about different ways that people work.
This makes me want to get pregnant right away so I can be uncomfortable again and then made more comfortable by you!
Ha! Do it! I will do my part to keep you comfy.


The lightest, thinnest model is very sensitive, with fast, bright and glassy sounds.
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Vanderbilt and UNLV will play a home-and-home football series in 2019 and 2023, the Commodores' sports information department announced Wednesday.
The 2019 contest will take place in Vanderbilt Stadium (Oct. 12), with the return visit to Las Vegas on September 16, 2023.
UNLV's Director of Athletics Desiree Reed-Francois confirmed the dates in a separate release.
UNLV also announced its 2019 home opener will be contested against Southern Utah in that release. That outing is slated for August 31, 2019.
UNLV and Vanderbilt have never faced off on the gridiron.
I truly have to believe if UNLV was not located in Las Vegas that Vandy would not a be hosting a home in home. Because Vegas is still continuing to grow & getting an NFL team as well, why not take the boys out to Vegas & show them a good time, city is beautiful place lit up at night.
Agreed….UNLV has nice history of getting bigger schools to travel there…..UNLV might be ready to seize Nevada as Boise did Idaho…..
UNLV should be in that sparkly new stadium by that home date.
Unfortunately, UNLV cannot attract more than 15,000-20,000 fans to a home game. The stadium will feel like a tomb if they don't get their act together.
I believe that UNLV will be better in the future.


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redpajama_set_name: RedPajamaGithub


text:
Sir Roger Bentham Stevens, GCMG (8 June 1906 – 20 February 1980) was a British academic, diplomat and civil servant.

Life
Stevens was born 8 June 1906. He was educated at Wellington College and Queen's College, Oxford. He married his first wife, Constance Hallam Hipwell (died 1976), in 1931, and they later had a son, Bryan Constant Sebastian Bentham Stevens.  His second wife was Jane Chandler (née Irving), whom he married in 1977.  He died on 20 February 1980, and she deposited his papers in the Churchill Archives, University of Cambridge in 1984.

Diplomatic career
In 1928 Stevens entered the UK Consular Service, serving in Buenos Aires, New York City, Antwerp, Denver, and the Foreign Office in London.

In 1951 he was appointed British Ambassador to Sweden, then in 1954, British Ambassador to Persia.  He wrote two books on Persia, The Land of the Great Sophy (1962) and First View of Persia (1964), and continued to contribute to academic journals on the same subject in later life. In 1958 he returned to London as Deputy Under-Secretary of State, Foreign Office, until 1963.

Other activities
In 1963 he took up the position of Vice-Chancellor of the University of Leeds which he held until 1970. Other positions were:
Advisor to First Secretary of State on Central Africa, 1963–1970
Chairman of Yorkshire and Humberside Economic Planning Council, 1965–1970,
Panel of Inquiry into Greater London Development Plan member, 1970–1972,
Chairman of the Committee on Mineral Planning Control, 1972–1974,
United Nations Administrative Tribunal (UNAT) member, 1972–1977.

Honours

Stevens was a KCMG and later GCMG.
He is commemorated in the Roger Stevens Building on the campus of Leeds University.

References

D. Wright (1981) Iran, Vol. 19, pp. iii–iv Sir Roger Stevens, G.C.M.G.

1906 births
1980 deaths
People educated at Wellington College, Berkshire
Alumni of The Queen's College, Oxford
Vice-Chancellors of the University of Leeds
Knights Grand Cross of the Order of St Michael and St George
Ambassadors of the United Kingdom to Iran
Ambassadors of the United Kingdom to Sweden
British expatriates in Argentina
British expatriates in the United States
British expatriates in Belgium

