text:
\section{Introduction}
\label{s:introduction}

In 2015 September, the Advanced Laser Interferometer Gravitational-wave Observatory (\acsu{LIGO}; \citealt{aLIGO}) made the first direct detection of an astrophysical gravitational-wave (\acsu{GW}) signal that turned out to be from a \ac{BBH} merger.
The LIGO Hanford and Livingston sites are the first two nodes of a growing global network of highly sensitive \ac{GW} facilities, soon to include Advanced Virgo \citep{AdVirgo}, KAGRA, and LIGO\nobreakdashes--India.
Some of the most promising astrophysical sources of \acp{GW} are also expected to produce broadband \ac{EM} emission and neutrinos.
This has created exciting new opportunities for joint broadband \ac{EM} observations and multi-messenger astronomy.

In a \ac{CBC} event, a tight binary comprised of two \acp{NS}, two \acp{BH}, or a \ac{NS} and a \ac{BH} experiences a runaway orbital decay due to gravitational radiation.
In a binary including at least one \ac{NS}---
a \ac{BNS} or \ac{NSBH} merger---we expect \ac{EM} signatures due to energetic outflows at different timescales and wavelengths.
If a relativistic jet forms, we may observe a prompt short \ac{GRB} lasting on the order of one second or less, followed by X\nobreakdashes-ray, optical, and radio afterglows of hours to days duration (e.g., \citealt{Eichler:1989,Narayan:1992,Nakar:2007,Berger:2014,Fong:2015}).
Rapid neutron capture in the sub-relativistic ejecta (e.g., \citealt{Lattimer:1976}) is hypothesized to produce a \acl{KN} or macronova, an optical and near-infrared signal lasting hours to weeks (e.g., \citealt{LP98}).
Eventually, we may observe a radio blast wave from this sub\nobreakdashes-relativistic outflow, detectable for months to years (e.g., \citealt{np11}).
Furthermore, several seconds prior to or tens of minutes after merger, we may see a coherent radio burst lasting milliseconds (e.g., \citealt{Hansen:2001,Zhang:2014}).
In short, a \ac{NS} binary can produce \ac{EM} radiation over a wide range of wavelengths and time scales.
On the other hand, in the case of a stellar-mass \ac{BBH}, the current consensus is that no significant \ac{EM} counterpart emission is expected except for those in highly improbable environments pervaded by large ambient magnetic fields or baryon densities.

The first campaign to find \ac{EM} counterparts triggered by low-latency \ac{GW} event candidates was carried out with the initial LIGO and Virgo detectors and several \ac{EM} astronomy facilities in 2009 and 2010 \citep{S6lowlatencyCBC,S6EMmethods,S6Swift,S6opticalEM}.
In preparing for Advanced detector operations, the LIGO and Virgo collaborations worked with the broader astronomy community to set up an evolved and greatly expanded \ac{EM} follow-up program.\footnote{See program description and participation information at \url{http://www.ligo.org/scientists/GWEMalerts.php}.}
\FIXME{Seventy-four} groups with access to ground- and space-based facilities joined, of which \FIXME{63} were operational during \ac{O1}.
Details of the 2009 to 2010 \ac{EM} follow campaign and changes for O1 are given in Section~1 of the Supplement \citep{GW150914-EMFOLLOW-SUPPLEMENT}.

After years of construction and commissioning, the Advanced LIGO detectors at Livingston, Louisiana, and Hanford, Washington, began observing in 2015 September with about $3.5$ times the distance reach ($>40$ times the sensitive volume) of the earlier detectors.
A strong \ac{GW} event was identified shortly after the pre-run calibration process was completed. Deep analysis of this event, initially called G184098 and later given the name GW150914, is presented in \citet{GW150914-DETECTION} and companion papers referenced therein.
In this paper we describe the initial low-latency analysis and event candidate selection (Section~\ref{s:detection}), the rapid determination of likely sky localization (Section~\ref{s:skymaps}), and the follow-up \ac{EM} observations carried out by partner facilities (Sections~\ref{s:emfollow}~and~\ref{s:limits}).
For analyses of those observations, we refer the reader to the now-public \ac{GCN}~circulars\footnote{All circulars related to GW150914 are collected at \url{http://gcn.gsfc.nasa.gov/other/GW150914.gcn3}}
and to a number of recent papers.
We end with a brief discussion of \ac{EM} counterpart detection prospects for future events.

\section{Data Analysis and Discovery}
\label{s:detection}

As configured for \ac{O1}, four low-latency pipelines continually search for transient signals that are coincident in the two detectors within the $10$\,ms light travel time separating them.
\acl{cWB} (\acsu{cWB}; \citealt{cWB-overview}) and \acl{oLIB} (\acsu{oLIB}; \citealt{oLIB}) both search for unmodeled \ac{GW} bursts \citep{GW150914-BURST}. GSTLAL \citep{LLOID,GW150914-GSTLAL}
and \acl{MBTA} (\acsu{MBTA};~\citealt{MBTA}) search specifically for \ac{NS} binary mergers using matched filtering.
Because \ac{CBC} waveforms can be precisely computed from general relativity, GSTLAL and \ac{MBTA} are more sensitive to \ac{CBC} signals than the burst search pipelines are.
All four detection pipelines report candidates within a few minutes of data acquisition.

LIGO conducted a series of engineering runs throughout Advanced LIGO's construction and commissioning to prepare to collect and analyze data in a stable configuration.
The \ac{ER8} began on 2015~August~17 at 15:00 and critical software was frozen by August 30.\footnote{All dates and times are in UT.}
The rest of \ac{ER8} was to be used to calibrate the detectors, to carry out diagnostic studies, to practice maintaining a high coincident duty cycle, and to train and tune the data analysis pipelines.
Calibration was complete by September~12 and \ac{O1} was scheduled to begin on September~18.
On {\OBSEVENTDATE}, \ac{cWB} reported a burst candidate to have occurred at {\OBSEVENTTIME} with a network \ac{SNR} of 23.45 and an estimated \ac{FAR} $< 0.371$ yr$^{-1}$ based on the available (limited at that time) data statistics.
Also, \ac{oLIB} reported a candidate with consistent timing and \ac{SNR}.
No candidates were reported at this time by the low-latency GSTLAL and \ac{MBTA} pipelines, ruling out a \ac{BNS} or \ac{NSBH} merger.

Although the candidate occurred before \ac{O1} officially began, the LIGO and Virgo collaborations decided to send an alert to partner facilites because the preliminary \ac{FAR} estimate satisfied our planned alert threshold of 1\,month$^{-1}$.
Although we had not planned to disseminate real-time \ac{GCN} notices before the formal start of \ac{O1}, most of the computing infrastructure was in place.
Basic data quality checks were done within hours of GW150914; both interferometers were stable and the data stream was free of artifacts \citep{GW150914-DETCHAR}.
A \ac{cWB} sky map was available 17 minutes after the data were recorded, and a \ac{LIB} sky map was available after 14\,hr.
After extra data integrity checks and an update to the \ac{GCN} server software, these two sky maps were communicated to observing partners in a \ac{GCN} circular nearly two days after the event occurred (GCN~\citegcn{18330}).
Mass estimates were not released in this initial circular, and observers may have assumed the event was associated with a \ac{BNS} system or a \ac{GW} burst (e.g., from a nearby core-collapse \acl{SN}; \acsu{SN}).
The knowledge that GW150914 was consistent with a \ac{BBH} inspiral and merger was only shared later on October~3 (GCN~\citegcn{18388}).
\begin{figure*}
    \includegraphics[width=\textwidth]{timeline}
    \caption{\label{fig:timeline}
        Timeline of observations of GW150914, separated by band and relative to the time of the \ac{GW} trigger.
        The top row shows \ac{GW} information releases.
        The bottom four rows show high-energy, optical, near-infrared, and radio observations, respectively. Optical spectroscopy and narrow-field radio observations are indicated with darker tick marks and boldface text.
        Table~\ref{table:footprints} reports more detailed information on the times of observations made with each instrument.
    }
\end{figure*}
Figure~\ref{fig:timeline} shows the chronology of the \ac{GW} detection alerts and follow-up observations.

The data were re-analyzed offline with two independent matched-filter searches using a template bank that includes both \ac{NS} binary and \ac{BBH} mergers.
The waveform was confirmed to be consistent with a \ac{BBH} merger and this information was shared with observers about three weeks after the event (GCN~\citegcn{18388}).
The \ac{FAR} was evaluated with the data collected through 20 October, reported to be less than 1 in 100 years (GCN~\citegcn{18851}; \citealt{GW150914-CBC}), and ultimately determined to be much lower.
The final results of the offline search are reported in \citet{GW150914-DETECTION}.

\section{Sky Maps}
\label{s:skymaps}

We produce and disseminate probability sky maps using a sequence of algorithms with increasing accuracy and computational cost.
Here, we compare four location estimates: the prompt \ac{cWB} and \ac{LIB} localizations that were initially shared with observing partners plus the rapid \ac{BAYESTAR} localization and the final localization from LALInference.
All four are shown in Fig.~\ref{fig:contours}.

\begin{figure*}[t]
    \includegraphics[width=\textwidth]{contours}
    \caption{\label{fig:contours}
        Comparison of different \ac{GW} sky maps, showing the 90\% credible level contours for each algorithm.
        This is an orthographic projection centered on the centroid of the \ac{LIB} localization.
        The inset shows the distribution of the polar angle $\theta_\mathrm{HL}$ (equivalently, the arrival time difference $\Delta t_\mathrm{HL}$).
    }
\end{figure*}

\ac{cWB} performs a constrained \acl{ML} estimate of the reconstructed signal on a sky grid \citep{cWB-overview} weighted by the detectors' antenna patterns \citep{BF2Y} and makes minimal assumptions about the waveform morphology.
With two detectors, this amounts to restricting the signal to only one of two orthogonal \ac{GW} polarizations throughout most of the sky. \ac{LIB} performs Bayesian inference assuming the signal is a sinusoidally modulated Gaussian \citep{oLIB}.
While this assumption may not perfectly match the data, it is flexible enough to produce reliable localizations for a wide variety of waveforms, including \ac{BBH} \acl{IMR} signals \citep{BF2Y}.
\acs{BAYESTAR} produces sky maps by triangulating the times, amplitudes, and phases on arrival supplied by all the \ac{CBC} pipelines \citep{BAYESTAR}. \acs{BAYESTAR} was not available promptly because the low-latency \ac{CBC} searches were not configured for \acp{BBH}; the localization presented here is derived from the offline \ac{CBC} search.
LALInference performs full forward modeling of the data using a parameterized \ac{CBC} waveform which allows for \ac{BH} spins and detector calibration uncertainties \citep{LALInference}.
It is the most accurate method for CBC signals but takes the most time due to the high dimensionality.
We present the same LALInference map as \citet{GW150914-PARAMESTIM}, with a spline interpolation procedure to include the potential effects of calibration uncertainties.
The \ac{BAYESTAR} and LALInference maps were shared with observers on 2016~January~13 (GCN~\citegcn{18858}), at the conclusion of the \ac{O1} run.
Since GW150914 is a \ac{CBC} event, we consider the LALInference map to be the most accurate, authoritative, and \textit{final} localization for this event.
This map has a 90\% credible region with area 630 deg$^2$.

All of the sky maps agree qualitatively, favoring a broad, long section of arc in the southern hemisphere and to a lesser extent a shorter section of nearly the same arc near the equator.
While the majority of \ac{LIB}'s probability is concentrated in the southern hemisphere, a non-trivial fraction of the 90\% confidence region extends into the northern hemisphere.
The LALInference sky map shows much less support in the northern hemisphere which is likely associated with the stronger constraints available with full \ac{CBC} waveforms.
The \ac{cWB} localization also supports an isolated hot spot near $\alpha \sim 9^\mathrm{h}, \delta \sim 5\arcdeg$,
where the detector responses make it possible to independently measure two polarization components.
In this region, cWB considers signals not constrained to have the elliptical polarization expected from a compact binary merger.

