text:
\section{Introduction}

The NICMOS UDF Treasury observations were designed to complement and enhance
the ACS optical UDF observations.  They provide an extension in wavelength
to $1.6 \micron$ and provide two additional bands which extend the rest band
energy and morphology measurements to longer wavelengths.  They also provide
the potential for viewing objects at redshifts beyond 7.5
where Lyman line and continuum absorption quench the flux in the ACS bands.
The additional wavelength coverage also helps distinguish between the influences
of age, metallicity and extinction.  As with previous deep field catalog publications
(\citet{wil96}, \citet{thm99} and \citet{beck04}) this paper is intended primarily
as a description of the observations, data analysis and source photometric properties
rather than a scientific evaluation of the implications of the observations.

Due to the relatively small field of the NICMOS camera 3 used in this program ($51\arcsec
\times 51\arcsec$), only a subsection ($144\arcsec \times 144\arcsec$) of the optical UDF was
covered.  This was done with a 3x3 tiling of the NICMOS images.  The NICMOS images extend a
few arc seconds beyond this subsection but at a significantly  decreased signal to noise.
All of the individual processed NICMOS images are available in the HST treasury archive
(MAST\footnote{http://archive.stsci.edu/prepds/udf/udf\_hlsp.html}) as are the raw images in the main HST archive.

The primary purpose of this paper is to provide a very detailed account of the data
reduction steps used to produce the treasury images and catalog stored in MAST
 so that users are aware
of the pedigree of the data and can reproduce the analysis if they wish.  Other users
may wish to alter the reduction steps if they prefer other choices than the ones made
here.  Finally we wish to convey the attributes and limitations of the catalog of sources.
Users in particular who wish to extract the faintest sources from the data will want
to use more aggressive extraction techniques than we have utilized in producing the
treasury catalog.

\section{Observations} \label{s-obs}

The NICMOS observations in the UDF (HST GO/9803) are centered on the
position 3\fh 32\fm 39.0\fs, -27
\arcdeg 47\arcmin 29.1\arcsec (J2000) at approximately the center of the ACS UDF
observations (see image at http://www.stsci.edu/hst/udf/parameters/\#Pointing).
The images lie in a 3x3 grid with centers separated by 45 arc seconds.  The
grid centers are dithered by 5 arc seconds in a 4x4 square pattern tilted at
22.5 degrees to the x axis of the images to reduce the effect of
intra pixel sensitivity variations.  The tilt of the pattern also
produces dithers that have fractional pixel offsets in the detector array.

The NICMOS UDF program consists of 144 orbits broken into two epochs: i) August 30,
2003 to September 14, 2003 and ii) November 2, 2003 to November 27, 2003.
The scheduled start of observations in mid August 2003 was delayed by a safing
of the NICMOS Cooling System (NCS) just prior to the beginning of observations.
All reference files such as flats and darks were obtained subsequent to the safing
event. The epochs are separated to enable the detection of SN Ia candidates and
to provide enough SAA crossing free orbits for high sensitivity. The images in
the two epochs are rotated by 90 degrees to accommodate the roll restrictions of the
spacecraft.  In the first epoch the y axis of the NICMOS camera 3 was oriented
40.925 degrees east of north, and in the second epoch 130.925 degrees east of north.
These orientations are the same as the two ACS orientations in an effort
to align the NICMOS and ACS images without the need for a rotation.  The
drizzled ACS images in MAST, however, were produced with the standard north
up and east left orientation.  The version 2 NICMOS treasury images supplied
to MAST are also oriented with north up unlike the version 1 NICMOS image.
The NICMOS version 2 images have been aligned with the ACS version 1 image
so that researchers can utilize the complete set of ACS and NICMOS images
without realignment or rotation, see \S~\ref{ss-dp}.

Each orbit contains a F110W and F160W band SPARS64, NSAMP = 24, 1344 second integration.
Figure~\ref{fig-qe} shows the total response of the two bands, including the detector
quantum efficiency. The F110W integration always preceded the F160W integration. Three orbits
comprise a single visit with the location of the image specified by a POSTARG from the
central reference position.  It is possible that the F160W images from the first orbit
of a visit may have received a small amount of earthshine in the last readout of
the NSAMP = 24 readout sequence.
This is due to the guide star acquisition time on the first orbit of the visit which takes
longer than the guide star reacquisition in the subsequent 2 orbits of the visit.
No correction has been made in the Treasury images for this effect. The three by three grid
was completed in three visits with each visit representing a 3 image strip stepped in the
detector x direction.  The visits were ordered to finish each 3 by 3 grid before starting
another and always in the same order.  This was done to maximize the time coverage for a
supernova event, should one occur. After the initial delay due to the NCS safing all of the
visits occurred in their expected order.

Subsequent analysis of the images indicated that the second half images were not an
exact repeat of the first half images.  In the second half 3 of the visits replaced
a center image with an image on the right hand side of the 3 image strip.
Tables~\ref{tb-pos1} and \ref{tb-pos2} list the visits with T, C, B indicating
top, center and bottom
for the epoch 1 visits and L, C, and R indicating left, center and right for the 2nd
epoch visits.  These refer to left, right, top and bottom of the NICMOS images in
their standard x and y orientations.

\section{Data Reduction}

Previous papers \citep{thm99,thm01,thm03} described details of the data reduction
procedures for deep field NICMOS observations.  Some of the procedures required
revision for post NCS installation data.  These changes and the provision of the
reduced images as a public Treasury Program data products warrants a detailed
description of the data reduction procedures even though some aspects have been
covered in the publications cited above.  All of the procedures utilize the
commercial Interactive Data Language (IDL) \footnote{IDL is a registered trademark of
Research Systems Incorporated, a Kodak company.} software and the IDL based Fits List
Calculator (FLC) \citep{lyt99} software.  These procedures were
developed primarily by RIT and ES for previous NICMOS observations.

\subsection{Basic Reduction}

The initial steps in the data reduction take advantage of the nondestructive readout
capability of the NICMOS detectors.  NICMOS detectors are read out at specified intervals
without erasing or altering the image.  This ability allows several data reduction advantages
not shared by CCD detectors.  The SPARS64 read pattern with 24 samples provides readouts
evenly spaced by 63.998 seconds after the first 2 samples that are spaced by 0.303 seconds.
All of the images in the NICMOS UDF observations were taken in this mode.  The steps
described in this section are done automatically in batch processing with no
interaction.  This is roughly equivalent to the STScI pipeline processing.

\subsubsection{First Read Subtraction}

The first step in the data reduction is the subtraction of the image obtained
in the first read from all subsequent reads.  This step eliminates the KTC
noise that is present in each of the individual photodiodes at the beginning of
an integration.  The number of reads carried through in the final processing is
then 23 reads rather than 24 after this step.

\subsubsection{Dark Current Subtraction}

After the first read subtraction the dark current image is subtracted from each of the
reads.  This is a very important step as the NICMOS detectors have dark current images with
very significant structure.  This structure is larger in magnitude than the signal from most
of the galaxies in the image.  The dark images are constructed from integrations in exactly
the same mode as the observations but with the cold blank filter in place.  This step differs
from the STScI pipeline that uses ``synthetic darks'' calculated from parameters developed
during the operation of NICMOS \citep{mob04a}.

\subsubsection{The UDF NICMOS Dark}

The NICMOS UDF dark is a median dark image obtained from dark integrations taken during the
earth occultation period in each of the orbits assigned to the NICMOS UDF program.
Operational constraints prevented dark integrations on 2 orbits but the remaining 142 dark
integrations were used to construct the median images.  There is a median dark image for each
read constructed from the medians of all of the dark images for that particular read.

Between visit 34 and visit 35 of the 48 visits in the NICMOS UDF program, the temperature set
point on the NCS was reduced by 0.1 K to compensate for the warmer conditions encountered
during the period when the earth's orbit is closest to the sun.  There was concern that this
set point change would alter the nature of the NICMOS darks since it is known that the darks
are temperature sensitive.  Comparison of a median of the darks taken before the set point
change with the median darks taken after the set point change did not reveal any differences
above the noise level in the observations.  The NICMOS UDF dark was therefore constructed
from the median of all of the darks before and after the set point change.

\subsubsection{Warm Pixels}

In the NCS era the NICMOS detectors operate at a significantly warmer
temperature than the previous operation with solid nitrogen cryogen.
There are several advantages to the warmer detector temperature but a
disadvantage is an increase in the number of ``hot'' and ``warm'' pixels.
Hot pixels are pixels with a dark current high enough to reach the
nonlinear response region in a 1000 second integration.  These pixels
are included in the list of bad pixels described in \S~\ref{ss-badpix}.
More difficult cases are the warm pixels that have elevated dark
current but not elevated enough to become nonlinear in a normal integration.
These pixels can be corrected through the dark image subtraction for
most types of integrations. The degree of elevation, however, is very
temperature dependent, and will vary over the normal range of temperature
variations inherent in the NCS operations.  The elevated dark current is in
many cases much larger than the signal encountered in faint galaxies.

The warm pixels contribute noise in two ways.  First is the normal
Poisson statistics inherent in a steady dark current and the second
is incomplete removal when the dark current varies from the median dark
current measured by the NICMOS UDF dark.  The presence of these
varying warm pixels altered the previous data reductions in two ways.
The first was the introduction of a more aggressive bad pixel list for
the UDF observations and the second was the introduction of post
processing procedures to detect the presence of warm pixel signals
and to separate them from true sources.  These procedures are described
in \S~\ref{ss-wpc}.

\subsubsection{Linearity Correction}

During thermal vacuum testing prior to launch and in cycle 7 the
linearity of each pixel was measured.  The point a which nonlinearity
set in and coefficients for a polynomial fit after that point were
determined for every pixel.  In the linearity correction stage
the signal of every pixel is checked to see if it is in the nonlinear range.
If it is above the linear range its signal is corrected using the
determined coefficients of the polynomial fit. If it is in the signal
range that is deemed uncorrectable it is marked as saturated and only
the reads occurring before saturation are used in the analysis. New
coefficients are being determined for post NCS operation. However, none of
the galaxies in the UDF reached signal levels requiring correction therefore
linearity is not an issue in this analysis.