redpajama_set_name: RedPajamaWikipedia


The pace of change in the cloud can be overwhelming. That's why we took the time on January 10th to help educate Office 365 customers. During our hour long webinar, we detailed some of the lesser-known and unheralded Office 365 features that can provide significant value to Microsoft customers. The most important part about this: in most cases, you already own the licensing. This webinar was all about helping you to leverage the technology investments that you've made.
If you weren't able to join us on January 10th, it's your lucky day. In this blog post, I'll recap some of the features that we covered. As a side note, we ran a couple of webinars of this same title back in early 2016. About half of the features discussed and shown last week were new to our presentation.
As mentioned above, this webinar was all about educating Office 365 customers about the lesser-known components of Office 365–the components that customers already own, but don't fully understand yet. I am not a Microsoft licensing junkie and I will only discuss licensing to the extent that this webinar recap requires. I have that narrowed down to two sentences. Every feature discussed is available in E3 and E5 licensing plans. Some, but not all of the features are available in Small Business and E1 plans. If you need more specifics, I'm happy to answer questions in a follow up conversation.
For the presentation, I divided these untapped features into two categories: Productivity and Security/Compliance. The first set of features that I will discuss fall under the Productivity category. These are the features that Microsoft added to help your users work smarter, collaborate more efficiently, and, generally, just get stuff done faster. The next set of features that I will discuss are the Security/Compliance features. These are the features that help to secure your organization's sensitive data and to meet industry or vendor compliance policies.
Office 365 Groups – A collaboration platform that Microsoft introduced to help employees work together outside of normal organizational silos. Groups includes shared calendars, email, a conversation feed, a notebook, and files. As opposed to traditional workspaces, Groups is based around the idea of end-user driven collaboration.
Microsoft Teams – Teams is the most recent edition to Microsoft's collaboration toolset. Building on the strengths of Groups (and including some integration), Teams emphasizes chat-based collaboration and integration with third-party tools like ZenDesk, Google Analytics, Constant Contact, and more.
Office 365 Planner – Planner is another feature that is based on the premise of Groups. Planner is a light-weight project planning platform that includes task creation, assignment, and process tracking. Integration with Teams and Groups adds more value to both platforms.
Azure Active Directory – Some of you may be familiar with Microsoft's Azure AD Premium offering as part of their Enterprise Mobility + Security Suite, but many don't know that they have a lighter-weight version available with your Office 365 subscription. Azure AD allows you configure Single-Sign On to third party cloud applications like Salesforce, Dropbox, Box, and 2,700 others. This saves your users from having to remember multiple sets of credentials and reduces the chance that they will continue poor security habits (like writing down their passwords). Advanced features like universal Multi-Factor Authentication and Self-Service Password Reset are available in the premium offering.
SharePoint Workflows – Many people know SharePoint as a document management system – which it does a good job of. However, the openness of the SharePoint platform often abstracts some of its strong process-based features. SharePoint Workflows can help to automate processes and increase efficiency. To help make the value of this more concrete, we've developed an out-of-the-box solution with pre-built workflows for HR departments. Ask your account manager or email info@peters.com for more information.
Data Loss Prevention – Data Loss Prevention is a compliance tool that is built into Exchange Online, SharePoint Online, and OneDrive for Business. It is a tool designed to prevent sensitive information from going to the wrong place. Sensitive information could be credit card information, social security numbers, other compliance standards, and any custom identifiers that you choose. This compliance engine scans documents and email to identify sensitive information and allows you to determine how it should be dealt with.
Message Encryption – Exchange Online Message Encryption is an email encryption solution that can be applied to emails based on Data Loss Prevention policies or other mail flow rules. This is a great tool for protecting sensitive information or allowing employees to encrypt any email that they choose. Authorized recipients inside and outside your organization can view the email contents securely.
Information Protection – Information Protection is a step beyond message encryption. Information Protection is document and email-level security. It allows for rules and actions that can take place on a particular document or email – prevent editing, prevent printing, prevent save as, prevent forwarding, etc. This can be applied to email, SharePoint, and OneDrive for Business. Microsoft also has a premium offering that extends this functionality to on-premises file servers.
Multi-Factor Authentication – Originally introduced for administrator accounts only, Multi-Factor Authentication in Office 365 has been extended to all users. Requiring a 2nd factor of authentication (like a mobile device code or phone call) can greatly increase the security of your environment. This is an especially important feature for administrator accounts.
Mobile Device Management – Mobile Device Management has become an increasingly important technology as organizations expand their Bring Your Own Device policies. Microsoft has built Mobile Device Management into Office 365 – allowing administrators to require passwords, force encryption, provision corporate email, and selectively wipe corporate data on devices. This is a subset of the features provided with Microsoft's Intune solution – but still a substantial offering for basic Mobile Device Management Needs.
This is just a subset of the features that Microsoft adds and enhances in Office 365 on a regular basis. As I mentioned at the outset, this forum doesn't allow me to dig deep in this particular post. We will have future posts that discuss some of these features at a deeper level but if you'd like to learn more, contact us and we can talk through your Office 365 strategy.
Be on the lookout in the next couple of weeks for blog posts and webinars that explore Peters' HRPortal solution, Microsoft Teams, and basic Office 365 collaboration strategy. In the meantime, email us at info@peters.com to discuss how your organization can get more out of Office 365.