Quantitative comparisons of the four sky maps can be found in section 2 of the Supplement \citep{GW150914-EMFOLLOW-SUPPLEMENT}.
The main feature in all of the maps is an annulus with polar angle $\theta_\mathrm{HL}$ determined by the arrival time difference $\Delta t_\mathrm{HL}$ between the two detectors.
However, refinements are possible due to phase as well as amplitude consistency and the mildly directional antenna patterns of the LIGO detectors \citep{Kasliwal:2014,F2Y}.
In particular, the detectors' antenna patterns dominate the modulation around the ring for un-modeled reconstructions through a correlation with the inferred distance of the source \citep{BF2Y}.
As shown in Fig.~\ref{fig:contours}, the algorithms all infer polar angles that are consistent at the $1\sigma$ level.

\section{Follow-up Observations}
\label{s:emfollow}

\begin{figure*}[t!]
    \includegraphics[width=\textwidth]{tiles}
    \caption{\label{fig:tiles}
        Footprints of observations in comparison with the 50\% and 90\% credible levels of the initially distributed \ac{GW} localization maps.
        Radio fields are shaded in red, optical/infrared fields are in green, and the \ac{XRT} fields are indicated by the blue circles.
        The all-sky \emph{Fermi} \ac{GBM}, \ac{LAT}, \emph{INTEGRAL} SPI\nobreakdashes-ACS, and MAXI observations are not shown.
        Where fields overlap, the shading is darker.
        The initial \ac{cWB} localization is shown as thin black contour lines and the \ac{LIB} localization as thick black lines.
        The inset highlights the \emph{Swift} observations consisting of a hexagonal grid and a selection of the \emph{a posteriori} most highly ranked galaxies.
        The \citet{SFDReddeningMap} reddening map is shown in the background to represent the Galactic plane.
        The projection is the same as in Fig.~\ref{fig:contours}.
    }
\end{figure*}

\FIXME{Twenty-five} participating teams of observers responded to the \ac{GW} alert to mobilize satellites and ground-based telescopes spanning 19 orders of magnitude in \ac{EM} wavelength.
Observations and archival analysis started shortly after the candidate was announced, two days after the event was recorded.
Most facilities followed tiling strategies based on the \ac{cWB} and \ac{LIB} sky maps.
Some groups, considering the possibility of a \ac{NS} merger or core-collapse \ac{SN}, selected fields based on the areal density of nearby galaxies or targeted the \ac{LMC} (e.g., \citealt{GW150914_DES_1}).
Had the \ac{BBH} nature of the signal been promptly available, most groups would not have favored local galaxies because \acs{LIGO}'s range for \ac{BBH} mergers is many times larger than that for \acp{BNS}.
Fig.~\ref{fig:tiles} displays the footprints of all reported observations. The campaign is summarized in Table~\ref{table:footprints} in terms of instruments, depth, time, and sky coverage. Some optical candidate counterparts were followed up spectroscopically and in the radio band as summarized in Table~\ref{table:followup}. The overall \ac{EM} follow-up  of GW150914 consisting of broad-band tiled observations and observations to characterize candidate counterparts are described in detail in Sections~3 through~5 of the Supplement \citep{GW150914-EMFOLLOW-SUPPLEMENT}.

Findings from these follow-up observations have been reported in several papers.
A weak transient signal was found in \emph{Fermi} GBM data 0.4\,s after the time of GW150914 \citep{GW150914_GBM}, but no corresponding signal was found in the \emph{INTEGRAL} SPI\nobreakdashes--ACS instrument \citep{GW150914_INTEGRAL} or \emph{AGILE} \citep{GW150914_AGILE}.
No GRB-like afterglow was found in X-rays with \emph{Swift} XRT \citep{GW150914_Swift} or MAXI (N.~Kawai~et~al., in preparation), in UV/optical with \emph{Swift} UVOT \citep{GW150914_Swift}, or at GeV energies with \emph{Fermi} LAT \citep{GW150914_LAT}.
Tiled observations with wide-field optical instruments listed in Table~\ref{table:footprints} found many transients, but spectroscopy with the instruments listed in Table~\ref{table:followup} along with further photometry showed that none of them were associated with GW150914 \citep{GW150914_iPTF,GW150914_pan_STARRPESSTO,GW150914_DES_2,GW150914_JGEM}.
\citet{GW150914_DES_1} used DECam to search for a missing supergiant in the \ac{LMC}, which would have been evidence for the collapse of a massive star that could have produced \acp{GW}, but failed to produce a typical core-collapse \ac{SN}.

\section{Coverage}
\label{s:limits}

Using the \ac{GW} data alone, we can only constrain the position of the source on the sky to an area of $\approx$600\,deg$^2$ (90\% confidence).  The inferred redshift is $z = \REDSHIFTCOMPACT$, corresponding to a luminosity distance of \DISTANCECOMPACT\,Mpc \citep{GW150914-PARAMESTIM}.

Table~\ref{table:footprints} lists the area tiled by each facility and the probability contained within those tiles, calculated with respect to the localization methods described in Section~\ref{s:skymaps}.

By far the most complete coverage of the area is at the highest energies.
The \emph{INTEGRAL} SPI\nobreakdashes--ACS provided the largest effective area in the 75\,keV\nobreakdashes--1\,MeV range, albeit with significantly varying detection efficiency. Owing to its nearly omnidirectional response, it had a full coverage of the GW probability map (GCN~\citegcn{18354}; \citealt{GW150914_INTEGRAL}). \emph{Fermi} \ac{GBM} captured 75\% of the localization at the time of the \ac{GW} trigger and the entire area by 25 minutes after (GCN~\citegcn{18339}). \emph{Fermi} LAT observations started 4200\,s after the trigger and the entire localization continued to be observed every three hours.

Coverage in X\nobreakdashes-rays is complete down to 10$^{-9}$\,erg\,cm$^{-2}$\,s$^{-1}$ with the MAXI observations, but
relatively sparse at fainter flux, with the \emph{Swift} \ac{XRT} tiles spanning about 5\,deg$^2$ and enclosing a probability of \FIXME{$\sim$0.3\%} in the energy range 0.3\nobreakdashes--10\,keV to a depth of 10$^{-13}$\nobreakdashes--10$^{-11}$\,erg\,cm$^{-2}$\,s$^{-1}$ (GCNs~\citegcn{18331}, \citegcn{18346}).

Optical facilities together tiled about \FIXME{900}\,deg$^2$ and captured a containment probability of over \FIXME{50\%} of the initial \ac{LIB} sky map and slightly less for the final LALInference sky map that was available after the observations were completed.
The depth varies widely among these facilities.
MASTER and Pan\nobreakdashes-STARRS1 covered the most area with their observations, while large areas also were covered by the \ac{IPTF}, \ac{DECAM}, \acl{VST} (\acsu{VST}; E. Brocato et al. 2016, in preparation), and La~Silla--QUEST.
The contained probability of the initial sky maps is dominated by MASTER, \ac{DECAM}, Pan\nobreakdashes-STARRS1, La~Silla--QUEST, and \ac{VST}, while the final sky map is contained best by MASTER, \ac{DECAM} and \ac{VST}.
Relatively small area and contained probability were covered by facilities that targeted nearby galaxies. The only wide-field near-infrared facility, the \ac{VISTA}, covered \FIXME{70}\,deg$^2$ and captured a containment probability of \FIXME{8\%} of the final LALInference sky map.

The radio coverage is also extensive, with a contained probability of \FIXME{86\%}, dominated by \ac{MWA} in the 118\,MHz band (GCN~\citegcn{18345}).

Table~\ref{table:followup} lists the observations done by large telescope spectrographs  and a radio facility to follow-up candidate optical counterparts.
Deep photometry, broadband observations, and spectroscopy identified the majority of the candidates to be normal population type Ia and type II \acp{SN}, with a few dwarf novae and \acp{AGN} that are all very likely unrelated to GW150914.
Candidate classification, comparison of redshift with the GW distance, and use of source age are crucial constraints to rule candidates in and out.
Detailed discussions of candidate selection, spectroscopic and broadband follow-up are presented in survey-specific publications about iPTF candidates \citep{GW150914_iPTF} and about PESSTO follow-up of Pan\nobreakdashes-STARRS1 candidates \citep{GW150914_pan_STARRPESSTO}.

\begin{deluxetable*}{lccc|r|rrrr|l}
\tablecaption{\label{table:footprints}Summary of Tiled Observations}
\tablewidth{\textwidth}
\tablecolumns{10}
\tablehead{
    \colhead{Facility/} &
    \colhead{} &
    \colhead{} &
    \colhead{} &
    \colhead{Area} &
    \multicolumn{4}{c}{Contained Probability (\%)} &
    \colhead{}
    \\
    \cline{6-9}
    \colhead{Instrument} &
    \colhead{Band\tablenotemark{a}} &
    Depth\tablenotemark{b} &
    \colhead{Time\tablenotemark{c}} &
    \colhead{(deg$^2$)} &
    \colhead{cWB} &
    \colhead{LIB} &
    \colhead{BSTR\tablenotemark{d}} &
    \colhead{LALInf} &
    \colhead{GCN}
    }
\startdata
\\[-1.5em]\cutinhead{Gamma-ray}
\emph{Fermi} LAT	&20\,MeV--	&$1.7\times10^{-9}$	&(every	&---	&100	&100	&100	&100	&\citegcn{18709}\\
	&300\,GeV	&	&3\,hr)	&	&	&	&	&	&\\
\emph{Fermi} GBM	&8\,keV\nobreakdashes--40\,MeV	&0.7--$5\times10^{-7}$	&(archival)	&---	&100	&100	&100	&100	&\citegcn{18339}\\
	&	&(0.1--1\,MeV)	&	&	&	&	&	&	&\\
INTEGRAL	&75\,keV--1\,MeV	&$1.3\times10^{-7}$	&(archival)	&---	&100	&100	&100	&100	&\citegcn{18354}\\
IPN	&15\,keV--10\,MeV	&$1\times10^{-7}$	&(archival)	&---	&100	&100	&100	&100	&---\\
\cutinhead{X-ray}
MAXI/GSC	&2--20\,keV	&$1\times10^{-9}$	&(archival)	&17900	&95	&89	&92	&84	&\citegcn{19013}\\
\emph{Swift} XRT	&0.3--10\,keV	&$5\times10^{-13}$ (gal.)	&2.3, 1, 1	&0.6	&0.03	&0.18	&0.04	&0.05	&\citegcn{18331}\\
	&	&2--$4\times10^{-12}$ (LMC)	&3.4, 1, 1	&4.1	&1.2	&1.9	&0.16	&0.26	&\citegcn{18346}\\
\cutinhead{Optical\tablenotemark{e}}
DECam	&$i, z$	&$i<22.5$, $z<21.5$	&3.9, 5, 22	&100	&38	&14	&14	&11	&\citegcn{18344}, \citegcn{18350}\\
iPTF	&$R$	&$R<20.4$	&3.1, 3, 1	&130	&2.8	&2.5	&0.0	&0.2	&\citegcn{18337}\\
KWFC	&$i$	&$i<18.8$	&3.4, 1, 1	&24	&0.0	&1.2	&0.0	&0.1	&\citegcn{18361}\\
MASTER	&C	&$<19.9$	&-1.1, 7, 7	&710	&50	&36	&55	&50	&\citegcn{18333}, \citegcn{18390}, \citegcn{18903}, \citegcn{19021}\\
Pan-STARRS1	&$i $	&$i < 19.2-20.8$	&3.2, 21, 42	&430	&28	&29	&2.0	&4.2	&\citegcn{18335}, \citegcn{18343}, \citegcn{18362}, \citegcn{18394}\\
La Silla--	&$g, r$ 	&$r < 21$	&3.8, 5, 0.1	&80	&23	&16	&6.2	&5.7	&\citegcn{18347}\\
\;\;QUEST	& 	&	&	&	&	&	&	&	&\\
SkyMapper	&$i, v$	&$i<19.1$, $v<17.1$	&2.4, 2, 3	&30	&9.1	&7.9	&1.5	&1.9	&\citegcn{18349}\\
\emph{Swift} UVOT	&$u$	&$u<19.8$ (gal.)	&2.3, 1, 1	&3	&0.7	&1.0	&0.1	&0.1	&\citegcn{18331}\\
	&$u$	&$u<18.8$ (LMC)	&3.4, 1, 1	&	&	&	&	&	&\citegcn{18346}\\
TAROT	&C	&$R<18$	&2.8, 5, 14	&30	&15	&3.5	&1.6	&1.9	&\citegcn{18332}, \citegcn{18348}\\
TOROS	&C	&$r<21$	&2.5, 7, 90	&0.6	&0.03	&0.0	&0.0	&0.0	&\citegcn{18338}\\
VST@ESO	&$r$	&$r<22.4$	&2.9, 6, 50	&90	&29	&10	&14	&10	&\citegcn{18336}, \citegcn{18397}\\
\cutinhead{Near Infrared}
VISTA@ESO	&$Y, J, K_S$	&$J<20.7$	&4.8, 1, 7	&70	&15	&6.4	&10	&8.0	&\citegcn{18353}\\
\cutinhead{Radio}
ASKAP	&863.5\,MHz	&5--15\,mJy	&7.5, 2, 6	&270	&82	&28	&44	&27	&\citegcn{18363}, \citegcn{18655}\\
LOFAR	&145\,MHz	&12.5\,mJy	&6.8, 3, 90	&100	&27	&1.3	&0.0	&0.1	&\citegcn{18364}, \citegcn{18424}, \citegcn{18690}\\
MWA	&118\,MHz	&200\,mJy	&3.5, 2, 8	&2800	&97	&72	&86	&86	&\citegcn{18345}\\
 \enddata
\tablenotetext{a}{Band: photon energy, optical or near-infrared filter (or C for clear unfiltered light), wavelength range, or central frequency.}
\tablenotetext{b}{Depth: gamma/X-ray limiting flux in erg\,cm$^{-2}$\,s$^{-1}$; $5\sigma$ optical/IR limiting magnitude (AB); and $5\sigma$ radio limiting spectral flux density in mJy. The reported values correspond to the faintest flux/magnitude of detectable sources in the images.}
\tablenotetext{c}{Elapsed time in days between start of observations and the time of GW150914 (2015~September~14~09:50:45), number of repeated observations of the same area, and total observation period in days.}
\tablenotetext{d}{BAYESTAR.}
\tablenotetext{e}{Searches for bright optical transients were also done by BOOTES-3 and Pi of the Sky. Details are given in the Supplement \citep{GW150914-EMFOLLOW-SUPPLEMENT}.}
\end{deluxetable*}