\subsubsection{Cosmic Ray Removal}

A cosmic ray event produces a sharp jump in signal intensity in the first
readout after the event.  Most events do not saturate the pixel and
subsequent readouts continue to monitor the incident flux.  At this point
in the analysis the readouts are stored as delta signal levels
between each readout.  The signal ``ramp'' is reconstructed by adding the
deltas together. The first step in cosmic ray detection is a linear fit to
the signal ramp, which will be a poor fit to the data if there is a cosmic
ray jump.  The residuals to the fit will be increasingly negative with a
sharp transition to positive after the event. The cosmic ray detection
procedure looks for the negative to positive transition as a
signature of a cosmic ray hit.  If it detects a residual transition above
the level expected from noise it removes the delta signal between the two
readouts before and after the event, recalculates the signal ramp and
fits a new linear solution.

The cosmic ray procedure rechecks the ramp to see if there was another cosmic ray hit
and removes the proper delta signal if one is detected.  If there is still a
detectable cosmic ray signature after the second refit the pixel is marked as bad
and no further correction attempt is made.  If the signal is saturated after the
cosmic ray hit only the signal obtained before the event is used in the analysis.
The final recorded signal is the value of the slope of the linear fit to the
signal ramp in adus per second.  Cosmic ray hits that occur in the 0.3 seconds
between the first and second read are detected as fits that do not intercept
zero, recalling that the first read is subtracted  from second so that the
second read is the first point in the ramp.  These hits do not affect the
calculated slope but are marked as cosmic ray hits in the data quality array
discussed later.

\subsubsection{Quadrant Bias Correction}

Each quadrant of the NICMOS detectors has a separate output amplifier to transmit
the analog signal to an A/D converter.  This was done to prevent the loss of an
entire detector array if there was a failure of an output amplifier.  As a side effect
of this design decision a small DC bias offset can occur between the 4
detector quadrants.  Although the offset is small, the effect is significant
relative to the faint galaxy signals in the UDF and can cause unreliable outputs
during the drizzle process.  Since there is significant sky background from
the zodiacal light it is difficult to determine the offset amount from a
simple inspection of the image.

The quadrant bias is removed via a procedure based on the bias removal
procedure developed by
Mark Dickinson as part of the STScI NICMOS team \citep{mob04b}.  The procedure utilizes the
flat field imprint produced on the DC signal by the flat field correction process.  Any flat
DC bias will be modulated by the variations in the flat field.  The process successively
subtracts a DC bias from each quadrant before it is flat fielded, applies the flat field and
then picks the bias subtraction that produces the minimum variation in the quadrant.  The
variation in the quadrant signal is measured by a gaussian fitting to the histogram of
pixel values in the images. To avoid any residual corner glow from the amplifiers
or other quadrant boundary anomalies only the quadrant region that is at least
20 pixels from the quadrant edges
is used to determine the quadrant bias. Bad pixels are also masked out to prevent them from
dominating the variation signal.  The output of variations from each bias correction is
fit by both a second order polynomial and by 5 point smoothing of the output.
In the cases encountered in the UDF images they are essentially identical.  The minimum
variation bias correction is selected as the minimum of the smoothed output.

Both positive and negative bias are subtracted as the bias can have either a positive or
negative value.  The bias subtraction used biases between -0.15 and 0.2 adus per second
incremented in 0.001 adus per second.
The procedure returns a warning if any bias corrections do not find a minimum in the provided
range of biases.  All of the UDF quadrant images had minimums within the range of biases in
the procedure.  An example of the gaussian width versus subtracted bias is shown in
Figure.~\ref{fig-bias}. Visual inspection of the images before and after background subtraction
confirmed that there were no detectable remaining quadrant bias offsets.
The procedure would be unnecessarily time consuming for images where
the objects were significantly brighter than the offsets and might not work in images where
the width of the pixel signal histograms are dominated by source variations rather than
noise.  Neither is the case for the UDF.  In reality the IDL code for this procedure
actually performs both the flat fielding and bad pixel correction.  These procedures,
however, are discussed individually in the following sections.

\subsubsection{Flat Fielding}

NICMOS flat fields are created internally.  The ``beam steering mirror'' internal
to the instrument lies at a optical pupil and is used to correct the spherical
aberration of the HST primary.  It can be illuminated from behind and the
reflective coating of the mirror was adjusted to be about $0.01\%$ transmitting
producing an illuminated pupil for flat fielding.  Flat fields are produced at
regular intervals during operation in all filters of each camera.  We used F110W
and F160W camera 3 flat field observations created on Sept. 9, 2003 from
proposal 9640.  The flat fields are analyzed in the identical manner as described
in the preceding steps.  The STScI reference flat fields were not used in this
analysis because they were based on flat fields observed previous to the NCS
safing event.

One of the effects that the flat field corrects is a slight vignetting along the
lower edge of camera 3.  For two reasons this correction was not effective in
the UDF fields.  First, the net effect has two components, vignetting of the
incoming astronomical flux and emission from the vignetting component which is
thought to be the edge of the mount for the field division mirror for camera 3.
For bright sources the vignetting is the dominant effect and the flat field
properly corrects the field.  For very faint images, such as the UDF, emission
can be a significant component which varies due to the natural temperature
variations in the aft shroud. Second, variations in geometry due to temperature
changes can affect the degree of vignetting.  Again the effect is slight for
bright sources but can be significant for the UDF signal levels.  For
these reasons the lower 20 rows of all UDF images were masked off in the drizzle
procedure described in section~\ref{ss-dp}.

\subsubsection{Bad Pixel Correction} \label{ss-badpix}

Bad pixels are defined as pixels with quantum efficiencies less than $10\%$ of
the average QE or with dark currents high enough to reach nonlinear signal
levels in 1000 seconds or less. In the post NCS era the list of bad pixels
has increased over the cycle 7 listing due to the higher temperature of the
detector creating more high dark current pixels.  Pixels which satisfy neither
criterion but are highly variable in their
dark current were also added to the list.  All bad pixel signals are replaced with the
median of the eight pixels surrounding them.  In the case of adjacent bad pixels that
number is reduced by the number of adjoining bad pixels.  All bad pixels are listed
in the data quality array which is an extension of the image or SCI array.
Table~\ref{tb-dqc} gives the decimal codes for each of the steps described above.
They are each a single, different, binary bit, so each combination of actions
performed on a pixel has a unique output code.  Note that only a few of the 16 bits
available for pixel actions are used in this analysis.  A full set of data quality
codes can be found in the NICMOS Handbook but only the ones listed here are used
in the NICMOS UDF Treasury data.  Even for the codes used they may in many cases
differ from the codes returned by the STScI pipeline analysis.  As an example, the
lists of bad pixels differ between the pipeline analysis and the analysis described
here.  Note that the data quality extensions only exist for the individual NICMOS
UDF images.  The drizzle procedure does not preserve these codes since many input
pixels contribute to a single drizzled output pixel.

\subsection{SSA Persistence Correction}

The program planners at STScI were careful to schedule the NICMOS UDF observations
in orbits that were not impacted by SAA passages.  None of the NICMOS UDF images
required any correction to remove SAA persistence.

\subsection{Earthshine Detection}

As mentioned in \S~\ref{s-obs} the last read of the first orbit in a visit may have
encountered increased earthshine due to the longer period of delay in a guide star
acquisition rather than reacquisition.  This would only affect the F160W images as
the readout sequence was always F110W and then F160W. We tested for this effect by
plotting the median of the delta increase in the F160W images as a function of
readout. In a few cases we saw a detectable rise in the last readout of the
first orbit in a visit.  The effect appeared minor enough that no correction
was attempted.

\subsection{Background Subtraction}

The primary background source in the UDF is zodiacal emission which is relatively
uniform across the small UDF field of view.  A median image of all of the images in
the F110W and the F160W filter determines the background for that filter.
The background is simply subtracted from each image in the proper filter.
The median image is extremely smooth with no indication of any residual
source structure.  This is similar to the results in the NHDF \citet{thm99} where
the spacing between images was much smaller than in the UDF. Since the
zodiacal backgrounds can be time dependent the first epoch and second epoch
background subtractions were done independently.

\subsection{Residual Bias Correction}

The removal of quadrant biases and the background subtraction should result in an
image that has a median value of nearly zero since most of the pixels in the image
are not in sources that are above the noise level. The minimums of the quadrant bias
curves in Figure~\ref{fig-bias}, however, are rather broad.  To compensate for this
each quadrant of every image was set to zero bias.  The bias was determined from
the median of the portion of the quadrants which
is 40 rows and columns away from the edge to avoid any contamination from residual
corner glow or uncorrected vignetting. Any detected bias was subtracted from the
entire quadrant to produce a zero bias image.  Inspection by eye of the zero bias
images did not find any detectable quadrant offsets.

\subsection{Warm Pixel Correction} \label{ss-wpc}

A new effect encountered in the NICMOS UDF images is warm pixel variation.  At
the higher operating temperature of the NCS cooling system, the NICMOS detectors
have more warm pixels than during the cycle 7 operation with solid nitrogen cryogen.
A warm pixel is defined as a pixel with an elevated dark current which is not high
enough to be declared a bad pixel by the criteria defined in \S~\ref{ss-badpix}.
For most applications warm pixels are adequately corrected by dark subtraction
but for the UDF they present two problems.  The first problem is that their dark
current is temperature sensitive and the NCS has slight temperature variations
within an orbital cycle and within a 24 hr day due to power cycles in HST operation.
The variation is small but is significant relative to faint UDF sources.  The
second problem is that the Poisson noise of the signal at the end of an integration
is also significant relative to a UDF source.  The individual images have single
or sometimes double pixels with signal levels of either positive or negative
high contrast relative to the surrounding pixels from the warm pixel effect.