After his debut film Strictly Ballroom (1992), writer/director Baz Luhrmann never looked back, creating lavish, ultra-stylish musicals William Shakespeare's Romeo + Juliet (1996) and Moulin Rouge! (2001), and let's not forget that $5 million Chanel commercial starring his cinematic muse, Nicole Kidman. With, Australia (2008), he decided to take national pride to a whole new level by creating a sweeping romantic epic about his home country that takes place between the World Wars and was made by and starring Australians. With a budget in the neighborhood of $130 million, the pressure was on Luhrmann now more than ever before to deliver at the box office and, while underperforming in North America, it went on to gross $200 million worldwide despite a lukewarm critical response.
Lady Sarah Ashley (Kidman) is a headstrong English aristocrat who travels to Northern Australia in 1939 to meet her husband at their ranch Faraway Downs. Within a few minutes of arriving, she meets her guide to this strange new land, a man known as the Drover (Hugh Jackman), a hard-drinking, two-fisted Australian version of a cowboy. They take an instant dislike to each other: she thinks that he's crude and uncultured and he thinks that she's too prim and proper.
They arrive at Faraway Downs to find her husband dead (apparently at the hands of an Aboriginal) and the ranch in disarray and in danger of being foreclosed. Mr. Carney (Bryan Brown), the local tycoon with a monopoly on the local economy, has his right-hand man, Mr. Fletcher (David Wenham) try to sabotage Lady Ashley. In order to save Faraway Downs, she has to drive 1,500 head of cattle to Darwin and so she enlists the help of the Drover. Along the way, they befriend a young Aboriginal boy named Nullah (Brandon Walters) whom she protects from being taken away and forced to assimilate with white folks.
As with his previous films, Luhrmann populates Australia with broad, stereotypical characters and tells a classic story. The film revels in archetypes: Ashley is a pure, upstanding woman, the Drover is the rugged western hero, Fletcher is the dastardly villain, and Nullah is the adorable child who narrates the story. As he proved with is previous films, Luhrmann has an uncanny knack for casting. Who can forget the undeniable chemistry between Leonardo DiCaprio and Claire Danes in Romeo + Juliet and the sparks that flew between Ewan McGregor and Nicole Kidman in Moulin Rouge!? He's at it again with this film with the casting of Hugh Jackman and Kidman as the romantic leads.
Jackman finally fulfills those early comparisons to Clint Eastwood, playing the Drover as a tough, dependable hero who's not afraid to show his vulnerable side. He's never been more charismatic as he proves to be equally adept at the physical demands and the emotional range that the role requires. No one knows how to photograph Kidman quite like Luhrmann. She looks stunning, even covered in a layer of dirt and dust from a cattle drive. At first, her stuffy English aristocrat comes off as a cartoonish stereotype but as her character becomes acclimatized to the country and she develops a bond with Nullah, she becomes warmer and more empathetic.
Beginning in 1939 and climaxing with the Japanese bombing of Darwin in 1942, Luhrmann's Australia mixes the larger-than-life melodrama of Gone with the Wind (1939) with the exciting cattle drive in Red River (1948) and with a dash of The Wizard of Oz (1939). His film clearly harkens back to the kind of cinema that they just don't make any more with very little CGI used and everything built from scratch and on location. Australia is the kind of ambitious Technicolor epic that might have been made by John Ford or George Stevens. It is a marvel of absolutely stunning cinematography – only Luhrmann could make the desolate outback look vibrant and alive. He alternates between sun-drenched day scenes and night scenes that appear to be impossibly illuminated by the stars.
One should not go into Australia expecting realism. Luhrmann presents a mythologized take on his country. Love him or hate him, you have to respect Luhrmann for not being afraid to wear his heart on his sleeve. He's arguably the most romantic filmmaker working today with the possible exception of Wong Kar-Wai. And with Australia, he has made an unabashed love letter to his homeland on a grand scale.


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1. Prominently display the DPRM banner/streamer within their office premises. The attached file provides the design and specifications. The banner template may be accessed at this link: http://bit.ly/dprm2018. They are free to choose between the English version and the Filipino version depending on their office's/locality's language preference. For inquiries regarding the banner, they may contact Ms. Gizelle Manuel at gmanuel@mail.pids.gov.ph.
2. Repost and share DPRM infographics, promotional videos, and other related announcements on the website and social media accounts of both central and regional offices. (Note: Kindly download the infographics and promotional videos on the DPRM website (http://dprm.pids.gov.ph) and PIDS social media (https://www.facebook.com/PIDS.PH/ and https://twitter.com/PIDS_PH).
Click here to view the DILG Memorandum Circular.