\begin{deluxetable*}{lclllll}[ht!]
\tablecaption{\label{table:followup}Summary of Follow-up Observations}
\tablewidth{\textwidth}
\tablecolumns{7}
\tablehead{\multicolumn{7}{c}{Spectroscopic Follow-up}}
\startdata
Instrument &  No. of Candidates & Discovery Survey & Epochs &  $\lambda$ (\AA) & $\Delta\lambda$\tablenotemark{a} (\AA)  & GCN\\
\tableline
KeckII+DEIMOS &  8 & iPTF & 1 & $4650-9600$        & $3.5$  & \citegcn{18337}, \citegcn{18341}\\
LT+SPRAT & 1 & Pan-STARRS1 & 1 & $4500-7500$ & $18$ & \citegcn{18370}, \citegcn{18371}\\
NTT+EFOSC2        &  10 & QUEST/Pan-STARRS1 & 1 & $3650-9250$ & $18$ & \citegcn{18359}, \citegcn{18395}\\
P200+DBSP          &  1 &  Pan-STARRS1 & 1& $3200-9000$ &  $4-8$ & \citegcn{18372}\\
UH2.2m+SNIFS         & 9 & Pan-STARRS1 & 1 & $3200-10000$ & $4-6$ & --- \\
\tableline
\multicolumn{7}{c}{Radio Follow-up}\\
\tableline
Instrument & No. of Candidates & Discovery Survey & Epochs & Freq. (GHz) & Lim. Flux\tablenotemark{b}  (uJy) & GCN\\
\tableline
VLA   & 1  & iPTF & 3 & 6 & $\lesssim 50$ & \citegcn{18420}, \citegcn{18474}, \citegcn{18914} \\
 \enddata
\tablenotetext{a}{Full width at half maximum resolution.}
\tablenotetext{b}{$5\sigma$, 2 GHz nominal bandwidth, $\approx 20$\,min on-source.}
\end{deluxetable*}

\section{Sensitivity}
\label{s:sensitivity}

The third column of Table~\ref{table:footprints} summarizes the depth of the follow-up program. We provide limiting flux, flux density, or magnitude for the different facilities.
We emphasize that these limits only apply to the fraction of the sky contours that have been followed up.
For example, the \ac{MWA} fields have an 86\% chance of containing the
source's sky location and provide no constraints on sky locations representing the remaining 14\%.

Because the follow-up program was primarily designed to search for counterparts to
\ac{BNS} and \ac{NSBH} mergers, it is interesting to note that the observational
campaign would have provided powerful constraints on such a system.
A \ac{BNS} coalescence could have been detected by LIGO during O1 at a distance
of $\sim70$ Mpc, averaged over sky position and
orientations \citep{O1-SENSITIVITY}.
A short \ac{GRB} afterglow similar to those that have been observed
by \emph{Swift} XRT would have been detectable at that distance.
Re-scaling the observed X-ray fluxes of short GRBs at 11\,hr after the event
would yield fluxes in the range
$2\times10^{-11}$ to $6\times 10^{-8}\,$erg\,cm$^{-2}$\,s$^{-1}$ \citep{Berger:2014}.
Kilonova emission from a \ac{BNS} merger at that distance would reach a peak apparent magnitude of 17--24 within a week or two after the merger (e.g., \citealt{2010MNRAS.406.2650M,BarnesKasenKilonova,Tanaka:2013,grossman2014MNRAS}).
This range overlaps with the depth reached in the optical and near-IR bands.
Finally, this BNS system might produce radio emission from tens of $\mu$Jy to tens of mJy (e.g., \citealt{hp:2015}) with different timescales spanning weeks to years. Tables~\ref{table:footprints}~and~\ref{table:followup} show that the radio observations from wide-field facilities were sensitive to mJy flux densities at low frequencies where fainter sources with longer timescales are expected, while the narrow-field VLA was sensitive to well localized radio transients down to   $\mu$Jy flux densities at frequencies above a few GHz.

\section{Conclusions}
\label{s:conclusion}

GW150914 is consistent with the inspiral
and merger of two \acp{BH} of masses $\MONESCOMPACT$ and
$\MTWOSCOMPACT\,\ensuremath{\mathrm{M}_\odot}$, respectively, resulting in the formation of a
final \ac{BH} of mass $\MFINALSCOMPACT\,\ensuremath{\mathrm{M}_\odot}$ \citep{GW150914-DETECTION}. In classical general relativity, a \emph{vacuum} \ac{BBH} merger does not produce any \ac{EM} or particle emission whatsoever.
Whereas supermassive \acp{BBH} in galactic centers may appear as dual \acp{AGN} or have other distinctive \ac{EM} signatures due to interactions with gas or magnetic fields,
stellar \ac{BBH} systems are not expected to possess detectable EM counterparts.
The background gas densities and magnetic field strengths should therefore be typical of the interstellar medium, which are many orders of magnitude smaller than the environments of \ac{EM} bright supermassive \acp{BBH}. Although GW150914 is loud in \acp{GW} and expected to be absent in all \ac{EM} bands,
thorough follow-up observations were pursued
to check for \ac{EM} emission. Future EM follow-ups of GW sources will shed light on the presence or absence of firm EM counterparts and astrophysical processes that may trigger EM emission from these systems.

The \ac{EM} campaign following GW150914 successfully demonstrates the capability
of the observing partners to cover large swaths of the sky localization area, to
identify candidates, and to activate larger telescopes for photometric and
spectroscopic characterization within a few days of an event.
We note that the information about the source's BBH nature and updated
sky maps were sent out 20 days and four months after the event,
respectively. This resulted in some instruments covering much less of
the probability region or to the required depth of GW150914 than they
may have planned for. We expect future
alerts to be issued within tens of minutes with more information
about the signal type and more rapid updates of
the maps. The follow-up efforts would have been sensitive to a wide range of
emission expected from BNS or NSBH mergers.
However, the widely variable
sensitivity reached across the sky localization area continues to be a
challenge for an \ac{EM} counterpart search.

The number of galaxies \citep[with luminosities $L \geqslant 0.1
  L^{\star}$;][]{Blanton:2003} within the comoving volume of $10^{-2}$ Gpc$^{3}$
corresponding to the 90$\%$ credible area of the LALInference sky map and within
the 90$\%$ confidence interval distance is $\sim10^{5}$.  Such a number makes it
impossible to identify the host galaxy in the absence of an \ac{EM} counterpart
detection. The presence of a third \ac{GW} detector such as Virgo would have
improved the sky localization of GW150914 to a few tens of square degrees both
for the unmodeled and \ac{CBC} searches. The future addition of more
\ac{GW} detectors to the global network \citep{ObservingScenarios} will
significantly improve the efficiency of searches for \ac{EM} counterparts.

In summary, we have described the \ac{EM} follow-up program carried out for the first \ac{GW} source detected by Advanced \ac{LIGO}.
Within two days of the initial tentative detection of
GW150914, a \ac{GCN} circular was sent to \ac{EM}
follow-up partners alerting them to the event
and providing them with initial sky maps.
\FIXME{Twenty-five} \ac{EM} observing teams mobilized their resources, and over the
ensuing three months observations were performed with a diverse array
of facilities over a broad wavelength range (from radio to $\gamma$-ray).
Findings from those observations are being disseminated in other papers.
The localization and broadband follow-up of this \ac{GW} event constitutes an important first step in a new era of gravitational wave multi-messenger astronomy.