Warm pixels are identified by their contrast with neighboring pixels.  The PSF of a point
source centered on a pixel provides a maximum contrast for a real source.  Pixels with
contrasts significantly greater than this are due to warm pixels.  The contrast was
computed for each pixel compared to the 8 pixels adjacent to the pixel.  A pixel is set
equal to the median of the 8 pixels if 3 conditions are met; i) its value is higher
than the 3$\sigma$ noise value in the image, ii) its value is higher relative to
the median of the adjacent pixels than a preset contrast value and iii) the value of
the surrounding median is less than a preset number of standard deviations.  The last
condition prevents peak clipping on point objects.  The contrast values were set to
6.0 for the F160W image and 8.0 for the F110W image which has a narrower PSF.  The
standard deviation limits were set to 2.5 for the F160W images and 2.0 for the F110W
images.  Any corrected pixel has the bad pixel flag set in the DQ image extension
so it can be identified.

\subsection{Drizzle Procedure} \label{ss-dp}

The treasury mosaic images were produced using the DRIZZLE procedure with
context images \citep{fru02}. The offsets for the NICMOS images were
determined by registering the NICMOS F110W images onto the ACS F850LP UDF
image in the HST archive which has a north up orientation and $0.03 \arcsec$ pixel
scale. The significant overlap between the two filters greatly reduces any errors due to
color dependent morphology, however, see \S~\ref{sss-psf} for an assessment of the
accuracy of the alignment.  The NICMOS F160W images which always immediately followed
the F110W images in an orbit were assumed to have the same offset as the F110W images
preceding them.  The ACS image was reduced to $0.09 \arcsec$ pixels by a simple 3x3
pixel addition of the image.  Individual NICMOS F110W images were then produced with
a drizzle PIXFRAC parameter of 0.6 and a SCALE parameter of $0.09/0.202863$ to
produce $0.09\arcsec$ output pixels. The denominator in the scale factor is the
pixel size of the distortion corrected NICMOS pixel.
The geometric distortion coefficients \cite{berg04} are given in Table~\ref{tb-dis}.
These coefficients are the constants for a cubic distortion correction of the form

\begin{equation}
xdist = a1 + a2\times x + a3 \times y +a5 \times x \times y + a6 \times y^2 + a7 \times x^3 + a8 \times x^2 \times y + a9 \times x \times y^3
\end{equation}

\noindent and an identical equation in b coefficients for the y position that governs
the placement of the pixels.  Compared to other HST instruments the correction is
relatively small.  The main component is the difference in plate scale between
the x and y directions due to a slight tilt in the camera 3 focal plane relative
to the plane of the detector. The tilt is due to the curvature of the focal plane.
Each $0.09 \arcsec$ NICMOS was rotated to a north up orientation using the ORIENTAT
value in the image header.

A three step process provided the positions of each F110W image relative
to the ACS F850LP image.  The first step was to shift the NICMOS images
to the positions indicated by their World Coordinate System (WCS) position
in the headers.  The second step was a non-interactive chi squared
minimization of the differences between the bright objects in the NICMOS
image and the nearest corresponding bright ACS object.
The ACS positions were determined with SE in the ABSOLUTE mode with the
threshold set at 0.03 ADUs per second.  Positions in the NIMCOS images
were also determined with SE in ABSOLUTE mode with the threshold set at
0.01 ADUs per second.  Both of these thresholds are quite bright to insure
a low source count per area.  This made the likelihood of wrong object
matching low.  The shifts were limited to plus or minus 10 pixels in
the X and Y directions in single pixel steps. The average position shift
in this step was on the order of 2 to 3 $0.09 \arcsec$
pixels.  The final shifts were determined by a similar chi squared minimization
of interactively selected NICMOS objects.  Usually three objects were selected
based on compact size and sufficient signal to noise.  Whenever fully visible
in a NICMOS image, the star near the center of the image was used as one of
the objects.  The more eastern star image appears to have contamination due to
a faint nearby object visible in the ACS images. Shifts in this step were
limited to plus or minus 1 pixel in 0.1 pixel steps.  The average position
adjustment in this third and final stage was 0.2 to 0.3 $0.09 \arcsec$
pixels.  These final positions were then used as the input to the drizzle
procedure.

\subsubsection{Individual Image Masking} \label{sss-msk}

The F110W and F160W images each have a general mask used in the drizzle process.  The
masks mask out the bottom 20 rows of the image to eliminate the partially vignetted
region at the bottom of camera 3.  They also mask out a portion of the upper right
hand corner of camera 3 where there is an area of rapidly changing quantum efficiency.
In addition they also mask out the known bad pixels and areas where some particles,
termed grot, cover detector pixels.  The large number of dithered images greatly
reduces the impact of the masked areas.  The masks are available in the STScI NICMOS
UDF Treasury version 2.0 archive in MAST.
Several of the images had artifacts such as satellite passage streaks that required
masking.  Individual masks were made for 20 F110W images and 31 F160W images.
Table~\ref{tb-msk} lists the masked images.  The masks are contained in the NICMOS
version 2.0 Treasury submission.

\subsubsection{Cosmic Ray Persistence} \label{sss-crp}

A few of the masks remove spurious objects created by cosmic ray persistence.
If a cosmic ray hit before the start of an integration produces a shower of particles,
cosmic ray persistence can give a resolved source that appears in the first F110W
image after the hit and more weakly in the following F160W image.  This exactly mimics
a high redshift galaxy.  The ACS image has no signal and the F110W-F160W color is blue.
The signature of this spurious event is that the source only appears in one set of
F110W and F160W images.  All of the NICMOS sources that did not have ACS counterparts
were inspected in each image.  Two spurious cosmic ray persistence sources were found
and masked out (see also \S~\ref{ss-igi}).

\subsubsection{Point Spread Functions} \label{sss-psf}

Unlike the deep NICMOS observations in the NHDF, the HST secondary mirror was not
adjusted to bring the camera 3 images into sharp focus.  The photometric gain was
not considered high enough to request the adjustment which would have put the
parallel ACS images significantly out of focus. The PSF at the focal plane of
camera 3 is therefore broader than the diffraction limited PSF observed by
NICMOS cameras 1 and 2.  To determine the PSFs of the UDF images two
measurements were performed.  The first was to measure the PSF of the bright
star at x = 1897.26, y = 1610.34 with Gaussian fitting.  The second bright star
at x = 1246.12, y = 1420.42 appears to be double with a faint companion.
The second measurement involved 42 camera 3 images in F110W
and F160W of the photometric calibration star P330-E taken after the NCS safing
event.  These were part of the Prop. 9995 calibration program of Mark Dickinson.
These images were drizzled in the same manner as the UDF images.  The PSF of the
drizzled F110W and F160W images were measured by the same Gaussian fitting as for
the UDF stellar images.  The results are listed in  Table~\ref{tab-psf} which
gives the measured major and minor axis FWHM values.  Table~\ref{tab-psf} also
gives the results of performing the same exercise on synthetic images produced
with the Tiny Tim software \citep{kri04} for the camera 3 focus utilized in the UDF
observations. The Tiny Tim and calibration star PSFs agree quit well but
the measured UDF stellar values are between 0.06 and 0.1 arc seconds wider.
This may reflect the accuracy of the mosaic position calculations.
The widths measured in an independently reduced image (see \S~\ref{ss-igi})
are very similar to our UDF image widths.  Any researcher that requires
extremely accurate object shapes, such as for weak lensing, may wish to
go to the original single images for size and shape measurements. Those
researchers should apply the geometric distortion corrections listed in
Table~\ref{tb-dis}.

\section{Image Size and Weight}

The full drizzled image does not have a uniform integration time over the image.
In particular the edges of the image have only one integration as opposed to the
average 16 integrations for the interior of the image.  The full drizzled image
has a size of 3500 by 3500 pixels, the same size and orientation as the ACS images
reduced to $0.09 \arcsec$ pixels. Experience with the NHDF images indicated that
source extraction in regions with less than half of the
average integration time was not profitable except in special cases
where a particular object near the edge of the total image required analysis.  Users
of the treasury image should be aware that the edges of the image have roughly a
$\sqrt{2}$ lower signal to noise than the central regions.  The exact weight for all
pixels is given by the weight images included in the treasury archive.  There are
some regions where the images overlap that have much higher integration times.  Users
who need a uniform selection criterion for analysis should be aware of these
differences in weight.

\section{Source Extraction}\label{s-se}

Source extraction in the science image was performed with the source extraction
program SExtractor (SE) version 2.3 \citep{ber96} in the dual image and rms
image mode. The source extraction includes the 4 ACS UDF images as well as
the NICMOS images.  The ACS extractions provided the source reality check
described in \S~\ref{ss-acs} and are included in the treasury catalog.

\subsection{Noise} \label{ss-noise}

Figure~\ref{fig-ns} shows the histograms of all of the pixel values in the
F110W and F160W image.  The majority of the pixels are well fit with a gaussian
centered on zero. The offsets from zero are $~7\times 10^{-5}$ ADUs/second for
both images. The positive tail deviating from a gaussian is the contribution
from the true sources in the field.  The width of the gaussian fit is an
indicator of the noise.  The gaussian fit gives noise levels of
$3.5\times 10^{-4}$ ADUs per second for the F110W image and
$3.7\times 10^{-4}$ ADUs per second for the F160W image.  This corresponds
to 0.55 and 0.58 nanojanskys respectively.  This is an underestimate of the
true noise as is partially indicated by the excess over the gaussian on the
negative side of the fit.  The drizzle procedure is known to introduce
correlation to the noise \citep{fru02}. \citet{fru02} give an expression for
the noise increase factor which gives a factor of 1.8 for the drizzle PIXFRAC
and SCALE parameters used in the images.  This yields $1\sigma$ noise values
of 1.0 and 1.2 nanojanskys per pixel.