\providecommand{\acrolowercase}[1]{\lowercase{#1}}

\begin{acronym}
\acro{2D}[2D]{two\nobreakdashes-dimensional}
\acro{2+1D}[2+1D]{2+1\nobreakdashes--dimensional}
\acro{3D}[3D]{three\nobreakdashes-dimensional}
\acro{2MASS}[2MASS]{Two Micron All Sky Survey}
\acro{AdVirgo}[AdVirgo]{Advanced Virgo}
\acro{AMI}[AMI]{Arcminute Microkelvin Imager}
\acro{AGN}[AGN]{active galactic nucleus}
\acroplural{AGN}[AGN\acrolowercase{s}]{active galactic nuclei}
\acro{aLIGO}[aLIGO]{Advanced \acs{LIGO}}
\acro{ASKAP}[ASKAP]{Australian \acl{SKA} Pathfinder}
\acro{ATCA}[ATCA]{Australia Telescope Compact Array}
\acro{ATLAS}[ATLAS]{Asteroid Terrestrial-impact Last Alert System}
\acro{BAT}[BAT]{Burst Alert Telescope\acroextra{ (instrument on \emph{Swift})}}
\acro{BATSE}[BATSE]{Burst and Transient Source Experiment\acroextra{ (instrument on \acs{CGRO})}}
\acro{BAYESTAR}[BAYESTAR]{BAYESian TriAngulation and Rapid localization}
\acro{BBH}[BBH]{binary black hole}
\acro{BHBH}[BHBH]{\acl{BH}\nobreakdashes--\acl{BH}}
\acro{BH}[BH]{black hole}
\acro{BNS}[BNS]{binary neutron star}
\acro{CARMA}[CARMA]{Combined Array for Research in Millimeter\nobreakdashes-wave Astronomy}
\acro{CASA}[CASA]{Common Astronomy Software Applications}
\acro{CFH12k}[CFH12k]{Canada--France--Hawaii $12\,288 \times 8\,192$ pixel CCD mosaic\acroextra{ (instrument formerly on the Canada--France--Hawaii Telescope, now on the \ac{P48})}}
\acro{CRTS}[CRTS]{Catalina Real-time Transient Survey}
\acro{CTIO}[CTIO]{Cerro Tololo Inter-American Observatory}
\acro{CBC}[CBC]{compact binary coalescence}
\acro{CCD}[CCD]{charge coupled device}
\acro{CDF}[CDF]{cumulative distribution function}
\acro{CGRO}[CGRO]{Compton Gamma Ray Observatory}
\acro{CMB}[CMB]{cosmic microwave background}
\acro{CRLB}[CRLB]{Cram\'{e}r\nobreakdashes--Rao lower bound}
\acro{cWB}[\acrolowercase{c}WB]{Coherent WaveBurst}
\acro{DASWG}[DASWG]{Data Analysis Software Working Group}
\acro{DBSP}[DBSP]{Double Spectrograph\acroextra{ (instrument on \acs{P200})}}
\acro{DCT}[DCT]{Discovery Channel Telescope}
\acro{DECAM}[DECam]{Dark Energy Camera\acroextra{ (instrument on the Blanco 4\nobreakdashes-m telescope at \acs{CTIO})}}
\acro{DES}[DES]{Dark Energy Survey}
\acro{DFT}[DFT]{discrete Fourier transform}
\acro{EM}[EM]{electromagnetic}
\acro{ER8}[ER8]{eighth engineering run}
\acro{FD}[FD]{frequency domain}
\acro{FAR}[FAR]{false alarm rate}
\acro{FFT}[FFT]{fast Fourier transform}
\acro{FIR}[FIR]{finite impulse response}
\acro{FITS}[FITS]{Flexible Image Transport System}
\acro{FLOPS}[FLOPS]{floating point operations per second}
\acro{FOV}[FOV]{field of view}
\acroplural{FOV}[FOV\acrolowercase{s}]{fields of view}
\acro{FTN}[FTN]{Faulkes Telescope North}
\acro{FWHM}[FWHM]{full width at half-maximum}
\acro{GBM}[GBM]{Gamma-ray Burst Monitor\acroextra{ (instrument on \emph{Fermi})}}
\acro{GCN}[GCN]{Gamma-ray Coordinates Network}
\acro{GMOS}[GMOS]{Gemini Multi-object Spectrograph\acroextra{ (instrument on the Gemini telescopes)}}
\acro{GRB}[GRB]{gamma-ray burst}
\acro{GSC}[GSC]{Gas Slit Camera}
\acro{GSL}[GSL]{GNU Scientific Library}
\acro{GTC}[GTC]{Gran Telescopio Canarias}
\acro{GW}[GW]{gravitational wave}
\acro{HAWC}[HAWC]{High\nobreakdashes-Altitude Water \v{C}erenkov Gamma\nobreakdashes-Ray Observatory}
\acro{HCT}[HCT]{Himalayan Chandra Telescope}
\acro{HEALPix}[HEALP\acrolowercase{ix}]{Hierarchical Equal Area isoLatitude Pixelization}
\acro{HEASARC}[HEASARC]{High Energy Astrophysics Science Archive Research Center}
\acro{HETE}[HETE]{High Energy Transient Explorer}
\acro{HFOSC}[HFOSC]{Himalaya Faint Object Spectrograph and Camera\acroextra{ (instrument on \acs{HCT})}}
\acro{HMXB}[HMXB]{high\nobreakdashes-mass X\nobreakdashes-ray binary}
\acroplural{HMXB}[HMXB\acrolowercase{s}]{high\nobreakdashes-mass X\nobreakdashes-ray binaries}
\acro{HSC}[HSC]{Hyper Suprime\nobreakdashes-Cam\acroextra{ (instrument on the 8.2\nobreakdashes-m Subaru telescope)}}
\acro{IACT}[IACT]{imaging atmospheric \v{C}erenkov telescope}
\acro{IIR}[IIR]{infinite impulse response}
\acro{IMACS}[IMACS]{Inamori-Magellan Areal Camera \& Spectrograph\acroextra{ (instrument on the Magellan Baade telescope)}}
\acro{IMR}[IMR]{inspiral-merger-ringdown}
\acro{IPAC}[IPAC]{Infrared Processing and Analysis Center}
\acro{IPN}[IPN]{InterPlanetary Network}
\acro{IPTF}[\acrolowercase{i}PTF]{intermediate \acl{PTF}}
\acro{ISM}[ISM]{interstellar medium}
\acro{ISS}[ISS]{International Space Station}
\acro{KAGRA}[KAGRA]{KAmioka GRAvitational\nobreakdashes-wave observatory}
\acro{KDE}[KDE]{kernel density estimator}
\acro{KN}[KN]{kilonova}
\acroplural{KN}[KNe]{kilonovae}
\acro{LAT}[LAT]{Large Area Telescope}
\acro{LCOGT}[LCOGT]{Las Cumbres Observatory Global Telescope}
\acro{LHO}[LHO]{\ac{LIGO} Hanford Observatory}
\acro{LIB}[LIB]{LALInference Burst}
\acro{LIGO}[LIGO]{Laser Interferometer \acs{GW} Observatory}
\acro{llGRB}[\acrolowercase{ll}GRB]{low\nobreakdashes-luminosity \ac{GRB}}
\acro{LLOID}[LLOID]{Low Latency Online Inspiral Detection}
\acro{LLO}[LLO]{\ac{LIGO} Livingston Observatory}
\acro{LMI}[LMI]{Large Monolithic Imager\acroextra{ (instrument on \ac{DCT})}}
\acro{LOFAR}[LOFAR]{Low Frequency Array}
\acro{LOS}[LOS]{line of sight}
\acroplural{LOS}[LOSs]{lines of sight}
\acro{LMC}[LMC]{Large Magellanic Cloud}
\acro{LSB}[LSB]{long, soft burst}
\acro{LSC}[LSC]{\acs{LIGO} Scientific Collaboration}
\acro{LSO}[LSO]{last stable orbit}
\acro{LSST}[LSST]{Large Synoptic Survey Telescope}
\acro{LT}[LT]{Liverpool Telescope}
\acro{LTI}[LTI]{linear time invariant}
\acro{MAP}[MAP]{maximum a posteriori}
\acro{MBTA}[MBTA]{Multi-Band Template Analysis}
\acro{MCMC}[MCMC]{Markov chain Monte Carlo}
\acro{MLE}[MLE]{\ac{ML} estimator}
\acro{ML}[ML]{maximum likelihood}
\acro{MOU}[MOU]{memorandum of understanding}
\acroplural{MOU}[MOUs]{memoranda of understanding}
\acro{MWA}[MWA]{Murchison Widefield Array}
\acro{NED}[NED]{NASA/IPAC Extragalactic Database}
\acro{NSBH}[NSBH]{neutron star\nobreakdashes--black hole}
\acro{NSBH}[NSBH]{\acl{NS}\nobreakdashes--\acl{BH}}
\acro{NSF}[NSF]{National Science Foundation}
\acro{NSNS}[NSNS]{\acl{NS}\nobreakdashes--\acl{NS}}
\acro{NS}[NS]{neutron star}
\acro{O1}[O1]{\acl{aLIGO}'s first observing run}
\acro{oLIB}[\acrolowercase{o}LIB]{Omicron+\acl{LIB}}
\acro{OT}[OT]{optical transient}
\acro{P48}[P48]{Palomar 48~inch Oschin telescope}
\acro{P60}[P60]{robotic Palomar 60~inch telescope}
\acro{P200}[P200]{Palomar 200~inch Hale telescope}
\acro{PC}[PC]{photon counting}
\acro{PESSTO}[PESSTO]{Public ESO Spectroscopic Survey of Transient Objects}
\acro{PSD}[PSD]{power spectral density}
\acro{PSF}[PSF]{point-spread function}
\acro{PS1}[PS1]{Pan\nobreakdashes-STARRS~1}
\acro{PTF}[PTF]{Palomar Transient Factory}
\acro{QUEST}[QUEST]{Quasar Equatorial Survey Team}
\acro{RAPTOR}[RAPTOR]{Rapid Telescopes for Optical Response}
\acro{REU}[REU]{Research Experiences for Undergraduates}
\acro{RMS}[RMS]{root mean square}
\acro{ROTSE}[ROTSE]{Robotic Optical Transient Search}
\acro{S5}[S5]{\ac{LIGO}'s fifth science run}
\acro{S6}[S6]{\ac{LIGO}'s sixth science run}
\acro{SAA}[SAA]{South Atlantic Anomaly}
\acro{SHB}[SHB]{short, hard burst}
\acro{SHGRB}[SHGRB]{short, hard \acl{GRB}}
\acro{SKA}[SKA]{Square Kilometer Array}
\acro{SMT}[SMT]{Slewing Mirror Telescope\acroextra{ (instrument on \acs{UFFO} Pathfinder)}}
\acro{SNR}[S/N]{signal\nobreakdashes-to\nobreakdashes-noise ratio}
\acro{SSC}[SSC]{synchrotron self\nobreakdashes-Compton}
\acro{SDSS}[SDSS]{Sloan Digital Sky Survey}
\acro{SED}[SED]{spectral energy distribution}
\acro{SGRB}[SGRB]{short \acl{GRB}}
\acro{SN}[SN]{supernova}
\acroplural{SN}[SN\acrolowercase{e}]{supernova}
\acro{SNIa}[\acs{SN}\,I\acrolowercase{a}]{Type~Ia \ac{SN}}
\acroplural{SNIa}[\acsp{SN}\,I\acrolowercase{a}]{Type~Ic \acp{SN}}
\acro{SNIcBL}[\acs{SN}\,I\acrolowercase{c}\nobreakdashes-BL]{broad\nobreakdashes-line Type~Ic \ac{SN}}
\acroplural{SNIcBL}[\acsp{SN}\,I\acrolowercase{c}\nobreakdashes-BL]{broad\nobreakdashes-line Type~Ic \acp{SN}}
\acro{SVD}[SVD]{singular value decomposition}
\acro{TAROT}[TAROT]{T\'{e}lescopes \`{a} Action Rapide pour les Objets Transitoires}
\acro{TDOA}[TDOA]{time delay on arrival}
\acroplural{TDOA}[TDOA\acrolowercase{s}]{time delays on arrival}
\acro{TD}[TD]{time domain}
\acro{TOA}[TOA]{time of arrival}
\acroplural{TOA}[TOA\acrolowercase{s}]{times of arrival}
\acro{TOO}[TOO]{target\nobreakdashes-of\nobreakdashes-opportunity}
\acroplural{TOO}[TOO\acrolowercase{s}]{targets of opportunity}
\acro{UFFO}[UFFO]{Ultra Fast Flash Observatory}
\acro{UHE}[UHE]{ultra high energy}
\acro{UVOT}[UVOT]{UV/Optical Telescope\acroextra{ (instrument on \emph{Swift})}}
\acro{VHE}[VHE]{very high energy}
\acro{VISTA}[VISTA@ESO]{Visible and Infrared Survey Telescope}
\acro{VLA}[VLA]{Karl G. Jansky Very Large Array}
\acro{VLT}[VLT]{Very Large Telescope}
\acro{VST}[VST@ESO]{\acs{VLT} Survey Telescope}
\acro{WAM}[WAM]{Wide\nobreakdashes-band All\nobreakdashes-sky Monitor\acroextra{ (instrument on \emph{Suzaku})}}
\acro{WCS}[WCS]{World Coordinate System}
\acro{WSS}[w.s.s.]{wide\nobreakdashes-sense stationary}
\acro{XRF}[XRF]{X\nobreakdashes-ray flash}
\acroplural{XRF}[XRF\acrolowercase{s}]{X\nobreakdashes-ray flashes}
\acro{XRT}[XRT]{X\nobreakdashes-ray Telescope\acroextra{ (instrument on \emph{Swift})}}
\acro{ZTF}[ZTF]{Zwicky Transient Facility}
\end{acronym}

\acknowledgements

See the Supplement \citep{GW150914-EMFOLLOW-SUPPLEMENT} for a full list of acknowledgements. This is LIGO document LIGO-P1500227-v12.