Figure~\ref{fig-apn} shows the histograms of the signals in a densely packed grid
of apertures of the same diameter as the three apertures, 6, 11 and 17 pixels,
used in the source extraction. The 175x175 grid is regularly spaced on 20 pixel
centers to provide 30,625 apertures.  Most of these do not contain sources
but the positive tail in Figure~\ref{fig-apn} indicates apertures with
positive source flux. The large number of apertures that fall off the
NICMOS image are not included in the analysis. The histograms are
roughly Gaussian shaped but only the 6 pixel aperture
histogram has an easily measurable FWHM.  The $1\sigma$ noise derived from the
FWHM is $3.7 \times 10^{-3}$ ADUs per sec for the F110W image. Similar results
were obtained for the F160W image. The expected noise from the
individual pixel noise described above, including the factor of 1.8, is
$3.5 \times 10^{-3}$ which is comparable to the measured value.  To the degree
that the aperture noises are truly Gaussian distributed, this indicates
that factor of 1.8 is a reasonable figure to account for the correlated noise
and that the aperture noise is approximately equal to the square root of the
number of pixels in the aperture times the individual pixel noise.  The
measured aperture noise in Janskys from the histogram is $5.8 \times 10^{-9}$
which is equivalent to an AB magnitude of 29.5 for the $0.54\arcsec$ diameter
aperture. The $5\sigma$ AB magnitude is 27.7 which we will take as the
appropriate value independent of source noise.
In observations of the NHDF-S \citet{lab03} with ISAAC on the VLT
found $1\sigma$ aperture noises of 28.6 and 28.1 for the J and H bands
with a $0.7\arcsec$ diameter aperture which gives $5\sigma$ values of
26.7 and 26.2.
The minimum number of contiguous pixels for a real source is set to 7 in
the extraction procedure.  The $5 \sigma$ noise for a point source detection
is then the noise in the 7 pixel aperture which gives AB magnitudes
of 30.35 and 30.15 for the F110W and F160W filters respectively.

\subsection{Detection Image}

SE in the two image mode uses a detection image to determine the position
and extent of sources.  The individual image source extraction is then
performed on exactly the same positions and regions determined from the
detection image.  The SE parameters regarding source geometry such as area
and ellipticity are determined by the detection image.  The detection image
for the treasury catalog is the simple sum of the F110W and F160W science
images.  Even though it is the sum of two images, the detection image has a
significantly lower signal to noise than any of the ACS UDF images except
for sources that are extremely red.  Users that are interested in the
NICMOS limits on faint ACS UDF sources should use the ACS images as the
detection image to perform the source extraction on the NICMOS images.
On the other hand very red sources may appear only in the NICMOS images.
Since we wish to provide an infrared catalog we chose to use the NICMOS
images for extraction.  Note that by combining the two NICMOS images there
is a bias against the very reddest sources that might only appear in the
F160W image.

\subsection{RMS Image} \label{ss-wi}

SE utilizes a rms image to determine the detection limit of a pixel signal when
operating in the RMS mode used in the treasury version 2.0 catalog.  The
drizzle procedure produces an observation time weight map that measures
the total integration time for every pixel but the weight map does not
take into account the large variations in quantum efficiency over the face
of the NICMOS detector array.  To account for the QE variations, the F110W
and F160W flat field images were drizzled in exactly
the same way as the UDF images, utilizing identical masks.  Note that the flat
field images are the multiplicative flats used in the normal image reductions.
As such they are high where the signal is low and vice versa. All subsequent
post drizzle procedures that were applied to the science images were also
applied to the drizzled flat images. Next the median of the drizzled flat
images was set to one and multiplied by the standard deviation determined in
\S~\ref{ss-noise}, adjusted by the correlation parameter of 1.8. These images
were then added together as the square root of the sum of the squares to
form the rms image for the detection image supplied to SE.  This rms image
properly represents the differences in QE across the detector and the
mapping of the differences onto the final science image.  The individual
F110W and F160W rms images were retained for use in the source extraction
described below.  The ACS rms images were assumed to be uniform and equal to
the standard deviations found in \S~\ref{ss-noise} for the individual ACS
images.  The individual filter rms images form the basis of the magnitude
and flux errors returned by SE.

\subsubsection{RMS Image Adjustments} \label{sss-ria}

Visual inspection of the detection image and the individual NICMOS drizzled images
revealed small areas where there were clearly higher regions of noise or residual
spurious artifacts.  These are usually regions of ``cross hatched'' noise or small
irregular regions of a few pixels with boundaries too sharp to be real sources.
Even though areas such as these were masked in the original images, the drizzle
process can produce additional areas due to rebinning process. Rather than
removing these regions from the images, the rms images were adjusted to guarantee
that they were not used in the source extraction.  The pixel regions with
adjusted rms values are given in a table supplied with the version 2 submission.
These regions can also be identified in the rms images themselves where they
have been set to 9.999. This procedure preserves the ignored areas
in the images so that they can be evaluated by other researchers
if they wish, just as the individual images, before masking, can
be retrieved from the archive.  Areas outside of the observed regions
were set to very high rms values on the order of 500. to 800.

\subsection{Extraction parameters}

SE's source extraction process is controlled by a configuration file that
gives the parameters for source extraction.  Some of the configuration
parameters used in the version 2.0 treasury source extraction are given in
Table~\ref{tb-separ}. The full configuration files used in the extraction
are included in the Treasury NICMOS UDF version 2.0 submission to MAST.
The parameters include a detection threshold of $1.4 \sigma$ and the
minimum number of contiguous pixels for a true source set to 7.  Note
that these parameters discriminate against faint point sources.

Although not evident from the documentation, SE runs in a dual rms image
mode.  In this mode two rms images are supplied in the WEIGHT\_IMAGE
parameter.  The first image is the rms image for the detection image and
the second is the rms image for the extraction image which is the UDF image
in each of the individual filters. The second rms image does not influence
the source selection but determines the error values returned by SE.

The photometric zero points in AB magnitude are 23.41 (F110W) and 23.22 (F160W).
The extraction parameters were adjusted to produce a clean extraction of sources
with a goal of no erroneous detections in the high signal to noise regions of the image.
This produces a relatively conservative catalog given the range of weighting
over the image. Visual inspection of the image indicates
that there are real sources that have been missed by the extraction process.  More
aggressive extraction parameters pick up these sources but also begin to find sources
of doubtful reality. (See \S~\ref{s-rel}.) Users who wish to have a more aggressive
extraction can use our parameters as a starting point and adjust them to produce the
required level of extraction.  Our parameters produced 1293 extracted sources.

\section{Catalog Construction}

All of the output values listed in the treasury catalog are outputs
from SE with no editing.  The source order has been rearranged to be
in order of increasing right ascension.  To maintain correspondence
with the segmentation images that were returned by SE, the original
source identification numbers assigned by SE are given in the catalog.
Ten of the sources detected by SE are not included in the catalog as
described in \S~\ref{ss-acs} leaving 1283 of the 1293 detected sources.

Each source has 90 entries, therefore, we do not include the table
in the paper.  The catalog is available at the STScI MAST site containing
the NICMOS version 2.0 high level science products.  That catalog is a
comma separated text file.  Columns 1-2 contain the ID number and the
ID number of the associated source in the version 1
I band based ACS UDF catalog.  The associated ACS source is the closest source
to the catalog source.  If there is no ACS source within 0.3 seconds of the
NICMOS source a 0 entry is made in column 2.  Column 3 gives the
distance to the associated source in arc seconds and column 4 gives
ID number of the source in the SE produced segmentation image which is
also provided in the MAST archive.  If a version 2 catalog of ACS sources
is produced we will attempt to provide a version 2.1 catalog
with the new ACS source identifications included.

Columns 5 and 6 give the x and y positions in pixels of the source in
the version 2.0 treasury image. Columns 7 and 8 are the RA and DEC
positions in degrees while columns 9 and 10 are the RA and DEC position
in traditional nomenclature. Columns 11-28 give the aperture AB magnitudes
of the source.  The 3 aperture magnitudes of the ACS F445W band are listed
first followed by the remaining ACS and NICMOS bands in order of wavelength.
Columns 29 through 34 list the isophotal magnitudes and columns 35 through
40 list auto magnitudes returned by SE in the same order.

Column 41 lists the number of pixels associated with the source in the SE
segmentation image.  Columns 42 through 47 list the FWHM in each band. Column 48
lists the position angle of the source returned by SE. Column 49 lists the
flag value returned by SE. No sources have been removed from the
catalog on the basis of the value of the SE error flag. Columns 50-55
list the XPEAK, YPEAK, XMIN, YMIN, XMAX,and YMAX values returned by SE.
The source is contained in a box defined by the minimum and maximum x and y
values.  Columns 56 and 57 give the ellipticity and elongation of the source
returned by SE. Column 58 contains the $0.6\arcsec$ diameter aperture AB
magnitude of the F160W band.

Columns 59-76 contain the aperture fluxes in the same order as the
aperture magnitudes. The fluxes are in ADU/sec.  The NICMOS gain is 6.5
electrons per ADU. Columns 77 through 82 list the isophotal fluxes and
columns 83 through 88 list auto fluxes returned by SE.  Columns 89 and
90 are the ISOAREA and ISOFAREA values returned by SE.

\subsection{Mini-Catalog} \label{ss-mc}

To be consistent with the ACS UDF submissions we have also constructed a
mini-catalog of the sources, part of which is included in the printed version
of the paper.  The whole catalog is available in the electronic version of
the paper.  The catalog appears in Table~\ref{tab-cat}.  There are some
differences relative to the ACS catalog available in MAST.  First the catalog is
ordered in RA with the associated ACS source ID and the segmentation ID in
columns 2 and 3.  The x and y positions followed by the RA and DEC in degrees
are in columns 4-7. Next are the position angle, ellipticity, half radius, FWHM
and stellarity in columns 8-12.  These are followed by the isophotal
magnitude,isophotal magnitude error, and signal to noise for the 4 ACS
and 2 NICMOS bands starting with the ACS F435W and ending with the NICMOS
F160W band.  The signal to noise is the ratio of the isophotoal flux to the
isophotal flux error returned by SE. The last entry in the table is the
value of the error flag returned by SE.  As in the larger table there has
been no effort to remove sources based on the SE error flag.  Due to space
constraints only the first few columns of the table are present in the
printed version.

\section{Source Reliability} \label{s-rel}

Although the extraction parameters were adjusted conservatively,
independent assessments of the source reliability are required.  The
following analyses and tests were performed to judge the reality of
the catalog sources.