\bibliographystyle{aasjournal}

redpajama_set_name: RedPajamaArXiv


text:
← The Merry Wives of Windsor (ASC vs BBC) I
No One Can Escape the Tentacles of the State →
The Merry Wives of Windsor (ASC vs BBC) I
Posted on Sunday: August 16, 2009 by Michael Hendry
Like everything else they've done, I've immensely enjoyed the American Shakespeare Center's production of The Merry Wives of Windsor, playing through the end of November, along with Much Ado About Nothing and Titus Andronicus (more about them later). 1 Henry IV will be added to the rotation in early September, George Villier's The Rehearsal (apparently a cruel parody of Dryden's tragedies) in October.
I don't really 'get' plays without seeing them more than once, and I've seen the ASC Merry Wives four times so far. However, before writing about the production, I thought I'd better look for something to compare it with — something besides their productions of other plays, I mean. I had never seen or read the play before seeing it here, and still haven't read any scholarship or general essays on it — didn't want to prejudice my reaction. I have now read it in the Arden edition with most of the notes, watched the 1982 BBC version (the only one available on DVD), and also watched one of the operatic versions, Salieri's Falstaff (1799), which I had previously seen at Wolftrap and once on DVD, though not recently. (I've also seen Verdi's Falstaff at the Met and on DVD, though not recently, and won't have much to say about it here.)
Here are my thought so far, for what they are worth:
Text: Both versions had a few cuts. The ASC omits the subplot about the three German horse-thieves (IV.3 and IV.5), along with some of the scholastic humor, though they include the "Castalian king urinal" (II.3), whatever that means (according to Arden, no one knows). The only cuts I noticed in the BBC version were a couple of jokes in the Latin lesson (IV.1) including (oddly) the one that comes across most clearly to a Latinless audience, the one about "the focative case", which anyone can hear is a dirty joke even if they've never heard of the vocative case in Latin or the anatomical meaning of 'case' in Elizabethan English.
Humor: In general, the ASC missed fewer opportunities for jokes. There were 3-4 jokes in the BBC version that I hadn't caught at ASC, mostly in Dr. Caius' French accent: he calls Anne Page 'On Podge'and his rival in love 'Sir Huge' and when he calls his servant 'that knave Rog-by' he pronounces the second word kuh-nave. I assume it is intentional that his repeated "by gar" sounds almost like 'bugger'. He also asks for his "green pox" (i.e. box), which is more a Welsh than a French accent, though there are other instances of that in the play.
On the other hand, the BBC production missed at least a dozen opportunities that ASC seized. I don't want to give too many examples, since I hope some of my readers will come to see the play and be as surprised and delighted by them as I was the first time around, but here are two:
The look on the face of Mistress Ford (Sarah Fallon) when she reads in Falstaff's letter (II.1) "You are not young, no more am I" and again when she overhears her husband's reaction to the news that Falstaff is wooing his wife, saying to Pistol "Why sir, my wife is not young".
When Ford (John Harrell) says "Buck? I would I could wash myself of the buck! Buck, buck, buck! Ay, buck! I warrant you, buck –" (III.1), he kicks the basket hard on each repetition of "buck". (I hope they arranged some sort of padding for that side of the basket, since Falstaff is in it and barely fits. Perhaps Ford is actually kicking the frame. I'll have to try sitting on that side of the stage next time I go.)
Sets and Props: The BBC set was of course far fancier, particularly the indoor scenes. I liked the huge timber that bisected Falstaff's room at waist-height and forced visitors to duck under it. His buck basket was nicer, too, though the clothes in it were far too generic: the ASC's clothes included a fair percentage of underwear. And Falstaff's hornèd hat was not obviously made from a football helmet, as at the ASC. On the other hand, Falstaff's gingham dress was better at the ASC. Of course, these are far from the most important features of a production.
Words: I had trouble hearing all the words in the BBC version. If this were a stage play recorded live, I could blame the technicians, but it was made for TV, so there's really no excuse. Not that the diction was terrible, but to take one tiny example, I wouldn't have comprehended Falstaff's comparison of Pistol and Nym to a "gemini of baboons" (II.2) if I hadn't already heard the phrase clearly at ASC. When I'm at the Blackfriars, I don't even notice the actors' competence in pronouncing and projecting their lines, and reinforcing them with gestures. I just take all that for granted until I see a non-ASC play.
Characters: I'm still gathering my thoughts about the various Pages and Fords. In the mean time, here are some notes on the other characters:
Falstaff: Richard Griffiths (BBC) was a disappointment: too short, too thin, too soft — almost effeminate, and way too young. He looked 25, and I was surprised to learn from IMDB that he was 35 when the film was made. Nolan Carey (ASC's Nym) played Falstaff in the MFA production of 2 Henry IV earlier this year, and also looked too young, but there's only so much you can do with makeup, and youthful looks are to be expected in a student production. He was tall enough and fat enough for the part, though his fat suit got a little carried away in the (how shall I put this?) man-boobs area. James Keegan's ASC Falstaff is, or appears to be, taller, fatter, older, and at the same time more vigorous than Griffiths, and he wears his fat suit very naturally. He is, in short, imposing. I've only dipped into my two recordings of Verdi's opera lately (Haitink at the Royal Opera House in 1999, with Bryn Terfel in the title role, and Muti at La Scala in 2001), but all three of the operatic Falstaffs I've seen have the appropriate height, heft, and general vigor and dominance. Muti's Falstaff, Ambrogio Maestri, ruins this with a hair style blatantly lifted from Krusty the Clown, but that's another story.
Bardolph, Pistol, Nym, and Mine Host of the Garter: With no doubling of roles and (presumably) a much larger budget, the BBC does a good job with these four. I found it hard to understand the stylistic jokes in both versions (Pistol's Marlovian boasting, Nym's "humors") and had to read about them in the Arden edition, but I suppose that is inevitable.
Shallow: Alan Bennett (BBC) is a harmless and very decrepit old man, while René Thornton, Jr. (ASC) is a hilariously dirty old perv, though he is too big and healthy to look quite as decrepit as he ought.
Slender: Richard O'Callaghan (BBC) is depicted as a fop, in fact looks a bit like some depictions of Shakespeare, and his "I am not altogether an ass" is fairly convincing. The ASC Slender (Chris Johnston) is altogether an ass and then some, and comes across as very young and a total dork — hilariously awful.
Fenton: Not much to say except that Tobias Shaw (ASC) is younger and much handsomer than his BBC counterpart.
Sir Hugh Evans: The BBC Sir Hugh's Welsh accent, though presumably authentic, was nearly undetectable, at least to my untutored ears. Apparently the BBC thought putting a real Welshman in the part (Tenniel Evans) would suffice, but his failure to audibly mix up his Bs and Ps and so on ruined many of the jokes. Perhaps they were afraid of offending the Welsh, but a fake Welshman with a comically-exaggerated accent, like Chris Seiler at the ASC, would have been funnier. (Cf. Henry James, "The Real Thing".)
Dr Caius: Daniel Rigney (ASC) looks much younger than Michael Bryant (BBC) and also (therefore?) less threatening, both to his servants and to Sir Hugh. I'm not sure whether that's a plus or a minus or just a difference. I'm also not sure whether making Dr Caius and Slender look twice the age of Anne Page is a good thing in so far as May-December matches are both historically plausible and creepy, or whether that distracts from the main lines of the plot. Still thinking about this.
Mistress Quickly: Without giving away too many details for those who haven't seen the play, Alison Glenzer (ASC) makes very effective use of her skirt and cleavage for comic purposes. The BBC Quickly was rather dull, at least by comparison.
Bit Parts: I don't have much to say about the servants except that I couldn't tell whether Ron Cook's Peter Simple (BBC) was supposed to be 15 or 40 — he always seemed to be one or the other, nothing in between, which was a bit disturbing, and his simpleness looked like cliché mental retardation, while Erin Baird (ASC) comes across as none too swift but mostly naïve and very young.
The BBC postmaster's boy and the other male 'bride' at the end were played by actual boys who could plausibly pass for girls. At least I'm assuming they were boys: it wasn't easy to tell, which I suppose was the point. More farcically, the ASC uses the two biggest available men in the cast, René Thornton, Jr. and Nolan Carey. In this case, as in most cases, I prefer farce to verisimilitude.
How to sum up? If you're anywhere near Staunton, Virginia, come see the play.
This entry was posted in Blackfriars, Culture: Plays, Theater Reviews. Bookmark the permalink.

redpajama_set_name: RedPajamaCommonCrawl


text:
Editors' ChoiceNeuroscience
"Spontaneous" Release Trigger
Stella M. Hurtley
Synaptic vesicle release occurs in different phases that can be tightly coupled to action potentials (synchronous), immediately following action potentials (asynchronous), or stochastic events not triggered by action potentials (spontaneous). The vesicle protein synaptotagmin is thought to act as the Ca2+ sensor in the synchronous phase, but for the other two phases, Ca2+ sensors have not been identified. Groffen et al. now show that cytoplasmic proteins known as Doc2 (double C2 domain) proteins are required for spontaneous release. Doc2 proteins promote membrane fusion in response to exceptionally low increases in Ca2+ and are several orders of magnitude more sensitive to Ca2+ than synaptotagmin. Doc2 and synaptotagmin compete for SNARE-complex binding during membrane fusion. A mutation that abolishes the Ca2+ dependence of Doc2b also abolishes the Ca2+ dependence of spontaneous release. Thus, Doc2 is a high-affinity Ca2+ sensor for spontaneous release that competes with synaptotagmin for SNARE complex binding.
A. J. Groffen, S. Martens, R. Díez Arazola, L. N. Cornelisse, N. Lozovaya, A. P. H. de Jong, N. A. Goriounova, R. L. P. Habets, Y. Takai, J. G. Borst, N. Brose, H. T. McMahon, M. Verhage, Doc2b is a high-affinity Ca2+ sensor for spontaneous neurotransmitter release. Science 327, 1614–1618 (2010). [Abstract] [Full Text]
You are going to email the following "Spontaneous" Release Trigger
By Stella M. Hurtley
Science Signaling 30 Mar 2010 : ec101
Spontaneous synaptic vesicle fusion is triggered by soluble proteins that compete with synaptotagmins to induce membrane curvature.


The Senate Appropriations Committee on Thursday unanimously advanced a fiscal 2019 spending bill that contains a 1.9 percent pay raise for civilian federal employees, going against President Trump's proposed pay freeze for next year.
Committee members voted down 29-2 a Republican amendment to strip the pay increase from the Financial Services and General Government Appropriations bill, which will now head to the full Senate. Ranking member Sen. Chris Van Hollen, D-Md., applauded the panel for preserving the small raise.
The House Appropriations Committee did not include any provisions on federal employee pay in its version of the general government spending bill, which effectively endorses the White House plan for a freeze released as part of President Trump's 2019 budget request. Neither House nor Senate appropriators have acted to advance the Trump administration's proposed $1 billion interagency workforce fund, pitched by officials at the Office of Management and Budget and the Office of Personnel Management as a way to fund pilot programs that institute pay for performance.
Some members of Congress also signed onto a bill earlier this year that would provide a 3 percent across-the-board raise for civilian federal employees. Van Hollen said he supports that measure as well.
Now some other key information on how this would affect your pension if you would retire by the end of October. Schedule your Personalized Federal Retirement Review so that we can explain how this will impact you.


text:
Services / VOIP services
BT Turns On 21CN, IPTV
Ray Le Maistre, Editor-in-Chief
BT Group plc (NYSE: BT; London: BTA) has transferred its first real customers from its PSTN to its 21CN next-generation network, starting a challenging five-year plan to migrate 20 million lines to the single all-IP infrastructure it is rolling out across the U.K. (See BT Switches on 21CN and BT: 21CN Slips, IPTV Nears.)
The British incumbent, which first unveiled its 21CN plans in June 2004, plans to have all its U.K. customers hooked up to the 21CN by 2011, a process that will cost £10 billion (US$19.5 billion) in capex and opex. Ultimately, BT plans to decommission its 16 legacy voice and data networks. (See BT: 21CN Slips, IPTV Nears and BT Moves Ahead With Mega Project.)
The carrier has also confirmed to Light Reading that it will launch its IPTV service, BT Vision, next Monday, Dec. 4. More on that later.
'Bishop, are you there?'
This morning, BT hooked up its first set of actual paying customers to its 21CN, and 11-year-old Laura Wess, a pupil at the Wick and Marcross Church in Wales Primary School, became the first person to make a call across the new infrastructure. According to BT, she called the Right Reverend John Davies, the bishop of St. Asaph in North Wales, who has responsibility for education for the Church in Wales.
It's not clear whether the call was blessed.
Laura's school is in the village of Wick, near Cardiff in South Wales, the area designated as the launching pad for 21CN. (See Wales to Get 21CN First.)
BT says more than 100 customers were switched over to the 21CN "in the early hours of this morning," and that "by the end of summer 2007, around 350,000 customer lines in South Wales are expected to have been migrated to the new infrastructure."
The first customers are connected to one of the newly installed MSANs (multiservice access nodes) supplied by Fujitsu Telecommunications Europe Ltd. housed in Wick's local exchange. In future exchanges "we will use either Fujitsu or Huawei Technologies Co. Ltd. ," says a spokeswoman. (See Fujitsu Shares Its 21CN Success and BT Unveils 21CN Suppliers.)
The Cardiff area is served by 50 local exchanges, while IP voice switching will be handled by Ericsson AB (Nasdaq: ERIC) systems installed in three new metro nodes, or "super telephone exchanges," as BT calls them. (See Ericsson to Bring Partners to 21CN Party.)
The spokeswoman says end users lines are being "physically disconnected from the legacy network and reconnected to 21CN" at the local exchange, while at a larger BT exchange in Cardiff, "the network data of [the] migrating customers was reconfigured, sending their incoming and outgoing calls from the Wick exchange on to 21CN."
BT staff will closely monitor the initial transfer before switching the rest of Wick's few hundred residents across to the 21CN. But the carrier isn't decommissioning any TDM gear just yet. "We'll start switching off legacy equipment when it makes sense to do so from an engineering perspective," says the spokeswoman.
Once the Cardiff area is all hooked up, BT plans to perform the same kind of migration in a number of major towns and cities, including London, Birmingham, Manchester, Belfast, Glasgow, Edinburgh, and, possibly, Crapstone, Devon.
Ovum Ltd. analyst Mike Cansfield believes that "Wick signals the start of a move in the U.K. from the networks and processes of the twentieth century into new networks and processes more appropriate to the Internet age of a new millennium." [Ed. note: Woohoo!]
But, adds Cansfield in a research note issued today, "as anyone with experience of project management knows, this is where the challenges really start. To complete the rollout in south Wales, and then across the rest of the U.K. by 2011, is an aggressive timescale. This will require all of BT's resources, those of its suppliers, and the rest of the industry to make it work on the ground. There is no certainty this can be achieved... This is just the start."
BT vision still under wraps
Separately, BT is promising to unveil its IPTV service to the media, and also make the service available to BT broadband customers, next Monday, Dec. 4.
The service, BT Vision, is powered by Microsoft Corp. (Nasdaq: MSFT) IPTV technology and will offer a wide range of content from an on-demand menu, delivered over the user's broadband connection, along with regular TV channels, delivered via a rooftop aerial and a special connection on the customer's set-top box. (See Microsoft Wins at BT, BT Unveils IPTV Service, BT Signs More IPTV Deals, BT Adds to Vision Content , and BT Adds Music Video Deal.)
That method puts less strain on the broadband connection, because only the on-demand, unicast content is delivered over the DSL connection.
BT, though, is being coy about the extent of its initial launch. While a spokesman says the availability of the service is not limited by geography, he couldn't commit to saying the service will be immediately available to all of BT's 3 million broadband customers in the U.K.
Until Monday, the carrier is saying only that it is planning "a full commercial launch," without actually explaining what that means.
BT has a lot of competition in the U.K. when it comes to TV and video entertainment. Cable operator ntl group ltd. (Nasdaq: NTLI) and satellite TV/broadband service provider Sky are both strong players in the digital TV market.
But BT is hoping that its English Premiership soccer deal, which will allow the carrier to show games between the likes of Manchester United, Chelsea, Arsenal, and Liverpool in "near live" time (starting about 5 hours after the game begins) beginning in September 2007, will attract customers. (See BT Wins Soccer Deal.)
— Ray Le Maistre, International News Editor, Light Reading
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tsat
12/5/2012 | 3:33:50 AM
re: BT Turns On 21CN, IPTV
We have been waiting for this for 8 years. Kudos to BT for taking up the challenge and working to make the true converged network a reality.
Don't be cynical. These little steps are very important to our industry.
-tsat
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How did the fame of online meeting rooms alternate deals within businesses?
There is no surprise directors loved using virtual deal rooms. You can work with your papers from any location and at any moment. They have plain interface. And the best part - virtual repository gives you a chance to not to attend the meeting physically.
Electronic data rooms let corporations share the important data speedily and safely. Deal room simplifies negotiations, accelerates business deals and boosts the control over the data. As we can see nowadays, the fame of virtual meeting rooms increases significantly and will not go away in the impending future.
What will electronic data room offer us in the future?
Let's start with that online repositories provide users with numerous features that allow brands to carry out partnerships smoothly and instantly. Virtual data room helps perfecting sales, the performance of employees and all other processes within the brand. As the electronic data room market expands, providers will offer new instruments in their software and come up with new solutions for businesses.
Additionally, online repositories allow to eliminate physical documents. It not only simplifies the files management process by erasing the need to create physical data rooms data room vdr and keep files. But the hustle physical documents create is not the only thing virtual repositories will fix. Let's care about the nature. The extreme waste of paper is one of the biggest issues modern environment has to deal with. So virtual deal rooms will also make corporations greener.
There is a important reason why CEOs pick virtual meeting rooms. And it's not about simplifying the management, to be honest. It's about the protection. Corporations deal with sensitive files all the time. They share it with partners, investors, employees and other parties that need to review files. And the data theft is the last thing business owners want to experience.
Another benefit is that busy leaders of firms can save a bit of time by participating in meetings online. Using electronic data rooms takes away the complications from the management of the meeting and makes it more dynamic. Thus, all participants will waste no time and hold negotiations promptly. Besides that, with virtual data rooms, parties can upgrade their communication since online meeting room gives users numerous that help them communicate.
Virtual data rooms are intuitive and require no training. And once the uploaded information is structured and the convenient system of folders is established, all members of the team can find the required data promptly. Including the fact that the online meeting room can be reached from any device and from any location, online meeting room is desirable to business owners because it gives them adaptability in a working process.
The whole Earth population goes online. And firms decide to use modern technologies too because they boost processes. It helps enterprises to work with remote professionals and make deals with partners and investors around the globe. Online deal rooms made remote business relationships even more simple and efficient. So in the approaching future, we can expect the growth of the number of virtual workflows. And since it requires as little time and money as possible, such relationships held within the electronic data room will allow companies to advance faster impacting the economy in general.
Designed by Nice Computer Man.