\subsection{Signal to Noise Values} \label{ss-snv}

The source extraction program, SE, returns flux errors as well as fluxes.
Figure~\ref{fig-snv} shows the measured signal to noise values for the
faint end of the catalog.  The ratio of the isophotal flux to isophotal
flux error is ploted versus isophotal magnitude.  There is significant
scatter in the values as expected.  The average magnitude for a signal
to noise ratio of 5 appears to be around an isophotal magnitude of
28.4 significantly fainter than the aperture test value of 27.7 found in
\S~\ref{ss-noise}.  The details of how SE computes its flux errors
are not immediately obvious so the value of 27.7 will be used.  The
rms images supplied to SE were multiplied by 1.8 for the expected
correlation due to drizzling so that should not be an explanation
for the difference.

\subsection{Negative Image}

As a check on noise induced sources we ran the identical extraction procedure
on the negative of the original source detection image.  The procedure produced
no detections from the negative image. This indicates that the number
of sources produced by noise is very low.

\subsection{Comparison with the ACS images} \label{ss-acs}

The presence of the much higher signal to noise ACS images provided a
second test of source reliability.  We checked for catalog sources that
had ACS F850LP $0.6\arcsec$ aperture diameter AB magnitudes fainter than 29.5.
The smallest aperture was chosen to minimize flux from overlapping sources.
We identified 22 sources out of the total 1293 sources that matched that
criterion.  Two of these sources are in the high redshift source list
of 5 sources described by \citet{bou04} where the Lyman break occurs
to the red of the ACS cutoff. \citet{bou04} used a more aggressive source
extraction which accounts for the extra three sources in their analysis.
The remaining 20 sources fell into 3 categories.  The first were legitimate
sources with ACS F850LP flux below the limit but clearly there under
visual inspection. There are 10 sources in this category.  The second
category is sources with clear flux in only the F160W band.  There are
2 sources in this category. The remaining 8 were sources that appear to be
noise artifacts by a subjective visual analysis. The 10 objects in the
last two categories do not appear in the catalog even though the 2 sources
with only F160W flux may be real.

\subsection{Comparison with an Independently Generated Image} \label{ss-igi}

The NICMOS UDF images were independently reduced at STScI by
Massimo Stiavelli, Bahram Mobasher and Louis Bergeron.  They very
graciously provided these images for comparison with our reductions.
Inspection of these images revealed two objects in our images
that were the result of cosmic ray persistence (See \S~\ref{sss-crp}).
These objects were masked out in the individual image they appeared in
for the final drizzle run. One NICMOS object that does not have an ACS
counterpart, object 937, \citet{bou04} UDF 818-886, does not appear
in the Stiavelli, Mobasher and Bergeron image. Inspection of our
individual images indicates that no single image contributed the
majority of the flux as would be expected for a cosmic ray persistence
event.  The object appears faintly in several of our individual
images in both filters.  To date we have not been able to resolve
why this discrepancy exists.  Users of the catalog should
be aware of this discrepancy, particularly because this source
satisfies the criteria for a galaxy at a redshift greater than 7.

\section{Conclusions}

Although this is a description of the data and techniques utilized in
constructing the NICMOS UDF Treasury Version 2.0 catalog, it has been
traditional (\citet{wil96}, \citet{thm99}) to show a number magnitude
diagram from the data. Figure~\ref{fig-mag} displays the number magnitude
diagram in AB magnitudes for the NICMOS F160W sources in the Ultra Deep Field.
The vertical error bars are calculated from number statistics only.
Other errors such as incompleteness, source noise, and large scale structure
are not included.  The fall off at AB magnitudes greater than 27 is
certainly due to incompleteness, partially due to the conservative source
extraction parameters used in the construction of the Treasury catalog.
Note that the magnitudes are aperture magnitudes in the smallest, $0.6\arcsec$,
aperture.  For comparison the F814W data from the NHDF \citep{wil96} are
also plotted.  The agreement is good, with the F160W plot possibly having
a slightly steeper slope, opposite to what was observed in the NHDF
\citep{thm03}.

\section{Acknowledgments}

We are extremely grateful to Massimo Stiavelli, Bahram Mobasher and Louis
Bergeron for pointing out objects in our reduction that did not appear in
their independent reduction of the same data and for providing one of us
(RIT) with the images for detailed comparison. We are grateful to all of
the personnel at STScI, and in particular Beth Perriello, who worked very
hard to make the NICMOS UDF observations a success. This task was made even
more difficult by the NCS safing that delayed the beginning of the
observations. This article is based on data from observations with the
NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science
Institute, which is operated by the Association of Universities for Research
in Astronomy under NASA contract NAS 5-26555.  The individual researchers are
funded in part by NASA Grant HST-GO-09803.01-A-G from the Space Telescope
Science Institute. ST received support from the Danish Natural Research
Council.

redpajama_set_name: RedPajamaArXiv


HEADHUNTERS SAYS The Quasimodo Pheasantail nymph is a perennial favorite on the Missouri. A traditional Flashback PT, but tied on the super-strong Tiemco 2488H curved nymph hook. We use this everywhere, and hang it off the back of a dry as well as dredging deep. This is a very popular fly on rivers with large strong trout, and a favorite among our "Land of the Giants" guides.


text:
Department of Agriculture will spray for gypsy moths this spring
Kitsap-Unknown
By CHARLEE GLOCK-JACKSON
FOR GIG HARBOR LIFE
Every summer the Washington State Department of Agriculture (WSDA) sets out 20,000 bright green traps to learn if there are any gypsy moths anywhere in the state.
Last summer they found 42 gypsy moths in different parts of the state, up from 27 found in 2014.
Ten of those were Asian gypsy moths, including one Asian gypsy moth found in Gig Harbor.
No Asian gypsy moths had been found in Washington since 1999 and because the Asian variety is an extremely dangerous pest that can decimate plants of all kinds, WSDA will conduct a three-phase eradication program in Gig Harbor this spring.
On Feb. 17, WSDA hosted an open house at the civic center to educate Gig Harbor residents and answer questions.
According to WSDA Pest Program Manager Jim Mara, the agency will make three aerial sprayings of Btk (Bacillus thuringiensis kurstaki), probably between mid-April to early May, over a square-mile area of Gig Harbor.
"The exact spraying time depends on the weather and also on the life-cycle of the moth," Mara said. "We want to spray as soon as the larvae start to emerge, which is usually around mid-April."
WSDA will spray every four or five days, three times in all. "We usually spray at first light, and we need a 24-hour window of no rain," he said.
Btk is a naturally occurring bacterial pathogen found in soils and on plants throughout the world. It's used to eradicate many pests, including the gypsy moth.
"We've found that it's the most effective biological treatment," said Rian Wojahn, WSDA eradication and survey coordinator.
Numerous studies have shown that Btk presents a very low risk to human health and will not harm beneficial insects such as bees, ladybugs, ants or parasitic wasps.
"It's also not harmful to animals, birds or fish," Mara said. "It has a good safety record, but we do suggest that people stay inside and keep their pets inside when the spraying is taking place."
Also, he added, there will be no spraying in areas where kids are present such as schools or parks.
Currently, there are no permanent populations of Asian gypsy moths in the state and WSDA wants to keep it that way.
One reason the Asian gypsy moth is so dangerous is that — unlike the European species — Asian female moths can fly, so they can lay their eggs anywhere.
"The female Asian gypsy moths have a great flight capability. If we didn't monitor and spray wherever we find these moths and they became established in Washington, there would likely be hundreds of thousands of acres of defoliation.
"And we would have to quarantine every nursery, tree farm and Christmas tree farm in the state."
For some reason Washington — especially western Washington — seems to be an ideal place for gypsy moths, even more "active" that California.
That may be because Washington has a dozen major ports with ships coming from all over the world, Mara said.
Last year WSDA found a number of egg clusters on ships, including a cluster on a ship from Russia tied up at the Port of Vancouver. They also found four clusters on ships at the Port of Tacoma.
It's also likely that people who visit or move to Washington unknowingly bring egg masses on their vehicles, furniture and other belongings, he added.
According to Wojan, the eradication and survey coordinator, Asian and European gypsy moths look so similar that DNA tests must be used to identify each species.
WSDA has set up a website where Gig Harbor residents can learn more about gypsy moths and download a map showing the specific area where spraying will occur. The department's spray schedule also will be posted and residents can sign up for notifications.
"Just type in your address and you'll see the schedule," Mara said. "A couple of weeks before the spraying starts, we'll announce the dates. And we'll also send out reminders."
Residents can sign up to receive notifications by text, email or phone. And WSDA also will notify city officials well in advance when spraying is planned.
WSDA will continue to set out traps every summer, and if no gypsy moths are found for three consecutive years, the eradication program will be considered a success.
For information, visit agr.wa.gov/gypsymoth.

redpajama_set_name: RedPajamaCommonCrawl


text:
'use strict';

const userConfig = require('./userConfig');
const store = userConfig.store;

// This module handles all request filtering
module.exports = function RequestFilter(session) {
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	const filter = {
		// TODO: Use getURL() or similar here instead?
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			'https://*.facebook.com/*',
			'https://*.messenger.com/*',
		],
	};

	session.defaultSession.webRequest.onBeforeSendHeaders(filter, (details, callback) => {
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			cancel = store.get(userConfig.PRIVACY_BLOCK_TYPING_INDICATOR, false);
		} else if (details.url.includes('change_read_status.php')) {
			cancel = store.get(userConfig.PRIVACY_BLOCK_SEEN_INDICATOR, false);
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	return {
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			retinaCookie = cookieValue;
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};

redpajama_set_name: RedPajamaGithub


Thank you for submitting an application to study on the Six-Month Course. This course runs in small cohorts so it is important that you secure your place as soon as possible. Once we received your application form, we will be in touch.