A lightweight duvet is your best choice if you're aiming to take pleasure in undisturbed sleep. Numerous duvets have different fillings that eventually choose its general weight. Amongst the a number of available alternatives, the goose down filled duvet is among the most comfy. And, while goose down is one of the most costly duvet fillings, it's truly worth it. It is durable and also works as a brilliant insulator. While this certain duvet range might be made use of by virtually anybody; folks suffering from back pain can benefit most from it.
You need to validate the material of the bedding sets as there are many fabrics that one could blend in and offer the product. However, you need to carefully see the quality of the product and afterwards go for the option process. There will be marked down costs for you in the online and for some items, they even offer at complimentary shipping cost. So, start now and search for the best quality bedding sets.
If you are looking for an economical down comforter, there are a couple of aspects to make note of as you compare probable selections on the internet and in other places. Down comforters can differ substantially asing per these facets, and some low-cost down comforters will be large amounts while some will not.
Did you understand that keeping your bed set clean can avoid you from being invaded by allergen? Regular cleaning of your sheets can avoid these slightly animals from taking control of your bed and causing allergies. That is why a duvet cover set is considered among the healthiest kinds of fitted 4ft sheets around. It can be washed as often as you like, unlike comforters. Everyone that has a comforter understands how hard it is to clean it in the cleaning piece of equipment. It is either too big or it needs to be dry cleaned. Dry cleaning can can cost a great deal of cash. That is why many people do not clean their comforters as often as they ought to which is when allergen take over.
A lightweight duvet is your finest choice if you're looking to take pleasure in undisturbed sleep. Various duvets have various fillings that eventually decide its all round weight. Among many accessible options, the goose down filled duvet is the most comfortable. And, while goose down is among the most pricey duvet fillings, it's worth it. It's sturdy and also works as a fantastic insulator. While this particular duvet type can be made use of by just about any person; folks having a hard time from pain in the back can benefit most from it.
If you are trying to find fresh face-lift, you might wish to attempt some of the variety of alternatives readily available for bed linen. From the designer want to some of the specialty items, you will discover what you are trying to find rather quickly. The many internet sites that are readily available online and there are many other options in retail stores will help you in your quest.
The first and essential thing that will keep you warm during the night is the fill rating. By understanding the fill rating, you can compare the rates to other brands of down comforters. The greater the fill rating, the warmer and more elegant the down comforter will be. One that has a fill rating of 500 or more is considered to be excellent. If you stay in an environment that does not get quite as cold, then possibly you would actually like one with a lower fill count. Fill counts refer to the density and number of feathers made use of in the product. Clearly ones with greater counts will be a bit more expensive, however may keep you toast warm during the night. Be sure to inspect around for the best offers. Numerous excellent finds can be found on the web.
There are multiple styles and designs of comforters made to fit your every requirement and requirements. If you want the geometric, clean lines that will improve and highlight a minimalistic space, you could wish to get the comforter that has a strong color on one side and a complementary color on the other side. These sorts of comforters generally have the contrasting color in piping on the sewing to offer you a chance to include interesting pillows to the bedding.
Although no real tog score exists in the UK requirements, you can still determine the quality of silk duvet. You can do this by knowing the grams of silk consisted of in per square meter of duvet material. A 2.4 tog score means 250 grams of silk; a 7.9 tog score means 400 grams of silk; and 10 to 13 tog score means 600 grams of silk.
One of the primary reasons why individuals choose fitted 4ft sheets sets is due to the fact that they do not want to spend too much on the bedroom project. Although, there are customers that do choose bedroom refurbishing every few years but those who can not pay for can still choose getting bedding sets that can bring out some good changes in the bedroom. Bedding sets are not too expensive and therefore even middle class individuals can manage it and utilize it when they want to refurbish their home. There are many sites that do sell bedding sets at inexpensive rates and therefore purchasers can search for it online.
There are people on the planet, which does not know the differentiation of bedding sets and low-cost linens and purchase them as per their preferred design and color. So, to achieve the concept and to make the consumer feel happy, there are some net stores for highest bedding sets. There are numerous designer and regular online stores, which has created pioneering and trendy designs.
Southwest bedspreads are the only selection for any southwestern, western or even Native American design. It's easy to get bedspreads online since they are growing in popularity daily. The southwest teems with color and life which rustic heat is what you catch in the beautiful Indian pattern bedspreads. Western design is also best for these rich materials.
Silk material has the capability to maintain the temperature level of the body over the night. It keeps one cool when the temperature level is warm exterior and warm when the temperature level is cool exterior. Preserving a more consistent temperature level throughout the night prevents overheating and allows the body to have actually a more relaxed and sound sleep.
The economy may also have something to do with the current reductions in fitted 4ft sheets costs. Cash flow is important to any company. And with retail sales dropping everywhere, merchants have to find a method to move the product. They might be offering simply to obtain cash in the registers throughout bumpy rides, or they may be offering bedding as a loss leader to obtain you into the establishment.
Looking for some fine Duvets? Well, you are better to getting them since below we will acquaint you better with this epitome of convenience. Today, a duvet is even more than just feathers interwoven in a cloth bag. You can discover lavishly soft down-proof fabrics stuffed with extremely fine-tuned and hygienic down of white goose. Stay comfortable and warm with ultra-soft and fluffy bedding throughout the freezing weather condition.
Not everyone can make the most of quality down filled bedding. You may be allergic to it. This is where option down comes in. It is the best option for allergy sufferers. This bedding will be basic to keep clean. You can quickly look after it. It will keep you warm and look excellent in all types of bedroom design. It may be a little heaver than a down comforter.
The expense of various selections can be an essential choice element. An expensive option will frequently wear more gradually than a low-cost one. One could also have to think about the expense of optional features or add ons. Some shopping selections are more costly than others. Online shopping is frequently relatively inexpensive, but many individuals value the opportunity to take a look at and deal with the product in a store.
A comforter is a kind of bed linen that is made use of for spreading out as a bedspread or over thinner bedspreads and layers of blankets. A comforter is always bigger than the bed size and is indicated to cover the sides of the bed to create a wrapping effect. Such bedding are thick blankets that are often quilted and fluffy.
Silk is a natural item. For a body, it is far much better than other synthetic item. It contains smooth fibers which do not trigger any harm to the skin. Not only this, it is highly resistant to mechanical and thermal forces, and excellent for preserving temperature of body. A great deal of people have shared their experience saying that silk minimizes sweating.
Bear in mind that these option down comforters are not made with down and will not be as warm as a comforter made with the goose or duck feathers but, they come extremely close. The most significant gain from an option down comforter obviously it that you will remove the risk of allergies so, you do not have to feel that you are out of luck when it pertains to convenience. Also bear in mind that the higher the thread count the fluffier and lighter your comforter will be.
An assortment of patterns and colors that rightly complement the decoration of your bedroom, designs in geometric print, flower prints not to mention ethnic designs, meticulous crafting you can get Bedsheets that rightly matches your choices. Yes, you can make your rooms much better locations to live in, enhancing the entire looks, yet economically. Even the most lovely of bedsheets will not burn a hole in your pocket. The technique depends on purchasing them at online shops where maximum discounts are provided. It is not only discounts that matter; what you get will be exclusive. Not all retailers or online shops sell bedspreads that are unique, innovative, and exclusive. A search online will well serve your purpose of finding the right online shopping site.
It need not be hard to discover reduced bedding online. If you understand exactly what you want, you must be able to discover bedroom furniture and luxury bedding at prices that you can easily manage using the Internet to shop.
Know exactly what kind of sleeper will assist you at the same time. Are you a regular, warm or cold sleeper? A routine sleeper means that this individual does not get too hot or too cold while sleeping. A cold sleeper commonly get cold throughout the night while sleeping. On the other hand, a warm sleeper is one who gets exceedingly hot throughout the night.
It is a preconceived notion, that if you are a guy, in your bedroom, your mattress is on the floor, with a camouflage blanket and clothing in boxes. That is far from the truth. Take the married man's bedroom. If it is manly, that does not mean it can not be enjoyable, romantic and even attracting the girl of the house. It is much easier to create a bedroom to reflect a guy's designs that a woman will delight in than it is to create a "girly" appearance that a guy will delight in and be comfy with.
Popular satin features two distinct sides, the dull and the shiny surface area. Sewage systems must be particular to bring together garments on the appropriate side so regarding reveal the distinct radiance and gloss. Although satin utilized to be produced totally of silk, it is nowadays produced with acetate, polyester, and nylon among others. These materials offer a cost-effective ways to obtain the lustrous structure satin supplies.


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Publisher of Dawson, Forsyth papers now will also oversee The Times
Stephanie Woody
Stephanie Woody has been named group publisher for The Times, Forsyth County News and Dawson County News, all owned by Metro Market Media based in Gainesville. The announcement was made this week by Charles H. Morris Jr., owner of MMM.
In her new position, Woody will be responsible for oversight of newspapers, websites, magazines, newsletters, digital marketing and special events for the local media operations in Hall, Forsyth and Dawson counties.
Woody had previously been serving as publisher of the Forsyth and Dawson County News.
"The community news industry is changing almost daily as we consistently develop ways to provide our customers with the information they need while remaining financially viable as businesses," said Morris. "Stephanie has a proven track record of success and has shown she understands the changes taking place in the industry. We are fortunate to have her lead our three local operations."
Woody will be involved in both revenue generation and content decisions for the three properties. She has been part of the MMM family of businesses for 20 years, working in both Dawson and Forsyth counties.
"I'm incredibly excited to take on this new challenge. Our communities need strong news organizations, and it is vital that we fill that role. We have to explore new opportunities in digital platforms and social media to make sure we are giving our readers the news experience they prefer while maintaining the legacy of excellence created by our traditional newspapers in each market," Woody said.
"I look forward to becoming involved in Hall County and continuing to be a part of the Forsyth and Dawson communities. This area is my home, and I want to be a part of making it better," she said.
Woody is a native of Forsyth County, having graduated from North Forsyth High School before attending North Georgia College and State University. She and her husband, Robbie Woody, have four children.
At The Times, Woody initially will be focused on advertising, marketing and revenue generation before expanding into other areas of responsibility. In that capacity she will continue to work with Norman Baggs, who serves as general manager for MMM.


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Q: Losing response object in async callback Alright, I've been searching high and low, and apparently I am missing a trick.
Standard NodeJS/Express combination, doing a database call (thistakesalotoftime()) which may take a while to complete. If I get a new request while the first one is in progress, the render result from the first task is sometimes streamed to the response from request #2.
Mind, I am somewhat fresh to NodeJS, coming from a mostly PHP background. Never had that problem with Apache :)
var express = require('express');
var app = express();
var mysql = require('mysql');

function thistakesalotoftime(cb) {
  var connection = mysql.createConnection({
    host     : '127.0.0.1',
    user     : 'bob',
    password : 'uncle'
  });

  connection.connect(function(err) {
    console.log('connected as id ' + connection.threadId);
  });

  connection.query('SELECT 1 + 1 AS solution', function (error, results, fields) {
    if (error) throw error;
    cb(results.solution);
  });
}

app.get('/', function (req, res) {
  thistakesalotoftime(function(data) {
    res.send(data);
  });
})

app.listen(3000, function () {
  console.log('Example app listening on port 3000!');
});

It happens even with this extremely simplified app instance. Do please enlighten me. Any and all tips welcome.

redpajama_set_name: RedPajamaStackExchange


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Working at Morris Nichols
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Litigation Suite
Intellectual Property Paralegal
Morris, Nichols, Arsht & Tunnell LLP seeks a full-time Paralegal to support its Intellectual Property practice group. The successful candidate for the role will be technologically savvy, have an intellectual curiosity for the law, and will work well under pressure in a team setting. This individual will proactively seek out ways to bring broad support and greater efficiencies to a fast-paced, sophisticated practice.
Compiling, preparing and summarizing written materials for use by attorneys in all phases of bankruptcy litigation
Drafting of routine court documents for attorney review and approval
Preparation of pleadings and other docketed material for service and filing, with a particular emphasis on electronic filing of documents using the Delaware District Court's CM/ECF system and related filing platforms
Maintaining case files and tracking/managing document discovery
Updating and otherwise managing attorney calendars with particular attention to court dates and other relevant case-related deadlines
Indexing, tracking and otherwise controlling exhibits and other materials for depositions, hearings or trials
Performing general administrative support functions as needed to meet deadlines and further the objectives of the practice group
Required Education and Experience
Strong organizational and administrative skills; detail-oriented
Proficiency in Microsoft Office suite of business software products, including Outlook, Word, Excel and PowerPoint
Team-focused: willing to perform any level of support task in order to meet the needs of the practice group as a whole
Technologically savvy: able to quickly master various software programs (e.g., court filing software, law firm billing and time-entry software, legal/business research platforms)
Excellent oral and written communication skills; ability to communicate professionally with a wide variety of audiences, including Firm leadership and court personnel
Availability to meet the needs of a busy litigation practice, including regular overtime work when necessary to meet client and court deadlines
Self-motivated; strong ability to anticipate issues proactively and deliver a high degree of customer service
Proven track record of reliability and responsibility
Associate's degree or paralegal certificate required; Bachelor's degree in a relevant field preferred
Interested candidates may submit resume to Eileen Ricci, HR Manager, via e-mail at HumanResources@morrisnichols.com.
Morris Nichols is an equal opportunity employer and values the talents and perspectives of our diverse team of professional staff, which enhance our ability to successfully serve our clients. Qualified candidates will receive consideration for employment without regard to race, color, religion, gender, sexual orientation, gender identity, national origin, age, disability, genetic information, veteran's status, marital status, or any other basis protected by applicable law.
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Stretched out along the fence line, the peloton splinters into clumps of riders. Shadows tumbling down hillsides. Pedalling not against the gradient but the wind. Silhouettes scattered along the next ridge. The gate opening relay starts, the off road equivalent of through and off, keep riding, no time for gate faff, might even finish in daylight this year. The sea getting closer and closer, before turning along the river, inland again. Into the forest and regrouping at the first control.
Another climb before dropping to the sea for real. Laughing, dodging sheep, and chasing shadows across fields. The furthest point from the start line, but knowing it's not half way. There's a lot of toing and froing and up and down to get back, and we'll turn back on ourselves at least once, but not until we've stopped for a half way pint. Tradition.
In and out of the valley for the third time today. Up and along and down and around the coombes between this valley to the next. Faster, stronger, better mates are waiting for longer and longer at the top of each climb, "Crack on, I can find my way back". Hoping that emergency gel kicks in soon. Mates waiting on a corner. Again. Climbing through the woods up the singletrack to the last summit, into dusk. Flicking lights on (no daylight finish again this year) and settle on the drops. Just a tarmac descent and then time to collapse in the pub.
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How would you like it if someone were to wake up one day and tell you that, you can now borrow any amount of airtime from MTN and don't payback, will you love it? I'm guessing that's a yes from the looks of it. Since the day that the borrowme credit feature was established on MTN, we MTN users have used it times without number, and at a certain time, someone must have prayed for this airtime not to be paid back. Well, the time has come for that not to happen.
* First and foremost, migrate to MTN MPULSE by dialling *344*1#.
* Dial *344*5*2*1*1# and add CHILD NUMBER then, the self-care pin and gift N50 to the SIM that is owing and that line must also be on MPULSE.


text:
Modern Muse: Arpita Shah's Feminist Take on Mughal Portraiture, Arpita Shah, δημοσίευση Daily Art Magazine [28/11/2022]
Left: Arpita Shah Harr-Joht, Modern Muse series, 2019, Birmingham Museums Trust, Birmingham, UK; Right: Arpita Shah Nilupa, Modern Muse series, 2019, Birmingham Museums Trust, Birmingham, UK. Courtesy of the artist.
Staging an intervention in art history, and specifically in Indian miniature portraiture, Arpita Shah replaces male Mughal emperors with inspiring modern female muses of South Asian origin. As well as being sitters, these women are collaborators in this subversive series, in which they are elevated to the status of empowered subjects on their own terms.
Shah spent the earlier part of her life living between India, Ireland, and the Middle East before settling in the UK. This migratory experience is reflected in her practice, which focuses on the notion of home, belonging, and shifting cultural identities, often symbolized through clothing. Working between photography and film, Shah draws on Asian and Eastern mythology to explore issues of cultural displacement in the Asian diaspora.


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Centaur Funds
Centaur is a company that sells mutual funds with $9M in assets under management. The average expense ratio from all mutual funds is 3.36%. 100.00% of all the mutual funds are no load funds. The oldest fund launched was in 2005. The average manager tenure for all managers at Centaur is 2.13 years. The company offers investors 1 mutual funds, in terms of the number of individual fund symbols. About this page + View less
Centaur is a company that sells mutual funds with $9M in assets under management. The average expense ratio from all mutual funds is 3.36%. 100.00% of all the mutual funds are no load... Centaur is a company that sells mutual funds with $9M in assets under management. The average expense ratio from all mutual funds is 3.36%. 100.00% of all the mutual funds are no load funds. The oldest fund launched was in 2005. The average manager tenure for all managers at Centaur is 2.13 years. The company offers investors 1 mutual funds, in terms of the number of individual fund symbols. View more View less
DCM/INNOVA High Dividend Income Innovation Fund
$9.02 M
Centaur ETFs
Centaur In The News
https://mutualfunds.com/fund-company/centaur-funds/
Centaur Research


text:
Q: How to add "0" to multiple parts of text value in Field Calculator with Python I have values in a text column that are as follows:
000_100

100_200

...

1000_1100

1100_1200

I want it to read:
0000_0100

0100_0200

...

1000_1100

1100_1200

I want all values to have the same number of characters, for example 9. The numbers in the hundreds separated by the "_" need a "0" infront for this to be accomplished. I saw that I can use zfill to add a "0" to the beginning, but is there a way to specify where to put a second "0"?

A: The zfill string method, along with some basic string splitting/joining, will let you do this very slickly:
def update_text(old_text):
    new_text_parts = [num.zfill(4) for num in old_text.split('_')]
    new_text = '_'.join(new_text_parts)
    return new_text

If you would prefer not to bother with a function in the Field Calculator code block, you can simplify this (as Mike T commented) to a single expression:
'_'.join(num.zfill(4) for num in !field!.split('_'))

A: If you are using Field Calculator, you can create a new field of text type and calculate the field to be:
def updateValue(textField):
  newval = textField.split('_')
  if len(newval[0]) == 3:
    newval[0] = '0' + newval[0]
  if len(newval[1]) == 3:
    newval[1] = '0' + newval[1]
  total_val = newval[0] + '_' + newval[1]
  return total_val

Remember to use the Advanced block as outlined in the Calculate Field examples (look at the Using code blocks section).
updateValue(!your_text_field!)


text:
title: Now
permalink: now/
profile: true
published: true
---

Now

Updated 15 November 2018

- trying to figure out Jekyll, microblog workflows. 🤷♂
- living and working in Brookyn, NY
- shopping for winter parkas
- updating my Ramen hit list
- planning the next adventure

This Now page inspired by [Derek Silvers](https://sivers.org/nowff)

redpajama_set_name: RedPajamaGithub


Reduce counties to 40 and enhance Economic Blocs; Democratic Party of Kenya Memorandum to The Building Bridges Initiative read in part.
Two decades after Raila said Kibaki Tosha! His party is returning the favour by supporting Baba's 3 tier government proposal. Referendum seems unstoppable if what was given as memorandum to the building bridges initiative by Kibaki's DP party is anything to go by.
Reduction of Counties to 40, Move Nairobi County to National Government, Replace Senate with Official Opposition in Counties, Scrap Women Representative Position, Scrap Nominated MCA position says DP Party to Building Bridges Initiative in their memorandum.
For efficiency in operation as opposed to having many counties, DP calls for the support of the newly formed Economic Blocs which include: the North Rift Economic Bloc (NOREB), the Central Kenya Economic Bloc (CKEB), the Lake Region Economic Bloc (LREB), Jumuiya ya Kaunti za Pwani (JKP), South Eastern Kenya Economic Bloc (SEKEB), Frontier Counties Development Council (FCDC).
After the highly contested 2017 presidential election which ended up in Supreme Court and subsequent nullification of the presidential results which saw second round presidential polls, the political temperatures, hatred, protests, loss of lives including of children it was evident that something drastic need to be done.
The political leaders of the two largest parties had only two options either to sit down reason and get the country back to normalcy or continue taking hard-line and plunge the country into anarchy. In their own wisdom they choose to obey the good book in Isaiah 1:18 which say: Come now, and let us reason together, saith the Lord: though your sins be as scarlet, they shall be as white as snow; though they be red like crimson, they shall be as wool.
The two leader's president Uhuru Kenyatta and Hon. Raila Odinga formed a team to look into issues that has been diving the country along tribal, political and social lines every 5 years since the inception of multiparty democracy in Kenya in 1992.
The 14-member team was unveiled in late April last year to set a roadmap to for the realisation of the nine-point plan of the unity deal. The team was to look into the following key areas; ethnic antagonism and competition, lack of national ethos, inclusivity, devolution, divisive elections, safety and security, corruption, shared prosperity and responsibilities and rights. Ambassador Martin Kimani and laywer James Mwangi were appointed to head the team and represent the two leaders respectively.
The team comprised of Dr Adams Oloo, Agnes Kavindu, Senator Amos Wako, Ms Florence Omose, Professor Saeed Mwanguni, Mzee James Matundura, Major (rtd) John Seii, Bishop Lawi Imathiu, Hon Maison Leshomo, Senator Mohamed Yusuf Haji, Morompi ole Ronkai, Bishop Peter Njenga, RoseMoseu and Zacheus Okoth who were charged with responsibility of visiting different parts of the country and collect views of the public on the nine grounds of contention identified by the two leaders.
Since its inception the team has been conducting County meeting and collecting memoranda from individuals, groups, parties, communities and organizations as to how they intend the nine points to be addressed.
On 7th March 2019 The Democratic Party of Kenya ("DP") had an opportunity to present its memorandum to the team. They gave proposals of weighty matters that they considered if they are addressed the county could be saved of the ever threatening post election violence that has been recurring after every five years.
DP addressed expressly three issues put forward by BBI namely: Devolution, Shared Prosperity and Divisive Elections.
Commission for Revenue Allocation Formula; DP proposes a more equitable formula that is 80% focused on the population, 15% on equalization, and with all the other factors comprising the balance 5%.
Reduction of Counties; DP proposes that the country reverts to the 40 districts that existed in the 1963 constitution which would mean eliminating seven counties some being Bomet, Vihiga, Nyamira, Siaya,Migori etc. and adding back Thika to end up with 40 counties.
Nairobi County be moved to National Government; DP proposes that Nairobi should be run under the national government. In this case, the President of Kenya should be empowered to nominate a Cabinet Secretary or Principal responsible for its management.
Scrap Women Representative Position; DP proposes that the National government comes up with mechanisms that support and give women a level playing field to compete with men while running for elective positions.
Scrap Nominated MCA position; assuming each MCA takes home Kes. 400,000 a month including allowances, scraping the position will save the Wanjiku 3.7 billion annually plus vehicle grants close to Kes. 2.3 billion, the party said in their memorandum.
Youth Empowerment; DP, proposes a bill to be put into law for both National and County governments to provide bank guaranteed for AGPO tenders so that, upon completion and certification of the supplies or works, the youth can go to the bank and receive payment, the proposal read. Government conducts Public Sector Reforms which includes lowering of the retirement age for public servants from the current 60 years to 50 years.
Supporting SME Businesses; DP proposes that the government supports SME businesses through the following: Harmonize taxes and reduce overlapping licensing requirements, require that all banks lend at least 10% of their loan portfolio to SMEs at preferential rates, cap the amount of money banks can loan to government at 25% of their loan book, establish and gazette an SME development council constituted by Cabinet Secretaries (inter-ministerial) who are entrusted with respective functions of the SME Sector. DP proposes Business/ Employment Requirements; They proposes digitizing through government portal information relating to job applications by youth such that employers can check these documents online at no cost to the job seeker. Also HELB nonpayment penalties and interests for unemployed youth should be waived.
Constituency Development Fund (CDF) Allocation; DP proposes review of the CDF allocation to be based purely on population. They further say that regulation of government borrowing should be enacted. On Natural Resource Benefits, they proposes establishment of a framework that will possibly end the emerging conflicts among the counties amidst demand for fair share of natural resources that fall within their territories.
Finally on Divisive Elections; DP's reference to divisive elections addresses not only opposition demands for electoral justice, but also an electoral system that greatly favors incumbency and installs a governing system built on ethnical alliances. Also, a faulty system that is sadly a winner takes all.
DP proposes that we maintain a Presidential system of government but expand the executive branch of government by re-introducing the office of the Prime Minister and two deputies, a proposal that could be key to achieving a more inclusive top leadership. All the five positions with a regional balance should be in the ballot as the lineup for the presidential candidate. "Recent history of the country shows faster development can be achieved with establishment of a more regionally balanced government" the party alluded.
In addition to this, DP proposes the runner's up in the presidential election to take up the role of the official Leader of Opposition which will command a paid package. The leader of opposition will pick a "shadow cabinet" from MPs of the opposition parties. The role of the shadow cabinet will be to follow and examine the work of each government department and develop policies in their specific areas as well as hold the government accountable to the public. The opposition will also represent an alternative government and is responsible for challenging the policies of the seating government and coming up with alternative policies where appropriate.


Professional malpractice refers to more than lawyers or doctors. It also includes accountants.
"Most people, when they hear the words 'professional malpractice,' think it refers to lawyers or doctors. While it may well refer to them, it is also a term used when talking about accounting malpractice. Simply put, accounting malpractice happens if any accounting professional is negligent in the performance of their duties," said Stephen M. Ozcomert, who handles personal injury cases, accidents, and malpractice law in Atlanta, Georgia.
To further explain professional standards for various individuals who are certified to practice, it's vital to know that the institutes that certify these professionals have a list that outlines what the standard of care is for their members to provide to their customers. The list says what standards of care need to be met to protect the public from harm, deceit, malfeasance, etc.
This isn't to say that all accountants, lawyers or doctors will abuse their positions, because most professionals are trustworthy and reliable. If the standard of care is not met in a profession, this may be considered negligence.
"In a case involving accounting malpractice, the plaintiff has to show the defendant was negligent and didn't meet the level of care expected – the common or customary care – in the accounting profession. An example of that would be the accountant not filing a client's tax return on time or not properly filling out the return and it results in a financial penalty to the client," Ozcomert said.
Generally speaking, there are four elements a plaintiff needs to meet to be successful in an accounting malpractice lawsuit. It must be shown that the accountant had a clear responsibility to the client; that the accountant didn't act responsibly; that the client was injured and that the accountant's actions were the proximate cause of the injury.
Not all cases are clear cut and straightforward and for this reason, if someone feels they have been financially harmed by the misdeeds of an accountant, talk to an Atlanta malpractice lawyer.
"You need to know your rights, what options you have and whether or not your potential case is actually malpractice or not, as some cases may not be malpractice. If you have questions about what you feel is a malpractice case, call me and we can discuss the details," Ozcomert said.