text:
Work on track at the new South Shore school Armfield Academy
The main high school building at Armfield Academy, in Lytham Road, South Shore.
Gazette Reporter
Published: 14:28 Friday 12 April 2019
What's happening?
Paving and landscaping work is going on outside the main high school building at the Armfield Academy, in Lytham Road, South Shore. The old Arnold school, which caters for both primary and secondary aged children, opened in September after a major overhaul, but building work there continues. Inside the main high school building, decorators have just started on the second floor and will be busy keeping ahead of carpet fitters who are due in next week. In turn, they will be keeping ahead of furniture suppliers who start their installations towards the end of April. The heating is now fully on and lighting well progressed, while specialist science laboratory benches have been installed and connected to power, gas, and water.
Is work on track?
Bosses at the Fylde Coast Academy Trust (FCAT), which runs Armfield and a number of Fylde coast schools, say it is. Named after the late Blackpool FC legend Jimmy Armfield, the school opened for year seven pupils and reception youngsters in September, and will continue to take 160 year sevens and 60 reception children each year – which means the school will be at full capacity by 2022. Armfield's nursery opened just after Christmas.
John Topping, FCAT's estates and community relations boss, said: "We are extremely pleased with the superb progress being made by our main contractor Conlons, and can see daily advancements in this facet of our new Armfield Academy."
Mr Topping said FCAT's central services team has moved into the refurbished former bursary building, and added: "It is such an advantage to have our key staff within HR, finance, governance, health and safety, data and IT, and estates and community relations all together."
Row over whether Lancashire families in poverty need "education in how to manage money"


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text:
Anthony Hamilton Almost Makes It Onto Another Classic Remake
As you probably know by now, Charlotte native Anthony Hamilton was among the group of 80 star musicians who assembled a couple of weeks ago to record "We Are The World: 25 For Haiti," a remake of the original 1985 classic that was led by Michael Jackson, Lionel Richie, and Quincy Jones. Well, another legendary Jones tune has been remade for Jones's upcoming album. Jermaine Dupri has produced a remake of "The Secret Garden," which when originally released in 1989 featured James Ingram, Al B. Sure, El DeBarge, and Barry White.
As Dupri explains in this MTV News video clip below, the new version, which hasn't been released yet, features Usher, Robin Thicke, Tyrese, Trey Songz, and White's original verse. Said Dupri, "It was hard because I wanted to put Anthony Hamilton on there, I wanted to put Maxwell...but it's only a four or five-guy spot."
Anthony Hamilton , Entertainment , Music , News
See Nelly This Afternoon
Another Side of CIAA Week
Celebrities in Charlotte for CIAA Week
Events for CIAA Week: February 22-28
Anthony Hamilton Almost Makes It Onto Another Clas...
KokoMo's Opens at JCSU
Today I Ate the Best Burger Ever
Local Ties on Olympic Ice
When It's a Great Idea to Pay Someone to Go Out wi...
Gerald Wallace Will Finish 2nd in Slam Dunk Contest
Public Photo Shoot Project Feb. 21
Brooklyn Decker Is the 2010 Sports Illustrated Swi...
5 Reasons Why We're Better Off with Michael Jordan...
Brooklyn's in the House
Fantasia Debuts 'Even Angels' Today, Appears on 'O...
The List: 2010 CIAA Events and Parties
You Can Still Treat Your Boo: Charlotte Restaurant...
I Didn't Know Rielle Hunter Lives in Charlotte


text:
NCAA ice hockey men's championships title wins 2019
Published by Christina Gough, Jun 18, 2020
The Frozen Four is a men's ice hockey championship which is the culmination of the college hockey season. The team from Michigan has won a record nine Frozen Four titles as of 2019.
Number of NCAA Frozen Four championship titles won as of 2019, by team
Records since 1992 do not include games against Canadian teams.
College Sports (NCAA)
NCAA Division I conferences and member institutions revenue distribution 2010-2020
National Collegiate Athletic Association (NCAA) expenses by segment 2012-2019
National Collegiate Athletic Association (NCAA) revenue by segment 2012-2019
NCAA television and licensing rights revenue 2011-2024
Christina Gough
Research expert covering sports and video gaming
Statistics on "NCAA college sports"
Portion of NCAA executives in the U.S. 2009-2019, by gender
NCAA athletic departments directors in 2018, by gender
NCAA purpose in the U.S. 2019
State of the NCAA system in the U.S. 2019
Number of student athletes in the United States in 2018, by gender
NCAA male athletes in the U.S. 2010-2019, by ethnicity
Share of NCAA female athletes in the U.S. 2010-2019, by ethnicity
Colleg enrollment duration of NCAA student athletes in the U.S. 2019
Student loans of NCAA student athletes in the U.S. 2019
Number of college scholarships by sport and gender 2020
Public opinion on paying student athletes in the U.S. 2019
Public interest in college football in the U.S. 2020
Attendance at Division I, II & III college football games 2003-2019
Average ticket price for college football games by conference 2020
Biggest college football stadiums by capacity in the U.S. 2019
NCAA college football TV ratings and viewership 2018
Most watched college football kickoff weekend games 2019
Respondents who prefer watching college football to NFL on TV in the U.S. 2020
Highest paid coaches in NCAA football 2019
Public interest in college men's basketball in the U.S. 2020
Public interest in college women's basketball in the U.S. 2020
NCAA division I men's basketball attendance leaders 2020
Highest paid coaches in NCAA basketball 2019
Attendance at NCAA basketball tournament games 2000-2018
NCAA basketball March Madness average TV viewership 2019
College basketball - TV ratings of NCAA national championship games 2019
Leading TV advertising categories during the NCAA championship 2019
Leading TV advertisers during the NCAA championship 2019
TV advertising spending during March Madness 2015-2019
College basketball - NCAA tournament appearances 1939-2019
NCAA men's basketball final four appearances by team 1999-2019
College hockey - Frozen Four appearances 1948 - 2019
College hockey - Frozen Four wins 1948 - 2019
Number of the NCAA men's Frozen Four games viewers in the U.S. 2009-2018
COVID-19: public opinion on playing college sports 2020
COVID-19: public opinion in the U.S. on delaying the NFL season 2020
COVID-19: public opinion on when live sports will restart as of April 2020
COVID-19: potential revenue loss from NCAA events 2020
COVID-19: potential revenue loss for March Madness 2020
COVID-19: potential media rights revenue loss per school for March Madness 2020
COVID-19: potential revenue loss per college for March Madness 2020
Most free throws in a March Madness game as of 2020
Most points scored in March Madness as of 2020
NCAA college basketball tournament revenue from ticket sales 2013
Most points scored in a single March Madness tournament as of 2020
Public interest in college women's basketball in the U.S. 2020, by age
Public interest in college women's basketball in the U.S. 2020, by gender
Public interest in college men's basketball in the U.S. 2020, by ethnicity
Highest paid sports coaches in the U.S. 2019
Public interest in college men's basketball in the U.S. 2020, by age
Money spent on NCAA championships travel by membership division 2011/12
Distribution of coaches for female NCAA teams 2018, by gender
Public interest in college men's basketball in the U.S. 2020, by gender
Number of college sports scholarships available by gender 2019
Most assists in a single March Madness game as of 2020
NCAA college basketball tournament average ticket price 2013
Internet households in Canada 2010-2025
Hospital bed count in MENA 2020, by country
Gini index forecast in Tanzania 2010-2025
Alcohol & tobacco consumer spending forecast in Western Africa 2010-2025
Healthcare consumer spending per capita forecast in Morocco 2010-2025
College Sports (NCAA) Sporting Goods Industry in the U.S. National Football League (NFL) National Basketball Association (NBA) Major League Baseball (MLB)
National Collegiate Athletic Association. (July 9, 2019). Number of NCAA Frozen Four championship titles won as of 2019, by team [Graph]. In Statista. Retrieved January 17, 2021, from https://www.statista.com/statistics/1096485/frozen-four-title-wins/
National Collegiate Athletic Association. "Number of NCAA Frozen Four championship titles won as of 2019, by team." Chart. July 9, 2019. Statista. Accessed January 17, 2021. https://www.statista.com/statistics/1096485/frozen-four-title-wins/
National Collegiate Athletic Association. (2019). Number of NCAA Frozen Four championship titles won as of 2019, by team. Statista. Statista Inc.. Accessed: January 17, 2021. https://www.statista.com/statistics/1096485/frozen-four-title-wins/
National Collegiate Athletic Association. "Number of Ncaa Frozen Four Championship Titles Won as of 2019, by Team." Statista, Statista Inc., 9 Jul 2019, https://www.statista.com/statistics/1096485/frozen-four-title-wins/
National Collegiate Athletic Association, Number of NCAA Frozen Four championship titles won as of 2019, by team Statista, https://www.statista.com/statistics/1096485/frozen-four-title-wins/ (last visited January 17, 2021)


After two consecutive weak fundraising quarters, embattled California Rep. Duncan Hunter finally posted a fundraising quarter in which he raised more than he spent.
The Republican has been dogged by a federal criminal investigation about spending campaign finance cash for personal use.
The investigation led him to spend more on legal feesthan he raised for the past two fundraising quarters.
But Hunter raised $210,268 for the first quarter of 2018 while spending $191,678, according to Rob Pyers, who runs California Target Book.
Still, Pyers noted that Hunter has spent 90 percent of all of his campaign cash on legal fees, for a total of $614,492.
Hunter also outraised his Democratic challengers.
Former Obama administration official Ammar Campa-Najjar raised a total of $205,242.99, while retired Navy SEAL Josh Butner raised $176,226.58 between Jan. 1 and March 31 of this year.
Hunter's perceived weakness has caused the contest between Campa-Najjar and Butner to turn ugly.
Butner saying Campa-Najjar was involved with a website that tied Butner's father to the Ku Klux Klan.
Campa-Najjar said Butner's campaign was behind a new story tying Campa-Najjar to his grandfather, who was a terrorist but died before Campa-Najjar was born.
Inside Elections with Nathan L. Gonzales still rates California's 50th District as Likely Republican.
Correction, April 16, 2018, 12:28 p.m. | A previous version of this story misstated Butner's fundraising total.


text:
UFOs over Peterborough, UK - October 25, 2014
UFO over Chile - October 24, 2014
UFO over Nashville, TN, USA - October 24, 2014
UFO over Italy - October 23, 2014
Breaking News! UFO fleet during a solar eclipse, Tijuana, Mexico - October 23, 2014
UFO over Sakurajima Volcano, Japan - October 22, 2014
Cigar Shaped UFO Appears In Lightening Storm On Car Dash Camera Footage October 2014
2 UFOs near ISS - October 21, 2014
UFO over Paris, France - October 21, 2014
UFO in Sky USA - October 19, 2014
UFO near ISS - October 19, 2014
UFO over Sydney, Australia - October 18, 2014
UFO over Moscow, Russia - October 16, 2014
UFO over Mexico - October 16, 2014
Huge UFO over Midlothian Scotland - October 16, 2014
UFOs Sighted At The Grand Canyon Area - October 15, 2014
A giant water monster! October 15, 2014
Massive UFO sightings over Popocatepetl Volcano. Large disc shape UFO - October 15, 2014
UFO Fleet Over Armenia - October 13, 2014
Cross Slabs Caught By Opportunity NASA 2014
▼ Oct 19 - Oct 26 (22)
Breaking News! UFO fleet during a solar eclipse, T...
UFO over Sakurajima Volcano, Japan - October 22, 2...
Cigar Shaped UFO Appears In Lightening Storm On Ca...
Huge UFO over Midlothian Scotland - October 16, 20...
UFOs Sighted At The Grand Canyon Area - October 15...
Massive UFO sightings over Popocatepetl Volcano. L...


text:
package hr.vsite.hive.services.javafx;

import javax.inject.Singleton;

import org.slf4j.Logger;
import org.slf4j.LoggerFactory;

import hr.vsite.hive.services.AbstractService;

import javafx.application.Application;
import javafx.application.Platform;

@Singleton
public class JavaFxService extends AbstractService {

	public static final String Key = "javafx";

	public JavaFxService() {
		super(Key);
	}

	@Override
	public void doInit() throws Exception {

		Platform.setImplicitExit(false);

		appThread = new Thread(new Runnable() {
			@Override
			public void run() {
				Application.launch(FxApplication.class);
			}
		});

		log.info("JavaFX service initialized");

	}

	@Override
	public void doStart() throws Exception {
		appThread.start();
		log.info("JavaFX service started");
	}

	@Override
	public void doStop() {
		Platform.exit();
		log.info("JavaFX service stopped");
	}

	@Override
	public void doDestroy() {
		log.info("JavaFX service destroyed");
	}

	private static final Logger log = LoggerFactory.getLogger(JavaFxService.class);

	private Thread appThread = null;

}


text:
Q: React-Native and ListView inside ScrollView I have to show a series of vertical ListView, and the user should navigate horizontally between them.
The horizontal scroll must be performed only for some events, like the touch of a button.
The vertical one of the ListViews must be completely droved by user's gestures.
I tried to obtain this effect configuring a ScrollView as horizontal and putting inside it the ListViews, but I found out that the vertical scroll results completely disabled.
How can I obtain the desired behavior?
Is there a ScrollView or ListView option I don't know about?
Should I change all the layout's structure?
Thank you.

A: Comes out that a vertical ListView (or ScrollView) inside an horizontal ScrollView will never work, until you set a value for the height (ex height: 400).
Hope this could help somebody else.

redpajama_set_name: RedPajamaStackExchange


text:
February 15, 2014 January 20, 2016 by Tim Marston
Many people still use electric fans instead of, and in addition to, their central air conditioning.
Some, simply, because there are financial and location restrictions on installing the A/C unit and others because they love the look of the newer fans. Today, electric fans are more fashion statements than anything else. Historically, they served a function and much needed purpose. Now, however, many designers integrate fans into the décor to make the area more appealing and to give the space more depth. Regardless of your reason for purchasing an electric fan, there is, no doubt, plenty of selection and a variety of manufacturers from which to choose. As a result, I have compiled a list of the top seven manufacturers of electric fans.
Of course, one of the oldest companies is General Electric. The original brass fan from more than one-hundred years ago is still being found at garage sales and in private collections. Although they had simple designs, they are now highly-sought after, as they look gorgeous with the written scroll GE lettering on the front. With three speeds and an oscillator, restored models have gone for as high as $500 on auction. Today, the company has a wide selection of ceiling fans, floor fans, reversible window fans, box fans and oscillating fans. Prices range from about $15 upwards to $1000 depending on what you are looking for.
Another mainstay in electric fan companies is Westinghouse. Because the manufacturer is so old, they too, have various fans that are considered antique and quite coveted because of their age and quality. The company's older fans are so popular that they have even replicated the originals for today's market. Although the originals, in good restored condition, fetch a nice price, the newer electric fans in the art deco genre are selling at around $400-$500 brand new.
Dating back to the same era, the original Hunter Fan Company was the first to produce a water-driven fan which was known the world over. Many people nowadays know the name for ceiling fans, but they still manufacture desk fans, pedestal fans, and exhaust fans. They continue to innovate and now offer the "Five Minute Ceiling Fan", the "Concert Breeze", the fan with an audio system, as well as a selection of portable collector fans in metal and fancy fans to match the bathroom. The brand is also popular for both its air purifiers and air conditioners.
The fourth electric fan manufacturer that comes to mind is Emerson, also boasting over a hundred years in business. The company was built upon reliability and quality and they seem to maintain the same standards today. Although the initial focus of the company was switching equipment for the railways, they quickly devised and patented a technology for a brush-type fan motor. This lead to the success of the desk fan, as it was somewhat portable and the average person could afford the unit. In the beginning, the company mandate was to further advance the performance, and of course, build the best in quality, but today, they also strive to make decorative and sharp-looking fans for the home and office.
With over fifty years of experience, Seabreeze Electric Corporation has been making portable electric fans that far exceed government safety regulations. For example, they produced the first "childproof" pulse action cooling fan named the "Cool Sweep™" for the North American market. Their "Turbo-Aire™" brand is synonymous with quality and durability.
Most people know Honeywell for their thermostats. But, they also produce floor fans, tower fans, stand fans, oscillating table fans, and multi-speed TurboForce® fans. While their electric fans are considered top quality, their prices are inexpensive ranging from $20-$60. Several have the removable grill for convenient cleaning and they can also be wall-mounted so that they are out of the way to save space. Finally, the company is known for manufacturing fans that are quiet, as found in the QuietSet™ technology in addition to being energy efficient.
In recent years, about forty years ago, a startup in Taiwan, called Air Monster®, began exporting its pedestal fans, high velocity metal fans, and table fans to the West. While the manufacturing plant is in Hong Kong, they now have an office in Los Angeles, CA.
Lastly, it is normal practice for companies to brand one name, but the parts are actually made from another manufacturer. So, you may see other fans in the marketplace that have lesser known names, but if you read the specifications, you will find that the patented pieces or the crucial parts are made from the best electric fan manufacturers.
Posted in: Uncategorized	|
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One thought on "The top manufacturers of electric fans"
Ramesh solanki says:
I want kids range ceiling fan's in bulk quantityof my brand name at a nominal price for resale.


Big attrition is not a good thing in any kind of job. In knowledge worker jobs attrition is very significant in the total cost of doing business. Most of the time though we can't really put a dollar figure on it. Let's say 1 out of 4 employee leave a team through out the year, and the ramp up for a job to get to the avg level of the team is 6months(50% of productivity of avg team member, so 3months of non productivity), on a team of 8 people. So conservatively for one person leaving 1.5month since less productive, replace the person (most likely a ghost - no time wasted), 3months no real consistent output, mentor time over the next 6months, 1.5month through out. The ideal output of the team with no attrition is 8people * 12months = 96man/months, with an attrition of 25%, a team loose at a minimum 12man/months or 2 * (1.5+3+1.5). And there is also the fact that the overall knowledge, or avg of the team will be trending down. More junior staff is less depth in the understanding of the system, so less productivity. So next time it's time to calculate the cost of the offshore team don't forget to add your attrition figure for 25% attrition rate, it is a minimum of additional 12.5% to the hourly rate. The best is to get into turn key solutions (project outsourcing) or have good performance indicators to monitor closely to have good leverage with the vendors.
There are so many different ways to bring up your kids! On my opinion, the first rule is spend with your child as much time as you can. resume writing service here can also help to find a good job!


text:
lisa lee curtis
"It's scary. Do it anyway."
Yes, Virginia, the rules have changed…
May 6, 2019 May 6, 2019 / L.L. Curtis
I remember the first time I was outraged by gender inequality. I mean legitimately outraged. It was 1996 and I found out that a male counterpart of mine was being paid a significant amount more than I, and I was completely shocked. How could this happen? How could this be permitted? Why was I being dismissed by my boss when I brought this obvious mistake to his attention? He was more concerned with how I found out than the fact that I was working my ass off and getting paid a fraction of my worth.
It was a slap in the face. I felt betrayed, and I remember thinking, twenty-three years ago, "It's 1996 for godssake."
It may have been the first time I acknowledged feeling betrayed or let down due to gender equality, but it was hardly the first time I felt that sting, that punch in the gut when, due to the fact that I was born the less "worthy" gender, I would be dismissed, laughed at, or violated with a slim chance at vindication.
It was my lot, you see. It was all of our lots, women who were "permitted" to receive an education, women who were now "allowed" in the workplace, taking jobs that were, in many people's minds, rightfully men's. "That's just how it is," I would hear. "You don't see me complaining about it," she would reply. "Boys will be boys," they would say with a knowing nod. "Don't make a fuss, no one likes a troublemaker, you should feel lucky you're even here, because back in my day…"
Keep your mouth shut. Don't be difficult.
But don't be easy.
Don't "give it up" to men. Don't show too much skin, you don't want people to think you're "loose." That's how you get a reputation, and then no one will want to date you, to marry you.
But don't be a prude. For crying out loud, don't be a prude. You should feel flattered when men pay attention to you. Yes, I know he's touchy feely, but it's not hurting anyone, don't make a fuss. They'll think you're frigid.
Women spend a lot of time during our childhoods fielding these mixed messages, all the while receiving loud and clear the most important one: Women are lesser. It took many years before I even batted an eye at comments like, "Ugh, don't be such a girl, don't act like a woman," always said with mocking and/or venom. No one wanted to be told they do ANYTHING like a girl, even girls. "I do not," I'd say. I'd show them that I wasn't inferior.
"You should feel lucky," I was told, " because in some countries, they only allow you to have two children so people kept the boys." It was shameful to have girls which seemed so strange to me since I knew that you NEEDED to have girls to carry on giving BIRTH to girls. "What happened to the girl babies?" I would ask, only to be told that we were disposable, that the girls were often killed immediately or, if lucky, abandoned, which often meant they were left to die.
I'd hear about men we knew who were ridiculed for only being able to make girl babies, as if that somehow detracted to their all-important manhood…whatever that meant. Yet, at the same time the women were berated for not producing the superior male infant.
Once I hit puberty in the 1980s, I spent a lot of time in an internal war with who I was and how I was supposed to be ashamed of it. I wanted to be desirable to men like the women on television, like the older girls in my school. I knew I was supposed to present myself in a manner for men to consume, and I knew it was shameful for me to reciprocate that desire. Without being told, I knew that it was important to please a man, but that if I demanded sexual satisfaction that I would be considered greedy, unreasonable, and a slut who "got around."
When my first serious boyfriend in high school broke up with me to date another girl (who, hilariously enough, wanted nothing to do with him), I went on a movie date with a boy who had recently graduated from our school. When the boyfriend who rejected me found out, he and his friends referred to me as a "syphilis infected bitch," or SIB for short. It was all very clever. And very much meant to send the message that because I had not sat around waiting for my boyfriend to reclaim me, that I was a disease-ridden slut, and no longer desirable. Until he was gracious enough to take me back.
As a teenager, I was groped, grabbed, penetrated by eager fingers I wasn't strong enough to fend off. After being offered a ride home from a school function, kidnapped (though I wouldn't call it that at the time) by another older boy with the intention of sexual assault. I was chastised for not being mature enough for "an adult relationship" when I resisted. When I tried once or twice to tell someone what happened because I was struggling emotionally with the after effects, I was told I shouldn't have gotten into his car. What did I think was going to happen?
I was inappropriately touched by my science teacher and, when I told him to take his hands off of me, he sent me to the office for insubordination. I reported the incident, and nothing was done, nor did I expect it to be. Because that's "how it was."
It was becoming increasingly clear to me what "the rules" were and how they were applied differently to men and to women. And that it wasn't just men enabling abuse I was on the receiving end.
By the time I left high school, I was angry.
I started to notice that more men were paying attention to me, or more accurately, to my body. But what I noticed almost equally as often was the venom I was on the receiving end from women who didn't even know me. Women whose husbands worked in close proximity to me.
It was confusing for me, and I tried to be more "polite" and to dress in a manner where I would be taken seriously, both by the men I worked with and the women who hated me for existing. It didn't take long before I was told by a woman in town that I was referred to as "the shop rag," and it took me a full few minutes to understand that it was assumed that I was servicing the men I worked with because I had the audacity to exist in a reasonably attractive young woman's body.
I became angrier. It was at that point, at the age of nineteen, that I developed the attitude of, "Do the time, do the crime." I would absolutely be the bad guy I was expected to be, much to the delight of many undeserving men. I was angrier and I was making other women angrier as well as they finally had a legitimate reason to hate and distrust me.
Before my next birthday, I was raped by two men after I willingly followed the one I was dating onto his friend's fishing boat. His friend's sister-in-law heard that "some slut" pulled a train with her husband and seven other guys. This got around and even more people were angry with me for what "I had done."
By my twenties, I had had it. I hated women, and I mistrusted men. I was in the full throws of internalized misogyny, and, as a women who believed 100% that I was as worthy as men, and frustrated that I wasn't paid as much as my male counterparts, I was also someone who would say horrible things about women because I believed the hype. I didn't understand how we were pitted against each other, I was too arrogant and/or proud to realize that I had been programmed to be exactly what men wanted me to be. And that was to be someone who sought men's approval and would step on other women to get it.
I would say, as a bisexual woman, that women only served one purpose to me: sex. "What else are they good for," I would laugh. The guys, because those were the only people I would surround myself due to my hatred of other women with little exception (and I honestly thought they saw me as their equal as well. I was wrong…isn't hindsight a bitch?), would laugh and laugh, almost beside themselves with disbelief and approval.
I became a complete, patriarchal tool. Because those were the rules. I didn't make them, but I learned to play by them. I was the cool girl who wouldn't be offended by misogynistic jokes. Other women were ridiculous and hysterical to me. I certainly wasn't one of them. I wasn't "like the other girls," as I was told frequently – one friend said I was "like a dude with tits" – and I would take as the ultimate compliment.
These had always been the rules, for women anyway: Play nice, you are lesser, but if you're not a problem, we'll let you sit at the table when we're not betraying your trust and/or your body.
It might have been 1996 and my discovery that my "guy friends" were being paid more than I was and that there seemed to be nothing I could do to change this that was the catalyst for my realization that I had been duped, though I certainly took a while longer to rectify some of my embarrassingly problematic behavior. I'm not exactly sure when I stopped believing that women were inferior and that if I just behaved a certain way, I would have that seat at the table. A while back, sure, but I didn't know how to fix it, so my behavior hadn't changed all that much.
I don't know when I started to make a real effort to, rather than cast judgment towards other women and level their…excuse me, OUR best interest over a man's, to make myself available as an ally to femme bodies and souls. It was embarrassingly recent, I can assure you of that. I'm no longer too proud or arrogant to acknowledge it.
I don't remember the exact time when I stopped playing by the rules, the rules men have set and women have helped facilitate as a survival mechanism, as a move to gain leverage that barely existed. I keep seeing articles, opinion pieces, etc. where women who are still fearful of repercussions come out and make statements in defense of harmful men that make me shake my head; because their defense or rationalization is both understandable, considering how "things were" for them back then, and outright dangerous because it's minimizing what women go though and are trying to put a stop to today.
And I see rebuttals with our anguished cries of, "THIS BEHAVIOR WAS NEVER OK, THE RULES HAVE NOT CHANGED, THIS WAS ALWAYS WRONG."
Yes, Virginia, the rules have changed.
They've been slow to change, and not everyone has gotten the memo. There are people who are fighting against this change, and some of those people are women. Sadly, more often than not, it's because they were subjected to the rules and are bitter than other women might not have to go through the same pain they did. "I went through it, and I turned out just fine."
It was acceptable to be pressured into sex in order to keep your job or in order to gain one.
It was also absolutely acceptable to rape your spouse "back then" because we were our husband's property. It was acceptable and legal even though it destroyed us on some level.
It was absolutely considered "a family matter" when you were on the receiving end of child abuse or domestic violence. Those were the rules. Don't make trouble.
We were not "allowed" to do too many things that we often take for granted now until just the last few decades. We didn't have permission to own property, to have our own credit card, to terminate a pregnancy within our own bodies, to run a goddamn marathon if we wanted to.
Those. Were. The. Rules. How on earth were we going to say no to men using our bodies for their entertainment? Who was going to object when we were "so lucky" as a teenager to be desired by older, powerful men? We were expected to facilitate it and we did. That's "just how it was" then unless you wanted the shit kicked out of you or worse. We should have done better, but we couldn't or we just plain didn't.
Those were, no question, the rules then. We didn't make the rules, men did. Men made the rules, and women followed them. Men were taught that it was ok to view women's bodies as objects and that they were lesser. If we believed it, why on earth wouldn't they? The arguments were very convincing, and their were repercussions for men who didn't follow the rules as well.
We absolutely do not have to forgive the people who facilitated and followed the rules that caused us harm. I have a hard enough forgiving myself for being played so readily. My finally waking the hell up doesn't absolve me of any damaged I caused to other women any more than the resigned statement of "that's the way it was back then" will undo damage to any woman including myself
Again, the rules HAVE changed. Or at least they are showing signs of changing. It's 2019 for godssake. We are gradually, as a movement, understanding our worth, and we are realizing our strength. We are no longer being quiet, and we are speaking up for even the women who are too scared or too programmed to use their voice. We are speaking up for those women still clinging to the rules like a screwed up security blanket, and we are speaking over those who set them in the first place.
We aren't letting men – or the women they've duped – get away with the status quo anymore. We can understand, we can choose to forgive, but there are no free passes when it comes to accountability.
We are stronger together, and we're making our own rules.
← Monsters and Dirty Tupperware
Free Speech, Comedy, and Not Being a Dick →
Advice From My Mother
Look At Us Go
My Brother Is.
How Can I Call Myself A Feminist?
I Committed Welfare Fraud
Fuck hate. You are loved. Let's dance.
Seeing My Father
Tapiola and the Big-Tittied Girlfriend
In Defense of Comedy and Other Potentially Unpleasant Experiences
I Won't Pray For You
Come Out, Come Out!
Goodnight, Robin.
Hoffman, Reckless Sex, and All The Answers
Ashley Madison, Expectations of Privacy, and Other Fairytales
A Day In The Life Of An Overweight Food Addict
Bathroom Etiquette For Women
What is the age of consent?
Agoraphobia – A Haiku
3 Steps to Feeling Pretty Again After Your Rape
Woman Ends Lifetime of Fat-Shaming By Only Eating Kale While In Public
But Did You Actually SEE him?
With Liberty and Justice For ALL…Unless I Disagree.
Sherri Holmes – Where are you?


Home / gynecology / Anti-HIV NanoViricide drug candidate shows promise in animal trials NanoViricides.
THE BUSINESS also said that pet studies for its drug applicants against bird flu are due to be planned at a major United States government research facility. The company has previously reported that animal studies against Ebola will be undertaken following the success of in vitro studies. These scholarly studies are continuing. NanoViricides, Inc. Is normally using injectable nanoviricides for its initial HIV research. Future plans demand the development of a long-acting anti-HIV skin patch. The Company feels that delivery method can lead to markedly improved individual compliance.. Anti-HIV NanoViricide drug candidate shows promise in animal trials NanoViricides, Inc said that it is anti-HIV drug candidates demonstrated significant therapeutic efficacy in the recently completed preliminary pet studies.While many people ascribe a foul odor to androstenone, usually that of stale urine or solid sweat, others come across the scent pleasant and sweet. Still others cannot smell it at all. New analysis from Rockefeller University, performed in collaboration with researchers at Duke University in North Carolina, reveals for the first time that this severe variability in peopl's perception of androstenone is due in large component to genetic variants in one odorant receptor called OR7D4. The study is reported September 16 as an advance on-line publication of the journal Character.